324 research outputs found
Discovery of blue companions to two southern Cepheids: WW Car and FN Vel
A large number of high-dispersion spectra of classical Cepheids were obtained
in the region of the CaII H+K spectral lines. The analysis of these spectra
allowed us to detect the presence of a strong Balmer line, H, for
several Cepheids, interpreted as the signature of a blue companion: the
presence of a sufficiently bright blue companion to the Cepheid results in a
discernible strengthening of the CaII H + Hepsilon line relative to the CaII K
line. We investigated 103 Cepheids, including those with known hot companions
(B5-B6 main-sequence stars) in order to test the method. We could confirm the
presence of a companion to WW Car and FN Vel (the existence of the former was
only suspected before) and we found that these companions are blue hot stars.
The method remains efficient when the orbital velocity changes in a binary
system cannot be revealed and other methods of binarity detection are not
efficient.Comment: 6 pages, 5 figures, 4 tables, published on MNRAS in March 201
Barium and Yttrium abundance in intermediate-age and old open clusters
Barium is a neutron capture element, that, in open clusters, is frequently
over-abundant with respect to the Iron. A clear explanation for this is still
missing. Additionally, its gradient across the Galactic disk is poorly
constrained. We measure the abundance of yttrium and barium using the synthetic
spectrum method from UVES high-resolution spectra of eight distant open
clusters, namely Ruprecht 4, Ruprecht 7, Berkeley 25, Berkeley 73, Berkeley 75,
NGC 6192, NGC 6404, and NGC 6583. The barium abundance was estimated using NLTE
approximation. We confirm that Barium is indeed over-abundant in most clusters,
especially young clusters. Finally, we investigated the trend of yttrium and
barium abundances as a function of distance in the Galaxy and ages. Several
scenarios for the barium over-abundance are then discussed.Comment: 9 pages, 10 figure
On the correlation of elemental abundances with kinematics among galactic disk stars
We have performed the detailed analysis of 174 high-resolution spectra of FGK
dwarfs obtained with the ELODIE echelle spectrograph at the Observatoire de
Haute-Provence. Abundances of Fe, Si and Ni have been determined from
equivalent widths under LTE approximation, whereas abundances of Mg have been
determined under NLTE approximation using equivalent widths of 4 lines and
profiles of 5 lines. Spatial velocities with an accuracy better than 1 km/s, as
well as orbits, have been computed for all stars. They have been used to define
2 subsamples kinematically representative of the thin disk and the thick disk
in order to highlight their respective properties. A transition occurs at
[Fe/H]=-0.3. Stars more metal-rich than this value have a flat distribution
with Zmax<1 kpc and sigma_W<20 km/s, and a narrow distribution of [alpha/Fe].
There exist stars in this metallicity regime which cannot belong to the thin
disk because of their excentric orbits, neither to the thick disk because of
their low scale height. Several thin disk stars are identified down to
[Fe/H]=-0.80. Their Mg enrichment is lower than thick disk stars with the same
metallicity. We confirm from a larger sample the results of Feltzing et al
(2003) and Bensby et al (2003) showing a decrease of [alpha/Fe] with [Fe/H] in
the thick disk interpreted as the signature of the SNIa which have
progressively enriched the ISM with iron. However our data suggest that the
star formation in the thick disk stopped when the enrichment was [Fe/H]=-0.30,
[Mg/Fe]=+0.20, [Si/Fe]=+0.17. A vertical gradient in [alpha/Fe] may exist in
the thick disk but should be confirmed with a larger sample. Finally we have
identified 2 new candidates of the HR1614 moving group.Comment: Accepted in A&A, 16 pages, 14 figure
Reddenings of FGK supergiants and classical Cepheids from spectroscopic data
Accurate and homogeneous atmospheric parameters (Teff, log (g), Vt, [Fe/H])
are derived for 74 FGK non-variable supergiants from high-resolution, high
signal-to-noise ratio, echelle spectra. Extremely high precision for the
inferred effective temperatures (10-40 K) is achieved by using the line-depth
ratio method. The new data are combined with atmospheric values for 164
classical Cepheids, observed at 675 different pulsation phases, taken from our
previously published studies. The derived values are correlated with unreddened
B-V colours compiled from the literature for the investigated stars in order to
obtain an empirical relationship of the form: (B-V)o = 57.984 - 10.3587(log
Teff)^2 + 1.67572(log Teff)^3 - 3.356(log (g)) + 0.0321(Vt) + 0.2615[Fe/H] +
0.8833((log (g))(log Teff)). The expression is used to estimate colour excesses
E(B-V) for individual supergiants and classical Cepheids, with a precision of
+-0.05 mag. for supergiants and Cepheids with n=1-2 spectra, reaching +-0.025
mag. for Cepheids with n>2 spectra, matching uncertainties for the most
sophisticated photometric techniques. The reddening scale is also a close match
to the system of space reddenings for Cepheids. The application range is for
spectral types F0--K0 and luminosity classes I and II.Comment: accepted for publication (MNRAS
The Distribution of the Elements in the Galactic Disk III. A Reconsideration of Cepheids from l = 30 to 250 Degrees
This paper reports on the spectroscopic investigation of 238 Cepheids in the
northern sky. Of these stars, about 150 are new to the study of the galactic
abundance gradient. These new Cepheids bring the total number of Cepheids
involved in abundance distribution studies to over 400. In this work we also
consider systematics between various studies and also those which result from
the choice of models. We find systematic variations exist at the 0.06 dex level
both between studies and model atmospheres. In order to control the systematic
effects our final gradients depend only on abundances derived herein. A simple
linear fit to the Cepheid data from 398 stars yields a gradient d[Fe/H]/dRG =
-0.062 \pm 0.002 dex/kpc which is in good agreement with previously determined
values. We have also reexamined the region of the "metallicity island" of Luck
et al. (2006). With the doubling of the sample in that region and our
internally consistent abundances, we find there is scant evidence for a
distinct island. We also find in our sample the first reported Cepheid (V1033
Cyg) with a pronounced Li feature. The Li abundance is consistent with the star
being on its red-ward pass towards the first giant branch.Comment: 66 pages including tables, 12 figures, Accepted Astronomical Journa
The Pulsation Mode and Distance of the Cepheid FF Aquilae
The determination of pulsation mode and distance for field Cepheids is a
complicated problem best resolved by a luminosity estimate. For illustration a
technique based on spectroscopic luminosity discrimination is applied to the
4.47d s-Cepheid FF Aql. Line ratios in high dispersion spectra of the variable
yield values of =-3.40+-0.02 s.e.(+-0.04 s.d.), average effective
temperature Teff=6195+-24 K, and intrinsic color (-)o = +0.506+-0.007,
corresponding to a reddening of E(B-V)=0.25+-0.01, or E(B-V)(B0)=0.26+-0.01.
The skewed light curve, intrinsic color, and luminosity of FF Aql are
consistent with fundamental mode pulsation for a small amplitude classical
Cepheid on the blue side of the instability strip, not a sinusoidal pulsator. A
distance of 413+-14 pc is estimated from the Cepheid's angular diameter in
conjunction with a mean radius of =39.0+-0.7 Rsun inferred from its
luminosity and effective temperature. The dust extinction towards FF Aql is
described by a ratio of total-to-selective extinction of
Rv=Av/E(B-V)=3.16+-0.34 according to the star's apparent distance modulus.Comment: To appear in ApJ
On the subject of the Ba overabundance in the open clusters stars
For eight distant open clusters, namely Ruprecht 4, Ruprecht 7, Berkeley 25, Berkeley 73, Berkeley 75, NGC 6192, NGC 6404, and NGC 6583, we determined the yttrium and barium abundances using the UVES, VLT spectra (ESO, Chile). The stars of one young cluster (Ruprecht 7) demonstrate significant barium overabundance( 3c0.55 dex) that can not be due to the determination error. We have considered the Ba abundance determination errors due to LTE approach, saturation of the lines, synthetic and observed barium line fitting, and the causes of the Ba overabundance associated with the Galactic disc enrichment or the origin of open clusters. Possible explanation for this overabundance can be the origin of n-capture elements enrichment of the clusters (galactic or extragalactic) or additional sources of the Ba production
The Cepheid Impostor HD 18391 and its Anonymous Parent Cluster
New and existing photometry for the G0 Ia supergiant HD 18391 is analyzed in
order to confirm the nature of the variablity previously detected in the star,
which lies off the hot edge of the Cepheid instability strip. Small-amplitude
variability at a level of \Delta V = 0.016+-0.002 is indicated, with a period
of P=123.04+-0.06 d. A weaker second signal may be present at P=177.84+-0.18
with \Delta V = 0.007+-0.002, likely corresponding to fundamental mode
pulsation if the primary signal represents overtone pulsation (123.04/177.84 =
0.69). The star, with a spectroscopic reddening of E(B-V) = 1.02, is associated
with heavily-reddened B-type stars in its immediate vicinity that appear to be
outlying members of an anonymous young cluster centered ~10 arcmin to the west
and 1661+-73 pc distant. The cluster has nuclear and coronal radii of r_n=3.5
arcmin and R_c=14 arcmin, respectively, while the parameters for HD 18391
derived from membership in the cluster with its outlying B stars are consistent
with those implied by its Cepheid-like pulsation, provided that it follows the
semi-period-luminosity relation expected of such objects. Its inferred
luminosity as a cluster member is M_V=-7.76+-0.10, its age (9+-1)x10^6 years,
and its evolutionary mass ~19 M_{\sun}. HD 18391 is not a classical Cepheid,
yet it follows the Cepheid period-luminosity relation closely, much like
another Cepheid impostor, V810 Cen.Comment: Accepted for Publication (Astronomische Nachrichten
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