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J/A+A/311/361      Evolution models of elliptical galaxies. II. (Tantalo+, 1996)

Spectro-photometric evolution of elliptical galaxies. II. Models with infall. Tantalo R., Chiosi C., Bressan A., Fagotto F. <Astron. Astrophys. 311, 361 (1996)> =1996A&A...311..361T (SIMBAD/NED BibCode)
ADC_Keywords: Models, evolutionary ; Photometry, UBVRIJKLMNH Keywords: galaxies: ellipticals - galaxies: evolution - galaxies: stellar content Abstract: In this paper we present new chemo-spectro-photometric models of elliptical galaxies in which infall of primordial gas is allowed to occur. They aim to simulate the collapse of a galaxy made of two components, i.e. luminous material and dark matter. The mass of the dark component is assumed to be constant in time, whereas that of the luminous material is supposed to accrete at a suitable rate. They also include the effect of galactic winds powered by supernova explosions and stellar winds from massive, early-type stars. The models are constrained to match a number of properties of elliptical galaxies, i.e. the slope and mean colours of the colour-magnitude relation (CMR), V versus (V-K), the UV excess as measured by the colour (1550-V) together with the overall shape of the integrated spectral energy distribution (ISED) in the ultraviolet, the relation between the Mg2 index and (1550-V), the mass to blue luminosity ratio M/LB as a function of the B luminosity, and finally the broad-band colours (U-B), (B-V), (V-I), (V-K), etc. The CMR is interpreted as a mass-metallicity sequence of old, nearly coeval objects, whose mean age is 15Gyr. Assuming the law of star formation to be proportional to Mgk(t) with k=1, the rate of star formation as function of time starts small, grows to a maximum, and then declines thus easily avoiding the excess of metal-poor stars found by BCF with the closed-box scheme (the analog of the G-Dwarf Problem in the solar vicinity). Owing to their stellar content, infall models can easily reproduce all the basic data of the galaxies under examination. As far as the UV excess is concerned, the same sources proposed by BCF are found to hold also with the infall scheme. H-HB and AGB manque stars of high metallicity play the dominant role, and provide a robust explanation of the correlation between the (1550-V) colour and the luminosity, mass and metallicity of the galaxies. Furthermore, these models confirm the potential of the (1550-V) colour as an age indicator in cosmology as already suggested by BCF. In the rest frame of a massive and metal-rich elliptical galaxy, this colour suffers from one major variation: at the onset of the so-called H-HB and AGB-manque stars (age about 5.6Gyr). This transition occurs at reasonably small red-shifts and therefore could be detected with the present-day instrumentation. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2 119 281 Integrated colors of single stellar populations
See also: J/A+A/335/823 : Evolution models of elliptical galaxies. III. (Tantalo+ 1998) Byte-by-byte Description of file: table2
Bytes Format Units Label Explanations
1- 6 F6.4 --- Z Metallicity 9- 15 F7.4 Gyr Age Age 18- 23 F6.3 mag Mv Integrated absolute visual magnitude 26- 31 F6.3 mag Mbol Integrated absolute bolometric magnitude 34- 39 F6.3 mag BC Bolometric correction 42- 47 F6.3 mag U-B U-B integrated color 50- 55 F6.3 mag B-V B-V integrated color 58- 63 F6.3 mag V-R V-R integrated color 66- 71 F6.3 mag R-I R-I integrated color 74- 79 F6.3 mag V-J V-J integrated color 82- 87 F6.3 mag V-K V-K integrated color 90- 95 F6.3 mag V-L V-L integrated color 98-103 F6.3 mag V-M V-M integrated color 106-111 F6.3 mag V-N V-N integrated color 114-119 F6.3 mag 1550-V 1550-V integrated color defined as in Burstein et al. 1988
Reference: Burstein D. et al. 1988, ApJ 328, 440 =1988ApJ...328..440B
(End) Patricia Bauer [CDS] 04-Apr-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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