Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/27033
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | CAPETTI, Alessandro | en_US |
dc.contributor.author | MASSARO, Francesco | en_US |
dc.contributor.author | BALDI, RANIERI DIEGO | en_US |
dc.date.accessioned | 2020-09-01T13:20:19Z | - |
dc.date.available | 2020-09-01T13:20:19Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/27033 | - |
dc.description.abstract | We built a catalog of 122 FR~II radio galaxies, called FRII{\sl{CAT}}, selected from a published sample obtained by combining observations from the NVSS, FIRST, and SDSS surveys. The catalog includes sources with redshift $\leq 0.15$, an edge-brightened radio morphology, and those with at least one of the emission peaks located at radius $r$ larger than 30 kpc from the center of the host. The radio luminosity at 1.4 GHz of the \FRII\ sources covers the range $L_{1.4} \sim 10^{39.5} - 10^{42.5}$ $\ergs$. The \FRII\ catalog has 90\% of low and 10\% of high excitation galaxies (LEGs and HEGs), respectively. The properties of these two classes are significantly different. The FRII{\sl{CAT}} LEGs are mostly luminous ($-20 \gtrsim M_r \gtrsim -24$), red early-type galaxies with black hole masses in the range $10^8 \lesssim M_{\rm BH} \lesssim 10^9 M_\odot$; they are essentially indistinguishable from the FR~Is belonging to the FRI{\sl{CAT}}. The HEG FR~IIs are associated with optically bluer and mid-IR redder hosts than the LEG FR~IIs and to galaxies and black holes that are smaller, on average, by a factor $\sim$2. FR~IIs have a factor $\sim$ 3 higher average radio luminosity than FR~Is. Nonetheless, most ($\sim 90$ \%) of the selected FR~IIs have a radio power that is lower, by as much as a factor of $\sim$100, than the transition value between FR~Is and FR~IIs found in the 3C sample. The correspondence between the morphological classification of FR~I and FR~II and the separation in radio power disappears when including sources selected at low radio flux thresholds, which is in line with previous results. In conclusion, a radio source produced by a low power jet can be edge brightened or edge darkened, and the outcome is not related to differences in the optical properties of the host galaxy. | en_US |
dc.language.iso | eng | en_US |
dc.title | FRIICAT: A FIRST catalog of FR~II radio galaxies | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/201630247 | en_US |
dc.identifier.scopus | 2-s2.0-85019083780 | en_US |
dc.identifier.isi | 000402313500081 | en_US |
dc.identifier.url | http://arxiv.org/abs/1703.03427v1 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/abs/2017/05/aa30247-16/aa30247-16.html | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 601 | en_US |
dc.relation.firstpage | A81 | en_US |
dc.relation.numberofpages | 16 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 3 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | 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 | 2017A&A...601A..81C | 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. Torino | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | IRA Bologna | - |
crisitem.author.orcid | 0000-0003-3684-4275 | - |
crisitem.author.orcid | 0000-0002-1824-0411 | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
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