Obscured Star Formation in the Host Galaxies of Superluminous Supernovae

Hatsukade, Bunyo; Tominaga, Nozomu; Hayashi, Masao; Konishi, Masahiro; Matsuda, Yoshihisa; Morokuma, Tomoki; Morokuma-Matsui, Kana; Motogi, Kazuhito; Niinuma, Kotaro; Tamura, Motohide

doi:10.3847/1538-4357/aab616

Cited by 22 publications

(29 citation statements)

References 65 publications

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“…Here we report the VLA detection of an unresolved radio source coincident with the location of the SLSN PTF10hgi (z = 0.098; Inserra et al 2013;Perley et al 2016;De Cia et al 2018) about 7.5 years post-explosion. This represents the first detection of radio emission coincident with a known SLSN on any timescale (e.g., Coppejans et al 2018;Hatsukade et al 2018). We investigate the various possible origins of the radio emission -star formation activity, AGN, SN blastwave, and an off-axis jet -and show that none are likely, although in each scenario such an origin would represent an exciting and novel result.…”

Section: Introductionmentioning

confidence: 82%

A Radio Source Coincident with the Superluminous Supernova PTF10hgi: Evidence for a Central Engine and an Analog of the Repeating FRB 121102?

Eftekhari

Berger

Margalit

et al. 2019

ApJL

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We present the detection of an unresolved radio source coincident with the position of the Type I superluminous supernova (SLSN) PTF10hgi (z = 0.098) about 7.5 years post-explosion, with a luminosity of L ν (6 GHz) ≈ 1.1 × 10 28 erg s −1 Hz −1 . This represents the first detection of radio emission coincident with a SLSN on any timescale. We investigate various scenarios for the origin of the radio emission: star formation activity, an active galactic nucleus, an off-axis jet, and a non-relativistic supernova blastwave. While any of these would be quite novel if confirmed, none appear likely when taken in context of the other properties of the host galaxy, previous radio observations of SLSNe, the sample of long gamma-ray bursts (LGRBs), and the general population of hydrogen-poor SNe. Instead, the radio emission is reminiscent of the quiescent radio source associated with the repeating FRB121102, which has been argued to be powered by a magnetar born in a SLSN or LGRB explosion several decades ago. We show that such a central engine powered nebula is consistent with the age and luminosity of the radio source. Our directed search for FRBs from the location of PTF10hgi using 40 min of VLA phased-array data reveals no detections to a limit of 22 mJy (7σ; 10 ms duration). We outline several follow-up observations that can conclusively establish the origin of the radio emission.

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Section: Introductionmentioning

confidence: 82%

A Radio Source Coincident with the Superluminous Supernova PTF10hgi: Evidence for a Central Engine and an Analog of the Repeating FRB 121102?

Eftekhari

Berger

Margalit

et al. 2019

ApJL

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“…It is usually reported that superluminous supernovae are characterized by absolute luminosities at maximum light of MAB ≲ −21 mag, total radiated energies of the order of 10 51 erg [10] and a preference for low-metallicity, star-forming environments [11,12,13,14,15,16]. There are two broad classes: SLSNe II, which exhibit signatures of hydrogen in their optical spectra, and SLSNe I, which do not.…”

Section: -Superluminous Supernovaementioning

confidence: 99%

Observational properties of extreme supernovae

Inserra

2019

Nat Astron

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The last ten years have opened up a new parameter space in time-domain astronomy with the discovery of transients defying our understanding of how stars explode. These extremes of the transient paradigm represent the brightest -called superluminous supernova -and the fastest -known as fast, blue optical transients -of the transient zoo. The number of their discoveries and information gained per event have witnessed an exponential growth that has benefited observational and theoretical studies. The collected dataset and the understanding of such events have surpassed any initial expectation and opened up a future exploding with potential, spanning from novel tools of high-redshift cosmological investigation to new insights into the final stages of massive stars. Here, the observational properties of extreme supernovae are reviewed and put in the context of their physics, possible progenitor scenarios and explosion mechanisms.Portraying the landscape of extreme transients is not a trivial task. Almost a decade ago astronomers discovered transients defying the standard paradigm of stellar explosion. Their luminosity and evolution cannot be explained by the two classical mechanisms of core-collapse[1] and thermonuclear[2] explosions. Their observables, altogether, cannot be overall explained by the interaction between an ejected expanding medium (i.e. ejecta) and a circum-stellar material (CSM) previously expelled by the dying star (e.g. IIn/Ibn supernovae), nor by what is expected and observed in Tidal Disruption Events (TDEs), where a star is gravitationally disrupted by a black hole. In the transient parameter space of peak luminosity versus rise-time ( Fig. 1) extreme transients lie above the lines representing the maximum possible luminosity from a standard supernova (SN) explosion.Such limits are determined using the standard diffusion formalism[3] and the maximum ratio of 56 Ni mass with respect to that of the ejecta as derived from theoretical [4] and observational studies

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“…We selected the oldest ten SLSN-I from the first large sample with well-characterized host galaxies Schulze et al (2018). b Late-time radio limit at 3 GHz by Hatsukade et al (2018).…”

Section: Observationsmentioning

confidence: 99%

A Search for Late-time Radio Emission and Fast Radio Bursts from Superluminous Supernovae

Law

Omand

Kashiyama

et al. 2019

ApJ

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We present results of a search for late-time radio emission and Fast Radio Bursts (FRBs) from a sample of type-I superluminous supernovae (SLSNe-I). We used the Karl G. Jansky Very Large Array to observe ten SLSN-I more than 5 years old at a frequency of 3 GHz. We searched fast-sampled visibilities for FRBs and used the same data to perform a deep imaging search for late-time radio emission expected in models of magnetar-powered supernovae. No FRBs were found. One SLSN-I, PTF10hgi, is detected in deep imaging, corresponding to a luminosity of 1.2 × 10 28 erg s −1 . This luminosity, considered with the recent 6 GHz detection of PTF10hgi in Eftekhari et al. (2019), supports the interpretation that it is powered by a young, fast-spinning (∼ ms spin period) magnetar with ∼ 15 M of partially ionized ejecta. Broadly, our observations are most consistent with SLSNe-I being powered by neutron stars with fast spin periods, although most require more free-free absorption than is inferred for PTF10hgi. We predict that radio observations at higher frequencies or in the near future will detect these systems and begin constraining properties of the young pulsars and their birth environments.

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Obscured Star Formation in the Host Galaxies of Superluminous Supernovae

Cited by 22 publications

References 65 publications

A Radio Source Coincident with the Superluminous Supernova PTF10hgi: Evidence for a Central Engine and an Analog of the Repeating FRB 121102?

A Radio Source Coincident with the Superluminous Supernova PTF10hgi: Evidence for a Central Engine and an Analog of the Repeating FRB 121102?

Observational properties of extreme supernovae

A Search for Late-time Radio Emission and Fast Radio Bursts from Superluminous Supernovae

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