A First Look into the Nature of JWST/MIRI 7.7 micron Sources from SMACS 0723

TL;DR

This study presents initial JWST MIRI 7.7 micron observations of the SMACS J0723.3-7327 field, revealing a diverse galaxy population up to redshift 10 and demonstrating the potential of mid-IR data to probe the early universe.

Contribution

First analysis of JWST MIRI 7.7 micron sources, showing their properties and high-redshift potential, highlighting the utility of mid-IR observations for studying the early universe.

Findings

Most galaxies are normal up to z=4

About 2% of sources are at z~9-10

Galaxies have stellar masses from 10^7 to 10^{11} Msun

Abstract

Until now, our knowledge of the extragalactic Universe at mid-IR wavelengths (> 5 microns) was limited to rare active galactic nuclei (AGN) and the brightest normal galaxies up to z~3. The advent of the JWST with its Mid-Infrared Instrument (MIRI) will revolutionise the ability of the mid-IR regime as a key wavelength domain to probe the high-z Universe. In this work we present a first study of JWST MIRI 7.7 micron sources selected with > 3 sigma significance from the lensing cluster field SMACS J0723.3-7327. We model their spectral energy distribution fitting with 13 JWST and HST broad bands, in order to obtain photometric redshifts and derived physical parameters for all these sources. We find that this 7.7 micron galaxy sample is mainly composed of normal galaxies up to z=4 and has a tail of about 2% of sources at higher redshifts to z~ 9-10. The vast majority of our galaxies have [3.6]-[7.7]<0 colours and very few of them need high dust extinction values (A_V=3 -6 mag) for their SED fitting. The resulting lensing-corrected stellar masses span the range 10^7-10^{11} Msun. Overall, our results clearly show that the first MIRI 7.7 micron observations of deep fields are already useful to probe the high-redshift Universe and suggest that the deeper 7.7 micron observations to be available very soon will open up, for the first time, the epoch of reionisation at mid-IR wavelengths.