44 research outputs found
Photometric quality of Dome C for the winter 2008 from ASTEP South
ASTEP South is an Antarctic Search for Transiting Exo- Planets in the South
pole field, from the Concordia station, Dome C, Antarctica. The instrument
consists of a thermalized 10 cm refractor observing a fixed 3.88\degree x
3.88\degree field of view to perform photometry of several thousand stars at
visible wavelengths (700-900 nm). The first winter campaign in 2008 led to the
retrieval of nearly 1600 hours of data. We derive the fraction of photometric
nights by measuring the number of detectable stars in the field. The method is
sensitive to the presence of small cirrus clouds which are invisible to the
naked eye. The fraction of night-time for which at least 50% of the stars are
detected is 74% from June to September 2008. Most of the lost time (18.5% out
of 26%) is due to periods of bad weather conditions lasting for a few days
("white outs"). Extended periods of clear weather exist. For example, between
July 10 and August 10, 2008, the total fraction of time (day+night) for which
photometric observations were possible was 60%. This confirms the very high
quality of Dome C for nearly continuous photometric observations during the
Antarctic winter
The EMCCD-Based Speckle Interferometer of the BTA 6-m Telescope: Description and First Results
The description is given for the speckle interferometer of the BTA 6-m
telescope of the SAO RAS based on a new detector with an electron
multiplication CCD. The main components of the instrument are microscope
objectives, interference filters and atmospheric dispersion correction prisms.
The PhotonMAX-512B CCD camera using a back-illuminated CCD97 allows up to 20
speckle images (with 512512 pix resolution) per second storage on the
hard drive. Due to high quantum efficiency (93% in the maximum at 550 nm), and
high transmission of its optical elements, the new camera can be used for
diffraction-limited (0.02) image reconstruction of stars under
good seeing conditions. The main advantages of the new system over the previous
generation BTA speckle interferometer are examined.Comment: 18 pages, 14 figure
Tests with a Carlina-type diluted telescope; Primary coherencing
Studies are under way to propose a new generation of post-VLTI
interferometers. The Carlina concept studied at the Haute- Provence Observatory
is one of the proposed solutions. It consists in an optical interferometer
configured like a diluted version of the Arecibo radio telescope: above the
diluted primary mirror made of fixed cospherical segments, a helium balloon (or
cables suspended between two mountains), carries a gondola containing the focal
optics. Since 2003, we have been building a technical demonstrator of this
diluted telescope. First fringes were obtained in May 2004 with two
closely-spaced primary segments and a CCD on the focal gondola. We have been
testing the whole optical train with three primary mirrors. The main aim of
this article is to describe the metrology that we have conceived, and tested
under the helium balloon to align the primary mirrors separate by 5-10 m on the
ground with an accuracy of a few microns. The servo loop stabilizes the mirror
of metrology under the helium balloon with an accuracy better than 5 mm while
it moves horizontally by 30 cm in open loop by 10-20 km/h of wind. We have
obtained the white fringes of metrology; i.e., the three mirrors are aligned
(cospherized) with an accuracy of {\approx} 1 micron. We show data proving the
stability of fringes over 15 minutes, therefore providing evidence that the
mechanical parts are stabilized within a few microns. This is an important step
that demonstrates the feasibility of building a diluted telescope using cables
strained between cliffs or under a balloon. Carlina, like the MMT or LBT, could
be one of the first members of a new class of telescopes named diluted
telescopes.Comment: 18 pages, 17 figures, A&A, accepte
ASTEP South: An Antarctic Search for Transiting ExoPlanets around the celestial South pole
ASTEP South is the first phase of the ASTEP project (Antarctic Search for
Transiting ExoPlanets). The instrument is a fixed 10 cm refractor with a 4kx4k
CCD camera in a thermalized box, pointing continuously a 3.88 degree x 3.88
degree field of view centered on the celestial South pole. ASTEP South became
fully functional in June 2008 and obtained 1592 hours of data during the 2008
Antarctic winter. The data are of good quality but the analysis has to account
for changes in the point spread function due to rapid ground seeing variations
and instrumental effects. The pointing direction is stable within 10 arcseconds
on a daily timescale and drifts by only 34 arcseconds in 50 days. A truly
continuous photometry of bright stars is possible in June (the noon sky
background peaks at a magnitude R=15 arcsec-2 on June 22), but becomes
challenging in July (the noon sky background magnitude is R=12.5 arcsec?2 on
July 20). The weather conditions are estimated from the number of stars
detected in the field. For the 2008 winter, the statistics are between 56.3 %
and 68.4 % of excellent weather, 17.9 % to 30 % of veiled weather and 13.7 % of
bad weather. Using these results in a probabilistic analysis of transit
detection, we show that the detection efficiency of transiting exoplanets in
one given field is improved at Dome C compared to a temperate site such as La
Silla. For example we estimate that a year-long campaign of 10 cm refractor
could reach an efficiency of 69 % at Dome C versus 45 % at La Silla for
detecting 2-day period giant planets around target stars from magnitude 10 to
15. This shows the high potential of Dome C for photometry and future planet
discoveries. [Short abstract
An investigation of the close environment of beta Cep with the VEGA/CHARA interferometer
High-precision interferometric measurements of pulsating stars help to
characterize their close environment. In 1974, a close companion was discovered
around the pulsating star beta Cep using the speckle interferometry technique
and features at the limit of resolution (20 milli-arcsecond or mas) of the
instrument were mentioned that may be due to circumstellar material. Beta Cep
has a magnetic field that might be responsible for a spherical shell or
ring-like structure around the star as described by the MHD models. Using the
visible recombiner VEGA installed on the CHARA long-baseline interferometer at
Mt. Wilson, we aim to determine the angular diameter of beta Cep and resolve
its close environment with a spatial resolution up to 1 mas level. Medium
spectral resolution (R=6000) observations of beta Cep were secured with the
VEGA instrument over the years 2008 and 2009. These observations were performed
with the S1S2 (30m) and W1W2 (100m) baselines of the array. We investigated
several models to reproduce our observations. A large-scale structure of a few
mas is clearly detected around the star with a typical flux relative
contribution of 0.23 +- 0.02. Our best model is a co-rotational geometrical
thin ring around the star as predicted by magnetically-confined wind shock
models. The ring inner diameter is 8.2 +- 0.8 mas and the width is 0.6 +- 0.7
mas. The orientation of the rotation axis on the plane of the sky is PA = 60 +-
1 deg, while the best fit of the mean angular diameter of beta Cep gives UD[V]
= 0.22 +- 0.05 mas. Our data are compatible with the predicted position of the
close companion of beta Cep. These results bring additional constraints on the
fundamental parameters and on the future MHD and asteroseismological models of
the star.Comment: Paper accepted for publication in A&A (in press
The Carlina-type diluted telescope: Stellar fringes on Deneb
Context. The performance of interferometers has largely been increased over
the last ten years. But the number of observable objects is still limited due
to the low sensitivity and imaging capability of the current facilities.
Studies have been done to propose a new generation of interferometers. Aims.
The Carlina concept studied at the Haute-Provence Observatory consists in an
optical interferometer configured as a diluted version of the Arecibo radio
telescope: above the diluted primary mirror made of fixed co-spherical
segments, a helium balloon or cables suspended between two mountains and/or
pylons, carries a gondola containing the focal optics. This concept does not
require delay lines. Methods. Since 2003, we have been building a technical
demonstrator of this diluted telescope. The main goals of this project were to
find the opto-mechanical solutions to stabilize the optics attached under
cables at several tens of meters above the ground, and to characterize this
diluted telescope under real conditions. In 2012, we have obtained metrology
fringes, and co-spherized the primary mirrors within one micron accuracy. In
2013, we have tested the whole optical train: servo loop, metrology, and the
focal gondola. Results. We obtained stellar fringes on Deneb in September 2013.
In this paper, we present the characteristics of these observations: quality of
the guiding, S /N reached, and possible improvements for a future system.
Conclusions. It is an important step that demonstrates the feasibility of
building a diluted telescope using cables strained between cliffs or pylons.
Carlina, like the MMT or LBT, could be one of the first members of a new class
of telescopes named Large Diluted Telescopes. Its optical architecture has many
advantages for future projects: Planet Formation Imager, Post-ELTs,
Interferometer in space.Comment: 8 pages, 7 figures, Astronomy & Astrophysic
The structure of H2O shells in Mira atmospheres: Correlation with disk brightness distributions and a spectrophotometric signature
Dynamic models of M-type Mira variables predict the occurrence of water
"shells", i.e. of zones of high H2O density and high H2O absorption inside the
stellar atmosphere. The density, position and width of these shells is closely
correlated with different types of two-component shapes of the intensity
distribution on the disk in the H, K and L near-continuum bandpasses. We
investigate these correlations and highlight the role of a spectrophotometric
H2O index that warns against serious complications in diameter measurements in
the case of substantial water contamination of the bandpass of observation.
Simultaneous spectrophotometric and interferometric measurements may allow
observers to estimate real continuum diameters more precisely.Comment: Accepted for publication in A &
Speckle Interferometry of Nearby Multiple Stars. IV. Measurements in 2004 and New Orbits
The results of speckle interferometric observations of 104 binary and 6
triple stars performed at the BTA 6 m telescope in 2004 October are presented.
Nearby low-mass stars are mostly observed for the program, among which 59 there
are new binaries recently discovered by the Hipparcos astrometric satellite.
Concurrently with the diffraction-limited position measurements we obtained 154
brightness ratio measurements of binary and multiple star components in
different bands of the visible spectrum. New, first-resolved binaries are the
symbiotic star CH Cyg with a weak companion at 0.043'' separation and the pair
of red dwarfs, GJ 913 = HIP 118212. In addition, we derived the orbital
parameters for two interferometric systems: the CN-giant pair HD 210211 = HIP
109281 (P=10.7 yr) and the G2V-K2V binary GJ 9830 = HIP 116259 (P=15.7 yr).Comment: 11 pages, 2 figures, accepted to Astrophysical Bulleti