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Start Over Subject supernovae Validation Level 2
171. Nearby supernova rates
ID:
ivo://CDS.VizieR/J/MNRAS/412/1419
Title:
Nearby supernova rates
Short Name:
J/MNRAS/412/1419
Date:
21 Oct 2021
Publisher:
CDS
Description:
This is the first paper of a series in which we present new measurements of the observed rates of supernovae (SNe) in the local Universe, determined from the Lick Observatory Supernova Search. We have obtained 2.3 million observations of 14 882 sample galaxies over an interval of 11 years (1998 March to 2008 December). We considered 1036 SNe detected in our sample and used an optimal subsample of 726 SNe (274 Type Ia SNe, 116 Type Ibc SNe and Type II 324 SNe) to determine our SN rates. This is the largest and most homogeneous set of nearby SNe ever assembled for this purpose, and ours is the first local SN rate analysis based on CCD imaging and modern image-subtraction techniques. In this paper, we lay the foundation of the study.
172. Neutrino cross sections for SNe
ID:
ivo://CDS.VizieR/J/ApJ/686/448
Title:
Neutrino cross sections for SNe
Short Name:
J/ApJ/686/448
Date:
21 Oct 2021
Publisher:
CDS
Description:
The neutrino-nucleus reaction cross sections of ^4^He and ^12^C are evaluated using new shell model Hamiltonians. Branching ratios of various decay channels are calculated to evaluate the yields of Li, Be, and B produced through the {nu}-process in supernova explosions. The new cross sections enhance the yields of ^7^Li and ^11^B produced during the supernova explosion of a 16.2M_{sun}_ star model compared to the case using the conventional cross sections by about 10%. On the other hand, the yield of ^10^B decreases by a factor of 2. The yields of ^6^Li, ^9^Be, and the radioactive nucleus ^10^Be are found at a level of ~10^-11^M_{sun}_. The temperature of {nu}_{mu},{tau}_ - and {nu}{bar}_{mu},{tau}_ - neutrinos inferred from the supernova contribution of ^11^B in Galactic chemical evolution models is constrained to the 4.3-6.5MeV range. The increase in the ^7^Li and ^11^B yields due to neutrino oscillations is demonstrated with the new cross sections.
173. New SNe in SDSS DR9
ID:
ivo://CDS.VizieR/J/MNRAS/450/905
Title:
New SNe in SDSS DR9
Short Name:
J/MNRAS/450/905
Date:
21 Oct 2021
Publisher:
CDS
Description:
Using a method to discover and classify supernovae (SNe) in galaxy spectra, we detect 91 Type Ia SNe (SNe Ia) and 16 Type II SNe (SNe II) among ~740000 galaxies of all types and ~215000 star-forming galaxies without active galactic nuclei, respectively, in Data Release 9 of the Sloan Digital Sky Survey. Of these SNe, 15 SNe Ia and eight SNe II are new discoveries reported here for the first time. We use our SN samples to measure SN rates per unit mass as a function of galaxy stellar mass, star-formation rate (SFR), and specific SFR (sSFR), as derived by the MPA-JHU Galspec pipeline. We show that correlations between SN Ia and SN II rates per unit mass and galaxy stellar mass, SFR, and sSFR can be explained by a combination of the respective SN delay-time distributions (the distributions of times that elapse between the formation of a stellar population and all ensuing SNe), the ages of the surveyed galaxies, the redshifts at which they are observed, and their star formation histories.
174. 90 new SNIa from SDSS DR7
ID:
ivo://CDS.VizieR/J/MNRAS/430/1746
Title:
90 new SNIa from SDSS DR7
Short Name:
J/MNRAS/430/1746
Date:
21 Oct 2021
Publisher:
CDS
Description:
Using a method to discover and classify supernovae (SNe) in galaxy spectra, we find 90 Type Ia SNe (SNe Ia) and 10 Type II SNe among the ~700000 galaxy spectra in the Sloan Digital Sky Survey Data Release 7 that have star-formation histories (SFHs) derived with the VErsatile SPectral Analysis code (VESPA). We use the SN Ia sample to measure SN Ia rates per unit stellar mass.
175. NGC 300 candidate supernova remnants
ID:
ivo://CDS.VizieR/J/other/Ser/184.19
Title:
NGC 300 candidate supernova remnants
Short Name:
J/other/Ser/184.
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present the results of a study of observational and identification techniques used for surveys and spectroscopy of candidate supernova remnants (SNRs) in the Sculptor Group galaxy NGC300. The goal of this study was to investigate the reliability of using [Sii]:Hα≥0.4 in optical SNR surveys and spectra as an identifying feature of extra-galactic SNRs (egSNRs), and also to investigate the effectiveness of the observing techniques (which are hampered by seeing conditions and telescope pointing errors) using this criterion in egSNR surveys and spectrographs. This study is based on original observations of these objects and archival data obtained from the Hubble Space Telescope which contained images of some of the candidate SNRs in NGC300. We found that the reliability of spectral techniques may be questionable and very high-resolution images may be needed to confirm a valid identification of some egSNRs.
176. NGC3278, SN2009bb host, ATCA and MUSE data
ID:
ivo://CDS.VizieR/J/A+A/618/A104
Title:
NGC3278, SN2009bb host, ATCA and MUSE data
Short Name:
J/A+A/618/A104
Date:
21 Oct 2021
Publisher:
CDS
Description:
The host galaxies of gamma-ray bursts (GRBs) have been claimed to have experienced a recent inflow of gas from the intergalactic medium. This is because their atomic gas distribution is not centred on their optical emission and because they are deficient in molecular gas given their high star-formation rates. Similar studies have not been conducted for host galaxies of relativistic supernovae (SNe), which may have similar progenitors. The potential similarity of the powering mechanisms of relativistic SNe and GRBs allowed us to make a prediction that relativistic SNe are born in environments similar to those of GRBs, i.e. rich in atomic gas. Here we embark on testing this hypothesis by analysing the properties of the host galaxy NGC 3278 of the relativistic SN 2009bb. This is the first time the atomic gas properties of a relativistic SN host is analysed and the first time resolved 21cm hydrogen line (HI) information is provided for a host of a SN of any type. We obtained radio observations with Australia Telescope Compact Array (ATCA) covering HI line; and optical integral field unit spectroscopy observations with Multi Unit Spectroscopic Explorer (MUSE) at the Very Large Telescope (VLT). Moreover, we analysed archival carbon monoxide (CO) and broad-band data for this galaxy. The atomic gas distribution of NGC3278 is not centred on the optical galaxy centre, but instead around a third of atomic gas resides in the region close to the SN position. This galaxy has a few times lower atomic and molecular gas masses than predicted from its star formation rate (SFR). Its specific star formation rate (sSFR=SFR/M*) is ~2-3 times higher than the main-sequence value, placing it at the higher end of the main sequence towards starburst galaxies. SN 2009bb exploded close to the region with the highest SFR density and the lowest age, as evident from high Halpha EW, corresponding to the age of the stellar population of ~5.5Myr. Assuming this timescale was the lifetime of the progenitor star, its initial mass would have been close to ~36M_{sun}_. As for GRB hosts, the gas properties of NGC3278 are consistent with a recent inflow of gas from the intergalactic medium, which explains the concentration of atomic gas close to the SN position and the enhanced SFR. Super-solar metallicity at the position of the SN (unlike for most of GRBs) may mean that relativistic explosions signal a recent inflow of gas (and subsequent star-formation), and their type (GRBs or SNe) is determined by either i) the metallicity of the inflowing gas (metal-poor gas results in a GRB explosion and metal-rich gas in a relativistic SN explosion without an accompanying GRB), or ii) by the efficiency of gas mixing (efficient mixing for SN hosts leading to quick disappearance of metal-poor regions), or iii) by the type of the galaxy (more metal-rich galaxies would result in only a small fraction of star-formation to be fuelled by metal-poor gas).
177. 56Ni masses in supernovae
ID:
ivo://CDS.VizieR/J/A+A/641/A177
Title:
56Ni masses in supernovae
Short Name:
J/A+A/641/A177
Date:
21 Oct 2021
Publisher:
CDS
Description:
The mass of synthesised radioactive material is an important power source for all supernova (SN) types. In addition, the difference of ^56^Ni yields statistics are relevant to constrain progenitor paths and explosion mechanisms. Here, we re-estimate the nucleosynthetic yields of ^56^Ni for a well-observed and well-defined sample of stripped-envelope SNe (SE-SNe) in a uniform manner. This allows us to investigate whether the observed hydrogen-rich-stripped-envelope (SN II-SE SN) ^56^Ni separation is due to real differences between these SN types or because of systematic errors in the estimation methods. We compiled a sample of well-observed SE-SNe and measured ^56^Ni masses through three different methods proposed in the literature: first, the classic "Arnett rule"; second the more recent prescription of Khatami & Kasen (2019ApJ...878...56K) and third using the tail luminosity to provide lower limit ^56^Ni masses. These SE-SN distributions were then compared to those compiled in this article. Results. Arnett's rule, as previously shown, gives ^56^Ni masses for SE-SNe that are considerably higher than SNe II. While for the distributions calculated using both the Khatami & Kasen (2019ApJ...878...56K) prescription and Tail ^56^Ni masses are offset to lower values than "Arnett values", their ^56^Ni distributions are still statistically higher than that of SNe II. Our results are strongly driven by a lack of SE-SN with low ^56^Ni masses, that are, in addition, strictly lower limits. The lowest SE-SN ^56^Ni mass in our sample is of 0.015M_{sun}_, below which are more than 25% of SNe II. We conclude that there exist real, intrinsic differences in the mass of synthesised radioactive material between SNe II and SE-SNe (types IIb, Ib, and Ic). Any proposed current or future CC SN progenitor scenario and explosion mechanism must be able to explain why and how such differences arise or outline a bias in current SN samples yet to be fully explored.
178. NIR K-corrections
ID:
ivo://CDS.VizieR/J/A+A/615/A45
Title:
NIR K-corrections
Short Name:
J/A+A/615/A45
Date:
21 Oct 2021
Publisher:
CDS
Description:
Type Ia Supernovae (SNe Ia) have been used as standardizable candles in the optical wavelengths to measure distances with an accuracy of ~7% out to redshift z~1.5. There is evidence that in the near-infrared (NIR) wavelengths SNe Ia are even better standard candles, however, NIR observations are much more time-consuming. We aim to test whether the NIR peak magnitudes could be accurately estimated with only a single observation obtained close to maximum light, provided that the time of B band maximum, the B-V color at maximum and the optical stretch parameter are known. We present multi-epoch UBVRI and single-epoch J and H photometric observations of 16 SNe Ia in the redshift range z=0.037-0.183, doubling the leverage of the current SN Ia NIR Hubble diagram and the number of SNe beyond redshift 0.04. This sample was analyzed together with 102 NIR and 458 optical light curves (LCs) of normal SNe Ia from the literature. Results. The analysis of 45 NIR LCs with well-sampled first maximum shows that a single template accurately describes the LCs if its time axis is stretched with the optical stretch parameter. This allows us to estimate the peak NIR magnitudes of SNe with only few observations obtained within ten days from B-band maximum. The NIR Hubble residuals show weak correlation with {Delta}M_15_ and the color excess E(B-V), and for the first time we report a potential dependence on the Jmax-Hmax color. With these corrections, the intrinsic NIR luminosity scatter of SNe Ia is estimated to be ~0.10mag, which is smaller than what can be derived for a similarly heterogeneous sample at optical wavelengths. Analysis of both NIR and optical data shows that the dust extinction in the host galaxies corresponds to a low RV~=1.8-1.9. We conclude that SNe Ia are at least as good standard candles in the NIR as in the optical and are potentially less affected by systematic uncertainties. We extended the NIR SN Ia Hubble diagram to its nonlinear part at z~0.2 and confirmed that it is feasible to accomplish this result with very modest sampling of the NIR LCs, if complemented by well-sampled optical LCs. With future facilities it will be possible to extend the NIR Hubble diagram beyond redshift z~=1, and our results suggest that the most efficient way to achieve this would be to obtain a single observation close to the NIR maximum.
179. Nucleosynthesis of massive metal-free stars
ID:
ivo://CDS.VizieR/J/ApJ/724/341
Title:
Nucleosynthesis of massive metal-free stars
Short Name:
J/ApJ/724/341
Date:
21 Oct 2021
Publisher:
CDS
Description:
The evolution and explosion of metal-free stars with masses 10-100M_{sun}_ are followed, and their nucleosynthetic yields, light curves, and remnant masses determined. Such stars would have been the first to form after the big bang and may have left a distinctive imprint on the composition of the early universe. When the supernova yields are integrated over a Salpeter initial mass function (IMF), the resulting elemental abundance pattern is qualitatively solar, but with marked deficiencies of odd-Z elements with 7<=Z<=13. Neglecting the contribution of the neutrino wind from the neutron stars that they form, no appreciable abundances are made for elements heavier than germanium. The computed pattern compares favorably with what has been observed in metal-deficient stars with [Z]<~-3. For the lower mass supernovae considered, the distribution of remnant masses clusters around typical modern neutron star masses, but above 20-30M-{sun}_, with the value depending on explosion energy, black holes are copiously formed by fallback, with a maximum hole mass of ~40M_{sun}_. A novel automated fitting algorithm is developed for determining optimal combinations of explosion energy, mixing, and IMF in the large model database to agree with specified data sets. The model is applied to the low-metallicity sample of Cayrel et al. (Cat. J/A+A/416/1117) and the two ultra-iron-poor stars HE0107-5240 and HE1327-2326. Best agreement with these very low metallicity stars is achieved with very little mixing, and none of the metal-deficient data sets considered show the need for a high-energy explosion component. In contrast, explosion energies somewhat less than 1.2B seem to be preferred in most cases.
180. Nucleosynthesis of p nuclides
ID:
ivo://CDS.VizieR/J/ApJ/854/18
Title:
Nucleosynthesis of p nuclides
Short Name:
J/ApJ/854/18
Date:
21 Oct 2021
Publisher:
CDS
Description:
The production of the heavy stable proton-rich isotopes between ^74^Se and ^196^Hg-the p nuclides-is due to the contribution from different nucleosynthesis processes, activated in different types of stars. Whereas these processes have been subject to various studies, their relative contributions to Galactic chemical evolution (GCE) are still a matter of debate. Here we investigate for the first time the nucleosynthesis of p nuclides in GCE by including metallicity and progenitor mass-dependent yields of core-collapse supernovae (ccSNe) into a chemical evolution model. We used a grid of metallicities and progenitor masses from two different sets of stellar yields and followed the contribution of ccSNe to the Galactic abundances as a function of time. In combination with previous studies on p-nucleus production in thermonuclear supernovae (SNIa), and using the same GCE description, this allows us to compare the respective roles of SNeIa and ccSNe in the production of p-nuclei in the Galaxy. The {gamma} process in ccSN is very efficient for a wide range of progenitor masses (13M_{sun}_-25M_{sun}_) at solar metallicity. Since it is a secondary process with its efficiency depending on the initial abundance of heavy elements, its contribution is strongly reduced below solar metallicity. This makes it challenging to explain the inventory of the p nuclides in the solar system by the contribution from ccSNe alone. In particular, we find that ccSNe contribute less than 10% of the solar p nuclide abundances, with only a few exceptions. Due to the uncertain contribution from other nucleosynthesis sites in ccSNe, such as neutrino winds or {alpha}-rich freeze out, we conclude that the light p-nuclides ^74^Se, ^78^Kr, ^84^Sr, and ^92^Mo may either still be completely or only partially produced in ccSNe. The {gamma}-process accounts for up to twice the relative solar abundances for ^74^Se in one set of stellar models and ^196^Hg in the other set. The solar abundance of the heaviest p nucleus ^196^Hg is reproduced within uncertainties in one set of our models due to photodisintegration of the Pb isotopes ^208,207,206^Pb. For all other p nuclides, abundances as low as 2% of the solar level were obtained.