Planck Galactic Cold Clumps (PGCCs) are considered to be the ideal targets to probe the early phases of star formation. We have conducted a survey of 72 young dense cores inside PGCCs in the Orion complex with the Atacama Large Millimeter/submillimeter Array (ALMA) at 1.3 mm (band 6) using three different configurations (resolutions ∼0.″35, 1.″0, and 7.″0) to statistically investigate their evolutionary stages and substructures. We have obtained images of the 1.3 mm continuum and molecular line emission (¹²CO, and SiO) at an angular resolution of ∼0.″35 (∼140 au) with the combined arrays. We find 70 substructures within 48 detected dense cores with median dust mass ∼0.093 M _⊙ and deconvolved size ∼0.″27. Dense substructures are clearly detected within the central 1000 au of four candidate prestellar cores. The sizes and masses of the substructures in continuum emission are found to be significantly reduced with protostellar evolution from Class 0 to Class I. We also study the evolutionary change in the outflow characteristics through the course of protostellar mass accretion. A total of 37 sources exhibit CO outflows, and 20 (>50%) show high-velocity jets in SiO. The CO velocity extents (ΔVs) span from 4 to 110 km s⁻¹ with outflow cavity opening angle width at 400 au ranging from [Θ_obs]₄₀₀∼0.″6–3.″9, which corresponds to 33.4–125.7. For the majority of the outflow sources, the ΔVs show a positive correlation with [Θ_obs]₄₀₀, suggesting that as protostars undergo gravitational collapse, the cavity opening of a protostellar outflow widens and the protostars possibly generate more energetic outflows.

普朗克银河冷团块（PGCC）被认为是探测恒星形成早期阶段的理想目标。我们使用三种不同的配置（分辨率约为0.“ 35，1.” 0）对Orion复杂的PGCC内部的72个年轻致密核进行了调查，这些阿塔卡马大型毫米/亚毫米阵列（ALMA）的直径为1.3 mm（波段6）。和7.“ 0）进行统计研究其进化阶段和子结构。我们获得了1.3 mm连续谱和分子线发射（¹² CO和SiO）的图像，组合阵列的角度分辨率为〜0。''35（〜140 au）。我们发现在48 70子检测到与中位数的尘埃块~0.093致密内核中号 _⊙和反卷积大小约为0.“ 27。在四个候选星前核心的中心1000 au内清楚地检测到了密集的子结构。研究发现，随着从0级到I级的原恒星演化，连续发射中的子结构的大小和质量显着减小。我们还研究了通过原恒星质量积聚过程流出特征的演变变化。共有37个排放源显示出CO流出，而20个排放源（> 50％）显示有SiO高速射流。该CO速度程度（Δ V S）跨度从4至110公里S ^-1与流出腔的开口角度宽度为400 AU范围从[Θ _OBS ] ₄₀₀〜0。“6-3。”9，其对应于33.4- 125.7。对于大多数流出源，ΔVs与[ _Θobs ] ₄₀₀呈正相关，表明当原恒星经历重力塌陷时，原恒星流出的空腔开口变宽，原恒星可能产生更多的高能流出。