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--- private:teleconsnotes20171018 [2017/10/18 16:25] – kyoung
+++ private:teleconsnotes20171018 [2017/10/24 14:50] (current) – hanany
@@ Line 17: / Line 17: @@
 Foregrounds Workshop
-The mission study is sponsoring a 3-day Foregrounds workshop in the University of California San Diego. The dates are Nov. 29 (Wednesday), Nov. 30 (Thursday), and Dec. 1 (Friday), 2017. Please mark your calendars. These dates are a change relative to our previous announcement, but they are more convenient for the vast majority of attendees. For travel purposes, the workshop will begin around 9 am on Monday and will end in the afternoon of Wednesday. Please register now.
+The mission study is sponsoring a 3-day Foregrounds workshop in the University of California San Diego. The dates are Nov. 29 (Wednesday), Nov. 30 (Thursday), and Dec. 1 (Friday), 2017. Please mark your calendars. These dates are a change relative to our previous announcement, but they are more convenient for the vast majority of attendees. For travel purposes, the workshop will begin around 9 am on Wednesday and will end in the early afternoon of Friday. Please register now.
 Spectrometer and Imager
@@ Line 25: / Line 25: @@
 The EC has invited studies from other working groups (Fundamental Physics, Extragalactic Science, Galactic Science) to assess the science trade-offs from a mission consisting of only a 1.4 m aperture imager compared to a 0.5 m aperture imager and a spectrometer. The contributions from these WG are available from the respective coordinators and are mostly posted on the wiki page.
-The EC expects a decision [between the two options] by the end of October. You are invited to look at the available documents and provide your thoughts on this issue to any of the EC members.
+The EC expects a decision by the end of October. You are invited to look at the available documents and provide your thoughts on this issue to any of the EC members.
 TeamX Design and Costing
@@ Line 44: / Line 44: @@
 Decision on imager and spectrometer delayed to 2 wks from today.
 periodic update comments
- * paragraph 3 of Spectrometer and Imager: remove text in []'s.  There are likely > 2 options.
+  * paragraph 3 of Spectrometer and Imager: remove text in []'s.  There are likely > 2 options.
 Spectrometer/Imager trade-off discussion
- * Dave: Galactic trade-offs, 30K 140cm vs 4K 50cm
+  * Dave: Galactic trade-offs, 30K 140cm vs 4K 50cm
-   * more detail than needed here, WG document
+    * more detail than needed here, WG document
-   * ultimate goal: resolve magnetic field from ISM to star formation scales and connect to high res telescopes, eg ALMA.
+    * ultimate goal: resolve magnetic field from ISM to star formation scales and connect to high res telescopes, eg ALMA.
-   * Goal 1: resolve HI to HII transition in clouds (magnetic field connection between cloud and ISM)
+    * Goal 1: resolve HI to HII transition in clouds (magnetic field connection between cloud and ISM)
-     * Both systems work.  4K slightly better.  Not resolution limited.
+      * Both systems work.  4K slightly better.  Not resolution limited.
-   * Goal 2: stellar cores in molecular clouds.  Sensitivity is no challenge.
+    * Goal 2: stellar cores in molecular clouds.  Sensitivity is no challenge.
-     * resolution is key. resolve cores and filaments.  See magnetic fields and star formation in situ.
+      * resolution is key. resolve cores and filaments.  See magnetic fields and star formation in situ.
-     * Planck got to 5', so 3' with 50 cm is small improvement.
+      * Planck got to 5', so 3' with 50 cm is small improvement.
-       * want 0.1 pc resolved.
+        * want 0.1 pc resolved.
-       * need beams < 2 arcmin.
+        * need beams < 2 arcmin.
-       * loose all clouds for 50cm case.
+        * loose all clouds for 50cm case.
-       * not frequency driven, just need resolution.
+        * not frequency driven, just need resolution.
-       * BLASTPol is can do similar science.  **A/I** Dave: check what BLASTPol can do.  How this compares?
+        * BLASTPol is can do similar science.  **A/I** Dave: check what BLASTPol can do.  How this compares?
-   * Goal #3.  map  mag field.  seeing clouds out to kpc.  how many resolve 1 pc scales?
+    * Goal #3.  map  mag field.  seeing clouds out to kpc.  how many resolve 1 pc scales?
-     * again resolution limited, not sensitivity
+      * again resolution limited, not sensitivity
-     * 1' --> 700 clouds. 3.4 kpc away.
+      * 1' --> 700 clouds. 3.4 kpc away.
-     * 3' --> 60 clouds.  1.4 kpc away.  survey less of galaxy.
+      * 3' --> 60 clouds.  1.4 kpc away.  survey less of galaxy.
-   * 4: Polarization spectrum.
+    * 4: Polarization spectrum.
-     * grain alignment and dust (John valincourt)
+      * grain alignment and dust (John valincourt)
-     * 4K may do slightly better.
+      * 4K may do slightly better.
-   * 5: Mag field in other galaxies.
+    * 5: Mag field in other galaxies.
-     * resolution limited. need 10 beams across galaxy
+      * resolution limited. need 10 beams across galaxy
-     * group excited about this, a real statiscal sample (100) at 1'.
+      * group excited about this, a real statiscal sample (100) at 1'.
-       * gets beyond local group if 1'
+        * gets beyond local group if 1'
-   * 6: Diffuse ISM
+    * 6: Diffuse ISM
-     * physics and properties of dust.  Closest tie to CMB foregrounds
+      * physics and properties of dust.  Closest tie to CMB foregrounds
-     * target with lowest flux, ~10x lower than molecular cloud envelopes
+      * target with lowest flux, ~10x lower than molecular cloud envelopes
-     * see turbulence power spectrum and field strength.
+      * see turbulence power spectrum and field strength.
-     * need < 4' beams
+      * need < 4' beams
-     * sensitivity is needed. 0.5 MJy/sr
+      * sensitivity is needed. 0.5 MJy/sr
-       * 4K sensitivity is big gain. get to 1% on 3' scales.
+        * 4K sensitivity is big gain. get to 1% on 3' scales.
-       * 30K gets to ~ 7% polarized dust at 10' smoothed.
+        * 30K gets to ~ 7% polarized dust at 10' smoothed.
-     * assuming 2 component dust, different polarization fractions. both at 3'
+      * assuming 2 component dust, different polarization fractions. both at 3'
-       * 30K error is 10's of %.
+        * 30K error is 10's of %.
-       * 4K error is 1%
+        * 4K error is 1%
-   * Overall:
+    * Overall:
-     * Sensitivity limits diffuse ISM, only that.
+      * Sensitivity limits diffuse ISM, only that.
-     * Resolution gains are molecular cloud science.
+      * Resolution gains are molecular cloud science.
-     * Dave's overall guess: Resolution is of more interest to community. Not unanimous.
+      * Dave's overall guess: Resolution is of more interest to community. Not unanimous.
-     * Shaul: Will need to translate this to broad science case. To present to broad non-expert community. Do offline.
+      * Shaul: Will need to translate this to broad science case. To present to broad non-expert community. Do offline.
- * Nick: Extragalactic science.
+  * Nick: Extragalactic science.
-  * Cluster cosmology (neutrino masses, w, wa):
+   * Cluster cosmology (neutrino masses, w, wa):
-    * resolution of 50cm loses ~1/4 of clusters. From thermal SZ.
+     * resolution of 50cm loses ~1/4 of clusters. From thermal SZ.
-    * if S4 exists, this has no real science impact.
+     * if S4 exists, this has no real science impact.
-      * real PICO benefit is in tau measurement
+       * real PICO benefit is in tau measurement
-    * no S4, 15-20% hit in measurement
+     * no S4, 15-20% hit in measurement
-  * CMB lensing S/N:
+   * CMB lensing S/N:
-    * PICO is good lensing experiment, comparable to S4, if 1.4m
+     * PICO is good lensing experiment, comparable to S4, if 1.4m
-    * simplest assumptions: no foregrounds, perfect delensing.
+     * simplest assumptions: no foregrounds, perfect delensing.
-    * better simulations are now set up.
+     * better simulations are now set up.
-  * CMB halo lensing (cluster masses).  50cm gives loss of 2-3x in mass sensitivity
+   * CMB halo lensing (cluster masses).  50cm gives loss of 2-3x in mass sensitivity
-    * larger beam (50cm) incorporates 2-halo term, so likely even more uncertainty.
+     * larger beam (50cm) incorporates 2-halo term, so likely even more uncertainty.
-  * y-map cleaned S/N.  numbers need to be rechecked.
+   * y-map cleaned S/N.  numbers need to be rechecked.
-  * Extragalatic point sources: largest loss at 50 cm.  Still qualitative estimates.
+   * Extragalatic point sources: largest loss at 50 cm.  Still qualitative estimates.
-    * 140cm find 3000 sources where Planck found 10.
+     * 140cm find 3000 sources where Planck found 10.
-    * 50cm, worse than Planck.
+     * 50cm, worse than Planck.
-  * Polarized point sources: can add confusion to r determination. 140cm mission informs on this. 50cm adds nothing new.
+   * Polarized point sources: can add confusion to r determination. 140cm mission informs on this. 50cm adds nothing new.
-  * Proto clusters: 140cm, image 1000's (dusty star forming galaxies). 50cm sees none.
+   * Proto clusters: 140cm, image 1000's (dusty star forming galaxies). 50cm sees none.
-  * Reionization with S3 ground based.
+   * Reionization with S3 ground based.
-    * both (50 and 140 cm) give good tau, and midpoint of reionization.
+     * both (50 and 140 cm) give good tau, and midpoint of reionization.
-  * Charles: all this wants more resolutions. This is done well from ground.  Not going to get more resolution than 1.4m. If all sky or high frequency helps a measurement space is appropriate.  We should emphasize distinctions between ground/space. Also emphasize complementary.
+   * Charles: all this wants more resolutions. This is done well from ground.  Not going to get more resolution than 1.4m. If all sky or high frequency helps a measurement space is appropriate.  We should emphasize distinctions between ground/space. Also emphasize complementary.
-  * Nick: space gets higher frequencies. So helps dusty galaxies and CIB mitigation.
+   * Nick: space gets higher frequencies. So helps dusty galaxies and CIB mitigation.
 Jamie via Shaul:  Jamie concerned: 140-50 cm trade-off may not be needed.  Smaller aperture may not be the cost saver. Maybe the right descope is to reduce FP size or #channels, #readout, power draw.

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