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Book of Abstracts How Galaxies form Stars Monday 22 August 2016 - Friday 26 August 2016 AlbaNova University Center, Stockholm University, Stockholm, Sweden Book of Abstracts Contents Opening Remarks, Setting the Stage (I) ............................ 1 Challenges and first results from CO and IR measurements in local Lyman Alpha Emitters 1 Beyond turbulence: a fundamentally different mode of star formation in Orion . 1 Superbubbles, Supernovae, and Deregulating Galaxies: Too Big Not to Fail . 2 The outer filaments of Centaurus A .............................. 2 Simulations of realistic dwarf galaxies including Population III feedback . 3 Blustering and Blasting - Stellar feedback and its Chemical Tracers ............ 4 The Hierarchical Distribution of Young Stellar Clusters in Nearby Galaxies . 4 Characterizing Dust Attenuation in Local Star Forming Galaxies .............. 5 Constraining the cloud-scale physics of star formation and feedback in galaxies across cos- mic time ........................................... 5 How black hole feedback may trigger star formation in galaxies .............. 6 Star Formation in the outer M83 XUV disk .......................... 6 Star Formation and Feedback in Low Metallicity Galaxies at z~2 .............. 7 The impact of galactic environment on star formation .................... 7 Theory of star formation and feedback (I) ........................... 8 The effect of galaxy dynamics on star formation (I) ..................... 8 The Gas-Star Cycle resolved from Galactic to Cloud Scale in Nearby Galaxies . 9 Synthetic observations of star formation tracers in disc galaxy simulations — the validation of a new method to constrain the cloud-scale physics of star formation and feedback 9 [CII] as a tracer of GMC formation .............................. 10 Cold gas and star formation on clump scales: an ALMA look at a prototypical z~2 galaxy 10 Triggered formation of cold gas from superbubbles ..................... 11 Feedback on Sub-Galactic Scales: Insights from Starburst Regions (I) . 11 iii The multi-scale physics of star and cluster formation in galaxies across cosmic time(I) . 12 Swift/UVOT Measurements of the UV Dust Extinction Curve and the Recent Star Formation History of the SMC and M33 ................................ 12 A high-z perspective on galaxy growth and star formation (I) . 13 Spatially-resolved Star Formation Rate and Stellar Mass of Spiral Galaxies in the Local Uni- verse : Quantifying The Inside-out Scenario of Disk Galaxies Formation . 13 Linking Galactic structure to star formation in the Milky Way . 14 State-of-the-art diagnostics for detecting gravitational instabilities in galaxy discs . 14 Sub-galactic scale modelling of Star Formation (I) ...................... 14 Of needles and haystacks: High-detail characterization of warm ISM in nearby starbursts 15 Unveiling the role of galactic rotation on star formation . 15 Cluster formation and evolution in M51 ............................ 16 Using far-infrared transitions to study star formation activity in galaxies . 16 Feedback efficiency in young stellar clusters inM83 ..................... 17 Galactic magnetic fields and the FIR-radio correlation at high redshifts . 18 Resolved stellar populations studied with MUSE crowded field 3D spectroscopy . 18 FADO: a novel spectral population synthesis tool for the exploration of galaxy evolution by means of genetic optimization under self-consistency boundary conditions . 19 The evolution of star-formation efficiency during galaxy interactions - lessons fromSDSS- selected post-mergers .................................... 19 The star formation law in Galactic high-mass star-forming molecular clouds. 20 Effect of diffuse background in spatially-resolved star-formation studies . 20 Tidal Tales of Minor Mergers: Star Formation in the Tidal Tails of Minor Mergers . 21 Using CO line ratios to trace the physical properties of molecular clouds . 22 Radial variations in elliptical galaxy stellar populations - constraints on mass-assembly from infrared spectroscopy ................................. 22 The transition from atomic to molecular gas in M33: a large scale investigation onthe formation of molecular clouds in a low metalicity environment . 22 The feedback of super star clusters on the ISM ........................ 23 The Lyman alpha reference sample .............................. 23 NGC1275: A Study of Star Formation in 4-Dimensions ................... 24 New Probes of Starburst Feedback and Circumgalactic OVI in Emission . 24 The YSC’s perspective of star formation ............................ 25 The Star Formation-Gas Relation in NGC4449 ........................ 25 How do supernovae regulate star formation and launch galactic winds? (I) . 25 The scaling laws of star-formation on galactic scales (I) ................... 26 Cloud-scale star formation relations (I) ............................ 26 Small-scale star formation/clusters (I) ............................. 27 Starbursting Dwarf Galaxies: Back in the Spotlight (I) .................... 27 Panel Discussion ........................................ 28 Summary and Closing Remarks: What Next? (I) ....................... 28 Panel Discussion ........................................ 28 Panel Discussion ........................................ 28 Welcome ............................................. 28 How Galaxies form Stars / Book of Abstracts 319 Opening Remarks, Setting the Stage (I) Global Properties at Low and High Redshifts (continuation) / 381 Challenges and first results from CO and IR measurements inlo- cal Lyman Alpha Emitters Author: Johannes Puschnig1 1 Stockholm University Corresponding Author: [email protected] Carbon Monoxide has proven to be a well-calibrated tracer of the total molecular gas content in galaxies at low and high redshift. However, CO observations in galaxies of subsolar metallicity remain challenging, even in the local universe. For that reason, the dust mass is often used to infer the molecular gas in low metallicity systems. I will present first results of CO and dust measurements in the Lyman Alpha Reference Sample (LARS), a sample of local Lyman Alpha emitting starburst galaxies, all of subsolar metallicity. Using multiple-J CO transitians obtained with APEX and the IRAM 30m telescope, as well as Herschel/PACS and WISE data in combination with physical dust models and PDR codes, properties of the star forming gas could be derived and CO and dust scaling relations studied. 382 Beyond turbulence: a fundamentally different mode of star for- mation in Orion Author: Amelia Stutz1 1 MPIA Corresponding Author: [email protected] We argue that Orion hosts a fundamentally different mode of star cluster formation relative to the nearby clouds (e.g., Taurus) that have been studied to death. By comparing 3 constituents of Orion A (gas, protostars, and pre-main-sequence stars), both morphologically and kinematically, we show the following. Essentially all of Orion A’s Integral Shaped Filament (ISF) protostars lie superposed on the ISF, while almost all pre-main-sequence stars do not. Combined with the fact that protostars move < 1 kms relative to the filament, while stars move several times faster, this implies that a slingshot mechanism may eject protostars from the dense filamentary cradle, thereby cutting off their accretion of new gas. The ISF is the3rdin a series of star bursts that are progressively moving south through Orion A, with separations of ~ 2 Myr in time and ~ 3 pc in space. This, combined with the ISF’s observed undulations (spatial and Page 1 How Galaxies form Stars / Book of Abstracts velocity), suggest that repeated propagation of transverse waves thru the filament is progressively digesting the gas that formerly connected Orion A and B into stars in approximately discrete episodes. The presence of transverse waves implies the action of a buoyant restoring force acting against gravity. Combined with previous observations of magnetic field geometry and strength in the ISF, this suggests that the ISF transverse waves are magnetically induced. The presence of straight filaments in low mass regions (e.g., Taurus and L1641) as well as in turbulence simulations indicates that Taurus-like filaments are a direct reflection of initial conditions. In contrast, the observed undulations of the ISF, the fact that the ISF is the only nearby cluster in formation, the fact that it has survived repeated burst of intense star formation, and the equality between the inferred gravitational potential energy and magnetic energy on ~ 1 pc scales near the filament ridge, together lead to the following conclusion. The key physical difference in Orion is that it ismassive enough to have survived initial star formation episode, allowing the ISF to undergo internal evolution leading to concentration of B-fields confined by a deep gravitational potential well. Star Formation and Feedback / 383 Superbubbles, Supernovae, and Deregulating Galaxies: Too Big Not to Fail Author: Ben Keller1 Co-author: James Wadsley 1 1 McMaster University Corresponding Author: [email protected] Mgalaxies, with halo masses ~10^12 Msun, live in an interesting part of parameter space. Not only are they the “turnover” in the galaxy mass Schecter function, they also have the highest stellar mass (and baryon) fraction, very low bulge-to-disk ratios, and dominate the star formation of the epoch they live in. In this talk I will present the results of a sample of 18 cosmological M galaxies, simulated using the state-of-the-art superbubble method for
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