mmt science symposium1 “false-color” 0.5-7 kev x-ray image of the bootes field thousands of agns...

MMT Science Symposium 1

“false-color” 0.5-7 keV X-ray image of the Bootes field

Thousands of AGNs in the 9.3 square degree Bootes field

* X-ray and infrared properties of AGN

* Using AGN to Map Cosmic Structure

MMT Science SymposiumJune 2006


CollaboratorsChandra (CfA)S. MurrayW. FormanA. KenterR. NarayanR. HickoxC. JonesSpitzer (JPL/Caltech/CfA)P. EisenhardtM. BrodwinV. GorjianM. Pahreand the IRAC Shallow Survey Team

Optical spectroscopy (OSU/Arizona)K. KochanekD. Eisensteinand the AGES Team

Optical photometry (NOAO)B. JanuzziA. DeyK. Brandand the NDWFS Team

and more…


Outline of TalkOutline of Talk

intointo AGNAGN What is the Xbootes Survey?What is the Xbootes Survey? Using Hectospec, Chandra, Spitzer to Using Hectospec, Chandra, Spitzer to

characterize AGNcharacterize AGN X-ray and IR properties of BLAGNX-ray and IR properties of BLAGN Mapping the cosmic web with AGNMapping the cosmic web with AGN The local environment of AGNThe local environment of AGN Future PlansFuture Plans

intointo AGNAGN What is the Xbootes Survey?What is the Xbootes Survey? Using Hectospec, Chandra, Spitzer to Using Hectospec, Chandra, Spitzer to

characterize AGNcharacterize AGN X-ray and IR properties of BLAGNX-ray and IR properties of BLAGN Mapping the cosmic web with AGNMapping the cosmic web with AGN The local environment of AGNThe local environment of AGN Future PlansFuture Plans


Bootes survey imaging dataOptical photometry: NOAO DWFS photometry B,R,I,J,K (Januzzi & Dey 1999)

Infrared: Spitzer IRAC Shallow Survey (Eisenhardt et al. 2004)

The Bootes field was observed with the IRAC camera on Spitzer in four bands: 3.6, 4.5, 5.8, 8.0 microns.

~30,000 sources are detected in all four IRAC bands.

X-ray: Chandra XBootes survey (Murray et al. 2004, Kenter et al. 2005), > 3000 X-ray sources


MMT Bootes surveyOptical spectroscopy: AGES survey w/ MMT/Hectospec

The first sample contains ~1000 broad line AGNs, 80 narrow-line AGNs, and 27,000 “normal” galaxies.


The XBootes SurveyThe XBootes SurveyXbootes:Xbootes: 126 Chandra ACIS pointings 126 Chandra ACIS pointings 5 ksec each field (630 ksec)5 ksec each field (630 ksec) Joint GTO and GO programJoint GTO and GO program 1414hh 32 32mm +34 +34 06’ 06’ 4642 sources detected (>=2 cts)4642 sources detected (>=2 cts)

625 spurious625 spurious 3293 sources detected (>=4 cts)3293 sources detected (>=4 cts)

22 spurious22 spurious

42 extended sources (>=10 cts)42 extended sources (>=10 cts)

ffminmin= 4(8)x10= 4(8)x10-15-15 erg cm erg cm-2-2 s s-1-1 (0.5-7 keV) (0.5-7 keV) 98% sources >=4 cts matched to NDWFS 98% sources >=4 cts matched to NDWFS

candidates (R<=26)candidates (R<=26)

Xbootes:Xbootes: 126 Chandra ACIS pointings 126 Chandra ACIS pointings 5 ksec each field (630 ksec)5 ksec each field (630 ksec) Joint GTO and GO programJoint GTO and GO program 1414hh 32 32mm +34 +34 06’ 06’ 4642 sources detected (>=2 cts)4642 sources detected (>=2 cts)

625 spurious625 spurious 3293 sources detected (>=4 cts)3293 sources detected (>=4 cts)

22 spurious22 spurious

42 extended sources (>=10 cts)42 extended sources (>=10 cts)

ffminmin= 4(8)x10= 4(8)x10-15-15 erg cm erg cm-2-2 s s-1-1 (0.5-7 keV) (0.5-7 keV) 98% sources >=4 cts matched to NDWFS 98% sources >=4 cts matched to NDWFS

candidates (R<=26)candidates (R<=26)

Murray et al. ApJ S 161, 1 (2005)

Kenter et al. ApJ S 161, 9 (2005)

Brand et al. ApJ, 641, 140 (2006)


Multiwavelength studies of AGNX-rays: direct probe of central engine and accretion luminosity

Optical/UV: probe of regions close to (BL) or farther from (NL) the black hole; most affected by extinction

Infrared: due to reprocessed emission from dust, heated by the central engine

ALL THREE can be used to select AGN

(Manners 2002)

(Urry & Padovani 1995)


AGN and Galaxy Evolution Survey (AGES)AGN and Galaxy Evolution Survey (AGES) MMT/Hectospec fiber MMT/Hectospec fiber

spectrographspectrograph 300 fibers/field300 fibers/field Complete galaxies I<19.5Complete galaxies I<19.5 Complete X-ray >4 cts and Complete X-ray >4 cts and

I<21.5I<21.5 ~27,000 galaxies~27,000 galaxies ~1,500 X-ray selected~1,500 X-ray selected

E.g., z=3.53 AGN with 12 X-ray E.g., z=3.53 AGN with 12 X-ray counts - - Lcounts - - Lxx=3x10=3x104545 erg s erg s-1-1 (0.5- (0.5- 7keV)7keV)

MMT/Hectospec fiber MMT/Hectospec fiber spectrographspectrograph

300 fibers/field300 fibers/field Complete galaxies I<19.5Complete galaxies I<19.5 Complete X-ray >4 cts and Complete X-ray >4 cts and

I<21.5I<21.5 ~27,000 galaxies~27,000 galaxies ~1,500 X-ray selected~1,500 X-ray selected

E.g., z=3.53 AGN with 12 X-ray E.g., z=3.53 AGN with 12 X-ray counts - - Lcounts - - Lxx=3x10=3x104545 erg s erg s-1-1 (0.5- (0.5- 7keV)7keV)

CXOXB J142547.4+352719


Samples of AGN

-> X-ray/optical Broad-line AGN-> X-ray/optical Narrow-line AGN-> X-ray/optical “normal” galaxies (XBONGS?)

-> Mid-infrared selected AGN(color-color criteria, Stern et al. 2005, Lacy et al. 2004)

photometric redshiftsfor those objects withno spectra (Brodwin etal. 2006)


Infrared selection of AGN

Following Stern et al. (2005)


X-ray vs. IR luminosity

Broad-line AGNs

IR AGNs

“Normal” galaxies

Narrow-line AGNs



Broad-line AGNs

IR AGNs

“Normal” galaxies

Narrow-line AGNs



Broad-line AGNsIR AGNs

Average X-ray fluxes from

stacking analysis


IR vs. UV luminosity (Hickox et al. 2006)

Broad-line AGNs

IR AGNs

* Using AGN to Observe the Cosmic Web

* Using AGN to Observe the Cosmic Web

Xbootes 9.3 Square Degree SurveyXbootes 9.3 Square Degree SurveyXbootes 9.3 Square Degree SurveyXbootes 9.3 Square Degree Survey


Large Scale StructureLarge Scale Structurez=0 z=1 z=3

OCDM

SCDM

LCDM

Jenkins et al., 1998 (ApJ, 499, 20-40)

Other SurveysOther Surveys DEEP2DEEP2

0.7 < z < 1.40.7 < z < 1.4 4 x 1 sq. deg4 x 1 sq. deg 40,000 redshifts40,000 redshifts

2dF2dF z<0.2z<0.2 1500 sq. deg1500 sq. deg 200,000 redshifts200,000 redshifts

SDSS (~12 AGN /sq deg)SDSS (~12 AGN /sq deg) z<2.3 z<2.3 6600 sq. deg6600 sq. deg 850,000 redshifts850,000 redshifts

Other SurveysOther Surveys DEEP2DEEP2

0.7 < z < 1.40.7 < z < 1.4 4 x 1 sq. deg4 x 1 sq. deg 40,000 redshifts40,000 redshifts

2dF2dF z<0.2z<0.2 1500 sq. deg1500 sq. deg 200,000 redshifts200,000 redshifts

SDSS (~12 AGN /sq deg)SDSS (~12 AGN /sq deg) z<2.3 z<2.3 6600 sq. deg6600 sq. deg 850,000 redshifts850,000 redshifts


Redshift DistributionsRedshift Distributions


• Not X-ray Selected (18,820)

• Most galaxies with z<0.7

• 531 z>1, must be AGN, but not detected in shallow x-ray survey

• X-ray Selected (1531)

• 306 “galaxies”

• 50 “narrow emission line”

• 1175 “AGN’

Survey Results (0 < z < 5)Survey Results (0 < z < 5)


Structure (0.25 < z < 0.50)Structure (0.25 < z < 0.50)


X-ray Selected AGN X-ray Selected AGN

At low z (<0.7), map the same At low z (<0.7), map the same structures as seen using galaxiesstructures as seen using galaxies

At higher z, similar X-ray AGN At higher z, similar X-ray AGN structures continue to be seenstructures continue to be seen

X-ray selected AGN are an efficient X-ray selected AGN are an efficient means to study large scale structure in means to study large scale structure in the redshift range 1-3 the redshift range 1-3

At low z (<0.7), map the same At low z (<0.7), map the same structures as seen using galaxiesstructures as seen using galaxies

At higher z, similar X-ray AGN At higher z, similar X-ray AGN structures continue to be seenstructures continue to be seen

X-ray selected AGN are an efficient X-ray selected AGN are an efficient means to study large scale structure in means to study large scale structure in the redshift range 1-3 the redshift range 1-3


2 Point 3-D Correlation for X-ray AGN2 Point 3-D Correlation for X-ray AGN

RedshiftRedshift rr0 0 hh100100

0.0 - 1.00.0 - 1.0 8.68.6

1.0 - 1.51.0 - 1.5 6.16.1

1.5 - 2.01.5 - 2.0 4.04.0Possible Evolution

X-ray AGN

( r ) =( r/r0)-1.71

r0 = 6.7h100


Mapping structure with AGNMapping structure with AGN Shallow survey covering Shallow survey covering

9.3 sq. deg yields 1200 9.3 sq. deg yields 1200 X-ray selected AGNX-ray selected AGN

AGN map the same AGN map the same structure at z<0.7 as do structure at z<0.7 as do galaxiesgalaxies

X-ray selected AGN can X-ray selected AGN can map large scale map large scale structures out to z~3 structures out to z~3 and search for evolution and search for evolution of structure as predicted of structure as predicted in numerical simulations in numerical simulations

Shallow survey covering Shallow survey covering 9.3 sq. deg yields 1200 9.3 sq. deg yields 1200 X-ray selected AGNX-ray selected AGN

AGN map the same AGN map the same structure at z<0.7 as do structure at z<0.7 as do galaxiesgalaxies

X-ray selected AGN can X-ray selected AGN can map large scale map large scale structures out to z~3 structures out to z~3 and search for evolution and search for evolution of structure as predicted of structure as predicted in numerical simulations in numerical simulations


AGN EnvironmentAGN Environment

• Local Galaxy Density may impact:

• Activity

• Type

• Luminosity

• …

• Local Galaxy Density may impact:

• Activity

• Type

• Luminosity

• …

Redshift Slice 0.41<z<0.43


Future PlansFuture Plans Chandra AO-8/HectospecChandra AO-8/Hectospec

Chandra proposal to re-survey Chandra proposal to re-survey Bootes to double number of Bootes to double number of AGN and measure variabiltyAGN and measure variabilty

1/3 with I<22.5 ?? -> 1300 1/3 with I<22.5 ?? -> 1300 additional Hectospec targetsadditional Hectospec targets

Questions --Questions -- How does environment affect the How does environment affect the

AGN (XBONGS vs BLAGN)?AGN (XBONGS vs BLAGN)? Why is X-ray emission less for IR Why is X-ray emission less for IR

brighter galaxies?brighter galaxies? Does cosmic structure change Does cosmic structure change

with redshift? with redshift? Can we identify a large population Can we identify a large population

of absorbed AGN?of absorbed AGN?

Chandra AO-8/HectospecChandra AO-8/Hectospec Chandra proposal to re-survey Chandra proposal to re-survey

Bootes to double number of Bootes to double number of AGN and measure variabiltyAGN and measure variabilty

1/3 with I<22.5 ?? -> 1300 1/3 with I<22.5 ?? -> 1300 additional Hectospec targetsadditional Hectospec targets

Questions --Questions -- How does environment affect the How does environment affect the

AGN (XBONGS vs BLAGN)?AGN (XBONGS vs BLAGN)? Why is X-ray emission less for IR Why is X-ray emission less for IR

brighter galaxies?brighter galaxies? Does cosmic structure change Does cosmic structure change

with redshift? with redshift? Can we identify a large population Can we identify a large population

of absorbed AGN?of absorbed AGN?


Summary (by Ryan Hickox)

Observations in a big wide field of nine whole square degreesShow us thousands upon thousands of new active galaxies

We can pick them out with Chandra, but if we wish to look insteadWe can also use their colors in the Spitzer infrared

As these AGNs get brighter in the UV and IR,Their X-rays also brighten, but more slow than linear

And while the picture for the broad-line AGNs is somewhat surea lot of IR objects may still be somewhat obscured

It will be great to test a model and to see what it predicts!Thank you all for your attention, here at MMT 2006


Infrared: AGN vs. starburst contribution?

Broad-lineAGNs

IR AGNs


Infrared selection of AGN

Dust heated by AGN

Colder dust/PAHs

(Glikman et al. 2005)

(Lagache et al. 2004)


IR vs. UV luminosity

Broad-line AGNs

IR AGNs

mmt science symposium1 “false-color” 0.5-7 kev x-ray image of the bootes field thousands of agns...

Documents

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infrared properties

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