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“So what do you do?” Chris Clark Pieter De Vis (IAS Paris) Sam Verstocken (Gent) Loretta Dunne (Cardiff) Haley Gomez (Cardiff) Simone Bianchi (Florence)

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“So what do you do?” Chris Clark Pieter De Vis (IAS Paris) Sam Verstocken (Gent) Loretta Dunne (Cardiff) Haley Gomez (Cardiff) Simone Bianchi (Florence) !

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Literature Values for κd Chris Clark Alton+ (2004); Demyk+ (2013); Köhler+ (2015); Clark+ (2016); Jones+ (2017); Clark+ (in prep.)

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Estimating κd with the HRS Chris Clark James+ (2002); Ciesla+ (2012); Clark+ (2016) κ500 = 0.051 m2 kg-1 (± 0.24 dex)

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Literature Values for κd Chris Clark Alton+ (2004); Demyk+ (2013); Köhler+ (2015); Clark+ (2016); Jones+ (2017); Clark+ (in prep.)

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M74 (NGC 628) & M83 (NGC 5236) Chris Clark Casasola+ (2017); Clark+ (2018); Clark+ (in prep.)

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Metallicity Map for M74 Chris Clark De Vis+ (in prep.); Clark+ (in prep.)

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SED-Fitting Example Chris Clark Clark+ (in prep.)

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Maps of κd across M74 & M83 Chris Clark Clark+ (in prep.)

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Gas Surface Density Against κd Chris Clark Clark+ (in prep.)

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Literature Values for κd Chris Clark Alton+ (2004); Demyk+ (2013); Köhler+ (2015); Clark+ (2016); Jones+ (2017); Clark+ (in prep.)

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BADGRS (Blue & Dusty Gas Rich Sources) Chris Clark Clark+ (2015); Dunne+ (2018) Near-IR VIKING Ks Optical SDSS gri Herschel 250 µm GALEX Far-UV

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Lots of Dust, Little Attenuation Chris Clark Clark+ (2015); Dunne+ (2018) More Extinction Less Extinction Dust Rich Dust Poor

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Dust from Evolved Stars Chris Clark Gomez+ (2012a); Gomez+ 2012(b); Clark (2015) Crab 160um Synchrotron Crab 160um Warm Dust Crab 160um Cold Dust

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Biology‽ Chris Clark https://github.com/Stargrazer82301/AstroCell Crab 160um Synchrotron Crab 160um Warm Dust Crab 160um Cold Dust

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Jack-Knife Cross-Validation Chris Clark De Vis+ (in prep.); Clark+ (in prep.)

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But... Chris Clark Mattsson+ (2012); Mattsson+ (2014); De Vis+ (in prep.); Clark+ (in prep.) How reliable are these findings, given that the method assumes a constant dust-to-metal ratio?

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Dust-to-Metals via Depletions • Wiseman+ (2016) and De Cia+ (2016) find DTM varies with metallicity, from DLA depletions; but for metallicities of >0.1 Z☉ this variation is less than factor of ≤2. • Jenkins+ (2009) find Milky Way variation of factor ≤2.7. Chris Clark De Cia+ (2016); Wiseman+ (2016); Clark+ (in prep.) Figure 7 from Wiseman+ (2016) Figure 15 from De Cia+ (2016) log10 (Z/Z☉ )

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Dust-to-Metals in Simulations 6 7 8 9 10 12+log10 (O/H) Chris Clark McKinnon+ (2016); Popping+ (2017); Clark+ (in prep.) Figure 5 from Popping+ (2017) Figure 15 from McKinnon+ (2016) • Popping+ (2017) find DTM varies by factor of <4 at metallicities >0.1 Z☉ in semi-analytic models. • McKinnon+ (2016) find DTM varies by factor of ≤3.5 at z<0.5 in hydrodynamical zoom-in simulations.

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Dust-to-Metals in THEMIS Chris Clark Jones+ (2017); Jones+ (2018); Clark+ (in prep.) • Dust-to-metals expected to vary by factor of ~3.6 in THEMIS dust model (Jones+ 2017;2018). • However, Jones+ predicts larger DTM in denser environments – which would actually increase the variation in κd compared to what we get from fixed DTM! Table 3 from Jones+ (2018)