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We explore properties of Type Ib and IIb SN progenitors that are produced bystable mass transfer in binary systems, using a new grid of stellar evolutionmodels from an initial primary mass in the range of 10 - 18 $\mathrm{M_\odot}$at solar and Large Magellanic Cloud metallicities. We find that blue and yellowsupergiant SN IIb progenitors (e.g., of SN 2008ax, SN 2011dh, SN 2016gkg) havea hydrogen envelope mass less than about 0.15 $\mathrm{M_\odot}$, mostlyresulting from early Case B mass transfer with relatively low initial massesand/or low metallicity. Red supergiant (RSG) SN IIb progenitors (e.g., of SN1993J, SN 2013df) are produced via late Case B mass transfer and have a moremassive hydrogen envelope ($M_\mathrm{H,env} > 0.15~\mathrm{M_\odot}$). SN Ibprogenitors are predominantly produced by early Case B mass transfer. Ourmodels predict that SN IIb progenitors are systematically more luminous in theoptical ($-8.0 \lesssim M_\mathrm{V} \lesssim -5.0$) than the majority of SN Ibprogenitors ($M_\mathrm{V} \gtrsim -5.0$) for our considered initial massrange. However, the optically bright progenitor of SN Ib iPTF13bvn (i.e.,$M_\mathrm{V} \simeq -6.5$) can be well explained by a relatively low-massprogenitor with a final mass of $\sim 3.0~\mathrm{M_\odot}$. The event rate ofblue and yellow SN IIb progenitors would increase as metallicity decreases,while the event rate of SN Ib progenitors would decrease instead. By contrast,the population of RSG SN IIb progenitors would not be significantly affected bymetallicity.

Type Ib and IIb supernova progenitors in interacting binary systems