Supernova 1991T and the Value of the Hubble Constant

Gibson, Brad K.; Stetson, P. B.

doi:10.1086/318905

Cited by 36 publications

(51 citation statements)

References 23 publications

(55 reference statements)

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“…As a result, there is some disagreement in the literature on the magnitudes of other standard candles. For example, two recent calibrations of the peak absolute magnitude of SNe Ia, based on the SNe Ia events in galaxies with known Cepheid distances result in slightly different magnitudes: M B = −19.56 (Parodi et al 2000) and M B = −19.32 (Gibson & Stetson 2001). The method based on modeling the expanding photospheres of SNe II is a "physical method" and is hence completely independent of the calibration of the local distance scale.…”

Section: Appendix A: Distances and Luminositiesmentioning

confidence: 99%

Oxygen and nitrogen abundances in nearby galaxies

Pilyugin¹,

Vı́lchez²,

Contini³

2004

A&A

302

409

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Abstract. We performed a compilation of more than 1000 published spectra of H  regions in spiral galaxies. The oxygen and nitrogen abundances in each H  region were recomputed in a homogeneous way, using the P-method. The radial distributions of oxygen and nitrogen abundances were derived. The correlations between oxygen abundance and macroscopic properties are examined. We found that the oxygen abundance in spiral galaxies correlates with its luminosity, rotation velocity, and morphological type: the correlation with the rotation velocity may be slightly tighter. There is a significant difference between the luminosity-metallicity relationship obtained here and that based on the oxygen abundances determined through the R 23 -calibrations. The oxygen abundance of NGC 5457 recently determined using direct measurements of T e (Kennicutt et al. 2003) agrees with the luminosity-metallicity relationship derived in this paper, but is in conflict with the luminosity-metallicity relationship derived with the R 23 -based oxygen abundances. The obtained luminosity-metallicity relation for spiral galaxies is compared to that for irregular galaxies. Our sample of galaxies shows evidence that the slope of the O/H − M B relationship for spirals (−0.079 ± 0.018) is slightly more shallow than that for irregular galaxies (−0.139 ± 0.011). The effective oxygen yields were estimated for spiral and irregular galaxies. The effective oxygen yield increases with increasing luminosity from M B ∼ −11 to M B ∼ −18 (or with increasing rotation velocity from V rot ∼ 10 km s −1 to V rot ∼ 100 km s −1 ) and then remains approximately constant. Irregular galaxies from our sample have effective oxygen yields lowered by a factor of 3 at maximum, i.e. irregular galaxies usually keep at least 1/3 of the oxygen they manufactured during their evolution.

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Section: Appendix A: Distances and Luminositiesmentioning

confidence: 99%

Oxygen and nitrogen abundances in nearby galaxies

Pilyugin¹,

Vı́lchez²,

Contini³

2004

A&A

302

409

View full text Add to dashboard Cite

show abstract

“…With such a range, astronomers could either largely reject the SN Ia models by the observed upper limits or find that almost all models were consistent (see Leising et al 1995 for an explanation of the difficulties simultaneously explaining the optical and gamma-ray observations of SN 1991T). New studies have narrowed the distances to a range of 11.3-14.0 Mpc (Richtler et al 2001;Gibson & Stetson 2001;Saha et al 2001). 9 For this work, we place NGC 4527 at 11.3 and 14.0 Mpc.…”

Section: Cgro Comptel and Osse Observ Vations Of Sn 1991tmentioning

confidence: 99%

“…Distance estimates have ranged from 9:6 AE 0:6 Mpc from planetary nebulae (Feldmeier et al 1997) to 11:6 AE 0:9 Mpc from Hubble Space Telescope (HST ) Cepheid period luminosity estimates (Tanvir et al 1995). Subsequent HST Cepheid period luminosity estimates place M96 at 9.9-11.3 Mpc (Gibson & Stetson 2001;Gibson et al 2000;Hjorth & Tanvir 1997), the range we use in this study. The CGRO team was able to begin observations at about maximum light.…”

Section: Cgro Comptel Observv Ations Of Sn 1998bumentioning

confidence: 99%

Unified One‐Dimensional Simulations of Gamma‐Ray Line Emission from Type Ia Supernovae

Milne

Hungerford

Fryer

et al. 2004

ApJ

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The light curves of Type Ia supernovae (SNe Ia) are powered by gamma rays emitted by the decay of radioactive elements such as 56 Ni and its decay products. These gamma rays are downscattered, absorbed, and eventually reprocessed into the optical emission that makes up the bulk of all SN observations. Detection of the gamma rays that escape the expanding star provide the only direct means to study this power source for SN Ia light curves. Unfortunately, disagreements between calculations for the gamma-ray lines have made it difficult to interpret any gamma-ray observations. Here we present a detailed comparison of the major gamma-ray line transport codes for a series of one-dimensional SN Ia models. Discrepancies in past results were due to errors in the codes, and the corrected versions of the seven different codes yield very similar results. This convergence of the simulation results allows us to infer more reliable information from the current set of gamma-ray observations of SNe Ia. The observations of SN 1986G, SN 1991T, and SN 1998bu are consistent with explosion models based on their classification:

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“…Data processing followed the precepts outlined in Gibson & Stetson (2001, and references therein). Instrumental photometry was provided by allframe (Stetson 1994), while a version of trial (Stetson 1996) – customized for WFPC2 data and the fitting of Cepheid light curves in the V and I photometric bands – was used for calibration and variable finding.…”

Section: Discussionmentioning

confidence: 99%

“…Unfortunately, no H ii regions in this field have thus far been observed. Adopting a conservative metallicity range of (as we did for the analysis of the NGC 4527 data set –Gibson & Stetson 2001) would increase the inferred mean true modulus by ∼ 0.08 mag.…”

Section: Discussionmentioning

confidence: 99%

The distance to Supernova 1998aq in NGC 3982

Stetson

Gibson

2001

Monthly Notices of the Royal Astronomical Society

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The distance to NGC 3982, host galaxy to the Type Ia supernova SN 1998aq, is derived using 32 Cepheids discovered in archival multi‐epoch Hubble Space Telescope observations. Employing recent Large Magellanic Cloud Cepheid period–luminosity relations and absolute zero‐point, we find a distance to NGC 3982 of , including both random (r) and systematic (s) uncertainties, and ignoring any metallicity dependence in the Cepheid period–luminosity relation. Still unpublished light curve photometry promises to make SN 1998aq one of the most important calibrators for the Type Ia supernova decline rate–peak luminosity relationship.

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Supernova 1991T and the Value of the Hubble Constant

Cited by 36 publications

References 23 publications

Oxygen and nitrogen abundances in nearby galaxies

Oxygen and nitrogen abundances in nearby galaxies

Unified One‐Dimensional Simulations of Gamma‐Ray Line Emission from Type Ia Supernovae

The distance to Supernova 1998aq in NGC 3982

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