The <i>Gaia</i>-ESO survey: a lithium depletion boundary age for NGC 2232

Binks, A. S.; Jeffries, R. D.; Jackson, R. J.; Franciosini, E.; Sacco, G. G.; Bayo, A.; Magrini, L.; Randich, S.; Arancibia-Silva, J.; Bergemann, M.; Bragaglia, A.; Gilmore, G.; Gonneau, A.; Hourihane, A.; Jofré, P.; Korn, A.; Morbidelli, L.; Prisinzano, L.; Worley, C. C.; Zaggia, S.

doi:10.1093/mnras/stab1351

Cited by 22 publications

(22 citation statements)

References 74 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…It provides stellar parameters, metallicity, and elemental abundances, radial velocities, and additional products, such as gravity index, chromospheric activity tracers, mass accretion rate diagnostics, and veiling. Several works in recent years have been devoted to the study of open clusters observed by the GES, among many we recall the latest ones: Bertelli Motta et al [76], Magrini et al [77,78,79], Prisinzano et al [80], Hatzidimitriou et al [81], Casali et al [82,83], Baratella et al [84], Randich et al [85], Jackson et al [86], Bonito et al [87], Gutiérrez Albarrán et al [88], Semenova et al [89], Binks et al [90]. In the following sections, we adopt the average abundances from IDR6 for the member stars of 57 clusters with ages ≥ 120 Myr published in Magrini et al [79].…”

Section: Gaia-esomentioning

confidence: 99%

Mapping the Galactic Metallicity Gradient with Open Clusters: The State-of-the-Art and Future Challenges

2022

View full text Add to dashboard Cite

In this paper, we make use of data collected for open cluster members by high-resolution spectroscopic surveys and programmes (i.e., APOGEE, Gaia-ESO, GALAH, OCCASO, and SPA). These data have been homogenised and then analysed as a whole. The resulting catalogue contains [Fe/H] and orbital parameters for 251 Galactic open clusters. The slope of the radial metallicity gradient obtained through 175 open clusters with high-quality metallicity determinations is −0.064 ± 0.007 dex kpc−1. The radial metallicity distribution traced by open clusters flattens beyond RGal = 12.1 ± 1.1 kpc. The slope traced by open clusters in the [Fe/H]-Lz diagram is −0.31 ± 0.02 × 103 dex km−1 kpc−1 s, but it flattens beyond Lz = 2769 ± 177 km kpc s−1. In this paper, we also review some high-priority practical challenges around the study of open clusters that will significantly push our understanding beyond the state-of-the-art. Finally, we compare the shape of the galactic radial metallicity gradient to those of other spiral galaxies.

show abstract

Section: Gaia-esomentioning

confidence: 99%

Mapping the Galactic Metallicity Gradient with Open Clusters: The State-of-the-Art and Future Challenges

2022

View full text Add to dashboard Cite

show abstract

“…This uncertainty, which is of ≈ 10 to 20%, is comparable to the most accurate stellar evolutionary dating methods, i.e. isochrone fitting and lithium depletion boundary (Meynet et al 2009;Soderblom 2010;Jeffries et al 2013;Martín et al 2018;Binks et al 2021), but the morphological method is much easier to apply to a particular cluster or stream as it does not need stellar evolutionary models or dedicated spectroscopic observations. However, the role of possible systematic errors (e.g.…”

Section: Applications and Limitationsmentioning

confidence: 80%

“…In general, the lithium depletion boundary method provides older ages (by ≈ 50%) than isochrone fitting (e.g. Soderblom 2010;Binks et al 2021). The difference between these two dating methods is not restricted to the youngest clusters.…”

Section: Introductionmentioning

confidence: 99%

Estimating the ages of open star clusters from properties of their extended tidal tails

Dinnbier,

Kroupa,

Šubr

et al. 2021

Preprint

View full text Add to dashboard Cite

The most accurate current methods for determining the ages of open star clusters, stellar associations and stellar streams are based on isochrone fitting or the lithium depletion boundary. We propose another method for dating these objects based on the morphology of their extended tidal tails, which have been recently discovered around several open star clusters. Assuming that the early-appearing tidal tails, the so called tidal tails I, originate from the stars released from the cluster during early gas expulsion, or that they form in the same star forming region as the cluster (i.e. being coeval with the cluster), we derive the analytical formula for the tilt angle β between the long axis of the tidal tail and the orbital direction for clusters or streams on circular trajectories. Since at a given Galactocentric radius, β is only a function of age t regardless of the initial properties of the cluster, we estimate the cluster age by inverting the analytical formula β = β(t). We illustrate the method on a sample of 12 objects, which we compiled from the literature, and we find a reasonable agreement with previous dating methods in ≈ 70% of the cases. This can probably be improved by taking into account the eccentricity of the orbits and by revisiting the dating methods based on stellar evolution. The proposed morphological method is suitable for relatively young clusters (age 300 Myr), where it provides a relative age error of the order of 10 to 20% for an error in the observed tilt angle of 5 • .

show abstract

“…Improved surveys for multiplicity, observational constraints on the initial conditions of pre-ms contraction, and a deeper understand-ing of the role of magnetic fields, rotation, and star spots in pre-ms evolution are needed to obtain robust ages and star formation histories in clouds and clusters (e.g. Binks et al 2021;Serna et al 2021;Cao et al 2022).…”

Section: Discussionmentioning

confidence: 99%

Low Mass Stars as Tracers of Star and Cluster Formation

Megeath,

Gutermuth,

Kounkel

2022

Preprint

View full text Add to dashboard Cite

We review the use of young low mass stars and protostars, or young stellar objects (YSOs), as tracers of star formation. Observations of molecular clouds at visible, infrared, radio and X-ray wavelengths can identify and characterize the YSOs populating these clouds, with the ability to detect deeply embedded objects and all evolutionary stages. Surveys with the Spitzer, Herschel, XMM-Newton and Chandra space telescopes have measured the spatial distribution of YSOs within a number of nearby (< 2.5 kpc) molecular clouds, showing surface densities varying by more than three orders of magnitude. These surveys have been used to measure the spatially varying star formation rates and efficiencies within clouds, and when combined with maps of the molecular gas, have led to the discovery of star-forming relations within clouds. YSO surveys can also characterize the structures, ages, and star formation histories of embedded clusters, and they illuminate the relationship of the clusters to the networks of filaments, hubs and ridges in the molecular clouds from which they form. Measurements of the proper motions and radial velocities of YSOs trace the evolving kinematics of clusters from the deeply embedded phases through gas dispersal, providing insights into the factors that shape the formation of bound clusters. On 100 pc scales that encompass entire star-forming complexes, Gaia is mapping the young associations of stars that have dispersed their natal gas and exist alongside molecular clouds. These surveys reveal the complex structures and motions in associations, and show evidence for supernova driven expansions. Remnants of these associations have now been identified by Gaia, showing that traces of star-forming structures can persist for a few hundred million years.

show abstract

The Gaia-ESO survey: a lithium depletion boundary age for NGC 2232

Cited by 22 publications

References 74 publications

Mapping the Galactic Metallicity Gradient with Open Clusters: The State-of-the-Art and Future Challenges

Mapping the Galactic Metallicity Gradient with Open Clusters: The State-of-the-Art and Future Challenges

Estimating the ages of open star clusters from properties of their extended tidal tails

Low Mass Stars as Tracers of Star and Cluster Formation

Contact Info

Product

Resources

About