69 research outputs found
Astrometry with the MCAO instrument MAD - An analysis of single-epoch data obtained in the layer-oriented mode
Context: Current instrument developments at the largest telescopes worldwide
have provisions for Multi-Conjugated Adaptive Optics (MCAO) modules. The large
field of view and more uniform correction provided by these systems is not only
highly beneficial for photometric studies but also for astrometric analysis of,
e.g., large dense clusters and exoplanet detection and characterization. The
Multi-conjugated Adaptive optics Demonstrator (MAD) is the first such
instrument and was temporarily installed and tested at the ESO/VLT in 2007. We
analyzed two globular cluster data sets in terms of achievable astrometric
precision. Data were obtained in the layer-oriented correction mode, one in
full MCAO correction mode with two layers corrected (NGC 6388) and the other
applying ground-layer correction only (47 Tuc). Aims: We aim at analyzing the
first available MCAO imaging data in the layer-oriented mode obtained with the
MAD instrument in terms of astrometric precision and stability. Methods: We
calculated Strehl maps for each frame in both data sets. Distortion corrections
were performed and the astrometric precision was analyzed by calculating mean
stellar positions over all frames and by investigation of the positional
residuals present in each frame after transformation to a
master-coordinate-frame. Results: The mean positional precision for stars
between K = 14-18 mag is ~1.2 mas in the full MCAO correction mode data of the
cluster NGC 6388. The precision measured in the GLAO data (47 Tuc) reaches ~1.0
mas for stars corresponding to 2MASS K magnitudes between 9 and 12. The
observations were such that stars in these magnitude ranges correspond to the
same detector flux range. The jitter movement used to scan a larger field of
view introduced additional distortions in the frames, leading to a degradation
of the achievable precision.Comment: 11 pages, 6 figures, accepted for publication in Astronomy &
Astrophysic
HR Del remnant anatomy using 2-D spectral data and 3-D photoionization shell models
The HR Del nova remnant was observed with the IFU-GMOS at Gemini North. The
spatially resolved spectral data cube was used in the kinematic, morphological
and abundance analysis of the ejecta. The line maps show a very clumpy shell
with two main symmetric structures. The first one is the outer part of the
shell seen in H-alpha, that forms two rings projected in the sky plane. These
ring structures correspond to a closed hourglass shape, first proposed by
Harman and O'Brien (2003). The equatorial emission enhancement is caused by the
superimposed hourglass structures in the line of sight. The second structure
seen only in the [OIII] and [NII] maps is located along the polar directions
inside the hourglass structure. Abundances gradients between the polar caps and
equatorial region were not found. However, the outer part of the shell seems to
be less abundant in Oxygen and Nitrogen than the inner regions. Detailed 2.5D
photoionization modeling of the 3D shell was performed using the mass
distribution inferred from the observations and the presence of mass clumps.
The resulting model grids are used to constrain the physical properties of the
shell as well as the central ionizing source. A sequence of 3D clumpy models
including a disk shaped ionization source is able to reproduce the ionization
gradients between polar and equatorial regions of the shell. Differences
between shell axial ratios in different lines can also be explained by
aspherical illumination. A total shell mass of 9 x 10-4 Msun is derived from
these models. We estimate that 50% to 70% of the shell mass is contained in
neutral clumps with density contrast up to a factor of 30.Comment: 31 pages 12 figures 4 tables title correcte
The Coronal Structure of AB Doradus
We perform a numerical simulation of the corona of the young, rapidly
rotating K0 dwarf AB Doradus using a global MHD model. The model is driven by a
surface map of the radial magnetic field constructed using Zeeman-Doppler
Imaging. We find that the global structure of the stellar corona is dominated
by strong azimuthal tangling of the magnetic field due to the rapid rotation.
The MHD solution enables us to calculate realistic Alfv\'en surfaces and we can
therefore estimate the stellar mass loss rate and angular momentum loss rate
without making undue theoretical simplifications. We consider three cases,
parametrized by the base density of the corona, that span the range of possible
solutions for the system. We find that overall, the mass and angular-momentum
loss rates are higher than in the solar case; the mass loss rates are 10 to 500
times higher, and the angular momentum loss rate can be up to
higher than present day solar values. Our simulations show that this model can
be use to constrain the wide parameter space of stellar systems. It also shows
that an MHD approach can provide more information about the physical system
over the commonly used potential field extrapolation.Comment: 13 pages, 7 figure
The CARMENES search for exoplanets around M dwarfs - Photospheric parameters of target stars from high-resolution spectroscopy
The new CARMENES instrument comprises two high-resolution and high-stability
spectrographs that are used to search for habitable planets around M dwarfs in
the visible and near-infrared regime via the Doppler technique. Characterising
our target sample is important for constraining the physical properties of any
planetary systems that are detected. The aim of this paper is to determine the
fundamental stellar parameters of the CARMENES M-dwarf target sample from
high-resolution spectra observed with CARMENES. We also include several M-dwarf
spectra observed with other high-resolution spectrographs, that is CAFE, FEROS,
and HRS, for completeness. We used a {chi}^2 method to derive the stellar
parameters effective temperature T_eff, surface gravity log g, and metallicity
[Fe/H] of the target stars by fitting the most recent version of the
PHOENIX-ACES models to high-resolution spectroscopic data. These stellar
atmosphere models incorporate a new equation of state to describe spectral
features of low-temperature stellar atmospheres. Since T_eff, log g, and [Fe/H]
show degeneracies, the surface gravity is determined independently using
stellar evolutionary models. We derive the stellar parameters for a total of
300 stars. The fits achieve very good agreement between the PHOENIX models and
observed spectra. We estimate that our method provides parameters with
uncertainties of {sigma} T_eff = 51 K, {sigma} log g = 0.07, and {sigma} [Fe/H]
= 0.16, and show that atmosphere models for low-mass stars have significantly
improved in the last years. Our work also provides an independent test of the
new PHOENIX-ACES models, and a comparison for other methods using
low-resolution spectra. In particular, our effective temperatures agree well
with literature values, while metallicities determined with our method exhibit
a larger spread when compared to literature results
Two Jovian planets around the giant star HD202696. A growing population of packed massive planetary pairs around massive stars?
We present evidence for a new two-planet system around the giant star
HD202696 (= HIP105056, BD+26 4118). The discovery is based on public HIRES
radial velocity measurements taken at Keck Observatory between July 2007 and
September 2014. We estimate a stellar mass of 1.91 for
HD202696, which is located close to the base of the red giant branch. A
two-planet self-consistent dynamical modeling MCMC scheme of the radial
velocity data followed by a long-term stability test suggests planetary orbital
periods of = 517.8 days and =
946.6 days, eccentricities of =
0.011 and = 0.028 , and
minimum dynamical masses of =
2.00\, and =
1.86,, respectively. Our stable MCMC
samples are consistent with orbital configurations predominantly in a mean
period ratio of 11:6 and its close-by high order mean-motion commensurabilities
with low eccentricities. For the majority of the stable configurations we find
an aligned or anti-aligned apsidal libration (i.e.\ librating
around 0 or 180), suggesting that the HD202696 system is likely
dominated by secular perturbations near the high-order 11:6 mean-motion
resonance. The HD202696 system is yet another Jovian mass pair around an
intermediate mass star with a period ratio below the 2:1 mean motion resonance.
Therefore, the HD202696 system is an important discovery, which may shed light
on the primordial disk-planet properties needed for giant planets to break the
strong 2:1 mean motion resonance and settle in more compact orbits.Comment: Accepted for publication in AJ on 18th December 2018. 15 pages, 11
Figures, 4 Tables (this .v2 is copy corrected and identical with the
published paper
Three years in the coronal life of AB Dor. I. Plasma emission measure distributions and abundances at different activity levels
The young active star AB Dor (K1 IV-V) has been observed 16 times in the last
three years with the XMM-Newton and Chandra observatories, totalling 650 ks of
high-resolution X-ray spectra. The XMM/RGS observations with the highest and
lowest average emission levels have been selected to study the coronal
properties of AB Dor in two different activity levels. We compare the results
based on the XMM data with those obtained from a higher resolution Chandra/HETG
spectrum, using the same line-based analysis technique. We have reconstructed
the plasma Emission Measure Distribution vs. temperature (EMD) in the range log
T(K) ~ 6.1-7.6, and we have determined the coronal abundances of AB Dor,
obtaining consistent results between the two instruments.The overall shape of
the EMD is also consistent with the one previously inferred from EUVE data. The
EMD shows a steep increase up to the peak at log T (K) ~ 6.9 and a substantial
amount of plasma in the range log T (K) ~ 6.9-7.3. The coronal abundances show
a clear trend of increasing depletion with respect to solar photospheric
values, for elements with increasing First Ionization Potential (FIP), down to
the Fe value ([Fe/H]=-0.57), followed by a more gradual recovery of the
photospheric values for elements with higher FIP. He-like triplets and Fe XXI
and Fe XXII lines ratios indicate electron densities log ne~10.8 cm^-3 at log
T(K) ~ 6.3 and log ne ~ 12.5 at log T(K) ~ 7, implying plasma pressures steeply
increasing with temperature. These results are interpreted in the framework of
a corona composed of different families of magnetic loop structures, shorter
than the stellar radius and in isobaric conditions, having pressures increasing
with the maximum plasma temperature, and which occupy a small fraction (f ~
10^-4 - 10^-6) of the stellar surface.Comment: Accepted by A&
Weighing The Non-Transiting Hot Jupiter Tau BOO b
We report the detection of the orbital velocity of non-transiting hot Jupiter
Tau Boo b. By employing high-resolution ground-based spectroscopy around 2.3
{\mu}m during one half night, we are able to detect carbon monoxide absorption
lines produced in the planet atmosphere, which shift significantly in
wavelength during the course of the observations due to the orbital motion of
the planet. This detection of the planetary signal results in the determination
of the orbital inclination being i = 47 (+7, -6) degrees and furthermore allow
us to solve for the exact planetary mass being mp = 5.6 (0.7) MJup. This
clearly confirms the planetary nature of the non-transiting companion to Tau
Boo.Comment: ApJ Letters, accepted; to appear on July 1st, 201
- …