Stellar Kinematic Constraints on Galactic Structure Models Revisited: Bar and Spiral Arm Resonances

Antoja, T.; Valenzuela, O.; Pichardo, B.; Moreno, E.; Figueras, F.; Fernández, D.

doi:10.1088/0004-637x/700/2/l78

Cited by 114 publications

(132 citation statements)

References 38 publications

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“…The radial dispersion is not very strong in M 67, but distorts what would be a box orbit. Thus, a moderate spiral potential has important effects in the kinematics of orbits near the Galactic plane, as is the case in M 67, and in general, as is the case for the solar-neighborhood stars (Antoja et al 2009). This result holds for the allowed variations in proper motion, radial velocity and distance, because the most important parameter that affects the orbit is the mass of the spiral arms.…”

Section: The Galactic Orbit Of M 67mentioning

confidence: 93%

Absolute proper motion of the Galactic open cluster M 67

Bellini

Bedin

Pichardo

et al. 2010

A&A

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We derived the absolute proper motion (PM) of the old, solar-metallicity Galactic open cluster M 67 using observations collected with CFHT (1997) and with LBT (2007). About 50 galaxies with relatively sharp nuclei allow us to determine the absolute PM of the cluster. We find (μ α cos δ, μ δ ) J2000.0 = (−9.6 ± 1.1, −3.7 ± 0.8) mas yr −1 . By adopting a line-of-sight velocity of 33.78 ± 0.18 km s −1 , and assuming a distance of 815 ± 50 pc, we explore the influence of the Galactic potential, with and without the bar and/or spiral arms, on the galactic orbit of the cluster.

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Section: The Galactic Orbit Of M 67mentioning

confidence: 93%

Absolute proper motion of the Galactic open cluster M 67

Bellini

Bedin

Pichardo

et al. 2010

A&A

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“…One striking example is the HR 1614 stream (Eggen 1978;Feltzing & Holmberg 2000;De Silva et al 2007b). Stellar streams can also originate from dynamical effects within the discs that are due to resonances with the bars or spiral arms (Dehnen 2000;Antoja et al 2009). Analysis of high-resolution spectra of nearby F and G dwarf stars has revealed that the stars in the Hercules stream have a wide range of stellar ages, metallicities, and element abundances (Bensby et al 2007).…”

Section: Introductionmentioning

confidence: 99%

The nature of the KFR08 stellar stream

Liu

Feltzing

Ruchti

2015

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The origin of the new kinematically identified metal-poor stellar stream, the KFR08 stream, has not been established to date. We present stellar parameters, stellar ages, and detailed elemental abundances for Na, Mg, Al, Si, Ca, Sc, Ti, Cr, Ni, Zn, Sr, Y, Zr, Ba, La, and Eu for 16 KFR08 stream members based on an analysis of high-resolution spectra. Based on the abundance ratios of 14 elements, we use the chemical tagging method to identify the stars with the same chemical composition that therefore might have a common birthplace, such as a cluster. Although three stars were tagged with similar elemental abundances ratios, we find that, statistically, it is not certain that they originate from a dissolved star cluster. This conclusion is consistent with the large dispersion of [Fe/H] (σ [Fe/H] = 0.29) among the 16 stream members. We find that our stars are α enhanced and that the abundance patterns of the stream members match the thick-disc population well. In addition, most of the stream stars have estimated stellar ages greater than 11 Gyr. These results, together with the hot kinematics of the stream stars, suggest that the KFR08 stream originated from the thick-disc population, which was perturbed by a massive merger in the early Universe.

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“…Recent theoretical approaches (e.g., Quillen 2003;Quillen & Minchev 2005;Chakrabarty 2007;Minchev & Quillen 2007;Antoja et al 2009;Minchev & Famaey 2010;McMillan 2013) have been tested to identify the dominant mechanism that drives the evolution of the velocity distribution of the stars in the solar neighborhood. In their models, they investigated the cases of the resonances that would be caused by either the Galactic bar, the spiral structure, or both.…”

Section: Introductionmentioning

confidence: 99%

Reliable probabilistic determination of membership in stellar kinematic groups in the young disk

Klutsch

Ferrero

Guillout

et al. 2014

A&A

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Context. Over the last century, the overdensities in the velocity distributions of nearby stars were attributed to stellar kinematic groups or moving groups. Although their reality was initially questioned, their existence is now supported by a confluence of evidence. Aims. To pursue investigations, quantitative methods should be clearly defined to identify new stars belonging to these groups. Here, we present two probabilistic methods to determine the likelihood of kinematic membership for possible candidates in five of the known young stellar kinematic groups -namely, Pleiades, IC 2391, Castor, Ursa Major, and Hyades -in which all are younger than 650 Myr. Methods. We tried different methods to handle kinematic data of their known members. We succeeded in developing two independent procedures able to identify new candidates of these five stellar stream. We tested the robustness of our two approaches by means of extensive Monte Carlo simulations. Results. Our methods are consistent with one another in more than 90% of cases and for almost all the stellar kinematic groups under scrutiny. The IC 2391 supercluster is an exception. Applying our statistical methods to a large sample of young low-mass stars, we confirmed almost all the likely members and good candidates of these stellar streams. We also proposed 39 additional candidates based on the agreement and the high likelihood of age and kinematic membership. Conclusions. These probabilistic methods are very powerful to reliably identify new candidate members of young stellar kinematic groups. However, the kinematic criteria alone are not sufficient to distinguish between coeval stars that are evaporated from open clusters and other field stars trapped by dynamical processes generated by galactic perturbations. The identification of stars belonging to the remnant of a past star-forming event can be possible with the help of additional information, such as indicators of chromospheric activity, age proxies (lithium abundance), and chemical composition.

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Stellar Kinematic Constraints on Galactic Structure Models Revisited: Bar and Spiral Arm Resonances

Cited by 114 publications

References 38 publications

Absolute proper motion of the Galactic open cluster M 67

Absolute proper motion of the Galactic open cluster M 67

The nature of the KFR08 stellar stream

Reliable probabilistic determination of membership in stellar kinematic groups in the young disk

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