Single arm interferometry to probe the scalar field dark matter

Abstract

We analyse the interaction of photons with a scalar dark matter field φand we propose to use a single arm interferometer to reveal this interaction and constrain the parameters of the scalar dark matter model. By considering a beam of coherent light and two spatially separated squeezing operations, we show that the interaction of photons with scalar dark matter leads to an observable deviation in the outgoing light state, with respect to free evolution. Therefore the single arm interferometer may yield a novel revelation method for scalar dark matter.

Figures (7)

• Figure 1: (Color online). Schematic depiction of the single-arm interferometer. A coherent laser beam, represented by the quantum state $\ket{\alpha}$, is emitted from the laser source. The beam first undergoes a squeezing operation $\hat{S}(r)$. This is followed by an inverse squeezing (antisqueezing) operation $\hat{S}^{-1}(r)$, which give the state $\ket{\alpha'}$ which is probed by a photodetector ($PD$).
• Figure 2: (Color online). Main picture: plot of $\delta(L)$ as function of $g_\gamma\in [10^{-34}, 10^{-33}] \, \mathrm{eV^{-1}}$ and $m_\phi\in [10^{-20}, 10^{-19}] \, \mathrm{eV}$. In the inset is plotted $\delta(L)$ as function of $g_\gamma\in [10^{-31}, 10^{-30}] \, \mathrm{eV^{-1}}$ and $m_\phi\in [10^{-13}, 10^{-12}] \, \mathrm{eV}$. We consider the arm length $L= 950\;\mathrm{km}$ and the photon wavelength $\lambda=1064\cdot 10^{-9}\;\mathrm{m}$.
• Figure 3: (Color online). Plot of $\frac{\Delta N}{N_{in}}$ as function of $g_\gamma\in [10^{-32}, 10^{-31}] \, \mathrm{eV^{-1}}$, and $m_\phi\in [ 10^{-16}, 2 \cdot 10^{-16}] \, \mathrm{eV}$. Main picture: we consider the squeezing parameter $r=1.7$, which corresponds to $15\; dB$ squeezed states of light. Inset picture: we use $r=0.6$, which is compatible with the value of the squeezing parameter of LIGO experiment. We utilized the same values of $L$ and $\lambda$ considered in Fig. \ref{['fig2']}.
• Figure 4: (Color online). Plot of $\frac{\Delta N}{N_{in}}$ as function of $g_\gamma\in [10^{-32}, 10^{-31}] \, \mathrm{eV^{-1}}$, and $m_\phi\in [0.5\cdot 10^{-18}, 10^{-18}] \, \mathrm{eV}$. Main picture: we consider $r=1.7$. Inset picture: $r=0.6$. The same values of $L$ and $\lambda$ considered in Figs. \ref{['fig2']} and \ref{['fig3']} are used.
• Figure 5: (Color online). Plot of $\frac{\Delta N}{N_{in}}$ as function of $g_\gamma\in [5 \cdot 10^{-35}, 10^{-34}] \, \mathrm{eV^{-1}}$, and $m_\phi\in [ 5\cdot 10^{-22}, 10^{-21}] \, \mathrm{eV}$. These values of the masses are typical of fuzzy cold dark matter Fuzzy. Main picture: we consider $r=1.7$. Inset picture: $r=0.6$. The same values of $L$ and $\lambda$ considered in Figs. \ref{['fig2']} and \ref{['fig3']} are used.