Gas-rich and gas-poor structures through the stream velocity effect
Name
1512.06862.pdf
Description
Submitted version
Size
2.4 MB
Format
Adobe PDF
Checksum (MD5)
4a55e01fdb08735c2dcceab304d7fad1
Author(s)
Popa, Cristina
Naoz, Smadar
Marinacci, Federico
Vogelsberger, Mark
Date Issued
2016
Journal
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP)
Citation
Popa, C., et al. "Gas-Rich and Gas-Poor Structures through the Stream Velocity Effect." Monthly Notices of the Royal Astronomical Society 460 2 (2016): 1625-39.
Version
Original manuscript
Abstract
© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Using adiabatic high-resolution numerical simulations, we quantify the effect of the streaming motion of baryons with respect to dark matter at the time of recombination on structure formation and evolution. Formally a second-order effect, the baryonic stream velocity has proven to have significant impact on dark matter halo abundance, as well as on the gas content and morphology of small galaxy clusters. In this work, we study the impact of stream velocity on the formation and gas content of haloes with masses up to 109 M⊙, an order of magnitude larger than previous studies. We find that the non-zero stream velocity has a sizable impact on the number density of haloes with masses ≲ few × 107 M⊙ up to z = 10, the final redshift of our simulations. Furthermore, the gas stream velocity induces a suppression of the gas fraction in haloes, which at z = 10 is ~10 per cent for objects with M ~ 107 M⊙, as well as a flattening of the gas density profiles in the inner regions of haloes. We further identify and study the formation, in the context of a non-zero stream velocity, of moderately long lived gas-dominated structures at intermediate redshifts 10 < z < 20, which Naoz and Narayan have recently proposed as potential progenitors of globular clusters.
MIT Department
MIT Kavli Institute for Astrophysics and Space Research
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Creative Commons Attribution-Noncommercial-Share Alike
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DOI of Published Version
https://doi.org/10.1093/MNRAS/STW1045
