I will present an overview of the instrumentation development program and strategic R&D interests of the Herzberg Astronomy and Astrophysics Research Center, part of the National Research Council of Canada. Active major facility class instrumentation development includes real time control systems for the ELT's ANDES and MORFEO  instruments, next generation correlators for ALMA and the SKA mid telescopes, opto-mechanical systems for the Gemini Infrared Multi-Object Spectrograph (GIRMOS) and the second generation of the Gemini Planet Imager (GPI2), as well as low noise amplifiers for SKA mid and CCAT. I discuss the related R&D program and technology development roadmaps, including but not limited to adaptive optics, high contrast imaging and detectors. Finally, I discuss the evolving Canadian astronomical landscape and highlight future opportunities.

Understanding how atmospheres move is key to understanding the inner workings of planets - how their material is distributed and the subsequent implications on their formation and potential to host life. In our own Solar System, the observable fingerprints of winds in spectra are easily accessible and have provided substantial input into the composition and formation of our gas giants. Until recently, however, directly measuring winds in exoplanet atmospheres remained out of reach.

In this talk, I will present recent results that use ESPRESSO in 4-UT mode to directly probe atmospheric winds on close-in exoplanets. By resolving individual atomic absorption lines during planetary transit, we can detect Doppler shifts caused by day-to-night flows and global circulation patterns at different depths in these distant worlds. These measurements provide the first direct three dimensional constraints on wind speeds and directions in exoplanet atmospheres.

I will outline the observational technique, discuss what these wind measurements tell us about atmospheric dynamics and energy transport under extreme irradiation, and highlight how such observations are opening a new window on comparative planetology beyond the Solar System — just in time for the ELT era.

Distinct sets of elements are produced from different nucleosynthesis processes in galaxies that occur in core-collapse supernovae (CCSNe), Type-Ia supernovae (SNe Ia), asymptotic-giant-branch stars (AGBs), and various other enrichment sources. I will discuss both supernova and AGB enrichment in galaxies, as probed from integrated deep emission-line spectra of star-forming galaxies (SFGs) with direct elemental abundances. Galactic chemical enrichment from SNe has historically been constrained by alpha-enrichment ([α/Fe]) and metallicity ([Fe/H]) measurements from deep absorption-line spectra of individual stars in the Milky Way (MW) and some local group dwarf galaxies (and a handful of massive ellipticals with deep integrated absorption-line spectra out to z~2). The vast majority of galaxies in the universe are SFGs, with their fraction increasing with increasing redshift. We have recently shown that for SFGs (having deep integrated spectra with temperature sensitive auroral lines, enabling direct abundance determination), the oxygen-to-argon abundance ratio, log(O/Ar), vs Ar abundance, 12+log(Ar/H), is analogous to [α/Fe] vs [Fe/H] for stars. At low-z (z<0.3) with SDSS observations of ~800 SFGs, we show that galaxy chemical enrichment history is driven primarily by the interplay of CCSNe and SNe Ia, with their impact varying with galaxy mass. With a smaller sample of 11 SFGs at high-z (z~1.3-7.7) with JWST/NIRSPEC and Keck/MOSFIRE, we show that MW-like CCSNe and SNe Ia dominated enrichment processes occur at least out to z~4, beyond which rapid but intermittent star-formation may be at play. On the other hand, AGB nucleosynthesis is probed in SFGs from relative abundances of N & O. NIRSPEC@JWST observations revealed a handful of SFGs at high-z with high N/O abundance ratio at low O/H, dubbed extreme N-emitters. Some attribute this to extreme enrichment mechanisms active only in the early universe. However, we found high N/O at low O/H for a sample of 19 low-z (z<0.5) SFGs (a five-fold increase compared to earlier) using DESI DR1 spectra. The enhanced N/O values can be explained using galactic chemical evolution (GCE) models having long-lived N-enhancement from AGBs, coupled with strong outflows.

Faint blazars are often difficult to identify, as their recognition typically requires cross-matching positional counterparts across radio, optical, and X-ray catalogs. To support high-energy studies for the Cherenkov Telescope Array Observatory (CTAO), we adopted an alternative approach. Starting from the Fermi-LAT 4FGL-DR4 catalog (5,062 γ-ray sources at galactic latitude |b| > 10°), we searched for blazar counterparts using Firmamento*, a web-based platform developed within the Open Universe initiative of UNOOSA. Firmamento integrates multi-frequency data and high-level analysis tools for spectral energy distribution (SED) studies.
By combining automated algorithms with visual inspection and validation by experts, high-school, and undergraduate students — given the large size of the sample — we discovered 421 new blazar associations, reducing the fraction of unassociated Fermi-LAT sources from 25% to 17%. The resulting catalog, 1FLAT, has been published in the Astrophysical Journal Supplement Series.
This talk presents both the scientific results and the educational framework behind this collaborative effort.

 

* https://firmamento.nyuad.nyu.edu/data_access