Kavli Affiliate: Luis C. Ho
| First 5 Authors: Boris S. Kalita, John D. Silverman, Emanuele Daddi, Wilfried Mercier, Luis C. Ho
| Summary:
Resolved stellar morphology of $z>1$ galaxies was inaccessible before JWST.
This limitation, due to the impact of dust on rest-frame UV light, had withheld
major observational conclusions required to understand the importance of clumps
in galaxy evolution. Essentially independent of this issue, we use the
rest-frame near-IR for a stellar-mass dependent clump detection method and
determine reliable estimations of selection effects. We exploit publicly
available JWST/NIRCam and HST/ACS imaging data from CEERS, to create a
stellar-mass based picture of clumps in a mass-complete sample of 418 galaxies
within a wide wavelength coverage of $0.5-4.6,mu$m and a redshift window of
$1 < z < 2$. We find that a near-IR detection gives access to a larger, and
possibly different, set of clumps within galaxies, with those also detected in
UV making up only $28%$. Whereas, $85%$ of the UV clumps are found to have a
near-IR counterpart. These near-IR clumps closely follow the UVJ classification
of their respective host galaxies, with these hosts mainly populating the
star-forming regime besides a fraction of them ($16%$) that can be considered
quiescent. The mass of the detected clumps are found to be within the range of
$10^{7.5-9.5},rm M_{odot}$, therefore expected to drive gas into galaxy
cores through tidal torques. The clump stellar mass function is found to have a
slope of $-1.50 pm 0.14$, indicating a hierarchical nature similar to that of
star-forming regions in the local Universe. Finally, we observe a radial
gradient of increasing clump mass towards the centre of galaxies.
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