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: -------------------------------------------------------------------------------- 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 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
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