Neutron stars: evolution and emission

Main Colloquium
Dr. Evan Keane
SCHEDULED
National University of Ireland, Galway

Neutron stars exhibit many of the most extreme phenomena ever observed. They are also the most precise astrophysical tools in existence. Fortunately they are readily observable, across the electromagnetic spectrum, from Birr to Bonn to Boolardy. In this talk I will describe what is, and is not, known about neutron stars, with particular emphasis on the inter-related topics of their evolution post-supernova and pulsar emission physics. I will describe the difficulties involved in identifying evolutionary tracks for neutron stars, and discuss some potential solutions to these. Considering the growing number of diverse observational classes within the 'neutron star zoo' I will describe how these groups are, and are not, evolutionarily linked to one another. I will also describe search strategies that might identify the most interesting undiscovered sources.

Physical and chemical properties during high-mass star formation

Informal Colloquium
Caroline Gieser
SCHEDULED
Max-Planck-Institut für Astronomie, Heidelberg

During high-mass star formation, fragmentation takes place on various spatial scales from giant molecular clouds down to disk scales. At the earliest evolutionary stages, high-mass protostars are still deeply embedded within their parental molecular cloud and can be studied best at high spatial resolution with interferometers at mm wavelengths. The IRAM/NOEMA large program CORE allows us to analyze the physical and chemical properties of a sample of luminous high-mass star-forming regions. The 1 mm dust continuum of the sample shows a large diversity of fragmentation properties. Using the spectral line emission, we are able to determine the physical structure (temperature and density) and molecular content of individual fragmented cores. Even though all regions are classified to harbor high-mass protostellar objects, the molecular content shows a high degree of complexity. By combining the observed core properties, we are able to estimate chemical timescales with the physical-chemical model MUSCLE. We find well-constrained density and temperature profiles in agreement with theoretical predictions. The molecular complexity in the core spectra can be explained by an age spread that is then confirmed by our physical-chemical modeling. The hot molecular cores show the greatest number of emission lines, but we also find evolved cores in which most molecules are destroyed and, thus, the spectra appear line-poor once again. Currently, we are expanding our sample with ALMA 3 mm observations of 11 additional high-mass star-forming regions at different evolutionary stages - from infrared dark clouds to ultra-compact HII regions - in order to further investigate the evolution of the physical and chemical properties on core scales.

The cradles of star and planet formation: disks, multiplicity, and stellar masses of low to intermediate-mass protostars

Main Colloquium
Dr. John Tobin
SCHEDULED
National Radio Astronomy Observatory, Charlottesville, USA

The formation of disks and multiple star systems are integral parts of the star and planet formation process. Most stellar mass must be accreted through a disk, disks are the future sites of planet formation, and disks will also give rise to companion stars. Using ALMA and the VLA, we are conducting large continuum surveys of protostars (with molecular lines toward a subset of the full sample) in the nearby Perseus and Orion star-forming regions (with 20-30 au resolution) to characterize the disk radii, disk masses, and frequency of multiplicity throughout the protostellar phase. The molecular line data enable us to measure the masses of the protostars and we are beginning to identify and characterize the formation environments of both low and intermediate mass protostars. We find clear changes in multiplicity properties with evolution that link back to their formation mechanisms, establishing a foundation from which multiplicity evolution must begin.

Towards prebiotic chemistry in the interstellar medium

Main Colloquium
Dr. Izaskun Jiménez-Serra
SCHEDULED
Centro de Astrobiología, Madrid, Spain

In the past decade, Astrochemistry has witnessed an impressive increase in the number of detections of complex organic molecules. Some of these species are of prebiotic interest such as glycolaldehyde, the simplest sugar, or amino acetonitrile, a possible precursor of glycine. Recently, we have reported the detection of several new complex organic species in the interstellar medium, such as hydroxylamine and ethanolamine, known to be intermediate species in the formation processes of ribonucleotides and phospholipids within theories for the origin of life. In this talk, I will present our recent efforts to establish whether key precursors of prebiotic systems chemistry can be found in space. I will also analyse how chemical complexity builds up in the interstellar medium thanks to observations of the complex organic content in starless/pre-stellar cores, which represent the initial conditions of Solar-system formation.

TBD

Promotionskolloquium
Weiwei Chen
SCHEDULED
Max-Planck-Institut für Radioastronomie

TBD

A NICER view of neutron stars

Main Colloquium
Prof. Anna Watts
SCHEDULED
Astronomical Institute Anton Pannekoek, University of Amsterdam

TBD

Planets are places: exoplanet atmosphere characterization in the 2020s and beyond

Main Colloquium
Dr. Laura Kreidberg
SCHEDULED
Max-Planck-Institut für Astronomie, Heidelberg

TBD

Astrophysics of Rotating Dust

Main Colloquium
Prof. Thiem Hoang
SCHEDULED
Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea

TBD

From galaxy-scale feedback through cosmic history to the microwave background temperature evolution: an updated view on the early Universe from new tools in (sub)mm astronomy

Main Colloquium
Prof. Dominik Riechers
SCHEDULED
Universität zu Köln

TBD

The PAH revolution: cold, dark carbon at the earliest stages of star formation

SFB Colloquium
Prof. Brett McGuire
SCHEDULED
Massachusetts Institute of Technology, Cambridge, USA

TBD

Illuminating the magnetised cosmic web

Main Colloquium
Dr. Shane O'Sullivan
SCHEDULED
Dublin City University

TBD

TBD

Special Colloquium
Prof. Adam Leroy
SCHEDULED
Ohio State University, USA

TBD

Our Galaxy’s Center: a Window into the High-Redshift Universe

Main Colloquium
Prof. Cara Battersby
SCHEDULED
University of Connecticut

Galaxy centers are the hubs of activity that drive galaxy evolution, from supermassive black holes to dense stellar clusters and feedback from newly-formed stars. Our own galaxy’s center has properties (densities, temperatures, and turbulent line widths) that are reminiscent of galaxies at the peak of cosmic star formation, but in our own cosmic backyard, where the interplay of these physical processes can be resolved in detail. In this talk, I will discuss gas inflow into our Galaxy’s Center, properties of the gas, and incipient star formation. I will discuss simulations of gas flows into the Galactic Center, which are thought to contribute to the unusual properties of star formation in this region, namely that it is producing 10 times fewer stars than predicted by standard scaling relations. I will describe observations of the gas and incipient star formation in this region, as well as discuss efforts to measure whether or not this unusual environment results in a change to the Initial Mass Function.