J/A+A/689/A65 ALMA line emission obs. of PDS 70 disk (Rampinelli+, 2024)
ALMA high-resolution observations unveil planet formation shaping
molecular emission in the PDS 70 disk.
Rampinelli L., Facchini S., Leemker M., Bae J., Benisty M., Teague R.,
Law C.J., Oberg K.I., Portilla-Revelo B., Cridland A.J.
<Astron. Astrophys. 689, A65 (2024)>
=2024A&A...689A..65R 2024A&A...689A..65R (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Spectroscopy ;
Radio sources
Keywords: astrochemistry - protoplanetary disks - stars: individual: PDS70
Abstract:
With two directly detected protoplanets, the PDS 70 system is a unique
source in which to study the complex interplay between forming planets
and their natal environment. The large dust cavity carved by the two
giant planets can affect the disk chemistry, and therefore the
molecular emission morphology. On the other hand, chemical properties
of the gas component of the disk are expected to leave an imprint on
the planetary atmospheres. In this work, we reconstruct the emission
morphology of a rich inventory of molecular tracers in the PDS 70
disk, and we look for possible chemical signatures of the two actively
accreting protoplanets, PDS b and c. We leverage Atacama Large
Millimeter/submillimeter Array (ALMA) band 6 high-angular-resolution
and deep- sensitivity line emission observations, together with image
and uv-plane techniques, to boost the detection of faint lines. We
robustly detect ring-shaped emission from 12CO, 13CO, C18O,
H13CN, HC15N, DCN, H2CO, CS, C2H, and H13CO+ lines in
unprecedented detail. Most of the molecular tracers show a peak of the
emission inside the millimeter dust peak. We interpret this as the
direct impact of the effective irradiation of the cavity wall, as a
result of the planet formation process. Moreover, we have found
evidence of an O-poor gas reservoir in the outer disk, which is
supported by the observations of bright C-rich molecules, the
non-detection of SO, and a lower limit on the CS/SO ratio of ∼1 .
Eventually, we provide the first detection of the c-C3H2
transitions at 218.73GHz, and the marginal detection of an azimuthal
asymmetry in the higher-energy H2CO (32,1-22,0) line, which
could be due to accretion heating near PDS 70b.
Description:
Datacubes used for the analysis stored with the following format
PDS70_.fits. For multiple lines of same molecule the
transition is specified in the name.
Objects:
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RA (2000) DE Designation(s)
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14 08 10.15 -41 23 52.5 PDS 70 = TIC 179413040
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
list.dat 156 15 List of fits datacubes
fits/* . 15 Individual fits datacubes
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See also:
J/A+A/632/A25 : PDS70 VLT/SPHERE images (Mesa+, 2019)
Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
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- 32 I3 --- Nz Number of slices
34- 56 A23 "datime" Obs.date Observation date
58- 64 F7.3 GHz bFreq Lower value of frequency interval
66- 72 F7.3 GHz BFreq Upper value of frequency interval
74- 84 E11.6 Hz dFreq Frequency resolution
86- 91 I6 Kibyte size Size of FITS file
93-115 A23 --- FileName Name of FITS file, in subdirectory fits
117-156 A40 --- Title Title of the FITS file
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Acknowledgements:
Luna Rampinelli, luna.rampinelli(at)unimi.it
(End) Luna Rampinelli [UniMi, Italy], Patricia Vannier [CDS] 01-Aug-2024