Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/32657
DC Field | Value | Language |
---|---|---|
dc.contributor.author | DELLA VALLE, Massimo | en_US |
dc.contributor.author | Panagia, Nino | en_US |
dc.date.accessioned | 2022-09-28T08:56:51Z | - |
dc.date.available | 2022-09-28T08:56:51Z | - |
dc.date.issued | 1992 | en_US |
dc.identifier.issn | 0004-6256 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/32657 | - |
dc.description.abstract | We have collected and analyzed the color excess data for the best photometrically studied type Ia supernovae (SNIa) which occurred in late type galaxies. From these data we find a ratio of the B band to selective extinction in the parent galaxies of R_B_ = A_B_/E(B-V)=3.35+/-0.25 (1σ). This indicates that the extinction curves in latetype galaxies have similar properties to that of our Galaxy. We obtain a new calibration for the absolute magnitude at maximum of SNIa in late type galaxies <M_B_> = - 19.24+/-0.18(1σ) + 5 log(H_0_/75), which is marginally brighter than the recent determinations for type Ia supernovae observed in elliptical (dust-free) galaxies, and appears to confirm the potential of SNIa as standard candles for distance determinations. Studying the distribution of the extinction in the parent galaxies we find an average half-width of selective extinction of {DELTA}[E(B-V)]=0.13+/-0.04 and a dispersion of extinction to SNe of σ[E(B-V)]=0.15+/-0.01. Allowing for extinction biases, the total width of the dust disk turns out to be 2τ_0_= 1.28+/-0.23 mag. These results imply that SNIa have a considerably broader distribution than the dust disk and confirm that they are older than old disk population objects, i.e., age > 1-2 billion years. Also, we conclude that total extinction thickness of late type galaxies is very similar to that of the Milky Way. | en_US |
dc.language.iso | eng | en_US |
dc.title | Type IA Supernovae in Late Type Galaxies: Reddening Correction, Scale Height, and Absolute Maximum Magnitude | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1086/116265 | en_US |
dc.identifier.scopus | 2-s2.0-0013003066 | en_US |
dc.identifier.url | https://api.elsevier.com/content/abstract/scopus_id/0013003066 | en_US |
dc.identifier.url | https://ui.adsabs.harvard.edu/abs/1992AJ....104..696D/abstract | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 104 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 696 | en_US |
dc.relation.lastpage | 703 | en_US |
dc.type.referee | REF_1 | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTRONOMICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 1992AJ....104..696D | 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.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0004-6256 | - |
crisitem.journal.ance | E016224 | - |
crisitem.author.dept | O.A. Capodimonte | - |
crisitem.author.orcid | 0000-0003-3142-5020 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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document.pdf | PDF editoriale | 843.87 kB | Adobe PDF | View/Open |
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