Press Release 02-06-03 Press Releases 2002 – 1999

FOR RELEASE: 09:20 a.m. MDT, June 3, 2002
17:20 MESZ, June 3, 2002

Sky Survey Unveils Star Cluster
Shredded By The Milky Way

Albuquerque, New Mexico, USA, and Heidelberg, Germany – A team of astronomers from the Sloan Digital Sky Survey (SDSS) collaboration has discovered a spectacular stream of stellar debris emanating from a star cluster that is being torn apart by the Milky Way.

Dr. Michael Odenkirchen and Dr. Eva Grebel from the Max Planck Institute for Astronomy (MPIA) in Heidelberg, Germany, are presenting these findings today at the American Astronomical Society (AAS) meeting in Albuquerque, New Mexico. The detection of this stream, the first of its kind, supports theorists' view that star clusters get destroyed by the tidal forces of the Milky Way. Researchers say such extended streams of tidal debris provide a new way to determine the mass distribution of the dark matter halo of our Galaxy.

star cluster Palomar 5   Fig. 1: Color-coded map of the distribution of stars emerging from the star cluster Palomar 5 (white blob). The two long tidal tails (orange) contain 1.3 times the mass of the cluster and delineate its orbit around the Milky Way (yellow line).

Pictures with higher resolution:
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fig1-hr.jpg JPG 1648x1069 pxl 88 KB
fig1-CMYK.eps EPS 3 MB Blank,
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fig1-CMYK-path.eps EPS 3 MB with path
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The orbit of Palomar 5   Fig. 2: The orbit (red line) of Palomar 5 in the halo of our Milky Way as reconstructed from the tidal tails and the known position, distance, and radial velocity of the cluster. The image used to illustrate the Milky Way Galaxy is courtesy of the Hubble Heritage project.

Pictures with higher resolution:
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»zipped« (reduced size)

The stars in the newly discovered stream are being torn from an ancient globular cluster named Palomar 5, which is located in the outer part of our Galaxy 75 000 light years away from the Sun. While typical globular clusters are massive, luminous concentrations of some hundred thousand stars, Palomar 5 by comparison looks faint and diffuse and contains only about ten thousand stars. This led astronomers to suspect that Palomar 5 might be a likely victim of the disruptive tides of the Milky Way. These »tides« arise because the Milky Way's gravitational pull is stronger on the cluster's near side than on the far side, thus tearing the cluster apart. However, the telltale debris from the disruption was difficult to find since it is hidden in a sea of foreground and background objects.

Using data from the SDSS and a special filtering technique, Odenkirchen and his collaborators have succeeded in making the stream of debris from Palomar 5 directly visible. »The excellent homogeneity, resolution, depth, and multi-color information of the SDSS observations have allowed us to separate faint former members of Palomar 5 from contaminating field stars and background galaxies,« says Odenkirchen, who is a postdoctoral researcher at the MPIA.

The SDSS is an international project that is creating a deep map of one quarter of the sky in five colors. The SDSS records objects up to 10 million times fainter than the faintest stars visible with the naked eye. The observations are carried out with a special wide-field camera on a dedicated 2.5-meter telescope at Apache Point Observatory, New Mexico. Team member Dr. Connie Rockosi of the University of Washington was one of the builders of the camera.

First direct evidence for the tidal disruption of Palomar 5 emerged two years ago from SDSS commissioning data that happened to include Palomar 5. Odenkirchen and collaborators were amazed to recover the characteristic S-shape signature of tidal debris from these data. »This was the first time that tidal tails of a star cluster were seen with convincing clarity«, says Grebel, an astronomer who leads the Galactic structure group at MPIA.

Meanwhile the SDSS has scanned a much larger region on the sky. Analyzing the new data the researchers found that the two tails emanating from Palomar 5 extend over an arc of ten degrees on the sky. This vast area corresponds to 20 times the diameter of the full moon on the sky or to a length of 13 000 light years in space. »Remarkably, we now find more mass in the tails than in the remaining cluster. We expect to detect the stream over an even larger area as the survey progresses,« Odenkirchen said.

The tails of Palomar~5 delineate the orbital path of this cluster and thus provide a unique opportunity to determine its motion around the Milky Way. »The motions of objects orbiting the Galactic halo are still poorly known. It normally takes decades to measure even only the instantaneous displacement of a globular cluster on the sky,« Grebel points out. »Finding additional coherent streams that extend over large portions of the sky we would be able to reconstruct Galactic orbits independent of a specific Galactic model,« says the MPIA's Dr. Walter Dehnen, who carried out extensive numerical simulations on the disruption of Palomar~5. The researchers expect that the geometry and the velocities of those tidal streams will become important tools for determining the mass of the dark matter halo of the Milky Way.

Together with the so-called Sagittarius stream, which emerges from a dwarf galaxy that is currently being accreted by the Milky Way, there are now two different examples of extended stream-like structures in the Galactic halo. Computer simulations suggest that globular clusters were much more numerous in the early days of the Milky Way, and that many of them have already been shredded by Galactic tides. As the survey proceeds the SDSS researchers will be able to test this prediction by searching for signs of tidal mass loss around other globular clusters. »The SDSS data base will ultimately allow us to estimate the total number of such streams,« says Professor Hans-Walter Rix, director of the MPIA. »This will clarify the role of tidal disruption in the build-up of the Galactic halo and provide a crucial test for galaxy formation models.«

The researchers participating in this work are Michael Odenkirchen, Eva Grebel, Walter Dehnen, and Hans-Walter Rix from the Max Planck Institute for Astronomy, Connie Rockosi of the University of Washington, Brian Yanny from Fermilab, and Heidi Newberg from the Rensselaer Polytechnic Institute.

The SDSS is a joint project of The University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, Los Alamos National Laboratory, the Max-Planck Institute for Astronomy (MPIA), the Max-Planck Institute for Astrophysics (MPA), New Mexico State University, Princeton University, the United States Naval Observatory, the University of Pittsburgh, and the University of Washington.

Funding for the SDSS has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society.

Dr. Jakob Staude
MPIA Public Information Office
Phone: (+49) 6221 – 528 229
Fax:   (+49) 6221 – 528 246

Press Releases 2002 – 1999