J/A+A/665/A128 LkHα 330 SPHERE/VLT and ALMA images (Pinilla+, 2022)
Distributions of gas and small and large grains in the LkHα 330 disk
trace a young planetary system.
Pinilla P., Benisty M., Kurtovic N.T., Bae J., Dong R., Zhu Z., Andrews S.,
Carpenter J., Ginski C., Huang J., Isella A., Perez L., Ricci L.,
Rosotti G., Villenave M., Wilner D.
<Astron. Astrophys. 665, A128 (2022)>
=2022A&A...665A.128P 2022A&A...665A.128P (SIMBAD/NED BibCode)
ADC_Keywords: Stars, pre-main sequence ; Accretion ; Carbon monoxide ;
Polarization
Keywords: planets and satellites: formation - circumstellar matter -
planet-disk interactions - protoplanetary disks
Abstract:
Planets that are forming around young stars are expected to leave
clear imprints in the distribution of the gas and dust of their
parental protoplanetary disks. In this paper, we present new scattered
light and millimeter observations of the protoplanetary disk around
LkHα 330, using SPHERE/VLT and ALMA, respectively. The
scattered-light SPHERE observations reveal an asymmetric ring at
around 45au from the star in addition to two spiral arms with similar
radial launching points at around 90au. The millimeter observations
from ALMA (resolution of 0.06''*0.04'') mainly show an asymmetric ring
located at 110au from the star. In addition to this asymmetry, there
are two faint symmetric rings at 60au and 200au. The 12CO, 13CO,
and C18O lines seem to be less abundant in the inner disk (these
observations have a resolution of 0.16''*0.11''). The 13CO peaks at
a location similar to the inner ring observed with SPHERE, suggesting
that this line is optically thick and traces variations of disk
temperature instead of gas surface-density variations, while the
C18O peaks slightly further away at around 60au. We compare our
observations with hydrodynamical simulations that include gas and dust
evolution, and conclude that a 10M{Jup} mass planet at 60au and in
an eccentric orbit (e=0.1) can qualitatively explain most of the
observed structures. A planet in a circular orbit leads to a much
narrower concentration in the millimeter emission, while a planet in a
more eccentric orbit leads to a very eccentric cavity as well. In
addition, the outer spiral arm launched by the planet changes its
pitch angle along the spiral due to the eccentricity and when it
interacts with the vortex, potentially appearing in observations as
two distinct spirals. Our observations and models show that LkHα
330, is an interesting target to search for (eccentric-) planets while
they are still embedded in their parental disk, making it an excellent
candidate for studies on planet-disk interaction.
Description:
We obtained observations of LkHα 330 at the Very Large Telescope
located at Cerro Paranal, Chile, using the SPHERE instrument, a
high-contrast imager with an extreme adaptive optics system under
program IDs 098.C-0760(B) and 100.C-0452(A) (PI: M. Benisty). In this
paper, we report new polarimetric observations taken on 2017-10-05 and
2017-10-11 and obtained in the near-infrared (J- (1.2um) and H-
(1.65um), respectively) with the IRDIS instrument. For all the IRDIS
observations presented in this paper, we use a 185 mas diameter
coronagraph (NALCYJH_S) to enhance the signal-to-noise ratio in the
outer disk regions. The plate scale is 12.26mas and 12.25mas per
pixel, for the J- and H- band data, respectively.
Objects:
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RA (2000) DE Designation(s)
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03 45 48.28 +32 24 11.9 LkHa 330 = HBC 20
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 221 8 List of fits images
fits/* . 8 Individual fits images
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See also:
J/A+A/564/A51 : 3mm maps of 4 transition disks (Pinilla+, 2014)
Byte-by-byte Description of file: list.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 23 I4 --- Nx Number of pixels along X-axis
25- 28 I4 --- Ny Number of pixels along Y-axis
30- 52 A23 "datime" Obs.date Observation date
54- 60 F7.3 GHz Freq ? Observed frequency
62- 65 I4 Kibyte size Size of FITS file
67-124 A58 --- FileName Name of FITS file, in subdirectory fits
126-221 A96 --- Title Title of the FITS file
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Acknowledgements:
Paola Pinilla, pinilla(at)mpia.de
(End) Patricia Vannier [CDS] 28-Jul-2022