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 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. Alow and
Ahigh refer to the integrated intensity of the low-frequency and
high-frequency fine-structure groups. The intrinsic intensity ratios,
R=Ahigh/Alow, 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:
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FileName Lrecl Records Explanations
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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
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Byte-by-byte Description of file: table1
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Bytes Format Units Label Explanations
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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
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Note (1): a: This value corresponds to the intense CO component which is
superimposed on a broader emission plateau.
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Byte-by-byte Description of file: table2
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Bytes Format Units Label Explanations
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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 --- neTpeak1 [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)
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Note (1): b: From Bujarrabal & Cernicharo (1994A&A...288..551B 1994A&A...288..551B)
Note (2): a: Not observed in the 1-0 line
Note (3): The intrinsic intensity ratios, R=Ahigh/Alow, 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
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Acknowledgements: Rafael Bachiller
(End) Patricia Bauer [CDS] 12-Aug-1996