362 results on '"Marois C"'
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2. The vector-apodizing phase plate coronagraph: design, current performance, and future development
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Doelman, D. S., Snik, F., Por, E. H., Bos, S. P., Otten, G. P. P. L., Kenworthy, M., Haffert, S. Y., Wilby, M., Bohn, A. J., Sutlieff, B. J., Miller, K., Ouellet, M., de Boer, J., Keller, C. U., Escuti, M. J., Shi, S., Warriner, N. Z., Hornburg, K. J., Birkby, J. L., Males, J., Morzinski, K. M., Close, L. M., Codona, J., Long, J., Schatz, L., Lumbres, J., Rodack, A., Van Gorkom, K., Hedglen, A, Guyon, O., Lozi, J., Groff, T., Chilcote, J., Jovanovic, N., Thibault, S., de Jonge, C., Allain, G., Vallée, C., Patel, D., Côté, O., Marois, C., Hinz, P., Stone, J., Skemer, A., Briesemeister, Z., Boehle, A., Glauser, A. M., Taylor, W., Baudoz, P., Huby, E., Absil, O., Carlomagno, B., and Delacroix, C.
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Over the last decade, the vector-apodizing phase plate (vAPP) coronagraph has been developed from concept to on-sky application in many high-contrast imaging systems on 8-m class telescopes. The vAPP is an geometric-phase patterned coronagraph that is inherently broadband, and its manufacturing is enabled only by direct-write technology for liquid-crystal patterns. The vAPP generates two coronagraphic PSFs that cancel starlight on opposite sides of the point spread function (PSF) and have opposite circular polarization states. The efficiency, that is the amount of light in these PSFs, depends on the retardance offset from half-wave of the liquid-crystal retarder. Using different liquid-crystal recipes to tune the retardance, different vAPPs operate with high efficiencies ($>96\%$) in the visible and thermal infrared (0.55 $\mu$m to 5 $\mu$m). Since 2015, seven vAPPs have been installed in a total of six different instruments, including Magellan/MagAO, Magellan/MagAO-X, Subaru/SCExAO, and LBT/LMIRcam. Using two integral field spectrographs installed on the latter two instruments, these vAPPs can provide low-resolution spectra (R$\sim$30) between 1 $\mu$m and 5 $\mu$m. We review the design process, development, commissioning, on-sky performance, and first scientific results of all commissioned vAPPs. We report on the lessons learned and conclude with perspectives for future developments and applications., Comment: 38 pages, 17 figures, accepted for publication in Applied Optics, added NSF grant acknowledgement
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- 2021
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3. Gemini Planet Imager Spectroscopy of the Dusty Substellar Companion HD 206893 B
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Ward-Duong, K., Patience, J., Follette, K., De Rosa, R. J., Rameau, J., Marley, M., Saumon, D., Nielsen, E. L., Rajan, A., Greenbaum, A. Z., Lee, J., Wang, J. J., Czekala, I., Duchêne, G., Macintosh, B., Ammons, S. Mark, Bailey, V. P., Barman, T., Bulger, J., Chen, C., Chilcote, J., Cotten, T., Doyon, R., Esposito, T. M., Fitzgerald, M. P., Gerard, B. L., Goodsell, S. J., Graham, J. R., Hibon, P., Hom, J., Hung, L. -W., Ingraham, P., Kalas, P., Konopacky, Q., Larkin, J. E., Maire, J., Marchis, F., Marois, C., Metchev, S., Millar-Blanchaer, M. A., Oppenheimer, R., Palmer, D., Perrin, M., Poyneer, L., Pueyo, L., Rantakyrö, F. T., Ren, B., Ruffio, J. -B., Savransky, D., Schneider, A. C., Sivaramakrishnan, A., Song, I., Soummer, R., Tallis, M., Thomas, S., Wallace, J. Kent, Wiktorowicz, S., and Wolff, S.
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Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
We present new near-infrared Gemini Planet Imager (GPI) spectroscopy of HD 206893 B, a substellar companion orbiting within the debris disk of its F5V star. The $J$, $H$, $K1$, and $K2$ spectra from GPI demonstrate the extraordinarily red colors of the object, confirming it as the reddest substellar object observed to date. The significant flux increase throughout the infrared presents a challenging atmosphere to model with existing grids. Best-fit values vary from 1200 K to 1800 K for effective temperature and from 3.0 to 5.0 for log($g$), depending on which individual wavelength band is fit and which model suite is applied. The extreme redness of the companion can be partially reconciled by invoking a high-altitude layer of sub-micron dust particles, similar to dereddening approaches applied to the peculiar red field L-dwarf population. However, reconciling the HD 206893 B spectra with even those of the reddest low-gravity L-dwarf spectra still requires the contribution of additional atmospheric dust, potentially due to the debris disk environment in which the companion resides. Orbit fitting from four years of astrometric monitoring is consistent with a $\sim$30-year period, orbital inclination of 147$^{\circ}$, and semimajor axis of 10 au, well within the estimated disk inner radius of $\sim$50 au. As one of very few substellar companions imaged interior to a circumstellar disk, the properties of this system offer important dynamical constraints on companion-disk interaction and provide a benchmark for substellar and planetary atmospheric study., Comment: Accepted for publication in AJ (October 15, 2020). 35 pages, 20 figures, with tables and appendices presented in their entirety
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- 2020
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4. Imaging the 44 AU Kuiper Belt-analogue debris ring around HD 141569A with GPI polarimetry
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Bruzzone, J. S., Metchev, S., Duchene, G., Millar-Blanchaer, M. A., Dong, R., Wang, J. J., Graham, J. R., Mazoyer, J., Wolff, S., Ammons, S. M., Schneider, A. C., Greenbaum, A. Z., Matthews, B. C., Arriaga, P., Bailey, V. P., Barman, T., Bulger, J., Chilcote, J., Cotten, T., De Rosa, R. J., Doyon, R., Fitzgerald, M. P., Follette, K. B., Gerard, B. L., Goodsell, S. J., Hibon, P., Hom, J., Hung, L. -W., Ingraham, P., Kalas, P., Konopacky, Q., Larkin, J. E., Macintosh, B., Maire, J., Marchis, F., Marois, C., Morzinski, K. M., Nielsen, E. L., Oppenheimer, R., Palmer, D., Patel, R., Patience, J., Perrin, M., Poyneer, L., Pueyo, L., Rajan, A., Rameau, J., Rantakyro, F. T., Savransky, D., Sivaramakrishnan, A., Song, I., Soummer, R., Thomas, S., Wallace, J. K., Ward-Duong, K., and Wiktorowicz, S.
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Astrophysics - Solar and Stellar Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present the first polarimetric detection of the inner disk component around the pre-main sequence B9.5 star HD 141569A. Gemini Planet Imager H-band (1.65 micron) polarimetric differential imaging reveals the highest signal-to-noise ratio detection of this ring yet attained and traces structure inwards to 0.25" (28 AU at a distance of 111 pc). The radial polarized intensity image shows the east side of the disk, peaking in intensity at 0.40" (44 AU) and extending out to 0.9" (100 AU). There is a spiral arm-like enhancement to the south, reminiscent of the known spiral structures on the outer rings of the disk. The location of the spiral arm is coincident with 12CO J=3-2 emission detected by ALMA, and hints at a dynamically active inner circumstellar region. Our observations also show a portion of the middle dusty ring at ~220 AU known from previous observations of this system. We fit the polarized H-band emission with a continuum radiative transfer Mie model. Our best-fit model favors an optically thin disk with a minimum dust grain size close to the blow-out size for this system: evidence of on-going dust production in the inner reaches of the disk. The thermal emission from this model accounts for virtually all of the far-infrared and millimeter flux from the entire HD 141569A disk, in agreement with the lack of ALMA continuum and CO emission beyond ~100 AU. A remaining 8-30 micron thermal excess a factor of ~2 above our model argues for a yet-unresolved warm innermost 5-15 AU component of the disk., Comment: 16 pages, 8 figures, accepted at AJ
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- 2019
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5. Directly Imaging Rocky Planets from the Ground
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Mazin, B., Artigau, É., Bailey, V., Baranec, C., Beichman, C., Benneke, B., Birkby, J., Brandt, T., Chilcote, J., Chun, M., Close, L., Currie, T., Crossfield, I., Dekany, R., Delorme, J. R., Dong, C., Dong, R., Doyon, R., Dressing, C., Fitzgerald, M., Fortney, J., Frazin, R., Gaidos, E., Guyon, O., Hashimoto, J., Hillenbrand, L., Howard, A., Jensen-Clem, R., Jovanovic, N., Kotani, T., Kawahara, H., Konopacky, Q., Knutson, H., Liu, M., Lu, J., Lozi, J., Macintosh, B., Males, J., Marley, M., Marois, C., Mawet, D., Meeker, S., Millar-Blanchaer, M., Mondal, S., Bose, S. N., Murakami, N., Murray-Clay, R., Narita, N., Pyo, T. S., Roberts, L., Ruane, G., Serabyn, G., Shields, A., Skemer, A., Simard, L., Stelter, D., Tamura, M., Troy, M., Vasisht, G., Wallace, J. K., Wang, J., and Wright, S.
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Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
Over the past three decades instruments on the ground and in space have discovered thousands of planets outside the solar system. These observations have given rise to an astonishingly detailed picture of the demographics of short-period planets, but are incomplete at longer periods where both the sensitivity of transit surveys and radial velocity signals plummet. Even more glaring is that the spectra of planets discovered with these indirect methods are either inaccessible (radial velocity detections) or only available for a small subclass of transiting planets with thick, clear atmospheres. Direct detection can be used to discover and characterize the atmospheres of planets at intermediate and wide separations, including non-transiting exoplanets. Today, a small number of exoplanets have been directly imaged, but they represent only a rare class of young, self-luminous super-Jovian-mass objects orbiting tens to hundreds of AU from their host stars. Atmospheric characterization of planets in the <5 AU regime, where radial velocity (RV) surveys have revealed an abundance of other worlds, is technically feasible with 30-m class apertures in combination with an advanced AO system, coronagraph, and suite of spectrometers and imagers. There is a vast range of unexplored science accessible through astrometry, photometry, and spectroscopy of rocky planets, ice giants, and gas giants. In this whitepaper we will focus on one of the most ambitious science goals --- detecting for the first time habitable-zone rocky (<1.6 R_Earth) exoplanets in reflected light around nearby M-dwarfs, Comment: 8 pages, 1 figure, Astro2020 Science White Paper
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- 2019
6. Lack of association between classical HLA genes and asymptomatic SARS-CoV-2 infection
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Marchal, A, Cirulli, E, Neveux, I, Bellos, E, Thwaites, R, Schiabor Barrett, K, Zhang, Y, Nemes-Bokun, I, Kalinova, M, Catchpole, A, Tangye, S, Spaan, A, Lack, J, Ghosn, J, Burdet, C, Gorochov, G, Tubach, F, Hausfater, P, Abel, L, Aiuti, A, Al-Muhsen, S, Al-Mulla, F, Amara, A, Anderson, M, Andreakos, E, Arias, A, Arkin, L, Feldman, H, Bastard, P, Belot, A, Biggs, C, Bogunovic, D, Bolze, A, Bondarenko, A, Borghesi, A, Bousfiha, A, Brodin, P, Bryceson, Y, Butte, M, Casanova, J, Casari, G, Christodoulou, J, Cobat, A, Colobran, R, Condino-Neto, A, Constantinescu, S, Cooper, M, Dalgard, C, Desai, M, Drolet, B, Duval, X, El Baghdadi, J, Eloy, P, Espinosa-Padilla, S, Fellay, J, Flores, C, Franco, J, Froidure, A, Gregersen, P, Grimbacher, B, Haerynck, F, Hagin, D, Halwani, R, Hammarstrom, L, Heath, J, Hsieh, E, Husebye, E, Imai, K, Itan, Y, Jouanguy, E, Kaja, E, Karamitros, T, Kisand, K, Ku, C, Lau, Y, Ling, Y, Lucas, C, Maniatis, T, Mansouri, D, Marodi, L, Mentre, F, Meyts, I, Milner, J, Mironska, K, Mogensen, T, Morio, T, Ng, L, Notarangelo, L, Novelli, A, Novelli, G, O'Farrelly, C, Okada, S, Okamoto, K, Ozcelik, T, Pan-Hammarstrom, Q, Pape, J, Perez de Diego, R, Perez-Tur, J, Perlin, D, Pesole, G, Planas, A, Prando, C, Pujol, A, Puel, A, Quintana-Murci, L, Ramaswamy, S, Renia, L, Resnick, I, Rodriguez-Gallego, C, Sancho-Shimizu, V, Sediva, A, Seppanen, M, Shahrooei, M, Shcherbina, A, Slaby, O, Snow, A, Soler-Palacin, P, Soumelis, V, Tancevski, I, Tayoun, A, Temel, S, Thorball, C, Tiberghien, P, Trouillet-Assant, S, Turvey, S, Uddin, K, Uddin, M, van de Beek, D, Vinh, D, von Bernuth, H, Wauters, J, Zatz, M, Zawadzki, P, Zhang, Q, Zhang, S, Bureau, S, Vacher, Y, Gysembergh-Houal, A, Demerville, L, Benleulmi-Chaachoua, A, Abad, S, Abassi, R, Abdellaoui, A, Abdelmalek, A, Abdoul, H, Abergel, H, Abeud, F, Abgrall, S, Abisror, N, Adechian, M, Aderdour, N, Admane, H, Adnet, F, Afritt, S, Agostini, H, Aguilar, C, Agut, S, Aiello, T, Kaci, M, Oufella, H, Ajeenthiravasan, G, Alauzy, V, Alby-Laurent, F, Allard, L, Alyanakian, M, Borrero, B, Amam, S, Amrouche, L, Andronikof, M, Anglicheau, D, Anguel, N, Annane, D, Aounzou, M, Aparicio, C, Aratus, G, Arlet, J, Arzoine, J, Aslangul, E, Assefi, M, Aubry, A, Audiffred, L, Audureau, E, Auger, C, Auregan, J, Awotar, C, Milla, S, Azan, D, Azemar, L, Azzouguen, B, Elrufaai, M, Badsi, A, Bakouboula, P, Balcerowiak, C, Balde, F, Baldivia, E, Bangamingo, E, Baptiste, A, Baran-Marszak, F, Barau, C, Barget, N, Baronnet, F, Barthelemy, R, Baudel, J, Baudry, C, Baudry, E, Beaugerie, L, Belamri, A, Belaube, N, Belilita, R, Bellassen, P, Belmokhtar, R, Beltran, I, Benainous, R, Benallaoua, M, Benamouzig, R, Benbara, A, Benhida, J, Benkhelouf, A, Benlagha, J, Benmostafa, C, Benothmane, S, Bentifraouine, M, Berard, L, Bernier, Q, Berti, E, Bertier, A, Berton, L, Bessis, S, Beurton, A, Bianco, C, Bianquis, C, Bidar, F, Blanche, P, Blayau, C, Bleibtreu, A, Blin, E, Bloch-Queyrat, C, Boissier, M, Bollens, D, Bolzoni, M, Bompard, R, Bonnet, N, Bonnouvrier, J, Botha, S, Boucenna, W, Bouchama, F, Bouchaud, O, Bouchghoul, H, Boudjebla, T, Boudjema, N, Bouffard, C, Bougle, A, Bouguerra, M, Bouras, L, Bourcier, A, Durand, A, Bourrier, A, Bouscarat, F, Bouvry, D, Bouziri, N, Bouzrara, O, Bribier, S, Brugier, D, Brunel, M, Bui, E, Buisson, A, Bukreyeva, I, Bureau, C, Cadranel, J, Cailhol, J, Calin, R, Vega, C, Canavaggio, P, Cancella, M, Cantin, D, Cao, A, Carbillon, L, Carlier, N, Cassard, C, Castor, G, Cauchy, M, Cha, O, Chaigne, B, Challal, S, Champion, K, Chariot, P, Chas, J, Chauveau, S, Chauvin, A, Chauvin, C, Chavarot, N, Chebbout, K, Cherai, M, Cherubini, I, Chevalier, A, Chiarabini, T, Chinet, T, Chocron, R, Choinier, P, Chommeloux, J, Choquet, C, Choupeaux, L, Chousterman, B, Ciocan, D, Clarke, A, Clavere, G, Clavier, F, Clement, K, Clerc, S, Cohen, Y, Cohen, F, Cohen, A, Coilly, A, Colboc, H, Colin, P, Collet, M, Comarmond, C, Combacon, E, Combes, A, Comparon, C, Constantin, J, Cordel, H, Cordier, A, Costantini, A, Chalumeau, N, Couffignal, C, Coupeau, D, Creange, A, Lamarre, Y, Da Silveira, C, Guibal El Kayani, S, De Castro, N, De Rycke, Y, Del Pozo, L, Delannoy, Q, Delay, M, Deleris, R, Delforge, J, Delphine, L, Demare, N, Demeret, S, Demoule, A, Deniau, A, Depret, F, Derolez, S, Derradji, O, Derridj, N, Descamps, V, Deschamps, L, Desconclois, C, Desnos, C, Desongins, K, Dhote, R, Diallo, B, Didier, M, Diemer, M, Diez, S, Djadi-Prat, J, Djamouri Monnory, F, Djebara, S, Djebra, N, Djietcheu, M, Djillali, H, Djouadi, N, Donneger, S, Santos, C, Dournon, N, Dres, M, Droctove, L, Drogrey, M, Dropy, M, Drouet, E, Dubosq, V, Dubreucq, E, Dubus, E, Duchemann, B, Duchenoy, T, Dudoignon, E, Dufau, R, Dumas, F, Duran, C, Duron, E, Durrbach, A, Duvivier, C, Ebstein, N, El Khalifa, J, Elabbadi, A, Elie, C, Ernotte, G, Esling, A, Etienne, M, Eyer, X, Fartoukh, M, Fayali, T, Fermaut, M, Fiorentino, A, Fliss, S, Fournier, M, Fournier, B, Francois, H, Freynet, O, Frigout, Y, Fromont, I, Fuentes, A, Furet, T, Galand, J, Garnier, M, Gaubert, A, Gaudry, S, Gaugain, S, Gauthier, D, Gautier, M, Georgin-Lavialle, S, Geromin, D, Ghalayini, M, Ghaleh, B, Ghezal, M, Gibelin, A, Gimeno, L, Girard, B, Leprieur, B, Gomes, D, Gomes-Pires, E, Gouge, A, Gouja, A, Goulet, H, Goupil, S, De Bouille, J, Gras, J, Greffe, S, Grimaldi, L, Guedeney, P, Guidet, B, Guillo, M, Gulczynski, M, Hadjam, T, Haguenauer, D, Hammal, S, Hammoudi, N, Hanon, O, Harrois, A, Hautem, C, Hekimian, G, Heming, N, Hermine, O, Ho, S, Houllier, M, Huot, B, Huscenot, T, Saied, W, Ikherbane, G, Imarazene, M, Ingiliz, P, Iratni, L, Jaureguiberry, S, Jean-Marc, J, Jeyarajasingham, D, Jouany, P, Jouis, V, Jourdaine, C, Kafif, O, Kallala, R, Katsahian, S, Kelesyan, L, Keo, V, Ketz, F, Khamis, W, Khelili, E, Khellaf, M, Kotokpo Youkou, C, Kounis, I, Kpalma, G, Krause, J, Labbe, V, Lacombe, K, Lacorte, J, Lafont, A, Lafont, E, Lagha, L, Lamhaut, L, Lancelot, A, Landman, C, Lanternier, F, Larcheveque, C, Combe, C, Lassel, L, Laverdant, B, Lavergne, C, Lavillegrand, J, Lazureanu, P, Le Guennec, L, Leberre, L, Leblanc, C, Leboyer, M, Lecomte, F, Lecorre, M, Leenhardt, R, Lefebvre, M, Lefebvre, B, Legendre, P, Leger, A, Legros, L, Legrosse, J, Lehuunghia, S, Lemarec, J, Leporrier-Ext, J, Lesein, M, Lesur, H, Levy, V, Levy, A, Lopes, E, Lopes, A, Lopez, V, Lopinto, J, Lortholary, O, Louadah, B, Loze, B, Lucas, M, Lucasamichi, A, Luong, L, Magazimama-Ext, A, Maingret, D, Mameri, L, Manivet, P, Mansouri, C, Marcault, E, Marey, J, Marin, N, Marois, C, Martin, O, Martineau, L, Martinez-Lopez, C, Martyniuck, P, De Farcy, P, Marzouk, N, Masmoudi, R, Mebazaa, A, Mechai, F, Mecozzi, F, Mediouni, C, Megarbane, B, Meghadecha, M, Mejean, E, Mekinian, A, Abdelhadi, N, Mekni, R, Meliti, T, Lima, B, Meng, P, Merbah, S, Messani, F, Messaoudi, Y, Mewasing, B, Meziane, L, Michelot-Burger, C, Mignot, F, Minka, F, Miyara, M, Moine, P, Molina, J, Montegnies-Boulet, A, Monti, A, Montlahuc, C, Montout, A, Moores, A, Morbieu, C, Mortelette, H, Mouly, S, Muzaffar, R, Nacerddine, C, Nadal, M, Nadif, H, Nassarmadji, K, Natella, P, Ndingamondze, S, Neraal, S, Nguyen, C, N'Guyen, B, Larmurier, I, Nlomenyengue, L, Noel, N, Nunes, H, Omar, E, Ouazene, Z, Ouedraogo, E, Ouelaa, W, Oukhedouma, A, Amara, Y, Oya, H, Oziel, J, Padilla, T, Paillaud, E, Paiva, S, Parfait, B, Parize, P, Parizot, C, Parrot, A, Pavot, A, Peaudecerf, L, Pene, F, Pepin, M, Pernet, J, Pernin, C, Petit, M, Peyrony, O, Pietri, M, Pietri, O, De Chambrun, M, Pinson, M, Pintado, C, Piquard, V, Pires, C, Planquette, B, Poirier, S, Pomel, A, Pons, S, Ponscarme, D, Pourcelot, A, Pourcher, V, Pouvaret, A, Prever, F, Previlon, M, Prevost, M, Provoost, M, Quemeneur, C, Rafat, C, Rami, A, Ranque, B, Raphael, M, Raphalen, J, Rastoin, A, Raux, M, Rebai, A, Reby, M, Regent, A, Regrag, A, Resche-Rigon, M, Ressaire, Q, Richard, C, Richard, M, Robert, M, Rohaut, B, Rolland-Debord, C, Ropers, J, Roque-Afonso, A, Rosso, C, Rousseaux, M, Rousseaux, N, Roux, S, Roux, L, Rouzaud, C, Rozes, A, Rubenstein, E, Sabate, J, Sabet, S, Sacleux, S, Kermanach, N, Saliba, F, Salmon, D, Savale, L, Savary, G, Sberro, R, Scemla, A, Schlemmer, F, Schwartz, M, Sedfi, S, Sefir-Kribel, S, Seksik, P, Sellier, P, Selves, A, Sembach, N, Semerano, L, Senat, M, Sene, D, Serris, A, Sese, L, Sghiouar, N, Sigaux, J, Siguier, M, Silvain, J, Simon, N, Simon, T, Skandri, L, Slimani, M, Snauwaert, A, Sokol, H, Soliman, H, Soltani, N, Soyer, B, Steg, G, Suarez, L, Szwebel, T, Taffame, K, Tandjaoui-Lambiotte, Y, Tantet, C, Tateo, M, Theodose, I, Thiebaud, P, Thomas, C, Tiercelet, K, Tisserand, J, Tomczak, C, Torelino, K, Touam-Ext, F, Toumi, L, Toury, G, Toy-Miou, M, Dinh Thanh Lien, O, Trandinh, A, Treluyer, J, Trinque, B, Truchot, J, Tubiana, S, Tunesi, S, Turpin, M, Turpin, A, Urbina, T, Narvaez, R, Uzunhan, Y, Vaittinadaayar, P, Valent, A, Valentian, M, Valin, N, Vallet, H, Vaz, M, Vazquezibarra, M, Vedie, B, Velly, L, Verstuyft, C, Viallette, C, Vicaut, E, Vignes, D, Vimpere, D, Virlouvet, M, Voiriot, G, Voisot, L, Weiss, E, Weiss, N, Winchenne, A, Yordanov, Y, Zafrani, L, Zaidan, M, Zaidi, W, Zak, C, Zarhrate-Ghoul, A, Zatout, O, Zeino, S, Zeitouni, M, Zemirli, N, Zerah, L, Zia, O, Ziol, M, Zolario, O, Zuber, J, Andrejak, C, Angoulvant, F, Bachelet, D, Bartoli, M, Basmaci, R, Behillil, S, Beluze, M, Benkerrou, D, Bhavsar, K, Bouadma, L, Bouchez, S, Bouscambert, M, Cervantes-Gonzalez, M, Chair, A, Chirouze, C, Coelho, A, Couffin-Cadiergues, S, D'Ortenzio, E, Debray, M, Deconinck, L, Deplanque, D, Descamps, D, Desvallee, M, Diallo, A, Diouf, A, Dorival, C, Dubos, F, Elharrar, B, Enouf, V, Esperou, H, Esposito-Farese, M, Devouge, E, Gault, N, Gaymard, A, Gigante, T, Gilg, M, Guedj, J, Hoctin, A, Hoffmann, I, Houas, I, Hulot, J, Jaafoura, S, Kaguelidou, F, Kali, S, Khalil, A, Khan, C, Laouenan, C, Laribi, S, Le, M, Le Hingrat, Q, Le Mestre, S, Le Nagard, H, Lescure, F, Letrou, S, Levy, Y, Lina, B, Lingas, G, Lucet, J, Malvy, D, Mambert, M, Meziane, A, Mouquet, 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U., Uzunhan Y., Vaittinadaayar P., Valent A., Valentian M., Valin N., Vallet H., Vaz M., Vazquezibarra M. -A., Vedie B., Velly L., Verstuyft C., Viallette C., Vicaut E., Vignes D., Vimpere D., Virlouvet M., Voiriot G., Voisot L., Weiss E., Weiss N., Winchenne A., Yordanov Y., Zafrani L., Zaidan M., Zaidi W., Zak C., Zarhrate-Ghoul A., Zatout O., Zeino S., Zeitouni M., Zemirli N., Zerah L., Zia O., Ziol M., Zolario O., Zuber J., Andrejak C., Angoulvant F., Bachelet D., Bartoli M., Basmaci R., Behillil S., Beluze M., Benkerrou D., Bhavsar K., Bouadma L., Bouchez S., Bouscambert M., Cervantes-Gonzalez M., Chair A., Chirouze C., Coelho A., Couffin-Cadiergues S., d'Ortenzio E., Debray M. -P., Deconinck L., Deplanque D., Descamps D., Desvallee M., Diallo A., Diouf A., Dorival C., Dubos F., Elharrar B., Enouf V., Esperou H., Esposito-Farese M., Devouge E. 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P., Euvrard R., Fabio G., Faivre L., Falck A., Fartoukh M., Faure M., Arquero M. F., Ferrer R., Ferreres J., Francois B., Fumado V., Fung K. S. C., Fusco F., Gagro A., Solis B. G., Garcon P., Gaussem P., Gayretli Z., Gil-Herrera J., Gilardin L., Gatineau A. G., Girona-Alarcon M., Cifuentes Godinez K. A., Goffard J. -C., Gonzales N., Gonzalez-Granado L. I., Gonzalez-Montelongo R., Guerder A., Gulhan B., Gumucio V. D., Hanitsch L. G., Gunst J., Gut M., Hadjadj J., Hancerli S., Hariyan T., Hatipoglu N., Heppekcan D., Hernandez-Brito E., Ho P. -K., Holanda-Pena M. S., Horcajada J. P., Hraiech S., Humbert L., Hung I. F. N., Iglesias A. D., Inigo-Campos A., Jamme M., Arranz M. J., Jimeno M. -T., Jordan I., Kanik-Yuksek S., Kara Y., Karahan A., Karbuz A., Yasar K. K., Kasapcopur O., Kashimada K., Keles S., Demirkol Y. K., Kido Y., Kizil C., Kilic A. O., Klocperk A., Koutsoukou A., Krol Z. J., Ksouri H., Kuentz P., Kwan A. M. C., Kwan Y. W. M., Kwok J. S. Y., Lagier J. -C., Lam D. S. Y., Lampropoulou V., Le Bourgeois F., Leo Y. -S., Lopez R. L., Leung D., Levin M., Levy M., Levy R., Li Z., Lilleri D., Adrian Bolanos Lima E. J., Linglart A., Lopez-Collazo E., Lorenzo-Salazar J. M., Louapre C., Lubetzki C., Lung K. -C., Luyt C. -E., Lye D. C., Magnone C., Marchioni E., Marioli C., Marjani M., Marques L., Pereira J. M., Martin-Nalda A., Pueyo D. M., Martinez-Picado J., Marzana I., Mata-Martinez C., Mathian A., Matos L. R. B., Matthews G. V., Mayaux J., McLaughlin-Garcia R., Meersseman P., Mege J. -L., Mekontso-Dessap A., Melki I., Meloni F., Meritet J. -F., Merlani P., Akcan O. M., Mezidi M., Migeotte I., Millereux M., Million M., Mirault T., Mircher C., Mirsaeidi M., Mizoguchi Y., Modi B. P., Mojoli F., Moncomble E., Melian A. M., Martinez A. M., Morandeira F., Morange P. -E., Mordacq C., Morelle G., Mouly S. J., Munoz-Barrera A., Nafati C., Nagashima S., Nakagama Y., Neven B., Neves J. F., Ng Y. -Y., Hubert Nielly, Medina Y. N., Cuadros E. N., Karabela S. N., Ocejo-Vinyals J. G., Oualha M., Ouedrani A., Ozkaya-Parlakay A., Pagani M., Papadaki M., Parola P., Pascreau T., Paul S., Paz-Artal E., Pedraza S., Gonzalez Pellecer N. C., Pellegrini S., Perez-Fernandez X. L., Philippe A., Philippot Q., Picod A., Pineton de Chambrun M., Piralla A., Planas-Serra L., Ploin D., Poissy J., Poncelet G., Poulakou G., Pouletty M. S., Pourshahnazari P., Qiu-Chen J. L., Quentric P., Rambaud T., Raoult D., Raoult V., Rebillat A. -S., Redin C., Resmini L., Ricart P., Richard J. -C., Rigo-Bonnin R., Rivet N., Riviere J. G., Rocamora-Blanch G., Rodero M. P., Rodrigo C., Rodriguez L. A., Rodriguez-Palmero A., Romero C. S., Rothenbuhler A., Roux D., Rovina N., Rozenberg F., Ruch Y., Ruiz M., Ruiz del Prado M. Y., Ruiz-Rodriguez J. C., Sabater-Riera J., Saks K., Salagianni M., Sanchez O., Sanchez-Montalva A., Sanchez-Ramon S., Schidlowski L., Schluter A., Schmidt J., Schmidt M., Schuetz C., Schweitzer C. E., Scolari F., Seijo L., Seminario A. G., Seng P., Senoglu S., Seppanen M., Llovich A. S., Siguret V., Siouti E., Smadja D. M., Smith N., Sobh A., Solanich X., Sole-Violan J., Soler C., Sozeri B., Stella G. M., Stepanovskiy Y., Stoclin A., Taccone F., Taupin J. -L., Tavernier S. J., Tello L. V., Terrier B., Thiery G., Thorn K., Thumerelle C., Tipu I., Tolstrup M., Tomasoni G., Toubiana J., Alvarez J. T., Triantafyllia V., Troya J., Tsang O. T. Y., Tserel L., Tso E. Y. K., Tucci A., Tuter Oz S. K., Ursini M. V., Utsumi T., Vabres P., Valencia-Ramos J., Van Den Rym A. M., Vandernoot I., Velez-Santamaria V., Zuniga Veliz S. P., Vidigal M. C., Viel S., Villain C., Vilaire-Meunier M. E., Villar-Garcia J., Vincent A., Van der Linden D., Volokha A., Vuotto F., Wauters E., Wu A. K. L., Wu T. -C., Yahsi A., Yesilbas O., Yildiz M., Young B. E., Yukselmis U., Zecca M., Zuccaro V., Van Praet J., Lambrecht B. 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- Abstract
Human genetic studies of critical COVID-19 pneumonia have revealed the essential role of type I interferon-dependent innate immunity to SARS-CoV-2 infection. Conversely, an association between the HLA-B∗15:01 allele and asymptomatic SARS-CoV-2 infection in unvaccinated individuals was recently reported, suggesting a contribution of pre-existing T cell-dependent adaptive immunity. We report a lack of association of classical HLA alleles, including HLA-B∗15:01, with pre-omicron asymptomatic SARS-CoV-2 infection in unvaccinated participants in a prospective population-based study in the United States (191 asymptomatic vs. 945 symptomatic COVID-19 cases). Moreover, we found no such association in the international COVID Human Genetic Effort cohort (206 asymptomatic vs. 574 mild or moderate COVID-19 cases and 1,625 severe or critical COVID-19 cases). Finally, in the Human Challenge Characterisation study, the three HLA-B∗15:01 individuals infected with SARS-CoV-2 developed symptoms. As with other acute primary infections studied, no classical HLA alleles favoring an asymptomatic course of SARS-CoV-2 infection were identified.
- Published
- 2024
7. Herpes simplex virus-2 meningo-encephalitis hiding a criminal case of fatal methylmercury poisoning
- Author
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Marois, C., primary, Lambrecq, V., additional, Leclercq, D., additional, Dufayet, L., additional, Plu, I., additional, and Langrand, J., additional
- Published
- 2024
- Full Text
- View/download PDF
8. The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics from 10 to 100 au
- Author
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Nielsen, EL, De Rosa, RJ, Macintosh, B, Wang, JJ, Ruffio, JB, Chiang, E, Marley, MS, Saumon, D, Savransky, D, Mark Ammons, S, Bailey, VP, Barman, T, Blain, C, Bulger, J, Burrows, A, Chilcote, J, Cotten, T, Czekala, I, Doyon, R, Duchene, G, Esposito, TM, Fabrycky, D, Fitzgerald, MP, Follette, KB, Fortney, JJ, Gerard, BL, Goodsell, SJ, Graham, JR, Greenbaum, AZ, Hibon, P, Hinkley, S, Hirsch, LA, Hom, J, Hung, LW, Ilene Dawson, R, Ingraham, P, Kalas, P, Konopacky, Q, Larkin, JE, Lee, EJ, Lin, JW, Maire, J, Marchis, F, Marois, C, Metchev, S, Millar-Blanchaer, MA, Morzinski, KM, Oppenheimer, R, Palmer, D, Patience, J, Perrin, M, Poyneer, L, Pueyo, L, Rafikov, RR, Rajan, A, Rameau, J, Rantakyrö, FT, Ren, B, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Tallis, M, Thomas, S, Ward-Duong, K, and Wolff, S
- Subjects
instrumentation: adaptive optics ,planetary systems ,planets and satellites: detection ,astro-ph.EP ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
We present a statistical analysis of the first 300 stars observed by the Gemini Planet Imager Exoplanet Survey. This subsample includes six detected planets and three brown dwarfs; from these detections and our contrast curves we infer the underlying distributions of substellar companions with respect to their mass, semimajor axis, and host stellar mass. We uncover a strong correlation between planet occurrence rate and host star mass, with stars M ∗ >1.5 M o more likely to host planets with masses between 2 and 13M Jup and semimajor axes of 3-100 au at 99.92% confidence. We fit a double power-law model in planet mass (m) and semimajor axis (a) for planet populations around high-mass stars (M ∗ >1.5 M o) of the form , finding α = -2.4 +0.8 and β = -2.0 +0.5, and an integrated occurrence rate of % between 5-13M Jup and 10-100 au. A significantly lower occurrence rate is obtained for brown dwarfs around all stars, with % of stars hosting a brown dwarf companion between 13-80M Jup and 10-100 au. Brown dwarfs also appear to be distributed differently in mass and semimajor axis compared to giant planets; whereas giant planets follow a bottom-heavy mass distribution and favor smaller semimajor axes, brown dwarfs exhibit just the opposite behaviors. Comparing to studies of short-period giant planets from the radial velocity method, our results are consistent with a peak in occurrence of giant planets between ∼1 and 10 au. We discuss how these trends, including the preference of giant planets for high-mass host stars, point to formation of giant planets by core/pebble accretion, and formation of brown dwarfs by gravitational instability.
- Published
- 2019
9. Direct Imaging of the HD 35841 Debris Disk: A Polarized Dust Ring from Gemini Planet Imager and an Outer Halo from HST/STIS
- Author
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Esposito, TM, Duchne, G, Kalas, P, Rice, M, Choquet, I, Ren, B, Perrin, MD, Chen, CH, Arriaga, P, Chiang, E, Nielsen, EL, Graham, JR, Wang, JJ, Rosa, RJD, Follette, KB, Ammons, SM, Ansdell, M, Bailey, VP, Barman, T, Bruzzone, JS, Bulger, J, Chilcote, J, Cotten, T, Doyon, R, Fitzgerald, MP, Goodsell, SJ, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Konopacky, Q, Larkin, JE, Macintosh, B, Maire, J, Marchis, F, Marois, C, Mazoyer, J, Metchev, S, Millar-Blanchaer, MA, Oppenheimer, R, Palmer, D, Patience, J, Poyneer, L, Pueyo, L, Rajan, A, Rameau, J, Rantakyrö, FT, Ryan, D, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, Wiktorowicz, S, and Wolff, S
- Subjects
circumstellar matter ,infrared: planetary systems ,stars: individual ,techniques: high angular resolution ,astro-ph.EP ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
We present new high resolution imaging of a light-scattering dust ring and halo around the young star HD 35841. Using spectroscopic and polarimetric data from the Gemini Planet Imager in H-band (1.6 μm), we detect the highly inclined (i = 85°) ring of debris down to a projected separation of ∼12 au (∼0.″12) for the first time. Optical imaging from HST/STIS shows a smooth dust halo extending outward from the ring to >140 au (>1.″4). We measure the ring's scattering phase function and polarization fraction over scattering angles of 22°-125°, showing a preference for forward scattering and a polarization fraction that peaks at ∼30% near the ansae. Modeling of the scattered-light disk indicates that the ring spans radii of ∼60-220 au, has a vertical thickness similar to that of other resolved dust rings, and contains grains as small as 1.5 μm in diameter. These models also suggest the grains have a low porosity, are more likely to consist of carbon than astrosilicates, and contain significant water ice. The halo has a surface brightness profile consistent with that expected from grains pushed by radiation pressure from the main ring onto highly eccentric but still bound orbits. We also briefly investigate arrangements of a possible inner disk component implied by our spectral energy distribution models, and speculate about the limitations of Mie theory for doing detailed analyses of debris disk dust populations.
- Published
- 2018
10. GPI Spectra of HR 8799 c, d, and e from 1.5 to 2.4 μm with KLIP Forward Modeling
- Author
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Greenbaum, AZ, Pueyo, L, Ruffio, JB, Wang, JJ, Rosa, RJD, Aguilar, J, Rameau, J, Barman, T, Marois, C, Marley, MS, Konopacky, Q, Rajan, A, Macintosh, B, Ansdell, M, Arriaga, P, Bailey, VP, Bulger, J, Burrows, AS, Chilcote, J, Cotten, T, Doyon, R, Duchêne, G, Fitzgerald, MP, Follette, KB, Gerard, B, Goodsell, SJ, Graham, JR, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Larkin, JE, Maire, J, Marchis, F, Metchev, S, Millar-Blanchaer, MA, Nielsen, EL, Norton, A, Oppenheimer, R, Palmer, D, Patience, J, Perrin, MD, Poyneer, L, Rantakyrö, FT, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, Wiktorowicz, S, and Wolff, S
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planets and satellites: gaseous planets ,stars: individual ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
We explore KLIP forward modeling spectral extraction on Gemini Planet Imager coronagraphic data of HR 8799, using PyKLIP, and show algorithm stability with varying KLIP parameters. We report new and re-reduced spectrophotometry of HR 8799 c, d, and e in the H and K bands. We discuss a strategy for choosing optimal KLIP PSF subtraction parameters by injecting simulated sources and recovering them over a range of parameters. The K1/K2 spectra for HR 8799 c and d are similar to previously published results from the same data set. We also present a K-band spectrum of HR 8799 e for the first time and show that our H-band spectra agree well with previously published spectra from the VLT/SPHERE instrument. We show that HR 8799 c and d show significant differences in their H and K spectra, but do not find any conclusive differences between d and e, nor between c and e, likely due to large error bars in the recovered spectrum of e. Compared to M-, L-, and T-type field brown dwarfs, all three planets are most consistent with mid- and late-L spectral types. All objects are consistent with low gravity, but a lack of standard spectra for low gravity limit the ability to fit the best spectral type. We discuss how dedicated modeling efforts can better fit HR 8799 planets' near-IR flux, as well as how differences between the properties of these planets can be further explored.
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- 2018
11. Automated data processing architecture for the gemini planet imager exoplanet survey
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Wang, JJ, Perrin, MD, Savransky, D, Arriaga, P, Chilcote, JK, De Rosa, RJ, Millar-Blanchaer, MA, Marois, C, Rameau, J, Wolff, SG, Shapiro, J, Ruffio, JB, Maire, J, Marchis, F, Graham, JR, Macintosh, B, Mark Ammons, S, Bailey, VP, Barman, TS, Bruzzone, S, Bulger, J, Cotton, T, Doyon, R, Duchêne, G, Fitzgerald, MP, Follette, KB, Goodsell, S, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Konopacky, QM, Larkin, JE, Marley, MS, Metchev, S, Nielsen, EL, Oppenheimer, R, Palmer, DW, Patience, J, Poyneer, LA, Pueyo, L, Rajan, A, Rantakyrö, FT, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Kent Wallace, J, Ward-Duong, K, and Wiktorowicz, SJ
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high contrast imaging ,exoplanets ,circumstellar disks ,data processing ,Gemini planet imager ,Data Cruncher ,astro-ph.IM ,astro-ph.EP ,Mathematical Sciences ,Physical Sciences - Abstract
The Gemini Planet Imager Exoplanet Survey (GPIES) is a multiyear direct imaging survey of 600 stars to discover and characterize young Jovian exoplanets and their environments. We have developed an automated data architecture to process and index all data related to the survey uniformly. An automated and flexible data processing framework, which we term the Data Cruncher, combines multiple data reduction pipelines (DRPs) together to process all spectroscopic, polarimetric, and calibration data taken with GPIES. With no human intervention, fully reduced and calibrated data products are available less than an hour after the data are taken to expedite follow up on potential objects of interest. The Data Cruncher can run on a supercomputer to reprocess all GPIES data in a single day as improvements are made to our DRPs. A backend MySQL database indexes all files, which are synced to the cloud, and a front-end web server allows for easy browsing of all files associated with GPIES. To help observers, quicklook displays show reduced data as they are processed in real time, and chatbots on Slack post observing information as well as reduced data products. Together, the GPIES automated data processing architecture reduces our workload, provides real-Time data reduction, optimizes our observing strategy, and maintains a homogeneously reduced dataset to study planet occurrence and instrument performance.
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- 2018
12. Evidence that the directly imaged planet HD 131399 Ab Is a Background Star
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Nielsen, EL, Rosa, RJD, Rameau, J, Wang, JJ, Esposito, TM, Millar-Blanchaer, MA, Marois, C, Vigan, A, Ammons, SM, Artigau, E, Bailey, VP, Blunt, S, Bulger, J, Chilcote, J, Cotten, T, Doyon, R, Duchêne, G, Fabrycky, D, Fitzgerald, MP, Follette, KB, Gerard, BL, Goodsell, SJ, Graham, JR, Greenbaum, AZ, Hibon, P, Hinkley, S, Hung, LW, Ingraham, P, Jensen-Clem, R, Kalas, P, Konopacky, Q, Larkin, JE, MacIntosh, B, Maire, J, Marchis, F, Metchev, S, Morzinski, KM, Murray-Clay, RA, Oppenheimer, R, Palmer, D, Patience, J, Perrin, M, Poyneer, L, Pueyo, L, Rafikov, RR, Rajan, A, Rantakyrö, FT, Ruffio, JB, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, Wiktorowicz, S, and Wolff, S
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astrometry ,instrumentation: adaptive optics ,planets and satellites: detection ,stars: individual ,techniques: image processing ,techniques: spectroscopic ,astro-ph.EP ,astro-ph.SR ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
We present evidence that the recently discovered, directly imaged planet HD 131399 Ab is a background star with nonzero proper motion. From new JHK1L′ photometry and spectroscopy obtained with the Gemini Planet Imager, VLT/SPHERE, and Keck/NIRC2, and a reanalysis of the discovery data obtained with VLT/SPHERE, we derive colors, spectra, and astrometry for HD 131399 Ab. The broader wavelength coverage and higher data quality allow us to reinvestigate its status. Its near-infrared spectral energy distribution excludes spectral types later than L0 and is consistent with a K or M dwarf, which are the most likely candidates for a background object in this direction at the apparent magnitude observed. If it were a physically associated object, the projected velocity of HD 131399 Ab would exceed escape velocity given the mass and distance to HD 131399 A. We show that HD 131399 Ab is also not following the expected track for a stationary background star at infinite distance. Solving for the proper motion and parallax required to explain the relative motion of HD 131399 Ab, we find a proper motion of 12.3 mas yr-1. When compared to predicted background objects drawn from a galactic model, we find this proper motion to be high but consistent with the top 4% fastest-moving background stars. From our analysis, we conclude that HD 131399 Ab is a background K or M dwarf.
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- 2017
13. Astrometric Monitoring of the HR 8799 Planets: Orbit Constraints from Self-Consistent Measurements
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Konopacky, Q. M., Marois, C., Macintosh, B. A., Galicher, R., Barman, T. S., Metchev, S. A., and Zuckerman, B.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
We present new astrometric measurements from our ongoing monitoring campaign of the HR 8799 directly imaged planetary system. These new data points were obtained with NIRC2 on the W.M. Keck II 10 meter telescope between 2009 and 2014. In addition, we present updated astrometry from previously published observations in 2007 and 2008. All data were reduced using the SOSIE algorithm, which accounts for systematic biases present in previously published observations. This allows us to construct a self-consistent data set derived entirely from NIRC2 data alone. From this dataset, we detect acceleration for two of the planets (HR 8799b and e) at $>$3$\sigma$. We also assess possible orbital parameters for each of the four planets independently. We find no statistically significant difference in the allowed inclinations of the planets. Fitting the astrometry while forcing coplanarity also returns $\chi^2$ consistent to within 1$\sigma$ of the best fit values, suggesting that if inclination offsets of $\lesssim$20$^{o}$ are present, they are not detectable with current data. Our orbital fits also favor low eccentricities, consistent with predictions from dynamical modeling. We also find period distributions consistent to within 1$\sigma$ with a 1:2:4:8 resonance between all planets. This analysis demonstrates the importance of minimizing astrometric systematics when fitting for solutions to highly undersampled orbits., Comment: 18 pages, 11 figures. Accepted for publication in AJ
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- 2016
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14. Characterizing 51 Eri b from 1 to 5 μm: A Partly Cloudy Exoplanet
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Rajan, A, Rameau, J, Rosa, RJD, Marley, MS, Graham, JR, Macintosh, B, Marois, C, Morley, C, Patience, J, Pueyo, L, Saumon, D, Ward-Duong, K, Ammons, SM, Arriaga, P, Bailey, VP, Barman, T, Bulger, J, Burrows, AS, Chilcote, J, Cotten, T, Czekala, I, Doyon, R, Duchêne, G, Esposito, TM, Fitzgerald, MP, Follette, KB, Fortney, JJ, Goodsell, SJ, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Johnson-Groh, M, Kalas, P, Konopacky, Q, Lafrenière, D, Larkin, JE, Maire, J, Marchis, F, Metchev, S, Millar-Blanchaer, MA, Morzinski, KM, Nielsen, EL, Oppenheimer, R, Palmer, D, Patel, RI, Perrin, M, Poyneer, L, Rantakyrö, FT, Ruffio, JB, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Vasisht, G, Wallace, JK, Wang, JJ, Wiktorowicz, S, and Wolff, S
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instrumentation: adaptive optics ,planets and satellites: atmospheres ,planets and satellites: composition ,planets and satellites: gaseous planets ,stars: individual ,astro-ph.EP ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
We present spectrophotometry spanning 1-5 μm of 51 Eridani b, a 2-10 planet discovered by the Gemini Planet Imager Exoplanet Survey. In this study, we present new K1 (1.90-2.19 μm) and K2 (2.10-2.40 μm) spectra taken with the Gemini Planet Imager as well as an updated L P (3.76 μm) and new M S (4.67 μm) photometry from the NIRC2 Narrow camera. The new data were combined with J (1.13-1.35 μm) and H (1.50-1.80 μm) spectra from the discovery epoch with the goal of better characterizing the planet properties. The 51 Eri b photometry is redder than field brown dwarfs as well as known young T-dwarfs with similar spectral type (between T4 and T8), and we propose that 51 Eri b might be in the process of undergoing the transition from L-type to T-type. We used two complementary atmosphere model grids including either deep iron/silicate clouds or sulfide/salt clouds in the photosphere, spanning a range of cloud properties, including fully cloudy, cloud-free, and patchy/intermediate-opacity clouds. The model fits suggest that 51 Eri b has an effective temperature ranging between 605 and 737 K, a solar metallicity, and a surface gravity of log(g) = 3.5-4.0 dex, and the atmosphere requires a patchy cloud atmosphere to model the spectral energy distribution (SED). From the model atmospheres, we infer a luminosity for the planet of -5.83 to -5.93 (logL/L⊙), leaving 51 Eri b in the unique position of being one of the only directly imaged planets consistent with having formed via a cold-start scenario. Comparisons of the planet SED against warm-start models indicate that the planet luminosity is best reproduced by a planet formed via core accretion with a core mass between 15 and 127 M⊕.
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- 2017
15. Improving and Assessing Planet Sensitivity of the GPI Exoplanet Survey with a Forward Model Matched Filter
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Ruffio, JB, Macintosh, B, Wang, JJ, Pueyo, L, Nielsen, EL, Rosa, RJD, Czekala, I, Marley, MS, Arriaga, P, Bailey, VP, Barman, T, Bulger, J, Chilcote, J, Cotten, T, Doyon, R, Duchene, G, Fitzgerald, MP, Follette, KB, Gerard, BL, Goodsell, SJ, Graham, JR, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Konopacky, Q, Larkin, JE, Maire, J, Marchis, F, Marois, C, Metchev, S, Millar-Blanchaer, MA, Morzinski, KM, Oppenheimer, R, Palmer, D, Patience, J, Perrin, M, Poyneer, L, Rajan, A, Rameau, J, Rantakyrö, FT, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, Wiktorowicz, S, and Wolff, S
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instrumentation: adaptive optics ,methods: statistical ,planetary systems ,surveys ,techniques: high angular resolution ,techniques: image processing ,Astronomy & Astrophysics ,Astronomical and Space Sciences ,Atomic ,Molecular ,Nuclear ,Particle and Plasma Physics ,Physical Chemistry ,Atomic ,Molecular ,Nuclear ,Particle and Plasma Physics ,Physical Chemistry (incl. Structural) - Abstract
We present a new matched-filter algorithm for direct detection of point sources in the immediate vicinity of bright stars. The stellar point-spread function (PSF) is first subtracted using a Karhunen-Loéve image processing (KLIP) algorithm with angular and spectral differential imaging (ADI and SDI). The KLIP-induced distortion of the astrophysical signal is included in the matched-filter template by computing a forward model of the PSF at every position in the image. To optimize the performance of the algorithm, we conduct extensive planet injection and recovery tests and tune the exoplanet spectra template and KLIP reduction aggressiveness to maximize the signal-to-noise ratio (S/N) of the recovered planets. We show that only two spectral templates are necessary to recover any young Jovian exoplanets with minimal S/N loss. We also developed a complete pipeline for the automated detection of point-source candidates, the calculation of receiver operating characteristics (ROC), contrast curves based on false positives, and completeness contours. We process in a uniform manner more than 330 data sets from the Gemini Planet Imager Exoplanet Survey and assess GPI typical sensitivity as a function of the star and the hypothetical companion spectral type. This work allows for the first time a comparison of different detection algorithms at a survey scale accounting for both planet completeness and false-positive rate. We show that the new forward model matched filter allows the detection of 50% fainter objects than a conventional cross-correlation technique with a Gaussian PSF template for the same false-positive rate.
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- 2017
16. An Optical/Near-infrared Investigation of HD 100546 b with the Gemini Planet Imager and MagAO
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Rameau, J, Follette, KB, Pueyo, L, Marois, C, MacIntosh, B, Millar-Blanchaer, M, Wang, JJ, Vega, D, Doyon, R, Lafrenire, D, Nielsen, EL, Bailey, V, Chilcote, JK, Close, LM, Esposito, TM, Males, JR, Metchev, S, Morzinski, KM, Ruffio, JB, Wolff, SG, Ammons, SM, Barman, TS, Bulger, J, Cotten, T, Rosa, RJD, Duchene, G, Fitzgerald, MP, Goodsell, S, Graham, JR, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Konopacky, Q, Larkin, JE, Maire, J, Marchis, F, Oppenheimer, R, Palmer, D, Patience, J, Perrin, MD, Poyneer, L, Rajan, A, Rantakyrö, FT, Marley, MS, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, and Wiktorowicz, S
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instrumentation: adaptive optics ,planet-disk interactions ,planetary systems ,stars: individual ,astro-ph.EP ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
We present H band spectroscopic and Hμ photometric observations of HD 100546 obtained with the Gemini Planet Imager and the Magellan Visible AO camera. We detect H band emission at the location of the protoplanet HD 100546 b, but show that the choice of data processing parameters strongly affects the morphology of this source. It appears point-like in some aggressive reductions, but rejoins an extended disk structure in the majority of the others. Furthermore, we demonstrate that this emission appears stationary on a timescale of 4.6 years, inconsistent at the 2σ level with a Keplerian clockwise orbit at 59 au in the disk plane. The H band spectrum of the emission is inconsistent with any type of low effective temperature object or accreting protoplanetary disk. It strongly suggests a scattered-light origin, as this is consistent with the spectrum of the star and the spectra extracted at other locations in the disk. A non-detection at the 5σ level of HD 100546 b in differential Hμ imaging places an upper limit, assuming the protoplanet lies in a gap free of extinction, on the accretion luminosity of 1.7 ? 10-4 L o and for 1 R Jup. These limits are comparable to the accretion luminosity and accretion rate of T-Tauri stars or LkCa 15 b. Taken together, these lines of evidence suggest that the H band source at the location of HD 100546 b is not emitted by a planetary photosphere or an accreting circumplanetary disk but is a disk feature enhanced by the point-spread function subtraction process. This non-detection is consistent with the non-detection in the K band reported in an earlier study but does not exclude the possibility that HD 100546 b is deeply embedded.
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- 2017
17. Complex Spiral Structure in the HD 100546 Transitional Disk as Revealed by GPI and MagAO
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Follette, KB, Rameau, J, Dong, R, Pueyo, L, Close, LM, Duchêne, G, Fung, J, Leonard, C, MacIntosh, B, Males, JR, Marois, C, Millar-Blanchaer, MA, Morzinski, KM, Mullen, W, Perrin, M, Spiro, E, Wang, J, Ammons, SM, Bailey, VP, Barman, T, Bulger, J, Chilcote, J, Cotten, T, De Rosa, RJ, Doyon, R, Fitzgerald, MP, Goodsell, SJ, Graham, JR, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Konopacky, Q, Larkin, JE, Maire, J, Marchis, F, Metchev, S, Nielsen, EL, Oppenheimer, R, Palmer, D, Patience, J, Poyneer, L, Rajan, A, Rantakyrö, FT, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Vega, D, Wallace, JK, Ward-Duong, K, Wiktorowicz, S, and Wolff, S
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instrumentation: adaptive optics ,planet-disk interaction ,protoplanetary disk ,stars: individual ,astro-ph.EP ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
We present optical and near-infrared high-contrast images of the transitional disk HD 100546 taken with the Magellan Adaptive Optics system (MagAO) and the Gemini Planet Imager (GPI). GPI data include both polarized intensity and total intensity imagery, and MagAO data are taken in Simultaneous Differential Imaging mode at Hα. The new GPI H-band total intensity data represent a significant enhancement in sensitivity and field rotation compared to previous data sets and enable a detailed exploration of substructure in the disk. The data are processed with a variety of differential imaging techniques (polarized, angular, reference, and simultaneous differential imaging) in an attempt to identify the disk structures that are most consistent across wavelengths, processing techniques, and algorithmic parameters. The inner disk cavity at 15 au is clearly resolved in multiple data sets, as are a variety of spiral features. While the cavity and spiral structures are identified at levels significantly distinct from the neighboring regions of the disk under several algorithms and with a range of algorithmic parameters, emission at the location of HD 100546 "c" varies from point-like under aggressive algorithmic parameters to a smooth continuous structure with conservative parameters, and is consistent with disk emission. Features identified in the HD 100546 disk bear qualitative similarity to computational models of a moderately inclined two-armed spiral disk, where projection effects and wrapping of the spiral arms around the star result in a number of truncated spiral features in forward-modeled images.
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- 2017
18. Integral Field Spectroscopy of the Low-mass Companion HD 984 B with the Gemini Planet Imager
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Johnson-Groh, M, Marois, C, De Rosa, RJ, Nielsen, EL, Rameau, J, Blunt, S, Vargas, J, Ammons, SM, Bailey, VP, Barman, TS, Bulger, J, Chilcote, JK, Cotten, T, Doyon, R, Duchêne, G, Fitzgerald, MP, Follette, KB, Goodsell, S, Graham, JR, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Konopacky, QM, Larkin, JE, Macintosh, B, Maire, J, Marchis, F, Marley, MS, Metchev, S, Millar-Blanchaer, MA, Oppenheimer, R, Palmer, DW, Patience, J, Perrin, M, Poyneer, LA, Pueyo, L, Rajan, A, Rantakyrö, FT, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Vega, D, Wallace, JK, Wang, JJ, Ward-Duong, K, Wiktorowicz, SJ, and Wolff, SG
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astro-ph.EP ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
We present new observations of the low-mass companion to HD 984 taken with the Gemini Planet Imager (GPI) as a part of the GPI Exoplanet Survey campaign. Images of HD 984 B were obtained in the J (1.12-1.3 μm) and H (1.50-1.80 μm) bands. Combined with archival epochs from 2012 and 2014, we fit the first orbit to the companion to find an 18 au (70-year) orbit with a 68% confidence interval between 14 and 28 au, an eccentricity of 0.18 with a 68% confidence interval between 0.05 and 0.47, and an inclination of 119°with a 68% confidence interval between 114°and 125°. To address the considerable spectral covariance in both spectra, we present a method of splitting the spectra into low and high frequencies to analyze the spectral structure at different spatial frequencies with the proper spectral noise correlation. Using the split spectra, we compare them to known spectral types using field brown dwarf and low-mass star spectra and find a best-fit match of a field gravity M6.5 ±1.5 spectral type with a corresponding temperature of K. Photometry of the companion yields a luminosity of log(Lbol/L⊙)=2.88 ± 0.07 dex with DUSTY models. Mass estimates, again from DUSTY models, find an age-dependent mass of 34 ±1 to 95 ±4 M Jup. These results are consistent with previous measurements of the object.
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- 2017
19. 1-2.4 μm Near-IR Spectrum of the Giant Planet β Pictoris b Obtained with the Gemini Planet Imager
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Chilcote, J, Pueyo, L, Rosa, RJD, Vargas, J, Macintosh, B, Bailey, VP, Barman, T, Bauman, B, Bruzzone, S, Bulger, J, Burrows, AS, Cardwell, A, Chen, CH, Cotten, T, Dillon, D, Doyon, R, Draper, ZH, Duchêne, G, Dunn, J, Erikson, D, Fitzgerald, MP, Follette, KB, Gavel, D, Goodsell, SJ, Graham, JR, Greenbaum, AZ, Hartung, M, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Konopacky, Q, Larkin, JE, Maire, J, Marchis, F, Marley, MS, Marois, C, Metchev, S, Millar-Blanchaer, MA, Morzinski, KM, Nielsen, EL, Norton, A, Oppenheimer, R, Palmer, D, Patience, J, Perrin, M, Poyneer, L, Rajan, A, Rameau, J, Rantakyrö, FT, Sadakuni, N, Saddlemyer, L, Savransky, D, Schneider, AC, Serio, A, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Wang, JJ, Ward-Duong, K, Wiktorowicz, S, and Wolff, S
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instrumentation: adaptive optics ,planetary systems ,stars: individual ,techniques:spectroscopic ,astro-ph.EP ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
Using the Gemini Planet Imager located at Gemini South, we measured the near-infrared (1.0-2.4 μm) spectrum of the planetary companion to the nearby, young star β Pictoris. We compare the spectrum obtained with currently published model grids and with known substellar objects and present the best matching models as well as the best matching observed objects. Comparing the empirical measurement of the bolometric luminosity to evolutionary models, we find a mass of 12.9 ±0.2 , an effective temperature of 1724 ±15 K, a radius of 1.46 ±0.01 , and a surface gravity of [dex] (cgs). The stated uncertainties are statistical errors only, and do not incorporate any uncertainty on the evolutionary models. Using atmospheric models, we find an effective temperature of 1700-1800 K and a surface gravity of -4.0 [dex] depending upon the model. These values agree well with other publications and with "hot-start" predictions from planetary evolution models. Further, we find that the spectrum of β Pic b best matches a low surface gravity L2 ±1 brown dwarf. Finally, comparing the spectrum to field brown dwarfs, we find the the spectrum best matches 2MASS J04062677-381210 and 2MASS J03552337+1133437.
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- 2017
20. DYNAMICAL MASS MEASUREMENT of the YOUNG SPECTROSCOPIC BINARY V343 NORMAE AaAb RESOLVED with the GEMINI PLANET IMAGER
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Nielsen, EL, Rosa, RJD, Wang, J, Rameau, J, Song, I, Graham, JR, Macintosh, B, Ammons, M, Bailey, VP, Barman, TS, Bulger, J, Chilcote, JK, Cotten, T, Doyon, R, Duchene, G, Fitzgerald, MP, Follette, KB, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Konopacky, QM, Larkin, JE, Maire, J, Marchis, F, Marley, MS, Marois, C, Metchev, S, Millar-Blanchaer, MA, Oppenheimer, R, Palmer, DW, Patience, J, Perrin, MD, Poyneer, LA, Pueyo, L, Rajan, A, Rantakyrö, FT, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, Wiktorowicz, SJ, and Wolff, SG
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planets and satellites: detection ,stars: individual ,astro-ph.SR ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
We present new spatially resolved astrometry and photometry from the Gemini Planet Imager of the inner binary of the young multiple star system V343 Normae, which is a member of the β Pictoris (β Pic) moving group. V343 Normae comprises a K0 and mid-M star in a ∼4.5 year orbit (AaAb) and a wide 10″ M5 companion (B). By combining these data with archival astrometry and radial velocities we fit the orbit and measure individual masses for both components of MAa = 1.10 ± 0.10 M⊙ and MAb = 0.290 ± 0.018 M⊙. Comparing to theoretical isochrones, we find good agreement for the measured masses and JHK band magnitudes of the two components consistent with the age of the β Pic moving group. We derive a model-dependent age for the β Pic moving group of 26 ±3 Myr by combining our results for V343 Normae with literature measurements for GJ 3305, which is another group member with resolved binary components and dynamical masses.
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- 2016
21. Discovery and spectroscopy of the young Jovian planet 51 Eri b with the Gemini Planet Imager
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Macintosh, B., Graham, J. R., Barman, T., De Rosa, R. J., Konopacky, Q., Marley, M. S., Marois, C., Nielsen, E. L., Pueyo, L., Rajan, A., Rameau, J., Saumon, D., Wang, J. J., Patience, J., Ammons, M., Arriaga, P., Artigau, E., Beckwith, S., Brewster, J., Bruzzone, S., Bulger, J., Burningham, B., Burrows, A. S., Chen, C., Chiang, E., Chilcote, J. K., Dawson, R. I., Dong, R., Doyon, R., Draper, Z. H., Duchêne, G., Esposito, T. M., Fabrycky, D., Fitzgerald, M. P., Follette, K. B., Fortney, J. J., Gerard, B., Goodsell, S., Greenbaum, A. Z., Hibon, P., Hinkley, S., Cotten, T. H., Hung, L. -W., Ingraham, P., Johnson-Groh, M., Kalas, P., Lafreniere, D., Larkin, J. E., Lee, J., Line, M., Long, D., Maire, J., Marchis, F., Matthews, B. C., Max, C. E., Metchev, S., Millar-Blanchaer, M. A., Mittal, T., Morley, C. V., Morzinski, K. M., Murray-Clay, R., Oppenheimer, R., Palmer, D. W., Patel, R., Perrin, M. D., Poyneer, L. A., Rafikov, R. R., Rantakyrö, F. T., Rice, E. L., Rojo, P., Rudy, A. R., Ruffio, J. -B., Ruiz, M. T., Sadakuni, N., Saddlemyer, L., Salama, M., Savransky, D., Schneider, A. C., Sivaramakrishnan, A., Song, I., Soummer, R., Thomas, S., Vasisht, G., Wallace, J. K., Ward-Duong, K., Wiktorowicz, S. J., Wolff, S. G., and Zuckerman, B.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
Directly detecting thermal emission from young extrasolar planets allows measurement of their atmospheric composition and luminosity, which is influenced by their formation mechanism. Using the Gemini Planet Imager, we discovered a planet orbiting the \$sim$20 Myr-old star 51 Eridani at a projected separation of 13 astronomical units. Near-infrared observations show a spectrum with strong methane and water vapor absorption. Modeling of the spectra and photometry yields a luminosity of L/LS=1.6-4.0 x 10-6 and an effective temperature of 600-750 K. For this age and luminosity, "hot-start" formation models indicate a mass twice that of Jupiter. This planet also has a sufficiently low luminosity to be consistent with the "cold- start" core accretion process that may have formed Jupiter., Comment: 29 pages, 3 figures, 2 tables, and Supplementary Materials. published in Science Express on Aug 13 2015. List of authors and the magnitudes of the star were correted
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- 2015
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22. Imaging an 80 au radius dust ring around the F5V star HD 157587
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Millar-Blanchaer, MA, Wang, JJ, Kalas, P, Graham, JR, Duchêne, G, Nielsen, EL, Perrin, M, Moon, DS, Padgett, D, Metchev, S, Ammons, SM, Bailey, VP, Barman, T, Bruzzone, S, Bulger, J, Chen, CH, Chilcote, J, Cotten, T, Rosa, RJD, Doyon, R, Draper, ZH, Esposito, TM, Fitzgerald, MP, Follette, KB, Gerard, BL, Greenbaum, AZ, Hibon, P, Hinkley, S, Hung, LW, Ingraham, P, Johnson-Groh, M, Konopacky, Q, Larkin, JE, MacIntosh, B, Maire, J, Marchis, F, Marley, MS, Marois, C, Matthews, BC, Oppenheimer, R, Palmer, D, Patience, J, Poyneer, L, Pueyo, L, Rajan, A, Rameau, J, Rantakyrö, FT, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Vega, D, Wallace, JK, Ward-Duong, K, Wiktorowicz, S, and Wolff, S
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planet-disk interactions ,stars: individual ,techniques: polarimetric ,astro-ph.EP ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
We present H-band near-infrared polarimetric imaging observations of the F5V star HD 157587 obtained with the Gemini Planet Imager (GPI) that reveal the debris disk as a bright ring structure at a separation of ∼80-100 au. The new GPI data complement recent Hubble Space Telescope/STIS observations that show the disk extending out to over 500 au. The GPI image displays a strong asymmetry along the projected minor axis as well as a fainter asymmetry along the projected major axis. We associate the minor and major axis asymmetries with polarized forward scattering and a possible stellocentric offset, respectively. To constrain the disk geometry, we fit two separate disk models to the polarized image, each using a different scattering phase function. Both models favor a disk inclination of ∼70° and a 1.5 ± 0.6 au stellar offset in the plane of the sky along the projected major axis of the disk. We find that the stellar offset in the disk plane, perpendicular to the projected major axis is degenerate with the form of the scattering phase function and remains poorly constrained. The disk is not recovered in total intensity due in part to strong adaptive optics residuals, but we recover three point sources. Considering the system's proximity to the galactic plane and the point sources' positions relative to the disk, we consider it likely that they are background objects and unrelated to the disk's offset from the star.
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- 2016
23. THE ORBIT and TRANSIT PROSPECTS for β PICTORIS b CONSTRAINED with ONE MILLIARCSECOND ASTROMETRY
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Wang, JJ, Graham, JR, Pueyo, L, Kalas, P, Millar-Blanchaer, MA, Ruffio, JB, Rosa, RJD, Ammons, SM, Arriaga, P, Bailey, VP, Barman, TS, Bulger, J, Burrows, AS, Cardwell, A, Chen, CH, Chilcote, JK, Cotten, T, Fitzgerald, MP, Follette, KB, Doyon, R, Duchêne, G, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Konopacky, QM, Larkin, JE, Macintosh, B, Maire, J, Marchis, F, Marley, MS, Marois, C, Metchev, S, Nielsen, EL, Oppenheimer, R, Palmer, DW, Patel, R, Patience, J, Perrin, MD, Poyneer, LA, Rajan, A, Rameau, J, Rantakyrö, FT, Savransky, D, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Vasisht, G, Vega, D, Wallace, JK, Ward-Duong, K, Wiktorowicz, SJ, and Wolff, SG
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astrometry ,planets and satellites: individual ,techniques: image processing ,astro-ph.EP ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
A principal scientific goal of the Gemini Planet Imager (GPI) is obtaining milliarcsecond astrometry to constrain exoplanet orbits. However, astrometry of directly imaged exoplanets is subject to biases, systematic errors, and speckle noise. Here, we describe an analytical procedure to forward model the signal of an exoplanet that accounts for both the observing strategy (angular and spectral differential imaging) and the data reduction method (Karhunen-Loève Image Projection algorithm). We use this forward model to measure the position of an exoplanet in a Bayesian framework employing Gaussian processes and Markov-chain Monte Carlo to account for correlated noise. In the case of GPI data on β Pic b, this technique, which we call Bayesian KLIP-FM Astrometry (BKA), outperforms previous techniques and yields 1σ errors at or below the one milliarcsecond level. We validate BKA by fitting a Keplerian orbit to 12 GPI observations along with previous astrometry from other instruments. The statistical properties of the residuals confirm that BKA is accurate and correctly estimates astrometric errors. Our constraints on the orbit of β Pic b firmly rule out the possibility of a transit of the planet at 10-σ significance. However, we confirm that the Hill sphere of β Pic b will transit, giving us a rare chance to probe the circumplanetary environment of a young, evolving exoplanet. We provide an ephemeris for photometric monitoring of the Hill sphere transit event, which will begin at the start of April in 2017 and finish at the end of January in 2018.
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- 2016
24. DISCOVERY of A SUBSTELLAR COMPANION to the NEARBY DEBRIS DISK HOST HR 2562
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Konopacky, QM, Rameau, J, Duchêne, G, Filippazzo, JC, Godfrey, PAG, Marois, C, Nielsen, EL, Pueyo, L, Rafikov, RR, Rice, EL, Wang, JJ, Ammons, SM, Bailey, VP, Barman, TS, Bulger, J, Bruzzone, S, Chilcote, JK, Cotten, T, Dawson, RI, Rosa, RJD, Doyon, R, Esposito, TM, Fitzgerald, MP, Follette, KB, Goodsell, S, Graham, JR, Greenbaum, AZ, Hibon, P, Hung, LW, Ingraham, P, Kalas, P, Lafrenière, D, Larkin, JE, Macintosh, BA, Maire, J, Marchis, F, Marley, MS, Matthews, BC, Metchev, S, Millar-Blanchaer, MA, Oppenheimer, R, Palmer, DW, Patience, J, Perrin, MD, Poyneer, LA, Rajan, A, Rantakyrö, FT, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Ward-Duong, K, Wiktorowicz, SJ, and Wolff, SG
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brown dwarfs ,instrumentation: adaptive optics ,planet-disk interactions ,stars: individual ,astro-ph.EP ,astro-ph.SR ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
We present the discovery of a brown dwarf companion to the debris disk host star HR 2562. This object, discovered with the Gemini Planet Imager (GPI), has a projected separation of 20.3 ± 0.3 au (0.″618 ± 0. ″004) from the star. With the high astrometric precision afforded by GPI, we have confirmed, to more than 5?, the common proper motion of HR 2562B with the star, with only a month-long time baseline between observations. Spectral data in the J-, H-, and K-bands show a morphological similarity to L/T transition objects. We assign a spectral type of L7 ± 3 to HR 2562Band derive a luminosity of log(Lbol/L⊙) = -4.62 ± 0.12, corresponding to a mass of 30 ± 15 MJup from evolutionary models at an estimated age of the system of 300-900 Myr. Although the uncertainty in the age of the host star is significant, the spectra and photometry exhibit several indications of youth for HR 2562B. The source has a position angle that is consistent with an orbit in the same plane as the debris disk recently resolved with Herschel. Additionally, it appears to be interior to the debris disk. Though the extent of the inner hole is currently too uncertain to place limits on the mass of HR 2562B, future observations of the disk with higher spatial resolution may be able to provide mass constraints. This is the first brown-dwarf-mass object found to reside in the inner hole of a debris disk, offering the opportunity to search for evidence of formation above the deuterium burning limit in a circumstellar disk.
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- 2016
25. The peculiar debris disk of HD 111520 as resolved by the Gemini Planet Imager
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Draper, ZH, Duchêne, G, Millar-Blanchaer, MA, Matthews, BC, Wang, JJ, Kalas, P, Graham, JR, Padgett, D, Ammons, SM, Bulger, J, Chen, C, Chilcote, JK, Doyon, R, Fitzgerald, MP, Follette, KB, Gerard, B, Greenbaum, AZ, Hibon, P, Hinkley, S, MacIntosh, B, Ingraham, P, Lafrenière, D, Marchis, F, Marois, C, Nielsen, EL, Oppenheimer, R, Patel, R, Patience, J, Perrin, M, Pueyo, L, Rajan, A, Rameau, J, Sivaramakrishnan, A, Vega, D, Ward-Duong, K, and Wolff, SG
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circumstellar matter ,stars: individual ,astro-ph.EP ,Astronomy & Astrophysics ,Astronomical and Space Sciences ,Atomic ,Molecular ,Nuclear ,Particle and Plasma Physics ,Physical Chemistry ,Atomic ,Molecular ,Nuclear ,Particle and Plasma Physics ,Physical Chemistry (incl. Structural) - Abstract
Using the Gemini Planet Imager, we have resolved the circumstellar debris disk around HD 111520 at a projected range of ∼30-100 AU in both total and polarized H-band intensity. The disk is seen edge-on at a position angle of 165° along the spine of emission. A slight inclination and asymmetric warp are covariant and alter the interpretation of the observed disk emission. We employ three point-spread function subtraction methods to reduce the stellar glare and instrumental artifacts to confirm that there is a roughly 2:1 brightness asymmetry between the NW and SE extension. This specific feature makes HD 111520 the most extreme example of asymmetric debris disks observed in scattered light among similar highly inclined systems, such as HD 15115 and HD 106906. We further identify a tentative localized brightness enhancement and scale height enhancement associated with the disk at ∼40 AU away from the star on the SE extension. We also find that the fractional polarization rises from 10% to 40% from 0.″5 to 0.″8 from the star. The combination of large brightness asymmetry and symmetric polarization fraction leads us to believe that an azimuthal dust density variation is causing the observed asymmetry.
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- 2016
26. THE PDS 66 CIRCUMSTELLAR DISK AS SEEN in POLARIZED LIGHT with the GEMINI PLANET IMAGER
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Wolff, SG, Perrin, M, Millar-Blanchaer, MA, Nielsen, EL, Wang, J, Cardwell, A, Chilcote, J, Dong, R, Draper, ZH, Duchěne, G, Fitzgerald, MP, Goodsell, SJ, Grady, CA, Graham, JR, Greenbaum, AZ, Hartung, M, Hibon, P, Hines, DC, Hung, LW, Kalas, P, Macintosh, B, Marchis, F, Marois, C, Pueyo, L, Rantakyrö, FT, Schneider, G, Sivaramakrishnan, A, and Wiktorowicz, SJ
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instrumentation: adaptive optics ,protoplanetary disks ,stars: individual ,techniques: high angular resolution ,techniques: polarimetric ,astro-ph.EP ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
We present H- and K-band imaging polarimetry for the PDS 66 circumstellar disk obtained during the commissioning of the Gemini Planet Imager (GPI). Polarization images reveal a clear detection of the disk in to the 0.″12 inner working angle (IWA) in the H band, almost three times closer to the star than the previous Hubble Space Telescope (HST) observations with NICMOS and STIS (0.″35 effective IWA). The centro-symmetric polarization vectors confirm that the bright inner disk detection is due to circumstellar scattered light. A more diffuse disk extends to a bright outer ring centered at 80 AU. We discuss several physical mechanisms capable of producing the observed ring + gap structure. GPI data confirm enhanced scattering on the east side of the disk that is inferred to be nearer to us. We also detect a lateral asymmetry in the south possibly due to shadowing from material within the IWA. This likely corresponds to a temporally variable azimuthal asymmetry observed in HST/STIS coronagraphic imaging.
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- 2016
27. The infrared imaging spectrograph (IRIS) for TMT: Latest science cases and simulations
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Wright, SA, Walth, G, Do, T, Marshall, D, Larkin, JE, Moore, AM, Adamkovics, M, Andersen, D, Armus, L, Barth, A, Cote, P, Cooke, J, Chisholm, EM, Davidge, T, Dunn, JS, Dumas, C, Ellerbroek, BL, Ghez, AM, Hao, L, Hayano, Y, Liu, M, Lopez-Rodriguez, E, Lu, JR, Mao, S, Marois, C, Pandey, SB, Phillips, AC, Schoeck, M, Subramaniam, A, Subramanian, S, Suzuki, R, Tan, JC, Terai, T, Treu, T, Simard, L, Weiss, JL, Wincentsen, J, Wong, M, and Zhang, K
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Infrared Imaging ,Infrared Spectroscopy ,Integral Field Spectrographs ,Adaptive Optics ,Data Simulator ,Giant Segmented Mirror Telescopes ,astro-ph.IM - Abstract
The Thirty Meter Telescope (TMT) first light instrument IRIS (Infrared Imaging Spectrograph) will complete its preliminary design phase in 2016. The IRIS instrument design includes a near-infrared (0.85-2.4 micron) integral field spectrograph (IFS) and imager that are able to conduct simultaneous diffraction-limited observations behind the advanced adaptive optics system NFIRAOS. The IRIS science cases have continued to be developed and new science studies have been investigated to aid in technical performance and design requirements. In this development phase, the IRIS science team has paid particular attention to the selection of filters, gratings, sensitivities of the entire system, and science cases that will benefit from the parallel mode of the IFS and imaging camera. We present new science cases for IRIS using the latest end-To-end data simulator on the following topics: Solar System bodies, the Galactic center, active galactic nuclei (AGN), and distant gravitationally-lensed galaxies. We then briefly discuss the necessity of an advanced data management system and data reduction pipeline.
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- 2016
28. The VAST Survey - IV. A wide brown dwarf companion to the A3V star $\zeta$ Delphini
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De Rosa, R. J., Patience, J., Ward-Duong, K., Vigan, A., Marois, C., Song, I., Macintosh, B., Graham, J. R., Doyon, R., Bessell, M. S., Lai, O., McCarthy, D. W., and Kulesa, C.
- Subjects
Astrophysics - Solar and Stellar Astrophysics - Abstract
We report the discovery of a wide co-moving substellar companion to the nearby ($D=67.5\pm1.1$ pc) A3V star $\zeta$ Delphini based on imaging and follow-up spectroscopic observations obtained during the course of our Volume-limited A-Star (VAST) multiplicity survey. $\zeta$ Del was observed over a five-year baseline with adaptive optics, revealing the presence of a previously-unresolved companion with a proper motion consistent with that of the A-type primary. The age of the $\zeta$ Del system was estimated as $525\pm125$ Myr based on the position of the primary on the colour-magnitude and temperature-luminosity diagrams. Using intermediate-resolution near-infrared spectroscopy, the spectrum of $\zeta$ Del B is shown to be consistent with a mid-L dwarf (L$5\pm2$), at a temperature of $1650\pm200$ K. Combining the measured near-infrared magnitude of $\zeta$ Del B with the estimated temperature leads to a model-dependent mass estimate of $50\pm15$ M$_{\rm Jup}$, corresponding to a mass ratio of $q=0.019\pm0.006$. At a projected separation of $910\pm14$ au, $\zeta$ Del B is among the most widely-separated and extreme-mass ratio substellar companions to a main-sequence star resolved to-date, providing a rare empirical constraint of the formation of low-mass ratio companions at extremely wide separations., Comment: 12 pages, 11 figures, accepted for publication in the Monthly Notices of the Royal Astronomical Society, 2014 September 25. Revised to incorporate typographical errors noted during the proofing process
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- 2014
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29. MOST light-curve analysis of the gamma Dor pulsator HR 8799, showing resonances and amplitude variations
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Sódor, Á., Chené, A. -N., De Cat, P., Bognár, Zs., Wright, D. J., Marois, C., Walker, G. A. H., Matthews, J. M., Kallinger, T., Rowe, J. F., Kuschnig, R., Guenther, D. B., Moffat, A. F. J., Rucinski, S. M., Sasselov, D., and Weiss, W. W.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
Context: The central star of the HR 8799 system is a gamma Doradus-type pulsator. The system harbours four planetary-mass companions detected by direct imaging, and is a good solar system analogue. The masses of the companions are not known accurately, because the estimation depends strongly on the age of the system, which is also not known with sufficient accuracy. Asteroseismic studies of the star might help to better constrain the age of HR 8799. We organized an extensive photometric and multi-site spectroscopic observing campaign for studying the pulsations of the central star. Aims: The aim of the present study is to investigate the pulsation properties of HR 8799 in detail via the ultra-precise 47-d-long nearly continuous photometry obtained with the MOST space telescope, and to find as many independent pulsation modes as possible, which is the prerequisite of an asteroseismic age determination. Methods: We carried out Fourier analysis of the wide-band photometric time series. Results: We find that resonance and sudden amplitude changes characterize the pulsation of HR 8799. The dominant frequency is always at f1 = 1.978 c/d. Many multiples of one ninth of the dominant frequency appear in the Fourier spectrum of the MOST data: n/9 f1, where n={1, 2, 3, 4, 5, 6, 7, 8, 9, 10, 13, 14, 17, 18}. Our analysis also reveals that many of these peaks show strong amplitude decrease and phase variations even on the 47-d time-scale. The dependencies between the pulsation frequencies of HR 8799 make the planned subsequent asteroseismic analysis rather difficult. We point out some resemblance between the light curve of HR 8799 and the modulated pulsation light curves of Blazhko RR Lyrae stars., Comment: Accepted for publication in Astronomy and Astrophysics. 8 pages, 4 figures
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- 2014
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30. First scattered-light image of the debris disk around HD 131835 with the gemini planet imager
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Hung, LW, Duchêne, G, Arriaga, P, Fitzgerald, MP, Maire, J, Marois, C, Millar-Blanchaer, MA, Bruzzone, S, Rajan, A, Pueyo, L, Kalas, PG, De Rosa, RJ, Graham, JR, Konopacky, Q, Wolff, SG, Ammons, SM, Chen, CH, Chilcote, JK, Draper, ZH, Esposito, TM, Gerard, B, Goodsell, S, Greenbaum, A, Hibon, P, Hinkley, S, MacIntosh, B, Marchis, F, Metchev, S, Nielsen, EL, Oppenheimer, R, Patience, JL, Perrin, MD, Rantakyrö, FT, Sivaramakrishnan, A, Wang, JJ, Ward-Duong, K, and Wiktorowicz, SJ
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circumstellar matter ,infrared: stars ,stars: individual ,astro-ph.EP ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
We present the first scattered-light image of the debris disk around HD 131835 in the H band using the Gemini Planet Imager. HD 131835 is a ∼15 Myr old A2IV star at a distance of ∼120 pc in the Sco-Cen OB association. We detect the disk only in polarized light and place an upper limit on the peak total intensity. No point sources resembling exoplanets were identified. Compared to its mid-infrared thermal emission, in scattered light the disk shows similar orientation but different morphology. The scattered-light disk extends from ∼75 to ∼210 AU in the disk plane with roughly flat surface density. Our Monte Carlo radiative transfer model can describe the observations with a model disk composed of a mixture of silicates and amorphous carbon. In addition to the obvious brightness asymmetry due to stronger forward scattering, we discover a weak brightness asymmetry along the major axis, with the northeast side being 1.3 times brighter than the southwest side at a 3σ level.
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- 2015
31. Rare predicted loss-of-function variants of type I IFN immunity genes are associated with life-threatening COVID-19
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Matuozzo, D, Talouarn, E, Marchal, A, Zhang, P, Manry, J, Seeleuthner, Y, Zhang, Y, Bolze, A, Chaldebas, M, Milisavljevic, B, Gervais, A, Bastard, P, Asano, T, Bizien, L, Barzaghi, F, Abolhassani, H, Abou Tayoun, A, Aiuti, A, Alavi Darazam, I, Allende, L, Alonso-Arias, R, Arias, A, Aytekin, G, Bergman, P, Bondesan, S, Bryceson, Y, Bustos, I, Cabrera-Marante, O, Carcel, S, Carrera, P, Casari, G, Chaibi, K, Colobran, R, Condino-Neto, A, Covill, L, Delmonte, O, El Zein, L, Flores, C, Gregersen, P, Gut, M, Haerynck, F, Halwani, R, Hancerli, S, Hammarstrom, L, Hatipoglu, N, Karbuz, A, Keles, S, Kyheng, C, Leon-Lopez, R, Franco, J, Mansouri, D, Martinez-Picado, J, Metin Akcan, O, Migeotte, I, Morange, P, Morelle, G, Martin-Nalda, A, Novelli, G, Novelli, A, Palabiyik, F, Pan-Hammarstrom, Q, de Diego, R, Planas-Serra, L, Pleguezuelo, D, Prando, C, Pujol, A, Reyes, L, Riviere, J, Rodriguez-Gallego, C, Rojas, J, Rovere-Querini, P, Schluter, A, Shahrooei, M, Sobh, A, Soler-Palacin, P, Tandjaoui-Lambiotte, Y, Tipu, I, Tresoldi, C, Troya, J, van de Beek, D, Zatz, M, Zawadzki, P, Al-Muhsen, S, Alosaimi, M, Alsohime, F, Baris-Feldman, H, Butte, M, Constantinescu, S, Cooper, M, Dalgard, C, Fellay, J, Heath, J, Lau, Y, Lifton, R, Maniatis, T, Mogensen, T, von Bernuth, H, Lermine, A, Vidaud, M, Boland, A, Deleuze, J, Nussbaum, R, Kahn-Kirby, A, Mentre, F, Tubiana, S, Gorochov, G, Tubach, F, Hausfater, P, Al-Mulla, F, Anderson, M, Andreakos, E, Feldman, H, Belot, A, Biggs, C, Bogunovic, D, Bondarenko, A, Bousfiha, A, Brodin, P, Bustamante, C, Chakravorty, S, Christodoulou, J, Desai, M, Drolet, B, Baghdadi, J, Espinosa-Padilla, S, Froidure, A, Hagin, D, Henrickson, S, Hsieh, E, Husebye, E, Imai, K, Itan, Y, Jarvis, E, Karamitros, T, Kisand, K, Ku, C, Ling, Y, Lucas, C, Marodi, L, Milner, J, Mironska, K, Morio, T, Ng, L, O'Farrelly, C, Okada, S, Planas, A, Quintana-Murci, L, Renia, L, Resnick, I, Sancho-Shimizu, V, Sediva, A, Seppanen, M, Shcherbina, A, Slaby, O, Snow, A, Spaan, A, Tancevski, I, Tangye, S, Ramaswamy, S, Turvey, S, Uddin, F, Uddin, M, Vinh, D, Casanova, J, Vacher, Y, Gysembergh-Houal, A, Demerville, L, Chachoua, A, Abad, S, Abassi, R, Abdellaoui, A, Abdelmalek, A, Abdoul, H, Abergel, H, Abeud, F, Abgrall, S, Abisror, N, Adechian, M, Aderdour, N, Admane, H, Adnet, F, Afritt, S, Agostini, H, Aguilar, C, Agut, S, Aiello, T, Kaci, M, Oufella, H, Ajeenthiravasan, G, Alauzy, V, Alby-Laurent, F, Allard, L, Alyanakian, M, Borrero, B, Amam, S, Amrouche, L, Andronikof, M, Anglicheau, D, Anguel, N, Annane, D, Aounzou, M, Aparicio, C, Aratus, G, Arlet, J, Arzoine, J, Aslangul, E, Assefi, M, Aubry, A, Audiffred, L, Audureau, E, Auger, C, Auregan, J, Awotar, C, Milla, S, Azan, D, Azemar, L, Azzouguen, B, Elrufaai, M, Badsi, A, Bakouboula, P, Balcerowiak, C, Balde, F, Baldivia, E, Bangamingo, E, Baptiste, A, Baran-Marszak, F, Barau, C, Barget, N, Baronnet, F, Barthelemy, R, Baudel, J, Baudry, C, Baudry, E, Beaugerie, L, Belamri, A, Belaube, N, Belilita, R, Bellassen, P, Belmokhtar, R, Beltran, I, Benainous, R, Benallaoua, M, Benamouzig, R, Benbara, A, Benhida, J, Benkhelouf, A, Benlagha, J, Benmostafa, C, Benothmane, S, Bentifraouine, M, Berard, L, Bernier, Q, Berti, E, Bertier, A, Berton, L, Bessis, S, Beurton, A, Bianco, C, Bianquis, C, Bidar, F, Blanche, P, Blayau, C, Bleibtreu, A, Blin, E, Bloch-Queyrat, C, Boissier, M, Bollens, D, Bolzoni, M, Bompard, R, Bonnet, N, Bonnouvrier, J, Botha, S, Boucenna, W, Bouchama, F, Bouchaud, O, Bouchghoul, H, Boudjebla, T, Boudjema, N, Bouffard, C, Bougle, A, Bouguerra, M, Bouras, L, Bourcier, A, Durand, A, Bourrier, A, Bouscarat, F, Bouvry, D, Bouziri, N, Bouzrara, O, Bribier, S, Brugier, D, Brunel, M, Bui, E, Buisson, A, Bukreyeva, I, Bureau, C, Cadranel, J, Cailhol, J, Calin, R, Vega, C, Canavaggio, P, Cancella, M, Cantin, D, Cao, A, Carbillon, L, Carlier, N, Cassard, C, Castor, G, Cauchy, M, Cha, O, Chaigne, B, Challal, S, Champion, K, Chariot, P, Chas, J, Chauveau, S, Chauvin, A, Chauvin, C, Chavarot, N, Chebbout, K, Cherai, M, Cherubini, I, Chevalier, A, Chiarabini, T, Chinet, T, Chocron, R, Choinier, P, Chommeloux, J, Choquet, C, Choupeaux, L, Chousterman, B, Ciocan, D, Clarke, A, Clavere, G, Clavier, F, Clement, K, Clerc, S, Cohen, Y, Cohen, F, Cohen, A, Coilly, A, Colboc, H, Colin, P, Collet, M, Comarmond, C, Combacon, E, Combes, A, Comparon, C, Constantin, J, Cordel, H, Cordier, A, Costantini, A, Chalumeau, N, Couffignal, C, Coupeau, D, Creange, A, Lamarre, Y, Da Silveira, C, Kayani, S, De Castro, N, De Rycke, Y, Del Pozo, L, Delannoy, Q, Delay, M, Deleris, R, Delforge, J, Delphine, L, Demare, N, Demeret, S, Demoule, A, Deniau, A, Depret, F, Derolez, S, Derradji, O, Derridj, N, Descamps, V, Deschamps, L, Desconclois, C, Desnos, C, Desongins, K, Dhote, R, Diallo, B, Didier, M, Diemer, M, Diez, S, Djadi-Prat, J, Monnory, F, Djebara, S, Djebra, N, Djietcheu, M, Djillali, H, Djouadi, N, Donneger, S, Dos Santos, C, Dournon, N, Dres, M, Droctove, L, Drogrey, M, 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B., Magazimama-Ext A., Maingret D., Mameri L., Manivet P., Mansouri C., Marcault E., Marey J., Marin N., Marois C., Martin O., Martineau L., Martinez-Lopez C., Martyniuck P., De Farcy P. M., Marzouk N., Masmoudi R., Mebazaa A., Mechai F., Mecozzi F., Mediouni C., Megarbane B., Meghadecha M., Mejean E., Mekinian A., Abdelhadi N. M., Mekni R., Meliti T. S., Lima B. M., Meng P., Merbah S., Messani F., Messaoudi Y., Mewasing B. -I., Meziane L., Michelot-Burger C., Mignot F., Minka F. H., Miyara M., Moine P., Molina J. -M., Montegnies-Boulet A., Monti A., Montlahuc C., Montout A. -L., Moores A., Morbieu C., Mortelette H., Mouly S., Muzaffar R., Nacerddine C. I., Nadal M., Nadif H., Nassarmadji K., Natella P., Ndingamondze S., Neraal S., Nguyen C., N'Guyen B., Larmurier I. N., Nlomenyengue L., Noel N., Nunes H., Omar E., Ouazene Z., Ouedraogo E., Ouelaa W., Oukhedouma A., Amara Y. 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U., Uzunhan Y., Vaittinadaayar P., Valent A., Valentian M., Valin N., Vallet H., Vaz M., Vazquezibarra M. -A., Vedie B., Velly L., Verstuyft C., Viallette C., Vicaut E., Vignes D., Vimpere D., Virlouvet M., Voiriot G., Voisot L., Weiss E., Weiss N., Winchenne A., Yordanov Y., Zafrani L., Zaidan M., Zaidi W., Zak C., Zarhrate-Ghoul A., Zatout O., Zeino S., Zeitouni M., Zemirli N., Zerah L., Zia O., Ziol M., Zolario O., Zuber J., Andrejak C., Angoulvant F., Bachelet D., Bartoli M., Basmaci R., Behilill S., Beluze M., Benkerrou D., Bhavsar K., Bouadma L., Bouchez S., Bouscambert M., Cervantes-Gonzalez M., Chair A., Coelho A., d'Ortenzio E., Debray M. -P., Deconinck L., Deplanque D., Descamps D., Desvallee M., Diallo A., Diouf A., Dorival C., Dubos F., Duval X., Elharrar B., Eloy P., Enouf V., Esperou H., Esposito-Farese M., Devouge E. F., Gault N., Gaymard A., Ghosn J., Gigante T., Gilg M., Guedj J., Hoctin A., Hoffmann I., Houas I., Hulot J. -S., Jaafoura S., Kaguelidou F., Kali S., Khalil A., Khan C., Laouenan C., Laribi S., Le M., Le Hingrat Q., Le Mestre S., Le Nagard H., Lescure F. -X., Levy Y., Lingas G., Lucet J. C., Malvy D., Mambert M., Meziane A., Mouquet H., Mullaert J., Neant N., Nguyen D., Noret M., Nseir S., Papadopoulos A., Paul C., Peiffer-Smadja N., Perpoint T., Petrov-Sanchez V., Peytavin G., Pham H., Picone O., Puechal O., Rabaud C., Rosa-Calatrava M., Rossignol B., Rossignol P., Roy C., Schneider M., Su R., Tardivon C., Tellier M. -C., Teoule F., Terrier O., Timsit J. -F., Tual C., Van Der Werf S., Vanel N., Veislinger A., Visseaux B., Wiedemann A., Yazdanpanah Y., Alavoine L., Behillil S., Burdet C., Charpentier C., Dechanet A., Ecobichon J. -L., Frezouls W., Houhou N., Lehacaut J., Letrou S., Lina B., Manchon P., Nouroudine M., Piquard V., Quintin C., Thy M., Vignali V., Chahine A., Waucquier N., Migaud M. -C., Djossou F., Mergeay-Fabre M., Lucarelli A., Demar M., Bruneau L., Gerardin P., Maillot A., Payet C., Laviolle B., Laine F., Paris C., Desille-Dugast M., Fouchard J., Pistone T., Perreau P., Gissot V., Goas C. L. 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E., Euvrard R., Fabio G., Faivre L., Falck A., Faure M., Arquero M. F., Ferrer R., Ferreres J., Francois B., Fumado V., Fung K. S. C., Fusco F., Gagro A., Solis B. G., Garcon P., Gaussem P., Gayretli Z., Gil-Herrera J., Gilardin L., Gatineau A. G., Girona-Alarcon M., Godinez K. A. C., Goffard J. -C., Gonzales N., Gonzalez-Granado L. I., Gonzalez-Montelongo R., Guerder A., Gulhan B., Gumucio V. D., Hanitsch L. G., Gunst J., Hadjadj J., Hariyan T., Heppekcan D., Hernandez-Brito E., Ho P. -K., Holanda-Pena M. S., Horcajada J. P., Hraiech S., Humbert L., Hung I. F. N., Iglesias A. D., Inigo-Campos A., Jamme M., Arranz M. J., Jimeno M. -T., Jordan I., Yuksek S. K., Kara Y. B., Karahan A., Yasar K. K., Kasapcopur O., Kashimada K., Demirkol Y. K., Kido Y., Kizil C., Kilic A. O., Klocperk A., Koutsoukou A., Krol Z. J., Ksouri H., Kuentz P., Kwan A. M. C., Kwan Y. W. M., Kwok J. S. Y., Lagier J. -C., Lam D. S. Y., Lampropoulou V., Le Bourgeois F., Leo Y. -S., Leung D., Levin M., Levy M., Levy R., Li Z., Lilleri D., Lima E. J. A. B., Linglart A., Lopez-Collazo E., Lorenzo-Salazar J. M., Louapre C., Lubetzki C., Lung K. -C., Luyt C. -E., Lye D. C., Magnone C., Marchioni E., Marioli C., Marjani M., Marques L., Pereira J. M., Pueyo D. M., Marzana I., Mata-Martinez C., Mathian A., Matos L. R. B., Matthews G. V., Mayaux J., McLaughlin-Garcia R., Meersseman P., Mege J. -L., Mekontso-Dessap A., Melki I., Meloni F., Meritet J. -F., Merlani P., Akcan O. M., Mezidi M., Millereux M., Million M., Mirault T., Mircher C., Mirsaeidi M., Mizoguchi Y., Modi B. P., Mojoli F., Moncomble E., Melian A. M., Martinez A. M., Morandeira F., Mordacq C., Mouly S. J., Munoz-Barrera A., Nafati C., Nagashima S., Nakagama Y., Neven B., Neves J. F., Ng Y. -Y., Nielly H., Medina Y. N., Cuadros E. N., Ocejo-Vinyals J. G., Okamoto K., Oualha M., Ouedrani A., Ozcelik T., Ozkaya-Parlakay A., Pagani M., Papadaki M., Parola P., Pascreau T., Paul S., Paz-Artal E., Pedraza S., Pellecer N. C. G., Pellegrini S., Perez-Fernandez X. L., Philippe A., Philippot Q., Picod A., Piralla A., Ploin D., Poissy J., Poncelet G., Poulakou G., Pouletty M. S., Pourshahnazari P., Qiu-Chen J. L., Quentric P., Rambaud T., Raoult D., Raoult V., Rebillat A. -S., Redin C., Resmini L., Ricart P., Richard J. -C., Rigo-Bonnin R., rivet N., Rocamora-Blanch G., Rodero M. P., Rodrigo C., Rodriguez L. A., Rodriguez-Palmero A., Romero C. S., Rothenbuhler A., Roux D., Rovina N., Rozenberg F., Ruch Y., Ruiz M., del Prado M. Y. R., Ruiz-Rodriguez J. C., Sabater-Riera J., Saks K., Salagianni M., Sanchez O., Sanchez-Montalva A., Sanchez-Ramon S., Schidlowski L., Schmidt J., Schmidt M., Schuetz C., Schweitzer C. E., Scolari F., Seijo L., Seminario A. G., Seng P., Senoglu S., Seppanen M., Llovich A. S., Siguret V., Siouti E., Smadja D. M., Smith N., Solanich X., Sole-Violan J., Soler C., Stella G. M., Stepanovskiy Y., Stoclin A., Taccone F., Taupin J. -L., Tavernier S. J., Tello L. V., Terrier B., Thiery G., Thorball C., Thorn K., Thumerelle C., Tolstrup M., Tomasoni G., Toubiana J., Alvarez J. T., Triantafyllia V., Trouillet-Assant S., Tsang O. T. Y., Tserel L., Tso E. Y. K., Tucci A., Oz S. K. T., Ursini M. V., Utsumi T., Vabres P., Valencia-Ramos J., Van Den Rym A. M., Vandernoot I., Velez-Santamaria V., Veliz S. P. Z., Vidigal M. C., Viel S., Villain C., Vilaire-Meunier M. E., Villar-Garcia J., Vincent A., Volokha A., Vuotto F., Wauters E., Wauters J., Wu A. K. L., Wu T. -C., Yahsi A., Yesilbas O., Yildiz M., Young B. E., Yukselmis U., Zecca M., Zuccaro V., Van Praet J., Lambrecht B. N., Van Braeckel E., Bosteels C., Hoste L., Hoste E., Bauters F., De Clercq J., Heijmans C., Slabbynck H., Naesens L., Florkin B., Boulanger C., Vanderlinden D., Berkell M., Carelli V., Malhotra S., Mattiaccio A., Pippucci T., Seri M., Tacconelli E., van Agtmael M., Algera A. G., Appelman B., van Baarle F., Bax D., Beudel M., Bogaard H. J., Bomers M., Bonta P., Bos L., Botta M., de Brabander J., de Bree G., de Bruin S., Buis D. T. P., Bugiani M., Bulle E., Cloherty O. C. A., Dijkstra M., Dongelmans D. A., Dujardin R. W. G., Elbers P., Fleuren L., Geijtenbeek S. G. T., Girbes A., Goorhuis B., Grobusch M. P., Hafkamp F., Hagens L., Hamann J., Harris V., Hemke R., Heunks S. M. H. L., Hollmann M., Horn J., Hovius J. W., de Jong M. D., Koning R., Lim E. H. T., van Mourik N., Nellen J., Nossent E. J., Paulus F., Peters E., Pina-Fuentes D. A. I., van der Poll T., Preckel B., Prins J. M., Raasveld J., Reijnders T., de Rotte M. C. F. J., Schinkel M., Schultz M. J., Schrauwen F. A. P., Schuurmans A., Schuurmans J., Sigaloff K., Slim M. A., Smeele P., Smit M., Stijnis C. S., Stilma W., Teunissen C., Thoral P., Tsonas A. M., Tuinman P. R., van der Valk M., Veelo D., Volleman C., de Vries H., Vught L. A., van Vugt M., Wouters D., Zwinderman A. H., Brouwer M. C., Wiersinga W. J., Vlaar A. P. J., Tompkins M. F., Alba C., Hupalo D. N., Rosenberger J., Sukumar G., Wilkerson M. D., Zhang X., Lack J., Oler A. J., Dobbs K., Danielson J. J., Biondi A., Bettini L. R., D'Angio' M., Beretta I., Imberti L., Sottini A., Quaresima V., Quiros-Roldan E., Rossi C., Meyts I., Zhang S. -Y., Puel A., Notarangelo L. D., Boisson-Dupuis S., Su H. C., Boisson B., Jouanguy E., Zhang Q., Abel L., and Cobat A.
- Abstract
Background: We previously reported that impaired type I IFN activity, due to inborn errors of TLR3- and TLR7-dependent type I interferon (IFN) immunity or to autoantibodies against type I IFN, account for 15–20% of cases of life-threatening COVID-19 in unvaccinated patients. Therefore, the determinants of life-threatening COVID-19 remain to be identified in ~ 80% of cases. Methods: We report here a genome-wide rare variant burden association analysis in 3269 unvaccinated patients with life-threatening COVID-19, and 1373 unvaccinated SARS-CoV-2-infected individuals without pneumonia. Among the 928 patients tested for autoantibodies against type I IFN, a quarter (234) were positive and were excluded. Results: No gene reached genome-wide significance. Under a recessive model, the most significant gene with at-risk variants was TLR7, with an OR of 27.68 (95%CI 1.5–528.7, P = 1.1 × 10−4) for biochemically loss-of-function (bLOF) variants. We replicated the enrichment in rare predicted LOF (pLOF) variants at 13 influenza susceptibility loci involved in TLR3-dependent type I IFN immunity (OR = 3.70[95%CI 1.3–8.2], P = 2.1 × 10−4). This enrichment was further strengthened by (1) adding the recently reported TYK2 and TLR7 COVID-19 loci, particularly under a recessive model (OR = 19.65[95%CI 2.1–2635.4], P = 3.4 × 10−3), and (2) considering as pLOF branchpoint variants with potentially strong impacts on splicing among the 15 loci (OR = 4.40[9%CI 2.3–8.4], P = 7.7 × 10−8). Finally, the patients with pLOF/bLOF variants at these 15 loci were significantly younger (mean age [SD] = 43.3 [20.3] years) than the other patients (56.0 [17.3] years; P = 1.68 × 10−5). Conclusions: Rare variants of TLR3- and TLR7-dependent type I IFN immunity genes can underlie life-threatening COVID-19, particularly with recessive inheritance, in patients under 60 years old.
- Published
- 2023
32. Direct imaging of an asymmetric debris disk in the HD 106906 planetary system
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Kalas, PG, Rajan, A, Wang, JJ, Millar-Blanchaer, MA, Duchene, G, Chen, C, Fitzgerald, MP, Dong, R, Graham, JR, Patience, J, Macintosh, B, Murray-Clay, R, Matthews, B, Rameau, J, Marois, C, Chilcote, J, Rosa, RJD, Doyon, R, Draper, ZH, Lawler, S, Ammons, SM, Arriaga, P, Bulger, J, Cotten, T, Follette, KB, Goodsell, S, Greenbaum, A, Hibon, P, Hinkley, S, Hung, LW, Ingraham, P, Konapacky, Q, Lafreniere, D, Larkin, JE, Long, D, Maire, J, Marchis, F, Metchev, S, Morzinski, KM, Nielsen, EL, Oppenheimer, R, Perrin, MD, Pueyo, L, Rantakyrö, FT, Ruffio, JB, Saddlemyer, L, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Soummer, R, Song, I, Thomas, S, Vasisht, G, Ward-Duong, K, Wiktorowicz, SJ, and Wolff, SG
- Subjects
circumstellar matter ,infrared: stars ,stars: individual ,techniques: high angular resolution ,astro-ph.EP ,Astronomy & Astrophysics ,Astronomical and Space Sciences ,Atomic ,Molecular ,Nuclear ,Particle and Plasma Physics ,Physical Chemistry ,Atomic ,Molecular ,Nuclear ,Particle and Plasma Physics ,Physical Chemistry (incl. Structural) - Abstract
We present the first scattered light detections of the HD 106906 debris disk using the Gemini/Gemini Planet Imager in the infrared and Hubble Space Telescope (HST)/Advanced Camera for Surveys in the optical. HD 106906 is a 13 Myr old F5V star in the Sco-Cen association, with a previously detected planet-mass candidate HD 106906b projected 650 AU from the host star. Our observations reveal a near edge-on debris disk that has a central cleared region with radius ∼50 AU, and an outer extent >500 AU. The HST data show that the outer regions are highly asymmetric, resembling the "needle" morphology seen for the HD 15115 debris disk. The planet candidate is oriented ∼21° away from the position angle of the primary's debris disk, strongly suggesting non-coplanarity with the system. We hypothesize that HD 106906b could be dynamically involved in the perturbation of the primary's disk, and investigate whether or not there is evidence for a circumplanetary dust disk or cloud that is either primordial or captured from the primary. We show that both the existing optical properties and near-infrared colors of HD 106906b are weakly consistent with this possibility, motivating future work to test for the observational signatures of dust surrounding the planet.
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- 2015
33. Astrometric confirmation and preliminary orbital parameters of the young exoplanet 51 eridani b with the gemini planet imager
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De Rosa, RJD, Nielsen, EL, Blunt, SC, Graham, JR, Konopacky, QM, Marois, C, Pueyo, L, Rameau, J, Ryan, DM, Wang, JJ, Bailey, V, Chontos, A, Fabrycky, DC, Follette, KB, MacIntosh, B, Marchis, F, Ammons, SM, Arriaga, P, Chilcote, JK, Cotten, TH, Doyon, R, Duchene, G, Esposito, TM, Fitzgerald, MP, Gerard, B, Goodsell, SJ, Greenbaum, AZ, Hibon, P, Ingraham, P, Johnson-Groh, M, Kalas, PG, Lafreniere, D, Maire, J, Metchev, S, Millar-Blanchaer, MA, Morzinski, KM, Oppenheimer, R, Patel, RI, Patience, JL, Perrin, MD, Rajan, A, Rantakyrö, FT, Ruffio, JB, Schneider, AC, Sivaramakrishnan, A, Song, I, Tran, D, Vasisht, G, Ward-Duong, K, and Wolff, SG
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planetary systems ,planets and satellites: detection ,stars: individual ,astro-ph.EP ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
We present new Gemini Planet Imager observations of the young exoplanet 51 Eridani b that provide further evidence that the companion is physically associated with 51 Eridani. Combining this new astrometric measurement with those reported in the literature, we significantly reduce the posterior probability that 51 Eridani b is an unbound foreground or background T-dwarf in a chance alignment with 51 Eridani to 2 × 10-7, an order of magnitude lower than previously reported. If 51 Eridani b is indeed a bound object, then we have detected orbital motion of the planet between the discovery epoch and the latest epoch. By implementing a computationally efficient Monte Carlo technique, preliminary constraints are placed on the orbital parameters of the system. The current set of astrometric measurements suggest an orbital semimajor axis of AU, corresponding to a period of years (assuming a mass of 1.75 Mo for the central star), and an inclination of deg. The remaining orbital elements are only marginally constrained by the current measurements. These preliminary values suggest an orbit that does not share the same inclination as the orbit of the distant M-dwarf binary, GJ 3305, which is a wide physically bound companion to 51 Eridani.
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- 2015
34. Discovery and spectroscopy of the young jovian planet 51 Eri b with the Gemini Planet Imager.
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Macintosh, B, Graham, JR, Barman, T, De Rosa, RJ, Konopacky, Q, Marley, MS, Marois, C, Nielsen, EL, Pueyo, L, Rajan, A, Rameau, J, Saumon, D, Wang, JJ, Patience, J, Ammons, M, Arriaga, P, Artigau, E, Beckwith, S, Brewster, J, Bruzzone, S, Bulger, J, Burningham, B, Burrows, AS, Chen, C, Chiang, E, Chilcote, JK, Dawson, RI, Dong, R, Doyon, R, Draper, ZH, Duchêne, G, Esposito, TM, Fabrycky, D, Fitzgerald, MP, Follette, KB, Fortney, JJ, Gerard, B, Goodsell, S, Greenbaum, AZ, Hibon, P, Hinkley, S, Cotten, TH, Hung, L-W, Ingraham, P, Johnson-Groh, M, Kalas, P, Lafreniere, D, Larkin, JE, Lee, J, Line, M, Long, D, Maire, J, Marchis, F, Matthews, BC, Max, CE, Metchev, S, Millar-Blanchaer, MA, Mittal, T, Morley, CV, Morzinski, KM, Murray-Clay, R, Oppenheimer, R, Palmer, DW, Patel, R, Perrin, MD, Poyneer, LA, Rafikov, RR, Rantakyrö, FT, Rice, EL, Rojo, P, Rudy, AR, Ruffio, J-B, Ruiz, MT, Sadakuni, N, Saddlemyer, L, Salama, M, Savransky, D, Schneider, AC, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Vasisht, G, Wallace, JK, Ward-Duong, K, Wiktorowicz, SJ, Wolff, SG, and Zuckerman, B
- Subjects
astro-ph.EP ,General Science & Technology - Abstract
Directly detecting thermal emission from young extrasolar planets allows measurement of their atmospheric compositions and luminosities, which are influenced by their formation mechanisms. Using the Gemini Planet Imager, we discovered a planet orbiting the ~20-million-year-old star 51 Eridani at a projected separation of 13 astronomical units. Near-infrared observations show a spectrum with strong methane and water-vapor absorption. Modeling of the spectra and photometry yields a luminosity (normalized by the luminosity of the Sun) of 1.6 to 4.0 × 10(-6) and an effective temperature of 600 to 750 kelvin. For this age and luminosity, "hot-start" formation models indicate a mass twice that of Jupiter. This planet also has a sufficiently low luminosity to be consistent with the "cold-start" core-accretion process that may have formed Jupiter.
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- 2015
35. Gemini planet imager observations of the au microscopii debris disk: Asymmetries within one arcsecond
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Wang, JJ, Graham, JR, Pueyo, L, Nielsen, EL, Millar-Blanchaer, M, Rosa, RJD, Kalas, P, Ammons, SM, Bulger, J, Cardwell, A, Chen, C, Chiang, E, Chilcote, JK, Doyon, R, Draper, ZH, Duchêne, G, Esposito, TM, Fitzgerald, MP, Goodsell, SJ, Greenbaum, AZ, Hartung, M, Hibon, P, Hinkley, S, Hung, LW, Ingraham, P, Larkin, JE, Macintosh, B, Maire, J, Marchis, F, Marois, C, Matthews, BC, Morzinski, KM, Oppenheimer, R, Patience, J, Perrin, MD, Rajan, A, Rantakyrö, FT, Sadakuni, N, Serio, A, Sivaramakrishnan, A, Soummer, R, Thomas, S, Ward-Duong, K, Wiktorowicz, SJ, and Wolff, SG
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circumstellar matter ,instrumentation: adaptive optics ,methods: data analysis ,planet-disk interactions ,stars: individual ,techniques: high angular resolution ,astro-ph.EP ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
We present Gemini Planet Imager (GPI) observations of AU Microscopii, a young M dwarf with an edge-on, dusty debris disk. Integral field spectroscopy and broadband imaging polarimetry were obtained during the commissioning of GPI. In our broadband imaging polarimetry observations, we detect the disk only in total intensity and find asymmetries in the morphology of the disk between the southeast (SE) and northwest (NW) sides. The SE side of the disk exhibits a bump at 1″ (10 AU projected separation) that is three times more vertically extended and three times fainter in peak surface brightness than the NW side at similar separations. This part of the disk is also vertically offset by 69 ± 30 mas to the northeast at 1″ when compared to the established disk midplane and is consistent with prior Atacama Large Millimeter/submillimeter Array and Hubble Space Telescope/Space Telescope Imaging Spectrograph observations. We see hints that the SE bump might be a result of detecting a horizontal sliver feature above the main disk that could be the disk backside. Alternatively, when including the morphology of the NW side, where the disk midplane is offset in the opposite direction ∼50 mas between 0.″4 and 1.″2, the asymmetries suggest a warp-like feature. Using our integral field spectroscopy data to search for planets, we are 50% complete for ∼4 MJup planets at 4 AU. We detect a source, resolved only along the disk plane, that could either be a candidate planetary mass companion or a compact clump in the disk.
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- 2015
36. β PICTORIS' INNER DISK in POLARIZED LIGHT and NEW ORBITAL PARAMETERS for β PICTORIS b
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Millar-Blanchaer, MA, Graham, JR, Pueyo, L, Kalas, P, Dawson, RI, Wang, J, Perrin, MD, Moon, DS, Macintosh, B, Ammons, SM, Barman, T, Cardwell, A, Chen, CH, Chiang, E, Chilcote, J, Cotten, T, Rosa, RJD, Draper, ZH, Dunn, J, Duchêne, G, Esposito, TM, Fitzgerald, MP, Follette, KB, Goodsell, SJ, Greenbaum, AZ, Hartung, M, Hibon, P, Hinkley, S, Ingraham, P, Jensen-Clem, R, Konopacky, Q, Larkin, JE, Long, D, Maire, J, Marchis, F, Marley, MS, Marois, C, Morzinski, KM, Nielsen, EL, Palmer, DW, Oppenheimer, R, Poyneer, L, Rajan, A, Rantakyrö, FT, Ruffio, JB, Sadakuni, N, Saddlemyer, L, Schneider, AC, Sivaramakrishnan, A, Soummer, R, Thomas, S, Vasisht, G, Vega, D, Wallace, JK, Ward-Duong, K, Wiktorowicz, SJ, and Wolff, SG
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astrometry ,planet-disk interactions ,planets and satellites: individual ,techniques: polarimetric ,astro-ph.EP ,Astronomy & Astrophysics ,Astronomical and Space Sciences ,Atomic ,Molecular ,Nuclear ,Particle and Plasma Physics ,Physical Chemistry ,Atomic ,Molecular ,Nuclear ,Particle and Plasma Physics ,Physical Chemistry (incl. Structural) - Abstract
We present H-band observations of β Pic with the Gemini Planet Imager's (GPI's) polarimetry mode that reveal the debris disk between ∼0.″3 (6 AU) and ∼1.″7 (33 AU), while simultaneously detecting β Pic b. The polarized disk image was fit with a dust density model combined with a Henyey-Greenstein scattering phase function. The best-fit model indicates a disk inclined to the line of sight () with a position angle (PA) (slightly offset from the main outer disk, ), that extends from an inner disk radius of to well outside GPI's field of view. In addition, we present an updated orbit for β Pic b based on new astrometric measurements taken in GPI's spectroscopic mode spanning 14 months. The planet has a semimajor axis of , with an eccentricity The PA of the ascending node is offset from both the outer main disk and the inner disk seen in the GPI image. The orbital fit constrains the stellar mass of β Pic to Dynamical sculpting by β Pic b cannot easily account for the following three aspects of the inferred disk properties: (1) the modeled inner radius of the disk is farther out than expected if caused by β Pic b; (2) the mutual inclination of the inner disk and β Pic b is when it is expected to be closer to zero; and (3) the aspect ratio of the disk () is larger than expected from interactions with β Pic b or self-stirring by the disk's parent bodies.
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- 2015
37. Polarimetry with the gemini planet imager: Methods, performance at first light, and the circumstellar ring around HR 4796A
- Author
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Perrin, MD, Duchene, G, Millar-Blanchaer, M, Fitzgerald, MP, Graham, JR, Wiktorowicz, SJ, Kalas, PG, Macintosh, B, Bauman, B, Cardwell, A, Chilcote, J, De Rosa, RJ, Dillon, D, Doyon, R, Dunn, J, Erikson, D, Gavel, D, Goodsell, S, Hartung, M, Hibon, P, Ingraham, P, Kerley, D, Konapacky, Q, Larkin, JE, Maire, J, Marchis, F, Marois, C, Mittal, T, Morzinski, KM, Oppenheimer, BR, Palmer, DW, Patience, J, Poyneer, L, Pueyo, L, Rantakyrö, FT, Sadakuni, N, Saddlemyer, L, Savransky, D, Soummer, R, Sivaramakrishnan, A, Song, I, Thomas, S, Wallace, JK, Wang, JJ, and Wolff, SG
- Subjects
circumstellar matter ,instrumentation: adaptive optics ,instrumentation: high angular resolution ,instrumentation: polarimeters ,polarization ,stars: individual ,astro-ph.EP ,astro-ph.IM ,Astronomy & Astrophysics ,Astronomical and Space Sciences ,Atomic ,Molecular ,Nuclear ,Particle and Plasma Physics ,Physical Chemistry ,Atomic ,Molecular ,Nuclear ,Particle and Plasma Physics ,Physical Chemistry (incl. Structural) - Abstract
We present the first results from the polarimetry mode of the Gemini Planet Imager (GPI), which uses anew integral field polarimetry architecture to provide high contrast linear polarimetry with minimal systematic biases between the orthogonal polarizations. We describe the design, data reduction methods, and performance of polarimetry with GPI. Point-spread function (PSF) subtraction via differential polarimetry suppresses unpolarized starlight by a factor of over 100, and provides sensitivity to circumstellar dust reaching the photon noise limit for these observations. in the case of the circumstellar disk around HR 4796A,GPI's advanced adaptive optics system reveals the disk clearly even prior to PSF subtraction. In polarized light, the disk is seen all the way in to its semi-minor axis for the first time. The disk exhibits surprisingly strong asymmetry in polarized intensity, with the west side ≳9 times brighter than the east side despite the fact that the east side is slightly brighter in total intensity. Based on a synthesis of the total and polarized intensities, we now believe that the west side is closer to us, contrary to most prior interpretations. Forward scattering by relatively large silicate dust particles leads to the strong polarized intensity on thewest side, and the ring must be slightly optically thick in order to explain the lower brightness in total intensity there. These findings suggest that the ring is geometrically narrow and dynamically cold, perhaps shepherded by larger bodies in the same manner as Saturn's Fring.
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- 2015
38. The first H-band spectrum of the giant planet β Pictoris b
- Author
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Chilcote, J, Barman, T, Fitzgerald, MP, Graham, JR, Larkin, JE, Macintosh, B, Bauman, B, Burrows, AS, Cardwell, A, De Rosa, RJ, Dillon, D, Doyon, R, Dunn, J, Erikson, D, Gavel, D, Goodsell, SJ, Hartung, M, Hibon, P, Ingraham, P, Kalas, P, Konopacky, Q, Maire, J, Marchis, F, Marley, MS, Marois, C, Millar-Blanchaer, M, Morzinski, K, Norton, A, Oppenheimer, R, Palmer, D, Patience, J, Perrin, M, Poyneer, L, Pueyo, L, Rantakyrö, FT, Sadakuni, N, Saddlemyer, L, Savransky, D, Serio, A, Sivaramakrishnan, A, Song, I, Soummer, R, Thomas, S, Wallace, JK, Wiktorowicz, S, and Wolff, S
- Subjects
infrared: general ,instrumentation: adaptive optics ,planetary systems ,stars: individual ,techniques: spectroscopic ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
Using the recently installed Gemini Planet Imager (GPI), we have obtained the first H-band spectrum of the planetary companion to the nearby young star β Pictoris. GPI is designed to image and provide low-resolution spectra of Jupiter-sized, self-luminous planetary companions around young nearby stars. These observations were taken covering the H band (1.65 μm). The spectrum has a resolving power of ∼45 and demonstrates the distinctive triangular shape of a cool substellar object with low surface gravity. Using atmospheric models, we find an effective temperature of 1600-1700K and a surface gravity of log(g) = 3.5-4.5 (cgs units). These values agree well with "hot-start" predictions from planetary evolution models for a gas giant with mass between 10 and 12 MJup and age between 10 and 20 Myr.
- Published
- 2015
39. The VAST Survey - III. The multiplicity of A-type stars within 75 pc
- Author
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De Rosa, R. J., Patience, J., Wilson, P. A., Schneider, A., Wiktorowicz, S. J., Vigan, A., Marois, C., Song, I., Macintosh, B., Graham, J. R., Doyon, R., Bessell, M. S., Thomas, S., and Lai, O.
- Subjects
Astrophysics - Solar and Stellar Astrophysics - Abstract
With a combination of adaptive optics imaging and a multi-epoch common proper motion search, we have conducted a large volume-limited (D $\le$ 75 pc) multiplicity survey of A-type stars, sensitive to companions beyond 30 au. The sample for the Volume-limited A-STar (VAST) survey consists of 435 A-type stars: 363 stars were observed with adaptive optics, 228 stars were searched for wide common proper motion companions and 156 stars were measured with both techniques. The projected separation coverage of the VAST survey extends from 30 to 45,000 au. A total of 137 stellar companions were resolved, including 64 new detections from the VAST survey, and the companion star fraction, projected separation distribution and mass ratio distribution were measured. The separation distribution forms a log-normal distribution similar to the solar-type binary distribution, but with a peak shifted to a significantly wider value of 387 (+132,-98) au. Integrating the fit to the distribution over the 30 to 10,000 au observed range, the companion star fraction for A-type stars is estimated as 33.8%+-2.6%. The mass ratio distribution of closer (<125 au) binaries is distinct from that of wider systems, with a flat distribution for close systems and a distribution that tends towards smaller mass ratios for wider binaries. Combining this result with previous spectroscopic surveys of A-type stars gives an estimate of the total companion star fraction of 68.9%+-7.0%. The most complete assessment of higher order multiples was estimated from the 156-star subset of the VAST sample with both adaptive optics and common proper motion measurements, combined with a literature search for companions, yielding a lower limit on the frequency of single, binary, triple, quadruple and quintuple A-type star systems of 56.4 (-4.0,+3.8), 32.1 (-3.5,+3.9), 9.0 (-1.8,+2.8), 1.9 (-0.6,+1.8) and 0.6 (-0.2,+1.4) per cent, respectively., Comment: 46 pages, 24 figures. Accepted for publication in the Monthly Notices of the Royal Astronomical Society, 7th October 2013
- Published
- 2013
- Full Text
- View/download PDF
40. Final A&T Stages of the Gemini Planet Finder
- Author
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Hartung, M., Macintosh, B., Poyneer, L., Savransky, D., Gavel, D., Palmer, D., Thomas, S., Dillon, D., Chilcote, J., Ingraham, P., Sadakuni, N., Wallace, K., Perin, M. D., Marois, C., Maire, J., Rantakyro, F., Hibon, P., Saddlemyer, L., and Goodsell, S.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The Gemini Planet Imager (GPI) is currently in its final Acceptance & Testing stages. GPI is an XAO system based on a tweeter & woofer architecture (43 & 9 actuators respectively across the pupil), with the tweeter being a Boston Michromachines $64^2$ MEMS device. The XAO AO system is tightly integrated with a Lyot apodizing coronagraph. Acceptance testing started in February 2013 at the University of California, Santa Cruz. A conclusive acceptance review was held in July 2013 and the instrument was found ready for shipment to the Gemini South telescope on Cerro Pachon, Chile. Commissioning at the telescope will take place by the end of 2013, matching the summer window of the southern hemisphere. According to current estimates the 3 year planet finding campaign (890 allocated hours) might discover, image, and spectroscopically analyze 20 to 40 new exo-planets. Final acceptance testing of the integrated instrument can always bring up surprises when using cold chamber and flexure rig installations. The latest developments are reported. Also, we will give an overview of GPI's lab performance, the interplay between subsystems such as the calibration unit (CAL) with the AO bench. We report on-going optimizations on the AO controller loop to filter vibrations and last but not least achieved contrast performance applying speckle nulling. Furthermore, we will give an outlook of possible but challenging future upgrades as the implementation of a predictive controller or exchanging the conventional 48x48 SH WFS with a pyramid. With the ELT era arising, GPI will proof as a versatile and path-finding testbed for AO technologies on the next generation of ground-based telescopes., Comment: 10 pages, 6 figures, submitted to Proceedings of AO4ELT3 conference, Florence, Italy, May 2013
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- 2013
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41. Encéphalopathies métaboliques
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Marois, C., Quirins, M., Hermann, B., Mouri, S., Bouzbib, C., Rudler, M., Thabut, D., and Weiss, N.
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- 2019
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42. The International Deep Planet Survey I. The frequency of wide-orbit massive planets around A-stars
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Vigan, A., Patience, J., Marois, C., Bonavita, M., De Rosa, R. J., Macintosh, B., Song, I., Doyon, R., Zuckerman, B., Lafrenière, D., and Barman, T.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
Breakthrough direct detections of planetary companions orbiting A-type stars confirm the existence of massive planets at relatively large separations, but dedicated surveys are required to estimate the frequency of similar planetary systems. To measure the first estimation of the giant exoplanetary systems frequency at large orbital separation around A-stars, we have conducted a deep-imaging survey of young (8-400 Myr), nearby (19-84 pc) A- and F-stars to search for substellar companions in the 10-300 AU range. The sample of 42 stars combines all A-stars observed in previous AO planet search surveys reported in the literature with new AO observations from VLT/NaCo and Gemini/NIRI. It represents an initial subset of the International Deep Planet Survey (IDPS) sample of stars covering M- to B-stars. The data were obtained with diffraction-limited observations in H- and Ks-band combined with angular differential imaging to suppress the speckle noise of the central stars, resulting in typical 5-sigma detection limits in magnitude difference of 12 mag at 1", 14 mag at 2" and 16 mag at 5" which is sufficient to detect massive planets. A detailed statistical analysis of the survey results is performed using Monte Carlo simulations. Considering the planet detections, we estimate the fraction of A-stars having at least one massive planet (3-14 MJup) in the range 5-320 AU to be inside 5.9-18.8% at 68% confidence, assuming a flat distribution for the mass of the planets. By comparison, the brown dwarf (15-75 MJup) frequency for the sample is 2.0-8.9% at 68% confidence in the range 5-320 AU. Assuming power law distributions for the mass and semimajor axis of the planet population, the AO data are consistent with a declining number of massive planets with increasing orbital radius which is distinct from the rising slope inferred from radial velocity (RV) surveys around evolved A-stars., Comment: 20 pages, 10 figures, 7 tables. Accepted for publication in A&A
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- 2012
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43. Images of a fourth planet orbiting HR 8799
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Marois, C., Zuckerman, B., Konopacky, Q. M., Macintosh, B., and Barman, T.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
High-contrast near-infrared imaging of the nearby star HR 8799 has shown three giant planets. Such images were possible due to the wide orbits (> 25 AU) and youth (< 100 Myr) of the imaged planets, which are still hot and bright as they radiate away gravitational energy acquired during their formation. A major area of contention in the extrasolar planet community is whether outer planets (> 10 AU) more massive than Jupiter form via one-step gravitational instabilities or, rather, via a two-step process involving accretion of a core followed by accumulation of a massive outer envelope composed primarily of hydrogen and helium. Here we report the presence of a fourth planet, interior to and about the same mass as the other three. The system, with this additional planet, represents a challenge for current planet formation models as none of them can explain the in situ formation of all four planets. With its four young giant planets and known cold/warm debris belts, the HR 8799 planetary system is a unique laboratory to study the formation and evolution of giant planets at wide > 10 AU separations., Comment: 20 pages, 4 figures, in press, Nature
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- 2010
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44. Exoplanet Characterization and the Search for Life
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Kasting, J., Traub, W., Roberge, A., Leger, A., Schwartz, A., Wooten, A., Vosteen, A., Lo, A., Brack, A., Tanner, A., Coustenis, A., Lane, B., Oppenheimer, B., Mennesson, B., Lopez, B., Grillmair, C., Beichman, C., Cockell, C., Hanot, C., McCarthy, C., Stark, C., Marois, C., Aime, C., Angerhausen, D., Montes, D., Wilner, D., Defrere, D., Mourard, D., Lin, D., Kite, E., Chassefiere, E., Malbet, F., Tian, F., Westall, F., Illingworth, G., Vasisht, G., Serabyn, G., Marcy, G., Bryden, G., White, G., Laughlin, G., Torres, G., Hammel, H., Ferguson, H., Shibai, H., Rottgering, H., Surdej, J., Wiseman, J., Ge, J., Bally, J., Krist, J., Monnier, J., Trauger, J., Horner, J., Catanzarite, J., Harrington, J., Nishikawa, J., Stapelfeldt, K., von Braun, K., Biazzo, K., Carpenter, K., Balasubramanian, K., Kaltenegger, L., Postman, M., Spaans, M., Turnbull, M., Levine, M., Burchell, M., Ealey, M., Kuchner, M., Marley, M., Dominik, M., Mountain, M., Kenworthy, M., Muterspaugh, M., Shao, M., Zhao, M., Tamura, M., Kasdin, N., Haghighipour, N., Kiang, N., Elias, N., Woolf, N., Mason, N., Absil, O., Guyon, O., Lay, O., Borde, P., Fouque, P., Kalas, P., Lowrance, P., Plavchan, P., Hinz, P., Kervella, P., Chen, P., Akeson, R., Soummer, R., Waters, R., Barry, R., Kendrick, R., Brown, R., Vanderbei, R., Woodruff, R., Danner, R., Allen, R., Polidan, R., Seager, S., MacPhee, S., Hosseini, S., Metchev, S., Kafka, S., Ridgway, S., Rinehart, S., Unwin, S., Shaklan, S., Brummelaar, T. ten, Mazeh, T., Meadows, V., Weiss, W., Danchi, W., Ip, W., and Rabbia, Y.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
Over 300 extrasolar planets (exoplanets) have been detected orbiting nearby stars. We now hope to conduct a census of all planets around nearby stars and to characterize their atmospheres and surfaces with spectroscopy. Rocky planets within their star's habitable zones have the highest priority, as these have the potential to harbor life. Our science goal is to find and characterize all nearby exoplanets; this requires that we measure the mass, orbit, and spectroscopic signature of each one at visible and infrared wavelengths. The techniques for doing this are at hand today. Within the decade we could answer long-standing questions about the evolution and nature of other planetary systems, and we could search for clues as to whether life exists elsewhere in our galactic neighborhood., Comment: 7 pages, 2 figures, submitted to Astro2010 Decadal Review
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- 2009
45. Gemini planet imager spectroscopy of the HR 8799 planets c and d
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Ingraham, P, Marley, MS, Saumon, D, Marois, C, Macintosh, B, Barman, T, Bauman, B, Burrows, A, Chilcote, JK, De Rosa, RJ, Dillon, D, Doyon, R, Dunn, J, Erikson, D, Fitzgerald, MP, Gavel, D, Goodsell, SJ, Graham, JR, Hartung, M, Hibon, P, Kalas, PG, Konopacky, Q, Larkin, JA, Maire, J, Marchis, F, McBride, J, Millar-Blanchaer, M, Morzinski, KM, Norton, A, Oppenheimer, R, Palmer, DW, Patience, J, Perrin, MD, Poyneer, LA, Pueyo, L, Rantakyrö, F, Sadakuni, N, Saddlemyer, L, Savransky, D, Soummer, R, Sivaramakrishnan, A, Song, I, Thomas, S, Kent Wallace, J, Wiktorowicz, SJ, and Wolff, SG
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infrared: planetary systems ,instrumentation: adaptive optics ,instrumentation: high angular resolution ,planets and satellites: atmospheres ,planets and satellites: gaseous planets ,techniques: imaging spectroscopy ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
During the first-light run of the Gemini Planet Imager we obtained K-band spectra of exoplanets HR 8799 c and d. Analysis of the spectra indicates that planet d may be warmer than planet c. Comparisons to recent patchy cloud models and previously obtained observations over multiple wavelengths confirm that thick clouds combined with horizontal variation in the cloud cover generally reproduce the planets' spectral energy distributions. When combined with the 3 to 4 μm photometric data points, the observations provide strong constraints on the atmospheric methane content for both planets. The data also provide further evidence that future modeling efforts must include cloud opacity, possibly including cloud holes, disequilibrium chemistry, and super-solar metallicity.
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- 2014
46. Direct Imaging of Multiple Planets Orbiting the Star HR 8799
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Marois, C., Macintosh, B., Barman, T., Zuckerman, B., Song, I., Patience, J., Lafreniere, D., and Doyon, R.
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Astrophysics - Abstract
Direct imaging of exoplanetary systems is a powerful technique that can reveal Jupiter-like planets in wide orbits, can enable detailed characterization of planetary atmospheres, and is a key step towards imaging Earth-like planets. Imaging detections are challenging due to the combined effect of small angular separation and large luminosity contrast between a planet and its host star. High-contrast observations with the Keck and Gemini telescopes have revealed three planets orbiting the star HR 8799, with projected separations of 24, 38, and 68 astronomical units. Multi-epoch data show counter-clockwise orbital motion for all three imaged planets. The low luminosity of the companions and the estimated age of the system imply planetary masses between 5 and 13 times that of Jupiter. This system resembles a scaled-up version of the outer portion of our Solar System., Comment: 30 pages, 5 figures, Research Article published online in Science Express Nov 13th, 2008
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- 2008
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47. Confidence Level and Sensitivity Limits in High Contrast Imaging
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Marois, C., Lafreniere, D., Macintosh, B., and Doyon, R.
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Astrophysics - Abstract
In long adaptive optics corrected exposures, exoplanet detections are currently limited by speckle noise originating from the telescope and instrument optics, and it is expected that such noise will also limit future high-contrast imaging instruments for both ground and space-based telescopes. Previous theoretical analysis have shown that the time intensity variations of a single speckle follows a modified Rician. It is first demonstrated here that for a circular pupil this temporal intensity distribution also represents the speckle spatial intensity distribution at a fix separation from the point spread function center; this fact is demonstrated using numerical simulations for coronagraphic and non-coronagraphic data. The real statistical distribution of the noise needs to be taken into account explicitly when selecting a detection threshold appropriate for some desired confidence level. In this paper, a technique is described to obtain the pixel intensity distribution of an image and its corresponding confidence level as a function of the detection threshold. Using numerical simulations, it is shown that in the presence of speckles noise, a detection threshold up to three times higher is required to obtain a confidence level equivalent to that at 5sigma for Gaussian noise. The technique is then tested using TRIDENT CFHT and angular differential imaging NIRI Gemini adaptive optics data. It is found that the angular differential imaging technique produces quasi-Gaussian residuals, a remarkable result compared to classical adaptive optic imaging. A power-law is finally derived to predict the 1-3*10^-7 confidence level detection threshold when averaging a partially correlated non-Gaussian noise., Comment: 29 pages, 13 figures, accepted to ApJ
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- 2007
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48. GQ Lup B Visible & Near-Infrared Photometric Analysis
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Marois, C., Macintosh, B., and Barman, T.
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Astrophysics - Abstract
We have re-analyzed archival HST and Subaru data of the recently discovered planetary mass companion (PMC) GQ Lup B. With these we produce the first R and I band photometry of the companion and fit a radius and effective temperature using detailed model atmospheres. We find an effective temperature of 2335 +/- 100K, and a radius of 0.38 +/- 0.05 Rsol and luminosity of log(L/Lsol) = -2.42 +/- 0.07 (at 140pc). Since we fit wavelengths that span most of the emitted radiation from GQ Lup this luminosity estimate is robust, with uncertainty dominated by the distance uncertainty (+/- 50 pc). The radius obtained for 140pc (0.38Rsol) is significantly larger than the one originally derived and larger than model predictions. The mass of the object is much more model-dependent than the radiative properties, but for the GAIA dusty models we find a mass between 10-20 MJup, in the range of the brown dwarf and PMC deuterium burning boundary. Assuming a distance of 140pc, observations fit to 1sigma the Baraffe evolution model for a ~15 MJup brown dwarf. Additionally, the F606W photometric band is significantly overluminous compared to model predictions and other brown dwarfs. Such overluminosity could be explained by a bright Halpha emission from chromospheric activity, interaction with another undetected companion, or accretion. Assuming that GQ Lup B has a bright Halpha emission line, its Halpha emission strength is 10^(-1.71 +/- 0.10) Lbol, significantly larger than field late-type dwarfs. GQ Lup B might be strongly accreting and still be in its formation phase., Comment: 14 pages, 3 figures, ApJL final accepted version
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- 2006
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49. Accurate Astrometry and Photometry of Saturated and Coronagraphic Point Spread Functions
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Marois, C., Lafreniere, D., Macintosh, B., and Doyon, R.
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Astrophysics - Abstract
Accurate astrometry and photometry of saturated and coronagraphic point spread functions (PSFs) are fundamental to both ground- and space-based high contrast imaging projects. For ground-based adaptive optics imaging, differential atmospheric refraction and flexure introduce a small drift of the PSF with time, and seeing and sky transmission variations modify the PSF flux distribution. For space-based imaging, vibrations, thermal fluctuations and pointing jitters can modify the PSF core position and flux. These effects need to be corrected to properly combine the images and obtain optimal signal-to-noise ratios, accurate relative astrometry and photometry of detected objects as well as precise detection limits. Usually, one can easily correct for these effects by using the PSF core, but this is impossible when high dynamic range observing techniques are used, like coronagrahy with a non-transmissive occulting mask, or if the stellar PSF core is saturated. We present a new technique that can solve these issues by using off-axis satellite PSFs produced by a periodic amplitude or phase mask conjugated to a pupil plane. It will be shown that these satellite PSFs track precisely the PSF position, its Strehl ratio and its intensity and can thus be used to register and to flux normalize the PSF. A laboratory experiment is also presented to validate the theory. This approach can be easily implemented in existing adaptive optics instruments and should be considered for future extreme adaptive optics coronagraph instruments and in high-contrast imaging space observatories., Comment: 25 pages, 6 figures, accepted for publication in ApJ
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- 2006
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50. Angular Differential Imaging: a Powerful High-Contrast Imaging Technique
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Marois, C., Lafreniere, D., Doyon, R., Macintosh, B., and Nadeau, D.
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Astrophysics - Abstract
Angular differential imaging is a high-contrast imaging technique that reduces quasi-static speckle noise and facilitates the detection of nearby companions. A sequence of images is acquired with an altitude/azimuth telescope while the instrument field derotator is switched off. This keeps the instrument and telescope optics aligned and allows the field of view to rotate with respect to the instrument. For each image, a reference PSF is constructed from other appropriately-selected images of the same sequence and subtracted to remove quasi-static PSF structure. All residual images are then rotated to align the field and are combined. Observed performances are reported for Gemini North data. It is shown that quasi-static PSF noise can be reduced by a factor \~5 for each image subtraction. The combination of all residuals then provides an additional gain of the order of the square root of the total number of acquired images. A total speckle noise attenuation of 20-50 is obtained for one-hour long observing sequences compared to a single 30s exposure. A PSF noise attenuation of 100 was achieved for two-hour long sequences of images of Vega, reaching a 5-sigma contrast of 20 magnitudes for separations greater than 8". For a 30-minute long sequence, ADI achieves 30 times better signal-to-noise than a classical observation technique. The ADI technique can be used with currently available instruments to search for ~1MJup exoplanets with orbits of radii between 50 and 300 AU around nearby young stars. The possibility of combining the technique with other high-contrast imaging methods is briefly discussed., Comment: 27 pages, 7 figures, accepted for publication in ApJ
- Published
- 2005
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