Light Curves of Hydrogen-poor Superluminous Supernovae from the Palomar Transient Factory

De, A.; Gal‐Yam, A.; Rubin, A.; Leloudas, G.; Vreeswijk, P. M.; Perley, D. A.; Quimby, R.; Yan, Lin; Sullivan, M.; Flörs, Andreas; Sollerman, J.; Bersier, D.; Cenko, S. Bradley; Gal-Yam, M.; Maguire, K.; Ofek, E. O.; Prentice, S.; Schulze, S.; Spyromilio, J.; Valenti, S.; Arcavi, I.; Corsi, A.; Howell, D. A.; Mazzali, P. A.; Kasliwal, M. M.; Taddia, F.; Yaron, O.

doi:10.3847/1538-4357/aab9b6

Cited by 139 publications

(142 citation statements)

References 120 publications

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“…This remains a controversial issue, to which SN 2017egm may bring some clarity. The slowly-declining SLSN I are often characterized by irregularities in the light curve that are most straightforwardly attributed to CSI (De Cia et al 2017). If a class of SLSN or a single example in the case of SN 2017egm argue for CSI despite the lack of narrow lines, then the implication of the lack of narrow lines must be reconsidered in all SLSN I.…”

Section: Discussionmentioning

confidence: 99%

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Circumstellar Interaction Models for the Bolometric Light Curve of Type I Superluminous SN 2017egm

Wheeler

Chatzopoulos

Vinkó

et al. 2017

ApJL

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We explore simple semi-analytic fits to the bolometric light curve of Gaia17biu/SN 2017egm, the most nearby hydrogen-deficient superluminous supernova (SLSN I) yet discovered. SN 2017egm has a quasi-bolometric light curve that is uncharacteristic of other SLSN I by having a nearly linear rise to maximum and decline from peak, with a very sharp transition. Magnetar models have difficulty explaining the sharp peak and may tend to be too bright 20 d after maximum. Light curves powered only by radioactive decay of 56 Ni fail on similar grounds and because they demand greater nickel mass than ejecta mass. Simple models based on circumstellar interaction do have a sharp peak corresponding to the epoch when the forward shock breaks out of the optically-thick circumstellar medium or the reverse shock reaches the inside of the ejecta. We find that models based on circumstellar interaction with a constant-density shell provide an interesting fit to the bolometric light curve from 15 d before to 15 d after peak light of SN 2017egm and that both magnetar and radioactive decay models fail to fit the sharp peak. Future photometric observations should easily discriminate basic CSI models from basic magnetar models. The implications of a CSI model are briefly discussed.

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Section: Discussionmentioning

confidence: 99%

“…Its peak brightness is on the low end of the distribution of SLSN I (De Cia et al 2017;Lunnan et al 2017) with a maximum of M ≈ -21. Even more interesting, perhaps, is the nature of the light curve.…”

Section: Introductionmentioning

confidence: 99%

Circumstellar Interaction Models for the Bolometric Light Curve of Type I Superluminous SN 2017egm

Wheeler

Chatzopoulos

Vinkó

et al. 2017

ApJL

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“…Inserra & Smartt 2014;Nicholl et al 2015;Inserra et al 2017b;Lunnan et al 2017), current surveys are starting to populate the lower luminosity end creating a continuum in luminosity between normal and superluminous SNe (see De Cia et al 2017).…”

Section: Methodsmentioning

confidence: 99%

Euclid: Superluminous supernovae in the Deep Survey

Inserra

Nichol

Scovacricchi

et al. 2018

A&A

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Context. In the last decade, astronomers have found a new type of supernova called 'superluminous supernovae' (SLSNe) due to their high peak luminosity and long light-curves. These hydrogen-free explosions (SLSNe-I) can be seen to z ∼ 4 and therefore, offer the possibility of probing the distant Universe. Aims. We aim to investigate the possibility of detecting SLSNe-I using ESA's Euclid satellite, scheduled for launch in 2020. In particular, we study the Euclid Deep Survey (EDS) which will provide a unique combination of area, depth and cadence over the mission. Methods. We estimated the redshift distribution of Euclid SLSNe-I using the latest information on their rates and spectral energy distribution, as well as known Euclid instrument and survey parameters, including the cadence and depth of the EDS. To estimate the uncertainties, we calculated their distribution with two different set-ups, namely optimistic and pessimistic, adopting different star formation densities and rates. We also applied a standardization method to the peak magnitudes to create a simulated Hubble diagram to explore possible cosmological constraints. Results. We show that Euclid should detect approximately 140 high-quality SLSNe-I to z ∼ 3.5 over the first five years of the mission (with an additional 70 if we lower our photometric classification criteria). This sample could revolutionize the study of SLSNe-I at z > 1 and open up their use as probes of star-formation rates, galaxy populations, the interstellar and intergalactic medium. In addition, a sample of such SLSNe-I could improve constraints on a time-dependent dark energy equation-of-state, namely w(a), when combined with local SLSNe-I and the expected SN Ia sample from the Dark Energy Survey. Conclusions. We show that Euclid will observe hundreds of SLSNe-I for free. These luminous transients will be in the Euclid data-stream and we should prepare now to identify them as they offer a new probe of the high-redshift Universe for both astrophysics and cosmology.

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“…It seems unlikely that for all three events Δt exp values are systematically overestimated by a factor of 2, which would make the true rise times for Gaia16apd and SN2017egm ∼15 days. This is too short for an SLSN-I (Nicholl et al 2015;De Cia et al 2017), making this explanation unlikely. Another possibility is that the assumption of T BB =T eff is no longer valid, with T eff T BB , which would imply a larger photospheric radius R and v phot .…”

Section: Tablementioning

confidence: 99%

“…More recently, De Cia et al (2017) and Nicholl et al (2017c) computed magnetar model parameters for a large sample of SLSNe-I by applying a single SED template to broadband LCs. This SED template is derived for the purpose of fitting broadband photometry.…”

Section: Introductionmentioning

confidence: 99%

Far-UV HST Spectroscopy of an Unusual Hydrogen-poor Superluminous Supernova: SN2017egm

Yan

Perley

et al. 2018

ApJ

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SN2017egm is the closest (z=0.03) H-poor superluminous supernova (SLSN-I) detected to date, and a rare example of an SLSN-I in a massive, metal-rich galaxy. We present the HST UV and optical spectra covering 1000-5500 Å, taken at +3 day relative to the peak. Our data reveal two absorption systems at redshifts matching the host galaxy NGC 3191 (z=0.0307) and its companion galaxy (z=0.0299) 73″ apart. Weakly damped Lyα absorption lines are detected at these two redshifts, with H I column densities of (3.0±0.8)×1019 and (3.7±0.9)×1019 cm −2 , respectively. This is an order of magnitude smaller than the H I column densities in the disks of nearby galaxies (>10 10 M e ) and suggests that SN2017egm is on the near side of NGC 3191 and has a low host extinction (E(B−V )∼0.007). Using unsaturated metal absorption lines, we find that the host of SN2017egm probably has a solar or higher metallicity and is unlikely to be a dwarf companion to NGC 3191. Comparison of early-time UV spectra of SN2017egm, Gaia16apd, iPTF13ajg, and PTF12dam finds that the continuum at λ>2800 Å is well fit by a blackbody, whereas the continuum at λ<2800 Å is considerably below the model. The degree of UV suppression varies from source to source, with the 1400-2800 Å continuum flux ratio of 1.5 for Gaia16apd and 0.4 for iPTF13ajg. This cannot be explained by the differences in magnetar power or blackbody temperature. Finally, the UV spectra reveal a common set of seven broad absorption features and their equivalent widths are similar (within a factor of 2) among the four events.

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Light Curves of Hydrogen-poor Superluminous Supernovae from the Palomar Transient Factory

Cited by 139 publications

References 120 publications

Circumstellar Interaction Models for the Bolometric Light Curve of Type I Superluminous SN 2017egm

Circumstellar Interaction Models for the Bolometric Light Curve of Type I Superluminous SN 2017egm

Euclid: Superluminous supernovae in the Deep Survey

Far-UV HST Spectroscopy of an Unusual Hydrogen-poor Superluminous Supernova: SN2017egm

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