Constraints on Neutrino Emission from Nearby Galaxies Using the 2MASS Redshift Survey and IceCube. (arXiv:1911.11809v1 [astro-ph.HE])

Constraints on Neutrino Emission from Nearby Galaxies Using the 2MASS Redshift Survey and IceCube. (arXiv:1911.11809v1 [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:+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:+V%2E_A/0/1/0/all/0/1">A. Balagopal V.</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:+Bastian_B/0/1/0/all/0/1">B. Bastian</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:+Baur_S/0/1/0/all/0/1">S. Baur</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:+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:+Bottcher_J/0/1/0/all/0/1">J. Böttcher</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:+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:+Buscher_J/0/1/0/all/0/1">J. Buscher</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:+Choi_S/0/1/0/all/0/1">S. Choi</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:+Coleman_A/0/1/0/all/0/1">A. Coleman</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:+Clercq_C/0/1/0/all/0/1">C. De Clercq</a>, et al. (293 additional authors not shown)

The distribution of galaxies within the local universe is characterized by
anisotropic features. Observatories searching for the production sites of
astrophysical neutrinos can take advantage of these features to establish
directional correlations between a neutrino dataset and overdensities in the
galaxy distribution in the sky. The results of two correlation searches between
a seven-year time-integrated neutrino dataset from the IceCube Neutrino
Observatory, and the 2MASS Redshift Survey (2MRS) catalog are presented here.
The first analysis searches for neutrinos produced via interactions between
diffuse intergalactic Ultra-High Energy Cosmic Rays (UHECRs) and the matter
contained within galaxies. The second analysis searches for low-luminosity
sources within the local universe, which would produce subthreshold multiplets
in the IceCube dataset that directionally correlate with galaxy distribution.
No significant correlations were observed in either analyses. Constraints are
presented on the flux of neutrinos originating within the local universe
through diffuse intergalactic UHECR interactions, as well as on the density of
standard candle sources of neutrinos at low luminosities.

http://arxiv.org/icons/sfx.gif