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

C. Lonsdale, Dubrovnik, May 13, 2014

C. Lonsdale, Dubrovnik, May 13, 2014

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

C. Lonsdale, Dubrovnik, May 13, 2014

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]

C. Lonsdale, Dubrovnik, May 13, 2014

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)

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

C. Lonsdale, Dubrovnik, May 13, 2014

C. Lonsdale, Dubrovnik, May 13, 2014

Exceptionally Obscured DOGs ?

Torus Models Rowan-Robinson 2000

C. Lonsdale, Dubrovnik, May 13, 2014

• 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

C. Lonsdale, Dubrovnik, May 13, 2014

8.4 kpc

X-band (8-12 GHz) A-array

Majority unresolved on 1-2 kpc scales

VLBA Results

C. Lonsdale, Dubrovnik, May 13, 2014

VLBA imaging of 90 at 5GHz beam ~ 100pc

VLBA Results

C. Lonsdale, Dubrovnik, May 13, 2014

J and Ks Imaging at VLT/ISAACAndrew Blain et al. in prep

C. Lonsdale, Dubrovnik, May 13, 2014

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