Answers ( in addition to questions) from quasar surveys Scott Croom (IoA, University of Sydn

Answers ( in addition to questions) from quasar surveys Scott Croom (IoA, University of Sydn

Answers ( in addition to questions) from quasar surveys Scott Croom (IoA, University of Sydn

Birkett, Melody, News Anchor has reference to this Academic Journal, PHwiki organized this Journal Answers ( in addition to questions) from quasar surveys Scott Croom (IoA, University of Sydney) With contributions from: Stephen Fine (Sydney), Jose da Angela, Tom Shanks (Durham) Gordon Richards (Drexel), Lance Miller, Ana Babic (Ox as long as d), Joss Bl in addition to -Hawthorn, Simon Ellis (Sydney) + the 2QZ, 2SLAQ in addition to AUS teams Outline Why quasar surveys (reasons, then in addition to now) 2QZ in addition to 2SLAQ. Evolution: the quasar luminosity function. Clustering, bias in addition to host mass. BH masses from quasar spectra. Unanswered questions Why quasar surveys (then) Original 2QZ science aims (circa 1995): LSS on scales 1 to 1000h-1Mpc. Clustering evolution as long as m in addition to bias. Alcock-Pacynski (1979) test as long as . QSO Luminosity function. In the mean time: SNe in addition to Dark Energy. M- relation. Reverbration mapping in addition to “virial methods”. WMAP in addition to other CMB measurements.

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Why quasar surveys (now) Highest impact 2QZ work: QSO luminosity function. Clustering evolution: implications as long as SMBHs in addition to galaxy as long as mation. Spectral analysis. The 2QZ: Vital statistics 2dF QSO Redshift Survey UKST photometry UV/optical colour selection: u,bJ,r bJ=18.0-20.85 722 deg2 2dF spectroscopy z~0.3-3.0 Vol: ~19 Gpc3 23660 QSOs Croom et al. (2001, 2004) 2SLAQ: Vital Statistics 2dF-SDSS LRG And QSO Survey SDSS photometry ugriz (~UVX) selection g<21.85 192 deg2 2dF spectroscopy z~0.3-3.0 Vol: ~5 Gpc3 10,000 faint QSOs + 10,000 LRGs (see David Wake talk) Richards et al. (2005), Croom et al. (2008) The 2SLAQ QSO LF Croom et al. 2008; (SDSS LF: Richards et al. 2006) The 2SLAQ+SDSS QSO LF Croom et al. (2008), see also Richards et al. (2005) Downsizing Brightest QSOs peak at z~2.5 (or higher). Faintest QSOs peak at z~1 (or lower). Croom et al. (2008) Downsizing (X-ray) Hasinger et al. (2005) 2QZ clustering evolution Croom et al. (2005) see also Myers et al. (2006; 2007), Porciani et al. (2004; 2006) QSO bias Croom et al. (2005) QSO DMH host mass Croom et al. (2005) The blue cloud in addition to red sequence MDH(QSO) ~ few x 1012h-1Msun ~ transition mass Simulations: Croton et al. (2006) Combo-17: Borch et al. (2006) SDSS: Blanton et al. (2006) 2SLAQ QSO clustering da Angela et al. (2008) 2SLAQ QSO clustering da Angela et al. (2008) Lidz et al. (2006), z=2 BH masses in addition to the virial method Broad-line emission region is assumed to be virialised in addition to so the width of a line gives vBLR. The radius-luminosity relation derived from reverberation mapping campaigns gives rBLR. rBLR~L0.5 Kaspi et al. (2005) 2SLAQ, 2QZ in addition to SDSS line widths Fine et al. (2008) Line width dispersion Fine et al. (2008) Comparison with Models Fine et al. (2008) – comparison to Hopkins, Hernquist et al. merger models. MBH vs MDH Mean zero-point: log(MBH)=8.40.2 at log(MDH)=12.5 Well matched to Robertson et al. (2006) simulations. Bigger points = higher redshift. Fine et al. (2006) Unanswered questions Radio emission – how The build up of SMBHs at z>3. Feedback, does it work If so, how Feedback Hopkins et al. (2005) After 1st passage. Merger of BHs. Quasar phase. Quasar has ended. (T = time in Gyr) Evidence as long as mergers Low-z HST host galaxy imaging (Schade et al. 2000) ACS: Bennert et al. (2008)

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Dissecting galaxies Single fibres: Missed flux. No spatial in as long as mation. Systematic biases. Can we combine the multiplexing of single fibre surveys in addition to the power of integral-field spectroscopy Hexabundles Fibres that can use existing positioning technology, but with multiple cores. Cladding only needs to be ~5-10 thickness. 1×91 manufactured, 1×397 by 2010. Expect excellent photometric qualities. 1×19 selective illumination 1×61 Bl in addition to -Hawthorn et al. (2008) Strawman concept FLAMES on VLT: 24 arcmin f-o-v Existing robot positioner (AAO built OzPoz). 40 1×397 hexabundles (~7 arcsec diameter). Feeding 4 MUSE (Laurent et al. 2006) style spectrographs. Science: Galaxy dynamics, merging. Stellar populations. AGN hosts. Bl in addition to -Hawthorn et al. (2008)

Summary 2SLAQ QSO LF: Not pure luminosity evolution. Significant downsizing: faint AGN peak at lower z. QSO Clustering: QSOs inhabit similar dark matter halos at z=0.5-2.5. No luminosity dependence found so far. Implies a range of accretion efficiencies as long as SMBHs. BH mass distribution: Distribution of BL widths narrows at bright magitudes. Appears bounded by Mass fn in addition to L/LEdd. BH mass vs DMH mass: M-M relation not evolving.

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