|
other query modes : |
Identifier query |
Coordinate query |
Criteria query |
Reference query |
Basic query |
Script submission |
TAP |
Output options |
Object types |
Help |
| Query : 2025A&A...693A.317Q |
2025A&A...693A.317Q - Astronomy and Astrophysics, volume 693A317 (2025/1-1)
Unveiling the binary nature of NGC 2323.
QIN S., ZHONG J., TANG T., JIANG Y., WANG L., WU K., ANDERS F., BALAGUER-NUNEZ L., LIU G., LI C., HOU J. and CHEN L.
Abstract (from CDS):
Context. As a well-known open cluster, NGC 2323 (also called M50) has been widely investigated for over a hundred years and has always been considered a classical single cluster.
Aims. We studied the binary structure nature of NGC 2323 with Gaia Data Release 3 (DR3).
Methods. We discovered the binary structure of NGC 2323 by the HDBSCAN algorithm based on the astrometric and photometric data from Gaia DR3. Then we employed the PETAR N-body code to investigate its binary structure origin.
Results. We found that NGC 2323 consists of two distinct subclusters (NGC 2323-a and NGC 2323-b) that are still gravitationally bound. They have very close positions (three-dimensional Δpos = 12.3 pc, σΔpos = 3.4 pc) and similar tangential velocities (two-dimensional ΔV = 2.2 km s–1, σΔV = 0.02 km s–1). The best isochrone fitting ages of the two clusters are the same (158 Myr), further proving their possibly common origin. The numerical N-body simulation suggests that the less massive cluster is unlikely to be the cluster tidal tails created by the differential rotation of the Milky Way.
Aims. We studied the binary structure nature of NGC 2323 with Gaia Data Release 3 (DR3).
Methods. We discovered the binary structure of NGC 2323 by the HDBSCAN algorithm based on the astrometric and photometric data from Gaia DR3. Then we employed the PETAR N-body code to investigate its binary structure origin.
Results. We found that NGC 2323 consists of two distinct subclusters (NGC 2323-a and NGC 2323-b) that are still gravitationally bound. They have very close positions (three-dimensional Δpos = 12.3 pc, σΔpos = 3.4 pc) and similar tangential velocities (two-dimensional ΔV = 2.2 km s–1, σΔV = 0.02 km s–1). The best isochrone fitting ages of the two clusters are the same (158 Myr), further proving their possibly common origin. The numerical N-body simulation suggests that the less massive cluster is unlikely to be the cluster tidal tails created by the differential rotation of the Milky Way.
Abstract Copyright: © The Authors 2025
Journal keyword(s): open clusters and associations: general - open clusters and associations: individual: NGC 2323
Simbad objects: 8
| Number of rows : 8 |
| N | Identifier | Otype |
ICRS (J2000) RA |
ICRS (J2000) DEC |
Mag U | Mag B | Mag V | Mag R | Mag I | Sp type |
#ref
1850 - 2026 |
#notes |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| 1 | NGC 752 | OpC | 01 56 53.7 | +37 45 06 | ~ | 712 | 0 | |||||
| 2 | NGC 869 | OpC | 02 18 57.0 | +57 08 02 | ~ | 504 | 0 | |||||
| 3 | NGC 884 | OpC | 02 22 15.7 | +57 08 59 | ~ | 503 | 0 | |||||
| 4 | NAME Magellanic Clouds | GrG | 03 00 | -71.0 | ~ | 7988 | 0 | |||||
| 5 | NGC 1193 | OpC | 03 05 56.4 | +44 22 58 | 12.6 | ~ | 97 | 0 | ||||
| 6 | NGC 2323 | OpC | 07 02 47.3 | -08 22 07 | ~ | 212 | 0 | |||||
| 7 | NAME Galactic Center | reg | 17 45 39.60213 | -29 00 22.0000 | ~ | 16269 | 0 | |||||
| 8 | IC 4665 | OpC | 17 46 04.0 | +05 36 54 | ~ | 407 | 0 |
To bookmark this query, right click on this link: simbad:objects in 2025A&A...693A.317Q and select 'bookmark this link' or equivalent in the popup menu