Abstract
ABSTRACT Observations show that stellar streams originating in satellite dwarf galaxies are frequent in the Universe. While such events are predicted by theory, it is not clear how many of the streams that are generated are washed out afterwards to the point in which it is impossible to detect them. Here, we study how these diffusion times are affected by the fact that typical gravitational potentials of the host galaxies can sustain chaotic orbits. We do this by comparing the behaviour of simulated stellar streams that reside in chaotic or non-chaotic regions of the phase space. We find that chaos does reduce the time interval in which streams can be detected. By analysing detectability criteria in configuration and velocity space, we find that the impact of these results on the observations depends on the quality of both the data and the underlying stellar halo model. For all the stellar streams, we obtain a similar upper limit to the detectable mass.
Highlights
Observations show that the destruction of dwarf satellite galaxies due to tidal fields associated to the gravitational potential of the host galaxy is frequent (Mantha et al 2018; Conselice et al 2009; Kauffmann & White 1993)
We summarize the results that we obtained from our simulations on the evolution of the streams an the impact of chaos on our ability to detect them
In Appendix A we prove with high significance the existence of a weak correlation between L and rmin for a large sample of test orbits, which in combination with the rs–t f correlation implies the existence of a weak L–t f correlation
Summary
Observations show that the destruction of dwarf satellite galaxies due to tidal fields associated to the gravitational potential of the host galaxy is frequent (Mantha et al 2018; Conselice et al 2009; Kauffmann & White 1993). Stellar streams are unavoidable consequences, either permanent or transitory, of this type of interaction (Morales et al 2018; Shipp et al 2018; Martınez-Delgado et al 2008). Davies & Wright 1977; Wright 1972; Helmi et al 1999; Helmi & White 1999), there is still much to be done on the application of stellar streams to galactic archaeology and cosmology. The properties of streams can be used to put constraints on the structure and evolution of the stellar and dark matter haloes of galaxies (Helmi et al 2017; Malhan et al 2018; Bovy 2016) as well as on the nature of the dark matter particles themselves (Banik et al 2018). Hendel & Johnston (2015) and Karademir et al (2019) have demonstrated that it is
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
