162 research outputs found
Diamonds in HD 97048
We present adaptive optics high angular resolution (\sim0\farcs1)
spectroscopic observations in the 3 m region of the Herbig Ae/Be star HD
97048. For the first time, we spatially resolve the emission in the diamond
features at 3.43 and 3.53 m and in the adjacent continuum. Using both the
intensity profiles along the slit and reconstructed two-dimensional images of
the object, we derive full-width at half-maximum sizes consistent with the
predictions for a circumstellar disk seen pole-on. The diamond emission
originates in the inner region ( AU) of the disk.Comment: ApJLetter, in pres
Adaptive Optics Feedback Control
This book is a collection of 19 articles which reflect the courses given at the Collège de France/Summer school “Reconstruction d'images − Applications astrophysiques“ held in Nice and Fréjus, France, from June 18 to 22, 2012. The articles presented in this volume address emerging concepts and methods that are useful in the complex process of improving our knowledge of the celestial objects, including Earth
Photometric characterization of exoplanets using angular and spectral differential imaging
The direct detection of exoplanets has been the subject of intensive research
in the recent years. Data obtained with future high-contrast imaging
instruments optimized for giant planets direct detection are strongly limited
by the speckle noise. Specific observing strategies and data analysis methods,
such as angular and spectral differential imaging, are required to attenuate
the noise level and possibly detect the faint planet flux. Even though these
methods are very efficient at suppressing the speckles, the photometry of the
faint planets is dominated by the speckle residuals. The determination of the
effective temperature and surface gravity of the detected planets from
photometric measurements in different bands is then limited by the photometric
error on the planet flux. In this work we investigate this photometric error
and the consequences on the determination of the physical parameters of the
detected planets. We perform detailed end-to-end simulation with the CAOS-based
Software Package for SPHERE to obtain realistic data representing typical
observing sequences in Y, J, H and Ks bands with a high contrast imager. The
simulated data are used to measure the photometric accuracy as a function of
contrast for planets detected with angular and spectral+angular differential
methods. We apply this empirical accuracy to study the characterization
capabilities of a high-contrast differential imager. We show that the expected
photometric performances will allow the detection and characterization of
exoplanets down to the Jupiter mass at angular separations of 1.0" and 0.2"
respectively around high mass and low mass stars with 2 observations in
different filter pairs. We also show that the determination of the planets
physical parameters from photometric measurements in different filter pairs is
essentialy limited by the error on the determination of the surface gravity.Comment: 13 pages, 7 figures, 4 tables. Accepted for publication in MNRA
Spectroscopic evidence for strong correlations between local superconducting gap and local Altshuler-Aronov density-of-states suppression in ultrathin NbN films
Disorder has different profound effects on superconducting thin films. For a
large variety of materials, increasing disorder reduces electronic screening
which enhances electron-electron repulsion. These fermionic effects lead to a
mechanism described by Finkelstein: when disorder combined to electron-electron
interactions increases, there is a global decrease of the superconducting
energy gap and of the critical temperature , the ratio
/ remaining roughly constant. In addition, in most films an
emergent granularity develops with increasing disorder and results in the
formation of inhomogeneous superconducting puddles. These gap inhomogeneities
are usually accompanied by the development of bosonic features: a pseudogap
develops above the critical temperature and the energy gap
starts decoupling from . Thus the mechanism(s) driving the appearance of
these gap inhomogeneities could result from a complicated interplay between
fermionic and bosonic effects. By studying the local electronic properties of a
NbN film with scanning tunneling spectroscopy (STS) we show that the
inhomogeneous spatial distribution of is locally strongly correlated
to a large depletion in the local density of states (LDOS) around the Fermi
level, associated to the Altshuler-Aronov effect induced by strong electronic
interactions. By modelling quantitatively the measured LDOS suppression, we
show that the latter can be interpreted as local variations of the film
resistivity. This local change in resistivity leads to a local variation of
through a local Finkelstein mechanism. Our analysis furnishes a purely
fermionic scenario explaining quantitatively the emergent superconducting
inhomogeneities, while the precise origin of the latter remained unclear up to
now.Comment: 11 pages, 4 figure
Shadows cast on the transition disk of HD 135344B. Multiwavelength VLT/SPHERE polarimetric differential imaging
The protoplanetary disk around the F-type star HD 135344B (SAO 206462) is in
a transition stage and shows many intriguing structures both in scattered light
and thermal (sub-)millimeter emission which are possibly related to planet
formation processes. We study the morphology and surface brightness of the disk
in scattered light to gain insight into the innermost disk regions, the
formation of protoplanets, planet-disk interactions traced in the surface and
midplane layers, and the dust grain properties of the disk surface. We have
carried out high-contrast polarimetric differential imaging (PDI) observations
with VLT/SPHERE and obtained polarized scattered light images with ZIMPOL in R-
and I-band and with IRDIS in Y- and J-band. The scattered light images reveal
with unprecedented angular resolution and sensitivity the spiral arms as well
as the 25 au cavity of the disk. Multiple shadow features are discovered on the
outer disk with one shadow only being present during the second observation
epoch. A positive surface brightness gradient is observed in the stellar
irradiation corrected images in southwest direction possibly due to an
azimuthally asymmetric perturbation of the temperature and/or surface density
by the passing spiral arms. The disk integrated polarized flux, normalized to
the stellar flux, shows a positive trend towards longer wavelengths which we
attribute to large aggregate dust grains in the disk surface. Part of the the
non-azimuthal polarization signal in the Uphi image of the J-band observation
could be the result of multiple scattering in the disk. The detected shadow
features and their possible variability have the potential to provide insight
into the structure of and processes occurring in the innermost disk regions.Comment: Accepted for publication in A&A, 20 pages, 15 figure
Exoplanet characterization with long slit spectroscopy
Extrasolar planets observation and characterization by high contrast imaging
instruments is set to be a very important subject in observational astronomy.
Dedicated instruments are being developed to achieve this goal with very high
efficiency. In particular, full spectroscopic characterization of low
temperature planetary companions is an extremely important milestone. We
present a new data analysis method for long slit spectroscopy (LSS) with
coronagraphy, which allows characterization of planetary companions of low
effective temperature. In a speckle-limited regime, this method allows an
accurate estimation and subtraction of the scattered starlight, to extract a
clean spectrum of the planetary companion. We performed intensive LSS
simulations with IDL/CAOS to obtain realistic spectra of low (R=35) and medium
(R=400) resolution in the J, H, and K bands. The simulated spectra were used to
test our method and estimate its performance in terms of contrast reduction and
extracted spectra quality. Our simulations are based on a software package
dedicated to the development of SPHERE, a second generation instrument for the
ESO-VLT. Our method allows a contrast reduction of 0.5 to 2.0 magnitudes
compared to the coronagraphic observations. For M0 and G0 stars located at 10
pc, we show that it would lead to the characterization of companions with Teff
of 600 K and 900 K respectively, at angular separations of 1.0 as. We also show
that errors in the wavelength calibration can produce significant errors in the
characterization, and must therefore be minimized as much as possible.Comment: 10 pages, 12 figures, 3 tables, accepted for publication in A&
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