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We present a sample of Type Icn supernovae (SNe Icn), a newly-discoveredclass of transients characterized by their interaction with H- and He-poorcircumstellar material (CSM). This sample is the largest collection of SNe Icnto date and includes observations of two published objects (SN 2019hgp and SN2021csp) as well as two objects (SN 2019jc and SN 2021ckj) not yet published inthe literature. The SNe Icn display a range of peak luminosities, rise times,and decline rates, as well as diverse late-time spectral features. Toinvestigate their explosion and progenitor properties we fit their bolometriclight curves to a semi-analytical model consisting of luminosity inputs fromcircumstellar interaction and radioactive decay of $^{56}$Ni. We infer lowejecta masses ($\lesssim$ 2 M$_\odot$) and $^{56}$Ni masses ($\lesssim$ 0.04M$_\odot$) from the light curves, suggesting that normal stripped-envelopesupernova (SESN) explosions within a dense CSM cannot be the underlyingmechanism powering SNe Icn. Additionally, we find that an upper limit on thestar formation rate density at the location of SN 2019jc lies at the lower endof a distribution of SESNe, in conflict with a massive star progenitor of thisobject. Based on the estimated ejecta masses, $^{56}$Ni masses, and explosionsite properties, we favor a low-mass, ultra-stripped star as the progenitor ofsome SNe Icn. For others, we suggest that a Wolf-Rayet star progenitor maybetter explain their observed properties. This study demonstrates that multipleprogenitor channels may produce SNe Icn and other interaction-poweredtransients.

The Diverse Properties of Type Icn Supernovae Point to Multiple Progenitor Channels