J/AJ/112/62         Quasar absorption-line systems (Tanner+ 1996)
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A study of quasar absorption-line systems with IRAS
       Tanner A.M., Bechtold J., Walker C.E., Black J.H., Cutri R.M.
      <Astron. J. 112, 62 (1996)>
      =1996AJ....112...62T      (SIMBAD/NED BibCode)
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ADC_Keywords: QSOs ; Redshifts ; Spectra, infrared

Mission_Name: IRAS


Abstract:
    A survey of quasar absorbers was conducted using the Infrared
    Astronomical Satellite (IRAS) database. Quasars with known intervening
    absorption-line systems and broad absorption line (BAL) QSOs were
    selected primarily from Junkkarinen et al. (1991ApJS...77..203J). Of
    the 570 quasars with IRAS data, 52 showed 3{sigma} or better
    detections in at least one band in SCANPI analysis. The origin of the
    IRAS flux could be from the absorption-line systems, other galaxies,
    or the quasar itself. The spectral energy distributions for quasars
    detected in the absorption-line sample and BAL QSOs were found to be
    redder than those of two control samples which suggests that some of
    the IRAS flux may arise in dust associated with the intervening
    galaxies. IRAS SUPERSCANPI processing was carried out for 77 quasars
    with known Mg II absorption at Zabs<1 to investigate the ensemble
    far-infrared properties of these objects. SUPERSCANPI processing
    evaluates the median flux for many different positions on the sky,
    resulting in an improvement in the effective sensitivity. A control
    sample consisting of objects with no Mg II absorption known at Zabs<1
    but with the same distribution of absolute V-magnitude, Zem and
    radio-loud fraction for the background quasars was also processed. The
    Mg II sample was detected at 3{sigma} or better in all four IRAS bands
    with a significantly larger flux than the control sample at 60µm
    and 100µm. If this far-infrared emission is from the absorber
    galaxies, then the far-infrared luminosity of the composite Mg II
    absorber was found to be comparable to that of a starbursting galaxy,
    although such a high star-formation rate is inconsistent with the
    optical and near-infrared colors of low-redshift Mg II systems. Four
    of the quasars with individual IRAS detections have intervening
    galaxies identified with the Mg II absorption-lines. The spectral
    energy distributions of these galaxies imply far-infrared luminosities
    in excess of what Arp 220 would give at their redshifts. While all the
    external evidence suggests that the detection of far-infrared emission
    from the absorber sample may not be connected to the presence of the
    Mg II absorber, we discuss future observations which may help explain
    our results.

File Summary:

       FileName      Lrecl  Records   Explanations

ReadMe            80        .   This file
table1            32       38   Additional quasar in absorption-line (AL) sample,
                               not in JHB (Cat. J/ApJS/77/203)
table2            32       34   Damped Ly{alpha} sample
table3           173       46   IRAS ADDSCAN detections
table4           173        6   BAL QSO's detected with IRAS ADDSCAN analysis
table5            42       77   Low redshift Mg II absorption line sample
table6            48       77   Control sample with no Mg II absorption for Zabs<1


Byte-by-byte Description of file:  table1  table2

   Bytes Format Units   Label     Explanations

   1-  8  A8    ---     QSO       Quasar name
       9  A1    ---     r_QSO     Reference (1)
  11- 15  F5.3  ---     zem       Emission redshift
  17- 21  F5.3  ---     zabs      ? Absorption redshift
  23- 27  F5.2  mag     Vmag      ? V magnitude from Hewitt & Burbidge
                                     (1993ApJS...87..451H)
  29- 32  F4.2  ---     RL        ? Radio loudness  (2)

Note (1): a : Steidel & Sargent (1992ApJS...80....1S)
          b : Aldcroft et al. (1994ApJS...93....1A)
          c : Lanzetta et al. (1991ApJS...77....1L)
          d : Junkkarinen et al. (1991, Cat. J/ApJS/77/203)
          e : White et al. (1993ApJ...407..456W)
          f : Turnshek et al. (1989ApJ...344..567T)
          g : Wolfe et al. (1986ApJS...61..249W)
          h : Francis & Hewitt (1993AJ....105.1633F)
Note (2): RL=log[fv(5GHz)/fv(V)], where fv(5GHz) is the radio flux density
              at 5GHz and [fv(V) is the V band flux density, based on 5 GHz
              flux densities from Veron-Cetty & Veron (1987, See Cat. VII/188)


Byte-by-byte Description of file:  table3  table4

   Bytes Format Units   Label     Explanations

   1-  8  A8    ---     QSO       Quasar name
   9- 11  A3    ---     Note      Note (1)
  13- 17  F5.3  ---     zem       ? Emission redshift
  19- 23  F5.2  mag     Vmag      ? V magnitude
  25- 32  F8.5  ---     zabs      ? Absorption redshift
  34- 35  I2    h       RAh       Right ascension (1950.0)
  37- 38  I2    min     RAm       Right ascension (1950.0)
  40- 44  F5.2  s       RAs       Right ascension (1950.0)
      46  A1    ---     DE-       Declination
  47- 48  I2    deg     DEd       Declination (1950.0)
  50- 51  I2    arcmin  DEm       Declination (1950.0)
  53- 56  F4.1  arcsec  DEs       Declination (1950.0)
      58  A1    ---     l_S12um   Limit flag on 12um
  59- 63  F5.3  Jy      S12um     IRAS flux at 12um (2)
  64- 68  F5.3  Jy      e_S12um   ? rms uncertainty on S12um
      70  A1    ---     l_S25um   Limit flag on 25um
  71- 75  F5.3  Jy      S25um     IRAS flux at 25um (2)
  77- 81  F5.3  Jy      e_S25um   ? rms uncertainty on S25um
      83  A1    ---     l_S60um   Limit flag on 60um (2)
  84- 88  F5.3  Jy      S60um     IRAS flux at 60um
  89- 93  F5.3  Jy      e_S60um   ? rms uncertainty on S60um
      94  A1    ---     l_S100um  Limit flag on 100um (2)
  95-100  F6.3  Jy      S100um    IRAS flux at 100um
 101-104  F4.2  Jy      e_S100um  ? rms uncertainty on S100um
 106-109  F4.2  ---     RL        ? Radio loudness (3)
     110  A1    ---     n_RL      [OBj] Note on RL (3)
 112-117  F6.4  ---     zabs2     ? Second absorption redshift
 119-124  F6.4  ---     zabs3     ? Second absorption redshift
 126-131  F6.4  ---     zabs4     ? Second absorption redshift
 133-138  F6.4  ---     zabs5     ? Second absorption redshift
 140-145  F6.4  ---     zabs6     ? Second absorption redshift
 147-152  F6.4  ---     zabs7     ? Second absorption redshift
 154-159  F6.4  ---     zabs8     ? Second absorption redshift
 161-166  F6.4  ---     zabs9     ? Second absorption redshift
 168-173  F6.4  ---     zabs10    ? Second absorption redshift

Note (2): 3 sigma upper limits given when not detected

Note (1): c : galaxies or quasars in vicinity visible on Palomar Sky Survey.
          d : UGC 439, IRAS source is 45 arcseconds northwest of quasar.
          e : bright stars nearby visible on Palomar Sky Survey.
          f : IRAS source is 1 arcminute northwest of quasar.
          g : IRAS source is 30 arcseconds southeast of quasar.
          h : IRAS source is 1 arcminute north of quasar.
          i : NGC 3067, IRAS source is 2 arcminutes southwest of quasar.
          k : IRAS source is 1 arcminute south of quasar.
          l : NGC 6045.
          m : ESO 400-G012.
Note (3): RL=log[fv(5GHz)/fv(V)], where fv(5GHz) is the radio flux density
              at 5GHz and [fv(V) is the V band flux density, based on 5 GHz
              flux densities from Veron-Cetty & Veron (1987, See Cat. VII/188)
              unless otherwise stated.
          j : RL based on 5 GHz flux densities from Kellerman et al.
               (1994AJ....108.1163K).
          B : BL Lac
          O : OVV


Byte-by-byte Description of file:  table5  table6

   Bytes Format Units   Label     Explanations

   1-  9  A9    ---     QSO       Quasar name
  10- 12  A3    ---     n_QSO     Note (1)
  15- 20  F6.4  ---     zem       ? Emission redshift
  22- 27  F6.4  ---     zabs      ? Absorption redshift
  29- 33  F5.2  mag     Vmag      V magnitude
  36- 40  F5.3  ---     RL        ? Radio loudness
      42  I1    ---     Ref       ? References, for table6 only (2)

Note (1): a: Objects with individual IRAS detections
          b: Removed for the control list for SUPERSCANPI without
              IRAS detections
Note (2): 1: Aldcroft et al. (1994ApJS...93....1A)
          2: Steidel & Sargent (1992ApJS...80....1S)
          3: Barthel et al. (1990A&AS...82..339B)


History: Prepared via OCR at CDS.
         In table6, for QSO 0736-0620, V=718.5 in the printed version,
          we change this value in 18.5 in the electronic table
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(End)                           James Marcout, Patricia Bauer [CDS]  17-Jun-1997