https://cmb-s4.uchicago.edu/wiki/api.php?action=feedcontributions&user=Jcarron&feedformat=atomCMB-S4 wiki - User contributions [en]2022-05-23T23:25:44ZUser contributionsMediaWiki 1.34.2https://cmb-s4.uchicago.edu/wiki/index.php?title=Iterative_curved_sky_s06b_nofg_lensing_templates&diff=11233Iterative curved sky s06b nofg lensing templates2020-04-10T14:42:50Z<p>Jcarron: </p>
<hr />
<div>Julien Carron, April 10 2020<br />
<br />
This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the associated lensing templates.<br />
<br />
The lensing B-mode templates should remove about 90% of the lensing power in the central region and are available as alm fits files in <br />
<br />
<code>/global/cscratch1/sd/jcarron/share_cmbs4/06b_nofg_carron_100420</code><br />
<br />
The CMB likelihood model used to build the maps include:<br />
<br />
* Curved-sky geometry<br />
* An inhomogeneous noise model built from the hit map <code>/project/projectdirs/cmbs4/expt_xx/06b/rhits/n2048.fits </code> together with the empirically estimated central noise value<br />
* Exact deprojection of all B-modes from 2 to 200, to ensure these modes are not used to build the lensing template<br />
* Used are E-modes from 2 to 3000 and B-modes from 200 to 3000<br />
* The same mean-field is used for each iteration<br />
<br />
All sims used 12 iterations, though a few less would have been enough. <br />
<br />
Caveats:<br />
<br />
* The approximation to the mean-field leaves a residual sometimes visible at low-L near the edges of the patch. This is however restricted to low lensing multipoles, and the impact on the B-template quality is expected to be very small<br />
* The tracer could be improved by going to higher CMB lmax, with maybe ~5% gain at high-L ~ 2000, but again this will have a small impact only on the B-template<br />
<br />
<br />
A typical cross-correlation to the input lensing looks like this (calculated in a central region of 900 sq. deg. within the s06b patch), where the L-modes relevant to the B-power are centred on L~500.<br />
The correlation there goes from ~85% to ~96%<br />
<br />
[[File:Cs_MAP_rho.pdf|400px]]<br />
<br />
The B-templates are built remapping the estimated unlensed E-mode.<br />
<br />
Across the central 900 sq. deg. region, I estimate the residual B-power after template substraction to be about 0.1 (for something close to 0.3 for the QE, the starting point)<br />
<br />
[[File:Cs_resAL.png]]<br />
<br />
Obviously the quality of the tracer and template degrades closer to the edges<br />
<br />
<br />
[[File:Cs_resB.png|1600px]]</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Iterative_curved_sky_s06b_nofg_lensing_templates&diff=11232Iterative curved sky s06b nofg lensing templates2020-04-10T14:26:08Z<p>Jcarron: </p>
<hr />
<div>Julien Carron, April 10 2020<br />
<br />
This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the associated lensing templates.<br />
<br />
The lensing B-mode templates should remove about 90% of the lensing power in the central region and are available as alm fits files in <br />
<br />
<code>/global/cscratch1/sd/jcarron/06b_nofg_carron_100420</code><br />
<br />
The CMB likelihood model used to build the maps include:<br />
<br />
* Curved-sky geometry<br />
* An inhomogeneous noise model built from the hit map <code>/project/projectdirs/cmbs4/expt_xx/06b/rhits/n2048.fits </code> together with the empirically estimated central noise value<br />
* Exact deprojection of all B-modes from 2 to 200, to ensure these modes are not used to build the lensing template<br />
* Used are E-modes from 2 to 3000 and B-modes from 200 to 3000<br />
* The same mean-field is used for each iteration<br />
<br />
All sims used 12 iterations, though a few less would have been enough. <br />
<br />
Caveats:<br />
<br />
* The approximation to the mean-field leaves a residual sometimes visible at low-L near the edges of the patch. This is however restricted to low lensing multipoles, and the impact on the B-template quality is expected to be very small<br />
* The tracer could be improved by going to higher CMB lmax, with maybe ~5% gain at high-L ~ 2000, but again this will have a small impact only on the B-template<br />
<br />
<br />
A typical cross-correlation to the input lensing looks like this (calculated in a central region of 900 sq. deg. within the s06b patch), where the L-modes relevant to the B-power are centred on L~500.<br />
The correlation there goes from ~85% to ~96%<br />
<br />
[[File:Cs_MAP_rho.pdf|400px]]<br />
<br />
The B-templates are built remapping the estimated unlensed E-mode.<br />
<br />
Across the central 900 sq. deg. region, I estimate the residual B-power after template substraction to be about 0.1 (for something close to 0.3 for the QE, the starting point)<br />
<br />
[[File:Cs_resAL.png]]<br />
<br />
Obviously the quality of the tracer and template degrades closer to the edges<br />
<br />
<br />
[[File:Cs_resB.png|1600px]]</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Iterative_curved_sky_s06b_nofg_lensing_templates&diff=11231Iterative curved sky s06b nofg lensing templates2020-04-10T14:25:36Z<p>Jcarron: </p>
<hr />
<div>Julien Carron, April 10 2020<br />
<br />
This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the associated lensing templates.<br />
<br />
The lensing B-mode templates should remove about 90% of the lensing power in the central region and are available as alm fits files in <br />
<br />
<code>/global/cscratch1/sd/jcarron/06b_nofg_carron_100420</code><br />
<br />
The CMB likelihood model used to build the maps include:<br />
<br />
* Curved-sky geometry<br />
* An inhomogeneous noise model built from the hit map <code>/project/projectdirs/cmbs4/expt_xx/06b/rhits/n2048.fits </code> together with the empirically estimated central noise value<br />
* Exact deprojection of all B-modes from 2 to 200, to ensure these modes are not used to build the lensing template<br />
* Used are E-modes from 2 to 3000 and B-modes from 200 to 3000<br />
* The same mean-field is used for each iteration<br />
<br />
All sims used 12 iterations, though a few less would have been enough. <br />
<br />
Caveats:<br />
<br />
* The approximation to the mean-field leaves a residual sometimes visible at low-L near the edges of the patch. This is however restricted to low lensing multipoles, and the impact on the B-template quality is expected to be very small<br />
* The tracer could be improved by going to higher CMB lmax, with maybe ~5% gain at high-L ~ 2000, but again this will have a small impact only on the B-template<br />
<br />
<br />
A typical cross-correlation to the input lensing looks like this (calculated in a central region of 900 sq. deg. within), where the L-modes relevant to the B-power are centred on L~500.<br />
The correlation there goes from ~85% to ~96%<br />
<br />
[[File:Cs_MAP_rho.pdf|400px]]<br />
<br />
The B-templates are built remapping the estimated unlensed E-mode<br />
<br />
Across the central 900 sq. deg. region, I estimate the residual B-power after template substraction to be about 0.1 (for something close to 0.3 for the QE, the starting point)<br />
<br />
[[File:Cs_resAL.png]]<br />
<br />
Obviously the quality of the tracer and template degrades closer to the edges<br />
<br />
<br />
[[File:Cs_resB.png|1600px]]</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Iterative_curved_sky_s06b_nofg_lensing_templates&diff=11230Iterative curved sky s06b nofg lensing templates2020-04-10T14:21:06Z<p>Jcarron: </p>
<hr />
<div>Julien Carron, April 10 2020<br />
<br />
This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the associated lensing templates.<br />
<br />
The lensing B-mode templates should remove about 90% of the lensing power in the central region and are available as alm fits files in <br />
<br />
<code>/global/cscratch1/sd/jcarron/06b_nofg_carron_100420</code><br />
<br />
The CMB likelihood model used to build the maps include:<br />
<br />
* Curved-sky geometry<br />
* An inhomogeneous noise model built from the hit map <code>/project/projectdirs/cmbs4/expt_xx/06b/rhits/n2048.fits </code> together with the empirically estimated central noise value<br />
* Exact deprojection of all B-modes from 2 to 200, to ensure these modes are not used to build the lensing template<br />
* Used are E-modes from 2 to 3000 and B-modes from 200 to 3000<br />
* The same mean-field is used for each iteration<br />
<br />
All sims used 12 iterations, though a few less would have been enough. Caveats:<br />
<br />
* The approximation to the mean-field leaves a residual sometimes visible at low-L near the edges of the patch. This is however restricted to low lensing multipoles, and the impact on the B-template quality is expected to be very small<br />
* The tracer could be improved by going to higher CMB lmax, with maybe ~5% gain at high-L ~ 2000, but again this will have a small impact only on the B-template<br />
<br />
<br />
A typical cross-correlation to the input lensing looks like this (calculated in a central region of 900 sq. deg. within), where the L-modes relevant to the B-power are centred on L~500.<br />
The correlation there goes from ~85% to ~96%<br />
<br />
[[File:Cs_MAP_rho.pdf|400px]]<br />
<br />
The B-templates are built remapping the estimated unlensed E-mode<br />
<br />
Across the central 900 sq. deg. region, I estimate the residual B-power after template substraction to be about 0.1 (for something close to 0.3 for the QE, the starting point)<br />
<br />
[[File:Cs_resAL.png]]<br />
<br />
Obviously the quality of the tracer and template degrades closer to the edges<br />
<br />
<br />
[[File:Cs_resB.png|1600px]]</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Iterative_curved_sky_s06b_nofg_lensing_templates&diff=11229Iterative curved sky s06b nofg lensing templates2020-04-10T14:09:04Z<p>Jcarron: </p>
<hr />
<div>Julien Carron, April 10 2020<br />
<br />
This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the associated lensing templates.<br />
<br />
<br />
The CMB likelihood model used to build the maps include:<br />
<br />
* Curved-sky geometry<br />
* An inhomogeneous noise model built from the hit map <code>/project/projectdirs/cmbs4/expt_xx/06b/rhits/n2048.fits </code> together with the empirically estimated central noise value<br />
* Exact deprojection of all B-modes from 2 to 200, to ensure these modes are not used to build the lensing template<br />
* Used are E-modes from 2 to 3000 and B-modes from 200 to 3000<br />
* The same mean-field is used for each iteration<br />
<br />
All sims used 12 iterations, though a few less would have been enough. Caveats:<br />
<br />
* The approximation to the mean-field leaves a residual sometimes visible at low-L near the edges of the patch. This is however restricted to low lensing multipoles, and the impact on the B-template quality is expected to be very small<br />
* The tracer could be improved by going to higher CMB lmax, with maybe ~5% gain at high-L ~ 2000, but again this will have a small impact only on the B-template<br />
<br />
<br />
A typical cross-correlation to the input lensing looks like this (calculated in a central region of 900 sq. deg. within), where the L-modes relevant to the B-power are centred on L~500.<br />
The correlation there goes from ~85% to ~96%<br />
<br />
[[File:Cs_MAP_rho.pdf|400px]]<br />
<br />
The B-templates are built remapping the estimated unlensed E-mode<br />
<br />
Across the central 900 sq. deg. region, I estimate the residual B-power after template substraction to be about 0.1 (for something close to 0.3 for the QE, the starting point)<br />
<br />
[[File:Cs_resAL.png]]<br />
<br />
Obviously the quality of the tracer and template degrades closer to the edges<br />
<br />
<br />
[[File:Cs_resB.png|1600px]]</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Cs_resB.png&diff=11228File:Cs resB.png2020-04-10T14:06:25Z<p>Jcarron: lensing B template for curved-sky MAP estimate</p>
<hr />
<div>lensing B template for curved-sky MAP estimate</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Iterative_curved_sky_s06b_nofg_lensing_templates&diff=11227Iterative curved sky s06b nofg lensing templates2020-04-10T14:05:55Z<p>Jcarron: </p>
<hr />
<div>Julien Carron, April 10 2020<br />
<br />
This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the associated lensing templates.<br />
<br />
<br />
The CMB likelihood model used to build the maps include:<br />
<br />
* Curved-sky geometry<br />
* An inhomogeneous noise model built from the hit map <code>/project/projectdirs/cmbs4/expt_xx/06b/rhits/n2048.fits </code> together with the empirically estimated central noise value<br />
* Exact deprojection of all B-modes from 2 to 200, to ensure these modes are not used to build the lensing template<br />
* Used are E-modes from 2 to 3000 and B-modes from 200 to 3000<br />
* The same mean-field is used for each iteration<br />
<br />
All sims used 12 iterations, though a few less would have been enough. Caveats:<br />
<br />
* The approximation to the mean-field leaves a residual sometimes visible at low-L near the edges of the patch. This is however restricted to low lensing multipoles, and the impact on the B-template quality is expected to be very small<br />
* The tracer could be improved by going to higher CMB lmax, with maybe ~5% gain at high-L ~ 2000, but again this will have a small impact only on the B-template<br />
<br />
<br />
A typical cross-correlation to the input lensing looks like this (calculated in a central region of 900 sq. deg. within), where the L-modes relevant to the B-power are centred on L~500.<br />
The correlation there goes from ~85% to ~96%<br />
<br />
[[File:Cs_MAP_rho.pdf|400px]]<br />
<br />
The B-templates are built remapping the estimated unlensed E-mode<br />
<br />
Across the central 900 sq. deg. region, I estimate the residual B-power after template substraction to be about 0.1 (for something close to 0.3 for the QE, the starting point)<br />
<br />
[[File:Cs_resAL.png]]<br />
<br />
Obviously the quality of the tracer and template degrades closer to the edges<br />
<br />
<br />
[[File:Cs_resB.png]]</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Iterative_curved_sky_s06b_nofg_lensing_templates&diff=11226Iterative curved sky s06b nofg lensing templates2020-04-10T13:51:25Z<p>Jcarron: </p>
<hr />
<div>Julien Carron, April 10 2020<br />
<br />
This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the associated lensing templates.<br />
<br />
<br />
The CMB likelihood model used to build the maps include:<br />
<br />
* Curved-sky geometry<br />
* An inhomogeneous noise model built from the hit map <code>/project/projectdirs/cmbs4/expt_xx/06b/rhits/n2048.fits </code> together with the empirically estimated central noise value<br />
* Exact deprojection of all B-modes from 2 to 200, to ensure these modes are not used to build the lensing template<br />
* Used are E-modes from 2 to 3000 and B-modes from 200 to 3000<br />
* The same mean-field is used for each iteration<br />
<br />
All sims used 12 iterations, though a few less would have been enough. Caveats:<br />
<br />
* The approximation to the mean-field leaves a residual sometimes visible at low-L near the edges of the patch. This is however restricted to low lensing multipoles, and the impact on the B-template quality is expected to be very small<br />
* The tracer could be improved by going to higher CMB lmax, with maybe ~5% gain at high-L ~ 2000, but again this will have a small impact only on the B-template<br />
<br />
<br />
A typical cross-correlation to the input lensing looks like this (calculated in a central region of 900 sq. deg. within), where the L-modes relevant to the B-power are centred on L~500.<br />
The correlation there goes from ~85% to ~96%<br />
<br />
[[File:Cs_MAP_rho.pdf|400px]]<br />
<br />
The B-templates are built remapping the estimated unlensed E-mode<br />
<br />
Across the central 900 sq. deg. region, I estimate the residual B-power after template substraction to be about 0.1 (for something close to 0.3 for the QE, the starting point)<br />
<br />
[[File:Cs_resAL.png]]<br />
<br />
Obviously the quality of the tracer and template degrades closer to the edges</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Iterative_curved_sky_s06b_nofg_lensing_templates&diff=11225Iterative curved sky s06b nofg lensing templates2020-04-10T13:40:14Z<p>Jcarron: </p>
<hr />
<div>Julien Carron, April 10 2020<br />
<br />
This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the associated lensing templates.<br />
<br />
The CMB likelihood model used to build the maps include:<br />
<br />
* Curved-sky geometry<br />
* An inhomogeneous noise model built from the hit map <code>/project/projectdirs/cmbs4/expt_xx/06b/rhits/n2048.fits </code> together with the empirically estimated central noise value<br />
* Exact deprojection of all B-modes from 2 to 200, to ensure these modes are not used to build the lensing template<br />
* Used are E-modes from 2 to 3000 and B-modes from 200 to 3000<br />
* The same mean-field is used for each iteration<br />
<br />
The approximation to the mean-field leaves a residual sometimes visible near the edges of the patch. This is however restricted to low lensing multipoles, and does not affect the B-template quality.<br />
<br />
A typical cross-correlation to the input lensing looks like this (calculated in a central region of 900 sq. deg. within), where the L-modes relevant to the B-power are centred on L~500.<br />
The correlation there goes from ~85% to ~96%<br />
<br />
[[File:Cs_MAP_rho.pdf|400px]]<br />
<br />
The B-templates are built remapping the estimated unlensed E-mode<br />
<br />
Across the central 900 sq. deg. region, I estimate the residual B-power after template substraction to be about 0.1 (for something close to 0.3 for the QE, the starting point)<br />
<br />
[[File:Cs_resAL.png]]<br />
<br />
Obviously the quality of the tracer and template degrades closer to the edges</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Iterative_curved_sky_s06b_nofg_lensing_templates&diff=11224Iterative curved sky s06b nofg lensing templates2020-04-10T13:35:04Z<p>Jcarron: </p>
<hr />
<div>Julien Carron, April 10 2020<br />
<br />
This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the associated lensing templates.<br />
<br />
The CMB likelihood model used to build the maps include:<br />
<br />
* Curved-sky geometry<br />
* An inhomogeneous noise model built from the hit map <code>/project/projectdirs/cmbs4/expt_xx/06b/rhits/n2048.fits </code> together with the empirically estimated central noise value<br />
* Exact deprojection of all B-modes from 2 to 200, to ensure these modes are not used to build the lensing template<br />
* Used are E-modes from 2 to 3000 and B-modes from 200 to 3000<br />
* The same mean-field is used for each iteration<br />
<br />
The approximation to the mean-field leaves a residual sometimes visible near the edges of the patch. This is however restricted to low lensing multipoles, and does not affect the B-template quality.<br />
<br />
A typical cross-correlation to the input lensing looks like this (calculated in the central region of the patch), where the L-modes relevant to the B-power are centred on L~500.<br />
The correlation there goes from ~85% to ~96%<br />
<br />
[[File:Cs_MAP_rho.pdf|400px]]<br />
<br />
The B-templates are built remapping the estimated unlensed E-mode<br />
<br />
Across the central region, I estimate the residual B-power after template substraction to be about 0.1 (for something close to 0.3 for the QE, the starting point)<br />
<br />
[[File:Cs_resAL.png]]</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Cs_MAP_rho.pdf&diff=11223File:Cs MAP rho.pdf2020-04-10T13:31:37Z<p>Jcarron: Jcarron uploaded a new version of File:Cs MAP rho.pdf</p>
<hr />
<div>Cross-correlation of curved-sky iterative rec. on s06b nofg to the input lensing map</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Iterative_curved_sky_s06b_nofg_lensing_templates&diff=11222Iterative curved sky s06b nofg lensing templates2020-04-10T13:31:22Z<p>Jcarron: </p>
<hr />
<div>Julien Carron, April 10 2020<br />
<br />
This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the associated lensing template.<br />
<br />
The CMB likelihood model used to build the maps include:<br />
<br />
* Curved-sky geometry<br />
* An inhomogeneous noise model built from the hit map <code>/project/projectdirs/cmbs4/expt_xx/06b/rhits/n2048.fits </code> together with the empirically estimated central noise value<br />
* Exact deprojection of all B-modes from 2 to 200, to ensure these modes are not used to build the lensing template<br />
* Used are E-modes from 2 to 3000 and B-modes from 200 to 3000<br />
* The same mean-field is used for each iteration<br />
<br />
The approximation to the mean-field leaves a residual sometimes visible near the edges of the patch. This is however restricted to low lensing multipoles, and does not affect the B-template quality.<br />
<br />
A typical cross-correlation to the input lensing looks like this (calculated in the central region of the patch)<br />
<br />
[[File:Cs_MAP_rho.pdf]]<br />
<br />
The B-templates are built remapping the estimated unlensed E-mode<br />
<br />
Across the central region, I estimate the residual B-power after template substraction to be about 0.1 (for something close to 0.3 for the QE, the starting point)<br />
<br />
[[File:Cs_resAL.png]]</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Iterative_curved_sky_s06b_nofg_lensing_templates&diff=11221Iterative curved sky s06b nofg lensing templates2020-04-10T13:31:10Z<p>Jcarron: </p>
<hr />
<div>Julien Carron, April 10 2020<br />
<br />
This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the associated lensing template.<br />
<br />
The CMB likelihood model used to build the maps include:<br />
<br />
* Curved-sky geometry<br />
* An inhomogeneous noise model built from the hit map <code>/project/projectdirs/cmbs4/expt_xx/06b/rhits/n2048.fits </code> together with the empirically estimated central noise value<br />
* Exact deprojection of all B-modes from 2 to 200, to ensure these modes are not used to build the lensing template<br />
* Used are E-modes from 2 to 3000 and B-modes from 200 to 3000<br />
* The same mean-field is used for each iteration<br />
<br />
The approximation to the mean-field leaves a residual sometimes visible near the edges of the patch. This is however restricted to low lensing multipoles, and does not affect the B-template quality.<br />
<br />
A typical cross-correlation to the input lensing looks like this (calculated in the central region of the patch)<br />
<br />
[[File:Cs_MAP_rho.pdf]]<br />
<br />
The B-templates are built remapping the estimated unlensed E-mode<br />
<br />
Across the central region, I estimate the residual B-power after template substraction to be about 0.1 (for something close to 0.3 for the QE, the starting point)<br />
<br />
[[File:Cs_resAL.png]]</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Cs_resAL.png&diff=11220File:Cs resAL.png2020-04-10T13:27:40Z<p>Jcarron: </p>
<hr />
<div></div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Iterative_curved_sky_s06b_nofg_lensing_templates&diff=11219Iterative curved sky s06b nofg lensing templates2020-04-10T13:27:28Z<p>Jcarron: </p>
<hr />
<div>Julien Carron, April 10 2020<br />
<br />
This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the associated lensing template.<br />
<br />
The CMB likelihood model used to build the maps include:<br />
<br />
* Curved-sky geometry<br />
* An inhomogeneous noise model built from the hit map <code>/project/projectdirs/cmbs4/expt_xx/06b/rhits/n2048.fits </code> together with the empirically estimated central noise value<br />
* Exact deprojection of all B-modes from 2 to 200, to ensure these modes are not used to build the lensing template<br />
* Used are E-modes from 2 to 3000 and B-modes from 200 to 3000<br />
* The same mean-field is used for each iteration<br />
<br />
The approximation to the mean-field leaves a residual sometimes visible near the edges of the patch. This is however restricted to low lensing multipoles, and does not affect the B-template quality.<br />
<br />
A typical cross-correlation to the input lensing looks like this (calculated in the central region of the patch)<br />
<br />
[[File:Cs_MAP_rho.pdf]]<br />
<br />
The B-templates are built remapping the estimated unlensed E-mode<br />
<br />
Across the central region, I estimate the residual B-power after template substraction to be about 0.1<br />
<br />
[[File:Cs_resAL.png]]</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Iterative_curved_sky_s06b_nofg_lensing_templates&diff=11218Iterative curved sky s06b nofg lensing templates2020-04-10T13:20:44Z<p>Jcarron: </p>
<hr />
<div>Julien Carron, April 10 2020<br />
<br />
This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the associated lensing template.<br />
<br />
The CMB likelihood model used to build the maps include:<br />
<br />
* Curved-sky geometry<br />
* An inhomogeneous noise model built from the hit map <code>/project/projectdirs/cmbs4/expt_xx/06b/rhits/n2048.fits </code> together with the empirically estimated central noise value<br />
* Exact deprojection of all B-modes from 2 to 200, to ensure these modes are not used to build the lensing template<br />
* Used are E-modes from 2 to 3000 and B-modes from 200 to 3000<br />
* The same mean-field is used for each iteration<br />
<br />
The approximation to the mean-field leaves a residual sometimes visible near the edges of the patch. This is however restricted to low lensing multipoles, and does not affect the B-template quality.<br />
<br />
A typical cross-correlation to the input lensing looks like this (calculated in the central region of the patch)<br />
<br />
[[File:Cs_MAP_rho.pdf]]<br />
<br />
The B-templates are built remapping the estimated unlensed E-mode<br />
<br />
Across the central region, I estimate the residual B-power after template substraction to be about 0.1</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Iterative_curved_sky_s06b_nofg_lensing_templates&diff=11217Iterative curved sky s06b nofg lensing templates2020-04-10T13:15:49Z<p>Jcarron: </p>
<hr />
<div>Julien Carron, April 10 2020<br />
<br />
This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the associated lensing template.<br />
<br />
The CMB likelihood model used to build the maps include:<br />
<br />
* Curved-sky geometry<br />
* An inhomogeneous noise model built from the hit map <code>/project/projectdirs/cmbs4/expt_xx/06b/rhits/n2048.fits </code> together with the empirically estimated central noise value<br />
* Exact deprojection of all B-modes from 2 to 200, to ensure these modes are not used to build the lensing template<br />
* Used are E-modes from 2 to 3000 and B-modes from 200 to 3000<br />
* The same mean-field is used for each iteration<br />
<br />
The approximation to the mean-field leaves a residual sometimes visible near the edges of the patch. This is however restricted to low lensing multipoles, and does not affect the B-template quality.</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Iterative_curved_sky_s06b_nofg_lensing_templates&diff=11216Iterative curved sky s06b nofg lensing templates2020-04-10T13:13:35Z<p>Jcarron: </p>
<hr />
<div>Julien Carron, April 10 2020<br />
<br />
This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the associated lensing template.<br />
<br />
The CMB likelihood model used to build the maps include:<br />
<br />
* Curved-sky geometry<br />
* An inhomogeneous noise model built from the hit map <code>/project/projectdirs/cmbs4/expt_xx/06b/rhits/n2048.fits </code> together with the empirically estimated central noise value<br />
* Exact deprojection of all B-modes from 2 to 200, to ensure these modes are not used to build the lensing template<br />
* Used are E-modes from 2 to 3000 and B-modes from 200 to 3000</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Iterative_curved_sky_s06b_nofg_lensing_templates&diff=11215Iterative curved sky s06b nofg lensing templates2020-04-10T13:10:25Z<p>Jcarron: Created page with "Julien Carron, April 10 2020 This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the asso..."</p>
<hr />
<div>Julien Carron, April 10 2020<br />
<br />
This pages describes the 100 iterative (maximum a posteriori, 'MAP') lensing map built from the s06b simulations without foreground, and the associated lensing template.</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Cs_MAP_rho.pdf&diff=11214File:Cs MAP rho.pdf2020-04-10T13:08:31Z<p>Jcarron: Cross-correlation of curved-sky iterative rec. on s06b nofg to the input lensing map</p>
<hr />
<div>Cross-correlation of curved-sky iterative rec. on s06b nofg to the input lensing map</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Cmbs4_iterativelensing.pdf&diff=10928File:Cmbs4 iterativelensing.pdf2020-03-31T15:43:56Z<p>Jcarron: Jcarron uploaded a new version of File:Cmbs4 iterativelensing.pdf</p>
<hr />
<div>slides for curved-sky iterative delensing s06b spring meeting</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Cmbs4_iterativelensing.pdf&diff=10925File:Cmbs4 iterativelensing.pdf2020-03-31T15:40:01Z<p>Jcarron: slides for curved-sky iterative delensing s06b spring meeting</p>
<hr />
<div>slides for curved-sky iterative delensing s06b spring meeting</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=LBNL-2020:_Low-ell_BB&diff=10924LBNL-2020: Low-ell BB2020-03-31T15:38:15Z<p>Jcarron: /* 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] [https://docs.google.com/presentation/d/1bI90NApMEv4W_suqxp9a89wMH_KEdfu0qRKs9S1GmLY/edit#slide=id.g726e0d289c_0_65 slides]<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][[: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 />
** 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] [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>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=LBNL-2020:_Low-ell_BB&diff=10923LBNL-2020: Low-ell BB2020-03-31T15:37:29Z<p>Jcarron: /* 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] [https://docs.google.com/presentation/d/1bI90NApMEv4W_suqxp9a89wMH_KEdfu0qRKs9S1GmLY/edit#slide=id.g726e0d289c_0_65 slides]<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][[: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 />
** 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] [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>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=R_Forecasting_Logbook&diff=7797R Forecasting Logbook2018-09-30T21:21:43Z<p>Jcarron: /* 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 r 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 />
== Telecon Notes ==<br />
<br />
[https://docs.google.com/document/d/1886yT1b6QDuWvsbAu5HmVv2Cl4pfH00YpK5Fv8dNzcM/edit?usp=sharing Telecon notes for r-forecasting]<br />
<br />
== Logbook Entries (reverse chronological) ==<br />
<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 August 27''': [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''': [[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://users.physics.harvard.edu/~buza/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://users.physics.harvard.edu/~buza/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://users.physics.harvard.edu/~buza/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://users.physics.harvard.edu/~buza/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://users.physics.harvard.edu/~buza/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://users.physics.harvard.edu/~buza/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://users.physics.harvard.edu/~buza/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>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Ready_for_delensing_use_lensing_maps_02.00&diff=7796Ready for delensing use lensing maps 02.002018-09-30T21:20:04Z<p>Jcarron: </p>
<hr />
<div>J. Carron Sept 30 2018. <br />
<br />
This page describe the 300 lensing tracers maps (healpy alm fits files, with lmax=3000) available at<br />
<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925/ready_for_delensing_use<br />
<br />
These maps were directly built from the quadratic estimated raw lensing maps [[Lensing reconstructions 02.00]], after Wiener-filtering and mean-field (contamination of the lensing estimate by mask and noise anisotropies) subtraction, as described below. They can be used as is for delensing. The lensing reconstructions were themselves built from this data: [[Sim map sets to demonstrate "real delensing" (02.00_and_02.09)]]<br />
<br />
There are 3 types of maps:<br />
<br />
* sim_ptt_????_lmax3000.fits<br />
<br />
built from temperature data only, with ???? from 0000 to 0099<br />
<br />
* sim_p_p_????_lmax3000.fits<br />
<br />
built from polarization data only,<br />
<br />
* sim_p_????_lmax3000.fits<br />
<br />
built from combination and temperature and polarization data (MV).<br />
<br />
=== Wiener-filter ===<br />
<br />
<br />
The Wiener-filter C / C + N0 is isotropic, and is given by the last column of the files<br />
<br />
clwf_{ptt, p_p, p}.dat<br />
<br />
in the same folder. The noise spectra are obtained empirically, by taking (twice) the spectrum of a lensing reconstruction where the two legs of the quadratic estimator are independent, and averaging over 100 such reconstructions.<br />
<br />
=== Mean-fields ===<br />
<br />
To subtract the mean-field from one lensing estimate, we have subtracted the average of the lensing reconstructions, excluding that very estimate (resulting in the average of 99 lensing maps). This adds a small, ~1% contribution to the reconstruction noise which is neglected in the Wiener-filter. This procedure also causes the simulations to be not exactly independent anymore, even if this is a small effect.</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Ready_for_delensing_use_lensing_maps_02.00&diff=7795Ready for delensing use lensing maps 02.002018-09-30T21:17:28Z<p>Jcarron: </p>
<hr />
<div>J. Carron Sept 30 2018. <br />
<br />
This page describe the 300 lensing tracers maps (healpy alm fits files, with lmax=3000) available at<br />
<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925/ready_for_delensing_use<br />
<br />
These maps were directly built from the quadratic estimated raw lensing maps [[Lensing reconstructions 02.00]], after Wiener-filtering and mean-field (contamination of the lensing estimate by mask and noise anisotropies) subtraction, as described below. They can be used as is for delensing.<br />
<br />
There are 3 types of maps:<br />
<br />
* sim_ptt_????_lmax3000.fits<br />
<br />
built from temperature data only, with ???? from 0000 to 0099<br />
<br />
* sim_p_p_????_lmax3000.fits<br />
<br />
built from polarization data only,<br />
<br />
* sim_p_????_lmax3000.fits<br />
<br />
built from combination and temperature and polarization data.<br />
<br />
=== Wiener-filter ===<br />
<br />
<br />
The Wiener-filter C / C + N0 is isotropic, and is given by the last column of the files<br />
<br />
clwf_{ptt, p_p, p}.dat<br />
<br />
in the same folder. The noise spectra are obtained empirically, by taking (twice) the spectrum of a lensing reconstruction where the two legs of the quadratic estimator are independent, and averaging over 100 such reconstructions.<br />
<br />
=== Mean-fields ===<br />
<br />
To subtract the mean-field from one lensing estimate, we have subtracted the average of the lensing reconstructions, excluding that very estimate (resulting in the average of 99 lensing maps). This adds a small, ~1% contribution to the reconstruction noise which is neglected in the Wiener-filter. This procedure also causes the simulations to be not exactly independent anymore, even if this is a small effect.</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Ready_for_delensing_use_lensing_maps_02.00&diff=7794Ready for delensing use lensing maps 02.002018-09-30T21:13:03Z<p>Jcarron: /* Wiener-filter */</p>
<hr />
<div>J. Carron Sept 30 2018. <br />
<br />
This page describe the 300 lensing tracers maps (healpy alm fits files, with lmax=3000) available at<br />
<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925/ready_for_delensing_use<br />
<br />
These maps were directly built from the quadratic estimated raw lensing maps [[Lensing reconstructions 02.00]], after Wiener-filtering and mean-field subtraction, as described below. They can be used as is for delensing.<br />
<br />
There are 3 types of maps:<br />
<br />
* sim_ptt_????_lmax3000.fits<br />
<br />
built from temperature data only, with ???? from 0000 to 0099<br />
<br />
* sim_p_p_????_lmax3000.fits<br />
<br />
built from polarization data only,<br />
<br />
* sim_p_????_lmax3000.fits<br />
<br />
built from combination and temperature and polarization data.<br />
<br />
=== Wiener-filter ===<br />
<br />
The Wiener-filter C / C + N0 is isotropic, and is given by the last column of the files<br />
<br />
clwf_{ptt, p_p, p}.dat<br />
<br />
in the same folder. The noise spectra are obtained empirically, by taking (twice) the spectrum of a lensing reconstruction where the two legs of the quadratic estimator are independent, and averaging over 100 such reconstructions.</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Ready_for_delensing_use_lensing_maps_02.00&diff=7793Ready for delensing use lensing maps 02.002018-09-30T21:11:01Z<p>Jcarron: Created page with "J. Carron Sept 30 2018. This page describe the 300 lensing tracers maps (healpy alm fits files, with lmax=3000) available at /project/projectdirs/cmbs4/reanalysis/phi_..."</p>
<hr />
<div>J. Carron Sept 30 2018. <br />
<br />
This page describe the 300 lensing tracers maps (healpy alm fits files, with lmax=3000) available at<br />
<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925/ready_for_delensing_use<br />
<br />
These maps were directly built from the quadratic estimated raw lensing maps [[Lensing reconstructions 02.00]], after Wiener-filtering and mean-field subtraction, as described below. They can be used as is for delensing.<br />
<br />
There are 3 types of maps:<br />
<br />
* sim_ptt_????_lmax3000.fits<br />
<br />
built from temperature data only, with ???? from 0000 to 0099<br />
<br />
* sim_p_p_????_lmax3000.fits<br />
<br />
built from polarization data only,<br />
<br />
* sim_p_????_lmax3000.fits<br />
<br />
built from combination and temperature and polarization data.<br />
<br />
=== Wiener-filter ===</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Lensing_reconstructions_02.00&diff=7792Lensing reconstructions 02.002018-09-30T20:33:10Z<p>Jcarron: </p>
<hr />
<div>J.Carron 27 Sept. 2018<br />
<br />
This page documents the 600 lensing maps (healpy alm fits files, lmax=3000, temperature, polarization and MV reconstruction) available at <br />
<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925<br />
<br />
These lensing maps were built from these CMB + noise + foreground maps (described at [[Sim map sets to demonstrate "real_delensing" (02.00 and 02.09)]]):<br />
<br />
/project/projectdirs/cmbs4/data_xx.yy/02.00/cmbs4_02p00_comb_f145_b04_ellmin30_map_2048_mc_{0000 to 0099}.fits<br />
<br />
The lensing maps have the usual quadratic esimator normalization (unbiased with respect to the input lensing, to a good approximation, with a lot of noise on small scales), and have contribution in them from the mask and noise anisotropies (mean-field). Maps further processed which are ready to use for delensing are described in [[Ready for delensing use lensing maps 02.00]]<br />
<br />
For illustration, the temperature (TT), polarization (PP) and Minimum Variance (MV) Wiener-filtered displacement reconstructions, together with the input, for realization 99:<br />
<br />
[[File:recmaps_cmbs4_apo.png]]<br />
<br />
There are 6 type of lensing maps, labeled <br />
<br />
*sim_ptt_????_lmax3000.fits <br />
lensing map from temperature only, simulation index ???? 0000 to 0099<br />
*sim_p_p_????_lmax3000.fits<br />
lensing map from polarization only<br />
*sim_p_????_lmax3000.fits<br />
lensing map from temperature and polarization (MV)<br />
*sim_xtt_????_lmax3000.fits<br />
lensing curl map from temperature, useful for null tests<br />
*sim_x_p_????_lmax3000.fits<br />
lensing curl map from polarization<br />
*sim_x_????_lmax3000.fits<br />
lensing curl from temperature and polarization (MV)<br />
<br />
The maps were built using the quadratic estimator implementation described [https://arxiv.org/abs/1807.06210 in the Planck 2018 CMB lensing paper],<br />
with the exception of the filtering, which is isotropic after application of a slightly apodized mask.<br />
<br />
== Map auto-spectra and mean-fields ==<br />
<br />
The raw auto-spectra of the map typically look like the left panel of this figure:<br />
<br />
[[File:Autospecs_rec2.png | 1200px]]<br />
<br />
On large scales there is a very srong contribution from the mask and noise variance map anisotropies (the mean-field). On small scales the recontruction noise N0 takes over.<br />
<br />
The mean-field has not been subtracted out from the maps on disk. This can be performed subtracting the lensing reconstructed maps averaged over a subset of the simulations. The right panel of the figure above shows the spectra of the same realization, after mean-field subtraction.<br />
<br />
The mean-field spectra themselves look like this:<br />
<br />
[[File:MF_cmbs4.png]]<br />
<br />
On small scales there is large Monte-Carlo noise in the spectrum estimate.<br />
<br />
== Fidelity to the input, delensing efficiency ==<br />
<br />
The empirical cross-correlation correlation to the input maps, as calculated across the entire patch is like this:<br />
<br />
[[File:cmbs4rho.png]]<br />
<br />
The square of this is the expected delensing efficiency. The true delensing efficiency will be bit higher in the center, and a bit lower in the edges.<br />
<br />
In order to use one of these maps for delensing, it is necessary to:<br />
* Subtract a mean-field estimate (for instance obtained as the average of the remaining simulations)<br />
* Wiener-filter the map. This can be performed multiplying the alm by the ratio C / C + N0 estimates for these maps provided in the last column of the files<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925/nlpp_{ptt, p_p, p}.dat<br />
<br />
== Lensing reconstruction fiducial parameters ==<br />
<br />
* CMB multipoles from 200 to 3000<br />
* Analysis mask: fmask.fits in same folder<br />
* Gaussian beam of 4 arcmin FWHM<br />
* Flat noise of 1.5 (T) and 2.12 (Pol.) muK-arcmin<br />
* FFP10 fiducial CMB spectra<br />
* Separate temperature and polarization filtering</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Lensing_reconstructions_02.00&diff=7778Lensing reconstructions 02.002018-09-28T09:28:46Z<p>Jcarron: </p>
<hr />
<div>J.Carron 27 Sept. 2018<br />
<br />
This page documents the 600 lensing maps (healpy alm fits files, lmax=3000, temperature, polarization and MV reconstruction) available at <br />
<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925<br />
<br />
These lensing maps were built from these CMB + noise + foreground maps (described at [[Sim map sets to demonstrate "real_delensing" (02.00 and 02.09)]]):<br />
<br />
/project/projectdirs/cmbs4/data_xx.yy/02.00/cmbs4_02p00_comb_f145_b04_ellmin30_map_2048_mc_{0000 to 0099}.fits<br />
<br />
For illustration, the temperature (TT), polarization (PP) and Minimum Variance (MV) Wiener-filtered displacement reconstructions, together with the input, for realization 99:<br />
<br />
[[File:recmaps_cmbs4_apo.png]]<br />
<br />
There are 6 type of lensing maps, labeled <br />
<br />
*sim_ptt_????_lmax3000.fits <br />
lensing map from temperature only, simulation index ???? 0000 to 0099<br />
*sim_p_p_????_lmax3000.fits<br />
lensing map from polarization only<br />
*sim_p_????_lmax3000.fits<br />
lensing map from temperature and polarization (MV)<br />
*sim_xtt_????_lmax3000.fits<br />
lensing curl map from temperature, useful for null tests<br />
*sim_x_p_????_lmax3000.fits<br />
lensing curl map from polarization<br />
*sim_x_????_lmax3000.fits<br />
lensing curl from temperature and polarization (MV)<br />
<br />
The maps were built using the quadratic estimator implementation described [https://arxiv.org/abs/1807.06210 in the Planck 2018 CMB lensing paper],<br />
with the exception of the filtering, which is isotropic after application of a slightly apodized mask.<br />
<br />
== Map auto-spectra and mean-fields ==<br />
<br />
The raw auto-spectra of the map typically look like the left panel of this figure:<br />
<br />
[[File:Autospecs_rec2.png | 1200px]]<br />
<br />
On large scales there is a very srong contribution from the mask and noise variance map anisotropies (the mean-field). On small scales the recontruction noise N0 takes over.<br />
<br />
The mean-field has not been subtracted out from the maps on disk. This can be performed subtracting the lensing reconstructed maps averaged over a subset of the simulations. The right panel of the figure above shows the spectra of the same realization, after mean-field subtraction.<br />
<br />
The mean-field spectra themselves look like this:<br />
<br />
[[File:MF_cmbs4.png]]<br />
<br />
On small scales there is large Monte-Carlo noise in the spectrum estimate.<br />
<br />
== Fidelity to the input, delensing efficiency ==<br />
<br />
The empirical cross-correlation correlation to the input maps, as calculated across the entire patch is like this:<br />
<br />
[[File:cmbs4rho.png]]<br />
<br />
The square of this is the expected delensing efficiency. The true delensing efficiency will be bit higher in the center, and a bit lower in the edges.<br />
<br />
In order to use one of these maps for delensing, it is necessary to:<br />
* Subtract a mean-field estimate (for instance obtained as the average of the remaining simulations)<br />
* Wiener-filter the map. This can be performed multiplying the alm by the ratio C / C + N0 estimates for these maps provided in the last column of the files<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925/nlpp_{ptt, p_p, p}.dat<br />
<br />
== Lensing reconstruction fiducial parameters ==<br />
<br />
* CMB multipoles from 200 to 3000<br />
* Analysis mask: fmask.fits in same folder<br />
* Gaussian beam of 4 arcmin FWHM<br />
* Flat noise of 1.5 (T) and 2.12 (Pol.) muK-arcmin<br />
* FFP10 fiducial CMB spectra<br />
* Separate temperature and polarization filtering</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Recmaps_cmbs4_apo.png&diff=7777File:Recmaps cmbs4 apo.png2018-09-28T09:08:55Z<p>Jcarron: Jcarron uploaded a new version of File:Recmaps cmbs4 apo.png</p>
<hr />
<div>Lensing reconstruction on /project/projectdirs/cmbs4/data_xx.yy/02.00/cmbs4_02p00_comb_f145_b04_ellmin30_map_2048_mc_0099.fits</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Recmaps_cmbs4_apo.png&diff=7776File:Recmaps cmbs4 apo.png2018-09-28T09:07:26Z<p>Jcarron: Jcarron uploaded a new version of File:Recmaps cmbs4 apo.png</p>
<hr />
<div>Lensing reconstruction on /project/projectdirs/cmbs4/data_xx.yy/02.00/cmbs4_02p00_comb_f145_b04_ellmin30_map_2048_mc_0099.fits</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Recmaps_cmbs4_apo.png&diff=7775File:Recmaps cmbs4 apo.png2018-09-28T09:06:20Z<p>Jcarron: Jcarron uploaded a new version of File:Recmaps cmbs4 apo.png</p>
<hr />
<div>Lensing reconstruction on /project/projectdirs/cmbs4/data_xx.yy/02.00/cmbs4_02p00_comb_f145_b04_ellmin30_map_2048_mc_0099.fits</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Lensing_reconstructions_02.00&diff=7774Lensing reconstructions 02.002018-09-28T08:27:57Z<p>Jcarron: </p>
<hr />
<div>J.Carron 27 Sept. 2018<br />
<br />
This page documents the 600 lensing maps (healpy alm fits files, lmax=3000, temperature, polarization and MV reconstruction) available at <br />
<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925<br />
<br />
These lensing maps were built from these CMB + noise + foreground maps (described at [[Sim map sets to demonstrate "real_delensing" (02.00 and 02.09)]]):<br />
<br />
/project/projectdirs/cmbs4/data_xx.yy/02.00/cmbs4_02p00_comb_f145_b04_ellmin30_map_2048_mc_{0000 to 0099}.fits<br />
<br />
For illustration, the temperature (TT), polarization (PP) and Minimum Variance (MV) Wiener-filtered displacement reconstructions, together with the input, for realization 99:<br />
<br />
[[File:recmaps_cmbs4_apo.png]]<br />
<br />
There are 6 type of lensing maps, labeled <br />
<br />
*sim_ptt_????_lmax3000.fits <br />
lensing map from temperature only, simulation index ???? 0000 to 0099<br />
*sim_p_p_????_lmax3000.fits<br />
lensing map from polarization only<br />
*sim_p_????_lmax3000.fits<br />
lensing map from temperature and polarization (MV)<br />
*sim_xtt_????_lmax3000.fits<br />
lensing curl map from temperature, useful for null tests<br />
*sim_x_p_????_lmax3000.fits<br />
lensing curl map from polarization<br />
*sim_x_????_lmax3000.fits<br />
lensing curl from temperature and polarization (MV)<br />
<br />
The maps were built using the quadratic estimator implementation described [https://arxiv.org/abs/1807.06210 in the Planck 2018 CMB lensing paper],<br />
with the exception of the filtering, which is isotropic after application of a slightly apodized mask.<br />
<br />
== Map auto-spectra and mean-fields ==<br />
<br />
The raw auto-spectra of the map typically look like the left panel of this figure:<br />
<br />
[[File:Autospecs_rec2.png | 1200px]]<br />
<br />
On large scales there is a very srong contribution from the mask and noise variance map anisotropies (the mean-field). On small scales the recontruction noise N0 takes over.<br />
<br />
The mean-field has not been subtracted out from the maps on disk. This can be performed subtracting the lensing reconstructed maps averaged over a subset of the simulations. The right panel of the figure above shows the spectra of the same realization, after mean-field subtraction.<br />
<br />
The mean-field spectra themselves look like this:<br />
<br />
[[File:MF_cmbs4.png]]<br />
<br />
<br />
== Fidelity to the input, delensing efficiency ==<br />
<br />
The empirical cross-correlation correlation to the input maps, as calculated across the entire patch is like this:<br />
<br />
[[File:cmbs4rho.png]]<br />
<br />
The square of this is the expected delensing efficiency. The true delensing efficiency will be bit higher in the center, and a bit lower in the edges.<br />
<br />
In order to use one of these maps for delensing, it is necessary to:<br />
* Subtract a mean-field estimate (for instance obtained as the average of the remaining simulations)<br />
* Wiener-filter the map. This can be performed multiplying the alm by the ratio C / C + N0 estimates for these maps provided in the last column of the files<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925/nlpp_{ptt, p_p, p}.dat<br />
<br />
== Lensing reconstruction fiducial parameters ==<br />
<br />
* CMB multipoles from 200 to 3000<br />
* Analysis mask: fmask.fits in same folder<br />
* Gaussian beam of 4 arcmin FWHM<br />
* Flat noise of 1.5 and 2.12 muK-arcmin<br />
* FFP10 fiducial CMB spectra<br />
* Separate temperature and polarization filtering</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Autospecs_rec2.png&diff=7773File:Autospecs rec2.png2018-09-28T08:09:43Z<p>Jcarron: Auto spectra of the lensing maps in /project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925</p>
<hr />
<div>Auto spectra of the lensing maps in /project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Lensing_reconstructions_02.00&diff=7769Lensing reconstructions 02.002018-09-27T14:30:22Z<p>Jcarron: </p>
<hr />
<div>J.Carron 27 Sept. 2018<br />
<br />
This page documents the 600 lensing maps (healpy alm fits files, lmax=3000, temperature, polarization and MV reconstruction) available at <br />
<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925<br />
<br />
These lensing maps were built from these CMB + noise + foreground maps:<br />
<br />
/project/projectdirs/cmbs4/data_xx.yy/02.00/cmbs4_02p00_comb_f145_b04_ellmin30_map_2048_mc_{0000 to 0099}.fits<br />
<br />
For illustration, the temperature (TT), polarization (PP) and Minimum Variance (MV) Wiener-filtered displacement reconstructions, together with the input, for realization 99:<br />
<br />
[[File:recmaps_cmbs4_apo.png]]<br />
<br />
There are 6 type of lensing maps, labeled <br />
<br />
*sim_ptt_????_lmax3000.fits <br />
lensing map from temperature only, simulation index ???? 0000 to 0099<br />
*sim_p_p_????_lmax3000.fits<br />
lensing map from polarization only<br />
*sim_p_????_lmax3000.fits<br />
lensing map from temperature and polarization (MV)<br />
*sim_xtt_????_lmax3000.fits<br />
lensing curl map from temperature, useful for null tests<br />
*sim_x_p_????_lmax3000.fits<br />
lensing curl map from polarization<br />
*sim_x_????_lmax3000.fits<br />
lensing curl from temperature and polarization (MV)<br />
<br />
The maps were built using the quadratic estimator implementation described [https://arxiv.org/abs/1807.06210 in the 2018 CMB lensing paper],<br />
with the exception of the filtering, which is isotropic after application of a slightly apodized mask.<br />
<br />
== Lensing reconstruction fiducial parameters ==<br />
<br />
* CMB multipoles from 200 to 3000<br />
* Analysis mask: fmask.fits in same folder<br />
* Gaussian beam of 4 arcmin FWHM<br />
* Flat noise of 1.5 and 2.12 muK-arcmin<br />
* FFP10 fiducial CMB spectra<br />
* Separate temperature and polarization filtering<br />
<br />
== Fidelity to the input, delensing efficiency ==<br />
<br />
The cross-correlation correlation to the input maps, as calculated across the entire patch is like this:<br />
<br />
[[File:cmbs4rho.png]]<br />
<br />
The square of this is the expected delensing efficiency. The true delensing efficiency will be bit higher in the center, and a bit lower in the edges.<br />
<br />
== Mean-fields ==<br />
The mean-field (here, contribution from the mask and noise anisotropies) has not been subtracted out from the maps on disk. The mean-field spectra look like this:<br />
<br />
[[File:MF_cmbs4.png]]<br />
<br />
The mean-field subtraction can be performed subtracting the lensing reconstructed maps averaged over a subset of the simulations.</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=R_Forecasting_Logbook&diff=7768R Forecasting Logbook2018-09-27T13:58:21Z<p>Jcarron: /* 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 r 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 />
== Telecon Notes ==<br />
<br />
[https://docs.google.com/document/d/1886yT1b6QDuWvsbAu5HmVv2Cl4pfH00YpK5Fv8dNzcM/edit?usp=sharing Telecon notes for r-forecasting]<br />
<br />
== Logbook Entries (reverse chronological) ==<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 August 27''': [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''': [[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://users.physics.harvard.edu/~buza/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://users.physics.harvard.edu/~buza/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://users.physics.harvard.edu/~buza/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://users.physics.harvard.edu/~buza/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://users.physics.harvard.edu/~buza/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://users.physics.harvard.edu/~buza/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://users.physics.harvard.edu/~buza/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>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Lensing_reconstructions_02.00&diff=7767Lensing reconstructions 02.002018-09-27T13:53:15Z<p>Jcarron: </p>
<hr />
<div>J.Carron 27 Sept. 2018<br />
<br />
This page documents the 600 lensing maps (healpy alm fits files, lmax=3000, temperature, polarization and MV reconstruction) available at <br />
<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925<br />
<br />
These lensing maps were built from these CMB + noise + foreground maps:<br />
<br />
/project/projectdirs/cmbs4/data_xx.yy/02.00/cmbs4_02p00_comb_f145_b04_ellmin30_map_2048_mc_{0000 to 0099}.fits<br />
<br />
For illustration, the temperature (TT), polarization (PP) and Minimum Variance (MV) Wiener-filtered displacement reconstructions, together with the input, for realization 99:<br />
<br />
[[File:recmaps_cmbs4_apo.png]]<br />
<br />
There are 6 type of lensing maps, labeled <br />
<br />
*sim_ptt_????_lmax3000.fits <br />
lensing map from temperature only, simulation index ???? 0000 to 0099<br />
*sim_p_p_????_lmax3000.fits<br />
lensing map from polarization only<br />
*sim_p_????_lmax3000.fits<br />
lensing map from temperature and polarization (MV)<br />
*sim_xtt_????_lmax3000.fits<br />
lensing curl map from temperature, useful for null tests<br />
*sim_x_p_????_lmax3000.fits<br />
lensing curl map from polarization<br />
*sim_x_????_lmax3000.fits<br />
lensing curl from temperature and polarization (MV)<br />
<br />
The maps were built using the quadratic estimator implementation described [https://arxiv.org/abs/1807.06210 in the 2018 CMB lensing paper],<br />
with the exception of the filtering, which is isotropic after application of a slightly apodized mask.<br />
<br />
== Reconstruction parameters ==<br />
<br />
* CMB multipoles from 200 to 3000<br />
* Analysis mask: fmask.fits in same folder<br />
* Gaussian beam of 4 arcmin FWHM<br />
* Flat noise of 1.5 and 2.12 muK-arcmin<br />
* FFP10 fiducial lensing spectra<br />
* Separate temperature and polarization filtering<br />
<br />
== Fidelity to the input, delensing efficiency ==<br />
<br />
The cross-correlation correlation to the input maps, as calculated across the entire patch is like this:<br />
<br />
[[File:cmbs4rho.png]]<br />
<br />
The square of this is the expected delensing efficiency. The true delensing efficiency will be bit higher in the center, and a bit lower in the edges.<br />
<br />
== Mean-fields ==<br />
The mean-field (here, contribution from the mask and noise anisotropies) has not been subtracted out from the maps on disk. The mean-field spectra look like this:<br />
<br />
[[File:MF_cmbs4.png]]<br />
<br />
The mean-field subtraction can be performed subtracting the lensing reconstructed maps averaged over a subset of the simulations.</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Lensing_reconstructions_02.00&diff=7766Lensing reconstructions 02.002018-09-27T13:45:41Z<p>Jcarron: </p>
<hr />
<div>J.Carron 27 Sept. 2018<br />
<br />
This page documents the 600 lensing maps (healpy alm fits files, lmax=3000) available at <br />
<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925<br />
<br />
There are 6 type of maps, labeled <br />
<br />
*sim_ptt_????_lmax3000.fits <br />
lensing map from temperature only, simulation index ???? 0000 to 0099<br />
*sim_p_p_????_lmax3000.fits<br />
lensing map from polarization only<br />
*sim_p_????_lmax3000.fits<br />
lensing map from temperature and polarization (MV)<br />
*sim_xtt_????_lmax3000.fits<br />
lensing curl map from temperature, useful for null tests<br />
*sim_x_p_????_lmax3000.fits<br />
lensing curl map from polarization<br />
*sim_x_????_lmax3000.fits<br />
lensing curl from temperature and polarization (MV)<br />
<br />
The maps were built using the quadratic estimator implementation described [https://arxiv.org/abs/1807.06210 in the 2018 CMB lensing paper],<br />
with the exception of the filtering, which is isotropic after application of a slightly apodized mask.<br />
<br />
These lensing maps were built from these CMB + noise + foreground maps:<br />
<br />
/project/projectdirs/cmbs4/data_xx.yy/02.00/cmbs4_02p00_comb_f145_b04_ellmin30_map_2048_mc_{0000 to 0099}.fits<br />
<br />
For illustration, the temperature (TT), polarization (PP) and Minimum Variance (MV) Wiener-filtered displacement reconstructions, together with the input, for realization 99:<br />
<br />
[[File:recmaps_cmbs4_apo.png]]<br />
== Reconstruction parameters ==<br />
<br />
* CMB multipoles from 200 to 3000<br />
* Analysis mask: fmask.fits in same folder<br />
* Gaussian beam of 4 arcmin FWHM<br />
* Flat noise of 1.5 and 2.12 muK-arcmin<br />
* FFP10 fiducial lensing spectra<br />
* Separate temperature and polarization filtering<br />
<br />
== Fidelity to the input ==<br />
<br />
The cross-correlation correlation to the input maps, as calculated across the entire patch is like this:<br />
<br />
[[File:cmbs4rho.png]]<br />
<br />
== Mean-fields ==<br />
The mean-field (here, contribution from the mask and noise anisotropies) has not been subtracted out from the maps on disk. The mean-field spectra look like this:<br />
<br />
[[File:MF_cmbs4.png]]<br />
<br />
The mean-field subtraction can be performed subtracting the lensing reconstructed maps averaged over a subset of the simulations.</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Lensing_reconstructions_02.00&diff=7765Lensing reconstructions 02.002018-09-27T13:45:00Z<p>Jcarron: </p>
<hr />
<div>J.Carron 27 Sept. 2018<br />
<br />
This page documents the 600 lensing maps (healpy alm fits files, lmax=3000) available at <br />
<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925<br />
<br />
There are 6 type of maps, labeled <br />
<br />
*sim_ptt_????_lmax3000.fits <br />
lensing map from temperature only, simulation index ???? 0000 to 0099<br />
*sim_p_p_????_lmax3000.fits<br />
lensing map from polarization only<br />
*sim_p_????_lmax3000.fits<br />
lensing map from temperature and polarization (MV)<br />
*sim_xtt_????_lmax3000.fits<br />
lensing curl map from temperature, useful for null tests<br />
*sim_x_p_????_lmax3000.fits<br />
lensing curl map from polarization<br />
*sim_x_????_lmax3000.fits<br />
lensing curl from temperature and polarization (MV)<br />
<br />
The maps were built using the quadratic estimator implementation described [https://arxiv.org/abs/1807.06210 in the 2018 CMB lensing paper],<br />
with the exception of the filtering, which is isotropic after application of a slightly apodized mask.<br />
<br />
These lensing maps were built from these CMB + noise + foreground maps:<br />
<br />
/project/projectdirs/cmbs4/data_xx.yy/02.00/cmbs4_02p00_comb_f145_b04_ellmin30_map_2048_mc_{0000 to 0099}.fits<br />
<br />
For illustration, the temperature (TT), polarization (PP) and Minimum Variance (MV) Wiener-filtered displacement reconstructions, together with the input, for realization 99:<br />
<br />
[[File:recmaps_cmbs4_apo.png]]<br />
== Reconstruction parameters ==<br />
<br />
* CMB multipoles from 200 to 3000<br />
* Analysis mask: fmask.fits in same folder<br />
* Gaussian beam of 4 arcmin FWHM<br />
* Flat noise of 1.5 and 2.12 muK-arcmin<br />
* FFP10 fiducial lensing spectra<br />
* Separate temperature and polarization filtering<br />
<br />
== Fidelity to the input ==<br />
<br />
The cross-correlation correlation to the input maps, as calculated across the entire patch is like this:<br />
<br />
[[File:cmbs4rho.png]]<br />
<br />
== Mean-fields ==<br />
The mean-field (here, contribution from the mask and noise anisotropies) has not been subtracted out from the maps on disk. The mean-field spectra look like this:<br />
<br />
[[File:MF_cmbs4.png]]<br />
<br />
The mean-field subtraction can be performed subtracting the lensing reconstructed maps averaged over a subset of the simulations.</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Lensing_reconstructions_02.00&diff=7764Lensing reconstructions 02.002018-09-27T13:41:53Z<p>Jcarron: </p>
<hr />
<div>J.Carron 27 Sept. 2018<br />
<br />
This page documents the 600 lensing maps (healpy alm fits files, lmax=3000) available at <br />
<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925<br />
<br />
There are 6 type of maps, labeled with <br />
<br />
*sim_ptt_????_lmax3000.fits <br />
lensing map from temperature only, simulation index ???? 0000 to 0099<br />
*sim_p_p_????_lmax3000.fits<br />
lensing map from polarization only<br />
*sim_p_????_lmax3000.fits<br />
lensing map from temperature and polarization (MV)<br />
*sim_xtt_????_lmax3000.fits<br />
lensing curl map from temperature, useful for null tests<br />
*sim_x_p_????_lmax3000.fits<br />
lensing curl map from polarization<br />
*sim_x_????_lmax3000.fits<br />
lensing curl from temperature and polarization (MV)<br />
<br />
The maps were built using the quadratic estimator implementation described [https://arxiv.org/abs/1807.06210 in the 2018 CMB lensing paper],<br />
with the exception of the filtering, which is isotropic after application of a slightly apodized mask.<br />
<br />
For illustration, the temperature (TT), polarization (PP) and Minimum Variance (MV) Wiener-filtered displacement reconstructions, together with the input, for realization 99:<br />
<br />
[[File:recmaps_cmbs4_apo.png]]<br />
== Reconstruction parameters ==<br />
<br />
* CMB multipoles from 200 to 3000<br />
* Analysis mask: fmask.fits in same folder<br />
* Gaussian beam of 4 arcmin FWHM<br />
* Flat noise of 1.5 and 2.12 muK-arcmin<br />
* FFP10 fiducial lensing spectra<br />
* Separate temperature and polarization filtering<br />
<br />
== Fidelity to the input ==<br />
<br />
The cross-correlation correlation to the input maps, as calculated across the entire patch is like this:<br />
<br />
[[File:cmbs4rho.png]]<br />
<br />
== Mean-fields ==<br />
The mean-field (here, contribution from the mask and noise anisotropies) has not been subtracted out from the maps on disk. The mean-field spectra look like this:<br />
<br />
[[File:MF_cmbs4.png]]<br />
<br />
The mean-field subtraction can be performed subtracting the lensing reconstructed maps averaged over a subset of the simulations.</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Lensing_reconstructions_02.00&diff=7763Lensing reconstructions 02.002018-09-27T13:40:55Z<p>Jcarron: </p>
<hr />
<div>This page documents the 600 lensing maps (healpy alm fits file, lmax=3000) available at <br />
<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925<br />
<br />
There are 6 type of maps, labeled with <br />
<br />
*sim_ptt_????_lmax3000.fits <br />
lensing map from temperature only, simulation index ???? 0000 to 0099<br />
*sim_p_p_????_lmax3000.fits<br />
lensing map from polarization only<br />
*sim_p_????_lmax3000.fits<br />
lensing map from temperature and polarization (MV)<br />
*sim_xtt_????_lmax3000.fits<br />
lensing curl map from temperature, useful for null tests<br />
*sim_x_p_????_lmax3000.fits<br />
lensing curl map from polarization<br />
*sim_x_????_lmax3000.fits<br />
lensing curl from temperature and polarization (MV)<br />
<br />
The maps were built using the quadratic estimator implementation described [https://arxiv.org/abs/1807.06210 in the 2018 CMB lensing paper],<br />
with the exception of the filtering, which is isotropic after application of a slightly apodized mask.<br />
<br />
For illustration, the temperature (TT), polarization (PP) and Minimum Variance (MV) Wiener-filtered displacement reconstructions, together with the input, for realization 99:<br />
<br />
[[File:recmaps_cmbs4_apo.png]]<br />
== Reconstruction parameters ==<br />
<br />
* CMB multipoles from 200 to 3000<br />
* Analysis mask: fmask.fits in same folder<br />
* Gaussian beam of 4 arcmin FWHM<br />
* Flat noise of 1.5 and 2.12 muK-arcmin<br />
* FFP10 fiducial lensing spectra<br />
* Separate temperature and polarization filtering<br />
<br />
== Fidelity to the input ==<br />
<br />
The cross-correlation correlation to the input maps, as calculated across the entire patch is like this:<br />
<br />
[[File:cmbs4rho.png]]<br />
<br />
== Mean-fields ==<br />
The mean-field (here, contribution from the mask and noise anisotropies) has not been subtracted out from the maps on disk. The mean-field spectra look like this:<br />
<br />
[[File:MF_cmbs4.png]]<br />
<br />
The mean-field subtraction can be performed subtracting the lensing reconstructed maps averaged over a subset of the simulations.</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Lensing_reconstructions_02.00&diff=7762Lensing reconstructions 02.002018-09-27T13:29:53Z<p>Jcarron: </p>
<hr />
<div>This page documents the 600 lensing maps (healpy alm fits file, lmax=3000) available at <br />
<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925<br />
<br />
There are 6 type of maps, labeled with <br />
<br />
sim_ptt_????_lmax3000.fits : lensing map from temperature only, simulation index ???? 0000 to 0099<br />
<br />
sim_p_p_????_lmax3000.fits : lensing map from polarization only<br />
<br />
sim_p_????_lmax3000.fits : lensing map from temperature and polarization (MV)<br />
<br />
sim_xtt_????_lmax3000.fits : lensing curl map from temperature, useful for null tests<br />
<br />
sim_x_p_????_lmax3000.fits : lensing curl map from polarization<br />
<br />
sim_x_????_lmax3000.fits : lensing curl from temperature and polarization (MV)<br />
<br />
The maps were built using the quadratic estimator implementation described [https://arxiv.org/abs/1807.06210 in the 2018 CMB lensing paper],<br />
with the exception of the filtering, which is isotropic after application of a slightly apodized mask. The filtering uses <br />
<br />
<br />
<br />
<br />
<br />
<br />
For illustration, the temperature (TT), polarization (PP) and Minimum Variance (MV) Wiener-filtered displacement reconstructions, together with the input, for realization 99:<br />
<br />
[[File:recmaps_cmbs4_apo.png]]<br />
== Reconstruction parameters ==<br />
<br />
== Fidelity to the input ==<br />
The cross-correlation correlation to the input maps, as calculated across the entire patch is roughly like this:<br />
<br />
[[File:cmbs4rho.png]]<br />
<br />
== Mean-fields ==<br />
The mean-field (here, contribution from the mask and noise anisotropies) has not been subtracted out from the maps on disk. The mean-field spectra look like this:<br />
<br />
[[File:MF_cmbs4.png]]<br />
<br />
The mean-field subtraction can be performed subtracting the lensing reconstructed maps averaged over a subset of the simulations.</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Lensing_reconstructions_02.00&diff=7761Lensing reconstructions 02.002018-09-27T13:22:49Z<p>Jcarron: </p>
<hr />
<div>This page documents the 600 lensing maps (healpy alm fits file, lmax=3000) available at <br />
<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925<br />
<br />
There are 6 type of maps, labeled with <br />
<br />
sim_ptt_????_lmax3000.fits : lensing map from temperature only, simulation index ???? 0000 to 0099<br />
<br />
sim_p_p_????_lmax3000.fits : lensing map from polarization only<br />
<br />
sim_p_????_lmax3000.fits : lensing map from temperature and polarization (MV)<br />
<br />
sim_xtt_????_lmax3000.fits : lensing curl map from temperature, useful for null tests<br />
<br />
sim_x_p_????_lmax3000.fits : lensing curl map from polarization<br />
<br />
sim_x_????_lmax3000.fits : lensing curl from temperature and polarization (MV)<br />
<br />
<br />
For illustration, the temperature (TT), polarization (PP) and Minimum Variance (MV) Wiener-filtered displacement reconstructions, together with the input, for realization 99:<br />
<br />
[[File:recmaps_cmbs4_apo.png]]<br />
<br />
The cross-correlation correlation to the input maps, as calculated across the entire patch is roughly like this:<br />
<br />
[[File:cmbs4rho.png]]<br />
<br />
The mean-field (here, contribution from the mask and noise anisotropies) has not been subtracted out from the maps on disk. The mean-field spectra look like this:<br />
<br />
[[File:MF_cmbs4.png]]<br />
<br />
The mean-field subtraction can be performed subtracting the lensing reconstructed maps averaged over a subset of the simulations.</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Lensing_reconstructions_02.00&diff=7760Lensing reconstructions 02.002018-09-27T13:17:50Z<p>Jcarron: Created page with "This page documents the 600 lensing maps (healpy alm fits file, lmax=3000) available at /project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_l..."</p>
<hr />
<div>This page documents the 600 lensing maps (healpy alm fits file, lmax=3000) available at <br />
<br />
/project/projectdirs/cmbs4/reanalysis/phi_recons/02.00_carron_180920/plms_sepTP_apo_lmin200lmax3000_fsky5pc_cut10_180925<br />
<br />
<br />
For illustration, the temperature (TT), polarization (PP) and Minimum Variance (MV) Wiener-filtered displacement reconstructions, together with the input, for realization 99:<br />
<br />
[[File:recmaps_cmbs4_apo.png]]<br />
<br />
The cross-correlation correlation to the input maps, as calculated across the entire patch is roughly like this:<br />
<br />
[[File:cmbs4rho.png]]<br />
<br />
The mean-field (here, contribution from the mask and noise anisotropies) has not been subtracted out from the maps on disk. The mean-field spectra look like this:<br />
<br />
[[File:MF_cmbs4.png]]<br />
<br />
The mean-field subtraction can be performed subtracting the lensing reconstructed maps averaged over a subset of the simulations.</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Cmbs4rho.png&diff=7759File:Cmbs4rho.png2018-09-27T13:17:22Z<p>Jcarron: Cross-corr. coefficient for the lensing rec. on 02.00</p>
<hr />
<div>Cross-corr. coefficient for the lensing rec. on 02.00</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:MF_cmbs4.png&diff=7758File:MF cmbs4.png2018-09-27T13:16:54Z<p>Jcarron: Mean-field for combined rec. on 02.00</p>
<hr />
<div>Mean-field for combined rec. on 02.00</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=File:Recmaps_cmbs4_apo.png&diff=7757File:Recmaps cmbs4 apo.png2018-09-27T13:03:30Z<p>Jcarron: Lensing reconstruction on /project/projectdirs/cmbs4/data_xx.yy/02.00/cmbs4_02p00_comb_f145_b04_ellmin30_map_2048_mc_0099.fits</p>
<hr />
<div>Lensing reconstruction on /project/projectdirs/cmbs4/data_xx.yy/02.00/cmbs4_02p00_comb_f145_b04_ellmin30_map_2048_mc_0099.fits</div>Jcarronhttps://cmb-s4.uchicago.edu/wiki/index.php?title=Sim_map_sets_to_demonstrate_%22real_delensing%22_(02.00_and_02.09)&diff=7756Sim map sets to demonstrate "real delensing" (02.00 and 02.09)2018-09-27T13:00:19Z<p>Jcarron: </p>
<hr />
<div>Feb 7 2018, Clem Pryke<br />
<br />
The current plan for CMB-S4 calls for a deep (fsky order 3%) survey with both small and large apertures hitting the same field.<br />
The small apertures will deliver very low noise at larger angular scales and the large apertures will provide the lensing reconstruction<br />
needed to "delens" the small aperture maps.<br />
For the [https://www.nsf.gov/mps/ast/aaac/cmb_s4/report/CMBS4_final_report_NL.pdf CDT report] appendix A simulations we "faked" delensing by simply turning down the strength of the lensing effect in<br />
the small aperture maps.<br />
The next step is to simulate coordinated small and large aperture maps and do a re-analysis including "real delensing".<br />
This post introduces two sets of such maps.<br />
This is built on the previous [[Experiment Definitions]] 02 set<br />
so the frequencies, resolutions, and noise levels do not exactly match the CDT report strawman configuration.<br />
However, they should be good enough to test lensing reconstruction in the presence of apodization, noise and (one form of) non-Gaussian foreground.<br />
<br />
Two sets of maps are provided on NERSC in directories '''/project/projectdirs/cmbs4/data_xx.yy/02.YY''' where YY=00 is a<br />
simple Gaussian foreground model and YY=09 is the non-Gaussian model kindly provided by Flavien Vansyngel - see<br />
[[Vansyngel Model]].<br />
<br />
The plot below shows the Q maps for realization 0001.<br />
The left three columns are the low res (small aperture) maps for 95/145/220GHz bands and<br />
the right three columns are the high res (large aperture) versions in the same bands.<br />
(There are additional low res bands not shown.)<br />
The top row of plots is a realization of lensed-LCDM at the appropriate resolution.<br />
The second row is the Vansyngel foreground model at each resolution (mostly dust).<br />
The third row is the experimental noise which blows up around the edge in an appopriate manner.<br />
It is hard to see but the edge taper is actually less for the high res due to smaller instantaneous<br />
field of view.<br />
The noise extends up to the pixel scale which is nside=512 for the low res maps and nside=2048 for<br />
the high res, so at the pixelization of this rendering the high res map is heavily aliased and<br />
the noise level looks higher than for the low res - in fact the white noise level is the same<br />
for e.g. 95GHz low and high res.<br />
The bottom row shows the combination of the above rows which is what one actually gets to measure.<br />
<br />
[[File:180207_f1.gif|border]][[Media:180207_f1.pdf]]<br />
<br />
A link to a pdf file is provided to the right of the plot above where you can zoom in and overcome the screen aliasing.<br />
Alternatively the plot below is pre-zoomed to the central region of the maps.<br />
In the top row one can now clearly see the loss of lensing signal in the low res maps, while the high res look nearly the same<br />
because the lensing signal is adequately resolved in all three bands.<br />
In the middle row at 220GHz we can see that the dust foreground model contains small scale structure which the low res telescope<br />
is unable to see.<br />
In the third row for the low res bands we can see the white noise cutting off at the Healpix pixel scale (the white<br />
noise level actually being the same between high and low res at each given frequency).<br />
<br />
[[File:180207_f2.gif|border]][[Media:180207_f2.pdf]]<br />
<br />
The overall goal is to jointly analyze the full set of low and high res maps for each realization and extract the<br />
maximum likelihood value of r, and then to take statistics over the available realizations to investigate bias and uncertainty<br />
for a given re-analysis technique.<br />
However, the task can be split.<br />
One way to proceed is to take the high res maps and analyze them alone to extract the lensing potential<br />
map phi.<br />
That can then be used to form a lensing template and fed forward to the next step in the re-analysis.<br />
<br />
Some more info on the sims is available at [[Data Challenge Map Sets 04.YY]].<br />
<br />
For a very first step one can take the high res masked lensed-LCDM single frequency map like<br />
'''/project/projectdirs/cmbs4/data_xx.yy/02.00/cmbs4_02_llcdm_f145_b04_ellmin30_map_2048_mc_0000.fits''' and run phi reconstruction.<br />
The appropriate "relative hits" mask is '''/project/projectdirs/cmbs4/expt_xx/02/rhits/n2048.fits'''.<br />
(The next step would be to compare to the true input phi map and these appear to be in the fourth binary table<br />
of '''/project/projectdirs/cmb/data/generic/cmb/ffp10/mc/scalar/ffp10_unlensed_scl_cmb_000_tebplm_mc_0000.fits''' etc.)<br />
<br />
(jcarron Sept 27 2018)<br />
Documentation on the lensing reconstruction on these maps is availaible at [[Lensing reconstructions 02.00]]</div>Jcarron