James Webb Space Telescope Feed Post

When, Where, and How Star Formation Happens in a Galaxy Pair at Cosmic Noon Using CANUCS JWST/NIRISS Grism Spectroscopy

Maps of the stellar mass surface density, segmentation of regions plus the Ha emitting clump in the red galaxy, dust (Av), Ha emission line flux surface density and SFRHa surface density, False colour image, Change in SFR from the broadband SFRs to the Ha SFRs, UV2300 surface density, log?(?2300) + equilibrium offset (1.65), and the SFRHa to SFRBB ratio. Panel A has been corrected for lensing, while Panels D, F, G, H, and I have been corrected for lensing and dust. Abstract: Spatially resolved studies are key to understanding when, where, and how stars form within galaxies. Using slitless grism spectra and broadband imaging from the CAnadian NIRISS Unbiased Cluster Survey (CANUCS) we study the spatially resolved properties of a strongly lensed (µ = 5.4±1.8) z = 0.8718 galaxy pair consisting of a blue face-on galaxy (10.2 ± 0.2 log(M/M?)) with multiple star-forming clumps and a dusty red edge-on galaxy (9.9 ± 0.3 log(M/M?)). We produce accurate Ha maps from JWST/NIRISS grism data using a new methodology that accurately models spatially varying continuum and emission line strengths. With spatially resolved indicators, we probe star formation on timescales of ~ 10 Myr (NIRISS Ha emission line maps) and ~ 100 Myr (UV imaging and broadband SED fits). Taking the ratio of the Ha to UV flux (?), we measure spatially resolved star formation burstiness. We find that in the face-on galaxy both Ha and broadband star formation rates (SFRs) drop at large galactocentric radii by a factor of ~ 4.7 and 3.8 respectively, while SFR over the last ~ 100 Myrs has increased by a factor of 1.6. Additionally, of the 20 clumps identified in the galaxy pair we find that 7 are experiencing bursty star formation, while 10 clumps are quenching and 3 are in equilibrium (either being in a state of steady star formation or post-burst). Our analysis reveals that the blue face-on galaxy disk is predominantly in a quenching or equilibrium phase. However, the most intense quenching within the galaxy is seen in the quenching clumps. This pilot study demonstrates what JWST/NIRISS data can reveal about spatially varying star formation in galaxies at Cosmic Noon.