Galactic spiral structure revealed by Gaia EDR3

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 (similar or equal to 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 degrees< l<270 degrees) 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.

Automated summary

By utilizing astrometry and integrated photometry data from the Gaia Early Data Release 3, this study maps the density variations of young upper main sequence (UMS) stars, open clusters, and classical Cepheids in the Galactic disc, revealing the location and extent of spiral arm segments. The resulting maps show large-scale arches with over-dense regions matching the distribution of bright open clusters, while the geometry of the arms in the III quadrant differs significantly from previous models, suggesting a larger pitch angle for the Perseus arm and a longer extent of the Local Arm.