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

Intro talk given to the ISM*@ST group meeting, introducing me and my science to the new (and old) members.

Transcript

1. “So, what are you for, exactly?” ISM✻@ST Intro Talk Chris Clark
2. Chris Clark Clark & Redfern (1988) Helston
3. Chris Clark Cardiff
4. Chris Clark
5. Chris Clark
6. Chris Clark
7. Chris Clark
8. Chris Clark
9. Chris Clark BBC (2009)
10. 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)
11. 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)
12. 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)
13. 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
14. 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)
15. Chris Clark Dust in a Type-II SN: The Crab (SN1054) Clark (PhD T., 2015)
16. Chris Clark The Crab: Synchrotron Power Law Gomez+ inc. Clark (2012b); Clark (PhD T., 2015) Spectral index map
17. 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
18. Chris Clark Herschel-ATLAS (Herschel Astrophysical Terahertz Large Area Survey) Eales+ (2010)
19. Chris Clark Dust-Detected H-ATLAS Low-z Galaxies Clark+ (2015) H-ATLAS 250 µm 15 < D < 45 Mpc SDSS gri-bands
20. 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.
21. Chris Clark BADGRS: Lots of Dust, Little Attenuation Clark+ (2015) More Attenuation Less Attenuation Dust Rich Dust Poor
22. Chris Clark BADGRS: Lots of Dust, Little Attenuation Clark+ (2015) M D /M S ~ 0.0005 M D /M S ~ 0.01
23. Chris Clark BADGRS: Lots of Dust, Little Attenuation Schofield (PhD, 2017)
24. Chris Clark BADGRS: The Peak of Dust-Richness Clark+ (2015) Older Younger Dust Rich Dust Poor
25. Chris Clark BADGRS: The Peak of Dust-Richness Clark+ (2015); De Vis (2017) Older Younger Dust Rich Dust Poor
26. Chris Clark BADGRS: Many Chemical Evolution Paths? De Vis+ (2017); Schofield (PhD T., 2017) Older Younger Dust Rich Dust Poor
27. Chris Clark BADGRS: Star Formation Still Ramping Up Schofield (PhD T., 2017)
28. 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 ☉
29. 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
30. 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
31. 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)
32. Chris Clark Biology‽
33. 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
35. Chris Clark DustPedia Photometry Clark+ (2018) Robust automated aperture photometry for extended sources.
36. Chris Clark DustPedia Photometry Clark+ (2018) Self-consistent photometry across many bands.
37. 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
38. 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…
39. 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
40. Chris Clark Gaussian Process Regression in M74 Clark+ (2019); De Vis+ (2019) M74 Metallicity Map M74 Metallicity Uncertainty
41. Chris Clark Gaussian Process Regression in M83 Clark+ (2019); De Vis+ (2019) M83 Metallicity Map M83 Metallicity Uncertainty
42. 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
43. 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…
44. Chris Clark M74 & M83 κd Compared to Literature Alton+ (2004); Demyk+ (2013); Köhler+ (2015); Clark+ (2016); Jones+ (2017); Clark+ (2019)
45. Chris Clark Issues Observing Extended Galaxies in FIR Meixner+ (2014); Roman-Duval+ (2017); Williams+ (2018); Clark+ (in prep.) Herschel only; little diffuse emission
46. 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…
47. 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
48. 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
49. 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
50. 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)
51. Questions welcome!
53. Chris Clark Gaussian Process Regression – Reliable! Clark+ (2019); De Vis+ (2019)
54. Chris Clark Alternate Models Clark+ (2019) M74 DTM ∝ radius DTM ∝ ISM density “Toy” model M83 CHAOS Z
55. Chris Clark Alternate Models Clark+ (2019) DTM ∝ radius DTM ∝ ISM density “Toy” model
56. Chris Clark CO r 2:1 Regression Leroy+ (2012); Clark+ (2019)
57. Chris Clark SED-Fitting Example Clark+ (2019)
58. 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)
59. 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)