X-ray Astronomy # 12Belinda Wilkes, 29 Nov : X-ray Astronomy Lecture 12 Super-Massive Black Holes, Jets, AGN, Quasars, Blazars Belinda Wilkes Chandra X-ray Center Smithsonian Astrophysical Observatory

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 Super-Massive Black Holes (SMBH) Active Galactic Nuclei (AGN): –Galaxy containing a SMBH (log M o =6-10) at its core –Strong, broad (~10 3 kms -1 ), high-ionization emission lines –Strong, narrow (~100 kms -1 ), low-ionization lines Many observational types, related via Unification models: –Quasars/Quasi-Stellar Objects (QSOs) –Seyfert galaxies (types: 1-2) Type 1: broad and narrow emission lines Type 2: narrow emission lines only –Broad Line Radio Galaxies –Narrow Line Radio Galaxies

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 X-rays and Active Galaxies AGN are multi-wavelength emitters: radio-X-ray (and γ-ray) Strong X-ray sources –X-ray surveys mostly see AGN so are a good way to find them –Provide information on nuclear regions –Major advances with current X-ray satellites Chandra + XMM-Newton’s main roles: –Finding new SMBHs: Surveys –High signal-to-noise CCD spectroscopy –High Resolution Spectroscopy –X-ray jets

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 Unification

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 The Nuclear Regions of an AGN View of Active Galaxy (AGN) depends on inclination Optical/UV light: obscured when edge- on Traditional surveys: optical/UV, soft X-ray Hard X-ray/IR/radio surveys see all Nuclear region of an AGN/Quasar

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 Unification Model: nuclear regions X-ray source Accretion Disk: OUV +soft X-ray emission Dusty material: near+mid IR emission X-ray reflection off cold/warm material Scattered, polarized light BROAD LINE REGION NARROW LINE REGION Type 1 Type 2

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 Spectral Energy Distributions of Active Galaxies Face-on View Elvis et al. 1994RadioX-ray Edge-on View E B-V =0.6

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 Emission Mechanisms Synchrotron Synchrotron + thermal Thermal: gas in accretion disk Synchrotron self- Compton from radio Synchrotron (beamed) Synchrotron Thermal: dust with wide temperature range (~ K) Thermal: gas in accretion disk (AD) Thermal Comptonisation of UV Radio-quiet Radio-loud Radio Infrared Optical/UV +soft X-ray Hard X-ray γ-ray

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 Complex Unification! X-ray surveys generally find: –Type 1 AGN - unobscured –Type 2 AGN – obscured –Consistent with simple Unification models But MANY exceptions: –Broad Absorption Line (BAL) –Red AGN –Intermediate types ( ) –XBONGs Disk-wind models (Konigl & Kartje 1994) Elvis Urry & Padovani

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 Surveys

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 To View the Population Optical and soft X-rays miss edge-on/obscured AGN and quasars An unbiased view of the population –X-ray surveys: Chandra, XMM-Newton –Infrared (IR) Surveys: 2MASS, Spitzer –Γ-ray: Integral –Low-frequency Radio: 3CR Many ongoing, deeper, multi-wavelength surveys, cover full range of possibly SEDs Can Unification explain the many varieties of AGN? 20 years ago Now

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 X-ray Surveys Strategy: layered surveys –Deep, narrow: all populations, small number sources, cosmic variance: Chandra Deep Field North:.08 deg 2 (1 ACIS-I field); 2 Msecs Chandra Deep Field South:.08 deg 2, 2 Msecs; + 4 flanking fields, 250 ksecs –Medium deep, wider: larger samples, miss faintest AGN, less cosmic variance: SWIRE: 0.6 deg 2, 70 ksecs COSMOS 0.6 deg 2, 200 ksec Groth Strip: 0.25 deg 2, 200 ksecs, 0.25 deg 2, 800 ksec

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 X-ray Surveys (cont) Layered Surveys (cont) –Shallow and Wide: very large samples, only brightest sources, little cosmic variance Bootes: 9 deg 2, 5-10 ksecs Multi-wavelength approach, finds more AGN types: –optical (ground based, HST) –Near-IR (ground-based) –Far-IR (Spitzer) –Radio (ground-based)

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 SWIRE/Chandra Survey 0.6 deg 2 contiguous, 70 ksecs Lockman Hole region of SWIRE Centered on Deepest VLA image X-ray flux limit: 2x erg cm -2 s -1 Depth: distinction between AGN and starbursts (undetected) (w/Lonsdale, Kilgard, Polletta, Smith, Owen, et al.)

X-ray Astronomy # 12Belinda Wilkes, 29 Nov unique X-ray sources to a limiting flux of 2x erg cm -2 s with secure IR counterparts and 626 secure optical counterparts >160 radio counterparts (analysis on-going) 75 spec z (so far) 49 X-ray sources coincident with optically extended galaxies 2 extended X-ray sources (clusters) Statistical Results SWIRE/Chandra Survey

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 SWIRE X-ray Sample Standard R vs X plot Blue lines indicate AGN region (not well- defined) Radio sources all over Extended sources in low L AGN region R X -ray

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 Current X-ray and IR Surveys → Broader range of SEDs Einstein-era: optically/radio-selected, blue bias (Elvis et al. 1994) HEAO: hard X-ray, reduces blue bias (Kuraskiewicz et al. 2003) 2MASS: J-K>2, red AGN, little/no blue bump (Kuraskiewicz et al. 2007, Fig 4b) IROptical

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 Obscured AGN log N H ~ Potential: – Numbers: geometry of central regions – Properties: information on obscuring material No single population (Alexander et al. 2003, Rosati et al. 2002): –Type 2 AGN/QSOs (Norman et al 2002, Kim et al. 2006) –Compton-thick AGN (Polletta et al. 2006) –XBONGS (Fiore et al. 2000, Kim et al. 2006) –Obscured type 1 AGN (Wilkes et al 2002 ) –Optically Highly Polarized Type 1 AGN (Smith et al. 2002)

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 Compton-thick AGN 5 hard X-ray selected (2 at z>2) 120 red, AGN-dominated, IR- selected: power-law SED, α IR >1.0 >25 Compton-thick AGN deg -2 40% optical O/IR AGN 60% host galaxy dominates 30% X-ray detected to F(.3-8)~ erg cm -2 s -1 (Polletta et al. 2006)

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 SWIRE: X-ray Compton-Thick QSO SW , z=2.54 X-ray HR~0.85, 11 cnts NLSy1 optical spectrum SED: –Obscured QSO, A V =4 –0.6% QSO type 1 (scattered light) (Polletta et al. 2006) X-rayOptical/IR

X-ray Astronomy # 12Belinda Wilkes, 29 Nov MASS Red (J-K>2) AGN w/Chandra 21 spectral fits: –Log N H ~22 –PL slope flatter for weaker X-rays Chandra data: Wilkes et al., in prep Red AGN: Hard X-ray Spectra

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 XMM-Newton Observations 8 X-ray-bright, 2MASS AGN: –Range of optical types and X-ray hardness ratio Variety of results: –Complexity in type 1 and 1.5s –Type 2 consistent with Unification –Variation in 3 (1 of each type) –No systematic error in Chandra data –BUT low S/N data are misleading Harder X-ray: due to N H + reflection (Wilkes, Pounds et al. 2005, 2007)

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 Complex Red Quasar: 2M Optical Type: 1.8 X-ray hard (HR=0.6) 2 scattering regions: –Blue: thin, small dust grains –Red: dusty region, red due to obscuration –Starlight dilution HST ACS imaging: –Blue fan (3.5” –Red fringe (polar, 2”) Schmidt et al 2007 Blue Red

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 XMM-Newton Data Unusually hard 2-10keV spectrum, HR~0.6 Requires: –Compton-thick PL –Unabsorbed Cold Reflection –Soft excess: warm ionized region –Scattered power law ~1.7% Wilkes, Pounds, Schmidt, in prep.

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 Over-the-Top View Courtesy Charlotte Garcia

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 Towards the Full Population We are finding a lot of new varieties of AGN Collecting so much data on so many sources takes a while We still do not have a census But we will!

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 GRATING SPECTRA

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 NGC3783 Seyfert 1, Redshift, z= , V= ksec HETG observation (Cycle 2 LP) Extremely rich emission and absorption spectrum 9 papers modeling physical and dynamical conditions and variability 3 or 4 co-spatial, out-flowing absorbers, range of ionization and velocity (Netzer et al 2003, Krongold et al 2003) Not many AGN sufficiently bright

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 JETS

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 Actual Chandra First Light Point Source to focus: Quasar PKS , z=0.5 X-ray Jet visible: 10” long, 400,000 lyrs Birth of a new research topic!

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 M87 Jet in Radio and X-rays Radio X-ray Double-lobed radio source with one- sided relativistic jet

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 X-ray/Radio Jets in Quasars M87 jet in X-ray, radio and optical

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 X-ray Emission Mechanisms Radio: Synchrotron emission Radio/X-ray ratio often constant along kpc jet length X-ray: Inverse-Compton (IC) Scattering IC Seed photons: –Self, i.e. synchrotron photons –Cosmic Microwave Background (CMB) Ongoing discussion!

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 Double Quasar Chandra: spatial + spectral resolution

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 NGC 6240: Galaxy with Double X-ray Core Starburst LINER z=0.0245

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 NGC 6240 Spectra NGC 6240: X-ray Spectrum Fe Kα (6.4keV) 2 2

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 NGC 6240 Movie

X-ray Astronomy # 12Belinda Wilkes, 29 Nov 2007 X-ray Studies of AGN Full View of Population: –from surveys, need Chandra - coming soon! Evolution of Population (not today): –from surveys, need Chandra - very close Low-resolution spectral studies: –progress made, XMM-Newton best instrument –need Con-X to push to high-redshift High-resolution spectral studies: –New capability, progress but is hard Jets: –New field, lots of progress, Chandra is primary instrument