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The Luminous Host Galaxy, Faint Supernova and Rapid Afterglow Rebrightening of GRB 100418A

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The Luminous Host Galaxy, Faint Supernova and Rapid Afterglow Rebrightening of GRB 100418A LJMU Research Online Postigo, ADU, Thone, CC, Bensch, K, van der Horst, AJ, Kann, DA, Cano, Z, Izzo, L, Goldoni, P, Martin, S, Filgas, R, Schady, P, Gorosabel, J, Bikmaev, I, Bremer, M, Burenin, R, Castro-Tirado, AJ, Covino, S, Fynbo, JPU, Garcia- Appadoo, D, de Gregorio-Monsalvo, I, Jelinek, M, Khamitov, I, Kamble, A, Kouveliotou, C, Kruehler, T, Leloudas, G, Melnikov, S, Nardini, M, Perley, DA, Petitpas, G, Pooley, G, Rau, A, Rol, E, Sanchez-Ramirez, R, Starling, RLC, Tanvir, NR, Wiersema, K, Wijers, RAMJ and Zafar, T The luminous host galaxy, faint supernova and rapid afterglow rebrightening of GRB 100418A http://researchonline.ljmu.ac.uk/id/eprint/10415/ Article Citation (please note it is advisable to refer to the publisher’s version if you intend to cite from this work) Postigo, ADU, Thone, CC, Bensch, K, van der Horst, AJ, Kann, DA, Cano, Z, Izzo, L, Goldoni, P, Martin, S, Filgas, R, Schady, P, Gorosabel, J, Bikmaev, I, Bremer, M, Burenin, R, Castro-Tirado, AJ, Covino, S, Fynbo, JPU, Garcia- Appadoo, D, de Gregorio-Monsalvo, I, Jelinek, M, Khamitov, I, Kamble, A, LJMU has developed LJMU Research Online for users to access the research output of the University more effectively. Copyright © and Moral Rights for the papers on this site are retained by the individual authors and/or other copyright owners. Users may download and/or print one copy of any article(s) in LJMU Research Online to facilitate their private study or for non-commercial research. You may not engage in further distribution of the material or use it for any profit-making activities or any commercial gain. The version presented here may differ from the published version or from the version of the record. Please see the repository URL above for details on accessing the published version and note that access may require a subscription. http://researchonline.ljmu.ac.uk/ For more information please contact [email protected] http://researchonline.ljmu.ac.uk/ A&A 620, A190 (2018) Astronomy https://doi.org/10.1051/0004-6361/201833636 & c ESO 2018 Astrophysics The luminous host galaxy, faint supernova and rapid afterglow rebrightening of GRB 100418A? A. de Ugarte Postigo1,2, C. C. Thöne1, K. Bensch1, A. J. van der Horst3,4, D. A. Kann1, Z. Cano1, L. Izzo1, P. Goldoni5, S. Martín6,7, R. Filgas8, P. Schady9, J. Gorosabel10,11,1, y, I. Bikmaev12,13, M. Bremer14, R. Burenin15,16, A. J. Castro-Tirado1, S. Covino17, J. P. U. Fynbo2,18, D. Garcia-Appadoo6, I. de Gregorio-Monsalvo6,7, M. Jelínek19, I. Khamitov20,12, A. Kamble21, C. Kouveliotou3,4, T. Krühler9, G. Leloudas2, S. Melnikov12,13, M. Nardini22, D. A. Perley23, G. Petitpas24, G. Pooley25, A. Rau9, E. Rol26,27, R. Sánchez-Ramírez28,1, R. L. C. Starling29, N. R. Tanvir29, K. Wiersema30, R. A. M. J. Wijers31, and T. Zafar32 (Affiliations can be found after the references) Received 13 June 2018 / Accepted 24 July 2018 ABSTRACT Context. Long gamma-ray bursts (GRBs) give us the chance to study both their extreme physics and the star-forming galaxies in which they form. Aims. 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. Methods. 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. Results. The light curve shows a very fast optical rebrightening, with an amplitude of ∼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 −1 gas beyond the star-forming regions. The host has a star formation rate of SFR = 12:2 M yr , a metallicity of 12 + log(O=H) = 8:55, and a mass 9 of 1:6 × 10 M . Conclusions. 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. Key words. gamma-ray burst: individual: GRB 100418A – supernovae: individual: GRB 100418A – galaxies: dwarf – ISM: abundances – ISM: kinematics and dynamics 1. Introduction in radio for periods of weeks, months, or, in some exceptional Long gamma-ray bursts (GRBs) are produced during the dramatic cases, years. This synchrotron radiation is characterised by sev- death of very massive stars in which the core collapses, forming eral power laws connected at characteristic frequencies (Sari et al. a black hole, while material is ejected through narrow polar jets 1998). By studying their evolution we can determine some of the (Rhoads 1997). In order to see the prominent gamma-ray emis- micro- and macro-physical parameters that drive the explosion. sion, the observer’s perspective needs to be within the opening Occasionally the GRB afterglow can also have a reverse-shock angle of the jet. In the most accepted model (Piran 1999), the component (Mészáros & Rees 1999; Nakar & Piran 2004), which gamma rays are produced during internal collisions of material originates within the shocked material that bounces back into the moving at ultrarelativistic speeds within the jets. When the ejecta jet after the encounter of the forward shock with the circumstellar collide with the material that surrounds the star, they are deceler- material. This reverse shock can be quite luminous but is typically ated and at the same time intense synchrotron radiation is emit- shorter lived than the forward shock. ted. This radiation can be observed at all wavelengths between In this basic afterglow model, the light curves are also radio and X-rays, and is known as the forward shock. This elec- expected to evolve according to simple broken power laws. tromagnetic emission is often observed for several days before it However, when sufficient sampling is available, the light curves fades away in optical and X-rays, but can occasionally be followed often deviate from a simple evolution, showing flares, bumps, and wiggles (e.g. Jakobsson et al. 2004; de Ugarte Postigo et al. ? This work makes use of data obtained at the following tele- 2005) that require the addition of further parameters into the scopes/observatories: VLT/Paranal (proposals 085.A-0009, 085.D- models. Energy injections either due to late central engine 0773), GTC/ORM (proposals GTC74-10A, GTCMULTIPLE2B- activity (Dai & Lu 1998; Zhang & Mészáros 2002) or to ejecta 17A), Keck/MK, Subaru/MK, 3.5m/CAHA, UKIRT/MK, WHT/ORM, simultaneously emitted at different velocities (Rees & Mészáros RTT150/TUBITAK, Spitzer, PdBI/IRAM, WSRT/RO, Ryle/MRAO, and SMA/MK. 1998; Sari & Mészáros 2000), structured jets (Mészáros et al. y Deceased. 1998), patchy shells (Nakar & Oren 2004), density fluctuations Article published by EDP Sciences A190, page 1 of 23 A&A 620, A190 (2018) −1 −1 (Wang & Loeb 2000; Ramirez-Ruiz et al. 2001), or double jets cosmology with a flat universe in which H0 = 67:8 km s Mpc , (Berger et al. 2003; Filgas et al. 2011; Kann et al. 2018) are Ωm = 0:308, and Ωλ = 0:692 (Planck Collaboration XIII 2016). α β some examples of models that try to explain some of the devia- We will follow the convention Fν / t ν to describe the tempo- tions from the standard model. ral and spectral evolution of the afterglow. Uncertainties are given Gamma-ray burst afterglows are some of the most lumi- at 68% (1σ) confidence level for one parameter of interest unless nous events known in astronomy and can be observed at virtu- stated otherwise, whereas upper limits are given at the 3σ confi- ally any redshift. The furthest spectroscopically confirmed GRB dence level. was measured at z = 8:2 (Tanvir et al. 2009; Salvaterra et al. 2009). Together with their clean synchrotron spectra, they are useful background light beacons for studying the absorption fea- 2. Observations tures of interstellar material within their host galaxies, the inter- 2.1. Swift observations galactic medium, and any intervening material along their lines of sight. Furthermore, being produced by very massive stars, GRB 100418A was detected by the Burst Alert Telescope (BAT) they are normally found in strongly star-forming (SF) galax- on-board the Neil Gehrels Swift Observatory (Swift hereafter) ies, and within them, not far from their actual birthplaces, since on 18 April 2010 at 21:10:08 UT (Marshall et al. 2010, T0 here- their progenitor stars have rather short lives. This means that after). The gamma-ray emission was characterised by two over- GRBs are great tools for stying SF galaxies throughout the Uni- lapping peaks, with a duration of T90 = 7±1 s in the 15–350 keV verse. Using GRBs to pinpoint these galaxies gives us the advan- range (where T90 is defined as the time during which 90% of the tage of being able to find even the faintest dwarf SF galaxies photons are collected, from 5% to 95% of the total emission), (Hjorth et al.
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