An international team of astronomers led by the Max Planck Institute for Astronomy (MPIA) has made a surprising discovery about the birthplace of groups of stars located in the halo of our Milky Way galaxy.
These halo stars are grouped together in giant structures that orbit the center of our galaxy, above and below the flat disk of the Milky Way. Researchers thought they may have formed from debris left behind by smaller galaxies that invaded the Milky Way in the past.
But in a study published today in the journal Nature, astronomers now have compelling evidence showing that some of these halo structures actually originate from the Milky Way’s disk itself, but were kicked out.
“This phenomenon is called galactic eviction,” said co-author Judy Cohen, Kate Van Nuys Page Professor of Astronomy at Caltech. “These structures are pushed off the plane of the Milky Way when a massive dwarf galaxy passes through the galactic disk. This passage causes oscillations, or waves, that eject stars from the disk, either above or below it depending on the direction that the perturbing mass is moving.”
“The oscillations can be compared to sound waves in a musical instrument,” said lead author Maria Bergemann of MPIA. “We call this ‘ringing’ in the Milky Way galaxy ‘galactoseismology,’ which has been predicted theoretically decades ago. We now have the clearest evidence for these oscillations in our galaxy’s disk obtained so far!”
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For the first time, Bergemann’s team presented detailed chemical abundance patterns of these halo stars using the W. M. Keck Observatory on Maunakea, Hawaii.
“The analysis of chemical abundances is a very powerful test, which allows, in a way similar to the DNA matching, to identify the parent population of the star. Different parent populations, such as the Milky Way disk or halo, dwarf satellite galaxies or globular clusters, are known to have radically different chemical compositions. So once we know what the stars are made of, we can immediately link them to their parent populations,” said Bergemann.
The scientists investigated 14 stars located in two different halo structures — the Triangulum-Andromeda (Tri-And) and the A13 stellar overdensities. These two structures lie on opposite sides of the Milky Way disk; about 14,000 light years above and below the Galactic plane.
The team obtained spectra of the halo stars using Keck Observatory’s High-Resolution Echelle Spectrometer (HIRES).
“The high throughput and high spectral resolution of HIRES were crucial to the success of the observations of the stars in the outer part of the Milky Way,” said Cohen. “Another key factor was the smooth operation of Keck Observatory; good pointing and smooth operation allows one to get spectra of more stars in only a few nights of observation. The spectra in this study were obtained in only one night of Keck time, which shows how valuable even a single night can be.”
The team also obtained a spectrum of one additional star taken with the European Southern Observatory’s Very Large Telescope (VLT) in Chile.
When comparing the chemical compositions of these stars with the ones found in other cosmic structures, the scientists were surprised to find that the chemical compositions are almost identical, both within and between these groups, and closely match the abundance patterns of the Milky Way outer disk stars.
This provides compelling evidence that the halo stars most likely originate from the Galactic thin disk (the younger part of Milky Way, strongly concentrated towards the Galactic plane) itself.
These findings are very exciting because they indicate the Milky Way’s disk and its dynamics are significantly more complex than previously thought.
“We showed that it may be fairly common for groups of stars in the disk to be relocated to more distant realms within the Milky Way — having been ‘kicked out’ by an invading satellite galaxy. Similar chemical patterns may also be found in other galaxies, indicating a potential galactic universality of this dynamic process,” said co-author Allyson Sheffield of LaGuardia Community College/CUNY.
As a next step, the astronomers plan to analyse the spectra of additional stars in the Tri-And and A13 overdensities, as well as stars in other stellar structures further away from the disk. They also plan to determine masses and ages of these stars so they can constrain the time limits of when this galactic eviction took place.
W. M. Keck Observatory
Maria Bergemann, Branimir Sesar, Judith G. Cohen, Aldo M. Serenelli, Allyson Sheffield, Ting S. Li, Luca Casagrande, Kathryn V. Johnston, Chervin F. P. Laporte, Adrian M. Price-Whelan, Ralph Schönrich, Andrew Gould. Two chemically similar stellar overdensities on opposite sides of the plane of the Galactic disk. Nature, 2018; DOI: 10.1038/nature25490
The Milky Way galaxy, perturbed by the tidal interaction with a dwarf galaxy, as predicted by N-body simulations. The locations of the observed stars above and below the disk, which are used to test the perturbation scenario, are indicated.
Credit: T. MUELLER/C. LAPORTE/NASA/JPL-CALTECH