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| Acronym | Expression |
| 3D | 3-Dimensional |
| ACF | AutoCorrelation Function |
| AGB | Asymptotic Giant Branch stars |
| AGN | Active Galactic Nucleus |
| AME | Anomalous Microwave Emission |
| BCD | Blue Compact Dwarf Galaxies |
| BEMBB | Broken-Emissivity Modified Black Body |
| BG | Big Grain |
| BH | Black Hole |
| CCD | Charge-Coupled Device |
| CDF | Cumulative Distribution Function |
| CGS | Centimetre-Gram-Second |
| CIB | Cosmic Infrared Background |
| CMB | Cosmic Microwave Background |
| CNP | Cosmic NanoParticles |
| CNM | Cold Neutral Medium |
| DCD | Disordered Charge Distribution |
| DDA | Discrete Dipole Approximation |
| DGL | Diffuse Galactic Light |
| DGS | Dwarf Galaxy Sample |
| DIB | Diffuse Interstellar Bands |
| DLA | Damped Lyman-Alpha systems |
| EMT | Effective Medium Theory |
| ERE | Extended Red Emission |
| ETG | Early-Type Galaxy |
| eVSG | evaporating Very Small Grains |
| FIR | Far-InfraRed |
| FUV | Far-UltraViolet |
| FWHM | Full Width at Half Maximum |
| GEMS | Glass with Embedded Metals and Sulfides |
| GRB | Gamma-Ray Burst |
| HB | Hierarchical Bayesian |
| HDR | Habilitation à Diriger des Recherches |
| HIM | Hot Ionized Medium |
| ICM | InterClump Medium |
| IDP | Interplanetary Dust Particles |
| iid | independent, identically distributed |
| IMF | Initial Mass Function |
| IR | InfraRed |
| ISD | InterStellar Dust |
| ISM | InterStellar Medium |
| ISRF | InterStellar Radiation Field |
| ISS | International Space Station |
| LIRG | Luminous InfraRed Galaxies |
| LMC | Large Magellanic Cloud |
| LIMS | Low- and Intermediate-Mass Stars |
| LTG | Late-Type Galaxy |
| MBB | Modified Black Body |
| MCRT | Monte-Carlo Radiative Transfer |
| MCMC | Markov Chain Monte-Carlo |
| MIR | Mid-InfraRed |
| MKS | Meter-Kilogram-Second |
| MKSA | Meter-Kilogram-Second-Ampere |
| ML | Machine-Learning |
| MLE | Maximum-Likelihood Estimation |
| MS | Main Sequence |
| MW | Milky Way |
| NHST | Null Hypothesis Significance Test |
| NIR | Near-InfraRed |
| NLP | Natural Language Processing |
| NS | Neutron Star |
| NUV | Near-UltraViolet |
| OOP | Out-Of-Plane |
| PAH | Polycyclic Aromatic Hydrocarbon |
| PCA | Principal Component Analysis |
| | Probability Density Function |
| PDR | PhotoDissociation Regions |
| PN | Planetary Nebula |
| ppb | part per billion |
| ppp | posterior predictive -value |
| QSO | Quasi-Stellar Object |
| RAT | Radiative Alignment Torques |
| SSC | Super Star Cluster |
| SED | Spectral Energy Distribution |
| SF | Star Formation |
| SFH | Star Formation History |
| SFR | Star Formation Rate |
| SI | International System of units |
| SLED | Spectral Line Energy Distribution |
| SMC | Small Magellanic Cloud |
| SN | SuperNova |
| SN Ia | Type Ia SuperNova |
| SN II | Type II SuperNova |
| SNR | SuperNova Remnant |
| sSFR | specific Star Formation Rate |
| SUE | Skewed Uncertainty Ellipse |
| TIR | Total InfraRed |
| TLS | Two-Level System |
| TPAGB | Thermally-Pulsing Asymptotic Giant Branch |
| TMA | Too Many Acronyms |
| UIB | Unidentified Infrared Bands |
| ULIRG | UltraLuminous InfraRed Galaxies |
| UV | UltraViolet |
| VCD | Very Cold Dust |
| VSG | Very Small Grain |
| YSO | Young Stellar Object |
| WD | White Dwarf |
| WIM | Warm Ionized Medium |
| WNM | Warm Neutral Medium |
| WR | Wolf Rayet star |
| ZAMS | Zero-Age Main Sequence |
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| Acronym | Telescope or Instrument |
| ALMA | Atacama Large Millimeter/submillimeter Array |
| APEX | Atacama Pathfinder Experiment |
| ATHENA | Advanced Telescope for High ENergy Astrophysics |
| BLAST | Balloon-borne Large Aperture Submillimeter Telescope |
| COBE | COsmic Background Explorer |
| CSO | Caltech Submilleter Observatory |
| DIRBE | Diffuse Infrared Background Experiment |
| DMR | Differential Microwave Radiometer |
| FIRAS | Far-InfraRed Absolute Spectrophotometer |
| FIS | Far-Infrared Surveyor |
| FUSE | Far Ultraviolet Spectroscopic Explorer |
| FTS | Fourier Transform Spectrometer |
| HFI | High Frequency Instrument |
| HIFI | Heterodyne Instrument for the Far-Infrared |
| HST | Hubble Space Telescope |
| IRAC | InfraRed Array Camera |
| IRAM | Institut de RadioAstronomie Millimétrique |
| IRAS | InfraRed Astronomical Satellite |
| IRC | InfraRed Camera |
| IRS | InfraRed Spectrograph |
| IRTF | InfraRed Telescope Facility |
| ISO | Infrared Space Observatory |
| IUE | International Ultraviolet Explorer |
| JCMT | James Clerk Maxwell Telescope |
| JWST | James Webb Space Telescope |
| KAO | Kuiper Airborne Observatory |
| LFI | Low Frequency Instrument |
| MIPS | Multiband Imaging Photometer for Spitzer |
| MIRI | Mid-InfraRed Instrument |
| MUSE | Multi Unit Spectroscopic Explorer |
| NCT | Nuclear Compton Telescope |
| NIKA2 | New IRAM Kids Arrays |
| NIRcam | Near-InfraRed Camera |
| NIRISS | Near-InfraRed Imager and Slitless Spectrograph |
| NIRspec | Near-InfraRed Spectrograph |
| OAO | Orbiting Astronomical Observatory |
| PACS | Photodetector Array Camera and Spectrometer |
| PILOT | Polarized Instrument for the Long-wavelength Observation of the Tenuous ISM |
| PRONAOS | PROjet National pour l’Observation Submillimétrique |
| SOFIA | Stratospheric Observatory for Infrared Astronomy |
| SPICA | SPace Infrared telescope for Cosmology and Astrophysics |
| SPIRE | Spectral and Photometric Imaging REceiver |
| UKIRT | United Kingdom InfraRed Telescope |
| VLT | Very Large Telescope |
| WIRO | Wyoming InfraRed Observatory |
| WISE | Wide-field Infrared survey Explorer |
| WMAP | Wilkinson Microwave Anisotropy Probe |
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| Acronym | Model Name |
| DGS | Dwarf Galaxy Survey |
| DustPedia | A definitive study of dust in the local Universe |
| HerBIE | HiERarchical Bayesian Inference for dust Emission |
| HERITAGE | HERschel Inventory of The Agents of Galaxy Evolution |
| SAGE | Surveying the Agents of Galaxy Evolution |
| THEMIS | The Heterogeneous Evolution Model for Interstellar Solids |
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Table A.4 gives the acronyms and spectral ranges of the most important electromagnetic domains. For each domain, we give the interval in photon wavelength, frequency and energy. There are slight variations of these intervals across the literature. The physical phenomena listed in the right column are indicative of the typical most dominant emission at the scale of a galaxy. Fig. A.1 shows where these different domains fall on the SED of a nearby galaxy.
| Abbreviation | Name | Spectral range | Predominant physical origin |
|
| Start | End |
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| HIGH ENERGIES
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| rays | … | 0.01 nm | Cosmic rays |
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| … | 30 EHz |
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| … | 0.12 GeV |
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| X | X rays | 0.01 nm | 10 nm | Accretion disks & coronal plasmas |
| 30 EHz | 0.03 EHz |
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| 120 keV | 0.12 keV |
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| UV-VISIBLE
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| EUV | Extreme-UV | 10 nm | 124 nm | Massive stars |
| 30 PHz | 2.4 PHz |
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| 120 eV | 10 eV |
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| FUV | Far-UltraViolet | 124 nm | 200 nm | Massive stars |
| 2.4 PHz | 1.5 PHz |
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| 10 eV | 6.2 eV |
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| NUV | Near-UV | 200 nm | 380 nm | Massive stars |
| 1.5 PHz | 0.8 PHz |
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| 6.2 eV | 3.3 eV |
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| vis. | Visible | 0.38 | 0.8 | Intermediate & low-mass stars |
| 0.8 PHz | 0.4 PHz |
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| 3.3 eV | 1.5 eV |
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| COLD UNIVERSE
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| NIR | Near-InfraRed | 0.8 | 5 | Circumstellar material |
| 400 THz | 60 THz |
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| 1.5 eV | 0.25 eV |
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| MIR | Mid-InfraRed | 5 | 40 | Aromatic features & hot dust |
| 60 THz | 7.5 THz |
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| 250 meV | 30 meV |
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| FIR | Far-InfraRed | 40 | 200 | Large ISM grains |
| 7.5 THz | 1.5 THz |
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| 30 meV | 6 meV |
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| submm | Submillimeter | 200 | 800 | Cold dust |
| 1.5 THz | 0.4 THz |
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| 6 meV | 1.5 meV |
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| RADIO/MICROWAVE
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| mm | Millimeter | 0.8 mm | 5 mm | Cold dust & free-free |
| 400 GHz | 60 GHz |
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| 1.5 meV | 0.25 meV |
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| cm | Centimeter | 0.5 cm | 6 cm | Free-free & synchrotron |
| 60 GHz | 5 GHz |
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| 250 eV | 20 eV |
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