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14 results on '"Fressin, F."'

2. ASTEP South: a first photometric analysis

Author

Crouzet, N., Guillot, T., M��karnia, D., Szul��gyi, J., Abe, L., Agabi, A., Fante��-Caujolle, Y., Gon��alves, I., Barbieri, M., Schmider, F. -X., Rivet, J. -P., Bondoux, E., Challita, Z., Pouzenc, C., Fressin, F., Valbousquet, F., Blazit, A., Bonhomme, S., Daban, J. -B., Gouvret, C., Bayliss, D., Zhou, G., and team, the ASTEP

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Phase (waves), FOS: Physical sciences, Binary number, Astronomy and Astrophysics, Astrophysics, Radial velocity, Photometry (optics), Quality (physics), Space and Planetary Science, Planet, Magnitude (astronomy), Short exposure, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract

The ASTEP project aims at detecting and characterizing transiting planets from Dome C, Antarctica, and qualifying this site for photometry in the visible. The first phase of the project, ASTEP South, is a fixed 10 cm diameter instrument pointing continuously towards the celestial South pole. Observations were made almost continuously during 4 winters, from 2008 to 2011. The point-to-point RMS of 1-day photometric lightcurves can be explained by a combination of expected statistical noises, dominated by the photon noise up to magnitude 14. This RMS is large, from 2.5 mmag at R=8 to 6% at R=14, because of the small size of ASTEP South and the short exposure time (30 s). Statistical noises should be considerably reduced using the large amount of collected data. A 9.9-day period eclipsing binary is detected, with a magnitude R=9.85. The 2-season lightcurve folded in phase and binned into 1000 points has a RMS of 1.09 mmag, for an expected photon noise of 0.29 mmag. The use of the 4 seasons of data with a better detrending algorithm should yield a sub-millimagnitude precision for this folded lightcurve. Radial velocity follow-up observations are conducted and reveal a F-M binary system. The detection of this 9.9-day period system with a small instrument such as ASTEP South and the precision of the folded lightcurve show the quality of Dome C for continuous photometric observations, and its potential for the detection of planets with orbital period longer than those usually detected from the ground., Comment: 5 pages, 3 figures, IAUS 288 conference proceedings

Published
2012
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3. Low False Positive Rate of Kepler Candidates Estimated From A Combination Of Spitzer And Follow-Up Observations

Author

Désert, JM, Charbonneau, D, Torres, G, Fressin, F, Ballard, S, Bryson, ST, Knutson, HA, Batalha, NM, Borucki, WJ, Brown, TM, Deming, D, Ford, EB, Fortney, JJ, Gilliland, RL, Latham, DW, and Seager, S

Subjects
detection [planets and satellites], Molecular, Astronomy & Astrophysics, Physical Chemistry, eclipses, Atomic, Particle and Plasma Physics, eclipsing [binaries], polarimetric [techniques], astro-ph.EP, Astrophysics::Solar and Stellar Astrophysics, Nuclear, Astrophysics::Earth and Planetary Astrophysics, planetary systems, Astronomical and Space Sciences, Astrophysics::Galaxy Astrophysics, Physical Chemistry (incl. Structural)
Abstract

© 2015. The American Astronomical Society. All rights reserved.. NASA's Kepler mission has provided several thousand transiting planet candidates during the 4 yr of its nominal mission, yet only a small subset of these candidates have been confirmed as true planets. Therefore, the most fundamental question about these candidates is the fraction of bona fide planets. Estimating the rate of false positives of the overall Kepler sample is necessary to derive the planet occurrence rate. We present the results from two large observational campaigns that were conducted with the Spitzer Space Telescope during the the Kepler mission. These observations are dedicated to estimating the false positive rate (FPR) among the Kepler candidates. We select a sub-sample of 51 candidates, spanning wide ranges in stellar, orbital, and planetary parameter space, and we observe their transits with Spitzer at 4.5 μm. We use these observations to measures the candidate's transit depths and infrared magnitudes. An authentic planet produces an achromatic transit depth (neglecting the modest effect of limb darkening). Conversely a bandpass-dependent depth alerts us to the potential presence of a blending star that could be the source of the observed eclipse: a false positive scenario. For most of the candidates (85%), the transit depths measured with Kepler are consistent with the transit depths measured with Spitzer as expected for planetary objects, while we find that the most discrepant measurements are due to the presence of unresolved stars that dilute the photometry. The Spitzer constraints on their own yield FPRs between 5% and depending on the Kepler Objects of Interest. By considering the population of the Kepler field stars, and by combining follow-up observations (imaging) when available, we find that the overall FPR of our sample is low. The measured upper limit on the FPR of our sample is 8.8% at a confidence level of 3σ. This observational result, which uses the achromatic property of planetary transit signals that is not investigated by the Kepler observations, provides an independent indication that Kepler's FPR is low.

Published
2015
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4. Kepler-62 : A five-planet system with planets of 1.4 and 1.6 Earth radii in the habitable zone

Author

Borucki, W.J., Agol, E., Fressin, F., Kaltenegger, L., Rowe, J., Isaacson, H., Fischer, D., Batalha, N., Lissauer, J.J., Marcy, G.W., Fabrycky, D., Dxe9sert, J.-M., Bryson, S.T., Barclay, Thomas, Bastien, F., Boss, A., Brugamyer, E., Buchhave, L.A., Burke, C., Caldwell, D.A., Carter, J., Charbonneau, D., Crepp, J.R., Christensen-Dalsgaard, J., Christiansen, J.L., Ciardi, D., Cochran, W.D., DeVore, E., Doyle, L., Dupree, A.K., Endl, M., Everett, M.E., Ford, E.B., Fortney, J., Gautier III, T.N., Geary, et al., Borucki, W.J., Agol, Fressin, Kaltenegger, Rowe, Isaacson, Fischer, Batalha, Lissauer, J.J., Marcy, G.W., Fabrycky, Dxe9sert, J.-M., Bryson, S.T., Barclay, Thomas, Bastien, Boss, Brugamyer, Buchhave, L.A., Burke, Caldwell, D.A., Carter, Charbonneau, Crepp, J.R., Christensen-Dalsgaard, Christiansen, J.L., Ciardi, Cochran, W.D., DeVore, Doyle, Dupree, A.K., Endl, Everett, M.E., Ford, E.B., Fortney, Gautier III, T.N., and Geary

Published
2013

5. Exoplanet characterization by proxy: A transiting 2.15 R⊕ planet near the habitable zone of the late k dwarf kepler-61

Author

Shporer, A., Crepp, J.R., Horch, E.P., Ballard, S., Everett, M.E., Fressin, F., Bryson, S.T., Torres, G., Charbonneau, D., Henze, C.E., Howell, S.B., Ciardi, D.R., Irwin, J., Newton, E., Desert, J.-M., and Mann, A.W.

Abstract

We present the validation and characterization of Kepler-61b: a 2.15 R ⊕ planet orbiting near the inner edge of the habitable zone of a low-mass star. Our characterization of the host star Kepler-61 is based upon a comparison with a set of spectroscopically similar stars with directly measured radii and temperatures. We apply a stellar prior drawn from the weighted mean of these properties, in tandem with the Kepler photometry, to infer a planetary radius for Kepler-61b of 2.15 ± 0.13 R ⊕ and an equilibrium temperature of 273 ± 13 K (given its period of 59.87756 ± 0.00020 days and assuming a planetary albedo of 0.3). The technique of leveraging the physical properties of nearby "proxy" stars allows for an independent check on stellar characterization via the traditional measurements with stellar spectra and evolutionary models. In this case, such a check had implications for the putative habitability of Kepler-61b: the planet is 10% warmer and larger than inferred from K-band spectral characterization. From the Kepler photometry, we estimate a stellar rotation period of 36 days, which implies a stellar age of >1 Gyr. We summarize the evidence for the planetary nature of the Kepler-61 transit signal, which we conclude is 30,000 times more likely to be due to a planet than a blend scenario. Finally, we discuss possible compositions for Kepler-61b with a comparison to theoretical models as well as to known exoplanets with similar radii and dynamically measured masses.

Published
2013
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6. Transiting exoplanets from the CoRoT space mission VIII. CoRoT-7b: the first super-Earth with measured radius

Author

Leger, A., Rouan, D., Jodi Schneider, Barge, P., Fridlund, M., Samuel, B., Ollivier, M., Guenther, E., Deleuil, M., Deeg Hj, Auvergne, M., Alonso, R., Aigrain, S., Alapini, A., Almenara Jm, Baglin, A., Barbieri, M., Bruntt, H., Pascal Bordé, Bouchy, F., Cabrera, J., Catala, C., Carone, L., Carpano, S., Csizmadia, S., Dvorak, R., Erikson, A., Ferraz-Mello, S., Foing, B., Grasset, O., Fressin, F., Gandolfi, D., Gillon, M., Gondoin, P., Guillot, T., Hatzes, A., Hebrard, G., Jorda, L., Lammer, H., Llebaria, A., Loeillet, B., Mayor, M., Mazeh, T., Moutou, C., Patzold, M., Pont, F., Queloz, D., Rauer, H., Renner, S., Samadi, R., Shporer, A., Sotin, C., Tingley, B., Wuchterl, G., Adda, M., Agogu, P., Appourchaux, T., Ballans, H., Baron, P., Beaufort, T., Bellenger, R., Berlin, R., Bernardi, P., Blouin, D., Baudin, F., Bodin, P., Boisnard, L., Boit, L., Bonneau, F., Borzeix, S., Briet, R., Buey Jt, Butler, B., Cailleau, D., Cautain, R., Chabaud Py, Chaintreuil, S., Chiavassa, F., Costes V, Parrho Vc, Fialho Fd, Decaudin, M., Defise Jm, Djalal, S., Epstein, G., Exil Ge, Faure, C., Fenouillet, T., Gaboriaud, A., Gallic, A., Gamet, P., Gavalda, P., Grolleau, E., Gruneisen, R., Gueguen, L., Guis, V., V. Guivarc'H, Guterman, P., Hallouard, D., Hasiba, J., Heuripeau, F., Huntzinger, G., Hustaix, H., Imad, C., Imbert, C., Johlander, B., Jouret, M., Journoud, P., Karioty, F., Kerjean, L., Lafaille, V., Lafond, L., Lam-Trong, T., Landiech, P., Lapeyrere, V., Larque, T., Laudet, P., Lautier, N., Lecann, H., Lefevre, L., Leruyet, B., Levacher, P., Magnan, A., Mazy, E., Mertens, F., Mesnager Jm, Meunier Jc, Michel Jp, Monjoin, W., Naudet, D., Nguyen-Kim, K., Orcesi Jl, Ottacher, H., Perez, R., Peter, G., Plasson, P., Plesseria Jy, Pontet, B., Pradines, A., Céline Quentin, Reynaud Jl, Rolland, G., Rollenhagen, F., Romagnan, R., Russ, N., Schmidt, R., Schwartz, N., Sebbag, I., Sedes, G., Smit, H., Steller Mb, Sunter, W., Surace, C., Tello, M., Tiphene, D., Toulouse, P., Ulmer, B., Vandermarcq, O., Vergnault, E., Vuillemin, A., Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), and Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA)

Subjects
[SDU.STU]Sciences of the Universe [physics]/Earth Sciences, ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2009

7. Technical development status of A STEP 400

Author

Daban, J, Gouvret, C, Agabi, A, Guillot, T, Fressin, F, Abe, L, Crouzet, N, Fanté-Caujolle, Y, Peron, S, Ottogalli, S, Rivet, J, Schmider, F, Valbousquet, F, Blanc, P, Dugù, M, Roussel, A, Assus, P, Bresson, Y, Blazit, A, Bondoux, E, Chatilla, Z, Le Van Suu, A, Merzougui, M, Fossat, E, Jeanneaux, F, Rauer, Heike, Erikson, Anders, Pont, F, Aigrain, S, and Tothill, N

Subjects
photometry, ARENA, Antartica, ASTEP, Dome C
Published
2008

8. A STEP: Towards a Large Photometric Survey for Exoplanets at Dome C

Author

Fressin, F., Guillot, T., Schmider, F.-X., Agabi, A., Moutou, C., Aigrain, S., Bouchy, F., Boer, M., Pont, F., Erikson, Anders, Rauer, Heike, and A STEP team

Subjects
Physics, Scintillation, transit search, Astrophysics::Instrumentation and Methods for Astrophysics, General Engineering, Astronomy, Astronomy and Astrophysics, Astrophysics, Schmidt camera, Exoplanet, law.invention, Telescope, Stars, exoplanets, Space and Planetary Science, law, Planet, Magnitude (astronomy), Astrophysics::Solar and Stellar Astrophysics, A STEP, Astrophysics::Earth and Planetary Astrophysics, Transit (astronomy), Astrophysics::Galaxy Astrophysics
Abstract

We present "A STEP" (Antarctica Search for Transiting Extrasolar Planets), a project dedicated to the search for planetary transits from Antartica. The project consists of a semi-automatic ∼40 cm telescope equipped with a 16-million-pixel CCD installed at Dome C. The site offers crucial assets for a ground-based exoplanet transit search: uninterrupted phase coverage, excellent weather, low air-mass variations and reduced scintillation. This system would be able to detect Pegasids transiting in front of stars as faint as magnitude sixteen and could also detect smaller planets in close-in period around brighter stars. This short term project is meant to be a photometric qualifyer for the site and the first stage of a massive detection campaign. A mid-term objective of 1000 detections for 2012 could be achieved either with many small telescopes or with a large Schmidt telescope with a large field of view. The project is relatively simple and cost-effective, and has the double purpose of qualifying the site and obtaining first-class scientific results. Our team is already familiar with transit detection with an automated telescope and cold temperature qualification. © EAS, EDP Sciences 2007.

Published
2007

9. The CoRoT exoplanet programme: exploring the gas-giant/terrestrial planet transition

Author

Aigrain, S., Barge, P., Deleuil, M., Fressin, F., Moutou, C., Queloz, D., Auvergne, M., Baglin, A., and Team, the CoRoT Exoplanet Science

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics
Abstract

CoRoT, which was launched successfully on the 27th of December 2006, is the first space mission to have the search for planetary transits at the heart of its science programme. It is expected to be able to detect transits of planets with radii down to approximately two Earth radii and periods up to approximately a month. Thus, CoRoT will explore the hereto uncharted area of parameter space which spans the transition between the gaseous giant planets discovered in large numbers from the ground, and terrestrial planets more akin to our own. This papers briefly sketches out the main technical characteristics of the mission before summarising estimates of its detection potential and presenting the data analysis and follow-up strategy., Comment: 10 pages, 2 figures. A version with full resolution figures is available from http://www.ast.cam.ac.uk/~suz/publi/CS14_corot.pdf

Published
2007
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10. Transdet: a Matched-filter based Algorithm for Transit Detection -- Application to Simulated COROT Light Curves

Author

Bordé, P., Fressin, F., Ollivier, M., Léger, A., Rouan, D., 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), Pôle Astronomie du LESIA, and 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris

Subjects
Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We present a matched-filter based algorithm for transit detection and its application to simulated COROT light curves. This algorithm stems from the work by Bord��, Rouan & L��ger (2003). We describe the different steps we intend to take to discriminate between planets and stellar companions using the three photometric bands provided by COROT. These steps include the search for secondary transits, the search for ellipsoidal variability, and the study of transit chromaticity. We also discuss the performance of this approach in the context of blind tests organized inside the COROT exoplanet consortium., 6 pages, 4 figures, in Transiting Extrasolar Planets Workshop, meeting held in Heidelberg, 25-28 September 2006

Published
2006

11. The A STEP project

Author

Fressin, F., Rauer, H., Erikson, A., Guillot, T., Gay, J., Rabbia, Y., Rivet, J.P., Pout, F., Bouchny, F., Monton, C., and Léger, A.

Published
2004

12. Transiting Exoplanet Survey Satellite (TESS)

Author

Ricker, G.~R., Winn, J.~N., Vanderspek, R, Latham, D.~W., Bakos, G.~Á., Bean, J.~L., Berta-Thompson, Z.~K., Brown, T.~M., Buchhave, L, Butler, N.~R., Butler, R.~P., Chaplin, W.~J., Charbonneau, D, Christensen-Dalsgaard, J, Clampin, M, Deming, D, Doty, J, De Lee, N, Dressing, C, Dunham, E.~W., Endl, M, Fressin, F, Ge, J, Henning, T, Holman, M.~J., Howard, A.~W., IDA, SHIGERU, Jenkins, J.~M., Jernigan, G, Johnson, J.~A., Kaltenegger, L, Kawai, Nobuyuki, Kjeldsen, H, Laughlin, G, Levine, A.~M., Lin, D, Lissauer, J.~J., MacQueen, P, Marcy, G, McCullough, P.~R., Morton, T.~D., Narita, N, Paegert, M, Palle, E, Pepe, F, Pepper, J, Quirrenbach, A, Rinehart, S.~A., Sasselov, D, Sato, Bunei, Seager, S, Sozzetti, A, Stassun, K.~G., Sullivan, P, Szentgyorgyi, A, Torres, G, Udry, S, and Villasenor, J

Published
2015

14. Expected Performance of the CoRoT Planet Search from Light Curve Beauty Contests

Author

Moutou, C., Aigrain, S., Almenara, J., Alonso, R., Auvergne, M., Barge, P., Blouin, D., Borde, P., Cabrera, J., Carone, L., Cautain, R., Deeg, H., Erikson, A., Fressin, F., Guis, V., Leger, A., Guterman, P., Irwin, M., Kabath, P., Antonino Francesco Lanza, Maceroni, C., Mazeh, T., Ollivier, M., Pont, F., Paetzold, M., Queloz, D., Rauer, H., Rouan, D., Schneider, J., Tamuz, O., Voss, H., Zucker, S., 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), Pôle Astronomie du LESIA, and 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)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience

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