We report a measurement of the E-mode polarization power spectrum of the cosmic microwave background (CMB) using 150 GHz data taken from 2014 July to 2016 December with the Polarbear experiment. We ...reach an effective polarization map noise level of - across an observation area of 670 square degrees. We measure the EE power spectrum over the angular multipole range , tracing the third to seventh acoustic peaks with high sensitivity. The statistical uncertainty on E-mode bandpowers is ∼2.3 at , with a systematic uncertainty of 0.5 . The data are consistent with the standard ΛCDM cosmological model with a probability-to-exceed of 0.38. We combine recent CMB E-mode measurements and make inferences about cosmological parameters in ΛCDM as well as in extensions to ΛCDM. Adding the ground-based CMB polarization measurements to the Planck data set reduces the uncertainty on the Hubble constant by a factor of 1.2 to . When allowing the number of relativistic species ( ) to vary, we find , which is in good agreement with the standard value of 3.046. Instead allowing the primordial helium abundance ( ) to vary, the data favor . This is very close to the expectation of 0.2467 from big bang nucleosynthesis. When varying both and , we find and .
The Allee effect is a positive relationship between any component of individual fitness and the density of conspecifics. Theoretical models predict that monogamy, where males and females are ...constrained from having multiple mates, is more susceptible to the Allee effect. In most termite species, including
Reticulitermes
spp., found new colonies by monogamous pairs (i.e., primary king and queen); however, little is known about the effects of alate density and flight timing on pairing and colony foundation success. In this study, a positive relationship between alate density and pairing success was observed in the subterranean termite,
Reticulitermes speratus
. Upon release of dealates (individuals after shedding wings) every 3 days for 9 days at 10, 20, 40, or 80 pairs/m
2
/day in a semi-natural field, no pairs were observed for the 10 pairs/m
2
/day treatment after 3 months. However, 7.5, 13.8, and 18.1% of dealates formed pairs in the 20, 40, and 80 pairs/m
2
/day groups, respectively. Most pairs (78.7%) comprised dealates released simultaneously, and 17.3 and 4% comprised dealates released 3 and 6 days apart, respectively.
R. speratus
also preferred brown rotten pine for colony foundations to white rotten oak. This study provides important new insights into the density effects and nest-site preference for termite colony foundation.
We present a measurement of the gravitational lensing deflection power spectrum reconstructed with two seasons of cosmic microwave background polarization data from the Polarbear experiment. ...Observations were taken at 150 GHz from 2012 to 2014 and surveyed three patches of sky totaling 30 square degrees. We test the consistency of the lensing spectrum with a cold dark matter cosmology and reject the no-lensing hypothesis at a confidence of 10.9 , including statistical and systematic uncertainties. We observe a value of AL = 1.33 0.32 (statistical) 0.02 (systematic) 0.07 (foreground) using all polarization lensing estimators, which corresponds to a 24% accurate measurement of the lensing amplitude. Compared to the analysis of the first-year data, we have improved the breadth of both the suite of null tests and the error terms included in the estimation of systematic contamination.
We present a measurement of the B-mode polarization power spectrum of the cosmic microwave background (CMB) using data taken from 2014 July to 2016 December with the Polarbear experiment. The CMB ...power spectra are measured using observations at 150 GHz with an instantaneous array sensitivity of on a 670 square degree patch of sky centered at (R.A., decl.) = (+0h12m0s, −59°18′). A continuously rotating half-wave plate is used to modulate polarization and to suppress low-frequency noise. We achieve 32 K arcmin effective polarization map noise with a knee in sensitivity of = 90, where the inflationary gravitational-wave signal is expected to peak. The measured B-mode power spectrum is consistent with a ΛCDM lensing and single dust component foreground model over a range of multipoles 50 ≤ ≤ 600. The data disfavor zero at 2.2 using this range of Polarbear data alone. We cross-correlate our data with Planck full mission 143, 217, and 353 GHz frequency maps and find the low- B-mode power in the combined data set to be consistent with thermal dust emission. We place an upper limit on the tensor-to-scalar ratio r < 0.90 at the 95% confidence level after marginalizing over foregrounds.
Background
Hyaluronan (HA) is an important constituent of extracellular matrix (ECM) in the skin, and HA degradation mediated by HYBID (KIAA1199) is suggested to be implicated in facial skin ...wrinkling in Japanese women. Ethnic difference in skin wrinkle formation is known between Caucasian and Japanese women, but no information is available for the relations of HA and HYBID expression levels with skin wrinkling in Caucasian women.
Methods
The skin surface roughness at the eye corner of the Caucasian female subjects was measured, and the skin specimens biopsied from the same areas were subjected to microarray gene analysis, HA staining, and immunohistochemistry for HYBID.
Results
Among the ECM genes and those related to ECM metabolism, only HYBID expression levels positively correlated with the skin roughness parameters. When the skin sample groups with high expression of HYBID or low expression of HYBID were compared, the HA staining intensity and the ratio of HYBID‐immunoreactive cells to total cells in the superficial dermis were significantly reduced and increased in the high‐HYBID‐expression group compared with the low‐HYBID‐expression group, respectively.
Conclusion
Our data suggest that like Japanese women, HYBID‐mediated reduction of HA in the superficial dermis is involved in the formation of wrinkles in Caucasian women.
We present an overview of the design and status of the
Polarbear
-2 and the Simons Array experiments.
Polarbear
-2 is a cosmic microwave background polarimetry experiment which aims to characterize ...the arc-minute angular scale B-mode signal from weak gravitational lensing and search for the degree angular scale B-mode signal from inflationary gravitational waves. The receiver has a 365 mm diameter focal plane cooled to 270 mK. The focal plane is filled with 7588 dichroic lenslet–antenna-coupled polarization sensitive transition edge sensor (TES) bolometric pixels that are sensitive to 95 and 150 GHz bands simultaneously. The TES bolometers are read-out by SQUIDs with 40 channel frequency domain multiplexing. Refractive optical elements are made with high-purity alumina to achieve high optical throughput. The receiver is designed to achieve noise equivalent temperature of 5.8
μ
K
CMB
s
in each frequency band.
Polarbear
-2 will deploy in 2016 in the Atacama desert in Chile. The Simons Array is a project to further increase sensitivity by deploying three
Polarbear
-2 type receivers. The Simons Array will cover 95, 150, and 220 GHz frequency bands for foreground control. The Simons Array will be able to constrain tensor-to-scalar ratio and sum of neutrino masses to
σ
(
r
)
=
6
×
10
-
3
at
r
=
0.1
and
∑
m
ν
(
σ
=
1
)
to 40 meV.
This study focuses on kinetic inductance detectors (KIDs) fabricated in external foundries using 6 and 8-inch processes. These processes allow us to fabricate large arrays of KIDs in a scalable ...manner. The support of such a wide variety of astronomical and particle-physics applications requires large numbers of superconducting detectors. For example, the sensitivity of the cosmic microwave background measurements has exponentially improved over the past few decades. The most significant advantage of KIDs is scalability to a large array due to the intrinsic frequency multiplexing scheme. The first step of fabricating a large array of KIDs is designing test chips to check the performance of the 6 and 8-inch micro-electro-mechanical system processes. The KIDs are made of a single pure aluminum film and consist of coplanar waveguide quarter wavelength resonators with a feedline. Each wafer is filled with 32 chips, where the chip size is 20 × 20 mm
2
, with 48 resonators on each chip. The chips are evaluated using a dilution refrigerator at temperatures ranging from 100 to 500 mK. The quality factor of the resonators, temperature dependency of the resonance frequency, and yields are comparable with those of the KIDs fabricated in a dedicated clean room for superconducting detectors.
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