Dust evolution in protoplanetary disks from small dust grains to pebbles is key to the planet formation process. The gas in protoplanetary disks should influence the vertical distribution of small dust grains (∼1 μm) in the disk. Utilizing archival near-infrared polarized light and millimeter observations, we can measure the scale height and flare parameter β of the small dust grain scattering surface and ¹²CO gas emission surface for three protoplanetary disks: IM Lup, HD 163296, and HD 97048 (CU Cha). For two systems, IM Lup and HD 163296, the ¹²CO gas and small dust grains at small radii from the star have similar heights, but at larger radii (>100 au), the dust grain scattering surface height is lower than the ¹²CO gas emission surface height. In the case of HD 97048, the small dust grain scattering surface has similar heights to the ¹²CO gas emission surface at all radii. We ran a protoplanetary disk radiative transfer model of a generic protoplanetary disk with TORUS and showed that there is no difference between the observed scattering surface and ¹²CO emission surface. We also performed analytical modeling of the system and found that gas-to-dust ratios larger than 100 could explain the observed difference in IM Lup and HD 163296. This is the first direct comparison of observations of gas and small dust grain height distribution in protoplanetary disks. Future observations of gas emission and near-infrared scattered-light instruments are needed to look for similar trends in other protoplanetary disks.

原行星盘中的尘埃从小尘埃颗粒到卵石的演化是行星形成过程的关键。在原行星盘的气体应该影响小的尘埃颗粒（〜1的垂直分布μ在盘米）。利用档案近红外偏振光和毫米波观测，我们可以测量三个原行星盘的小尘埃颗粒散射面和¹² CO气体发射面的标高和耀斑参数β：IM Lup、HD 163296和HD 97048（CU查）。对于两个系统，IM Lup 和 HD 163296，来自恒星的小半径处的¹² CO 气体和小尘埃颗粒具有相似的高度，但在较大半径（> 100 au）处，尘埃颗粒散射面高度低于¹²CO 气体排放面高度。在 HD 97048 的情况下，小尘埃颗粒散射表面在所有半径上都具有与¹² CO 气体排放表面相似的高度。我们使用 TORUS 运行了一个通用原行星盘的原行星盘辐射传递模型，结果表明观察到的散射表面与¹²CO排放面。我们还对该系统进行了分析建模，发现大于 100 的气尘比可以解释在 IM Lup 和 HD 163296 中观察到的差异。这是对原行星中气体和小尘粒高度分布的首次直接比较。磁盘。未来需要对气体发射和近红外散射光仪器进行观测，以寻找其他原行星盘的类似趋势。