J/A+A/625/A21 High contrast images of NZ Lup (Boccaletti+, 2019)
Two cold belts in the debris disk around the G-type star NZ Lup.
Boccaletti A., Thebault P., Pawellek N., Lagrange A.-M., Galicher R.,
Desidera S., Milli J., Kral Q., Bonnefoy M., Augereau J.-C., Maire A.L.,
Henning T., Beust H., Rodet L., Avenhaus H., Bhowmik K., Bonavita M.,
Chauvin G., Cheetham A., Cudel M., Feldt M., Gratton R., Halbergerg J.,
Janin-Potiron P., Langlois M., Menard F., Mesa D., Meyer M., Peretti S.,
Perrot C., Schmidt T., Sissa E., Vigan A., Rickman E., Magnard Y.,
Maurel D., Moeller-Nilsson O., Perret D., Sauvage J.-F.
<Astron. Astrophys. 625, A21 (2019)>
=2019A&A...625A..21B 2019A&A...625A..21B (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Stars, G-type
Keywords: stars: individual: NZ Lup - planet-disk interactions -
techniques: high angular resolution - techniques: image processing
Abstract:
Planetary systems hold the imprint of the formation and of the
evolution of planets especially at young ages, and in particular at
the stage when the gas has dissipated leaving mostly secondary dust
grains. The dynamical perturbation of planets in the dust distribution
can be revealed with high-contrast imaging in a variety of structures.
SPHERE, the high-contrast imaging device installed at the VLT, was
designed to search for young giant planets in long period, but is also
able to resolve fine details of planetary systems at the scale of
astronomical units in the scattered-light regime. As a young and
nearby star, NZ Lup was observed in the course of the SPHERE survey. A
debris disk had been formerly identified with HST/NICMOS. We observed
this system in the near-infrared with the camera in narrow and broad
band filters and with the integral field spectrograph. High contrasts
are achieved by the mean of pupil tracking combined with angular
differential imaging algorithms. The high angular resolution provided
by SPHERE allows us to reveal a new feature in the disk which is
interpreted as a superimposition of two belts of planetesimals located
at stellocentric distances of ∼85 and ∼115au, and with a mutual
inclination of about 5°. Despite the very high inclination of the
disk with respect to the line of sight, we conclude that the presence
of a gap, that is, a void in the dust distribution between the belts,
is likely. We discuss the implication of the existence of two belts
and their relative inclination with respect to the presence of
planets.
Description:
SPHERE/IRDIS and SPHERE/IFS total intensity images of NZ Lup, in
contrast delivered by post-processing with respect to the maximum of
the star's PSF.
Objects:
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RA (2000) DE Designation(s)
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15 53 27.29 -42 16 00.7 NZ Lup = HD 141943
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 164 4 List of fits images
fits/* . 4 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- 10 F10.6 deg RAdeg Right Ascension of center (J2000)
11- 19 F9.5 deg DEdeg Declination of center (J2000)
21- 24 I4 --- Nx Number of pixels along X-axis
26- 29 I4 --- Ny Number of pixels along Y-axis
31- 54 A24 "datime" Obs.date Observation date
56- 59 I4 Kibyte size Size of FITS file
61-110 A50 --- FileName Name of FITS file, in subdirectory fits
112-164 A53 --- Title Title of the FITS file
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Acknowledgements:
Anthony Boccaletti, Anthony.Boccaletti(at)obspm.fr
(End) Patricia Vannier [CDS] 01-Apr-2019