Access to Astronomical Catalogues

J/A+A/407/791    ACO 370, 2218 and 2390 fluxes at 7 and 15um   (Metcalfe+, 2003)
An ISOCAM survey through gravitationally lensing galaxy clusters.
I. Source lists and source counts for A370, A2218 and A2390.
    Metcalfe L., Kneib J.-P., McBreen B., Altieri B., Biviano A., Delaney M.,
    Elbaz D., Kessler M.F., Leech K., Okumura K., Ott S., Perez-Martinez R.,
    Sanchez-Fernandez C., Schulz B.
   <Astron. Astrophys. 407, 791 (2003)>
   =2003A&A...407..791M
ADC_Keywords: Clusters, galaxy ; Infrared sources

Mission_Name: ISO

Keywords: surveys - galaxies: clusters: individual: Abell 370 -
          galaxies: clusters: individual: Abell 2218 -
          galaxies: clusters: individual: Abell 2390 - gravitational lensing -
          infrared: galaxies

Abstract:
    ESA's Infrared Space Observatory (ISO) was used to perform a deep
    survey with ISOCAM through three massive gravitationally lensing
    clusters of galaxies. The total area surveyed depends on source flux,
    with nearly seventy square arcminutes covered for the brighter flux
    levels in maps centred on the three clusters Abell 370, Abell 2218 and
    Abell 2390. We present maps and photometry at 6.7um (hereafter 7um)
    and 14.3um (hereafter 15um), showing a total of 145 mid-infrared
    sources and the associated source counts.

File Summary:

       FileName      Lrecl  Records   Explanations

ReadMe            80        .   This file
table4.dat       103       20   15um sources detected in the field of Abell  370
table5.dat       105       46   15um sources detected in the field of Abell 2218
table6.dat       105       28   15um sources detected in the field of Abell 2390
table7.dat       103       11   7um sources detected in the field of Abell  370
table8.dat       103       48   7um sources detected in the field of Abell 2218
table9.dat       103       25   7um sources detected in the field of Abell 2390


See also:
     B/iso : ISO Observation Log of validated data (ISO Data Centre, 2001)
    VI/101 : ISO Observation Log (ISO Team, 2001)


Byte-by-byte Description of file: table?.dat

   Bytes Format Units   Label     Explanations

   1-  3  A3    ---     ---       [ACO]
   5- 12  A8    ---     Name      Sequential number, NNNN NNa (1)
      13  A1    ---     f_Name    [-+] -: source seen only at 15um
                                       +: source seen only at 7um
  15- 19  F5.3  ---     Signal    Source signal in detector units, at 7 or 15um
  21- 25  F5.3  ---     e_Signal  rms uncertainty on Signal
  27- 32  F6.2  ---     Sign      Significance of the detection
                                   (S/σfloor)
  34- 38  F5.3  mJy     Flux      Flux density, at 7 or 15um
  40- 44  F5.3  mJy     e_Flux    rms uncertainty on Flux
  46- 50  D5.3  mJy     Flens     Intrinsic flux density after correction for
                                   lensing amplification, at 7 or 15um
  52- 56  F5.3  mJy     e_Flens   rms uncertainty on Flens
  58- 59  I2    h       RAh       Right ascension (J2000)
  61- 62  I2    min     RAm       Right ascension (J2000)
  64- 67  F4.1  s       RAs       Right ascension (J2000)
      69  A1    ---     DE-       Declination sign (J2000)
  70- 71  I2    deg     DEd       Declination  (J2000)
  73- 74  I2    arcmin  DEm       Declination (J2000)
  76- 77  I2    arcsec  DEs       Declination (J2000)
  79- 84  F6.4  ---     z         ? Spectroscopic redshift (3)
  87-103  A17   ---     r_z       Notes and reference for z (2)

Note (1): In table7.dat:
    ISOA221828+ (ACO 2218 28 +) and 45+ ACO 2218 45 + are extended
    sources even at ISO resolution. The reduction algorithm is not adapted
    to treat extended structure and the transformation of extended
    structure has not been characterised. No attempt has been made here to
    correct for this in the case of these two cluster sources. For these
    sources, the quoted fluxes should be regarded as probable
    underestimates, especially in the case of ISOA221828+.
Note (2): Redshift references:
     B   = Barger et al. (1999AJ....117.2656B)
     C   = Cowie et al. (2001ApJ...551L...9C)
     Eb  = Ebbels et al., 1998MNRAS.295...75E
     I   = Ivison et al. (1998MNRAS.298..583I).
     K   = Kneib, unpublished.
     L1  = LeBorgne et al. (1991A&AS...88..133L)
     L2  = LeBorgne et al., 1992A&AS...95...87L
     M   = Mellier et al. (1988A&A...199...13M);
     N   = NED
     P   = Pello et al., 1991ApJ...366..405P
     S01 = Smail et al. (2001, Cat. J/MNRAS/323/839)
     S8  = Soucail et al. (1988A&AS...73..471S);
     S9  = Soucail et al. (1999A&A...343L..70S);
     Y   = Yee et al. (1996, Cat. J/ApJS/102/289)
     SED = Spectral fitting
Note (3): the redshift has been assigned to 0 for stars,
    or to 0.7 (median redshift of the background population) 
    for background objects lacking spectroscopic redshift
    (the redshift has then no reference assigned).


History:
    From electronic version of the journal
(End)                         James Marcout, Patricia Bauer [CDS]    24-Oct-2003