Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011mnras.417..801m&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 417, Issue 2, pp. 801-811.
Astronomy and Astrophysics
Astronomy
5
Galaxies: Haloes, Quasars: Absorption Lines, Quasars: Emission Lines, Galaxies: Star Formation
Scientific paper
We present an empirical connection between cold (˜104 K) gas in galactic haloes and star formation. Using a sample of more than 8500 Mg II absorbers from Sloan Digital Sky Survey (SDSS) quasar spectra, we report the detection of a 15σ correlation between the rest equivalent width W0 of Mg II absorbers and the associated [O II] luminosity, an estimator of star formation rate.
This correlation has interesting implications: using only observable quantities we show that Mg II absorbers trace a substantial fraction of the global [O II] luminosity density and recover the overall star formation history of the Universe derived from classical emission estimators up to z˜ 2. We then show that the distribution function of Mg II rest equivalent widths, dN/dW0, inherits both its shape and amplitude from the [O II] luminosity function Φ(L). These distributions can be naturally connected, without any free parameter.
Our results imply a high covering factor of cold gas around star-forming galaxies: C≳ 0.5, favouring outflows as the mechanism responsible for Mg II absorption. We then argue that intervening Mg II absorbers and blueshifted Mg II absorption seen in the spectra of star-forming galaxies are essentially the same systems, implying that the observed outflowing gas can reach radii of ˜50 kpc. These results not only shed light on the nature of Mg II absorbers but also provide us with a new probe of star formation, in absorption, i.e. in a way which does not suffer from dust extinction and with a redshift-independent sensitivity. As shown in this analysis, such a tool can be applied in a noise-dominated regime, i.e. using a data set for which emission lines are not detected in individual objects. This is of particular interest for high-redshift studies.
Menard Brice
Nestor Daniel
Quider Anna
Rao Sandhya
Turnshek David
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