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Article: High Angular Resolution ALMA Images of Dust and Molecules in the SN 1987A Ejecta

TitleHigh Angular Resolution ALMA Images of Dust and Molecules in the SN 1987A Ejecta
Authors
KeywordsLARGE-MAGELLANIC-CLOUD
OPTICAL-PROPERTIES
SUPERNOVA 1987A
MASSIVE STARS
INFRARED PROPERTIES
Issue Date2019
PublisherAmerican Astronomical Society, co-published with Institute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/
Citation
The Astrophysical Journal, 2019, v. 886 n. 1, p. article no. 51 How to Cite?
AbstractWe present high angular resolution (similar to 80 mas) ALMA continuum images of the SN.1987A system, together with CO J = 2 -> 1, J = 6 -> 5, and SiO J = 5 -> 4 to J = 7 -> 6 images, which clearly resolve the ejecta (dust continuum and molecules) and ring (synchrotron continuum) components. Dust in the ejecta is asymmetric and clumpy, and overall the dust fills the spatial void seen in H alpha images, filling that region with material from heavier elements. The dust clumps generally fill the space where CO J = 6 -> 5 is fainter, tentatively indicating that these dust clumps and CO are locationally and chemically linked. In these regions, carbonaceous dust grains might have formed after dissociation of CO. The dust grains would have cooled by radiation, and subsequent collisions of grains with gas would also cool the gas, suppressing the CO J = 6 -> 5 intensity. The data show a dust peak spatially coincident with the molecular hole seen in previous ALMA CO J = 2 -> 1 and SiO J = 5 -> 4 images. That dust peak, combined with CO and SiO line spectra, suggests that the dust and gas could be at higher temperatures than the surrounding material, though higher density cannot be totally excluded. One of the possibilities is that a compact source provides additional heat at that location. Fits to the far-infrared-millimeter spectral energy distribution give ejecta dust temperatures of 18-23 K. We revise the ejecta dust mass to M-dust = 0.2-0.4 M-circle dot for carbon or silicate grains, or a maximum of <0.7 M-circle dot for a mixture of grain species, using the predicted nucleosynthesis yields as an upper limit.
Persistent Identifierhttp://hdl.handle.net/10722/280003
ISSN
2017 Impact Factor: 5.551
2015 SCImago Journal Rankings: 3.266
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorCigan, P-
dc.contributor.authorMatsuura, M-
dc.contributor.authorGomez, HL-
dc.contributor.authorIndebetouw, R-
dc.contributor.authorAbellán, F-
dc.contributor.authorGabler, M-
dc.contributor.authorRichards, A-
dc.contributor.authorAlp, D-
dc.contributor.authorDavis, TA-
dc.contributor.authorJanka, HT-
dc.contributor.authorSpyromilio, J-
dc.contributor.authorBarlow, MJ-
dc.contributor.authorBurrows, D-
dc.contributor.authorDwek, E-
dc.contributor.authorFransson, C-
dc.contributor.authorGaensler, B-
dc.contributor.authorLarsson, J-
dc.contributor.authorBouchet, P-
dc.contributor.authorLundqvist, P-
dc.contributor.authorMarcaide, JM-
dc.contributor.authorNg, C-Y-
dc.contributor.authorPark, S-
dc.contributor.authorRoche, P-
dc.contributor.authorvan Loon, JT-
dc.contributor.authorWheeler, JC-
dc.contributor.authorZanardo, G-
dc.date.accessioned2019-12-23T08:24:50Z-
dc.date.available2019-12-23T08:24:50Z-
dc.date.issued2019-
dc.identifier.citationThe Astrophysical Journal, 2019, v. 886 n. 1, p. article no. 51-
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/10722/280003-
dc.description.abstractWe present high angular resolution (similar to 80 mas) ALMA continuum images of the SN.1987A system, together with CO J = 2 -> 1, J = 6 -> 5, and SiO J = 5 -> 4 to J = 7 -> 6 images, which clearly resolve the ejecta (dust continuum and molecules) and ring (synchrotron continuum) components. Dust in the ejecta is asymmetric and clumpy, and overall the dust fills the spatial void seen in H alpha images, filling that region with material from heavier elements. The dust clumps generally fill the space where CO J = 6 -> 5 is fainter, tentatively indicating that these dust clumps and CO are locationally and chemically linked. In these regions, carbonaceous dust grains might have formed after dissociation of CO. The dust grains would have cooled by radiation, and subsequent collisions of grains with gas would also cool the gas, suppressing the CO J = 6 -> 5 intensity. The data show a dust peak spatially coincident with the molecular hole seen in previous ALMA CO J = 2 -> 1 and SiO J = 5 -> 4 images. That dust peak, combined with CO and SiO line spectra, suggests that the dust and gas could be at higher temperatures than the surrounding material, though higher density cannot be totally excluded. One of the possibilities is that a compact source provides additional heat at that location. Fits to the far-infrared-millimeter spectral energy distribution give ejecta dust temperatures of 18-23 K. We revise the ejecta dust mass to M-dust = 0.2-0.4 M-circle dot for carbon or silicate grains, or a maximum of <0.7 M-circle dot for a mixture of grain species, using the predicted nucleosynthesis yields as an upper limit.-
dc.languageeng-
dc.publisherAmerican Astronomical Society, co-published with Institute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/-
dc.relation.ispartofThe Astrophysical Journal-
dc.rightsThe Astrophysical Journal. Copyright © American Astronomical Society, co-published with Institute of Physics Publishing, Inc.-
dc.subjectLARGE-MAGELLANIC-CLOUD-
dc.subjectOPTICAL-PROPERTIES-
dc.subjectSUPERNOVA 1987A-
dc.subjectMASSIVE STARS-
dc.subjectINFRARED PROPERTIES-
dc.titleHigh Angular Resolution ALMA Images of Dust and Molecules in the SN 1987A Ejecta-
dc.typeArticle-
dc.identifier.emailNg, C-Y: ncy@astro.physics.hku.hk-
dc.identifier.authorityNg, C-Y=rp01706-
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.3847/1538-4357/ab4b46-
dc.identifier.hkuros308759-
dc.identifier.volume886-
dc.identifier.issue1-
dc.identifier.spagearticle no. 51-
dc.identifier.epagearticle no. 51-
dc.identifier.isiWOS:000499366000001-
dc.publisher.placeUnited States-

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