Article

The host of GRB 030323 at $\mathsf{\textit{z}=3.372}$: A very high column density DLA system with a low metallicity

P. M. VreeswijkEuropean Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Santiago 19, ChileS. L. EllisonEuropean Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Santiago 19, ChileC. LedouxEuropean Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Santiago 19, ChileR. A. M. J. WijersAstronomical Institute “Anton Pannekoek”, University of Amsterdam & Center for High Energy Astrophysics, Kruislaan 403, 1098 SJ Amsterdam, The NetherlandsJ. P. U. FynboDepartment of Physics and Astronomy, Århus University, Ny Munkegade, 8000 Århus C, DenmarkP. MøllerEuropean Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, GermanyA. HendenUniversities Space Research Association / US Naval Observatory Flagstaff Station, PO Box 1149, Flagstaff AZ 86002-1149, USAJ. HjorthG. MasiPhysics Department, University of Rome “Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, ItalyE. RolAstronomical Institute “Anton Pannekoek”, University of Amsterdam & Center for High Energy Astrophysics, Kruislaan 403, 1098 SJ Amsterdam, The NetherlandsB. L. JensenN. TanvirDepartment of Physical Sciences, University of Hertfordshire, College Lane, Hatfield, Herts AL10 9AB, UKA. LevanDepartment of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH, UKJ. M. Castro CerónSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218-2463, USAJ. GorosabelInstituto de Astrofísica de Andalucía (IAA-CSIC), Apartado de Correos, 3004, 18080 Granada, SpainA. J. Castro-TiradoInstituto de Astrofísica de Andalucía (IAA-CSIC), Apartado de Correos, 3004, 18080 Granada, SpainA. S. FruchterSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218-2463, USAC. KouveliotouNSSTC, SD-50, 320 Sparkman Dr., Huntsville, AL 35805, USAI. BurudSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218-2463, USAJ. RhoadsSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218-2463, USAN. MasettiIstituto di Astrofisica Spaziale e Fisica Cosmica – Sezione di Bologna, CNR, via Gobetti 101, 40129 Bologna, ItalyE. PalazziIstituto di Astrofisica Spaziale e Fisica Cosmica – Sezione di Bologna, CNR, via Gobetti 101, 40129 Bologna, ItalyE. PianINAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, 34131 Trieste, ItalyH. PedersenL. KaperAstronomical Institute “Anton Pannekoek”, University of Amsterdam & Center for High Energy Astrophysics, Kruislaan 403, 1098 SJ Amsterdam, The NetherlandsA. GilmoreDepartment of Physics and Astronomy, University of Canterbury, Christchurch, New ZealandP. KilmartinDepartment of Physics and Astronomy, University of Canterbury, Christchurch, New ZealandJ. V. BuckleJoint Astronomy Centre, 660 N, A'ohoku Place, Hilo, Hawaii, HI 96720, USAM. S. SeigarJoint Astronomy Centre, 660 N, A'ohoku Place, Hilo, Hawaii, HI 96720, USAD. H. HartmannDepartment of Physics & Astronomy, Clemson University, Clemson, SC 29634-0978, USAK. LindsayDepartment of Physics & Astronomy, Clemson University, Clemson, SC 29634-0978, USAE. P. J. van den HeuvelAstronomical Institute “Anton Pannekoek”, University of Amsterdam & Center for High Energy Astrophysics, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands

2004en

ABI

Abstract

We present photometry and spectroscopy of the afterglow of GRB 030323. VLT spectra of the afterglow show damped Lyα (DLA) absorption and low- and high-ionization lines at a redshift . The inferred neutral hydrogen column density, , is larger than any (GRB- or QSO-) DLA column density inferred directly from Lyα in absorption. From the afterglow photometry, we derive a conservative upper limit to the host-galaxy extinction: mag. The iron abundance is , while the metallicity of the gas as measured from sulphur is . We derive an upper limit on the H2 molecular fraction of . In the Lyα trough, a Lyα emission line is detected, which corresponds to a star-formation rate (not corrected for dust extinction) of roughly 1 M yr-1. All these results are consistent with the host galaxy of GRB 030323 consisting of a low metallicity gas with a low dust content. We detect fine-structure lines of silicon, *, which have never been clearly detected in QSO-DLAs; this suggests that these lines are produced in the vicinity of the GRB explosion site. Under the assumption that these fine-structure levels are populated by particle collisions, we estimate the volume density to be cm-3. HST/ACS imaging 4 months after the burst shows an extended mag object at a distance of 014 (1 kpc) from the early afterglow location, which presumably is the host galaxy of GRB 030323.

Identifiers

DOI: 10.1051/0004-6361:20040086

Citations and references

Cited by 30 references

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