The multichord stellar occultation on 2019 October 22 by the trans-Neptunian object (84922) 2003 VS$_2

A&A 663, A121 (2022) We predicted, observed, and analyzed the multichord stellar occultation of the Second Gaia Data Release (Gaia DR2) source 3449076721168026624 (m$_v$ = 14.1 mag) by the plutino object 2003 VS$_2$ (hereafter, VS$_2$) on 2019 October 22. We also carried out photometric observat...

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Hauptverfasser: Vara-Lubiano, M, Benedetti-Rossi, G, Santos-Sanz, P, Ortiz, J. L, Sicardy, B, Popescu, M, Morales, N, Rommel, F. L, Morgado, B, Pereira, C. L, Álvarez-Candal, A, Fernández-Valenzuela, E, Souami, D, Ilic, D, Vince, O, Bachev, R, Semkov, E, Nedelcu, D. A, Şonka, A, Hudin, L, Boaca, M, Inceu, V, Curelaru, L, Gherase, R, Turcu, V, Moldovan, D, Mircea, L, Predatu, M, Teodorescu, M, Stoian, L, Juravle, A, Braga-Ribas, F, Desmars, J, Duffard, R, Lecacheux, J, Camargo, J. I. B, Assafin, M, Vieira-Martins, R, Pribulla, T, Husárik, M, Sivanič, P, Pal, A, Szakats, R, Kiss, C, Alonso-Santiago, J, Frasca, A, Szabó, G. M, Derekas, A, Szigeti, L, Drozdz, M, Ogloza, W, Skvaruc, J, Ciabattari, F, Delincak, P, Di Marcantonio, P, Iafrate, G, Coretti, I, Baldini, V, Baruffetti, P, Klös, O, Dumitrescu, V, Mikuž, H, Mohar, A
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creator Vara-Lubiano, M
Benedetti-Rossi, G
Santos-Sanz, P
Ortiz, J. L
Sicardy, B
Popescu, M
Morales, N
Rommel, F. L
Morgado, B
Pereira, C. L
Álvarez-Candal, A
Fernández-Valenzuela, E
Souami, D
Ilic, D
Vince, O
Bachev, R
Semkov, E
Nedelcu, D. A
Şonka, A
Hudin, L
Boaca, M
Inceu, V
Curelaru, L
Gherase, R
Turcu, V
Moldovan, D
Mircea, L
Predatu, M
Teodorescu, M
Stoian, L
Juravle, A
Braga-Ribas, F
Desmars, J
Duffard, R
Lecacheux, J
Camargo, J. I. B
Assafin, M
Vieira-Martins, R
Pribulla, T
Husárik, M
Sivanič, P
Pal, A
Szakats, R
Kiss, C
Alonso-Santiago, J
Frasca, A
Szabó, G. M
Derekas, A
Szigeti, L
Drozdz, M
Ogloza, W
Skvaruc, J
Ciabattari, F
Delincak, P
Di Marcantonio, P
Iafrate, G
Coretti, I
Baldini, V
Baruffetti, P
Klös, O
Dumitrescu, V
Mikuž, H
Mohar, A
description A&A 663, A121 (2022) We predicted, observed, and analyzed the multichord stellar occultation of the Second Gaia Data Release (Gaia DR2) source 3449076721168026624 (m$_v$ = 14.1 mag) by the plutino object 2003 VS$_2$ (hereafter, VS$_2$) on 2019 October 22. We also carried out photometric observations to derive the rotational light curve amplitude and rotational phase of VS$_2$ during the stellar occultation. Combining the results and assuming a triaxial shape, we derived the 3D shape of VS$_2$. Out of the 39 observatories involved in the observational campaign, 12 sites reported a positive detection; this makes it one of the best observed stellar occultations by a TNO so far. We obtained a rotational light curve amplitude of ${\Delta}$m = 0.264 $\pm$ 0.017 mag, a mean area-equivalent diameter of D$_{A_{eq}}$ = 545 $\pm$ 13 km, and a geometric albedo of 0.134 $\pm$ 0.010. The best triaxial shape obtained for VS$_2$ has semiaxes a = 339 $\pm$ 5 km, b = 235 $\pm$ 6 km, and c = 226 $\pm$ 8 km. The derived aspect angle is ${\theta}$ = 59${\deg} \pm$ 2${\deg}$ or its supplementary ${\theta}$ = 121${\deg} \pm$ 2${\deg}$, depending on the north-pole position. The spherical-volume equivalent diameter is D$_{V_{eq}}$ = 524 $\pm$ 7 km. If we consider large albedo patches on its surface, the semi-major axis of the ellipsoid could be ~10 km smaller. These results are compatible with the previous ones determined from the single-chord 2013 and four-chord 2014 stellar occultations and with the effective diameter and albedo derived from Herschel and Spitzer data. They provide evidence that VS$_2$'s 3D shape is not compatible with a homogeneous triaxial body in hydrostatic equilibrium, but it might be a differentiated body and/or might be sustaining some stress. No secondary features related to rings or material orbiting around VS$_2$ were detected.
doi_str_mv 10.48550/arxiv.2205.12878
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L ; Álvarez-Candal, A ; Fernández-Valenzuela, E ; Souami, D ; Ilic, D ; Vince, O ; Bachev, R ; Semkov, E ; Nedelcu, D. A ; Şonka, A ; Hudin, L ; Boaca, M ; Inceu, V ; Curelaru, L ; Gherase, R ; Turcu, V ; Moldovan, D ; Mircea, L ; Predatu, M ; Teodorescu, M ; Stoian, L ; Juravle, A ; Braga-Ribas, F ; Desmars, J ; Duffard, R ; Lecacheux, J ; Camargo, J. I. B ; Assafin, M ; Vieira-Martins, R ; Pribulla, T ; Husárik, M ; Sivanič, P ; Pal, A ; Szakats, R ; Kiss, C ; Alonso-Santiago, J ; Frasca, A ; Szabó, G. M ; Derekas, A ; Szigeti, L ; Drozdz, M ; Ogloza, W ; Skvaruc, J ; Ciabattari, F ; Delincak, P ; Di Marcantonio, P ; Iafrate, G ; Coretti, I ; Baldini, V ; Baruffetti, P ; Klös, O ; Dumitrescu, V ; Mikuž, H ; Mohar, A</creator><creatorcontrib>Vara-Lubiano, M ; Benedetti-Rossi, G ; Santos-Sanz, P ; Ortiz, J. L ; Sicardy, B ; Popescu, M ; Morales, N ; Rommel, F. L ; Morgado, B ; Pereira, C. L ; Álvarez-Candal, A ; Fernández-Valenzuela, E ; Souami, D ; Ilic, D ; Vince, O ; Bachev, R ; Semkov, E ; Nedelcu, D. A ; Şonka, A ; Hudin, L ; Boaca, M ; Inceu, V ; Curelaru, L ; Gherase, R ; Turcu, V ; Moldovan, D ; Mircea, L ; Predatu, M ; Teodorescu, M ; Stoian, L ; Juravle, A ; Braga-Ribas, F ; Desmars, J ; Duffard, R ; Lecacheux, J ; Camargo, J. I. B ; Assafin, M ; Vieira-Martins, R ; Pribulla, T ; Husárik, M ; Sivanič, P ; Pal, A ; Szakats, R ; Kiss, C ; Alonso-Santiago, J ; Frasca, A ; Szabó, G. M ; Derekas, A ; Szigeti, L ; Drozdz, M ; Ogloza, W ; Skvaruc, J ; Ciabattari, F ; Delincak, P ; Di Marcantonio, P ; Iafrate, G ; Coretti, I ; Baldini, V ; Baruffetti, P ; Klös, O ; Dumitrescu, V ; Mikuž, H ; Mohar, A</creatorcontrib><description>A&amp;A 663, A121 (2022) We predicted, observed, and analyzed the multichord stellar occultation of the Second Gaia Data Release (Gaia DR2) source 3449076721168026624 (m$_v$ = 14.1 mag) by the plutino object 2003 VS$_2$ (hereafter, VS$_2$) on 2019 October 22. We also carried out photometric observations to derive the rotational light curve amplitude and rotational phase of VS$_2$ during the stellar occultation. Combining the results and assuming a triaxial shape, we derived the 3D shape of VS$_2$. Out of the 39 observatories involved in the observational campaign, 12 sites reported a positive detection; this makes it one of the best observed stellar occultations by a TNO so far. We obtained a rotational light curve amplitude of ${\Delta}$m = 0.264 $\pm$ 0.017 mag, a mean area-equivalent diameter of D$_{A_{eq}}$ = 545 $\pm$ 13 km, and a geometric albedo of 0.134 $\pm$ 0.010. The best triaxial shape obtained for VS$_2$ has semiaxes a = 339 $\pm$ 5 km, b = 235 $\pm$ 6 km, and c = 226 $\pm$ 8 km. The derived aspect angle is ${\theta}$ = 59${\deg} \pm$ 2${\deg}$ or its supplementary ${\theta}$ = 121${\deg} \pm$ 2${\deg}$, depending on the north-pole position. The spherical-volume equivalent diameter is D$_{V_{eq}}$ = 524 $\pm$ 7 km. If we consider large albedo patches on its surface, the semi-major axis of the ellipsoid could be ~10 km smaller. These results are compatible with the previous ones determined from the single-chord 2013 and four-chord 2014 stellar occultations and with the effective diameter and albedo derived from Herschel and Spitzer data. They provide evidence that VS$_2$'s 3D shape is not compatible with a homogeneous triaxial body in hydrostatic equilibrium, but it might be a differentiated body and/or might be sustaining some stress. 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B</creatorcontrib><creatorcontrib>Assafin, M</creatorcontrib><creatorcontrib>Vieira-Martins, R</creatorcontrib><creatorcontrib>Pribulla, T</creatorcontrib><creatorcontrib>Husárik, M</creatorcontrib><creatorcontrib>Sivanič, P</creatorcontrib><creatorcontrib>Pal, A</creatorcontrib><creatorcontrib>Szakats, R</creatorcontrib><creatorcontrib>Kiss, C</creatorcontrib><creatorcontrib>Alonso-Santiago, J</creatorcontrib><creatorcontrib>Frasca, A</creatorcontrib><creatorcontrib>Szabó, G. M</creatorcontrib><creatorcontrib>Derekas, A</creatorcontrib><creatorcontrib>Szigeti, L</creatorcontrib><creatorcontrib>Drozdz, M</creatorcontrib><creatorcontrib>Ogloza, W</creatorcontrib><creatorcontrib>Skvaruc, J</creatorcontrib><creatorcontrib>Ciabattari, F</creatorcontrib><creatorcontrib>Delincak, P</creatorcontrib><creatorcontrib>Di Marcantonio, P</creatorcontrib><creatorcontrib>Iafrate, G</creatorcontrib><creatorcontrib>Coretti, I</creatorcontrib><creatorcontrib>Baldini, V</creatorcontrib><creatorcontrib>Baruffetti, P</creatorcontrib><creatorcontrib>Klös, O</creatorcontrib><creatorcontrib>Dumitrescu, V</creatorcontrib><creatorcontrib>Mikuž, H</creatorcontrib><creatorcontrib>Mohar, A</creatorcontrib><title>The multichord stellar occultation on 2019 October 22 by the trans-Neptunian object (84922) 2003 VS$_2</title><description>A&amp;A 663, A121 (2022) We predicted, observed, and analyzed the multichord stellar occultation of the Second Gaia Data Release (Gaia DR2) source 3449076721168026624 (m$_v$ = 14.1 mag) by the plutino object 2003 VS$_2$ (hereafter, VS$_2$) on 2019 October 22. We also carried out photometric observations to derive the rotational light curve amplitude and rotational phase of VS$_2$ during the stellar occultation. Combining the results and assuming a triaxial shape, we derived the 3D shape of VS$_2$. Out of the 39 observatories involved in the observational campaign, 12 sites reported a positive detection; this makes it one of the best observed stellar occultations by a TNO so far. We obtained a rotational light curve amplitude of ${\Delta}$m = 0.264 $\pm$ 0.017 mag, a mean area-equivalent diameter of D$_{A_{eq}}$ = 545 $\pm$ 13 km, and a geometric albedo of 0.134 $\pm$ 0.010. The best triaxial shape obtained for VS$_2$ has semiaxes a = 339 $\pm$ 5 km, b = 235 $\pm$ 6 km, and c = 226 $\pm$ 8 km. The derived aspect angle is ${\theta}$ = 59${\deg} \pm$ 2${\deg}$ or its supplementary ${\theta}$ = 121${\deg} \pm$ 2${\deg}$, depending on the north-pole position. The spherical-volume equivalent diameter is D$_{V_{eq}}$ = 524 $\pm$ 7 km. If we consider large albedo patches on its surface, the semi-major axis of the ellipsoid could be ~10 km smaller. These results are compatible with the previous ones determined from the single-chord 2013 and four-chord 2014 stellar occultations and with the effective diameter and albedo derived from Herschel and Spitzer data. They provide evidence that VS$_2$'s 3D shape is not compatible with a homogeneous triaxial body in hydrostatic equilibrium, but it might be a differentiated body and/or might be sustaining some stress. No secondary features related to rings or material orbiting around VS$_2$ were detected.</description><subject>Physics - Earth and Planetary Astrophysics</subject><subject>Physics - Solar and Stellar Astrophysics</subject><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><sourceid>GOX</sourceid><recordid>eNqFjrEOgjAURbs4GPUDnHyDgw5geUAss9E46SBxJaWWUAOUlGLk763E3eQmN7k5NzmELAPqRyyO6Y6bt3r5iDT2A2R7NiVFWkqo-8oqUWrzgM7KquIGtBBu5FbpBlyQBglchdW5NIAI-QDWHa3hTeddZGv7RnFH5k8pLGxYlCBu3YuGcL-tM5yTScGrTi5-PSOr0zE9nL3RKGuNqrkZsq9ZNpqF_4kPfx9ArQ</recordid><startdate>20220525</startdate><enddate>20220525</enddate><creator>Vara-Lubiano, M</creator><creator>Benedetti-Rossi, G</creator><creator>Santos-Sanz, P</creator><creator>Ortiz, J. L</creator><creator>Sicardy, B</creator><creator>Popescu, M</creator><creator>Morales, N</creator><creator>Rommel, F. L</creator><creator>Morgado, B</creator><creator>Pereira, C. 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M</creatorcontrib><creatorcontrib>Derekas, A</creatorcontrib><creatorcontrib>Szigeti, L</creatorcontrib><creatorcontrib>Drozdz, M</creatorcontrib><creatorcontrib>Ogloza, W</creatorcontrib><creatorcontrib>Skvaruc, J</creatorcontrib><creatorcontrib>Ciabattari, F</creatorcontrib><creatorcontrib>Delincak, P</creatorcontrib><creatorcontrib>Di Marcantonio, P</creatorcontrib><creatorcontrib>Iafrate, G</creatorcontrib><creatorcontrib>Coretti, I</creatorcontrib><creatorcontrib>Baldini, V</creatorcontrib><creatorcontrib>Baruffetti, P</creatorcontrib><creatorcontrib>Klös, O</creatorcontrib><creatorcontrib>Dumitrescu, V</creatorcontrib><creatorcontrib>Mikuž, H</creatorcontrib><creatorcontrib>Mohar, A</creatorcontrib><collection>arXiv.org</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Vara-Lubiano, M</au><au>Benedetti-Rossi, G</au><au>Santos-Sanz, P</au><au>Ortiz, J. L</au><au>Sicardy, B</au><au>Popescu, M</au><au>Morales, N</au><au>Rommel, F. L</au><au>Morgado, B</au><au>Pereira, C. L</au><au>Álvarez-Candal, A</au><au>Fernández-Valenzuela, E</au><au>Souami, D</au><au>Ilic, D</au><au>Vince, O</au><au>Bachev, R</au><au>Semkov, E</au><au>Nedelcu, D. A</au><au>Şonka, A</au><au>Hudin, L</au><au>Boaca, M</au><au>Inceu, V</au><au>Curelaru, L</au><au>Gherase, R</au><au>Turcu, V</au><au>Moldovan, D</au><au>Mircea, L</au><au>Predatu, M</au><au>Teodorescu, M</au><au>Stoian, L</au><au>Juravle, A</au><au>Braga-Ribas, F</au><au>Desmars, J</au><au>Duffard, R</au><au>Lecacheux, J</au><au>Camargo, J. I. B</au><au>Assafin, M</au><au>Vieira-Martins, R</au><au>Pribulla, T</au><au>Husárik, M</au><au>Sivanič, P</au><au>Pal, A</au><au>Szakats, R</au><au>Kiss, C</au><au>Alonso-Santiago, J</au><au>Frasca, A</au><au>Szabó, G. M</au><au>Derekas, A</au><au>Szigeti, L</au><au>Drozdz, M</au><au>Ogloza, W</au><au>Skvaruc, J</au><au>Ciabattari, F</au><au>Delincak, P</au><au>Di Marcantonio, P</au><au>Iafrate, G</au><au>Coretti, I</au><au>Baldini, V</au><au>Baruffetti, P</au><au>Klös, O</au><au>Dumitrescu, V</au><au>Mikuž, H</au><au>Mohar, A</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The multichord stellar occultation on 2019 October 22 by the trans-Neptunian object (84922) 2003 VS$_2</atitle><date>2022-05-25</date><risdate>2022</risdate><abstract>A&amp;A 663, A121 (2022) We predicted, observed, and analyzed the multichord stellar occultation of the Second Gaia Data Release (Gaia DR2) source 3449076721168026624 (m$_v$ = 14.1 mag) by the plutino object 2003 VS$_2$ (hereafter, VS$_2$) on 2019 October 22. We also carried out photometric observations to derive the rotational light curve amplitude and rotational phase of VS$_2$ during the stellar occultation. Combining the results and assuming a triaxial shape, we derived the 3D shape of VS$_2$. Out of the 39 observatories involved in the observational campaign, 12 sites reported a positive detection; this makes it one of the best observed stellar occultations by a TNO so far. We obtained a rotational light curve amplitude of ${\Delta}$m = 0.264 $\pm$ 0.017 mag, a mean area-equivalent diameter of D$_{A_{eq}}$ = 545 $\pm$ 13 km, and a geometric albedo of 0.134 $\pm$ 0.010. The best triaxial shape obtained for VS$_2$ has semiaxes a = 339 $\pm$ 5 km, b = 235 $\pm$ 6 km, and c = 226 $\pm$ 8 km. The derived aspect angle is ${\theta}$ = 59${\deg} \pm$ 2${\deg}$ or its supplementary ${\theta}$ = 121${\deg} \pm$ 2${\deg}$, depending on the north-pole position. The spherical-volume equivalent diameter is D$_{V_{eq}}$ = 524 $\pm$ 7 km. If we consider large albedo patches on its surface, the semi-major axis of the ellipsoid could be ~10 km smaller. These results are compatible with the previous ones determined from the single-chord 2013 and four-chord 2014 stellar occultations and with the effective diameter and albedo derived from Herschel and Spitzer data. They provide evidence that VS$_2$'s 3D shape is not compatible with a homogeneous triaxial body in hydrostatic equilibrium, but it might be a differentiated body and/or might be sustaining some stress. No secondary features related to rings or material orbiting around VS$_2$ were detected.</abstract><doi>10.48550/arxiv.2205.12878</doi><oa>free_for_read</oa></addata></record>
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identifier DOI: 10.48550/arxiv.2205.12878
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subjects Physics - Earth and Planetary Astrophysics
Physics - Solar and Stellar Astrophysics
title The multichord stellar occultation on 2019 October 22 by the trans-Neptunian object (84922) 2003 VS$_2
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