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ISM✻@ST Intro Talk 2021

ISM✻@ST Intro Talk 2021

Intro talk given to the ISM*@ST group meeting, introducing me and my science to the new (and old) members, updated for 2021.

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Chris Clark

May 03, 2021
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Transcript

  1. Remote Intro Talk II… ISM✻@ST Intro Talk 2021 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 Herschel Maps of Type-Ia SNe Remnants Gomez &

    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)
  12. Chris Clark Type-Ia SNe: Resolved Temps Gomez & Clark+ (2012a);

    Clark (PhD T., 2015) Kepler’s supernova; Thot (left) and Tcold (right) Tycho’s supernova; Thot (left) and Tcold (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
  13. 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)
  14. Chris Clark Dust in a Type-II SN: The Crab (SN1054)

    Clark (PhD T., 2015)
  15. 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☉ of supernova dust in the Crab Nebula Subsequent studies report values across 0.04–0.22 M☉ range
  16. Chris Clark Herschel-ATLAS (Herschel Astrophysical Terahertz Large Area Survey) Eales+

    (2010)
  17. Chris Clark Dust-Detected H-ATLAS Low-z Galaxies Clark+ (2015) H-ATLAS 250

    µm 15 < D < 45 Mpc SDSS gri-bands
  18. 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/Ks > 25), flocculent, HI-dominated galaxies make up the majority of a blind low-z blind 250 µm selected survey.
  19. Chris Clark BADGRS: Lots of Dust, Little Attenuation Eales+ (2010);

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

    MD /MS ~ 0.0005 MD /MS ~ 0.01
  21. Chris Clark BADGRS: Lots of Dust, Little Attenuation Schofield (PhD,

    2017) BADGR Non-BADGR
  22. Chris Clark BADGRS: The Peak of Dust-Richness Clark+ (2015) Older

    Younger Dust Rich Dust Poor
  23. Chris Clark BADGRS: The Peak of Dust-Richness Clark+ (2015); De

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

    Schofield (PhD T., 2017) Older Younger Dust Rich Dust Poor
  25. Chris Clark BADGRS: Super Low MH2 /Mdust ? Dunne+ (2018)

    IRAM 30m CO(1–0) ICO = 0.2–2 K km s-1 FWHM = 30–100 km s-1 MH2 /Mdust = 2–27 (Z-based XCO – MW XCO ) Z = 0.5–1 Z☉
  26. 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
  27. 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 κd values. Commonly-used standard values span a factor of ~3 range
  28. Chris Clark Estimating κd with the HRS (the Herschel Reference

    Survey) Alton+ (2004); Demyk+ (2013); Köhler+ (2015); Clark+ (2016); Jones+ (2017); Clark+ (2019) κ500 = 0.051 m2 kg-1 (± 0.24 dex)
  29. Chris Clark Biology‽

  30. 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
  31. None
  32. Chris Clark DustPedia Photometry Clark+ (2018) Robust automated aperture photometry

    for extended sources.
  33. Chris Clark DustPedia Photometry Clark+ (2018) Self-consistent photometry across many

    bands.
  34. 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 κd values. Commonly-used standard values span a factor of ~3 range
  35. Chris Clark Data for Mapping κd Within Galaxies Clark+ (2018);

    Clark+ (2019) M83 M74 But also need metallicity maps to calculate κd . These don’t normally exist for nearby galaxies…
  36. 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
  37. Chris Clark Gaussian Process Regression in M74 Clark+ (2019); De

    Vis+ (2019) M74 Metallicity Map M74 Metallicity Uncertainty
  38. Chris Clark Maps of κd in Nearby Galaxies! Clark+ (2018);

    Clark+ (2019) M74 κd map M83 κd map UV-NIR-FIR image for reference UV-NIR-FIR image for reference
  39. Chris Clark κd vs ISM Surface Density Clark+ (2018); Clark+

    (2019) Appears that κd is anticorrelated with ISM density. Opposite of what is predicted by models…
  40. Chris Clark M74 & M83 κd Compared to Literature Alton+

    (2004); Demyk+ (2013); Köhler+ (2015); Clark+ (2016); Jones+ (2017); Clark+ (2019)
  41. 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 (kike the Magellanic Clouds), where IRAS has severe gain problems. Urm, I suppose I could try using Akari? … Good point. How about JCMT? Or ISO? …Never observed more than tiny parts of the Magellanic Clouds. I suppose that leaves…
  42. Chris Clark Only ‘Trustworthy’ Data is COBE & Planck! Meixner+

    (2014); Roman-Duval+ (2017); Williams+ (2018); Clark+ (in prep.) Herschel-SPIRE 250 µm COBE-DIRBE 240 µm
  43. 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 x IRAS FIR data, large and medium angular scales (COBE x IRAS) + Planck FIR-submm data, large & medium angular scales Herschel FIR-submm data, small angular scales ((COBE x IRAS) + Planck) x Herschel FIR-submm data, large & medium & small angular scales x → “Feathered with” + → “In concert with”
  44. Chris Clark Some Bands Observed at All Scales Clark+ (in

    prep.) COBE 100 µm IRAS 100 µm COBE feathered with IRAS COBE feathered with IRAS
  45. Chris Clark Combine Alllll the Data in Fourier Space… Clark+

    (in prep.)
  46. Chris Clark Restoring Extended Emission by Feathering Meixner+ (2014); Roman-Duval+

    (2017); Williams+ (2018); Clark+ (in prep.) Herschel only; little diffuse emission Herschel et al; Fourier-combined
  47. Chris Clark Relative Difference When Feathering Meixner+ (2014); Roman-Duval+ (2017);

    Williams+ (2018); Clark+ (in prep.) LMC SMC M31 M33
  48. Chris Clark Foreground Subtraction Roman-Duval+ (2017); Clark+ (in prep.)

  49. Chris Clark SED Fitting Using Pixels Binned by HI Clark+

    (in prep.) FIR HI Dust Density Dust Temperature
  50. Chris Clark SED Fitting Using Pixels Binned by HI Clark+

    (in prep.) FIR HI Dust Density Dust Temperature
  51. Chris Clark Evolution in Gas/Dust in Extreme Densities Roman-Duval+ (2017);

    Clark+ (in prep.) LMC SMC From fitting SEDs of fluxes averaged in bins of H column Julia’s 2017 Results
  52. Chris Clark Stacking AGB Stars Scicluna+ (subm.); Clark+ (in prep.)

    Radial profile of Planck 350 μ m stack Very-work-in-progress stacked SED Planck 350 μm stack
  53. Chris Clark Looking for Dust in Leo P Clark+ (in

    prep.)
  54. Chris Clark Carbon Depletions via 158um [CII] Absorption Jenkins (2009);

    Clark+ (in prep.)
  55. Questions welcome!

  56. None
  57. Chris Clark The Crab: Synchrotron Power Law Gomez+ inc. Clark

    (2012b); Clark (PhD T., 2015) Spectral index map
  58. Chris Clark BADGRS: Star Formation Still Ramping Up Schofield (PhD

    T., 2017)
  59. Chris Clark Gaussian Process Regression – Reliable! Clark+ (2019); De

    Vis+ (2019)
  60. Chris Clark Alternate Models Clark+ (2019) M74 DTM ∝ radius

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

    ∝ ISM density “Toy” model
  62. Chris Clark CO r2:1 Regression Leroy+ (2012); Clark+ (2019)

  63. Chris Clark SED-Fitting Example Clark+ (2019)

  64. 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)
  65. Chris Clark Feathering In-Out Simulations Clark+ (in prep.)