2,148 research outputs found
Non-parametric strong lens inversion of SDSS J1004+4112
In this article we study the well-known strong lensing system SDSS
J1004+4112. Not only does it host a large-separation lensed quasar with
measured time-delay information, but several other lensed galaxies have been
identified as well. A previously developed strong lens inversion procedure that
is designed to handle a wide variety of constraints, is applied to this lensing
system and compared to results reported in other works. Without the inclusion
of a tentative central image of one of the galaxies as a constraint, we find
that the model recovered by the other constraints indeed predicts an image at
that location. An inversion which includes the central image provides tighter
constraints on the shape of the central part of the mass map. The resulting
model also predicts a central image of a second galaxy where indeed an object
is visible in the available ACS images. We find masses of 2.5x10^13 M_O and
6.1x10^13 M_O within a radius of 60 kpc and 110 kpc respectively, confirming
the results from other authors. The resulting mass map is compatible with an
elliptical generalization of a projected NFW profile, with r_s = 58_{-13}^{+21}
arcsec and c_vir = 3.91 +/- 0.74. The orientation of the elliptical NFW profile
follows closely the orientation of the central cluster galaxy and the overall
distribution of cluster members.Comment: 11 pages, accepted for publication in MNRA
Probing the extended non-Fermi liquid regimes of MnSi and Fe
Recent studies show that the non-Fermi liquid (NFL) behavior of MnSi and Fe
spans over an unexpectedly broad pressure range, between the critical pressure
p_c and around 2p_c. In order to determine the extension of their NFL regions,
we analyze the evolution of the resistivity rho(T) A(p)T^n at higher pressures.
We find that in MnSi the n=3/2 exponent holds below 4.8 GPa=3 p_c, but it
increases above that pressure. At 7.2 GPa we observe the low temperature Fermi
liquid exponent n=2 whereas for T>1.5 K, n=5/3. Our measurements in Fe show
that the NFL behavior rho T^{5/3} extends at least up to 30.5 GPa, above the
entire superconducting (SC) region. In the studied pressure range, the onset of
the SC transition reduces by a factor 10 down to T_c^onset(30.5 GPa)=0.23 K,
while the A-coefficient diminishes monotonically by around 50%.Comment: 2 pages, 2 figures, Proceedings SCES 200
The final candidate from the JVAS/CLASS search for 6 arcsec to 15 arcsec image separation lensing
A search for 6 arcsec to 15 arcsec image separation lensing in the Jodrell
Bank-Very Large Array Astrometric Survey (JVAS) and the Cosmic Lens All-Sky
Survey (CLASS) by Phillips et al. found thirteen group and cluster
gravitational lens candidates. Through radio and optical imaging and
spectroscopy, Phillips et al. ruled out the lensing hypothesis for twelve of
the candidates. In this paper, new optical imaging and spectroscopy of
J0122+427, the final lens candidate from the JVAS/CLASS 6 arcsec to 15 arcsec
image separation lens search, are presented. This system is found not to be a
gravitational lens, but is just two radio-loud active galactic nuclei that are
separated by ~10 arcsec on the sky and are at different redshifts. Therefore,
it is concluded that there are no gravitational lenses in the JVAS and CLASS
surveys with image separations between 6 arcsec to 15 arcsec. This result is
consistent with the expectation that group- and cluster-scale dark matter
haloes are inefficient lenses due to their relatively flat inner density
profiles.Comment: 5 pages, 3 figures, 2 tables, accepted for publication in MNRA
The Rewards of Patience: An 822 Day Time Delay in the Gravitational Lens SDSS J1004+4112
We present 107 new epochs of optical monitoring data for the four brightest
images of the gravitational lens SDSS J1004+4112 observed between October 2006
and June 2007. Combining this data with the previously obtained light curves,
we determine the time delays between images A, B and C. We confirm our previous
measurement finding that A leads B by dt_BA=40.6+-1.8 days, and find that image
C leads image A by dt_CA=821.6+-2.1 days. The lower limit on the remaining
delay is that image D lags image A by dt_AD>1250 days. Based on the
microlensing of images A and B we estimate that the accretion disk size at a
rest wavelength of 2300 angstrom is 10^{14.8+-0.3} cm for a disk inclination of
cos{i}=1/2, which is consistent with the microlensing disk size-black hole mass
correlation function given our estimate of the black hole mass from the MgII
line width of logM_BH/M_sun=8.44+-0.14. The long delays allow us to fill in the
seasonal gaps and assemble a continuous, densely sampled light curve spanning
5.7 years whose variability implies a structure function with a logarithmic
slope of gamma = 0.35+-0.02. As C is the leading image, sharp features in the C
light curve can be intensively studied 2.3 years later in the A/B pair,
potentially allowing detailed reverberation mapping studies of a quasar at
minimal cost.Comment: Submitted to ApJ, 12 pages, 3 figure
Electron-phonon interaction in the t-J model
We derive a t-J model with electron-phonon coupling from the three-band
model, considering modulation of both hopping and Coulomb integrals by phonons.
While the modulation of the hopping integrals dominates, the modulation of the
Coulomb integrals cannot be neglected. The model explains the experimentally
observed anomalous softening of the half-breathing mode upon doping and a
weaker softening of the breathing mode. It is shown that other phonons are not
strongly influenced, and, in particular, the coupling to a buckling mode is not
strong in this model.Comment: 4 pages, RevTeX, 3 eps figures; final version with minor correction
Critical Temperature and Condensate Fraction of a Fermion Pair Condensate
We report on measurements of the critical temperature and the temperature
dependence of the condensate fraction for a fermion pair condensate of 6Li
atoms. The Bragg spectroscopy is employed to determine the critical temperature
and the condensate fraction after a fast magnetic field ramp to the molecular
side of the Feshbach resonance. Our measurements reveal the level-off of the
critical temperature and the limiting behavior of condensate fraction near the
unitarity limit
The Sloan Digital Sky Survey Quasar Lens Search. IV. Statistical Lens Sample from the Fifth Data Release
We present the second report of our systematic search for strongly lensed
quasars from the data of the Sloan Digital Sky Survey (SDSS). From extensive
follow-up observations of 136 candidate objects, we find 36 lenses in the full
sample of 77,429 spectroscopically confirmed quasars in the SDSS Data Release
5. We then define a complete sample of 19 lenses, including 11 from our
previous search in the SDSS Data Release 3, from the sample of 36,287 quasars
with i<19.1 in the redshift range 0.6<z<2.2, where we require the lenses to
have image separations of 1"<\theta<20" and i-band magnitude differences
between the two images smaller than 1.25 mag. Among the 19 lensed quasars, 3
have quadruple-image configurations, while the remaining 16 show double images.
This lens sample constrains the cosmological constant to be
\Omega_\Lambda=0.84^{+0.06}_{-0.08}(stat.)^{+0.09}_{-0.07}(syst.) assuming a
flat universe, which is in good agreement with other cosmological observations.
We also report the discoveries of 7 binary quasars with separations ranging
from 1.1" to 16.6", which are identified in the course of our lens survey. This
study concludes the construction of our statistical lens sample in the full
SDSS-I data set.Comment: 37 pages, 2 figures and 5 tables, accepted to A
Chandra Observations of SDSS J1004+4112: Constraints on the Lensing Cluster and Anomalous X-Ray Flux Ratios of the Quadruply Imaged Quasar
We present results from Chandra observations of SDSS J1004+4112, a strongly
lensed quasar system with a maximum image separation of 15". All four bright
images of the quasar, as well as resolved X-ray emission originating from the
lensing cluster, are clearly detected. The emission from the lensing cluster
extends out to approximately 1.5 arcmin. We measure the bolometric X-ray
luminosity and temperature of the lensing cluster to be 4.7e44 erg s^-1 and 6.4
keV, consistent with the luminosity-temperature relation for distant clusters.
The mass estimated from the X-ray observation shows excellent agreement with
the mass derived from gravitational lensing. The X-ray flux ratios of the
quasar images differ markedly from the optical flux ratios, and the combined
X-ray spectrum of the images possesses an unusually strong Fe Kalpha emission
line, both of which are indicative of microlensing.Comment: 9 pages, 5 figures. Accepted for publication in ApJ. Version with
high-quality color figures at
http://cosmic.riken.jp/ota/publications/index.htm
Measuring Microlensing using Spectra of Multiply Lensed Quasars
We report on a program of spectroscopic observations of
gravitationally-lensed QSOs with multiple images. We seek to establish whether
microlensing is occurring in each QSO image using only single-epoch
observations. We calculate flux ratios for the cores of emission lines in image
pairs to set a baseline for no microlensing. The offset of the continuum flux
ratios relative to this baseline yields the microlensing magnification free
from extinction, as extinction affects the continuum and the lines equally.
When we find chromatic microlensing, we attempt to constrain the size of the
QSO accretion disk. SDSSJ1004+4112 and HE1104-1805 show chromatic microlensing
with amplitudes and mag,
respectively. Modeling the accretion disk with a Gaussian source () of size and using magnification maps
to simulate microlensing we find ) and for SDSS1004+4112, and
) and
for HE1104-1805. For SDSSJ1029+2623 we find strong chromaticity
of mag in the continuum flux ratio, which probably arises from
microlensing although not all the available data fit within this explanation.
For Q0957+561 we measure B-A magnitude differences of 0.4 mag, much greater
than the 0.05 mag amplitude usually inferred from lightcurve variability.
It may substantially modify the current interpretations of microlensing in this
system, likely favoring the hypothesis of smaller sources and/or larger
microdeflectors. For HS0818+1227, our data yield posible evidence of
microlensing.Comment: 45pp, 17figs, ApJ accepted (june 4th 2012
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