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

The Magellanic Bridge is the nearest low-metallicity, tidally strippedenvironment, offering a unique high-resolution view of physical conditions inmerging and forming galaxies. In this paper we present analysis of candidatemassive young stellar objects (YSOs), i.e., {\it in situ, current} massive starformation (MSF) in the Bridge using {\it Spitzer} mid-IR and complementaryoptical and near-IR photometry. While we definitely find YSOs in the Bridge,the most massive are $\sim10 M_\odot$, $\ll45 M_\odot$ found in the LargeMagellanic Cloud (LMC). The intensity of MSF in the Bridge also appearsdecreasing, as the most massive YSOs are less massive than those formed in thepast. To investigate environmental effects on MSF, we have compared propertiesof massive YSOs in the Bridge to those in the LMC. First, YSOs in the Bridgeare apparently less embedded than in the LMC: 81% of Bridge YSOs show opticalcounterparts, compared to only 56% of LMC sources with the same range of mass,circumstellar dust mass, and line-of-sight extinction. Circumstellar envelopesare evidently more porous or clumpy in the Bridge's low-metallicityenvironment. Second, we have used whole samples of YSOs in the LMC and theBridge to estimate the probability of finding YSOs at a given \hi\ columndensity, N(HI). We found that the LMC has $\sim3\times$ higher probability thanthe Bridge for N(HI) $>10\times10^{20}$ cm$^{-2}$, but the trend reverses atlower N(HI). Investigating whether this lower efficiency relative to HI is dueto less efficient molecular cloud formation, or less efficient cloud collapse,or both, will require sensitive molecular gas observations.

Spitzer View of Massive Star Formation in the Tidally Stripped Magellanic Bridge