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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. 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:
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 --- 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)
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=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
Acknowledgements: Rafael Bachiller
(End) Patricia Bauer [CDS] 12-Aug-1996
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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