Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/28401
DC Field | Value | Language |
---|---|---|
dc.contributor.author | BRAITO, Valentina | en_US |
dc.contributor.author | Reeves, J. N. | en_US |
dc.contributor.author | Matzeu, G. A. | en_US |
dc.contributor.author | SEVERGNINI, Paola | en_US |
dc.contributor.author | Ballo, L. | en_US |
dc.contributor.author | CACCIANIGA, Alessandro | en_US |
dc.contributor.author | CAMPANA, Sergio | en_US |
dc.contributor.author | CICONE, CLAUDIA | en_US |
dc.contributor.author | DELLA CECA, Roberto | en_US |
dc.contributor.author | Turner, T. J. | en_US |
dc.date.accessioned | 2020-11-17T17:37:12Z | - |
dc.date.available | 2020-11-17T17:37:12Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/28401 | - |
dc.description.abstract | We present the discovery of a new candidate for a fast disc wind, in the nearby Seyfert 2 galaxy MCG-03-58-007. This wind is discovered in a deep Suzaku observation that was performed in 2010. Overall the X-ray spectrum of MCG-03-58-007 is highly absorbed by a neutral column density of N<SUB>H</SUB> ∼10<SUP>23</SUP> cm<SUP>-2</SUP>, in agreement with the optical classification as a type 2 active galactic nucleus. In addition, this observation unveiled the presence of two deep absorption troughs at E = 7.4 ± 0.1 and 8.5 ± 0.2 keV. If associated with blueshifted Fe XXVI, these features can be explained with the presence of two highly ionized (log ξ/erg cm s<SUP>-1</SUP> ∼5.5) and high column density (N<SUB>H</SUB> ∼ 5-8 × 10<SUP>23</SUP> cm<SUP>-2</SUP>) outflowing absorbers with v<SUB>out1</SUB> ∼ -0.1c and v<SUB>out2</SUB> ∼ -0.2c. The disc wind detected during this observation is most likely launched from within a few hundreds gravitational radii from the central black and has a kinetic output that matches the prescription for significant feedback. The presence of the lower velocity component of the disc wind is independently confirmed by the analysis of a follow-up XMM-Newton and NuSTAR observation. A faster (v<SUB>out</SUB> ∼ -0.35c) component of the wind is also seen in this second observation. During this observation we also witnessed an occultation event lasting ∆t ∼ 120 ks, which we ascribe to an increase of the opacity of the disc wind (∆N<SUB>H</SUB> ∼ 1.4 × 10<SUP>24</SUP> cm<SUP>-2</SUP>). Our interpretation is that the slow zone (v<SUB>out</SUB> ∼ -0.1c) of the wind is the most stable but inhomogeneous component, while the faster zones could be associated with two different inner streamlines of the wind. | en_US |
dc.language.iso | eng | en_US |
dc.title | A new powerful and highly variable disc wind in an AGN-star-forming galaxy, the case of MCG-03-58-007 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/sty1697 | en_US |
dc.identifier.scopus | 2-s2.0-85051562079 | en_US |
dc.identifier.isi | 000441382300054 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article-abstract/479/3/3592/5046490 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 479 | en_US |
dc.relation.issue | 3 | en_US |
dc.relation.firstpage | 3592 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2018MNRAS.479.3592B | 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. Brera | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.dept | O.A. Brera | - |
crisitem.author.orcid | 0000-0002-2629-4989 | - |
crisitem.author.orcid | 0000-0001-5619-5896 | - |
crisitem.author.orcid | 0000-0002-2339-8264 | - |
crisitem.author.orcid | 0000-0001-6278-1576 | - |
crisitem.author.orcid | 0000-0003-0522-6941 | - |
crisitem.author.orcid | 0000-0001-7551-2252 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
1807.00548.pdf | 530.25 kB | Adobe PDF | View/Open | |
sty1697.pdf | PDF editoriale | 728.55 kB | Adobe PDF | View/Open |
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