Distance to the Brick cloud using stellar kinematics

Context. The central molecular zone at the Galactic center is currently being studied intensively to understand how star formation proceeds under the extreme conditions of a galactic nucleus. Knowing the position of molecular clouds along the line of sight toward the Galactic center has had importan...

Descripción completa

Detalles Bibliográficos
Autores: Martínez-Arranz, Á., Schödel, Rainer, Nogueras-Lara, Francisco, Shahzamanian, B.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2022
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/272992
Acceso en línea:http://hdl.handle.net/10261/272992
Access Level:acceso abierto
Palabra clave:Proper motions
Infrared: general
Stars: kinematics and dynamics
Galaxy: center
Techniques: high angular resolution
Galaxy: structure
id ES_186e66c8fde6ba4fa4d5569f3c8b43b0
oai_identifier_str oai:digital.csic.es:10261/272992
network_acronym_str ES
network_name_str España
repository_id_str
spelling Distance to the Brick cloud using stellar kinematicsMartínez-Arranz, Á.Schödel, RainerNogueras-Lara, FranciscoShahzamanian, B.Proper motionsInfrared: generalStars: kinematics and dynamicsGalaxy: centerTechniques: high angular resolutionGalaxy: structureContext. The central molecular zone at the Galactic center is currently being studied intensively to understand how star formation proceeds under the extreme conditions of a galactic nucleus. Knowing the position of molecular clouds along the line of sight toward the Galactic center has had important implications in our understanding of the physics of the gas and star formation in the central molecular zone. It was recently claimed that the dense molecular cloud G0.253 + 0.016 (the Brick) has a distance of ∼7.20 kpc from the Sun. That would place it outside of the central molecular zone, and therefore of the nuclear stellar disk, but still inside the Bulge. Aims. Theoretical considerations as well as observational studies show that stars that belong to the nuclear stellar disk have different kinematics from those that belong to the inner Bulge. Therefore, we aim to constrain the distance to the Brick by studying the proper motions of the stars in the area. Methods. We used ESO HAWK-I/VLT imaging data from epochs 2015 and 2019 to compute proper motions on the Brick and in a nearby comparison field free of dark clouds. Results. The stellar population seen toward the nuclear stellar disk shows the following three kinematic components: (1) Bulge stars with an isotropic velocity dispersion of ∼3.5 micro-arc second per year; (2) eastward moving stars on the near side of the nuclear stellar disk; and (3) westward moving stars on the far side of the nuclear stellar disk. We clearly see all three components toward the comparison field. However, toward the Brick, which blocks the light from stars behind it, we can only see kinematic components (1) and (2). Conclusions. While the Brick blocks the light from stars on the far side of the nuclear stellar disk, the detection of a significant component of eastward streaming stars implies that the Brick must be located inside the nuclear stellar disk and, therefore, that it forms part of the central molecular zone. © ESO 2022.We acknowledge financial support from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709). We acknowledge financial support from national project PGC2018-095049-B-C21 (MCIU/AEI/FEDER, UE). FN-L gratefully acknowledges support by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) – Project-ID 138713538 – SFB 881 (“The Milky Way System”, subproject B8), and the sponsorship provided by the Federal Ministry for Education and Research of Germany through the Alexander von Humboldt Foundation.Peer reviewedEDP SciencesMinisterio de Ciencia e Innovación (España)European CommissionGerman Research FoundationConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202220222022info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/272992reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MICINN//SEV-2017-0709info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PGC2018-095049-B-C21http://dx.doi.org/10.1051/0004-6361/202243263Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2729922026-05-22T06:33:51Z
dc.title.none.fl_str_mv Distance to the Brick cloud using stellar kinematics
title Distance to the Brick cloud using stellar kinematics
spellingShingle Distance to the Brick cloud using stellar kinematics
Martínez-Arranz, Á.
Proper motions
Infrared: general
Stars: kinematics and dynamics
Galaxy: center
Techniques: high angular resolution
Galaxy: structure
title_short Distance to the Brick cloud using stellar kinematics
title_full Distance to the Brick cloud using stellar kinematics
title_fullStr Distance to the Brick cloud using stellar kinematics
title_full_unstemmed Distance to the Brick cloud using stellar kinematics
title_sort Distance to the Brick cloud using stellar kinematics
dc.creator.none.fl_str_mv Martínez-Arranz, Á.
Schödel, Rainer
Nogueras-Lara, Francisco
Shahzamanian, B.
author Martínez-Arranz, Á.
author_facet Martínez-Arranz, Á.
Schödel, Rainer
Nogueras-Lara, Francisco
Shahzamanian, B.
author_role author
author2 Schödel, Rainer
Nogueras-Lara, Francisco
Shahzamanian, B.
author2_role author
author
author
dc.contributor.none.fl_str_mv Ministerio de Ciencia e Innovación (España)
European Commission
German Research Foundation
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Proper motions
Infrared: general
Stars: kinematics and dynamics
Galaxy: center
Techniques: high angular resolution
Galaxy: structure
topic Proper motions
Infrared: general
Stars: kinematics and dynamics
Galaxy: center
Techniques: high angular resolution
Galaxy: structure
description Context. The central molecular zone at the Galactic center is currently being studied intensively to understand how star formation proceeds under the extreme conditions of a galactic nucleus. Knowing the position of molecular clouds along the line of sight toward the Galactic center has had important implications in our understanding of the physics of the gas and star formation in the central molecular zone. It was recently claimed that the dense molecular cloud G0.253 + 0.016 (the Brick) has a distance of ∼7.20 kpc from the Sun. That would place it outside of the central molecular zone, and therefore of the nuclear stellar disk, but still inside the Bulge. Aims. Theoretical considerations as well as observational studies show that stars that belong to the nuclear stellar disk have different kinematics from those that belong to the inner Bulge. Therefore, we aim to constrain the distance to the Brick by studying the proper motions of the stars in the area. Methods. We used ESO HAWK-I/VLT imaging data from epochs 2015 and 2019 to compute proper motions on the Brick and in a nearby comparison field free of dark clouds. Results. The stellar population seen toward the nuclear stellar disk shows the following three kinematic components: (1) Bulge stars with an isotropic velocity dispersion of ∼3.5 micro-arc second per year; (2) eastward moving stars on the near side of the nuclear stellar disk; and (3) westward moving stars on the far side of the nuclear stellar disk. We clearly see all three components toward the comparison field. However, toward the Brick, which blocks the light from stars behind it, we can only see kinematic components (1) and (2). Conclusions. While the Brick blocks the light from stars on the far side of the nuclear stellar disk, the detection of a significant component of eastward streaming stars implies that the Brick must be located inside the nuclear stellar disk and, therefore, that it forms part of the central molecular zone. © ESO 2022.
publishDate 2022
dc.date.none.fl_str_mv 2022
2022
2022
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/272992
url http://hdl.handle.net/10261/272992
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/MICINN//SEV-2017-0709
info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PGC2018-095049-B-C21
http://dx.doi.org/10.1051/0004-6361/202243263
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
_version_ 1869403984984276992
score 15,812429

Similares en LA Referencia