002783494 001__ 2783494
002783494 005__ 20211217100110.0
002783494 0248_ $$aoai:cds.cern.ch:2783494$$pcerncds:FULLTEXT$$pcerncds:CERN:FULLTEXT$$pcerncds:CERN
002783494 037__ $$9arXiv$$aarXiv:2110.01582$$chep-ex
002783494 035__ $$9arXiv$$aoai:arXiv.org:2110.01582
002783494 035__ $$9Inspire$$aoai:inspirehep.net:1938284$$d2021-10-13T18:18:49Z$$h2021-10-14T02:30:01Z$$mmarcxml$$ttrue$$uhttps://inspirehep.net/api/oai2d
002783494 035__ $$9Inspire$$a1938284
002783494 041__ $$aeng
002783494 100__ $$aChiles, [email protected]$$uNIST, Boulder$$vNational Institute of Standards and Technology, 325 Broadway, Boulder, CO 80305
002783494 245__ $$9arXiv$$aFirst Constraints on Dark Photon Dark Matter with Superconducting Nanowire Detectors in an Optical Haloscope
002783494 269__ $$c2021-10-04
002783494 300__ $$a14 p
002783494 520__ $$9arXiv$$aUncovering the nature of dark matter is one of the most important goals of particle physics. Light bosonic particles, such as the dark photon, are well-motivated candidates: they are generally long-lived, weakly-interacting, and naturally produced in the early universe. In this work, we report on LAMPOST (Light $A$' Multilayer Periodic Optical SNSPD Target), a proof-of-concept experiment searching for dark photon dark matter in the $\sim$ eV mass range, via coherent absorption in a multi-layer dielectric haloscope. Using a superconducting nanowire single-photon detector (SNSPD), we achieve efficient photon detection with a dark count rate (DCR) of $\sim$ 6 x 10$^{6}$ counts/sec. The observed count rate in our detector differed insignificantly from a reference SNSPD, enabling our prototype experiment to set new limits for the dark photon dark matter kinetic mixing parameter $\epsilon$ $_{\sim}^{<}$ 10$^{-12}$ and find no evidence for dark photon dark matter over a mass range of $\sim$ 0.7-0.8 eV (photon wavelength $\sim$ 1550-1770 nm). This performance demonstrates that, with feasible upgrades, our architecture could probe significant new parameter space for dark photon and axion dark matter in the meV to 10 eV mass range.
002783494 540__ $$3preprint$$aarXiv nonexclusive-distrib 1.0$$uhttp://arxiv.org/licenses/nonexclusive-distrib/1.0/
002783494 595_D $$aG$$d2021-10-13$$sfullabs
002783494 65017 $$2arXiv$$aphysics.ins-det
002783494 65017 $$2SzGeCERN$$aDetectors and Experimental Techniques
002783494 65017 $$2arXiv$$ahep-ph
002783494 65017 $$2SzGeCERN$$aParticle Physics - Phenomenology
002783494 65017 $$2arXiv$$aastro-ph.CO
002783494 65017 $$2SzGeCERN$$aAstrophysics and Astronomy
002783494 65017 $$2arXiv$$ahep-ex
002783494 65017 $$2SzGeCERN$$aParticle Physics - Experiment
002783494 690C_ $$aCERN
002783494 690C_ $$aPREPRINT
002783494 700__ $$aCharaev, [email protected]$$uMIT$$vMassachusetts Institute of Technology, 50 Vassar Street, Cambridge, MA 02139, USA
002783494 700__ $$aLasenby, Robert$$uStanford U., ITP$$vStanford Institute for Theoretical Physics, Stanford University, Stanford, CA 94305, USA
002783494 700__ $$aBaryakhtar, Masha$$uNew York U., CCPP$$uWashington U., Seattle$$vDepartment of Physics, University of Washington, Seattle WA 98195, USA$$vNew York University CCPP, New York, NY, 10003, United States
002783494 700__ $$aHuang, Junwu$$uPerimeter Inst. Theor. Phys.$$vPerimeter Institute for Theoretical Physics, Waterloo, Ontario, N2L 2Y5, Canada
002783494 700__ $$aRoshko, Alexana$$uNIST, Boulder$$vNational Institute of Standards and Technology, 325 Broadway, Boulder, CO 80305
002783494 700__ $$aBurton, George$$uNIST, Boulder$$vNational Institute of Standards and Technology, 325 Broadway, Boulder, CO 80305
002783494 700__ $$aColangelo, Marco$$uMIT$$vMassachusetts Institute of Technology, 50 Vassar Street, Cambridge, MA 02139, USA
002783494 700__ $$aVan Tilburg, Ken$$uNew York U., CCPP$$uFlatiron Inst., New York$$vNew York University CCPP, New York, NY, 10003, United States$$vCenter for Computational Astrophysics, Flatiron Institute, New York, NY 10010, USA
002783494 700__ $$aArvanitaki, Asimina$$uPerimeter Inst. Theor. Phys.$$vPerimeter Institute for Theoretical Physics, Waterloo, Ontario, N2L 2Y5, Canada
002783494 700__ $$aNam, Sae Woo$$uNIST, Boulder$$vNational Institute of Standards and Technology, 325 Broadway, Boulder, CO 80305
002783494 700__ $$aBerggren, Karl K.$$uMIT$$vMassachusetts Institute of Technology, 50 Vassar Street, Cambridge, MA 02139, USA
002783494 8564_ $$82326311$$s599013$$uhttps://cds.cern.ch/record/2783494/files/box.png$$y00005 (a) Assembled haloscope core with fiber collimator. Inset: backside of dielectric stack prior to core assembly. (b) A haloscope enclosure mounted on the 300 mK stage of cryostat. (c) View of light-tight enclosure.
002783494 8564_ $$82326312$$s214271$$uhttps://cds.cern.ch/record/2783494/files/raytracing.png$$y00007 (a-f) Non-sequential ray tracing results for various misalignment configurations, showing ray intercepts at the plane of the detector. Fifty-thousand rays were used for ray-tracing. The detector's active area is indicated by the white boxes. Coloration represents incoherent intensity on the plane of the detector determined by ray intercepts. Inset: coordinate system used for displacements. (g) Ray tracing of the improved optical design using a longer focal length lens which achieves 93\% OCE. Inset: Ray intercepts at the detector plane for the improved design.
002783494 8564_ $$82326313$$s8736$$uhttps://cds.cern.ch/record/2783494/files/pfig2.png$$y00002 Calculated time-averaged power $P$ absorbed from dark photon DM with mass $m_{A'}$ by the layered target, normalised to the power $P_0$ absorbed by a uniform mirror. The thin purple curve shows the power absorbed by a target with parameters given by their respective measured central values, while the magenta curve shows the minimum power obtained by varying the parameters within measurement uncertainties (see Methods). The substrate thickness is assumed to physically vary by $\gtrsim 10 {\rm \, \mu m}$ over the target area; this accounts for the magenta curve sometimes falling above the purple curve of constant substrate thickness.
002783494 8564_ $$82326314$$s128942$$uhttps://cds.cern.ch/record/2783494/files/apparatus_small.png$$y00001 The LAMPOST prototype haloscope apparatus. (a) Exploded view with element details. Inset: assembled view. b) Schematic cross-sectional and top-views of the dielectric stack target responsible for DM-signal photon conversion, with designed values of different dimensions, \textit{g}: Aperture diameter, 10 mm; \textit{d}: Wafer diameter, 52 mm; \textit{t\textsubscript{s}}: Substrate thickness, 525 $\mu$m; \textit{t\textsubscript{asi}}: Amorphous silicon layer thickness, $\sim$292 nm; \textit{t\textsubscript{s}}:~SiO\textsubscript{2} layer thickness, $\sim$548 nm. See Supplementary Materials for details of the film characterization.
002783494 8564_ $$82326315$$s20466$$uhttps://cds.cern.ch/record/2783494/files/kfig3.png$$y00003 LAMPOST constraints on dark photon DM with mass $m_{A'}$ and kinetic mixing $\epsilon$. The magenta shaded region shows the $90\%$ limit set by our experiment. The dashed curve shows the $90\%$ limit obtained without background subtraction. The thin purple curve corresponds to the reach of an equivalent experiment with an improved SDE of $90\%$. Existing limits on dark photon DM from the FUNK~\cite{PhysRevD.102.042001}, SENSEI~\cite{PhysRevLett.125.171802} and Xenon10~\cite{PhysRevLett.107.051301} experiments and from the non-detection of Solar dark photons by Xenon1T~\cite{PhysRevD.102.115022} are shown in gray.
002783494 8564_ $$82326316$$s41591$$uhttps://cds.cern.ch/record/2783494/files/physics_sketch.png$$y00000 Sketch of the LAMPOST concept. The dark photon dark matter field $A'$ converts to photons in a layered dielectric target. These photons are focused by a lens onto a small, low-noise SNSPD detector.
002783494 8564_ $$82326317$$s68985$$uhttps://cds.cern.ch/record/2783494/files/stack_stem.png$$y00004 STEM and SEM images of the fabricated stack. (a) Top-view showing numerous small pits occupying a small portion of the surface area. (b) Image of the entire stack, showing one pitted area extending through several layers. (c) High-magnification TEM image of one amorphous silicon layer.
002783494 8564_ $$82326318$$s51921$$uhttps://cds.cern.ch/record/2783494/files/Long_time_all_2021.png$$y00011 Experimental results of long-duration integration experiment with large-area SNSPDs mounted into a haloscope. Red points correspond to the signal obtained from a device aligned with the lens, while black points show counts taken from a reference detector placed far from focus of the target.
002783494 8564_ $$82326319$$s2005188$$uhttps://cds.cern.ch/record/2783494/files/2110.01582.pdf$$yFulltext
002783494 8564_ $$82326320$$s48951$$uhttps://cds.cern.ch/record/2783494/files/SNSPD_REF.png$$y00009 Normalized count rate as a function of the absolute bias current measured at 1550 nm for the primary SNSPD and reference SNSPD with identical geometry. Inset: DCR as a function of the bias current taken from both detectors.
002783494 8564_ $$82326321$$s42391$$uhttps://cds.cern.ch/record/2783494/files/PCR_1550_1700nm.png$$y00010 Normalized count rate as a function of the absolute bias current measured at 1550 nm (open red dots) and 1700 nm (green dots) wavelengths. Data was taken at 300 mK of bath temperature. The SNSPDs show pronounced saturation at both wavelengths. Inset: Comparison of DCRs with optical fiber connected (filled circles) and disconnected (open circles).
002783494 8564_ $$82326322$$s378987$$uhttps://cds.cern.ch/record/2783494/files/SEM.png$$y00008 Scanning electron micrograph of nanowires after fabrication. Scale bar: 1 $\mu$m
002783494 8564_ $$82326323$$s35212$$uhttps://cds.cern.ch/record/2783494/files/alignmentmethod.png$$y00006 Optical system used in ray-tracing and alignment planning. (a) Propagation of the red alignment beam through the aperture, resulting in a position of best focus \textit{z\textsubscript{align}} for the detector during the initial alignment. (b) Effective behavior of the DM signal photon source as an annulus with a modified position of best focus ($\ z_{align}-dz_{signal}$).
002783494 960__ $$a11
002783494 980__ $$aPREPRINT