Kavli Affiliate: John D. Silverman
| 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 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. However, there
is likely contribution from blending of smaller unresolved structures.
Furthermore, we observe a radial gradient of increasing clump mass towards the
centre of galaxies. This trend could be an indication of clump migration, but
accurate star-formation measurements would be required to confirm such a
scenario.
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