Sharpening up Galactic all-sky maps with complementary data - A machine learning approach


This page contains the simulated maps as well as the reconstructions of the simulated and observed all-sky maps from arxiv:1806.04161

The results are provided in PDF and FITS (HEALPix) format. The FITS files can be accessed by, e.g., NIFTy, a Python module.

You can Download all as .zip file.

Description PDF File Data File
Simulation Mock I mock1.pdf mock1.fits
Simulation Mock II mock2.pdf mock2.fits
Simulation Mock III mock3.pdf mock3.fits
Simulation Mock IV mock4.pdf mock4.fits
Simulation Mock V mock5.pdf mock5.fits
Simulation Mock VI mock6.pdf mock6.fits
Smoothed map of Mock I mock1_smooth.pdf mock1_smooth.fits
     
Difference between Mock I and smoothed Mock I mock1-mock1_smooth.pdf mock1-mock1_smooth.fits
Prediction of Mock I mock1_pred.pdf mock1_pred.fits
Difference between Mock I and its prediction mock1-mock1_pred.pdf mock1-mock1_pred.fits
Prediction of the smoothed Mock I map mock1_smooth_pred.pdf mock1_smooth_pred.fits
Difference between Mock&thinksp;I and the prediction of the smoothed Mock I map mock1-mock1_smooth_pred.pdf mock1-mock1_smooth_pred.fits
Prediction of Mock I with only the disk information mock1_onlydisk_pred.pdf mock1_onlydisk_pred.fits
Difference between Mock I and the prediction with only the disk information mock1-mock1_onlydisk_pred.pdf mock1-mock1_onlydisk_pred.fits
Absolute values of the difference map between Mock I and the prediction with only the disk information mock1-mock1_onlydisk_pred_abs.pdf mock1-mock1_onlydisk_pred_abs.fits
Standard deviation of the prediction of Mock I with only the disk information mock1_onlydisk_pred_std.pdf mock1_onlydisk_pred_std.fits
Prediction of Mock I with the disk and only a small part of the southern hemisphere information mock1_diskpart_pred.pdf mock1_diskpart_pred.fits
Difference between Mock I and the prediction with the disk and only a small part of the southern hemisphere information mock1-mock1_diskpart_pred.pdf mock1-mock1_diskpart_pred.fits
Prediction of Mock I with the southern hemisphere information mock1_half_pred.pdf mock1_half_pred.fits
Difference between Mock I and the prediction with the southern hemisphere information mock1-mock1_half_pred.pdf mock1-mock1_half_pred.fits
     
Prediction of the 0.885 keV ROSAT map trained with K = 3 Gaussians rosat_pred_3.pdf rosat_pred_3.fits
Difference between the original and the predicted 0.885 keV ROSAT map trained with K = 3 Gaussians rosat-rosat_pred_3.pdf rosat-rosat_pred_3.fits
Prediction of the 0.885 keV ROSAT map trained with K = 18 Gaussians rosat_pred_18.pdf rosat_pred_18.fits
Difference between the original and the predicted 0.885 keV ROSAT map trained with K = 18 Gaussians rosat-rosat_pred_18.pdf rosat-rosat_pred_18.fits
Prediction of the 1.70 GeV FERMI map trained with K = 3 Gaussians fermi_pred_3.pdf fermi_pred_3.fits
Difference between the original and the predicted 1.70 GeV FERMI map trained with K = 3 Gaussians fermi-fermi_pred_3.pdf fermi-fermi_pred_3.fits
Prediction of the 1.70 GeV FERMI map trained with K = 18 Gaussians fermi_pred_18.pdf fermi_pred_18.fits
Difference between the original and the predicted 1.70 GeV FERMI map trained with K = 18 Gaussians fermi-fermi_pred_3.pdf fermi-fermi_pred_3.fits
Prediction of the hadronic component hadronic_pred.pdf hadronic_pred.fits
Difference between the original and the predicted hadronic component hadronic-hadronic_pred.pdf hadronic-hadronic_pred.fits
Prediction of the leptonic component leptonic_pred.pdf leptonic_pred.fits
Difference between the original and the predicted leptonic component leptonic-leptonic_pred.pdf leptonic-leptonic_pred.fits
Prediction of the hadronic component given the CO line emission, the Planck HFI maps, and the infrared regimes hadronic_pred_comp.pdf hadronic_pred_comp.fits
Difference between the predicted hadronic component and its prediction given the CO line emission, the Planck HFI maps, and the infrared regimes hadronic_pred-hadronic_pred_comp.pdf hadronic_pred-hadronic_pred_comp.fits
Prediction of the hadronic component given the radio continuum emission, the Planck LFI maps, and the X-ray regime hadronic_pred_nocomp.pdf hadronic_pred_nocomp.fits
Difference between the predicted hadronic component and its prediction given the radio continuum emission, the Planck LFI maps, and the X-ray regime hadronic_pred-hadronic_pred_nocomp.pdf hadronic_pred-hadronic_pred_nocomp.fits
Prediction of the leptonic component given the radio continuum emission, the Planck LFI maps, and the X-ray regime leptonic_pred_comp.pdf leptonic_pred_comp.fits
Difference between the predicted leptonic component and its prediction given the radio continuum emission, the Planck LFI maps, and the X-ray regime leptonic_pred-leptonic_pred_comp.pdf leptonic_pred-leptonic_pred_comp.fits
Prediction of the leptonic component given the CO line emission, the Planck HFI maps, and the infrared regimes leptonic_pred_nocomp.pdf leptonic_pred_nocomp.fits
Difference between the predicted leptonic component and its prediction given the CO line emission, the Planck HFI maps, and the infrared regimes leptonic_pred-leptonic_pred_nocomp.pdf leptonic_pred-leptonic_pred_nocomp.fits
Color coding of the probability of the individual GMM components for the magnitude vector of a pixel rgb.pdf r.fits g.fits b.fits

Contact

Ancla Müller

Astronomical Institut Ruhr-Universtät Bochum
Universitätsstraße 150
44801 Bochum
Germany


Torsten Enßlin

Max Planck Institute for Astrophysics
Karl Schwarzschild Straße 1
80741 Garching
Germany












Page last updated on 2018-03-07.