First Star-Forming Structures in Fuzzy Cosmic Filaments

Philip Mocz, Anastasia Fialkov, Mark Vogelsberger, Fernando Becerra, Mustafa A. Amin, Sownak Bose, Michael Boylan-Kolchin, Pierre Henri Chavanis, Lars Hernquist, Lachlan Lancaster, Federico Marinacci, Victor H. Robles, Jesús Zavala

Rannsóknarafurð: Framlag til fræðitímaritsGreinritrýni

40 Tilvitnanir (Scopus)


In hierarchical models of structure formation, the first galaxies form in low-mass dark matter potential wells, probing the behavior of dark matter on kiloparsec scales. Even though these objects are below the detection threshold of current telescopes, future missions will open an observational window into this emergent world. In this Letter, we investigate how the first galaxies are assembled in a "fuzzy" dark matter (FDM) cosmology where dark matter is an ultralight ∼10-22 eV boson and the primordial stars are expected to form along dense dark matter filaments. Using a first-of-its-kind cosmological hydrodynamical simulation, we explore the interplay between baryonic physics and unique wavelike features inherent to FDM. In our simulation, the dark matter filaments show coherent interference patterns on the boson de Broglie scale and develop cylindrical solitonlike cores, which are unstable under gravity and collapse into kiloparsec-scale spherical solitons. Features of the dark matter distribution are largely unaffected by the baryonic feedback. On the contrary, the distributions of gas and stars, which do form along the entire filament, exhibit central cores imprinted by dark matter - a smoking gun signature of FDM.

Upprunalegt tungumálEnska
Númer greinar141301
FræðitímaritPhysical Review Letters
Númer tölublaðs14
ÚtgáfustaðaÚtgefið - 2 okt. 2019


Funding Information:
We thank Jerry Ostriker, Mariangela Lisanti, David Spergel, Scott Tremaine, James Bullock, Frenk van den Bosch, Paul Shapiro, Jim Stone, Vasily Belokurov, and Aaron Szasz for discussions related to an earlier version of this Letter. We would also like to thank the anonymous referees who have helped improve the content and presentation of the Letter. The authors acknowledge the Texas Advanced Computing Center at The University of Texas at Austin for providing high-performance computing resources that have contributed to the research results reported within this Letter (XSEDE Allocation TG-AST170020). Some computations were run on the Odyssey cluster supported by the FAS Division of Science, Research Computing Group at Harvard University. Support (P. M.) for this work was provided by NASA through Einstein Postdoctoral Fellowship Grant No. PF7-180164 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under Contract No. NAS8-03060. A. F. is supported by the Royal Society (URF). M. A. is supported by DOE Award No. DE-SC0018216 and thanks the Yukawa Institute for Theoretical Physics at Kyoto University, where this work was completed during the YITP-T-19-02 on “Resonant instabilities in cosmology.” S. B. acknowledges support from Harvard University through the ITC Fellowship. M. B. K. acknowledges support from NSF Grant No. AST-1517226 and CAREER Grant No. AST-1752913 and from NASA Grant No. NNX17AG29G, and HST-AR-14282, HST-AR-14554, HST-AR-15006, and HST-GO-14191 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA Contract No. NAS5-26555. F. M. is supported by the program “Rita Levi Montalcini” of the Italian MIUR. V. H. R. was supported by a Gary A. McCue Postdoctoral Fellowship. J. Z. acknowledges support by a Grant of Excellence from the Icelandic Research Fund (Grant No. 173929-051).

Publisher Copyright:
© 2019 American Physical Society.


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