dc.contributor.author |
Amit Kumar |
|
dc.contributor.author |
Brajesh Kumar |
|
dc.contributor.author |
Pandey, S. B |
|
dc.contributor.author |
Sahu, D. K |
|
dc.contributor.author |
Singh, A |
|
dc.contributor.author |
Anupama, G. C |
|
dc.contributor.author |
Aryan, Amar |
|
dc.contributor.author |
Gupta, Rahul |
|
dc.contributor.author |
Anirban Dutta |
|
dc.contributor.author |
Misra, K |
|
dc.date.accessioned |
2021-07-02T10:46:19Z |
|
dc.date.available |
2021-07-02T10:46:19Z |
|
dc.date.issued |
2021-04 |
|
dc.identifier.citation |
Monthly Notices of the Royal Astronomical Society, Vol. 502, No. 2, pp. 1678–1693 |
en_US |
dc.identifier.issn |
1365-2966 |
|
dc.identifier.uri |
http://hdl.handle.net/2248/7766 |
|
dc.description |
Restricted Access |
en_US |
dc.description.abstract |
We investigate the observational properties of a hydrogen-deficient superluminous supernova (SLSN) SN 2020ank (at z = 0.2485), with the help of early phase observations carried out between –21 and +52 d since g-band maximum. Photometrically, SN 2020ank is one of the brightest SLSN (Mg,peak∼ –21.84 ± 0.10 mag), having fast pre-peak rising and post-peak decaying rates. The bolometric light curve of SN 2020ank exhibits a higher peak luminosity (Lmax) of ∼ (3.9 ± 0.7) × 1044 erg s−1 and appears to be symmetric around the peak with Lrisemax/e ≈Lfallmax/e ≈ 15 d. The semi-analytical light-curve modelling using the minim code suggests a spin-down millisecond magnetar with Pi∼ 2.2 ± 0.5 ms and B∼ (2.9 ± 0.1) ×1014 G as a possible powering source for SN 2020ank. The possible magnetar origin and excess ultraviolet flux at early epochs indicate a central-engine based powering source for SN 2020ank. Near-peak spectra of SN 2020ank are enriched with the W-shaped O II features but with the weaker signatures of C II and Fe III. Using the estimated rise time of ∼ 27.9 d and the photospheric velocity of ∼ 12 050 km s−1, we constrain the ejecta mass to ∼ 7.2 M⊙ and the kinetic energy of ∼6.3 × 1051 erg. The near-peak spectrum of SN 2020ank exhibits a close spectral resemblance with that of fast-evolving SN 2010gx. The absorption features of SN 2020ank are blueshifted compared to Gaia16apd, suggesting a higher expansion velocity. The spectral similarity with SN 2010gx and comparatively faster spectral evolution than PTF12dam (a slow-evolving SLSN) indicate the fast-evolving behaviour of SN 2020ank. |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
Oxford University Press on behalf of the Royal Astronomical Society |
en_US |
dc.relation.uri |
https://doi.org/10.1093/mnras/staa4047 |
|
dc.rights |
© The Royal Astronomical Society |
|
dc.subject |
Techniques: photometric |
en_US |
dc.subject |
Techniques: spectroscopic |
en_US |
dc.subject |
Supernovae: general |
en_US |
dc.subject |
Supernovae: individual: SN 2020ank |
en_US |
dc.title |
SN 2020ank: a bright and fast-evolving H-deficient superluminous supernova |
en_US |
dc.type |
Article |
en_US |