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1. General Relativistic effects and the NIR variability of Sgr A* II: A systematic approach to temporal asymmetry

Author

von Fellenberg, Sebastiano D., Witzel, Gunther, Bauboeck, Michi, Chung, Hui-Hsuan, Marchili, Nicola, Martinez, Greg, Sadun-Bordoni, Matteo, Bourdarot, Guillaume, Do, Tuan, Drescher, Antonia, Fazio, Giovanni, Eisenhauer, Frank, Genzel, Reinhard, Gillessen, Stefan, Hora, Joseph L., Mang, Felix, Ott, Thomas, Smith, Howard A., Ros, Eduardo, Ribeiro, Diogo C., Widmann, Felix, Willner, S. P., and Zensus, J. Anton

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

A systematic study, based on the third-moment structure function, of Sgr A*'s variability finds an exponential rise time $\tau_{1,\rm{obs}}=14.8^{+0.4}_{-1.5}~\mathrm{minutes}$ and decay time $\tau_{2,\rm{obs}}=13.1^{+1.3}_{-1.4}~\mathrm{minutes}$. This symmetry of the flux-density variability is consistent with earlier work, and we interpret it as caused by the dominance of Doppler boosting, as opposed to gravitational lensing, in Sgr~A*'s light curve. A relativistic, semi-physical model of Sgr~A* confirms an inclination angle $i<45$ degrees. The model also shows that the emission of the intrinsic radiative process can have some asymmetry even though the observed emission does not. The third-moment structure function, which is a measure of the skewness of the light-curve increments, may be a useful summary statistic in other contexts of astronomy because it senses only temporal asymmetry, i.e., it averages to zero for any temporally symmetric signal., Comment: Accepted for publication in A&A letters

Published
2024
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2. 2023 Astrophotonics Roadmap: pathways to realizing multi-functional integrated astrophotonic instruments

Author

Jovanovic, Nemanja, Gatkine, Pradip, Anugu, Narsireddy, Amezcua-Correa, Rodrigo, Thakur, Ritoban Basu, Beichman, Charles, Bender, Chad, Berger, Jean-Philippe, Bigioli, Azzurra, Bland-Hawthorn, Joss, Bourdarot, Guillaume, Bradford, Charles M., Broeke, Ronald, Bryant, Julia, Bundy, Kevin, Cheriton, Ross, Cvetojevic, Nick, Diab, Momen, Diddams, Scott A., Dinkelaker, Aline N., Duis, Jeroen, Eikenberry, Stephen, Ellis, Simon, Endo, Akira, Figer, Donald F., Fitzgerald, Michael, Gris-Sanchez, Itandehui, Gross, Simon, Grossard, Ludovic, Guyon, Olivier, Haffert, Sebastiaan Y., Halverson, Samuel, Harris, Robert J., He, Jinping, Herr, Tobias, Hottinger, Philipp, Huby, Elsa, Ireland, Michael, Jenson-Clem, Rebecca, Jewell, Jeffrey, Jocou, Laurent, Kraus, Stefan, Labadie, Lucas, Lacour, Sylvestre, Laugier, Romain, Ławniczuk, Katarzyna, Lin, Jonathan, Leifer, Stephanie, Leon-Sava, Sergio, Martin, Guillermo, Martinache, Frantz, Martinod, Marc-Antoine, Mazin, Benjamin A., Minardi, Stefano, Monnier, John D., Moreira, Reinan, Mourard, Denis, Nayak, Abani Shankar, Norris, Barnaby, Obrzud, Ewelina, Perraut, Karine, Reynaud, François, Sallum, Steph, Schiminovich, David, Schwab, Christian, Serbayn, Eugene, Soliman, Sherif, Stoll, Andreas, Tang, Liang, Tuthill, Peter, Vahala, Kerry, Vasisht, Gautam, Veilleux, Sylvain, Walter, Alexander B., Wollack, Edward J., Xin, Yinzi, Yang, Zongyin, Yerolatsitis, Stephanos, Zhang, Yang, and Zou, Chang-Ling

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract

Photonics offer numerous functionalities that can be used to realize astrophotonic instruments. The most spectacular example to date is the ESO Gravity instrument at the Very Large Telescope in Chile. Integrated astrophotonic devices stand to offer critical advantages for instrument development, including extreme miniaturization, as well as integration, superior thermal and mechanical stabilization owing to the small footprint, and high replicability offering cost savings. Numerous astrophotonic technologies have been developed to address shortcomings of conventional instruments to date, including for example the development of photonic lanterns, complex aperiodic fiber Bragg gratings, complex beam combiners to enable long baseline interferometry, and laser frequency combs for high precision spectral calibration of spectrometers. Despite these successes, the facility implementation of photonic solutions in astronomical instrumentation is currently limited because of (1) low throughputs from coupling to fibers, coupling fibers to chips, propagation and bend losses, device losses, etc, (2) difficulties with scaling to large channel count devices needed for large bandwidths and high resolutions, and (3) efficient integration of photonics with detectors, to name a few. In this roadmap, we identify 24 areas that need further development. We outline the challenges and advances needed across those areas covering design tools, simulation capabilities, fabrication processes, the need for entirely new components, integration and hybridization and the characterization of devices. To realize these advances the astrophotonics community will have to work cooperatively with industrial partners who have more advanced manufacturing capabilities. With the advances described herein, multi-functional instruments will be realized leading to novel observing capabilities for both ground and space platforms., Comment: 191 pages, 47 figures. This is the version of the article before peer review or editing, as submitted by an author to J. Phys. Photonics. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at https://iopscience.iop.org/article/10.1088/2515-7647/ace869/meta

Published
2023
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3. On-sky demonstration at Palomar Observatory of the near-IR, high-resolution VIPA spectrometer

Author

Carlotti, Alexis, Bidot, Alexis, Mouillet, David, Correia, Jean-Jacques, Jocou, Laurent, Curaba, Stéphane, Delboulbé, Alain, Coarer, Etienne Le, Rabou, Patrick, Bourdarot, Guillaume, Forveille, Thierry, Bondils, Xavier, Vasisht, Gautam, Mawet, Dimitri, Burruss, Rick S., Oppenheimer, Rebecca, Doyon, René, Artigau, Etienne, and Vallée, Philippe

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

A near-IR high-resolution, R=80000 spectrometer has been developed at IPAG to directly characterize the atmosphere of exoplanets using adaptive optics (AO) assisted telescopes, and a single-mode fiber-injection unit. A first technical test with the 200' Hale telescope at Palomar Observatory occurred in March 2022 using the PALM3000 AO system offered by this telescope. Observations have also been made at the same time with the PARVI spectrometer so that a direct comparison can be made between the two instruments. This spectrometer uses a virtually imaged phased array (VIPA) instead of an echelle grating, resulting in a very compact optical layout that fits in a 0.25m3 cryostat. Using a quarter of an H2RG detector, the spectrometer analyses the middle part of the H-band, from 1.57 to 1.7 microns for 2 sources whose light is transferred from the telescope to the spectrometer using single-mode fibers. By design, the transmission of the spectrometer is expected to be 40-50%, which is 2-3 times higher than the transmission of current high-resolution spectrometers such as CRIRES+ and NIRSPEC. A damaged cross-disperser limited it to 21%, however. A replacement grating with a correct, twice as high efficiency has been procured after the on-sky demonstration. In addition to recalling the main specifications of the VIPA spectrometer, this paper presents the control software, the calibration process, and the reduction pipeline that have been developed for the instrument. It also presents the results of the on-sky technical test with the Hale telescope, as well as measurements of the effective resolution and transmission, along with a comparison of a spectrum of the sun obtained with the spectrometer with the BASS2000 reference spectrum. Planned modifications are also discussed. That includes the integration of a new dedicated H2RG detector, and of K-band optics.

Published
2023
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4. The GRAVITY+ Project: Towards All-sky, Faint-Science, High-Contrast Near-Infrared Interferometry at the VLTI

Author

Collaboration, GRAVITY, Abuter, Roberto, Alarcon, Patricio, Allouche, Fatme, Amorim, Antonio, Bailet, Christophe, Bedigan, Helen, Berdeu, Anthony, Berger, Jean-Philippe, Berio, Philippe, Bigioli, Azzurra, Blaho, Richard, Boebion, Olivier, Bolzer, Marie-Lena, Bonnet, Henri, Bourdarot, Guillaume, Bourget, Pierre, Brandner, Wolfgang, Cardenas, Cesar, Conzelmann, Ralf, Comin, Mauro, Clénet, Yann, Courtney-Barrer, Benjamin, Dallilar, Yigit, Davies, Ric, Defrère, Denis, Delboulbé, Alain, Delplancke-Ströbele, Françoise, Dembet, Roderick, de Zeeuw, Tim, Drescher, Antonia, Eckart, Andreas, Édouard, Clemence, Eisenhauer, Frank, Fabricius, Maximilian, Feuchtgruber, Helmut, Finger, Gert, Schreiber, Natascha M. Förster, Fuenteseca, Eloy, Garcia, Enrique, Garcia, Paulo, Gao, Feng, Gendron, Eric, Genzel, Reinhard, Gil, Juan Pablo, Gillessen, Stefan, Gomes, Tiago, Gonté, Frédéric, Gouvret, Carole, Guajardo, Patricia, Guidolin, Ivan, Guieu, Sylvain, Guzmann, Ronald, Hackenberg, Wolfgang, Haddad, Nicolas, Hartl, Michael, Haubois, Xavier, Haußmann, Frank, Heißel, Gernot, Henning, Thomas, Hippler, Stefan, Hönig, Sebastian, Horrobin, Matthew, Hubin, Norbert, Jacqmart, Estelle, Jocou, Laurent, Kaufer, Andreas, Kervella, Pierre, Kirchbauer, Jean-Paul, Kolb, Johan, Korhonen, Heidi, Kreidberg, Laura, Krempl, Peter, Lacour, Sylvestre, Lagarde, Stephane, Lai, Olivier, Lapeyrère, Vincent, Laugier, Romain, Bouquin, Jean-Baptiste Le, Leftley, James, Léna, Pierre, Lewis, Steffan, Lutz, Dieter, Magnard, Yves, Mang, Felix, Marcotto, Aurelie, Maurel, Didier, Mérand, Antoine, Millour, Florentin, More, Nikhil, Nowack, Hugo, Nowak, Matthias, Oberti, Sylvain, Olivares, Francisco, Ott, Thomas, Pallanca, Laurent, Paumard, Thibaut, Perraut, Karine, Perrin, Guy, Petrov, Romain, Pfuhl, Oliver, Pourré, Nicolas, Rabien, Sebastian, Rau, Christian, Riquelme, Miguel, Robbe-Dubois, Sylvie, Rochat, Sylvain, Salman, Muhammad, Scherbarth, Malte, Schöller, Markus, Schubert, Joseph, Schuhler, Nicolas, Shangguan, Jinyi, Shchekaturov, Pavel, Shimizu, Taro, Scheithauer, Silvia, Sevin, Arnaud, Soenke, Christian, Soulez, Ferreol, Spang, Alain, Stadler, Eric, Straubmeier, Christian, Sturm, Eckhard, Sykes, Calvin, Tacconi, Linda, Tischer, Helmut, Tristram, Konrad, Vincent, Frédéric, von Fellenberg, Sebastiano, Uysal, Sinem, Widmann, Felix, Wieprecht, Ekkehard, Wiezorrek, Erich, Woillez, Julien, Yazıcı, Şenol, and Zins, Gérard

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The GRAVITY instrument has been revolutionary for near-infrared interferometry by pushing sensitivity and precision to previously unknown limits. With the upgrade of GRAVITY and the Very Large Telescope Interferometer (VLTI) in GRAVITY+, these limits will be pushed even further, with vastly improved sky coverage, as well as faint-science and high-contrast capabilities. This upgrade includes the implementation of wide-field off-axis fringe-tracking, new adaptive optics systems on all Unit Telescopes, and laser guide stars in an upgraded facility. GRAVITY+ will open up the sky to the measurement of black hole masses across cosmic time in hundreds of active galactic nuclei, use the faint stars in the Galactic centre to probe General Relativity, and enable the characterisation of dozens of young exoplanets to study their formation, bearing the promise of another scientific revolution to come at the VLTI., Comment: Published in the ESO Messenger

Published
2023
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5. AMICal Sat: A sparse RGB imager on board a 2U cubesat to study the aurora

Author

Barthelemy, Mathieu, Robert, Elisa, Kalegaev, Vladimir, Grennerat, Vincent, Sequies, Thierry, Bourdarot, Guillaume, Coarer, Etienne Le, Correia, Jean-Jacques, and Rabou, Patrick

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

AMICal sat, a dedicated 2U cubesat, has been developed, in order to monitor the auroral emissions, with a dedicated imager. It aims to help to reconstruct the low energy electrons fluxes up to 30 keV in Earth auroral regions. It includes an imager entirely designed in Grenoble University Space Center. The imager uses a 1.3 Mpixels sparse RGB CMOS detector and a wide field objective (f=22.5 mm). The satellite platform has been built by the polish company Satrevolution. Launched September, 3rd, 2020 from Kuru (French Guyana) on board the Vega flight 16, it produces its first images in October 2020. The aim of this paper is to describe the design of the payload especially the optics and the proximity electronics, to describe the use of the payload for space weather purpose. A preliminary analysis of a first image showing the relevance of such an instrument for auroral monitoring is performed. This analysis allowed to reconstruct from one of the first images the local electron input flux at the top of the atmosphere during the exposure time., Comment: Submitted to IEEE-JMASS. Under review

Published
2022

6. Toward a large bandwidth photonic correlator for infrared heterodyne interferometry

Author

Bourdarot, Guillaume, de Chatellus, Hugues Guillet, and Berger, Jean-Philippe

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Infrared heterodyne interferometry has been proposed as a practical alternative for recombining a large number of telescopes over kilometric baselines in the mid-infrared. However, the current limited correlation capacities impose strong restrictions on the sensitivity of this appealing technique. In this paper, we propose to address the problem of transport and correlation of wide-bandwidth signals over kilometric distances by introducing photonic processing in infrared heterodyne interferometry. We describe the architecture of a photonic double-sideband correlator for two telescopes, along with the experimental demonstration of this concept on a proof-of-principle test bed. We demonstrate the \textit{a posteriori} correlation of two infrared signals previously generated on a two-telescope simulator in a double-sideband photonic correlator. A degradation of the signal-to-noise ratio of $13\%$, equivalent to a noise factor $\text{NF}=1.15$, is obtained through the correlator, and the temporal coherence properties of our input signals are retrieved from these measurements. Our results demonstrate that photonic processing can be used to correlate heterodyne signals with a potentially large increase of detection bandwidth. These developments open the way to photonic processing of wide bandwidth signals for mid-infrared heterodyne interferometry, in particular for a large number of telescopes and for direct imager recombiners., Comment: 7 pages, 4 figures. Accepted in Astronomy & Astrophysics

Published
2020
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7. Experimental test of a 40 cm-long R=100 000 spectrometer for exoplanet characterisation

Author

Bourdarot, Guillaume, Coarer, Etienne Le, Mouillet, David, Correia, Jean-Jacques, Jocou, Laurent, Rabou, Patrick, Carlotti, Alexis, Bonfils, Xavier, Artigau, Etienne, Vallee, Philippe, Doyon, Rene, Forveille, Thierry, Stadler, Eric, Magnard, Yves, and Vigan, Arthur

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

High-resolution spectroscopy is a key element for present and future astronomical instrumentation. In particular, coupled to high contrast imagers and coronagraphs, high spectral resolution enables higher contrast and has been identified as a very powerful combination to characterise exoplanets, starting from giant planets now, up to Earth-like planet eventually for the future instruments. In this context, we propose the implementation of an innovative echelle spectrometer based on the use of VIPA (Virtually Imaged Phased Array, Shirasaki 1996). The VIPA itself is a particular kind of Fabry-Perot interferometer, used as an angular disperser with much greater dispersive power than common diffraction grating. The VIPA is an efficient, small component (3 cm x 2.4 cm), that takes the very advantage of single mode injection in a versatile design. The overall instrument presented here is a proof-of-concept of a compact, high-resolution (R > 80 000) spectrometer, dedicated to the H and K bands, in the context of the project High-Dispersion Coronagrahy developed at IPAG. The optical bench has a foot-print of 40 cm x 26 cm ; it is fed by two Single-Mode Fibers (SMF), one dedicated to the companion, and one to the star and/or to a calibration channel, and is cooled down to 80 K. This communication first presents the scientific and instrumental context of the project, and the principal merit of single-mode operations in high-resolution spectrometry. After recalling the physical structure of the VIPA and its implementation in an echelle-spectrometer design, it then details the optical design of the spectrometer. In conclusion, further steps (integration, calibration, coupling with adaptive optics) and possible optimization are briefly presented. Keywords: Echelle Spectrometer, High Spectral Resolution, Exoplanets, High-Dispersion Coronography, Infrared, Adaptive Optics, SPHERE

Published
2018
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8. Nanobob: A Cubesat Mission Concept For Quantum Communication Experiments In An Uplink Configuration

Author

Kerstel, Erik, Gardelein, Arnaud, Barthelemy, Mathieu, Gilot, Yves, LeCoarer, Etienne, Rodrigo, Juana, Sequies, Thierry, Borne, Vincent, Bourdarot, Guillaume, Christidis, Alexis, Segura, Jesus, Boulanger, Benoit, Boutou, Veronique, Bouzat, Mylene, Chabanol, Mathieu, Fesquet, Laurent, Fourati, Hassen, Moulin, Michel, Niot, Jean-Michel, Bastos, Rodrigo Possamai, Robu, Bogdan, Rolland, Etienne, Toru, Sylvain, Fink, Matthias, Joshi, Siddarth Koduru, and Ursin, Rupert

Subjects
Quantum Physics
Abstract

We present a ground-to-space quantum key distribution (QKD) mission concept and the accompanying feasibility study for the development of the low earth orbit CubeSat payload. The quantum information is carried by single photons with the binary codes represented by polarization states of the photons. Distribution of entangled photons between the ground and the satellite can be used to certify the quantum nature of the link: a guarantee that no eavesdropping can take place. By placing the entangled photon source on the ground, the space segments contains only the less complex detection system, enabling its implementation in a compact enclosure, compatible with the 12U CubeSat standard (12 dm3). This reduces the overall cost of the project, making it an ideal choice as a pathfinder for future European quantum communication satellite missions. The space segment is also more versatile than one that contains the source since it is compatible with a multiple of QKD protocols (not restricted to entangled photon schemes) and can be used in quantum physics experiments, such as the investigation of entanglement decoherence. Other possible experiments include atmospheric transmission/turbulence characterization, dark area mapping, fine pointing and tracking, and accurate clock synchronization; all crucial for future global scale quantum communication efforts., Comment: The CSUG Team: Yves Gilot, Etienne LeCoarer, Juana Rodrigo, Thierry Sequies, Vincent Borne, Guillaume Bourdarot, Alexis Christidis, Jesus Segura, Benoit Boulanger, Veronique Boutou, Mylene Bouzat, Mathieu Chabanol, Laurent Fesquet, Hassen Fourati, Michel Moulin, Jean-Michel Niot, Rodrigo Possamai Bastos, Bogdan Robu, Etienne Rolland, Sylvain Toru. Higher quality fig., more concise section 1.7

Published
2017

9. Experimental demonstration of a crossed cubes nuller for coronagraphy and interferometry

Author

Henault, Francois, Arezki, Brahim, Bourdarot, Guillaume, and Spang, Alain

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Optics
Abstract

In this communication we present the first experimental results obtained on the Crossed-cubes nuller (CCN), that is a new type of Achromatic phase shifter (APS) based on a pair of crossed beamsplitter cubes. We review the general principle of the CCN, now restricted to two interferometric outputs for achieving better performance, and describe the experimental apparatus developed in our laboratory. It is cheap, compact, and easy to align. The results demonstrate a high extinction rate in monochromatic light and confirm that the device is insensitive to its polarization state. Finally, the first lessons from the experiment are summarized and discussed in view of future space missions searching for extra-solar planets located in the habitable zone, either based on a coronagraphic telescope or a sparse-aperture nulling interferometer, Comment: 12 pages

Published
2016
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10. Bi-directional frequency shifting loops for real-time processing of broadband RF signals

Author

Bourdarot Guillaume, Berger Jean-Philippe, and Guillet de Chatellus Hugues

Subjects
Physics, QC1-999
Abstract

Analog photonic techniques can perform better than conventional digital electronics, which have significant limitations when it comes to processing fast RF signals on the fly. We show that a simple photonic architecture, based on a bi-directional frequency-shifting loop, makes it possible to calculate in real time the cross-correlation function of two broadband signals for about 200 values of their delay simultaneously. Additionally, our architecture also enables to perform spectral analysis of signals with 16 GHz instantaneous bandwidth, 100 % probability of interception, and detection electronics below 10 MSa/s.

Published
2023
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11. 2023 Astrophotonics Roadmap: pathways to realizing multi-functional integrated astrophotonic instruments

Author

Jovanovic, Nemanja, primary, Gatkine, Pradip, additional, Anugu, Narsireddy, additional, Amezcua-Correa, Rodrigo, additional, Basu Thakur, Ritoban, additional, Beichman, Charles, additional, Bender, Chad F., additional, Berger, Jean-Philippe, additional, Bigioli, Azzurra, additional, Bland-Hawthorn, Joss, additional, Bourdarot, Guillaume, additional, Bradford, Charles M, additional, Broeke, Ronald, additional, Bryant, Julia, additional, Bundy, Kevin, additional, Cheriton, Ross, additional, Cvetojevic, Nick, additional, Diab, Momen, additional, Diddams, Scott A, additional, Dinkelaker, Aline N, additional, Duis, Jeroen, additional, Eikenberry, Stephen, additional, Ellis, Simon, additional, Endo, Akira, additional, Figer, Donald F, additional, Fitzgerald, Michael P., additional, Gris-Sanchez, Itandehui, additional, Gross, Simon, additional, Grossard, Ludovic, additional, Guyon, Olivier, additional, Haffert, Sebastiaan Y, additional, Halverson, Samuel, additional, Harris, Robert J, additional, He, Jinping, additional, Herr, Tobias, additional, Hottinger, Philipp, additional, Huby, Elsa, additional, Ireland, Michael, additional, Jenson-Clem, Rebecca, additional, Jewell, Jeffrey, additional, Jocou, Laurent, additional, Kraus, Stefan, additional, Labadie, Lucas, additional, Lacour, Sylvestre, additional, Laugier, Romain, additional, Ławniczuk, Katarzyna, additional, Lin, Jonathan, additional, Leifer, Stephanie, additional, Leon-Saval, Sergio, additional, Martin, Guillermo, additional, Martinache, Frantz, additional, Martinod, Marc-Antoine, additional, Mazin, Benjamin A, additional, Minardi, Stefano, additional, Monnier, John D, additional, Moreira, Reinan, additional, Mourard, Denis, additional, Nayak, Abani Shankar, additional, Norris, Barnaby, additional, Obrzud, Ewelina, additional, Perraut, Karine, additional, Reynaud, François, additional, Sallum, Steph, additional, Schiminovich, David, additional, Schwab, Christian, additional, Serbayn, Eugene, additional, Soliman, Sherif, additional, Stoll, Andreas, additional, Tang, Liang, additional, Tuthill, Peter, additional, Vahala, Kerry, additional, Vasisht, Gautam, additional, Veilleux, Sylvain, additional, Walter, Alexander B, additional, Wollack, Edward J, additional, Xin, Yinzi, additional, Yang, Zongyin, additional, Yerolatsitis, Stephanos, additional, Zhang, Yang, additional, and Zou, Chang-Ling, additional

Published
2023
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13. AMICal Sat and ATISE: two space missions for auroral monitoring

Author

Barthelemy Mathieu, Kalegaev Vladimir, Vialatte Anne, Le Coarer Etienne, Kerstel Erik, Basaev Alexander, Bourdarot Guillaume, Prugniaux Melanie, Sequies Thierry, Rolland Etienne, Aubert Emmanuelle, Grennerat Vincent, Ayasso Hacheme, Busom Vidal Arnau, Apper Fabien, Stepanov Mikhail, Escudier Benedicte, Croize Laurence, Romand Frederic, Payan Sebastien, and Panasyuk Mikhail

Subjects
aurora, airglow, spectroscopy, space weather, visible, Meteorology. Climatology, QC851-999
Abstract

A lack of observable quantities renders it generally difficult to confront models of Space Weather with experimental data and drastically reduces the forecast accuracy. This is especially true for the region of Earth’s atmosphere between altitudes of 90 km and 300 km, which is practically inaccessible, except by means of remote sensing techniques. For this reason auroral emissions are an interesting proxy for the physical processes taking place in this region. This paper describes two future space missions, AMICal Sat and ATISE, that will rely on CubeSats to observe the aurora. These satellites will perform measurements of auroral emissions in order to reconstruct the deposition of particle precipitations in auroral regions. ATISE is a 12U CubeSat with a spectrometer and imager payloads. The spectrometer is built using the micro-Spectrometer-On-a-Chip (μSPOC) technology. It will work in the 370–900 nm wavelength range and allow for short exposure times of around 1 s. The spectrometer will have six lines of sight. The joint imager is a miniaturized wide-field imager based on the Teledyne-E2V ONYX detector in combination with a large aperture objective. Observation will be done at the limb and will enable reconstruction of the vertical profile of the auroral emissions. ATISE is planned to be launched in mid 2021. AMICal Sat is a 2U CubeSat that will embed the imager of ATISE and will observe the aurora both in limb and nadir configurations. This imager will enable measuring vertical profiles of the emission when observing in a limb configuration similar to that of ATISE. It will map a large part of the night side auroral oval with a resolution of the order of a few km. Both the spectrometer and imager will be calibrated with a photometric precision better than 10% using the moon as a wide-field, stable and extended source. Ground-based demonstrators of both instruments have been tested in 2017 in Norway and Svalbard. Even though some issues still need to be solved, the first results are very encouraging for the planned future space missions. Data interpretation will be done using the forward Transsolo code, a 1D kinetic code solving the Boltzmann equation along a local vertical and enabling simulation of the thermospheric and ionospheric emissions using precipitation data as input.

Published
2018
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14. On-sky demonstration at Palomar Observatory of the near-IR, high-resolution VIPA spectrometer

Author

Carlotti, Alexis, Bidot, Alexis, Mouillet, David, Correia, Jean-Jacques, Jocou, Laurent, Curaba, Stéphane, Delboulbé, Alain, Coarer, Etienne Le, Rabou, Patrick, Bourdarot, Guillaume, Forveille, Thierry, Bondils, Xavier, Vasisht, Gautam, Mawet, Dimitri, Burruss, Rick S., Oppenheimer, Rebecca, Doyon, René, Artigau, Etienne, and Vallée, Philippe

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Earth and Planetary Astrophysics
Abstract

A near-IR high-resolution, R=80000 spectrometer has been developed at IPAG to directly characterize the atmosphere of exoplanets using adaptive optics (AO) assisted telescopes, and a single-mode fiber-injection unit. A first technical test with the 200' Hale telescope at Palomar Observatory occurred in March 2022 using the PALM3000 AO system offered by this telescope. Observations have also been made at the same time with the PARVI spectrometer so that a direct comparison can be made between the two instruments. This spectrometer uses a virtually imaged phased array (VIPA) instead of an echelle grating, resulting in a very compact optical layout that fits in a 0.25m3 cryostat. Using a quarter of an H2RG detector, the spectrometer analyses the middle part of the H-band, from 1.57 to 1.7 microns for 2 sources whose light is transferred from the telescope to the spectrometer using single-mode fibers. By design, the transmission of the spectrometer is expected to be 40-50%, which is 2-3 times higher than the transmission of current high-resolution spectrometers such as CRIRES+ and NIRSPEC. A damaged cross-disperser limited it to 21%, however. A replacement grating with a correct, twice as high efficiency has been procured after the on-sky demonstration. In addition to recalling the main specifications of the VIPA spectrometer, this paper presents the control software, the calibration process, and the reduction pipeline that have been developed for the instrument. It also presents the results of the on-sky technical test with the Hale telescope, as well as measurements of the effective resolution and transmission, along with a comparison of a spectrum of the sun obtained with the spectrometer with the BASS2000 reference spectrum. Planned modifications are also discussed. That includes the integration of a new dedicated H2RG detector, and of K-band optics.

Published
2022

16. GRAVITY+ Wide: towards hundreds of z ~ 2 AGN

Author

Drescher, Antonia, primary, Fabricius, Maximilian, additional, Shimizu, Taro, additional, Woillez, Julien, additional, Bourget, Pierre, additional, Widmann, Felix, additional, Shangguan, Jinyi, additional, Straubmeier, Christian, additional, Horrobin, Matthew, additional, Schuhler, Nicolas, additional, Eisenhauer, Frank, additional, Gonté, Frederic, additional, Gillessen, Stefan, additional, Ott, Thomas, additional, Perrin, Guy, additional, Paumard, Thibaut, additional, Brandner, Wolfgang, additional, Kreidberg, Laura, additional, Perraut, Karine, additional, Le Bouquin, Jean-Baptiste, additional, Garcia, Paulo J. V., additional, Hoenig, Sebastian, additional, Defrère, Denis, additional, Bourdarot, Guillaume, additional, Feuchtgruber, Helmut, additional, Genzel, Reinhard, additional, Hartl, Michael, additional, Haussmann, Frank, additional, Lutz, Dieter, additional, More, Nikhil, additional, Rau, Christian, additional, Sauter, Jonas, additional, Uysal, Sinem, additional, Wessely, Patrick, additional, Wieprecht, Ekkehard, additional, Wimmer, Lukas, additional, and Yazici, Senol, additional

Published
2022
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17. GRAVITY faint: reducing noise sources in GRAVITY+ with a fast metrology attenuation system

Author

Widmann, Felix, primary, Gillessen, Stefan, additional, Ott, Thomas, additional, Shimizu, Taro, additional, Eisenhauer, Frank, additional, Fabricius, Maximilian, additional, Woillez, Julien, additional, Gonté, Frédéric, additional, Horrobin, Matthew, additional, Shangguan, Jingyi, additional, Yazici, Senol, additional, Perrin, Guy, additional, Paumard, Thibaut, additional, Brandner, Wolfgang, additional, Kreidberg, Laura, additional, Straubmeier, Christian, additional, Perraut, Karin, additional, Le Bouquin, Jean-Baptiste, additional, Garcia, Paulo, additional, Hönig, Sebastian, additional, Defrère, Denis, additional, Bourdarot, Guillaume, additional, Drescher, Antonia, additional, Feuchtgruber, Helmut, additional, Genzel, Reinhard, additional, Hartl, Michael, additional, Lutz, Dieter, additional, More, Nikhil, additional, Rau, Christian, additional, Uysal, Sinem, additional, and Wieprecht, Ekkehard, additional

Published
2022
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20. GRAVITY plus Wide: Towards hundreds of z similar to 2 AGN

Author

Drescher, Antonia, Fabricius, Maximilian, Shimizu, Taro, Woillez, Julien, Bourget, Pierre, Widmann, Felix, Shangguan, Jingyi, Straubmeier, Christian, Horrobin, Matthew, Schuhler, Nicolas, Eisenhauer, Frank, Gonte, Frederic, Gillessen, Stefan, Ott, Thomas, Perrin, Guy, Paumard, Thibaut, Brandner, Wolfgang, Kreidberg, Laura, Perraut, Karine, Le Bouquin, Jean-Baptiste, Garcia, Paulo, Honig, Sebastian, Defrere, Denis, Bourdarot, Guillaume, Feuchtgruber, Helmut, Genzel, Reinhard, Hartl, Michael, Haussmann, Frank, Lutz, Dieter, More, Nikhil, Rau, Christian, Sauter, Jonas, Uysal, Sinem, Wessely, Patrick, Wieprecht, Ekkehard, Wimmer, Lukas, Yazici, Senol, Merand, A, Sallum, S, and Sanchez-Bermudez, J

Subjects
Technology, Science & Technology, GRAVITY, Physical Sciences, Optics, Astronomy & Astrophysics, interferometry, Instruments & Instrumentation, near-infrared, wide-angle fringe tracking, VLTI
Abstract

ispartof: OPTICAL AND INFRARED INTERFEROMETRY AND IMAGING VIII vol:12183 ispartof: Conference on Optical and Infrared Interferometry and Imaging VIII Part of SPIE Astronomical Telescopes and Instrumentation Conference location:CANADA, Montreal date:17 Jul - 22 Jul 2022 status: published

Published
2022

22. The GRAVITY+ Project: Towards All-sky, Faint-Science, High-Contrast Near-Infrared Interferometry at the VLTI

Author

Collaboration, GRAVITY+, Abuter, Roberto, Alarcon, Patricio, Allouche, Fatme, Amorim, Antonio, Bailet, Christophe, Bedigan, Helen, Berdeu, Anthony, Berger, Jean-Philippe, Berio, Philippe, Bigioli, Azzurra, Blaho, Richard, Boebion, Olivier, Bolzer, Marie-Lena, Bonnet, Henri, Bourdarot, Guillaume, Bourget, Pierre, Brandner, Wolfgang, Cardenas, Cesar, Conzelmann, Ralf, Comin, Mauro, Clénet, Yann, Courtney-Barrer, Benjamin, Dallilar, Yigit, Davies, Ric, Defrère, Denis, Delboulbé, Alain, Delplancke-Ströbele, Françoise, Dembet, Roderick, de Zeeuw, Tim, Drescher, Antonia, Eckart, Andreas, Édouard, Clemence, Eisenhauer, Frank, Fabricius, Maximilian, Feuchtgruber, Helmut, Finger, Gert, Schreiber, Natascha M. Förster, Fuenteseca, Eloy, Garcia, Enrique, Garcia, Paulo, Gao, Feng, Gendron, Eric, Genzel, Reinhard, Gil, Juan Pablo, Gillessen, Stefan, Gomes, Tiago, Gonté, Frédéric, Gouvret, Carole, Guajardo, Patricia, Guidolin, Ivan, Guieu, Sylvain, Guzmann, Ronald, Hackenberg, Wolfgang, Haddad, Nicolas, Hartl, Michael, Haubois, Xavier, Haußmann, Frank, Heißel, Gernot, Henning, Thomas, Hippler, Stefan, Hönig, Sebastian, Horrobin, Matthew, Hubin, Norbert, Jacqmart, Estelle, Jocou, Laurent, Kaufer, Andreas, Kervella, Pierre, Kirchbauer, Jean-Paul, Kolb, Johan, Korhonen, Heidi, Kreidberg, Laura, Krempl, Peter, Lacour, Sylvestre, Lagarde, Stephane, Lai, Olivier, Lapeyrère, Vincent, Laugier, Romain, Bouquin, Jean-Baptiste Le, Leftley, James, Léna, Pierre, Lewis, Steffan, Lutz, Dieter, Magnard, Yves, Mang, Felix, Marcotto, Aurelie, Maurel, Didier, Mérand, Antoine, Millour, Florentin, More, Nikhil, Nowack, Hugo, Nowak, Matthias, Oberti, Sylvain, Olivares, Francisco, Ott, Thomas, Pallanca, Laurent, Paumard, Thibaut, Perraut, Karine, Perrin, Guy, Petrov, Romain, Pfuhl, Oliver, Pourré, Nicolas, Rabien, Sebastian, Rau, Christian, Riquelme, Miguel, Robbe-Dubois, Sylvie, Rochat, Sylvain, Salman, Muhammad, Scherbarth, Malte, Schöller, Markus, Schubert, Joseph, Schuhler, Nicolas, Shangguan, Jinyi, Shchekaturov, Pavel, Shimizu, Taro, Scheithauer, Silvia, Sevin, Arnaud, Soenke, Christian, Soulez, Ferreol, Spang, Alain, Stadler, Eric, Straubmeier, Christian, Sturm, Eckhard, Sykes, Calvin, Tacconi, Linda, Tischer, Helmut, Tristram, Konrad, Vincent, Frédéric, von Fellenberg, Sebastiano, Uysal, Sinem, Widmann, Felix, Wieprecht, Ekkehard, Wiezorrek, Erich, Woillez, Julien, Yazıcı, Şenol, and Zins, Gérard

Subjects
FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The GRAVITY instrument has been revolutionary for near-infrared interferometry by pushing sensitivity and precision to previously unknown limits. With the upgrade of GRAVITY and the Very Large Telescope Interferometer (VLTI) in GRAVITY+, these limits will be pushed even further, with vastly improved sky coverage, as well as faint-science and high-contrast capabilities. This upgrade includes the implementation of wide-field off-axis fringe-tracking, new adaptive optics systems on all Unit Telescopes, and laser guide stars in an upgraded facility. GRAVITY+ will open up the sky to the measurement of black hole masses across cosmic time in hundreds of active galactic nuclei, use the faint stars in the Galactic centre to probe General Relativity, and enable the characterisation of dozens of young exoplanets to study their formation, bearing the promise of another scientific revolution to come at the VLTI., Comment: Published in the ESO Messenger

Published
2022
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26. Interférométrie hétérodyne moyen-infrarouge pour l'imagerie des environnements protoplanétaires

Author

Bourdarot, Guillaume and STAR, ABES

Subjects
Young stars, Photonics, Heterodyne detection, Mid-Infrared, Formation planétaire, Moyen-Infrarouge, Planet Formation, Photonique, Astronomical interferometry, Étoiles jeunes, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], Détection hétérodyne, Interferométrie astronomique
Abstract

This thesis work focuses on the study at the astronomical scale of young stars and their protoplanetary disks with infrared interferometry. This work includes both observational and instrumental aspects. In the observational part, we focus on the accretion outburst occuring in the formation of young stars through a temporal monitoring of FU Orionis with 20 years of near-infrared interferometric data, in order to put constraints on the instability mechanisms at play in the disk. Although infrared interferometry is a powerful technique to constrain the structure of the inner region of young objects, its capability to perform complete image reconstruction of protoplanetary disk is still limited. In the instrumental part of this work, we explore the extension of infrared interferometers to the recombination of a large number of telescopes and kilometric baselines in the mid-infrared, such as proposed in the framework of the Planet Formation Imager (PFI) initiative. In this perspective, infrared heterodyne interferometry represents a potential interesting technology, despite its lower sensitivity. In this work, we propose the revisit the architecture of an infrared heterodyne interferometric system at the light of the recent progresses in the field of mid-infrared technologies. On a theoretical level, we analyze the sensitivity performances of a interferometer integrating these recent progresses, and clarify the fundamental limitations in sensitivity due to the intrinsic quantum noise of this technique. Among the different technological challenges of heterodyne interferometry, we propose to address the problem of bandwidth limitation and of the correlation of a large number of wideband radiofrequency signals by introducing the use of analog photonic correlation. We describe the principles and the experimental demonstration of a simple, double-sideband analog correlator. We then present the extension of this concept to a wideband multi-delay correlator for RF signal processing based on a bidirectional fiber frequency shifting loop. In a last part, we present the preliminary implementation of a laboratory demonstrator at 10μm dedicated to the validation of the complete detection and correlation chain devised in this thesis. Finally, based on the scalability of this technique, we describe the concept of a technological pathfinder combining the 8 telescopes of the Very Large Telescopes Interferometer (VLTI) at 10μm. We discuss its potential application to the imaging of bright young stars and its implication in the perspective of a PFI., Ce travail de thèse porte sur l'étude des étoiles jeunes et de leur disque protoplanétaire à l'échelle de l'unité astronomique par interférométrie infrarouge. Il inclut à la fois des aspects observationnels et instrumentaux. Dans la partie observationnelle, nous nous concentrons sur les sursauts d'accrétion intervenant dans la formation des étoiles jeunes, à travers l'analyse de 20 ans de données d'observations interferométriques de l'étoile FU Orionis, afin d'apporter des contraintes sur le mécanisme d'instabilité à l'oeuvre dans son disque d'accrétion. Bien que l'interferométrie soit une technique puissante pour contraindre les parties internes des objets jeunes, sa capacité de reconstruction d'images de disques protoplanétaires est encore limitée. Dans la partie instrumentale de ce travail, nous explorons la capacité d'étendre la technique d'interférométrie infrarouge à un grand nombre de télescopes et des lignes de bases kilométriques dans le moyen-infrarouge, comme proposé dans le cadre de l'initiative internationale "Planet Formation Imager" (PFI). Dans cette perspective, la technique d'interferométrie hétérodyne présente un potentiel intéressant, malgré ses limites de sensibilité intrinsèque. Dans ce travail, nous proposons de revoir l'architecture d'un système interferométrique hétérodyne à la lumière des récents progrès dans le domaine des technologies moyen-infarouge. D'un point de vue théorique, nous analysons les performances en sensibilité attendues d'un système intégrant ces progrès techniques récents, et proposons de clarifier les limites de sensibilité fondamentales de cette technique dues au bruit quantique inhérent à ce schéma de détection. Parmi les différents défis technologiques de l'interferométrie hétérodyne, nous proposons d'aborder le problème de la limitation en bande-passante et de corrélation d'un grand nombre de signaux radio-fréquences (RF) à large bande passante, en introduisant l'utilisation d'un schéma de corrélation analogique photonique. Nous commençons par décrire le fonctionnement et l'implémentation d'un corrélateur analogique (double-sideband) simple. Nous présentons ensuite l'extension de ce concept à un corrélateur multi-délai de signaux RFs à grande bande passante, reposant sur une architecture de boucle à décalage de fréquence bi-directionnelle. Dans une dernière partie, nous présentons l'implémentation d'un démonstrateur de laboratoire à 10μm dédié à la validation de la chaîne complète de détection et de corrélation proposée dans cette thèse. Pour finir, nous décrivons le concept d'un instrument pouvant combiner les 8 télescopes de l'interferomètre du Very Large Telescope (VLTI) à 10μm. Nous discutons l'application potentielle de ce concept à l'imagerie d'étoiles jeunes brillantes, et les implications de ce concept dans la perspective d'un grand interferomètre destiné à l'imagerie de la formation planétaire tel que le Planet Formation Imager.

Published
2021

27. Mid-infrared heterodyne interferometry for planet formation studies

Author

Berger, Jean-Philippe and Bourdarot, Guillaume

Abstract

The Planet Formation Imager (PFI) project is an international effort to define the architecture and the technological roadmap for a next-generation long baseline interferometric facility operating in the infrared. PFI aims at reaching an angular resolution and sensitivity sufficient to resolve the composition and kinematic properties of circumplanetary disks surrounding planets in the making. Although direct mid-infrared interferometry such as the one carried at VLTI is currently privileged for sensitivity reasons it comes at a price of a costly and complex infrastructure. In this presentation we will discuss how technological progresses in the field of mid-IR lasers, time synchronisation, high bandwidth mid-IR detectors and photonics correlation might render mid-infrared heterodyne interferometry competitive again while providing an important simplification of the infrastructure. We will end up comparing direct detection schemes with an heterodyne concept.

Published
2020
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30. High-resolution spectroscopy of diffraction-limited sources: laboratory tests of an innovative near-IR demonstrator

Author

Carlotti, Alexis, primary, Mouillet, David, additional, Bidot, Alexis, additional, Bourdarot, Guillaume, additional, Correia, Jean-Jacques, additional, Jocou, Laurent, additional, Delboulbé, Alain, additional, Le Coarer, Etienne P., additional, Doyon, René, additional, Artigau, Étienne, additional, Vallée, Philippe, additional, Roux, Alain, additional, Feautrier, Philippe, additional, Rabou, Patrick, additional, Forveille, Thierry, additional, Bonfils, Xavier, additional, Lo-Cascio, Guillaume, additional, Parthasarathy, Ambarish, additional, Mawet, Dimitri, additional, Vasisht, Gautam, additional, Vigan, Arthur, additional, and Otten, Gilles, additional

Published
2020
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31. On-sky demonstration at Palomar Observatory of the near-IR, high-resolution VIPA spectrometer

Author

Evans, Christopher J., Bryant, Julia J., Motohara, Kentaro, Carlotti, Alexis, Bidot, Alexis, Mouillet, David, Correia, Jean-Jacques, Jocou, Laurent, Curaba, Stephane, Delboulbé, Alain, Le Coarer, Etienne, Rabou, Patrick, Bourdarot, Guillaume, Forveille, Thierry, Bonfils, Xavier, Vasisht, Gautam, Mawet, Dimitri, Burruss, Rick S., Oppenheimer, Rebecca, Doyon, René, Artigau, Etienne, and Vallée, Philippe

Published
2022
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32. GRAVITY+ Wide: towards hundreds of z ~ 2 AGN

Author

Mérand, Antoine, Sallum, Stephanie, Sanchez-Bermudez, Joel, Drescher, Antonia, Fabricius, Maximilian, Shimizu, Taro, Woillez, Julien, Bourget, Pierre, Widmann, Felix, Shangguan, Jinyi, Straubmeier, Christian, Horrobin, Matthew, Schuhler, Nicolas, Eisenhauer, Frank, Gonté, Frederic, Gillessen, Stefan, Ott, Thomas, Perrin, Guy, Paumard, Thibaut, Brandner, Wolfgang, Kreidberg, Laura, Perraut, Karine, Le Bouquin, Jean-Baptiste, Garcia, Paulo, Hönig, Sebastian, Defrère, Denis, Bourdarot, Guillaume, Feuchtgruber, Helmut, Genzel, Reinhard, Hartl, Michael, Haussmann, Frank, Lutz, Dieter, More, Nikhil, Rau, Christian, Sauter, Jonas, Uysal, Sinem, Wessely, Patrick, Wieprecht, Ekkehard, Wimmer, Lukas, and Yazici, Senol

Published
2022
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33. GRAVITY faint: reducing noise sources in GRAVITY+ with a fast metrology attenuation system

Author

Mérand, Antoine, Sallum, Stephanie, Sanchez-Bermudez, Joel, Widmann, Felix, Gillessen, Stefan, Ott, Thomas, Shimizu, Taro, Eisenhauer, Frank, Fabricius, Maximilian, Woillez, Julien, Gonté, Frédéric, Horrobin, Matthew, Shangguan, Jingyi, Yazici, Senol, Perrin, Guy, Paumard, Thibaut, Brandner, Wolfgang, Kreidberg, Laura, Straubmeier, Christian, Perraut, Karin, Le Bouquin, Jean-Baptiste, Garcia, Paulo, Hönig, Sebastian, Defrère, Denis, Bourdarot, Guillaume, Drescher, Antonia, Feuchtgruber, Helmut, Genzel, Reinhard, Hartl, Michael, Lutz, Dieter, More, Nikhil, Rau, Christian, Uysal, Sinem, and Wieprecht, Ekkehard

Published
2022
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34. Bringing the New Adaptive Optics Module for Interferometry (NAOMI) into Operation

Author

Gonté, Frédéric, Abad, Jose Antonio, Abuter, Roberto, Aller Carpentier, Emmanuel, Alonso, Jaime, Andofalto, Luigi, Barriga, Pablo, Berger, Jean-Philippe, Beuzit, Jean-Luc, Blanchard, Israel, Bonnet, Henri, Bourdarot, Guillaume, Bourget, Pierre, Brast, Roland, Bristow, Paul, Caniguante, Luis, Cerda, Susana, Cid, Claudia, Correa, Alex, Cottalorda, Eric, Courtney-Barrer, Benjamin, Darré, Pascaline, Delabre, Bernard, Delboulbé, Alain, Dembet, Roderick, Donaldson, Ronald, Dorn, Reinhold, Dupeyron, Jorge, Dupuy, Christophe, Egner, Sebastian, Eisenhauer, Frank, Faundez, Lorena, Fedrigo, Enrico, Fischer, Gerhard, Frank, Christoph, Fuenteseca, Eloy, Gitton, Philippe, Guerlet, Thibaut, Guieu, Sylvain, Gutierrez, Pablo, Haguenauer, Pierre, Haimerl, Andreas, Haubois, Xavier, Heritier, Cédric, Huber, Stefan, Hubin, Norbert, Jolley, Paul, Jocou, Laurent, Kirchbauer, Jean-Paul, Kolb, Johann, Kosmalski, Johan, Krempl, Peter, La Fuente, Carlos, Le Bouquin, Jean-Baptiste, Le Louarn, Miska, Lilley, Paul, Lopez, Bruno, Lopez, Marcelo, Magnard, Yves, Marchetti, Enrico, Mclay, Stewart, Meilland, Anthony, Meister, Alexander, Mérand, Antoine, Moulin, Thibaut, Pasquini, Luca, Paufique, Jérôme, Percheron, Isabelle, Pettazzi, Lorenzo, Pfuhl, Oliver, Phan, Duc, Pino, Andres, Pirani, Werther, Quentin, Jutta, Rakich, Andrew, Ramirez, Andrés, Ridings, Robert, Riedel, Mario, Reyes, Javier, Rochat, Sylvain, Sanchez, Juan, Santos Tomás, Gonsalo, Schmid, Christian, Shchekaturov, Pavel, Schuhler, Nicolas, Seidel, Matthias, Soenke, Christian, Stadler, Eric, Stephan, Christian, Suárez, Marcos, Todorović, Mirko, Valdes, Guillermo, Verinaud, Cristophe, Woillez, Julien, Zins, Gérard, and Zúñiga-Fernández, Sebastian

Abstract

NAOMI was developed by a consortium composed of IPAG and ESO. Its Provisional Acceptance Chile review was held in April 2019. The NAOMI systems that have been installed on the Auxiliary Telescopes make the Very Large Telescope Interferometer (VLTI) and its instruments much less dependent on the atmospheric and dome seeing conditions. NAOMI increases the interferometer’s operability and improves the performance of its instruments and, very early on, was identified as being critical to the VLTI. In this article, we review the project, describe its principles and architecture, and offer a preview of the improvements it brings to VLTI instruments., Published in The Messenger vol. 177, pp. 19-23, September 2019.

Published
2019
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35. Nanobob: a CubeSat mission concept for quantum communication experiments in an uplink configuration

Author

Kerstel, Erik, Gardelein, Arnaud, Barthelemy, Mathieu, Fourati, Hassen, Gilot, Yves, Lecoarer, Etienne, Rodrigo, Juana, Sequies, Thierry, Borne, Vincent, Bourdarot, Guillaume, Burlet, Jean-Yves, Christidis, Alexis, Segura, Jesus, Boulanger, Benoit, Boutou, Veronique, Bouzat, Mylene, Chabanol, Mathieu, Fesquet, Laurent, Moulin, Michel, Niot, Jean-Michel, Bastos, Rodrigo Possamai, Robu, Bogdan, Rolland, Etienne, Toru, Sylvain, Fink, Matthias, Ursin, Rupert, Joshi, Siddarth Koduru, Laboratoire Interdisciplinaire de Physique [Saint Martin d’Hères] (LIPhy), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Joseph Fourier - Grenoble 1 (UJF), Université Grenoble Alpes (UGA), Air Liquide Advanced Technologies [Sassenage] (ALAT), Air Liquide [Siège Social], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Networked Controlled Systems (NECS), Inria Grenoble - Rhône-Alpes, Institut National de Recherche en Informatique et en Automatique (Inria)-Institut National de Recherche en Informatique et en Automatique (Inria)-Département Automatique (GIPSA-DA), Grenoble Images Parole Signal Automatique (GIPSA-lab), Université Pierre Mendès France - Grenoble 2 (UPMF)-Université Stendhal - Grenoble 3-Université Joseph Fourier - Grenoble 1 (UJF)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Pierre Mendès France - Grenoble 2 (UPMF)-Université Stendhal - Grenoble 3-Université Joseph Fourier - Grenoble 1 (UJF)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Grenoble Images Parole Signal Automatique (GIPSA-lab), Université Pierre Mendès France - Grenoble 2 (UPMF)-Université Stendhal - Grenoble 3-Université Joseph Fourier - Grenoble 1 (UJF)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Pierre Mendès France - Grenoble 2 (UPMF)-Université Stendhal - Grenoble 3-Université Joseph Fourier - Grenoble 1 (UJF)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), STMicroelectronics [Grenoble] (ST-GRENOBLE), Rolls Royce PLC, OPTIMA - Optique et Matériaux, Institut Néel (NEEL), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Techniques of Informatics and Microelectronics for integrated systems Architecture (TIMA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), SYSCO (GIPSA-SYSCO), Département Automatique (GIPSA-DA), Polytech Grenoble, Institute for Quantum Optics and Quantum Information [Innsbruck] (IQOQI), Austrian Academy of Sciences (OeAW), Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Centre Spatial Universitaire de Grenoble ( CSUG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Optique et Matériaux (NEEL - OPTIMA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Techniques de l'Informatique et de la Microélectronique pour l'Architecture des systèmes intégrés (TIMA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Grenoble Images Parole Signal Automatique (GIPSA-lab ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Grenoble Images Parole Signal Automatique (GIPSA-lab ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), GIPSA - Systèmes non linéaires et complexité (GIPSA-SYSCO), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), and Optique et Matériaux (OPTIMA )

Subjects
[SPI.OTHER]Engineering Sciences [physics]/Other, Photon, Quantum decoherence, Space segment, Quantum entanglement, Quantum key distribution, lcsh:Atomic physics. Constitution and properties of matter, Topology, 7. Clean energy, 01 natural sciences, Quantum, [SPI.AUTO]Engineering Sciences [physics]/Automatic, 010309 optics, Entanglement, Photon entanglement, 0103 physical sciences, Electronic engineering, lcsh:QC350-467, Electrical and Electronic Engineering, Quantum information, 010306 general physics, Quantum information science, ComputingMilieux_MISCELLANEOUS, Physics, QKD, CubeSat, Condensed Matter Physics, Atomic and Molecular Physics, and Optics, lcsh:QC170-197, PACS 8542, Control and Systems Engineering, Satellite, Cryptography, lcsh:Optics. Light, Uplink
Abstract

We present a ground-to-space quantum key distribution (QKD) mission concept and the accompanying feasibility study for the development of the associated low earth orbit nanosatellite payload. The quantum information is carried by single photons with the binary codes represented by polarization states of the photons. Distribution of entangled photons between the ground and the satellite can be used to certify the quantum nature of the link: a guarantee that no eavesdropping can take place. By placing the entangled photon source on the ground, the space segments contains “only” the less complex detection system, enabling its implementation in a compact enclosure, compatible with the 12U CubeSat standard ( ${\sim}12~\mbox{dm}^{3}$ ). This reduces the overall cost of the project, making it an ideal choice as a pathfinder for future European quantum communication satellite missions. The space segment is also more versatile than one that contains the source since it is compatible with a multiple of QKD protocols (not restricted to entangled photon schemes) and can be used in quantum physics experiments, such as the investigation of entanglement decoherence. Other possible experiments include atmospheric transmission/turbulence characterization, dark area mapping, fine pointing and tracking, and accurate clock synchronization; all crucial for future global scale quantum communication efforts.

Published
2018

38. Experimental test of a 40 cm-long R=100 000 spectrometer for exoplanet characterisation

Author

Bourdarot, Guillaume, primary, Le Coarer, Etienne, primary, Mouillet, David, primary, Jocou, Laurent, primary, Rabou, Patrick, primary, Correia, Jean-Jacques, primary, Bonfils, Xavier, primary, Stadler, Eric, primary, Carlotti, Alexis, primary, Forveille, Thierry, primary, Vigan, Arthur, primary, Artigau, Etienne, primary, Doyon, René, primary, Vallée, Philippe, primary, and Magnard, Yves, primary

Published
2018
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