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

Author

Abuter, R., Allouche, F., Amorim, A., Bailet, C., Berdeu, A., Berger, J. -P., Berio, P., Bigioli, A., Boebion, O., Bolzer, M. -L., Bonnet, H., Bourdarot, G., Bourget, P., Brandner, W., Cao, Y., Conzelmann, R., Comin, M., Clénet, Y., Courtney-Barrer, B., Davies, R., Defrère, D., Delboulbé, A., Delplancke-Ströbele, F., Dembet, R., Dexter, J., de Zeeuw, P. T., Drescher, A., Eckart, A., Édouard, C., Eisenhauer, F., Fabricius, M., Feuchtgruber, H., Finger, G., Schreiber, N. M. Förster, Garcia, P., Lopez, R. Garcia, Gao, F., Gendron, E., Genzel, R., Gil, J. P., Gillessen, S., Gomes, T., Gonté, F., Gouvret, C., Guajardo, P., Guieu, S., Hackenberg, W., Haddad, N., Hartl, M., Haubois, X., Haußmann, F., Heißel, G., Henning, Th., Hippler, S., Hönig, S. F., Horrobin, M., Hubin, N., Jacqmart, E., Jocou, L., Kaufer, A., Kervella, P., Kolb, J., Korhonen, H., Lacour, S., Lagarde, S., Lai, O., Lapeyrère, V., Laugier, R., Bouquin, J. -B. Le, Leftley, J., Léna, P., Lewis, S., Liu, D., Lopez, B., Lutz, D., Magnard, Y., Mang, F., Marcotto, A., Maurel, D., Mérand, A., Millour, F., More, N., Netzer, H., Nowacki, H., Nowak, M., Oberti, S., Ott, T., Pallanca, L., Paumard, T., Perraut, K., Perrin, G., Petrov, R., Pfuhl, O., Pourré, N., Rabien, S., Rau, C., Riquelme, M., Robbe-Dubois, S., Rochat, S., Salman, M., Sanchez-Bermudez, J., Santos, D. J. D., Scheithauer, S., Schöller, M., Schubert, J., Schuhler, N., Shangguan, J., Shchekaturov, P., Shimizu, T. T., Sevin, A., Soulez, F., Spang, A., Stadler, E., Sternberg, A., Straubmeier, C., Sturm, E., Sykes, C., Tacconi, L. J., Tristram, K. R. W., Vincent, F., von Fellenberg, S., Uysal, S., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Zins, G., Abuter, R., Allouche, F., Amorim, A., Bailet, C., Berdeu, A., Berger, J. -P., Berio, P., Bigioli, A., Boebion, O., Bolzer, M. -L., Bonnet, H., Bourdarot, G., Bourget, P., Brandner, W., Cao, Y., Conzelmann, R., Comin, M., Clénet, Y., Courtney-Barrer, B., Davies, R., Defrère, D., Delboulbé, A., Delplancke-Ströbele, F., Dembet, R., Dexter, J., de Zeeuw, P. T., Drescher, A., Eckart, A., Édouard, C., Eisenhauer, F., Fabricius, M., Feuchtgruber, H., Finger, G., Schreiber, N. M. Förster, Garcia, P., Lopez, R. Garcia, Gao, F., Gendron, E., Genzel, R., Gil, J. P., Gillessen, S., Gomes, T., Gonté, F., Gouvret, C., Guajardo, P., Guieu, S., Hackenberg, W., Haddad, N., Hartl, M., Haubois, X., Haußmann, F., Heißel, G., Henning, Th., Hippler, S., Hönig, S. F., Horrobin, M., Hubin, N., Jacqmart, E., Jocou, L., Kaufer, A., Kervella, P., Kolb, J., Korhonen, H., Lacour, S., Lagarde, S., Lai, O., Lapeyrère, V., Laugier, R., Bouquin, J. -B. Le, Leftley, J., Léna, P., Lewis, S., Liu, D., Lopez, B., Lutz, D., Magnard, Y., Mang, F., Marcotto, A., Maurel, D., Mérand, A., Millour, F., More, N., Netzer, H., Nowacki, H., Nowak, M., Oberti, S., Ott, T., Pallanca, L., Paumard, T., Perraut, K., Perrin, G., Petrov, R., Pfuhl, O., Pourré, N., Rabien, S., Rau, C., Riquelme, M., Robbe-Dubois, S., Rochat, S., Salman, M., Sanchez-Bermudez, J., Santos, D. J. D., Scheithauer, S., Schöller, M., Schubert, J., Schuhler, N., Shangguan, J., Shchekaturov, P., Shimizu, T. T., Sevin, A., Soulez, F., Spang, A., Stadler, E., Sternberg, A., Straubmeier, C., Sturm, E., Sykes, C., Tacconi, L. J., Tristram, K. R. W., Vincent, F., von Fellenberg, S., Uysal, S., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., and Zins, G.

Abstract

Tight relationships exist in the local universe between the central stellar properties of galaxies and the mass of their supermassive black hole. These suggest galaxies and black holes co-evolve, with the main regulation mechanism being energetic feedback from accretion onto the black hole during its quasar phase. A crucial question is how the relationship between black holes and galaxies evolves with time; a key epoch to probe this relationship is at the peaks of star formation and black hole growth 8-12 billion years ago (redshifts 1-3). Here we report a dynamical measurement of the mass of the black hole in a luminous quasar at a redshift of 2, with a look back time of 11 billion years, by spatially resolving the broad line region. We detect a 40 micro-arcsecond (0.31 pc) spatial offset between the red and blue photocenters of the H$\alpha$ line that traces the velocity gradient of a rotating broad line region. The flux and differential phase spectra are well reproduced by a thick, moderately inclined disk of gas clouds within the sphere of influence of a central black hole with a mass of 3.2x10$^{8}$ solar masses. Molecular gas data reveal a dynamical mass for the host galaxy of 6x10$^{11}$ solar masses, which indicates an under-massive black hole accreting at a super-Eddington rate. This suggests a host galaxy that grew faster than the supermassive black hole, indicating a delay between galaxy and black hole formation for some systems., Comment: 5 pages Main text, 8 figures, 2 tables, to be published in Nature, under embargo until 29 January 2024 16:00 (London)

Published
2024
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2. First light for GRAVITY Wide Large separation fringe tracking for the Very Large Telescope Interferometer

Author

Abuter, R., Allouche, F., Amorim, A., Bailet, C., Bauboeck, M., Berger, J-P, Berio, P., Bigioli, A., Boebion, O., Bolzer, M. L., Bonnet, H., Bourdarot, G., Bourget, P., Brandner, W., Clenet, Y., Courtney-Barrer, B., Dallilar, Y., Davies, R., Defrere, D., Delboulbe, A., Delplancke, F., Dembet, R., de Zeeuw, P. T., Drescher, A., Eckart, A., Edouard, C., Eisenhauer, F., Fabricius, M., Feuchtgruber, H., Finger, G., Schreiber, N. M. Foerster, Garcia, E., Garcia, P., Gao, F., Gendron, E., Genzel, R., Gil, J. P., Gillessen, S., Gomes, T., Gonte, F., Gouvret, C., Guajardo, P., Guieu, S., Hartl, M., Haubois, X., Haussmann, F., Heissel, G., Henning, Th, Hippler, S., Honig, S., Horrobin, M., Hubin, N., Jacqmart, E., Jochum, L., Jocou, L., Kaufer, A., Kervella, P., Korhonen, H., Kreidberg, L., Lacour, S., Lagarde, S., Lai, O., Lapeyrere, V, Laugier, R., Le Bouquin, J-B, Leftley, J., Lena, P., Lutz, D., Mang, F., Marcotto, A., Maurel, D., Merand, A., Millour, F., More, N., Nowacki, H., Nowak, M., Oberti, S., Ott, T., Pallanca, L., Paumard, T., Perraut, K., Perrin, G., Petrov, R., Pfuhl, O., Pourre, N., Rabien, S., Rau, C., Robbe-Dubois, S., Rochat, S., Salman, M., Scholler, M., Schubert, J., Schuhler, N., Shangguan, J., Shimizu, T., Scheithauer, S., Sevin, A., Soulez, F., Spang, A., Stadler, E., Stadler, J., Straubmeier, C., Sturm, E., Tacconi, L. J., Tristram, K. R. W., Vincent, F., von Fellenberg, S., Uysal, S., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Young, A., Zins, G., Abuter, R., Allouche, F., Amorim, A., Bailet, C., Bauboeck, M., Berger, J-P, Berio, P., Bigioli, A., Boebion, O., Bolzer, M. L., Bonnet, H., Bourdarot, G., Bourget, P., Brandner, W., Clenet, Y., Courtney-Barrer, B., Dallilar, Y., Davies, R., Defrere, D., Delboulbe, A., Delplancke, F., Dembet, R., de Zeeuw, P. T., Drescher, A., Eckart, A., Edouard, C., Eisenhauer, F., Fabricius, M., Feuchtgruber, H., Finger, G., Schreiber, N. M. Foerster, Garcia, E., Garcia, P., Gao, F., Gendron, E., Genzel, R., Gil, J. P., Gillessen, S., Gomes, T., Gonte, F., Gouvret, C., Guajardo, P., Guieu, S., Hartl, M., Haubois, X., Haussmann, F., Heissel, G., Henning, Th, Hippler, S., Honig, S., Horrobin, M., Hubin, N., Jacqmart, E., Jochum, L., Jocou, L., Kaufer, A., Kervella, P., Korhonen, H., Kreidberg, L., Lacour, S., Lagarde, S., Lai, O., Lapeyrere, V, Laugier, R., Le Bouquin, J-B, Leftley, J., Lena, P., Lutz, D., Mang, F., Marcotto, A., Maurel, D., Merand, A., Millour, F., More, N., Nowacki, H., Nowak, M., Oberti, S., Ott, T., Pallanca, L., Paumard, T., Perraut, K., Perrin, G., Petrov, R., Pfuhl, O., Pourre, N., Rabien, S., Rau, C., Robbe-Dubois, S., Rochat, S., Salman, M., Scholler, M., Schubert, J., Schuhler, N., Shangguan, J., Shimizu, T., Scheithauer, S., Sevin, A., Soulez, F., Spang, A., Stadler, E., Stadler, J., Straubmeier, C., Sturm, E., Tacconi, L. J., Tristram, K. R. W., Vincent, F., von Fellenberg, S., Uysal, S., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Young, A., and Zins, G.

Abstract

GRAVITY+ is the upgrade for GRAVITY and the Very Large Telescope Interferometer (VLTI) with wide-separation fringe tracking, new adaptive optics, and laser guide stars on all four 8 m Unit Telescopes (UTs) to enable ever-fainter, all-sky, high-contrast, milliarcsecond interferometry. Here we present the design and first results of the first phase of GRAVITY+, known as GRAVITY Wide. GRAVITY Wide combines the dual-beam capabilities of the VLTI and the GRAVITY instrument to increase the maximum separation between the science target and the reference star from 2 arcseconds with the 8 m UTs up to several 10 arcseconds, limited only by the Earth's turbulent atmosphere. This increases the sky-coverage of GRAVITY by two orders of magnitude, opening up milliarcsecond resolution observations of faint objects and, in particular, the extragalactic sky. The first observations in 2019-2022 include the first infrared interferometry of two redshift z similar to 2 quasars, interferometric imaging of the binary system HD 105913A, and repeat observations of multiple star systems in the Orion Trapezium Cluster. We find the coherence loss between the science object and fringe-tracking reference star well described by the turbulence of the Earth's atmosphere. We confirm that the larger apertures of the UTs result in higher visibilities for a given separation due to the broader overlap of the projected pupils on the sky and provide predictions for visibility loss as a function of separation to be used for future planning.

Published
2022

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

Author

Collaboration, GRAVITY+, Abuter, R., Allouche, F., Amorim, A., Bailet, C., Bauböck, M., Berger, J. -P., Berio, P., Bigioli, A., Boebion, O., Bolzer, M. L., Bonnet, H., Bourdarot, G., Bourget, P., Brandner, W., Clénet, Y., Courtney-Barrer, B., Dallilar, Y., Davies, R., Defrère, D., Delboulbé, A., Delplancke, F., Dembet, R., de Zeeuw, P. T., Drescher, A., Eckart, A., Édouard, C., Eisenhauer, F., Fabricius, M., Feuchtgruber, H., Finger, G., Schreiber, N. M. Förster, Garcia, E., Garcia, P., Gao, F., Gendron, E., Genzel, R., Gil, J. P., Gillessen, S., Gomes, T., Gonté, F., Gouvret, C., Guajardo, P., Guieu, S., Hartl, M., Haubois, X., Haußmann, F., Heißel, G., Henning, Th., Hippler, S., Hönig, S., Horrobin, M., Hubin, N., Jacqmart, E., Jochum, L., Jocou, L., Kaufer, A., Kervella, P., Korhonen, H., Kreidberg, L., Lacour, S., Lagarde, S., Lai, O., Lapeyrère, V., Laugier, R., Bouquin, J. -B. Le, Leftley, J., Léna, P., Lutz, D., Mang, F., Marcotto, A., Maurel, D., Mérand, A., Millour, F., More, N., Nowacki, H., Nowak, M., Oberti, S., Ott, T., Pallanca, L., Paumard, T., Perraut, K., Perrin, G., Petrov, R., Pfuhl, O., Pourré, N., Rabien, S., Rau, C., Robbe-Dubois, S., Rochat, S., Salman, M., Schöller, M., Schubert, J., Schuhler, N., Shangguan, J., Shimizu, T., Scheithauer, S., Sevin, A., Soulez, F., Spang, A., Stadler, E., Stadler, J., Straubmeier, C., Sturm, E., Tacconi, L. J., Tristram, K. R. W., Vincent, F., von Fellenberg, S., Uysal, S., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Young, A., Zins, G., Collaboration, GRAVITY+, Abuter, R., Allouche, F., Amorim, A., Bailet, C., Bauböck, M., Berger, J. -P., Berio, P., Bigioli, A., Boebion, O., Bolzer, M. L., Bonnet, H., Bourdarot, G., Bourget, P., Brandner, W., Clénet, Y., Courtney-Barrer, B., Dallilar, Y., Davies, R., Defrère, D., Delboulbé, A., Delplancke, F., Dembet, R., de Zeeuw, P. T., Drescher, A., Eckart, A., Édouard, C., Eisenhauer, F., Fabricius, M., Feuchtgruber, H., Finger, G., Schreiber, N. M. Förster, Garcia, E., Garcia, P., Gao, F., Gendron, E., Genzel, R., Gil, J. P., Gillessen, S., Gomes, T., Gonté, F., Gouvret, C., Guajardo, P., Guieu, S., Hartl, M., Haubois, X., Haußmann, F., Heißel, G., Henning, Th., Hippler, S., Hönig, S., Horrobin, M., Hubin, N., Jacqmart, E., Jochum, L., Jocou, L., Kaufer, A., Kervella, P., Korhonen, H., Kreidberg, L., Lacour, S., Lagarde, S., Lai, O., Lapeyrère, V., Laugier, R., Bouquin, J. -B. Le, Leftley, J., Léna, P., Lutz, D., Mang, F., Marcotto, A., Maurel, D., Mérand, A., Millour, F., More, N., Nowacki, H., Nowak, M., Oberti, S., Ott, T., Pallanca, L., Paumard, T., Perraut, K., Perrin, G., Petrov, R., Pfuhl, O., Pourré, N., Rabien, S., Rau, C., Robbe-Dubois, S., Rochat, S., Salman, M., Schöller, M., Schubert, J., Schuhler, N., Shangguan, J., Shimizu, T., Scheithauer, S., Sevin, A., Soulez, F., Spang, A., Stadler, E., Stadler, J., Straubmeier, C., Sturm, E., Tacconi, L. J., Tristram, K. R. W., Vincent, F., von Fellenberg, S., Uysal, S., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Young, A., and Zins, G.

Abstract

GRAVITY+ is the upgrade of GRAVITY and the Very Large Telescope Interferometer (VLTI) with wide-separation fringe tracking, new adaptive optics, and laser guide stars on all four 8~m Unit Telescopes (UTs), for ever fainter, all-sky, high contrast, milliarcsecond interferometry. Here we present the design and first results of the first phase of GRAVITY+, called GRAVITY Wide. GRAVITY Wide combines the dual-beam capabilities of the VLTI and the GRAVITY instrument to increase the maximum separation between the science target and the reference star from 2 arcseconds with the 8 m UTs up to several 10 arcseconds, limited only by the Earth's turbulent atmosphere. This increases the sky-coverage of GRAVITY by two orders of magnitude, opening up milliarcsecond resolution observations of faint objects, and in particular the extragalactic sky. The first observations in 2019 - 2022 include first infrared interferometry of two redshift $z\sim2$ quasars, interferometric imaging on the binary system HD 105913A, and repeated observations of multiple star systems in the Orion Trapezium Cluster. We find the coherence loss between the science object and fringe-tracking reference star well described by the turbulence of the Earth's atmosphere. We confirm that the larger apertures of the UTs result in higher visibilities for a given separation due to larger overlap of the projected pupils on sky and give predictions for visibility loss as a function of separation to be used for future planning., Comment: 15 pages, 12 figures, 5 tables. Accepted by A&A

Published
2022
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4. The mass of Beta Pictoris c from Beta Pictoris b orbital motion

Author

Lacour, S., Wang, J. J., Rodet, L., Nowak, M., Shangguan, J., Beust, H., Lagrange, A. -M., Abuter, R., Amorim, A., Asensio-Torres, R., Benisty, M., Berger, J. -P., Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M. -L., Bonnefoy, M., Bonnet, H., Bourdarot, G., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Choquet, E., Christiaens, V., Clénet, Y., Foresto, V. Coudé du, Cridland, A., Dembet, R., Dexter, J., de Zeeuw, P. T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Gao, F., Garcia, P., Lopez, R. Garcia, Gendron, E., Genzel, R., Gillessen, S., Girard, J. H., Haubois, X., Heißel, G., Henning, Th., Hinkley, S., Hippler, S., Horrobin, M., Houllé, M., Hubert, Z., Jocou, L., Kammerer, J., Keppler, M., Kervella, P., Kreidberg, L., Lapeyrère, V., Bouquin, J. -B. Le, Léna, P., Lutz, D., Maire, A. -L., Mérand, A., Mollière, P., Monnier, J. D., Mouillet, D., Nasedkin, E., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Pfuhl, O., Rickman, E., Pueyo, L., Rameau, J., Rousset, G., Rustamkulov, Z., Samland, M., Shimizu, T., Sing, D., Stadler, J., Stolker, T., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., von Fellenberg, S. D., Ward-Duong, K., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Young, A., Collaboration, the GRAVITY, Lacour, S., Wang, J. J., Rodet, L., Nowak, M., Shangguan, J., Beust, H., Lagrange, A. -M., Abuter, R., Amorim, A., Asensio-Torres, R., Benisty, M., Berger, J. -P., Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M. -L., Bonnefoy, M., Bonnet, H., Bourdarot, G., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Choquet, E., Christiaens, V., Clénet, Y., Foresto, V. Coudé du, Cridland, A., Dembet, R., Dexter, J., de Zeeuw, P. T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Gao, F., Garcia, P., Lopez, R. Garcia, Gendron, E., Genzel, R., Gillessen, S., Girard, J. H., Haubois, X., Heißel, G., Henning, Th., Hinkley, S., Hippler, S., Horrobin, M., Houllé, M., Hubert, Z., Jocou, L., Kammerer, J., Keppler, M., Kervella, P., Kreidberg, L., Lapeyrère, V., Bouquin, J. -B. Le, Léna, P., Lutz, D., Maire, A. -L., Mérand, A., Mollière, P., Monnier, J. D., Mouillet, D., Nasedkin, E., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Pfuhl, O., Rickman, E., Pueyo, L., Rameau, J., Rousset, G., Rustamkulov, Z., Samland, M., Shimizu, T., Sing, D., Stadler, J., Stolker, T., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., von Fellenberg, S. D., Ward-Duong, K., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Young, A., and Collaboration, the GRAVITY

Abstract

We aim to demonstrate that the presence and mass of an exoplanet can now be effectively derived from the astrometry of another exoplanet. We combined previous astrometry of $\beta$ Pictoris b with a new set of observations from the GRAVITY interferometer. The orbital motion of $\beta$ Pictoris b is fit using Markov chain Monte Carlo simulations in Jacobi coordinates. The inner planet, $\beta$ Pictoris c, was also reobserved at a separation of 96\,mas, confirming the previous orbital estimations. From the astrometry of planet b only, we can (i) detect the presence of $\beta$ Pictoris c and (ii) constrain its mass to $10.04^{+4.53}_{-3.10}\,M_{\rm Jup}$. If one adds the astrometry of $\beta$ Pictoris c, the mass is narrowed down to $9.15^{+1.08}_{-1.06}\,M_{\rm Jup}$. The inclusion of radial velocity measurements does not affect the orbital parameters significantly, but it does slightly decrease the mass estimate to $8.89^{+0.75}_{-0.75}\,M_{\rm Jup}$. With a semimajor axis of $2.68\pm0.02$\,au, a period of $1221\pm15$ days, and an eccentricity of $0.32\pm0.02$, the orbital parameters of $\beta$ Pictoris c are now constrained as precisely as those of $\beta$ Pictoris b. The orbital configuration is compatible with a high-order mean-motion resonance (7:1). The impact of the resonance on the planets' dynamics would then be negligible with respect to the secular perturbations, which might have played an important role in the eccentricity excitation of the outer planet., Comment: Accepted in A&A Letter

Published
2021
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5. GRAVITY K-band spectroscopy of HD 206893 B: brown dwarf or exoplanet

Author

Kammerer, J., Lacour, S., Stolker, T., Mollière, P., Sing, D. K., Nasedkin, E., Kervella, P., Wang, J. J., Ward-Duong, K., Nowak, M., Abuter, R., Amorim, A., Asensio-Torres, R., Bauböck, M., Benisty, M., Berger, J. -P., Beust, H., Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M. -L., Bonnefoy, M., Bonnet, H., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Choquet, E., Christiaens, V., Clénet, Y., Foresto, V. Coudé du, Cridland, A., Dembet, R., Dexter, J., de Zeeuw, P. T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Gao, F., Garcia, P., Lopez, R. Garcia, Gendron, E., Genzel, R., Gillessen, S., Girard, J., Haubois, X., Heißel, G., Henning, T., Hinkley, S., Hippler, S., Horrobin, M., Houllé, M., Hubert, Z., Jocou, L., Keppler, M., Kreidberg, L., Lagrange, A. -M., Lapeyrère, V., Bouquin, J. -B. Le, Léna, P., Lutz, D., Maire, A. -L., Mérand, A., Monnier, J. D., Mouillet, D., Müller, A., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Pfuhl, O., Pueyo, L., Rameau, J., Rodet, L., Rousset, G., Rustamkulov, Z., Shangguan, J., Shimizu, T., Stadler, J., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., von Fellenberg, S. D., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Collaboration, GRAVITY, Kammerer, J., Lacour, S., Stolker, T., Mollière, P., Sing, D. K., Nasedkin, E., Kervella, P., Wang, J. J., Ward-Duong, K., Nowak, M., Abuter, R., Amorim, A., Asensio-Torres, R., Bauböck, M., Benisty, M., Berger, J. -P., Beust, H., Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M. -L., Bonnefoy, M., Bonnet, H., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Choquet, E., Christiaens, V., Clénet, Y., Foresto, V. Coudé du, Cridland, A., Dembet, R., Dexter, J., de Zeeuw, P. T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Gao, F., Garcia, P., Lopez, R. Garcia, Gendron, E., Genzel, R., Gillessen, S., Girard, J., Haubois, X., Heißel, G., Henning, T., Hinkley, S., Hippler, S., Horrobin, M., Houllé, M., Hubert, Z., Jocou, L., Keppler, M., Kreidberg, L., Lagrange, A. -M., Lapeyrère, V., Bouquin, J. -B. Le, Léna, P., Lutz, D., Maire, A. -L., Mérand, A., Monnier, J. D., Mouillet, D., Müller, A., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Pfuhl, O., Pueyo, L., Rameau, J., Rodet, L., Rousset, G., Rustamkulov, Z., Shangguan, J., Shimizu, T., Stadler, J., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., von Fellenberg, S. D., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., and Collaboration, GRAVITY

Abstract

We aim to reveal the nature of the reddest known substellar companion HD 206893 B by studying its near-infrared colors and spectral morphology and by investigating its orbital motion. We fit atmospheric models for giant planets and brown dwarfs and perform spectral retrievals with petitRADTRANS and ATMO on the observed GRAVITY, SPHERE, and GPI spectra of HD 206893 B. To recover its unusual spectral features, we include additional extinction by high-altitude dust clouds made of enstatite grains in the atmospheric model fits. We also infer the orbital parameters of HD 206893 B by combining the $\sim 100~\mu\text{as}$ precision astrometry from GRAVITY with data from the literature and constrain the mass and position of HD 206893 C based on the Gaia proper motion anomaly of the system. The extremely red color and the very shallow $1.4~\mu\text{m}$ water absorption feature of HD 206893 B can be fit well with the adapted atmospheric models and spectral retrievals. Altogether, our analysis suggests an age of $\sim 3$-$300~\text{Myr}$ and a mass of $\sim 5$-$30~\text{M}_\text{Jup}$ for HD 206893 B, which is consistent with previous estimates but extends the parameter space to younger and lower-mass objects. The GRAVITY astrometry points to an eccentric orbit ($e = 0.29^{+0.06}_{-0.11}$) with a mutual inclination of $< 34.4~\text{deg}$ with respect to the debris disk of the system. While HD 206893 B could in principle be a planetary-mass companion, this possibility hinges on the unknown influence of the inner companion on the mass estimate of $10^{+5}_{-4}~\text{M}_\text{Jup}$ from radial velocity and Gaia as well as a relatively small but significant Argus moving group membership probability of $\sim 61\%$. However, we find that if the mass of HD 206893 B is $< 30~\text{M}_\text{Jup}$, then the inner companion HD 206893 C should have a mass between $\sim 8$-$15~\text{M}_\text{Jup}$., Comment: 28 pages, 19 figures, accepted for publication in A&A

Published
2021
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6. The mass of beta Pictoris c from beta Pictoris b orbital motion

Author

Lacour, S., Wang, J. J., Rodet, L., Nowak, M., Shangguan, J., Beust, H., Lagrange, A-M, Abuter, R., Amorim, A., Asensio-Torres, R., Benisty, M., Berger, J-P, Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M-L, Bonnefoy, M., Bonnet, H., Bourdarot, G., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Choquet, E., Christiaens, V, Clenet, Y., du Foresto, V. Coude, Cridland, A., Dembet, R., Dexter, J., de Zeeuw, T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Gao, F., Garcia, P., Lopez, R. Garcia, Gendron, E., Genzel, R., Gillessen, S., Girard, J. H., Haubois, X., Heissel, G., Henning, Th, Hinkley, S., Hippler, S., Horrobin, M., Houlle, M., Hubert, Z., Jocou, L., Kammerer, J., Keppler, M., Kervella, P., Kreidberg, L., Lapeyrere, V, Le Bouquin, J-B, Lena, P., Lutz, D., Maire, A-L, Merand, A., Molliere, P., Monnier, J. D., Mouillet, D., Nasedkin, E., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Pfuhl, O., Rickman, E., Pueyo, L., Rameau, J., Rousset, G., Rustamkulov, Z., Samland, M., Shimizu, T., Sing, D., Stadler, J., Stolker, T., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., von Fellenberg, S. D., Ward-Duong, K., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Young, A., Lacour, S., Wang, J. J., Rodet, L., Nowak, M., Shangguan, J., Beust, H., Lagrange, A-M, Abuter, R., Amorim, A., Asensio-Torres, R., Benisty, M., Berger, J-P, Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M-L, Bonnefoy, M., Bonnet, H., Bourdarot, G., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Choquet, E., Christiaens, V, Clenet, Y., du Foresto, V. Coude, Cridland, A., Dembet, R., Dexter, J., de Zeeuw, T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Gao, F., Garcia, P., Lopez, R. Garcia, Gendron, E., Genzel, R., Gillessen, S., Girard, J. H., Haubois, X., Heissel, G., Henning, Th, Hinkley, S., Hippler, S., Horrobin, M., Houlle, M., Hubert, Z., Jocou, L., Kammerer, J., Keppler, M., Kervella, P., Kreidberg, L., Lapeyrere, V, Le Bouquin, J-B, Lena, P., Lutz, D., Maire, A-L, Merand, A., Molliere, P., Monnier, J. D., Mouillet, D., Nasedkin, E., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Pfuhl, O., Rickman, E., Pueyo, L., Rameau, J., Rousset, G., Rustamkulov, Z., Samland, M., Shimizu, T., Sing, D., Stadler, J., Stolker, T., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., von Fellenberg, S. D., Ward-Duong, K., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., and Young, A.

Abstract

Aims. We aim to demonstrate that the presence and mass of an exoplanet can now be effectively derived from the astrometry of another exoplanet. Methods. We combined previous astrometry of beta Pictoris b with a new set of observations from the GRAVITY interferometer. The orbital motion of beta Pictoris b is fit using Markov chain Monte Carlo simulations in Jacobi coordinates. The inner planet, beta Pictoris c, was also reobserved at a separation of 96 mas, confirming the previous orbital estimations. Results. From the astrometry of planet b only, we can (i) detect the presence of beta Pictoris c and (ii) constrain its mass to 10.04(-3.10)(+4.53) M-Jup . If one adds the astrometry of beta Pictoris c, the mass is narrowed down to 9.15(-1.06)(+1.08) M-Jup. The inclusion of radial velocity measurements does not affect the orbital parameters significantly, but it does slightly decrease the mass estimate to 8.89(-0.75)(+0.75) M-Jup.With a semimajor axis of 2.68 +/- 0.02 au, a period of 1221 +/- 15 days, and an eccentricity of 0.32 +/- 0.02, the orbital parameters of beta Pictoris c are now constrained as precisely as those of beta Pictoris b. The orbital configuration is compatible with a high-order mean-motion resonance (7:1). The impact of the resonance on the planets' dynamics would then be negligible with respect to the secular perturbations, which might have played an important role in the eccentricity excitation of the outer planet.

Published
2021

7. GRAVITY K-band spectroscopy of HD 206893 B Brown dwarf or exoplanet

Author

Kammerer, J., Lacour, S., Stolker, T., Molliere, P., Sing, D. K., Nasedkin, E., Kervella, P., Wang, J. J., Ward-Duong, K., Nowak, M., Abuter, R., Amorim, A., Asensio-Torres, R., Baubock, M., Benisty, M., Berger, J-P, Beust, H., Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M-L, Bonnefoy, M., Bonnet, H., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Choquet, E., Christiaens, V, Clenet, Y., du Foresto, V. Coude, Cridland, A., Dembet, R., Dexter, J., de Zeeuw, P. T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Gao, F., Garcia, P., Lopez, R. Garcia, Gendron, E., Genzel, R., Gillessen, S., Girard, J., Haubois, X., Heissel, G., Henning, T., Hinkley, S., Hippler, S., Horrobin, M., Houlle, M., Hubert, Z., Jocou, L., Keppler, M., Kreidberg, L., Lagrange, A-M, Lapeyrere, V, Le Bouquin, J-B, Lena, P., Lutz, D., Maire, A-L, Merand, A., Monnier, J. D., Mouillet, D., Muller, A., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Pfuhl, O., Pueyo, L., Rameau, J., Rodet, L., Rousset, G., Rustamkulov, Z., Shangguan, J., Shimizu, T., Stadler, J., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., von Fellenberg, S. D., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Kammerer, J., Lacour, S., Stolker, T., Molliere, P., Sing, D. K., Nasedkin, E., Kervella, P., Wang, J. J., Ward-Duong, K., Nowak, M., Abuter, R., Amorim, A., Asensio-Torres, R., Baubock, M., Benisty, M., Berger, J-P, Beust, H., Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M-L, Bonnefoy, M., Bonnet, H., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Choquet, E., Christiaens, V, Clenet, Y., du Foresto, V. Coude, Cridland, A., Dembet, R., Dexter, J., de Zeeuw, P. T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Gao, F., Garcia, P., Lopez, R. Garcia, Gendron, E., Genzel, R., Gillessen, S., Girard, J., Haubois, X., Heissel, G., Henning, T., Hinkley, S., Hippler, S., Horrobin, M., Houlle, M., Hubert, Z., Jocou, L., Keppler, M., Kreidberg, L., Lagrange, A-M, Lapeyrere, V, Le Bouquin, J-B, Lena, P., Lutz, D., Maire, A-L, Merand, A., Monnier, J. D., Mouillet, D., Muller, A., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Pfuhl, O., Pueyo, L., Rameau, J., Rodet, L., Rousset, G., Rustamkulov, Z., Shangguan, J., Shimizu, T., Stadler, J., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., von Fellenberg, S. D., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., and Yazici, S.

Abstract

Context. Near-infrared interferometry has become a powerful tool for studying the orbital and atmospheric parameters of substellar companions. Aims. We aim to reveal the nature of the reddest known substellar companion HD 206893 B by studying its near-infrared colors and spectral morphology and by investigating its orbital motion. Methods. We fit atmospheric models for giant planets and brown dwarfs and perform spectral retrievals with petitRADTRANS and ATMO on the observed GRAVITY, SPHERE, and GPI spectra of HD 206893 B. To recover its unusual spectral features, first and foremost its extremely red near-infrared color, we include additional extinction by high-altitude dust clouds made of enstatite grains in the atmospheric model fits. However, forsterite, corundum, and iron grains predict similar extinction curves for the grain sizes considered here. We also infer the orbital parameters of HD 206893 B by combining the similar to 100 mu as precision astrometry from GRAVITY with data from the literature and constrain the mass and position of HD 206893 C based on the Gaia proper motion anomaly of the system. Results. The extremely red color and the very shallow 1.4 mu m water absorption feature of HD 206893 B can be fit well with the adapted atmospheric models and spectral retrievals. By comparison with AMES-Cond evolutionary tracks, we find that only some atmosphericmodels predict physically plausible objects. Altogether, our analysis suggests an age of similar to 3-300 Myr and a mass of similar to 5-30 M-Jup for HD 206893 B, which is consistent with previous estimates but extends the parameter space to younger and lower-mass objects. The GRAVITY astrometry points to an eccentric orbit (e = 0.29(-0.11)(+0.06)) with a mutual inclination of <34.4 deg with respect to the debris disk of the system. Conclusions. While HD 206893 B could in principle be a planetary-mass companion, this possibility hinges on the unknown influence of the inner companion on the mass estimate o

Published
2021

8. GRAVITY K-band spectroscopy of HD 206893 B Brown dwarf or exoplanet

Author

Kammerer, J., Lacour, S., Stolker, T., Molliere, P., Sing, D. K., Nasedkin, E., Kervella, P., Wang, J. J., Ward-Duong, K., Nowak, M., Abuter, R., Amorim, A., Asensio-Torres, R., Baubock, M., Benisty, M., Berger, J-P, Beust, H., Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M-L, Bonnefoy, M., Bonnet, H., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Choquet, E., Christiaens, V, Clenet, Y., du Foresto, V. Coude, Cridland, A., Dembet, R., Dexter, J., de Zeeuw, P. T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Gao, F., Garcia, P., Lopez, R. Garcia, Gendron, E., Genzel, R., Gillessen, S., Girard, J., Haubois, X., Heissel, G., Henning, T., Hinkley, S., Hippler, S., Horrobin, M., Houlle, M., Hubert, Z., Jocou, L., Keppler, M., Kreidberg, L., Lagrange, A-M, Lapeyrere, V, Le Bouquin, J-B, Lena, P., Lutz, D., Maire, A-L, Merand, A., Monnier, J. D., Mouillet, D., Muller, A., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Pfuhl, O., Pueyo, L., Rameau, J., Rodet, L., Rousset, G., Rustamkulov, Z., Shangguan, J., Shimizu, T., Stadler, J., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., von Fellenberg, S. D., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Kammerer, J., Lacour, S., Stolker, T., Molliere, P., Sing, D. K., Nasedkin, E., Kervella, P., Wang, J. J., Ward-Duong, K., Nowak, M., Abuter, R., Amorim, A., Asensio-Torres, R., Baubock, M., Benisty, M., Berger, J-P, Beust, H., Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M-L, Bonnefoy, M., Bonnet, H., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Choquet, E., Christiaens, V, Clenet, Y., du Foresto, V. Coude, Cridland, A., Dembet, R., Dexter, J., de Zeeuw, P. T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Gao, F., Garcia, P., Lopez, R. Garcia, Gendron, E., Genzel, R., Gillessen, S., Girard, J., Haubois, X., Heissel, G., Henning, T., Hinkley, S., Hippler, S., Horrobin, M., Houlle, M., Hubert, Z., Jocou, L., Keppler, M., Kreidberg, L., Lagrange, A-M, Lapeyrere, V, Le Bouquin, J-B, Lena, P., Lutz, D., Maire, A-L, Merand, A., Monnier, J. D., Mouillet, D., Muller, A., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Pfuhl, O., Pueyo, L., Rameau, J., Rodet, L., Rousset, G., Rustamkulov, Z., Shangguan, J., Shimizu, T., Stadler, J., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., von Fellenberg, S. D., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., and Yazici, S.

Abstract

Context. Near-infrared interferometry has become a powerful tool for studying the orbital and atmospheric parameters of substellar companions. Aims. We aim to reveal the nature of the reddest known substellar companion HD 206893 B by studying its near-infrared colors and spectral morphology and by investigating its orbital motion. Methods. We fit atmospheric models for giant planets and brown dwarfs and perform spectral retrievals with petitRADTRANS and ATMO on the observed GRAVITY, SPHERE, and GPI spectra of HD 206893 B. To recover its unusual spectral features, first and foremost its extremely red near-infrared color, we include additional extinction by high-altitude dust clouds made of enstatite grains in the atmospheric model fits. However, forsterite, corundum, and iron grains predict similar extinction curves for the grain sizes considered here. We also infer the orbital parameters of HD 206893 B by combining the similar to 100 mu as precision astrometry from GRAVITY with data from the literature and constrain the mass and position of HD 206893 C based on the Gaia proper motion anomaly of the system. Results. The extremely red color and the very shallow 1.4 mu m water absorption feature of HD 206893 B can be fit well with the adapted atmospheric models and spectral retrievals. By comparison with AMES-Cond evolutionary tracks, we find that only some atmosphericmodels predict physically plausible objects. Altogether, our analysis suggests an age of similar to 3-300 Myr and a mass of similar to 5-30 M-Jup for HD 206893 B, which is consistent with previous estimates but extends the parameter space to younger and lower-mass objects. The GRAVITY astrometry points to an eccentric orbit (e = 0.29(-0.11)(+0.06)) with a mutual inclination of <34.4 deg with respect to the debris disk of the system. Conclusions. While HD 206893 B could in principle be a planetary-mass companion, this possibility hinges on the unknown influence of the inner companion on the mass estimate o

Published
2021

9. The mass of beta Pictoris c from beta Pictoris b orbital motion

Author

Lacour, S., Wang, J. J., Rodet, L., Nowak, M., Shangguan, J., Beust, H., Lagrange, A-M, Abuter, R., Amorim, A., Asensio-Torres, R., Benisty, M., Berger, J-P, Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M-L, Bonnefoy, M., Bonnet, H., Bourdarot, G., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Choquet, E., Christiaens, V, Clenet, Y., du Foresto, V. Coude, Cridland, A., Dembet, R., Dexter, J., de Zeeuw, T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Gao, F., Garcia, P., Lopez, R. Garcia, Gendron, E., Genzel, R., Gillessen, S., Girard, J. H., Haubois, X., Heissel, G., Henning, Th, Hinkley, S., Hippler, S., Horrobin, M., Houlle, M., Hubert, Z., Jocou, L., Kammerer, J., Keppler, M., Kervella, P., Kreidberg, L., Lapeyrere, V, Le Bouquin, J-B, Lena, P., Lutz, D., Maire, A-L, Merand, A., Molliere, P., Monnier, J. D., Mouillet, D., Nasedkin, E., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Pfuhl, O., Rickman, E., Pueyo, L., Rameau, J., Rousset, G., Rustamkulov, Z., Samland, M., Shimizu, T., Sing, D., Stadler, J., Stolker, T., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., von Fellenberg, S. D., Ward-Duong, K., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Young, A., Lacour, S., Wang, J. J., Rodet, L., Nowak, M., Shangguan, J., Beust, H., Lagrange, A-M, Abuter, R., Amorim, A., Asensio-Torres, R., Benisty, M., Berger, J-P, Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M-L, Bonnefoy, M., Bonnet, H., Bourdarot, G., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Choquet, E., Christiaens, V, Clenet, Y., du Foresto, V. Coude, Cridland, A., Dembet, R., Dexter, J., de Zeeuw, T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Gao, F., Garcia, P., Lopez, R. Garcia, Gendron, E., Genzel, R., Gillessen, S., Girard, J. H., Haubois, X., Heissel, G., Henning, Th, Hinkley, S., Hippler, S., Horrobin, M., Houlle, M., Hubert, Z., Jocou, L., Kammerer, J., Keppler, M., Kervella, P., Kreidberg, L., Lapeyrere, V, Le Bouquin, J-B, Lena, P., Lutz, D., Maire, A-L, Merand, A., Molliere, P., Monnier, J. D., Mouillet, D., Nasedkin, E., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Pfuhl, O., Rickman, E., Pueyo, L., Rameau, J., Rousset, G., Rustamkulov, Z., Samland, M., Shimizu, T., Sing, D., Stadler, J., Stolker, T., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., von Fellenberg, S. D., Ward-Duong, K., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., and Young, A.

Abstract

Aims. We aim to demonstrate that the presence and mass of an exoplanet can now be effectively derived from the astrometry of another exoplanet. Methods. We combined previous astrometry of beta Pictoris b with a new set of observations from the GRAVITY interferometer. The orbital motion of beta Pictoris b is fit using Markov chain Monte Carlo simulations in Jacobi coordinates. The inner planet, beta Pictoris c, was also reobserved at a separation of 96 mas, confirming the previous orbital estimations. Results. From the astrometry of planet b only, we can (i) detect the presence of beta Pictoris c and (ii) constrain its mass to 10.04(-3.10)(+4.53) M-Jup . If one adds the astrometry of beta Pictoris c, the mass is narrowed down to 9.15(-1.06)(+1.08) M-Jup. The inclusion of radial velocity measurements does not affect the orbital parameters significantly, but it does slightly decrease the mass estimate to 8.89(-0.75)(+0.75) M-Jup.With a semimajor axis of 2.68 +/- 0.02 au, a period of 1221 +/- 15 days, and an eccentricity of 0.32 +/- 0.02, the orbital parameters of beta Pictoris c are now constrained as precisely as those of beta Pictoris b. The orbital configuration is compatible with a high-order mean-motion resonance (7:1). The impact of the resonance on the planets' dynamics would then be negligible with respect to the secular perturbations, which might have played an important role in the eccentricity excitation of the outer planet.

Published
2021

10. The mass of Beta Pictoris c from Beta Pictoris b orbital motion

Author

Lacour, S., Wang, J. J., Rodet, L., Nowak, M., Shangguan, J., Beust, H., Lagrange, A. -M., Abuter, R., Amorim, A., Asensio-Torres, R., Benisty, M., Berger, J. -P., Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M. -L., Bonnefoy, M., Bonnet, H., Bourdarot, G., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Choquet, E., Christiaens, V., Clénet, Y., Foresto, V. Coudé du, Cridland, A., Dembet, R., Dexter, J., de Zeeuw, P. T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Gao, F., Garcia, P., Lopez, R. Garcia, Gendron, E., Genzel, R., Gillessen, S., Girard, J. H., Haubois, X., Heißel, G., Henning, Th., Hinkley, S., Hippler, S., Horrobin, M., Houllé, M., Hubert, Z., Jocou, L., Kammerer, J., Keppler, M., Kervella, P., Kreidberg, L., Lapeyrère, V., Bouquin, J. -B. Le, Léna, P., Lutz, D., Maire, A. -L., Mérand, A., Mollière, P., Monnier, J. D., Mouillet, D., Nasedkin, E., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Pfuhl, O., Rickman, E., Pueyo, L., Rameau, J., Rousset, G., Rustamkulov, Z., Samland, M., Shimizu, T., Sing, D., Stadler, J., Stolker, T., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., von Fellenberg, S. D., Ward-Duong, K., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Young, A., Collaboration, the GRAVITY, Lacour, S., Wang, J. J., Rodet, L., Nowak, M., Shangguan, J., Beust, H., Lagrange, A. -M., Abuter, R., Amorim, A., Asensio-Torres, R., Benisty, M., Berger, J. -P., Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M. -L., Bonnefoy, M., Bonnet, H., Bourdarot, G., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Choquet, E., Christiaens, V., Clénet, Y., Foresto, V. Coudé du, Cridland, A., Dembet, R., Dexter, J., de Zeeuw, P. T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Gao, F., Garcia, P., Lopez, R. Garcia, Gendron, E., Genzel, R., Gillessen, S., Girard, J. H., Haubois, X., Heißel, G., Henning, Th., Hinkley, S., Hippler, S., Horrobin, M., Houllé, M., Hubert, Z., Jocou, L., Kammerer, J., Keppler, M., Kervella, P., Kreidberg, L., Lapeyrère, V., Bouquin, J. -B. Le, Léna, P., Lutz, D., Maire, A. -L., Mérand, A., Mollière, P., Monnier, J. D., Mouillet, D., Nasedkin, E., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Pfuhl, O., Rickman, E., Pueyo, L., Rameau, J., Rousset, G., Rustamkulov, Z., Samland, M., Shimizu, T., Sing, D., Stadler, J., Stolker, T., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., von Fellenberg, S. D., Ward-Duong, K., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Young, A., and Collaboration, the GRAVITY

Abstract

We aim to demonstrate that the presence and mass of an exoplanet can now be effectively derived from the astrometry of another exoplanet. We combined previous astrometry of $\beta$ Pictoris b with a new set of observations from the GRAVITY interferometer. The orbital motion of $\beta$ Pictoris b is fit using Markov chain Monte Carlo simulations in Jacobi coordinates. The inner planet, $\beta$ Pictoris c, was also reobserved at a separation of 96\,mas, confirming the previous orbital estimations. From the astrometry of planet b only, we can (i) detect the presence of $\beta$ Pictoris c and (ii) constrain its mass to $10.04^{+4.53}_{-3.10}\,M_{\rm Jup}$. If one adds the astrometry of $\beta$ Pictoris c, the mass is narrowed down to $9.15^{+1.08}_{-1.06}\,M_{\rm Jup}$. The inclusion of radial velocity measurements does not affect the orbital parameters significantly, but it does slightly decrease the mass estimate to $8.89^{+0.75}_{-0.75}\,M_{\rm Jup}$. With a semimajor axis of $2.68\pm0.02$\,au, a period of $1221\pm15$ days, and an eccentricity of $0.32\pm0.02$, the orbital parameters of $\beta$ Pictoris c are now constrained as precisely as those of $\beta$ Pictoris b. The orbital configuration is compatible with a high-order mean-motion resonance (7:1). The impact of the resonance on the planets' dynamics would then be negligible with respect to the secular perturbations, which might have played an important role in the eccentricity excitation of the outer planet., Comment: Accepted in A&A Letter

Published
2021
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11. GRAVITY K-band spectroscopy of HD 206893 B: brown dwarf or exoplanet

Author

Kammerer, J., Lacour, S., Stolker, T., Mollière, P., Sing, D. K., Nasedkin, E., Kervella, P., Wang, J. J., Ward-Duong, K., Nowak, M., Abuter, R., Amorim, A., Asensio-Torres, R., Bauböck, M., Benisty, M., Berger, J. -P., Beust, H., Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M. -L., Bonnefoy, M., Bonnet, H., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Choquet, E., Christiaens, V., Clénet, Y., Foresto, V. Coudé du, Cridland, A., Dembet, R., Dexter, J., de Zeeuw, P. T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Gao, F., Garcia, P., Lopez, R. Garcia, Gendron, E., Genzel, R., Gillessen, S., Girard, J., Haubois, X., Heißel, G., Henning, T., Hinkley, S., Hippler, S., Horrobin, M., Houllé, M., Hubert, Z., Jocou, L., Keppler, M., Kreidberg, L., Lagrange, A. -M., Lapeyrère, V., Bouquin, J. -B. Le, Léna, P., Lutz, D., Maire, A. -L., Mérand, A., Monnier, J. D., Mouillet, D., Müller, A., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Pfuhl, O., Pueyo, L., Rameau, J., Rodet, L., Rousset, G., Rustamkulov, Z., Shangguan, J., Shimizu, T., Stadler, J., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., von Fellenberg, S. D., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Collaboration, GRAVITY, Kammerer, J., Lacour, S., Stolker, T., Mollière, P., Sing, D. K., Nasedkin, E., Kervella, P., Wang, J. J., Ward-Duong, K., Nowak, M., Abuter, R., Amorim, A., Asensio-Torres, R., Bauböck, M., Benisty, M., Berger, J. -P., Beust, H., Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M. -L., Bonnefoy, M., Bonnet, H., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Choquet, E., Christiaens, V., Clénet, Y., Foresto, V. Coudé du, Cridland, A., Dembet, R., Dexter, J., de Zeeuw, P. T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Gao, F., Garcia, P., Lopez, R. Garcia, Gendron, E., Genzel, R., Gillessen, S., Girard, J., Haubois, X., Heißel, G., Henning, T., Hinkley, S., Hippler, S., Horrobin, M., Houllé, M., Hubert, Z., Jocou, L., Keppler, M., Kreidberg, L., Lagrange, A. -M., Lapeyrère, V., Bouquin, J. -B. Le, Léna, P., Lutz, D., Maire, A. -L., Mérand, A., Monnier, J. D., Mouillet, D., Müller, A., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Pfuhl, O., Pueyo, L., Rameau, J., Rodet, L., Rousset, G., Rustamkulov, Z., Shangguan, J., Shimizu, T., Stadler, J., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., von Fellenberg, S. D., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., and Collaboration, GRAVITY

Abstract

We aim to reveal the nature of the reddest known substellar companion HD 206893 B by studying its near-infrared colors and spectral morphology and by investigating its orbital motion. We fit atmospheric models for giant planets and brown dwarfs and perform spectral retrievals with petitRADTRANS and ATMO on the observed GRAVITY, SPHERE, and GPI spectra of HD 206893 B. To recover its unusual spectral features, we include additional extinction by high-altitude dust clouds made of enstatite grains in the atmospheric model fits. We also infer the orbital parameters of HD 206893 B by combining the $\sim 100~\mu\text{as}$ precision astrometry from GRAVITY with data from the literature and constrain the mass and position of HD 206893 C based on the Gaia proper motion anomaly of the system. The extremely red color and the very shallow $1.4~\mu\text{m}$ water absorption feature of HD 206893 B can be fit well with the adapted atmospheric models and spectral retrievals. Altogether, our analysis suggests an age of $\sim 3$-$300~\text{Myr}$ and a mass of $\sim 5$-$30~\text{M}_\text{Jup}$ for HD 206893 B, which is consistent with previous estimates but extends the parameter space to younger and lower-mass objects. The GRAVITY astrometry points to an eccentric orbit ($e = 0.29^{+0.06}_{-0.11}$) with a mutual inclination of $< 34.4~\text{deg}$ with respect to the debris disk of the system. While HD 206893 B could in principle be a planetary-mass companion, this possibility hinges on the unknown influence of the inner companion on the mass estimate of $10^{+5}_{-4}~\text{M}_\text{Jup}$ from radial velocity and Gaia as well as a relatively small but significant Argus moving group membership probability of $\sim 61\%$. However, we find that if the mass of HD 206893 B is $< 30~\text{M}_\text{Jup}$, then the inner companion HD 206893 C should have a mass between $\sim 8$-$15~\text{M}_\text{Jup}$., Comment: 28 pages, 19 figures, accepted for publication in A&A

Published
2021
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