Who is Karl? (2020 edition)

95bba3a98c20be969c4fb42ea31ae4ae?s=47 Karl Gordon
February 24, 2020

Who is Karl? (2020 edition)

Introduction talk for the ISM@ST research group.

95bba3a98c20be969c4fb42ea31ae4ae?s=128

Karl Gordon

February 24, 2020
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Transcript

  1. Who is Karl? Karl D. Gordon STScI, Baltimore, MD USA

    ISM@ST Research Group 24 Feb 2020 kgordon@stsci.edu @karllark2000 karllark@github “Have Dust – Will Study”
  2. Outline • What is Dust? – Extinction Curves (FUV, UV,

    optical, NIR, MIR) – Emission (Mid-IR, Far-IR, Optical) – Radiative Transfer • Galaxy Attenuation Curves & full UV-submm SEDs – Dust Grain Modeling (putting it together) • Nearby Galaxies – Magellanic Clouds, M31, M33, Local Group • Baysian Statistics & Distributed Coding • Instrumentation – Spitzer/MIPS, JWST/MIRI – Data Reduction Pipelines and Absolute Flux Calibration • Runner, Brewer, Woodworker
  3. Extinction Curves • Ultraviolet/optical – MW: optical (new broad features!)

    – SMC: 5→20 (bumps rare) – M31/M33 (like MW) • Near- & Mid-IR – In prep (2020!) Gordon et al. (2009, ApJ, 705, 1320) Gordon et al. (2003, ApJ, 594, 279) Extension to 912 A – still rising! LMC/SMC do not follow MW R(V) relation
  4. New SMC Extinction Curves Gordon et al. (202x, in prep.)

  5. The BEAST & MegaBEAST Gordon et al. (2016, ApJ, 826,

    104) Baysian Extinction And Stellar Tool Focused on fitting millions of SEDs of stars in nearby galaxies PHAT, SMIDGE, Scylla, ... https://github.com/BEAST-Fitting/beast https://github.com/BEAST-Fitting/megabeast Broad wavelength coverage breaks degeneracies
  6. Dust Emission – Aromatic Features Aromatic (PAH) features show evidence

    of processing in Hard radiation fields Gordon et al. (2008, ApJ, 682, 336)
  7. Dust Emission – Far-Infrared Gordon et al. (2014, ApJ, 797,

    85) Broken Emissivity model better than lots of cold dust
  8. Dust Emission - Optical • ERE (0.7 micron) – Extended

    Red Emission – Photoluminescence – Present in diffuse ISM – Carbonaceous grains? – Silicon nanoparticles? • New feature (1.5 micron) – Iron? • JWST GTO/ERS – Excitation wavelengths For aromatic/PAHs, aliphatics, new features! Gordon et al. (2000, ApJ, 544, 859) NW filament in reflection nebula NGC 7023
  9. ERE Excitation Wavelength Similar to H2 (FUV) Witt, Gordon, et

    al. (2006, ApJ, 636, 303)
  10. Radiative Transfer • DIRTY RT Code – Gordon+; Misselt+ (2001)

    • Study albedo & g • Compute galaxy attenuation curves • Predict galaxy SEDs Reflection nebulae albedos Steinacker, Baes, & Gordon (2013, ARA&A, 51, 63) Gordon (2013, Astrophysics of Dust, 77)
  11. Galaxies Attenuation Curves Attenuation + IR Emission Law, Gordon, &

    Misselt (2018, ApJS, 236, 32) Witt & Gordon (2000, ApJ, 528, 799)
  12. Dust Grain Modeling Gordon & Misselt (202x, in prep) Adding

    in dust scattering constraints possible (and lots of personal learning)
  13. Nearby Galaxies SINGS, LVL, KINGFISH SAGE-LMC, SAGE-SMC, SAGE-Spec, HERITAGE PHAT,

    HTTP, SMIDGE, METAL
  14. Bayesian & Distributed Coding • Bayesian techniques for fitting –

    Provided the tool I’ve always wanted to handle (correlated) data uncertainties – Priors allow for quantifying assumptions – BEAST, DustBFF, DGFit, … • Distributed coding – DIRTY early example (two coders) – BEAST the forcing function – Python in Astronomy meeting – Skill, not just tools
  15. Sptizer/MIPS • Early hire onto the MIPS team • 8

    years – 4 before launch, 4 after • Instrument team data reduction pipeline lead – MIPS DAT – Team included Chad Engelbracht, Karl Misselt, Jane Morrison, James Muzerolle • Lead the 70 micron absolute flux calibration • Lots of science – Focused on nearby galaxies
  16. JWST/MIRI • Early hire to MIRI team • 13+ years

    • Early years included all instrument aspects – Operations, user interaction, data reduction • Now focus on data reduction and calibration – Lead of JWST Baseline Pipeline → algorithms for all instruments – Lead of JWST AbsFlux WG → surface brightness/flux calibration for all instruments
  17. Brewer

  18. Woodworker

  19. Runner

  20. Thanks

  21. Career Trajectory • BA in Physics (Wittenberg Univ. - Ohio)

    – Testing power electronics in high radiation environments – Hot star Teff, logg from spectroscopy • MS, PhD in Physics (Univ. of Toledo – Ohio) – Extended Red Emission in the Diffuse ISM – Dust radiative transfer – Echelle spectroscopy of stars with 1m telescope • Postdoc, Geoff Clayton (Louisiana State Univ) – Extinction curves, grant writing, observing • Research staff, George Rieke (Univ. of Arizona) – Instrumentation, data reduction pipelines • Astronomer (STScI)
  22. Large Projects • Like to work with others • Instrument

    and Science Teams – Spitzer/MIPS, JWST/MIRI • Spitzer Legacies and Herschel Key Projects – Nearby Galaxies: SINGS, LVL, KINGFISH – Magellanic Clouds: SAGE-LMC, SAGE-SMC, SAGE-Spec • Hubble Large Programs – PHAT, HTTP, SMIDGE, METAL, Scylla, LUVIT, ... • ISM@ST Group!