More Masters at the Fair

Shapley, John

doi:10.2307/772231

Cited by 1 publication

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“…There is evidence of stellar debris tidally stripped by the LMC lying in its eastern regions (Nidever et al 2013;Subramanian et al 2017). Centrally, the SMC displays a less prominent bar as well as an eastern wing structure first observed by Shapley (1940), departing from the northern end of the bar toward the LMC. Recent mapping of the SMC by El Youssoufi et al (2019) has shown the morphology of the younger stellar populations to be highly irregular and largely limited to the SMC bar and eastern wing, tracing the perturbed gaseous reservoir of the SMC (Stanimirović et al 2004), with recent star formation expected to have occurred in these regions (see, e.g., Irwin et al 1990;El Youssoufi et al 2019).…”

Section: Introductionmentioning

confidence: 88%

Magellanic Mayhem: Metallicities and Motions

Grady

Belokurov

Evans

2021

ApJ

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We assemble a catalog of Magellanic Cloud red giants from Data Release 2 of the Gaia mission and, utilizing machine-learning methods, obtain photometric metallicity estimates for them. In doing so, we are able to chemically map the entirety of the Magellanic System at once. Our maps reveal a plethora of substructure within our red giant sample, with the Large Magellanic Cloud (LMC) bar and spiral arm being readily apparent. We uncover a curious spiral-like feature in the southern portion of the LMC disk, hosting relatively metal-rich giants and likely a by-product of historic encounters with the Small Magellanic Cloud (SMC). Modeling the LMC as an inclined thin disk, we find a shallow metallicity gradient of −0.048 ± 0.001 dex kpc −1 out to ∼12°from the center of the dwarf. We see evidence that the SMC is disrupting, with its outer isodensity contours displaying the S-shape symptomatic of tidal stripping. On studying the proper motions of the SMC giants, we observe a population of them being violently dragged toward the larger Cloud. The perturbed stars predominantly lie in front of the SMC, and we interpret that they exist as a tidal tail of the dwarf, trailing in its motion and undergoing severe disruption from the LMC. We find the metallicity structure in the Magellanic Bridge region to be complex, with evidence for a composite nature in this stellar population, consisting of both LMC and SMC debris.Unified Astronomy Thesaurus concepts: Galaxies (573); Local Group (929); Large Magellanic Cloud (903); Small Magellanic Cloud (1468)

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