Improved Receiver Noise Calibration for ADMX Axion Search: 4.54 to 5.41 $μ$eV

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Main Authors:	Guzzetti, M., Zhang, D., Goodman, C., Hanretty, C., Sinnis, J., Rosenberg, L. J, Rybka, G., Clarke, John, Siddiqi, I., Chou, A. S., Hollister, M., Knirck, S., Sonnenschein, A., Caligiure, T. J., Gleason, J. R., Hipp, A. T., Sikivie, P., Solano, M. E., Sullivan, N. S., Tanner, D. B., Khatiwada, R., Carosi, G., Du, N., Cisneros, C., Robertson, N., Woollett, N., Duffy, L. D., Boutan, C., Braine, T., Oblath, N. S., Taubman, M. S., Lentz, E., Daw, E. J., Mostyn, C., Perry, M. G., Bartram, C., Dyson, T. A., Kuo, C. L., Ruppert, S., Withers, M. O., Yi, A. K., McAllister, B. T., Buckley, J. H., Gaikwad, C., Hoffman, J., Murch, K., Russell, J., Goryachev, M., Hartman, E., Quiskamp, A., Tobar, M. E.
Format:	Preprint
Published:	2024
Subjects:	High Energy Physics - Experiment
Online Access:	Acceder al recurso
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author	Guzzetti, M. Zhang, D. Goodman, C. Hanretty, C. Sinnis, J. Rosenberg, L. J Rybka, G. Clarke, John Siddiqi, I. Chou, A. S. Hollister, M. Knirck, S. Sonnenschein, A. Caligiure, T. J. Gleason, J. R. Hipp, A. T. Sikivie, P. Solano, M. E. Sullivan, N. S. Tanner, D. B. Khatiwada, R. Carosi, G. Du, N. Cisneros, C. Robertson, N. Woollett, N. Duffy, L. D. Boutan, C. Braine, T. Oblath, N. S. Taubman, M. S. Lentz, E. Daw, E. J. Mostyn, C. Perry, M. G. Bartram, C. Dyson, T. A. Kuo, C. L. Ruppert, S. Withers, M. O. Yi, A. K. McAllister, B. T. Buckley, J. H. Gaikwad, C. Hoffman, J. Murch, K. Russell, J. Goryachev, M. Hartman, E. Quiskamp, A. Tobar, M. E.
author_facet	Guzzetti, M. Zhang, D. Goodman, C. Hanretty, C. Sinnis, J. Rosenberg, L. J Rybka, G. Clarke, John Siddiqi, I. Chou, A. S. Hollister, M. Knirck, S. Sonnenschein, A. Caligiure, T. J. Gleason, J. R. Hipp, A. T. Sikivie, P. Solano, M. E. Sullivan, N. S. Tanner, D. B. Khatiwada, R. Carosi, G. Du, N. Cisneros, C. Robertson, N. Woollett, N. Duffy, L. D. Boutan, C. Braine, T. Oblath, N. S. Taubman, M. S. Lentz, E. Daw, E. J. Mostyn, C. Perry, M. G. Bartram, C. Dyson, T. A. Kuo, C. L. Ruppert, S. Withers, M. O. Yi, A. K. McAllister, B. T. Buckley, J. H. Gaikwad, C. Hoffman, J. Murch, K. Russell, J. Goryachev, M. Hartman, E. Quiskamp, A. Tobar, M. E.
contents	Axions are a well-motivated candidate for dark matter. The preeminent method to search for axion dark matter is known as the axion haloscope, which makes use of the conversion of axions to photons in a large magnetic field. Due to the weak coupling of axions to photons however, the expected signal strength is exceptionally small. To increase signal strength, many haloscopes make use of resonant enhancement and high gain amplifiers, while also taking measures to keep receiver noise as low as possible such as the use of dilution refrigerators and ultra low-noise electronics. In this paper we derive the theoretical noise model based on the sources of noise found within a typical axion haloscope receiver chain, using the Axion Dark Matter eXperiment (ADMX) as a case study. We present examples of different noise calibration measurements at 1280~MHz taken during ADMX's most recent data-taking run. These new results shed light on a previously unidentified interaction between the cavity and JPA, as well as provide a better understanding of the systematic uncertainty on the system noise temperature used in the axion search analysis for this data-taking run. Finally, the consistency between the measurements and the detailed model provide suggestions for future improvements within ADMX and other axion haloscopes to reach a lower noise temperature.
format	Preprint
id	arxiv_https___arxiv_org_abs_2411_07172
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	Improved Receiver Noise Calibration for ADMX Axion Search: 4.54 to 5.41 $μ$eV Guzzetti, M. Zhang, D. Goodman, C. Hanretty, C. Sinnis, J. Rosenberg, L. J Rybka, G. Clarke, John Siddiqi, I. Chou, A. S. Hollister, M. Knirck, S. Sonnenschein, A. Caligiure, T. J. Gleason, J. R. Hipp, A. T. Sikivie, P. Solano, M. E. Sullivan, N. S. Tanner, D. B. Khatiwada, R. Carosi, G. Du, N. Cisneros, C. Robertson, N. Woollett, N. Duffy, L. D. Boutan, C. Braine, T. Oblath, N. S. Taubman, M. S. Lentz, E. Daw, E. J. Mostyn, C. Perry, M. G. Bartram, C. Dyson, T. A. Kuo, C. L. Ruppert, S. Withers, M. O. Yi, A. K. McAllister, B. T. Buckley, J. H. Gaikwad, C. Hoffman, J. Murch, K. Russell, J. Goryachev, M. Hartman, E. Quiskamp, A. Tobar, M. E. High Energy Physics - Experiment Axions are a well-motivated candidate for dark matter. The preeminent method to search for axion dark matter is known as the axion haloscope, which makes use of the conversion of axions to photons in a large magnetic field. Due to the weak coupling of axions to photons however, the expected signal strength is exceptionally small. To increase signal strength, many haloscopes make use of resonant enhancement and high gain amplifiers, while also taking measures to keep receiver noise as low as possible such as the use of dilution refrigerators and ultra low-noise electronics. In this paper we derive the theoretical noise model based on the sources of noise found within a typical axion haloscope receiver chain, using the Axion Dark Matter eXperiment (ADMX) as a case study. We present examples of different noise calibration measurements at 1280~MHz taken during ADMX's most recent data-taking run. These new results shed light on a previously unidentified interaction between the cavity and JPA, as well as provide a better understanding of the systematic uncertainty on the system noise temperature used in the axion search analysis for this data-taking run. Finally, the consistency between the measurements and the detailed model provide suggestions for future improvements within ADMX and other axion haloscopes to reach a lower noise temperature.
title	Improved Receiver Noise Calibration for ADMX Axion Search: 4.54 to 5.41 $μ$eV
topic	High Energy Physics - Experiment
url	https://arxiv.org/abs/2411.07172