529 research outputs found
Complementarity of dark matter detectors in light of the neutrino background
Direct detection dark matter experiments looking for WIMP-nucleus elastic
scattering will soon be sensitive to an irreducible background from neutrinos
which will drastically affect their discovery potential. Here we explore how
the neutrino background will affect future ton-scale experiments considering
both spin-dependent and spin-independent interactions. We show that combining
data from experiments using different targets can improve the dark matter
discovery potential due to target complementarity. We find that in the context
of spin-dependent interactions, combining results from several targets can
greatly enhance the subtraction of the neutrino background for WIMP masses
below 10 GeV/c and therefore probe dark matter models to lower
cross-sections. In the context of target complementarity, we also explore how
one can tune the relative exposures of different target materials to optimize
the WIMP discovery potential.Comment: 13 pages, 12 figures, 3 table
Microscopic interface phonon modes in structures of GaAs quantum dots embedded in AlAs shells
By means of a microscopic valence force field model, a series of novel
microscopic interface phonon modes are identified in shell quantum dots(SQDs)
composed of a GaAs quantum dot of nanoscale embedded in an AlAs shell of a few
atomic layers in thickness. In SQDs with such thin shells, the basic principle
of the continuum dielectric model and the macroscopic dielectric function are
not valid any more. The frequencies of these microscopic interface modes lie
inside the gap between the bulk GaAs band and the bulk AlAs band, contrary to
the macroscopic interface phonon modes. The average vibrational energies and
amplitudes of each atomic shell show peaks at the interface between GaAs and
AlAs. These peaks decay fast as their penetrating depths from the interface
increase.Comment: 13 pages, 4 figure
Divergence of Dipole Sums and the Nature of Non-Lorentzian Exponentially Narrow Resonances in One-Dimensional Periodic Arrays of Nanospheres
Origin and properties of non-Lorentzian spectral lines in linear chains of
nanospheres are discussed. The lines are shown to be super-exponentially narrow
with the characteristic width proportional to exp[-C(h/a)^3] where C is a
numerical constant, h the spacing between the nanospheres in the chain and a
the sphere radius. The fine structure of these spectral lines is also
investigated.Comment: 9 pages, 4 figure
On the use of Purcell factors for plasmon antennas
The Purcell factor is the standard figure of merit for spontaneous emission
enhancement in microcavities, that has also been proposed to describe emission
enhancements for plasmonic resonances. A comparison is made of quality factor,
mode volume and Purcell factor for single and coupled plasmon spheres to exact
calculations of emission rates. The paper explains why the Purcell factor is
not appropriate for plasmon antennas.Comment: 3 pages, 2 figure
Gravity in the Local Universe : density and velocity fields using CosmicFlows-4
This article publicly releases three-dimensional reconstructions of the local
Universe gravitational field below z=0.8 that were computed using the
CosmicFlows-4 catalog of 56,000 galaxy distances and its sub-sample of 1,008
type Ia supernovae distances. The article also provides measurements of the
growth rate of structure using the pairwise correlation of radial peculiar
velocities f sigma8 = 0.38(+/-0.04) (ungrouped CF4), f sigma8 = 0.36(+/-0.05)
(grouped CF4), f sigma8 = 0.30(+/-0.06) (SNIa) and of the bulk flow in the 3D
reconstructed Local Universe of 230 +/- 136 km s-1 at 300 Mpc of distance from
the observer. The exploration of 10,000 reconstructions gives that the
distances delivered by the Cosmicflows-4 catalog are compatible with a Hubble
constant of H0 = 74.5 +/- 0.1 (grouped CF4), H0 = 75.0 +/- 0.35 (ungrouped CF4)
and H0 = 75.5 +/- 0.95 (CF4 SNIa subsample).Comment: Submitted A&A Oct 31st, 2022 / (AA/2022/45331) / Accepted January
2023 All Figures and values updated after the december 2022 major correction
in CF4 catalo
Refractive-index sensing with ultra-thin plasmonic nanotubes
We study the refractive-index sensing properties of plasmonic nanotubes with
a dielectric core and ultra-thin metal shell. The few-nm thin metal shell is
described by both the usual Drude model and the nonlocal hydrodynamic model to
investigate the effects of nonlocality. We derive an analytical expression for
the extinction cross section and show how sensing of the refractive index of
the surrounding medium and the figure-of-merit are affected by the shape and
size of the nanotubes. Comparison with other localized surface plasmon
resonance sensors reveals that the nanotube exhibits superior sensitivity and
comparable figure-of-merit
NIKA2: a mm camera for cluster cosmology
Galaxy clusters constitute a major cosmological probe. However, Planck 2015
results have shown a weak tension between CMB-derived and cluster-derived
cosmological parameters. This tension might be due to poor knowledge of the
cluster mass and observable relationship.
As for now, arcmin resolution Sunyaev-Zeldovich (SZ) observations ({\it e.g.}
SPT, ACT and Planck) only allowed detailed studies of the intra cluster medium
for low redshift clusters () high
resolution and high sensitivity SZ observations are needed. With both a wide
field of view (6.5 arcmin) and a high angular resolution (17.7 and 11.2 arcsec
at 150 and 260 GHz), the NIKA2 camera installed at the IRAM 30-m telescope
(Pico Veleta, Spain) is particularly well adapted for these observations. The
NIKA2 SZ observation program will map a large sample of clusters (50) at
redshifts between 0.5 and 0.9. As a pilot study for NIKA2, several clusters of
galaxies have been observed with the pathfinder, NIKA, at the IRAM 30-m
telescope to cover the various configurations and observation conditions
expected for NIKA2.
High resolution SZ observations at the IRAM 30-m telescope with NIKA
High resolution observations of the thermal Sunyaev-Zel'dovich (tSZ) effect
are necessary to allow the use of clusters of galaxies as a probe for large
scale structures at high redshifts. With its high resolution and dual-band
capability at millimeter wavelengths, the NIKA camera can play a significant
role in this context. NIKA is based on newly developed Kinetic Inductance
Detectors (KIDs) and operates at the IRAM 30m telescope, Pico Veleta, Spain. In
this paper, we give the status of the NIKA camera, focussing on the KID
technology. We then present observations of three galaxy clusters: RX
J1347.5-1145 as a demonstrator of the NIKA capabilities and the recent
observations of CL J1226.9+3332 (z = 0.89) and MACS J0717.5+3745 (z = 0.55). We
also discuss prospects for the final NIKA2 camera, which will have a 6.5
arcminute field of view with about 5000 detectors in two bands at 150 and 260
GHz
NIKA 2: next-generation continuum/polarized camera at the IRAM 30 m telescope and its prototype
NIKA 2 (New Instrument of Kids Array) is a next generation continuum and
polarized instrument successfully installed in October 2015 at the IRAM 30 m
telescope on Pico-Veleta (Granada, Spain). NIKA 2 is a high resolution
dual-band camera, operating with frequency multiplexed LEKIDs (Lumped Element
Kinetic Inductance Detectors) cooled at 100 mK. Dual color images are obtained
thanks to the simultaneous readout of a 1020 pixels array at 2 mm and 1140 x 2
pixels arrays at 1.15 mm with a final resolution of 18 and 12 arcsec
respectively, and 6.5 arcmin of Field of View (FoV). The two arrays at 1.15 mm
allow us to measure the linear polarization of the incoming light. This will
place NIKA 2 as an instrument of choice to study the role of magnetic fields in
the star formation process. The NIKA experiment, a prototype for NIKA 2 with a
reduced number of detectors (about 400 LEKIDs) and FoV (1.8 arcmin), has been
successfully operated at the IRAM 30 telescope in several open observational
campaigns. The performance of the NIKA 2 polarization setup has been
successfully validated with the NIKA prototype.Comment: 5 pages, 4 figures, proceeding for the conference: Extragalactic
radio surveys 201
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