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PFS Science White Paper PFS Science White Paper Prepared by the PFS Science Collaborations Contents 1 Introduction: Rationale for and Capabilities of a Wide-Field Spectrograph for Subaru . 5 1.1 Scientific Rationale ..................................... 5 1.2 The history of the PFS concept .............................. 6 1.3 Galaxy Redshifts from zero to > 10 ............................ 8 1.4 Large-Scale Structure, Baryon Oscillations and Weak Lensing ............. 9 1.5 Galaxy Evolution Studies ................................. 10 1.6 Spectroscopy of quasars .................................. 11 1.7 Spectroscopic Surveys at z > 5 .............................. 12 1.8 Stellar Spectroscopy .................................... 13 References .......................................... 13 2 Spectrograph Design ..................................... 15 2.1 The Collimator and the Fibers .............................. 16 2.2 The Gratings ........................................ 17 2.3 The Dichroics ........................................ 18 2.4 The Cameras ........................................ 18 2.5 Spectrograph Performance ................................. 20 2.6 The Next Steps ....................................... 22 2.7 Science and Survey Design ................................. 22 2.8 Spectrograph Design .................................... 23 3 HSC Survey .......................................... 31 4 Cosmology with SuMIRe HSC/PFS Survey ......................... 33 4.1 Executive Summary .................................... 33 4.2 Background ......................................... 34 4.3 Cosmology with SuMIRe HSC/PFS galaxy surveys ................... 39 4.4 Needs for accurately modeling BAO ........................... 64 4.5 Modeling BAOs in 2D from perturbation theory .................... 64 4.6 Implications to SuMIRe PFS survey ........................... 68 4.7 Testing gravity with multipole power spectrum ..................... 69 References .......................................... 71 5 Galactic Archaeology ..................................... 77 5.1 Background ......................................... 77 5.2 Key Science Goals ..................................... 78 5.3 Proposed Survey and its Requirements .......................... 93 References .......................................... 106 6 Galaxy evolution ....................................... 109 6.1 Introduction: Reaching the epoch (z ∼ 2) of massive galaxy formation and black hole growth109 6.2 Unique spectral capabilities for galaxy surveys with PFS ................ 110 6.3 A wide area survey for galaxy and AGN studies ..................... 111 3 Contents 6.4 Science ............................................ 114 References .......................................... 133 7 Dust-shrouded Star Formation and Black Hole Accretion ................. 135 7.1 Background ......................................... 135 7.2 Key Science Goals ..................................... 138 7.3 Proposed Survey and its Requirements .......................... 144 7.4 Synergy with SPICA .................................... 145 References .......................................... 145 8 High Redshift Galaxies .................................... 147 8.1 Summary .......................................... 147 8.2 Science Drivers ....................................... 147 8.3 Proposed Survey and its Requirements (Tentative Plan) ................ 161 References .......................................... 162 9 QSO (AGN) science with PFS ................................ 167 9.1 Science Goals ........................................ 167 9.2 QSO Luminosity Function at z < 6 ............................ 172 9.3 Clustering Properties and Environments of QSOs at z < 6 ............... 177 9.4 Evolution of Supermassive Blackholes (SMBHs) at z < 6 ................ 179 9.5 Cosmic Chemical Evolution at z < 6 ........................... 183 9.6 Identification of Further QSOs at z > 6 ......................... 187 9.7 Ancillary Brown Dwarf Science .............................. 193 9.8 Low-Luminosity AGNs Selected by Optical Variability ................. 198 9.9 Summary of the Request for PFS Specification and Survey ............... 201 References .......................................... 202 10 Quasar Absorption Lines ................................... 205 10.1 A Brief History of the Studies of the Quasar Absorption Lines ............. 205 10.2 Key Science Goals ..................................... 207 10.3 Proposed Survey and its Requirements .......................... 210 References .......................................... 212 11 Star Formation History .................................... 215 11.1 Science Goals ........................................ 215 11.2 Proposed Survey and its Requirements .......................... 217 References .......................................... 219 4 1 Introduction: Rationale for and Capabilities of a Wide-Field Spectrograph for Subaru Michael Strauss (Princeton), Jim Gunn (Princeton), et al. 1.1 Scientific Rationale Wide-field surveys of the sky are tremendously powerful and versatile astronomical tools. While they are often designed with very specific scientific goals, their census of the heavens typically has impact in a broad range of astronomical areas. The best example of this is the Sloan Digital Sky Survey (SDSS; York et al. (2000)). It was conceived at a time (the late 1980’s) when the nature of the large-scale distribution of galaxies was only hinted at by the largest redshift surveys of the time (de Lapparent et al. 1986; Kirshner et al. 1987) and so it took as its goal a comprehensive redshift survey of a million galaxies over a volume of about 2 × 108 h−3Mpc3, to characterize the galaxy power spectrum and topology of large-scale structure on the largest scales. The SDSS redshift survey indeed fulfilled this scientific goal (Strauss et al. 2009; Gott et al. 2005; Eisenstein et al. 2005; Percival et al. 2010), but the imaging and spectroscopic data gathered to do so allowed it to make fundamental breakthroughs in many other areas of astrophysics, including asteroid science (Ivezi´cet al. 2002), the discovery of brown dwarfs (Strauss et al. 1999); the largest sample by far of spectroscopically confirmed white dwarfs (Eisenstein et al. 2006), the kinematics (Bond et al. 2010) and substructure (Belokurov et al. 2006) of the Galactic Halo, the discovery of dwarf companions to the Milky Way, the detailed photometric properties of nearby galaxies (Blanton et al. 2003), the measurement of the Supernova 1a Hubble Diagram (Kessler et al. 2009), the evolution of quasars (Richards et al. 2006), and the reionization of the early universe (Fan et al. 2006), to name but a few. Indeed, there have been over 3500 refereed papers to date that reference SDSS in their title or abstract, and based on the number of highly cited papers, it is considered the most productive telescope facility of the past decade (beating Keck, HST, and others; Madrid & Macchetto (2009)). Inspired by the SDSS and other wide-field surveys in the ultraviolet (GALEX), near-infrared (2MASS), and radio (Becker et al. 1995), a wide variety of next-generation imaging surveys are on-going or planned, including of course Hyper-SuprimeCam (HSC) on Subaru. However, one of the great strengths of the SDSS is the combination of its imaging and spectroscopic surveys, and while there are wide-field spectroscopic surveys being planned for the next generation (HETDEX on the Hobby-Eberly Telescope, BigBOSS on the Kitt Peak 4-m, the Large Sky Area Multi-Object Fibre Spectroscopic Telescope (LAMOST) in China, and the near-infrared Fiber Multi-Object Spectrograph (FMOS) on Subaru), these are all limited in wavelength coverage, throughput, or 5 Chapter 1: Introduction: Rationale for and Capabilities of a Wide-Field Spectrograph for Subaru scope of the survey they will carry out. This white paper describes the exciting possibility of building a wide-field fiber-fed spectrograph for the Subaru Telescope, which is unique among 8- meter-class telescopes in having a field of view of 1.5◦ diameter. The scientific potential for such a facility is vast, and this white paper outlines some of the principal scientific opportunities it would enable. We make the case that reaching the full scientific potential of the next generation of imaging surveys in general and HSC in particular, from the formation history of the Milky Way halo to the nature of galaxies at the epoch of reionization, requires a massively multiplexed spectrograph with high throughput and resolution and a wavelength coverage from 3800A˚ to 1.3 microns. This wavelength coverage is driven by the need to obtain emission-line redshifts of galaxies over the full range (z = 0 to z > 10, with no gaps). The wide-field corrector on the Subaru telescope has limited throughput outside of this spectral range. In addition, the natural atmospheric cutoff between the J and H bands, and the need for a cooled spectrograph at wavelengths beyond 1.3µm, make this a natural cutoff for such a spectrograph. In what follows, we refer to this instrument as the Prime Focus Spectrograph (PFS). Indeed, we imagine four spectrographs, each receiving light from 600 fibers with 1.1300 entrance aperture, and each covering the full spectral range from 3800A˚ to 1.3 microns. This white paper is still in its early stages. The various chapters have been largely written inde- pendently, and therefore don’t make completely uniform assumptions about the capabilities of the spectrograph, including wavelength coverage, resolution,
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