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\section*{fuzzy dark matter}

\hypertarget{context}{}\subsubsection*{{Context}}\label{context}

\hypertarget{physics}{}\paragraph*{{Physics}}\label{physics}

[[!include physicscontents]]

\hypertarget{fields_and_quanta}{}\paragraph*{{Fields and quanta}}\label{fields_and_quanta}

[[!include fields and quanta - table]]

\hypertarget{contents}{}\section*{{Contents}}\label{contents}

\noindent\hyperlink{idea}{Idea}\dotfill \pageref*{idea} \linebreak
\noindent\hyperlink{References}{References}\dotfill \pageref*{References} \linebreak
\noindent\hyperlink{original_articles}{Original articles}\dotfill \pageref*{original_articles} \linebreak
\noindent\hyperlink{mond_phenomenology}{MOND Phenomenology}\dotfill \pageref*{mond_phenomenology} \linebreak
\noindent\hyperlink{ReferencesTensionWithHydrogenLineSpectroscopy}{Tension with 21cm hydrogen line}\dotfill \pageref*{ReferencesTensionWithHydrogenLineSpectroscopy} \linebreak
\noindent\hyperlink{review}{Review}\dotfill \pageref*{review} \linebreak
\noindent\hyperlink{numerics_and_experiment}{Numerics and experiment}\dotfill \pageref*{numerics_and_experiment} \linebreak


\hypertarget{idea}{}\subsection*{{Idea}}\label{idea}

A model for [[dark matter]] made up of massive but extremely light [[particles]], whose [[de Broglie wavelength]] is at the scale of galaxies.

The idea is that on scales above that of galaxies, the predictions of fuzzy dark matter agree with the standard cold dark matter models that work exceptionally well on [[cosmology|cosmological scales]], while on scales of the size of galaxies the [[quantum physics|quantum]] properties of these light particles become relevant and change their effect just so as to fix the problems (see also [[MOND]]) that standard cold dark matter models have on these scales.

A natural candidate for such ultra-light particles are [[axions]].

This kind of model was brought up independently by several groups of authors (see \hyperlink{Lee17}{Lee 17} for historical survey) with early precursors going back as far as (\hyperlink{BaldeschiGelminiRuffini83}{Baldeschi-Gelmini-Ruffini 83}), and accordingly goes by a number of different names, including the following:

\begin{itemize}%
\item \emph{[[Bose-Einstein condensate]] (BEC) dark matter} (\hyperlink{Sin92}{Sin 92}, \hyperlink{SikivieYang09}{Sikivie-Yang 09})


\item \emph{[[superfluid]] dark matter} (\hyperlink{BerezhianiKhoury15}{Berezhiani-Khoury 15}, \hyperlink{Khoury16}{Khoury 16})


\item \emph{fuzzy dark matter} (\hyperlink{WuBarkanaGruzinov00}{Wu-Barkana-Gruzinov 00})


\item \emph{ultra-light [[axion]]} (\hyperlink{ErkenSikivieTamYang12}{Erken-Sikivie-Tam-Yang 12})


\item \emph{wave dark matter}


\item \emph{repulsive dark matter}



\end{itemize}
and more.

The suggestion that fuzzy dark matter induces the observed almost-flat galactic rotation curves (``[[MOND]]'') seems to go back to (\hyperlink{Sin92}{Sin 92}). Further pointers are in (\hyperlink{Lee17}{Lee 17, p. 3}):

\begin{quote}%
There are many works explaining the rotation curves of dwarf 17, 23, 69, and large galaxies 29, 43, 70–78 in this model.


\end{quote}
More recently, detection of the [[21cm hydrogen line]] from cosmic dawn indicates that star formation set in earlier than compatible with fuzzy dark matter models (\hyperlink{Nebrin17}{Nebrin 17}, \hyperlink{NebrinGharaMellema18}{Nebrin-Ghara-Mellema 18}). This would rule out substantial contributions of fuzzy dark matter.



\hypertarget{References}{}\subsection*{{References}}\label{References}

\hypertarget{original_articles}{}\subsubsection*{{Original articles}}\label{original_articles}

Early precursors of the idea include

\begin{itemize}%
\item M. R. Baldeschi, G. B. Gelmini, and R. Ruffini, Physics Letters B 122, 221 (1983).

\end{itemize}
The role of the [[Bose-Einstein condensate]] of [[axions]] on galactic scales was considered in

\begin{itemize}%
\item Sang-Jin Sin, \emph{Late time Cosmological Phase Transition and Galactic Halo as Bose-liquid}, Phys.Rev.D50:3650-3654,1994 (\href{https://arxiv.org/abs/hep-ph/9205208}{arXiv:hep-ph/9205208})


\item [[Pierre Sikivie]], Q. Yang, \emph{Bose-Einstein Condensation of Dark Matter Axions}, Phys.Rev.Lett.103:111301, 2009 (\href{https://arxiv.org/abs/0901.1106}{arXiv:0901.1106})


\item O. Erken, [[Pierre Sikivie]], H. Tam, Q. Yang, \emph{Cosmic axion thermalization}, Phys. Rev. D 85, 063520 2012 (\href{https://arxiv.org/abs/1111.1157}{arXiv:1111.1157})



\end{itemize}
The proposal in the guise of ``fuzzy dark matter'' is originally due to

\begin{itemize}%
\item Wayne Hu, Rennan Barkana, Andrei Gruzinov, \emph{Cold and Fuzzy Dark Matter}, Phys.Rev.Lett. 85 (2000) 1158-1161 (\href{https://arxiv.org/abs/astro-ph/0003365}{arXiv:astro-ph/0003365})

\end{itemize}
A detailed discussion is in

\begin{itemize}%
\item [[Lam Hui]], [[Jeremiah Ostriker]], [[Scott Tremaine]], [[Edward Witten]], \emph{On the hypothesis that cosmological dark matter is composed of ultra-light bosons}, Phys. Rev. D 95, 043541 (2017) (\href{https://arxiv.org/abs/1610.08297}{arXiv:1610.08297})

\end{itemize}
Some thoughts on the quantum [[measurement problem]] for fuzzy DM particles with huge macroscopic [[Compton wavelengths]] is in

\begin{itemize}%
\item Adam D. Helfer, \emph{Quantum measurement and fuzzy dark matter} (\href{https://arxiv.org/abs/1809.04946}{arXiv:1809.04946})

\end{itemize}
\hypertarget{mond_phenomenology}{}\subsubsection*{{MOND Phenomenology}}\label{mond_phenomenology}

Discussion of how [[superfluid]] aspects of [[axion|axionic]] fuzzy dark matter reproduce [[MOND]] [[phenomenology]] is in

\begin{itemize}%
\item [[Lasha Berezhiani]], [[Justin Khoury]], \emph{Theory of Dark Matter Superfluidity}, Phys. Rev. D 92, 103510 (2015) (\href{https://arxiv.org/abs/1507.01019}{arXiv:1507.01019})


\item [[Justin Khoury]], \emph{Another Path for the Emergence of Modified Galactic Dynamics from Dark Matter Superfluidity}, Phys. Rev. D 93, 103533 (2016) (\href{https://arxiv.org/abs/1602.05961}{arXiv:1602.05961})


\item JiJi Fan, \emph{Ultralight Repulsive Dark Matter and BEC} (\href{https://arxiv.org/abs/1603.06580}{arXiv:1603.06580})


\item Andrea Addazi, Antonino Marciano, \emph{UV completion of a theory of Superfluid Dark Matter} (\href{https://arxiv.org/abs/1801.04083}{arXiv:1801.04083})



\end{itemize}
\hypertarget{ReferencesTensionWithHydrogenLineSpectroscopy}{}\subsubsection*{{Tension with 21cm hydrogen line}}\label{ReferencesTensionWithHydrogenLineSpectroscopy}

Strong constraints on fuzzy dark matter from observation of the cosmic [[21cm hydrogen line]] are claimed and discussed in

\begin{itemize}%
\item Adam Lidz, [[Lam Hui]], \emph{The Implications of a Pre-reionization 21 cm Absorption Signal for Fuzzy Dark Matter}, Phys. Rev. D 98, 023011 (2018) (\href{https://arxiv.org/abs/1805.01253}{arXiv:1805.01253})


\item Olof Nebrin, \emph{Cosmic Dawn in a Fuzzy Universe: Constraining the nature of Dark Matterwith 21 cm Cosmology}, Stockholm 2017 (\href{http://www.diva-portal.org/smash/record.jsf?pid=diva2%3A1195402&dswid=-8037}{diva2:1195402}, \href{http://su.diva-portal.org/smash/record.jsf?pid=diva2%3A1195402&dswid=6755}{urn:nbn:se:su:diva-154861})


\item Olof Nebrin, Raghunath Ghara, Garrelt Mellema, \emph{Fuzzy Dark Matter at Cosmic Dawn: New 21-cm Constraints} (\href{https://arxiv.org/abs/1812.09760}{arXiv:1812.09760}, \href{https://www.reddit.com/r/Physics/comments/a9zeeb/my_first_paper_fuzzy_dark_matter_at_cosmic_dawn/}{reddit})



\end{itemize}
\hypertarget{review}{}\subsubsection*{{Review}}\label{review}

Review includes

\begin{itemize}%
\item David J. E. Marsh, \emph{Axion Cosmology} (\href{https://arxiv.org/abs/1510.07633}{arXiv:1510.07633})


\item Jae-Weon Lee, \emph{Brief History of Ultra-light Scalar Dark Matter Models} (\href{https://arxiv.org/abs/1704.05057}{arXiv:1704.05057})



\end{itemize}
\hypertarget{numerics_and_experiment}{}\subsubsection*{{Numerics and experiment}}\label{numerics_and_experiment}

Comparison to [[experiment]] (observation) is discussed in

\begin{itemize}%
\item Bohua Li, Tanja Rindler-Daller, and Paul R. Shapiro, \emph{Cosmological constraints on Bose-Einstein-condensed scalar field dark matter}, Phys. Rev. D 89, 083536, 2014 (\href{https://arxiv.org/abs/1310.6061}{arXiv:1310.6061})


\item Hsi-Yu Schive, Tzihong Chiueh, Tom Broadhurst, \emph{Cosmic structure as the quantum interference of a coherent dark wave}, Nature Physics 10, 496--499 (2014) (\href{http://www.nature.com/nphys/journal/v10/n7/abs/nphys2996.html}{doi:10.1038/nphys2996})


\item Nilanjan Banik, Adam J. Christopherson, [[Pierre Sikivie]], Elisa Maria Todarello, \emph{New astrophysical bounds on ultralight axionlike particles}, Phys. Rev. D 95, 043542 (2017) (\href{https://arxiv.org/abs/1701.04573}{arXiv:1701.04573})



\end{itemize}
Claim that the galaxy core-cusp problem is not resolved after all is discussed in

\begin{itemize}%
\item Heling Deng, Mark P. Hertzberg, Mohammad Hossein Namjoo, Ali Masoumi, \emph{Can Light Dark Matter Solve the Core-Cusp Problem?} (\href{https://arxiv.org/abs/1804.05921}{arXiv:1804.05921})

\end{itemize}
Computer simulation of [[structure formation]] with fuzzy dark matter:

\begin{itemize}%
\item Philip Mocz et al., \emph{First Star-Forming Structures in Fuzzy Cosmic Filaments}, Phys. Rev. Lett. 123, 141301 – 2019 (\href{https://doi.org/10.1103/PhysRevLett.123.141301}{doi:10.1103/PhysRevLett.123.141301})

\end{itemize}
[[!redirects Bose-Einstein condensate dark matter]] [[!redirects BEC dark matter]]

[[!redirects axion dark matter]]



\end{document}