Kavli Affiliate: Luis C. Ho
| First 5 Authors: Boris S. Kalita, John D. Silverman, Emanuele Daddi, Connor Bottrell, Luis C. Ho
| Summary:
A key question in galaxy evolution has been the importance of the apparent
`clumpiness’ of high redshift galaxies. Until now, this property has been
primarily investigated in rest-frame UV, limiting our understanding of their
relevance. Are they short-lived or are associated with more long-lived massive
structures that are part of the underlying stellar disks? We use JWST/NIRCam
imaging from CEERS to explore the connection between the presence of these
`clumps’ in a galaxy and its overall stellar morphology, in a mass-complete
($log,M_{*}/M_{odot} > 10.0$) sample of galaxies at $1.0 < z < 2.0$.
Exploiting the uninterrupted access to rest-frame optical and near-IR light, we
simultaneously map the clumps in galactic disks across our wavelength coverage,
along with measuring the distribution of stars among their bulges and disks.
Firstly, we find that the clumps are not limited to rest-frame UV and optical,
but are also apparent in near-IR with $sim 60,%$ spatial overlap. This
rest-frame near-IR detection indicates that clumps would also feature in the
stellar-mass distribution of the galaxy. A secondary consequence is that these
will hence be expected to increase the dynamical friction within galactic disks
leading to gas inflow. We find a strong negative correlation between how clumpy
a galaxy is and strength of the bulge. This firmly suggests an evolutionary
connection, either through clumps driving bulge growth, or the bulge
stabilizing the galaxy against clump formation, or a combination of the two.
Finally, we find evidence of this correlation differing from rest-frame optical
to near-IR, which could suggest a combination of varying formation modes for
the clumps.
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