428 research outputs found
The origin of the spurious iron spread in the globular cluster NGC 3201
NGC 3201 is a globular cluster suspected to have an intrinsic spread in the
iron content. We re-analysed a sample of 21 cluster stars observed with
UVES-FLAMES at the Very Large Telescope and for which Simmerer et al. found a
0.4 dex wide [Fe/H] distribution with a metal-poor tail. We confirmed that when
spectroscopic gravities are adopted, the derived [Fe/H] distribution spans ~0.4
dex. On the other hand, when photometric gravities are used, the metallicity
distribution from Fe I lines remains large, while that derived from Fe II lines
is narrow and compatible with no iron spread. We demonstrate that the
metal-poor component claimed by Simmerer et al. is composed by asymptotic giant
branch stars that could be affected by non local thermodynamical equilibrium
effects driven by iron overionization. This leads to a decrease of the Fe I
abundance, while leaving the Fe II abundance unaltered. A similar finding has
been already found in asymptotic giant branch stars of the globular clusters M5
and 47 Tucanae. We conclude that NGC 3201 is a normal cluster, with no evidence
of intrinsic iron spread.Comment: Accepted for publication by ApJ, 7 pages, 4 figure
Chemical abundances in the nucleus of the Sagittarius dwarf spheroidal galaxy
We present Iron, Magnesium, Calcium, and Titanium abundances for 235 stars in
the central region of the Sagittarius dwarf spheroidal galaxy (within 9.0
arcmin ~70 pc from the center) from medium-resolution Keck/DEIMOS spectra. All
the considered stars belong to the massive globular cluster M54 or to the
central nucleus of the galaxy (Sgr,N). In particular we provide abundances for
109 stars with [Fe/H] > -1.0, more than doubling the available sample of
spectroscopic metallicity and alpha-elements abundance estimates for Sgr dSph
stars in this metallicity regime. Also, we find the first confirmed member of
the Sagittarius dwarf spheroidal with [Fe/H]< -2.0 based on analysis of iron
lines. We find for the first time a metallicity gradient in the Sgr,N
population, whose peak iron abundance goes from [Fe/H]=-0.38 for R < 2.5 arcmin
to [Fe/H]=-0.57 for 5.0 < R < 9.0 arcmin. On the other hand the trends of
[Mg/Fe], [Ca/Fe], and [Ti/Fe] with [Fe/H] are the same over the entire region
explored by our study. We reproduce the observed chemical patterns of the
Sagittarius dwarf spheroidal as a whole with a chemical evolution model
implying a high mass progenitor ( M_(DM)=6 X 10^{10} Msun ) and a significant
event of mass-stripping occurred a few Gyr ago, presumably starting at the
first peri-Galactic passage after infall.Comment: Accepted for publication to A&A, 12 pages, 14 figures, 1 tabl
Exploiting the Gaia EDR3 photometry to derive stellar temperatures
We present new colour -- effective temperature (Teff) transformations based
on the photometry of the early third data release (EDR3) of the Gaia/ESA
mission. These relations are calibrated on a sample of about 600 dwarf and
giant stars for which Teff have been previously determined with the InfraRed
Flux Method from dereddened colours. The 1 dispersion of the
transformations is of 60-80 K for the pure Gaia colours BP-RP, BP-G , G-RP,
improving to 40-60 K for colours including the 2MASS K-band, namely BP-K, RP-K
and G-K, We validate these relations in the most challenging case of dense
stellar fields, where the Gaia EDR3 photometry could be less reliable,
providing guidance for a safe use of Gaia colours in crowded environments . We
compare the Teff from the Gaia EDR3 colours with those obtained from standard
V-K colours for stars in three Galactic globular clusters of different
metallicity, namely NGC 104, NGC 6752 and NGC 7099. The agreement between the
two estimates of Teff is excellent, with mean differences between -50 and +50
K, depending on the colour, and with 1 dispersions around the mean Teff
differences of 25-50 K for most of the colours and below 10 K for BP-K and G-K
. This demonstrates that these colours are analogue to V-K , as Teff
indicators.Comment: 12 pages. Accepted for publication on A&
Probing the MSP prenatal stage: the optical identification of the X-ray burster EXO 1745-248 in Terzan 5
We report on the optical identification of the neutron star burster EXO
1745-248 in Terzan 5. The identification was performed by exploiting HST/ACS
images acquired in Director's Discretionary Time shortly after (approximately 1
month) the Swift detection of the X-ray burst. The comparison between these
images and previous archival data revealed the presence of a star that
currently brightened by ~3 magnitudes, consistent with expectations during an
X-ray outburst. The centroid of this object well agrees with the position, in
the archival images, of a star located in the Turn-Off/Sub Giant Branch region
of Terzan 5. This supports the scenario that the companion should has recently
filled its Roche Lobe. Such a system represents the pre-natal stage of a
millisecond pulsar, an evolutionary phase during which heavy mass accretion on
the compact object occurs, thus producing X-ray outbursts and re-accelerating
the neutron star.Comment: ApJ Letter, in pres
Evolution and Nucleosynthesis of AGB stars in Three Magellanic Cloud Clusters
We present stellar evolutionary sequences for asymptotic giant branch (AGB)
stars in the Magellanic Cloud clusters NGC 1978, NGC 1846 and NGC 419. The new
stellar models for the three clusters match the observed effective temperatures
on the giant branches, the oxygen-rich to carbon-rich transition luminosities,
and the AGB-tip luminosities. A major finding is that a large amount of
convective overshoot (up to 3 pressure scale heights) is required at the base
of the convective envelope during third dredge-up in order to get the correct
oxygen-rich to carbon-rich transition luminosity. The stellar evolution
sequences are used as input for detailed nucleosynthesis calculations. For NGC
1978 and NGC 1846 we compare our model results to the observationally derived
abundances of carbon and oxygen. We find that additional mixing processes
(extra-mixing) are required to explain the observed abundance patterns. For NGC
1846 we conclude that non-convective extra-mixing processes are required on
both the RGB and the AGB, in agreement with previous studies. For NGC 1978 it
is possible to explain the C/O and 12C/13C abundances of both the O-rich and
the C-rich AGB stars by assuming that the material in the intershell region
contains high abundances of both C and O. This may occur during a thermal pulse
when convective overshoot at the inner edge of the flash-driven convective
pocket dredges C and O from the core to the intershell. For NGC 419 we provide
our predicted model abundance values although there are currently no published
observed abundance studies for the AGB stars in this cluster.Comment: 16 figures, 3 tables, Accepted for publication in Ap
The Terzan 5 puzzle: discovery of a third, metal-poor component
We report on the discovery of 3 metal-poor giant stars in Terzan 5, a complex
stellar system in the the Galactic bulge, known to have two populations at
[Fe/H]=-0.25 and +0.3. For these 3 stars we present new echelle spectra
obtained with NIRSPEC at Keck II, which confirm their radial velocity
membership and provide average [Fe/H]=-0.79 dex iron abundance and
[alpha/Fe]=+0.36 dex enhancement. This new population extends the metallicity
range of Terzan~5 0.5 dex more metal poor, and it has properties consistent
with having formed from a gas polluted by core collapse supernovae.Comment: Accepted for publication on ApJ Lette
Confronto fra stime di pericolosità sismica in Italia
Allo scopo di valutare l’attendibilità delle stime di pericolosità sismica recentemente proposte per l’Italia sulla base
di un approccio standard basato sull’impiego di informazioni geologiche (zone sismogenetiche) e sismologiche
(catalogo sismico epicentrale), viene proposto un confronto con stime di pericolosità effettuate a partire dall’analisi
statistica delle storie sismiche di sito relative alle 1401 località per le quali esistono informazioni circa glie effetti
macrosismici osservati in occasione di almeno dieci terremoti del passato. In particolare, sono stati messi a
confronto i valori dell’accelerazione massima orizzontale del moto del suolo corrispondente ad una probabilità di
eccedenza del 10% in 50 anni dedotti con l’approccio standard, con i valori dell’intensità macrosismica
corrispondente alle stesse probabilità di eccedenza per un tempo di ritorno di 50 anni. Il confronto, effettuato con
una procedura non parametrica che non richiede l’impiego relazioni di conversione empiriche, indica che le
differenze osservate sono fortemente correlate con la geometria delle zone sismotettoniche utilizzate nell’approccio
standard. In particolare, la zonazione sembra incompleta (sembrano esistere zone “nascoste”) e a tratti troppo
grossolana (a causa della scarsità dei dati disponibili) per rappresentare adeguatamente i processi sismogenici attivi
nell’area italiana
A chemical trompe-l'\oe{}il: no iron spread in the globular cluster M22
We present the analysis of high-resolution spectra obtained with UVES and
UVES-FLAMES at the Very Large Telescope of 17 giants in the globular cluster
M22, a stellar system suspected to have an intrinsic spread in the iron
abundance. We find that when surface gravities are derived spectroscopically
(by imposing to obtain the same iron abundance from FeI and FeII lines) the
[Fe/H] distribution spans ~0.5 dex, according to previous analyses. However,
the gravities obtained in this way correspond to unrealistic low stellar masses
(0.1-0.5 Msun) for most of the surveyed giants. Instead, when photometric
gravities are adopted, the [FeII/H] distribution shows no evidence of spread at
variance with the [FeI/H] distribution. This difference has been recently
observed in other clusters and could be due to non-local thermodynamical
equilibrium effects driven by over-ionization mechanisms, that mainly affect
the neutral species (thus providing lower [FeI/H]) but leave [FeII/H]
unaltered. We confirm that the s-process elements show significant star-to-star
variations and their abundances appear to be correlated with the difference
between [FeI/H] and [FeII/H]. This puzzling finding suggests that the peculiar
chemical composition of some cluster stars may be related to effects able to
spuriously decrease [FeI/H]. We conclude that M22 is a globular cluster with no
evidence of intrinsic iron spread, ruling out that it has retained the
supernovae ejecta in its gravitational potential well.Comment: Accepted for publication to ApJ; 33 pages, 10 figures, 6 table
First evidence of fully spatially mixed first and second generations in globular clusters: the case of NGC 6362
We present the first evidence of multiple populations in the Galactic
globular cluster NGC 6362. We used optical and near-UV Hubble Space Telescope
and ground based photometry, finding that both the sub giant and red giant
branches are split in two parallel sequences in all color magnitude diagrams
where the F336W filter (or U band) is used. This cluster is one of the least
massive globulars (M_tot~5x10^4 M_sun) where multiple populations have been
detected so far. Even more interestingly and at odds with any previous finding,
we observe that the two identified populations share the same radial
distribution all over the cluster extension. NGC 6362 is the first system where
stars from different populations are found to be completely spatially mixed.
Based on N-body and hydrodynamical simulations of multiple stellar generations,
we argue that, to reproduce these findings, NGC 6362 should have lost up to the
80% of its original massComment: Accepted for publication by ApJ Letters; 6 pages, 5 figure
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