Mapping luminous hot stars in the Galaxy

Zari, E.; Rix, Hans─Walter; Frankel, Neige; Xiang, Maosheng; Poggio, E.; Drimmel, R.; Tkachenko, A.

doi:10.1051/0004-6361/202039726

Cited by 48 publications

(55 citation statements)

References 78 publications

(96 reference statements)

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“…In any case these two catalogues share sufficiently large overlap of OBA stars given their different selection criteria and purposes. Zari et al (2021) estimate their completeness level for O-and B-type stars to be around 86-90% from cross-matching with the catalogues by Liu et al (2019) and the Galactic O-Star Spectroscopic Survey (Sota et al 2014;Maíz Apellániz et al 2016).…”

Section: Discussionmentioning

confidence: 96%

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An all-sky sample of intermediate- to high-mass OBA-type eclipsing binaries observed by TESS

IJspeert

Tkachenko

Johnston

et al. 2021

A&A

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Context. Intermediate-to high-mass stars are the least numerous types of stars, and they are less well understood than their more numerous low-mass counterparts in terms of their internal physical processes. Modelling the photometric variability of a large sample of main-sequence intermediate-to high-mass stars in eclipsing binary systems will help to improve the models for such stars. Aims. Our goal is to compose a homogeneously compiled sample of main-sequence intermediate-to high-mass OBA-type dwarfs in eclipsing binary systems from TESS photometry. We search for binaries with and without pulsations and determine their approximate ephemerides. Methods. Our selection starts from a catalogue of dwarfs with colours corresponding to those of OBA-type dwarfs in the TESS Input Catalog. We develop a new automated method aimed at detecting eclipsing binaries in the presence of a strong pulsational and/or rotational signal relative to the eclipse depths and apply it to publicly available 30-minute cadence TESS light curves. Results. Using targets with TESS magnitudes below 15 and cuts in the 2MASS magnitude bands of J − H < 0.045 and J − K < 0.06 as the most stringent criteria, we arrive at a total of 189 981 intermediate-to high-mass candidates, 91193 of which have light curves from at least one of two data reduction pipelines. The eclipsing binary detection and subsequent manual check for false positives resulted in 3155 unique OBA-type eclipsing binary candidates. Conclusions. Our sample of eclipsing binary stars in the intermediate-to high-mass regime allows for future binary (and asteroseismic) modelling with the aim to better understand the internal physical processes in this hot part of the main sequence.

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Section: Discussionmentioning

confidence: 96%

“…In a recent work by Zari et al (2021) an OBA-type catalogue was produced using a Gaia magnitude cutoff of G < 16 for the purpose of mapping hot stars in the Galaxy. Their catalogue contains 988 202 entries with an estimated 45% of the stars hotter than A0.…”

Section: Discussionmentioning

confidence: 99%

An all-sky sample of intermediate- to high-mass OBA-type eclipsing binaries observed by TESS

IJspeert

Tkachenko

Johnston

et al. 2021

A&A

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“…-The 'Z21' UMS sample, which contains the stars in the 'filtered' sample from Zari et al (2021). Similarly to P18, Z21 selected their UMS initial sample by applying simple colour cuts combining Gaia DR3 and 2MASS photometry.…”

Section: Upper Main Sequence Starsmentioning

confidence: 99%

Galactic spiral structure revealed byGaiaEDR3

Poggio

Drimmel

Cantat-Gaudin

et al. 2021

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Using the astrometry and integrated photometry from the Gaia Early Data Release 3, we map the density variations in the distribution of young upper main sequence (UMS) stars, open clusters, and classical Cepheids in the Galactic disc within several kiloparsecs of the Sun. We derive maps of relative over- and under-dense regions for UMS stars in the Galactic disc using both bivariate kernel density estimators and wavelet transformations. The resulting overdensity maps exhibit large-scale arches that extend in a clumpy but coherent way over the entire sampled volume, indicating the location of the spiral arm segments in the vicinity of the Sun. Peaks in the UMS overdensity are well matched by the distribution of young and intrinsically bright open clusters. By applying a wavelet transformation to a sample of classical Cepheids, we find that their overdensities possibly extend the spiral arm segments on a larger scale (≃10 kpc from the Sun). While the resulting map based on the UMS sample is generally consistent with previous models of the Sagittarius-Carina spiral arm, the geometry of the arms in the III quadrant (galactic longitudes 180° < l < 270°) differs significantly from that suggested by many previous models. In particular, we find that our maps favour a larger pitch angle for the Perseus arm, and that the Local Arm extends into the III quadrant at least 4 kpc past the position of the Sun, giving it a total length of at least 8 kpc.

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“…Smaller boxes and circles indicate greater distances, and arrows indicate proper motions. amined the spatial distribution of previously identified OB stars, while Zari et al (2021) and Poggio et al (2021) have characterized a photometrically selected sample of upper-main-sequence stars.…”

Section: Introductionmentioning

confidence: 99%

A high pitch angle structure in the Sagittarius Arm

Kuhn

Benjamin

Zucker

et al. 2021

A&A

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Context. In spiral galaxies, star formation tends to trace features of the spiral pattern, including arms, spurs, feathers, and branches. However, in our own Milky Way, it has been challenging to connect individual star-forming regions to their larger Galactic environment owing to our perspective from within the disk. One feature in nearly all modern models of the Milky Way is the Sagittarius Arm, located inward of the Sun with a pitch angle of ∼12 • . Aims. We map the 3D locations and velocities of star-forming regions in a segment of the Sagittarius Arm using young stellar objects (YSOs) from the Spitzer/IRAC Candidate YSO (SPICY) catalog to compare their distribution to models of the arm. Methods. Distances and velocities for these objects are derived from Gaia EDR3 astrometry and molecular line surveys. We infer parallaxes and proper motions for spatially clustered groups of YSOs and estimate their radial velocities from the velocities of spatially associated molecular clouds. Results. We identify 25 star-forming regions in the Galactic longitude range ∼ 4. • 0-18. • 5 arranged in a narrow, ∼1 kpc long linear structure with a high pitch angle of ψ = 56 • and a high aspect ratio of ∼7:1. This structure includes massive star-forming regions such as M8, M16, M17, and M20. The motions in the structure are remarkably coherent, with velocities in the direction of Galactic rotation of |V ϕ | ≈ 240 ± 3 km s −1 (slightly higher than average) and slight drifts inward (V R ≈ −4.3 km s −1 ) and in the negative Z direction (V Z ≈ −2.9 km s −1 ). The rotational shear experienced by the structure is ∆Ω = 4.6 km s −1 kpc −1 . Conclusions. The observed 56 • pitch angle is remarkably high for a segment of the Sagittarius Arm. We discuss possible interpretations of this feature as a substructure within the lower pitch angle Sagittarius Arm, as a spur, or as an isolated structure.

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Mapping luminous hot stars in the Galaxy

Cited by 48 publications

References 78 publications

An all-sky sample of intermediate- to high-mass OBA-type eclipsing binaries observed by TESS

An all-sky sample of intermediate- to high-mass OBA-type eclipsing binaries observed by TESS

Galactic spiral structure revealed byGaiaEDR3

A high pitch angle structure in the Sagittarius Arm

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