SUPERLUMINOUS SUPERNOVA SN 2015bn IN THE NEBULAR PHASE: EVIDENCE FOR THE ENGINE-POWERED EXPLOSION OF A STRIPPED MASSIVE STAR

Nicholl, M.; Berger, E.; Margutti, R.; Chornock, R.; Blanchard, P. K.; Jerkstrand, A.; Smartt, S. J.; Arcavi, I.; Challis, P.; Chambers, K.; Chen, Ting-Wan; Cowperthwaite, P. S.; Gal‐Yam, A.; Hosseinzadeh, G.; Howell, D. A.; Inserra, C.; Kankare, E.; Magnier, E. A.; Maguire, K.; Mazzali, P. A.; McCully, C.; Milisavljevic, Dan; Smith, K.; Taubenberger, S.; Valenti, S.; Wainscoat, R. J.; Yaron, O.; Young, D. R.

doi:10.3847/2041-8205/828/2/l18

Cited by 108 publications

(129 citation statements)

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“…Jerkstrand et al (2017);Nicholl et al (2016a) pointed out that the late-time spectrum of the SLSN SN 2015bn is very similar to SN 1998bw. Since our FORS2 spectrum shows that LSQ14mo is less than five times more luminous than SN 1998bw at late phases, this suggests an upper limit for the nickel mass of five times the nickel mass in SN 1998bw.…”

Section: Late-time Spectrum Of Lsq14mo Compared To Sn 1998bwmentioning

confidence: 99%

“…Instead, the similarity of the late-time nebular spectra of a number of energetic SNe Ic (e.g. SN 1998bw) and those of SLSNe has been identified by Jerkstrand et al (2017); Nicholl et al (2016a). Jerkstrand et al (2017) find that at least 10M of oxygen is required in the ejecta to produce the strong [O i] lines and that the material must be highly clumped.…”

Section: Introductionmentioning

confidence: 99%

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The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

Chen

Nicholl

Smartt

et al. 2017

A&A

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We present and analyse an extensive dataset of the superluminous supernova (SLSN) LSQ14mo (z = 0.256), consisting of a multicolour lightcurve from −30 d to +70 d in the rest-frame (relative to maximum light) and a series of six spectra from PESSTO covering −7 d to +50 d. This is among the densest spectroscopic coverage, and best-constrained rising lightcurve, for a fast-declining hydrogenpoor SLSN. The bolometric lightcurve can be reproduced with a millisecond magnetar model with ∼ 4 M ejecta mass, and the temperature and velocity evolution is also suggestive of a magnetar as the power source. Spectral modelling indicates that the SN ejected ∼ 6 M of CO-rich material with a kinetic energy of ∼ 7 × 10 51 erg, and suggests a partially thermalised additional source of luminosity between −2 d and +22 d. This may be due to interaction with a shell of material originating from pre-explosion mass loss. We further present a detailed analysis of the host galaxy system of LSQ14mo. PESSTO and GROND imaging show three spatially resolved bright regions, and we used the VLT and FORS2 to obtain a deep (five-hour exposure) spectra of the SN position and the three star-forming regions, which are at a similar redshift. The FORS spectrum at +300 days shows no trace of SN emission lines and we place limits on the strength of [O i] from comparisons with other Ic supernovae. The deep spectra provides a unique chance to investigate spatial variations in the host star-formation activity and metallicity. The specific star-formation rate is similar in all three components, as is the presence of a young stellar population. However, the position of LSQ14mo exhibits a lower metallicity, with 12 + log(O/H) = 8.2 in both the R 23 and N2 scales (corresponding to ∼ 0.3 Z ). We propose that the three bright regions in the host system are interacting, which thus triggers star formation and forms young stellar populations.

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Section: Late-time Spectrum Of Lsq14mo Compared To Sn 1998bwmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

Chen

Nicholl

Smartt

et al. 2017

A&A

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“…X-ray observations of the SLSN-I 2015bn (Nicholl et al 2016a(Nicholl et al , 2016b 1´-. Black filled circles: X-ray luminosity limits from Swift-XRT.…”

Section: Sn 2015bnmentioning

confidence: 99%

Results from a Systematic Survey of X-Ray Emission from Hydrogen-poor Superluminous SNe

Margutti

Chornock

Metzger

et al. 2018

ApJ

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We present the results from a sensitive X-ray survey of 26 nearby hydrogen-poor superluminous supernovae (SLSNe-I) with Swift, Chandra, and XMM. This data set constrains the SLSN evolution from a few days until ∼2000 days after explosion, reaching a luminosity limit L x ∼10 40 erg s −1 and revealing the presence of significant X-ray emission possibly associated with PTF 12dam. No SLSN-I is detected above L 10 erg s-, suggesting that the luminous X-ray emission L x ∼10 45 erg s −1 associated with SCP 60F6 is not common among SLSNe-I. We constrain the presence of off-axis gamma-ray burst (GRB) jets, ionization breakouts from magnetar engines and the density in the sub-parsec environments of SLSNe-I through inverse Compton emission. The deepest limits rule out the weakest uncollimated GRB outflows, suggesting that if the similarity of SLSNe-I with GRB/SNe extends to their fastest ejecta, then SLSNe-I are either powered by energetic jets pointed far away from our line of sight (θ>30°), or harbor failed jets that do not successfully break through the stellar envelope. Furthermore, if a magnetar central engine is responsible for the exceptional luminosity of SLSNe-I, our X-ray analysis favors large magnetic fields B 2 10 14 >´G and ejecta masses M M 3 ej > ☉ , in agreement with optical/UV studies. Finally, we constrain the pre-explosion mass-loss rate of stellar progenitors of SLSNe-I. For PTF 12dam we infer M M 2 10 yr 5 1 <´--☉, suggesting that the SN shock interaction with an extended circumstellar medium is unlikely to supply the main source of energy powering the optical transient and that some SLSN-I progenitors end their lives as compact stars surrounded by a low-density medium similar to long GRBs and type Ib/c SNe.

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“…8), even 56 Ni-powered LCs may not exactly follow the 56 Co decay because of asphericity. Latephase spectra can also be a way to distinguish them (e.g., Mazzali et al 2001;Gal-Yam et al 2009;Dessart et al 2012;Jerkstrand et al 2016a,b;Nicholl et al 2016b). Observations in X-rays and γ-rays may also distinguish the two energy sources (e.g., Levan et al 2013;Metzger et al 2014).…”

Section: Magnetar Vsmentioning

confidence: 99%

Properties of Magnetars Mimicking ⁵⁶Ni-Powered Light Curves in Type IC Superluminous Supernovae

Moriya

Chen

Langer

2017

ApJ

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Many Type Ic superluminous supernovae have light-curve decline rates after their luminosity peak which are close to the nuclear decay rate of 56 Co, consistent with the interpretation that they are powered by 56 Ni and possibly pair-instability supernovae. However, their rise times are typically shorter than those expected from pair-instability supernovae, and Type Ic superluminous supernovae are often suggested to be powered by magnetar spin-down. If magnetar spin-down is actually a major mechanism to power Type Ic superluminous supernovae, it should be able to produce decline rates similar to the 56 Co decay rate rather easily. In this study, we investigate the conditions for magnetars under which their spin-down energy input can behave like the 56 Ni nuclear decay energy input. We find that an initial magnetic field strength within a certain range is sufficient to keep the magnetar energy deposition within a factor of a few of the 56 Co decay energy for several hundreds of days. Magnetar spin-down needs to be by almost pure dipole radiation with the braking index close to 3 to mimic 56 Ni in a wide parameter range. Not only late-phase 56 Co-decay-like light curves, but also rise time and peak luminosity of most 56 Ni-powered light curves can be reproduced by magnetars. Bolometric light curves for more than 700 days are required to distinguish the two energy sources solely by them. We expect that more slowly-declining superluminous supernovae with short rise times should be found if they are mainly powered by magnetar spin-down.

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SUPERLUMINOUS SUPERNOVA SN 2015bn IN THE NEBULAR PHASE: EVIDENCE FOR THE ENGINE-POWERED EXPLOSION OF A STRIPPED MASSIVE STAR

Cited by 108 publications

References 50 publications

The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

Results from a Systematic Survey of X-Ray Emission from Hydrogen-poor Superluminous SNe

Properties of Magnetars Mimicking ⁵⁶Ni-Powered Light Curves in Type IC Superluminous Supernovae

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SUPERLUMINOUS SUPERNOVA SN 2015bn IN THE NEBULAR PHASE: EVIDENCE FOR THE ENGINE-POWERED EXPLOSION OF A STRIPPED MASSIVE STAR

Cited by 108 publications

References 50 publications

The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

The evolution of superluminous supernova LSQ14mo and its interacting host galaxy system

Results from a Systematic Survey of X-Ray Emission from Hydrogen-poor Superluminous SNe

Properties of Magnetars Mimicking 56Ni-Powered Light Curves in Type IC Superluminous Supernovae

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Product

Resources

About

Properties of Magnetars Mimicking ⁵⁶Ni-Powered Light Curves in Type IC Superluminous Supernovae