1,346 research outputs found
Mid-infrared interferometry of the massive young stellar object NGC 2264 IRS 1
The optically invisible infrared-source NGC 2264 IRS 1 is thought to be a
massive young stellar object (~10 Msun). Although strong infrared excess
clearly shows that the central object is surrounded by large amounts of
circumstellar material, no information about the spatial distribution of this
circumstellar material has been available until now. We used the ESO Very Large
Telescope Interferometer to perform long-baseline interferometric observations
of NGC 2264 IRS 1 in the mid-infrared regime. Our observations resolve the
circumstellar material around NGC 2264 IRS 1, provide the first direct
measurement of the angular size of the mid-infrared emission, and yield direct
constraints on the spatial distribution of the dust. We use different
approaches (a geometrical model, a temperature-gradient model, and radiative
transfer models) to jointly model the observed interferometric visibilities and
the spectral energy distribution. The derived visibility values between ~0.02
and ~0.3 show that the mid-infrared emission is clearly resolved. The
characteristic size of the MIR-emission region is ~30-60 AU; this value is
typical for other YSOs with similar or somewhat lower luminosities. A
comparison of the sizes for the two position angles shows a significant
elongation of the dust distribution. Simple spherical envelope models are
therefore inconsistent with the data. The radiative transfer modeling of our
data suggests that we observe a geometrically thin and optically thick
circumstellar disk with a mass of about 0.1 Msun. Our modeling indicates that
NGC 2264 IRS 1 is surrounded by a flat circumstellar disk that has properties
similar to disks typically found around lower-mass young stellar objects. This
result supports the assumption that massive young stellar objects form via
accretion from circumstellar disks.Comment: 11 pages, accepted for publication in A&
Near-infrared spectroscopy of EX Lupi in outburst
EX Lup is the prototype of the EXor class of young eruptive stars: objects
showing repetitive brightenings due to increased accretion from the
circumstellar disk to the star. In this paper, we report on medium-resolution
near-infrared spectroscopy of EX\,Lup taken during its extreme outburst in
2008, as well as numerical modeling with the aim of determining the physical
conditions around the star. We detect emission lines from atomic hydrogen,
helium, and metals, as well as first overtone bandhead emission from carbon
monoxide. Our results indicate that the emission lines are originating from gas
located in a dust-free region within ~ 0.2 AU of the star. The profile of the
CO bandhead indicates that the CO gas has a temperature of 2500 K, and is
located in the inner edge of the disk or in the outer parts of funnel flows.
The atomic metals are probably co-located with the CO. Some metallic lines are
fluorescently excited, suggesting direct exposure to ultraviolet photons. The
Brackett series indicates emission from hot (10000 K) and optically thin gas.
The hydrogen lines display a strong spectro-astrometric signal, suggesting that
the hydrogen emission is probably not coming from an equatorial boundary layer;
a funnel flow or disk wind origin is more likely. This picture is broadly
consistent with the standard magnetospheric accretion model usually assumed for
normally accreting T Tauri stars. Our results also set constraints on the
eruption mechanism, supporting a model where material piles up around the
corotation radius and episodically falls onto the star.Comment: 12 pages, 8 figures, 1 table, accepted for publication in Ap
Discovery of a stellar companion to the nearby solar-analogue HD 104304
Sun-like stars are promising candidates to host exoplanets and are often
included in exoplanet surveys by radial velocity (RV) and direct imaging. In
this paper we report on the detection of a stellar companion to the nearby
solar-analogue star HD 104304, which previously was considered to host a
planetary mass or brown dwarf companion. We searched for close stellar and
substellar companions around extrasolar planet host stars with high angular
resolution imaging to characterize planet formation environments. The detection
of the stellar companion was achieved by high angular resolution measurements,
using the "Lucky Imaging" technique at the ESO NTT 3.5m with the AstraLux Sur
instrument. We combined the results with VLT/NACO archive data, where the
companion could also be detected. The results were compared to precise RV
measurements of HD 104304, obtained at the Lick and Keck observatories from
2001-2010.
We confirmed common proper motion of the binary system. A spectral type of
M4V of the companion and a mass of 0.21 M_Sun was derived. Due to comparison of
the data with RV measurements of the unconfirmed planet candidate listed in the
Extrasolar Planets Encyclopaedia, we suggest that the discovered companion is
the origin of the RV trend and that the inclination of the orbit of
approximately 35 degrees explains the relatively small RV signal.Comment: 4 pages, 4 PNG figures, use aa.cls, accepted for publication in
Astronomy & Astrophysic
Ground--state energies and widths of He and Li
We extract energies and widths of the ground states of He and Li from
recent single--level R--matrix fits to the spectra of the H)He and the He)Li reactions. The widths
obtained differ significantly from the formal R--matrix values but they are
close to those measured as full widths at half maxima of the spectra in various
experiments. The energies are somewhat lower than those given by usual
estimates of the peak positions. The extracted values are close to the
S--matrix poles calculated previously from the multi--term analyses of the
N-He elastic scattering data.Comment: 3 pages, no figures, uses revtex.sty, accepted for publication in
PRC, uuencoded postscript and tex-files available at
ftp://is1.kph.tuwien.ac.at/pub/ohu/fwidth.u
Final Results from phase II of the Mainz Neutrino Mass Search in Tritium Decay
The paper reports on the improved Mainz experiment on tritum
spectroscopy which yields a 10 times' higher signal to background ratio than
before. The main experimental effects and systematic uncertainties have been
investigated in side experiments and possible error sources have been
eliminated. Extensive data taking took place in the years 1997 to 2001. A
residual analysis of the data sets yields for the square of the electron
antineutrino mass the final result of eV/c. We derive an upper limit of
eV/c at 95% confidence level for the mass itself.Comment: 22 pages, 22 figures submitted to EPJ
The CRESST Dark Matter Search
We present first competitive results on WIMP dark matter using the
phonon-light-detection technique. A particularly strong limit for WIMPs with
coherent scattering results from selecting a region of the phonon-light plane
corresponding to tungsten recoils. The observed count rate in the neutron band
is compatible with the rate expected from neutron background. CRESST is
presently being upgraded with a 66 channel SQUID readout system, a neutron
shield and a muon veto system. This results in a significant improvement in
sensitivity.Comment: 6 pages, 3 figures, to be published in the proceedings of the 5th
International Workshop on the Identification and Detection of Dark Matter IDM
2004, Edinburgh, Sept. 2004, World Scientifi
Visual/infrared interferometry of Orion Trapezium stars: Preliminary dynamical orbit and aperture synthesis imaging of the Theta 1 Orionis C system
Located in the Orion Trapezium cluster, Theta 1 Orionis C is one of the
youngest and nearest high-mass stars (O5-O7) and also known to be a close
binary system. Using new multi-epoch visual and near-infrared bispectrum
speckle interferometric observations obtained at the BTA 6 m telescope, and
IOTA near-infrared long-baseline interferometry, we trace the orbital motion of
the Theta 1 Ori C components over the interval 1997.8 to 2005.9, covering a
significant arc of the orbit. Besides fitting the relative position and the
flux ratio, we apply aperture synthesis techniques to our IOTA data to
reconstruct a model-independent image of the Theta 1 Ori C binary system.
The orbital solutions suggest a high eccentricity (e approx. 0.91) and
short-period (P approx. 10.9 yrs) orbit. As the current astrometric data only
allows rather weak constraints on the total dynamical mass, we present the two
best-fit orbits. From these orbital solutions one can be favoured, implying a
system mass of 48 M_sun and a distance to the Trapezium cluster of 434 pc. When
also taking the measured flux ratio and the derived location in the HR-diagram
into account, we find good agreement for all observables, assuming a spectral
type of O5.5 for Theta 1 Ori C1 (M=34.0 M_sun) and O9.5 for C2 (M=15.5 M_sun).
We find indications that the companion C2 is massive itself, which makes it
likely that its contribution to the intense UV radiation field of the Trapezium
cluster is non-negligible. Furthermore, the high eccentricity of the
preliminary orbit solution predicts a very small physical separation during
periastron passage (approx. 1.5 AU, next passage around 2007.5), suggesting
strong wind-wind interaction between the two O stars.Comment: 13 pages, 9 figures, Accepted for publication in Astronomy &
Astrophysic
The vicinity of the galactic supergiant B[e] star CPD -57 2874 from near- and mid-IR long baseline spectro-interferometry with the VLTI (AMBER and MIDI)
We present the first spectro-interferometric observations of the
circumstellar envelope (CSE) of a B[e] supergiant (CPD -57 2874), performed
with the Very Large Telescope Interferometer (VLTI) using the beam-combiner
instruments AMBER (near-IR interferometry with three 8.3 m Unit Telescopes or
UTs) and MIDI (mid-IR interferometry with two UTs). Our observations of the CSE
are well fitted by an elliptical Gaussian model with FWHM diameters varying
linearly with wavelength. Typical diameters measured are
mas or AU (adopting a distance of 2.5 kpc) at
2.2\micron, and mas or AU at
12\micron. We show that a spherical dust model reproduces the SED but it
underestimates the MIDI visibilities, suggesting that a dense equatorial disk
is required to account for the compact dust-emitting region observed. Moreover,
the derived major-axis position angle in the mid-IR (\simeq144\degr) agrees
well with previous polarimetric data, hinting that the hot-dust emission
originates in a disk-like structure. Our results support the non-spherical CSE
paradigm for B[e] supergiants.Comment: To appear in the ASP proceedings of the Workshop "Stars with the B[e]
Phenomenon
The high-mass disk candidates NGC7538IRS1 and NGC7538S
Context: The nature of embedded accretion disks around forming high-mass
stars is one of the missing puzzle pieces for a general understanding of the
formation of the most massive and luminous stars. Methods: Using the Plateau de
Bure Interferometer at 1.36mm wavelengths in its most extended configuration we
probe the dust and gas emission at ~0.3",corresponding to linear resolution
elements of ~800AU. Results: NGC7538IRS1 remains a single compact and massive
gas core with extraordinarily high column densities, corresponding to visual
extinctions on the order of 10^5mag, and average densities within the central
2000AU of ~2.1x10^9cm^-3 that have not been measured before. We identify a
velocity gradient across in northeast-southwest direction that is consistent
with the mid-infrared emission, but we do not find a gradient that corresponds
to the proposed CH3OH maser disk. The spectral line data toward NGC7538IRS1
reveal strong blue- and red-shifted absorption toward the mm continuum peak
position. The red-shifted absorption allows us to estimate high infall rates on
the order of 10^-2 Msun/yr. Although we cannot prove that the gas will be
accreted in the end, the data are consistent with ongoing star formation
activity in a scaled-up low-mass star formation scenario. Compared to that,
NGC7538S fragments in a hierarchical fashion into several sub-sources. While
the kinematics of the main mm peak are dominated by the accompanying jet, we
find rotational signatures from a secondary peak. Furthermore, strong spectral
line differences exist between the sub-sources which is indicative of different
evolutionary stages within the same large-scale gas clump.Comment: 15 pages, 12 figures, accepted for A&
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