Bicep3
is a 550-mm aperture telescope with cold, on-axis, refractive optics designed to observe at the 95-GHz band from the South Pole. It is the newest member of the
Bicep
/
Keck
family of ...inflationary probes specifically designed to measure the polarization of the cosmic microwave background (CMB) at degree angular scales.
Bicep3
is designed to house 1280 dual-polarization pixels, which, when fully populated, totals to
∼
9
×
the number of pixels in a single
Keck
95-GHz receiver, thus further advancing the
Bicep
/
Keck
program’s 95 GHz mapping speed.
Bicep3
was deployed during the austral summer of 2014–2015 with nine detector tiles, to be increased to its full capacity of 20 in the second season. After instrument characterization, measurements were taken, and CMB observation commenced in April 2015. Together with multi-frequency observation data from Planck,
Bicep2
, and the
Keck Array
,
Bicep3
is projected to set upper limits on the tensor-to-scalar ratio to
r
≲
0.03
at 95 % C.L.
Winner of the Association for Slavic, East European, and Eurasian Studies' Reginald Zelnik Book Prize in History. Through close study of Russian, Eurasian, and Central Asian ethnographic, ...administrative, literary, and missionary sources, this book shows how traditional Islamic education among the people of Tsarist Russia's Middle Volga region (today's Tatarstan) helped to Islamize the area's Turkic peoples, setting the stage for the development of modernist Islam in Russia. "Agnes Nilufer Kefeli's thorough and imaginative use of sources is notable. She makes use of Russian official sources from the State Archives of Tatarstan and elsewhere, but she also consults a broad range of nonarchival Islamic sources, including Tatar-language Arabic-script popular literature. This makes the book highly original and important to both Russian history and Islamic studies."—Allen Frank
We report the results of a joint analysis of data from BICEP2/Keck Array and Planck. BICEP2 and Keck Array have observed the same approximately 400 deg^{2} patch of sky centered on RA 0 h, Dec. ...-57.5°. The combined maps reach a depth of 57 nK deg in Stokes Q and U in a band centered at 150 GHz. Planck has observed the full sky in polarization at seven frequencies from 30 to 353 GHz, but much less deeply in any given region (1.2 μK deg in Q and U at 143 GHz). We detect 150×353 cross-correlation in B modes at high significance. We fit the single- and cross-frequency power spectra at frequencies ≥150 GHz to a lensed-ΛCDM model that includes dust and a possible contribution from inflationary gravitational waves (as parametrized by the tensor-to-scalar ratio r), using a prior on the frequency spectral behavior of polarized dust emission from previous Planck analysis of other regions of the sky. We find strong evidence for dust and no statistically significant evidence for tensor modes. We probe various model variations and extensions, including adding a synchrotron component in combination with lower frequency data, and find that these make little difference to the r constraint. Finally, we present an alternative analysis which is similar to a map-based cleaning of the dust contribution, and show that this gives similar constraints. The final result is expressed as a likelihood curve for r, and yields an upper limit r_{0.05}<0.12 at 95% confidence. Marginalizing over dust and r, lensing B modes are detected at 7.0σ significance.
Atrial fibrillation (AF) is common among hemodialysis (HD) patients and is associated with high mortality. P wave dispersion (PWD) is a noninvasive electrocardiographic marker of paroxysmal AF. Our ...aim was to evaluate the effect of HD session on PWD.
Twenty-five patients (mean age 63 years, 10 males) with sinus rhythm and undergoing chronic HD treatment were included. Blood samples were drawn and 12-lead electrocardiograms were recorded immediately before HD session, at the 2nd hour during HD and at the end of the HD session. The difference between maximum and minimum P wave durations was calculated as PWD.
PWD significantly increased during HD sessions compared with predialysis values (41 +/- 12 vs. 21 +/- 10 ms, respectively, p < 0.001), then decreased to a value of 24 +/- 7 ms at the completion of HD, which was not significantly different from the predialysis values. PWD during HD was significantly correlated with predialysis systolic and diastolic blood pressure (r = 0.42, p = 0.037, and r = 0.59, p = 0.002, respectively) and predialysis serum potassium level (r = 0.44, p = 0.031). Linear regression model revealed that predialysis diastolic blood pressure (p = 0.002), predialysis serum potassium level (p = 0.037) and the amount of ultrafiltration (p = 0.048) were the significant predictors of prolonged PWD during HD.
PWD increases significantly during HD sessions. This may increase the risk of AF episodes during HD. High diastolic blood pressure and serum potassium level before HD and ultrafiltration amount may predict prolonged PWD during HD.
ABSTRACT We present measurements of polarization lensing using the 150 GHz maps, which include all data taken by the BICEP2 and Keck Array Cosmic Microwave Background polarization experiments up to ...and including the 2014 observing season (BK14). Despite their modest angular resolution ( ), the excellent sensitivity (∼3 K-arcmin) of these maps makes it possible to directly reconstruct the lensing potential using only information at larger angular scales ( ). From the auto-spectrum of the reconstructed potential, we measure an amplitude of the spectrum to be (Planck ΛCDM prediction corresponds to ) and reject the no-lensing hypothesis at , which is the highest significance achieved to date using an EB lensing estimator. Taking the cross-spectrum of the reconstructed potential with the Planck 2015 lensing map yields . These direct measurements of are consistent with the ΛCDM cosmology and with that derived from the previously reported BK14 B-mode auto-spectrum ( ). We perform a series of null tests and consistency checks to show that these results are robust against systematics and are insensitive to analysis choices. These results unambiguously demonstrate that the B modes previously reported by BICEP/Keck at intermediate angular scales ( ) are dominated by gravitational lensing. The good agreement between the lensing amplitudes obtained from the lensing reconstruction and B-mode spectrum starts to place constraints on any alternative cosmological sources of B modes at these angular scales.
We present a constraint on the tensor-to-scalar ratio, r, derived from measurements of cosmic microwave background (CMB) polarization B-modes with "delensing," whereby the uncertainty on r ...contributed by the sample variance of the gravitational lensing B-modes is reduced by cross-correlating against a lensing B-mode template. This template is constructed by combining an estimate of the polarized CMB with a tracer of the projected large-scale structure. The large-scale-structure tracer used is a map of the cosmic infrared background derived from Planck satellite data, while the polarized CMB map comes from a combination of South Pole Telescope, bicep/Keck, and Planck data. We expand the bicep/Keck likelihood analysis framework to accept a lensing template and apply it to the bicep/Keck dataset collected through 2014 using the same parametric foreground modeling as in the previous analysis. From simulations, we find that the uncertainty on r is reduced by ∼10%, from σ(r)=0.024 to 0.022, which can be compared with a ∼26% reduction obtained when using a perfect lensing template or if there were zero lensing B-modes. Applying the technique to the real data, the constraint on r is improved from r0.05<0.090 to r0.05<0.082 (95% C.L.). This is the first demonstration of improvement in an r constraint through delensing.
ABSTRACT The Keck Array is a system of cosmic microwave background polarimeters, each similar to the Bicep2 experiment. In this paper we report results from the 2012 to 2013 observing seasons, during ...which the Keck Array consisted of five receivers all operating in the same (150 GHz) frequency band and observing field as Bicep2. We again find an excess of B-mode power over the lensed-ΛCDM expectation of >5 in the range 30 < < 150 and confirm that this is not due to systematics using jackknife tests and simulations based on detailed calibration measurements. In map difference and spectral difference tests these new data are shown to be consistent with Bicep2. Finally, we combine the maps from the two experiments to produce final Q and U maps which have a depth of 57 nK deg (3.4 K arcmin) over an effective area of 400 deg2 for an equivalent survey weight of 250,000 K−2. The final BB band powers have noise uncertainty a factor of 2.3 times better than the previous results, and a significance of detection of excess power of >6 .
ABSTRACT We have developed antenna-coupled transition-edge sensor bolometers for a wide range of cosmic microwave background (CMB) polarimetry experiments, including Bicep2, Keck Array, and the ...balloon borne Spider. These detectors have reached maturity and this paper reports on their design principles, overall performance, and key challenges associated with design and production. Our detector arrays repeatedly produce spectral bands with 20%-30% bandwidth at 95, 150, or 230 GHz. The integrated antenna arrays synthesize symmetric co-aligned beams with controlled side-lobe levels. Cross-polarized response on boresight is typically , consistent with cross-talk in our multiplexed readout system. End-to-end optical efficiencies in our cameras are routinely 35% or higher, with per detector sensitivities of NET ∼ 300 . Thanks to the scalability of this design, we have deployed 2560 detectors as 1280 matched pairs in Keck Array with a combined instantaneous sensitivity of , as measured directly from CMB maps in the 2013 season. Similar arrays have recently flown in the Spider instrument, and development of this technology is ongoing.
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