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We report a sample of 463 high-mass starless clump (HMSC) candidates within$-60\deg<l<60\deg$ and $-1\deg<b<1\deg$. This sample has been singled out from10861 ATLASGAL clumps. All of these sources are not associated with any knownstar-forming activities collected in SIMBAD and young stellar objectsidentified using color-based criteria. We also make sure that the HMSCcandidates have neither point sources at 24 and 70 \micron~nor strong extendedemission at 24 $\mu$m. Most of the identified HMSCs are infrared ($\le24$$\mu$m) dark and some are even dark at 70 $\mu$m. Their distribution showscrowding in Galactic spiral arms and toward the Galactic center and somewell-known star-forming complexes. Many HMSCs are associated with large-scalefilaments. Some basic parameters were attained from column density and dusttemperature maps constructed via fitting far-infrared and submillimetercontinuum data to modified blackbodies. The HMSC candidates have sizes, masses,and densities similar to clumps associated with Class II methanol masers andHII regions, suggesting they will evolve into star-forming clumps. More than90% of the HMSC candidates have densities above some proposed thresholds forforming high-mass stars. With dust temperatures and luminosity-to-mass ratiossignificantly lower than that for star-forming sources, the HMSC candidates areexternally heated and genuinely at very early stages of high-mass starformation. Twenty sources with equivalent radius $r_\mathrm{eq}<0.15$ pc andmass surface density $\Sigma>0.08$ g cm$^{-2}$ could be possible high-massstarless cores. Further investigations toward these HMSCs would undoubtedlyshed light on comprehensively understanding the birth of high-mass stars.

High-mass Starless Clumps in the inner Galactic Plane: the Sample and Dust Properties