46,371 research outputs found
\u27How To\u27 Guide for Synthesizing NERRs Marsh Monitoring Data
The purpose of this guide is to provide a user-friendly and informative guide on âHow toâ synthesize salt marsh data from theNational Estuarine Research Reserve System (NERRs). In this guide, we outline and detail the steps taken from requesting/cataloguing data to summarizing these data through visual and statistical analysis. These methods can be used at a single or multiple site(s) as well as over multiple years. Though this guide is specific to NERRs and focuses on plant community data, it may also be useful for other monitoring parameters and programs to guide protocol design and analyses. Here, we conduct a synthesis of New England salt marshes using NERRs data collected from the past decade
Dissecting Photometric redshift for Active Galactic Nuclei using XMM- and Chandra-COSMOS samples
With this paper, we release accurate photometric redshifts for 1692
counterparts to Chandra sources in the central square degree of the COSMOS
field. The availability of a large training set of spectroscopic redshifts that
extends to faint magnitudes enabled photometric redshifts comparable to the
highest quality results presently available for normal galaxies. We demonstrate
that morphologically extended, faint X-ray sources without optical variability
are more accurately described by a library of normal galaxies (corrected for
emission lines) than by AGN-dominated templates, even if these sources have
AGN-like X-ray luminosities. Preselecting the library on the bases of the
source properties allowed us to reach an accuracy sigma_(Delta z/(1+z_spec))
\sim0.015 with a fraction of outliers of 5.8% for the entire Chandra-COSMOS
sample. In addition, we release revised photometric redshifts for the 1735
optical counterparts of the XMM-detected sources over the entire 2 sq. deg.of
COSMOS. For 248 sources, our updated photometric redshift differs from the
previous release by Delta z>0.2. These changes are predominantly due to the
inclusion of newly available deep H-band photometry H_AB=24 mag. We illustrate
once again the importance of a spectroscopic training sample and how an
assumption about the nature of a source together with the number and the depth
of the available bands influence the accuracy of the photometric redshifts
determined for AGN. These considerations should be kept in mind when defining
the observational strategies of upcoming large surveys targeting AGN, such as
eROSITA at X-ray energies and ASKAP/EMU in the radio band.Comment: ApJ, accepted for publication. Data also available at
http://www.ipp.mpg.de/~msalv/PHOTOZ_XCOSMO
Panchromatic spectral energy distributions of Herschel sources
(abridged) Far-infrared Herschel photometry from the PEP and HerMES programs
is combined with ancillary datasets in the GOODS-N, GOODS-S, and COSMOS fields.
Based on this rich dataset, we reproduce the restframe UV to FIR ten-colors
distribution of galaxies using a superposition of multi-variate Gaussian modes.
The median SED of each mode is then fitted with a modified version of the
MAGPHYS code that combines stellar light, emission from dust heated by stars
and a possible warm dust contribution heated by an AGN. The defined Gaussian
grouping is also used to identify rare sources. The zoology of outliers
includes Herschel-detected ellipticals, very blue z~1 Ly-break galaxies,
quiescent spirals, and torus-dominated AGN with star formation. Out of these
groups and outliers, a new template library is assembled, consisting of 32 SEDs
describing the intrinsic scatter in the restframe UV-to-submm colors of
infrared galaxies. This library is tested against L(IR) estimates with and
without Herschel data included, and compared to eight other popular methods
often adopted in the literature. When implementing Herschel photometry, these
approaches produce L(IR) values consistent with each other within a median
absolute deviation of 10-20%, the scatter being dominated more by fine tuning
of the codes, rather than by the choice of SED templates. Finally, the library
is used to classify 24 micron detected sources in PEP GOODS fields. AGN appear
to be distributed in the stellar mass (M*) vs. star formation rate (SFR) space
along with all other galaxies, regardless of the amount of infrared luminosity
they are powering, with the tendency to lie on the high SFR side of the "main
sequence". The incidence of warmer star-forming sources grows for objects with
higher specific star formation rates (sSFR), and they tend to populate the
"off-sequence" region of the M*-SFR-z space.Comment: Accepted for publication in A&A. Some figures are presented in low
resolution. The new galaxy templates are available for download at the
address http://www.mpe.mpg.de/ir/Research/PEP/uvfir_temp
Measurement of the polarisation of W bosons produced with large transverse momentum in pp collisions at sqrt(s) = 7 TeV with the ATLAS experiment
This paper describes an analysis of the angular distribution of W->enu and
W->munu decays, using data from pp collisions at sqrt(s) = 7 TeV recorded with
the ATLAS detector at the LHC in 2010, corresponding to an integrated
luminosity of about 35 pb^-1. Using the decay lepton transverse momentum and
the missing transverse energy, the W decay angular distribution projected onto
the transverse plane is obtained and analysed in terms of helicity fractions
f0, fL and fR over two ranges of W transverse momentum (ptw): 35 < ptw < 50 GeV
and ptw > 50 GeV. Good agreement is found with theoretical predictions. For ptw
> 50 GeV, the values of f0 and fL-fR, averaged over charge and lepton flavour,
are measured to be : f0 = 0.127 +/- 0.030 +/- 0.108 and fL-fR = 0.252 +/- 0.017
+/- 0.030, where the first uncertainties are statistical, and the second
include all systematic effects.Comment: 19 pages plus author list (34 pages total), 9 figures, 11 tables,
revised author list, matches European Journal of Physics C versio
Object Detection Through Exploration With A Foveated Visual Field
We present a foveated object detector (FOD) as a biologically-inspired
alternative to the sliding window (SW) approach which is the dominant method of
search in computer vision object detection. Similar to the human visual system,
the FOD has higher resolution at the fovea and lower resolution at the visual
periphery. Consequently, more computational resources are allocated at the
fovea and relatively fewer at the periphery. The FOD processes the entire
scene, uses retino-specific object detection classifiers to guide eye
movements, aligns its fovea with regions of interest in the input image and
integrates observations across multiple fixations. Our approach combines modern
object detectors from computer vision with a recent model of peripheral pooling
regions found at the V1 layer of the human visual system. We assessed various
eye movement strategies on the PASCAL VOC 2007 dataset and show that the FOD
performs on par with the SW detector while bringing significant computational
cost savings.Comment: An extended version of this manuscript was published in PLOS
Computational Biology (October 2017) at
https://doi.org/10.1371/journal.pcbi.100574
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