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Article: Near-infrared polarimetric study of the bipolar nebula IRAS 19312+1950

TitleNear-infrared polarimetric study of the bipolar nebula IRAS 19312+1950
Authors
KeywordsPolarization
Radiative Transfer
Stars: Agb And Post-Agb
Issue Date2007
PublisherE D P Sciences. The Journal's web site is located at http://www.aanda.org
Citation
Astronomy And Astrophysics, 2007, v. 470 n. 3, p. 957-963 How to Cite?
AbstractAims. We have investigated the properties of the central star and dust in the bipolar nebula IRAS 19312+1950, which is an unusual object showing the characteristics of a supergiant, a young stellar object, and an asymptotic giant branch (AGB) star. Methods. We obtained H-band Polarimetric data of IRAS 19312+1950 using the near-infrared camera (CIAO) on the 8 m Subaru telescope. In order to investigate the physical properties of the central star and the nebula, we performed radiative transfer modeling and compared the model results with the observed spectral energy distributions (SEDs), the radial profiles of the total intensity image, and the fraction of linear polarization map. Results. The total intensity image shows a nearly spherical core with ∼3″ radius, an S-shaped arm extending ∼10″ in the northwest to southeast direction, and an extended lobe towards the southwest. The polarization map shows a centro-symmetric vector alignment in almost the entire nebula and low polarizations along the S-shaped arm. These results suggest that the nebula is accompanied by a central star, and the S-shaped arm has a physically ring-like structure. From our radiative transfer modeling, we estimated the stellar temperature, the bolometric luminosity, and the current mass-loss rate to be 2800 K, 7000 L⊙, and 5.3 × 10-6 M ⊙ yr-1, respectively. Conclusions. Taking into account previous observational results, such as the detection of SiO maser emissions and silicate absorption feature in the 10 μm spectrum, our dust radiative transfer analysis based on our near-infrared imaging polarimetry suggests that (1) the central star of IRAS 19312+1950 is likely to be an oxygen-rich, dust-enshrouded AGB star and (2) most of the circumstellar material originates from other sources (e.g. ambient dark clouds) rather than being a result of mass loss from the central star. © ESO 2007.
Persistent Identifierhttp://hdl.handle.net/10722/175077
ISSN
2014 Impact Factor: 4.378
2015 SCImago Journal Rankings: 2.446
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorMurakawa, Ken_US
dc.contributor.authorNakashima, Jen_US
dc.contributor.authorOhnaka, Ken_US
dc.contributor.authorDeguchi, Sen_US
dc.date.accessioned2012-11-26T08:49:08Z-
dc.date.available2012-11-26T08:49:08Z-
dc.date.issued2007en_US
dc.identifier.citationAstronomy And Astrophysics, 2007, v. 470 n. 3, p. 957-963en_US
dc.identifier.issn0004-6361en_US
dc.identifier.urihttp://hdl.handle.net/10722/175077-
dc.description.abstractAims. We have investigated the properties of the central star and dust in the bipolar nebula IRAS 19312+1950, which is an unusual object showing the characteristics of a supergiant, a young stellar object, and an asymptotic giant branch (AGB) star. Methods. We obtained H-band Polarimetric data of IRAS 19312+1950 using the near-infrared camera (CIAO) on the 8 m Subaru telescope. In order to investigate the physical properties of the central star and the nebula, we performed radiative transfer modeling and compared the model results with the observed spectral energy distributions (SEDs), the radial profiles of the total intensity image, and the fraction of linear polarization map. Results. The total intensity image shows a nearly spherical core with ∼3″ radius, an S-shaped arm extending ∼10″ in the northwest to southeast direction, and an extended lobe towards the southwest. The polarization map shows a centro-symmetric vector alignment in almost the entire nebula and low polarizations along the S-shaped arm. These results suggest that the nebula is accompanied by a central star, and the S-shaped arm has a physically ring-like structure. From our radiative transfer modeling, we estimated the stellar temperature, the bolometric luminosity, and the current mass-loss rate to be 2800 K, 7000 L⊙, and 5.3 × 10-6 M ⊙ yr-1, respectively. Conclusions. Taking into account previous observational results, such as the detection of SiO maser emissions and silicate absorption feature in the 10 μm spectrum, our dust radiative transfer analysis based on our near-infrared imaging polarimetry suggests that (1) the central star of IRAS 19312+1950 is likely to be an oxygen-rich, dust-enshrouded AGB star and (2) most of the circumstellar material originates from other sources (e.g. ambient dark clouds) rather than being a result of mass loss from the central star. © ESO 2007.en_US
dc.languageengen_US
dc.publisherE D P Sciences. The Journal's web site is located at http://www.aanda.orgen_US
dc.relation.ispartofAstronomy and Astrophysicsen_US
dc.subjectPolarizationen_US
dc.subjectRadiative Transferen_US
dc.subjectStars: Agb And Post-Agben_US
dc.titleNear-infrared polarimetric study of the bipolar nebula IRAS 19312+1950en_US
dc.typeArticleen_US
dc.identifier.emailNakashima, J: junichi@hku.hken_US
dc.identifier.authorityNakashima, J=rp00764en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1051/0004-6361:20066574en_US
dc.identifier.scopuseid_2-s2.0-34547702361en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-34547702361&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume470en_US
dc.identifier.issue3en_US
dc.identifier.spage957en_US
dc.identifier.epage963en_US
dc.identifier.isiWOS:000248190700014-
dc.publisher.placeFranceen_US
dc.identifier.scopusauthoridMurakawa, K=7101870698en_US
dc.identifier.scopusauthoridNakashima, J=35485342300en_US
dc.identifier.scopusauthoridOhnaka, K=7006432722en_US
dc.identifier.scopusauthoridDeguchi, S=7006314159en_US

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