Revisiting the Fundamental Parameters of 49 New Star Clusters in Gaia DR2

Li, Zhongmu; Deng, Yangyang; Chen, Jing

doi:10.3847/1538-4365/abeb68

Cited by 15 publications

(8 citation statements)

References 43 publications

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“…The Powerful CMD code (Li et al 2017) is applied to fitting the CMDs of SCs (similar to Li et al 2021). Because the Powerful CMD code does not include the magnitudes of the Gaia observation, we transform the G BP and G RP magnitudes to V and I magnitudes, via the transformation functions of Riello et al (2021), which is somewhat different from Jordi et al (2010).…”

Section: Fundamental Parameters Of Fof Ocsmentioning

confidence: 99%

LISC Catalog of Star Clusters. II. High Galactic Latitude Open Clusters in Gaia EDR3

Mao

2023

ApJS

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It is well known that there are few open clusters (OCs) in the high-latitude region of the Milky Way galaxy, because most star formation takes place in the thin disk. It is therefore crucial to look for high Galactic latitude OCs, in order to understand OCs and the Galactic parts outside the plane well. This work looks for high Galactic latitude OCs in Gaia Early Data Release 3, and determines their basic parameters from color–magnitude diagrams (CMDs) if the main sequence is included in CMDs. The friend-of-friend method is applied to the determination of the membership of stars. Star groups with more than 20 bright (G < 18 mag) stars are taken as OC candidates, and these candidates are finally verified by the observed CMDs including stars fainter than 18 mag in the G band. After crossmatching with previous catalogs, 56 new OC candidates are found in the high Galactic latitude region with ∣b∣ ≥ 25°, in which 35 have somewhat clear CMDs and are suggested as newly discovered OCs. Finally, eight of the new OCs are confirmed again by the pyUPMASK technique. The new sample increases the total number of known high Galactic latitude OC candidates significantly. The distance modulus, color excess, metallicity, age, and binary fraction of 35 newly discovered OCs are determined by fitting their observed CMDs to the ASPS stellar population models. All the results are included in the new star cluster catalog, LISC, as its second part (LISC II).

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Section: Fundamental Parameters Of Fof Ocsmentioning

confidence: 99%

LISC Catalog of Star Clusters. II. High Galactic Latitude Open Clusters in Gaia EDR3

Mao

2023

ApJS

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“…Although the main parameters of clusters have been estimated by the above isochrone fitting method, the accuracy of these parameters needs to be improved. Since most of the observed CMDs display multiple MSs, blue stragglers, and extended MS turnoffs, the theoretical isochrones that Similar to our previous works, e.g., Li et al (2021), Li et al (2022a), Chen et al (2022), andLi et al (2022b), we build the synthetic CMDs based on V versus (V − I) CMD using some transformation functions provided by Jordi et al (2010). Considering the quality caused by the conversion, a residual…”

Section: Properties Of Clustersmentioning

confidence: 99%

“…Open clusters (OCs) are one of the most important sources to survey Galactic populations, and many Galactic OC catalogs are publicly available, such as the WEBDE database (Mermilliod 1995), DAML02 (Dias et al 2002), MWSC (Kharchenko et al 2013), CG18 (Cantat-Gaudin et al 2018), CG19 (Castro-Ginard et al 2019), B19 (Bica et al 2019), Liu & Pang (2019) catalog (LP hereafter), CG20 (Cantat-Gaudin & Anders 2020), and LISC (Li et al 2021;Li et al 2022a;Li et al 2022b). As the precision of data and efficiency of algorithms continue to improve, some of known clusters have a chance to be revisited, and the number of identified and denied star clusters is increasing.…”

Section: Introductionmentioning

confidence: 99%

Revisit of 77 Clusters Candidates with Multiple Main Sequences using Gaia DR3

Chen,

Li,

Zhang

et al. 2024

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Gaia DR3 data provide the latest and full astrometric data for more than 1.5 billion sources, and these allow us to revisit the 77 special open cluster candidates collected from LISC star cluster catalog. According to their unclear color–magnitude-diagram (CMD) morphology, they are difficult to be ensured as real open clusters (OCs), and their cluster properties are still poorly known. We perform a cluster census by reidentification for these clusters using pyUPMASK based on the photometric and astrometric stellar information. We have redetected these 77 objects and they should be real OCs, of which five clusters are potential binary clusters. Their basic parameters are obtained by fitting isochrones to observed CMDs. Our results show that their CMDs display more clean main sequences (MSs) and less member stars lying on the right of lower MSs relative to most of clusters in our initial sample, but broad MSs have not changed significantly. We suggest that efficient clustering algorithm combined with precision data can only partly reduce some stars lying on the right of lower MSs, and a simple stellar population of binary and rotating stars can partly reproduce multiple MS phenomena, including split and broad MSs.

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“…The Platais 8 open cluster was discovered by Platais et al (1998) and has received relatively little attention since. It was included in the sample of Yen et al (2018), but not those of Meingast et al (2020) and Li et al (2021). Theia 92 seems to include the core of Platais 8 and a possible trailing tidal tail behind this core (see Figure 3b).…”

Section: The Platais 8 Systemmentioning

confidence: 99%

A Number of Nearby Moving Groups may be Fragments of Dissolving Open Clusters

Gagné,

Faherty,

Moranta

et al. 2021

Preprint

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We propose that fourteen co-moving groups of stars uncovered by Kounkel & Covey (2019) may be related to known nearby moving groups and bridge those and nearby open clusters with similar ages and space velocities. This indicates that known nearby moving groups may be spatially much more extended than previously though, and some of them might be parts of tidal tails around the cores of known open clusters, reminiscent of those recently found around the Hyades and a handful of other nearby clusters. For example, we find that both the nearby Carina and Columba associations may be linked to Theia 208 from Kounkel & Covey ( 2019) and together form parts of a large tidal tail around the Platais 8 open cluster. The AB Doradus moving group and Theia 301 may form a trailing tidal tail behind the Pleiades open cluster, with hints of a possible leading tidal tail in Theia 369. We similarly find that IC 2391 and its tidal tails identified by Meingast et al. ( 2020) may be extended by the nearby Argus association and are possibly further extended by Theia 115. The nearby Octans and Octans-Near associations, as well as Theia 94 and 95, may form a large tidal tail leading the poorly studied Platais 5 open cluster candidate. While a preliminary analysis of Gaia color-magnitude sequences hint that these structures are plausibly related, more observational evidence is still required to corroborate their consistent ages and space velocities. These observations may change our current understanding of nearby moving groups and the different pathways through which they can form. While some moving groups may have formed loosely in extended star-formation events with rich spatial structure, others may in fact correspond to the tidal tails of nearby open clusters.

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Revisiting the Fundamental Parameters of 49 New Star Clusters in Gaia DR2

Cited by 15 publications

References 43 publications

LISC Catalog of Star Clusters. II. High Galactic Latitude Open Clusters in Gaia EDR3

LISC Catalog of Star Clusters. II. High Galactic Latitude Open Clusters in Gaia EDR3

Revisit of 77 Clusters Candidates with Multiple Main Sequences using Gaia DR3

A Number of Nearby Moving Groups may be Fragments of Dissolving Open Clusters

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