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J/PASP/117/199        IRTS carbon stars                       (Le Bertre+, 2005)

Carbon stars in the Infrared Telescope in Space Survey. Le Bertre T., Tanaka M., Yamamura I., Murakami H., MacConnell D.J. <Publ. Astron. Soc. Pac., 117, 199-206 (2005)> =2005PASP..117..199L
ADC_Keywords: Stars, carbon ; Photometry, infrared Abstract: We have identified 139 cool carbon stars in the near-infrared spectrophotometric survey of the Infrared Telescope in Space (IRTS) from the conspicuous presence of molecular absorption bands at 1.8, 3.1, and 3.8µm. Among them, 14 are new bright (K∼4.0-7.0) Carbon stars. We find a trend relating the 3.1µm band strength to the (K-L') color index, which is known to correlate with mass-loss rate. This could be an effect of a relation between the depth of the 3.1µm feature and the degree of development of the extended stellar atmosphere where dust starts to form. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 69 143 IRTS carbon stars
See also: III/227 : General Cat. of galactic Carbon stars, 3d Ed. (Alksnis+ 2001) J/A+A/227/82 : JHKLM photometry of 'IRAS-discovered' stars (Epchtein+, 1990) J/A+A/324/1059 : C-rich stars IR and UBVRI photometry (Le Bertre 1997) J/A+A/334/609 : Carbon stars IR photometry (Guglielmo+ 1998) J/A+A/376/997 : Galactic mass-losing AGB stars (Le Bertre+, 2001) J/A+A/369/178 : Effective temperatures of carbon-rich stars (Bergeat+, 2001) J/A+AS/99/31 : Identification of C stars in IRAS (Guglielmo+ 1993) J/PASP/115/351 : Infrared Southern Cool Carbon Stars (MacConnell, 2003) J/A+A/403/943 : Galactic mass-losing AGB stars. II. (Le Bertre+, 2003) J/ApJS/112/557 : Classification of IRAS Sources (Kwok+ 1997) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 10 A10 --- NIRS NIRS (Near-Infrared Spectrometer) name ([LTY2003] NIRS HHMMm+DDMM in Simbad) 12 A1 --- m_NIRS [NS] Multiplicity flag on NIRS 14- 19 F6.2 deg GLON Galactic longitude 21- 26 F6.2 deg GLAT Galactic latitude 28- 31 F4.2 mag Kmag K band magnitude 33- 36 F4.2 mag K-L' K-L' color index 38- 41 F4.2 --- 3.1um 3.1µm index (1) 43- 52 A10 --- IRAS IRAS name 54- 57 A4 --- --- [CGCS] 59- 62 I4 --- CGCS ? CGCS number (Cat. III/227) 64- 69 A6 --- Com Comments (2)
Note (1): To identify carbon stars in the NIRS PSC (Near-Infrared Spectrometer Point Source Catalog), we use the 3.1µm index defined in Paper II (2003, Cat. J/A+A/403/943). This index gives the depth of the band (at 3.1µm) relative to the continuum (taken at 2.9 and 3.3µm); the maximum depth is obtained for an index value of 0.0, whereas a value 0.5 indicates a flat spectrum. Note (2): Comments, defined as follows: a = A 30 minute exposure plate obtained by D.J. MacConnell shows nothing at this position. The R DSS2 plate has a faint star 3" southeast of the IRAS position. b = A 30 minute exposure plate obtained by D.J. MacConnell shows a faint continuum (short and red) that has a general character of a carbon star but is too underexposed to be certain, although it has been tentatively identified as a C star by MacConnell (1979A&AS...38..335M). The R DSS2 plate has a bright star at the IRAS position. c = A 60 minute exposure plate obtained by D.J. MacConnell shows nothing at the IRAS position. d = The 2.9-3.5m spectrum was also presented by Groenewegen et al. (1994A&A...287..163G). e = A 60 minute exposure plate obtained by D.J. MacConnell has a very red, non-C star east of the IRAS position, which probably corresponds to the bright star 32" away at position angle 66° on the DDS2 I plate. f = LRS spectrum C (11µm SiC emission; Kwok et al. 1997, Cat. J/ApJS/112/557); tentative identification as a C star by Chen & Chen (2003AJ....125.2215C) g = The 3.1µm index is larger than 0.45 (2003, Cat. J/A+A/403/943). h = The 3.1µm index is larger than 0.45 (M. Tanaka et al. 2005, in preparation).
History: From electronic version of the journal References: Le Bertre et al., Paper I 2001A&A...376..997L, Cat. J/A+A/376/997 Le Bertre et al., Paper II 2003A&A...403..943L, Cat. J/A+A/403/943
(End) Marianne Brouty [CDS] 03-Mar-2006
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