FRESCO: The Paschen-\(\alpha\) Star Forming Sequence at Cosmic Noon

• Published in: arXiv.org
• Main Authors: Neufeld, Chloe, Pieter van Dokkum, Yasmeen Asali, Covelo-Paz, Alba, Leja, Joel, Lin, Jamie, Matthee, Jorryt, Oesch, Pascal A, Reddy, Naveen A, Shivaei, Irene, Whitaker, Katherine E, Wuyts, Stijn, Brammer, Gabriel, Marchesini, Danilo, Maseda, Michael V, Naidu, Rohan P, Nelson, Erica J, Velichko, Anna, Weibel, Andrea, Xiao, Mengyuan
• Format: Paper
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 10.07.2024
• Subjects: Galaxies; Ionization; Luminosity; Physical properties; Star & galaxy formation; Star formation rate; Stellar mass
• ISSN: 2331-8422

We present results from the JWST First Reionization Epoch Spectroscopically Complete Observations survey (FRESCO) on the star forming sequence of galaxies at \(1.0<z<1.7\), around the peak of the cosmic star formation history. Star formation rates (SFRs) are measured from the redshifted, nearly dust-insensitive Paschen-\(\alpha\) emission line, and stellar mass measurements include the F444W (4.4 \(\mu\)m; rest-frame H) band. We find SFRs of galaxies with \(M*>9.5 M_\odot\) that are lower than found in many earlier studies by up to 0.6 dex, but in good agreement with recent results obtained with the Prospector fitting framework. The difference log(SFR(Pa\(\alpha\))-SFR(Prospector)) is -0.09 \(\pm\) 0.04 dex at \(10^{10-11} M_\odot\). We also measure the empirical relation between Paschen-\(\alpha\) luminosity and rest-frame H band magnitude and find that the scatter is only 0.04 dex lower than that of the SFR-M* relation and is much lower than the systematic differences among relations in the literature due to various methods of converting observed measurements to physical properties. We additionally identify examples of sources -- that, with standard cutoffs via the UVJ diagram, would be deemed quiescent -- with significant, typically extended, Paschen-\(\alpha\) emission. Our results may be indicative of the potential unification of methods used to derive the star forming sequence with careful selection of star forming galaxies and independent star formation rate and stellar mass indicators.