Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/24204
DC Field | Value | Language |
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dc.contributor.author | Bensch, K. | en_US |
dc.contributor.author | del Olmo, A. | en_US |
dc.contributor.author | Sulentic, J. | en_US |
dc.contributor.author | Perea, J. | en_US |
dc.contributor.author | MARZIANI, Paola | en_US |
dc.date.accessioned | 2020-04-23T12:42:27Z | - |
dc.date.available | 2020-04-23T12:42:27Z | - |
dc.date.issued | 2015 | en_US |
dc.identifier.issn | 0250-6335 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/24204 | - |
dc.description.abstract | We present a preliminary analysis of X-ray data of quasars in the context of the 4D eigenvector 1 parameter space (Sulentic et al. 2000a, b). 4DE1 serves as a surrogate H-R diagram for representing empirical diversity among quasars and identifying the physical drivers of the diversity. The soft X-ray spectral index (Γ<SUB>soft</SUB>) was adopted as one of the key 4DE1 that correlates contrasting extremes in Type 1 properties. 4DE1 motivated the hypothesis of two quasar populations (A and B) divided by L/ L <SUB>EDD</SUB>≈0.2. Pop. A is a largely radio-quiet population with FWHM H β<4000 km/s and often showing a soft X-ray excess. Pop. B is a mix of radio-quiet and a majority of RL quasars shows only a hard X-ray power-law SED. The X-ray separation was based upon earlier ROSAT and ASCA data but we now confirm this dichotomy with large samples of X-ray spectra obtained with XMM-Newton and SWIFT. One popular idea connects the soft excess in Pop. A quasars as a signature of thermal emission from a hot accretion disk in sources radiating close to the Eddington limit. <P /> | en_US |
dc.language.iso | eng | en_US |
dc.title | Measures of the Soft X-ray Excess as an Eigenvector 1 Parameter for Active Galactic Nuclei | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1007/s12036-015-9355-8 | en_US |
dc.identifier.scopus | 2-s2.0-84956844290 | en_US |
dc.identifier.isi | 000368698700006 | en_US |
dc.identifier.url | https://link.springer.com/article/10.1007%2Fs12036-015-9355-8 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 36 | en_US |
dc.relation.issue | 4 | en_US |
dc.relation.firstpage | 467 | en_US |
dc.type.referee | REF_1 | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | JOURNAL OF ASTROPHYSICS AND ASTRONOMY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2015JApA...36..467B | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegherò 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. Padova | - |
crisitem.author.orcid | 0000-0002-6058-4912 | - |
crisitem.journal.journalissn | 0250-6335 | - |
crisitem.journal.ance | E090630 | - |
Appears in Collections: | 1.01 Articoli in rivista |
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File | Description | Size | Format | |
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bensch2015.pdf | 543.46 kB | Adobe PDF | View/Open |
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