The XMM-Newton hard band wide angle Survey Nicoletta Carangelo and Silvano Molendi (IASF-MI(CNR))...
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Transcript of The XMM-Newton hard band wide angle Survey Nicoletta Carangelo and Silvano Molendi (IASF-MI(CNR))...
The XMM-Newton hard The XMM-Newton hard band wide angle Surveyband wide angle SurveyNicoletta Carangelo and Silvano Molendi (IASF-Nicoletta Carangelo and Silvano Molendi (IASF-
MI(CNR))MI(CNR))
Epic Consortium Meeting Palazzo Steri, Palermo, 14-16 October 2003
The Cosmic X-ray The Cosmic X-ray BackgroundBackground
Giacconi et al. 1962
XRB as superposition of unabsorbed and absorbed
AGNs
Comastri et al. 1995
Several self-consistent synthesis models (e.g.
Madau,Ghisellini & Fabian 1994; Comastri et al. 1995;
Gilli, Salvati & Hasinger 2001), Franceschini, Braito
& Fadda 2002; Gandhi & Fabian 2003) of the XRB based on the unification
schemes of AGNs
KEY INGREDIENT: NH
Lack of any X-ray luminosity function for Type 2 AGNsLack of any X-ray luminosity function for Type 2 AGNs Absorbing column density (NAbsorbing column density (NHH) distribution: assumed ) distribution: assumed
to be independent of z and L and has been treated ad to be independent of z and L and has been treated ad free parameter in the fitting procedurefree parameter in the fitting procedure
IS THE ONLY PARAMETER IN THE MODEL IS THE ONLY PARAMETER IN THE MODEL THAT HAS NOT BEEN CONSTRAINED BY ANY THAT HAS NOT BEEN CONSTRAINED BY ANY
DIRECT MEASUREMENTDIRECT MEASUREMENT
The Cosmic X-ray The Cosmic X-ray Background:Background:
critical parameters of the critical parameters of the modelmodel
Gilli et al. 1999
Several works but all affected by selection
effects, incompleteness
problems or by biases related to the
absorption
Obtain a more reliable NH distribution according to criteria independent of absorption effects
GOAL
We need….
HARD BAND
[7-11] keV
The less biased against absorbed
objectsAccurate X-ray Spectroscopy and characterization of the sources
XMM
High XMM throughput
+
selection of bright objects
XMM-Newton Serendipitous XMM-Newton Serendipitous Survey in the hard band [7-11] Survey in the hard band [7-11]
keVkeV
GOAL
To build a local reference sample less affected that any other by NH
bias Study its properties and compare these with those of other deeper and non local samples
NH distribution: a solid determination from direct spectral modelling
Constrain the XRLF of absorbed objects and the unification schemes and AGN synthesis models of the XRB
Relative importance of the reflection component and EW of the Fe lines
The XMM-Newton hard The XMM-Newton hard band wide angle Survey: band wide angle Survey:
the samplethe sampleAnalyzed ALL XMM-EPIC fields including Target of
Opportunity Observations (ToO), publically available before October 1st 2003 selected
following these criteria
Objects at high galactic latitude |b|>27 and excluding Magellanic Clouds
With exposure time texp>10 ksec
With Full Frame Observations in PN
A total of 140 fields observed A total of 140 fields observed
Survey covers about 40 square degreesSurvey covers about 40 square degrees Searching for rare objectsSearching for rare objects
A total of A total of 8080 sources have been detected in the [7- sources have been detected in the [7-11] keV band down to a limiting flux of about F[7-11] keV band down to a limiting flux of about F[7-11]=3 1011]=3 10-14-14 erg cm erg cm-2-2 s s-1-1
The XMM-Newton hard The XMM-Newton hard band wide angle Survey: band wide angle Survey:
the samplethe sample
Cross-correlation of the 80 Cross-correlation of the 80 source X-ray position source X-ray position
The XMM-Newton hard band The XMM-Newton hard band wide angle Survey: wide angle Survey:
the samplethe sampleNED
For 15 objetcs the optical counterpart is known with a measured z
For 5 objects more than one optical counterpart within 0.2’ with measured z DSS For 47 sources optical
counterpart visible in the R plates (Rlim=21)
R≤22-23Fiore et al. 2003
HELLAS2XMM (Baldi et al. 2002)
CDFN (Barger et al. 2002)
LH (Baldi et al. 2001; Mainieri et al. 2002)
SSA13 (Mushotzky et al. 2000; Barger et al. 2001)
The XMM-Newton hard band The XMM-Newton hard band wide angle Survey: wide angle Survey:
data handlingdata handlingData reduction using the XMM-SAS v5.4Data reduction using the XMM-SAS v5.4
Baldi et al. (2002) pipeline implemented Baldi et al. (2002) pipeline implemented for [7-11] keV bandfor [7-11] keV band
Merge together the MOS and PN images to
increase the S/N of the sources
Automatic Spectral pipeline
Cleaned event files
SOURCE SPECTRUM30”<rext<45”
BACKGROUND SPETRUMrbkg=3rext
PN(single,double,s+d)-MOS1-MOS2-MOS(=MOS1+MOS2)
Automatic Spectral pipeline
SPECTRAL MODEL IN THE 0.4 -10 keV ENERGY RANGE
The XMM-Newton hard band The XMM-Newton hard band wide angle Survey:wide angle Survey:preliminary spectral preliminary spectral
characterizationcharacterization Model wabs(pow) in the 2-10 keV band
Preliminary measure of NH~30-35% with NH>1022
HELLAS2XMM-(4.5-10 keV): sp.analy
HELLAS2XMM-HR (Baldi et al. 2002)
CDFS (Giacconi et al. 2002)
ASCA MSS (Ueda et al. 2001)
Piccinotti et al. 1982
Comastri et al. 2001
The XMM-Newton hard band The XMM-Newton hard band wide angle Survey:wide angle Survey:
preliminary multiwavelength preliminary multiwavelength studystudy
A large fraction of obscured AGNs resides in objects with an extreme
X/O
Redshift and luminosity
distribution key parameters to test synthesis models of
XRBHigh X/O •Hard spectra
•Correlation X/O-L[2-10] for optically obscured AGNs
•Large majority are Ty2 QSO
•NIR observations:
•Correlations R-K colors and X/O: X/O>10 R-K>5
•Host galaxies are ellipticalsSee Fiore et al. 2003, Mignoli et al. 2003
X/O Fiore et al. 2003 Survey [7-11] keV(Hellas2XMM [2-10] keV)
0.1-3 55% 40%
3-10 21% 14%
>10 24% 46%
Survey in the hard band and at high X-ray flux
Best method to find objects with extreme X/O and for which optical follow-up is
attainable with present class of telescopes
The XMM-Newton hard The XMM-Newton hard band wide angle Survey: band wide angle Survey:
a particular example a particular example
wabs[1](mekal[2]+zwabs[3](pexrav[4]+zgauss[5])
z
z=0.31±0.03 NH~ 1023 cm-2
L[2-10]keV=1.5 1044 erg s-1
QSO2
Carangelo et al. 2003 (astro-ph/0309732)
ConclusionConclusion
XMM survey in the hard [7-11] keV band which allows for the XMM survey in the hard [7-11] keV band which allows for the first time to perform an accurate spectral analysis and first time to perform an accurate spectral analysis and caracterization of a local reference sample less affected than caracterization of a local reference sample less affected than any other by Nany other by NHH bias bias
NNHH distribution distribution XLF of absorbed objectsXLF of absorbed objects
THIS IS THE BEST WE CAN DO WITH THE CURRENT THIS IS THE BEST WE CAN DO WITH THE CURRENT GENERATION OF X-RAY SATELLITES GENERATION OF X-RAY SATELLITES
FutureFutureOptical follow-upOptical follow-up TNG & ESO 3.6mTNG & ESO 3.6m
Multiwavelength properties: Multiwavelength properties: X/O-L[2-10] X/O-L[2-10] see Fiore et al. see Fiore et al. 20032003
X/O-(R-K) X/O-(R-K) see Mignoli see Mignoli et al. 2003et al. 2003