ADC/CDS Standard Document for Catalog:
/journal_tables/A+A/319/235/

1. Use the ADC Data Viewer Suite to visualize the data.
2. Get the data files via anonymous FTP. (See Note.)

J/A+A/319/235       CN in circumstellar envelopes survey (Bachiller+ 1997)
================================================================================
A survey of CN in circumstellar envelopes
     Bachiller R., Fuente A., Bujarrabal V., Colomer F., Loup C., 
     Omont A., de Jong T.
    <Astron. Astrophys. 319, 235 (1997)>
    =1997A&A...319..235B      (SIMBAD/NED BibCode)
================================================================================
ADC_Keywords: Stars, giant ; Abundances
Keywords: stars: circumstellar matter - stars: AGB, post AGB -
          stars: abundances - radio lines: stars - molecular processes

Description:
    We list in Table 1 the observed stars together with some of their
    characteristics. Distances, expansion velocities, mass loss rates, and
    spectral types are taken from the compilations of Bujarrabal et al.
    (1994) <J/A+A/285/247> and Loup et al. (1993A&AS...99..291). The
    sample includes C-rich and O-rich objects, some S-stars, a few
    proto-PN, and a young PN (NGC7027). See paper for more details. In
    Table 2, we give some of the observational parameters. A_low_ and
    A_high_ refer to the integrated intensity of the low-frequency and
    high-frequency fine-structure groups. The intrinsic intensity ratios,
    R=A_high_/A_low_, are R(1-0)=2 and R(2-1)=1.8. In principle, the
    observation of several components with different intrinsic strengths
    allows an estimate of the line optical depth, and the value of R gives
    an estimate of the envelope thickness.

File Summary:
--------------------------------------------------------------------------------
  FileName      Lrecl  Records   Explanations
--------------------------------------------------------------------------------
ReadMe            80        .   This file
table1           101       42   Circumstellar envelopes observed in the CN lines
table2            63       42   CN observational results
tables.tex        79      187   LaTeX version of the tables
--------------------------------------------------------------------------------

Byte-by-byte Description of file: table1
--------------------------------------------------------------------------------
   Bytes Format Units   Label     Explanations
--------------------------------------------------------------------------------
       1  A1    ---     Type      [CO ] C: C-rich object, O: O-rich object,
                                        blank: Other objects
   3- 13  A11   ---     Name      Star name
  15- 16  I2    h       RAh       Right ascension (1950.0)
  18- 19  I2    min     RAm       Right ascension (1950.0)
  21- 24  F4.1  s       RAs       Right ascension (1950.0)
      26  A1    ---     DE-       Declination sign
  27- 28  I2    deg     DEd       Declination (1950.0)
  30- 31  I2    arcmin  DEm       Declination (1950.0)
  33- 34  I2    arcsec  DEs       Declination (1950.0)
  36- 39  I4    kpc     Dist      Distance
  41- 46  E6.1  km/s    ExpV      Expansion velocity
  49- 50  I2 solMass/yr DMass     Mass loss rate
      51  A1    ---   n_DMass     [a] Note on mass loss rate (1)
  53- 72  A20   ---     Comment   Spectral type and comments
--------------------------------------------------------------------------------
Note (1): a: This value corresponds to the intense CO component which is
              superimposed on a broader emission plateau.
--------------------------------------------------------------------------------

Byte-by-byte Description of file: table2
--------------------------------------------------------------------------------
   Bytes Format Units   Label     Explanations
--------------------------------------------------------------------------------
       1  A1    ---     Type      [CO ] C: C-rich object, O: O-rich object,
                                        blank: Other objects
   3- 13  A11   ---     Name      Source name
      15  A1    ---   l_Tpeak1    [~] Limit flag on Tpeak1
  16- 19  F4.2  K       Tpeak1    ? Peak temperature (N=1->0)
  21- 24  F4.1  K.km/s  Ahigh1    ? Integrated intensity of the high-frequency
                                     fine-structure groups (N=1->0)
      25  A1    ---   n_Ahigh1    [b] Note on Ahigh1 (1)
  27- 30  F4.1  K.km/s  Alow1     ? Integrated intensity of the low-frequency
                                     fine-structure groups (N=1->0)
  33- 35  F3.1  ---     R1->0     ? Intensity ratio Ahigh1/Alow1 (N=1->0) (3)
  37- 38  I2    mK    e_Tpeak1    ? rms uncertainty on Tpeak1 (N=1->0)
      39  A1    --- n_e_Tpeak1    [a] Note on e_Tpeak1 (2)
  41- 44  F4.2  K       Tpeak2    ? Peak temperature (N=2->1)
  46- 49  F4.1  K.km/s  Ahigh2    ? Integrated intensity of the high-frequency
                                     fine-structure groups (N=2->1)
  51- 54  F4.1  K.km/s  Alow2     ? Integrated intensity of the low-frequency
                                     fine-structure groups (N=2->1)
  57- 59  F3.1  ---     R2->1     ? Intensity ratio Ahigh2/Alow2 (N=2->1) (3)
  61- 63  I3    mK    e_Tpeak2    ? rms uncertainty on Tpeak2 (N=2->1)
--------------------------------------------------------------------------------
Note (1): b: From Bujarrabal & Cernicharo (1994A&A...288..551B)
Note (2): a: Not observed in the 1-0 line
Note (3): The intrinsic intensity ratios, R=A_high_/A_low_, are R(1-0)=2 and
           R(2-1)=1.8. In principle, the observation of several components with
           different intrinsic strengths allows an estimate of the line optical
           depth, and the value of R gives an estimate of the envelope thickness
--------------------------------------------------------------------------------

Acknowledgements: Rafael Bachiller <bachiller@conga.oan.es>
================================================================================
(End)                                         Patricia Bauer [CDS]   12-Aug-1996