Rapid response mode observations of GRB 160203A: Looking for fine-structure line variability at z = 3.52
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F24%3A00599422" target="_blank" >RIV/67985815:_____/24:00599422 - isvavai.cz</a>
Result on the web
<a href="https://hdl.handle.net/11104/0356915" target="_blank" >https://hdl.handle.net/11104/0356915</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1051/0004-6361/202244098" target="_blank" >10.1051/0004-6361/202244098</a>
Alternative languages
Result language
angličtina
Original language name
Rapid response mode observations of GRB 160203A: Looking for fine-structure line variability at z = 3.52
Original language description
Context. Gamma-ray bursts are the most energetic known explosions. Although they fade rapidly, they give us the opportunity to measure redshift and important properties of their host galaxies. We report the photometric and spectroscopic study of the Swift GRB 160203A at z = 3.518, and its host galaxy. Fine-structure absorption lines, detected in the afterglow at different epochs, allow us to investigate variability due to the strong fading background source. Aims. We obtained two optical to near-infrared spectra of the GRB afterglow with X-shooter on ESO/VLT, 18 minutes and 5.7 hours after the burst, allowing us to investigate temporal changes of fine-structure absorption lines. Methods. We measured H I column density log N(HI/cm(-2)) = 21.75 +/- 0.10, and several heavy-element ions along the GRB sightline in the host galaxy, among which Si II, Al II, Al III, C II, Ni II, Si IV, C IV, Zn II and Fe II, and Fe II* and Si II* fine-structure transitions from energetic levels excited by the afterglow, at the common redshift z = 3.518. We measured [M/H](TOT) =0.78 +/- 0.13 and a [Zn/Fe](FIT) = 0.69 +/- 0.15, representing the total (dust corrected) metallicity and dust depletion, respectively. We detected additional intervening systems along the line of sight at z = 1.03, z = 1.26, z = 1.98, z = 1.99, z = 2.20, and z = 2.83. We could not measure significant variability in the strength of the fine-structure lines throughout all the observations and determined an upper limit for the GRB distance from the absorber of d < 300 pc, adopting the canonical UV pumping scenario. However, we note that the quality of our data is not sufficient to conclusively rule out collisions as an alternative mechanism. Results. GRB 160203A belongs to a growing sample of GRBs with medium resolution spectroscopy, provided by the Swift/X-shooter legacy programme, which enables a detailed investigation of the interstellar medium in high-redshift GRB host galaxies. In particular, this host galaxy shows relatively high metal enrichment and dust depletion already in place when the universe was only 1.8 Gyr old.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
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Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2024
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Astronomy & Astrophysics
ISSN
0004-6361
e-ISSN
1432-0746
Volume of the periodical
690
Issue of the periodical within the volume
Oct.
Country of publishing house
FR - FRANCE
Number of pages
15
Pages from-to
A35
UT code for WoS article
001322370900003
EID of the result in the Scopus database
2-s2.0-85205471522