Resolving Galaxy Ecosystems Across All Scales: Dust around Massive Stars Is Agnostic to Galactic Environment: New Insights from PHAT/BEAST

Transcript

1. Dust around Massive Stars is Agnostic to Galactic Environment New Insights from PHAT and BEAST Christina Willecke Lindberg Graduate Student, Johns Hopkins University In Collaboration with Claire Murray (STScI) Julianne Dalcanton (Flatiron Institute) Josh Peek (STScI) Karl Gordon (STScI)
2. Resolving Galaxy Ecosystems 12-15-2023 30 Doradus Nebula in LMC HST WFC3 and ACS Red: Hydrogen Blue: Oxygen (Sabbi et al. 2013, Sabbi et al. 2016) 10.17909/T9RP4V Galactic Ecosystem between the ISM and Stars Christina Willecke Lindberg (clindbe2@jhu.edu)
3. Resolving Galaxy Ecosystems 12-15-2023 30 Doradus Nebula in LMC HST WFC3 and ACS Red: Hydrogen Blue: Oxygen (Sabbi et al. 2013, Sabbi et al. 2016) 10.17909/T9RP4V Gas forms stars Galactic Ecosystem between the ISM and Stars Christina Willecke Lindberg (clindbe2@jhu.edu)
4. Christina Willecke Lindberg (clindbe2@jhu.edu) Resolving Galaxy Ecosystems 12-15-2023 30 Doradus Nebula in LMC HST WFC3 and ACS Red: Hydrogen Blue: Oxygen (Sabbi et al. 2013, Sabbi et al. 2016) 10.17909/T9RP4V Gas forms stars Galactic Ecosystem between the ISM and Stars Feedback destroys ISM
5. Christina Willecke Lindberg (clindbe2@jhu.edu) Resolving Galaxy Ecosystems 12-15-2023 30 Doradus Nebula in LMC HST WFC3 and ACS Red: Hydrogen Blue: Oxygen (Sabbi et al. 2013, Sabbi et al. 2016) 10.17909/T9RP4V Gas forms stars Feedback compresses ISM Galactic Ecosystem between the ISM and Stars Feedback destroys ISM
6. Christina Willecke Lindberg (clindbe2@jhu.edu) Resolving Galaxy Ecosystems 12-15-2023 30 Doradus Nebula in LMC HST WFC3 and ACS Red: Hydrogen Blue: Oxygen (Sabbi et al. 2013, Sabbi et al. 2016) 10.17909/T9RP4V Gas forms stars Feedback compresses ISM Galactic Ecosystem between the ISM and Stars Feedback destroys ISM Density of ISM around massive stars
7. Christina Willecke Lindberg (clindbe2@jhu.edu) Resolving Galaxy Ecosystems 12-15-2023 30 Doradus Nebula in LMC HST WFC3 and ACS Red: Hydrogen Blue: Oxygen (Sabbi et al. 2013, Sabbi et al. 2016) 10.17909/T9RP4V Gas forms stars Feedback compresses ISM Galactic Ecosystem between the ISM and Stars Feedback destroys ISM Where are massive stars located in galaxies, and what sort of environment are they in? Density of ISM around massive stars
8. Christina Willecke Lindberg (clindbe2@jhu.edu) Resolving Galaxy Ecosystems 12-15-2023 Extragalactic Galaxies Milky Way • Resolved stars • Limited range in environments • Unresolved stars • Broad range in environments ESA/Webb, NASA & CSA, J. Lee and the PHANGS-JWST Team. Acknowledgement: J. Schmidt ESA/Gaia/DPAC, CC BY-SA 3.0 IGO
9. Christina Willecke Lindberg (clindbe2@jhu.edu) Resolving Galaxy Ecosystems 12-15-2023 Extragalactic Galaxies Milky Way • Resolved stars • Limited range in environments • Unresolved stars • Broad range in environments Andromeda Galaxy (M31) ESA/Webb, NASA & CSA, J. Lee and the PHANGS-JWST Team. Acknowledgement: J. Schmidt ESA/Gaia/DPAC, CC BY-SA 3.0 IGO - Andromeda Galaxy M32 M33
10. Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) How can we identify massive stars with photometry? PHAT; Dalcanton et al., (2012) Andromeda Galaxy (M ) Fact Sheet • ~ kpc away • Can resolve individual stars • Inclined by ~ • Largest galaxy in Local Group • Panchromatic Hubble Andromeda Treasury (PHAT) • 1/3 of galaxy disk • NUV-VIS-NIR coverage • +100 million stars 31 750 70o
11. How can we identify massive stars with photometry? PHAT; Dalcanton et al., (2012) Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Relative Intensity Wavelength (Angstrom) M O-stars 31 Massey et al., (2016) Massive stars can be identi fi ed via their spectra
12. How can we identify massive stars with photometry? PHAT; Dalcanton et al., (2012) Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) λ
13. How can we identify massive stars with photometry? PHAT; Dalcanton et al., (2012) Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) λ
14. How can we identify massive stars with photometry? PHAT; Dalcanton et al., (2012) Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) λ Massive stars extinguished by dust are as bright as regular stars at visible and IR wavelengths
15. How can we identify massive stars with photometry? PHAT; Dalcanton et al., (2012) Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Need broad wavelength coverage (UV) to identify massive stars
16. λ VISIBLE Flux NIR NUV Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) The Brief Overview of the Bayesian Extinction and Stellar Tool BEAST; Gordon et al., (2016)
17. Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) The Brief Overview of the Bayesian Extinction and Stellar Tool λ VISIBLE Flux NIR NUV 1. Fit spectral energy distribution (SED) with stellar model STELLAR MODEL [initial mass, age, metallicity] BEAST; Gordon et al., (2016)
18. Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) The Brief Overview of the Bayesian Extinction and Stellar Tool STELLAR MODEL [initial mass, age, metallicity] + DUST MODEL [extinction (AV), grain size (RV), extinction curve] 2. Apply extinction effects to stellar SED λ VISIBLE Flux NIR NUV BEAST; Gordon et al., (2016)
19. Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) The Brief Overview of the Bayesian Extinction and Stellar Tool STELLAR MODEL [initial mass, age, metallicity] + DUST MODEL [extinction (AV), grain size (RV), extinction curve] λ VISIBLE Flux NIR NUV BEAST; Gordon et al., (2016) Priors
20. Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) The Brief Overview of the Bayesian Extinction and Stellar Tool BEAST; Gordon et al., (2016) STELLAR MODEL [initial mass, age, metallicity] + DUST MODEL [extinction (AV), grain size (RV), extinction curve] λ VISIBLE Flux NIR NUV Marginalize 6D posterior to get 1D posteriors for each model parameter Priors
21. Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) +42,000 massive star candidates in the PHAT region Minit ≥ 8M⊙ Lindberg, Murray, Dalcanton et al. (submitted) Background: Spitzer 24-micron emission (Gordon et al. 2016)
22. +42,000 massive star candidates in the PHAT region Minit ≥ 8M⊙ Christina Willecke Lindberg (clindbe2@jhu.edu) Resolving Galaxy Ecosystems 12-15-2023 Most stars in star-forming rings Background: Spitzer 24-micron emission (Gordon et al. 2016) Lindberg, Murray, Dalcanton et al. (submitted)
23. +42,000 massive star candidates in the PHAT region Minit ≥ 8M⊙ Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Most stars in star-forming rings Lindberg, Murray, Dalcanton et al. (submitted) Also stars between rings Background: Spitzer 24-micron emission (Gordon et al. 2016)
24. +42,000 massive star candidates in the PHAT region Minit ≥ 8M⊙ Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Most stars in star-forming rings Also stars between rings Background: Spitzer 24-micron emission (Gordon et al. 2016) Massive stars between rings: In-situ formation or migration? Lindberg, Murray, Dalcanton et al. (submitted)
25. Quantifying stellar density /galactic environment Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) X parsecs X parsecs
26. Quantifying stellar density /galactic environment Christina Willecke Lindberg (clindbe2@jhu.edu) Resolving Galaxy Ecosystems 12-15-2023 X parsecs X parsecs Density = N stars (X/9) pc2
27. 0 0 0 0 0 0 1 0 0 0 0 1 0 0 0 0 0 0 0 0 0 0 0 1 0 0 0 0 0 0 0 1 0 0 1 0 0 0 1 0 1 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 1 0 0 0 1 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 Quantifying stellar density /galactic environment Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Source density only ’s or ’s 0 1 X parsecs X parsecs Density = N stars (X/9) pc2
28. 0 1 0 1 0 0 0 1 1 1 0 1 1 0 0 1 0 0 1 0 0 0 0 0 0 Quantifying stellar density /galactic environment Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Source density only ’s or ’s 0 1 X parsecs X parsecs Density = N stars (X/5) pc2
29. 1 1 1 1 2 1 1 0 1 Quantifying stellar density /galactic environment Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Source density only ’s or ’s 0 1 X parsecs X parsecs Density = N stars (X/3) pc2
30. Quantifying stellar density /galactic environment Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) X parsecs X parsecs k Kernel Density Estimation
31. Quantifying stellar density /galactic environment Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) X parsecs X parsecs k Kernel Density Estimation Pro: Continuous range of source densities
32. Quantifying stellar density /galactic environment Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) X parsecs X parsecs k Kernel Density Estimation Pro: Continuous range of source densities Only need to calculate density at locations of massive stars
33. Quantifying stellar density /galactic environment Christina Willecke Lindberg Resolving Galaxy Ecosystems 12-15-2023 X parsecs X parsecs k Kernel Density Estimation Pro: Continuous range of source densities Only need to calculate density at locations of massive stars
34. Quantify galactic environment using stellar density Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Lindberg et al. (submitted) (k=100 pc) X X
35. Av Line-of-Sight (BEAST-derived) Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Distribution of Stellar Densities Lindberg et al. (submitted) Galactic Environment (stellar density)
36. Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Multi-scale ISM Tracer - Dust Map (25-pc resolution) Dalcanton et al. (2015) 0.0 0.4 0.8 1.2 1.6 2.0 2.4 2.8 3.2 3.6 4.0 Median Av
37. Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) 25-pc Av across Galactic Environment 25-pc Dust Content (RGB-derived) 25-pc Av (RGB-derived) Lindberg et al. (submitted) Galactic Environment (stellar density)
38. Av Line-of-Sight (BEAST-derived) Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Theoretical LOS Av of Runaway Massive Stars across Stellar Densities 25-pc Dust Content (RGB-derived) Av Line-of-Sight (runaway stars) 25-pc Dust Content (RGB-derived) Lindberg et al. (submitted) 25-pc Av (RGB-derived)
39. Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Measured LOS Av of Massive Stars across Stellar Densities 25-pc Dust Content (RGB-derived) Av Line-of-Sight (BEAST-derived) Lindberg et al. (submitted) . 0.5-pc Av Line-of-Sight (BEAST-derived)
40. Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Measured LOS Av of Massive Stars across Stellar Densities 25-pc Dust Content (RGB-derived) Av Line-of-Sight (BEAST-derived) Lindberg et al. (submitted) . 0.5-pc Av Line-of-Sight (BEAST-derived)
41. Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Measured LOS Av of Massive Stars across Stellar Densities 25-pc Dust Content (RGB-derived) 0.5-pc Av Line-of-Sight (BEAST-derived) Lindberg et al. (submitted) 25-pc Av (RGB-derived)
42. Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Measured LOS Av of Massive Stars across Stellar Densities 25-pc Dust Content (RGB-derived) Av Line-of-Sight (BEAST-derived) Gap in dense regions: Effect of pre- supernovae or cumulative feedback? Lindberg et al. (submitted) 0.5-pc Av Line-of-Sight (BEAST-derived) 25-pc Av (RGB-derived)
43. Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Measured LOS Av of Massive Stars across Stellar Densities 25-pc Dust Content (RGB-derived) Av Line-of-Sight (BEAST-derived) Dust in sparse regions: Massive stars located in ISM not resolvable at 25-pc Evidence of in-situ formation? Lindberg et al. (submitted) Gap in dense regions: Effect of pre- supernovae or cumulative feedback? 0.5-pc Av Line-of-Sight (BEAST-derived) 25-pc Av (RGB-derived)
44. Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) Measured LOS Av of Massive Stars across Stellar Densities 25-pc Dust Content (RGB-derived) Av Line-of-Sight (BEAST-derived) Dust in sparse regions: Massive stars located in ISM not resolvable at 25-pc Evidence of in-situ formation? Lindberg et al. (submitted) Need follow-up observations to con fi rm in-situ formation! Gap in dense regions: Effect of pre- supernovae or cumulative feedback? 0.5-pc Av Line-of-Sight (BEAST-derived) 25-pc Av (RGB-derived)
45. Dust around Massive Stars is Agnostic to Galactic Environment Lindberg et al. (2024) https://arxiv.org/abs/2401.10991 1. Identified over 42,000 main-sequence massive star candidates in the PHAT region of M31 using broadband photometry (Dalcanton+12) characterized by the BEAST (Gordon+16), available at https:// archive.stsci.edu/hlsp/phathighmass. 2. At 25-pc resolution, Av is correlated with galactic environment 3. At ~0.5-pc resolution, line-of-sight Av is not correlated with galactic environment and remains constant across all disk environments 4. Discrepancy between the two measurements indicates that massive stars in sparse environments are not runaway stars, but likely formed in situ from ISM structures unresolved at 25-pc 5. Future: Study can be repeated for any galaxies with broad photometric coverage (i.e. SMC/LMC, M33, etc.) Resolving Galaxy Ecosystems 12-15-2023 Christina Willecke Lindberg (clindbe2@jhu.edu) 25-pc Dust Content (RGB-derived) Av Line-of-Sight (BEAST-derived) Thank you!