Abstract
The Radcliffe Wave is a 2.7-kpc long sinusoidal wave-like structure and it consists of many star forming regions in the Solar Neighbourhood. Most of these star forming clouds share similar motion in space. One exception is the Lacerta complex, a poorly studied region physically close to the Radcliffe Wave. Our goal was to analyse Lacerta’s young stellar population and find out why they bear this peculiar motion. Clustering Gaia data with HDBSCAN resulted in 9 groups containing a total of 1476 stars as cluster members. Additional radial velocities were used to determine the 3D motion of the groups. We find that unlike the rest of the Radcliffe Wave, the clusters of Lacerta are moving towards the Solar System, and possibly related to the Cepheus Spur. Relative 3D velocities show that Lacerta OB1 is expanding radially. We fitted isochrones to colour - absolute magnitude diagrams to determine the ages and masses of the cluster members. Apart from Lacerta OB1 and another group, all of the remaining clusters are too old to be considered young. These age estimations are consistent with that of other large cluster catalogues. We also studied the dust distribution and calculated masses of clouds located in the region.
Originalsprache | Englisch |
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Publikationsstatus | Veröffentlicht - 1 Juli 2024 |
ÖFOS 2012
- 103003 Astronomie
- 103004 Astrophysik