Search for neutrino emission from hard X-ray AGN with IceCube
Active Galactic Nuclei (AGN) are promising candidate sources of high-energy astrophysical neutrinos since they provide environments rich in matter and photon targets where cosmic ray interactions may lead to the production of gamma rays and neutrinos. We searched for high-energy neutrino emission fr...
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| creator | Adams, J Alameddine, J. M Andeen, K Ashida, Y Athanasiadou, S Bai, X V, A. Balagopal Bellenghi, C Bontempo, F Meneguolo, C. Boscolo Böttcher, J Braun, J Butterfield, D Carpio, J Chattopadhyay, S Chau, N Clark, B. A Coleman, A Collin, G. H Corley, R DeLaunay, J. J Desai, A Dierichs, P Domi, A Draper, L Dujmovic, H Eidenschink, L Evans, J Fan, K. L Feigl, N Fox, D Garcia, M Garg, G Glaser, C Gonzalez, J. G Hamdaoui, H Minh, M. Ha Häußler, J Hussain, R Ishihara, A Jain, S Jeong, M Jones, B. J. P Kamp, N Kang, D Kang, X Karl, M Kauer, M Zathul, A. Khatee Kiryluk, J Kontrimas, T Kovacevich, M Kowalski, M Gualda, C. Lagunas Latseva, S Lauber, F Lee, J. W Liao, J Liubarska, M Mariscal, C. J. Lozano Luszczak, W Mahn, K. B. M Merten, L Moore, R. W Morii, Y Park, N Parker, G. K Plum, M Rack-Helleis, J Ravn, M Rifaie, A Robertson, S Ruhe, T Ruohan, L Ryckbosch, D Santander, M Schieler, H Schlüter, B Schlüter, F Schmeisser, N Schröder, F. G Myhr, P. Sevle Soldin, D Spannfellner, C Stamatikos, M Thwaites, J Toscano, S Upadhyay, A. K Vannerom, D Venugopal, M Vereecken, M Wang, A Weigel, P Wendt, C Werthebach, J Williams, D. R Witthaus, L Yuan, T Zhang, Z Zimmerman, M |
| description | Active Galactic Nuclei (AGN) are promising candidate sources of high-energy
astrophysical neutrinos since they provide environments rich in matter and
photon targets where cosmic ray interactions may lead to the production of
gamma rays and neutrinos. We searched for high-energy neutrino emission from
AGN using the $\textit{Swift}$-BAT Spectroscopic Survey (BASS) catalog of hard
X-ray sources and 12 years of IceCube muon track data. First, upon performing a
stacked search, no significant emission was found. Second, we searched for
neutrinos from a list of 43 candidate sources and found an excess from the
direction of two sources, Seyfert galaxies NGC 1068 and NGC 4151. We observed
NGC 1068 at flux $\phi_{\nu_{\mu}+\bar{\nu}_{\mu}}$ = $4.02_{-1.52}^{+1.58}
\times 10^{-11}$ TeV$^{-1}$ cm$^{-2}$ s$^{-1}$ normalized at 1 TeV, with
power-law spectral index, $\gamma$ = 3.10$^{+0.26}_{-0.22}$, consistent with
previous IceCube results. The observation of a neutrino excess from the
direction of NGC 4151 is at a post-trial significance of 2.9$\sigma$. If
interpreted as an astrophysical signal, the excess observed from NGC 4151
corresponds to a flux $\phi_{\nu_{\mu}+\bar{\nu}_{\mu}}$ =
$1.51_{-0.81}^{+0.99} \times 10^{-11}$ TeV$^{-1}$ cm$^{-2}$ s$^{-1}$ normalized
at 1 TeV and $\gamma$ = 2.83$^{+0.35}_{-0.28}$. |
| doi_str_mv | 10.48550/arxiv.2406.06684 |
| format | Article |
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astrophysical neutrinos since they provide environments rich in matter and
photon targets where cosmic ray interactions may lead to the production of
gamma rays and neutrinos. We searched for high-energy neutrino emission from
AGN using the $\textit{Swift}$-BAT Spectroscopic Survey (BASS) catalog of hard
X-ray sources and 12 years of IceCube muon track data. First, upon performing a
stacked search, no significant emission was found. Second, we searched for
neutrinos from a list of 43 candidate sources and found an excess from the
direction of two sources, Seyfert galaxies NGC 1068 and NGC 4151. We observed
NGC 1068 at flux $\phi_{\nu_{\mu}+\bar{\nu}_{\mu}}$ = $4.02_{-1.52}^{+1.58}
\times 10^{-11}$ TeV$^{-1}$ cm$^{-2}$ s$^{-1}$ normalized at 1 TeV, with
power-law spectral index, $\gamma$ = 3.10$^{+0.26}_{-0.22}$, consistent with
previous IceCube results. The observation of a neutrino excess from the
direction of NGC 4151 is at a post-trial significance of 2.9$\sigma$. If
interpreted as an astrophysical signal, the excess observed from NGC 4151
corresponds to a flux $\phi_{\nu_{\mu}+\bar{\nu}_{\mu}}$ =
$1.51_{-0.81}^{+0.99} \times 10^{-11}$ TeV$^{-1}$ cm$^{-2}$ s$^{-1}$ normalized
at 1 TeV and $\gamma$ = 2.83$^{+0.35}_{-0.28}$.</description><identifier>DOI: 10.48550/arxiv.2406.06684</identifier><language>eng</language><subject>Physics - High Energy Astrophysical Phenomena</subject><creationdate>2024-06</creationdate><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,885</link.rule.ids><linktorsrc>$$Uhttps://arxiv.org/abs/2406.06684$$EView_record_in_Cornell_University$$FView_record_in_$$GCornell_University$$Hfree_for_read</linktorsrc><backlink>$$Uhttps://doi.org/10.48550/arXiv.2406.06684$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Adams, J</creatorcontrib><creatorcontrib>Alameddine, J. M</creatorcontrib><creatorcontrib>Andeen, K</creatorcontrib><creatorcontrib>Ashida, Y</creatorcontrib><creatorcontrib>Athanasiadou, S</creatorcontrib><creatorcontrib>Bai, X</creatorcontrib><creatorcontrib>V, A. Balagopal</creatorcontrib><creatorcontrib>Bellenghi, C</creatorcontrib><creatorcontrib>Bontempo, F</creatorcontrib><creatorcontrib>Meneguolo, C. Boscolo</creatorcontrib><creatorcontrib>Böttcher, J</creatorcontrib><creatorcontrib>Braun, J</creatorcontrib><creatorcontrib>Butterfield, D</creatorcontrib><creatorcontrib>Carpio, J</creatorcontrib><creatorcontrib>Chattopadhyay, S</creatorcontrib><creatorcontrib>Chau, N</creatorcontrib><creatorcontrib>Clark, B. A</creatorcontrib><creatorcontrib>Coleman, A</creatorcontrib><creatorcontrib>Collin, G. H</creatorcontrib><creatorcontrib>Corley, R</creatorcontrib><creatorcontrib>DeLaunay, J. J</creatorcontrib><creatorcontrib>Desai, A</creatorcontrib><creatorcontrib>Dierichs, P</creatorcontrib><creatorcontrib>Domi, A</creatorcontrib><creatorcontrib>Draper, L</creatorcontrib><creatorcontrib>Dujmovic, H</creatorcontrib><creatorcontrib>Eidenschink, L</creatorcontrib><creatorcontrib>Evans, J</creatorcontrib><creatorcontrib>Fan, K. L</creatorcontrib><creatorcontrib>Feigl, N</creatorcontrib><creatorcontrib>Fox, D</creatorcontrib><creatorcontrib>Garcia, M</creatorcontrib><creatorcontrib>Garg, G</creatorcontrib><creatorcontrib>Glaser, C</creatorcontrib><creatorcontrib>Gonzalez, J. G</creatorcontrib><creatorcontrib>Hamdaoui, H</creatorcontrib><creatorcontrib>Minh, M. Ha</creatorcontrib><creatorcontrib>Häußler, J</creatorcontrib><creatorcontrib>Hussain, R</creatorcontrib><creatorcontrib>Ishihara, A</creatorcontrib><creatorcontrib>Jain, S</creatorcontrib><creatorcontrib>Jeong, M</creatorcontrib><creatorcontrib>Jones, B. J. P</creatorcontrib><creatorcontrib>Kamp, N</creatorcontrib><creatorcontrib>Kang, D</creatorcontrib><creatorcontrib>Kang, X</creatorcontrib><creatorcontrib>Karl, M</creatorcontrib><creatorcontrib>Kauer, M</creatorcontrib><creatorcontrib>Zathul, A. Khatee</creatorcontrib><creatorcontrib>Kiryluk, J</creatorcontrib><creatorcontrib>Kontrimas, T</creatorcontrib><creatorcontrib>Kovacevich, M</creatorcontrib><creatorcontrib>Kowalski, M</creatorcontrib><creatorcontrib>Gualda, C. Lagunas</creatorcontrib><creatorcontrib>Latseva, S</creatorcontrib><creatorcontrib>Lauber, F</creatorcontrib><creatorcontrib>Lee, J. W</creatorcontrib><creatorcontrib>Liao, J</creatorcontrib><creatorcontrib>Liubarska, M</creatorcontrib><creatorcontrib>Mariscal, C. J. Lozano</creatorcontrib><creatorcontrib>Luszczak, W</creatorcontrib><creatorcontrib>Mahn, K. B. M</creatorcontrib><creatorcontrib>Merten, L</creatorcontrib><creatorcontrib>Moore, R. W</creatorcontrib><creatorcontrib>Morii, Y</creatorcontrib><creatorcontrib>Park, N</creatorcontrib><creatorcontrib>Parker, G. K</creatorcontrib><creatorcontrib>Plum, M</creatorcontrib><creatorcontrib>Rack-Helleis, J</creatorcontrib><creatorcontrib>Ravn, M</creatorcontrib><creatorcontrib>Rifaie, A</creatorcontrib><creatorcontrib>Robertson, S</creatorcontrib><creatorcontrib>Ruhe, T</creatorcontrib><creatorcontrib>Ruohan, L</creatorcontrib><creatorcontrib>Ryckbosch, D</creatorcontrib><creatorcontrib>Santander, M</creatorcontrib><creatorcontrib>Schieler, H</creatorcontrib><creatorcontrib>Schlüter, B</creatorcontrib><creatorcontrib>Schlüter, F</creatorcontrib><creatorcontrib>Schmeisser, N</creatorcontrib><creatorcontrib>Schröder, F. G</creatorcontrib><creatorcontrib>Myhr, P. Sevle</creatorcontrib><creatorcontrib>Soldin, D</creatorcontrib><creatorcontrib>Spannfellner, C</creatorcontrib><creatorcontrib>Stamatikos, M</creatorcontrib><creatorcontrib>Thwaites, J</creatorcontrib><creatorcontrib>Toscano, S</creatorcontrib><creatorcontrib>Upadhyay, A. K</creatorcontrib><creatorcontrib>Vannerom, D</creatorcontrib><creatorcontrib>Venugopal, M</creatorcontrib><creatorcontrib>Vereecken, M</creatorcontrib><creatorcontrib>Wang, A</creatorcontrib><creatorcontrib>Weigel, P</creatorcontrib><creatorcontrib>Wendt, C</creatorcontrib><creatorcontrib>Werthebach, J</creatorcontrib><creatorcontrib>Williams, D. R</creatorcontrib><creatorcontrib>Witthaus, L</creatorcontrib><creatorcontrib>Yuan, T</creatorcontrib><creatorcontrib>Zhang, Z</creatorcontrib><creatorcontrib>Zimmerman, M</creatorcontrib><title>Search for neutrino emission from hard X-ray AGN with IceCube</title><description>Active Galactic Nuclei (AGN) are promising candidate sources of high-energy
astrophysical neutrinos since they provide environments rich in matter and
photon targets where cosmic ray interactions may lead to the production of
gamma rays and neutrinos. We searched for high-energy neutrino emission from
AGN using the $\textit{Swift}$-BAT Spectroscopic Survey (BASS) catalog of hard
X-ray sources and 12 years of IceCube muon track data. First, upon performing a
stacked search, no significant emission was found. Second, we searched for
neutrinos from a list of 43 candidate sources and found an excess from the
direction of two sources, Seyfert galaxies NGC 1068 and NGC 4151. We observed
NGC 1068 at flux $\phi_{\nu_{\mu}+\bar{\nu}_{\mu}}$ = $4.02_{-1.52}^{+1.58}
\times 10^{-11}$ TeV$^{-1}$ cm$^{-2}$ s$^{-1}$ normalized at 1 TeV, with
power-law spectral index, $\gamma$ = 3.10$^{+0.26}_{-0.22}$, consistent with
previous IceCube results. The observation of a neutrino excess from the
direction of NGC 4151 is at a post-trial significance of 2.9$\sigma$. If
interpreted as an astrophysical signal, the excess observed from NGC 4151
corresponds to a flux $\phi_{\nu_{\mu}+\bar{\nu}_{\mu}}$ =
$1.51_{-0.81}^{+0.99} \times 10^{-11}$ TeV$^{-1}$ cm$^{-2}$ s$^{-1}$ normalized
at 1 TeV and $\gamma$ = 2.83$^{+0.35}_{-0.28}$.</description><subject>Physics - High Energy Astrophysical Phenomena</subject><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2024</creationdate><recordtype>article</recordtype><sourceid>GOX</sourceid><recordid>eNotj7FOwzAUAL0woMIHMPF-IMF2_BJnYKgiKJUqGOjAFj3bz4olkiCnBfr3iMJ02-lOiBslS2MR5R3l7_RZaiPrUta1NZfi_pUp-wHinGHi4yGnaQYe07KkeYKY5xEGygHeikwnWG-e4SsdBth67o6Or8RFpPeFr_-5EvvHh333VOxeNttuvSuobkyBAVsVGs_Ks8TWBd1IRMdIaJWNzrfWkIpVawxKr7RmCtiQxhgdGq2qlbj90577-4-cRsqn_vejP39UP5WiQac</recordid><startdate>20240610</startdate><enddate>20240610</enddate><creator>Adams, J</creator><creator>Alameddine, J. M</creator><creator>Andeen, K</creator><creator>Ashida, Y</creator><creator>Athanasiadou, S</creator><creator>Bai, X</creator><creator>V, A. Balagopal</creator><creator>Bellenghi, C</creator><creator>Bontempo, F</creator><creator>Meneguolo, C. 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Khatee ; Kiryluk, J ; Kontrimas, T ; Kovacevich, M ; Kowalski, M ; Gualda, C. Lagunas ; Latseva, S ; Lauber, F ; Lee, J. W ; Liao, J ; Liubarska, M ; Mariscal, C. J. Lozano ; Luszczak, W ; Mahn, K. B. M ; Merten, L ; Moore, R. W ; Morii, Y ; Park, N ; Parker, G. K ; Plum, M ; Rack-Helleis, J ; Ravn, M ; Rifaie, A ; Robertson, S ; Ruhe, T ; Ruohan, L ; Ryckbosch, D ; Santander, M ; Schieler, H ; Schlüter, B ; Schlüter, F ; Schmeisser, N ; Schröder, F. G ; Myhr, P. Sevle ; Soldin, D ; Spannfellner, C ; Stamatikos, M ; Thwaites, J ; Toscano, S ; Upadhyay, A. K ; Vannerom, D ; Venugopal, M ; Vereecken, M ; Wang, A ; Weigel, P ; Wendt, C ; Werthebach, J ; Williams, D. R ; Witthaus, L ; Yuan, T ; Zhang, Z ; Zimmerman, M</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a674-5d591d7ce1ce059bd27055be5a5818fbc984a1f394450c122ead57a25ffb54213</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2024</creationdate><topic>Physics - High Energy Astrophysical Phenomena</topic><toplevel>online_resources</toplevel><creatorcontrib>Adams, J</creatorcontrib><creatorcontrib>Alameddine, J. M</creatorcontrib><creatorcontrib>Andeen, K</creatorcontrib><creatorcontrib>Ashida, Y</creatorcontrib><creatorcontrib>Athanasiadou, S</creatorcontrib><creatorcontrib>Bai, X</creatorcontrib><creatorcontrib>V, A. Balagopal</creatorcontrib><creatorcontrib>Bellenghi, C</creatorcontrib><creatorcontrib>Bontempo, F</creatorcontrib><creatorcontrib>Meneguolo, C. Boscolo</creatorcontrib><creatorcontrib>Böttcher, J</creatorcontrib><creatorcontrib>Braun, J</creatorcontrib><creatorcontrib>Butterfield, D</creatorcontrib><creatorcontrib>Carpio, J</creatorcontrib><creatorcontrib>Chattopadhyay, S</creatorcontrib><creatorcontrib>Chau, N</creatorcontrib><creatorcontrib>Clark, B. A</creatorcontrib><creatorcontrib>Coleman, A</creatorcontrib><creatorcontrib>Collin, G. H</creatorcontrib><creatorcontrib>Corley, R</creatorcontrib><creatorcontrib>DeLaunay, J. J</creatorcontrib><creatorcontrib>Desai, A</creatorcontrib><creatorcontrib>Dierichs, P</creatorcontrib><creatorcontrib>Domi, A</creatorcontrib><creatorcontrib>Draper, L</creatorcontrib><creatorcontrib>Dujmovic, H</creatorcontrib><creatorcontrib>Eidenschink, L</creatorcontrib><creatorcontrib>Evans, J</creatorcontrib><creatorcontrib>Fan, K. L</creatorcontrib><creatorcontrib>Feigl, N</creatorcontrib><creatorcontrib>Fox, D</creatorcontrib><creatorcontrib>Garcia, M</creatorcontrib><creatorcontrib>Garg, G</creatorcontrib><creatorcontrib>Glaser, C</creatorcontrib><creatorcontrib>Gonzalez, J. G</creatorcontrib><creatorcontrib>Hamdaoui, H</creatorcontrib><creatorcontrib>Minh, M. Ha</creatorcontrib><creatorcontrib>Häußler, J</creatorcontrib><creatorcontrib>Hussain, R</creatorcontrib><creatorcontrib>Ishihara, A</creatorcontrib><creatorcontrib>Jain, S</creatorcontrib><creatorcontrib>Jeong, M</creatorcontrib><creatorcontrib>Jones, B. J. P</creatorcontrib><creatorcontrib>Kamp, N</creatorcontrib><creatorcontrib>Kang, D</creatorcontrib><creatorcontrib>Kang, X</creatorcontrib><creatorcontrib>Karl, M</creatorcontrib><creatorcontrib>Kauer, M</creatorcontrib><creatorcontrib>Zathul, A. Khatee</creatorcontrib><creatorcontrib>Kiryluk, J</creatorcontrib><creatorcontrib>Kontrimas, T</creatorcontrib><creatorcontrib>Kovacevich, M</creatorcontrib><creatorcontrib>Kowalski, M</creatorcontrib><creatorcontrib>Gualda, C. Lagunas</creatorcontrib><creatorcontrib>Latseva, S</creatorcontrib><creatorcontrib>Lauber, F</creatorcontrib><creatorcontrib>Lee, J. W</creatorcontrib><creatorcontrib>Liao, J</creatorcontrib><creatorcontrib>Liubarska, M</creatorcontrib><creatorcontrib>Mariscal, C. J. Lozano</creatorcontrib><creatorcontrib>Luszczak, W</creatorcontrib><creatorcontrib>Mahn, K. B. M</creatorcontrib><creatorcontrib>Merten, L</creatorcontrib><creatorcontrib>Moore, R. W</creatorcontrib><creatorcontrib>Morii, Y</creatorcontrib><creatorcontrib>Park, N</creatorcontrib><creatorcontrib>Parker, G. K</creatorcontrib><creatorcontrib>Plum, M</creatorcontrib><creatorcontrib>Rack-Helleis, J</creatorcontrib><creatorcontrib>Ravn, M</creatorcontrib><creatorcontrib>Rifaie, A</creatorcontrib><creatorcontrib>Robertson, S</creatorcontrib><creatorcontrib>Ruhe, T</creatorcontrib><creatorcontrib>Ruohan, L</creatorcontrib><creatorcontrib>Ryckbosch, D</creatorcontrib><creatorcontrib>Santander, M</creatorcontrib><creatorcontrib>Schieler, H</creatorcontrib><creatorcontrib>Schlüter, B</creatorcontrib><creatorcontrib>Schlüter, F</creatorcontrib><creatorcontrib>Schmeisser, N</creatorcontrib><creatorcontrib>Schröder, F. G</creatorcontrib><creatorcontrib>Myhr, P. Sevle</creatorcontrib><creatorcontrib>Soldin, D</creatorcontrib><creatorcontrib>Spannfellner, C</creatorcontrib><creatorcontrib>Stamatikos, M</creatorcontrib><creatorcontrib>Thwaites, J</creatorcontrib><creatorcontrib>Toscano, S</creatorcontrib><creatorcontrib>Upadhyay, A. K</creatorcontrib><creatorcontrib>Vannerom, D</creatorcontrib><creatorcontrib>Venugopal, M</creatorcontrib><creatorcontrib>Vereecken, M</creatorcontrib><creatorcontrib>Wang, A</creatorcontrib><creatorcontrib>Weigel, P</creatorcontrib><creatorcontrib>Wendt, C</creatorcontrib><creatorcontrib>Werthebach, J</creatorcontrib><creatorcontrib>Williams, D. R</creatorcontrib><creatorcontrib>Witthaus, L</creatorcontrib><creatorcontrib>Yuan, T</creatorcontrib><creatorcontrib>Zhang, Z</creatorcontrib><creatorcontrib>Zimmerman, M</creatorcontrib><collection>arXiv.org</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Adams, J</au><au>Alameddine, J. M</au><au>Andeen, K</au><au>Ashida, Y</au><au>Athanasiadou, S</au><au>Bai, X</au><au>V, A. Balagopal</au><au>Bellenghi, C</au><au>Bontempo, F</au><au>Meneguolo, C. Boscolo</au><au>Böttcher, J</au><au>Braun, J</au><au>Butterfield, D</au><au>Carpio, J</au><au>Chattopadhyay, S</au><au>Chau, N</au><au>Clark, B. A</au><au>Coleman, A</au><au>Collin, G. H</au><au>Corley, R</au><au>DeLaunay, J. J</au><au>Desai, A</au><au>Dierichs, P</au><au>Domi, A</au><au>Draper, L</au><au>Dujmovic, H</au><au>Eidenschink, L</au><au>Evans, J</au><au>Fan, K. L</au><au>Feigl, N</au><au>Fox, D</au><au>Garcia, M</au><au>Garg, G</au><au>Glaser, C</au><au>Gonzalez, J. G</au><au>Hamdaoui, H</au><au>Minh, M. Ha</au><au>Häußler, J</au><au>Hussain, R</au><au>Ishihara, A</au><au>Jain, S</au><au>Jeong, M</au><au>Jones, B. J. P</au><au>Kamp, N</au><au>Kang, D</au><au>Kang, X</au><au>Karl, M</au><au>Kauer, M</au><au>Zathul, A. Khatee</au><au>Kiryluk, J</au><au>Kontrimas, T</au><au>Kovacevich, M</au><au>Kowalski, M</au><au>Gualda, C. Lagunas</au><au>Latseva, S</au><au>Lauber, F</au><au>Lee, J. W</au><au>Liao, J</au><au>Liubarska, M</au><au>Mariscal, C. J. Lozano</au><au>Luszczak, W</au><au>Mahn, K. B. M</au><au>Merten, L</au><au>Moore, R. W</au><au>Morii, Y</au><au>Park, N</au><au>Parker, G. K</au><au>Plum, M</au><au>Rack-Helleis, J</au><au>Ravn, M</au><au>Rifaie, A</au><au>Robertson, S</au><au>Ruhe, T</au><au>Ruohan, L</au><au>Ryckbosch, D</au><au>Santander, M</au><au>Schieler, H</au><au>Schlüter, B</au><au>Schlüter, F</au><au>Schmeisser, N</au><au>Schröder, F. G</au><au>Myhr, P. Sevle</au><au>Soldin, D</au><au>Spannfellner, C</au><au>Stamatikos, M</au><au>Thwaites, J</au><au>Toscano, S</au><au>Upadhyay, A. K</au><au>Vannerom, D</au><au>Venugopal, M</au><au>Vereecken, M</au><au>Wang, A</au><au>Weigel, P</au><au>Wendt, C</au><au>Werthebach, J</au><au>Williams, D. R</au><au>Witthaus, L</au><au>Yuan, T</au><au>Zhang, Z</au><au>Zimmerman, M</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Search for neutrino emission from hard X-ray AGN with IceCube</atitle><date>2024-06-10</date><risdate>2024</risdate><abstract>Active Galactic Nuclei (AGN) are promising candidate sources of high-energy
astrophysical neutrinos since they provide environments rich in matter and
photon targets where cosmic ray interactions may lead to the production of
gamma rays and neutrinos. We searched for high-energy neutrino emission from
AGN using the $\textit{Swift}$-BAT Spectroscopic Survey (BASS) catalog of hard
X-ray sources and 12 years of IceCube muon track data. First, upon performing a
stacked search, no significant emission was found. Second, we searched for
neutrinos from a list of 43 candidate sources and found an excess from the
direction of two sources, Seyfert galaxies NGC 1068 and NGC 4151. We observed
NGC 1068 at flux $\phi_{\nu_{\mu}+\bar{\nu}_{\mu}}$ = $4.02_{-1.52}^{+1.58}
\times 10^{-11}$ TeV$^{-1}$ cm$^{-2}$ s$^{-1}$ normalized at 1 TeV, with
power-law spectral index, $\gamma$ = 3.10$^{+0.26}_{-0.22}$, consistent with
previous IceCube results. The observation of a neutrino excess from the
direction of NGC 4151 is at a post-trial significance of 2.9$\sigma$. If
interpreted as an astrophysical signal, the excess observed from NGC 4151
corresponds to a flux $\phi_{\nu_{\mu}+\bar{\nu}_{\mu}}$ =
$1.51_{-0.81}^{+0.99} \times 10^{-11}$ TeV$^{-1}$ cm$^{-2}$ s$^{-1}$ normalized
at 1 TeV and $\gamma$ = 2.83$^{+0.35}_{-0.28}$.</abstract><doi>10.48550/arxiv.2406.06684</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext_linktorsrc |
| identifier | DOI: 10.48550/arxiv.2406.06684 |
| ispartof | |
| issn | |
| language | eng |
| recordid | cdi_arxiv_primary_2406_06684 |
| source | arXiv.org |
| subjects | Physics - High Energy Astrophysical Phenomena |
| title | Search for neutrino emission from hard X-ray AGN with IceCube |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-10T22%3A28%3A30IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-arxiv_GOX&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Search%20for%20neutrino%20emission%20from%20hard%20X-ray%20AGN%20with%20IceCube&rft.au=Adams,%20J&rft.date=2024-06-10&rft_id=info:doi/10.48550/arxiv.2406.06684&rft_dat=%3Carxiv_GOX%3E2406_06684%3C/arxiv_GOX%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_id=info:pmid/&rfr_iscdi=true |