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Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array WISE-NVSS AGN: Luminous.

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Presentation on theme: "Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array WISE-NVSS AGN: Luminous."— Presentation transcript:

1 Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array WISE-NVSS AGN: Luminous Quasars Caught in Their Youth Carol Lonsdale, NRAO Collaborators: Mark Lacy, Amy Kimball, Jim Condon, Andrew Blain, Minjin Kim, Mark Whittle, Colin Lonsdale, Paul Martini, Jim Condon, Roberto Assef, Dan Stern, Cho-Wei Tsai, Belinda Wilkes, Carrie Bridge, Sara Petty, Katey Alatalo, Luis Ho, Peter Eisenhardt, Tom Jarrett, Robyn Smith

2 Outline Goals – Understand the nature of the reddest and most luminous obscured QSOs – Laboratories for studying the interactions between young radio jets and the ISM – Signposts to the most massive halos during the epoch when massive clusters began virializing. The WISE-NVSS red QSO sample ALMA, VLA & VLBA results Conclusions C. Lonsdale, Dubrovnik, May 13, 2014

3 Previous Mid-IR AGN Selection Methods and Samples AGN are found in a ‘color wedge’ in the Spitzer/IRAC color-color diagram. Lacy et al 2004 (figure) Stern et al 2005 X-ray observations: the reddest sources in MIR/optical are highly obscured. Polletta et al 2007, 08, 09 Lanzuisi et al 2009 (figure) Power-law DOGs (Dust Obscured Galaxies) Dey et al 2008 Bussman et al 2012 (figures)

4 Lacy et al (2013): extensive, complete survey of quasars selected using generous IRAC color selection: – 670 redshifts, 521 AGN, Reaching L  – 0.5 < z < 4.5 – Sample is dominated by obscured AGN – Evidence for morphological disturbances – Differ from SMGs: Higher dust temperatures Lower CO masses Weaker PAHs C. Lonsdale, Dubrovnik, May 13, 2014 Donley (2008) selection less contaminated with starbursts. Lacy et al. (2013) more complete for AGN Previous Mid-IR AGN Selection Methods and Samples

5 The WISE-NVSS Mid-IR/Radio-selected, Obscured, QSO study Lonsdale et al (2014) Cross-match of WISE very red selection with NVSS compact radio- sources Radio selection: indicate (young) AGN present investigate effects of jet-induced feedback signpost the most massive clusters / protoclusters (Venemans et al 2007) WISE color selection: 156 srcs, 0.3% Stern et al 2013 AGN selection C. Lonsdale, Dubrovnik, May 13, 2014

6 Eisenhardt et al Wu et al Bridge et al Very similar WISE selection but RADIO-BLIND WISE: The WISE Red Samples compared to Spitzer DOGs Has all-sky coverage with enough depth to see quasars to z > 4 Finds brighter, redder & rarer samples than Spitzer Bridge et al 2013 brighter redder

7 49 observed with Cycle 0 ALMA at 345 GHz to constrain cool dust TBD from 1 st ALMA conf slides. observations, images, spectra, luminosities, radio powers antennas 90s on source mJy rms 55% detections C. Lonsdale, Dubrovnik, May 13, 2014

8 Spectroscopy for 43; Luminosities SOAR 4m, CTIO, Palomar 200 inch, VLT/XShooter: high excitation narrow lines Magellan 8m, FIRE NIR: [OIII]: evidence for shocks & outflows; (Kim et al 2103) ULIRG - HyLIRG AGN luminosities CIV MgII CIV HeII CIV CIII]NeI V Lyα NV CIV MgII CIII] C. Lonsdale, Dubrovnik, May 13, 2014

9 Low 870 / 22μm flux ratios: MIR-dominated Most robust result comes from using the data as observed no assumptions about SED shape or k-correction required -The ALMA sample lies well below starburst- dominated SMGs and most templates -Some, especially the limits, are consistent with intrinsic SEDs of Mullaney et al (2011) C. Lonsdale, Dubrovnik, May 13, 2014 Templates from Polletta et al. (2008) Torus model: Honig et al. (2006)

10 Normalized (4.6μm) Rest-frame SEDs Our Radio Intermediate sample and the radio-blind WISE samples are similar in MIR SED shape Herschel & ALMA data: SED shape is AGN-dominated Much redder in MIR than templates MIR-dominated: Hot DOGs

11 As expected, the Spitzer-selected DOGs are not as red C. Lonsdale, Dubrovnik, May 13, 2014

12 Exceptionally Obscured DOGs ?

13 Torus Models Rowan-Robinson 2000 C. Lonsdale, Dubrovnik, May 13, 2014 Av = 50 mag. n( r ) ~ r -1 T inner = K T outer =50-160K

14 Full Torus + Starburst Modeling A. Efstatiou et al. in prep.

15 JVLA X-band A and B-array Imaging, 156 QSOs C. Lonsdale, Dubrovnik, May 13, kpc X-band (8-12 GHz) A-array Majority unresolved on 1-2 kpc scales

16 VLBA Results C. Lonsdale, Dubrovnik, May 13, 2014 VLBA imaging of 90 at 5GHz beam ~ 100pc

17 VLBA Results C. Lonsdale, Dubrovnik, May 13, 2014

18 J and Ks Imaging at VLT/ISAAC Andrew Blain et al. in prep C. Lonsdale, Dubrovnik, May 13, 2014

19 Conclusions C. Lonsdale, Dubrovnik, May 13, 2014 Strongly MIR-dominated Redder at λ < 10μm than any other known quasar samples Luminosities – L  Similar to Spitzer PL DOGs but redder and more MIR- dominated SFRs hard to constrain because SEDs can be fit with warm AGN-heated dust Compact in the radio at 8 GHz on kpc scales Range of morphologies at 5GHz on few pc scales

20 Lacy et al (2013): extensive, complete survey of quasars selected using generous IRAC color selection: – 670 redshifts, 521 AGN, Reaching L  – 0.5 < z < 4.5 – Sample is dominated by obscured AGN – Evidence for morphological disturbances – Differ from SMGs: Higher dust temperatures Lower CO masses Weaker PAHs C. Lonsdale, Dubrovnik, May 13, 2014 Previous Mid-IR AGN Selection Methods and Samples

21 MIR torus model, Sajina et al (2012) Covering range of Nenkova et al (2008) clumpy torus models Luminosities & dust masses Sajina et al. (2012) T d = 120K T d = 58K T d = 71K T d = 105K T d = 147K Free T d FIR fit β=1.5 Fixed T d FIR fit 50K, β =2 30K, β =1.5

22 Lacy et al 50K model Log L 3GHz (W/Hz) Log L FIR Log L AGN Log L FIR Log L AGN De Breuck et al (2010) hi z RGs More AGN-dominated than Lacy et al (2103) overall MIR-selected AGN population No correlation: radio-FIR luminosity Strong correlation: radio- AGN luminosity Probably a redshift- selection effect


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