BASS. XLVIII. [Ne V] λ3427 Emission in Powerful Nearby Active Galactic Nuclei
We investigate the high-ionization, narrow [Ne V ] λ 3427 line emission in a sample of over 340 ultrahard X-ray (14–195 keV) selected active galactic nuclei (AGN) drawn from the BAT AGN Spectroscopic Survey project. The analysis includes measurements in individual and stacked spectra and considers s...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/ade879 |
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| author | Tomer Reiss Benny Trakhtenbrot Claudio Ricci Franz E. Bauer Michael J. Koss Kohei Ichikawa Darshan Kakkad Richard Mushotzky Kyuseok Oh Alessandro Peca Rudolf Bär Yaherlyn Diaz Fiona Harrison Meredith C. Powell Eleonora Sani Daniel Stern C. Megan Urry |
| author_facet | Tomer Reiss Benny Trakhtenbrot Claudio Ricci Franz E. Bauer Michael J. Koss Kohei Ichikawa Darshan Kakkad Richard Mushotzky Kyuseok Oh Alessandro Peca Rudolf Bär Yaherlyn Diaz Fiona Harrison Meredith C. Powell Eleonora Sani Daniel Stern C. Megan Urry |
| author_sort | Tomer Reiss |
| collection | DOAJ |
| description | We investigate the high-ionization, narrow [Ne V ] λ 3427 line emission in a sample of over 340 ultrahard X-ray (14–195 keV) selected active galactic nuclei (AGN) drawn from the BAT AGN Spectroscopic Survey project. The analysis includes measurements in individual and stacked spectra and considers several key AGN properties such as X-ray luminosity, supermassive black hole (SMBH) mass, Eddington ratios, and line-of-sight column density. The [Ne V ] λ 3427 line is robustly detected in ≈43% (146/341) of the AGN in our sample, with no significant trends between the detection rate and key AGN/SMBH properties. In particular, the detection rate remains high even at the highest levels of obscuration (>70% for ${\mathrm{log}}\,\left[{N}_{{\rm{H}}}/{\mathrm{cm}}^{-2}\right])\gtrsim 23$ ). On the other hand, even some of our highest signal-to-noise spectra (S/N > 50) lack a robust [Ne v] detection. The typical (median) scaling ratios between [Ne v] line emission and (ultra)hard X-ray emission in our sample are ${\mathrm{log}}\,{L}_{[{\rm{Ne}}\,{\rm\small{V}}]}/{L}_{14-150\,{\rm{keV}}}\simeq -3.75$ and ${\mathrm{log}}\,{L}_{[{\rm{Ne}}\,{\rm\small{V}}]}/{L}_{2-10\,{\rm{keV}}}\simeq -3.36$ . The scatter on these scaling ratios, ≲0.5 dex, is comparable to, and indeed smaller than, what is found for other commonly used tracers of AGN radiative outputs (e.g., [O III ] λ 5007). Otherwise, we find no significant relations between the (relative) strength of [Ne v] and the basic AGN/SMBH properties under study, in contrast with simple expectations from models of SMBH accretion flows. Our results reaffirm the usability of [Ne v] as an AGN tracer even in highly obscured systems, including dual AGN and high-redshift sources. |
| format | Article |
| id | doaj-art-3f569b0e09324aeb862e25868d9493a8 |
| institution | Kabale University |
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| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-3f569b0e09324aeb862e25868d9493a82025-08-20T03:39:15ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198918810.3847/1538-4357/ade879BASS. XLVIII. [Ne V] λ3427 Emission in Powerful Nearby Active Galactic NucleiTomer Reiss0Benny Trakhtenbrot1https://orcid.org/0000-0002-3683-7297Claudio Ricci2https://orcid.org/0000-0001-5231-2645Franz E. Bauer3https://orcid.org/0000-0002-8686-8737Michael J. Koss4https://orcid.org/0000-0002-7998-9581Kohei Ichikawa5https://orcid.org/0000-0002-4377-903XDarshan Kakkad6https://orcid.org/0000-0002-2603-2639Richard Mushotzky7https://orcid.org/0000-0002-7962-5446Kyuseok Oh8https://orcid.org/0000-0002-5037-951XAlessandro Peca9https://orcid.org/0000-0003-2196-3298Rudolf Bär10https://orcid.org/0000-0001-5481-8607Yaherlyn Diaz11https://orcid.org/0000-0002-8604-1158Fiona Harrison12https://orcid.org/0000-0002-4226-8959Meredith C. Powell13https://orcid.org/0000-0003-2284-8603Eleonora Sani14https://orcid.org/0000-0002-3140-4070Daniel Stern15https://orcid.org/0000-0003-2686-9241C. Megan Urry16https://orcid.org/0000-0002-0745-9792School of Physics and Astronomy, Tel Aviv University , Tel Aviv 69978, Israel ; bennyt@tauex.tau.ac.ilSchool of Physics and Astronomy, Tel Aviv University , Tel Aviv 69978, Israel ; bennyt@tauex.tau.ac.il; Max-Planck-Institut für extraterrestrische Physik , Gießenbachstraße 1, 85748 Garching, Germany; Excellence Cluster ORIGINS , Boltzmannsstraße 2, 85748, Garching, GermanyInstituto de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales , Av. Ejército Libertador 441, Santiago, Chile; Kavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People’s Republic of ChinaInstituto de Alta Investigación, Universidad de Tarapacá , Casilla 7D, Arica, ChileEureka Scientific , 2452 Delmer Street, Suite 100, Oakland, CA 94602-3017, USAAstronomical Institute, Tohoku University , Aramaki, Aoba-ku, Sendai, Miyagi 980-8578, Japan; Frontier Research Institute for Interdisciplinary Sciences, Tohoku University , Sendai 980-8578, Japan; Global Center for Science and Engineering, Faculty of Science and Engineering, Waseda University , 3-4-1, Okubo, Shinjuku, Tokyo 169-8555, JapanCentre for Astrophysics Research, University of Hertfordshire , Hatfield, AL10 9AB, UKDepartment of Astronomy, University of Maryland , College Park, MD 20742, USA; Joint Space-Science Institute, University of Maryland , College Park, MD 20742, USAKorea Astronomy & Space Science institute , 776, Daedeokdae-ro, Yuseong-gu, Daejeon 34055, Republic of KoreaEureka Scientific , 2452 Delmer Street, Suite 100, Oakland, CA 94602-3017, USA; Department of Physics, Yale University , P.O. Box 208120, New Haven, CT 06520, USAInstitute for Particle Physics and Astrophysics , ETH Zürich, Wolfgang-Pauli-Strasse 27, CH-8093 Zürich, SwitzerlandInstituto de Estudios Astrofísicos, Facultad de Ingeniería y Ciencias, Universidad Diego Portales , Av. Ejército Libertador 441, Santiago, ChileCahill Center for Astronomy and Astrophysics, California Institute of Technology , Pasadena, CA 91125, USALeibniz-Institut für Astrophysik Potsdam (AIP) , An der Sternwarte 16, 14482 Potsdam, Germany; Kavli Institute for Particle Astrophysics and Cosmology, Stanford University , 452 Lomita Mall, Stanford, CA 94305, USAEuropean Southern Observatory , Alonso de Córdova 3107, Casilla 19, Santiago 19001, ChileJet Propulsion Laboratory, California Institute of Technology , 4800 Oak Grove Drive, MS 169-224, Pasadena, CA 91109, USADepartment of Physics, Yale University , P.O. Box 208120, New Haven, CT 06520, USA; Yale Center for Astronomy and Astrophysics , 52 Hillhouse Avenue, New Haven, CT 06511, USAWe investigate the high-ionization, narrow [Ne V ] λ 3427 line emission in a sample of over 340 ultrahard X-ray (14–195 keV) selected active galactic nuclei (AGN) drawn from the BAT AGN Spectroscopic Survey project. The analysis includes measurements in individual and stacked spectra and considers several key AGN properties such as X-ray luminosity, supermassive black hole (SMBH) mass, Eddington ratios, and line-of-sight column density. The [Ne V ] λ 3427 line is robustly detected in ≈43% (146/341) of the AGN in our sample, with no significant trends between the detection rate and key AGN/SMBH properties. In particular, the detection rate remains high even at the highest levels of obscuration (>70% for ${\mathrm{log}}\,\left[{N}_{{\rm{H}}}/{\mathrm{cm}}^{-2}\right])\gtrsim 23$ ). On the other hand, even some of our highest signal-to-noise spectra (S/N > 50) lack a robust [Ne v] detection. The typical (median) scaling ratios between [Ne v] line emission and (ultra)hard X-ray emission in our sample are ${\mathrm{log}}\,{L}_{[{\rm{Ne}}\,{\rm\small{V}}]}/{L}_{14-150\,{\rm{keV}}}\simeq -3.75$ and ${\mathrm{log}}\,{L}_{[{\rm{Ne}}\,{\rm\small{V}}]}/{L}_{2-10\,{\rm{keV}}}\simeq -3.36$ . The scatter on these scaling ratios, ≲0.5 dex, is comparable to, and indeed smaller than, what is found for other commonly used tracers of AGN radiative outputs (e.g., [O III ] λ 5007). Otherwise, we find no significant relations between the (relative) strength of [Ne v] and the basic AGN/SMBH properties under study, in contrast with simple expectations from models of SMBH accretion flows. Our results reaffirm the usability of [Ne v] as an AGN tracer even in highly obscured systems, including dual AGN and high-redshift sources.https://doi.org/10.3847/1538-4357/ade879Active galactic nucleiX-ray active galactic nucleiGalaxy nucleiHigh energy astrophysics |
| spellingShingle | Tomer Reiss Benny Trakhtenbrot Claudio Ricci Franz E. Bauer Michael J. Koss Kohei Ichikawa Darshan Kakkad Richard Mushotzky Kyuseok Oh Alessandro Peca Rudolf Bär Yaherlyn Diaz Fiona Harrison Meredith C. Powell Eleonora Sani Daniel Stern C. Megan Urry BASS. XLVIII. [Ne V] λ3427 Emission in Powerful Nearby Active Galactic Nuclei The Astrophysical Journal Active galactic nuclei X-ray active galactic nuclei Galaxy nuclei High energy astrophysics |
| title | BASS. XLVIII. [Ne V] λ3427 Emission in Powerful Nearby Active Galactic Nuclei |
| title_full | BASS. XLVIII. [Ne V] λ3427 Emission in Powerful Nearby Active Galactic Nuclei |
| title_fullStr | BASS. XLVIII. [Ne V] λ3427 Emission in Powerful Nearby Active Galactic Nuclei |
| title_full_unstemmed | BASS. XLVIII. [Ne V] λ3427 Emission in Powerful Nearby Active Galactic Nuclei |
| title_short | BASS. XLVIII. [Ne V] λ3427 Emission in Powerful Nearby Active Galactic Nuclei |
| title_sort | bass xlviii ne v λ3427 emission in powerful nearby active galactic nuclei |
| topic | Active galactic nuclei X-ray active galactic nuclei Galaxy nuclei High energy astrophysics |
| url | https://doi.org/10.3847/1538-4357/ade879 |
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