Using an InGrid Detector to Search for Solar Chameleons with CAST

Desch, Klaus; Lupberger, Michael; Kaminski, Jochen; Krieger, Christoph

Contribution to a conference proceedings/Contribution to a book

PUBDB-2017-00125

Using an InGrid Detector to Search for Solar Chameleons with CAST

Desch, K. ; Kaminski, J. ; Krieger, C. ; Lupberger, M.

2015
Verlag Deutsches Elektronen-Synchrotron Hamburg
ISBN: 978-3-935702-43-0

Desch, Klaus "Using an InGrid Detector to Search for Solar Chameleons with CAST" in Proceedings, 11th Patras Workshop on Axions, WIMPs and WISPs (Axion-WIMP 2015) / Irastorza, Igor G., Redondo, Javier, Carmona, José Manuel, Cebrian, Susana, Dafni, Theopisti, Iguaz, Francisco J., Luzon, Gloria (eds.), Verlag Deutsches Elektronen-Synchrotron : 2015 ; AXION-WIMP 2015 : 11th Patras Workshop on Axions, WIMPs and WISPs, 2015-06-22 - 2015-06-26, Zaragoza
11th Patras Workshop on Axions, WIMPs and WISPs, AXION-WIMP 2015, Zaragoza, Spain, 22 Jun 2015 - 26 Jun 2015 Hamburg : Verlag Deutsches Elektronen-Synchrotron, DESY-PROC 35-38 (2015) [10.3204/DESY-PROC-2015-02/desch_klaus]

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Please use a persistent id in citations: doi:10.3204/DESY-PROC-2015-02/desch_klaus

Abstract: We report on the construction, operation experience, and preliminary background measurements of an InGrid detector, i.e.~a MicroMegas detector with CMOS pixel readout. The detector was mounted in the focal plane of the Abrixas X-Ray telescope at the CAST experiment at CERN. The detector is sensitive to soft X-Rays in a broad energy range \J{(0.3--10)~keV } and thus enables the search for solar chameleons. Smooth detector operation during CAST data taking in autumn 2014 has been achieved. \J{A p}reliminary analysis of background data indicates a background rate of \J{(1--5)}$ \times 10^{-5}~\mathrm{keV}^{-1}\mathrm{cm}^{-2}\mathrm{s}^{-1}$ above 2~keV and $\sim 3\times 10^{-4}~\mathrm{keV}^{-1}\mathrm{cm}^{-2}\mathrm{s}^{-1}$ around 1~keV. An expected limit of $\beta_\gamma \lesssim 5\times 10^{10}$ on the chameleon photon coupling is estimated in case of absence of an excess in solar tracking data. We also discuss the prospects for future operation of the detector.

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