Optical polarimetric and near-infrared photometric study of the RCW95 galactic H II region

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dc.creatorJaime Ignacio Vargas González
dc.creatorAlexandre Roman Lopes
dc.creatorFábio Pereira Santos
dc.creatorGabriel Armando Pellegatti Franco
dc.creatorJoão Francisco Coelho dos Santos Junior
dc.creatorFrancisco Ferreira de Souza Maia
dc.creatorDavid Sanmartim
dc.date.accessioned2023-09-12T11:55:56Z
dc.date.accessioned2025-09-08T23:06:31Z
dc.date.available2023-09-12T11:55:56Z
dc.date.issued2017
dc.description.sponsorshipCNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológico
dc.description.sponsorshipFAPEMIG - Fundação de Amparo à Pesquisa do Estado de Minas Gerais
dc.format.mimetypepdf
dc.identifier.doihttps://doi.org/10.1093/mnras/stx2753
dc.identifier.issn1365-2966
dc.identifier.urihttps://hdl.handle.net/1843/58583
dc.languageeng
dc.publisherUniversidade Federal de Minas Gerais
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsAcesso Aberto
dc.subjectAstronomia
dc.subjectMeio interestelar
dc.subjectEstrelas
dc.subject.otherStars
dc.subject.otherInterestellar medium
dc.subject.otherOpen clusters and associations
dc.titleOptical polarimetric and near-infrared photometric study of the RCW95 galactic H II region
dc.typeArtigo de periódico
local.citation.epage68
local.citation.spage55
local.citation.volume474
local.description.resumoWe carried out an optical polarimetric study in the direction of the RCW 95 star-forming region in order to probe the sky-projected magnetic field structure by using the distribution of linear polarization segments which seem to be well aligned with the more extended cloud component. A mean polarization angle of θ = 49∘.8 ± 7∘.7 was derived. Through the spectral dependence analysis of polarization it was possible to obtain the total-to-selective extinction ratio (RV) by fitting the Serkowski function, resulting in a mean value of RV = 2.93 ± 0.47. The foreground polarization component was estimated and is in agreement with previous studies in this direction of the Galaxy. Further, near-infrared (NIR) images from Vista Variables in the Via Láctea (VVV) survey were collected to improve the study of the stellar population associated with the H ii region. The Automated Stellar Cluster Analysis algorithm was employed to derive structural parameters for two clusters in the region, and a set of PAdova and TRieste Stellar Evolution Code (parsec) isochrones was superimposed on the decontaminated colour–magnitude diagrams to estimate an age of about 3 Myr for both clusters. Finally, from the NIR photometry study combined with spectra obtained with the Ohio State Infrared Imager and Spectrometer mounted at the Southern Astrophysics Research Telescope we derived the spectral classification of the main ionizing sources in the clusters associated with IRAS 15408−5356 and IRAS 15412−5359, both objects classified as O4V stars.
local.identifier.orcidhttps://orcid.org/0000-0002-1379-4204
local.identifier.orcidhttps://orcid.org/0000-0003-2020-2649
local.identifier.orcidhttps://orcid.org/0000-0002-2569-4032
local.identifier.orcidhttps://orcid.org/0000-0002-9238-9521
local.publisher.countryBrasil
local.publisher.departmentICX - DEPARTAMENTO DE FÍSICA
local.publisher.initialsUFMG
local.url.externahttps://academic.oup.com/mnras/article/474/1/55/4563630

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