- ID:
- ivo://CDS.VizieR/J/A+A/477/717
- Title:
- Spectroscopy of Type Ia supernovae
- Short Name:
- J/A+A/477/717
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a quantitative study of a new data set of high redshift Type Ia supernovae spectra, observed at the Gemini telescopes during the first 34 months of the Supernova Legacy Survey. During this time 123 supernovae candidates were observed, of which 87 have been identified as SNe Ia at a median redshift of z=0.720. Spectra from the entire second year of the survey and part of the third year (59 total SNe candidates with 46 confirmed SNe Ia) are published here for the first time. The spectroscopic measurements made on this data set are used determine if these distant SNe comprise a population similar to those observed locally. Rest-frame equivalent width and ejection velocity measurements are made on four spectroscopic features. Corresponding measurements are presented for a set of 167 spectra from 24 low-z SNe Ia from the literature.
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- ID:
- ivo://CDS.VizieR/J/A+A/621/A109
- Title:
- Ssynthetic spectra of supernovae models
- Short Name:
- J/A+A/621/A109
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Observational surveys are now able to detect an increasing number of transients, such as core-collapse supernovae (SN) and powerful non-terminal outbursts (SN impostors). Dedicated spectroscopic facilities can follow up these events shortly after detection. Here we investigate the properties of these explosions at early times.We use the radiative transfer code CMFGEN to build an extensive library of spectra simulating the interaction of supernovae and their progenitor's winds/circumstellar medium (CSM).We consider a range of progenitor mass-loss rates (dM/dt=5x10^-4^ to 10^-2^ M_{sun}/yr), abundances (solar, CNO-processed, and He-rich), and SN luminosities (L=1.9x10^8^ to 2.5x10^10^L_{sun}_). The models simulate events ~=1-day after explosion, and we assume a fixed location of the shock front as R_in_=8.6x10^13^cm. We show that the large range of massive star properties at the pre-SN stage causes a diversity of early-time interacting SN and impostors. We identify three main classes of early-time spectra consisting of relatively high-ionisation (e.g. HeII and OVI), medium-ionisation (e.g. CIII and NIII), and low-ionisation lines (e.g. HeI and FeII/III). They are regulated by L and the CSM density. Given a progenitor wind velocity v_inf_, our models also place a lower limit of dM/dt>~5x10^-4^(v_inf_=150km/s)M_{sun}_/yr for detection of CSM interaction signatures in observed spectra. Early-time SN spectra should provide clear constraints on progenitors by measuring H, He, and CNO abundances if the progenitors come from single stars. The connections are less clear considering the effects of binary evolution. Nevertheless, our models provide a clear path for linking the final stages of massive stars to their post-explosion spectra at early times, and guiding future observational follow-up of transients with facilities such as the Zwicky Transient Facility.
- ID:
- ivo://CDS.VizieR/J/ApJ/764/21
- Title:
- Stellar evolutionary models with 13-120Msun
- Short Name:
- J/ApJ/764/21
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the first set of a new generation of models of massive stars with a solar composition extending between 13 and 120M_{sun}_, computed with and without the effects of rotation. We included two instabilities induced by rotation: the meridional circulation and the shear instability. We implemented two alternative schemes to treat the transport of the angular momentum: the advection-diffusion formalism and the simpler purely diffusive one. The full evolution from the pre-main sequence up to the pre-supernova stage is followed in detail with a very extended nuclear network. The explosive yields are provided for a variety of possible mass cuts and are available at the Web site http://www.iasf-roma.inaf.it/orfeo/public_html. We find that both the He and the CO core masses are larger than those of their non-rotating counterparts. Also the C abundance left by the He burning is lower than in the non-rotating case, especially for stars with an initial mass of 13-25M_{sun}_, and this affects the final mass-radius relation, basically the final binding energy, at the pre-supernova stage. The elemental yields produced by a generation of stars rotating initially at 300km/s do not change substantially with respect to those produced by a generation of non-rotating massive stars, the main differences being a slight overproduction of the weak s-component and a larger production of F. Since rotation also affects the mass-loss rate, either directly or indirectly, we find substantial differences in the lifetimes as O-type and Wolf-Rayet subtypes between the rotating and non-rotating models. The maximum mass exploding as Type IIP supernova ranges between 15 and 20M _{sun}_ in both sets of models (this value depends basically on the larger mass-loss rates in the red supergiant phase due to the inclusion of the dust-driven wind). This limiting value is in remarkably good agreement with current estimates.
- ID:
- ivo://CDS.VizieR/J/ApJ/867/108
- Title:
- Stellar masses and rest-frame u-g colors of SNIa
- Short Name:
- J/ApJ/867/108
- Date:
- 03 Dec 2021 00:48:50
- Publisher:
- CDS
- Description:
- Recent analyses suggest that distance residuals measured from Type Ia supernovae (SNe Ia) are correlated with local host galaxy properties within a few kiloparsecs of the SN explosion. However, the well-established correlation with global host galaxy properties is nearly as significant, with a shift of 0.06mag across a low to high mass boundary (the mass step). Here, with 273 SNe Ia at z<0.1, we investigate whether the stellar masses and rest-frame u-g colors of regions within 1.5kpc of the SN Ia explosion site are significantly better correlated with SN distance measurements than global properties or properties measured at random locations in SN hosts. At >~2{sigma} significance, local properties tend to correlate with distance residuals better than properties at random locations, though despite using the largest low-z sample to date, we cannot definitively prove that a local correlation is more significant than a random correlation. Our data hint that SNe observed by surveys that do not target a pre-selected set of galaxies may have a larger local mass step than SNe from surveys that do, an increase of 0.071+/-0.036mag (2.0{sigma}). We find a 3{sigma} local mass step after global mass correction, evidence that SNe Ia should be corrected for their local mass, but we note that this effect is insignificant in the targeted low-z sample. Only the local mass step remains significant at >2{sigma} after global mass correction, and we conservatively estimate a systematic shift in H0 measurements of -0.14km/s/Mpc with an additional uncertainty of 0.14km/s/Mpc, ~10% of the present uncertainty.
- ID:
- ivo://CDS.VizieR/II/201
- Title:
- Sternberg SN Catalogue, 1994Sep.
- Short Name:
- II/201
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a revised version of "Sternberg Astronomical Institute Supernova Catalogue" which includes data on 930 extragalactic supernovae (SNe) discovered up to September 1, 1994 and the main data on their parent galaxies. The description of previous version was presented by Tsvetkov and Bartunov (1993). The main improvements are the following: 1. The RC3 catalogue (de Vaucouleurs et al., 1991) was used instead of the RC2 as main source of data for parent galaxies. 2. For recent supernovae we included some magnitudes at maximum light from Hamuy et al. (1993) and compared our data with those of van den Bergh (1993). We also corrected some velocities of galaxies according to Huchra et al. (1994). 3. Some galaxy identifications from the MCG ( M ) were replaced by the ones from the PGC and the UGC. The identifications were adopted with this order of preference: NGC (IC) - UGC (ESO) - MCG - PGC - others 4. Photographic magnitudes from the PGC ( marked '*' ) and from IAU circulars ( marked 'C' ) were used when no other data were available. 5. Some errors were found in the previous version, and many new identifications for the galaxies previously listed as "ANON" were adopted. 6. We included several precise astrometric positions of SNe from Porter (1993).
- ID:
- ivo://CDS.VizieR/II/218
- Title:
- Sternberg Supernova Catalogue
- Short Name:
- II/218
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The catalogue presents the main data on 1362 extragalactic supernovae (SNe) discovered up to July 13, 1998 and on their parent galaxies. SNe are ordered by Right Ascension of their parent galaxies. Data for parent galaxies were compiled from the following catalogues: RC3 (de Vaucouleurs et al., 1991, Cat. <VII/155>); UGC (Nilson, 1973. Cat. <VII/26>); PGC (Paturel et al., 1989, Cat. <VII/119>); MCG (Vorontsov-Velyaminov et al., 1962-1968, Cat. <VII/62>, <VII/100>); ESO (Lauberts, 1982, Cat. <VII/34>); CfA (Huchra et al., 1994, see Cat <VII/193>), and from van den Bergh (1994, Cat. <J/ApJS/92/219>). Main source of morphological types, major diameters and axial ratios was the RC3; the data from other sources have been reduced to the system of RC3. Photographic magnitudes of galaxies were adopted from the UGC and the PGC together with individual data from the literature. The sources of recession velocities or cz values were the RC3, the CfA, the PGC and IAU Circulars. Position angles were taken from the RC3, UGC and the ESO catalogues, and inclination angles were mainly derived from data in RC3 according to Holmberg (1958MeLu2.136....1H). Some data for SNe and parent galaxies were adopted from GCVS (Samus et al., 1995, Cat. <II/205>)
- ID:
- ivo://CDS.VizieR/II/256
- Title:
- Sternberg Supernova Catalogue, 2004 version
- Short Name:
- II/256
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We describe the Sternberg Astronomical Institute (SAI) catalog of supernovae. We show that the radial distributions of type-Ia, type-Ibc and type-II supernovae differ in the central parts of spiral galaxies and are similar in their outer regions, while the radial distribution of type-Ia supernovae in elliptical galaxies differs that in spiral and lenticular galaxies. We give a list a supernovae that are farthest from the galactic centers, estimate their relative expulsion rate, and discuss their possible origins.
- ID:
- ivo://CDS.VizieR/J/MNRAS/448/2766
- Title:
- Strong lines in the optical/NIR for SN 2002bo
- Short Name:
- J/MNRAS/448/2766
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present 1D non-local thermodynamic equilibrium time-dependent radiative transfer simulations of a Chandrasekhar-mass delayed-detonation model which synthesizes 0.51 M_{sun}_ of ^56^Ni, and confront our results to the Type Ia supernova (SN Ia) 2002bo over the first 100d of its evolution. Assuming only homologous expansion, this same model reproduces the bolometric and multiband light curves, the secondary near-infrared (NIR) maxima, and the optical and NIR spectra. The chemical stratification of our model qualitatively agrees with previous inferences by Stehle et al. (2005MNRAS.360.1231S), but reveals significant quantitative differences for both iron-group and intermediate-mass elements. We show that +/-0.1 M_{sun}_ (i.e. +/-20 per cent) variations in ^56^Ni mass have a modest impact on the bolometric and colour evolution of our model. One notable exception is the U band, where a larger abundance of iron-group elements results in less opaque ejecta through ionization effects, our model with more ^56^Ni displaying a higher near-ultraviolet flux level. In the NIR range, such variations in ^56^Ni mass affect the timing of the secondary maxima but not their magnitude, in agreement with observational results. Moreover, the variation in the I, J, and K_s_ magnitudes is less than 0.1 mag within ~ 10d from bolometric maximum, confirming the potential of NIR photometry of SNe Ia for cosmology. Overall, the delayed-detonation mechanism in single Chandrasekhar-mass white dwarf progenitors seems well suited for SN 2002bo and similar SNe Ia displaying a broad SiII 6355{AA} line. Whatever multidimensional processes are at play during the explosion leading to these events, they must conspire to produce an ejecta comparable to our spherically symmetric model.
- ID:
- ivo://CDS.VizieR/J/A+A/584/A62
- Title:
- SUDARE VST-OmegaCAM search supernova rates
- Short Name:
- J/A+A/584/A62
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We describe the observing strategy, data reduction tools, and early results of a supernova (SN) search project, named SUDARE, conducted with the ESO VST telescope, which is aimed at measuring the rate of the different types of SNe in the redshift range 0.2<z<0.8. The search was performed in two of the best studied extragalactic fields, CDFS and COSMOS, for which a wealth of ancillary data are available in the literature or in public archives. We developed a pipeline for the data reduction and rapid identification of transients. As a result of the frequent monitoring of the two selected fields, we obtained light curve and colour information for the transients sources that were used to select and classify SNe by means of an especially developed tool. To accurately characterise the surveyed stellar population, we exploit public data and our own observations to measure the galaxy photometric redshifts and rest frame colours. We obtained a final sample of 117 SNe, most of which are SN Ia (57%) with the remaining ones being core collapse events, of which 44% are type II, 22% type IIn and 34% type Ib/c. To link the transients, we built a catalogue of ~1.3x10^5^ galaxies in the redshift range 0<z<=1, with a limiting magnitude K_AB_=23.5mag. We measured the SN rate per unit volume for SN Ia and core collapse SNe in different bins of redshifts. The values are consistent with other measurements from the literature. The dispersion of the rate measurements for SNe-Ia is comparable to the scatter of the theoretical tracks for single degenerate (SD) and double degenerate (DD) binary systems models, therefore it is not possible to disentangle among the two different progenitor scenarios. However, among the three tested models (SD and the two flavours of DD that either have a steep DDC or a wide DDW delay time distribution), the SD appears to give a better fit across the whole redshift range, whereas the DDC better matches the steep rise up to redshift ~1.2. The DDW instead appears to be less favoured. Unlike recent claims, the core collapse SN rate is fully consistent with the prediction that is based on recent estimates of star formation history and standard progenitor mass range.
- ID:
- ivo://CDS.VizieR/J/MNRAS/448/1206
- Title:
- Superluminous supernovae in faint galaxies
- Short Name:
- J/MNRAS/448/1206
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Pan-STARRS1 (PS1) survey has obtained imaging in five bands (griz y_P1_) over 10 Medium Deep Survey (MDS) fields covering a total of 70 square degrees. This paper describes the search for apparently hostless supernovae (SNe) within the first year of PS1 MDS data with an aim of discovering superluminous supernovae (SLSNe). A total of 249 hostless transients were discovered down to a limiting magnitude of M_AB_~23.5, of which 76 were classified as Type Ia supernovae (SNe Ia). There were 57 SNe with complete light curves that are likely core-collapse SNe (CCSNe) or type Ic SLSNe and 12 of these have had spectra taken. Of these 12 hostless, non-Type Ia SNe, 7 were SLSNe of type Ic at redshifts between 0.5 and 1.4. This illustrates that the discovery rate of type Ic SLSNe can be maximized by concentrating on hostless transients and removing normal SNe Ia. We present data for two possible SLSNe; PS1-10pm (z=1.206) and PS1-10ahf (z=1.1), and estimate the rate of type Ic SLSNe to be between 3^+3^_-2_x10^-5^ and 8^+2^_-1_x10^-5^ that of the CCSN rate within 0.3<=z<=1.4 by applying a Monte Carlo technique. The rate of slowly evolving, type Ic SLSNe (such as SN2007bi) is estimated as a factor of 10 lower than this range.
