298 research outputs found
Interpreting the photometry and spectroscopy of directly imaged planets: a new atmospheric model applied to beta Pictoris b and SPHERE observations
We aim to interpret future photometric and spectral measurements from these
instruments, in terms of physical parameters of the planets, with an
atmospheric model using a minimal number of assumptions and parameters.
We developed Exoplanet Radiative-convective Equilibrium Model (Exo-REM) to
analyze the photometric and spectro- scopic data of directly imaged planets.
The input parameters are a planet's surface gravity (g), effective temperature
(Teff ), and elemental composition. The model predicts the equilibrium
temperature profile and mixing ratio profiles of the most important gases.
Opacity sources include the H2-He collision-induced absorption and molecular
lines from eight compounds (including CH4 updated with the Exomol line list).
Absorption by iron and silicate cloud particles is added above the expected
condensation levels with a fixed scale height and a given optical depth at some
reference wavelength. Scattering was not included at this stage.
We applied Exo-REM to photometric and spectral observations of the planet
beta Pictoris b obtained in a series of near-IR filters. We derived Teff = 1550
+- 150 K, log(g) = 3.5 +- 1, and radius R = 1.76 +- 0.24 RJup (2-{\sigma} error
bars from photometric measurements). These values are comparable to those found
in the literature, although with more conservative error bars, consistent with
the model accuracy. We were able to reproduce, within error bars, the J- and
H-band spectra of beta Pictoris b. We finally investigated the precision to
which the above parameterComment: 15 pages, 14 figures, accepted by A&
Titan's atmosphere as observed by Cassini/VIMS solar occultations: CH, CO and evidence for CH absorption
We present an analysis of the VIMS solar occultations dataset, which allows
us to extract vertically resolved information on the characteristics of Titan's
atmosphere between 100-700 km with a characteristic vertical resolution of 10
km. After a series of data treatment procedures, 4 occultations out of 10 are
retained. This sample covers different seasons and latitudes of Titan. The
transmittances show clearly the evolution of the haze and detect the detached
layer at 310 km in Sept. 2011 at mid-northern latitudes. Through the inversion
of the transmission spectra with a line-by-line radiative transfer code we
retrieve the vertical distribution of CH and CO mixing ratio. The two
methane bands at 1.4 and 1.7 {\mu}m are always in good agreement and yield an
average stratospheric abundance of %. This is significantly less
than the value of 1.48% obtained by the GCMS/Huygens instrument. The analysis
of the residual spectra after the inversion shows that there are additional
absorptions which affect a great part of the VIMS wavelength range. We
attribute many of these additional bands to gaseous ethane, whose near-infrared
spectrum is not well modeled yet. Ethane contributes significantly to the
strong absorption between 3.2-3.5 {\mu}m that was previously attributed only to
C-H stretching bands from aerosols. Ethane bands may affect the surface windows
too, especially at 2.7 {\mu}m. Other residual bands are generated by stretching
modes of C-H, C-C and C-N bonds. In addition to the C-H stretch from aliphatic
hydrocarbons at 3.4 {\mu}m, we detect a strong and narrow absorption at 3.28
{\mu}m which we tentatively attribute to the presence of PAHs in the
stratosphere. C-C and C-N stretching bands are possibly present between 4.3-4.5
{\mu}m. Finally, we obtain the CO mixing ratio between 70-170 km. The average
result of ppm is in good agreement with previous studies.Comment: 51 pages, 28 figure
Simulated performance of the molecular mapping for young giant exoplanets with the Medium Resolution Spectrometer of JWST/MIRI
Young giant planets are the best targets for characterization with direct
imaging. The Medium Resolution Spectrometer (MRS) of the Mid-Infrared
Instrument (MIRI) of the recently launched James Webb Space Telescope (JWST)
will give access to the first spectroscopic data for direct imaging above 5
m with unprecedented sensitivity at a spectral resolution up to 3700. This
will provide a valuable complement to near-infrared data from ground-based
instruments for characterizing these objects. We aim to evaluate the
performance of MIRI/MRS to detect molecules in the atmosphere of exoplanets and
to constrain atmospheric parameters using Exo-REM atmospheric models. The
molecular mapping technique, based on cross-correlation with synthetic models,
has been introduced recently. This promising detection and characterization
method is tested on simulated MIRI/MRS data. Directly imaged planets can be
detected with MIRI/MRS, and we are able to detect molecules (HO, CO,
NH, CH, HCN, PH, CO) at various angular separation depending on
the strength of the molecular features and brightness of the target. We find
that the stellar spectral type has a weak impact on the detection level. This
method is globally most efficient for planets with temperatures below 1500 K,
for bright targets and angular separation greater than 1. Our parametric
study allows us to anticipate the ability to characterize planets that would be
detected in the future. The MIRI/MRS will give access to molecular species not
yet detected in exoplanetary atmospheres. The detection of molecules as
indicators of the temperature of the planets will make it possible to
discriminate between the various hypotheses of the preceding studies, and the
derived molecular abundance ratios should bring new constraints on planetary
formation scenarios.Comment: 25 pages, 13 figure
New laboratory measurements of CH4 in Titan's conditions and a reanalysis of the DISR near-surface spectra at the Huygens landing site
International audienceLaboratory spectra of methane-nitrogen mixtures have been recorded in the near-infrared range (1.0 - 1.65 µm) in conditions similar to Titan's near surface, to facilitate the interpretation of the DISR/DLIS spectra taken during the last phase of the descent of the Huygens Probe, when the surface was illuminated by a surface science lamp. We used a 0.03 cm-1 spectral resolution, adequate to resolve the lines at high pressure (pN2 ~ 1.5 bar). By comparing the laboratory spectra with synthetic calculations in the well-studied ν2 + 2ν3 band (7515-7620 cm-1), we determine a methane absorption column density of 178±20 cm-am and a temperature of 118±10 K in our experiment. From this, we derive the methane absorption coefficients over 1.0-1.65 µm with a 0.03 cm-1 sampling, allowing for the extrapolation of the results to any other methane column density under the relevant pressure and temperature conditions. We then revisit the calibration and analysis of the Titan "lamp-on" DLIS spectra. We infer a 5.1±0.8 % methane mixing ratio in the first 25 m of Titan's atmosphere. The CH4 mixing ratio measured 90 sec after landing from a distance of 45 cm is found to be 0.92±0.25 times this value, thus showing no post-landing outgassing of methane in excess of ̴ 20 %. Finally, we determine the surface reflectivity as seen from 25 m and 45 cm and find that the 1500 nm absorption band is deeper in the post-landing spectrum as compared to pre-landing
Upper limits for undetected trace species in the stratosphere of Titan
In this paper we describe a first quantitative search for several molecules
in Titan's stratosphere in Cassini CIRS infrared spectra. These are: ammonia
(NH3), methanol (CH3OH), formaldehyde (H2CO), and acetonitrile (CH3CN), all of
which are predicted by photochemical models but only the last of which
observed, and not in the infrared. We find non-detections in all cases, but
derive upper limits on the abundances from low-noise observations at 25{\deg}S
and 75{\deg}N. Comparing these constraints to model predictions, we conclude
that CIRS is highly unlikely to see NH3 or CH3OH emissions. However, CH3CN and
H2CO are closer to CIRS detectability, and we suggest ways in which the
sensitivity threshold may be lowered towards this goal.Comment: 11 pages plus 6 figure file
Deuterium chemistry in protoplanetary disks II The inner 30 AU
We present the results of models of the chemistry, including deuterium, in
the inner regions of protostellar disks. We find good agreement with recent gas
phase observations of several (non--deuterated) species. We also compare our
results with observations of comets and find that in the absence of other
processing e.g. in the accretion shock at the surface of the disk, or by mixing
in the disk, the calculated D/H ratios in ices are higher than measured and
reflect the D/H ratio set in the molecular cloud phase. Our models give quite
different abundances and molecular distributions to other inner disk models
because of the differences in physical conditions in the model disk. This
emphasizes how changes in the assumptions about the density and temperature
distribution can radically affect the results of chemical models.Comment: Accepted by Astrophysical Journa
Titan's Prolific Propane: The Cassini CIRS Perspective
In this paper we select large spectral averages of data from the Cassini
Composite Infrared Spectrometer (CIRS) obtained in limb-viewing mode at low
latitudes (30S--30N), greatly increasing the path length and hence
signal-to-noise ratio for optically thin trace species such as propane. By
modeling and subtracting the emissions of other gas species, we demonstrate
that at least six infrared bands of propane are detected by CIRS, including two
not previously identified in Titan spectra. Using a new line list for the range
1300-1400cm -1, along with an existing GEISA list, we retrieve propane
abundances from two bands at 748 and 1376 cm-1. At 748 cm-1 we retrieve 4.2 +/-
0.5 x 10(-7) (1-sigma error) at 2 mbar, in good agreement with previous
studies, although lack of hotbands in the present spectral atlas remains a
problem. We also determine 5.7 +/- 0.8 x 10(-7) at 2 mbar from the 1376 cm-1
band - a value that is probably affected by systematic errors including
continuum gradients due to haze and also an imperfect model of the n6 band of
ethane. This study clearly shows for the first time the ubiquity of propane's
emission bands across the thermal infrared spectrum of Titan, and points to an
urgent need for further laboratory spectroscopy work, both to provide the line
positions and intensities needed to model these bands, and also to further
characterize haze spectral opacity. The present lack of accurate modeling
capability for propane is an impediment not only for the measurement of propane
itself, but also for the search for the emissions of new molecules in many
spectral regions.Comment: 7 Figures, 3 Tables. Typeset in Latex with elsart.cls. In press for
Planetary and Space Scienc
Evidence for carbonyl sulfide (OCS) conversion to CO in the lower atmosphere of Venus
The chemical regimes in the atmosphere of Venus vary from photochemistry in the middle atmosphere to thermal equilibrium chemistry in the lower atmosphere and the surface. Many chemical cycles have been proposed, but few details about these cycles are fully verified by comparison between observations and modeling. Recent high-quality data of carbonyl sulfide (OCS) and CO from ground-based and Venus Express observations provide a unique opportunity to test our understanding of chemistry and transport in the lower atmosphere of Venus. The spatial distributions of OCS and CO in the atmosphere reflect a sensitive balance between chemistry and transport. On the basis of our updated photochemical model and winds from Lee et al.'s (2007) general circulation model, we study the chemistry and transport in a simplified two-dimensional chemistry-transport model. OCS is produced by heterogeneous reactions on the surface; the middle atmosphere is a net sink for OCS. The combination of data and modeling provides strong evidence for the loss of OCS by conversion to CO. The detailed chemical mechanism is currently unknown, although a number of speculations have been proposed. The sensitivity of the distributions of OCS and CO to model parameters is reported
Excitation energies, photoionization cross sections, and asymmetry parameters of the methyl and silyl radicals
NEDA—NEutron Detector Array
The NEutron Detector Array, NEDA, will form the next generation neutron detection system that has been designed to be operated in conjunction with γ-ray arrays, such as the tracking-array AGATA, to aid nuclear spectroscopy studies. NEDA has been designed to be a versatile device, with high-detection efficiency, excellent neutron-γ discrimination, and high rate capabilities. It will be employed in physics campaigns in order to maximise the scientific output, making use of the different stable and radioactive ion beams available in Europe. The first implementation of the neutron detector array NEDA with AGATA 1π was realised at GANIL. This manuscript reviews the various aspects of NEDA
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