Determination of the Hubble constant from observations of Cepheid variables in the galaxy M96

Tanvir, N. R.; Shanks, T.; Ferguson, Henry C.; Robinson, D. K.

doi:10.1038/377027a0

Cited by 125 publications

(124 citation statements)

References 41 publications

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“…The host galaxy M 96 had a HST-Cepheid-determined distance of 11.6 ± 0.9 Mpc (Tanvir et al 1995), later revised to 11.3 ± 0.9 Mpc by Hjorth & Tanvir (1997). This makes SN1998bu one of seven SN observed in galaxies with a distance set by Cepheid measurements.…”

Section: Discussionmentioning

confidence: 99%

COMPTEL upper limits for the $^{\sf 56}$Coγ-ray emission from SN1998bu

Georgii

Plüschke

Diehl

et al. 2002

A&A

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Abstract. Supernova 1998bu in the galaxy M 96 was observed by COMPTEL for a total of 88 days starting 17 days after the explosion. We searched for a signal in the 847 keV and 1238 keV lines of radioactive 56 Co from this type Ia supernova. Using several different analysis methods, we did not detect SN1998bu. Our measurements should have been sensitive enough to detect 60 Co gamma-rays as predicted from supernova models. Our 2σ flux limit is 2.3 × 10 −5 photons cm −2 s −1 ; this would correspond to 0.35 M of ejected 56 Ni, if SN1998bu were at a distance of 11.3 Mpc and transparent to MeV gamma rays for the period of our measurements. We discuss our measurements in the context of common supernova models, and conclude disfavoring a supernova event with large mixing and major parts of the freshly-generated radioactivity in outer layers.

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Section: Discussionmentioning

confidence: 99%

COMPTEL upper limits for the $^{\sf 56}$Coγ-ray emission from SN1998bu

Georgii

Plüschke

Diehl

et al. 2002

A&A

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“…Four of these SNe Ia were spectroscopically normal ) and the single spectrum that is available for the fifth, SN 1895B (Schaefer 1995b), is consistent with normalcy. In addition, as discussed by BRB95, the Cepheid-based distance to M96 measured by Tanvir et al (1995) appears to have effectively measured the distance to a fellow member of the Leo Spur (Tully 1987), NGC 3627, and its spectroscopically normal SN 1989B. The dispersions of the Cepheid-calibrated absolute magnitudes of these six SNe Ia (all in blue galaxies) are very small (σ(M B ) = 0.17, σ(M V ) = 0.09; BRB95).…”

Section: Cepheid Calibrationsmentioning

confidence: 99%

Type Ia Supernovae as Extragalactic Distance Indicators

Branch

Nugent

Fisher

1997

Thermonuclear Supernovae

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Abstract. Because Type Ia supernovae (SNe Ia) are not perfect standard candles, it is important to be able to use distance-independent observables (DIOs) to define subsets of SNe Ia that are "nearly standard candles" or to correct SN Ia absolute magnitudes to make them nearly homogeneous ("standardized candles"). This is not crucial for the measurement of H 0 , but it is for the measurement of q 0 and of parent-galaxy peculiar velocities. We discuss the use of various photometric and spectroscopic SN Ia DIOs, and a parent-galaxy DIO, for this purpose. We also discuss the status of the absolute-magnitude calibration of SNe Ia. We find that SNe Ia, whether calibrated by means of (1) Cepheids in their parent galaxies, (2) fitting their optical-ultraviolet spectra with detailed non-LTE model atmosphere calculations, or (3) by considering that the light curve is powered by the decay of radioactive 56 Ni, firmly indicate that the value of H 0 is low, less than or about 60 km s −1 Mpc −1 . Some issues regarding the determination of q 0 by means of SNe Ia are discussed briefly. Finally, we conjecture that even if q 0 =0.5, there probably is no cosmic age problem.

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“…The list comprises (1) 15 galaxies that were observed as part of the Key Project, (2) three galaxies whose Cepheid distances H 0 Silbermann et al 1996 ; (3) Silbermann et al 1999 ;(4) Ferrarese et al 2000b ;(5) Mould et al 2000a ;(6) Phelps et al 1998 ; (7) Madore & Freedman 1991 ;(8) Ferrarese et al 1998 ;(9) Freedman et al 1994 ;(10) Kelson et al 1999 ;(11) Sakai et al 1999 ;(12) Graham et al 1997 ;(13) Tanvir et al 1995 ;(14) Gibson et al 2000 ;(15) Rawson et al 1997 ;(16) Saha et al 1999 ;(17) Turner et al 1998 ;(18) Macri et al 1999 ;(19) Saha et al 1996 ; (20) Graham et al 1999 ; (21) Hughes et al 1998. Vol.…”

Section: Cepheid Distancesmentioning

confidence: 99%

TheHubble Space TelescopeKey Project on the Extragalactic Distance Scale. XXIV. The Calibration of Tully‐Fisher Relations and the Value of the Hubble Constant

Sakai

Mould

Hughes

et al. 2000

ApJ

202

224

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This paper presents the calibration ofTully-Fisher relations based on Cepheid distances BV RIH~0 .5 to 21 galaxies within 25 Mpc and 23 clusters within 10,000 km s~1. These relations have been applied to several distant cluster surveys in order to derive a value for the Hubble constant, mainly concentrat-H 0 , ing on an I-band all-sky survey by Giovanelli and collaborators, consisting of total I magnitudes and 50% line width data for D550 galaxies in 16 clusters. For comparison, we also derive the values of H 0 using surveys in the B and V bands by Bothun and collaborators, and in H band by Aaronson and collaborators. Careful comparisons with various other databases from the literature suggest that the H-band data, which have isophotal magnitudes extrapolated from aperture magnitudes rather than total magnitudes, are subject to systematic uncertainties. Taking a weighted average of the estimates of Hubble constants from four surveys, we obtain (random)^7 (systematic). We have also H 0 \ 71^4 investigated how the value of is a †ected by various systematic uncertainties, such as the internal H 0 extinction correction method used, Tully-Fisher slopes and shapes, a possible metallicity dependence of the Cepheid period-luminosity relation, and cluster population incompleteness bias.

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Determination of the Hubble constant from observations of Cepheid variables in the galaxy M96

Cited by 125 publications

References 41 publications

COMPTEL upper limits for the $^{\sf 56}$Coγ-ray emission from SN1998bu

COMPTEL upper limits for the $^{\sf 56}$Coγ-ray emission from SN1998bu

Type Ia Supernovae as Extragalactic Distance Indicators

TheHubble Space TelescopeKey Project on the Extragalactic Distance Scale. XXIV. The Calibration of Tully‐Fisher Relations and the Value of the Hubble Constant

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