The Structure of Young Stellar Clusters!
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1 Heidelberg University, Centre for Astronomy! Institute for Theoretical Astrophysics! Dimitrios A. Gouliermis! The Structure of Young Stellar Clusters! with! Sacha Hony, Stefan Schmeja, Ralf S. Klessen, et al.!
2 Understanding Clustered Star Formation! Question What is the clustering of stars at birth (and after)?! Key Issues Typical length-scales of Stellar Clustering.! Time-scale for Star Formation / Structure survival.! What processes determine these parameters?! Requirement Complete samples of resolved young stellar populations! 2!
3 The MW Magellanic Clouds System! Credit: dakotalapse.com 3!
4 The Region NGC 346/N66 Walborn et al. 1978! De Boer & Savage 1980! Niemela et al. 1986! Chu & Kennicutt 1988! Massey et al. 1989! Ye et al. 1991! Cortusi et al. 2000! Rubio et al. 2000! Walborn et al. 2000! Koenigsberger et al. 2000! Hoopes et al. 2001! Nazé et al. 2002! Danforth et al. 2003! Nazé et al. 2004! Reid et al. 2006! Evans et al. 2006! Gouliermis et al. 2006! Sabbi et al. 2007! Simon et al. 2007! Hennekemper et al. 2008! Hunter et al. 2008! Gouliermis et al. 2008! Sabbi et al. 2009! Schmeja et al. 2009! Cignoni et al. 2010! eso Photo Release Cignoni et al. 2011! Credit: Henri Boffin Gouliermis et al. 2014!
5 The Star-Forming Complex NGC 346! NGC 346 (N66) in the SMC! HST Program GO (PI: A. Nota)! Template of mixed populations! Photometric Catalogs:! Nota et al ApJL, 640, 29! Gouliermis et al ApJS, 166, 549! Credit: NASA/ESA HST & A. Nota (STScI)! 60% of the star formation! occurred earlier than ~ 5 Gyr ago! (Cignoni et al AJ, 141, 31)! 5!
6 Stellar Clustering in NGC 346! Schmeja, Gouliermis & Klessen 2009 (ApJ, 694, 367)! PMS Stars Sub-Clusters! Nearest-Neighbor Density Map! Ten individual stellar structures! One dominant aggregate! Sizes: 1 20 pc! Stellar Numbers: few ~1500! Brightness: V = mag! ~ 70% PMS stars within 1"! ~ 40% Clustered PMS stars (2")! Q = ! Substructure in 70% of clusters! 6!
7 Stellar Clustering Morphology in NGC 346! Gouliermis, Hony & Klessen 2014 (MNRAS, 439, 3775)! Kernel Density Estimation Map! N E 50 (~ 14 pc) 7!
8 Stellar Clustering and Star Formation! Different Stages of Cluster formation Correlation and Anti-correlation of IR peaks with PMS Sub-clusters! Obvious relation between! #stellar clustering and SF! #centers.! IRAC (8 µm) + MIPS (24 µm) Connection between! #stellar and ISM! #morphology.! YSO candidates indicate! #that SF is ongoing.! YSO candidates (Spitzer): Simon et al. 2007, ApJ, 669, 327! !
9 Characterizing Clustering with the Q-Param! Minimal Spanning Tree and Q! Cartwright & Whitworth 2004, MNRAS 348, 589! Q NGC346 $ 0.8! Q = MST mean edge - length Average separation " m s / R c D The Q-Parameter method is inconclusive in determining the nature of NGC 346! 9!
10 The Autocorrelation Function (ACF)! Peebles, P. J. E. 1973, ApJ, 185, 413! Gomez, M. et al. 1993, AJ 105,1927! 1+ "( r) = 1 n N N # i=1 Definition based on Peebles P. J. E. & Hauser M. J., 1974, ApJSS, 28, 19! n i ( r) The fractal dimension D 2 of the structure is related to the autocorrelation function slope (power-law index)! as:! D 2 = " + 2 Typical values of turbulent-driven hierarchy in the ISM: D 2 = ! (Sreenivasan K.R. 1991, Ann. Rev. Fluid Mechanics 23, 539;! Elmegreen & Scalo 2004, ARA&A, 42, 211)! 10!
11 The ACF of NGC 346! At r % 6 pc! 1+ " r ( ) # r $0.18 D 2 $ 1.8! At 6 % r % 20 pc! 1+ " r ( ) # r $0.58 D 2 $ 1.4! 11!
12 Characterizing Clustering is strenuous! Stellar Pair Separations PDF! p(r j ) = N # i=1 2N ij N( N "1)dr NGC 346 Random Field Centr. Conc. Cluster The separations PDF gives false evidence of a condensed cluster! 12!
13 The ACF of Centrally Condensed Clusters! Clusters Models from Elson, Fall & Freeman (1987, ApJ, 323, 54)! ( ) = f + 1+ % r 0 $ " f r ) * # & ( ' 2,. - /0 / 2 + f field, r c = "( 2 2 /0 /1) 1/ 2 13!
14 Surface Density Profiles can be misleading! Stellar Surface Density Profile! Autocorrelation Function! A good-fitting density profile misinterprets stellar clustering.! The Autocorrelation function is a more robust representation.! 14!
15 Synthetic Self-Similar Distributions! Box-counting algorithm! Bate et al. 1998, MNRAS, 297, 1163! Cartwright & Whitworth 2004, MNRAS, 348, 589! D3 = 2.6 D3 = 2.0 D = ln N ran /ln N div D3 = N div : N div number of total subcubes N ran : Number of cubes to be further divided D N ran = N div! Dimitrios Gouliermis! The Early Life of Stellar Clusters Copenhagen November 3, 2014!! 15!
16 NGC 346 is a Centrally Condensed Cluster! embedded in a Fractal Stellar Distribution! Gouliermis, Hony & Klessen 2014 (MNRAS, 439, 3775)! Best-Models Parameters:! r c $ 9 (2.5 pc)! " $ ! D 3 $ 2.3! f cl $ 40%! Power-law break at ~6 pc! Shift in the correlated properties of young stars on scales <100 pc.! 16!
17 Implications in our Understanding of CSF! The Origin of the bimodal distribution can be due to Nature: Bimodal star formation (clustered + distributed).! # # #(Bonnell et al. 2011)! Nurture: Dynamically merging sub-structures! # # #(Klessen & Burkert 2000; Bonnell, Bate & Vine 2003)! and depends on the initial conditions (Parker et al. 2013) Sub-structured super-virial agglomerations can evolve to systems like NGC 346! Implications about Self-similar Distributions Turbulent-Induced Hierarchy produces D 3 ~ ! #(Federrath et al. 2009; Girichidis et al. 2012; Dale, et al. 2013)! However, early dynamical evolution will partly erase substructure! #(Scally & Clarke 2002; Goodwin & Whitworth 2004)! How much of the original Hierarchy has been retained in the last 3 to 5 Myr?! 17!
18 PoI: Large Scale Structure & ISM relation! See Sacha Hony s talk later today Daniela Calzetti & 20+ collaborators NGC 6503 Gouliermis & the LEGUS Team, in preparation Star counts follow roughly the gas, i.e., dust column density.! 18!
19 Clusters typically form in Groups! [OII]+[OIII]+Hα LH 48 LH 47 LH 49 a) Spitzer 8μm (PAH and dust emission). # Blue contours: CO emission (Wong et al. 2011). # Red dots: YSOs (Chen et al. 2009; Carlson, et al. 2012).# b) MPG/ESO 2.2m WFI.# #Credit: F. Comeron and N. Delmotte (ESO).# 19!
20 Take-away messages! Stellar clustering at birth is complex.! Analysis methods require simulations.! Clusters are born in Clusters.! Bimodal stellar clustering on GMC-scales verified.! Scale where Gravity prevails identified at few pc.! Turbulence induces self-similar stellar topology in SF regions.! 20!
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