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J/ApJ/348/98        LMC AGB stars IRAS fluxes (Reid+ 1990)

Luminous asymptotic giant branch stars in the Large Magellanic Cloud Reid N., Tinney C., Mould J. <Astrophys. J. 348, 98 (1990)> =1990ApJ...348...98R
ADC_Keywords: Magellanic Clouds ; Stars, giant ; Infrared sources Keywords: galaxies: Magellanic clouds - galaxies: stellar content - infrared: sources - stars: evolution - stars: late-type - stars: long-period variables Abstract: We present the results of a search for optically obscured asymptotic giant branch (AGB) stars in the Large Magellanic Cloud (LMC), combining data obtained using the IRAS satellite with near-infrared photographic plate material of a 15deg2 region in the northern LMC. Of the 156 IRAS sources that are detected either in separate cross-scans or in more than one passband, 63 have [12-25] colors consistent with their being either stellar photospheres or circumstellar dust shells. Seventeen of these we identify with bright (Ic<9) foreground stars in our own Galaxy, while a further 17 are associated with red supergiants in the LMC. Of the remaining stars, no more than five are likely to be optically visible AGB stars, while the rest have no obvious optical counterpart. This immediately rules out the presence of sufficient high-luminosity "cocoon" stars to explain the observed deficit of several hundred luminous (Mbol←6) AGB stars between the predictions of standard models of AGB evolution and the observed luminosity function. It remains possible that most of the unidentified sources are dusty AGB stars, evolving through a phase of enhanced mass loss toward becoming planetary nebulae. We infer bolometric magnitudes as low as Mbol~-5 for these sources and suggest that this phase can be triggered at low luminosities, truncating AGB evolution and leading to the observed scarcity of asymptotic giant branch stars with bolometric magnitudes brighter than -6.0mag. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 82 156 TRM selected sources in LMC north
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 3 A3 --- --- [TRM] 5- 7 I3 --- TRM TRM designation (1) 9 I1 h RAh Right ascension (1950) 11- 12 I2 min RAm Right ascension (1950) 14- 17 F4.1 s RAs Right ascension (1950) 19 A1 --- DE- Declination sign 20- 21 I2 deg DEd Declination (1950) 23- 24 I2 arcmin DEm Declination (1950) 26- 27 I2 arcsec DEs Declination (1950) 29 I1 --- Scan [1/3] Information on the scan directions (2) 31- 36 F6.3 Jy S12 ? Flux density at 12 µm (3) 38- 43 F6.3 Jy S25 ? Flux density at 25 µm (3) 45- 50 F6.2 Jy S60 ? Flux density at 60 µm (3) 53- 57 F5.1 Jy S100 ? Flux density at 100 µm (3) 59 A1 --- PSC [*] PSC association, see note (4) 61 A1 --- Rej [YN] Rejection (Y: yes, N: no) 63- 82 A20 --- Com Comments on rejection (6)
Note (1): TRM (1990ApJ...348...98R) selected sources in the LMC north field. Note (2): Information on the scan directions in which each source was detected unambiguously is given: 1 = detected in EW scan 2 = detected in NS scan 3 = detected in both EW and NS scans Note (3): Fluxes listed in this table assume a flux distribution which varies as ν-1 (see Sec. IV). Blank entries in the S12, S25, S60, or S100 columns imply either that no flux was detected at that wavelength, or that the region was so confused that the source extraction algorithm was unable to extract any flux, or that the flux density measurement is not reliable. Note (4): Sources marked with a "*" have been associated positionally with an object in the IRAS PSC (Cat. II/125) Note (6): The comments use the abbreviations: S100 = Source was rejected because it had S100>S60>2*S25. S60 = Source was rejected because it had S60>2*S25. S25≫S12 = Source was rejected because it had S25>4*S12. GC, C, NSO = Source was rejected because it coincided with a globular cluster, open cluster, or clearly nonstellar object on the V or I band Schmidt plates. PN = Source was rejected because it coincided with a planetary nebula (Sanduleak refs). Hα = Source coincided with a knot of Half in the LMC emission-line survey of Davies et al. (1976MmRAS..81...89D) (c), (u) = Source extraction algorithm was unable to produce a meaningful flux estimate at that wavelength, due to either (c) source confusion or (u) unselected source; however, it is clear from the IRAS maps that there is sufficient 60 µm or 100 µm flux present to reject the source. 1 = TRM 147 showed some weak evidence fro 60 µm flux which was not selected by IPAC source extractor. Since this source had a PSC 60µm flux greater than its 25 µm flux, it was therefore rejected. The flux conditions were held to be stronger reasons for source rejection, so although a number of sources listed as being rejected on this basis were also coincident positionally with globular clusters, galaxies, etc., only the flux conditions has been listed here.
History: Prepared via OCR at CDS. References: Davies, Elliott, and Meaburn 1976, Mem. R.A.S. 81, 89 =1976MmRAS..81...89D Ried, Tinney and Mould 1990, ApJ 348, 98 (TRM) =1990ApJ...348...98R Sanduleak 1984 in IAU Symposium 108, p. 231 =1984IAUS..108..231S Sanduleak et al., 1978, PASP 90, 621 =1978PASP...90..621S
(End) Patricia Bauer [CDS] 30-Sep-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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