470 research outputs found
Hidden itinerant-spin phase in heavily-overdoped La2-xSrxCuO4 revealed by dilute Fe doping: A combined neutron scattering and angle-resolved photoemission study
We demonstrated experimentally a direct way to probe a hidden propensity to
the formation of spin density wave (SDW) in a non-magnetic metal with strong
Fermi surface nesting. Substituting Fe for a tiny amount of Cu (1%) induced an
incommensurate magnetic order below 20 K in heavily-overdoped La2-xSrxCuO4
(LSCO). Elastic neutron scattering suggested that this order cannot be ascribed
to the localized spins on Cu or doped Fe. Angle-resolved photoemission
spectroscopy (ARPES), combined with numerical calculations, revealed a strong
Fermi surface nesting inherent in the pristine LSCO that likely drives this
order. The heavily-overdoped Fe-doped LSCO thus represents the first plausible
example of the long-sought "itinerant-spin extreme" of cuprates, where the
spins of itinerant doped holes define the magnetic ordering ground state. This
finding complements the current picture of cuprate spin physics that highlights
the predominant role of localized spins at lower dopings. The demonstrated set
of methods could potentially apply to studying hidden density-wave
instabilities of other "nested" materials on the verge of density wave
ordering.Comment: Abstract and discussion revised; to appear in Phys. Rev. Let
Novel electronic wave interference patterns in nanographene sheets
Superperiodic patterns with a long distance in a nanographene sheet observed
by STM are discussed in terms of the interference of electronic wave functions.
The period and the amplitude of the oscillations decrease spatially in one
direction. We explain the superperiodic patterns with a static linear potential
theoretically. In the k-p model, the oscillation period decreases, and agrees
with experiments. The spatial difference of the static potential is estimated
as 1.3 eV for 200 nm in distance, and this value seems to be reasonable in
order that the potential difference remains against perturbations, for example,
by phonon fluctuations and impurity scatterings. It turns out that the
long-distance oscillations come from the band structure of the two-dimensional
graphene sheet.Comment: Published as a LETTER in J. Phys.: Condens. Matter; 8 pages; 6
figures; Online version at
http://www.iop.org/EJ/S/3/1256/0hJAmc5sCL6d.7sOO.BtLw/abstract/0953-8984/14/3
6/10
The Quasar-LBG Two-point Angular Cross-correlation Function at z ~ 4 in the COSMOS Field
In order to investigate the origin of quasars, we estimate the bias factor
for low-luminosity quasars at high redshift for the first time. In this study,
we use the two-point angular cross-correlation function (CCF) for both
low-luminosity quasars at and Lyman-break galaxies
(LBGs). Our sample consists of both 25 low-luminosity quasars (16 objects are
spectroscopically confirmed low-luminosity quasars) in the redshift range
and 835 color-selected LBGs with at
in the COSMOS field. We have made our analysis for the following two
quasar samples; (1) the spectroscopic sample (the 16 quasars confirmed by
spectroscopy), and (2) the total sample (the 25 quasars including 9 quasars
with photometric redshifts). The bias factor for low-luminosity quasars at
is derived by utilizing the quasar-LBG CCF and the LBG
auto-correlation function. We then obtain the upper limits of the bias
factors for low-luminosity quasars, that are 5.63 and 10.50 for the total and
the spectroscopic samples, respectively. These bias factors correspond to the
typical dark matter halo masses, log
and , respectively. This result is not inconsistent with the predicted
bias for quasars which is estimated by the major merger models.Comment: 13 pages, 9 figures, Accepted for publication in Ap
Constraints on the faint end of the quasar luminosity function at z~5 in the COSMOS field
We present the result of our low-luminosity quasar survey in the redshift
range of 4.5 < z < 5.5 in the COSMOS field. Using the COSMOS photometric
catalog, we selected 15 quasar candidates with 22 < i' < 24 at z~5, that are ~
3 mag fainter than the SDSS quasars in the same redshift range. We obtained
optical spectra for 14 of the 15 candidates using FOCAS on the Subaru Telescope
and did not identify any low-luminosity type-1 quasars at z~5 while a
low-luminosity type-2 quasar at z~5.07 was discovered. In order to constrain
the faint end of the quasar luminosity function at z~5, we calculated the
1sigma confidence upper limits of the space density of type-1 quasars. As a
result, the 1sigma confidence upper limits on the quasar space density are Phi<
1.33*10^{-7} Mpc^{-3} mag^{-1} for -24.52 < M_{1450} < -23.52 and Phi<
2.88*10^{-7} Mpc^{-3} mag^{-1} for -23.52 < M_{1450} < -22.52. The inferred
1sigma confidence upper limits of the space density are then used to provide
constrains on the faint-end slope and the break absolute magnitude of the
quasar luminosity function at z~5. We find that the quasar space density
decreases gradually as a function of redshift at low luminosity (M_{1450} ~
-23), being similar to the trend found for quasars with high luminosity
(M_{1450}<-26). This result is consistent with the so-called downsizing
evolution of quasars seen at lower redshifts.Comment: 8 pages, 9 figures, 1 table, accepted for publication in Ap
Numerical Galaxy Catalog -I. A Semi-analytic Model of Galaxy Formation with N-body simulations
We construct the Numerical Galaxy Catalog (GC), based on a semi-analytic
model of galaxy formation combined with high-resolution N-body simulations in a
-dominated flat cold dark matter (CDM) cosmological model.
The model includes several essential ingredients for galaxy formation, such as
merging histories of dark halos directly taken from N-body simulations,
radiative gas cooling, star formation, heating by supernova explosions
(supernova feedback), mergers of galaxies, population synthesis, and extinction
by internal dust and intervening HI clouds. As the first paper in a series
using this model, we focus on basic photometric, structural and kinematical
properties of galaxies at present and high redshifts. Two sets of model
parameters are examined, strong and weak supernova feedback models, which are
in good agreement with observational luminosity functions of local galaxies in
a range of observational uncertainty. Both models agree well with many
observations such as cold gas mass-to-stellar luminosity ratios of spiral
galaxies, HI mass functions, galaxy sizes, faint galaxy number counts and
photometric redshift distributions in optical pass-bands, isophotal angular
sizes, and cosmic star formation rates. In particular, the strong supernova
feedback model is in much better agreement with near-infrared (K'-band) faint
galaxy number counts and redshift distribution than the weak feedback model and
our previous semi-analytic models based on the extended Press-Schechter
formalism. (Abridged)Comment: 26 pages including 27 figures, accepted for publication in ApJ,
full-resolution version is available at
http://grape.astron.s.u-tokyo.ac.jp/~yahagi/nugc
Hierarchical Formation of Galaxies with Dynamical Response to Supernova-Induced Gas removal
We reanalyze the formation and evolution of galaxies in the hierarchical
clustering scenario. Using a semi-analytic model (SAM) of galaxy formation
described in this paper, which we hereafter call the Mitaka model, we
extensively investigate the observed scaling relations of galaxies among
photometric, kinematic, structural and chemical characteristics. In such a
scenario, spheroidal galaxies are assumed to be formed by major merger and
subsequent starburst, in contrast to the traditional scenario of monolithic
cloud collapse. As a new ingredient of SAMs, we introduce the effects of
dynamical response to supernova-induced gas removal on size and velocity
dispersion, which play an important role on dwarf galaxy formation. In previous
theoretical studies of dwarf galaxies based on the monolithic cloud collapse
given by Yoshii & Arimoto and Dekel & Silk, the dynamical response was treated
in the extremes of a purely baryonic cloud and a baryonic cloud fully supported
by surrounding dark matter. To improve this simple treatment, in our previous
paper, we formulated the dynamical response in more realistic, intermediate
situations between the above extremes. While the effects of dynamical response
depend on the mass fraction of removed gas from a galaxy, how much amount of
the gas remains just after major merger depends on the star formation history.
A variety of star formation histories are generated through the Monte Carlo
realization of merging histories of dark halos, and it is found that our SAM
naturally makes a wide variety of dwarf galaxies and their dispersed
characteristics as observed. (Abridged)Comment: 24 pages including 29 figures, using emulateapj.cls; accepted for
publication in Ap
The Hyper Suprime-Cam SSP Survey: Overview and Survey Design
Hyper Suprime-Cam (HSC) is a wide-field imaging camera on the prime focus of
the 8.2m Subaru telescope on the summit of Maunakea in Hawaii. A team of
scientists from Japan, Taiwan and Princeton University is using HSC to carry
out a 300-night multi-band imaging survey of the high-latitude sky. The survey
includes three layers: the Wide layer will cover 1400 deg in five broad
bands (), with a point-source depth of . The
Deep layer covers a total of 26~deg in four fields, going roughly a
magnitude fainter, while the UltraDeep layer goes almost a magnitude fainter
still in two pointings of HSC (a total of 3.5 deg). Here we describe the
instrument, the science goals of the survey, and the survey strategy and data
processing. This paper serves as an introduction to a special issue of the
Publications of the Astronomical Society of Japan, which includes a large
number of technical and scientific papers describing results from the early
phases of this survey.Comment: 14 pages, 7 figures, 5 tables. Corrected for a typo in the
coordinates of HSC-Wide spring equatorial field in Table
STM observation of electronic wave interference effect in finite-sized graphite with dislocation-network structures
Superperiodic patterns near a step edge were observed by STM on
several-layer-thick graphite sheets on a highly oriented pyrolitic graphite
substrate, where a dislocation network is generated at the interface between
the graphite overlayer and the substrate. Triangular- and rhombic-shaped
periodic patterns whose periodicities are around 100 nm were observed on the
upper terrace near the step edge. In contrast, only outlines of the patterns
similar to those on the upper terrace were observed on the lower terrace. On
the upper terrace, their geometrical patterns gradually disappeared and became
similar to those on the lower terrace without any changes of their periodicity
in increasing a bias voltage. By assuming a periodic scattering potential at
the interface due to dislocations, the varying corrugation amplitudes of the
patterns can be understood as changes in LDOS as a result of the beat of
perturbed and unperturbed waves, i.e. the interference in an overlayer. The
observed changes in the image depending on an overlayer height and a bias
voltage can be explained by the electronic wave interference in the ultra-thin
overlayer distorted under the influence of dislocation-network structures.Comment: 8 pages; 6 figures; Paper which a part of cond-mat/0311068 is
disscussed in detai
Superconductivity in the Intercalated Graphite Compounds C6Yb and C6Ca
In this letter we report the discovery of superconductivity in the
isostructural graphite intercalation compounds C6Yb and C6Ca, with transition
temperatures of 6.5K and 11.5K respectively. A structural characterisation of
these compounds shows them to be hexagonal layered systems in the same class as
other graphite intercalates. If we assume that all the outer s-electrons are
transferred from the intercalant to the graphite sheets, then the charge
transfer in these compounds is comparable to other superconducting graphite
intercalants such as C8K 1,2 . However, the superconducting transition
temperatures of C6Yb and C6Ca are up to two orders of magnitude greater.
Interestingly, superconducting upper critical field studies and resistivity
measurements suggest that these compounds are significantly more isotropic than
pure graphite. This is unexpected as the effect of introducing the intercalant
is to move the graphite layer further apart.Comment: 2 Figures. Please see accompanying theoretical manuscript,
"Electronic Structure of the Superconducting Graphite Intercalates" by Csanyi
et al., cond-mat/050356
Charge ordering and antiferromagnetic exchange in layered molecular crystals of the theta type
We consider the electronic properties of layered molecular crystals of the
type theta-DA, where A is an anion and D is a donor molecule such as
BEDT-TTF [where BEDT-TTF is bis-(ethylenedithia-tetrathiafulvalene)] which is
arranged in the theta type pattern within the layers. We argue that the
simplest strongly correlated electron model that can describe the rich phase
diagram of these materials is the extended Hubbard model on the square lattice
at a quarter filling. In the limit where the Coulomb repulsion on a single site
is large, the nearest-neighbour Coulomb repulsion, V, plays a crucial role.
When V is much larger than the intermolecular hopping integral t the ground
state is an insulator with charge ordering. In this phase antiferromagnetism
arises due to a novel fourth-order superexchange process around a plaquette on
the square lattice. We argue that the charge ordered phase is destroyed below a
critical non-zero value V, of the order of t. Slave boson theory is used to
explicitly demonstrate this for the SU(N) generalisation of the model, in the
large N limit. We also discuss the relevance of the model to the all-organic
family beta''-(BEDT-TTF)SFYSO where Y = CHCF, CH, CHF.Comment: 15 pages, 6 eps figure
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