A revisit to agglomerates of early-type Hipparcos stars

TL;DR

This study uses clustering algorithms to analyze the spatial distribution of early-type Hipparcos stars, identifying known and new stellar agglomerates, and providing detailed characterization of their properties and sub-structures.

Contribution

It introduces a systematic clustering approach to identify and analyze stellar agglomerates, including the discovery of a new young open cluster, P Puppis, and detailed sub-structure analysis of OB complexes.

Findings

Identified 35 stellar agglomerates, including known and new clusters.

Discovered P Puppis as a new nearby young open cluster.

Confirmed or found new sub-structures within OB complexes.

Abstract

We study the spatial structure and sub-structure of regions rich in Hipparcos stars with blue B_T-V_T colours. These regions, which comprise large stellar complexes, OB associations, and young open clusters, are tracers of on-going star formation in the Galaxy. The DBSCAN (Density-Based Spatial Clustering of Applications with Noise) data clustering algorithm is used to look for spatial overdensities of early-type stars. Once an overdensity, "agglomerate", is identified, we carry out a data and bibliographic compilation of their star member candidates. The actual membership in agglomerate of each early-type star is studied based on its heliocentric distance, proper motion, and previous spectro-photometric information. We identify 35 agglomerates of early-type Hipparcos stars. Most of them are associated to previously known clusters and OB associations. The previously unknown P Puppis agglomerate is subject of a dedicated study with Virtual Observatory tools. It is actually a new, nearby, young open cluster (d ~ 470 pc, age ~ 20 Ma) with a clear radial density gradient. We list P Puppis and other six agglomerates (including NGC 2451 A, vdBH 23, and Trumpler 10) as new sites for substellar searches because of their youth, closeness, and spatial density. We investigate in detail the sub-structure in the Orion, CMa-Pup and Pup-Vel OB complexes ("super-agglomerates"). We confirm or discover some stellar overdensities in the Orion complex, like the 25 Ori group, the Horsehead region (including the sigma Orionis cluster), and the eta Orionis agglomerate. Finally, we derive accurate parallactic distances to the Pleiades, NGC 2451 A, and IC 2391, describe several field early-type stars at d < 200 pc, and discuss the incompleteness of our search.