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dc.contributor.authorCoutens, Aen
dc.contributor.authorLiu, HBen
dc.contributor.authorJiménez-Serra, Ien
dc.contributor.authorBourke, TLen
dc.contributor.authorForbrich, Jen
dc.contributor.authorHoare, Men
dc.contributor.authorLoinard, Len
dc.contributor.authorTesti, Len
dc.contributor.authorAudard, Men
dc.contributor.authorCaselli, Pen
dc.contributor.authorChacón-Tanarro, Aen
dc.contributor.authorCodella, Cen
dc.contributor.authorFrancesco, J Dien
dc.contributor.authorFontani, Fen
dc.contributor.authorHogerheijde, Men
dc.contributor.authorJohansen, Aen
dc.contributor.authorJohnstone, Den
dc.contributor.authorMaddison, Sen
dc.contributor.authorPanić, Oen
dc.contributor.authorPérez, LMen
dc.contributor.authorPodio, Len
dc.contributor.authorPunanova, Aen
dc.contributor.authorRawlings, JMCen
dc.contributor.authorSemenov, Den
dc.contributor.authorTazzari, Marcoen
dc.contributor.authorTobin, JJen
dc.contributor.authorWiel, MHD van deren
dc.contributor.authorLangevelde, HJ vanen
dc.contributor.authorVlemmings, Wen
dc.contributor.authorWalsh, Cen
dc.contributor.authorWilner, Den
dc.date.accessioned2019-10-11T23:30:25Z
dc.date.available2019-10-11T23:30:25Z
dc.date.issued2019-11en
dc.identifier.issn0004-6361
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/297764
dc.description.abstractObservations of young stellar objects (YSOs) in centimeter bands can probe the continuum emission from growing dust grains, ionized winds, and magnetospheric activity that are intimately connected to the evolution of protoplanetary disks and the formation of planets. We carried out sensitive continuum observations toward the Ophiuchus A star-forming region, using the Karl G. Jansky Very Large Array (VLA) at 10 GHz over a field-of-view of 6′ and with a spatial resolution of θmaj ×θmin ~ 0.′′4 × 0.′′2. We achieved a 5 μJy beam−1 rms noise level at the center of our mosaic field of view. Among the 18 sources we detected, 16 were YSOs (three Class 0, five Class I, six Class II, and two Class III) and two were extragalactic candidates. We find that thermal dust emission generally contributed less than 30% of the emission at 10 GHz. The radio emission is dominated by other types of emission, such as gyro-synchrotron radiation from active magnetospheres, free–free emission from thermal jets, free–free emission from the outflowing photoevaporated disk material, and synchrotron emission from accelerated cosmic-rays in jet or protostellar surface shocks. These different types of emission could not be clearly disentangled. Our non-detections for Class II/III disks suggest that extreme UV-driven photoevaporation is insufficient to explain disk dispersal, assuming that the contribution of UV photoevaporating stellar winds to radio flux does not evolve over time. The sensitivity of our data cannot exclude photoevaporation due to the role of X-ray photons as an efficient mechanism for disk dispersal. Deeper surveys using the Square Kilometre Array (SKA) will have the capacity to provide significant constraints to disk photoevaporation.
dc.description.sponsorshipERC STFC Horizon 2020
dc.publisherEDP Sciences
dc.rightsAttribution 4.0 International
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/
dc.subjectastro-ph.SRen
dc.subjectastro-ph.SRen
dc.subjectastro-ph.GAen
dc.titleVLA cm-wave survey of young stellar objects in the Oph A cluster: constraining extreme UV- and X-ray-driven disk photo-evaporation -- A pathfinder for Square Kilometre Array studiesen
dc.typeArticle
prism.numberA58en
prism.publicationDate2019en
prism.publicationNameAstronomy and Astrophysicsen
prism.volume631en
dc.identifier.doi10.17863/CAM.44817
dcterms.dateAccepted2019-09-04en
rioxxterms.versionofrecord10.1051/0004-6361/201935340en
rioxxterms.versionVoR
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserveden
rioxxterms.licenseref.startdate2019-11en
dc.contributor.orcidTazzari, Marco [0000-0003-3590-5814]
dc.identifier.eissn1432-0746
rioxxterms.typeJournal Article/Reviewen
pubs.funder-project-idEuropean Research Council (341137)
cam.issuedOnline2019-10-21en
dc.identifier.urlhttp://dx.doi.org/10.1051/0004-6361/201935340en
rioxxterms.freetoread.startdate2100-01-01


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Attribution 4.0 International
Except where otherwise noted, this item's licence is described as Attribution 4.0 International