%0 Journal Article
%T The 13th Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the SDSS-IV Survey Mapping Nearby Galaxies at Apache Point Observatory
%A Albareti, Franco D. 
%A Allende Prieto, Carlos 
%A Almeida, Andres 
%A Anders, Friedrich 
%A Anderson, Scott 
%A Andrews, Brett H. 
%A Aragón-Salamanca, Alfonso 
%A Argudo-Fernández, Maria 
%A Armengaud, Eric 
%A Aubourg, Eric 
%A Avila-Reese, Vladimir 
%A Badenes, Carles 
%A Bailey, Stephen 
%A Barbuy, Beatriz 
%A Barger, Kat 
%A Barrera-Ballesteros, Jorge 
%A Bartosz, Curtis 
%A Basu, Sarbani 
%A Bates, Dominic 
%A Battaglia, Giuseppina 
%A Baumgarten, Falk 
%A Baur, Julien 
%A Bautista, Julian 
%A Beers, Timothy C. 
%A Belfiore, Francesco 
%A Bershady, Matthew 
%A Bertran de Lis, Sara 
%A Bird, Jonathan C. 
%A Bizyaev, Dmitry 
%A Blanc, Guillermo A. 
%A Blanton, Michael 
%A Blomqvist, Michael 
%A Bolton, Adam S. 
%A Borissova, J. 
%A Bovy, Jo 
%A Nielsen Brandt, William 
%A Brinkmann, Jonathan 
%A Brownstein, Joel R. 
%A Bundy, Kevin 
%A Burtin, Etienne 
%A Busca, Nicolás G. 
%A Orlando Camacho Chavez, Hugo 
%A Cano Díaz, M. 
%A Cappellari, Michele 
%A Carrera, Ricardo 
%A Chen, Yanping 
%A Cherinka, Brian 
%A Cheung, Edmond 
%A Chiappini, Cristina 
%A Chojnowski, Drew 
%A Chuang, Chia-Hsun 
%A Chung, Haeun 
%A Cirolini, Rafael Fernando 
%A Clerc, Nicolas 
%A Cohen, Roger E. 
%A Comerford, Julia M. 
%A Comparat, Johan 
%A Correa do Nascimento, Janaina 
%A Cousinou, Marie-Claude 
%A Covey, Kevin 
%A Crane, Jeffrey D. 
%A Croft, Rupert 
%A Cunha, Katia 
%A Darling, Jeremy 
%A Davidson, James W., Jr. 
%A Dawson, Kyle 
%A Da Costa, Luiz 
%A Da Silva Ilha, Gabriele 
%A Deconto Machado, Alice 
%A Delubac, Timothée 
%A De Lee, Nathan 
%A De la Macorra, Axel 
%A De la Torre, Sylvain 
%A Diamond-Stanic, Aleksandar M. 
%A Donor, John 
%A Downes, Juan Jose 
%A Drory, Niv 
%A Du, Cheng 
%A Du Mas des Bourboux, Hélion 
%A Dwelly, Tom 
%A Ebelke, Garrett 
%A Eigenbrot, Arthur 
%A Eisenstein, Daniel J. 
%A Elsworth, Yvonne P. 
%A Emsellem, Eric 
%A Eracleous, Michael 
%A Escoffier, Stephanie 
%A Evans, Michael L. 
%A Falcón-Barroso, Jesús 
%A Fan, Xiaohui 
%A Favole, Ginevra 
%A Fernandez-Alvar, Emma 
%A Fernandez-Trincado, J. G. 
%A Feuillet, Diane 
%A Fleming, Scott W. 
%A Font-Ribera, Andreu 
%A Freischlad, Gordon 
%A Frinchaboy, Peter 
%A Fu, Hai 
%A Gao, Yang 
%A Garcia, Rafael A. 
%A Garcia-Dias, R. 
%A Garcia-Hernández, D. A. 
%A Garcia Pérez, Ana E. 
%A Gaulme, Patrick 
%A Ge, Junqiang 
%A Geisler, Douglas 
%A Gillespie, Bruce 
%A Gil Marin, Hector 
%A Girardi, Léo 
%A Goddard, Daniel 
%A Gomez Maqueo Chew, Yilen 
%A Gonzalez-Perez, Violeta 
%A Grabowski, Kathleen 
%A Green, Paul 
%A Grier, Catherine J. 
%A Grier, Thomas 
%A Guo, Hong 
%A Guy, Julien 
%A Hagen, Alex 
%A Hall, Matt 
%A Harding, Paul 
%A Harley, R. E. 
%A Hasselquist, Sten 
%A Hawley, Suzanne 
%A Hayes, Christian R. 
%A Hearty, Fred 
%A Hekker, Saskia 
%A Hernandez Toledo, Hector 
%A Ho, Shirley 
%A Hogg, David W. 
%A Holley-Bockelmann, Kelly 
%A Holtzman, Jon A. 
%A Holzer, Parker H. 
%A Hu, Jian 
%A Huber, Daniel 
%A Hutchinson, Timothy Alan 
%A Hwang, Ho Seong 
%A Ibarra-Medel, Héctor J. 
%A Ivans, Inese I. 
%A Ivory, KeShawn 
%A Jaehnig, Kurt 
%A Jensen, Trey W. 
%A Johnson, Jennifer A. 
%A Jones, Amy 
%A Jullo, Eric 
%A Kallinger, T. 
%A Kinemuchi, Karen 
%A Kirkby, David 
%A Klaene, Mark 
%A Kneib, Jean-Paul 
%A Kollmeier, Juna A. 
%A Lacerna, Ivan 
%A Lane, Richard R. 
%A Lang, Dustin 
%A Laurent, Pierre 
%A Law, David R. 
%A Leauthaud, Alexie 
%A Le Goff, Jean-Marc 
%A Li, Chen 
%A Li, Cheng 
%A Li, Niu 
%A Li, Ran 
%A Liang, Fu-Heng 
%A Liang, Yu 
%A Lima, Marcos 
%A Lin, Lihwai 
%A Lin, Lin 
%A Lin, Yen-Ting 
%A Liu, Chao 
%A Long, Dan 
%A Lucatello, Sara 
%A MacDonald, Nicholas 
%A MacLeod, Chelsea L. 
%A Mackereth, J. Ted 
%A Mahadevan, Suvrath 
%A Geimba Maia, Marcio Antonio 
%A Maiolino, Roberto 
%A Majewski, Steven R. 
%A Malanushenko, Olena 
%A Malanushenko, Viktor 
%A Dullius Mallmann, Nícolas 
%A Manchado, Arturo 
%A Maraston, Claudia 
%A Marques-Chaves, Rui 
%A Martinez Valpuesta, Inma 
%A Masters, Karen L. 
%A Mathur, Savita 
%A McGreer, Ian D. 
%A Merloni, Andrea 
%A Merrifield, Michael R. 
%A Meszáros, Szabolcs 
%A Meza, Andres 
%A Miglio, Andrea 
%A Minchev, Ivan 
%A Molaverdikhani, Karan 
%A Montero-Dorta, Antonio D. 
%A Mosser, Benoit 
%A Muna, Demitri 
%A Myers, Adam 
%A Nair, Preethi 
%A Nandra, Kirpal 
%A Ness, Melissa 
%A Newman, Jeffrey A. 
%A Nichol, Robert C. 
%A Nidever, David L. 
%A Nitschelm, Christian 
%A O’Connell, Julia 
%A Oravetz, Audrey 
%A Oravetz, Daniel J. 
%A Pace, Zachary 
%A Padilla, Nelson 
%A Palanque-Delabrouille, Nathalie 
%A Pan, Kaike 
%A Parejko, John 
%A Paris, Isabelle 
%A Park, Changbom 
%A Peacock, John A. 
%A Peirani, Sebastien 
%A Pellejero-Ibanez, Marcos 
%A Penny, Samantha 
%A Percival, Will J. 
%A Percival, Jeffrey W. 
%A Perez-Fournon, Ismael 
%A Petitjean, Patrick 
%A Pieri, Matthew 
%A Pinsonneault, Marc H. 
%A Pisani, Alice 
%A Prada, Francisco 
%A Prakash, Abhishek 
%A Price-Jones, Natalie 
%A Raddick, M. Jordan 
%A Rahman, Mubdi 
%A Raichoor, Anand 
%A Barboza Rembold, Sandro 
%A Reyna, A. M. 
%A Rich, James 
%A Richstein, Hannah 
%A Ridl, Jethro 
%A Riffel, Rogemar A. 
%A Riffel, Rogério 
%A Rix, Hans-Walter 
%A Robin, Annie C. 
%A Rockosi, Constance M. 
%A Rodríguez-Torres, Sergio 
%A Rodrigues, Thaíse S. 
%A Roe, Natalie 
%A Lopes, A. Roman 
%A Román-Zúñiga, Carlos 
%A Ross, Ashley J. 
%A Rossi, Graziano 
%A Ruan, John 
%A Ruggeri, Rossana 
%A Runnoe, Jessie C. 
%A Salazar-Albornoz, Salvador 
%A Salvato, Mara 
%A Sanchez, Sebastian F. 
%A Sanchez, Ariel G. 
%A Sanchez-Gallego, José R. 
%A Santiago, Basílio Xavier 
%A Schiavon, Ricardo 
%A Schimoia, Jaderson S. 
%A Schlafly, Eddie 
%A Schlegel, David J. 
%A Schneider, Donald P. 
%A Schönrich, Ralph 
%A Schultheis, Mathias 
%A Schwope, Axel 
%A Seo, Hee-Jong 
%A Serenelli, Aldo 
%A Sesar, Branimir 
%A Shao, Zhengyi 
%A Shetrone, Matthew 
%A Shull, Michael 
%A Silva Aguirre, Victor 
%A Skrutskie, M. F. 
%A Slosar, Anže 
%A Smith, Michael 
%A Smith, Verne V. 
%A Sobeck, Jennifer 
%A Somers, Garrett 
%A Souto, Diogo 
%A Stark, David V. 
%A Stassun, Keivan G. 
%A Steinmetz, Matthias 
%A Stello, Dennis 
%A Storchi Bergmann, Thaisa 
%A Strauss, Michael A. 
%A Streblyanska, Alina 
%A Stringfellow, Guy S. 
%A Suarez, Genaro 
%A Sun, Jing 
%A Taghizadeh-Popp, Manuchehr 
%A Tang, Baitian 
%A Tao, Charling 
%A Tayar, Jamie 
%A Tembe, Mita 
%A Thomas, Daniel 
%A Tinker, Jeremy 
%A Tojeiro, Rita 
%A Tremonti, Christy 
%A Troup, Nicholas 
%A Trump, Jonathan R. 
%A Unda-Sanzana, Eduardo 
%A Valenzuela, O. 
%A Van den Bosch, Remco 
%A Vargas-Magaña, Mariana 
%A Vazquez, Jose Alberto 
%A Villanova, Sandro 
%A Vivek, M. 
%A Vogt, Nicole 
%A Wake, David 
%A Walterbos, Rene 
%A Wang, Yuting 
%A Wang, Enci 
%A Weaver, Benjamin Alan 
%A Weijmans, Anne-Marie 
%A Weinberg, David H. 
%A Westfall, Kyle B. 
%A Whelan, David G. 
%A Wilcots, Eric 
%A Wild, Vivienne 
%A Williams, Rob A. 
%A Wilson, John 
%A Wood-Vasey, W. M. 
%A Wylezalek, Dominika 
%A Xiao, Ting 
%A Yan, Renbin 
%A Yang, Meng 
%A Ybarra, Jason E. 
%A Yeche, Christophe 
%A Yuan, Fang-Ting 
%A Zakamska, Nadia 
%A Zamora, Olga 
%A Zasowski, Gail 
%A Zhang, Kai 
%A Zhao, Cheng 
%A Zhao, Gong-Bo 
%A Zheng, Zheng 
%A Zheng, Zheng 
%A Zhou, Zhi-Min 
%A Zhu, Guangtun 
%A Zinn, Joel C. 
%A Zou, Hu
%+ AA(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain ; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain ;), AB(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), AC(Instituto de Investigación Multidisciplinario en Ciencia y Tecnología, Universidad de La Serena, Benavente 980, La Serena, Chile), AD(Leibniz-Institut fuer Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AE(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), AF(PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA <ID system="ORCID">0000-0001-8085-5890</ID>), AG(School of Physics and Astronomy, University of Nottingham, University Park, Nottingham, NG7 2RD, UK <ID system="ORCID">0000-0001-8215-1256</ID>), AH(Unidad de Astronomía, Universidad de Antofagasta, Avenida Angamos 601, Antofagasta 1270300, Chile ; Shanghai Astronomical Observatory, Chinese Academy of Science, 80 Nandan Road, Shanghai 200030, P. R. China), AI(IRFU, CEA, Centre d’Etudes Saclay, F-91191 Gif-Sur-Yvette Cedex, France), AJ(APC, University of Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cite, France), AK(Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, México D.F., 04510 Mexico <ID system="ORCID">0000-0002-3461-2342</ID>), AL(PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA <ID system="ORCID">0000-0003-3494-343X</ID>), AM(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AN(Universidade de São Paulo, IAG, Rua do Matão 1226, São Paulo 05508-900, Brazil ; Laboratório Interinstitucional de e-Astronomia—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil), AO(Department of Physics & Astronomy, Texas Christian University, Fort Worth, TX 76129, USA <ID system="ORCID">0000-0001-5817-0932</ID>), AP(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA <ID system="ORCID">0000-0003-2405-7258</ID>), AQ(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), AR(Department of Astronomy, Yale University, 52 Hillhouse Avenue, New Haven, CT 06511, USA <ID system="ORCID">0000-0002-6163-3472</ID>), AS(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK), AT(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), AU(Leibniz-Institut fuer Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany; Humboldt-Universitat zu Berlin, Institut für Physik, Newtonstrasse 15, D-12589, Berlin, Germany), AV(IRFU, CEA, Centre d’Etudes Saclay, F-91191 Gif-Sur-Yvette Cedex, France), AW(Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA), AX(Department of Physics and JINA Center for the Evolution of the Elements, University of Notre Dame, Notre Dame, IN 46556, USA <ID system="ORCID">0000-0003-4573-6233</ID>), AY(Cavendish Laboratory, University of Cambridge, 19 J. J. Thomson Avenue, Cambridge CB3 0HE, UK ; University of Cambridge, Kavli Institute for Cosmology, Cambridge, CB3 0HE, UK), AZ(Department of Astronomy, University of Wisconsin-Madison, 475 N. Charter St., Madison WI 53706, USA <ID system="ORCID">0000-0002-3131-4374</ID>), BA(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), BB(Department of Physics and Astronomy, Vanderbilt University, 6301 Stevenson Center, Nashville, TN, 37235, USA), BC(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA ; Department of Astronomy, New Mexico State University, Las Cruces, NM 88003, USA ; Sternberg Astronomical Institute, Moscow State University, Moscow 119992, Russia <ID system="ORCID">0000-0002-3601-133X</ID>), BD(Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA, 91101, USA ; Departamento de Astronomía, Universidad de Chile, Camino del Observatorio 1515, Las Condes, Santiago, Chile ; Centro de Astrofísica y Tecnologías Afines (CATA), Camino del Observatorio 1515, Las Condes, Santiago, Chile), BE(Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, NY 10003, USA <ID system="ORCID">0000-0003-1641-6222</ID>), BF(Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, F-13388, Marseille, France), BG(Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA; National Optical Astronomy Observatory, 950 N Cherry Ave., Tucson, AZ 85719, USA), BH(Instituto de Física y Astronomía, Universidad de Valparaíso, Av. Gran Bretaña 1111, Playa, Ancha, Casilla 5030, Chile ; Millennium Institute of Astrophysics (MAS), Monseñor Sotero Sanz 100, oficina 104, Providencia, Santiago, Chile), BI(Department of Astronomy and Astrophysics, University of Toronto, 50 St. George St., Toronto, ON M55 3H4, Canada ; Dunlap Institute for Astronomy & Astrophysics, University of Toronto, 50 St. George St., Toronto, ON M5S 3H4, Canada <ID system="ORCID">0000-0001-6855-442X</ID>), BJ(Department of Astronomy and Astrophysics, Eberly College of Science, The Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA ; Institute for Gravitation and the Cosmos, Pennsylvania State University, University Park, PA 16802, USA ; Department of Physics, The Pennsylvania State University, University Park, PA 16802, USA), BK(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA), BL(Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA <ID system="ORCID">0000-0002-8725-1069</ID>), BM(Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan <ID system="ORCID">0000-0001-9742-3138</ID>), BN(IRFU, CEA, Centre d’Etudes Saclay, F-91191 Gif-Sur-Yvette Cedex, France), BO(APC, University of Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cite, France), BP(Laboratório Interinstitucional de e-Astronomia—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil ; Departamento de Física Matemática, Instituto de Física, Universidade de São Paulo, CP 66318, CEP 05314-970, São Paulo, SP, Brazil), BQ(Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, México D.F., 04510 Mexico), BR(Sub-department of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK <ID system="ORCID">0000-0002-1283-8420</ID>), BS(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain <ID system="ORCID">0000-0001-6143-8151</ID>), BT(New York University Abu Dhabi, P.O. Box 129188, Abu Dhabi, United Arab Emirates), BU(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA), BV(Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan <ID system="ORCID">0000-0001-8546-1428</ID>), BW(Leibniz-Institut fuer Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), BX(Department of Astronomy, New Mexico State University, Las Cruces, NM 88003, USA <ID system="ORCID">0000-0001-9984-0891</ID>), BY(Leibniz-Institut fuer Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), BZ(Korea Institute for Advanced Study, 85 Hoegiro, Dongdaemun-gu, Seoul 02455, Korea <ID system="ORCID">0000-0002-3043-2555</ID>), CA(Laboratório Interinstitucional de e-Astronomia—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil ; Departamento de Física, Centro de Ciências Naturais e Exatas, Universidade Federal de Santa Maria, 97105-900, Santa Maria, RS, Brazil), CB(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstraße, D-85741 Garching, Germany), CC(Departamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile), CD(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, 389 UCB, Boulder, CO 80309, USA), CE(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain ; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain), CF(Laboratório Interinstitucional de e-Astronomia—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil ; Instituto de Física, Universidade Federal do Rio Grande do Sul, Campus do Vale, Porto Alegre, RS, 91501-907, Brazil), CG(Aix Marseille Université, CNRS/IN2P3, Centre de Physique des Particules de Marseille, UMR 7346, 13288, Marseille, France), CH(Department of Physics and Astronomy, Western Washington University, 516 High Street, Bellingham, WA 98225, USA <ID system="ORCID">0000-0001-6914-7797</ID>), CI(Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA, 91101, USA <ID system="ORCID">0000-0002-5226-787X</ID>), CJ(Department of Physics and McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213, USA), CK(Observatório Nacional, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brazil), CL(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, 389 UCB, Boulder, CO 80309, USA <ID system="ORCID">0000-0003-2511-2060</ID>), CM(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), CN(Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA <ID system="ORCID">0000-0002-0553-3805</ID>), CO(Laboratório Interinstitucional de e-Astronomia—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil ; Observatório Nacional, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brazil), CP(Laboratório Interinstitucional de e-Astronomia—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil ; Departamento de Física, Centro de Ciências Naturais e Exatas, Universidade Federal de Santa Maria, 97105-900, Santa Maria, RS, Brazil), CQ(Laboratório Interinstitucional de e-Astronomia—LIneA, Rua Gal. 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José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil ; Departamento de Física, Centro de Ciências Naturais e Exatas, Universidade Federal de Santa Maria, 97105-900, Santa Maria, RS, Brazil), JB(Department of Physics and Astronomy, Western Washington University, 516 High Street, Bellingham, WA 98225, USA), JC(IRFU, CEA, Centre d’Etudes Saclay, F-91191 Gif-Sur-Yvette Cedex, France), JD(Department of Physics & Astronomy, Texas Christian University, Fort Worth, TX 76129, USA), JE(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstraße, D-85741 Garching, Germany), JF(Laboratório Interinstitucional de e-Astronomia—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil ; Departamento de Física, Centro de Ciências Naturais e Exatas, Universidade Federal de Santa Maria, 97105-900, Santa Maria, RS, Brazil), JG(Laboratório Interinstitucional de e-Astronomia—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil ; Instituto de Física, Universidade Federal do Rio Grande do Sul, Campus do Vale, Porto Alegre, RS, 91501-907, Brazil), JH(Max-Planck-Institut für Astronomie, Konigstuhl 17, D-69117 Heidelberg, Germany <ID system="ORCID">0000-0003-4996-9069</ID>), JI(Institut UTINAM, CNRS-UMR6213, OSU THETA, Université Bourgogne-Franche-Comté, 41bis avenue de l’Observatoire, 25010 Besançon Cedex, France), JJ(Department of Astronomy and Astrophysics, University of California, Santa Cruz and UC Observatories, Santa Cruz, CA, 95064, USA), JK(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), JL(Laboratório Interinstitucional de e-Astronomia—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil ; Osservatorio Astronomico di Padova—INAF, Vicolo dell’Osservatorio 5, I-35122, Padova, Italy; Dipartimento di Fisica e Astronomia, Università di Padova, Vicolo dell’Osservatorio 2, I-35122 Padova, Italy), JM(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), JN(Departamento de Fisica y Astronomia, Universidad de La Serena, Cisternas 1200, La Serena, 0000-0002-1379-4204, Chile), JO(Instituto de Astronomía, Universidad Nacional Autónoma de México, Unidad Académica en Ensenada, Ensenada BC 22860, Mexico <ID system="ORCID">0000-0001-8600-4798</ID>), JP(Center for Cosmology and AstroParticle Physics, The Ohio State University, 191 W. Woodruff Ave., Columbus, OH 43210, USA), JQ(Department of Astronomy and Space Science, Sejong University, Seoul 143-747, Korea), JR(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA <ID system="ORCID">0000-0001-8665-5523</ID>), JS(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK), JT(Department of Astronomy and Astrophysics, Eberly College of Science, The Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, Pennsylvania State University, University Park, PA 16802, USA), JU(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstraße, D-85741 Garching, Germany), JV(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstraße, D-85741 Garching, Germany <ID system="ORCID">0000-0001-7116-9303</ID>), JW(Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, México D.F., 04510 Mexico <ID system="ORCID">0000-0001-6444-9307</ID>), JX(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstraße, D-85741 Garching, Germany), JY(Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA), JZ(Laboratório Interinstitucional de e-Astronomia—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil ; Instituto de Física, Universidade Federal do Rio Grande do Sul, Campus do Vale, Porto Alegre, RS, 91501-907, Brazil), KA(Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK), KB(Laboratório Interinstitucional de e-Astronomia—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil ; Instituto de Física, Universidade Federal do Rio Grande do Sul, Campus do Vale, Porto Alegre, RS, 91501-907, Brazil <ID system="ORCID">0000-0002-5640-6697</ID>), KC(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; <ID system="ORCID">0000-0002-3569-7421</ID>), KD(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA <ID system="ORCID">0000-0002-5042-5088</ID>), KE(Department of Astronomy and Astrophysics, Eberly College of Science, The Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, Pennsylvania State University, University Park, PA 16802, USA), KF(Sub-department of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK <ID system="ORCID">0000-0002-4236-3091</ID>), KG(Observatoire de la Côte d’Azur, Laboratoire Lagrange, F-06304 Nice Cedex 4, France <ID system="ORCID">0000-0002-6590-1657</ID>), KH(Leibniz-Institut fuer Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), KI(Department of Physics and Astronomy, Ohio University, Clippinger Labs, Athens, OH 45701, USA), KJ(Institute of Space Sciences (IEEC-CSIC), Carrer de Can Magrans, E-08193, Barcelona, Spain), KK(Max-Planck-Institut für Astronomie, Konigstuhl 17, D-69117 Heidelberg, Germany <ID system="ORCID">0000-0002-0834-3978</ID>), KL(Shanghai Astronomical Observatory, Chinese Academy of Science, 80 Nandan Road, Shanghai 200030, P. R. China), KM(University of Texas at Austin, McDonald Observatory, McDonald Observatory, TX, 79734, USA <ID system="ORCID">0000-0003-0509-2656</ID>), KN(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, 389 UCB, Boulder, CO 80309, USA <ID system="ORCID">0000-0002-4594-9936</ID>), KO(Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark <ID system="ORCID">0000-0002-6137-903X</ID>), KP(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), KQ(Brookhaven National Laboratory, Upton, NY 11973, USA), KR(Department of Astronomy, University of Wisconsin-Madison, 475 N. Charter St., Madison WI 53706, USA), KS(National Optical Astronomy Observatories, Tucson, AZ, 85719, USA), KT(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), KU(Department of Physics and Astronomy, Vanderbilt University, 6301 Stevenson Center, Nashville, TN, 37235, USA; Department of Astronomy, The Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA), KV(Observatório Nacional, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brazil), KW(Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan <ID system="ORCID">0000-0002-3746-2853</ID>), KX(Department of Physics and Astronomy, Vanderbilt University, 6301 Stevenson Center, Nashville, TN, 37235, USA <ID system="ORCID">0000-0002-3481-9052</ID>), KY(Leibniz-Institut fuer Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany <ID system="ORCID">0000-0001-6516-7459</ID>), KZ(Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia ; School of Physics, The University of New South Wales, Sydney NSW 2052, Australia <ID system="ORCID">0000-0002-4879-3519</ID>), LA(Laboratório Interinstitucional de e-Astronomia—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil ; Instituto de Física, Universidade Federal do Rio Grande do Sul, Campus do Vale, Porto Alegre, RS, 91501-907, Brazil), LB(Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA <ID system="ORCID">0000-0002-0106-7755</ID>), LC(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), LD(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, 389 UCB, Boulder, CO 80309, USA <ID system="ORCID">0000-0003-1479-3059</ID>), LE(Instituto de Astronomía, Universidad Nacional Autónoma de México, Unidad Académica en Ensenada, Ensenada BC 22860, Mexico <ID system="ORCID">0000-0002-2011-4924</ID>), LF(Department of Physics & Astronomy, Texas Christian University, Fort Worth, TX 76129, USA), LG(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA), LH(Departamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile <ID system="ORCID">0000-0002-0066-0346</ID>), LI(Aix Marseille Université, CNRS/IN2P3, Centre de Physique des Particules de Marseille, UMR 7346, 13288, Marseille, France; Tsinghua Center for Astrophysics and Department of Physics, Tsinghua University, Beijing 100084, P. R. China), LJ(Department of Astronomy, The Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA <ID system="ORCID">0000-0002-4818-7885</ID>), LK(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), LL(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK), LM(Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, NY 10003, USA), LN(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK), LO(Department of Astronomy, University of Wisconsin-Madison, 475 N. Charter St., Madison WI 53706, USA), LP(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA <ID system="ORCID">0000-0003-3248-3097</ID>), LQ(Department of Astronomy and Astrophysics, Eberly College of Science, The Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA; <ID system="ORCID">0000-0002-1410-0470</ID>), LR(Unidad de Astronomía, Universidad de Antofagasta, Avenida Angamos 601, Antofagasta 1270300, Chile), LS(Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, México D.F., 04510 Mexico), LT(Max-Planck-Institut für Astronomie, Konigstuhl 17, D-69117 Heidelberg, Germany <ID system="ORCID">0000-0002-0420-6159</ID>), LU(Instituto de Física, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, Mexico), LV(Brookhaven National Laboratory, Upton, NY 11973, USA), LW(Departamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile), LX(Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA), LY(Department of Astronomy, New Mexico State University, Las Cruces, NM 88003, USA), LZ(Department of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK ; Department of Physics, University of North Carolina Asheville, One University Heights, Asheville, NC 28804, USA <ID system="ORCID">0000-0002-6047-1010</ID>), MA(Department of Astronomy, New Mexico State University, Las Cruces, NM 88003, USA <ID system="ORCID">0000-0002-0782-3064</ID>), MB(National Astronomy Observatories, Chinese Academy of Science, 20A Datun Rd., Chaoyang District, Beijing, 100012, P. R. China; Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK), MC(Shanghai Astronomical Observatory, Chinese Academy of Science, 80 Nandan Road, Shanghai 200030, P. R. China <ID system="ORCID">0000-0003-1588-9394</ID>), MD(Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, NY 10003, USA), ME(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK), MF(Department of Astronomy, The Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA; Center for Cosmology and AstroParticle Physics, The Ohio State University, 191 W. Woodruff Ave., Columbus, OH 43210, USA <ID system="ORCID">0000-0001-7775-7261</ID>), MG(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK), MH(Physics Department, Austin College, Sherman, TX 75092, USA), MI(Department of Astronomy, University of Wisconsin-Madison, 475 N. Charter St., Madison WI 53706, USA), MJ(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK), MK(Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK), ML(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), MM(PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA <ID system="ORCID">0000-0001-7113-1233</ID>), MN(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA <ID system="ORCID">0000-0003-2212-6045</ID>), MO(), MP(Department of Physics and Astronomy, University of Kentucky, 505 Rose St., Lexington, KY 40506, USA <ID system="ORCID">0000-0003-1025-1711</ID>), MQ(Tsinghua Center for Astrophysics and Department of Physics, Tsinghua University, Beijing 100084, P. R. China), MR(Instituto de Astronomía, Universidad Nacional Autónoma de México, Unidad Académica en Ensenada, Ensenada BC 22860, Mexico; Department of Physics, Bridgewater College, 402 E. College St., Bridgewater, VA 22812, USA <ID system="ORCID">0000-0002-3576-4508</ID>), MS(IRFU, CEA, Centre d’Etudes Saclay, F-91191 Gif-Sur-Yvette Cedex, France), MT(Shanghai Astronomical Observatory, Chinese Academy of Science, 80 Nandan Road, Shanghai 200030, P. R. China), MU(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA <ID system="ORCID">0000-0001-6100-6869</ID>), MV(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), MW(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA), MX(Department of Physics and Astronomy, University of Kentucky, 505 Rose St., Lexington, KY 40506, USA <ID system="ORCID">0000-0002-9808-3646</ID>), MY(Tsinghua Center for Astrophysics and Department of Physics, Tsinghua University, Beijing 100084, P. R. China), MZ(National Astronomy Observatories, Chinese Academy of Science, 20A Datun Rd., Chaoyang District, Beijing, 100012, P. R. China; Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK <ID system="ORCID">0000-0003-4726-6714</ID>), NA(National Astronomy Observatories, Chinese Academy of Science, 20A Datun Rd., Chaoyang District, Beijing, 100012, P. R. China <ID system="ORCID">0000-0003-1887-6732</ID>), NB(Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA), NC(National Astronomy Observatories, Chinese Academy of Science, 20A Datun Rd., Chaoyang District, Beijing, 100012, P. R. China <ID system="ORCID">0000-0002-4135-0977</ID>), ND(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA; <ID system="ORCID">0000-0002-7574-8078</ID>), NE(Department of Astronomy, The Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA <ID system="ORCID">0000-0002-7550-7151</ID>), NF(National Astronomy Observatories, Chinese Academy of Science, 20A Datun Rd., Chaoyang District, Beijing, 100012, P. R. China <ID system="ORCID">0000-0002-6684-3997</ID>)
%B The Astrophysical Journal Supplement Series
%V 233
%D 2017
%8 December 1, 2017
%K atlases;  catalogs;  surveys 
%U http://adsabs.harvard.edu/abs/2017ApJS..233...25A
%X The fourth generation of the Sloan Digital Sky Survey (SDSS-IV) began 
observations in 2014 July. It pursues three core programs: the Apache 
Point Observatory Galactic Evolution Experiment 2 (APOGEE-2), Mapping 
Nearby Galaxies at APO (MaNGA), and the Extended Baryon Oscillation 
Spectroscopic Survey (eBOSS). As well as its core program, eBOSS 
contains two major subprograms: the Time Domain Spectroscopic Survey 
(TDSS) and the SPectroscopic IDentification of ERosita Sources 
(SPIDERS). This paper describes the first data release from SDSS-IV, 
Data Release 13 (DR13). DR13 makes publicly available the first 1390 
spatially resolved integral field unit observations of nearby galaxies 
from MaNGA. It includes new observations from eBOSS, completing the 
Sloan Extended QUasar, Emission-line galaxy, Luminous red galaxy Survey 
(SEQUELS), which also targeted variability-selected objects and 
X-ray-selected objects. DR13 includes new reductions of the SDSS-III 
BOSS data, improving the spectrophotometric calibration and redshift 
classification, and new reductions of the SDSS-III APOGEE-1 data, 
improving stellar parameters for dwarf stars and cooler stars. DR13 
provides more robust and precise photometric calibrations. Value-added 
target catalogs relevant for eBOSS, TDSS, and SPIDERS and an updated 
red-clump catalog for APOGEE are also available. This paper describes 
the location and format of the data and provides references to important 
technical papers. The SDSS web site, <A 
href="http://www.sdss.org">http://www.sdss.org</A>, provides links to 
the data, tutorials, examples of data access, and extensive 
documentation of the reduction and analysis procedures. DR13 is the 
first of a scheduled set that will contain new data and analyses from 
the planned ∼6 yr operations of SDSS-IV.
%3 10.3847/1538-4365/aa8992
%= eprint: arXiv:1608.02013
%@ 0067-0049

%0 Journal Article
%T Baryon acoustic oscillations from the complete SDSS-III Lyα-quasar cross-correlation function at z = 2.4
%A du Mas des Bourboux, Hélion 
%A Le Goff, Jean-Marc 
%A Blomqvist, Michael 
%A Busca, Nicolás G. 
%A Guy, Julien 
%A Rich, James 
%A Yèche, Christophe 
%A Bautista, Julian E. 
%A Burtin, Étienne 
%A Dawson, Kyle S. 
%A Eisenstein, Daniel J. 
%A Font-Ribera, Andreu 
%A Kirkby, David 
%A Miralda-Escudé, Jordi 
%A Noterdaeme, Pasquier 
%A Palanque-Delabrouille, Nathalie 
%A Pâris, Isabelle 
%A Petitjean, Patrick 
%A Pérez-Ràfols, Ignasi 
%A Pieri, Matthew M. 
%A Ross, Nicholas P. 
%A Schlegel, David J. 
%A Schneider, Donald P. 
%A Slosar, Anže 
%A Weinberg, David H. 
%A Zarrouk, Pauline
%+ AA(IRFU, CEA, Université Paris-Saclay, 91191, Gif-sur-Yvette, France <EMAIL>rich@hep.saclay.cea.fr</EMAIL>), AB(IRFU, CEA, Université Paris-Saclay, 91191, Gif-sur-Yvette, France), AC(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), AD(APC, Université Paris Diderot-Paris 7, CNRS/IN2P3, CEA, Observatoire de Paris, 10 rue A. Domon & L. Duquet, 75014, Paris, France), AE(LPNHE, CNRS/IN2P3, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris 7, 4 place Jussieu, 75252, Paris Cedex, France), AF(IRFU, CEA, Université Paris-Saclay, 91191, Gif-sur-Yvette, France), AG(IRFU, CEA, Université Paris-Saclay, 91191, Gif-sur-Yvette, France; Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA, 94720, USA), AH(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT, 84112, USA), AI(IRFU, CEA, Université Paris-Saclay, 91191, Gif-sur-Yvette, France), AJ(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT, 84112, USA), AK(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA, 02138, USA), AL(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA, 94720, USA; Department of Physics and Astronomy, University College London, Gower Street, London, UK), AM(Department of Physics and Astronomy, University of California, Irvine, CA, 92697, USA), AN(Institució Catalana de Recerca i Estudis Avançats, 08010 Barcelona, Catalonia, Spain; Institució de Ciències del Cosmos, Universitat de Barcelona (UB-IEEC), 080028 Barcelona, Catalonia, Spain), AO(Université Paris 6 et CNRS, Institut d'Astrophysique de Paris, 98 bis Blvd. Arago, 75014, Paris, France), AP(IRFU, CEA, Université Paris-Saclay, 91191, Gif-sur-Yvette, France), AQ(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), AR(Université Paris 6 et CNRS, Institut d'Astrophysique de Paris, 98 bis Blvd. Arago, 75014, Paris, France), AS(Institució de Ciències del Cosmos, Universitat de Barcelona (UB-IEEC), 080028 Barcelona, Catalonia, Spain), AT(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), AU(SUPA, Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, EH9 3HJ, UK), AV(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA, 94720, USA), AW(Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA, 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA, 16802, USA), AX(Brookhaven National Laboratory, 2 Center Road, Upton, NY, 11973, USA), AY(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH, 43210, USA), AZ(IRFU, CEA, Université Paris-Saclay, 91191, Gif-sur-Yvette, France)
%B Astronomy and Astrophysics
%V 608
%D 2017
%8 December 1, 2017
%K cosmological parameters;  dark energy;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2017A%26A...608A.130D
%X We present a measurement of baryon acoustic oscillations (BAO) in the 
cross-correlation of quasars with the Lyα-forest flux transmission 
at a mean redshift of z = 2.40. The measurement uses the complete Sloan 
Digital Sky Survey (SDSS-III) data sample: 168 889 forests and 234 367 
quasars from the SDSS data release DR12. In addition to the statistical 
improvement on our previous study using DR11, we have implemented 
numerous improvements at the analysis level enabling a more accurate 
measurement of this cross-correlation. We have also developed the first 
simulations of the cross-correlation that allow us to test different 
aspects of our data analysis and to search for potential systematic 
errors in the determination of the BAO peak position. We measure the two 
ratios D<SUB>H</SUB>(z = 2.40) /r<SUB>d</SUB> = 9.01 ± 0.36 and 
D<SUB>M</SUB>(z = 2.40) /r<SUB>d</SUB> = 35.7 ± 1.7, where the 
errors include marginalization over the non-linear velocity of quasars 
and the cross-correlation of metals and quasars, among other effects. 
These results are within 1.8σ of the prediction of the 
flat-ΛCDM model describing the observed cosmic microwave 
background anisotropies. We combine this study with the Lyα-forest 
auto-correlation function, yielding D<SUB>H</SUB>(z = 2.40) 
/r<SUB>d</SUB> = 8.94 ± 0.22 and D<SUB>M</SUB>(z = 2.40) 
/r<SUB>d</SUB> = 36.6 ± 1.2, within 2.3σ of the same 
flat-ΛCDM model.
%3 10.1051/0004-6361/201731731
%= eprint: arXiv:1708.02225
%@ 0004-6361

%0 Journal Article
%T Using galaxy pairs to investigate the three-point correlation function in the squeezed limit
%A Yuan, Sihan 
%A Eisenstein, Daniel J. 
%A Garrison, Lehman H.
%+ AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA <ID system="ORCID">0000-0002-5992-7586</ID>), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA), AC(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 472
%D 2017
%8 November 1, 2017
%P 577-590
%K methods: analytical;  galaxies: haloes;  dark matter;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2017MNRAS.472..577Y
%X We investigate the three-point correlation function (3PCF) in the 
squeezed limit by considering galaxy pairs as discrete objects and 
cross-correlating them with the galaxy field. We develop an efficient 
algorithm using fast Fourier transforms to compute such 
cross-correlations and their associated pair-galaxy bias b<SUB>p, 
g</SUB> and the squeezed 3PCF coefficient Q<SUB>eff</SUB>. We implement 
our method using N-body cosmological simulations and a fiducial halo 
occupation distribution (HOD) and present the results in both the real 
space and redshift space. In real space, we observe a peak in b<SUB>p, 
g</SUB> and Q<SUB>eff</SUB> at pair separation of ∼2 Mpc, attributed 
to the fact that galaxy pairs at 2 Mpc separation trace the most massive 
dark matter haloes. We also see strong anisotropy in the b<SUB>p, 
g</SUB> and Q<SUB>eff</SUB> signals that track the large-scale 
filamentary structure. In redshift space, both the 2 Mpc peak and the 
anisotropy are significantly smeared out along the line of sight due to 
finger-of-God effect. In both the real space and redshift space, the 
squeezed 3PCF shows a factor of 2 variation, contradicting the 
hierarchical ansatz, but offering rich information on the galaxy-halo 
connection. Thus, we explore the possibility of using the squeezed 3PCF 
to constrain the HOD. When we compare two simple HOD models that are 
closely matched in their projected two-point correlation function 
(2PCF), we do not yet see a strong variation in the 3PCF that is clearly 
disentangled from variations in the projected 2PCF. Nevertheless, we 
propose that more complicated HOD models, e.g. those incorporating 
assembly bias, can break degeneracies in the 2PCF and show a 
distinguishable squeezed 3PCF signal.
%3 10.1093/mnras/stx2032
%= eprint: arXiv:1705.03464
%@ 0035-8711

%0 Journal Article
%T The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements from DR12 galaxy clustering - towards an accurate model
%A Chuang, Chia-Hsun 
%A Pellejero-Ibanez, Marcos 
%A Rodríguez-Torres, Sergio 
%A Ross, Ashley J. 
%A Zhao, Gong-bo 
%A Wang, Yuting 
%A Cuesta, Antonio J. 
%A Rubiño-Martín, J. A. 
%A Prada, Francisco 
%A Alam, Shadab 
%A Beutler, Florian 
%A Eisenstein, Daniel J. 
%A Gil-Marín, Héctor 
%A Grieb, Jan Niklas 
%A Ho, Shirley 
%A Kitaura, Francisco-Shu 
%A Percival, Will J. 
%A Rossi, Graziano 
%A Salazar-Albornoz, Salvador 
%A Samushia, Lado 
%A Sánchez, Ariel G. 
%A Satpathy, Siddharth 
%A Slosar, Anže 
%A Thomas, Daniel 
%A Tinker, Jeremy L. 
%A Tojeiro, Rita 
%A Vargas-Magaña, Mariana 
%A Vazquez, Jose A. 
%A Brownstein, Joel R. 
%A Nichol, Robert C. 
%A Olmstead, Matthew D.
%+ AA(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AB(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany; Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Departamento Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), AC(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica M8, Universidad Autonoma de Madrid (UAM), Cantoblanco, E-28049, Madrid, Spain), AD(Center for Cosmology and Astroparticle Physics, Department of Physics, The Ohio State University, OH 43210, USA; Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK <ID system="ORCID">0000-0002-7522-9083</ID>), AE(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; National Astronomy Observatories, Chinese Academy of Science, Beijing, 100012, P.R.China), AF(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; National Astronomy Observatories, Chinese Academy of Science, Beijing, 100012, P.R.China), AG(Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, E-08028 Barcelona, Spain), AH(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200, La Laguna, Tenerife, Spain; Departamento Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), AI(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica M8, Universidad Autonoma de Madrid (UAM), Cantoblanco, E-28049, Madrid, Spain; Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía, E-18080 Granada, Spain), AJ(Sorbonne Universités, Institut Lagrange de Paris (ILP), 98 bis Boulevard Arago, F-75014 Paris, France; Laboratoire de Physique Nucléaire et de Hautes Energies, Université Pierre et Marie Curie, 4 Place Jussieu, F-75005 Paris, France), AK(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley CA 94720, USA <ID system="ORCID">0000-0003-0467-5438</ID>), AL(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AM(Sorbonne Universités, Institut Lagrange de Paris (ILP), 98 bis Boulevard Arago, F-75014 Paris, France; Laboratoire de Physique Nucléaire et de Hautes Energies, Université Pierre et Marie Curie, 4 Place Jussieu, F-75005 Paris, France), AN(Universitäts-Sternwarte München, Scheinerstrasse 1, D-81679, Munich, Germany; Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany <ID system="ORCID">0000-0003-2178-0694</ID>), AO(Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley CA 94720, USA; McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA; The McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA; Departments of Physics and Astronomy, University of California, Berkeley, CA 94720, USA), AP(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley CA 94720, USA; Departments of Physics and Astronomy, University of California, Berkeley, CA 94720, USA), AQ(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AR(Department of Physics and Astronomy, Sejong University, Seoul 143-747, Korea), AS(Universitäts-Sternwarte München, Scheinerstrasse 1, D-81679, Munich, Germany; Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AT(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; Kansas State University, Manhattan, KS 66506, USA; Brookhaven National Laboratory, Upton, NY 11973, UK), AU(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AV(McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA; The McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA <ID system="ORCID">0000-0003-0034-1916</ID>), AW(Brookhaven National Laboratory, Upton, NY 11973, UK), AX(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AY(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), AZ(School of Physics and Astronomy, University of St Andrews, St Andrews, KY16 9SS, UK <ID system="ORCID">0000-0001-5191-2286</ID>), BA(Instituto de Física, Universidad Nacional Autónoma de México, Ciudad de México, Apdo. Postal 20-364, México), BB(Brookhaven National Laboratory, Upton, NY 11973, UK), BC(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), BD(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), BE(Department of Chemistry and Physics, King's College, 133 North River St, Wilkes Barre, PA 18711, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 471
%D 2017
%8 October 1, 2017
%P 2370-2390
%K cosmological parameters;  distance scale;  large-scale structure of Universe;  cosmology: observations
%U http://adsabs.harvard.edu/abs/2017MNRAS.471.2370C
%X We analyse the broad-range shape of the monopole and quadrupole 
correlation functions of the Baryon Oscillation Spectroscopic Survey 
Data Release 12 (DR12) CMASS and LOWZ galaxy sample to obtain 
constraints on the Hubble expansion rate H(z), the angular-diameter 
distance D<SUB>A</SUB>(z), the normalized growth rate 
f(z)σ<SUB>8</SUB>(z) and the physical matter density 
Ω<SUB>m</SUB> h<SUP>2</SUP>. We adopt wide and flat priors on all 
model parameters in order to ensure the results are those of a 
'single-probe' galaxy clustering analysis. We also marginalize over 
three nuisance terms that account for potential observational 
systematics affecting the measured monopole. However, such Monte Carlo 
Markov Chain analysis is computationally expensive for advanced 
theoretical models. We develop a new methodology to speed up the 
analysis. Using the range 40 h<SUP>-1</SUP> Mpc < s < 180 
h<SUP>-1</SUP> Mpc, we obtain 
{D<SUB>A</SUB>(z)r<SUB>s,fid</SUB>/r<SUB>s</SUB> (Mpc), 
H(z)r<SUB>s</SUB>/r<SUB>s,fid</SUB> km s<SUP>-1</SUP> Mpc<SUP>-1</SUP>, 
f(z)σ<SUB>8</SUB>(z), Ω<SUB>m</SUB> h<SUP>2</SUP>} = {956 
± 28, 75.0 ± 4.0, 0.397 ± 0.073, 0.143 ± 
0.017} at z = 0.32 and {1421 ± 23, 96.7 ± 2.7, 0.497 
± 0.058, 0.137 ± 0.015} at z = 0.59 where r<SUB>s</SUB> is 
the comoving sound horizon at the drag epoch and r<SUB>s,fid</SUB> = 
147.66 Mpc for the fiducial cosmology used in this study. Combining our 
measurements with Planck data, we obtain Ω<SUB>m</SUB> = 0.306 
± 0.009, H<SUB>0</SUB> = 67.9 ± 0.7 km s<SUP>-1</SUP> 
Mpc<SUP>-1</SUP> and σ<SUB>8</SUB> = 0.815 ± 0.009 assuming 
Λcold dark matter (CDM); Ω<SUB>k</SUB> = 0.000 ± 
0.003 and w = -1.02 ± 0.08 assuming owCDM. Our results show no 
tension with the flat ΛCDM cosmological paradigm. This paper is 
part of a set that analyses the final galaxy clustering data set from 
Baryon Oscillation Spectroscopic Survey.
%3 10.1093/mnras/stx1641
%= eprint: arXiv:1607.03151
%@ 0035-8711

%0 Journal Article
%T Dynamical dark energy in light of the latest observations
%A Zhao, Gong-Bo 
%A Raveri, Marco 
%A Pogosian, Levon 
%A Wang, Yuting 
%A Crittenden, Robert G. 
%A Handley, Will J. 
%A Percival, Will J. 
%A Beutler, Florian 
%A Brinkmann, Jonathan 
%A Chuang, Chia-Hsun 
%A Cuesta, Antonio J. 
%A Eisenstein, Daniel J. 
%A Kitaura, Francisco-Shu 
%A Koyama, Kazuya 
%A L'Huillier, Benjamin 
%A Nichol, Robert C. 
%A Pieri, Matthew M. 
%A Rodriguez-Torres, Sergio 
%A Ross, Ashley J. 
%A Rossi, Graziano 
%A Sánchez, Ariel G. 
%A Shafieloo, Arman 
%A Tinker, Jeremy L. 
%A Tojeiro, Rita 
%A Vazquez, Jose A. 
%A Zhang, Hanyu
%+ AA(National Astronomical Observatories, Chinese Academy of Sciences, 100012, Beijing, China; Institute of Cosmology and Gravitation, University of Portsmouth, PO1 3FX, Portsmouth, UK; National Astronomical Observatories, Chinese Academy of Sciences, 100012, Beijing, China; Institute of Cosmology and Gravitation, University of Portsmouth, PO1 3FX, Portsmouth, UK; National Astronomical Observatories, Chinese Academy of Sciences, 100012, Beijing, China; Institute of Cosmology and Gravitation, University of Portsmouth, PO1 3FX, Portsmouth, UK; National Astronomical Observatories, Chinese Academy of Sciences, 100012, Beijing, China; Institute of Cosmology and Gravitation, University of Portsmouth, PO1 3FX, Portsmouth, UK), AB(Kavli Institute for Cosmological Physics, Enrico Fermi Institute, The University of Chicago, 60637, Chicago, IL, USA; Institute Lorentz, Leiden University, PO Box 9506, 2300 RA, Leiden, Netherlands; Kavli Institute for Cosmological Physics, Enrico Fermi Institute, The University of Chicago, 60637, Chicago, IL, USA; Institute Lorentz, Leiden University, PO Box 9506, 2300 RA, Leiden, Netherlands), AC(Institute of Cosmology and Gravitation, University of Portsmouth, PO1 3FX, Portsmouth, UK; Department of Physics, Simon Fraser University, V5A 1S6, Burnaby, BC, Canada; Institute of Cosmology and Gravitation, University of Portsmouth, PO1 3FX, Portsmouth, UK; Department of Physics, Simon Fraser University, V5A 1S6, Burnaby, BC, Canada), AD(National Astronomical Observatories, Chinese Academy of Sciences, 100012, Beijing, China; Institute of Cosmology and Gravitation, University of Portsmouth, PO1 3FX, Portsmouth, UK; National Astronomical Observatories, Chinese Academy of Sciences, 100012, Beijing, China; Institute of Cosmology and Gravitation, University of Portsmouth, PO1 3FX, Portsmouth, UK), AE(Institute of Cosmology and Gravitation, University of Portsmouth, PO1 3FX, Portsmouth, UK), AF(Astrophysics Group, Cavendish Laboratory, J. J. Thomson Avenue, CB3 0HE, Cambridge, UK; Kavli Institute for Cosmology, Madingley Road, CB3 0HA, Cambridge, UK; Astrophysics Group, Cavendish Laboratory, J. J. Thomson Avenue, CB3 0HE, Cambridge, UK; Kavli Institute for Cosmology, Madingley Road, CB3 0HA, Cambridge, UK), AG(Institute of Cosmology and Gravitation, University of Portsmouth, PO1 3FX, Portsmouth, UK), AH(Institute of Cosmology and Gravitation, University of Portsmouth, PO1 3FX, Portsmouth, UK), AI(Apache Point Observatory, PO Box 59, 88349, Sunspot, NM, USA), AJ(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, E-28049, Cantoblanco, Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482, Potsdam, Germany; Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, E-28049, Cantoblanco, Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482, Potsdam, Germany), AK(Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC- UB), Martí i Franquès 1, E-08028, Barcelona, Spain; Departamento de Física, Universidad de Córdoba, Campus de Rabanales, Edificio Albert Einstein, E-14071, Córdoba, Spain; Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC- UB), Martí i Franquès 1, E-08028, Barcelona, Spain; Departamento de Física, Universidad de Córdoba, Campus de Rabanales, Edificio Albert Einstein, E-14071, Córdoba, Spain), AL(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, 02138, Cambridge, MA, USA), AM(Instituto de Astrofísica de Canarias, 38205 San Crist obal de La Laguna, Santa Cruz de Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206, La Laguna, Tenerife, Spain; Instituto de Astrofísica de Canarias, 38205 San Crist obal de La Laguna, Santa Cruz de Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206, La Laguna, Tenerife, Spain), AN(Institute of Cosmology and Gravitation, University of Portsmouth, PO1 3FX, Portsmouth, UK), AO(Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-gu, 34055, Daejeon, Korea), AP(Institute of Cosmology and Gravitation, University of Portsmouth, PO1 3FX, Portsmouth, UK), AQ(Aix Marseille Université, CNRS, Laboratoire d'Astrophysique de Marseille, UMR 7326, 13388, Marseille, France), AR(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, E-28049, Cantoblanco, Madrid, Spain; Campus of International Excellence UAM+CSIC, E-28049, Cantoblanco, Madrid, Spain; Departamento de Física Teórica, Universidad Autónoma de Madrid, E-28049, Cantoblanco, Madrid, Spain; Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, E-28049, Cantoblanco, Madrid, Spain; Campus of International Excellence UAM+CSIC, E-28049, Cantoblanco, Madrid, Spain; Departamento de Física Teórica, Universidad Autónoma de Madrid, E-28049, Cantoblanco, Madrid, Spain; Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, E-28049, Cantoblanco, Madrid, Spain; Campus of International Excellence UAM+CSIC, E-28049, Cantoblanco, Madrid, Spain; Departamento de Física Teórica, Universidad Autónoma de Madrid, E-28049, Cantoblanco, Madrid, Spain; Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, E-28049, Cantoblanco, Madrid, Spain; Campus of International Excellence UAM+CSIC, E-28049, Cantoblanco, Madrid, Spain; Departamento de Física Teórica, Universidad Autónoma de Madrid, E-28049, Cantoblanco, Madrid, Spain), AS(Institute of Cosmology and Gravitation, University of Portsmouth, PO1 3FX, Portsmouth, UK; Center for Cosmology and AstroParticle Physics, The Ohio State University, 43210, Columbus, OH, USA; Institute of Cosmology and Gravitation, University of Portsmouth, PO1 3FX, Portsmouth, UK; Center for Cosmology and AstroParticle Physics, The Ohio State University, 43210, Columbus, OH, USA), AT(Department of Astronomy and Space Science, Sejong University, 143-747, Seoul, Korea), AU(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstraße, 85741, Garching, Germany), AV(Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-gu, 34055, Daejeon, Korea; University of Science and Technology, 217 Gajeong-ro, Yuseong-gu, 34113, Daejeon, Korea; Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro, Yuseong-gu, 34055, Daejeon, Korea; University of Science and Technology, 217 Gajeong-ro, Yuseong-gu, 34113, Daejeon, Korea), AW(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, 10003, New York, NY, USA), AX(School of Physics and Astronomy, University of St Andrews, North Haugh, KY16 9SS, St Andrews, UK), AY(Brookhaven National Laboratory, Building 510, 11973, Upton, NY, USA), AZ(National Astronomical Observatories, Chinese Academy of Sciences, 100012, Beijing, China)
%B Nature Astronomy
%V 1
%D 2017
%8 September 1, 2017
%P 627-632
%U http://adsabs.harvard.edu/abs/2017NatAs...1..627Z
%X A flat Friedmann-Robertson-Walker universe dominated by a cosmological 
constant (Λ) and cold dark matter (CDM) has been the working 
model preferred by cosmologists since the discovery of cosmic 
acceleration<SUP>1,2</SUP>. However, tensions of various degrees of 
significance are known to be present among existing datasets within the 
ΛCDM framework<SUP>3-11</SUP>. In particular, the Lyman-α 
forest measurement of the baryon acoustic oscillations (BAO) by the 
Baryon Oscillation Spectroscopic Survey<SUP>3</SUP> prefers a smaller 
value of the matter density fraction Ω<SUB>M</SUB> than that 
preferred by cosmic microwave background (CMB). Also, the recently 
measured value of the Hubble constant, H<SUB>0</SUB> = 73.24 ± 
1.74 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP> (ref. <SUP>12</SUP>), is 
3.4σ higher than the 66.93 ± 0.62 km s<SUP>-1</SUP> 
Mpc<SUP>-1</SUP> inferred from the Planck CMB data<SUP>7</SUP>. In this 
work, we investigate whether these tensions can be interpreted as 
evidence for a non-constant dynamical dark energy. Using the 
Kullback-Leibler divergence<SUP>13</SUP> to quantify the tension between 
datasets, we find that the tensions are relieved by an evolving dark 
energy, with the dynamical dark energy model preferred at a 3.5σ 
significance level based on the improvement in the fit alone. While, at 
present, the Bayesian evidence for the dynamical dark energy is 
insufficient to favour it over ΛCDM, we show that, if the current 
best-fit dark energy happened to be the true model, it would be 
decisively detected by the upcoming Dark Energy Spectroscopic Instrument 
survey<SUP>14</SUP>.
%3 10.1038/s41550-017-0216-z
%= eprint: arXiv:1701.08165
%@ 2397-3366

%0 Journal Article
%T The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample
%A Alam, Shadab 
%A Ata, Metin 
%A Bailey, Stephen 
%A Beutler, Florian 
%A Bizyaev, Dmitry 
%A Blazek, Jonathan A. 
%A Bolton, Adam S. 
%A Brownstein, Joel R. 
%A Burden, Angela 
%A Chuang, Chia-Hsun 
%A Comparat, Johan 
%A Cuesta, Antonio J. 
%A Dawson, Kyle S. 
%A Eisenstein, Daniel J. 
%A Escoffier, Stephanie 
%A Gil-Marín, Héctor 
%A Grieb, Jan Niklas 
%A Hand, Nick 
%A Ho, Shirley 
%A Kinemuchi, Karen 
%A Kirkby, David 
%A Kitaura, Francisco 
%A Malanushenko, Elena 
%A Malanushenko, Viktor 
%A Maraston, Claudia 
%A McBride, Cameron K. 
%A Nichol, Robert C. 
%A Olmstead, Matthew D. 
%A Oravetz, Daniel 
%A Padmanabhan, Nikhil 
%A Palanque-Delabrouille, Nathalie 
%A Pan, Kaike 
%A Pellejero-Ibanez, Marcos 
%A Percival, Will J. 
%A Petitjean, Patrick 
%A Prada, Francisco 
%A Price-Whelan, Adrian M. 
%A Reid, Beth A. 
%A Rodríguez-Torres, Sergio A. 
%A Roe, Natalie A. 
%A Ross, Ashley J. 
%A Ross, Nicholas P. 
%A Rossi, Graziano 
%A Rubiño-Martín, Jose Alberto 
%A Saito, Shun 
%A Salazar-Albornoz, Salvador 
%A Samushia, Lado 
%A Sánchez, Ariel G. 
%A Satpathy, Siddharth 
%A Schlegel, David J. 
%A Schneider, Donald P. 
%A Scóccola, Claudia G. 
%A Seo, Hee-Jong 
%A Sheldon, Erin S. 
%A Simmons, Audrey 
%A Slosar, Anže 
%A Strauss, Michael A. 
%A Swanson, Molly E. C. 
%A Thomas, Daniel 
%A Tinker, Jeremy L. 
%A Tojeiro, Rita 
%A Magaña, Mariana Vargas 
%A Vazquez, Jose Alberto 
%A Verde, Licia 
%A Wake, David A. 
%A Wang, Yuting 
%A Weinberg, David H. 
%A White, Martin 
%A Wood-Vasey, W. Michael 
%A Yèche, Christophe 
%A Zehavi, Idit 
%A Zhai, Zhongxu 
%A Zhao, Gong-Bo
%+ AA(Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213, USA; The McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA), AB(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AC(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AD(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AE(Apache Point Observatory, New Mexico State University, PO Box 59, Sunspot, NM 88349, USA; Sternberg Astronomical Institute, Moscow State University, Universitetski pr. 13, 119992 Moscow, Russia), AF(Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, 43210 Ohio, USA), AG(Department Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA; National Optical Astronomy Observatory, 950 N Cherry Ave, Tucson, AZ 85719, USA), AH(Department Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AI(Department of Physics, Yale University, 260 Whitney Ave, New Haven, CT 06520, USA), AJ(Instituto de Física Teórica (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AK(Instituto de Física Teórica (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica M8, Universidad Autónoma de Madrid, E-28049 Cantoblanco, Madrid, Spain), AL(Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, E-08028 Barcelona, Spain), AM(Department Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AN(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), AO(CPPM, Aix-Marseille Université, CNRS/IN2P3, CPPM UMR 7346, F-13288 Marseille, France), AP(Institut Lagrange de Paris (ILP), Sorbonne Universités, 98 bis Boulevard Arago, F-75014 Paris, France; Laboratoire de Physique Nucléaire et de Hautes Energies, Université Pierre et Marie Curie, 4 Place Jussieu, F-75005 Paris, France), AQ(Universitäts-Sternwarte München, Scheinerstrasse 1, D-81679 Munich, Germany; Max-Planck-Institut für Extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85748 Garching, Germany), AR(Department of Astronomy, University of California at Berkeley, Berkeley, CA 94720, USA), AS(Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213, USA; The McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA), AT(Apache Point Observatory, New Mexico State University, PO Box 59, Sunspot, NM 88349, USA), AU(Department of Physics and Astronomy, UC Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697, USA), AV(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany; Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; Department of Astronomy, University of California at Berkeley, Berkeley, CA 94720, USA), AW(Apache Point Observatory, New Mexico State University, PO Box 59, Sunspot, NM 88349, USA), AX(Apache Point Observatory, New Mexico State University, PO Box 59, Sunspot, NM 88349, USA), AY(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AZ(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), BA(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), BB(Department of Chemistry and Physics, King's College, 133 North River St, Wilkes Barre, PA 18711, USA), BC(Apache Point Observatory, New Mexico State University, PO Box 59, Sunspot, NM 88349, USA), BD(Department of Physics, Yale University, 260 Whitney Ave, New Haven, CT 06520, USA), BE(CEA, Centre de Saclay, IRFU/SPP, F-91191 Gif-sur-Yvette, France), BF(Apache Point Observatory, New Mexico State University, PO Box 59, Sunspot, NM 88349, USA), BG(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200 La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), BH(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), BI(Institut d'Astrophysique de Paris, Université Paris 6 et CNRS, 98bis Boulevard Arago, F-75014 Paris, France), BJ(Instituto de Física Teórica (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Instituto de Astrofísica de Andalucía (CSIC), E-18080 Granada, Spain), BK(Department of Astrophysical Sciences, Princeton University, Ivy Lane, Princeton, NJ 08544, USA), BL(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; Department of Physics, University of California, 366 LeConte Hall, Berkeley, CA 94720, USA), BM(Instituto de Física Teórica (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica M8, Universidad Autónoma de Madrid, E-28049 Cantoblanco, Madrid, Spain), BN(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), BO(Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, 43210 Ohio, USA; Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), BP(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ, UK), BQ(Department of Astronomy and Space Science, Sejong University, Seoul 143-747, Korea), BR(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200 La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), BS(Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan; Max Planck Institut für Astrophysik, Karl-Schwarzschild-Straße 1, D-85740 Garching bei München, Germany), BT(Universitäts-Sternwarte München, Scheinerstrasse 1, D-81679 Munich, Germany; Max-Planck-Institut für Extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85748 Garching, Germany), BU(Department of Physics, Kansas State University, 116 Cardwell Hall, Manhattan, KS 66506, USA), BV(Max-Planck-Institut für Extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85748 Garching, Germany), BW(Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213, USA; The McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA), BX(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), BY(Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA), BZ(Instituto de Física Teórica (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Facultad de Ciencias Astronómicas y Geofísicas - Universidad Nacional de La Plata. Paseo del Bosque S/N, 1900 La Plata, Argentina; CONICET, Rivadavia 1917, 1033 Buenos Aires, Argentina), CA(Department of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, OH 45701, USA), CB(Brookhaven National Laboratory, Bldg 510, Upton, NY 11973, USA), CC(Apache Point Observatory, New Mexico State University, PO Box 59, Sunspot, NM 88349, USA), CD(Brookhaven National Laboratory, Bldg 510, Upton, NY 11973, USA), CE(Department of Astrophysical Sciences, Princeton University, Ivy Lane, Princeton, NJ 08544, USA), CF(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), CG(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), CH(Center for Cosmology and Particle Physics, New York University, New York, NY 10003, USA), CI(School of Physics and Astronomy, University of St Andrews, St Andrews KY16 9SS, UK), CJ(Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213, USA; The McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA; Instituto de Física, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, México), CK(Brookhaven National Laboratory, Bldg 510, Upton, NY 11973, USA), CL(Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, E-08028 Barcelona, Spain; ICREA (Institució Catalana de Recerca i Estudis Avançats) Passeig Lluís Companys 23, E-08010 Barcelona, Spain; Harvard-Smithsonian Center for Astrophysics, Radcliffe Institute for Advanced Study and ITC, Harvard University, MA 02138, USA; Institute of Theoretical Astrophysics, University of Oslo, 0315 Oslo, Norway), CM(Department of Astronomy, University of Wisconsin-Madison, 475 N. Charter Street, Madison, WI 53706, USA; Department of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK), CN(National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, P.R. China; Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), CO(Department of Astronomy, Ohio State University, Columbus, 43210 Ohio, USA; Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, 43210 Ohio, USA), CP(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; Department of Physics, University of California, 366 LeConte Hall, Berkeley, CA 94720, USA), CQ(PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, 3941 O'Hara Street, Pittsburgh, PA 15260, USA), CR(CEA, Centre de Saclay, IRFU/SPP, F-91191 Gif-sur-Yvette, France), CS(Department of Astronomy, Case Western Reserve University, Cleveland, OH 44106, USA), CT(School of Physics and Astronomy, University of St Andrews, St Andrews KY16 9SS, UK), CU(National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, P.R. China; Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK)
%B Monthly Notices of the Royal Astronomical Society
%V 470
%D 2017
%8 September 1, 2017
%P 2617-2652
%K distance scale;  large-scale structure of Universe;  cosmology: observations
%U http://adsabs.harvard.edu/abs/2017MNRAS.470.2617A
%X We present cosmological results from the final galaxy clustering data 
set of the Baryon Oscillation Spectroscopic Survey, part of the Sloan 
Digital Sky Survey III. Our combined galaxy sample comprises 1.2 million 
massive galaxies over an effective area of 9329 deg<SUP>2</SUP> and 
volume of 18.7 Gpc<SUP>3</SUP>, divided into three partially overlapping 
redshift slices centred at effective redshifts 0.38, 0.51 and 0.61. We 
measure the angular diameter distance D<SUB>M</SUB> and Hubble parameter 
H from the baryon acoustic oscillation (BAO) method, in combination with 
a cosmic microwave background prior on the sound horizon scale, after 
applying reconstruction to reduce non-linear effects on the BAO feature. 
Using the anisotropic clustering of the pre-reconstruction density 
field, we measure the product D<SUB>M</SUB>H from the Alcock-Paczynski 
(AP) effect and the growth of structure, quantified by 
fσ<SUB>8</SUB>(z), from redshift-space distortions (RSD). We 
combine individual measurements presented in seven companion papers into 
a set of consensus values and likelihoods, obtaining constraints that 
are tighter and more robust than those from any one method; in 
particular, the AP measurement from sub-BAO scales sharpens constraints 
from post-reconstruction BAOs by breaking degeneracy between 
D<SUB>M</SUB> and H. Combined with Planck 2016 cosmic microwave 
background measurements, our distance scale measurements simultaneously 
imply curvature Ω<SUB>K</SUB> = 0.0003 ± 0.0026 and a dark 
energy equation-of-state parameter w = -1.01 ± 0.06, in strong 
affirmation of the spatially flat cold dark matter (CDM) model with a 
cosmological constant (ΛCDM). Our RSD measurements of 
fσ<SUB>8</SUB>, at 6 per cent precision, are similarly consistent 
with this model. When combined with supernova Ia data, we find 
H<SUB>0</SUB> = 67.3 ± 1.0 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP> 
even for our most general dark energy model, in tension with some direct 
measurements. Adding extra relativistic species as a degree of freedom 
loosens the constraint only slightly, to H<SUB>0</SUB> = 67.8 ± 
1.2 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP>. Assuming flat ΛCDM, we 
find Ω<SUB>m</SUB> = 0.310 ± 0.005 and H<SUB>0</SUB> = 67.6 
± 0.5 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP>, and we find a 95 per 
cent upper limit of 0.16 eV c<SUP>-2</SUP> on the neutrino mass sum.
%3 10.1093/mnras/stx721
%= eprint: arXiv:1607.03155
%@ 0035-8711

%0 Journal Article
%T The Apache Point Observatory Galactic Evolution Experiment (APOGEE)
%A Majewski, Steven R. 
%A Schiavon, Ricardo P. 
%A Frinchaboy, Peter M. 
%A Allende Prieto, Carlos 
%A Barkhouser, Robert 
%A Bizyaev, Dmitry 
%A Blank, Basil 
%A Brunner, Sophia 
%A Burton, Adam 
%A Carrera, Ricardo 
%A Chojnowski, S. Drew 
%A Cunha, Kátia 
%A Epstein, Courtney 
%A Fitzgerald, Greg 
%A García Pérez, Ana E. 
%A Hearty, Fred R. 
%A Henderson, Chuck 
%A Holtzman, Jon A. 
%A Johnson, Jennifer A. 
%A Lam, Charles R. 
%A Lawler, James E. 
%A Maseman, Paul 
%A Mészáros, Szabolcs 
%A Nelson, Matthew 
%A Nguyen, Duy Coung 
%A Nidever, David L. 
%A Pinsonneault, Marc 
%A Shetrone, Matthew 
%A Smee, Stephen 
%A Smith, Verne V. 
%A Stolberg, Todd 
%A Skrutskie, Michael F. 
%A Walker, Eric 
%A Wilson, John C. 
%A Zasowski, Gail 
%A Anders, Friedrich 
%A Basu, Sarbani 
%A Beland, Stephane 
%A Blanton, Michael R. 
%A Bovy, Jo 
%A Brownstein, Joel R. 
%A Carlberg, Joleen 
%A Chaplin, William 
%A Chiappini, Cristina 
%A Eisenstein, Daniel J. 
%A Elsworth, Yvonne 
%A Feuillet, Diane 
%A Fleming, Scott W. 
%A Galbraith-Frew, Jessica 
%A García, Rafael A. 
%A García-Hernández, D. Aníbal 
%A Gillespie, Bruce A. 
%A Girardi, Léo 
%A Gunn, James E. 
%A Hasselquist, Sten 
%A Hayden, Michael R. 
%A Hekker, Saskia 
%A Ivans, Inese 
%A Kinemuchi, Karen 
%A Klaene, Mark 
%A Mahadevan, Suvrath 
%A Mathur, Savita 
%A Mosser, Benoît 
%A Muna, Demitri 
%A Munn, Jeffrey A. 
%A Nichol, Robert C. 
%A O'Connell, Robert W. 
%A Parejko, John K. 
%A Robin, A. C. 
%A Rocha-Pinto, Helio 
%A Schultheis, Matthias 
%A Serenelli, Aldo M. 
%A Shane, Neville 
%A Silva Aguirre, Victor 
%A Sobeck, Jennifer S. 
%A Thompson, Benjamin 
%A Troup, Nicholas W. 
%A Weinberg, David H. 
%A Zamora, Olga
%+ AA(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA <ID system="ORCID">0000-0003-2025-3147</ID>), AB(Gemini Observatory, 670 N. A’Ohoku Place, Hilo, HI 96720, USA ; Astrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool, L3 5RF, UK), AC(Department of Physics and Astronomy, Texas Christian University, Fort Worth, TX 76129, USA <ID system="ORCID">0000-0002-0740-8346</ID>), AD(Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain ; 16 Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain <ID system="ORCID">0000-0002-0084-572X</ID>), AE(Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA), AF(Apache Point Observatory and New Mexico State University, P.O. Box 59, Sunspot, NM, 88349-0059, USA ; Sternberg Astronomical Institute, Moscow State University, Universitetsky prosp. 13, Moscow, Russia <ID system="ORCID">0000-0002-3601-133X</ID>), AG(Pulse Ray Machining & Design, 4583 State Route 414, Beaver Dams, NY 14812 USA), AH(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), AI(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), AJ(Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain ; 16 Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain <ID system="ORCID">0000-0001-6143-8151</ID>), AK(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA; New Mexico State University, Las Cruces, NM 88003, USA <ID system="ORCID">0000-0001-9984-0891</ID>), AL(Observatório Nacional, Rio de Janeiro, RJ 20921-400, Brazil ; Steward Observatory, University of Arizona, Tucson, AZ 85721, USA), AM(The Ohio State University, Columbus, OH 43210, USA), AN(New England Optical Systems, 237 Cedar Hill Street, Marlborough, MA 01752 USA), AO(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA; Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain <ID system="ORCID">0000-0003-2184-6198</ID>), AP(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA; Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Laboratory, University Park PA 16802, USA), AQ(Pulse Ray Machining & Design, 4583 State Route 414, Beaver Dams, NY 14812 USA), AR(New Mexico State University, Las Cruces, NM 88003, USA <ID system="ORCID">0000-0002-9771-9622</ID>), AS(The Ohio State University, Columbus, OH 43210, USA <ID system="ORCID">0000-0001-7258-1834</ID>), AT(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), AU(Department of Physics, University of Wisconsin-Madison, 1150 University Avenue, Madison, WI 53706, USA <ID system="ORCID">0000-0001-5579-9233</ID>), AV(Steward Observatory, University of Arizona, Tucson, AZ 85721, USA), AW(Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain ; 16 Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain ; ELTE Gothard Astrophysical Observatory, H-9704 Szombathely, Szent Imre Herceg St. 112, Hungary ;), AX(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), AY(Dunlap Institute for Astronomy and Astrophysics, University of Toronto, Toronto, Ontario, Canada), AZ(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA; Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA <ID system="ORCID">0000-0002-1793-3689</ID>), BA(The Ohio State University, Columbus, OH 43210, USA <ID system="ORCID">0000-0002-7549-7766</ID>), BB(University of Texas at Austin, McDonald Observatory, Fort Davis, TX 79734, USA <ID system="ORCID">0000-0003-0509-2656</ID>), BC(Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA), BD(Steward Observatory, University of Arizona, Tucson, AZ 85721, USA; National Optical Astronomy Observatories, PO Box 26732, Tucson, AZ 85719, USA), BE(New England Optical Systems, 237 Cedar Hill Street, Marlborough, MA 01752 USA), BF(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), BG(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), BH(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), BI(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA; Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA), BJ(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), BK(Department of Astronomy, Yale University, PO Box 208101, New Haven, CT 06520-8101 USA <ID system="ORCID">0000-0002-6163-3472</ID>), BL(Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80303, USA ; Center for Astrophysics and Space Astronomy, University of Colorado Boulder, Boulder, CO 80303, USA), BM(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA <ID system="ORCID">0000-0003-1641-6222</ID>), BN(Institute for Advanced Study, Einstein Drive, Princeton, NJ 08540, USA ; Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON M5S 3H4, Canada; <ID system="ORCID">0000-0001-6855-442X</ID>), BO(Department of Physics and Astronomy, University of Utah, 115 S 1400 E #201 Salt Lake City, UT 84112 USA <ID system="ORCID">0000-0002-8725-1069</ID>), BP(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA; NASA Goddard Space Flight Center, Code 667, Greenbelt, MD 20771, USA <ID system="ORCID">0000-0001-5926-4471</ID>), BQ(School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT, UK ; Stellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark <ID system="ORCID">0000-0002-5714-8618</ID>), BR(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), BS(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., MS #20, Cambridge, MA 02138, USA), BT(School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT, UK), BU(New Mexico State University, Las Cruces, NM 88003, USA <ID system="ORCID">0000-0002-3101-5921</ID>), BV(Computer Sciences Corporation, 3700 San Martin Dr, Baltimore, MD 21218, USA ; Space Telescope Science Institute, 3700 San Martin Dr, Baltimore, MD 21218, USA <ID system="ORCID">0000-0003-0556-027X</ID>), BW(Department of Physics and Astronomy, University of Utah, 115 S 1400 E #201 Salt Lake City, UT 84112 USA), BX(Laboratoire AIM, CEA/DSM—CNRS— Univ. Paris Diderot—IRFU/SAp, Centre de Saclay, F-91191 Gif-sur-Yvette Cedex, France), BY(Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain ; 16 Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain <ID system="ORCID">0000-0002-1693-2721</ID>), BZ(Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA), CA(Osservatorio Astronomico di Padova—INAF, Vicolo dell’Osservatorio 5, I-35122 Padova, Italy ; Laboratório Interinstitucional de e-Astronomia—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil <ID system="ORCID">0000-0002-6301-3269</ID>), CB(Department of Astrophysical Sciences, Peyton Hall, Princeton University 08544, USA), CC(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA; New Mexico State University, Las Cruces, NM 88003, USA), CD(New Mexico State University, Las Cruces, NM 88003, USA <ID system="ORCID">0000-0001-7294-9766</ID>), CE(Stellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark ; Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, D-37077 Göttingen, Germany <ID system="ORCID">0000-0002-1463-726X</ID>), CF(Department of Physics and Astronomy, University of Utah, 115 S 1400 E #201 Salt Lake City, UT 84112 USA), CG(Apache Point Observatory and New Mexico State University, P.O. Box 59, Sunspot, NM, 88349-0059, USA <ID system="ORCID">0000-0001-7908-7724</ID>), CH(Apache Point Observatory and New Mexico State University, P.O. Box 59, Sunspot, NM, 88349-0059, USA), CI(Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Laboratory, University Park PA 16802, USA <ID system="ORCID">0000-0001-9596-7983</ID>), CJ(Space Science Institute, 4750 Walnut street, Suite 205, Boulder, CO 80301 USA <ID system="ORCID">0000-0002-0129-0316</ID>), CK(LESIA, CNRS, Université Pierre et Marie Curie, Universit Denis Diderot, Observatoire de Paris, F-92195 Meudon Cedex, France), CL(The Ohio State University, Columbus, OH 43210, USA), CM(US Naval Observatory, Flagstaff Station, 10391 West Naval Observatory Road, Flagstaff, AZ 86005-8521, USA <ID system="ORCID">0000-0002-4603-4834</ID>), CN(Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth, UK), CO(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA <ID system="ORCID">0000-0002-8190-7573</ID>), CP(Department of Physics, Yale University, 260 Whitney Ave, New Haven, CT 06520, USA), CQ(Institut Utinam, CNRS UMR6213, Université de Franche-Comté, OSU THETA Franche-Comté-Bourgogne, Observatoire de Besançon, BP 1615, F-25010 Besançon Cedex, France), CR(Laboratório Interinstitucional de e-Astronomia—LIneA, Rua Gal. José Cristino 77, Rio de Janeiro, RJ—20921-400, Brazil ; Universidade Federal do Rio de Janeiro, Observatório do Valongo, Ladeira do Pedro Antônio 43, 20080-090 Rio de Janeiro, Brazil), CS(Université de Nice Sophia-Antipolis, CNRS, Observatoire de Côte d’Azur, Laboratoire Lagrange, F-06304 Nice Cedex 4, France <ID system="ORCID">0000-0002-6590-1657</ID>), CT(Institute of Space Sciences (CSIC-IEEC) Campus UAB, Torre C5 parell 2 Bellaterra, E-08193 Spain), CU(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA <ID system="ORCID">0000-0003-1024-7739</ID>), CV(Stellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark <ID system="ORCID">0000-0002-6137-903X</ID>), CW(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA), CX(Department of Physics and Astronomy, Texas Christian University, Fort Worth, TX 76129, USA), CY(Department of Astronomy, University of Virginia, Charlottesville, VA 22904-4325, USA <ID system="ORCID">0000-0003-3248-3097</ID>), CZ(The Ohio State University, Columbus, OH 43210, USA <ID system="ORCID">0000-0001-7775-7261</ID>), DA(Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain ; 16 Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain)
%B The Astronomical Journal
%V 154
%D 2017
%8 September 1, 2017
%K Galaxy: abundances;  Galaxy: evolution;  Galaxy: formation;  Galaxy: kinematics and dynamics;  Galaxy: stellar content;  Galaxy: structure
%U http://adsabs.harvard.edu/abs/2017AJ....154...94M
%X The Apache Point Observatory Galactic Evolution Experiment (APOGEE), one 
of the programs in the Sloan Digital Sky Survey III (SDSS-III), has now 
completed its systematic, homogeneous spectroscopic survey sampling all 
major populations of the Milky Way. After a three-year observing 
campaign on the Sloan 2.5 m Telescope, APOGEE has collected a half 
million high-resolution (R ˜ 22,500), high signal-to-noise ratio 
(>100), infrared (1.51-1.70 μm) spectra for 146,000 stars, 
with time series information via repeat visits to most of these stars. 
This paper describes the motivations for the survey and its overall 
design—hardware, field placement, target selection, 
operations—and gives an overview of these aspects as well as the 
data reduction, analysis, and products. An index is also given to the 
complement of technical papers that describe various critical survey 
components in detail. Finally, we discuss the achieved survey 
performance and illustrate the variety of potential uses of the data 
products by way of a number of science demonstrations, which span from 
time series analysis of stellar spectral variations and radial velocity 
variations from stellar companions, to spatial maps of kinematics, 
metallicity, and abundance patterns across the Galaxy and as a function 
of age, to new views of the interstellar medium, the chemistry of star 
clusters, and the discovery of rare stellar species. As part of SDSS-III 
Data Release 12 and later releases, all of the APOGEE data products are 
publicly available.
%3 10.3847/1538-3881/aa784d
%= eprint: arXiv:1509.05420
%@ 0004-6256

%0 Journal Article
%T The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: tomographic BAO analysis of DR12 combined sample in configuration space
%A Wang, Yuting 
%A Zhao, Gong-Bo 
%A Chuang, Chia-Hsun 
%A Ross, Ashley J. 
%A Percival, Will J. 
%A Gil-Marín, Héctor 
%A Cuesta, Antonio J. 
%A Kitaura, Francisco-Shu 
%A Rodriguez-Torres, Sergio 
%A Brownstein, Joel R. 
%A Eisenstein, Daniel J. 
%A Ho, Shirley 
%A Kneib, Jean-Paul 
%A Olmstead, Matthew D. 
%A Prada, Francisco 
%A Rossi, Graziano 
%A Sánchez, Ariel G. 
%A Salazar-Albornoz, Salvador 
%A Thomas, Daniel 
%A Tinker, Jeremy 
%A Tojeiro, Rita 
%A Vargas-Magaña, Mariana 
%A Zhu, Fangzhou
%+ AA(National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, P. R. China; Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AB(National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, P. R. China; Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AC(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AD(Center for Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USA), AE(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AF(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AG(Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC- UB), Martí i Franquès 1, E-08028 Barcelona, Spain), AH(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AI(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AJ(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AK(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), AL(McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA; Lawrence Berkeley National Laboratory, 1 Cyclotron Rd, Berkeley, CA 94720, USA; Department of Physics, University of California, Berkeley, CA 94720, USA), AM(Laboratoire d'Astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, CH-1290 Versoix, Switzerland), AN(Department of Chemistry and Physics, King's College, 133 North River St, Wilkes Barre, PA 18711, USA), AO(Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain), AP(Department of Astronomy and Space Science, Sejong University, Seoul 143-747, Korea), AQ(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AR(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany; Universität Sternwarte Muänchen, Ludwig Maximilian Universität, München, Scheinerstrasse 1, D-81679 Munich, Germany), AS(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AT(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), AU(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK), AV(Instituto de Fisica, Universidad Nacional Autonoma de Mexico, Apdo. Postal 20-364, Mexico), AW(Department of Physics, Yale University, New Haven, CT 06511, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 469
%D 2017
%8 August 1, 2017
%P 3762-3774
%K dark energy;  distance scale
%U http://adsabs.harvard.edu/abs/2017MNRAS.469.3762W
%X We perform a tomographic baryon acoustic oscillations (BAOs) analysis 
using the two-point galaxy correlation function measured from the 
combined sample of Baryon Oscillation Spectroscopic Survey Data Release 
12 (BOSS DR12), which covers the redshift range of 0.2 < z < 0.75. 
Upon splitting the sample into multiple overlapping redshift slices to 
extract the redshift information of galaxy clustering, we obtain a 
measurement of D<SUB>A</SUB>(z)/r<SUB>d</SUB> and H(z)r<SUB>d</SUB> at 
nine effective redshifts with the full covariance matrix calibrated 
using MultiDark-Patchy mock catalogues. Using the reconstructed galaxy 
catalogues, we obtain the precision of 1.3-2.2 per cent for 
D<SUB>A</SUB>(z)/r<SUB>d</SUB> and 2.1-6.0 per cent for 
H(z)r<SUB>d</SUB>. To quantify the gain from the tomographic 
information, we compare the constraints on the cosmological parameters 
using our nine-bin BAO measurements, the consensus three-bin BAO and 
redshift space distortion measurements at three effective redshifts in 
Alam et al., and the non-tomographic (one-bin) BAO measurement at a 
single effective redshift. Comparing the nine-bin with one-bin 
constraint result, it can improve the dark energy Figure of Merit by a 
factor of 1.24 for the Chevallier-Polarski-Linder parametrization for 
equation-of-state parameter w<SUB>DE</SUB>. The errors of w<SUB>0</SUB> 
and w<SUB>a</SUB> from nine-bin constraints are slightly improved when 
compared to the three-bin constraint result.
%3 10.1093/mnras/stx1090
%= eprint: arXiv:1607.03154
%@ 0035-8711

%0 Journal Article
%T Modelling the large-scale redshift-space 3-point correlation function of galaxies
%A Slepian, Zachary 
%A Eisenstein, Daniel J.
%+ AA(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley CA 94720, USA; Berkeley Center for Cosmological Physics, University of California, Berkeley, CA 94720, USA), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 469
%D 2017
%8 August 1, 2017
%P 2059-2076
%K cosmology: theory;  distance scale;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2017MNRAS.469.2059S
%X We present a configuration-space model of the large-scale galaxy 3-point 
correlation function (3PCF) based on leading-order perturbation theory 
and including redshift-space distortions (RSD). This model should be 
useful in extracting distance-scale information from the 3PCF via the 
baryon acoustic oscillation method. We include the first redshift-space 
treatment of biasing by the baryon-dark matter relative velocity. 
Overall, on large scales the effect of RSD is primarily a 
renormalization of the 3PCF that is roughly independent of both physical 
scale and triangle opening angle; for our adopted Ω<SUB>m</SUB> 
and bias values, the rescaling is a factor of ˜1.8. We also present 
an efficient scheme for computing 3PCF predictions from our model, 
important for allowing fast exploration of the space of cosmological 
parameters in future analyses.
%3 10.1093/mnras/stx490
%= eprint: arXiv:1607.03109
%@ 0035-8711

%0 Journal Article
%T Detection of baryon acoustic oscillation features in the large-scale three-point correlation function of SDSS BOSS DR12 CMASS galaxies
%A Slepian, Zachary 
%A Eisenstein, Daniel J. 
%A Brownstein, Joel R. 
%A Chuang, Chia-Hsun 
%A Gil-Marín, Héctor 
%A Ho, Shirley 
%A Kitaura, Francisco-Shu 
%A Percival, Will J. 
%A Ross, Ashley J. 
%A Rossi, Graziano 
%A Seo, Hee-Jong 
%A Slosar, Anže 
%A Vargas-Magaña, Mariana
%+ AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AC(Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA), AD(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AE(Sorbonne Universités, Institut Lagrange de Paris (ILP), 98 bis Boulevard Arago, F-75014 Paris, France; Laboratoire de Physique Nucléaire et de Hautes Energies, Université Pierre et Marie Curie, 4 Place Jussieu, F-75005 Paris, France), AF(Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley CA 94720, USA; McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA; Department of Physics, University of California, Berkeley, CA 94720, USA), AG(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AH(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AI(Center for Cosmology and Astroparticle Physics, Department of Physics, The Ohio State University, OH 43210, USA), AJ(Department of Physics and Astronomy, Sejong University, Seoul, 143-747, Korea), AK(Department of Physics and Astronomy, Ohio University, Clippinger Labs, Athens, OH 45701, USA), AL(Brookhaven National Laboratory, Upton, NY 11973, USA), AM(Instituto de Física, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, México)
%B Monthly Notices of the Royal Astronomical Society
%V 469
%D 2017
%8 August 1, 2017
%P 1738-1751
%K cosmology: observations;  distance scale;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2017MNRAS.469.1738S
%X We present the large-scale three-point correlation function (3PCF) of 
the Sloan Digital Sky Survey DR12 Constant stellar Mass (CMASS) sample 
of 777 202 Luminous Red Galaxies, the largest-ever sample used for a 
3PCF or bispectrum measurement. We make the first high-significance 
(4.5σ) detection of baryon acoustic oscillations (BAO) in the 
3PCF. Using these acoustic features in the 3PCF as a standard ruler, we 
measure the distance to z = 0.57 to 1.7 per cent precision (statistical 
plus systematic). We find D<SUB>V</SUB> = 2024 ± 29 Mpc (stat) 
± 20 Mpc (sys) for our fiducial cosmology (consistent with Planck 
2015) and bias model. This measurement extends the use of the BAO 
technique from the two-point correlation function (2PCF) and power 
spectrum to the 3PCF and opens an avenue for deriving additional 
cosmological distance information from future large-scale structure 
redshift surveys such as DESI. Our measured distance scale from the 3PCF 
is fairly independent from that derived from the pre-reconstruction 2PCF 
and is equivalent to increasing the length of BOSS by roughly 10 per 
cent; reconstruction appears to lower the independence of the distance 
measurements. Fitting a model including tidal tensor bias yields a 
moderate-significance (2.6σ) detection of this bias with a value 
in agreement with the prediction from local Lagrangian biasing.
%3 10.1093/mnras/stx488
%= eprint: arXiv:1607.06097
%@ 0035-8711

%0 Journal Article
%T The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: on the measurement of growth rate using galaxy correlation functions
%A Satpathy, Siddharth 
%A Alam, Shadab 
%A Ho, Shirley 
%A White, Martin 
%A Bahcall, Neta A. 
%A Beutler, Florian 
%A Brownstein, Joel R. 
%A Chuang, Chia-Hsun 
%A Eisenstein, Daniel J. 
%A Grieb, Jan Niklas 
%A Kitaura, Francisco 
%A Olmstead, Matthew D. 
%A Percival, Will J. 
%A Salazar-Albornoz, Salvador 
%A Sánchez, Ariel G. 
%A Seo, Hee-Jong 
%A Thomas, Daniel 
%A Tinker, Jeremy L. 
%A Tojeiro, Rita
%+ AA(Department of Physics, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA; The McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA), AB(Department of Physics, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA; The McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA), AC(Department of Physics, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA; The McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA; Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; Departments of Physics and Astronomy, University of California, Berkeley, CA 94720, USA), AD(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; Departments of Physics and Astronomy, University of California, Berkeley, CA 94720, USA), AE(Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA), AF(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AG(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AH(Departamento de Física Teórica, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AI(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), AJ(Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Scheinerstrasse 1, D-81679 Munich, Germany; Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AK(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; Departments of Physics and Astronomy, University of California, Berkeley, CA 94720, USA; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AL(Department of Chemistry and Physics, King's College, 133 North River St, Wilkes Barre, PA 18711, USA), AM(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AN(Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Scheinerstrasse 1, D-81679 Munich, Germany; Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AO(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AP(Department of Physics and Astronomy, Ohio University, Clippinger Labs, Athens, OH 45701, USA), AQ(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AR(Center for Cosmology and Particle Physics and Department of Physics, New York University, New York, NY 10003, USA), AS(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KY16 9SS, UK)
%B Monthly Notices of the Royal Astronomical Society
%V 469
%D 2017
%8 August 1, 2017
%P 1369-1382
%K galaxies: statistics;  dark energy;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2017MNRAS.469.1369S
%X We present a measurement of the linear growth rate of structure, f, from 
the Sloan Digital Sky Survey III (SDSS-III) Baryon Oscillation 
Spectroscopic Survey (BOSS) Data Release 12 (DR12) using convolution 
Lagrangian perturbation theory (CLPT) with Gaussian streaming redshift 
space distortions (GSRSD) to model the two-point statistics of BOSS 
galaxies in DR12. The BOSS-DR12 data set includes 1198 006 massive 
galaxies spread over the redshift range 0.2 < z < 0.75. These 
galaxy samples are categorized in three redshift bins. Using CLPT-GSRSD 
in our analysis of the combined sample of the three redshift bins, we 
report measurements of fσ<SUB>8</SUB> for the three redshift bins. 
We find fσ<SUB>8</SUB> = 0.430 ± 0.054 at z<SUB>eff</SUB> = 
0.38, fσ<SUB>8</SUB> = 0.452 ± 0.057 at z<SUB>eff</SUB> = 
0.51 and fσ<SUB>8</SUB> = 0.457 ± 0.052 at z<SUB>eff</SUB> 
= 0.61. Our results are consistent with the predictions of Planck 
Λ cold dark matter-general relativity. Our constraints on the 
growth rates of structure in the Universe at different redshifts serve 
as a useful probe, which can help distinguish between a model of the 
Universe based on dark energy and models based on modified theories of 
gravity. This paper is part of a set that analyses the final galaxy 
clustering data set from BOSS. The measurements and likelihoods 
presented here are combined with others in Alam et al., to produce the 
final cosmological constraints from BOSS.
%3 10.1093/mnras/stx883
%= eprint: arXiv:1607.03148
%@ 0035-8711

%0 Journal Article
%T Deriving photometric redshifts using fuzzy archetypes and self-organizing maps - II. Implementation
%A Speagle, Joshua S. 
%A Eisenstein, Daniel J.
%+ AA(Department of Astronomy, Harvard University, 60 Garden St, MS 46, Cambridge, MA 02138, USA; Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwanoha 5-1-5, Kashiwa, Chiba 277-8583, Japan), AB(Department of Astronomy, Harvard University, 60 Garden St, MS 46, Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 469
%D 2017
%8 July 1, 2017
%P 1205-1224
%K methods: statistical;  techniques: photometric;  galaxies: distances and redshifts
%U http://adsabs.harvard.edu/abs/2017MNRAS.469.1205S
%X With an eye towards the computational requirements of future large-scale 
surveys such as Euclid and Large Synoptic Survey Telescope (LSST) that 
will require photometric redshifts (photo-z's) for ≳ 10<SUP>9</SUP> 
objects, we investigate a variety of ways that 'fuzzy archetypes' can be 
used to improve photometric redshifts and explore their respective 
statistical interpretations. We characterize their relative performance 
using an idealized LSST ugrizY and Euclid YJH mock catalogue of 10 000 
objects spanning z = 0-6 at Y = 24 mag. We find most schemes are able to 
robustly identify redshift probability distribution functions that are 
multimodal and/or poorly constrained. Once these objects are flagged and 
removed, the results are generally in good agreement with the strict 
accuracy requirements necessary to meet Euclid weak lensing goals for 
most redshifts between 0.8 ≲ z ≲ 2. These results demonstrate 
the statistical robustness and flexibility that can be gained by 
combining template-fitting and machine-learning methods and provide 
useful insights into how astronomers can further exploit the 
colour-redshift relation.
%3 10.1093/mnras/stx510
%@ 0035-8711

%0 Journal Article
%T Deriving photometric redshifts using fuzzy archetypes and self-organizing maps - I. Methodology
%A Speagle, Joshua S. 
%A Eisenstein, Daniel J.
%+ AA(Department of Astronomy, Harvard University, 60 Garden St., MS 46, Cambridge, MA 02138, USA; Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwanoha 5-1-5, Kashiwa, Chiba 277-8583, Japan), AB(Department of Astronomy, Harvard University, 60 Garden St., MS 46, Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 469
%D 2017
%8 July 1, 2017
%P 1186-1204
%K methods: statistical;  techniques: photometric;  galaxies: distances and redshifts
%U http://adsabs.harvard.edu/abs/2017MNRAS.469.1186S
%X We propose a method to substantially increase the flexibility and power 
of template fitting-based photometric redshifts by transforming a large 
number of galaxy spectral templates into a corresponding collection of 
'fuzzy archetypes' using a suitable set of perturbative priors designed 
to account for empirical variation in dust attenuation and emission-line 
strengths. To bypass widely separated degeneracies in parameter space 
(e.g. the redshift-reddening degeneracy), we train self-organizing maps 
(SOMs) on large 'model catalogues' generated from Monte Carlo sampling 
of our fuzzy archetypes to cluster the predicted observables in a 
topologically smooth fashion. Subsequent sampling over the SOM then 
allows full reconstruction of the relevant probability distribution 
functions (PDFs). This combined approach enables the multimodal 
exploration of known variation among galaxy spectral energy 
distributions with minimal modelling assumptions. We demonstrate the 
power of this approach to recover full redshift PDFs using discrete 
Markov chain Monte Carlo sampling methods combined with SOMs constructed 
from Large Synoptic Survey Telescope ugrizY and Euclid YJH mock 
photometry.
%3 10.1093/mnras/stw1485
%@ 0035-8711

%0 Journal Article
%T The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: towards a computationally efficient analysis without informative priors
%A Pellejero-Ibanez, Marcos 
%A Chuang, Chia-Hsun 
%A Rubiño-Martín, J. A. 
%A Cuesta, Antonio J. 
%A Wang, Yuting 
%A Zhao, Gongbo 
%A Ross, Ashley J. 
%A Rodríguez-Torres, Sergio 
%A Prada, Francisco 
%A Slosar, Anže 
%A Vazquez, Jose A. 
%A Alam, Shadab 
%A Beutler, Florian 
%A Eisenstein, Daniel J. 
%A Gil-Marín, Héctor 
%A Grieb, Jan Niklas 
%A Ho, Shirley 
%A Kitaura, Francisco-Shu 
%A Percival, Will J. 
%A Rossi, Graziano 
%A Salazar-Albornoz, Salvador 
%A Samushia, Lado 
%A Sánchez, Ariel G. 
%A Satpathy, Siddharth 
%A Seo, Hee-Jong 
%A Tinker, Jeremy L. 
%A Tojeiro, Rita 
%A Vargas-Magaña, Mariana 
%A Brownstein, Joel R. 
%A Nichol, Robert C. 
%A Olmstead, Matthew D.
%+ AA(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200 La Laguna, Tenerife, Spain; Departamento Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain; Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AB(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AC(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38200 La Laguna, Tenerife, Spain; Departamento Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), AD(Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, E-08028 Barcelona, Spain), AE(National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AF(National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China; Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AG(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; Center for Cosmology and Astroparticle Physics, Department of Physics, The Ohio State University, OH 43210, USA), AH(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica M8, Universidad Autonoma de Madrid (UAM), Cantoblanco, E-28049 Madrid, Spain), AI(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía, E-18080 Granada, Spain), AJ(Brookhaven National Laboratory, Upton, NY 11973, USA), AK(Brookhaven National Laboratory, Upton, NY 11973, USA), AL(Department of Physics, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA; The McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA), AM(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA), AN(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA), AO(Sorbonne Universités, Institut Lagrange de Paris (ILP), 98 bis Boulevard Arago, F-75014 Paris, France; Laboratoire de Physique Nucléaire et de Hautes Energies, Université Pierre et Marie Curie, 4 Place Jussieu, F-75005 Paris, France), AP(Universitäts-Sternwarte München, Scheinerstrasse 1, D-81679 Munich, Germany; Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AQ(Department of Physics, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA; The McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA), AR(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA; Departments of Physics and Astronomy, University of California, Berkeley, CA 94720, USA), AS(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AT(Department of Physics and Astronomy, Sejong University, Seoul 143-747, Korea), AU(Universitäts-Sternwarte München, Scheinerstrasse 1, D-81679 Munich, Germany; Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AV(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; Kansas State University, Manhattan, KS 66506, USA; National Abastumani Astrophysical Observatory, Ilia State University, 2A Kazbegi Ave., GE-1060 Tbilisi, Georgia), AW(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AX(Department of Physics, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA; The McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave., Pittsburgh, PA 15213, USA), AY(Department of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, OH 45701, USA), AZ(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), BA(School of Physics and Astronomy, University of St Andrews, St Andrews, KY16 9SS, UK), BB(Instituto de Fisica, Universidad Nacional Autónoma de México, Ciudad de México, Apdo. Postal 20-364, México), BC(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), BD(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), BE(Department of Chemistry and Physics, King's College, 133 North River St, Wilkes Barre, PA 18711, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 468
%D 2017
%8 July 1, 2017
%P 4116-4133
%K cosmological parameters;  distance scale;  large-scale structure of Universe;  cosmology: observations
%U http://adsabs.harvard.edu/abs/2017MNRAS.468.4116P
%X We develop a new computationally efficient methodology called 
double-probe analysis with the aim of minimizing informative priors 
(those coming from extra probes) in the estimation of cosmological 
parameters. Using our new methodology, we extract the dark energy 
model-independent cosmological constraints from the joint data sets of 
the Baryon Oscillation Spectroscopic Survey (BOSS) galaxy sample and 
Planck cosmic microwave background (CMB) measurements. We measure the 
mean values and covariance matrix of {R, l<SUB>a</SUB>, 
Ω<SUB>b</SUB>h<SUP>2</SUP>, n<SUB>s</SUB>, log(A<SUB>s</SUB>), 
Ω<SUB>k</SUB>, H(z), D<SUB>A</SUB>(z), 
f(z)σ<SUB>8</SUB>(z)}, which give an efficient summary of the 
Planck data and two-point statistics from the BOSS galaxy sample. The 
CMB shift parameters are R=√{Ω _m H_0^2} r(z_*) and 
l<SUB>a</SUB> = πr(z<SUB>*</SUB>)/r<SUB>s</SUB>(z<SUB>*</SUB>), where 
z<SUB>*</SUB> is the redshift at the last scattering surface, and 
r(z<SUB>*</SUB>) and r<SUB>s</SUB>(z<SUB>*</SUB>) denote our comoving 
distance to the z<SUB>*</SUB> and sound horizon at z<SUB>*</SUB>, 
respectively; Ω<SUB>b</SUB> is the baryon fraction at z = 0. This 
approximate methodology guarantees that we will not need to put 
informative priors on the cosmological parameters that galaxy clustering 
is unable to constrain, I.e. Ω<SUB>b</SUB>h<SUP>2</SUP> and 
n<SUB>s</SUB>. The main advantage is that the computational time 
required for extracting these parameters is decreased by a factor of 60 
with respect to exact full-likelihood analyses. The results obtained 
show no tension with the flat Λ cold dark matter (ΛCDM) 
cosmological paradigm. By comparing with the full-likelihood exact 
analysis with fixed dark energy models, on one hand we demonstrate that 
the double-probe method provides robust cosmological parameter 
constraints that can be conveniently used to study dark energy models, 
and on the other hand we provide a reliable set of measurements assuming 
dark energy models to be used, for example, in distance estimations. We 
extend our study to measure the sum of the neutrino mass using different 
methodologies, including double-probe analysis (introduced in this 
study), full-likelihood analysis and single-probe analysis. From 
full-likelihood analysis, we obtain Σm<SUB>ν</SUB> < 0.12 
(68 per cent), assuming ΛCDM and Σm<SUB>ν</SUB> < 
0.20 (68 per cent) assuming owCDM. We also find that there is degeneracy 
between observational systematics and neutrino masses, which suggests 
that one should take great care when estimating these parameters in the 
case of not having control over the systematics of a given sample.
%3 10.1093/mnras/stx751
%@ 0035-8711

%0 Journal Article
%T Sloan Digital Sky Survey IV: Mapping the Milky Way, Nearby Galaxies, and the Distant Universe
%A Blanton, Michael R. 
%A Bershady, Matthew A. 
%A Abolfathi, Bela 
%A Albareti, Franco D. 
%A Allende Prieto, Carlos 
%A Almeida, Andres 
%A Alonso-García, Javier 
%A Anders, Friedrich 
%A Anderson, Scott F. 
%A Andrews, Brett 
%A Aquino-Ortíz, Erik 
%A Aragón-Salamanca, Alfonso 
%A Argudo-Fernández, Maria 
%A Armengaud, Eric 
%A Aubourg, Eric 
%A Avila-Reese, Vladimir 
%A Badenes, Carles 
%A Bailey, Stephen 
%A Barger, Kathleen A. 
%A Barrera-Ballesteros, Jorge 
%A Bartosz, Curtis 
%A Bates, Dominic 
%A Baumgarten, Falk 
%A Bautista, Julian 
%A Beaton, Rachael 
%A Beers, Timothy C. 
%A Belfiore, Francesco 
%A Bender, Chad F. 
%A Berlind, Andreas A. 
%A Bernardi, Mariangela 
%A Beutler, Florian 
%A Bird, Jonathan C. 
%A Bizyaev, Dmitry 
%A Blanc, Guillermo A. 
%A Blomqvist, Michael 
%A Bolton, Adam S. 
%A Boquien, Médéric 
%A Borissova, Jura 
%A van den Bosch, Remco 
%A Bovy, Jo 
%A Brandt, William N. 
%A Brinkmann, Jonathan 
%A Brownstein, Joel R. 
%A Bundy, Kevin 
%A Burgasser, Adam J. 
%A Burtin, Etienne 
%A Busca, Nicolás G. 
%A Cappellari, Michele 
%A Delgado Carigi, Maria Leticia 
%A Carlberg, Joleen K. 
%A Carnero Rosell, Aurelio 
%A Carrera, Ricardo 
%A Chanover, Nancy J. 
%A Cherinka, Brian 
%A Cheung, Edmond 
%A Gómez Maqueo Chew, Yilen 
%A Chiappini, Cristina 
%A Doohyun Choi, Peter 
%A Chojnowski, Drew 
%A Chuang, Chia-Hsun 
%A Chung, Haeun 
%A Cirolini, Rafael Fernando 
%A Clerc, Nicolas 
%A Cohen, Roger E. 
%A Comparat, Johan 
%A da Costa, Luiz 
%A Cousinou, Marie-Claude 
%A Covey, Kevin 
%A Crane, Jeffrey D. 
%A Croft, Rupert A. C. 
%A Cruz-Gonzalez, Irene 
%A Garrido Cuadra, Daniel 
%A Cunha, Katia 
%A Damke, Guillermo J. 
%A Darling, Jeremy 
%A Davies, Roger 
%A Dawson, Kyle 
%A de la Macorra, Axel 
%A Dell'Agli, Flavia 
%A De Lee, Nathan 
%A Delubac, Timothée 
%A Di Mille, Francesco 
%A Diamond-Stanic, Aleks 
%A Cano-Díaz, Mariana 
%A Donor, John 
%A José Downes, Juan 
%A Drory, Niv 
%A du Mas des Bourboux, Hélion 
%A Duckworth, Christopher J. 
%A Dwelly, Tom 
%A Dyer, Jamie 
%A Ebelke, Garrett 
%A Eigenbrot, Arthur D. 
%A Eisenstein, Daniel J. 
%A Emsellem, Eric 
%A Eracleous, Mike 
%A Escoffier, Stephanie 
%A Evans, Michael L. 
%A Fan, Xiaohui 
%A Fernández-Alvar, Emma 
%A Fernandez-Trincado, J. G. 
%A Feuillet, Diane K. 
%A Finoguenov, Alexis 
%A Fleming, Scott W. 
%A Font-Ribera, Andreu 
%A Fredrickson, Alexander 
%A Freischlad, Gordon 
%A Frinchaboy, Peter M. 
%A Fuentes, Carla E. 
%A Galbany, Lluís 
%A Garcia-Dias, R. 
%A García-Hernández, D. A. 
%A Gaulme, Patrick 
%A Geisler, Doug 
%A Gelfand, Joseph D. 
%A Gil-Marín, Héctor 
%A Gillespie, Bruce A. 
%A Goddard, Daniel 
%A Gonzalez-Perez, Violeta 
%A Grabowski, Kathleen 
%A Green, Paul J. 
%A Grier, Catherine J. 
%A Gunn, James E. 
%A Guo, Hong 
%A Guy, Julien 
%A Hagen, Alex 
%A Hahn, ChangHoon 
%A Hall, Matthew 
%A Harding, Paul 
%A Hasselquist, Sten 
%A Hawley, Suzanne L. 
%A Hearty, Fred 
%A Gonzalez Hernández, Jonay I. 
%A Ho, Shirley 
%A Hogg, David W. 
%A Holley-Bockelmann, Kelly 
%A Holtzman, Jon A. 
%A Holzer, Parker H. 
%A Huehnerhoff, Joseph 
%A Hutchinson, Timothy A. 
%A Hwang, Ho Seong 
%A Ibarra-Medel, Héctor J. 
%A da Silva Ilha, Gabriele 
%A Ivans, Inese I. 
%A Ivory, KeShawn 
%A Jackson, Kelly 
%A Jensen, Trey W. 
%A Johnson, Jennifer A. 
%A Jones, Amy 
%A Jönsson, Henrik 
%A Jullo, Eric 
%A Kamble, Vikrant 
%A Kinemuchi, Karen 
%A Kirkby, David 
%A Kitaura, Francisco-Shu 
%A Klaene, Mark 
%A Knapp, Gillian R. 
%A Kneib, Jean-Paul 
%A Kollmeier, Juna A. 
%A Lacerna, Ivan 
%A Lane, Richard R. 
%A Lang, Dustin 
%A Law, David R. 
%A Lazarz, Daniel 
%A Lee, Youngbae 
%A Le Goff, Jean-Marc 
%A Liang, Fu-Heng 
%A Li, Cheng 
%A Li, Hongyu 
%A Lian, Jianhui 
%A Lima, Marcos 
%A Lin, Lihwai 
%A Lin, Yen-Ting 
%A Bertran de Lis, Sara 
%A Liu, Chao 
%A de Icaza Lizaola, Miguel Angel C. 
%A Long, Dan 
%A Lucatello, Sara 
%A Lundgren, Britt 
%A MacDonald, Nicholas K. 
%A Deconto Machado, Alice 
%A MacLeod, Chelsea L. 
%A Mahadevan, Suvrath 
%A Geimba Maia, Marcio Antonio 
%A Maiolino, Roberto 
%A Majewski, Steven R. 
%A Malanushenko, Elena 
%A Malanushenko, Viktor 
%A Manchado, Arturo 
%A Mao, Shude 
%A Maraston, Claudia 
%A Marques-Chaves, Rui 
%A Masseron, Thomas 
%A Masters, Karen L. 
%A McBride, Cameron K. 
%A McDermid, Richard M. 
%A McGrath, Brianne 
%A McGreer, Ian D. 
%A Medina Peña, Nicolás 
%A Melendez, Matthew 
%A Merloni, Andrea 
%A Merrifield, Michael R. 
%A Meszaros, Szabolcs 
%A Meza, Andres 
%A Minchev, Ivan 
%A Minniti, Dante 
%A Miyaji, Takamitsu 
%A More, Surhud 
%A Mulchaey, John 
%A Müller-Sánchez, Francisco 
%A Muna, Demitri 
%A Munoz, Ricardo R. 
%A Myers, Adam D. 
%A Nair, Preethi 
%A Nandra, Kirpal 
%A Correa do Nascimento, Janaina 
%A Negrete, Alenka 
%A Ness, Melissa 
%A Newman, Jeffrey A. 
%A Nichol, Robert C. 
%A Nidever, David L. 
%A Nitschelm, Christian 
%A Ntelis, Pierros 
%A O'Connell, Julia E. 
%A Oelkers, Ryan J. 
%A Oravetz, Audrey 
%A Oravetz, Daniel 
%A Pace, Zach 
%A Padilla, Nelson 
%A Palanque-Delabrouille, Nathalie 
%A Alonso Palicio, Pedro 
%A Pan, Kaike 
%A Parejko, John K. 
%A Parikh, Taniya 
%A Pâris, Isabelle 
%A Park, Changbom 
%A Patten, Alim Y. 
%A Peirani, Sebastien 
%A Pellejero-Ibanez, Marcos 
%A Penny, Samantha 
%A Percival, Will J. 
%A Perez-Fournon, Ismael 
%A Petitjean, Patrick 
%A Pieri, Matthew M. 
%A Pinsonneault, Marc 
%A Pisani, Alice 
%A Poleski, Radosław 
%A Prada, Francisco 
%A Prakash, Abhishek 
%A Queiroz, Anna Bárbara de Andrade 
%A Raddick, M. Jordan 
%A Raichoor, Anand 
%A Barboza Rembold, Sandro 
%A Richstein, Hannah 
%A Riffel, Rogemar A. 
%A Riffel, Rogério 
%A Rix, Hans-Walter 
%A Robin, Annie C. 
%A Rockosi, Constance M. 
%A Rodríguez-Torres, Sergio 
%A Roman-Lopes, A. 
%A Román-Zúñiga, Carlos 
%A Rosado, Margarita 
%A Ross, Ashley J. 
%A Rossi, Graziano 
%A Ruan, John 
%A Ruggeri, Rossana 
%A Rykoff, Eli S. 
%A Salazar-Albornoz, Salvador 
%A Salvato, Mara 
%A Sánchez, Ariel G. 
%A Aguado, D. S. 
%A Sánchez-Gallego, José R. 
%A Santana, Felipe A. 
%A Santiago, Basílio Xavier 
%A Sayres, Conor 
%A Schiavon, Ricardo P. 
%A da Silva Schimoia, Jaderson 
%A Schlafly, Edward F. 
%A Schlegel, David J. 
%A Schneider, Donald P. 
%A Schultheis, Mathias 
%A Schuster, William J. 
%A Schwope, Axel 
%A Seo, Hee-Jong 
%A Shao, Zhengyi 
%A Shen, Shiyin 
%A Shetrone, Matthew 
%A Shull, Michael 
%A Simon, Joshua D. 
%A Skinner, Danielle 
%A Skrutskie, M. F. 
%A Slosar, Anže 
%A Smith, Verne V. 
%A Sobeck, Jennifer S. 
%A Sobreira, Flavia 
%A Somers, Garrett 
%A Souto, Diogo 
%A Stark, David V. 
%A Stassun, Keivan 
%A Stauffer, Fritz 
%A Steinmetz, Matthias 
%A Storchi-Bergmann, Thaisa 
%A Streblyanska, Alina 
%A Stringfellow, Guy S. 
%A Suárez, Genaro 
%A Sun, Jing 
%A Suzuki, Nao 
%A Szigeti, Laszlo 
%A Taghizadeh-Popp, Manuchehr 
%A Tang, Baitian 
%A Tao, Charling 
%A Tayar, Jamie 
%A Tembe, Mita 
%A Teske, Johanna 
%A Thakar, Aniruddha R. 
%A Thomas, Daniel 
%A Thompson, Benjamin A. 
%A Tinker, Jeremy L. 
%A Tissera, Patricia 
%A Tojeiro, Rita 
%A Hernandez Toledo, Hector 
%A de la Torre, Sylvain 
%A Tremonti, Christy 
%A Troup, Nicholas W. 
%A Valenzuela, Octavio 
%A Martinez Valpuesta, Inma 
%A Vargas-González, Jaime 
%A Vargas-Magaña, Mariana 
%A Vazquez, Jose Alberto 
%A Villanova, Sandro 
%A Vivek, M. 
%A Vogt, Nicole 
%A Wake, David 
%A Walterbos, Rene 
%A Wang, Yuting 
%A Weaver, Benjamin Alan 
%A Weijmans, Anne-Marie 
%A Weinberg, David H. 
%A Westfall, Kyle B. 
%A Whelan, David G. 
%A Wild, Vivienne 
%A Wilson, John 
%A Wood-Vasey, W. M. 
%A Wylezalek, Dominika 
%A Xiao, Ting 
%A Yan, Renbin 
%A Yang, Meng 
%A Ybarra, Jason E. 
%A Yèche, Christophe 
%A Zakamska, Nadia 
%A Zamora, Olga 
%A Zarrouk, Pauline 
%A Zasowski, Gail 
%A Zhang, Kai 
%A Zhao, Gong-Bo 
%A Zheng, Zheng 
%A Zheng, Zheng 
%A Zhou, Xu 
%A Zhou, Zhi-Min 
%A Zhu, Guangtun B. 
%A Zoccali, Manuela 
%A Zou, Hu
%+ AA(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA <ID system="ORCID">0000-0003-1641-6222</ID>), AB(Department of Astronomy, University of Wisconsin-Madison, 475 N. Charter St., Madison, WI 53726, USA <ID system="ORCID">0000-0002-3131-4374</ID>), AC(Department of Physics and Astronomy, University of California, Irvine, Irvine, CA 92697, USA), AD(Instituto de Física Teórica (IFT) UAM/CSIC, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain ; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain ;), AE(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain <ID system="ORCID">0000-0002-0084-572X</ID>), AF(Departamento de Física, Facultad de Ciencias, Universidad de La Serena, Cisternas 1200, La Serena, Chile), AG(Unidad de Astronomía, Fac. Cs. Básicas, Universidad de Antofagasta, Avda. U. de Antofagasta 02800, Antofagasta, Chile ; Instituto Milenio de Astrofísica, Av. Vicuña Mackenna 4860, Macul, Santiago, Chile <ID system="ORCID">0000-0003-3496-3772</ID>), AH(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AI(Department of Astronomy, Box 351580, University of Washington, Seattle, WA 98195, USA), AJ(PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA <ID system="ORCID">0000-0001-8085-5890</ID>), AK(Instituto de Astronomía, Universidad Nacional Autónoma de México, A.P. 70-264, 04510, México, D.F., México), AL(School of Physics & Astronomy, University of Nottingham, Nottingham, NG7 2RD, UK <ID system="ORCID">0000-0001-8215-1256</ID>), AM(Unidad de Astronomía, Fac. Cs. Básicas, Universidad de Antofagasta, Avda. U. de Antofagasta 02800, Antofagasta, Chile), AN(CEA, Centre de Saclay, IRFU, F-91191, Gif-sur-Yvette, France), AO(APC, University of Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cite, France), AP(Instituto de Astronomía, Universidad Nacional Autónoma de México, A.P. 70-264, 04510, México, D.F., México), AQ(PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA <ID system="ORCID">0000-0003-3494-343X</ID>), AR(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AS(Department of Physics and Astronomy, Texas Christian University, Fort Worth, TX 76129, USA <ID system="ORCID">0000-0001-5817-0932</ID>), AT(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA <ID system="ORCID">0000-0003-2405-7258</ID>), AU(Department of Astronomy, Box 351580, University of Washington, Seattle, WA 98195, USA), AV(School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, KY16 9SS, UK), AW(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany; Humboldt-Universität zu Berlin, Institut für Physik, Newtonstrasse 15, D-12589, Berlin, Germany), AX(Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA), AY(The Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA <ID system="ORCID">0000-0002-1691-8217</ID>), AZ(Department of Physics and JINA Center for the Evolution of the Elements, University of Notre Dame, Notre Dame, IN 46556 USA <ID system="ORCID">0000-0003-4573-6233</ID>), BA(Cavendish Laboratory, University of Cambridge, 19 J. J. Thomson Avenue, Cambridge CB3 0HE, UK ; Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK), BB(Steward Observatory, The University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA <ID system="ORCID">0000-0003-4384-7220</ID>), BC(Vanderbilt University, Department of Physics & Astronomy, 6301 Stevenson Center Ln., Nashville, TN 37235, USA <ID system="ORCID">0000-0002-1814-2002</ID>), BD(Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USA), BE(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK), BF(Vanderbilt University, Department of Physics & Astronomy, 6301 Stevenson Center Ln., Nashville, TN 37235, USA), BG(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA ; Sternberg Astronomical Institute, Moscow State University, Moscow <ID system="ORCID">0000-0002-3601-133X</ID>), BH(The Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA), BI(Aix Marseille Univ, CNRS, LAM, Laboratoire d’Astrophysique de Marseille, Marseille, France), BJ(Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA; National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA), BK(Unidad de Astronomía, Fac. Cs. Básicas, Universidad de Antofagasta, Avda. U. de Antofagasta 02800, Antofagasta, Chile), BL(Instituto Milenio de Astrofísica, Av. Vicuña Mackenna 4860, Macul, Santiago, Chile ; Departamento de Fśica y Astronomía, Universidad de Valparaiíso, Av. Gran Bretan a 1111, Playa Ancha, Casilla 5030, Valparaiso, Chile), BM(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany <ID system="ORCID">0000-0002-0420-6159</ID>), BN(Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON, M5S 3H4, Canada ; Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, Ontario M5S 3H4, Canada ; <ID system="ORCID">0000-0001-6855-442X</ID>), BO(Department of Astronomy and Astrophysics, Eberly College of Science, The Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA ; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA ; Department of Physics, The Pennsylvania State University, University Park, PA 16802, USA <ID system="ORCID">0000-0002-0167-2453</ID>), BP(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA), BQ(Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA <ID system="ORCID">0000-0002-8725-1069</ID>), BR(Kavli Institute for the Physics and Mathematics of the Universe, Todai Institutes for Advanced Study, the University of Tokyo, Kashiwa, 277-8583, Japan ; University of California Observatories, University of California, Santa Cruz, CA 95064, USA <ID system="ORCID">0000-0001-9742-3138</ID>), BS(Center for Astrophysics and Space Science, University of California San Diego, La Jolla, CA 92093, USA <ID system="ORCID">0000-0002-6523-9536</ID>), BT(CEA, Centre de Saclay, IRFU, F-91191, Gif-sur-Yvette, France), BU(APC, University of Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cite, France), BV(Sub-department of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK <ID system="ORCID">0000-0002-1283-8420</ID>), BW(Instituto de Astronomía, Universidad Nacional Autónoma de México, A.P. 70-264, 04510, México, D.F., México), BX(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA ; NASA Goddard Space Flight Center, Code 667, Greenbelt, MD 20771, USA ; Department of Terrestrial Magnetism, Carnegie Institution for Science, 5241 Broad Branch Road, NW, Washington, DC 20015, USA <ID system="ORCID">0000-0001-5926-4471</ID>), BY(Laboratório Interinstitucional de e-Astronomia, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brasil ; Observatório Nacional, Rio de Janeiro, Brazil <ID system="ORCID">0000-0003-3044-5150</ID>), BZ(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain <ID system="ORCID">0000-0001-6143-8151</ID>), CA(Department of Astronomy, New Mexico State University, Box 30001, MSC 4500, Las Cruces NM 88003, USA), CB(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA), CC(Kavli Institute for the Physics and Mathematics of the Universe, Todai Institutes for Advanced Study, the University of Tokyo, Kashiwa, 277-8583, Japan <ID system="ORCID">0000-0001-8546-1428</ID>), CD(Instituto de Astronomía, Universidad Nacional Autónoma de México, A.P. 70-264, 04510, México, D.F., México), CE(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), CF(Department of Astronomy and Space Science, Sejong University, Seoul 143-747, Korea), CG(Department of Astronomy, New Mexico State University, Box 30001, MSC 4500, Las Cruces NM 88003, USA <ID system="ORCID">0000-0001-9984-0891</ID>), CH(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), CI(Korea Institute for Advanced Study, 85 Hoegiro, Dongdaemun-gu, Seoul 02455, Korea <ID system="ORCID">0000-0002-3043-2555</ID>), CJ(Laboratório Interinstitucional de e-Astronomia, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brasil ; Departamento de Física, CCNE, Universidade Federal de Santa Maria, 97105-900, Santa Maria, RS, Brazil), CK(Max-Planck-Institut für Extraterrestrische Physik, Gießenbachstr. 1, D-85748 Garching, Germany), CL(Department of Astronomy, Universidad de Concepción, Chile), CM(Instituto de Física Teórica (IFT) UAM/CSIC, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain ; Max-Planck-Institut für Extraterrestrische Physik, Gießenbachstr. 1, D-85748 Garching, Germany), CN(Laboratório Interinstitucional de e-Astronomia, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brasil ; Observatório Nacional, Rio de Janeiro, Brazil), CO(Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France), CP(Department of Physics and Astronomy, Western Washington University, 516 High Street, Bellingham, WA 98225, USA <ID system="ORCID">0000-0001-6914-7797</ID>), CQ(The Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA <ID system="ORCID">0000-0002-5226-787X</ID>), CR(Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213, USA), CS(Instituto de Astronomía, Universidad Nacional Autónoma de México, A.P. 70-264, 04510, México, D.F., México), CT(Departamento de Física, Facultad de Ciencias, Universidad de La Serena, Cisternas 1200, La Serena, Chile), CU(Steward Observatory, The University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721-0065, USA; Observatório Nacional, Rio de Janeiro, Brazil), CV(Departamento de Física, Facultad de Ciencias, Universidad de La Serena, Cisternas 1200, La Serena, Chile; Department of Astronomy, University of Virginia, 530 McCormick Road, Charlottesville, VA 22904-4325, USA), CW(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, 389 UCB, Boulder, CO 80309-0389, USA <ID system="ORCID">0000-0003-2511-2060</ID>), CX(Sub-department of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK <ID system="ORCID">0000-0001-7897-3812</ID>), CY(Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA <ID system="ORCID">0000-0002-0553-3805</ID>), CZ(Instituto de Física, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, México), DA(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), DB(Department of Physics, Geology, and Engineering Tech, Northern Kentucky University, Highland Heights, KY 41099, USA <ID system="ORCID">0000-0002-3657-0705</ID>), DC(Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland), DD(Las Campanas Observatory, Colina El Pino Casilla 601 La Serena, Chile), DE(Department of Astronomy, University of Wisconsin-Madison, 475 N. 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J. Thomson Avenue, Cambridge CB3 0HE, UK ; Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK), HD(Department of Astronomy, University of Virginia, 530 McCormick Road, Charlottesville, VA 22904-4325, USA <ID system="ORCID">0000-0003-2025-3147</ID>), HE(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA), HF(Apache Point Observatory, P.O. 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Libertador Bernardo O’Higgins 1058, Santiago de Chile), IE(Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USA), IF(University of Alabama, Tuscaloosa, AL 35487, USA), IG(Max-Planck-Institut für Extraterrestrische Physik, Gießenbachstr. 1, D-85748 Garching, Germany <ID system="ORCID">0000-0002-7150-9192</ID>), IH(Laboratório Interinstitucional de e-Astronomia, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brasil ; Instituto de Fśica, Universidade Federal do Rio Grande do Sul, Campus do Vale, Porto Alegre, RS, 91501-970, Brazil), II(Instituto de Astronomía, Universidad Nacional Autónoma de México, A.P. 70-264, 04510, México, D.F., México), IJ(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany), IK(PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA <ID system="ORCID">0000-0001-8684-2222</ID>), IL(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK), IM(National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA <ID system="ORCID">0000-0002-1793-3689</ID>), IN(Unidad de Astronomía, Fac. 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Ara go, F-75014 Paris, France), JE(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), JF(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK), JG(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK), JH(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain <ID system="ORCID">0000-0002-2807-6459</ID>), JI(Université Paris 6 et CNRS, Institut dAstrophysique de Paris, 98bis blvd. Ara go, F-75014 Paris, France), JJ(Aix Marseille Univ, CNRS, LAM, Laboratoire d’Astrophysique de Marseille, Marseille, France), JK(Department of Astronomy, The Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA <ID system="ORCID">0000-0002-7549-7766</ID>), JL(Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France; Université Paris 6 et CNRS, Institut dAstrophysique de Paris, 98bis blvd. Ara go, F-75014 Paris, France), JM(Department of Astronomy, The Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA), JN(Instituto de Física Teórica (IFT) UAM/CSIC, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain ; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain), JO(PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA <ID system="ORCID">0000-0003-4451-4444</ID>), JP(Laboratório Interinstitucional de e-Astronomia, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brasil ; Instituto de Fśica, Universidade Federal do Rio Grande do Sul, Campus do Vale, Porto Alegre, RS, 91501-970, Brazil), JQ(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA), JR(CEA, Centre de Saclay, IRFU, F-91191, Gif-sur-Yvette, France; Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland), JS(Laboratório Interinstitucional de e-Astronomia, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brasil ; Departamento de Física, CCNE, Universidade Federal de Santa Maria, 97105-900, Santa Maria, RS, Brazil), JT(Department of Physics and Astronomy, Texas Christian University, Fort Worth, TX 76129, USA), JU(Laboratório Interinstitucional de e-Astronomia, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brasil ; Departamento de Física, CCNE, Universidade Federal de Santa Maria, 97105-900, Santa Maria, RS, Brazil), JV(Laboratório Interinstitucional de e-Astronomia, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brasil ; Instituto de Fśica, Universidade Federal do Rio Grande do Sul, Campus do Vale, Porto Alegre, RS, 91501-970, Brazil), JW(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany <ID system="ORCID">0000-0003-4996-9069</ID>), JX(Institut UTINAM, CNRS UMR6213, Univ. Bourgogne Franche-Comté, OSU THETA Franche-Comté-Bourgogne, Observatoire de Besançon, BP 1615, F-25010 Besançon Cedex, France), JY(University of California Observatories, University of California, Santa Cruz, CA 95064, USA ; Department of Astronomy and Astrophysics, University of California Santa Cruz, 1156 High St., Santa Cruz, CA, 95064, USA), JZ(Instituto de Física Teórica (IFT) UAM/CSIC, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain ; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain ; Departamento de Física Teórica M8, Universidad Autonóma de Madrid (UAM), Cantoblanco, E-28049, Madrid, Spain), KA(Departamento de Física, Facultad de Ciencias, Universidad de La Serena, Cisternas 1200, La Serena, Chile <ID system="ORCID">0000-0002-1379-4204</ID>), KB(Instituto de Astronomía, Universidad Nacional Autónoma de México, Unidad Académica en Ensenada, Ensenada BC 22860, México <ID system="ORCID">0000-0001-8600-4798</ID>), KC(Instituto de Astronomía, Universidad Nacional Autónoma de México, A.P. 70-264, 04510, México, D.F., México), KD(Center for Cosmology and AstroParticle Physics, The Ohio State University, 191 W. Woodruff Ave., Columbus, OH 43210, USA), KE(Department of Astronomy and Space Science, Sejong University, Seoul 143-747, Korea), KF(Department of Astronomy, Box 351580, University of Washington, Seattle, WA 98195, USA <ID system="ORCID">0000-0001-8665-5523</ID>), KG(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK), KH(Kavli Institute for Particle Astrophysics & Cosmology, P. O. Box 2450, Stanford University, Stanford, CA 94305, USA ; SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA <ID system="ORCID">0000-0001-9376-3135</ID>), KI(Max-Planck-Institut für Extraterrestrische Physik, Gießenbachstr. 1, D-85748 Garching, Germany), KJ(Max-Planck-Institut für Extraterrestrische Physik, Gießenbachstr. 1, D-85748 Garching, Germany <ID system="ORCID">0000-0001-7116-9303</ID>), KK(Max-Planck-Institut für Extraterrestrische Physik, Gießenbachstr. 1, D-85748 Garching, Germany), KL(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), KM(Department of Astronomy, Box 351580, University of Washington, Seattle, WA 98195, USA), KN(Universidad de Chile, Av. Libertador Bernardo O’Higgins 1058, Santiago de Chile <ID system="ORCID">0000-0002-4023-7649</ID>), KO(Laboratório Interinstitucional de e-Astronomia, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brasil ; Instituto de Fśica, Universidade Federal do Rio Grande do Sul, Campus do Vale, Porto Alegre, RS, 91501-970, Brazil), KP(Department of Astronomy, Box 351580, University of Washington, Seattle, WA 98195, USA), KQ(Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK), KR(Laboratório Interinstitucional de e-Astronomia, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brasil ; Instituto de Fśica, Universidade Federal do Rio Grande do Sul, Campus do Vale, Porto Alegre, RS, 91501-970, Brazil), KS(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; <ID system="ORCID">0000-0002-3569-7421</ID>), KT(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA <ID system="ORCID">0000-0002-5042-5088</ID>), KU(Department of Astronomy and Astrophysics, Eberly College of Science, The Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA), KV(Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Blvd de l’Observatoire, F-06304 Nice, France <ID system="ORCID">0000-0002-6590-1657</ID>), KW(Instituto de Astronomía, Universidad Nacional Autónoma de México, Unidad Académica en Ensenada, Ensenada BC 22860, México), KX(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), KY(Department of Physics and Astronomy, Ohio University, Clippinger Labs, Athens, OH 45701, USA), KZ(Shanghai Astronomical Observatory, Chinese Academy of Science, 80 Nandan Road, Shanghai 200030, China), LA(Shanghai Astronomical Observatory, Chinese Academy of Science, 80 Nandan Road, Shanghai 200030, China <ID system="ORCID">0000-0002-3073-5871</ID>), LB(McDonald Observatory, University of Texas at Austin, 3640 Dark Sky Dr., Fort Davis, TX 79734, USA <ID system="ORCID">0000-0003-0509-2656</ID>), LC(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, 389 UCB, Boulder, CO 80309-0389, USA <ID system="ORCID">0000-0002-4594-9936</ID>), LD(Department of Physics and JINA Center for the Evolution of the Elements, University of Notre Dame, Notre Dame, IN 46556 USA), LE(Department of Astronomy, Box 351580, University of Washington, Seattle, WA 98195, USA), LF(Department of Astronomy, University of Virginia, 530 McCormick Road, Charlottesville, VA 22904-4325, USA), LG(Brookhaven National Laboratory, Upton, NY 11973, USA), LH(National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA), LI(Department of Astronomy, University of Virginia, 530 McCormick Road, Charlottesville, VA 22904-4325, USA), LJ(Laboratório Interinstitucional de e-Astronomia, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brasil ; Universidade Federal do ABC, Centro de Ciȩncias Naturais e Humanas, Av. dos Estados, 5001, Santo André, SP, 09210-580, Brazil), LK(Vanderbilt University, Department of Physics & Astronomy, 6301 Stevenson Center Ln., Nashville, TN 37235, USA), LL(Observatório Nacional, Rio de Janeiro, Brazil), LM(Kavli Institute for the Physics and Mathematics of the Universe, Todai Institutes for Advanced Study, the University of Tokyo, Kashiwa, 277-8583, Japan <ID system="ORCID">0000-0002-3746-2853</ID>), LN(Vanderbilt University, Department of Physics & Astronomy, 6301 Stevenson Center Ln., Nashville, TN 37235, USA <ID system="ORCID">0000-0002-3481-9052</ID>), LO(Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349, USA), LP(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany <ID system="ORCID">0000-0001-6516-7459</ID>), LQ(Laboratório Interinstitucional de e-Astronomia, 77 Rua General José Cristino, Rio de Janeiro, 20921-400, Brasil ; Instituto de Fśica, Universidade Federal do Rio Grande do Sul, Campus do Vale, Porto Alegre, RS, 91501-970, Brazil <ID system="ORCID">0000-0003-1772-0023</ID>), LR(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), LS(Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, University of Colorado, 389 UCB, Boulder, CO 80309-0389, USA <ID system="ORCID">0000-0003-1479-3059</ID>), LT(Instituto de Astronomía, Universidad Nacional Autónoma de México, Unidad Académica en Ensenada, Ensenada BC 22860, México <ID system="ORCID">0000-0002-2011-4924</ID>), LU(Department of Physics and Astronomy, Texas Christian University, Fort Worth, TX 76129, USA), LV(Kavli Institute for the Physics and Mathematics of the Universe, Todai Institutes for Advanced Study, the University of Tokyo, Kashiwa, 277-8583, Japan), LW(ELTE Gothard Astrophysical Observatory, H-9704 Szombathely, Szent Imre herceg st. 112, Hungary), LX(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA), LY(Department of Astronomy, Universidad de Concepción, Chile <ID system="ORCID">0000-0002-0066-0346</ID>), LZ(Aix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, France; Tsinghua Center for Astrophysics & Department of Physics, Tsinghua University, Beijing 100084, China), MA(Department of Astronomy, The Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA <ID system="ORCID">0000-0002-4818-7885</ID>), MB(Department of Astronomy, University of Virginia, 530 McCormick Road, Charlottesville, VA 22904-4325, USA), MC(The Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA;), MD(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA), ME(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK), MF(Department of Physics and Astronomy, Texas Christian University, Fort Worth, TX 76129, USA), MG(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), MH(Departamento de Física, Facultad de Ciencias Exactas, Universidad Andres Bello, Av. Fernandez Concha 700, Las Condes, Santiago, Chile <ID system="ORCID">0000-0001-5242-2844</ID>), MI(School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, KY16 9SS, UK), MJ(Instituto de Astronomía, Universidad Nacional Autónoma de México, A.P. 70-264, 04510, México, D.F., México), MK(Aix Marseille Univ, CNRS, LAM, Laboratoire d’Astrophysique de Marseille, Marseille, France), ML(Department of Astronomy, University of Wisconsin-Madison, 475 N. Charter St., Madison, WI 53726, USA), MM(Department of Astronomy, University of Virginia, 530 McCormick Road, Charlottesville, VA 22904-4325, USA <ID system="ORCID">0000-0003-3248-3097</ID>), MN(Instituto de Astronomía, Universidad Nacional Autónoma de México, A.P. 70-264, 04510, México, D.F., México), MO(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), MP(Departamento de Física, Facultad de Ciencias, Universidad de La Serena, Cisternas 1200, La Serena, Chile), MQ(Instituto de Física, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, México), MR(Brookhaven National Laboratory, Upton, NY 11973, USA), MS(Department of Astronomy, Universidad de Concepción, Chile), MT(Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA), MU(Department of Astronomy, New Mexico State University, Box 30001, MSC 4500, Las Cruces NM 88003, USA), MV(Department of Physics, University of North Carolina Asheville, One University Heights, Asheville, NC 28804, USA; Department of Physical Sciences, The Open University, Milton Keynes, MK7 6AA, UK <ID system="ORCID">0000-0002-6047-1010</ID>), MW(Department of Astronomy, New Mexico State University, Box 30001, MSC 4500, Las Cruces NM 88003, USA <ID system="ORCID">0000-0002-0782-3064</ID>), MX(National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, China), MY(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA; National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA), MZ(School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, KY16 9SS, UK), NA(Department of Astronomy, The Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA; Center for Cosmology and AstroParticle Physics, The Ohio State University, 191 W. Woodruff Ave., Columbus, OH 43210, USA <ID system="ORCID">0000-0001-7775-7261</ID>), NB(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth, PO1 3FX, UK; Department of Astronomy and Astrophysics, University of California Santa Cruz, 1156 High St., Santa Cruz, CA, 95064, USA), NC(Department of Physics, Austin College, Sherman, TX 75090, USA), ND(School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, KY16 9SS, UK), NE(Department of Astronomy, University of Virginia, 530 McCormick Road, Charlottesville, VA 22904-4325, USA), NF(PITT PACC, Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA <ID system="ORCID">0000-0001-7113-1233</ID>), NG(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA <ID system="ORCID">0000-0003-2212-6045</ID>), NH(Shanghai Astronomical Observatory, Chinese Academy of Science, 80 Nandan Road, Shanghai 200030, China), NI(Department of Physics and Astronomy, University of Kentucky, 505 Rose St., Lexington, KY, 40506-0055, USA <ID system="ORCID">0000-0003-1025-1711</ID>), NJ(School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, KY16 9SS, UK), NK(Instituto de Astronomía, Universidad Nacional Autónoma de México, Unidad Académica en Ensenada, Ensenada BC 22860, México; Department of Physics, Bridgewater College, 402 E. College St., Bridgewater, VA 22812 USA <ID system="ORCID">0000-0002-3576-4508</ID>), NL(CEA, Centre de Saclay, IRFU, F-91191, Gif-sur-Yvette, France), NM(Center for Astrophysical Sciences, Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA <ID system="ORCID">0000-0001-6100-6869</ID>), NN(Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), NO(CEA, Centre de Saclay, IRFU, F-91191, Gif-sur-Yvette, France), NP(Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA; Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles St., Baltimore, MD 21218, USA), NQ(Department of Physics and Astronomy, University of Kentucky, 505 Rose St., Lexington, KY, 40506-0055, USA), NR(National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, China), NS(National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, China), NT(Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA <ID system="ORCID">0000-0003-1887-6732</ID>), NU(National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, China), NV(National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, China <ID system="ORCID">0000-0002-4135-0977</ID>), NW(Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles St., Baltimore, MD 21218, USA ; <ID system="ORCID">0000-0002-7574-8078</ID>), NX(Instituto Milenio de Astrofísica, Av. Vicuña Mackenna 4860, Macul, Santiago, Chile ; Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Av. Vicuna Mackenna 4860, 782-0436 Macul, Santiago, Chile), NY(National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, China <ID system="ORCID">0000-0002-6684-3997</ID>)
%B The Astronomical Journal
%V 154
%D 2017
%8 July 1, 2017
%K cosmology: observations;  galaxies: general;  Galaxy: general;  instrumentation: spectrographs;  stars: general;  surveys
%U http://adsabs.harvard.edu/abs/2017AJ....154...28B
%X We describe the Sloan Digital Sky Survey IV (SDSS-IV), a project 
encompassing three major spectroscopic programs. The Apache Point 
Observatory Galactic Evolution Experiment 2 (APOGEE-2) is observing 
hundreds of thousands of Milky Way stars at high resolution and high 
signal-to-noise ratios in the near-infrared. The Mapping Nearby Galaxies 
at Apache Point Observatory (MaNGA) survey is obtaining spatially 
resolved spectroscopy for thousands of nearby galaxies (median z˜ 
0.03). The extended Baryon Oscillation Spectroscopic Survey (eBOSS) is 
mapping the galaxy, quasar, and neutral gas distributions between z˜ 
0.6 and 3.5 to constrain cosmology using baryon acoustic oscillations, 
redshift space distortions, and the shape of the power spectrum. Within 
eBOSS, we are conducting two major subprograms: the SPectroscopic 
IDentification of eROSITA Sources (SPIDERS), investigating X-ray AGNs 
and galaxies in X-ray clusters, and the Time Domain Spectroscopic Survey 
(TDSS), obtaining spectra of variable sources. All programs use the 2.5 
m Sloan Foundation Telescope at the Apache Point Observatory; 
observations there began in Summer 2014. APOGEE-2 also operates a second 
near-infrared spectrograph at the 2.5 m du Pont Telescope at Las 
Campanas Observatory, with observations beginning in early 2017. 
Observations at both facilities are scheduled to continue through 2020. 
In keeping with previous SDSS policy, SDSS-IV provides regularly 
scheduled public data releases; the first one, Data Release 13, was made 
available in 2016 July.
%3 10.3847/1538-3881/aa7567
%= eprint: arXiv:1703.00052
%@ 0004-6256

%0 Journal Article
%T The large-scale three-point correlation function of the SDSS BOSS DR12 CMASS galaxies
%A Slepian, Zachary 
%A Eisenstein, Daniel J. 
%A Beutler, Florian 
%A Chuang, Chia-Hsun 
%A Cuesta, Antonio J. 
%A Ge, Jian 
%A Gil-Marín, Héctor 
%A Ho, Shirley 
%A Kitaura, Francisco-Shu 
%A McBride, Cameron K. 
%A Nichol, Robert C. 
%A Percival, Will J. 
%A Rodríguez-Torres, Sergio 
%A Ross, Ashley J. 
%A Scoccimarro, Román 
%A Seo, Hee-Jong 
%A Tinker, Jeremy 
%A Tojeiro, Rita 
%A Vargas-Magaña, Mariana
%+ AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AC(Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley CA 94720, USA), AD(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AE(Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, E-08028 Barcelona, Spain), AF(Astronomy Department, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA), AG(Sorbonne Universités, Institut Lagrange de Paris (ILP), 98 bis Boulevard Arago, F-75014 Paris, France; Laboratoire de Physique Nucléaire et de Hautes Energies, Université Pierre et Marie Curie, 4 Place Jussieu, F-75005 Paris, France; Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AH(Bruce and Astrid McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA), AI(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AJ(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AK(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AL(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AM(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica M8, Universidad Autonoma de Madrid (UAM), Cantoblanco, E-28049 Madrid, Spain), AN(Center for Cosmology and Astroparticle Physics, Department of Physics, The Ohio State University, OH 43210, USA), AO(Center for Cosmology and Particle Physics, New York University, 4 Washington Place, NY 1003, New York, USA), AP(Department of Physics and Astronomy, Ohio University, Clippinger Labs, Athens, OH 45701, USA), AQ(Center for Cosmology and Particle Physics, New York University, 4 Washington Place, NY 1003, New York, USA), AR(University of St Andrews, North Haugh, St Andrews Fife KY16 9SS, UK), AS(Instituto de Física, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, México)
%B Monthly Notices of the Royal Astronomical Society
%V 468
%D 2017
%8 June 1, 2017
%P 1070-1083
%K cosmology: observations;  distance scale;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2017MNRAS.468.1070S
%X We report a measurement of the large-scale three-point correlation 
function of galaxies using the largest data set for this purpose to 
date, 777 202 luminous red galaxies in the Sloan Digital Sky Survey 
Baryon Acoustic Oscillation Spectroscopic Survey (SDSS BOSS) DR12 CMASS 
sample. This work exploits the novel algorithm of Slepian & 
Eisenstein to compute the multipole moments of the 3PCF in O(N^2) time, 
with N the number of galaxies. Leading-order perturbation theory models 
the data well in a compressed basis where one triangle side is 
integrated out. We also present an accurate and computationally 
efficient means of estimating the covariance matrix. With these 
techniques, the redshift-space linear and non-linear bias are measured, 
with 2.6 per cent precision on the former if σ<SUB>8</SUB> is 
fixed. The data also indicate a 2.8σ preference for the BAO, 
confirming the presence of BAO in the three-point function.
%3 10.1093/mnras/stw3234
%@ 0035-8711

%0 Journal Article
%T The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmic flows and cosmic web from luminous red galaxies
%A Ata, Metin 
%A Kitaura, Francisco-Shu 
%A Chuang, Chia-Hsun 
%A Rodríguez-Torres, Sergio 
%A Angulo, Raul E. 
%A Ferraro, Simone 
%A Gil-Marín, Hector 
%A McDonald, Patrick 
%A Hernández Monteagudo, Carlos 
%A Müller, Volker 
%A Yepes, Gustavo 
%A Autefage, Mathieu 
%A Baumgarten, Falk 
%A Beutler, Florian 
%A Brownstein, Joel R. 
%A Burden, Angela 
%A Eisenstein, Daniel J. 
%A Guo, Hong 
%A Ho, Shirley 
%A McBride, Cameron 
%A Neyrinck, Mark 
%A Olmstead, Matthew D. 
%A Padmanabhan, Nikhil 
%A Percival, Will J. 
%A Prada, Francisco 
%A Rossi, Graziano 
%A Sánchez, Ariel G. 
%A Schlegel, David 
%A Schneider, Donald P. 
%A Seo, Hee-Jong 
%A Streblyanska, Alina 
%A Tinker, Jeremy 
%A Tojeiro, Rita 
%A Vargas-Magana, Mariana
%+ AA(Leibniz Institut für Astrophysik (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AB(Leibniz Institut für Astrophysik (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA; Departments of Physics and Astronomy, University of California, Berkeley, CA 94720, USA; Instituto de Astrofisica de Canarias (IAC), Calle Via Lactea s/n, E-38200 La Laguna, Spain; Departamento de Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), AC(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz Institut für Astrophysik (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AD(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AE(Centro de Estudios de Física del Cosmos de Aragón (CEFCA), Plaza San Juan, 1, planta 2, E-44001 Teruel, Spain,), AF(Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA; Departments of Physics and Astronomy, University of California, Berkeley, CA 94720, USA), AG(Sorbonne Universités, Institut Lagrange de Paris (ILP), 98 bis Boulevard Arago, F-75014 Paris, France; Laboratoire de Physique Nucléaire et de Hautes Energies, Université Pierre et Marie Curie, 4 Place Jussieu, F-75005 Paris, France; Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AH(Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA), AI(Centro de Estudios de Física del Cosmos de Aragón (CEFCA), Plaza San Juan, 1, planta 2, E-44001 Teruel, Spain,), AJ(Leibniz Institut für Astrophysik (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AK(Departamento de Física Teórica, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AL(Leibniz Institut für Astrophysik (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AM(Leibniz Institut für Astrophysik (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AN(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AO(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AP(Yale Center for Astronomy and Astrophysics, Yale University, New Haven, CT 06520, USA), AQ(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), AR(Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Shanghai 200030, China), AS(Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213, USA), AT(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), AU(Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD 21218, USA), AV(Department of Chemistry and Physics, King's College, 133 North River St, Wilkes Barre, PA 18711, USA), AW(Yale Center for Astronomy and Astrophysics, Yale University, New Haven, CT 06520, USA), AX(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AY(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía, E-18080 Granada, Spain), AZ(Department of Astronomy and Space Science, Sejong University, Seoul 143-747, Korea), BA(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), BB(Departments of Physics and Astronomy, University of California, Berkeley, CA 94720, USA), BC(Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA), BD(Department of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, OH 45701, USA), BE(Instituto de Astrofisica de Canarias (IAC), Calle Via Lactea s/n, E-38200 La Laguna, Spain), BF(Center for Cosmology and Particle Physics, New York University, 4 Washington Place, New York, NY 10003, USA), BG(University of St Andrews, North Haugh, St Andrews Fife, KY16 9SS, UK), BH(Instituto de Física, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, 01000 México D.F., Mexico)
%B Monthly Notices of the Royal Astronomical Society
%V 467
%D 2017
%8 June 1, 2017
%P 3993-4014
%K methods: numerical;  catalogues;  galaxies: statistics;  cosmology: theory;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2017MNRAS.467.3993A
%X We present a Bayesian phase-space reconstruction of the cosmic 
large-scale matter density and velocity fields from the Sloan Digital 
Sky Survey-III Baryon Oscillations Spectroscopic Survey Data Release 12 
CMASS galaxy clustering catalogue. We rely on a given Λ cold dark 
matter cosmology, a mesh resolution in the range of 6-10 h<SUP>-1</SUP> 
Mpc, and a lognormal-Poisson model with a redshift-dependent non-linear 
bias. The bias parameters are derived from the data and a general 
renormalized perturbation theory approach. We use combined Gibbs and 
Hamiltonian sampling, implemented in the argo code, to iteratively 
reconstruct the dark matter density field and the coherent peculiar 
velocities of individual galaxies, correcting hereby for coherent 
redshift space distortions. Our tests relying on accurate N-body-based 
mock galaxy catalogues show unbiased real space power spectra of the 
non-linear density field up to k ˜ 0.2 h Mpc<SUP>-1</SUP>, and 
vanishing quadrupoles down to r ˜ 20 h<SUP>-1</SUP> Mpc. We also 
demonstrate that the non-linear cosmic web can be obtained from the 
tidal field tensor based on the Gaussian component of the reconstructed 
density field. We find that the reconstructed velocities have a 
statistical correlation coefficient compared to the true velocities of 
each individual light-cone mock galaxy of r ˜ 0.68 including about 
10 per cent of satellite galaxies with virial motions (about r = 0.75 
without satellites). The power spectra of the velocity divergence agree 
well with theoretical predictions up to k ˜ 0.2 h Mpc<SUP>-1</SUP>. 
This work will be especially useful to improve, for example, baryon 
acoustic oscillation reconstructions, kinematic Sunyaev-Zeldovich, 
integrated Sachs-Wolfe measurements or environmental studies.
%3 10.1093/mnras/stx178
%= eprint: arXiv:1605.09745
%@ 0035-8711

%0 Journal Article
%T Measurement of baryon acoustic oscillation correlations at z = 2.3 with SDSS DR12 Lyα-Forests
%A Bautista, Julian E. 
%A Busca, Nicolás G. 
%A Guy, Julien 
%A Rich, James 
%A Blomqvist, Michael 
%A du Mas des Bourboux, Hélion 
%A Pieri, Matthew M. 
%A Font-Ribera, Andreu 
%A Bailey, Stephen 
%A Delubac, Timothée 
%A Kirkby, David 
%A Le Goff, Jean-Marc 
%A Margala, Daniel 
%A Slosar, Anže 
%A Vazquez, Jose Alberto 
%A Brownstein, Joel R. 
%A Dawson, Kyle S. 
%A Eisenstein, Daniel J. 
%A Miralda-Escudé, Jordi 
%A Noterdaeme, Pasquier 
%A Palanque-Delabrouille, Nathalie 
%A Pâris, Isabelle 
%A Petitjean, Patrick 
%A Ross, Nicholas P. 
%A Schneider, Donald P. 
%A Weinberg, David H. 
%A Yèche, Christophe
%+ AA(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT, 84112, USA), AB(APC, Université Paris Diderot-Paris 7, CNRS/IN2P3, CEA, Observatoire de Paris, 10 rue A. Domon & L. Duquet, 75013, Paris, France), AC(LPNHE, CNRS/IN2P3, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris 7, 4 place Jussieu, 75252, Paris CEDEX, France), AD(IRFU, CEA, Université Paris-Saclay, 91191, Gif-sur-Yvette, France <EMAIL>rich@hep.saclay.cea.fr</EMAIL>), AE(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), AF(IRFU, CEA, Université Paris-Saclay, 91191, Gif-sur-Yvette, France), AG(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), AH(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA, 94720, USA; Department of Physics and Astronomy, University College London, Gower Street, London, UK), AI(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA, 94720, USA), AJ(Laboratoire d'Astrophysique, École Polytechnique Fedérale de Lausanne, 1015, Lausanne, Switzerland), AK(Department of Physics and Astronomy, University of California, Irvine, CA, 92697, USA), AL(IRFU, CEA, Université Paris-Saclay, 91191, Gif-sur-Yvette, France), AM(Department of Physics and Astronomy, University of California, Irvine, CA, 92697, USA), AN(Brookhaven National Laboratory, 2 Center Road, Upton, NY, 11973, USA), AO(Brookhaven National Laboratory, 2 Center Road, Upton, NY, 11973, USA), AP(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT, 84112, USA), AQ(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT, 84112, USA), AR(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA, 02138, USA), AS(Institució Catalana de Recerca i Estudis Avançats, 08010 Barcelona, Catalonia, Spain; Institució de Ciéncies del Cosmos, Universitat de Barcelona (UB-IEEC), 08007 Barcelona, Catalonia, Spain), AT(Université Paris 6 et CNRS, Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014, Paris, France), AU(IRFU, CEA, Université Paris-Saclay, 91191, Gif-sur-Yvette, France), AV(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388, Marseille, France), AW(Université Paris 6 et CNRS, Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014, Paris, France), AX(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, EH9 3HJ, UK), AY(Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA, 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA, 16802, USA), AZ(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH, 43210, USA), BA(IRFU, CEA, Université Paris-Saclay, 91191, Gif-sur-Yvette, France; Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA, 94720, USA)
%B Astronomy and Astrophysics
%V 603
%D 2017
%8 June 1, 2017
%K cosmological parameters;  dark energy
%U http://adsabs.harvard.edu/abs/2017A%26A...603A..12B
%X We have used flux-transmission correlations in Lyα forests to 
measure the imprint of baryon acoustic oscillations (BAO). The study 
uses spectra of 157 783 quasars in the redshift range 2.1 ≤ z ≤ 
3.5 from the Sloan Digital Sky Survey (SDSS) data release 12 (DR12). 
Besides the statistical improvements on our previous studies using SDSS 
DR9 and DR11, we have implemented numerous improvements in the analysis 
procedure, allowing us to construct a physical model of the correlation 
function and to investigate potential systematic errors in the 
determination of the BAO peak position. The Hubble distance, 
D<SUB>H</SUB> = c/H(z), relative to the sound horizon is D<SUB>H</SUB>(z 
= 2.33) /r<SUB>d</SUB> = 9.07 ± 0.31. The best-determined 
combination of comoving angular-diameter distance, D<SUB>M</SUB>, and 
the Hubble distance is found to be 
D<SUB>H</SUB><SUP>0.7</SUP>D<SUB>M</SUB><SUP>0.3</SUP> /r<SUB>d</SUB> = 
13.94 ± 0.35. This value is 1.028 ± 0.026 times the 
prediction of the flat-ΛCDM model consistent with the cosmic 
microwave background (CMB) anisotropy spectrum. The errors include 
marginalization over the effects of unidentified high-density absorption 
systems and fluctuations in ultraviolet ionizing radiation. 
Independently of the CMB measurements, the combination of our results 
and other BAO observations determine the open-ΛCDM density 
parameters to be Ω<SUB>M</SUB> = 0.296 ± 0.029, 
Ω<SUB>Λ</SUB> = 0.699 ± 0.100 and 
Ω<SUB>k</SUB> = -0.002 ± 0.119.
%3 10.1051/0004-6361/201730533
%= eprint: arXiv:1702.00176
%@ 0004-6361

%0 Journal Article
%T The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: higher order correlations revealed by germ-grain Minkowski functionals
%A Wiegand, Alexander 
%A Eisenstein, Daniel J.
%+ AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 467
%D 2017
%8 May 1, 2017
%P 3361-3378
%K methods: data analysis;  methods: statistical;  cosmology: observations;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2017MNRAS.467.3361W
%X We probe the higher order clustering of the galaxies in the final data 
release (DR12) of the Sloan Digital Sky Survey Baryon Oscillation 
Spectroscopic Survey (BOSS), using the method of germ-grain Minkowski 
functionals (MFs). Our sample consists of 410 615 BOSS galaxies from the 
northern Galactic cap in the redshift range 0.450-0.595. We show the MFs 
to be sensitive to contributions up to the six-point correlation 
function for this data set. We ensure with a custom angular mask that 
the results are more independent of boundary effects than in previous 
analyses of this type. We extract the higher order part of the MFs and 
quantify the difference to the case without higher order correlations. 
The resulting χ<SUP>2</SUP> value of over 10 000 for a modest number 
of degrees of freedom, O(200), indicates a 100σ deviation and 
demonstrates that we have a highly significant signal of the 
non-Gaussian contributions to the galaxy distribution. This statistical 
power can be useful in testing models with differing higher order 
correlations. Comparing the galaxy data to the quick particle mesh and 
MultiDark(MD)-Patchy mocks, we find that the latter better describes the 
observed structure. From an order-by-order decomposition, we expect 
that, for example, already a reduction of the amplitude of the MD-Patchy 
mock power spectrum by 5 per cent would remove the remaining tension.
%3 10.1093/mnras/stx292
%= eprint: arXiv:1609.08613
%@ 0035-8711

%0 Journal Article
%T The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the Fourier space wedges of the final sample
%A Grieb, Jan Niklas 
%A Sánchez, Ariel G. 
%A Salazar-Albornoz, Salvador 
%A Scoccimarro, Román 
%A Crocce, Martín 
%A Dalla Vecchia, Claudio 
%A Montesano, Francesco 
%A Gil-Marín, Héctor 
%A Ross, Ashley J. 
%A Beutler, Florian 
%A Rodríguez-Torres, Sergio 
%A Chuang, Chia-Hsun 
%A Prada, Francisco 
%A Kitaura, Francisco-Shu 
%A Cuesta, Antonio J. 
%A Eisenstein, Daniel J. 
%A Percival, Will J. 
%A Vargas-Magaña, Mariana 
%A Tinker, Jeremy L. 
%A Tojeiro, Rita 
%A Brownstein, Joel R. 
%A Maraston, Claudia 
%A Nichol, Robert C. 
%A Olmstead, Matthew D. 
%A Samushia, Lado 
%A Seo, Hee-Jong 
%A Streblyanska, Alina 
%A Zhao, Gong-bo
%+ AA(Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Scheinerstraße 1, D-81679 München, Germany; Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AB(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AC(Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Scheinerstraße 1, D-81679 München, Germany; Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AD(Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, NY 10003, USA), AE(Institut de Ciències de l'Espai, IEEC-CSIC, Campus UAB, F. de Ciències, Torre C5 par-2, E-Barcelona 08193, Spain), AF(Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, E-38205 La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, Av. del Astrofísico Francisco Sánchez s/n, E-38206 La Laguna, Tenerife, Spain), AG(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AH(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; Sorbonne Universités, Institut Lagrange de Paris (ILP), 98 bis Boulevard Arago, F-75014 Paris, France; Laboratoire de Physique Nucléaire et de Hautes Energies, Université Pierre et Marie Curie, 4 Place Jussieu, F-75005 Paris, France), AI(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; Center for Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USA), AJ(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA), AK(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AL(Departamento de Física Teórica, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut für Astrophysik (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AM(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía, E-18080 Granada, Spain), AN(Leibniz-Institut für Astrophysik (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AO(Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Martíi Franquès 1, E-08028 Barcelona, Spain), AP(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), AQ(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AR(Instituto de Física, UNAM, PO Box 20-364, 01000 México D.F., Mexico), AS(Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, NY 10003, USA), AT(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK), AU(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AV(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AW(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AX(Department of Chemistry and Physics, King's College, 133 North River St, Wilkes Barre, PA 18711, USA), AY(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; Kansas State University, Manhattan, KS 66506, USA; National Abastumani Astrophysical Observatory, Ilia State University, 2A Kazbegi Ave, GE-1060 Tbilisi, Georgia), AZ(Department of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, OH 45701, USA), BA(Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, E-38205 La Laguna, Tenerife, Spain), BB(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, P. R. China)
%B Monthly Notices of the Royal Astronomical Society
%V 467
%D 2017
%8 May 1, 2017
%P 2085-2112
%K cosmology: observations;  cosmological parameters;  dark energy;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2017MNRAS.467.2085G
%X We extract cosmological information from the anisotropic power-spectrum 
measurements from the recently completed Baryon Oscillation 
Spectroscopic Survey (BOSS), extending the concept of clustering wedges 
to Fourier space. Making use of new fast-Fourier-transform-based 
estimators, we measure the power-spectrum clustering wedges of the BOSS 
sample by filtering out the information of Legendre multipoles ℓ 
> 4. Our modelling of these measurements is based on novel approaches 
to describe non-linear evolution, bias and redshift-space distortions, 
which we test using synthetic catalogues based on large-volume N-body 
simulations. We are able to include smaller scales than in previous 
analyses, resulting in tighter cosmological constraints. Using three 
overlapping redshift bins, we measure the angular-diameter distance, the 
Hubble parameter and the cosmic growth rate, and explore the 
cosmological implications of our full-shape clustering measurements in 
combination with cosmic microwave background and Type Ia supernova data. 
Assuming a Λ cold dark matter (ΛCDM) cosmology, we 
constrain the matter density to Ω <SUB>M</SUB>= 
0.311_{-0.010}^{+0.009} and the Hubble parameter to H_0 = 
67.6_{-0.6}^{+0.7} km s^{-1 Mpc^{-1}}, at a confidence level of 68 per 
cent. We also allow for non-standard dark energy models and 
modifications of the growth rate, finding good agreement with the 
ΛCDM paradigm. For example, we constrain the equation-of-state 
parameter to w = -1.019_{-0.039}^{+0.048}. This paper is part of a set 
that analyses the final galaxy-clustering data set from BOSS. The 
measurements and likelihoods presented here are combined with others in 
Alam et al. to produce the final cosmological constraints from BOSS.
%3 10.1093/mnras/stw3384
%= eprint: arXiv:1607.03143
%@ 0035-8711

%0 Journal Article
%T The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: anisotropic galaxy clustering in Fourier space
%A Beutler, Florian 
%A Seo, Hee-Jong 
%A Saito, Shun 
%A Chuang, Chia-Hsun 
%A Cuesta, Antonio J. 
%A Eisenstein, Daniel J. 
%A Gil-Marín, Héctor 
%A Grieb, Jan Niklas 
%A Hand, Nick 
%A Kitaura, Francisco-Shu 
%A Modi, Chirag 
%A Nichol, Robert C. 
%A Olmstead, Matthew D. 
%A Percival, Will J. 
%A Prada, Francisco 
%A Sánchez, Ariel G. 
%A Rodriguez-Torres, Sergio 
%A Ross, Ashley J. 
%A Ross, Nicholas P. 
%A Schneider, Donald P. 
%A Tinker, Jeremy 
%A Tojeiro, Rita 
%A Vargas-Magaña, Mariana
%+ AA(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA <EMAIL>florian.beutler@port.ac.uk</EMAIL>), AB(Department of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, OH 45701, USA), AC(Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan; Max-Planck-Institut f ür Astrophysik, Karl-Schwarzschild-Strasse 1, D-85740 Garching bei M ünchen, Germany), AD(Instituto de F ísica Te órica, (UAM/CSIC), Universidad Aut ónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut f ür Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AE(Institut de Ci ències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Mart í i Franqu ès 1, E-08028 Barcelona, Spain), AF(Harvard -Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), AG(Sorbonne Universit és, Institut Lagrange de Paris (ILP), 98 bis Boulevard Arago, F-75014 Paris, France; Laboratoire de Physique Nuclaire et de Hautes Energies, Universit é Pierre et Marie Curie, 4 Place Jussieu, F-75005 Paris, France), AH(Max-Planck-Institut f ür extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany; Universit äts-Sternwarte M ünchen, Ludwig-Maximilians-Universit ät M ünchen, Scheinerstra ße 1, D-81679 M ünchen, Germany), AI(Department of Astronomy, University of California, Berkeley, CA 94720, USA), AJ(Leibniz-Institut f ür Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AK(Department of Physics, University of California, Berkeley, CA 94720, USA), AL(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AM(Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA), AN(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AO(Instituto de F ísica Te órica, (UAM/CSIC), Universidad Aut ónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM +CSIC, Cantoblanco, E-28049 Madrid, Spain; Instituto de Astrof ísica de Andaluc ía (CSIC), Glorieta de la Astronom ía, E-18080 Granada, Spain), AP(Max-Planck-Institut f ür extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AQ(Instituto de F ísica Te órica, (UAM/CSIC), Universidad Aut ónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM +CSIC, Cantoblanco, E-28049 Madrid, Spain), AR(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK; Sorbonne Universit és, Institut Lagrange de Paris (ILP), 98 bis Boulevard Arago, F-75014 Paris, France), AS(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ, UK), AT(Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA), AU(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), AV(School of Physics and Astronomy, University of St Andrews, St Andrews, Fife KY16 9SS, UK), AW(Instituto de Fisica, Universidad Nacional Autonoma de Mexico, Apdo. Postal 20-364, Mexico City, M éxico.)
%B Monthly Notices of the Royal Astronomical Society
%V 466
%D 2017
%8 April 1, 2017
%P 2242-2260
%K gravitation;  surveys;  cosmological parameters;  cosmology: observations;  dark energy;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2017MNRAS.466.2242B
%X We investigate the anisotropic clustering of the Baryon Oscillation 
Spectroscopic Survey (BOSS) Data Release 12 sample, which consists of 
1198 006 galaxies in the redshift range 0.2 < z < 0.75 and a sky 
coverage of 10 252 deg<SUP>2</SUP>. We analyse this data set in Fourier 
space, using the power-spectrum multipoles to measure redshift-space 
distortions simultaneously with the Alcock-Paczynski effect and the 
baryon acoustic oscillation scale. We include the power-spectrum 
monopole, quadrupole and hexadecapole in our analysis and compare our 
measurements with a perturbation-theory-based model, while properly 
accounting for the survey window function. To evaluate the reliability 
of our analysis pipeline, we participate in a mock challenge, which 
results in systematic uncertainties significantly smaller than the 
statistical uncertainties. While the high-redshift constraint on 
fσ<SUB>8</SUB> at z<SUB>eff</SUB> = 0.61 indicates a small 
(˜1.4σ) deviation from the prediction of the Planck 
ΛCDM (Λ cold dark matter) model, the low-redshift 
constraint is in good agreement with Planck ΛCDM. This paper is 
part of a set that analyses the final galaxy clustering data set from 
BOSS. The measurements and likelihoods presented here are combined with 
others in Alam et al. to produce the final cosmological constraints from 
BOSS.
%3 10.1093/mnras/stw3298
%= eprint: arXiv:1607.03150
%@ 0035-8711

%0 Journal Article
%T The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: tomographic BAO analysis of DR12 combined sample in Fourier space
%A Zhao, Gong-Bo 
%A Wang, Yuting 
%A Saito, Shun 
%A Wang, Dandan 
%A Ross, Ashley J. 
%A Beutler, Florian 
%A Grieb, Jan Niklas 
%A Chuang, Chia-Hsun 
%A Kitaura, Francisco-Shu 
%A Rodriguez-Torres, Sergio 
%A Percival, Will J. 
%A Brownstein, Joel R. 
%A Cuesta, Antonio J. 
%A Eisenstein, Daniel J. 
%A Gil-Marín, Héctor 
%A Kneib, Jean-Paul 
%A Nichol, Robert C. 
%A Olmstead, Matthew D. 
%A Prada, Francisco 
%A Rossi, Graziano 
%A Salazar-Albornoz, Salvador 
%A Samushia, Lado 
%A Sánchez, Ariel G. 
%A Thomas, Daniel 
%A Tinker, Jeremy L. 
%A Tojeiro, Rita 
%A Weinberg, David H. 
%A Zhu, Fangzhou
%+ AA(National Astronomy Observatories, Chinese Academy of Science, Beijing, 100012, P.R.China; Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK <EMAIL>gbzhao@nao.cas.cn</EMAIL>), AB(National Astronomy Observatories, Chinese Academy of Science, Beijing, 100012, P.R.China; Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AC(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Starße 1, D-85740 Garching bei München, Germany; Kavli Institute for the Physics and Mathematics of the Universe (IPMU), The University of Tokyo, Kashiwa, Chiba 277-8583, Japan), AD(National Astronomy Observatories, Chinese Academy of Science, Beijing, 100012, P.R.China), AE(Center for Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USA; Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AF(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA), AG(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany; Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Scheinerstraße 1, D-81679 München, Germany), AH(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AI(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AJ(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AK(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AL(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AM(Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC- UB), Martí i Franquès 1, E-08028 Barcelona, Spain), AN(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), AO(Institut Lagrange de Paris (ILP), Sorbonne Universités, 98 bis Boulevard Arago, F-75014 Paris, France; Laboratoire de Physique Nucléaire et de Hautes Energies, Université Pierre et Marie Curie, 4 Place Jussieu, F-75005 Paris, France; Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AP(Laboratoire d'Astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, CH-1290 Versoix, Switzerland), AQ(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AR(Department of Chemistry and Physics, King's College, 133 North River St, Wilkes Barre, PA 18711, USA), AS(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AT(Department of Astronomy and Space Science, Sejong University, Seoul 143-747, Korea), AU(Universitäts-Sternwarte München, Ludwig-Maximilians-Universität Munchen, Scheinerstraße 1, D-81679 München, Germany; Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AV(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AW(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AX(Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AY(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), AZ(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK), BA(Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA; Center for Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USA), BB(Department of Physics, Yale University, New Haven, CT 06511, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 466
%D 2017
%8 April 1, 2017
%P 762-779
%K galaxies: distances and redshifts;  cosmological parameters;  cosmology: observations;  dark energy;  distance scale;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2017MNRAS.466..762Z
%X We perform a tomographic baryon acoustic oscillations (BAO) analysis 
using the monopole, quadrupole and hexadecapole of the redshift-space 
galaxy power spectrum measured from the pre-reconstructed combined 
galaxy sample of the completed Sloan Digital Sky Survey Baryon 
Oscillation Spectroscopic Survey (BOSS) Data Release12 covering the 
redshift range of 0.20 < z < 0.75. By allowing for overlap between 
neighbouring redshift slices, we successfully obtained the isotropic and 
anisotropic BAO distance measurements within nine redshift slices to a 
precision of 1.5-3.4 per cent for D<SUB>V</SUB>/r<SUB>d</SUB>, 1.8-4.2 
per cent for D<SUB>A</SUB>/r<SUB>d</SUB> and 3.7-7.5 per cent for H 
r<SUB>d</SUB>, depending on effective redshifts. We provide our BAO 
measurement of D<SUB>A</SUB>/r<SUB>d</SUB> and H r<SUB>d</SUB> with the 
full covariance matrix, which can be used for cosmological implications. 
Our measurements are consistent with those presented in Alam et al., in 
which the BAO distances are measured at three effective redshifts. We 
constrain dark energy parameters using our measurements and find an 
improvement of the Figure-of-Merit of dark energy in general due to the 
temporal BAO information resolved. This paper is a part of a set that 
analyses the final galaxy clustering data set from BOSS.
%3 10.1093/mnras/stw3199
%= eprint: arXiv:1607.03153
%@ 0035-8711

%0 Journal Article
%T PRIMUS+DEEP2: The Dependence of Galaxy Clustering on Stellar Mass and Specific Star Formation Rate at 0.2 < z < 1.2
%A Coil, Alison L. 
%A Mendez, Alexander J. 
%A Eisenstein, Daniel J. 
%A Moustakas, John
%+ AA(Center for Astrophysics and Space Sciences, Department of Physics, University of California, 9500 Gilman Drive, La Jolla, CA 92093, USA <ID system="ORCID">0000-0002-2583-5894</ID>), AB(Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA <ID system="ORCID">0000-0002-7726-1722</ID>), AC(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AD(Department of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211, USA)
%B The Astrophysical Journal
%V 838
%D 2017
%8 April 1, 2017
%K galaxies: evolution;  galaxies: halos;  galaxies: high-redshift;  large-scale structure of universe
%U http://adsabs.harvard.edu/abs/2017ApJ...838...87C
%X We present results on the clustering properties of galaxies as a 
function of both stellar mass and specific star formation rate (sSFR) 
using data from the PRIMUS and DEEP2 galaxy redshift surveys spanning 
0.2< z< 1.2. We use spectroscopic redshifts of over 100,000 
galaxies covering an area of 7.2 deg<SUP>2</SUP> over five separate 
fields on the sky, from which we calculate cosmic variance errors. We 
find that the galaxy clustering amplitude is as strong of a function of 
sSFR as of stellar mass, and that at a given sSFR, it does not 
significantly depend on stellar mass within the range probed here. We 
further find that within the star-forming population and at a given 
stellar mass, galaxies above the main sequence of star formation with 
higher sSFR are less clustered than galaxies below the main sequence 
with lower sSFR. We also find that within the quiescent population, 
galaxies with higher sSFR are less clustered than galaxies with lower 
sSFR, at a given stellar mass. We show that the galaxy clustering 
amplitude smoothly increases with both increasing stellar mass and 
decreasing sSFR, implying that galaxies likely evolve across the main 
sequence, not only along it, before galaxies eventually become 
quiescent. These results imply that the relation of stellar mass to halo 
mass, which connects galaxies to dark matter halos, likely depends on 
sSFR.
%3 10.3847/1538-4357/aa63ec
%= eprint: arXiv:1609.09090
%@ 0004-637X

%0 Journal Article
%T The Color and Stellar Mass Dependence of Small-scale Galaxy Clustering in SDSS-III BOSS
%A Law-Smith, Jamie 
%A Eisenstein, Daniel J.
%+ AA(Department of Astronomy and Astrophysics, University of California Santa Cruz, CA 95064, USA <EMAIL>lawsmith@ucsc.edu</EMAIL> <ID system="ORCID">0000-0001-8825-4790</ID>), AB(Center for Astrophysics, Harvard University, 60 Garden Street, Cambridge, MA 02138, USA)
%B The Astrophysical Journal
%V 836
%D 2017
%8 February 1, 2017
%K cosmology: observations;  galaxies: evolution;  galaxies: halos;  large-scale structure of universe;  methods: statistical
%U http://adsabs.harvard.edu/abs/2017ApJ...836...87L
%X We measure the color and stellar mass dependence of clustering in 
spectroscopic galaxies at 0.6 < z < 0.65 using data from the 
Baryon Oscillation Spectroscopic Survey component of the Sloan Digital 
Sky Survey. We greatly increase the statistical precision of our 
clustering measurements by using the cross-correlation of 66,657 
spectroscopic galaxies to a sample of 6.6 million fainter photometric 
galaxies. The clustering amplitude w(R) is measured as the ratio of the 
mean excess number of photometric galaxies found within a specified 
radius annulus around a spectroscopic galaxy to that from a random 
photometric galaxy distribution. We recover many of the familiar trends 
at high signal-to-noise ratio. We find the ratio of the clustering 
amplitudes of red and blue massive galaxies to be 
{w}<SUB>{red</SUB>}/{w}<SUB>{blue</SUB>}=1.92+/- 0.11 in our smallest 
annulus of 75-125 kpc. At our largest radii (2-4 Mpc), we 
find {w}<SUB>{red</SUB>}/{w}<SUB>{blue</SUB>}=1.24+/- 0.05. Red galaxies 
therefore have denser environments than their blue counterparts at z 
˜ 0.625, and this effect increases with decreasing radius. 
Irrespective of color, we find that w(R) does not obey a simple 
power-law relation with radius, showing a dip around 1 Mpc. Holding 
stellar mass fixed, we find a clear differentiation between clustering 
in red and blue galaxies, showing that clustering is not solely 
determined by stellar mass. Holding color fixed, we find that clustering 
increases with stellar mass, especially for red galaxies at small scales 
(more than a factor of 2 effect over 0.75 dex in stellar mass).
%3 10.3847/1538-4357/836/1/87
%= eprint: arXiv:1702.03933
%@ 0004-637X

%0 Journal Article
%T The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Fourier space
%A Beutler, Florian 
%A Seo, Hee-Jong 
%A Ross, Ashley J. 
%A McDonald, Patrick 
%A Saito, Shun 
%A Bolton, Adam S. 
%A Brownstein, Joel R. 
%A Chuang, Chia-Hsun 
%A Cuesta, Antonio J. 
%A Eisenstein, Daniel J. 
%A Font-Ribera, Andreu 
%A Grieb, Jan Niklas 
%A Hand, Nick 
%A Kitaura, Francisco-Shu 
%A Modi, Chirag 
%A Nichol, Robert C. 
%A Percival, Will J. 
%A Prada, Francisco 
%A Rodriguez-Torres, Sergio 
%A Roe, Natalie A. 
%A Ross, Nicholas P. 
%A Salazar-Albornoz, Salvador 
%A Sánchez, Ariel G. 
%A Schneider, Donald P. 
%A Slosar, Anže 
%A Tinker, Jeremy 
%A Tojeiro, Rita 
%A Vargas-Magaña, Mariana 
%A Vazquez, Jose A.
%+ AA(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA <EMAIL>florian.beutler@port.ac.uk</EMAIL>), AB(Department of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, OH 45701, USA), AC(Department of Physics, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA), AD(Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA), AE(Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan; Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, D-85740 Garching bei München, Germany), AF(Department of Physics and Astronomy, University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, USA; National Optical Astronomy Observatory, 950 N Cherry Ave, Tucson, AZ 85719, USA), AG(Department of Physics and Astronomy, University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, USA), AH(Instituto de Física Teórica (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AI(Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, E-08028 Barcelona, Spain), AJ(Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA), AK(Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA; Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan), AL(Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Scheinerstraße 1, D-81679 München, Germany; Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AM(Department of Astronomy, University of California, Berkeley, CA 94720, USA), AN(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AO(Department of Physics, University of California, Berkeley, CA 94720, USA), AP(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AQ(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AR(Instituto de Física Teórica (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía, E-18080 Granada, Spain), AS(Instituto de Física Teórica (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain), AT(Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA), AU(Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ, UK), AV(Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Scheinerstraße 1, D-81679 München, Germany; Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AW(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AX(Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA), AY(Brookhaven National Laboratory, Upton, NY 11973, USA), AZ(Center for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USA), BA(School of Physics and Astronomy, University of St. Andrews, St Andrews, Fife KY16 9SS, UK), BB(Instituto de Fisica, Universidad Nacional Autonoma de Mexico, Apdo. Postal 20-364, Mexico), BC(Brookhaven National Laboratory, Upton, NY 11973, USA)
%B Monthly Notices of the Royal Astronomical Society
%V 464
%D 2017
%8 January 1, 2017
%P 3409-3430
%K gravitation;  surveys;  cosmological parameters;  cosmology: observations;  dark energy;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2017MNRAS.464.3409B
%X We analyse the baryon acoustic oscillation (BAO) signal of the final 
Baryon Oscillation Spectroscopic Survey (BOSS) data release (DR12). Our 
analysis is performed in the Fourier space, using the power spectrum 
monopole and quadrupole. The data set includes 1198 006 galaxies over 
the redshift range 0.2 < z < 0.75. We divide this data set into 
three (overlapping) redshift bins with the effective redshifts 
z<SUB>eff</SUB> = 0.38, 0.51 and 0.61. We demonstrate the reliability of 
our analysis pipeline using N-body simulations as well as ˜1000 
MultiDark-Patchy mock catalogues that mimic the BOSS-DR12 target 
selection. We apply density field reconstruction to enhance the BAO 
signal-to-noise ratio. By including the power spectrum quadrupole we can 
separate the line of sight and angular modes, which allows us to 
constrain the angular diameter distance D<SUB>A</SUB>(z) and the Hubble 
parameter H(z) separately. We obtain two independent 1.6 and 1.5 per 
cent constraints on D<SUB>A</SUB>(z) and 2.9 and 2.3 per cent 
constraints on H(z) for the low (z<SUB>eff</SUB> = 0.38) and high 
(z<SUB>eff</SUB> = 0.61) redshift bin, respectively. We obtain two 
independent 1 and 0.9 per cent constraints on the angular averaged 
distance D<SUB>V</SUB>(z), when ignoring the Alcock-Paczynski effect. 
The detection significance of the BAO signal is of the order of 8σ 
(post-reconstruction) for each of the three redshift bins. Our results 
are in good agreement with the Planck prediction within Λ cold 
dark matter. This paper is part of a set that analyses the final galaxy 
clustering data set from BOSS. The measurements and likelihoods 
presented here are combined with others in Alam et al. to produce the 
final cosmological constraints from BOSS.
%3 10.1093/mnras/stw2373
%= eprint: arXiv:1607.03149
%@ 0035-8711

%0 Journal Article
%T The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the configuration-space clustering wedges
%A Sánchez, Ariel G. 
%A Scoccimarro, Román 
%A Crocce, Martín 
%A Grieb, Jan Niklas 
%A Salazar-Albornoz, Salvador 
%A Dalla Vecchia, Claudio 
%A Lippich, Martha 
%A Beutler, Florian 
%A Brownstein, Joel R. 
%A Chuang, Chia-Hsun 
%A Eisenstein, Daniel J. 
%A Kitaura, Francisco-Shu 
%A Olmstead, Matthew D. 
%A Percival, Will J. 
%A Prada, Francisco 
%A Rodríguez-Torres, Sergio 
%A Ross, Ashley J. 
%A Samushia, Lado 
%A Seo, Hee-Jong 
%A Tinker, Jeremy 
%A Tojeiro, Rita 
%A Vargas-Magaña, Mariana 
%A Wang, Yuting 
%A Zhao, Gong-Bo
%+ AA(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany <EMAIL>arielsan@mpe.mpg.de</EMAIL>), AB(Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, NY 10003, USA), AC(Institut de Ciències de l'Espai, IEEC-CSIC, Campus UAB, Carrer de Can Magrans, s/n, E-08193 Bellaterra, Barcelona, Spain), AD(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany; Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Scheinerstrasse 1, D-81679 Munich, Germany), AE(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany; Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Scheinerstrasse 1, D-81679 Munich, Germany), AF(Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, E-38205 La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, Av. del Astrofísico Francisco Sánchez s/n, E-38206 La Laguna, Tenerife, Spain), AG(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany; Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Scheinerstrasse 1, D-81679 Munich, Germany), AH(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK; Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AI(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AJ(Instituto de Física Teórica, UAM/CSIC, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany), AK(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), AL(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; Leibniz-Institut für Astrophysik Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany; Departments of Physics and Astronomy, University of California, Berkeley, CA 94720, USA), AM(Department of Chemistry and Physics, King's College, 133 North River St, Wilkes Barre, PA 18711, USA), AN(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AO(Instituto de Física Teórica, UAM/CSIC, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía, E-18080 Granada, Spain), AP(Instituto de Física Teórica, UAM/CSIC, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AQ(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK; Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, OH 43210, USA), AR(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK; Kansas State University, Manhattan, KS 66506, USA; National Abastumani Astrophysical Observatory, Ilia State University, 2A Kazbegi Ave, GE-1060 Tbilisi, Georgia), AS(Department of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, OH 45701, USA), AT(Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, NY 10003, USA), AU(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK), AV(Instituto de Física, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, 01000 México, D.F., Mexico; Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15217, USA; McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15217, USA), AW(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK; National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, People's Republic of China), AX(Institute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK; National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, People's Republic of China)
%B Monthly Notices of the Royal Astronomical Society
%V 464
%D 2017
%8 January 1, 2017
%P 1640-1658
%K cosmological parameters;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2017MNRAS.464.1640S
%X We explore the cosmological implications of anisotropic clustering 
measurements in configuration space of the final galaxy samples from 
Data Release 12 of the Sloan Digital Sky Survey III Baryon Oscillation 
Spectroscopic Survey. We implement a new detailed modelling of the 
effects of non-linearities, bias and redshift-space distortions that can 
be used to extract unbiased cosmological information from our 
measurements for scales s ≳ 20 h<SUP>-1</SUP> Mpc. We combined the 
information from Baryon Oscillation Spectroscopic Survey (BOSS) with the 
latest cosmic microwave background (CMB) observations and Type Ia 
supernovae samples and found no significant evidence for a deviation 
from the Λ cold dark matter (ΛCDM) cosmological model. In 
particular, these data sets can constrain the dark energy 
equation-of-state parameter to w<SUB>DE</SUB> = -0.996 ± 0.042 
when to be assumed time independent, the curvature of the Universe to 
Ω<SUB>k</SUB> = -0.0007 ± 0.0030 and the sum of the 
neutrino masses to ∑m<SUB>ν</SUB> < 0.25 eV at 95 per cent 
confidence levels. We explore the constraints on the growth rate of 
cosmic structures assuming f(z) = 
Ω<SUB>m</SUB>(z)<SUP>γ</SUP> and obtain γ = 0.609 
± 0.079, in good agreement with the predictions of general 
relativity of γ = 0.55. We compress the information of our 
clustering measurements into constraints on the parameter combinations 
D<SUB>V</SUB>(z)/r<SUB>d</SUB>, F<SUB>AP</SUB>(z) and 
fσ<SUB>8</SUB>(z) at z<SUB>eff</SUB> = 0.38, 0.51 and 0.61 with 
their respective covariance matrices and find good agreement with the 
predictions for these parameters obtained from the best-fitting 
ΛCDM model to the CMB data from the Planck satellite. This paper 
is part of a set that analyses the final galaxy clustering data set from 
BOSS. The measurements and likelihoods presented here are combined with 
others by Alam et al. to produce the final cosmological constraints from 
BOSS.
%3 10.1093/mnras/stw2443
%= eprint: arXiv:1607.03147
%@ 0035-8711

%0 Journal Article
%T The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: combining correlated Gaussian posterior distributions
%A Sánchez, Ariel G. 
%A Grieb, Jan Niklas 
%A Salazar-Albornoz, Salvador 
%A Alam, Shadab 
%A Beutler, Florian 
%A Ross, Ashley J. 
%A Brownstein, Joel R. 
%A Chuang, Chia-Hsun 
%A Cuesta, Antonio J. 
%A Eisenstein, Daniel J. 
%A Kitaura, Francisco-Shu 
%A Percival, Will J. 
%A Prada, Francisco 
%A Rodríguez-Torres, Sergio 
%A Seo, Hee-Jong 
%A Tinker, Jeremy 
%A Tojeiro, Rita 
%A Vargas-Magaña, Mariana 
%A Vazquez, Jose A. 
%A Zhao, Gong-Bo
%+ AA(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstrasse 1, D-85741 Garching, Germany <EMAIL>arielsan@mpe.mpg.de</EMAIL>), AB(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstrasse 1, D-85741 Garching, Germany; Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Scheinerstrasse 1, D-81679 Munich, Germany), AC(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstrasse 1, D-85741 Garching, Germany; Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Scheinerstrasse 1, D-81679 Munich, Germany), AD(Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15217, USA; McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15217, USA), AE(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA), AF(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, OH 43210, USA), AG(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AH(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AI(Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, E-08028 Barcelona, Spain), AJ(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AK(Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany; Departments of Physics and Astronomy, University of California, Berkeley, CA 94720, USA), AL(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK), AM(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Instituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía, E-18080 Granada, Spain), AN(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica, Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain), AO(Department of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, OH 45701, USA), AP(Center for Cosmology and Particle Physics, New York University, New York, NY 10003, USA), AQ(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK), AR(Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15217, USA; McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15217, USA; Instituto de Fisica, Universidad Nacional Autónoma de México, Apartado Postal 20-364, 01000 México D.F., Mexico), AS(Brookhaven National Laboratory, Building 510, Upton, NY 11973, USA), AT(Institute of Cosmology & Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth PO1 3FX, UK; National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, P.R. China)
%B Monthly Notices of the Royal Astronomical Society
%V 464
%D 2017
%8 January 1, 2017
%P 1493-1501
%K cosmological parameters;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2017MNRAS.464.1493S
%X The cosmological information contained in anisotropic galaxy clustering 
measurements can often be compressed into a small number of parameters 
whose posterior distribution is well described by a Gaussian. We present 
a general methodology to combine these estimates into a single set of 
consensus constraints that encode the total information of the 
individual measurements, taking into account the full covariance between 
the different methods. We illustrate this technique by applying it to 
combine the results obtained from different clustering analyses, 
including measurements of the signature of baryon acoustic oscillations 
and redshift-space distortions, based on a set of mock catalogues of the 
final SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS). Our 
results show that the region of the parameter space allowed by the 
consensus constraints is smaller than that of the individual methods, 
highlighting the importance of performing multiple analyses on galaxy 
surveys even when the measurements are highly correlated. This paper is 
part of a set that analyses the final galaxy clustering data set from 
BOSS. The methodology presented here is used in Alam et al. to produce 
the final cosmological constraints from BOSS.
%3 10.1093/mnras/stw2495
%= eprint: arXiv:1607.03146
%@ 0035-8711

%0 Journal Article
%T The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: observational systematics and baryon acoustic oscillations in the correlation function
%A Ross, Ashley J. 
%A Beutler, Florian 
%A Chuang, Chia-Hsun 
%A Pellejero-Ibanez, Marcos 
%A Seo, Hee-Jong 
%A Vargas-Magaña, Mariana 
%A Cuesta, Antonio J. 
%A Percival, Will J. 
%A Burden, Angela 
%A Sánchez, Ariel G. 
%A Grieb, Jan Niklas 
%A Reid, Beth 
%A Brownstein, Joel R. 
%A Dawson, Kyle S. 
%A Eisenstein, Daniel J. 
%A Ho, Shirley 
%A Kitaura, Francisco-Shu 
%A Nichol, Robert C. 
%A Olmstead, Matthew D. 
%A Prada, Francisco 
%A Rodríguez-Torres, Sergio A. 
%A Saito, Shun 
%A Salazar-Albornoz, Salvador 
%A Schneider, Donald P. 
%A Thomas, Daniel 
%A Tinker, Jeremy 
%A Tojeiro, Rita 
%A Wang, Yuting 
%A White, Martin 
%A Zhao, Gong-bo
%+ AA(Center for Cosmology and AstroParticle Physics, The Ohio State University, Columbus, OH 43210, USA; Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK <EMAIL>ashley.jacob.ross@gmail.com</EMAIL>), AB(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK; Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA), AC(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AD(Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea, s/n, E-38205 La Laguna, Tenerife, Spain; Departamento Astrofísica, Universidad de La Laguna (ULL), E-38206 La Laguna, Tenerife, Spain), AE(Department of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, OH 45701, USA), AF(Instituto de Fisica, Universidad Nacional Autonoma de Mexico, Apdo. Postal 20-364, Mexico), AG(Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, E-08028 Barcelona, Spain), AH(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AI(Department of Physics, Yale University, 260 Whitney Ave, New Haven, CT 06520, USA; Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AJ(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AK(Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Scheinerstraße 1, D-81679 München, Germany; Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AL(Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA), AM(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AN(Department of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USA), AO(Harvard-Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA), AP(Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA; Department of Physics, McWilliams Center for Cosmology, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA; Department of Physics, University of California, Berkeley, CA 94720, USA), AQ(Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany), AR(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AS(Department of Chemistry and Physics, King's College, 133 North River St, Wilkes Barre, PA 18711, USA), AT(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Instituto de Astrofísica de Andalucía (CSIC), E-18080 Granada, Spain), AU(Instituto de Física Teórica, (UAM/CSIC), Universidad Autónoma de Madrid, Cantoblanco, E-28049 Madrid, Spain; Campus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, Spain; Departamento de Física Teórica M8, Universidad Autonóma de Madrid (UAM), Cantoblanco, E-28049 Madrid, Spain), AV(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Starße 1, D-85740 Garching bei München, Germany; Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan), AW(Universitäts-Sternwarte München, Ludwig-Maximilians-Universität München, Scheinerstraße 1, D-81679 München, Germany; Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, Germany), AX(Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA), AY(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), AZ(Department of Physics, Center for Cosmology and Particle Physics, New York University, 4 Washington Place, New York, NY 10003, USA), BA(School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK), BB(National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, P.R. China; Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK), BC(Lawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USA; Department of Physics, University of California, Berkeley, CA 94720, USA; Department of Astronomy, University of California, Berkeley, CA 94720, USA), BD(Institute of Cosmology & Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth PO1 3FX, UK; National Astronomy Observatories, Chinese Academy of Science, Beijing 100012, P.R. China)
%B Monthly Notices of the Royal Astronomical Society
%V 464
%D 2017
%8 January 1, 2017
%P 1168-1191
%K cosmology: observations;  large-scale structure of Universe
%U http://adsabs.harvard.edu/abs/2017MNRAS.464.1168R
%X We present baryon acoustic oscillation (BAO) scale measurements 
determined from the clustering of 1.2 million massive galaxies with 
redshifts 0.2 < z < 0.75 distributed over 9300 deg<SUP>2</SUP>, as 
quantified by their redshift-space correlation function. In order to 
facilitate these measurements, we define, describe, and motivate the 
selection function for galaxies in the final data release (DR12) of the 
SDSS III Baryon Oscillation Spectroscopic Survey (BOSS). This includes 
the observational footprint, masks for image quality and Galactic 
extinction, and weights to account for density relationships intrinsic 
to the imaging and spectroscopic portions of the survey. We simulate the 
observed systematic trends in mock galaxy samples and demonstrate that 
they impart no bias on BAO scale measurements and have a minor impact on 
the recovered statistical uncertainty. We measure transverse and radial 
BAO distance measurements in 0.2 < z < 0.5, 0.5 < z < 0.75, 
and (overlapping) 0.4 < z < 0.6 redshift bins. In each redshift 
bin, we obtain a precision that is 2.7 per cent or better on the radial 
distance and 1.6 per cent or better on the transverse distance. The 
combination of the redshift bins represents 1.8 per cent precision on 
the radial distance and 1.1 per cent precision on the transverse 
distance. This paper is part of a set that analyses the final galaxy 
clustering data set from BOSS. The measurements and likelihoods 
presented here are combined with others in Alam et al. to produce the 
final cosmological constraints from BOSS.
%3 10.1093/mnras/stw2372
%= eprint: arXiv:1607.03145
%@ 0035-8711

%0 Journal Article
%T PRIMUS: One- and Two-halo Galactic Conformity at 0.2 < z < 1
%A Berti, Angela M. 
%A Coil, Alison L. 
%A Behroozi, Peter S. 
%A Eisenstein, Daniel J. 
%A Bray, Aaron D. 
%A Cool, Richard J. 
%A Moustakas, John
%+ AA(Center for Astrophysics and Space Sciences, Department of Physics, University of California, 9500 Gilman Drive, La Jolla, San Diego, CA 92093, USA <ID system="ORCID">0000-0003-3582-6649</ID>), AB(Center for Astrophysics and Space Sciences, Department of Physics, University of California, 9500 Gilman Drive, La Jolla, San Diego, CA 92093, USA <ID system="ORCID">0000-0002-2583-5894</ID>), AC(Department of Astronomy, University of California at Berkeley, Berkeley, CA 94720, USA;), AD(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AE(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA), AF(MMT Observatory, Tucson, AZ 85721, USA), AG(Department of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211, USA)
%B The Astrophysical Journal
%V 834
%D 2017
%8 January 1, 2017
%K galaxies: evolution;  galaxies: statistics
%U http://adsabs.harvard.edu/abs/2017ApJ...834...87B
%X We test for galactic conformity at 0.2< z< 1.0 to a projected 
distance of 5 Mpc using spectroscopic redshifts from the PRism 
MUlti-object Survey (PRIMUS). Our sample consists of ˜60,000 
galaxies in five separate fields covering a total of ˜5.5 square 
degrees, which allows us to account for cosmic variance. We identify 
star-forming and quiescent “isolated primary” (I.e., 
central) galaxies using isolation criteria and cuts in specific star 
formation rate. We match the redshift and stellar mass distributions of 
these samples to control for correlations between quiescent fraction and 
redshift and stellar mass. We detect a significant (>3σ) 
one-halo conformity signal, or an excess of star-forming neighbors 
around star-forming central galaxies, of ˜5% on scales of 0-1 Mpc 
and a 2.5σ two-halo signal of ˜1% on scales of 1-3 Mpc. 
These signals are weaker than those detected in the Sloan Digital Sky 
Survey and are consistent with galactic conformity being the result of 
large-scale tidal fields and reflecting assembly bias. We also measure 
the star-forming fraction of central galaxies at fixed stellar mass as a 
function of large-scale environment and find that central galaxies are 
more likely to be quenched in overdense environments, independent of 
stellar mass. However, we find that environment does not affect the star 
formation efficiency of central galaxies, as long as they are forming 
stars. We test for redshift and stellar mass dependence of the 
conformity signal within our sample and show that large volumes and 
multiple fields are required at intermediate redshift to adequately 
account for cosmic variance.
%3 10.3847/1538-4357/834/1/87
%= eprint: arXiv:1608.05084
%@ 0004-637X