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J/A+A/488/675  Infrared photometry of mass-losing AGB stars  (Guandalini+, 2008)

Infrared photometry and evolution of mass-losing AGB stars. II. Luminosity and colors of MS and S stars. Guandalini R., Busso M. <Astron. Astrophys. 488, 675 (2008)> =2008A&A...488..675G
ADC_Keywords: Stars, giant ; Stars, S ; Photometry, infrared Keywords: stars: fundamental parameters - stars: AGB and post-AGB - stars: evolution - infrared: stars - stars: variables: general Abstract: Asymptotic giant branch (AGB) phases mark the end of the evolution for low- and intermediate-mass stars. Our understanding of the mechanisms through which they eject the envelope and our assessment of their contribution to the mass return to the interstellar medium and to the chemical evolution of Galaxies are hampered by poor knowledge of their luminosities and mass loss rates, both for C-rich and for O-rich sources. We plan to establish criteria permitting a more quantitative determination of luminosities (and subsequently of mass loss rates) for the various types of AGB stars on the basis of infrared fluxes. In this paper, in particular, we concentrate on O-rich and s-element-rich MS, S stars and include a small sample of SC stars. We reanalyze the absolute bolometric magnitudes and colors of MS, S, SC stars on the basis of a sample of intrinsic (single) and extrinsic (binary) long period variables. We derive bolometric corrections as a function of near- and mid-infrared colors, adopting as references a group of stars for which the spectral energy distribution could be reconstructed in detail over a large wavelength range. We determine the absolute HR diagrams, and compare luminosities and colors of S-type giants with those, previously derived, of C-rich AGB stars. Luminosity estimates are also verified on the basis of existing period-luminosity relations valid for O-rich Miras. S star bolometric luminosities are almost indistinguishable from those of C-rich AGB stars. On the contrary, their circumstellar envelopes are thinner and less opaque. Despite this last property the IR wavelengths remain dominant, with the bluest stars having their maximum emission in the H or K(short) bands. Near-to-mid infrared color differences are in any case smaller than for C stars. Based on period-luminosity relations for O-rich Miras and on Magnitude-color relations for the same variables we show how approximate distances (hence intrinsic parameters) for sources of so far unknown parallax can be inferred. We argue that most of the sources have a rather small mass (<2M); dredge-up might then be not effective enough to let the C/O ratio exceed unity. Description: Tables 11 and 12 present the data of the "Sub-sample D" discussed in the paper. In particular, Table 11 shows for each source the different denominations, the coordinates, spectral type, variability type and period. Instead, photometric fluxes in near- and mid-infrared, apparent bolometric magnitudes and an indication if the star is Intrinsic or Extrinsic are reported in Table 12. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table11.dat 88 530 Sample D - First part table12.dat 94 530 Sample D - Second part
See also: III/168 : General Catalog of S Stars, second edition (Stephenson 1984) Byte-by-byte Description of file: table11.dat
Bytes Format Units Label Explanations
1- 10 A10 --- IRAS IRAS designation 12- 20 A9 --- Name Other designation 23- 30 A8 --- CSS Stephenson designation, Cat. III/168 33- 34 I2 h RAh ICRS right ascension (ep=2000 eq=2000) 36- 37 I2 min RAm ICRS right ascension (ep=2000 eq=2000) 39- 45 F7.4 s RAs ICRS right ascension (ep=2000 eq=2000) 47 A1 --- DE- ICRS declination sign (ep=2000 eq=2000) 48- 49 I2 deg DEd ICRS declination (ep=2000 eq=2000) 51- 52 I2 arcmin DEm ICRS declination (ep=2000 eq=2000) 54- 59 F6.3 arcsec DEs ICRS declination (ep=2000 eq=2000) 61- 77 A17 --- SpType Spectral Type from GCVS 79- 81 A3 --- Var Variability Type from GCVS 83- 88 F6.1 d Per ? Period (from GCVS)
Byte-by-byte Description of file: table12.dat
Bytes Format Units Label Explanations
1- 9 A9 --- Name Designation of the source 11- 17 F7.3 Jy FJ ? Flux in J band 19- 25 F7.2 Jy FH ? Flux in H band 27- 33 F7.2 Jy FK ? Flux in K band 35- 40 F6.2 Jy F8.8 ? Flux in 8.8um band 42- 46 F5.1 Jy F9.8 ? Flux in 9.8um band 48- 52 F5.1 Jy F11.7 ? Flux in 11.7um band 54- 59 F6.2 Jy F12.5 ? Flux in 12.5um band 61- 66 F6.2 Jy FD ? Flux in D (14.65um) MSX band 68- 73 F6.2 Jy FE ? Flux in E (21.34um) MSX band 75- 82 A8 --- refIR Origin of the Mid-IR data (MSX or IRAS-LRS) 84- 88 F5.2 mag mbol ? Apparent bolometric magnitude 90- 94 A5 --- I/E Intrinsic (I) and/or Extrinsic (E) source
Acknowledgements: Roald Guandalini, guandalini(at)fisica.unipg.it References: Guandalini et al., Paper I 2006A&A...445.1069G
(End) Patricia Vannier [CDS] 15-Jul-2008
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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