========================================================================== VI/125 Theoretical spectra of red giants and supergiants (Lancon+, 2007) The following files can be converted to FITS (extension .fit .fgz or .fiZ) table1.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=VI/125 ==========================================================================
drwxr-xr-x 119 cats archive 4096 May 12 09:53 [Up] drwxr-xr-x 5 cats archive 4096 May 12 09:52 [TAR file] -rw-r--r-- 1 cats archive 461 Aug 18 2007 .message -r--r--r-- 1 cats archive 5013 Aug 18 2007 ReadMe drwxr-xr-x 2 cats archive 12288 Aug 14 2007 m15rsg drwxr-xr-x 2 cats archive 12288 Feb 28 2007 m15solar drwxr-xr-x 2 cats archive 4096 Feb 28 2007 m1solar -r--r--r-- 1 cats archive 22282 Mar 6 2007 table1.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : VI/125 Theoretical spectra of red giants and supergiants (Lancon+, 2007) ================================================================================ Near-IR spectra of red supergiants and giants. I- Models with solar and with mixing-induced surface abundance ratios. Lancon A., Hauschildt P.H., Ladjal D., Mouhcine M. <Astron. Astrophys. 468, 205 (2007)> =2007A&A...468..205L ================================================================================ ADC_Keywords: Stars, giant ; Stars, supergiant ; Spectra, infrared ; Models Keywords: stars: fundamental parameters - stars: abundances - infrared: stars - stars: atmospheres Abstract: It remains difficult to interpret the near-IR emission of young stellar populations. One main reason is our incomplete understanding of the spectra of luminous red stars. This work provides a grid of theoretical spectra of red giant (RG) and red supergiant (RSG) stars, that extends through optical and near-IR wavelengths. For the first time, models are also provided with modified surface abundances of C, N and O, as a step towards accounting for the changes that occur due to convective dredge-up in red supergiants or may occur at earlier evolutionary stages in the case of rotation. The aims are (i) to assess how well current models reproduce observed spectra, in particular in the near-IR; (ii) to quantify the effects of the abundance changes on the spectra; and (iii) to determine how these changes affect estimates of fundamental stellar parameters. Description: Each FITS file in this directory contains a theoretical stellar spectrum. The spherical model atmospheres and the synthetic spectra were computed with PHOENIX version 13.11.00B as described in the article, with an initial wavelength sampling step of 0.01nm in the wavelength range of interest [510nm-2490nm]. The spectra made available here have been smoothed with a Gaussian with a full width at half maximum of 0.2nm. They are resampled with a wavelength step of 0.025nm.