105 research outputs found
Coupling MOAO with Integral Field Spectroscopy: specifications for the VLT and the E-ELT
[Abridged] We have developed an end-to-end simulation to specify the science
requirements of a MOAO-fed integral field spectrograph on either an 8m or 42m
telescope. Our simulations re-scales observations of local galaxies or results
from numerical simulations of disk or interacting galaxies. For the current
analysis, we limit ourselves to a local disk galaxy which exhibits simple
rotation and a simulation of a merger. We have attempted to generalize our
results by introducing the simple concepts of "PSF contrast" which is the
amount of light polluting adjacent spectra which we find drives the smallest EE
at a given spatial scale. The choice of the spatial sampling is driven by the
"scale-coupling", i.e., the relationship between the IFU pixel scale and the
size of the features that need to be recovered by 3D spectroscopy in order to
understand the nature of the galaxy and its substructure. Because the dynamical
nature of galaxies are mostly reflected in their large-scale motions, a
relatively coarse spatial resolution is enough to distinguish between a
rotating disk and a major merger. Although we used a limited number of
morpho-kinematic cases, our simulations suggest that, on a 42m telescope, the
choice of an IFU pixel scale of 50-75 mas seems to be sufficient. Such a coarse
sampling has the benefit of lowering the exposure time to reach a specific
signal-to-noise as well as relaxing the performance of the MOAO system. On the
other hand, recovering the full 2D-kinematics of z~4 galaxies requires high
signal-to-noise and at least an EE of 34% in 150 mas (2 pixels of 75 mas).
Finally, we carried out a similar study at z=1.6 with a MOAO-fed spectrograph
for an 8m, and find that at least an EE of 30% at 0.25 arcsec spatial sampling
is required to understand the nature of disks and mergers.Comment: 17 pages, 20 figures, accepted for publication in the MNRA
A search for circumstellar dust disks with ADONIS
We present results of a coronographic imaging search for circumstellar dust
disks with the Adaptive Optics Near Infrared System (ADONIS) at the ESO 3.6m
telescope in La Silla (Chile). 22 candidate stars, known to be orbited by a
planet or to show infrared excess radiation, were examined for circumstellar
material. In the PSF-subtracted images no clear disk was found. We further
determine the detection sensitivities and outline how remaining atmospheric
fluctuations still can hamper adaptive optics observations.Comment: To appear in A&A, in pres
High-contrast Imaging Study on the Candidate Companions Around the Star AH Lep
AH Lep (R.A._(J2000) = 05 34 09.16, decl._(J2000) = −15 17 03.18) is a young, nearby, solar-type star (G2V). Gaia DR2 and BANYAN Sigma provide a 99.9% probability of the star belonging to the Columba moving group (Zuckerman et al. 2011), yielding an estimated age of 42^(+6)_(-4) Myr (Bell et al. 2015). It has a parallax of p = 17.26 mas, corresponding to a distance of d = 57.9 pc (Gaia Collaboration et al. 2018). The star has been reported to have variable photospheric and X-ray emission (e.g., Burleigh et al. 1998; Cutispoto et al. 2003)
Vision Suisse de la Bretagne chez Cambry.
ISBN : 978-2-901737-80-3 ; 231 p.International audienceUne vingtaine de fois dans son fameux Voyage, Cambry rapproche les paysages du Finistère de ceux de la Suisse. Dans la plupart des cas, ces comparaisons tournent à l'avantage de son département breton. Une telle fréquence, renforcée par une certaine constance de l'interprétation, ne sautait être fortuite. Aussi conviendra-t-il, après avoir examiné ces références, de trouver une signification qui pourrait faire de Cambry, le premier révélateur d'une Bretagne élue d'un celtisme en quête d'identité topographique
Orbital Dynamics of Multi-Planet Systems with Eccentricity Diversity
Since exoplanets were detected using the radial velocity method, they have
revealed a diverse distribution of orbital configurations. Amongst these are
planets in highly eccentric orbits (e > 0.5). Most of these systems consist of
a single planet but several have been found to also contain a longer period
planet in a near-circular orbit. Here we use the latest Keplerian orbital
solutions to investigate four known systems which exhibit this extreme
eccentricity diversity; HD 37605, HD 74156, HD 163607, and HD 168443. We place
limits on the presence of additional planets in these systems based on the
radial velocity residuals. We show that the two known planets in each system
exchange angular momentum through secular oscillations of their eccentricities.
We calculate the amplitude and timescale for these eccentricity oscillations
and associated periastron precession. We further demonstrate the effect of
mutual orbital inclinations on the amplitude of high-frequency eccentricity
oscillations. Finally, we discuss the implications of these oscillations in the
context of possible origin scenarios for unequal eccentricities.Comment: 12 pages, 9 figures, accepted for publication in the Astrophysical
Journa
Laboratory comparison of coronagraphic concepts under dynamical seeing and high-order adaptive optics correction
The exoplanetary science through direct imaging and spectroscopy will largely
expand with the forthcoming development of new instruments at the VLT (SPHERE),
Gemini (GPI), Subaru (HiCIAO), and Palomar (Project 1640) observatories. All
these ground-based adaptive optics instruments combine extremely high
performance adaptive optics (XAO) systems correcting for the atmospheric
turbulence with advanced starlight-cancellation techniques such as coronagraphy
to deliver contrast ratios of about 10-6 to 10-7. While the past fifteen years
have seen intensive research and the development of high-contrast coronagraph
concepts, very few concepts have been tested under dynamical seeing conditions
(either during sky observation or in a realistic laboratory environment). In
this paper, we discuss the results obtained with four different coronagraphs --
phase and amplitude types -- on the High-Order Testbench (HOT), the adaptive
optics facility developed at ESO. This facility emphasizes realistic conditions
encountered at a telescope (e.g., VLT), including a turbulence generator and a
high-order adaptive optics system. It enables to evaluate the performance of
high-contrast coronagraphs in the near-IR operating with an AO-corrected PSF of
90% Strehl ratio under 0.5 arcsec dynamical seeing.Comment: Accepted for publication in MNRA
CASE REPORT - Reactivated toxoplasmosis presenting with non-tender hepatomegaly in a patient with HIV infection
No Abstract African Journal of Health Sciences Vol. 14 (1-2) 2007: pp. 97-9
On the Origin of the Eccentricities of Extrasolar Planets
We develop a phenomenological theory that aims to account for the origin of
the large eccentricities of extrasolar planets and that of the small
eccentricities in the solar system, the preference for apsidal alignment in
non-resonant multiplanet systems, and the origin of the similarities in the
eccentricity distribution of extra-solar planets and that of spectroscopic
binary stars. We show that if a physical process is weakly dependent on the
local dynamics of the companion and imparts a small relative acceleration to
the star-companion system, the eccentricity of the companion's orbit is excited
to large values depending on the direction and duration of acceleration. A
natural candidate for such processes are asymmetric stellar jets and star-disk
winds. When the acceleration originates from a precessing jet, large
eccentricities can be excited by the resonance of the jet's precession
frequency with the induced acceleration's excitation frequency even for nearly
perpendicular jets. Precession also reduces the eccentricity amplitude far
inside the resonance radius. The acceleration's strength is best constrained in
multiplanet systems because of the companions' mutual gravitational
perturbations, while the acceleration's duration is bounded by the condition
that the residual velocity imparted to the star is smaller than the stellar
velocity dispersion in the Galaxy. In the outer parts of the star-companion
system where the acceleration excitation time is comparable to or smaller than
the orbital period, significant radial migration takes place which may have
important consequences for the dynamics of the minor body populations in the
solar system. The theory is illustrated with the Andromedae binary
system.Comment: 41 pages, 14 figures, accepted for publication in the Astronomical
Journa
Telescope interferometers: an alternative to classical wavefront sensors
Several types of Wavefront Sensors (WFS) are nowadays available in the field
of Adaptive Optics (AO). Generally speaking, their basic principle consists in
measuring slopes or curvatures of Wavefront Errors (WFE) transmitted by a
telescope, subsequently reconstructing WFEs digitally. Such process, however,
does not seem to be well suited for evaluating co-phasing or piston errors of
future large segmented telescopes in quasi real-time. This communication
presents an original, recently proposed technique for direct WFE sensing. The
principle of the device, which is named "Telescope-Interferometer" (TI), is
based on the addition of a reference optical arm into the telescope pupil
plane. Then incident WFEs are deduced from Point Spread Function (PSF)
measurements at the telescope focal plane. Herein are described two different
types of TIs, and their performance are discussed in terms of intrinsic
measurement accuracy and spatial resolution. Various error sources are studied
by means of numerical simulations, among which photon noise sounds the most
critical. Those computations finally help to define the application range of
the TI method in an AO regime, including main and auxiliary telescope diameters
and magnitude of the guide star. Some practical examples of optical
configurations are also described and commented.Comment: 12 pages, 10 figure
- …