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The NASA concept mission ORCAS (Orbiting Configurable Artificial Star) aimsto provide near diffraction-limited angular resolution at visible andnear-infrared wavelengths using laser signals from space-based cubesats asAdaptive Optics beacons for ground-based 8-30 meter telescopes, in particularthe 10 meter Keck Telescopes. When built as designed, ORCAS+Keck would deliverimages of ~0.01-0.02" FWHM at 0.5-1.2 micron wavelength that reach AB<31 magfor point sources in a few hours over a 5x5" FOV that includes IFUcapabilities. We summarize the potential of high-resolution faint galaxyscience with ORCAS. We show that the ability to detect optical-near-IR pointsources with r_e>0.01" FWHM to AB<31 mag will yield about 5.0x10^6 faintstar-forming (SF) clumps per square degree, or ~0.4 per arcsec^2. From recentHST lensing data, the typical intrinsic (unlensed) sizes of SF clumps at z~1-7will be r_e ~1-80 m.a.s. to AB<31 mag, with intrinsic (unmagnified) fluxes asfaint as AB<35-36 mag when searching with ORCAS around the critical curves oflensing clusters imaged with HST and JWST. About half of these SF clumps willhave sizes below the ORCAS diffraction limit, and the other half will beslightly resolved, but still mostly above the ORCAS surface brightness (SB)limits. ORCAS will address how galaxies assemble from smaller clumps to stabledisks by measuring ages, metallicities, and gradients of clumps withingalaxies. ORCAS can monitor caustic transits of individual stars in SF clumpsat z>1-2 that have been detected with HST, and those that may be detected withJWST at z>6 at extreme magnifications (mu>10^3-10^5) for the first stars andtheir stellar mass black hole accretion disks. ORCAS provides a uniqueopportunity to obtain a statistical census of individual stars at cosmologicaldistances, leveraging the largest telescopes only available on the ground.

Galaxy Science with ORCAS: Faint Star-Forming Clumps to AB$\leq$31 mag and r$_e$$\geq$ 0.01"