Hindawi Advances in Astronomy Volume 2017, Article ID 8929054, 41 pages https://doi.org/10.1155/2017/8929054 Review Article The Observer’s Guide to the Gamma-Ray Burst Supernova Connection Zach Cano,1,2 Shan-Qin Wang,3,4 Zi-Gao Dai,3,4 and Xue-Feng Wu5,6 1 Centre for Astrophysics and Cosmology, Science Institute, University of Iceland, Dunhagi 5, 107 Reykjavik, Iceland 2Instituto de Astrof´ısica de Andaluc´ıa (IAA-CSIC), Glorieta de la Astronom´ıa s/n, 18008 Granada, Spain 3School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China 4Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing, China 5Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China 6Joint Center for Particle, Nuclear Physics and Cosmology, Nanjing University-Purple Mountain Observatory, Nanjing 210008, China Correspondence should be addressed to Zach Cano; [email protected] Received 7 April 2016; Accepted 29 November 2016; Published 11 April 2017 Academic Editor: Josep M. Trigo-Rodr´ıguez Copyright © 2017 Zach Cano et al. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. We present a detailed report of the connection between long-duration gamma-ray bursts (GRBs) and their accompanying supernovae (SNe). The discussion presented here places emphasis on how observations, and the modelling of observations, have constrained what we know about GRB-SNe. We discuss their photometric and spectroscopic properties, their role as cosmological probes, including their measured luminosity–decline relationships, and how they can be used to measure the Hubble constant. We present a statistical summary of their bolometric properties and use this to determine the properties of the “average” GRB-SN. We discuss their geometry and consider the various physical processes that are thought to power the luminosity of GRB-SNe and whether differences exist between GRB-SNe and the SNe associated with ultra-long-duration GRBs. We discuss how observations of their environments further constrain the physical properties of their progenitor stars and give a brief overview of the current theoretical paradigms of their central engines. We then present an overview of the radioactively powered transients that have been photometrically associated with short-duration GRBs, and we conclude by discussing what additional research is needed to further our understanding of GRB-SNe, in particular the role of binary-formation channels and the connection of GRB-SNe with superluminous SNe. 1. Introduction was truly representative of the general LGRB population. This uncertainty persisted for almost five years until the spec- Observations have proved the massive-star origins of long- troscopic association between cosmological/high-luminosity ∼8×1050 −1 duration GRBs (LGRBs) beyond any reasonable doubt. The GRB 030329 ( 훾,iso erg s ) and SN 2003dh [4– temporal and spatial connection between GRB 980425 and 6]. GRB 030329 had an exceptionally bright optical afterglow broad-lined type Ic (IcBL) SN 1998bw offered the first clues to (AG; see Figures 2 and 3), and a careful decomposition of the their nature [1, 2] (Figure 1). The close proximity of this event photometric and spectroscopic observations was required in ( = 0.00866; ∼40 Mpc), which is still the closest GRB to order to isolate the SN features from the dominant AG light date, resulted in it becoming one of the most, if not the most, [7] (see Section 2.1 and Figure 4). As was seen for SN 1998bw, scrutinized GRB-SN in history. It was shown that SN 1998bw SN 2003dh was a type IcBL SN, and its kinetic energy was in 52 had a very large kinetic energy (see Section 4 and Table 3) excess of 10 erg,showingthatittoowasahypernova. 52 of ∼2–5×10 erg, which led it to being referred to as a The launch of the Swift satellite [8] dramatically changed hypernova [3]. However, given several peculiarities of its - the way we studied GRBs and the GRB-SN association, and ray properties, including its underluminous -ray luminosity thenumberofeventsdetectedbythismissionhashelped ∼5×1046 −1 ( 훾,iso erg s ), it was doubted whether this event increase the GRB-SN sample size by a factor of three since 2 Advances in Astronomy 10−13 −7d −2d 10−14 +1d +4d +11d +22d −15 const 10 +45d + ) +64d −1 +94d Å 2 −16 12 − 10 cm 13 1 − +125 d 14 10−17 I−1 (erg s 15 휆 R − 0.5 f +201 d (mag) 16 V 10−18 17 B 18 U+1 +376 d 19 10−19 0510 20 30 40 060 70 8090 100 4000 6000 8000 10000 t−t0 (d) 휆 (Å) Figure 1: GRB 980425/SN 1998bw: the archetype GRB-SN. Host image (ESO 184-G82) is from [1], where the position of the optical transient is clearly visible. Optical light curves are from [9] and spectra from [2]. −2.05 18 t + SN 1998bw V-band (z = 0.16854,훿t=0) SN 2003dh SN 1998bw 4.0 d 19 7.4 d 8.3 d 8.3 d R 20 9.9 d 12.2 d 15.9 constant units) (arbitrary d + 15.1 d 21 휆 f 20.1 d 20.3 d 27.8 d 27.1 d 22 0 20 40 60 3000 4000 5000 6000 7000 8000 9000 Days after March 29.4842 Rest wavelength (Å) (a) (b) Figure 2: (a) The photometric (-band) evolution of GRB 030329/SN 2003dh, from [6]; (b) the spectral evolution of GRB 030329/SN 2003dh, as compared with that of SN 1998bw, from [4]. the pre-Swift era. This includes, among many others, the well- focused the majority of the content on achievements made studied events GRB 060218/SN 2006aj, GRB 100316D/SN in the 10 years since [11] was published. In this review and 2010bh, GRB 111209A/SN 2011kl, GRB 120422A/SN 2012bz, many others [12–19], thorough historical accounts of the GRB 130427A/SN 2013cq, and GRB 130702A/SN 2013dx. A development of the gamma-ray burst supernova (GRB-SN) full list of the references to these well-studied spectroscopic connection are presented, and we encourage the reader to GRB-SN associations is found in Table 4. consult the detailed presentation given in section one of [11] This review paper represents a continuation of other for further details. In Tables 2 and 3 we present the most review articles presented to date, including the seminal comprehensive database yet compiled of the observational work by Woosley and Bloom (2006) [11]. As such, we have and physical properties of the GRB prompt emission and Advances in Astronomy 3 011121 021211 15 030329 041006 050525A 060904B 20 081007 (mag) 090618 R 091127 101219B 111209A 25 130702A GRB-SN bumps 130831A 140606B 10−3 0.01 0.1 1 10 100 t−t0 (observer-frame days) Figure 3: A mosaic of GRB-SNe (AG + SN). Clear SN bumps are observed for all events except SN 2003dh, for which the SN’s properties had to be carefully decomposed from photometric and spectroscopic observations [7]. The lack of an unambiguous SN bump in this case is not surprising given the brightness of its AG relative to the other GRB-SN in the plot: SN 2013dx was at a comparable redshift ( = 0.145, compared with = 0.1685 for 2003dh), but its AG was much fainter (2–5 mag) at a given moment in time. The redshift range probed in this mosaic spans almost an order of magnitude (0.145 < < 1.006) and shows the variation in peak observed magnitude for GRB-SNe. It is important to remember that given the large span of distances probed here, observer-frame -band samples a wide range of rest-frame SEDs (from -band to -band). GRB 090618 GRB 090618 0.01 0.1 GRB 090618 AG + SN + host AG + SN SN 0.1 10−3 0.01 10−4 0.01 −3 10 SN model −5 −4 10 Flux density (mJy) density Flux (mJy) density Flux 10 AG model (mJy) density Flux 10−3 0.1 1 10 100 0.1 1 10 100 10 100 t−t0 (days) t−t0 (days) t−t0 (days) (a) (b) (c) Figure 4: An example decomposition of the optical (-band) light curve of GRB 090618 [10]. (a) For a given GRB-SN event, the single-filter monochromatic flux is attributed as arising from three sources: the AG, the SN, and a constant source of flux from the host galaxy. (b)Once the observations have been dereddened, the host flux is removed, either via the image-subtraction technique or by being mathematically subtracted away. At this point a mathematical model composed of one or more power laws punctuated by break-times is fit to the early light curve to determine the temporal behaviour of the AG. (c) Once the AG model has been determined, it is subtracted from the observations leaving just light from the SN. GRB-SNe, respectively, which consists of 46 GRB-SNe. It is been renormalized to this cosmological model. Foreground the interpretation of these data which forms a substantial extinctions were calculated using the dust extinction maps contribution to this review. We have adopted the grading of [21, 22]. Unless stated otherwise, errors are statistical only. scheme devised by [17] to assign a significance of the GRB- Nomenclature is as follows: denotes the standard deviation SN association to each event, where A is strong spectroscopic of a sample, whereas the root-mean square of a sample is evidence, B is a clear light curve bump as well as some expressed as RMS. A symbol with an overplotted bar denotes spectroscopic evidence resembling a GRB-SN, C is a clear an average value.