"So What Are You For, Exactly?" - ISM✻@ST Intro Talk

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“So, what are you for, exactly?” ISM✻@ST Intro Talk Chris Clark

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Chris Clark Clark & Redfern (1988) Helston

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Chris Clark Cardiff

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Chris Clark

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Chris Clark

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Chris Clark

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Chris Clark

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Chris Clark

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Chris Clark BBC (2009)

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Chris Clark Dust in Type-Ia SNe? Gomez & Clark+ (2012a); Clark (PhD T., 2015) Kepler’s Supernova (SN1604) Tycho’s Supernova (SN1572) (optical & X-ray images)

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Chris Clark Dust in Type-Ia SNe: Kepler’s SN Gomez & Clark+ (2012a); Clark (PhD T., 2015) Herschel-PACS (70, 100, 160 μm) Herschel-SPIRE (250, 350, 500 μm)

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Chris Clark Dust in Type-Ia SNe: Tycho’s SN Gomez & Clark+ (2012a); Clark (PhD T., 2015) Herschel-PACS (70, 100, 160 μm) Herschel-SPIRE (250, 350, 500 μm)

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Chris Clark Type-Ia SNe: Resolved Temps Gomez & Clark+ (2012a); Clark (PhD T., 2015) Kepler’s supernova; T hot (left) and T cold (right) Tycho’s supernova; T hot (left) and T cold (right) (Forgive the jet colour scale; I was young and didn’t know better!) Negligible dust manufactured by Type-Ia supernovæ Which means all the iron depleted into dust got there some other way

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Chris Clark Dust in a Type-II SN: The Crab (SN1054) Gomez+ inc. Clark (2012b); Clark (PhD T., 2015) Herschel-PACS (70, 100, 160 μm) Herschel-SPIRE (250, 350, 500 μm)

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Chris Clark Dust in a Type-II SN: The Crab (SN1054) Clark (PhD T., 2015)

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Chris Clark The Crab: Synchrotron Power Law Gomez+ inc. Clark (2012b); Clark (PhD T., 2015) Spectral index map

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Chris Clark The Crab: Component Separation Gomez+ inc. Clark (2012b); Clark (PhD T., 2015) Synchrotron @ 160 μm Hot dust @ 160 μm Cold dust @ 160 μm We found 0.11 M ☉ supernova dust in the Crab Nebula Subsequent studies report values across 0.04–0.22 M ☉ range

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Chris Clark Herschel-ATLAS (Herschel Astrophysical Terahertz Large Area Survey) Eales+ (2010)

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Chris Clark Dust-Detected H-ATLAS Low-z Galaxies Clark+ (2015) H-ATLAS 250 µm 15 < D < 45 Mpc SDSS gri-bands

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Chris Clark BADGRS: Blue & Dusty Gas Rich Sources Clark+ (2015) Near-IR VIKING Ks Optical SDSS gri H-ATLAS 250 µm GALEX Far-UV Very blue (flux ratio FUV/K s > 25), flocculent, HI-dominated galaxies make up the majority of a blind low-z blind 250 µm selected survey.

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Chris Clark BADGRS: Lots of Dust, Little Attenuation Clark+ (2015) More Attenuation Less Attenuation Dust Rich Dust Poor

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Chris Clark BADGRS: Lots of Dust, Little Attenuation Clark+ (2015) M D /M S ~ 0.0005 M D /M S ~ 0.01

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Chris Clark BADGRS: Lots of Dust, Little Attenuation Schofield (PhD, 2017)

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Chris Clark BADGRS: The Peak of Dust-Richness Clark+ (2015) Older Younger Dust Rich Dust Poor

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Chris Clark BADGRS: The Peak of Dust-Richness Clark+ (2015); De Vis (2017) Older Younger Dust Rich Dust Poor

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Chris Clark BADGRS: Many Chemical Evolution Paths? De Vis+ (2017); Schofield (PhD T., 2017) Older Younger Dust Rich Dust Poor

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Chris Clark BADGRS: Star Formation Still Ramping Up Schofield (PhD T., 2017)

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Chris Clark BADGRS: Super Low M H2 /M dust ? Dunne+ (2018) IRAM 30m CO(1–0) I CO = 0.2–2 K km s-1 FWHM = 30–100 km s-1 M H2 /M dust = 2–27 (Z-based X CO – MW X CO ) Z = 0.5–1 Z ☉

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Chris Clark BADGR Follow-Up: JINGLE (Preliminary) Saintonge+ (2018); Lamperti+ (2020); Clark+ (in prep.) More Attenuation Less Attenuation Dust Rich Dust Poor JINGLE JCMT dust & gas in Nearby Galaxies Legacy Exploration

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Chris Clark Literature Values for κd (the Mass Opacity Coeff) Alton+ (2004); Demyk+ (2013); Köhler+ (2015); Clark+ (2016); Jones+ (2017); Clark+ (2019) Several dex total range in κ d values. Commonly-used standard values span a factor of ~3 range

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Chris Clark Estimating κd with the HRS (the Herschel Reference Survey) Alton+ (2004); Demyk+ (2013); Köhler+ (2015); Clark+ (2016); Jones+ (2017); Clark+ (2019) κ 500 = 0.051 m2 kg-1 (± 0.24 dex)

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Chris Clark Biology‽

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Chris Clark DustPedia Database Davies+ (2017); Clark+ (2018) • The DustPedia sample (Davies+, 2017) covers all 875 nearby (D<40 Mpc) extended (1’ < D25 < 1°) galaxies observed by Herschel. • Standardised imagery & photometry spanning 42 UV–microwave bands (Clark+, 2018). • Homogenised atomic & molecular gas values for 764 & 255 DustPedia galaxies respectively (; De Vis+, 2019; Casasola+, 2020). • 10000 consistently-determined gas- phase metallicity datapoints (from IFU, slit, and fibre spectra) for 492 DustPedia galaxies (De Vis+, 2019). UV-NIR-FIR montage of some of the galaxies in the DustPedia database

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Chris Clark DustPedia Photometry Clark+ (2018) Robust automated aperture photometry for extended sources.

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Chris Clark DustPedia Photometry Clark+ (2018) Self-consistent photometry across many bands.

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Chris Clark Data for Mapping κd Within Galaxies Clark+ (2018); Clark+ (2019) M83 M74 But also need metallicity maps to calculate κ d . These don’t normally exist for nearby galaxies…

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Chris Clark Metallicity Mapping in Nearby Galaxies Clark+ (2019); De Vis+ (2019) Lots of individual metallicity points from individual metallicity spectra. But need to turn into metallicty map… M74 M83

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Chris Clark Gaussian Process Regression in M74 Clark+ (2019); De Vis+ (2019) M74 Metallicity Map M74 Metallicity Uncertainty

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Chris Clark Gaussian Process Regression in M83 Clark+ (2019); De Vis+ (2019) M83 Metallicity Map M83 Metallicity Uncertainty

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Chris Clark Maps of κd in Nearby Galaxies! Clark+ (2018); Clark+ (2019) M74 κ d map M83 κ d map UV-NIR-FIR image for reference UV-NIR-FIR image for reference

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Chris Clark κd vs ISM Surface Density Clark+ (2018); Clark+ (2019) Appears that κ d is anticorrelated with ISM density. Opposite of what is predicted by models…

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Chris Clark M74 & M83 κd Compared to Literature Alton+ (2004); Demyk+ (2013); Köhler+ (2015); Clark+ (2016); Jones+ (2017); Clark+ (2019)

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Chris Clark Issues Observing Extended Galaxies in FIR Meixner+ (2014); Roman-Duval+ (2017); Williams+ (2018); Clark+ (in prep.) Herschel only; little diffuse emission

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Chris Clark So, You Want to Study Dust in the Magellanic Clouds? Roman-Duval+ (2017); Clark+ (in prep.) • Herschel! • …Except faint structure at the edges got removed as ‘background’, as the map was too small; large-scale features get filtered out. • Okay, Planck then! • …And Planck is great! But its shortest band is 350μm, so you can’t constrain dust temperature. And beam is 10x worse than Herschel. • How about Spitzer? • …Only covers the shorter wavelengths, and iffy resolution. Plus, severe non-linearity issues at high surface brightness for 160μm. • But there’s always IRAS, right? • …Unless you want to observe something that is extended and has very high surface brightness. Like the Magellanic Clouds. • Urm, I suppose I could try using Akari? • … • Good point. How about JCMT? Or ISO? • …Never observed more than tiny parts of the Clouds. • I suppose that leaves…

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Chris Clark Only Trustworthy Data is COBE! Meixner+ (2014); Roman-Duval+ (2017); Williams+ (2018); Clark+ (in prep.) Herschel-SPIRE 250 µm COBE-DIRBE 240 µm

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Chris Clark Feathering in Fourier Space Williams+ (2018); Clark+ (in prep.) COBE 100 µm IRAS 100 µm COBE feathered with IRAS COBE feathered with IRAS

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Chris Clark Combine Alllll the Data in Fourier Space… Clark+ (in prep.) COBE Far-infrared data, large angular scales IRAS Far-infrared data, medium angular scales Planck Submm data, large & medium angular scales COBE + IRAS FIR data, large and medium angular scales COBE + IRAS + Planck FIR-submm data, large & medium angular scales Herschel FIR-submm data, small angular scales COBE + IRAS + Planck + Herschel FIR-submm data, large & medium & small angular scales

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Chris Clark Issues Observing Extended Galaxies in FIR Meixner+ (2014); Roman-Duval+ (2017); Williams+ (2018); Clark+ (in prep.) Herschel only; little diffuse emission Herschel et al; Fourier-combined (WIP)

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Questions welcome!

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Chris Clark Gaussian Process Regression – Reliable! Clark+ (2019); De Vis+ (2019)

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Chris Clark Alternate Models Clark+ (2019) M74 DTM ∝ radius DTM ∝ ISM density “Toy” model M83 CHAOS Z

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Chris Clark Alternate Models Clark+ (2019) DTM ∝ radius DTM ∝ ISM density “Toy” model

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Chris Clark CO r 2:1 Regression Leroy+ (2012); Clark+ (2019)

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Chris Clark SED-Fitting Example Clark+ (2019)

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Chris Clark Dust-to-Metals in THEMIS Jones+ (2017); Jones+ (2018) Dust-to-metals expected to vary by factor of ~3.6 in THEMIS dust model (Jones+ 2017;2018). Table 3 from Jones+ (2018)

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Chris Clark Dust-to-Metals from Depletions Jenkins (2009); De Cia+ (2016); Wiseman+ (2016) 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. Figure 7 from Wiseman+ (2016) Figure 15 from De Cia+ (2016)