Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/24894
DC Field | Value | Language |
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dc.contributor.author | Koss, Michael J. | en_US |
dc.contributor.author | Assef, R. | en_US |
dc.contributor.author | Baloković, M. | en_US |
dc.contributor.author | Stern, D. | en_US |
dc.contributor.author | Gandhi, P. | en_US |
dc.contributor.author | Lamperti, I. | en_US |
dc.contributor.author | Alexander, D. M. | en_US |
dc.contributor.author | Ballantyne, D. R. | en_US |
dc.contributor.author | Bauer, F. E. | en_US |
dc.contributor.author | Berney, S. | en_US |
dc.contributor.author | Brandt, W. N. | en_US |
dc.contributor.author | COMASTRI, Andrea | en_US |
dc.contributor.author | Gehrels, N. | en_US |
dc.contributor.author | Harrison, F. A. | en_US |
dc.contributor.author | Lansbury, G. | en_US |
dc.contributor.author | Markwardt, C. | en_US |
dc.contributor.author | Ricci, C. | en_US |
dc.contributor.author | Rivers, E. | en_US |
dc.contributor.author | Schawinski, K. | en_US |
dc.contributor.author | Trakhtenbrot, B. | en_US |
dc.contributor.author | Treister, E. | en_US |
dc.contributor.author | Urry, C. Megan | en_US |
dc.date.accessioned | 2020-05-15T16:05:11Z | - |
dc.date.available | 2020-05-15T16:05:11Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/24894 | - |
dc.description.abstract | We present a new metric that uses the spectral curvature (SC) above 10 keV to identify Compton-thick active galactic nuclei (AGNs) in low-quality Swift/Burst Alert Telescope (BAT) X-ray data. Using NuSTAR, we observe nine high SC-selected AGNs. We find that high-sensitivity spectra show that the majority are Compton-thick (78% or 7/9) and the remaining two are nearly Compton-thick (N <SUB>H</SUB> ≃ (5-8) × 10<SUP>23</SUP> cm<SUP>-2</SUP> ). We find that the SC<SUB> BAT </SUB> and SC<SUB> NuSTAR </SUB> measurements are consistent, suggesting that this technique can be applied to future telescopes. We tested the SC method on well-known Compton-thick AGNs and found that it is much more effective than broadband ratios (e.g., 100% using SC versus 20% using 8-24 keV/3-8 keV). Our results suggest that using the >10 keV emission may be the only way to identify this population since only two sources show Compton-thick levels of excess in the Balmer decrement corrected [O III] to observed X-ray emission ratio ({F}<SUB>[{{O</SUB>}{{III}}]}/{F}<SUB>2{--</SUB>10 {keV}}<SUP>{obs</SUP>}\gt 1) and WISE colors do not identify most of them as AGNs. Based on this small sample, we find that a higher fraction of these AGNs are in the final merger stage (<10 kpc) than typical BAT AGNs. Additionally, these nine obscured AGNs have, on average, ≈4× higher accretion rates than other BAT-detected AGNs (< {λ }<SUB>{Edd</SUB>}> \=\0.068+/- 0.023 compared to < {λ }<SUB>{Edd</SUB>}> \=\0.016+/- 0.004). The robustness of SC at identifying Compton-thick AGNs implies that a higher fraction of nearby AGNs may be Compton-thick (≈22%) and the sum of black hole growth in Compton-thick AGNs (Eddington ratio times population percentage) is nearly as large as mildly obscured and unobscured AGNs. | en_US |
dc.language.iso | eng | en_US |
dc.title | A New Population of Compton-thick AGNs Identified Using the Spectral Curvature above 10 keV | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/0004-637X/825/2/85 | en_US |
dc.identifier.scopus | 2-s2.0-84978492689 | en_US |
dc.identifier.isi | 000381940800003 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/0004-637X/825/2/85 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/0004-637X/825/2/85/pdf | en_US |
dc.relation.medium | ELETTRONICO | en_US |
dc.relation.volume | 825 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 85 | en_US |
dc.relation.lastpage | 102 | en_US |
dc.relation.numberofpages | 18 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 22 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2016ApJ...825...85K | 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 | 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.orcid | 0000-0003-3451-9970 | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
1604.07825.pdf | postprint | 3.63 MB | Adobe PDF | View/Open |
Koss_2016_ApJ_825_85.pdf | pdf editoriale | 3.93 MB | Adobe PDF | View/Open |
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