Nowak, M., Lacour, S., Molliere, P., Wang, J., Charnay, B., van Dishoeck, E. F., Abuter, R., Amorim, A., Berger, J. P., Beust, H., Bonnefoy, M., Bonnet, H., Brandner, W., Buron, A., Cantalloube, F., Collin, C., Chapron, F., Clenet, Y., du Foresto, V. Coude, de Zeeuw, P. T., Dembet, R., Dexter, J., Duvert, G., Eckart, A., Eisenhauer, F., Schreiber, N. M. Foerster, Fedou, P., Lopez, R. Garcia, Gao, F., Gendron, E., Genzel, R., Gillessen, S., Haussmann, F., Henning, T., Hippler, S., Hubert, Z., Jocou, L., Kervella, P., Lagrange, A. -M., Lapeyrere, V., Le Bouquin, J. -B., Lena, P., Maire, A. -L., Ott, T., Paumard, T., Paladini, C., Perraut, K., Perrin, G., Pueyo, L., Pfuhl, O., Rabien, S., Rau, C., Rodriguez-Coira, G., Rousset, G., Scheithauer, S., Shangguan, J., Straub, O., Straubmeier, C., Sturm, E., Tacconi, L. J., Vincent, F., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S. and Ziegler, D. (2020). Peering into the formation history of beta Pictoris b with VLTI/GRAVITY long-baseline interferometry. Astron. Astrophys., 633. LES ULIS CEDEX A: EDP SCIENCES S A. ISSN 1432-0746

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Abstract

Context. beta Pictoris is arguably one of the most studied stellar systems outside of our own. Some 30 yr of observations have revealed a highly-structured circumstellar disk, with rings, belts, and a giant planet: beta Pictoris b. However very little is known about how this system came into being. Aims. Our objective is to estimate the C/O ratio in the atmosphere of beta Pictoris b and obtain an estimate of the dynamical mass of the planet, as well as to refine its orbital parameters using high-precision astrometry. Methods. We used the GRAVITY instrument with the four 8.2 m telescopes of the Very Large Telescope Interferometer to obtain K-band spectro-interferometric data on beta Pic b. We extracted a medium resolution (R = 500) K-band spectrum of the planet and a high-precision astrometric position. We estimated the planetary C/O ratio using two different approaches (forward modeling and free retrieval) from two different codes (ExoREM and petitRADTRANS, respectively). Finally, we used a simplified model of two formation scenarios (gravitational collapse and core-accretion) to determine which can best explain the measured C/O ratio. Results. Our new astrometry disfavors a circular orbit for beta Pic b (e = 0.15(-0.04)(+0.05)). Combined with previous results and with HIPPARCOS/Gaia measurements, this astrometry points to a planet mass of M = 12.7 +/- 2.2 M-Jup. This value is compatible with the mass derived with the free-retrieval code petitRADTRANS using spectral data only. The forward modeling and free-retrieval approches yield very similar results regarding the atmosphere of beta Pic b. In particular, the C/O ratios derived with the two codes are identical (0.43 +/- 0.05 vs. 0.43(-0.03)(+0.04)). We argue that if the stellar C/O in beta Pic is Solar, then this combination of a very high mass and a low C/O ratio for the planet suggests a formation through core-accretion, with strong planetesimal enrichment.

Item Type: Journal Article
Creators:
CreatorsEmailORCIDORCID Put Code
Nowak, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Lacour, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Molliere, P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Wang, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Charnay, B.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
van Dishoeck, E. F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Abuter, R.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Amorim, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Berger, J. P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Beust, H.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Bonnefoy, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Bonnet, H.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Brandner, W.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Buron, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Cantalloube, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Collin, C.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Chapron, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Clenet, Y.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
du Foresto, V. CoudeUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
de Zeeuw, P. T.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Dembet, R.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Dexter, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Duvert, G.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Eckart, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Eisenhauer, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Schreiber, N. M. FoersterUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Fedou, P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Lopez, R. GarciaUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Gao, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Gendron, E.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Genzel, R.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Gillessen, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Haussmann, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Henning, T.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Hippler, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Hubert, Z.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Jocou, L.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Kervella, P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Lagrange, A. -M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Lapeyrere, V.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Le Bouquin, J. -B.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Lena, P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Maire, A. -L.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Ott, T.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Paumard, T.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Paladini, C.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Perraut, K.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Perrin, G.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Pueyo, L.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Pfuhl, O.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Rabien, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Rau, C.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Rodriguez-Coira, G.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Rousset, G.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Scheithauer, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Shangguan, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Straub, O.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Straubmeier, C.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Sturm, E.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Tacconi, L. J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Vincent, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Widmann, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Wieprecht, E.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Wiezorrek, E.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Woillez, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Yazici, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Ziegler, D.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
URN: urn:nbn:de:hbz:38-348557
DOI: 10.1051/0004-6361/201936898
Journal or Publication Title: Astron. Astrophys.
Volume: 633
Date: 2020
Publisher: EDP SCIENCES S A
Place of Publication: LES ULIS CEDEX A
ISSN: 1432-0746
Language: English
Faculty: Unspecified
Divisions: Unspecified
Subjects: no entry
Uncontrolled Keywords:
KeywordsLanguage
LOW-MASS STARS; BROWN DWARFS; PLANETARY-ATMOSPHERES; EVOLUTIONARY MODELS; DUST; TEMPERATURE; CONSISTENT; RETRIEVAL; EFFICIENT; JUPITERMultiple languages
Astronomy & AstrophysicsMultiple languages
URI: http://kups.ub.uni-koeln.de/id/eprint/34855

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