86 research outputs found
Search for Associations Containing Young stars (SACY): Chemical tagging IC 2391 & the Argus association
We explore the possible connection between the open cluster IC 2391 and the
unbound Argus association identified by the SACY survey. In addition to common
kinematics and ages between these two systems, here we explore their chemical
abundance patterns to confirm if the two substructures shared a common origin.
We carry out a homogenous high-resolution elemental abundance study of eight
confirmed members of IC 2391 as well as six members of the Argus association
using UVES spectra. We derive spectroscopic stellar parameters and abundances
for Fe, Na, Mg, Al, Si, Ca, Ti, Cr, Ni and Ba.
All stars in the open cluster and Argus association were found to share
similar abundances with the scatter well within the uncertainties, where [Fe/H]
= -0.04 +/-0.03 for cluster stars and [Fe/H] = -0.06 +/-0.05 for Argus stars.
Effects of over-ionisation/excitation were seen for stars cooler than roughly
5200K as previously noted in the literature. Also, enhanced Ba abundances of
around 0.6 dex were observed in both systems. The common ages, kinematics and
chemical abundances strongly support that the Argus association stars
originated from the open cluster IC 2391. Simple modeling of this system find
this dissolution to be consistent with two-body interactions.Comment: 17 pages, 7 figs, accepted for publication in MNRA
HST/NICMOS observations of a proto-brown dwarf candidate
We present deep HST/NICMOS observations peering through the outflow cavity of
the protostellar candidate IRAS 04381+2540 in the Taurus Molecular Cloud-1. A
young stellar object as central source, a jet and a very faint and close (0.6")
companion are identified. The primary and the companion have similar colours,
consistent with strong reddening. We argue that the companion is neither a
shock-excited knot nor a background star. The colour/magnitude information
predicts a substellar upper mass limit for the companion, but the final
confirmation will require spectroscopic information. Because of its geometry,
young age and its rare low-mass companion, this system is likely to provide a
unique insight into the formation of brown dwarfs.Comment: Astronomy & Astrophysics Letters, in press; 4 pages, 2 figure
A brown dwarf companion to the intermediate-mass star HR6037
In the course of an imaging survey we have detected a visual companion to the
intermediate-mass star HR 6037. In this letter, we present two epoch
observations of the binary with NACO/VLT, and near-IR spectroscopy of the
secondary with ISAAC/VLT. The NACO observations allow us to confirm HR 6037B as
a co-moving companion. Its J and H band ISAAC spectra suggest the object has an
spectral type of M9+-1, with a surface gravity intermediate between that of 10
Myr dwarfs and field dwarfs with identical spectral type. The comparison of its
Ks-band photometry with evolutionary tracks allows us to derive a mass,
effective temperature, and surface gravity of 62+-20 MJup, Teff = 2330+-200 K,
and log g = 5.1+-0.2, respectively. The small mass ratio of the binary, -0.03,
and its long orbital period, -5000 yr, makes HR 6037 a rare and uncommon binary
system.Comment: (5 pages, 4 figures, accepted for publication in A&A Letters
Very Low Mass Stars and Brown Dwarfs in Taurus-Auriga
We present high resolution optical spectra obtained with the HIRES
spectrograph on the Keck I telescope of low mass T Tauri stars and brown dwarfs
(LMTTs) in Taurus-Auriga. Of particular interest is the previously classified
"continuum T Tauri star" GM Tau, which has a spectral type of M6.5 and a mass
just below the stellar/substellar boundary. None of the LMTTs in Taurus are
rapidly rotating (vsini < 30 km/s), unlike low mass objects in Orion. Many of
the slowly rotating, non-accreting stars and brown dwarfs exhibit prominent
H-alpha emission (EWs of 3 - 36 A), indicative of active chromospheres. We
demonstrate empirically that the full-width at 10% of the H-alpha emission
profile peak is a more practical and possibly more accurate indicator of
accretion than either the equivalent width of H-alpha or optical veiling:
10%-widths > 270 km/s are classical T Tauri stars (i.e. accreting), independent
of stellar spectral type. Although LMTTs can have accretion rates comparable to
that of more typical, higher-mass T Tauri stars (e.g. K7-M0), the average mass
accretion rate appears to decrease with decreasing mass. The diminished
frequency of accretion disks for LMTTs, in conjunction with their lower, on
average, mass accretion rates, implies that they are formed with less massive
disks than higher-mass T Tauri stars. The radial velocities, circumstellar
properties and known binaries do not support the suggestion that many of the
lowest mass members of Taurus have been ejected from higher stellar density
regions within the cloud. Instead, LMTTs appear to have formed and are evolving
in the same way as higher-mass T Tauri stars, but with smaller disks and
shorter disk lifetimes.Comment: 27 pages, plus 8 figures, accepted for publication in Ap
Optical Spectroscopy of the Surface Population of the rho Ophiuchi Molecular Cloud: The First Wave of Star Formation
We present the results of optical spectroscopy of 139 stars obtained with the
Hydra multi-object spectrograph. The objects extend over a 1.3 square degree
area surrounding the main cloud of the rho Oph complex. The objects were
selected from narrowband images to have H alpha in emission. Using the presence
of strong H alpha emission, lithium absorption, location in the
Hertzsprung-Russell diagram, or previously reported x-ray emission, we were
able to identify 88 objects as young stars associated with the cloud. Strong H
alpha emission was confirmed in 39 objects with line widths consistent with
their origin in magnetospheric accretion columns. Two of the strongest
emission-line objects are young, x-ray emitting brown dwarf candidates with M8
spectral types. Comparisons of the bolometric luminosities and effective
temperatures with theoretical models suggest a medianage for this population of
2.1 Myr which is signifcantly older than the ages derived for objects in the
cloud core. It appears that these stars formed contemporaneously with low mass
stars in the Upper Scorpius subgroup, likely triggered by massive stars in the
Upper-Centaurus subgroup.Comment: 35 pages of postscript which includes seven figures (some of which
are multi-panel) and four postscript tables. Astronomical Journal (in press
Binary frequency of very young brown dwarfs at separations smaller than 3 AU
Searches for companions of brown dwarfs by direct imaging mainly probe
orbital separations > 3-10 AU. On the other hand, previous radial velocity
surveys of brown dwarfs are mainly sensitive to separations smaller than 0.6
AU. It has been speculated that the peak of the separation distribution of
brown dwarf binaries lies right in the unprobed range. This work extends
high-precision radial velocity surveys of brown dwarfs for the first time out
to 3 AU. Based on more than six years UVES/VLT spectroscopy the binary
frequency of brown dwarfs and (very) low-mass stars (M4.25-M8) in ChaI was
determined: 18% for the whole sample and 10% for the subsample of ten brown
dwarfs and VLMS (M < 0.1 Msun). Two spectroscopic binaries were confirmed, the
brown dwarf candidate ChaHa8 (previously discovered by Joergens & Mueller) and
the low-mass star CHXR74. Since their orbital separations appear to be 1 AU or
greater, the binary frequency at < 1 AU might be less than 10%. Now for the
first time companion searches of (young) brown dwarfs cover the whole orbital
separation range, and the following observational constraints for models of
brown dwarf formation can be derived: (i) the frequency of brown dwarf and very
low-mass stellar binaries at 3
AU; i.e. direct imaging surveys do not miss a significant fraction of brown
dwarf binaries; (ii) the overall binary frequency of brown dwarfs and very
low-mass stars is 10-30 %; (iii) the decline in the separation distribution of
brown dwarfs towards smaller separations seems to occur between 1 and 3 AU;
(iv) the observed continuous decrease in the binary frequency from the stellar
to the substellar regime is confirmed at < 3 AU providing further evidence of a
continuous formation mechanism from low-mass stars to brown dwarfs.Comment: 17 pages, 14 figures, Accepted by A&A, minor language editin
An old nearby quadruple system Gliese 225.2
We discovered a new component E in the nearby multiple system Gliese 225.2, making it quadruple. We derive a preliminary 24-yr astrometric orbit of this new sub-system C,E and a slightly improved orbit of the 68-yr pair A,B. The orientations of the A,B and C,E orbits indicate that they may be close to coplanarity. The orbit of AB,CE is rather wide and does not allow to determine its curvature reliably. Thus, the 390 yr orbit computed by Baize (1980, Inf. Circ. IAU Comm., 26(80)) was premature. The infrared colors and magnitudes of components A, B, and C match standard values for dwarfs of spectral types K5V, M0V, and K4V, respectively. The new component E, 3 magnitudes below the Main Sequence, has an anomalously blue color index. We estimate its mass as roughly 0.2 solar from the astrometric orbit, although there remains some inconsistency in the data hinting on a higher mass or on the existence of additional components in the system. Large space velocities indicate that Gliese 225.2 belongs to the thick Galactic disk and is not young. This quadruple system survived for a long time and should be dynamically stable. © ESO 2005
Gliese 225.2: An old (stable?) quadruplet
We discovered with adaptive optics a new component E in the nearby multiple system Gliese 225.2, making it quadruple. We derive a preliminary 24-yr astrometric orbit of this new sub-system C,E and a slightly improved orbit of the 68-yr pair A,B. The orientations of the A,B and C,E orbits indicate that they may be close to coplanarity. The 390-yr orbit of AB,CE computed by Baize (1980) was premature, the period is much longer. Large space velocities indicate that Gliese 225.2 belongs to the thick galactic disk and is not young. This quadruple system survived for a long time and should be dynamically stable. © 2008 Springer-Verlag Berlin Heidelberg
The Evolution of Circumstellar Disks in Ophiuchus Binaries
Four Ophiuchus binaries, two Class I systems and two Class II systems, with
separations of ~450-1100 AU, were observed with the Owens Valley Radio
Observatory (OVRO) millimeter interferometer. In each system, the 3 mm
continuum maps show dust emission at the location of the primary star, but no
emission at the position of the secondary. This result is different from
observations of less evolved Class 0 binaries, in which dust emission is
detected from both sources. The nondetection of secondary disks is, however,
similar to the dust distribution seen in wide Class II Taurus binaries. The
combined OVRO results from the Ophiuchus and Taurus binaries suggest that
secondary disk masses are significantly lower than primary disk masses by the
Class II stage, with initial evidence that massive secondary disks are reduced
by the Class I stage. Although some of the secondaries retain hot inner disk
material, the early dissipation of massive outer disks may negatively impact
planet formation around secondary stars. Masses for the circumprimary disks are
within the range of masses measured for disks around single T Tauri stars and,
in some cases, larger than the minimum mass solar nebula. More massive primary
disks are predicted by several formation models and are broadly consistent with
the observations. Combining the 3 mm data with previous 1.3 mm observations,
the dust opacity power-law index for each primary disk is estimated. The
opacity index values are all less than the scaling for interstellar dust,
possibly indicating grain growth within the circumprimary disks
WISE J061213.85-303612.5: a new T-dwarf binary candidate
Context. T and Y dwarfs are among the coolest and least luminous objects detected, and they can help to understand the properties of giant planets. Up to now, there are more than 350 T dwarfs that have been identified thanks to large imaging surveys in the infrared, and their multiplicity properties can shed light on the formation process.
Aims. The aim of this work is to look for companions around a sample of seven ultracoool objects. Most of them have been discovered by the WISE observatory and have not been studied before for multiplicity.
Methods. We observed a sample six T dwarfs and one L9 dwarf with the Laser Guide Star (LGS) and NAOS-CONICA, the adaptive optics (AO) facility, and the near infrared camera at the ESO Very Large Telescope. We observed all the objects in one or more near-IR filters (JHK_s).
Results. From the seven observed objects, we have identified a subarcsecond binary system, WISE J0612-3036, composed of two similar components with spectral types of T6. We measure a separation of ρ = 350 ± 5 mas and a position angle of PA = 235 ± 1°. Using the mean absolute magnitudes of T6 dwarfs in the 2MASS JHK_s bands, we estimate a distance of d = 31 ± 6 pc and derive a projected separation of ρ ~ 11 ± 2 au. Another target, WISE J2255-3118, shows a very faint object at 1.̋3 in the K_s image. The object is marginally detected in H, and we derive a near infrared color of H − Ks> 0.1 mag. HST/WFC3 public archival data reveals that the companion candidate is an extended source. Together with the derived color, this suggests that the source is most probably a background galaxy. The five other sources are apparently single, with 3-σ sensitivity limits between H = 19–21 for companions at separations ≥ 0.̋5.
Conclusions. WISE 0612-3036 is probably a new T-dwarf binary composed of two T6 dwarfs. As in the case of other late T-dwarf binaries, it shows a mass ratio close to 1, although its projected separation, ~11 au, is larger than the average (~5 au). Additional observations are needed to confirm that the system is bound
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