Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/28747
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Agliozzo, C. | en_US |
dc.contributor.author | Mehner, A. | en_US |
dc.contributor.author | Phillips, N. M. | en_US |
dc.contributor.author | LETO, PAOLO | en_US |
dc.contributor.author | Groh, J. H. | en_US |
dc.contributor.author | Noriega-Crespo, A. | en_US |
dc.contributor.author | BUEMI, CARLA SIMONA | en_US |
dc.contributor.author | Cavallaro, Francesco | en_US |
dc.contributor.author | Cerrigone, L. | en_US |
dc.contributor.author | INGALLINERA, Adriano | en_US |
dc.contributor.author | Paladini, R. | en_US |
dc.contributor.author | Pignata, G. | en_US |
dc.contributor.author | TRIGILIO, CORRADO | en_US |
dc.contributor.author | UMANA, Grazia Maria Gloria | en_US |
dc.date.accessioned | 2020-12-09T12:15:38Z | - |
dc.date.available | 2020-12-09T12:15:38Z | - |
dc.date.issued | 2019 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/28747 | - |
dc.description.abstract | The luminous blue variable (LBV) RMC 143 is located in the outskirts of the 30 Doradus complex, a region rich with interstellar material and hot luminous stars. We report the 3σ sub-millimetre detection of its circumstellar nebula with ALMA. The observed morphology in the sub-millimetre is different than previously observed with HST and ATCA in the optical and centimetre wavelength regimes. The spectral energy distribution (SED) of RMC 143 suggests that two emission mechanisms contribute to the sub-mm emission: optically thin bremsstrahlung and dust. Both the extinction map and the SED are consistent with a dusty massive nebula with a dust mass of 0.055 ± 0.018 M<SUB>☉</SUB> (assuming κ<SUB>850</SUB> = 1.7 cm<SUP>2</SUP> g<SUP>-1</SUP>). To date, RMC 143 has the most dusty LBV nebula observed in the Magellanic Clouds. We have also re-examined the LBV classification of RMC 143 based on VLT/X-shooter spectra obtained in 2015/16 and a review of the publication record. The radiative transfer code CMFGEN is used to derive its fundamental stellar parameters. We find an effective temperature of ∼8500 K, luminosity of log(L/L<SUB>☉</SUB>) = 5.32, and a relatively high mass-loss rate of 1.0 × 10<SUP>-5</SUP> M<SUB>☉</SUB> yr<SUP>-1</SUP>. The luminosity is much lower than previously thought, which implies that the current stellar mass of ∼8 M<SUB>☉</SUB> is comparable to its nebular mass of ∼5.5 M<SUB>☉</SUB> (from an assumed gas-to-dust ratio of 100), suggesting that the star has lost a large fraction of its initial mass in past LBV eruptions or binary interactions. While the star may have been hotter in the past, it is currently not hot enough to ionize its circumstellar nebula. We propose that the nebula is ionized externally by the hot stars in the 30 Doradus star-forming region. <P />The ALMA and ATCA maps, and Tables 1 and 4, are only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr/">http://cdsarc.u-strasbg.fr</A> (ftp://130.79.128.5) or via <A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/626/A126">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/626/A126</A>Phase 3 X-shooter spectra are available in the ESO data archive. | en_US |
dc.language.iso | eng | en_US |
dc.title | A massive nebula around the luminous blue variable star RMC 143 revealed by ALMA | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/201935239 | en_US |
dc.identifier.scopus | 2-s2.0-85068330381 | en_US |
dc.identifier.isi | 000472594200003 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/full_html/2019/06/aa35239-19/aa35239-19.html | en_US |
dc.identifier.url | https://arxiv.org/pdf/1904.08013.pdf | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 626 | en_US |
dc.relation.firstpage | A126 | en_US |
dc.relation.numberofpages | 13 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 14 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | USA | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | ASTRONOMY & ASTROPHYSICS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2019A&A...626A.126A | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_6 Stars and stellar systems | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.orcid | 0000-0003-4864-2806 | - |
crisitem.author.orcid | 0000-0002-7288-4613 | - |
crisitem.author.orcid | 0000-0003-1856-6806 | - |
crisitem.author.orcid | 0000-0002-3137-473X | - |
crisitem.author.orcid | 0000-0002-1216-7831 | - |
crisitem.author.orcid | 0000-0002-6972-8388 | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
aa35239-19.pdf | PDF editoriale | 4.19 MB | Adobe PDF | View/Open |
1904.08013.pdf | arXiv | 4.16 MB | Adobe PDF | View/Open |
Page view(s)
56
checked on Apr 26, 2024
Download(s)
66
checked on Apr 26, 2024
Google ScholarTM
Check
Altmetric
Altmetric
Items in DSpace are published in Open Access, unless otherwise indicated.