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The Spatial Resolution Project aims to quantify stellar feedback by studying nearby galaxies at different spatial scales, using readily available, co-spatial Integral Field Unit (IFU) and Hubble Space Telescope (HST) data. We are analyzing nine nearby galaxies on three different spatial scales: 1-10s parsec scales, where feedback is driven; intermediate 100 pc scales, where feedback shapes the life cycle of molecular clouds; and large kpc scales, where feedback impacts the baryon cycle of galaxies. Building on a method developed by McLeod et al. (2020), we aim to identify and characterize individual feedback-driving massive stars. By applying this method to nine galaxies, our aims are to: (1) produce a comprehensive catalog of massive stars beyond the Magellanic Clouds; (2) derive a systematic census of cloud-scale feedback and massive stars as a function of galaxy properties; and (3) deliver an open-source analysis framework for future instruments. We are also constructing color-magnitude diagrams to determine spatially resolved star formation histories and test the fidelity of stellar population synthesis models. Additionally, we will investigate how observations of galaxy properties change with spatial resolution, linking nearby galaxies to the high-redshift universe, by mimicking observations at higher redshifts. Ultimately, the Spatial Reolsution Project will provide crucial empirical data for current numerical models of galaxy evolution.

Integral field spectrographs (also known as integral field units, or IFUs) have the capability of obtaining spatially and spectrally resolved images of the targeted object. This means that, for each individual pixel of an IFU image, there is a spectrum spanning over the entire wavelength range of the instrument. The image obtained from the observations is therefore not a 2D image at all, but rather a 3D data cube, where the two spatial dimensions (right ascension and declination) are extended by the third spectral dimension.

The advantage of an IFU is that, on top of the photometric inforamtion, a kinematical analysis is made possible. I have been working with data from the optical IFU MUSE and the near-infrared IFU KMOS (both mounted on the Very Large Telescope in Chile), targeting star forming regions in the Milky Way and soon also in our neighbour, the Large Magellanic Cloud. With the data I try to understand how we can trace and quantify the feedback of star formation in these regions.

The challenge of using IFUs for nearby star forming regions is given by the fact that one single telescope pointing is not enough to cover the entire desired area: instead, we have to rely on making mosaics, which (after data reduction) correspond to very big datacubes up to GB sizes. Handling these cubes in a smart way, and especially, analysing them, can be a challenge, and that is why I decided to make the scripts I have written for this purpose available to the public. Soon, you will be able to use MUSEpy for your MUSE data, and the upgraded version of it (IFUpy) for your IFU datacubes!

I am part of the SIGNALS survey (PI Laurie Rousseau-Nepton), an ambitious observing program which will observe a volume-limited sample of 39 local (< 10 Mpc) star-forming galaxies with the Imaging Fourier Transform Spectrograph SITELLE mounted on the Canada-France-Hawaii Telescope.

With spatial resolutions of 2 to 40 pc, we will be able to study star formation and stellar feedback in an unprecedented statistical sample of HII regions. Within the collaboration, the international team of astronomers will fully exploit this incredibly rich data set to analyze hot topics such as the properties of the interstellar medium, young star clusters, the dynamics of gas and stars, stellar feedback.

Visit the SIGNALS website to learn more!