scholarly journals A rate study of Type Ia supernovae with Subaru/XMM-Newton Deep Survey

2009 ◽  
Vol 5 (S262) ◽  
pp. 358-361
Author(s):  
Yutaka Ihara ◽  
Mamoru Doi ◽  
Tomoki Morokuma ◽  
Raynald Pain ◽  
Naohiro Takanashi ◽  
...  
Keyword(s):  
Star Formation ◽  
Light Curve ◽  
Delay Time ◽  
Detection Efficiency ◽  
Light Curves ◽  
Star Formation History ◽  
Type Ia Supernovae ◽  
Wide Range ◽  
Type Ia ◽  
Ia Supernovae

AbstractWe present a measurement of the rate of high-z Type Ia supernovae (SNe Ia) using multi-epoch observations of Subaru/XMM-Newton Deep Field (SXDF) with Suprime-Cam on the Subaru Telescope. Although SNe Ia are regarded as a standard candle, progenitor systems of SNe Ia have not been resolved yet. One of the key parameters to show the progenitor systems by observations is the delay time distribution between the binary system formation and subsequent SN explosion. Recently, a wide range of delay time is studied by SN Ia rates compared with an assumed cosmic star formation history. If SNe Ia with short delay time are dominant, the cosmic SN Ia rate evolution should closely trace that of the cosmic star formation. In order to detect a lot of high-z SNe Ia and measure SN Ia rates, we repeatedly carried out wide and deep imaging observations in the í-band with Suprime-Cam in 2002 (FoV~1 deg2, mi < 25.5 mag). We obtained detailed light curves of the variable objects, and 50 objects are classified as SNe Ia using the light curve fitting method at the redshift range of 0.2 < z < 1.3. In order to check the completeness and contamination of the light curve classification method, we performed Monte Carlo simulations and generated ~100,000 light curves of SNe Ia and II from templates. The control time and detection efficiency of the SN survey are also calculated using the artificial light curves. We derived an increasing trend of rates at around z ~ 1.2. Our results are almost consistent with other SN Ia rate results from low-z to high-z. Our results are the first results of high-z SN Ia rates with large statistics using light curves obtained by ground based telescopes, and give us visions of the SN rate studies for the future.

scholarly journals Constraints on the density distribution of type Ia supernovae ejecta inferred from late-time light-curve flattening

2020 ◽  
Vol 493 (4) ◽  
pp. 5617-5624
Author(s):  
Doron Kushnir ◽  
Eli Waxman
Keyword(s):  
Light Curve ◽  
Weighted Average ◽  
Far Infrared ◽  
Average Density ◽  
Light Curves ◽  
Type Ia Supernovae ◽  
Late Time ◽  
Simple Method ◽  
Type Ia ◽  
Ia Supernovae

ABSTRACT The finite time, τdep, over which positrons from β+ decays of 56Co deposit energy in type Ia supernovae ejecta lead, in case the positrons are trapped, to a slower decay of the bolometric luminosity compared to an exponential decline. Significant light-curve flattening is obtained when the ejecta density drops below the value for which τdep equals the 56Co lifetime. We provide a simple method to accurately describe this ‘delayed deposition’ effect, which is straightforward to use for analysis of observed light curves. We find that the ejecta heating is dominated by delayed deposition typically from 600 to 1200 d, and only later by longer lived isotopes 57Co and 55Fe decay (assuming solar abundance). For the relatively narrow 56Ni velocity distributions of commonly studied explosion models, the modification of the light curve depends mainly on the 56Ni mass-weighted average density, 〈ρ〉t3. Accurate late-time bolometric light curves, which may be obtained with JWST far-infrared (far-IR) measurements, will thus enable to discriminate between explosion models by determining 〈ρ〉t3 (and the 57Co and 55Fe abundances). The flattening of light curves inferred from recent observations, which is uncertain due to the lack of far-IR data, is readily explained by delayed deposition in models with $\langle \rho \rangle t^{3} \approx 0.2\, \mathrm{M}_{\odot }\, (10^{4}\, \textrm{km}\, \textrm{s}^{-1})^{-3}$, and does not imply supersolar 57Co and 55Fe abundances.

scholarly journals Light Curves of Type Ia Supernovae

2021 ◽  
Vol 47 (1) ◽  
pp. 1-11
Author(s):  
A. V. Lyutykh ◽  
M. V. Pruzhinskaya ◽  
S. I. Blinnikov
Keyword(s):  
Light Curve ◽  
Empirical Relation ◽  
Light Curves ◽  
Physical Parameters ◽  
Type Ia Supernovae ◽  
Type Ia ◽  
Ia Supernovae

Abstract We have studied the light curves of type Ia supernovae (SNe Ia) and the physical parameters inferred from them. We have constructed both analytical and numerical light curves of SNe Ia. Using an empirical relation between the SN luminosity and light-curve parameters, we have managed to impose constraints on the hydrodynamic solutions obtained by the STELLA code and to produce a sample of models that describe the observational properties of real SNe maximally accurately. With this sample we have established a relationship between the opacity in SN Ia ejecta and the parameters being determined directly from observations. The method has been tested on two classical SNe Ia as an example: 2011fe and 2012fr. The presented approach allows the opacity to be found without resorting to time-consuming computations.

scholarly journals Light Curve Models for SN 2009dc

2011 ◽  
Vol 7 (S281) ◽  
pp. 314-315
Author(s):  
Yasuomi Kamiya
Keyword(s):  
Light Curve ◽  
White Dwarfs ◽  
Light Curves ◽  
Host Galaxy ◽  
Type Ia Supernovae ◽  
Radiation Hydrodynamics ◽  
One Dimensional ◽  
Type Ia ◽  
Ia Supernovae

AbstractSimplified explosion models of super-Chandrasekhar-mass C-O white dwarfs (WDs) are constructed with parameters such as WD mass and 56Ni mass. Their light curves are obtained by solving one-dimensional equations of radiation hydrodynamics, and compared with the observations of SN 2009dc, one of the overluminous Type Ia supernovae, to estimate its properties. As a result, the progenitor of SN 2009dc is suggested to be a 2.2–2.4-M⊙ C-O WD with 1.2–1.4 M⊙ of 56Ni, if the extinction by its host galaxy is negligible.

scholarly journals An investigation of 56Ni shells as the source of early light curve bumps in type Ia supernovae

2020 ◽  
Vol 642 ◽  
pp. A189
Author(s):  
M. R. Magee ◽  
K. Maguire
Keyword(s):  
Light Curve ◽  
Light Curves ◽  
Radioactive Material ◽  
Type Ia Supernovae ◽  
Spectral Evolution ◽  
Strong Suppression ◽  
Shell Models ◽  
Type Ia ◽  
Optical Light Curve ◽  
Ia Supernovae

An excess of flux (i.e. a bump) in the early light curves of type Ia supernovae has been observed in a handful of cases. Multiple scenarios have been proposed to explain this excess flux. Recently, it has been shown that for at least one object (SN 2018oh) the excess emission observed could be the result of a large amount of 56Ni in the outer ejecta (∼0.03 M⊙). We present a series of model light curves and spectra for ejecta profiles containing 56Ni shells of varying masses (0.01, 0.02, 0.03, and 0.04 M⊙) and widths. We find that even for our lowest mass 56Ni shell, an increase of >2 magnitudes is produced in the bolometric light curve at one day after explosion relative to models without a 56Ni shell. We show that the colour evolution of models with a 56Ni shell differs significantly from those without and shows a colour inversion similar to some double-detonation explosion models. Furthermore, spectra of our 56Ni shell models show that strong suppression of flux between ∼3700–4000 Å close to maximum light appears to be a generic feature for this class of model. Comparing our models to observations of SNe 2017cbv and 2018oh, we show that a 56Ni shell of 0.02–0.04 M⊙ can match shapes of the early optical light curve bumps, but the colour and spectral evolution are in disagreement. Our models also predict a strong UV bump that is not observed. This would indicate that an alternative origin for the flux excess is necessary. In addition, based on existing explosion scenarios, producing such a 56Ni shell in the outer ejecta as required to match the light curve shape, without the presence of additional short-lived radioactive material, may prove challenging. Given that only a small amount of 56Ni in the outer ejecta is required to produce a bump in the light curve, such non-monotonically decreasing 56Ni distributions in the outer ejecta must be rare, if they were to occur at all.

scholarly journals Delay Time Distributions of Type Ia Supernovae from Galaxy and Cosmic Star Formation Histories

2020 ◽  
Vol 890 (2) ◽  
pp. 140 ◽  
Author(s):  
Louis-Gregory Strolger ◽  
Steven A. Rodney ◽  
Camilla Pacifici ◽  
Gautham Narayan ◽  
Or Graur
Keyword(s):  
Star Formation ◽  
Delay Time ◽  
Type Ia Supernovae ◽  
Type Ia ◽  
Ia Supernovae ◽  
Star Formation Histories

scholarly journals Determining the 56Ni distribution of type Ia supernovae from observations within days of explosion

2020 ◽  
Vol 634 ◽  
pp. A37 ◽  
Author(s):  
M. R. Magee ◽  
K. Maguire ◽  
R. Kotak ◽  
S. A. Sim ◽  
J. H. Gillanders ◽  
...  
Keyword(s):  
Light Curve ◽  
Current Model ◽  
Light Curves ◽  
Radioactive Isotopes ◽  
Type Ia Supernovae ◽  
Maximum Light ◽  
Thermonuclear Supernovae ◽  
Type Ia ◽  
Model Set ◽  
Ia Supernovae

Recent studies have shown how the distribution of 56Ni within the ejected material of type Ia supernovae can have profound consequences on the observed light curves. Observations at early times can therefore provide important details on the explosion physics in thermonuclear supernovae, which are poorly constrained. To this end, we present a series of radiative transfer calculations that explore variations in the 56Ni distribution. Our models also show the importance of the density profile in shaping the light curve, which is often neglected in the literature. Using our model set, we investigate the observations that are necessary to determine the 56Ni distribution as robustly as possible within the current model set. We find that this includes observations beginning at least ∼14 days before B-band maximum, extending to approximately maximum light with a relatively high (≲3 day) cadence, and in at least one blue and one red band (such as B and R, or g and r) are required. We compare a number of well-observed type Ia supernovae that meet these criteria to our models and find that the light curves of ∼70–80% of objects in our sample are consistent with being produced solely by variations in the 56Ni distributions. The remaining supernovae show an excess of flux at early times, indicating missing physics that is not accounted for within our model set, such as an interaction or the presence of short-lived radioactive isotopes. Comparing our model light curves and spectra to observations and delayed detonation models demonstrates that while a somewhat extended 56Ni distribution is necessary to reproduce the observed light curve shape, this does not negatively affect the spectra at maximum light. Investigating current explosion models shows that observations typically require a shallower decrease in the 56Ni mass towards the outer ejecta than is produced for models of a given 56Ni mass. Future models that test differences in the explosion physics and detonation criteria should be explored to determine the conditions necessary to reproduce the 56Ni distributions found here.

scholarly journals The rate of type Ia Supernovae and the Star Formation History

2009 ◽  
Author(s):  
L. Greggio ◽  
E. Cappellaro ◽  
Giuliana Giobbi ◽  
Amedeo Tornambe ◽  
Gabriella Raimondo ◽  
...  
Keyword(s):  
Star Formation ◽  
Star Formation History ◽  
Type Ia Supernovae ◽  
Formation History ◽  
Type Ia ◽  
Ia Supernovae

scholarly journals Correlation of the rate of Type Ia supernovae with the parent galaxy properties: Light and shadows

2019 ◽  
Vol 625 ◽  
pp. A113 ◽  
Author(s):  
L. Greggio ◽  
E. Cappellaro
Keyword(s):  
Binary Systems ◽  
Cosmological Parameters ◽  
Stellar Populations ◽  
Star Formation History ◽  
Close Binary ◽  
Type Ia Supernovae ◽  
Wide Range ◽  
Type Ia ◽  
Ia Supernovae ◽  
Parent Galaxy

Context. The identification of the progenitors of Type Ia supernovae (SNIa) is extremely important in several astrophysical contexts, ranging from stellar evolution in close binary systems to evaluating cosmological parameters. Determining the distribution of the delay times (DTD) of SNIa progenitors can shed light on their nature. The DTD can be constrained by analysing the correlation between the SNIa rate and those properties of the parent galaxy which trace the average age of their stellar populations. Aims. We investigate the diagnostic capabilities of this correlation by examining its systematics with the various parameters at play: simple stellar population models, the adopted description for the star formation history (SFH) in galaxies, and the way in which the masses of the galaxies are evaluated. Methods. We computed models for the diagnostic correlations for a variety of input ingredients and for a few astrophysically motivated DTD laws appropriate for a wide range of possibilities for the SNIa progenitors. The models are compared to the results of three independent observational surveys. Results. The scaling of the SNIa rate with the properties of the parent galaxy is sensitive to all input ingredients mentioned above. This is a severe limitation on the possibility to discriminate alternative DTDs. In addition, current surveys show some discrepancies for the reddest and bluest galaxies, likely because of limited statistics and the inhomogeneity of the observations. For galaxies with intermediate colours the rates are in agreement, leading to a robust determination of the productivity of SNIa from stellar populations of ≃0.8 events per 1000 M⊙. Conclusions. Large stastistics of SNIa events along with accurate measurements of the SFH in the galaxies are required to derive firm constraints on the DTD. The LSST will achieve these results by providing a homogeneous, unbiased, and vast database on both SNIa and galaxies.

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