iPTF17cw: An Engine-driven Supernova Candidate Discovered Independent of a Gamma-Ray Trigger

Corsi, A.; Cenko, S. Bradley; Kasliwal, M. M.; Quimby, R.; Kulkarni, S. R.; Frail, D. A.; Goldstein, A.; Blagorodnova, N.; Connaughton, V.; Perley, D. A.; Singer, L. P.; Copperwheat, C. M.; Fremling, C.; Kupfer, Thomas; Piascik, A. S.; Steele, I. A.; Taddia, F.; Vedantham, H. K.; Kutyrev, A.; Palliyaguru, N.; Roberts, O. J.; Sollerman, J.; Troja, E.; Veilleux, Sylvain

doi:10.3847/1538-4357/aa85e5

Cited by 28 publications

(30 citation statements)

References 89 publications

(153 reference statements)

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“…References: AT 2018cow (Margutti et al 2019), ZTF18abvkwla (see footnote 43, Ho et al 2020), TDEs (Zauderer et al 2011;Berger et al 2012;Cenko et al 2012b;Alexander et al 2016Alexander et al , 2017, GRBs, and SNe (Margutti et al 2013a(Margutti et al , 2014a) and references therein. 42 A class of stellar explosions that show mildly relativistic outflows but no detected higher-energy γ-ray counterparts (GRBs) associated with relativistic jets (Soderberg et al 2010a;Margutti et al 2014a;Chakraborti et al 2015;Corsi et al 2017).…”

Section: Notesmentioning

confidence: 99%

A Mildly Relativistic Outflow from the Energetic, Fast-rising Blue Optical Transient CSS161010 in a Dwarf Galaxy

Coppejans

Margutti

Terreran

et al. 2020

ApJL

151

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We present X-ray and radio observations of the Fast Blue Optical Transient CRTS-CSS161010 J045834 −081803 (CSS161010 hereafter) at t=69-531 days. CSS161010 shows luminous X-ray (L x ∼5× 10 39 erg s −1 ) and radio (L ν ∼10 29 erg s −1 Hz −1 ) emission. The radio emission peaked at ∼100 days posttransient explosion and rapidly decayed. We interpret these observations in the context of synchrotron emission from an expanding blast wave. CSS161010 launched a mildly relativistic outflow with velocity Γβc0.55c at ∼100 days. This is faster than the non-relativistic AT 2018cow (Γβc∼0.1c) and closer to ZTF18abvkwla (Γβc0.3c at 63 days). The inferred initial kinetic energy of CSS161010 (E k 10 51 erg) is comparable to that of long gamma-ray bursts, but the ejecta mass that is coupled to the mildly relativistic outflow is significantly larger ( -). This is consistent with the lack of observed γ-rays. The luminous X-rays were produced by a different emission component to the synchrotron radio emission. CSS161010 is located at ∼150 Mpc in a dwarf galaxy with stellar mass M * ∼10 7 M e and specific star formation rate sSFR∼0.3 Gyr −1 . This mass is among the lowest inferred for host galaxies of explosive transients from massive stars. Our observations of CSS161010 are consistent with an engine-driven aspherical explosion from a rare evolutionary path of a H-rich stellar progenitor, but we cannot rule out a stellar tidal disruption event on a centrally located intermediate-mass black hole. Regardless of the physical mechanism, CSS161010 establishes the existence of a new class of rare

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Section: Notesmentioning

confidence: 99%

A Mildly Relativistic Outflow from the Energetic, Fast-rising Blue Optical Transient CSS161010 in a Dwarf Galaxy

Coppejans

Margutti

Terreran

et al. 2020

ApJL

151

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“…Data for PTF 11cmh and PTF 11qcj are from the 5 GHz light curve in Corsi et al (2016). Data for iPTF 17cw are from the 2.8 GHz light curve in Corsi et al (2017). Data for ZTF 18aaqjovh are from Ho et al (2020b).…”

Section: X-ray Emissionmentioning

confidence: 99%

“…To make progress on understanding the GRB-LLGRB-SN connection, wide-field high-cadence optical surveys can be used in conjunction with radio and X-ray follow-up observations to discover GRB-related phenomena without relying on a GRB trigger (e.g., Soderberg et al 2010;Cenko et al 2013;Margutti et al 2014;Corsi et al 2017). To this end, for the past 2 yr, we have been conducting a systematic search for enginedriven explosions using the high cadence (6× night -1 ) and nightly cadence (2× night -1 ) surveys of the Zwicky Transient Facility (ZTF; Bellm et al 2019b;Graham et al 2019), which have a combined area of 5000 deg 2 (Bellm et al 2019a).…”

Section: Introductionmentioning

confidence: 99%

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SN 2020bvc: A Broad-line Type Ic Supernova with a Double-peaked Optical Light Curve and a Luminous X-Ray and Radio Counterpart

Kulkarni

Perley

et al. 2020

ApJ

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We present optical, radio, and X-ray observations of SN 2020bvc (=ASASSN-20bs, ZTF 20aalxlis), a nearby (= z 0.0252; d=114 Mpc) broad-line (BL) Type Ic supernova (SN) and the first double-peaked Ic-BL discovered without a gamma-ray burst (GRB) trigger. Our observations show that SN 2020bvc shares several properties in common with the Ic-BL SN 2006aj, which was associated with the low-luminosity gamma-ray burst (LLGRB) 060218. First, the 10 GHz radio luminosity (»-L 10 erg s radio 37 1) is brighter than ordinary core-collapse SNe but fainter than LLGRB SNe such as SN 1998bw (associated with LLGRB 980425). We model our VLA observations (spanning 13-43 days) as synchrotron emission from a mildly relativistic (v  0.3c) forward shock. Second, with Swift and Chandra, we detect X-ray emission (L X ≈10 41 ergs 1) that is not naturally explained as inverse Compton emission or part of the same synchrotron spectrum as the radio emission. Third, high-cadence (6× night-1) data from the Zwicky Transient Facility (ZTF) show a double-peaked optical light curve, the first peak from shock cooling of extended low-mass material (mass <-M M 10 e 2  at radius R e >10 12 cm) and the second peak from the radioactive decay of Ni 56. SN 2020bvc is the first double-peaked Ic-BL SN discovered without a GRB trigger, so it is noteworthy that it shows X-ray and radio emission similar to LLGRB SNe. For four of the five other nearby (z0.05) Ic-BL SNe with ZTF high-cadence data, we rule out a first peak like that seen in SN 2006aj and SN 2020bvc, i.e., that lasts ≈1 dayand reaches a peak luminosity M≈−18. Follow-up X-ray and radio observations of Ic-BL SNe with well-sampled early optical light curves will establish whether double-peaked optical light curves are indeed predictive of LLGRB-like X-ray and radio emission. Unified Astronomy Thesaurus concepts: Radio transient sources (2008); High energy astrophysics (739); Transient sources (1851); Core-collapse supernovae (304); Supernovae (1668); Type Ic supernovae (1730); X-ray transient sources (1852); Gamma-ray bursts (629) Supporting material: data behind figure, machine-readable table

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“…Recently, Prentice & Mazzali (2017) presented a physically motivated classification of SE-SNe, in which they found that all GRB-SNe are Type Ic-3; conversely, not all Type Ic SNe with high expansion speeds are associated with GRBs and almost all of these non-GRB SNe have N > 3 in the classification scheme of Prentice & Mazzali (2017). In rare cases, such Type Ic-BL SNe show evidence for relativistic ejecta but without an associated GRB, for example SN 2009bb (Soderberg et al 2010;Pignata et al 2011), SN 2012ap (Margutti et al 2014;Milisavljevic et al 2015a), and iPTF17cw (Corsi et al 2017), the latter possibly being associated with a GRB. A&A 624, A143 (2019) The GRB 111209A, discovered by the Neil Gehrels Swift Observatory satellite (Gehrels et al 2004), is a truly remarkable event, at 25 ks the second-longest (after GRB 170714A;D'Ai et al 2017;Kann et al 2017) GRB ever discovered (Golenetskii et al 2011;Gendre et al 2013), and one of the very rare ultralong GRBs (ULGRBs; Levan et al 2014;henceforth L14; see also Levan 2015).…”

Section: Introductionmentioning

confidence: 97%

Highly luminous supernovae associated with gamma-ray bursts

Канн

Schady

et al. 2019

A&A

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Context. GRB 111209A, one of the longest gamma-ray bursts (GRBs) ever observed, is linked to SN 2011kl, which is the most luminous GRB supernova (SN) detected so far. Several lines of evidence indicate that this GRB-SN is 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 this GRB-SN could be radioactively powered, and whether it represents an extreme version of a GRB-SN or an underluminous superluminous SN (SLSN). Methods. We modelled SN 2011kl using SN 1998bw as a template and derived a bolometric light curve including near-infrared data. We compared the properties of SN 2011kl to literature results on stripped-envelope and SLSNe. Results. A comparison in the k, s context, i.e. comparing SN 2011kl 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 is spectrally very dissimilar to other events because it is significantly bluer/hotter. Although SN 2011kl does not reach the classical luminosity threshold of SLSNe and evolves faster than any of these objects, it resembles SLSNe more than the classical GRB-associated broad-lined Type Ic SNe in several aspects. Conclusions. GRB 111209A was a very energetic event, both at early (prompt emission) and at very late (SN) times. We show in a companion publication that with the exception of the extreme duration, the GRB and afterglow parameters are in agreement with the known distributions for these parameters. SN 2011kl, on the other hand, is exceptional both in luminosity and spectral characteristics, indicating that GRB 111209A was likely not powered by a standard-model collapsar central engine, further supporting our earlier conclusions. Instead, it reveals the possibility of a direct link between GRBs and SLSNe.

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iPTF17cw: An Engine-driven Supernova Candidate Discovered Independent of a Gamma-Ray Trigger

Cited by 28 publications

References 89 publications

A Mildly Relativistic Outflow from the Energetic, Fast-rising Blue Optical Transient CSS161010 in a Dwarf Galaxy

A Mildly Relativistic Outflow from the Energetic, Fast-rising Blue Optical Transient CSS161010 in a Dwarf Galaxy

SN 2020bvc: A Broad-line Type Ic Supernova with a Double-peaked Optical Light Curve and a Luminous X-Ray and Radio Counterpart

Highly luminous supernovae associated with gamma-ray bursts

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