Main Colloquium
Dr. Harish Vedantham	ORATED

Netherlands Institute for Radio Astronomy, Dwingeloo

Low frequency (< few hundred MHz) radio observations uniquely trace several processes that determine the habitability of exoplanets. Coronal plasma ejections that erode planetary atmospheres can be detected using the characteristic radio bursts they emit. Planetary magnetic fields that largely determine the planetary defence against the stellar onslaught can also be detected using radio observations. Radio observations of such phenomena in the solar system are commonplace. I will argue that the extrasolar frontier is now also within reach thanks to powerful new low-frequency telescopes such as LOFAR and uGMRT. I will describe an observational program using LOFAR to systematically survey the low-frequency radio sky for stellar, brown dwarf and exoplanetary emission with unprecedented sensitivities reaching a fraction of a milliJansky at 150 MHz and below. I will present some early successes of this campaign including (a) the discovery of evidence for magnetic interaction between a star and its planet and (b) the discovery of a cold brown dwarf directly in the radio band using its magnetospheric emissions. I will end with an outlook for harnessing radio astronomy’s unique diagnostic capabilities to advance exoplanet science.

	Special Colloquium
Prof. Hua-bai Li	ORATED

The Chinese University of Hong Kong

The Zeeman effect and dust grain alignment are two major methods for probing magnetic fields (B-fields) in molecular clouds, mainly motivated by the study of star formation, as the B-field may regulate gravitational contraction and channel turbulence velocity. I will review our recent observations of B-fields and how we interpret them with numerical simulations. We found that turbulence is sub-Alfvénic in bulk cloud volumes but can turn slightly super-Alfvénic in cloud cores due to the density enhancement. The consequences of the largely ordered cloud B-fields on fragmentation, turbulence, and star formation are observed. If time allows, I will also introduce the first direct detection of ambipolar diffusion between neutral/ion turbulent eddies.

	SFB Colloquium
Dr. Holger Kreckel	ORATED

Max-Planck-Institut für Kernphysik, Heidelberg

The Cryogenic Storage Ring (CSR) at the Max Planck Institute for Nuclear Physics in Heidelberg is the largest electrostatic storage ring project in the world. The CSR combines electrostatic ion optics with extreme vacuum and cryogenic temperatures. The storage ring has a circumference of 35 m, and all deflectors are housed in experimental vacuum chambers that can be cooled down to 5 K. It has been shown that within a few minutes of storage inside the CSR infrared-active molecular ions (e.g., CH+, HeH+ and OH-) cool to their lowest rotational quantum states by spontaneous emission of radiation. Equipped with an ion-neutral collision setup and a low-energy electron cooler, the CSR offers unique possibilities for astrochemical experiments under true interstellar conditions. I will present an overview of the capabilities of the CSR, along with first experimental results on collision experiments between cold molecular ions and neutral atoms, free electrons, and photons, yielding quantum state-selective rate coefficients for astrophysically important processes.

	Main Colloquium
Dr. Geronimo Villanueva	ORATED

NASA Goddard Space Flight Center, Greenbelt, USA

We recently established that Mars lost an ocean’s worth of water, while the Curiosity rover has recently detected organics on the Martian surface and in the atmosphere. Venus may have been covered by water, while organic rich oceans have been suggested to exist under the surface of Europa, Enceladus and on Titan. If these planets/moons had a rich chemical and diverse past, how much of these biomarkers were lost to space, and how much are currently available for life? Are sub-surface habitable niches connecting now with the atmosphere?  The answers to these fundamental questions of planetary evolution and habitability lie in robotic investigations of the planet’s surface and atmosphere. In the last decade, we have obtained the most comprehensive search for organic material in the Martian atmosphere and we are now sending powerful probes to Venus and beyond, permitting us to probe these planets/moons with unprecedented sensitivity. In particular, we are preparing for the human exploration of Mars, and these recent insights about Mars’ past habitability are greatly assisting us in identifying the most promising research sites. In this talk, I will present our latest discoveries with ExoMars/TGO about Mars, our exploration plans with JWST of Europa and Enceladus, and our latest findings with SOFIA and ground-based observatories of Venus, Europa and Mars.

	Main Colloquium
Dr. Mark Walker	CANCELED

Manly Astrophysics, Australia

TBD

	Main Colloquium
Dr. Nabila Aghanim	ORATED

Institut d'astrophysique spatiale, Université Paris-Saclay, France

The cosmic web is made of nodes, filaments, sheets and voids that are well traced by the distribution of galaxies. Numerical simulations suggest that about 40% of the total baryons in the cosmic web are in the form of warm/hot baryons hidden in the filamentary structure between clusters of galaxies. I will present how the combined use of surveys in the optical, in the millimeter (via the Sunyaev-Zel'dovich signal measured by Planck) and in the X-rays allows us to study the largest structures of the Universe. Combining these observables, we detect the cosmic web elements, measure their gas content and tackle the problem of characterising and quantifying the hot hidden baryons in the filamentary structure of the cosmic web.

	Main Colloquium
Dr. Adam Ingram	ORATED

Newcastle University, Newcastle upon Tyne, UK

Stellar-mass black holes accreting gas from a binary partner (X-ray binaries) and supermassive black holes accreting gas from their host galaxy (active galactic nuclei, AGN) can emit a huge X-ray flux from the vicinity of the black hole event horizon. This can be exploited to probe the strong field regime of General Relativity and measure the properties of the black hole: its mass and angular momentum. For all but two objects in the Universe, the vicinity of the accreting BH is far too small to directly image, necessitating the use of mapping techniques that exploit rapid X-ray variability. I will talk about X-ray reverberation mapping, which utilises the relativistically broadened iron emission line that results from centrally emitted X-rays reflecting from the disk. Modelling the light-crossing delay between reflected and directly observed X-rays returns a black hole mass measurement. I will summarise our efforts to measure the mass of stellar and supermassive black holes with our X-ray reverberation mapping code RELTRANS, including our first proof-of-principle constraint on Cygnus X-1. I will then describe how we can use RELTRANS for an even more ambitious goal: measuring the Hubble constant, H0. This is possible because the shape of the reflection spectrum depends on the intensity of illuminating flux, meaning that modelling with RELTRANS can effectively turn bright nearby AGN into standard candles. New, independent methods to measure H0 are currently highly desirable because modelling of the cosmic microwave background returns an H0 value in >4 sigma tension with the value derived from the traditional distance ladder. I will show that the statistical precision required to prefer one of these two discrepant values is achievable with a sample of ~25 AGN. I will discuss the improvements to our model that are required to achieve such a measurement in reality.

	Special Colloquium
Dr. Michael Janssen	ORATED

Max-Planck-Institut für Radioastronomie

Centaurus A is the closest radio galaxy to Earth and has been studied extensively as a laboratory for AGN feedback and potential UHECR source after its discovery as one of the first extragalactic radio sources in 1949. I will present the results from our EHT observations of this southern source. Compared to previous VLBI studies, we have imaged the AGN jet of Cen A at a 16x sharper resolution and 10x higher observing frequency. This allows us to probe the launching region of an extragalactic radio jet on sub-lightday scales. We can directly compare our image to VLBI observations of M87 at a lower frequency, as both probe the same size scales in terms of gravitational radii. Based on the similarity of these jets, we show that our observations provide further support for the fundamental plane of black hole activity in an intermediate mass regime. From the location of the resolved radio core in Cen A, we predict the source's black hole shadow to be visible at THz frequencies, which marks Cen A for future high-frequency space VLBI missions. I will conclude with an outlook of our next observational and modeling steps.

	Special Colloquium
Theodore Macioce	ORATED

Caltech, Pasadena, USA

Part 1: Measuring the kinetic Sunyaev-Zel’dovich (kSZ) effect is a promising technique to constrain both cosmic growth and galaxy cluster formation. Detecting the kSZ effect in massive galaxy clusters will become increasingly feasible as millimeter-wave telescopes gain sensitivity and resolving power over multiple frequency bands. While such kSZ measurements will have unprecedented sensitivity, they will also be contaminated by emission from dusty star-forming galaxies, primary anisotropies of the cosmic microwave background (CMB), and the typically dominant thermal SZ signal, making analysis efforts difficult. Current kSZ forecasts account for these contaminants in a simplified way, relying on assumptions that may not apply in the high-resolution regime. Moreover, they typically use Fisher matrix analyses, which cannot give a fully accurate description of the degeneracies among the physical parameters describing the cluster. We present a new mock observation and analysis pipeline for kSZ images that uses more detailed noise models and more sophisticated analysis methods to extract peculiar velocities, temperatures, and optical depths more accurately. With these mock observations, we will inform the designs of next-generation millimeter telescopes targeting kSZ observations by identifying the optimal instrumentation choices for both cosmological and cluster-scale constraints. The software pipeline we develop will also be directly usable as an analysis tool once observations from such telescopes become available. Part 2: Silicon optics can greatly benefit future millimeter and submillimeter astronomical instruments thanks to silicon's useful properties such as low loss, high refractive index, and high strength. However, silicon's high index (n = 3.4) necessitates antireflection (AR) treatment, which has proven a major challenge, especially for the multilayer treatments required for wide spectral bandwidths. In this talk, we present our approach to this challenge, in which we develop a wide-bandwidth integral AR structure for silicon optics that uses a novel fabrication technique that combines deep reactive ion etching (DRIE) and wafer bonding. We have previously demonstrated a two-layer AR structure for windows over a 1.6:1 bandwidth and are currently fabricating a four-layer coating for a 4:1 bandwidth. Here, we focus on a design for a six-layer structure optimized to give -20 dB reflection between 80 and 420 GHz (5.25:1 bandwidth), which will be useful for future multicolor SZ observations.

	Main Colloquium
Prof. Talvikki Hovatta	ORATED

Finnish Centre for Astronomy with ESO, University of Turku, Finland

Blazars are active galactic nuclei where relativistic plasma jets are launched from the vicinity of the supermassive black hole at the center of the galaxy. These jets are efficient particle accelerators and can transport energy from the nucleus of the galaxy to the integalactic medium far outside the galaxy itself. Magnetic fields are thought to play a crucial role in both launching and collimation of blazar jets, keeping them collimated all the way to kiloparsec scales. In my talk, I will discuss how polarization observations in the radio, millimeter, and optical bands can be used to constrain the magnetic field structure in parsec- and kiloparsec-scale jets of blazars. I will use the archetypal blazar 3C273 as an example, and present new results from ALMA millimeter wavelength observations of the central region and the termination hotspot.

	Main Colloquium
Prof. Annalisa Bonafede	ORATED

Dipartimento di Fisica e Astronomia, Università di Bologna, Italy

Galaxy clusters are a gold mine to understand particle acceleration mechanisms in plasmas. The intra-cluster medium is indeed composed of a hot and tenuous gas co-existing with a large-scale magnetic field, that can originate synchrotron radio emission in presence of relativistic cosmic-ray electrons. Synchrotron radio emission is observed from galaxy clusters in several forms. Theoretical models link the diffuse radio emission to turbulent and shock acceleration during cluster mergers, but the mechanisms are still poorly understood. The advent of low frequency radio instruments such as LOFAR, MeerKAT, and ASKAP, has allowed us to make important steps forwards in this field. At the same time, new unexpected sources of emission have been discovered, posing new questions about particle acceleration and magnetic field amplification in these environments. In this talk, I will present the new picture that is emerging in these years, focussing both on what we have understood and on the questions that new discoveries are posing.

	Main Colloquium
Prof. Alexander Tchekhovskoy	ORATED

Northwestern University, Evanston, Illinois, USA

In this talk, I will review the physics of accretion and outflows, focusing on the relativistic jets, as revealed by 3D general relativistic simulations of magnetized plasma near spinning black holes. I will discuss the conditions necessary for jet formation, what the jets can reveal about the central engine, the effects the jets can have on their environment.

	Special Colloquium
Prof. Abigail Vieregg	ORATED

University of Chicago

The detection of high energy astrophysical neutrinos is an important step toward understanding the most energetic cosmic accelerators. IceCube, a large optical detector at the South Pole, has observed the first astrophysical neutrinos and identified at least one potential source. However, the best sensitivity at the highest energies comes from detectors that look for coherent radio Cherenkov emission from neutrino interactions. I will give an overview of the state of current experimental efforts, including recent results, and then discuss a suite of new experiments designed to discover neutrinos at the highest energies and push the energy threshold for radio detection down to overlap with the energy range probed by IceCube, thus covering the full astrophysical energy range out to the highest energies, and opening up new phase space for discovery. These include ground-based experiments such as RNO-G and IceCube-Gen2, as well as the balloon-borne experiment PUEO.

	Main Colloquium
Dr. Mélanie Chevance	ORATED

Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg

The cycling of matter in galaxies between molecular clouds, stars and feedback is a major driver of galaxy evolution. However, it remains a major challenge to derive a theory of how galaxies turn their gas into stars and how stellar feedback affects the subsequent star formation on the cloud scale, as a function of the galactic environment. Star formation in galaxies is expected to be highly dependent on the galactic structure and dynamics, because it results from a competition between mechanisms such as gravitational collapse, shear, spiral arm passages, cloud-cloud collisions, and feedback processes such as supernovae, stellar winds, photoionization and radiation pressure. A statistically representative sample of galaxies is therefore needed to probe the wide range of conditions under which stars form. I will present the first systematic characterisation of the evolutionary timeline of the giant molecular cloud (GMC) lifecycle, star-formation and feedback in the PHANGS sample of star-forming disc galaxies. I will show that GMC are short-lived (10-30 Myr) and are dispersed after about one dynamical timescale by stellar feedback, between 1 and 5 Myr after massive stars emerge. Although the coupling efficiency of early feedback mechanisms such as photoionisation and stellar winds is limited to a few tens of percent, it is sufficient to disperse the parent molecular cloud prior to supernova explosions. This limits the integrated star formation efficiencies of GMCs to 2 to 10 per cent. These findings reveal that star formation in galaxies is fast and inefficient, and is governed by cloud-scale, environmentally-dependent, dynamical processes. These measurements constitute a fundamental test for numerical sub-grid recipes of star-formation and feedback in simulations of galaxy formation and evolution.

	Main Colloquium
Dr. Aina Palau	ORATED

Instituto de Radioastronomía y Astrofísica, UNAM, Morelia, Mexico

How stellar clusters form and what determines their number of objects and stellar densities are long-standing questions, intimately related to the fragmentation properties of molecular clouds. It is thought that a number of properties of molecular clouds could influence and determine how clouds fragment. Some of these properties are the density and temperature structure, related to thermal support and gravity, turbulence, stellar feedback, initial angular momentum, and magnetic fields. In this talk I will present an observational campaign aimed at disentangling which of these properties finally control the fragmentation process in the dense parts of molecular clouds, from 0.2 to 0.005 pc scales. Special emphasis will be put on our latest result, a study of the relation between fragmentation and the magnetic field, where we observationally tested, for the first time in a statistically significant sample, the theoretical prediction that a strong magnetic field should suppress fragmentation.

	Special Colloquium
Dr. Bernhard Schulz	ORATED

Deutsches SOFIA Institut and NASA Ames Research Center

The Stratospheric Observatory for Infrared Astronomy (SOFIA) continues to operate in its 9th Cycle with ever increasing efficiency. SOFIA is the only general user observatory for the next 15 years that reaches the for ground-based observatories largely inaccessible infrared/submm wavelength range. As such it maintains a regular delivery of unique astronomical results from this important spectral window. The talk will provide a short description of this US/German collaboration and its capabilities, a selection of scientific highlights, and insights into the status of the project. It will discuss the implementation of important transformative changes over the past two years and planned future developments. In particular included are NASA's long-term instrumentation roadmap and the currently ongoing complementary effort on the German/European side to exploit a key capability of this observatory, keeping its instrumentation at the cutting edge of technology and further optimizing its scientific output.

	Main Colloquium
Prof. Henk Hoekstra	ORATED

Leiden Observatory, the Netherlands

In past century we have learned much about the origin and evolution of the Universe. We now know the Universe is 13.8 billion years old, but its main ingredients remain a mystery: atoms make up only 5%. The rest consists of dark matter and dark energy, components for which we lack a fundamental physical theory. Better observations are needed to guide theory and ESA’s Euclid satellite is designed to do just that. Euclid is scheduled for launch in 2022 and will map the distribution of dark matter in the Universe as a function of cosmic time. However many challenges remain if we want to extract accurate cosmological information from these complex data.

	Main Colloquium
Prof. Alvaro Hacar	ORATED

Institute for Astrophysics, University of Vienna

High-mass stars determine the physical and chemical evolution of the Universe. High-mass stars are typically found in dense stellar clusters and are associated to densest and more dynamic gas structures in our Galaxy. However, the precise formation mechanisms of these massive objects in clusters remain under debate, particularly in comparison to the better understood origin of low-mass objects formed in isolation. The new EMERGE ERC-StG project (http://emerge.alvarohacar.com) proposes a novel approach for the study of the initial conditions for the formation of high-mass stars with ALMA. During my talk I will present the first technical and scientific results of this project exploring where and how the origin of stars of different masses and the different modes of star formation are closely connected to the structure and properties of the gas prior to their formation.

	Main Colloquium
Prof. Andrea Mignone	ORATED

Università di Torino, Italy

Recent advancements for the state-of-the-art modelling of astrophysical plasma via numerical simulations are presented. The talk focuses mainly on the development of particle-gas hybrid schemes, suitable for the numerical modeling of different astrophysical environments, such as proto-planetary disks with dust, ion kinetic processes such as diffusive shock acceleration, large-scale transport of cosmic rays (CR) electrons and related non-thermal emission signatures. The MHD-PIC hybrid equation model, for the interaction between a collisionless thermal plasma and a population of non-thermal cosmic-ray (CR) particles, is examined in detail and applications to diffusive shock acceleration are presented.

	Promotionskolloquium
Yuxin Lin	ORATED

Max-Planck-Institut für Radioastronomie

Galactic-scale surveys from millimeter to infrared wavelengths in the last decades have identified numerous massive molecular clumps (~1 pc in size, >500 M_solar in mass), which are believed to be nurseries of OB star clusters. In this thesis, we report intermediate spatial resolution (~0.1 pc) observations towards selected samples of massive clumps and reveal their physical structures, including fragmentation properties, density, temperature, dynamical state and their evolution during massive proto-cluster formation. In the first project, we analyse 350 micron dust images using APEX-SABOCA of >200 massive clumps. Combined with space-based submm/FIR archival data, we obtain 10'' dust temperature and hydrogen column density maps, providing accurate estimates of physical properties. We resolved large populations of quiescent and star-forming cores and show that a large clump mass reservoir is essential for the mass accumulation onto massive cores. In the second project, using wide-band SMA and APEX spectroscopic observations at 1 mm, we present evolutionary variations of the radial profiles of temperature, density and dynamical state of the massive clumps, corroborated by abundance ratios of molecules as evolutionary indicators. We find that most of the clump temperature profiles on spatial scales of 0.1-1 pc are strongly shaped by centrally emerging protostars. The gas densities and the gradient of gas densities increase with the clump's luminosity-to-mass ratio, and is compatible with the variations of radial profiles of the virial parameter, suggesting a gravo-turbulent picture of clump gas dynamics. The hierarchical gas structure of massive clumps are unveiled by quantifying both the radial density profiles of the bulk gas (~10^4 cm^-3) and the dense gas (>~10^6-10^8 cm^-3) structures, which indicate spatially and temporally varying dense gas conversions and star formation efficiencies. Finally, this line of work is extended to five early-stage massive clumps in W43-main, an extreme Galactic OB cluster forming massive cloud. With wide-band NOEMA and IRAM 30m observations at 3 mm, we investigate in particular the impact of cloud-cloud collisions on the enhancement of dense gas, and on the formation and fragmentation of early-stage cores. [Referees: Prof. Dr. Karl Menten, Prof. Dr. Pavel Kroupa, Prof. Dr. Ian Brock, Prof. Dr. Hubert Schorle]

	Special Colloquium
TBD TBD	CANCELED

TBD

TBD

	Promotionskolloquium
Prajwal Voraganti Padmanabh	ORATED

Max-Planck-Institut für Radioastronomie

Pulsars are rapidly rotating, strongly magnetised neutron stars with spin periods ranging from few milliseconds to tens of seconds. They emit beams of electromagnetic radiation that are predominantly detected as periodic pulsations at the radio end of the spectrum. Since the first pulsar detection in 1967, there have been close to 3000 such systems discovered and they have proven to be excellent tools for a variety of scientific applications. Despite the large number of discoveries, there exist several open questions pertaining to fundamental physics as well as pulsar evolution that can be addressed by pushing the boundary of pulsars beyond the current population census. The first part of my talk will focus on radio pulsar searches conducted with the MeerKAT radio telescope. I describe a processing infrastructure built with open source tools for conducting wide field-of-view searches with hundreds of synthesised beams. I use this setup for targeted binary pulsar searches on globular cluster Terzan 5. I also introduce the MPIfR Galactic plane survey (MGPS), a commensal survey covering science cases for pulsars, fast transients, Galactic magnetic fields, continuum emission, and spectral lines. My focus will be on pulsar searches conducted on a pilot survey as part of MGPS. The second part of my talk will focus on two projects. First, I will talk about a collaboration with the technology firm SAP to use their Data Intelligence framework for comparing machine learning models for pulsar candidate classification on a large scale using 3.2 million candidates generated from the HTRU South low-latitude survey. Second, I will present an investigation of the pulse profile instability of PSR J1022+1001, a pulsar belonging to two pulsar timing arrays and thus of interest for nanohertz gravitational wave searches. In this analysis, data spanning 20 years including two different recording instruments from the Effelsberg telescope and a recording instrument from the Parkes telescopes were used. By accounting for instrumental effects like polarisation miscalibration and propagation effects like interstellar scintillation, up to 25 per cent of the instability could be explained. This indicates that the observed instability is most likely intrinsic to the pulsar. [Referees: Prof. Dr. Michael Kramer, Prof. Dr. Frank Bertoldi, Prof. Dr. Simon Stellmer, Prof. Dr. Robert Glaum]

	Main Colloquium
Prof. C. Megan Urry	ORATED

Yale Center for Astronomy and Astrophysics, New Haven, USA

Every massive galaxy has a supermassive black hole at its center, which has grown episodically during phases of rapid accretion. Surveys of Active Galactic Nuclei (AGN) probe this growth history and thus are important both for understanding the properties of supermassive black holes and for quantifying their impact on galaxy evolution. We show that multi-wavelength data are particularly important for mitigating strong selection biases, since most AGN are heavily obscured and thus look like inactive galaxies in optical surveys. Furthermore, a “wedding cake” combination of survey depths and areas is needed to sample the full range in luminosity and redshift. With the AHA survey at X-ray+infrared+optical wavelengths, we measured supermassive black hole growth over the last ~12 billion years, and thus the amount of energy deposited in AGN host galaxies throughout that time. Contrary to leading theoretical models, a close look at AGN host galaxies suggests that for only a minority does merger-triggered AGN “feedback” cause rapid quenching of star formation.

	Main Colloquium
Dr. Paul Hartogh	ORATED

Max-Planck-Institut für Sonnensystemforschung, Göttingen

JUICE – JUpiter ICy moons Explorer – is the first large class mission of ESA’s Cosmic Vision 2015 - 2025 programme. The JUICE satellite is planned to be launched in September 2022 and its Jupiter orbit insertion is foreseen in 2031. The primary mission in the Jupiter system will take about three years. The focus of the mission is Jupiter itself and the Galilean satellites, their internal oceans and potential habitability. Recent ground-based observations of Europa and Ganymede showed water vapour plumes, probably related to geysers on their surfaces. JUICE intends to identify the geysers, monitor their potential activity and molecular and isotopic composition in order to constrain satellite formation models and development processes (of chemical, physical and potentially biologic nature) in the interior of their oceans. Jupiter itself is seen as an archetype of a gas giant. A better understanding of its atmospheric processes will be a baseline for a better understanding of gas giants outside our solar system. JUICE will characterize the general circulation of Jupiter’s atmosphere, its meteorology, chemistry and structure between the upper cloud deck and the ionosphere and magnetosphere. The Submillimetre Wave Instrument (SWI) is one of 10 scientific instruments on the JUICE satellite. SWI covers two spectral bands between 530 and 1275 GHz. Details will be presented about the functionality and specifications of the instrument, required technology developments during the last decades and how the unique capabilities of SWI will help to answer key JUICE science questions.

	Promotionskolloquium
Richa Sharma	ORATED

Max-Planck-Institut für Radioastronomie

X-ray binaries are stellar systems consisting of a compact object (either a neutron star or a black hole) accreting matter from a companion star. Some of the X-ray binaries form relativistic jets where plasma accelerates close to the speed of light. The relativistic jets have been extensively studied, and the most advanced research in this field investigates changes in the jets’ core position and short-term flaring events. The thesis approaches the former topic with a semi-analytical code and the latter topic with new observations. First, we explored and established the relationship between the core position and jet spectrum using a code of a synchrotron emitting, self-absorbed jet by varying the jet inclination angle and relativistic electron density. Then, we investigated short-term variability in the flux of the X-ray binary system LSI +61°303. We used radio and X-ray data of the source obtained with WSRT and Suzaku telescopes, respectively. Timing analysis revealed periodic oscillations of ∼ 1 h (radio) and ∼ 2.5 h (X-ray), albeit at different epochs. To explore the simultaneous radio and X-ray emission from the source, we observed it with AMI-LA and XMM–Newton telescopes. Correlation analysis established for the first time that emission at both wavelengths is highly correlated and has implications on the nature of the physical processes in the system. [Referees: Priv.-Doz. Dr. Maria Massi, Prof. Dr. Norbert Langer, Prof. Dr. Ian Brock, Prof. Dr. Zeinab Abdullah]

	Promotionskolloquium
Nina Brinkmann	ORATED

Max-Planck-Institut für Radioastronomie

Observations of molecular emission lines in the radio and (sub)millimetre wavelength regimes provide insights into the interiors of molecular clouds which are inaccessible by other forms of radiation. Technological advancements are now allowing observations of molecules in distant galaxies, but our ability to interpret these data are limited by our knowledge of exactly how and where molecular emission lines originate within our own galaxy. Until recent years, observational biases caused by pre-selection of either certain positions in a molecular cloud or of a few molecular lines only allowed very selective studies. This thesis describes the acquisition and analysis of the first spectroscopically unbiased data set of the northern part of the prominent Orion A molecular cloud in the 1.3 mm atmospheric window. We develop templates of distinct regions and contrast their respective emission profiles, explore the reliability of commonly used line ratios as a tool to infer physical parameters, examine correlations between different molecular species and isotopologues, and calculate line luminosities. We further report on the surprising first detection of larger-scale CF+ emission in a variety of environments and aim to explain its widespread and fairly uniform distribution. Our data set also enables us to examine the nature of the so-called radical region within Orion A and to determine whether or not it is a distinct entity characterised by unusual molecular abundances. [Referees: Prof. Dr. Karl M. Menten, Prof. Dr. Pavel Kroupa, Prof. Dr. Klaus Desch, Prof. Dr. med. Ines Gütgemann]

	Main Colloquium
Prof. Roger Deane	ORATED

University of the Witwatersrand and University of Pretoria, South Africa

MeerKAT is the world’s most sensitive radio interferometer in its class and has demonstrated its potential through several impressive and in some cases, unexpected results. This has been enabled in large part by the excellent imaging fidelity offered by the 64-antenna array. However, several attributes of the telescope and decimetre radio sky make full scientific utilisation a challenge, necessitating significant algorithmic development. I will present a suite of my group’s early MeerKAT results related to galaxy and AGN evolution, and discuss some of the synergistic scientific potential with respect to VLBI programmes. I will also discuss how technical development has been and will continue to be leveraged between MeerKAT (and MeerKAT+, SKA1-mid) with both centimetre and millimetre-wave VLBI arrays, including the African VLBI Network and the (ng)EHT.

	Main Colloquium
Prof. Victoria Kaspi	ORATED

McGill University, Montreal, Canada

Fast Radio Bursts (FRBs) are a newly recognized and puzzling phenomenon consisting of few-millisecond bursts of radio waves coming from cosmological distances. They are ubiquitous, with all-sky rates of roughly 1000 per day, signaling a not uncommon yet powerful explosion of presently unknown origin. Recently there has been significant observational progress on understanding FRBs and recognizing their potential as novel cosmological probes, in large part thanks to the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst Project (CHIME/FRB). In this talk I review what is known about FRBs, and describe some of the latest CHIME/FRB results related to FRB origin and distribution in the Universe.

	Main Colloquium
Prof. Naomi McClure-Griffiths	ORATED

The Australian National University, Canberra

The evolution of galaxies is partially regulated by their infall and outflow of gas. Many simulations of galaxy formation and evolution have highlighted the importance of feedback in reproducing the observable Universe. Huge superbubbles and outflows, formed from the stellar winds and supernovae, dominate the observed structure of neutral hydrogen within many galaxies, including the nearby Small and Large Magellanic Clouds, which we can study with a physical resolution unmatched anywhere else in the Universe. As the most numerous galaxies in the Universe, dwarf galaxies may be important candidates for populating the intergalactic medium with enriched gas. Although star formation rates in dwarf galaxies can be lower than their more massive, starburst counterparts, these low mass systems have small gravitational potential wells and thereby find it difficult to maintain their star-forming material in the presence of intense stellar feedback. In this talk I will present new atomic hydrogen (HI) data from the Australian SKA Pathfinder (ASKAP) on the Small Magellanic Cloud. Using these data we have discovered that the Small Magellanic Cloud (SMC) has massive stellar feedback driven HI outflows. The outflows are comprised of cold filamentary gas extending up ~2 kpc from the main galaxy, with temperatures of T< 500 K and widths as small as 50 pc. We estimate a significant atomic gas mass flux in the range 0.2 - 1 solar mass per year, which may contribute to feeding the Magellanic Stream. I will also discuss recent observations and future plans for the Magellanic System with Galactic ASKAP Survey.

	Special Colloquium
Prof. Caitlin Casey	ORATED

University of Texas, Austin, USA

Although rare in the nearby Universe, gas-rich galaxies with extraordinary star-formation rates (100-1000x the Milky Way, at >100 Msun/year) represent the typical massive galaxy in the early Universe ~10 billion years ago. These galaxies’ high star-formation rates are predominantly obscured by dust which absorbs and re-radiates >95% of the energy from massive stars in the (sub)millimeter/far-infrared, hence they are often called dusty star-forming galaxies (DSFGs). Though our physical understanding of this highly obscured, heterogeneous population has matured significantly over the past decade thanks to ALMA, the prevalence of such systems at higher redshifts (z>4) is highly uncertain. I will discuss current efforts with ALMA and future surveys to learn more about these highly obscured galaxies beyond z~4. The detection of incredibly dust-rich systems (>10^9 Msun of dust) at these early epochs is key to understanding both the early formation mechanisms of dust (from supernovae, AGB stars and via grain growth in the ISM) and the assembly history of the Universe’s most massive galaxies and their rich, over dense environments. Last, I will also discuss efforts to transform our understanding of the reionization process of the Universe using future JWST datasets aimed at studying rare galaxies and sampling the Universe’s large scale structure.

	Promotionskolloquium
Arshia Jacob	ORATED

Max-Planck-Institut für Radioastronomie

The nature and distribution of atomic and molecular gas in the interstellar medium (ISM) is of great interest to astrophysicists because it is this gas that provides the raw material for the formation of new stars. This thesis investigates hydride molecules in the ISM and their use as diagnostics of its different phases. Particular emphasis is given to the central CH radical, a probe of diffuse and translucent molecular clouds, including those not traced by the otherwise common CO. I will detail our searches for the rare isotopologues of CH and address questions regarding the origin of another molecule, CH2, which despite being chemically associated with the ubiquitous CH, has largely remained elusive. And lastly, I will discuss the transition from the diffuse atomic to the diffuse and translucent molecular phases of the ISM by extending our view of the chemistry of argonium, ArH+, a tracer of almost purely atomic gas. [Referees: Prof. Dr. Karl M. Menten, Prof. Dr. Pavel Kroupa, Prof. Dr. Simon Stellmer, Prof. Dr. Hubert Schorle]

	Main Colloquium
Dr. Sylvia Plöckinger	ORATED

Lorentz Institute for theoretical physics, Leiden University, The Netherlands

Simulations are an invaluable tool in astrophysics to test theories relating to processes that take millions and billions of years. Within the last decades, cosmological simulations have drastically improved on their power to compare simulation with observations: from simulations only tracing the gravitational effects of cosmic structure formation ("dark matter only / N-body simulations") to fully hydro-dynamic simulations that form galaxy populations resembling observed galaxies. An upcoming new generation of cosmological simulations further advances the opportunities for a more direct comparison to observed galaxies. This is not only achieved by an increased mass and spatial resolution, but also by an innovative physical and chemical model of the gas phases of the interstellar medium (ionized, neutral atomic, molecular). This allows to self-consistently model the multi-phase interstellar medium (ISM) and produce more realistic mock observations. I will present first results of these new simulations and show how a multi-phase ISM can impact some of the small-scale challenges of the current standard cosmological model. This improved model for baryon physics also allows us to better study the impact on the formation of dwarf galaxies on the assumed dark matter particle. This will be illustrated by performing statistical test on the galaxy populations within cold and warm (sterile neutrino) dark matter simulations.

	Master Colloquium
Aparna Venkateshwaran	ORATED

Max-Planck-Institut für Radioastronomie

SPT2349-56 is a protocluster discovered via the 2500 deg2 South Pole Telescope (SPT) survey (Williamson et al., 2011). In this thesis, we study the kinematics and morphologies of the galaxies that are found in the core of SPT2349-56 using high-resolution (~ 1.7 kpc scale at z = 4.303) 850-micrometer dust continuum and [CII] data. Kinematical modelling of the galaxies using the 3DFIT task in 3DBAROLO gives a mean V/sigma = 5.0 +- 2.3. This implies that the galaxies agree with simulations that suggest galaxies at this redshift should be dynamically hotter, or dispersion dominated. To study the surface brightness profiles of the SPT sample, we use the ELLPROF task in 3DBAROLO and a PYTHON code to first construct the observed 850-micrometer dust and [CII] gas profiles. We then fit beam-convolved Sérsic functions to the observed profiles and derive the intrinsic brightness profiles. Lastly, we compare the intrinsic profiles to the intrinsic 160-micrometer dust profiles of three local (z ~ 0.1) starburst-galaxies – Centaurus A, NGC253 and NGC4945. [Referees: Prof. Dr. Karl Menten, Prof. Dr. Pavel Kroupa]

	Master Colloquium
Aparna Venkateshwaran	CANCELED

Max-Planck-Institut für Radioastronomie

TBD

	Main Colloquium
Dr. Hongsheng Zhao	ORATED

University of St Andrews, UK

A rare coincidence of scales in standard particle physics is needed to explain why \$\Lambda\$ or the negative pressure of cosmological dark energy (DE) coincides with the positive pressure \$P_0\$ of random motion of dark matter (DM) in bright galaxies. As a specific proof of concept we construct a smooth extension of GR with a simple kinetic Lagrangian of a four-velocity vector field \$V^\mu\$. We check whether the pressure from the V-field can bend space-time sufficiently to replace the roles of DE, Cold DM and heavy neutrinos in explaining anomalous accelerations at all scales.

	Main Colloquium
Prof. Jacqueline Hodge	ORATED

Leiden Observatory, the Netherlands

A substantial fraction of the Universe's star formation is heavily enshrouded by dust, and this basic fact has long been a hindrance to the development of a complete picture of galaxy evolution. Now, thanks to the advent of the Atacama Large Millimeter Array (ALMA) and the upgrades to the Karl G. Jansky Very Large Array (VLA), our view of dusty star formation at high-redshift is undergoing a radical transformation. I will present recent ALMA and JVLA observations of the gas, dust, and dust-unbiased star formation in high-redshift galaxies down to ~kpc and even sub-kpc scales, providing key insight into the morphology, dynamics, dark matter halo masses, and ISM physics in these systems. These observations have important implications for our understanding of the formation of the dustiest galaxies in the universe, which will soon be revealed in unprecedented detail by JWST.

	Special Colloquium
Prof. Monika Moscibrodzka	ORATED

Radboud University, Nijmegen, The Netherlands

The Event Horizon Telescope Collaboration, who produced the first ever image of a black hole, has just revealed a new view of the massive object at the centre of the M87 galaxy: how it looks in polarised light. This is the first time astronomers have been able to resolve polarisation this close to the edge of a black hole. A detailed theoretical understanding of near black hole processes is now crucial to interpret these new observations. I will review our current efforts to model polarimetric properties of light produced in synchrotron processes in plasma falling towards the event horizon and on theoretical insigths from the new observations of M87 core. The particular focus will be given to modeling and understanding the circular polarization of near horizon emission and its spatial and temporal handedness stability.

	Main Colloquium
Prof. Jan Palous	ORATED

Astronomical Institute of the Academy of Sciences of the Czech Republic, Prague

We explore the possibility of feeding the Super Massive Black Holes in galactic centers by expanding Supernova remnants. The shell expansion is simulated with hydrodynamical codes FLASH and RING using different approximations describing the thin shell expansion in the ISM. The simulations are performed in the homogeneous and also in the inhomogeneous turbulent medium. It shows that the supernovae occurring at specific places near the galaxy rotational axis can feed the central accretion disk surrounding the SMBH. The mass deposited into the central parsec by individual supernovae varies between 10 and 1000 solar masses depending on the ambient density and the distribution of supernovae in space. Supernovae occurring in the aftermath of a starburst event near a galactic center can supply within 30 Myr two to three order of magnitude more mass into the central parsec. The fate of that mass splits between the growth of the SMBH and outflow from the nuclear disk.

	SFB Colloquium
Dr. Richard Wünsch	ORATED

Astronomical institute of the Czech Academy of Sciences, Prague

I will present a novel fast radiation transport algorithm TreeRay, suitable to work together with hydrodynamic codes. It is based on reverse ray tracing combined with tree-based accelerated integration. TreeRay is implemented in the adaptive mesh refinement code FLASH, however, the method itself is independent of the host code and can be implemented in any grid based or particle based hydrodynamics code. A key advantage of TreeRay is that its computational cost is independent of the number of sources, making it suitable for simulations with many point sources (e.g. massive star clusters) as well as simulations where diffuse emission is important. A very efficient communication and tree-walk strategy enables TreeRay to achieve almost ideal parallel scalings. TreeRay can easily be extended with modules to treat radiative transfer at different wavelengths and to implement related physical processes. I will focus on the module calculating ionising radiation using the On-the-Spot approximation and describe various tests demonstrating that complicated simulations of star clusters with feedback from multiple massive stars become feasible with TreeRay. Finally, I will show several applications where TreeRay has been used, including project SILCC (SImulating Life Cycle of Clouds) - complex simulations of the interstellar medium in a part of the galactic disk, designed to capture the full matter cycle between gas and stars.

	Main Colloquium
Dr. Nadine Neumayer	ORATED

Max-Planck-Institut für Astronomie, Heidelberg

The centers of massive galaxies are special in many ways, not least because apparently all of them host supermassive black holes. Since the discovery of a number of relations linking the mass of this central black hole to the large scale properties of the surrounding galaxy bulge it has been suspected that the growth of the central black hole is intimately connected to the evolution of its host galaxy. However, at lower masses, and especially for bulgeless galaxies, the situation is much less clear. Interestingly, these galaxies often host massive star clusters at their centers, and unlike black holes, these nuclear star clusters provide a visible record of the accretion of stars and gas into the nucleus. I will present our ongoing observing programme of the nearest nuclear star clusters, including the ones in our Milky Way and the Sagittarius dwarf galaxy. These observations provide important information on the formation mechanism of nuclear star clusters, allow us to measure potential black hole masses and give clues on how black holes get to the centres of galaxies.

	Main Colloquium
Prof. Adam Deller	ORATED

Swinburne University of Technology, Hawthorn, Australia

The detection in gravitational waves of two merging neutron stars by LIGO/Virgo in 2017 fired the starting gun on a new era of multi-messenger GW/EM astronomy. Observations of GW170817 provided a wealth of information, first identifying its host galaxy and distance via the short-lived optical/NIR kilonova that followed the merger, and later with an extended campaign monitoring the relativistic outflow launched in the final throes of the merger. Radio and X-ray light curve modelling provided considerable insight as to the nature of this outflow, but even half a year after the merger, it was still unclear whether the highly relativistic jet launched by the merger had been contained by the mildly relativistic cocoon of material it slammed into, or if it had in fact punched free. The smoking gun evidence for a successful jet, of the kind observed in short GRBs, came only when milliarcsecond resolution radio imaging precisely measured the apparent superluminal motion of the source position. In this talk, I will revisit the results of VLBI observations of GW170817 and show how these were compared to hydrodynamical and analytical models to constrain the jet parameters and system viewing angle. I will show how this information was used to provide an improved standard siren measurement of the Hubble constant compared to the GW data alone, and review how improving VLBI instrumentation (higher sensitivities, wider fields-of-view) will enable similar measurements to be made for more distant merger afterglows in future LIGO/Virgo runs.

	Main Colloquium
Dr. Fabian Walter	ORATED

MPIA, Heidelberg

I will report on some of the results emerging from the ALMA large program ASPECS that obtained deep (sub-)millimeter imaging of the Hubble Ultra-Deep Field (H-UDF). The observations provide a census of dust and molecular gas in the H-UDF, down to masses that are typical of main-sequence galaxies at redshifts 1-3. The resulting data enable a great range of studies, from the characterisation of individual galaxies, capitalizing on the unique multi-wavelength database available for the H-UDF, to CO excitation studies that constrain the gas properties. Stacking analyses in dust continuum and CO line emission, using available H-UDF galaxy catalogues and precise redshifts from VLT/MUSE, helped to constrain the emission of galaxy samples that are too faint to be detected individually. The nature of the observations (full ALMA spectral scans) provides a census of dust and molecular gas in the cosmic volume defined by the H-UDF. The resulting cosmic molecular gas density as a function of redshift shows an order of magnitude decrease from z~2 to z=0. This is markably different from the atomic gas phase that shows a rather flat redshift dependence. With other measurements from the literature, these results are used to put additional observational constraints on the gas (net) accretion flows, needed to explain the build-up of stellar mass in galaxies, and are compared to cosmological galaxy formation simulations.

	SFB Colloquium
Prof. Jes Jørgensen	ORATED

Niels Bohr Institute, University of Copenhagen

The environments in which young stars form show a rich and varied chemistry. Understanding how, when and where complex organic and potentially prebiotic molecules are formed in these regions is a fundamental goal of astrochemistry. With the Atacama Large Millimeter/submillimeter Array (ALMA) we are moving into a new territory for these studies with ALMA's high sensitivity for faint lines, high spectral resolution which limits line confusion, and high angular resolution making it possible to study the structure of young protostars on solar-system scales. In this talk I will present some of our recent ALMA results concerning the chemistry taking place in star forming regions. I will discuss the implications of these results on the formation of complex organic molecules around young protostars and the link between the birth environments of these protostars, the conditions in their protoplanetary disks and eventually the chemistry in emerging solar systems.

	Main Colloquium
Prof. Feryal Özel	ORATED

University of Arizona

Recent observational advances with the Event Horizon Telescope, GRAVITY, and LIGO/VIRGO have opened up new avenues for studying black hole physics at horizon scales. In this talk, I will discuss what we have learned about the spacetimes of astrophysical black holes and how strong-field gravity is imprinted on their images. I will also present how the observations help us model and understand the heating and acceleration of plasmas on horizon scales.

	Main Colloquium
Prof. Mike Hudson	ORATED

University of Waterloo, Canada

Peculiar velocities - deviations from Hubble expansion - are the only practical probe of the growth of matter density fluctuations on very large scales in the nearby Universe. I will discuss recent measurements of cosmological parameters based on our approach of predicting peculiar velocities from the density field. This yields interesting results for the rms density fluctuations on 8 Mpc/h scales and their growth rate that may require new physics beyond the standard Lambda Cold Dark Matter model.

	Promotionskolloquium
Marilyn Cruces	ORATED

Max-Planck-Institut für Radioastronomie

I present the study of two radio transient phenomena: pulsars and Fast Radio Bursts (FRBs). Pulsars are superb natural laboratories for fundamental physics such as placing limits on the equation of state of ultra-dense matter and testing theories of gravity in the strong-field regime. FRBs are bright flashes of millisecond duration detected exclusively at radio frequencies. Their astrophysical origin is yet unknown. I present the ongoing pulsar survey using the world largest single-dish radio telescope, the Five-hundred-meter Aperture Spherical radio Telescope (FAST). In the follow-up observing campaign at Effelsberg, I monitored 10 pulsars discovered in the early commissioning phase of FAST. A highlight is PSR J2338+4818, the widest pulsar--white dwarf binary system with the most massive companion known to-date. In the following section, I model the long-term evolution of millisecond pulsars to understand their lower magnetic field strengths when compared to normal pulsars. I show that the observed magnetic field strengths of pulsars in binary systems can be well reproduced by a magnetic field decay driven by ambipolar diffusion. Lastly, I present an extensive multi-wavelength campaign on FRB121102, the first discovered repeating FRB. With 36 bursts detected with Effelsberg over four years, I find a periodic window of activity of 161+/-5 days. [Referees: Prof. Dr. Michael Kramer, Prof. Dr. Norbert Langer, Prof. Dr. Simon Stellmer, and Prof. Dr. Volkmar Gieselmann]

	Main Colloquium
Prof. Luis Rodríguez	ORATED

Instituto de Radioastronomia y Astrofisica, UNAM, Mexico

Wolf-Rayet (WR) stars are evolved massive stars, characterized by high luminosities and fast and dense stellar winds. We have detected a radio continuum pinwheel associated with WR 147, a nitrogen-rich WR star. These structures have been detected in the infrared around a handful of late-type carbon-rich WR stars with massive companions, where dust has formed in the zone where the two winds collide and produced a plume of dense gas and dust that is carried out with the WR wind. As the binary system rotates, an Archimedean spiral is produced. The resulting pinwheel contains information on wind speeds, wind-momentum ratio, and orbital parameters. However, WR 147 is a WN star and the formation of dust is unlikely, so a different emission mechanism must be at work. Our analysis of the data suggests that in this case the emission is dominantly of a nonthermal nature (synchrotron). It is possible that the pinwheels associated with WN stars will be detectable only as nonthermal emitters at radio wavelengths. From the characteristics of the pinwheel we estimate a period of 1.7 yr for the binary system (the WN star and a companion yet undetected directly) that is responsible for the pinwheel.

	Main Colloquium
Prof. Shrinivas Kulkarni	ORATED

California Institute of Technology, Pasadena, USA

The Universe began only with hydrogen and helium. It is cosmic explosions which build up the periodic table. Astronomers have now identified several classes of cosmic explosions of which supernovae constitute the largest group. The Palomar Transient Factory was an innovative 2-telescope experiment, and its successor, the Zwicky Transient Factory (ZTF), is a high tech project with gigantic CCD cameras, sophisticated algorithms (employing machine and deep learning) and robust pipelines, and squarely aimed to systematically find "blips and booms in the middle of the night". The speaker will talk about the great returns and surprises from this project: super-luminous supernovae, new classes of transients, new light on progenitors of supernovae, detection of gamma-ray bursts by purely optical techniques, troves of compact binary stars of interest to the LISA mission, asteroids in the interior of Venus and more. ZTF is now considered to be the stepping stone for LSST.

	Main Colloquium
Prof. Di Li	ORATED

National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China

We will release the first internationally open call-for-proposal for the The Five-hundred-meter Aperture Spherical radio Telescope (FAST) in the coming April. Previously, more than 100 PI-led science programs and five major surveys have been approved by the science committee. These observation have resulted in more than 40 publications, including two on the Nature magazine. I report a few highlights here, particularly from the CRAFTS survey, which is an unprecedented large-scale commensal survey. Enabled by a novel calibration technique, CRAFTS simultaneously records pulsar, Galactic HI, extra-galactic HI, and transient data streams. CRAFTS has discovered more than 150 new pulsars, including at least one DNS system. We have imaged about 5% of the full sky, including the Lockman hole, the Orion region, etc. CRAFTS has also resulted in 5 new FRBs, including one high DM repeater that has been localized.

	Promotionskolloquium
Felix Pötzl	ORATED

MPIfR

Supermassive black holes in the centres of radio-loud active galactic nuclei (AGN) can produce collimated relativistic outflows (jets). Magnetic fields are thought to play a key role in the formation and collimation of these jets, but the details are much debated. In my PhD thesis work I investigate mainly two methods of estimating the magnetic field strength and morphology on scales of a few 1000 gravitational radii of the central black hole. I will present the concept for high-accuracy core shift measurements at mm-wavelengths with source-frequency phase referencing observations, as well as an analysis of high-resolution space-VLBI data in full polarisation of the bright quasar 3C 345 obtained within the RadioAstron mission. The latter gives us insight on the magnetic field, where I present an analysis of the polarisation structure, the spectral index, Faraday rotation, as well as the brightness temperature of the source. This provides us with the picture of a jet with predominantly toroidal magnetic field, where plane-perpendicular shocks quench the magnetic field perpendicular to the jet direction, which also causes the jet to be partly out of equipartition. [Referees: Prof. Dr. Anton Zensus, Prof. Dr. Andreas Eckart, Prof. Dr. Susanne Crewell, and Dr. Steffen Rost]

	Promotionskolloquium
Henning Hilmarsson	ORATED

Max-Planck-Institut für Radioastronomie

Fast radio bursts (FRBs) are bright, energetic, millisecond duration radio transients of extragalactic origin. While over 100 FRBs have been detected, their origin is still unknown. Most FRB sources have only been seen to produce a single burst, but repeated bursts have been detected from 22. During this colloquium, I will discuss the main projects of my PhD work. The first project is on observations of superluminous supernovae (SLSNe) and long gamma-ray bursts (LGRBs), where we observed 10 SLSNe/LGRBs for 50 hours in search for repeating FRB sources using the C+ (5-9 GHz) receiver on Effelsberg. SLSNe and LGRBs were targeted due to their host galaxy sharing similarities to the host galaxy of the first discovered repeating FRB, FRB121102. The second project is on observations of FRB121102, where we investigate its long-term rotation measure (RM) evolution. We obtain 16 new RMs from November 2017 to August 2019, expanding the RM sample of FRB121102 up to 2.5 years. During this time, the RM of FRB121102 has showed a significant decrease in RM. We compare the RM evolution of FRB121102 to models that estimate the RM evolution from within a supernova remnant, and the RM evolution of the Galactic center magnetar, J1745-2900. [Referees: Prof. Dr. Michael Kramer, Prof. Dr. Norbert Langer, Prof. Dr. Simon Stellmer, and Prof. Dr. Robert Glaum]

	Main Colloquium
Dr. Coryn Bailer-Jones	ORATED

Max-Planck-Institut für Astronomie, Heidelberg

The first two interstellar objects (ISOs), 1I/'Oumuamua and 2I/Borisov, were discovered in 2017 and 2019 as they passed within a couple of astronomical units of the Earth and Sun. Using ground-based and HST data to reconstruct their orbits, together with Gaia data to trace back the positions of stars in the solar neighbourhood, we searched for stars that encountered these ISOs in the past (Bailer-Jones et al. 2018, 2020). A close, slow encounter could indicate that the ISO originated from that stellar system. We identified some such encounters, in particular one at 0.07 pc for 2I/Borisov. But how likely is this to be the parent star? What factors do we need to take into account to determine this? What are the prospects for more confident detections in the future? And what are ISOs anyway?

	Main Colloquium
Prof. Dennis Lehmkuhl	ORATED

Institute of Philosophy, University of Bonn

The Nobel Prize of 2020 was awarded to Roger Penrose for his singularity theorem of 1965, which the Nobel foundation interpreted as ''the discovery that black hole formation is a robust prediction of the general theory of relativity.'' However, the 1965 paper does not mention the term "black hole" but speaks of gravitational collapse and spacetime singularities, starting with remarks on Schwarzschild's 1916 solution to the Einstein field equations. In this talk, I will put Penrose's singularity theorem in its historical context, starting with Einstein's and Schwarzschild's interpretation of the Schwarzschild metric in the late 1910s and 1920s, and discuss how the metric was linked to the question of gravitational collapse by Oppenheimer and Snyder in the late 1930s, and reconsidered by Wheeler and others in the 1950s and 1960s. I will describe which conceptual and technical advances Penrose had to invent and combine in order to come up with his singularity theorem to go beyond considerations of specific spacetimes like that of Schwarzschild, and show why the theorem was such a game-changer. Finally, I will discuss different possible interpretations of the theorem.

	Main Colloquium
Prof. Stefan Jordan	ORATED

Zentrum für Astronomie der Universität Heidelberg

On December 3, 2020, the first (early) part of Gaia's third star catalogue will be published. Based on 34 months of Gaia observations it contains a significant increase in the number of entries compared to Gaia DR2: position measurements of more than 1.8 billion stars as well as proper motions, parallaxes, and broad-band photometry for about 1.4 billion stars. Additionally, both the precision and accuracy of the astrometric data has significantly improved, especially the determination of proper motions. Together with the release of the star catalogue, four papers are published, impressively demonstrating the scientific potential of the Gaia EDR3 catalogue.

	Main Colloquium
Dr. Jose Gómez	ORATED

Instituto de Astrofísica de Andalucía (CSIC), Granada, Spain

Mass accretion onto the supermassive black holes that power AGN leads to the formation of highly collimated relativistic jets that radiate across the entire electromagnetic spectrum, from radio to γ-rays. Over the past decades, AGN jets have been repeatedly studied through centimeter VLBI observations, but the resolution provided is just a step behind the necessary to resolve the compact regions in the vicinity of the central black hole where jets are formed, collimated, and accelerated. This limitation has recently been overcome by two technological improvements. On one side, the space VLBI mission RadioAstron has allowed us to increase the virtual size of our VLBI telescopes to as large as the distance to the Moon, achieving angular resolutions as small as 20 microarcseconds. On the other side, the participation of ALMA in millimeter VLBI arrays, such as the EHT and GMVA, has not only allowed the EHT to capture the first image of a black hole, but also holds the potential to actually address for the first time the fundamental questions of how gravity works in the strong-field regime near the event horizon, how accretion leads to the formation of relativistic jets, and what are the sites and mechanisms for the production of high energy emission in blazars. In this talk we summarize the results from our RadioAstron Key Science Program, which in combination with quasi-simultaneous GMVA and EHT observations provide us the sharpest view of blazars jets to probe the magnetic field and innermost jet regions in a sample of the brightest blazars to test jet formation models.

	Main Colloquium
Prof. Karin Öberg	ORATED

Harvard University, Cambridge, USA

The past decades have revealed that planets are incredibly common, and incredibly diverse. The origins of planets and their compositions are intimately linked to the chemical environments within which planets assemble, i.e. to the chemistry of planet-forming disks. The arrival of ALMA has provided observational access to disk chemistry, revealing disk snowlines, abundant organic molecules, and curious chemical gradients and sub-structures across the planet and comet forming zones. The most recent development is the execution of the ALMA Large Program MAPS (Molecules with ALMA on Planet-forming Scales), which has enabled us to zoom in on disk chemical structures at scales of 10-30 au. In parallel to these observational developments, astrochemistry models and laboratory experiments are providing new clues on what chemistry is likely to occur in different disk environments. I will present highlights from the MAPS program, as well as some recent laboratory astrochemistry discoveries. I will discuss how these new observational and laboratory data are affecting our understanding of the chemistry of planet formation, the chemical habitability of mature planetary systems, and the history of our own Solar System.

	SFB Colloquium
Dr. Catherine Walsh	ORATED

University of Leeds, UK

Protoplanetary disks around young stars are the factories of planetary systems. These structures contain all the material - dust, gas, and ice - that will build planets and other bodies such as comets. Hence, understanding the physics and chemistry of disks provides much needed insight into the conditions under which planets form, and determining their molecular content reveals the raw ingredients of planetary atmospheres. In this colloquium I will present early results from the first ALMA Large Program dedicated to the observation of molecular line emission from protoplanetary disks around nearby young stars at high angular resolution (0.1'' - 0.3''), titled Molecules with ALMA on Planet-Forming Scales or MAPS. I will present images that reveal intriguing sub-structure in emergent line emission from key organic molecules such as CO, C2H, HCN, and CH3CN.  I will discuss the link between known dust substructure and the observed line emission, and will present results from quantitative analyses of source properties such as radial mass distribution, chemical structure, ionisation structure, and elemental composition of the gas.  I will also discuss how observations in the gas-phase of large organic molecules provide insight into the composition of the icy-comet building reservoir around other stars. Finally I will discuss how early results from MAPS have provided the most detailed studies to date of the chemistry of planet formation.

	Main Colloquium
Dr. Sylvia Plöckinger	CANCELED

Lorentz Institute for theoretical physics, Leiden University, The Netherlands

Simulations are an invaluable tool in astrophysics to test theories relating to processes that take millions and billions of years. Within the last decades, cosmological simulations have drastically improved on their power to compare simulation with observations: from simulations only tracing the gravitational effects of cosmic structure formation ("dark matter only / N-body simulations") to fully hydro-dynamic simulations that form galaxy populations resembling observed galaxies. An upcoming new generation of cosmological simulations further advances the opportunities for a more direct comparison to observed galaxies. This is not only achieved by an increased mass and spatial resolution, but also by an innovative physical and chemical model of the gas phases of the interstellar medium (ionized, neutral atomic, molecular). This allows to self-consistently model the multi-phase interstellar medium (ISM) and produce more realistic mock observations. I will present first results of these new simulations and show how a multi-phase ISM can impact some of the small-scale challenges of the current standard cosmological model. This improved model for baryon physics also allows us to better study the impact on the formation of dwarf galaxies on the assumed dark matter particle. This will be illustrated by performing statistical test on the galaxy populations within cold and warm (sterile neutrino) dark matter simulations.

	Master Colloquium
Kartik Rajan Neralwar	ORATED

Max-Planck-Institut für Radioastronomie

The high spatial and spectral resolution of the SEDIGISM data has allowed us to investigate the physics of the molecular interstellar medium at an unprecedented level of detail. Duarte-Cabral et al. 2020 (MNRAS, 2609D) has produced a catalog of more than 10,000 molecular cloud structures from the full survey data using the Spectral Clustering for Interstellar Molecular Emission Segmentation (SCIMES) algorithm. In this project, we objectively characterize the resolved properties of these SEDIGISM clouds, in particular their morphology. The project consists of three parts. In the first part, we classify the clouds based on their morphological properties using the J-plots (Jaffa et al. 2018, MNRAS, 477, 1940J) and by visual inspection. We observe that most of the molecular clouds are elongated structures independent of the Galactic environment. In the second part, we search for possible correlations between cloud morphologies and their properties such as size, mass, velocity dispersion, surface density, and virial parameter and analyze the influence of the Galactic environment (like spiral arms, distance from the Galactic center) on the cloud properties. We find evidence showing that cloud morphologies are connected to integrated properties, and relate them to the physical processes behind them. We also plot the scaling relation between various cloud properties from the literature (like Larson's relation) and observe that the ring-like clouds show noticeable variations than other morphologies. Lastly, we correlate the SEDIGISM clouds with structures identified through other surveys, i.e. ATLASGAL filamentary structures and the bubbles from the HiGAL survey. This has helped us identify the coherent ATLASGAL and HiGAL structures as well as new elongated and ring-like clouds which could be further followed up for detailed studies. [Referees: Prof. Karl Menten, Prof. Pavel Kroupa]