CCA XMC Workshop: Constraining the 3D Structure of the XMC with Scylla

Transcript

1. Christina W. Lindberg (JHU) Advisor: Claire Murray (STScI) XMC “Milky Clouds over Manhattan’’ Meeting 2-28-24 Constraining the 3D ISM Structure of the XMC with Scylla Murray+24b (in prep)
2. Survey Data Science Goals BEAST Method Simulation Test Case Future Work Christina W. Lindberg (JHU) • Pure-parallel HST imaging survey that operated alongside the Ultraviolet (UV) Legacy Library of Young Stars as Essential Standards (ULLYSES) survey • Deep photometric coverage from the near UV to NIR with Wide Field Camera 3 (WFC3) in fi elds parallel to ULLYSES targets • First data release consists of 96 fi elds imaged over 342 orbits (Murray+2024b, in prep). Future releases will include all survey data (roughly 20 additional fi elds expected).
3. 1. Probe detailed star formation histories 
 [K. McQuinn, R. Cohen, C. Burhenne] 2. Resolve dust properties variation with interstellar environment 
 [C. Murray, C. Clark] 3. Constrain the multi-dimensional structure of the ISM of the XMC
 [C. Lindberg] Christina W. Lindberg (JHU) Survey Data Science Goals BEAST Method Simulation Test Case Future Work Primary Science Goals
4. 1. Probe detailed star formation histories 
 [K. McQuinn, R. Cohen, C. Burhenne] 2. Resolve dust properties variation with interstellar environment 
 [C. Murray, C. Clark] 3. Constrain the multi-dimensional structure of the ISM of the XMC
 [C. Lindberg] Christina W. Lindberg (JHU) Survey Data Science Goals BEAST Method Simulation Test Case Future Work Primary Science Goals
5. 1. Probe detailed star formation histories 
 [K. McQuinn, R. Cohen, C. Burhenne] 2. Resolve dust properties variation with interstellar environment 
 [C. Murray, C. Clark] 3. Constrain the multi-dimensional structure of the ISM of the XMC
 [C. Lindberg] What is the distance to dusty gas structures in the XMC? Christina W. Lindberg (JHU) Survey Data Science Goals BEAST Method Simulation Test Case Future Work Primary Science Goals
6. old stars young stars LEGEND Survey Data Science Goals BEAST Method Simulation Test Case Future Work Multi-Dimensional Structure of the ISM Christina W. Lindberg (JHU)
7. old stars young stars LEGEND Survey Data Science Goals BEAST Method Simulation Test Case Future Work Multi-Dimensional Structure of the ISM Christina W. Lindberg (JHU) Stars behind dust are extinguished
8. old stars young stars LEGEND old stars young stars LEGEND Survey Data Science Goals BEAST Method Simulation Test Case Future Work Multi-Dimensional Structure of the ISM Christina W. Lindberg (JHU)
9. old stars young stars LEGEND Use HI radial measurements to set # of gas clouds (e.g. Pingel+22) Survey Data Science Goals BEAST Method Simulation Test Case Future Work Multi-Dimensional Structure of the ISM Christina W. Lindberg (JHU)
10. λ VISIBLE Flux NIR NUV Survey Data Science Goals BEAST Method Simulation Test Case Future Work Bayesian Extinction and Stellar Tool Christina W. Lindberg (JHU) Gordon+16
11. STELLAR MODEL [initial mass, age, metallicity, distance] + λ VISIBLE Flux NIR NUV 1. Fit spectral energy distribution (SED) with stellar model Survey Data Science Goals BEAST Method Simulation Test Case Future Work Bayesian Extinction and Stellar Tool Christina W. Lindberg (JHU) Gordon+16
12. STELLAR MODEL [initial mass, age, metallicity, distance] + DUST MODEL [extinction (AV), grain size (RV), extinction curve] λ VISIBLE Flux NIR NUV 2. Apply extinction e ff ects to stellar SED Survey Data Science Goals BEAST Method Simulation Test Case Future Work Bayesian Extinction and Stellar Tool Christina W. Lindberg (JHU) Gordon+16
13. STELLAR MODEL [initial mass, age, metallicity, distance] + DUST MODEL [extinction (AV), grain size (RV), extinction curve] λ VISIBLE Flux NIR NUV Priors Survey Data Science Goals BEAST Method Simulation Test Case Future Work Bayesian Extinction and Stellar Tool Christina W. Lindberg (JHU) Gordon+16
14. STELLAR MODEL [initial mass, age, metallicity, distance] + DUST MODEL [extinction (AV), grain size (RV), extinction curve] λ VISIBLE Flux NIR NUV Marginalize 7D posterior to get 1D posteriors for each model parameter Priors Christina W. Lindberg (JHU) Survey Data Science Goals BEAST Method Simulation Test Case Future Work Bayesian Extinction and Stellar Tool Gordon+16
15. Survey Data Science Goals BEAST Method Simulation Test Case Future Work Bayesian Extinction and Stellar Tool Christina W. Lindberg (JHU) Need broad wavelength coverage to break degeneracies between Av, temperature, and distance.
16. Christina W. Lindberg (JHU) Survey Data Science Goals BEAST Method Simulation Test Case Future Work Cloud at 62 kpc Exponential stellar distance distribution -10 kpc +10 kpc Av = ~3 mag Distance Foreground Dust Av = ~0.5 mag A Single Dust Cloud
17. Christina W. Lindberg (JHU) Survey Data Science Goals BEAST Method Simulation Test Case Future Work A Single Dust Cloud Cloud at 62 kpc Exponential stellar distribution -10 kpc +10 kpc Av = 3 mag
18. Christina W. Lindberg (JHU) Survey Data Science Goals BEAST Method Simulation Test Case Future Work A Single Dust Cloud
19. Christina W. Lindberg (JHU) Survey Data Science Goals BEAST Method Simulation Test Case Future Work 30 Doradus Kim+99
20. Christina W. Lindberg (JHU) Survey Data Science Goals BEAST Method Simulation Test Case Future Work 30 Doradus Kim+99
21. Christina W. Lindberg (JHU) Survey Data Science Goals BEAST Method Simulation Test Case Future Work 30 Doradus Sabbi+13 Kim+99
23. Wong +22
24. Survey Data Science Goals BEAST Method Simulation Test Case Future Work 30 Doradus Christina W. Lindberg (JHU) Cyan sources on high-vel CO Magenta sources on low-vel CO Grey sources on no CO Wong +22 LMC 22 (6 fi lters)
25. Survey Data Science Goals BEAST Method Simulation Test Case Future Work 30 Doradus Christina W. Lindberg (JHU) Distance [kpc] (Weighted by integrated CO) Distance [kpc] (Weighted by integrated CO) Cut along DEC-axis Cut along RA-axis
26. Survey Data Science Goals BEAST Method Simulation Test Case Summary Future Work Christina W. Lindberg (JHU) Questions? • For Scylla fi elds in star forming regions • Obtain distance fi ts to individual structures in the fi eld • Compare with locations of massive stars • Learn lots of cool stuff about the star forming regions! • For all other Scylla fi elds • Obtain general distance fi ts to diffuse gas structures • Correlate these distance fi ts to GASKAP HI emission to construct global 3D model of the SMC and LMC • Collaborate with simulators to improve constrains on XMC dynamical history • Help Chris Clark with D/G ratios! Murray+24b (in prep)