MNRAS-2014-Hoffmann-1197-210.pdf (1.26 MB)
Subhaloes gone Notts: subhaloes as tracers of the dark matter halo shape
journal contributionposted on 2015-03-18, 15:42 authored by K. Hoffmann, S. Planelles, E. Gaztañaga, A. Knebe, F. R. Pearce, H. Lux, J. Onions, Stuart I. Muldrew, P. Elahi, P. Behroozi, Y. Ascasibar, J. Han, M. Maciejewski, M. E. Merchan, M. Neyrinck, A. N. Ruiz, M. A. Sgro
We study the shapes of subhalo distributions from four dark-matter-only simulations of Milky Way-type haloes. Comparing the shapes derived from the subhalo distributions at high resolution to those of the underlying dark matter fields, we find the former to be more triaxial if the analysis is restricted to massive subhaloes. For three of the four analysed haloes, the increased triaxiality of the distributions of massive subhaloes can be explained by a systematic effect caused by the low number of objects. Subhaloes of the fourth halo show indications for anisotropic accretion via their strong triaxial distribution and orbit alignment with respect to the dark matter field. These results are independent of the employed subhalo finder. Comparing the shape of the observed Milky Way satellite distribution to those of high-resolution subhalo samples from simulations, we find agreement for samples of bright satellites, but significant deviations if faint satellites are included in the analysis. These deviations might result from observational incompleteness.
This paper was initiated at the Subhaloes going Notts workshop in Dovedale, UK, which was funded by the European Commissions Framework Programme 7, through the Marie Curie Initial Training Network Cosmo- Comp (PITN-GA-2009-238356). We wish to thank the Virgo Consortium for allowing the use of the Aquarius data set and Adrian Jenkins for assisting with the data. KH is supported by beca FI from Generalitat de Catalunya. He acknowledges Noam Libeskind for a fruitful discussion. SP and HL acknowledge a fellowship from the European Commission’s Framework Programme 7, through the Marie Curie Initial Training Network CosmoComp (PITN-GA-2009-238356). SP also acknowledges support by the PRIN-INAF09 project ‘Towards an Italian Network for Computational Cosmology’ and by Spanish Ministerio de Ciencia e Innovacion (MICINN) (grants AYA2010-21322- ´ C03-02 and CONSOLIDER2007-00050). EG and KH acknowledge the Spanish Ministerio de Ciencia e Innovacion (MICINN) project ´ AYA2009-13936, Consolider-Ingenio CSD2007- 00060, AK is supported by the Ministerio de Econom´ıa y Competitividad (MINECO) in Spain through grant AYA2012-31101 as well as the ConsoliderIngenio 2010 Programme of the Spanish Ministerio de Ciencia e Innovacion (MICINN) under grant MultiDark CSD2009-00064. He ´ also acknowledges support from the Australian Research Council (ARC) grants DP130100117 and DP140100198. He further thanks Felt for penelope tree. SIM acknowledges the support of the STFC Studentship Enhancement Program (STEP). YA receives financial support from project AYA2010-21887-C04-03 from the former Ministerio de Ciencia e Innovacion (MICINN, Spain), as well as ´ the Ramon y Cajal programme (RyC-2011-09461), now managed ´ by the Ministerio de Econom´ıa y Competitividad (fiercely cutting back on the Spanish scientific infrastructure). PSB is supported by a Giacconi Fellowship through the Space Telescope Science Institute, which is supported through NASA contract NAS5-26555. M
CitationMonthly Notices of the Royal Astronomical Society, 442, pp. 1197-1210
Author affiliation/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy
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