110 citations · 437 across the 17 of their papers we have counts for
13 papers · 1 filter
A JWST project on 47 Tucanae. Binaries among multiple populations
A. P. Milone, A. F. Marino, M. Bernizzoni +25
Almost all globular clusters (GCs) contain multiple populations consisting of stars with varying helium and light-element abundances. These populations include first-population sta…
Mass loss along the red giant branch of the intermediate stellar populations in NGC6752 and NGC2808
M. Tailo, A. P. Milone, A. F. Marino +15
The morphology of the Horizontal Branch (HB) in Globular Clusters (GC) is among the early evidences that they contain multiple populations of stars. Indeed, the location of each st…
Planetary Nebulae of the Large Magellanic Cloud II: the connection with the progenitors' properties
P. Ventura, S. Tosi, D. A. García-Hernández +6
The study of planetary nebulae (PNe) offers the opportunity of evaluating the efficiency of the dust production mechanism during the very late asymptotic giant branch (AGB) phases.…
Hubble Space Telescope survey of Magellanic Cloud star clusters. Binaries among the split main sequences of NGC 1818, NGC 1850, and NGC 2164
F. Muratore, A. P. Milone, F. D'Antona +15
Nearly all star clusters younger than ~600 Myr exhibit extended main sequence turn offs and split main sequences (MSs) in their color-magnitude diagrams. Works based on both photom…
GN-z11: witnessing the formation of second generation stars and an accreting massive black hole in a massive star cluster
F. D'Antona, E. Vesperini, F. Calura +7
We explore the possibility that the N-rich young proto-galaxy GN-z11 recently observed at z=10.6 by the James Webb Space Telescope is the result of the formation of second generati…
Dust from evolved stars: a pilot analysis of the AGB to PN transition
F. Dell'Agli, S. Tosi, D. Kamath +5
We present a novel approach to address dust production by low- and intermediate-mass stars. We study the asymptotic giant branch (AGB) phase, during which the formation of dust tak…
Characterization of M-stars in the LMC in the JWST era
E. Marini, F. Dell'Agli, M. Di Criscienzo +8
We study the M-type asymptotic giant branch (AGB) population of the Large Magellanic Cloud (LMC) by characterizing the individual sources in terms of the main properties of the pro…
Evolved stars in the Local Group galaxies - III. AGB and RSG stars in Sextans A
F. Dell'Agli, M. Di Criscienzo, D. A. García-Hernández +4
We study the evolved stellar population of the galaxy Sextans A. This galaxy is one of the lowest metallicity dwarfs in which variable asymptotic giant branch stars have been detec…
Evolved stars in the Local Group galaxies - II. AGB, RSG stars and dust production in IC10
F. Dell'Agli, M. Di Criscienzo, P. Ventura +4
We study the evolved stellar population of the Local Group galaxy IC10, with the aim of characterizing the individual sources observed and to derive global information on the galax…
Studying the evolution of AGB stars in the Gaia epoch
M. Di Criscienzo, P. Ventura, D. A. Garcia-Hernandez +6
We present asymptotic giant branch (AGB) models of solar metallicity, to allow the interpretation of observations of Galactic AGB stars, whose distances should be soon available af…
Planetary Nebulae in the Small Magellanic Cloud
P. Ventura, L. Stanghellini, M. Di Criscienzo +2
We analyse the planetary nebulae (PNe) population of the Small Magellanic Cloud (SMC), based on evolutionary models of stars with metallicities in the range $10^{-3} \leq Z \leq 4\…
AGB stars in the SMC: evolution and dust properties based on Spitzer observations
F. Dell'Agli, D. A. García-Hernández, P. Ventura +3
We study the population of asymptotic giant branch (AGB) stars in the Small Magellanic Cloud (SMC) by means of full evolutionary models of stars of mass 1Msun < M < 8Msun, evolved…
Dust from AGBs: relevant factors and modelling uncertainties
P. Ventura, F. Dell'Agli, R. Schneider +5
The dust formation process in the winds of Asymptotic Giant Branch stars is discussed, based on full evolutionary models of stars with mass in the range MM$\leq 8…