Modulated scan high cadence LAT
October 25, 2019 - Reijo Keskitalo
This post refines the work shown in High_cadence_LAT_from_Chile. We show how to modulate the scan rate to achieve maximally uniform integration depth across a maximal sky area.
Let us assume that,
- is the observatory latitude, measured in radians from the Equator
- is the observing azimuth, measured in radians from North. East is at
- is the observing elevation, measured in radians from the horizon.
- is the declination on the celestial sphere.
Then we can write the declination as a function of the observatory latitude and observing azimuth and elevation.
Moreover, we can write for the rate at which declination changes in terms of the azimuthal rate
where the final form follows from application of . The time, , spent observing at a specific declination is inversely proportional to the rate at which the declination changes
If we consider the fact that the sky area at each latitude is proportional to , the integration time per unit sky area, , is
where we have dropped the constant factor
From it is evident that for the observing depth to be uniform ( to be constant), the azimuthal scanning rate must satisfy
and explicitly, the azimuthal rate on the sky, , will depend on some base azimuthal rate on the telescope, , as
Modulating the azimuthal scanning rate is limited by maximum azimuthal rate of the telescope and, to a lesser degree, the azimuthal acceleration of the telescope.
Here is a plot of the modulation factor as a function of the telescope azimuth:
It is obvious that sweeping close to 180 degrees is unfeasible as it would require the telescope to move very fast as it approaches the turnaround. A factor of 2 or 3 (throw of 160 or 170 degrees) is achievable, especially if the base scanning rate is low enough.
Pushing for extreme azimuth ranges is not even required for the sky area, as we quickly enter the domain of diminishing returns:
Assuming a base scanning rate of 0.75 deg/s, low acceleration of 1 deg/s^2, throw between 20 and 160 degrees and observing elevation of 30 degrees:
The top row shows one simulated back-and-forth scan, the bottom row shows 10 consecutive sweeps. The telescope never moves faster than 2.75 deg/s in azimuth.
We simulated full year hit maps with a reduced focal plane and sampling rate using constant and modulated scan rates. We considered three observing elevations: 30, 40 and 50 degrees and chose the azimuth ranges to keep the maximum modulation factor at 2.75:
- 30 deg elevation : Az = [19, 161] deg
- 40 deg elevation : Az = [21, 159] deg
- 50 deg elevation : Az = [26, 154] deg
In the following plot, left column hit maps use constant scan rate, right column is from the modulated scan rate. The titles of each panel show the raw, signal and noise dominated fskies.
We found a simple mathematical form ( ) of modulated scan rate that achieves uniform integration depth across all declinations. Allowing for a non-constant azimuthal scanning rate seems essential if we are to achieve high cadence (for transient science) and effective sky area (critical for Neff and other science targets). Once the hardware limits are known, it is straightforward to define the scan strategy that fits within those limits.
Update including elevation nods
August 31, 2020 - Mike Niemack
Sigurd Naess proposed adding elevation nods to improve cross-linking in the large area LAT surveys. This was studied by Haruki Ebina (Cornell) working with Mike Niemack, Jason Stevens, Thuong Hoang, and Steve Choi and is being considered for SO and CCAT-prime observations. Here is a report on this analysis: File:Update on Modulated High cadence LAT survey strategies from Chile 20200831.pdf
In brief, executing ~1 deg amplitude elevation nods combined with wide varying azimuthal velocity scans appears to be a promising approach to achieve a high-cadence survey strategy with substantially better cross-linking than we can achieve with the current ACT strategy.
Thinking about the LAT and LATR optical performance, based on previous discussions I suggest that we keep the LATR at a fixed angle while the telescope elevation nods. This will result in small pointing offsets on the order of 4’ for the outer optics tubes that will need to be taken into account in the pointing model. The changes in beam shape will be tiny though, since 4’ is a small fraction of the angular size of an optics tube.