My research in a nutshell

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Marjorie Decleir Intro-talk @ ISM group meeting March 23rd 2020 My research in a nutshell

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Lichtervelde Gent Who am I and where do I come from?

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B.S. in Physics and Astronomy (2013) M.S. in Physics and Astronomy (2015) PhD in Astronomy (November 2019) Supervisors: Maarten Baes, Ilse De Looze Postdoc at STScI Supervisor: Karl Gordon Who am I and where do I come from?

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Interstellar dust Minor fraction of ISM… à Why do we care?? …But crucial constituent! Temperature of interstellar gas Formation of H2 Shielding dark matter, 90% stars, 7% ISM, 3% star & planet formation gas, 99% dust, 1%

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absorption scattering extinction emission

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wavelength (Å) extinction extinction slope 2175Å bump attenuation

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geometry dust properties wavelength (Å) attenuation Spot the 7 differences!

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DustKING attenuation wavelength (Å)

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attenuation wavelength (Å) transmission Swift GALEX 2175Å bump

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Standard pipeline: not suitable New pipeline for extended sources Swift ata eduction of xtended wift ources ode ode https://github.com/mdcleir/DRESSCode

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Co-add the frames per year, per filter … … … raw image sky map aspect corrected map aspect correction summed image corrected image corrections: coincidence loss large scale sensitivity variations sensitivity loss combined image final image raw image sky map aspect corrected map raw image sky map aspect corrected map summed image corrected image summed image corrected image Combine images of different years calibration quality map exposure map large scale sensitivity map

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NGC628 = M74

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wavelength light

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wavelength (Å) attenuation slope bump slope bump

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wavelength (Å) attenuation

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Higher AV à shallower slope Higher AFUV à steeper slope But higher AV à higher AFUV ?? Decleir+2019 slope bump V-band attenuation (AV ) attenuation wavelength (Å)

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wavelength (Å) attenuation

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slope slope bump bump AV AV slope AV Stellar mass gas mass dust mass SFR metallicity PAH IRAC 8µm inclination Hubble type

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attenuation wavelength (Å) slope bump wavelength (Å) attenuation

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wavelength (µm) NIR extinction curves wavelength (µm) flux flux Pair method

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wavelength (µm) NIR extinction curves SpeX spectrograph - Infrared Telescope Facility (IRTF) on Mauna Kea - medium-resolution - 0.7-5.3 µm SXD = Short wavelength cross-dispersed mode LXD = Long wavelength cross-dispersed mode IUE SpeX SXD SpeX LXD IRS flux

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wavelength (µm) NIR extinction curves IUE SpeX SXD SpeX LXD IRS RV dependence? New features? extinction To be continued…

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DUST MEANS THIRSTY West Flemish for behinners