We report the discovery of 25 new open clusters resulting from a search in dense low galactic latitude fields. We also provide, for the first time, structural and astrophysical parameters for the new findings and 34 other recently discovered open clusters using Gaia DR2 data. The candidates were confirmed by jointly inspecting the vector point diagrams and spatial distribution. The discoveries were validated by matching near known objects and comparing their mean astrometric parameters with the available literature. A decontamination algorithm was applied to the three-dimensional astrometric space to derive membership likelihoods for clusters stars. By rejecting stars with low membership likelihoods, we built decontaminated colour-magnitude diagrams and derived the clusters astrophysical parameters by isochrone fitting. The structural parameters were also derived by King-profile fittings over the stellar distributions. The investigated clusters are mainly located within 3 kpc from the Sun, with ages ranging from 30 Myr to 3.2 Gyr and reddening limited to E(B-V)=2.5. On average, our cluster sample presents less concentrated structures than Gaia DR2 confirmed clusters, since the derived core radii are larger while the tidal radii are not significantly different. Most of them are located in the IV quadrant of the Galactic disc at low latitudes, therefore they are immersed in dense fields characteristic of the inner Milky Way.

中文翻译：

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使用 Gaia DR2 在致密恒星场中发现银河疏散星团及其天体物理特性

我们报告发现了 25 个新的疏散星团，这些星团是在密集的低银河纬度场中进行的搜索。我们还首次使用 Gaia DR2 数据为新发现和其他 34 个最近发现的疏散星团提供了结构和天体物理参数。通过联合检查矢量点图和空间分布来确定候选人。通过匹配附近的已知物体并将它们的平均天体测量参数与可用文献进行比较来验证这些发现。将去污算法应用于三维天体测量空间以推导出星团恒星的隶属可能性。通过拒绝成员可能性低的恒星，我们构建了净化后的颜色-星等图，并通过等时线拟合得出了星团的天体物理参数。结构参数也由恒星分布的 King-profile 拟合得出。被调查的星团主要位于距太阳 3 kpc 以内，年龄从 30 Myr 到 3.2 Gyr 不等，红化仅限于 E(BV)=2.5。平均而言，我们的集群样本呈现出比 Gaia DR2 确认的集群更不集中的结构，因为派生的核心半径更大，而潮汐半径没有显着差异。它们中的大部分位于低纬度的银盘IV象限，因此它们沉浸在具有内部银河系特征的密集场中。我们的集群样本呈现出比 Gaia DR2 确认的集群更不集中的结构，因为派生的核心半径更大，而潮汐半径没有显着差异。它们中的大部分位于低纬度的银盘IV象限，因此它们沉浸在具有内部银河系特征的密集场中。我们的集群样本呈现出比 Gaia DR2 确认的集群更不集中的结构，因为导出的核心半径更大，而潮汐半径没有显着差异。它们中的大部分位于低纬度的银盘IV象限，因此它们沉浸在具有内部银河系特征的密集场中。