The Magellanic Clouds — two nearby dwarf galaxies easily visible to the naked eye in the southern hemisphere — are key to understanding the dynamics and evolution of the Local Group of galaxies. Can an in-depth look at these galaxies’ outer regions help us make sense of their complicated interaction history?

A Closer Look at Our Galactic Neighbors

The Small and Large Magellanic Clouds (SMC and LMC) have been well studied, but these dwarf satellite galaxies continue to inspire new discoveries. Among them is the origin of the Magellanic Stream — a swath of neutral hydrogen trailing the Magellanic Clouds and spanning more than half a million light-years.

It was originally thought that the Magellanic Stream was the result of tidal interactions during close encounters with the Milky Way, but precise proper motion surveys revealed that the LMC and SMC are either passing near the Milky Way for the first time or are in a long (~4-billion-year) orbit around our galaxy — so the Magellanic Stream must result from interactions between the two galaxies themselves.

How long have the LMC and SMC been interacting, and how have these interactions shaped the two galaxies? A key to understanding the history of these dwarf galaxies is mapping the weakly gravitationally bound stars at their far edges that may be pulled into tidal streams or bulges as each galaxy is distorted by the presence of the other.

Mapping the Edges of Galaxies

Dougal Mackey (Australian National University) and collaborators used visible and near-infrared images taken by the Dark Energy Camera (DECam) — the workhorse instrument of the Dark Energy Survey — to map the faint outskirts of the LMC and SMC.

Though the purpose of the Dark Energy Survey is to better understand the nature of dark energy through observations of supernovae, weak gravitational lenses, and galaxy clusters, its sensitive imaging system and wide field of view (2.2 degrees in diameter) make it well-suited to exploring the faint fringes of nearby galaxies.

The DECam images of the Magellanic Clouds probed to a surface brightness of 32 magnitudes per square arcsecond, allowing Mackey and collaborators to investigate how different stellar populations are distributed in the outer regions of these galaxies.

Structures Revealed in Faint Starlight

Mapping the density of stars revealed distinct stellar substructures on the outskirts of the LMC and SMC. While previous studies discovered isolated substructures on the outer limits of the LMC, the panoramic view from this study highlights the interconnected nature of the structures.

One important finding is that the intermediate-age (1.5–4 Gyr) stellar population of the SMC is distinctly offset from the ancient (~11 Gyr) stellar population. This result suggests that the Magellanic Clouds may have been gravitationally linked as far back as several billion years — hinting that these galaxies are on their first trip past the Milky Way. Future simulation work may provide a more cohesive picture of the LMC–SMC interaction, helping us better understand how our near neighbors have evolved.

Citation

Dougal Mackey et al 2018 ApJL 858 L21. doi:10.3847/2041-8213/aac175

Related Journal Articles

Low Surface Brightness Imaging of the Magellanic System: Imprints of Tidal Interactions between the Clouds in the Stellar Periphery doi: 10.3847/0004-637X/825/1/20

SMASH: Survey of the MAgellanic Stellar History doi: 10.3847/1538-3881/aa8d1c

An Ultra-faint Galaxy Candidate Discovered in Early Data from the Magellanic Satellites Survey doi: 10.3847/2041-8205/833/1/L5

OGLE-ING the Magellanic System: Stellar Populations in the Magellanic Bridge doi: 10.1088/0004-637X/795/2/108

SMASH 1: A Very Faint Globular Cluster Disrupting in the Outer Reaches of the LMC? doi: 10.3847/2041-8205/830/1/L10

Beasts of the Southern Wild: Discovery of Nine Ultra Faint Satellites in the Vicinity of the Magellanic Clouds. doi: 10.1088/0004-637X/805/2/130

This post originally appeared on AAS Nova, which features research highlights from the journals of the American Astronomical Society.