Maqola

A tale of two GRB-SNe at a common redshift of z=0.54

Z. CanoAstrophysics Research Institute , Liverpool John Moores University , LiverpoolD. BersierC. GuidorziAstrophysics Research Institute , Liverpool John Moores University , LiverpoolR. MarguttiINAF -Osservatorio Astronomico di Brera , via E. Bianchi 46 , 23807 , Merate , LC , ItalyK. M. SvenssonDepartment of Physics , University of Warwick , CoventryS. KobayashiAstrophysics Research Institute , Liverpool John Moores University , LiverpoolA. MelandriINAF -Osservatorio Astronomico di Brera , via E. Bianchi 46 , 23807 , Merate , LC , ItalyK. WiersemaDepartment of Physics and Astronomy , University of Leicester , LeicesterA. PozanenkoSpace Research Institute of RAS , Profsoyuznaya , 84/32 , Moscow , RussiaA. J. van der HorstNASA/Marshall Space Flight Center , Huntsville , AL , USAG. G. PooleyA. Fernandez-SotoInstituto de Fisica de Cantabria (CSIC-UC) , E39005- Santander , SpainA. J. Castro-TiradoInstituto de Astrofísica de Andalucía (IAA-CSIC) , Granada , SpainA. de Ugarte PostigoM. ImCEOU , Department of Physics & Astronomy , Seoul National University , Seoul , KoreaA. P. KambleAstronomical Institute , University of Amsterdam , XH Amsterdam , the NetherlandsD. SahuIndian Institute of Astrophysics , Bangalore , IndiaJ. Alonso-LoriteObservatori Astronómic de la Universitat de València , Valencia , SpainG. AnupamaIndian Institute of Astrophysics , Bangalore , IndiaJ. L. BibbyUniversity of Sheffield , Department of Physics & Astronomy , SheffieldM. J. BurgdorfSOFIA Science Center , NASA Ames Research Center , Moffett Field CA , USAN. ClayAstrophysics Research Institute , Liverpool John Moores University , LiverpoolP. A. CurranAstrophysique, Instrumentation et ModélisationT. A. FatkhullinSpecial Astrophysical Observatory of Russian Academy of Science (SAO-RAS) , Nizhnij Arkhyz , Karachai-Cherkessia , RussiaA. S. FruchterSpace Telescope Science Institute , Baltimore , MD , USAP. GarnavichPhysics Department , University of Notre Dame , Notre Dame , IN , USAA. GombocCentre of Excellence SPACE-SI , Aškerčeva cesta 12 , SI-1000 Ljubljana SloveniaJ. GorosabelInstituto de Astrofísica de Andalucía (IAA-CSIC) , Granada , SpainJ. F. GrahamSpace Telescope Science Institute , Baltimore , MD , USAU. GurugubelliIndian Institute of Astrophysics , Bangalore , IndiaJ. HaislipK. HuangAcademia Sinica Institute of Astronomy and Astrophysics , Taipei , TaiwanA. HuxorUniversity of Bristol , H. H. Wills Physics Laboratory , BristolM. IbrahimovUlugh Beg Astronomical Institute , Tashkent , UzbekistanY. JeonCEOU , Department of Physics & Astronomy , Seoul National University , Seoul , KoreaY.-B. JeonCEOU , Department of Physics & Astronomy , Seoul National University , Seoul , KoreaK. IvarsenD. KasenZ . Cano et al. 31 University of California , Santa Cruz , CA , USAE. KlunkoC. KouveliotouSpace Science Office , VP62 , NASA/Marshall Space Flight Center , Huntsville , AL , USAA. LaCluyzeA. J. LevanDepartment of Physics , University of Warwick , CoventryV. LoznikovSpace Research Institute of RAS , Profsoyuznaya , 84/32 , Moscow , RussiaP. A. MazzaliA. S. MoskvitinSpecial Astrophysical Observatory of Russian Academy of Science (SAO-RAS) , Nizhnij Arkhyz , Karachai-Cherkessia , RussiaC. MottramAstrophysics Research Institute , Liverpool John Moores University , LiverpoolC. G. MundellAstrophysics Research Institute , Liverpool John Moores University , LiverpoolP. E. NugentComputational Cosmology Center , Lawrence Berkeley National Laboratory , Berkeley , CA , USAM. NysewanderSpace Telescope Science Institute , Baltimore , MD , USAP. T. O’BrienW.-K. ParkCEOU , Department of Physics & Astronomy , Seoul National University , Seoul , KoreaV. PerisObservatori Astronómic de la Universitat de València , Valencia , SpainE. PianScuola Normale Superiore , Piazza Cavalieri 7 , Pisa , ItalyD. ReichartJ. E. RhoadsSchool of Earth and Space Exploration , Arizona State University , Tempe , AZ , USAE. RolUniversity of AmsterdamV. RumyantsevSRI Crimean Astrophysical Observatory , Nauchny , Crimea , UkraineV. ScowcroftCarnegie Observatories , 813 Santa Barbara Street , Pasadena , California , USAD. ShakhovskoySRI Crimean Astrophysical Observatory , Nauchny , Crimea , UkraineE. SmallAstrophysics Research Institute , Liverpool John Moores University , LiverpoolR. J. SmithAstrophysics Research Institute , Liverpool John Moores University , LiverpoolV. V. SokolovSpecial Astrophysical Observatory of Russian Academy of Science (SAO-RAS) , Nizhnij Arkhyz , Karachai-Cherkessia , RussiaR. L. C. StarlingDepartment of Physics and Astronomy , University of Leicester , LeicesterI. SteeleAstrophysics Research Institute , Liverpool John Moores University , LiverpoolR. G. StromN. R. TanvirDepartment of Physics and Astronomy , University of Leicester , LeicesterY. TsaprasZ . Cano et al. 31 University of California , Santa Cruz , CA , USAY. UrataZ . Cano et al. 31 University of California , Santa Cruz , CA , USAO. VăduvescuZ . Cano et al. 31 University of California , Santa Cruz , CA , USAA. VolnovaZ . Cano et al. 31 University of California , Santa Cruz , CA , USAA. VolvachSRI Crimean Astrophysical Observatory , Nauchny , Crimea , UkraineR. A. M. J. WijersUniversity of AmsterdamS. E. WoosleyZ . Cano et al. 31 University of California , Santa Cruz , CA , USAD. R. YoungZ . Cano et al. 31 University of California , Santa Cruz , CA , USA

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Annotatsiya

We present ground-based and Hubble Space Telescope optical observations of the optical transients (OTs) of long-duration Gamma Ray Bursts (GRBs) 060729 and 090618, both at a redshift of z = 0.54.For GRB 060729, bumps are seen in the optical light curves (LCs), and the late-time broad-band spectral energy distributions (SEDs) of the OT resemble those of local Type Ic supernovae (SNe).For GRB 090618, the dense sampling of our optical observations has allowed us to detect well-defined bumps in the optical LCs, as well as a change in colour, that are indicative of light coming from a core-collapse SN.The accompanying SNe for both events are individually compared with SN1998bw, a known GRB supernova, and SN1994I, a typical Type Ic supernova without a known GRB counterpart, and in both cases the brightness and temporal evolution more closely resemble SN1998bw.We also exploit our extensive optical and radio data for GRB 090618, as well as the publicly available Swift-XRT data, and discuss the properties of the afterglow at early times.In the context of a simple jet-like model, the afterglow of GRB 090618 is best explained by the presence of a jet-break at tt o > 0.5 d.We then compare the rest-frame, peak V-band absolute magnitudes of all of the GRB and X-Ray Flash (XRF)-associated SNe with a large sample of local Type Ibc SNe, concluding that, when host extinction is considered, the peak magnitudes of the GRB/XRF-SNe cannot be distinguished from the peak magnitudes of non-GRB/XRF SNe.

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DOI: 10.1111/j.1365-2966.2010.18164.x

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