Keck/OSIRIS Paβ high-contrast imaging of the PDS 70 planetary system
Taichi Uyama
- Fonction : Auteur
Yuhiko Aoyama
- Fonction : Auteur
Charles Beichman
- Fonction : Auteur
Jun Hashimoto
- Fonction : Auteur
Ruobing Dong
- Fonction : Auteur
Yasuhiro Hasegawa
- Fonction : Auteur
Masahiro Ikoma
- Fonction : Auteur
Dimitri Mawet
- Fonction : Auteur
Michael Mcelwain
- Fonction : Auteur
Jean-Baptiste Ruffio
- Fonction : Auteur
Kevin Wagner
- Fonction : Auteur
Jason Wang
- Fonction : Auteur
Yifan Zhou
- Fonction : Auteur
Résumé
We present a high-contrast imaging search for Paβ line emission from protoplanets in the PDS 70 system with Keck/OSIRIS integral field spectroscopy. We applied the high-resolution spectral differential imaging technique to the OSIRIS J-band data but did not detect the Paβ line at the level predicted using the parameters of Hashimoto et al. (2020). This lack of Paβ emission suggests the VLT/MUSE-based study may have overestimated the line width of Hα. We compared our Paβ detection limits with the previous Hα flux and Hβ limits and estimated AV to be~0.9 and 2.0 for PDS 70 b and c respectively. In particular, PDS 70 b's AV is much smaller than implied by high-contrast near-infrared studies, which suggests the infrared-continuum photosphere and the hydrogen-emitting regions exist at different heights above the forming planet.
Domaines
Planète et Univers [physics]Format du dépôt | Notice |
---|---|
Type de dépôt | Communication dans un congrès |
Titre |
en
Keck/OSIRIS Paβ high-contrast imaging of the PDS 70 planetary system
|
Résumé |
en
We present a high-contrast imaging search for Paβ line emission from protoplanets in the PDS 70 system with Keck/OSIRIS integral field spectroscopy. We applied the high-resolution spectral differential imaging technique to the OSIRIS J-band data but did not detect the Paβ line at the level predicted using the parameters of Hashimoto et al. (2020). This lack of Paβ emission suggests the VLT/MUSE-based study may have overestimated the line width of Hα. We compared our Paβ detection limits with the previous Hα flux and Hβ limits and estimated A<SUB>V</SUB> to be~0.9 and 2.0 for PDS 70 b and c respectively. In particular, PDS 70 b's A<SUB>V</SUB> is much smaller than implied by high-contrast near-infrared studies, which suggests the infrared-continuum photosphere and the hydrogen-emitting regions exist at different heights above the forming planet.
|
Auteur(s) |
Taichi Uyama
, Chen Xie
1
, Yuhiko Aoyama
, Charles Beichman
, Jun Hashimoto
, Ruobing Dong
, Yasuhiro Hasegawa
, Masahiro Ikoma
, Dimitri Mawet
, Michael Mcelwain
, Jean-Baptiste Ruffio
, Kevin Wagner
, Jason Wang
, Yifan Zhou
1
LAM -
Laboratoire d'Astrophysique de Marseille
( 179944 )
- Pôle de l'Étoile Site de Château-Gombert 38, rue Frédéric Joliot-Curie 13388 Marseille cedex 13
- France
|
Comité de lecture |
Oui
|
Langue du document |
Anglais
|
Vulgarisation |
Non
|
Audience |
Internationale
|
Actes |
Oui
|
Date de publication |
2022
|
Volume |
54
|
Titre du congrès |
AASTCS9, Exoplanets 4, id. 102.173. Bulletin of the American Astronomical Society
|
Date début congrès |
2022
|
Ville |
à renseigner
|
Pays |
zz
|
Domaine(s) |
|
ADS Id | 2022BAAS...54e.173U |
Loading...