pptx - Leiden Observatory
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Radio source surveys and populations Ken Kellermann National Radio Astronomy Observatory Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array Radio Survey Discoveries • • • • • • June 13, 2013 Radio galaxies (1949) Cosmic evolution (1955) Quasars (1963) IPS (1964) Pulsars (1967) Gravitational lenses (1979) Georgefest 2 Radio source surveys and populations • Radio source surveys – History – Curent status – Problems • VLA and JVLA Deep Surveys – CDFS & ECDFS – Lockman Hole (SWIRES) • Populations – Strong source population – MicroJy population – NanoJy population? • RQ Quasars June 13, 2013 Georgefest 3 Radio Source Surveys 13,000 hr 3000 hr 2400 hr 2000 hr 1700 hr 1000 hr Norris et al., 2013 Georgefest 4 Radio galaxies “Positions of Three Discrete Sources of Galactic Radio-Frequency Radiation” – Bolton, Stanley, and Slee, 1949 Crab M87 NGC 5128 1954 Cygnus A, z = 0.05 Baade & Minkowski, 1954 June 13, 2013 Georgefest 5 Radio Source Counts π π = πΎπ π₯ π₯ = −1.5 Sydney Mills Cross Bernie Mills X = -1.85 X=-3 Cambridge 2C and 3C Martin Ryle Georgefest 6 Radio Source Surveys VLA, WSRT, ATCA, GMRT Molonglo 100 MHz – 22 GHz e-MERLIN, LOFAR, ASKAP, MeerKAT, SKA All Sky surveys Cosmology-Large Scale Structure FR I & FR II Radio Galaxies, RL Quasars • • • • • Limited Area Surveys Populations – Galaxy Evolution AGN, SFG, RQ Quasars • • • • • • NVSS FIRST WENSS SUMSS AT20 Georgefest E-CDFS HDFN HDFS COSMOS SWIRES - Lockman Hole Phoenix 7 Owen & Morrison, 2008 Condon (1984) compilation FR I & FR II Radio Galaxies – Quasars Kellermann et al., 2008 June 13, 2013 Georgefest 8 JVLA Observations of the OwenMorrison field (SWIRE) Lockman Hole) • α = 10h46m00s, δ = +59°01′00″ • ν = 3 πΊπ»π§ (2 GHz BW) • C configuration (3-km) • θ = 8 arcsec • τ = 50 hrs • σn = 1.0 μJy • σc = 1.2 μJy Georgefest 9 MicroJy Radio Source Counts O&M 2008 Condon 1989 Condon 2012 Problems • • • μJy count discrepancy natural confusion at 100 nJy Non thermal sky temperature • • • • • • • Sample Variance – NO Noise bias Statistical weight corrections primary beam Bandwidth smearing Time smearing corrections Multiple component sources • Resolution corrections Log Jy Georgefest 10 ARCADE 2 – Excess Sky Brightness ππ(3πΊπ»π§) = 54 ± 6 ππΎ 3, 8, 10, 30, 90 GHz (Fixen et al. 2011) Georgefest 11 Sky background implications survey limits ARCADE 2 Condon, 1989; Wilman 2008 Condon et al., 2012 _ π > 6 π₯ 104 ππππππ 2 VLA Survey of the CDFS • Chandra 4 Msec Survey (Xue et al. 2011) – 740 X-ray sources – π > 10−17 ergs/sec • VLA Survey (Miller et al., ApJS 205, 2013) – – – – 20 cm; 240 hrs; 6 pointings; Ω = 0.3 deg VLA C configuration (1.6 x 2.8 arcmin resolution) σ = 6.4 μJy 883 radio sources S > 37 μJy • 268 detected at X-rays (Vattakunnel et al, 2010) • 839 (95%) OIR counterparts – 678 (82%) redshifts - 274 spectroscopic (Bonzini et al. 2012) – Spitzer IRAC SIMPLE 3.6, 4.5, 5.8, 8 μm (91%) (Damen et al. 2010) – Spitzer MIPS FIDEL 24 μm (88%) (Dickenson et al. 2007) • Population Classification (Bonzini et al. submitted) June 13, 2013 Georgefest 13 Chandra Deep Field South 7.5 μJy VLA 6.5 μJy 4 Msec exposure 740 X-ray sources S >10-17 ergs/sec ESO 2.2m/WFI z < 27.3 Spectra - VLT GOODS-S HST B, V, I, z < 28 IRAC 3.6, 4.5, 5.8. 8.0 μm MIPS FIDEL 24 μm MUSYC K (VLT) < 22.4 Georgefest Hubble UDF 976 ks exposure B, V, I, z 10,000 galaxies mag 29 14 S > 1 mJy • FR I &S >FR II RG • RL Qusars RL AGN • R > 1.4 • Lx > 1042 ergs/sec • NIR (IRAC) colors • FIR: q < 1.7 June 13, 2013 RQ AGN • R ≤ 1.4 • Lx > 1042 ergs/sec • NIR (IRAC) colors • FIR: q ~ 1.7 Georgefest Star forming galaxies Radio-FIR: q ~ 1.7 R = log(Sr/SV) < 1.7 Lr< 1024 W/Hz Not E galaxy Lx < 1042 ergs/sec No VLBI component μJy radio sources • SFG • AGN • RL AGN • RQ AGN (SF) Padovani et al. in preparation 15 Quasi-stellar Galaxies June 13, 2013 Georgefest 16 Radio Loud and Radio Quiet QSOs Two populations? Separate Population • • • • • • • • • • • • • • • • Continuous Distribution Kellermann et al., 1989, 1994 Miller, et al, 1990, 1993 Sopp & Alexander, 1991 Visnovsky et al., 1992 Peterson, 1997 Kukula et al., 1998 Krolik, 1999 Kembhavi & Narlikar, 1999 Ivezic, et al., 2002, 2004 Laor, 2004 Jiang et al. 2007 White et al., 2007 Zamfir et al., 2008 Balokovic et al., 2012 Kimball et al., 2011 Condon et al., 2013 • • • • • • Georgefest White et al. 2000 Lacy et al., , 2001 Cirasuolo, et al. 2003 Barvainis, et al., 2005 Rafter et al., 2009 Mahony et al. 2012 17 JVLA Observations of SDSS QSOs Kimball et al. 2012, ApJ ,739, L29 • • • • • • • • 179 SDSS QSOs 5 < ν < 7 πΊπ»π§ 14 < π < 19 0.2 < π§ < 0.3; Mi < - 23 τ~ 30 πππ σ ~ 6 μπ½π¦ RQ QSOs πΏ ≤ 1023.5 W/Hz RQ QSOs due to SF in host galaxy Georgefest 18 Summary • All Sky surveys sample powerful radio galaxies and quasars – S > 1 mJy – First indication of cosmic evolution. • microJy radio sources are driven by a mixture of SF and SMBHs • RQ QSOs differ from RL QSOs and are powered primarily by star formation in the host galaxy. • ARCADE 2 observations suggest a population of nanoJy sources not associated with galaxies • Number Counts rapidly converge at low flux desnities – SKA will not be limited by natural confusion • The JVLA is by far the most sensitive radio telescope available – Will learn more about submicroJy population June 13, 2013 Georgefest 19
