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Angela Adamo22/08/2016, 09:00
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Göran Östlin (Stockholm University)22/08/2016, 09:10
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Ralf Klessen (Heidelberg University, Center for Astronomy)22/08/2016, 09:45Stars and star clusters are the fundamental visible building blocks of galaxies at present days as well as in the early universe. They form by gravitational collapse in regions of high density in the complex multi-phase interstellar medium (ISM). The process of stellar birth is controlled by the intricate interplay between the self-gravity of the star-forming gas and various opposing...Go to contribution page
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Steve Longmore (Liverpool John Moore University)22/08/2016, 11:15The formation environment of stars in massive, dense stellar clusters is similar to the environment of stars forming in galaxies at a redshift of 1 - 3, at the peak star formation rate density of the Universe. As massive clusters are still forming at the present day at a fraction of the distance to high-redshift galaxies they offer an opportunity to understand the processes controlling...Go to contribution page
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Alex Hygate (Max Planck Institute of Astronomy (MPIA)/Astronomisches Rechen-Institut, University of Heidelberg (ARI/ZAH), Heidelberg, Germany)22/08/2016, 12:00In this contribution, I will discuss a new method of observationally measuring the key quantities describing the cloud-scale physics of star formation and feedback, such as the cloud lifetime, feedback timescale, star formation efficiency, mass loading factor, etc. (Kruijssen & Longmore, 2014). This method for the first time allows us to probe these physics over a large galaxy sample and...Go to contribution page
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Paul Clark (Cardiff University)22/08/2016, 12:20The timescale over which GMCs form and disperse sets the timescale for star formation. Until recently, most observational studies of GMCs have focused on the molecular tracers, which are good probe of the cool interiors of the clouds, but have a limited ability to trace the dynamics of the transition to the warm neutral medium (WNM). In this study, we assess the ability of [CII]...Go to contribution page
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Daniel Haydon (Astronomisches Rechen-Institut, University of Heidelberg (ARI/ZAH), Germany)22/08/2016, 12:40A major problem in star/cluster formation and feedback is to constrain the cloud-scale physics across galactic environment and cosmic time. A promising solution has been put forward by Kruijssen & Longmore (2014), who present a statistical method for measuring ill-constrained cloud-scale quantities such as the cloud lifetime, star formation / feedback time-scales, star formation...Go to contribution page
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Diederik Kruijssen (Heidelberg University (ARI/ZAH))22/08/2016, 14:30Stellar clusters are a fundamental (by)product of the galactic-scale star formation process. I will discuss how recent theoretical insights in cluster formation and evolution have led to a unified understanding of stellar clustering across cosmic time, from local open clusters and associations to old globular cluster populations. I will conclude by discussing our recent work on the...Go to contribution page
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Angela Adamo (Stockholm University)22/08/2016, 15:15
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Kathryn Grasha (University of Massachusetts)22/08/2016, 15:35A turbulent interstellar medium will drive the hierarchical nature of star formation, resulting in a smoothly varying distribution of substructure, where bound star clusters occupy the smallest, densest regions. We use young stellar clusters to trace the unbound hierarchical star-forming structures for several nearby galaxies drawn from the Legacy ExtraGalactic UV Survey (LEGUS). We...Go to contribution page
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Matteo Messa (Stockholm University)22/08/2016, 16:25While star formation has been long studied on the single-star scale and on the galaxy scale, the link between these two widely separated scales still needs to be firmly established. We use the new high-resolution NUV and U band HST observations from LEGUS (Legacy Extra Galactic UV Survey) to study the nearby interacting spiral galaxy M51 at the intermediate scale of the star cluster...Go to contribution page
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Jay Gallagher (Dept of Astronomy, University of Wisconsin-Madison)22/08/2016, 16:45This talk will briefly review patterns of star formation in NGC 1275, the brightest galaxy in the Perseus cluster. NGC 1275 is of special interest as it contains examples of unusual modes of star formation in a complex environment. Young massive star clusters detected via HST UV imaging are associated with gaseous filaments that are arrayed over 10s of kpc around the center of the...Go to contribution page
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22/08/2016, 17:15J. Gallagher, R. Klessen, S. Longmore, D. KruijssenGo to contribution page
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Amanda Heiderman (University of Virginia)23/08/2016, 09:00
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Oscar Agertz (University of Surrey)23/08/2016, 09:45I will review recent advances in sub-galactic scale modelling of star formation, with a particular emphasize on the interplay between star formation and stellar feedback and how this impacts galaxy formation and evolution over cosmic time.Go to contribution page
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Andreas Schruba (Max-Planck-Institut für extraterrestrische Physik)23/08/2016, 11:00State-of-the-art instrumentation is currently revolutionizing our view on the gas-star cycle in nearby galaxies by resolving individual star-forming clouds and their young stellar population. I will highlight recent results from several concerted legacy-type surveys targeting galaxies in the Local Group and Local Universe. This includes (a) the structure of the atomic and molecular gas...Go to contribution page
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Nimisha Kumari (Institute of Astronomy, Cambridge, United Kingdom)23/08/2016, 11:20The Kennicutt-Schmidt law relating the surface densities of the star-formation rate (SFR) and gas (atomic and molecular) is a widely-accepted star-formation law. However, it is a disk-averaged law smoothing over local variations, and hence may not provide an explanation for the local relationship between SFR and gas density at the sub-galactic scale. To further probe this, various groups...Go to contribution page
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Sarah Ragan (University of Leeds)23/08/2016, 11:40In the era of multi-wavelength surveys of the Milky Way, we are well-equipped to observationally characterise the conditions necessary for star formation on parsec size-scales. With this wealth of information, we can now not only ask the question of what these conditions are, but also why they arise where they do. I employ the Herschel Galactic Plane survey (Hi-GAL) to study the connection...Go to contribution page
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Camilo Penaloza (Cardiff University)23/08/2016, 12:00Over the past decade, there has been a move to better connect observations with numerical simulations. In this work we focus on mimicking the CO emission for simulated Giant Molecular Clouds (GMCs). We performed a set of smooth particle hydrodynamics (SPH) simulations with time-dependent chemistry, in which environmental conditions such as mass, density, size, metallicity and Interstellar...Go to contribution page
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Karl Schuster23/08/2016, 12:20M33 was mapped in the CO 2-1 transition with a resolution of 50 pc. The IRAM M33 mapping project covers a complete area out to galactic radii of 7 kpc. Combining these data with HI and and FIR dust measurements on similar scales allows to extend the method used by Sandstroem 2011 by introducing an additional local CO dark molecular gas column density. We discuss potential influence of...Go to contribution page
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Francoise Combes (Observatoire de Paris, LERMA)23/08/2016, 14:30Beyond the observed proportionality between surface densities of molecular gas and star formation, the efficiency of star formation varies significantly with environment. I will review the situations where the star formation is triggered by dynamical processes, such as bars or spirals, tidal interactions, ram-pressure due to AGN feedback or in groups and clusters.Go to contribution page
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Alessandro Romeo (Chalmers University of Technology)23/08/2016, 15:15Gravitational instabilities play a primary role in shaping the structure and powering the star formation activity of disc galaxies. We review the effort made by theorists to provide the astronomical community with reliable disc stability diagnostics. The most well-known diagnostic is Toomre's Q parameter, but there are newer and more powerful tools for detecting gravitational...Go to contribution page
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Jose Utreras (Universidad de Chile)23/08/2016, 15:45Knowing how efficiently stars are formed in galaxies is fundamental to understand the evolution of our universe. Unfortunately, several physical processes governing star formation are dynamically coupled in the non-linear regime, complicating the study of their independent effects. Here we use numerical experiments to study the effects of galactic rotation, employing the Adaptive Mesh...Go to contribution page
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Mark Sargent23/08/2016, 16:35The bimodal distribution of galaxy-integrated star-formation efficiencies (SFE) in the Schmidt-Kennicutt plane (i.e. the SFR vs. M(H2) diagram) has been the subject of much debate in recent years. Is the proposed split into a ‘sequence of disks’ and a ‘sequence of starbursts’ a genuine effect or rather an artefact of selection effects or assumptions underlying the calculation of molecular...Go to contribution page
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23/08/2016, 17:15A. Heiderman, R. Kennicutt, F. Combes, O. AgertzGo to contribution page
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Anne Jaskot (Smith College)24/08/2016, 09:00Although few in number, massive stars play an outsize role in reshaping their local and global environments. Using observations of starburst regions in low-redshift galaxies, I will highlight the importance of Wolf-Rayet stellar winds, binary stellar populations, supernovae, and geometry in clearing out neutral gas from star-forming environments. This feedback from sub-galactic scales...Go to contribution page
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Chang-Goo Kim (Princeton University)24/08/2016, 09:45Supernova (SN) explosions inject a prodigious amount of energy into the interstellar medium (ISM). This powerful feedback implies that SNe are a major driver of turbulence and galactic winds, and may be the dominant regulator of star formation (SF) in disk galaxies. Our understanding of the interaction of SN(e) with the ISM have gradually improved over many decades. However, a complete and...Go to contribution page
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Ben Keller (McMaster University)24/08/2016, 10:30M* galaxies, 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*...Go to contribution page
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Arjan Bik (Stockholm University)24/08/2016, 11:20The feedback of massive stars and star clusters has a dramatic effect on the surrounding interstellar matter (ISM), affecting the shape and fate of galaxies as a whole. The molecular ISM in which the stars are formed is transformed to a warm ionized medium by means of the Lyman continuum output as well as the stellar wind and supernovae of the massive stars in the galaxy. The large...Go to contribution page
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Katherine HOLLYHEAD (Astrophysics Research Institute)24/08/2016, 11:40The initial stages of star cluster formation (the first 10 Myr) are still not entirely clear, though this age is highly important for understanding their subsequent evolution and that of the galaxy itself. We have studied a sample of young massive clusters (<10 Myr, >5000 solar masses) in nearby spiral galaxy M83, using archival HST WFC3 data available on the HST Legacy Archive. By...Go to contribution page
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Peter Creasey (University of California at Riverside (UCR))24/08/2016, 12:00The mechanisms of feedback in which Milky-Way and smaller galaxies are regulated by events on scales of parsecs and below is still poorly understood. In this talk I will look at hydrodynamical simulations on cosmological and interstellar medium scales and tease out some of the dynamical and chemical indicators at small and large (galaxy population) scales that can be used to identify the...Go to contribution page
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Robbert Verbeke (Ghent University)24/08/2016, 12:20Dwarf 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...Go to contribution page
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Evangelia Ntormousi (CEA/Saclay)24/08/2016, 12:40The large-scale shocks formed by the clustered feedback of young stars are considered an important source of mechanical energy for the interstellar medium and a trigger of molecular cloud formation. Their interaction sites are locations where kinetic energy and magnetic field are redistributed between ISM phases. In this work we study the role of turbulence and magnetic fields in the...Go to contribution page
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Wako Ishibashi (ETH Zurich)24/08/2016, 13:00Black hole feedback is often invoked to suppress star formation in galaxies by driving galaxy-scale outflows. However, radiative feedback from the central black hole may actually trigger star formation within those galactic outflows. In our picture, new stars are formed at increasingly larger radii in the outflowing shell, with young stellar populations gradually populating the outer...Go to contribution page
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Amelie Saintonge (University College London)25/08/2016, 09:00Over the past 5 years, it has become possible to assemble measurements of molecular gas in large samples of normal star-forming galaxies up to z=2. These observations have been key in establishing the currently favoured model for galaxy evolution, which is centered around the cycling of gas in and out of galaxies and the efficiency of the star formation process. While star formation is a...Go to contribution page
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Kathryn Kreckel (MPIA)25/08/2016, 09:45While spiral arms are the most prominent sites for star formation in disk galaxies, interarm star formation contributes significantly to the overall star formation budget. However, it is still an open question if the star formation proceeds differently in the arm and inter-arm environment. We use deep VLT/MUSE optical IFU spectroscopy to resolve and fully characterize the physical...Go to contribution page
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Abdurrouf Abdurrouf (Astronomical Institute, Tohoku University)25/08/2016, 10:05According to Lambda CDM paradigm of hierarchical galaxy formation, galactic disks were form gradually from inside to outside (“inside-out” scenario of galaxy formation). In spite of this being a long-known prediction, but very few observational evidences have been brought forward to support it. In order to sought the indication of this “inside-out” scenario in the local universe and also...Go to contribution page
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Quentin SALOME (LERMA, Observatoire de Paris)25/08/2016, 10:25Recent 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...Go to contribution page
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Isadora Chaves Bicalho (Observatoire de Paris)25/08/2016, 11:15The spatially resolved star formation law has been studied in great detail in galaxies in recent years. At high surface density, when most of the gas is molecular, the Kennicutt-Schmidt relation is almost linear providing a constant gas consumption time-scale of about 3Gyr (e.g Bigiel et al. 2011, Saintonge et al 2011). However the star formation efficiency (SFE) falls very quickly when...Go to contribution page
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Rodrigo Herrera-Camus (Max Planck Institute for Extraterrestrial Physics)25/08/2016, 11:35The [CII] 158 um and [NII] 122 and 205 um far-infrared transitions are powerful tracers of the neutral and ionized gas in the interstellar medium of local and high-z galaxies. In this talk I will discuss the ability of these lines to trace the star formation activity in a wide range of environments that include low metallicity, normal, star-forming galaxies, AGN, LIRGS and high-z...Go to contribution page
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Martin Roth (Leibniz Institute for Astrophysics Potsdam (AIP))25/08/2016, 11:55We present first results from a study of resolved stellar populations in the 2 Mpc distant sculptor group disk galaxy NGC300 using integral field spectroscopy with MUSE. From data cubes obtained under conditions of excellent seeing we are able to extract on the order of 1500 stellar spectra per pointing of 1.5 hours observing time, using the PampelMuse code that has already...Go to contribution page
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Karen Knierman (Arizona State University)25/08/2016, 12:25While major mergers and their tidal debris are well studied, equal mass galaxy mergers are relatively rare compared to minor mergers (mass ratio <0.3). Minor mergers are less energetic than major mergers, but more common in the observable universe, and thus likely played a pivotal role in the formation of most large galaxies. Tidal debris regions have large amounts of neutral gas but a...Go to contribution page
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Alton Padraig (Durham University)25/08/2016, 12:45Massive elliptical galaxies are thought to form in two stages - first, the formation of a central core via fast dissipative processes by z~2, followed by the accumulation of mass through (mostly minor) dry mergers. A combination of evidence from spectroscopy, lensing, and stellar dynamics appears to suggest that in the most massive central cores stars form according to a 'bottom-heavy' IMF...Go to contribution page
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Janice Lee (Space Telescope Science Institute)25/08/2016, 14:30Since the discovery of "isolated extragalactic H II regions" by Sargent & Searle in 1970, low mass dwarf galaxies experiencing intense bursts of star formation have periodically become the subject of frenetic research because of their unusual and discordant properties. Today, the study of massive star formation and its impact on the interstellar medium seems to be at a major crossroad,...Go to contribution page
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Stijn Wuyts (University of Bath)25/08/2016, 15:15For many years, far-infrared and optical/near-infrared astronomers focused on largely disjoint samples of high-redshift galaxies. While the far-infrared community primarily studied luminous and dusty starbursting monsters, detailed spectroscopic analyses in the (rest-)optical preferentially targeted less obscured systems. With the increased sensitivity offered by Herschel, PdBI-NOEMA and...Go to contribution page
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Dawn Erb (University of Wisconsin Milwaukee)25/08/2016, 16:30Low mass, low metallicity galaxies are the most likely source of the photons that reionized the universe, but the relationships between low metallicity star formation, galactic outflows, and the escape of ionizing radiation at high redshifts are still unclear. Using rest-frame UV and optical spectra of lensed and unlensed low metallicity galaxies at z~2, I will discuss constraints on the...Go to contribution page
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25/08/2016, 17:00A. Jaskot, A. Saintonge, C. G. Kim, J. Lee, S. WuytsGo to contribution page
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Andrew Battisti (UMass Amherst)26/08/2016, 09:00The presence of dust in galaxies can significantly alter their observed spectral energy distribution. If not properly accounted for, this effect can lead to incorrect values of derived physical quantities such as the star formation rate, stellar mass, and photometric redshift. Virtually all studies of star forming galaxies, both local and distant, make use the attenuation curve derived...Go to contribution page
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Anna Cibinel (Astronomy Centre, U. of Sussex)26/08/2016, 09:20Key aspects of galaxy evolution including bulge formation and quenching may be regulated by the dynamics of large star forming clumps which are almost ubiquitous in the gas-rich ISM medium of normal high redshift galaxies. The impact of clump-driven dynamical processes on the evolution of galaxies depends crucially on whether these giant clumps are transient phenomena or not. Clump...Go to contribution page
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Lea Hagen (Penn State University)26/08/2016, 09:40The Swift Ultraviolet/Optical Telescope (UVOT) is uniquely suited to study star formation and dust extinction in nearby galaxies. I will discuss results from the Small Magellanic Cloud (SMC) and M33, for which we have unprecedented observations in three near-UV bands from 1700-3000 A at 2.5" resolution. We combine our UV imaging with archival optical and infrared data to model the...Go to contribution page
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Matthew Hayes (Stockholm University)26/08/2016, 10:00I will present the first image of an individual extragalactic object in which the coronal gas phase (T ~300,000 K) is both isolated and spatially resolved, by targeting the O VI doublet at 1032,1037 Å in emission. The combination of HST UV imaging and spectroscopy provides unique new insights into the mass, cooling, kinematics, and ultimately the fate of gas that has been heated by...Go to contribution page
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Jennifer Schober (Nordita)26/08/2016, 11:00Magnetic fields are omnipresent in local galaxies and can affect the star formation process crucially. Observational evidence between the coupling of the magnetic field and the star formation rate (SFR) comes from the far-infrared(FIR)-radio correlation which holds over more than six orders of magnitude. While the FIR radiation is a tracer of the SFR, radio emission is typically...Go to contribution page
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Polychronis Papaderos (Instituto de Astrofísica e Ciências do Espaço, Centro de Astrofísica da Universidade do Porto)26/08/2016, 11:20Despite significant progress over the past decades, all state-of-the-art population spectral synthesis (pss) codes suffer from two major conceptual deficiencies that limit their potential of gaining sharp insights into the star formation history (SFH) of star-forming (SF) galaxies and potentially introduce substantial biases in studies of their physical properties (e.g., stellar mass and...Go to contribution page
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Jens Melinder26/08/2016, 11:40The Lyman apha reference sample (LARS) is a major multiwavelength imaging and spectroscopic campaign of local normal star-forming galaxies, UV-luminous starburst systems, and luminous infrared galaxies using HST and ground-based telescopes. The aim of this survey is to probe what physical conditions and processes regulate the emission of Lyα radiation on local and global galactic scales....Go to contribution page
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Daniela Calzetti (UMASS)26/08/2016, 13:30Using recent 1.1 mm maps of the dust continuum of NGC4449 obtained with the Large Millimiter Telescope (LMT), we derive a high-angular resolution map of the gas in this nearby dwarf starburst galaxy. We combine the gas map with star formation rate tracers at optical and infrared wavelengths, and investigate the SFR-gas relation at ~250 parsec resolution.Go to contribution page
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Thøger Emil Rivera-Thorsen (Stockholm University)26/08/2016, 13:50The ISM of starburst galaxies is well known to contain a wide variety of physical conditions and be kinematically complex. Yet, when describing it spectroscopically, a single number is often relied on to characterize each physical property, derived from data integrated over the entire slit. Here, we present a highly detailed spatial and kinematic decomposition of 2D spectra of three...Go to contribution page
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Johannes Puschnig (Stockholm University)26/08/2016, 14:10Carbon 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...Go to contribution page
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Robert Kennicutt (University of Cambridge)26/08/2016, 14:30
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Amelia Stutz (MPIA)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...Go to contribution page
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Ricardo Retes (INAOE)We study the star formation (SF) law in 12 Galactic molecular clouds with ongoing high-mass star formation (HMSF) activity, as traced by the presence of a bright IRAS source and other HMSF tracers. We define the molecular cloud (MC) associated to each IRAS source using 13^CO line emission, and count the young stellar objects (YSOs) within these clouds using GLIMPSE and MIPSGAL Spitzer...Go to contribution page
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