Connecting the density structure of molecular clouds with star formation
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1 Connecting the density structure of molecular clouds with star formation Max-Planck-Institute for Astronomy With: Federrath, C., Alves, J., Tan J C., Beuther H., Stutz, A., Henning T., Abreu Vicente, J., Hacar, A., Mattern M.
2 Empirical relations Gas physics e.g., Krumholz & McKee (2005) Padoan & Nordlund (2011) Hennebelle & Chabrier (2011, 2013) Zamora-Avile et al. (2012) Krumholz et al. (2012) Federrath & Klessen (2013),
3 s = ln (ρ/ρ0) e.g., Krumholz & McKee (2005) Padoan & Nordlund (2011) Hennebelle & Chabrier (2011, 2013) Zamora-Avile et al. (2012) Krumholz et al. (2012) Federrath & Klessen (2013), Critical density for star formation Probability density function of gas density ( -PDF)
4 s = ln (ρ/ρ0) Probability density function of gas density ( -PDF) Lack of systematic observational constraints until < decade ago.
5 Entire galaxy Giant molecular clouds Star-forming structures PAWS team/iram/nasa HST/ T. A. Rector 10 kpc Kainulainen et al. (2009) 100 pc 1 pc Stutz & Kainulainen (2015)
6 1 pc 10 pc 100 pc 1 kpc 10 kpc ~35 pc N-PDFs (shifted) Herschel-derived column density Stutz & Kainulainen Stutz & Kainulainen (2015)
7 1 pc 10 pc 100 pc 1 kpc 10 kpc ~35 pc Based on data from Stutz & Kainulainen (2015) and Sadavoy et al. (2013, 2014) N (class 0) / region Herschel-derived column density Stutz & Kainulainen Stutz & Kainulainen (2015) bottom-heavy N-PDF top-heavy N-PDF
8 1 pc 10 pc 100 pc 1 kpc 10 kpc power-law slope ~ -1 Star-forming clouds Kainulainen et al. (2009) ~25 clouds in the Solar neighborhood No Star formation
9 1 pc 10 pc 100 pc 1 kpc 10 kpc slope -1 Clouds that have HII regions slope -1 ATLASGAL 870 um data PDF Star-forming Clouds 330 regions slope -1 Starless clumps Abreu Vicente et al. (2015) Log N/<N>
10 1 pc 10 pc 100 pc 1 kpc 10 kpc Hughes et al. (2013) Top-heaviness of N-PDFs correlates with Σ(star clusters) ESA/Planck gallery Credit: PAWS team/iram/nasa HST/T. A. Rector (University of Alaska Anchorage)
11 Universal trend: correlation between the (column) density distribution and star formation
12 From gravo-turbulent simulations: Ward et al. (2014) slope -1 Turbulence-induced initial condition TIME see also Federrath et al. (2013); Federrath & Klessen (2013) Gravity-dominated state
13 Universal trend: correlation between the (column) density distribution and star formation 1 pc 10 pc 100 pc 1 kpc 10 kpc A new recipe for star formation in Solar neighbourhood Kainulainen et al. (2014, Science)
14 3D modelling to estimate gas densities ( -PDFs) Column density map 2D projection of the 3D model - Hierarchical structure modelling using wavelet filtering and structure reconstruction with prolate spheroids (see Kainulainen et al. 2014, Science).
15 Results: -PDFs of Molecular Clouds The -PDF: (2 examples out of 16) σ No star formation Kainulainen et al. (2014, Science) Active star formation
16 Results: -PDFs of Molecular Clouds The -PDF: (2 examples out of 16) Critical density (scrit) for star formation σ No star formation Kainulainen et al. (2014, Science) Active star formation
17 Relative density structure affects analytic SF laws s = ln (ρ/ρ0) Probability density function of gas density ( -PDF) Critical density for star formation
18 SFRff (density recipe) SFRff (YSO counts) Based on Kainulainen et al. (2014, Science)
19 Conclusions Universal link between density statistics and star formation Positive correlation between top-heaviness of (column) density PDFs and SF surface density from 1 pc pc scales Observationally constrained star formation laws Robust observational constraints for ISM evolution models.
20 Evaluating gas densities ( -PDFs) from projected data Column density map Structure identification Scales pc - Method tested against MHD turbulence simulations.
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