Gamma Ray Burst Lecture Discovery
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The Optical Afterglow of GRB 000911: Evidence for an Associated Supernova??
A&A 378, 996–1002 (2001) Astronomy DOI: 10.1051/0004-6361:20011282 & c ESO 2001 Astrophysics The optical afterglow of GRB 000911: Evidence for an associated supernova?? D. Lazzati1,S.Covino2, G. Ghisellini2,D.Fugazza2,S.Campana2,P.Saracco2,P.A.Price3,4,E.Berger3, S. Kulkarni3, E. Ramirez–Ruiz1,A.Cimatti5, M. Della Valle5, S. di Serego Alighieri5,A.Celotti6, F. Haardt7,G.L.Israel8, and L. Stella8 1 Institute of Astronomy, University of Cambridge, Madingley Road, CB3 0HA Cambridge, UK 2 Osservatorio Astronomico di Brera, Via Bianchi 46, 23807 Merate (Lc), Italy 3 Palomar Observatory, 105-24, California Institute of Technology, Pasadena, CA 91125, USA 4 Research School of Astronomy & Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston, ACT 2611, Australia 5 Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy 6 SISSA/ISAS, via Beirut 4, 34014 Trieste, Italy 7 Universit`a dell’Insubria, Via Lucini 3, 22100 Como, Italy 8 Osservatorio Astronomico di Roma, Via Frascati 33, 00040 Monteporzio Catone, Italy Received 12 July 2001 / Accepted 12 September 2001 Abstract. We present photometric and spectroscopic observations of the late afterglow of GRB 000911, starting ∼1 day after the burst event and lasting ∼8 weeks. We detect a moderately significant re–brightening in the R, I and J lightcurves, associated with a sizable reddening of the spectrum. This can be explained through the presence of an underlying supernova, outshining the afterglow ∼30 days after the burst event. Alternative explanations are discussed. Key words. gamma rays: bursts – supernovae: general 1. Introduction (Djorgovskij et al. 1999), a moderate amount of multiband data but lacked spectroscopic coverge. -
Evidence for Supernova Light in All Gamma-Ray Burst Afterglow A
Clemson University TigerPrints Publications Physics and Astronomy Winter 12-13-2004 Evidence for Supernova Light in all Gamma-Ray Burst Afterglow A. Zeh Thüringer Landessternwarte Tautenburg S. Klose Thüringer Landessternwarte Tautenburg Dieter H. Hartmann Department of Physics and Astronomy, Clemson University, [email protected] Follow this and additional works at: https://tigerprints.clemson.edu/physastro_pubs Recommended Citation Please use publisher's recommended citation. This Article is brought to you for free and open access by the Physics and Astronomy at TigerPrints. It has been accepted for inclusion in Publications by an authorized administrator of TigerPrints. For more information, please contact [email protected]. 22nd Texas Symposium on Relativistic Astrophysics at Stanford University, Dec. 13-17, 2004 Evidence for Supernova Light in All Gamma-Ray Burst Afterglows A. Zeh, S. Klose Thur¨ inger Landessternwarte Tautenburg, 07778 Tautenburg, Germany D. H. Hartmann Department of Physics and Astronomy, Clemson University, Clemson, SC 29634-0978 We present an update of our systematic analyses of all Gamma-Ray Burst (GRB) afterglow data, now published through the end of 2004, in an attempt to detect the predicted supernova light component. We fit the observed photometric light curves as the sum of an afterglow, an underlying host galaxy, and a supernova component. The latter is modeled using published UBV RI light curves of SN 1998bw as a template. The total sample of afterglows with established redshifts contains now 29 bursts (GRB 970228 - GRB 041006). For 13 of them a weak supernova excess (scaled to SN 1998bw) was found. In agreement with our earlier result [47] we find that also in the updated sample all bursts with redshift ∼< 0.7 show a supernova excess in their afterglow light curves. -
No Supernovae Associated with Two Long-Duration Γ-Ray Bursts
1 No supernovae associated with two long-duration γ-ray bursts Johan P. U. Fynbo1, Darach Watson1, Christina C. Thöne1, Jesper Sollerman1,2, Joshua S. Bloom3, Tamara M. Davis1, Jens Hjorth1, Páll Jakobsson4, Uffe G. Jørgensen5, John F. Graham6, Andrew S. Fruchter6, David Bersier7, Lisa Kewley8, Arnaud Cassan9, José María Castro Cerón1, Suzanne Foley10, Javier Gorosabel11, Tobias C. Hinse5, Keith D. Horne12, Brian L. Jensen1, Sylvio Klose13, Daniel Kocevski3, Jean-Baptiste Marquette14, Daniel Perley3, Enrico Ramirez-Ruiz15,16, Maximilian D. Stritzinger1, Paul M. Vreeswijk17,18, Ralph A. M. Wijers19, Kristian G. Woller5, Dong Xu1, Marta Zub6 1Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark 2Department of Astronomy, Stockholm University, Sweden 3Department of Astronomy, University of California at Berkeley, 601 Campbell Hall, Berkeley, CA 94720, USA 4Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, Herts, AL10 9AB, UK 5Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark 6Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, Maryland 21218, USA 7Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD, UK 2 8University of Hawaii, Institute of Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, US 9Astronomisches Rechen-Institut (ARI), Zentrum für Astronomie der Universität Heidelberg (ZAH), Mönchof Str. -
1 the X-Ray Telescope on Board Swift
1 THE X-RAY TELESCOPE ON BOARD SWIFT: STATUS AND MAIN RESULTS G. Tagliaferri1, S. Campana1, G. Chincarini1,2, P. Giommi3, G. Cusumano4, D.N. Burrows5, J.E. Hill5,6, J.A. Kennea5, J.A. Nousek5, J.P. Osborne7, P.T. O’Brien7, A. Wells7, L. Angelini6, and on behalf of the XRT team1 1INAF-Osservatorio Astronomico di Brera, Via Bianchi 46, 23807 Merate, Italy 2Universita` degli Studi di Milano-Bicocca, P.za delle Scienze 3, 20126 Milano, Italy 3ASI Science Data Center, Via G. Galilei, 00044 Frascati, Italy 4INAF-IASF Palermo, Via U. La Malfa 153, 90146 Palermo, Italy 5Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA 6NASA Goddard Space Flight Center, MD 20771, USA 7University of Leicester, Department of Physics and Astronomy, Leicester, LE 17 RH, UK ABSTRACT of the GRBs, if not all, had an associated X-ray after- glow only about 60% of them had also an optical after- glow, i.e. a good fraction of them were dark–GRBs. For The X-ray Telescope (XRT), on board the Swift satellite, a general review on these topics see Zhang & Meszaros provides: automated source detection and position with (2004) and Piran (2005). Therefore, it was clear that to few arcsecond accuracy within few seconds from target properly study the GRBs, and in particular the associ- acquisition; CCD spectroscopy and imaging capability ated afterglows, we needed a fast-reaction satellite capa- (0.2-10 keV), with the capability of detecting a milliCrab ble of detecting GRBs and of performing immediate mul- source in about 10 seconds; automatic adjusting of the tiwavelength follow-up observations, in particular in the CCD readout mode to optimize the science return as the X-ray and optical bands. -
Lecture 19 Black Holes and Gamma-Ray Bursts
Black holes in nature – end points of stellar evolution • In our galaxy alone, theory suggests 50 million black holes (2 SN per century for 1010 years ¼ of which make black holes • Most massive galaxies have massive black holes Lecture 19 at their centers (109 galaxies) • Dozens of black hole binary x-ray sources per Black Holes and galaxy – at least Gamma-Ray Bursts • One gravitational radiation detection so far http://apod.nasa.gov/apod/astropix.html They are out there… Some Properties of Black Holes Kinds of black holes: • Entirely defined by their mass, rotation rate, and charge. All memory of how the hole was made Mass Size is lost. Almost like an elementary particle. “Black holes Class have no hair” (Wheeler, Israel, Hawking, etc.) (solar masses) • Believed that all the mass is concentrated at the AGN Supermassive ~105 - 1010 0.001 - 10 AU center in a small quantum-mechanical singularity Intermediate ~1000 ~ R • The effective density of stellar mass black holes, as ? earth defined by their event horizons is very high, but there are supermassive black hole in active galactic nuclei Stellar ~10 ~30 km with average densities no greater than water. they are just XRBin very big (this ignores the central concentration in a singularity though.) The average density matters to tidal forces. ? Primordial Up to ~Moon Up to ~0.1 mm • The gravitational field of a black hole close to the event horizon is complicated, but by the time you are ⎛ 2GM ⎞ ⎛ M ⎞ RS = 2 = 2.96 km ⎜ ⎟ several Schwarzschild radii away, it is indistinguishable ⎜ c ⎟ M ⎝ ⎠ ⎝ ⎠ from that of an ordinary star. -
Possible Class of Nearby Gamma-Ray Burst / Gravitational Wave Sources
Possible Class of Nearby Gamma-Ray Burst / Gravitational Wave Sources Jay P. Norris NASAIGoddard Space Flight Center Laboratoly for High Energy Astrophysics Abstract. A possible subclass of gamma-ray bursts - those with few, wide pulses, spectral lags of order one to several seconds, and soft spectra - has been identified. Their Log[N]-Logpp] distribution approximates a -312 power-law, suggesting homogeneity and relatively nearby sources. These mostly dim bursts account for - 50% of the BATSE sample of long bursts near that instrument’s trigger threshold, suggesting that this subluminous class constitutes a more common variety than the more familiar burst sources which lie at truly cosmological distances. Theoretical scenarios predicted such a class, motivated by their exemplar GRB 980425 (SN 1998bw) lying at a distance of - 38 Mpc. The observations are explained by invoking off-axis viewing of the GRB jet and/or bulk Lorentz factors of order a few. Long-lag bursts show a tendency to concentrate near the Supergalactic Plane with a quadrupole moment of -0.10 * 0.04, similar to that for SNe type Ib/c within the same volume. The rate of the observed subluminous bursts is of order % that of SNe Ibk. Evidence for a sequential relationship between SNe Ib/c and GRBs is critiqued for two cases, as simultaneity of the SN and GRB events may be important for detection of the expected gravitational wave signal; at most, SN to GRB delays appear to be a few days. SN asymmetries and ultrarelativistic GRB jets suggest the possibility of rapid rotation in the pre-collapse objects, a primary condition required for highly non- axisymmetric SN collapse to produce strong gravitational waves. -
Four GRB-Supernovae at Redshifts Between 0.4 and 0.8 the Bursts GRB 071112C, 111228A, 120714B, and 130831A?
Astronomy & Astrophysics manuscript no. ms c ESO 2018 August 9, 2018 Four GRB-Supernovae at Redshifts between 0.4 and 0.8 The bursts GRB 071112C, 111228A, 120714B, and 130831A? S. Klose1, S. Schmidl1, D. A. Kann1; 2, A. Nicuesa Guelbenzu1, S. Schulze3; 4; 5, J. Greiner6, F. Olivares5; 7, T. Krühler6, P. Schady6, P. M. J. Afonso8, R. Filgas9, J. P. U. Fynbo10, D. A. Perley11, A. Rau6, A. Rossi12, K. Takats5, M. Tanga6, A. C. Updike13, and K. Varela6 (Affiliations can be found after the references) Received 29 January 2018 ABSTRACT Twenty years ago, GRB 980425/SN 1998bw revealed that long Gamma-Ray Bursts (GRBs) are physically associated with broad-lined type Ic supernovae. Since then more than 1000 long GRBs have been localized to high angular precision, but only in ∼ 50 cases the underlying supernova (SN) component was identified. Using the multi-channel imager GROND (Gamma-Ray Burst Optical Near-Infrared Detector) at ESO/La Silla, during the last ten years we have devoted a substantial amount of observing time to reveal and to study SN components in long-GRB afterglows. Here we report on four more GRB-SNe (associated with GRBs 071112C, 111228A, 120714B, and 130831A) which were discovered and/or followed-up with GROND and whose redshifts lie between z = 0:4 and 0.8. We study their afterglow light curves, follow the associated SN bumps over several weeks, and characterize their host galaxies. Using SN 1998bw as a template, the derived SN explosion parameters are fully consistent with the corresponding properties of the so-far known GRB-SN ensemble, with no evidence for an evolution of their properties as a function of redshift. -
Ahypernova'model for SN 1998Bw Associated with Gamma-Ray Burst Of
Under embargo at NATURE (accepted July 27; submitted June 11, 1998) A ‘Hypernova’ model for SN 1998bw associated with gamma-ray burst of 25 April 1998 1 K. Iwamoto∗, P.A. Mazzali†, K. Nomoto∗,††, H. Umeda∗,††, T. Nakamura∗, F. Patat‡, I.J. Danziger†, T.R. Young∗, T. Suzuki∗,††, T. Shigeyama∗,††, T. Augusteijn‡, V. Doublier‡, J.-F. Gonzalez‡, H. Boehnhardt‡, J. Brewer‡ O.R. Hainaut‡, C. Lidman‡, B. Leibundgut⋆, E. Cappellaro§, M. Turatto§, T.J. Galamak, P.M. Vreeswijkk, C. Kouveliotou¶, J. van Paradijsk,‡‡, E. Pian∗∗, E. Palazzi∗∗, F. Frontera∗∗ ∗Department of Astronomy, School of Science, University of Tokyo, Tokyo 113-0033, Japan †Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, I-34131 Trieste, Italy ‡European Southern Observatory, Casilla 19001, Santiago 19, Chile §Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, I-35122 Padova, Italy kAstronomical Institute “Anton Pannekoek”, University of Amsterdam, and Center for High Energy Astrophysics, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands ⋆European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748, Garching, Germany ¶NASA Marshall Space Flight Center, ES-84, Huntsville, AL 35812, USA ∗∗Istituto Tecnologie e Studio Radiazioni Extraterrestri, CNR, Bologna, Italy ††Research Center for the Early Universe, School of Science, University of Tokyo, Tokyo 113-0033, Japan ‡‡Department of Physics, University of Alabama, Huntsville, AL 35899, USA arXiv:astro-ph/9806382v2 6 Aug 1998 1Partially based on observations collected at ESO-La Silla 1 The discovery of the peculiar supernova (SN) 1998bw and its possible association with the gamma-ray burst (GRB) 9804251,2,3 provide new clues to the understanding of the explosion mechanism of very massive stars and to the origin of some classes of gamma- ray bursts. -
Rapid ROSAT Observations of Small Gamma-Ray Burst Error Boxes
Rapid ROSAT Observations of small Gamma-Ray Burst Error Boxes Jochen Greiner Astrophysical Institute Potsdam, 14482 Potsdam, Germany Abstract. I summarize the use of the ROSAT satellite over the last months for the investigation of well localized GRB error boxes. In particular, I report about the attempts for and results of quick follow-up observations (including the GRBs localized with BeppoSAX and RXTE) with ROSAT with its capability to achieve 10′′ locations of X-ray afterglow sources. INTRODUCTION The discovery of X-ray afterglow emission with the narrow-field instruments of the BeppoSAX satellite (Costa et al. 1997) has given a dramatic boost to both, observations and theoretical investigations of gamma-ray bursts (GRBs) over the last few months. In particular, this finding has triggered a wealth of rapid follow-up observations in the X-ray, optical, infrared and radio bands. This has even lead to the development of a strategy of localizing the X-ray afterglow of strong GRBs with non-imaging X-ray instruments (scanning with the PCA onboard RXTE). Also, a procedure has been set up to recognize when individual dwells of the RXTE all-sky monitor cover BATSE burst locations and to derive arcmin size locations within a few hours (Smith et al. 1998). arXiv:astro-ph/9711207v1 18 Nov 1997 X-ray follow up observations are primarily performed with the ASCA and ROSAT satellites. While ASCA’s unique strengths are the very rapid response time (1–2 days) and the high spectral resolution of its X-ray CCD camera (Murakami et al. 1998), ROSAT can provide arcsec positioning and, due to its superb sensitivity, a rather long lever arm for studying the X-ray intensity decay up to 14 days after a GRB. -
Highly Luminous Supernovae Associated with Gamma-Ray Bursts
Astronomy & Astrophysics manuscript no. msAnA˙SN2011kl˙v4 c ESO 2019 March 11, 2019 Highly luminous supernovae associated with gamma-ray bursts I.: GRB 111209A/SN 2011kl in the context of stripped-envelope and superluminous supernovae⋆ D. A. Kann1,2,3,4, P. Schady2, F. Olivares E.5, S. Klose1, A. Rossi6,1, D. A. Perley7,8,9, T. Kr¨uhler2,8,10, J. Greiner2,3, A. Nicuesa Guelbenzu1, J. Elliott2,11, F. Knust2, R. Filgas12, E. Pian5,13, P. Mazzali14,15, J. P. U. Fynbo8, G. Leloudas16,8, P. M. J. Afonso17, C. Delvaux2, J. F. Graham2, A. Rau2, S. Schmidl1, S. Schulze18,19,20, M. Tanga2, A. C. Updike21, and K. Varela2 (Affiliations can be found after the references) Received 22 June 2016 / Accepted ABSTRACT Context. GRB 111209A, one of the longest Gamma-Ray Bursts (GRBs) ever observed, is linked to SN 2011kl, the most luminous GRB-Supernova (SN) detected so far, which shows evidence for being powered by a magnetar central engine. Aims. We place SN 2011kl into the context of large samples of SNe, addressing in more detail the question of whether it could be radioactively powered, and whether it represents an extreme version of a GRB-SN or an underluminous Superluminous SN (SLSN). Methods. We model SN 2011kl using SN 1998bw as a template and derive a bolometric light curve including near-infrared data. We compare the properties of SN 2011kl to literature results on stripped-envelope and superluminous supernovae. Results. Comparison in the k, s context, i.e., comparing it to SN 1998bw templates in terms of luminosity and light-curve stretch, clearly shows SN 2011kl is the most luminous GRB-SN to date, and it is spectrally very dissimilar to other events, being significantly bluer/hotter. -
The Color Evolution of the Optical Afterglow of GRB 030329 and the Implications for the Underlying Supernova SN 2003Dh
A&A 427, 901–905 (2004) Astronomy DOI: 10.1051/0004-6361:20041548 & c ESO 2004 Astrophysics The color evolution of the optical afterglow of GRB 030329 and the implications for the underlying supernova SN 2003dh V. Š im on 1,R.Hudec1, and G. Pizzichini2 1 Astronomical Institute, Academy of Sciences of the Czech Republic, 251 65 Ondrejov,ˇ Czech Republic e-mail: [email protected] 2 IASF/CNR, Sezione di Bologna, via Gobetti 101, 40129 Bologna, Italy Received 4 February 2004 / Accepted 30 June 2004 Abstract. We find that the color indices (B − V)0,(V − R)0,(R − I)0,(I − J)0 in the observer frame of the optical afterglow (OA) of GRB 030329 during t − T0 < 10 days are consistent with those of a uniform group of 25 OAs of GRBs, previously analyzed by Šimon et al. (2001; 2003a). The synchrotron component with parameters similar to those of the other 25 OAs was thus initially dominant in the optical and IR spectrum of the OA of GRB 030329. Following the arguments of Šimon et al. (2001), it also appears that either GRB 030329 was not located deep inside a star-forming region or that the local dust was destroyed by ≈− . − = . the intense initial flash. The absolute R magnitude of this event MR0 26 6 mag in the rest frame at (t T0)rest 0 25 days is in good agreement with the typical brightness of the OAs analyzed by Šimon et al. (2001). We detected large color variations of the OA of GRB 030329 only for t − T0 > 12 days, which suggest a rapid evolution of the spectrum of the underlying SN 2003dh. -
Observing the Gamma-Ray Burst–Supernova Connection with 1M-Class Aperture Telescopes Corinne Maly Taylor Clemson University, [email protected]
Clemson University TigerPrints All Theses Theses 8-2018 Observing the Gamma-Ray Burst–Supernova Connection with 1m-class Aperture Telescopes Corinne Maly Taylor Clemson University, [email protected] Follow this and additional works at: https://tigerprints.clemson.edu/all_theses Recommended Citation Taylor, Corinne Maly, "Observing the Gamma-Ray Burst–Supernova Connection with 1m-class Aperture Telescopes" (2018). All Theses. 2904. https://tigerprints.clemson.edu/all_theses/2904 This Thesis is brought to you for free and open access by the Theses at TigerPrints. It has been accepted for inclusion in All Theses by an authorized administrator of TigerPrints. For more information, please contact [email protected]. Observing the Gamma-Ray Burst{Supernova Connection with 1m-class Aperture Telescopes A Thesis Presented to the Graduate School of Clemson University In Partial Fulfillment of the Requirements for the Degree Master of Science Physics by Corinne Maly Taylor August 2018 Accepted by: Dr. Dieter Hartmann, Committee Chair Dr. M´at´e Ad´amkovics´ Dr. Joan Marler Abstract Observations over the past two decades indicate that some gamma-ray bursts (GRBs) are associated with core-collapse supernovae (SNe). We explore the connection between nature's two biggest explosions by reviewing their photometric properties and standard models. Using three small telescopes (1-m class) belonging to the Southeastern Association for Research in Astronomy (SARA) consortium, we observed four events and present our findings here. These events include a connected GRB-SN (GRB 171205A/SN 2017iuk), an orphan afterglow (AT 2018cow), a burst with a faint afterglow (GRB 180620A), and a burst with no afterglow (GRB 180514).