References of "Absil, Olivier"
     in
Bookmark and Share    
See detailInfrared Interferometric Gravity Darkening Observations of Vega with CHARA/FLUOR
Aufdenberg, J.; Mérand, A.; Coudé Du Foresto, V. et al

in Coudé du Foresto, Vincent; Rouan, Daniel; Rousset, Gérard (Eds.) Visions for Infrared Astronomy (2006, March)

We have obtained high-precision measurements of Vega at projected baselines between 103 m and 273 m with the CHARA Array using the (FLUOR) beam combiner in the K' band. A strongly gravity-darkened model ... [more ▼]

We have obtained high-precision measurements of Vega at projected baselines between 103 m and 273 m with the CHARA Array using the (FLUOR) beam combiner in the K' band. A strongly gravity-darkened model atmosphere is in general agreement with both our interferometric data and archival spectrophotometry. This model indicates that Vega is rotating at 91%ofitsangular break-uprateandthatthepole-to-equator effectivetemperaturedifference is 2250 K. [less ▲]

Detailed reference viewed: 8 (0 ULg)
Full Text
Peer Reviewed
See detailInstrumental stability requirements for exoplanet detection with a nulling interferometer: variability noise as a central issue
Chazelas, Bruno; Brachet, Frank; Bordé, Pascal et al

in Applied Optics (2006), 45

We revisit the nulling interferometer performances that are needed for direct detection and the spectroscopic analysis of exoplanets, e.g., with the DARWIN [European Space Agency-SCI 12 (2000)] or TPF-I ... [more ▼]

We revisit the nulling interferometer performances that are needed for direct detection and the spectroscopic analysis of exoplanets, e.g., with the DARWIN [European Space Agency-SCI 12 (2000)] or TPF-I [JPL Publ. 05-5, (2005)] missions. Two types of requirement are found, one concerning the mean value of the instrumental nulling function <nl(lambda)> and another regarding its stability. The stress is usually put on the former. It is stringent at short wavelengths but somewhat relaxed at longer wavelengths. The latter, which we call the variability noise condition, does not usually receive enough attention. It is required regardless of telescope size and stellar distance. The results from three nulling experiments performed in laboratories around the world are reported and compared with the requirements. All three exhibit 1/f noise that is incompatible with the performances required by the mission. As pointed out by Lay [Appl. Opt. 43, 6100-6123 (2004)], this stability problem is not fully solved by modulation techniques. Adequate solutions must be found that are likely to include servo systems using the stellar signal itself as a reference and internal metrology with high stability. [less ▲]

Detailed reference viewed: 12 (1 ULg)
Full Text
See detailThe prospects of detecting exo-planets with the Ground-based European Nulling Interferometer Experiment (GENIE)
den Hartog, R.; Absil, Olivier ULg; Gondoin, P. et al

in Aime, C.; Vakili, F. (Eds.) Direct Imaging of Exoplanets: Science & Techniques (2006)

The European Space Agency's Darwin and NASA's Terrestrial Planet Finder (TPF) are among the most challenging space science missions ever considered. Their principal objective is to detect Earth-like ... [more ▼]

The European Space Agency's Darwin and NASA's Terrestrial Planet Finder (TPF) are among the most challenging space science missions ever considered. Their principal objective is to detect Earth-like planets around nearby stars and to characterize their atmospheres. Darwin and TPF-I are currently conceived as nulling interferometers with free-flying telescopes. Within the frame of the Darwin program, the ESA and the European Southern Observatory (ESO), supported by European industries and scientific institutes, have performed two parallel Phase A studies of a ground-based nulling interferometry experiment (GENIE) at the site of ESO's Very Large Telescope Interferometer (VLTI) in Paranal, Chile. GENIE will demonstrate several key technologies required for the Darwin mission. Its science objectives include the detection and characterization of dust disks and low-mass companions around nearby stars. These studies have established detailed instrumental designs, in which GENIE will operate in the L' band around 3.8 microns as a single Bracewell nulling or constructive interferometer, using either two Auxiliary or two Unit Telescopes. The studies were supported by detailed numerical simulations which indicated the possibility of detection and low-resolution spectroscopy in nulling mode of extra-solar giant planets (EGPs) with atmospheric temperatures down to 700 K, provided that a proper calibration of instrumental effects is applied. Detection of circumstellar exo-zodiacal (EZ) dust clouds is possible down to 0.5 mJy, with interesting prospects for the characterization of planet-forming disks. [less ▲]

Detailed reference viewed: 4 (0 ULg)
Full Text
See detailPEGASE: a DARWIN/TPF pathfinder
Ollivier, M.; Le Duigou, J.-M.; Mourard, D. et al

in Aime, C.; Vakili, F. (Eds.) Direct Imaging of Exoplanets: Science & Techniques (2006)

The space mission PEGASE, proposed to the CNES (Centre National d'Etudes Spatiales = French Space Agency) in the framework of its call for scientific proposals : "formation flying missions", is a 2 ... [more ▼]

The space mission PEGASE, proposed to the CNES (Centre National d'Etudes Spatiales = French Space Agency) in the framework of its call for scientific proposals : "formation flying missions", is a 2-aperture interferometer, composed by 3 free flying satellites (2 siderostats and 1 beam combiner), allowing baselines from 50 to 500 m in both nulling and visibility modes. With an angular resolution of a few mas and a spectral resolution of several tens in the spectral range 2.5-5 microns, PEGASE has several goals:science : spectroscopy of hot jupiters (Pegasides) and brown dwarves, exploration of the inner part of protoplanetary diskstechnology : validation in real space conditions of formation flying, nulling and visibility interferometry concepts.PEGASE has been studied at a 0-level. In this paper, we summarize the scientific program and associated technological and mission trade-off coming from this 0-level study. We also discuss how PEGASE can be considered as a TPF/DARWIN pathfinder in an international roadmap towards more complex space interferometry missions such as DARWIN/TPF. [less ▲]

Detailed reference viewed: 11 (0 ULg)
Full Text
See detailALADDIN: an optimized ground-based precursor for DARWIN
Coudé du Foresto, Vincent; Absil, Olivier ULg; Barillot, Marc et al

in Aime, C.; Vakili, F. (Eds.) Direct Imaging of Exoplanets: Science & Techniques (2006)

The ALADDIN concept is an integrated Antarctic-based L-band experiment whose purpose is to demonstrate nulling interferometry and to prepare the DARWIN mission. Because of their privileged location, the ... [more ▼]

The ALADDIN concept is an integrated Antarctic-based L-band experiment whose purpose is to demonstrate nulling interferometry and to prepare the DARWIN mission. Because of their privileged location, the relatively modest collectors (1 m) and baseline (up to 40 m) are sufficient to achieve a sensitivity (in terms of detectable zodi levels) which is about twice better than that of a nulling instrument on a large interferometer (such as GENIE at the VLTI), and to reach the 20-zodi threshold value identified to carry out the DARWIN precursor science. These numbers are based on a preliminary design study by Alcatel Alenia Space and were obtained using the same simulation software as the one employed for GENIE. The integrated design enables top-level optimization and full access to the light collectors for the duration of the experiment, while reducing the complexity of the nulling breadboard. [less ▲]

Detailed reference viewed: 6 (1 ULg)
See detailPEGASE... towards DARWIN
Ollivier, M.; Le Duigou, J.-M.; Mourard, D. et al

in Casoli, F.; Contini, T.; Hameury, J.-M. (Eds.) et al SF2A-2005: Semaine de l'Astrophysique Francaise (2005, December 01)

The space mission PEGASE, proposed to CNES in the framework of its call for scientific proposals on "formation flying", is a 2-aperture interferometer, composed by 3 free flying satellites. With an ... [more ▼]

The space mission PEGASE, proposed to CNES in the framework of its call for scientific proposals on "formation flying", is a 2-aperture interferometer, composed by 3 free flying satellites. With an angular resolution of a few mas and a spectral resolution of several tens in the spectral range 2.5-5 mum, PEGASE has several goals: - science: spectroscopy of hot jupiters (Pegasides) and brown dwarves, exploration of the inner part of protoplanetary disks; - technology: validation in real space conditions of formation flying, nulling and visibility interferometry concepts. PEGASE, presently in 0-phase study takes place in the context of DARWIN preparation. We detail in this paper the present situation of this project [less ▲]

Detailed reference viewed: 7 (0 ULg)
Full Text
Peer Reviewed
See detailAnnular Groove Phase Mask Coronagraph
Mawet, D.; Riaud, Pierre ULg; Absil, Olivier ULg et al

in Astrophysical Journal (2005), 633

We present a new phase mask coronagraph consisting in an optical vortex induced by a space-variant surface relief subwavelength grating. Phase mask coronagraphy is a recent technique aiming at ... [more ▼]

We present a new phase mask coronagraph consisting in an optical vortex induced by a space-variant surface relief subwavelength grating. Phase mask coronagraphy is a recent technique aiming at accommodating both high dynamic and high angular resolution imaging of faint sources around bright objects such as exoplanets orbiting their parent stars or host galaxies of active galactic nuclei. Subwavelength gratings are known to be artificially birefringent. Their unique dispersive characteristics can be controlled through the grating geometry in order to synthesize achromatic phase shifters. We show that implementing them in a ring-shaped way produces a fully symmetric and achromatic coronagraph without any gap or ``dead zone.'' The practical manufacturing of the device is also discussed. [less ▲]

Detailed reference viewed: 14 (5 ULg)
Full Text
See detailFirst evidence for a resolved structure in the inner Vega system
Absil, Olivier ULg

Poster (2005, October 01)

We report on infrared interferometric observations of Vega obtained in May and June 2005 with the FLUOR instrument installed on the CHARA interferometer. The combination of short and long baselines has ... [more ▼]

We report on infrared interferometric observations of Vega obtained in May and June 2005 with the FLUOR instrument installed on the CHARA interferometer. The combination of short and long baselines has allowed us to study the brightness distribution of the stellar photosphere, and to detect a spatial component which is over-resolved at our lowest resolution (~15 milli-arcseconds). This would be attributed to structure much larger than Vega, but within the CHARA/FLUOR field-of-view (about 1 arcsecond in radius, i.e., 8 AU around Vega). The contrast between the resolved flux and the central star is only slightly above the 1% level in K band. This emission could be interpreted as the first direct detection of thermal and/or scattered light emanating from the innermost part of the Vega debris disk, which is thought to be continuously replenished by asteroid collisions and/or comet evaporation. The possibility of a close stellar or sub-stellar companion is also investigated. [less ▲]

Detailed reference viewed: 4 (0 ULg)
See detailThe four-quadrant ZOG and annular groove phase mask coronagraphs
Mawet, Dimitri; Riaud, Pierre ULg; Absil, Olivier ULg et al

in Coulter, Daniel R (Ed.) Techniques and Instrumentation for Detection of Exoplanets II (2005, August 01)

Phase mask coronagraphy is a technique aiming at accommodating both high dynamic and high angular resolution imaging of faint sources around bright objects such as exo-planets orbiting their parent stars ... [more ▼]

Phase mask coronagraphy is a technique aiming at accommodating both high dynamic and high angular resolution imaging of faint sources around bright objects such as exo-planets orbiting their parent stars or host galaxies around Active Galactic Nuclei. We present two new phase mask coronagraphs implemented with subwavelength diffractive optical elements consisting of optimized surface-relief gratings. The first one is an evolution of the Four Quadrant Phase Mask coronagraph, which resolves the Ï phase shift chromaticity problem: the Four Quadrant Zeroth Order Grating (4QZOG). The second one is a totally new design consisting of an optical vortex induced by a space-variant grating: the Annular Groove Phase Mask (AGPM) coronagraph is fully symmetric and free from any "shaded zones". Some manufacturing hints are given. [less ▲]

Detailed reference viewed: 30 (6 ULg)
Full Text
Peer Reviewed
See detailLimitation of the Pupil Replication Technique in the Presence of Instrumental Defects
Riaud, Pierre ULg; Mawet, Dimitri; Absil, Olivier ULg

in Astrophysical Journal Letters (2005), 628

Pupil replication has been proposed by Greenaway et al. as a new optical technique to improve the suppression of starlight in high dynamic imaging. This Letter extends numerical simulations in the two ... [more ▼]

Pupil replication has been proposed by Greenaway et al. as a new optical technique to improve the suppression of starlight in high dynamic imaging. This Letter extends numerical simulations in the two-dimensional case with various realistic imperfections (surface error, chromatic smearing, and pupil shift). These results demonstrate some strong limitations compared to single-pupil apodization techniques for exoplanet detection. [less ▲]

Detailed reference viewed: 4 (0 ULg)
See detailPerspectives for next generation ground- and space-based interferometers (plenary session, invited)
Absil, Olivier ULg; Mawet, Dimitri

Scientific conference (2005, July 07)

The advent of large interferometric facilities such as the VLTI has recently offered the opportunity to the astronomical community to study various targets with an unprecedented angular resolution in the ... [more ▼]

The advent of large interferometric facilities such as the VLTI has recently offered the opportunity to the astronomical community to study various targets with an unprecedented angular resolution in the near- and mid-infrared. In this talk, we shortly review the main scientific topics that have largely benefited from interferometric studies in the past years, and present the future scientific challenges for interferometry. Some of these challenges will already be (partially) within reach when the second generation of VLTI instrumentation comes online, but most of them require more ambitious facilities to be built in the future. In this review talk, we recall the basic concepts of optical/IR interferometry and present some perspectives for future ground- and space-based interferometric facilities. Both approaches lead to major technological challenges that need to be overcome in the next decade. [less ▲]

Detailed reference viewed: 11 (0 ULg)
See detailDétection des exoplanètes avec le VLTI (invited)
Absil, Olivier ULg

Scientific conference (2005, May 30)

Detailed reference viewed: 6 (0 ULg)
Full Text
See detailInterférométrie destructive: du sol à l’espace
Absil, Olivier ULg

Scientific conference (2005, March 22)

Detailed reference viewed: 7 (0 ULg)
See detailThe PEGASE project: characterisation of "Pegasi planets" and Brown Dwarfs
Baudoz, P.; Rouan, D.; Schneider, J. et al

in Combes, F.; Barret, D.; Contini, T. (Eds.) et al SF2A-2004: Semaine de l'Astrophysique Francaise (2004, December 01)

I will present the PEGASE project proposed within the framework of the CNES call for idea on flights in formation. This ambitious project, gathering a dozen laboratories, proposes an interferometry ... [more ▼]

I will present the PEGASE project proposed within the framework of the CNES call for idea on flights in formation. This ambitious project, gathering a dozen laboratories, proposes an interferometry mission in infrared I(1.5 to 6 µm) with spectroscopic capabilities. The bases of the interferometer will reach up to 500m, giving to PEGASE a resolution higher than the milli-arcsecond. The interferometric recombination includes a very simple mode, measurement of the visibility by excursion of the optical path difference and a mode in black fringe or nulling. The very high angular resolution of the instrument and high dynamical range with the nulling mode will allow to consider exciting scientific objectives: the characterization of Pegasids or hot Jupiters, the study of the internal structure and the atmospheres of brown dwarfs and the analysis of the internal areas of proto-planetary disks. I will first of all describe the basic configuration of the mission and will show that its simplicity ensures the feasibility of the project. I will explain then the relevance of such an instrument for the characterization of Pegasids. I will detail finally the various possible technical options to be attached to the initial version, in order to increase the effectiveness of the mission and to extend its scientific objectives. [less ▲]

Detailed reference viewed: 5 (0 ULg)
Full Text
See detailThe simulated detection of low-mass companions with GENIE
den Hartog, Roland H; Absil, Olivier ULg; Gondoin, Philippe A et al

in Traub, Wesley; Monnier, John; Schöller, Markus (Eds.) New Frontiers in Stellar Interferometry (2004, October 01)

The prime objective of GENIE (Ground-based European Nulling Interferometry Experiment) is to obtain experience with the design, construction and operation of an IR nulling interferometer, as a preparation ... [more ▼]

The prime objective of GENIE (Ground-based European Nulling Interferometry Experiment) is to obtain experience with the design, construction and operation of an IR nulling interferometer, as a preparation for the DARWIN / TPF mission. In this context, the detection of a planet orbiting another star would provide an excellent demonstration of nulling interferometry. Doing this through the atmosphere, however, is a formidable task. In this paper we assess the prospects of detecting with nulling interferometry on ESO's VLTI, low-mass companions in orbit around their parent stars. With the GENIE science simulator (GENIEsim) we can model realistic detection scenarios for the GENIE instrument operating in the VLTI environment, and derive detailed requirements on control-loop performance, IR background subtraction and the accuracy of the photometry calibration. We analyse the technical feasibility of several scenarios for the detection of low-mass companions in the L'-band. [less ▲]

Detailed reference viewed: 6 (0 ULg)
Full Text
See detailDarwin-GENIE: a nulling instrument at the VLTI
Gondoin, Philippe A; Absil, Olivier ULg; den Hartog, Roland H et al

in Traub, Wesley (Ed.) New Frontiers in Stellar Interferometry (2004, October 01)

Darwin is one of the most challenging space projects ever considered by the European Space Agency (ESA). Its principal objectives are to detect Earth-like planets around nearby stars and to characterise ... [more ▼]

Darwin is one of the most challenging space projects ever considered by the European Space Agency (ESA). Its principal objectives are to detect Earth-like planets around nearby stars and to characterise their atmospheres. Darwin is conceived as a space "nulling interferometer" which makes use of on-axis destructive interferences to extinguish the stellar light while keeping the off-axis signal of the orbiting planet. Within the frame of the Darwin program, the European Space Agency (ESA) and the European Southern Observatory (ESO) intend to build a ground-based technology demonstrator called GENIE (Ground based European Nulling Interferometry Experiment). Such a ground-based demonstrator built around the Very Large Telescope Interferometer (VLTI) in Paranal will test some of the key technologies required for the Darwin Infrared Space Interferometer. It will demonstrate that nulling interferometry can be achieved in a broad mid-IR band as a precursor to the next phase of the Darwin program. The instrument will operate in the L' band around 3.8 mum, where the thermal emission from the telescopes and the atmosphere is reduced. GENIE will be able to operate in two different configurations, i.e. either as a single Bracewell nulling interferometer or as a double-Bracewell nulling interferometer with an internal modulation scheme. [less ▲]

Detailed reference viewed: 11 (0 ULg)
Full Text
See detailThree telescope nuller based on multibeam injection into single-mode waveguide
Karlsson, Anders L; Wallner, Oswald; Perdigues Armengol, Josep M et al

in Traub, Wesley (Ed.) New Frontiers in Stellar Interferometry (2004, October 01)

Nulling interferometry of exo-solar planets requires as a minimum two telescopes, of which one is phase shifted by 180 degrees, such that the on-axis stellar object is cancelled, while the light from the ... [more ▼]

Nulling interferometry of exo-solar planets requires as a minimum two telescopes, of which one is phase shifted by 180 degrees, such that the on-axis stellar object is cancelled, while the light from the off-axis planet interferes constructively. Improvement of the nulling performance and the introduction of chopping leads to space interferometers of four or more telescopes and a separate spacecraft dedicated to beam recombination, as currently baselined for Darwin and TPF. It has recently been demonstrated that the stellar leaks mainly affects the integration times for near-by target stars [o,c]. Considering that there are only a few near-by targets and that the integrations times for each of these is short compared to that of distant stars, it appears advantageous to simplify the interferometer, by accepting higher levels of stellar leaks for near-by targets. A simple, chopping nulling interferometer can be obtained by adding one equal size telescope to the basic two telescope nulling interferometer. Modulation is obtained by applying time-varying phase-shifts to the beams before recombination, i.e. inherent modulation [d]. The recombination of 3 multi-axial beams is achieved by coupling into a single mode waveguide, leading to high modulation and coupling efficiencies, and a single focal plane [i]. Linear and circular telescope configurations are proposed and investigated, including a discussion on the need of a separate spacecraft for beam recombination. The associated transmission and modulation maps and efficiencies are calculated and discussed. [less ▲]

Detailed reference viewed: 12 (0 ULg)
Full Text
See detailInfluence of atmospheric turbulence on the performance and design of GENIE
Absil, Olivier ULg; den Hartog, Roland; Gondoin, Philippe et al

in Traub, Wesley; Monnier, John; Schöller, Markus (Eds.) New Frontiers in Stellar Interferometry (2004, October 01)

Two competitive design studies for the Ground-based European Nulling Interferometer Experiment (GENIE) have been initiated by the European Space Agency and the European Southern Observatory in November ... [more ▼]

Two competitive design studies for the Ground-based European Nulling Interferometer Experiment (GENIE) have been initiated by the European Space Agency and the European Southern Observatory in November 2003. The GENIE instrument will most probably consist of a two-telescope Bracewell interferometer, using the 8-m Unit Telescopes and/or the 1.8-m Auxiliary Telescopes of the VLTI, and working in the infrared L' band (3.5 - 4.1 microns). A critical issue affecting the overall performance of the instrument is its capability to compensate for the phase and intensity fluctuations produced by the atmospheric turbulence. In this paper, we present the basic principles of phase and intensity control by means of real-time servo loops in the context of GENIE. We then propose a preliminary design for these servo loops and estimate their performance using GENIEsim, the science simulation software for the GENIE instrument. [less ▲]

Detailed reference viewed: 10 (0 ULg)
Full Text
See detailThermal background fluctuations at 10 micron measured with VLTI/MIDI
Absil, Olivier ULg; Bakker, Eric; Schoeller, Markus et al

in Traub, Wesley; Monnier, John; Schöller, Markus (Eds.) New Frontiers in Stellar Interferometry (2004, October 01)

We present an experiment to measure the thermal background level and its fluctuations with the European Southern Observatory (ESO) Very Large Telescope Interferometer (VLTI). The Mid Infrared Instrument ... [more ▼]

We present an experiment to measure the thermal background level and its fluctuations with the European Southern Observatory (ESO) Very Large Telescope Interferometer (VLTI). The Mid Infrared Instrument (MIDI) operating between 8 and 12 micron was used in both dispersed and non-dispersed modes. By using an interferometric instrument, in non-interferometric mode, we probe the same optical path as can be expected for other infrared interferometric instruments, e.g. GENIE and MIDI itself. Most of the infrared thermal background detected with MIDI originates from the VLTI infrastructure. This can be attributed to the absence of a pupil re-imaging mirror. Only for a small region around the optical axis of the system the signal from the VLTI infrastructure can be considered small and the atmospheric background fluctuations can be characterized. The fluctuations of the thermal emission are described in terms of their power spectral densities (PSD). We have identified two regions in the PSD. For the low frequency range (0-10 Hz) the fluctuations are dominated by the Earth atmosphere. The slope of the log-log PSD is close to -1. For the high frequency (larger than 10 Hz) range the fluctuations are due to photon noise and the PSD flattens off. Many narrow peaks are present in the PSD. Peaks at 1 and 50 Hz occur in almost all data sets and are identified as the effects of the MIDI closed cycle cooler and the power lines respectively. Other peaks at 10 and 30 Hz, as well as peaks above 50 Hz, are assumed to be VLTI or MIDI-specific frequencies. [less ▲]

Detailed reference viewed: 6 (0 ULg)
See detailPEGASE - A space interferometer for the spectro-photometry of Pegasides
Absil, Olivier ULg

Scientific conference (2004, August 25)

Pegase is an answer to the CNES call for ideas for a scientific payload on its Formation Flying technological mission. It proposes a Bracewell interferometer operating in the infrared (1.5 – 6 microns ... [more ▼]

Pegase is an answer to the CNES call for ideas for a scientific payload on its Formation Flying technological mission. It proposes a Bracewell interferometer operating in the infrared (1.5 – 6 microns) and visible regimes. It has small telescopes (40 cm) but a substantial baseline (25 to 500 m). Its angular resolution reaches 1 mas at 4 microns and 100 micro-as at 0.4 microns. Its main scientific objectives are the spectroscopic study of weak companions including pegasides and brown dwarfs bounded to other stars. The goal is to determine the composition of the atmospheres of these objects as well as their cloud structure. [less ▲]

Detailed reference viewed: 6 (0 ULg)