Hi Immanuel,
Looks largely fine. I assume we will have opportunity to update
numbers. Please strike the last sentence about "we expect to publish
such measurements soon." SPIE is in late June--let's count on
publication before then. In any case the statement is not necessary.
John
On 12/8/13, 12:15 PM, Immanuel Buder wrote:
Hi all
Below is a draft abstract I'm planning to submit for SPIE 2014. The
deadline is Monday, and I'm currently in transit to Pole so that makes
coordination a bit difficult. I plan to submit when it is Monday in NZ
time, after ECW issue. I will try to address all comments received by
that time; although, I may not be able to email you back until later.
Also, I haven't slept in ~30 hours, so if this email is incoherent,
that's why.
Eric especially let me know if you want me to put something to integrate
better with your abstract. Although I'm not planning to say anything
about BICEP3 besides a brief advertisement, I'm CCing BICEP3 list in
case they want anything more/less.
Title: BICEP2 and Keck Array: Upgrades and Improved Beam Characterization
Finding evidence for inflation by detecting B-modes in the cosmic
microwave background (CMB) polarization at large angular scales remains
one of the most compelling experimental challenges in cosmology today.
BICEP2 and the Keck Array are part of a program of experiments at the
South Pole
whose main goal is to demonstrate the sensitivity and systematic control
necessary
for tensor-to-scalar ratio r <~ 0.01 measurements.
Beam imperfections that are not sufficiently accounted for are a major
potential source of spurious polarization that could interfere with that
goal.
The strategy of BICEP2 and Keck Array is to completely characterize
their telescopes' polarized beam response with a combination of in-lab,
pre-deployment, and on-site calibrations.
I will report the status of these experiments, focusing on continued
improved understanding of their beams.
Far-field measurements of the BICEP2 beam with a chopped thermal source,
combined with analysis improvements, show that the level of residual
beam-induced systematic errors is below r ~ 0.01.
Similar measurements have been made for the Keck Array.
On-site measurements of Keck Array showed unexpected side lobes that
were terminating on the absorptive telescope forebaffles.
Follow-up lab measurements confirmed these side lobes were due to
inadequate blackening of the cryogenic telescopes, and in late 2013 the
five telescopes were upgraded on site with improved interior baffles.
These baffles have substantially reducted total optical loading, leading
to a ~ 10% increase in mapping speed for the 2014 observing season.
The sensitivity of Keck Array continues to improve: for the 2013 season
it was 9.5 uK*sqrt(s) NET.
In 2014 we converted two of the 150 GHz cameras to 100 GHz for
foreground separation.
The sensitivity at 100 GHz is ~ 20 uK*sqrt(s) per camera.
We have shown that the BICEP2/Keck telescope technology is sufficient
for the goal of measuring r at the 0.01 level.
We expect to publish such measurements soon.
Furthermore, the program is continuing with BICEP3, a 100-GHz telescope
with ??? detectors.
Immanuel Buder
Postdoctoral Fellow
Harvard-Smithsonian Center for Astrophysics
(office) 617 495 7567
(office) 160 Concord Ave., M-114C
(mail) 60 Garden St. MS 42
Cambridge, MA 02138
ibuder(a)gmail.com <mailto:ibuder@gmail.com>
<mailto:ibuder@cfa.harvard.edu>
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___________________________________________________________________
John Kovac
Associate Professor, Harvard University Astronomy Department
160 Concord Ave rm 310, Cambridge MA 02138, 617-496-0611
jmkovac(a)cfa.harvard.edu
CURRENTLY AT SOUTH POLE