STScI HotSci: Tracing the Multi-phase ISM via Dust Extinction with UV Photometry in Nearby Galaxies

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1. Tracing the Multi-Phase ISM via Dust Extinction with UV Photometry in Nearby Galaxies Christina W. Lindberg Johns Hopkins University NASA, ESA, and E. Sabbi (STScI) HST WFC3/UVIS F275W, F336W, F775W
2. Tracing the 1. Multi-Phase ISM - Motivation 2. Dust Extinction - Method 3. UV Photometry - Data 4. Nearby Galaxies - Science NASA, ESA, and E. Sabbi (STScI) HST WFC3/UVIS F275W, F336W, F775W
3. NASA, ESA, and E. Sabbi (STScI) HST WFC3/UVIS F275W, F336W, F775W Molecular structures Ionized gas Diffuse atomic gas 12CO (2-1) H-alpha 21-cm HI Gas tracers only trace speci c ISM phases
4. NASA, ESA, and E. Sabbi (STScI) HST WFC3/UVIS F275W, F336W, F775W Molecular structures Ionized gas Diffuse atomic gas 12CO (2-1) H-alpha 21-cm HI Dust Dust Dust Dust Dust Dust Dust Can use extinction to trace multi-phase ISM
5. λ UV IR Measuring Extinction using Stars Extinguished stellar spectrum Dust will preferentially extinguish shorter wavelengths Bayesian Extinction And Stellar Tool (BEAST) Gordon+16
6. λ UV IR Measuring Extinction using Stars Infer amount of dust along line-of-sight Can infer dust using just photometry, meaning we can measure extinction to thousands of stars at once. Bayesian Extinction And Stellar Tool (BEAST) Gordon+16
7. λ UV IR Bayesian Extinction And Stellar Tool (BEAST) Gordon+16 Only optical and IR coverage UV coverage is critical for breaking degeneracy between extinction and stellar temperature. UV Coverage is Critical
8. F275W F336W F475W F814W F110W F160W Scylla Survey (PI: Claire Murray) Lindberg+2024b (in prep) Dust Mapping with Extinction
9. Dust Extinction Scylla Survey (PI: Claire Murray) Lindberg+2024b (in prep) 5 pc Dust Mapping with Extinction
10. Dust Extinction Scylla Survey (PI: Claire Murray) Lindberg+2024b (in prep) 5 pc Dust Mapping with Extinction
11. 2D Gaussian Processes (kriging) to interpolate underlying dust structure Dust Extinction Scylla Survey (PI: Claire Murray) Lindberg+2024b (in prep) 5 pc Dust Mapping with Extinction
12. Dust Extinction Scylla Survey (PI: Claire Murray) Lindberg+2024b (in prep) 5 pc Dust Mapping with Extinction 2D Gaussian Processes (kriging) to interpolate underlying dust structure
13. Can create highest-resolution dust maps ever in external galaxies, and independent of dust emission Dust IR Emission Dust Extinction Dust Extinction Matches Dust Emission 5 pc
14. Extinction maps provide a fully independent benchmark tracer of the multi-phase ISM. Can use high-res extinction maps to: 1. Quantify dust emissivity at low metallicity 2. Compare spatial distribution of dust with HI/CO Calibrate relations and constrain fraction of CO-dark molecular gas 3. Measure the e ects of pre-supernova feedback from massive stars → Scylla Survey (PI: Claire Murray) Lindberg+2024b (in prep) Science Enabled with Extinction Maps 5 pc
15. Other galaxies with panchromatic photometry that we can create extinction maps for: • M31: PHAT/PHAST • M33: PHATTER • SMC/LMC: Scylla + SMIDGE + METAL + HTTP • LUVIT, METAL-Z, etc. Andromeda Galaxy (M31; 760 kpc) Existing Opportunities in Local Group Galaxies Triangulum Galaxy (M33; 970 kpc ) *proximity, size, and locations of galaxies not to scale LMC (50 kpc) SMC (60 kpc) IC 1613 (730 kpc) Sextans A (90 kpc)
16. Cycle 31: HST/JWST coverage of N83/N84 in SMC Wing - tidally disrupted region (PI Lindberg) Cycle 32: Four Low-z Local Group dwarf galaxies (IC 10, IC 1613, NGC 6822, WLM ) with existing VLA HI coverage (PI Dalcanton) Upcoming Opportunities
17. *proximity, size, and locations of galaxies not to scale LMC (50 kpc) SMC (60 kpc) IC 1613 (730 kpc) Sextans A (90 kpc) Potential Opportunities in Local Group Galaxies Andromeda Galaxy (M31; 760 kpc) Triangulum Galaxy (M33; 970 kpc )
18. Andromeda Galaxy (M31; 760 kpc) Triangulum Galaxy (M33; 970 kpc ) *proximity, size, and locations of galaxies not to scale LMC (50 kpc) SMC (60 kpc) IC 1613 (730 kpc) Sextans A (90 kpc) UGC05373 (1.3 Mpc) UGC04305 (3.2 Mpc) NGC 2366 (3.4 Mpc) NGC 4163 (3.0 Mpc) NGC 4190 (2.9 Mpc) NGC 2403 (3.0 Mpc) Potential Opportunities in Local Group Galaxies IC 5152 (1.8 Mpc) UGC12613 (1.3 Mpc) NGC 1313 (3.9 Mpc) NGC 3077 (4.0 Mpc) NGC 300 (1.8 Mpc) NGC 3109 (1.3 Mpc) NGC 7793 (3.7 Mpc) M81 (3.7 Mpc) M82 (3.7 Mpc) NGC 2976 (3.6 Mpc)
19. Future of HST : HST is the only telescope that can provide this resolution of UV coverage for the next decade. How do we optimize HST with new era of IR telescopes?
20. 1. Motivation: Dust extinction provides a multi-phase tracer of the ISM. 2. Method: Can construct independent parsec-scale extinction maps using just multi-band photometry of resolved stellar populations. 3. Data: HST is the only telescope that can provide this resolution of UV coverage for the next decade. 4. Science: (1) Metallicity-dependent dust emissivity; (2) Calibrate gas tracers with total ISM; (3) Massive star feedback. Tracing the Multi-Phase ISM via Dust Extinction with UV Photometry in Nearby Galaxies Dust Extinction 5 pc Christina W. Lindberg (JHU) Dust IR Emission