http://hea-www.harvard.edu/CHAMP

The Chandra Multi-wavelength The Chandra Multi-wavelength Project (ChaMP)Project (ChaMP)

PIs: Paul Green & Belinda WilkesPIs: Paul Green & Belinda WilkesX-ray: Dong-Woo KimX-ray: Dong-Woo Kim

Imaging: Rob Cameron, Wayne BarkhouseImaging: Rob Cameron, Wayne BarkhouseSpectroscopy: John SilvermanSpectroscopy: John Silvermanand the ChaMP Collaborationand the ChaMP Collaboration

Serendipitous X-ray Survey using Chandra Archival Data

http://hea-www.harvard.edu/CHAMP

Principal MotivationsPrincipal Motivations

Sample Sample X-ray selectedX-ray selected AGN across AGN across L,zL,z plane planeStudy populations contributing to the CXRBStudy populations contributing to the CXRBFind high-Find high-zz clusters to constrain Cosmology clusters to constrain CosmologyStudy cosmic variance and clusteringStudy cosmic variance and clusteringSample DLySample DLyαα absorbers to XSQSOs absorbers to XSQSOsDetect mass limits of stellar coronal emissionDetect mass limits of stellar coronal emission

Quasar and AGN Evolution: Quasar and AGN Evolution: What do we know? What do we know?

Optical surveys: Unobscured population (view the BLR and/or NLR)

Technically feasible for wide and deep sky coverage to sample to z~6

0<z<2 depletion of fuel? (Cavaliere & Vittorini 2000) z>3 SMBH growth and highly efficient accretion? (Wyithe & Loeb 2002 etc.)

2dF (Boyle et al. 2000) SDSS (Fan et al. 2001)

Quasar and AGN EvolutionQuasar and AGN EvolutionPast X-ray Past X-ray surveyssurveys

Cosmic X-Ray Background (CXRB):

Significant obscured population

(Gilli et al. 2001, Comastri et al. 1995)

Einstein Medium Sensitivity Survey

(Maccacaro et al. 1991; EMSS)

420 AGNs, z<2 and fx>10-13 erg s-1 cm-2

resolved ~40% CXRB at 2 keV

ROSAT (Miyaji et al. 2000)

Compilation of various depth surveys

690 AGNs with 8 at z>3

resolved ~90% 0.5-2.0 keV CXRB

Luminosity evolution similar to optical surveys

ROSAT Luminosity function

Space Density of Luminous QuasarsSpace Density of Luminous Quasars

Optical and radio Optical and radio LFs peak at LFs peak at zz~2~2

X-ray space X-ray space density density MAY MAY flatten at flatten at zz>3>3

Need more high-Need more high-z, X-ray selected z, X-ray selected AGNAGN

(Miyaji et al 2000)

Chandra AdvancesChandra Advances ~1” positions, small PSF & low background

10-100× fainter flux limitsunambiguous source IDsSource extent and morphology

XMM is Complementary

44× Effective Area + larger Field-of-View Effective Area + larger Field-of-ViewHarder energy band: 0.5-20 keVHarder energy band: 0.5-20 keV

Do High and Low L AGN Evolve Do High and Low L AGN Evolve Differently?Differently?

Redshift distribution of deep Chandra sources

Obscured AGN population resides at z<1.5

Barger et al., Cowie et al. 2003

● 1043 < Lx(2-8 keV)< 1044 erg/s

○ 1044 < Lx < 1045 erg/s

Quasar and AGN EvolutionQuasar and AGN EvolutionCurrent Chandra and XMM deep surveysCurrent Chandra and XMM deep surveys

Resolved ~80-90% of the 2-8 keV CXRB

CDF-N (Brandt et al. 02) , CDF-S (Giacconi et al 01), Lockman Hole (Hasinger et al. 01)

CXRB is not a fully solved issue

Chandra bandpass

Com

astri

et a

l. 19

95

Hard CXRB Dominated by “Bright” SourcesHard CXRB Dominated by “Bright” Sources

Cowie et al. (2002)

Outline of the ChaMPOutline of the ChaMP135 selected ACIS fields from Cycles 1&2 X-ray source detection & photometrySource IDs via optical imaging: g’ r’ i’Classification in X-ray/optical multicolor plane Optical spectroscopy of bright subsampleRadio: NVSS+FIRST; VLA2MASS; near-IR Imaging (TBD)

ChaMP Field DistributionChaMP Field Distribution

137 Cycle 1&2 ACIS Fields: ~14 sq. deg137 Cycle 1&2 ACIS Fields: ~14 sq. deg Exposure times 2-190 ksecExposure times 2-190 ksec ~6000 X-ray sources~6000 X-ray sources

Predicted Number CountsPredicted Number Counts

4000 AGN (800 abs’bd) 4000 AGN (800 abs’bd) 2000 galaxies, 200-300 2000 galaxies, 200-300 M stars, 40 clustersM stars, 40 clusters

Chandra Deep Surveys: Chandra Deep Surveys: 1&2 Msec (ACIS-I)1&2 Msec (ACIS-I)

ROSAT compilation ROSAT compilation (Miyaji et al. 2000)(Miyaji et al. 2000)

Grimes, Green, KimGrimes, Green, Kim

ChaMP logN-logSChaMP logN-logS

Soft Band Hard Band

Bridges flux gaps between ROSAT, ASCA &Bridges flux gaps between ROSAT, ASCA & Chandra Deep FieldsChandra Deep Fields

7.1 7.1

Kim et al. 2003

ChaMP logN-logS: ResultsChaMP logN-logS: Results

Soft band differential logN-logS requires a Soft band differential logN-logS requires a broken powerlawbroken powerlaw

ββbrightbright=2.3±0.2=2.3±0.2,, ββfaintfaint=1.7±0.1, S=1.7±0.1, Sbreakbreak=6=6×10×10-15-15

Hard band: Hard band: ββ=1.3±0.1 single PL acceptable=1.3±0.1 single PL acceptable Both consistent with XMMBoth consistent with XMM (Baldi et al. 2001),(Baldi et al. 2001), CDF-N CDF-N (Brandt et al. 2001)(Brandt et al. 2001)

7.1 7.1

Kim et al. 2003

cgsSbreakfntbrt15

,1.07.1,2.03.2 106

Cosmic VarianceCosmic Variance??• 62 fields62 fields• counts>20; counts>20; θθ<400”<400”• typical errors showntypical errors shown• No significant No significant Cosmic Variance!Cosmic Variance!• 3C295 cluster field 3C295 cluster field exposures markedexposures marked• 100ksec exposure 100ksec exposure belies earlier claim of belies earlier claim of overdensityoverdensity

7.1 7.1

Kim et al. 2003

ChaMP logN-logS: ClustersChaMP logN-logS: Clusters

7.1 7.1

Kim et al. 2003

29 cluster target fields 33 non-cluster fields

X-ray SimulationsX-ray Simulations

SAOSAC raytrace simulations

Grid of off-axis angles

10 – 1000 count sources

Std XPIPE detection & Photometry

Compare input/output

- detection rates

- positions

- fluxes

Wavdetect Positional UncertaintiesWavdetect Positional Uncertainties

Typically <1‘’

Strong increase with θ due to PSF

Greatly improved after detection by a 2d wavdet pass using small kernel

Centroid uncertainty decreases for strong sources.

Optical IdentificationOptical Identification

With reduced, stacked NOAO MOSAIC imagesWith reduced, stacked NOAO MOSAIC images Detect sources with Detect sources with SExtractorSExtractor Astrometric solution: Astrometric solution: GSC II, <0.3” rmsGSC II, <0.3” rms Cross-correlate X-ray and opticalCross-correlate X-ray and optical Fine tune X-ray astrometryFine tune X-ray astrometry Prioritize counterparts by X-O distancePrioritize counterparts by X-O distance Visual check of all optical IDsVisual check of all optical IDs

P. Green, W. Barkhouse. R. Cameron, J. Silverman, A. Mossman

X-ray/Optical MatchingX-ray/Optical Matching

NOAO 4m/MOSAICNOAO 4m/MOSAIC Sloan Sloan g’ r’ i’ g’ r’ i’ Automated OAA Automated OAA

dependent matchingdependent matching Visual inspectionVisual inspection

Cameron, Silverman, Green

Optical CounterpartsOptical CounterpartsGreen et al. 2003:

6 fields>30ksec

483 sources > 3e-16

328 optical IDs (68%)

125 spectra (25%)

194 sources > 3e-15

156 optical IDs (78%)

78 spectra (40%)

spectra for 64% of r<22 IDs

55 sources > 1e-14

52 optical IDs (95%)

34 spectra (62%)

spectra for 72% of r<22 IDs

Optical Spectroscopic ProgramOptical Spectroscopic ProgramJ. Silverman, P. Green, P. Smith (Steward), S. Ellison (PUC), C. Foltz (NSF), J. Silverman, P. Green, P. Smith (Steward), S. Ellison (PUC), C. Foltz (NSF),

C. Smith, M. Smith (CTIO), E. Colmenero-Romero (SAAO)C. Smith, M. Smith (CTIO), E. Colmenero-Romero (SAAO)• Spectroscopic identification r’<23

FLWO/1.5m FAST, SAAO

-longslit (Queue observing)

KPNO/WIYN, CTIO/4m 19

-HYDRA multi-fiber (FOV 1 deg)

KPNO/4m 3

-MARS(Multi-aperture red spectrograph)

Telescope/Instrument # of nights

Magellan/6.5m 9

-LDSS-2 multi-slit spectrograph

(FOV ~5’)

MMT/6.5m 9

-long slit

30/40 clear nights (~400 spectra)Additional spectra from J. Huchra, G. Torres, W. Brown, K. Adelberger, K. Krisciunas(CTIO), B. Kirshner

Quasars at z > 3Quasars at z > 3

Chandra Image30 ksec exposure

ACIS-S

ACIS-I

8.5’

2’ x 2’ FOV

r’=21.5 r’=20.6

r’=22.0 r’=21.5

Covering the LCovering the Lxx-z Plane-z Plane

ChaMP complements ChaMP complements the CDFs by finding the CDFs by finding numerous: numerous:

high-z, high-L high-z, high-L QSOsQSOs

low-z, moderate-L low-z, moderate-L AGNAGN

Covering the LCovering the Loo-z Plane-z Plane

ChaMP garners high-L galaxies and QSOs.But ~no galaxies beyond z~0.8 !

Galaxy z limit set by r’<22

Optical vs. X-ray FluxesOptical vs. X-ray Fluxes BLAGN and stars BLAGN and stars well-separatedwell-separated Different sample Different sample than optical surveysthan optical surveys

Some ALGs have Some ALGs have QSO-like fQSO-like fxx/f/foptopt

Many bright X-ray Many bright X-ray sources unmatched sources unmatched to to r r =25=25

Hidden AGNHidden AGN Hard sources Hard sources

appear at fappear at fX X <10<10-14 -14

May compose May compose CXRBCXRB

Many have no Many have no broad lines: Optical broad lines: Optical Type2 AGN?Type2 AGN?

Yes! LYes! LX X >10>1043 43

X-ray, optical X-ray, optical absorption not 1:1absorption not 1:1

X-ray absorption propertiesX-ray absorption properties

•As expected, BLAGN are predominately unobscured

•Hard X-ray Sources are obscured AGN (Lx >10^42 erg/s)

• NELG and ALG have a wide range of X-ray spectral properties

• No type II QSOs detected -selection effect -5 detected in the CDF-S -1 “ “ “ CDF-N

Normal galaxy (optical)

z=0.228 r’=19.6

Soft=2 counts Hard=89 counts

Soft: 0.3-2.5 keV Hard : 2.5-8.0 keV

Absorbed ObjectsAbsorbed Objects

X-ray faint objects tend to be redder X-ray hard objects tend to be redder

ChaMP X-ray Spectral FitsChaMP X-ray Spectral Fits CHaMP’s XFit

pipeline uses Slang scripting running Sherpa fitting in CIAO

Cts>Cts> #Params#Params

5050 22

100100 33

300300 44

500500 55

10001000 66

Fits span 28 models (35 for known z)

Serendipitous ClustersSerendipitous Clusters

z=0.3? cluster with extended X-ray emission

Serendipitous ClustersSerendipitous Clusters

z=0.72 QSO with extended X-ray emissionoffset from QSO by rcore

Spin-Off ProjectsSpin-Off Projects

Clusters from optical Clusters from optical andand X-ray images X-ray imagesLenses, pairs, jetsLenses, pairs, jetsVariability pipeline (Bayesian block Variability pipeline (Bayesian block

analysis)analysis)Damped LyDamped Lyαα survey surveyAGN-AGN and AGN-galaxy clusteringAGN-AGN and AGN-galaxy clustering

X-ray Properties of Optically X-ray Properties of Optically Selected ClustersSelected Clusters

Select clusters from both optical and X-ray images.

Use VTP on photometric catalog for optical cluster detection (Ramella et al. 2001). Use color slices to raise sensitivity to red sequence.

Damped LyDamped Lyαα Survey Survey

• ΩDLA increases with optical magnitude (Ellison et al. 2001)

• Radio-selected quasar results show higher n(z) at 1σ

• Are optical QSO DLA surveys are dust-biased?

• ChaMP z>2 QSOs with r>20 will provide a stringent test

Clustering & QSO LifetimesClustering & QSO Lifetimes

Current LimitsCurrent Limits Proximity Effect Proximity Effect T TQSO QSO >10>1055 yr yr Overall Population Overall Population T TQSOQSO<10<1099 yr yr

QSO LifetimeQSO Lifetime Space DensitySpace Density Halo MassHalo Mass ClusteringClustering

shortshort commoncommon typicaltypical weakweak

longlong rarerare massivemassive strongstrong

(Martini & Weinberg 2001; Haiman & Lam 2001)

ChaMP & the CommunityChaMP & the Community

ChaMP fields: ~20% of archived Cycle 1&2 targetsChaMP fields: ~20% of archived Cycle 1&2 targets Public database: X-ray sources, optical IDs, Public database: X-ray sources, optical IDs,

matched optical images, photometry and colors matched optical images, photometry and colors Will enhance Chandra science return!Will enhance Chandra science return! Graduate student thesis projects available.Graduate student thesis projects available.

Thanks to NASA for CXC Archival Research funding, to NOAO for

telescope time awarded, and thanks to the whole ChaMP Collaboration!

http://hea-www.harvard.edu/CHAMP

ChaMP Results to DateChaMP Results to Date

‘‘Cosmic Variance’ consistent with Poisson Cosmic Variance’ consistent with Poisson No significant source overabundance No significant source overabundance

associated with clustersassociated with clusters ααoxox or or ffxx/f/frr dependence on L or z consistent with dependence on L or z consistent with

expectations from LF simulations + limitsexpectations from LF simulations + limits Half the objects with Lx>10Half the objects with Lx>104343 are hard; are hard;

presumably obscured AGNpresumably obscured AGN Wide area suitable for samples of rare objects.Wide area suitable for samples of rare objects.