https://cmb-s4.uchicago.edu/wiki/api.php?action=feedcontributions&user=Wlwu&feedformat=atomCMB-S4 wiki - User contributions [en]2022-11-29T07:19:01ZUser contributionsMediaWiki 1.34.2https://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p1&diff=12230Delensing LAT relative Nhits v0p12020-12-15T05:36:56Z<p>Wlwu: /* Results */</p>
<hr />
<div>This is a 2nd in a series of postings that document the process to answer the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
Previous posting: [[ Delensing_LAT_relative_Nhits_v0p0 | Delensing_LAT_relative_Nhits_v0p0 ]]<br />
<br />
== Background/Summary ==<br />
This posting is written in response to a discussion from the scan-strategy call: if we have tophat-like hit patterns for the LAT, given fixed total N-hits, how would the delensed A_L change if the tophat pattern covers all the pixels hit by SATs vs the smaller tophat hit pattern given in the [[https://github.com/CMB-S4/s4_design_sim_tool DM reference-design sims ]]. <br />
<br />
Note that in the DM reference-design sims, the LAT (Pole-LAT-MFL1) N-hit pattern doesn't cover all the pixels hit by the Pole SAT-MF(HS1/HS2/LS1/LS2). So the regions outside the LAT hit would not have delensing. <br />
<br />
Key takeaways:<br />
* In the reference-design sims, the LAT hits cover about 50% of the SAT hit pattern; within that region, it gets 85% of the total number of hits. <br />
* Delensed A_L is ~0.09 in the reference-design LAT region.<br />
* Delensed A_L is ~0.12 if spreading the LAT hits across all the pixels seen by the SAT. <br />
<br />
== Method ==<br />
* I used information from one LAT and one SAT (both Pole) for extracting all the numbers (using just white noise)<br />
** LAT: Pole-LAT-MFL1 (93GHz, 2.2 FWHM); the N-hits for the MFs are the same.<br />
** SAT: Pole-SAT-MFLS1 (85GHz); the N-hits for all the MFs are the same.<br />
* I calculate the noise spectra from the LAT-MFL1 noise map (/global/cfs/cdirs/cmbs4/dm/dstool/output/s4_reference_design_noise_atmo_7splits/LAT-MFL1_pole/cmbs4_KCMB_LAT-MFL1_pole_nside4096_1_of_1.fits) and estimate the equivalent white noise level in uK-arcmin to be ~0.7uK-arcmin.<br />
* For the effective white noise level when spreading all the hits uniformly, I scale the uK-arcmin number by sqrt(new_area/old_area). <br />
* The delensed A_L is from DSR fig.68.<br />
<br />
== Results ==<br />
'''Fig.1 Pole LAT-MFL1 EE/BB noise '''<br />
<br />
[[File:1207_LAT-MFL1_nlev_ukam.png|border|600px]]<br />
<br />
A TF corrected N_ell included [[Media:1214_EE_noise_compare_low-ellBB_DC06_dsr_simtool.png | here]] (also include comparison with Low-ell BB DC06 sim Pole LAT 95GHz noise).<br />
<br />
'''Fig.2 Pole LAT-MFL1 Nhits '''<br />
<br />
[[File:1207_LAT-MFL1_nhits.png|border|600px]]<br />
<br />
'''Fig.3 Pole SAT-MFLS1 Nhits cut with LAT-MFL1 tophat'''<br />
<br />
[[File:1207_SAT-MFLS1_Nhits_bound.png |border|600px]]<br />
<br />
'''Fig.4 Pole SAT-MFLS1 map noise uK-arcmin'''<br />
<br />
[[File:1207_SAT-MFLS1_map_ukam.png |border|600px]]<br />
<br />
'''Fig.5 Pole LAT-MFL1 map noise uK-arcmin'''<br />
<br />
[[File:1207_LAT-MFL1_map_nlev_ukam.png |border|600px]]</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:1214_EE_noise_compare_low-ellBB_DC06_dsr_simtool.png&diff=12229File:1214 EE noise compare low-ellBB DC06 dsr simtool.png2020-12-15T05:34:21Z<p>Wlwu: </p>
<hr />
<div></div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p1&diff=12228Delensing LAT relative Nhits v0p12020-12-15T05:34:10Z<p>Wlwu: /* Results */</p>
<hr />
<div>This is a 2nd in a series of postings that document the process to answer the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
Previous posting: [[ Delensing_LAT_relative_Nhits_v0p0 | Delensing_LAT_relative_Nhits_v0p0 ]]<br />
<br />
== Background/Summary ==<br />
This posting is written in response to a discussion from the scan-strategy call: if we have tophat-like hit patterns for the LAT, given fixed total N-hits, how would the delensed A_L change if the tophat pattern covers all the pixels hit by SATs vs the smaller tophat hit pattern given in the [[https://github.com/CMB-S4/s4_design_sim_tool DM reference-design sims ]]. <br />
<br />
Note that in the DM reference-design sims, the LAT (Pole-LAT-MFL1) N-hit pattern doesn't cover all the pixels hit by the Pole SAT-MF(HS1/HS2/LS1/LS2). So the regions outside the LAT hit would not have delensing. <br />
<br />
Key takeaways:<br />
* In the reference-design sims, the LAT hits cover about 50% of the SAT hit pattern; within that region, it gets 85% of the total number of hits. <br />
* Delensed A_L is ~0.09 in the reference-design LAT region.<br />
* Delensed A_L is ~0.12 if spreading the LAT hits across all the pixels seen by the SAT. <br />
<br />
== Method ==<br />
* I used information from one LAT and one SAT (both Pole) for extracting all the numbers (using just white noise)<br />
** LAT: Pole-LAT-MFL1 (93GHz, 2.2 FWHM); the N-hits for the MFs are the same.<br />
** SAT: Pole-SAT-MFLS1 (85GHz); the N-hits for all the MFs are the same.<br />
* I calculate the noise spectra from the LAT-MFL1 noise map (/global/cfs/cdirs/cmbs4/dm/dstool/output/s4_reference_design_noise_atmo_7splits/LAT-MFL1_pole/cmbs4_KCMB_LAT-MFL1_pole_nside4096_1_of_1.fits) and estimate the equivalent white noise level in uK-arcmin to be ~0.7uK-arcmin.<br />
* For the effective white noise level when spreading all the hits uniformly, I scale the uK-arcmin number by sqrt(new_area/old_area). <br />
* The delensed A_L is from DSR fig.68.<br />
<br />
== Results ==<br />
'''Fig.1 Pole LAT-MFL1 EE/BB noise '''<br />
<br />
[[File:1207_LAT-MFL1_nlev_ukam.png|border|600px]]<br />
<br />
A TF corrected N_ell included [[File: 1214_EE_noise_compare_low-ellBB_DC06_dsr_simtool.png | here]] (also include comparison with Low-ell BB DC06 sim Pole LAT 95GHz noise).<br />
<br />
'''Fig.2 Pole LAT-MFL1 Nhits '''<br />
<br />
[[File:1207_LAT-MFL1_nhits.png|border|600px]]<br />
<br />
'''Fig.3 Pole SAT-MFLS1 Nhits cut with LAT-MFL1 tophat'''<br />
<br />
[[File:1207_SAT-MFLS1_Nhits_bound.png |border|600px]]<br />
<br />
'''Fig.4 Pole SAT-MFLS1 map noise uK-arcmin'''<br />
<br />
[[File:1207_SAT-MFLS1_map_ukam.png |border|600px]]<br />
<br />
'''Fig.5 Pole LAT-MFL1 map noise uK-arcmin'''<br />
<br />
[[File:1207_LAT-MFL1_map_nlev_ukam.png |border|600px]]</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p1&diff=12219Delensing LAT relative Nhits v0p12020-12-09T19:30:23Z<p>Wlwu: /* Results */</p>
<hr />
<div>This is a 2nd in a series of postings that document the process to answer the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
Previous posting: [[ Delensing_LAT_relative_Nhits_v0p0 | Delensing_LAT_relative_Nhits_v0p0 ]]<br />
<br />
== Background/Summary ==<br />
This posting is written in response to a discussion from the scan-strategy call: if we have tophat-like hit patterns for the LAT, given fixed total N-hits, how would the delensed A_L change if the tophat pattern covers all the pixels hit by SATs vs the smaller tophat hit pattern given in the [[https://github.com/CMB-S4/s4_design_sim_tool DM reference-design sims ]]. <br />
<br />
Note that in the DM reference-design sims, the LAT (Pole-LAT-MFL1) N-hit pattern doesn't cover all the pixels hit by the Pole SAT-MF(HS1/HS2/LS1/LS2). So the regions outside the LAT hit would not have delensing. <br />
<br />
Key takeaways:<br />
* In the reference-design sims, the LAT hits cover about 50% of the SAT hit pattern; within that region, it gets 85% of the total number of hits. <br />
* Delensed A_L is ~0.09 in the reference-design LAT region.<br />
* Delensed A_L is ~0.12 if spreading the LAT hits across all the pixels seen by the SAT. <br />
<br />
== Method ==<br />
* I used information from one LAT and one SAT (both Pole) for extracting all the numbers (using just white noise)<br />
** LAT: Pole-LAT-MFL1 (93GHz, 2.2 FWHM); the N-hits for the MFs are the same.<br />
** SAT: Pole-SAT-MFLS1 (85GHz); the N-hits for all the MFs are the same.<br />
* I calculate the noise spectra from the LAT-MFL1 noise map (/global/cfs/cdirs/cmbs4/dm/dstool/output/s4_reference_design_noise_atmo_7splits/LAT-MFL1_pole/cmbs4_KCMB_LAT-MFL1_pole_nside4096_1_of_1.fits) and estimate the equivalent white noise level in uK-arcmin to be ~0.7uK-arcmin.<br />
* For the effective white noise level when spreading all the hits uniformly, I scale the uK-arcmin number by sqrt(new_area/old_area). <br />
* The delensed A_L is from DSR fig.68.<br />
<br />
== Results ==<br />
'''Fig.1 Pole LAT-MFL1 EE/BB noise '''<br />
<br />
[[File:1207_LAT-MFL1_nlev_ukam.png|border|600px]]<br />
<br />
'''Fig.2 Pole LAT-MFL1 Nhits '''<br />
<br />
[[File:1207_LAT-MFL1_nhits.png|border|600px]]<br />
<br />
'''Fig.3 Pole SAT-MFLS1 Nhits cut with LAT-MFL1 tophat'''<br />
<br />
[[File:1207_SAT-MFLS1_Nhits_bound.png |border|600px]]<br />
<br />
'''Fig.4 Pole SAT-MFLS1 map noise uK-arcmin'''<br />
<br />
[[File:1207_SAT-MFLS1_map_ukam.png |border|600px]]<br />
<br />
'''Fig.5 Pole LAT-MFL1 map noise uK-arcmin'''<br />
<br />
[[File:1207_LAT-MFL1_map_nlev_ukam.png |border|600px]]</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p1&diff=12218Delensing LAT relative Nhits v0p12020-12-09T19:29:09Z<p>Wlwu: /* Results */</p>
<hr />
<div>This is a 2nd in a series of postings that document the process to answer the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
Previous posting: [[ Delensing_LAT_relative_Nhits_v0p0 | Delensing_LAT_relative_Nhits_v0p0 ]]<br />
<br />
== Background/Summary ==<br />
This posting is written in response to a discussion from the scan-strategy call: if we have tophat-like hit patterns for the LAT, given fixed total N-hits, how would the delensed A_L change if the tophat pattern covers all the pixels hit by SATs vs the smaller tophat hit pattern given in the [[https://github.com/CMB-S4/s4_design_sim_tool DM reference-design sims ]]. <br />
<br />
Note that in the DM reference-design sims, the LAT (Pole-LAT-MFL1) N-hit pattern doesn't cover all the pixels hit by the Pole SAT-MF(HS1/HS2/LS1/LS2). So the regions outside the LAT hit would not have delensing. <br />
<br />
Key takeaways:<br />
* In the reference-design sims, the LAT hits cover about 50% of the SAT hit pattern; within that region, it gets 85% of the total number of hits. <br />
* Delensed A_L is ~0.09 in the reference-design LAT region.<br />
* Delensed A_L is ~0.12 if spreading the LAT hits across all the pixels seen by the SAT. <br />
<br />
== Method ==<br />
* I used information from one LAT and one SAT (both Pole) for extracting all the numbers (using just white noise)<br />
** LAT: Pole-LAT-MFL1 (93GHz, 2.2 FWHM); the N-hits for the MFs are the same.<br />
** SAT: Pole-SAT-MFLS1 (85GHz); the N-hits for all the MFs are the same.<br />
* I calculate the noise spectra from the LAT-MFL1 noise map (/global/cfs/cdirs/cmbs4/dm/dstool/output/s4_reference_design_noise_atmo_7splits/LAT-MFL1_pole/cmbs4_KCMB_LAT-MFL1_pole_nside4096_1_of_1.fits) and estimate the equivalent white noise level in uK-arcmin to be ~0.7uK-arcmin.<br />
* For the effective white noise level when spreading all the hits uniformly, I scale the uK-arcmin number by sqrt(new_area/old_area). <br />
* The delensed A_L is from DSR fig.68.<br />
<br />
== Results ==<br />
'''Fig.1 Pole LAT-MFL1 EE/BB noise '''<br />
<br />
[[File:1207_LAT-MFL1_nlev_ukam3.png|border|600px]]<br />
<br />
'''Fig.2 Pole LAT-MFL1 Nhits '''<br />
<br />
[[File:1207_LAT-MFL1_nhits.png|border|600px]]<br />
<br />
'''Fig.3 Pole SAT-MFLS1 Nhits cut with LAT-MFL1 tophat'''<br />
<br />
[[File:1207_SAT-MFLS1_Nhits_bound.png |border|600px]]<br />
<br />
'''Fig.4 Pole SAT-MFLS1 map noise uK-arcmin'''<br />
<br />
[[File:1207_SAT-MFLS1_map_ukam.png |border|600px]]<br />
<br />
'''Fig.5 Pole LAT-MFL1 map noise uK-arcmin'''<br />
<br />
[[File:1207_LAT-MFL1_map_nlev_ukam.png |border|600px]]</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p1&diff=12217Delensing LAT relative Nhits v0p12020-12-09T19:27:53Z<p>Wlwu: /* Results */</p>
<hr />
<div>This is a 2nd in a series of postings that document the process to answer the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
Previous posting: [[ Delensing_LAT_relative_Nhits_v0p0 | Delensing_LAT_relative_Nhits_v0p0 ]]<br />
<br />
== Background/Summary ==<br />
This posting is written in response to a discussion from the scan-strategy call: if we have tophat-like hit patterns for the LAT, given fixed total N-hits, how would the delensed A_L change if the tophat pattern covers all the pixels hit by SATs vs the smaller tophat hit pattern given in the [[https://github.com/CMB-S4/s4_design_sim_tool DM reference-design sims ]]. <br />
<br />
Note that in the DM reference-design sims, the LAT (Pole-LAT-MFL1) N-hit pattern doesn't cover all the pixels hit by the Pole SAT-MF(HS1/HS2/LS1/LS2). So the regions outside the LAT hit would not have delensing. <br />
<br />
Key takeaways:<br />
* In the reference-design sims, the LAT hits cover about 50% of the SAT hit pattern; within that region, it gets 85% of the total number of hits. <br />
* Delensed A_L is ~0.09 in the reference-design LAT region.<br />
* Delensed A_L is ~0.12 if spreading the LAT hits across all the pixels seen by the SAT. <br />
<br />
== Method ==<br />
* I used information from one LAT and one SAT (both Pole) for extracting all the numbers (using just white noise)<br />
** LAT: Pole-LAT-MFL1 (93GHz, 2.2 FWHM); the N-hits for the MFs are the same.<br />
** SAT: Pole-SAT-MFLS1 (85GHz); the N-hits for all the MFs are the same.<br />
* I calculate the noise spectra from the LAT-MFL1 noise map (/global/cfs/cdirs/cmbs4/dm/dstool/output/s4_reference_design_noise_atmo_7splits/LAT-MFL1_pole/cmbs4_KCMB_LAT-MFL1_pole_nside4096_1_of_1.fits) and estimate the equivalent white noise level in uK-arcmin to be ~0.7uK-arcmin.<br />
* For the effective white noise level when spreading all the hits uniformly, I scale the uK-arcmin number by sqrt(new_area/old_area). <br />
* The delensed A_L is from DSR fig.68.<br />
<br />
== Results ==<br />
'''Fig.1 Pole LAT-MFL1 EE/BB noise '''<br />
<br />
[[File:1207_LAT-MFL1_nlev_ukam2.png|border|600px]]<br />
<br />
'''Fig.2 Pole LAT-MFL1 Nhits '''<br />
<br />
[[File:1207_LAT-MFL1_nhits.png|border|600px]]<br />
<br />
'''Fig.3 Pole SAT-MFLS1 Nhits cut with LAT-MFL1 tophat'''<br />
<br />
[[File:1207_SAT-MFLS1_Nhits_bound.png |border|600px]]<br />
<br />
'''Fig.4 Pole SAT-MFLS1 map noise uK-arcmin'''<br />
<br />
[[File:1207_SAT-MFLS1_map_ukam.png |border|600px]]<br />
<br />
'''Fig.5 Pole LAT-MFL1 map noise uK-arcmin'''<br />
<br />
[[File:1207_LAT-MFL1_map_nlev_ukam.png |border|600px]]</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p1&diff=12216Delensing LAT relative Nhits v0p12020-12-09T19:27:23Z<p>Wlwu: /* Results */</p>
<hr />
<div>This is a 2nd in a series of postings that document the process to answer the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
Previous posting: [[ Delensing_LAT_relative_Nhits_v0p0 | Delensing_LAT_relative_Nhits_v0p0 ]]<br />
<br />
== Background/Summary ==<br />
This posting is written in response to a discussion from the scan-strategy call: if we have tophat-like hit patterns for the LAT, given fixed total N-hits, how would the delensed A_L change if the tophat pattern covers all the pixels hit by SATs vs the smaller tophat hit pattern given in the [[https://github.com/CMB-S4/s4_design_sim_tool DM reference-design sims ]]. <br />
<br />
Note that in the DM reference-design sims, the LAT (Pole-LAT-MFL1) N-hit pattern doesn't cover all the pixels hit by the Pole SAT-MF(HS1/HS2/LS1/LS2). So the regions outside the LAT hit would not have delensing. <br />
<br />
Key takeaways:<br />
* In the reference-design sims, the LAT hits cover about 50% of the SAT hit pattern; within that region, it gets 85% of the total number of hits. <br />
* Delensed A_L is ~0.09 in the reference-design LAT region.<br />
* Delensed A_L is ~0.12 if spreading the LAT hits across all the pixels seen by the SAT. <br />
<br />
== Method ==<br />
* I used information from one LAT and one SAT (both Pole) for extracting all the numbers (using just white noise)<br />
** LAT: Pole-LAT-MFL1 (93GHz, 2.2 FWHM); the N-hits for the MFs are the same.<br />
** SAT: Pole-SAT-MFLS1 (85GHz); the N-hits for all the MFs are the same.<br />
* I calculate the noise spectra from the LAT-MFL1 noise map (/global/cfs/cdirs/cmbs4/dm/dstool/output/s4_reference_design_noise_atmo_7splits/LAT-MFL1_pole/cmbs4_KCMB_LAT-MFL1_pole_nside4096_1_of_1.fits) and estimate the equivalent white noise level in uK-arcmin to be ~0.7uK-arcmin.<br />
* For the effective white noise level when spreading all the hits uniformly, I scale the uK-arcmin number by sqrt(new_area/old_area). <br />
* The delensed A_L is from DSR fig.68.<br />
<br />
== Results ==<br />
'''Fig.1 Pole LAT-MFL1 EE/BB noise '''<br />
<br />
[[File:1207_LAT-MFL1_nlev_ukam.png|border|600px]]<br />
<br />
'''Fig.2 Pole LAT-MFL1 Nhits '''<br />
<br />
[[File:1207_LAT-MFL1_nhits.png|border|600px]]<br />
<br />
'''Fig.3 Pole SAT-MFLS1 Nhits cut with LAT-MFL1 tophat'''<br />
<br />
[[File:1207_SAT-MFLS1_Nhits_bound.png |border|600px]]<br />
<br />
'''Fig.4 Pole SAT-MFLS1 map noise uK-arcmin'''<br />
<br />
[[File:1207_SAT-MFLS1_map_ukam.png |border|600px]]<br />
<br />
'''Fig.5 Pole LAT-MFL1 map noise uK-arcmin'''<br />
<br />
[[File:1207_LAT-MFL1_map_nlev_ukam.png |border|600px]]</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p1&diff=12215Delensing LAT relative Nhits v0p12020-12-09T19:26:52Z<p>Wlwu: /* Results */</p>
<hr />
<div>This is a 2nd in a series of postings that document the process to answer the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
Previous posting: [[ Delensing_LAT_relative_Nhits_v0p0 | Delensing_LAT_relative_Nhits_v0p0 ]]<br />
<br />
== Background/Summary ==<br />
This posting is written in response to a discussion from the scan-strategy call: if we have tophat-like hit patterns for the LAT, given fixed total N-hits, how would the delensed A_L change if the tophat pattern covers all the pixels hit by SATs vs the smaller tophat hit pattern given in the [[https://github.com/CMB-S4/s4_design_sim_tool DM reference-design sims ]]. <br />
<br />
Note that in the DM reference-design sims, the LAT (Pole-LAT-MFL1) N-hit pattern doesn't cover all the pixels hit by the Pole SAT-MF(HS1/HS2/LS1/LS2). So the regions outside the LAT hit would not have delensing. <br />
<br />
Key takeaways:<br />
* In the reference-design sims, the LAT hits cover about 50% of the SAT hit pattern; within that region, it gets 85% of the total number of hits. <br />
* Delensed A_L is ~0.09 in the reference-design LAT region.<br />
* Delensed A_L is ~0.12 if spreading the LAT hits across all the pixels seen by the SAT. <br />
<br />
== Method ==<br />
* I used information from one LAT and one SAT (both Pole) for extracting all the numbers (using just white noise)<br />
** LAT: Pole-LAT-MFL1 (93GHz, 2.2 FWHM); the N-hits for the MFs are the same.<br />
** SAT: Pole-SAT-MFLS1 (85GHz); the N-hits for all the MFs are the same.<br />
* I calculate the noise spectra from the LAT-MFL1 noise map (/global/cfs/cdirs/cmbs4/dm/dstool/output/s4_reference_design_noise_atmo_7splits/LAT-MFL1_pole/cmbs4_KCMB_LAT-MFL1_pole_nside4096_1_of_1.fits) and estimate the equivalent white noise level in uK-arcmin to be ~0.7uK-arcmin.<br />
* For the effective white noise level when spreading all the hits uniformly, I scale the uK-arcmin number by sqrt(new_area/old_area). <br />
* The delensed A_L is from DSR fig.68.<br />
<br />
== Results ==<br />
'''Fig.1 Pole LAT-MFL1 EE/BB noise '''<br />
<br />
[[File:1207_LAT-MFL1_nlev_ukam2.png|border|600px]]<br />
<br />
'''Fig.2 Pole LAT-MFL1 Nhits '''<br />
<br />
[[File:1207_LAT-MFL1_nhits.png|border|600px]]<br />
<br />
'''Fig.3 Pole SAT-MFLS1 Nhits cut with LAT-MFL1 tophat'''<br />
<br />
[[File:1207_SAT-MFLS1_Nhits_bound.png |border|600px]]<br />
<br />
'''Fig.4 Pole SAT-MFLS1 map noise uK-arcmin'''<br />
<br />
[[File:1207_SAT-MFLS1_map_ukam.png |border|600px]]<br />
<br />
'''Fig.5 Pole LAT-MFL1 map noise uK-arcmin'''<br />
<br />
[[File:1207_LAT-MFL1_map_nlev_ukam.png |border|600px]]</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:1207_LAT-MFL1_nlev_ukam.png&diff=12214File:1207 LAT-MFL1 nlev ukam.png2020-12-09T19:26:38Z<p>Wlwu: Wlwu uploaded a new version of File:1207 LAT-MFL1 nlev ukam.png</p>
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<div></div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:1207_LAT-MFL1_map_nlev_ukam.png&diff=12208File:1207 LAT-MFL1 map nlev ukam.png2020-12-08T04:27:38Z<p>Wlwu: </p>
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<div></div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:1207_SAT-MFLS1_map_ukam.png&diff=12207File:1207 SAT-MFLS1 map ukam.png2020-12-08T04:27:28Z<p>Wlwu: </p>
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<div></div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:1207_SAT-MFLS1_Nhits_bound.png&diff=12206File:1207 SAT-MFLS1 Nhits bound.png2020-12-08T04:27:17Z<p>Wlwu: </p>
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<div></div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:1207_LAT-MFL1_nhits.png&diff=12205File:1207 LAT-MFL1 nhits.png2020-12-08T04:27:05Z<p>Wlwu: </p>
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<div></div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:1207_LAT-MFL1_nlev_ukam.png&diff=12204File:1207 LAT-MFL1 nlev ukam.png2020-12-08T04:26:18Z<p>Wlwu: </p>
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<div></div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p1&diff=12203Delensing LAT relative Nhits v0p12020-12-08T04:26:00Z<p>Wlwu: Created page with "This is a 2nd in a series of postings that document the process to answer the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\..."</p>
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<div>This is a 2nd in a series of postings that document the process to answer the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
Previous posting: [[ Delensing_LAT_relative_Nhits_v0p0 | Delensing_LAT_relative_Nhits_v0p0 ]]<br />
<br />
== Background/Summary ==<br />
This posting is written in response to a discussion from the scan-strategy call: if we have tophat-like hit patterns for the LAT, given fixed total N-hits, how would the delensed A_L change if the tophat pattern covers all the pixels hit by SATs vs the smaller tophat hit pattern given in the [[https://github.com/CMB-S4/s4_design_sim_tool DM reference-design sims ]]. <br />
<br />
Note that in the DM reference-design sims, the LAT (Pole-LAT-MFL1) N-hit pattern doesn't cover all the pixels hit by the Pole SAT-MF(HS1/HS2/LS1/LS2). So the regions outside the LAT hit would not have delensing. <br />
<br />
Key takeaways:<br />
* In the reference-design sims, the LAT hits cover about 50% of the SAT hit pattern; within that region, it gets 85% of the total number of hits. <br />
* Delensed A_L is ~0.09 in the reference-design LAT region.<br />
* Delensed A_L is ~0.12 if spreading the LAT hits across all the pixels seen by the SAT. <br />
<br />
== Method ==<br />
* I used information from one LAT and one SAT (both Pole) for extracting all the numbers (using just white noise)<br />
** LAT: Pole-LAT-MFL1 (93GHz, 2.2 FWHM); the N-hits for the MFs are the same.<br />
** SAT: Pole-SAT-MFLS1 (85GHz); the N-hits for all the MFs are the same.<br />
* I calculate the noise spectra from the LAT-MFL1 noise map (/global/cfs/cdirs/cmbs4/dm/dstool/output/s4_reference_design_noise_atmo_7splits/LAT-MFL1_pole/cmbs4_KCMB_LAT-MFL1_pole_nside4096_1_of_1.fits) and estimate the equivalent white noise level in uK-arcmin to be ~0.7uK-arcmin.<br />
* For the effective white noise level when spreading all the hits uniformly, I scale the uK-arcmin number by sqrt(new_area/old_area). <br />
* The delensed A_L is from DSR fig.68.<br />
<br />
== Results ==<br />
'''Fig.1 Pole LAT-MFL1 EE/BB noise '''<br />
<br />
[[File:1207_LAT-MFL1_nlev_ukam.png|border|600px]]<br />
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'''Fig.2 Pole LAT-MFL1 Nhits '''<br />
<br />
[[File:1207_LAT-MFL1_nhits.png|border|600px]]<br />
<br />
'''Fig.3 Pole SAT-MFLS1 Nhits cut with LAT-MFL1 tophat'''<br />
<br />
[[File:1207_SAT-MFLS1_Nhits_bound.png |border|600px]]<br />
<br />
'''Fig.4 Pole SAT-MFLS1 map noise uK-arcmin'''<br />
<br />
[[File:1207_SAT-MFLS1_map_ukam.png |border|600px]]<br />
<br />
'''Fig.5 Pole LAT-MFL1 map noise uK-arcmin'''<br />
<br />
[[File:1207_LAT-MFL1_map_nlev_ukam.png |border|600px]]</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=12202Simulation and Forecasting Logbook2020-12-08T02:58:12Z<p>Wlwu: /* Logbook Entries (reverse chronological) */</p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2020 Dec 7''': [[ Delensing_LAT_relative_Nhits_v0p1 | Delensing LAT relative Nhits, v0.1 ]] (K Wu)<br />
* '''2020 Nov 30''': [[Observation_matrix]] (Bischoff, Borrill, Keskitalo, Kisner, Simon & Zonca) Updated on 2020-12-07<br />
* '''2020 Nov 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20201128_dc6_LT_07_09/ ML searches with LT on 06 sims- results on models with non-Gaussian foregrounds - v2] (Caterina)<br />
* '''2020 Nov 16''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20201116_noise_int_down How N_ell integrates down with N_det in Keck 2013 data (5x150GHz receivers)] (Clem)<br />
* '''2020 Nov 16''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20201116_dc6_LT_07_09 ML searches with LT on 06 sims- results on models with non-Gaussian foregrounds] (Caterina)<br />
* '''2020 Nov 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20201110_bkfinal_06blt0709 BK-style power spectra of 06b.00/07/09 with iterative lensing templates] (Clem)<br />
* '''2020 Oct 19''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20201019_k2018_obseff Observing efficiency for BICEP3 and Keck during 2018] (Clem)<br />
* '''2020 Oct 13''': [[Correlation of iteratively reconstructed lensing templates to ideal for 06b III]] (Clem Pryke)<br />
* '''2020 Oct 12''': [[N eff Forecasting Comparison with DRAFT ILC]] (Srini Raghunathan)<br />
* '''2020 September 29''': [[File:transient_cadence_092920.pdf|Transient Cadence Information]] (N. Whitehorn)<br />
* '''2020 September 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200928_ML_dc06/ ML searches with LT on 06 sims - updated final files] (C. Umiltà)<br />
* '''2020 September 10''': [https://github.com/CMB-S4/s4mapbasedsims/blob/master/202006_reference_design/README.md DM reference design simulations] (Andrea Zonca and Reijo Keskitalo)<br />
* '''2020 September 08''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200908_ML_with_LT_on_06sims/ ML searches with LT on 06 sims] (C. Umiltà)<br />
* '''2020 August 31''': [[Atmosphere and number of detectors]] (Colin Bischoff and Reijo Keskitalo)<br />
* '''2020 August 28''': [[Atmospheric sanity check]] (Reijo Keskitalo)<br />
* '''2020 August 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200817_DM_AWG_sim/index.html Inspecting DM reference design sims] (Colin Bischoff), UPDATED 2020-08-20<br />
* '''2020 August 14''': [[Point source sensitivity from uK-arcmin/beam]] (Gil Holder)<br />
* '''2020 July 31''': [[Correlation of iteratively reconstructed lensing templates to ideal for 06b II]] (Clem Pryke)<br />
* '''2020 July 28''': [[ Delensing_LAT_relative_Nhits_v0p0 | Delensing LAT relative Nhits, v0.0 ]] (K Wu)<br />
* '''2020 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200709_bkfinal_06blt BK-style power spectra of 06b with iterative lensing templates] (Clem)<br />
* '''2020 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200708_itrecon_noise Investigation of iterative lensing templates] (Clem)<br />
* '''2020 July 7''': SAT split band justification slides [https://docs.google.com/presentation/d/1685uV44VTBhk8Nm3HIzQUSsgmgYQOZNLz3qUPIDeDqk/edit#slide=id.p v1], [https://docs.google.com/presentation/d/1vkF0nVrH7DjPAuga-njxnW6i5UbCwEgLNg1Iu9-oS0Q/edit#slide=id.p v2] (Colin Bischoff)<br />
* '''2020 July 7''': [[Delensing sensitivity - map-based delensing]] (Raphael Flauger)<br />
* '''2020 June 30''': [[Checking BB purity in re-analysis II]] (Clem Pryke)<br />
* '''2020 June 30''': [[White noise levels for high cadence scan at elevation of 40 degrees]] (Raphael Flauger)<br />
* '''2020 June 19''': [[Delensing sensitivity - updated sensitivities, beams, TT noise]] (Raphael Flauger)<br />
* '''2020 June 18''': [[Correlation of iteratively reconstructed lensing templates to ideal for 06b]] (Clem Pryke)<br />
* '''2020 June 11''': [[Map-based simulations for split and full bands]] (Raphael Flauger)<br />
* '''2020 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200611_splitbands/ Signal-to-noise on foregrounds from split band difference maps] (C. Bischoff)<br />
* '''2020 June 06''': [[Background on 20 GHz channel]] (Raphael Flauger)<br />
* '''2020 June 04''': [[Delensing sensitivity - preliminary results]] (Raphael Flauger)<br />
* '''2020 June 04''': [[N_eff Forecasting Comparison with DRAFT ILC|N_eff Forecasting Comparison with DRAFT ILC]] (Joel Meyers, Srini Raghunathan, Benjamin Wallisch)<br />
* '''2020 May 19''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200519_DM_AWG_noise/ Noise comparison between DM and Low-&#x2113; BB sims] (C. Bischoff)<br />
* '''2020 April 26''': [[Bayesian_vs_Template_Delensing|Bayesian vs. Template Delensing]] (Marius Millea)<br />
* '''2020 April 10''': [[Iterative curved sky s06b nofg lensing templates]] (Julien Carron)<br />
* '''2020 March 06''': [[Flat-sky_joint_MAP_lensing_template_for_06b_simulations|Flat-sky joint MAP lensing template for 06b simulations]] (Marius Millea)<br />
* '''2020 February 08''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200208_06_sims_details/ Data Challenge 06 simulations details] (C. Umiltà)<br />
* '''2020 February 07''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200207_ILC_maps_part3 Preliminary ILC maps part 3] (C. Umiltà)<br />
* '''2020 January 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200110_ILC_maps_part2 Preliminary ILC maps part 2] (C. Umiltà)<br />
* '''2019 December 14''': [[Correlation of reconstructed lensing template to ideal for 06b.00]] (Clem Pryke)<br />
* '''2019 December 12''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20191209_ILC_maps_prelim Preliminary ILC maps part 1] (C. Umiltà)<br />
* '''2019 November 12''': [[SAT detector counts, NET, and overall efficiency from DSR]] (C. Bischoff)<br />
* '''2019 November 12''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20191112_bk_scans Actual BK scanning trajectory] (Clem)<br />
* '''2019 November 1''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20191101_dc06_specsmaps DSR Sim Map Set 06 - some spectra and map check plots] (Clem)<br />
* '''2019 October 25''': [[Modulated scan high cadence LAT]] (Reijo)<br />
* '''2019 October 16''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20191016_dc06_dsr DSR Sim Map Set 06 with simple scaling from BK15] (Clem)<br />
* '''2019 September 16''': [[PureB by Messenger Method]] (Michael Ray, Colin Bischoff)<br />
* '''2019 August 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190829_noise_params_DSR/ Noise parameters for the DC5 DSR-like data challenge] (Ben Racine)<br />
* '''2019 June 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190607_LATSTM/ LAT CDT-STM Noise Levels] (Victor Buza)<br />
* '''2019 May 19''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190519_about_DSR_AppendixA_plots_and_table/ sigma(r) vs r: plots and tables for the DSR] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190509_b3_obseff Observing efficiency reality check] (Clem)<br />
* '''2019 May 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190511_sigmar_vs_r_galcuts/ sigma(r) vs r: possible figures for the DSR (v4): Galactic cuts added (In progress)] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 11''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 May 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190507_sigmar_vs_r_combined_hits/ sigma(r) vs r: possible figures for the DSR (v3): More realistic combination and fixed 20GHz] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 6''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 April 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190430_sigmar_vs_r_forDSR/ sigma(r) vs r: possible figures for the DSR (v2): more optimal weighting] (Ben Racine and Raphael Flauger)<br />
* '''2019 April 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190501_obseff Efficiency for Reijo's observation pattern sims] (Clem)<br />
* '''2019 April 29''': [[Fisher forecasts for inverse noise variance weighting]] (Raphael)<br />
* '''2019 April 22''': [[WAFTT results part 3]] (Raphael)<br />
* '''2019 April 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190418_sigmar_vs_r/ sigma(r) vs r: possible figures for the DSR] (Ben Racine)<br />
* '''2019 April 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190410_closedloop_BK15_S4 Zero order closed loop test of performance based scaling - ML search] (Ben Racine)<br />
* '''2019 March 31''': [[Analysis results for configurations 30-33]] (Raphael)<br />
* '''2019 March 30''': [[Characterization of simulations for configurations 30-33]] (Raphael)<br />
* '''2019 March 26''': [[Simulations for configurations with different frequency coverage]] (Raphael)<br />
* '''2019 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190326_bkfinal_05 Zero order closed loop test of performance based scaling - BK15 regen power spectra] (Clem)<br />
* '''2019 March 25''': [[Deeper SAT from Chile II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Wider SAT from the Pole II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Deep SAT from the Pole]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 18''': [https://cmb-s4.org/wiki/index.php/Optimal_lensing_fermilab Details on optimal lensing Fermilab presentation / 02.xx real delensing] (Marius Millea)<br />
* '''2019 March 18''': [[High cadence LAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 March 18''': [[WAFTT results part 2]] (Raphael)<br />
* '''2019 March 18''': [[Wider SAT from the Pole]] (Reijo Keskitalo)<br />
* '''2019 March 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook//20190308_MLsearch_no85no145/ Maximum likelihood search results without 85GHz and 145GHz] (Ben Racine)<br />
* '''2019 March 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_noiseparams_bk15_forS4/ BK15 noise levels for S4 sims] (Ben Racine) <br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181127_bpwf_DC4 A look at DC4 bandpower window functions] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Neff and beams from field sources|Neff and a back-of-the-envelope estimate of beam uncertainty from field sources]] (Tom C.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p0&diff=12190Delensing LAT relative Nhits v0p02020-12-01T06:37:10Z<p>Wlwu: /* Results */</p>
<hr />
<div>This posting documents initial stabs at answering the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
<br />
== Background ==<br />
So far (e.g. in low-ell BB Data Challenge 06), the relative Nhits maps of the Delensing LAT is taken to be identical to those of the Pole Deep SATs. Given that the lensing template is generated from CMB x phi(CMB, CMB) as opposed to direct imaging of map fluctuations in other components, one would expect the S/N of the lensing modes vs those of the other components to scale differently for the same input noise. <br />
<br />
In this post, I use a very simple case to build intuition. Specifically, I answer this question: given a single-frequency SAT Nhits map, what should the Delensing LAT distribution of noise levels be such that S/N = 1 for the residual lensing modes. <br />
<br />
In the regime where delensing is the limiting factor for sigma(r), this would give a close approximation of the actual distribution of noise levels (and hence Nhits) for the Delensing LAT. I list the next steps in order to make this more realistic and applicable to the survey design of the Delensing LAT.<br />
<br />
== Method ==<br />
* Generate 100 realizations of 1/ell noise given the DSR configuration of the SAT 95GHz Pole deep survey on flatsky (1 arcmin pixels) using this [[Delensing_sensitivity_-_updated_sensitivities,_beams,_TT_noise#SAT_specifications | table ]];<br />
* Apply scale factor specified below table 1 of this [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200208_06_sims_details/ posting ] ;<br />
* Divide the noise map by the square-root of the SAT 95GHz relative hits map;<br />
* Calculate the noise levels in uK-arcmin per pixel by measuring the standard deviation of each pixel across the 100 realizations of noise; this gives the white noise level. <br />
* Scale the noise levels by ~1.17 in order to estimate the noise levels at ell~100 (factor is eyeballed from input 1/ell noise spectrum); <br />
* Estimate (by interpolation of inputs to fig.68 of the DSR and extended to higher pol noise levels) the input Delensing LAT noise levels (at 95GHz, i.e. 2.6' FWHM) required in order for the residual lensing power to match the SAT noise power.<br />
<br />
== Results ==<br />
<br />
'''Fig.1 DC05 95GHz Pole Deep SAT noise levels [uK-arcmin]'''<br />
<br />
[[File:0728_SAT95ghz_ell100_nlev_ukam.png|border|600px]]<br />
<br />
* The color range is set to 0-5uK-arcmin. Where the color saturates, the lensing modes are imaged to S/N~1. The algorithm would not assign any weight for the LAT in this region.<br />
<br />
'''Fig.2 required LAT noise levels for residual lensing S/N=1 [uK-arcmin]'''<br />
<br />
[[File:0728_LAT95ghz_nlev_ukam.png|border|600px]]<br />
<br />
* The color stretch is the same in this figure as the one above. There are some regions below 5uK-arcmin in the SAT noise map but don't have information in this LAT map. There will be the wide field LAT overlap for these regions (with Q/U noise levels of ~3uK-arcmin at 95/150 bands) so anything in LAT that doesn't require ~< 5uK-arcmin could be allocated to the wide-field LAT.<br />
<br />
<br />
'''Fig.3 SAT vs LAT noise level slices'''<br />
<br />
[[File:0728_noise_ukam_SAT_LAT_slices.png|border|600px]]<br />
<br />
* This shows the noise level slices of the SAT vs the LAT. The Nhit map shape scales as 1/(nlev)^2. <br />
* We see that the slope of change of the LAT noise is much faster than the SAT noise -- i.e. as the Nhits of the SAT decreases, the Nhits of the LAT should decrease more quickly to keep delensed residuals S/N=1. <br />
* In other words, given the same total Nhits, we should concentrate more of the observing time closer to the center of the map for the LAT as compared to the SAT (in this simple setup).<br />
<br />
<br />
Noise level note (added 2020-11-26): The central patch of the LAT noise level map corresponds to ~0.18uK-arcmin white noise. For reference, using the V3R0 Delensing LAT setup (with white noise of 0.5uK-arcmin) scaled with this relative hits map gives noise fluctuations in the central patch equivalent to 0.4uK-arcmin. So the V3R0 LAT setup would still leave the delensed residual slightly dominate over white noise (in this single freq. toy setup).<br />
<br />
== Next steps ==<br />
* To account for foregrounds, and optimize the relative Nhit of the delensing LAT to minimize sigma(r), one can match the S/N of the delensed residuals to a map of SAT S/N of foregrounds from some component-separation methods. <br />
* Use AL^res numbers using input noise-curves generated post ILC.<br />
* Check the Nhits of the wide-field LAT in the Pole Deep patch and calculate the equivalent noise levels. This can inform us on how much of the Delensing LAT observing can be concentrated on the deepest of the Pole Deep patches.<br />
* This analysis doesn't account for the deflection of modes. The LAT maps should cover slightly larger areas (~few arcmin) at the same depths in order to estimate the lensing B modes that get deflected from slightly outside the boundary definition of the 'deepest' part of the Pole Deep map. <br />
* Map-based analysis.</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p0&diff=11625Delensing LAT relative Nhits v0p02020-07-29T02:20:03Z<p>Wlwu: /* Next steps */</p>
<hr />
<div>This posting documents initial stabs at answering the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
<br />
== Background ==<br />
So far (e.g. in low-ell BB Data Challenge 06), the relative Nhits maps of the Delensing LAT is taken to be identical to those of the Pole Deep SATs. Given that the lensing template is generated from CMB x phi(CMB, CMB) as opposed to direct imaging of map fluctuations in other components, one would expect the S/N of the lensing modes vs those of the other components to scale differently for the same input noise. <br />
<br />
In this post, I use a very simple case to build intuition. Specifically, I answer this question: given a single-frequency SAT Nhits map, what should the Delensing LAT distribution of noise levels be such that S/N = 1 for the residual lensing modes. <br />
<br />
In the regime where delensing is the limiting factor for sigma(r), this would give a close approximation of the actual distribution of noise levels (and hence Nhits) for the Delensing LAT. I list the next steps in order to make this more realistic and applicable to the survey design of the Delensing LAT.<br />
<br />
== Method ==<br />
* Generate 100 realizations of 1/ell noise given the DSR configuration of the SAT 95GHz Pole deep survey on flatsky (1 arcmin pixels) using this [[Delensing_sensitivity_-_updated_sensitivities,_beams,_TT_noise#SAT_specifications | table ]];<br />
* Apply scale factor specified below table 1 of this [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200208_06_sims_details/ posting ] ;<br />
* Divide the noise map by the square-root of the SAT 95GHz relative hits map;<br />
* Calculate the noise levels in uK-arcmin per pixel by measuring the standard deviation of each pixel across the 100 realizations of noise; this gives the white noise level. <br />
* Scale the noise levels by ~1.17 in order to estimate the noise levels at ell~100 (factor is eyeballed from input 1/ell noise spectrum); <br />
* Estimate (by interpolation of inputs to fig.68 of the DSR and extended to higher pol noise levels) the input Delensing LAT noise levels (at 95GHz, i.e. 2.6' FWHM) required in order for the residual lensing power to match the SAT noise power.<br />
<br />
== Results ==<br />
<br />
'''Fig.1 DC05 95GHz Pole Deep SAT noise levels [uK-arcmin]'''<br />
<br />
[[File:0728_SAT95ghz_ell100_nlev_ukam.png|border|600px]]<br />
<br />
* The color range is set to 0-5uK-arcmin. Where the color saturates, the lensing modes are imaged to S/N~1. The algorithm would not assign any weight for the LAT in this region.<br />
<br />
'''Fig.2 required LAT noise levels for residual lensing S/N=1 [uK-arcmin]'''<br />
<br />
[[File:0728_LAT95ghz_nlev_ukam.png|border|600px]]<br />
<br />
* The color stretch is the same in this figure as the one above. There are some regions below 5uK-arcmin in the SAT noise map but don't have information in this LAT map. There will be the wide field LAT overlap for these regions (with Q/U noise levels of ~3uK-arcmin at 95/150 bands) so anything in LAT that doesn't require ~< 5uK-arcmin could be allocated to the wide-field LAT.<br />
<br />
<br />
'''Fig.3 SAT vs LAT noise level slices'''<br />
<br />
[[File:0728_noise_ukam_SAT_LAT_slices.png|border|600px]]<br />
<br />
* This shows the noise level slices of the SAT vs the LAT. The Nhit map shape scales as 1/(nlev)^2. <br />
* We see that the slope of change of the LAT noise is much faster than the SAT noise -- i.e. as the Nhits of the SAT decreases, the Nhits of the LAT should decrease more quickly to keep delensed residuals S/N=1. <br />
* In other words, given the same total Nhits, we should concentrate more of the observing time closer to the center of the map for the LAT as compared to the SAT (in this simple setup).<br />
<br />
== Next steps ==<br />
* To account for foregrounds, and optimize the relative Nhit of the delensing LAT to minimize sigma(r), one can match the S/N of the delensed residuals to a map of SAT S/N of foregrounds from some component-separation methods. <br />
* Use AL^res numbers using input noise-curves generated post ILC.<br />
* Check the Nhits of the wide-field LAT in the Pole Deep patch and calculate the equivalent noise levels. This can inform us on how much of the Delensing LAT observing can be concentrated on the deepest of the Pole Deep patches.<br />
* This analysis doesn't account for the deflection of modes. The LAT maps should cover slightly larger areas (~few arcmin) at the same depths in order to estimate the lensing B modes that get deflected from slightly outside the boundary definition of the 'deepest' part of the Pole Deep map. <br />
* Map-based analysis.</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p0&diff=11624Delensing LAT relative Nhits v0p02020-07-29T02:09:00Z<p>Wlwu: /* Results */</p>
<hr />
<div>This posting documents initial stabs at answering the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
<br />
== Background ==<br />
So far (e.g. in low-ell BB Data Challenge 06), the relative Nhits maps of the Delensing LAT is taken to be identical to those of the Pole Deep SATs. Given that the lensing template is generated from CMB x phi(CMB, CMB) as opposed to direct imaging of map fluctuations in other components, one would expect the S/N of the lensing modes vs those of the other components to scale differently for the same input noise. <br />
<br />
In this post, I use a very simple case to build intuition. Specifically, I answer this question: given a single-frequency SAT Nhits map, what should the Delensing LAT distribution of noise levels be such that S/N = 1 for the residual lensing modes. <br />
<br />
In the regime where delensing is the limiting factor for sigma(r), this would give a close approximation of the actual distribution of noise levels (and hence Nhits) for the Delensing LAT. I list the next steps in order to make this more realistic and applicable to the survey design of the Delensing LAT.<br />
<br />
== Method ==<br />
* Generate 100 realizations of 1/ell noise given the DSR configuration of the SAT 95GHz Pole deep survey on flatsky (1 arcmin pixels) using this [[Delensing_sensitivity_-_updated_sensitivities,_beams,_TT_noise#SAT_specifications | table ]];<br />
* Apply scale factor specified below table 1 of this [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200208_06_sims_details/ posting ] ;<br />
* Divide the noise map by the square-root of the SAT 95GHz relative hits map;<br />
* Calculate the noise levels in uK-arcmin per pixel by measuring the standard deviation of each pixel across the 100 realizations of noise; this gives the white noise level. <br />
* Scale the noise levels by ~1.17 in order to estimate the noise levels at ell~100 (factor is eyeballed from input 1/ell noise spectrum); <br />
* Estimate (by interpolation of inputs to fig.68 of the DSR and extended to higher pol noise levels) the input Delensing LAT noise levels (at 95GHz, i.e. 2.6' FWHM) required in order for the residual lensing power to match the SAT noise power.<br />
<br />
== Results ==<br />
<br />
'''Fig.1 DC05 95GHz Pole Deep SAT noise levels [uK-arcmin]'''<br />
<br />
[[File:0728_SAT95ghz_ell100_nlev_ukam.png|border|600px]]<br />
<br />
* The color range is set to 0-5uK-arcmin. Where the color saturates, the lensing modes are imaged to S/N~1. The algorithm would not assign any weight for the LAT in this region.<br />
<br />
'''Fig.2 required LAT noise levels for residual lensing S/N=1 [uK-arcmin]'''<br />
<br />
[[File:0728_LAT95ghz_nlev_ukam.png|border|600px]]<br />
<br />
* The color stretch is the same in this figure as the one above. There are some regions below 5uK-arcmin in the SAT noise map but don't have information in this LAT map. There will be the wide field LAT overlap for these regions (with Q/U noise levels of ~3uK-arcmin at 95/150 bands) so anything in LAT that doesn't require ~< 5uK-arcmin could be allocated to the wide-field LAT.<br />
<br />
<br />
'''Fig.3 SAT vs LAT noise level slices'''<br />
<br />
[[File:0728_noise_ukam_SAT_LAT_slices.png|border|600px]]<br />
<br />
* This shows the noise level slices of the SAT vs the LAT. The Nhit map shape scales as 1/(nlev)^2. <br />
* We see that the slope of change of the LAT noise is much faster than the SAT noise -- i.e. as the Nhits of the SAT decreases, the Nhits of the LAT should decrease more quickly to keep delensed residuals S/N=1. <br />
* In other words, given the same total Nhits, we should concentrate more of the observing time closer to the center of the map for the LAT as compared to the SAT (in this simple setup).<br />
<br />
== Next steps ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p0&diff=11623Delensing LAT relative Nhits v0p02020-07-29T01:55:47Z<p>Wlwu: /* Results */</p>
<hr />
<div>This posting documents initial stabs at answering the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
<br />
== Background ==<br />
So far (e.g. in low-ell BB Data Challenge 06), the relative Nhits maps of the Delensing LAT is taken to be identical to those of the Pole Deep SATs. Given that the lensing template is generated from CMB x phi(CMB, CMB) as opposed to direct imaging of map fluctuations in other components, one would expect the S/N of the lensing modes vs those of the other components to scale differently for the same input noise. <br />
<br />
In this post, I use a very simple case to build intuition. Specifically, I answer this question: given a single-frequency SAT Nhits map, what should the Delensing LAT distribution of noise levels be such that S/N = 1 for the residual lensing modes. <br />
<br />
In the regime where delensing is the limiting factor for sigma(r), this would give a close approximation of the actual distribution of noise levels (and hence Nhits) for the Delensing LAT. I list the next steps in order to make this more realistic and applicable to the survey design of the Delensing LAT.<br />
<br />
== Method ==<br />
* Generate 100 realizations of 1/ell noise given the DSR configuration of the SAT 95GHz Pole deep survey on flatsky (1 arcmin pixels) using this [[Delensing_sensitivity_-_updated_sensitivities,_beams,_TT_noise#SAT_specifications | table ]];<br />
* Apply scale factor specified below table 1 of this [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200208_06_sims_details/ posting ] ;<br />
* Divide the noise map by the square-root of the SAT 95GHz relative hits map;<br />
* Calculate the noise levels in uK-arcmin per pixel by measuring the standard deviation of each pixel across the 100 realizations of noise; this gives the white noise level. <br />
* Scale the noise levels by ~1.17 in order to estimate the noise levels at ell~100 (factor is eyeballed from input 1/ell noise spectrum); <br />
* Estimate (by interpolation of inputs to fig.68 of the DSR and extended to higher pol noise levels) the input Delensing LAT noise levels (at 95GHz, i.e. 2.6' FWHM) required in order for the residual lensing power to match the SAT noise power.<br />
<br />
== Results ==<br />
<br />
'''Fig.1 DC05 95GHz Pole Deep SAT noise levels [uK-arcmin]'''<br />
<br />
[[File:0728_SAT95ghz_ell100_nlev_ukam.png|border|600px]]<br />
<br />
'''Fig.2 required LAT noise levels for residual lensing S/N=1 [uK-arcmin]'''<br />
<br />
[[File:0728_LAT95ghz_nlev_ukam.png|border|600px]]<br />
<br />
'''Fig.3 SAT vs LAT noise level slices'''<br />
<br />
[[File:0728_noise_ukam_SAT_LAT_slices.png|border|600px]]<br />
<br />
== Next steps ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:0728_noise_ukam_SAT_LAT_slices.png&diff=11622File:0728 noise ukam SAT LAT slices.png2020-07-29T01:55:23Z<p>Wlwu: </p>
<hr />
<div></div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:0728_LAT95ghz_nlev_ukam.png&diff=11621File:0728 LAT95ghz nlev ukam.png2020-07-29T01:55:09Z<p>Wlwu: </p>
<hr />
<div></div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:0728_SAT95ghz_ell100_nlev_ukam.png&diff=11620File:0728 SAT95ghz ell100 nlev ukam.png2020-07-29T01:54:54Z<p>Wlwu: </p>
<hr />
<div></div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p0&diff=11619Delensing LAT relative Nhits v0p02020-07-29T01:54:33Z<p>Wlwu: /* Results */</p>
<hr />
<div>This posting documents initial stabs at answering the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
<br />
== Background ==<br />
So far (e.g. in low-ell BB Data Challenge 06), the relative Nhits maps of the Delensing LAT is taken to be identical to those of the Pole Deep SATs. Given that the lensing template is generated from CMB x phi(CMB, CMB) as opposed to direct imaging of map fluctuations in other components, one would expect the S/N of the lensing modes vs those of the other components to scale differently for the same input noise. <br />
<br />
In this post, I use a very simple case to build intuition. Specifically, I answer this question: given a single-frequency SAT Nhits map, what should the Delensing LAT distribution of noise levels be such that S/N = 1 for the residual lensing modes. <br />
<br />
In the regime where delensing is the limiting factor for sigma(r), this would give a close approximation of the actual distribution of noise levels (and hence Nhits) for the Delensing LAT. I list the next steps in order to make this more realistic and applicable to the survey design of the Delensing LAT.<br />
<br />
== Method ==<br />
* Generate 100 realizations of 1/ell noise given the DSR configuration of the SAT 95GHz Pole deep survey on flatsky (1 arcmin pixels) using this [[Delensing_sensitivity_-_updated_sensitivities,_beams,_TT_noise#SAT_specifications | table ]];<br />
* Apply scale factor specified below table 1 of this [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200208_06_sims_details/ posting ] ;<br />
* Divide the noise map by the square-root of the SAT 95GHz relative hits map;<br />
* Calculate the noise levels in uK-arcmin per pixel by measuring the standard deviation of each pixel across the 100 realizations of noise; this gives the white noise level. <br />
* Scale the noise levels by ~1.17 in order to estimate the noise levels at ell~100 (factor is eyeballed from input 1/ell noise spectrum); <br />
* Estimate (by interpolation of inputs to fig.68 of the DSR and extended to higher pol noise levels) the input Delensing LAT noise levels (at 95GHz, i.e. 2.6' FWHM) required in order for the residual lensing power to match the SAT noise power.<br />
<br />
== Results ==<br />
<br />
'''Fig.1 DC05 95GHz Pole Deep SAT noise levels [uK-arcmin]'''<br />
[[File:0728_SAT95ghz_ell100_nlev_ukam.png|border|600px]]<br />
<br />
'''Fig.2 required LAT noise levels for residual lensing S/N=1 [uK-arcmin]'''<br />
[[File:0728_LAT95ghz_nlev_ukam.png|border|600px]]<br />
<br />
'''Fig.3 SAT vs LAT noise level slices'''<br />
[[File:0728_noise_ukam_SAT_LAT_slices.png|border|600px]]<br />
<br />
== Next steps ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p0&diff=11604Delensing LAT relative Nhits v0p02020-07-28T19:02:10Z<p>Wlwu: /* Method */</p>
<hr />
<div>This posting documents initial stabs at answering the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
<br />
== Background ==<br />
So far (e.g. in low-ell BB Data Challenge 06), the relative Nhits maps of the Delensing LAT is taken to be identical to those of the Pole Deep SATs. Given that the lensing template is generated from CMB x phi(CMB, CMB) as opposed to direct imaging of map fluctuations in other components, one would expect the S/N of the lensing modes vs those of the other components to scale differently for the same input noise. <br />
<br />
In this post, I use a very simple case to build intuition. Specifically, I answer this question: given a single-frequency SAT Nhits map, what should the Delensing LAT distribution of noise levels be such that S/N = 1 for the residual lensing modes. <br />
<br />
In the regime where delensing is the limiting factor for sigma(r), this would give a close approximation of the actual distribution of noise levels (and hence Nhits) for the Delensing LAT. I list the next steps in order to make this more realistic and applicable to the survey design of the Delensing LAT.<br />
<br />
== Method ==<br />
* Generate 100 realizations of 1/ell noise given the DSR configuration of the SAT 95GHz Pole deep survey on flatsky (1 arcmin pixels) using this [[Delensing_sensitivity_-_updated_sensitivities,_beams,_TT_noise#SAT_specifications | table ]];<br />
* Apply scale factor specified below table 1 of this [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200208_06_sims_details/ posting ] ;<br />
* Divide the noise map by the square-root of the SAT 95GHz relative hits map;<br />
* Calculate the noise levels in uK-arcmin per pixel by measuring the standard deviation of each pixel across the 100 realizations of noise; this gives the white noise level. <br />
* Scale the noise levels by ~1.17 in order to estimate the noise levels at ell~100 (factor is eyeballed from input 1/ell noise spectrum); <br />
* Estimate (by interpolation of inputs to fig.68 of the DSR and extended to higher pol noise levels) the input Delensing LAT noise levels (at 95GHz, i.e. 2.6' FWHM) required in order for the residual lensing power to match the SAT noise power.<br />
<br />
== Results ==<br />
<br />
== Next steps ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p0&diff=11603Delensing LAT relative Nhits v0p02020-07-28T18:58:08Z<p>Wlwu: /* Method */</p>
<hr />
<div>This posting documents initial stabs at answering the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
<br />
== Background ==<br />
So far (e.g. in low-ell BB Data Challenge 06), the relative Nhits maps of the Delensing LAT is taken to be identical to those of the Pole Deep SATs. Given that the lensing template is generated from CMB x phi(CMB, CMB) as opposed to direct imaging of map fluctuations in other components, one would expect the S/N of the lensing modes vs those of the other components to scale differently for the same input noise. <br />
<br />
In this post, I use a very simple case to build intuition. Specifically, I answer this question: given a single-frequency SAT Nhits map, what should the Delensing LAT distribution of noise levels be such that S/N = 1 for the residual lensing modes. <br />
<br />
In the regime where delensing is the limiting factor for sigma(r), this would give a close approximation of the actual distribution of noise levels (and hence Nhits) for the Delensing LAT. I list the next steps in order to make this more realistic and applicable to the survey design of the Delensing LAT.<br />
<br />
== Method ==<br />
* Generate 100 realizations of 1/ell noise given the DSR configuration of the SAT 95GHz Pole deep survey on flatsky (1 arcmin pixels) using this [[Delensing_sensitivity_-_updated_sensitivities,_beams,_TT_noise#SAT_specifications | table ]];<br />
* Apply scale factor specified below table 1 of this [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200208_06_sims_details/ posting ] ;<br />
* Divide the noise map by the square-root of the SAT 95GHz relative hits map;<br />
* Calculate the noise levels in uK-arcmin per pixel by measuring the standard deviation of each pixel across the 100 realizations of noise; this gives the white noise level. <br />
* Scale the noise levels by ~1.17 in order to estimate the noise levels at ell~100 (factor is eyeballed from input 1/ell noise spectrum); <br />
* Estimate (by interpolation of inputs to fig.68 of the DSR and extended to higher pol noise levels) the input Delensing LAT noise levels (at 95GHz, i.e. 2.6' FWHM) required in order for the residual lensing power to match the SAT noise.<br />
<br />
== Results ==<br />
<br />
== Next steps ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p0&diff=11602Delensing LAT relative Nhits v0p02020-07-28T18:56:50Z<p>Wlwu: /* Background */</p>
<hr />
<div>This posting documents initial stabs at answering the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
<br />
== Background ==<br />
So far (e.g. in low-ell BB Data Challenge 06), the relative Nhits maps of the Delensing LAT is taken to be identical to those of the Pole Deep SATs. Given that the lensing template is generated from CMB x phi(CMB, CMB) as opposed to direct imaging of map fluctuations in other components, one would expect the S/N of the lensing modes vs those of the other components to scale differently for the same input noise. <br />
<br />
In this post, I use a very simple case to build intuition. Specifically, I answer this question: given a single-frequency SAT Nhits map, what should the Delensing LAT distribution of noise levels be such that S/N = 1 for the residual lensing modes. <br />
<br />
In the regime where delensing is the limiting factor for sigma(r), this would give a close approximation of the actual distribution of noise levels (and hence Nhits) for the Delensing LAT. I list the next steps in order to make this more realistic and applicable to the survey design of the Delensing LAT.<br />
<br />
== Method ==<br />
* Generate 100 realizations of 1/ell noise given the DSR configuration of the SAT 95GHz Pole deep survey on flatsky (1 arcmin pixels) using this [[Delensing_sensitivity_-_updated_sensitivities,_beams,_TT_noise#SAT_specifications | table ]];<br />
* Apply scale factor specified below table 1 of this [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200208_06_sims_details/ posting ] ;<br />
* Divide the noise map by the square-root of the SAT 95GHz relative hits map;<br />
* Calculate the noise levels in uK-arcmin per pixel by measuring the standard deviation of each pixel across the 100 realizations of noise; this gives the white noise level. <br />
* Scale the noise levels by ~1.17 in order to estimate the noise levels at ell~100 (factor is eyeballed from input 1/ell noise spectrum); <br />
* Estimate (by interpolation) the input Delensing LAT noise levels (at 95GHz, i.e. 2.6' FWHM) required in order for the residual lensing power to match the SAT noise.<br />
<br />
== Results ==<br />
<br />
== Next steps ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p0&diff=11601Delensing LAT relative Nhits v0p02020-07-28T18:56:13Z<p>Wlwu: /* Background */</p>
<hr />
<div>This posting documents initial stabs at answering the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
<br />
== Background ==<br />
So far (e.g. in low-ell BB Data Challenge 06), the relative Nhits maps of the Delensing LAT is taken to be identical to those of the Pole Deep SATs. Given that the lensing template is generated from CMB x phi(CMB, CMB) as opposed to direct imaging of map fluctuations in other components, one would expect the S/N of the lensing modes vs those of the other components to scale differently for the same input noise. <br />
<br />
In this post, I use a very simple case to build intuition. Specifically, I answer this question: given a single-frequency SAT Nhits map, what should the Delensing LAT distribution of noise levels be such that S/N = 1 for the residual lensing modes. <br />
<br />
In the regime where delensing is the limiting factor for sigma(r), this would give a close approximation of what the actual distribution of noise levels (and hence Nhits) for the Delensing LAT. I list the next steps in order to make this more realistic and applicable to survey design of the Delensing LAT.<br />
<br />
== Method ==<br />
* Generate 100 realizations of 1/ell noise given the DSR configuration of the SAT 95GHz Pole deep survey on flatsky (1 arcmin pixels) using this [[Delensing_sensitivity_-_updated_sensitivities,_beams,_TT_noise#SAT_specifications | table ]];<br />
* Apply scale factor specified below table 1 of this [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200208_06_sims_details/ posting ] ;<br />
* Divide the noise map by the square-root of the SAT 95GHz relative hits map;<br />
* Calculate the noise levels in uK-arcmin per pixel by measuring the standard deviation of each pixel across the 100 realizations of noise; this gives the white noise level. <br />
* Scale the noise levels by ~1.17 in order to estimate the noise levels at ell~100 (factor is eyeballed from input 1/ell noise spectrum); <br />
* Estimate (by interpolation) the input Delensing LAT noise levels (at 95GHz, i.e. 2.6' FWHM) required in order for the residual lensing power to match the SAT noise.<br />
<br />
== Results ==<br />
<br />
== Next steps ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p0&diff=11600Delensing LAT relative Nhits v0p02020-07-28T18:55:57Z<p>Wlwu: /* Background */</p>
<hr />
<div>This posting documents initial stabs at answering the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
<br />
== Background ==<br />
So far (e.g. in low-ell BB Data Challenge 06), the relative Nhits maps of the Delensing LAT is taken to be identical to those of the Pole Deep SATs. Given that the lensing template is generated from CMB x phi(CMB, CMB) as opposed to direct imaging of map fluctuations in other components, one would expect the S/N of the lensing modes vs those of the other components to scale differently for the same input noise. <br />
<br />
In this post, I use a very simple case to build intuition. Specifically, I answer this question: given a single-frequency SAT Nhits map, what should the Delensing LAT distribution of noise levels be such that S/N = 1 for the residual lensing modes. <br />
<br />
In the regime where delensing is the limiting factor of sigma(r), this would give a close approximation of what the actual distribution of noise levels (and hence Nhits) for the Delensing LAT. I list the next steps in order to make this more realistic and applicable to survey design of the Delensing LAT.<br />
<br />
== Method ==<br />
* Generate 100 realizations of 1/ell noise given the DSR configuration of the SAT 95GHz Pole deep survey on flatsky (1 arcmin pixels) using this [[Delensing_sensitivity_-_updated_sensitivities,_beams,_TT_noise#SAT_specifications | table ]];<br />
* Apply scale factor specified below table 1 of this [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200208_06_sims_details/ posting ] ;<br />
* Divide the noise map by the square-root of the SAT 95GHz relative hits map;<br />
* Calculate the noise levels in uK-arcmin per pixel by measuring the standard deviation of each pixel across the 100 realizations of noise; this gives the white noise level. <br />
* Scale the noise levels by ~1.17 in order to estimate the noise levels at ell~100 (factor is eyeballed from input 1/ell noise spectrum); <br />
* Estimate (by interpolation) the input Delensing LAT noise levels (at 95GHz, i.e. 2.6' FWHM) required in order for the residual lensing power to match the SAT noise.<br />
<br />
== Results ==<br />
<br />
== Next steps ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p0&diff=11599Delensing LAT relative Nhits v0p02020-07-28T18:54:52Z<p>Wlwu: /* Method */</p>
<hr />
<div>This posting documents initial stabs at answering the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
<br />
== Background ==<br />
So far (e.g. in low-ell BB Data Challenge 06), the relative Nhits maps of the Delensing LAT is taken to be identical to those of the Pole Deep SATs. Given that the lensing template is generated from CMB x phi(CMB, CMB) as opposed to direct imaging of map fluctuations in other components, one would expect the S/N of the lensing modes vs those of the other components to scale differently for the same input noise. <br />
<br />
In this post, I use a very simple case to build intuition. Specifically, I answer this question: given a single-frequency SAT Nhits map, what should the Delensing LAT distribution of noise levels be in order for the S/N = 1 for the residual lensing modes. <br />
<br />
In the regime where delensing is the limiting factor of sigma(r), this would give a close approximation of what the actual distribution of noise levels (and hence Nhits) for the Delensing LAT. I list the next steps in order to make this more realistic and applicable to survey design of the Delensing LAT. <br />
<br />
<br />
== Method ==<br />
* Generate 100 realizations of 1/ell noise given the DSR configuration of the SAT 95GHz Pole deep survey on flatsky (1 arcmin pixels) using this [[Delensing_sensitivity_-_updated_sensitivities,_beams,_TT_noise#SAT_specifications | table ]];<br />
* Apply scale factor specified below table 1 of this [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200208_06_sims_details/ posting ] ;<br />
* Divide the noise map by the square-root of the SAT 95GHz relative hits map;<br />
* Calculate the noise levels in uK-arcmin per pixel by measuring the standard deviation of each pixel across the 100 realizations of noise; this gives the white noise level. <br />
* Scale the noise levels by ~1.17 in order to estimate the noise levels at ell~100 (factor is eyeballed from input 1/ell noise spectrum); <br />
* Estimate (by interpolation) the input Delensing LAT noise levels (at 95GHz, i.e. 2.6' FWHM) required in order for the residual lensing power to match the SAT noise.<br />
<br />
== Results ==<br />
<br />
== Next steps ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Delensing_LAT_relative_Nhits_v0p0&diff=11598Delensing LAT relative Nhits v0p02020-07-28T18:40:26Z<p>Wlwu: Created page with "This posting documents initial stabs at answering the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? == B..."</p>
<hr />
<div>This posting documents initial stabs at answering the question: how should the Nhits map of the Delensing LAT be optimized in order to minimize <math>\sigma(r)</math>? <br />
<br />
<br />
== Background ==<br />
So far (e.g. in low-ell BB Data Challenge 06), the relative Nhits maps of the Delensing LAT is taken to be identical to those of the Pole Deep SATs. Given that the lensing template is generated from CMB x phi(CMB, CMB) as opposed to direct imaging of map fluctuations in other components, one would expect the S/N of the lensing modes vs those of the other components to scale differently for the same input noise. <br />
<br />
In this post, I use a very simple case to build intuition. Specifically, I answer this question: given a single-frequency SAT Nhits map, what should the Delensing LAT distribution of noise levels be in order for the S/N = 1 for the residual lensing modes. <br />
<br />
In the regime where delensing is the limiting factor of sigma(r), this would give a close approximation of what the actual distribution of noise levels (and hence Nhits) for the Delensing LAT. I list the next steps in order to make this more realistic and applicable to survey design of the Delensing LAT. <br />
<br />
<br />
== Method ==<br />
<br />
== Results ==<br />
<br />
== Next steps ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Simulation_and_Forecasting_Logbook&diff=11597Simulation and Forecasting Logbook2020-07-28T18:09:49Z<p>Wlwu: /* Logbook Entries (reverse chronological) */</p>
<hr />
<div>This is an index page for logbook-style postings that cover the interconnected topics of sky modeling, simulations, and forecasting for CMB-S4. <br />
<br />
Some guidelines for use:<br />
* '''Postings should include enough context''' so that a reader can jump in and figure out what is going on. It is ''not'' necessary to write an extensive introduction to every posting -- context can be in the form of links to older postings, paper citations, etc.<br />
* Postings should represent a snapshot of work in progress. It's ok to post incomplete results, but recommended that you include notes about what is missing, what you are still planning to work on, etc. <br />
* If you have work that extends or improves an old posting, you should add it as a new posting (that includes links back to the old work as appropriate). Don't update old postings, as they should provide a chronological record of progress.<br />
* On this index page, add a link to your posting with the date, a descriptive posting title, and your full name. This logbook covers a wide range of topics, so titles will be really important to keep it useful. Don't name your posting something like "Forecasting for S4"!<br />
* Links should be added in reverse-chronological order (newest at the top). Your posting can either be written up on another wiki page or it can be a link to some externally hosted webpage (useful if you want to include a javascript plots pager).<br />
<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
* '''2020 July 28''': [[ Delensing_LAT_relative_Nhits_v0p0 | Delensing LAT relative Nhits, v0.0 ]] (K Wu)<br />
* '''2020 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200709_bkfinal_06blt BK-style power spectra of 06b with interative lensing templates] (Clem)<br />
* '''2020 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200708_itrecon_noise Investigation of iterative lensing templates] (Clem)<br />
* '''2020 July 7''': SAT split band justification slides [https://docs.google.com/presentation/d/1685uV44VTBhk8Nm3HIzQUSsgmgYQOZNLz3qUPIDeDqk/edit#slide=id.p v1], [https://docs.google.com/presentation/d/1vkF0nVrH7DjPAuga-njxnW6i5UbCwEgLNg1Iu9-oS0Q/edit#slide=id.p v2] (Colin Bischoff)<br />
* '''2020 July 7''': [[Delensing sensitivity - map-based delensing]] (Raphael Flauger)<br />
* '''2020 June 30''': [[Checking BB purity in re-analysis II]] (Clem Pryke)<br />
* '''2020 June 30''': [[White noise levels for high cadence scan at elevation of 40 degrees]] (Raphael Flauger)<br />
* '''2020 June 19''': [[Delensing sensitivity - updated sensitivities, beams, TT noise]] (Raphael Flauger)<br />
* '''2020 June 18''': [[Correlation of iteratively reconstructed lensing templates to ideal for 06b]] (Clem Pryke)<br />
* '''2020 June 11''': [[Map-based simulations for split and full bands]] (Raphael Flauger)<br />
* '''2020 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200611_splitbands/ Signal-to-noise on foregrounds from split band difference maps] (C. Bischoff)<br />
* '''2020 June 06''': [[Background on 20 GHz channel]] (Raphael Flauger)<br />
* '''2020 June 04''': [[Delensing sensitivity - preliminary results]] (Raphael Flauger)<br />
* '''2020 June 04''': [[N_eff Forecasting Comparison with DRAFT ILC|N_eff Forecasting Comparison with DRAFT ILC]] (Joel Meyers, Srini Raghunathan, Benjamin Wallisch)<br />
* '''2020 May 19''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200519_DM_AWG_noise/ Noise comparison between DM and Low-&#x2113; BB sims] (C. Bischoff)<br />
* '''2020 April 26''': [[Bayesian_vs_Template_Delensing|Bayesian vs. Template Delensing]] (Marius Millea)<br />
* '''2020 April 10''': [[Iterative curved sky s06b nofg lensing templates]] (Julien Carron)<br />
* '''2020 March 06''': [[Flat-sky_joint_MAP_lensing_template_for_06b_simulations|Flat-sky joint MAP lensing template for 06b simulations]] (Marius Millea)<br />
* '''2020 February 07''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200207_ILC_maps_part3 Preliminary ILC maps part 3] (C. Umiltà)<br />
* '''2020 January 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20200110_ILC_maps_part2 Preliminary ILC maps part 2] (C. Umiltà)<br />
* '''2019 December 14''': [[Correlation of reconstructed lensing template to ideal for 06b.00]] (Clem Pryke)<br />
* '''2019 December 12''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20191209_ILC_maps_prelim Preliminary ILC maps part 1] (C. Umiltà)<br />
* '''2019 November 12''': [[SAT detector counts, NET, and overall efficiency from DSR]] (C. Bischoff)<br />
* '''2019 November 12''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20191112_bk_scans Actual BK scanning trajectory] (Clem)<br />
* '''2019 November 1''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20191101_dc06_specsmaps DSR Sim Map Set 06 - some spectra and map check plots] (Clem)<br />
* '''2019 October 25''': [[Modulated scan high cadence LAT]] (Reijo)<br />
* '''2019 October 16''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20191016_dc06_dsr DSR Sim Map Set 06 with simple scaling from BK15] (Clem)<br />
* '''2019 September 16''': [[PureB by Messenger Method]] (Michael Ray, Colin Bischoff)<br />
* '''2019 August 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190829_noise_params_DSR/ Noise parameters for the DC5 DSR-like data challenge] (Ben Racine)<br />
* '''2019 June 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190607_LATSTM/ LAT CDT-STM Noise Levels] (Victor Buza)<br />
* '''2019 May 19''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190519_about_DSR_AppendixA_plots_and_table/ sigma(r) vs r: plots and tables for the DSR] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190509_b3_obseff Observing efficiency reality check] (Clem)<br />
* '''2019 May 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190511_sigmar_vs_r_galcuts/ sigma(r) vs r: possible figures for the DSR (v4): Galactic cuts added (In progress)] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 11''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 May 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190507_sigmar_vs_r_combined_hits/ sigma(r) vs r: possible figures for the DSR (v3): More realistic combination and fixed 20GHz] (Ben Racine and Raphael Flauger)<br />
* '''2019 May 6''': [[Update_on_Fisher_forecasts]] (Raphael)<br />
* '''2019 April 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190430_sigmar_vs_r_forDSR/ sigma(r) vs r: possible figures for the DSR (v2): more optimal weighting] (Ben Racine and Raphael Flauger)<br />
* '''2019 April 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190501_obseff Efficiency for Reijo's observation pattern sims] (Clem)<br />
* '''2019 April 29''': [[Fisher forecasts for inverse noise variance weighting]] (Raphael)<br />
* '''2019 April 22''': [[WAFTT results part 3]] (Raphael)<br />
* '''2019 April 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190418_sigmar_vs_r/ sigma(r) vs r: possible figures for the DSR] (Ben Racine)<br />
* '''2019 April 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190410_closedloop_BK15_S4 Zero order closed loop test of performance based scaling - ML search] (Ben Racine)<br />
* '''2019 March 31''': [[Analysis results for configurations 30-33]] (Raphael)<br />
* '''2019 March 30''': [[Characterization of simulations for configurations 30-33]] (Raphael)<br />
* '''2019 March 26''': [[Simulations for configurations with different frequency coverage]] (Raphael)<br />
* '''2019 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190326_bkfinal_05 Zero order closed loop test of performance based scaling - BK15 regen power spectra] (Clem)<br />
* '''2019 March 25''': [[Deeper SAT from Chile II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Wider SAT from the Pole II]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 25''': [[Deep SAT from the Pole]] (Reijo Keskitalo and Julian Borrill)<br />
* '''2019 March 18''': [https://cmb-s4.org/wiki/index.php/Optimal_lensing_fermilab Details on optimal lensing Fermilab presentation / 02.xx real delensing] (Marius Millea)<br />
* '''2019 March 18''': [[High cadence LAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 March 18''': [[WAFTT results part 2]] (Raphael)<br />
* '''2019 March 18''': [[Wider SAT from the Pole]] (Reijo Keskitalo)<br />
* '''2019 March 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook//20190308_MLsearch_no85no145/ Maximum likelihood search results without 85GHz and 145GHz] (Ben Racine)<br />
* '''2019 March 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190303_MLsearch_bpmax_dep/ Maximum likelihood search results: dependence on the multipole range] (Ben Racine)<br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_noiseparams_bk15_forS4/ BK15 noise levels for S4 sims] (Ben Racine) <br />
* '''2019 February 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190220_S4_NET_forecasts_III/ CMB-S4 NET follow-ups II] (Denis Barkats, Ben Racine-updated on Feb 25) <br />
* '''2019 February 18''': [[Correlation of reconstructed lensing template to ideal II]] (Clem Pryke)<br />
* '''2019 February 18''': [[Fisher calcs of 04b/04c for larger value of r]] (Raphael posted by Clem)<br />
* '''2019 February 14''': [[Deeper SAT from Chile]] (Reijo Keskitalo)<br />
* '''2019 January 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190130_Matrix_first_try/ Matrix-based purification analysis: First try] (B.Racine, J.Willmert) ''Updated 2019 Feb 17th''<br />
* '''2019 January 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190123_S4_NET_forecasts_II/ CMB-S4 NET follow-ups I] (Denis Barkats, J. Kovac, Ben Racine-updated on Feb 25) <br />
* '''2019 January 15''': [[Correlation of reconstructed lensing template to ideal]] (Clem Pryke)<br />
* '''2019 January 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190120_dc02_ML_LT/ Maximum likelihood search results for Data Challenge 02.00 with two different lensing templates] (C. Umiltà)<br />
* '''2019 January 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190117_MLsearch04d/ Maximum likelihood search results for Data Challenge 04d.00, new BK14 mask reanalysis] (Ben Racine)<br />
* '''2019 January 15''': [[Noise models and sky fractions for WAFTT]] (Raphael)<br />
* '''2019 January 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20190111_bkfinal_04bcd BK-style power spectra of 04/04b/04c/04d masks (adding BK14 mask)] (Clem)<br />
* '''2018 December 9''': [[Optimal Bayesian delensing progress update]] (Marius Millea) <br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_bkfinal_02lt BK-style power spectra of 02 with Carron lensing templates] (Clem)<br />
* '''2018 December 7''': [[Problems with PS2HAT estimator at low ell]] (Clem Pryke)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181116_bpbias_study Bandpower bias study] (Ben Racine)<br />
* '''2018 December 7''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181207_expval_input_ML_search Maximum likelihood search with expectation values as input] (C. Umiltà)<br />
* '''2018 November 28''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181128_toy_sims Effective sky fraction] (Clem)<br />
* '''2018 November 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181127_bpwf_DC4 A look at DC4 bandpower window functions] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/ Maximum likelihood search results for Data Challenge 04, v2] (Ben Racine)<br />
* '''2018 November 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181111_dc04_flatpriors/index_abc.html Maximum likelihood search results for Data Challenge 04b and 04c, v2] (Ben Racine)<br />
* '''2018 November 16''': [[Analytic approximation for r likelihood]] (C. Bischoff) ''Updated 2018-11-20''<br />
* '''2018 November 12''': [[Detection significance for r=0.003]] (C. Bischoff)<br />
* '''2018 November 9''': [[Bad realizations in gsync/gdust sims]] (Clem Pryke)<br />
* '''2018 November 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181108_dc02_ML_LT Maximum likelihood search results for Data Challenge 02.00 with an ideal lensing template] (C. Umiltà)<br />
* '''2018 November 5''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181105_toy_sims Attempt to understand sigma(r) results with different hit maps] (Clem)<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181018_1Dmodel_tapering_study Simple 1D model to study the effect of different observation strategies on the bandpower statistics.] (Ben Racine, Victor Buza, John Kovac) ''Updated 2018 Dec 14th''<br />
* '''2018 October 29''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20181029_bkfinal_02lt BK-style power spectra of 02 with ideal lensing templates] (Clem)<br />
* '''2018 October 26''': [[Checking BB purity in re-analysis for alternate masks]] (Clem Pryke)<br />
* '''2018 October 23''': [[Estimated observing efficiency for past and current telescopes, version 2]] (C. Bischoff, Y. Chinone, T. Crawford, M. Hasselfield)<br />
* '''2018 October 14''': [[Estimates of delensing efficiency]] (Raphael)<br />
* '''2018 October 14''': [[Analysis of 04, 04b, 04c simulations]] (Raphael) [[Analysis of 04, 04b, 04c simulations comp]] (Ben)<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_0to9/ Maximum likelihood search results for Data Challenge 04, models 0 to 9] (Ben Racine) ''Updated 2018 Oct 2nd''<br />
* '''2018 September 30''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180930_dc04_abc_model_0123789_ML/ Maximum likelihood search results for Data Challenge 04b and 04c, model 00, 01, 02, 03, 07, 08 and 09] (Ben Racine)<br />
* '''2018 September 30''': [[Ready for delensing use lensing maps 02.00]] (Julien Carron)<br />
* '''2018 September 28''': [[Towards lensing template]] (Clem Pryke)<br />
* '''2018 September 27''': [[Lensing reconstructions 02.00]] (Julien Carron)<br />
* '''2018 September 26''': [[Lensing map reconstruction from 02.00 sims w/ and w/o foreground+inhomogeneous noise]] (Toshiya Namikawa)<br />
* '''2018 September 25''': [[Estimated observing efficiency for past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180925_bkfinal_04bc BK-style power spectra of 04/04b/04c masks for 00/01/02/03/07/08/09 foreground models] (Clem)<br />
* '''2018 September 12''': [[Low ell noise from past and current telescopes]] (C. Bischoff)<br />
* '''2018 September 5''': [[Phi reconstruction on 02.00 sims III]] (Anton Baleato)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_abc_model00_07_ML_proper_bp/ Maximum likelihood search results for Data Challenge 04b and 04c, for sky models 00 and 07] (Ben Racine)<br />
* '''2018 August 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180831_dc04_fixed_bp/ Maximum likelihood search results for Data Challenge 04, fixed bandpasses] (Ben Racine)<br />
* '''2018 August 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180827_bkfinal_04 Sims with nominal Chile and Pole masks III - BK-style power spectra of 04b.YY and 04c.YY] (Clem)<br />
* '''2018 August 27''': [[Sims with nominal Chile and Pole masks II]] (Clem P.)<br />
* '''2018 August 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180826_dc04_fixed/ Maximum likelihood search results for Data Challenge 04, fixed] (V.Buza, B.Racine)<br />
* '''2018 August 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180824_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) FIXED] (Caterina Umilta)<br />
* '''2018 August 24''': [[Amplitude modulated Gaussian dust sims]] (Clem P.)<br />
* '''2018 August 17''': [[Sims with nominal Chile and Pole masks]] (Clem P.)<br />
* '''2018 August 10''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180810_noise/ Achieved performance roundup] (C. Bischoff)<br />
* '''2018 August 7''': [[Pre-reference-design noise specifications for large-aperture forecasting]] (Tom Crawford, Matthew Hasselfield, Gil Holder, Lloyd Knox)<br />
* '''2018 August 6''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180805_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm vs 52cm aperture (w/ high-res/low-res 20 GHz)] (V.Buza)<br />
* '''2018 July 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180708_dc04/ Maximum likelihood search results for Data Challenge 04] (V.Buza)<br />
* '''2018 July 6''': [[Phi reconstruction on 02.00 sims II]] (Anton Baleato and Clem Pryke)<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180611_s4opt/ Performance-based Fisher optimization for CMB-S4, 44cm aperture] (V.Buza) -- see corrected August 6th Update!<br />
* '''2018 June 11''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180609_S4_noise_simulation_arbitrary_coverage/ Recipe to generate performance based S4 simulations with arbitrary sky distribution (in progress)] (B.Racine, V.Buza)<br />
* '''2018 April 29''': [[Phi reconstruction on 02.00 sims]] (Anton Baleato)<br />
* '''2018 April 25''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180425_r_equivalent_maps/ Smallfield r-equivalent Maps] (Kenny Lau)<br />
* '''2018 April 4''': [[Sky masks for simulations III]] (Clem P.)<br />
* '''2018 March 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180323_bkfinal_04/ BK-style power spectra of v04.00-06 sims (CDT report config) BROKEN] (Clem)<br />
* '''2018 March 16''': [[ILC noise for large apertures at CDT noise levels]] (Raphael Flauger posted by Clem)<br />
* '''2018 March 16''': [[Sky masks for simulations II]] (Clem P.)<br />
* '''2018 February 19''': [[Sky masks for simulations]] (Clem P.)<br />
* '''2018 February 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20180218_s4opt/ Performance-based Fisher optimization for CMB-S4, v3] (Victor Buza)<br />
* '''2018 February 7''': [[Sim map sets to demonstrate "real delensing" (02.00 and 02.09)]] (Clem P.)<br />
* '''2018 February 6''': [[Data Challenge Map Sets 04.YY]] (Clem P.)<br />
* '''2017 December 8''': [[Vansyngel Model]] (Clem P.)<br />
* '''2017 November 6''': [[Bandpass Convention - What does flat mean]] (Clem P.) - followup notes added Nov 20<br />
* '''2017 September 27''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170927_dc02/ Maximum likelihood search results for Data Challenge 02] (Bischoff, Buza, Willmert)<br />
* '''2017 September 13''': [[Bias on r from Band Center Errors]] (Palladino, Willmert, Bischoff)<br />
* '''2017 September 8''': [[Checking dust decorrelation in Raphael MHD based dust sim]] (Clem P.)<br />
* '''2017 September 6''': [[New NET Calculator and Validation]] (Denis Barkats)<br />
* '''2017 September 1''': [[Resolution at 20 GHz]] (Raphael)<br />
* '''2017 August 31''': [[Bias on r from additive systematics]] (Palladino, Willmert, Bischoff)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_bkfinal_03.00/ BK-style power spectra for 1000 realizations of v03.00,.03 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 August 18 ''': [[Neff_and_Beam_Calibration| Neff and Beam Calibration]] (Dan)<br />
* '''2017 August 18''': [[Ideal delensing templates from flat-sky QE, first pass]] (Kyle Story)<br />
* '''2017 August 18''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170818_HR/ High-Res studies for CMB-S4 (draft, v2)] (Victor Buza)<br />
* '''2017 August 18''': [[Comments from Anthony Challinor and Rupert Allison regarding the impact of Galactic Foregrounds on lensing]] (Neelima)<br />
* '''2017 August 11''': [[Joint Synchrotron and Dust Maps from Simulations]] (B. Hensley)<br />
* '''2017 August 9''': [[Dust Emission From Halos]] (Jim & Jean-Baptiste)<br />
* '''2017 August 9''': [[SZ Clusters update]] (Mat & Nick)<br />
* '''2017 August 4''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170804_HR/ High-Res studies for CMB-S4 (preliminary draft)] (Victor Buza); perhaps a reference of interest https://arxiv.org/abs/1707.02259<br />
* '''2017 July 10''': [[Additive systematics for data challenge 03]] (Bischoff, Palladino, Buza, Kovac)<br />
* '''2017 July 6''': [[Detection significance and sky fraction, dust decorrelation]](Raphael)<br />
* '''2017 July 3''': [[Toy highly decorrelated dust model]] (Clem P.)<br />
* '''2017 June 27''': [[Checking dust decorrelation in models d1/d4/d7 and hipdt]] (Clem P.)<br />
* '''2017 June 23''': [[Neff and beams from field sources|Neff and a back-of-the-envelope estimate of beam uncertainty from field sources]] (Tom C.)<br />
* '''2017 June 23''': [[Dust_delensing_firstlook|Dust delensing update]] (Alex)<br />
* '''2017 June 23''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170623_bkfinal_02.00/ BK-style power spectra for 1000 realizations of v02.00–06 CMB-S4 simulation maps] (Justin Willmert) ''Updated 2017 Sep 08''<br />
* '''2017 June 22''': [[Warm-up exercise for delensing]] (Raphael)<br />
* '''2017 June 19''': [[SZ Clusters update]] (Mat, Nick)<br />
* '''2017 June 11''': [[Notes from May 31 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 June 9''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170525_s4syst/ Introducing systematics for CMB-S4] ((Victor Buza), with input from Colin Bischoff, John Kovac)<br />
* '''2017 June 9''': [[Dust_delensing_firstlook]] (Alex)<br />
* '''2017 June 9''': [[r-forecasting: high and low ell coordination|r-forecasting: update on high and low ell coordination]] (Neelima+Colin Hill writing)<br />
* '''2017 June 1''': [[Residuals for DC 01.01 and DC 01.02]] (Raphael)<br />
* '''2017 June 1''': [[Levels of foregrounds in Gaussian and PySM simulations]] (Raphael)<br />
* '''2017 May 26''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170511_s4dc1/ S4 DC 01.xx analysis, v2] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 May 26 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ Updated v01.02 in "BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps"] (Justin Willmert)<br />
* '''2017 May 15''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170515_chkS4/ N_ell spectra for CMB-S4 DC2.0] (Victor Buza)<br />
* '''2017 May 15''': [[Rev 2 PySM a2d4f1s3 maps]] (Clem P.)<br />
* '''2017 May 12''': [[r-forecasting: high and low ell coordination|r-forecasting: high and low ell coordination]] (lensers writing)<br />
* '''2017 May 8''': [[Checking PySM maps]] (Clem P.)<br />
* '''2017 May 2''': [[Notes from April 26 telecon on science requirements for clusters/high-ell]] (Steve)<br />
* '''2017 May 1''': [[r-forecasting: delensing discussion|r-forecasting delensing discussion]] (Neelima and Blake)<br />
* '''2017 April 28 ''': [[Update_on_Neff_Forecasts| Update on Neff Forecasts]] (Dan)<br />
* '''2017 April 26 ''': [http://www.cosmo.bnl.gov/www/msyriac/web/work/sigma8plots.html Update on cluster number counts forecast including w_a] (Mat and Nick)<br />
* '''2017 April 21 ''': [[lensing-DE|Update on a lensing-based DE forecast]] (Jo, Siddharth)<br />
* '''2017 April 18 ''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170411_bkfinal_01.00/ BK-style power spectra for 1000 realizations of v01.00–02 CMB-S4 simulation maps] (Justin Willmert)<br />
* '''2017 April 18 ''': [[S4-Lensing|S4 measurement requirements for neutrino mass and delensing - first pass]] (Neelima/Blake)<br />
* '''2017 April 17 ''': [[HiDPol|HI-based dust polarization model for r forecasts]] (Tuhin)<br />
* '''2017 April 05 ''': [[lensing-DE|Notes on one path to lensing-based DE forecasts]] (Jo)<br />
* '''2017 April 05 ''': [[Notes from April 5 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 April 05''': [https://cmb-s4.org/CMB-S4workshops/images/Sigma8_z_prep.pdf Sigma8(z) SPT clusters (placeholder) ] (S Bocquet)<br />
* '''2017 April 04''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170404_s4opt/ Updated Performance-based Fisher optimization for CMB-S4 (using bands v1.99)] (Victor Buza, Updated 2017.04.21)<br />
* '''2017 March 31 ''': [[Data Challenge analysis - DC1.0, DC1.1, DC1.2]] (Raphael)<br />
* '''2017 March 30 ''': [[Notes from March 28 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 29''': [[CMB-S4 frequency bands v1.99]] (John Kovac, Band-definition working group)<br />
* '''2017 March 28''': [[Adding higher res delensing "band"]] (Clem P.)<br />
* '''2017 March 27''': [[01.01 sim input maps - first try]] (Clem P.)<br />
* '''2017 March 23''': [[01.00 sim input maps]] (Clem P.)<br />
* '''2017 March 20''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170221_S4_NET_forecasts/ S4 Band sensitivity comparison follow-up] (Denis Barkats, John Kovac)<br />
* '''2017 March 17''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20170317_s4dc1/ S4 DC1.0 analysis] (Victor Buza, Colin Bischoff, Justin Willmert)<br />
* '''2017 March 17 ''': [[Media:Telecon_03172017_optimization_for_CMBS4.pdf]]: Optimization methodology for SO (Josquin)<br />
* '''2017 March 16 ''': [[ P_k_science_case| P(k) science case]] (Colin, Simone, Nick, David)<br />
* '''2017 March 15 ''': [[Notes from March 15 telecon on science requirements for clusters/high-ell]] (Jim)<br />
* '''2017 March 15 ''': [[CMB halo lensing sensitivity as a function of map sensitivity and resolution]] (Jim & Jean-Baptiste)<br />
* '''2017 March 15 ''': [[w and gamma | w and Delta gamma constraints from sigma_8 (z)]] (Mat & Nick)<br />
* '''2017 March 10 ''': [[Notes from March 8 telecon on science requirements for clusters/high-ell]] (Jim & Steve)<br />
* '''2017 March 8 ''': [[reionization_requirements| Reionization science]] (Simone & Marcelo)<br />
* '''2017 March 8 ''': [[High ell topics | High ell topics ]] (Jim)<br />
* '''2017 March 8 ''': [[SZ_s8_z | sigma 8 of z constraints ]] (Mat, Nick)<br />
* '''2017 March 8 ''': [[Szcounts | Number counts update for 1.0', 1.5', 2.0']] (Nick, Mat)<br />
* '''2017 March 8 ''': [[SZastro | SZ astrophysics with DESI ]](Nick, Simone, Emanuel, David)<br />
* '''2017 February 24''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/20170224_cmbs4_dc1_final/ BK-style processing of DC1.0 maps to spectra] (Justin Willmert, Colin Bischoff)<br />
* '''2017 February 15 ''': [[Extragalactic lensing sims| Update on extragalactic phase-2 lensing sims]] (Marcelo, George, Dick, others)<br />
* '''2017 February 15 ''': [[Plan for next Galactic Phase-2sims| Plan for next Galactic phase-2 sims]] (Jo, Ben)<br />
* '''2017 February 10 ''': [[Resolution of foreground-cleaned map]] (Mat, Neelima, Blake, Alex, others)<br />
* '''2017 February 10 ''': [[Nongaussian dust in lensing]] (Alex, Mat, Neelima, Blake, others)<br />
* '''2017 January 30''': [[Aliased power in noise maps]] (Bischoff, Updated 2017-02-02)<br />
* '''2017 January 23''': [[CMBS4 Band Sensitivity Comparison]] (Charlie Hill)<br />
* '''2017 January 12''': [http://bicep.rc.fas.harvard.edu/cbischoff/20170112_data_challenge_1/ Maps for CMB-S4 data challenge 1] (Bischoff, Pryke, Buza)<br />
* '''2016 December 21''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20161220_chkS4/ N_ell spectra for the CMB-S4 data challenge, and updated &sigma;(r) checkpoints] (Victor Buza, Updated 2017.02.01)<br />
* '''2016 November 30''': [[First steps to sim input maps]] (Clem P.)<br />
* '''2016 November 4''': [[Tophat bands for Data Challenge]] (Bischoff)<br />
* '''2016 July 8''': [[fsky|Dependence of foregrounds on sky fraction]] (Raphael)<br />
* '''2016 July 8''': [[SciBookPowspecTheoryFig|Three choices for Science Book Figure 5 (theory power spectrum & current BB points)]] (Tom C.)<br />
* '''2016 July 8''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20160707_s4plots/ S4 Inflation Chapter Plot Suggestions, V2] (Victor Buza)<br />
* '''2016 July 6''': [[w_cosntraint|Preliminary w constraint]] (Alessandro)<br />
* '''2016 June 24''': [[nsr|Preliminary ns-r plot for discussion]] (Raphael)<br />
* '''2016 June 16''': [[DelensingImpact| Impact Of Delensing On sigma(r)]] (Neelima/Mat)<br />
* '''2016 June 16''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20160616_s4plots/ S4 Inflation Chapter Plot Suggestions] (Victor Buza)<br />
* '''2016 June 10''': [[MapBasedRb| Map-based &sigma;(r) forecasts V2]] (David/Jo/Ben)<br />
* '''2016 June 3''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20160531_fisher/ &sigma;(r) forecasting checkpoints, V2] (Victor Buza)<br />
* '''2016 June 3''': [[ BTTfixedeffort | Forecasts for fnl BTT beam/fixed effort]] (Daan)<br />
* '''2016 May 31''': [[ForecastPatchyReion| Forecasts for patchy reionization]] (Vera, Alex, Nick)<br />
* '''2016 May 26''': [[Forecasting | Forecasts on neutrino mass]] (Nam, Mat, Neelima)<br />
* '''2016 May 26''': [[ KSZ| Forecasts on kSZ S/N]] (Simone, Emmanuel, Colin)<br />
* '''2016 May 26''': [[ Forecastfiso_planck| Forecast on correlated and anti-correlated CDM isocurvature f_iso]] (Kimmy, Cora, updated with plots 20160602)<br />
* '''2016 May 24''': [[ BTTNoiseBeam | Forecasts on fnl BTT beam/FWHM]] (Daan)<br />
* '''2016 May 22''': [[ ForecastAxions| Update on the axion isocurvature constraints for changing sensitivity and resolution]] (Renee)<br />
* '''2016 May 21''': [[ Forecastpann| Forecast on dark matter annihilation parameter p_ann]] (Kimmy, Cora)<br />
* '''2016 May 20''': [[NeffNoiseBeam| Forecasts on Neff and Yp]] (Joel, Alex)<br />
* '''2016 May 20''': [[ForecastEDE| Forecasts on Early Dark Energy]] (Erminia)<br />
* '''2016 May 20''': [[ForecastCompIsocurv| Forecasts on compensated isocurvature varying sensitivity, resolution and sky coverage]] (Julian, Ely)<br />
* '''2016 May 20''': [[ForecastBirefring| Forecasts on birefringence varying sensitivity and resolution]] (Vera, Alex)<br />
* '''2016 May 20''': [[ForecastStrings| Forecasts on string tension varying sensitivity and resolution]] (Renee)<br />
* '''2016 May 20''': [[RobustForecast| Cosmological forecasts including component separation and iterative delensing]] (Stephen Feeney and Josquin Errard)<br />
* '''2016 May 19''': [[MapBasedR| Map-based &sigma;(r) forecasts]] (David A.)<br />
* '''2016 May 18''': [[Shear_calibration_LSST|LSST shear calibration with CMB S4]] (Emmanuel Schaan)<br />
* '''2016 May 13''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20150505_fisher/ &sigma;(r) forecasting checkpoints] (Victor Buza)<br />
* '''2016 May 13''': [[NonGaussianitiesTTT| CMBS-4 forecasts local and equilateral scalar Ngs using TTT]] (daan)<br />
* '''2016 May 13''': [[ForecastingSims|Simulations for r forecasts]] (Jo/Ben/David)<br />
* '''2016 May 6''': [[DMInteractionsComplementarity|DM interactions: complementarity]] (Vera)<br />
* '''2016 May 6''': [[Scenarios| Scenarios]] (Scott, Vera)<br />
* ''' 2016 May 3''': [[ForecastAxions |Effect of S4 specs on axion density parameters]] (Renee)<br />
* '''2016 April 30''': [[ForecastNu| Effect of S4 specs on neutrino parameters]] (Erminia)<br />
* '''2016 April 28''': [http://web.stanford.edu/~wlwu/posting/20160421_lensres/ Delensing residuals with low-ell foregrounds] (Kimmy Wu)<br />
* '''2016 April 28''': [[NonGaussianities| CMBS-4 forecast for tensor NGs]] (daan)<br />
* '''2016 April 19''': [[ForecastingStep1| Checking basic parameters for nominal case]] (Jo + multiple authors)<br />
* '''2016 April 5''': [[Forecasting|Setting up non-r Fisher-based parameter forecasts]] (Jo + others)<br />
* '''2016 March 31''': [http://bicep.rc.fas.harvard.edu/CMB-S4/analysis_logbook/vbuza/20150331_fisher/ Fisher projections for &sigma;(r) based on achieved performance] (Victor Buza)<br />
* '''2016 January 27''': [https://cmb-s4.org/CMB-S4workshops/index.php/File:sptpol_ptsrc_polfrac_500d.pdf Quick estimate of mean-squared polarization fraction for SPTpol sources] (Tom Crawford)</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=LBNL-2020:_Cosmology_with_CMB-S4&diff=11182LBNL-2020: Cosmology with CMB-S42020-04-02T15:57:32Z<p>Wlwu: /* Thursday April 2 */</p>
<hr />
<div>== Workshop overview ==<br />
<br />
This workshop continues a successful series of meetings bringing together the CMB experimental and theoretical community to plan a coordinated, stage-4 ground-based CMB experiment. <br />
<br />
Due to COVID-19 quarantining the meeting will be held entirely remotely, 9:00am to 1:30pm Pacific Daylight Time, Monday March 30th to Thursday April 2nd.<br />
<br />
== Meeting Info & Registration ==<br />
<br />
Please continue to register at the website despite the remote nature of the event.<br />
<br />
[http://cmbs4lbl2020.lbl.gov Official Workshop Website: Registration, Participants, Logistics].<br />
<br />
== Remote Meeting Considerations ==<br />
<br />
All sessions will be held remotely by zoom.<br />
* Plenary sessions will all use https://lbnl.zoom.us/j/912694106<br />
* Parallel sessions will have connection details on their wiki page<br />
<br />
All participants should<br />
* Connect using a browser or the zoom app if at all possible so that you can use the "raise hand" button to contribute, especially in the plenary sessions.<br />
* Connect with a full name so that the session convenors and other participants can identify you.<br />
* Mute your line whenever you are not speaking.<br />
* Disable video so that we don't overwhelm participants with limited bandwidth.<br />
* Join the '''#lbnl2020''' channel on the [https://cmb-s4.slack.com CMB-S4 Slack workspace], email [mailto:zonca@sdsc.edu zonca@sdsc.edu] if you need an invitation<br />
<br />
== Agenda ==<br />
<br />
'''Note: All times below are US Pacific timezone!'''<br />
<br />
=== Monday March 30 ===<br />
<br />
https://lbnl.zoom.us/j/912694106<br />
<br />
[https://docs.google.com/document/d/1BrrX4yqEsi1rSaPJhLWqEPrtRu5_msqU_wGkC8VBxCI Plenary google doc]<br />
<br />
09:00 - Plenary 1 (Borrill/Carlstrom)<br />
* Collaboration Overview [https://docs.google.com/presentation/d/1-dOQywsPQ44AolMzNKYRyGgJMaVpCNn25Etvyn5sAMg slides] <br />
<br />
10:00 - Plenary 2 (Yeck)<br />
* Project Overview [https://docs.google.com/presentation/d/1M1XwAhYIBxVfOrRwQE7llzV_w5d4fS8JND7bFGSHjYo slides]<br />
<br />
11:00 - Break<br />
<br />
11:30 - Plenary 3 (McMahon)<br />
* Baseline Design Issues: Detectors, Readout, Modules [https://docs.google.com/presentation/d/1W2VNsbTsO-i8tf_ajjJeEce2lTYEDP2U4ZMjpF-l3cY slides]<br />
<br />
12:30 - Plenary 4 (Vieregg)<br />
* Baseline Design Issues: LAT, SAT, DAQ, DM, Sites [https://docs.google.com/presentation/d/10LzUhw0NrNVN0rxAObuTLVTK-Pmg-e7M-otfYdbwx4A slides]<br />
<br />
=== Tuesday March 31 ===<br />
<br />
09:00 - Parallel 1<br />
* [[LBNL-2020: Detectors_Readout_Modules | Detectors, Readout, Modules]] (Wollack/Benson)<br />
* [[LBNL-2020: LAT | Large Aperture Telescopes]] (Carlstrom/Niemack)<br />
* [[LBNL-2020: DAQ | Data Acquisition]] (Newburgh)<br />
* [[LBNL-2020: Low-ell_BB | Low-ell BB]] (Bischoff/Wu) Zoom line: https://fnal.zoom.us/j/5196960377 <br />
* [[LBNL-2020: Maps-to-Spectra | Maps-to-Spectra]] (Loverde/Reichardt)<br />
<br />
11:00 - Break<br />
<br />
11:30 - Parallel 2<br />
* [[LBNL-2020: Detectors_Readout_Modules | Detectors, Readout, Modules (cont)]] (Wollack/Benson)<br />
* [[LBNL-2020: SAT | Small Aperture Telescopes]] (Kovac/Kusaka)<br />
* [[LBNL-2020: DM | Data Management]] (Borrill/Crawford)<br />
* [[LBNL-2020: Sources | Sources]] (Battaglia/Vieira)<br />
* [[LBNL-2020: Maps-to-Other | Maps-to-Other Statistics]] (Sherwin/Alvarez)<br />
<br />
=== Wednesday April 1 ===<br />
<br />
09:00 - Parallel 3<br />
* [[LBNL-2020: Testing_Facilities | Testing Facilities]] (Benson)<br />
* [[LBNL-2020: Telescope_Interfaces: Sites_and_I&C | Telescope Interfaces: Sites and I&C]] (Ruhl/Arnold)<br />
* [[LBNL-2020: Cold_Optics | Cold Optics]] (McMahon)[https://lbnl.zoom.us/j/189656154 zoom]<br />
* [[LBNL-2020: S2M_Flowdown | Science-to-Measurement Flowdown]] (Lawrence)<br />
<br />
10:00 - Parallel 4<br />
* [[LBNL-2020: Telescope_Interfaces: DRM_and_DAQ | Telescope Interfaces: Detectors/Readout/Modules and DAQ]] (Zivick)<br />
* [[LBNL-2020: Cold_Optics | Cold Optics (cont)]] (McMahon) [https://lbnl.zoom.us/j/189656154 zoom]<br />
* [[LBNL-2020: S2M_Flowdown | Science-to-Measurement Flowdown (cont)]] (Lawrence)<br />
<br />
11:00 - Break<br />
<br />
11:30 - Parallel 5<br />
* [[LBNL-2020: M2T_Flowdown | Measurement-to-Technical Flowdown]] (Lawrence)<br />
* [[LBNL-2020: DAQ_DM_Sites_Interfaces | DAQ / DM / Sites Interfaces]] (Rahlin)<br />
* [[LBNL-2020: Galactic_Foreground_Modeling | Galactic Foreground Modeling]] (Hensley/Thorne)<br />
* [[LBNL-2020: Extragalactic_Foreground_Modeling | Extragalactic Foreground Modeling]] (van Engelen/Omori)<br />
<br />
12:30 - Parallel 6<br />
* [[LBNL-2020: M2T_Flowdown | Measurement-to-Technical Flowdown (cont)]] (Lawrence)<br />
* [[LBNL-2020: Transients: Science_Pipelines_Data | Transients: Science, Pipelines, Data]] (Holder)<br />
* [[LBNL-2020: Galactic_Foreground_Modeling | Galactic Foreground Modeling (cont)]] (Hensley/Thorne)<br />
* [[LBNL-2020: Cross-correlations_and_Complimentarity_for_LSS | Cross-correlations and Complimentarity for LSS]] (Ferraro)<br />
<br />
=== Thursday April 2 ===<br />
<br />
https://lbnl.zoom.us/j/912694106<br />
<br />
[https://docs.google.com/document/d/1BrrX4yqEsi1rSaPJhLWqEPrtRu5_msqU_wGkC8VBxCI Plenary google doc]<br />
<br />
09:00 - Plenary 5 (Barron)<br />
* Parallel Reports 1-2<br />
** Detectors, Readout, Modules (Wollack/Benson) [https://docs.google.com/presentation/d/1PZYsin7-p43xjiRQjk5kkDx52AYDhNZXQ9WW0P0ezx0/edit?usp=sharing]<br />
** Large Aperture Telescopes (Carlstrom/Niemack) [https://docs.google.com/presentation/d/1U0dC5ccAbct3p9cWyN2pbfa4gUy7iaUanL1VtUJ10KY/edit?usp=sharing slides]<br />
** Data Acquisition (Newburgh) [https://docs.google.com/presentation/d/1pne1X7llS9qAd7FpcHVSnBUWCrv0iv6ar9Jf5BWG0u4/edit?usp=sharing]<br />
** Low-ell BB (Bischoff/Wu) [https://docs.google.com/presentation/d/1JJrV1l_LH7JXR8QzshLO12rhW3BAM8WrGqQEh8I3sGY/edit?usp=sharing slides]<br />
** Small Aperture Telescopes (Kovac/Kusaka) [https://docs.google.com/presentation/d/1hMRtVbB7qfFBtoIIZlrFZjZzUZ2JO0WGtl8aRtCzyKw/edit#slide=id.p slides]<br />
** Data Management (Borrill/Crawford) [https://docs.google.com/presentation/d/10EzuCy0T9TeoLlDT7awP5U0Ja-p7RbJau_fdTJ9B4sw slides]<br />
** Sources (Battaglia/Vieira)<br />
** Maps-to-Other Statistics (Sherwin/Alvarez) [https://docs.google.com/presentation/d/1lOrQVNkP-EhwUunz1v3LjHrf1Xdg4S2ifCCHQY4h5is/edit?usp=sharing slides]<br />
** Maps-to-Spectra (Loverde/Reichardt)<br />
<br />
<br />
11:00 - Break<br />
<br />
11:30 - Plenary 6 (Borrill/Carlstrom)<br />
* Parallel Reports 3-6<br />
** Testing Facilities (Benson) [https://docs.google.com/presentation/d/1IehNzZnqKq_MV0yiOCkDNUeXBJJ7pS8dRw2vJVcXjUI/edit?usp=sharing]<br />
** Telescope Interfaces: Sites and I&C (Ruhl/Arnold) [https://docs.google.com/presentation/d/15um5oYesRHs6cKzcm3mc5NwyYpYz8FsmJQqYIEraLKU/edit?usp=sharing slides]<br />
** Telescope Interfaces: Detectors/Readout/Modules and DAQ (Zivick) [https://docs.google.com/presentation/d/1DnXIoVpEC6_6TB7WAGXV4Oj7tU3X9-4leoSasL-urZ8/edit?usp=sharing slides]<br />
** Cold Optics (McMahon)<br />
** Science-to-Measurement Flowdown (Lawrence)<br />
** Measurement-to-Technical Flowdown (Lawrence)<br />
** DAQ / DM / Sites Interfaces (Rahlin) [https://docs.google.com/presentation/d/1Npp-ZXRVS2v7K6PpdNCrNSvYFa938Mj0QeB5PRZQnic/edit?usp=sharing slides]<br />
** Galactic Foreground Modeling (Hensley/Thorne)<br />
** Extragalactic Foreground Modeling (van Engelen/Omori) [https://docs.google.com/presentation/d/1WJm510raqYMvKQupgOt7CrSOOYZZEgnQsFBfiUVOH2c/edit?usp=sharing slides]<br />
** Cross-correlations and Complimentary for LSS (Ferraro)<br />
** Transients: Science, Pipelines, Data (Holder) [https://docs.google.com/presentation/d/1VgQqPfOCy_Q2_6Si3jr-nvdR7H3yIwkqGju-AE9G-x0/edit?usp=sharing slides]<br />
* Town Hall<br />
* Closeout</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=LBNL-2020:_Low-ell_BB&diff=10971LBNL-2020: Low-ell BB2020-03-31T17:21:49Z<p>Wlwu: /* Agenda */</p>
<hr />
<div>== Connection details ==<br />
<br />
Parallel 1, session D. Tuesday March 31, 9:00 to 11:00 am pacific.<br />
<br />
https://fnal.zoom.us/j/5196960377<br />
<br />
Monitor: Kimmy Wu<br />
<br />
Scribe: Colin Bischoff, [https://docs.google.com/document/d/1FN8A8Yb6AGY7eGVLSxXdkXcB-WIEG4oANisLcuv8ty0/edit# google doc for notes] (to be transferred to wiki)<br />
<br />
== Charge ==<br />
<br />
The primary focus of this meeting will be technical and scientific progress towards the baseline design in general and the summer agency review in particular.<br />
<br />
* Present results from or statuses of data challenge 6 with real delensing incorporated<br />
* Foreground models / sims<br />
** Impact of foregrounds on delensing.<br />
** Foregrounds at low-ell <br />
* Sketch path(s) forward for data challenges:<br />
** What questions need answering by the summer’s agency review that need results from data challenges?<br />
* Outline trade studies that need to be done (or present results of trade studies) for the delensing LAT<br />
** Sensitivity vs resolution<br />
** Frequency allocation<br />
* Outline trade studies that need to be done (or present results of trade studies) for SATs<br />
** Do we need 20GHz?<br />
<br />
== Agenda ==<br />
<br />
* Results from data challenge 06 [45 min]<br />
** Parametrized likelihood + lensing template [Bischoff, 15 min] [https://docs.google.com/presentation/d/1bI90NApMEv4W_suqxp9a89wMH_KEdfu0qRKs9S1GmLY/edit#slide=id.g726e0d289c_0_65 slides]<br />
** Bayesian optimal analysis [Millea, 15 min] [https://docs.google.com/presentation/d/19ArC5olLsiz-Xl3Cm0w5LgyyzY7lECuDG4KSCqORZEk/edit?usp=sharing slides]<br />
** SO XForecast pipeline [Errard, 15 min] [https://www.dropbox.com/s/u3gq105bm86k2rp/CMBS4_lowellBB_LBNL_March2020.pdf?dl=0 slides]<br />
* Next steps for data challenges [45 min]<br />
** ILC maps to study impacts on foregrounds [Umilt&agrave;, 10 min][[:File: LBNL-Lowell_BB-ILC.pdf | slides]]<br />
** Exact curve-sky iterative lensing estimation [Carron, 10 min] [[:File: Cmbs4_iterativelensing.pdf | slides]]<br />
** Low ell foregrounds [[https://docs.google.com/presentation/d/1zywbOcyp579rUUOi0BzsQB308Fab5weHx254FhDwqH8/edit?usp=sharing Hensley], 15 min]<br />
** What other questions do we need to address using data challenges? [all]<br />
* Inputs for summer agency review [20 min]<br />
** Forecasting tool for Flowdown group [McMahon, 10 min] [https://docs.google.com/presentation/d/1nvKwzamazJmfpInylkX1JIgCbG9AnlYi5nRjb8MdOV8/edit?usp=sharing slides]<br />
** Design justification studies [Wu, 10 min] [https://docs.google.com/presentation/d/1FrartvnO9tZtD26hHonQqK1AeoLMzPXZOutqw3BezxE/edit?usp=sharing slides ] <br />
*** Sensitivity vs resolution for delensing LAT<br />
*** Frequency allocation for delensing LAT<br />
*** Justification for split-bands on SATs<br />
*** Justification for 20 GHz on delensing LAT<br />
<br />
== Notes ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=LBNL-2020:_Cosmology_with_CMB-S4&diff=10944LBNL-2020: Cosmology with CMB-S42020-03-31T16:05:53Z<p>Wlwu: /* Tuesday March 31 */</p>
<hr />
<div>== Workshop overview ==<br />
<br />
This workshop continues a successful series of meetings bringing together the CMB experimental and theoretical community to plan a coordinated, stage-4 ground-based CMB experiment. <br />
<br />
Due to COVID-19 quarantining the meeting will be held entirely remotely, 9:00am to 1:30pm Pacific Daylight Time, Monday March 30th to Thursday April 2nd.<br />
<br />
== Meeting Info & Registration ==<br />
<br />
Please continue to register at the website despite the remote nature of the event.<br />
<br />
[http://cmbs4lbl2020.lbl.gov Official Workshop Website: Registration, Participants, Logistics].<br />
<br />
== Remote Meeting Considerations ==<br />
<br />
All sessions will be held remotely by zoom.<br />
* Plenary sessions will all use https://lbnl.zoom.us/j/912694106<br />
* Parallel sessions will have connection details on their wiki page<br />
<br />
All participants should<br />
* Connect using a browser or the zoom app if at all possible so that you can use the "raise hand" button to contribute, especially in the plenary sessions.<br />
* Connect with a full name so that the session convenors and other participants can identify you.<br />
* Mute your line whenever you are not speaking.<br />
* Disable video so that we don't overwhelm participants with limited bandwidth.<br />
* Join the '''#lbnl2020''' channel on the [https://cmb-s4.slack.com CMB-S4 Slack workspace], email [mailto:zonca@sdsc.edu zonca@sdsc.edu] if you need an invitation<br />
<br />
== Agenda ==<br />
<br />
'''Note: All times below are US Pacific timezone!'''<br />
<br />
=== Monday March 30 ===<br />
<br />
https://lbnl.zoom.us/j/912694106<br />
<br />
[https://docs.google.com/document/d/1BrrX4yqEsi1rSaPJhLWqEPrtRu5_msqU_wGkC8VBxCI Plenary google doc]<br />
<br />
09:00 - Plenary 1 (Borrill/Carlstrom)<br />
* Collaboration Overview [https://docs.google.com/presentation/d/1-dOQywsPQ44AolMzNKYRyGgJMaVpCNn25Etvyn5sAMg slides] <br />
<br />
10:00 - Plenary 2 (Yeck)<br />
* Project Overview [https://docs.google.com/presentation/d/1M1XwAhYIBxVfOrRwQE7llzV_w5d4fS8JND7bFGSHjYo slides]<br />
<br />
11:00 - Break<br />
<br />
11:30 - Plenary 3 (McMahon)<br />
* Baseline Design Issues: Detectors, Readout, Modules [https://docs.google.com/presentation/d/1W2VNsbTsO-i8tf_ajjJeEce2lTYEDP2U4ZMjpF-l3cY slides]<br />
<br />
12:30 - Plenary 4 (Vieregg)<br />
* Baseline Design Issues: LAT, SAT, DAQ, DM, Sites [https://docs.google.com/presentation/d/10LzUhw0NrNVN0rxAObuTLVTK-Pmg-e7M-otfYdbwx4A slides]<br />
<br />
=== Tuesday March 31 ===<br />
<br />
09:00 - Parallel 1<br />
* [[LBNL-2020: Detectors_Readout_Modules | Detectors, Readout, Modules]] (Wollack/Benson)<br />
* [[LBNL-2020: LAT | Large Aperture Telescopes]] (Carlstrom/Niemack)<br />
* [[LBNL-2020: DAQ | Data Acquisition]] (Newburgh)<br />
* [[LBNL-2020: Low-ell_BB | Low-ell BB]] (Bischoff/Wu) Zoom line: https://fnal.zoom.us/j/5196960377 <br />
* [[LBNL-2020: Maps-to-Spectra | Maps-to-Spectra]] (Loverde/Reichardt)<br />
<br />
11:00 - Break<br />
<br />
11:30 - Parallel 2<br />
* [[LBNL-2020: Detectors_Readout_Modules | Detectors, Readout, Modules (cont)]] (Wollack/Benson)<br />
* [[LBNL-2020: SAT | Small Aperture Telescopes]] (Kovac/Kusaka)<br />
* [[LBNL-2020: DM | Data Management]] (Borrill/Crawford)<br />
* [[LBNL-2020: Sources | Sources]] (Battaglia/Vieira)<br />
* [[LBNL-2020: Maps-to-Other | Maps-to-Other Statistics]] (Sherwin/Alvarez)<br />
<br />
=== Wednesday April 1 ===<br />
<br />
09:00 - Parallel 3<br />
* [[LBNL-2020: Testing_Facilities | Testing Facilities]] (Benson)<br />
* [[LBNL-2020: Telescope_Interfaces: Sites_and_I&C | Telescope Interfaces: Sites and I&C]] (Ruhl/Arnold)<br />
* [[LBNL-2020: Cold_Optics | Cold Optics]] (McMahon)<br />
* [[LBNL-2020: S2M_Flowdown | Science-to-Measurement Flowdown]] (Lawrence)<br />
<br />
10:00 - Parallel 4<br />
* [[LBNL-2020: Telescope_Interfaces: DRM_and_DAQ | Telescope Interfaces: Detectors/Readout/Modules and DAQ]] (Zivick)<br />
* [[LBNL-2020: Cold_Optics | Cold Optics (cont)]] (McMahon)<br />
* [[LBNL-2020: S2M_Flowdown | Science-to-Measurement Flowdown (cont)]] (Lawrence)<br />
<br />
11:00 - Break<br />
<br />
11:30 - Parallel 5<br />
* [[LBNL-2020: M2T_Flowdown | Measurement-to-Technical Flowdown]] (Lawrence)<br />
* [[LBNL-2020: DAQ_DM_Sites_Interfaces | DAQ / DM / Sites Interfaces]] (Rahlin)<br />
* [[LBNL-2020: Galactic_Foreground_Modeling | Galactic Foreground Modeling]] (Hensley/Thorne)<br />
* [[LBNL-2020: Extragalactic_Foreground_Modeling | Extragalactic Foreground Modeling]] (van Engelen/Omori)<br />
<br />
12:30 - Parallel 6<br />
* [[LBNL-2020: M2T_Flowdown | Measurement-to-Technical Flowdown (cont)]] (Lawrence)<br />
* [[LBNL-2020: Transients: Science_Pipelines_Data | Transients: Science, Pipelines, Data]] (Holder)<br />
* [[LBNL-2020: Galactic_Foreground_Modeling | Galactic Foreground Modeling (cont)]] (Hensley/Thorne)<br />
* [[LBNL-2020: Cross-correlations_and_Complimentarity_for_LSS | Cross-correlations and Complimentarity for LSS]] (Ferraro)<br />
<br />
=== Thursday April 2 ===<br />
<br />
https://lbnl.zoom.us/j/912694106<br />
<br />
[https://docs.google.com/document/d/1BrrX4yqEsi1rSaPJhLWqEPrtRu5_msqU_wGkC8VBxCI Plenary google doc]<br />
<br />
09:00 - Plenary 5 (Barron)<br />
* Parallel Reports 1-2<br />
<br />
11:00 - Break<br />
<br />
11:30 - Plenary 6 (Borrill/Carlstrom)<br />
* Parallel Reports 3-6<br />
* Town Hall<br />
* Closeout</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=LBNL-2020:_Low-ell_BB&diff=10895LBNL-2020: Low-ell BB2020-03-31T05:14:23Z<p>Wlwu: /* Agenda */</p>
<hr />
<div>== Connection details ==<br />
<br />
Parallel 1, session D. Tuesday March 31, 9:00 to 11:00 am pacific.<br />
<br />
https://lbnl.zoom.us/j/676588242<br />
<br />
Monitor: Kimmy Wu<br />
<br />
Scribe: Colin Bischoff<br />
<br />
== Charge ==<br />
<br />
The primary focus of this meeting will be technical and scientific progress towards the baseline design in general and the summer agency review in particular.<br />
<br />
* Present results from or statuses of data challenge 6 with real delensing incorporated<br />
* Foreground models / sims<br />
** Impact of foregrounds on delensing.<br />
** Foregrounds at low-ell <br />
* Sketch path(s) forward for data challenges:<br />
** What questions need answering by the summer’s agency review that need results from data challenges?<br />
* Outline trade studies that need to be done (or present results of trade studies) for the delensing LAT<br />
** Sensitivity vs resolution<br />
** Frequency allocation<br />
* Outline trade studies that need to be done (or present results of trade studies) for SATs<br />
** Do we need 20GHz?<br />
<br />
== Agenda ==<br />
<br />
* Results from data challenge 06 [45 min]<br />
** Parametrized likelihood + lensing template [Bischoff, 15 min]<br />
** Bayesian optimal analysis [Millea, 15 min]<br />
** SO XForecast pipeline [Errard, 15 min]<br />
* Next steps for data challenges [45 min]<br />
** ILC maps to study impacts on foregrounds [Umilt&agrave;, 10 min]<br />
** Exact curve-sky iterative lensing estimation [Carron, 10 min]<br />
** Low ell foregrounds [[https://docs.google.com/presentation/d/1zywbOcyp579rUUOi0BzsQB308Fab5weHx254FhDwqH8/edit?usp=sharing Hensley], 15 min]<br />
** Interface with Data Management sims [Borrill/Crawford, 10 min]<br />
** What other questions do we need to address using data challenges? [all]<br />
* Inputs for summer agency review [20 min]<br />
** Forecasting tool for Flowdown group [McMahon, 10 min]<br />
** Design justification studies [Wu, 10 min] [https://docs.google.com/presentation/d/1FrartvnO9tZtD26hHonQqK1AeoLMzPXZOutqw3BezxE/edit?usp=sharing slides ] <br />
*** Sensitivity vs resolution for delensing LAT<br />
*** Frequency allocation for delensing LAT<br />
*** Justification for split-bands on SATs<br />
*** Justification for 20 GHz on delensing LAT<br />
<br />
== Notes ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=LBNL-2020:_Low-ell_BB&diff=10791LBNL-2020: Low-ell BB2020-03-29T21:31:59Z<p>Wlwu: /* Agenda */</p>
<hr />
<div>== Connection details ==<br />
<br />
Parallel 1, session D. Tuesday March 31, 9:00 to 11:00 am pacific.<br />
<br />
https://lbnl.zoom.us/j/676588242<br />
<br />
Monitor: Kimmy Wu<br />
<br />
Scribe: Colin Bischoff<br />
<br />
== Charge ==<br />
<br />
The primary focus of this meeting will be technical and scientific progress towards the baseline design in general and the summer agency review in particular.<br />
<br />
* Present results from or statuses of data challenge 6 with real delensing incorporated<br />
* Foreground models / sims<br />
** Impact of foregrounds on delensing.<br />
** Foregrounds at low-ell <br />
* Sketch path(s) forward for data challenges:<br />
** What questions need answering by the summer’s agency review that need results from data challenges?<br />
* Outline trade studies that need to be done (or present results of trade studies) for the delensing LAT<br />
** Sensitivity vs resolution<br />
** Frequency allocation<br />
* Outline trade studies that need to be done (or present results of trade studies) for SATs<br />
** Do we need 20GHz?<br />
<br />
== Agenda ==<br />
<br />
* Results from data challenge 06 [45 min]<br />
** Parametrized likelihood + lensing template [Bischoff, 15 min]<br />
** Bayesian optimal analysis [Millea, 15 min]<br />
** SO XForecast pipeline [Errard, 15 min]<br />
* Next steps for data challenges<br />
** ILC maps to study impacts on foregrounds [Umilt&agrave;, 10 min]<br />
** Exact curve-sky iterative lensing estimation [Carron, 10 min]<br />
** Low ell foregrounds [Hensley, 15 min]<br />
** Interface with Data Management sims [Borrill/Crawford]<br />
** What other questions do we need to address using data challenges? [all]<br />
* Inputs for summer agency review<br />
** Forecasting tool for Flowdown group [McMahon]<br />
** Design justification studies [Wu]<br />
*** Sensitivity vs resolution for delensing LAT<br />
*** Frequency allocation for delensing LAT<br />
*** Justification for split-bands on SATs<br />
*** Justification for 20 GHz on delensing LAT<br />
<br />
== Notes ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=LBNL-2020:_Low-ell_BB&diff=10776LBNL-2020: Low-ell BB2020-03-28T23:15:35Z<p>Wlwu: /* Agenda */</p>
<hr />
<div>== Connection details ==<br />
<br />
Parallel 1, session D. Tuesday March 31, 9:00 to 11:00 am pacific.<br />
<br />
https://lbnl.zoom.us/j/676588242<br />
<br />
Monitor: Kimmy Wu<br />
<br />
Scribe: Colin Bischoff<br />
<br />
== Charge ==<br />
<br />
The primary focus of this meeting will be technical and scientific progress towards the baseline design in general and the summer agency review in particular.<br />
<br />
* Present results from or statuses of data challenge 6 with real delensing incorporated<br />
* Foreground models / sims<br />
** Impact of foregrounds on delensing.<br />
** Foregrounds at low-ell <br />
* Sketch path(s) forward for data challenges:<br />
** What questions need answering by the summer’s agency review that need results from data challenges?<br />
* Outline trade studies that need to be done (or present results of trade studies) for the delensing LAT<br />
** Sensitivity vs resolution<br />
** Frequency allocation<br />
* Outline trade studies that need to be done (or present results of trade studies) for SATs<br />
** Do we need 20GHz?<br />
<br />
== Agenda ==<br />
<br />
* Results from data challenge 06 [45 min]<br />
** Parametrized likelihood + lensing template [Bischoff, 15 min]<br />
** Bayesian optimal analysis [Millea, 15 min]<br />
** SO XForecast pipeline [Errard, 15 min]<br />
* Next steps for data challenges<br />
** ILC maps to study impacts on foregrounds [Umilt&agrave;, 10 min]<br />
** Exact curve-sky iterative lensing estimation [Carron]<br />
** Low ell foregrounds [Hensley]<br />
** Interface with Data Management sims [Borrill/Crawford]<br />
** What other questions do we need to address using data challenges? [all]<br />
* Inputs for summer agency review<br />
** Forecasting tool for Flowdown group [McMahon]<br />
** Design justification studies [Wu]<br />
*** Sensitivity vs resolution for delensing LAT<br />
*** Frequency allocation for delensing LAT<br />
*** Justification for split-bands on SATs<br />
*** Justification for 20 GHz on delensing LAT<br />
<br />
== Notes ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=LBNL-2020:_Low-ell_BB&diff=10775LBNL-2020: Low-ell BB2020-03-28T23:14:55Z<p>Wlwu: /* Agenda */</p>
<hr />
<div>== Connection details ==<br />
<br />
Parallel 1, session D. Tuesday March 31, 9:00 to 11:00 am pacific.<br />
<br />
https://lbnl.zoom.us/j/676588242<br />
<br />
Monitor: Kimmy Wu<br />
<br />
Scribe: Colin Bischoff<br />
<br />
== Charge ==<br />
<br />
The primary focus of this meeting will be technical and scientific progress towards the baseline design in general and the summer agency review in particular.<br />
<br />
* Present results from or statuses of data challenge 6 with real delensing incorporated<br />
* Foreground models / sims<br />
** Impact of foregrounds on delensing.<br />
** Foregrounds at low-ell <br />
* Sketch path(s) forward for data challenges:<br />
** What questions need answering by the summer’s agency review that need results from data challenges?<br />
* Outline trade studies that need to be done (or present results of trade studies) for the delensing LAT<br />
** Sensitivity vs resolution<br />
** Frequency allocation<br />
* Outline trade studies that need to be done (or present results of trade studies) for SATs<br />
** Do we need 20GHz?<br />
<br />
== Agenda ==<br />
<br />
* Results from data challenge 06 [45 min]<br />
** Parametrized likelihood + lensing template [Bischoff, 15 min]<br />
** Bayesian optimal analysis [Millea, 15 min]<br />
** SO XForecast pipeline [Errard, 15 min]<br />
* Next steps for data challenges<br />
** ILC maps to study impacts on foregrounds [Umilt&agrave;, 10 min]<br />
** Exact curve-sky iterative lensing estimation [Carron]<br />
** Low ell foregrounds [Hensley]<br />
** Interface with Data Management sims [Crawford]<br />
** What other questions do we need to address using data challenges? [all]<br />
* Inputs for summer agency review<br />
** Forecasting tool for Flowdown group [McMahon]<br />
** Design justification studies [Wu]<br />
*** Sensitivity vs resolution for delensing LAT<br />
*** Frequency allocation for delensing LAT<br />
*** Justification for split-bands on SATs<br />
*** Justification for 20 GHz on delensing LAT<br />
<br />
== Notes ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=LBNL-2020:_Low-ell_BB&diff=10700LBNL-2020: Low-ell BB2020-03-24T16:11:01Z<p>Wlwu: /* Agenda */</p>
<hr />
<div>== Connection details ==<br />
<br />
Parallel 1, session D. Tuesday March 31, 9:00 to 11:00 am pacific.<br />
<br />
https://lbnl.zoom.us/j/676588242<br />
<br />
Monitor: Kimmy Wu<br />
<br />
Scribe: Colin Bischoff<br />
<br />
== Charge ==<br />
<br />
The primary focus of this meeting will be technical and scientific progress towards the baseline design in general and the summer agency review in particular.<br />
<br />
* Present results from or statuses of data challenge 6 with real delensing incorporated<br />
* Foreground models / sims<br />
** Impact of foregrounds on delensing.<br />
** Foregrounds at low-ell <br />
* Sketch path(s) forward for data challenges:<br />
** What questions need answering by the summer’s agency review that need results from data challenges?<br />
* Outline trade studies that need to be done (or present results of trade studies) for the delensing LAT<br />
** Sensitivity vs resolution<br />
** Frequency allocation<br />
* Outline trade studies that need to be done (or present results of trade studies) for SATs<br />
** Do we need 20GHz?<br />
<br />
== Agenda ==<br />
<br />
* Results from data challenge 06 [45 min]<br />
** Parametrized likelihood + lensing template [Bischoff, 15 min]<br />
** Bayesian optimal analysis [Millea, 15 min]<br />
** SO XForecast pipeline [Errard, 15 min]<br />
* Next steps for data challenges<br />
** ILC maps to study impacts on foregrounds [Umilt&agrave;, 10 min]<br />
** Impacts of foregrounds on delensing [van Engelen]<br />
** Low ell foregrounds [Hensley]<br />
** Interface with Data Management sims [Crawford]<br />
** What other questions do we need to address using data challenges? [all]<br />
* Inputs for summer agency review<br />
** Forecasting tool for Flowdown group [McMahon]<br />
** Design justification studies [Wu]<br />
*** Sensitivity vs resolution for delensing LAT<br />
*** Frequency allocation for delensing LAT<br />
*** Justification for split-bands on SATs<br />
*** Justification for 20 GHz on delensing LAT<br />
<br />
== Notes ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=LBNL-2020:_Low-ell_BB&diff=10691LBNL-2020: Low-ell BB2020-03-23T17:47:08Z<p>Wlwu: /* Agenda */</p>
<hr />
<div>== Connection details ==<br />
<br />
Parallel 1, session D. Tuesday March 31, 9:00 to 11:00 am pacific.<br />
<br />
https://lbnl.zoom.us/j/676588242<br />
<br />
Monitor: Kimmy Wu<br />
<br />
Scribe: Colin Bischoff<br />
<br />
== Charge ==<br />
<br />
The primary focus of this meeting will be technical and scientific progress towards the baseline design in general and the summer agency review in particular.<br />
<br />
* Present results from or statuses of data challenge 6 with real delensing incorporated<br />
* Foreground models / sims<br />
** Impact of foregrounds on delensing.<br />
** Foregrounds at low-ell <br />
* Sketch path(s) forward for data challenges:<br />
** What questions need answering by the summer’s agency review that need results from data challenges?<br />
* Outline trade studies that need to be done (or present results of trade studies) for the delensing LAT<br />
** Sensitivity vs resolution<br />
** Frequency allocation<br />
* Outline trade studies that need to be done (or present results of trade studies) for SATs<br />
** Do we need 20GHz?<br />
<br />
== Agenda ==<br />
<br />
* Results from data challenge 06 [45 min]<br />
** Parametrized likelihood + lensing template [Bischoff, 15 min]<br />
** Bayesian optimal analysis [Millea, 15 min]<br />
** SO XForecast pipeline [Errard, 15 min]<br />
* Next steps for data challenges<br />
** ILC maps to study impacts on foregrounds [Umilt&agrave;]<br />
** Impacts of foregrounds on delensing [van Engelen]<br />
** Low ell foregrounds [Hensley]<br />
** Interface with Data Management sims [Crawford]<br />
** What other questions do we need to address using data challenges? [all]<br />
* Inputs for summer agency review<br />
** Forecasting tool for Flowdown group [McMahon]<br />
** Design justification studies [Wu]<br />
*** Sensitivity vs resolution for delensing LAT<br />
*** Frequency allocation for delensing LAT<br />
*** Justification for split-bands on SATs<br />
*** Justification for 20 GHz on delensing LAT<br />
<br />
== Notes ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=LBNL-2020:_Low-ell_BB&diff=10690LBNL-2020: Low-ell BB2020-03-23T17:46:27Z<p>Wlwu: /* Agenda */</p>
<hr />
<div>== Connection details ==<br />
<br />
Parallel 1, session D. Tuesday March 31, 9:00 to 11:00 am pacific.<br />
<br />
https://lbnl.zoom.us/j/676588242<br />
<br />
Monitor: Kimmy Wu<br />
<br />
Scribe: Colin Bischoff<br />
<br />
== Charge ==<br />
<br />
The primary focus of this meeting will be technical and scientific progress towards the baseline design in general and the summer agency review in particular.<br />
<br />
* Present results from or statuses of data challenge 6 with real delensing incorporated<br />
* Foreground models / sims<br />
** Impact of foregrounds on delensing.<br />
** Foregrounds at low-ell <br />
* Sketch path(s) forward for data challenges:<br />
** What questions need answering by the summer’s agency review that need results from data challenges?<br />
* Outline trade studies that need to be done (or present results of trade studies) for the delensing LAT<br />
** Sensitivity vs resolution<br />
** Frequency allocation<br />
* Outline trade studies that need to be done (or present results of trade studies) for SATs<br />
** Do we need 20GHz?<br />
<br />
== Agenda ==<br />
<br />
* Results from data challenge 06 [45 min]<br />
** Parametrized likelihood + lensing template [Bischoff, 15 min]<br />
** Bayesian optimal analysis [Millea, 15 min]<br />
** SO XForecast pipeline [Errard, 15 min]<br />
* Next steps for data challenges<br />
** Impacts of foregrounds on delensing [van Engelen, Umilt&agrave;]<br />
** Low ell foregrounds [Hensley]<br />
** Interface with Data Management sims [Crawford]<br />
** What other questions do we need to address using data challenges? [all]<br />
* Inputs for summer agency review<br />
** Forecasting tool for Flowdown group [McMahon]<br />
** Design justification studies [Wu]<br />
*** Sensitivity vs resolution for delensing LAT<br />
*** Frequency allocation for delensing LAT<br />
*** Justification for split-bands on SATs<br />
*** Justification for 20 GHz on delensing LAT<br />
<br />
== Notes ==</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Low-ell_BB&diff=10532Low-ell BB2020-02-26T18:59:26Z<p>Wlwu: </p>
<hr />
<div>This analysis working group is focused on the goal of constraining primordial gravitational waves / inflation using low-ell B-mode polarization.<br />
<br />
== Organization ==<br />
<br />
* Coordinators: Kimmy Wu (<code>wlwu at kicp dot uchicago dot edu</code>) and Colin Bischoff (<code>bischocn@ucmail.uc.edu</code>)<br />
* Email list: [https://cmb-s4.org/mailman/listinfo/gravitationalwaves gravitational waves]<br />
* Telecons: every other Monday at 12:30 eastern / 11:30 central / 9:30 pacific ([https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg@group.calendar.google.com calendar]). [https://docs.google.com/document/d/1886yT1b6QDuWvsbAu5HmVv2Cl4pfH00YpK5Fv8dNzcM/edit Telecon notes]<br />
* [[Science_Council|Science Council wiki page]]<br />
<br />
== Past and Current Work ==<br />
<br />
* [[Simulation and Forecasting Logbook]]<br />
* [[Data Challenges]]<br />
* [[LowellBB_Project_List|Low-ell BB Project List]]<br />
<br />
== Publications ==<br />
<br />
=== CMB-S4 Forecasted Constraints on Primoridal Gravitational Waves ===<br />
<br />
* Contact: Victor Buza<br />
* TeX repository: [https://github.com/CMB-S4/ForecastingPapers CMB-S4/ForecastingPapers]<br />
* [https://docs.google.com/document/d/1RUqbMDuNFQLFOkKZhZw_99qJ_EljtuorhKFBYyTNTMI/edit# Editing notes], [http://spud.spa.umn.edu/~pryke/s4_forecast_paper.pdf auto-gen pdf]<br />
* Status (2020-02-17): sent paper draft to Publications Board for internal review<br />
<br />
== Collaboration meetings ==<br />
<br />
=== [[UCSD-2019:_Cosmology_with_CMB-S4|UCSD-2019]] ===<br />
<br />
* [[Media:Flauger_191017_PGW.pdf|Working group update]] (Flauger)<br />
* [[UCSD-2019:_Science_Theme:_PGW_%26_Inflation|Science parallel]] and [[Media:191018_Summary.pdf|summary slides]]<br />
* [[UCSD-2019:_Analysis/Pipeline_Working_Group:_Low-ell_BB|Analysis working group parallel]] with notes<br />
<br />
=== [[Fermilab-2019:_Cosmology_with_CMB-S4|Fermilab-2019]] ===<br />
<br />
* [https://docs.google.com/presentation/d/18UsMRhIHlk8mrWkIuoSwpLPfTPXZbwceW0EhQ4ixGQ8/edit#slide=id.p Working group update] (Pryke)<br />
<br />
=== [[Princeton-2018:_Cosmology_with_CMB-S4|Princeton-2018]] ===<br />
<br />
* [[Media:GWPrinceton.pdf|Working group update]] (Flauger)<br />
* [[Media:R_forecast_update.pdf|r forecasting update]] (Pryke) ''slides not actually shown at meeting''<br />
* [[Media:Small_area_forecast.pdf|Noise Tiger Team small area forecast]] (Bischoff)<br />
<br />
=== [[Argonne-2018:_Cosmology_with_CMB-S4|Argonne-2018]] ===<br />
<br />
* [[Argonne-2018:P1-4|Forecasting delensing parallel]], [[Media:SlidesDelensingSession.pdf|summary slides]]<br />
* [[Argonne-2018:P3-2|Forecasting systematics parallel]], [[Media:P3-2_summary.pdf|summary slides]]<br />
* [[Argonne-2018:P3-3|Forecasting sky model parallel]], [[Media:Argonne_Summary_Flauger.pdf|summary slides]]<br />
<br />
=== [[Harvard-2017:_Cosmology_with_CMB-S4|Harvard-2017]] ===<br />
<br />
* [[Harvard-2017:T2|Systematics and noise realism parallel]], [[Media:Parallel_T2.pdf|summary slides]]<br />
* [[Harvard-2017:T3|Sky modeling, component separation, lensing reconstruction]], [[Media:S4Review.pdf|summary slides]]<br />
<br />
=== [[SLAC-2017:_Cosmology_with_CMB-S4|SLAC-2017]] ===<br />
<br />
* [[Media:R_forecasting_Knox.key.pdf|Simulations for r forecasting]] (Knox)<br />
* [[SLAC-2017:FSM_Large_angular_scales|Foregrounds, systematics, modeling for large angular scales parallel]]<br />
<br />
=== [[UChicago-2016:_Cosmology_with_CMB-S4|UChicago-2016]] ===<br />
<br />
* [[Chicago-2016:_Inflation|Science Book Chapter 2 - Inflation]]<br />
* [[Chicago-2016:_r_Forecasting|r forecasting parallel]]<br />
<br />
=== [[LBNL-2016:_Cosmology_with_CMB-S4|LBNL-2016]] ===<br />
<br />
* [[LBNL-2016:_Inflation|Inflation breakout]], [[LBNL-2016:_Inflation_Summary|summary]]<br />
* [[LBNL-2016:_Foregrounds_for_Inflation_and_Lensing|Foregrounds for inflation and lensing breakout]], [[Plenary_Summary|summary]]<br />
* [[LBNL-2016:_Sky_Modeling|Sky modeling breakout]]<br />
<br />
=== [[UMICH-2015:_Cosmology_with_CMB-S4|Michigan-2015]] ===<br />
<br />
* [[UMICH-2015:_Inflation|Inflation breakout]]</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Foreground_Simulation_Requirements&diff=10498Foreground Simulation Requirements2020-02-10T18:43:30Z<p>Wlwu: /* Low-ell BB */</p>
<hr />
<div>Foreground simulation requirements vary from group to group. Below each AWG describes what they require in foreground simulations in order for the data simulations made from those foreground models to be sufficient for addressing their flowdown questions. <br />
<br />
====Low-ell BB====<br />
<br />
For the r analysis, we need both large-scale Galactic foreground simulations and small-scale Galactic and extragalactic foreground simulations. The small scale sims are relevant for studying the impact of foreground on lensing reconstruction and thus delensing on r. <br />
<br />
For the extragalactic foregrounds in temperature, the requirements would be similar to the Maps2OtherStats group. We will need mode detailed foreground sims in polarization than other groups, e.g. polarized point sources, small scale Galactic foregrounds. <br />
<br />
Specifically, we would like<br />
* diffuse polarized foregrounds with realistic (but not totally pessimistic) levels of complication<br />
* non-Gaussianity in the foregrounds to test lensing reconstruction / delensing<br />
* models that contain small (fsky ~ 3%) regions of low polarized foreground amplitude, i.e. the BICEP/Keck patch with A_dust = 5 uK^2 at 353 GHz<br />
<br />
====Maps2Cell====<br />
'''Synopsis:''' The Foreground sim requirements for the power spectrum science are closely related to the Neutrino mass set for Maps2Other (delensing TE/EE introduces the same dependency on lensing reconstruction). <br />
<br />
'''Neff:'''<br />
<br />
Foreground modeling / simulation requirements:<br />
<br />
- Polarized galactic foreground simulations, ideally including non-Gaussian small-scale structure<br />
<br />
- Temperature and polarization extragalactic foreground simulations: correlated tSZ, CIB, kSZ, sources, lensing<br />
<br />
Simulation availability and need:<br />
<br />
-Polarized non-Gaussian sims: mainly Vansyngel - more needed! <br />
<br />
-Extragalactic “foregrounds”: Sehgal, Websky, Multidark, MDPL2,...<br />
<br />
'''SZ, CIB spectra:'''<br />
<br />
Foreground modeling / simulation requirements:<br />
<br />
-Temperature extragalactic foreground simulations: correlated tSZ, CIB, kSZ, sources, lensing<br />
<br />
Simulation availability and need:<br />
<br />
-Extragalactic “foregrounds”: Sehgal, Websky, Multidark, MDPL2,...<br />
<br />
====Maps2OtherStats====<br />
<br />
<br />
====Sources====<br />
<br />
* Clusters & proto-clusters: Something like the Websky extragalactic sky or enhanced Sehgal et al simulations are sufficient for cluster, proto-cluster, and SMG detection forecasting. Details, extragalactic simulations for 60 percent of the sky, including radio, CIB, lensing, and SZ signals, resolving down to ~a few 10^12 solar mass halos (a optical HOD would be great too). Having the simulated noise from the scanning strategy on top of that with the various depths from the deep and wide surveys would be ideal. Including variants of the experimental configurations would be great if we wanted to try and optimize for source science. A further iteration would be to have a simulated polarized extragalactic sky from websky or something like that.<br />
<br />
* Transients/GRBs: Can we inject sources into the TOD simulations? Can Toast do this? That's what we need.</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Foreground_Simulation_Requirements&diff=10497Foreground Simulation Requirements2020-02-10T18:30:31Z<p>Wlwu: /* Low-ell BB */</p>
<hr />
<div>Foreground simulation requirements vary from group to group. Below each AWG describes what they require in foreground simulations in order for the data simulations made from those foreground models to be sufficient for addressing their flowdown questions. <br />
<br />
====Low-ell BB====<br />
<br />
For the r analysis, we need both large-scale Galactic foreground simulations and small-scale Galactic and extragalactic foreground simulations. The small scale sims are relevant for studying the impact of foreground on lensing reconstruction and thus delensing on r. <br />
<br />
For the extragalactic foregrounds in temperature, the requirements would be similar to the Maps2OtherStats group. We will need higher S/N foreground sims in polarization than other groups.<br />
<br />
====Maps2Cell====<br />
'''Synopsis:''' The Foreground sim requirements for the power spectrum science are closely related to the Neutrino mass set for Maps2Other (delensing TE/EE introduces the same dependency on lensing reconstruction). <br />
<br />
'''Neff:'''<br />
<br />
Foreground modeling / simulation requirements:<br />
<br />
- Polarized galactic foreground simulations, ideally including non-Gaussian small-scale structure<br />
<br />
- Temperature and polarization extragalactic foreground simulations: correlated tSZ, CIB, kSZ, sources, lensing<br />
<br />
Simulation availability and need:<br />
<br />
-Polarized non-Gaussian sims: mainly Vansyngel - more needed! <br />
<br />
-Extragalactic “foregrounds”: Sehgal, Websky, Multidark, MDPL2,...<br />
<br />
'''SZ, CIB spectra:'''<br />
<br />
Foreground modeling / simulation requirements:<br />
<br />
-Temperature extragalactic foreground simulations: correlated tSZ, CIB, kSZ, sources, lensing<br />
<br />
Simulation availability and need:<br />
<br />
-Extragalactic “foregrounds”: Sehgal, Websky, Multidark, MDPL2,...<br />
<br />
====Maps2OtherStats====<br />
<br />
<br />
====Sources====<br />
<br />
* Clusters & proto-clusters: Something like the Websky extragalactic sky or enhanced Sehgal et al simulations are sufficient for cluster, proto-cluster, and SMG detection forecasting. Details, extragalactic simulations for 60 percent of the sky, including radio, CIB, lensing, and SZ signals, resolving down to ~a few 10^12 solar mass halos (a optical HOD would be great too). Having the simulated noise from the scanning strategy on top of that with the various depths from the deep and wide surveys would be ideal. Including variants of the experimental configurations would be great if we wanted to try and optimize for source science. A further iteration would be to have a simulated polarized extragalactic sky from websky or something like that.<br />
<br />
* Transients/GRBs: Can we inject sources into the TOD simulations? Can Toast do this? That's what we need.</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=LowellBB_Project_List&diff=10343LowellBB Project List2019-11-25T18:23:14Z<p>Wlwu: /* Threads that can use more attention */</p>
<hr />
<div><br />
Summary of low-ell BB work so far and sketch of plans forward (Oct 2019 UCSD meeting): [[https://docs.google.com/presentation/d/164NM-vBg0DvYUgGAtbZ1XgIgBNFFloOTWmcewPEsIGQ/edit?usp=sharing slides]]<br />
<br />
= On-going projects =<br />
<br />
- Bayesian r-analysis<br />
- MAP phi estimate extension to curved-sky<br />
- Foreground clean map for phi reconstruction<br />
- Cross-spectra parametric r-pipeline<br />
<br />
= Threads that can use more attention =<br />
- Impacts of Galactic foregrounds on delensing <br />
- Instrumental systematics impacts on delensing<br />
- Instrumental systematics impacts on degree-scale measurements<br />
- Field selection for the deep survey<br />
- Forecast comparison between S4 and SO sims<br />
- Development of additional foreground models/sims, and development of an approach to managing our uncertainty about foreground properties and how this impacts flowdown to design.<br />
<br />
Join by working on [[Data_Challenges]]!</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=LowellBB_Project_List&diff=10339LowellBB Project List2019-11-22T19:14:05Z<p>Wlwu: Created page with " Summary of low-ell BB work so far and sketch of plans forward (Oct 2019 UCSD meeting): https://docs.google.com/presentation/d/164NM-vBg0DvYUgGAtbZ1XgIgBNFFloOTWmcewPEsIGQ/e..."</p>
<hr />
<div><br />
Summary of low-ell BB work so far and sketch of plans forward (Oct 2019 UCSD meeting): [[https://docs.google.com/presentation/d/164NM-vBg0DvYUgGAtbZ1XgIgBNFFloOTWmcewPEsIGQ/edit?usp=sharing slides]]<br />
<br />
= On-going projects =<br />
<br />
- Bayesian r-analysis<br />
- MAP phi estimate extension to curved-sky<br />
- Foreground clean map for phi reconstruction<br />
- Cross-spectra parametric r-pipeline<br />
<br />
= Threads that can use more attention =<br />
- Impacts of Galactic foregrounds on delensing <br />
- Instrumental systematics impacts on delensing<br />
- Instrumental systematics impacts on degree-scale measurements<br />
- Field selection for the deep survey<br />
- Forecast comparison between S4 and SO sims<br />
<br />
Join by working on [[Data_Challenges]]!</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Science_Council&diff=10338Science Council2019-11-22T19:07:41Z<p>Wlwu: /* Analysis Working Groups */</p>
<hr />
<div>The Science Council consists of two co-Chairs and the co-Coordinators of four Analysis Working Groups (AWGs). We list the working groups here, together with information<br />
about their activities -- such as information about when they meet and links to meeting notes. The co-Chairs are Gil Holder (gil.holder@gmail.com) and Lloyd Knox (lknox@ucdavis.edu).<br />
<br />
===Overview===<br />
Our main focus now is "flowing down" the science to measurement requirements in preparation for CD-1/PDR. <br />
<br />
===Analysis Working Groups===<br />
<br />
====Low-ell BB==== <br />
- Co-Coordinators: Colin Bischoff (bischocn@ucmail.uc.edu) and Kimmy Wu (wlwu_at_kicp_dot_uchicago_dot_edu)<br />
- Meeting Notes: https://docs.google.com/document/d/1886yT1b6QDuWvsbAu5HmVv2Cl4pfH00YpK5Fv8dNzcM<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: [[Data_Challenges|r forecast sim set summary]]<br />
- Project list: [[LowellBB_Project_List | LowellBB_Project List]]<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
- Forecast paper draft: [http://spud.spa.umn.edu/~pryke/s4_forecast_paper.pdf auto update pdf]<br />
<br />
====Maps2Cell====<br />
- Co-Coordinators: Marilena Loverde (marilena.loverde@stonybrook.edu) and Christian Reichardt (christian.reichardt@unimelb.edu.au)<br />
- Project list: [[Maps2Cell_Project_List | Maps2CellProject List]]<br />
- Meeting Notes: [https://docs.google.com/document/d/1GevFM9MsQ716W3hobVKcFbP0rJWeff5d2F34jJ1V8c8/edit?usp=sharing[Link]]<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: N/A<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Maps2OtherStats====<br />
- Co-Coordinators: Blake Sherwin (sherwin@damtp.cam.ac.uk) and Marcelo Alvarez (marcelo.alvarez@berkeley.edu)<br />
- Meeting Notes: [https://docs.google.com/document/d/1uRkComeC4h9pJfWbkq0sK-NwvWp51asDVXny8BTH2YA/edit?usp=sharing[Link]]<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: N/A<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Sources====<br />
- Co-Coordinators: Joaquin Vieira (jvieira@illinois.edu) and Nick Battaglia (nbatta@astro.cornell.edu)<br />
- Meeting Notes: [https://docs.google.com/document/d/1rImHymDp3tGvd91k-d_bzD3060aejsyOcJ-h4TPKaxY/edit?usp=sharing[Link]]<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: N/A<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
===Historical Stuff below here===<br />
<br />
====Science White Papers====<br />
<br />
We are envisioning a series of SWP submitted by the January 2019 deadline. The papers will describe the entirety of science deliverable with observations in CMB frequency bands (loosely defined). The SWPs are common to the entire community; they will not discuss nor highlight any specific project. All interested members of the community are invited to participate in writing and endorsing any of these papers. <br />
<br />
SWP drafts that are ready for comment are available here:<br />
1) Neutrino Mass from Cosmology<br />
Link to the draft: http://dvorkin.physics.harvard.edu/Astro2020_Neutrino_Mass.pdf<br />
Contact person: Cora Dvorkin (cdvorkin@g.harvard.edu)<br />
2) Primordial non-Gaussianity <br />
Link to the draft:https://www.overleaf.com/read/bfsyyxfdqnvq<br />
Contact Person: Daan Meerburg (daanmeerburg@gmail.com) <br />
3) Dark Matter Physics with Cosmological Probes<br />
Link to the draft [PRELIMINARY, incomplete]: https://github.com/veragluscevic/Astro2020-DM-Cosmology<br />
Contact person: Vera Gluscevic (vera.gluscevic@gmail.com)<br />
4) Dark Energy<br />
Link to the draft: https://www.overleaf.com/read/phkpmjbjydwq<br />
Contact person: Anze Slosar (anze@bnl.gov)<br />
5) Features in the primordial power spectrum<br />
Link to the draft: https://www.overleaf.com/read/kyxzvmrbqpgy<br />
Contact person: Anze Slosar (anze@bnl.gov)<br />
6) Messengers from the Early Universe: Cosmic Neutrinos and Other Light Relics <br />
Link to the draft: https://www.overleaf.com/read/ybxqdqnhvtkm<br />
Contact person: Dan Green (drgreen@ucsd.edu)<br />
7) Testing gravity and particle physics with cosmic microwave background constraints on gravitational waves<br />
Link to the draft: https://www.overleaf.com/read/dsfnphrxfgbn<br />
Contact person: Sarah Shandera (shandera@gmail.com)<br />
8) Probing Feedback in Galaxy Formation with Millimeter-wave Observations<br />
Link to the draft: https://www.overleaf.com/read/ypcrxscjwnwr<br />
Contact people: Colin Hill (jch@ias.edu) and Nick Battaglia (nbatta@astro.cornell.edu)<br />
9) Reionization with the CMB <br />
Link to the draft: https://www.overleaf.com/read/bhdvxzqbprkf<br />
Contact people: Marcelo Alvarez (marcelo.alvarez@berkeley.edu) and Cora Dvorkin (cdvorkin@g.harvard.edu)<br />
<br />
<br />
The SWP are limited to 5 pages or fewer each, and we highly recommend that anyone wishing to contribute will read the short National Academies solicitation. Excerpting this key passage from the call may be helpful here:<br />
<br />
White papers should:<br />
- Identify scientific opportunities and compelling scientific themes for the coming decade, particularly those that have arisen from recent advances and accomplishments in astronomy and astrophysics;<br />
- Describe the scientific context of the importance of these opportunities, including connections to other parts of astronomy and astrophysics and, where appropriate, to the advancement of our broader scientific understanding;<br />
- While focusing on science, not specific missions or projects, describe and quantify the key advances in observation, measurement, theory, and/or computation necessary to realize the scientific opportunities within the decade 2020-2030 and beyond.<br />
<br />
To facilitate engagement and coordination of activities, we have created a wiki page (https://zzz.physics.umn.edu/decadal2020/doku.php?id=start) with a (non-comprehensive) list of potential science white papers with relevance to our community. Listed there are titles, and (mostly blank) fields for listing who is actively participating in the creation of the white paper, who has taken on a coordinating role, and links to relevant documentation for that white paper (github repos, online notes, etc.). <br />
<br />
The purpose of the wiki page is to give all of us a comprehensive view of science white paper activity of relevance to the CMB community, make it possible for would-be contributors to join existing efforts, and to allow any of us to spot gaps and work to fill them. The list of paper titles on the wiki now is just to get us started -- we expect it to evolve as, e.g., some topics get split into two or more different white papers, and new topics altogether are added. Anyone wishing to edit the wiki should contact Shaul Hanany (hanany@umn.edu) to get the appropriate permissions.<br />
<br />
====CMB-S4 Decadal Survey Report====<br />
<br />
Each AWG (with some exceptions) is charged with producing a 5-page section, the main elements of the Science Chapter of the DSR, on the science to be done with the CMB-S4 surveys. Our target for completion of a first draft of the DSR is November 2018. <br />
<br />
=====Draft Schedule for Production of Science Chapter sections=====<br />
<br />
- Friday, Sept 28: Long and rough draft completed<br />
- Friday, Oct 19: 5-page rough draft completed<br />
- Friday, Nov 3: cleaned-up draft ready to go out for review and comment<br />
- Wednesday, Nov 21: comments due back to AWGs<br />
- Friday, Dec 7: DSR chapter finalized<br />
- Dec 11 to 13: Internal DSR review in Washington, D.C. Each AWG should have one co-coordinator there<br />
<br />
===Former SC Analysis Working Groups===<br />
<br />
====Primordial Gravitational Waves==== <br />
- Co-Coordinators: Raphael Flauger (flauger@physics.utexas.edu) and Clem Pryke (pryke@physics.umn.edu)<br />
- Meeting Notes: https://docs.google.com/document/d/1886yT1b6QDuWvsbAu5HmVv2Cl4pfH00YpK5Fv8dNzcM<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: [[Data_Challenges|r forecast sim set summary]]<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
- Forecast paper draft: [http://spud.spa.umn.edu/~pryke/s4_forecast_paper.pdf[auto update pdf]]<br />
<br />
====Primordial Density Perturbations====<br />
- Co-Coordinators: Cora Dvorkin (cdvorkin@g.harvard.edu) & Daan Meerburg (daanmeerburg@gmail.com)<br />
<br />
- Telecons on-needed basis; see [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Light Relics====<br />
- Co-Coordinators: Daniel Green (drgreen@physics.ucsd.edu) and Joel Meyers (jmeyers@cita.utoronto.ca)<br />
- Forecasting Setup: [[Forecasting|Non-r Forecasting Page]]<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Neutrino Mass====<br />
- Co-Coordinators: Marilena Loverde (marilena.loverde@stonybrook.edu) and Blake Sherwin (sherwin@damtp.cam.ac.uk)<br />
- Meeting notes: https://cmb-s4.org/wiki/index.php/Neutrino_Mass_WG_Telecon<br />
- Call summaries: https://docs.google.com/document/d/1TWaU75wN1kqbYD1qkwzcJA9fZXGviKSezj3EnlP-ep8/edit?usp=sharing<br />
- Meeting times: will be posted; typically Tuesday 11am ET<br />
====Dark Energy ====<br />
- Co-Coordinators: Anze Slosar (anze@bnl.gov), and David Alonso (David.Alonso@physics.ox.ac.uk)<br />
- Meeting Notes: https://docs.google.com/document/d/13RTNgJNlWd098EPLnQrAAlstqDtyE850P9HnNFqCJZk/edit?usp=sharing<br />
- Meetings organized on as-needed basis.<br />
<br />
====Dark Matter====<br />
- Co-Coordinators: Vera Gluscevic (verag@ias.edu), and Dan Grin (dgrin@haverford.edu)<br />
- DM interactions meeting minutes: https://docs.google.com/document/d/1RxG07ebylnbXqSHFIIujBl6kO-olEUY9XPM4kyy0EXs/edit<br />
- Telecons on-needed basis; see [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
).<br />
<br />
====Galaxy Formation and Evolution====<br />
- Co-Coordinators: Marcelo Alvarez (marcelo.alvarez@berkeley.edu) and Colin Hill (jcolin.hill@gmail.com)<br />
- Meeting Notes: https://docs.google.com/document/d/11vsmV9fdDd29Kds2WmEh5MddEP7BAO16xMnoxV-MwZY/edit?usp=sharing<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Legacy Catalogs====<br />
- Co-Coordinators: Lindsey Bleem (lbleem@anl.gov) and Douglas Scott (dscott@phas.ubc.ca)<br />
- Meeting Notes: https://docs.google.com/document/d/169aZRZiqL3uJ2Eg9LY3ytAlR5UPCesJGp4lfVIAFWyA/edit?usp=sharing<br />
- Meeting Times: TBD; will be posted [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Science_Council&diff=10235Science Council2019-10-25T00:36:23Z<p>Wlwu: /* Low-ell BB */</p>
<hr />
<div>The Science Council consists of two co-Chairs and the co-Coordinators of four Analysis Working Groups (AWGs). We list the working groups here, together with information<br />
about their activities -- such as information about when they meet and links to meeting notes. The co-Chairs are Gil Holder (gil.holder@gmail.com) and Lloyd Knox (lknox@ucdavis.edu).<br />
<br />
===Overview===<br />
Our main focus now is "flowing down" the science to measurement requirements in preparation for CD-1/PDR. <br />
<br />
===Analysis Working Groups===<br />
<br />
====Low-ell BB==== <br />
- Co-Coordinators: Colin Bischoff (bischocn@ucmail.uc.edu) and Kimmy Wu (wlwu_at_kicp_dot_uchicago_dot_edu)<br />
- Meeting Notes: https://docs.google.com/document/d/1886yT1b6QDuWvsbAu5HmVv2Cl4pfH00YpK5Fv8dNzcM<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: [[Data_Challenges|r forecast sim set summary]]<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
- Forecast paper draft: [http://spud.spa.umn.edu/~pryke/s4_forecast_paper.pdf auto update pdf]<br />
<br />
====Maps2Cell====<br />
<br />
====Maps2OtherStats====<br />
<br />
====Sources====<br />
- Co-Coordinators: Joaquin Vieira (jvieira@illinois.edu) and Nick Battaglia (nbatta@astro.cornell.edu)<br />
- Meeting Notes: [https://docs.google.com/document/d/1rImHymDp3tGvd91k-d_bzD3060aejsyOcJ-h4TPKaxY/edit?usp=sharing[Link]]<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: N/A<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
- Forecast paper draft: Link<br />
<br />
===Historical Stuff below here===<br />
<br />
====Science White Papers====<br />
<br />
We are envisioning a series of SWP submitted by the January 2019 deadline. The papers will describe the entirety of science deliverable with observations in CMB frequency bands (loosely defined). The SWPs are common to the entire community; they will not discuss nor highlight any specific project. All interested members of the community are invited to participate in writing and endorsing any of these papers. <br />
<br />
SWP drafts that are ready for comment are available here:<br />
1) Neutrino Mass from Cosmology<br />
Link to the draft: http://dvorkin.physics.harvard.edu/Astro2020_Neutrino_Mass.pdf<br />
Contact person: Cora Dvorkin (cdvorkin@g.harvard.edu)<br />
2) Primordial non-Gaussianity <br />
Link to the draft:https://www.overleaf.com/read/bfsyyxfdqnvq<br />
Contact Person: Daan Meerburg (daanmeerburg@gmail.com) <br />
3) Dark Matter Physics with Cosmological Probes<br />
Link to the draft [PRELIMINARY, incomplete]: https://github.com/veragluscevic/Astro2020-DM-Cosmology<br />
Contact person: Vera Gluscevic (vera.gluscevic@gmail.com)<br />
4) Dark Energy<br />
Link to the draft: https://www.overleaf.com/read/phkpmjbjydwq<br />
Contact person: Anze Slosar (anze@bnl.gov)<br />
5) Features in the primordial power spectrum<br />
Link to the draft: https://www.overleaf.com/read/kyxzvmrbqpgy<br />
Contact person: Anze Slosar (anze@bnl.gov)<br />
6) Messengers from the Early Universe: Cosmic Neutrinos and Other Light Relics <br />
Link to the draft: https://www.overleaf.com/read/ybxqdqnhvtkm<br />
Contact person: Dan Green (drgreen@ucsd.edu)<br />
7) Testing gravity and particle physics with cosmic microwave background constraints on gravitational waves<br />
Link to the draft: https://www.overleaf.com/read/dsfnphrxfgbn<br />
Contact person: Sarah Shandera (shandera@gmail.com)<br />
8) Probing Feedback in Galaxy Formation with Millimeter-wave Observations<br />
Link to the draft: https://www.overleaf.com/read/ypcrxscjwnwr<br />
Contact people: Colin Hill (jch@ias.edu) and Nick Battaglia (nbatta@astro.cornell.edu)<br />
9) Reionization with the CMB <br />
Link to the draft: https://www.overleaf.com/read/bhdvxzqbprkf<br />
Contact people: Marcelo Alvarez (marcelo.alvarez@berkeley.edu) and Cora Dvorkin (cdvorkin@g.harvard.edu)<br />
<br />
<br />
The SWP are limited to 5 pages or fewer each, and we highly recommend that anyone wishing to contribute will read the short National Academies solicitation. Excerpting this key passage from the call may be helpful here:<br />
<br />
White papers should:<br />
- Identify scientific opportunities and compelling scientific themes for the coming decade, particularly those that have arisen from recent advances and accomplishments in astronomy and astrophysics;<br />
- Describe the scientific context of the importance of these opportunities, including connections to other parts of astronomy and astrophysics and, where appropriate, to the advancement of our broader scientific understanding;<br />
- While focusing on science, not specific missions or projects, describe and quantify the key advances in observation, measurement, theory, and/or computation necessary to realize the scientific opportunities within the decade 2020-2030 and beyond.<br />
<br />
To facilitate engagement and coordination of activities, we have created a wiki page (https://zzz.physics.umn.edu/decadal2020/doku.php?id=start) with a (non-comprehensive) list of potential science white papers with relevance to our community. Listed there are titles, and (mostly blank) fields for listing who is actively participating in the creation of the white paper, who has taken on a coordinating role, and links to relevant documentation for that white paper (github repos, online notes, etc.). <br />
<br />
The purpose of the wiki page is to give all of us a comprehensive view of science white paper activity of relevance to the CMB community, make it possible for would-be contributors to join existing efforts, and to allow any of us to spot gaps and work to fill them. The list of paper titles on the wiki now is just to get us started -- we expect it to evolve as, e.g., some topics get split into two or more different white papers, and new topics altogether are added. Anyone wishing to edit the wiki should contact Shaul Hanany (hanany@umn.edu) to get the appropriate permissions.<br />
<br />
====CMB-S4 Decadal Survey Report====<br />
<br />
Each AWG (with some exceptions) is charged with producing a 5-page section, the main elements of the Science Chapter of the DSR, on the science to be done with the CMB-S4 surveys. Our target for completion of a first draft of the DSR is November 2018. <br />
<br />
=====Draft Schedule for Production of Science Chapter sections=====<br />
<br />
- Friday, Sept 28: Long and rough draft completed<br />
- Friday, Oct 19: 5-page rough draft completed<br />
- Friday, Nov 3: cleaned-up draft ready to go out for review and comment<br />
- Wednesday, Nov 21: comments due back to AWGs<br />
- Friday, Dec 7: DSR chapter finalized<br />
- Dec 11 to 13: Internal DSR review in Washington, D.C. Each AWG should have one co-coordinator there<br />
<br />
===Former SC Analysis Working Groups===<br />
<br />
====Primordial Gravitational Waves==== <br />
- Co-Coordinators: Raphael Flauger (flauger@physics.utexas.edu) and Clem Pryke (pryke@physics.umn.edu)<br />
- Meeting Notes: https://docs.google.com/document/d/1886yT1b6QDuWvsbAu5HmVv2Cl4pfH00YpK5Fv8dNzcM<br />
- Shared logbook: [[Simulation_and_Forecasting_Logbook|Simulations and Forecasting Log Book]]<br />
- Data challenge summary pages: [[Data_Challenges|r forecast sim set summary]]<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
- Forecast paper draft: [http://spud.spa.umn.edu/~pryke/s4_forecast_paper.pdf[auto update pdf]]<br />
<br />
====Primordial Density Perturbations====<br />
- Co-Coordinators: Cora Dvorkin (cdvorkin@g.harvard.edu) & Daan Meerburg (daanmeerburg@gmail.com)<br />
<br />
- Telecons on-needed basis; see [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Light Relics====<br />
- Co-Coordinators: Daniel Green (drgreen@physics.ucsd.edu) and Joel Meyers (jmeyers@cita.utoronto.ca)<br />
- Forecasting Setup: [[Forecasting|Non-r Forecasting Page]]<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Neutrino Mass====<br />
- Co-Coordinators: Marilena Loverde (marilena.loverde@stonybrook.edu) and Blake Sherwin (sherwin@damtp.cam.ac.uk)<br />
- Meeting notes: https://cmb-s4.org/wiki/index.php/Neutrino_Mass_WG_Telecon<br />
- Call summaries: https://docs.google.com/document/d/1TWaU75wN1kqbYD1qkwzcJA9fZXGviKSezj3EnlP-ep8/edit?usp=sharing<br />
- Meeting times: will be posted; typically Tuesday 11am ET<br />
====Dark Energy ====<br />
- Co-Coordinators: Anze Slosar (anze@bnl.gov), and David Alonso (David.Alonso@physics.ox.ac.uk)<br />
- Meeting Notes: https://docs.google.com/document/d/13RTNgJNlWd098EPLnQrAAlstqDtyE850P9HnNFqCJZk/edit?usp=sharing<br />
- Meetings organized on as-needed basis.<br />
<br />
====Dark Matter====<br />
- Co-Coordinators: Vera Gluscevic (verag@ias.edu), and Dan Grin (dgrin@haverford.edu)<br />
- DM interactions meeting minutes: https://docs.google.com/document/d/1RxG07ebylnbXqSHFIIujBl6kO-olEUY9XPM4kyy0EXs/edit<br />
- Telecons on-needed basis; see [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
).<br />
<br />
====Galaxy Formation and Evolution====<br />
- Co-Coordinators: Marcelo Alvarez (marcelo.alvarez@berkeley.edu) and Colin Hill (jcolin.hill@gmail.com)<br />
- Meeting Notes: https://docs.google.com/document/d/11vsmV9fdDd29Kds2WmEh5MddEP7BAO16xMnoxV-MwZY/edit?usp=sharing<br />
- Meeting Times: Look for our meetings on the [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]<br />
<br />
====Legacy Catalogs====<br />
- Co-Coordinators: Lindsey Bleem (lbleem@anl.gov) and Douglas Scott (dscott@phas.ubc.ca)<br />
- Meeting Notes: https://docs.google.com/document/d/169aZRZiqL3uJ2Eg9LY3ytAlR5UPCesJGp4lfVIAFWyA/edit?usp=sharing<br />
- Meeting Times: TBD; will be posted [https://calendar.google.com/calendar/embed?src=t7l87lpt7g2t6a7ak4qh0t72qg%40group.calendar.google.com&ctz=America%2FLos_Angeles[CMB-S4 Google Calendar]]</div>Wlwuhttps://cmb-s4.uchicago.edu/wiki/index.php?title=UCSD-2019:_Cross-Cut:_Delensing&diff=10161UCSD-2019: Cross-Cut: Delensing2019-10-19T15:25:51Z<p>Wlwu: /* Notes */</p>
<hr />
<div>[https://cmb-s4.org/wiki/index.php/UCSD-2019:_Cosmology_with_CMB-S4#Agenda Link back to agenda]<br />
<br />
== Charge ==<br />
General charge to all parallels:<br />
<br />
We need to use the October collaboration meeting to advance our preparations for CD-1. Right away, we need to:<br />
* Identify key decisions that must be made (and justified) prior to CD-1,<br />
* Make progress on (or actually make) those decisions, <br />
* Lay out a timeline and process for making each decision, consistent with the post-decision work and internal reviews that will be needed to complete preparations for CD-1,<br />
* Ensure that those timelines and processes are understood and supported by the collaboration, and that we (together) believe we can follow them.<br />
<br />
Specific charge to this '''delensing cross-cut session''':<br />
* For the de-lensing LAT, what are the benefits and costs of variation in angular resolution (dish size) for legacy survey science goals? <br />
* What is minimum dish size / throughput needed for delensing? Would multiple smaller telescopes be better than one bigger one? (both r + Neff)<br />
* What are the effects of foregrounds on delensing (both for r and Neff)<br />
<br />
== Remote Attendance ==<br />
https://zoom.us/j/412621262?pwd=djdRc3YvVEZVWGVWMVJHNTZyemtKQT09<br />
<br />
== Agenda ==<br />
<br />
1) On-going work related to delensing (50 min - 1hr): <br />
* f_NL<br />
** Will Coulton on delensing for f_NL [[File: wcoulton.pdf]]<br />
* Foregrounds<br />
** Anton Baleato Lizancos on biases to delensing from CIB and EB estimator [[File: AntonBL_S4meeting.pdf]]<br />
** Marius Millea on incorporating foregrounds in Bayesian delensing [[File:Millea_cmbs4_sandiego_2019.pdf]]<br />
<!-- ** Alex van Engelen on Galactic foreground impacts --><br />
<!-- ** Kimmy Wu on CIB non-Gaussianity impacts on delensed bandpower covariances --><br />
* N_eff<br />
** Selim Hotinli on delensing for N_eff [[File:SelimHotinli_CMBS4_UCSD.pdf]]<br />
<br />
<br />
2) What are some of the questions that need answering for moving CMB-S4 to CD-1 readiness in delensing (1hr): <br />
* How map non-idealities impact delensing efficiency [[File: File.pdf]] (Toshiya Namikawa)<br />
* Discussion on instrumental systematics: [https://docs.google.com/presentation/d/19IHIesZkqBL7GajtV4NTVoIh1XBBCqXZnPXSkdwflTA/edit?usp=sharing need inputs from all!] (Kimmy Wu)<br />
* What inputs are needed in order to address session charges [https://docs.google.com/presentation/d/1E43NIMJR1wQAUhoe5BoDxI6dqrFkUoJUa6fxeibzj9c/edit?usp=sharing discussion]<br />
<br />
== Notes ==<br />
<br />
*Coulton: Delensing for fNL<br />
**Q: why is bias from using internal delensing smaller in bispectrum vs in power spectrum? <br />
**When using f(NL) = 0 sims, no bias; now there is ~10% bias <br />
**Q: Have you considered foregrounds?<br />
<br />
* Anton: EB estimator biases to delensing and Galactic dust biases in CIB to delensing<br />
** ell cuts in input B-modes are effective in removing biases.<br />
** Dust biases to delensing using CIB as tracers are small for SO requirements.<br />
<br />
*Toshiya: Anisotropic window + inhomogeneous noise effects<br />
**How much do you have to worry about missing modes in the delensing LAT? <br />
**Can S4 use the wide area LAT/SO LAT to fill out the delensing LAT missing modes due to scan patterns from the South Pole? We should not rely on external experiments for our mission critical tasks. <br />
**Lots of back and forth about how much these effects affect S4.<br />
<br />
*Marius: forward foreground modeling<br />
** Q: is this linear? Get all orders in phi, lensing operation is linear<br />
** Incorporate foregrounds in Bayesian framework first pass with poisson sources 1-halo term modeling<br />
** Q: does this work better than bias-hardening? Probably, if model is accurate. ES: in bias-hardening; you subtract the form of the point sources no matter what and incur a noise penalty though a more optimal step is to weight the bias and the increased variance. Here it's likely more optimal. <br />
** Q: How well do you have to know the statistics of the foregrounds? Need to be able to get the model correctly<br />
** Q: How to use this to constraint number counts for low-flux limits? have to choose dN/dS model in this procedure, or can sample dN/dS.<br />
** Q: How do you know the sims are right? The same question that everyone is trying to answer<br />
** Q: How does this bridge to more standard analysis? Can remove low ell B modes in input map, and generate phi instead of sample parameters.<br />
<br />
*Delensing for Neff - Selim <br />
**N_eff vs Yp degeneracy breaking when delensing is incorporated<br />
**TE gives the best constraints for N_eff<br />
**Q:Maybe gradient inversion is better for the intermediate scales?<br />
**When Yp not fixed to BBN consistency, sigma(N_eff) degrades to ~0.15? <br />
**How much, without marginalizing over Yp, does delensing help in sigma(N_eff)? Not very much. With Y_p, get ~30% improvement<br />
** This is an update to Joel’s forecast in which the iterative code includes all the other estimators (previously it's EB only).<br />
<br />
*Discussion regarding the session charges:<br />
** Do we weight the cluster/transient science goals the same as r science goal when designing the delensing LAT? Yes. So we have to do a joint optimization of sky/beam/freq bands for all three goals.<br />
** The sky coverage is likely driven by the SAT survey. The beam size is likely driven by cluster/transient needs. Frequency distribution needs more study from both the delensing side and the cluster side.<br />
** What is minimum dish size / throughput needed for delensing? See Fig 68 in DSR. Do we need more detailed studies?<br />
** Bonus question from Tom Crawford: "how much do you gain in sigma(r) by matching the degree-scale weight map vs. uniformly covering the full nonzero-weight region?”<br />
** Foreground impacts are discussed through the presentations.</div>Wlwu