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Spectral Variations in Early-Type Galaxies as a Function of Mass.

Concannon, Rose, Caldwell

    The Astrophysical Journal
    |June 13, 2000
    PubMed
    Summary

    Spectral analysis of galaxies reveals Balmer lines offer greater dynamic range for stellar population age determination than Mg(2). Lower mass galaxies show more recent star formation.

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    Editor's note.

    Chirality·2001

    Area of Science:

    • Astronomy and Astrophysics
    • Galactic Astronomy
    • Stellar Evolution

    Background:

    • Galactic E/S0 galaxies are crucial for understanding stellar population properties.
    • Spectral indicators like Mg(2), Hbeta, and Hn/Fe are used to probe galaxy evolution.
    • Previous studies have explored the relationship between spectral features and galaxy properties.

    Purpose of the Study:

    • To quantify the strengths of three spectral indicators (Mg(2), Hbeta, Hn/Fe) in a sample of 100 E/S0 galaxies.
    • To determine the intrinsic scatter in these indices as a function of internal velocity dispersion.
    • To assess the relative utility of these indices for determining stellar population age and metallicity.

    Main Methods:

    • Integrated light spectroscopy of 100 field and cluster E/S0 galaxies.
    • Measurement of spectral indices: Mg(2), Hbeta, and Hn/Fe.
    • Linear regression analysis accounting for nonuniform errors to determine intrinsic scatter versus velocity dispersion.

    Main Results:

    • Significantly more intrinsic scatter was found in the Balmer line indices (Hbeta, Hn/Fe) compared to the Mg(2) index.
    • The Balmer indices demonstrate a greater dynamic range for assessing stellar population age.
    • Intrinsic scatter in spectral indices is markedly larger for galaxies with lower velocity dispersion.

    Conclusions:

    • Balmer line indices are superior to Mg(2) for constraining stellar population ages in E/S0 galaxies.
    • Lower mass galaxies (lower velocity dispersion) exhibit evidence of more recent star formation.
    • These findings contribute to understanding the diverse evolutionary pathways of early-type galaxies.

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