agn in x-ray surveys
DESCRIPTION
AGN in X-Ray Surveys. For Astro597 Jian Wu November 10, 2004. OUTLINE. Part I AGN Surveys in Different Bands Part II AGN X-ray Surveys. Part I AGN Surveys in Different Bands. AGN Surveys in different bands Retrospect Optical selection and implications Radio selection - PowerPoint PPT PresentationTRANSCRIPT
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AGN in X-Ray SurveysAGN in X-Ray Surveys
For Astro597
Jian Wu
November 10, 2004
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OUTLINEOUTLINE
Part IAGN Surveys in Different Bands
Part IIAGN X-ray Surveys
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Part IPart IAGN Surveys in Different Bands AGN Surveys in Different Bands AGN Surveys in different bands
– Retrospect – Optical selection and implications– Radio selection– Infrared selection– High-Energy selection
Selection Effects
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Part IIPart IIAGN X-ray SurveysAGN X-ray Surveys
Soft X-rays SurveysHard X-ray Surveys
– Pre-Chandra and XMM-Newton– Deep Chandra and XMM-Newton Surveys
Deep Extragalactic X-ray Surveys2Ms Chandra Point-Source CATA
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Part IPart I
AGN Surveys in Different Bands
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RetrospectRetrospect
Lamppost Effect– find something in where we can find it
Three types of surveys– Find object– Find object consistently– Find with well-defined selection criteria
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RetrospectRetrospectFirst indication (optical)
– NGC1068-broad emission lines (Fath, 1913)– M87-jet (Curtis 1917)– Extragalactic radio sources– The origin of name for quasar (Schmidt et.al., 1
964)
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Retrospect Retrospect Early AGN Surveys
– Cambridge xC Surveys– Markarian Survey– Zwichky Survey
Recent Large Surveys– 2dF– SDSS
How to find AGN-SED– Power law (1013Hz-1020Hz)– Highly ionized Emission lines-C N O– Low-ionization emission lines-Fe
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Optical SelectionOptical Selection
Principle (Sandage 1971)– Systematic optical color deviation from starlight
Bonus– Photometric red-shift estimation
Declaration of “complete samples” Fatal bug
– Lb does not correlated well with Lgalaxy → cannot see low luminosity AGN in massive galaxies (contamination)
Aftermath– Omission (radio, IR, X-ray)
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Optical selection effect– Luminosities– Hard to evaluate
Alternatives – Variability– Absence of proper motion
Optical SelectionOptical Selection
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Radio SelectionRadio Selection Principles
– Flat-spectrum, compact radio source– Object with low IR/radio– morphology
Advantages – Efficient– Sensitive – Accurate – Find objects omitted by optical techniques
Disadvantages– Incomplete (selection effect)– Star-forming region
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Infrared SelectionInfrared Selection
Disadvantages– Color difference is subtle– Equivalent width insufficient – An Island
Potential advantages– mid-IR to be a “pivot point” in SED– PAH and high ionization IR lines
Prospect– SIRTF
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High-Energy SelectionHigh-Energy Selection
X-ray and γ-rayDisadvantages
– Soft X-ray suffer from larger extinction– Red-shift distribution– γ-ray position– Soft X-ray bias
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Selection EffectSelection Effect
Dilution of the optical/IR brightness and color by the starlight.
ObscurationAnother selection effect
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Part IIPart II
AGN X-ray Surveys
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AdvantagesAdvantages
High contrast between AGN and stellar light
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Advantages Advantages Penetrating power of X-rays.
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Advantages Advantages
Great sensitivity of Chandra and XMM-Newton
ACIS
(ergs-cm-2 sec-1 in 10 5 s)
HRC (ergs-cm-2 sec -1 in 10 5 s )
4×10-15 4×10-15
EPIC MOS
(ergs-cm-2 sec-1 in 10 5 s)
EPIC pn(ergs-cm-2 sec -1 in 10 5 s )
~ 4×10-14 ~ 4×10-14
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Advantages Advantages
Accurate positions from Chandra– ~ 0.5 arcsec
Einstein EXOSAT ROSAT BBXRT/ASCA
Chandra XMM-Newton
4 18 4 75 0.5 20
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Advantages Advantages
A relatively large fraction of the bolometric energy (3-20%) is radiated in the classical X-ray bands.
High area density (400 deg-2) Large amplitude and frequency of variability in
the X-ray band. Little Contamination from other objects High red-shift quasars are easy to detect Close to the black hole
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Early X-ray SurveysEarly X-ray Surveys
Uhuru (1970 10-1973 3) [2-20 keV]Ariel-V (1973 10-1980 3) [0.3-40 keV]HEAO-1 (1977 8-1979 1) [0.2keV-10MeV]
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Soft X-ray SurveysSoft X-ray Surveys
Einstein (1978 11-1981 4) [0.2-20 keV]ROSAT (1990 1-1999 2) [0.1-2.5 keV]
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Soft X-ray SurveysSoft X-ray SurveysFruit
– Moderate correlation of optical and X-ray
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Hard X-ray surveysHard X-ray surveys
ASCA (1993 2-2001 3) [0.4-10 keV]BeppoSAX (1996 4-2002 4) [0.1-300 keV]Fruit
– ~ 500 serendipitous sources over ~ 100 deg2
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Deep Deep ChandraChandra and and XMMXMM--NewtonNewton SurveysSurveys
Chandra (1999 7-present)XMM-Newton (1999 10-present)
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Deep Deep ChandraChandra and and XMMXMM--NewtonNewton SurveysSurveys
Fruit– Numerous “optically dull” objects– Greatly enlarge the AGN population
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Deep Extragalactic X-ray SurveysDeep Extragalactic X-ray Surveys
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Deep Extragalactic X-ray SurveysDeep Extragalactic X-ray Surveys
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Deep Extragalactic X-ray SurveysDeep Extragalactic X-ray Surveys
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Deep Extragalactic X-ray SurveysDeep Extragalactic X-ray Surveys
Source classification difficulties– Too faint to be identified by optical spectrum– Many of the X-ray sources have modest optical
luminosities, often due to obscuration– “schism” between optical (type1 and type2) and
X-ray (unobscured and obscured )
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Deep Extragalactic X-ray SurveysDeep Extragalactic X-ray Surveys
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Deep Extragalactic X-ray SurveysDeep Extragalactic X-ray Surveys
Basic AGN Types– Unobscured AGN– Obscured AGN with clear optical/UV AGN sig
natures.– Optically faint X-ray sources– XBONGs
(X-ray Bright Optically Normal Galaxies)
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AGN Red-shift DistributionAGN Red-shift Distribution
Most AGN in deep X-ray surveys have z =0~2
Redshift distribution show “spikes” in z=0.5~2.5
[Bargar et al. 2002] [Bargar et al. 2003]
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Luminosity-redshift PlotLuminosity-redshift Plot
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AGN Selection CompletenessAGN Selection Completeness
Reasons of incompleteness– Compton thick AGN– Luminous at non-X-ray, but X-ray weak
How many we haven’t seen
2000-3000 deg-2
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Key results from DEXSKey results from DEXS
Large optically selected luminous quasars– PLE (Pure luminosity Evolution)
Moderate-luminosity AGN– LDDE (luminosity-dependent density
evolution)
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Comoving space densityComoving space density
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X-ray constraintsX-ray constraints
Sky density– Bottom line (z > 4) ~ 30-150 deg-2
– AGN contribution to reionization at z ~ 6 is small Accretion[z>4] ~ Accretion[local] Infrared and sub-millimeter
– star-forming processes AGN/sub-mm galaxies >=40%. X-ray survey should remain an effective way to fi
nd AGN at the highest redshift
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Future prospectsFuture prospects
Detailed cosmic history of SMBH accretionThe nature of AGN activity in young,
forming galaxiesX-ray measurements of clustering and
large-scale structureThe X-ray properties of cosmologically
distant starburst and normal galaxies
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The 2Ms CDF-NThe 2Ms CDF-N
Main CATAlog– High significant Chand
ra sources
Supplementary CATAlog
– Lower significance Chandra sources
20 observations
447.8 arcmin2
Flux limit=2.5×10-17 erg cm-2 s-1 (0.5-2.0 keV)
Flux limit=1.4 ×10-16 erg cm-2 s-1 (2.0-8.0 keV)
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Data reductionData reduction
CIAO– Chandra Interactive
Analysis of Observations
Radiation damage Quantum Efficiency
Losses Bad column Bad pixel Cosmic ray afterglow Standard pixel
randomization Potential background
events
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Production of CATAlogsProduction of CATAlogs
Technique feature – Matched filter
Accuracy of the X-ray source position
Correlation of optically bright sources with lower significance Chandra sources
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Image and Exposure Map CreationImage and Exposure Map Creation
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Standard BandsStandard Bands
5.0 keV0.1 0.2 0.4 0.8
FB
SB
SB1 SB2 HB1 HB2
HB
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Point-source DetectionPoint-source Detection
Key criterion
1×10-5
supplementary optically bright source CATAlog
False positive probability 1×10-7
main CATAlog
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Source Position RefinementSource Position Refinement
X –ray 1.4GHz Radio 5.2
503 sources
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Position of sources in mainPosition of sources in main138 NEW!138 NEW!
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Supplementary Optically Supplementary Optically Bright Chandra Source CATABright Chandra Source CATA
X –ray Optical R-band 5.1
79 sources
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Primary analysis of SPrimary analysis of S
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X-ray Band ratioX-ray Band ratio
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Color-Color DiagramColor-Color DiagramSB2/SB1 vs. HB1/SB2SB2/SB1 vs. HB1/SB2
8.1
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Color-Color DiagramColor-Color DiagramHB1/SB2 vs. HB2/HB1HB1/SB2 vs. HB2/HB1
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BackgroundBackground
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ProspectsProspects
Doubling the exposure of a Chandra observation leads to an increase in sensitivity between and .
The number of background counts is often negligible.
Negative K-correction of absorbed AGN emission
2 2
Longer and longer
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