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749 results on '"Pinte, C."'

153. Discovery of a planetary-mass companion within the gap of the transition disk around PDS 70

Author

Keppler, M, Benisty, M, Müller, A, Henning, T, Van Boekel, R, Cantalloube, F, Ginski, C, Van Holstein, RG, Maire, AL, Pohl, A, Samland, M, Avenhaus, H, Baudino, JL, Boccaletti, A, De Boer, J, Bonnefoy, M, Chauvin, G, Desidera, S, Langlois, M, Lazzoni, C, Marleau, GD, 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, AM, Launhardt, R, Matter, A, Ménard, F, Milli, J, Mollière, P, Olofsson, J, Pérez, L, Pinilla, P, Pinte, C, Quanz, SP, Schmidt, T, Udry, S, Wahhaj, Z, Williams, JP, 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, JC, Baruffolo, A, Baudoz, P, Bazzon, A, Beuzit, JL, Blanchard, P, Brems, SS, 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, Gluck, L, Gry, C, Hubin, N, Hugot, E, Jaquet, M, Le Mignant, D, Llored, M, Madec, F, Magnard, Y, Martinez, P, Maurel, D, Pawellek, Nicole [0000-0002-9385-9820], and Apollo - University of Cambridge Repository

Subjects
planets and satellites: detection, stars: individual: PDS 70, radiative transfer, protoplanetary disks, scattering, Astrophysics::Solar and Stellar Astrophysics, techniques: high angular resolution, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
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.

Published
2020
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155. Gap, shadows, spirals, and streamers : SPHERE observations of binary-disk interactions in GG Tauri A

Author

Keppler, M., Penzlin, A., Benisty, M., van Boekel, R., Henning, T., van Holstein, R. G., Kley, W., Garufi, A., Ginski, C., Brandner, W., Bertrang, G. H.-M., Boccaletti, A., de Boer, J., Bonavita, M., Brown Sevilla, S., Chauvin, G., Dominik, C., Janson, Markus, Langlois, M., Lodato, G., Maire, A.-L., Ménard, F., Pantin, E., Pinte, C., Stolker, T., Szulágyi, J., Thebault, P., Villenave, M., Zurlo, A., Rabou, P., Feautrier, P., Feldt, M., Madec, F., Wildi, F., Keppler, M., Penzlin, A., Benisty, M., van Boekel, R., Henning, T., van Holstein, R. G., Kley, W., Garufi, A., Ginski, C., Brandner, W., Bertrang, G. H.-M., Boccaletti, A., de Boer, J., Bonavita, M., Brown Sevilla, S., Chauvin, G., Dominik, C., Janson, Markus, Langlois, M., Lodato, G., Maire, A.-L., Ménard, F., Pantin, E., Pinte, C., Stolker, T., Szulágyi, J., Thebault, P., Villenave, M., Zurlo, A., Rabou, P., Feautrier, P., Feldt, M., Madec, F., and Wildi, F.

Abstract

Context. A large portion of stars is found to be part of binary or higher-order multiple systems. The ubiquity of planets found around single stars raises the question of whether and how planets in binary systems form. Protoplanetary disks are the birthplaces of planets, and characterizing them is crucial in order to understand the planet formation process. Aims. Our goal is to characterize the morphology of the GG Tau A disk, one of the largest and most massive circumbinary disks. We also aim to trace evidence for binary-disk interactions. Methods. We obtained observations in polarized scattered light of GG Tau A using the SPHERE/IRDIS instrument in the H-band filter. We analyzed the observed disk morphology and substructures. We ran 2D hydrodynamical models to simulate the evolution of the circumbinary ring over the lifetime of the disk. Results. The disk and also the cavity and the inner region are highly structured, with several shadowed regions, spiral structures, and streamer-like filaments. Some of these are detected here for the first time. The streamer-like filaments appear to connect the outer ring with the northern arc. Their azimuthal spacing suggests that they may be generated through periodic perturbations by the binary, which tear off material from the inner edge of the outer disk once during each orbit. By comparing observations to hydrodynamical simulations, we find that the main features, in particular, the gap size, but also the spiral and streamer filaments, can be qualitatively explained by the gravitational interactions of a binary with a semimajor axis of similar to 35 au on an orbit coplanar with the circumbinary ring.

Published
2020
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156. A faint companion around CrA-9: protoplanet or obscured binary?

Author

Christiaens, V, primary, Ubeira-Gabellini, M-G, additional, Cánovas, H, additional, Delorme, P, additional, Pairet, B, additional, Absil, O, additional, Casassus, S, additional, Girard, J H, additional, Zurlo, A, additional, Aoyama, Y, additional, Marleau, G-D, additional, Spina, L, additional, van der Marel, N, additional, Cieza, L, additional, Lodato, G, additional, Pérez, S, additional, Pinte, C, additional, Price, D J, additional, and Reggiani, M, additional

Published
2021
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158. Observations of edge-on protoplanetary disks with ALMA

Author

Villenave, M., primary, Ménard, F., additional, Dent, W. R. F., additional, Duchêne, G., additional, Stapelfeldt, K. R., additional, Benisty, M., additional, Boehler, Y., additional, van der Plas, G., additional, Pinte, C., additional, Telkamp, Z., additional, Wolff, S., additional, Flores, C., additional, Lesur, G., additional, Louvet, F., additional, Riols, A., additional, Dougados, C., additional, Williams, H., additional, and Padgett, D., additional

Published
2020
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159. Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): A close low-mass companion to ET Cha

Author

Ginski, C., primary, Ménard, F., additional, Rab, Ch., additional, Mamajek, E. E., additional, van Holstein, R. G., additional, Benisty, M., additional, Manara, C. F., additional, Asensio Torres, R., additional, Bohn, A., additional, Birnstiel, T., additional, Delorme, P., additional, Facchini, S., additional, Garufi, A., additional, Gratton, R., additional, Hogerheijde, M., additional, Huang, J., additional, Kenworthy, M., additional, Langlois, M., additional, Pinilla, P., additional, Pinte, C., additional, Ribas, Á., additional, Rosotti, G., additional, Schmidt, T. O. B., additional, van den Ancker, M., additional, Wahhaj, Z., additional, Waters, L. B. F. M., additional, Williams, J., additional, and Zurlo, A., additional

Published
2020
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160. Ongoing flyby in the young multiple system UX Tauri

Author

Ménard, F., primary, Cuello, N., additional, Ginski, C., additional, van der Plas, G., additional, Villenave, M., additional, Gonzalez, J.-F., additional, Pinte, C., additional, Benisty, M., additional, Boccaletti, A., additional, Price, D. J., additional, Boehler, Y., additional, Chripko, S., additional, de Boer, J., additional, Dominik, C., additional, Garufi, A., additional, Gratton, R., additional, Hagelberg, J., additional, Henning, Th., additional, Langlois, M., additional, Maire, A. L., additional, Pinilla, P., additional, Ruane, G. J., additional, Schmid, H. M., additional, van Holstein, R. G., additional, Vigan, A., additional, Zurlo, A., additional, Hubin, N., additional, Pavlov, A., additional, Rochat, S., additional, Sauvage, J.-F., additional, and Stadler, E., additional

Published
2020
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161. Gap, shadows, spirals, and streamers: SPHERE observations of binary-disk interactions in GG Tauri A

Author

Keppler, M., primary, Penzlin, A., additional, Benisty, M., additional, van Boekel, R., additional, Henning, T., additional, van Holstein, R. G., additional, Kley, W., additional, Garufi, A., additional, Ginski, C., additional, Brandner, W., additional, Bertrang, G. H.-M., additional, Boccaletti, A., additional, de Boer, J., additional, Bonavita, M., additional, Brown Sevilla, S., additional, Chauvin, G., additional, Dominik, C., additional, Janson, M., additional, Langlois, M., additional, Lodato, G., additional, Maire, A.-L., additional, Ménard, F., additional, Pantin, E., additional, Pinte, C., additional, Stolker, T., additional, Szulágyi, J., additional, Thebault, P., additional, Villenave, M., additional, Zurlo, A., additional, Rabou, P., additional, Feautrier, P., additional, Feldt, M., additional, Madec, F., additional, and Wildi, F., additional

Published
2020
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162. A family portrait of disk inner rims around Herbig Ae/Be stars

Author

Kluska, J., primary, Berger, J.-P., additional, Malbet, F., additional, Lazareff, B., additional, Benisty, M., additional, Le Bouquin, J.-B., additional, Absil, O., additional, Baron, F., additional, Delboulbé, A., additional, Duvert, G., additional, Isella, A., additional, Jocou, L., additional, Juhasz, A., additional, Kraus, S., additional, Lachaume, R., additional, Ménard, F., additional, Millan-Gabet, R., additional, Monnier, J. D., additional, Moulin, T., additional, Perraut, K., additional, Rochat, S., additional, Pinte, C., additional, Soulez, F., additional, Tallon, M., additional, Thi, W.-F., additional, Thiébaut, E., additional, Traub, W., additional, and Zins, G., additional

Published
2020
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163. Nine Localized Deviations from Keplerian Rotation in the DSHARP Circumstellar Disks: Kinematic Evidence for Protoplanets Carving the Gaps

Author

Pinte, C., primary, Price, D. J., additional, Ménard, F., additional, Duchêne, G., additional, Christiaens, V., additional, Andrews, S. M., additional, Huang, J., additional, Hill, T., additional, van der Plas, G., additional, Perez, L. M., additional, Isella, A., additional, Boehler, Y., additional, Dent, W. R. F., additional, Mentiplay, D., additional, and Loomis, R. A., additional

Published
2020
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164. HD 172555: Detection of 63 micrometers [OI] Emission in a Debris Disc

Author

Riviere-Marichalar, P, Barrado, D, Augereau, J. -C, Thi, W. F, Roberge, A, Eiroa, C, Montesinos, B, Meeus, G, Howard, C, Sandell, G, Duchene, G, Dent, W. R. F, Lebreton, J, Mendigutia, I, Huelamo, N, Menard, F, and Pinte, C

Subjects
Astrophysics
Abstract

Context. HD 172555 is a young A7 star belonging to the Beta Pictoris Moving Group that harbours a debris disc. The Spitzer IRS spectrum of the source showed mid-IR features such as silicates and glassy silica species, indicating the presence of a warm dust component with small grains, which places HD 172555 among the small group of debris discs with such properties. The IRS spectrum also shows a possible emission of SiO gas. Aims. We aim to study the dust distribution in the circumstellar disc of HD 172555 and to asses the presence of gas in the debris disc. Methods. As part of the GASPS Open Time Key Programme, we obtained Herschel-PACS photometric and spectroscopic observations of the source. We analysed PACS observations of HD 172555 and modelled the Spectral Energy Distribution (SED) with a modified blackbody and the gas emission with a two-level population model with no collisional de-excitation. Results. We report for the first time the detection of [OI] atomic gas emission at 63.18 micrometers in the HD 172555 circumstellar disc.We detect excesses due to circumstellar dust toward HD 172555 in the three photometric bands of PACS (70, 100, and 160 m). We derive a large dust particle mass of (4.8 plus-minus 0.6)x10(exp -4) Mass compared to Earth and an atomic oxygen mass of 2.5x10(exp -2)R(exp 2) Mass compared to Earth, where R in AU is the separation between the star and the inner disc. Thus, most of the detected mass of the disc is in the gaseous phase.

Published
2012

165. Observations of Herbig Ae/Be Stars with Herschel/PACS: The Atomic and Molecular Contents of Their Protoplanetary Discs

Author

Meeus, G, Montesinos, B, Mendigutia, I, Kamp, I, Thi, W. F, Eiroa, C, Grady, C. A, Mathews, G, Sandell, G, Martin-Zaidi, C, Brittain, S, Dent, W. R. F, Howard, C, Menard, F, Pinte, C, Roberge, A, Vandenbussche, B, and Williams, J. P

Subjects
Astronomy
Abstract

We observed a sample of 20 representative Herbig Ae/Be stars and 5 A-type debris discs with PACS onboard Herschel, as part of the GAS in Protoplanetary Systems (GASPS) project. The observations were done in spectroscopic mode, and cover the far-infrared lines of [OI], [CII], CO, CH+, H20, and OH. We have a [OI]63 micro/ detection rate of 100% for the Herbig Ae/Be and 0% for the debris discs. The [OI] 145 micron line is only detected in 25% and CO J = 18-17 in 45% (and fewer cases for higher J transitions) of the Herbig Ae/Be stars, while for [CII] 157 micron, we often find spatially variable background contamination. We show the first detection of water in a Herbig Ae disc, HD 163296, which has a settled disc. Hydroxyl is detected as well in this disc. First seen in HD 100546, CH+ emission is now detected for the second time in a Herbig Ae star, HD 97048. We report fluxes for each line and use the observations as line diagnostics of the gas properties. Furthermore, we look for correlations between the strength of the emission lines and either the stellar or disc parameters, such as stellar luminosity, ultraviolet and X-ray flux. accretion rate, polycyclic aromatic hydrocarbon (PAH) band strength, and flaring. We find that the stellar ultraviolet flux is the dominant excitation mechanism of [OI] 63 micron, with the highest line fluxes being found in objects with a large amount of flaring and among the largest PAH strengths. Neither the amount of accretion nor the X-ray luminosity has an influence on the line strength. We find correlations between the line flux of [OI]63 micron and [OI] 145 micron, CO J = IS-17 and [OI] 6300 A, and between the continuum flux at 63 micron and at 1.3 mm, while we find weak correlations between the line flux. of [OI] 63 micron and the PAH luminosity, the line flux of CO J = 3-2, the continuum flux at 63 pm, the stellar effective temperature, and the Br-gamma luminosity. Finally, we use a combination of the [OI] 63 micron and C(12)O J = 2-1 line fluxes to obtain order of magnitude estimates of the disc gas masses, in agreement with the values that we find from detailed modelling of two Herbig Ae/Be stars, HD 163296 and HD 169142.

Published
2012
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166. An Icy Kuiper Belt Around the Young Solar-type Star HD 181327

Author

Lebreton, J, Augereau, J.-C, Thi, W.-F, Roberge, A, Donaldson, J, Schneider, G, Maddison, S. T, Menard, F, Riviere-Marichalar, P, Matthews, G. S, Kamp, I, Pinte, C, Dent, W. R. F, Barrado, D, Duchene, G, Gonzalez, J.-F, Grady C. A, Meeus,G, Pantin, E, Williams, J. P, and Woitke, P

Subjects
Astronomy
Abstract

Context. HD 181327 is a young main sequence F5/F6 V star belonging to the Beta Pictoris moving group (age approx.. 12 Myr). It harbors an optically thin belt of circumstellar material at radius approx.. 90 AU, presumed to result from collisions in a population of unseen planetesimals. Aims. We aim to study the dust properties in the belt in details, and to constrain the gas-to-dust ratio. Methods. We obtained far-infrared photometric observations of HD 181327 with the PACS instrument onboard the Herschel Space Observatory, complemented by new 3.2 mm observations carried with the ATCA array. The geometry of the belt is constrained with newly reduced HST/NICMOS scattered light images that allow the degeneracy between the disk geometry and the dust properties to be broken. We then use the radiative transfer code GRaTeR to compute a large grid of models, and we identify the grain models that best reproduce the spectral energy distribution (SED) through a Bayesian analysis. We attempt to detect the oxygen and ionized carbon fine-structure lines with Herschel/PACS spectroscopy, providing observables to our photochemical code ProDiMo. Results. The HST observations confirm that the dust is confined in a narrow belt. The continuum is detected with Herschel/PACS completing nicely the SED in the far-infrared. The disk is marginally resolved with both PACS and ATCA. A medium integration of the gas spectral lines only provides upper limits on the [OI] and [CII] line fluxes.We show that the HD 181327 dust disk consists of micron-sized grains of porous amorphous silicates and carbonaceous material surrounded by an important layer of ice, for a total dust mass of approx.. 0.05 Solar Mass (in grains up to 1 mm). We discuss evidences that the grains consists of fluffy aggregates. The upper limits on the gas atomic lines do not provide unambiguous constraints: only if the PAH abundance is high, the gas mass must be lower than approx. 17 Solar Mass. Conclusions. Despite the weak constraints on the gas disk, the age of HD 181327 and the properties of the dust disk suggest that it has passed the stage of gaseous planets formation. The dust reveals a population of icy planetesimals, similar to the primitive Edgeworth-Kuiper belt, that may be a source for the future delivery of water and volatiles onto forming terrestrial planets.

Published
2012
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167. An Icy Kuiper-Belt Around the Young Solar-Type Star HD 181327

Author

Lebreton, J, Augereau, J.-C, Thi, W.-F, Roberge, A, Donaldson, J, Schneider, G, Maddison, S. T, Menard, F, Riviere-Marichalar, P, Mathews, G. S, Kamp, I, Pinte, C, Dent, W. R. F, Barrado, D, Duchene, G, Gonzalez, J.-F, Grady, C. A, Meeus, G, Pantin, E, Williams, J. P, and Woitke, P

Subjects
Astronomy
Abstract

HD 181327 is a young Main Sequence F5/F6 V star belonging to the Beta Pictoris moving group (age approx 12 Myr). It harbors an optically thin belt of circumstellar material at approx90 AU, presumed to result from collisions in a populat.ion of unseen planetesimals. Aims. We aim to study the dust properties in the belt in great details, and to constrain the gas-to-dust ratio. Methods. We obtained far-IR photometric observations of HD 181327 with the PACS instrument onboard the Herschel Space Observatory, complemented by new 3.2 nun observations carried with the ATCA array. The geometry of the belt is constrained with newly reduced HST /NICMOS scattered light images that break the degeneracy between the disk geometry and the dust properties. We then use the radiative transfer code GRaTer to compute a large grid of dust models, and we apply a Bayesian inference method to identify the grain models that best reproduce the SED. We attempt to detect the oxygen and ionized carbon fine-structure lines with Herschel/PACS spectroscopy, providing observables to our photochemical code ProDiMo. Results. The HST observations confirm that the dust is confined in a narrow belt. The continuum is detected with Herschel/PACS completing nicely the SED in the far-infrared. The disk is marginally resolved with both PACS and ATCA. A medium integration of the gas spectral lines only provides upper limits on the [OI] and [CII] line fluxes. We show that the HD 181327 dust disk consists of micron-sized grains of porous amorphous silicates and carbonaceous material surrounded by an import.ant layer of ice for a total dust mass of approx 0.05 stellar Mass. We discuss evidences that the grains consists of fluffy aggregates. The upper limits on the gas atomic lines do not provide unambiguous constraints: only if the PAH abundance is high, the gas mass must be lower than approx 17 Stellar Mass Conclusions. Despite the weak constraints on the gas disk, the age of HD 181327 and the properties of the dust disk suggest that it has passed the stage of gaseous planets formation. The dust reveals a population of icy planetesimals, similar to the primitive Edgeworth-Kuiper Belt, that may be a source for the future delivery of water and volatiles onto forming terrestrial planets.

Published
2011

168. Gas Modelling in the Disc of HD 163296

Author

Tilling, I, Woitke, P, Meeus, G, Mora, A, Montesinos, B, Riviere-Marichalar, P, Eiroa, C, Thi, W. -F, Isella, A, Roberge, A, Martin-Zaidi, C, Kamp, I, Pinte, C, Sandell, G, Vacca, W. D, Menard, F, Mendigutia, I, Duchene, G, Dent, W. R. F, Aresu, G, Meijerink, R, and Spaans, M

Subjects
Astronomy
Abstract

We present detailed model fits to observations of the disc around the Herbig Ae star HD 163296. This well-studied object has an age of approx. 4Myr, with evidence of a circumstellar disc extending out to approx. 540AU. We use the radiation thermo-chemical disc code ProDiMo to model the gas and dust in the circumstellar disc of HD 163296, and attempt to determine the disc properties by fitting to observational line and continuum data. These include new Herschel/PACS observations obtained as part of the open-time key program GASPS (Gas in Protoplanetary Systems), consisting of a detection of the [Oi] 63 m line and upper limits for several other far infrared lines. We complement this with continuum data and ground-based observations of the CO-12 3-2, 2-1 and CO-13 J=1-0 line transitions, as well as the H2 S(1) transition. We explore the effects of stellar ultraviolet variability and dust settling on the line emission, and on the derived disc properties. Our fitting efforts lead to derived gas/dust ratios in the range 9-100, depending on the assumptions made. We note that the line fluxes are sensitive in general to the degree of dust settling in the disc, with an increase in line flux for settled models. This is most pronounced in lines which are formed in the warm gas in the inner disc, but the low excitation molecular lines are also affected. This has serious implications for attempts to derive the disc gas mass from line observations. We derive fractional PAH abundances between 0.007 and 0.04 relative to ISM levels. Using a stellar and UV excess input spectrum based on a detailed analysis of observations, we find that the all observations are consistent with the previously assumed disc geometry

Published
2011

169. Constraining protoplanetary disc mass using the GI wiggle.

Author

Terry, J P, Hall, C, Longarini, C, Lodato, G, Toci, C, Veronesi, B, Paneque-Carreño, T, and Pinte, C

Subjects
ACCRETION disks, GRAVITATIONAL instability, STELLAR mass, ORIGIN of planets, PROTOPLANETARY disks, PLANETARY mass
Abstract

Exoplanets form in protoplanetary accretion discs. The total protoplanetary disc mass is the most fundamental parameter, since it sets the mass budget for planet formation. Although observations with the Atacama Large Millimeter/Submillimeter array (ALMA) have dramatically increased our understanding of these discs, total protoplanetary disc mass remains difficult to measure. If a disc is sufficiently massive (≳10 per cent of the host star mass), it can excite gravitational instability (GI). Recently, it has been revealed that GI leaves kinematic imprints of its presence known as the 'GI Wiggle'. In this work, we use numerical simulations to determine an approximately linear relationship between the amplitude of the wiggle and the host disc-to-star mass ratio, and show that measurements of the amplitude are possible with the spatial and spectral capabilities of ALMA. These measurements can therefore be used to constrain disc-to-star mass ratio. [ABSTRACT FROM AUTHOR]

Published
2022
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170. protoplanetary disc around HD 169142: circumstellar or circumbinary?

Author

Poblete, P P, Cuello, N, Pérez, S, Marino, S, Calcino, J, Macías, E, Ribas, Á, Zurlo, A, Cuadra, J, Montesinos, M, Zúñiga-Fernández, S, Bayo, A, Pinte, C, Ménard, F, and Price, D J

Subjects
PROTOPLANETARY disks, GAS distribution, PLANETARY orbits
Abstract

Stellar binaries represent a substantial fraction of stellar systems, especially among young stellar objects. Accordingly, binaries play an important role in setting the architecture of a large number of protoplanetary discs. Binaries in coplanar and polar orientations with respect to the circumbinary disc are stable configurations and could induce non-axisymmetric structures in the dust and gas distributions. In this work, we suggest that the structures shown in the central region of the protoplanetary disc HD 169142 are produced by the presence of an inner stellar binary and a circumbinary (P-type) planet. We find that a companion with a mass ratio of 0.1, semimajor axis of 9.9 au, eccentricity of 0.2, and inclination of 90°, together with a 2  M J coplanar planet on a circular orbit at 45 au reproduce the structures at the innermost ring observed at 1.3 mm and the shape of spiral features in scattered light observations. The model predicts changes in the disc's dust structure, and star's astrometric parameters, which would allow testing its veracity by monitoring this system over the next 20 yr. [ABSTRACT FROM AUTHOR]

Published
2022
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171. High-fidelity Imaging of the Inner AU Mic Debris Disk: Evidence of Differential Wind Sculpting?

Author

Molaverdikhani, K., Trifonov, T., Mollière, P., Frankel, N., Messina, S., Biller, B. A., Roux, A., Damasso, M., Del Sordo, F., Brandner, W., Kervella, P., Mugnier, L., Romero, C., Sozzetti, A., Antichi, J., Huby, E., N’Diaye, M., Kitzmann, D., Tang, Y. W., Habart, E., Beck, T. L., Potier, A., Singh, G., Di Folco, E., Péricaud, J., Dutrey, A., Chapillon, E., Guilloteau, S., Piétu, V., Pawellek, N., Brown, S., Buey, T., Moeller-Nilsson, O., Stolker, T., Hunziker, S., Abe, L., Avenhaus, H., Baruffolo, A., Bazzon, A., Costille, A., Daban, J.-B., Downing, M., Engler, N., Gisler, D., Hubin, N., Puget, P., Quanz, S. P., Roelfsema, R., Salasnich, B., Siebenmorgen, R., Suarez, M., Szulágyi, J., Thalmann, Ch., Pohl, A., Fantinel, D., Maurel, D., Origné, A., Petit, C., Rigal, F., Girard, J. H., Mouillet, D., Dohlen, K., Snik, F., Keller, C. U., Ginski, C., Stam, D. M., Wahhaj, Z., Kasper, M., Schmid, H. M., Perret, D., Dominik, C., Turatto, M., Beuzit, J.-L., Keppler, M., Rodet, L., Charnay, B., Bae, J., De Boer, J., Müller, A., Pairet, B., Antoniucci, S., Brown Sevilla, S., Cascone, E., Claudi, R. U., Lagadec, E., Martinez, P., Meunier, N., Petrus, S., Pinte, C., Rochat, S., Sauvage, J.-F., Peretti, S., Ségransan, D., Lavie, B., Baudino, J.-L., Janson, M., Heng, Kevin, Udry, S., Daemgen, S., Le Coroller, H., Samland, M., Carbillet, M., Carle, M., Hugot, E., Magnard, Y., Moulin, T., Pavlov, A., Pragt, J., Rabou, P., Rousset, G., Sevin, A., Soenke, C., Stadler, E., Weber, L., Wildi, F., Bhowmik, T., Thébault, P., Kral, Q., Mazoyer, J., van Holstein, R. G., Baudoz, P., Galicher, R., Olofsson, J., Pantin, E., Perrot, C., Mesa, D., Langlois, M., Garufi, A., Gratton, R., Desidera, S., D'Orazi, V., Flasseur, O., Barbieri, M., Benisty, M., Henning, Th., Ligi, R., Sissa, E., Vigan, A., Zurlo, A., Bonnefoy, M., Cantalloube, F., Chauvin, G., Cheetham, A. C., De Caprio, V., Delorme, P., Feldt, M., Fusco, T., Gluck, L., Hagelberg, J., Lazzoni, C., Madec, F., Maire, A.-L., Ménard, F., Meyer, M. R., Ramos, J., Rickman, E. L., Rouan, D., Schmidt, T., van der Plas, G., D’Orazi, V., De Caprio, V, Van der Plas, G, Wisniewski, John P., Kowalski, Adam F., Davenport, James R. A., Schneider, Glenn, Grady, Carol A., Hebb, Leslie, Lawson, Kellen D., Augereau, Jean-Charles, Boccaletti, A., Brown, Alexander, Debes, John H., Gaspar, Andras, Henning, Thomas K., Hines, Dean C., Kuchner, Marc J., Lagrange, Anne-Marie, Milli, Julien, Sezestre, Elie, Stark, Christopher C., Thalmann, Christian, Wisniewski, John, Kowalski, Adam, Davenport, James, Grady, Carol, Lawson, Kellen, Debes, John, Henning, Thomas, Hines, Dean, Kuchner, Marc, Stark, Christopher, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
planets and satellites: detection, 010504 meteorology & atmospheric sciences, planets and satellites: dynamical evolution and stability, stars: individual: HD 117214, stars: individual: AB Aur, techniques: image processing, Astrophysics, M dwarf stars, 01 natural sciences, stars: individual: HD 19467, accretion, Debris disks, Astrophysics::Solar and Stellar Astrophysics, infrared: planetary systems, 010303 astronomy & astrophysics, instrumentation: spectrographs, Physics, Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: atmospheres, [PHYS]Physics [physics], planet-disk interactions, accretion disks, stars: individual: HD 32297, protoplanetary disks, stars: individual: Proxima, Exoplanet, Astrophysics - Solar and Stellar Astrophysics, binaries: general, techniques: imaging spectroscopy, techniques: interferometric, stars individual: HIP 65875, planets and satellites: individual: Proxima c, Astrophysics::Earth and Planetary Astrophysics, methods: observational, radio lines: stars, binaries: spectroscopic, brown dwarfs, (stars:) planetary systems, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Brown dwarf, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, stars: pre-main sequence, instrumentation: adaptive optics, planets and satellites: terrestrial planets, stars: individual: PDS70, instrumentation: high angular resolution, 0103 physical sciences, planetary systems, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Debris disk, polarization, HD 163296, Stellar rotation, Starspot, techniques: high angular resolution, Astronomy and Astrophysics, Planetary system, methods: data analysis, binaries: visual, Starspots, techniques: polarimetric, Polar wind, Space and Planetary Science, Circumstellar disks, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Heliosphere, Astrophysics - Earth and Planetary Astrophysics
Abstract

The Astrophysical Journal Letters, 883 (1), ISSN:1967-2014, ISSN:2041-8213

Published
2019

172. A search for accreting young companions embedded in circumstellar disks

Author

Cugno, G., Quanz, S. P., Hunziker, S., Stolker, T., Schmid, H. M., Avenhaus, H., Baudoz, P., Bohn, A. J., Bonnefoy, M., Buenzli, E., Chauvin, G., Cheetham, A., Desidera, S., Dominik, C., Feautrier, P., Feldt, M., Ginski, C., Girard, J. H., Gratton, R., Hagelberg, J., Hugot, E., Janson, M., Lagrange, A.-M., Langlois, M., Magnard, Y., Maire, A.-L., Ménard, F., Meyer, M., Milli, J., Mordasini, C., Pinte, C., Pragt, J., Roelfsema, R., Rigal, F, Szulagyi, J., Van Boekel, R., van der Plas, G., Vigan, Arthur, Wahhaj, Z., Zurlo, A., Girard, H., Institute for Particle Physics and Astrophysics [ETH Zürich] (IPA), Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Stockholm University, European Southern Observatory (ESO), Physikalisches Institut [Bern], Universität Bern [Bern], NOVA Optical Infrared Instrumentation Group, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université de Genève = University of Geneva (UNIGE), Universiteit Leiden, Universität Bern [Bern] (UNIBE), and ANR-16-CE31-0013,PLANET-FORMING-DISKS,De meilleurs modèles pour de meilleures données(2016)

Subjects
planet-disk interactions, planets and satellites: detection, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], techniques: high angular resolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], planetary systems
Abstract

International audience; Context. In recent years, our understanding of giant planet formation progressed substantially. There have even been detections of a few young protoplanet candidates still embedded in the circumstellar disks of their host stars. The exact physics that describes the accretion of material from the circumstellar disk onto the suspected circumplanetary disk and eventually onto the young, forming planet is still an open question. Aims: We seek to detect and quantify observables related to accretion processes occurring locally in circumstellar disks, which could be attributed to young forming planets. We focus on objects known to host protoplanet candidates and/or disk structures thought to be the result of interactions with planets. Methods: We analyzed observations of six young stars (age 3.5-10 Myr) and their surrounding environments with the SPHERE/ZIMPOL instrument on the Very Large Telescope (VLT) in the Hα filter (656 nm) and a nearby continuum filter (644.9 nm). We applied several point spread function (PSF) subtraction techniques to reach the highest possible contrast near the primary star, specifically investigating regions where forming companions were claimed or have been suggested based on observed disk morphology. Results: We redetect the known accreting M-star companion HD142527 B with the highest published signal to noise to date in both Hα and the continuum. We derive new astrometry (r=62.8-2.7+2.1 mas and PA=(98.7±1.8)°) and photometry (ΔN_Ha = 6.3-0.3+0.2 mag, ΔB_Ha = 6.7 ± 0.2 mag and ΔCnt_Ha = 7.3-0.2+0.3 mag) for the companion in agreement with previous studies, and estimate its mass accretion rate (Ṁ ≈ 1-2 × 10-10 M⊙yr-1). A faint point-like source around HD135344 B (SAO206462) is also investigated, but a second deeper observation is required to reveal its nature. No other companions are detected. In the framework of our assumptions we estimate detection limits at the locations of companion candidates around HD100546, HD169142, and MWC 758 and calculate that processes involving Hα fluxes larger than 8 × 10-14-10-15 erg s-1 cm-2 (Ṁ > 10-10-10-12 M⊙yr-1) can be excluded. Furthermore, flux upper limits of 10-14-10-15 erg s-1 cm-2 (Ṁ < 10-11-10-12 M⊙yr-1) are estimated within the gaps identified in the disks surrounding HD135344 B and TW Hya. The derived luminosity limits exclude Hα signatures at levels similar to those previously detected for the accreting planet candidate LkCa15 b. Based on observations collected at the Paranal Observatory, ESO (Chile). Program ID: 096.C-0248(B), 096.C-0267(A),096.C-0267(B), 095.C-0273(A), 095.C-0298(A).The reduced images (FITS files) are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/622/A156

Published
2019

173. SPHERE dynamical and spectroscopic characterization of HD 142527B

Author

Claudi, R., Maire, A.-L., Mesa, D., Cheetham, A., Fontanive, C., Gratton, R., Zurlo, A., Avenhaus, H., Bhowmik, T., Biller, B., Boccaletti, A., Bonavita, M., Bonnefoy, M., Cascone, E., Chauvin, G., Delboulbé, A., Desidera, S., D'Orazi, V., Feautrier, P., Feldt, M., Flammini Dotti, F., Girard, J. H., Giro, E., Janson, M., Hagelberg, J., Keppler, M., Kopytova, T., Lacour, S., Lagrange, A.-M., Langlois, M., Lannier, J., Le Coroller, H., Ménard, F., Messina, S., Meyer, M., Millward, M., Olofsson, J., PAVLOV, A., Peretti, S., Perrot, C., Pinte, C., Pragt, J., Ramos, J., Rochat, S., Rodet, L., Roelfsema, R., Rouan, D., Salter, G., Schmidt, T., Sissa, E., Thebault, P., Udry, S., Vigan, Arthur, D’Orazi, V., Girard, H., INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institute for Particle Physics and Astrophysics [ETH Zürich] (IPA), Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)-Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Capodimonte (OAC), Stockholm University, Geneva Observatory, University of Geneva [Switzerland], NOVA Optical Infrared Instrumentation Group, Universidade de Lisboa (ULISBOA), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université de Genève = University of Geneva (UNIGE), Observatoire de Paris, Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Universidade de Lisboa = University of Lisbon (ULISBOA)

Subjects
010504 meteorology & atmospheric sciences, media_common.quotation_subject, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), Type (model theory), 01 natural sciences, Omega, Spectral line, instrumentation: high angular resolution, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Eccentricity (behavior), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, Physics, Orbital elements, Earth and Planetary Astrophysics (astro-ph.EP), stars: formation, Accretion (meteorology), protoplanetary disks, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, techniques: imaging spectroscopy, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], stars: individual: HD 142527, Energy (signal processing), Astrophysics - Earth and Planetary Astrophysics
Abstract

We detect the accreting low-mass companion HD142527B at a separation of 73 mas (11.4 au) from the star. No other companions with mass greater than 10 MJ are visible in the field of view of IFS (\sim 100 au centered on the star) or in the IRDIS field of view (\sim 400 au centered on the star). Measurements from IFS, SAM IFS, and IRDIS suggest an M6 spectral type for HD142527B, with an uncertainty of one spectral subtype, compatible with an object of M=0.11 \pm 0.06 MSun and R=0.15 \pm 0.07 RSun. The determination of the mass remains a challenge using contemporary evolutionary models, as they do not account for the energy input due to accretion from infalling material. We consider that the spectral type of the secondary may also be earlier than the type we derived from IFS spectra. From dynamical considerations, we further constrain the mass to 0.26^{+0.16}_{-0.14} MSun , which is consistent with both our spectroscopic analysis and the values reported in the literature. Following previous methods, the lower and upper dynamical mass values correspond to a spectral type between M2.5 and M5.5 for the companion. By fitting the astrometric points, we find the following orbital parameters: a period of P=35-137 yr; an inclination of i=121-130 deg.; , a value of Omega=124-135 deg for the longitude of node, and an 68% confidence interval of \sim 18 - 57 au for the separation at periapsis. Eccentricity and time at periapsis passage exhibit two groups of values: \sim0.2-0.45 and \sim0.45-0.7 for e, and \sim 2015-2020 and \sim2020-2022 for T_0. While these orbital parameters might at first suggest that HD142527B is not the companion responsible for the outer disk truncation, a previous hydrodynamical analysis of this system showed that they are compatible with a companion that is able to produce the large cavity and other observed features., Comment: 15, pages, 11 figures, Accepted for publication on Astronomy and Astrophysics

Published
2019

174. PDS 70 b: Evidence for a circumplanetary disc around the fIrst directly imaged protoplanet

Author

Christiaens, V., Cantalloube, F., Casassus, S., Price, D., Absil, O., Pinte, C., Girard, J., and Montesinos, M.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The observed properties of the major moons of Jupiter — and of other gas giants — have suggested that they formed within a circumplanetary disc. This prediction has been supported by theoretical calculations and numerical simulations of increasing complexity over the past few decades. Despite intensive search, circumplanetary discs had until now eluded detection. In this talk, I will present the first observational evidence for a circumplanetary disc, around recently imaged protoplanet PDS 70 b. Our detection is based on a new near-IR spectrum acquired with VLT/SINFONI. We tested several hypotheses (atmospheric emission alone, variable extinction, combination of atmospheric and circumplanetary disc emission) to explain the spectrum and show that models considering atmospheric emission alone consistently underpredict the longward portion of the spectrum. Our best fit is obtained with a combined atmospheric and circumplanetary disc model, with emission from the circumplanetary disc accounting for the apparent excess IR emission.

Published
2019

175. A search for accreting young companions embedded in circumstellar disks High-contrast H alpha imaging with VLT/SPHERE

Author

Cugno, G., Quanz, S. P., Hunziker, S., Stolker, T., Schmid, H. M., Avenhaus, H., Baudoz, P., Bohn, A. J., Bonnefoy, M., Buenzli, E., Chauvin, G., Cheetham, A., Desidera, S., Dominik, C., Feautrier, P., Feldt, M., Ginski, C., Girard, J. H., Gratton, R., Hagelberg, J., Hugot, E., Janson, Markus, Lagrange, A. -M., Langlois, M., Magnard, Y., Maire, A. -L., Menard, F., Meyer, M., Milli, J., Mordasini, C., Pinte, C., Pragt, J., Roelfsema, R., Rigal, F., Szulagyi, J., van Boekel, R., van der Plas, G., Vigan, A., Wahhaj, Z., Zurlo, A., Cugno, G., Quanz, S. P., Hunziker, S., Stolker, T., Schmid, H. M., Avenhaus, H., Baudoz, P., Bohn, A. J., Bonnefoy, M., Buenzli, E., Chauvin, G., Cheetham, A., Desidera, S., Dominik, C., Feautrier, P., Feldt, M., Ginski, C., Girard, J. H., Gratton, R., Hagelberg, J., Hugot, E., Janson, Markus, Lagrange, A. -M., Langlois, M., Magnard, Y., Maire, A. -L., Menard, F., Meyer, M., Milli, J., Mordasini, C., Pinte, C., Pragt, J., Roelfsema, R., Rigal, F., Szulagyi, J., van Boekel, R., van der Plas, G., Vigan, A., Wahhaj, Z., and Zurlo, A.

Abstract

Context. In recent years, our understanding of giant planet formation progressed substantially. There have even been detections of a few young protoplanet candidates still embedded in the circumstellar disks of their host stars. The exact physics that describes the accretion of material from the circumstellar disk onto the suspected circumplanetary disk and eventually onto the young, forming planet is still an open question. Aims. We seek to detect and quantify observables related to accretion processes occurring locally in circumstellar disks, which could be attributed to young forming planets. We focus on objects known to host protoplanet candidates and/or disk structures thought to be the result of interactions with planets. Methods. We analyzed observations of six young stars (age 3.5-10 Myr) and their surrounding environments with the SPHERE/ZIMPOL instrument on the Very Large Telescope (VLT) in the H alpha filter (656 nm) and a nearby continuum filter (644.9 nm). We applied several point spread function (PSF) subtraction techniques to reach the highest possible contrast near the primary star, specifically investigating regions where forming companions were claimed or have been suggested based on observed disk morphology. Results. We redetect the known accreting M-star companion HD142527 B with the highest published signal to noise to date in both H alpha and the continuum. We derive new astrometry (r = 62.8(-2.7)(+2.1)mas and PA = (98.7 +/- 1.8)degrees) and photometry (Delta N_Ha = 6.3-(+0.2)(0.3) mag, Delta B_Ha = 6.7 +/- 0.2 mag and Delta Cnt_Ha= 7.3(-0.2)(+0.3) mag) for the companion in agreement with previous studies, and estimate its mass accretion rate (M approximate to 1-2 x 10(-10) M-circle dot yr(-1)). A faint point-like source around HD135344 B (SA0206462) is also investigated, but a second deeper observation is required to reveal its nature. No other companions are detected. In the framework of our assumptions we estimate detection limits at the loc

Published
2019
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176. SPHERE dynamical and spectroscopic characterization of HD142527B

Author

Claudi, R., Maire, A. -L., Mesa, D., Cheetham, A., Fontanive, C., Gratton, R., Zurlo, A., Avenhaus, H., Bhowmik, T., Biller, B., Boccaletti, A., Bonavita, M., Bonnefoy, M., Cascone, E., Chauvin, G., Delboulbe, A., Desidera, S., D'Orazi, V., Feautrier, P., Feldt, M., Dotti, F. Flammini, Girard, J. H., Giro, E., Janson, Markus, Hagelberg, J., Keppler, M., Kopytova, T., Lacour, S., Lagrange, A. -M., Langlois, M., Lannier, J., Le Coroller, H., Menard, F., Messina, S., Meyer, M., Millward, M., Olofsson, J., Pavlov, A., Peretti, S., Perrot, C., Pinte, C., Pragt, J., Ramos, J., Rochat, S., Rodet, L., Roelfsema, R., Rouan, D., Salter, G., Schmidt, T., Sissa, E., Thebault, P., Udry, S., Vigan, A., Claudi, R., Maire, A. -L., Mesa, D., Cheetham, A., Fontanive, C., Gratton, R., Zurlo, A., Avenhaus, H., Bhowmik, T., Biller, B., Boccaletti, A., Bonavita, M., Bonnefoy, M., Cascone, E., Chauvin, G., Delboulbe, A., Desidera, S., D'Orazi, V., Feautrier, P., Feldt, M., Dotti, F. Flammini, Girard, J. H., Giro, E., Janson, Markus, Hagelberg, J., Keppler, M., Kopytova, T., Lacour, S., Lagrange, A. -M., Langlois, M., Lannier, J., Le Coroller, H., Menard, F., Messina, S., Meyer, M., Millward, M., Olofsson, J., Pavlov, A., Peretti, S., Perrot, C., Pinte, C., Pragt, J., Ramos, J., Rochat, S., Rodet, L., Roelfsema, R., Rouan, D., Salter, G., Schmidt, T., Sissa, E., Thebault, P., Udry, S., and Vigan, A.

Abstract

Aims. HD142527 is one of the most frequently studied Herbig Ae/Be stars with a transitional disk that hosts a large cavity that is up to about 100 au in radius. For this reason, it has been included in the guaranteed time observation (GTO) SpHere INfrared survey for Exoplanets (SHINE) as part of the Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) at the Very Large Telescope (VLT) in order to search for low-mass companions that might explain the presence of the gap. SHINE is a large survey within about 600 young nearby stars are observed with SPHERE with the aim to constrain the occurrence and orbital properties of the giant planet population at large (>5 au) orbital separation around young stars. Methods. We used the IRDIFS observing mode of SPHERE (IRDIS short for infrared dual imaging and spectrograph plus IFS or integral field spectrograph) without any coronagraph in order to search for and characterize companions as close as 30 mas of the star. Furthermore, we present the first observations that ever used the sparse aperture mask (SAM) for SPHERE both in IRDIFS and IRDIFS_EXT modes. All the data were reduced using the dedicated SPHERE pipeline and dedicated algorithms that make use of the principal component analysis (PCA) and reference differential imaging (RDI) techniques. Results. We detect the accreting low-mass companion HD142527B at a separation of 73 mas (11.4 au) from the star. No other companions with mass greater than 10 M-J are visible in the field of view of IFS (similar to 100 au centered on the star) or in the IRDIS field of view (similar to 400 au centered on the star). Measurements from IFS, SAM IFS, and IRDIS suggest an M6 spectral type for HD142527B, with an uncertainty of one spectral subtype, compatible with an object of M = 0.11 +/- 0.06 M-circle dot and R = 0.15 +/- 0.07 R-circle dot. The determination of the mass remains a challenge using contemporary evolutionary models, as they do not account for the energy input due to

Published
2019
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177. Resolving faint structures in the debris disk around TWA 7

Author

Olofsson, J., van Holstein, R. G., Boccaletti, A., Janson, M., Thebault, P., Gratton, R., Lazzoni, C., Kral, Q., Bayo, A., Canovas, H., Caceres, C., Ginski, C., Pinte, C., Asensio-Torres, R., Chauvin, G., Desidera, S., Henning, Th., Langlois, M., Milli, J., Schlieder, J. E., Schreiber, M. R., Augereau, J.-C., Bonnefoy, M., Buenzli, E., Brandner, W., Durkan, S., Engler, N., Feldt, M., Godoy, N., Grady, C., Hagelberg, J., Lagrange, A.-M., Lannier, J., Ligi, R., Maire, A.-L., Mawet, D., Ménard, F., Mesa, D., Mouillet, D., Peretti, S., Perrot, C., Salter, G., Schmidt, T., Sissa, E., Thalmann, C., Vigan, Arthur, Abe, L., Feautrier, P., Le Mignant, D., Moulin, T., PAVLOV, A., Rabou, P., Rousset, G., Roux, A., Schreiber, R., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Stockholm University, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Geneva Observatory, University of Geneva [Switzerland], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Copernicus Astronomical Center of the Polish Academy of Sciences (CAMK), Polish Academy of Sciences (PAN), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Universiteit Leiden, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université de Genève = University of Geneva (UNIGE), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), ANR-16-CE31-0013,PLANET-FORMING-DISKS,De meilleurs modèles pour de meilleures données(2016), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics - Solar and Stellar Astrophysics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], instrumentation: high angular resolution, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, instrumentation: polarimeters, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, circumstellar matter, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Debris disks are the intrinsic by-products of the star and planet formation processes. Most likely due to instrumental limitations and their natural faintness, little is known about debris disks around low-mass stars, especially when it comes to spatially resolved observations. We present new VLT/SPHERE IRDIS Dual-Polarization Imaging (DPI) observations in which we detect the dust ring around the M2 spectral type star TWA\,7. Combined with additional Angular Differential Imaging observations we aim at a fine characterization of the debris disk and setting constraints on the presence of low-mass planets. We model the SPHERE DPI observations and constrain the location of the small dust grains, as well as the spectral energy distribution of the debris disk, using the results inferred from the observations, and perform simple N-body simulations. We find that the dust density distribution peaks at 25 au, with a very shallow outer power-law slope, and that the disk has an inclination of 13 degrees with a position angle of 90 degrees East of North. We also report low signal-to-noise detections of an outer belt at a distance of ~52 au from the star, of a spiral arm in the Southern side of the star, and of a possible dusty clump at 3.9 au. These findings seem to persist over timescales of at least a year. Using the intensity images, we do not detect any planets in the close vicinity of the star, but the sensitivity reaches Jovian planet mass upper limits. We find that the SED is best reproduced with an inner disk at 7 au and another belt at 25 au. We report the detections of several unexpected features in the disk around TWA\,7. A yet undetected 100 M$_\oplus$ planet with a semi-major axis at 20-30 au could possibly explain the outer belt as well as the spiral arm. We conclude that stellar winds are unlikely to be responsible for the spiral arm., Comment: Accepted by A&A, 17 pages

Published
2018

178. Resolving faint structures in the debris disk around TWA 7. Tentative detections of an outer belt, a spiral arm, and a dusty cloud

Author

Olofsson, J., van Holstein, R. G., Boccaletti, A., Janson, M., Thébault, P., Gratton, R., Lazzoni, C., Kral, Q., Bayo, A., Canovas, H., Caceres, C., Ginski, C., Pinte, C., Asensio-Torres, R., Chauvin, G., Desidera, S., Henning, Th., Langlois, M., Milli, J., Schlieder, J. E., Schreiber, M. R., Augereau, J. -C., Bonnefoy, M., Buenzli, E., Brandner, W., Durkan, S., Engler, N., Feldt, M., Godoy, N., Grady, C., Hagelberg, J., Lagrange, A. -M., Lannier, J., Ligi, R., Maire, A. -L., Mawet, D., F. Ménard, D. Mesa, Mouillet, D., Peretti, S., Perrot, C., Salter, G., Schmidt, T., Sissa, E., Thalmann, C., Vigan, A., Abe, L., Feautrier, P., Le Mignant, D., Moulin, T., Pavlov, A., Rabou, P., and Roux, G. Rousset and A.

Published
2018

179. VLT/SPHERE exploration of the young multiplanetary system PDS70

Author

Mesa, D., primary, Keppler, M., additional, Cantalloube, F., additional, Rodet, L., additional, Charnay, B., additional, Gratton, R., additional, Langlois, M., additional, Boccaletti, A., additional, Bonnefoy, M., additional, Vigan, A., additional, Flasseur, O., additional, Bae, J., additional, Benisty, M., additional, Chauvin, G., additional, de Boer, J., additional, Desidera, S., additional, Henning, T., additional, Lagrange, A.-M., additional, Meyer, M., additional, Milli, J., additional, Müller, A., additional, Pairet, B., additional, Zurlo, A., additional, Antoniucci, S., additional, Baudino, J.-L., additional, Brown Sevilla, S., additional, Cascone, E., additional, Cheetham, A., additional, Claudi, R. U., additional, Delorme, P., additional, D’Orazi, V., additional, Feldt, M., additional, Hagelberg, J., additional, Janson, M., additional, Kral, Q., additional, Lagadec, E., additional, Lazzoni, C., additional, Ligi, R., additional, Maire, A.-L., additional, Martinez, P., additional, Menard, F., additional, Meunier, N., additional, Perrot, C., additional, Petrus, S., additional, Pinte, C., additional, Rickman, E. L., additional, Rochat, S., additional, Rouan, D., additional, Samland, M., additional, Sauvage, J.-F., additional, Schmidt, T., additional, Udry, S., additional, Weber, L., additional, and Wildi, F., additional

Published
2019
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180. Kinematic detection of a planet carving a gap in a protoplanetary disk

Author

Pinte, C., primary, van der Plas, G., additional, Ménard, F., additional, Price, D. J., additional, Christiaens, V., additional, Hill, T., additional, Mentiplay, D., additional, Ginski, C., additional, Choquet, E., additional, Boehler, Y., additional, Duchêne, G., additional, Perez, S., additional, and Casassus, S., additional

Published
2019
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182. Optical polarised phase function of the HR 4796A dust ring

Author

Milli, J., primary, Engler, N., additional, Schmid, H. M., additional, Olofsson, J., additional, Ménard, F., additional, Kral, Q., additional, Boccaletti, A., additional, Thébault, P., additional, Choquet, E., additional, Mouillet, D., additional, Lagrange, A.-M., additional, Augereau, J.-C., additional, Pinte, C., additional, Chauvin, G., additional, Dominik, C., additional, Perrot, C., additional, Zurlo, A., additional, Henning, T., additional, Beuzit, J.-L., additional, Avenhaus, H., additional, Bazzon, A., additional, Moulin, T., additional, Llored, M., additional, Moeller-Nilsson, O., additional, Roelfsema, R., additional, and Pragt, J., additional

Published
2019
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183. Separating extended disc features from the protoplanet in PDS 70 using VLT/SINFONI

Author

Christiaens, V, primary, Casassus, S, additional, Absil, O, additional, Cantalloube, F, additional, Gomez Gonzalez, C, additional, Girard, J, additional, Ramírez, R, additional, Pairet, B, additional, Salinas, V, additional, Price, D J, additional, Pinte, C, additional, Quanz, S P, additional, Jordán, A, additional, Mawet, D, additional, and Wahhaj, Z, additional

Published
2019
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184. Consistent dust and gas models for protoplanetary disks

Author

Dionatos, O., primary, Woitke, P., additional, Güdel, M., additional, Degroote, P., additional, Liebhart, A., additional, Anthonioz, F., additional, Antonellini, S., additional, Baldovin-Saavedra, C., additional, Carmona, A., additional, Dominik, C., additional, Greaves, J., additional, Ilee, J. D., additional, Kamp, I., additional, Ménard, F., additional, Min, M., additional, Pinte, C., additional, Rab, C., additional, Rigon, L., additional, Thi, W. F., additional, and Waters, L. B. F. M., additional

Published
2019
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186. Spatial segregation of dust grains in transition disks

Author

Villenave, M., primary, Benisty, M., additional, Dent, W. R. F., additional, Ménard, F., additional, Garufi, A., additional, Ginski, C., additional, Pinilla, P., additional, Pinte, C., additional, Williams, J. P., additional, de Boer, J., additional, Morino, J.-I., additional, Fukagawa, M., additional, Dominik, C., additional, Flock, M., additional, Henning, T., additional, Juhász, A., additional, Keppler, M., additional, Muro-Arena, G., additional, Olofsson, J., additional, Pérez, L. M., additional, van der Plas, G., additional, Zurlo, A., additional, Carle, M., additional, Feautrier, P., additional, Pavlov, A., additional, Pragt, J., additional, Ramos, J., additional, Sauvage, J.-F., additional, Stadler, E., additional, and Weber, L., additional

Published
2019
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187. SPHERE dynamical and spectroscopic characterization of HD142527B

Author

Claudi, R., Maire, A. -L., Mesa, D., Cheetham, A., Fontanive, C., Gratton, R., Zurlo, A., Avenhaus, H., Bhowmik, T., Biller, B., Boccaletti, A., Bonavita, M., Bonnefoy, M., Cascone, E., Chauvin, G., Delboulbè, A., Desidera, S., D'Orazi, V., Feautrier, P., Feldt, M., Dotti, F. Flammini, Girard, J. H., Giro, E., Janson, M., Hagelberg, J., Keppler, M., Kopytova, T., Lacour, S., Lagrange, A. -M., Langlois, M., Lannier, J., Coroller, H. Le, Menard, F., Messina, S., Meyer, M., Millward, M., Olofsson, J., Pavlov, A., Peretti, S., Perrot, C., Pinte, C., Pragt, J., Ramos, J., Rochat, S., Rodet, L., Roelfsema, R., Rouan, D., Salter, G., Schmidt, T., Sissa, E., Thebault, P., Udry, S., Vigan, A., Claudi, R., Maire, A. -L., Mesa, D., Cheetham, A., Fontanive, C., Gratton, R., Zurlo, A., Avenhaus, H., Bhowmik, T., Biller, B., Boccaletti, A., Bonavita, M., Bonnefoy, M., Cascone, E., Chauvin, G., Delboulbè, A., Desidera, S., D'Orazi, V., Feautrier, P., Feldt, M., Dotti, F. Flammini, Girard, J. H., Giro, E., Janson, M., Hagelberg, J., Keppler, M., Kopytova, T., Lacour, S., Lagrange, A. -M., Langlois, M., Lannier, J., Coroller, H. Le, Menard, F., Messina, S., Meyer, M., Millward, M., Olofsson, J., Pavlov, A., Peretti, S., Perrot, C., Pinte, C., Pragt, J., Ramos, J., Rochat, S., Rodet, L., Roelfsema, R., Rouan, D., Salter, G., Schmidt, T., Sissa, E., Thebault, P., Udry, S., and Vigan, A.

Abstract

We detect the accreting low-mass companion HD142527B at a separation of 73 mas (11.4 au) from the star. No other companions with mass greater than 10 MJ are visible in the field of view of IFS (\sim 100 au centered on the star) or in the IRDIS field of view (\sim 400 au centered on the star). Measurements from IFS, SAM IFS, and IRDIS suggest an M6 spectral type for HD142527B, with an uncertainty of one spectral subtype, compatible with an object of M=0.11 \pm 0.06 MSun and R=0.15 \pm 0.07 RSun. The determination of the mass remains a challenge using contemporary evolutionary models, as they do not account for the energy input due to accretion from infalling material. We consider that the spectral type of the secondary may also be earlier than the type we derived from IFS spectra. From dynamical considerations, we further constrain the mass to 0.26^{+0.16}_{-0.14} MSun , which is consistent with both our spectroscopic analysis and the values reported in the literature. Following previous methods, the lower and upper dynamical mass values correspond to a spectral type between M2.5 and M5.5 for the companion. By fitting the astrometric points, we find the following orbital parameters: a period of P=35-137 yr; an inclination of i=121-130 deg.; , a value of Omega=124-135 deg for the longitude of node, and an 68% confidence interval of \sim 18 - 57 au for the separation at periapsis. Eccentricity and time at periapsis passage exhibit two groups of values: \sim0.2-0.45 and \sim0.45-0.7 for e, and \sim 2015-2020 and \sim2020-2022 for T_0. While these orbital parameters might at first suggest that HD142527B is not the companion responsible for the outer disk truncation, a previous hydrodynamical analysis of this system showed that they are compatible with a companion that is able to produce the large cavity and other observed features., Comment: 15, pages, 11 figures, Accepted for publication on Astronomy and Astrophysics

Published
2018
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188. A search for accreting young companions embedded in circumstellar disks: High-contrast H$\alpha$ imaging with VLT/SPHERE

Author

Cugno, G., Quanz, S. P., Hunziker, S., Stolker, T., Schmid, H. M., Avenhaus, H., Baudoz, P., Bohn, A. J., Bonnefoy, M., Buenzli, E., Chauvin, G., Cheetham, A., Desidera, S., Dominik, C., Feautrier, P., Feldt, M., Ginski, C., Girard, J. H., Gratton, R., Hagelberg, J., Hugot, E., Janson, M., Lagrange, A. -M., Langlois, M., Magnard, Y., Maire, A. -L., Menard, F., Meyer, M., Milli, J., Mordasini, C., Pinte, C., Pragt, J., Roelfsema, R., Rigal, F., Szulágyi, J., van Boekel, R., van der Plas, G., Vigan, A., Wahhaj, Z., Zurlo, A., Cugno, G., Quanz, S. P., Hunziker, S., Stolker, T., Schmid, H. M., Avenhaus, H., Baudoz, P., Bohn, A. J., Bonnefoy, M., Buenzli, E., Chauvin, G., Cheetham, A., Desidera, S., Dominik, C., Feautrier, P., Feldt, M., Ginski, C., Girard, J. H., Gratton, R., Hagelberg, J., Hugot, E., Janson, M., Lagrange, A. -M., Langlois, M., Magnard, Y., Maire, A. -L., Menard, F., Meyer, M., Milli, J., Mordasini, C., Pinte, C., Pragt, J., Roelfsema, R., Rigal, F., Szulágyi, J., van Boekel, R., van der Plas, G., Vigan, A., Wahhaj, Z., and Zurlo, A.

Abstract

Aims: We want to detect and quantify observables related to accretion processes occurring locally in circumstellar disks, which could be attributed to young forming planets. We focus on objects known to host protoplanet candidates and/or disk structures thought to be the result of interactions with planets. Methods: We analyzed observations of 6 young stars (age $3.5-10$ Myr) and their surrounding environments with the SPHERE/ZIMPOL instrument on the VLT in the H$\alpha$ filter (656 nm) and a nearby continuum filter (644.9 nm). Results: We re-detect the known accreting M-star companion HD142527 B with the highest published signal to noise to date in both H$\alpha$ and the continuum. We derive new astrometry ($r = 62.8^{+2.1}_{-2.7}$ mas and $\text{PA} = (98.7\,\pm1.8)^\circ$) and photometry ($\Delta$N_Ha=$6.3^{+0.2}_{-0.3}$ mag, $\Delta$B_Ha=$6.7\pm0.2$ mag and $\Delta$Cnt_Ha=$7.3^{+0.3}_{-0.2}$ mag) for the companion in agreement with previous studies, and estimate its mass accretion rate ($\dot{M}\approx1-2\,\times10^{-10}\,M_\odot\text{ yr}^{-1}$). A faint point-like source around HD135344 B (SAO206462) is also investigated, but a second deeper observation is required to reveal its nature. No other companions are detected. In the framework of our assumptions we estimate detection limits at the locations of companion candidates around HD100546, HD169142 and MWC758 and calculate that processes involving H$\alpha$ fluxes larger than $\sim8\times10^{-14}-10^{-15}\,\text{erg/s/cm}^2$ ($\dot{M}>10^{-10}-10^{-12}\,M_\odot\text{ yr}^{-1}$) can be excluded. Furthermore, flux upper limits of $\sim10^{-14}-10^{-15}\,\text{erg/s/cm}^2$ ($\dot{M}<10^{-11}-10^{-12}\,M_\odot \text{ yr}^{-1}$) are estimated within the gaps identified in the disks surrounding HD135344B and TW Hya., Comment: Accepted for publication in A&A (20 pages, 18 figures)

Published
2018
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189. Consistent dust and gas models for protoplanetary disks III. Models for selected objects from the FP7 DIANA project

Author

Woitke, P., Kamp, I., Antonellini, S., Anthonioz, F., Baldovin-Saveedra, C., Carmona, A., Dionatos, O., Dominik, C., Greaves, J., Güdel, M., Ilee, J. D., Liebhardt, A., Menard, F., Min, M., Pinte, C., Rab, C., Rigon, L., Thi, W. -F., Thureau, N., Waters, L. B. F. M., Woitke, P., Kamp, I., Antonellini, S., Anthonioz, F., Baldovin-Saveedra, C., Carmona, A., Dionatos, O., Dominik, C., Greaves, J., Güdel, M., Ilee, J. D., Liebhardt, A., Menard, F., Min, M., Pinte, C., Rab, C., Rigon, L., Thi, W. -F., Thureau, N., and Waters, L. B. F. M.

Abstract

The European FP7 project DIANA has performed a coherent analysis of a large set of observations from protoplanetary disks by means of thermo-chemical disk models. The collected data include extinction-corrected stellar UV and X-ray input spectra (as seen by the disk), photometric fluxes, low and high resolution spectra, interferometric data, emission line fluxes, line velocity profiles and line maps. We define and apply a standardized modelling procedure to simultaneously fit all these data by state-of-the-art modelling codes (ProDiMo, MCFOST, MCMax) which solve the continuum and line radiative transfer, disk chemistry, and the heating & cooling balance for both the gas and the dust. We allow for up to two radial disk zones to obtain our best-fitting models that have about 20 free parameters. This approach is novel and unique in its completeness and level of consistency. In this paper, we present the results from pure SED fitting for 27 objects and from the all inclusive DIANA-standard models for 14 objects. We fit most infrared to millimeter emission line fluxes within a factor better than 3, simultaneously with SED, PAH features and radial brightness profiles extracted from images at various wavelengths. Our analysis shows a number of Herbig Ae and T Tauri stars with very cold and massive outer disks which are situated at least partly in the shadow of a tall and gas-rich inner disk. The disk masses derived are often in excess to previously published values, since these disks are partially optically thick even at millimeter wavelength and so cold that they emit less than in the Rayleigh-Jeans limit. Some line observations cannot be reproduced by the models, probably caused by foreground cloud absorption or object variability. Our data collection, the fitted physical disk parameters as well as the full model output are available at an online database (http://www.univie.ac.at/diana)., Comment: 70 pages, 35 figures, 22 tables, accepted by PASP

Published
2018
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190. Submillimetre dust polarisation and opacity in the HD163296 protoplanetary ring system

Author

Dent, W. R. F., Pinte, C., Cortes, P. C., Ménard, F., Hales, A., Fomalont, E., de Gregorio-Monsalvo, I., Dent, W. R. F., Pinte, C., Cortes, P. C., Ménard, F., Hales, A., Fomalont, E., and de Gregorio-Monsalvo, I.

Abstract

We present ALMA images of the sub-mm continuum polarisation and spectral index of the protoplanetary ringed disk HD163296. The polarisation fraction at 870{\mu}m is measured to be ~0.9% in the central core and generally increases with radius along the disk major axis. It peaks in the gaps between the dust rings, and the largest value (~4%) is found between rings 1 and 2. The polarisation vectors are aligned with the disk minor axis in the central core, but become more azimuthal in the gaps, twisting by up to +/-9degrees in the gap between rings 1 and 2. These general characteristics are consistent with a model of self-scattered radiation in the ringed structure, without requiring an additional dust alignment mechanism. The 870/1300{\mu}m dust spectral index exhibits minima in the centre and the inner rings, suggesting these regions have high optical depths. However, further refinement of the dust or the disk model at higher resolution is needed to reproduce simultaneously the observed degree of polarisation and the low spectral index., Comment: 5 pages +2 pages supplemental data. v2 - revised figures and final values; conclusions unchanged

Published
2018
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191. 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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192. Kinematic evidence for an embedded protoplanet in a circumstellar disc

Author

Pinte, C., Price, D. J., Menard, F., Duchene, G., Dent, W. R. F., Hill, T., de Gregorio-Monsalvo, I., Hales, A., Mentiplay, D., Pinte, C., Price, D. J., Menard, F., Duchene, G., Dent, W. R. F., Hill, T., de Gregorio-Monsalvo, I., Hales, A., and Mentiplay, D.

Abstract

Discs of gas and dust surrounding young stars are the birthplace of planets. However, direct detection of protoplanets forming within discs has proved elusive to date. We present the detection of a large, localized deviation from Keplerian velocity in the protoplanetary disc surrounding the young star HD163296. The observed velocity pattern is consistent with the dynamical effect of a two Jupiter-mass planet orbiting at a radius $\approx$ 260au from the star., Comment: Accepted for publication to ApJL, 8 pages, 5 figures

Published
2018
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193. Modelling mid-infrared molecular emission lines from T Tauri stars

Author

Woitke, P., Min, M., Thi, W. -F., Roberts, C., Carmona, A., Kamp, I., Menard, F., Pinte, C., Woitke, P., Min, M., Thi, W. -F., Roberts, C., Carmona, A., Kamp, I., Menard, F., and Pinte, C.

Abstract

We introduce a new modelling framework called FLiTs to simulate infrared line emission spectra from protoplanetary discs. This paper focuses on the mid-IR spectral region between 9.7 um to 40 um for T Tauri stars. The generated spectra contain several tens of thousands of molecular emission lines of H2O, OH, CO, CO2, HCN, C2H2, H2 and a few other molecules, as well as the forbidden atomic emission lines of SI, SII, SIII, SiII, FeII, NeII, NeIII, ArII and ArIII. In contrast to previously published works, we do not treat the abundances of the molecules nor the temperature in the disc as free parameters, but use the complex results of detailed 2D ProDiMo disc models concerning gas and dust temperature structure, and molecular concentrations. FLiTs computes the line emission spectra by ray tracing in an efficient, fast and reliable way. The results are broadly consistent with R=600 Spitzer/IRS observational data of T Tauri stars concerning line strengths, colour, and line ratios. In order to achieve that agreement, however, we need to assume either a high gas/dust mass ratio of order 1000, or the presence of illuminated disc walls at distances of a few au. The molecules in these walls cannot be photo-dissociated easily by UV because of the large densities in the walls which favour their re-formation. Most observable molecular emission lines are found to be optically thick, rendering a standard analysis with column densities difficult. We find that the difference between gas and dust temperatures in the disc surface is important for the line formation. We briefly discuss the effects of C/O ratio and choice of chemical rate network on these results. Our analysis offers new ways to infer the chemical and temperature structure of T Tauri discs from future JWST/MIRI observations, and to possibly detect secondary illuminated disc walls based on their specific mid-IR molecular signature., Comment: accepted by A&A, 13 figures, 4 tables

Published
2018
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194. Resolving faint structures in the debris disk around TWA7

Author

Olofsson, J., van Holstein, R. G., Boccaletti, A., Janson, M., Thébault, P., Gratton, R., Lazzoni, C., Kral, Q., Bayo, A., Canovas, H., Caceres, C., Ginski, C., Pinte, C., Asensio-Torres, R., Chauvin, G., Desidera, S., Henning, Th., Langlois, M., Milli, J., Schlieder, J. E., Schreiber, M. R., Augereau, J. -C., Bonnefoy, M., Buenzli, E., Brandner, W., Durkan, S., Engler, N., Feldt, M., Godoy, N., Grady, C., Hagelberg, J., Lagrange, A. -M., Lannier, J., Ligi, R., Maire, A. -L., Mawet, D., Ménard, F., Mesa, D., Mouillet, D., Peretti, S., Perrot, C., Salter, G., Schmidt, T., Sissa, E., Thalmann, C., Vigan, A., Abe, L., Feautrier, P., Mignant, D. Le, Moulin, T., Pavlov, A., Rabou, P., Rousset, G., Roux, A., Olofsson, J., van Holstein, R. G., Boccaletti, A., Janson, M., Thébault, P., Gratton, R., Lazzoni, C., Kral, Q., Bayo, A., Canovas, H., Caceres, C., Ginski, C., Pinte, C., Asensio-Torres, R., Chauvin, G., Desidera, S., Henning, Th., Langlois, M., Milli, J., Schlieder, J. E., Schreiber, M. R., Augereau, J. -C., Bonnefoy, M., Buenzli, E., Brandner, W., Durkan, S., Engler, N., Feldt, M., Godoy, N., Grady, C., Hagelberg, J., Lagrange, A. -M., Lannier, J., Ligi, R., Maire, A. -L., Mawet, D., Ménard, F., Mesa, D., Mouillet, D., Peretti, S., Perrot, C., Salter, G., Schmidt, T., Sissa, E., Thalmann, C., Vigan, A., Abe, L., Feautrier, P., Mignant, D. Le, Moulin, T., Pavlov, A., Rabou, P., Rousset, G., and Roux, A.

Abstract

Debris disks are the intrinsic by-products of the star and planet formation processes. Most likely due to instrumental limitations and their natural faintness, little is known about debris disks around low-mass stars, especially when it comes to spatially resolved observations. We present new VLT/SPHERE IRDIS Dual-Polarization Imaging (DPI) observations in which we detect the dust ring around the M2 spectral type star TWA\,7. Combined with additional Angular Differential Imaging observations we aim at a fine characterization of the debris disk and setting constraints on the presence of low-mass planets. We model the SPHERE DPI observations and constrain the location of the small dust grains, as well as the spectral energy distribution of the debris disk, using the results inferred from the observations, and perform simple N-body simulations. We find that the dust density distribution peaks at 25 au, with a very shallow outer power-law slope, and that the disk has an inclination of 13 degrees with a position angle of 90 degrees East of North. We also report low signal-to-noise detections of an outer belt at a distance of ~52 au from the star, of a spiral arm in the Southern side of the star, and of a possible dusty clump at 3.9 au. These findings seem to persist over timescales of at least a year. Using the intensity images, we do not detect any planets in the close vicinity of the star, but the sensitivity reaches Jovian planet mass upper limits. We find that the SED is best reproduced with an inner disk at 7 au and another belt at 25 au. We report the detections of several unexpected features in the disk around TWA\,7. A yet undetected 100 M$_\oplus$ planet with a semi-major axis at 20-30 au could possibly explain the outer belt as well as the spiral arm. We conclude that stellar winds are unlikely to be responsible for the spiral arm., Comment: Accepted by A&A, 17 pages

Published
2018
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195. Dust modeling of the combined ALMA and SPHERE datasets of HD163296. Is HD163296 really a Meeus group II disk?

Author

Muro-Arena, G. A., Dominik, C., Waters, L. B. F. M., Min, M., Klarmann, L., Ginski, C., Isella, A., Benisty, M., Pohl, A., Garufi, A., Hagelberg, J., Langlois, M., Menard, F., Pinte, C., Sezestre, E., van der Plas, G., Villenave, M., Delboulbé, A., Magnard, Y., Möller-Nilsson, O., Pragt, J., Rabou, P., Roelfsema, R., Muro-Arena, G. A., Dominik, C., Waters, L. B. F. M., Min, M., Klarmann, L., Ginski, C., Isella, A., Benisty, M., Pohl, A., Garufi, A., Hagelberg, J., Langlois, M., Menard, F., Pinte, C., Sezestre, E., van der Plas, G., Villenave, M., Delboulbé, A., Magnard, Y., Möller-Nilsson, O., Pragt, J., Rabou, P., and Roelfsema, R.

Abstract

Context. Multi-wavelength observations are indispensable in studying disk geometry and dust evolution processes in protoplanetary disks. Aims. We aimed to construct a 3-dimensional model of HD 163296 capable of reproducing simultaneously new observations of the disk surface in scattered light with the SPHERE instrument and thermal emission continuum observations of the disk midplane with ALMA. We want to determine why the SED of HD 163296 is intermediary between the otherwise well-separated group I and group II Herbig stars. Methods. The disk was modelled using the Monte Carlo radiative transfer code MCMax3D. The radial dust surface density profile was modelled after the ALMA observations, while the polarized scattered light observations were used to constrain the inclination of the inner disk component and turbulence and grain growth in the outer disk. Results. While three rings are observed in the disk midplane in millimeter thermal emission at $\sim$80, 124 and 200 AU, only the innermost of these is observed in polarized scattered light, indicating a lack of small dust grains on the surface of the outer disk. We provide two models capable of explaining this difference. The first model uses increased settling in the outer disk as a mechanism to bring the small dust grains on the surface of the disk closer to the midplane, and into the shadow cast by the first ring. The second model uses depletion of the smallest dust grains in the outer disk as a mechanism for decreasing the optical depth at optical and NIR wavelengths. In the region outside the fragmentation-dominated regime, such depletion is expected from state-of-the-art dust evolution models. We studied the effect of creating an artificial inner cavity in our models, and conclude that HD 163296 might be a precursor to typical group I sources., Comment: 15 pages, 12 figures

Published
2018
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196. The Circumstellar Disk and Asymmetric outflow of the EX Lup Outburst System

Author

Hales, A. S., Peréz, S., Saito, M., Pinte, C., Knee, L., de Gregorio-Monsalvo, I., López, C., Plunkett, A., Córtes, P., Corder, S., Cieza, L., Hales, A. S., Peréz, S., Saito, M., Pinte, C., Knee, L., de Gregorio-Monsalvo, I., López, C., Plunkett, A., Córtes, P., Corder, S., and Cieza, L.

Abstract

We present Atacama Large Millimeter/submillimeter Array (ALMA) observations at 0.3 arcsec-resolution of EX Lup, the prototype of the EXor class of outbursting pre-main sequence stars. The circumstellar disk of EX Lup is resolved for the first time in 1.3mm continuum emission and in the $J$=2--1 spectral line of three isotopologues of CO. At the spatial resolution and sensitivity achieved, the compact dust continuum disk shows no indications of clumps, fragments, or asymmetries above 5-sigma level. Radiative transfer modeling constrains the characteristic radius of the dust disk to 23 au and a total dust mass of 1.0$\times$10$^{-4}$ M$_\odot$ (33 M_earth), similar to other EXor sources. The $^{13}$CO and C$^{18}$O line emission trace the disk rotation and are used to constrain the disk geometry, kinematics, and a total gas disk mass of 5.1$\times$10$^{-4}$ M$_\odot$. The $^{12}$CO emission extends out to a radius of 200 au and is asymmetric, with one side deviating from Keplerian rotation. We detect blue-shifted, $^{12}$CO arc-like emission located 0.8 arcsec to the north-west, and spatially disconnected from the disk emission. We interpret this extended structure as the brightened walls of a cavity excavated by an outflow, which are more commonly seen in FUor sources. Such outflows have also been seen in the borderline FU/EXor object V1647 Ori, but not towards EXor objects. Our detection provides evidence that the outflow phenomenon persists into the EXor phase, suggesting that FUor and EXor objects are a continuous population in which outflow activity declines with age, with transitional objects such as EX Lup and V1647 Ori.

Published
2018
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197. First scattered light detection of a nearly edge-on transition disk around the T Tauri star RY Lup

Author

Langlois, M., Pohl, A., Lagrange, A. -M., Maire, A. - L., Mesa, D., Boccaletti, A., Gratton, R., Denneulin, L., Klahr, H., Vigan, A., Benisty, M., Dominik, C., Bonnefoy, M., Menard, F., Avenhaus, H., Cheetham, A., Van Boekel, R., de Boer, J., Chauvin, G., Desidera, S., Feldt, M., Galicher, R., Ginski, C., Girard, J., Henning, T., Janson, M., Kopytova, T., Kral, Q., Ligi, R., Messina, S., Peretti, S., Pinte, C., Sissa, E., Stolker, T, Zurlo, A., Magnard, Y., Blanchard, P., Buey, T., Suarez, M., Cascone, E., Moller-Nilsson, O., Weber, L., Petit, C., Pragt, J., Langlois, M., Pohl, A., Lagrange, A. -M., Maire, A. - L., Mesa, D., Boccaletti, A., Gratton, R., Denneulin, L., Klahr, H., Vigan, A., Benisty, M., Dominik, C., Bonnefoy, M., Menard, F., Avenhaus, H., Cheetham, A., Van Boekel, R., de Boer, J., Chauvin, G., Desidera, S., Feldt, M., Galicher, R., Ginski, C., Girard, J., Henning, T., Janson, M., Kopytova, T., Kral, Q., Ligi, R., Messina, S., Peretti, S., Pinte, C., Sissa, E., Stolker, T, Zurlo, A., Magnard, Y., Blanchard, P., Buey, T., Suarez, M., Cascone, E., Moller-Nilsson, O., Weber, L., Petit, C., and Pragt, J.

Abstract

Transition disks are considered sites of ongoing planet formation, and their dust and gas distributions could be signposts of embedded planets. The transition disk around the T Tauri star RY Lup has an inner dust cavity and displays a strong silicate emission feature. Using high-resolution imaging we study the disk geometry, including non-axisymmetric features, and its surface dust grain, to gain a better understanding of the disk evolutionary process. Moreover, we search for companion candidates, possibly connected to the disk. We obtained high-contrast and high angular resolution data in the near-infrared with the VLT/SPHERE extreme adaptive optics instrument whose goal is to study the planet formation by detecting and characterizing these planets and their formation environments through direct imaging. We performed polarimetric imaging of the RY~Lup disk with IRDIS (at 1.6 microns), and obtained intensity images with the IRDIS dual-band imaging camera simultaneously with the IFS spectro-imager (0.9-1.3 microns). We resolved for the first time the scattered light from the nearly edge-on circumstellar disk around RY~Lup, at projected separations in the 100 \,au range. The shape of the disk and its sharp features are clearly detectable at wavelengths ranging from 0.9 to 1.6 microns. We show that the observed morphology can be interpreted as spiral arms in the disk. This interpretation is supported by in-depth numerical simulations. We also demonstrate that these features can be produced by one planet interacting with the disk. We also detect several point sources which are classified as probable background objects.

Published
2018
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198. Polarimetric imaging of protoplanetary disks from the optical to sub-mm

Author

De Boer, Jos, Ménard, F., Pinte, C., van der Plas, G., and Snik, F.

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

To learn how planets form from the smallest building blocks within protoplanetary disks, we first need to know how dust grains grow from micron to mm sizes. Polarimetry across the spectrum has proven to be sensitive to grain properties like dust size distribution and composition and thus can be used to characterize the scattering grains. However, polarization measured with radio interferometric arrays is rarely studied in concert with optical polarimetry.\nOur team has successfully calibrated the NIR polarimetric imaging mode of VLT\/SPHERE, hence upgrading the instrument from a high-contrast imager to a robust tool for quantitative characterization. In this presentation, we will discuss which lessons can be learned by comparing polarimetry in the optical and sub-mm and explore for which science cases both techniques can complement each other. When we combine the polarimetric capabilities of the most advanced optical high-contrast imagers (e.g., Gemini GPI or VLT SPHERE) with that of ALMA we will be able to study the spatial distribution of an extensive range of different grains, which allows us to take an essential step towards a deeper understanding of planet formation.

Published
2017
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199. Three Years of SPHERE: The Latest View of the Morphology and Evolution of Protoplanetary Discs

Author

Garufi, A., Benisty, M., Stolker, T., Avenhaus, H., Boer, J. de, Pohl, A., Quanz, S.P., Dominik, C., Ginski, C., Thalmann, C., Boekel, R., Boccaletti, A., Henning, T., Janson, M., Salter, G., Schmid, H.M., Sissa, E., Langlois, M., Beuzit, J.-L., Chauvin, G., Mouillet, D., Augereau, J.-C., Bazzon, A., Biller, B., Bonnefoy, M., Buenzli, E., Cheetham, A., Daemgen, S., Desidera, S., Engler, N., Feldt, M., Girard, J., Gratton, R., Hagelberg, J., Keller, C.U., Keppler, M., Kenworthy, M.A., Kral, Q., Lopez, B., Maire, A.-L., Menard, F., Mesa, D., Messina, S., Meyer, M.R., Milli, J., Min, M., Muller, A., Olofsson, J., Pawellek, N., Pinte, C., Szulagyi, J., Vigan, A., Wahhaj, Z., Waters, R., Zurlo, A., and Low Energy Astrophysics (API, FNWI)

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Spatially resolving the immediate surroundings of young stars is a key challenge for the planet formation community. SPHERE on the VLT represents an important step forward by increasing the opportunities offered by optical or near-infrared imaging instruments to image protoplanetary discs. The Guaranteed Time Observation Disc team has concentrated much of its efforts on polarimetric differential imaging, a technique that enables the efficient removal of stellar light and thus facilitates the detection of light scattered by the disc within a few au from the central star. These images reveal intriguing complex disc structures and diverse morphological features that are possibly caused by ongoing planet formation in the disc. An overview of the recent advances enabled by SPHERE is presented.

Published
2017

200. Near-infrared scattered light properties of the HR 4796 A dust ring

Author

Milli, J., Vigan, Arthur, Mouillet, D., Lagrange, A.M., Augereau, J., Pinte, C., Mawet, D., Schmid, M., Boccaletti, A., Matra, L., Kral, Q., Ertel, S., Chauvin, G., Bazzon, A., Menard, F., Beuzit, J., Thalmann, C., Dominik, C., Feldt, M., Henning, T., Min, M., Girard, J., Galicher, R., Bonnefoy, M., Fusco, T., De Boer, J., Janson, M., Maire, A.L., Mesa, D., Schlieder, J. E., European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Franco-Chilien d'Astronomie (LFCA), Universidad de Concepción [Chile]-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Chile, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Steward Observatory, University of Arizona, Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, SRON Netherlands Institute for Space Research (SRON), ONERA - The French Aerospace Lab [Châtillon], ONERA, Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Department of Astronomy, Stockholm University, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), NASA ExoPlanet Science Institute (NExScI), California Institute of Technology (CALTECH), ANR-14-CE33-0018,GIPSE,Exploration des planetes géantes extrasolaires(2014), European Project: 279973,EC:FP7:ERC,ERC-2011-StG_20101014,DEBRIS(2012), European Project: 226604,EC:FP7:INFRA,FP7-INFRASTRUCTURES-2008-1,OPTICON(2009), European Project: 312430,EC:FP7:INFRA,FP7-INFRASTRUCTURES-2012-1-RTD,OPTICON(2013), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Universidad de Chile = University of Chile [Santiago] (UCHILE)-Pontificia Universidad Católica de Chile (UC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Universidad de Concepción - University of Concepcion [Chile], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), ONERA-Université Paris Saclay (COmUE), Universiteit Leiden, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and California Institute of Technology (CALTECH)-NASA

Subjects
[PHYS]Physics [physics], Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Scattering, Planetary systems, Detection, High angular resolution, [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Planets and satellites, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation, Astrophysics::Galaxy Astrophysics, Planet-disk interactions
Abstract

International audience; Context. HR 4796 A is surrounded by a debris disc, observed in scattered light as an inclined ring with a high surface brightness. Past observations have raised several questions. First, a strong brightness asymmetry detected in polarised reflected light has recently challenged our understanding of scattering by the dust particles in this system. Secondly, the morphology of the ring strongly suggests the presence of planets, although no planets have been detected to date.Aims. We aim here at measuring with high accuracy the morphology and photometry of the ring in scattered light, in order to derive the phase function of the dust and constrain its near-infrared spectral properties. We also want to constrain the presence of planets and set improved constraints on the origin of the observed ring morphology.Methods. We obtained high-angular resolution coronagraphic images of the circumstellar environment around HR 4796 A with VLT/SPHERE during the commissioning of the instrument in May 2014 and during guaranteed-time observations in February 2015. The observations reveal for the first time the entire ring of dust, including the semi-minor axis that was previously hidden either behind the coronagraphic spot or in the speckle noise.Results. We determine empirically the scattering phase function of the dust in the H band from 13.6° to 166.6°. It shows a prominent peak of forward scattering, never detected before, for scattering angles below 30°. We analyse the reflectance spectra of the disc from the 0.95 μm to 1.6 μm, confirming the red colour of the dust, and derive detection limits on the presence of planetary mass objects.Conclusions. We confirm which side of the disc is inclined towards the Earth. The analysis of the phase function, especially below 45°, suggests that the dust population is dominated by particles much larger than the observation wavelength, of about 20 μm. Compact Mie grains of this size are incompatible with the spectral energy distribution of the disc, however the observed rise in scattering efficiency beyond 50° points towards aggregates which could reconcile both observables. We do not detect companions orbiting the star, but our high-contrast observations provide the most stringent constraints yet on the presence of planets responsible for the morphology of the dust.

Published
2017

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