Diffuse Emission of High-Energy Neutrinos from a Global Fit to Cosmic Rays

Model of diffuse emission of high-energy neutrinos from a global fit of cosmic rays and model of high-energy neutrino emission from unresolved pulsar-powered sources. The maps presented in the form of <em>HEALPix </em>maps (Gorski et al 2005, ApJ, 622, 759) of per-flavor intensity in units of GeV^-1 cm^-2 s^-1 sr^-1 at 50 logarithmically spaced energies between 10 GeV and 10⁸ GeV. We use a value of NSIDE=256 and the RING binning scheme. We here make available our fiducial model, which is calculated assuming the <em>Ferrière 2001</em> cosmic ray source distribution, the <em>AAfrag</em> hadronic production cross sections and the <em>GALPROP</em> gas maps. We calculated the emission from unresolved sources following Vecchiotti et al. 2022, ApJ, 928, 19. In Version 2 of this dataset, we also make available the local cosmic ray fluxes of our fiducial model obtained from a global fit to cosmic ray data together with the corresponding 68% and 95% uncertainty bands. These are shown in figure 6 of arXiv:2211.15607. The nuclear fluxes are in (GeV/n)^-1 m^-2 s^-1 sr^-1, the fluxes of electrons and positrons are in GeV^-1 m^-2 s^-1 sr^-1 . The fluxes are local interstellar fluxes without solar modulation. In Version 3 of this dataset, we add the fiducial diffuse gamma ray model calculated assuming the <em>Ferrière 2001</em> cosmic ray source distribution, the <em>AAfrag</em> hadronic production cross sections as well as the <em>GALPROP</em> gas maps and ISRF model. We separately make available 3 maps: The hadronic emission on neutral atomic gas, the hadronic emission on molecular gas and the leptonic emission from Inverse Compton Scattering. Similar to the dataset of the fiducial neutrino model, the maps are presented in the form of <em>HEALPix </em>maps (Gorski et al 2005, ApJ, 622, 759) in units of GeV^-1 cm^-2 s^-1 sr^-1. We use a value of NSIDE=256 and the RING binning scheme. For the hadronic maps, the intensity is given at 50 logarithmically spaced energies between 10 GeV and 10⁸ GeV. For the leptonic maps from Inverse Compton Scattering, the intensity is given at 48 logarithmically spaced energies between 1 GeV and 10⁶ GeV. The structure of the files is somewhat different from the file containing the fiducial neutrino model. This is to allow for easy use of the gamma ray maps with the <em>gammapy</em> package (Deil et al. 2017, arXiv:1709.01751). Also available in Version 3 are the full spatio-spectral cosmic ray distributions in the Milky Way as predicted by our fiducial model. The nuclear fluxes are given for each species in (GeV/n)^-1 m^-2 s^-1 sr^-1 at 63 energies between 1 GeV and 10⁹ GeV. The leptonic fluxes are given for each species in GeV^-1 m^-2 s^-1 sr^-1 at 36 energies between 1 GeV and 10⁵ GeV. All fluxes are given on a spatial grid at 81 galactocentric radii from 0 kpc to 20 kpc and 61 distances perpendicular to the galactic plane between -6 kpc and 6 kpc. Finally, a word of caution about the extra component of cosmic ray leptons included in our model: This component is contained in the last <em>HDUnit</em> of the <em>fits</em> file containing the leptonic cosmic ray distributions. It is there denoted as a flux of electrons. It must, however, also be added to the flux of positrons to achieve correct results. Please refer to arXiv:2211.15607 for further details. When using these models in your research work, please refer to this Zenodo dataset and the publication.本数据集包含基于宇宙线全局拟合得到的高能中微子弥散辐射模型，以及来自未解析脉冲星驱动源的高能中微子辐射模型。相关分布图以HEALPix格式呈现，给出每种中微子风味的强度，单位为GeV⁻¹ cm⁻² s⁻¹ sr⁻¹，能量范围覆盖10 GeV至10^8 GeV，共50个对数间隔的能量点。我们采用NSIDE=256的参数值与RING分箱方案。 本数据集提供我们的基准模型，该模型基于Ferrière 2001提出的宇宙射线源分布、AAfrag强子产生截面以及GALPROP气体分布图计算得到。我们参照Vecchiotti等人2022年（ApJ, 928, 19）的研究计算了未解析源的辐射信号。 在本数据集的V2版本中，我们还提供了通过宇宙线数据全局拟合得到的基准模型的局地宇宙线通量，及其对应的68%与95%置信区间不确定度带。相关内容详见arXiv:2211.15607的图6。核通量的单位为(GeV/n)⁻¹ m⁻² s⁻¹ sr⁻¹，电子与正电子通量的单位为GeV⁻¹ m⁻² s⁻¹ sr⁻¹。所有通量均为未考虑太阳调制的局地星际通量。 在本数据集的V3版本中，我们新增了基于Ferrière 2001宇宙射线源分布、AAfrag强子产生截面、GALPROP气体分布图以及星际辐射场（ISRF）模型计算得到的基准弥散伽马射线模型。我们单独提供了三类分布图：中性原子气体上的强子辐射分布图、分子气体上的强子辐射分布图，以及逆康普顿散射产生的轻子辐射分布图。 与基准中微子模型数据集一致，该分布图采用HEALPix格式（Gorski等人2005年，ApJ, 622, 759），单位为GeV⁻¹ cm⁻² s⁻¹ sr⁻¹，同样采用NSIDE=256参数与RING分箱方案。强子辐射分布图的强度计算覆盖10 GeV至10^8 GeV的50个对数间隔能量点；而逆康普顿散射轻子辐射分布图的强度则覆盖1 GeV至10^6 GeV的48个对数间隔能量点。 该数据集的文件结构与基准中微子模型数据集略有不同，这是为了便于使用Gammapy工具包（Deil等人2017年，arXiv:1709.01751）加载伽马射线分布图。V3版本还提供了基准模型预测的银河系全域时空光谱宇宙线分布数据。每种核组分的通量单位为(GeV/n)⁻¹ m⁻² s⁻¹ sr⁻¹，覆盖1 GeV至10^9 GeV的63个能量点；每种轻组分的通量单位为GeV⁻¹ m⁻² s⁻¹ sr⁻¹，覆盖1 GeV至10^5 GeV的36个能量点。所有通量均采用空间网格存储，包含81个银心半径数据点（范围0 kpc至20 kpc）以及61个银道面垂直距离数据点（范围-6 kpc至6 kpc）。 最后，请注意本模型中包含的额外宇宙线轻子组分：该组分存储于轻子宇宙线分布FITS文件的最后一个HDU（表头数据单元）中，其被标记为电子通量。但为获得正确结果，该通量需同时叠加至正电子通量中。更多细节请参阅arXiv:2211.15607。 若在研究工作中使用本模型，请引用本Zenodo数据集及相关发表论文。