REVIEW 6 cited by
The Milky Way as Seen by Classical Cepheids II: Spiral Structure
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
Signed reviews
read the original abstract
As a relatively young and bright population and the archetype of standard candles, classical Cepheids are an ideal population on which to trace the non-axisymmetric structure in the young stellar disk to large distances. We used the new distances derived in Paper I based on mid-IR WISE photometry for a selected sample of 2857 dynamically young Cepheids to trace the spiral arms of the Milky Way. The Perseus and Sagittarius-Carina arms are clearly evident in the third and fourth Galactic quadrants, while the Local and Scutum arms are much weaker, and extinction severely limits our view of the latter innermost spiral arm. Pitch angles were derived for each arm over various ranges of Galactic azimuth, each covering at least 90deg in azimuth. Our method of detecting spiral arms and deriving pitch angles does not rely on pre-assigning sources to specific arms. While the spiral structure in the first and second quadrant is not obvious in part because of extinction effects, it is not inconsistent with the structure seen in the third and fourth quadrants. In summary, the Cepheids allow us to map spiral structure in the third and fourth Galactic quadrants where currently few masers have astrometric parallaxes, significantly extending our understanding of the Milky Way at large scales.
Forward citations
Cited by 6 Pith papers
-
The Galactic inner spiral arms revealed by the Gaia ESO Survey chemical abundances. Metallicity and [Mg/Fe] ratios
Chemical abundance excess maps from Gaia-ESO Survey data reveal enhanced [Fe/H] and depleted [Mg/Fe] along the Scutum and Sagittarius inner spiral arms.
-
Tracing the W3/W4/W5 and Perseus complex dynamical evolution with star clusters
The Perseus star-forming complex is probably not dispersing; its apparent expansion is a projection effect of clusters orbiting the Galaxy, and LISCA I and W345 formed a few hundred parsecs apart about 20 to 30 Myr ago.
-
A non-axisymmetric potential for the Milky Way disk
A backward-integration fit to Gaia DR3 stellar velocities yields a Milky Way disk potential with a bar pattern speed of 37 km/s/kpc and two spiral modes at 13.1 and 16.4 km/s/kpc.
-
Signatures of simulated spiral arms on radial actions
Spiral arms and low-radial-action regions coincide in most of 23 simulated disc galaxies, supporting the use of Gaia radial action maps to trace Milky Way spiral arms and recent disturbances.
-
Unveiling the Milky Way with a Gaia DR3 census of OB-type stars within 2 kpc. I. Tracing local Galactic structure, massive star-forming regions and core-collapse supernova progenitors
A Gaia DR3-based census of 105,971 OB stars within 2 kpc maps local Galactic structure and identifies over 4,200 core-collapse supernova or black hole progenitor candidates.
-
Multiwavelength study of observed and predicted pulsation properties of First overtone Cepheids in the Magellanic Clouds
First-overtone Cepheids in the Magellanic Clouds show statistically significant break-points in period-color, period-luminosity, and amplitude-color relations near P=2.5 d, with a further LMC break near P=0.58 d, and ...
Discussion (0). Continue with ORCID to comment.