Our galaxy is a giant ‘smoothie’ of blended stars and gas but a new study tells us where the components came from
In its early days, the Milky Way was like a giant smoothie, as if galaxies consisting of billions of stars, and an enormous amount of gas had been thrown together into a gigantic blender. But a new study picks apart this mixture by analysing individual stars to identify which originated inside the galaxy and which began life outside.
“Although the Milky Way is our home galaxy, we still do not understand how it formed and evolved,” says researcher Sven Buder from the ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) and the Australian National University (ANU).
His paper, published this week in the Monthly Notices of the Royal Astronomical Society, analyses the light from stars in detail, helping to understand what elements went into the creation of the Milky Way we know today.
“The Milky Way ate up lots of smaller galaxies but, until recently, we did not have enough evidence of that to say for sure,” Buder says.
“That’s because simple images of stars in our Milky Way look the same – whether they were born inside the galaxy or outside and then blended into the galaxy.”
Buder and colleagues in the Galactic Archaeology with HERMES (GALAH) team used Australia’s largest optical telescope, the Anglo-Australian Telescope (AAT), at Siding Spring Observatory to split light from more than 600,000 stars into wavelengths with the HERMES (High Efficiency and Resolution Multi-Element Spectrograph) instrument.
This effectively creates 600,000 stellar rainbows known as spectra.
Within each of these rainbows are specific bands of light – rather like tiny unique barcodes – that vary depending on a star’s chemical composition.
“If an image is worth a thousand words, these spectra are worth more than a thousand pictures,” says Buder. “By ‘scanning’ these stellar barcodes, we measured how abundant 30 elements, such as sodium, iron, magnesium, and manganese, were, and how they appeared in different concentrations depending on where the star was born.”
This discovery is an early step towards reconstructing a picture of the “childhood” of the Milky Way to get an idea of the size of the galaxies that it consumed in the process.
“It could also help us understand how several of the features of the galaxy we know today came into being,” says Buder.
One mystery the new observations could help solved is why there are two distinct groups of stars in the disc that we see as the “milky” band in the night sky.
“The Milky Way spread out across the night sky is a familiar sight, and when we look at it, we are actually gazing into the centre of our galaxy with its billions of stars,” says Buder.
“But we are looking at two populations of stars, one much older than the other. The old stars have moved so they look like they bulge out of the main plane of the Milky Way, while the younger stars form a much thinner band in the plane.
“But we don’t know why this has happened and our latest findings of the remnants of gigantic, galactic collisions may help us understand,” says Buder.
Buder’s paper provides the latest revelations relying on data from the Gaia project – an ambitious satellite mission to chart a three-dimensional map of the Milky Way to help understand its orbits, composition, formation, and evolution.
The Gaia satellite measurements can help us to find candidates of previously extragalactic stars, because they still move differently from a typical Milky Way star. But the extragalactic origin of a star can only be confirmed by its chemical fingerprint.
The GALAH survey is an Australian-led Large Observing Program using the HERMES instrument to obtain the highest spectral resolution multi-dimensional datasets for more than a million stars of all ages and locations in the Milky Way, to trace the full history of the Galaxy.
The HERMES instrument was built by the Australian Astronomical Observatory, which has since become the Astralis Instrumentation Consortium. Astralis receives $5M per year from the NCRIS programme, and combines expertise from Macquarie University, the University of Sydney, and ANU. Astralis will strengthen Australia’s competitiveness for instrumentation contracts at major observatories world-wide.
For more information
Tamzin Byrne, tamzin@scienceinpublic.com.au
Niall Byrne, niall@scienceinpublic.com.au
Available for interview
Dr Sven Buder, sven.buder@anu.edu.au
Images
CAPTION: A simulation of a collision between the young Milky Way and a smaller galaxy – Dr Tobias Buck (AIP/MPIA/NYU).
CAPTION: Just by looking at how abundant are sodium, iron, magnesium, and manganese in a star, we can tell apart stars born in the Milky Way (green) or outside (yellow).
CAPTION: The Milky Way has two distinct populations of stars, one older than the other. The older stars have moved so they look like they bulge out of the main plane of the Milky Way, while the younger stars form a much thinner band in the plane..
Paper Details
The GALAH Survey: chemical tagging and chrono-chemodynamics of accreted halo stars with GALAH+ DR3 and Gaia eDR3
DOI: https://doi.org/10.1093/mnras/stab3504
Authors
Sven Buder, Karin Lind, Melissa K Ness, Diane K Feuillet, Danny Horta, Stephanie Monty, Tobias Buck, Thomas Nordlander, Joss Bland-Hawthorn, Andrew R Casey, Gayandhi M De Silva, Valentina D’Orazi, Ken C Freeman, Michael R Hayden, Janez Kos, Sarah L Martell, Geraint F Lewis, Jane Lin, Katharine J Schlesinger, Sanjib Sharma, Jeffrey D Simpson, Dennis Stello, Daniel B Zucker, Tomaž Zwitter, Ioana Ciucă, Jonathan Horner, Chiaki Kobayashi, Yuan-Sen Ting (丁源森), Rosemary F G Wyse.
Abstract
Since the advent of Gaia astrometry, it is possible to identify massive accreted systems within the Galaxy through their unique dynamical signatures. One such system, Gaia-Sausage-Enceladus (GSE), appears to be an early ‘building block’ given its virial mass >1010M⊙ at infall (z ∼ 1−3). In order to separate the progenitor population from the background stars, we investigate its chemical properties with up to 30 element abundances from the GALAH+ Survey Data Release 3 (DR3). To inform our choice of elements for purely chemically selecting accreted stars, we analyse 4164 stars with low-α abundances and halo kinematics. These are most different to the Milky Way stars for abundances of Mg, Si, Na, Al, Mn, Fe, Ni, and Cu. Based on the significance of abundance differences and detection rates, we apply Gaussian mixture models to various element abundance combinations. We find the most populated and least contaminated component, which we confirm to represent GSE, contains 1049 stars selected via [Na/Fe] versus [Mg/Mn] in GALAH+ DR3. We provide tables of our selections and report the chrono-chemodynamical properties (age, chemistry, and dynamics). Through a previously reported clean dynamical selection of GSE stars, including 30<√(JR/kpckms−1)<55, we can characterize an unprecedented 24 abundances of this structure with GALAH+ DR3. With our chemical selection we characterize the dynamical properties of the GSE, for example mean J√(R/kpckms−1)=26+9−14. We find only (29±1) per cent of the GSE stars within the clean dynamical selection region. Our methodology will improve future studies of accreted structures and their importance for the formation of the Milky Way.
More about ASTRO 3D
ASTRO 3D is a seven-year $40-million Centre of Excellence project funded by the Australian Government through the Australian Research Council. The Centre began in June 2017 and will end in June 2024. It hosts around 200 investigators and professional staff, mostly based at six nodes: the Australian National University, Curtin University, Swinburne University of Technology, University of Melbourne, University of Sydney, and University of Western Australia. https://astro3d.org.au/