The blue anbd visual absolute magnitude distributions of Type IA supernovae

1995 ◽  
Vol 439 ◽  
pp. 558 ◽  
Author(s):  
Thomas E. Vaughan ◽  
David Branch ◽  
Douglas L. Miller ◽  
Saul Perlmutter
Keyword(s):  
Absolute Magnitude ◽  
Type Ia Supernovae ◽  
Type Ia ◽  
Ia Supernovae

Optical and UV studies of type Ia supernovae SN 2009ig and SN 2012cg

2019 ◽  
Vol 487 (2) ◽  
pp. 1886-1904 ◽  
Author(s):  
N K Chakradhari ◽  
D K Sahu ◽  
G C Anupama
Keyword(s):  
Maximum Velocity ◽  
Absolute Magnitude ◽  
Type Ia Supernovae ◽  
Strength Ratio ◽  
Rate Parameter ◽  
Spectral Evolution ◽  
Maximum Phase ◽  
Decline Rate ◽  
Type Ia ◽  
Ia Supernovae

Abstract We present an extensive optical–ultraviolet photometry and analysis of a series of optical spectra of type Ia supernovae SN 2009ig and SN 2012cg. The observations range from −15 to +185 d for SN 2009ig and from −14 to 316 d for SN 2012cg, with respect to maximum light in B band. Both SN 2009ig and SN 2012cg exhibit similar properties. They have similar decline rate parameter (Δm15(B)true = 0.92 ± 0.04 for SN 2009ig and 0.93 ± 0.06 for SN 2012cg) and B band peak absolute magnitude (−19.45 ± 0.40 mag for SN 2009ig and −19.50 ± 0.31 mag for SN 2012cg). Their early spectra show high-velocity features in Si ii and Ca ii lines. The strong Fe iii, Si iii, and weak Si ii λ5972 line during pre-maximum phase are indicative of hot photosphere. The post-maximum velocity evolution shows a plateau like phase with velocities ∼13 000 km s−1 for SN 2009ig and ∼10 000 km s−1 for SN 2012cg. Both events show spectral evolution similar to normal SNe Ia and fall in LVG and Core Normal subgroup. Both have smaller strength ratio [$\cal R$(Si ii) = 0.17 for SN 2009ig and 0.20 for SN 2012cg] consistent with smaller Δm15(B). Peak bolometric luminosities ($\log L_\text{bol}^\text{max}$) of these events are estimated as 43.17 ± 0.16 and 43.24 ± 0.11 erg s−1 suggesting that 0.60 ± 0.20 M⊙ of 56Ni was synthesized in the explosion of SN 2009ig and 0.72 ± 0.31 M⊙ in SN 2012cg.

scholarly journals Testing the evolution of the absolute magnitude of type Ia supernovae and cosmological parameters

2021 ◽  
pp. 484-489
Author(s):  
A. P. Mahtessian ◽  
G. S. Karapetian ◽  
M. A. Hovhannisyan ◽  
V. H. Movsisyan ◽  
L. A. Mahtessian
Keyword(s):  
Computer Simulations ◽  
Cosmological Parameters ◽  
Absolute Magnitude ◽  
Type Ia Supernovae ◽  
Zero Density ◽  
Type Ia ◽  
The Absolute ◽  
Ia Supernovae ◽  
The Universe

Computer simulations show that, in estimating cosmological parameters, the best agreement between theory and observation is achieved by assuming the evolution of the absolute magnitude of type Ia supernovae. This requires only 0.3m of evolution for the time corresponding to z = 1. This leads to zero density of hidden energy in the Universe.

scholarly journals Probing cosmic opacity with the type Ia supernovae and Hubble parameter

2020 ◽  
Vol 80 (9) ◽  
Author(s):  
Bing Xu ◽  
Kaituo Zhang ◽  
Qihong Huang
Keyword(s):  
Hubble Parameter ◽  
Likelihood Function ◽  
Nuisance Parameter ◽  
Hubble Constant ◽  
Absolute Magnitude ◽  
Type Ia Supernovae ◽  
Spatial Curvature ◽  
Type Ia ◽  
Ia Supernovae ◽  
Best Fit

AbstractIn this paper, we probe the cosmic opacity with the newest Pantheon type Ia supernovae (SNIa) and the observational Hubble parameter $$\left( H(z)\right) $$ H ( z ) data based on the $$\Lambda $$ Λ CDM and wCDM models with or without spatial curvature. In the analysis, we marginalize the likelihood function of SNIa data over the pertinent nuisance parameter $${\mathcal {M}}$$ M , a combination of the absolute magnitude of SNIa $$M_{\mathrm{B}}$$ M B and the Hubble constant $$H_0$$ H 0 , with a flat prior. Two parameterizations of the optical depth $$\tau (z)$$ τ ( z ) associated to the cosmic absorption, namely $$\tau (z)=2\varepsilon z$$ τ ( z ) = 2 ε z and $$\tau (z)= (1+z)^{2\varepsilon }-1$$ τ ( z ) = ( 1 + z ) 2 ε - 1 , are adopted. We find that the results are not sensitive to the fiducial cosmological models, the spatial curvature and parameterizations of $$\tau (z)$$ τ ( z ) . Moreover, the results from the Pantheon data alone are consistent with a transparent universe ($$\varepsilon =0$$ ε = 0 ). And once the H(z) data is combined, $$\varepsilon =0$$ ε = 0 falls within the 68% confidence level (CL) of the best fit when a flat $$H_0$$ H 0 prior or the distance priors are used, while it falls within the 95% CL when a Gaussian distribution prior of $$H_0=74.03\pm 1.42$$ H 0 = 74.03 ± 1.42 km $$\mathrm {s}^{-1}\, \mathrm {Mpc}^{-1}$$ s - 1 Mpc - 1 is used.

scholarly journals A new measurement of the Hubble constant using Type Ia supernovae calibrated with surface brightness fluctuations

2021 ◽  
Vol 647 ◽  
pp. A72 ◽  
Author(s):  
Nandita Khetan ◽  
Luca Izzo ◽  
Marica Branchesi ◽  
Radosław Wojtak ◽  
Michele Cantiello ◽  
...  
Keyword(s):  
Surface Brightness ◽  
Hubble Constant ◽  
Absolute Magnitude ◽  
Host Galaxy ◽  
Type Ia Supernovae ◽  
Distance Measurements ◽  
Surface Brightness Fluctuations ◽  
Type Ia ◽  
Red Giant ◽  
Ia Supernovae

We present a new calibration of the peak absolute magnitude of Type Ia supernovae (SNe Ia) based on the surface brightness fluctuations (SBF) method, aimed at measuring the value of the Hubble constant. We build a sample of calibrating anchors consisting of 24 SNe hosted in galaxies that have SBF distance measurements. Applying a hierarchical Bayesian approach, we calibrate the SN Ia peak luminosity and extend the Hubble diagram into the Hubble flow by using a sample of 96 SNe Ia in the redshift range 0.02 < z < 0.075, which was extracted from the Combined Pantheon Sample. We estimate a value of H0 = 70.50 ± 2.37 (stat.) ± 3.38 (sys.) km s−1 Mpc−1 (i.e., 3.4% stat., 4.8% sys.), which is in agreement with the value obtained using the tip of the red giant branch calibration. It is also consistent, within errors, with the value obtained from SNe Ia calibrated with Cepheids or the value inferred from the analysis of the cosmic microwave background. We find that the SNe Ia distance moduli calibrated with SBF are on average larger by 0.07 mag than those calibrated with Cepheids. Our results point to possible differences among SNe in different types of galaxies, which could originate from different local environments and/or progenitor properties of SNe Ia. Sampling different host galaxy types, SBF offers a complementary approach to using Cepheids, which is important in addressing possible systematics. As the SBF method has the ability to reach larger distances than Cepheids, the impending entry of the Vera C. Rubin Observatory and JWST into operation will increase the number of SNe Ia hosted in galaxies where SBF distances can be measured, making SBF measurements attractive for improving the calibration of SNe Ia, as well as in the estimation of H0.

Hard X‐Rays and Gamma Rays from Type Ia Supernovae

1998 ◽  
Vol 492 (1) ◽  
pp. 228-245 ◽  
Author(s):  
P. Hoflich ◽  
J. C. Wheeler ◽  
A. Khokhlov
Keyword(s):  
Gamma Rays ◽  
Type Ia Supernovae ◽  
X Rays ◽  
Type Ia ◽  
Ia Supernovae

scholarly journals Gravitational Collapse versus Thermonuclear Explosion of Degenerate Stellar Cores

1994 ◽  
Vol 147 ◽  
pp. 186-213
Author(s):  
J. Isern ◽  
R. Canal
Keyword(s):  
Neutron Star ◽  
White Dwarfs ◽  
Light Curves ◽  
Type Ia Supernovae ◽  
Radioactive Elements ◽  
Border Line ◽  
Thermonuclear Explosion ◽  
Type Ia ◽  
Γ Rays ◽  
Ia Supernovae

AbstractIn this paper we review the behavior of growing stellar degenerate cores. It is shown that ONeMg white dwarfs and cold CO white dwarfs can collapse to form a neutron star. This collapse is completely silent since the total amount of radioactive elements that are expelled is very small and a burst of γ-rays is never produced. In the case of an explosion (always carbonoxygen cores), the outcome fits quite well the observed properties of Type Ia supernovae. Nevertheless, the light curves and the velocities measured at maximum are very homogeneous and the diversity introduced by igniting at different densities is not enough to account for the most extreme cases observed. It is also shown that a promising way out of this problem could be the He-induced detonation of white dwarfs with different masses. Finally, we outline that the location of the border line which separetes explosion from collapse strongly depends on the input physics adopted.

Sign in / Sign up

Export Citation Format

Share Document