Julia's intro talk

Transcript

1. Who is Julia Roman-Duval? ISM Group Meeting February 12, 2018
2. In a nutshell… • Born in Caen, Normandie, France
3. In a nutshell… • I went to aerospace engineering school (“Grande Ecole”) in France • Got my PhD from Boston University in 2009 • I have been at STScI since 2009 • 2 year postdoc with Karl and Margaret • ESA-AURA Astronomer since 2011
4. I have been a globe trotter
5. Spent my childhood in Reunion Island, it was awesome
6. Science Topic #1: Properties and distribution of molecular gas in the Milky Way and the Magellanic Clouds
7. Distances to Molecular Clouds in the Milky Way
8. Distances to Molecular Clouds in the Milky Way Roman-Duval+2009
9. Properties and Distribution of GMCs • With distances, you get masses! Roman-Duval+2010
10. Quantifying diffuse and dense molecular gas in the milky way • In the Milky Way, we can spatially resolve different gas components • We use large-scale surveys of 12CO and 13CO * Galactic Ring Survey (GRS, 13CO) * University of Massachusetts Stony Brook survey (UMSB) in 12CO * EXeter-FCRAO survey (EXFC) in 12CO and 13CO (outer Galaxy) * ThrUMMS survey (12CO and 13CO) * 45” beam • Follow a statistical method, no cloud decomposition • See Roman-Duval+2016 for details GRS + UMSB EXFC 55-100 EXFC 135-165 ThRUMMS New in 2017
11. DIFFUSE AND DENSE MOLECULAR GAS Integrated intensity maps of the diffuse and dense CO gas in the Outer Galaxy (135°<l<165° , -4°<b<5°, clouds roughly 3 kpc away). GRS GRS (Inner Galaxy) I(12CO) [K km/s] DIFFUSE DENSE
12. Spatial distribution of CO gas in the Milky Way Face-on surface density computed on 100 pc scales in the total, diffuse, and dense components TOTAL DENSE DIFFUSE GRS+UMSB EXFC ThrUMMS GC GC GC +2 kpc +2 kpc +2 kpc Roman-Duval+2016
13. Radial distribution of diffuse and dense gas • The fraction of diffuse gas increases from 10-20% at Rgal =2-6 kpc, to 50% beyond the Solar Circle Rgal [kpc] S gal (H2 ) [Mo pc-2] Dense/total ratio Dense Diffuse GRS GMCs The diffuse CO gas represents 25% of the total H 2 mass (6.5×108 M o ) Roman-Duval+2016
14. Turbulence in GMCs • Characterized turbulence statistics in HD simulations and observations (CO 1-0): Turbulence is intermittent (Burgers type, shocks) Roman-Duval+2011 CO Observations CO Simulations
15. ALMA in the LMC and SMC SMC N42 CO 1-0 (ALMA) Spitzer 8 µm Spitzer 24 µm Spitzer 24 µm CO 1-0 (NANTEN) Ha 15 pc
16. Science Topic #2: Dust Properties in Nearby Galaxies
17. HERITAGE Survey: PACS Data Processing 2 years of my life, it was hard…
18. Success! • Derived dust masses (Gordon+2014) • Derived HI/H2 transition and G/D in atomic gas vs molecular gas (Roman- Duval+2014) H/D molecular gas < 200 H/D atomic gas = 380 HI/H2 transition at S(HI) = 40 Mo pc-2 Hydrogen Surface Density [Mo pc-2] Dust Surface Density [Mo pc-2]
19. Beating the systematics with hi-resolution + all-sky surveys • Roman-Duval+2017 Depletions Depletions IRAS + Planck + 21 cm + CO IRAS+ Planck + 21 cm + CO
20. Beating the systematics with hi-resolution + all-sky surveys • Ongoing ADAP
21. The METAL HST Project 101 prime (STIS/COS) + 101 parallel (WFC3) orbits with HST to probe the variations of dust properties and abundance and the growth and destruction of dust grains in the LMC ISM at Z = 0.5 Zo ✕ Metal Targets (33) O SN remnants (Temim+2015) HI (Kim+2003) Herschel/PACS 160 µm (Meixner+2013) CO 1-0 (MAGMA, Wong+2011) GO- 13778 (PI Jenkins) is obtaining similar spectra in the SMC at Z = 0.2 Zo J. Roman-Duval 21
22. Depletions and extinction in the LMC 250 µm A V
23. Science Topic #3: How to run faster, longer, stronger?
24. Marathon Olympic team trials (2016) Boston Marathon 2017 California International Marathon (2015) This is me This is Desiree Linden!!!!!