Table A.1.
Overview of the data sets used in this study.
| Mission/ survey | Astrophysical contribution | Frequency range | Maps | References |
|---|---|---|---|---|
| Haslam radio | Synchrotron radiation from the interactions of cosmic ray electrons with magnetic fields in the ISM. | 408 MHz | 1 | Haslam et al. (1982), Remazeilles et al. (2015) |
| Reich radio | 1420 MHz | 1 | Reich (1982), Reich & Reich (1986), Reich et al. (2001) | |
| HI line emission radio | Emission from atomic hydrogen hyper fine level transitions. Proxy of the atomic hydrogen column density. | 21 cm | 1 | HI4PI Collaboration (2016) |
| Planck microwave | Low frequency range is dominated by synchrotron emission, high frequency range by thermal dust emission. Further emission originates from the CO-line, spinning dust (rotating dust grains), free-free (electron-ion collisions), and the CMB. | 30–857 GHz | 9 | Planck Collaboration I (2016) |
| AKARI far-infrared | Thermal dust emission. | 90–160 μm | 3 | Doi et al. (2015) |
| IRIS infrared | 12–100 μm | 4 | Neugebauer et al. (1984), Miville-Deschênes & Lagache (2005) | |
| Hα line emission | Hydrogen transitions from the second to the first excited state. Proxy for the amount of warm to hot, partly ionized diffuse gas in the vicinity of the Sun (as self-absorbed). | 656.3 nm | 1 | Dennison et al. (1999), Gaustad et al. (2001), Madsen et al. (2001), Finkbeiner (2003) |
| ROSAT X-ray | Emission from hot, largely ionized gas regions of the ISM with typically low density. | 0.197–1.545 keV | 6 | Snowden et al. (1995, 1997), Freyberg (1998), Freyberg & Egger (1999) |
| Fermi γ-ray | Low energy range is dominated by hadronic interactions of cosmic ray protons with the ISM, high energy range is dominated by leptonic interactions of cosmic ray electrons with the Galactic photon field (inverse-Compton scattering). | 0.85–217.22 GeV | 9 | Atwood et al. (2009), Ackermann et al. (2012), Selig et al. (2015) |
Notes. Data was preprocessed by Müller et al. (2018) as described in Sect. 2.1. Our data compilation D consists of 35 all-sky maps at different frequencies. The columns of the table specify (1) the mission or survey which provided the corresponding maps, (2) the astrophysical origin of the brightness in the maps, (3) the frequency or wavelength range, (4) the number of maps that belong to the specific mission or survey, and (5) the corresponding bibliographic reference.
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