FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W1991238077> ?p ?o ?g. }

• W1991238077 abstract "We have undertaken an X-ray survey of a far-infrared flux-limited sample of seven nearby edge-on starburst galaxies. The data are presented in the first paper of this series by Dahlem, Weaver, & Heckman. Here, we examine the two X-ray-brightest sample members, NGC 253 and M82, in a self-consistent manner, taking account of the spatial distribution of the X-ray emission in choosing our spectral models. Both galaxies require at least three components to model the 0.1-10.0 keV spectrum, but the modeling is by no means unique. There is significant X-ray absorption in the disk of NGC 253. When this is accounted for in spectral fits to the emission between ~0.2 and 2.0 keV, we find that multitemperature thermal plasma models with significant underlying soft X-ray absorption are more consistent with the imaging data than single-temperature models with highly subsolar abundances or models with minimal absorption and nonequilibrium thermal ionization conditions, as have been proposed by others. Our three-component models do not require absolute abundances that are inconsistent with solar values or unusually supersolar ratios of the α-burning elements with respect to Fe (as claimed previously). We conclude that with current data, the technique of measuring abundances in starburst galaxies via X-ray spectral modeling is highly uncertain. Much improved spatial/spectral resolution and increased sensitivity are required. Based on the pointlike nature of much of the X-ray emission in the PSPC hard-band image of NGC 253, we suggest that a significant fraction of the extended X-ray emission in the 3-10 keV band seen along the disk of the galaxy with ASCA and BeppoSAX (Cappi et al.) is composed of discrete sources in the disk, as opposed to purely diffuse, hot gas. If a significant amount of the hard X-ray emission were due to unresolved point sources with weak Fe Kα emission (e.g., X-ray binaries), this could explain the low Fe abundances of ~ solar derived by Cappi et al. for pure thermal models." @default.
• W1991238077 created "2016-06-24" @default.
• W1991238077 creator A5035116183 @default.
• W1991238077 creator A5060762383 @default.
• W1991238077 creator A5067012196 @default.
• W1991238077 date "2000-05-10" @default.
• W1991238077 modified "2023-09-27" @default.
• W1991238077 title "An X‐Ray Minisurvey of Nearby Edge‐on Starburst Galaxies. II. The Question of Metal Abundance" @default.
• W1991238077 cites W1515782557 @default.
• W1991238077 cites W1975349204 @default.
• W1991238077 cites W1993018461 @default.
• W1991238077 cites W1999296687 @default.
• W1991238077 cites W2004310296 @default.
• W1991238077 cites W2014881373 @default.
• W1991238077 cites W2015861399 @default.
• W1991238077 cites W2018812337 @default.
• W1991238077 cites W2033300749 @default.
• W1991238077 cites W2034485266 @default.
• W1991238077 cites W2035225065 @default.
• W1991238077 cites W2035467611 @default.
• W1991238077 cites W2039720425 @default.
• W1991238077 cites W2053852021 @default.
• W1991238077 cites W2063766803 @default.
• W1991238077 cites W2065640906 @default.
• W1991238077 cites W2067658081 @default.
• W1991238077 cites W2079516303 @default.
• W1991238077 cites W2080259687 @default.
• W1991238077 cites W2084504151 @default.
• W1991238077 cites W2149710854 @default.
• W1991238077 cites W2154219156 @default.
• W1991238077 cites W3022520032 @default.
• W1991238077 cites W3098578749 @default.
• W1991238077 cites W3100627232 @default.
• W1991238077 cites W3103295801 @default.
• W1991238077 cites W3103376294 @default.
• W1991238077 cites W3105149290 @default.
• W1991238077 cites W3106285595 @default.
• W1991238077 cites W3106305967 @default.
• W1991238077 cites W3122944995 @default.
• W1991238077 cites W4232738008 @default.
• W1991238077 doi "https://doi.org/10.1086/308786" @default.
• W1991238077 hasPublicationYear "2000" @default.
• W1991238077 type Work @default.
• W1991238077 sameAs 1991238077 @default.
• W1991238077 citedByCount "33" @default.
• W1991238077 countsByYear W19912380772012 @default.
• W1991238077 countsByYear W19912380772015 @default.
• W1991238077 countsByYear W19912380772020 @default.
• W1991238077 crossrefType "journal-article" @default.
• W1991238077 hasAuthorship W1991238077A5035116183 @default.
• W1991238077 hasAuthorship W1991238077A5060762383 @default.
• W1991238077 hasAuthorship W1991238077A5067012196 @default.
• W1991238077 hasConcept C120665830 @default.
• W1991238077 hasConcept C121332964 @default.
• W1991238077 hasConcept C125287762 @default.
• W1991238077 hasConcept C1276947 @default.
• W1991238077 hasConcept C145148216 @default.
• W1991238077 hasConcept C153294291 @default.
• W1991238077 hasConcept C191897082 @default.
• W1991238077 hasConcept C192562407 @default.
• W1991238077 hasConcept C198291218 @default.
• W1991238077 hasConcept C204530211 @default.
• W1991238077 hasConcept C44870925 @default.
• W1991238077 hasConcept C4839761 @default.
• W1991238077 hasConcept C62520636 @default.
• W1991238077 hasConcept C68709404 @default.
• W1991238077 hasConcept C82706917 @default.
• W1991238077 hasConcept C96141758 @default.
• W1991238077 hasConcept C98444146 @default.
• W1991238077 hasConceptScore W1991238077C120665830 @default.
• W1991238077 hasConceptScore W1991238077C121332964 @default.
• W1991238077 hasConceptScore W1991238077C125287762 @default.
• W1991238077 hasConceptScore W1991238077C1276947 @default.
• W1991238077 hasConceptScore W1991238077C145148216 @default.
• W1991238077 hasConceptScore W1991238077C153294291 @default.
• W1991238077 hasConceptScore W1991238077C191897082 @default.
• W1991238077 hasConceptScore W1991238077C192562407 @default.
• W1991238077 hasConceptScore W1991238077C198291218 @default.
• W1991238077 hasConceptScore W1991238077C204530211 @default.
• W1991238077 hasConceptScore W1991238077C44870925 @default.
• W1991238077 hasConceptScore W1991238077C4839761 @default.
• W1991238077 hasConceptScore W1991238077C62520636 @default.
• W1991238077 hasConceptScore W1991238077C68709404 @default.
• W1991238077 hasConceptScore W1991238077C82706917 @default.
• W1991238077 hasConceptScore W1991238077C96141758 @default.
• W1991238077 hasConceptScore W1991238077C98444146 @default.
• W1991238077 hasLocation W19912380771 @default.
• W1991238077 hasOpenAccess W1991238077 @default.
• W1991238077 hasPrimaryLocation W19912380771 @default.
• W1991238077 hasRelatedWork W1974047653 @default.
• W1991238077 hasRelatedWork W1977457396 @default.
• W1991238077 hasRelatedWork W1991238077 @default.
• W1991238077 hasRelatedWork W2004310296 @default.
• W1991238077 hasRelatedWork W2015861399 @default.
• W1991238077 hasRelatedWork W2034781494 @default.
• W1991238077 hasRelatedWork W2035467611 @default.
• W1991238077 hasRelatedWork W2044509713 @default.
• W1991238077 hasRelatedWork W2052926897 @default.
• W1991238077 hasRelatedWork W2053852021 @default.
• W1991238077 hasRelatedWork W2063361568 @default.

• next