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THE ATACAMA COS},Mlogy TELESCOPE: PHYSICAL SU13l\!ITTED 2011l JUNE 25: ACCEPTED 2010 SEPTnmER X Preprint typeset using E~TEX style eIllulateapj v. lIllO/Of) THE ATACAMA COS},mLOGY TELESCOPE: PHYSICAL PROPERTIES AND PT.;'RITY OF A GALAXY CLUSTER SAMPLE SELECTED VIA THE SUNYAEV-ZEUDOVICH EFFECT l 2 2 1 FELIPE MENANTEAU ,JORGE GONZiI.LEZ . JEAN-BAPTISTE JUIN , TOBIAS A. l\IARRIAGE: , ERIK D. REESE!, 2 2 VIVIANA ACQUAVIVAl'l, PAULA AGUIRRE , JOHN vVILLIAl\l ApPEL:'. ANDREvV J. BAKERI, L. FELIPE BARlUENTOS , 7 I i ELlA S. BAl'TISTELd' , J. RICHARD BOND , SUDEEP DAS', AMRUTA J. DESHPANDE , MARK J. DEVLIN , SIMON DICKER", 7 JOANNA DUNKLEY", ROLANDO DUNNER2. THOMAS ESSINGER-HILEMAN'\ JOSEPH VI.'. FOWLER:;, A!\'lIR HAJIAN , lO 11 I2 MARK HALPERN]{), MATTHEW HASSELFIELD , CARLOS HERN ..l.NDEZ-MONTEAGUD0 , l\IATT HILTON , ADAM D. HINCKS~', 2 l RENEE HLOZEK!'. KEVIN M. HUFFENBERGERl:l, JOHN P. HUGHESl.±, LEOPOLDO INFANTE , KENT D. IRWIN!~, JEFF KLEIN , 1 16 I ARTHUR KOSOWSKy " YEN-TING LIN , DANICA MARSDEN , KAVILAN l\IOODLEyI2, MICHAEL D. NIEMACKI~, 17 l l\:IICHAEL R. NOLTA', LYMAN A. PAGE'" LUCAS PARKER'" BRUCE PARTRIDGE , NEELIMA SEHGAL " JON SIEVERS'. i I 21l 2l DAVID N. SPERGEL", SUZANNE T. STAGGS" DANIEL SWETZ· , ERIC SWITZER :!, ROBERT THORNTON . Hy TRAC " l2 RYAN WARNE AND ED VVOLLACK22, submitted 2010 June 25; accepted 2010 Septembe-r 8 ABSTRACT vVe present optical and X-ray properties for the first confirmed galaxy cluster sample selected by the Sunyaev-Zel'dovich Effect from 148 GHz maps over 455 square degrees of sky made with the Atacama Cosmology Telescope. These maps. coupled with multi-band imaging on 4-meter-class optical telescopes, have yielded a sample of 23 galaxy clusters with redshifts between 0.118 and 1.066. Of these 23 clusters, 10 are newly discovered. The selection of this sample is approximately mass limited and essentially independent of redshift. \Ve provide optical positions, images, redshifts and X-ray fluxes and luminosities for the full sample, and X-ray temperatures of an important subset. The mass limit of the full sample is around 8.0 x 1014 j\1s . with a number distribution that peaks around a redshift of 0.4. For the 10 highest significance SZE-seleded cluster candidates, all of which are optically confirmed, the mass threshold is 1 x 10 15 Ms and the redshift range is 0.167 to 1.066. Archival observations from Cha.ndra, XAIM-Newton. and ROSAT provide X-ray luminosities and temperatures that are broadly consistent with this mass threshold. Our optical follow-up procedure also allowed us to assess the purity of the ACT cluster sample. Eighty (one hundred) percent of the 148 GHz candidates with signal-to-noise ratios greater than 5.1 (5.7) are confirmed as massive clusters. The reported sample represents one of the largest SZE-selected sample of massive clusters over all redshifts within a cosmologically-significant survey volume, which will enable cosmological studies as well as future studies on the evolution, morphology, and stellar populations in the most massive clusters in the Universe. Subject hea.dings: cosmic background radiation cosmology: observations galaxies: distances and redshifts galaxies: clusters: general _. large-scale structure of universe 1 Rutgers University, Department of Physics & Astronomy, 136 Frelinghuysen Rd, Piscataway, NJ 08854, USA 14 NIST Quantum Devices Group, 325 Broadway I\lailcode 2 Departamento de Astronomfa y Astroffsica, Facultad de Ffsica, Pontificfa U niversidad CatOlica de Chile, Casilla 306, San­ 817.03, Boulder, CO, USA 80305 tiarro 22, Chile 15 University of Pittsburgh, Physics & Astronomy Depart­ 3" Department of Astrophysical Sciences, Peyton HalL Prince­ ment, 100 Allen Hall, 3941 O'Hara Street, Pittsburgh, PA 15260, ton University, Princeton, NJ 08544, USA USA 16 Institute for the Phvsics and Mathematics of the Universe. 4 University of Pennsylvania, Physics and Astronomy, 209 South 33rd Street, Philadelphia, PA 19104, USA The University of Tokyo; Kashiwa, Chiba 277-8568, Japan 17 Department of Physics and Astronomy, Haverford College, 5 Joseph Henry Laboratories of Physics, Jadwin Hall, Prince­ University, Princeton, NJ, USA 08544 Haverford, PA, USA 19041 Department of Physics. University of Rome "La Sapienza", 18 Kavli Institute for Particle Astrophysics and Cosmology, Piazzale Aldo I\joro 5, 1-00185 Rome, Italy Stanford University, Stanford, CA 94305, USA 19 Kavli Institute for Cosmological Physics. Laboratory for As­ 7 Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON, Canada l\l5S 3H8 trophysics and Space Research. 5620 South Ellis Ave., Chicago, 8 Berkeley Center for Cosmological Physics, UC Berkeley. 366 IL. USA 60637 Le Conte Hall. Berkeley, CA 94720 20 Department of Physics West Chester University of Penn- 9 Department of Astrophysics, Oxford University. Oxford. UK West Chester. PA. 19383 OX13RH Harvard-Smithsonian Center for Astrophysics, Harvard MA 02138 10 Department of Physics and Astronomy, University of Columbia. Vancouver. BC. Canada V6T lZ4 Space Flight Center, Max Planck Institut fur Astrophysik, Postfach 1317. D­ Gat'ching bei l\1iinchen. Germany t Based on observations made with ESO at the La University of KwaZulu-NataL Ast.ronh·v'l<r.s & Silla Observatories under programme ID vo'±.n,-V'J",' Research Unit. School of Mathematical Cluemceb. Visiting astronomer, Cerro Tololo Inter-American Observa­ Africa. National Optical Astronomy Observatory, which are oper­ Department of Physics, of :\1iami, 1320 Campo by the Association of Universities for Research in Astron­ Sano A venue, Coral Gables. FL omy. under contract with the National Science Foundation. 2 Menanteau et a1. 1. INTRODUCTION Clusters of galaxies mark the largest virialized struc­ tureR in the Vniverse, and their formation and evolution 90% rates depend on cosmological parameters and the ki~le­ matieR of the dark matter. The cluster maSH functlOn constrains the normalization of the matter power Hpec­ trurn, typically expressed as 178, the root-mean-square (nns) mass fiuctuation on a scale of 8 h,-IMpc. As.?' result, the number of clusters as a functlOn of redsl:Ift N 50% provides a powerful constraint on b.oth. the expansIon. V history of the Universe and the graVItatIOnal growth of z structure within it (see Carlstrom et al. 2002, and refer­ 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 ences therein). Both functions are strongly infiuence? by the matter content nAJ and the equation of state of the '4 so-called "dark energy" that comprises most of the effec­ 4 XlO M0 tive energy density in the Universe. Galaxy cluster.s also 6 XlO'4M0 harbor a significant fraction of the visible baryons m the 8 xlO'4 M0 Universe, in the form of a hot intracluster medium that 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 leaves an imprint on the Cosmic Microwave Background Redshift (CMB) radiation though the Sunyaev Zel' dovich . Effect (SZE) (Sunyaev & Zel'dovich 1972). At frequencIes be­ Figure L The predicted number of clusters .more massi--:e than 4. 6 and 8 X 10141'..1(-) (solid lines) as a functIOn of redshIft and low the SZ null frequency around 218 GHz, clusters ap­ n~rmalized to unity from the mass function of Tinker et al. (2008). pear as small (;S 1mK) decrements in the temperature For reference we show the 50% and 90% fractional completeness of the CMB. levels as dashed lines. The inset shows the normalized differential Selecting clusters through the strength of their SZE dN/ dz distribution over the same redshift range and maSs limits. signal has key advantages over other metho~s of selec­ jiK Sl/2 array sensitivity to efficiently search for massive tion: (1) it is relatively independent of redshIft, (2) ac­ galaxy clusters using the SZE. T~e first ACT SZE ChIS­ cording to simulations, the SZE fiux (Y y dn. where J tel'S detected in the 2008 observatIon season are reported y is the usual Compton y-parameter) should be cleanly in Hincks et a1. (2009) and the first analysis of the ACT related to the cluster mass with low scatter (Motl et 148 GHz CMB power spectrum reaching to arcminute a1. 2005; Nagai 2006; Reid & Spergel 2006), and (3) ac­ scales is presented in Fowler et al. (2010). cording to simulations the SZE signal is more robust to This paper introduces the first sample of optIcally­ baryonic astrophysics (cooling, AGN f~edback). Tl:us confirmed SZE clusters from the ACT 2008148 GHz data an SZE-selected sample could offer a relIable correlatIOn (see High et a1. 2010, for the recent SPT duster follo,,:-up with cluster mass. which is the key cosmological prop­ study) and, for the first time, character~zes 0 bservatIOn­ erty, particularly at high redshift. However, optical and ally the purity of an SZE survey. For thIS purpose we .se­ X-i'ay observations are crucial to confi~m the ~ZE de­ lected candidate galaxy clusters from ACT maps cove~mg tections and calibrate the Y-mass relatIOn predIcted by 455 square degrees (a comoving volume of 2.46 Gpc' at simulations. z < 1.2) using a rigorous and uniformly controlled.proce­ The SZE has been the focus of a considerable Illnn­ dure (see Marriage et al. 2010). Subsequently, durmg the ber of observational efforts over the past three decades. 2009B semester, we imaged candidates in the bands g, r, Some of the earliest convincing measurements were made and i on 4-m class telescopes to confirm the presence of by Birkinshaw et al. (1984) observing at 20 GHz on the a brightest cluster galaxy (BCG) and an accompanying 40-m telescope of the Owens Valley Radio Observatory. red sequence of cluster members. .. Each individual cluster detection required many hours In two companion papers we deSCrIbe 1Il detaIl the of telescope time, typically spread out over several years.
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