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
MMT Science Symposium 2
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…
MMT Science Symposium 3
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
MMT Science Symposium 4
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 Science Symposium 5
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.
MMT Science Symposium 6
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)
MMT Science Symposium 7
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)
MMT Science Symposium 8
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
MMT Science Symposium 9
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)
MMT Science Symposium 10
Infrared selection of AGN
Following Stern et al. (2005)
MMT Science Symposium 11
X-ray vs. IR luminosity
Broad-line AGNs
IR AGNs
“Normal” galaxies
Narrow-line AGNs
MMT Science Symposium 12
X-ray vs. IR luminosity
Broad-line AGNs
IR AGNs
“Normal” galaxies
Narrow-line AGNs
MMT Science Symposium 13
X-ray vs. IR luminosity
Broad-line AGNsIR AGNs
Average X-ray fluxes from
stacking analysis
MMT Science Symposium 14
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
MMT Science Symposium 16
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
MMT Science Symposium 17
Redshift DistributionsRedshift Distributions
MMT Science Symposium 18
• 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)
MMT Science Symposium 19
Structure (0.25 < z < 0.50)Structure (0.25 < z < 0.50)
MMT Science Symposium 20
Structure (0.25 < z < 0.50)Structure (0.25 < z < 0.50)
MMT Science Symposium 21
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
MMT Science Symposium 22
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
MMT Science Symposium 23
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
MMT Science Symposium 24
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
MMT Science Symposium 25
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?
MMT Science Symposium 26
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
MMT Science Symposium 27
Infrared: AGN vs. starburst contribution?
Broad-lineAGNs
IR AGNs
MMT Science Symposium 28
Infrared selection of AGN
Dust heated by AGN
Colder dust/PAHs
(Glikman et al. 2005)
(Lagache et al. 2004)
MMT Science Symposium 29
IR vs. UV luminosity
Broad-line AGNs
IR AGNs