Volume 613, May 2018
|Number of page(s)||5|
|Section||Letters to the Editor|
|Published online||23 May 2018|
Letter to the Editor
Searching for Hα emitting sources around MWC 758
Centro de Astrobiología (CSIC-INTA),
Camino bajo del Castillo s/n,
Villanueva de la Cañada, Madrid, Spain
2 Unidad Mixta Internacional Franco-Chilena de Astronomía, CNRS/INSU UMI 3386 and Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
3 Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
4 ETH Zurich, Institute of Particle Physics and Astrophysics, Wolfgang-Pauli-Strasse 27, 8093 Zurich, Switzerland
5 Maynooth University Department of Experimental Physics, National University of Ireland, Maynooth Co. Kildare, Ireland
6 European Southern Observatory, Alonso de Cordova 3107, Casilla 19, Vitacura, Santiago, Chile
7 INAF-Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy
8 Joint ALMA Observatory, Alonso de Córdova 3107, Vitacura, Santiago, Chile
9 Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, allée Geoffroy Saint-Hilaire, 33615 Pessac, France
10 ESAC Science Data Centre, ESA-ESAC, Madrid, Spain
11 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
12 Universidad Autónoma de Madrid, Dpto. Física Teórica, Madrid, Spain
13 Laboratoire AIM, CEA/DRF, CNRS, Université Paris Diderot, IRFU/DAS, 91191 Gif-sur-Yvette, France
Accepted: 22 March 2018
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 ~111 mas 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 ~7.6 mag at 111 mas, the separation of the previously detected planet candidate. This contrast translates into a Hα line luminosity of LHα ≲ 5×10−5 L⊙ at 111 mas. 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 < 3.7 × 10−4 L⊙ for the protoplanet candidate. For the predicted mass range of MWC 758b, 0.5–5 MJup, this implies accretion rates smaller than Ṁ < 3.4 × (10−8−10−9)M⊙ yr−1, for an average planet radius of 1.1 RJup. 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 ≲3.2 RJup.
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.
Key words: stars: pre-main sequence / planetary systems / stars: individual: MWC758 / accretion, accretion disks / techniques: high angular resolution
The reduced images are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/613/L5
© ESO 2018
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