20,190 research outputs found
Fitting stochastic predator-prey models using both population density and kill rate data
Most mechanistic predator-prey modelling has involved either parameterization
from process rate data or inverse modelling. Here, we take a median road: we
aim at identifying the potential benefits of combining datasets, when both
population growth and predation processes are viewed as stochastic. We fit a
discrete-time, stochastic predator-prey model of the Leslie type to simulated
time series of densities and kill rate data. Our model has both environmental
stochasticity in the growth rates and interaction stochasticity, i.e., a
stochastic functional response. We examine what the kill rate data brings to
the quality of the estimates, and whether estimation is possible (for various
time series lengths) solely with time series of population counts or biomass
data. Both Bayesian and frequentist estimation are performed, providing
multiple ways to check model identifiability. The Fisher Information Matrix
suggests that models with and without kill rate data are all identifiable,
although correlations remain between parameters that belong to the same
functional form. However, our results show that if the attractor is a fixed
point in the absence of stochasticity, identifying parameters in practice
requires kill rate data as a complement to the time series of population
densities, due to the relatively flat likelihood. Only noisy limit cycle
attractors can be identified directly from population count data (as in inverse
modelling), although even in this case, adding kill rate data - including in
small amounts - can make the estimates much more precise. Overall, we show that
under process stochasticity in interaction rates, interaction data might be
essential to obtain identifiable dynamical models for multiple species. These
results may extend to other biotic interactions than predation, for which
similar models combining interaction rates and population counts could be
developed
EEOC v. Union Independiente Autentica de la AAA and Autoridad de Acueductos y Alcantarillados and Ondeo de Puerto Rico
A note on Gorenstein monomial curves
Let be an arbitrary field. In this note, we show that if a sequence of
relatively prime positive integers defines a
Gorenstein non complete intersection monomial curve in
, then there exist two vectors and such
that and are
also Gorenstein non complete intersection affine monomial curves for almost all
Where are compact groups in the local Universe?
The purpose of this work is to perform a statistical analysis of the location
of compact groups in the Universe from observational and semi-analytical points
of view. We used the velocity-filtered compact group sample extracted from the
Two Micron All Sky Survey for our analysis. We also used a new sample of galaxy
groups identified in the 2M++ galaxy redshift catalogue as tracers of the
large-scale structure. We defined a procedure to search in redshift space for
compact groups that can be considered embedded in other overdense systems and
applied this criterion to several possible combinations of different compact
and galaxy group subsamples. We also performed similar analyses for simulated
compact and galaxy groups identified in a 2M++ mock galaxy catalogue
constructed from the Millennium Run Simulation I plus a semi-analytical model
of galaxy formation. We observed that only of the compact groups can
be considered to be embedded in larger overdense systems, that is, most of the
compact groups are more likely to be isolated systems. The embedded compact
groups show statistically smaller sizes and brighter surface brightnesses than
non-embedded systems. No evidence was found that embedded compact groups are
more likely to inhabit galaxy groups with a given virial mass or with a
particular dynamical state. We found very similar results when the analysis was
performed using mock compact and galaxy groups. Based on the semi-analytical
studies, we predict that of the embedded compact groups probably are 3D
physically dense systems. Finally, real space information allowed us to reveal
the bimodal behaviour of the distribution of 3D minimum distances between
compact and galaxy groups. The location of compact groups should be carefully
taken into account when comparing properties of galaxies in environments that
are a priori different.Comment: 14 pages, 5 figures, 8 tables. Accepted for publication in Astronomy
& Astrophysics. Tables B1 and B2 will only be available in electronic form at
the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via
http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A
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