From AAS NOVA: “Disentangling the History of the Magellanic Clouds”

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From AAS NOVA

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The Milky Way’s largest satellite galaxies, the Magellanic Clouds, have a complicated interaction history. [ESO/S. Brunier]

Magellanic Bridge ESA_Gaia satellite. Image credit V. Belokurov D. Erkal A. Mellinger.

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?

Large Magellanic Cloud. Adrian Pingstone December 2003

Small Magellanic Cloud. NASA/ESA Hubble and ESO/Digitized Sky Survey 2

A Closer Look at Our Galactic Neighbors

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A combined optical and radio view of the Milky Way and the Magellanic Stream, shown in pink. [David L. Nidever, et al., NRAO/AUI/NSF and Mellinger, Leiden/Argentine/Bonn Survey, Parkes Observatory, Westerbork Observatory, and Arecibo Observatory]

NRAO/Karl V Jansky VLA, on the Plains of San Agustin fifty miles west of Socorro, NM, USA, at an elevation of 6970 ft (2124 m)

CSIRO/Parkes Observatory, located 20 kilometres north of the town of Parkes, New South Wales, Australia

Westerbork Synthesis Radio Telescope, an aperture synthesis interferometer near World War II Nazi detention and transit camp Westerbork, north of the village of Westerbork, Midden-Drenthe, in the northeastern Netherlands

NAIC Arecibo Observatory operated by University of Central Florida, Yang Enterprises and UMET

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.

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A map of the density of ancient stars surrounding the Magellanic Clouds reveals extended structures to the north and south of the LMC, while the western regions of the galaxy (to the right) are truncated.[Adapted from Mackey et al. 2018]

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.

Dark Energy Survey


Dark Energy Camera [DECam], built at FNAL


NOAO/CTIO Victor M Blanco 4m Telescope which houses the DECam at Cerro Tololo, Chile, housing DECam at an altitude of 7200 feet

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.

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Stellar density maps for young (<1 Gyr) and intermediate-age (1.5–4 Gyr) populations. The young stars trace a bridge between the galaxies, while the intermediate-age stars are offset from the ancient stars in the direction of the LMC. [Adapted from Mackey et al. 2018]

Citation

Dougal Mackey et al 2018 ApJL 858 L21.http://iopscience.iop.org/article/10.3847/2041-8213/aac175/meta

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