851 research outputs found
Semidirect product gauge group and quantization of hypercharge
In the Standard Model the hypercharges of quarks and leptons are not
determined by the gauge group alone. We show that, if we choose the semidirect product group
as its gauge group,
the hyperchages are settled to be . In
addition, the conditions for gauge-anomaly cancellation give strong
constraints. As a result, the ratios of the hypercharges are uniquely
determined and the gravitational anomaly is automatically canceled. The
standard charge assignment to quarks and leptons can be properly reproduced.
For exotic matter fields their hypercharges are also discussed.Comment: 17 pages, 2 tables; LaTeX; typos corrected, references added or
replaced, argument in Secs. 2 and 3 revised, results unchanged; to be
published in Phys. Rew.
NMR studies of the incommensurate helical antiferromagnet EuCo2P2 : determination of the antiferromagnetic propagation vector
Recently Ding et al. [Phys. Rev. B 95, 184404 (2017)] reported that their
nuclear magnetic resonance (NMR) study on EuCoAs successfully
characterized the antiferromagnetic (AFM) propagation vector of the
incommensurate helix AFM state, showing that NMR is a unique tool for
determination of the spin structures in incommensurate helical AFMs. Motivated
by this work, we have carried out Eu, P and Co NMR
measurements on the helical antiferromagnet EuCoP with an AFM ordering
temperature = 66.5 K. An incommensurate helical AFM structure was
clearly confirmed by Eu and P NMR spectra on single crystalline
EuCoP in zero magnetic field at 1.6 K and its external magnetic field
dependence. Furthermore, based on Co NMR data in both the paramagnetic
and the incommensurate AFM states, we have determined the model-independent
value of the AFM propagation vector k = (0, 0, 0.73 0.09)2/ where
is the -axis lattice parameter. The temperature dependence of k is also
discussed.Comment: 8 pages, 10 figures, accepted for publication in Phys. Rev. B. arXiv
admin note: substantial text overlap with arXiv:1704.0629
New Improved Photometric Redshifts of Galaxies in the HDF
We report new improved photometric redshifts of 1048 galaxies in the Hubble
Deep Field (HDF). A standard chi^2 minimizing method is applied to seven-color
UBVIJHK photometry by Fernandez-Soto, Lanzetta, & Yahil (1999). We use 187
template SEDs representing a wide variety of morphology and age of observed
galaxies based on a population synthesis model by Kodama & Arimoto (1997). We
introduce two new recipes. First, the amount of the internal absorption is
changed as a free parameter in the range of E(B-V)=0.0 to 0.5 with an interval
of 0.1. Second, the absorption due to intergalactic HI clouds is also changed
by a factor of 0.5, 1.0, and 1.5 around the opacity given by Madau (1995). The
total number of template SEDs is thus 187x6x3=3,366, except for the redshift
grid. The dispersion sigma_z of our photometric redshifts with respect to
spectroscopic redshifts is sigma_z=0.08 and 0.24 for z2, respectively,
which are smaller than the corresponding values (sigma_z=0.09 and 0.45) by
Fernandez-Soto et al. Improvement is significant, especially in z>2. This is
due to smaller systematic errors which are largely reduced mainly by including
three opacities due to intergalactic HI clouds. We discuss redshift
distribution N(z) and cosmic star formation rate based on our new photometric
redshifts.Comment: 24 pages including 16 eps figures; accepted for publication in Ap
Dirac-Surface-State Modulated Spin Dynamics in a Ferrimagnetic Insulator at Room Temperature
This work demonstrates dramatically modified spin dynamics of magnetic
insulator (MI) by the spin-momentum locked Dirac surface states of the adjacent
topological insulator (TI) which can be harnessed for spintronic applications.
As the Bi-concentration x is systematically tuned in 5 nm thick (BixSb1-x)2Te3
TI film, the weight of the surface relative to bulk states peaks at x = 0.32
when the chemical potential approaches the Dirac point. At this concentration,
the Gilbert damping constant of the precessing magnetization in 10 nm thick
Y3Fe5O12 MI film in the MI/TI heterostructures is enhanced by an order of
magnitude, the largest among all concentrations. In addition, the MI acquires
additional strong magnetic anisotropy that favors the in-plane orientation with
similar Bi-concentration dependence. These extraordinary effects of the Dirac
surface states distinguish TI from other materials such as heavy metals in
modulating spin dynamics of the neighboring magnetic layer
The Optical/Near-Infrared Light Curves of SN 2002ap for the First 140 Days after Discovery
Supernova (SN) 2002ap in M74 was observed in the bands for the
first 40 days following its discovery (2002 January 29) until it disappeared
because of solar conjunction, and then in June after it reappeared. The
magnitudes and dates of peak brightness in each band were determined. While the
rate of increase of the brightness before the peak is almost independent of
wavelength, the subsequent rate of decrease becomes smaller with wavelength
from the to the band, and is constant at wavelengths beyond . The
photometric evolution is faster than in the well-known ``hypernovae''
SNe~1998bw and 1997ef, indicating that SN 2002ap ejected less mass. The
bolometric light curve of SN 2002ap for the full period of observations was
constructed. The absolute magnitude is found to be much fainter than that of SN
1998bw, but is similar to that of SN 1997ef, which lies at the faint end of the
hypernova population. The bolometric light curve at the early epochs was best
reproduced with the explosion of a C+O star that ejects 2.5~M_\sun with
kinetic energy . A comparison of the
predicted brightness of SN 2002ap with that observed after solar conjunction
may imply that -ray deposition at the later epochs was more efficient
than in the model. This may be due to an asymmetric explosion.Comment: 15 pages, 6 figures, quality of figure1 is reduced for smaller
filesize, accepted for publication in Ap
A Discovery of Rapid Optical Flares from Low-Luminosity Active Nuclei in Massive Galaxies
We report a serendipitous discovery of six very low-luminosity active
galactic nuclei (AGNs) only by optical variability in one-month baseline. The
detected flux variability is ~ 1-5% of the total luminosity of host galaxies.
Careful subtraction of host galaxy components in nuclear regions indicates that
the fractional variability (Delta F / F) of the nuclei is of order unity. At
least one of them is showing a compelling flaring activity within just a few
days, which appears to be quite different from previously known AGN
variability. We obtained spectroscopic data for the one showing the largest
flare and confirmed that it is in fact an AGN at z = 0.33 with an estimated
black hole mass of ~10^8 M_sun. As a possible interpretation, we suggest that
these activities are coming from the region around the black hole event
horizon, which is physically similar to the recently discovered near-infrared
flares of our Galactic nucleus. It is indicated that our Galaxy is not special,
and that surprisingly rapid flaring activity in optical/near-infrared bands may
be commonly hidden in nuclei of apparently normal galaxies with low Eddington
ratios, in contrast to the variability of well-studied luminous AGNs or
quasars.Comment: Accepted to ApJ Letter
Photometric Response Functions of the SDSS Imager
The monochromatic illumination system is constructed to carry out in situ
measurements of the response function of the mosaicked CCD imager used in the
Sloan Digital Sky Survey (SDSS). The system is outlined and the results of the
measurements, mostly during the first 6 years of the SDSS, are described. We
present the reference response functions for the five colour passbands derived
from these measurements, and discuss column to column variations and variations
in time, and also their effects on photometry. We also discuss the effect
arising from various, slightly different response functions of the associated
detector systems that were used to give SDSS photometry. We show that the
calibration procedures of SDSS remove these variations reasonably well with the
resulting final errors from variant response functions being unlikely to be
larger than 0.01 mag for g, r, i, and z bands over the entire duration of the
survey. The considerable aging effect is uncovered in the u band, the response
function showing a 30% decrease in the throughput in the short wavelength side
during the survey years, which potentially causes a systematic error in
photometry. The aging effect is consistent with variation of the instrumental
sensitivity in u-band, which is calibrated out. The expected colour variation
is consistent with measured colour variation in the catalog of repeated
photometry. The colour variation is delta (u-g) ~ 0.01 for most stars, and at
most delta (u-g) ~ 0.02 mag for those with extreme colours. We verified in the
final catalogue that no systematic variations in excess of 0.01 mag are
detected in the photometry which can be ascribed to aging and/or seasonal
effects except for the secular u-g colour variation for stars with extreme
colours.Comment: 54 pages, 18 figures, 7 tables, accepted for publication in A
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