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J/ApJ/472/509       Lyman-alpha Forest in Q0000-26                    (Lu+ 1996)
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The Lyman-alpha Forest at z about 4: Keck HIRES Observations of Q0000-26
    Lu L., Sargent W.L.W., Womble D.S., Takada-Hidai M.
   <Astrophy. J. 472, 509 (1996)>
   =1996ApJ...472..509L
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ADC_Keywords: QSOs

Abstract:
   This file contains the list of absorption lines found in the spectrum
   of the zem=4.1 quasar Q0000-26 obtained with the 10m Keck I telescope.
   The spectrum has a resolution of 6.6 km/s, with typical
   signal-to-noise ratio 25-35 per resolution element. The absorption
   lines found in the Lyman-alpha forest region has been deblended using
   the Voigt profile fitting routine VPFIT from Robert Carswell and
   colleagues; redshift, column density, and Doppler width are provided
   for each line in the list.

File Summary:
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 FileName       Lrecl       Records      Explanations
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ReadMe             80             .      This file
lu1.dat            65           489      Measured wavelengths
lu2.dat            43            82      Redshifts
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Byte-by-byte Description of file: lu1.dat
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 Bytes     Format     Units    Label     Explanations
--------------------------------------------------------------------------------
  1-  3    I3         ---      No        Running number
  5- 11    F7.2       0.1nm    lambda    Wave length
 13- 23    A11        ---      ID        Element identification
 25- 32    F8.6       km/s     z         Redshift 
 34- 41    F8.6       km/s     e_z       Mean error of z
 43- 47    F5.1       km/s     b         Effective radial velocity dispersion
 49- 52    F4.1       km/s     e_b       Mean error of b
 54- 58    F5.2       m-4      logN      logN (column density)
 60- 63    F4.2       m-4      e_logN    Mean error of logN
     65    I1         ---      n_No     *?Note on observation
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Note on n_No:
   1 = This Lyman alpha line is associated with identified metal systems.
   2 = This feature agrees with the expected position of S II lambda 1253
       in the zabs)=3.39 damped Lyman alpha system. The identification is
       tentative.
   3 = The Si II lambda 1260, and 1304 lines are fitted simultaneously
       with the Si II lambda 1526 line redward of Lyman alpha emission.
   4 = The Fe II lambda 2344 absorption is fitted simultaneously with the
       Fe II lambda 2586, and 2600 absorption redward of Lyman alpha
       emission.
   5 = The O I lambda 1302 absorption is fitted with the redshift and the
       Doppler width fixed to those of the corresponding Si II components
       in the same system, hence there are no error estimates for the
       redshifts and Doppler widths. One of the components is rejected by
       VPFIT as not necessary.
   6 = The C II lambda 1334 absorption is badly blended with the strong
       Lyman alpha absorption corresponding to the zabs)=3.8190 C IV
       system. Only one component of C II is clearly discernible.
   7 = Contaminated by cosmic rays or poorly subtracted night sky lines.
   8 = This feature has a statistical significance above 3 sigma but less
       than 4 sigma.
   9 = Blended with telluric absorption lines.
   10 = The corresponding C IV lambda 1550 absorption occurs in a
       corrupted part of the spectrum caused by an ink mark on the CCD.
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Byte-by-byte Description of file: lu2.dat
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 Bytes     Format     Units    Label    Explanations
--------------------------------------------------------------------------------
  1-  3    I3         ---      No       ?Running number
  5- 11    F7.2       0.1nm    lambda   ?Wave length
 13- 17    F5.3       0.1nm    lam_obs  ?Observed wave length
 19- 23    F5.3       0.1nm    e_lambda ?Mean error of observed wave length
 25- 33    A9         ---      ID        Element identification
 35- 40    F6.4       km/s     z        ?Redshift 
 42- 43    I2         ---      n_No    *?Note on observation
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Note on n_No:
    See note on n_No for lu1.dat 
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(End)       N. G. Roman           [SSDOO/ADC]         14-Jun-1997