1,226 research outputs found
Comparison between Observed and Theoretical Red Giant Branch Luminosity Functions of Galactic Globular Clusters
V-band luminosity functions have been obtained for the upper main-sequence,
sub-giant branch and red giant branch of 18 galactic globular clusters from HST
data. A comparison with four sets of theoretical models has been performed. In
contrast with what was found in several previous works, a Good general
agreement has been found between the observed and theoretical LF at any
metallicity [M/H]<-0.7. Possible discrepancies at higher metallicity, in the
upper part of the RGB, need to be confirmed with further observational data and
by extending all the models to the most metal rich regime. The SGB shape has
been used to set an upper limit to the cluster age, and consequently a lower
limit on the cluster distance. A discussion on the still open problem of the
mismatch between the observed and theoretical RGB bump location is also
presented.Comment: Accepted for publication in A&
Evidence of the inhomogeneity of the stellar population in the differentially reddened globular cluster NGC 3201
We report on evidence of the inhomogeneity (multiplicity) of the stellar
population in the Galactic globular cluster (GC) NGC 3201, which is irregularly
reddened across its face. We carried out a more detailed and careful analysis
of our recently published new multi-color photometry in a wide field of the
cluster with particular emphasis on the U band. Using the photometric data
corrected for differential reddening, we found for the first time two key signs
of the inhomogeneity in the cluster's stellar population and of its radial
variation in the GC. These are (1) an obvious trend in the color-position
diagram, based on the (U-B) color-index, of red giant branch (RGB) stars, which
shows that the farther from the cluster's center, the bluer on average the
(U-B) color of the stars is; and (2) the dependence of the radial distribution
of sub-giant branch (SGB) stars in the cluster on their U magnitude, where
brighter stars are less centrally concentrated than their fainter counterparts
at a confidence level varying between 99.2% and 99.9% depending on the
color-index used to select the stars. The same effects were recently found by
us in the GC NGC 1261. However, contrary to NGC 1261, we are not able to
unambiguously suggest which of the sub-populations of SGB/RGB stars can be the
progenitor of blue and red horizontal branch stars of the cluster. Apart from
M4, NGC 3201 is another GC very probably with an inhomogeneous stellar
population, which has essentially lower mass than the most massive Galactic GCs
where multiple stellar populations were unambiguously detected for the first
timeComment: 5 pages, 4 figure
The Luminosity and Mass Function of the Globular Cluster NGC1261
I-band CCD images of two large regions of the Galactic globular cluster NGC
1261 have been used to construct stellar luminosity functions (LF) for 14000
stars in three annuli from 1.4' from the cluster center to the tidal radius.
The LFs extend to M_I~8 and tend to steepen from the inner to the outer
annulus, in agreement with the predictions of the multimass King-Michie model
that we have calculated for this cluster. The LFs have been transformed into
mass functions. Once corrected for mass segregation the global mass function of
NGC 1261 has a slope x_0=0.8+/-0.5Comment: 9 pages, A&A macros, accepted for publication in A&
Galactic Globular Clusters as a test for Very Low-Mass stellar models
We make use of the Next Generation model atmospheres by Allard et al. (1997)
and Hauschildt, Allard & Baron (1999) to compute theoretical models for low and
very low-mass stars for selected metallicities in the range Z= 0.0002 to 0.002.
On this basis, we present theoretical predictions covering the sequence of
H-burning stars as observed in galactic globulars from the faint end of the
Main Sequence up to, and beyond, the cluster Turn Off. The role played by the
new model atmospheres is discussed, showing that present models appear in
excellent agreement with models by Baraffe et al. (1997) as computed on quite
similar physical basis. One finds that the theoretical mass-luminosity
relations based on this updated set of models, are in good agreement with the
empirical data provided by Henry & McCarthy (1993). Comparison with HST
observation discloses that the location in the Color-Magnitude diagram of the
lower Main Sequence in galactic globular clusters appears again in good
agreement with the predicted sensitive dependence of these sequences on the
cluster metallicity.Comment: accepted for pubblication on MNRA
Mass accretion rates from multi-band photometry in the Carina Nebula: the case of Trumpler 14
We present a study of the mass accretion rates of pre-Main Sequence (PMS)
stars in the cluster Trumpler 14 (Tr14) in the Carina Nebula. Using optical
multi-band photometry we were able to identify 356 PMS stars showing H-alpha
excess emission with equivalent width EW(H-alpha)>20\AA. We interpret this
observational feature as indication that these objects are still actively
accreting gas from their circumstellar medium. From a comparison of the HR
diagram with PMS evolutionary models we derive ages and masses of the PMS
stars. We find that most of the PMS objects are younger than 10 Myr with a
median age of ~3 Myr. Surprisingly, we also find that ~20% of the mass
accreting objects are older than 10 Myr. For each PMS star in Trumpler 14 we
determine the mass accretion rate () and discuss its dependence
on mass and age. We finally combine the optical photometry with near-IR
observations to build the spectral energy distribution (SED) for each PMS star
in Tr14. The analysis of the SEDs suggests the presence of transitional discs
in which a large amount of gas is still present and sustains accretion onto the
PMS object at ages older than 10 Myr. Our results, discussed in light of recent
recent discoveries with Herschel of transitional discs containing a massive gas
component around the relatively old PSM stars TW Hydrae, 49 Ceti, and HD 95086,
support a new scenario in which old and evolved debris discs still host a
significant amount of gas.Comment: 12 pages, 13 figures, accepted for publication on A&
Mass accretion rates from multiband photometry in the Carina Nebula: The case of Trumpler 14
open8siWe present a study of the mass accretion rates of pre-main sequence (PMS) stars in the cluster Trumpler 14 (Tr 14) in the Carina Nebula. Using optical multiband photometry we were able to identify 356 PMS stars showing Hα excess emission with equivalent width EW(Hα) > 20 Å. We interpret this observational feature as an indication that these objects are still actively accreting gas from their circumstellar medium. From a comparison of the HR diagram with PMS evolutionary models we derive ages and masses of the PMS stars. We find that most of the PMS objects are younger than 10 Myr with a median age of ~3 Myr. Surprisingly, we also find that ~20% of the mass accreting objects are older than 10 Myr. For each PMS star in Trumpler 14 we determine the mass accretion rate (Ṁacc) and discuss its dependence on mass and age. We finally combine the optical photometry with near-IR observations to build the spectral energy distribution (SED) for each PMS star in Tr 14. The analysis of the SEDs suggests the presence of transitional discs in which a large amount of gas is still present and sustains accretion onto the PMS object at ages older than 10 Myr. Our results, discussed in light of recent recent discoveries with Herschel of transitional discs containing a massive gas component around the relatively old PMS stars TW Hydrae, 49 Ceti, and HD 95086, support a new scenario n which old and evolved debris discs still host a significant amount of gas.openBeccari, G.; De Marchi, G.; Panagia, N.; Valenti, E.; Carraro, G.; Romaniello, M.; Zoccali, M.; Weidner, C.Beccari, G.; De Marchi, G.; Panagia, N.; Valenti, E.; Carraro, Giovanni; Romaniello, M.; Zoccali, M.; Weidner, C
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