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systematicswg:telecons:2018-05-03 [2018/05/14 10:43] – created bcrillsystematicswg:telecons:2018-05-03 [2018/05/14 10:50] (current) – bcrill
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 May 3 Face to face meeting May 3 Face to face meeting
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 present: Jacques, Maurizio, Reijo, Julian, Shaul, Brendan  present: Jacques, Maurizio, Reijo, Julian, Shaul, Brendan
  
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     * A limiting factor is Galaxy bias… but let's say in the future we solve this.     * A limiting factor is Galaxy bias… but let's say in the future we solve this.
            * Maurizio would like to do a CMB-only sim with 1/f noise solving for calibration and determining time scale over which this is feasible.  Assesses impact of noise on the calibration vs. time.  Provide some bound on detector stability requirement.            * Maurizio would like to do a CMB-only sim with 1/f noise solving for calibration and determining time scale over which this is feasible.  Assesses impact of noise on the calibration vs. time.  Provide some bound on detector stability requirement.
- ○ In a week, get the gains.  Then.. Use these recovered gains as inputs to produce sky maps.  Hopefully done in a few weeks. +    * In a week, get the gains.  Then.. Use these recovered gains as inputs to produce sky maps.  Hopefully done in a few weeks. 
- ○ In CORE paper, got 0.01% with a 96 hour time scale, 12 hours may not be good enough. +    * In CORE paper, got 0.01% with a 96 hour time scale, 12 hours may not be good enough. 
- ○ Get a reference for stability of TES bolos as seen in SPIDER (from Hannes and Jeff) +    * Get a reference for stability of TES bolos as seen in SPIDER (from Hannes and Jeff) 
- ○ OK, great.  But this level of reconstructed gain at the ~0.1 to 1% level may not be good enough. +    * OK, great.  But this level of reconstructed gain at the ~0.1 to 1% level may not be good enough. 
- ○ Determine time scale / accuracy of calibration that is needed on the detector side. +    * Determine time scale / accuracy of calibration that is needed on the detector side. 
- • Absolute angle rotation +   * Absolute angle rotation 
- ○ TBC: Relative angle of each detector to mean angle could be iteratively solved (?) +    * TBC: Relative angle of each detector to mean angle could be iteratively solved (?) 
- ○ Solve for error of individual detectors vs. the mean, and look at the distribution -> gives lower bound on final error in absolute angle +    * Solve for error of individual detectors vs. the mean, and look at the distribution -> gives lower bound on final error in absolute angle 
- ○ How well can we jointly solve for cosmic birefringence and an absolute polarimeter angle error using EB (along lines of Eric's presentation)? +           * How well can we jointly solve for cosmic birefringence and an absolute polarimeter angle error using EB (along lines of Eric's presentation)? **Need to ask Eric about this.** 
- ○ Need to ask Eric about this. +   * Sidelobes 
- • Sidelobes +    * Convolution of timeline with GRASP beams. 
- ○ Convolution of timeline with GRASP beams. +    * Karl's GRASP output was converted to b_lm's (w/help from Ashdown) 
- ○ Karl's GRASP output was converted to b_lm's (w/help from Ashdown) +    * Andrea now has 4pi beam files: small issue being fixed by Andrea: ask Andrea status 
- ○ Andrea now has 4pi beam files: small issue being fixed by Andrea: ask Andrea status +    * Power spectrum of sidelobe signal or map of sidelobe pickup 
- ○ Power spectrum of sidelobe signal or map of sidelobe pickup +    * Generate convolution with the the x- and y- polarization detectors in one pixel 
- ○ Generate convolution with the the x- and y- polarization detectors in one pixel +    * Have to cut out the main lobe of the beam prior to convolution Either central pixel (1x1 degree), or a little bit more of the near sidelobes just to be safe.  Karl to take care of that. 
- ○ Have to cut out the main lobe of the beam prior to convolution +    * What sky do we convolve with? Just use pysm that is interfaced with toast: include Galaxy and dipole, maybe separately (?) 
- § Either central pixel (1x1 degree), or a little bit more of the near sidelobes just to be safe.  +    * Look at amplitude of map: compare to 1 nK -> maybe a BB spectrum with a sky cut. 
- § Karl to take care of that. +    * Ask Andrea for not just an entire year, but also maybe one precession in order to identify where the pickup is coming from. 
- ○ What sky do we convolve with? Just use pysm that is interfaced with toast: include Galaxy and dipole, maybe separately (?) + * Possibly identify design changes to baffles
- ○ Look at amplitude of map: compare to 1 nK -> maybe a BB spectrum with a sky cut. +
- ○ Ask Andrea for not just an entire year, but also maybe one precession in order to identify where the pickup is coming from. +
- ○ Possibly identify design changes to baffles+
   
- • An important question: will ground calibration be carried out at individual detector level at a high level of accuracy? (bandpass, time constants, linearity, etc.) +   * An important question: will ground calibration be carried out at individual detector level at a high level of accuracy? (bandpass, time constants, linearity, etc.) 
- ○ What does S4 / Simons do really? +     * What does S4 / Simons do really? 
- ○ What did Roger O'Brient assume about integration & test for PICO +     * What did Roger O'Brient assume about integration & test for PICO 
- ○ Do we need new processes? AI?+     * Do we need new processes? AI?
   
systematicswg/telecons/2018-05-03.1526312638.txt.gz · Last modified: 2018/05/14 10:43 by bcrill

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