Publications (21)31.2 Total impact
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Article: NEAT: a space born astrometric mission for the detection and characterization of nearby habitable planetary systems
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ABSTRACT: The NEAT (Nearby Earth Astrometric Telescope) mission is a proposal submitted to ESA for its 2010 call for M-size mission within the Cosmic Vision 2015-2025 plan. The main scientific goal of the NEAT mission is to detect and characterize planetary systems in an exhaustive way down to 1 Earth mass in the habitable zone and further away, around nearby stars for F, G, and K spectral types. This survey would provide the actual planetary masses, the full characterization of the orbits including their inclination, for all the components of the planetary system down to that mass limit. NEAT will continue the work performed by Hipparcos and Gaia by reaching a precision that is improved by two orders of magnitude on pointed targets.07/2012; -
Article: SPICES: Spectro-Polarimetric Imaging and Characterization of Exoplanetary Systems
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ABSTRACT: SPICES (Spectro-Polarimetric Imaging and Characterization of Exoplanetary Systems) is a five-year M-class mission proposed to ESA Cosmic Vision. Its purpose is to image and characterize long-period extrasolar planets and circumstellar disks in the visible (450 - 900 nm) at a spectral resolution of about 40 using both spectroscopy and polarimetry. By 2020/22, present and near-term instruments will have found several tens of planets that SPICES will be able to observe and study in detail. Equipped with a 1.5 m telescope, SPICES can preferentially access exoplanets located at several AUs (0.5-10 AU) from nearby stars ($<$25 pc) with masses ranging from a few Jupiter masses to Super Earths ($\sim$2 Earth radii, $\sim$10 M$_{\oplus}$) as well as circumstellar disks as faint as a few times the zodiacal light in the Solar System.03/2012; -
Article: High precision astrometry mission for the detection and characterization of nearby habitable planetary systems with the Nearby Earth Astrometric Telescope (NEAT)
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ABSTRACT: A complete census of planetary systems around a volume-limited sample of solar-type stars (FGK dwarfs) in the Solar neighborhood (ensuremath densuremath<?iensuremath> $leq$ 15 pc) with uniform sensitivity down to Earth-mass planets within their Habitable Zones out to several AUs would be a major milestone in extrasolar planets astrophysics. This fundamental goal can be achieved with a mission concept such as NEAT--the Nearby Earth Astrometric Telescope. NEAT is designed to carry out space-borne extremely-high-precision astrometric measurements at the 0.05 ensuremathmuas (1 ensuremath ensuremathsigmaensuremath<?iensuremath>) accuracy level, sufficient to detect dynamical effects due to orbiting planets of mass even lower than Earth?s around the nearest stars. Such a survey mission would provide the actual planetary masses and the full orbital geometry for all the components of the detected planetary systems down to the Earth-mass limit. The NEAT performance limits can be achieved by carrying out differential astrometry between the targets and a set of suitable reference stars in the field. The NEAT instrument design consists of an off-axis parabola single-mirror telescope (D = 1 m), a detector with a large field of view located 40 m away from the telescope and made of 8 small movable CCDs located around a fixed central CCD, and an interferometric calibration system monitoring dynamical Young?s fringes originating from metrology fibers located at the primary mirror. The mission profile is driven by the fact that the two main modules of the payload, the telescope and the focal plane, must be located 40 m away leading to the choice of a formation flying option as the reference mission, and of a deployable boom option as an alternative choice. The proposed mission architecture relies on the use of two satellites, of about 700 kg each, operating at L2 for 5 years, flying in formation and offering a capability of more than 20,000 reconfigurations. The two satellites will be launched in a stacked configuration using a Soyuz ST launch vehicle. The NEAT primary science program will encompass an astrometric survey of our 200 closest F-, G- and K-type stellar neighbors, with an average of 50 visits each distributed over the nominal mission duration. The main survey operation will use approximately 70% of the mission lifetime. The remaining 30% of NEAT observing time might be allocated, for example, to improve the characterization of the architecture of selected planetary systems around nearby targets of specific interest (low-mass stars, young stars, etc.) discovered by Gaia, ground-based high-precision radial-velocity surveys, and other programs. With its exquisite, surgical astrometric precision, NEAT holds the promise to provide the first thorough census for Earth-mass planets around stars in the immediate vicinity of our Sun.Experimental Astronomy. 07/2011; -
Article: The QSO HE0450-2958: Scantily dressed or heavily robed? A normal quasar as part of an unusual ULIRG
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ABSTRACT: (Abridged) The luminous z=0.286 quasar HE0450-2958 is interacting with a companion galaxy at 6.5 kpc distance and the whole system is a ULIRG. A so far undetected host galaxy triggered the hypothesis of a mostly "naked" black hole (BH) ejected from the companion by three-body interaction. We present new HST/NICMOS 1.6micron imaging data at 0.1" resolution and VLT/VISIR 11.3micron images at 0.35" resolution that for the first time resolve the system in the near- and mid-infrared. We combine these with existing optical HST and CO maps. (i) At 1.6micron we find an extension N-E of the quasar nucleus that is likely a part of the host galaxy, though not its main body. If true, this places HE0450-2958 directly onto the M_BH-M_bulge-relation for nearby galaxies. (ii) HE0450-2958 is consistent with lying at the high-luminosity end of Narrow-Line Seyfert 1 Galaxies, and more exotic explanations like a "naked quasar" are unlikely. (iii) All 11.3micron radiation in the system is emitted by the quasar nucleus, which is radiating at super-Eddington rate, L/L_Edd=6.2+3.8-1.8, or 12 M_sun/yr. (iv) The companion galaxy is covered in optically thick dust and is not a collisional ring galaxy. It emits in the far infrared at ULIRG strength, powered by Arp220-like star formation (strong starburst-like). An M82-like SED is ruled out. (v) With its black hole accretion rate HE0450-2958 produces not enough new stars to maintain its position on the M_BH-M_bulge-relation, and star formation and black hole accretion are spatially disjoint; the bulge has to grow by redistribution of preexisting stars. (vi) Systems similar to HE0450-2958 with spatially disjoint ULIRG-strength star formation and quasar activity are rare. At z<0.43 we only find <4% (3/77) candidates for a similar configuration. Comment: 12 pages, 6 figures, accepted for publication in ApJ06/2009; -
Article: METIS - the Mid-infrared E-ELT Imager and Spectrograph
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ABSTRACT: METIS, the Mid-infrared ELT Imager and Spectrograph (formerly called MIDIR), is a proposed instrument for the European Extremely Large Telescope (E-ELT), currently undergoing a phase-A study. The study is carried out within the framework of the ESO-sponsored E-ELT instrumentation studies. METIS will be designed to cover the E-ELT science needs at wavelengths longward of 3um, where the thermal background requires different operating schemes. In this paper we discuss the main science drivers from which the instrument baseline has been derived. Specific emphasis has been given to observations that require very high spatial and spectral resolution, which can only be achieved with a ground-based ELT. We also discuss the challenging aspects of background suppression techniques, adaptive optics in the mid-IR, and telescope site considerations. The METIS instrument baseline includes imaging and spectroscopy at the atmospheric L, M, and N bands with a possible extension to Q band imaging. Both coronagraphy and polarimetry are also being considered. However, we note that the concept is still not yet fully consolidated. The METIS studies are being performed by an international consortium with institutes from the Netherlands, Germany, France, United Kingdom, and Belgium. Comment: 15 pages, to be published in Proc SPIE 7014: Ground-based & Airborne Instrumentation for Astronomy II07/2008; -
Article: Multi-wavelength observations of Galactic hard X-ray sources discovered by INTEGRAL. II. The environment of the companion star
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ABSTRACT: Context: The INTEGRAL mission has led to the discovery of a new type of supergiant X-ray binaries (SGXBs), whose physical properties differ from those of previously known SGXBs. Those sources are in the course of being unveiled by means of multi-wavelength X-rays, optical, near- and mid-infrared observations, and two classes are appearing. The first class consists of obscured persistent SGXBs and the second is populated by the so-called supergiant fast X-ray transients (SFXTs). Aims: We report here mid-infrared (MIR) observations of the companion stars of twelve SGXBs from these two classes in order to assess the contribution of the star and the material enshrouding the system to the total emission.} Methods: We used data from observations we carried out at ESO/VLT with VISIR, as well as archival and published data, to perform broad-band spectral energy distributions of the companion stars and fitted them with a combination of two black bodies representing the star and a MIR excess due to the absorbing material enshrouding the star, if there was any. Results: We detect a MIR excess in the emission of IGR J16318-4848, IGR J16358-4726, and perhaps IGR J16195-4945. The other sources do not exhibit any MIR excess even when the intrinsic absorption is very high. (abridged) Comment: A&A in press, The official date of acceptance is 25/01/2008, 17 pages, 4 figures, 9 tables. New version with english language editing required by editor, note added in proof02/2008; -
Article: VISIR/VLT mid-infrared imaging of Seyfert nuclei: Nuclear dust emission and the Seyfert-2 dichotomy
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ABSTRACT: Half of the Seyfert-2 galaxies escaped detection of broad lines in their polarised spectra observed so far. Some authors have suspected that these non-HBLRs contain real Sy2 nuclei without intrinsic broad line region hidden behind a dust torus. If this were true, then their nuclear structure would fundamentally differ from that of Sy2s with polarised broad lines: in particular, they would not be explained by orientation-based AGN unification. Further arguments for two physically different Sy2 populations have been derived from the warm and cool IRAS F25/F60 ratios. These ratios, however, refer to the entire host galaxies and are unsuitable to conclusively establish the absence of a nuclear dust torus. Instead, a study of the Seyfert-2 dichotomy should be performed on the basis of nuclear properties only. Here we present the first comparison between [OIII] 5007A and mid-infrared imaging at matching spatial resolution. Exploring the Seyfert-2 dichotomy we find that the distributions of nuclear mid-infrared/[OIII] luminosity ratios are indistinguishable for Sy1s and Sy2s with and without detected polarised broad lines and irrespective of having warm or cool IRAS F25/F60 ratios. We find no evidence for the existence of a population of real Sy2s with a deficit of nuclear dust emission. Our results suggest 1) that all Seyfert nuclei possess the same physical structure including the putative dust torus and 2) that the cool IRAS colours are caused by a low contrast of AGN to host galaxy. Then the Seyfert-2 dichotomy is explained in part by unification of non-HBLRs with narrow-line Sy1s and to a larger rate by observational biases caused by a low AGN/host contrast and/or an unfavourable scattering geometry. Comment: 11 pages, 6 figures, accepted by A&A07/2007; -
Article: Submillimetre/TeraHertz Astronomy at Dome C with CEA filled bolometer array
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ABSTRACT: Submillimetre/TeraHertz (e.g. 200, 350, 450 microns) astronomy is the prime technique to unveil the birth and early evolution of a broad range of astrophysical objects. A major obstacle to carry out submm observations from ground is the atmosphere. Preliminary site testing and atmospheric transmission models tend to demonstrate that Dome C could offer the best conditions on Earth for submm/THz astronomy. The CAMISTIC project aims to install a filled bolometer-array camera with 16x16 pixels on IRAIT at Dome C and explore the 200-$\mu$m windows for potential ground-based observations. Comment: 6 pages02/2007; -
Article: Anatomy of a flaring proto-planetary disk around a young intermediate-mass star.
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ABSTRACT: Although planets are being discovered around stars more massive than the Sun, information about the proto-planetary disks where such planets have built up is sparse. We have imaged mid-infrared emission from polycyclic aromatic hydrocarbons at the surface of the disk surrounding the young intermediate-mass star HD 97048 and characterized the disk. The disk is in an early stage of evolution, as indicated by its large content of dust and its hydrostatic flared geometry, indicative of the presence of a large amount of gas that is well mixed with dust and gravitationally stable. The disk is a precursor of debris disks found around more-evolved A stars such as beta-Pictoris and provides the rare opportunity to witness the conditions prevailing before (or during) planet formation.Science 11/2006; 314(5799):621-3. · 31.20 Impact Factor -
Article: CAMISTIC: THz/submm astronomy at Dome C in Antarctica
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ABSTRACT: Submillimetre (submm) astronomy is the prime technique to unveil the birth and early evolution of a broad range of astrophysical objects. It is a relatively new branch of observational astrophysics which focuses on studies of the cold Universe, i.e., objects radiating a significant – if not dominant – fraction of their energy at wavelengths ranging from ∼ 100 μm to ∼ 1 mm. Submm continuum observations are particularly powerful to measure the luminosities, temperatures and masses of cold dust emitting objects. Examples of such objects include star-forming clouds in our Galaxy, prestellar cores and deeply embedded protostars, protoplanetary disks around young stars, as well as nearby starburst galaxies and dust-enshrouded high-redshift galaxies in the early Universe.Proceedings of the International Astronomical Union 07/2006; 2:709 - 710. -
Article: Astronomical Telescopes and Instrumentation
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ABSTRACT: VISIR is the mid-infrared instrument installed in 2004 at the Cassegrain focus of MELIPAL, one of the four 8-meter telescopes of the European Very Large Telescope program. This cryogenic instrument, optimized for diffraction-limited performances in both mid-infrared atmospheric windows (N and Q bands), combines imaging capabilities and long-slit grating spectroscopy with spectral resolutions up to R=25000 at 10 μm and 12500 at 20 μm. The contract to design and build VISIR was signed in November 1996 between the European Southern Observatory (ESO) and a French-Dutch consortium of institutes led by Service d'Astrophysique of Commissariat a l'Energie Atomique (CEA). After extensive tests in the laboratory, VISIR was shipped to Paranal in March 2004. After successful commissioning between May and August 2004 and science verification between September 2004 and January 2005, routine science operations started in April 2005. The status of VISIR after 2 years of operation at the telescope is reviewed. This complex instrument, which features 14 cryogenic actuators to set the various observing possibilities, has been working without technical failure. The on-sky sensitivities are close to expectations. The median seeing conditions at Paranal (about 0.8-0.9 arcsec in the visible) are an issue to get routinely diffraction-limited images. Simple tip tilt adaptative corrections would be needed. For bright enough sources (a few Jansky), the so-called "burst mode", which allows to store up to 1500 individual frames (10-50 ms each) can be used to retrieve, off-line, diffraction-limited angular resolution (0.3 arcsec at 10 microns).© (2006) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.06/2006; -
Article: An emission ring at 20 microns around the HAEBE star AB Aurigae: unveiling the disc structure
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ABSTRACT: Isolated HAEBE stars are believed to represent an intermediate stage of objects between young stellar objects surrounded by massive, optically thick, gaseous and dusty disks and Vega like stars surrounded by debris disks. The star AB Aur is already known for being surrounded by an intermediate-stage dust disk emitting a fairly large infrared and (sub-)millimetric excess. Until now, the outer disk structure has only been resolved at millimeter wavelengths and at optical wavelength coronographic imaging. We have obtained 20 microns images which show an unexpected ellipse-shaped disk structure in emission at a distance of about 260 AU from the central star. Large azimuthal asymmetries in brightness can be noticed and the center of the ellipse does not coincide with the star. A simple, pure geometrical model based on an emission ring of uniform surface brightness, but having an intrinsic eccentricity succeeds in fitting the observations. These observations give for the first time clues on a very peculiar structure of pre-main-sequence disk geometry, i.e. a non uniform increase in the disk thickness unlike the common usual sketch of a disk with a constant flaring angle. They provide also valuable informations on the disk inclination as well as its dust composition; at such a large distance from the star, only transient heating of very small particles can explain such a bright ring of emission at mid-infrared wavelengths. Finally, the increase of thickness inferred by the model could be caused by disk instabilities; the intrinsic eccentricity of the structure might be a clue to the presence of a massive body undetected yet.03/2004; -
Article: Astronomical Telescopes and Instrumentation
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ABSTRACT: Since the beginning of the VISIR project, the calibration aspects have been taken into account as an integral part of the design. In order to provide the user and the archive with high quality and well-controlled data, it is mandatory to have, during the routine observation phase, all calibration observations as part of the instrument set-up activities and as part of the actual Astronomical Observing Template. We propose here to review the calibration of VISIR observations. After a description of the various hardware tools which have been introduced for calibration purposes (warm calibration unit, distortion grid, pupil imaging optics, wavelength calibration modules), we will present the calibrations in four astronomical categories (spatial resolution, photometry, astrometry and wavelength calibration). Cross-calibrations between the Imager and Spectrometer subsystems will also be addressed.© (2003) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.03/2003; -
Article: Molecular and Ionic shocks in the Supernova Remnant 3C391
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ABSTRACT: New observations of the supernova remnant 3C391 are in the H2 2.12 micron and [Fe II] 1.64 micron narrow-band filters at the Palomar 200-inch telescope, and in the 5-15 micron CVF on ISOCAM. Shocked H2 emission was detected from the region 3C391:BML, where broad millimeter CO and CS lines had previously been detected. A new H2 clump was confirmed to have broad CO emission, demonstrating that the near-infrared H2 images can trace previously undetected molecular shocks. The [Fe II] emission has a significantly different distribution, being brightest in the bright radio bar, at the interface between the supernova remnant and the giant molecular cloud, and following filaments in the radio shell. The near-infrared [Fe II] and the mid-infrared 12-18 micron filter images are the first images to reveal the radiative shell of 3C391. The mid-infrared spectrum is dominated by bright ionic lines and H2 S(2) through S(7). There are no aromatic hydrocarbons associated with the shocks, nor is their any mid-infrared continuum, suggesting that macromolecules and very small grains are destroyed. Comparing 3C391 to the better-studied IC443, both remnants have molecular- and ionic-dominated regions; for 3C391, the ionic-dominated region is the interface into the giant molecular cloud, showing that the main bodies of giant molecular clouds contain significant regions with densities 100 to 1000/cm^3 and a small filling factor with higher-density. The molecular shocked region resolves into 16 clumps of H2 emission, with some fainter diffuse emission but with no associated near-infrared continuum sources. One of the clumps is coincident with a previously-detected OH 1720 MHz maser. These clumps are interpreted as a cluster of pre-stellar, dense molecular cores that are presently being shocked by the supernova blast wave.08/2001; -
Article: Header for SPIE use
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ABSTRACT: In this paper, we present the status of VISIR, the mid-infrared instrument to be installed in 2001 at the Cassegrain focus of YEPUN, the telescope unit number 4 of the European Very Large Telescope program. This cryogenic instrument, optimized for both mid-infrared atmospheric windows (N and Q band), combines imaging capabilities over a field up to about 1 arcmin at the diffraction limit of the telescope, and long-slit (>30 arcsec) grating spectroscopy capabilities with various spectral resolution up to 25000 at 10 m and 12500 at 20 m. The contract to design and build VISIR was signed in November 1996 between the European Southern Observatory (ESO) and a French-Dutch consortium of institutes led by Service d'Astrophysique of Commissariat l'Energie Atomique (CEA). A key step in the project has been passed in 1999: the Final Design Review. The instrument is now in the manufacturing phase. Several subsystems have already been built and tested. The integration of the whole instrument is scheduled to start in December 2000.05/2000; -
Article: Astronomical Telescopes & Instrumentation
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ABSTRACT: In this paper, we present VISIR, the mid-IR instrument to be installed in 2001 on the telescope unit number 3 or the European Very Large Telescope program. The instrument combines imaging capabilities over a field up to about 1 arcmin at the diffraction limit of the telescope, and long- slit grating spectroscopy capabilities with various spectral resolutions. The contract to design and build VISIR was signed in November 1996 between ESO and a French-Dutch consortium of institutes. One year after the signature of the contract, VISIR has successfully passed the preliminary design review. The results of the first year of studies are presented here.Emphasis is put on the optical design which is in its final form.© (1998) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.08/1998; -
Article: First tests of the coronagraphic device of MIRI/JWST
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ABSTRACT: One of the main objectives of the instrument MIRI, the Mid-InfraRed Instrument, of the JWST is the direct detection and characterization of extrasolar giant planets. For that purpose, a coronagraphic device including three Four-Quadrant Phase Masks and a Lyot coronagraph working in mid-infrared, has been developed. We present here the results of the first test campaign of the coronagraphic system in the mid-infrared in the facility developed at the CEA. The performances are compared to the expected ones from the coronagraphic simulations. The accuracy of the centering procedures is also evaluated to validate the choice of the on-board centering algorithm. -
Article: The QSO HEÂ 0450-2958: scantily dressed or heavily robed? A normal quasar as part of an unusual ULIRG
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ABSTRACT: The luminous z = 0.286 quasar HEÂ 0450-2958 is interacting with a companion galaxy at 6.5 kpc distance and the whole system radiates in the infrared (IR) at the level of an ultraluminous infrared galaxy (ULIRG). A so far undetected host galaxy triggered the hypothesis of a mostly "naked" black hole (BH) ejected from the companion by three-body interaction. We present new Hubble Space Telescope (HST)/NICMOS 1.6 mum imaging data at 0farcs1 resolution and VLT/VISIR 11.3 mum images at 0farcs35 resolution that are for the first time resolving the system in the near- and mid-infrared. We combine these data with existing optical HST and CO maps. (1) At 1.6 mum we find an extension NE of the quasar nucleus that is likely a part of the host galaxy, though not its main body. If true, a combination with upper limits on a main body co-centered with the quasar brackets the host-galaxy luminosity to within a factor of ~4 and places HEÂ 0450-2958 directly onto the M BH -- M bulge relation for nearby galaxies. (2) A dust-free line of sight to the quasar suggests a low dust obscuration of the host galaxy, but the formal upper limit for star formation (SF) lies at 60 M sun yr--1. HEÂ 0450-2958 is consistent with lying at the high-luminosity end of Narrow-Line Seyfert 1 Galaxies, and more exotic explanations like a "naked quasar" are unlikely. (3) All 11.3 mum radiation in the system is emitted by the quasar nucleus. It has warm ULIRG-strength IR emission powered by BH accretion and is radiating at super-Eddington rate, L/L Edd = 6.2+3.8 --1.8, or 12 M sun yr--1. (4) The companion galaxy is covered in optically thick dust and is not a collisional ring galaxy. It emits in the far-infrared at ULIRG strength, powered by Arp220-like SF (strong starburst-like). An M82-like SED is ruled out. (5) With its BH accretion rate, HEÂ 0450-2958 produces not enough new stars to maintain its position on the M BH -- M bulge relation, and SF and BH accretion are spatially disjoint. This relation can either only be maintained averaging over a longer timescale (lsim500 Myr) and/or the bulge has to grow by redistribution of pre-existing stars. (6) Systems similar to HEÂ 0450-2958 with spatially disjoint ULIRG-strength star formation and quasar activity might be common at high redshifts but at z < 0.43 we only find <4% (3/77) candidates for a similar configuration.The Astrophysical Journal, v.700, 1820-1830 (2009). -
Article: Instrument concept and science case for the mid-IR E-ELT imager and spectrograph METIS
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ABSTRACT: METIS is the 'Mid-infrared ELT Imager and Spectrograph', the only planned thermal/mid-IR instrument for the E-ELT. METIS will provide diffraction limited imaging in the atmospheric L/M and N-band from 3 - 14 üm over an 18"Ãâ18" field of view (FOV). The imager also includes high contrast coronagraphy and low-resolution (900 <= R <= 5000) long slit spectroscopy and polarimetry. In addition, an IFU fed, high resolution spectrograph at L/M band will provide a spectral resolution of R ~ 100,000 over a 0.4"Ãâ1.5" FOV. The adaptive optics (AO) system is relatively simple, and METIS can reach its full performance with the adaptive correction provided by the telescope - and occasionally even under seeing limited conditions. On a 42m ELT, METIS will provide state-of-the-art mid-IR performance from the ground. The science case for METIS is based on proto-planetary disks, characterization of exoplanets, formation of our Solar System, growth of supermassive black holes, and the dynamics of high-z galaxies. With the focus on highest angular resolution and highest spectral resolution, METIS is highly complementary to JWST and ALMA. This paper summarizes the science case for METIS, and describes the instrument concept, performance and operational aspects.McLean, Ian S.; Ramsay, Suzanne K.; Takami, Hideki: Ground-based and Airborne Instrumentation for Astronomy III, SPIE, 77352G-77352G-16 (2010). -
Article: METIS: System engineering and optical design of the mid-infrared E-ELT instrument
SPIE, v.7735 (2010).
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Institutions
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2006
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Université Paris Diderot - Paris 7
Paris, Ile-de-France, France
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2001–2006
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Commissariat à l'énergie atomique et aux énergies alternatives
- • Direction des Sciences de la Matière (DSM)
- • Centre d'Etudes de Saclay
Gif-sur-Yvette, Ile-de-France, France
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