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

JWST/NIRISS grism data and false colour images. In each of the panels, we have marked objects of interest. The bottom right panel shows the multiply imaged QMP (1.A-D) in the MACS J0417.5-1154 cluster, here we see four of the five images of the galaxy, the fifth being under the BCG (2). The top left panel shows the image of the QMP we will be examining as it is the most magnified and least contaminated of the multiple images. The top right and bottom left panels show the NIRISS grism data in all orients and filters, focusing on the image of the QMP we are using. 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.