Bicep2-list April 2013

bicep2-list@lists.fas.harvard.edu

15 participants
18 discussions

BICEP2 Team meeting today (30 Apr 2013) noon Eastern, followed by pipeline telecon

by John Kovac

Hi all, BICEP2 telecon today at the usual time, followed by CMB pipeline discussion: Tuesday, 30 Apr 2013 12:00 Eastern, 11:00 Central, 9:00 am Pacific Phone: 1-866-890-3820 (toll: 1-334-323-7229) Passcode: 59702175 # Our group-edited agenda is in the telecon notes http://goo.gl/LNvpx Thank you Walt for filling in much of it ahead of time. Clem and anyone else please continue to add appropriate items. Current snapshot is below. John Agenda: 1) General business panlfs downtime 4/29-5/3 (announced last week): impacts? collaboration meeting followups publication policy, talk postings, MOUs writing up instrument / systematics / observations topics 2) Review final report on mapmaking inputs [ Walt ] http://bicep0.caltech.edu/~bicep2/papers/final_reports/mapmaking/ 3) Other final report items and action item review - See Harvard meeting AI’s below 4) Preview of new postings 2013 Apr 23: Temperature Planck maps reobserved with BICEP2 (SRH) 2013 Apr 23: Field Outline (JET) 2013 Apr 23: Statistical precision of the polarization angle determination with the galactic field maps of BICEP2 (SRH) 2013 Apr 23: Fix Map Pager (CLP) 2013 Apr 24: Checking our pointing calculations (RWO) 2013 Apr 24: Feasibility of "traditional" noise sims for BICEP2+Keck (RWO) 2013 Apr 24: Fixing the parallactic angle calculation (RWO) 2013 Apr 25: Active Thermal Control (PID) test (UPDATED) (JPK) 2013 Apr 26: Sign Flip Noise in Comparison to Regular Noise Sims (updated) (STF) 2013 Apr 29: Cross vs. Auto Spectra, version 2 (STF) 2013 Apr 29: FTS: Attempting to Increase Repeatability With Illumination Cuts (UPDATED) (JPK) [ BICEP2 team meeting ends after one hour. ] [ Pipeline agenda to be filled in by Clem and previewed during the last stage of the main telecon ] -- ___________________________________________________________________ John Kovac jmkovac(a)cfa.harvard.edu Assistant Professor, Astronomy and Physics, Harvard University 160 Concord Ave rm 310, Cambridge MA 02138, 617-496-0611

10 years, 9 months

Re: [Bicep2-list] [keckarray] rel gain deproj

by Clem Pryke

> I for one was surprised to be reminded, clicking through this pager, > that the effect of the arc vs RAdec projection is subdominant to relgain > deproj, but not to diffpoint deproj. Is that right? I think so. > If so, and if you've been hoping we can avoid relgain deproj, then why > haven't we been pushing the arc projection? Well I think the thought was that for Kendrick+A/B+RA/Dec the residual E/B leakage was low enough that it was subdominant to noise - so it didn't matter. Although for B2 3yr I'm not sure that is still true. I think you also argued that the simple mapping of scans to x-direction in the RA/Dec projection made the 2d aps easier to interpret - although it's not like looking at those damn plots seems to have taught us much recently ;-) Clem -- ********************************************************************** Clem Pryke - Associate Professor - Physics University of Minnesota, Room 313 Tate, 116 Church Street S.E. Minneapolis, MN, 55455 Tel: 612-624-7578 Fax: 612-624-4578 email: pryke(a)physics.umn.edu **********************************************************************

11 years

Re: [Bicep2-list] [keckarray] rel gain deproj

by Clem Pryke

> there is a large increase in variance when rel gain deproj is > turned on. It is somewhat a surprise because there shouldn't be > too many modes removed, naively. We have known this for some time and I am interested to hear that you think it's surprising. Chris investigated the E/B mix which comes from deproj in this post: http://bicep.caltech.edu/~spuder/analysis_logbook/analysis/20120925_sim1227… Click: - yes pol (no systematics) - n2048/n512 no common A/B - Kendrick We are seeing the residual E/B mixing which comes from our dumb ra/dec flat sky projection. Click the "n2048... arc proj button" to see this reduced further. Going back to the "n2048/n512 no common A/B" option we can now click deproj="relgain" and see a large increase in the E/B mix - and scatter thereof. This is why I have been been keen not to use relgain if we can possibly help it. Now click "n2048/n512 ... noisy template" - not much change. Now click deproj type="per-scanset" - this is fitting the deproj coefficient per 50 minute scanset rather than per phase (10 scansets). We see increase in the amplitude - and scatter - of the E/B mixing. So this last matches your expectation. > I suspect that as our integration time increases However I suspect the leakage does not go up with integration time - if it did it would be way more in Chris sim1234 which is full tag set sims versus the pager above which is tag subset. > and also as our number of pairs increases (from B2 to Keck), the # of > modes we remove also increases.. >From Stefan's plots I think it is not vastly larger. We should check... Clem -- ********************************************************************** Clem Pryke - Associate Professor - Physics University of Minnesota, Room 313 Tate, 116 Church Street S.E. Minneapolis, MN, 55455 Tel: 612-624-7578 Fax: 612-624-4578 email: pryke(a)physics.umn.edu **********************************************************************

11 years

rel gain deproj

by Chao-Lin Kuo

I won't be able to stay long enough for the discussion of postings so I'm sending an idea. In this http://bmode.caltech.edu/~spuder/keck_analysis_logbook/analysis/20130424_re… and other postings it was shown that there is a large increase in variance when rel gain deproj is turned on. It is somewhat a surprise because there shouldn't be too many modes removed, naively. If we have one detector pair that is indeed the case. Now we have tons of detector pairs, and we allow the *relative* relgain between the pairs to vary on pretty fast time scale. And we observe large scatters in the rel gain parameters derived - meaning different modes (in the final coadded map). I suspect that as our integration time increases and also as our number of pairs increases (from B2 to Keck), the # of modes we remove also increases.. Chao-Lin

11 years

Galactic field polarization: precision and future observations?

by Sergi R. Hildebrandt

Hi All, Apologies I had to leave before getting into my temperature post. Walt has let me know that it would be interesting to show some results for the galactic plane. Please find here a beginning for a discussion that would be good to have clear sooner than later since 2013 season is running. http://bicep.caltech.edu/~spuder/analysis_logbook/ Suggestions very welcome. That's why it is a quick post to be continued (Keck/ BICEP2xKeck)! All the best, gal-B2/Keckers, Sergi -- Dr Sergi Hildebrandt Rafels Jet Propulsion Laboratory ---------------- California Institute of Technology 169-217 Cahill-383 4800 Oak Grove Drive 1200, E. California Bvd Pasadena, CA, 91109 Pasadena, CA, 91125 MC/169-237 MC/367-17 1-818-354-0220 1-626-395-2147

11 years

Planck ESLAB slides

by Randol Aikin

Hi All, For those of you not on the Caltech obscos list, please see the note below from Olivier - this presentation in particular: http://www.rssd.esa.int/SA/PLANCK/docs/eslab47/Session09_Data_Processing/47… Randol Begin forwarded message: > From: "Dore, Olivier P (3267)" <Olivier.P.Dore(a)jpl.nasa.gov> > Subject: [Obscos] Planck ESLAB slides > Date: April 21, 2013 12:38:57 PM PDT > To: ObsCos group <obscos(a)astro.caltech.edu> > > Hey all, > Just wanted to point you to the presentations from the very good Planck meeting from two weeks ago in The Netherlands. > http://www.rssd.esa.int/index.php?project=PLANCK&page=47_ESLAB > A lot of good stuff in there. Besides Planck results, I particularly enjoyed the presentations by Zaldarriaga, Mukhanov, Freedman and Page. > Also, if you are interested in dust polarization (if not, you should!), I recommend the presentations of Bernard and Aumont. > Definitely worth a look. > Olivier > > ---------------- > Olivier Doré > olivier.p.dore(a)jpl.nasa.gov > +(1) 626 375 6347 > > > > > > > > > > > > _______________________________________________ > Obscos mailing list > Obscos(a)astro.caltech.edu > http://astro.caltech.edu:88/mailman/listinfo/obscos

11 years

BICEP2 Team meeting today (8 Jan 2013) noon Eastern

by John Kovac

Hi all, A reminder of our first BICEP2 team meeting of the new year, back at our usual time today: Tuesday 8 Jan 2013 9:00 am Pacific, 12:00 eastern, 6:00am Pole Phone: 1-866-890-3820 (toll: 1-334-323-7229) Passcode:59702175 As the agenda below reflects, I expect we will have a very limited pipeline discussion today. Walt, can you please take notes? 1) General business: - online logbook updated for Nov/Dec? [Jon, Colin, …] - status of getting B2 summer data onto odyssey [Walt, Colin] - votes on telecon time for next 5 weeks: 9am or 11am Pacific? 2) Organizing efforts toward results: BICEP2 operations are complete. We'll be reorienting these meetings toward organizing our efforts to produce and publish results. As we discussed in our last (28 Dec) meeting, we'll be starting to match individuals with assignments for "final reports" on B2 sub-threads on reduction and instrument characterization. These are an evolution of the threads we started outlining in November. On the B2 analysis call today Walt volunteered to start a separate index page for these reports, which we see as roughly mapping into sections of papers. Proposed guidelines: 1. unlike logbook postings, these documents get edited and updated until we publish 2. each report connects the topic to what is needed for the B2 science results--what final numbers or tests are needed, and why. 3. review past experiments experience, esp. B1 approach 4. provide an overview of tasks remaining 5. summarize (with links) work done in postings, and where appropriate summarize the existing B2 data. 6. Format can be either html or google doc. Authors should seek and incorporate all group feedback to converge on a consensus doc, ready to extract conclusions for publication. Example report topics: - thermal systematics - magnetic systematics - spectral response - temporal transfer function - RPS-derived polarization chi's and epsilons - pol cal consistency checks from Yukical / pixel polrasters - far sidelobes ... To drive this forward we need your buy-in both on format and assignments. Thread coordinators, please think about topics within your threads that need reports. Those who can't join tomorrow, send feedback and/or offers to take assignments. Today we'll agree on format, organization of topics under threads, and initial assignments. Walt will continue this process on next Tuesday's meeting (I'll be in transit). For future meetings I hope we can schedule reviews of specific reports. 3) B-spectrum Pipeline limited attendance expected today brief update on data reduction [Walt, Angiola] brief update from Jamie T on few degree sidelobes T->P sims (Jamie=monopole, Chris=quadrupole) other updates from ongoing work 4) AOB -- ___________________________________________________________________ John Kovac jmkovac(a)cfa.harvard.edu Assistant Professor, Astronomy and Physics, Harvard University 160 Concord Ave rm 310, Cambridge MA 02138, 617-496-0611

11 years

Fwd: intensity comparison

by Sergi R. Hildebrandt

Hi All, I'll post it later with some more comments. Sergi ---------- Forwarded message ---------- From: Jamie Bock Date: Tuesday, April 23, 2013 Subject: intensity comparison To: "Sergi R. Hildebrandt" <srh(a)caltech.edu> Hi Sergi, Why don’t you send around or post your intensity comparison (attached) given all the emails floating around? Maybe most of the improvement can be realized by changing the boundary since the blob at the edge is so bright (equal to the CMB at 353). Jamie ++++++++++++++++++++++++++++++++++++++++++++++++++++ Caltech (MTTh) JPL (WF) M/S 367-17 M/S 169-327 California Inst. of Technology Jet Propulsion Laboratory Pasadena, CA 91125 Pasadena, CA 91109 Voice: (626)-395-2017 (818)-354-0715 Fax: (626)-395-2366 (818)-354-8895 ++++++++++++++++++++++++++++++++++++++++++++++++++++ -- Dr Sergi Hildebrandt Rafels Jet Propulsion Laboratory ---------------- California Institute of Technology 169-217 Cahill-383 4800 Oak Grove Drive 1200, E. California Bvd Pasadena, CA, 91109 Pasadena, CA, 91125 MC/169-237 MC/367-17 1-818-354-0220 1-626-395-2147

11 years

Re: [Bicep2-list] ***SPAM*** Planck ESLAB slides

by Clem Pryke

In Aumont slide 9 C_l^BB=0.1 uK^2 @ 350GHz, ell=100 and 70% sky. For 30% of sky the value is factor 10 lower. Reading off slide 12 @ 350x353 I get the same numerical value for 70% sky - which is odd as the y-axis label now says C_l/2pi. So I think one of the axis labels may be incorrect. Based on the r=0.1 curve I think it is this plot which is wrong. So if we take the 143x143 curve and scale it down by factor 10 based on slide 9 we have dust BB kissing the r=0.1 line for 30% sky. This doesn't seem too good for us. Of course these plots all have some component separation in effect - a model of the CMB has been subtracted as it says in slide 4. But for BB this model presumably does very little - we see sensible black body behavior of the inferred dust spectrum all the way down to 143GHz in the lower right panel of slide 12. Clem -- ********************************************************************** Clem Pryke - Associate Professor - Physics University of Minnesota, Room 313 Tate, 116 Church Street S.E. Minneapolis, MN, 55455 Tel: 612-624-7578 Fax: 612-624-4578 email: pryke(a)physics.umn.edu **********************************************************************

11 years

Last week's collaboration meeting: thanks to all, and especially Irene and Sam

by John Kovac

Dear all, I'd like to thank each of you for contributing to the BICEP2 and Keck Array collaboration meeting. Last week turned out to be a difficult one here in Boston, and the effort you all put into preparing substantive discussions, and the flexibility shown, particularly with our mega-telecon during Friday's lockdown, contributed to a very effective meeting nonetheless. I think huge progress for BICEP2 analysis and Keck planning has come out of what we reviewed. Thanks to all of you who led discussions and who took notes, and particularly to Immanuel for keeping track of the agenda and schedule and to Kirit and Jon for setting up the google hangout. Two people deserve special thanks, and Friday didn't give us a proper chance to do so in person: Irene Coyle, our Harvard group administrator, ran the meeting logistics beautifully, making sure everyone was housed, seated, fed, and caffeinated at all times. Sam Harrison, our engineer extraordinaire, set up the room, computers, wireless, phones, and photos. Sam had postponed the start date of his (very exciting) new position with Draper Labs just to be with us through last week's meeting. Please join with me in thanking Irene and Sam, and in wishing Sam the best of luck in his new position! John -- ___________________________________________________________________ John Kovac jmkovac(a)cfa.harvard.edu Assistant Professor, Astronomy and Physics, Harvard University 160 Concord Ave rm 310, Cambridge MA 02138, 617-496-0611

11 years

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Bicep2-list April 2013