Radio Emission from the Cocoon of a GRB Jet: Implications for Relativistic Supernovae and Off-axis GRB Emission

Colle, Fabio De; Kumar, Pawan; Aguilera-Dena, David R.

doi:10.3847/1538-4357/aad04d

Cited by 25 publications

(16 citation statements)

References 51 publications

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“…SN 2009bb was discovered by the galaxy-targeted survey, the CHilean Automatic Supernova sEarch (CHASE; Pignata et al 2009a) on 21 March 2009 (Pignata et al 2009b) at the position of 10:31:33.8762, −39:57:30.022 (Bietenholz et al 2010) and was a broad-line type-Ic supernova (Stritzinger et al 2009). Radio and optical behaviour, and the relativistic ejecta velocity of SN 2009bb were very similar to those of low-z GRBs, especially GRB 980425 (SN1998bw; Soderberg et al 2010;Bietenholz et al 2010;Pignata et al 2011;De Colle et al 2018).…”

Section: Introductionmentioning

confidence: 60%

Relativistic supernova 2009bb exploded close to an atomic gas cloud

Michalowski

Gentile

Krühler

et al. 2018

A&A

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Context. The host galaxies of gamma-ray bursts (GRBs) have been claimed to have experienced a recent inflow of gas from the intergalactic medium. This is because their atomic gas distribution is not centred on their optical emission and because they are deficient in molecular gas given their high star formation rates (SFRs). Similar studies have not been conducted for host galaxies of relativistic supernovae (SNe), which may have similar progenitors. Aims. The potential similarity of the powering mechanisms of relativistic SNe and GRBs allowed us to make a prediction that relativistic SNe are born in environments similar to those of GRBs, that is, ones which are rich in atomic gas. Here we embark on testing this hypothesis by analysing the properties of the host galaxy NGC 3278 of the relativistic SN 2009bb. This is the first time the atomic gas properties of a relativistic SN host are provided and the first time resolved 21 cm-hydrogen-line (H I) information is provided for a host of an SN of any type in the context of the SN position. Methods. We obtained radio observations with the Australia Telescope Compact Array (ATCA) covering the H I line, and optical integral field unit spectroscopy observations with the Multi Unit Spectroscopic Explorer (MUSE) at the Very Large Telescope (VLT). Moreover, we analysed archival carbon monoxide (CO) and multi-wavelength data for this galaxy. Results. The atomic gas distribution of NGC 3278 is not centred on the optical galaxy centre, but instead around a third of atomic gas resides in the region close to the SN position. This galaxy has a few times lower atomic and molecular gas masses than predicted from its SFR. Its specific SFR (sSFR ≡ SFR/M*) is approximately two to three times higher than the main-sequence value, placing it at the higher end of the main sequence, towards starburst galaxies. SN 2009bb exploded close to the region with the highest SFR density and the lowest age, as evident from high Hα EW, corresponding to the age of the stellar population of ~5.5 Myr. Assuming this timescale was the lifetime of the progenitor star, its initial mass would have been close to ~36 M⊙. Conclusions. As for GRB hosts, the gas properties of NGC 3278 are consistent with a recent inflow of gas from the intergalactic medium, which explains the concentration of atomic gas close to the SN position and the enhanced SFR. Super-solar metallicity at the position of the SN (unlike for most GRBs) may mean that relativistic explosions signal a recent inflow of gas (and subsequent star formation), and their type (GRBs or SNe) is determined either (i) by the metallicity of the inflowing gas, so that metal-poor gas results in a GRB explosion and metal-rich gas (for example a minor merger with an evolved galaxy or re-accretion of expelled gas) results in a relativistic SN explosion without an accompanying GRB, or (ii) by the efficiency of gas mixing (efficient mixing for SN hosts leading to a quick disappearance of metal-poor regions), or (iii) by the type of the galaxy (more metal-rich galaxies would result in only a small fraction of star formation being fuelled by metal-poor gas).

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Section: Introductionmentioning

confidence: 60%

Relativistic supernova 2009bb exploded close to an atomic gas cloud

Michalowski

Gentile

Krühler

et al. 2018

A&A

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“…lution of the slow-cooling synchrotron spectrum would suggest a delayed peak in the radio emission. This last scenario opens the possibility that the early radio emission is contaminated by another component, which could be the tail of the radio cocoon emission (De Colle et al 2018a). We also note that a good fit can be obtained with a less stratified environment and smaller observing angles (an R −2 medium is not the best choice for our models; a more detailed analysis will be presented in a future publication).…”

Section: Discussionmentioning

confidence: 91%

“…X-ray emission from the cocoon of a successful GRB is expected to peak a few hundred seconds after the explosion, and then to decay quickly (De Colle et al 2018a), similarly to what is seen in SN 2017iuk (Izzo et al 2019), thus not representing an important contribution in the emission on the observed timescale (≈days).…”

Section: Discussionmentioning

confidence: 92%

Broad-line type Ic SN 2020bvc

Izzo

Auchettl

Hjorth

et al. 2020

A&A

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Long-duration gamma-ray bursts (GRBs) are almost unequivocally associated with very energetic, broad-line supernovae of Type Ic-BL. While the gamma-ray emission is emitted in narrow jets, the SN emits radiation isotropically. Therefore, it has been hypothesized that some SN Ic-BL not associated with GRBs arise from events with inner engines such as off-axis GRBs or choked jets. Here we present observations of the nearby (d = 120 Mpc) SN 2020bvc (ASAS-SN 20bs) that support this scenario. Swift-UVOT observations reveal an early decline (up to two days after explosion), while optical spectra classify it as a SN Ic-BL with very high expansion velocities (≈70 000 km s−1), similar to that found for the jet-cocoon emission in SN 2017iuk associated with GRB 171205A. Moreover, the Swift X-Ray Telescope and CXO X-ray Observatory detected X-ray emission only three days after the SN and decaying onward, which can be ascribed to an afterglow component. Cocoon and X-ray emission are both signatures of jet-powered GRBs. In the case of SN 2020bvc, we find that the jet is off axis (by ≈23 degrees), as also indicated by the lack of early (≈1 day) X-ray emission, which explains why no coincident GRB was detected promptly or in archival data. These observations suggest that SN 2020bvc is the first orphan GRB detected through its associated SN emission.

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“…Unfortunately, telling whether a misaligned relativistic jet is present is not easy, since all the radiation is relativistically beamed away from the line of sight. The slow but steady brightening was shown to be consistent with the presence of a jet, its energy contribution along the line of sight growing with the deceleration of the external shock (Xiao et al, 2017;De Colle et al, 2018;Finstad et al, 2018;Granot et al, 2018b;Lamb and Kobayashi, 2018;Lazzati et al, 2018;Fraija et al, 2019a;Fraija et al, 2019b;Beniamini et al, 2020b;Oganesyan et al, 2020). However, a radially stratified spherical outflow could reproduce the observations as well, albeit at the price of adding a never observed before component to the models (Li et al, 2018;Mooley et al, 2018c;Nakar and Piran, 2018;Salafia et al, 2018).…”

Section: The Afterglowmentioning

confidence: 76%

Short Duration Gamma-Ray Bursts and Their Outflows in Light of GW170817

Lazzati

2020

Front. Astron. Space Sci.

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Radio Emission from the Cocoon of a GRB Jet: Implications for Relativistic Supernovae and Off-axis GRB Emission

Cited by 25 publications

References 51 publications

Relativistic supernova 2009bb exploded close to an atomic gas cloud

Relativistic supernova 2009bb exploded close to an atomic gas cloud

Broad-line type Ic SN 2020bvc

Short Duration Gamma-Ray Bursts and Their Outflows in Light of GW170817

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