Occaso

Carrera, R.; Casamiquela, L.; Carbajo-Hijarrubia, J.; Balaguer-Núñez, L.; Jordi, C.; Romero-Gómez, M.; Blanco-Cuaresma, S.; Cantat-Gaudin, T.; Lillo-Box, J.; Masana, E.; Pancino, E.

doi:10.1051/0004-6361/202141832

Cited by 12 publications

(9 citation statements)

References 87 publications

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“…Several studies have combined Gaia astrometry with groundbased radial velocities with the purpose of studying the kinematics of the OC population (e.g. Soubiran et al 2018;Carrera et al 2022). Tarricq et al (2021) studied the 3D kinematics and age dependence of the OC population, also providing orbital parameters for 1382 OCs.…”

Section: Introductionmentioning

confidence: 99%

Hunting for open clusters inGaiaEDR3: 628 new open clusters found with OCfinder

Castro-Ginard

Jordi

Luri

et al. 2022

A&A

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Context. The improvements in the precision of the published data in Gaia EDR3 with respect to Gaia DR2, particularly for parallaxes and proper motions, offer the opportunity to increase the number of known open clusters in the Milky Way by detecting farther and fainter objects that have thus far gone unnoticed. Aims. Our aim is to continue to complete the open cluster census in the Milky Way with the detection of new stellar groups in the Galactic disc. We use Gaia EDR3 up to magnitude G = 18 mag, increasing the magnitude limit and therefore the search volume explored in one unit with respect to our previous studies. Methods. We used the OCfinder method to search for new open clusters in Gaia EDR3 using a big data environment. As a first step, OCfinder identified stellar statistical overdensities in five-dimensional astrometric space (position, parallax, and proper motions) using the DBSCAN clustering algorithm. Then, these overdensities were classified into random statistical overdensities or real physical open clusters using a deep artificial neural network trained on well-characterised G, GBP – GRP colour-magnitude diagrams. Results. We report the discovery of 628 new open clusters within the Galactic disc, with most of them being located beyond 1 kpc from the Sun. From the estimation of ages, distances, and line-of-sight extinctions of these open clusters, we see that young clusters align following the Galactic spiral arms while older ones are dispersed in the Galactic disc. Furthermore, we find that most open clusters are located at low Galactic altitudes with the exception of a few groups older than 1 Gyr. Conclusions. We show the success of the OCfinder method leading to the discovery of a total of 1274 open clusters (joining the discoveries here with the previous ones based on Gaia DR2), which represents almost 50% of the known population. Our ability to perform big data searches on a large volume of the Galactic disc, together with the higher precision in Gaia EDR3, enable us to keep completing the census with the discovery of new open clusters.

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Section: Introductionmentioning

confidence: 99%

Hunting for open clusters inGaiaEDR3: 628 new open clusters found with OCfinder

Castro-Ginard

Jordi

Luri

et al. 2022

A&A

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“…Then, we proceeded with the combination, normalisation, and merge of the different orders. All the steps were performed with the tools developed in the framework of the OCCASO 3 survey and described in detail by Carrera et al (2022).…”

Section: Target Selection Observations and Data Reductionmentioning

confidence: 99%

“…Radial velocities, v rad , were measured as in Carrera et al (2022). Briefly, the radial velocities of the 1D combined spectra were obtained by measuring the Doppler shifts of the spectral lines using the classical cross-correlation method (e.g Tonry & Davis 1979).…”

Section: Radial Velocitiesmentioning

confidence: 99%

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One Star to Tag Them All (OSTTA)

Carrera

Casamiquela

Bragaglia³

et al. 2022

A&A

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Context. Open clusters are ideal laboratories to investigate a variety of astrophysical topics, from the properties of the Galactic disc to stellar evolution models. For this purpose, we need to know their chemical composition in detail. Unfortunately, the number of systems with chemical abundances determined from high resolution spectroscopy remains small. Aims. Our aim is to increase the number of open clusters with radial velocities and chemical abundances determined from high resolution spectroscopy by sampling a few stars in clusters which had not been previously studied. Methods. We obtained high resolution spectra with the FIbre-fed Echelle Spectrograph at Nordic Optical Telescope for 41 stars belonging to 20 open clusters. These stars have high astrometric membership probabilities determined from the Gaia second data release. Results. We derived radial velocites for all the observed stars which were used to confirm their membership to the corresponding clusters. For Gulliver 37, we cannot be sure the observed star is a real member. We derived atmospheric parameters for the 32 stars considered to be real cluster members. We discarded five stars because they have very low gravity or their atmospheric parameters were not properly constrained due to low signal-to-noise ratio spectra. Therefore, detailed chemical abundances were determined for 28 stars belonging to 17 clusters. For most of them, this is the first chemical analysis available in the literature. Finally, we compared the clusters in our sample to a large population of well-studied clusters. The studied systems follow the trends, both chemical and kinematical, described by the majority of open clusters. It is worth mentioning that the three most metal-poor studied clusters (NGC 1027, NGC 1750, and Trumpler 2) are enhanced in Si, but not in the other α-elements studied (Mg, Ca, and Ti).

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Section: Radial Velocitiesmentioning

confidence: 99%

One Star to Tag Them All (OSTTA): I. Radial velocities and chemical abundances for 20 poorly studied open clusters

Carrera,

Casamiquela,

Bragaglia

et al. 2022

Preprint

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Context. Open clusters are ideal laboratories to investigate a variety of astrophysical topics, from the properties of the Galactic disc to stellar evolution models. For this purpose, we need to know their chemical composition in detail. Unfortunately, the number of systems with chemical abundances determined from high resolution spectroscopy remains small. Aims. Our aim is to increase the number of open clusters with radial velocities and chemical abundances determined from high resolution spectroscopy by sampling a few stars in clusters which had not been previously studied. Methods. We obtained high resolution spectra with the FIbre-fed Echelle Spectrograph (FIES) at Nordic Optical Telescope (NOT) for 41 stars belonging to 20 open clusters. These stars have high astrometric membership probabilities determined from the Gaia second data release. Results. We derived radial velocites for all the observed stars which were used to confirm their membership to the corresponding clusters. For Gulliver 37, we cannot be sure the observed star is a real member. We derived atmospheric parameters for the 32 stars considered to be real cluster members. We discarded five stars because they have very low gravity or their atmospheric parameters were not properly constrained due to low signal-to-noise ratio spectra. Therefore, detailed chemical abundances were determined for 28 stars belonging to 17 clusters. For most of them, this is the first chemical analysis available in the literature. Finally, we compared the clusters in our sample to a large population of well-studied clusters. The studied systems follow the trends, both chemical and kinematical, described by the majority of open clusters. It is worth mentioning that the three most metal-poor studied clusters (NGC 1027, NGC 1750, and Trumpler 2) are enhanced in Si, but not in the other α-elements studied (Mg, Ca, and Ti).

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Occaso

Cited by 12 publications

References 87 publications

Hunting for open clusters inGaiaEDR3: 628 new open clusters found with OCfinder

Hunting for open clusters inGaiaEDR3: 628 new open clusters found with OCfinder

One Star to Tag Them All (OSTTA)

One Star to Tag Them All (OSTTA): I. Radial velocities and chemical abundances for 20 poorly studied open clusters

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