Quick Search:

uzh logo
Browse by:

Zurich Open Repository and Archive

Maintenance: Tuesday, 5.7.2016, 07:00-08:00

Maintenance work on ZORA and JDB on Tuesday, 5th July, 07h00-08h00. During this time there will be a brief unavailability for about 1 hour. Please be patient.

Permanent URL to this publication: http://dx.doi.org/10.5167/uzh-30851

Klimentowski, J; Lokas, E L; Kazantzidis, S; Mayer, L; Mamon, G A; Prada, F (2009). The orientation and kinematics of inner tidal tails around dwarf galaxies orbiting the Milky Way. Monthly Notices of the Royal Astronomical Society, 400(4):2162-2168.

Accepted Version
View at publisher


Using high-resolution collisionless N-body simulations, we study the properties of tidal tails formed in the immediate vicinity of a two-component dwarf galaxy evolving in a static potential of the Milky Way (MW). The stellar component of the dwarf is initially in the form of a disc and the galaxy is placed on an eccentric orbit motivated by cold dark matter based cosmological simulations. We measure the orientation, density and velocity distribution of the stars in the tails. Due to the geometry of the orbit, in the vicinity of the dwarf, where the tails are densest and therefore most likely to be detectable, they are typically oriented towards the MW and not along the orbit. We report on an interesting phenomenon of 'tidal tail flipping': on the way from the pericentre to the apocentre, the old tails following the orbit are dissolved and new ones pointing towards the MW are formed over a short time-scale. We also find a tight linear relation between the velocity of stars in the tidal tails and their distance from the dwarf. Using mock data sets, we demonstrate that if dwarf spheroidal (dSph) galaxies in the vicinity of the MW are tidally affected their kinematic samples are very likely contaminated by tidally stripped stars which tend to artificially inflate the measured velocity dispersion. The effect is stronger for dwarfs on their way from the pericentre to the apocentre due to the formation of new tidal tails after pericentre. Realistic mass estimates of dSph galaxies thus require removal of these stars from kinematic samples.


34 citations in Web of Science®
32 citations in Scopus®
Google Scholar™



42 downloads since deposited on 26 Feb 2010
12 downloads since 12 months

Detailed statistics

Additional indexing

Item Type:Journal Article, refereed, original work
Communities & Collections:07 Faculty of Science > Institute for Computational Science
Dewey Decimal Classification:530 Physics
Uncontrolled Keywords:galaxies: dwarf; galaxies: fundamental parameters; galaxies: kinematics and dynamics; Local Group; dark matter
Date:December 2009
Deposited On:26 Feb 2010 15:30
Last Modified:05 Apr 2016 13:56
Funders:Center for Cosmology, Astro-Particle Physics (CCAPP) at The Ohio State University, Polish Ministry of Science and Higher Education [NN203025333], LEA Astronomie France Pologne programme of CNRS/PAN, European Science Foundation
Additional Information:The attached file is a preprint (accepted version) of an article published in Monthly Notices of the Royal Astronomical Society. The definitive version is available at www3.interscience.wiley.com
Publisher DOI:10.1111/j.1365-2966.2009.15626.x
Related URLs:http://arxiv.org/abs/0908.4022

Users (please log in): suggest update or correction for this item

Repository Staff Only: item control page