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The Pal 5 Star Stream Gaps

Galberg, R. G. and Grillmair, C. J. and Hetherington, Nathan (2012) The Pal 5 Star Stream Gaps. Astrophysical Journal, 760 (1). Art. No. 75. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20121219-102906111

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Abstract

Pal 5 is a low-mass, low-velocity-dispersion, globular cluster with spectacular tidal tails. We use the Sloan Digital Sky Survey Data Release 8 data to extend the density measurements of the trailing star stream to 23 deg distance from the cluster, at which point the stream runs off the edge of the available sky coverage. The size and the number of gaps in the stream are measured using a filter which approximates the structure of the gaps found in stream simulations. We find 5 gaps that are at least 99% confidence detections with about a dozen gaps at 90% confidence. The statistical significance of a gap is estimated using bootstrap resampling of the control regions on either side of the stream. The density minimum closest to the cluster is likely the result of the epicyclic orbits of the tidal outflow and has been discounted. To create the number of 99% confidence gaps per unit length at the mean age of the stream requires a halo population of nearly a thousand dark matter sub-halos with peak circular velocities above 1 km s^(–1) within 30 kpc of the galactic center. These numbers are a factor of about three below cold stream simulation at this sub-halo mass or velocity but, given the uncertainties in both measurement and more realistic warm stream modeling, are in substantial agreement with the LCDM prediction.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/760/1/75DOIArticle
http://iopscience.iop.org/0004-637X/760/1/75PublisherArticle
ORCID:
AuthorORCID
Grillmair, C. J.0000-0003-4072-169X
Additional Information:© 2012 American Astronomical Society. Received 2012 June 2; accepted 2012 October 1; published 2012 November 6. This research is supported by NSERC and CIfAR. We thank the referee, Andreas Küpper, for constructive comments. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. Facility: Sloan
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
NSFUNSPECIFIED
Department of Energy (DOE)UNSPECIFIED
Subject Keywords:dark matter; galaxies: dwarf; Local Group
Issue or Number:1
Record Number:CaltechAUTHORS:20121219-102906111
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20121219-102906111
Official Citation:The Pal 5 Star Stream Gaps R. G. Carlberg, C. J. Grillmair, and Nathan Hetherington doi:10.1088/0004-637X/760/1/75
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:36045
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:19 Dec 2012 18:51
Last Modified:03 Oct 2019 04:34

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