Ripples in Spacetime from Broken Supersymmetry

Article
Report number	arXiv:2011.13949
Title	Ripples in Spacetime from Broken Supersymmetry
Author(s)	Craig, Nathaniel (UC, Santa Barbara) ; Levi, Noam (Tel Aviv U.) ; Mariotti, Alberto (Brussels U., IIHE ; Intl. Solvay Inst., Brussels) ; Redigolo, Diego (CERN ; INFN, Florence)
Publication	2021-02-22
Imprint	2020-11-27
Number of pages	66
Note	66 pages latex, fifteen figures incorporated
In:	JHEP 2102 (2021) 184
DOI	10.1007/JHEP02(2021)184
Subject category	hep-th ; Particle Physics - Theory ; hep-ph ; Particle Physics - Phenomenology
Abstract	We initiate the study of gravitational wave (GW) signals from first-order phase transitions in supersymmetry-breaking hidden sectors. Such phase transitions often occur along a pseudo-flat direction universally related to supersymmetry (SUSY) breaking in hidden sectors that spontaneously break $R$-symmetry. The potential along this pseudo-flat direction imbues the phase transition with a number of novel properties, including a nucleation temperature well below the scale of heavy states (such that the temperature dependence is captured by the low-temperature expansion) and significant friction induced by the same heavy states as they pass through bubble walls. In low-energy SUSY-breaking hidden sectors, the frequency of the GW signal arising from such a phase transition is guaranteed to lie within the reach of future interferometers given existing cosmological constraints on the gravitino abundance. Once a mediation scheme is specified, the frequency of the GW peak correlates with the superpartner spectrum. Current bounds on supersymmetry are compatible with GW signals at future interferometers, while the observation of a GW signal from a SUSY-breaking hidden sector would imply superpartners within reach of future colliders.
Copyright/License	publication: © 2021-2024 The Authors (License: CC-BY-4.0), sponsored by SCOAP³ preprint: (License: arXiv nonexclusive-distrib 1.0)

$Parameter space of low energy SUSY-breaking models in the $(\sqrt{F},\beta_H)$ plane, with $\alpha=0.3$ and $T_{\text{r.h.}}=\sqrt{F}$ (see Sec.~\eqref{sec:FOPTandGWs} for definitions). The GW reach is computed by requiring the strength of the SGBW signal at the peak frequency to intersect with the PLI curve of a given GW interferometer (see Appendix~\ref{ssub:pli_curves} for details). The {\bf colored regions} show the reach for a signal generated from plasma waves which is generically the dominant one in our scenarios (see Sec.~\ref{sec:FOPTandGWs}). The {\bf cyan region} with $\beta_H<10$ imples a large fine-tuning in our setups (see discussion around Eq.~\eqref{eq:betaFT}, the parametric discussion in Sec.~\ref{sec:anatomy} and the explicit evaluation in the models of Sec.~\ref{sec:models}). In the {\bf red shaded} region gravitino pair production is excluded by a $\gamma+\text{MET}$ search at LEP with $\mathcal{L}=0.24\text{ fb}^{-1}$~\cite{Brignole:1997sk}, the gray region is excluded by ATLAS bounds $j+\text{MET}$ at $\sqrt{s}=8\text{ TeV}$ and $\mathcal{L}=10.5\text{ fb}^{-1}$~\cite{Brignole:1998me,Maltoni:2015twa}. The {\bf dotted gray} and {\bf dotted red} lines are the projection of the $\gamma+\text{MET}$ reach at FCC-hh with $\sqrt{s}=100\text{ TeV}$ and $\mathcal{L}=30\text{ ab}^{-1}$ and a future high energy lepton collider (HELC) with $\sqrt{s}=30\text{ TeV}$ and $\mathcal{L}=100\text{ ab}^{-1}$. The {\bf dark green shaded} region with {\bf dark green arrows} indicates the bound on the SUSY-breaking scale derived from the LHC bound on gluinos $m_{\tilde{g}}$ 2\text{ TeV}$, requiring the messenger sector to be perturbative. The two {\bf dark green} and {\bf light green} bands show the impact of the present LHC bounds~\cite{Aaboud:2018doq,Aaboud:2018mna,ATLAS:2019vcq,ATLAS-CONF-2020-047} and the future FCC-hh reach on gluinos~\cite{Arkani-Hamed:2015vfh} for perturbative messenger sectors with $g_M\in(0.01,0.1)$ (see Eq.~\eqref{eq:gluinomass} for a definition of $g_M$). The region between these two lines will be naturally populated by the model discussed in Sec.~\ref{sec:FD} and Sec.~\ref{sec:gaugemediation}. The {\bf dark blue arrows} on the right hand side shows the \emph{ultralight gravitino window} where $m_{3/2}\leq 16\text{ eV}$ and the gravitino does not poses any cosmological challenge with $\kappa=1$ (see Eq.~\eqref{eq:m32} for a definition) and the \emph{gravitino dark matter window} where $\kappa\ll1$ and the full gravitino mass is heavier than the gravitino mass contribution set by $\sqrt{F}$. The {\bf dark cyan} region marked as \emph{inaccessible in LESB} is always excluded by a combination of gravitino overabundance~\cite{Hall:2013uga} and BBN constraints~\cite{Jedamzik:2006xz} (see Sec.~\ref{sec:pheno} for details)." width="200px"/> $The reach of future GW interferometers in the $(\alpha,\beta_H)$ plane for two different scales of FOPTs, assuming the signal is dominated by sound waves given by Eq.~\ref{eq:swsignal}. The shaded regions are obtain by requiring the signal at the peak in Eq.~\eqref{eq:poweratpeak} to be inside the PLI curve of a given experiment. {\bf Left:} $T_n=10^5\text{ GeV}$ corresponds to LESB scenarios with an ultralight gravitino LSP and $\kappa=1$. {\bf Right:} $T_n=10^7\text{ GeV}$ corresponds to LESB scenarios with gravitino DM and $\kappa\ll1$. We will exhibit calculable scenarios of this type in Sec.~\ref{sec:models}.$ $The reach of future GW interferometers in the $(\alpha,\beta_H)$ plane for two different scales of FOPTs, assuming the signal is dominated by sound waves given by Eq.~\ref{eq:swsignal}. The shaded regions are obtain by requiring the signal at the peak in Eq.~\eqref{eq:poweratpeak} to be inside the PLI curve of a given experiment. {\bf Left:} $T_n=10^5\text{ GeV}$ corresponds to LESB scenarios with an ultralight gravitino LSP and $\kappa=1$. {\bf Right:} $T_n=10^7\text{ GeV}$ corresponds to LESB scenarios with gravitino DM and $\kappa\ll1$. We will exhibit calculable scenarios of this type in Sec.~\ref{sec:models}.$ Show more plots

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