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  • 1
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    The Carnegie Supernova Project II (2020)
    EDP Sciences
    Details
    Publication Date: 2020-09-01
    Description: We present optical and near-infrared photometry and spectroscopy of the Type IIn supernova, (SN) 2014ab, obtained by the Carnegie Supernova Project II and initiated immediately after its optical discovery. We also study public mid-infrared photometry obtained by the Wide-field Infrared Survey Explorer satellite extending from 56 days prior to the optical discovery to over 1600 days. The light curve of SN 2014ab evolves slowly, while the spectra exhibit strong emission features produced from the interaction between rapidly expanding ejecta and dense circumstellar matter. The light curve and spectral properties are very similar to those of SN 2010jl. The estimated mass-loss rate of the progenitor of SN 2014ab is of the order of 0.1 M⊙ yr−1 under the assumption of spherically symmetric circumstellar matter and steady mass loss. Although the mid-infrared luminosity increases due to emission from dust, which is characterized by a blackbody temperature close to the dust evaporation temperature (∼2000 K), there were no clear signatures of in situ dust formation observed within the cold dense shell located behind the forward shock in SN 2014ab in the early phases. Mid-infrared emission of SN 2014ab may originate from pre-existing dust located within dense circumstellar matter that is heated by the SN shock or shock-driven radiation. Finally, for the benefit of the community, we also present five near-infrared spectra of SN 2010jl obtained between 450 to 1300 days post-discovery in the appendix.
    Print ISSN: 0004-6361
    Electronic ISSN: 1432-0746
    Topics: Physics
    Published by EDP Sciences
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  • 2
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    Rapidly evolving faint transients from stripped-envelope electron-capture supernovae (2016)
    Oxford University Press
    Details
    Publication Date: 2016-07-13
    Description: We investigate the expected rates and bolometric light-curve properties of stripped-envelope electron-capture supernovae (ECSNe) using stellar models from the Binary Population and Spectral Synthesis code. We find that 0.8 per cent ( Z = 0.020) and 1.2 per cent ( Z = 0.004) of core-collapse supernovae are stripped-envelope ECSNe. Their typical ejecta masses are estimated to be about 0.3 M ( Z = 0.020) and 0.6 M ( Z = 0.004). Assuming ECSN explosion properties from numerical explosion simulations, an explosion energy of 1.5 x 10 50 erg and a 56 Ni mass of 2.5 x 10 –3 M , we find that stripped-envelope ECSNe have a typical rise time of around 7 d ( Z = 0.020) or 13 d ( Z = 0.004) and peak luminosity of around 10 41 ergs –1 (–13.8 mag, Z = 0.020) or 7 x 10 40 erg s –1 (–13.4 mag, Z = 0.004). Their typical ejecta velocities are around 7000 km s –1 ( Z = 0.020) or 5000 km s –1 ( Z = 0.004). Thus, stripped-envelope ECSNe are observed as rapidly evolving faint transients with relatively small velocities. SN 2008ha-like supernovae, which are the faintest kind of SN 2002cx-like (also known as Type Iax) supernovae, may be related to stripped-envelope ECSNe.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 3
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    Constraining the ellipticity of strongly magnetized neutron stars powering superluminous supernovae (2016)
    Oxford University Press
    Details
    Publication Date: 2016-05-07
    Description: Superluminous supernovae (SLSNe) have been suggested to be powered by strongly magnetized, rapidly rotating neutron stars which are often called magnetars. In this process, rotational energy of the magnetar is radiated via magnetic dipole radiation and heats the supernova ejecta. However, if magnetars are highly distorted in their geometric shape, rotational energy is mainly lost as gravitational wave radiation and thus such magnetars cannot power SLSNe. By simply comparing electromagnetic and gravitational wave emission time-scales, we constrain upper limits to the ellipticity of magnetars by assuming that they power the observed SLSNe. We find that their ellipticity typically needs to be less than about a few 10 –3 . This indicates that the toroidal magnetic field strengths in these magnetars are typically less than a few 10 16 G so that their distortions remain small. Because light-curve modelling of SLSNe shows that their dipole magnetic field strengths are of the order of 10 14 G, the ratio of poloidal to toroidal magnetic field strengths is found to be larger than ~0.01 in magnetars powering SLSNe.
    Print ISSN: 1745-3925
    Electronic ISSN: 1745-3933
    Topics: Physics
    Published by Oxford University Press
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  • 4
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    An analytic bolometric light curve model of interaction-powered supernovae and its application to Type IIn supernovae (2013)
    Oxford University Press
    Details
    Publication Date: 2013-09-26
    Description: We present an analytic model for bolometric light curves which are powered by the interaction between supernova ejecta and a dense circumstellar medium. This model is aimed at modelling Type IIn supernovae to determine the properties of their supernova ejecta and circumstellar medium. Our model is not restricted to the case of steady mass loss and can be applied broadly. We only consider the case in which the optical depth of the unshocked circumstellar medium is not high enough to affect the light curves. We derive the luminosity evolution based on an analytic solution for the evolution of a dense shell created by the interaction. We compare our model bolometric light curves to observed bolometric light curves of three Type IIn supernovae (2005ip, 2006jd, 2010jl) and show that our model can constrain their supernova ejecta and circumstellar medium properties. Our analytic model is supported by numerical light curves from the same initial conditions.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 5
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    Observable fractions of core-collapse supernova light curves brightened by binary companions (2015)
    Oxford University Press
    Details
    Publication Date: 2015-05-14
    Description: Many core-collapse supernova progenitors are presumed to be in binary systems. If a star explodes in a binary system, the early supernova light curve can be brightened by the collision of the supernova ejecta with the companion star. The early brightening can be observed when the observer is in the direction of the hole created by the collision. Based on a population synthesis model, we estimate the fractions of core-collapse supernovae in which the light-curve brightening by the collision can be observed. We find that 0.19 per cent of core-collapse supernova light curves can be observed with the collisional brightening. Type Ibc supernova light curves are more likely to be brightened by the collision (0.53 per cent) because of the high fraction of the progenitors being in binary systems and their proximity to the companion stars. Type II and IIb supernova light curves are less affected (~10 –3 and ~10 –2 per cent, respectively). Although the early, slow light-curve declines of some Type IIb and Ibc supernovae are argued to be caused by the collision with the companion star (e.g. SN 2008D), the small expected fraction, as well as the unrealistically small separation required, disfavour the argument. The future transient survey by the Large Synoptic Survey Telescope is expected to detect ~10 Type Ibc supernovae with the early collisional brightening per year, and they will be able to provide information on supernova progenitors in binary systems.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 6
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    Early ultraviolet signatures from the interaction of Type Ia supernova ejecta with a stellar companion (2015)
    Oxford University Press
    Details
    Publication Date: 2015-10-03
    Description: The progenitors of Type Ia supernovae (SNe Ia) are not yet fully understood. The two leading progenitor scenarios are the single-degenerate (SD) scenario and the double-degenerate scenario. In the SD scenario, the collision of the SN Ia ejecta with its companion star is expected to produce detectable ultraviolet (UV) emission in the first few days after the SN explosion within certain viewing angles. A strong UV flash has recently been detected in an SN 2002es-like peculiar SN Ia iPTF14atg by Cao et al., which is interpreted as evidence of an early-time UV signature due to SN ejecta interacting with its companion star, supporting the SD scenario. In this paper, we present the expected luminosity distributions of early-time UV emission arising from SN Ia ejecta–companion interaction by performing binary population synthesis calculations for different progenitor systems in the SD scenario. Our theoretical predictions will be helpful for future early-time observations of SNe Ia to constrain their possible progenitors. Assuming the observed strong UV pulse of iPTF14atg was indeed produced by the SN ejecta–companion interaction, our population synthesis model suggests that the progenitor system of iPTF14atg is most likely a red-giant donor binary system, and it is unlikely to have been a main-sequence or helium-star donor system.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 7
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    Detectability of high-redshift superluminous supernovae with upcoming optical and near-infrared surveys - II. Beyond z = 6 (2013)
    Oxford University Press
    Details
    Publication Date: 2013-10-08
    Description: Observational identification of the first stars is one of the great challenges in the modern astronomy. Although a single first star is too faint to be detected, supernova explosions of the first stars can be bright enough. An important question is whether such supernovae can be detected in the limited observational area with realistic observational resources. We perform detailed simulations to study the detectability of superluminous supernovae (SLSNe) at high redshifts, using the observationally calibrated star formation rate density and supernova occurrence rate. We show that a 100 deg 2 survey with the limiting magnitude of 26 mag in near-infrared wavelengths will be able to discover about 10 SLSNe at z 〉 10. If the survey is extended to 200 deg 2 with 27 mag depth, about 10 SLSNe can be discovered at z 〉 15. We emphasize that the observations at ≥3 μm are crucial to detect and select SLSNe at z 〉 10. Our simulations are also applied to the planned survey with Euclid , Wide-Field Infrared Survey Telescope ( WFIRST ) and Wide-field Imaging Surveyor for High-redshift ( WISH ). These surveys will be able to detect about 1000, 400 and 3000 SLSNe up to z  ~ 5, 7 and 12, respectively. We conclude that detection of SLSNe at z 〉 10 is in fact achievable in the near future.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 8
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    Mass-loss histories of Type IIn supernova progenitors within decades before their explosion (2014)
    Oxford University Press
    Details
    Publication Date: 2014-03-21
    Description: We present results of a systematic study of the mass-loss properties of Type IIn supernova progenitors within decades before their explosion. We apply an analytic light-curve model to 11 Type IIn supernova bolometric light curves to derive the circumstellar medium properties. We reconstruct the mass-loss histories based on the estimated circumstellar medium properties. The estimated mass-loss rates are mostly higher than 10 –3 M yr –1 and they are consistent with those obtained by other methods. The mass-loss rates are often found to be constantly high within decades before their explosion. This indicates that there exists some mechanism to sustain the high mass-loss rates of Type IIn supernova progenitors for at least decades before their explosion. Thus, the shorter eruptive mass-loss events observed in some Type IIn supernova progenitors are not always responsible for creating their dense circumstellar media. In addition, we find that Type IIn supernova progenitors may tend to increase their mass-loss rates as they approach to the time of their explosion. We also show a detailed comparison between our analytic prediction and numerical results.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 9
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    A hot and fast ultra-stripped supernova that likely formed a compact neutron star binary (2018)
    American Association for the Advancement of Science (AAAS)
    In: Science
    Details
    Publication Date: 2018-10-12
    Description: Compact neutron star binary systems are produced from binary massive stars through stellar evolution involving up to two supernova explosions. The final stages in the formation of these systems have not been directly observed. We report the discovery of iPTF 14gqr (SN 2014ft), a type Ic supernova with a fast-evolving light curve indicating an extremely low ejecta mass (0.2 solar masses) and low kinetic energy (2 x 10 50 ergs). Early photometry and spectroscopy reveal evidence of shock cooling of an extended helium-rich envelope, likely ejected in an intense pre-explosion mass-loss episode of the progenitor. Taken together, we interpret iPTF 14gqr as evidence for ultra-stripped supernovae that form neutron stars in compact binary systems.
    Keywords: Astronomy
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Geosciences , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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  • 10
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    Synthetic light curves of shocked dense circumstellar shells (2013)
    Oxford University Press
    Details
    Publication Date: 2013-03-02
    Description: We investigate numerically the light curves (LCs) of shocked circumstellar shells, which it has been suggested might reproduce the observed LC of superluminous SN 2006gy analytically. In the previous analytical model, the effects of recombination and bolometric correction on LCs were not taken into account. To see these effects, we perform numerical radiation hydrodynamic calculations of shocked shells using stella , which can treat multigroup radiation transfer numerically with realistic opacities. We show that the effects of recombination and bolometric correction are significant and that the analytical model should be compared with the bolometric LC rather than a single-band LC. We find that shocked circumstellar shells having a rapid LC decline initially because of adiabatic expansion, rather than luminosity increase, and these shocked shells fail to explain the LC properties of SN 2006gy. However, our synthetic LCs are qualitatively similar to those of superluminous SN 2003ma and SN 1988Z and the latter objects may be related to shocked circumstellar shells.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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