2016A&A...588A...8G


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.08CET02:37:50

2016A&A...588A...8G - Astronomy and Astrophysics, volume 588A, 8-8 (2016/4-1)

The SPHERE view of the planet-forming disk around HD 100546.

GARUFI A., QUANZ S.P., SCHMID H.M., MULDERS G.D., AVENHAUS H., BOCCALETTI A., GINSKI C., LANGLOIS M., STOLKER T., AUGEREAU J.-C., BENISTY M., LOPEZ B., DOMINIK C., GRATTON R., HENNING T., JANSON M., MENARD F., MEYER M.R., PINTE C., SISSA E., VIGAN A., ZURLO A., BAZZON A., BUENZLI E., BONNEFOY M., BRANDNER W., CHAUVIN G., CHEETHAM A., CUDEL M., DESIDERA S., FELDT M., GALICHER R., KASPER M., LAGRANGE A.-M., LANNIER J., MAIRE A.L., MESA D., MOUILLET D., PERETTI S., PERROT C., SALTER G. and WILDI F.

Abstract (from CDS):

Context. The mechanisms governing planet formation are not fully understood. A new era of high-resolution imaging of protoplanetary disks has recently started, thanks to new instruments such as SPHERE, GPI, and ALMA. The planet formation process can now be directly studied by imaging both planetary companions embedded in disks and their effect on disk morphology.
Aims. We image disk features that could be potential signs of planet-disk interaction with unprecedented spatial resolution and sensitivity. Two companion candidates have been claimed in the disk around the young Herbig Ae/Be star HD 100546. Thus, this object serves as an excellent target for our investigation of the natal environment of giant planets.
Methods. We exploit the power of extreme adaptive optics operating in conjunction with the new high-contrast imager SPHERE to image HD 100546 in scattered light. We obtained the first polarized light observations of this source in the visible (with resolution as fine as 2AU) and new H and K band total intensity images that we analyzed with the pynpoint package.
Results. The disk shows a complex azimuthal morphology, where multiple scattering of photons most likely plays an important role. High brightness contrasts and arm-like structures are ubiquitous in the disk. A double-wing structure (partly due to angular differential imaging processing) resembles a morphology newly observed in inclined disks. Given the cavity size in the visible (11AU), the CO emission associated to the planet candidate c might arise from within the circumstellar disk. We find an extended emission in the K band at the expected location of b. The surrounding large-scale region is the brightest in scattered light. There is no sign of any disk gap associated to b.

Abstract Copyright: © ESO, 2016

Journal keyword(s): techniques: polarimetric - planet-disk interactions - circumstellar matter

Simbad objects: 8

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Number of rows : 8

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 HD 36112 Ae* 05 30 27.5286772598 +25 19 57.082162439   8.57 8.27     A8Ve 382 0
2 HD 100546c Pl? 11 33 25.4404858122 -70 11 41.239343121           ~ 13 0
3 HD 100546 Be* 11 33 25.4404858122 -70 11 41.239343121   6.71 6.30   6.64 A0VaekB8_lB 669 1
4 HD 100546b Pl 11 33 25.4404858122 -70 11 41.239343121           ~ 36 0
5 CPD-36 6759 Y*O 15 15 48.4459023859 -37 09 16.026315179   9.21 8.708     F8V 374 1
6 HD 142527 Ae* 15 56 41.8888096574 -42 19 23.245384377   9.04 8.34     F6III 503 1
7 V* AK Sco Ae* 16 54 44.8497760618 -36 53 18.560813962 9.80 9.63 9.00     F5V 244 1
8 HD 169142 Ae* 18 24 29.7799676975 -29 46 49.328597698   8.42 8.16     F1VekA3mA3_lB? 352 2

    Equat.    Gal    SGal    Ecl

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