Locating dust and molecules in the inner circumstellar environment of R Sculptoris with MATISSE
J. Drevon
(1)
,
F. Millour
(1)
,
P. Cruzalèbes
(1)
,
C. Paladini
(2)
,
J. Hron
(3)
,
A. Meilland
(1)
,
F. Allouche
(1)
,
K.-H. Hofmann
(4)
,
S. Lagarde
(1)
,
B. Lopez
(1)
,
A. Matter
(1)
,
R. Petrov
(1)
,
S. Robbe-Dubois
(1)
,
D. Schertl
(4)
,
M. Wittkowski
(5)
,
G. Zins
(2)
,
P. Ábrahám
(6)
,
P. Antonelli
(1)
,
U. Beckmann
(4)
,
P. Berio
(1)
,
F. Bettonvil
(7)
,
A. Glindemann
(5)
,
U. Graser
(8)
,
M. Heininger
(4)
,
Thomas Henning
(8)
,
Jacob W. Isbell
(8)
,
Walter Jaffe
(9)
,
Lucas Labadie
(10)
,
Christoph Leinert
(8)
,
Michael Lehmitz
(8)
,
Sébastien Morel
(1)
,
Klaus Meisenheimer
(8)
,
Anthony Soulain
(11, 1, 12)
,
Josef Varga
(9)
,
Gerd Weigelt
(4)
,
Julien Woillez
(5)
,
Jean-Charles Augereau
(13)
,
Roy van Boekel
(8)
,
Leonard Burtscher
(9)
,
William Danchi
(14)
,
Carsten Dominik
(15)
,
Violetta Gamez-Rosas
(9)
,
Vincent Hocdé
(16)
,
M. Hogerheijde
(9, 15)
,
Lucia Klarmann
(8)
,
Elena Kokoulina
(1)
,
James Leftley
(1)
,
Ph. Stee
(1)
,
Farrokh Vakili
(1)
,
Rens Waters
(17, 7)
,
Sebastian Wolf
(18)
,
Gideon Yoffe
(8)
1
LAGRANGE -
Joseph Louis LAGRANGE
2 ESO - European Southern Observatory [Santiago]
3 University of Vienna [Vienna]
4 MPIFR - Max-Planck-Institut für Radioastronomie
5 ESO - European Southern Observatory
6 Konkoly Observatory
7 SRON - SRON Netherlands Institute for Space Research
8 MPIA - Max Planck Institute for Astronomy
9 Leiden Observatory [Leiden]
10 I. Physikalisches Institut [Köln]
11 UGA - Université Grenoble Alpes
12 School of Physics [Sydney]
13 IPAG - Institut de Planétologie et d'Astrophysique de Grenoble
14 GSFC - NASA Goddard Space Flight Center
15 AI PANNEKOEK - Astronomical Institute Anton Pannekoek
16 Nicolaus Copernicus University [Toruń]
17 Radboud - Astronomy Department, Radboud University Nijmegen
18 CAU - Christian-Albrechts-Universität zu Kiel = Christian-Albrechts University of Kiel = Université Christian-Albrechts de Kiel
2 ESO - European Southern Observatory [Santiago]
3 University of Vienna [Vienna]
4 MPIFR - Max-Planck-Institut für Radioastronomie
5 ESO - European Southern Observatory
6 Konkoly Observatory
7 SRON - SRON Netherlands Institute for Space Research
8 MPIA - Max Planck Institute for Astronomy
9 Leiden Observatory [Leiden]
10 I. Physikalisches Institut [Köln]
11 UGA - Université Grenoble Alpes
12 School of Physics [Sydney]
13 IPAG - Institut de Planétologie et d'Astrophysique de Grenoble
14 GSFC - NASA Goddard Space Flight Center
15 AI PANNEKOEK - Astronomical Institute Anton Pannekoek
16 Nicolaus Copernicus University [Toruń]
17 Radboud - Astronomy Department, Radboud University Nijmegen
18 CAU - Christian-Albrechts-Universität zu Kiel = Christian-Albrechts University of Kiel = Université Christian-Albrechts de Kiel
Jean-Charles Augereau
- Fonction : Auteur
- PersonId : 761402
- ORCID : 0000-0002-2725-6415
- IdRef : 175126216
Carsten Dominik
- Fonction : Auteur
- PersonId : 755731
- ORCID : 0000-0002-3393-2459
M. Hogerheijde
- Fonction : Auteur
- PersonId : 762821
- ORCID : 0000-0001-5217-537X
Ph. Stee
- Fonction : Auteur
- PersonId : 744913
- IdHAL : philippe-stee
- ORCID : 0000-0001-8220-0636
- IdRef : 061743798
Sebastian Wolf
- Fonction : Auteur
- PersonId : 1142983
- ORCID : 0000-0003-0832-6315
Résumé
Context. Asymptotic giant branch (AGB) stars are one of the main sources of dust production in the Galaxy. However, it is not yet clear what this process looks like and where the dust happens to be condensing in the circumstellar environment.
Aims. By characterizing the location of the dust and the molecules in the close environment of an AGB star, we aim to achieve a better understanding the history of the dust formation process.
Methods. We observed the carbon star R Scl with the thermal-infrared VLTI/MATISSE instrument in L- and N-bands. The high angular resolution of the VLTI observations (as small as 4.4 mas in the L-band and 15 mas in the N-band with ATs), combined with a large uv-plane coverage allowed us to use image reconstruction methods. To constrain the dust and molecules’ location, we used two different methods: one using MIRA image reconstruction algorithm and the second using the 1D code RHAPSODY.
Results. We found evidence of C2H2 and HCN molecules between 1 and 3.4 R⋆ which is much closer to the star than the location of the dust (between 3.8 and 17.0 R⋆). We also estimated a mass-loss rate of 1.2 ± 0.4 × 10−6 M⊙ yr−1. In the meantime, we confirmed the previously published characteristics of a thin dust shell, composed of amorphous carbon (amC) and silicon carbide (SiC). However,
no clear SiC feature has been detected in the MATISSE visibilities. This might be caused by molecular absorption that can affect the shape of the SiC band at 11.3 μm.
Conclusions. The appearance of the molecular shells is in good agreement with predictions from dynamical atmosphere models. For the first time, we co-located dust and molecules in the environment of an AGB star. We confirm that the molecules are located closer to the star than the dust. The MIRA images unveil the presence of a clumpy environment in the fuzzy emission region beyond 4.0 R⋆.
Furthermore, with the available dynamic range and angular resolution, we did not detect the presence of a binary companion. To solve this problem, additional observations combining MATISSE and SAM-VISIR instrument should enable this detection in future studies.
Origine : Fichiers produits par l'(les) auteur(s)