Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/31706
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Vito, F. | en_US |
dc.contributor.author | Brandt, W. N. | en_US |
dc.contributor.author | Ricci, F. | en_US |
dc.contributor.author | Congiu, E. | en_US |
dc.contributor.author | Connor, T. | en_US |
dc.contributor.author | Bañados, E. | en_US |
dc.contributor.author | Bauer, F. E. | en_US |
dc.contributor.author | GILLI, Roberto | en_US |
dc.contributor.author | Luo, B. | en_US |
dc.contributor.author | Mazzucchelli, C. | en_US |
dc.contributor.author | MIGNOLI, Marco | en_US |
dc.contributor.author | Shemmer, O. | en_US |
dc.contributor.author | Vignali, C. | en_US |
dc.contributor.author | CALURA, Francesco | en_US |
dc.contributor.author | COMASTRI, Andrea | en_US |
dc.contributor.author | DECARLI, ROBERTO | en_US |
dc.contributor.author | Gallerani, S. | en_US |
dc.contributor.author | Nanni, R. | en_US |
dc.contributor.author | Brusa, M. | en_US |
dc.contributor.author | Cappelluti, N. | en_US |
dc.contributor.author | Civano, F. | en_US |
dc.contributor.author | Zamorani, G. | en_US |
dc.date.accessioned | 2022-03-18T13:34:23Z | - |
dc.date.available | 2022-03-18T13:34:23Z | - |
dc.date.issued | 2021 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/31706 | - |
dc.description.abstract | Context. The discovery of hundreds of quasi-stellar objects (QSOs) in the first gigayear of the Universe powered by already grown supermassive black holes (SMBHs) challenges our knowledge of SMBH formation. In particular, investigations of z > 6 QSOs that present notable properties can provide unique information on the physics of fast SMBH growth in the early Universe. Aims. We present the results of follow-up observations of the z = 6.515 radio-quiet QSO PSO167-13, which is interacting with a close companion galaxy. The PSO167-13 system has recently been proposed to host the first heavily obscured X-ray source at high redshift. The goals of these new observations are to confirm the existence of the X-ray source and to investigate the rest-frame UV properties of the QSO. Methods. We observed the PSO167-13 system with Chandra/ACIS-S (177 ks) and obtained new spectroscopic observations (7.2 h) with Magellan/FIRE. Results. No significant X-ray emission is detected from the PSO167-13 system, suggesting that the obscured X-ray source previously tentatively detected was either due to a strong background fluctuation or is highly variable. The upper limit (90% confidence level) on the X-ray emission of PSO167-13 (L2-10 keV < 8.3 × 1043 erg s-1) is the lowest available for a z > 6 QSO. The ratio between the X-ray and UV luminosity of αox < -1.95 makes PSO167-13 a strong outlier from the αox - LUV and LX - Lbol relations. In particular, its X-ray emission is more than six times weaker than the expectation based on its UV luminosity. The new Magellan/FIRE spectrum of PSO167-13 is strongly affected by unfavorable sky conditions, but the tentatively detected C IV and Mg II emission lines appear strongly blueshifted. Conclusions. The most plausible explanations for the X-ray weakness of PSO167-13 are intrinsic weakness or small-scale absorption by Compton-thick material. The possible strong blueshift of its emission lines hints at the presence of nuclear winds, which could be related to its X-ray weakness. | en_US |
dc.language.iso | eng | en_US |
dc.title | Chandra and Magellan /FIRE follow-up observations of PSO167-13: An X-ray weak QSO at z = 6.515 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/202140399 | en_US |
dc.identifier.scopus | 2-s2.0-85107079327 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/abs/2021/05/aa40399-21/aa40399-21.html | en_US |
dc.identifier.url | https://api.elsevier.com/content/abstract/scopus_id/85107079327 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 649 | en_US |
dc.relation.firstpage | A133 | en_US |
dc.type.referee | REF_1 | 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.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 | 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 | OAS Bologna | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.dept | OAS Bologna | - |
crisitem.author.orcid | 0000-0001-8121-6177 | - |
crisitem.author.orcid | 0000-0002-9087-2835 | - |
crisitem.author.orcid | 0000-0002-6175-0871 | - |
crisitem.author.orcid | 0000-0003-3451-9970 | - |
crisitem.author.orcid | 0000-0002-2662-8803 | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
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Vito2021_aa40399-21.pdf | Pdf editoriale | 646.88 kB | Adobe PDF | View/Open |
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