- ID:
- ivo://CDS.VizieR/J/ApJ/908/232
- Title:
- SN 2020bvc optical and near-IR spectra
- Short Name:
- J/ApJ/908/232
- Date:
- 11 Mar 2022
- Publisher:
- CDS
- Description:
- We present near-IR (NIR) and optical observations of the Type Ic supernova (SN Ic) SN 2020oi in the galaxy M100 and the broad-lined SN Ic SN 2020bvc in UGC 9379, using Gemini, Las Cumbres Observatory, Southern Astrophysical Telescope, and other ground-based telescopes. The NIR spectrum of SN 2020oi at day 63 since the explosion shows strong CO emissions and a rising K-band continuum, which is the first unambiguous dust detection from an SN Ic. Non-LTE CO modeling shows that CO is still optically thick and that the lower limit to the CO mass is 10^-3^M_{sun}_. The dust temperature is 810 K, and the dust mass is ~10^-5^M_{sun}_. We explore the possibilities that the dust is freshly formed in the ejecta, heated dust in the preexisting circumstellar medium, and an infrared echo. The light curves of SN 2020oi are consistent with a STELLA model with canonical explosion energy, 0.07M_{sun}_ Ni mass, and 0.7M_{sun}_ ejecta mass. A model of high explosion energy of 10^52^erg, 0.4M_{sun}_ Ni mass, and 6.5M_{sun}_ ejecta mass with the circumstellar matter reproduces the double-peaked light curves of SN 2020bvc. We observe temporal changes of absorption features of the IR CaII triplet, SI at 1.043{mu}m, and FeII at 5169{AA}. The blueshifted lines indicate high velocities, up to 60000km/s for SN 2020bvc and 20000km/s for SN 2020oi, and the expansion velocity rapidly declines before the optical maximum. We present modeled spectral signatures and diagnostics of CO and SiO molecular bands between 1.4 and 10{mu}m.
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- ID:
- ivo://CDS.VizieR/J/MNRAS/394/2266
- Title:
- SN 2005cs one-year photometry
- Short Name:
- J/MNRAS/394/2266
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the results of the one-year long observational campaign of the type II plateau SN 2005cs, which exploded in the nearby spiral galaxy M51 (the Whirlpool galaxy). This extensive data set makes SN 2005cs the best observed low-luminosity, ^56^Ni-poor type II plateau event so far and one of the best core-collapse supernovae ever.
- ID:
- ivo://CDS.VizieR/J/A+A/655/A90
- Title:
- SN 2020cxd multi-photometry
- Short Name:
- J/A+A/655/A90
- Date:
- 22 Feb 2022
- Publisher:
- CDS
- Description:
- We present observations and analysis of SN 2020cxd, a low-luminosity (LL), long-lived Type IIP supernova (SN). This object was a clear outlier in the magnitude-limited SN sample recently presented by the Zwicky Transient Facility (ZTF) Bright Transient Survey. We demonstrate that SN 2020cxd is an additional member of the group of LL SNe, and discuss the rarity of LL SNe in the context of the ZTF survey, and how further studies of these faintest members of the core-collapse (CC) SN family might help understand the underlying initial mass function for stars that explode. We present optical light curves (LCs) from the ZTF in the $gri$ bands and several epochs of ultra-violet data from the Neil Gehrels Swift Observatory as well as a sequence of optical spectra. We construct colour curves, a bolometric LC, compare ejecta-velocity and black-body temperature evolutions for LL SNe, as well as for typical Type II SNe. Furthermore, we adopt a Monte Carlo code that fits semi-analytic models to the LC of SN 2020cxd, which allows the estimation of physical parameters. Using our late-time nebular spectra, we also compare against SN II spectral synthesis models from the literature to constrain the progenitor properties of SN 2020cxd. The LCs of SN 2020cxd show great similarity with those of LL SNe IIP, in luminosity, timescale and colours. Also the spectral evolution of SN 2020cxd is that of a Type IIP SN. The spectra show prominent and narrow P-Cygni lines, indicating low expansion velocities. This is one of the faintest LL SNe observed, with an absolute plateau magnitude of M_r_=-14.5mag, and also one with the longest plateau lengths, with a duration of 118 days. Finally, the velocities measured from the nebular emission lines are among the lowest ever seen in a SN, with intrinsic Full Width at Half Maximum of 478km/s. The underluminous late-time exponential LC tail indicates that the mass of ^56^Ni ejected during the explosion is much smaller than the average of normal SNe IIP, we estimate M_^56^Ni_=0.003M+{sun+_. The Monte Carlo fitting of the bolometric LC suggests that the progenitor of SN 2020cxd had a radius of R_0_=1.3x10^13^cm, kinetic energy of E_kin_=4.3x10^50^erg, and ejecta mass M_ej_=9.5M_{sun}_. From the bolometric LC, we estimate the total radiated energy E_rad_=1.52x10^48^erg. Using our late-time nebular spectra, we compare against SN II spectral synthesis models to constrain the progenitor Zero-age Main-sequence mass and found it likely to be <~15M_{sun}+. SN 2020cxd is a LL Type IIP SN. The inferred progenitor parameters and the features observed in the nebular spectrum favour a low-energy, Ni-poor, iron CC SN from a low mass ~12M_{sun}_ red supergiant.
- ID:
- ivo://CDS.VizieR/J/MNRAS/410/585
- Title:
- SN 2009dc BVRI light curves
- Short Name:
- J/MNRAS/410/585
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In this paper, we present and analyse optical photometry and spectra of the extremely luminous and slowly evolving Type Ia supernova (SN Ia) 2009dc, and offer evidence that it is a super-Chandrasekhar mass (SC) SN Ia and thus has a SC white dwarf (WD) progenitor. Optical spectra of SN 2007if, a similar object, are also shown. SN 2009dc had one of the most slowly evolving light curves ever observed for a SN Ia, with a rise time of ~23d and {DELTA}m_15_(B)=0.72mag. We calculate a lower limit to the peak bolometric luminosity of ~2.4x10^43^erg/s, though the actual value is likely almost 40 per cent larger. Optical spectra of SN 2009dc and SN 2007if obtained near maximum brightness exhibit strong CII features (indicative of a significant amount of unburned material), and the post-maximum spectra are dominated by iron-group elements (IGEs). All of our spectra of SN 2009dc and SN 2007if also show low expansion velocities. However, we see no strong evidence in SN 2009dc for a velocity `plateau' near maximum light like the one seen in SN 2007if. The high luminosity and low expansion velocities of SN 2009dc lead us to derive a possible WD progenitor mass of more than 2M_{sun}_ and a 56Ni mass of about 1.4-1.7M_{sun}_.
- ID:
- ivo://CDS.VizieR/J/A+A/562/A17
- Title:
- SN 2011dh - The first 100 days
- Short Name:
- J/A+A/562/A17
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present optical and near-infrared (NIR) photometry and spectroscopy of the Type IIb supernova (SN) 2011dh for the first 100 days. We complement our extensive dataset with Swift ultra-violet (UV) and Spitzer mid-infrared (MIR) data to build a UV to MIR bolometric lightcurve using both photometric and spectroscopic data. Hydrodynamical modelling of the SN based on this bolometric lightcurve have been presented in Bersten et al. (2012ApJ...757...31B).
- ID:
- ivo://CDS.VizieR/J/A+A/580/A142
- Title:
- SN 2011dh. The first two years
- Short Name:
- J/A+A/580/A142
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present optical and near-infrared (NIR) photometry and spectroscopy as well as modelling of the lightcurves of the Type IIb supernova (SN) 2011dh. Our extensive dataset, for which we present the observations obtained after day 100, spans two years, and complemented with Spitzer mid-infrared (MIR) data, we use it to build an optical-to-MIR bolometric lightcurve between days 3 and 732.
- ID:
- ivo://CDS.VizieR/J/ApJ/778/L19
- Title:
- SN 2011dh (type IIb) 3.6 and 4.5um light curves
- Short Name:
- J/ApJ/778/L19
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present Spitzer observations at 3.6 and 4.5{mu}m of the supernova SN 2011dh (PTF 11eon) in M51 from 18 days to 625 days after explosion. The mid-infrared emission peaks at 24 days after explosion at a few x10^7^L _{sun}_, and decays more slowly than the visible-light bolometric luminosity. The infrared color temperature cools for the first 90 days and then is constant. Simple numerical models of a thermal echo can qualitatively reproduce the early behavior. At late times, the mid-IR light curve cannot be explained by a simple thermal echo model, suggesting additional dust heating or line emission mechanisms. We also propose that thermal echoes can serve as effective probes to uncover supernovae in heavily obscured environments, and speculate that under the right conditions, integrating the early epoch of the mid-infrared light curve may constrain the total energy in the shock breakout flash.
- ID:
- ivo://CDS.VizieR/J/other/PZ/28.8
- Title:
- SN 2004dj UBVRI light curves
- Short Name:
- J/other/PZ/28.8
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- CCD UBVRI photometry is presented for type II SN 2004dj for about 1200 days, starting on day 2 past discovery. The photometric behaviour is typical of SNe II-P, although some minor peculiarities are noticed. We compare the photometric data for the host cluster S96 before and after the SN 2004dj outburst and do not find any significant changes.
- ID:
- ivo://CDS.VizieR/J/ApJ/689/377
- Title:
- SNe Ia as NIR standard candles from PAIRITEL
- Short Name:
- J/ApJ/689/377
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have obtained 1087 NIR (JHK_s_) measurements of 21 SNe Ia using PAIRITEL, nearly doubling the number of well-sampled NIR SN Ia light curves. These data strengthen the evidence that SNe Ia are excellent standard candles in the NIR, even without correction for optical light-curve shape. We construct fiducial NIR templates for normal SNe Ia from our sample, excluding only the three known peculiar SNe Ia: SN 2005bl, SN 2005hk, and SN 2005ke. The H-band absolute magnitudes in this sample of 18 SNe Ia have an intrinsic rms of only 0.15mag with no correction for light-curve shape. We found a relationship between the H-band extinction and optical color excess of A_H_=0.2E(B-V). This variation is as small as the scatter in distance modulus measurements currently used for cosmology based on optical light curves after corrections for light-curve shape. Combining the homogeneous PAIRITEL measurements with 23 SNe Ia from the literature, these 41 SNe Ia have standard H-band magnitudes with an rms scatter of 0.16mag. The good match of our sample with the literature sample suggests there are few systematic problems with the photometry.
- ID:
- ivo://CDS.VizieR/J/ApJS/219/13
- Title:
- SNe Ia light curves for the LSQ-CSP sample
- Short Name:
- J/ApJS/219/13
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The La Silla/QUEST Variability Survey (LSQ) and the Carnegie Supernova Project (CSP II) are collaborating to discover and obtain photometric light curves for a large sample of low-redshift (z<0.1) Type Ia supernovae (SNe Ia). The supernovae are discovered in the LSQ survey using the 1m ESO Schmidt telescope at the La Silla Observatory with the 10 square degree QUEST camera. The follow-up photometric observations are carried out using the 1m Swope telescope and the 2.5m du Pont telescopes at the Las Campanas Observatory. This paper describes the survey, discusses the methods of analyzing the data, and presents the light curves for the first 31 SNe Ia obtained in the survey. The SALT 2.4 supernova light-curve fitter was used to analyze the photometric data, and the Hubble diagram for this first sample is presented. The measurement errors for these supernovae averaged 4%, and their intrinsic spread was 14%.
