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97 results on '"Maurel, D"'

1. A dynamical measure of the black hole mass in a quasar 11 billion years ago

Author: Abuter, R., Allouche, F., Amorim, A., Bailet, C., Berdeu, A., Berger, J. -P., Berio, P., Bigioli, A., Boebion, O., Bolzer, M. -L., Bonnet, H., Bourdarot, G., Bourget, P., Brandner, W., Cao, Y., Conzelmann, R., Comin, M., Clénet, Y., Courtney-Barrer, B., Davies, R., Defrère, D., Delboulbé, A., Delplancke-Ströbele, F., Dembet, R., Dexter, J., de Zeeuw, P. T., Drescher, A., Eckart, A., Édouard, C., Eisenhauer, F., Fabricius, M., Feuchtgruber, H., Finger, G., Schreiber, N. M. Förster, Garcia, P., Lopez, R. Garcia, Gao, F., Gendron, E., Genzel, R., Gil, J. P., Gillessen, S., Gomes, T., Gonté, F., Gouvret, C., Guajardo, P., Guieu, S., Hackenberg, W., Haddad, N., Hartl, M., Haubois, X., Haußmann, F., Heißel, G., Henning, Th., Hippler, S., Hönig, S. F., Horrobin, M., Hubin, N., Jacqmart, E., Jocou, L., Kaufer, A., Kervella, P., Kolb, J., Korhonen, H., Lacour, S., Lagarde, S., Lai, O., Lapeyrère, V., Laugier, R., Bouquin, J. -B. Le, Leftley, J., Léna, P., Lewis, S., Liu, D., Lopez, B., Lutz, D., Magnard, Y., Mang, F., Marcotto, A., Maurel, D., Mérand, A., Millour, F., More, N., Netzer, H., Nowacki, H., Nowak, M., Oberti, S., Ott, T., Pallanca, L., Paumard, T., Perraut, K., Perrin, G., Petrov, R., Pfuhl, O., Pourré, N., Rabien, S., Rau, C., Riquelme, M., Robbe-Dubois, S., Rochat, S., Salman, M., Sanchez-Bermudez, J., Santos, D. J. D., Scheithauer, S., Schöller, M., Schubert, J., Schuhler, N., Shangguan, J., Shchekaturov, P., Shimizu, T. T., Sevin, A., Soulez, F., Spang, A., Stadler, E., Sternberg, A., Straubmeier, C., Sturm, E., Sykes, C., Tacconi, L. J., Tristram, K. R. W., Vincent, F., von Fellenberg, S., Uysal, S., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Zins, G., Abuter, R., Allouche, F., Amorim, A., Bailet, C., Berdeu, A., Berger, J. -P., Berio, P., Bigioli, A., Boebion, O., Bolzer, M. -L., Bonnet, H., Bourdarot, G., Bourget, P., Brandner, W., Cao, Y., Conzelmann, R., Comin, M., Clénet, Y., Courtney-Barrer, B., Davies, R., Defrère, D., Delboulbé, A., Delplancke-Ströbele, F., Dembet, R., Dexter, J., de Zeeuw, P. T., Drescher, A., Eckart, A., Édouard, C., Eisenhauer, F., Fabricius, M., Feuchtgruber, H., Finger, G., Schreiber, N. M. Förster, Garcia, P., Lopez, R. Garcia, Gao, F., Gendron, E., Genzel, R., Gil, J. P., Gillessen, S., Gomes, T., Gonté, F., Gouvret, C., Guajardo, P., Guieu, S., Hackenberg, W., Haddad, N., Hartl, M., Haubois, X., Haußmann, F., Heißel, G., Henning, Th., Hippler, S., Hönig, S. F., Horrobin, M., Hubin, N., Jacqmart, E., Jocou, L., Kaufer, A., Kervella, P., Kolb, J., Korhonen, H., Lacour, S., Lagarde, S., Lai, O., Lapeyrère, V., Laugier, R., Bouquin, J. -B. Le, Leftley, J., Léna, P., Lewis, S., Liu, D., Lopez, B., Lutz, D., Magnard, Y., Mang, F., Marcotto, A., Maurel, D., Mérand, A., Millour, F., More, N., Netzer, H., Nowacki, H., Nowak, M., Oberti, S., Ott, T., Pallanca, L., Paumard, T., Perraut, K., Perrin, G., Petrov, R., Pfuhl, O., Pourré, N., Rabien, S., Rau, C., Riquelme, M., Robbe-Dubois, S., Rochat, S., Salman, M., Sanchez-Bermudez, J., Santos, D. J. D., Scheithauer, S., Schöller, M., Schubert, J., Schuhler, N., Shangguan, J., Shchekaturov, P., Shimizu, T. T., Sevin, A., Soulez, F., Spang, A., Stadler, E., Sternberg, A., Straubmeier, C., Sturm, E., Sykes, C., Tacconi, L. J., Tristram, K. R. W., Vincent, F., von Fellenberg, S., Uysal, S., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., and Zins, G.
Abstract: Tight relationships exist in the local universe between the central stellar properties of galaxies and the mass of their supermassive black hole. These suggest galaxies and black holes co-evolve, with the main regulation mechanism being energetic feedback from accretion onto the black hole during its quasar phase. A crucial question is how the relationship between black holes and galaxies evolves with time; a key epoch to probe this relationship is at the peaks of star formation and black hole growth 8-12 billion years ago (redshifts 1-3). Here we report a dynamical measurement of the mass of the black hole in a luminous quasar at a redshift of 2, with a look back time of 11 billion years, by spatially resolving the broad line region. We detect a 40 micro-arcsecond (0.31 pc) spatial offset between the red and blue photocenters of the H$\alpha$ line that traces the velocity gradient of a rotating broad line region. The flux and differential phase spectra are well reproduced by a thick, moderately inclined disk of gas clouds within the sphere of influence of a central black hole with a mass of 3.2x10$^{8}$ solar masses. Molecular gas data reveal a dynamical mass for the host galaxy of 6x10$^{11}$ solar masses, which indicates an under-massive black hole accreting at a super-Eddington rate. This suggests a host galaxy that grew faster than the supermassive black hole, indicating a delay between galaxy and black hole formation for some systems., Comment: 5 pages Main text, 8 figures, 2 tables, to be published in Nature, under embargo until 29 January 2024 16:00 (London)
Published: 2024
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2. Signs of late infall and possible planet formation around DR Tau using VLT/SPHERE and LBTI/LMIRCam

Author: Mesa, D., Ginski, C., Gratton, R., Ertel, S., Wagner, K., Bonavita, M., Fedele, D., Meyer, M., Henning, T., Langlois, M., Garufi, A., Antoniucci, S., Claudi, R., Defrère, D., Desidera, S., Janson, Markus, Pawellek, N., Rigliaco, E., Squicciarini, V., Zurlo, A., Boccaletti, A., Bonnefoy, M., Cantalloube, F., Chauvin, G., Feldt, M., Hagelberg, J., Hugot, E., Lagrange, A.-M., Lazzoni, C., Maurel, D., Perrot, C., Petit, C., Rouan, D., Vigan, A., Mesa, D., Ginski, C., Gratton, R., Ertel, S., Wagner, K., Bonavita, M., Fedele, D., Meyer, M., Henning, T., Langlois, M., Garufi, A., Antoniucci, S., Claudi, R., Defrère, D., Desidera, S., Janson, Markus, Pawellek, N., Rigliaco, E., Squicciarini, V., Zurlo, A., Boccaletti, A., Bonnefoy, M., Cantalloube, F., Chauvin, G., Feldt, M., Hagelberg, J., Hugot, E., Lagrange, A.-M., Lazzoni, C., Maurel, D., Perrot, C., Petit, C., Rouan, D., and Vigan, A.
Abstract: Context. Protoplanetary disks around young stars often contain substructures like rings, gaps, and spirals that could be caused by interactions between the disk and forming planets. Aims. We aim to study the young (1-3 Myr) star DR Tau in the near-infrared and characterize its disk, which was previously resolved through submillimeter interferometry with ALMA, and to search for possible substellar companions embedded into it. Methods. We observed DR Tau with VLT/SPHERE both in polarized light (H broad band) and total intensity (in Y, J, H, and K spectral bands). We also performed L' band observations with LBTI/LMIRCam on the Large Binocular Telescope (LBT). We applied differential imaging techniques to analyze both the polarized data, using dual beam polarization imaging, and the total intensity data, using angular and spectral differential imaging. Results. We found two previously undetected spirals extending north-east and south of the star, respectively. We further detected an arc-like structure north of the star. Finally a bright, compact and elongated structure was detected at a separation of 303 +/- 10 mas and a position angle 21.2 +/- 3.7 degrees, just at the root of the north-east spiral arm. Since this feature is visible both in polarized light and total intensity and has a blue spectrum, it is likely caused by stellar light scattered by dust. Conclusions. The two spiral arms are at different separations from the star, have very different pitch angles, and are separated by an apparent discontinuity, suggesting they might have a different origin. The very open southern spiral arm might be caused by infalling material from late encounters with cloudlets into the formation environment of the star itself. The compact feature could be caused by interaction with a planet in formation still embedded in its dust envelope and it could be responsible for launching the north-east spiral. We estimate a mass of the putative embedded object of the order of few M-Jup.
Published: 2022
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3. First light for GRAVITY Wide Large separation fringe tracking for the Very Large Telescope Interferometer

Author: Abuter, R., Allouche, F., Amorim, A., Bailet, C., Bauboeck, M., Berger, J-P, Berio, P., Bigioli, A., Boebion, O., Bolzer, M. L., Bonnet, H., Bourdarot, G., Bourget, P., Brandner, W., Clenet, Y., Courtney-Barrer, B., Dallilar, Y., Davies, R., Defrere, D., Delboulbe, A., Delplancke, F., Dembet, R., de Zeeuw, P. T., Drescher, A., Eckart, A., Edouard, C., Eisenhauer, F., Fabricius, M., Feuchtgruber, H., Finger, G., Schreiber, N. M. Foerster, Garcia, E., Garcia, P., Gao, F., Gendron, E., Genzel, R., Gil, J. P., Gillessen, S., Gomes, T., Gonte, F., Gouvret, C., Guajardo, P., Guieu, S., Hartl, M., Haubois, X., Haussmann, F., Heissel, G., Henning, Th, Hippler, S., Honig, S., Horrobin, M., Hubin, N., Jacqmart, E., Jochum, L., Jocou, L., Kaufer, A., Kervella, P., Korhonen, H., Kreidberg, L., Lacour, S., Lagarde, S., Lai, O., Lapeyrere, V, Laugier, R., Le Bouquin, J-B, Leftley, J., Lena, P., Lutz, D., Mang, F., Marcotto, A., Maurel, D., Merand, A., Millour, F., More, N., Nowacki, H., Nowak, M., Oberti, S., Ott, T., Pallanca, L., Paumard, T., Perraut, K., Perrin, G., Petrov, R., Pfuhl, O., Pourre, N., Rabien, S., Rau, C., Robbe-Dubois, S., Rochat, S., Salman, M., Scholler, M., Schubert, J., Schuhler, N., Shangguan, J., Shimizu, T., Scheithauer, S., Sevin, A., Soulez, F., Spang, A., Stadler, E., Stadler, J., Straubmeier, C., Sturm, E., Tacconi, L. J., Tristram, K. R. W., Vincent, F., von Fellenberg, S., Uysal, S., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Young, A., Zins, G., Abuter, R., Allouche, F., Amorim, A., Bailet, C., Bauboeck, M., Berger, J-P, Berio, P., Bigioli, A., Boebion, O., Bolzer, M. L., Bonnet, H., Bourdarot, G., Bourget, P., Brandner, W., Clenet, Y., Courtney-Barrer, B., Dallilar, Y., Davies, R., Defrere, D., Delboulbe, A., Delplancke, F., Dembet, R., de Zeeuw, P. T., Drescher, A., Eckart, A., Edouard, C., Eisenhauer, F., Fabricius, M., Feuchtgruber, H., Finger, G., Schreiber, N. M. Foerster, Garcia, E., Garcia, P., Gao, F., Gendron, E., Genzel, R., Gil, J. P., Gillessen, S., Gomes, T., Gonte, F., Gouvret, C., Guajardo, P., Guieu, S., Hartl, M., Haubois, X., Haussmann, F., Heissel, G., Henning, Th, Hippler, S., Honig, S., Horrobin, M., Hubin, N., Jacqmart, E., Jochum, L., Jocou, L., Kaufer, A., Kervella, P., Korhonen, H., Kreidberg, L., Lacour, S., Lagarde, S., Lai, O., Lapeyrere, V, Laugier, R., Le Bouquin, J-B, Leftley, J., Lena, P., Lutz, D., Mang, F., Marcotto, A., Maurel, D., Merand, A., Millour, F., More, N., Nowacki, H., Nowak, M., Oberti, S., Ott, T., Pallanca, L., Paumard, T., Perraut, K., Perrin, G., Petrov, R., Pfuhl, O., Pourre, N., Rabien, S., Rau, C., Robbe-Dubois, S., Rochat, S., Salman, M., Scholler, M., Schubert, J., Schuhler, N., Shangguan, J., Shimizu, T., Scheithauer, S., Sevin, A., Soulez, F., Spang, A., Stadler, E., Stadler, J., Straubmeier, C., Sturm, E., Tacconi, L. J., Tristram, K. R. W., Vincent, F., von Fellenberg, S., Uysal, S., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Young, A., and Zins, G.
Abstract: GRAVITY+ is the upgrade for GRAVITY and the Very Large Telescope Interferometer (VLTI) with wide-separation fringe tracking, new adaptive optics, and laser guide stars on all four 8 m Unit Telescopes (UTs) to enable ever-fainter, all-sky, high-contrast, milliarcsecond interferometry. Here we present the design and first results of the first phase of GRAVITY+, known as GRAVITY Wide. GRAVITY Wide combines the dual-beam capabilities of the VLTI and the GRAVITY instrument to increase the maximum separation between the science target and the reference star from 2 arcseconds with the 8 m UTs up to several 10 arcseconds, limited only by the Earth's turbulent atmosphere. This increases the sky-coverage of GRAVITY by two orders of magnitude, opening up milliarcsecond resolution observations of faint objects and, in particular, the extragalactic sky. The first observations in 2019-2022 include the first infrared interferometry of two redshift z similar to 2 quasars, interferometric imaging of the binary system HD 105913A, and repeat observations of multiple star systems in the Orion Trapezium Cluster. We find the coherence loss between the science object and fringe-tracking reference star well described by the turbulence of the Earth's atmosphere. We confirm that the larger apertures of the UTs result in higher visibilities for a given separation due to the broader overlap of the projected pupils on the sky and provide predictions for visibility loss as a function of separation to be used for future planning.
Published: 2022

4. Upgrading the high contrast imaging facility SPHERE: science drivers and instrument choices

Author: Boccaletti, A., Chauvin, G., Wildi, F., Milli, J., Stadler, E., Diolaiti, E., Gratton, R., Vidal, F., Loupias, M., Langlois, M., Cantalloube, F., N'Diaye, M., Gratadour, D., Ferreira, F., Tallon, M., Mazoyer, J., Segransan, D., Mouillet, D., Beuzit, J. -L., Bonnefoy, M., Galicher, R., Vigan, A., Snellen, I., Feldt, M., Desidera, S., Rousseau, S., Baruffolo, A., Goulas, C., Baudoz, P., Bechet, C., Benisty, M., Bianco, A., Carry, B., Cascone, E., Charnay, B., Choquet, E., Christiaens, V., Cortecchia, F., de Caprio, V., De Rosa, A., Desgrange, C., D'Orazi, V., Douté, S., Frangiamore, M., Gendron, E., Ginski, C., Huby, E., Keller, C., Kulcsár, C., Landman, R., Lagarde, S., Lagadec, E., Lagrange, A. -M., Kasper, M. Lombini M., Ménard, F., Magnard, Y., Malaguti, G., Maurel, D., Mesa, D., Morgante, G., Pantin, E., Pichon, T., Potier, A., Rabou, P., Rochat, S., Terenzi, L., Thiébaut, E., Tallon-Bosc, I., Raynaud, H. -F., Rouan, D., Sevin, A., Schiavone, F., Schreiber, L., Zanutta, A., Boccaletti, A., Chauvin, G., Wildi, F., Milli, J., Stadler, E., Diolaiti, E., Gratton, R., Vidal, F., Loupias, M., Langlois, M., Cantalloube, F., N'Diaye, M., Gratadour, D., Ferreira, F., Tallon, M., Mazoyer, J., Segransan, D., Mouillet, D., Beuzit, J. -L., Bonnefoy, M., Galicher, R., Vigan, A., Snellen, I., Feldt, M., Desidera, S., Rousseau, S., Baruffolo, A., Goulas, C., Baudoz, P., Bechet, C., Benisty, M., Bianco, A., Carry, B., Cascone, E., Charnay, B., Choquet, E., Christiaens, V., Cortecchia, F., de Caprio, V., De Rosa, A., Desgrange, C., D'Orazi, V., Douté, S., Frangiamore, M., Gendron, E., Ginski, C., Huby, E., Keller, C., Kulcsár, C., Landman, R., Lagarde, S., Lagadec, E., Lagrange, A. -M., Kasper, M. Lombini M., Ménard, F., Magnard, Y., Malaguti, G., Maurel, D., Mesa, D., Morgante, G., Pantin, E., Pichon, T., Potier, A., Rabou, P., Rochat, S., Terenzi, L., Thiébaut, E., Tallon-Bosc, I., Raynaud, H. -F., Rouan, D., Sevin, A., Schiavone, F., Schreiber, L., and Zanutta, A.
Abstract: SPHERE+ is a proposed upgrade of the SPHERE instrument at the VLT, which is intended to boost the current performances of detection and characterization for exoplanets and disks. SPHERE+ will also serve as a demonstrator for the future planet finder (PCS) of the European ELT. The main science drivers for SPHERE+ are 1/ to access the bulk of the young giant planet population down to the snow line ($3-10$ au), to bridge the gap with complementary techniques (radial velocity, astrometry); 2/ to observe fainter and redder targets in the youngest ($1-10$\,Myr) associations compared to those observed with SPHERE to directly study the formation of giant planets in their birth environment; 3/ to improve the level of characterization of exoplanetary atmospheres by increasing the spectral resolution in order to break degeneracies in giant planet atmosphere models. Achieving these objectives requires to increase the bandwidth of the xAO system (from $\sim$1 to 3\,kHz) as well as the sensitivity in the infrared (2 to 3\,mag). These features will be brought by a second stage AO system optimized in the infrared with a pyramid wavefront sensor. As a new science instrument, a medium resolution integral field spectrograph will provide a spectral resolution from 1000 to 5000 in the J and H bands. This paper gives an overview of the science drivers, requirements and key instrumental trade-off that were done for SPHERE+ to reach the final selected baseline concept., Comment: To appear in the Proceedings of the SPIE Astronomical Telescopes + Instrumentation (2022), 13 pages, 6 figure
Published: 2022

5. First Light for GRAVITY Wide: Large Separation Fringe Tracking for the Very Large Telescope Interferometer

Author: Collaboration, GRAVITY+, Abuter, R., Allouche, F., Amorim, A., Bailet, C., Bauböck, M., Berger, J. -P., Berio, P., Bigioli, A., Boebion, O., Bolzer, M. L., Bonnet, H., Bourdarot, G., Bourget, P., Brandner, W., Clénet, Y., Courtney-Barrer, B., Dallilar, Y., Davies, R., Defrère, D., Delboulbé, A., Delplancke, F., Dembet, R., de Zeeuw, P. T., Drescher, A., Eckart, A., Édouard, C., Eisenhauer, F., Fabricius, M., Feuchtgruber, H., Finger, G., Schreiber, N. M. Förster, Garcia, E., Garcia, P., Gao, F., Gendron, E., Genzel, R., Gil, J. P., Gillessen, S., Gomes, T., Gonté, F., Gouvret, C., Guajardo, P., Guieu, S., Hartl, M., Haubois, X., Haußmann, F., Heißel, G., Henning, Th., Hippler, S., Hönig, S., Horrobin, M., Hubin, N., Jacqmart, E., Jochum, L., Jocou, L., Kaufer, A., Kervella, P., Korhonen, H., Kreidberg, L., Lacour, S., Lagarde, S., Lai, O., Lapeyrère, V., Laugier, R., Bouquin, J. -B. Le, Leftley, J., Léna, P., Lutz, D., Mang, F., Marcotto, A., Maurel, D., Mérand, A., Millour, F., More, N., Nowacki, H., Nowak, M., Oberti, S., Ott, T., Pallanca, L., Paumard, T., Perraut, K., Perrin, G., Petrov, R., Pfuhl, O., Pourré, N., Rabien, S., Rau, C., Robbe-Dubois, S., Rochat, S., Salman, M., Schöller, M., Schubert, J., Schuhler, N., Shangguan, J., Shimizu, T., Scheithauer, S., Sevin, A., Soulez, F., Spang, A., Stadler, E., Stadler, J., Straubmeier, C., Sturm, E., Tacconi, L. J., Tristram, K. R. W., Vincent, F., von Fellenberg, S., Uysal, S., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Young, A., Zins, G., Collaboration, GRAVITY+, Abuter, R., Allouche, F., Amorim, A., Bailet, C., Bauböck, M., Berger, J. -P., Berio, P., Bigioli, A., Boebion, O., Bolzer, M. L., Bonnet, H., Bourdarot, G., Bourget, P., Brandner, W., Clénet, Y., Courtney-Barrer, B., Dallilar, Y., Davies, R., Defrère, D., Delboulbé, A., Delplancke, F., Dembet, R., de Zeeuw, P. T., Drescher, A., Eckart, A., Édouard, C., Eisenhauer, F., Fabricius, M., Feuchtgruber, H., Finger, G., Schreiber, N. M. Förster, Garcia, E., Garcia, P., Gao, F., Gendron, E., Genzel, R., Gil, J. P., Gillessen, S., Gomes, T., Gonté, F., Gouvret, C., Guajardo, P., Guieu, S., Hartl, M., Haubois, X., Haußmann, F., Heißel, G., Henning, Th., Hippler, S., Hönig, S., Horrobin, M., Hubin, N., Jacqmart, E., Jochum, L., Jocou, L., Kaufer, A., Kervella, P., Korhonen, H., Kreidberg, L., Lacour, S., Lagarde, S., Lai, O., Lapeyrère, V., Laugier, R., Bouquin, J. -B. Le, Leftley, J., Léna, P., Lutz, D., Mang, F., Marcotto, A., Maurel, D., Mérand, A., Millour, F., More, N., Nowacki, H., Nowak, M., Oberti, S., Ott, T., Pallanca, L., Paumard, T., Perraut, K., Perrin, G., Petrov, R., Pfuhl, O., Pourré, N., Rabien, S., Rau, C., Robbe-Dubois, S., Rochat, S., Salman, M., Schöller, M., Schubert, J., Schuhler, N., Shangguan, J., Shimizu, T., Scheithauer, S., Sevin, A., Soulez, F., Spang, A., Stadler, E., Stadler, J., Straubmeier, C., Sturm, E., Tacconi, L. J., Tristram, K. R. W., Vincent, F., von Fellenberg, S., Uysal, S., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Young, A., and Zins, G.
Abstract: GRAVITY+ is the upgrade of GRAVITY and the Very Large Telescope Interferometer (VLTI) with wide-separation fringe tracking, new adaptive optics, and laser guide stars on all four 8~m Unit Telescopes (UTs), for ever fainter, all-sky, high contrast, milliarcsecond interferometry. Here we present the design and first results of the first phase of GRAVITY+, called GRAVITY Wide. GRAVITY Wide combines the dual-beam capabilities of the VLTI and the GRAVITY instrument to increase the maximum separation between the science target and the reference star from 2 arcseconds with the 8 m UTs up to several 10 arcseconds, limited only by the Earth's turbulent atmosphere. This increases the sky-coverage of GRAVITY by two orders of magnitude, opening up milliarcsecond resolution observations of faint objects, and in particular the extragalactic sky. The first observations in 2019 - 2022 include first infrared interferometry of two redshift $z\sim2$ quasars, interferometric imaging on the binary system HD 105913A, and repeated observations of multiple star systems in the Orion Trapezium Cluster. We find the coherence loss between the science object and fringe-tracking reference star well described by the turbulence of the Earth's atmosphere. We confirm that the larger apertures of the UTs result in higher visibilities for a given separation due to larger overlap of the projected pupils on sky and give predictions for visibility loss as a function of separation to be used for future planning., Comment: 15 pages, 12 figures, 5 tables. Accepted by A&A
Published: 2022
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6. Signs of late infall and possible planet formation around DR Tau using VLT/SPHERE and LBTI/LMIRCam

Author: Mesa, D., Ginski, C., Gratton, R., Ertel, S., Wagner, K., Bonavita, M., Fedele, D., Meyer, M., Henning, T., Langlois, M., Garufi, A., Antoniucci, S., Claudi, R., Defrere, D., Desidera, S., Janson, M., Pawellek, N., Rigliaco, E., Squicciarini, V., Zurlo, A., Boccaletti, A., Bonnefoy, M., Cantalloube, F., Chauvin, G., Feldt, M., Hagelberg, J., Hugot, E., Lagrange, A. -M., Lazzoni, C., Maurel, D., Perrot, C., Petit, C., Rouan, D., Vigan, A., Mesa, D., Ginski, C., Gratton, R., Ertel, S., Wagner, K., Bonavita, M., Fedele, D., Meyer, M., Henning, T., Langlois, M., Garufi, A., Antoniucci, S., Claudi, R., Defrere, D., Desidera, S., Janson, M., Pawellek, N., Rigliaco, E., Squicciarini, V., Zurlo, A., Boccaletti, A., Bonnefoy, M., Cantalloube, F., Chauvin, G., Feldt, M., Hagelberg, J., Hugot, E., Lagrange, A. -M., Lazzoni, C., Maurel, D., Perrot, C., Petit, C., Rouan, D., and Vigan, A.
Abstract: Context. Protoplanetary disks around young stars often contain substructures like rings, gaps, and spirals that could be caused by interactions between the disk and forming planets. Aims. We aim to study the young (1-3 Myr) star DR Tau in the near-infrared and characterize its disk, which was previously resolved through sub-millimeter interferometry with ALMA, and to search for possible sub-stellar companions embedded into it. Methods. We observed DR Tau with VLT/SPHERE both in polarized light (H broad band) and total intensity (in Y, J, H, and K spectral bands). We also performed L' band observations with LBTI/LMIRCam on the Large Binocular Telescope (LBT). Results. We found two previously undetected spirals extending north-east and south of the star, respectively. We further detected an arc-like structure north of the star. Finally a bright, compact and elongated structure was detected at separation of 303 +/- 10 mas and position angle 21.2 +/- 3.7 degrees, just at the root of the north-east spiral arm. Since this feature is visible both in polarized light and in total intensity and has a flat spectrum it is likely caused by stellar light scattered by dust. Conclusions. The two spiral arms are at different separation from the star, have very different pitch angles, and are separated by an apparent discontinuity, suggesting they might have a different origin. The very open southern spiral arm might be caused by infalling material from late encounters with cloudlets into the formation environment of the star itself. The compact feature could be caused by interaction with a planet in formation still embedded in its dust envelope and it could be responsible for launching the north-east spiral. We estimate a mass of the putative embedded object of the order of few M_Jup ., Comment: 13 pages, 11 Figures. Accepted for publications on A&A
Published: 2021
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7. TOI-269 b: An eccentric sub-Neptune transiting a M2 dwarf revisited with ExTrA

Author: Cointepas, M., Almenara, J. M., Bonfils, X., Bouchy, F., Astudillo-Defru, N., Murgas, F., Otegi, J. F., Wyttenbach, A., Anderson, D. R., Artigau, E., Martins, B. L. Canto, Charbonneau, D., Collins, K. A., Collins, K. I., Correia, J-J., Curaba, S., Delboulbe, A., Delfosse, X., Diaz, R. F., Dorn, C., Doyon, R., Feautrier, P., Figueira, P., Forveille, T., Gaisne, G., Gan, T., Gluck, L., Helled, R., Hellier, C., Jocou, L., Kern, P., Lafrasse, S., Law, N., Leao, I. C., Lovis, C., Magnard, Y., Mann, A. W., Maurel, D., de Medeiros, J. R., Melo, C., Moulin, T., Pepe, F., Rabou, P., Rochat, S., Rodriguez, D. R., Roux, A., Santos, N. C., Segransan, D., Stadler, E., Ting, E. B., Twicken, J. D., Udry, S., Waalkes, W. C., West, R. G., Wunsche, A., Ziegler, C., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Winn, J., Jenkins, J. M., Cointepas, M., Almenara, J. M., Bonfils, X., Bouchy, F., Astudillo-Defru, N., Murgas, F., Otegi, J. F., Wyttenbach, A., Anderson, D. R., Artigau, E., Martins, B. L. Canto, Charbonneau, D., Collins, K. A., Collins, K. I., Correia, J-J., Curaba, S., Delboulbe, A., Delfosse, X., Diaz, R. F., Dorn, C., Doyon, R., Feautrier, P., Figueira, P., Forveille, T., Gaisne, G., Gan, T., Gluck, L., Helled, R., Hellier, C., Jocou, L., Kern, P., Lafrasse, S., Law, N., Leao, I. C., Lovis, C., Magnard, Y., Mann, A. W., Maurel, D., de Medeiros, J. R., Melo, C., Moulin, T., Pepe, F., Rabou, P., Rochat, S., Rodriguez, D. R., Roux, A., Santos, N. C., Segransan, D., Stadler, E., Ting, E. B., Twicken, J. D., Udry, S., Waalkes, W. C., West, R. G., Wunsche, A., Ziegler, C., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Winn, J., and Jenkins, J. M.
Abstract: We present the confirmation of a new sub-Neptune close to the transition between super-Earths and sub-Neptunes transiting the M2 dwarf TOI- 269 (TIC 220479565, V = 14.4 mag, J = 10.9 mag, Rstar = 0.40 Rsun, Mstar = 0.39 Msun, d = 57 pc). The exoplanet candidate has been identified in multiple TESS sectors, and validated with high-precision spectroscopy from HARPS and ground-based photometric follow-up from ExTrA and LCO-CTIO. We determined mass, radius, and bulk density of the exoplanet by jointly modeling both photometry and radial velocities with juliet. The transiting exoplanet has an orbital period of P = 3.6977104 +- 0.0000037 days, a radius of 2.77 +- 0.12 Rearth, and a mass of 8.8 +- 1.4 Mearth. Since TOI-269 b lies among the best targets of its category for atmospheric characterization, it would be interesting to probe the atmosphere of this exoplanet with transmission spectroscopy in order to compare it to other sub-Neptunes. With an eccentricity e = 0.425+0.082-0.086, TOI-269 b has one of the highest eccentricities of the exoplanets with periods less than 10 days. The star being likely a few Gyr old, this system does not appear to be dynamically young. We surmise TOI-269 b may have acquired its high eccentricity as it migrated inward through planet-planet interactions., Comment: 23 pages, 16 figures, Accepted for publication in A&A
Published: 2021
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8. The SPHERE Infrared Survey for Exoplanets (SHINE): I. Sample Definition and Target Characterization

Author: Desidera, S., Chauvin, G., Bonavita, M., Messina, S., Lecoroller, H., Schmidt, T., Gratton, R., Lazzoni, C., Meyer, M., Schlieder, J., Cheetham, A., Hagelberg, J., Bonnefoy, M., Feldt, M., Lagrange, A. -M., Langlois, M., Vigan, A., Tan, T. G., Hambsch, F. -J., Millward, M., Alcalá, J., Benatti, S., Brandner, W., Carson, J., Covino, E., Delorme, P., D'Orazi, V., Janson, M., Rigliaco, E., Beuzit, J. -L., Biller, B., Boccaletti, A., Dominik, C., Cantalloube, F., Fontanive, C., Galicher, R., Henning, T., Lagadec, E., Ligi, R., Maire, A. -L., Menard, F., Mesa, D., Müller, A., Samland, M., Schmid, H. M., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Asensio-Torres, R., Kopytova, T., Rickman, E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbé, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le Mignant, D., Möller-Nilsson, O., Llored, M., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., Wildi, F., Desidera, S., Chauvin, G., Bonavita, M., Messina, S., Lecoroller, H., Schmidt, T., Gratton, R., Lazzoni, C., Meyer, M., Schlieder, J., Cheetham, A., Hagelberg, J., Bonnefoy, M., Feldt, M., Lagrange, A. -M., Langlois, M., Vigan, A., Tan, T. G., Hambsch, F. -J., Millward, M., Alcalá, J., Benatti, S., Brandner, W., Carson, J., Covino, E., Delorme, P., D'Orazi, V., Janson, M., Rigliaco, E., Beuzit, J. -L., Biller, B., Boccaletti, A., Dominik, C., Cantalloube, F., Fontanive, C., Galicher, R., Henning, T., Lagadec, E., Ligi, R., Maire, A. -L., Menard, F., Mesa, D., Müller, A., Samland, M., Schmid, H. M., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Asensio-Torres, R., Kopytova, T., Rickman, E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbé, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le Mignant, D., Möller-Nilsson, O., Llored, M., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., and Wildi, F.
Abstract: Large surveys with new-generation high-contrast imaging instruments are needed to derive the frequency and properties of exoplanet populations with separations from ~5 to 300 au. A careful assessment of the stellar properties is crucial for a proper understanding of when, where, and how frequently planets form, and how they evolve. The sensitivity of detection limits to stellar age makes this a key parameter for direct imaging surveys. Aims. We describe the SpHere INfrared survey for Exoplanets (SHINE), the largest direct imaging planet-search campaign initiated at the VLT in 2015 in the context of the SPHERE Guaranteed Time Observations of the SPHERE consortium. In this first paper we present the selection and the properties of the complete sample of stars surveyed with SHINE, focusing on the targets observed during the first phase of the survey (from February 2015 to February 2017). This early sample composed of 150 stars is used to perform a preliminary statistical analysis of the SHINE data, deferred to two companion papers presenting the survey performance, main discoveries, and the preliminary statistical constraints set by SHINE. Methods. Based on a large database collecting the stellar properties of all young nearby stars in the solar vicinity (including kinematics, membership to moving groups, isochrones, lithium abundance, rotation, and activity), we selected the original sample of 800 stars that were ranked in order of priority according to their sensitivity for planet detection in direct imaging with SPHERE. The properties of the stars that are part of the early statistical sample wererevisited, including for instance measurements from the Gaia Data Release 2. Rotation periods were derived for the vast majority of the late-type objects exploiting TESS light curves and dedicated photometric observations. Results. The properties of individual targets and of the sample as a whole are presented. © ESO 2021.
Published: 2021

9. The SPHERE infrared survey for exoplanets (SHINE) : III. The demographics of young giant exoplanets below 300 au with SPHERE

Author: Vigan, A., Fontanive, C., Meyer, M., Biller, B., Bonavita, M., Feldt, M., Desidera, S., Marleau, G-D, Emsenhuber, A., Galicher, R., Rice, K., Forgan, D., Mordasini, C., Gratton, R., Le Coroller, H., Maire, A-L, Cantalloube, F., Chauvin, G., Cheetham, A., Hagelberg, J., Lagrange, A-M, Langlois, M., Bonnefoy, M., Beuzit, J-L, Boccaletti, A., D'Orazi, V, Delorme, P., Dominik, C., Henning, Th, Janson, Markus, Lagadec, E., Lazzoni, C., Ligi, R., Menard, F., Mesa, D., Messina, S., Moutou, C., Muller, A., Perrot, C., Samland, Matthias, Schmid, H. M., Schmidt, T., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Abe, L., Antichi, J., Asensio-Torres, R., Baruffolo, A., Baudoz, P., Baudrand, J., Bazzon, A., Blanchard, P., Bohn, A. J., Sevilla, S. Brown, Carbillet, M., Carle, M., Cascone, E., Charton, J., Claudi, R., Costille, A., De Caprio, V, Delboulbe, A., Dohlen, K., Engler, N., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Girard, J. H., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Le Mignant, D., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Moller-Nilsson, O., Mouillet, D., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rickman, E. L., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J-F, Sevin, A., Soenke, C., Stadler, E., Suarez, M., Wahhaj, Z., Weber, L., Wildi, F., Vigan, A., Fontanive, C., Meyer, M., Biller, B., Bonavita, M., Feldt, M., Desidera, S., Marleau, G-D, Emsenhuber, A., Galicher, R., Rice, K., Forgan, D., Mordasini, C., Gratton, R., Le Coroller, H., Maire, A-L, Cantalloube, F., Chauvin, G., Cheetham, A., Hagelberg, J., Lagrange, A-M, Langlois, M., Bonnefoy, M., Beuzit, J-L, Boccaletti, A., D'Orazi, V, Delorme, P., Dominik, C., Henning, Th, Janson, Markus, Lagadec, E., Lazzoni, C., Ligi, R., Menard, F., Mesa, D., Messina, S., Moutou, C., Muller, A., Perrot, C., Samland, Matthias, Schmid, H. M., Schmidt, T., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Abe, L., Antichi, J., Asensio-Torres, R., Baruffolo, A., Baudoz, P., Baudrand, J., Bazzon, A., Blanchard, P., Bohn, A. J., Sevilla, S. Brown, Carbillet, M., Carle, M., Cascone, E., Charton, J., Claudi, R., Costille, A., De Caprio, V, Delboulbe, A., Dohlen, K., Engler, N., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Girard, J. H., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Le Mignant, D., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Moller-Nilsson, O., Mouillet, D., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rickman, E. L., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J-F, Sevin, A., Soenke, C., Stadler, E., Suarez, M., Wahhaj, Z., Weber, L., and Wildi, F.
Abstract: The SpHere INfrared Exoplanet (SHINE) project is a 500-star survey performed with SPHERE on the Very Large Telescope for the purpose of directly detecting new substellar companions and understanding their formation and early evolution. Here we present an initial statistical analysis for a subsample of 150 stars spanning spectral types from B to M that are representative of the full SHINE sample. Our goal is to constrain the frequency of substellar companions with masses between 1 and 75 MJup and semimajor axes between 5 and 300 au. For this purpose, we adopt detection limits as a function of angular separation from the survey data for all stars converted into mass and projected orbital separation using the BEX-COND-hot evolutionary tracks and known distance to each system. Based on the results obtained for each star and on the 13 detections in the sample, we use a Markov chain Monte Carlo tool to compare our observations to two different types of models. The first is a parametric model based on observational constraints, and the second type are numerical models that combine advanced core accretion and gravitational instability planet population synthesis. Using the parametric model, we show that the frequencies of systems with at least one substellar companion are 23.0−9.7+13.5, 5.8−2.8+4.7, and 12.6−7.1+12.9% for BA, FGK, and M stars, respectively. We also demonstrate that a planet-like formation pathway probably dominates the mass range from 1–75 MJup for companions around BA stars, while for M dwarfs, brown dwarf binaries dominate detections. In contrast, a combination of binary star-like and planet-like formation is required to best fit the observations for FGK stars. Using our population model and restricting our sample to FGK stars, we derive a frequency of 5.7−2.8+3.8%, consistent with predictions from the parametric model. More generally, the frequency values that we derive are in excellent agreement with values obtained in previous studies.
Published: 2021
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10. The SPHERE infrared survey for exoplanets (SHINE) I. Sample definition and target characterization

Author: Desidera, S., Chauvin, G., Bonavita, M., Messina, S., LeCoroller, H., Schmidt, T., Gratton, R., Lazzoni, C., Meyer, M., Schlieder, J., Cheetham, A., Hagelberg, J., Bonnefoy, M., Feldt, M., Lagrange, A-M, Langlois, M., Vigan, A., Tan, T. G., Hambsch, F-J, Millward, M., Benatti, S., Brandner, W., Carson, J., Covino, E., Delorme, P., D'Orazi, V, Janson, Markus, Rigliaco, E., Beuzit, J-L, Biller, B., Boccaletti, A., Dominik, C., Cantalloube, F., Fontanive, C., Galicher, R., Henning, Th, Lagadec, E., Ligi, R., Maire, A-L, Menard, F., Mesa, D., Samland, M., Schmid, H. M., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Asensio-Torres, R., Kopytova, T., Rickman, E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., De Caprio, V, Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le Mignant, D., Llored, M., Moulin, T., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J-F, Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., Wildi, F., Desidera, S., Chauvin, G., Bonavita, M., Messina, S., LeCoroller, H., Schmidt, T., Gratton, R., Lazzoni, C., Meyer, M., Schlieder, J., Cheetham, A., Hagelberg, J., Bonnefoy, M., Feldt, M., Lagrange, A-M, Langlois, M., Vigan, A., Tan, T. G., Hambsch, F-J, Millward, M., Benatti, S., Brandner, W., Carson, J., Covino, E., Delorme, P., D'Orazi, V, Janson, Markus, Rigliaco, E., Beuzit, J-L, Biller, B., Boccaletti, A., Dominik, C., Cantalloube, F., Fontanive, C., Galicher, R., Henning, Th, Lagadec, E., Ligi, R., Maire, A-L, Menard, F., Mesa, D., Samland, M., Schmid, H. M., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Asensio-Torres, R., Kopytova, T., Rickman, E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., De Caprio, V, Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le Mignant, D., Llored, M., Moulin, T., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J-F, Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., and Wildi, F.
Abstract: Context. Large surveys with new-generation high-contrast imaging instruments are needed to derive the frequency and properties of exoplanet populations with separations from ~5 to 300 au. A careful assessment of the stellar properties is crucial for a proper understanding of when, where, and how frequently planets form, and how they evolve. The sensitivity of detection limits to stellar age makes this a key parameter for direct imaging surveys. Aims. We describe the SpHere INfrared survey for Exoplanets (SHINE), the largest direct imaging planet-search campaign initiated at the VLT in 2015 in the context of the SPHERE Guaranteed Time Observations of the SPHERE consortium. In this first paper we present the selection and the properties of the complete sample of stars surveyed with SHINE, focusing on the targets observed during the first phase of the survey (from February 2015 to February 2017). This early sample composed of 150 stars is used to perform a preliminary statistical analysis of the SHINE data, deferred to two companion papers presenting the survey performance, main discoveries, and the preliminary statistical constraints set by SHINE. Methods. Based on a large database collecting the stellar properties of all young nearby stars in the solar vicinity (including kinematics, membership to moving groups, isochrones, lithium abundance, rotation, and activity), we selected the original sample of 800 stars that were ranked in order of priority according to their sensitivity for planet detection in direct imaging with SPHERE. The properties of the stars that are part of the early statistical sample wererevisited, including for instance measurements from the Gaia Data Release 2. Rotation periods were derived for the vast majority of the late-type objects exploiting TESS light curves and dedicated photometric observations. Results. The properties of individual targets and of the sample as a whole are presented.
Published: 2021
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11. Signs of late infall and possible planet formation around DR Tau using VLT/SPHERE and LBTI/LMIRCam

Author: Mesa, D., Ginski, C., Gratton, R., Ertel, S., Wagner, K., Bonavita, M., Fedele, D., Meyer, M., Henning, T., Langlois, M., Garufi, A., Antoniucci, S., Claudi, R., Defrere, D., Desidera, S., Janson, M., Pawellek, N., Rigliaco, E., Squicciarini, V., Zurlo, A., Boccaletti, A., Bonnefoy, M., Cantalloube, F., Chauvin, G., Feldt, M., Hagelberg, J., Hugot, E., Lagrange, A. -M., Lazzoni, C., Maurel, D., Perrot, C., Petit, C., Rouan, D., Vigan, A., Mesa, D., Ginski, C., Gratton, R., Ertel, S., Wagner, K., Bonavita, M., Fedele, D., Meyer, M., Henning, T., Langlois, M., Garufi, A., Antoniucci, S., Claudi, R., Defrere, D., Desidera, S., Janson, M., Pawellek, N., Rigliaco, E., Squicciarini, V., Zurlo, A., Boccaletti, A., Bonnefoy, M., Cantalloube, F., Chauvin, G., Feldt, M., Hagelberg, J., Hugot, E., Lagrange, A. -M., Lazzoni, C., Maurel, D., Perrot, C., Petit, C., Rouan, D., and Vigan, A.
Abstract: Context. Protoplanetary disks around young stars often contain substructures like rings, gaps, and spirals that could be caused by interactions between the disk and forming planets. Aims. We aim to study the young (1-3 Myr) star DR Tau in the near-infrared and characterize its disk, which was previously resolved through sub-millimeter interferometry with ALMA, and to search for possible sub-stellar companions embedded into it. Methods. We observed DR Tau with VLT/SPHERE both in polarized light (H broad band) and total intensity (in Y, J, H, and K spectral bands). We also performed L' band observations with LBTI/LMIRCam on the Large Binocular Telescope (LBT). Results. We found two previously undetected spirals extending north-east and south of the star, respectively. We further detected an arc-like structure north of the star. Finally a bright, compact and elongated structure was detected at separation of 303 +/- 10 mas and position angle 21.2 +/- 3.7 degrees, just at the root of the north-east spiral arm. Since this feature is visible both in polarized light and in total intensity and has a flat spectrum it is likely caused by stellar light scattered by dust. Conclusions. The two spiral arms are at different separation from the star, have very different pitch angles, and are separated by an apparent discontinuity, suggesting they might have a different origin. The very open southern spiral arm might be caused by infalling material from late encounters with cloudlets into the formation environment of the star itself. The compact feature could be caused by interaction with a planet in formation still embedded in its dust envelope and it could be responsible for launching the north-east spiral. We estimate a mass of the putative embedded object of the order of few M_Jup ., Comment: 13 pages, 11 Figures. Accepted for publications on A&A
Published: 2021
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12. TOI-269 b: An eccentric sub-Neptune transiting a M2 dwarf revisited with ExTrA

Author: Cointepas, M., Almenara, J. M., Bonfils, X., Bouchy, F., Astudillo-Defru, N., Murgas, F., Otegi, J. F., Wyttenbach, A., Anderson, D. R., Artigau, E., Martins, B. L. Canto, Charbonneau, D., Collins, K. A., Collins, K. I., Correia, J-J., Curaba, S., Delboulbe, A., Delfosse, X., Diaz, R. F., Dorn, C., Doyon, R., Feautrier, P., Figueira, P., Forveille, T., Gaisne, G., Gan, T., Gluck, L., Helled, R., Hellier, C., Jocou, L., Kern, P., Lafrasse, S., Law, N., Leao, I. C., Lovis, C., Magnard, Y., Mann, A. W., Maurel, D., de Medeiros, J. R., Melo, C., Moulin, T., Pepe, F., Rabou, P., Rochat, S., Rodriguez, D. R., Roux, A., Santos, N. C., Segransan, D., Stadler, E., Ting, E. B., Twicken, J. D., Udry, S., Waalkes, W. C., West, R. G., Wunsche, A., Ziegler, C., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Winn, J., Jenkins, J. M., Cointepas, M., Almenara, J. M., Bonfils, X., Bouchy, F., Astudillo-Defru, N., Murgas, F., Otegi, J. F., Wyttenbach, A., Anderson, D. R., Artigau, E., Martins, B. L. Canto, Charbonneau, D., Collins, K. A., Collins, K. I., Correia, J-J., Curaba, S., Delboulbe, A., Delfosse, X., Diaz, R. F., Dorn, C., Doyon, R., Feautrier, P., Figueira, P., Forveille, T., Gaisne, G., Gan, T., Gluck, L., Helled, R., Hellier, C., Jocou, L., Kern, P., Lafrasse, S., Law, N., Leao, I. C., Lovis, C., Magnard, Y., Mann, A. W., Maurel, D., de Medeiros, J. R., Melo, C., Moulin, T., Pepe, F., Rabou, P., Rochat, S., Rodriguez, D. R., Roux, A., Santos, N. C., Segransan, D., Stadler, E., Ting, E. B., Twicken, J. D., Udry, S., Waalkes, W. C., West, R. G., Wunsche, A., Ziegler, C., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Winn, J., and Jenkins, J. M.
Abstract: We present the confirmation of a new sub-Neptune close to the transition between super-Earths and sub-Neptunes transiting the M2 dwarf TOI- 269 (TIC 220479565, V = 14.4 mag, J = 10.9 mag, Rstar = 0.40 Rsun, Mstar = 0.39 Msun, d = 57 pc). The exoplanet candidate has been identified in multiple TESS sectors, and validated with high-precision spectroscopy from HARPS and ground-based photometric follow-up from ExTrA and LCO-CTIO. We determined mass, radius, and bulk density of the exoplanet by jointly modeling both photometry and radial velocities with juliet. The transiting exoplanet has an orbital period of P = 3.6977104 +- 0.0000037 days, a radius of 2.77 +- 0.12 Rearth, and a mass of 8.8 +- 1.4 Mearth. Since TOI-269 b lies among the best targets of its category for atmospheric characterization, it would be interesting to probe the atmosphere of this exoplanet with transmission spectroscopy in order to compare it to other sub-Neptunes. With an eccentricity e = 0.425+0.082-0.086, TOI-269 b has one of the highest eccentricities of the exoplanets with periods less than 10 days. The star being likely a few Gyr old, this system does not appear to be dynamically young. We surmise TOI-269 b may have acquired its high eccentricity as it migrated inward through planet-planet interactions., Comment: 23 pages, 16 figures, Accepted for publication in A&A
Published: 2021
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13. The SPHERE infrared survey for exoplanets (SHINE) -- II. Observations, Data reduction and analysis Detection performances and early-results

Author: Langlois, M., Gratton, R., Lagrange, A. -M., Delorme, P., Boccaletti, A., Bonnefoy, M., Maire, A. -L., Mesa, D., Chauvin, G., Desidera, S., Vigan, A., Cheetham, A., Hagelberg, J., Feldt, M., Meyer, M., Rubini, P., Coroller, H. Le, Cantalloube, F., Biller, B., Bonavita, M., Bhowmik, T., Brandner, W., Daemgen, S., D'Orazi, V., Flasseur, O., Fontanive, C., Galicher, R., Girard, J., Janin-Potiron, P., Janson, M., Keppler, M., Kopytova, T., Lagadec, E., Lannier, J., Lazzoni, C., Ligi, R., Meunier, N., Perreti, A., Perrot, C., Rodet, L., Romero, C., Rouan, D., Samland, M., Salter, G., Sissa, E., Schmidt, T., Zurlo, A., Mouillet, D., Denis, L., Thiebaut, E., Milli, J., Wahhaj, Z., Beuzit, J. -L., Dominik, C., Henning, Th., Menard, F., Muller, A., Schmid, H. M., Turatto, M., Udry, S., Abe, L., Antichi, J., Allard, F., Baruffolo, A., Baudoz, P., Baudrand, J., Bazzon, A., Blanchard, P., Carbillet, M., Carle, M., Cascone, E., Charton, J., Claudi, R., Costille, A., De Caprio, V., Delboulbe, A., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Mignant, D. Le, Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Messina, S., Moller-Nilsson, O., Mugnier, L., Moulin, T., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., Wildi, F., Rickman, E., Langlois, M., Gratton, R., Lagrange, A. -M., Delorme, P., Boccaletti, A., Bonnefoy, M., Maire, A. -L., Mesa, D., Chauvin, G., Desidera, S., Vigan, A., Cheetham, A., Hagelberg, J., Feldt, M., Meyer, M., Rubini, P., Coroller, H. Le, Cantalloube, F., Biller, B., Bonavita, M., Bhowmik, T., Brandner, W., Daemgen, S., D'Orazi, V., Flasseur, O., Fontanive, C., Galicher, R., Girard, J., Janin-Potiron, P., Janson, M., Keppler, M., Kopytova, T., Lagadec, E., Lannier, J., Lazzoni, C., Ligi, R., Meunier, N., Perreti, A., Perrot, C., Rodet, L., Romero, C., Rouan, D., Samland, M., Salter, G., Sissa, E., Schmidt, T., Zurlo, A., Mouillet, D., Denis, L., Thiebaut, E., Milli, J., Wahhaj, Z., Beuzit, J. -L., Dominik, C., Henning, Th., Menard, F., Muller, A., Schmid, H. M., Turatto, M., Udry, S., Abe, L., Antichi, J., Allard, F., Baruffolo, A., Baudoz, P., Baudrand, J., Bazzon, A., Blanchard, P., Carbillet, M., Carle, M., Cascone, E., Charton, J., Claudi, R., Costille, A., De Caprio, V., Delboulbe, A., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Mignant, D. Le, Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Messina, S., Moller-Nilsson, O., Mugnier, L., Moulin, T., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., Wildi, F., and Rickman, E.
Abstract: Over the past decades, direct imaging has confirmed the existence of substellar companions (exoplanets or brown dwarfs) on wide orbits (>10 au) from their host stars. To understand their formation and evolution mechanisms, we have initiated in 2015 the SPHERE infrared survey for exoplanets (SHINE), a systematic direct imaging survey of young, nearby stars to explore their demographics.} {We aim to detect and characterize the population of giant planets and brown dwarfs beyond the snow line around young, nearby stars. Combined with the survey completeness, our observations offer the opportunity to constrain the statistical properties (occurrence, mass and orbital distributions, dependency on the stellar mass) of these young giant planets.} {In this study, we present the observing and data analysis strategy, the ranking process of the detected candidates, and the survey performances for a subsample of 150 stars, which are representative of the full SHINE sample. The observations were conducted in an homogeneous way from February 2015 to February 2017 with the dedicated ground-based VLT/SPHERE instrument equipped with the IFS integral field spectrograph and the IRDIS dual-band imager covering a spectral range between 0.9 and 2.3 $\mu$m. We used coronographic, angular and spectral differential imaging techniques to reach the best detection performances for this study down to the planetary mass regime.}
Published: 2021
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14. The SPHERE infrared survey for exoplanets (SHINE)- I Sample definition and target characterization

Author: Desidera, S., Chauvin, G., Bonavita, M., Messina, S., LeCoroller, H., Schmidt, T., Gratton, R., Lazzoni, C., Meyer, M., Schlieder, J., Cheetham, A., Hagelberg, J., Bonnefoy, M., Feldt, M., Lagrange, A-M., Langlois, M., Vigan, A., Tan, T. G., Hambsch, F. -J., Millward, M., Alcala, J., Benatti, S., Brandner, W., Carson, J., Covino, E., Delorme, P., D'Orazi, V., Janson, M., Rigliaco, E., Beuzit, J. -L., Biller, B., Boccaletti, A., Dominik, C., Cantalloube, F., Fontaniv, C., Galicher, R., Henning, Th., Lagadec, E., Ligi, R., Maire, A-L., Menard, F., Mesa, D., Muller, A., Samland, M., Schmid, H. M., Sissa, E., Turatto, M., Udry, S., Asensio-Torres, A. Zurlo R., Kopytova, T., Rickman, E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbe, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Mignant, D. Le, Moller-Nilsson, O., Llored, M., Moulin, T., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramon, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., Wildi, F., Desidera, S., Chauvin, G., Bonavita, M., Messina, S., LeCoroller, H., Schmidt, T., Gratton, R., Lazzoni, C., Meyer, M., Schlieder, J., Cheetham, A., Hagelberg, J., Bonnefoy, M., Feldt, M., Lagrange, A-M., Langlois, M., Vigan, A., Tan, T. G., Hambsch, F. -J., Millward, M., Alcala, J., Benatti, S., Brandner, W., Carson, J., Covino, E., Delorme, P., D'Orazi, V., Janson, M., Rigliaco, E., Beuzit, J. -L., Biller, B., Boccaletti, A., Dominik, C., Cantalloube, F., Fontaniv, C., Galicher, R., Henning, Th., Lagadec, E., Ligi, R., Maire, A-L., Menard, F., Mesa, D., Muller, A., Samland, M., Schmid, H. M., Sissa, E., Turatto, M., Udry, S., Asensio-Torres, A. Zurlo R., Kopytova, T., Rickman, E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbe, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Mignant, D. Le, Moller-Nilsson, O., Llored, M., Moulin, T., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramon, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., and Wildi, F.
Abstract: Large surveys with new-generation high-contrast imaging instruments are needed to derive the frequency and properties of exoplanet populations with separations from $\sim$5 to 300 AU. A careful assessment of the stellar properties is crucial for a proper understanding of when, where, and how frequently planets form, and how they evolve. The sensitivity of detection limits to stellar age makes this a key parameter for direct imaging surveys. We describe the SpHere INfrared survey for Exoplanets (SHINE), the largest direct imaging planet-search campaign initiated at the VLT in 2015 in the context of the SPHERE Guaranteed Time Observations of the SPHERE consortium. In this first paper we present the selection and the properties of the complete sample of stars surveyed with SHINE, focusing on the targets observed during the first phase of the survey (from February 2015 to February 2017). This early sample composed of 150 stars is used to perform a preliminary statistical analysis of the SHINE data, deferred to two companion papers presenting the survey performance, main discoveries, and the preliminary statistical constraints set by SHINE. Based on a large database collecting the stellar properties of all young nearby stars in the solar vicinity (including kinematics, membership to moving groups, isochrones, lithium abundance, rotation, and activity), we selected the original sample of 800 stars that were ranked in order of priority according to their sensitivity for planet detection in direct imaging with SPHERE. The properties of the stars that are part of the early statistical sample were revisited, including for instance measurements from the GAIA Data Release 2.
Published: 2021
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15. Shadowing and multiple rings in the protoplanetary disk of HD 139614

Author: Muro-Arena, G. A., Benisty, M., Ginski, C., Dominik, C., Facchini, S., Villenave, M., van Boekel, R., Chauvin, G., Garufi, A., Henning, T., Janson, M., Keppler, M., Matter, A., Menard, F., Stolker, T., Zurlo, A., Blanchard, P., Maurel, D., Moeller-Nilsson, O., Petit, C., Roux, A., Sevin, A., Wildi, F., Muro-Arena, G. A., Benisty, M., Ginski, C., Dominik, C., Facchini, S., Villenave, M., van Boekel, R., Chauvin, G., Garufi, A., Henning, T., Janson, M., Keppler, M., Matter, A., Menard, F., Stolker, T., Zurlo, A., Blanchard, P., Maurel, D., Moeller-Nilsson, O., Petit, C., Roux, A., Sevin, A., and Wildi, F.
Abstract: Context. Shadows in scattered light images of protoplanetary disks are a common feature and support the presence of warps or misalignments between disk regions. These warps are possibly caused by an inclined (sub-)stellar companion embedded in the disk. Aims. We aim to study the morphology of the protoplanetary disk around the Herbig Ae star HD 139614 based on the first scattered light observations of this disk, which we model with the radiative transfer code MCMax3D. Methods. We obtained J- and H-band observations that show strong azimuthal asymmetries in polarized scattered light with VLT/SPHERE. In the outer disk, beyond similar to 30 au, a broad shadow spans a range of similar to 240 deg in position angle, in the east. A bright ring at similar to 16 au also shows an azimuthally asymmetric brightness, with the faintest side roughly coincidental with the brightest region of the outer disk. Additionally, two arcs are detected at similar to 34 and similar to 50 au. We created a simple four-zone approximation to a warped disk model of HD 139614 in order to qualitatively reproduce these features. The location and misalignment of the disk components were constrained from the shape and location of the shadows they cast. Results. We find that the shadow on the outer disk covers a range of position angles too wide to be explained by a single inner misaligned component. Our model requires a minimum of two separate misaligned zones - or a continuously warped region - to cast this broad shadow on the outer disk. A small misalignment of similar to 4 degrees between adjacent components can reproduce most of the observed shadow features. Conclusions. Multiple misaligned disk zones, potentially mimicking a warp, can explain the observed broad shadows in the HD 139614 disk. A planetary mass companion in the disk, located on an inclined orbit, could be responsible for such a feature and for the dust-depleted gap responsible for a dip in the SED.
Published: 2020
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16. The SPHERE infrared survey for exoplanets (SHINE). III. The demographics of young giant exoplanets below 300 au with SPHERE

Author: Vigan, A., Fontanive, C., Meyer, M., Biller, B., Bonavita, M., Feldt, M., Desidera, S., Marleau, G. -D., Emsenhuber, A., Galicher, R., Rice, K., Forgan, D., Mordasini, C., Gratton, R., Coroller, H. Le, Maire, A. -L., Cantalloube, F., Chauvin, G., Cheetham, A., Hagelberg, J., Lagrange, A. -M., Langlois, M., Bonnefoy, M., Beuzit, J. -L., Boccaletti, A., D'Orazi, V., Delorme, P., Dominik, C., Henning, Th., Janson, M., Lagadec, E., Lazzoni, C., Ligi, R., Menard, F., Mesa, D., Messina, S., Moutou, C., Müller, A., Perrot, C., Samland, M., Schmid, H. M., Schmidt, T., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Abe, L., Antichi, J., Asensio-Torres, R., Baruffolo, A., Baudoz, P., Baudrand, J., Bazzon, A., Blanchard, P., Bohn, A. J., Sevilla, S. Brown, Carbillet, M., Carle, M., Cascone, E., Charton, J., Claudi, R., Costille, A., De Caprio, V., Delboulbé, A., Dohlen, K., Engler, N., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Girard, J. H., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Mignant, D. Le, Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Möller-Nilsson, O., Mouillet, D., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rickman, E. L., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Wahhaj, Z., Weber, L., Wildi, F., Vigan, A., Fontanive, C., Meyer, M., Biller, B., Bonavita, M., Feldt, M., Desidera, S., Marleau, G. -D., Emsenhuber, A., Galicher, R., Rice, K., Forgan, D., Mordasini, C., Gratton, R., Coroller, H. Le, Maire, A. -L., Cantalloube, F., Chauvin, G., Cheetham, A., Hagelberg, J., Lagrange, A. -M., Langlois, M., Bonnefoy, M., Beuzit, J. -L., Boccaletti, A., D'Orazi, V., Delorme, P., Dominik, C., Henning, Th., Janson, M., Lagadec, E., Lazzoni, C., Ligi, R., Menard, F., Mesa, D., Messina, S., Moutou, C., Müller, A., Perrot, C., Samland, M., Schmid, H. M., Schmidt, T., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Abe, L., Antichi, J., Asensio-Torres, R., Baruffolo, A., Baudoz, P., Baudrand, J., Bazzon, A., Blanchard, P., Bohn, A. J., Sevilla, S. Brown, Carbillet, M., Carle, M., Cascone, E., Charton, J., Claudi, R., Costille, A., De Caprio, V., Delboulbé, A., Dohlen, K., Engler, N., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Girard, J. H., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Mignant, D. Le, Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Möller-Nilsson, O., Mouillet, D., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rickman, E. L., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Wahhaj, Z., Weber, L., and Wildi, F.
Abstract: The SHINE project is a 500-star survey performed with SPHERE on the VLT for the purpose of directly detecting new substellar companions and understanding their formation and early evolution. Here we present an initial statistical analysis for a subsample of 150 stars that are representative of the full SHINE sample. Our goal is to constrain the frequency of substellar companions with masses between 1 and 75 MJup and semimajor axes between 5 and 300 au. We adopt detection limits as a function of angular separation from the survey data for all stars converted into mass and projected orbital separation using the BEX-COND-hot evolutionary tracks and known distance to each system. Based on the results obtained for each star and on the 13 detections in the sample, we use a MCMC tool to compare our observations to two different types of models. The first is a parametric model based on observational constraints, and the second type are numerical models that combine advanced core accretion and gravitational instability planet population synthesis. Using the parametric model, we show that the frequencies of systems with at least one substellar companion are $23.0_{-9.7}^{+13.5}\%$, $5.8_{-2.8}^{+4.7}\%$, and $12.6_{-7.1}^{+12.9}\%$ for BA, FGK, and M stars, respectively. We also demonstrate that a planet-like formation pathway probably dominates the mass range from 1-75 MJup for companions around BA stars, while for M dwarfs, brown dwarf binaries dominate detections. In contrast, a combination of binary star-like and planet-like formation is required to best fit the observations for FGK stars. Using our population model and restricting our sample to FGK stars, we derive a frequency of $5.7_{-2.8}^{+3.8}\%$, consistent with predictions from the parametric model. More generally, the frequency values that we derive are in excellent agreement with values obtained in previous studies., Comment: 24 pages, 14 figures, 3 tables. Accepted for publication in A&A
Published: 2020
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17. The circumstellar environment of EX Lup: the SPHERE and SINFONI views

Author: Rigliaco, E., Gratton, R., Kospal, A., Mesa, D., D'Orazi, V., Abraham, P., Desidera, S., Ginski, C., van Holstein, R. G., Dominik, C., Garufi, A., Henning, T., Menard, F., Zurlo, A., Baruffolo, A., Maurel, D., Blanchard, P., Weber, L., Rigliaco, E., Gratton, R., Kospal, A., Mesa, D., D'Orazi, V., Abraham, P., Desidera, S., Ginski, C., van Holstein, R. G., Dominik, C., Garufi, A., Henning, T., Menard, F., Zurlo, A., Baruffolo, A., Maurel, D., Blanchard, P., and Weber, L.
Abstract: EX Lup is a well-studied T Tauri star that represents the prototype of young eruptive stars EXors. In this paper we analyze new adaptive optics imaging and spectroscopic observations of EX Lup and its circumstellar environment in near-infrared in its quiescent phase. We observed EX Lup with the high contrast imager SPHERE/IRDIS in the dual-beam polarimetric imaging mode to resolve the circumstellar environment in near-infrared scattered light. We complemented these data with earlier SINFONI spectroscopy. We resolve for the first time in scattered light a compact feature around EX Lup azimuthally extending from 280deg to 360deg, and radially extending from 0.3arcsec to 0.55arcsec in the plane of the disk. We explore two different scenarios for the detected emission. One accounting for the emission as coming from the brightened walls of the cavity excavated by the outflow whose presence was suggested by ALMA observations in the J=3-2 line of 12CO. The other accounts for the emission as coming from an inclined disk. We detect for the first time a more extended circumstellar disk in scattered light, which shows that a region between 10 and 30 au is depleted of mum-size grains. We compare the J-, H- and K-band spectra obtained with SINFONI in quiescence with the spectra taken during the outburst, showing that all the emission lines were due to the episodic accretion event. Conclusions. Based on the morphology analysis we favour the scenario in which the scattered light is coming from a circumstellar disk rather than the outflow around EX Lup. We analyze the origin of the observed feature either as coming from a continuous circumstellar disk with a cavity, or from the illuminated wall of the outer disk or from a shadowed disk. Moreover, we discuss what is the origin of the mum-size grains depleted region, exploring the possibility that a sub-stellar companion may be the cause of it., Comment: Accepted for publication by A&A, 10 pages, 8 figures
Published: 2020
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18. The SPHERE infrared survey for exoplanets (SHINE). III. The demographics of young giant exoplanets below 300 au with SPHERE

Author: Vigan, A., Fontanive, C., Meyer, M., Biller, B., Bonavita, M., Feldt, M., Desidera, S., Marleau, G. -D., Emsenhuber, A., Galicher, R., Rice, K., Forgan, D., Mordasini, C., Gratton, R., Coroller, H. Le, Maire, A. -L., Cantalloube, F., Chauvin, G., Cheetham, A., Hagelberg, J., Lagrange, A. -M., Langlois, M., Bonnefoy, M., Beuzit, J. -L., Boccaletti, A., D'Orazi, V., Delorme, P., Dominik, C., Henning, Th., Janson, M., Lagadec, E., Lazzoni, C., Ligi, R., Menard, F., Mesa, D., Messina, S., Moutou, C., Müller, A., Perrot, C., Samland, M., Schmid, H. M., Schmidt, T., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Abe, L., Antichi, J., Asensio-Torres, R., Baruffolo, A., Baudoz, P., Baudrand, J., Bazzon, A., Blanchard, P., Bohn, A. J., Sevilla, S. Brown, Carbillet, M., Carle, M., Cascone, E., Charton, J., Claudi, R., Costille, A., De Caprio, V., Delboulbé, A., Dohlen, K., Engler, N., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Girard, J. H., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Mignant, D. Le, Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Möller-Nilsson, O., Mouillet, D., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rickman, E. L., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Wahhaj, Z., Weber, L., Wildi, F., Vigan, A., Fontanive, C., Meyer, M., Biller, B., Bonavita, M., Feldt, M., Desidera, S., Marleau, G. -D., Emsenhuber, A., Galicher, R., Rice, K., Forgan, D., Mordasini, C., Gratton, R., Coroller, H. Le, Maire, A. -L., Cantalloube, F., Chauvin, G., Cheetham, A., Hagelberg, J., Lagrange, A. -M., Langlois, M., Bonnefoy, M., Beuzit, J. -L., Boccaletti, A., D'Orazi, V., Delorme, P., Dominik, C., Henning, Th., Janson, M., Lagadec, E., Lazzoni, C., Ligi, R., Menard, F., Mesa, D., Messina, S., Moutou, C., Müller, A., Perrot, C., Samland, M., Schmid, H. M., Schmidt, T., Sissa, E., Turatto, M., Udry, S., Zurlo, A., Abe, L., Antichi, J., Asensio-Torres, R., Baruffolo, A., Baudoz, P., Baudrand, J., Bazzon, A., Blanchard, P., Bohn, A. J., Sevilla, S. Brown, Carbillet, M., Carle, M., Cascone, E., Charton, J., Claudi, R., Costille, A., De Caprio, V., Delboulbé, A., Dohlen, K., Engler, N., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Girard, J. H., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Mignant, D. Le, Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Möller-Nilsson, O., Mouillet, D., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rickman, E. L., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Wahhaj, Z., Weber, L., and Wildi, F.
Abstract: The SHINE project is a 500-star survey performed with SPHERE on the VLT for the purpose of directly detecting new substellar companions and understanding their formation and early evolution. Here we present an initial statistical analysis for a subsample of 150 stars that are representative of the full SHINE sample. Our goal is to constrain the frequency of substellar companions with masses between 1 and 75 MJup and semimajor axes between 5 and 300 au. We adopt detection limits as a function of angular separation from the survey data for all stars converted into mass and projected orbital separation using the BEX-COND-hot evolutionary tracks and known distance to each system. Based on the results obtained for each star and on the 13 detections in the sample, we use a MCMC tool to compare our observations to two different types of models. The first is a parametric model based on observational constraints, and the second type are numerical models that combine advanced core accretion and gravitational instability planet population synthesis. Using the parametric model, we show that the frequencies of systems with at least one substellar companion are $23.0_{-9.7}^{+13.5}\%$, $5.8_{-2.8}^{+4.7}\%$, and $12.6_{-7.1}^{+12.9}\%$ for BA, FGK, and M stars, respectively. We also demonstrate that a planet-like formation pathway probably dominates the mass range from 1-75 MJup for companions around BA stars, while for M dwarfs, brown dwarf binaries dominate detections. In contrast, a combination of binary star-like and planet-like formation is required to best fit the observations for FGK stars. Using our population model and restricting our sample to FGK stars, we derive a frequency of $5.7_{-2.8}^{+3.8}\%$, consistent with predictions from the parametric model. More generally, the frequency values that we derive are in excellent agreement with values obtained in previous studies., Comment: 24 pages, 14 figures, 3 tables. Accepted for publication in A&A
Published: 2020
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19. The circumstellar environment of EX Lup: the SPHERE and SINFONI views

Author: Rigliaco, E., Gratton, R., Kospal, A., Mesa, D., D'Orazi, V., Abraham, P., Desidera, S., Ginski, C., van Holstein, R. G., Dominik, C., Garufi, A., Henning, T., Menard, F., Zurlo, A., Baruffolo, A., Maurel, D., Blanchard, P., Weber, L., Rigliaco, E., Gratton, R., Kospal, A., Mesa, D., D'Orazi, V., Abraham, P., Desidera, S., Ginski, C., van Holstein, R. G., Dominik, C., Garufi, A., Henning, T., Menard, F., Zurlo, A., Baruffolo, A., Maurel, D., Blanchard, P., and Weber, L.
Abstract: EX Lup is a well-studied T Tauri star that represents the prototype of young eruptive stars EXors. In this paper we analyze new adaptive optics imaging and spectroscopic observations of EX Lup and its circumstellar environment in near-infrared in its quiescent phase. We observed EX Lup with the high contrast imager SPHERE/IRDIS in the dual-beam polarimetric imaging mode to resolve the circumstellar environment in near-infrared scattered light. We complemented these data with earlier SINFONI spectroscopy. We resolve for the first time in scattered light a compact feature around EX Lup azimuthally extending from 280deg to 360deg, and radially extending from 0.3arcsec to 0.55arcsec in the plane of the disk. We explore two different scenarios for the detected emission. One accounting for the emission as coming from the brightened walls of the cavity excavated by the outflow whose presence was suggested by ALMA observations in the J=3-2 line of 12CO. The other accounts for the emission as coming from an inclined disk. We detect for the first time a more extended circumstellar disk in scattered light, which shows that a region between 10 and 30 au is depleted of mum-size grains. We compare the J-, H- and K-band spectra obtained with SINFONI in quiescence with the spectra taken during the outburst, showing that all the emission lines were due to the episodic accretion event. Conclusions. Based on the morphology analysis we favour the scenario in which the scattered light is coming from a circumstellar disk rather than the outflow around EX Lup. We analyze the origin of the observed feature either as coming from a continuous circumstellar disk with a cavity, or from the illuminated wall of the outer disk or from a shadowed disk. Moreover, we discuss what is the origin of the mum-size grains depleted region, exploring the possibility that a sub-stellar companion may be the cause of it., Comment: Accepted for publication by A&A, 10 pages, 8 figures
Published: 2020
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20. Post-conjunction detection of beta Pictoris b with VLT/SPHERE

Author: Lagrange, A. -M., Boccaletti, A., Langlois, M., Chauvin, G., Gratton, R., Beust, H., Desidera, S., Milli, J., Bonnefoy, M., Cheetham, A., Feldt, M., Meyer, M., Vigan, A., Biller, B., Bonavita, M., Baudino, J. -L., Cantalloube, F., Cudel, M., Daemgen, S., Delorme, P., D'Orazi, V., Girard, J., Fontanive, C., Hagelberg, J., Janson, Markus, Keppler, M., Koypitova, T., Galicher, R., Lannier, J., Le Coroller, H., Ligi, R., Maire, A. -L., Mesa, D., Messina, S., Müeller, A., Peretti, S., Perrot, C., Rouan, D., Salter, G., Samland, M., Schmidt, T., Sissa, E., Zurlo, A., Beuzit, J. -L., Mouillet, D., Dominik, C., Henning, T., Lagadec, E., Ménard, F., Schmid, H. -M., Turatto, M., Udry, S., Bohn, A. J., Charnay, B., Gonzales, C. A. Gomez, Gry, C., Kenworthy, M., Kral, Q., Mordasini, C., Moutou, C., van der Plas, G., Schlieder, J. E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbe, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le Mignant, D., Möller-Nilsson, O., Llored, M., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Szulagyi, J., Wildi, F., Lagrange, A. -M., Boccaletti, A., Langlois, M., Chauvin, G., Gratton, R., Beust, H., Desidera, S., Milli, J., Bonnefoy, M., Cheetham, A., Feldt, M., Meyer, M., Vigan, A., Biller, B., Bonavita, M., Baudino, J. -L., Cantalloube, F., Cudel, M., Daemgen, S., Delorme, P., D'Orazi, V., Girard, J., Fontanive, C., Hagelberg, J., Janson, Markus, Keppler, M., Koypitova, T., Galicher, R., Lannier, J., Le Coroller, H., Ligi, R., Maire, A. -L., Mesa, D., Messina, S., Müeller, A., Peretti, S., Perrot, C., Rouan, D., Salter, G., Samland, M., Schmidt, T., Sissa, E., Zurlo, A., Beuzit, J. -L., Mouillet, D., Dominik, C., Henning, T., Lagadec, E., Ménard, F., Schmid, H. -M., Turatto, M., Udry, S., Bohn, A. J., Charnay, B., Gonzales, C. A. Gomez, Gry, C., Kenworthy, M., Kral, Q., Mordasini, C., Moutou, C., van der Plas, G., Schlieder, J. E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbe, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le Mignant, D., Möller-Nilsson, O., Llored, M., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Szulagyi, J., and Wildi, F.
Abstract: Context. With an orbital distance comparable to that of Saturn in the solar system, beta Pictoris b is the closest (semi-major axis similar or equal to 9 au) exoplanet that has been imaged to orbit a star. Thus it offers unique opportunities for detailed studies of its orbital, physical, and atmospheric properties, and of disk-planet interactions. With the exception of the discovery observations in 2003 with NaCo at the Very Large Telescope (VLT), all following astrometric measurements relative to beta Pictoris have been obtained in the southwestern part of the orbit, which severely limits the determination of the planet's orbital parameters. Aims. We aimed at further constraining beta Pictoris b orbital properties using more data, and, in particular, data taken in the northeastern part of the orbit. Methods. We used SPHERE at the VLT to precisely monitor the orbital motion of beta beta Pictoris b since first light of the instrument in 2014. Results. We were able to monitor the planet until November 2016, when its angular separation became too small (125 mas, i.e., 1.6 au) and prevented further detection. We redetected beta Pictoris b on the northeast side of the disk at a separation of 139 mas and a PA of 30 degrees in September 2018. The planetary orbit is now well constrained. With a semi-major axis (sma) of a = 9.0 +/- 0.5 au (1 sigma), it definitely excludes previously reported possible long orbital periods, and excludes beta Pictoris b as the origin of photometric variations that took place in 1981. We also refine the eccentricity and inclination of the planet. From an instrumental point of view, these data demonstrate that it is possible to detect, if they exist, young massive Jupiters that orbit at less than 2 au from a star that is 20 pc away.
Published: 2019
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21. Shadowing and multiple rings in the protoplanetary disk of HD 139614

Author: Muro-Arena, G. A., Benisty, M., Ginski, C., Dominik, C., Facchini, S., Villenave, M., van Boekel, R., Chauvin, G., Garufi, A., Henning, T., Janson, M., Keppler, M., Matter, A., Ménard, F., Stolker, T., Zurlo, A., Blanchard, P., Maurel, D., Moeller-Nilsson, O., Petit, C., Roux, A., Sevin, A., Wildi, F., Muro-Arena, G. A., Benisty, M., Ginski, C., Dominik, C., Facchini, S., Villenave, M., van Boekel, R., Chauvin, G., Garufi, A., Henning, T., Janson, M., Keppler, M., Matter, A., Ménard, F., Stolker, T., Zurlo, A., Blanchard, P., Maurel, D., Moeller-Nilsson, O., Petit, C., Roux, A., Sevin, A., and Wildi, F.
Abstract: Shadows in scattered light images of protoplanetary disks are a common feature and support the presence of warps or misalignments between disk regions. These warps are possibly due to an inclined (sub-)stellar companion embedded in the disk. We study the morphology of the protoplanetary disk around the Herbig Ae star HD 139614 based on the first scattered light observations of this disk, which we model with the radiative transfer code MCMax3D. We obtained J- and H-band observations in polarized scattered light with VLT/SPHERE that show strong azimuthal asymmetries. In the outer disk, beyond ~30 au, a broad shadow spans a range of ~240{\deg} in position angle, in the East. A bright ring at ~16 au also shows an azimuthally asymmetric brightness, with the faintest side roughly coincidental with the brightest region of the outer disk. Additionally, two arcs are detected at ~34 au and ~50 au. We created a simple 4-zone approximation to a warped disk model of HD 139614 in order to qualitatively reproduce these features. The location and misalignment of the disk components were constrained from the shape and location of the shadows they cast. We find that the shadow on the outer disk covers a range of position angle too wide to be explained by a single inner misaligned component. Our model requires a minimum of two separate misaligned zones -- or a continuously warped region -- to cast this broad shadow on the outer disk. A small misalignment of ~4{\deg} between adjacent components can reproduce most of the observed shadow features. Multiple misaligned disk zones, potentially mimicing a warp, can explain the observed broad shadows in the HD 139614 disk. A planetary mass companion in the disk, located on an inclined orbit, could be responsible for such a feature and for the dust depleted gap responsible for a dip in the SED., Comment: Accepted for publication in A&A
Published: 2019
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22. The polarimetric imaging mode of VLT/SPHERE/IRDIS II: Characterization and correction of instrumental polarization effects

Author: van Holstein, R. G., Girard, J. H., de Boer, J., Snik, F., Milli, J., Stam, D. M., Ginski, C., Mouillet, D., Wahhaj, Z., Schmid, H. M., Keller, C. U., Langlois, M., Dohlen, K., Vigan, A., Pohl, A., Carbillet, M., Fantinel, D., Maurel, D., Origné, A., Petit, C., Ramos, J., Rigal, F., Sevin, A., Boccaletti, A., Coroller, H. Le, Dominik, C., Henning, T., Lagadec, E., Ménard, F., Turatto, M., Udry, S., Chauvin, G., Feldt, M., Beuzit, J. -L., van Holstein, R. G., Girard, J. H., de Boer, J., Snik, F., Milli, J., Stam, D. M., Ginski, C., Mouillet, D., Wahhaj, Z., Schmid, H. M., Keller, C. U., Langlois, M., Dohlen, K., Vigan, A., Pohl, A., Carbillet, M., Fantinel, D., Maurel, D., Origné, A., Petit, C., Ramos, J., Rigal, F., Sevin, A., Boccaletti, A., Coroller, H. Le, Dominik, C., Henning, T., Lagadec, E., Ménard, F., Turatto, M., Udry, S., Chauvin, G., Feldt, M., and Beuzit, J. -L.
Abstract: Context. Circumstellar disks and self-luminous giant exoplanets or companion brown dwarfs can be characterized through direct-imaging polarimetry at near-infrared wavelengths. SPHERE/IRDIS at the Very Large Telescope has the capabilities to perform such measurements, but uncalibrated instrumental polarization effects limit the attainable polarimetric accuracy. Aims. We aim to characterize and correct the instrumental polarization effects of the complete optical system, i.e. the telescope and SPHERE/IRDIS. Methods. We create a detailed Mueller matrix model in the broadband filters Y-, J-, H- and Ks, and calibrate it using measurements with SPHERE's internal light source and observations of two unpolarized stars. We develop a data-reduction method that uses the model to correct for the instrumental polarization effects, and apply it to observations of the circumstellar disk of T Cha. Results. The instrumental polarization is almost exclusively produced by the telescope and SPHERE's first mirror and varies with telescope altitude angle. The crosstalk primarily originates from the image derotator (K-mirror). At some orientations, the derotator causes severe loss of signal (>90% loss in H- and Ks-band) and strongly offsets the angle of linear polarization. With our correction method we reach in all filters a total polarimetric accuracy of <0.1% in the degree of linear polarization and an accuracy of a few degrees in angle of linear polarization. Conclusions. The correction method enables us to accurately measure the polarized intensity and angle of linear polarization of circumstellar disks, and is a vital tool for detecting unresolved (inner) disks and measuring the polarization of substellar companions. We have incorporated the correction method in a highly-automatic end-to-end data-reduction pipeline called IRDAP which is publicly available at https://irdap.readthedocs.io., Comment: 28 pages, 25 figures
Published: 2019
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23. SPHERE: the exoplanet imager for the Very Large Telescope

Author: Beuzit, J. -L., Vigan, A., Mouillet, D., Dohlen, K., Gratton, R., Boccaletti, A., Sauvage, J. -F., Schmid, H. M., Langlois, M., Petit, C., Baruffolo, A., Feldt, M., Milli, J., Wahhaj, Z., Abe, L., Anselmi, U., Antichi, J., Barette, R., Baudrand, J., Baudoz, P., Bazzon, A., Bernardi, P., Blanchard, P., Brast, R., Bruno, P., Buey, T., Carbillet, M., Carle, M., Cascone, E., Chapron, F., Chauvin, G., Charton, J., Claudi, R., Costille, A., De Caprio, V., Delboulbé, A., Desidera, S., Dominik, C., Downing, M., Dupuis, O., Fabron, C., Fantinel, D., Farisato, G., Feautrier, P., Fedrigo, E., Fusco, T., Gigan, P., Ginski, C., Girard, J., Giro, E., Gisler, D., Gluck, L., Gry, C., Henning, T., Hubin, N., Hugot, E., Incorvaia, S., Jaquet, M., Kasper, M., Lagadec, E., Lagrange, A. -M., Coroller, H. Le, Mignant, D. Le, Ruyet, B. Le, Lessio, G., Lizon, J. -L., Llored, M., Lundin, L., Madec, F., Magnard, Y., Marteaud, M., Martinez, P., Maurel, D., Ménard, F., Mesa, D., Möller-Nilsson, O., Moulin, T., Moutou, C., Origné, A., Parisot, J., Pavlov, A., Perret, D., Pragt, J., Puget, P., Rabou, P., Ramos, J., Reess, J. -M., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Saisse, M., Salasnich, B., Santambrogio, E., Scuderi, S., Segransan, D., Sevin, A., Siebenmorgen, R., Soenke, C., Stadler, E., Suarez, M., Tiphène, D., Turatto, M., Udry, S., Vakili, F., Waters, L. B. F. M., Weber, L., Wildi, F., Zins, G., Zurlo, A., Beuzit, J. -L., Vigan, A., Mouillet, D., Dohlen, K., Gratton, R., Boccaletti, A., Sauvage, J. -F., Schmid, H. M., Langlois, M., Petit, C., Baruffolo, A., Feldt, M., Milli, J., Wahhaj, Z., Abe, L., Anselmi, U., Antichi, J., Barette, R., Baudrand, J., Baudoz, P., Bazzon, A., Bernardi, P., Blanchard, P., Brast, R., Bruno, P., Buey, T., Carbillet, M., Carle, M., Cascone, E., Chapron, F., Chauvin, G., Charton, J., Claudi, R., Costille, A., De Caprio, V., Delboulbé, A., Desidera, S., Dominik, C., Downing, M., Dupuis, O., Fabron, C., Fantinel, D., Farisato, G., Feautrier, P., Fedrigo, E., Fusco, T., Gigan, P., Ginski, C., Girard, J., Giro, E., Gisler, D., Gluck, L., Gry, C., Henning, T., Hubin, N., Hugot, E., Incorvaia, S., Jaquet, M., Kasper, M., Lagadec, E., Lagrange, A. -M., Coroller, H. Le, Mignant, D. Le, Ruyet, B. Le, Lessio, G., Lizon, J. -L., Llored, M., Lundin, L., Madec, F., Magnard, Y., Marteaud, M., Martinez, P., Maurel, D., Ménard, F., Mesa, D., Möller-Nilsson, O., Moulin, T., Moutou, C., Origné, A., Parisot, J., Pavlov, A., Perret, D., Pragt, J., Puget, P., Rabou, P., Ramos, J., Reess, J. -M., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Saisse, M., Salasnich, B., Santambrogio, E., Scuderi, S., Segransan, D., Sevin, A., Siebenmorgen, R., Soenke, C., Stadler, E., Suarez, M., Tiphène, D., Turatto, M., Udry, S., Vakili, F., Waters, L. B. F. M., Weber, L., Wildi, F., Zins, G., and Zurlo, A.
Abstract: Observations of circumstellar environments to look for the direct signal of exoplanets and the scattered light from disks has significant instrumental implications. In the past 15 years, major developments in adaptive optics, coronagraphy, optical manufacturing, wavefront sensing and data processing, together with a consistent global system analysis have enabled a new generation of high-contrast imagers and spectrographs on large ground-based telescopes with much better performance. One of the most productive is the Spectro-Polarimetic High contrast imager for Exoplanets REsearch (SPHERE) designed and built for the ESO Very Large Telescope (VLT) in Chile. SPHERE includes an extreme adaptive optics system, a highly stable common path interface, several types of coronagraphs and three science instruments. Two of them, the Integral Field Spectrograph (IFS) and the Infra-Red Dual-band Imager and Spectrograph (IRDIS), are designed to efficiently cover the near-infrared (NIR) range in a single observation for efficient young planet search. The third one, ZIMPOL, is designed for visible (VIR) polarimetric observation to look for the reflected light of exoplanets and the light scattered by debris disks. This suite of three science instruments enables to study circumstellar environments at unprecedented angular resolution both in the visible and the near-infrared. In this work, we present the complete instrument and its on-sky performance after 4 years of operations at the VLT., Comment: Final version accepted for publication in A&A
Published: 2019
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24. Two cold belts in the debris disk around the G-type star NZ Lup

Author: Boccaletti, A., Thébault, P., Pawellek, N., Lagrange, A. -M., Galicher, R., Desidera, S., Milli, J., Kral, Q., Bonnefoy, M., Augereau, J. -C., Maire, A. -L., Henning, T., Beust, H., Rodet, L., Avenhaus, H., Bhowmik, T., Bonavita, M., Chauvin, G., Cheetham, A., Cudel, M., Feldt, M., Gratton, R., Hagelberg, J., Janin-Potiron, P., Langlois, M., Ménard, F., Mesa, D., Meyer, M., Peretti, S., Perrot, C., Schmidt, T., Sissa, E., Vigan, A., Rickman, E., Magnard, Y., Maurel, D., Moeller-Nilsson, O., Perret, D., Sauvage, J. -F., Boccaletti, A., Thébault, P., Pawellek, N., Lagrange, A. -M., Galicher, R., Desidera, S., Milli, J., Kral, Q., Bonnefoy, M., Augereau, J. -C., Maire, A. -L., Henning, T., Beust, H., Rodet, L., Avenhaus, H., Bhowmik, T., Bonavita, M., Chauvin, G., Cheetham, A., Cudel, M., Feldt, M., Gratton, R., Hagelberg, J., Janin-Potiron, P., Langlois, M., Ménard, F., Mesa, D., Meyer, M., Peretti, S., Perrot, C., Schmidt, T., Sissa, E., Vigan, A., Rickman, E., Magnard, Y., Maurel, D., Moeller-Nilsson, O., Perret, D., and Sauvage, J. -F.
Abstract: Planetary systems hold the imprint of the formation and of the evolution of planets especially at young ages, and in particular at the stage when the gas has dissipated leaving mostly secondary dust grains. The dynamical perturbation of planets in the dust distribution can be revealed with high-contrast imaging in a variety of structures. SPHERE, the high-contrast imaging device installed at the VLT, was designed to search for young giant planets in long period, but is also able to resolve fine details of planetary systems at the scale of astronomical units in the scattered-light regime. As a young and nearby star, NZ Lup was observed in the course of the SPHERE survey. A debris disk had been formerly identified with HST/NICMOS. We observed this system in the near-infrared with the camera in narrow and broad band filters and with the integral field spectrograph. High contrasts are achieved by the mean of pupil tracking combined with angular differential imaging algorithms. The high angular resolution provided by SPHERE allows us to reveal a new feature in the disk which is interpreted as a superimposition of two belts of planetesimals located at stellocentric distances of $\sim$85 and $\sim$115\,au, and with a mutual inclination of about 5$\degb$. Despite the very high inclination of the disk with respect to the line of sight, we conclude that the presence of a gap, that is, a void in the dust distribution between the belts, is likely. We discuss the implication of the existence of two belts and their relative inclination with respect to the presence of planets., Comment: accepted in Astronomy and Astrophysics
Published: 2019
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25. Two cold belts in the debris disk around the G-type star NZ Lup

Author: Boccaletti, A., Thébault, P., Pawellek, N., Lagrange, A. -M., Galicher, R., Desidera, S., Milli, J., Kral, Q., Bonnefoy, M., Augereau, J. -C., Maire, A. -L., Henning, T., Beust, H., Rodet, L., Avenhaus, H., Bhowmik, T., Bonavita, M., Chauvin, G., Cheetham, A., Cudel, M., Feldt, M., Gratton, R., Hagelberg, J., Janin-Potiron, P., Langlois, M., Ménard, F., Mesa, D., Meyer, M., Peretti, S., Perrot, C., Schmidt, T., Sissa, E., Vigan, A., Rickman, E., Magnard, Y., Maurel, D., Moeller-Nilsson, O., Perret, D., Sauvage, J. -F., Boccaletti, A., Thébault, P., Pawellek, N., Lagrange, A. -M., Galicher, R., Desidera, S., Milli, J., Kral, Q., Bonnefoy, M., Augereau, J. -C., Maire, A. -L., Henning, T., Beust, H., Rodet, L., Avenhaus, H., Bhowmik, T., Bonavita, M., Chauvin, G., Cheetham, A., Cudel, M., Feldt, M., Gratton, R., Hagelberg, J., Janin-Potiron, P., Langlois, M., Ménard, F., Mesa, D., Meyer, M., Peretti, S., Perrot, C., Schmidt, T., Sissa, E., Vigan, A., Rickman, E., Magnard, Y., Maurel, D., Moeller-Nilsson, O., Perret, D., and Sauvage, J. -F.
Abstract: Planetary systems hold the imprint of the formation and of the evolution of planets especially at young ages, and in particular at the stage when the gas has dissipated leaving mostly secondary dust grains. The dynamical perturbation of planets in the dust distribution can be revealed with high-contrast imaging in a variety of structures. SPHERE, the high-contrast imaging device installed at the VLT, was designed to search for young giant planets in long period, but is also able to resolve fine details of planetary systems at the scale of astronomical units in the scattered-light regime. As a young and nearby star, NZ Lup was observed in the course of the SPHERE survey. A debris disk had been formerly identified with HST/NICMOS. We observed this system in the near-infrared with the camera in narrow and broad band filters and with the integral field spectrograph. High contrasts are achieved by the mean of pupil tracking combined with angular differential imaging algorithms. The high angular resolution provided by SPHERE allows us to reveal a new feature in the disk which is interpreted as a superimposition of two belts of planetesimals located at stellocentric distances of $\sim$85 and $\sim$115\,au, and with a mutual inclination of about 5$\degb$. Despite the very high inclination of the disk with respect to the line of sight, we conclude that the presence of a gap, that is, a void in the dust distribution between the belts, is likely. We discuss the implication of the existence of two belts and their relative inclination with respect to the presence of planets., Comment: accepted in Astronomy and Astrophysics
Published: 2019
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26. SPHERE: the exoplanet imager for the Very Large Telescope

Author: Beuzit, J. -L., Vigan, A., Mouillet, D., Dohlen, K., Gratton, R., Boccaletti, A., Sauvage, J. -F., Schmid, H. M., Langlois, M., Petit, C., Baruffolo, A., Feldt, M., Milli, J., Wahhaj, Z., Abe, L., Anselmi, U., Antichi, J., Barette, R., Baudrand, J., Baudoz, P., Bazzon, A., Bernardi, P., Blanchard, P., Brast, R., Bruno, P., Buey, T., Carbillet, M., Carle, M., Cascone, E., Chapron, F., Chauvin, G., Charton, J., Claudi, R., Costille, A., De Caprio, V., Delboulbé, A., Desidera, S., Dominik, C., Downing, M., Dupuis, O., Fabron, C., Fantinel, D., Farisato, G., Feautrier, P., Fedrigo, E., Fusco, T., Gigan, P., Ginski, C., Girard, J., Giro, E., Gisler, D., Gluck, L., Gry, C., Henning, T., Hubin, N., Hugot, E., Incorvaia, S., Jaquet, M., Kasper, M., Lagadec, E., Lagrange, A. -M., Coroller, H. Le, Mignant, D. Le, Ruyet, B. Le, Lessio, G., Lizon, J. -L., Llored, M., Lundin, L., Madec, F., Magnard, Y., Marteaud, M., Martinez, P., Maurel, D., Ménard, F., Mesa, D., Möller-Nilsson, O., Moulin, T., Moutou, C., Origné, A., Parisot, J., Pavlov, A., Perret, D., Pragt, J., Puget, P., Rabou, P., Ramos, J., Reess, J. -M., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Saisse, M., Salasnich, B., Santambrogio, E., Scuderi, S., Segransan, D., Sevin, A., Siebenmorgen, R., Soenke, C., Stadler, E., Suarez, M., Tiphène, D., Turatto, M., Udry, S., Vakili, F., Waters, L. B. F. M., Weber, L., Wildi, F., Zins, G., Zurlo, A., Beuzit, J. -L., Vigan, A., Mouillet, D., Dohlen, K., Gratton, R., Boccaletti, A., Sauvage, J. -F., Schmid, H. M., Langlois, M., Petit, C., Baruffolo, A., Feldt, M., Milli, J., Wahhaj, Z., Abe, L., Anselmi, U., Antichi, J., Barette, R., Baudrand, J., Baudoz, P., Bazzon, A., Bernardi, P., Blanchard, P., Brast, R., Bruno, P., Buey, T., Carbillet, M., Carle, M., Cascone, E., Chapron, F., Chauvin, G., Charton, J., Claudi, R., Costille, A., De Caprio, V., Delboulbé, A., Desidera, S., Dominik, C., Downing, M., Dupuis, O., Fabron, C., Fantinel, D., Farisato, G., Feautrier, P., Fedrigo, E., Fusco, T., Gigan, P., Ginski, C., Girard, J., Giro, E., Gisler, D., Gluck, L., Gry, C., Henning, T., Hubin, N., Hugot, E., Incorvaia, S., Jaquet, M., Kasper, M., Lagadec, E., Lagrange, A. -M., Coroller, H. Le, Mignant, D. Le, Ruyet, B. Le, Lessio, G., Lizon, J. -L., Llored, M., Lundin, L., Madec, F., Magnard, Y., Marteaud, M., Martinez, P., Maurel, D., Ménard, F., Mesa, D., Möller-Nilsson, O., Moulin, T., Moutou, C., Origné, A., Parisot, J., Pavlov, A., Perret, D., Pragt, J., Puget, P., Rabou, P., Ramos, J., Reess, J. -M., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Saisse, M., Salasnich, B., Santambrogio, E., Scuderi, S., Segransan, D., Sevin, A., Siebenmorgen, R., Soenke, C., Stadler, E., Suarez, M., Tiphène, D., Turatto, M., Udry, S., Vakili, F., Waters, L. B. F. M., Weber, L., Wildi, F., Zins, G., and Zurlo, A.
Abstract: Observations of circumstellar environments to look for the direct signal of exoplanets and the scattered light from disks has significant instrumental implications. In the past 15 years, major developments in adaptive optics, coronagraphy, optical manufacturing, wavefront sensing and data processing, together with a consistent global system analysis have enabled a new generation of high-contrast imagers and spectrographs on large ground-based telescopes with much better performance. One of the most productive is the Spectro-Polarimetic High contrast imager for Exoplanets REsearch (SPHERE) designed and built for the ESO Very Large Telescope (VLT) in Chile. SPHERE includes an extreme adaptive optics system, a highly stable common path interface, several types of coronagraphs and three science instruments. Two of them, the Integral Field Spectrograph (IFS) and the Infra-Red Dual-band Imager and Spectrograph (IRDIS), are designed to efficiently cover the near-infrared (NIR) range in a single observation for efficient young planet search. The third one, ZIMPOL, is designed for visible (VIR) polarimetric observation to look for the reflected light of exoplanets and the light scattered by debris disks. This suite of three science instruments enables to study circumstellar environments at unprecedented angular resolution both in the visible and the near-infrared. In this work, we present the complete instrument and its on-sky performance after 4 years of operations at the VLT., Comment: Final version accepted for publication in A&A
Published: 2019
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27. Shadowing and multiple rings in the protoplanetary disk of HD 139614

Author: Muro-Arena, G. A., Benisty, M., Ginski, C., Dominik, C., Facchini, S., Villenave, M., van Boekel, R., Chauvin, G., Garufi, A., Henning, T., Janson, M., Keppler, M., Matter, A., Ménard, F., Stolker, T., Zurlo, A., Blanchard, P., Maurel, D., Moeller-Nilsson, O., Petit, C., Roux, A., Sevin, A., Wildi, F., Muro-Arena, G. A., Benisty, M., Ginski, C., Dominik, C., Facchini, S., Villenave, M., van Boekel, R., Chauvin, G., Garufi, A., Henning, T., Janson, M., Keppler, M., Matter, A., Ménard, F., Stolker, T., Zurlo, A., Blanchard, P., Maurel, D., Moeller-Nilsson, O., Petit, C., Roux, A., Sevin, A., and Wildi, F.
Abstract: Shadows in scattered light images of protoplanetary disks are a common feature and support the presence of warps or misalignments between disk regions. These warps are possibly due to an inclined (sub-)stellar companion embedded in the disk. We study the morphology of the protoplanetary disk around the Herbig Ae star HD 139614 based on the first scattered light observations of this disk, which we model with the radiative transfer code MCMax3D. We obtained J- and H-band observations in polarized scattered light with VLT/SPHERE that show strong azimuthal asymmetries. In the outer disk, beyond ~30 au, a broad shadow spans a range of ~240{\deg} in position angle, in the East. A bright ring at ~16 au also shows an azimuthally asymmetric brightness, with the faintest side roughly coincidental with the brightest region of the outer disk. Additionally, two arcs are detected at ~34 au and ~50 au. We created a simple 4-zone approximation to a warped disk model of HD 139614 in order to qualitatively reproduce these features. The location and misalignment of the disk components were constrained from the shape and location of the shadows they cast. We find that the shadow on the outer disk covers a range of position angle too wide to be explained by a single inner misaligned component. Our model requires a minimum of two separate misaligned zones -- or a continuously warped region -- to cast this broad shadow on the outer disk. A small misalignment of ~4{\deg} between adjacent components can reproduce most of the observed shadow features. Multiple misaligned disk zones, potentially mimicing a warp, can explain the observed broad shadows in the HD 139614 disk. A planetary mass companion in the disk, located on an inclined orbit, could be responsible for such a feature and for the dust depleted gap responsible for a dip in the SED., Comment: Accepted for publication in A&A
Published: 2019
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28. The polarimetric imaging mode of VLT/SPHERE/IRDIS II: Characterization and correction of instrumental polarization effects

Author: van Holstein, R. G., Girard, J. H., de Boer, J., Snik, F., Milli, J., Stam, D. M., Ginski, C., Mouillet, D., Wahhaj, Z., Schmid, H. M., Keller, C. U., Langlois, M., Dohlen, K., Vigan, A., Pohl, A., Carbillet, M., Fantinel, D., Maurel, D., Origné, A., Petit, C., Ramos, J., Rigal, F., Sevin, A., Boccaletti, A., Coroller, H. Le, Dominik, C., Henning, T., Lagadec, E., Ménard, F., Turatto, M., Udry, S., Chauvin, G., Feldt, M., Beuzit, J. -L., van Holstein, R. G., Girard, J. H., de Boer, J., Snik, F., Milli, J., Stam, D. M., Ginski, C., Mouillet, D., Wahhaj, Z., Schmid, H. M., Keller, C. U., Langlois, M., Dohlen, K., Vigan, A., Pohl, A., Carbillet, M., Fantinel, D., Maurel, D., Origné, A., Petit, C., Ramos, J., Rigal, F., Sevin, A., Boccaletti, A., Coroller, H. Le, Dominik, C., Henning, T., Lagadec, E., Ménard, F., Turatto, M., Udry, S., Chauvin, G., Feldt, M., and Beuzit, J. -L.
Abstract: Context. Circumstellar disks and self-luminous giant exoplanets or companion brown dwarfs can be characterized through direct-imaging polarimetry at near-infrared wavelengths. SPHERE/IRDIS at the Very Large Telescope has the capabilities to perform such measurements, but uncalibrated instrumental polarization effects limit the attainable polarimetric accuracy. Aims. We aim to characterize and correct the instrumental polarization effects of the complete optical system, i.e. the telescope and SPHERE/IRDIS. Methods. We create a detailed Mueller matrix model in the broadband filters Y-, J-, H- and Ks, and calibrate it using measurements with SPHERE's internal light source and observations of two unpolarized stars. We develop a data-reduction method that uses the model to correct for the instrumental polarization effects, and apply it to observations of the circumstellar disk of T Cha. Results. The instrumental polarization is almost exclusively produced by the telescope and SPHERE's first mirror and varies with telescope altitude angle. The crosstalk primarily originates from the image derotator (K-mirror). At some orientations, the derotator causes severe loss of signal (>90% loss in H- and Ks-band) and strongly offsets the angle of linear polarization. With our correction method we reach in all filters a total polarimetric accuracy of <0.1% in the degree of linear polarization and an accuracy of a few degrees in angle of linear polarization. Conclusions. The correction method enables us to accurately measure the polarized intensity and angle of linear polarization of circumstellar disks, and is a vital tool for detecting unresolved (inner) disks and measuring the polarization of substellar companions. We have incorporated the correction method in a highly-automatic end-to-end data-reduction pipeline called IRDAP which is publicly available at https://irdap.readthedocs.io., Comment: 28 pages, 25 figures
Published: 2019
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29. Discovery of a brown dwarf companion to the star HIP 64892

Author: Cheetham, A., Bonnefoy, M., Desidera, S., Langlois, M., Vigan, A., Schmidt, T., Olofsson, J., Chauvin, G., Klahr, H., Gratton, R., D'Orazi, V., Henning, T., Janson, M., Biller, B., Peretti, S., Hagelberg, J., Ségransan, D., Udry, S., Mesa, D., Sissa, E., Kral, Q., Schlieder, J., Maire, A. -L., Mordasini, C., Menard, F., Zurlo, A., Beuzit, J. -L., Feldt, M., Mouillet, D., Meyer, M., Lagrange, A. -M., Boccaletti, A., Keppler, M., Kopytova, T., Ligi, R., Rouan, D., Le, Coroller, H., Dominik, C., Lagadec, E., Turatto, M., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Blanchard, P., Buey, T., Carbillet, M., Carle, M., Cascone, E., Claudi, R., Costille, A., Delboulbé, A., De, Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Giro, E., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le, Mignant, D., Möller-Nilsson, O., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., Wildi, F., Cheetham, A., Bonnefoy, M., Desidera, S., Langlois, M., Vigan, A., Schmidt, T., Olofsson, J., Chauvin, G., Klahr, H., Gratton, R., D'Orazi, V., Henning, T., Janson, M., Biller, B., Peretti, S., Hagelberg, J., Ségransan, D., Udry, S., Mesa, D., Sissa, E., Kral, Q., Schlieder, J., Maire, A. -L., Mordasini, C., Menard, F., Zurlo, A., Beuzit, J. -L., Feldt, M., Mouillet, D., Meyer, M., Lagrange, A. -M., Boccaletti, A., Keppler, M., Kopytova, T., Ligi, R., Rouan, D., Le, Coroller, H., Dominik, C., Lagadec, E., Turatto, M., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Blanchard, P., Buey, T., Carbillet, M., Carle, M., Cascone, E., Claudi, R., Costille, A., Delboulbé, A., De, Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Giro, E., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le, Mignant, D., Möller-Nilsson, O., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., and Wildi, F.
Abstract: We report the discovery of a bright, brown dwarf companion to the star HIP 64892, imaged with VLT/SPHERE during the SHINE exoplanet survey. The host is a B9.5V member of the Lower-Centaurus-Crux subgroup of the Scorpius Centaurus OB association. The measured angular separation of the companion (1.2705 ± 0.0023”) corresponds to a projected distance of 159 ± 12 AU. We observed the target with the dual-band imaging and long-slit spectroscopy modes of the IRDIS imager to obtain its spectral energy distribution (SED) and astrometry. In addition, we reprocessed archival NACO L-band data, from which we also recover the companion. Its SED is consistent with a young (<30 Myr), low surface gravity object with a spectral type of M9γ ± 1. From comparison with the BT-Settl atmospheric models we estimate an effective temperature of Teff = 2600 ± 100 K, and comparison of the companion photometry to the COND evolutionary models yields a mass of ∼29−37 MJ at the estimated age of 16+−157 Myr for the system. The star HIP 64892 is a rare example of an extreme-mass ratio system (q ∼ 0.01) and will be useful for testing models relating to the formation and evolution of such low-mass objects. © ESO 2018
Published: 2018

30. Dynamical masses of M-dwarf binaries in young moving groups I. The case of TWA22 and GJ2060

Author: Rodet, L., Bonnefoy, M., Durkan, Stephen, Beust, H., Lagrange, A. -M., Schlieder, J. E., Janson, Markus, Grandjean, A., Chauvin, G., Messina, S., Maire, A. -L., Brandner, W., Girard, J., Delorme, P., Biller, B., Bergfors, C., Lacour, S., Feldt, M., Henning, T., Boccaletti, A., Le Bouquin, J. -B., Berger, J. -P., Monin, J. -L., Udry, S., Peretti, S., Segransan, D., Allard, F., Homeier, D., Vigan, A., Langlois, M., Hagelberg, J., Menard, F., Bazzon, A., Beuzit, J. -L., Delboulbe, A., Desidera, S., Gratton, R., Lannier, J., Ligi, R., Maurel, D., Mesa, D., Meyer, M., Pavlov, A., Ramos, J., Rigal, R., Roelfsema, R., Salter, G., Samland, M., Schmidt, T., Stadler, E., Weber, L., Rodet, L., Bonnefoy, M., Durkan, Stephen, Beust, H., Lagrange, A. -M., Schlieder, J. E., Janson, Markus, Grandjean, A., Chauvin, G., Messina, S., Maire, A. -L., Brandner, W., Girard, J., Delorme, P., Biller, B., Bergfors, C., Lacour, S., Feldt, M., Henning, T., Boccaletti, A., Le Bouquin, J. -B., Berger, J. -P., Monin, J. -L., Udry, S., Peretti, S., Segransan, D., Allard, F., Homeier, D., Vigan, A., Langlois, M., Hagelberg, J., Menard, F., Bazzon, A., Beuzit, J. -L., Delboulbe, A., Desidera, S., Gratton, R., Lannier, J., Ligi, R., Maurel, D., Mesa, D., Meyer, M., Pavlov, A., Ramos, J., Rigal, R., Roelfsema, R., Salter, G., Samland, M., Schmidt, T., Stadler, E., and Weber, L.
Abstract: Context. Evolutionary models are widely used to infer the mass of stars, brown dwarfs, and giant planets. Their predictions are thought to be less reliable at young ages (<200 Myr) and in the low-mass regime (< 1 M-circle dot). GJ 2060AB and TWA22AB are two rare astrometric M-dwarf binaries, respectively members of the AB Doradus (AB Dor) and Beta Pictoris (beta Pic) moving groups. As their dynamical mass can be measured to within a few years, they can be used to calibrate the evolutionary tracks and set new constraints on the age of young moving groups. Aims. We provide the first dynamical mass measurement of GJ 2060 and a refined measurement of the total mass of TWA22. We also characterize the atmospheric properties of the individual components of GJ 2060 that can be used as inputs to the evolutionary models. Methods. We used NaCo and SPHERE observations at VLT and archival Keck/NIRC2 data to complement the astrometric monitoring of the binaries. We combined the astrometry with new HARPS radial velocities (RVs) and FEROS RVs of GJ 2060. We used a Markov chain MonteCarlo (MCMC) module to estimate posteriors on the orbital parameters and dynamical masses of GJ 2060AB and TWA22AB from the astrometry and RVs. Complementary data obtained with the integral field spectrograph VLT /SINFONI were gathered to extract the individual near-infrared (1.1-2.5 mu m) medium-resolution (R similar to 1500 2000) spectra of GJ 2060A and B. We compared the spectra to those of known objects and to grids of BT-SETTL model spectra to infer the spectral type, bolometric luminosities, and temperatures of those objects. Results. We find a total mass of 0 : 18 +/- 0 : 02 M-circle dot for TWA22, which is in good agreement with model predictions at the age of the fi Pic moving group. We obtain a total mass of 1 : 09 +/- 0 : 10 M-circle dot for GJ 2060. We estimate a spectral type of M1 +/- 0.5, L/L-circle dot = -1.20 +/- 0.05 dex, and T-eff = 3700 +/- 100 K for GJ 2060 A. The B component i
Published: 2018
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31. The GJ 504 system revisited Combining interferometric, radial velocity, and high contrast imaging data

Author: Bonnefoy, M., Perraut, K., Lagrange, A. -M., Delorme, P., Vigan, A., Line, M., Rodet, L., Ginski, C., Mourard, D., Marleau, G. -D., Samland, M., Tremblin, P., Ligi, R., Cantalloube, F., Molliere, P., Charnay, B., Kuzuhara, M., Janson, Markus, Morley, C., Homeier, D., D'Orazi, V., Klahr, H., Mordasini, C., Lavie, B., Baudino, J. -L., Beust, H., Peretti, S., Bartucci, A. Musso, Mesa, D., Bezard, B., Boccaletti, A., Galicher, R., Hagelberg, J., Desidera, S., Biller, B., Maire, A. -L., Allard, F., Borgniet, S., Lannier, J., Meunier, N., Desort, M., Alecian, E., Chauvin, G., Langlois, M., Henning, T., Mugnier, L., Mouillet, D., Gratton, R., Brandt, T., Mc Elwain, M., Beuzit, J. -L., Tamura, M., Hori, Y., Brandner, W., Buenzli, E., Cheetham, A., Cudel, M., Feldt, M., Kasper, M., Keppler, M., Kopytova, T., Meyer, M., Perrot, C., Rouan, D., Salter, G., Schmidt, T., Sissa, E., Zurlo, A., Wildi, F., Blanchard, P., De Caprio, V., Delboulbe, A., Maurel, D., Moulin, T., Pavlov, A., Rabou, P., Ramos, J., Roelfsema, R., Rousset, G., Stadler, E., Rigal, F., Weber, L., Bonnefoy, M., Perraut, K., Lagrange, A. -M., Delorme, P., Vigan, A., Line, M., Rodet, L., Ginski, C., Mourard, D., Marleau, G. -D., Samland, M., Tremblin, P., Ligi, R., Cantalloube, F., Molliere, P., Charnay, B., Kuzuhara, M., Janson, Markus, Morley, C., Homeier, D., D'Orazi, V., Klahr, H., Mordasini, C., Lavie, B., Baudino, J. -L., Beust, H., Peretti, S., Bartucci, A. Musso, Mesa, D., Bezard, B., Boccaletti, A., Galicher, R., Hagelberg, J., Desidera, S., Biller, B., Maire, A. -L., Allard, F., Borgniet, S., Lannier, J., Meunier, N., Desort, M., Alecian, E., Chauvin, G., Langlois, M., Henning, T., Mugnier, L., Mouillet, D., Gratton, R., Brandt, T., Mc Elwain, M., Beuzit, J. -L., Tamura, M., Hori, Y., Brandner, W., Buenzli, E., Cheetham, A., Cudel, M., Feldt, M., Kasper, M., Keppler, M., Kopytova, T., Meyer, M., Perrot, C., Rouan, D., Salter, G., Schmidt, T., Sissa, E., Zurlo, A., Wildi, F., Blanchard, P., De Caprio, V., Delboulbe, A., Maurel, D., Moulin, T., Pavlov, A., Rabou, P., Ramos, J., Roelfsema, R., Rousset, G., Stadler, E., Rigal, F., and Weber, L.
Abstract: Context. The G-type star GJ504A is known to host a 3-35 M-Jup companion whose temperature, mass, and projected separation all contribute to making it a test case for planet formation theories and atmospheric models of giant planets and light brown dwarfs. Aims. We aim at revisiting the system age, architecture, and companion physical and chemical properties using new complementary interferometric, radial-velocity, and high-contrast imaging data. Methods. We used the CHARA interferometer to measure GJ504A's angular diameter and obtained an estimation of its radius in combination with the HIPPARCOS parallax. The radius was compared to evolutionary tracks to infer a new independent age range for the system. We collected dual imaging data with IRDIS on VLT/SPHERE to sample the near-infrared (1.02-2.25 mu m) spectral energy distribution (SED) of the companion. The SED was compared to five independent grids of atmospheric models (petitCODE, Exo-REM, BT-SETTL, Morley et al., and ATMO) to infer the atmospheric parameters of GJ 504b and evaluate model-to-model systematic errors. In addition, we used a specific model grid exploring the effect of different C/O ratios. Contrast limits from 2011 to 2017 were combined with radial velocity data of the host star through the MESS2 tool to define upper limits on the mass of additional companions in the system from 0.01 to 100 au. We used an MCMC fitting tool to constrain the companion's orbital parameters based on the measured astrometry, and dedicated formation models to investigate its origin. Results. We report a radius of 1.35 +/- 0.04 R-circle dot for GJ504A. The radius yields isochronal ages of 21 +/- 2 Myr or 4.0 +/- 1.8 Gyr for the system and line-of-sight stellar rotation axis inclination of 162.4(-4.3)(+3.8) degrees or 18.6(-3.8)(+4.3) degrees. We re-detect the companion in the Y2, Y3, J3, H2, and K1 dual-band images. The complete 1-4 mu m SED shape of GJ504b is best reproduced by T8-T9.5 objects with intermediate ages (&lt
Published: 2018
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32. Discovery of a planetary-mass companion within the gap of the transition disk around PDS 70

Author: Keppler, M., Benisty, M., Mueller, A., Henning, Th., van Boekel, R., Cantalloube, F., Ginski, C., van Holstein, R. G., Maire, A. -L., Pohl, A., Samland, M., Avenhaus, H., Baudino, J. -L., Boccaletti, A., de Boer, J., Bonnefoy, M., Chauvin, G., Desidera, S., Langlois, M., Lazzoni, C., Marleau, G. -D., Mordasini, C., Pawellek, N., Stolker, T., Vigan, A., Zurlo, A., Birnstiel, T., Brandner, W., Feldt, M., Flock, M., Girard, J., Gratton, R., Hagelberg, J., Isella, A., Janson, Markus, Juhasz, A., Kemmer, J., Kral, Q., Lagrange, A. -M., Launhardt, R., Matter, A., Menard, F., Milli, J., Molliere, P., Olofsson, J., Perez, L., Pinilla, P., Pinte, C., Quanz, S. P., Schmidt, T., Udry, S., Wahhaj, Z., Williams, J. P., Buenzli, E., Cudel, M., Dominik, C., Galicher, R., Kasper, M., Lannier, J., Mesa, D., Mouillet, D., Peretti, S., Perrot, C., Salter, G., Sissa, E., Wildi, F., Abe, L., Antichi, J., Augereau, J. -C., Baruffolo, A., Baudoz, P., Bazzon, A., Beuzit, J. -L., Blanchard, P., Brems, S. S., Buey, T., De Caprio, V., Carbillet, M., Carle, M., Cascone, E., Cheetham, A., Claudi, R., Costille, A., Delboulbe, A., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Giro, E., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Le Mignant, D., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Meyer, M., Moeller-Nilsson, O., Moulin, T., Mugnier, L., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramose, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Turatto, M., Weber, L., Keppler, M., Benisty, M., Mueller, A., Henning, Th., van Boekel, R., Cantalloube, F., Ginski, C., van Holstein, R. G., Maire, A. -L., Pohl, A., Samland, M., Avenhaus, H., Baudino, J. -L., Boccaletti, A., de Boer, J., Bonnefoy, M., Chauvin, G., Desidera, S., Langlois, M., Lazzoni, C., Marleau, G. -D., Mordasini, C., Pawellek, N., Stolker, T., Vigan, A., Zurlo, A., Birnstiel, T., Brandner, W., Feldt, M., Flock, M., Girard, J., Gratton, R., Hagelberg, J., Isella, A., Janson, Markus, Juhasz, A., Kemmer, J., Kral, Q., Lagrange, A. -M., Launhardt, R., Matter, A., Menard, F., Milli, J., Molliere, P., Olofsson, J., Perez, L., Pinilla, P., Pinte, C., Quanz, S. P., Schmidt, T., Udry, S., Wahhaj, Z., Williams, J. P., Buenzli, E., Cudel, M., Dominik, C., Galicher, R., Kasper, M., Lannier, J., Mesa, D., Mouillet, D., Peretti, S., Perrot, C., Salter, G., Sissa, E., Wildi, F., Abe, L., Antichi, J., Augereau, J. -C., Baruffolo, A., Baudoz, P., Bazzon, A., Beuzit, J. -L., Blanchard, P., Brems, S. S., Buey, T., De Caprio, V., Carbillet, M., Carle, M., Cascone, E., Cheetham, A., Claudi, R., Costille, A., Delboulbe, A., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Giro, E., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Le Mignant, D., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Meyer, M., Moeller-Nilsson, O., Moulin, T., Mugnier, L., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramose, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Turatto, M., and Weber, L.
Abstract: Context. Young circumstellar disks are the birthplaces of planets. Their study is of prime interest to understand the physical and chemical conditions under which planet formation takes place. Only very few detections of planet candidates within these disks exist, and most of them are currently suspected to be disk features. Aims. In this context, the transition disk around the young star PDS 70 is of particular interest, due to its large gap identified in previous observations, indicative of ongoing planet formation. We aim to search for the presence of an embedded young planet and search for disk structures that may be the result of disk-planet interactions and other evolutionary processes. Methods. We analyse new and archival near-infrared images of the transition disk PDS 70 obtained with the VLT/SPHERE, VLT/NaCo, and Gemini/NICI instruments in polarimetric differential imaging and angular differential imaging modes. Results. We detect a point source within the gap of the disk at about 195 mas (similar to 22 au) projected separation. The detection is confirmed at five different epochs, in three filter bands and using different instruments. The astrometry results in an object of bound nature, with high significance. The comparison of the measured magnitudes and colours to evolutionary tracks suggests that the detection is a companion of planetary mass. The luminosity of the detected object is consistent with that of an L-type dwarf, but its IR colours are redder, possibly indicating the presence of warm surrounding material. Further, we confirm the detection of a large gap of similar to 54 au in size within the disk in our scattered light images, and detect a signal from an inner disk component. We find that its spatial extent is very likely smaller than similar to 17 au in radius, and its position angle is consistent with that of the outer disk. The images of the outer disk show evidence of a complex azimuthal brightness distribution which is different at differ
Published: 2018
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33. VLT/SPHERE astrometric confirmation and orbital analysis of the brown dwarf companion HR 2562 B

Author: Maire, A. -L., Rodet, L., Lazzoni, C., Boccaletti, A., Brandner, W., Galicher, R., Cantalloube, F., Mesa, D., Klahr, H., Beust, H., Chauvin, G., Desidera, S., Janson, Markus, Keppler, M., Olofsson, J., Augereau, J. -C., Daemgen, S., Henning, T., Thebault, P., Bonnefoy, M., Feldt, M., Gratton, R., Lagrange, A. -M., Langlois, M., Meyer, M. R., Vigan, A., D'Orazi, V., Hagelberg, J., Le Coroller, H., Ligi, R., Rouan, D., Samland, M., Schmidt, T., Udry, S., Zurlo, A., Abe, L., Carle, M., Delboulbe, A., Feautrier, P., Magnard, Y., Maurel, D., Moulin, T., Pavlov, A., Perret, D., Petit, C., Ramos, J. R., Rigal, F., Roux, A., Weber, L., Maire, A. -L., Rodet, L., Lazzoni, C., Boccaletti, A., Brandner, W., Galicher, R., Cantalloube, F., Mesa, D., Klahr, H., Beust, H., Chauvin, G., Desidera, S., Janson, Markus, Keppler, M., Olofsson, J., Augereau, J. -C., Daemgen, S., Henning, T., Thebault, P., Bonnefoy, M., Feldt, M., Gratton, R., Lagrange, A. -M., Langlois, M., Meyer, M. R., Vigan, A., D'Orazi, V., Hagelberg, J., Le Coroller, H., Ligi, R., Rouan, D., Samland, M., Schmidt, T., Udry, S., Zurlo, A., Abe, L., Carle, M., Delboulbe, A., Feautrier, P., Magnard, Y., Maurel, D., Moulin, T., Pavlov, A., Perret, D., Petit, C., Ramos, J. R., Rigal, F., Roux, A., and Weber, L.
Abstract: Context. A low-mass brown dwarf has recently been imaged around HR 2562 (HD 50571), a star hosting a debris disk resolved in the far infrared. Interestingly, the companion location is compatible with an orbit coplanar with the disk and interior to the debris belt. This feature makes the system a valuable laboratory to analyze the formation of substellar companions in a circumstellar disk and potential disk-companion dynamical interactions. Aims. We aim to further characterize the orbital motion of HR 2562 B and its interactions with the host star debris disk. Methods. We performed a monitoring of the system over similar to 10 months in 2016 and 2017 with the VLT/SPHERE exoplanet imager. Results. We confirm that the companion is comoving with the star and detect for the first time an orbital motion at high significance, with a current orbital motion projected in the plane of the sky of 25 mas (similar to 0.85 au) per year. No orbital curvature is seen in the measurements. An orbital fit of the SPHERE and literature astrometry of the companion without priors on the orbital plane clearly indicates that its orbit is (quasi-)coplanar with the disk. To further constrain the other orbital parameters, we used empirical laws for a companion chaotic zone validated by N-body simulations to test the orbital solutions that are compatible with the estimated disk cavity size. Non-zero eccentricities (>0.15) are allowed for orbital periods shorter than 100 yr, while only moderate eccentricities up to similar to 0.3 for orbital periods longer than 200 yr are compatible with the disk observations. A comparison of synthetic Herschel images to the real data does not allow us to constrain the upper eccentricity of the companion.
Published: 2018
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34. Discovery of a brown dwarf companion to the star HIP 64892

Author: Cheetham, A., Bonnefoy, M., Desidera, S., Langlois, M., Vigan, A., Schmidt, T., Olofsson, J., Chauvin, G., Klahr, H., Gratton, R., D'Orazi, V., Henning, T., Janson, Markus, Biller, B., Peretti, S., Hagelberg, J., Segransan, D., Udry, S., Mesa, D., Sissa, E., Kral, Q., Schlieder, J., Maire, A. -L., Mordasini, C., Menard, F., Zurlo, A., Beuzit, J. -L., Feldt, M., Mouillet, D., Meyer, M., Lagrange, A. -M., Boccaletti, A., Keppler, M., Kopytova, T., Ligi, R., Rouan, D., Le Coroller, H., Dominik, C., Lagadec, E., Turatto, M., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Blanchard, P., Buey, T., Carbillet, M., Carle, M., Cascone, E., Claudi, R., Costille, A., Delboulbe, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Giro, E., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le Mignant, D., Moeller-Nilsson, O., Moulin, T., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., Wildi, F., Cheetham, A., Bonnefoy, M., Desidera, S., Langlois, M., Vigan, A., Schmidt, T., Olofsson, J., Chauvin, G., Klahr, H., Gratton, R., D'Orazi, V., Henning, T., Janson, Markus, Biller, B., Peretti, S., Hagelberg, J., Segransan, D., Udry, S., Mesa, D., Sissa, E., Kral, Q., Schlieder, J., Maire, A. -L., Mordasini, C., Menard, F., Zurlo, A., Beuzit, J. -L., Feldt, M., Mouillet, D., Meyer, M., Lagrange, A. -M., Boccaletti, A., Keppler, M., Kopytova, T., Ligi, R., Rouan, D., Le Coroller, H., Dominik, C., Lagadec, E., Turatto, M., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Blanchard, P., Buey, T., Carbillet, M., Carle, M., Cascone, E., Claudi, R., Costille, A., Delboulbe, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Giro, E., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Le Mignant, D., Moeller-Nilsson, O., Moulin, T., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., and Wildi, F.
Abstract: We report the discovery of a bright, brown dwarf companion to the star HIP 64892, imaged with VLT/SPHERE during the SHINE exoplanet survey. The host is a B9.5V member of the Lower-Centaurus-Crux subgroup of the Scorpius Centaurus OB association. The measured angular separation of the companion (1.2705 +/- 0.0023) corresponds to a projected distance of 159 +/- 12AU. We observed the target with the dual-band imaging and long-slit spectroscopy modes of the IRDIS imager to obtain its spectral energy distribution (SED) and astrometry. In addition, we reprocessed archival NACO L-band data, from which we also recover the companion. Its SED is consistent with a young (<30 Myr), low surface gravity object with a spectral type of M9 gamma +/- 1. From comparison with the BT-Settl atmospheric models we estimate an effective temperature of T-eff = 2600 +/- 100 K, and comparison of the companion photometry to the COND evolutionary models yields a mass of similar to 29-37 M-J at the estimated age of 16(-7)(+15) Myr for the system. The star HIP 64892 is a rare example of an extreme-mass ratio system (q similar to 0.01) and will be useful for testing models relating to the formation and evolution of such low-mass objects.
Published: 2018
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35. Astrometric and photometric accuracies in high contrast imaging : The SPHERE speckle calibration tool (SpeCal)

Author: Galicher, R., Boccaletti, A., Mesa, D., Delorme, P., Gratton, R., Langlois, M., Lagrange, A. -M., Maire, A. -L., Le Coroller, H., Chauvin, G., Biller, B., Cantalloube, F., Janson, Markus, Lagadec, E., Meunier, N., Vigan, A., Hagelberg, J., Bonnefoy, M., Zurlo, A., Rocha, S., Maurel, D., Jaquet, M., Buey, T., Weber, L., Galicher, R., Boccaletti, A., Mesa, D., Delorme, P., Gratton, R., Langlois, M., Lagrange, A. -M., Maire, A. -L., Le Coroller, H., Chauvin, G., Biller, B., Cantalloube, F., Janson, Markus, Lagadec, E., Meunier, N., Vigan, A., Hagelberg, J., Bonnefoy, M., Zurlo, A., Rocha, S., Maurel, D., Jaquet, M., Buey, T., and Weber, L.
Abstract: Context. The consortium of the Spectro-Polarimetric High-contrast Exoplanet REsearch installed at the Very Large Telescope (SPHERE/VLT) has been operating its guaranteed observation time (260 nights over five years) since February 2015. The main part of this time (200 nights) is dedicated to the detection and characterization of young and giant exoplanets on wide orbits. Aims. The large amount of data must be uniformly processed so that accurate and homogeneous measurements of photometry and astrometry can be obtained for any source in the field. Methods. To complement the European Southern Observatory pipeline, the SPHERE consortium developed a dedicated piece of software to process the data. First, the software corrects for instrumental artifacts. Then, it uses the speckle calibration tool (SpeCal) to minimize the stellar light halo that prevents us from detecting faint sources like exoplanets or circumstellar disks. SpeCal is meant to extract the astrometry and photometry of detected point-like sources (exoplanets, brown dwarfs, or background sources). SpeCal was intensively tested to ensure the consistency of all reduced images (cADI, Loci, TLoci, PCA, and others) for any SPHERE observing strategy (ADI, SDI, ASDI as well as the accuracy of the astrometry and photometry of detected point-like sources. Results. SpeCal is robust, user friendly, and efficient at detecting and characterizing point-like sources in high contrast images. It is used to process all SPHERE data systematically, and its outputs have been used for most of the SPHERE consortium papers to date. SpeCal is also a useful framework to compare different algorithms using various sets of data (different observing modes and conditions). Finally, our tests show that the extracted astrometry and photometry are accurate and not biased.
Published: 2018
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36. New disk discovered with VLT/SPHERE around the M star GSC 07396-00759

Author: Sissa, E., Olofsson, J., Vigan, A., Augereau, J. C., D'Orazi, V., Desidera, S., Gratton, R., Langlois, M., Rigliaco, E., Boccaletti, A., Kral, Q., Lazzoni, C., Mesa, D., Messina, S., Sezestre, E., Thébault, P., Zurlo, A., Bhowmik, T., Bonnefoy, M., Chauvin, G., Feldt, M., Hagelberg, J., Lagrange, A. -M., Janson, Markus, Maire, A. -L., Ménard, F., Schlieder, J., Schmidt, T., Szulágyi, J., Stadler, E., Maurel, D., Delboulbé, A., Feautrier, P., Ramos, J., Rigal, F., Sissa, E., Olofsson, J., Vigan, A., Augereau, J. C., D'Orazi, V., Desidera, S., Gratton, R., Langlois, M., Rigliaco, E., Boccaletti, A., Kral, Q., Lazzoni, C., Mesa, D., Messina, S., Sezestre, E., Thébault, P., Zurlo, A., Bhowmik, T., Bonnefoy, M., Chauvin, G., Feldt, M., Hagelberg, J., Lagrange, A. -M., Janson, Markus, Maire, A. -L., Ménard, F., Schlieder, J., Schmidt, T., Szulágyi, J., Stadler, E., Maurel, D., Delboulbé, A., Feautrier, P., Ramos, J., and Rigal, F.
Abstract: Debris disks are usually detected through the infrared excess over the photospheric level of their host star. The most favorable stars for disk detection are those with spectral types between A and K, while the statistics for debris disks detected around low-mass M-type stars is very low, either because they are rare or because they are more difficult to detect. Terrestrial planets, on the other hand, may be common around M-type stars. Here, we report on the discovery of an extended (likely) debris disk around the M-dwarf GSC 07396-00759. The star is a wide companion of the close accreting binary V4046 Sgr. The system probably is a member of the beta Pictoris Moving Group. We resolve the disk in scattered light, exploiting high-contrast, high-resolution imagery with the two near-infrared subsystems of the VLT/SPHERE instrument, operating in the YJ bands and the H2H3 doublet. The disk is clearly detected up to 1.5 '' (similar to 110 au) from the star and appears as a ring, with an inclination i similar to 83 degrees, and a peak density position at similar to 70 au. The spatial extension of the disk suggests that the dust dynamics is affected by a strong stellar wind, showing similarities with the AU Mic system that has also been resolved with SPHERE. The images show faint asymmetric structures at the widest separation in the northwest side. We also set an upper limit for the presence of giant planets to 2 M-J. Finally, we note that the 2 resolved disks around M-type stars of 30 such stars observed with SPHERE are viewed close to edge-on, suggesting that a significant population of debris disks around M dwarfs could remain undetected because of an unfavorable orientation.
Published: 2018
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37. Post conjunction detection of $\beta$ Pictoris b with VLT/SPHERE

Author: Lagrange, A. -M., Boccaletti, A., Langlois, M., Chauvin, G., Gratton, R., Beust, H., Desidera, S., Milli, J., Bonnefoy, M., Cheetham, A., Feldt, M., Meyer, M., Vigan, A., Biller, B., Bonavita, M., Baudino, J. -L., Cantalloube, F., Cudel, M., Daemgen, S., Delorme, P., D'Orazi, V., Girard, J., Fontanive, C., Hagelberg, J., Janson, M., Keppler, M., Koypitova, T., Galicher, R., Lannier, J., Coroller, H. Le, Ligi, R., Maire, A. -L., Mesa, D., Messina, S., Mueller, A., Peretti, S., Perrot, C., Rouan, D., Salter, G., Samland, M., Schmidt, T., Sissa, E., Zurlo, A., Beuzit, J. -L., Mouillet, D., Dominik, C., Henning, T., Lagadec, E., Menard, F., Schmid, H. -M., Turatto, M., Udry, S., Bohn, A. J., Charnay, B., Gonzales, C. A. Gomez, Gry, C., Kenworthy, M., Kral, Q., Mordasini, C., Moutou, C., van der Plas, G., Schlieder, J. E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbe, A., de Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Mignant, D. Le, Moller-Nilsson, O., Llored, M., Moulin, T., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Szulagyi, J., Wildi, F., Lagrange, A. -M., Boccaletti, A., Langlois, M., Chauvin, G., Gratton, R., Beust, H., Desidera, S., Milli, J., Bonnefoy, M., Cheetham, A., Feldt, M., Meyer, M., Vigan, A., Biller, B., Bonavita, M., Baudino, J. -L., Cantalloube, F., Cudel, M., Daemgen, S., Delorme, P., D'Orazi, V., Girard, J., Fontanive, C., Hagelberg, J., Janson, M., Keppler, M., Koypitova, T., Galicher, R., Lannier, J., Coroller, H. Le, Ligi, R., Maire, A. -L., Mesa, D., Messina, S., Mueller, A., Peretti, S., Perrot, C., Rouan, D., Salter, G., Samland, M., Schmidt, T., Sissa, E., Zurlo, A., Beuzit, J. -L., Mouillet, D., Dominik, C., Henning, T., Lagadec, E., Menard, F., Schmid, H. -M., Turatto, M., Udry, S., Bohn, A. J., Charnay, B., Gonzales, C. A. Gomez, Gry, C., Kenworthy, M., Kral, Q., Mordasini, C., Moutou, C., van der Plas, G., Schlieder, J. E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbe, A., de Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Mignant, D. Le, Moller-Nilsson, O., Llored, M., Moulin, T., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Szulagyi, J., and Wildi, F.
Abstract: With an orbital distance comparable to that of Saturn in the solar system, \bpic b is the closest (semi-major axis $\simeq$\,9\,au) exoplanet that has been imaged to orbit a star. Thus it offers unique opportunities for detailed studies of its orbital, physical, and atmospheric properties, and of disk-planet interactions. With the exception of the discovery observations in 2003 with NaCo at the Very Large Telescope (VLT), all following astrometric measurements relative to \bpic have been obtained in the southwestern part of the orbit, which severely limits the determination of the planet's orbital parameters. We aimed at further constraining \bpic b orbital properties using more data, and, in particular, data taken in the northeastern part of the orbit. We used SPHERE at the VLT to precisely monitor the orbital motion of beta \bpic b since first light of the instrument in 2014. We were able to monitor the planet until November 2016, when its angular separation became too small (125 mas, i.e., 1.6\,au) and prevented further detection. We redetected \bpic b on the northeast side of the disk at a separation of 139\,mas and a PA of 30$^{\circ}$ in September 2018. The planetary orbit is now well constrained. With a semi-major axis (sma) of $a = 9.0 \pm 0.5$ au (1 $\sigma $), it definitely excludes previously reported possible long orbital periods, and excludes \bpic b as the origin of photometric variations that took place in 1981. We also refine the eccentricity and inclination of the planet. From an instrumental point of view, these data demonstrate that it is possible to detect, if they exist, young massive Jupiters that orbit at less than 2 au from a star that is 20 pc away., Comment: accepted by A&A
Published: 2018
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38. Discovery of a planetary-mass companion within the gap of the transition disk around PDS 70

Author: Keppler, M., Benisty, M., Müller, A., Henning, Th., van Boekel, R., Cantalloube, F., Ginski, C., van Holstein, R. G., Maire, A. -L., Pohl, A., Samland, M., Avenhaus, H., Baudino, J. -L., Boccaletti, A., de Boer, J., Bonnefoy, M., Chauvin, G., Desidera, S., Langlois, M., Lazzoni, C., Marleau, G., Mordasini, C., Pawellek, N., Stolker, T., Vigan, A., Zurlo, A., Birnstiel, T., Brandner, W., Feldt, M., Flock, M., Girard, J., Gratton, R., Hagelberg, J., Isella, A., Janson, M., Juhasz, A., Kemmer, J., Kral, Q., Lagrange, A. -M., Launhardt, R., Matter, A., Ménard, F., Milli, J., Mollière, P., Olofsson, J., Perez, L., Pinilla, P., Pinte, C., Quanz, S. P., Schmidt, T., Udry, S., Wahhaj, Z., Williams, J. P., Buenzli, E., Cudel, M., Dominik, C., Galicher, R., Kasper, M., Lannier, J., Mesa, D., Mouillet, D., Peretti, S., Perrot, C., Salter, G., Sissa, E., Wildi, F., Abe, L., Antichi, J., Augereau, J. -C., Baruffolo, A., Baudoz, P., Bazzon, A., Beuzit, J. -L., Blanchard, P., Brems, S. S., Buey, T., De Caprio, V., Carbillet, M., Carle, M., Cascone, E., Cheetham, A., Claudi, R., Costille, A., Delboulbé, A., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Mignant, D. Le, Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Meyer, M., Moeller-Nilsson, O., Moulin, T., Mugnier, L., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Turatto, M., Weber, L., Keppler, M., Benisty, M., Müller, A., Henning, Th., van Boekel, R., Cantalloube, F., Ginski, C., van Holstein, R. G., Maire, A. -L., Pohl, A., Samland, M., Avenhaus, H., Baudino, J. -L., Boccaletti, A., de Boer, J., Bonnefoy, M., Chauvin, G., Desidera, S., Langlois, M., Lazzoni, C., Marleau, G., Mordasini, C., Pawellek, N., Stolker, T., Vigan, A., Zurlo, A., Birnstiel, T., Brandner, W., Feldt, M., Flock, M., Girard, J., Gratton, R., Hagelberg, J., Isella, A., Janson, M., Juhasz, A., Kemmer, J., Kral, Q., Lagrange, A. -M., Launhardt, R., Matter, A., Ménard, F., Milli, J., Mollière, P., Olofsson, J., Perez, L., Pinilla, P., Pinte, C., Quanz, S. P., Schmidt, T., Udry, S., Wahhaj, Z., Williams, J. P., Buenzli, E., Cudel, M., Dominik, C., Galicher, R., Kasper, M., Lannier, J., Mesa, D., Mouillet, D., Peretti, S., Perrot, C., Salter, G., Sissa, E., Wildi, F., Abe, L., Antichi, J., Augereau, J. -C., Baruffolo, A., Baudoz, P., Bazzon, A., Beuzit, J. -L., Blanchard, P., Brems, S. S., Buey, T., De Caprio, V., Carbillet, M., Carle, M., Cascone, E., Cheetham, A., Claudi, R., Costille, A., Delboulbé, A., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Mignant, D. Le, Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Meyer, M., Moeller-Nilsson, O., Moulin, T., Mugnier, L., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Turatto, M., and Weber, L.
Abstract: Young circumstellar disks are of prime interest to understand the physical and chemical conditions under which planet formation takes place. Only very few detections of planet candidates within these disks exist, and most of them are currently suspected to be disk features. In this context, the transition disk around the young star PDS 70 is of particular interest, due to its large gap identified in previous observations, indicative of ongoing planet formation. We aim to search for the presence of planets and search for disk structures indicative for disk-planet interactions and other evolutionary processes. We analyse new and archival near-infrared (NIR) images of the transition disk PDS 70 obtained with the VLT/SPHERE, VLT/NaCo and Gemini/NICI instruments in polarimetric differential imaging (PDI) and angular differential imaging (ADI) modes. We detect a point source within the gap of the disk at about 195 mas (about 22 au) projected separation. The detection is confirmed at five different epochs, in three filter bands and using different instruments. The astrometry results in an object of bound nature, with high significance. The comparison of the measured magnitudes and colours to evolutionary tracks suggests that the detection is a companion of planetary mass. We confirm the detection of a large gap of about 54 au in size within the disk in our scattered light images, and detect a signal from an inner disk component. We find that its spatial extent is very likely smaller than about 17 au in radius. The images of the outer disk show evidence of a complex azimuthal brightness distribution which may in part be explained by Rayleigh scattering from very small grains. Future observations of this system at different wavelengths and continuing astrometry will allow us to test theoretical predictions regarding planet-disk interactions, planetary atmospheres and evolutionary models., Comment: 23 pages, accepted by A&A
Published: 2018
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39. Dynamical masses of M-dwarf binaries in young moving groups: I - The case of TWA 22 and GJ 2060

Author: Rodet, L., Bonnefoy, M., Durkan, S., Beust, H., Lagrange, A-M, Schlieder, J. E., Janson, M., Grandjean, A., Chauvin, G., Messina, S., Maire, A. -L., Brandner, W., Girard, J., Delorme, P., Biller, B., Bergfors, C., Lacour, S., Feldt, M., Henning, T., Boccaletti, A., Bouquin, J. -B. Le, Berger, J. -P., Monin, J. -L., Udry, S., Peretti, S., Segransan, D., Allard, F., Homeier, D., Vigan, A., Langlois, M., Hagelberg, J., Menard, F., Bazzon, A., Beuzit, J. -L., Delboulbe, A., Desidera, S., Gratton, R., Lannier, J., Ligi, R., Maurel, D., Mesa, D., Meyer, M., Pavlov, A., Ramos, J., Rigal, R., Roelfsema, R., Salter, G., Samland, M., Schmidt, T., Stadler, E., Weber, L., Rodet, L., Bonnefoy, M., Durkan, S., Beust, H., Lagrange, A-M, Schlieder, J. E., Janson, M., Grandjean, A., Chauvin, G., Messina, S., Maire, A. -L., Brandner, W., Girard, J., Delorme, P., Biller, B., Bergfors, C., Lacour, S., Feldt, M., Henning, T., Boccaletti, A., Bouquin, J. -B. Le, Berger, J. -P., Monin, J. -L., Udry, S., Peretti, S., Segransan, D., Allard, F., Homeier, D., Vigan, A., Langlois, M., Hagelberg, J., Menard, F., Bazzon, A., Beuzit, J. -L., Delboulbe, A., Desidera, S., Gratton, R., Lannier, J., Ligi, R., Maurel, D., Mesa, D., Meyer, M., Pavlov, A., Ramos, J., Rigal, R., Roelfsema, R., Salter, G., Samland, M., Schmidt, T., Stadler, E., and Weber, L.
Abstract: Evolutionary models are widely used to infer the mass of stars, brown dwarfs, and giant planets. Their predictions are thought to be less reliable at young ages ($<$ 200 Myr) and in the low-mass regime ($\mathrm{<1~M_{\odot}}$). GJ 2060 AB and TWA 22 AB are two rare astrometric M-dwarf binaries respectively members of the AB Doradus and Beta Pictoris moving groups. As their dynamical mass can be measured within a few years, they can be used to calibrate the evolutionary tracks and set new constraints on the age of young moving groups. We find a total mass of $\mathrm{0.18\pm 0.02~M_\odot}$ for TWA 22. That mass is in good agreement with model predictions at the age of the Beta Pic moving group. We obtain a total mass of $\mathrm{1.09 \pm 0.10~M_{\odot}}$ for GJ 2060. We estimate a spectral type of M$1\pm0.5$, $\mathrm{L/L_{\odot}=-1.20\pm0.05}$ dex, and $\mathrm{T_{eff}=3700\pm100}$ K for GJ 2060 A. The B component is a M$3\pm0.5$ dwarf with $\mathrm{L/L_{\odot}=-1.63\pm0.05}$ dex and $\mathrm{T_{eff}=3400\pm100}$ K. The dynamical mass of GJ 2060 AB is inconsistent with the most recent models predictions (BCAH15, PARSEC) for an ABDor age in the range 50-150 Myr. It is 10 to 20\% (1-2 sigma, depending on the assumed age) above the models predictions, corresponding to an underestimation of $0.10$ to $0.20~\mathrm{M_\odot}$. Coevality suggests a young age for the system ($\sim$ 50 Myr) according to most evolutionary models. TWA 22 validates the predictions of recent evolutionary tracks at $\sim$20 Myr. On the other hand, we evidence a 1-2 sigma mismatch between the predicted and observed mass of GJ 2060 AB. This slight departure may indicate that one of the star hosts a tight companion. Alternatively, this would confirm the models tendency to underestimate the mass of young low-mass stars., Comment: Accepted for publication in A&A. 26 pages, 22 figures, 12 tables
Published: 2018
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40. VLT/SPHERE astrometric confirmation and orbital analysis of the brown dwarf companion HR 2562 B

Author: Maire, A. -L., Rodet, L., Lazzoni, C., Boccaletti, A., Brandner, W., Galicher, R., Cantalloube, F., Mesa, D., Klahr, H., Beust, H., Chauvin, G., Desidera, S., Janson, M., Keppler, M., Olofsson, J., Augereau, J. -C., Daemgen, S., Henning, T., Thébault, P., Bonnefoy, M., Feldt, M., Gratton, R., Lagrange, A. -M., Langlois, M., Meyer, M. R., Vigan, A., D'Orazi, V., Hagelberg, J., Coroller, H. Le, Ligi, R., Rouan, D., Samland, M., Schmidt, T., Udry, S., Zurlo, A., Abe, L., Carle, M., Delboulbé, A., Feautrier, P., Magnard, Y., Maurel, D., Moulin, T., Pavlov, A., Perret, D., Petit, C., Ramos, J. R., Rigal, F., Roux, A., Weber, L., Maire, A. -L., Rodet, L., Lazzoni, C., Boccaletti, A., Brandner, W., Galicher, R., Cantalloube, F., Mesa, D., Klahr, H., Beust, H., Chauvin, G., Desidera, S., Janson, M., Keppler, M., Olofsson, J., Augereau, J. -C., Daemgen, S., Henning, T., Thébault, P., Bonnefoy, M., Feldt, M., Gratton, R., Lagrange, A. -M., Langlois, M., Meyer, M. R., Vigan, A., D'Orazi, V., Hagelberg, J., Coroller, H. Le, Ligi, R., Rouan, D., Samland, M., Schmidt, T., Udry, S., Zurlo, A., Abe, L., Carle, M., Delboulbé, A., Feautrier, P., Magnard, Y., Maurel, D., Moulin, T., Pavlov, A., Perret, D., Petit, C., Ramos, J. R., Rigal, F., Roux, A., and Weber, L.
Abstract: Context. A low-mass brown dwarf has been recently imaged around HR 2562 (HD 50571), a star hosting a debris disk resolved in the far infrared. Interestingly, the companion location is compatible with an orbit coplanar with the disk and interior to the debris belt. This feature makes the system a valuable laboratory to analyze the formation of substellar companions in a circumstellar disk and potential disk-companion dynamical interactions. Aims. We aim to further characterize the orbital motion of HR 2562 B and its interactions with the host star debris disk. Methods. We performed a monitoring of the system over ~10 months in 2016 and 2017 with the VLT/SPHERE exoplanet imager. Results. We confirm that the companion is comoving with the star and detect for the first time an orbital motion at high significance, with a current orbital motion projected in the plane of the sky of 25 mas (~0.85 au) per year. No orbital curvature is seen in the measurements. An orbital fit of the SPHERE and literature astrometry of the companion without priors on the orbital plane clearly indicates that its orbit is (quasi-)coplanar with the disk. To further constrain the other orbital parameters, we used empirical laws for a companion chaotic zone validated by N-body simulations to test the orbital solutions that are compatible with the estimated disk cavity size. Non-zero eccentricities (>0.15) are allowed for orbital periods shorter than 100 yr, while only moderate eccentricities up to ~0.3 for orbital periods longer than 200 yr are compatible with the disk observations. A comparison of synthetic Herschel images to the real data does not allow us to constrain the upper eccentricity of the companion., Comment: Accepted for publication in A&A. 14 pages, 14 figures, 3 tables. Updated to match published paper. Bug in the computation of the distributions of times at periastron passages corrected, minor effects on other orbital parameters
Published: 2018
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41. The GJ 504 system revisited. Combining interferometric, radial velocity, and high contrast imaging data

Author: Bonnefoy, M., Perraut, K., Lagrange, A. -M., Delorme, P., Vigan, A., Line, M., Rodet, L., Ginski, C., Mourard, D., Marleau, G. -D., Samland, M., Tremblin, P., Ligi, R., Cantalloube, F., Mollière, P., Charnay, B., Kuzuhara, M., Janson, M., Morley, C., Homeier, D. D., Orazi, V. D, Klahr, H., Mordasini, C., Lavie, B., Baudino, J. -L., Beust, H., Peretti, S., Bartucci, A. Musso, Mesa, D., Bézard, B., Boccaletti, A., Galicher, R., Hagelberg, J., Desidera, S., Biller, B., Maire, A. -L., Allard, F., Borgniet, S., Lannier, J., Meunier, N., Desort, M., Alecian, E., Chauvin, G., Langlois, M., Henning, T., Mugnier, L., Mouillet, D., Gratton, R., Brandt, T., Elwain, M. Mc, Beuzit, J. -L., Tamura, M., Hori, Y., Brandner, W., Buenzli, E., Cheetham, A, Cudel, M., Feldt, M., Kasper, M., Keppler, M., Kopytova, T., Meyer, M., Perrot, C., Rouan, D., Salter, G, Schmidt, T., Sissa, E., Zurlo, A., Wildi, F., Blanchard, P., De Caprio, V., Delboulbé, A., Maurel, D., Moulin, T., Pavlov, A., Rabou, P., Ramos, J., Roelfsema, R., Rousset, G., Stadler, E., Rigal, F., Weber, L., Bonnefoy, M., Perraut, K., Lagrange, A. -M., Delorme, P., Vigan, A., Line, M., Rodet, L., Ginski, C., Mourard, D., Marleau, G. -D., Samland, M., Tremblin, P., Ligi, R., Cantalloube, F., Mollière, P., Charnay, B., Kuzuhara, M., Janson, M., Morley, C., Homeier, D. D., Orazi, V. D, Klahr, H., Mordasini, C., Lavie, B., Baudino, J. -L., Beust, H., Peretti, S., Bartucci, A. Musso, Mesa, D., Bézard, B., Boccaletti, A., Galicher, R., Hagelberg, J., Desidera, S., Biller, B., Maire, A. -L., Allard, F., Borgniet, S., Lannier, J., Meunier, N., Desort, M., Alecian, E., Chauvin, G., Langlois, M., Henning, T., Mugnier, L., Mouillet, D., Gratton, R., Brandt, T., Elwain, M. Mc, Beuzit, J. -L., Tamura, M., Hori, Y., Brandner, W., Buenzli, E., Cheetham, A, Cudel, M., Feldt, M., Kasper, M., Keppler, M., Kopytova, T., Meyer, M., Perrot, C., Rouan, D., Salter, G, Schmidt, T., Sissa, E., Zurlo, A., Wildi, F., Blanchard, P., De Caprio, V., Delboulbé, A., Maurel, D., Moulin, T., Pavlov, A., Rabou, P., Ramos, J., Roelfsema, R., Rousset, G., Stadler, E., Rigal, F., and Weber, L.
Abstract: The G-type star GJ504A is known to host a 3 to 35 MJup companion whose temperature, mass, and projected separation all contribute to make it a test case for the planet formation theories and for atmospheric models of giant planets and light brown dwarfs. We collected data from the CHARA interferometer, SOPHIE spectrograph, and VLT/SPHERE high contrast imager to revisit the properties of the system. We measure a radius of 1.35+/- 0.04Rsun for GJ504A which yields isochronal ages of 21+/-2Myr or 4.0+/-1.8Gyr for the system and line-of-sight stellar rotation axis inclination of $162.4_{-4.3}^{+3.8}$ degrees or $18.6_{-3.8}^{+4.3}$ degrees. We re-detect the companion in the Y2, Y3, J3, H2, and K1 dual band SPHERE images. The complete 1-4 $\mu$m SED shape of GJ504b is best reproduced by T8-T9.5 objects with intermediate ages ($\leq1.5$Gyr), and/or unusual dusty atmospheres and/or super-solar metallicities. All six atmospheric models used yield $\mathrm{T_{eff}=550 \pm 50}$K for GJ504b and point toward a low surface gravity (3.5-4.0 dex). The accuracy on the metallicity value is limited by model-to-model systematics. It is not degenerate with the C/O ratio. We derive $\mathrm{log\:L/L_{\odot}=-6.15\pm0.15}$ dex for the companion compatible with masses of $\mathrm{M=1.3^{+0.6}_{-0.3}M_{Jup}}$ and $\mathrm{M=23^{+10}_{-9} M_{Jup}}$ for the young and old age ranges, respectively. The semi-major axis (sma) is above 27.8 au and the eccentricity lower than 0.55. The posterior on GJ~504b's orbital inclination suggests a misalignment with GJ~504A rotation axis. We combine the radial velocity and multi-epoch imaging data to exclude additional objects (90\% prob.) more massive than 2.5 and 30 $\mathrm{M_{Jup}}$ with sma in the range 0.01-80 au for the young and old system ages, respectively. The companion is in the envelope of the population of planets synthetized with our core-accretion model., Comment: 33 pages, 25 figures. Accepted in Astronomy and Astrophysics
Published: 2018
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42. Astrometric and photometric accuracies in high contrast imaging: The SPHERE speckle calibration tool (SpeCal)

Author: Galicher, R., Boccaletti, A., Mesa, D., Delorme, P., Gratton, R., Langlois, M., Lagrange, A. -M., Maire, A. -L., Coroller, H. Le, Chauvin, G., Biller, B., Cantalloube, F., Janson, M., Lagadec, E., Meunier, N., Vigan, A., Hagelberg, J., Bonnefoy, M., Zurlo, A., Rocha, S., Maurel, D., Jaquet, M., Buey, T., Weber, L., Galicher, R., Boccaletti, A., Mesa, D., Delorme, P., Gratton, R., Langlois, M., Lagrange, A. -M., Maire, A. -L., Coroller, H. Le, Chauvin, G., Biller, B., Cantalloube, F., Janson, M., Lagadec, E., Meunier, N., Vigan, A., Hagelberg, J., Bonnefoy, M., Zurlo, A., Rocha, S., Maurel, D., Jaquet, M., Buey, T., and Weber, L.
Abstract: The consortium of the Spectro-Polarimetric High-contrast Exoplanet REsearch installed at the Very Large Telescope (SPHERE/VLT) has been operating its guaranteed observation time (260 nights over five years) since February 2015. The main part of this time (200 nights) is dedicated to the detection and characterization of young and giant exoplanets on wide orbits. The large amount of data must be uniformly processed so that accurate and homogeneous measurements of photometry and astrometry can be obtained for any source in the field. To complement the European Southern Observatory pipeline, the SPHERE consortium developed a dedicated piece of software to process the data. First, the software corrects for instrumental artifacts. Then, it uses the speckle calibration tool (SpeCal) to minimize the stellar light halo that prevents us from detecting faint sources like exoplanets or circumstellar disks. SpeCal is meant to extract the astrometry and photometry of detected point-like sources (exoplanets, brown dwarfs, or background sources). SpeCal was intensively tested to ensure the consistency of all reduced images (cADI, Loci, TLoci, PCA, and others) for any SPHERE observing strategy (ADI, SDI, ASDI as well as the accuracy of the astrometry and photometry of detected point-like sources. SpeCal is robust, user friendly, and efficient at detecting and characterizing point-like sources in high contrast images. It is used to process all SPHERE data systematically, and its outputs have been used for most of the SPHERE consortium papers to date. SpeCal is also a useful framework to compare different algorithms using various sets of data (different observing modes and conditions). Finally, our tests show that the extracted astrometry and photometry are accurate and not biased., Comment: 11 pages, 9 figures, 5 tables, accepted in A&A
Published: 2018
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43. Discovery of a brown dwarf companion to the star HIP 64892

Author: Cheetham, A., Bonnefoy, M., Desidera, S., Langlois, M., Vigan, A., Schmidt, T., Olofsson, J., Chauvin, G., Klahr, H., Gratton, R., D'Orazi, V., Henning, T., Janson, M., Biller, B., Peretti, S., Hagelberg, J., Ségransan, D., Udry, S., Mesa, D., Sissa, E., Kral, Q., Schlieder, J., Maire, A. -L., Mordasini, C., Menard, F., Zurlo, A., Beuzit, J. -L., Feldt, M., Mouillet, D., Meyer, M., Lagrange, A. -M., Boccaletti, A., Keppler, M., Kopytova, T., Ligi, R., Rouan, D., Coroller, H. Le, Dominik, C., Lagadec, E., Turatto, M., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Blanchard, P., Buey, T., Carbillet, M., Carle, M., Cascone, E., Claudi, R., Costille, A., Delboulbé, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Giro, E., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Mignant, D. Le, Möller-Nilsson, O., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., Wildi, F., Cheetham, A., Bonnefoy, M., Desidera, S., Langlois, M., Vigan, A., Schmidt, T., Olofsson, J., Chauvin, G., Klahr, H., Gratton, R., D'Orazi, V., Henning, T., Janson, M., Biller, B., Peretti, S., Hagelberg, J., Ségransan, D., Udry, S., Mesa, D., Sissa, E., Kral, Q., Schlieder, J., Maire, A. -L., Mordasini, C., Menard, F., Zurlo, A., Beuzit, J. -L., Feldt, M., Mouillet, D., Meyer, M., Lagrange, A. -M., Boccaletti, A., Keppler, M., Kopytova, T., Ligi, R., Rouan, D., Coroller, H. Le, Dominik, C., Lagadec, E., Turatto, M., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Blanchard, P., Buey, T., Carbillet, M., Carle, M., Cascone, E., Claudi, R., Costille, A., Delboulbé, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Giro, E., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Mignant, D. Le, Möller-Nilsson, O., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., and Wildi, F.
Abstract: We report the discovery of a bright, brown dwarf companion to the star HIP 64892, imaged with VLT/SPHERE during the SHINE exoplanet survey. The host is a B9.5V member of the Lower-Centaurus-Crux subgroup of the Scorpius Centaurus OB association. The measured angular separation of the companion ($1.2705\pm0.0023$") corresponds to a projected distance of $159\pm12$ AU. We observed the target with the dual-band imaging and long-slit spectroscopy modes of the IRDIS imager to obtain its SED and astrometry. In addition, we reprocessed archival NACO L-band data, from which we also recover the companion. Its SED is consistent with a young (<30 Myr), low surface gravity object with a spectral type of M9$_{\gamma}\pm1$. From comparison with the BT-Settl atmospheric models we estimate an effective temperature of $T_{\textrm{eff}}=2600 \pm 100$ K, and comparison of the companion photometry to the COND evolutionary models yields a mass of $\sim29-37$ M$_{\text{J}}$ at the estimated age of $16^{+15}_{-7}$ Myr for the system. HIP 64892 is a rare example of an extreme-mass ratio system ($q\sim0.01$) and will be useful for testing models relating to the formation and evolution of such low-mass objects., Comment: 12 pages, 11 figures, accepted for publication in A&A
Published: 2018
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44. Post conjunction detection of $\beta$ Pictoris b with VLT/SPHERE

Author: Lagrange, A. -M., Boccaletti, A., Langlois, M., Chauvin, G., Gratton, R., Beust, H., Desidera, S., Milli, J., Bonnefoy, M., Cheetham, A., Feldt, M., Meyer, M., Vigan, A., Biller, B., Bonavita, M., Baudino, J. -L., Cantalloube, F., Cudel, M., Daemgen, S., Delorme, P., D'Orazi, V., Girard, J., Fontanive, C., Hagelberg, J., Janson, M., Keppler, M., Koypitova, T., Galicher, R., Lannier, J., Coroller, H. Le, Ligi, R., Maire, A. -L., Mesa, D., Messina, S., Mueller, A., Peretti, S., Perrot, C., Rouan, D., Salter, G., Samland, M., Schmidt, T., Sissa, E., Zurlo, A., Beuzit, J. -L., Mouillet, D., Dominik, C., Henning, T., Lagadec, E., Menard, F., Schmid, H. -M., Turatto, M., Udry, S., Bohn, A. J., Charnay, B., Gonzales, C. A. Gomez, Gry, C., Kenworthy, M., Kral, Q., Mordasini, C., Moutou, C., van der Plas, G., Schlieder, J. E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbe, A., de Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Mignant, D. Le, Moller-Nilsson, O., Llored, M., Moulin, T., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Szulagyi, J., Wildi, F., Lagrange, A. -M., Boccaletti, A., Langlois, M., Chauvin, G., Gratton, R., Beust, H., Desidera, S., Milli, J., Bonnefoy, M., Cheetham, A., Feldt, M., Meyer, M., Vigan, A., Biller, B., Bonavita, M., Baudino, J. -L., Cantalloube, F., Cudel, M., Daemgen, S., Delorme, P., D'Orazi, V., Girard, J., Fontanive, C., Hagelberg, J., Janson, M., Keppler, M., Koypitova, T., Galicher, R., Lannier, J., Coroller, H. Le, Ligi, R., Maire, A. -L., Mesa, D., Messina, S., Mueller, A., Peretti, S., Perrot, C., Rouan, D., Salter, G., Samland, M., Schmidt, T., Sissa, E., Zurlo, A., Beuzit, J. -L., Mouillet, D., Dominik, C., Henning, T., Lagadec, E., Menard, F., Schmid, H. -M., Turatto, M., Udry, S., Bohn, A. J., Charnay, B., Gonzales, C. A. Gomez, Gry, C., Kenworthy, M., Kral, Q., Mordasini, C., Moutou, C., van der Plas, G., Schlieder, J. E., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Baudrand, J., Blanchard, P., Bazzon, A., Buey, T., Carbillet, M., Carle, M., Charton, J., Cascone, E., Claudi, R., Costille, A., Deboulbe, A., de Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Gigan, P., Giro, E., Gisler, D., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Mignant, D. Le, Moller-Nilsson, O., Llored, M., Moulin, T., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Szulagyi, J., and Wildi, F.
Abstract: With an orbital distance comparable to that of Saturn in the solar system, \bpic b is the closest (semi-major axis $\simeq$\,9\,au) exoplanet that has been imaged to orbit a star. Thus it offers unique opportunities for detailed studies of its orbital, physical, and atmospheric properties, and of disk-planet interactions. With the exception of the discovery observations in 2003 with NaCo at the Very Large Telescope (VLT), all following astrometric measurements relative to \bpic have been obtained in the southwestern part of the orbit, which severely limits the determination of the planet's orbital parameters. We aimed at further constraining \bpic b orbital properties using more data, and, in particular, data taken in the northeastern part of the orbit. We used SPHERE at the VLT to precisely monitor the orbital motion of beta \bpic b since first light of the instrument in 2014. We were able to monitor the planet until November 2016, when its angular separation became too small (125 mas, i.e., 1.6\,au) and prevented further detection. We redetected \bpic b on the northeast side of the disk at a separation of 139\,mas and a PA of 30$^{\circ}$ in September 2018. The planetary orbit is now well constrained. With a semi-major axis (sma) of $a = 9.0 \pm 0.5$ au (1 $\sigma $), it definitely excludes previously reported possible long orbital periods, and excludes \bpic b as the origin of photometric variations that took place in 1981. We also refine the eccentricity and inclination of the planet. From an instrumental point of view, these data demonstrate that it is possible to detect, if they exist, young massive Jupiters that orbit at less than 2 au from a star that is 20 pc away., Comment: accepted by A&A
Published: 2018
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45. Dynamical masses of M-dwarf binaries in young moving groups: I - The case of TWA 22 and GJ 2060

Author: Rodet, L., Bonnefoy, M., Durkan, S., Beust, H., Lagrange, A-M, Schlieder, J. E., Janson, M., Grandjean, A., Chauvin, G., Messina, S., Maire, A. -L., Brandner, W., Girard, J., Delorme, P., Biller, B., Bergfors, C., Lacour, S., Feldt, M., Henning, T., Boccaletti, A., Bouquin, J. -B. Le, Berger, J. -P., Monin, J. -L., Udry, S., Peretti, S., Segransan, D., Allard, F., Homeier, D., Vigan, A., Langlois, M., Hagelberg, J., Menard, F., Bazzon, A., Beuzit, J. -L., Delboulbe, A., Desidera, S., Gratton, R., Lannier, J., Ligi, R., Maurel, D., Mesa, D., Meyer, M., Pavlov, A., Ramos, J., Rigal, R., Roelfsema, R., Salter, G., Samland, M., Schmidt, T., Stadler, E., Weber, L., Rodet, L., Bonnefoy, M., Durkan, S., Beust, H., Lagrange, A-M, Schlieder, J. E., Janson, M., Grandjean, A., Chauvin, G., Messina, S., Maire, A. -L., Brandner, W., Girard, J., Delorme, P., Biller, B., Bergfors, C., Lacour, S., Feldt, M., Henning, T., Boccaletti, A., Bouquin, J. -B. Le, Berger, J. -P., Monin, J. -L., Udry, S., Peretti, S., Segransan, D., Allard, F., Homeier, D., Vigan, A., Langlois, M., Hagelberg, J., Menard, F., Bazzon, A., Beuzit, J. -L., Delboulbe, A., Desidera, S., Gratton, R., Lannier, J., Ligi, R., Maurel, D., Mesa, D., Meyer, M., Pavlov, A., Ramos, J., Rigal, R., Roelfsema, R., Salter, G., Samland, M., Schmidt, T., Stadler, E., and Weber, L.
Abstract: Evolutionary models are widely used to infer the mass of stars, brown dwarfs, and giant planets. Their predictions are thought to be less reliable at young ages ($<$ 200 Myr) and in the low-mass regime ($\mathrm{<1~M_{\odot}}$). GJ 2060 AB and TWA 22 AB are two rare astrometric M-dwarf binaries respectively members of the AB Doradus and Beta Pictoris moving groups. As their dynamical mass can be measured within a few years, they can be used to calibrate the evolutionary tracks and set new constraints on the age of young moving groups. We find a total mass of $\mathrm{0.18\pm 0.02~M_\odot}$ for TWA 22. That mass is in good agreement with model predictions at the age of the Beta Pic moving group. We obtain a total mass of $\mathrm{1.09 \pm 0.10~M_{\odot}}$ for GJ 2060. We estimate a spectral type of M$1\pm0.5$, $\mathrm{L/L_{\odot}=-1.20\pm0.05}$ dex, and $\mathrm{T_{eff}=3700\pm100}$ K for GJ 2060 A. The B component is a M$3\pm0.5$ dwarf with $\mathrm{L/L_{\odot}=-1.63\pm0.05}$ dex and $\mathrm{T_{eff}=3400\pm100}$ K. The dynamical mass of GJ 2060 AB is inconsistent with the most recent models predictions (BCAH15, PARSEC) for an ABDor age in the range 50-150 Myr. It is 10 to 20\% (1-2 sigma, depending on the assumed age) above the models predictions, corresponding to an underestimation of $0.10$ to $0.20~\mathrm{M_\odot}$. Coevality suggests a young age for the system ($\sim$ 50 Myr) according to most evolutionary models. TWA 22 validates the predictions of recent evolutionary tracks at $\sim$20 Myr. On the other hand, we evidence a 1-2 sigma mismatch between the predicted and observed mass of GJ 2060 AB. This slight departure may indicate that one of the star hosts a tight companion. Alternatively, this would confirm the models tendency to underestimate the mass of young low-mass stars., Comment: Accepted for publication in A&A. 26 pages, 22 figures, 12 tables
Published: 2018
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46. The GJ 504 system revisited. Combining interferometric, radial velocity, and high contrast imaging data

Author: Bonnefoy, M., Perraut, K., Lagrange, A. -M., Delorme, P., Vigan, A., Line, M., Rodet, L., Ginski, C., Mourard, D., Marleau, G. -D., Samland, M., Tremblin, P., Ligi, R., Cantalloube, F., Mollière, P., Charnay, B., Kuzuhara, M., Janson, M., Morley, C., Homeier, D. D., Orazi, V. D, Klahr, H., Mordasini, C., Lavie, B., Baudino, J. -L., Beust, H., Peretti, S., Bartucci, A. Musso, Mesa, D., Bézard, B., Boccaletti, A., Galicher, R., Hagelberg, J., Desidera, S., Biller, B., Maire, A. -L., Allard, F., Borgniet, S., Lannier, J., Meunier, N., Desort, M., Alecian, E., Chauvin, G., Langlois, M., Henning, T., Mugnier, L., Mouillet, D., Gratton, R., Brandt, T., Elwain, M. Mc, Beuzit, J. -L., Tamura, M., Hori, Y., Brandner, W., Buenzli, E., Cheetham, A, Cudel, M., Feldt, M., Kasper, M., Keppler, M., Kopytova, T., Meyer, M., Perrot, C., Rouan, D., Salter, G, Schmidt, T., Sissa, E., Zurlo, A., Wildi, F., Blanchard, P., De Caprio, V., Delboulbé, A., Maurel, D., Moulin, T., Pavlov, A., Rabou, P., Ramos, J., Roelfsema, R., Rousset, G., Stadler, E., Rigal, F., Weber, L., Bonnefoy, M., Perraut, K., Lagrange, A. -M., Delorme, P., Vigan, A., Line, M., Rodet, L., Ginski, C., Mourard, D., Marleau, G. -D., Samland, M., Tremblin, P., Ligi, R., Cantalloube, F., Mollière, P., Charnay, B., Kuzuhara, M., Janson, M., Morley, C., Homeier, D. D., Orazi, V. D, Klahr, H., Mordasini, C., Lavie, B., Baudino, J. -L., Beust, H., Peretti, S., Bartucci, A. Musso, Mesa, D., Bézard, B., Boccaletti, A., Galicher, R., Hagelberg, J., Desidera, S., Biller, B., Maire, A. -L., Allard, F., Borgniet, S., Lannier, J., Meunier, N., Desort, M., Alecian, E., Chauvin, G., Langlois, M., Henning, T., Mugnier, L., Mouillet, D., Gratton, R., Brandt, T., Elwain, M. Mc, Beuzit, J. -L., Tamura, M., Hori, Y., Brandner, W., Buenzli, E., Cheetham, A, Cudel, M., Feldt, M., Kasper, M., Keppler, M., Kopytova, T., Meyer, M., Perrot, C., Rouan, D., Salter, G, Schmidt, T., Sissa, E., Zurlo, A., Wildi, F., Blanchard, P., De Caprio, V., Delboulbé, A., Maurel, D., Moulin, T., Pavlov, A., Rabou, P., Ramos, J., Roelfsema, R., Rousset, G., Stadler, E., Rigal, F., and Weber, L.
Abstract: The G-type star GJ504A is known to host a 3 to 35 MJup companion whose temperature, mass, and projected separation all contribute to make it a test case for the planet formation theories and for atmospheric models of giant planets and light brown dwarfs. We collected data from the CHARA interferometer, SOPHIE spectrograph, and VLT/SPHERE high contrast imager to revisit the properties of the system. We measure a radius of 1.35+/- 0.04Rsun for GJ504A which yields isochronal ages of 21+/-2Myr or 4.0+/-1.8Gyr for the system and line-of-sight stellar rotation axis inclination of $162.4_{-4.3}^{+3.8}$ degrees or $18.6_{-3.8}^{+4.3}$ degrees. We re-detect the companion in the Y2, Y3, J3, H2, and K1 dual band SPHERE images. The complete 1-4 $\mu$m SED shape of GJ504b is best reproduced by T8-T9.5 objects with intermediate ages ($\leq1.5$Gyr), and/or unusual dusty atmospheres and/or super-solar metallicities. All six atmospheric models used yield $\mathrm{T_{eff}=550 \pm 50}$K for GJ504b and point toward a low surface gravity (3.5-4.0 dex). The accuracy on the metallicity value is limited by model-to-model systematics. It is not degenerate with the C/O ratio. We derive $\mathrm{log\:L/L_{\odot}=-6.15\pm0.15}$ dex for the companion compatible with masses of $\mathrm{M=1.3^{+0.6}_{-0.3}M_{Jup}}$ and $\mathrm{M=23^{+10}_{-9} M_{Jup}}$ for the young and old age ranges, respectively. The semi-major axis (sma) is above 27.8 au and the eccentricity lower than 0.55. The posterior on GJ~504b's orbital inclination suggests a misalignment with GJ~504A rotation axis. We combine the radial velocity and multi-epoch imaging data to exclude additional objects (90\% prob.) more massive than 2.5 and 30 $\mathrm{M_{Jup}}$ with sma in the range 0.01-80 au for the young and old system ages, respectively. The companion is in the envelope of the population of planets synthetized with our core-accretion model., Comment: 33 pages, 25 figures. Accepted in Astronomy and Astrophysics
Published: 2018
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47. Discovery of a planetary-mass companion within the gap of the transition disk around PDS 70

Author: Keppler, M., Benisty, M., Müller, A., Henning, Th., van Boekel, R., Cantalloube, F., Ginski, C., van Holstein, R. G., Maire, A. -L., Pohl, A., Samland, M., Avenhaus, H., Baudino, J. -L., Boccaletti, A., de Boer, J., Bonnefoy, M., Chauvin, G., Desidera, S., Langlois, M., Lazzoni, C., Marleau, G., Mordasini, C., Pawellek, N., Stolker, T., Vigan, A., Zurlo, A., Birnstiel, T., Brandner, W., Feldt, M., Flock, M., Girard, J., Gratton, R., Hagelberg, J., Isella, A., Janson, M., Juhasz, A., Kemmer, J., Kral, Q., Lagrange, A. -M., Launhardt, R., Matter, A., Ménard, F., Milli, J., Mollière, P., Olofsson, J., Perez, L., Pinilla, P., Pinte, C., Quanz, S. P., Schmidt, T., Udry, S., Wahhaj, Z., Williams, J. P., Buenzli, E., Cudel, M., Dominik, C., Galicher, R., Kasper, M., Lannier, J., Mesa, D., Mouillet, D., Peretti, S., Perrot, C., Salter, G., Sissa, E., Wildi, F., Abe, L., Antichi, J., Augereau, J. -C., Baruffolo, A., Baudoz, P., Bazzon, A., Beuzit, J. -L., Blanchard, P., Brems, S. S., Buey, T., De Caprio, V., Carbillet, M., Carle, M., Cascone, E., Cheetham, A., Claudi, R., Costille, A., Delboulbé, A., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Mignant, D. Le, Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Meyer, M., Moeller-Nilsson, O., Moulin, T., Mugnier, L., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Turatto, M., Weber, L., Keppler, M., Benisty, M., Müller, A., Henning, Th., van Boekel, R., Cantalloube, F., Ginski, C., van Holstein, R. G., Maire, A. -L., Pohl, A., Samland, M., Avenhaus, H., Baudino, J. -L., Boccaletti, A., de Boer, J., Bonnefoy, M., Chauvin, G., Desidera, S., Langlois, M., Lazzoni, C., Marleau, G., Mordasini, C., Pawellek, N., Stolker, T., Vigan, A., Zurlo, A., Birnstiel, T., Brandner, W., Feldt, M., Flock, M., Girard, J., Gratton, R., Hagelberg, J., Isella, A., Janson, M., Juhasz, A., Kemmer, J., Kral, Q., Lagrange, A. -M., Launhardt, R., Matter, A., Ménard, F., Milli, J., Mollière, P., Olofsson, J., Perez, L., Pinilla, P., Pinte, C., Quanz, S. P., Schmidt, T., Udry, S., Wahhaj, Z., Williams, J. P., Buenzli, E., Cudel, M., Dominik, C., Galicher, R., Kasper, M., Lannier, J., Mesa, D., Mouillet, D., Peretti, S., Perrot, C., Salter, G., Sissa, E., Wildi, F., Abe, L., Antichi, J., Augereau, J. -C., Baruffolo, A., Baudoz, P., Bazzon, A., Beuzit, J. -L., Blanchard, P., Brems, S. S., Buey, T., De Caprio, V., Carbillet, M., Carle, M., Cascone, E., Cheetham, A., Claudi, R., Costille, A., Delboulbé, A., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Giro, E., Gisler, D., Gluck, L., Gry, C., Hubin, N., Hugot, E., Jaquet, M., Mignant, D. Le, Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Meyer, M., Moeller-Nilsson, O., Moulin, T., Mugnier, L., Origne, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Turatto, M., and Weber, L.
Abstract: Young circumstellar disks are of prime interest to understand the physical and chemical conditions under which planet formation takes place. Only very few detections of planet candidates within these disks exist, and most of them are currently suspected to be disk features. In this context, the transition disk around the young star PDS 70 is of particular interest, due to its large gap identified in previous observations, indicative of ongoing planet formation. We aim to search for the presence of planets and search for disk structures indicative for disk-planet interactions and other evolutionary processes. We analyse new and archival near-infrared (NIR) images of the transition disk PDS 70 obtained with the VLT/SPHERE, VLT/NaCo and Gemini/NICI instruments in polarimetric differential imaging (PDI) and angular differential imaging (ADI) modes. We detect a point source within the gap of the disk at about 195 mas (about 22 au) projected separation. The detection is confirmed at five different epochs, in three filter bands and using different instruments. The astrometry results in an object of bound nature, with high significance. The comparison of the measured magnitudes and colours to evolutionary tracks suggests that the detection is a companion of planetary mass. We confirm the detection of a large gap of about 54 au in size within the disk in our scattered light images, and detect a signal from an inner disk component. We find that its spatial extent is very likely smaller than about 17 au in radius. The images of the outer disk show evidence of a complex azimuthal brightness distribution which may in part be explained by Rayleigh scattering from very small grains. Future observations of this system at different wavelengths and continuing astrometry will allow us to test theoretical predictions regarding planet-disk interactions, planetary atmospheres and evolutionary models., Comment: 23 pages, accepted by A&A
Published: 2018
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48. Astrometric and photometric accuracies in high contrast imaging: The SPHERE speckle calibration tool (SpeCal)

Author: Galicher, R., Boccaletti, A., Mesa, D., Delorme, P., Gratton, R., Langlois, M., Lagrange, A. -M., Maire, A. -L., Coroller, H. Le, Chauvin, G., Biller, B., Cantalloube, F., Janson, M., Lagadec, E., Meunier, N., Vigan, A., Hagelberg, J., Bonnefoy, M., Zurlo, A., Rocha, S., Maurel, D., Jaquet, M., Buey, T., Weber, L., Galicher, R., Boccaletti, A., Mesa, D., Delorme, P., Gratton, R., Langlois, M., Lagrange, A. -M., Maire, A. -L., Coroller, H. Le, Chauvin, G., Biller, B., Cantalloube, F., Janson, M., Lagadec, E., Meunier, N., Vigan, A., Hagelberg, J., Bonnefoy, M., Zurlo, A., Rocha, S., Maurel, D., Jaquet, M., Buey, T., and Weber, L.
Abstract: The consortium of the Spectro-Polarimetric High-contrast Exoplanet REsearch installed at the Very Large Telescope (SPHERE/VLT) has been operating its guaranteed observation time (260 nights over five years) since February 2015. The main part of this time (200 nights) is dedicated to the detection and characterization of young and giant exoplanets on wide orbits. The large amount of data must be uniformly processed so that accurate and homogeneous measurements of photometry and astrometry can be obtained for any source in the field. To complement the European Southern Observatory pipeline, the SPHERE consortium developed a dedicated piece of software to process the data. First, the software corrects for instrumental artifacts. Then, it uses the speckle calibration tool (SpeCal) to minimize the stellar light halo that prevents us from detecting faint sources like exoplanets or circumstellar disks. SpeCal is meant to extract the astrometry and photometry of detected point-like sources (exoplanets, brown dwarfs, or background sources). SpeCal was intensively tested to ensure the consistency of all reduced images (cADI, Loci, TLoci, PCA, and others) for any SPHERE observing strategy (ADI, SDI, ASDI as well as the accuracy of the astrometry and photometry of detected point-like sources. SpeCal is robust, user friendly, and efficient at detecting and characterizing point-like sources in high contrast images. It is used to process all SPHERE data systematically, and its outputs have been used for most of the SPHERE consortium papers to date. SpeCal is also a useful framework to compare different algorithms using various sets of data (different observing modes and conditions). Finally, our tests show that the extracted astrometry and photometry are accurate and not biased., Comment: 11 pages, 9 figures, 5 tables, accepted in A&A
Published: 2018
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49. VLT/SPHERE astrometric confirmation and orbital analysis of the brown dwarf companion HR 2562 B

Author: Maire, A. -L., Rodet, L., Lazzoni, C., Boccaletti, A., Brandner, W., Galicher, R., Cantalloube, F., Mesa, D., Klahr, H., Beust, H., Chauvin, G., Desidera, S., Janson, M., Keppler, M., Olofsson, J., Augereau, J. -C., Daemgen, S., Henning, T., Thébault, P., Bonnefoy, M., Feldt, M., Gratton, R., Lagrange, A. -M., Langlois, M., Meyer, M. R., Vigan, A., D'Orazi, V., Hagelberg, J., Coroller, H. Le, Ligi, R., Rouan, D., Samland, M., Schmidt, T., Udry, S., Zurlo, A., Abe, L., Carle, M., Delboulbé, A., Feautrier, P., Magnard, Y., Maurel, D., Moulin, T., Pavlov, A., Perret, D., Petit, C., Ramos, J. R., Rigal, F., Roux, A., Weber, L., Maire, A. -L., Rodet, L., Lazzoni, C., Boccaletti, A., Brandner, W., Galicher, R., Cantalloube, F., Mesa, D., Klahr, H., Beust, H., Chauvin, G., Desidera, S., Janson, M., Keppler, M., Olofsson, J., Augereau, J. -C., Daemgen, S., Henning, T., Thébault, P., Bonnefoy, M., Feldt, M., Gratton, R., Lagrange, A. -M., Langlois, M., Meyer, M. R., Vigan, A., D'Orazi, V., Hagelberg, J., Coroller, H. Le, Ligi, R., Rouan, D., Samland, M., Schmidt, T., Udry, S., Zurlo, A., Abe, L., Carle, M., Delboulbé, A., Feautrier, P., Magnard, Y., Maurel, D., Moulin, T., Pavlov, A., Perret, D., Petit, C., Ramos, J. R., Rigal, F., Roux, A., and Weber, L.
Abstract: Context. A low-mass brown dwarf has been recently imaged around HR 2562 (HD 50571), a star hosting a debris disk resolved in the far infrared. Interestingly, the companion location is compatible with an orbit coplanar with the disk and interior to the debris belt. This feature makes the system a valuable laboratory to analyze the formation of substellar companions in a circumstellar disk and potential disk-companion dynamical interactions. Aims. We aim to further characterize the orbital motion of HR 2562 B and its interactions with the host star debris disk. Methods. We performed a monitoring of the system over ~10 months in 2016 and 2017 with the VLT/SPHERE exoplanet imager. Results. We confirm that the companion is comoving with the star and detect for the first time an orbital motion at high significance, with a current orbital motion projected in the plane of the sky of 25 mas (~0.85 au) per year. No orbital curvature is seen in the measurements. An orbital fit of the SPHERE and literature astrometry of the companion without priors on the orbital plane clearly indicates that its orbit is (quasi-)coplanar with the disk. To further constrain the other orbital parameters, we used empirical laws for a companion chaotic zone validated by N-body simulations to test the orbital solutions that are compatible with the estimated disk cavity size. Non-zero eccentricities (>0.15) are allowed for orbital periods shorter than 100 yr, while only moderate eccentricities up to ~0.3 for orbital periods longer than 200 yr are compatible with the disk observations. A comparison of synthetic Herschel images to the real data does not allow us to constrain the upper eccentricity of the companion., Comment: Accepted for publication in A&A. 14 pages, 14 figures, 3 tables. Updated to match published paper. Bug in the computation of the distributions of times at periastron passages corrected, minor effects on other orbital parameters
Published: 2018
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50. Discovery of a brown dwarf companion to the star HIP 64892

Author: Cheetham, A., Bonnefoy, M., Desidera, S., Langlois, M., Vigan, A., Schmidt, T., Olofsson, J., Chauvin, G., Klahr, H., Gratton, R., D'Orazi, V., Henning, T., Janson, M., Biller, B., Peretti, S., Hagelberg, J., Ségransan, D., Udry, S., Mesa, D., Sissa, E., Kral, Q., Schlieder, J., Maire, A. -L., Mordasini, C., Menard, F., Zurlo, A., Beuzit, J. -L., Feldt, M., Mouillet, D., Meyer, M., Lagrange, A. -M., Boccaletti, A., Keppler, M., Kopytova, T., Ligi, R., Rouan, D., Coroller, H. Le, Dominik, C., Lagadec, E., Turatto, M., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Blanchard, P., Buey, T., Carbillet, M., Carle, M., Cascone, E., Claudi, R., Costille, A., Delboulbé, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Giro, E., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Mignant, D. Le, Möller-Nilsson, O., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., Wildi, F., Cheetham, A., Bonnefoy, M., Desidera, S., Langlois, M., Vigan, A., Schmidt, T., Olofsson, J., Chauvin, G., Klahr, H., Gratton, R., D'Orazi, V., Henning, T., Janson, M., Biller, B., Peretti, S., Hagelberg, J., Ségransan, D., Udry, S., Mesa, D., Sissa, E., Kral, Q., Schlieder, J., Maire, A. -L., Mordasini, C., Menard, F., Zurlo, A., Beuzit, J. -L., Feldt, M., Mouillet, D., Meyer, M., Lagrange, A. -M., Boccaletti, A., Keppler, M., Kopytova, T., Ligi, R., Rouan, D., Coroller, H. Le, Dominik, C., Lagadec, E., Turatto, M., Abe, L., Antichi, J., Baruffolo, A., Baudoz, P., Blanchard, P., Buey, T., Carbillet, M., Carle, M., Cascone, E., Claudi, R., Costille, A., Delboulbé, A., De Caprio, V., Dohlen, K., Fantinel, D., Feautrier, P., Fusco, T., Giro, E., Gluck, L., Hubin, N., Hugot, E., Jaquet, M., Kasper, M., Llored, M., Madec, F., Magnard, Y., Martinez, P., Maurel, D., Mignant, D. Le, Möller-Nilsson, O., Moulin, T., Origné, A., Pavlov, A., Perret, D., Petit, C., Pragt, J., Puget, P., Rabou, P., Ramos, J., Rigal, F., Rochat, S., Roelfsema, R., Rousset, G., Roux, A., Salasnich, B., Sauvage, J. -F., Sevin, A., Soenke, C., Stadler, E., Suarez, M., Weber, L., and Wildi, F.
Abstract: We report the discovery of a bright, brown dwarf companion to the star HIP 64892, imaged with VLT/SPHERE during the SHINE exoplanet survey. The host is a B9.5V member of the Lower-Centaurus-Crux subgroup of the Scorpius Centaurus OB association. The measured angular separation of the companion ($1.2705\pm0.0023$") corresponds to a projected distance of $159\pm12$ AU. We observed the target with the dual-band imaging and long-slit spectroscopy modes of the IRDIS imager to obtain its SED and astrometry. In addition, we reprocessed archival NACO L-band data, from which we also recover the companion. Its SED is consistent with a young (<30 Myr), low surface gravity object with a spectral type of M9$_{\gamma}\pm1$. From comparison with the BT-Settl atmospheric models we estimate an effective temperature of $T_{\textrm{eff}}=2600 \pm 100$ K, and comparison of the companion photometry to the COND evolutionary models yields a mass of $\sim29-37$ M$_{\text{J}}$ at the estimated age of $16^{+15}_{-7}$ Myr for the system. HIP 64892 is a rare example of an extreme-mass ratio system ($q\sim0.01$) and will be useful for testing models relating to the formation and evolution of such low-mass objects., Comment: 12 pages, 11 figures, accepted for publication in A&A
Published: 2018
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