- 3.3.1 The Tip of the Red Giant Branch 76. - 6.2 High Versus Low Values of the Hubble Constant:. - and the expansion, geometry and history of the Universe. - Cross: position of the Sun. - Dotted line: plane of symmetry of the open clusters. - Trumpler’s discovery of the effects of interstellar dust grains in the 1930s. - Figure 1.3 Trumpler’s (1930) view of the distribution of open and globular clusters in the Milky Way. - isotropic) velocity dispersions of the Galactic Centre star cluster. - 1548–1553, Copyright 2009, with permission of the AAS.). - of the Galactic Centre reveal ≈100 S stars 8 within 1 of Sgr A. - R ˚uˇziˇcka et al., Astrophysical Journal, 691, Spatial motion of the Magellanic Clouds: tidal models ruled out?, p. - LMC–Small Magellanic Cloud (SMC) system in the context of the Local Group of galaxies (e.g. - YJK s survey of the Magellanic system (Cioni et al. - after correction of the latter depth estimates by a factor 1/. - The localization of the third acoustic peak in the WMAP 5-year data (Komatsu et al. - Riess et al., Astrophys- ical Journal, 699, A redetermination of the Hubble constant with the Hubble Space Telescope from a differential distance ladder, p. - Babusiaux C and Gilmore G 2005 The structure of the Galactic bar. - Bekki K 2008 A possible common halo of the Magellanic Clouds. - First results and description of the program. - Herschel W 1785 On the construction of the heavens. - Lindblad B 1927 On the nature of the spiral nebulae. - Infrared photometry of the SiO target stars. - Reid MJ 1993 The distance to the center of the Galaxy. - Table 2.1 Stars within 3 pc of the Sun. - (Courtesy of the European Space Agency/C. - Figure 2.5 Centre of the galaxy Messier 82. - 2010 for a recent review of the pitfalls associated with the latter. - 36–43, Copyright 2008, with permission of the IAU.). - Figure 2.10 Slope of the ML relation (de Grijs et al. - where W 0 is the width of the emission core (in km s − 1. - As a result, a fairly reliable estimate of the distance to the cluster can be obtained.. - 2006 for a simple application, resulting in the discovery of the ‘Field of Streams’. - The large symbols show SDSS observations of the GC M13. - Based on a careful review of the literature and their own data analysis, Juri´c et al. - Established by Means of the Five Regular Geometric Solids).. - A critical quality assessment of the Hipparcos Catalogue. - van Leeuwen F 2007b Validation of the new Hipparcos reduction. - 0.4 M ) because of the long equilibrium time associated with 3 He.. - 137—146, Copyright 1944, with permission of the AAS.). - Majewski, Globular Clusters, Stellar Populations and the Formation of the Milky Way, p. - As a key rung of the distance ladder, this. - The K-band magnitude of the red clump as a distance indicator, p. - 3.3.1 The Tip of the Red Giant Branch. - Figure 3.7 Example of an application of the edge detection technique (Mager et al. - (Right) Value of the edge detector response. - Mager et al., Astrophysical Journal, 689, Metallicity-corrected tip of the red giant branch distance to NGC 4258, p. - strength of the. - U et al. - Figure 3.11 Location of the classical instability strip and other variable stars in the HRD. - 151–158, Copyright 1999, with permission of the IAU.). - K-band PL slope of based on ogle microlensing observations in the direction of the Galactic bulge (see also Matsunaga et al. - On the basis of the results of Soszy´nski et al. - Pulsating variables in the lower part of the instability strip (i.e. - on or close to the turn- off of the main sequence. - and days on the basis of the ultraviolet N iii] and N iv]. - and, thus, a similar underestimate of the distance. - The shape of the alternate eclipses – i.e. - For a more detailed basic description of the method, see Paczy´nski (1997), Guinan et al. - 2010 for detailed accounts of the systematic uncertainties involved). - The values in the denominators are a priori estimates for each of the disc parameters (Herrnstein et al. - Alves DR 2000 K-band calibration of the red clump luminosity. - Catelan M 1996 The distance modulus of the Large Magellanic Cloud. - Eddington AS 1920 The internal constitution of the stars. - Ellipticity of the ring. - The K-band magnitude of the red clump as a distance indicator. - Evolution of the surface properties. - Calibration of the surface brightness–color relations. - Comparison of the Large and Small Magellanic Clouds. - Lindblad B 1925 Star-streaming and the structure of the stellar system. - Majewski SR 1999 Stellar populations and the formation of the Milky Way. - Astro- nomical Society of the Pacific.. - The tip of the red giant branch as a distance indicator. - Evolution of the Universe of Galaxies (ed. - Astronomical Society of the Pacific.. - Detection of the brightest stars in NGC 4523. - Analysis of the eclipsing binary V69 in the globular cluster 47 Tuc. - A critical quality assessment of the Hipparcos catalogue. - Zinn R and Searle L 1976 The masses of the anomalous Cepheids in the Draco system. - 2005), scale inversely with the square of the distance. - (b) Best-fitting model of the galaxy’s overall light distribution. - (c) Residual after subtraction of the model. - toward a three-dimensional picture of the Fornax cluster core, p. - The effect of the population differences required. - Ostriker, Astrophysical Journal, 474, Destruction of the Galactic globular cluster system, p. - projected velocity dispersion profile of the M87 GC system (Cˆot´e et al. - 15–39, Copyright 2004, with permission of the KAS.). - Com- bined with the definition of the effective surface brightness,. - projection of the FP provided by the D n − σ relation (Dressler et al. - assuming a distance to the centre of the Virgo cluster of 16 Mpc. - Hogg et al., Astrophysical Journal, 601, The dependence on environment of the color–. - Eddington AS 1929 The Nature of the Physical World, p. - Population effects on the bright cut-off of the PNLF. - The physical origins of the Fundamental Plane scaling relations. - Calibration of the linear sizes of extragalactic Hii regions. - On the physics of the luminosity function. - Controlling parameters of the stellar populations. - 5.1.1 Determination of the Current Expansion Rate of the Universe. - Physically, the Hubble constant corresponds to the current expansion rate of the Universe. - redshift survey’s 3D map of the distribution of galaxies. - The expansion rate of the Universe is given by. - None of the other core-collapse-type SNe (e.g