J/ApJ/683/321 Metallicities of GRB, DLA, and Lyα galaxies (Fynbo+, 2008)
Reconciling the metallicity distributions of gamma-ray burst, damped Lyα,
and Lyman break galaxies at z∼3.
Fynbo J.P.U., Prochaska J.X., Sommer-Larsen J., Dessauges-Zavadsky M.,
Moller P.
<Astrophys. J., 683, 321-328 (2008)>
=2008ApJ...683..321F 2008ApJ...683..321F
ADC_Keywords: QSOs ; Abundances ; Models
Keywords: gamma rays: bursts - ISM: general
Abstract:
We test the hypothesis that the host galaxies of long-duration
gamma-ray bursts (GRBs) as well as quasar-selected damped Lyα
(DLA) systems are drawn from the population of UV-selected
star-forming, high-z galaxies (generally referred to as Lyman break
galaxies). Specifically, we compare the metallicity distributions of
the GRB and DLA populations against simple models where these galaxies
are drawn randomly from the distribution of star-forming galaxies
according to their star formation rate and HI cross section,
respectively. We find that it is possible to match both observational
distributions assuming very simple and constrained relations between
luminosity, metallicity, and HI sizes. The simple model can be tested
by observing the luminosity distribution of GRB host galaxies and by
measuring the luminosity and impact parameters of DLA-selected
galaxies as a function of metallicity. Our results support the
expectation that GRB and DLA samples, in contrast with
magnitude-limited surveys, provide an almost complete census of z∼3
star-forming galaxies that are not heavily obscured.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 27 315 Results for QSO-DLA
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 F3.1 --- t The Holmberg slope parameter
5- 8 F4.1 --- alpha Parameter α in Schechter LF (1)
10- 13 E4.0 --- Lmin Minimum luminosity in units of L*
15- 19 F5.2 [kpc-1] log(gamma*) Log of the metallicity gradient (2)
21 A1 --- l_PKS Limit flag on PKS
23- 27 F5.3 --- PKS Probability from K-S test analysis
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Note (1): The form of the luminosity function is approximated by a
Schechter function φ(L) ∝ Lα.exp(-L) if L is
the luminosity measured at rest-frame 1700Å (see section 2.1)
Note (2): γ=γ*R*/RHI according to Boissier & Prantzos
(2001MNRAS.325..321B 2001MNRAS.325..321B). We consider γ* values ranging from
-0.01 to -0.07dex/kpc. See section 2.3 for further details.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 26-Nov-2010