Master Colloquium
Vishalika Sharma	SCHEDULED

MPIfR

Galaxies with similar stellar mass can exhibit different substantially star rates. These differences can arise from variations in the molecular gas reservoir or the efficiency with which it is converted into stars, or both. Understanding the Relative Solutions of Two Factors is the important for what determines star formation on the other hand over the different galaxy populations. Many resolved studies have begun to become both molecular gas content and its star efficiency formation across and below the main-sequence, but their relative contribution and radial dependence remain unclear. In this work, I present the radial distribution of molecular gas across the star-forming main using CO(2-1) observations of 258 nearby KILOGAS galaxies. Both CO-detected and non-detected sources are included are included, co-igating the bias towards CO-bright and gas-rich systems. Galaxies are classified by their integrated main-sequence offset, ∆MS, starburst, star-forming, green-valley and quiescent populations. Spectral stacking is used to recover average CO emission from both detected and faint emission or non-detected sources. Overall, the results show that both molecular gas availability and star formation efficiency contribute to the differences in star formation activity across ∆MS, with their relative importance radius with.

	Promotionskolloquium
Gerrit Fabian Grutzeck	SCHEDULED

MPIfR

The increasing bandwidth of modern radio astronomical receivers demands new digital signal processing architectures that combine hard real-time performance with high computational flexibility. This talk presents the U-Board, a closely coupled heterogeneous platform integrating an FPGA, a GPU-based System-on-Module, and a wideband analogue frontend providing up to 5.2 GHz of instantaneous bandwidth for signal generation and acquisition. Rather than focusing on a single instrument, the U-Board was developed as a universal backend for radio astronomy and laboratory spectroscopy. Its capabilities are demonstrated through three applications, with particular emphasis on the MKID readout for the APEX telescope in Chile and U-SAGE, a backend for chirped-pulse Fourier transform molecular spectroscopy. For the APEX MKID camera, the new readout reduces the median detector noise by 12 %, corresponding to an expected 26 % reduction in mapping time. In laboratory spectroscopy, U-SAGE combines phase-coherent signal generation and acquisition within a single platform and achieves Allan stability beyond 10^8 integrations, more than three orders of magnitude beyond the previous experimental setup. The presented results demonstrate that the U-Board provides a compact, versatile, and scalable platform for next-generation millimeter and sub-millimeter instrumentation, enabling both more sensitive astronomical observations and highly stable broadband spectroscopy.

	Main Colloquium
Professor Ilse de Looze	SCHEDULED

Ghent University

Interstellar dust accounts for a small fraction of the interstellar medium (ISM) mass. Yet, dust grains play a pivotal role in the heating and cooling balance of gas clouds, facilitate the formation of simple to complex organic molecules, and obscure roughly half of the starlight in galaxies. To fully unravel the impact of dust grains on the star formation process and how dust grains lead to the formation of planetary material, we first need to understand how dust forms and evolves in the ISM. In this talk, I will summarise our current knowledge of the dust lifecycle; from its formation in stellar sources, to its further growth in the ISM through accretion processes, and the eventual processing and/or destruction of dust grains through supernova shocks, sputtering in hot gas, photo-processing by harsh radiation and the removal of dust through gaseous outflows. I will conclude by exploring how the formation, growth and destruction of dust shape the rapid build-up of dust and metals in the early Universe.

	Informal Colloquium
Dr.ir. Stefanie A. Brackenhoff	SCHEDULED

Delft University of Technology, The Netherlands

DESHIMA 2.0 is an integrated superconducting spectrometer that uses an MKID filterbank to instantaneously cover the 200-400 GHz band with 339 spectral channels. I will discuss deep DESHIMA 2.0 integrations used to determine the spectroscopic redshifts of Dusty Star-Forming Galaxies, which are a major population tracing dust-obscured star formation at high redshifts. We observe them in position-switching mode, which offers a high sensitivity for unresolved targets. I will show the calibration and analysis strategies, performance metrics, and preliminary astronomical spectra. I will highlight how combining emission from several weak CO lines in the same galaxy can provide redshift constraints, even when individual line detections are challenging. Understanding systematics in DESHIMA 2.0 data provides crucial lessons for future on-chip imaging spectrometers, such as TIFUUN. This successor to DESHIMA 2.0 combines many on-chip spectrometers into two integral field units. It will rapidly map large cosmological volumes, to offer two complementary scientific probes: a survey of individually detected bright line-emitting galaxies, and line-intensity mapping of [C II]. In the second part of my talk, I will present TIFUUN, its planned observations, preliminary sensitivity forecasts, and preliminary data analysis strategies. In addition to presenting DESHIMA 2.0 and TIFUUN, this talk highlights that increasing multiplexing does not automatically translate into more astrophysical information: the return depends on how calibration, instrumental systematics, observational effects and statistical inference are jointly handled. Developing these analysis strategies is therefore an essential and scientific part of turning increasingly data-rich (sub)mm measurements into new astrophysical constraints.