The<i>Hubble Space Telescope</i>Key Project on the Extragalactic Distance Scale. XXVI. The Calibration of Population II Secondary Distance Indicators and the Value of the Hubble Constant

Ferrarese, Laura; Mould, Jeremy; Kennicutt, Robert C.; Huchra, J. P.; Ford, H. C.; Freedman, Wendy L.; Stetson, P. B.; Madore, Barry F.; Sakai, Shoko; Gibson, Brad K.; Graham, J. A.; Hughes, Shaun M. G.; Illingworth, G. D.; Kelson, Daniel D.; Macri, Lucas M.; Sebo, Kim; Silbermann, N. A.

doi:10.1086/308309

Cited by 241 publications

(240 citation statements)

References 86 publications

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“…Here, we determine the distance from TRGB in the I band, which has proven to be an excellent distance indicator for metal-poor, old stellar populations (e.g., Lee et al 1993;Sakai et al 1996;Ferrarese et al 2000;Bellazzini et al 2001;McConnachie et al 2004;Mouhcine et al 2005). Visual inspection of our CMD shows a transition in the number counts at m F 814W ∼ 24.0, albeit with a small number of stars.…”

Section: Tip Of the Red Giant Branchmentioning

confidence: 98%

DEEPHST/ACS PHOTOMETRY OF THE M81 HALO

Durrell

Sarajedini

Chandar

2010

ApJ

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We present a deep color-magnitude diagram (CMD) for individual stars in the halo of the nearby spiral galaxy M81, at a projected distance of 19 kpc, based on data taken with the Advanced Camera for Surveys on the Hubble Space Telescope (HST). The CMD reveals a red giant branch (RGB) that is narrow and fairly blue, and a horizontal branch that has stars that lie mostly redward of the RR Lyrae instability strip. We derive a mean metallicity of [M/H] = −1.15 ± 0.11 and age of 9 ± 2 Gyr for the dominant population in our field, from the shape of the RGB, the magnitude of the red clump, and the location of the RGB bump. We compare our metallicity and age results with those found previously for stars in different locations within M81 and in the spheroids of other nearby galaxies.

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Section: Tip Of the Red Giant Branchmentioning

confidence: 98%

DEEPHST/ACS PHOTOMETRY OF THE M81 HALO

Durrell

Sarajedini

Chandar

2010

ApJ

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“…Other works point out more limitations and shortcomings of the method (e.g. Racine and Harris 1992;Tammann and Sandage 1999;Ferrarese et al 2000b). The recent review of GCLF as distance indicator by Richtler (2003) examines in particular those galaxies that yield discrepant distance measurements when the GCLF distances are compared to those of surface brightness fluctuation method, concluding that discrepant cases are most probably caused by peculiar globular cluster populations that are not uniformly old, and therefore inapplicable for the method.…”

Section: Introductionmentioning

confidence: 99%

Globular cluster luminosity function as distance indicator

Rejkuba¹

2012

Astrophys Space Sci

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Globular cluster luminosity function as distance indicatorM. Rejkuba 1 Globular clusters are among the first objects used to establish the distance scale of the Universe. In the 1970-ies it has been recognized that the differential magnitude distribution of old globular clusters is very similar in different galaxies presenting a peak at M V ∼ −7.5. This peak magnitude of the so-called Globular Cluster Luminosity Function has been then established as a secondary distance indicator. The intrinsic accuracy of the method has been estimated to be of the order of ∼ 0.2 mag, competitive with other distance determination methods. Lately the study of the Globular Cluster Systems has been used more as a tool for galaxy formation and evolution, and less so for distance determinations. Nevertheless, the collection of homogeneous and large datasets with the ACS on board HST presented new insights on the usefulness of the Globular Cluster Luminosity Function as distance indicator. I discuss here recent results based on observational and theoretical studies, which show that this distance indicator depends on complex physics of the cluster formation and dynamical evolution, and thus can have dependencies on Hubble type, environment and dynamical history of the host galaxy. While the corrections are often relatively small, they can amount to important systematic differences that make the Globular Cluster Luminosity Function a less accurate distance indicator with respect to some other standard candles.

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“…The σ parameters derived here are slightly larger than previous studies. It has long been known that the peak of the GCLF is nearly constant in different galaxies, providing a standard indicator for the cosmological distance measurement (Racine 1968;Hanes 1977;Ferrarese et al 2000). However, several studies (Crampton et al 1985;Gnedin 1997;Barmby et al 2001) presented that GCLF varies between MR and MP, inner and outer subsamples within a galaxy, and GCLF peak becomes fainter as the local density of galaxies increases (Blakeslee & Tonry 1996).…”

Section: Luminosity Functionmentioning

confidence: 99%

New 2mass Near-Infrared Photometry for Globular Clusters in M31

Wang

et al. 2014

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We present 2MASS JHK s photometry for 913 star clusters and candidates in the field of M31, which are selected from the latest Revised Bologna Catalog of M31 globular clusters (GCs) and candidates. The photometric measurements in this paper supplement this catalog, and provide a most comprehensive and homogeneous photometric catalog for M31 GCs in the JHK s bandpasses. In general, our photometry is consistent with previous measurements. The globular cluster luminosity function (GCLF) peaks for the confirmed GCs derived by fitting a t 5 distribution using maximum likelihood method are: J 0 = 15.348 +0.206 −0.208 , H 0 = 14.703 +0.176 −0.180 , and K s0 = 14.534 +0.142 −0.146 , all of which agree well with previous studies. The GCLFs are different between metalrich (MR) and metal-poor (MP), inner and outer subpopulations, as that MP clusters are fainter than their MR counterparts, and the inner clusters are brighter than the outer ones, which confirm previous results. The NIR colors of the GC candidates are on average redder than those of the confirmed GCs, which lead to an obscure bimodal distribution of the color indices. The relation of (V − K s ) 0 and metallicity shows a notable departure from linearity, with a shallower slope towards the redder end. The color-magnitude diagram (CMD) and colorcolor diagram show that many GC candidates are located out of the evolutionary tracks, suggesting that some of them may be false M31 GC candidates. The CMD also shows that the initial mass function of M31 GCs covers a large range, and the majority of the clusters have initial masses between 10 3 and 10 6 M ⊙ .

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TheHubble Space TelescopeKey Project on the Extragalactic Distance Scale. XXVI. The Calibration of Population II Secondary Distance Indicators and the Value of the Hubble Constant

Cited by 241 publications

References 86 publications

DEEPHST/ACS PHOTOMETRY OF THE M81 HALO

DEEPHST/ACS PHOTOMETRY OF THE M81 HALO

Globular cluster luminosity function as distance indicator

New 2mass Near-Infrared Photometry for Globular Clusters in M31

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