The Type IA supernova 1989B in NGC 3627 (M66)

Wells, Lisa A.; Phillips, M. M.; Suntzeff, Nicholas B.; Heathcote, Steve; Hamuy, M.; Navarrete, Mauricio; Fernández, M.; Weller, W.; Schommer, R. A.; Kirshner, R.; Leibundgut, B.; Willner, S. P.; Peletier, Reynier F.; Schlegel, Eric M.; Wheeler, J. C.; Harkness, Robert; Bell, David; Matthews, J. M.; Filippenko, A. V.; Shields, J. C.; Richmond, M.; Jewitt, David; Luu, Jane; Tran, H. D.; Appleton, P. N.; Robson, E. I.; Tyson, J. A.; Guhathakurta, Puragra; Eder, J.; Bond, Howard E.; Potter, Michael; Veilleux, Sylvain; Porter, Alain C.; Humphreys, R. M.; Janes, K. A.; Williams, T. B.; Costa, E.; Ruíz, M. T.; Lee, J. T.; Lutz, J. H.; Rich, R. Michael; Winkler, P. F.; Tyson, Neil deGrasse

doi:10.1086/117236

Cited by 130 publications

(79 citation statements)

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“…The BVI light curve parameters are mainly based on CCD photometry of Wells et al (1994) and compiled in RTS05. The maximum magnitudes agree within 0.02 mag with independent templet fits by Wang et al …”

Section: The Sn 1989b In Ngc 3627mentioning

confidence: 99%

The luminosity of supernovae of type Ia from tip of the red-giant branch distances and the value ofH₀

Tammann¹,

Reindl²

2013

A&A

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Distances from the tip of the red-giant branch (TRGB) in the halo population of galaxies -calibrated through RR Lyr stars as well as tied to Hipparcos parallaxes and further supported by stellar models -are used to determine the luminosity of six nearby type Ia supernovae (SN 2011fe, 2007sr, 1998bu, 1989B, 1972E, and 1937C). The result is M corr V = −19.41 ± 0.05. If this value is applied to 62 SNe Ia with 3000 < v < 20, 000 km s −1 a large-scale value of the Hubble constant follows of H 0 = 64.0 ± 1.6 ± 2.0. The SN HST Project gave H 0 = 62.3 ± 1.3 ± 5.0 from ten Cepheid-calibrated SNe Ia. The near agreement of young Population I (Cepheids) and old, metal-poor Population II (TRGB) distance indicators is satisfactory. The combined weighted result is H 0 = 63.7 ± 2.3 (i.e. ±3.6%). The value will be helpful to constrain models of the early Universe.

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Section: The Sn 1989b In Ngc 3627mentioning

confidence: 99%

The luminosity of supernovae of type Ia from tip of the red-giant branch distances and the value ofH₀

Tammann¹,

Reindl²

2013

A&A

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“…These comprised combined de-reddened UV-optical spectra of SN 1990N at −14 and −7 days (Leibundgut et al 1991), SN 1989B at −5 (Wells et al 1994 and UV spectra from the IUE archive), SN 1981B (Branch et al 1983), SN 1992A at +5, +9 and +17 (Kirshner et al 1993), and SN 2001el between +30 and +66 (from HS T archive). For spectra that did not cover the full 2000-9000 Å range we extrapolated to 9000 Å using spectra of SN 2003du.…”

Section: The Bolometric Light Curvementioning

confidence: 99%

SN 2003du: 480 days in the life of a normal type Ia supernova

Stanishev¹,

Goobar²,

Benetti

et al. 2007

A&A

163

156

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Aims. We present a study of the optical and near-infrared (NIR) properties of the Type Ia Supernova (SN Ia) 2003du.Methods. An extensive set of optical and NIR photometry and low-resolution long-slit spectra was obtained using a number of facilities. The observations started 13 days before B-band maximum light and continued for 480 days with exceptionally good time sampling. The optical photometry was calibrated through the S-correction technique. Results. The UBVRIJHK light curves and the color indices of SN 2003du closely resemble those of normal SNe Ia. SN 2003du reached a B-band maximum of 13.49 ± 0.02 mag on JD2 452 766.38 ± 0.5. We derive a B-band stretch parameter of 0.988 ± 0.003, which corresponds to ∆m 15 = 1.02 ±0.05, indicative of a SN Ia of standard luminosity. The reddening in the host galaxy was estimated by three methods, and was consistently found to be negligible. Using an updated calibration of the V and JHK absolute magnitudes of SNe Ia, we find a distance modulus µ = 32.79 ± 0.15 mag to the host galaxy, UGC 9391. We measure a peak uvoir bolometric luminosity of 1.35(±0.20) × 10 43 erg s −1 and Arnett's rule implies that M56 Ni 0.68 ± 0.14 M of 56 Ni was synthesized during the explosion. Modeling of the uvoir bolometric light curve also indicates M56 Ni in the range 0.6−0.8 M . The spectral evolution of SN 2003du at both optical and NIR wavelengths also closely resembles normal SNe Ia. In particular, the Si ii ratio at maximum R(Si ii) = 0.22 ± 0.02 and the time evolution of the blueshift velocities of the absorption line minima are typical. The pre-maximum spectra of SN 2003du showed conspicuous high-velocity features in the Ca ii H&K doublet and infrared triplet, and possibly in Si ii λ6355, lines. We compare the time evolution of the profiles of these lines with other well-observed SNe Ia and we suggest that the peculiar pre-maximum evolution of Si ii λ6355 line in many SNe Ia is due to the presence of two blended absorption components.

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“…cases because its structure resembles those of DD models but it has some problems with the high velocities of Si lines in SN1994D . Wells et al (1994). In the lower left plot, the photospheric velocity of the delayed detonation model M37 is given in comparison with the expansion velocities implied by the line shifts of Mg II and SiII.…”

Section: Comparison Between Observation and Models Predictionsmentioning

confidence: 99%

Explosion Models, Light Curves, Spectra and H o

Höflich

Khokhlov

Wheeler

et al. 1997

Thermonuclear Supernovae

Self Cite

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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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The Type IA supernova 1989B in NGC 3627 (M66)

Cited by 130 publications

References 0 publications

The luminosity of supernovae of type Ia from tip of the red-giant branch distances and the value ofH₀

The luminosity of supernovae of type Ia from tip of the red-giant branch distances and the value ofH₀

SN 2003du: 480 days in the life of a normal type Ia supernova

Explosion Models, Light Curves, Spectra and H o

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The Type IA supernova 1989B in NGC 3627 (M66)

Cited by 130 publications

References 0 publications

The luminosity of supernovae of type Ia from tip of the red-giant branch distances and the value ofH0

The luminosity of supernovae of type Ia from tip of the red-giant branch distances and the value ofH0

SN 2003du: 480 days in the life of a normal type Ia supernova

Explosion Models, Light Curves, Spectra and H o

Contact Info

Product

Resources

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The luminosity of supernovae of type Ia from tip of the red-giant branch distances and the value ofH₀

The luminosity of supernovae of type Ia from tip of the red-giant branch distances and the value ofH₀