880 research outputs found
Passivation of Grid-Following VSCs: A Comparison Between Active Damping and Multi-Sampled PWM
This article compares different strategies used to enhance the stability properties of grid-following voltage-source converters (VSCs). Because of digital delays, VSC admittance exhibits a nonpassive zone, which introduces negative damping and may destabilize the grid-connected operation. It is shown that typically used active damping (AD) strategies only bring positive impact up to a certain frequency, while deteriorating admittance properties around and above the Nyquist frequency. Multi-sampled pulsewidth modulation (MS-PWM) greatly extends the passive admittance region, using only a single-loop current controller. Experimental admittance measurements are performed on a single-phase VSC, up to twice the switching frequency. Subsequently, different grid-connected scenarios are tested to show that MS-PWM retains stable operation, where AD methods cause instability. This article also offers analytic modeling and experimental measurements of noise propagation for compared strategies. It is shown that derivative-based AD is not highly sensitive; however, MS-PWM offers additional noise suppression
Sensitive observations at 1.4 and 250 GHz of z > 5 QSOs
We present 1.4 and 5 GHz observations taken with the Very Large Array (VLA),
and observations at 250 GHz obtained with the Max-Planck millimeter bolometer
(MAMBO) at the IRAM 30~m telescope, of ten optically selected Quasi-stellar
Objects (QSOs) at 5.0 < z < 6.28. Four sources are detected at 1.4 GHz two of
which are radio loud and are also detected at 5 GHz. These results are roughly
consistent with there being no evolution of the radio-loud QSO fraction out to
z~6.
Three sources have been detected at 250 GHz or 350 GHz at much higher levels
than their 1.4 GHz flux densities suggesting that the observed mm emission is
likely thermal emission from warm dust, although more exotic possibilities
cannot be precluded.
The highest redshift source in our sample (J1030+0524 at z=6.28) is not
detected at 1.4 or 250 GHz, but four fairly bright radio sources (flux density
at 1.4GHz > 0.2 mJy) are detected in a 2' field centered on the QSO, including
an edge-brightened ('FRII') double radio source with an extent of about 1'.
A similar over-density of radio sources is seen in the field of the highest
redshift QSO J1148+5251. We speculate that these over-densities of radio
sources may indicate clusters along the lines-of-sight, in which case
gravitational lensing by the cluster could magnify the QSO emission by a factor
2 or so without giving rise to arcsecond-scale distortions in the optical
images of the QSOs.Comment: 25 pages, 12 figures. accepted by A
A subarcsecond near-infrared view of massive galaxies at z > 1 with Gemini Multiconjugate Adaptive Optics
We present images taken using the Gemini South Adaptive Optics Imager (GSAOI)
with the Gemini Multiconjugate Adaptive Optics System (GeMS) in three 2
arcmin fields in the Spitzer Extragalactic Representative Volume Survey.
These GeMS/GSAOI observations are among the first resolution
data in the near-infrared spanning extragalactic fields exceeding
in size. We use these data to estimate galaxy sizes, obtaining
results similar to those from studies with the Hubble Space Telescope, though
we find a higher fraction of compact star forming galaxies at . To
disentangle the star-forming galaxies from active galactic nuclei (AGN), we use
multiwavelength data from surveys in the optical and infrared, including
far-infrared data from Herschel, as well as new radio continuum data from the
Australia Telescope Compact Array and Very Large Array. We identify
ultraluminous infrared galaxies (ULIRGs) at , which consist of a
combination of pure starburst galaxies and Active Galactic Nuclei
(AGN)/starburst composites. The ULIRGs show signs of recent merger activity,
such as highly disturbed morphologies and include a rare candidate triple AGN.
We find that AGN tend to reside in hosts with smaller scale sizes than purely
star-forming galaxies of similar infrared luminosity. Our observations
demonstrate the potential for MCAO to complement the deeper galaxy surveys to
be made with the James Webb Space Telescope.Comment: 20 pages, AJ, in pres
Extended [CII] Emission in Local Luminous Infrared Galaxies
We present Herschel/PACS observations of extended [CII]157.7{\mu}m line
emission detected on ~ 1 - 10 kpc scales in 60 local luminous infrared galaxies
(LIRGs) from the Great Observatories All-sky LIRG Survey (GOALS). We find that
most of the extra-nuclear emission show [CII]/FIR ratios >~ 4 x 10^-3, larger
than the mean ratio seen in the nuclei, and similar to those found in the
extended disks of normal star-forming galaxies and the diffuse inter-stellar
medium (ISM) of our Galaxy. The [CII] "deficits" found in the most luminous
local LIRGs are therefore restricted to their nuclei. There is a trend for
LIRGs with warmer nuclei to show larger differences between their nuclear and
extra-nuclear [CII]/FIR ratios. We find an anti-correlation between [CII]/FIR
and the luminosity surface density, {\Sigma}_IR, for the extended emission in
the spatially-resolved galaxies. However, there is an offset between this trend
and that found for the LIRG nuclei. We use this offset to derive a beam
filling-factor for the star-forming regions within the LIRG disks of ~ 6 %
relative to their nuclei. We confront the observed trend to photo-dissociation
region (PDR) models and find that the slope of the correlation is much
shallower than the model predictions. Finally, we compare the correlation found
between [CII]/FIR and {\Sigma}_IR with measurements of high-redshift
starbursting IR-luminous galaxies.Comment: Accepted for publication in ApJ Letters. 5 pages, 2 figure
The Compact Linear ee Collider (CLIC): Accelerator and Detector
The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear
ee collider under development by international collaborations hosted by
CERN. This document provides an overview of the design, technology, and
implementation aspects of the CLIC accelerator and the detector. For an optimal
exploitation of its physics potential, CLIC is foreseen to be built and
operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV,
for a site length ranging between 11 km and 50 km. CLIC uses a two-beam
acceleration scheme, in which normal-conducting high-gradient 12 GHz
accelerating structures are powered via a high-current drive beam. For the
first stage, an alternative with X-band klystron powering is also considered.
CLIC accelerator optimisation, technical developments, and system tests have
resulted in significant progress in recent years. Moreover, this has led to an
increased energy efficiency and reduced power consumption of around 170 MW for
the 380 GeV stage, together with a reduced cost estimate of approximately 6
billion CHF. The detector concept, which matches the physics performance
requirements and the CLIC experimental conditions, has been refined using
improved software tools for simulation and reconstruction. Significant progress
has been made on detector technology developments for the tracking and
calorimetry systems. The construction of the first CLIC energy stage could
start as early as 2026 and first beams would be available by 2035, marking the
beginning of a physics programme spanning 25-30 years and providing excellent
sensitivity to Beyond Standard Model physics, through direct searches and via a
broad set of precision measurements of Standard Model processes, particularly
in the Higgs and top-quark sectors.Comment: Input to the European Particle Physics Strategy Update on behalf of
the CLIC and CLICdp Collaboration
Differences in Ultrasonic Vocalizations Between Wild and Laboratory California Mice (\u3cem\u3ePeromyscus californicus\u3c/em\u3e)
Background: Ultrasonic vocalizations (USVs) emitted by muroid rodents, including laboratory mice and rats, are used as phenotypic markers in behavioral assays and biomedical research. Interpretation of these USVs depends on understanding the significance of USV production by rodents in the wild. However, there has never been a study of muroid rodent ultrasound function in the wild and comparisons of USVs produced by wild and laboratory rodents are lacking to date. Here, we report the first comparison of wild and captive rodent USVs recorded from the same species, Peromyscus californicus.
Methodology and Principal Findings: We used standard ultrasound recording techniques to measure USVs from California mice in the laboratory (Peromyscus Genetic Stock Center, SC, USA) and the wild (Hastings Natural History Reserve, CA, USA). To determine which California mouse in the wild was vocalizing, we used a remote sensing method that used a 12- microphone acoustic localization array coupled with automated radio telemetry of all resident Peromyscus californicus in the area of the acoustic localization array. California mice in the laboratory and the wild produced the same types of USV motifs. However, wild California mice produced USVs that were 2–8 kHz higher in median frequency and significantly more variable in frequency than laboratory California mice.
Significance: The similarity in overall form of USVs from wild and laboratory California mice demonstrates that production of USVs by captive Peromyscus is not an artifact of captivity. Our study validates the widespread use of USVs in laboratory rodents as behavioral indicators but highlights that particular characteristics of laboratory USVs may not reflect natural conditions
The dark matter halo shape of edge-on disk galaxies - II. Modelling the HI observations: methods
This is the second paper of a series in which we attempt to put constraints
on the flattening of dark halos in disk galaxies. For this purpose, we observe
the HI in edge-on galaxies, where it is in principle possible to measure the
force field in the halo vertically and radially from gas layer flaring and
rotation curve decomposition respectively. To calculate the force fields, we
need to analyse the observed XV diagrams to accurately measure all three
functions that describe the planar kinematics and distribution of a galaxy: the
radial HI surface density, the rotation curve and the HI velocity dispersion.
In this paper, we discuss the improvements and limitations of the methods
previously used to measure these HI properties. We extend the constant velocity
dispersion method to include determination of the HI velocity dispersion as a
function of galactocentric radius and perform extensive tests on the quality of
the fits. We will apply this 'radial decomposition XV modelling method' to our
HI observations of 8 HI-rich, late-type, edge-on galaxies in the third paper of
this series.Comment: Accepted for publication by Astronomy & Astrophysics. For a higher
resolution version see
http://www.astro.rug.nl/~vdkruit/jea3/homepage/12566.pd
Explaining the [C II] 157.7µm Deficit in Luminous Infrared Galaxies - First Results from a Herschel/PACS Study of the GOALS Sample
We present the first results of a survey of the [C II] 157.7 μm emission line in 241 luminous infrared galaxies (LIRGs) comprising the Great Observatories All-sky Survey (GOALS) sample, obtained with the PACS instrument on board the Herschel Space Observatory. The [C II] luminosities, L_([C II]), of the LIRGs in GOALS range from ∼ 10^7 to 2×10^9 L_⊙. We find that LIRGs show a tight correlation
of [C II]/FIR with far-IR flux density ratios, with a strong negative trend spanning from ∼ 10^(−2) to 10^(−4), as the average temperature of dust increases. We find correlations between the [C II]/FIR ratio and the strength of the 9.7 μm silicate absorption feature as well as with the luminosity surface density of the mid-IR emitting region (∑_(MIR)), suggesting that warmer, more compact starbursts have substantially smaller [C II]/FIR ratios. Pure star-forming LIRGs have a mean [C II]/FIR∼ 4 × 10^(−3),
while galaxies with low 6.2 μm PAH equivalent widths (EWs), indicative of the presence of active galactic nuclei (AGN), span the full range in [C II]/FIR. However, we show that even when only pure star-forming galaxies are considered, the [C II]/FIR ratio still drops by an order of magnitude, from 10^(−2) to 10^(−3), with ∑_(MIR) and ∑_(IR), implying that the [C II] 157.7 μm luminosity is not a good indicator
of the star formation rate (SFR) for most LIRGs, for it does not scale linearly with the warm dust emission most likely associated to the youngest stars. Moreover, even in LIRGs in which we detect an AGN in the mid-IR, the majority (2/3) of galaxies show [C II]/FIR≥ 10^(−3) typical of high 6.2 μm PAH EW sources, suggesting that most AGNs do not contribute significantly to the far-IR emission. We provide an empirical relation between the [C II]/FIR and the specific SFR (SSFR) for star-forming LIRGs. Finally, we present predictions for the starburst size based on the observed [C II] and far-IR luminosities which should be useful for comparing with results from future surveys of high-redshift galaxies with ALMA and CCAT
The Spatial Extent of (U)LIRGs in the mid-Infrared I: The Continuum Emission
We present an analysis of the extended mid-infrared (MIR) emission of the
Great Observatories All-Sky LIRG Survey (GOALS) sample based on 5-15um low
resolution spectra obtained with the IRS on Spitzer. We calculate the fraction
of extended emission as a function of wavelength for the galaxies in the
sample, FEE_lambda. We can identify 3 general types of FEE_lambda: one where it
is constant, one where features due to emission lines and PAHs appear more
extended than the continuum, and a third which is characteristic of sources
with deep silicate absorption at 9.7um. More than 30% of the galaxies have a
median FEE_lambda larger than 0.5 implying that at least half of their MIR
emission is extended. Luminous Infrared Galaxies (LIRGs) display a wide range
of FEE in their warm dust continuum (0<=FEE_13.2um<=0.85). The large values of
FEE_13.2um that we find in many LIRGs suggest that their extended MIR continuum
emission originates in scales up to 10kpc. The mean size of the LIRG cores at
13.2um is 2.6kpc. However, once the LIR of the systems reaches the threshold of
~10^11.8Lsun, all sources become clearly more compact, with FEE_13.2um<=0.2,
and their cores are unresolved. Our estimated upper limit for the core size of
ULIRGs is less than 1.5kpc. The analysis indicates that the compactness of
systems with LIR>~10^11.25Lsun strongly increases in those classified as
mergers in their final stage of interaction. The FEE_13.2um is also related to
the contribution of an active galactic nucleus (AGN) to the MIR. Galaxies which
are more AGN-dominated are less extended, independently of their LIR. We
finally find that the extent of the MIR continuum emission is correlated with
the far-IR IRAS log(f_60um/f_100um) color. This enables us to place a lower
limit to the area in a galaxy from where the cold dust emission may originate,
a prediction which can be tested soon with the Herschel Space Telescope.Comment: 18 pages, 8 figures, accepted for publication in Ap
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