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Holger Müller (Astrophysik/I. Physikalisches Institut; Universität zu Köln)8/21/25, 1:00 PMInvited talk
As of April 2025, about 330 molecules have been detected in the interstellar medium and circumstellar environments of late-type stars (e.g., https://cdms.astro.uni-koeln.de/classic/molecules), many of these detected in recent years. They include complex organic molecules, ions, radicals, (cyano derivatives of) polycyclic aromatic hydrocarbons, and others. In addition, minor isotopic species or...
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Tram Le (Leiden University)8/21/25, 1:40 PMContributed talk
Complex organic molecules (COMs) are synthesized on dust grain surfaces and later released into the gas phase, where they have been widely observed across diverse physical environments—from tranquil clouds to regions of star formation. They thus serve as valuable indicators of the local physical and chemical characteristics of these environments. Accurate models that can account for the...
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Youxin Wang (MPIFR)8/21/25, 2:00 PMContributed talk
Many complex organic molecules (COMs) in star forming regions are believed to form on the surfaces of dust grains or in their ice mantles. Therefore, we expect both the reduced metallicity and dust-to-gas ratio in the outer Galaxy to have an impact on the chemical composition of these regions. To test this, we use NOEMA to perform an imaging spectral line survey of the hot core candidate...
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Laura Ann Busch (Max Planck Institute for Extraterrestrial Physics)8/21/25, 2:20 PMContributed talk
The $^{12}$C/$^{13}$C isotopic ratio serves as a fundamental probe of chemical evolution in the interstellar medium (ISM), with a canonical local value of $\sim$68 that decreases towards the Galactic centre and increases towards larger Galactocentric distances. Yet, recent observations across a broad range of environments in the solar neighbourhood—from prestellar cores to Class II disks and...
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Wonju Kim (University of Cologne)8/21/25, 2:40 PMContributed talk
Understanding the physical and chemical interstellar medium (ISM) is the first step to understanding star formation/evolution and, ultimately, planet formation. The formation of molecular gas occurs in diffuse/translucent clouds. These clouds are also closely associated with the progenitors of molecular clouds and clumps, which are the potential birthplaces of stars. It is in this initial...
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Gary Melnick (CfA)8/21/25, 3:20 PMContributed talk
Karl Menten and I spent our early careers at the Center for Astrophysics. It was (and still is) a large institution, and there was a high chance we might have gone through those years without ever meeting. But Karl, being Karl, made sure that wasn’t the case. He learned of my interest in studying water, despite the challenges of doing so from within the Earth’s atmosphere. Perhaps it was these...
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Yaoting Yan (Max-Planck-Institut für Radioastronomie)8/21/25, 3:40 PMContributed talk
Molecular maser lines are signposts of star formation, probing the excitation and kinematics of very compact regions in the close environment of young stellar objects and providing useful targets for trigonometric parallax measurements. With the Effelsberg 100-m telescope, we discovered widespread non-metastable NH3 maser emission toward 17 high-mass star-forming regions (HMSFRs) in the Milky...
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Paola Caselli (MPE)8/21/25, 4:00 PMContributed talk
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