ITC Lunch: Resolving the Multi-Scale Interstellar Medium in Local Group Galaxies

Transcript

1. Christina W. Lindberg (JHU) Resolving the Multi-Scale Interstellar Medium of Local Group Galaxies ITC Lunch Reading between the Stars
2. The interstellar medium is multi-scale 1 kpc Meidt+2023 Fahrion+2024 NGC 628 30 Doradus 10 pc Horsehead Nebula NASA Heritage Team 0.1 pc Christina W. Lindberg (JHU) ITC Lunch Talk Christina W. Lindberg (JHU) ITC Lunch Talk
3. 1 kpc Meidt+2023 Fahrion+2024 NGC 628 30 Doradus 10 pc Horsehead Nebula NASA Heritage Team 0.1 pc Christina W. Lindberg (JHU) ITC Lunch Talk Galaxy evolution is governed by small-scale processes Christina W. Lindberg (JHU) ITC Lunch Talk
4. 1 kpc Meidt+2023 Fahrion+2024 NGC 628 30 Doradus 10 pc Horsehead Nebula NASA Heritage Team 0.1 pc Christina W. Lindberg (JHU) ITC Lunch Talk Galaxy evolution is governed by small-scale processes Need to study ISM at parsec-scales across metallicities and galactic environments Christina W. Lindberg (JHU) ITC Lunch Talk
5. SMC D = 60 kpc Z = 0.2 Z⊙ Galaxy Mass Can study small-scale effects in Local Group galaxies LMC D = 50 kpc Z = 0.5 Z⊙ NGC 6822 D = 470 kpc Z = 0.2 Z⊙ IC 10 D = 660 kpc Z = 0.25 Z⊙ M31 D = 760 kpc Z = +1 Z⊙ IC 1613 D = 760 kpc Z = 0.15 Z⊙ M33 D = 850 kpc Z = 0.5 Z⊙ WLM D = 970 kpc Z = 0.13 Z⊙ Distance + many smaller galaxies Christina W. Lindberg (JHU) ITC Lunch Talk Christina W. Lindberg (JHU) ITC Lunch Talk
6. + many smaller galaxies SMC D = 60 kpc Z = 0.2 Z⊙ Galaxy Mass Can study small-scale effects in Local Group galaxies LMC D = 50 kpc Z = 0.5 Z⊙ NGC 6822 D = 470 kpc Z = 0.2 Z⊙ IC 10 D = 660 kpc Z = 0.25 Z⊙ M31 D = 760 kpc Z = +1 Z⊙ IC 1613 D = 760 kpc Z = 0.15 Z⊙ M33 D = 850 kpc Z = 0.5 Z⊙ WLM D = 970 kpc Z = 0.13 Z⊙ NGC 346 Christina W. Lindberg (JHU) ITC Lunch Talk Distance Christina W. Lindberg (JHU) ITC Lunch Talk
7. SMC D = 60 kpc Z = 0.2 Z⊙ Galaxy Mass LMC D = 50 kpc Z = 0.5 Z⊙ NGC 6822 D = 470 kpc Z = 0.2 Z⊙ IC 10 D = 660 kpc Z = 0.25 Z⊙ M31 D = 760 kpc Z = +1 Z⊙ IC 1613 D = 760 kpc Z = 0.15 Z⊙ M33 D = 850 kpc Z = 0.5 Z⊙ WLM D = 970 kpc Z = 0.13 Z⊙ HST Stars are resolvable in Local Group galaxies Distance + many smaller galaxies Christina W. Lindberg (JHU) ITC Lunch Talk
8. SMC D = 60 kpc Z = 0.2 Z⊙ Galaxy Mass LMC D = 50 kpc Z = 0.5 Z⊙ NGC 6822 D = 470 kpc Z = 0.2 Z⊙ IC 10 D = 660 kpc Z = 0.25 Z⊙ M31 D = 760 kpc Z = +1 Z⊙ IC 1613 D = 760 kpc Z = 0.15 Z⊙ M33 D = 850 kpc Z = 0.5 Z⊙ WLM D = 970 kpc Z = 0.13 Z⊙ HST Stars are resolvable in Local Group galaxies Can characterize individual stars Distance + many smaller galaxies Christina W. Lindberg (JHU) ITC Lunch Talk Christina W. Lindberg (JHU) ITC Lunch Talk
9. SMC D = 60 kpc Z = 0.2 Z⊙ Galaxy Mass LMC D = 50 kpc Z = 0.5 Z⊙ NGC 6822 D = 470 kpc Z = 0.2 Z⊙ IC 10 D = 660 kpc Z = 0.25 Z⊙ M31 D = 760 kpc Z = +1 Z⊙ IC 1613 D = 760 kpc Z = 0.15 Z⊙ M33 D = 850 kpc Z = 0.5 Z⊙ WLM D = 970 kpc Z = 0.13 Z⊙ HST Stars are resolvable in Local Group galaxies Can characterize individual stars Distance + many smaller galaxies Christina W. Lindberg (JHU) ITC Lunch Talk Can use extinction from dust as phase-agnostic tracer of the ISM Christina W. Lindberg (JHU) ITC Lunch Talk
10. λ UV IR Bayesian Extinction And Stellar Tool (BEAST) Gordon+16 We can measure dust extinction using stars Intrinsic stellar spectrum Christina W. Lindberg (JHU) ITC Lunch Talk Christina W. Lindberg (JHU) ITC Lunch Talk
11. λ UV IR We can measure dust extinction using stars Dust extinction Christina W. Lindberg (JHU) ITC Lunch Talk Bayesian Extinction And Stellar Tool (BEAST) Gordon+16 Christina W. Lindberg (JHU) ITC Lunch Talk
12. λ UV IR We can measure dust extinction using stars Extinguished stellar spectrum Christina W. Lindberg (JHU) ITC Lunch Talk Bayesian Extinction And Stellar Tool (BEAST) Gordon+16 Christina W. Lindberg (JHU) ITC Lunch Talk
13. λ UV IR We can measure dust extinction using stars Extinguished stellar spectrum Christina W. Lindberg (JHU) ITC Lunch Talk Bayesian Extinction And Stellar Tool (BEAST) Gordon+16 Dust will preferentially extinguish shorter wavelengths Christina W. Lindberg (JHU) ITC Lunch Talk
14. λ UV IR Infer amount of dust along line-of-sight We can measure dust extinction using stars Christina W. Lindberg (JHU) ITC Lunch Talk Bayesian Extinction And Stellar Tool (BEAST) Gordon+16 Christina W. Lindberg (JHU) ITC Lunch Talk
15. λ UV IR Infer amount of dust along line-of-sight We can measure dust extinction using stars Christina W. Lindberg (JHU) ITC Lunch Talk Bayesian Extinction And Stellar Tool (BEAST) Gordon+16 Christina W. Lindberg (JHU) ITC Lunch Talk
16. λ UV IR Infer amount of dust along line-of-sight We can measure dust extinction using stars Christina W. Lindberg (JHU) ITC Lunch Talk Bayesian Extinction And Stellar Tool (BEAST) Gordon+16 Can infer dust using just photometry, meaning we can measure extinction to thousands of stars at once. Christina W. Lindberg (JHU) ITC Lunch Talk
17. • Pure-parallel 500-orbit HST imaging survey that operated alongside the Ultraviolet (UV) Legacy Library of Young Stars as Essential Standards (ULLYSES) survey Scylla • UV-to-IR photometry with HST Wide Field Camera 3 (WFC3) • 89 fi elds with +3-7 fi lter coverage SMC Background: HI emission LMC
 Background: HI emission Murray+2024b Christina W. Lindberg (JHU) ITC Lunch Talk Christina W. Lindberg (JHU) ITC Lunch Talk
18. F275W F336W F475W F814W F110W F160W Scylla Survey (PI: Claire Murray) Lindberg+24b (submitted), +25 (in prep) Stellar Av probes the underlying multi-phase ISM Christina W. Lindberg (JHU) ITC Lunch Talk Christina W. Lindberg (JHU) ITC Lunch Talk
19. F275W F336W F475W F814W F110W F160W Stellar Av probes the underlying multi-phase ISM Scylla Survey (PI: Claire Murray) Lindberg+24b (submitted), +25 (in prep) Christina W. Lindberg (JHU) ITC Lunch Talk Christina W. Lindberg (JHU) ITC Lunch Talk
20. Dust Extinction 5 pc Stellar Av probes the underlying multi-phase ISM Scylla Survey (PI: Claire Murray) Lindberg+24b (submitted), +25 (in prep) Christina W. Lindberg (JHU) ITC Lunch Talk Christina W. Lindberg (JHU) ITC Lunch Talk
21. Dust Extinction 5 pc Stellar Av probes the underlying multi-phase ISM Scylla Survey (PI: Claire Murray) Lindberg+24b (submitted), +25 (in prep) Christina W. Lindberg (JHU) ITC Lunch Talk Christina W. Lindberg (JHU) ITC Lunch Talk
22. 2D Gaussian Processes to interpolate underlying dust structure Dust Extinction 5 pc Stellar Av probes the underlying multi-phase ISM Scylla Survey (PI: Claire Murray) Lindberg+24b (submitted), +25 (in prep) Christina W. Lindberg (JHU) ITC Lunch Talk Christina W. Lindberg (JHU) ITC Lunch Talk
23. Dust Extinction Dust IR Emission 5 pc Dust extinction matches dust emission Christina W. Lindberg (JHU) ITC Lunch Talk 36” (14-pc) Clark+21 5 pc Christina W. Lindberg (JHU) ITC Lunch Talk
24. Dust extinction matches ancillary ISM tracers Christina W. Lindberg (JHU) ITC Lunch Talk 1.8” (0.4-pc) Dust Extinction Molecular Gas CO; Wong+22 5 pc Christina W. Lindberg (JHU) ITC Lunch Talk
25. 5 pc Tons of science enabled with extinction maps! Extinction maps provide a fully independent benchmark tracer of the multi-phase ISM. Future science enabled:
 1. Dust emissivity at low metallicity 2. Spatial distribution of dust vs atomic (HI) and molecular (CO) gas 
 Calibrate relations and constrain fraction of CO-dark molecular gas at low metallicity → Christina W. Lindberg (JHU) ITC Lunch Talk Scylla Survey (PI: Claire Murray) Lindberg+24b (submitted), +25 (in prep) Christina W. Lindberg (JHU) ITC Lunch Talk
26. Tons of science enabled with extinction maps! Extinction maps provide a fully independent benchmark tracer of the multi-phase ISM. Future science enabled:
 1. Dust emissivity at low metallicity 2. Spatial distribution of dust vs atomic (HI) and molecular (CO) gas 
 Calibrate relations and constrain fraction of CO-dark molecular gas at low metallicity → Christina W. Lindberg (JHU) ITC Lunch Talk Scylla Survey (PI: Claire Murray) Lindberg+24b (submitted), +25 (in prep) Christina W. Lindberg (JHU) ITC Lunch Talk
27. Extinction maps provide a fully independent benchmark tracer of the multi-phase ISM. Future science enabled:
 1. Dust emissivity at low metallicity 2. Spatial distribution of dust vs atomic (HI) and molecular (CO) gas 
 Calibrate relations and constrain fraction of CO-dark molecular gas at low metallicity 3. E ff ects of pre-supernova feedback from massive stars → 5 pc Tons of science enabled with extinction maps! Christina W. Lindberg (JHU) ITC Lunch Talk Scylla Survey (PI: Claire Murray) Lindberg+24b (submitted), +25 (in prep) Christina W. Lindberg (JHU) ITC Lunch Talk
28. SMC D = 60 kpc Z = 0.2 Z⊙ Distance LMC D = 50 kpc Z = 0.5 Z⊙ NGC 6822 D = 470 kpc Z = 0.2 Z⊙ IC 10 D = 660 kpc Z = 0.25 Z⊙ M31 D = 760 kpc Z = +1 Z⊙ IC 1613 D = 760 kpc Z = 0.15 Z⊙ M33 D = 850 kpc Z = 0.5 Z⊙ WLM D = 970 kpc Z = 0.13 Z⊙ Lots of Local Group galaxies with panchromatic coverage… NGC 3109 D = 1.33 Mpc Z = 0.2 Z⊙ Sextans A D = 1.44 Mpc Z = <0.1 Z⊙ Sextans B D = 1.43 Mpc Z = <0.1 Z⊙ Antlia D = 1.37 Mpc Z = <0.1 Z⊙ Leo A D = 740 kpc Z = <0.1 Z⊙ Aquarius D = 980 kpc Z = <0.1 Z⊙ SagDIG D = 1.08 Mpc Z = <0.1 Z⊙ Leo P D = 1.62 Mpc Z = <0.1 Z⊙ *proximity, size, and locations of galaxies not to scale Christina W. Lindberg (JHU) ITC Lunch Talk Christina W. Lindberg (JHU) ITC Lunch Talk Local UltraViolet and Infrared Treasury (Boyer, Gilbert)
29. Cycle 31 (PI C. Lindberg) HST/JWST coverage of N83/N84 in SMC Wing - tidally disrupted region Cycle 32 (PI J. Dalcanton) Four Low-z Local Group dwarf galaxies (IC 10, IC 1613, NGC 6822, WLM) with existing VLA HI coverage And even more to come! Christina W. Lindberg (JHU) ITC Lunch Talk
30. The Multi-Scale Interstellar Medium of Local Group Galaxies Christina W. Lindberg (clindbe2@jhu.edu) • Extinction maps provide a fully independent benchmark tracer of the multi-phase ISM. • Will constrain dust emissivity, CO-dark molecular gas, and parsec-scale morphology of ISM at low-Z. Future work • Expand stellar SED- fi tting and dust mapping to other Local Group galaxies with resolved stars (M31, M33, IC10, IC1613, WLM, etc.). • Characterize ISM morphology as a function of metallicity to understand star formation and feedback broadly. Lindberg+24b Lindberg+25