Abstract
Recently, a considerable amount of attention has been given to the search for ultralight dark matter by measuring the oscillating length changes in the arm cavities of gravitational wave detectors. Although gravitational wave detectors are extremely sensitive for measuring the differential arm length changes, the sensitivity to dark matter is largely attenuated, as the effect of dark matter is mostly common to arm cavity test masses. Here, we propose to use auxiliary length channels, which measure the changes in the power and signal recycling cavity lengths and the differential Michelson interferometer length. The sensitivity to dark matter can be enhanced by exploiting the fact that auxiliary interferometers are more asymmetric than two arm cavities. We show that the sensitivity to $U(1)_{B-L}$ gauge boson dark matter with masses below $7\times 10^{-14}$ eV can be greatly enhanced when our method is applied to a cryogenic gravitational wave detector KAGRA, which employs sapphire test masses and fused silica auxiliary mirrors. We show that KAGRA can probe more than an order of magnitude of unexplored parameter space at masses around $1.5 \times 10^{-14}$ eV, without any modifications to the existing interferometer.
Highlights
Despite strong observational evidence for the existence of dark matter, its identity and properties remain a mystery
We show that the sensitivity to Uð1ÞB−L gauge boson dark matter with masses below 7 × 10−14 eV can be greatly enhanced when our method is applied to a cryogenic gravitational wave detector KAGRA, which employs sapphire test masses and fused silica auxiliary mirrors
We focus on the massive vector field coupled with B or B − L current JνD, whose Lagrangian is given by where Fμν ≡ ∂μAν − ∂νAμ is the field strength, mA is the mass of the vector field, and εD is the gauge coupling constant normalized to the electromagnetic coupling constant e
Summary
Despite strong observational evidence for the existence of dark matter, its identity and properties remain a mystery. Several proposals have been made to search for such vector fields by measuring the oscillating forces acting on mirrors with laser interferometers [15,16,17,18] Among these proposals to probe various ultralight dark matter candidates, the use of gravitational wave detectors is often ment considered, owing to their sensitivity, on the order of e1x0t−r2e0mmel=yphffiHiffigffiffizffihffi displaceat around. We especially consider vector fields and show that the sensitivity can be improved compared to the search using the main differential arm length channel, when the main test masses and auxiliary mirrors have different charges to which the dark matter is coupled This condition is satisfied for the coupling between the Uð1ÞB−L gauge field and cryogenic gravitational wave detectors such as KAGRA, which employ sapphire test masses and fused silica auxiliary mirrors.
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