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)
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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