TY - JOUR
T1 - Kinematic Evidence for an Embedded Planet in the IM Lupi Disk
AU - Verrios, Harrison J.
AU - Price, Daniel J.
AU - Pinte, Christophe
AU - Hilder, Thomas
AU - Calcino, Josh
N1 - Funding Information:
D.J.P. thanks Judit Szulagyi for useful discussions about the perils of vacuum cleaner sink particles at the “Kinematics of Planet Formation” meeting in 2019; also Giuseppe Lodato and Richard Teague for useful discussions. J.C. acknowledges support from LANL/LDRD program (approved for release as LA-UR-21-31387). We used OzSTAR and Gadi supercomputing facilities funded by Swinburne University (OzSTAR) and the Australian Government via the National Computing Initiative. D.P. and C.P. acknowledge Australian Research Council funding via DP180104235 and FT170100040. We made use of ALMA data: ADS/JAO.ALMA#2018.1.01055.L, ADS/JAO.ALMA#2016.1.00484.L. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. We thank the referee for useful suggestions.
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/7/1
Y1 - 2022/7/1
N2 - We test the hypothesis that an embedded giant planet in the IM Lupi protostellar disk can produce velocity kinks seen in CO line observations as well as the spiral arms seen in scattered light and continuum emission. We inject planets into 3D hydrodynamics simulations of IM Lupi, generating synthetic observations using Monte Carlo radiative transfer. We find that an embedded planet of 2-3 M Jup can reproduce non-Keplerian velocity perturbations, or “kinks”, in the 12CO J = 2-1 channel maps. Such a planet can also explain the spiral arms seen in 1.25 mm dust continuum emission and 1.6 μm scattered-light images. We show that the wake of the planet can be traced in the observed peak velocity map, which appears to closely follow the morphology expected from our simulations and from analytic models of planet-disk interaction.
AB - We test the hypothesis that an embedded giant planet in the IM Lupi protostellar disk can produce velocity kinks seen in CO line observations as well as the spiral arms seen in scattered light and continuum emission. We inject planets into 3D hydrodynamics simulations of IM Lupi, generating synthetic observations using Monte Carlo radiative transfer. We find that an embedded planet of 2-3 M Jup can reproduce non-Keplerian velocity perturbations, or “kinks”, in the 12CO J = 2-1 channel maps. Such a planet can also explain the spiral arms seen in 1.25 mm dust continuum emission and 1.6 μm scattered-light images. We show that the wake of the planet can be traced in the observed peak velocity map, which appears to closely follow the morphology expected from our simulations and from analytic models of planet-disk interaction.
UR - http://www.scopus.com/inward/record.url?scp=85135239096&partnerID=8YFLogxK
U2 - 10.3847/2041-8213/ac7f44
DO - 10.3847/2041-8213/ac7f44
M3 - Article
AN - SCOPUS:85135239096
SN - 2041-8205
VL - 934
JO - The Astrophysical Journal Letters
JF - The Astrophysical Journal Letters
IS - 1
M1 - L11
ER -