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J/A+A/444/79  XMM observations of Lockman Hole brightest AGNs   (Mateos+, 2005)
XMM-Newton observations of the Lockman Hole.
IV: spectra of the brightest AGN.
    Mateos S., Barcons X., Carrera F.J., Ceballos M.T., Hasinger G.,
    Lehmann I., Fabian A.C., Streblyanska A.
   <Astron. Astrophys., 444, 79-99 (2005)>
   =2005A&A...444...79M
ADC_Keywords: X-ray sources ; Surveys ; Active gal. nuclei

Keywords: X-rays: general - X-rays: diffuse background - surveys -
          galaxies: active

Abstract:
    This paper presents the results of a detailed X-ray spectral analysis
    of a sample of 123 X-ray sources detected with XMM-Newton in the
    Lockman Hole field. This is the deepest observation carried out with
    XMM-Newton with more that 600ks of good EPIC-pn data. We have
    spectra with good signal to noise (>500 source counts) for all objects
    down to 0.2-12keV fluxes of 5x10-15erg/cm2/s (flux limit of
    6x10-16erg/cm2/s in the 0.5-2 and 2-10keV bands). At the time of
    the analysis, we had optical spectroscopic identifications for 60% of
    the sources, 46 being optical type-1 AGN and 28 optical type-2 AGN.
    Using a single power law model our sources' average spectral slope
    hardens at faint 0.5-2keV fluxes but not at faint 2-10keV fluxes.

File Summary:

       FileName      Lrecl  Records   Explanations

ReadMe            80        .   This file
table8.dat       112      123   X-ray catalogue


See also:
   J/A+A/393/425 : Spectral analysis of Lockman Hole (Mainieri+, 2002)
   J/A+A/329/482 : ROSAT Deep Survey in the Lockman Hole (Hasinger+, 1998)
   J/A+A/398/901 : VLA survey at 6cm in the Lockman Hole (Ciliegi+, 2003)
   J/A+A/413/843 : Far IR survey in the Lockman Hole (Kawara+, 2004)
   J/A+A/427/23  : 14.3um survey in the Lockman Hole (Fadda+, 2004)
   J/A+A/427/773 : ISOCAM 14.3um Deep Survey in Lockman Hole (Rodighiero+, 2004)
   J/AJ/125/2521 : 2MASS6x survey of the Lockman Hole (Beichman+, 2003)
   J/PASJ/53/445 : ASCA Deep survey in Lockman Hole Field (Ishisaki+, 2001)


Byte-by-byte Description of file: table8.dat

   Bytes Format Units     Label       Explanations

   1-  4  I4    ---       [MBC2005]   [5/2045] Source sequential number
   6-  8  I3    ---       RDS         ? X-ray source ROSAT number (RDS NNN)
  10- 13  A4    ---       RDSO        Optical Source ROSAT number (RDS NNNA)
  15- 16  I2    h         RAh         Right ascension (J2000.0) (1)
  18- 19  I2    min       RAm         Right ascension (J2000.0) (1)
  21- 25  F5.2  s         RAs         Right ascension (J2000.0) (1)
      27  A1    ---       DE-         Declination sign (J2000.0) (1)
  28- 29  I2    deg       DEd         Declination (J2000.0) (1)
  31- 32  I2    arcmin    DEm         Declination (J2000.0) (1)
  34- 38  F5.2  arcsec    DEs         Declination (J2000.0) (1)
  40- 44  A5    ---       Class       Source classification from optical
                                       spectroscopy
  45- 46  A2    ---       n_Class     [* ] **: BAL QSO
  48- 52  F5.3  ---       z           ?=- Redshift
  54- 59  A6    ---       Model       Best fit spectral model (2)
  61- 64  F4.2  ---       Gamma       Power law spectral slope
  66- 69  F4.2  ---       e_Gamma     Power law spectral slope low error bar
  71- 74  F4.2  ---       E_Gamma     Power law spectral slope high error bar
  76- 80  F5.2  [cm-2]    log(Abs)    ? Logarithm of the column density
                                         of excess absorption (3)
  82- 85  F4.2  [cm-2]    e_log(Abs)  ? Low error bar of column density
                                         of excess absorption
  87- 90  F4.2  [cm-2]    E_log(Abs)  ? High error bar of column density
                                         of excess absorption
  92- 95  F4.2  10-17W/m2 F(0.5-2)keV  Flux in the [0.5-2]keV band
  97-100  F4.2  10-17W/m2 F(2-10)keV  Flux in the [2-10]keV band
 102-106  F5.2  [10-7W]  L(0.5-2)keV  ? Logarithm of luminosity in the
                                         [0.5-2]keV rest-frame band (4)
 108-112  F5.2  [10-7W]   L(2-10)keV  ? Logarithm of the luminosity in the
                                         [2-10]keV rest-frame band

Note (1): The coordinates of the sources RA and DE, are not the X-ray
     positions from the Lockman Hole catalogue (H. Brunner et al. 2005,
     in prep.), but the centres of the regions used to extract the spectra
     of the objects.
Note (2): Best fit spectral model as follows:
   SPL  = Single power law
   APL  = Absorbed power law
   SE   = Soft excess emission
   CAPL = Absorption with partial covering absorber
   2SPL = Two power laws (to fit spectral hardening at high energies)
Note (3): Intrinsic rest-frame absorption if the source is already identified.
          Observed absorption if the source is still unidentified
Note (4): Luminosities are corrected for the effect of absorption.



Acknowledgements: Silvia Mateos, sm279(at)star.le.ac.uk


References:
  Hasinger et al.,     Paper I        2001A&A...365L..45H
  Mainieri et al.,     Paper II       2002A&A...393..425M, Cat. J/A+A/393/425
  Streblyanska et al., Paper III      2005A&A...432..395S
(End)                                      Patricia Vannier [CDS]    01-Dec-2005