I downgraded the Red Pitaya back to OS 2.00-18 due to runtime errors during measurement. Once I did this, the device appeared to work much better than it has the last few weeks. First, it appears we can actually see the cutoff of the added low-pass filters that were added in to the RIN setup. Second, there does appear to be a difference again between the FROSTI ON state versus the dark state (i.e. FROSTI OFF). A long measurement of the ADC noise floor in the current configuration still needs to be recorded, but it does appear that the recent highlighted issues with the Red Pitaya have been solved.

Attached below are updated ASD plots for the FROSTI RIN measurements. The parameters set for this are the following:

• DFT Size (N): 16384
• Sampling Frequency (F_s): 7.629 kHz
• Resolution (F_s/N): 0.93
• CH0 DC Voltage w/FROSTI ON: 113.6 mV
• CH0 DC Voltage w/FROSTI OFF: -5.7 mV
• CH1 DC Voltage w/FROSTI ON: 113.0 mV
• CH1 DC Voltage w/FROSTI OFF: -5.7 mV

Each measurement was recorded over a roughly two-day period. Before each spectrum was computed, the time-series signals were AC-coupled (i.e. the DC offset was subtracted from the data). The low-pass filters are still attached for dark and light noise measurements. ADC noise is measured with two 50-ohm terminators attached to the Red Pitaya inputs rather than the IR photodetectors.

I have begun the (hopefully) final RIN measurements at 3:30 PM today. If you need to go into the cleanroom at any time between now and Sunday (the 22nd), please do not touch the FROSTI, the Red Pitaya, the photodetectors, or any of the wiring.

Attached below are updated plots for the FROSTI RIN measurements for Jan 14 group meeting.

On Tuesday, we prepared the FROSTI for disassembly in anticipation of the APS filming that is set to take place in the labs. The FROSTI has been unbolted from the optical table in the cleanroom, with its wires weighted down and the majority of its screws removed to ensure an easy removal of the reflectors during the filming process.

On Tuesday (Jan 21), we took the FROSTI apart in front of a filming crew. It was a success! The footage is going to be used in an APS video detailing the experimental cosmology research conducted in the department.

The FROSTI reflectors, heater elements, and legs were all bagged separately and a currently being stored in the cleanroom. If you need to do any work in there, please be mindful of these parts. The elements are currently on the shelf above the optical table, and the reflectors are placed on the table in the back corner.

Below is a preview of the final RIN figure that will be included in the FROSTI instrument paper. A quick summary of what is shown below:

The original RIN CSD measurement is shown on the top panel in red. Frequency bins that exhibit external electronics noise (ex. ADC, photodetector noise, etc.) are identified and shaded in gray. These noisy bins are then excluded from the dataset before beginning the next step in the analysis process: rebinning. Here, the resolution of the spectrum can be changed by averaging frequency bins together within a specified interval, with the goal of pushing the measurement curve closer to the A+ requirement shown in the figure. For demonstration below, the spectrum goes from a resolution of ~0.93 Hz to 14.90 Hz.

Upon final review of the FROSTI analysis included in the (hopefully) soon-to-be submitted instrument paper, I've made some adjustments to the reflectivity analysis that estimates the amount of power delivered to the test mass by the FROSTI. Initially, as detailed in elog 447, the delivered power was approximated to be 12.6 W (later adjusted to 12.9 W), with roughly 18% of this power being reflected by the test mass. After some final adjustments, this value now is closer to 12.0 W, with 10.2 W absorbed (15% power reflection). Below is a table showing the updated values for the FROSTI prototype tests:

Updated ADC noise spectra measurements using diaggui.

NOTE: Will update plots with proper axes

Slides

After acquiring some new equipment for the labs, a few of us spent time on Thursday and Friday sorting through everything and storing them into their appropriate places. New vacuum parts, power supplies, cables, and much more were included. The rooms are now ready for the lab tours commencing Tuesday afternoon.

Below is attached the ADC noise floor of two CyMAC channels vs the Red Pitaya.

The frequency resolution of these RIN spectra are 16 Hz, with N_meas = 19,308,426 for the CyMAC, and N_meas = 263,024.

I've been looking into the performances of individual channels on the Cymac by computing their individual PSDs and corresponding CSDs that show their noise relation to each other. It appears some channels do have lower noise floors than others, and some combinations of these actually do perform similar to the Red Pitaya (showing below the CSD between CHs 3 and 5), although it doesn't look like it's much of an improvement. The best method as of now still appears to be phase-locking two separate ADCs to reduce the correlated noise floor further.

This can be further discussed at the July 22, 2025 group meeting.

Updated CyMAC measurement, comparing 260 hrs of measurement time vs. 405 hrs.

Below are slides giving an update on RH O6 design progress.

Below are slides discussing RIN infrastructural updates related to the CyMAC.

Slides

A# Profile optimization update for 01/28/2026 group meeting.

Slides updating progress on FROSTI A# irradiance profiles and reflector design. Edge roll-off is now included for thermoelastic deformation corrections.

Slides covering a new approach to optimizing for A# FROSTI profiles. In particular, we start looking at just optimal RH correction. Once this profile is determined, we then minimize the residual further with FROSTI profiles.

cleaning cleanroom and particle count

• 12:30 pm: Tyler and Aiden started organizing cables in cleanroom
• 12:35 pm: started particle count in flow bench
• 0.3 u: 11681
• 0.5 u: 3284
• 1.0 u: 1039
• 12:50 pm: started cleanroom particle count
  • zone 3:
    • 0.3 u: 14549
    • 0.5 u: 10351
    • 1.0 u: 6194
• zone 4:
  • 0.3 u: 10808
  • 0.5 u: 4655
  • 1.0 u: 1953
• 1:07 pm: began surface check and wipedown, including softwalls
• 1:19 pm: started vacuuming the floor
• 1:28 pm: finished vacuuming the floor
• 1:29 pm: started mopping the floor
• 1:33 pm: finished mopping the floor
• 1:34 pm: started cleaning the buckets
• 1:37 pm: started mopping with IPA wipes
• 1:39 pm: finished mopping with IPA wipes
• 1:40 pm: changed sticky floor mats
• 1:41 pm: started particle count
  • zone 3:
    • 0.3 u: 8397
    • 0.5 u: 5071
    • 1.0 u: 2618
• zone 4:
  • 0.3 u: 6651
  • 0.5 u: 4323
  • 1.0 u: 2120