Ly-alpha emitters: blue dwarfs or supermassive ULIRGs? Evidence for a transition with redshift

Details Ly-alpha emitters: blue dwarfs or supermassive ULIRGs? Evidence for a transition with redshift Ly-alpha emitters: blue dwarfs or supermassive ULIRGs? Evidence for a transition with redshift

2009-11-03

arxiv.org/abs/0911.0419v2

Astronomy and Astrophysics, Volume 508, Issue 2, 2009, pp.L21-L25

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

5 pages, 5 figures, 1 table, published in A&A, 508, L21

Scientific paper

10.1051/0004-6361/200913407

The traditional view that Ly-alpha emission and dust should be mutually exclusive has been questioned more and more often; most notably, the observations of Ly-alpha emission from ULIRGs seem to counter this view. In this paper we seek to address the reverse question. How large a fraction of Ly-alpha selected galaxies are ULIRGs? Using two samples of 24/25 Ly-alpha emitting galaxies at z = 0.3/2.3, we perform this test, including results at z = 3.1, and find that, whereas the ULIRG fraction at z = 3.1 is very small, it systematically increases towards lower redshifts. There is a hint that this evolution may be quite sudden and that it happens around a redshift of z ~ 2.5. After measuring the infrared luminosities of the Ly-alpha emitters, we find that they are in the normal to ULIRG range in the lower redshift sample, while the higher redshift galaxies all have luminosities in the ULIRG category. The Ly-alpha escape fractions for these infrared bright galaxies are in the range 1-100 % in the z = 0.3 galaxies, but are very low in the z = 2.3 galaxies, 0.4 % on average. The unobscured star formation rates are very high, ranging from 500 to more than 5000 M_sun/yr, and the dust attenuation derived are in the range 0.0 < A_V < 3.5.

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