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1. MINDS. JWST/MIRI Reveals a Dynamic Gas-rich Inner Disk inside the Cavity of SY Cha

Author

Kamber R. Schwarz, Thomas Henning, Valentin Christiaens, Danny Gasman, Matthias Samland, Giulia Perotti, Hyerin Jang, Sierra L. Grant, Benoît Tabone, Maria Morales-Calderón, Inga Kamp, Ewine F. van Dishoeck, Manuel Güdel, Pierre-Olivier Lagage, David Barrado, Alessio Caratti o Garatti, Adrian M. Glauser, Tom P. Ray, Bart Vandenbussche, L. B. F. M. Waters, Aditya M. Arabhavi, Jayatee Kanwar, Göran Olofsson, Donna Rodgers-Lee, Jürgen Schreiber, and Milou Temmink

Subjects
Protoplanetary disks, Infrared spectroscopy, James Webb Space Telescope, Molecular spectroscopy, Astrophysics, QB460-466
Abstract

SY Cha is a T Tauri star surrounded by a protoplanetary disk with a large cavity seen in the millimeter continuum but has the spectral energy distribution of a full disk. Here we report the first results from JWST/Mid-InfraRed Instrument (MIRI) Medium Resolution Spectrometer (MRS) observations taken as part of the MIRI mid-INfrared Disk Survey (MINDS) GTO Program. The much improved resolution and sensitivity of MIRI-MRS compared to Spitzer enables a robust analysis of the previously detected H _2 O, CO, HCN, and CO _2 emission as well as a marginal detection of C _2 H _2 . We also report the first robust detection of mid-infrared OH and rovibrational CO emission in this source. The derived molecular column densities reveal the inner disk of SY Cha to be rich in both oxygen- and carbon-bearing molecules. This is in contrast to PDS 70, another protoplanetary disk with a large cavity observed with JWST, which displays much weaker line emission. In the SY Cha disk, the continuum, and potentially the line, flux varies substantially between the new JWST observations and archival Spitzer observations, indicative of a highly dynamic inner disk.

Published
2024
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2. Life beyond 30: Probing the −20 < M UV < −17 Luminosity Function at 8 < z < 13 with the NIRCam Parallel Field of the MIRI Deep Survey

Author

Pablo G. Pérez-González, Luca Costantin, Danial Langeroodi, Pierluigi Rinaldi, Marianna Annunziatella, Olivier Ilbert, Luis Colina, Hans Ulrik Nørgaard-Nielsen, Thomas R. Greve, Göran Östlin, Gillian Wright, Almudena Alonso-Herrero, Javier Álvarez-Márquez, Karina I. Caputi, Andreas Eckart, Olivier Le Fèvre, Álvaro Labiano, Macarena García-Marín, Jens Hjorth, Sarah Kendrew, John P. Pye, Tuomo Tikkanen, Paul van der Werf, Fabian Walter, Martin Ward, Arjan Bik, Leindert Boogaard, Sarah E. I. Bosman, Alejandro Crespo Gómez, Steven Gillman, Edoardo Iani, Iris Jermann, Jens Melinder, Romain A. Meyer, Thibaud Moutard, Ewine van Dishoek, Thomas Henning, Pierre-Olivier Lagage, Manuel Guedel, Florian Peissker, Tom Ray, Bart Vandenbussche, Ángela García-Argumánez, and Rosa María Mérida

Subjects
Galaxy formation, Galaxy evolution, Early universe, High-redshift galaxies, Broad band photometry, James Webb Space Telescope, Astrophysics, QB460-466
Abstract

We present the ultraviolet luminosity function and an estimate of the cosmic star formation rate density at 8 < z < 13 derived from deep NIRCam observations taken in parallel with the MIRI Deep Survey of the Hubble Ultra Deep Field (HUDF), NIRCam covering the parallel field 2. Our deep (40 hr) NIRCam observations reach an F277W magnitude of 30.8 (5 σ ), more than 2 mag deeper than JWST public data sets already analyzed to find high-redshift galaxies. We select a sample of 44 z > 8 galaxy candidates based on their dropout nature in the F115W and/or F150W filters, a high probability for their photometric redshifts, estimated with three different codes, being at z > 8, good fits based on χ ^2 calculations, and predominant solutions compared to z < 8 alternatives. We find mild evolution in the luminosity function from z ∼ 13 to z ∼ 8, i.e., only a small increase in the average number density of ∼0.2 dex, while the faint-end slope and absolute magnitude of the knee remain approximately constant, with values α = − 2.2 ± 0.1, and M ^* = − 20.8 ± 0.2 mag. Comparing our results with the predictions of state-of-the-art galaxy evolution models, we find two main results: (1) a slower increase with time in the cosmic star formation rate density compared to a steeper rise predicted by models; (2) nearly a factor of 10 higher star formation activity concentrated in scales around 2 kpc in galaxies with stellar masses ∼10 ^8 M _⊙ during the first 350 Myr of the universe, z ∼ 12, with models matching better the luminosity density observational estimations ∼150 Myr later, by z ∼ 9.

Published
2023
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3. MINDS. The Detection of 13CO2 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk

Author

Sierra L. Grant, Ewine F. van Dishoeck, Benoît Tabone, Danny Gasman, Thomas Henning, Inga Kamp, Manuel Güdel, Pierre-Olivier Lagage, Giulio Bettoni, Giulia Perotti, Valentin Christiaens, Matthias Samland, Aditya M. Arabhavi, Ioannis Argyriou, Alain Abergel, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alessio Caratti o Garatti, Vincent Geers, Adrian M. Glauser, Rodrigo Guadarrama, Hyerin Jang, Jayatee Kanwar, Fred Lahuis, Maria Morales-Calderón, Michael Mueller, Cyrine Nehmé, Göran Olofsson, Eric Pantin, Nicole Pawellek, Tom P. Ray, Donna Rodgers-Lee, Silvia Scheithauer, Jürgen Schreiber, Kamber Schwarz, Milou Temmink, Bart Vandenbussche, Marissa Vlasblom, L. B. F. M. Waters, Gillian Wright, Luis Colina, Thomas R. Greve, Kay Justannont, and Göran Östlin

Subjects
Protoplanetary disks, Planet formation, Astrophysics, QB460-466
Abstract

We present JWST-MIRI Medium Resolution Spectrometer (MRS) spectra of the protoplanetary disk around the low-mass T Tauri star GW Lup from the MIRI mid-INfrared Disk Survey Guaranteed Time Observations program. Emission from ^12 CO _2 , ^13 CO _2 , H _2 O, HCN, C _2 H _2 , and OH is identified with ^13 CO _2 being detected for the first time in a protoplanetary disk. We characterize the chemical and physical conditions in the inner few astronomical units of the GW Lup disk using these molecules as probes. The spectral resolution of JWST-MIRI MRS paired with high signal-to-noise data is essential to identify these species and determine their column densities and temperatures. The Q branches of these molecules, including those of hot bands, are particularly sensitive to temperature and column density. We find that the ^12 CO _2 emission in the GW Lup disk is coming from optically thick emission at a temperature of ∼400 K. ^13 CO _2 is optically thinner and based on a lower temperature of ∼325 K, and thus may be tracing deeper into the disk and/or a larger emitting radius than ^12 CO _2 . The derived ${N}_{{\mathrm{CO}}_{2}}$ / ${N}_{{{\rm{H}}}_{2}{\rm{O}}}$ ratio is orders of magnitude higher than previously derived for GW Lup and other targets based on Spitzer-InfraRed-Spectrograph data. This high column density ratio may be due to an inner cavity with a radius in between the H _2 O and CO _2 snowlines and/or an overall lower disk temperature. This paper demonstrates the unique ability of JWST to probe inner disk structures and chemistry through weak, previously unseen molecular features.

Published
2023
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4. A 3D Drizzle Algorithm for JWST and Practical Application to the MIRI Medium Resolution Spectrometer

Author

David R. Law, Jane E. Morrison, Ioannis Argyriou, Polychronis Patapis, J. Álvarez-Márquez, Alvaro Labiano, and Bart Vandenbussche

Subjects
Astronomy, QB1-991
Abstract

We describe an algorithm for application of the classic “drizzle” technique to produce 3D spectral cubes using data obtained from the slicer-type integral field unit (IFU) spectrometers on board the James Webb Space Telescope. This algorithm relies upon the computation of overlapping volume elements (composed of two spatial dimensions and one spectral dimension) between the 2D detector pixels and the 3D data cube voxels, and is greatly simplified by treating the spatial and spectral overlaps separately at the cost of just 0.03% in spectrophotometric fidelity. We provide a matrix-based formalism for the computation of spectral radiance, variance, and covariance from arbitrarily dithered data and comment on the performance of this algorithm for the Mid-Infrared Instrument’s Medium Resolution IFU Spectrometer. We derive a series of simplified scaling relations to account for covariance between cube spaxels in spectra extracted from such cubes, finding multiplicative factors ranging from 1.5–3 depending on the wavelength range and kind of data cubes produced. Finally, we discuss how undersampling produces periodic amplitude modulations in the extracted spectra in addition to those naturally produced by fringing within the instrument; reducing such undersampling artifacts below 1% requires a four-point dithering strategy and spectral extraction radii of 1.5 times the point-spread function FWHM or greater.

Published
2023
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5. The Mid-infrared Instrument for JWST and Its In-flight Performance

Author

Gillian S. Wright, George H. Rieke, Alistair Glasse, Michael Ressler, Macarena García Marín, Jonathan Aguilar, Stacey Alberts, Javier Álvarez-Márquez, Ioannis Argyriou, Kimberly Banks, Pierre Baudoz, Anthony Boccaletti, Patrice Bouchet, Jeroen Bouwman, Bernard R. Brandl, David Breda, Stacey Bright, Steven Cale, Luis Colina, Christophe Cossou, Alain Coulais, Misty Cracraft, Wim De Meester, Daniel Dicken, Michael Engesser, Mireya Etxaluze, Ori D. Fox, Scott Friedman, Henry Fu, Danny Gasman, András Gáspár, René Gastaud, Vincent Geers, Adrian Michael Glauser, Karl D. Gordon, Thomas Greene, Thomas R. Greve, Timothy Grundy, Manuel Güdel, Pierre Guillard, Peter Haderlein, Ryan Hashimoto, Thomas Henning, Dean Hines, Bryan Holler, Örs Hunor Detre, Amir Jahromi, Bryan James, Olivia C. Jones, Kay Justtanont, Patrick Kavanagh, Sarah Kendrew, Pamela Klaassen, Oliver Krause, Alvaro Labiano, Pierre-Olivier Lagage, Scott Lambros, Kirsten Larson, David Law, David Lee, Mattia Libralato, Jose Lorenzo Alverez, Margaret Meixner, Jane Morrison, Migo Mueller, Katherine Murray, Matthew Mycroft, Richard Myers, Omnarayani Nayak, Bret Naylor, Bryony Nickson, Alberto Noriega-Crespo, Göran Östlin, Brian O’Sullivan, Richard Ottens, Polychronis Patapis, Konstantin Penanen, Martin Pietraszkiewicz, Tom Ray, Michael Regan, Anthony Roteliuk, Pierre Royer, Piyal Samara-Ratna, Bridget Samuelson, Beth A. Sargent, Silvia Scheithauer, Analyn Schneider, Jürgen Schreiber, Bryan Shaughnessy, Evan Sheehan, Irene Shivaei, G. C. Sloan, Laszlo Tamas, Kelly Teague, Tea Temim, Tuomo Tikkanen, Samuel Tustain, Ewine F. van Dishoeck, Bart Vandenbussche, Mark Weilert, Paul Whitehouse, and Schuyler Wolff

Published
2023
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6. JWST MIRI/MRS in-flight absolute flux calibration and tailored fringe correction for unresolved sources

Author

Danny Gasman, Ioannis Argyriou, G. C. Sloan, Bernhard Aringer, Javier Álvarez-Márquez, Ori Fox, Alistair Glasse, Adrian Glauser, Olivia C. Jones, Kay Justtanont, Patrick J. Kavanagh, Pamela Klaassen, Alvaro Labiano, Kirsten Larson, David R. Law, Michael Mueller, Omnarayani Nayak, Alberto Noriega-Crespo, Polychronis Patapis, Pierre Royer, and Bart Vandenbussche

Subjects
stars, MODEL ATMOSPHERES, SAMPLE, PARSECS, data analysis, FOS: Physical sciences, Astronomy & Astrophysics, methods, ASTROPY, spectrographs, SPACE-TELESCOPE, infrared: stars, Instrumentation and Methods for Astrophysics (astro-ph.IM), detectors, instrumentation: spectrographs, instrumentation, SPECTRUM, Science & Technology, SPECTROSCOPY, instrumentation: detectors, Astronomy and Astrophysics, methods: data analysis, infrared: stars [instrumentation], LINE LISTS, SPITZER, Space and Planetary Science, Physical Sciences, infrared, Astrophysics - Instrumentation and Methods for Astrophysics, PROJECT
Abstract

Context. The Medium Resolution Spectrometer (MRS) is one of the four observing modes of JWST/MIRI. Using JWST in-flight data of unresolved (point) sources, we can derive the MRS absolute spectral response function (ASRF) starting from raw data. Spectral fringing, caused by coherent reflections inside the detector arrays, plays a critical role in the derivation and interpretation of the MRS ASRF. The fringe corrections implemented in the current pipeline are not optimal for non-extended sources, and a high density of molecular features particularly inhibits an accurate correction. Aims. In this paper, we present an alternative way to calibrate the MIRI/MRS data. Firstly, we derive a fringe correction that accounts for the dependence of the fringe properties on the MIRI/MRS pupil illumination and detector pixel sampling of the point spread function. Secondly, we derive the MRS ASRF using an absolute flux calibrator observed across the full 5- 28 µm wavelength range of the MRS. Thirdly, we apply the new ASRF to the spectrum of a G dwarf and compare it with the output of the JWST/MIRI default data reduction pipeline. Finally, we examine the impact of the different fringe corrections on the detectability of molecular features in the G dwarf and K giant. Methods. The absolute flux calibrator HD 163466 (A-star) was used to derive tailored point source fringe flats at each of the default dither locations of the MRS. The fringe-corrected point source integrated spectrum of HD 163466 was used to derive the MRS ASRF using a theoretical model for the stellar continuum. A cross-correlation was run to quantify the uncertainty on the detection of CO, SiO, and OH in the K giant and CO in the G dwarf for different fringe corrections. Results. The point-source-tailored fringe correction and ASRF are found to perform at the same level as the current corrections, beating down the fringe contrast to the sub-percent level in the G dwarf in the longer wavelengths, whilst mitigating the alteration of real molecular features. The same tailored solutions can be applied to other MRS unresolved targets. Target acquisition is required to ensure the pointing is accurate enough to apply this method. A pointing repeatability issue in the MRS limits the effectiveness of the tailored fringe flats is at short wavelengths. Finally, resulting spectra require no scaling to make the sub-bands match, and a dichroic spectral leak at 12.2 µm is removed., Astronomy & Astrophysics, 673, ISSN:0004-6361, ISSN:1432-0746

Published
2023

7. MARVEL: the Mercator radial-velocity facility

Author

Gert Raskin, Jacob Pember, Christian Schwab, Bart Vandenbussche, Gerardo Avila, Julian Stürmer, Hans Van Winckel, Denis Defrère, Pierre Royer, Andrew Tkachenko, Joris De Ridder, Hugues Sana, Joel Harman, William Humphreys, Robyn Sharman, Chris Waring, and Alistair Glasse

Published
2022
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8. PLATO camera ghosts: simulations and measurements on the engineering model (EM)

Author

Martin Pertenaïs, Matthias Ammler-von Eiff, Matteo Burresi, Juan Cabrera, Jacopo Farinato, Nicolas Gorius, Rik Huygen, Demetrio Magrin, Cesar Martin Garcia, Matteo Munari, Sara Regibo, Pierre Royer, Bart Vandenbussche, Tim van Kempen, Coyle, LE, Matsuura, S, and Perrin, MD

Subjects
Technology, Science & Technology, AIT, Optics, ghost, straylight, PLATO, Engineering, exoplanets, Physical Sciences, exoplanet, Engineering, Aerospace, Instruments & Instrumentation
Abstract

ispartof: SPACE TELESCOPES AND INSTRUMENTATION 2022: OPTICAL, INFRARED, AND MILLIMETER WAVE vol:12180 ispartof: Conference on Space Telescopes and Instrumentation - Optical, Infrared, and Millimeter Wave location:CANADA, Montreal date:17 Jul - 22 Jul 2022 status: published

Published
2022
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9. CubeSpec: optical payload design

Author

Gert Raskin, Jeroen Demaeyer, Bart Vandenbussche, Domnic Bowman, Jan Goris, Maarten Kempenaers, Jacob Pember, Pierre Royer, Job Schuermans, Andrew Tkachenko, Dirk Vandepitte, Wim De Munter, Jelle Lanting, Hugues Sana, Coyle, LE, Matsuura, S, and Perrin, MD

Subjects
Technology, Science & Technology, Engineering, Physical Sciences, CubeSat, Optical design, Optics, Engineering, Aerospace, Instruments & Instrumentation, Telescope, Spectroscopy
Abstract

ispartof: SPACE TELESCOPES AND INSTRUMENTATION 2022: OPTICAL, INFRARED, AND MILLIMETER WAVE vol:12180 ispartof: Conference on Space Telescopes and Instrumentation - Optical, Infrared, and Millimeter Wave location:CANADA, Montreal date:17 Jul - 22 Jul 2022 status: published

Published
2022
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12. L-band nulling interferometry at the VLTI with Asgard/Hi-5: status and plans

Author

Denis Defrère, Azzurra Bigioli, Colin Dandumont, Germain Garreau, Romain Laugier, Marc-Antoine Martinod, Olivier Absil, Jean-Philippe Berger, Emilie Bouzerand, Benjamin Courtney-Barrer, Alexandre Emsenhuber, Steve Ertel, Jonathan Gagne, Adrian M. Glauser, Simon Gross, Michael J. Ireland, Harry-Dean Kenchington Goldsmith, Jacques Kluska, Stefan Kraus, Lucas Labadie, Victor Laborde, Alain Léger, Jarron Leisenring, Jérôme Loicq, Guillermo Martin, Johan Morren, Alexis Matter, Alexandra Mazzoli, Kwinten Missiaen, Salman Muhammad, Marc Ollivier, Gert Raskin, Hélène Rousseau, Ahmed Sanny, Simon Verlinden, Bart Vandenbussche, Julien Woillez, Merand, A, Sallum, S, and Sanchez-Bermudez, J

Subjects
Technology, Science & Technology, high contrast imaging, optical fibers, exozodiacal disks, FOS: Physical sciences, CONSTRAINTS, Optics, DUST, Astronomy & Astrophysics, VLTI, long baseline interferometry, exoplanets, Physical Sciences, Nulling interferometry, DISCS, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Instruments & Instrumentation, high angular resolution
Abstract

Hi-5 is the L'-band (3.5-4.0 $\mu$m) high-contrast imager of Asgard, an instrument suite in preparation for the visitor focus of the VLTI. The system is optimized for high-contrast and high-sensitivity imaging within the diffraction limit of a single UT/AT telescope. It is designed as a double-Bracewell nulling instrument producing spectrally-dispersed (R=20, 400, or 2000) complementary nulling outputs and simultaneous photometric outputs for self-calibration purposes. In this paper, we present an update of the project with a particular focus on the overall architecture, opto-mechanical design of the warm and cold optics, injection system, and development of the photonic beam combiner. The key science projects are to survey (i) nearby young planetary systems near the snow line, where most giant planets are expected to be formed, and (ii) nearby main sequence stars near the habitable zone where exozodiacal dust that may hinder the detection of Earth-like planets. We present an update of the expected instrumental performance based on full end-to-end simulations using the new GRAVITY+ specifications of the VLTI and the latest planet formation models., Comment: 16 pages, 9 figures, SPIE 2022 "Astronomical Telescopes and Instrumentation" manuscript 12183-16

Published
2022
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13. MARVEL:Extracting high-precision radial velocities of exoplanet hosts

Author

Nicholas Jannsen, Dries Seynaeve, Joris De Ridder, Julian Stürmer, Jacob Pember, Christian Schwab, Lars A. Buchhave, Gert Raskin, Bart Vandenbussche, Hugues Sana, Andrew Tkachenko, Pierre Royer, Wim De Meester, Hans Van Winckel, Ignasi Ribas, Adler, David S., Seaman, Robert L., Benn, Chris R., Adler, DS, Seaman, RL, and Benn, CR

Subjects
Simulations, Technology, Radial velocity, Science & Technology, Spectrograph, Exoplanets, Optics, Astronomy & Astrophysics, Engineering, Pipeline, Physical Sciences, CM S(-1), Engineering, Aerospace, Instruments & Instrumentation, Telescopes
Abstract

The future ESA space mission PLATO aims to detect thousands of exoplanets, including Earth-like planets, and constrain their radius and mean density. To achieve this goal, the space based photometric observations are not enough but need to be complemented by ground-based observations to measure the Radial Velocity (RV) of the exoplanet host stars. MARVEL is such a facility consisting of four 80 cm telescope linked through optical fibers to a single high-resolution echelle spectrograph, designed for high-precision RV measurements with a uncertainty of 1 ms -1. MARVEL is build by a consortium led by the KU Leuven with contributions from the UK, Austria, Australia, Sweden, Denmark, and Spain, and will be commissioned in 2023. To reach such high RV precision, not only ultra-stable hardware is currently being developed, but also a state-of-The-Art data processing pipeline for which we present the first results in this poster.

Published
2022
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14. PLATO EM first cryogenic vacuum test campaign PSF results

Author

Francesco Borsa, Andrea Cottinelli, Nicolas Gorius, Claudio Arena, Bart Vandenbussche, Sara Regibo, Rik Huygen, Pierre Royer, Martin Pertenais, Cesar Martin, Thierry Appourchaux, Jose Lorenzo Alvarez, Tim A. van Kempen, Wouter Laauwen, Isabella Pagano, and Roberto Ragazzoni

Subjects
Hartmann mask, Ensquared energy fractions, Best focus search, PLATO, PSF
Published
2022
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15. The telescope assembly of the Ariel space mission

Author

Emanuele Pace, Andrea Tozzi, Manuel Adler Abreu, Gustavo Alonso, Bruno Barroqueiro, Giovanni Bianucci, Andrea Bocchieri, Daniele Brienza, Anna Brucalassi, Matteo Burresi, Rodolfo Canestrari, Luca Carbonaro, João Castanheira, Paolo Chioetto, Josep Colomé Ferrer, Carlos Compostizo, Fausto Cortecchia, Fabio D'Anca, Ciro Del Vecchio, Emiliano Diolaiti, Paul Eccleston, Salma Fahmy, Alejandro Fernandez Soler, Debora Ferruzzi, Mauro Focardi, Sara Freitas, Camille Galy, Andres Garcia Perez, Daniele Gottini, Samuele Grella, Gabriele Grisoni, Elisa Guerriero, Jean-Philippe Halain, Marie-Laure Hellin, Lucia Ianni, Marcella Iuzzolino, Delphine Jollet, Matteo Lombini, Ricardo Machado, Giuseppe Malaguti, Alexandra Mazzoli, Giuseppina Micela, Federico Miceli, Giuseppe Mondello, Gianluca Morgante, Lorenzo Mugnai, Luca Naponiello, Vladmiro Noce, Enzo Pascale, Javier Perez Alvarez, Raffaele Piazzolla, Carlo Pompei, Giampaolo Preti, Stephane Roose, Mario Salatti, Jean-Christophe Salvignol, Antonio Scippa, Christophe Serre, Carlo Simoncelli, Frederico Teixeira, Luca Terenzi, Giovanna Tinetti, Leonardo Tommasi, Elisabetta Tommasi Di Vigano, Bart Vandenbussche, Dervis Vernani, and Paola Zuppella

Subjects
mirror, telescopes, optical benches, aluminum, manufacturing, off axis mirror, coating, interfaces, space operations, cryogenics
Published
2022

16. MARVEL: optical fibre link

Author

Gerardo Avila, Gert Raskin, Christian Schwab, Jacob Pember, Bart Vandenbussche, Hans Van Winckel, Carlos Guirao, Roman Guemperlein, Julian Stürmer, Evans, CJ, Bryant, JJ, and Motohara, K

Subjects
Technology, astronomical instrumentation, Science & Technology, modal scrambling, Optical fibres, photometric scrambling, Physical Sciences, Optics, Instruments & Instrumentation
Abstract

ispartof: GROUND-BASED AND AIRBORNE INSTRUMENTATION FOR ASTRONOMY IX vol:12184 ispartof: Conference on Ground-Based and Airborne Instrumentation for Astronomy IX location:CANADA, Montreal date:17 Jul - 22 Jul 2022 status: published

Published
2022

17. Alignment and Integration of the first PLATO Camera

Author

Pierre Royer, Ann Baeke, Guilhem Terrasa, Rik Huygen, Sara Regibo, Jacopo Farinato, Demetrio Magrin, Alexandra Mazzoli, Miriam Pajas, Bart Vandenbussche, Aline Hermans, Gabriel Millou, Daniele Vassallo, Ana Balado, Lionel Clermont, Andrea Cottinelli, Lorenza Ferrari, Nicolas Gorius, Wouter Laauwen, Yves Levillain, Andrea Novi, Isabella Pagano, Martin Pertenaïs, Gonzalo Ramos Zapata, Mario Salatti, Tim A. van Kempen, Coyle, LE, Matsuura, S, and Perrin, MD

Subjects
Technology, AIV, Science & Technology, bolting, Integration, AIT, spacecraft integration, Optics, alignment, integration, Cryo-vacuum, PLATO, focus, Ambient, Engineering, Physical Sciences, Ground Support Equipment, Focussing, Hartmann, Engineering, Aerospace, Instruments & Instrumentation, Alignment, camera
Abstract

ispartof: SPACE TELESCOPES AND INSTRUMENTATION 2022: OPTICAL, INFRARED, AND MILLIMETER WAVE vol:12180 ispartof: Conference on Space Telescopes and Instrumentation - Optical, Infrared, and Millimeter Wave location:CANADA, Montreal date:17 Jul - 22 Jul 2022 status: published

Published
2022

18. The Science Performance of JWST as Characterized in Commissioning

Author

Jane Rigby, Marshall Perrin, Michael McElwain, Randy Kimble, Scott Friedman, Matt Lallo, René Doyon, Lee Feinberg, Pierre Ferruit, Alistair Glasse, Marcia Rieke, George Rieke, Gillian Wright, Chris Willott, Knicole Colon, Stefanie Milam, Susan Neff, Christopher Stark, Jeff Valenti, Jim Abell, Faith Abney, Yasin Abul-Huda, D. Scott Acton, Evan Adams, David Adler, Jonathan Aguilar, Nasif Ahmed, Loïc Albert, Stacey Alberts, David Aldridge, Marsha Allen, Martin Altenburg, Javier Álvarez-Márquez, Catarina Alves de Oliveira, Greg Andersen, Harry Anderson, Sara Anderson, Ioannis Argyriou, Amber Armstrong, Santiago Arribas, Etienne Artigau, Amanda Arvai, Charles Atkinson, Gregory Bacon, Thomas Bair, Kimberly Banks, Jaclyn Barrientes, Bruce Barringer, Peter Bartosik, William Bast, Pierre Baudoz, Thomas Beatty, Katie Bechtold, Tracy Beck, Eddie Bergeron, Matthew Bergkoetter, Rachana Bhatawdekar, Stephan Birkmann, Ronald Blazek, Claire Blome, Anthony Boccaletti, Torsten Böker, John Boia, Nina Bonaventura, Nicholas Bond, Kari Bosley, Ray Boucarut, Matthew Bourque, Jeroen Bouwman, Gary Bower, Charles Bowers, Martha Boyer, Larry Bradley, Greg Brady, Hannah Braun, David Breda, Pamela Bresnahan, Stacey Bright, Christopher Britt, Asa Bromenschenkel, Brian Brooks, Keira Brooks, Bob Brown, Matthew Brown, Patricia Brown, Andy Bunker, Matthew Burger, Howard Bushouse, Steven Cale, Alex Cameron, Peter Cameron, Alicia Canipe, James Caplinger, Francis Caputo, Mihai Cara, Larkin Carey, Stefano Carniani, Maria Carrasquilla, Margaret Carruthers, Michael Case, Riggs Catherine, Don Chance, George Chapman, Stéphane Charlot, Brian Charlow, Pierre Chayer, Bin Chen, Brian Cherinka, Sarah Chichester, Zack Chilton, Taylor Chonis, Mark Clampin, Charles Clark, Kerry Clark, Dan Coe, Benee Coleman, Brian Comber, Tom Comeau, Dennis Connolly, James Cooper, Rachel Cooper, Eric Coppock, Matteo Correnti, Christophe Cossou, Alain Coulais, Laura Coyle, Misty Cracraft, Mirko Curti, Steven Cuturic, Katherine Davis, Michael Davis, Bruce Dean, Amy DeLisa, Wim deMeester, Nadia Dencheva, Nadezhda Dencheva, Joseph DePasquale, Jeremy Deschenes, Örs Hunor Detre, Rosa Diaz, Dan Dicken, Audrey DiFelice, Matthew Dillman, William Dixon, Jesse Doggett, Tom Donaldson, Rob Douglas, Kimberly DuPrie, Jean Dupuis, John Durning, Nilufar Easmin, Weston Eck, Chinwe Edeani, Eiichi Egami, Ralf Ehrenwinkler, Jonathan Eisenhamer, Michael Eisenhower, Michelle Elie, James Elliott, Kyle Elliott, Tracy Ellis, Michael Engesser, Nestor Espinoza, Odessa Etienne, Mireya Etxaluze, Patrick Falini, Matthew Feeney, Malcolm Ferry, Joseph Filippazzo, Brian Fincham, Mees Fix, Nicolas Flagey, Michael Florian, Jim Flynn, Erin Fontanella, Terrance Ford, Peter Forshay, Ori Fox, David Franz, Henry Fu, Alexander Fullerton, Sergey Galkin, Anthony Galyer, Macarena García Marín, Jonathan P. Gardner, Lisa Gardner, Dennis Garland, Bruce Garrett, Danny Gasman, Andras Gaspar, Daniel Gaudreau, Peter Gauthier, Vincent Geers, Paul Geithner, Mario Gennaro, Giovanna Giardino, Julien Girard, Mark Giuliano, Kirk Glassmire, Adrian Glauser, Stuart Glazer, John Godfrey, David Golimowski, David Gollnitz, Fan Gong, Shireen Gonzaga, Michael Gordon, Karl Gordon, Paul Goudfrooij, Thomas Greene, Matthew Greenhouse, Stefano Grimaldi, Andrew Groebner, Timothy Grundy, Pierre Guillard, Irvin Gutman, Kong Q. Ha, Peter Haderlein, Andria Hagedorn, Kevin Hainline, Craig Haley, Maryam Hami, Forrest Hamilton, Heidi Hammel, Carl Hansen, Tom Harkins, Michael Harr, Jessica Hart, Quyen Hart, George Hartig, Ryan Hashimoto, Sujee Haskins, William Hathaway, Keith Havey, Brian Hayden, Karen Hecht, Chris Heller-Boyer, Caroline Henriques, Alaina Henry, Karl Hermann, Scarlin Hernandez, Brigette Hesman, Brian Hicks, Bryan Hilbert, Dean Hines, Melissa Hoffman, Sherie Holfeltz, Bryan J. 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Subjects
Science & Technology, Observatories, Infrared astronomy, Astronomical instrumentation, INFRARED SPECTROGRAPH NIRSPEC, FOS: Physical sciences, Astronomy and Astrophysics, Astronomy & Astrophysics, Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, Physical Sciences, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

This paper characterizes the actual science performance of the James Webb Space Telescope (JWST), as determined from the six month commissioning period. We summarize the performance of the spacecraft, telescope, science instruments, and ground system, with an emphasis on differences from pre-launch expectations. Commissioning has made clear that JWST is fully capable of achieving the discoveries for which it was built. Moreover, almost across the board, the science performance of JWST is better than expected; in most cases, JWST will go deeper faster than expected. The telescope and instrument suite have demonstrated the sensitivity, stability, image quality, and spectral range that are necessary to transform our understanding of the cosmos through observations spanning from near-earth asteroids to the most distant galaxies., Comment: 5th version as accepted to PASP; 31 pages, 18 figures; https://iopscience.iop.org/article/10.1088/1538-3873/acb293

Published
2022
Full Text
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19. Ariel: Enabling planetary science across light-years

Author

Giovanna Tinetti, Paul Eccleston, Carole Haswell, Pierre-Olivier Lagage, Jérémy Leconte, Theresa Lüftinger, Giusi Micela, Michel Min, Göran Pilbratt, Ludovic Puig, Mark Swain, Leonardo Testi, Diego Turrini, Bart Vandenbussche, Maria Rosa Zapatero Osorio, Anna Aret, Jean-Philippe Beaulieu, Buchhave, Lars A., Martin Ferus, Matt Griffin, Manuel Guedel, Paul Hartogh, Pedro Machado, Giuseppe Malaguti, Enric Pallé, Mirek Rataj, Tom Ray, Ignasi Ribas, Robert Szabó, Jonathan Tan, Stephanie Werner, Francesco Ratti, Carsten Scharmberg, Jean-Christophe Salvignol, Nathalie Boudin, Jean-Philippe Halain, Martin Haag, Pierre-Elie Crouzet, Ralf Kohley, Kate Symonds, Florian Renk, Andrew Caldwell, Manuel Abreu, Gustavo Alonso, Jerome Amiaux, Michel Berthé, Georgia Bishop, Neil Bowles, Manuel Carmona, Deirdre Coffey, Josep Colomé, Martin Crook, Lucile Désjonqueres, Díaz, José J., Rachel Drummond, Mauro Focardi, Gómez, Jose M., Warren Holmes, Matthijs Krijger, Zsolt Kovacs, Tom Hunt, Richardo Machado, Gianluca Morgante, Marc Ollivier, Roland Ottensamer, Emanuele Pace, Teresa Pagano, Enzo Pascale, Chris Pearson, Søren Møller Pedersen, Moshe Pniel, Stéphane Roose, Giorgio Savini, Richard Stamper, Peter Szirovicza, Janos Szoke, Ian Tosh, Francesc Vilardell, Joanna Barstow, Luca Borsato, Sarah Casewell, Quentin Changeat, Benjamin Charnay, Svatopluk Civiš, Vincent Coudé du Foresto, Athena Coustenis, Nicolas Cowan, Camilla Danielski, Olivier Demangeon, Pierre Drossart, Edwards, Billy N., Gabriella Gilli, Therese Encrenaz, Csaba Kiss, Anastasia Kokori, Masahiro Ikoma, Juan Carlos Morales, Joao Mendonca, Andrea Moneti, Lorenzo Mugnai, Antonio García Muñoz, Ravit Helled, Mihkel Kama, Yamila Miguel, Nikos Nikolaou, Isabella Pagano, Olja Panic, Miriam Rengel, Hans Rickman, Marco Rocchetto, Subhajit Sarkar, Franck Selsis, Jonathan Tennyson, Angelos Tsiaras, Olivia Venot, Krisztián Vida, Waldmann, Ingo P., Sergey Yurchenko, Gyula Szabó, Rob Zellem, Ahmed Al-Refaie, Javier Perez Alvarez, Lara Anisman, Axel Arhancet, Jaume Ateca, Robin Baeyens, Barnes, John R., Taylor Bell, Serena Benatti, Katia Biazzo, Maria Błęcka, Aldo Stefano Bonomo, José Bosch, Diego Bossini, Jeremy Bourgalais, Daniele Brienza, Anna Brucalassi, Giovanni Bruno, Hamish Caines, Simon Calcutt, Tiago Campante, Rodolfo Canestrari, Nick Cann, Giada Casali, Albert Casas, Giuseppe Cassone, Christophe Cara, Ludmila Carone, Nathalie Carrasco, Paolo Chioetto, Fausto Cortecchia, Markus Czupalla, Chubb, Katy L., Angela Ciaravella, Antonio Claret, Riccardo Claudi, Claudio Codella, Maya Garcia Comas, Gianluca Cracchiolo, Patricio Cubillos, Vania Da Peppo, Leen Decin, Clemence Dejabrun, Elisa Delgado-Mena, Anna Di Giorgio, Emiliano Diolaiti, Caroline Dorn, Vanessa Doublier, Eric Doumayrou, Georgina Dransfield, Luc Dumaye, Emma Dunford, Antonio Jimenez Escobar, Vincent Van Eylen, Maria Farina, Davide Fedele, Alejandro Fernández, Benjamin Fleury, Sergio Fonte, Jean Fontignie, Luca Fossati, Bernd Funke, Camille Galy, Zoltán Garai, Andrés García, Alberto García-Rigo, Antonio Garufi, Giuseppe Germano Sacco, Paolo Giacobbe, Alejandro Gómez, Arturo Gonzalez, Francisco Gonzalez-Galindo, Davide Grassi, Caitlin Griffith, Mario Giuseppe Guarcello, Audrey Goujon, Amélie Gressier, Aleksandra Grzegorczyk, Tristan Guillot, Gloria Guilluy, Peter Hargrave, Marie-Laure Hellin, Enrique Herrero, Matt Hills, Benoit Horeau, Yuichi Ito, Niels Christian Jessen, Petr Kabath, Szilárd Kálmán, Yui Kawashima, Tadahiro Kimura, Antonín Knížek, Laura Kreidberg, Ronald Kruid, Kruijssen, Diederik J. M., Petr Kubelík, Luisa Lara, Sebastien Lebonnois, David Lee, Maxence Lefevre, Tim Lichtenberg, Daniele Locci, Matteo Lombini, Alejandro Sanchez Lopez, Andrea Lorenzani, Ryan MacDonald, Laura Magrini, Jesus Maldonado, Emmanuel Marcq, Alessandra Migliorini, Darius Modirrousta-Galian, Karan Molaverdikhani, Sergio Molinari, Paul Mollière, Vincent Moreau, Giuseppe Morello, Gilles Morinaud, Mario Morvan, Moses, Julianne I., Salima Mouzali, Nariman Nakhjiri, Luca Naponiello, Norio Narita, Valerio Nascimbeni, Athanasia Nikolaou, Vladimiro Noce, Fabrizio Oliva, Pietro Palladino, Andreas Papageorgiou, Vivien Parmentier, Giovanni Peres, Javier Pérez, Santiago Perez-Hoyos, Manuel Perger, Cesare Cecchi Pestellini, Antonino Petralia, Anne Philippon, Arianna Piccialli, Marco Pignatari, Giampaolo Piotto, Linda Podio, Gianluca Polenta, Giampaolo Preti, Theodor Pribulla, Manuel Lopez Puertas, Monica Rainer, Jean-Michel Reess, Paul Rimmer, Séverine Robert, Albert Rosich, Loic Rossi, Duncan Rust, Ayman Saleh, Nicoletta Sanna, Eugenio Schisano, Laura Schreiber, Victor Schwartz, Antonio Scippa, Bálint Seli, Sho Shibata, Caroline Simpson, Oliver Shorttle, Skaf, N., Konrad Skup, Mateusz Sobiecki, Sergio Sousa, Alessandro Sozzetti, Judit Šponer, Lukas Steiger, Paolo Tanga, Paul Tackley, Jake Taylor, Matthias Tecza, Luca Terenzi, Pascal Tremblin, Andrea Tozzi, Amaury Triaud, Loïc Trompet, Shang-Min Tsai, Maria Tsantaki, Diana Valencia, Ann Carine Vandaele, Mathieu Van der Swaelmen, Adibekyan Vardan, Gautam Vasisht, Allona Vazan, Ciro Del Vecchio, Dave Waltham, Piotr Wawer, Thomas Widemann, Paulina Wolkenberg, Gordon Hou Yip, Yuk Yung, Mantas Zilinskas, Tiziano Zingales, Paola Zuppella, University College of London [London] (UCL), Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), Université de Bordeaux (UB), Agence Spatiale Européenne = European Space Agency (ESA), SRON Netherlands Institute for Space Research (SRON), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Bologna (OABO), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), European Space Agency, Agence Spatiale Européenne (ESA), European Space Agency (ESA), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Giovanna Tinetti, Paul Eccleston, Carole Haswell, Pierre-Olivier Lagage, Jérémy Leconte, Theresa Lüftinger, Giusi Micela, Michel Min, Göran Pilbratt, Ludovic Puig, Mark Swain, Leonardo Testi, Diego Turrini, Bart Vandenbussche, Maria Rosa Zapatero Osorio, Anna Aret, Jean-Philippe Beaulieu, Lars Buchhave, Martin Feru, Matt Griffin, Manuel Guedel, Paul Hartogh, Pedro Machado, Giuseppe Malaguti, Enric Pallé, Mirek Rataj, Tom Ray, Ignasi Riba, Robert Szabó, Jonathan Tan, Stephanie Werner, Francesco Ratti, Carsten Scharmberg, Jean-Christophe Salvignol, Nathalie Boudin, Jean-Philippe Halain, Martin Haag, Pierre-Elie Crouzet, Ralf Kohley, Kate Symond, Florian Renk, Andrew Caldwell, Manuel Abreu, Gustavo Alonso, Jerome Amiaux, Michel Berthé, Georgia Bishop, Neil Bowle, Manuel Carmona, Deirdre Coffey, Josep Colomé, Martin Crook, Lucile Désjonquere, José J. Díaz, Rachel Drummond, Mauro Focardi, Jose M. Gómez, Warren Holme, Matthijs Krijger, Zsolt Kovac, Tom Hunt, Richardo Machado, Gianluca Morgante, Marc Ollivier, Roland Ottensamer, Emanuele Pace, Teresa Pagano, Enzo Pascale, Chris Pearson, Søren Møller Pedersen, Moshe Pniel, Stéphane Roose, Giorgio Savini, Richard Stamper, Peter Szirovicza, Janos Szoke, Ian Tosh, Francesc Vilardell, Joanna Barstow, Luca Borsato, Sarah Casewell, Quentin Changeat, Benjamin Charnay, Svatopluk Civiš, Vincent Coudé du Foresto, Athena Cousteni, Nicolas Cowan, Camilla Danielski, Olivier Demangeon, Pierre Drossart, Billy N. Edward, Gabriella Gilli, Therese Encrenaz, Csaba Ki, Anastasia Kokori, Masahiro Ikoma, Juan Carlos Morale, João Mendonça, Andrea Moneti, Lorenzo Mugnai, Antonio García Muñoz, Ravit Helled, Mihkel Kama, Yamila Miguel, Nikos Nikolaou, Isabella Pagano, Olja Panic, Miriam Rengel, Hans Rickman, Marco Rocchetto, Subhajit Sarkar, Franck Selsi, Jonathan Tennyson, Angelos Tsiara, Olivia Venot, Krisztián Vida, Ingo P. Waldmann, Sergey Yurchenko, Gyula Szabó, Rob Zellem, Ahmed Al-Refaie, Javier Perez Alvarez, Lara Anisman, Axel Arhancet, Jaume Ateca, Robin Baeyen, John R. Barne, Taylor Bell, Serena Benatti, Katia Biazzo, Maria Błęcka, Aldo Stefano Bonomo, José Bosch, Diego Bossini, Jeremy Bourgalai, Daniele Brienza, Anna Brucalassi, Giovanni Bruno, Hamish Caine, Simon Calcutt, Tiago Campante, Rodolfo Canestrari, Nick Cann, Giada Casali, Albert Casa, Giuseppe Cassone, Christophe Cara, Ludmila Carone, Nathalie Carrasco, Paolo Chioetto, Fausto Cortecchia, Markus Czupalla, Katy L. Chubb, Angela Ciaravella, Antonio Claret, Riccardo Claudi, Claudio Codella, Maya Garcia Coma, Gianluca Cracchiolo, Patricio Cubillo, Vania Da Peppo, Leen Decin, Clemence Dejabrun, Elisa Delgado-Mena, Anna Di Giorgio, Emiliano Diolaiti, Caroline Dorn, Vanessa Doublier, Eric Doumayrou, Georgina Dransfield, Luc Dumaye, Emma Dunford, Antonio Jimenez Escobar, Vincent Van Eylen, Maria Farina, Davide Fedele, Alejandro Fernández, Benjamin Fleury, Sergio Fonte, Jean Fontignie, Luca Fossati, Bernd Funke, Camille Galy, Zoltán Garai, Andrés García, Alberto García-Rigo, Antonio Garufi, Giuseppe Germano Sacco, Paolo Giacobbe, Alejandro Gómez, Arturo Gonzalez, Francisco Gonzalez-Galindo, Davide Grassi, Caitlin Griffith, Mario Giuseppe Guarcello, Audrey Goujon, Amélie Gressier, Aleksandra Grzegorczyk, Tristan Guillot, Gloria Guilluy, Peter Hargrave, Marie-Laure Hellin, Enrique Herrero, Matt Hill, Benoit Horeau, Yuichi Ito, Niels Christian Jessen, Petr Kabath, Szilárd Kálmán, Yui Kawashima, Tadahiro Kimura, Antonín Knížek, Laura Kreidberg, Ronald Kruid, Diederik J. M. Kruijssen, Petr Kubelík, Luisa Lara, Sebastien Lebonnoi, David Lee, Maxence Lefevre, Tim Lichtenberg, Daniele Locci, Matteo Lombini, Alejandro Sanchez Lopez, Andrea Lorenzani, Ryan MacDonald, Laura Magrini, Jesus Maldonado, Emmanuel Marcq, Alessandra Migliorini, Darius Modirrousta-Galian, Karan Molaverdikhani, Sergio Molinari, Paul Mollière, Vincent Moreau, Giuseppe Morello, Gilles Morinaud, Mario Morvan, Julianne I. Mose, Salima Mouzali, Nariman Nakhjiri, Luca Naponiello, Norio Narita, Valerio Nascimbeni, Athanasia Nikolaou, Vladimiro Noce, Fabrizio Oliva, Pietro Palladino, Andreas Papageorgiou, Vivien Parmentier, Giovanni Pere, Javier Pérez, Santiago Perez-Hoyo, Manuel Perger, Cesare Cecchi Pestellini, Antonino Petralia, Anne Philippon, Arianna Piccialli, Marco Pignatari, Giampaolo Piotto, Linda Podio, Gianluca Polenta, Giampaolo Preti, Theodor Pribulla, Manuel Lopez Puerta, Monica Rainer, Jean-Michel Ree, Paul Rimmer, Séverine Robert, Albert Rosich, Loic Rossi, Duncan Rust, Ayman Saleh, Nicoletta Sanna, Eugenio Schisano, Laura Schreiber, Victor Schwartz, Antonio Scippa, Bálint Seli, Sho Shibata, Caroline Simpson, Oliver Shorttle, N. Skaf, Konrad Skup, Mateusz Sobiecki, Sergio Sousa, Alessandro Sozzetti, Judit Šponer, Lukas Steiger, Paolo Tanga, Paul Tackley, Jake Taylor, Matthias Tecza, Luca Terenzi, Pascal Tremblin, Andrea Tozzi, Amaury Triaud, Loïc Trompet, Shang-Min Tsai, Maria Tsantaki, Diana Valencia, Ann Carine Vandaele, Mathieu Van der Swaelmen, Adibekyan Vardan, Gautam Vasisht, Allona Vazan, Ciro Del Vecchio, Dave Waltham, Piotr Wawer, Thomas Widemann, Paulina Wolkenberg, Gordon Hou Yip, Yuk Yung, Mantas Zilinska, Tiziano Zingale, Paola Zuppella, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), and Cardon, Catherine

Subjects
[SDU] Sciences of the Universe [physics], Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Settore FIS/05 - Astronomia E Astrofisica, [SDU]Sciences of the Universe [physics], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysic, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Earth and Planetary Astrophysics, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract

Ariel, the Atmospheric Remote-sensing Infrared Exoplanet Large-survey, was adopted as the fourth medium-class mission in ESA's Cosmic Vision programme to be launched in 2029. During its 4-year mission, Ariel will study what exoplanets are made of, how they formed and how they evolve, by surveying a diverse sample of about 1000 extrasolar planets, simultaneously in visible and infrared wavelengths. It is the first mission dedicated to measuring the chemical composition and thermal structures of hundreds of transiting exoplanets, enabling planetary science far beyond the boundaries of the Solar System. The payload consists of an off-axis Cassegrain telescope (primary mirror 1100 mm x 730 mm ellipse) and two separate instruments (FGS and AIRS) covering simultaneously 0.5-7.8 micron spectral range. The satellite is best placed into an L2 orbit to maximise the thermal stability and the field of regard. The payload module is passively cooled via a series of V-Groove radiators; the detectors for the AIRS are the only items that require active cooling via an active Ne JT cooler. The Ariel payload is developed by a consortium of more than 50 institutes from 16 ESA countries, which include the UK, France, Italy, Belgium, Poland, Spain, Austria, Denmark, Ireland, Portugal, Czech Republic, Hungary, the Netherlands, Sweden, Norway, Estonia, and a NASA contribution., Comment: Ariel Definition Study Report, 147 pages. Reviewed by ESA Science Advisory Structure in November 2020. Original document available at: https://www.cosmos.esa.int/documents/1783156/3267291/Ariel_RedBook_Nov2020.pdf/

Published
2021
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21. Unveiling the obscured universe with SPICA, A joint infrared space observatory

Author

Martin Giard, Hideo Matsuhara, Hidehiro Kaneda, Takashi Onaka, Charles Bradford, Toru Yamada, Franz Kerschbaum, Oliver Krause, Bart Vandenbussche, Jan Tauber, Matt Griffin, Mika Juvela, Frank Helmich, Yasuo Doi, Peter Roelfsema, Marc Audard, Astrid Heske, Jesus Martin-Pintado, Shiang-Yu Wang, Hiroshi Shibai, David Elbaz, Marc Sauvage, Francisco Najarro, Pieter Dieleman, Willem Jellema, Inga Kamp, Gert De Lange, Bengt Larsson, Tohru Nagao, David Naylor, Jacques Rouquet, Luigi Spinoglio, Ryszard Szczerba, Floris van der Tak, and Astronomy

Subjects
Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The mid/far infrared hosts a wealth of spectral information that allows direct determination of the physical state of matter in a large variety of astronomical objects, unhindered by foreground obscuration. Accessing this domain is essential for astronomers to much better grasp the fundamental physical processes underlying the evolution of many types of celestial objects, ranging from protoplanetary systems in our own milky way to 10-12 billion year old galaxies at the high noon of galaxy formation in our universe. The joint ESA/JAXA SPICA space mission will give such access for the astronomical community at large, by providing an observatory with unprecedented mid- to far-infrared imaging, polarimetric and spectroscopic capabilities. With a launch expected to happen in 2032, it will be the ideal complement of the space based (ATHENA) and ground based facilities available at this time (ELT, TMT, ALMA, SKA), so that the entire high energy to radio electromagnetic spectrum will be accessible to world astronomers with unprecedented power and sensitivity. The SPICA mission, under development as a joint ESA/JAXA project, will combine a 2.5-meter diameter telescope cooled to below 8 K with instruments employing state-of-the-art ultra-sensitive detectors. Instead of using liquid cryogen, a combination of passive cooling and mechanical coolers is employed to cool both the telescope and the instruments, allowing the mission lifetime to extend significantly beyond the required three years. SPICA offers spectroscopy instruments with spectral resolving power ranging from R~50 through 11000 in the 17-230 μm domain as well as R~28.000 spectroscopy between 12 and 18 μm. The state-of-the-art Transition Edge Detectors in the 35-230 μm detectors in the SAFARI spectrometer will provide an unprecedented sensitivity of ~5×10−20 W/m2 (5σ/1hr) - at least two orders of magnitude improvement over what has been attained to date. With the 10'x12' large Field of View SMI imager SPICA will be able to very efficiently do sensitive large area 30-37 μm broad band mapping. In addition the B-BOP instrument will provide accurate polarimetric imaging at 70, 220 and 350 μm With this exceptional leap in performance, new domains in infrared astronomy will become accessible, allowing us, for example, to unravel definitively galaxy evolution and metal production over cosmic time, to study dust formation and evolution from very early epochs onwards, and to trace the gas, dust and ice evolution in planetary systems.

Published
2021

22. The SAFARI grating spectrometer for SPICA: Extreme spectroscopic sensitivity in the FAR-IR

Author

Charles M. Bradford, Mika Juvela, Luigi Spinoglio, Martin Giard, Bart Vandenbussche, Floris van der Tak, Oliver Krause, Csaba Kiss, Pieter Dieleman, Franz Kerschbaum, Frank Helmich, R. Szczerba, Stafford Withington, Peter Roelfsema, Willem Jellema, David A. Naylor, Shoko Jin, Marc Audard, Yasuo Doi, Bengt Larsson, Shiang-Yu Wang, Jaap Evers, Francisco Najarro, and Gert de Lange

Subjects
010309 optics, Physics, 0103 physical sciences, Galaxy formation and evolution, Astronomy, 02 engineering and technology, Spica, Sensitivity (control systems), Grating spectrometer, 021001 nanoscience & nanotechnology, 0210 nano-technology, 01 natural sciences, Cosmic dust
Published
2020
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23. The joint infrared space observatory SPICA: unveiling the obscured universe

Author

Willem Jellema, Gert de Lange, Toru Yamada, Takashi Onaka, Francisco Najarro, Marc Sauvage, Shoko Jin, R. Szczerba, Tohru Nagao, Hiroshi Shibai, Stafford Withington, Inga Kamp, Bart Vandenbussche, Takao Nakagawa, Hideko Nomura, Hiroyuki Ogawa, David Elbaz, Matthew Joseph Griffin, Charles M. Bradford, Mika Juvela, Jacques Rouquet, Hideo Matsuhara, Floris van der Tak, Csaba Kiss, Kotaro Kohno, Shiang-Yu Wang, Martin Giard, Pieter Dieleman, Peter Roelfsema, Yasuo Doi, Jesús Martín-Pintado, David A. Naylor, Marc Audard, A. Heske, Jan Tauber, Frank Helmich, Franz Kerschbaum, Hidehiro Kaneda, Bengt Larsson, Mitsuhiko Honda, Luigi Spinoglio, and Oliver Krause

Subjects
Astronomical Objects, Physics, media_common.quotation_subject, Milky Way, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, 02 engineering and technology, Spica, 021001 nanoscience & nanotechnology, 01 natural sciences, Physics::History of Physics, Galaxy, Universe, 010309 optics, Far infrared, Observatory, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Earth and Planetary Astrophysics, 0210 nano-technology, Astrophysics::Galaxy Astrophysics, media_common
Abstract

The mid/far infrared hosts a wealth of spectral information that allows direct determination of the physical state of matter in a large variety of astronomical objects, unhindered by foreground obscuration. Accessing this domain is essential for astronomers to much better grasp the fundamental physical processes underlying the evolution of many types of celestial objects, ranging from protoplanetary systems in our own milky way to 10-12 billion year old galaxies at the high noon of galaxy formation in our universe. The joint ESA/JAXA SPICA mission will give such access for the astronomical community at large, by providing an observatory with unprecedented mid- to far-infrared imaging, polarimetric and spectroscopic capabilities.

Published
2020
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24. On the optical alignment of the PLATO cameras

Author

M. Dami, Davide Greggio, G. Ramos Zapata, Martin Pertenais, Luca Marafatto, Pierre Royer, Rik Huygen, Y. Levillain, S. Regibo, Ann Baeke, Valentina Viotto, M. Pajas, J. De Ridder, Demetrio Magrin, Bart Vandenbussche, Lionel Clermont, Jacopo Farinato, A. L. Valverde Guijarro, and A. Belen Balado Margeli

Subjects
Error estimate, Simulations, Focal plane, Computer science, Payload, business.industry, Optical alignment, Astrophysics::Instrumentation and Methods for Astrophysics, Image plane, Bearing (navigation), PLATO, Field curvature, Exoplanet, law.invention, Telescope, Cardinal point, Optics, Planet, law, Cryo-vacuum test, Astrophysics::Earth and Planetary Astrophysics, business, Petzval field curvature
Abstract

PLATO is an exoplanet hunting mission from the European Space Agency. It is a medium-class mission, with alaunch foreseen in 2026. Its prime objective is to uncover Earth-sized planets residing in the habitable zone of theirhost star. The payload consists of 26 cameras with a very wide field-of-view. While the operational temperatureof the cameras will be−80◦C, the focal plane of each camera will be integrated with its telescope assembly(bearing the optics) at room temperature. The degradation of the optical quality at ambient, combined with thedetector dark current and with the very high accuracy required from the alignment process bring a number ofinteresting challenges. In the present article, we review the alignment concept, present optical simulations of themeasurements at ambient along with their analysis, and present an error budget for the optical measurements.The derivation of this error budget is easily applicable to all optical measurements to be performed during thealignment, i.e. the definition of the best image plane at the operational temperature and the optical alignmentitself, at room temperature.

Published
2020
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25. A white light collimator for Plato camera integration support

Author

Lionel Clermont, Ann Baeke, Alexandre Cabral, Bart Vandenbussche, João Coelho, Pedro Santos, David Castro Alves, and Manuel Abreu

Subjects
Computer science, business.industry, Aperture, Process (computing), Collimator, law.invention, Telescope, Optics, Cardinal point, law, business, Focus (optics), Adaptive optics, Beam (structure)
Abstract

A fiber fed, wide beam collimator was developed as a tool to support the Assembly, Integration and Verification (AIV) tasks associated to the integration of the ESA-PLATO telescope unit (TOU) to the focal plane, for the 26 cameras that are going to be assembled at the Centre Spatial de Liege (CSL). This collimator will work as source for the alignment process at ambient temperature, providing a white light beam that must comply with a series of critical requirements, namely high spatial uniformity over an clear aperture of 150 mm (better than 85%), Wavefront Error associated to focus aberration at the level of λ/30 rms and high flux stability over time (2% in 24h). This paper will present the steps taken towards the development, manufacture and integration of this collimator, as well as the tests devised to evaluate requirements compliance.

Published
2020
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26. Design of the electrical ground support equipment for the PLATO camera AIV

Author

Bart Vandenbussche, Pierre Royer, Rik Huygen, C. Ruiz de Galarreta Fanjul, and S. Regibo

Subjects
Scheme (programming language), Ground support equipment, Ground, Payload, business.industry, Computer science, computer.software_genre, law.invention, Software framework, Telescope, law, Computer data storage, business, Host (network), computer, Computer hardware, computer.programming_language
Abstract

PLATO is an ESA mission to hunt for Earth-sized exoplanets in the habitable zone of their host star. The heart of the payload consists of 26 wide-field cameras. We develop a Common Electrical Ground Support Equipment (EGSE) framework for the testing and verification of these cameras. The focal planes are aligned to the telescope optics at ambient temperature and the performance verification is done at operational temperature in thermal-vacuum conditions in different facilities. The Common-EGSE system will guarantee that tests are executed via the same procedures and are analyzed identically, by providing a software framework that can be tuned for site-specific hardware and avoids duplicate developments. The Common EGSE provides commanding for the camera and the Ground Support Equipment (GSE), telemetry monitoring, logging, data storage, and data analysis. In addition, the design allows for sharing commanding and analysis scripts. We present the design of the system and the generic commanding scheme for test setup hardware.

Published
2020
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27. CUBESPEC: Stellar spectroscopy on a CubeSat platform

Author

Wim De Munter, Owais Ahmad Bhat, Pierre Royer, V. Moreau, Jacob Mølbach Nissen, Tjorven Delabie, Andrew Tkachenko, Filip Heylen, Gert Raskin, Bart Vandenbussche, Jelle Lanting, Warre Verheyden, Hugues Sana, Ries Vanderperren, Dominik Bowman, jan Goris, Leonardo Ghizoni, Jeroen De Maeyer, Olivier Verhamme, Bram Vandoren, Dirk Vandepitte, Etienne Renotte, Arne Verhoeven, and Maarten Kempenaers

Subjects
Physics, Spacecraft, business.industry, Payload, Astrophysics::Instrumentation and Methods for Astrophysics, Cassegrain reflector, Primary mirror, Optics, CubeSat, Astrophysics::Earth and Planetary Astrophysics, Spectral resolution, business, Spectroscopy, Spectrograph
Abstract

CUBESPEC is an ESA in-orbit demonstration 6U CubeSat mission, currently in phase A/B. CUBESPEC will deliver months long series of high-resolution spectroscopy to study the structure of massive stars. The payload consists of a Cassegrain telescope with a rectangular primary mirror of 9 x 19 cm2 and a compact high-resolution echelle spectrograph. We aim at a 2023 launch demonstrating the CUBESPEC concept: providing the astronomical community with a generic solution for affordable space-based spectroscopy. The spectrograph design can be configured with minimal hardware changes for low spectral resolution (R = 50) up to high resolution (R ~ 50000) over a over wavelength ranges between 200–1000nm. CUBESPEC will use the KU Leuven ADCS for coarse pointing of the spacecraft, supplemented with a fine-guidance system using a fast steering mirror to center the source on the spectrograph slit. We present the CUBESPEC design and mission analysis, and give an update of the project status.

Published
2020
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28. MARVEL, a four-telescope array for high-precision radial-velocity monitoring

Author

Ignasi Ribas, S. Halverson, Hugues Sana, S. Prins, G. Avila, Bart Vandenbussche, J. Perez Padilla, J. Stuermer, L. Decin, Manuel Guedel, Denis Defrere, A. Glasse, Don Pollacco, Andrew Tkachenko, Lars A. Buchhave, David H. Atkinson, Giovanna Tinetti, Alexis Brandeker, Pierre Royer, Cyprien Lanthermann, Gert Raskin, Jacob Pember, J. De Ridder, H. Van Winckel, Christian Schwab, Johan Morren, Evans, CJ, Bryant, JJ, Motohara, K, Evans, Christopher J., Bryant, Julia J., and Motohara, Kentaro

Subjects
Physics, Radial velocity, Optical fiber, Spectrograph, media_common.quotation_subject, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy, Exoplanet, Space exploration, law.invention, Telescope, Planet, Observatory, law, Sky, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Telescopes, media_common
Abstract

Since the first discovery of a planet outside of our Solar System in 1995, exoplanet research has shifted from detecting to characterizing worlds around other stars. The TESS (NASA, launched 2019) and PLATO mission (ESA, planned launch 2026) will find and constrain the size of thousands of exoplanets around bright stars all over the sky. Radial velocity measurements are needed to characterize the orbit and mass, and complete the picture of densities and composition of the exoplanet systems found. The Ariel mission (ESA, planned launch 2028) will characterize exoplanet atmospheres with infrared spectroscopy. Characterization of stellar activity using optical spectroscopy from the ground is key to retrieve the spectral footprint of the planetary atmosphere in Ariel's spectra. To enable the scientific harvest of the TESS, PLATO and Ariel space missions, we plan to install MARVEL as an extension of the existing Mercator Telescope at the Roque De Los Muchachos Observatory on La Palma (SPAIN). MARVEL consists of an array of four 80 cm telescopes linked through optical fibers to a single high-resolution echelle spectrograph, optimized for extreme-precision radial velocity measurements. It can observe the radial velocities of four different stars simultaneously or, alternatively, combine the flux from four telescopes pointing to a single faint target in one spectrum. MARVEL is constructed by a KU Leuven (Belgium) led collaboration, with contributions from the UK, Austria, Australia, Sweden, Denmark and Spain. In this paper, we present the MARVEL instrument with special focus on the optical design and expected performance of the spectrograph, and report on the status of the project., SPIE Astronomical Telescopes + Instrumentation 2020, Ground-based and Airborne Instrumentation for Astronomy VIII

Published
2020
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29. Optimizing MARVEL for the radial velocity follow up of TESS and PLATO transiting exoplanets

Author

Andrew Tkachenko, Christian Schwab, Hans Van Winckel, Pierre Royer, Denis Defrere, Cyprien Lanthermann, Joris De Ridder, Gert Raskin, Hugues Sana, Bart Vandenbussche, Adler, DS, Seaman, RL, and Benn, CR

Subjects
Radial velocity, Stars, Computer science, Sky, Planet, media_common.quotation_subject, Orbit (dynamics), Astronomy, Astrophysics::Earth and Planetary Astrophysics, Transit (astronomy), Space exploration, Exoplanet, media_common
Abstract

The space missions TESS and PLATO plan to double the number of 4000 exoplanets already discovered and will measure the size of thousands of exoplanets around the brightest stars in the sky, allowing ground-based radial velocity spectroscopy follow-up to determine the orbit and mass of the detected planets. The new facility we are developing, MARVEL (Raskin et al. this conference1 ), will enable the ground-based follow-up of large numbers of exoplanet detections expected from TESS and PLATO, which cannot be carried out only by the current facilities that achieve the necessary radial velocity accuracy of 1 ms-1 or less. This paper presents the MARVEL observation strategy and performance analysis based on predicted PLATO transit detection yield simulations. The resulting observation scenario baseline will help in the instrument design choices and demonstrate the effectiveness of MARVEL as a TESS and PLATO science enabling facility.

Published
2020

30. The CubeSpec space mission

Author

Andrew Tkachenko, Stefano Garcia, Dominic M. Bowman, Bram Vandoren, T. Van Reeth, Gert Raskin, Bart Vandenbussche, Pierre Royer, Tjorven Delabie, and Hugues Sana

Subjects
oscillations [stars], Astronomy, CANIS-MAJORIS VARIABLES, FOS: Physical sciences, Context (language use), asteroseismology, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, LINE-PROFILE VARIATIONS, Asteroseismology, early-type [stars], Photometry (optics), M-CIRCLE-DOT, massive [stars], BETA-CEPHEI-STAR, Astrophysics::Solar and Stellar Astrophysics, CubeSat, COMPLEX ASTEROSEISMOLOGY, Instrumentation and Methods for Astrophysics (astro-ph.IM), Spectrograph, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, Science & Technology, UNIVERSITY STELLAR INTERFEROMETER, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Stars, MOMENT METHOD, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Physical Sciences, Magnitude (astronomy), B-TYPE STARS, Satellite, NONRADIAL PULSATION MODES, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, NU-ERIDANI, spectrographs [instrumentation]
Abstract

Context. There is currently a niche for providing high-cadence, high resolution, time-series optical spectroscopy from space, which can be filled by using a low-cost cubesat mission. The Belgian-led ESA CubeSpec mission is specifically designed to provide space-based, low-cost spectroscopy with specific capabilities that can be optimised for a particular science need. Approved as an ESA in-orbit demonstrator, the CubeSpec satellite's primary science objective will focus on obtaining high-cadence, high resolution optical spectroscopic data to facilitate asteroseismology of pulsating massive stars. Aims. In this first paper, we aim to search for pulsating massive stars suitable for the CubeSpec mission, specifically $\beta$ Cep stars, which typically require time series spectroscopy to identify the geometry of their pulsation modes. Methods. Based on the science requirements needed to enable asteroseismology of massive stars with the capabilities of CubeSpec's spectrograph, we combine a literature study for pulsation with the analysis of recent high-cadence time series TESS photometry to classify the variability for stars brighter than V < 4 mag and between O9 and B3 in spectral type. Results. Among the 90 stars that meet our magnitude and spectral type requirements, we identify 23 promising $\beta$ Cep stars with high-amplitude (non-)radial pulsation modes with frequencies below 7 d$^{-1}$. Using further constraints on projected rotational velocities, pulsation amplitudes and number of pulsation modes, we devise a prioritised target list for the CubeSpec mission according to its science requirements and the potential of the targets for asteroseismology. The full target catalogue further provide a modern TESS-based review of line profile and photometric variability properties among bright O9-B3 stars., Comment: 14 pages, accepted for publication in A&A

Published
2022
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31. Stellar pulsation and granulation as noise sources in exoplanet transit spectroscopy in the ARIEL space mission

Author

Andreas Papageorgiou, Subhajit Sarkar, Bart Vandenbussche, Ioannis Argyriou, and Enzo Pascale

Subjects
Stars: activity, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Infrared: planetary systems, Space vehicles: instruments, 01 natural sciences, Spitzer Space Telescope, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Transit (astronomy), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Scale height, Exoplanet, Stars, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Stellar pulsation, Noise (radio), Astrophysics - Earth and Planetary Astrophysics
Abstract

© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. Stellar variability from pulsations and granulation presents a source of correlated noise that can impact the accuracy and precision of multiband photometric transit observations of exoplanets. This can potentially cause biased measurements in the transmission or emission spectrum or underestimation of the final error bars on the spectrum. ARIEL is a future space telescope and instrument designed to perform a transit spectroscopic survey of a large sample of exoplanets. In this paper, we perform simulations to assess the impact of stellar variability arising from pulsations and granulation on ARIEL observations of GJ 1214b and HD 209458b.We take into account the correlated nature of stellar noise, quantify it, and compare it to photon noise. In the range 1.95-7.8 μm, stellar pulsation and granulation noise has insignificant impact compared to photon noise for both targets. In the visual range, the contribution increases significantly but remains small in absolute terms and will have minimal impact on the transmission spectra of the targets studied. The impact of pulsation and granulation will be greatest for planets with low scale height atmospheres and long transit times around bright stars. ispartof: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY vol:481 issue:3 pages:2871-2877 status: published

Published
2018
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32. Wavelength calibration and resolving power of the JWST MIRI Medium Resolution Spectrometer

Author

Adrian Glauser, J. Alvarez-Marquez, David R. Law, Bart Vandenbussche, Bernhard R. Brandl, Polychronis Patapis, B. Shaughnessy, Alistair Glasse, Alvaro Labiano, Fred Lahuis, Michael Mueller, Pierre Royer, Kay Justtanont, Alberto Noriega-Crespo, Juan Rafael Martínez-Galarza, and Ioannis Argyriou

Subjects
Physics::Instrumentation and Detectors, FOS: Physical sciences, Instrumentation: spectrographs, MIDINFRARED INSTRUMENT, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, Computer Science::Digital Libraries, Spectral line, Infrared: general, THERMAL-EXPANSION MEASUREMENTS, Integral field spectrograph, Optics, Methods: data analysis, data analysis [methods], Instrumentation: detectors, Spectral resolution, Spectroscopy, Instrumentation and Methods for Astrophysics (astro-ph.IM), general [infrared], TEMPERATURE, Solar and Stellar Astrophysics (astro-ph.SR), Earth and Planetary Astrophysics (astro-ph.EP), Physics, Science & Technology, detectors [instrumentation], Spectrometer, Pixel, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, WEBB-SPACE-TELESCOPE, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Physics::History of Physics, Wavelength, IV, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Physical Sciences, Astrophysics - Instrumentation and Methods for Astrophysics, business, Fabry–Pérot interferometer, spectrographs [instrumentation], Astrophysics - Earth and Planetary Astrophysics
Abstract

The Mid-Infrared Instrument (MIRI) on-board JWST will provide imaging, coronagraphy, low-resolution spectroscopy and medium-resolution spectroscopy at unprecedented sensitivity levels in the mid-infrared wavelength range. The Medium-Resolution Spectrometer (MRS) of MIRI is an integral field spectrograph that provides diffraction-limited spectroscopy between 4.9 and 28.3 um, within a FOV varying from 13 to 56" square. From ground testing, we calculate the physical parameters essential to general observers and calibrating the wavelength solution and resolving power of the MRS is critical for maximising the scientific performance of the instrument. We have used ground-based observations of discrete spectral features in combination with Fabry-Perot etalon spectra to characterize the wavelength solution and spectral resolving power of the MRS. We present the methodology used to derive the MRS spectral characterisation, which includes the precise wavelength coverage of each MRS sub-band, computation of the resolving power as a function of wavelength, and measuring slice-dependent spectral distortions. The resolving power varies from R3500 in channel 1 to R1500 in channel 4. Based on the ground test data, the wavelength calibration accuracy is estimated to be below one tenth of a pixel, with small systematic shifts due to the target position within a slice for unresolved sources, that have a maximum amplitude of about 0.25 spectral resolution elements. Based on ground test data, the MRS complies with the spectral requirements for both the R and wavelength accuracy for which it was designed. We also present the commissioning strategies and targets that will be followed to update the spectral characterisation of the MRS., 13 pages. Accepted for publication in A&A

Published
2021
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33. an integrated payload design for the atmospheric remote-sensing infrared exoplanet large-survey (ARIEL): results from phase A and forward look to phase B1

Author

Jean-Philippe Beaulieu, Miroslaw Rataj, Emanuele Pace, T. Hunt, Georgia Bishop, Isabel Escudero Sanz, Bart Vandenbussche, Manuel Güdel, Tom Ray, Gianluca Morgante, Kevin Middleton, Paul Hartogh, Paul Eccleston, J.-L. Auguères, Ignasi Ribas, Giuseppina Micela, Mauro Focardi, Giuseppe Malaguti, Marc Ollivier, Enzo Pascale, Giovanna Tinetti, Michiel Min, William Taylor, Vania Da Deppo, University College of London [London] (UCL), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut für Astrophysik [Wien], Universität Wien, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Dpto. de Organización de Empresas, Escuela Técnica Superior de Ingeniería Industrial de Barcelona, Universitat Politècnica de Catalunya [Barcelona] (UPC), CNR Institute for Photonics and Nanotechnologies (IFN), Consiglio Nazionale delle Ricerche [Roma] (CNR), Instituto Italiano di Tecnologia (IIT), Ministero dell'Istruzione-Ministero dell'Economia e Finanze, Institut de Génomique Fonctionnelle de Lyon (IGFL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Recherche Agronomique (INRA)-École normale supérieure - Lyon (ENS Lyon), Cardiff University, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Institut National de la Recherche Agronomique (INRA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), and École normale supérieure de Lyon (ENS de Lyon)-Institut National de la Recherche Agronomique (INRA)-Université Claude Bernard Lyon 1 (UCBL)

Subjects
[PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astronomy, Space, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, law.invention, Telescope, law, 0103 physical sciences, 010303 astronomy & astrophysics, Transit (satellite), Instrumentation, Astrophysics::Galaxy Astrophysics, Spectroscopy, Remote sensing, Integrated design, Spectrometer, 010308 nuclear & particles physics, Payload, Atmosphere, Exoplanets, Astrophysics::Instrumentation and Methods for Astrophysics, Photometer, Exoplanet, 13. Climate action, Orbit (dynamics), Astrophysics::Earth and Planetary Astrophysics, Transit, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; ARIEL (the Atmospheric Remote-sensing Infrared Exoplanet Large-survey) has been selected by ESA as the next medium-class science mission (M4), expected to be launched in 2028. The mission will be devoted to observing spectroscopically in the infrared a large population of warm and hot transiting exoplanets (temperatures from 500 K to 3000 K) in our nearby Galactic neighborhood, opening a new discovery space in the field of extrasolar planets and enabling the understanding of the physics and chemistry of these far away worlds. ARIEL was selected for implementation by ESA in March 2018 from three candidate missions that underwent parallel phase A studies. This paper gives an overview of the design at the end of phase A and discusses plans for its evolution during phase B1, in the run-up to mission adoption. ARIEL is based on a 1 m class telescope feeding two instruments: a moderate resolution spectrometer covering the wavelengths from 1.95 to 7.8 microns; and a three-channel photometer (which also acts as a fine guidance sensor) with bands between 0.5 and 1.2 microns combined with a low resolution spectrometer covering 1.25 to 1.9 microns. During its 3.5 years of operation from an L2 orbit, ARIEL will continuously observe exoplanets transiting their host star. This paper presents an overall view of the integrated design of the payload proposed for this mission. The design tightly integrates the various payload elements in order to allow the exacting photometric stability targets to be met, while providing simultaneous spectral and photometric data from the visible to the mid-infrared. We identify and discuss the key requirements and technical challenges for the payload and describe the trade-offs that were assessed during phase A, culminating in the baseline design for phase B1. We show how the design will be taken forward to produce a fully integrated and calibrated payload for ARIEL that can be built within the mission and programmatic constraints and will meet the challenging scientific performance required for transit spectroscopy.

Published
2018
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34. Automatized alignment of the focal plane assemblies on the PLATO cameras

Author

Pascal Blain, Lionel Clermont, Rik Huygen, Pierre Royer, Bart Vandenbussche, Jérôme Jacobs, Ann Baeke, Jean-Philippe Halain, and Manuel Abreu

Subjects
Cosmic Vision, Pixel, Computer science, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Process (computing), Planetary system, Translation (geometry), Collimated light, Cardinal point, Optics, Astrophysics::Earth and Planetary Astrophysics, Focus (optics), business
Abstract

PLATO (PLAnetary Transits and Oscillation of stars) is a medium-class space mission part of the ESA Cosmic vision program. Its goal is to find and study extrasolar planetary systems, emphasizing on planets located in habitable zone around solar-like stars. PLATO is equipped with 26 cameras, operating between 500 and 1000nm. The alignment of the focal plane assembly (FPA) with the optical assembly is a time consuming process, to be performed for each of the 26 cameras. An automatized method has been developed to fasten this process. The principle of the alignment is to illuminate the camera with a collimated beam and to vary the position of the FPA to search for the position which minimizes the RMS spot diameter. To reduce the total number of measurements which is performed, the alignment method is done by iteratively searching for the best focus, decreasing at each step the error on the estimated best focus by a factor 2. Because the spot size at focus is similar to the pixel, it would not be possible with this process alone to reach an alignment accuracy of less than several tens of microns. Dithering, achieved by in-plane translation of the focal plane and image recombination, is thus used to increase the sampling of the spot and decrease the error on the merit function.

Published
2018
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35. SPICA: a joint infrared space observatory (Conference Presentation)

Author

Luigi Spinoglio, Martin Giard, Oliver Krause, Floris van der Tak, Hideo Matsuhara, Francisco Najarro, Bart Vandenbussche, Matthew Joseph Griffin, Kees Wafelbakker, Gert de Lange, Sue Madden, Ciska Kemper, Franz Kerschbaum, Yasuo Doi, Kotaro Kohno, Toru Yamada, Hidehiro Kaneda, Marc Audard, David A. Naylor, Charles M. Bradford, Takashi Onaka, Frank Helmich, Hiroshi Shibai, Lee Armus, Bengt Larsson, Inga Kamp, Takao Nakagawa, Hiroyuki Ogawa, and Peter Roelfsema

Subjects
Physics, Infrared astronomy, Milky Way, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Spica, Planetary system, Galaxy, law.invention, Telescope, law, Galaxy formation and evolution, Astrophysics::Earth and Planetary Astrophysics, Stellar evolution, Astrophysics::Galaxy Astrophysics
Abstract

Measurements in the infrared wavelength domain allow us to assess directly the physical state and energy balance of cool matter in space, thus enabling the detailed study of the various processes that govern the formation and early evolution of stars and planetary systems in the Milky Way and of galaxies over cosmic time. Previous infrared missions, from IRAS to Herschel, have revealed a great deal about the obscured Universe, but sensitivity has been limited because up to now it has not been possible to fly a telescope that is both large and cold. Such a facility is essential to address key astrophysical questions, especially concerning galaxy evolution and the development of planetary systems. SPICA is a mission concept aimed at taking the next step in mid- and far-infrared observational capability by combining a large and cold telescope with instruments employing state-of-the-art ultra-sensitive detectors. The mission concept foresees a 2.5-meter diameter telescope cooled to below 8 K. Rather than using liquid cryogen, a combination of passive cooling and mechanical coolers will be used to cool both the telescope and the instruments. With cooling not dependent on a limited cryogen supply, the mission lifetime can extend significantly beyond the required three years. The combination of low telescope background and instruments with state-of-the-art detectors means that SPICA can provide a huge advance on the capabilities of previous missions. The SPICA instrument complement offers spectral resolving power ranging from ~50 through 11000 in the 17-230 µm domain as well as ~28.000 spectroscopy between 12 and 18 µm. Additionally, SPICA will be capable of efficient 30-37 µm broad band mapping, and small field spectroscopic and polarimetric imaging in the 100-350 µm range. SPICA will enable far infrared spectroscopy with an unprecedented sensitivity of ~5x10-20 W/m2 (5σ/1hr) - at least two orders of magnitude improvement over what has been attained to date. With this exceptional leap in performance, new domains in infrared astronomy will become accessible, allowing us, for example, to unravel definitively galaxy evolution and metal production over cosmic time, to study dust formation and evolution from very early epochs onwards, and to trace the formation history of planetary systems.

Published
2018
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36. The SAFARI grating spectrometer for the SPICA space observatory (Conference Presentation)

Author

Charles M. Bradford, Martin Giard, Jian-Rong Gao, Matthew Joseph Griffin, Gert de Lange, Bart Vandenbussche, Franz Kerschbaum, Brian Jackson, Marc Audard, Francisco Najarro, David A. Naylor, Jonas Zmuidzinas, Peter Roelfsema, Albrecht Poglitch, Willem Jellema, and Kees Wafelbakker

Subjects
Physics, Telescope, Interferometry, Far infrared, Spectrometer, Observatory, law, Infrared telescope, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Spica, Spectral resolution, law.invention
Abstract

The European/Japanese SPace Infrared telescope for Cosmology and Astrophysics, SPICA, will provide astronomers with a long awaited new window on the universe. Having a large cold telescope cooled to less than 8K above absolute zero, SPICA will provide a unique environment where instruments are limited only by the cosmic background itself. A consortium of European, north American and Asian institutes has been established to design and implement the SpicA FAR infrared Instrument SAFARI, an extremely sensitive spectrometer designed to fully exploit this extremely low far infrared background environment provided by the SPICA observatory. SAFARI’s extremely sensitive Transition Edge Sensing detectors will allow astronomers to very efficiently obtain moderate to high resolution spectra of many thousands of obscured celestial objects in the far infrared, allowing a full spectroscopic characterisation of this objects. Efficiently obtaining such a large number of complete spectra will be essential to address several fundamental questions in current astrophysics: how do galaxies form and evolve over cosmic time?, what is the true nature of our own Milky Way?, and why and where do planets like those in our own solar system come into being? The basic SAFARI instrument is a highly sensitive Grating Spectrometer with a spectral resolution R of about 300 and a line sensitivity of a few x 10^-20 W/√Hz (5σ-1h). By routing the signal through a Martin-Puplett interferometer a high resolution mode is implemented providing R~11000 at 34 μm to R~1500 at 230 μm. The instrument operates in four wavelength bands, simultaneously covering the full 34-230μm range. Each band has three arrays of about 300 TES sensors providing three spatial and 300 spectral outputs. To limit the number of signal wires between the cold focal plan and the warm electronics units a 160 pixel/channel Frequency Domain Multiplexing scheme is employed.

Published
2018
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37. Fringing solution for the mid-infrared instrument on-board the James Webb Space Telescope

Author

Martyn Wells, Ioannis Argyriou, and Bart Vandenbussche

Subjects
Physics, Spectrometer, Physics::Instrumentation and Detectors, business.industry, Detector, James Webb Space Telescope, Astrophysics::Instrumentation and Methods for Astrophysics, Context (language use), Fresnel equations, Optics, Reflection (physics), business, Fabry–Pérot interferometer, Data reduction
Abstract

The Mid-Infrared Instrument (MIRI) on-board the James Webb Space Telescope (JWST) performs medium resolution spectroscopy in the 5 to 28.5micron wavelength range. The Medium-Resolution Spectrometer (MRS) of MIRI uses two Si:As impurity band conduction detector arrays. Coherent reflection of infrared light within the MIRI MRS detectors results in fringing; the detector layers act as efficient Fabry-Perot etalons. In this paper we present three methods to calibrate out the fringes, as part of the MIRI data reduction pipeline. The methods are presented in the context of the investigations on the fringing seen in the MIRI flight model ground test data. The investigations show that the detector fringe transmission depends on the illumination pattern of the observed source on the detector. Optical stimuli of different spatial extents and position in the field-of-view yield different fringe patterns in their extracted spectra. An optical model of the MIRI detectors is hence proposed. By solving the Fresnel equations across the model optical layers, a source-specific fringe correction is derived.

Published
2018
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38. Spectrum extraction from detector plane images for the medium-resolution spectrometer of the mid-Infrared Instrument on-board the James Webb Space Telescope

Author

Bart Vandenbussche, Ioannis Argyriou, and Ruyman Azzollini

Subjects
Physics, Photometry (optics), Point spread function, Optics, Spectrometer, Pixel, business.industry, Detector, James Webb Space Telescope, Astrophysics::Instrumentation and Methods for Astrophysics, business, Spectroscopy, Spectral line
Abstract

The Mid-Infrared Instrument (MIRI) on-board the James Webb Space Telescope (JWST) performs mediumresolution spectroscopy in the 5 to 28.5micron wavelength range. In this paper two algorithms are presented that will be used to extract 1D spectra from the 2D absolutely calibrated detector science frames acquired with the Medium-Resolution Spectrometer (MRS) of MIRI. The first spectral extraction algorithm performs standard aperture photometry on point and extended sources. The second algorithm, applicable only to point sources, uses the instrument point spread function (PSF) and the pixel signal variance as a weighting function, to extract the signal from the detector pixels in an optimized way. This "optimal" extraction is also optimal in the case of faint source observations. The two algorithms are tested on MIRI ground test data and compared. For point sources, the optimal extraction algorithm is found to be more reliable than the aperture extraction algorithm.

Published
2018
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39. Testing and calibrating an advanced cubesat attitude determination and control system

Author

Tjorven Delabie, Wim De Munter, Bart Vandenbussche, Dirk Vandepitte, Gert Raskin, Bram Vandoren, Lystrup, M, MacEwen, HA, and Fazio, GG

Subjects
010309 optics, Computer science, Attitude determination, Control system, 0103 physical sciences, CubeSat, Control engineering, 02 engineering and technology, 021001 nanoscience & nanotechnology, 0210 nano-technology, 01 natural sciences
Abstract

© COPYRIGHT SPIE. Downloading of the abstract is permitted for personal use only. CubeSat technology is evolving rapidly. With the increased performance of these small spacecraft platforms, astronomical missions on CubeSats will be flown in the near future. These types of missions have very demanding requirements in terms of spacecraft pointing. At the KU Leuven university, we have developed a compact, highaccuracy attitude determination and control system for CubeSats. The system uses three reaction wheels and a star tracker to deliver high agility and accuracy. In this paper, we will discuss the test and calibration campaign that was carried out. This campaign was instrumental in achieving the performance required by astronomical missions. ispartof: SPACE TELESCOPES AND INSTRUMENTATION 2018: OPTICAL, INFRARED, AND MILLIMETER WAVE vol:10698 ispartof: Conference on Space Telescopes and Instrumentation - Optical, Infrared, and Millimeter Wave location:Austin, TX date:10 Jun - 15 Jun 2018 status: published

Published
2018
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40. The phase a study of the ESA M4 mission candidate ARIEL

Author

Paul Eccleston, Kate Symonds, Jérémy Leconte, Paulina Wolkenberg, I. Escudero, Göran Pilbratt, Paul Hartogh, Giovanna Tinetti, Diego Turrini, R. Kohley, Bram de Vogeleer, Giuseppina Micela, A. Heske, Bart Vandenbussche, Pierre-Elie Crouzet, Pierre Drossart, L. Puig, Marc Ollivier, University of Valencia, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, ECLIPSE 2018, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Institut de Génomique Fonctionnelle de Lyon (IGFL), École normale supérieure - Lyon (ENS Lyon)-Institut National de la Recherche Agronomique (INRA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), University College of London [London] (UCL), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk (PAN), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Recherche Agronomique (INRA)-École normale supérieure - Lyon (ENS Lyon), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), École normale supérieure de Lyon (ENS de Lyon)-Institut National de la Recherche Agronomique (INRA)-Université Claude Bernard Lyon 1 (UCBL), and National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR)

Subjects
Engineering, Solar System, Cosmic Vision, 010308 nuclear & particles physics, business.industry, Jupiter (rocket family), [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astronomy and Astrophysics, Context (language use), Planetary system, 7. Clean energy, 01 natural sciences, Exoplanet, Planetary science, Aeronautics, 13. Climate action, Space and Planetary Science, 0103 physical sciences, business, 010303 astronomy & astrophysics, Transit (satellite)
Abstract

© 2018, The Author(s). ARIEL, the Atmospheric Remote sensing Infrared Exoplanet Large survey, is one of the three M-class mission candidates competing for the M4 launch slot within the Cosmic Vision science programme of the European Space Agency (ESA). As such, ARIEL has been the subject of a Phase A study that involved European industry, research institutes and universities from ESA member states. This study is now completed and the M4 down-selection is expected to be concluded in November 2017. ARIEL is a concept for a dedicated mission to measure the chemical composition and structure of hundreds of exoplanet atmospheres using the technique of transit spectroscopy. ARIEL targets extend from gas giants (Jupiter or Neptune-like) to super-Earths in the very hot to warm zones of F to M-type host stars, opening up the way to large-scale, comparative planetology that would place our own Solar System in the context of other planetary systems in the Milky Way. A technical and programmatic review of the ARIEL mission was performed between February and May 2017, with the objective of assessing the readiness of the mission to progress to the Phase B1 study. No critical issues were identified and the mission was deemed technically feasible within the M4 programmatic boundary conditions. In this paper we give an overview of the final mission concept for ARIEL as of the end of the Phase A study, from scientific, technical and operational perspectives. ispartof: EXPERIMENTAL ASTRONOMY vol:46 issue:1 pages:211-239 status: published

Published
2018
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41. The Mid-Infrared Instrument for theJames Webb Space Telescope, IX: Predicted Sensitivity

Author

George H. Rieke, Bart Vandenbussche, Alistair Glasse, E. Bauwens, Michael E. Ressler, Tuomo Tikkanen, Macarena Garcia-Marin, Steffen Rost, and G. S. Wright

Subjects
Physics, Photon, Spectrometer, James Webb Space Telescope, Detector, Mid infrared, FOS: Physical sciences, Astronomy and Astrophysics, Transmission (telecommunications), Space and Planetary Science, Flight model, Sensitivity (control systems), Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Remote sensing
Abstract

We present an estimate of the performance that will be achieved during on orbit operations of the JWST Mid Infrared Instrument, MIRI. The efficiency of the main imager and spectrometer systems in detecting photons from an astronomical target are presented, based on measurements at sub-system and instrument level testing, with the end-to-end transmission budget discussed in some detail. The brightest target fluxes that can be measured without saturating the detectors are provided. The sensitivity for long duration observations of faint sources is presented in terms of the target flux required to achieve a signal to noise ratio of 10 after a 10,000 second observation. The algorithms used in the sensitivity model are presented, including the understanding gained during testing of the MIRI Flight Model and flight-like detectors.

Published
2015
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42. An Accurate and Efficient Gaussian Fit Centroiding Algorithm for Star Trackers

Author

Bart Vandenbussche, Tjorven Delabie, and Joris De Schutter

Subjects
Pixel, Aerospace Engineering, Centroid, Star (graph theory), Hybrid algorithm, Star tracker, Power (physics), symbols.namesake, Space and Planetary Science, symbols, Gaussian function, Gaussian grid, Algorithm, Mathematics
Abstract

This paper presents a novel centroiding algorithm for star trackers. The proposed algorithm, which is referred to as the Gaussian Grid algorithm, fits an elliptical Gaussian function to the measured pixel data and derives explicit expressions to determine the centroids of the stars. In tests, the algorithm proved to yield accuracy comparable to that of the most accurate existing algorithms, while being significantly less computationally intensive. Hence, the Gaussian Grid algorithm can deliver high centroiding accuracy to spacecraft with limited computational power. Furthermore, a hybrid algorithm is proposed in which the Gaussian Grid algorithm yields an accurate initial estimate for a least squares fitting method, resulting in a reduced number of iterations and hence reduced computational cost. The low computational cost allows to improve performance by acquiring the attitude estimates at a higher rate or use more stars in the estimation algorithms. It is also a valuable contribution to the expanding field of small satellites, where it could enable low-cost platforms to have highly accurate attitude estimation.

Published
2014
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43. Highly Efficient Attitude-Estimation Algorithm for Star Trackers Using Optimal Image Matching

Author

Joris De Schutter, Bart Vandenbussche, and Tjorven Delabie

Subjects
Track algorithm, BitTorrent tracker, Iterative method, Applied Mathematics, Aerospace Engineering, A* search algorithm, Computer Science::Computers and Society, Star tracker, law.invention, Reduction (complexity), Geographic coordinate conversion, Space and Planetary Science, Control and Systems Engineering, law, Singular value decomposition, Electrical and Electronic Engineering, Algorithm, Mathematics
Abstract

This paper presents a novel attitude-estimation algorithm for spacecraft using a star tracker. The algorithm is based on an efficient approach to match the stars of two images optimally on top of each other, hence the name of the algorithm: attitude estimation using image matching. In tests, attitude estimation using image matching proved to be as robust as the most robust existing methods, and faster than the fast iterative methods. On top of this, attitude estimation using image matching allows, in a lot of cases, the elimination of a computationally intensive coordinate conversion, which normally precedes the attitude-estimation algorithm. The computational cost of this conversion step is several times higher than that of the attitude-estimation algorithm itself, and so this elimination yields a huge increase in efficiency as compared to the existing algorithms. This significant reduction in computational cost allows to obtain the attitude estimates at a higher rate, implement more accurate centroiding...

Published
2013
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44. The enigmatic nature of the circumstellar envelope and bow shock surrounding Betelgeuse as revealed by Herschel

Author

Pierre Royer, Nick L. J. Cox, Leen Decin, A. J. van Marle, and Bart Vandenbussche

Subjects
Betelgeuse, Physics, Astrophysics::High Energy Astrophysical Phenomena, General Engineering, Astronomy, Astronomy and Astrophysics, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Radius, Astrophysics, Circumstellar envelope, Interstellar medium, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Red supergiant, Bow shock (aerodynamics), Astrophysics::Galaxy Astrophysics, Convection cell
Abstract

Context. The interaction between stellar winds and the interstellar medium (ISM) can create complex bow shocks. The photometers on board the Herschel Space Observatory are ideally suited to studying the morphologies of these bow shocks. Aims. We aim to study the circumstellar environment and wind-ISM interaction of the nearest red supergiant, Betelgeuse. Methods.Herschel PACS images at 70, 100, and 160 μm and SPIRE images at 250, 350, and 500 μm were obtained by scanning the region around Betelgeuse. These data were complemented with ultraviolet GALEX data, near-infrared WISE data, and radio 21 cm GALFA-HI data. The observational properties of the bow shock structure were deduced from the data and compared with hydrodynamical simulations. Results. The infrared Herschel images of the environment around Betelgeuse are spectacular, showing the occurrence of multiple arcs at ~6–7′ from the central target and the presence of a linear bar at ~9′. Remarkably, no large-scale instabilities are seen in the outer arcs and linear bar. The dust temperature in the outer arcs varies between 40 and 140 K, with the linear bar having the same colour temperature as the arcs. The inner envelope shows clear evidence of a non-homogeneous clumpy structure (beyond 15′′), probably related to the giant convection cells of the outer atmosphere. The non-homogeneous distribution of the material even persists until the collision with the ISM. A strong variation in brightness of the inner clumps at a radius of ~2′ suggests a drastic change in mean gas and dust density ~32 000 yr ago. Using hydrodynamical simulations, we try to explain the observed morphology of the bow shock around Betelgeuse. Conclusions. Different hypotheses, based on observational and theoretical constraints, are formulated to explain the origin of the multiple arcs and the linear bar and the fact that no large-scale instabilities are visible in the bow shock region. We infer that the two main ingredients for explaining these phenomena are a non-homogeneous mass-loss process and the influence of the Galactic magnetic field. The hydrodynamical simulations show that a warm interstellar medium, reflecting a warm neutral or partially ionized medium, or a higher temperature in the shocked wind also prevent the growth of strong instabilities. The linear bar is probably an interstellar structure illuminated by Betelgeuse itself.

Published
2013
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45. ARIEL – Atmospheric Remote-Sensing Infrared Exoplanet Large-survey

Author

Tinetti, Giovanna, Drossart, Pierre, Eccleston, Paul, Hartogh, Paul, Leconte, Jérémy, Micela, Giusi, Ollivier, Marc, Pilbratt, Göran, Puig, Ludovic, Turrini, Diego, Bart Vandenbussche, Wolkenberg, Paulina, Ariel Consortium, Ariel Esa Study Team, University College of London [London] (UCL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, ECLIPSE 2016, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Institut de Génomique Fonctionnelle de Lyon (IGFL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Recherche Agronomique (INRA)-École normale supérieure - Lyon (ENS Lyon), University of Valencia, Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), École normale supérieure de Lyon (ENS de Lyon)-Institut National de la Recherche Agronomique (INRA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), École normale supérieure - Lyon (ENS Lyon)-Institut National de la Recherche Agronomique (INRA)-Université Claude Bernard Lyon 1 (UCBL), Polska Akademia Nauk (PAN), and Pomies, Marie-Paule

Subjects
Astrophysics::Instrumentation and Methods for Astrophysics, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::Earth and Planetary Astrophysics
Abstract

International audience; The Atmospheric Remote-Sensing Infrared Exoplanet Large-survey (ARIEL) is one of the three candidate missions selected by the European Space Agency (ESA) for its next medium-class science mission due for launch in 2026. The goal of the ARIEL mission is to investigate the atmospheres of several hundreds planets orbiting distant stars in order to address the fundamental questions on how planetary systems form and evolve.During its four (with a potential extension to six) years mission ARIEL will observe 500+ exoplanets in the visible and the infrared with its meter-class telescope in L2. ARIEL targets will include Jupiter- and Neptune-size down to super-Earth and Earth-size around different types of stars. The main focus of the mission will be on hot and warm planets orbiting very close to their star, as they represent a natural laboratory in which to study the chemistry and formation of exoplanets. In cooler planets, different gases separate out through condensation and sinking into distinct cloud layers. The scorching heat experienced by hot exoplanets overrides these processes and keeps all molecular species circulating throughout the atmosphere.The ARIEL mission concept has been developed by a consortium of more than 50 institutes from 12 countries, which include UK, France, Italy, Germany, the Netherlands, Poland, Spain, Belgium, Austria, Denmark, Ireland and Portugal. The analysis of ARIEL spectra and photometric data will allow to extract the chemical fingerprints of gases and condensates in the planets' atmospheres, including the elemental composition for the most favorable targets. It will also enable the study of thermal and scattering properties of the atmosphere as the planet orbit around the star.ARIEL will have an open data policy, enabling rapid access by the general community to the high-quality exoplanet spectra that the core survey will deliver.

Published
2016

46. The mid-infrared instrument for the James Webb space telescope: IV. The low resolution spectrometer

Author

David W. Wright, Gabby Aitink-Kroes, Kay Justtanont, Peter Hastings, Friedrich Mueller, Jane E. Morrison, I. Martínez-Delgado, L. B. F. M. Waters, David W. Lee, Thodori Nakos, Juan Rafael Martínez-Galarza, Fred Lahuis, Brian O'Sullivan, Alistair Glasse, Th. Henning, Eva Schmalzl, Ad Oudenhuysen, Bob Kruizinga, Bernhard R. Brandl, J. Sykes, Bart Vandenbussche, E. F. van Dishoeck, Angus Gallie, V. C. Geers, Evert Pauwels, Rieks Jager, J. W. Pel, M. P. Thelen, P. Parr-Burman, Martyn Wells, Steven Beard, R.-R. Rohloff, Adrian M. Glauser, Hubregt J. Visser, Michael Meijers, G. S. Wright, Ruyman Azzollini, Lars Venema, Low Energy Astrophysics (API, FNWI), and Kapteyn Astronomical Institute

Subjects
Diffraction, Point spread function, Image quality, FOS: Physical sciences, OPTICAL MATERIALS, 7. Clean energy, THERMAL-EXPANSION MEASUREMENTS, Optics, Astrophysics::Solar and Stellar Astrophysics, Spectroscopy, Transit (satellite), TEMPERATURE, Instrumentation and Methods for Astrophysics (astro-ph.IM), Remote sensing, Physics, OPT - Optics, TS - Technical Sciences, Spectrometer, business.industry, Low resolution, James Webb Space Telescope, Resolution (electron density), Astronomy and Astrophysics, Ranging, Exoplanet, Stars, Transmission (telecommunications), Space and Planetary Science, Nano Technology, Astrophysics::Earth and Planetary Astrophysics, Coaxial, Electronics, business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Low Resolution Spectrometer of the MIRI, which forms part of the imager module, will provide R~100 long-slit and slitless spectroscopy from 5 to 12 micron. The design is optimised for observations of compact sources, such as exoplanet host stars. We provide here an overview of the design of the LRS, and its performance as measured during extensive test campaigns, examining in particular the delivered image quality, dispersion, and resolving power, as well as spectrophotometric performance, flatfield accuracy and the effects of fringing. We describe the operational concept of the slitless mode, which is optimally suited to transit spectroscopy of exoplanet atmospheres. The LRS mode of the MIRI was found to perform consistently with its requirements and goals., Comment: published in PASP, vol. 127, issue 953, pp.623-632, 2015

Published
2016
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47. Data mining spacecraft telemetry: towards generic solutions to automatic health monitoring and status characterisation

Author

Rik Huygen, Moritz Korte-Stapff, Jose Martinez, W. De Meester, David J. Evans, Bart Vandenbussche, S. Regibo, J. De Ridder, and Pierre Royer

Subjects
Spacecraft, Computer science, business.industry, SIGNAL (programming language), 0211 other engineering and technologies, Process (computing), 020206 networking & telecommunications, 02 engineering and technology, computer.software_genre, Set (abstract data type), Telemetry, 021105 building & construction, 0202 electrical engineering, electronic engineering, information engineering, Data mining, business, computer
Abstract

We present the first results of a study aimed at finding new and efficient ways to automatically process spacecraft telemetry for automatic health monitoring. The goal is to reduce the load on the flight control team while extending the "checkability" to the entire telemetry database, and provide efficient, robust and more accurate detection of anomalies in near real time. We present a set of effective methods to (a) detect outliers in the telemetry or in its statistical properties, (b) uncover and visualise special properties of the telemetry and (c) detect new behavior. Our results are structured around two main families of solutions. For parameters visiting a restricted set of signal values, i.e. all status parameters and about one third of all the others, we focus on a transition analysis, exploiting properties of Poincare plots. For parameters with an arbitrarily high number of possible signal values, we describe the statistical properties of the signal via its Kernel Density Estimate. We demonstrate that this allows for a generic and dynamic approach of the soft-limit definition. Thanks to a much more accurate description of the signal and of its time evolution, we are more sensitive and more responsive to outliers than the traditional checks against hard limits. Our methods were validated on two years of Venus Express telemetry. They are generic for assisting in health monitoring of any complex system with large amounts of diagnostic sensor data. Not only spacecraft systems but also present-day astronomical observatories can benefit from them.

Published
2016
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48. The MIRI Medium Resolution Spectrometer calibration pipeline

Author

Alistair Glasse, Dan Dicken, Karl D. Gordon, Kay Justtanont, Adrian Glauser, Bart Vandenbussche, David R. Law, George H. Rieke, Gillian S. Wright, Fred Lahuis, M. Garcia-Marin, Vincent Geers, Ruymán Azzollini, M. Müller, Jane E. Morrison, Alvaro Labiano, Steven Beard, Pamela Klaassen, Jeremy Bailey, and Astronomy

Subjects
010504 meteorology & atmospheric sciences, Spectrometer, Point source, Computer science, Pipeline (computing), James Webb Space Telescope, FOS: Physical sciences, 01 natural sciences, Field (computer science), 0103 physical sciences, Calibration, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Remote sensing
Abstract

The Mid-Infrared Instrument (MIRI) Medium Resolution Spectrometer (MRS) is the only mid-IR Integral Field Spectrometer on board James Webb Space Telescope. The complexity of the MRS requires a very specialized pipeline, with some specific steps not present in other pipelines of JWST instruments, such as fringe corrections and wavelength offsets, with different algorithms for point source or extended source data. The MRS pipeline has also two different variants: the baseline pipeline, optimized for most foreseen science cases, and the optimal pipeline, where extra steps will be needed for specific science cases. This paper provides a comprehensive description of the MRS Calibration Pipeline from uncalibrated slope images to final scientific products, with brief descriptions of its algorithms, input and output data, and the accessory data and calibration data products necessary to run the pipeline., Comment: 10 pages, 8 figures

Published
2016

49. The science of ARIEL (Atmospheric Remote-sensing Infrared Exoplanet Large-survey)

Author

Manuel Güdel, Ignasi Ribas, P. Malaguti, M. R. Zapatero-Osorio, L. Puig, Neil Bowles, Franck Selsis, Emanuele Pace, A. Coustenis, Michiel Min, Jean-Philippe Beaulieu, M. Rataj, G. S. Wright, Göran Pilbratt, William Taylor, Tom Ray, Paulina Wolkenberg, Ingo Waldmann, Matthew Joseph Griffin, V. Coudé du Foresto, Marco Rocchetto, Tiziano Zingales, François Forget, Joanna K. Barstow, Olivia Venot, T. Encrenaz, Diego Turrini, Jérémy Leconte, Bart Vandenbussche, Paul Hartogh, P. O. Lagage, Giuseppina Micela, A. Heske, Marc Ollivier, Pierre Drossart, Enzo Pascale, M. Friswell, A. Moneti, Subhajit Sarkar, Giovanna Tinetti, Jonathan Tennyson, Juan Carlos Morales, Paul Eccleston, Leen Decin, University College of London [London] (UCL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, ECLIPSE 2016, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Institut de Génomique Fonctionnelle de Lyon (IGFL), École normale supérieure de Lyon (ENS de Lyon)-Institut National de la Recherche Agronomique (INRA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), University of Valencia, Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute for Astronomy [Vienna], University of Vienna [Vienna], Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Dpto. de Organización de Empresas, Escuela Técnica Superior de Ingeniería Industrial de Barcelona, Universitat Politècnica de Catalunya [Barcelona] (UPC), Department of Physics and Astronomy [Leicester], University of Leicester, Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), College of Engineering, Swansea Univ, School of Physics and Astronomy [Cardiff], Cardiff University, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Università degli studi di Verona = University of Verona (UNIVR), Department of Physics and Astronomy [UCL London], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), McMaster University [Hamilton, Ontario], Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Max Planck Institute for Solar System Research (MPS), École normale supérieure - Lyon (ENS Lyon)-Institut National de la Recherche Agronomique (INRA)-Université Claude Bernard Lyon 1 (UCBL), European Space Agency (ESA), Polska Akademia Nauk (PAN), University of Oxford [Oxford], École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Università degli Studi di Verona, University College of London [London] ( UCL ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Max Planck Institute for Solar System Research ( MPS ), Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), INAF - Osservatorio Astronomico di Palermo ( OAPa ), Istituto Nazionale di Astrofisica ( INAF ), Institut de Génomique Fonctionnelle de Lyon ( IGFL ), École normale supérieure - Lyon ( ENS Lyon ) -Institut National de la Recherche Agronomique ( INRA ) -Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique ( CNRS ), European Space Research and Technology Centre ( ESTEC ), European Space Agency ( ESA ), Space Research Centre [Warsaw] ( CBK ), Polska Akademia Nauk ( PAN ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Astronomical Institute Anton Pannekoek ( AI PANNEKOEK ), University of Amsterdam [Amsterdam] ( UvA ), Universidad Politécnica de Cataluña, Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), Laboratoire de Météorologie Dynamique (UMR 8539) ( LMD ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -École polytechnique ( X ) -École des Ponts ParisTech ( ENPC ) -Centre National de la Recherche Scientifique ( CNRS ) -Département des Géosciences - ENS Paris, École normale supérieure - Paris ( ENS Paris ) -École normale supérieure - Paris ( ENS Paris ), School of Physics & Astronomy [Cardiff], Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, K.U.Leuven, Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Recherche Agronomique (INRA)-École normale supérieure - Lyon (ENS Lyon), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), and University of Verona (UNIVR)

Subjects
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Orbital mechanics, Stellar classification, 7. Clean energy, 01 natural sciences, Space missions, Space exploration, Astrobiology, law.invention, 010309 optics, Telescope, law, Planet, 0103 physical sciences, Electronic, Atmospheric science, Exoplanets, IR spectroscopy, Electronic, Optical and Magnetic Materials, Condensed Matter Physics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Applied Mathematics, Electrical and Electronic Engineering, Optical and Magnetic Materials, 010303 astronomy & astrophysics, Physics, space missions, atmospheric science, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Planetary system, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Exoplanet, 13. Climate action, Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics
Abstract

International audience; The Atmospheric Remote-Sensing Infrared Exoplanet Large-survey (ARIEL) is one of the three candidate missions selected by the European Space Agency (ESA) for its next medium-class science mission due for launch in 2026. The goal of the ARIEL mission is to investigate the atmospheres of several hundred planets orbiting distant stars in order to address the fundamental questions on how planetary systems form and evolve. During its four (with a potential extension to six) years mission ARIEL will observe 500+ exoplanets in the visible and the infrared with its meter-class telescope in L2. ARIEL targets will include gaseous and rocky planets down to the Earth-size around different types of stars. The main focus of the mission will be on hot and warm planets orbiting close to their star, as they represent a natural laboratory in which to study the chemistry and formation of exoplanets. The ARIEL mission concept has been developed by a consortium of more than 50 institutes from 12 countries, which include UK, France, Italy, Germany, the Netherlands, Poland, Spain, Belgium, Austria, Denmark, Ireland and Portugal. The analysis of the ARIEL spectra and photometric data in the 0.5-7.8 micron range will allow to extract the chemical fingerprints of gases and condensates in the planets' atmospheres, including the elemental composition for the most favorable targets. It will also enable the study of thermal and scattering properties of the atmosphere as the planet orbit around the star. ARIEL will have an open data policy, enabling rapid access by the general community to the high-quality exoplanet spectra that the core survey will deliver.

Published
2016
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50. Herschel detects oxygen in the β Pictoris debris disk

Author

Walter Kieran Gear, Rik Huygen, Eric Pantin, Göran Pilbratt, H. Walker, Paul M. Harvey, S. J. Leeks, Bruce Sibthorpe, Alexis Brandeker, Ana M. Heras, Christoffel Waelkens, René Liseau, J. Di Francesco, William R. F. Dent, Göran Olofsson, M. J. Barlow, Pierre Royer, Wayne S. Holland, Malcolm Fridlund, Bart Vandenbussche, B. Acke, Rob Ivison, Joris Blommaert, Marvin L. Cohen, Gianni Cataldi, Tanya L. Lim, Michiel R. Hogerheijde, Jane S. Greaves, Carsten Dominik, Brenda C. Matthews, Adrian Glauser, and Low Energy Astrophysics (API, FNWI)

Subjects
Planetesimal, Absorption spectroscopy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, beta Pictoris, 01 natural sciences, circumstellar matter, Spitzer Space Telescope, Early-type stars, Planet, early-type [Stars], 0103 physical sciences, Individual stars, Beta Pictoris, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, Debris disk, 010308 nuclear & particles physics, Torus, Astronomy and Astrophysics, Circumstellar matter, individual: beta Pictoris [Stars], 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics
Abstract

The young star β Pictoris is well known for its dusty debris disk produced through collisional grinding of planetesimals, kilometre-sized bodies in orbit around the star. In addition to dust, small amounts of gas are also known to orbit the star; this gas is likely the result of vaporisation of violently colliding dust grains. The disk is seen edge on and from previous absorption spectroscopy we know that the gas is very rich in carbon relative to other elements. The oxygen content has been more difficult to assess, however, with early estimates finding very little oxygen in the gas at a C/O ratio that is 20× higher than the cosmic value. A C/O ratio that high is difficult to explain and would have far-reaching consequences for planet formation. Here we report on observations by the far-infrared space telescope Herschel, using PACS, of emission lines from ionised carbon and neutral oxygen. The detected emission from C+ is consistent withthat previously reported observed by the HIFI instrument on Herschel, while the emission from O is hard to explain without assuming a higher density region in the disk, perhaps in the shape of a clump or a dense torus required to sufficiently excite the O atoms. A possible scenario is that the C/O gas is produced by the same process responsible for the CO clump recently observed by the Atacama Large Millimeter/submillimeter Array in the disk and that the redistribution of the gas takes longer than previously assumed. A more detailed estimate of the C/O ratio and the mass of O will have to await better constraints on the C/O gas spatial distribution.

Published
2016
Full Text
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