Clark+ (2012a); Clark (PhD T., 2015) Tycho’s SNR in Herschel-SPIRE (250, 350, 500 μm) Kepler’s SNR in Herschel-SPIRE (250, 350, 500 μm) Negligible dust manufactured by Type-Ia supernovæ Which means all the iron depleted into dust got there some other way
Clark (PhD T., 2015) Synchrotron @ 160 μm Hot dust @ 160 μm Cold dust @ 160 μm We found 0.11 M☉ of supernova dust in the Crab Nebula Subsequent studies report values across 0.04–0.22 M☉ range
from Herschel maps during the data reduction Herschel data therefore missing lowest density ISM, whilst IRAS (& Planck) data missing highest density ISM Extended Emission Missing from Herschel IRAS 100 μm 300” resolution Herschel 100 μm 10” resolution
(in prep.); Gordon+ (2014) Dust Density Dust Temperature β2 β1 Break Wavelength 500um Excess Every pixel’s Spectral Energy Distribution (SED) fit using a broken- emissivity modified blackbody model. (Note, these figures are rotated 90° clockwise from North.) LMC SMC M31 M33
prep.) Over 1 dex increases in G/D with density suggest very significant grain growth H surface density values on x-axis have been corrected for inclination. We can probe to 10x higher densities in LMC and SMC, because they are ~10x closer than M31 and M33, hence have ~10x better density resolution.
(2015) Near-IR VIKING Ks Optical SDSS gri H-ATLAS 250 µm GALEX Far-UV Very blue (flux ratio FUV/Ks > 25), flocculent, HI-dominated galaxies make up the majority of a blind low-z blind 250 µm selected survey.
prep.); Clark+ (2019) Fainter points: Dust mass absorption coefficient is constant Bold points: Dust mass absorption coefficient falls according to power law of -0.4 above a transition density (M31 & M33 transition density = 4 M⊙ pc-2 LMC transition density = 40 M⊙ pc-2)
positions Random shuffle 1 Random shuffle 2 Random shuffle 3 Coords are shuffled to random positions offset in Galactic longitude, between -10 and +10 deg (but not within 1.5 deg of actual source coord).