2023AJ....166..257B

Query : 2023AJ....166..257B

2023AJ....166..257B - Astron. J., 166, 257 (2023/December-0)

First VLTI/GRAVITY Observations of HIP 65426 b: Evidence for a Low or Moderate Orbital Eccentricity.

BLUNT S., BALMER W.O., WANG J.J., LACOUR S., PETRUS S., BOURDAROT G., KAMMERER J., POURRE N., RICKMAN E., SHANGGUAN J., WINTERHALDER T., ABUTER R., AMORIM A., ASENSIO-TORRES R., BENISTY M., BERGER J.-P., BEUST H., BOCCALETTI A., BOHN A., BONNEFOY M., BONNET H., BRANDNER W., CANTALLOUBE F., CASELLI P., CHARNAY B., CHAUVIN G., CHAVEZ A., CHOQUET E., CHRISTIAENS V., CLENET Y., COUDE DU FORESTO V., CRIDLAND A., DEMBET R., DRESCHER A., DUVERT G., ECKART A., EISENHAUER F., FEUCHTGRUBER H., GARCIA P., GARCIA LOPEZ R., GENDRON E., GENZEL R., GILLESSEN S., GIRARD J.H., HAUBOIS X., HEISSEL G., HENNING T., HINKLEY S., HIPPLER S., HORROBIN M., HOULLE M., HUBERT Z., JOCOU L., KEPPLER M., KERVELLA P., KREIDBERG L., LAGRANGE A.-M., LAPEYRERE V., LE BOUQUIN J.-B., LENA P., LUTZ D., MAIRE A.-L., MANG F., MARLEAU G.-D., MERAND A., MOLLIERE P., MONNIER J.D., MORDASINI C., MOUILLET D., NASEDKIN E., NOWAK M., OTT T., OTTEN G.P.P.L., PALADINI C., PAUMARD T., PERRAUT K., PERRIN G., PFUHL O., PUEYO L., RAMEAU J., RODET L., RUSTAMKULOV Z., SHIMIZU T., SING D., STOLKER T., STRAUBMEIER C., STURM E., TACCONI L.J., VAN DISHOECK E.F., VIGAN A., VINCENT F., WARD-DUONG K., WIDMANN F., WIEPRECHT E., WIEZORREK E., WOILLEZ J., YAZICI S., YOUNG A. (The exoGRAVITY Collaboration)

Abstract (from CDS):

Giant exoplanets have been directly imaged over orders of magnitude of orbital separations, prompting theoretical and observational investigations of their formation pathways. In this paper, we present new VLTI/GRAVITY astrometric data of HIP 65426 b, a cold, giant exoplanet which is a particular challenge for most formation theories at a projected separation of 92 au from its primary. Leveraging GRAVITY's astrometric precision, we present an updated eccentricity posterior that disfavors large eccentricities. The eccentricity posterior is still prior dependent, and we extensively interpret and discuss the limits of the posterior constraints presented here. We also perform updated spectral comparisons with self-consistent forward-modeled spectra, finding a best-fit ExoREM model with solar metallicity and C/O = 0.6. An important caveat is that it is difficult to estimate robust errors on these values, which are subject to interpolation errors as well as potentially missing model physics. Taken together, the orbital and atmospheric constraints paint a preliminary picture of formation inconsistent with scattering after disk dispersal. Further work is needed to validate this interpretation. Analysis code used to perform this work is available on GitHub: https://github.com/sblunt/hip65426.

Abstract Copyright: © 2023. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Exoplanets - Exoplanet formation - Astrometry - Optical interferometry

Simbad objects: 10

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Number of rows : 10
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 * bet Pic b Pl 05 47 17.0876901 -51 03 59.441135           ~ 627 1
2 * bet Pic c Pl 05 47 17.0876901 -51 03 59.441135           ~ 108 0
3 HD 73900 ** 08 39 22.1083105800 -36 36 24.011860968   6.526 6.114     F3/5V 54 0
4 HD 91881 ** 10 36 04.50734 -26 40 31.7332       7.21   F5V 73 0
5 NAME Lower Centaurus Crux As* 12 19 -57.1           ~ 565 1
6 HD 116434 ** 13 24 36.0977360304 -51 30 16.044711840   7.08 6.98   6.87 A2V 95 0
7 HD 116434C BD* 13 24 36.13 -51 30 16.7           L5-7 123 1
8 HD 123227 ** 14 07 41.5263183624 -49 52 03.409704588       7.17   G3V 42 0
9 HD 163296 Ae* 17 56 21.2881851168 -21 57 21.871819008 7.00 6.93 6.85 6.86 6.67 A3VaekA1mA1 1301 0
10 HD 218396 El* 23 07 28.7157209544 +21 08 03.310767492   6.21 5.953     F0+VkA5mA5 1285 0

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