Development of an MKID frequency-to-pixel LED mapper for SPT-3G+
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arXiv
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| Main Authors: | , , , , , , , |
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| Format: | Preprint |
| Published: |
2024
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| _version_ | 1866916659350994944 |
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| author | Martsen, E. S. Barry, P. S. Benson, B. A. Dibert, K. R. Fichman, K. N. Natoli, T. Rouble, M. Yu, C. |
| author_facet | Martsen, E. S. Barry, P. S. Benson, B. A. Dibert, K. R. Fichman, K. N. Natoli, T. Rouble, M. Yu, C. |
| contents | SPT-3G+ is the next-generation camera for the South Pole Telescope (SPT). SPT is designed to measure the cosmic microwave background (CMB) and the mm/sub-mm sky. The planned focal plane consists of 34,000 microwave kinetic inductance detectors (MKIDs), divided among three observing bands centered at 220, 285, and 345 GHz. Each readout line is designed to measure 800 MKIDs over a 500 MHz bandwidth, which places stringent constraints on the accuracy of the frequency placement required to limit resonator collisions that reduce the overall detector yield. To meet this constraint, we are developing a two-step process that first optically maps the resonance to a physical pixel location, and then next trims the interdigitated capacitor (IDC) to adjust the resonator frequency. We present a cryogenic LED apparatus operable at 300 mK for the optical illumination of SPT-3G+ detector arrays. We demonstrate integration of the LED controls with the GHz readout electronics (RF-ICE) to take data on an array of prototype SPT-3G+ detectors. We show that this technique is useful for characterizing defects in the resonator frequency across the detector array and will allow for improvements in the detector yield. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2411_17878 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Development of an MKID frequency-to-pixel LED mapper for SPT-3G+ Martsen, E. S. Barry, P. S. Benson, B. A. Dibert, K. R. Fichman, K. N. Natoli, T. Rouble, M. Yu, C. Instrumentation and Methods for Astrophysics SPT-3G+ is the next-generation camera for the South Pole Telescope (SPT). SPT is designed to measure the cosmic microwave background (CMB) and the mm/sub-mm sky. The planned focal plane consists of 34,000 microwave kinetic inductance detectors (MKIDs), divided among three observing bands centered at 220, 285, and 345 GHz. Each readout line is designed to measure 800 MKIDs over a 500 MHz bandwidth, which places stringent constraints on the accuracy of the frequency placement required to limit resonator collisions that reduce the overall detector yield. To meet this constraint, we are developing a two-step process that first optically maps the resonance to a physical pixel location, and then next trims the interdigitated capacitor (IDC) to adjust the resonator frequency. We present a cryogenic LED apparatus operable at 300 mK for the optical illumination of SPT-3G+ detector arrays. We demonstrate integration of the LED controls with the GHz readout electronics (RF-ICE) to take data on an array of prototype SPT-3G+ detectors. We show that this technique is useful for characterizing defects in the resonator frequency across the detector array and will allow for improvements in the detector yield. |
| title | Development of an MKID frequency-to-pixel LED mapper for SPT-3G+ |
| topic | Instrumentation and Methods for Astrophysics |
| url | https://arxiv.org/abs/2411.17878 |