2018A&A...613L...5H


Query : 2018A&A...613L...5H

2018A&A...613L...5H - Astronomy and Astrophysics, volume 613, L5-5 (2018/5-1)

Searching for Hα emitting sources around MWC 758. SPHERE/ZIMPOL high-contrast imaging.

HUELAMO N., CHAUVIN G., SCHMID H.M., QUANZ S.P., WHELAN E., LILLO-BOX J., BARRADO D., MONTESINOS B., ALCALA J.M., BENISTY M., DE GREGORIO-MONSALVO I., MENDIGUTIA I., BOUY H., MERIN B., DE BOER J., GARUFI A. and PANTIN E.

Abstract (from CDS):

Context. MWC 758 is a young star surrounded by a transitional disk. The disk shows an inner cavity and spiral arms that could be caused by the presence of protoplanets. Recently, a protoplanet candidate has been detected around MWC 758 through high-resolution L'-band observations. The candidate is located inside the disk cavity at a separation of ∼111mas from the central star, and at an average position angle of ∼165.5°. Aims. We aim at detecting accreting protoplanet candidates within the disk of MWC 758 through angular spectral differential imaging (ASDI) observations in the optical regime. In particular, we explore the emission at the position of the detected planet candidate. Methods. We have performed simultaneous adaptive optics observations in the Hα line and the adjacent continuum using SPHERE/ZIMPOL at the Very Large Telescope (VLT). Results. The data analysis does not reveal any Hα signal around the target. The derived contrast curve in the B_Ha filter allows us to derive a 5σ upper limit of ∼7.6mag at 111mas, the separation of the previously detected planet candidate. This contrast translates into a Hα line luminosity of L≤5x10–5L at 111mas. Assuming that LHα scales with Lacc as in classical T Tauri stars (CTTSs) as a first approximation, we can estimate an accretion luminosity of Lacc<3.7x10–4L for the protoplanet candidate. For the predictedmass range of MWC 758b, 0.5-5MJup, this implies accretion rates smaller than M<3.4x(10–8-10–9)M/yr, for an average planet radius of 1.1RJup. Therefore, our estimates are consistent with the predictions of accreting circumplanetary accretion models for Rin=1RJup. The ZIMPOL line luminosity is consistent with the Hα upper limit predicted by these models for truncation radii ≤3.2RJup. Conclusions. The non-detection of any Hα emitting source in the ZIMPOL images does not allow us to unveil the nature of the L' detected source. Either it is a protoplanet candidate or a disk asymmetry.

Abstract Copyright: © ESO 2018

Journal keyword(s): stars: pre-main sequence - planetary systems - stars: individual: MWC758 - accretion, accretion disks - techniques: high angular resolution

VizieR on-line data: <Available at CDS (J/A+A/613/L5): list.dat fits/*>

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 - 2022
#notes
1 HD 19445 PM* 03 08 25.5883873084 +26 19 51.400965175 8.29 8.52 8.06 7.60 7.27 G2VFe-3 752 0
2 V* FW Tau Or* 04 29 29.7076208400 +26 16 52.768899480       15.85   M5.5 127 0
3 V* DH Tau B LM* 04 29 41.66 +26 32 56.5           M9.25 67 1
4 EM* LkCa 15b Pl 04 39 17.7912813350 +22 21 03.387667491           ~ 71 1
5 HD 36112 Ae* 05 30 27.5285630040 +25 19 57.076288752   8.57 8.27     A8Ve 416 0
6 2MASS J15491331-3539118 LM* 15 49 13.3077704592 -35 39 11.761171488           M4 104 0
7 HD 142527b Pl? 15 56 41.8888096574 -42 19 23.245384377           ~ 21 0
8 NAME GSC 06214-00210B LM* 16 21 54.678 -20 43 11.33           ~ 68 0

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2022.05.28-22:25:49

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