Post on 19-Feb-2016
description
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.