X TrA through the eyes of MATISSE: More evidence of clumpy molecular layers around C-type asymptotic giant branch stars
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2025
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| author | Răstău, V. Paladini, C. Drevon, J. Hron, J. Kerschbaum, F. Wittkowski, M. Fonfria, J. P. Montargès, M. Khouri, T. Vlemmings, W. Olofsson, H. Ohnaka, K. Alonso-Hernandez, J. Contreras, C. Sánchez Velilla-Prieto, L. Danchi, W. C. Rau, G. Lykou, F. Sanchez-Bermudez, J. Lopez, B. Höfner, S. Aringer, B. Planquart, L. Cruzalèbes, P. Weigelt, G. |
| author_facet | Răstău, V. Paladini, C. Drevon, J. Hron, J. Kerschbaum, F. Wittkowski, M. Fonfria, J. P. Montargès, M. Khouri, T. Vlemmings, W. Olofsson, H. Ohnaka, K. Alonso-Hernandez, J. Contreras, C. Sánchez Velilla-Prieto, L. Danchi, W. C. Rau, G. Lykou, F. Sanchez-Bermudez, J. Lopez, B. Höfner, S. Aringer, B. Planquart, L. Cruzalèbes, P. Weigelt, G. |
| contents | Aims. The goal of this study is to further the understanding of the wind formation mechanism in asymptotic giant branch (AGB) stars through the analysis of the close environment (within a few stellar radii) of the carbon star X TrA.
Methods. X TrA was observed for the first time with the Mid-Infrared SpectroScopic Experiment instrument (MATISSE) in the L and N bands in low spectral resolution mode (R=30), and its close surroundings were mapped in specific wavelength ranges corresponding to specific molecules ($C_2H_2$ and HCN, at 3.1 and 3.8 $μ$m) and dust (amorphous carbon and, for example, Sic at 11.3 $μ$m), via image reconstruction techniques.
Results. The angular diameter of the star ranges from 10 mas in the L band pseudo-continuum (3.5 $μ$m) to 20 mas at 3.1 and 11.3 $μ$m. The reconstructed images show some mild elongated features (along the east-west direction) and asymmetric protrusions, which are most evident around 3.1 $μ$m. Imaging results highlight the clumpy nature of the circumstellar environment, starting from the photospheric region up to more distant layers.
Conclusions. The angular diameters found for X TrA in the image data are in agreement with previous photospheric diameter estimates (following VLTI/MIDI 8-13 $μ$m observations), and their wavelength dependence is similar to values found for other carbon stars observed with MATISSE (R Scl and V Hya). The 3.1 $μ$m images presented here show highly asymmetric features, another case of a C-rich star with irregular morphologies close to the stellar disk; this supports the notion that the $C_2H_2+HCN$ abundance distribution usually originates from a clumpy layer around carbon stars. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2512_03910 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | X TrA through the eyes of MATISSE: More evidence of clumpy molecular layers around C-type asymptotic giant branch stars Răstău, V. Paladini, C. Drevon, J. Hron, J. Kerschbaum, F. Wittkowski, M. Fonfria, J. P. Montargès, M. Khouri, T. Vlemmings, W. Olofsson, H. Ohnaka, K. Alonso-Hernandez, J. Contreras, C. Sánchez Velilla-Prieto, L. Danchi, W. C. Rau, G. Lykou, F. Sanchez-Bermudez, J. Lopez, B. Höfner, S. Aringer, B. Planquart, L. Cruzalèbes, P. Weigelt, G. Solar and Stellar Astrophysics Aims. The goal of this study is to further the understanding of the wind formation mechanism in asymptotic giant branch (AGB) stars through the analysis of the close environment (within a few stellar radii) of the carbon star X TrA. Methods. X TrA was observed for the first time with the Mid-Infrared SpectroScopic Experiment instrument (MATISSE) in the L and N bands in low spectral resolution mode (R=30), and its close surroundings were mapped in specific wavelength ranges corresponding to specific molecules ($C_2H_2$ and HCN, at 3.1 and 3.8 $μ$m) and dust (amorphous carbon and, for example, Sic at 11.3 $μ$m), via image reconstruction techniques. Results. The angular diameter of the star ranges from 10 mas in the L band pseudo-continuum (3.5 $μ$m) to 20 mas at 3.1 and 11.3 $μ$m. The reconstructed images show some mild elongated features (along the east-west direction) and asymmetric protrusions, which are most evident around 3.1 $μ$m. Imaging results highlight the clumpy nature of the circumstellar environment, starting from the photospheric region up to more distant layers. Conclusions. The angular diameters found for X TrA in the image data are in agreement with previous photospheric diameter estimates (following VLTI/MIDI 8-13 $μ$m observations), and their wavelength dependence is similar to values found for other carbon stars observed with MATISSE (R Scl and V Hya). The 3.1 $μ$m images presented here show highly asymmetric features, another case of a C-rich star with irregular morphologies close to the stellar disk; this supports the notion that the $C_2H_2+HCN$ abundance distribution usually originates from a clumpy layer around carbon stars. |
| title | X TrA through the eyes of MATISSE: More evidence of clumpy molecular layers around C-type asymptotic giant branch stars |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2512.03910 |