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21/10/2013, 09:00Dissociative recombination of molecular ions is an important process in the gas phase chemistry of the interstellar medium. This process has been successfully studied for a wide range of systems in storage ring merged-beam experiments using, e.g., the Test Storage Ring (TSR) in Heidelberg. However, for cold ion chemistry processes these experiments hit limitations. On the one hand the thermal...Go to contribution page
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Roberto Galvan-Madrid (ESO-Garching)21/10/2013, 09:00The Multi-Scale Continuum and Line Exploration of W49 (MUSCLE W49) is a comprehensive gas and dust survey of the parental giant molecular cloud (GMC) of W49A, the most luminous ($L \sim 10^{7.3} L_{sun}$) star-formation region in the Milky Way. The project has multiple components that cover the entire GMC at different scales and angular resolutions. We present results from observations with...Go to contribution page
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Tigran Arshakian (Universität zu Köln)21/10/2013, 09:00We develop a wavelet-based cross-correlation (WCC) method to study the correlation between characteristic structures in molecular clouds as a function of scale. The method compares a pair of maps observed in different tracers, at different wavelenghts or in different velocity ranges. Advantages of the WCC: (i) it allows to measure the correlation coefficient and structural offset between two...Go to contribution page
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László Szücs (Universität Heidelberg, ZAH, ITA)21/10/2013, 09:00Carbon monoxide molecule (CO) and its isotopes are frequently used as tracers of column density in studies of the dense interstellar medium. The most abundant CO isotope, $^{12}$CO, is usually optically thick in intermediate and high density regions and so provides only a lower limit for the column density. In these regions, less abundant isotopes are used, such as $^{13}$CO. To relate...Go to contribution page
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21/10/2013, 09:00The study of ion chemistry in the interstellar medium (ISM) requires among others knowledge about cross sections and branching ratios for the recombination of atomic and molecular ions with low-energy electrons. In the case of singly charged atomic ions, experimental studies only exist for the lightest systems while for the heavier systems of astrophysical relevance, i.e., N+ to Ni+, all rate...Go to contribution page
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21/10/2013, 09:00Dissociative recombination (DR) of molecular ions is a key chemical process in the cold interstellar medium (ISM). DR affects the composition, charge state, and energy balance of such environments. Astrochemical models of the ISM require reliable total DR cross sections as well as knowledge of the chemical composition and excitation states of the neutral DR products. Theory cannot reliably...Go to contribution page
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21/10/2013, 09:00We present laboratory measurements of the wavelength-dependent dust opacity for amorphous Mg/Fe-silicate particles in the far-infrared range. Such amorphous silicates represent likely the major dust component in interstellar space. Their opacity bears a strong temperature dependence, which is not yet fully explored. We have synthesized silicates with a variable Mg/Fe ratio and have measured...Go to contribution page
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Dr David Hubber (Excellence Cluster Universe)21/10/2013, 09:00We present GANDALF, a new hybrid SPH and N-body code for combined star formation, planet formation and star cluster studies. GANDALF is written in C++ to perform the main hydrodynamic and gravitational computations. GANDALF also includes a python library to allow interactive simulations and visualisation. Initial conditions can also be generated inside python allowing simple control of setting...Go to contribution page
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Ke Wang (ESO)21/10/2013, 09:00We present high-resolution Submillimeter Array (SMA) 1.3 and 0.88 mm broad band observations, and Jansky Very Large Array (JVLA) observations in NH3 (J,K) = (1,1) up to (5,5), as well as H2O and CH3OH maser lines toward the two most massive and dense molecular clumps (>~10^3 Msun within <1pc) in the filamentary IR-dark cloud (IRDC) G11.11-0.12, also known as the "Snake" nebula. The sensitive...Go to contribution page
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Jeong-Gyu Kim (Seoul National University)21/10/2013, 09:00The neutral component of the interstellar medium (ISM) is segregated into the cold neutral medium (CNM) and warm neutral medium (WNM) as a result of thermal instability. It was found that the CNM--WNM evaporation interface, across which the CNM undergoes thermal expansion, is linearly unstable to corrugational disturbances, in complete analogy with the Darrieus-Landau instability (DLI)...Go to contribution page
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Dr Stefano Bovino21/10/2013, 09:00The study of the ISM includes a large set of processes and phenomena that needs an ac- curate modeling and which are often CPU-demanding: chemistry, cooling, heating, dust evolution, photochemistry, and many others. To cope with these we developed a package, named KROME, which is designed to manage the chemistry and the related phenomena with ease. It consists of a Python pre-processor that...Go to contribution page
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21/10/2013, 09:00The Lupus I cloud complex is located in the collision zone between two expanding super-bubbles that are driven by the massive stars in two sub-groups of the ScoCen OB association. With a distance of just 150 pc, it represents the nearest example where we can study how such a collision process forms new dense clouds in the ISM. With multi-wavelength data available, we are able to condcut a...Go to contribution page
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Andy Pon (University of Leeds)21/10/2013, 09:00Molecular clouds exhibit large linewidths, which are usually interpreted as being due to supersonic turbulence. This turbulence plays a key role in many theories of star formation, as it is believed to help support and fragment molecular clouds. Current numerical MHD simulations show that the turbulent energy of a molecular cloud dissipates on the order of a crossing time, but do not...Go to contribution page
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Robertas Aluzas (School of Physics and Astronomy, University of Leeds)21/10/2013, 09:00The interstellar medium (ISM) is highly structured and inhomogeneous. Density enhancements (clouds) that occupy a small volume fraction can dominate the mass fraction. The interaction between clouds and flows is a key process affecting the behaviour and evolution of the ISM, with implications for star formation and galaxy evolution. For instance, dense clouds may be destroyed by a flow, while...Go to contribution page
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Jonathan Heiner (CRyA, UNAM Morelia)21/10/2013, 09:00Cold, self-absorbing atomic hydrogen can be seen as absorption features in the broader HI profile. However, unless emission of molecular gas (typically CO) at the same velocity as the absorption feature is detected, it is not always possible to distinguish between self-absorption and the lack of HI emission. Ideally one would want to dispense with the need to detect molecular emission, since...Go to contribution page
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21/10/2013, 09:00We propose in this work to look at the mobility of C+ ions moving in a neutral helium gas. The calculations are performed for the cooled buffer gas into three steps. The first step consists of calculating the interaction potentials corresponding to the dimers which dissociate into C+(2P)-He(1S) and C+(4P)-He(1S). This task is accomplished with MOLPRO. Then, following the suggestions stated in...Go to contribution page
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Jonathan Smoker (European Southern Observatory (VLT))21/10/2013, 09:00We describe a search for tiny-scale structure in the interstellar medium using archive twin-epoch measurements of resolution 42,000 and 120,000 towards hundreds of stars. Our aim is to discover more examples of time-variation in the interstellar medium and determine if they can be explained by varying physical conditions, the statistical properties of the ISM, or by ""real"" structures such as...Go to contribution page
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21/10/2013, 09:00We present a suite of simulations of a vertical stratified box with extents of +- 20 kpc and a footprint of 1 kpc^2 including self-gravity, supernova feedback, magnetic fields and a resolution of 2pc. We are able to resolve the ISM structure in the disk midplane and follow SN ejecta using tracer particles based on an Monte-Carlo advection scheme. The large vertical extents allow us to follow...Go to contribution page
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21/10/2013, 09:00We numerically study the volume density probability density function (n-PDF) and the column density probability density function (\sigma-PDF) resulting from thermally bistable turbulent flows with and without self-gravity. For this aim we analyze three- dimensional hydrodynamic models in periodic boxes of 100pc by side with forced turbulence at large scales and different Mach numbers (M). At...Go to contribution page
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Catherine McEvoy (Queen's University Belfast)21/10/2013, 09:00The tiny scale structure (from 1 AU to 1 pc) of the ISM is generally poorly understood. High resolution optical spectroscopic observations, both new and archival, have been used to delve into this tiny structure to see just how ubiquitous it is and to try to understand what causes such variation to occur. Interstellar absorption lines from a selection of 96 O and B type stars spectra,...Go to contribution page
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Simon Bihr (Max Planck Institute for Astronomy)21/10/2013, 09:00How do molecular clouds form from the diffuse atomic interstellar medium? To address this and further questions we are conducting the THOR survey, a galactic plane survey (l = 15 to 60dec and b = -1 to +1dec) of the 21cm HI line, four OH lines, and 20 recombination lines as well as the continuum from 1 to 2 GHz at a spatial resolution of ~20arcsec. We got granted 110 hours at the VLA in...Go to contribution page
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Ji-hyun Kang (Korea Astronomy and Space Science Institute)21/10/2013, 09:00Turbulence study of the neutral hydrogen gas associated with supernova remnants (SNRs) has not been done so far, in spite of the fact that many HI surveys have been used to characterize the turbulent interstellar medium. This is mainly because the shocked HI emission of SNRs is difficult to be distinguished from the ambient HI emission in the Galactic Plane. We notice that some expanding HI...Go to contribution page
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Juan Camilo Ibañez (ZAH/ITA)21/10/2013, 09:00Studying how self-gravitating turbulence in the interstellar medium determines the morphology, density profile and velocity dispersion of dense molecular clouds is key to understand the initial conditions of star formation. We use the Flash adaptive mesh refinement magnetohydrodynamics code to perform three-dimensional numerical simulations of a vertical column of the interstellar medium...Go to contribution page
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Cinthya Herrera (NAOJ)21/10/2013, 09:00The Antennae are a spectacular example of a burst of star formation triggered by the encounter of two galaxies. They are an ideal source to understand how the dynamics of galaxies in mergers trigger the star formation. In the Antennae, most of the newly formed stars are observed in massive clusters (up to 10^7 Msun), dubbed super star clusters, located in the region where the two galaxies...Go to contribution page
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Lukas Konstandin (Institut für Theoretische Astrophysik, Heidelberg)21/10/2013, 09:00Observations reveal that supersonic turbulence is prevalent in star forming clouds. The density and velocity field within these clouds indicate complex, chaotic, and filamentary structures, where turbulent motions interact with shocks. Therefore, understanding the properties of turbulence is a prerequisite for developing a comprehensive theory of star formation in the ISM. We study a set of...Go to contribution page
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Andreas Burkert (LMU)21/10/2013, 09:00
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Norbert S. Schulz (MIT)21/10/2013, 09:00The interstellar medium (ISM) absorbs and scatters X-rays and its signatures can be used to diagnose its states of matter, compositions, and dynamical properties. With the availability of precision X-ray optics and spectrometers as onboard the Chandra X-ray Observatory, scattering halos around bright X-ray sources and K/L shell X-ray absorption are now observed and masured in detail....Go to contribution page
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Ralf Klessen (ZAH/ITA, University of Heidelberg)21/10/2013, 09:15
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Dr Stefanie Walch (Max-Planck-Institut für Astrophysik)21/10/2013, 09:55review talk
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Kazunari Iwasaki (Nagoya University)21/10/2013, 11:05contributed talkNonlinear evolution of bistable interstellar medium is investigated using two-dimensional simulations with a realistic cooling rate, heat conduction, and physical viscosity. The calculation is performed in periodic boundary conditions without any external forcing. As the initial condition, spatially uniform unstable gas under thermal equilibrium is considered. At the initial stage, the...Go to contribution page
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Evangelia Ntormousi (SAp/CEA Saclay)21/10/2013, 11:20contributed talkRecent observational results have shown that local interstellar filaments follow a thickness distribution which is surprisingly narrowly peaked at 0.1 pc for a wide range of column densities. This fact is pertinent to the study of interstellar gases as a fingerprint of the physical mechanisms acting on that scale. But what can create structure of a characteristic size when both gravity and...Go to contribution page
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Peter Scicluna (ESO)21/10/2013, 11:35contributed talkThe spatial distribution of dust has significant influence on the observed extinction curve. As a result, when observing anisotropic, clumpy or turbulent environments the aperture may contain a wealth of unresolved structure. Hence, observations only probe an effective optical depth and effective extinction curve. In order to elucidate and quantify the impact of unresolved structure we perform...Go to contribution page
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Hans Zinnecker (Deutsches SOFIA Institut)21/10/2013, 11:50contributed talkI will present a short summary of the status of SOFIA, the Stratospheric Observatory for Infrared Astronomy. SOFIA has been deployed to the Southern Hemisphere in July 2013 and completed 9 successful flights out of Christchurch, New Zealand. Some amazing results from from these FIR observations with GREAT are emerging, including detection of the 2.5 THz OH and 2.7 THz HD ground state...Go to contribution page
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Joao Alves (University of Vienna)21/10/2013, 12:05review talkUnderstanding how matter is organized inside a molecular cloud is key to understand where and how stars form. In this talk we summarize the main results from our ongoing program on NIR extinction on nearby molecular clouds, complemented with recent Herschel archival data. Our sample comprises all the nearby molecular cloud complexes in their entirety, from Pipe Nebula to the Orion complex,...Go to contribution page
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Nicola Schneider (LAB Bordeaux)21/10/2013, 14:15contributed talk
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Doris Arzoumanian (IAS Orsay)21/10/2013, 14:30contributed talkHerschel dust continuum images have revealed the ubiquity of filaments in the interstellar medium (ISM) and their fundamental role in the star formation process. Planck dust polarization observations trace the magnetic field structure of the ISM. Filamentary structures are formed by the interplay of interstellar turbulence, gravity and magnetic field. What is the role of these various...Go to contribution page
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Gesa Bertrang (ITAP, University of Kiel)21/10/2013, 14:45contributed talkThe influence of magnetic fields on the star-forming process is still under debate. A very good environment to study this influence is given in low-mass star-forming regions, so-called Bok globules. These objects are less affected by other processes, such as large-scale turbulences. The magnetic field strength and structure in the dense inner regions of these globules can be determined by...Go to contribution page
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Jouni Kainulainen (Max-Planck-Institute for Astronomy)21/10/2013, 15:00contributed talkSupersonic turbulence has a profound impact on the density structure of the cold interstellar medium (ISM). Consequently, observations of the ISM density structure can be used to constrain the fundamental properties of turbulence. However in practice, connecting the observed density structure to theoretical predictions is greatly hampered by the inability of observations to probe the wide...Go to contribution page
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Rowan Smith (ZAH/ITA University of Heidelberg)21/10/2013, 15:15contributed talkFilaments are seen throughout the ISM, from long filamentary IRDCs to individual filamentary sites of star formation. Using the moving mesh code AREPO we can investigate filament formation on all scales, as the unique combination of a Lagrangian mesh with a Riemann solver results in an extremely accurate treatment of shocks and discontinuities. I will describe how filamentary molecular clouds...Go to contribution page
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Fabian Heitsch (University of North Carolina Chapel Hill)21/10/2013, 16:00review talkReviewGo to contribution page
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Patrick Hennebelle (SAp/CEA Saclay)21/10/2013, 16:30review talk
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Paul Clark (ZAH/ITA, University of Heidelberg)21/10/2013, 17:00contributed talkTo date, numerical studies of the IMF have adopted initial conditions that are very dense -- often comparable to the densities of individual prestellar cores that are observed in giant molecular clouds (GMCs). These calculations, which start in the regime where the gas and dust are already strongly coupled, can say nothing about conditions we observe in nearby star-forming regions. In...Go to contribution page
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Jo Barnes (University of St Andrews)21/10/2013, 17:15contributed talkWe investigate 3D photoionisation models of the Diffuse Ionised Gas (DIG). Our simulations show that in a supernova-driven, turbulent magnetised medium photons from OB stars in the Galactic plane are able to travel many kiloparsecs and reach heights required to ionise the DIG. To reach these heights photons travel through ?bubbles? evacuated by supernovae close to the midplane of the...Go to contribution page
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Prof. Edith Falgarone (LERMA/LRA Ecole Normale Supérieure)21/10/2013, 17:30The diffuse interstellar medium has long been known to harbor a remarkable molecular richness, that cannot be understood in the framework of state-of-the-art UV-driven chemistry. Absorption spectroscopy performed with Herschel/HIFI reveals unexpected large abundances of small hydrides that are the building blocks of interstellar chemistry in the diffuse medium. Because they are so abundant...Go to contribution page
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Matthew Bate (University of Exeter)22/10/2013, 09:00review talk
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Paula Stella Teixeira (University of Vienna, Department of Astrophysics)22/10/2013, 09:40contributed talkIt is well established for several decades that filamentary structures are very common in star forming molecular clouds. Observational studies of how these structures evolve and fragment to form cores (and subsequently stars) may ultimately lead us to better understand how the core mass function (CMF) and stellar initial mass function (IMF) are assembled. The fragmentation of these filamentary...Go to contribution page
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Enrique Vazquez-Semadeni (CRyA, UNAM)22/10/2013, 09:55contributed talkI present results from numerical simulations and an analytical model of the formation and gravitational collapse of giant molecular clouds (GMCs). The clouds develop a network of filaments at various scales, whose physical properties we compare with recent observations. Simulations including ionizing stellar feedback show that its effect is the destruction of the local star-forming...Go to contribution page
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Katharine Johnston (MPIA, Heidelberg)22/10/2013, 10:10contributed talkThe massive infrared dark cloud G0.253+0.016 projected 45pc from the Galactic centre contains 10^5 Msun of dense gas whilst being mostly devoid of observed star formation tracers. To scrutinise the gas properties of G0.253+0.016, we have carried out a concerted SMA and IRAM 30m study of this enigmatic cloud in dust continuum, CO isotopologues as low-density tracers, as well as CH3OH and SiO as...Go to contribution page
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Cornelia Jäger (Laboratory Astrophysics Group of the Max Planck Institute for Astronomy)22/10/2013, 10:55review talk
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Holger Kreckel (MPIK, Heidelberg)22/10/2013, 11:35contributed talkAs an ever increasing number of molecules are observed in interstellar space, accurate laboratory data on their formation and destruction processes will be required to understand interstellar reaction networks. Astrochemical models have identified ion-molecule reactions as one of the drivers for the buildup of molecules in space. On the other hand, dissociative recombination with free...Go to contribution page
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Andreas Wolf (MPIK, Heidelberg)22/10/2013, 11:50contributed talkLow energy collisions of electrons with atomic and molecular ions are among the most basic microscopic interactions in the interstellar medium. Electron-ion recombination limits the abundance of charged atoms molecules and, as dissociative recombination of molecular ions, produces neutral radical fragments for gas phase reaction chains. Moreover, electron impact excitation can influence...Go to contribution page
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Simon Glover (ZAH/ITA University of Heidelberg)22/10/2013, 12:05review talk
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Thomas Henning (MPIA Heidelberg)22/10/2013, 14:05review talk
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Marta Alves (Institut d'Astrophysique Spatiale (IAS))22/10/2013, 14:35contributed talkThe Planck all-sky survey has opened a new window in our understanding of interstellar dust emission in extending to sub-millimetre wavelengths and microwave frequencies the detailed mapping of dust emission provided by past infrared missions. Such a wide frequency coverage allows us to probe the spectral energy distribution (SED) of large and cold dust grains, which are the bulk of the dust...Go to contribution page
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Henrik Beuther (MPIA)22/10/2013, 14:50contributed talkThe interstellar medium (ISM) is mainly comprised of ionized, neutral atomic and molecular gas. One of the most important constituents of these phases is carbon in its ionized/neutral/molecular form (C^+, C^0 and CO). However, until recently a coherent analysis of the different phases at adequate resolution (Jeans length ~0.2pc) is lacking. We therefore conducted at study of the spectral lines...Go to contribution page
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Bastian Gundlach (Institut für Geophysik und extraterrestrischer Physik, TU Braunschweig)22/10/2013, 15:05contributed talkGrain growth by coagulation of ice and dust particles has been postulated and observed in the densest and coldest interstellar clouds. Thus, we have performed laboratory experiments in order to simulate inter-particle collisions in these environments. The experiments were used to measure the sticking threshold of micrometer-sized water ice particles for different grain sizes, velocities, and...Go to contribution page
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Ralf Siebenmorgen (ESO)22/10/2013, 15:20contributed talkWe present a model for the diffuse interstellar dust that explains the observed wavelength-dependence of extinction, emission, linear and circular polarisation of light. The model is set up with a small number of parameters. It consists of a mixture of amorphous carbon and silicate grains with sizes from the molecular domain of 0.5 up to about 500nm. Dust grains with radii larger than 6nm are...Go to contribution page
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Svitlana Zhukovska (Max Planck Institute for Astronomy)22/10/2013, 16:05contributed talkDust grains are indispensable part of the matter cycle, which plays an important role in many physical processes in the ISM. Interstellar dust content is determined by the interplay between dust formation by stars, destruction in the ISM and dust growth by mantle accretion in the ISM. The relative importance of these processes depends on both the stage of galactic evolution and metallicity...Go to contribution page
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Adam Leroy (NRAO Charlottesville)22/10/2013, 16:20review talk
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Diederik Kruijssen (MPA Garching)22/10/2013, 17:00contributed talkGalactic star formation (SF) relations are known to develop substantial scatter or even change form when considered below a certain spatial scale. I will quantify how this behaviour should be expected due to the incomplete statistical sampling of independent star-forming regions. Other included limiting factors are the incomplete sampling of SF tracers from the stellar initial mass function...Go to contribution page
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Sarah Ragan (Max Planck Institute for Astronomy)22/10/2013, 17:15contributed talkThe question of how high-mass stars form relies fundamentally on the initial conditions. Due to the large distances to high-mass star-forming complexes and their precursors known as infrared-dark clouds (IRDCs), high-angular resolution is required to resolve individual cores. With the advent of Herschel, we now have access to the wavelength regime in which the cold dust comprising the clouds...Go to contribution page
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Javier A. Rodon (ESO)22/10/2013, 17:30contributed talkRodón, J. A. (1): Beuther, H. (2): Zhang, Q. (3): Schilke, P. (4) (1) European Southern Observatory; (2) Max-Planck Institut für Astronomie; (3) Harvard-Smithsonian Center for Astrophysics; (4) Universität zu Köln In the last decade, we have started to spatially resolve the small gas and dust condensations in high-mass star-forming regions that will eventually become a massive star or...Go to contribution page
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Amelia Stutz (MPIA)22/10/2013, 17:45contributed talkUnderstanding how the gas environment within molecular clouds influences the properties of protostars is a key step towards understanding the physical factors that control star formation. We report on analysis of the connection between molecular cloud environment and protostellar properties using the Herschel Orion Protostar Survey (HOPS), a large multi-observatory survey of protostars...Go to contribution page
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Phil Cigan (New Mexico Tech)23/10/2013, 09:00Many FIR studies target systems that have typical or enhanced abundances of heavy elements, but what is the picture for the low-metallicity regime? We present a comparison of HI and [CII] observations for five extremely metal-poor dwarf galaxies from the LITTLE THINGS survey. The galaxies we discuss have 12+log(O/H) = 7.4 - 7.8, some of the lowest-metallicity galaxies observed in [CII]. Our...Go to contribution page
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Guangxing Li (MPIfR)23/10/2013, 09:00Guang-Xing Li, Friedrich Wyrowski, Karl Menten and Arnaud Belloche Max-Planck Institut fuer Radioastronomie, Bonn, Germany Star formation occurs in molecular gas. In the previous studies, the structure of the molecular gas has been studied in terms of molecular clouds, but overlooked beyond the cloud scale. In this work, we present an observational study of the molecular gas at l~ 50....Go to contribution page
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Dominique Meyer23/10/2013, 09:00This poster presents a grid of models following the wind-ISM interaction of massive runaway stars from the main-sequence to the supernova stage. The included physics takes into account optically-thin radiative heating and cooling, together with electronic thermal conduction and assumes that the stars are moving in a medium which density corresponds to the one of the Galactic plan. Emissions...Go to contribution page
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Anahi Caldu Primo (MPIA)23/10/2013, 09:00We present evidence for the presence of a high-dispersion molecular gas component in nearby galaxies as traced through the CO(2-1) emission. The measured dispersion is higher than predicted if it was just due to the cold dense molecular gas phase in a galaxy's disk. Our analysis is based on a comprehensive study of the velocity dispersions of the atomic and molecular gas components in the...Go to contribution page
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Mykola Petrov (University of Vienna)23/10/2013, 09:00The galactic evolution is dominated by gas dynamics which can include gas infall and outflows, galactic fountains, and more and can be understandable due to differences in dynamics, thermal energies and element abundances of the gas phases. To follow the chemical and temporal evolution of galaxies it is necessary to model the gasdynamics combined with stellar dynamics, the star-gas energy and...Go to contribution page
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Kathryn Kreckel (MPIA)23/10/2013, 09:00Galactic winds are important for regulating feedback within galaxies and contribute to shaping the multi-phase ISM. We employ optical IFU observations and Herschel PACS spectroscopy to examine the kinematics and energetics of the outflow within NGC 2146. Hosting a starburst driven wind similar to M82, this late-phase merger and LIRG exhibits evidence for outflows in the dust as well as the...Go to contribution page
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Deidre Hunter (Lowell Observatory)23/10/2013, 09:00Metallicity is not a passive result of galaxy evolution, but a crucial driver. Dwarf galaxies are low in heavy elements, which has consequences for the ability to form cold, dense clouds that form stars. Molecular cores shrink and atomic envelopes grow in star-forming clouds as the metallicity drops (Bolatto et al. 2011). For this reason, CO had not been detected at log(O/H)+12 < 8.0 (Schruba...Go to contribution page
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Fatemeh Tabatabaei23/10/2013, 09:00Bars are generally considered as an important transform mechanism of molecular gas toward the central regions of galaxies. Numerical simulations suggest that barred galaxies tend to have more of their gas mass concentrated in their centers. On the other hand, it is possible that the central mass concentration is affected by more than just the presence of bars. We mapped the giant barred...Go to contribution page
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Nickolas Moeckel (USM)23/10/2013, 09:00The Scorpius-Centaurus OB association is the nearest region of recent massive star formation. With several distinct stellar groups ranging in age from a few to ~15 Myr, it presents an interesting labratory to explore the interaction between stellar feedback, the ISM, and the formation of clusters and associations from molecular clouds. An apparent age sequence along the association raises the...Go to contribution page
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Stefan Ohm (Dept of Physics and Astronomy, University of Leicester)23/10/2013, 09:00Westerlund 1 (Wd 1) is the most massive stellar cluster in the Galaxy and associated with an extended region of TeV emission. Here we report the results of a search for GeV $\gamma$-ray emission in this region. The analysis is based on ~4.5 years of Fermi-LAT data and reveals significantly extended emission which we model as a Gaussian, resulting in a best-fit sigma of $\sigma$_S = $(0.475 \pm...Go to contribution page
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Nalin Vutisalchavakul (University of Texas at Austin)23/10/2013, 09:00Combining several large scale Galactic plane surveys, we studied the gas distribution and star formation activities in part of the Galactic plane. Star formation rates were determined from infrared data obtained from WISE and Spitzer surveys. The Bolocam Galactic Plane Survey provided the data of 1.1mm dust continuum and dense gas tracers, while the Galactic Ring Survey provided the data of...Go to contribution page
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Oleg Egorov (Sternberg Astronomical Institute of Lomonosow Moscow State University)23/10/2013, 09:00We present observations and analysis of two dwarf Irr galaxies in M81 group - IC 2574 and Holmberg II. Their 21 cm images of these galaxies show multiple shell-like structures with sizes up to 1-2 kpc, so-called supergiant shells (SGS), most probably created by stellar feedback from several generations of stars. According to modern understanding the SGS expansion triggers new bursts of star...Go to contribution page
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Emeric Bron (LUTH - Observatoire de Paris/Université Paris Diderot)23/10/2013, 09:00The process of H2 formation on dust grains is the first step in the increase in chemical complexity leading to the multitude of molecules revealed by the latest generation of telescopes. It controls the transition from atomic to molecular gas and the resulting molecular chemistry through the central role of H2 in the chemical network. The formation rate in a diffuse medium has been inferred...Go to contribution page
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Mr Alessandro Ballone (USM/MPE, Garching)23/10/2013, 09:00A. Ballone, M. Schartmann, A. Burkert, S. Gillessen, R. Genzel, T.K. Fritz, F. Eisenhauer, O Pfuhl, T. Ott The origin of the dense gas cloud "G2" discovered in the Galactic Center (Gillessen et al. 2012) is still a debated puzzle. G2 might be a diffuse cloud or the result of an outflow from an invisible star embedded in it. I will present the first attempt of detailed simulations of...Go to contribution page
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Jennifer Schober (ZAH / Uni Heidelberg)23/10/2013, 09:00Magnetic fields influence many processes in the ISM strongly. In the primordial ISM they are usually not considered, as they are assumed not to be dynamically important yet. In the presence of turbulence, however, the small-scale dynamo can amplify weak seed fields by randomly stretching, twisting and folding the field lines. The details of this process depend on the nature of turbulence, i.e....Go to contribution page
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Mr Sebastian Körtgen23/10/2013, 09:00Authors: Bastian Körtgen, Daniel Seifried, and Robi Banerjee Affil: Hamburger Sternwarte, University of Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany Molecular clouds represent the birthplaces of stars. Their study is therefore essential to understand the formation of stars. In this study, we present two sets of simulations to analyse the formation and evolution of molecular clouds by...Go to contribution page
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Adam Ritchey (University of Washington)23/10/2013, 09:00We present a detailed analysis of the physical conditions in shocked interstellar clouds along two lines of sight through the Vela supernova remnant using new high-resolution HST/STIS spectra acquired at FUV wavelengths. From the relative populations of collisionally-excited fine-structure levels in C I and O I, we derive unique solutions for the gas density and kinetic temperature in discrete...Go to contribution page
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Volker Weiss23/10/2013, 09:00In order to help clarifying the role of protostellar jets and outflows as potential drivers for stirring the turbulence of molecular clouds, we assess physical parameters of outflows such as energy and momentum and combine near-infrared and radio data of well-investigated regions, use excitation models to account for missing transitions, and keep the time-variability of the flows as well as...Go to contribution page
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23/10/2013, 09:00We investigate the correlation between the radio continuum and far-infrared (FIR) emission in the Fireworks galaxy NGC6946. The nonthermal radio-FIR correlation changes with both star formation and magnetic field strengths. The FIR-to-radio ratio is linearly correlated with the total magnetic field strength. This connection is self-consistent and independent from the star formation feedback....Go to contribution page
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Maximilian Brunner (USM/LMU)23/10/2013, 09:00In galaxies stars are formed from a reservoir of cold molecular gas. For star formation to continue this reservoir has to be fueled with extragalactic material or else the gas is depleted. In this project we use the SPH-code GADGET to simulate a spiral galaxy that is constantly fed with new gas at a rate of five solar masses per year. We find that the star formation rate tries to adjust to the...Go to contribution page
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Mordecai-Mark Mac Low (AMNH New York)23/10/2013, 09:00review talk
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23/10/2013, 09:00Dust particles have an important impact on the astrophysics of the interstellar medium (ISM) ranging from chemistry and thermodynamics of the gas up to the dynamics of star formation. The life-cycle of interstellar dust begins with the nucleation and growth of grains in explosive ejecta or steady winds of stars. Investigations of pre-solar grains enclosed in meteorites, for example, revealed...Go to contribution page
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Thomas Gerner (MPIA)23/10/2013, 09:00Understanding the chemical evolution of young (high-mass) star-forming regions is a central topic in star formation research. The chemistry is employed as a unique tool: 1) to investigate the underlying physical processes and 2) to characterize the evolution of the chemical composition. With these aims in mind, we observed a sample of 59 high-mass star-forming regions at different evolutionary...Go to contribution page
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23/10/2013, 09:00The Sagittarius B2 (SgrB2) molecular cloud is a well-known region of high-mass star formation close to the Galactic Center. Its hot molecular core SgrB2 (M) contains at least 36 HII regions and 12 sub-mm cores. A full line survey of SgrB2 (M) has been obtained using the HIFI spectrometer aboard of the Herschel Observatory as part of the guaranteed-time key-project "Herschel/HIFI Observations...Go to contribution page
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Adam Ginsburg (University of Colorado, Boulder / European Southern Observatory)23/10/2013, 09:00Turbulence is one of the primary processes governing star formation. Many recent theories have determined the overall star formation rate of gas and even the shape of the initial mass function based purely on turbulent initial conditions. The key property governing star formation rates is the density distribution of the gas, which determines how much gas is above some "critical density" for...Go to contribution page
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Katharina Fierlinger (LMU)23/10/2013, 09:00
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Amnart Sukom (The Graduate University for Advanced Studies)23/10/2013, 09:00We present first wide-field deep near-infrared imaging polarimetry (15'x60') of the Orion A Integral Shape Filament obtained with SIRPOL, simultaneous JHKs imaging polarimeter on the IRSF telescope. Most derived magnetic field orientations from aperture polarimetry are perpendicular to the elongation of the ISF. The extended H-band polarization pattern confirms the hourglass shaped structure...Go to contribution page
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Joanne Dawson (CSIRO Astronomy and Space Science)23/10/2013, 09:40contributed talkI will examine the role of large-scale stellar feedback in the formation of new molecular clouds. The theoretical context for this is the compression, cooling and fragmentation of the atomic medium in turbulent shocks and flows, of which the ubiquitous ""supershells"" formed by multiple supernovae and stellar winds are one example. I will first report CO(J=1-0) and HI 21cm observations of the...Go to contribution page
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James Dale (Excellence Cluster Universe, Garching b. München)23/10/2013, 09:55contributed talkOn the scale of galactic disks, supernovae are likely to be the most important form of stellar feedback on the ISM. However, the environment in which the supernovae explode is likely to have been strongly modified by the action of other kinds of feedback, particularly the earlier photoionization and winds from the exploding stars. I will present SPH simulations of a parameter space of giant...Go to contribution page
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Matthias Gritschneder (Univ California, Santa Cruz)23/10/2013, 10:10contributed talkWe study the evolution of molecular clouds under the influence of ionizing radiation. First, we propose that the Pipe Nebula is an HII region swept up by the B2 star theta Ophiuchi. We propose the nebula is currently containing a three phase medium. By means of analytical calculations, we are able to show that the current size, mass and pressure of the region can be explained in this...Go to contribution page
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Andrea Gatto (MPA)23/10/2013, 10:25contributed talkTurbulence is believed to be a crucial component of the interstellar medium's energetic budget. However, its origin and injection scales are still a matter of debate. Following e.g. Mac Low & Klessen (2004), energy injection from Supernova explosions is able to generate and maintain the observed level of turbulence in the ISM, at least in ""normal"" star-forming galaxies. In addition, a...Go to contribution page
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Thomas Peters (Institut für Theoretische Physik, Universität Zürich)23/10/2013, 11:10contributed talkH II regions are important signatures of star formation, play an important role in destroying the parental molecular clouds in which stars form, and, while still in the ultracompact phase, give insight into the process of high-mass star formation. I will present simulations that consistently follow the gravitational collapse of a massive molecular cloud, the subsequent build-up and...Go to contribution page
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Eric Keto (Harvard-Smithsonian Center for Astrophysics)23/10/2013, 11:25contributed talkHII regions are the clearest sign of the formation of the most massive stars, and ionization feedback could be responsible for a number of other phenomena observed in the ISM. For example, the general field of turbulence is suspected to be driven, at least in part, by the expansion of HII regions. Ionization feedback may also be responsible, along with stellar winds, for the bubbles seen...Go to contribution page
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Prof. Thomas Preibisch (USM/LMU)23/10/2013, 11:40contributed talkThe Carina Nebula constitutes the closest galactic analog of a giant extragalactic HII region. The combination of its large population of very massive stars and its moderate distance of 2.3 kpc makes it an ideal target for detailed studies of small-scale phenomena of the stellar feedback on the surrounding clouds in a starburst-like environment. In the last few years, we have performed several...Go to contribution page
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Dominique Meyer (Argelander Institut fur Astronomie, Bonn)23/10/2013, 11:55contributed talkObservations of stellar wind bow shocks can be used to constrain stellar, circumstellar and interstellar medium (ISM) properties. This presentation aims at introducing a grid of two-dimensional hydrodynamical simulations of wind-ISM interaction of massive runaway stars. This explores the combined effects of space velocities (ranging from 20 to 70 km/s) and initial masses (ranging from 10 to 40...Go to contribution page
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Jonathan Mackey (AIfA, Uni. Bonn)23/10/2013, 12:10contributed talkAt least 25 per cent of massive stars are ejected from their parent cluster, becoming runaways or exiles, travelling with often-supersonic space velocities through the interstellar medium (ISM). Their H II regions can strongly impact the structure of the ISM: the overpressurised H II region imparts kinetic energy and momentum to the ISM; it compresses and/or evaporates dense clouds; and it can...Go to contribution page
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Ellen Zweibel (University of Wisconsin)24/10/2013, 09:00review talk
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Richard Crutcher (University of Illinois)24/10/2013, 09:30review talk
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Francois Boulanger (Institut d'Astrophysique Spatiale)24/10/2013, 10:00contributed talkThe Planck satellite has completed the first whole sky map of dust polarization in emission. The data is revealing a new sky we have started to explore. The observations have the sensitivity and angular resolution to image dust polarization over the whole sky. For the first time, we have the data needed to characterize the structure of the Galactic magnetic field and its coupling with...Go to contribution page
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Alex Hill (CSIRO Astronomy & Space Science)24/10/2013, 10:15contributed talkHigh velocity clouds (HVCs) observed around the Milky Way trace the interaction between the Galactic disk and halo and may provide fuel for star formation in the disk. However, hydrodynamic work suggests that HVCs should not be able to survive passage through the Galactic halo as far as observed. We present an analysis of Faraday rotation observations which we have used to measure magnetic...Go to contribution page
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Stefan Reißl (Christian-Albrechts-Universität zu Kiel, Institut für Theoretische Physik und Astrophysik)24/10/2013, 11:00contributed talkMagnetic fields in the interstellar medium (ISM) critically affect many astrophysical processes in various environments and scales, such as the collapse of molecular clouds, the formation of jets, and accretion of matter through circumstellar disks. However, vital questions still remain unanswered due to an apparently complex structure of the magnetic field on various scales and so far rather...Go to contribution page
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91. The far-infrared - radio correlation: Star formation and magnetic field amplification in the ISMDominik Schleicher (Institut für Astrophysik Göttingen)24/10/2013, 11:15contributed talkThe presence of magnetic fields is well-established in the interstellar medium of galaxies, which can be probed via the far-infrared - radio correlation even at high redshift. The latter corresponds to a correlation between the star formation rate and the magnetic field strength in galaxies. In this talk, I will show how such a correlation can be obtained as a result of turbulent magnetic...Go to contribution page
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Alberto Bolatto (University of Maryland)24/10/2013, 11:30review talk
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Andreas Burkert (USM/LMU)24/10/2013, 12:00review talk
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Brent Groves (MPIA)24/10/2013, 14:00contributed talkIn the local universe the mass of gas in galaxies is usually measured through the combination of the 21cm HI line, tracing the atomic gas, and the CO sub-millimeter lines that trace the molecular interstellar medium (ISM). However, the dust infrared continuum provides another tracer of the ISM mass, through two paths; the correlation of dust and gas mass, and the association of the total IR...Go to contribution page
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Manuel Behrendt (MPE, Garching)24/10/2013, 14:15contributed talkWe perform high resolution hydrodynamical simulations of gas-rich disks to get a better understanding of the origin and peculiar properties of the dominating structures in z=2 massive disk galaxies. Their structure is irregular, they have highly turbulent motions and high gas fractions of 30-80%. Stars form with enormous rates of a factor of 10-100 higher than in the Milky Way. The star...Go to contribution page
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Maria Kapala (Max Planck Institute for Astronomy)24/10/2013, 14:30contributed talkThe [CII] 158 micron line is typically the brightest emission line from star-forming galaxies and arises from both the ionized and neutral phases of the ISM. As a strong line it has been suggested both as a tracer of star-formation and a diagnostic of the ISM, but first we must distinguish the ISM phases it arises from and understand how it is excited. To address these issues we have...Go to contribution page
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Jin Koda (Stony Brook University)24/10/2013, 14:45contributed talkI will discuss the formation and evolution of giant molecular clouds (GMCs) in spiral galaxies. The evolution appears quite different between the molecule-rich and atom-rich galaxies. GMCs exist almost exclusively along HI spiral arms and filaments in atom-rich galaxies, suggesting that they form and finish their short lifetimes within the HI arms. However, in molecular-rich galaxies, GMCs are...Go to contribution page
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Dr Martin Krause (Max-Planck-Institut für extraterrestrische Physik)24/10/2013, 15:00contributed talkWith sizes from below 100 pc to just above 1kpc, superbubbles are structuring the ISM on scales in between the larger scale spiral arms and the smaller, turbulent molecular cloud scales. With 3D hydrodynamics simulation of the entire stellar evolution of and the interaction between an ensemble of massive stars we are able to explain at least some of the apparent width of observed bubbles...Go to contribution page
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Ute Lisenfeld (Universidad Granada)24/10/2013, 15:15contributed talkIn galaxy collisions gas and stars can be torn out of the parent galaxies, giving rise to tails and bridges of gas and to intergalactic star forming region of different sizes. These regions are ideal to study the conditions for the onset of star formation in very simple environments which are different from those in spiral galaxies. I will describe and compare the molecular gas properties...Go to contribution page
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Andreas Schruba (MPE, Garching)24/10/2013, 16:00contributed talkI summarize first results from a large CARMA survey to image CO(1-0) emission at high sensitivity and resolution (20pc, 1km/s) in the nearby Andromeda galaxy (M31). This survey augments a new extensive set of multi-wavelength data including Hubble, Spitzer, Herschel, VLA photometry and spectroscopy that provide an unprecedented knowledge of the stars, dust, and gas in M31. We are able to...Go to contribution page
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Rahul Shetty (ZAH/ITA, University of Heidelberg)24/10/2013, 16:15contributed talkThe star formation rate is observed to be strongly correlated with the gas surface density. This correlation is well described as a power-law with index N, now known as the Kennicutt-Schmidt (KS) relationship. Previous efforts have inferred N=1.5 when considering both resolved observations of galaxies as well as unresolved starbursting systems. More recently, analysis of resolved observations...Go to contribution page
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Javier Zaragoza-Cardiel (Instituto de Astrofísica de Canarias)24/10/2013, 16:30contributed talkWe have used interacting galaxies to explore the properties of high luminosity star forming zones. With the GHaFaS Fabry-Perot spectrometer on the 4.2m William Herschel Telescope (La Palma) we have used Halpha emission to obtain complete 2D mapping in surface brightness, velocity, and velocity dispersion of 8 paris of interecting galaxies. The detailed kinematics reveal global features such as...Go to contribution page
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Steven Longmore (Liverpool John Moores University)24/10/2013, 16:45
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Timothy Davis (ESO)24/10/2013, 17:25contributed talkThe centres of early-type galaxies are extreme environments, with strong radiation fields from old stars, high metallicities, alpha-enhancements, deep potential wells, and a high incidence of AGN. It has been shown in recent years that despite these extreme conditions a sizeable proportion of these galaxies have a cold ISM, with atomic/molecular gas and dust reservoirs. We have carried out a...Go to contribution page
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Vladimir Dogiel (P.N.Lebedev Institute of Physics)24/10/2013, 17:40contributed talkWe investigate the origin of the diffuse 6.4~keV line emission and the source of H$_2$ ionization in the diffuse molecular gas of the Galactic center (GC) region. We showed that Fe atoms are most likely ionized by X-ray photons emitted by Sgr~A$^\ast$ during a previous period of flaring activity of the supermassive black hole. The H$_2$ molecules of the diffuse gas can not be ionized by...Go to contribution page
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Tsuyoshi Inoue (Aoyama Gakuin University)25/10/2013, 09:00review talk
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Sabrina Casanova (MPIK, Heidelberg)25/10/2013, 09:40contributed talkWe solve the transport equations of cosmic rays inside a molecular cloud assuming an arbitrary energy and space dependent diffusion coefficient. Cosmic rays penetrating the cloud produce gamma-ray emission through pp collisions with the ambient gas. For small diffusion coefficients inside the cloud we expect the gamma-ray spectrum from the cloud to be harder than the Galactic diffuse emission...Go to contribution page
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Philipp Girichidis (MPA Garching)25/10/2013, 09:55contributed talkWe explore the impact of cosmic rays (CR) on the structure of the ISM, the turbulence in the Galactic disk, and how/to what extent cosmic rays drive Galactic outflows. We include the production of cosmic rays in SN remnants in a stratified box and follow the coupled system of gas and cosmic ray fluid self-consistently in three-dimensional adaptive mesh refinement simulations. The coupled...Go to contribution page
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Miwa Goto (USM/LMU)25/10/2013, 10:10contributed talkCosmic ray is a unique place that high-energy astrophysics meets low-energy chemistry. The ion molecule H3+ is the best chemical probe of the cosmic ray ionization rate, because of the simplicity of the chemical process. Meanwhile, a new gamma-ray observation identified a point like source near Sgr A*. To produce the gamma-ray flux discovered by HESS collaboration by a neutral pion decay, one...Go to contribution page
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Ruizhi Yang (Purple Mountain Observatory)25/10/2013, 10:25contributed talkWe report the results of our study on the energy spectra and absolute fluxes of cosmic rays (CRs) in the Local Galaxy based on three-year $\gamma$-ray observations of ten nearby giant molecular clouds (GMCs) belongs to the Gould Belt, with the Fermi Large Area Telescope (LAT). The $\gamma$-ray signals obtained with high statistical significance allow the determination of $\gamma$-ray spectra...Go to contribution page
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Linda Tacconi (MPE, Garching)25/10/2013, 11:10review talk
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Avishai Dekel (The Hebrew University)25/10/2013, 11:40review talk
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Muhammad Latif (Institute for Astrohphysics, Göttingen)25/10/2013, 12:10contributed talkSupermassive black holes have been observed even at redshift 7, their formation and growth need to be highly efficient in order to obtain final masses of more than 10^9 solar. Theoretical models suggest the formation of their seeds in dark matter halos with virial temperatures above 10^4 K at z~15, as such halos may cool efficiently via atomic hydrogen. At the same time, in order to avoid...Go to contribution page
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Dr Thorsten Naab (MPA)25/10/2013, 12:25contributed talkOutflows and the structure of the ISM in high-redshift galaxies Recent observations of high-redshift galaxies indicate that the conditions in their ISM are distinctively different to local galaxies. High formation rates of stars embedded in an extremely dense and highly turbulent interstellar medium with high molecular gas fractions and strong gas outflows are ubiquitous. We present new...Go to contribution page
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Silke Andree (1. Physikalisches Institut, Universität zu Köln)PosterPhoton-dominated regions (PDRs), in which the interstellar far-UV radiation field determines the energy balance and the chemistry of the ISM, form the interface between HII regions and molecular clouds. PDR emission dominates the infrared and sub-millimetre spectra in star forming regions. To understand the interplay between far-UV radiation and star formation in molecular clouds it is ...Go to contribution page
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Gary Ferland (Univ of Kentucky)contributed talkThe 2013 release of the plasma simulation code Cloudy, described in arXiv:1302.4485, includes significantly improved gas and grain physics. I compare these predictions with existing models of a variety of objects, and "universal" fitting formulate for gas cooling rates. Large differences are present.Go to contribution page
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Deidre Hunter (Lowell Observatory)PosterCO at Low-metallicity: Molecular Clouds in the dwarf galaxy WLM +++ "Metallicity is not a passive result of galaxy evolution, but a crucial driver. Dwarf galaxies are low in heavy elements, which has consequences for the ability to form cold, dense clouds that form stars. Molecular cores shrink and atomic envelopes grow in star-forming clouds as the metallicity drops (Bolatto et al....Go to contribution page
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Jonathan Braithwaite (University of Bonn)PosterFrom pulsar scintillations we infer the presence of density variations in the ISM, and there are reasons to believe that the effect is caused mainly by sheet-like structures. It has been suggested that these may be current sheets. I present arguments from basic MHD theory that this is exactly what we should expect, as well as results from simple simulations of decaying turbulence which...Go to contribution page
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Stephanie Juneau (CEA Saclay)PosterNebular line diagnostic diagrams probing the physical state of the ISM and/or the ionization sources in galaxies (star formation versus active galactic nuclei [AGN]) have been used extensively yet their behavior and interpretation at high redshifts are poorly understood. We present an empirical approach that takes into account both selection effects - due to emission line detection limit - and...Go to contribution page
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Dominik Bomans (Astronomical Institute of the Ruhr-University Bochum)PosterGalactic outflows and winds are key ingredients for the birth and live of galaxies in the intergalactic medium. Via outflows the halos of galaxies are structured, heated, and enriched with heavy elements. Galactic outflows may also major drivers of the turbulence of halo gas. Using integral field spectroscopy data from the ongoing CALIFA survey (observing a statistically well defined sample of...Go to contribution page
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Tuhin Ghosh (Institut d'Astrophysique Spatiale)PosterPlanck has mapped the polarization of the sky emission at microwave frequencies with unprecedented sensitivity. We use the data to characterise the frequency dependence of Galactic polarization. We make use of the cross-correlation analysis which is an established method to characterise the spectral properties of Galactic emission at microwave frequencies. We take the Planck 353 GHz HFI...Go to contribution page
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Dr David HubberPosterWe present GANDALF, a new hybrid SPH and N-body code for combined star formation, planet formation and star cluster studies. GANDALF is written in C++ to perform the main hydrodynamic and gravitational computations. GANDALF also includes a python library to allow interactive simulations and visualisation. Initial conditions can also be generated inside python allowing simple control of...Go to contribution page
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Brice Menard (Johns Hopkins Univ.)contributed talk
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Saman Moradian Jahoudbejari (University of Guilan)contributed talkThe sudden, intense outburst and explosion of gamma ray in the depths of the universe is known as GRB (Gamma Ray Burst).This phenomenon was known for decades as one of mysterious astronomical phenomena. Today it has been known that some of these explosions are relevant with supernovae, and other related to magnetars(which is a type of neutron star with a very strong magnetic field).Discovery...Go to contribution page
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Stefano Bovino (Institut für Astrophysik, Georg-August Universität Göttingen)PosterThe study of the ISM includes a large set of processes and phenomena that needs an accurate modeling and which are often CPU-demanding: chemistry, cooling, heating, dust evolution, photochemistry, and many others. To cope with these we developed a package, named KROME, which is designed to manage the chemistry and the related phenomena with ease. It consists of a Python pre-processor that...Go to contribution page
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Archana Soam (Aryabhatta Research Institute of Observational Sciences (ARIES))PosterIn our study we tried to undersatnd the importance of magnetic field in the very low mass star formation in Bok Globules using optical polarisation techniques. We have studied the starless, prestellar and star forming cores to see the change in magnetic field at different evolutionary stages. We have also also observed cometary globule LBN437 (Gal96-15) extending the previous work done by...Go to contribution page
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Marissa Rosenberg (Leiden Observatory)contributed talk(Ultra) Luminous Infrared Galaxies ((U)LIRGs) are galaxies exhibiting an extremely high infrared luminosity and may be the evolutionary transition phase between starburst galaxies and QSOs. Understanding the heating and cooling mechanisms in these galaxies give us insight to the driving mechanisms that fuel this transition. Molecular emission lines play a crucial role in the cooling of...Go to contribution page
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Martin Ilgner (University Observatory Munich)PosterThe evolution of the ISM and of the IGM is strongly influenced by the fraction of ionizing radiation which escapes young massive clusters and galaxies. Results obtained by recent computational models indicate a wide range of values for the escape fraction. However, since these models were primarily designed to test single aspects they forecast tendencies rather than presenting a coherent...Go to contribution page
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Arindwam Chakrabortycontributed talkThe study of projected magnetic field geometry and dust grain characteristics of the molecular cloud in relation with their other properties like structure and kinematics can give great insight into the role played for the formation and evolution of dark clouds by the magnetic field in shaping the structure and dynamics of these objects. In this paper we present the results obtained from...Go to contribution page
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Bram Ochsendorf (Leiden Observatory)PosterMassive stars drive the evolution of the interstellar medium of galaxies and its observational characteristics through their radiative and mechanical energy input. It has been thought that fast stellar winds from massive stars sweep up the ambient gas to form 'bubbles' of hot gas, surrounded by dense shells of ionized and neutral gas. Infrared surveys of the Milky Way have revealed that bubble...Go to contribution page
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Jan Forbrich (University of Vienna/Smithsonian)contributed talkA few years ago, extinction mapping provided us with a first detailed look at the starless core population of the Pipe Nebula, a molecular cloud at a distance of only 130 pc. Using sensitive mid-infrared Spitzer observations, we showed that its star formation rate is very low, in an interesting contrast to the Rho Oph region next door or Taurus, two clouds in a similar mass range. Here, we ...Go to contribution page
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Stefanie Walch (Max-Planck-Institute for Astrophysics)contributed talkMolecular clouds are cold, dense, and turbulent filamentary structures that condense out of the multi-phase interstellar medium. They are also the sites of star formation. The minority of new-born stars is massive, but these stars are particularly important for the fate of their parental molecular clouds. I will present results from high-performance, three-dimensional simulations that show the...Go to contribution page
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Ged Kitchener (Centre for Astrophysics Research, University of Hertfordshire)contributed talkWe present a 6-cm radio continuum (RC) survey with the JVLA in C-configuration of the LITTLE THINGS sample of 39 local, gas-rich dwarf galaxies, and explore the radio continuum - Far Infrared (RC-FIR) relation in such systems. We generate images with a resolution of 3? and an rms noise of ~5muJy/beam, and detect significant emission in about half of our sample. We double the luminosity range...Go to contribution page
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Yu Gao (Purple Mountain Observatory)contributed talkWe first show that the disk-averaged surface star formation rate (SFR) density has the tightest linear correlation with that of the dense molecular gas (traced by HCN), not the molecular gas (H2) or total gas (HI+H2). This is consistent with the tight FIR-HCN correlation established globally for both dense cores and star-forming galaxies near and far. The Kennicutt-Schmidt law that relates the...Go to contribution page
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