55 research outputs found
Proper Motions and CCD-photometry of Stars in the Region of the Open Cluster Trumpler 2
The results of the complex study of galactic open cluster Trumpler 2 are
presented. In order to obtain the proper motions the positions of 2600 stars up
to the limit magnitude B ~ 16.25 mag in the area 80x80 arcmin around the
cluster were measured on 6 plates with the maximal epoch difference of 63
years. The root-mean error of the relative proper motions is 4.2 mas/yr. The
catalogue of BV magnitudes of all the stars in the investigated area was
compiled. Astrometric selection of the cluster members within the region of
R<16 arcmin from the center of the cluster was made by means of the W.Sanders
method. In that field 192 stars were found to have the individual membership
probability greater then 85%, 148 of them are situated within the
+/-3sigma_(B-V) band around the main sequence of the cluster. They are
considered to be cluster members by two criteria. The U-B ~ B-V diagram plotted
for the astrometrical cluster members by the data taken from the Washington
catalogue of the UBV photometry in the galactic cluster fields (Hoag et
al.1961) made it possible to redefine the value of the color excess E(B-V)=0.40
mag. The superposition of the MS of the cluster with the ZAMS Schmidt-Kaler
leads to the coincidence at the value of the apparent distance module
(V-Mv)=10.50 which corresponds to the distance r=725 pc. The luminosity and
mass functions of the Trumpler 2 were constructed and the value of the slope
Gamma=-1.90+/-0.22 was determined. The cluster age of 8.913x10^7 yr was
determined. It is shown that the red giant on the late stage of the evolution
(st N.1095) belongs to cluster and indicates the brightness variability. The
possibility that the number of both known and recently discovered variables are
cluster members was considered. Tables 2,3,3A,5 will be only available in the
electronic form.Comment: 14 pages, 7 figure
Radial velocity measurements of B stars in the Scorpius-Centaurus association
We derive single-epoch radial velocities for a sample of 56 B-type stars
members of the subgroups Upper Scorpius, Upper Centaurus Lupus and Lower
Centaurus Crux of the nearby Sco-Cen OB association. The radial velocity
measurements were obtained by means of high-resolution echelle spectra via
analysis of individual lines. The internal accuracy obtained in the
measurements is estimated to be typically 2-3 km/s, but depends on the
projected rotational velocity of the target. Radial velocity measurements taken
for 2-3 epochs for the targets HD120307, HD142990 and HD139365 are variable and
confirm that they are spectroscopic binaries, as previously identified in the
literature. Spectral lines from two stellar components are resolved in the
observed spectra of target stars HD133242, HD133955 and HD143018, identifying
them as spectroscopic binaries.Comment: accepted for publication in A&
Chemical abundances and kinematics of barium stars
In this paper we present an homogeneous analysis of photospheric abundances
based on high-resolution spectroscopy of a sample of 182 barium stars and
candidates. We determined atmospheric parameters, spectroscopic distances,
stellar masses, ages, luminosities and scale height, radial velocities,
abundances of the Na, Al, -elements, iron-peak elements, and s-process
elements Y, Zr, La, Ce, and Nd. We employed the local-thermodynamic-equilibrium
model atmospheres of Kurucz and the spectral analysis code {\sc moog}. We found
that the metallicities, the temperatures and the surface gravities for barium
stars can not be represented by a single gaussian distribution. The abundances
of -elements and iron peak elements are similar to those of field giants
with the same metallicity. Sodium presents some degree of enrichment in more
evolved stars that could be attributed to the NeNa cycle. As expected, the
barium stars show overabundance of the elements created by the s-process. By
measuring the mean heavy-element abundance pattern as given by the ratio
[s/Fe], we found that the barium stars present several degrees of enrichment.
We also obtained the [hs/ls] ratio by measuring the photospheric abundances of
the Ba-peak and the Zr-peak elements. Our results indicated that the [s/Fe] and
the [hs/ls] ratios are strongly anti-correlated with the metallicity. Our
kinematical analysis showed that 90% of the barium stars belong to the thin
disk population. Based on their luminosities, none of the barium stars are
luminous enough to be an AGB star, nor to become self-enriched in the s-process
elements. Finally, we determined that the barium stars also follow an
age-metallicity relation.Comment: 30 pages, 26 figures, 18 tables, accepted for publication in MNRA
On the common origin of the AB Dor moving group and the Pleiades cluster
AB Dor is the nearest identified moving group. As with other such groups, the
age is important for understanding of several key questions. It is important,
for example, in establishing the origin of the group and also in comparative
studies of the properties of planetary systems, eventually surrounding some of
the AB Dor group members, with those existing in other groups. For AB Dor two
rather different estimates for its age have been proposed: a first one, of the
order of 50 Myr, by Zuckerman and coworkers from a comparison with
Tucana/Horologium moving group and a second one of about 100-125 Myr by Luhman
and coworkers from color-magnitude diagrams (CMD). Using this last value and
the closeness in velocity space of AB Dor and the Pleiades galactic cluster,
Luhman and coworkers suggested coevality for these systems. Because strictly
speaking such a closeness does not still guarantee coevality, here we address
this problem by computing and comparing the full 3D orbits of AB Dor, Pleiades,
alpha Persei and IC 2602. The latter two open clusters have estimated ages of
about 85-90 Myr and 50 Myr. The resulting age 119 20 Myr is consistent
with AB Dor and Pleiades being coeval. Our solution and the scenario of open
cluster formation proposed by Kroupa and collaborators suggest that the AB Dor
moving group may be identified with the expanding subpopulation (Group I)
present in this scenario. We also discuss other related aspects as iron and
lithium abundances, eventual stellar mass segregation during the formation of
the systems and possible fraction of debris discs in AB Dor group.Comment: 11 pages, 5 figures and 2 table
CD-62°1346: An extreme halo or hypervelocity CH star?
High-velocity halo stars provide important information about the properties of the extreme Galactic halo. The study of unbound and bound Population II stars permits us to better estimate the mass of the halo. Aims: We carried out a detailed spectroscopic and kinematic study and have significantly refined the distance and the evolutionary state of the star. Methods: Its atmospheric parameters, chemical abundances and kinematical properties were determined using high-resolution optical spectroscopy and employing the local-thermodynamic-equilibrium model atmospheres of Kurucz and the spectral analysis code moog. Results: We found that CD-62°1346 is a metal-poor ([Fe/H] = -1.6) evolved giant star with Teff = 5300 K and log g = 1.7. The star exhibits high carbon and s-element abundances typical of CH stars. It is also a lead star. Our kinematic analysis of its 3D space motions shows that this star has a highly eccentric (e = 0.91) retrograde orbit with an apogalactic distance of ~100 kpc, exceeding by a factor of two the distance of the Magellanic Clouds. The star travels with very high velocity relative to the Galactocentric reference frame (VGRF = 570 km s-1). Conclusions: CD-62°1346 is an evolved giant star and not a subgiant star, as was considered earlier. Whether it is bound or unbound to the Galaxy depends on the assumed mass and on the adopted Galactic potential. We also show that the star HD 5223 is another example of a high-velocity CH star that exceeds the Galactic escape velocity. Possible origins of these two high-velocity stars are briefly discussed. CD-62°1346 and HD 5223 are the first red giant stars to join the restricted group of hypervelocity stars.Fil: Pereira, C. B.. MinistĂ©rio de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; BrasilFil: Jilinski, E.. MinistĂ©rio de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil. Universidade do Estado de Rio do Janeiro; Brasil. Russian Academy of Sciences. Pulkovo Observatory; RusiaFil: Drake, N. A.. MinistĂ©rio de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil. Russian Academy of Sciences. Pulkovo Observatory; RusiaFil: de Castro, D. B.. MinistĂ©rio de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; BrasilFil: Ortega, V. G.. MinistĂ©rio de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; BrasilFil: Chavero, Carolina Andrea. Universidad Nacional de CĂłrdoba. Observatorio AstronĂłmico de CĂłrdoba; Argentina. Consejo Nacional de Investigaciones CientĂficas y TĂ©cnicas; ArgentinaFil: Roig, Fernando Virgilio. MinistĂ©rio de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasi
Memberships and CM Diagrams of the Open Cluster NGC 7243
The results of astrometric and photometric investigations of the open cluster
NGC 7243 are presented. Proper motions of 2165 stars with root-mean-square
error of 1.1 mas/yr were obtained by means of PDS scanning of astrometric
plates covering the time interval of 97 years. A total of 211 cluster members
down to V=15.5 mag have been identified. V and B magnitudes have been
determined for 2118 and 2110 stars respectively. Estimations of mass (348Mo < M
< 522Mo), age (t=2.5x10^8 yr), distance (r=698 pc) and reddening (E(B-V)=0.24)
of the cluster NGC 7243 have been made.Comment: 24 pages, 15 figures. Submitted to Astronomy and Astrophysic
A formation scenario of young stellar groups in the region of the Scorpio Centaurus OB association
The main objective of this work is to investigate the role played by Lower
Centaurus Crux (LCC) and Upper Centaurus Lupus (UCL), both subcomponents of the
Scorpio Centaurus OB association (Sco-Cen), in the formation of the groups beta
Pictoris, TW Hydrae and the eta Chamaeleontis cluster. The dynamical evolution
of all the stellar groups involved and of the bubbles and shells blown by LCC
and UCL are calculated and followed from the past to the present. This leads to
a formation scenario in which (1) the groups beta Pictoris, TW Hydrae were
formed in the wake of the shells created by LCC and UCL, (2) the young cluster
eta Chamaeleontis was born as a consequence of the collision of the shells of
LCC and UCL, and (3) the formation of Upper Scorpius (US), the other main
subcomponent of the Sco-Cen association, may have been started by the same
process that created eta Chamaeleontis
A brown dwarf desert for intermediate mass stars in Sco OB2?
We present JHK observations of 22 intermediate-mass stars in Sco OB2,
obtained with VLT/NACO. The survey was performed to determine the status of
(sub)stellar candidate companions of A and late-B members. The distinction
between companions and background stars is by a comparison with isochrones and
statistical arguments. We are sensitive to companions in the separation range
0.1''-11'' (13-1430 AU) and K<17. We detect 62 secondaries of which 18 are
physical companions (3 new), 11 candidates, and 33 background stars. The
companion masses are in the range 0.03<M<1.19 Msun, with mass ratios
0.06<q<0.55. We include in our sample a subset of 9 targets with multi-color
ADONIS observations from Kouwenhoven et al. (2005). In the ADONIS survey
secondaries with K12 as
background stars. Our multi-color analysis demonstrates that the simple K=12
criterion correctly classifies the secondaries in ~80% of the cases. We
reanalyse the total ADONIS/NACO sample and conclude that of the 176
secondaries, 25 are physical companions, 55 are candidates, and 96 are
background stars. Although we are sensitive and complete to brown dwarfs as
faint as K=14 in the separation range 130-520 AU, we detect only one, giving a
brown dwarf companion fraction of 0.5% (M>30 MJ). However, the number of brown
dwarfs is consistent with an extrapolation of the stellar companion mass
distribution. This indicates that the physical mechanism for the formation of
brown dwarfs around intermediate mass stars is similar to that of stellar
companions, and that the embryo ejection mechanism does not need to be invoked
in order to explain the small number of brown dwarf companions among these
stars.Comment: 29 pages, 9 figures, accepted by A&
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