Spectrophotometry of simulated Stellar Populations
Short Name:
J/A+A/392/1
Date:
21 Oct 2021
Publisher:
CDS
Description:
A new set of evolutionary synthesis spectra are presented for Simple Stellar Populations (SSPs) covering ranges in metallicity from 0.02<=Z/Z_{sun}_<=2.5 and ages from 4*10^6^yr<=t<=16Gyr. They are based on the most recent isochrones from the Padova group that extend earlier models by the inclusion of the thermal pulsing AGB phase for stars in the mass range 2M_{sun}_<=m<=7M_{sun}_ in accordance with the fuel consumption theorem. We show that with respect to earlier models, inclusion of the TP-AGB phase leads to significant changes in the (V-I) and (V-K) colors of SSPs in the age range from 10^8^ to >~10^9^yr. Using model atmosphere spectra from Lejeune et al. (1997, Cat. <J/A+AS/125/229>, 1998, Cat. <J/A+AS/130/65>), we calculate the spectral evolution of single burst populations of various metallicities covering the wavelength range from 90{AA} through 160{mu}m. Isochrone spectra are convolved with filter response functions to describe the time evolution of luminosities and colors in Johnson, Thuan & Gunn, Koo, HST, Washington and Stroemgren filters. The models and their results are not only intended for use in the interpretation of star clusters but also for combination with any kind of dynamical galaxy formation and/or evolution model that contains a star formation criterion. Moreover, the evolution of these single burst single metallicity stellar populations is readily folded with any kind of star formation -- and eventually chemical enrichment -- history to describe the evolutionary spectral synthesis of composite stellar populations like galaxies of any type with continuous or discontinuous star formation. For these latter purposes we also present the time evolution of ejection rates for gas and metals for two different Initial Mass Functions (IMFs) as well as cosmological and evolutionary corrections for all the filters as a function of redshift for 0<=z<=5 and two different cosmologies.
We have analyzed the optical spectra of 67 symbiotic stars and objects suspected of being symbiotic, and found 18 new symbiotic systems. This is the largest homogeneous set of optical spectrophotometric data for symbiotic binaries ever studied. We have derived the reddenings and distances for all systems, estimated the IR classes (S and D) for the new systems, and determined the location of the hot components in the Hertzsprung-Russell diagram.
Spectral energy distributions were photoelectrically measured from 320 to 860 nm with a resolution of 1 nm in equidistant steps of 1 nm for 60 bright southern and equatorial stars of intermediate and late spectral types for all luminosity classes. Flux curves for individual stars are plotted with a resolution of 1 nm and tabulated in steps of 5 nm. Typical internal mean errors of fluxes measured in different nights are less than 0.02mag in the spectral range from 400 nm to 860 nm, and rise to a maximum of about 0.05mag for wavelengths below 400 nm.
The present catalogue contains 2238 energy distribution data for 1588 objects in the spectral region 320-817nm by steps of 2.5nm. It is based on the following spectrophotometric catalogues: Kharitonov et al. (1), Alekseev et al. (the "Chilean Catalogue") (2), Willstrop (3), Glushneva et al. (the "Moscow Catalogue") (4,5,6), Burnashev's observations of stars obtained at the Crimean Astrophysical Observatory. Comparison of these catalogues and their reductions to the uniform spectrophotometric system has been carried out by Burnashev (7). The catalogue is divided in three parts: 1) Part 1 contains the data published in the catalogues by Kharitonov (1), Glushneva (4,5,6) and Willstrop(3). 2) Part 2 contains the data (and their r.m.s) of the "Chilean Catalogue" (Alekseev et al.(2)) and Burnashev's observations of some stars, obtained at the Crimean Astrophysical Observatory during 1974-1982. The observations of some variables, obtained in Chile, Are also presented. This part contains also tables of the Hydrogen continuum radiation for several temperatures (5000; 10000;15000;20000;40000;80000 K) according to Boyarchuk et al.(9), which may be useful for the analysis of the spectra of some variables. 3) Part 3 contains data of Parts 1 and 2 reduced to the uniform spectrophotometric system of the "Chilean Catalogue" in the range 320-735nm. The absolute calibration based on energy distribution of the primary standard Alpha Lyrae, according to Kharitonov (10), being the mean of the absolute calibrations of Kharitonov et al.(11), Hayes and Latham (12), Tug et al.(13).
New spectrophotometric data for 3 galactic and 23 LMC F to G supergiants are presented. The wavelength range of the spectra is 3400 to 6400{AA}, the resolution about 10{AA}. The mean transformational error of the fluxes is 0.03mag. The S/N ratio is about 100 and 30 for galactic and LMC stars, respectively. Details about the reduction one may found in Oestreicher & Schmidt-Kaler (1998MNRAS.299..625O) and Malyuto et al. (1997MNRAS.286..500M). The fluxes are given in magnitudes according to the system of Hayes & Latham (1975ApJ...197..593H). For each star an ASCII file is given with the name of the first identifier. In the first column the wavelength, in the second column the flux is given.
We present echelle spectrophotometry of the Galactic H II region S311. The data have been taken with the Very Large Telescope Ultraviolet-Visual Echelle Spectrograph in the 3100-10400{AA} range. We have measured the intensities of 263 emission lines; 178 are permitted lines of H^0^, D^0^ (deuterium), He^0^, C^0^, C^+^, N^0^, N^+^, O^0^, O^+^, S^+^, Si^0^, Si^+^, Ar^0^ and Fe^0^; some of them are produced by recombination and others mainly by fluorescence.
We report new spectroscopic and photometric observations of the parent stars of the recently discovered transiting planets TrES-3 and TrES-4. A detailed abundance analysis based on high-resolution spectra yields [Fe/H]=-0.19+/-0.08, Teff=5650+/-75K, and logg=4.4+/-0.1 for TrES-3, and [Fe/H]=+0.14+/-0.09, Teff=6200+/-75K, and logg=4.0+/-0.1 for TrES-4. The accuracy of the effective temperatures is supported by a number of independent consistency checks. The spectroscopic orbital solution for TrES-3 is improved with our new radial velocity measurements of that system, as are the light-curve parameters for both systems based on newly acquired photometry for TrES-3 and a reanalysis of existing photometry for TrES-4. With these revised stellar parameters, we obtain improved values for the planetary masses and radii. We find M_p_=1.910^+0.075^_-0.080_M_Jup_, R_p_=1.336^+0.031^_-0.036_R_Jup_ for TrES-3, and M_p_=0.925+/-0.082M_Jup_, R_p_=1.783^+0.093^_-0.086_R_Jup_ for TrES-4. We confirm TrES-4 as the planet with the largest radius among the currently known transiting hot Jupiters.
The results of visual and near-infrared spectrophotometric observations for 77 variable stars obtained during 1971-1991 in Chile, Armenia and Bolivia. The quasi-monochromatic extra-atmospheric fluxes from the stars are given in absolute energy units (W/m^2^/m) at all wavelengths of the spectral range at 2.5 nm intervals.
Drift-scan mode (3600-6800{AA}) spectra with 500<R<1000 resolution are presented for 333 galaxies members to nearby clusters, covering the whole Hubble sequence. The majority (225) were obtained for galaxies in the Virgo cluster where a completeness of 36%, if all Hubble types are considered, and of 5 %, restricting to late-types, was reached at mp<=16. Our data can be therefore considered representative of the integrated spectral properties of giant and dwarf galaxies in this cluster. Intensities and equivalent widths (EWs) are derived for the principal lines, both in emission and in absorption. Deblending of the underlying absorption from emission was achieved in most cases.
The catalog contains spectrophotometry at approximately 10-Angstrom resolution for 173 southern Wolf-Rayet stars. All observations were made at the Cerro Tololo Inter-American Observatory between November 1981 and February 1985 with SIT-vidicon detector. The catalog includes synthetic photometry, and fluxes in the range 3400-7300 Angstroms for most known Wolf-Rayet stars in the Large Magellanic Cloud and in the range 3400-4700 Angstroms for all known Wolf-Rayet stars in the Small Magellanic Cloud.