Tip of the Red Giant Branch distances to galaxies with composite stellar populations

Salaris, Maurizio; Girardi, L.

doi:10.1111/j.1365-2966.2005.08689.x

Cited by 69 publications

(75 citation statements)

References 45 publications

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“…A similar value was also reported by Sakai et al (2000). The cause of this discrepancy is related to the age distribution of the LMC stars and a different metal mixture than in globular clusters from which the above calibration was obtained (Salaris & Girardi 2005).…”

Section: Metallicity Determinationsupporting

confidence: 82%

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The Araucaria Project: On the Tip of the Red Giant Branch Distance Determination to the Magellanic Clouds

Górski

Pietrzyński

Gieren

et al. 2016

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We present a precise optical and near-infrared determination of the tip of the red giant branch (TRGB) brightness in the Large and Small Magellanic Clouds (respectively, LMC and SMC). The commonly used calibrations of the absolute magnitude of the TRGB lead to an overestimation of the distance to the LMC and SMC in the K band, and an underestimation of the distance in the optical I band for both galaxies. Reported discrepancies are at the level of 0.2 mag, with respect to the very accurate distance determinations to both MCs based on late-type eclipsing binaries. The differential distances between the LMC and SMC obtained in the J and K bands, and for the bolometric brightness are consistent with each other, and with the results obtained from eclipsing binaries and other distance indicators.

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Section: Metallicity Determinationsupporting

confidence: 82%

“…As pointed out by Salaris & Girardi (2005), in the case of the LMC, the photometric calibration leads to a much lower metallicity than the spectroscopic measurements. For our LMC fields, the mean metallicity calculated from the (V -I) color is −1.23 ± 0.07 dex.…”

Section: Metallicity Determinationmentioning

confidence: 98%

The Araucaria Project: On the Tip of the Red Giant Branch Distance Determination to the Magellanic Clouds

Górski

Pietrzyński

Gieren

et al. 2016

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“…The reason is that in this age range M TRGB As discussed in Barker et al (2004), Salaris & Girardi (2005), Cassisi & Salaris (2013), applying this type of TRGB calibrations to galaxies with a star formation that reaches ages Górski et al (2016). To circumvent this problem it is appropriate to use an M TRGB I − (V − I) TRGB relation, whereby the TRGB colour essentially accounts for the star formation history of the observed population.…”

Section: The Trgb As Distance Indicatormentioning

confidence: 99%

The brightness of the red giant branch tip

Serenelli

Weiß

Cassisi

et al. 2017

A&A

107

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Context. The brightness of the tip of the Red Giant Branch is a useful reference quantity for several fields of astrophysics. An accurate theoretical prediction is needed for such purposes. Aims. We intend to provide a solid theoretical prediction for it, valid for a reference set of standard physical assumptions, and mostly independent of numerical details. Methods. We examine the dependence on physical assumptions and numerical details, for a wide range of metallicities and masses, and based on two different stellar evolution codes. We adjust differences between the codes to treat the physics as identical as possible. After we have succeeded in reproducing the tip brightness between the codes, we present a reference set of models based on the most up to date physical inputs, but neglecting microscopic diffusion, and convert theoretical luminosities to observed infrared colours suitable for observations of resolved populations of stars and include analytic fits to facilitate their use. Results. We find that consistent use of updated nuclear reactions, including an appropriate treatment of the electron screening effects, and careful time-stepping on the upper red giant branch are the most important aspects to bring initially discrepant theoretical values into agreement. Small, but visible differences remain unexplained for very low metallicities and mass values at and above 1.2 M ⊙ , corresponding to ages younger than 4 Gyr. The colour transformations introduce larger uncertainties than the differences between the two stellar evolution codes. Conclusions. We demonstrate that careful stellar modeling allows an accurate prediction for the luminosity of the Red Giant Branch tip. Differences to empirically determined brightnesses may result either from insufficient colour transformations or from deficits in the constitutional physics. We present the best-tested theoretical reference values to date.

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“…In a galaxy such as IC 1613 which has undergone continuous star formation the opposing effects of these population characteristics can make it difficult to interpret any change in the measured TRGB magnitude (Salaris & Girardi 2005), however in conjunction with the derived [Fe/H] abundance below, any variation in the TRGB may help us to better understand the age and metallicity distribution of the giant population in IC 1613.…”

Section: The Trgbmentioning

confidence: 99%

The AGB population in IC 1613 usingJHKphotometry

Sibbons

Ryan

Irwin

et al. 2014

A&A

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Context. A member of the Local Group, IC 1613 is a gas rich irregular dwarf galaxy that appears to have formed stars continuously over the last 10 Gyr and is relatively independent of external influences from other galaxies. Aims. This paper aims to study the spatial distribution of the asymptotic giant branch (AGB) population in IC 1613 and its metallicity. Methods. Using WFCAM on UKIRT, high quality JHK photometry of an area of 0.8 deg 2 centered on IC 1613 was obtained. The data have been used to isolate the C-and M-type components of the AGB population and using their number ratio, C/M, a global mean metallicity has been derived. The metallicity and the tip of the red giant branch magnitude (TRGB) have been studied as a function of distance from the galactic centre and as a function of azimuthal angle. Results. The TRGB has been found to be at K 0 = 18.25 ± 0.15 mag. The colour separation between the C-and M-type components of the AGB population has been located at (J − K) 0 = 1.15 ± 0.05 mag, giving a global C/M ratio of 0.52 ± 0.04 and from this an iron abundance of [Fe/H] = −1.26 ± 0.07 dex has been calculated. Conclusions. The AGB population has been detected out to a radial distance of 4.5 kpc in the de-projected plane of the galaxy. The measured TRGB is consistent with previous measurements and no significant variation is detected in the TRGB or in metallicity either with galactocentric distance or azimuthal angle.

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Tip of the Red Giant Branch distances to galaxies with composite stellar populations

Cited by 69 publications

References 45 publications

The Araucaria Project: On the Tip of the Red Giant Branch Distance Determination to the Magellanic Clouds

The Araucaria Project: On the Tip of the Red Giant Branch Distance Determination to the Magellanic Clouds

The brightness of the red giant branch tip

The AGB population in IC 1613 usingJHKphotometry

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