The luminous host galaxy, faint supernova and rapid afterglow rebrightening of GRB 100418A

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F68407700%3A21670%2F18%3A00329951" target="_blank" >RIV/68407700:21670/18:00329951 - isvavai.cz</a>

Result on the web

<a href="https://www.aanda.org/articles/aa/pdf/2018/12/aa33636-18.pdf" target="_blank" >https://www.aanda.org/articles/aa/pdf/2018/12/aa33636-18.pdf</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201833636" target="_blank" >10.1051/0004-6361/201833636</a>

Result language

angličtina

Original language name

The luminous host galaxy, faint supernova and rapid afterglow rebrightening of GRB 100418A

Original language description

Long gamma-ray bursts (GRBs) give us the chance to study both their extreme physics and the star-forming galaxies in which they form. GRB 100418A, at a redshift of z = 0.6239, had a bright optical and radio afterglow, and a luminous star-forming host galaxy. This allowed us to study the radiation of the explosion as well as the interstellar medium of the host both in absorption and emission. We collected photometric data from radio to X-ray wavelengths to study the evolution of the afterglow and the contribution of a possible supernova (SN) and three X-shooter spectra obtained during the first 60 h. The light curve shows a very fast optical rebrightening, with an amplitude of similar to 3 magnitudes, starting 2.4 h after the GRB onset. This cannot be explained by a standard external shock model and requires other contributions, such as late central-engine activity. Two weeks after the burst we detect an excess in the light curve consistent with a SN with peak absolute magnitude MV = -18.5 mag, among the faintest GRB-SNe detected to date. The host galaxy shows two components in emission, with velocities differing by 130 km s(-1), but otherwise having similar properties. While some absorption and emission components coincide, the absorbing gas spans much higher velocities, indicating the presence of gas beyond the star-forming regions. The host has a star formation rate of SFR = 12:2M(circle dot)yr(-1), a metallicity of 12 + log(O/H) = 8.55, and a mass of 1.6 x 10(9) M-circle dot. GRB 100418A is a member of a class of afterglow light curves which show a steep rebrightening in the optical during the first day, which cannot be explained by traditional models. Its very faint associated SN shows that GRB-SNe can have a larger dispersion in luminosities than previously seen. Furthermore, we have obtained a complete view of the host of GRB 100418A owing to its spectrum, which contains a remarkable number of both emission and absorption lines.

Czech name

—

Czech description

—

Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

—

OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

<a href="/en/project/EF16_019%2F0000766" target="_blank" >EF16_019/0000766: Engineering applications of microworld physics</a><br>

Continuities

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Publication year

2018

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Volume of the periodical

620

Issue of the periodical within the volume

December

Country of publishing house

FR - FRANCE

Number of pages

25

Pages from-to

190-214

UT code for WoS article

000453501600001

EID of the result in the Scopus database

2-s2.0-85058891423