Dataset: Muon Neutrino Effective Areas

About this Dataset

Muon Neutrino Effective Areas

Total 2001 entries
It can be useful for ML based on the average effective area across a bin -- A _ Eff _ cm2
It can be useful for ML based on prediction E _ nu / GeV _ min or E _ nu / GeV _ max

BE CAREFULL WITH ZEROS(0)

COLUMNS:

E _ nu / GeV _ min
E _ nu / GeV _ max
Dec _ nu _ min _ deg
Dec _ nu _ max _ deg
A _ Eff _ cm2

The events contained in this release correspond to the IceCube's time-integrated point source search with 10 years of data [2]. Please refer to the description of the sample and known changes in the text at [1].

The data contained in this release of IceCube’s point source sample shows evidence of a cumulative excess of events from four sources (NGC 1068, TXS 0506+056, PKS 1424+240, and GB6 J1542+6129) from a catalogue of 110 potential sources. NGC 1068 gives the largest excess and is coincidentally the hottest spot in the full Northern sky search [1].

Data from IC86-2012 through IC86-2014 used in [2] use an updated selection and reconstruction compared to the 7 year time-integrated search [3] and the detection of the 2014-2015 neutrino flare from the direction of TXS 0506+056 [4]. The 7 year and 10 year versions of the sample show overlaps of between 80 and 90%.

An a posteriori cross check of the updated sample has been performed on TXS 0506+056 showing two previously-significant cascade-like events removed in the newer sample. These two events occur near the blazar's position during the TXS flare and give large reconstructed energies, but are likely not well-modeled by the track-like reconstructions included in this selection. While the events are unlikely to be track-like, their contribution to previous results has been handled properly.

While the significance of the 2014-2015 TXS 0505+56 flare has decreased from p=7.0e-5 to 8.1e-3, the change is a result of changes to the sample and not of increased data. No problems have been identified with the previously published results and since we have no reason a priori to prefer the new sample over the old sample, these results do not supercede those in [4].

This release contains data beginning in 2008 (IC40) until the spring of 2018 (IC86-2017). This release duplicates and supplants previously released data from 2012 and earlier. Events from this release cannot be combined with any other releases.

The effective area is a property of the detector and selection which, when convolved with a flux model, gives the expected rate of events in the detector. Here we release the muon neutrino effective areas for each season of data.

The effective areas are averaged over bins using simulated muon neutrino events ranging from 100 GeV to 100 PeV. Because the response varies widely in both energy and declination, we provide the tabulated response in these two dimensions. Due to IceCube's unique position at the south pole, the effective area is uniform in right ascension for timescales longer than 1 day. It varies by about 10% as a function of azimuth, an effect which may be important for shorter timescales.

log10(E_nu/GeV)_min, log10(E_nu/GeV)_max: The minimum and maximum of the energy bin used to caclulate the average effective area. Note that this uses the neutrino's true energy and not the reconstructed muon energy.
Dec_nu_min[deg], Dec_nu_max[deg]: The minimum and maximum of the declination of the neutrino origin. Again, note that this is the true direction of the neutrino and not the reconstructed muon direction.
A _ Eff _ cm2: The average effective area across a bin.

References:
[1] IceCube Data for Neutrino Point-Source Searches: Years 2008-2018, [[ArXiv link]]
[2] Time-integrated Neutrino Source Searches with 10 years of IceCube Data, Phys. Rev. Lett. 124, 051103 (2020)
[3] All-sky search for time-integrated neutrino emission from astrophysical sources with 7 years of IceCube data, Astrophys. J., 835 (2017) no. 2, 151
[4] Neutrino emission from the direction of the blazar TXS 0506+056 prior to the IceCube-170922A alert, Science 361, 147-151 (2018)
[5] Energy Reconstruction Methods in the IceCube Neutrino Telescope, JINST 9 (2014), P03009
[6] Methods for point source analysis in high energy neutrino telescopes, Astropart.Phys.29:299-305,2008

Last Update:
28 January 2021

Tables

Ic40 Effectivearea Ic40 Effectivearea

@kaggle.brsdincer_muon_neutrino_effective_areas.ic40_effectivearea_ic40_effectivearea

17.68 KB
2000 rows
5 columns


CREATE TABLE ic40_effectivearea_ic40_effectivearea (
  "e_nu_gev_min" DOUBLE,
  "e_nu_gev_max" DOUBLE,
  "dec_nu_min_deg" DOUBLE,
  "dec_nu_max_deg" DOUBLE,
  "a_eff_cm2" DOUBLE
);

Ic59 Effectivearea Ic59 Effectivearea

@kaggle.brsdincer_muon_neutrino_effective_areas.ic59_effectivearea_ic59_effectivearea

17.23 KB
2000 rows
5 columns


CREATE TABLE ic59_effectivearea_ic59_effectivearea (
  "e_nu_gev_min" DOUBLE,
  "e_nu_gev_max" DOUBLE,
  "dec_nu_min_deg" DOUBLE,
  "dec_nu_max_deg" DOUBLE,
  "a_eff_cm2" DOUBLE
);

Ic79 Effectivearea Ic79 Effectivearea

@kaggle.brsdincer_muon_neutrino_effective_areas.ic79_effectivearea_ic79_effectivearea

17.31 KB
2000 rows
5 columns


CREATE TABLE ic79_effectivearea_ic79_effectivearea (
  "e_nu_gev_min" DOUBLE,
  "e_nu_gev_max" DOUBLE,
  "dec_nu_min_deg" DOUBLE,
  "dec_nu_max_deg" DOUBLE,
  "a_eff_cm2" DOUBLE
);

Ic86 Ii Effectivearea Ic86 Ii Effectivearea

@kaggle.brsdincer_muon_neutrino_effective_areas.ic86_ii_effectivearea_ic86_ii_effectivearea

17.97 KB
2000 rows
5 columns


CREATE TABLE ic86_ii_effectivearea_ic86_ii_effectivearea (
  "e_nu_gev_min" DOUBLE,
  "e_nu_gev_max" DOUBLE,
  "dec_nu_min_deg" DOUBLE,
  "dec_nu_max_deg" DOUBLE,
  "a_eff_cm2" DOUBLE
);

Ic86 I Effectivearea Ic86 I Effectivearea

@kaggle.brsdincer_muon_neutrino_effective_areas.ic86_i_effectivearea_ic86_i_effectivearea

17.36 KB
2000 rows
5 columns


CREATE TABLE ic86_i_effectivearea_ic86_i_effectivearea (
  "e_nu_gev_min" DOUBLE,
  "e_nu_gev_max" DOUBLE,
  "dec_nu_min_deg" DOUBLE,
  "dec_nu_max_deg" DOUBLE,
  "a_eff_cm2" DOUBLE
);