Two cold belts in the debris disk around the G-type star NZ Lup. (arXiv:1904.02746v1 [astro-ph.EP])

Two cold belts in the debris disk around the G-type star NZ Lup. (arXiv:1904.02746v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Boccaletti_A/0/1/0/all/0/1">A. Boccaletti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thebault_P/0/1/0/all/0/1">P. Thébault</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pawellek_N/0/1/0/all/0/1">N. Pawellek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lagrange_A/0/1/0/all/0/1">A.-M. Lagrange</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galicher_R/0/1/0/all/0/1">R. Galicher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desidera_S/0/1/0/all/0/1">S. Desidera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Milli_J/0/1/0/all/0/1">J. Milli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kral_Q/0/1/0/all/0/1">Q. Kral</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonnefoy_M/0/1/0/all/0/1">M. Bonnefoy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Augereau_J/0/1/0/all/0/1">J.-C. Augereau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maire_A/0/1/0/all/0/1">A.-L. Maire</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henning_T/0/1/0/all/0/1">T. Henning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beust_H/0/1/0/all/0/1">H. Beust</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodet_L/0/1/0/all/0/1">L. Rodet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avenhaus_H/0/1/0/all/0/1">H. Avenhaus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhowmik_T/0/1/0/all/0/1">T. Bhowmik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonavita_M/0/1/0/all/0/1">M. Bonavita</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chauvin_G/0/1/0/all/0/1">G. Chauvin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cheetham_A/0/1/0/all/0/1">A. Cheetham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cudel_M/0/1/0/all/0/1">M. Cudel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feldt_M/0/1/0/all/0/1">M. Feldt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gratton_R/0/1/0/all/0/1">R. Gratton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hagelberg_J/0/1/0/all/0/1">J. Hagelberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Janin_Potiron_P/0/1/0/all/0/1">P. Janin-Potiron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Langlois_M/0/1/0/all/0/1">M. Langlois</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Menard_F/0/1/0/all/0/1">F. Ménard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mesa_D/0/1/0/all/0/1">D. Mesa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meyer_M/0/1/0/all/0/1">M. Meyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peretti_S/0/1/0/all/0/1">S. Peretti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perrot_C/0/1/0/all/0/1">C. Perrot</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schmidt_T/0/1/0/all/0/1">T. Schmidt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sissa_E/0/1/0/all/0/1">E. Sissa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vigan_A/0/1/0/all/0/1">A. Vigan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rickman_E/0/1/0/all/0/1">E. Rickman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Magnard_Y/0/1/0/all/0/1">Y. Magnard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maurel_D/0/1/0/all/0/1">D. Maurel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moeller_Nilsson_O/0/1/0/all/0/1">O. Moeller-Nilsson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perret_D/0/1/0/all/0/1">D. Perret</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sauvage_J/0/1/0/all/0/1">J.-F. Sauvage</a>

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 $sim$85 and $sim$115,au,
and with a mutual inclination of about 5$degb$. 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.

The dynamical perturbation of planets in the dust distribution can be
revealed with high-contrast imaging in a variety of structures.

We discuss the implication of the existence of two belts and their relative
inclination with respect to the presence of planets.

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