The<i>Hubble Space Telescope</i>Extragalactic Distance Scale Key Project. X. The Cepheid Distance to NGC 7331

Hughes, Shaun M. G.; Han, Mingsheng; Hoessel, John G.; Freedman, Wendy L.; Kennicutt, Robert C.; Mould, Jeremy; Saha, Abhijit; Stetson, P. B.; Madore, Barry F.; Silbermann, N. A.; Harding, Paul; Ferrarese, Laura; Ford, H. C.; Gibson, Brad K.; Graham, J. A.; Hill, Robert S.; Huchra, J. P.; Illingworth, G. D.; Phelps, Randy L.; Sakai, Shoko

doi:10.1086/305808

Cited by 52 publications

(13 citation statements)

References 59 publications

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“…REFERENCES.È(1) Freedman & Madore 1990 ; (2) Ferrarese et al 1998 ;(11) Freedman et al 1994 ;(12) Kelson et al 1999 ;(13) Sakai et al 1999 ; (14) Graham et al 1997 ;(15) Tanvir et al 1995 ;(16) Rawson et al 1997 ;(17) Gibson et al 1999 ;(18) Newman et al 2001 ;(19) Ferrarese et al 1996 ;(20) Turner et al 1998 ;(21) Macri et al 1999 ;(22) Graham et al 1999 ;(23) Kelson et al 1996 ; (24) Hughes et al 1998 ;(25) Freedman 1988. (V [I) slope, the new relation predicts systematically larger reddenings for Cepheids of increasing period. As a result, the di †erences in distance between the previous and the new calibration will be largest for galaxies at greater distances, where the mean period of the samples is larger (since a greater fraction of shorter period Cepheids will fall below the detection threshold in the most distant targets).…”

Section: New Revised Cepheid Distancesmentioning

confidence: 99%

Final Results from theHubble Space TelescopeKey Project to Measure the Hubble Constant

Freedman

Madore

Gibson

et al. 2001

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We present here the Ðnal results of the Hubble Space T elescope (HST ) Key Project to measure the Hubble constant. We summarize our method, the results, and the uncertainties, tabulate our revised distances, and give the implications of these results for cosmology. Our results are based on a Cepheid calibration of several secondary distance methods applied over the range of about 60È400 Mpc. The analysis presented here beneÐts from a number of recent improvements and reÐnements, including (1) a larger LMC Cepheid sample to deÐne the Ðducial period-luminosity (PL) relations, (2) a more recent HST Wide Field and Planetary Camera 2 (WFPC2) photometric calibration, (3) a correction for Cepheid metallicity, and (4) a correction for incompleteness bias in the observed Cepheid PL samples. We adopt a distance modulus to the LMC (relative to which the more distant galaxies are measured) of mag, or 50 kpc. New, revised distances are given for the 18 spiral galaxies for k 0 (LMC) \ 18.50^0.10 which Cepheids have been discovered as part of the Key Project, as well as for 13 additional galaxies with published Cepheid data. The new calibration results in a Cepheid distance to NGC 4258 in better agreement with the maser distance to this galaxy. Based on these revised Cepheid distances, we Ðnd values (in km s~1 Mpc~1) of (random)^6 (systematic) (Type Ia supernovae),

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Section: New Revised Cepheid Distancesmentioning

confidence: 99%

Final Results from theHubble Space TelescopeKey Project to Measure the Hubble Constant

Freedman

Madore

Gibson

et al. 2001

ApJ

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3,073

236

2,743

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“…NGC 7331 had many WFPC2 images available in the HST archive, largely because this galaxy was a target for the HST Cepheid Key Project (Hughes et al 1998). We made combined images from multiple observations of two different pointings located 3.5 0 and 5 0 from the galaxy (see Table 6).…”

Section: Estimating the Contamination From Background Galaxies With Hmentioning

confidence: 99%

Global Properties of the Globular Cluster Systems of Four Spiral Galaxies

et al. 2007

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We present results from a wide-field imaging study of the globular cluster (GC) systems of a sample of edge-on, SbSc spiral galaxies $7-20 Mpc away. This study is part of a larger survey of the ensemble properties of the GC populations of giant galaxies. We imaged the galaxies in BVR filters with large-format CCD detectors on the WIYN 3.5 m telescope to projected radii of $20-40 kpc. For four galaxies (NGC 2683, NGC 3556, NGC 4157, and NGC 7331), we quantify the radial distributions of the GC systems and estimate the total number, luminosity-and mass-normalized specific frequencies (S N and T ), and blue (metal-poor) fraction of GCs. A fifth galaxy (NGC 3044) was apparently too distant for us to have detected its GC system. Our S N for NGC 2683 is 2.5 times smaller than the previously published value, likely due in part to reduced contamination from non-GCs. For the spiral galaxies analyzed for the survey to date, the average number of GCs is 170 AE 40, and the weighted mean values of S N and T are 0:8 AE 0:2 and 1:4 AE 0:3, respectively. We use the survey data to derive a relationship between the radial extent of the GC system and host galaxy mass over a factor of 20 in mass. Finally, we confirm the trend, identified in previous survey papers, of increasing specific frequency of metal-poor GCs with increasing galaxy mass. We compare the data with predictions from a simple model and show that carefully quantifying the numbers of metal-poor GCs in galaxies can constrain the formation redshifts of the GCs and their host galaxies.

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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

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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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TheHubble Space TelescopeExtragalactic Distance Scale Key Project. X. The Cepheid Distance to NGC 7331

Cited by 52 publications

References 59 publications

Final Results from theHubble Space TelescopeKey Project to Measure the Hubble Constant

Final Results from theHubble Space TelescopeKey Project to Measure the Hubble Constant

Global Properties of the Globular Cluster Systems of Four Spiral Galaxies

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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