View
4
Download
0
Category
Preview:
Citation preview
The X-ray Background
Günther Hasinger, MPE Garching
CDFS: J. Bergeron, S. Borgani, R. Giacconi, R. Gilli, R. Gilmozzi, K. Kellerman, L. Kewley, A. Koekemoer, I. Lehmann, V. Mainieri, M. Nonino, C. Norman, M. Romaniello, P. Rosati, E. Schreier, A. Streblyanskaya, G. Szokoly, P. Tozzi, J.X. Wang, W. Zheng, A. Zirm
Lockman Hole: X. Barcons, H. Böhringer, H. Brunner, A. Fabian, A. Finoguenov, Y. Hashimoto, P. Henry, I. Lehmann, V. Mainieri, I. Matute, M. Schmidt, A. Streblyanskaya, G. Szokoly, M. Worsley
Overall Sample & Luminosity Function: T. Miyaji, M. Schmidt
22nd Texas Symposium, SLAC Stanford, December 14th, 2004
ROSAT
XMM-Newton
Chandra
ROSAT
ROSAT
The X-ray Background
The background is the Echo of the formationof Supermassive Black Holes throughout thehistory of the Universe !
X-ray Background Spectrum
=> E<2keV XRB resolved; at E>5keV still very much work to do!
Revnivtsev et al., 2003 RXTE
XMM LH resolvedWorsley et al. 2004
from Gilli 2003
CLASXS
CLASXS
LargeX-ray
surveys
COSMOS/XMM
COSMOS/XMM
DUO Deep
DUO Wide
DUO Wide
DUO Deep
ROSITA
ROSITA
XEUS
E-CDFS
E-CDFS
XEUS
XMM Slew
Lockman
Lockman
Alexander et al. 2003, AJ, 126, 539
The Deepest X-ray Surveys
CDF-N (HDF-N) CDF-S (ACS UDF)
Brandt & Hasinger, ARAA 2005
Ultra Deep Field2.28p
AGN - opt. faint
1.69pAGN - opt. faint
0.773AGN - XBONG
0.665AGN - XBONG
3.064AGN - Ty 2
3.193AGN - Ty 1, unobs
1.216AGN - Ty 1, unobs
1.65pAGN - opt. faint
1.82pAGN - opt. faint
1.53pAGN - opt. faint
4.29pAGN - opt. faint
0.414Starburst
0.438Starburst
0.456Starburst
1.309AGN - XBONG
CDF-SACS UDF
Courtesy:S. Beckwith
> 95% have spectro- or photo-z thanks to VLT, GOODS, GEMS, ACF UDS etc. Photo-z at higher z, but all peak at z~0.7
Num
bero
f Sou
rcesSzokoly et al., 2004
(spectro-z)Wolf et al., 2004(Combo-17)Zheng et al., 2004Mainieri et al., 2004(photo-z)
Redshift
CDFS Optical IDs
Type 2 fraction
Local Seyferts
Fraction of type-2‘s decreses with luminosityUeda et al., 2003; Szokoly et al., 2004
Lockman Hole800 ks XMM-Newton observation
Keck Spectroscopy:Lehmann et al., 2001 M. Schmidt, P. Henry
Average rest-frame spectra show relativistic Fe-lines
Good news for XEUS/Con-X
Streblyanskaya et al., 2004
type-2 AGNEW~400eV
type-1 AGNEW~600eV
Large equivalent width canbe explained by 3 x solar metallicity.BH spin within reach.
The type-1 AGN 0.5-2keV X-ray luminosity function
Multi-Cone Surveys• Type-1 AGN in the 0.5-2 keV band
– Continuation of ROSAT work, most sensitive & complete
• ROSAT Samples (Miyaji et al., 2000)– ROSAT Bright Survey: 203 (0) AGN (Schwope et al., 2000)– RASS Selected North: 134 (5) AGN (Appenzeller et al., 1996)– RASS NEP Survey: 101 (9) AGN (Gioia et al., 2003)– RIXOS serendipitous: 194 (14) AGN (Mason et al., 2000)– ROSAT Deep Surveys: 84 (7) AGN (e.g. Schmidt et al., 1998)
• XMM Deep Survey (Mainieri et al., 2002)– Lockman Hole: 48 (8) AGN (Lehmann et al., 2001 ++)
• Chandra Deep Surveys– CDF North/HDF-N: 67 (21) AGN (Barger et al., 2003)– CDFS spec.+phot.: 113 (1) AGN (Szokoly, Zheng et al. 2003)
• Total: 944 (65) AGN1Yellow: unidentified
Multi-Cone SurveysSurvey Area Hubble Diagram
0.0
0.1
1.0
10.0
100.0
1000.0
10000.0
100000.0
0.001 0.100 10.000 1000.000
Flux [10-14 cgs]
Solid
Ang
le [d
eg2 ]
tot. AreacorrectedRBSAppNEPSRixosRMSXMMCDFSHDFN
0.001
0.010
0.100
1.000
10.000
41 42 43 44 45 46 47 48
log LX [erg/s]
Red
shift
RBSAppNEPSRixosRMSXMMCDFSHDFN
Multi-cone logN-logS
XLF0.5-2 keV
type-1 AGN
Luminosity-dependentdensity evolution(LDDE) confirmed
AGN Space Density φ(z)
Hasinger, Miyaji & Schmidt, 2004,A&A submitted
M. Schmidt methodT. Miyaji treatment(dotted: upper limit)
Semianalytic Model Comparison
-7.4-7.3-7.2-7.1
-7-6.9-6.8-6.7-6.6-6.5-6.4-6.3-6.2-6.1
-6-5.9-5.8-5.7-5.6-5.5-5.4-5.3-5.2-5.1
-5-4.9-4.8-4.7-4.6-4.5-4.4-4.3-4.2-4.1
-4-3.9-3.8-3.7
0 0.5 1 1.5 2 2.5 3 3.5 4 4.5 5 5.5
-8
-7.5
-7
-6.5
-6
-5.5
-5
-4.5
-4
0 0.5 1 1.5 2 2.5 3 3.5 4 4.5 5 5.5
Hasinger, Miyaji & Schmidt, 2004,A&A submitted
M. Schmidt methodT. Miyaji treatment(dotted: upper limit)-10.00
-9.50
-9.00
-8.50
-8.00
-7.50
-7.00
-6.50
-6.00
0 0.5 1 1.5 2 2.5 3 3.5 4 4.5 5 5.5
Wyithe & Loeb, 2003, ApJ, arbitrary norm
Menci et al., 2004, ApJ, arbitrary norm
Hasinger, Miyaji & Schmidt, 2005 Ueda et al., 2003, based on ~1000 AGN-1 based on ~250 AGN
Densities in soft and hard band
Very similar behaviour in hard and soft band. Soft samples go deeper and are more complete.
Local BH mass vs. accreted BH massfunction
•Accreted Black Hole massfunction derived from X-raybackground can be comparedwith the mass function of dormant relic black holes in local galaxies (Soltan 1982).
•These two estimates can bereconciled, if an energyconversion efficiency of ε=0.1 is assumed.
•Such high efficiencyrequires a spinning Kerr-BH! Marconi et al., 2004, MNRAS
X-ray vs. optical QSOs
Very large solid angle deepsurveys arerequired to discover z>5 QSOs
E-CDFSXMM/COSMOSDUO
High-z decline now seen in X-rays at all luminosities!
Wide & Deep Chandra and XMM surveys
#1 #2
PI: N. Brandt (PSU); 4x250 ksec
1.5 d
egre
e s
½ de
gree
Observations are ongoing
Extended Chandra HST/XMM-NewtonDeep Field South COSMOS Field
PI: N. Scoville (Caltech); XMM: 1.4 Msec, G. Hasinger (MPE)
Dark Universe Observatory
10°10°
Current SMEX competition; PI: R. Griffiths (CMU)
DUO will detect same number z>3 QSO, than are known from all othersurveys to date, including SDSS & 2dF
Summary• X-ray background practically resolved below 2 keV• At 2-10 keV about 50% resolved; still work to do• Type-2 QSOs found, type-2 fraction decreases
with LX• Background AGN have strong relativistic Fe line• Luminosity-dependent density evolution• Seyferts peak much later than QSO• Anti-hierarchical evolution not predicted even by
most recent semi-analytic models
=> Need (at least) 2 modes of BH accretionRole of accretion through mergers?
Binary Black Holes in Major
Mergers
NGC 6240
Komossa et al., 2003
Several more BinaryBlack Holes claimedin the meantime. BBH could bepresent in a fractionof normal quasars.
Major accretionmode for quasars?
Co-evolutionof Galaxyand BH
Simulation by Tiziana de Matteo, Volker Springel (MPA) & Lars Hernquist (CfA)
Black Hole Mass
Black Hole Luminosity
Star Formation Rate
Thank you very much !
Recommended