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Please use this identifier to cite or link to this item: http://cmuir.cmu.ac.th/jspui/handle/6653943832/57891
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dc.contributor.authorW. Patwongen_US
dc.contributor.authorS. Komonjindaen_US
dc.contributor.authorN. A-Thanoen_US
dc.date.accessioned2018-09-05T03:52:40Z-
dc.date.available2018-09-05T03:52:40Z-
dc.date.issued2017-10-20en_US
dc.identifier.issn17426596en_US
dc.identifier.issn17426588en_US
dc.identifier.other2-s2.0-85034043457en_US
dc.identifier.other10.1088/1742-6596/901/1/012020en_US
dc.identifier.urihttps://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85034043457&origin=inwarden_US
dc.identifier.urihttp://cmuir.cmu.ac.th/jspui/handle/6653943832/57891-
dc.description.abstract© Published under licence by IOP Publishing Ltd. Radial velocity observations for members of the Ori OB1d association in the nebula NGC 1977 were obtained using the MRES spectrograph with the 2.4 m telescope at Thai National Observatory. Radial velocities of 2MASS J05352174-0453118, HD 37059, HD 294264 are detectable for the first time with a value of 30.02, 32.19 and 60.27 km/s, respectively. Combining the obtained radial velocities from this research with database proper motion, it was found that all observed star are moving in a different direction. This might be a result from the fact that Ori OB1d is dynamically young with active ongoing star formation. The association is small and loose. Members are less gravitationally bound and the cluster is expanding.en_US
dc.subjectPhysics and Astronomyen_US
dc.titleRadial velocity observations of OB1d association in NGC 1977en_US
dc.typeConference Proceedingen_US
article.title.sourcetitleJournal of Physics: Conference Seriesen_US
article.volume901en_US
article.stream.affiliationsChiang Mai Universityen_US
article.stream.affiliationsNational Astronomical Research Institute of Thailanden_US
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