A new Determination of the Hubble Parameter using Galaxy Linear Diameters

Goodwin, S. P.; Gribbin, John; Hendry, M.

doi:10.1086/118641

Cited by 7 publications

(5 citation statements)

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“…We took as our 'best-fit' estimate of H 0 the value which gave the minimum KS distance -obtaining H 0 = 42 kms −1 Mpc −1 . This value agrees with Sandage (1993a,b), who used M31 and M101 as standard rulers, and is consistent with the analysis of Goodwin, Gribbin & Hendry (1997), who obtained H 0 = 52±6±8 kms −1 Mpc −1 using galaxy linear diameters and a similar calibrating sample. However, their second uncertainty was an estimate of the difference in the mean intrinsic diameter of the local calibrating galaxies compared with the distant sample (even after correction for Malmquist bias) -a difference which might be systematically negative given the strategy of the HST Key Project to observe 'Grand Design' spirals (Kennicutt et al 1995).…”

Section: Methods and Application Using Galaxy Diameterssupporting

confidence: 91%

“…Sandage 1994; Sandage, Tammann & Federspiel 1995) to more detailed parametric statistical models of the distance indicator and selection function (cf. Hendry & Simmons 1994; Triay, Lachièze‐Rey & Rauzy 1994; Goodwin, Gribbin & Hendry 1997, hereafter GGH97; Giovanelli et al 1997; Theureau et al 1997). All of these methods involve either implicitly or explicitly a number of parametric model assumptions concerning the distribution function of the distance indicator and the observational selection, and the spatial distribution of the observed galaxies.…”

Section: Introductionmentioning

confidence: 99%

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A robust method for measuring the Hubble parameter

Hendry

Rauzy

Goodwin

et al. 2001

Monthly Notices of the Royal Astronomical Society

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We obtain a robust, non-parametric, estimate of the Hubble constant from galaxy linear diameters calibrated using HST Cepheid distances. Our method is independent of the parametric form of the diameter function and the spatial distribution of galaxies and is insensitive to Malmquist bias. We include information on the galaxy rotation velocities; unlike Tully-Fisher, however, we retain a fully non-parametric treatment. We find $H_0=66\pm6$ km/s/Mpc, somewhat larger than previous results using galaxy diameters.Comment: 4 pages, 1 figure, Cosmic Flows Workshop, Victoria B.C. Canada, July 1999, ed. S. Courteau, M. Strauss & J. Willick, ASP conf. serie

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Section: Methods and Application Using Galaxy Diameterssupporting

confidence: 91%

Section: Introductionmentioning

confidence: 99%

A robust method for measuring the Hubble parameter

Hendry

Rauzy

Goodwin

et al. 2001

Monthly Notices of the Royal Astronomical Society

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“…There are large-scale CO(1−0) surveys in the outer disk of the MW (e.g., Wouterloot & Brand 1989;Brand & Wouterloot 1994;Digel et al 1994;Snell et al 2002;Yang et al 2002;Brunt et al 2003;Nakagawa et al 2005;Sun et al 2015). The optical edge of the MW disk is around R 25 ∼ 13.4 kpc (Goodwin et al 1997(Goodwin et al , 1998 with considerable uncertainty due to its edge-on projection. The galactocentric radius of 1.24R 25 , corresponding to the 1 kpc 2 region in M83, is r gal ∼ 16.7 kpc for the MW.…”

Section: Comparisons To Previous Studiesmentioning

confidence: 99%

First Detection of the Molecular Cloud Population in the Extended Ultraviolet Disk of M83

Koda

Watson

Combes

et al. 2022

ApJ

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We report a CO(J = 3−2) detection of 23 molecular clouds in the extended ultraviolet (XUV) disk of the spiral galaxy M83 with the Atacama Large Millimeter/submillimeter Array. The observed 1 kpc2 region is at about 1.24 times the optical radius (R 25) of the disk, where CO(J = 2–1) was previously not detected. The detection and nondetection, as well as the level of star formation (SF) activity in the region, can be explained consistently if the clouds have the mass distribution common among Galactic clouds, such as Orion A—with star-forming dense clumps embedded in thick layers of bulk molecular gas, but in a low-metallicity regime where their outer layers are CO-deficient and CO-dark. The cloud and clump masses, estimated from CO(3−2), range from 8.2 × 102 to 2.3 × 104 M ⊙ and from 2.7 × 102 to 7.5 × 103 M ⊙, respectively. The most massive clouds appear similar to Orion A in star formation activity as well as in mass, as expected if the cloud mass structure is common. The overall low SF activity in the XUV disk could be due to the relative shortage of gas in the molecular phase. The clouds are distributed like chains up to 600 pc (or longer) in length, suggesting that the trigger of cloud formation is on large scales. The common cloud mass structure also justifies the use of high-J CO transitions to trace the total gas mass of clouds, or galaxies, even in the high-z universe. This study is the first demonstration that CO(3−2) is an efficient tracer of molecular clouds even in low-metallicity environments.

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“…Spaenhauer 1978;Tammann et al 1979;Teerikorpi 1984Teerikorpi , 1997Bottinelli et al 1986, Sandage 1996, 1999b, 2002Theureau et al 1997;Goodwin et al 1997;Paturel et al 1998;Ekholm et al 1999;Butkevich et al 2005, for a tutorial see Sandage et al 1995). Spaenhauer 1978;Tammann et al 1979;Teerikorpi 1984Teerikorpi , 1997Bottinelli et al 1986, Sandage 1996, 1999b, 2002Theureau et al 1997;Goodwin et al 1997;Paturel et al 1998;Ekholm et al 1999;Butkevich et al 2005, for a tutorial see Sandage et al 1995).…”

Section: The First Galaxy Distancesunclassified

The Ups and Downs of the Hubble Constant

Tammann

2006

Reviews in Modern Astronomy

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A brief history of the determination of the Hubble constant H_0 is given. Early attempts following Lemaitre (1927) gave much too high values due to errors of the magnitude scale, Malmquist bias and calibration problems. By 1962 most authors agreed that 75< H_0 <130. After 1975 a dichotomy arose with values near 100 and others around 55. The former came from apparent-magnitude-limited samples and were affected by Malmquist bias. New distance indicators were introduced; they were sometimes claimed to yield high values of H_0, but the most recent data lead to H_0 in the 60's, yet with remaining difficulties as to the zero-point of the respective distance indicators. SNe Ia with their large range and very small luminosity dispersion (avoiding Malmquist bias) offer a unique opportunity to determine the large-scale value of H_0. Their maximum luminosity can be well calibrated from 10 SNe Ia in local parent galaxies whose Cepheids have been observed with HST. An unforeseen difficulty - affecting all Cepheid distances - is that their P-L relation varies from galaxy to galaxy, presumably in function of metallicity. A proposed solution is summarized here. The conclusion is that H_0 = 63.2 +/- 1.3 (random) +/- 5.3 (systematic) on all scales. The expansion age becomes then (with Omega_m=0.3, Omega_Lambda=0.7) 15.1 Gyr.Comment: 30 pages, 12 figures, 2 tables. 79th Annual Scientific Meeting of the Astronomische Gesellschaft 2005, Karl-Schwarzschild-Lecture, to appear in Reviews in Modern Astronomy, 19,

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A new Determination of the Hubble Parameter using Galaxy Linear Diameters

Cited by 7 publications

References 0 publications

A robust method for measuring the Hubble parameter

A robust method for measuring the Hubble parameter

First Detection of the Molecular Cloud Population in the Extended Ultraviolet Disk of M83

The Ups and Downs of the Hubble Constant

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