اشترك بالحزمة الذهبية واحصل على وصول غير محدود شمرا أكاديميا
تسجيل مستخدم جديدSearch for multi-messenger signals in NOvA coincident with LIGO/Virgo detections
95
0
0.0
(
0
)
اسأل ChatGPT حول البحث
ﻻ يوجد ملخص باللغة العربية
Using the NOvA neutrino detectors, a broad search has been performed for any signal coincident with 28 gravitational wave events detected by the LIGO/Virgo Collaboration between September 2015 and July 2019. For all of these events, NOvA is sensitive to possible arrival of neutrinos and cosmic rays of GeV and higher energies. For five (seven) events in the NOvA Far (Near) Detector, timely public alerts from the LIGO/Virgo Collaboration allowed recording of MeV-scale events. No signal candidates were found.
قيم البحث
اقرأ أيضاً
A search is performed for supernova-like neutrino interactions coincident with 76 gravitational wave events detected by the LIGO/Virgo Collaboration. For 40 of these events, full readout of the time around the gravitational wave is available from the
NOvA Far Detector. For these events, we set limits on the fluence of the sum of all neutrino flavors of $F < 7(4)times 10^{10}mathrm{cm}^{-2}$ at 90% C.L. assuming energy and time distributions corresponding to the Garching supernova models with masses 9.6(27)$mathrm{M}_odot$. Under the hypothesis that any given gravitational wave event was caused by a supernova, this corresponds to a distance of $r > 29(50)$kpc at 90% C.L. Weaker limits are set for other gravitational wave events with partial Far Detector data and/or Near Detector data.
We summarize initial results for high-energy neutrino counterpart searches coinciding with gravitational-wave events in LIGO/Virgos GWTC-2 catalog using IceCubes neutrino triggers. We did not find any statistically significant high-energy neutrino co
unterpart and derived upper limits on the time-integrated neutrino emission on Earth as well as the isotropic equivalent energy emitted in high-energy neutrinos for each event.
We report a search for a magnetic monopole component of the cosmic-ray flux in a 95-day exposure of the NOvA experiments Far Detector, a 14 kt segmented liquid scintillator detector designed primarily to observe GeV-scale electron neutrinos. No event
s consistent with monopoles were observed, setting an upper limit on the flux of $2times 10^{-14} mathrm{cm^{-2}s^{-1}sr^{-1}}$ at 90% C.L. for monopole speed $6times 10^{-4} < beta < 5times 10^{-3}$ and mass greater than $5times 10^{8}$ GeV. Because of NOvAs small overburden of 3 meters-water equivalent, this constraint covers a previously unexplored low-mass region.
Presented is the description of a new and general method used to search for $gamma$-ray counterparts to gravitational-wave (GW) triggers. This method is specifically applied to single GW detector triggers. Advanced LIGO data from observing runs O1 an
d O2 were analyzed, thus each GW trigger comes from either the LIGO-Livingston or the LIGO-Hanford interferometer. For each GW trigger, Fermi Gamma-ray Burst Monitor data is searched and the most significant subthreshold signal counterpart is selected. Then, a methodology is defined in order to establish which of GW-$gamma$-ray pairs are likely to have a common origin. For that purpose an association ranking statistic is calculated from which a false alarm rate is derived. The events with the highest ranking statistics are selected for further analysis consisting of LIGO detector characterization and parameter estimation. The $gamma$-ray signal characteristics are also evaluated. We find no significant candidates from the search.
We report constraints on light dark matter (DM) models using ionization signals in the XENON1T experiment. We mitigate backgrounds with strong event selections, rather than requiring a scintillation signal, leaving an effective exposure of $(22 pm 3)
$ tonne-days. Above $sim!0.4,mathrm{keV}_mathrm{ee}$, we observe $<1 , text{event}/(text{tonne} times text{day} times text{keV}_text{ee})$, which is more than one thousand times lower than in similar searches with other detectors. Despite observing a higher rate at lower energies, no DM or CEvNS detection may be claimed because we cannot model all of our backgrounds. We thus exclude new regions in the parameter spaces for DM-nucleus scattering for DM masses $m_chi$ within $3-6,mathrm{GeV}/mathrm{c}^2$, DM-electron scattering for $m_chi > 30,mathrm{MeV}/mathrm{c}^2$, and absorption of dark photons and axion-like particles for $m_chi$ within $0.186 - 1 , mathrm{keV}/mathrm{c}^2$.
سجل دخول لتتمكن من نشر تعليقات
التعليقات
جاري جلب التعليقات
سجل دخول لتتمكن من متابعة معايير البحث التي قمت باختيارها
