Gerhart Hauptmann der Schlesier

Reichart, Walter A.; Voigt, Felix A.

doi:10.2307/40093028

Cited by 3 publications

(3 citation statements)

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“…The EFOSC2 photometry was obtained using UBVR+griz filters, and was taken on the same nights as EFOSC2 spectroscopy. The EFOSC2 data were augmented by observations from other ground-based telescopes including the Panchromatic Robotic Optical Monitoring and Polarimetry Telescopes (PROMPT; Reichart et al 2005 (Smartt et al 2015) while the PROMPT, SMARTS and LCOGT images were reduced automatically by their respective instrument-specific pipelines.…”

Section: Datamentioning

confidence: 99%

On Type IIn/Ia-CSM supernovae as exemplified by SN 2012ca

Inserra

Fraser

Smartt

et al. 2016

Mon. Not. R. Astron. Soc.

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We present the complete set of ultra-violet, optical and near-infrared photometry and spectroscopy for SN 2012ca, covering the period from 6 days prior to maximum light, until 531 days after maximum. The spectroscopic time series for SN 2012ca is essentially unchanged over 1.5 years, and appear to be dominated at all epochs by signatures of interaction with a dense circumstellar medium rather than the underlying supernova (SN). At late phases, we see a near infrared excess in flux which is possibly associated with dust formation, although without any signs of accompanying line shifts. SN 2012ca is a member of the set of type of the ambiguous IIn/Ia-CSM SNe, the nature of which have been debated extensively in the literature. The two leading scenarios are either a type Ia SN exploding within a dense CSM from a non-degenerate, evolved companion, or a core-collapse SN from a massive star. While some members of the population have been unequivocally associated with type Ia SNe, in other cases the association is less certain. While it is possible that SN 2012ca does arise from a thermonuclear SN, this would require a relatively high (between 20 and 70 per cent) efficiency in converting kinetic energy to optical luminosity, and a massive (∼ 2.3 − 2.6 M ) circumstellar medium. On the basis of energetics, and the results of simple modelling, we suggest that SN 2012ca is more likely associated with a corecollapse SN. This would imply that the observedset of similar SNe to SN 2012ca is in fact originated by two populations, and while these are drawn from physically distinct channels, they can have observationally similar properties.

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Section: Datamentioning

confidence: 99%

On Type IIn/Ia-CSM supernovae as exemplified by SN 2012ca

Inserra

Fraser

Smartt

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The optical photometric follow up of SN 2011hs was almost entirely obtained with the 0.41m Panchromatic Robotic Optical Monitoring and Polarimetry Telescope (PROMPT; Reichart et al 2005) and the 50cm CATA500 Telescope, both located at the CTIO, which offered BVRI+u ′ g ′ r ′ i ′ z ′ and BV+u ′ g ′ r ′ i ′ coverage, respectively. Additional optical (UBVRI) data were acquired at the du Pont Telescope, a 2.5m-class telescope at LCO, using the Wide Field Reimaging CCD Camera (WFCCD), and at the 3.6m ESO New Technology Telescope (NTT), mounted with the ESO Faint Object Spectrograph and Camera 2 (EFOSC2).…”

Section: Optical and Nir Photometrymentioning

confidence: 99%

SN 2011hs: a fast and faint Type IIb supernova from a supergiant progenitor

Bufano¹,

Pignata²,

Bersten³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Observations spanning a large wavelength range, from X-ray to radio, of the Type IIb supernova 2011hs are presented, covering its evolution during the first year after explosion. The optical light curve presents a narrower shape and a fainter luminosity at peak than previously observed for Type IIb SNe. High expansion velocities are measured from the broad absorption H I and He I lines. From the comparison of the bolometric light curve and the time evolution of the photospheric velocities with hydrodynamical models, we found that SN 2011hs is consistent with the explosion of a 3-4 M ⊙ He-core progenitor star, corresponding to a main sequence mass of 12-15 M ⊙ , that ejected a mass of 56 Ni of about 0.04 M ⊙ , with an energy of E = 8.5 × 10 50 erg. Such a low-mass progenitor scenario is in full agreement with the modelling of the nebular spectrum taken at ∼215 days from maximum. From the modelling of the adiabatic cooling phase, we infer a progenitor radius of ≈500-600 R ⊙ , clearly pointing to an extended progenitor star. The radio light curve of SN 2011hs yields a peak luminosity similar to that of SN 1993J, but with a higher mass loss rate and a wind density possibly more similar to that of SN 2001ig. Although no significant deviations from a smooth decline have been found in the radio light curves, we cannot rule out the presence of a binary companion star.

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“…The Galactic reddening toward the SN line of sight is E(B − V ) = 0.06 mag (Schlafly & Finkbeiner 2011), which we correct for in the following. Spectro-photometric follow-up was obtained by PESSTO with NTT+EFOSC2, PROMPT (Reichart et al 2005), Swift+UVOT and ANU+WiFeS in optical, while in near infrared (NIR) with NTT+SOFI. Images and spectra were reduced in the standard fashion, and the NTT data were processed within the PESSTO pipeline as in Valenti et al (2013); Fraser et al (2013).…”

Section: Observations and Data Analysismentioning

confidence: 99%

SN2012ca: a stripped envelope core-collapse SN interacting with dense circumstellar medium

Inserra

Smartt

Scalzo

et al. 2013

Monthly Notices of the Royal Astronomical Society: Letters

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We report optical and near-infrared observations of SN2012ca with the Public ESO Spectroscopy Survey of Transient Objects (PESSTO), spread over one year since discovery. The supernova (SN) bears many similarities to SN1997cy and to other events classified as Type IIn but which have been suggested to have a thermonuclear origin with narrow hydrogen lines produced when the ejecta impact a hydrogen-rich circumstellar medium (CSM). Our analysis, especially in the nebular phase, reveals the presence of oxygen, magnesium and carbon features. This suggests a core collapse explanation for SN2012ca, in contrast to the thermonuclear interpretation proposed for some members of this group. We suggest that the data can be explained with a hydrogen and helium deficient SN ejecta (Type I) interacting with a hydrogen-rich CSM, but that the explosion was more likely a Type Ic core-collapse explosion than a Type Ia thermonuclear one. This suggests two channels (both thermonuclear and stripped envelope core-collapse) may be responsible for these SN 1997cy-like events.

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Gerhart Hauptmann der Schlesier

Cited by 3 publications

References 0 publications

On Type IIn/Ia-CSM supernovae as exemplified by SN 2012ca

On Type IIn/Ia-CSM supernovae as exemplified by SN 2012ca

SN 2011hs: a fast and faint Type IIb supernova from a supergiant progenitor

SN2012ca: a stripped envelope core-collapse SN interacting with dense circumstellar medium

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