English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Stellar mass is a fundamental parameter that is key to our understanding ofstellar formation and evolution, as well as the characterization of nearbyexoplanet companions. Historically, stellar masses have been derived fromlong-term observations of visual or spectroscopic binary star systems. Whileadvances in high-resolution imaging have enabled observations of systems withshorter orbital periods, stellar mass measurements remain challenging, andrelatively few have been precisely measured. We present a new statisticalapproach to measuring masses for populations of stars. Using Gaia astrometry,we analyze the relative orbital motion of $>3,800$ wide binary systemscomprising low-mass stars to establish a Mass-Magnitude relation in the Gaia$G_\mathrm{RP}$ band spanning the absolute magnitude range$14.5>M_{G_\mathrm{RP}}>4.0$, corresponding to a mass range of$0.08$~M$_{\odot}\lesssim M\lesssim1.0$~M$_{\odot}$. This relation is directlyapplicable to $>30$ million stars in the Gaia catalog. Based on comparison toexisting Mass-Magnitude relations calibrated for 2MASS $K_{s}$ magnitudes, weestimate that the internal precision of our mass estimates is $\sim$10$\%$. Weuse this relation to estimate masses for a volume-limited sample of$\sim$18,200 stars within 50~pc of the Sun and the present-day field massfunction for stars with $M\lesssim 1.0$~M$_{\odot}$, which we find peaks at0.16~M$_{\odot}$. We investigate a volume-limited sample of wide binary systemswith early K dwarf primaries, complete for binary mass ratios $q>0.2$, andmeasure the distribution of $q$ at separations $>100$~au. We find that ourdistribution of $q$ is not uniformly distributed, rather decreasing towards$q=1.0$.

A Mass-Magnitude Relation for Low-mass Stars Based on Dynamical Measurements of Thousands of Binary Star Systems