WISE-NVSS AGN: Luminous Quasars Caught in Their Youth
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Transcript of WISE-NVSS AGN: Luminous Quasars Caught in Their Youth
Atacama Large Millimeter/submillimeter ArrayExpanded Very Large Array
Robert C. Byrd Green Bank TelescopeVery Long Baseline Array
WISE-NVSS AGN: Luminous Quasars Caught in Their Youth
Carol Lonsdale, NRAOCollaborators: 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
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
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, 09Lanzuisi et al 2009 (figure) Power-law DOGs (Dust
Obscured Galaxies) Dey et al 2008Bussman et al 2012 (figures)
• 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
Donley (2008) selection less contaminated with starbursts.
Lacy et al. (2013) more complete for AGN
Previous Mid-IR AGN Selection Methods and Samples
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)
WISEcolorselection:156 srcs, 0.3%
Stern et al 2013 AGN selection
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Eisenhardt et al. 2012Wu et al. 2103Bridge et al. 2013
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 2013brighter
redder
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 mJy rms• 55% detections
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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] NeIV
Lyα NV CIV
MgIICIII]
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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)
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Templates from Polletta et al. (2008)Torus model: Honig et al. (2006)
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
As expected, the Spitzer-selected DOGs are not as red
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C. Lonsdale, Dubrovnik, May 13, 2014
Exceptionally Obscured DOGs ?
Torus Models Rowan-Robinson 2000
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• Av = 50 mag.
• n( r ) ~ r-1
• Tinner =500-1600K
• Touter=50-160K
Full Torus + Starburst ModelingA. Efstatiou et al. in prep.
JVLA X-band A and B-array Imaging, 156 QSOs
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8.4 kpc
X-band (8-12 GHz) A-array
Majority unresolved on 1-2 kpc scales
VLBA Results
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VLBA imaging of 90 at 5GHz beam ~ 100pc
VLBA Results
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J and Ks Imaging at VLT/ISAACAndrew Blain et al. in prep
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Conclusions
C. Lonsdale, Dubrovnik, May 13, 2014
• 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
• 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
Previous Mid-IR AGN Selection Methods and Samples
MIR torus model, Sajina et al (2012) Covering range of Nenkova et al (2008) clumpy torus models
Luminosities & dust masses
Sajina et al. (2012)
Td = 120K
Td = 58K
Td = 71K
Td = 105K
Td = 147K
Free Td FIR fitβ=1.5
Fixed Td FIR fit50K, β=230K, β=1.5
Lacy et al50K model
Log
L 3GH
z (W
/Hz)
Log LFIR
Log LAGN
Log
L FIR
Log LAGN
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