Evidence of a dynamically evolving Galactic warp

Poggio, E.; Drimmel, R.; Andrae, R.; Bailer‐Jones, C. A. L.; Fouesneau, M.; Lattanzi, M. G.; Smart, R. L.; Spagna, A.

doi:10.1038/s41550-020-1017-3

Cited by 71 publications

(78 citation statements)

References 55 publications

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“…The quantity h z = 0.15 kpc is the disc scale height (cf. Poggio et al 2020), and L = 3.5 kpc is the best fit scalelength of the young (<1 Gyr) disc, where we have used the model presented in Frankel et al (2018) with the data and method in Frankel et al (2019).…”

Section: B2 Structural Modelmentioning

confidence: 99%

Mapping luminous hot stars in the Galaxy

Zari

Rix

Frankel

et al. 2021

A&A

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Luminous hot stars (MKs ≲ 0 mag and Teff ≳ 8000 K) dominate the stellar energy input to the interstellar medium throughout cosmological time, are used as laboratories to test theories of stellar evolution and multiplicity, and serve as luminous tracers of star formation in the Milky Way and other galaxies. Massive stars occupy well-defined loci in colour–colour and colour–magnitude spaces, enabling selection based on the combination of Gaia EDR3 astrometry and photometry and 2MASS photometry, even in the presence of substantive dust extinction. In this paper we devise an all-sky sample of such luminous OBA-type stars, which was designed to be complete rather than very pure, providing targets for spectroscopic follow-up with the SDSS-V survey. To estimate the purity and completeness of our catalogue, we derive stellar parameters for the stars in common with LAMOST DR6 and we compare the sample to other O and B-type star catalogues. We estimate ‘astro-kinematic’ distances by combining parallaxes and proper motions with a model for the expected velocity and density distribution of young stars; we show that this adds useful constraints on the distances and therefore luminosities of the stars. With these distances we map the spatial distribution of a more stringently selected subsample across the Galactic disc, and find it to be highly structured, with distinct over- and under-densities. The most evident over-densities can be associated with the presumed spiral arms of the Milky Way, in particular the Sagittarius-Carina and Scutum-Centaurus arms. Yet, the spatial picture of the Milky Way’s young disc structure emerging in this study is complex, and suggests that most young stars in our Galaxy (tage < tdyn) are not neatly organised into distinct spiral arms. The combination of the comprehensive spectroscopy to come from SDSS-V (yielding velocities, ages, etc.) with future Gaia data releases will be crucial in order to reveal the dynamical nature of the spiral arms themselves.

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Section: B2 Structural Modelmentioning

confidence: 99%

Mapping luminous hot stars in the Galaxy

Zari

Rix

Frankel

et al. 2021

A&A

Self Cite

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“…Meanwhile, the kinematical and height signal of the warp and gas infall origins are also unraveled in Wang et al (2020d). Some other works about warp signals with different tracers and methods could also be found in Poggio et al (2018Poggio et al ( , 2020.…”

Section: The Mid-plane Displacements Of the Diskmentioning

confidence: 99%

The Flare and Warp of the Young Stellar Disk traced with LAMOST DR5 OB-type stars

Yu,

Wang,

Cui

et al. 2021

Preprint

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We present analysis of the spatial density structure for the outer disk from 8−14 kpc with the LAMOST DR5 13534 OB-type stars. We discover the clear and similar flaring signatures beyond 8 kpc for which the scale height is from 0.14 to 0.5 kpc in the north and south side, implying that the flaring is possibly symmetrical in the Milky Way disk. We reveal that the thickness of the OB stellar disk is similar with our previous thin disk traced by red giant branch stars, possibly implying that secular evolution is not the main contributor to the flaring but other scenarios such as interactions with passing dwarf galaxies should be more possible. When comparing the OB stellar disk with the gas disk, the former one is moderately thicker than the later one, meaning that one could tentatively use young OB-type stars to trace the gas properties. Meanwhile, we unravel that the scale length of the young OB stellar disk is 1.17 ± 0.05 kpc, which is shorter than gas disk, comfirming that the gas disk is more extended than stellar disk. What is more, by considering the mid-plane displacements (Z 0 ) in our density model we find that almost all are within 100 pc with the increasing trend as Galactocentric distance increases, which looks like the warp signal in young stellar population but the scenarios will need to be investigated in more detail.

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“…The quantity h z = 0.15 kpc is the disc scale height (cfr. Poggio et al 2020), and L = 3.5 kpc is the best fit scale-length of the young (< 1Gyr) disk, where we have used the model presented in Frankel et al (2018) with the data and method in Frankel et al (2019).…”

Section: Appendix B1: Kinematic Modelmentioning

confidence: 99%

Mapping Luminous Hot Stars in the Galaxy

Zari,

Rix,

Frankel

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

Luminous hot stars (M Ks 0 mag and T eff 8000 K) dominate the stellar energy input to the interstellar medium (ISM) throughout cosmological time, they are laboratories to test theories of stellar evolution and multiplicity, and they serve as luminous tracers of star formation in the Milky Way and other galaxies. Massive stars occupy well-defined loci in colour-colour and colour-magnitude spaces, enabling selection based on the combination of Gaia EDR3 astrometry and photometry and 2MASS photometry, even in the presence of substantive dust extinction. In this paper we devise an all-sky sample of such luminous OBA-type stars, designed to be quite complete rather than very pure, to serve as targets for spectroscopic follow-up with the SDSS-V survey. To estimate the purity and completeness of our catalogue, we derive stellar parameters for the stars in common with LAMOST DR6 and we compare the sample to other O and B-type star catalogues. We estimate "astro-kinematic" distances by combining parallaxes and proper motions with a model for the expected velocity and density distribution of young stars; we show that this adds useful contraints on the stars' distances, and hence luminosities. With these distances we map the spatial distribution of a more stringently selected sub-sample across the Galactic disk, and find it to be highly structured, with distinct over-and under-densities. The most evident over-densities can be associated with the presumed spiral arms of the Milky Way, in particular the Sagittarius-Carina and Scutum-Centaurus arms. Yet, the spatial picture of the Milky Way's young disc structure emerging in this study is complex, and suggests that most young stars in our Galaxy (t age < t dyn ) are not neatly organised into distinct spiral arms. The combination of the comprehensive spectroscopy to come from SDSS-V (yielding velocities, ages, etc..) with future Gaia data releases will be crucial to reveal the dynamical nature of the spiral arm themselves.

show abstract

Evidence of a dynamically evolving Galactic warp

Cited by 71 publications

References 55 publications

Mapping luminous hot stars in the Galaxy

Mapping luminous hot stars in the Galaxy

The Flare and Warp of the Young Stellar Disk traced with LAMOST DR5 OB-type stars

Mapping Luminous Hot Stars in the Galaxy

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