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The 3rd data release of the Gaia mission includes orbital solutions for $>10^5$ single-lined spectroscopic binaries, representing more than an order ofmagnitude increase in sample size over all previous studies. This dataset is atreasure trove for searches for quiescent black hole + normal star binaries. Weinvestigate one population of black hole candidate binaries highlighted in thedata release: sources near the main sequence in the color-magnitude diagram(CMD) with dynamically-inferred companion masses $M_2$ larger than theCMD-inferred mass of the luminous star. We model light curves, spectral energydistributions, and archival spectra of the 14 such objects in DR3 withhigh-significance orbital solutions and inferred $M_2 > 3\,M_{\odot}$. We findthat 100\% of these sources are mass-transfer binaries containing a highlystripped lower giant donor ($0.2 \lesssim M/M_{\odot} \lesssim 0.4$) and muchmore massive ($2 \lesssim M/M_{\odot} \lesssim 2.5$) main-sequence accretor.The Gaia orbital solutions are for the donors, which contribute about half thelight in the Gaia RVS bandpass but only $\lesssim 20\%$ in the $g-$band. Theaccretors' broad spectral features likely prevented the sources from beingclassified as double-lined. The donors are all close to Roche lobe-filling($R/R_{\rm Roche\,lobe}>0.8$), but modeling suggests that a majority aredetached ($R/R_{\rm Roche\,lobe}<1$). Binary evolution models predict thatthese systems will soon become detached helium white dwarf + main sequence "ELCVn" binaries. Our investigation highlights both the power of Gaia data forselecting interesting sub-populations of binaries and the ways in which binaryevolution can bamboozle standard CMD-based stellar mass estimates.

What are the spectroscopic binaries with high mass functions near the Gaia DR3 main sequence?