J/A+A/673/A39 SPHERE DPI image of HD121617 in J band (Perrot+, 2023)
Morphology of the gas-rich debris disk around HD 121617 with SPHERE
observations in polarized light.
Perrot C., Olofsson J., Kral Q., Thebault P., Montesinos M., Kennedy G.,
Bayo A., Iglesias D., van Holstein R., Pinte C.
<Astron. Astrophys. 673, A39 (2023)>
=2023A&A...673A..39P 2023A&A...673A..39P (SIMBAD/NED BibCode)
ADC_Keywords: Stars, early-type ; Photometry, infrared ; Polarization
Keywords: techniques: polarimetric - techniques: high angular resolution -
methods: observational - infrared: planetary systems -
protoplanetary disks - zodiacal dust
Abstract:
Debris disks are the signposts of collisionally eroding planetesimal
circumstellar belts, whose study can put important constraints on the
structure of extrasolar planetary systems. The best constraints on the
morphology of disks are often obtained from spatially resolved
observations in scattered light. Here, we investigate the young
(∼16Myr) bright gas-rich debris disk around HD 121617.
We use new scattered-light observations with VLT/SPHERE to
characterize the morphology and the dust properties of this disk. From
these properties we can then derive constraints on the physical and
dynamical environment of this system, for which significant amounts of
gas have been detected.
The disk morphology is constrained by linear-polarimetric observations
in the J band. Based on our modeling results and archival photometry,
we also model the SED to put constraints on the total dust mass and
the dust size distribution. We explore different scenarios that could
explain these new constraints.
We present the first resolved image in scattered light of the debris
disk HD 121617. We fit the morphology of the disk, finding a
semi-major axis of 78.3±0.2au, an inclination of 43.1±0.2° and
a position angle of the major axis with respect to north, of
239.8±0.3°, compatible with the previous continuum and CO
detection with ALMA. Our analysis shows that the disk has a very sharp
inner edge, possibly sculpted by a yet-undetected planet or gas drag.
While less sharp, its outer edge is steeper than expected for
unperturbed disks, which could also be due to a planet or gas drag,
but future observations probing the system farther from the main belt
would help explore this further. The SED analysis leads to a dust mass
of 0.21±0.02M⊕ and a minimum grain size of 0.87±0.12um,
smaller than the blowout size by radiation pressure, which is not
unexpected for very bright collisionally active disks.
Description:
The fits files contains the reduced SPHERE polarimetric observation in
broadband J used in fig 1. (the Q_phi and the U_phi images). The raw
images are available on the ESO archives and can be reduced with the
ESO pipeline, the SPHERE data center
(https://sphere.osug.fr/spip.php?rubrique16) or the pipeline IRDAP
(see reference in the paper).
Objects:
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RA (2000) DE Designation(s)
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13 57 41.12 -47 00 34.2 HD 121617 = IRAS 13545-4645
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
list.dat 103 2 List of fits images
fits/* . 2 Individual fits images
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Byte-by-byte Description of file: list.dat
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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- 26 F7.5 arcsec/pix scale Scale of the image
28- 31 I4 --- Nx Number of pixels along X-axis
33- 36 I4 --- Ny Number of pixels along Y-axis
38- 61 A24 "datime" Obs.date Observation date
63- 66 F4.2 um lambda Wavelength for observed band
68- 71 I4 Kibyte size Size of FITS file
73- 81 A9 --- FileName Name of FITS file, in subdirectory fits
83-103 A21 --- Title Title of the FITS file
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Acknowledgements:
Clement Perrot, clement.perrot(at)obspm.fr
(End) Patricia Vannier [CDS] 13-Feb-2023