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J/A+A/311/361      Evolution models of elliptical galaxies. II. (Tantalo+, 1996)
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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)
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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 Mg_2_ index and (1550-V), the mass to blue luminosity ratio M/L_B_
    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
    M_g_^k^(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:
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  FileName  Lrecl  Records   Explanations
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ReadMe         80        .   This file
table2        119      281   Integrated colors of single stellar populations
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See also:
   J/A+A/335/823 : Evolution models of elliptical galaxies. III. (Tantalo+ 1998)

Byte-by-byte Description of file: table2
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   Bytes Format   Units   Label     Explanations
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   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
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References:
  Burstein D. et al. 1988, ApJ 328, 440  =1988ApJ...328..440B
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(End)                                         Patricia Bauer [CDS]   04-Apr-1996