The counterjet of HH 30: New light on its binary driving source

We present new [SII] images of the Herbig-Haro (HH) 30 jet and counterjet observed in 2006, 2007, and 2010 that, combined with previous data, allowed us to measure with improved accuracy the positions and proper motions of the jet and counterjet knots. Our results show that the motion of the knots i...

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Detalles Bibliográficos
Autores: Estalella, Robert, López, Rosario, Anglada Pons, Guillem Josep, Gomez, Gabriel, Riera, Angels, Carrasco-González, Carlos
Tipo de recurso: artículo
Estado:Versión aceptada para publicación
Fecha de publicación:2012
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/417245
Acceso en línea:http://hdl.handle.net/10261/417245
Access Level:acceso abierto
Palabra clave:Herbig
Haro objects
ISM: individual objects (HH 30)
ISM: jets and outflows
Stars: formation
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oai_identifier_str oai:digital.csic.es:10261/417245
network_acronym_str ES
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repository_id_str
spelling The counterjet of HH 30: New light on its binary driving sourceEstalella, RobertLópez, RosarioAnglada Pons, Guillem JosepGomez, GabrielRiera, AngelsCarrasco-González, CarlosHerbigHaro objectsISM: individual objects (HH 30)ISM: jets and outflowsStars: formationWe present new [SII] images of the Herbig-Haro (HH) 30 jet and counterjet observed in 2006, 2007, and 2010 that, combined with previous data, allowed us to measure with improved accuracy the positions and proper motions of the jet and counterjet knots. Our results show that the motion of the knots is essentially ballistic, with the exception of the farthest knots, which trace the large-scale "C"-shape bending of the jet. The observed bending of the jet can be produced by a relative motion of the HH 30 star with respect to its surrounding environment, caused either by a possible proper motion of the HH 30 star, or by the entrainment of environment gas by the red lobe of the nearby L1551-IRS5 outflow. Alternatively, the bending can be produced by the stellar wind from a nearby classical T Tauri star, identified in the Two Micron All Sky Survey catalog as J04314418+181047. The proper motion velocities of the knots of the counterjet show more variations than those of the jet. In particular, we identify two knots of the counterjet that have the same kinematic age but whose velocities differ by almost a factor of two. Thus, it appears from our observations that counterjet knots launched simultaneously can be ejected with very different velocities. We confirm that the observed wiggling of the jet and counterjet arises from the orbital motion of the jet source in a binary system. Precession, if present at all, is of secondary importance in shaping the jet. We derive an orbital period of τ o = 114 ± 2yr and a mass function of mμ 3 c = 0.014 ± 0.006 M ⊙. For a mass of the system of m = 0.45 ± 0.04 M ⊙ (the value inferred from observations of the CO kinematics of the disk), we obtain a mass of m j = 0.31 ± 0.04 M ⊙ for the jet source, a mass of m c = 0.14 ± 0.03 M ⊙ for the companion, and a binary separation of a = 18.0 ± 0.6AU. This binary separation coincides with the value required to account for the size of the inner hole observed in the disk, which has been attributed to tidal truncation in a binary system. © © 2012. The American Astronomical Society. All rights reserved.G. A., R. E., R. L., A. R., and C. C.-G. are partially supported by Spanish MCI grants AYA2008-06189-C03 and AYA2011- 30228-C03, and FEDER funds. We acknowledge Pau Estalella for his helpful comments on the use of the Halton sequence. The data presented here were taken at the 2.5 m Isaac Newton Telescope, the 4.2 m William Herschel Telescope, and the 2.6 m Nordic Optical Telescope at the Observatorio del Roque de los Muchachos of the Instituto de Astrof´ısica de Canarias.Peer reviewedIOP PublishingMinisterio de Ciencia e Innovación (España)European CommissionConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202620262012info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Postprintinfo:eu-repo/semantics/acceptedVersionhttp://hdl.handle.net/10261/417245reponame: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//AYA2008-06189-C03-03info:eu-repo/grantAgreement/MICINN//AYA2011-30228-C03http://dx.doi.org/10.1088/0004-6256/144/2/61Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/4172452026-05-22T06:33:51Z
dc.title.none.fl_str_mv The counterjet of HH 30: New light on its binary driving source
title The counterjet of HH 30: New light on its binary driving source
spellingShingle The counterjet of HH 30: New light on its binary driving source
Estalella, Robert
Herbig
Haro objects
ISM: individual objects (HH 30)
ISM: jets and outflows
Stars: formation
title_short The counterjet of HH 30: New light on its binary driving source
title_full The counterjet of HH 30: New light on its binary driving source
title_fullStr The counterjet of HH 30: New light on its binary driving source
title_full_unstemmed The counterjet of HH 30: New light on its binary driving source
title_sort The counterjet of HH 30: New light on its binary driving source
dc.creator.none.fl_str_mv Estalella, Robert
López, Rosario
Anglada Pons, Guillem Josep
Gomez, Gabriel
Riera, Angels
Carrasco-González, Carlos
author Estalella, Robert
author_facet Estalella, Robert
López, Rosario
Anglada Pons, Guillem Josep
Gomez, Gabriel
Riera, Angels
Carrasco-González, Carlos
author_role author
author2 López, Rosario
Anglada Pons, Guillem Josep
Gomez, Gabriel
Riera, Angels
Carrasco-González, Carlos
author2_role author
author
author
author
author
dc.contributor.none.fl_str_mv Ministerio de Ciencia e Innovación (España)
European Commission
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Herbig
Haro objects
ISM: individual objects (HH 30)
ISM: jets and outflows
Stars: formation
topic Herbig
Haro objects
ISM: individual objects (HH 30)
ISM: jets and outflows
Stars: formation
description We present new [SII] images of the Herbig-Haro (HH) 30 jet and counterjet observed in 2006, 2007, and 2010 that, combined with previous data, allowed us to measure with improved accuracy the positions and proper motions of the jet and counterjet knots. Our results show that the motion of the knots is essentially ballistic, with the exception of the farthest knots, which trace the large-scale "C"-shape bending of the jet. The observed bending of the jet can be produced by a relative motion of the HH 30 star with respect to its surrounding environment, caused either by a possible proper motion of the HH 30 star, or by the entrainment of environment gas by the red lobe of the nearby L1551-IRS5 outflow. Alternatively, the bending can be produced by the stellar wind from a nearby classical T Tauri star, identified in the Two Micron All Sky Survey catalog as J04314418+181047. The proper motion velocities of the knots of the counterjet show more variations than those of the jet. In particular, we identify two knots of the counterjet that have the same kinematic age but whose velocities differ by almost a factor of two. Thus, it appears from our observations that counterjet knots launched simultaneously can be ejected with very different velocities. We confirm that the observed wiggling of the jet and counterjet arises from the orbital motion of the jet source in a binary system. Precession, if present at all, is of secondary importance in shaping the jet. We derive an orbital period of τ o = 114 ± 2yr and a mass function of mμ 3 c = 0.014 ± 0.006 M ⊙. For a mass of the system of m = 0.45 ± 0.04 M ⊙ (the value inferred from observations of the CO kinematics of the disk), we obtain a mass of m j = 0.31 ± 0.04 M ⊙ for the jet source, a mass of m c = 0.14 ± 0.03 M ⊙ for the companion, and a binary separation of a = 18.0 ± 0.6AU. This binary separation coincides with the value required to account for the size of the inner hole observed in the disk, which has been attributed to tidal truncation in a binary system. © © 2012. The American Astronomical Society. All rights reserved.
publishDate 2012
dc.date.none.fl_str_mv 2012
2026
2026
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Postprint
info:eu-repo/semantics/acceptedVersion
format article
status_str acceptedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/417245
url http://hdl.handle.net/10261/417245
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//AYA2008-06189-C03-03
info:eu-repo/grantAgreement/MICINN//AYA2011-30228-C03
http://dx.doi.org/10.1088/0004-6256/144/2/61
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
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
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score 15.81155

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