Updated parameters of 1743 open clusters based on <i>Gaia</i> DR2

Dias, W. S.; Monteiro, H.; Moitinho, A.; Lépine, J. R. D.; Carraro, G.; Paunzen, E.; Alessi, B. S.; Villela, L.

doi:10.1093/mnras/stab770

Cited by 173 publications

(269 citation statements)

References 52 publications

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“…The present version of the catalog contains 1,750 clusters, which is the first update of the New Catalog of Optically Visible Open Clusters and Candidates (DAML) (Dias et al, 2002) in the Gaia era (see all details in Dias et al, 2021). The distribution of clusters in the Galactic disk is shown in Figure 1, with color proportional to the age, clearly indicating the arms in the solar neighborhood.…”

Section: The Sample Of Open Clustersmentioning

confidence: 99%

The Distribution of Open Clusters in the Galaxy

Monteiro

Barros²,

Dias

et al. 2021

Front. Astron. Space Sci.

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In this work we explore the new catalog of galactic open clusters that became available recently, containing 1,750 clusters that have been re-analyzed using the Gaia DR2 catalog to determine the stellar memberships. We used the young open clusters as tracers of spiral arms and determined the spiral pattern rotation speed of the Galaxy and the corotation radius, the strongest Galactic resonance. The sample of open clusters used here is increased by dozens of objects with respect to our previous works. In addition, the distances and ages values are better determined, using improvements to isochrone fitting and including an updated extinction polynomial for the Gaia DR2 photometric band-passes, and the Galactic abundance gradient as a prior for metallicity. In addition to the better age determinations, the catalog contains better positions in the Galactic plane and better proper motions. This allow us to discuss not only the present space distribution of the clusters, but also the space distribution of the clusters's birthplaces, obtained by integration of the orbits for a time equal to their age. The value of the rotation velocity of the arms (28.5 ± 1.0 km s−1 kpc−1) implies that the corotation radius (Rc) is close to the solar Galactic orbit (Rc/R0 = 1.01±0.08), which is supported by other observational evidence discussed in this text. A simulation is presented, illustrating the motion of the clusters in the reference frame of corotation. We also present general statistics of the catalog of clusters, like spatial distribution, distribution relative to height from the Galactic plane, and distribution of ages and metallicity. An important feature of the space distribution, the corotation gap in the gas distribution and its consequences for the young clusters, is discussed.

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Section: The Sample Of Open Clustersmentioning

confidence: 99%

The Distribution of Open Clusters in the Galaxy

Monteiro

Barros²,

Dias

et al. 2021

Front. Astron. Space Sci.

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“…Many of them have determined mean proper motions and membership probabilities (Sampedro et al, 2017;Dias et al, 2018). Since the publication of Gaia DR2 (Brown et al, 2018), on the one hand, the parameters of known OCs have been updated (Cantat-Gaudin et al, 2018;Soubiran et al, 2018;Bossini et al, 2019;Monteiro and Dias, 2019;Dias et al, 2021;Tarricq et al, 2021). On the other hand, a large number of new OCs and candidates have been identified (e.g., see Castro-Ginard et al, 2018;Cantat-Gaudin et al, 2019;Castro-Ginard et al, 2019;Sim et al, 2019;Liu and Pang, 2019;Hao et al, 2020;Castro-Ginard et al, 2020;Ferreira et al, 2020;He et al, 2021a;Hunt and Reffert, 2021;Ferreira et al, 2021).…”

Section: Young Open Clustersmentioning

confidence: 99%

“…In the past few years, there has been significant progress in observations by taking advantage of the VLBI observations in the radio band (Reid et al, 2019;Hirota et al, 2020) and Gaia astrometry measurements in the optical band (Prusti et al, 2016). Accurate parallaxes and proper motions have been obtained for a large number of HMSFR masers (e.g., Reid et al, 2019), HII regions (e.g., , O-type stars (e.g., Xu et al, 2021), young open clusters (OCs, e.g., Dias et al, 2021), and evolved stars (e.g., Khoperskov et al, 2020). Additionally, many giant molecular clouds (GMCs) have had accurately determined distances based on the multi-wavelength survey data from optical to infrared bands or the astrometric data of foreground/background stars (Yan et al, 2019;Chen et al, 2020).…”

Section: Introductionmentioning

confidence: 99%

The Spiral Structure in the Solar Neighborhood

Hou

2021

Front. Astron. Space Sci.

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The spiral structure in the solar neighborhood is an important issue in astronomy. In the past few years, there has been significant progress in observation. The distances for a large number of good spiral tracers, i.e., giant molecular clouds, high-mass star-formation region masers, HII regions, O-type stars, and young open clusters, have been accurately estimated, making it possible to depict the detailed properties of nearby spiral arms. In this work, we first give an overview about the research status for the Galaxy’s spiral structure based on different types of tracers. Then the objects with distance uncertainties better than 15% and <0.5 kpc are collected and combined together to depict the spiral structure in the solar neighborhood. Five segments related with the Perseus, Local, Sagittarius-Carina, Scutum-Centaurus, and Norma arms are traced. With the large dataset, the parameters of the nearby arm segments are fitted and updated. Besides the dominant spiral arms, some substructures probably related to arm spurs or feathers are also noticed and discussed.

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“…In panel b) of the same figure lines of the constant q values are overlapped on the Pleiades star distribution. To this aim, we employed the Pleiades fundamental parameters from the catalog of Dias et al (2021), namely, the distance 135 pc, logarithm of age 8.1, A V = 0.168, and a solar metallicity (Dias et al (2021) give [F e/H] = 0.032 ± 0.029) .…”

Section: The Binary Population Of the Pleiades Clustermentioning

confidence: 99%

Unresolved Binaries in the Intermediate Mass Range in the Pleiades Star Cluster

Malofeeva,

Seleznev,

Carraro

2022

Preprint

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The identification of binary stars of different mass ratios in resolved stellar populations is a challenging task. We show how the photometric diagram constructed with the pseudo-colors (H-W2)-W1 vs W2-(BP-K) can be employed to estimate the binary and multiple star ratios and the distribution of their component mass ratio q effectively. As an application, we investigate the Pleiades star cluster in the range of primary component mass between 0.5 and 1.8 M ⊙ . The binary star ratio is found to be between 0.54±0.11 and 0.70±0.14. On the other hand, the ratio of systems with multiplicity more than 2 is between 0.10±0.00 and 0.14±0.01. The distribution of the component mass ratio q has been approximated by a power law with the exponent between -0.53±0.10 and -0.63±0.22. Below 0.5 M ⊙ , we expect a large number of brown dwarfs among secondary components.

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Updated parameters of 1743 open clusters based on Gaia DR2

Cited by 173 publications

References 52 publications

The Distribution of Open Clusters in the Galaxy

The Distribution of Open Clusters in the Galaxy

The Spiral Structure in the Solar Neighborhood

Unresolved Binaries in the Intermediate Mass Range in the Pleiades Star Cluster

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