Proof that Some Galaxies Are “LIERs”

You might think that astronomers could easily tell the difference between a black hole and a white dwarf — but nature can be deceptive.

Astronomers from the Sloan Digital Sky Survey (SDSS) this morning announced the results of a new study that reveals the true origin of puzzling light from nearby galaxies. Results were presented at the 227th meeting of the American Astronomical Society in Kissimmee, Florida.

“We now know that white dwarfs, not central black holes, explain these observations,” says Francesco Belfiore, the lead author of the study and a graduate student at the University of Cambridge. “Because we know that white dwarfs are to blame, we are much closer to understanding how galaxies retire from the star-formation business.”

To solve the mystery, Belfiore’s team looked at the thin interstellar gas that lies between stars in nearby galaxies. They used information from the emission lines of the spectra of that hot, glowing gas to decode what energy source lights it up. Understanding the origin of these emission lines is far from straightforward. In particular, astronomers have long been puzzled by the energy source for a particular state of gas in galaxies: The source must be hotter than newly formed stars but cooler than the radiation from a violently accreting black hole, like a quasar.

The leading theory used to be that this gas was lit by a wimpy active galactic nucleus, which is only accreting very small amounts of gas. This idea was supported by the fact that nuclear regions of many galaxies show such Low-Ionization Nuclear Emission-line Regions, which were therefore called LINERs.

“LINERs are a 35-year-old puzzle,” says Belfiore. “In recent years, several astronomers have argued against the mainstream interpretation and presented evidence that not all LINERs are due to black holes. The new SDSS data gave us a chance to take a new look at this question and evaluate possible alternative theories.

Previous spectroscopic observations were insufficient because they generally covered only a small portion of a galaxy near its center. A new SDSS instrument, called MaNGA (Mapping Nearby Galaxies at Apache Point Observatory), is now capable of obtaining spectroscopic data for the whole galaxy at once.

“To get the data we need, we use a simple but innovative design,” says Kevin Bundy from the Kavli Institute for the Physics and Mathematics of the universe (Kavli IPMU), Principal Investigator for the MaNGA survey and co-author of the study. “We tie together a few dozen optical fibers into a large hexagonal bundle and point them at a galaxy. The bundle covers most of the galaxy and each fiber measures the spectrum at a different point.”

Belfiore and his collaborators used the MaNGA data to map the state of gas and stars throughout more than 600 LINER galaxies. “By taking advantage of the fact that MaNGA can get data for an entire galaxy at once, we have revealed that the sources lighting the gas up must be distributed throughout the galaxy, even tens of thousands of light-years away from the central black hole. This proves that the emission lines we see cannot all be due to central black holes,” says Belfiore.

Claudia Maraston of the University of Portsmouth, a co-author of the study, explains the most likely answer to the LINER puzzle. “White dwarfs are revealed as stars lose their outer gas envelopes and expose their hot cores, which still glows at millions of degrees. These newly-exposed white dwarfs are the ideal sources to light up the interstellar gas and produce the emission lines we see,” says Maraston.

Although this mechanism was originally suggested to be important only in elliptical galaxies, the new MaNGA data reveals that it is in fact common in both elliptical and spiral galaxies. “In the spiral galaxies, the gas shining as LINERs is the dying gasp of star formation being quenched as gas reservoirs are depleted in inner regions and star formation moves to the outer suburbs. In the elliptical galaxies, where almost all star formation occurred rapidly in the early days of the universe, this glowing gas represents a ‘rejuvenation’ of the dormant galaxy,” says Belfiore. “Donated gas, from dying stars within the galaxy or from a merging galaxy, is now able to intercept the extreme radiation and make the galaxy shine again, albeit only as a LINER.”

With the extensive mapping of low-ionization emission-line regions outside of the nuclei of galaxies, far removed from central supermassive black holes, but close to newly born white dwarfs, the ‘N’ for ‘nuclear’ in the LINER acronym must disappear.

The truth, then, is this: many galaxies are LIERs.

PIO Contacts:
Jennifer Johnson
SDSS Scientific Spokesperson
The Ohio State University
johnson.3064@osu.edu
+1 (614) 893-2132

Jordan Raddick
SDSS Public Information Officer
Johns Hopkins University
raddick@jhu.edu
+1 (443) 570-7105

Science Contacts:
Francesco Belfiore
University of Cambridge / Kavli Institute for Cosmology / Member of the UK Participation Group
fb338@cam.ac.uk
+44 (0)1223 746434

Roberto Maiolino
University of Cambridge / Kavli Institute for Cosmology / Member of the UK Participation Group
r.maiolino@mrao.cam.ac.uk
+44 (0)1223 761661

Kevin Bundy
Kavli Institute for the Physics and Mathematics of the universe
kevin.bundy@ipmu.jp
+81 (0)4-7136-6513

Image (2100 x 1500 pixels, 300 dpi):
https://dl.dropboxusercontent.com/u/23495063/liers.png
This image shows SDSS observations of one of the LIER galaxies used in this study. The underlying image is from the SDSS and includes a scale bar. The pink hexagon shows the size of the MaNGA fiber optic bundle. The region inside the hexagon shows the newly-derived map of interstellar gas from MaNGA. The presence of the gas throughout the galaxy eliminates the black hole explanation (pictured at the top left) and favors the white dwarf explanation (bottom right). Credit: Jennifer Johnson (The Ohio State University) and the SDSS Collaboration; black hole: NASA/Dana Berry/SkyWorks Animation; white dwarf: NASA/JPL (Raghvendra Sahai)

Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is http://www.sdss.org.

SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofisica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the universe (IPMU) / University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut fur Astrophysik Potsdam (AIP), Max-Planck-Institut fur Astronomie (MPIA Heidelberg), Max-Planck-Institut fur Astrophysik (MPA Garching), Max-Planck-Institut fur Extraterrestrische Physik (MPE), National Astronomical Observatory of China, New Mexico State University, New York University, University of Notre Dame, Observatorio Nacional / MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autonoma de Mexico, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University.