3,107 research outputs found
Survival of several Rhizobium/Bradyrhizobium strains on different inoculant formulations and inoculated seeds
The effect of a variety factors on the survival of several rhizobia strains on inoculants and inoculated seeds has been evaluated. Since the rhizobia strains showed different cell-density-evolution patterns on peat-based inoculants and on inoculated seeds, several inoculant formulations with highly effective Rhizobium/ Bradyrhizobium strains (for Lupinus, Hedysarum, Phaseolus and Glycine max. ) were monitored under the following storage conditions: (a) the inoculants were kept refrigerated (at 4°C), or (b) at room temperature (25°C). The effect of water content (30–50%, w/w) in the inoculants as well as that of several seed-coating adhesives were also investigated. Alternative carriers including perlite and vermiculite were tested. For all of the strains, survival on sterile peat-based inoculants was higher than on the corresponding unsterile peat formulation; for the latter, refrigerated storage conditions are recommended to ensure high bacterial densities. The water content of the inoculants had a differential effect on strain survival depending on the sterility of the peat, such that a high water content was more detrimental when unsterilized peat was employed. The best adherent for rhizobia survival was a gum arabic/water solution. Perlite was as effective as peat in maintaining a high population of rhizobia, at least for 6 months of storage
Evolution of Chemistry in the envelope of Hot Corinos (ECHOS). I. Extremely young sulphur chemistry in the isolated Class 0 object B335
Within the project Evolution of Chemistry in the envelope of HOt corinoS
(ECHOS), we present a study of sulphur chemistry in the envelope of the Class 0
source B335 through observations in the spectral range 7, 3, and 2 mm. We have
modelled observations assuming LTE and LVG approximation. We have also used the
code Nautilus to study the time evolution of sulphur species. We have detected
20 sulphur species with a total gas-phase S abundance similar to that found in
the envelopes of other Class 0 objects, but with significant differences in the
abundances between sulphur carbon chains and sulphur molecules containing
oxygen and nitrogen. Our results highlight the nature of B335 as a source
especially rich in sulphur carbon chains unlike other Class 0 sources. The low
presence or absence of some molecules, such as SO and SO+, suggests a chemistry
not particularly influenced by shocks. We, however, detect a large presence of
HCS+ that, together with the low rotational temperatures obtained for all the S
species (<15 K), reveals the moderate or low density of the envelope of B335.
We also find that observations are better reproduced by models with a sulphur
depletion factor of 10 with respect to the sulphur cosmic elemental abundance.
The comparison between our model and observational results for B335 reveals an
age of 10t10 yr, which highlights the particularly early
evolutionary stage of this source. B335 presents a different chemistry compared
to other young protostars that have formed in dense molecular clouds, which
could be the result of accretion of surrounding material from the diffuse cloud
onto the protostellar envelope of B335. In addition, the analysis of the
SO2/C2S, SO/CS, and HCS+/CS ratios within a sample of prestellar cores and
Class 0 objects show that they could be used as good chemical evolutionary
indicators of the prestellar to protostellar transition
NEXT-100 Technical Design Report (TDR). Executive Summary
In this Technical Design Report (TDR) we describe the NEXT-100 detector that
will search for neutrinoless double beta decay (bbonu) in Xe-136 at the
Laboratorio Subterraneo de Canfranc (LSC), in Spain. The document formalizes
the design presented in our Conceptual Design Report (CDR): an
electroluminescence time projection chamber, with separate readout planes for
calorimetry and tracking, located, respectively, behind cathode and anode. The
detector is designed to hold a maximum of about 150 kg of xenon at 15 bar, or
100 kg at 10 bar. This option builds in the capability to increase the total
isotope mass by 50% while keeping the operating pressure at a manageable level.
The readout plane performing the energy measurement is composed of Hamamatsu
R11410-10 photomultipliers, specially designed for operation in low-background,
xenon-based detectors. Each individual PMT will be isolated from the gas by an
individual, pressure resistant enclosure and will be coupled to the sensitive
volume through a sapphire window. The tracking plane consists in an array of
Hamamatsu S10362-11-050P MPPCs used as tracking pixels. They will be arranged
in square boards holding 64 sensors (8 times8) with a 1-cm pitch. The inner
walls of the TPC, the sapphire windows and the boards holding the MPPCs will be
coated with tetraphenyl butadiene (TPB), a wavelength shifter, to improve the
light collection.Comment: 32 pages, 22 figures, 5 table
Future care for long-term cancer survivors: towards a new model
Purpose: The increase in the prevalence "long-term cancer survivor” (LCS) patients is expected to increase the cost of LCS care. The aim of this study was to obtain information that would allow to optimise the current model of health management in Spain to adapt it to one of efficient LCS patient care. Methods: This qualitative study was carried out using Delphi methodology. An advisory committee defined the criteria for participation, select the panel of experts, prepare the questionnaire, interpret the results and draft the final report. Results: 232 people took part in the study (48 oncologists). Absolute consensus was reached in three of the proposed sections: oncological epidemiology, training of health professionals and ICT functions. Conclusion: The role of primary care in the clinical management of LCS patients needs to be upgraded, coordination with the oncologist and hospital care is essential. The funding model needs to be adapted to determine the funding conditions for new drugs and technologiesOpen Access funding provided thanks to the CRUE-CSIC
agreement with Springer Nature. This project was funded by AZ. The
funding party did not influence the opinion of the authors. All the
authors have accepted the participation as advisers of the ASISTO
group and give their consent for the publication of the documen
Parameterization Effects in the analysis of AMI Sunyaev-Zel'dovich Observations
Most Sunyaev--Zel'dovich (SZ) and X-ray analyses of galaxy clusters try to
constrain the cluster total mass and/or gas mass using parameterised models and
assumptions of spherical symmetry and hydrostatic equilibrium. By numerically
exploring the probability distributions of the cluster parameters given the
simulated interferometric SZ data in the context of Bayesian methods, and
assuming a beta-model for the electron number density we investigate the
capability of this model and analysis to return the simulated cluster input
quantities via three rameterisations. In parameterisation I we assume that the
T is an input parameter. We find that parameterisation I can hardly constrain
the cluster parameters. We then investigate parameterisations II and III in
which fg(r200) replaces temperature as a main variable. In parameterisation II
we relate M_T(r200) and T assuming hydrostatic equilibrium. We find that
parameterisation II can constrain the cluster physical parameters but the
temperature estimate is biased low. In parameterisation III, the virial theorem
replaces the hydrostatic equilibrium assumption. We find that parameterisation
III results in unbiased estimates of the cluster properties. We generate a
second simulated cluster using a generalised NFW (GNFW) pressure profile and
analyse it with an entropy based model to take into account the temperature
gradient in our analysis and improve the cluster gas density distribution. This
model also constrains the cluster physical parameters and the results show a
radial decline in the gas temperature as expected. The mean cluster total mass
estimates are also within 1 sigma from the simulated cluster true values.
However, we find that for at least interferometric SZ analysis in practice at
the present time, there is no differences in the AMI visibilities between the
two models. This may of course change as the instruments improve.Comment: 19 pages, 13 tables, 24 figure
Small-scale solar magnetic fields
As we resolve ever smaller structures in the solar atmosphere, it has become
clear that magnetism is an important component of those small structures.
Small-scale magnetism holds the key to many poorly understood facets of solar
magnetism on all scales, such as the existence of a local dynamo, chromospheric
heating, and flux emergence, to name a few. Here, we review our knowledge of
small-scale photospheric fields, with particular emphasis on quiet-sun field,
and discuss the implications of several results obtained recently using new
instruments, as well as future prospects in this field of research.Comment: 43 pages, 18 figure
Gas phase Elemental abundances in Molecular cloudS (GEMS) VII. Sulfur elemental abundance
Gas phase Elemental abundances in molecular CloudS (GEMS) is an IRAM 30m
large program aimed at determining the elemental abundances of carbon (C),
oxygen (O), nitrogen (N), and sulfur (S) in a selected set of prototypical
star-forming filaments. In particular, the elemental abundance of S remains
uncertain by several orders of magnitude and its determination is one of the
most challenging goals of this program. We have carried out an extensive
chemical modeling of the fractional abundances of CO, HCO, HCN, HNC, CS,
SO, HS, OCS, and HCS to determine the sulfur depletion toward the 244
positions in the GEMS database. These positions sample visual extinctions from
A 3 mag to 50 mag, molecular hydrogen densities ranging from a
few 10~cm to 310~cm, and T 1035 K.
Most of the positions in Taurus and Perseus are best fitted assuming early-time
chemistry, t=0.1 Myr, (0.51)10 s,
and [S/H]1.510. On the contrary, most of the positions in
Orion are fitted with t=1~Myr and 10 s.
Moreover, 40% of the positions in Orion are best fitted assuming the
undepleted sulfur abundance, [S/H]1.510. Our results
suggest that sulfur depletion depends on the environment. While the abundances
of sulfur-bearing species are consistent with undepleted sulfur in Orion, a
depletion factor of 20 is required to explain those observed in Taurus
and Perseus. We propose that differences in the grain charge distribution in
the envelopes of the studied clouds might explain these variations. The shocks
associated with past and ongoing star formation could also contribute to
enhance [S/H] in Orion.Comment: 22 pages, 15 figures, Astronomy and Astrophysics, in pres
The Pierre Auger Observatory III: Other Astrophysical Observations
Astrophysical observations of ultra-high-energy cosmic rays with the Pierre
Auger ObservatoryComment: Contributions to the 32nd International Cosmic Ray Conference,
Beijing, China, August 201
Measurement of the Depth of Maximum of Extensive Air Showers above 10^18 eV
We describe the measurement of the depth of maximum, Xmax, of the
longitudinal development of air showers induced by cosmic rays. Almost four
thousand events above 10^18 eV observed by the fluorescence detector of the
Pierre Auger Observatory in coincidence with at least one surface detector
station are selected for the analysis. The average shower maximum was found to
evolve with energy at a rate of (106 +35/-21) g/cm^2/decade below 10^(18.24 +/-
0.05) eV and (24 +/- 3) g/cm^2/decade above this energy. The measured
shower-to-shower fluctuations decrease from about 55 to 26 g/cm^2. The
interpretation of these results in terms of the cosmic ray mass composition is
briefly discussed.Comment: Accepted for publication by PR
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