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18 results on '"Bettonvil, F."'

1. Locating dust and molecules in the inner circumstellar environment of R~Sculptoris with MATISSE

Author

Drevon, Julien, Millour, Florentin, Cruzalèbes, Pierre, Paladini, Claudia, Hron, Josef, Meilland, A., Allouche, F., Hofmann, K. -H., Lagarde, S., Lopez, B., Matter, A., Petrov, R., Robbe-Dubois, S., Schertl, D., Wittkowski, M., Zins, G., Ábrahám, P., Antonelli, P., Beckmann, U., Berio, P., Bettonvil, F., Glindemann, A., Graser, U., Heininger, M., Henning, Thomas, Isbell, Jacob W., Jaffe, Walter, Labadie, Lucas, Leinert, Christoph, Lehmitz, Michael, Morel, Sébastien, Meisenheimer, Klaus, Soulain, Anthony, Varga, Josef, Weigelt, Gerd, Woillez, Julien, Augereau, Jean-Charles, van Boekel, Roy, Burtscher, Leonard, Danchi, William, Dominik, Carsten, Gamez-Rosas, Violetta, Hocdé, Vincent, Hogerheijde, M., Klarmann, Lucia, Kokoulina, Elena, Leftley, James, Stee, Ph., Vakili, Farrokh, Waters, Rens, Wolf, Sebastian, and Yoffe, Gideon

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

AGB stars are one of the main sources of dust production in the Galaxy. However, it is not clear what this process looks like and where the dust is condensing in the circumstellar environment. 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. We observed the carbon star R Scl with the VLTI-MATISSE instrument in L- and N-bands. The high angular resolution of the VLTI observations, 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: MIRA image reconstruction and the 1D code RHAPSODY. We found evidence of C2H2 and HCN molecules between 1 and 3.4 Rstar which is much closer to the star than the location of the dust (between 3.8 and 17.0 Rstar). We also estimated a mass-loss rate of 1.2+-0.4x10-6 Msun per yr. 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 micron. 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 Rstar. Furthermore, with the available dynamic range and angular resolution, we did not detect the presence of a binary companion. Additional observations combining MATISSE and SAM-VISIR instrument should enable this detection in future studies., Comment: 19 pages, published in A&A

Published
2022
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2. The extended atmosphere and circumstellar environment of the cool evolved star VX Sagittarii as seen by MATISSE

Author

Chiavassa, A., Kravchenko, K., Montargès, M., Millour, F., Matter, A., Freytag, B., Wittkowski, M., Hocdé, V., Cruzalèbes, P., Allouche, F., Lopez, B., Lagarde, S., Petrov, R. G., Meilland, A., Robbe-Dubois, S., Hofmann, K. -H., Weigelt, G., Berio, P., Bendjoya, P., Bettonvil, F., de Souza, A. Domiciano, Heininger, M., Henning, Th., Isbell, J. W., Jaffe, W., Labadie, L., Lehmitz, M., Meisenheimer, K., Soulain, A., Varga, J., Augereau, J. -C., van Boekel, R., Burtscher, L., Danchi, W. C., Dominik, C., Drevon, J., Rosas, V. Gámez, Hogerheijde, M. R., Hron, J., Klarmann, L., Kokoulina, E., Lagadec, E., Leftley, J., Mosoni, L., Nardetto1, N., Paladini, C., Pantin, E., Schertl, D., Stee, P., Szabados, L., Waters, R., Wolf, S., and Yoffe, G.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Context. VX Sgr is a cool, evolved, and luminous red star whose stellar parameters are difficult to determine, which affects its classification. Aims. We aim to spatially resolve the photospheric extent as well as the circumstellar environment. Methods. We used interferometric observations obtained with the MATISSE instrument in the L (3 to 4 {\mu}m), M (4.5 to 5 {\mu}m), and N (8 to 13 {\mu}m) bands. We reconstructed monochromatic images using the MIRA software. We used 3D radiation-hydrodynamics (RHD) simulations carried out with CO5BOLD and a uniform disc model to estimate the apparent diameter and interpret the stellar surface structures. Moreover, we employed the radiative transfer codes Optim3D and Radmc3D to compute the spectral energy distribution for the L, M, and N bands, respectively. Results. MATISSE observations unveil, for the first time, the morphology of VX Sgr across the L, M, and N bands. The reconstructed images show a complex morphology with brighter areas whose characteristics depend on the wavelength probed. We measured the angular diameter as a function of the wavelength and showed that the photospheric extent in the L and M bands depends on the opacity through the atmosphere. In addition to this, we also concluded that the observed photospheric inhomogeneities can be interpreted as convection-related surface structures. The comparison in the N band yielded a qualitative agreement between the N band spectrum and simple dust radiative transfer simulations. However, it is not possible to firmly conclude on the interpretation of the current data because of the difficulty in constraing the model parameters using the limited accuracy of our absolute flux calibration. Conclusions. MATISSE observations and the derived reconstructed images unveil the appearance of the stellar surface and circumstellar environment across a very large spectral domain for the first time., Comment: Accepted for publication on Astronomy and Astrophysics

Published
2021
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3. VLTI-MATISSE L- and N-band aperture-synthesis imaging of the unclassified B[e] star FS Canis Majoris

Author

Hofmann, K. -H., Bensberg, A., Schertl, D., Weigelt, G., Wolf, S., Meilland, A., Millour, F., Waters, L. B. F. M., Kraus, S., Ohnaka, K., Lopez, B., Petrov, R. G., Lagarde, S., Berio, Ph., Allouche, F., Robbe-Dubois, S., Jaffe, W., Henning, Th., Paladini, C., Schöller, M., Mérand, A., Glindemann, A., Beckmann, U., Heininger, M., Bettonvil, F., Zins, G., Woillez, J., Bristow, P., Stee, P., Vakili, F., van Boekel, R., Hogerheijde, M. R., Dominik, C., Augereau, J. -C., Matter, A., Hron, J., Pantin, E., Rivinius, Th., de Wit, W. -J., Varga, J., Klarmann, L., Meisenheimer, K., Rosas, V. Gámez, Burtscher, L., Leftley, J., Isbell, J. W., Yoffe, G., Kokoulina, E., Danchi, W. C., Cruzalèbes, P., de Souza, A. Domiciano, Drevon, J., Hocdé, V., Kreplin, A., Labadie, L., Connot, C., Nußbaum, E., Lehmitz, M., Antonelli, P., Graser, U., and Leinert, C.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Context: FS Canis Majoris (FS CMa, HD 45677) is an unclassified B[e] star surrounded by an inclined dust disk. The evolutionary stage of FS CMa is still debated. Perpendicular to the circumstellar disk, a bipolar outflow was detected. Infrared aperture-synthesis imaging provides us with a unique opportunity to study the disk structure. Aims: Our aim is to study the intensity distribution of the disk of FS CMa in the mid-infrared L and N bands. Methods: We performed aperture-synthesis imaging of FS CMa with the MATISSE instrument (Multi AperTure mid-Infrared SpectroScopic Experiment) in the low spectral resolution mode to obtain images in the L and N bands. We computed radiative transfer models that reproduce the L- and N-band intensity distributions of the resolved disks. Results: We present L- and N-band aperture-synthesis images of FS CMa reconstructed in the wavelength bands of 3.4-3.8 and 8.6-9.0 micrometer. In the L-band image, the inner rim region of an inclined circumstellar disk and the central object can be seen with a spatial resolution of 2.7 milliarcsec (mas). An inner disk cavity with an angular diameter of 6x12mas is resolved. The L-band disk consists of a bright northwestern (NW) disk region and a much fainter southeastern (SE) region. The images suggest that we are looking at the bright inner wall of the NW disk rim, which is on the far side of the disk. In the N band, only the bright NW disk region is seen. In addition to deriving the inclination and the inner disk radius, fitting the reconstructed brightness distributions via radiative transfer modeling allows one to constrain the innermost disk structure, in particular the shape of the inner disk rim., Comment: accepted for publication in A&A

Published
2021
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4. The European Solar Telescope

Author

Quintero Noda, C., primary, Schlichenmaier, R., additional, Bellot Rubio, L. R., additional, Löfdahl, M. G., additional, Khomenko, E., additional, Jurčák, J., additional, Leenaarts, J., additional, Kuckein, C., additional, González Manrique, S. J., additional, Gunár, S., additional, Nelson, C. J., additional, de la Cruz Rodríguez, J., additional, Tziotziou, K., additional, Tsiropoula, G., additional, Aulanier, G., additional, Aboudarham, J., additional, Allegri, D., additional, Alsina Ballester, E., additional, Amans, J. P., additional, Asensio Ramos, A., additional, Bailén, F. J., additional, Balaguer, M., additional, Baldini, V., additional, Balthasar, H., additional, Barata, T., additional, Barczynski, K., additional, Barreto Cabrera, M., additional, Baur, A., additional, Béchet, C., additional, Beck, C., additional, Belío-Asín, M., additional, Bello-González, N., additional, Belluzzi, L., additional, Bentley, R. D., additional, Berdyugina, S. V., additional, Berghmans, D., additional, Berlicki, A., additional, Berrilli, F., additional, Berkefeld, T., additional, Bettonvil, F., additional, Bianda, M., additional, Bienes Pérez, J., additional, Bonaque-González, S., additional, Brajša, R., additional, Bommier, V., additional, Bourdin, P.-A., additional, Burgos Martín, J., additional, Calchetti, D., additional, Calcines, A., additional, Calvo Tovar, J., additional, Campbell, R. J., additional, Carballo-Martín, Y., additional, Carbone, V., additional, Carlin, E. S., additional, Carlsson, M., additional, Castro López, J., additional, Cavaller, L., additional, Cavallini, F., additional, Cauzzi, G., additional, Cecconi, M., additional, Chulani, H. M., additional, Cirami, R., additional, Consolini, G., additional, Coretti, I., additional, Cosentino, R., additional, Cózar-Castellano, J., additional, Dalmasse, K., additional, Danilovic, S., additional, De Juan Ovelar, M., additional, Del Moro, D., additional, del Pino Alemán, T., additional, del Toro Iniesta, J. C., additional, Denker, C., additional, Dhara, S. K., additional, Di Marcantonio, P., additional, Díaz Baso, C. J., additional, Diercke, A., additional, Dineva, E., additional, Díaz-García, J. J., additional, Doerr, H.-P., additional, Doyle, G., additional, Erdelyi, R., additional, Ermolli, I., additional, Escobar Rodríguez, A., additional, Esteban Pozuelo, S., additional, Faurobert, M., additional, Felipe, T., additional, Feller, A., additional, Feijoo Amoedo, N., additional, Femenía Castellá, B., additional, Fernandes, J., additional, Ferro Rodríguez, I., additional, Figueroa, I., additional, Fletcher, L., additional, Franco Ordovas, A., additional, Gafeira, R., additional, Gardenghi, R., additional, Gelly, B., additional, Giorgi, F., additional, Gisler, D., additional, Giovannelli, L., additional, González, F., additional, González, J. B., additional, González-Cava, J. M., additional, González García, M., additional, Gömöry, P., additional, Gracia, F., additional, Grauf, B., additional, Greco, V., additional, Grivel, C., additional, Guerreiro, N., additional, Guglielmino, S. L., additional, Hammerschlag, R., additional, Hanslmeier, A., additional, Hansteen, V., additional, Heinzel, P., additional, Hernández-Delgado, A., additional, Hernández Suárez, E., additional, Hidalgo, S. L., additional, Hill, F., additional, Hizberger, J., additional, Hofmeister, S., additional, Jägers, A., additional, Janett, G., additional, Jarolim, R., additional, Jess, D., additional, Jiménez Mejías, D., additional, Jolissaint, L., additional, Kamlah, R., additional, Kapitán, J., additional, Kašparová, J., additional, Keller, C. U., additional, Kentischer, T., additional, Kiselman, D., additional, Kleint, L., additional, Klvana, M., additional, Kontogiannis, I., additional, Krishnappa, N., additional, Kučera, A., additional, Labrosse, N., additional, Lagg, A., additional, Landi Degl’Innocenti, E., additional, Langlois, M., additional, Lafon, M., additional, Laforgue, D., additional, Le Men, C., additional, Lepori, B., additional, Lepreti, F., additional, Lindberg, B., additional, Lilje, P. B., additional, López Ariste, A., additional, López Fernández, V. A., additional, López Jiménez, A. C., additional, López López, R., additional, Manso Sainz, R., additional, Marassi, A., additional, Marco de la Rosa, J., additional, Marino, J., additional, Marrero, J., additional, Martín, A., additional, Martín Gálvez, A., additional, Martín Hernando, Y., additional, Masciadri, E., additional, Martínez González, M., additional, Matta-Gómez, A., additional, Mato, A., additional, Mathioudakis, M., additional, Matthews, S., additional, Mein, P., additional, Merlos García, F., additional, Moity, J., additional, Montilla, I., additional, Molinaro, M., additional, Molodij, G., additional, Montoya, L. M., additional, Munari, M., additional, Murabito, M., additional, Núñez Cagigal, M., additional, Oliviero, M., additional, Orozco Suárez, D., additional, Ortiz, A., additional, Padilla-Hernández, C., additional, Paéz Mañá, E., additional, Paletou, F., additional, Pancorbo, J., additional, Pastor Cañedo, A., additional, Pastor Yabar, A., additional, Peat, A. W., additional, Pedichini, F., additional, Peixinho, N., additional, Peñate, J., additional, Pérez de Taoro, A., additional, Peter, H., additional, Petrovay, K., additional, Piazzesi, R., additional, Pietropaolo, E., additional, Pleier, O., additional, Poedts, S., additional, Pötzi, W., additional, Podladchikova, T., additional, Prieto, G., additional, Quintero Nehrkorn, J., additional, Ramelli, R., additional, Ramos Sapena, Y., additional, Rasilla, J. L., additional, Reardon, K., additional, Rebolo, R., additional, Regalado Olivares, S., additional, Reyes García-Talavera, M., additional, Riethmüller, T. L., additional, Rimmele, T., additional, Rodríguez Delgado, H., additional, Rodríguez González, N., additional, Rodríguez-Losada, J. A., additional, Rodríguez Ramos, L. F., additional, Romano, P., additional, Roth, M., additional, Rouppe van der Voort, L., additional, Rudawy, P., additional, Ruiz de Galarreta, C., additional, Rybák, J., additional, Salvade, A., additional, Sánchez-Capuchino, J., additional, Sánchez Rodríguez, M. L., additional, Sangiorgi, M., additional, Sayède, F., additional, Scharmer, G., additional, Scheiffelen, T., additional, Schmidt, W., additional, Schmieder, B., additional, Scirè, C., additional, Scuderi, S., additional, Siegel, B., additional, Sigwarth, M., additional, Simões, P. J. A., additional, Snik, F., additional, Sliepen, G., additional, Sobotka, M., additional, Socas-Navarro, H., additional, Sola La Serna, P., additional, Solanki, S. K., additional, Soler Trujillo, M., additional, Soltau, D., additional, Sordini, A., additional, Sosa Méndez, A., additional, Stangalini, M., additional, Steiner, O., additional, Stenflo, J. O., additional, Štěpán, J., additional, Strassmeier, K. G., additional, Sudar, D., additional, Suematsu, Y., additional, Sütterlin, P., additional, Tallon, M., additional, Temmer, M., additional, Tenegi, F., additional, Tritschler, A., additional, Trujillo Bueno, J., additional, Turchi, A., additional, Utz, D., additional, van Harten, G., additional, van Noort, M., additional, van Werkhoven, T., additional, Vansintjan, R., additional, Vaz Cedillo, J. J., additional, Vega Reyes, N., additional, Verma, M., additional, Veronig, A. M., additional, Viavattene, G., additional, Vitas, N., additional, Vögler, A., additional, von der Lühe, O., additional, Volkmer, R., additional, Waldmann, T. A., additional, Walton, D., additional, Wisniewska, A., additional, Zeman, J., additional, Zeuner, F., additional, Zhang, L. Q., additional, Zuccarello, F., additional, and Collados, M., additional

Published
2022
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5. Locating dust and molecules in the inner circumstellar environment of R Sculptoris with MATISSE

Author

Drevon, J., primary, Millour, F., additional, Cruzalèbes, P., additional, Paladini, C., additional, Hron, J., additional, Meilland, A., additional, Allouche, F., additional, Hofmann, K.-H., additional, Lagarde, S., additional, Lopez, B., additional, Matter, A., additional, Petrov, R., additional, Robbe-Dubois, S., additional, Schertl, D., additional, Scicluna, P., additional, Wittkowski, M., additional, Zins, G., additional, Ábrahám, P., additional, Antonelli, P., additional, Beckmann, U., additional, Berio, P., additional, Bettonvil, F., additional, Glindemann, A., additional, Graser, U., additional, Heininger, M., additional, Henning, Th., additional, Isbell, J. W., additional, Jaffe, W., additional, Labadie, L., additional, Leinert, C., additional, Lehmitz, M., additional, Morel, S., additional, Meisenheimer, K., additional, Soulain, A., additional, Varga, J., additional, Weigelt, G., additional, Woillez, J., additional, Augereau, J.-C., additional, van Boekel, R., additional, Burtscher, L., additional, Danchi, W. C., additional, Dominik, C., additional, Gámez Rosas, V., additional, Hocdé, V., additional, Hogerheijde, M. R., additional, Klarmann, L., additional, Kokoulina, E., additional, Leftley, J., additional, Stee, P., additional, Vakili, F., additional, Waters, R., additional, Wolf, S., additional, and Yoffe, G., additional

Published
2022
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6. The dusty heart of Circinus

Author

Isbell, J. W., primary, Meisenheimer, K., additional, Pott, J.-U., additional, Stalevski, M., additional, Tristram, K. R. W., additional, Sanchez-Bermudez, J., additional, Hofmann, K.-H., additional, Gámez Rosas, V., additional, Jaffe, W., additional, Burtscher, L., additional, Leftley, J., additional, Petrov, R., additional, Lopez, B., additional, Henning, T., additional, Weigelt, G., additional, Allouche, F., additional, Berio, P., additional, Bettonvil, F., additional, Cruzalebes, P., additional, Dominik, C., additional, Heininger, M., additional, Hogerheijde, M., additional, Lagarde, S., additional, Lehmitz, M., additional, Matter, A., additional, Meilland, A., additional, Millour, F., additional, Robbe-Dubois, S., additional, Schertl, D., additional, van Boekel, R., additional, Varga, J., additional, and Woillez, J., additional

Published
2022
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7. The extended atmosphere and circumstellar environment of the cool evolved star VX Sagittarii as seen by MATISSE★

Author

Chiavassa, A., Kravchenko, K., Montargès, M., Millour, F., Matter, A., Freytag, B., Wittkowski, M., Hocdé, V., Cruzalèbes, P., Allouche, F., Lopez, B., Lagarde, S., Petrov, R.G., Meilland, A., Robbe-Dubois, S., Hofmann, K-H, Weigelt, G., Berio, P., Bendjoya, P., Bettonvil, F., Domiciano de Souza, A., Heininger, M., Henning, T., Isbell, J.W., Jaffe, W., Labadie, L., Lehmitz, M., Meisenheimer, K., Soulain, A., Varga, J., Augereau, J.-C., Boekel, R. van, Burtscher, L., Danchi, W.C., Dominik, C., Drevon, J., Gamez Rosas, V., Hogerheijde, M.R., Hron, J., Klarmann, L., Kokoulina, E., Lagadec, E., Leftley, J., Mosoni, L., Nardetto, N., Paladini, C., Pantin, E., Schertl, D., Stee, P., Szabados, L., Waters, R., Wolf, S., Yoffe, G., Chiavassa, A., Kravchenko, K., Montargès, M., Millour, F., Matter, A., Freytag, B., Wittkowski, M., Hocdé, V., Cruzalèbes, P., Allouche, F., Lopez, B., Lagarde, S., Petrov, R.G., Meilland, A., Robbe-Dubois, S., Hofmann, K-H, Weigelt, G., Berio, P., Bendjoya, P., Bettonvil, F., Domiciano de Souza, A., Heininger, M., Henning, T., Isbell, J.W., Jaffe, W., Labadie, L., Lehmitz, M., Meisenheimer, K., Soulain, A., Varga, J., Augereau, J.-C., Boekel, R. van, Burtscher, L., Danchi, W.C., Dominik, C., Drevon, J., Gamez Rosas, V., Hogerheijde, M.R., Hron, J., Klarmann, L., Kokoulina, E., Lagadec, E., Leftley, J., Mosoni, L., Nardetto, N., Paladini, C., Pantin, E., Schertl, D., Stee, P., Szabados, L., Waters, R., Wolf, S., and Yoffe, G.

Abstract

Contains fulltext : 247415.pdf (Publisher’s version ) (Open Access)

Published
2022

8. The extended atmosphere and circumstellar environment of the cool evolved star VX Sagittarii as seen by MATISSE star

Author

Chiavassa, A., Kravchenko, K., Montarges, M., Millour, F., Matter, A., Freytag, Bernd, Wittkowski, M., Hocde, V, Cruzalebes, P., Allouche, F., Lopez, B., Lagarde, S., Petrov, R. G., Meilland, A., Robbe-Dubois, S., Hofmann, K-H, Weigelt, G., Berio, P., Bendjoya, P., Bettonvil, F., de Souza, A. Domiciano, Heininger, M., Henning, Th, Isbell, J. W., Jaffe, W., Labadie, L., Lehmitz, M., Meisenheimer, K., Soulain, A., Varga, J., Augereau, J-C, van Boekel, R., Burtscher, L., Danchi, W. C., Dominik, C., Drevon, J., Rosas, V. Gamez, Hogerheijde, M. R., Hron, J., Klarmann, L., Kokoulina, E., Lagadec, E., Leftley, J., Mosoni, L., Nardetto, N., Paladini, C., Pantin, E., Schertl, D., Stee, P., Szabados, L., Waters, R., Wolf, S., Yoffe, G., Chiavassa, A., Kravchenko, K., Montarges, M., Millour, F., Matter, A., Freytag, Bernd, Wittkowski, M., Hocde, V, Cruzalebes, P., Allouche, F., Lopez, B., Lagarde, S., Petrov, R. G., Meilland, A., Robbe-Dubois, S., Hofmann, K-H, Weigelt, G., Berio, P., Bendjoya, P., Bettonvil, F., de Souza, A. Domiciano, Heininger, M., Henning, Th, Isbell, J. W., Jaffe, W., Labadie, L., Lehmitz, M., Meisenheimer, K., Soulain, A., Varga, J., Augereau, J-C, van Boekel, R., Burtscher, L., Danchi, W. C., Dominik, C., Drevon, J., Rosas, V. Gamez, Hogerheijde, M. R., Hron, J., Klarmann, L., Kokoulina, E., Lagadec, E., Leftley, J., Mosoni, L., Nardetto, N., Paladini, C., Pantin, E., Schertl, D., Stee, P., Szabados, L., Waters, R., Wolf, S., and Yoffe, G.

Abstract

Context. VX Sgr is a cool, evolved, and luminous red star whose stellar parameters are difficult to determine, which affects its classification. Aims. We aim to spatially resolve the photospheric extent as well as the circumstellar environment. Methods. We used interferometric observations obtained with the MATISSE instrument in the L (3-4 mu m), M (4.5-5 mu m), and N (8-13 mu m) bands. We reconstructed monochromatic images using the MIRA software. We used 3D radiation-hydrodynamics simulations carried out with (COBOLD)-B-5 and a uniform disc model to estimate the apparent diameter and interpret the stellar surface structures. Moreover, we employed the radiative transfer codes OPTIM3D and RADMC3D to compute the spectral energy distribution for the L, M, and N bands, respectively. Results. MATISSE observations unveil, for the first time, the morphology of VX Sgr across the L, M, and N bands. The reconstructed images show a complex morphology with brighter areas whose characteristics depend on the wavelength probed. We measured the angular diameter as a function of the wavelength and showed that the photospheric extent in the L and M bands depends on the opacity through the atmosphere. In addition to this, we also concluded that the observed photospheric inhomogeneities can be interpreted as convection-related surface structures. The comparison in the N band yielded a qualitative agreement between the N-band spectrum and simple dust radiative transfer simulations. However, it is not possible to firmly conclude on the interpretation of the current data because of the difficulty in constraing the model parameters using the limited accuracy of our absolute flux calibration. Conclusions. MATISSE observations and the derived reconstructed images unveil the appearance of VX Sgr's stellar surface and circumstellar environment across a very large spectral domain for the first time.

Published
2022
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9. VLTI-MATISSE L- and N-band aperture-synthesis imaging of the unclassified B[e] star FS Canis Majoris

Author

Hofmann, K-H, Bensberg, A., Schertl, D., Weigelt, G., Wolf, S., Meilland, A., Millour, F., Waters, L. B. F. M., Kraus, S., Ohnaka, K., Lopez, B., Petrov, R. G., Lagarde, S., Berio, Ph, Allouche, F., Robbe-Dubois, S., Jaffe, W., Henning, Th, Paladini, C., Schoeller, M., Merand, A., Glindemann, A., Beckmann, U., Heininger, M., Bettonvil, F., Zins, G., Woillez, J., Bristow, P., Stee, P., Vakili, F., van Boekel, R., Hogerheijde, M. R., Dominik, C., Augereau, J-C, Matter, A., Hron, J., Pantin, E., Rivinius, Th, De Wit, W-J, Varga, J., Klarmann, L., Meisenheimer, K., Rosas, V. Gamez, Burtscher, L., Leftley, J., Isbell, J. W., Yoffe, G., Kokoulina, E., Danchi, W. C., Cruzalebes, P., Domiciano de Souza, A., Drevon, J., Hocde, V, Kreplin, A., Labadie, L., Connot, C., Nussbaum, E., Lehmitz, M., Antonelli, P., Graser, U., Leinert, C., Hofmann, K-H, Bensberg, A., Schertl, D., Weigelt, G., Wolf, S., Meilland, A., Millour, F., Waters, L. B. F. M., Kraus, S., Ohnaka, K., Lopez, B., Petrov, R. G., Lagarde, S., Berio, Ph, Allouche, F., Robbe-Dubois, S., Jaffe, W., Henning, Th, Paladini, C., Schoeller, M., Merand, A., Glindemann, A., Beckmann, U., Heininger, M., Bettonvil, F., Zins, G., Woillez, J., Bristow, P., Stee, P., Vakili, F., van Boekel, R., Hogerheijde, M. R., Dominik, C., Augereau, J-C, Matter, A., Hron, J., Pantin, E., Rivinius, Th, De Wit, W-J, Varga, J., Klarmann, L., Meisenheimer, K., Rosas, V. Gamez, Burtscher, L., Leftley, J., Isbell, J. W., Yoffe, G., Kokoulina, E., Danchi, W. C., Cruzalebes, P., Domiciano de Souza, A., Drevon, J., Hocde, V, Kreplin, A., Labadie, L., Connot, C., Nussbaum, E., Lehmitz, M., Antonelli, P., Graser, U., and Leinert, C.

Abstract

Context. FS Canis Majoris (FS CMa, HD 45677) is an unclassified B[e] star surrounded by an inclined dust disk. The evolutionary stage of FS CMa is still debated. Perpendicular to the circumstellar disk, a bipolar outflow was detected. Infrared aperture-synthesis imaging provides us with a unique opportunity to study the disk structure. Aims. Our aim is to study the intensity distribution of the disk of FS CMa in the mid-infrared L and N bands. Methods. We performed aperture-synthesis imaging of FS CMa with the MATISSE instrument (Multi AperTure mid-Infrared SpectroScopic Experiment) in the low spectral resolution mode to obtain images in the L and N bands. We computed radiative transfer models that reproduce the L- and N-band intensity distributions of the resolved disks. Results. We present L- and N-band aperture-synthesis images of FS CMa reconstructed in the wavelength bands of 3.4-3.8 and 8.6-9.0 mu m. In the L-band image, the inner rim region of an inclined circumstellar disk and the central object can be seen with a spatial resolution of 2.7 milliarcsec (mas). An inner disk cavity with an angular diameter of similar to 6 x 12 mas is resolved. The L-band disk consists of a bright northwestern (NW) disk region and a much fainter southeastern (SE) region. The images suggest that we are looking at the bright inner wall of the NW disk rim, which is on the far side of the disk. In the N band, only the bright NW disk region is seen. In addition to deriving the inclination and the inner disk radius, fitting the reconstructed brightness distributions via radiative transfer modelling allows one to constrain the innermost disk structure, in particular the shape of theinner disk rim.

Published
2022

10. Locating dust and molecules in the inner circumstellar environment of R Sculptoris with MATISSE

Author

Drevon, J., Millour, F., Cruzalebes, P., Paladini, C., Hron, J., Meilland, A., Allouche, F., Hofmann, K. -h., Lagarde, S., Lopez, B., Matter, A., Petrov, R., Robbe-Dubois, S., Schertl, D., Scicluna, P., Wittkowski, M., Zins, G., abraham, P., Antonelli, P., Beckmann, U., Berio, P., Bettonvil, F., Glindemann, A., Graser, U., Heininger, M., Henning, Th., Isbell, J. W., Jaffe, W., Labadie, L., Leinert, C., Lehmitz, M., Morel, S., Meisenheimer, K., Soulain, A., Varga, J., Weigelt, G., Woillez, J., Augereau, J. -c., van Boekel, R., Burtscher, L., Danchi, W. C., Dominik, C., Gamez Rosas, V., Hocde, V., Hogerheijde, M. R., Klarmann, L., Kokoulina, E., Leftley, J., Stee, P., Vakili, F., Waters, R., Wolf, S., Yoffe, G., Drevon, J., Millour, F., Cruzalebes, P., Paladini, C., Hron, J., Meilland, A., Allouche, F., Hofmann, K. -h., Lagarde, S., Lopez, B., Matter, A., Petrov, R., Robbe-Dubois, S., Schertl, D., Scicluna, P., Wittkowski, M., Zins, G., abraham, P., Antonelli, P., Beckmann, U., Berio, P., Bettonvil, F., Glindemann, A., Graser, U., Heininger, M., Henning, Th., Isbell, J. W., Jaffe, W., Labadie, L., Leinert, C., Lehmitz, M., Morel, S., Meisenheimer, K., Soulain, A., Varga, J., Weigelt, G., Woillez, J., Augereau, J. -c., van Boekel, R., Burtscher, L., Danchi, W. C., Dominik, C., Gamez Rosas, V., Hocde, V., Hogerheijde, M. R., Klarmann, L., Kokoulina, E., Leftley, J., Stee, P., Vakili, F., Waters, R., Wolf, S., and Yoffe, G.

Abstract

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 x 10(-6) M-circle dot 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 mu m. 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 o

Published
2022

11. MATISSE, the VLTI mid-infrared imaging spectro-interferometer

Author

Lopez, B., Lagarde, S., Petrov, R. G., Jaffe, W., Antonelli, P., Allouche, F., Berio, P., Matter, A., Meilland, A., Millour, F., Robbe-Dubois, S., Henning, Th, Weigelt, G., Glindemann, A., Agocs, T., Bailet, Ch, Beckmann, U., Bettonvil, F., van Boekel, R., Bourget, P., Bresson, Y., Bristow, P., Cruzalebes, P., Eldswijk, E., Caujolle, Y. Fantei, Herrera, J. C. Gonzalez, Graser, U., Guajardo, P., Heininger, M., Hofmann, K-H, Kroes, G., Laun, W., Lehmitz, M., Leinert, C., Meisenheimer, K., Morel, S., Neumann, U., Paladini, C., Percheron, I, Riquelme, M., Schoeller, M., Stee, Ph, Venema, L., Woillez, J., Zins, G., Abraham, P., Abadie, S., Abuter, R., Accardo, M., Adler, T., Alonso, J., Augereau, J-C, Boehm, A., Bazin, G., Beltran, J., Bensberg, A., Boland, W., Brast, R., Burtscher, L., Castillo, R., Chelli, A., Cid, C., Clausse, J-M, Connot, C., Conzelmann, R. D., Danchi, W-C, Delbo, M., Drevon, J., Dominik, C., van Duin, A., Ebert, M., Eisenhauer, F., Flament, S., Frahm, R., Rosas, V. Gamez, Gabasch, A., Gallenne, A., Garces, E., Girard, P., Glazenborg, A., Gonte, F. Y. J., Guitton, F., de Haan, M., Hanenburg, H., Haubois, X., Hocde, V, Hogerheijde, M., ter Horst, R., Hron, J., Hummel, C. A., Hubin, N., Huerta, R., Idserda, J., Isbell, J. W., Ives, D., Jakob, G., Jasko, A., Jochum, L., Klarmann, L., Klein, R., Kragt, J., Kuindersma, S., Kokoulina, E., Labadie, L., Lacour, S., Leftley, J., Le Poole, R., Lizon, J-L, Lopez, M., Lykou, F., Merand, A., Marcotto, A., Mauclert, N., Maurer, T., Mehrgan, L. H., Meisner, J., Meixner, K., Mellein, M., Menut, J. L., Mohr, L., Mosoni, L., Navarro, R., Nussbaum, E., Pallanca, L., Pantin, E., Pasquini, L., Duc, T. Phan, Pott, J-U, Pozna, E., Richichi, A., Ridinger, A., Rigal, F., Rivinius, Th, Roelfsema, R., Rohloff, R-R, Rousseau, S., Salabert, D., Schertl, D., Schuhler, N., Schuil, M., Shabun, K., Soulain, A., Stephan, C., Toledo, P., Tristram, K., Tromp, N., Vakili, F., Varga, J., Vinther, J., Waters, L. B. F. M., Wittkowski, M., Wolf, S., Wrhel, F., Yoffe, G., Lopez, B., Lagarde, S., Petrov, R. G., Jaffe, W., Antonelli, P., Allouche, F., Berio, P., Matter, A., Meilland, A., Millour, F., Robbe-Dubois, S., Henning, Th, Weigelt, G., Glindemann, A., Agocs, T., Bailet, Ch, Beckmann, U., Bettonvil, F., van Boekel, R., Bourget, P., Bresson, Y., Bristow, P., Cruzalebes, P., Eldswijk, E., Caujolle, Y. Fantei, Herrera, J. C. Gonzalez, Graser, U., Guajardo, P., Heininger, M., Hofmann, K-H, Kroes, G., Laun, W., Lehmitz, M., Leinert, C., Meisenheimer, K., Morel, S., Neumann, U., Paladini, C., Percheron, I, Riquelme, M., Schoeller, M., Stee, Ph, Venema, L., Woillez, J., Zins, G., Abraham, P., Abadie, S., Abuter, R., Accardo, M., Adler, T., Alonso, J., Augereau, J-C, Boehm, A., Bazin, G., Beltran, J., Bensberg, A., Boland, W., Brast, R., Burtscher, L., Castillo, R., Chelli, A., Cid, C., Clausse, J-M, Connot, C., Conzelmann, R. D., Danchi, W-C, Delbo, M., Drevon, J., Dominik, C., van Duin, A., Ebert, M., Eisenhauer, F., Flament, S., Frahm, R., Rosas, V. Gamez, Gabasch, A., Gallenne, A., Garces, E., Girard, P., Glazenborg, A., Gonte, F. Y. J., Guitton, F., de Haan, M., Hanenburg, H., Haubois, X., Hocde, V, Hogerheijde, M., ter Horst, R., Hron, J., Hummel, C. A., Hubin, N., Huerta, R., Idserda, J., Isbell, J. W., Ives, D., Jakob, G., Jasko, A., Jochum, L., Klarmann, L., Klein, R., Kragt, J., Kuindersma, S., Kokoulina, E., Labadie, L., Lacour, S., Leftley, J., Le Poole, R., Lizon, J-L, Lopez, M., Lykou, F., Merand, A., Marcotto, A., Mauclert, N., Maurer, T., Mehrgan, L. H., Meisner, J., Meixner, K., Mellein, M., Menut, J. L., Mohr, L., Mosoni, L., Navarro, R., Nussbaum, E., Pallanca, L., Pantin, E., Pasquini, L., Duc, T. Phan, Pott, J-U, Pozna, E., Richichi, A., Ridinger, A., Rigal, F., Rivinius, Th, Roelfsema, R., Rohloff, R-R, Rousseau, S., Salabert, D., Schertl, D., Schuhler, N., Schuil, M., Shabun, K., Soulain, A., Stephan, C., Toledo, P., Tristram, K., Tromp, N., Vakili, F., Varga, J., Vinther, J., Waters, L. B. F. M., Wittkowski, M., Wolf, S., Wrhel, F., and Yoffe, G.

Abstract

Context. Optical interferometry is at a key development stage. The Very Large Telescope Interferometer (VLTI) has established a stable, robust infrastructure for long-baseline interferometry that is usable by general astronomical observers. The present second-generation instruments offer a wide wavelength coverage and improved performance. Their sensitivity and measurement accuracy lead to data and images of high reliability. Aims. We have developed the Multi AperTure mid-Infrared SpectroScopic Experiment (MATISSE) to access, for the first time, high resolution imaging in a wide spectral domain. Many front-line topics are explored with this new equipment, including: stellar activity and mass loss; planet formation and evolution in the gas and dust disks around young stars; and environment interaction and accretion processes around super massive black holes in active galactic nuclei. Methods. The instrument is a spectro-interferometric imager in the transmission windows called L, M, and N, from 2.8 to 13.0 microns, combining four optical beams from the VLTI's unit or auxiliary telescopes. Its concept, related observing procedure, data reduction, and calibration approach, is the product of 30 years of instrumental research and has benefitted from the expertise developed in the frame of the VLTI's first generation instruments. The instrument utilises a multi-axial beam combination that delivers spectrally dispersed fringes. The signal provides the following quantities at several spectral resolutions: photometric flux, coherent fluxes, visibilities, closure phases, wavelength differential visibilities and phases, and aperture-synthesis imaging. Results. This article provides an overview of the physical principle of the instrument and its functionalities. The motivation of the choice of the instrumental concept and the characteristics of the delivered signal are detailed with a description of the observing modes and of their performance limit. MATISSE offers four spectra

Published
2022

12. MATISSE, the VLTI mid-infrared imaging spectro-interferometer

Author

Lopez, B., primary, Lagarde, S., additional, Petrov, R. G., additional, Jaffe, W., additional, Antonelli, P., additional, Allouche, F., additional, Berio, P., additional, Matter, A., additional, Meilland, A., additional, Millour, F., additional, Robbe-Dubois, S., additional, Henning, Th., additional, Weigelt, G., additional, Glindemann, A., additional, Agocs, T., additional, Bailet, Ch., additional, Beckmann, U., additional, Bettonvil, F., additional, van Boekel, R., additional, Bourget, P., additional, Bresson, Y., additional, Bristow, P., additional, Cruzalèbes, P., additional, Eldswijk, E., additional, Fanteï Caujolle, Y., additional, González Herrera, J. C., additional, Graser, U., additional, Guajardo, P., additional, Heininger, M., additional, Hofmann, K.-H., additional, Kroes, G., additional, Laun, W., additional, Lehmitz, M., additional, Leinert, C., additional, Meisenheimer, K., additional, Morel, S., additional, Neumann, U., additional, Paladini, C., additional, Percheron, I., additional, Riquelme, M., additional, Schoeller, M., additional, Stee, Ph., additional, Venema, L., additional, Woillez, J., additional, Zins, G., additional, Ábrahám, P., additional, Abadie, S., additional, Abuter, R., additional, Accardo, M., additional, Adler, T., additional, Alonso, J., additional, Augereau, J.-C., additional, Böhm, A., additional, Bazin, G., additional, Beltran, J., additional, Bensberg, A., additional, Boland, W., additional, Brast, R., additional, Burtscher, L., additional, Castillo, R., additional, Chelli, A., additional, Cid, C., additional, Clausse, J.-M., additional, Connot, C., additional, Conzelmann, R. D., additional, Danchi, W.-C., additional, Delbo, M., additional, Drevon, J., additional, Dominik, C., additional, van Duin, A., additional, Ebert, M., additional, Eisenhauer, F., additional, Flament, S., additional, Frahm, R., additional, Gámez Rosas, V., additional, Gabasch, A., additional, Gallenne, A., additional, Garces, E., additional, Girard, P., additional, Glazenborg, A., additional, Gonté, F. Y. J., additional, Guitton, F., additional, de Haan, M., additional, Hanenburg, H., additional, Haubois, X., additional, Hocdé, V., additional, Hogerheijde, M., additional, ter Horst, R., additional, Hron, J., additional, Hummel, C. A., additional, Hubin, N., additional, Huerta, R., additional, Idserda, J., additional, Isbell, J. W., additional, Ives, D., additional, Jakob, G., additional, Jaskó, A., additional, Jochum, L., additional, Klarmann, L., additional, Klein, R., additional, Kragt, J., additional, Kuindersma, S., additional, Kokoulina, E., additional, Labadie, L., additional, Lacour, S., additional, Leftley, J., additional, Le Poole, R., additional, Lizon, J.-L., additional, Lopez, M., additional, Lykou, F., additional, Mérand, A., additional, Marcotto, A., additional, Mauclert, N., additional, Maurer, T., additional, Mehrgan, L. H., additional, Meisner, J., additional, Meixner, K., additional, Mellein, M., additional, Menut, J. L., additional, Mohr, L., additional, Mosoni, L., additional, Navarro, R., additional, Nußbaum, E., additional, Pallanca, L., additional, Pantin, E., additional, Pasquini, L., additional, Phan Duc, T., additional, Pott, J.-U., additional, Pozna, E., additional, Richichi, A., additional, Ridinger, A., additional, Rigal, F., additional, Rivinius, Th., additional, Roelfsema, R., additional, Rohloff, R.-R., additional, Rousseau, S., additional, Salabert, D., additional, Schertl, D., additional, Schuhler, N., additional, Schuil, M., additional, Shabun, K., additional, Soulain, A., additional, Stephan, C., additional, Toledo, P., additional, Tristram, K., additional, Tromp, N., additional, Vakili, F., additional, Varga, J., additional, Vinther, J., additional, Waters, L. B. F. M., additional, Wittkowski, M., additional, Wolf, S., additional, Wrhel, F., additional, and Yoffe, G., additional

Published
2022
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13. MATISSE, the VLTI mid-infrared imaging spectro-interferometer at the time of the first published astrophysical results

Author

Lagarde, S., Meilland, A., Lopez, B., Petrov, R.G., Allouche, F., Matter, A., Augereau, J.-C., Berio, P., Bettonvil, F., Van Boekel, R., Bristow, P., Cruzalèbes, P., Danchi, W.C., Glindemann, A., Hadjara, M., Henninger, M., Hogerheijde, M.R., Jaffe, W.J., Leftley, J., Lehmitz, M., Millour, F., Paladini, C., Pantin, E., Riquelme, M., Rivinius, T., Robbe-Dubois, S., Schoeller, M., Varga, J., Weigelt, G., Woillez, J., Zins, G., Mérand, A., Sallum, S., Sanchez-Bermudez, J., Mérand, A., Sallum, S., and Sanchez-Bermudez, J.

Published
2022

14. VLTI-MATISSE L- and N-band aperture-synthesis imaging of the unclassified B[e] star FS Canis Majoris

Author

Hofmann, K.-H., primary, Bensberg, A., additional, Schertl, D., additional, Weigelt, G., additional, Wolf, S., additional, Meilland, A., additional, Millour, F., additional, Waters, L. B. F. M., additional, Kraus, S., additional, Ohnaka, K., additional, Lopez, B., additional, Petrov, R. G., additional, Lagarde, S., additional, Berio, Ph., additional, Allouche, F., additional, Robbe-Dubois, S., additional, Jaffe, W., additional, Henning, Th., additional, Paladini, C., additional, Schöller, M., additional, Mérand, A., additional, Glindemann, A., additional, Beckmann, U., additional, Heininger, M., additional, Bettonvil, F., additional, Zins, G., additional, Woillez, J., additional, Bristow, P., additional, Stee, P., additional, Vakili, F., additional, van Boekel, R., additional, Hogerheijde, M. R., additional, Dominik, C., additional, Augereau, J.-C., additional, Matter, A., additional, Hron, J., additional, Pantin, E., additional, Rivinius, Th., additional, de Wit, W.-J., additional, Varga, J., additional, Klarmann, L., additional, Meisenheimer, K., additional, Gámez Rosas, V., additional, Burtscher, L., additional, Leftley, J., additional, Isbell, J. W., additional, Yoffe, G., additional, Kokoulina, E., additional, Danchi, W. C., additional, Cruzalèbes, P., additional, Domiciano de Souza, A., additional, Drevon, J., additional, Hocdé, V., additional, Kreplin, A., additional, Labadie, L., additional, Connot, C., additional, Nußbaum, E., additional, Lehmitz, M., additional, Antonelli, P., additional, Graser, U., additional, and Leinert, C., additional

Published
2022
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15. The extended atmosphere and circumstellar environment of the cool evolved star VX Sagittarii as seen by MATISSE

Author

Chiavassa, A., primary, Kravchenko, K., additional, Montargès, M., additional, Millour, F., additional, Matter, A., additional, Freytag, B., additional, Wittkowski, M., additional, Hocdé, V., additional, Cruzalèbes, P., additional, Allouche, F., additional, Lopez, B., additional, Lagarde, S., additional, Petrov, R. G., additional, Meilland, A., additional, Robbe-Dubois, S., additional, Hofmann, K.-H., additional, Weigelt, G., additional, Berio, P., additional, Bendjoya, P., additional, Bettonvil, F., additional, Domiciano de Souza, A., additional, Heininger, M., additional, Henning, Th., additional, Isbell, J. W., additional, Jaffe, W., additional, Labadie, L., additional, Lehmitz, M., additional, Meisenheimer, K., additional, Soulain, A., additional, Varga, J., additional, Augereau, J.-C., additional, van Boekel, R., additional, Burtscher, L., additional, Danchi, W. C., additional, Dominik, C., additional, Drevon, J., additional, Gámez Rosas, V., additional, Hogerheijde, M. R., additional, Hron, J., additional, Klarmann, L., additional, Kokoulina, E., additional, Lagadec, E., additional, Leftley, J., additional, Mosoni, L., additional, Nardetto, N., additional, Paladini, C., additional, Pantin, E., additional, Schertl, D., additional, Stee, P., additional, Szabados, L., additional, Waters, R., additional, Wolf, S., additional, and Yoffe, G., additional

Published
2022
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18. Thermal imaging of dust hiding the black hole in NGC 1068.

Author

Gámez Rosas V, Isbell JW, Jaffe W, Petrov RG, Leftley JH, Hofmann KH, Millour F, Burtscher L, Meisenheimer K, Meilland A, Waters LBFM, Lopez B, Lagarde S, Weigelt G, Berio P, Allouche F, Robbe-Dubois S, Cruzalèbes P, Bettonvil F, Henning T, Augereau JC, Antonelli P, Beckmann U, van Boekel R, Bendjoya P, Danchi WC, Dominik C, Drevon J, Gallimore JF, Graser U, Heininger M, Hocdé V, Hogerheijde M, Hron J, Impellizzeri CMV, Klarmann L, Kokoulina E, Labadie L, Lehmitz M, Matter A, Paladini C, Pantin E, Pott JU, Schertl D, Soulain A, Stee P, Tristram K, Varga J, Woillez J, Wolf S, Yoffe G, and Zins G

Abstract

In the widely accepted 'unified model' 1 solution of the classification puzzle of active galactic nuclei, the orientation of a dusty accretion torus around the central black hole dominates their appearance. In 'type-1' systems, the bright nucleus is visible at the centre of a face-on torus. In 'type-2' systems the thick, nearly edge-on torus hides the central engine. Later studies suggested evolutionary effects 2 and added dusty clumps and polar winds 3 but left the basic picture intact. However, recent high-resolution images 4 of the archetypal type-2 galaxy NGC 1068 5,6 , suggested a more radical revision. The images displayed a ring-like emission feature that was proposed to be hot dust surrounding the black hole at the radius where the radiation from the central engine evaporates the dust. That ring is too thin and too far tilted from edge-on to hide the central engine, and ad hoc foreground extinction is needed to explain the type-2 classification. These images quickly generated reinterpretations of the dichotomy between types 1 and 2 7,8 . Here we present new multi-band mid-infrared images of NGC 1068 that detail the dust temperature distribution and reaffirm the original model. Combined with radio data (J.F.G. and C.M.V.I., manuscript in preparation), our maps locate the central engine that is below the previously reported ring and obscured by a thick, nearly edge-on disk, as predicted by the unified model. We also identify emission from polar flows and absorbing dust that is mineralogically distinct from that towards the Milky Way centre., (© 2022. The Author(s), under exclusive licence to Springer Nature Limited.)

Published
2022
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