SUPER-LUMINOUS TYPE Ic SUPERNOVAE: CATCHING A MAGNETAR BY THE TAIL

Inserra, C.; Smartt, S. J.; Jerkstrand, A.; Valenti, S.; Fraser, M.; Wright, D. E.; Smith, Kenneth; Chen, Ting-Wan; Kotak, R.; Pastorello, A.; Nicholl, M.; Bresolin, Fabio; Kudritzki, R. P.; Benetti, S.; Botticella, M. T.; Burgett, W. S.; Chambers, K.; Ergon, M.; Flewelling, H.; Fynbo, J. P. U.; Geier, S.; Hodapp, Klaus W.; Howell, D. A.; Huber, M. E.; Kaiser, Nick; Leloudas, G.; Magill, L.; Magnier, E. A.; McCrum, M.; Metcalfe, N.; Price, P. A.; Rest, A.; Sollerman, J.; Sweeney, William E.; Taddia, F.; Taubenberger, S.; Tonry, J.; Wainscoat, R. J.; Waters, C.; Young, D. R.

doi:10.1088/0004-637x/770/2/128

Cited by 387 publications

(711 citation statements)

References 82 publications

(159 reference statements)

Supporting

Mentioning

662

Contrasting

Unclassified

Order By: Relevance

“…There were attempts to reproduce the light curve of SN 1998bw by a pure-magnetar model and pure-56 Ni model ( Figure 19 of Inserra et al 2013). The failure of these models calls for alternative models for SNe Ic-BL, manifesting the investigation of magnetar plus 56 Ni model presented in this work.…”

Section: Discussionmentioning

confidence: 92%

“…If one focuses on the data within one year after explosion, the t −2 tail in the magnetar model easily parallels that expected from 56 Co decay and one cannot unambiguously tell if it is the magnetar or 56 Co that is powering the light curve (Woosley 2010;Inserra et al 2013). Only at very late phases can one distinguish between magnetar model and 56 Co decay model.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Wang

Liu

et al. 2017

ApJ

View full text Add to dashboard Cite

Broad-lined type Ic supernovae (SNe Ic-BL) are peculiar stellar explosions that distinguish themselves from ordinary SNe. Some SNe Ic-BL are associated with long-duration ( 2 s) gamma-ray bursts (GRBs). Black holes and magnetars are two types of compact objects that are hypothesized to be central engines of GRBs. In spite of decades of investigations, no direct evidence for the formation of black holes or magnetars has been found for GRBs so far. Here we report the finding that the early peak (t 50 days) and late-time (t 300 days) slow decay displayed in the light curves of both SNe 1998bw (associated with GRB 980425) and 2002ap (not GRB-associated) can be attributed to magnetar spin-down with initial rotation period P 0 ∼ 20 ms, while the intermediate-time (50 t 300 days) exponential decline is caused by radioactive decay of 56 Ni. The connection between the early peak and late-time slow decline in the light curves is unexpected in alternative models. We thus suggest that GRB 980425 and SN 2002ap were powered by magnetars.

show abstract

Section: Discussionmentioning

confidence: 92%

Section: Introductionmentioning

confidence: 99%

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Wang

Liu

et al. 2017

ApJ

View full text Add to dashboard Cite

show abstract

“…The first is that of SLSNe, which do not generally exhibit hydrogen or helium lines in spectra and show no spectral signatures of interaction between fast moving ejecta and circumstellar shells, and thus are classified as SLSNe type I or type Ic (e.g. Pastorello et al 2010;Quimby et al 2011;Chomiuk et al 2011;Inserra et al 2013;Howell et al 2013;Nicholl et al 2013). The lightcurves of SLSNe type I span a wide range of rise (∼ 15-40 d) and decline timescales (∼ 30-100 d).…”

Section: Introductionmentioning

confidence: 99%

“…Firstly, the millisecond magnetar model can reproduce a wide range of lightcurves, fitting both fast and slow decliners (e.g. Inserra et al 2013;Nicholl et al 2013); Chen et al (2015) found that the slowly-fading late-time lightcurve also fits a magnetar model well if the escape of high-energy gamma rays is taken into account (for time-varying leakage see Wang et al 2015). In contrast, the PISN model can only explain slowly-fading lightcurve events, such as SN 2007bi, which was initially suggested to be a PISN (Gal-Yam et al 2009) based on a 56 Co decay-like tail.…”

Section: Introductionmentioning

confidence: 99%

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

Chen

Nicholl

Smartt

et al. 2017

A&A

Self Cite

View full text Add to dashboard Cite

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.

show abstract

“…Most notably, estimates of Si II and Fe II conflict when 6000-6400 Å spectral features are interpreted to be dominated by Si II, while model spectra producing mostly signatures of Si II are consistently too blue in wavelength when compared with observations (cf. Mazzali et al 2000;Inserra et al 2013;Lyman et al 2016). …”

Section: Introductionmentioning

confidence: 99%

LINE IDENTIFICATIONS OF TYPE I SUPERNOVAE: ON THE DETECTION OF Si II FOR THESE HYDROGEN-POOR EVENTS

Parrent

Milisavljević

Söderberg

et al. 2016

ApJ

View full text Add to dashboard Cite

Here we revisit line identifications of type I supernovae (SNe I) and highlight trace amounts of unburned hydrogen as an important free parameter for the composition of the progenitor. Most one-dimensional stripped-envelope models of supernovae indicate that observed features near 6000-6400 Å in typeI spectra are due to more than Si IIλ6355. However, while an interpretation of conspicuous Si IIλ6355 can approximate 6150 Å absorption features for all SNe Ia during the first month of free expansion, similar identifications applied to 6250 Å features of SNe Ib and Ic have not been as successful. When the corresponding synthetic spectra are compared with highquality timeseries observations, the computed spectra are frequently too blue in wavelength. Some improvement can be achieved with Fe II lines that contribute redward of 6150 Å; however, the computed spectra either remain too blue or the spectrum only reaches a fair agreement when the rise-time to peak brightness of the model conflicts with observations by a factor of two. This degree of disagreement brings into question the proposed explosion scenario. Similarly, a detection of strong Si IIλ6355 in the spectra of broadlined Ic and super-luminous events of type I/R is less convincing despite numerous model spectra used to show otherwise. Alternatively, we suggest 6000-6400 Å features are possibly influenced by either trace amounts of hydrogen or blueshifted absorption and emission in Hα, the latter being an effect which is frequently observed in the spectra of hydrogen-rich, SNe II.

show abstract

SUPER-LUMINOUS TYPE Ic SUPERNOVAE: CATCHING A MAGNETAR BY THE TAIL

Cited by 387 publications

References 82 publications

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

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

LINE IDENTIFICATIONS OF TYPE I SUPERNOVAE: ON THE DETECTION OF Si II FOR THESE HYDROGEN-POOR EVENTS

Contact Info

Product

Resources

About