WISE-NVSS AGN: Luminous Quasars Caught in Their Youth

1. 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, KateyAlatalo, Luis Ho, Peter Eisenhardt, Tom Jarrett, Robyn Smith Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array

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) • Deyet al 2008 • Bussman et al 2012 (figures)

4. Previous Mid-IR AGN Selection Methods and Samples • Lacy et al (2013): extensive, complete survey of quasars selected using generous IRAC color selection: • 670 redshifts, 521 AGN, Reaching 1014 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 Donley (2008) selection less contaminated with starbursts. Lacy et al. (2013) more complete for AGN C. Lonsdale, Dubrovnik, May 13, 2014

5. The WISE-NVSS Mid-IR/Radio-selected, Obscured, QSO studyLonsdale 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. The WISE Red Samples compared to Spitzer DOGs Eisenhardt et al. 2012 Wu et al. 2103 Bridge et al. 2013 Very similar WISE selection but RADIO-BLIND WISE: Bridge et al 2013 brighter • Has all-sky coverage with enough depth to see quasars to z > 4 • Finds brighter, redder & rarer samples than Spitzer redder C. Lonsdale, Dubrovnik, May 13, 2014

7. 49 observed with Cycle 0 ALMA at 345 GHz to constrain cool dust • TBD from 1st ALMA conf slides. observations, images, spectra, luminosities, radio powers • 15-23 antennas • 90s on source • 0.3-0.5 mJyrms • 55% detections C. Lonsdale, Dubrovnik, May 13, 2014

8. Spectroscopy for 43; Luminosities MgII CIV CIV • 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 HeII CIII] NeIV 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) Templates from Polletta et al. (2008) Torus model: Honig et al. (2006) C. Lonsdale, Dubrovnik, May 13, 2014

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 ? C. Lonsdale, Dubrovnik, May 13, 2014

13. Torus Models Rowan-Robinson 2000 • Av = 50 mag. • n( r ) ~ r-1 • Tinner =500-1600K • Touter=50-160K C. Lonsdale, Dubrovnik, May 13, 2014

14. Full Torus + Starburst ModelingA. Efstatiou et al. in prep.

15. JVLA X-band A and B-array Imaging, 156 QSOs X-band (8-12 GHz) A-array Majority unresolved on 1-2 kpc scales 8.4 kpc C. Lonsdale, Dubrovnik, May 13, 2014

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

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

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

19. Conclusions • Strongly MIR-dominated • Redder at λ < 10μm than any other known quasar samples • Luminosities 1012.5– 1014 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 C. Lonsdale, Dubrovnik, May 13, 2014

20. Previous Mid-IR AGN Selection Methods and Samples • Lacy et al (2013): extensive, complete survey of quasars selected using generous IRAC color selection: • 670 redshifts, 521 AGN, Reaching 1014 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

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

22. No correlation: radio-FIR luminosity Lacy et al 50K model Log LFIR Log L3GHz (W/Hz) Log LFIR De Breuck et al (2010) hi z RGs Log LAGN More AGN-dominated than Lacy et al (2103) overall MIR-selected AGN population • Strong correlation: radio-AGN luminosity • Probably a redshift-selection effect Log LAGN