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Report of Contributions How Galaxies form Stars Report of Contributions https://indico.fysik.su.se/e/5696 How Galaxies for … / Report of Contributions Opening Remarks, Setting the Stag … Contribution ID: 319 Type: not specified Opening Remarks, Setting the Stage (I) Monday, 22 August 2016 09:10 (35 minutes) Presenter: ÖSTLIN, Göran (Stockholm University) September 30, 2021 Page 1 How Galaxies for … / Report of Contributions Challenges and first results from C … Contribution ID: 381 Type: not specified Challenges and first results from CO and IR measurements in local Lyman Alpha Emitters Friday, 26 August 2016 14:10 (20 minutes) 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. Primary author: PUSCHNIG, Johannes (Stockholm University) Presenter: PUSCHNIG, Johannes (Stockholm University) Session Classification: Global Properties at Low and High Redshifts (continuation) September 30, 2021 Page 2 How Galaxies for … / Report of Contributions Beyond turbulence: a fundamenta … Contribution ID: 382 Type: not specified Beyond turbulence: a fundamentally different mode of star formation in Orion 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 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. Primary author: STUTZ, Amelia (MPIA) Presenter: STUTZ, Amelia (MPIA) September 30, 2021 Page 3 How Galaxies for … / Report of Contributions Superbubbles, Supernovae, and De … Contribution ID: 383 Type: not specified Superbubbles, Supernovae, and Deregulating Galaxies: Too Big Not to Fail Wednesday, 24 August 2016 10:30 (20 minutes) 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 handling feedback from Type II Supernovae. I will show that the key to obtaining a realistic stellar mass to halo mass relation (SMHMR) is preventing the runaway growth of a massive bulge by driving outflows with large mass-loadings. If this happens, SN feedback alone can no longer effectively drive out- flows from the galaxy, and star formation becomes unregulated. This is a key piece of evidence that the peak of the SMHMR is due to the shut down of SN regulation and the beginning of AGN regulation in more massive halos. I will also show how the interaction between hot outflows and the disk ISM, together with the potential well they live within, sets how much mass is entrained in a galactic wind/fountain, and how this can halt SN-driven winds in high- mass galaxies. Primary author: KELLER, Ben (McMaster University) Co-author: Dr WADSLEY, James (McMaster University) Presenter: KELLER, Ben (McMaster University) Session Classification: Star Formation and Feedback September 30, 2021 Page 4 How Galaxies for … / Report of Contributions The outer filaments of Centaurus A Contribution ID: 384 Type: not specified The outer filaments of Centaurus A Thursday, 25 August 2016 10:25 (20 minutes) Recent studies suggest that AGN can regulate the gas accretion and thus slow down star formation (negative feedback). However, evidence of AGN positive feedback is also invoked in a few radio galaxies (eg. Centaurus A, Minkowski’s Object, 3C 285, …). I will present a multi-wavelength study of the northern filaments of Centaurus A. These filaments of gas and young stars extend on scales up to 15 kpc, aligned with the radio-jet. Along the radio jet, CO emission has been detected in a HI shell (Schiminovich et al. 1994, Charmandaris et al. 2000). We also detected CO in a large area along the filaments. By confronting the CO data to archival Herschel-FIR and GALEX-FUV data, we determine that the gas in the filaments is very inefficient to form stars (with depletion time of a few Gyr). This is strengthened by archival ALMA data that revealed the presence of unresolved CO(2-1) emitting clumps. We showed that these clumps are probably not gravitationally bound. From our recent APEX data, we can now constrain the molecular gas dynamics in the filaments. By comparison with neutral HI (from VLA) and ionised gas (from VIMOS and MUSE), we confirm evidences of a dynamical effect of the radio jeton the gas along the jet direction. We also lay the foundations for upcoming high angular resolution ALMA data at large scales (in the scheduling queue). Primary author: SALOME, Quentin (LERMA, Observatoire de Paris) Co-authors: Dr COMBES, Françoise (LERMA, Observatoire de Paris); Dr SALOME, Philippe (LERMA, Observatoire de Paris); Dr HAMER, Stephen (CRAL, Observatoire de Lyon) Presenter: SALOME, Quentin (LERMA, Observatoire de Paris) Session Classification: Star Formation Properties in The Local Universe September 30, 2021 Page 5 How Galaxies for … / Report of Contributions Simulations of realistic dwarf gala … Contribution ID: 385 Type: not specified Simulations of realistic dwarf galaxies including Population III feedback Wednesday, 24 August 2016 12:20 (20 minutes) Dwarf galaxies occupy the faint end of the galaxy mass function and their properties are often regarded as strong tests for cosmological and galaxy evolution models. Indeed, their shallow gravitational potential makes them very susceptible to both external and internal processes, such as ram-pressure stripping and supernova feedback. Using computer simulations, the effects of such processes can be tested (e.g. Mayer et al. 2006, Governato et al. 2010). To do this, the properties of the simulated galaxies need to be closely compared to a broad range of observed galaxy properties and scaling relations. We present the results of N-body/SPH simulations including radiative cooling, star formation, chemical enrichment, stellar feedback, heating by the cosmic UV background, and feedback from Popula- tion III stars (Verbeke et al. 2015) and show that these compare very well to observed galaxies over the entire dwarf galaxy regime, unlike simulations without Population III feedback. We therefore conclude that Popula- tion III stars played a crucial role in the evolution of (dwarf) galaxies. Furthermore, we stress the importance of the way simulations are analyzed. The more in line these mock observations are with real observational techniques, the more reliable the comparison. Obtaining for example the rotational velocity from HI kinematics and metallicities from RGB stars (Kirby et al. 2013) are thus very important and can greatly affect the interpretation of the simulations. As a recent result, we use these realistic simulated dwarf galaxies and investigate different mech-
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