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2D kinematics of massive stars near the Galactic Centre

Identificadores del recurso

Monthly Notices of the Royal Astronomical Society 500(3): 3213-3239(2021)

0035-8711

https://academic.oup.com/mnras/article-abstract/500/3/3213/5960177

http://hdl.handle.net/20.500.12666/564

10.1093/mnras/staa3329

1365-2966

http://dx.doi.org/10.13039/501100011033

https://doi.org/10.13039/501100007757

Procedencia

(DIGITAL.INTA)

Ficha

Título:: 2D kinematics of massive stars near the Galactic Centre
Tema:: Proper Motions; Stars: massive; Galaxy: centre; Open clsuters and associations: individual: Quintuplet; Open clusters and associations: individual; Arches
Descripción:: The presence of massive stars (MSs) in the region close to the Galactic Centre (GC) poses several questions about their origin. The harsh environment of the GC favours specific formation scenarios, each of which should imprint characteristic kinematic features on the MSs. We present a 2D kinematic analysis of MSs in a GC region surrounding Sgr A* based on high-precision proper motions obtained with the Hubble Space Telescope. Thanks to a careful data reduction, well-measured bright stars in our proper-motion catalogues have errors better than 0.5 mas yr−1. We discuss the absolute motion of the MSs in the field and their motion relative to Sgr A*, the Arches, and the Quintuplet. For the majority of the MSs, we rule out any distance further than 3–4 kpc from Sgr A* using only kinematic arguments. If their membership to the GC is confirmed, most of the isolated MSs are likely not associated with either the Arches or Quintuplet clusters or Sgr A*. Only a few MSs have proper motions, suggesting that they are likely members of the Arches cluster, in agreement with previous spectroscopic results. Line-of-sight radial velocities and distances are required to shed further light on the origin of most of these massive objects. We also present an analysis of other fast-moving objects in the GC region, finding no clear excess of high-velocity escaping stars. We make our astro-photometric catalogues publicly available.; ML and AB acknowledge support from STScI grants GO 12915 and 13771. DJL acknowledges support from the Spanish Government Ministerio de Ciencia, Innovacion y Universidades through grants PGC-2018-091 3741-B-C22 and from the Canarian Agency for Research, Innovation and Information Society (ACIISI), of the Canary Islands Government, and the European Regional Development Fund (ERDF), under grant with reference ProID2017010115. LRP acknowledges support from the Generalitat Valenciana through the grant PROMETEO/2019/041. LRB acknowledges partial support by MIUR under PRIN programme no. 2017Z2HSMF. The authors thank the anonymous referee for the useful comments and suggestions. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia MultilateralAgreement. This research made use of Astropy,10 a community-developed core PYTHON package for Astronomy (Astropy Collaboration 2013, 2018). This research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France.; Peerreview
Idioma:: English
Relación:: info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PGC2018-0913741-B-C22
Autor/Productor:: Libralato, M.; Lennon, D. J.; Bellini, A.; Van der Marel, R.; Clark, S. J.; Najarro, F.; Patrick, Lee R.; Anderson, J.; Bedin, L. R.; Crowther, P. A.; Mink, S. E.; Evans, C. J.; Platais, I.; Sabbi, E.; Sohn, S. T.
Editor:: Oxford Academics: Oxford University Press
Otros colaboradores/productores:: Bedin, L. [0000-0003-4080-6466]; Patrick, L. [0000-0002-9015-0269]; Libralato, M. [0000-0001-9673-7397]; Agencia Estatal de Investigación (AEI); Agencia Canaria de Investigación, Innovación y Sociedad de la Información (ACIISI); Generalitat Valenciana; Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR)
Derechos:: info:eu-repo/semantics/restrictedAccess; Copyright © 2020, Oxford University Press
Fecha:: 2022-02-15T13:17:19Z; 2021-01-14
Tipo de recurso:: info:eu-repo/semantics/article; info:eu-repo/semantics/publishedVersion; http://purl.org/coar/resource_type/c_6501
Formato:: application/pdf

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38. <dim:field element="description" lang="es" mdschema="dc" qualifier="sponsorship">ML and AB acknowledge support from STScI grants GO 12915 and 13771. DJL acknowledges support from the Spanish Government Ministerio de Ciencia, Innovacion y Universidades through grants PGC-2018-091 3741-B-C22 and from the Canarian Agency for Research, Innovation and Information Society (ACIISI), of the Canary Islands Government, and the European Regional Development Fund (ERDF), under grant with reference ProID2017010115. LRP acknowledges support from the Generalitat Valenciana through the grant PROMETEO/2019/041. LRB acknowledges partial support by MIUR under PRIN programme no. 2017Z2HSMF. The authors thank the anonymous referee for the useful comments and suggestions. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia MultilateralAgreement. This research made use of Astropy,10 a community-developed core PYTHON package for Astronomy (Astropy Collaboration 2013, 2018). This research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France.</dim:field>
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3. <creator>Lennon, D. J.</creator>
4. <creator>Bellini, A.</creator>
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6. <creator>Clark, S. J.</creator>
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8. <creator>Patrick, Lee R.</creator>
9. <creator>Anderson, J.</creator>
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13. <creator>Evans, C. J.</creator>
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16. <creator>Sohn, S. T.</creator>
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19. <contributor>Libralato, M. [0000-0001-9673-7397]</contributor>
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22. <contributor>Generalitat Valenciana</contributor>
23. <contributor>Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR)</contributor>
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30. <description>The presence of massive stars (MSs) in the region close to the Galactic Centre (GC) poses several questions about their origin. The harsh environment of the GC favours specific formation scenarios, each of which should imprint characteristic kinematic features on the MSs. We present a 2D kinematic analysis of MSs in a GC region surrounding Sgr A* based on high-precision proper motions obtained with the Hubble Space Telescope. Thanks to a careful data reduction, well-measured bright stars in our proper-motion catalogues have errors better than 0.5 mas yr−1. We discuss the absolute motion of the MSs in the field and their motion relative to Sgr A*, the Arches, and the Quintuplet. For the majority of the MSs, we rule out any distance further than 3–4 kpc from Sgr A* using only kinematic arguments. If their membership to the GC is confirmed, most of the isolated MSs are likely not associated with either the Arches or Quintuplet clusters or Sgr A*. Only a few MSs have proper motions, suggesting that they are likely members of the Arches cluster, in agreement with previous spectroscopic results. Line-of-sight radial velocities and distances are required to shed further light on the origin of most of these massive objects. We also present an analysis of other fast-moving objects in the GC region, finding no clear excess of high-velocity escaping stars. We make our astro-photometric catalogues publicly available.</description>
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1. <mods:name>
  1. <mods:namePart>Libralato, M.</mods:namePart>
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2. <mods:name>
  1. <mods:namePart>Lennon, D. J.</mods:namePart>
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3. <mods:name>
  1. <mods:namePart>Bellini, A.</mods:namePart>
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4. <mods:name>
  1. <mods:namePart>Van der Marel, R.</mods:namePart>
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5. <mods:name>
  1. <mods:namePart>Clark, S. J.</mods:namePart>
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6. <mods:name>
  1. <mods:namePart>Najarro, F.</mods:namePart>
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7. <mods:name>
  1. <mods:namePart>Patrick, Lee R.</mods:namePart>
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8. <mods:name>
  1. <mods:namePart>Anderson, J.</mods:namePart>
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9. <mods:name>
  1. <mods:namePart>Bedin, L. R.</mods:namePart>
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10. <mods:name>
  1. <mods:namePart>Crowther, P. A.</mods:namePart>
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11. <mods:name>
  1. <mods:namePart>Mink, S. E.</mods:namePart>
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12. <mods:name>
  1. <mods:namePart>Evans, C. J.</mods:namePart>
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13. <mods:name>
  1. <mods:namePart>Platais, I.</mods:namePart>
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14. <mods:name>
  1. <mods:namePart>Sabbi, E.</mods:namePart>
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15. <mods:name>
  1. <mods:namePart>Sohn, S. T.</mods:namePart>
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16. <mods:extension>
  1. <mods:dateAvailable encoding="iso8601">2022-02-15T13:17:19Z</mods:dateAvailable>
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  1. <mods:dateIssued encoding="iso8601">2021-01-14</mods:dateIssued>
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19. <mods:identifier type="citation">Monthly Notices of the Royal Astronomical Society 500(3): 3213-3239(2021)</mods:identifier>
20. <mods:identifier type="issn">0035-8711</mods:identifier>
21. <mods:identifier type="other">https://academic.oup.com/mnras/article-abstract/500/3/3213/5960177</mods:identifier>
22. <mods:identifier type="uri">http://hdl.handle.net/20.500.12666/564</mods:identifier>
23. <mods:identifier type="doi">10.1093/mnras/staa3329</mods:identifier>
24. <mods:identifier type="e-issn">1365-2966</mods:identifier>
25. <mods:identifier type="funder">http://dx.doi.org/10.13039/501100011033</mods:identifier>
26. <mods:identifier type="funder">https://doi.org/10.13039/501100007757</mods:identifier>
27. <mods:abstract>The presence of massive stars (MSs) in the region close to the Galactic Centre (GC) poses several questions about their origin. The harsh environment of the GC favours specific formation scenarios, each of which should imprint characteristic kinematic features on the MSs. We present a 2D kinematic analysis of MSs in a GC region surrounding Sgr A* based on high-precision proper motions obtained with the Hubble Space Telescope. Thanks to a careful data reduction, well-measured bright stars in our proper-motion catalogues have errors better than 0.5 mas yr−1. We discuss the absolute motion of the MSs in the field and their motion relative to Sgr A*, the Arches, and the Quintuplet. For the majority of the MSs, we rule out any distance further than 3–4 kpc from Sgr A* using only kinematic arguments. If their membership to the GC is confirmed, most of the isolated MSs are likely not associated with either the Arches or Quintuplet clusters or Sgr A*. Only a few MSs have proper motions, suggesting that they are likely members of the Arches cluster, in agreement with previous spectroscopic results. Line-of-sight radial velocities and distances are required to shed further light on the origin of most of these massive objects. We also present an analysis of other fast-moving objects in the GC region, finding no clear excess of high-velocity escaping stars. We make our astro-photometric catalogues publicly available.</mods:abstract>
28. <mods:language>
  1. <mods:languageTerm>eng</mods:languageTerm>
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29. <mods:accessCondition type="useAndReproduction">Copyright © 2020, Oxford University Press</mods:accessCondition>
30. <mods:accessCondition type="useAndReproduction">info:eu-repo/semantics/restrictedAccess</mods:accessCondition>
31. <mods:accessCondition type="useAndReproduction">info:eu-repo/semantics/restrictedAccess</mods:accessCondition>
32. <mods:subject>
  1. <mods:topic>Proper Motions</mods:topic>
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33. <mods:subject>
  1. <mods:topic>Stars: massive</mods:topic>
  </mods:subject>
34. <mods:subject>
  1. <mods:topic>Galaxy: centre</mods:topic>
  </mods:subject>
35. <mods:subject>
  1. <mods:topic>Open clsuters and associations: individual: Quintuplet</mods:topic>
  </mods:subject>
36. <mods:subject>
  1. <mods:topic>Open clusters and associations: individual</mods:topic>
  </mods:subject>
37. <mods:subject>
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1. <dc:title>2D kinematics of massive stars near the Galactic Centre</dc:title>
2. <dc:creator>Libralato, M.</dc:creator>
3. <dc:creator>Lennon, D. J.</dc:creator>
4. <dc:creator>Bellini, A.</dc:creator>
5. <dc:creator>Van der Marel, R.</dc:creator>
6. <dc:creator>Clark, S. J.</dc:creator>
7. <dc:creator>Najarro, F.</dc:creator>
8. <dc:creator>Patrick, Lee R.</dc:creator>
9. <dc:creator>Anderson, J.</dc:creator>
10. <dc:creator>Bedin, L. R.</dc:creator>
11. <dc:creator>Crowther, P. A.</dc:creator>
12. <dc:creator>Mink, S. E.</dc:creator>
13. <dc:creator>Evans, C. J.</dc:creator>
14. <dc:creator>Platais, I.</dc:creator>
15. <dc:creator>Sabbi, E.</dc:creator>
16. <dc:creator>Sohn, S. T.</dc:creator>
17. <dc:contributor>Bedin, L. [0000-0003-4080-6466]</dc:contributor>
18. <dc:contributor>Patrick, L. [0000-0002-9015-0269]</dc:contributor>
19. <dc:contributor>Libralato, M. [0000-0001-9673-7397]</dc:contributor>
20. <dc:contributor>Agencia Estatal de Investigación (AEI)</dc:contributor>
21. <dc:contributor>Agencia Canaria de Investigación, Innovación y Sociedad de la Información (ACIISI)</dc:contributor>
22. <dc:contributor>Generalitat Valenciana</dc:contributor>
23. <dc:contributor>Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR)</dc:contributor>
24. <dc:subject>Proper Motions</dc:subject>
25. <dc:subject>Stars: massive</dc:subject>
26. <dc:subject>Galaxy: centre</dc:subject>
27. <dc:subject>Open clsuters and associations: individual: Quintuplet</dc:subject>
28. <dc:subject>Open clusters and associations: individual</dc:subject>
29. <dc:subject>Arches</dc:subject>
30. <dcterms:abstract>The presence of massive stars (MSs) in the region close to the Galactic Centre (GC) poses several questions about their origin. The harsh environment of the GC favours specific formation scenarios, each of which should imprint characteristic kinematic features on the MSs. We present a 2D kinematic analysis of MSs in a GC region surrounding Sgr A* based on high-precision proper motions obtained with the Hubble Space Telescope. Thanks to a careful data reduction, well-measured bright stars in our proper-motion catalogues have errors better than 0.5 mas yr−1. We discuss the absolute motion of the MSs in the field and their motion relative to Sgr A*, the Arches, and the Quintuplet. For the majority of the MSs, we rule out any distance further than 3–4 kpc from Sgr A* using only kinematic arguments. If their membership to the GC is confirmed, most of the isolated MSs are likely not associated with either the Arches or Quintuplet clusters or Sgr A*. Only a few MSs have proper motions, suggesting that they are likely members of the Arches cluster, in agreement with previous spectroscopic results. Line-of-sight radial velocities and distances are required to shed further light on the origin of most of these massive objects. We also present an analysis of other fast-moving objects in the GC region, finding no clear excess of high-velocity escaping stars. We make our astro-photometric catalogues publicly available.</dcterms:abstract>
31. <dcterms:dateAccepted>2022-02-15T13:17:19Z</dcterms:dateAccepted>
32. <dcterms:available>2022-02-15T13:17:19Z</dcterms:available>
33. <dcterms:created>2022-02-15T13:17:19Z</dcterms:created>
34. <dcterms:issued>2021-01-14</dcterms:issued>
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36. <dc:identifier>Monthly Notices of the Royal Astronomical Society 500(3): 3213-3239(2021)</dc:identifier>
37. <dc:identifier>0035-8711</dc:identifier>
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44. <dc:language>eng</dc:language>
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46. <dc:rights>Copyright © 2020, Oxford University Press</dc:rights>
47. <dc:rights>info:eu-repo/semantics/restrictedAccess</dc:rights>
48. <dc:rights>info:eu-repo/semantics/restrictedAccess</dc:rights>
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  1. <dc:title>2D kinematics of massive stars near the Galactic Centre</dc:title>
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  3. <dc:creator>Lennon, D. J.</dc:creator>
  4. <dc:creator>Bellini, A.</dc:creator>
  5. <dc:creator>Van der Marel, R.</dc:creator>
  6. <dc:creator>Clark, S. J.</dc:creator>
  7. <dc:creator>Najarro, F.</dc:creator>
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  10. <dc:creator>Bedin, L. R.</dc:creator>
  11. <dc:creator>Crowther, P. A.</dc:creator>
  12. <dc:creator>Mink, S. E.</dc:creator>
  13. <dc:creator>Evans, C. J.</dc:creator>
  14. <dc:creator>Platais, I.</dc:creator>
  15. <dc:creator>Sabbi, E.</dc:creator>
  16. <dc:creator>Sohn, S. T.</dc:creator>
  17. <dc:contributor>Bedin, L. [0000-0003-4080-6466]</dc:contributor>
  18. <dc:contributor>Patrick, L. [0000-0002-9015-0269]</dc:contributor>
  19. <dc:contributor>Libralato, M. [0000-0001-9673-7397]</dc:contributor>
  20. <dc:contributor>Agencia Estatal de Investigación (AEI)</dc:contributor>
  21. <dc:contributor>Agencia Canaria de Investigación, Innovación y Sociedad de la Información (ACIISI)</dc:contributor>
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  23. <dc:contributor>Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR)</dc:contributor>
  24. <dc:subject>Proper Motions</dc:subject>
  25. <dc:subject>Stars: massive</dc:subject>
  26. <dc:subject>Galaxy: centre</dc:subject>
  27. <dc:subject>Open clsuters and associations: individual: Quintuplet</dc:subject>
  28. <dc:subject>Open clusters and associations: individual</dc:subject>
  29. <dc:subject>Arches</dc:subject>
  30. <dc:description>The presence of massive stars (MSs) in the region close to the Galactic Centre (GC) poses several questions about their origin. The harsh environment of the GC favours specific formation scenarios, each of which should imprint characteristic kinematic features on the MSs. We present a 2D kinematic analysis of MSs in a GC region surrounding Sgr A* based on high-precision proper motions obtained with the Hubble Space Telescope. Thanks to a careful data reduction, well-measured bright stars in our proper-motion catalogues have errors better than 0.5 mas yr−1. We discuss the absolute motion of the MSs in the field and their motion relative to Sgr A*, the Arches, and the Quintuplet. For the majority of the MSs, we rule out any distance further than 3–4 kpc from Sgr A* using only kinematic arguments. If their membership to the GC is confirmed, most of the isolated MSs are likely not associated with either the Arches or Quintuplet clusters or Sgr A*. Only a few MSs have proper motions, suggesting that they are likely members of the Arches cluster, in agreement with previous spectroscopic results. Line-of-sight radial velocities and distances are required to shed further light on the origin of most of these massive objects. We also present an analysis of other fast-moving objects in the GC region, finding no clear excess of high-velocity escaping stars. We make our astro-photometric catalogues publicly available.</dc:description>
  31. <dc:date>2022-02-15T13:17:19Z</dc:date>
  32. <dc:date>2022-02-15T13:17:19Z</dc:date>
  33. <dc:date>2021-01-14</dc:date>
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  39. <dc:identifier>10.1093/mnras/staa3329</dc:identifier>
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  42. <dc:identifier>https://doi.org/10.13039/501100007757</dc:identifier>
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  45. <dc:rights>Copyright © 2020, Oxford University Press</dc:rights>
  46. <dc:rights>info:eu-repo/semantics/restrictedAccess</dc:rights>
  47. <dc:rights>info:eu-repo/semantics/restrictedAccess</dc:rights>
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