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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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 |
format | Article |
fullrecord | <record><control><sourceid>arxiv_GOX</sourceid><recordid>TN_cdi_arxiv_primary_2205_12878</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2205_12878</sourcerecordid><originalsourceid>FETCH-arxiv_primary_2205_128783</originalsourceid><addsrcrecordid>eNqFjrEOgjAURbs4GPUDnHyDgw5geUAss9E46SBxJaWWUAOUlGLk763E3eQmN7k5NzmELAPqRyyO6Y6bt3r5iDT2A2R7NiVFWkqo-8oqUWrzgM7KquIGtBBu5FbpBlyQBglchdW5NIAI-QDWHa3hTeddZGv7RnFH5k8pLGxYlCBu3YuGcL-tM5yTScGrTi5-PSOr0zE9nL3RKGuNqrkZsq9ZNpqF_4kPfx9ArQ</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype></control><display><type>article</type><title>The multichord stellar occultation on 2019 October 22 by the trans-Neptunian object (84922) 2003 VS$_2</title><source>arXiv.org</source><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</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&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><identifier>DOI: 10.48550/arxiv.2205.12878</identifier><language>eng</language><subject>Physics - Earth and Planetary Astrophysics ; Physics - Solar and Stellar Astrophysics</subject><creationdate>2022-05</creationdate><rights>http://creativecommons.org/licenses/by/4.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,885</link.rule.ids><linktorsrc>$$Uhttps://arxiv.org/abs/2205.12878$$EView_record_in_Cornell_University$$FView_record_in_$$GCornell_University$$Hfree_for_read</linktorsrc><backlink>$$Uhttps://doi.org/10.1051/0004-6361/202141842$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.48550/arXiv.2205.12878$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Vara-Lubiano, M</creatorcontrib><creatorcontrib>Benedetti-Rossi, G</creatorcontrib><creatorcontrib>Santos-Sanz, P</creatorcontrib><creatorcontrib>Ortiz, J. L</creatorcontrib><creatorcontrib>Sicardy, B</creatorcontrib><creatorcontrib>Popescu, M</creatorcontrib><creatorcontrib>Morales, N</creatorcontrib><creatorcontrib>Rommel, F. L</creatorcontrib><creatorcontrib>Morgado, B</creatorcontrib><creatorcontrib>Pereira, C. L</creatorcontrib><creatorcontrib>Álvarez-Candal, A</creatorcontrib><creatorcontrib>Fernández-Valenzuela, E</creatorcontrib><creatorcontrib>Souami, D</creatorcontrib><creatorcontrib>Ilic, D</creatorcontrib><creatorcontrib>Vince, O</creatorcontrib><creatorcontrib>Bachev, R</creatorcontrib><creatorcontrib>Semkov, E</creatorcontrib><creatorcontrib>Nedelcu, D. A</creatorcontrib><creatorcontrib>Şonka, A</creatorcontrib><creatorcontrib>Hudin, L</creatorcontrib><creatorcontrib>Boaca, M</creatorcontrib><creatorcontrib>Inceu, V</creatorcontrib><creatorcontrib>Curelaru, L</creatorcontrib><creatorcontrib>Gherase, R</creatorcontrib><creatorcontrib>Turcu, V</creatorcontrib><creatorcontrib>Moldovan, D</creatorcontrib><creatorcontrib>Mircea, L</creatorcontrib><creatorcontrib>Predatu, M</creatorcontrib><creatorcontrib>Teodorescu, M</creatorcontrib><creatorcontrib>Stoian, L</creatorcontrib><creatorcontrib>Juravle, A</creatorcontrib><creatorcontrib>Braga-Ribas, F</creatorcontrib><creatorcontrib>Desmars, J</creatorcontrib><creatorcontrib>Duffard, R</creatorcontrib><creatorcontrib>Lecacheux, J</creatorcontrib><creatorcontrib>Camargo, J. I. 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$_2</title><description>A&A 663, A121 (2022) We predicted, observed, and analyzed the multichord stellar occultation of
the Second Gaia Data Release (Gaia DR2) source 3449076721168026624 (m$_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. L</creator><creator>Álvarez-Candal, A</creator><creator>Fernández-Valenzuela, E</creator><creator>Souami, D</creator><creator>Ilic, D</creator><creator>Vince, O</creator><creator>Bachev, R</creator><creator>Semkov, E</creator><creator>Nedelcu, D. A</creator><creator>Şonka, A</creator><creator>Hudin, L</creator><creator>Boaca, M</creator><creator>Inceu, V</creator><creator>Curelaru, L</creator><creator>Gherase, R</creator><creator>Turcu, V</creator><creator>Moldovan, D</creator><creator>Mircea, L</creator><creator>Predatu, M</creator><creator>Teodorescu, M</creator><creator>Stoian, L</creator><creator>Juravle, A</creator><creator>Braga-Ribas, F</creator><creator>Desmars, J</creator><creator>Duffard, R</creator><creator>Lecacheux, J</creator><creator>Camargo, J. I. B</creator><creator>Assafin, M</creator><creator>Vieira-Martins, R</creator><creator>Pribulla, T</creator><creator>Husárik, M</creator><creator>Sivanič, P</creator><creator>Pal, A</creator><creator>Szakats, R</creator><creator>Kiss, C</creator><creator>Alonso-Santiago, J</creator><creator>Frasca, A</creator><creator>Szabó, G. M</creator><creator>Derekas, A</creator><creator>Szigeti, L</creator><creator>Drozdz, M</creator><creator>Ogloza, W</creator><creator>Skvaruc, J</creator><creator>Ciabattari, F</creator><creator>Delincak, P</creator><creator>Di Marcantonio, P</creator><creator>Iafrate, G</creator><creator>Coretti, I</creator><creator>Baldini, V</creator><creator>Baruffetti, P</creator><creator>Klös, O</creator><creator>Dumitrescu, V</creator><creator>Mikuž, H</creator><creator>Mohar, A</creator><scope>GOX</scope></search><sort><creationdate>20220525</creationdate><title>The multichord stellar occultation on 2019 October 22 by the trans-Neptunian object (84922) 2003 VS$_2</title><author>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</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-arxiv_primary_2205_128783</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><topic>Physics - Earth and Planetary Astrophysics</topic><topic>Physics - Solar and Stellar Astrophysics</topic><toplevel>online_resources</toplevel><creatorcontrib>Vara-Lubiano, M</creatorcontrib><creatorcontrib>Benedetti-Rossi, G</creatorcontrib><creatorcontrib>Santos-Sanz, P</creatorcontrib><creatorcontrib>Ortiz, J. L</creatorcontrib><creatorcontrib>Sicardy, B</creatorcontrib><creatorcontrib>Popescu, M</creatorcontrib><creatorcontrib>Morales, N</creatorcontrib><creatorcontrib>Rommel, F. 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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&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> |
fulltext | fulltext_linktorsrc |
identifier | DOI: 10.48550/arxiv.2205.12878 |
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language | eng |
recordid | cdi_arxiv_primary_2205_12878 |
source | arXiv.org |
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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