54 research outputs found
Interferometry as a tool to calibrate evolutionary tracks
Up to now, the only way to determine the masses of single stars at different ages was to use the evolutionary tracks. Depending on the authors the evolutionary tracks for stars of the same masses are different. It is therefore important to test which models better predict the observations. In this PhD-thesis I present methods to determine physical parameters of young and evolved stars, combining spectroscopy with optical interferometry. The first part of the thesis discuss PMS stars, while the second part giant stars. Combining optical interferometry with spectroscopy it is possible to measure the dynamical masses of stars in binary systems. In the case of PMS stars I performed a spectroscopic survey to search for young binaries. The result was the collection of a sample of 13 young spectroscopic binary (SB). For these, I determined the orbital parameters and in two cases the mass ratios. For HD113449 I obtained interferometric observations with AMBER@VLTI. Combing these data with the spectroscopy, I determined the masses of the components of HD113449. Comparing these mass values and the mass ratios of the two SBs with different set of evolutionary tracks, I found that the Baraffe et al. (1998) tracks fit the observations best. In the case of the test of evolutionary tracks of giant stars, I measured the diameters of 30 giant stars using AMBER@VLTI and the CHARA array. A test was done comparing the diameters estimated from different set of evolutionary tracks with the interferometrically measured ones. This test showed that the Salasnich et al. (2000) models are the ones best fitting the observations. In the case of HD170693, I also obtained time series observations with the high resolution spectrograph at the TLS Tautenburg, deriving the oscillation frequencies from the measured radial velocities. Combining these informations with the interferometric diameter, I obtained the mass of this giant, which is in good agreement with the one from the models
RR Lyrae stars in the Andromeda satellite galaxies
In this contribution we summarize results on the search for variable stars and the study of the resolved stellar populations in four dwarf spheroidal satellites of the Andromeda galaxy that we have observed with the Large Binocular Cameras (LBC) at the Large Binocular Telescope (LBT)
Variable stars in the ultra-faint dwarf spheroidal galaxy Ursa Major I
We have performed the first study of the variable star population of Ursa
Major I (UMa I), an ultra-faint dwarf satellite recently discovered around the
Milky Way by the Sloan Digital Sky Survey. Combining time series observations
in the B and V bands from four different telescopes, we have identified seven
RR Lyrae stars in UMa I, of which five are fundamental-mode (RRab) and two are
first-overtone pulsators (RRc). Our V, B-V color-magnitude diagram of UMa I
reaches V~23 mag (at a signal-to-noise ratio of ~ 6) and shows features typical
of a single old stellar population. The mean pulsation period of the RRab stars
= 0.628, {\sigma} = 0.071 days (or = 0.599, {\sigma} = 0.032 days,
if V4, the longest period and brightest variable, is discarded) and the
position on the period-amplitude diagram suggest an Oosterhoff-intermediate
classification for the galaxy. The RR Lyrae stars trace the galaxy horizontal
branch at an average apparent magnitude of = 20.43 +/- 0.02 mag
(average on 6 stars and discarding V4), giving in turn a distance modulus for
UMa I of (m-M)0 = 19.94 +/- 0.13 mag, distance d= 97.3 +6.0/-5.7 kpc, in the
scale where the distance modulus of the Large Magellanic Cloud is 18.5 +/- 0.1
mag. Isodensity contours of UMa I red giants and horizontal branch stars
(including the RR Lyrae stars identified in this study) show that the galaxy
has an S-shaped structure, which is likely caused by the tidal interaction with
the Milky Way. Photometric metallicities were derived for six of the UMa I RR
Lyrae stars from the parameters of the Fourier decomposition of the V-band
light curves, leading to an average metal abundance of [Fe/H] = -2.29 dex
({\sigma} = 0.06 dex, average on 6 stars) on the Carretta et al. metallicity
scale.Comment: Accepted for publication in Ap
An LBT view of the Andromeda’s satellite galaxies
Results are presented on deep (V â1⁄4 26.5 mag) time series observations of four dwarf spheroidal galaxies (dSphs) in the Andromeda (M31) complex, namely, And XIX, And XXI, And XXV and And XXVII, that we have observed with the Large Binocular Telescope (LBT). We discovered in these galaxies a total of over 200 RR Lyrae stars and 19 Anomalous Cepheids. We also characterised the stellar populations and the spatial distributions of these dSphs
Dwarf spheroidal satellites of M31: I. Variable stars and stellar populations in Andromeda XIX
We present B,V time-series photometry of Andromeda XIX (And XIX), the most
extended (half-light radius of 6.2') of Andromeda's dwarf spheroidal
companions, that we observed with the Large Binocular Cameras at the Large
Binocular Telescope. We surveyed a 23'x 23' area centered on And XIX and
present the deepest color magnitude diagram (CMD) ever obtained for this
galaxy, reaching, at V~26.3 mag, about one magnitude below the horizontal
branch (HB). The CMD shows a prominent and slightly widened red giant branch,
along with a predominantly red HB, which, however, extends to the blue to
significantly populate the classical instability strip. We have identified 39
pulsating variable stars, of which 31 are of RR Lyrae type and 8 are Anomalous
Cepheids (ACs). Twelve of the RR Lyrae variables and 3 of the ACs are located
within And XIX's half light radius. The average period of the fundamental mode
RR Lyrae stars ( = 0.62 d, \sigma= 0.03 d) and the period-amplitude
diagram qualify And XIX as an Oosterhoff-Intermediate system. From the average
luminosity of the RR Lyrae stars ( = 25.34 mag, \sigma= 0.10 mag) we
determine a distance modulus of (m-M)= mag in a scale where
the distance to the Large Magellanic Cloud (LMC) is mag. The ACs
follow a well defined Period-Wesenheit (PW) relation that appears to be in very
good agreement with the PW relationship defined by the ACs in the LMC.Comment: accepted for publication in Ap
VARIABLE STARS AND STELLAR POPULATIONS IN ANDROMEDA XXV. III. A CENTRAL CLUSTER OR THE GALAXY NUCLEUS?
We present B and V time series photometry of Andromeda XXV, the third galaxy in our program on the Andromeda’s satellites, which we have imaged with the Large Binocular Cameras of the Large Binocular Telescope. The field of Andromeda XXV is found to contain 62 variable stars, for which we present light curves and characteristics of the light variation (period, amplitudes, variability type, mean magnitudes, etc.). The sample includes 57 RR Lyrae variables (46 fundamental-mode—RRab, and 11 first-overtone—RRc, pulsators), 3 anomalous Cepheids, 1 eclipsing binary system, and 1 unclassified variable. The average period of the RRab stars ( =0.60 σ = 0.04 days) and the period–amplitude diagram place Andromeda XXV in the class of the Oosterhoff-Intermediate objects. From the average luminosity of the RR Lyrae stars we derive for the galaxy a distance modulus of (m–M)0 = 24.63 ± 0.17 mag. The color–magnitude diagram reveals the presence in Andromeda XXV of a single, metal-poor ([Fe/H] = ‑1.8 dex) stellar population as old as ∼10–12 Gyr, traced by a conspicuous red giant branch and the large population of RR Lyrae stars. We discovered a spherically shaped high density of stars near the galaxy center. This structure appears to be at a distance consistent with Andromeda XXV and we suggest it could either be a star cluster or the nucleus of Andromeda XXV. We provide a summary and compare the number and characteristics of the pulsating stars in the M31 satellites analyzed so far for variability.
Based on data collected with the Large Binocular Cameras at the Large Binocular Telescope
Variable Stars and Stellar Populations in Andromeda XXVII. IV. An Off-centered, Disrupted Galaxy
We present B and V time-series photometry of the M31 satellite galaxy Andromeda XXVII (And XXVII) that we observed with the Large Binocular Cameras of the Large Binocular Telescope. In the field of And XXVII we have discovered a total of 90 variables: 89 RR Lyrae stars and 1 Anomalous Cepheid. The average period of the fundamental mode RR Lyrae stars (RRab) < {P}{ab}> =0.59 {days} (σ = 0.05 day) and the period–amplitude diagram place And XXVII in the class of Oosterhoff I/Intermediate objects. Combining information from the color–magnitude diagram (CMD) and the variable stars, we find evidence for a single old and metal-poor stellar population with [Fe/H] ∼ ‑1.8 dex and t ∼ 13 Gyr in And XXVII. The spatial distributions of RR Lyrae and red giant branch (RGB) stars give clear indication that And XXVII is a completely disrupted system. This is also supported by the spread observed along the line of sight in the distance to the RR Lyrae stars. The highest concentration of RGB and RR Lyrae stars is found in a circular area of 4 arcmin in radius, centered about 0.°2 in the southeast direction from Richardson et al.’s center coordinates of And XXVII. The CMD of this region is well-defined, with a prominent RGB and 15 RR Lyrae stars (out of the 18 found in the region) tracing a very tight horizontal branch at < V({RR})> =25.24 {mag} σ = 0.06 mag (average over 15 stars). We show that And XXVII is a strong candidate building block of the M31 halo.
Based on data collected with the Large Binocular Cameras at the Large Binocular Telescope, PI: G. Clementini
Angular Diameters and Effective Temperatures of Twenty-five K Giant Stars from the CHARA Array
Using Georgia State University's CHARA Array interferometer, we measured
angular diameters for 25 giant stars, six of which host exoplanets. The
combination of these measurements and Hipparcos parallaxes produce physical
linear radii for the sample. Except for two outliers, our values match angular
diameters and physical radii estimated using photometric methods to within the
associated errors with the advantage that our uncertainties are significantly
lower. We also calculated the effective temperatures for the stars using the
newly-measured diameters. Our values do not match those derived from
spectroscopic observations as well, perhaps due to the inherent properties of
the methods used or because of a missing source of extinction in the stellar
models that would affect the spectroscopic temperatures
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