x-ray emission properties of blagn in the xmm-2df wide angle survey s. mateos, m.g. watson, j. a....

X-ray emission properties of X-ray emission properties of BLAGN in the BLAGN in the

XMM-2dF Wide Angle SurveyXMM-2dF Wide Angle Survey

S. Mateos, M.G. Watson, J. A. Tedds and the XMM-Newton Survey Science Centre

Department of Physics and Astronomy, University of Leicester

MotivationMotivationWide field surveys are essential to compile large enough samples Wide field surveys are essential to compile large enough samples of objects at 2-10 keV fluxes ~10of objects at 2-10 keV fluxes ~10-15-15-10-10-14-14 cgs to characterise the cgs to characterise the dominant population contributing to the Cosmic X-ray dominant population contributing to the Cosmic X-ray Background (CXRB)Background (CXRB)

The sample of BLAGN in The sample of BLAGN in XMM-2dF Wide Angle SurveyXMM-2dF Wide Angle Survey is one of is one of the largest samples of X- ray selected BLAGN assembled so far the largest samples of X- ray selected BLAGN assembled so far

Unique resource to study the overall optical and X-ray emission Unique resource to study the overall optical and X-ray emission properties of the population of faint Active Galactic Nuclei (AGN)properties of the population of faint Active Galactic Nuclei (AGN)

•Continuum shape, soft excess and X-ray absorption Continuum shape, soft excess and X-ray absorption propertiesproperties

•Constrain the fraction of X-ray absorbed BLAGN and the Constrain the fraction of X-ray absorbed BLAGN and the distribution of column densitiesdistribution of column densities

•Cosmic evolution of the emission properties and Cosmic evolution of the emission properties and dependence with X-ray luminositydependence with X-ray luminosity


2dF optical multi-fibre spectroscopy on the AAT obtained for 68 2dF optical multi-fibre spectroscopy on the AAT obtained for 68 XMM-NewtonXMM-Newton fields (t fields (texpexp ~ few tens of ksec) over an area of >15deg ~ few tens of ksec) over an area of >15deg22

More than 3000 sources with X-ray fluxes above ~10More than 3000 sources with X-ray fluxes above ~10 -14-14 cgs and cgs and optical counterparts brighter than V~21 observed and reduced. optical counterparts brighter than V~21 observed and reduced.

978 serendipitous X-ray sources with S (0.5-4.5 keV)>10-14 erg cm-2 s-1

spectroscopically identified:

641 BLAGN (65.5%)157 NELG (16%)

57 Gal (5.8%)123 Stars (12.6%)

BLAGN in the XMM-2dF Wide Angle SurveyBLAGN in the XMM-2dF Wide Angle Survey All 119 All 119 XMM-Newton XMM-Newton observations with overlap on the original observations with overlap on the original

area covered by the 2dF observations reprocessed using the area covered by the 2dF observations reprocessed using the latest pipeline of the second latest pipeline of the second XMM-NewtonXMM-Newton Serendipitous Source Serendipitous Source Catalogue 2XMM (pre-release: 2XMMp available at Catalogue 2XMM (pre-release: 2XMMp available at http://xmmssc-www.star.le.ac.ukhttp://xmmssc-www.star.le.ac.uk) )

Typical fluxes~break in the X-ray Typical fluxes~break in the X-ray source countssource counts

2-10 keV flux2-10 keV flux

X-ray spectral analysisX-ray spectral analysis

Co-added MOS and pn spectra obtained for each objectCo-added MOS and pn spectra obtained for each object

Selected 496 from 641 BLAGN with Selected 496 from 641 BLAGN with XMM-NewtonXMM-Newton X-ray spectra of X-ray spectra of sufficient quality for detailed X-ray spectral analysis sufficient quality for detailed X-ray spectral analysis

Simple power law and absorbed power law model fits Simple power law and absorbed power law model fits

Single-source analysis of brightest objects to constrain the Single-source analysis of brightest objects to constrain the presence and properties of additional spectral components (such presence and properties of additional spectral components (such as soft excess) in progressas soft excess) in progress

>70% objects with more>70% objects with morethan 150 EPIC net ctsthan 150 EPIC net cts

=1.96 ± 0.05=0.22 ± 0.03

BLAGN overall emission properties: BLAGN overall emission properties: broad band continuum shapebroad band continuum shape

Most BLAGN spectra from 0.2-12 keV (observer frame) best fitted with a power law although significant intrinsic dispersion in measured values detected


No clear trend with redshift up to z~4No clear trend with redshift up to z~4

The apparent hardening of The apparent hardening of at higher z at higher z produced by undetected soft excess emission at produced by undetected soft excess emission at

lower zlower z


Continuum shape does not show Continuum shape does not show obvious dependence with X-ray luminosity obvious dependence with X-ray luminosity

2-10 keV lum2-10 keV lum

BLAGN overall emission properties: BLAGN overall emission properties: intrinsic X-ray absorptionintrinsic X-ray absorption

X-ray absorption detected (F-testX-ray absorption detected (F-test≥95%≥95%) in 38 BLAGN (~8%)) in 38 BLAGN (~8%)

BLAGN at z=0.132BLAGN at z=0.132=1.55 =1.55 ± 0.2± 0.2NNHH=22.2 =22.2 ± 0.3 ± 0.3 cmcm-2-2

log (Llog (L2-102-10)=43.53)=43.53 cgs cgs

kT=0.20 kT=0.20 ± 0.04 keV± 0.04 keV


The hardening of The hardening of with X-ray flux known to be mostly with X-ray flux known to be mostly due to undetected X-ray absorptiondue to undetected X-ray absorption

Best fit Best fit values values

2-10 keV flux2-10 keV flux0.5-2 keV flux0.5-2 keV flux


No correlation between No correlation between and Nand NHH

Typical values of absorbing column density NTypical values of absorbing column density NHH~10~102121cmcm-2-2

For sources with NFor sources with NHH>10>102222 cm cm-2-2 existing correlation of optical and existing correlation of optical and

X-ray emission properties unclearX-ray emission properties unclear


Fraction of absorbed BLAGN does not depend on X-ray luminosity Fraction of absorbed BLAGN does not depend on X-ray luminosity or redshiftor redshift

<L<L2-102-10> = 44.2 unabsorbed BLAGN> = 44.2 unabsorbed BLAGN

<L<L2-102-10> = 44.3 absorbed BLAGN> = 44.3 absorbed BLAGN


No evident dependence of absorbing column density No evident dependence of absorbing column density with luminosity or redshift with luminosity or redshift

ConclusionsConclusions

0.2-12 keV emission0.2-12 keV emission of most BLAGN is best fitted with a power law of most BLAGN is best fitted with a power law • mean continuum shape ~1.96 mean continuum shape ~1.96 • intrinsic dispersion ~0.22 intrinsic dispersion ~0.22

Continuum shape Continuum shape • no significant evolution up to redshifts of ~4no significant evolution up to redshifts of ~4• no luminosity dependence in range 10no luminosity dependence in range 104242-10-104545erg serg s-1-1

Absorbed BLAGNAbsorbed BLAGN do not seem to occur preferentially at any particular do not seem to occur preferentially at any particular redshift or luminosityredshift or luminosity

X-ray absorption detected in ~8% of our BLAGNX-ray absorption detected in ~8% of our BLAGN • observed hardening of mean continuum shape with 0.5-2 keV flux observed hardening of mean continuum shape with 0.5-2 keV flux suggests that X-ray absorption is still undetected in a number of suggests that X-ray absorption is still undetected in a number of objects in our sampleobjects in our sample• no obvious dependence with redshift or luminosityno obvious dependence with redshift or luminosity• typical values ~10typical values ~102121 cm cm-2 -2 –a substantial fraction with detected –a substantial fraction with detected NNHH>10>1022 22 cmcm-2-2

• Existing correlation of optical and X-ray properties unclearExisting correlation of optical and X-ray properties unclear


Leicester University (UK)Leicester University (UK)

Mullard Space Science Laboratory-UCL (UK)Mullard Space Science Laboratory-UCL (UK)

Instituto de Física de Cantabria CSIC-UC (SpainInstituto de Física de Cantabria CSIC-UC (Spain)

Astrophysikalisches Institut Potsdam (Germany)Astrophysikalisches Institut Potsdam (Germany)

on behalf of the XMM-Newton Survey Science Centreon behalf of the XMM-Newton Survey Science Centrehttp://xmmssc-www.star.le.ac.ukhttp://xmmssc-www.star.le.ac.uk

Conclusions(I)Conclusions(I)

•The 0.2-12 keV emission of most BLAGN is best fitted The 0.2-12 keV emission of most BLAGN is best fitted with a power law with mean continuum shape of ~1.96 with a power law with mean continuum shape of ~1.96 although with a significant intrinsic dispersion of ~0.22 although with a significant intrinsic dispersion of ~0.22 around the mean measured valuearound the mean measured value

•The overal X-ray emission properties (continuum The overal X-ray emission properties (continuum shape and X-ray absorption) of our BLAGN do not shape and X-ray absorption) of our BLAGN do not seem to show any significant evolution up to redshifts seem to show any significant evolution up to redshifts of ~4 or luminosity dependence within the luminosity of ~4 or luminosity dependence within the luminosity range 10range 104242-10-104545erg serg s-1-1

•X-ray absorption was detected in ~8% of our BLAGN, X-ray absorption was detected in ~8% of our BLAGN, although the observed hardening of the mean continuum although the observed hardening of the mean continuum shape with 0.5-2 keV flux suggests that X-ray absorption shape with 0.5-2 keV flux suggests that X-ray absorption is still undetected in a number of objects in our sample is still undetected in a number of objects in our sample

Conclusions(II)Conclusions(II)

•The observed absorption column densities in our The observed absorption column densities in our sample of BLAGN have typical values ~10sample of BLAGN have typical values ~102121 cm cm-2-2, , whithout obvious dependence with redshift or whithout obvious dependence with redshift or luminosityluminosity

•Absorbed BLAGN do not seem to occur preferentially at Absorbed BLAGN do not seem to occur preferentially at any particular redshift or luminosity any particular redshift or luminosity

x-ray emission properties of blagn in the xmm-2df wide angle survey s. mateos, m.g. watson, j. a....

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