Low Hubble Constant from the Physics of Type Ia Supernovae

Nugent, P.; Branch, David; Baron, E.; Fisher, Adam; Vaughan, Thomas E.; Hauschildt, P. H.

doi:10.1103/physrevlett.75.394

Cited by 37 publications

(28 citation statements)

References 26 publications

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“…The mass of 56 Ni synthesized during explosion can be estimated following the principle that the bolometric luminosity, L bol , at maximum light is proportional to the instantaneous rate of radioactive decay (Arnett 1982). The simplified formulation of Arnett's rule, to estimate the mass of 56 Ni, , as proposed by Nugent et al (1995), involves α, the ratio of bolometric to radioactivity luminosity, and , the radioactivity luminosity per unit nickel mass, which depends on the rise time of the supernova to maximum light. The peak UBVRI bolometric luminosity for SN 2009jf is estimated as 3 +0.6 −0.5 × 10 42 erg s −1 ; the quoted uncertainty is mainly due to the uncertainty in H 0 .…”

Section: Absolute Magnitude Bolometric Light Curve and Mass Of 56nimentioning

confidence: 99%

Optical studies of SN 2009jf: a Type Ib supernova with an extremely slow decline and aspherical signature

Sahu

Gurugubelli

Anupama

et al. 2011

Monthly Notices of the Royal Astronomical Society

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Optical UBVRI photometry and medium‐resolution spectroscopy of the Type Ib supernova SN 2009jf, during the period from ∼ −15 to +250 d, with respect to the B maximum are reported. The light curves are broad, with an extremely slow decline. The early post‐maximum decline rate in the V band is similar to SN 2008D; however, the late‐phase decline rate is slower than other Type Ib supernovae studied. With an absolute magnitude of MV=−17.96 ± 0.19 at peak, SN 2009jf is a normally bright supernova. The peak bolometric luminosity and the energy deposition rate via the 56Ni →56Co chain indicate that ∼0.17+0.03−0.03 M⊙ of 56Ni was ejected during the explosion. The He i 5876 Å line is clearly identified in the first spectrum of day ∼ −15, at a velocity of ∼16 000 km s−1. The [O i] 6300–6364 Å line seen in the nebular spectrum has a multipeaked and asymmetric emission profile, with the blue peak being stronger. The estimated flux in this line implies that ≳1.34 M⊙ oxygen was ejected. The slow evolution of the light curves of SN 2009jf indicates the presence of a massive ejecta. The high expansion velocity in the early phase and broader emission lines during the nebular phase suggest it to be an explosion with a large kinetic energy. A simple qualitative estimate leads to the ejecta mass of Mej= 4–9 M⊙ and kinetic energy EK= 3–8 × 1051 erg. The ejected mass estimate is indicative of an initial main‐sequence mass of ≳20–25 M⊙.

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Section: Absolute Magnitude Bolometric Light Curve and Mass Of 56nimentioning

confidence: 99%

Optical studies of SN 2009jf: a Type Ib supernova with an extremely slow decline and aspherical signature

Sahu

Gurugubelli

Anupama

et al. 2011

Monthly Notices of the Royal Astronomical Society

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“…It may be encouraging that the result of different SN Ia based methods agree if SN Ia are not treated as as standard candles. Hamuy et al (1995) found 65±5, Riess et al (1995) give 67±5, and Fisher et al (1995), Nugent et al (1995b) and Branch et al, (1995) get a values of 60 ± 10, 60 ± 12 and 58 ± 7, respectively. From our models, both the empirical relations between M V /dM (15) like-relations and the ansatz to deselect subluminous SNeIa seems to be justified, but we expect an individual dispersion of ≈ 20% (Hamuy et al 1995b).…”

Section: Distance Determinations H O and Q Omentioning

confidence: 99%

Explosion Models, Light Curves, Spectra and H o

Höflich

Khokhlov

Wheeler

et al. 1997

Thermonuclear Supernovae

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Abstract. From the spectra and light curves it is clear that SNIa events are thermonuclear explosions of white dwarfs. However, details of the explosion are highly under debate. Here, we present detailed models which are consistent with respect to the explosion mechanism, the optical and infrared light curves (LC), and the spectral evolution. This leaves the description of the burning front and the structure of the white dwarf as the only free parameters. The explosions are calculated using one-dimensional Lagrangian codes including nuclear networks. Subsequently, optical and IR-LCs are constructed. Detailed NLTE-spectra are computed for several instants of time using the density, chemical and luminosity structure resulting from the LCs. The general methods and critical tests are presented (sect. 2).Different models for the thermonuclear explosion are discussed including detonations, deflagrations, delayed detonations, pulsating delayed detonations (PDD) and helium detonations (sect.3). Comparisons between theoretical and observed LCs and spectra provide an insight into details of the explosion and nature of the progenitor stars (sect. 4 & 5). We try to answer several related questions. Are subluminous SNe Ia a group different from 'normal' SN Ia (sect. 5)? Can we understand observed properties of the LCs and spectra (sect. 4)? What do we learn about the progenitor evolution and its metallicity (sect. 3, Figs. 4,5)? Do successful SN Ia models depend on the type of the host galaxy (Table 2) Using both the spectral and LC information, theoretical models allow for a determination of the Hubble constant independent from 'local' distance indicators such as δ Cephei stars. H o is found to be 67 ± 9 km s −1 M pc −1 and, from SN1988U, q o equals 0.7 ± 1. within 95 % confidence levels.

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“…In addition, the B and V filter functions are given according to Bessell (1990). The horizontal lines at about 5500Å give the mean flux level in V which would be required for BC of 0.1 m (dots) and 0.30 m (dashed dotted, new value of Nugent 1995 (private communication) based on spectral fits (Nugent et al 1995b)). …”

Section: Appendix: Remark On Bolometric Correctionsmentioning

confidence: 99%

Explosion Models for Type IA Supernovae: A Comparison with Observed Light Curves, Distances, H 0, and Q 0

Hoêflich¹,

Khokkhlov²

1996

ApJ

464

538

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Theoretical monochromatic light curves and photospheric expansion velocities are compared with observations of 27 Type Ia supernovae (SNe Ia). A set of 37 models has been considered which encompasses all currently discussed explosion scenarios for Type Ia supernovae including deflagrations, detonations, delayed detonations, pulsating delayed detonations and tamped detonations of Chandrasekhar mass, and Helium detonations of low mass white dwarfs. The explosions are calculated using one-dimensional Lagrangian hydro and radiation-hydro codes with incorporated nuclear networks. Subsequently, light curves are constructed using our LC scheme which includes an implicit radiation transport, expansion opacities, a Monte-Carlo γ-ray transport, and molecular and dust formation. For some supernovae, results of detailed non-LTE calculations have been considered.Observational properties of our series of models are discussed, in particular, the relation between the absolute brightness, post-maximum decline rates, the colors at several moments of time, etc. All models with a 56 Ni production larger than ≈ 0.4M ⊙ produce light curves of similar brightness. The influence of the cosmological red shift on the light curves and on the correction for interstellar reddening is discussed.Based on data rectification of the standard deviation, a quantitative procedure to fit the observations has been used to the determine the free parameters, i.e. the distance, the reddening, and the time of the explosion. Fast rising light curves (e.g., SN 1981B and SN 1994D) can be reproduced by delayed detonation models or deflagration models similar to W7. Slowly rising (t max ≥ 16 days) light curves (e.g., SN 1984A and SN 1990N) cannot be reproduced by standard detonation, deflagration, or delayed detonation models. To obtain an acceptable agreement with observations, models are required where the C/O white dwarf is surrounded by an unburnt extended envelope of typically 0.2 to 0.4 M ⊙ which may either be pre-existing or produced during the explosion. Our interpretation of the light curves is also supported by the photospheric expansion velocities. Mainly due to the fast increase of the γ radiation produced by the outer 56 Ni , the post maximum decline of Helium detonations tends to be faster compared to observations of normal bright SNe Ia.Strongly subluminous SNe Ia can be understood in the framework of pulsating delayed detonations, both from the absolute brightness and the colors. Alternatively, subluminosity can be produced within the scenario of helium detonations in low mass white dwarfs of about 0.6 to 0.8 M ⊙ if the explosion occurs when rather little Helium has been accreted. However, even subluminous Helium detonation models are very blue at maximum light owing to heating in the outer layers and brighter models show a fast postmaximum decline, in contradiction to the observations. 3We find evidence for a correlation between the type of host galaxy and the explosion mechanism. In spiral galaxies, about the same amount of prompt exp...

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Low Hubble Constant from the Physics of Type Ia Supernovae

Cited by 37 publications

References 26 publications

Optical studies of SN 2009jf: a Type Ib supernova with an extremely slow decline and aspherical signature

Optical studies of SN 2009jf: a Type Ib supernova with an extremely slow decline and aspherical signature

Explosion Models, Light Curves, Spectra and H o

Explosion Models for Type IA Supernovae: A Comparison with Observed Light Curves, Distances, H 0, and Q 0

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