Limits on point-like sources of ultra-high-energy neutrinos with the Pierre Auger Observatory. (arXiv:1906.07419v1 [astro-ph.HE])
The <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_Pierre_Auger/0/1/0/all/0/1">Pierre Auger Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Aab_A/0/1/0/all/0/1">A. Aab</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abreu_P/0/1/0/all/0/1">P. Abreu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aglietta_M/0/1/0/all/0/1">M. Aglietta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Albuquerque_I/0/1/0/all/0/1">I.F.M. Albuquerque</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Albury_J/0/1/0/all/0/1">J.M. Albury</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allekotte_I/0/1/0/all/0/1">I. Allekotte</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Almela_A/0/1/0/all/0/1">A. Almela</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castillo_J/0/1/0/all/0/1">J. Alvarez Castillo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alvarez_Muniz_J/0/1/0/all/0/1">J. Alvarez-Muñiz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anastasi_G/0/1/0/all/0/1">G.A. Anastasi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anchordoqui_L/0/1/0/all/0/1">L. Anchordoqui</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andrada_B/0/1/0/all/0/1">B. Andrada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andringa_S/0/1/0/all/0/1">S. Andringa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aramo_C/0/1/0/all/0/1">C. Aramo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asorey_H/0/1/0/all/0/1">H. Asorey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Assis_P/0/1/0/all/0/1">P. Assis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avila_G/0/1/0/all/0/1">G. Avila</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Badescu_A/0/1/0/all/0/1">A.M. Badescu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bakalova_A/0/1/0/all/0/1">A. Bakalova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Balaceanu_A/0/1/0/all/0/1">A. Balaceanu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barbato_F/0/1/0/all/0/1">F. Barbato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luz_R/0/1/0/all/0/1">R.J. Barreira Luz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baur_S/0/1/0/all/0/1">S. Baur</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Becker_K/0/1/0/all/0/1">K.H. Becker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bellido_J/0/1/0/all/0/1">J.A. Bellido</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berat_C/0/1/0/all/0/1">C. Berat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertaina_M/0/1/0/all/0/1">M.E. Bertaina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertou_X/0/1/0/all/0/1">X. Bertou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biermann_P/0/1/0/all/0/1">P.L. Biermann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biteau_J/0/1/0/all/0/1">J. Biteau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blanco_A/0/1/0/all/0/1">A. Blanco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blazek_J/0/1/0/all/0/1">J. Blazek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bleve_C/0/1/0/all/0/1">C. Bleve</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bohacova_M/0/1/0/all/0/1">M. Boháčová</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boncioli_D/0/1/0/all/0/1">D. Boncioli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonifazi_C/0/1/0/all/0/1">C. Bonifazi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Borodai_N/0/1/0/all/0/1">N. Borodai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Botti_A/0/1/0/all/0/1">A.M. Botti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brack_J/0/1/0/all/0/1">J. Brack</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bretz_T/0/1/0/all/0/1">T. Bretz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bridgeman_A/0/1/0/all/0/1">A. Bridgeman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Briechle_F/0/1/0/all/0/1">F.L. Briechle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buchholz_P/0/1/0/all/0/1">P. Buchholz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bueno_A/0/1/0/all/0/1">A. Bueno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buitink_S/0/1/0/all/0/1">S. Buitink</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buscemi_M/0/1/0/all/0/1">M. Buscemi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caballero_Mora_K/0/1/0/all/0/1">K.S. Caballero-Mora</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caccianiga_L/0/1/0/all/0/1">L. Caccianiga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calcagni_L/0/1/0/all/0/1">L. Calcagni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cancio_A/0/1/0/all/0/1">A. Cancio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Canfora_F/0/1/0/all/0/1">F. Canfora</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caracas_I/0/1/0/all/0/1">I. Caracas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carceller_J/0/1/0/all/0/1">J.M. Carceller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caruso_R/0/1/0/all/0/1">R. Caruso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castellina_A/0/1/0/all/0/1">A. Castellina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Catalani_F/0/1/0/all/0/1">F. Catalani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cataldi_G/0/1/0/all/0/1">G. Cataldi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cazon_L/0/1/0/all/0/1">L. Cazon</a>, et al. (333 additional authors not shown)
With the Surface Detector array (SD) of the Pierre Auger Observatory we can
detect neutrinos with energy between $10^{17},$eV and $10^{20},$eV from
point-like sources across the sky, from close to the Southern Celestial Pole up
to $60^circ$ in declination, with peak sensitivities at declinations around
$sim -53^circ$ and $sim+55^circ$, and an unmatched sensitivity for arrival
directions in the Northern hemisphere. A search has been performed for
highly-inclined air showers induced by neutrinos of all flavours with no
candidate events found in data taken between 1 Jan 2004 and 31 Aug 2018. Upper
limits on the neutrino flux from point-like steady sources have been derived as
a function of source declination. An unrivaled sensitivity is achieved in
searches for transient sources with emission lasting over an hour or less, if
they occur within the field of view corresponding to the zenith angle range
between $60^circ$ and $~95^circ$ where the SD of the Pierre Auger Observatory
is most sensitive to neutrinos.
With the Surface Detector array (SD) of the Pierre Auger Observatory we can
detect neutrinos with energy between $10^{17},$eV and $10^{20},$eV from
point-like sources across the sky, from close to the Southern Celestial Pole up
to $60^circ$ in declination, with peak sensitivities at declinations around
$sim -53^circ$ and $sim+55^circ$, and an unmatched sensitivity for arrival
directions in the Northern hemisphere. A search has been performed for
highly-inclined air showers induced by neutrinos of all flavours with no
candidate events found in data taken between 1 Jan 2004 and 31 Aug 2018. Upper
limits on the neutrino flux from point-like steady sources have been derived as
a function of source declination. An unrivaled sensitivity is achieved in
searches for transient sources with emission lasting over an hour or less, if
they occur within the field of view corresponding to the zenith angle range
between $60^circ$ and $~95^circ$ where the SD of the Pierre Auger Observatory
is most sensitive to neutrinos.
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