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Andreas Burkert (LMU)27/04/2015, 13:30
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Svitlana Zhukovska (MPIA)27/04/2015, 15:30
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Mr Alessandro Ballone (USM/MPE, Garching)27/04/2015, 17:00
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Prof. Thomas Giesen (Universität Kassel)28/04/2015, 09:00
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Simon Glover28/04/2015, 11:00
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Prof. Stefanie Walch (Universität zu Köln)28/04/2015, 14:30
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Prof. Robi Banerjee (Universität Hamburg)28/04/2015, 16:30
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Volker Ossenkopf (Universität Köln)29/04/2015, 09:00Session1, WednesdayUnfortunately, it is impossible to resolve the full three-dimensional distribution of densities, velocities and magnetic fields in molecular clouds through astronomical observations as we are bound to celestial positions and a frequency scale. The frequency scale, allows to address the velocity distribution through molecular line observations. The relation between underlying ppp-structures and...Go to contribution page
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Jonathan Mackey (AIfA, Uni Bonn, and I. Physikalisches Institut, Uni. Köln)29/04/2015, 09:15Mass loss from massive stars is very important for determining their evolution and death, but their wind properties can be difficult to measure and are often very uncertain. Main sequence massive stars have fast and highly ionized winds, driving bubbles in their surroundings that have proven surprisingly difficult to detect. We have run simulations showing that wind bubbles are typically...Go to contribution page
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Prof. Stefanie Walch (Universität zu Köln)29/04/2015, 09:30Session1, WednesdayMolecular 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 as their feedback drives turbulence and regulates star formation. I will present results...Go to contribution page
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Svitlana Zhukovska (MPIA)29/04/2015, 09:45Session1, WednesdayInterstellar dust is an ubiquitous component of the ISM playing an active role in shaping its physical and chemical structure from the earliest evolution of galaxies. In order to improve the understanding of dust properties as a function of environment we employ models of dust evolution, including main sources and sinks of dust and constraints from observations. Local dwarf galaxies allow to...Go to contribution page
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Sebastian Haid (Universität zu Köln)29/04/2015, 10:00Session1, WednesdaySupernovae inject a large amount of energy and momentum into the interstellar medium. This is important to set phase structures, regulate star formation or drive outflows. An immediate result of this interaction is turbulence, also in the surroundings of supernovae. The density profile of the ambient medium crucially influences the evolution of the remnant. We provide a semi-analytic...Go to contribution page
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Tobias Röhser (Universität Bonn)29/04/2015, 10:10Session1, WednesdayIntermediate-Velocity Clouds (IVCs) are HI clouds in the lower galactic halo that are thought to be related to a galactic fountain process. Most IVCs are predominantly atomic with a negligible fraction of molecular hydrogen (H_2) while molecular IVCs (MIVCs) are extremely rare. With respect to the galactic fountain hypothesis, IVCs and in particular MIVCs might be an important ingredient for...Go to contribution page
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Annika Franeck (Universität zu Köln)29/04/2015, 10:20C+ fine structure emission has recently been studied with Herschel and Sofia. The results promote C+ as a tracer for star formation in galactic discs or CO-dark molecular gas. Furthermore, the scale height of the C+ emission in the Milky Way and in distant galaxies is not well understood. Does it trace the disc dynamics? Using RADMC-3D, we post-process three-dimensional,...Go to contribution page
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Dr Sandra Brünken (Universität zu Köln)29/04/2015, 11:00Session2, WednesdayContributed talkSandra Brünken and Stephan Schlemmer, I. Physikalisches Institut, Universität zu Köln, Germany The PAH hypothesis associates the unidentified infrared (UIR) emission bands observed in many astronomical environments to the fluorescence of large polycyclic aromatic hydrocarbons (PAHs) that are excited by the interstellar radiation field. Whereas the presence of PAHs in space is now widely...Go to contribution page
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Dr Melanie Schnell (Universität Hamburg)29/04/2015, 11:15Session2, WednesdayContributed talkThe observed variations in molecular abundances in interstellar space originate from both physical and chemical reasons. We will use a combination of chirped-pulse Fourier transform rotational spectroscopy in different frequency ranges with telescope observations to analyse the molecular composition of the universe. By exploring the interstellar molecular complexity and by discovering new...Go to contribution page
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Dr Cornelia Jäger (Friedrich-Schiller-Universität Jena)29/04/2015, 11:30Session2, WednesdayContributed talkThe condensation of carbonaceous and siliceous dust under conditions prevailing in molecular clouds has been experimentally studied. For this purpose, molecular species including refractory elements were deposited on cold substrates. The gaseous precursors of such condensation processes in the ISM are formed by erosion of dust grains in supernova shocks. In the laboratory, we have produced the...Go to contribution page
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Pierre Mohr (Friedrich Schiller University Jena)29/04/2015, 11:45Session2, WednesdayContributed talkP. Mohr, F. Lewen, H. Mutschke In this project, we have synthesized glassy Mg-Fe silicates as interstellar-dust analog materials and have determined their absorption/emission coefficients at low temperatures in the wavelength range from 50 micrometers to 4 millimeters. We have found a strong dependence of the dust opacity on the temperature and a moderate depencence on the chemical...Go to contribution page
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Daniel Lenz (Universität Bonn)29/04/2015, 11:55Session2, WednesdayContributed talkThe correlation between neutral hydrogen and dust has been extensively studied since the IRAS mission. This led to important insights into gas and dust physics, the accretion history of the Milky Way and eventually the distribution of the CO-dark molecular gas. For a full-sky analysis, the spatial resolution of these studies was limited by the angular resolution of the HI data of about one...Go to contribution page
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Roxana Chira (ESO)29/04/2015, 12:05Dust emission surveys at sub-mm and far-infrared wavelengths, e. g. by Herschel, provide new possibilities to study star formation in filamentary molecular clouds. The column density and temperature profiles that are derived with these observations rely on models that describe dust particles in a time-constant environment. Thereby, it is assumed that all the dust is visible for the observer....Go to contribution page
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Prof. Thomas Giesen (Universität Kassel)29/04/2015, 14:30Short carbon chains are fundamental for the chemistry of stellar and interstellar ambiances: They are omnipresent throughout the interstellar medium, they likely participate in the formation of long carbon chains and they are products in photo-fragmentation processes of larger species. Triatomic carbon C3 exhibits a mid-infrared ν3 antisymmetric stretching mode and a ν2 bending vibration at...Go to contribution page
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Dr Matthias Gritschneder (Universitaetssternwarte Muenchen)29/04/2015, 14:45We investigate the fate of B44, a giant trunk in the Ophiuchus region. Employing the AMR-code RAMSES, we are able to show that the wisps and striations visible in the recent Planck Observations can be explained by the hydrodynamical interaction of the trunk with the wind caused by the massive stars in this region.Go to contribution page
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Dr Martin Krause (MPE)29/04/2015, 15:00Session2, WednesdayContributed talkThe Scorpius Centaurus OB association (parallactic distances 118-145 pc) is the closest massive star group to the Sun. Its extent of more than 50 degrees on the sky ensures spatially resolved information from radio up to gamma ray frequencies. We analyse multiwavelength data for the different gaseous component: hot X-ray emitting bubbles, swept-up HI and molecular shells, dusty filaments and...Go to contribution page
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Anna Faye Mc Leod (ESO)29/04/2015, 15:15Session2, WednesdayContributed talkThe results of the first publication from our FuSIOn (Feedback in massive star forming regions: from SImulations to Observations) project, in which we seek to validate the predictions of numerical simulations of star forming clouds that include feedback in the form of stellar winds and photo-ionisation by comparing them with observations, are presented. We observed the iconic Pillars of...Go to contribution page
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Mrs Anna Schauer (Universität Heidelberg)29/04/2015, 15:25Session2, WednesdayContributed talkPopulation III (or Pop III) stars can influence their surroundings in several ways and by so doing regulate subsequent star formation. Their radiation may ionize or photodissociate H2 in the surrounding interstellar medium and break out to affect other halos. Even if ionizing photons are trapped, Lyman-Werner (LW) photons may still escape the halo and photodissociate H2 in nearby halos,...Go to contribution page
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Katharina Wollenberg (Universität Heidelberg)29/04/2015, 15:35Session2, WednesdayContributed talkJ031300 is now the most metal-poor star discovered to date, with a maximum Fe abundance of 10^(-7.1) solar. Two possible Pop III supernova candidates have been identified, with progenitor masses of 12.4 and 60 Msun, whose nucleosynthetic yields that are a good match to the chemical abundances found in J031300. However, explaining the actual metallicity of J031300 also requires an...Go to contribution page
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29/04/2015, 16:15
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Philipp Schneider (USM/LMU)29/04/2015, 17:05
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Mr Alessandro Ballone (USM/MPE, Garching)29/04/2015, 17:15Session2, WednesdayContributed talkThe evolution of the dust cloud G2, discovered by Gillessen et al. (2012), has been continuously monitored from 2004 to now. The most recent position-velocity diagrams, obtained from the integral field spectrograph SINFONI at VLT, clearly show that G2 has experienced the pericenter passage. Thus, G2 is now subject to the maximum tidal field of the supermassive black hole and hydrodynamical...Go to contribution page
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Sara Rezaei Khosbakht (MPIA Heidelberg)29/04/2015, 17:25Session2, WednesdayContributed talkSara Rezaei Kh., C. A. L. Bailer-Jones, R. J. Hanson Max-Planck-Institut fϋr Astronomie, Kӧnigstuhl 17, 69117 Heidelberg, Germany We present a non-parametric model to mode probabilistically the three-dimensional distribution of dust in the Milky Way. Knowledge of dust distribution in the Galaxy is required when estimating intrinsic stellar properties which are in turn necessary to estimate...Go to contribution page
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Daniel Kröll (Universität Bonn)29/04/2015, 17:35Session2, WednesdayContributed talkSuperbubbles and bubbles in the interstellar medium are formed by winds of massive stars and their supernova explosions. Knowing the properties of these bubbles is key to determine the energy input by stellar groups and its history. We study the hydrogen structures in the vicinity of the closest OB Association, the Scorpius-Centaurus association at 140 pc distance. We investigate if our model...Go to contribution page
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Benjamin Gaczkowski (USM/LMU)30/04/2015, 09:00Session2, WednesdayContributed talkToday molecular cloud formation is attributed to collisions of large-scale flows in the ISM. Such flows can be driven by stellar feedback processes and supernovae. The numerous massive stars in the three sub-groups of the Sco-Cen OB-association created a huge system of expanding loop-like H I structures around each of the sub-groups. The Lupus I molecular cloud is situated in the middle...Go to contribution page
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Dr Guang-Xing Li (USM)30/04/2015, 09:15Session2, WednesdayContributed talkIn this talk I will present the G-virial method, which allows to quantify (1) the importance of gravity in molecular clouds in the position-position-velocity (PPV) space, and (2) properties of the gas condensations in molecular clouds. After introducing the method, I will discuss how to study the importance of gravity in star formation, and how we can link different models and simulations with...Go to contribution page
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Dr Alberto Sanna (MPIfR Bonn)30/04/2015, 09:30Session2, WednesdayContributed talkAt an early stage of stellar evolution, massive young stellar objects (YSOs) inject large amounts of mechanical energy into the ISM by powerful outflow phenomena, which are a main outcome of mass accretion onto the protostar. In turn, this outflow activity provides a major source of turbulent energy for the cluster gas. In this context, it is fundamental to properly characterize the dynamical...Go to contribution page
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Simon Glover (Universität Heidelberg)30/04/2015, 09:45Session2, WednesdayContributed talkNumerical simulations of star formation and stellar feedback have now advanced to the point where they routinely include relatively sophisticated treatments of the microphysics of the ISM. However, much of the predictive power of these simulations can only be harnessed if we can convert their results into synthetic observables that can be compared with observations of the real ISM. In this...Go to contribution page
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Ms María Jesús Jiménez (Institut für Theoretische Astrophysik, Zentrum für Astronomie der Universität Heidelberg, Germany)30/04/2015, 10:00Session2, WednesdayContributed talkThe efficiency of star formation in other galaxies is often studied only focusing on molecular gas traced by CO emission due to the faintness of other lines. However the emission coming from lines such as HCN or HCO+ is an essential tool to probe the actual dense gas. Therefore one of the key ways to probe the physics conditions in the star forming gas and as importantly, study if and how...Go to contribution page
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Volker Weiss (TLS Tautenburg)30/04/2015, 10:10Proto-stellar outflows are a signpost of stellar birth. Despite many investigations of such flows, their impact on the parental molecular cloud is still highly disputed. Simulations suggest that proto-stellar outflows are too weak to replenish turbulent energy globally, and thus have little influence on stabilizing the cloud. On the other hand, observations show that outflows can generate...Go to contribution page
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Nicolas Guillard (ESO)30/04/2015, 10:20Session2, WednesdayContributed talkObservations of dwarfs galaxies suggest that Black Holes (BHs) and Nuclear Clusters (NCs) are co-evolving with their hosts. However, their formation and how they are fueled is still unclear. NCs, unlike BHs, may provide a visible record of the accretion of stars and gas. Therefore, they can be used as probes for the gas and star fueling of the nuclei of dwarfs galaxies. Whether NCs form via...Go to contribution page
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Neven Tomicic (MPIA)30/04/2015, 10:25Galaxy clusters are large virialized collections of galaxies. Galaxies contribute about 5% to the mass of the cluster, the intracluster medium about 10% and the dark matter up to 85%. These structures are formed from galaxy protoclusters. A protocluster is an early type of clusters with fewer galaxies and an observed higher number densities of galaxies, compared to other parts of the observed...Go to contribution page
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Neven Tomicic (MPIA)30/04/2015, 10:25Session2, WednesdayContributed talkThe cold interstellar medium (ISM) provides the raw materials out of which stars form. However, many open questions remain regarding how cooling, phase transitions, star formation, and feedback interplay, what the effects of both local and global environment on these processes are, and how they connect to large scale galaxy evolution. Many of these processes, which occur on <<100 pc spatial...Go to contribution page
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Timea Csengeri (MPIfR Bonn)30/04/2015, 11:00Session2, WednesdayContributed talkThe ATLASGAL survey is one of the most sensitive and extensive ground-based survey of the inner Galaxy at sub-millimeter wavelengths, and provides an unprecedented view on all stages of massive star formation. Over 10 000 compact sources have been identified (Csengeri et al. 2014), and we have made substantial progress in characterising various evolutionary stages of the evolution of massive...Go to contribution page
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Katharina Fierlinger (LMU)30/04/2015, 11:15Giant molecular clouds (GMCs) are reshuffled by stellar winds and supernova explosions of massive stars. These processes -- which we call stellar feedback -- create bubbles in the interstellar medium and insert newly produced heavy elements and kinetic energy into their surroundings, possibly driving turbulence in GMCs. Most of this energy is thermalized and immediately removed from the GMC by...Go to contribution page
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Mr Andrea Gatto (Max Planck Institute for Astrophysics)30/04/2015, 11:30Session2, WednesdayContributed talkSupernova (SN) explosions are an important component for shaping the interstellar medium (ISM). They produce its hottest phase while driving turbulent motions in the warm and cold gas. Globally, these random motions could provide a net turbulent support and help to regulate star formation. The impact of SNe on the ISM is, however, strongly dependent on the thermodynamic properties of the...Go to contribution page
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Anabele-Linda Pardi (Max-Plank-Institut fur Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching, Germany)30/04/2015, 11:40Session2, WednesdayContributed talkWe carry out three-dimensional MHD simulations of the magnetised multiphase interstellar medium (ISM) focusing on the connection between chemical and magnetic evolution. The simulations of periodic boxes include a complex chemical network tracking molecule formation and destruction. We also include supernova (SN) feedback. Magnetic field saturation occurs when the field dissipation and...Go to contribution page
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Anabele-Linda Pardi (Max-Plank-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching, Germany)30/04/2015, 11:40Session2, WednesdayContributed talkCo-authors: Philipp Girichidis1, Thorsten Naab1, Stefanie Walch2, Andrea Gatto1, Richard Wünsch3, Simon C.O. Glover4, Ralf S. Klessen4,5,6, Paul C. Clark7, Christian Baczynski4, Thomas Peters1,8 1Max-Plank-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching, Germany 2Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany 3Astronomical...Go to contribution page
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Maximilian Eisenreich (MPA)30/04/2015, 11:50Session2, WednesdayContributed talkWe use hydrodynamical simulations to study the influence of AGN accretion and feedback on the late morphological and kinematic evolution of the hot and cold interstellar medium and young stars in isolated early-type galaxies (ETGs). The complex interplay of gas cooling from a hot halo, feedback from star formation (metal and energy return from supernova Ia and II, AGB winds) and gas accretion...Go to contribution page
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Aaron Bryant30/04/2015, 12:00
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Caroline Reinert, Harald Mutschke (Friedrich Schiller University Jena)30/04/2015, 14:30Surprisingly little data are available on the absorption/emission index of water ice for submillimeter wavelengths. We present new spectroscopic measurements for crystalline water ice cooled to low temperatures and derive a simple T-dependent model for the opacity based on power lawsGo to contribution page
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Dr Sunil Kumar Sudhakaran (Max-Planck-Institut für Kernphysik)30/04/2015, 14:45Session2, WednesdayContributed talkOne of the long-standing mysteries in astronomy is the origin of the interstellar absorption features that are observed in the visible to near infrared range and dubbed as the diffuse interstellar bands (DIBs). Despite the observation of several hundred lines, none of them has been unambiguously attributed to a chemical species. A potential candidate believed to be responsible for some of...Go to contribution page
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Ke Wang (ESO)30/04/2015, 15:00Co-authors: Leonardo Testi(1), Adam Ginsburg(1), Malcolm Walmsley(2,3),Sergio Molinari(4), Eugenio Schisano(4) 1. ESO - European Southern Observatory, Garching bei München, Germany 2. INAF - Osservatorio astrofisico di Arcetri, Firenze, Italy 3. Dublin Institute of Advanced Studie, Dublin, Ireland 4. Istituto di Astrofisica e Planetologia Spaziali (IAPS) INAF, Roma, Italy The ubiquity...Go to contribution page
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Udo Ziegler (AIP)Session2, WednesdayContributed talkThe interaction of supernova remnants with interstellar clouds can produce dense gas aggregations which eventually get compressed enough to form prestellar cores. Numerical simulations of shocked clouds by isolated supernova remnants help to filter necessary conditions for core triggering and to enlighten the role of individual physical processes involved like magnetohydrodynamics, radiative...Go to contribution page
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Dr Judith Ngomou (USM/LMU)
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Dr Nicola Schneider (LAB Bordeaux)Session2, WednesdayContributed talkSince long, there are claims that stars form only above certain thresholds of (column) density, and that the rate of star formation (SFR) in a galaxy can be linked to physical properties of the interstellar gas from which stars are forming. With the Herschel photometric maps (70-500 micron) of Galactic clouds, it is now possible to determine rather precisely their column density structure,...Go to contribution page
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Andreas Burkert (LMU)
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