Neutrinos below 100 TeV from the southern sky employing refined veto techniques to IceCube data. (arXiv:1902.05792v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_IceCube/0/1/0/all/0/1">IceCube Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Aartsen_M/0/1/0/all/0/1">M. G. Aartsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ackermann_M/0/1/0/all/0/1">M. Ackermann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adams_J/0/1/0/all/0/1">J. Adams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguilar_J/0/1/0/all/0/1">J. A. Aguilar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ahlers_M/0/1/0/all/0/1">M. Ahlers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ahrens_M/0/1/0/all/0/1">M. Ahrens</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alispach_C/0/1/0/all/0/1">C. Alispach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Altmann_D/0/1/0/all/0/1">D. Altmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andeen_K/0/1/0/all/0/1">K. Andeen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_T/0/1/0/all/0/1">T. Anderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ansseau_I/0/1/0/all/0/1">I. Ansseau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anton_G/0/1/0/all/0/1">G. Anton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arguelles_C/0/1/0/all/0/1">C. Argüelles</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Auffenberg_J/0/1/0/all/0/1">J. Auffenberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Axani_S/0/1/0/all/0/1">S. Axani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Backes_P/0/1/0/all/0/1">P. Backes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bagherpour_H/0/1/0/all/0/1">H. Bagherpour</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bai_X/0/1/0/all/0/1">X. Bai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barbano_A/0/1/0/all/0/1">A. Barbano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barwick_S/0/1/0/all/0/1">S. W. Barwick</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baum_V/0/1/0/all/0/1">V. Baum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bay_R/0/1/0/all/0/1">R. Bay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beatty_J/0/1/0/all/0/1">J. J. Beatty</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:+Tjus_J/0/1/0/all/0/1">J. Becker Tjus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+BenZvi_S/0/1/0/all/0/1">S. BenZvi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Berley_D/0/1/0/all/0/1">D. Berley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernardini_E/0/1/0/all/0/1">E. Bernardini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Besson_D/0/1/0/all/0/1">D. Z. Besson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Binder_G/0/1/0/all/0/1">G. Binder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bindig_D/0/1/0/all/0/1">D. Bindig</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blaufuss_E/0/1/0/all/0/1">E. Blaufuss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blot_S/0/1/0/all/0/1">S. Blot</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bohm_C/0/1/0/all/0/1">C. Bohm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Borner_M/0/1/0/all/0/1">M. Börner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boser_S/0/1/0/all/0/1">S. Böser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Botner_O/0/1/0/all/0/1">O. Botner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bourbeau_E/0/1/0/all/0/1">E. Bourbeau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bourbeau_J/0/1/0/all/0/1">J. Bourbeau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bradascio_F/0/1/0/all/0/1">F. Bradascio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Braun_J/0/1/0/all/0/1">J. Braun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bretz_H/0/1/0/all/0/1">H.-P. Bretz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bron_S/0/1/0/all/0/1">S. Bron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brostean_Kaiser_J/0/1/0/all/0/1">J. Brostean-Kaiser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burgman_A/0/1/0/all/0/1">A. Burgman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Busse_R/0/1/0/all/0/1">R. S. Busse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carver_T/0/1/0/all/0/1">T. Carver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_C/0/1/0/all/0/1">C. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cheung_E/0/1/0/all/0/1">E. Cheung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chirkin_D/0/1/0/all/0/1">D. Chirkin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clark_K/0/1/0/all/0/1">K. Clark</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Classen_L/0/1/0/all/0/1">L. Classen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Collin_G/0/1/0/all/0/1">G. H. Collin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Conrad_J/0/1/0/all/0/1">J. M. Conrad</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coppin_P/0/1/0/all/0/1">P. Coppin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Correa_P/0/1/0/all/0/1">P. Correa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cowen_D/0/1/0/all/0/1">D. F. Cowen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cross_R/0/1/0/all/0/1">R. Cross</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dave_P/0/1/0/all/0/1">P. Dave</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andre_J/0/1/0/all/0/1">J. P. A. M. de André</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clercq_C/0/1/0/all/0/1">C. De Clercq</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DeLaunay_J/0/1/0/all/0/1">J. J. DeLaunay</a>, et al. (272 additional authors not shown)
Many Galactic sources of gamma rays, such as supernova remnants, are expected
to produce neutrinos with a typical energy cutoff well below 100 TeV. For the
IceCube Neutrino Observatory located at the South Pole, the southern sky,
containing the inner part of the Galactic plane and the Galactic Center, is a
particularly challenging region at these energies, because of the large
background of atmospheric muons. In this paper, we present recent advancements
in data selection strategies for track-like muon neutrino events with energies
below 100 TeV from the southern sky. The strategies utilize the outer detector
regions as veto and features of the signal pattern to reduce the background of
atmospheric muons to a level which, for the first time, allows IceCube
searching for point-like sources of neutrinos in the southern sky at energies
between 100 GeV and several TeV in the muon neutrino charged current channel.
No significant clustering of neutrinos above background expectation was
observed in four years of data recorded with the completed IceCube detector.
Upper limits on the neutrino flux for a number of spectral hypotheses are
reported for a list of astrophysical objects in the southern hemisphere.
Many Galactic sources of gamma rays, such as supernova remnants, are expected
to produce neutrinos with a typical energy cutoff well below 100 TeV. For the
IceCube Neutrino Observatory located at the South Pole, the southern sky,
containing the inner part of the Galactic plane and the Galactic Center, is a
particularly challenging region at these energies, because of the large
background of atmospheric muons. In this paper, we present recent advancements
in data selection strategies for track-like muon neutrino events with energies
below 100 TeV from the southern sky. The strategies utilize the outer detector
regions as veto and features of the signal pattern to reduce the background of
atmospheric muons to a level which, for the first time, allows IceCube
searching for point-like sources of neutrinos in the southern sky at energies
between 100 GeV and several TeV in the muon neutrino charged current channel.
No significant clustering of neutrinos above background expectation was
observed in four years of data recorded with the completed IceCube detector.
Upper limits on the neutrino flux for a number of spectral hypotheses are
reported for a list of astrophysical objects in the southern hemisphere.
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