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| 001 | 295130 | ||
| 005 | 20211110133411.0 | ||
| 024 | 7 | _ | |a 10.3204/DESY-PROC-2011-04/povey_rhys |2 datacite_doi |
| 037 | _ | _ | |a PUBDB-2016-01078 |
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| 088 | 1 | _ | |a DESY-PROC-2011-04 |
| 088 | _ | _ | |a DESY-PROC-2011-04 |2 DESY |
| 100 | 1 | _ | |a Povey, Rhys G. |0 P:(DE-HGF)0 |b 0 |
| 111 | 2 | _ | |a 7th Patras Workshop on Axions, WIMPs and WISPs |g AXION-WIMP 2011 |c Mykonos |d 2011-06-27 - 2011-07-01 |w Greece |
| 245 | _ | _ | |a Microwave hidden sector photons at UWA |
| 260 | _ | _ | |c 2011 |b Deutsches Elektronen-Synchrotron, DESY |a Hamburg |
| 300 | _ | _ | |a 64-67 |
| 336 | 7 | _ | |a Conference Paper |0 33 |2 EndNote |
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| 336 | 7 | _ | |a INPROCEEDINGS |2 BibTeX |
| 520 | _ | _ | |a In these proceedings we present the latest progress on our microwave cavity light shining through a wall hidden sector photon experiment, as well as introduce a new method of hidden sector photon detection. Our new experiment uses a high Q superconducting Niobium emitter cavity and moderate Q room temperature copper detector cavity separated by ample shielding. The projected sensitivity of our setup to the kinetic mixing factor is $\chi \sim 1.8 \times 10^{-8}$ at a hidden sector photon mass of 52.1 $\mu$eV. A new technique for detecting hidden sector photons using a threshold crossing is also presented. |
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| 700 | 1 | _ | |a Hartnett, John G. |0 P:(DE-HGF)0 |b 1 |
| 700 | 1 | _ | |a Tobar, Michael E. |0 P:(DE-HGF)0 |b 2 |
| 773 | _ | _ | |a 10.3204/DESY-PROC-2011-04/povey_rhys |
| 787 | 0 | _ | |a Schumann, Marc et.al. |d 2011 |i IsPartOf |0 PUBDB-2016-01039 |r DESY-PROC-2011-04 |t Proceedings, 7th Patras Workshop on Axions, WIMPs and WISPs |
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