JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
AGN and Surveys with the new X-ray observatories
Xavier Barcons
Instituto de Física de Cantabria (CSIC-UC)
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Index
• Introduction: The AGN paradigm and X-ray observations• New windows with the new X-ray observatories• The inner disk: Fe line diagnostics• The circum-nuclear environment: warm absorbers, jets
and outflows• Challenges to the AGN unified model• X-ray Surveys, Obscured accretion, and the X-ray
background• A few questions for the future
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Acknowledgements
• The IFCA X-ray Astronomy group: Francisco Carrera, Maite Ceballos, Silvia Mateos, Amalia Corral, Jacobo Ebrero
• The XMM-Newton Survey Science Centre, especially: Mike Watson, Mat Page, Tommaso Maccacaro, Roberto Della Ceca, Paola Severgnini, Axel Schwope, etc.
• The Lockman Hole team, especially: Günther Hasinger, Alina Streblyanska, Ingo Lehmann, Thomas Boller and the
• Andy Fabian
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
The X-ray view of an AGNThe X-ray view of an AGN
C. Done, Durham U
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
The X-ray spectrum of an AGN
Radiation from the accretion disk, reprocessed by a relativistic electron corona
Reflection (fluorescence lines and Compton recoil bump)
Absorbers
Soft excess (direct disk radiation)
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
The new X-ray observatories
Chandra (NASA)July 1999
XMM-Newton (ESA)December 1999
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
How does an X-ray telescope work?
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Chandra
• High-resolution camera (HRC): Micro-Channel Plate
• Advanced CCD Imaging Spectrometer (ACIS)
• Low Energy Transmission Grating Spectrometer (LETGS): 0.08-2 keV, E/E=30-2000 (+HRC-S)
• High Energy Transmission Grating Spectrometer (HETGS): 0.4-10 keV, E/E1000 (+ACIS-S)
• Spatially resolved (0.5“) low resolution spectroscopy (E/E~20-50)
• Intermediate resolution dispersive spectroscopy (0.02-0.04 Ang, E/E~200-500)
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
XMM-Newton• Spatially resolved (15“) low-
resolution spectroscopy (E/E~20-50)
• Intermediate resolution dispersive spectrometry (0.03-0.06 Ang, E/E~200-500)
• EPIC: (3) CCD spectroscopic imaging cameras 0.1-12 keV
• (2) Reflection Grating Spectrometers (RGS): 0.05-3 keV
• (1) Optical monitor (OM): Optical/UV imaging and grism spectroscopy.
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Comparison between Chandra and XMM-Newton
XMM-Newton:
•Effective area 0.4 m2
•Angular resolution: 15’’ HEW•Limiting sensitivity: 10-15 erg cm-2 s-1
Chandra:
•Effective area: 0.08 m2
•Angular resolution: 0.5’’ HEW•Limiting sensitivity: <10-16 erg cm-2 s-1
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
New windows: Hard X-ray energies
Sensitivity to hard X-rayenergies (up to 12 keV
with XMM-Newton) RosatXMM/Chandra
log NH=
Absorbed sources can be seen!
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
New windows: high-resolution imaging over wide FOV
XMM-Newton imagesa FOV of 30’ with
moderate resolution (15”)
Chandra images down to Sub-arcsec resolution
(0.5-1”)
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
New windows: moderate resolution dispersive spectroscopy
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
The inner disk: Fe line diagnostics
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Radiation from the accretion disk
Incident radiation Reflection
Transmission
Emission
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Reflection from cold matter
George & Fabian 91
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
XMM-Newton spectrum of the Circinus Galaxy
Fe Kα,β and Ni Kα
Molendi, Bianchi & Matt 03
Fluorescence lines
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Reflection from photoionized matter(Ross & Fabian 93, 04)
Incr
easi
ng io
nisa
tion
para
met
er
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Relativistic line broadening
Schwarzschild
Kerr
Fabian et al 91
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Discovery of broad Fe lines
ASCATanaka et al 1995
MCG-6-30-15
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
More broad lines in AGNMCG-5-23-16 (Dewangan 2003) NGC 3516 (Turner 02)
PG 1211+143 (Pounds 2003) IRAS 18325 (Iwasawa 2004)
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
XMM-Newton observations of the Fe line in MCG-6-30-15
pn
MOS 1,2
Vaughan 04
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Simultaneous XMM-Newton and BeppoSAX observations of MCG-6-30-15
Comptonreflectionhump
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Spectral changes seen in MCG-6-30-15
The Fe line stays virtually constant, in spite of strongchanges in the continuum:
NO REVERBERATION?
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Spectrum of the variable component
Understanding spectral variability in MCG-6-30-15
Spectrum of the constant component
Fe line
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Light bending model in a Kerr BH
KevinRauchJHU
Miniutti et al 03,04
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatoriesRegime III: large source height and anti-correlationRegime II: intermediate source height and constant
Fe line
IIIIII
Fe line – PLC correlation
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
The variety of Fe line profiles
Reeves et al (2001)
Disk
Torus
XMM
Nandra (2001)
ASCA
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
More relativistic emission lines?
Branduardi-Raymont et al (2001)Lee et al (2001)
ChandraXMM
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Ionised absorbers, outflows and jets
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Warm absorbers: the low resolution viewH1419+480
z=0.07229
IUE
XMM-Newton
Barcons, Carrera & Ceballos 2003b
X-ray ionized absorbers ~“Associated” UV absorbers
Photoionisation edge
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
The high-resolution view of warm absorbers
Sako et al 2001
Fe MUnresolvedTransition Array (UTA)
Low ionisation component
High ionisation component
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
NGC 3783 (Krongold et al 2003)Chandra/HETGS
~100 features detected; Two-phase absorbing medium, pressure equilibrium Outflowing velocity ~750 km/s; Turbulence ~300 km/s
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Jets detected in X-raysPks 0637-752:
First “point-like” targetfor Chandra
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Jets commonly seen in X-rays
Cen-A
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
M87
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
3C273
Chandra
Marshall et al (2001)
MERLIN HSTChandra
SEDs indicate that synchrotron might be dominant in most knots,but additional processes mightBe required in other cases.
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
NGC 6240
Binary BHs in the centres of AGN
ChandraKomossa et al (2002)
NGC 6240
Starburst
AGN
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Challenges to the AGN unified model
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
The unified AGN scheme confronts X-ray observations
Maiolino (2001)
Since type 2 AGN are seen through absorbing material, they should display higherphotoelectric absorption in X-rays
… but there are apparent discrepancies:•Type 1 AGN with absorbed X-rayspectra•Type 1.8/1.9/2 AGN with low orno photoelectric absorption
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Type 1 AGN (moderately) absorbed in X-rays
S 0.5-4.5 keV= 7.2 x 10-14 erg cm-2 s-1
z=0.872 NH=2.81021 cm-2
Broad-Line AGN
L 2-10=3.21044 erg s-1
WHT/ISIS
XMM
XMMU J061515.2+710204
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
A type1.9 AGN with no absorption
Barcons, Carrera & Ceballos 2003
H1320+551, z=0.0653Seyfert 1.8/1.9H/H>27Expected absorption: >1022 cm-2
XMM-Newton:Disk + reprocessingAbsorption<1020 cm-2
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Photoelectric absorptionThe AXIS surveySlim(0.5-4.5 keV)~10-14 erg cm-2 s-1
•10% of type 1 AGN are absorbed(with NH<1022 cm-2) •40% of type 2 AGN are absorbed
Mateos et al (2004a)
The Lockman Hole surveySlim(0.5-4.5 keV)~10-14 erg cm-2 s-1
•15% (<30% at 3) of type 1 AGN are absorbed (with NH<1022 cm-2) •80% (>50% at 3) of type 2 AGN are absorbed. But 5/28 are unabsorbed
Mateos et al (2004b)
See talk byMaite Ceballos
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Options/explanations
• The 10-15% of absorbed type 1 AGN could be ~BALs, or hosted by edge-on galaxies [this should be testable]
• Unabsorbed type 2 AGN:– These are Compton-thick Seyfert 2 galaxies, where only
unabsorbed scattered X-rays are seen [but Fe line is weak or absent and should be very strong]
– Optical spectroscopy properties and X-ray absorption agree with each other, but the absorbing material varies [should be testable with simultaneous X-ray and optical spectroscopy]
– The optical spectroscopic properties are intrinsic to the Broad Line Region, and not associated to absorbing material.
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
X-ray/optical mismatches: variability?Simultaneous XMM-Newton and 3.5m/CAHA spectroscopy ofMkn 993; z=0.0155 (Changing type Seyfert)
3.5m/TWINXMM
Optical: Seyfert 1.8Balmer decrement=9(NH~ 5 1021 cm-2)
X-ray: weak absorption (NH~ 7 1020 cm-2)
Poster by A. Corral
Optical spectral typeintrinsic to BLR,
not due to absorption
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
X-ray Surveys, obscured accretion and the X-ray
background.
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
The XMM-Newton Survey Science Centre serendipitous sky Surveys
• Thanks to its large field of view and sensitivity, every XMM-Newton pointing discovers ~30-150 serendipitous X-ray sources.
• The 1XMM source catalogue contains 30000 sources. The 2XMM catalogue will contain 150000 X-ray sources
• The Survey Science Centre sky survey consists of:
– Core programme:• Bright Source Sample• Medium Flux Survey• Faint Surveys (i.e., LH)• Galactic Plane Surveys
– Optical imaging programme of many XMM-Newton fields
– Statistical identification of many catalogued sources
OY Car
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
The X-ray background and the AGN unified model
• The spectral energy distribution of the XRB peaks at ~30 keV, far beyond existing X-ray telescopes.
• Unified model: The XRB is produced by a superposition of unabsorbed and absorbed AGN.
• Predictions:– The majority of accretion onto
super-massive black holes is absorbed
– A large number of type 2 QSOs is expected.
Gilli et al 2000
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Optically dull, X-ray luminous galaxies
z=0.044LX=1042 erg/s
TNG
Subaru
=1.7NH=2 1023 cm-2
XMM
Severgnini et al (2003)
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Type 2 (Radio) QSOs•Selected by its X-ray emission•Only narrow emission lines at z=1.246•X-ray luminosity > 1045 erg/s•Double-lobed radio-source•X-ray emission unrelatedto radio lobes•“Normal” AGN mildly absorbed in X-rays
Barcons et al 1998Barcons et al 2003
XMM
VLA
RX J1011.2+5545
NH=4 1022 cm-2
XMM
WHT/ISIS
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Type-2 Radio-Quiet QSOs
AAT/2dF(Mat Page)
XMM
NH~5 1022 cm-2
z=2.978 (Ly, CIV, CIII])X-ray flux (2-10 keV) = 8 10-15 erg cm-2 s-1
Intrinsic X-ray luminosity = 4 1044 erg s-1
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
The various classes of AGN
15
16
17
18
19
20
21
22
23
24
25
1 10 100
X-ray flux 0.5-4.5 keV (10-14 erg cm-2 s-1)
r/R
op
tica
l mag
nit
ud
e
FX/Fopt=1
FX/Fopt=10
FX/Fopt=0.1
AGN
Obscured AGN
Gal
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Optical colours of X-ray sources
Optical colours
-1,0
-0,5
0,0
0,5
1,0
1,5
2,0
2,5
3,0
-1,0 0,0 1,0 2,0 3,0
g'-r'
r'-i
'
QSOs
Early-typegalaxies
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
The Chandra deep fields
• The bulk of X-ray emissivity (50%) in the Universe (AGNs) occurs at z<1
• Sources are increasingly reddened in the optical, including EROs.
Tozzi et al 2001, Barger et al 2003, Alexander et al 2003
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
The redshift distribution in deep X-ray surveys
Barger et al (2003)
MostlyAGN-2
MostlyAGN-1
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Obscured accretion
• Most of the growth of the black holes by accretion occurs in obscured sources.
• Assuming that the growth of BHs is dominated by accretion and not by mergers, the local BH density can set constraints on the amount of obscured accretion
Salvati et al (2004)
JENAM, 13 Sep 2004 AGN and Surveys with the new X-ray observatories
Some questions for the future
• Perform reverberation mapping on relevant timescales.• Test properties of supermassive black holes out to very
high z’s (mass, angular momentum, accretion rate)• Reach the “thermal limit” in X-ray high-resolution
spectroscopy to do proper Astrophysics on circumnuclear matter
• Trace the cosmic evolution of obscured and unobscured accretion
• What was first: Supermassive Black Holes or Stars in the history of galaxies?