The μ Tau Association: A 60 Myr Old Coeval Group at 150 pc from the Sun

Gagné, Jonathan; Mamajek, Eric E.; Mann, Andrew W.; Faherty, Jacqueline K.; Bédard, Antoine

doi:10.3847/1538-4357/abb77e

Cited by 39 publications

(49 citation statements)

References 146 publications

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“…A larger dataset on similarly young stars (Figure 8b) provides n = 1, within uncertainty. A long period for one star in µ Tau [32] tightly constrains n. The contrasting case of the Solar Neighborhood, which was culled to fast rotators with Π < 4 days [33], provides a reasonable fit due to the large number of points (481). This culling removes the old, slow stars and apparently reduces the effect of episodic production.…”

Section: Associations and The Solar Neighborhoodmentioning

confidence: 98%

“…Ground-based measurements differ from the remotely probed clusters and associations, where the curvature is controlled by the intermediate values, since bins for slow and fast rotators are underpopulated. [31]; (b) A wide range of masses in the µ Tau association, which includes a B2 star and pre-main sequence stars [32]. Arrow points to the slow rotator; (c) Fast rotators in the Solar Neighborhood [33].…”

Section: Ground-based Measurements and A Comparison To Kepler Missionsmentioning

confidence: 99%

“…Panels are ordered by increasing sample size. Symbols as in Figure 5: (a) Pre-main sequence stars of the Scorpious-Centaurus OB association from[31]; (b) A wide range of masses in the µ Tau association, which includes a B2 star and pre-main sequence stars[32]. Arrow points to the slow rotator; (c) Fast rotators in the Solar Neighborhood[33].…”

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confidence: 99%

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Quantification of Sub-Solar Star Ages from the Symmetry of Conjugate Histograms of Spin Period and Angular Velocity

Criss

Hofmeister

2021

Symmetry

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Empirical laws proposed for the decline in star spin with time have heretofore been tested using ambiguous fitting models. We develop an analytical inverse model that uses histogram data to unequivocally determine the physical law governing how dwarf star spin depends on time (t) and mass (M). We analyze shapes of paired histograms of axial rotation period (П) and angular velocity (ω = 2π/П) to utilize the fact that a variable and its reciprocal are governed by the same physics. Copious data on open clusters are used to test the formula ∂ω/∂t ∝ − ωn where n is unrestricted, and thus covers diverse possibilities. Histogram conjugates for each of 15 clusters with 120 to 812 measurements provide n = 1.13 ± 0.19. Results are independent of initial spin rate, bin size, cluster parameters, and star mass. Notably, 11 large clusters with mostly M-types yield fits with n = 1.07 ± 0.12. Associations behave similarly. Only exponential decay (n = 1) explains the similar shapes of the conjugate histograms for the spin period and angular velocity, despite the asymmetric (inverse) relationship of these variables. This rate law is consistent with viscous dissipation. Forward modeling confirms that n is near unity and further shows that coeval formation of all stars in a cluster does not occur. We therefore explore a constant rate of star production, which is reasonable for tiny stars. Inverse models show that episodic production increases with mass, but is unimportant below ~0.55 MSun. We infer star and cluster ages, and find that star production becomes less regular with time, as interstellar gas and dust are progressively depleted. Our new analytical approach of extracting a physical law from conjugate histograms is general and widely applicable.

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Section: Associations and The Solar Neighborhoodmentioning

confidence: 98%

Section: Ground-based Measurements and A Comparison To Kepler Missionsmentioning

confidence: 99%

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Quantification of Sub-Solar Star Ages from the Symmetry of Conjugate Histograms of Spin Period and Angular Velocity

Criss

Hofmeister

2021

Symmetry

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“…The stars in the solar vicinity represent a rich and diverse population dominated by, on average, low-mass stars of several gi-gayears in age (e.g., Binney et al 2000;Hinkel et al 2017), but also interspersed, at least at distances up to ∼150 pc, with dynamically distinct groups of young stars (e.g., Gagné et al 2018;Binks et al 2020;Gagné et al 2020). Their proximity allows precise distance determinations and a detailed understanding of their astrophysical properties without great concern for extinction and reddening.…”

Section: Luminosity Function In the Solar Neighborhoodmentioning

confidence: 99%

Fine structure in the luminosity function in young stellar populations with Gaia DR2

Guo

Koter

Kaper

et al. 2021

A&A

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Context. A pioneering study showed that the fine structure in the luminosity function (LF) of young star clusters contains information about the evolutionary stage (age) and composition of the stellar population. The notable features include the H-peak, which is the result of the onset of hydrogen burning turning pre-main sequence stars into main sequence stars. The feature moves toward the faint end of the LF, and eventually disappears as the population evolves. Another detectable feature is the Wielen dip, a dip at MV ≃ 7 mag in the LF first identified in 1974 for stars in the solar environment. Later studies also identified this feature in the LF of star clusters. The Wielen dip is caused by the increased importance of H− opacity in a certain range of low-mass stars. Aims. We studied the detailed structure in the luminosity function using the data from Gaia DR2 and PARSEC stellar evolution models with the aim to further our understanding of young stellar populations. Methods. We analyzed the astrometric properties of stars in the solar neighborhood (< 20 pc) and in various relatively nearby (< 400 pc) young (< 50 Myr) open clusters and OB associations, and compare the features in the luminosity function with those generated by PARSEC models. Results. The Wielen dip is confirmed in the LF of all the populations, including the solar neighborhood, at MG ≃ 7 mag. The H-peak is present in the LF of the field stars in the solar neighborhood. It likely signals that the population is mixed with a significant number of stars younger than 100 Myr. The H-peak is found in the LF of young open clusters and OB associations, and its location varies with age. The PARSEC evolutionary models predict that the H-peak moves from ∼ − 1 mag towards ∼ + 6 mag in MG for populations with ages increasing from 1 to ∼70 Myr. Our observations with Gaia DR2 confirm the evolution of the H-peak from ∼5 Myr up to ∼47 Myr. We provide a calibration function between MG and age that works in the age domain between 1 and 30 Myr. Conclusions. The fine structure in the luminosity function in young stellar populations can be used to estimate their age.

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“…We took as the basis for our cluster sample the x-y maps from Meingast et al (2021) (their figure A.2). In addition to these structures, which still surround gravitationally bound clusters, we include two tidal streams into our sample: the Psc-Eri stream from Meingast et al (2019) with an age determination of Curtis et al (2019), and the µ Tauri association from Gagné et al (2020). 4) as illustrated in the top panel of Fig.…”

Section: Age Determinationmentioning

confidence: 99%

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

Dinnbier,

Kroupa,

Šubr

et al. 2021

Preprint

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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 • .

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The μ Tau Association: A 60 Myr Old Coeval Group at 150 pc from the Sun

Cited by 39 publications

References 146 publications

Quantification of Sub-Solar Star Ages from the Symmetry of Conjugate Histograms of Spin Period and Angular Velocity

Quantification of Sub-Solar Star Ages from the Symmetry of Conjugate Histograms of Spin Period and Angular Velocity

Fine structure in the luminosity function in young stellar populations with Gaia DR2

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

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