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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 693832.0, MPI für Astronomie / Publikationen_mpia
Dynamics in the satellite system of Triangulum: is And XXII a dwarf satellite of M33?
Authors:Chapman, S. C.; Widrow, L.; Collins, M. L. M.; Dubinski, J.; Ibata, R. A.; Rich, M.; Ferguson, A. M. N.; Irwin, M. J.; Lewis, G. F.; Martin, N.; McConnachie, A.; Peñarrubia, J.; Tanvir, N.
Date of Publication (YYYY-MM-DD):2013
Title of Journal:Monthly Notices of the Royal Astronomical Society
Volume:430
Start Page:37
End Page:49
Audience:Not Specified
Abstract / Description:We present results from a spectroscopic survey of the dwarf spheroidal galaxy And XXII and the two extended clusters EC1 and EC2. These three objects are candidate satellites of the Triangulum galaxy, M33, which itself is likely a satellite of M31. We use the DEep Imaging Multi-Object Spectrograph (DEIMOS) mounted on the Keck II telescope to derive radial velocities for candidate member stars of these objects and thereby identify the stars that are most likely actual members. 11 probable stellar members are found for And XXII. We obtain an upper limit of σv < 6.0 km s-1 for the velocity dispersion of And XXII, [Fe/H] ˜ -1.6 for its metallicity and 255 pc for the Plummer radius of its projected density profile. We construct a colour-magnitude diagram for And XXII and identify both the red giant branch and the horizontal branch. The position of the latter is used to derive a heliocentric distance to And XXII of 853 ± 26 kpc. The combination of the radial velocity, distance and angular position of And XXII indicate that it is a strong candidate as the first known satellite of M33 and one of the very few examples of a galactic satellite of a satellite. N-body simulations imply that this conclusion is unchanged even if M31 and M33 had a strong encounter in the past few Gyr. We test the hypothesis that the extended clusters highlight tidally stripped galaxies by searching for an excess cloud of halo-like stars in their vicinity. We find such a cloud for the case of EC1 but not for EC2. The three objects imply a dynamical mass for M33 that is consistent with previous estimates.
Free Keywords:instrumentation: spectrographs; galaxies: dwarf; galaxies: individual: M31; galaxies: individual: M33
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0035-8711 %R 10.1093/mnras/sts392
URL:http://cdsads.u-strasbg.fr/abs/2013MNRAS.430...37C
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