16 research outputs found
Characterizing Exoplanets in the Visible and Infrared: A Spectrometer Concept for the EChO Space Mission
Transit-spectroscopy of exoplanets is one of the key observational techniques
to characterize the extrasolar planet and its atmosphere. The observational
challenges of these measurements require dedicated instrumentation and only the
space environment allows an undisturbed access to earth-like atmospheric
features such as water or carbon-dioxide. Therefore, several exoplanet-specific
space missions are currently being studied. One of them is EChO, the Exoplanet
Characterization Observatory, which is part of ESA's Cosmic Vision 2015-2025
program, and which is one of four candidates for the M3 launch slot in 2024. In
this paper we present the results of our assessment study of the EChO
spectrometer, the only science instrument onboard this spacecraft. The
instrument is a multi-channel all-reflective dispersive spectrometer, covering
the wavelength range from 400 nm to 16 microns simultaneously with a moderately
low spectral resolution. We illustrate how the key technical challenge of the
EChO mission - the high photometric stability - influences the choice of
spectrometer concept and drives fundamentally the instrument design. First
performance evaluations underline the fitness of the elaborated design solution
for the needs of the EChO mission.Comment: 20 pages, 8 figures, accepted for publication in the Journal of
Astronomical Instrumentatio
CHEOPS: a space telescope for ultra-high precision photometry of exoplanet transits
The CHaracterising ExOPlanet Satellite (CHEOPS) is a joint ESA-Switzerland space mission dedicated to search for exoplanet transits by means of ultra-high precision photometry whose launch readiness is expected end 2017. The CHEOPS instrument will be the first space telescope dedicated to search for transits on bright stars already known to host planets. By being able to point at nearly any location on the sky, it will provide the unique capability of determining accurate radii for a subset of those planets for which the mass has already been estimated from ground-based spectroscopic surveys. CHEOPS will also provide precision radii for new planets discovered by the next generation ground-based transits surveys (Neptune-size and smaller). The main science goals of the CHEOPS mission will be to study the structure of exoplanets with radii typically ranging from 1 to 6 Earth radii orbiting bright stars. With an accurate knowledge of masses and radii for an unprecedented sample of planets, CHEOPS will set new constraints on the structure and hence on the formation and evolution of planets in this mass range. To reach its goals CHEOPS will measure photometric signals with a precision of 20 ppm in 6 hours of integration time for a 9th magnitude star. This corresponds to a signal to noise of 5 for a transit of an Earth-sized planet orbiting a solar-sized star (0.9 solar radii). This precision will be achieved by using a single frame-transfer backside illuminated CCD detector cool down at 233K and stabilized within {10 mK . The CHEOPS optical design is based on a Ritchey-Chretien style telescope with 300 mm effective aperture diameter, which provides a defocussed image of the target star while minimizing straylight using a dedicated field stop and baffle system. As CHEOPS will be in a LEO orbit, straylight suppression is a key point to allow the observation of faint stars. The telescope will be the only payload on a spacecraft platform providing pointing stability of < 8 arcsec rms, power of 60W for instrument operations and downlink transmission of at least 1.2GBit/day. Both CHEOPS paylaod and platform will rely mainly on components with flight heritage. The baseline CHEOPS mission fits within the technical readiness requirements, short development time and the cost envelope defined by ESA in its first call for S-missions. It represents a breakthrough opportunity in furthering our understanding of the formation and evolution of planetary systems
The CHEOPS (characterising exoplanet satellite) mission: telescope optical design, development status and main technical and programmatic challenges
CHEOPS (CHaracterising ExOPlanet Satellite) is the first ESA Small Mission as part of the ESA Cosmic Vision program 2015-2025 and it is planned launch readiness end of 2017. The mission lead is performed in a partnership between Switzerland, led by the University of Bern, and the European Space Agency with important contributions from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The CHEOPS mission will be the first space telescope dedicated to search for exoplanetary transits on bright stars already known to host planets by performing ultrahigh precision photometry on bright starts whose mass has been already estimated through spectroscopic surveys on ground based observations. The number of exoplanets in the mass range 1-30 MEarth for which both mass and radius are known with a good precision is extremely limited also considering the last two decades of high-precision radial velocity measurement campaigns and the highly successful space missions dedicated to exoplanets transit searches (CoRoT and Kepler)
Transiting exoplanets from the CoRoT space mission. VIII. CoRoT-7b: the first super-Earth with measured radius
Copyright © The European Southern Observatory (ESO)Aims. We report the discovery of very shallow (ΔF/F ≈ 3.4×10−4), periodic dips in the light curve of an active V = 11.7 G9V star observed by the CoRoT satellite, which we interpret as caused by a transiting companion. We describe the 3-colour CoRoT data and complementary ground-based observations that support the planetary nature of the companion.
Methods. We used CoRoT colours information, good angular resolution ground-based photometric observations in- and out- of transit, adaptive optics imaging, near-infrared spectroscopy, and preliminary results from radial velocity measurements, to test the diluted eclipsing binary scenarios.
The parameters of the host star were derived from optical spectra, which were then combined with the CoRoT light curve to derive parameters of the companion.
Results. We examined all conceivable cases of false positives carefully, and all the tests support the planetary hypothesis. Blends with separation >0.40'' or triple systems are almost excluded with a 8 × 10−4 risk left. We conclude that, inasmuch we have been exhaustive, we have discovered a planetary companion, named CoRoT-7b, for which we derive a period of 0.853 59 ± 3 × 10−5 day and a radius of Rp = 1.68 ± 0.09 REarth. Analysis of preliminary radial velocity data yields an upper limit of 21 MEarth for the companion mass, supporting the finding.
Conclusions. CoRoT-7b is very likely the first Super-Earth with a measured radius. This object illustrates what will probably become a common situation with missions such as Kepler, namely the need to establish the planetary origin of transits in the absence of a firm radial velocity detection and mass measurement. The composition of CoRoT-7b remains loosely constrained without a precise mass. A very high surface temperature on its irradiated face, ≈1800–2600 K at the substellar point, and a very low one, ≈50 K, on its dark face assuming no atmosphere, have been derived
The Herschel-PACS grating mechanism: mechanical and optical performance
The Photodetector Array Camera and Spectrometer (PACS), on board the Herschel Space Observatory, is designed for imaging and low and medium resolution spectroscopy in the wavelength region between 57 and 210 μm. This paper reports the design and the testing results of the grating cryogenic mechanism of the PACS spectrometer. The PACS diffraction grating is made from an aluminium substrate, mechanically ruled with a periodicity of 8.5 grooves per mm and gold coated for optimum reflectivity at PACS operating wavelengths. The grating mechanism is capable of accurate positioning (4") of the flat diffraction grating within a large angular throw (44°) in cryogenic environment (4.2 K). Technologies of actuators, position sensors, bearings, servo-control and cryogenic test set-up are presented. The grating mechanism was thoroughly tested, alone and when integrated in the PACS Focal Plane Unit (FPU). The tests were performed in cryogenic conditions, in a set-up fully representative of the flight conditions. Actual mechanical and optical performance obtained with the Flight Model (FM) is presented in detail. Quality of the angular positioning of the mechanism, spectral resolution and optical quality of the grating are analysed.status: publishe
New applications of rapid prototyping and rapid manufacturing (RP/RM) technologies for space instrumentation
In the frame of a research project, CRIF, KUL and CSL have investigated the possibility to use rapid prototyping and rapid manufacturing (RP/RM) techniques during space instrument development. Rapid prototyping and rapid manufacturing terms gather several techniques with the common baseline that parts are built layer by layer, starting from a CAD model. These techniques imply powder, paste or liquid and are applicable to polymers, ceramics and metals. In a first step, the major advantages of these techniques have been presented to Belgian industries implied in the space sector and, as a result of the discussions, development goals for the project have been identified. Several types of use have also been pointed, from demonstration mock-up to real space hardware. In parallel to technical developments, several case studies and tests have been performed. The case studies have shown that the rapid manufacturing allows complex geometries to be created. A drastic decrease of the number of separate parts and bolted junctions ease the predictability of the mechanical and thermal behaviour and limit the risk of imperfect junction. As a result of the project, a guidelines document has been issued to give as much information as possible on how to perform a space instrument design using the advantages of RP/RM techniques
Optical design of the Optical Monitoring Camera (OMC) of INTEGRAL
The Optical Monitoring Camera (OMC) will observe the optical
emission from the main targets of the gamma-ray instruments onboard the ESA
mission INTEGRAL. The OMC is based on a refractive optics with an aperture
of 50 mm focused onto a large format CCD ( pixels), and a
field of view of 5\degr\times5\degr. This paper describes the design of the
optical system and the optical baffles of the OMC.
CHEOPS: A SPACE TELESCOPE FOR ULTRA-HIGH PRECISION PHOTOMETRY OF EXOPLANET TRANSITS
The CHaracterising ExOPlanet Satellite (CHEOPS) is a joint ESA-Switzerland space mission dedicated to
search for exoplanet transits by means of ultra-high precision photometry whose launch readiness is expected
end 2017. The CHEOPS instrument will be the first space telescope dedicated to search for transits on bright
stars already known to host planets. By being able to point at nearly any location on the sky, it will provide the
unique capability of determining accurate radii for a subset of those planets for which the mass has already been
estimated from ground-based spectroscopic surveys. CHEOPS will also provide precision radii for new planets
discovered by the next generation ground-based transits surveys (Neptune-size and smaller). The main science
goals of the CHEOPS mission will be to study the structure of exoplanets with radii typically ranging from 1 to
6 Earth radii orbiting bright stars. With an accurate knowledge of masses and radii for an unprecedented sample
of planets, CHEOPS will set new constraints on the structure and hence on the formation and evolution of
planets in this mass range. To reach its goals CHEOPS will measure photometric signals with a precision of 20
ppm in 6 hours of integration time for a 9th magnitude star. This corresponds to a signal to noise of 5 for a
transit of an Earth-sized planet orbiting a solar-sized star (0.9 solar radii). This precision will be achieved by
using a single frame-transfer backside illuminated CCD detector cool down at 233K and stabilized within ~10
mK . The CHEOPS optical design is based on a Ritchey-Chretien style telescope with 300 mm effective
aperture diameter, which provides a defocussed image of the target star while minimizing straylight using a
dedicated field stop and baffle system. As CHEOPS will be in a LEO orbit, straylight suppression is a key point
to allow the observation of faint stars. The telescope will be the only payload on a spacecraft platform providing
pointing stability of < 8 arcsec rms, power of 60W for instrument operations and downlink transmission of at
least 1.2GBit/day. Both CHEOPS paylaod and platform will rely mainly on components with flight heritage.
The baseline CHEOPS mission fits within the technical readiness requirements, short development time and the
cost envelope defined by ESA in its first call for S-missions. It represents a breakthrough opportunity in
furthering our understanding of the formation and evolution of planetary systems
OMC: An Optical Monitoring Camera for INTEGRAL - Instrument description and performance
The Optical Monitoring Camera (OMC) will observe the optical emission from the prime targets of the gammaray instruments onboard the ESA mission INTEGRAL, with the support of the JEM-X monitor in the X-ray domain. This capability will provide invaluable diagnostic information on the nature and the physics of the sources over a broad wavelength range. Its main scientific objectives are: ( 1) to monitor the optical emission from the sources observed by the gamma- and X-ray instruments, measuring the time and intensity structure of the optical emission for comparison with variability at high energies, and ( 2) to provide the brightness and position of the optical counterpart of any gamma- or X-ray transient taking place within its field of view. The OMC is based on a refractive optics with an aperture of 50 mm focused onto a large format CCD (1024 x 2048 pixels) working in frame transfer mode (1024 x 1024 pixels imaging area). With a field of view of 5degrees x 5degrees it will be able to monitor sources down to magnitude V = 18. Typical observations will perform a sequence of different integration times, allowing for photometric uncertainties below 0.1 mag for objects with V less than or equal to 16