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Spectral and orbital characterisation of the directly imaged giant planet HIP 65426 b
Vise andre og tillknytning
Rekke forfattare: 412019 (engelsk)Inngår i: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 622, artikkel-id A80Artikkel i tidsskrift (Fagfellevurdert) Published
Abstract [en]

HIP 65426 b is a recently discovered exoplanet imaged during the course of the SPHERE-SHINE survey. Here we present new L' and M' observations of the planet from the NACO instrument at the VLT from the NACO-ISPY survey, as well as a new Y-H spectrum and K-band photometry from SPHERE-SHINE. Using these data, we confirm the nature of the companion as a warm, dusty planet with a mid-L spectral type. From comparison of its SED with the BT-Settl atmospheric models, we derive a best-fit effective temperature of T-eff = 1618 +/- 7 K, surface gravity log g = 3 : 78(-0.03)(+0.04) and radius R = 1.17 +/- 0.04 R-J (statistical uncertainties only). Using the DUSTY and COND isochrones we estimate a mass of 8 +/- 1 MJ. Combining the astrometric measurements from our new datasets and from the literature, we show the first indications of orbital motion of the companion (2.6 sigma significance) and derive preliminary orbital constraints. We find a highly inclined orbit (i = 107(+13)(-10) deg) with an orbital period of 800(+1200)(-400) yr. We also report SPHERE sparse aperture masking observations that investigate the possibility that HIP 65426 b was scattered onto its current orbit by an additional companion at a smaller orbital separation. From this data we rule out the presence of brown dwarf companions with masses greater than 16 M-J at separations larger than 3AU, significantly narrowing the parameter space for such a companion.

sted, utgiver, år, opplag, sider
2019. Vol. 622, artikkel-id A80
Emneord [en]
stars: individual: HIP 65426, planets and satellites: atmospheres, techniques: high angular resolution, planets and satellites: detection, planetary systems
HSV kategori
Identifikatorer
URN: urn:nbn:se:su:diva-166781DOI: 10.1051/0004-6361/201834112ISI: 000457210500003OAI: oai:DiVA.org:su-166781DiVA, id: diva2:1295738
Tilgjengelig fra: 2019-03-12 Laget: 2019-03-12 Sist oppdatert: 2019-03-12bibliografisk kontrollert

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