text:
package org.apache.servicecomb.core.transport;

import java.util.Arrays;
import java.util.List;
import java.util.Map;

import org.apache.servicecomb.core.Endpoint;
import org.apache.servicecomb.core.SCBEngine;
import org.apache.servicecomb.core.Transport;
import org.apache.servicecomb.foundation.common.exceptions.ServiceCombException;
import org.apache.servicecomb.registry.api.registry.MicroserviceInstance;
import org.junit.Assert;
import org.junit.Test;

import mockit.Expectations;
import mockit.Injectable;
import mockit.Mocked;

public class TestTransportManager {
  @Test
  public void testTransportManagerInitFail(@Mocked SCBEngine scbEngine, @Injectable Transport transport)
      throws Exception {
    new Expectations() {
      {
        transport.getName();
        result = "test";
        transport.init();
        result = false;
        transport.canInit();
        result = true;
      }
    };
    List<Transport> transports = Arrays.asList(transport);

    TransportManager manager = new TransportManager();
    manager.addTransportsBeforeInit(transports);

    manager.init(scbEngine);
    Assert.assertEquals(manager.findTransport("test"), transport);
  }

  @Test
  public void testTransportManagerInitSucc(@Mocked SCBEngine scbEngine, @Injectable Transport transport,
      @Injectable Endpoint endpoint, @Injectable MicroserviceInstance instance) throws Exception {
    new Expectations() {
      {
        transport.getName();
        result = "test";
        transport.canInit();
        result = true;
        transport.init();
        result = true;
        transport.getPublishEndpoint();
        result = endpoint;
      }
    };
    List<Transport> transports = Arrays.asList(transport);

    TransportManager manager = new TransportManager();
    manager.addTransportsBeforeInit(transports);

    manager.init(scbEngine);
    Assert.assertEquals(manager.findTransport("test"), transport);
  }

  @Test
  public void testGroupByName(@Mocked Transport t1, @Mocked Transport t2_1, @Mocked Transport t2_2) {
    new Expectations() {
      {
        t1.getName();
        result = "t1";

        t2_1.getName();
        result = "t2";
        t2_2.getName();
        result = "t2";
      }
    };

    TransportManager manager = new TransportManager();
    manager.addTransportsBeforeInit(Arrays.asList(t1, t2_1, t2_2));

    Map<String, List<Transport>> groups = manager.groupByName();
    Assert.assertEquals(2, groups.size());
    Assert.assertEquals(1, groups.get("t1").size());
    Assert.assertEquals(t1, groups.get("t1").get(0));
    Assert.assertEquals(2, groups.get("t2").size());
    Assert.assertEquals(t2_1, groups.get("t2").get(0));
    Assert.assertEquals(t2_2, groups.get("t2").get(1));
  }

  @Test
  public void testCheckTransportGroupInvalid(@Mocked Transport t1, @Mocked Transport t2) {
    new Expectations() {
      {
        t1.getOrder();
        result = 1;

        t2.getOrder();
        result = 1;
      }
    };

    TransportManager manager = new TransportManager();
    List<Transport> group = Arrays.asList(t1, t2);

    try {
      manager.checkTransportGroup(group);
      Assert.fail("must throw exception");
    } catch (ServiceCombException e) {
      Assert.assertEquals(
          "org.apache.servicecomb.core.$Impl_Transport and org.apache.servicecomb.core.$Impl_Transport have the same order 1",
          e.getMessage());
    }
  }

  @Test
  public void testCheckTransportGroupValid(@Mocked Transport t1, @Mocked Transport t2) {
    new Expectations() {
      {
        t1.getOrder();
        result = 1;

        t2.getOrder();
        result = 2;
      }
    };

    TransportManager manager = new TransportManager();
    List<Transport> group = Arrays.asList(t1, t2);

    try {
      manager.checkTransportGroup(group);
    } catch (ServiceCombException e) {
      Assert.fail("must not throw exception: " + e.getMessage());
    }
  }

  @Test
  public void testChooseOneTransportFirst(@Mocked Transport t1, @Mocked Transport t2) {
    new Expectations() {
      {
        t1.getOrder();
        result = 1;
        t1.canInit();
        result = true;

        t2.getOrder();
        result = 2;
      }
    };

    TransportManager manager = new TransportManager();
    List<Transport> group = Arrays.asList(t1, t2);

    Assert.assertEquals(t1, manager.chooseOneTransport(group));
  }

  @Test
  public void testChooseOneTransportSecond(@Mocked Transport t1, @Mocked Transport t2) {
    new Expectations() {
      {
        t1.getOrder();
        result = Integer.MAX_VALUE;
        t1.canInit();
        result = true;

        t2.getOrder();
        result = -1000;
        t2.canInit();
        result = false;
      }
    };

    TransportManager manager = new TransportManager();
    List<Transport> group = Arrays.asList(t1, t2);

    Assert.assertEquals(t1, manager.chooseOneTransport(group));
  }

  @Test
  public void testChooseOneTransportNone(@Mocked Transport t1, @Mocked Transport t2) {
    new Expectations() {
      {
        t1.getName();
        result = "t";
        t1.getOrder();
        result = 1;
        t1.canInit();
        result = false;

        t2.getOrder();
        result = 2;
        t2.canInit();
        result = false;
      }
    };

    TransportManager manager = new TransportManager();
    List<Transport> group = Arrays.asList(t1, t2);

    try {
      manager.chooseOneTransport(group);
      Assert.fail("must throw exception");
    } catch (ServiceCombException e) {
      Assert.assertEquals("all transport named t refused to init.", e.getMessage());
    }
  }
}


From time to time I think it is important to create a photo session for myself. Landscape photographers or hobbyists have more opportunity for something like this. But since my hobby is also my profession I like to find some time where I have an idea that I want to make into a cute little session. Being a kid photographer this can also be challenging as I think kids guide their own sessions. I may have an idea but if a kid has a different one, we roll with it. No one can make a two year old do something they don't want to right? ha. Anyway...Since making the move to Oregon City I have been enjoying exploring my surroundings. Growing up in such a small town, Oregon City makes me feel right at home. The downtown strip is reminiscent to main street in my old hometown. So I thought that was the best place to start....going back to my roots...exploring an old town with lots of character. I snagged my daughter and her two friends and we headed to downtown OC. I wanted the girls to be a little more "hipster" which my daughter now informs me that there were Three Stylish Hipsters for the shoot. She is hilarious. All three humored me though and totally Rocked their impromptu session. Towards the end of the session the girls started being incredibly silly....which led me to my next adventure for the month of June. (you may have seen my posts "BE SILLY" #besillyforbliss). Stay tuned for that post coming soon. Thanks to my three beautiful models for making my fun little idea an awesome photo session! I could not have pulled this off without these three silly girls.


Get this Sea Breeze Seashell Themed Bed in a Bag Set, which includes a variety of pieces. The bedding set has a seashell pattern with a variety of beach elements.
Build your own coastal retreat right in your bedroom with the Sea Breeze Mini Bed in a Bag Set by CHF. The nautical bed in a bag set includes a reversible comforter, two pillow shams (one with twin), and a coordinating sheet set. Shells and coral in a soft ocean blue, sand beige, an ivory color palette make this bedding set perfectly tranquil. The comforter reverses to an all-over ocean blue and ivory coral and the coordinating sheets come in a tonal beige shell pattern. Pieces are machine washable and come in popular size options. Twin Set Dimensions:Comforter: 86L x 64W in. Sham: 26L x 20W in. Pillowcase: 30L x 20W in. Fitted sheet: 75L x 39W x 10D in. Flat sheet: 96L x 66W in. Full Set Dimensions:Comforter: 86L x 76W in. Sham: 26L x 20W in. Pillowcase: 30L x 20W in. Fitted sheet: 75L x 54W x 10D in. Flat sheet: 96L x 81W in. Queen Set Dimensions:Comforter: 96L x 90W in. Sham: 26L x 20W in. Pillowcase: 30L x 20W in. Fitted sheet: 78L x 80W x 10D in. Flat sheet: 102L x 90W in. King Set Dimensions:Comforter: 96L x 108W in. Sham: 26L x 20W in. Pillowcase: 30L x 20W in. Fitted sheet: 80L x 60W x 12D in. Flat sheet: 102L x 108W in. About CHF Industries CHF Industries, based in New York, is known for its home textile products and is the largest private-label supplier of retail-specific bedding products. CHF offers a diverse range of window products like panels, valances, shades, kitchen tiers, and even window hardware. CHF innovates with fashionable solutions such as energy-efficient interlined window panels, taking steps to introduce organic products to protect the environment. Choice of size. Comforter, 1-2 pillow shams, fitted sheet, flat sheet, 1-2 pillowcases. 180-thread count, 60% cotton and 40% polyester construction. 100% polyester fill. Shells and coral in ocean blue, sand, and ivory. Comforter reverses to blue and ivory coral. Sheets in tonal beige shell pattern. Machine-washable.


AMAZING SPIDER-MAN #33 CGC 8.5 CLASSIC COVER HIGH GRADE DITKO ART OW/W PGS 1966 Well centered cover. Very nice presenting 8.5 Old CGC case with inner well, open sides, and top label. Case is in excellent condition. GLARE FROM SCANNER MAY BE PRESENT ON PHOTOS. The item "AMAZING SPIDER-MAN #33 CGC 8.5 CLASSIC COVER HIGH GRADE DITKO ART OWithW PGS 1966" is in sale since Friday, November 2, 2018.
This item is in the category "Collectibles\Comics\Silver Age (1956-69)\Superhero\Spider-Man". The seller is "eides_entertainment" and is located in Pittsburgh, Pennsylvania. This item can be shipped to United States, Canada, United Kingdom, Denmark, Romania, Slovakia, Bulgaria, Czech republic, Finland, Hungary, Latvia, Lithuania, Malta, Estonia, Australia, Greece, Portugal, Cyprus, Slovenia, Japan, China, Sweden, South Korea, Indonesia, Taiwan, South africa, Thailand, Belgium, France, Hong Kong, Ireland, Netherlands, Poland, Spain, Italy, Germany, Austria, Israel, Mexico, New Zealand, Philippines, Singapore, Switzerland, Norway, Saudi arabia, Ukraine, United arab emirates, Qatar, Kuwait, Bahrain, Croatia, Malaysia, Brazil, Chile, Colombia, Costa rica, Panama, Trinidad and tobago, Guatemala, Honduras, Jamaica, Bahamas, Viet nam, Uruguay, Egypt, Jordan, Sri lanka, Luxembourg, Nicaragua, Peru, Paraguay.


Elise Doane posed with the Halifax agave when it was in bloom in 2018. She believes she may have donated it 30 years ago. Submitted by Elise Doane.
Hundreds of people lined up outside the Public Gardens Thursday hoping to score one of the 158 seeds from Halifax's famous Agave Maria.
Nicknamed Agave Maria, the plant moved to the Public Gardens last April when its meters-long asparagus-like stalk became too tall for the municipality's greenhouse.
The agave became somewhat of a celebrity around this time as well. Thought to have been dying, the plant cheated death and achieved full bloom in the summer.
Some people, like Dwayne Sawchyn, waited in line for over an hour Thursday, anxious to get their seeds and head for warmer pastures.
"I never line up for anything, but hey this would definitely be a plant with a story," he said.
Agave plants only flower once over their lifetime, signifying the end of their lives, but one woman near the back of the line was thinking about the beginning of the plant's life.
Elise Doane believes Agave Maria may have been an agave she donated to the gardens more than 30 years ago.
"There's no way to know for sure, but it would be a really fun way for it to come full circle," she said.
On a trip to the Virgin Islands, Doane brought home her agave, but it got too big to care for.
"I had to get rid of it. The park was willing to take it and I think this may actually be it," she said.
She called the Public Gardens several times about the plant, but they didn't have a record of who donated it. Still, she was looking forward to possibly getting a seed.
"It would be so, so cool to be able to get one," she said.
The seeds went quickly and were handed out within six minutes.
More than 50 people, including Doane, didn't get a seed.
Well, I'm extremely happy to see that my Son Dwayne Sawchyn was a Happy One to get a seed. He will treasure and nurture it with great care and love.
Thank you all for the happy growing season to come.
Too bad since the lineup for the seeds was long the person who was distributing them gave out two ore three seeds so all went home with some. Side the plant grows really big that's all the need. Where does one hear this news the seeds would be distributed?


FISH (Fluorescence in situ Hybridization) It is a technique used to analyze sperm chromosomes, allowing study numerical and structural alterations.
These analyzes have revealed that about 6% of patients with normal somatic karyotype consulting for infertility it presents meiotic alterations in their spermatogenic cells. This percentage may be increased to a 17,5% in individuals with severe oligoasthenoteratozoospermia and normozoospermic patients with one or more previous IVF failures, up 27%. These cases can affect the production of gametes with chromosomal abnormalities, at the same time, increases the risk of having children affected.
1st Floor - Query 11.
What is necessary to carry out artificial insemination?


text:
\section{Introduction}
As the detection rate of gravitation waves (GWs) from merging
double-compact-object (DCO) binaries increases with the sensitivity of the
ground-based GW detector network
\citep{Aso2013,LIGOScientificCollaboration2015,Acernese2015,Abbott2018,Buikema2020,Tse2019,Acernese2019,Akutsu2021},
we are beginning to constrain the astrophysical processes which shape the
evolution of GW progenitor populations. One of the most common ways to study
progenitor populations of GW mergers is through population synthesis simulations
of stellar populations from a host of formation environments. In the case of isolated binary star evolution, merging
double compact objects can form from massive binary stars through the
standard stable mass transfer or common envelope channels
\citep[e.g.][]{Belczynski2002, Dominik2012, Belczynski2016, Stevenson2017, Zevin2020, Bavera2021, Broekgaarden2021, VanSon2022}
as well as through chemically homogenous evolution \citep{Mandel2016, Marchant2016, deMink2016}
or with population III stars \citep[e.g.][]{Belczynski2004, Kinugawa2014, Inayoshi2016, Inayoshi2017, Tanikawa2021, Tanikawa2022}.
Merging DCO binaries can also originate from a wide variety of dynamically active environments including
triple (or higher multiple) systems \citep[e.g.][]{Antonini2017, Silsbee2017, Fragione2019, VignaGomez2021},
as well as young stellar clusters \citep[e.g.][]{Ziosi2014, Banerjee2017, DiCarlo2020, Chattopadhyay2022},
globular clusters \citep[e.g.][]{PortegiesZwart2000, OLeary2006, Downing2010, Samsing2014, Rodriguez2015, Rodriguez2016, Askar2017, Rodriguez2019},
nuclear star clusters \citep[][]{Miller2009, Antonini2016}, or a mix of all three \citep[e.g.][]{Mapelli2022}.
Finally, more exotic channels like active galactic nuclei which combine both gravitational and gas interactions
\citep[e.g.][]{McKernan2018, McKernan2020, Secunda2020, Ford2021} or primordial black holes \citep[e.g.][]{Bird2016, AliHaimoud2017}
can produce merging DCOs observable with a ground-based detector network. For a discussion of the relative rates of each
formation environment and channels within, see \citet{Mandel2022} and references therein.

Traditionally, population synthesis studies simulate merging DCO populations
with a Monte-Carlo approach.  Using theoretically motivated distributions of
initial parameters like age, metallicity, component mass, orbital separation,
and eccentricity, initial populations are evolved with fixed astrophysical
assumptions, or population synthesis hyperparameter settings like the stability
of Roche-overflow mass transfer, common envelope ejection efficiency, or the
strength of compact-object natal kicks, to produce a
synthetic catalog of DCO mergers which can be compared to parameterized models
derived from observations. This approach relies on several assumptions, both in
the simulations and model parameterizations fitted to the GW data, which are
unlikely to be fully correct.  For example, there is no reason to suppose that
the entire population of DCOs should evolve with the same fixed hyperparameters;
there is no a priori reason the fitted parameterized model should capture the
relevant features of the observed DCO distributions to correspond to the binary
physics of interest; etc. A better approach would be to compare progenitor
parameters and hyperparameter settings directly to DCO observations, treating
the population synthesis model as a mapping from progenitor to merger
parameters; merger parameters can then be mapped into observations using a
gravitational waveform family, and parameter inference proceeds in the usual
way, propagating information back up the mapping chain
\citep[e.g.][]{Veitch2015}.  A similar methodology, though with \emph{fixed}
hyperparameter settings, was advanced in \citet{Andrews2018,Andrews2021}, as we
discuss in more detail below.

Attempting to approach such an improved inference procedure for evolutionary
hyperparameters using traditional en mass Monte Carlo simulations of entire
populations of DCO mergers is computationally infeasible. Even with recent
developments in using emulators to speed up the simulation process
\citep[e.g.][]{Wong2021}, training the emulators still requires a significant
amount of computation to cover a wide range of uncertainty in the hyperparemeter
space. As an example, to emulate a model with $10$ parameters, the simplest way
to construct a training set of simulations is to run simulations on a grid which
varies combinations of uncertain physics. For $10$ uncertain physical processes,
if we consider $2$ variations for each physical process this would still require
$1024$ simulations. Because population synthesis simulations require hundreds to
thousands of cpu hours, training an emulator which spans a high dimensional
uncertainty space remains an impossibility at present.  Thus inference of
hyperpameter settings must proceed \emph{dynamically}, generating trial DCO
systems via population synthesis recipes to match a particular observation one-
or few-at-a-time while simultaneously adjusting the hyperparameters. (Eventually
it may be even be possible to use more physically-motivated modeling of binary
physics \citep[e.g.][]{Gallego-Garcia2021} in such a procedure.)

\citet{Andrews2021} (hereafter A21) used \texttt{DartBoard} \citep{Andrews2018}
to determine the ZAMS parameters which produce GW150914-like BBH merger based on
posterior samples for GW150914 and a fixed set of hyperparameters which define
assumptions for how isolated binary-star interactions proceed using
\texttt{COSMIC}, a binary population synthesis code \citep{Breivik2020}. The
approach is very similar to the one advocated here \emph{except} that
\citet{Andrews2021} treated the evolutionary hyperparameters for the binary
physics as fixed within each analysis.  The key extension in this work, which
will enable population modeling of \emph{both} progenitor parameters and
hyperparemeter settings, including any possible \emph{dependence} of
hyperparameter settings on progenitor parameters, is to allow these
hyperparameters to vary at the same time as intrinsic properties of the
progenitor system to produce a joint inference over the intrinsic properties of
the progenitor and the necessary hyperparameter settings to produce the observed
merger properties.

In full: we propose a method to ``backward" model each GW event to its
progenitor state while allowing the hyperparameters to vary across their full
range of physical uncertainty following a two-stage process. First, we solve a
root finding problem to obtain guesses that are likely to produce the desired
system properties in the joint progenitor--hyperparameter space. We then sample
the posterior in the joint space that is induced by the DCO merger observations
using a Markov chain Monte Carlo (MCMC) algorithm that is initialized by the
roots found in the previous stage.  We demonstrate our algorithm in a realistic
setting by producing a posterior over progenitor properties and \texttt{COSMIC}
hyperparameters implied by the observation of GW150914.

We find that the progenitor properties and even the ability to produce a
GW150914-like merger event is strongly correlated with hyperparameter settings;
different assumptions about the black hole masses at merger in GW150914 imply
wildly different formation channels and ZAMS progenitor masses for this event
and some nearby combinations of ZAMS masses are unable, with any reasonable
hyperparameter settings, to produce a DCO merger like GW150914.  We further
exhibit preliminary results of an ongoing analysis over the entire GWTC-3
catalog \citep{GWTC-3} that suggest that the accretion efficiency in stable mass
transfer may depend non-trivially on the primary black hole mass in merging
systems; our methodology allows for a systematic study of such dependencies,
which we will explore more fully in future work.

The rest of the paper is structured as
follows: We detail our method in Sec. ~\ref{sec:method}. In Sec.
~\ref{sec:result}, we show the results of applying our method to a number of
real events. We discuss the implications of this work and future direction in
Sec. ~\ref{sec:discussion}.

\section{Method}
\label{sec:method}

We define the progenitor's zero age main sequence (ZAMS) properties like
mass, orbital period, and eccentricity as progenitor parameters $\bm{\theta'}$, the parameters
that control different uncertain physical prescriptions such as wind strength and common
envelope efficiency as hyperparameters $\bm{\lambda}$, and random variables
that affect certain stochastic process such as whether CO natal kick unbinds a
binary as $\bm{X}$. To avoid clutter in the following derivation, we denote all
the parameters related to mapping a particular progenitor system into a GW event
collectively as evolutionary parameters $\bm{\Theta}$, which includes
$\bm{\theta'}$, $\bm{\lambda}$, and $\bm{X}$.

Once all the parameters including a particular draw of all the random variables
represented by $\bm{X}$ are known, the population synthesis code is a
deterministic function that transforms the properties of the progenitors into
the GW parameters $\bm{\theta}$:
\begin{equation}
    \bm{\theta} = \bm{f}\left( \bm{\Theta} \right).
\end{equation}
The mapping $\bm{f}$ from $\bm{\Theta}$ to $\bm{\theta}$ can be many-to-one
due to degeneracies in the different physical processes and initial parameters
of the GW event progenitors.
In order to draw inferences about $\bm{\Theta}$ from GW data, we
must be able to evaluate the likelihood of that data at fixed progenitor
parameters, namely
\begin{equation}
    p\left( d \mid \bm{\Theta} \right) = p\left( d \mid \bm{\theta} = \bm{f}\left( \bm{\Theta} \right) \right).
\end{equation}
The equality holds because the likelihood depends only on the gravitational
waveform generated by parameters $\bm{\theta}$ onto which the progenitor
parameters map.  In principle this likelihood could be computed at arbitrary
values of $\bm{\Theta}$ using the same machinery that is used to estimate source
parameters in GW catalogs \citep{Veitch2015,Ashton2019,Romero-Shaw2020,GWTC-3}
to develop samples of progenitor parameters, hyperparameters, and random
variables in $\bm{\Theta}$ from a posterior density.

Since the GW likelihood function
ultimately depends only on the GW parameters $\theta$, and GWTC-3 already has samples over these parameters from a posterior density
\begin{equation}
    p\left( \bm{\theta} \mid d \right) \propto p\left( d \mid \bm{\theta} \right) \pi_\mathrm{GW} \left( \bm{\theta} \right),
\end{equation}
where $\pi_\mathrm{GW}$ is the prior density used for sampling, we can save the
computational cost associated with evaluating the GW likelihood by rewriting the
posterior density of $\bm{\Theta}$ in terms of the posterior density of
$\bm{\theta}$, namely

\begin{align}
    p(\bm{\Theta} | d) = \frac{p(\bm{\theta}(\bm{\Theta})| d) \pi(\bm{\Theta})}{\pi_\mathrm{GW}(\bm{\theta}(\bm{\Theta}))}.
\end{align}
We apply a kernel density estimator with a Gaussian kernel to the posterior
samples released in GWTC-3 to estimate $p(\bm{\theta}(\bm{\Theta})|d)$.

Including hyperparameters and random variables
drastically increases the dimensionality of the problem, which can make the
sampling process much more computationally expensive to converge. To speed up
the convergence, we first solve a root-finding problem to find points
$\bm{\Theta}$ that will generate GW parameters $\bm{\theta}$ close to the bulk
of the posterior density of a GW event.  We then use those points to initialize
a set of chains in the MCMC process.

For each posterior sample point in the GW-observable space,
we can find the corresponding evolutionary parameters by solving an optimization problem that minimizes
the mean square difference between the GW event parameters and evolutionary parameters as:

\begin{align}
\mathcal{L}(\bm{\Theta},\bm{\theta}) = ||f(\bm{\Theta})-\bm{\theta}||^2.
\label{eq:loss}
\end{align}

In principle, we should only accept solutions that exactly reproduce the LVK posterior samples in the GW-observable space.
However, it is not feasible to achieve such a condition in practice, therefore we relax the condition in eq.~\ref{eq:loss}
to a small acceptance threshold. For this study, we picked a threshold of $10^{-2}$. To make sure we find a reasonably
complete set of progenitor parameters that corresponds to the posterior sample point, we use 1000 different initial guesses
in solving the optimization problem. As long as the solution fulfills the acceptance criteria, the root is as valid as all
other roots that fulfill the same acceptance criteria, \emph{regardless to its initial guess}.
This means, we have the freedom to choose the set of initial guesses however we think might benefit the optimization.

Most of the points in the evolutionary parameter space do not produce DCO mergers in a Hubble time. For systems that do not merge,
we set the binary masses to be $0$ such that the gradient for the same systems is also $0$ and leads the root finder to get stuck on
its first step.{\footnote{On a plateau of constant loss, the root finder performs no better than a random guess.
Because of this, a root finder in a high dimensional space will require a significant amount of computation
to get close to a solution.}} Therefore, it is beneficial to choose initial guesses in region of the evolutionary parameter
space that are likely to produce DCO mergers. To construct a list of initial guesses, we evolve a set of
ZAMS parameters uniformly sampled from the initial binary parameter space, then keep the systems that
merge within a Hubble time.

Retaining explicit control over random variables allows us to marginalize over
their contribution, and thus allows us to focus on progenitor parameters and
hyperparameters. The strength and direction of natal kicks for compact objects
are directly specified in the \texttt{COMPAS} binary population synthesis code
\citep{Riley2022} and can also be specified in \texttt{COSMIC}, however
this requires the user to specify the strength and direction of natal kicks as
inputs through a user-specified pre-processing script.  In this study, we use
\texttt{COSMIC} in it's default state which does not specify the kick strength
and direction at run time.
This means that the process of evolving the binary
is not fully deterministic. Thus, even if the root-finding algorithm performs
perfectly, forward modelling a set of roots does not guarantee that the
simulated population reproduces exactly the set of posterior samples due to
randomness in the evolution of each binary. To assure that the recovered
progenitor and hyperparameters robustly correspond to the posterior in the
GW-observable space, we push forward (or ``reproject'') the recovered
evolutionary parameters to the GW-observable space to check whether the
reprojected posterior agrees with the posterior given by the LVK collaboration.

We use KL divergence to measure the agreement between the two posterior
distributions as:
\begin{align}
D_{KL}(P||Q) = \int P(\bm{x}) \log(P(\bm{x})/Q(\bm{x})) dx.
\label{eq:KLdivergence}
\end{align}

\noindent A small KL divergence means the reprojected \texttt{COSMIC} posterior is similar to the original posterior in the
observable space, and is thus a viable channel for that specific event. Otherwise, it either means \texttt{COSMIC}
can only explain part of the posterior or cannot explain the event at all. This is completely expected behavior since
\texttt{COSMIC}, and isolated binary evolution more generally, carries its own assumptions and is expected to
fail in reproducing a subset of the event in GWTC-3. One example of this is GW events with at least one component
with mass above the pair instability supernova mass limit \citep{Woosley2017, Farmer2019}.
The reprojection could also be subject to stochasticity in the evolution of each binary.
To account for this, we reproject the posterior multiple times with different random seeds and
check whether the KL divergence varies significantly. A varying KL divergence means a particular GW event is subject
to randomness in the evolution of the progenitor, and extra caution should be used when interpreting the result.

\section{Results}
\label{sec:result}

\begin{table*}[hbt!]
    \begin{center}
    \begin{tabular}{ l l l }
    \hline
    \hline
    Parameters &  Description & Optimization range\\
    \hline
    \hline
    Observables &\ &\  \\
    \hline
    \hline
    $m_{\rm 1, GW}$ & Primary mass of the GW event & NA \\
    $m_{\rm 2, GW}$ & Secondary mass of the GW event  & NA\\
    \hline
    \hline
    Progenitor parameters &\ &\  \\
    \hline
    \hline
    $m_{\rm 1, ZAMS}$ & Primary mass at ZAMS & $[10,150]\ M_{\odot}$\\
    $m_{\rm 2, ZAMS}$ & Secondary mass at ZAMS & $[10,150]\ M_{\odot}$\\
    $t_{\rm orb}$ & Orbital period at ZAMS & $[5,5000]$ days\\
    $e$ & Eccentricity at ZAMS & $[0,1]$\\
    $Z$ & Metallicity at ZAMS & $[10^{-4},2\times10^{-2}]$\\
    $z$ & Redshift at ZAMS & NA\\
    \hline
    \hline
    hyperparameters &\ &\ \\
    \hline
    \hline

    $\alpha$ & Common envelope efficiency & $[0.1,10]$\\
    $f_{\rm acc}$ & Fraction of accretion during stable mass transfer & $[0,1]$\\
    $q_{\rm crit,3}$ & Critical mass ratio on the Hertzsprung Gap & $[0.1,10]$\\
    $\sigma$ & Root mean square of Maxwellian natal kick distribution& $[10,300]\ {\rm km/s}$\\

    \hline
    \hline
    \end{tabular}
    \caption{A list of parameters used in this study.}
    \label{tab:parameters}
    \end{center}
\end{table*}

We apply the method described in section \ref{sec:method} to the first GW event GW150914 \citep{GW150914}.
We use the \texttt{Overall\_posterior} posterior samples for GW150914,
publicly available from the Gravitational wave Open Science Center \citep{LIGOScientific:2019lzm}.
The parameters involved in the analysis and the range we allow for the inference are tabulated in table \ref{tab:parameters}.
The spin of BHs formed in isolated binaries depends strongly on the angular
momentum transport in massive stars which is still highly uncertain (see however \citet{Fuller2019, Bavera2020}),
therefore we only consider the two component masses in the observable space in both the
root-finding stage and the MCMC stage. For progenitor parameters, we characterize each guess with
five parameters: the two component masses $M_{\rm 1,ZAMS}$ and $M_{\rm 2,ZAMS}$, the orbital period $t_{\rm orb}$,
the eccentricity $e$, and the metallicity $Z$ at ZAMS. Note that the progenitor formation redshift is not
obtained through the root-finding process because the formation redshift does not intrinsically affect
the evolution of the binary. Instead, we compute the time it takes for the binary to evolve from
formation to the merger and add this time to the lookback time when a GW event is observed and limit the total
time to merger to be less than $13.7\,\rm{Gyr}$.
Using the total lookback time, we can compute the redshift of the binary at ZAMS formation following the
Planck 2018 cosmological model \citep{Planck2018}.
The main benefit of post-processing the redshift in this way is that we do not rely on a particular assumption
of star formation rate (SFR) distribution when we solve for the posterior distribution in redshift.
This means we can put the prior on formation redshift (or in general, metallicity-redshfit distribution) in
by reweighting the posterior distribution according to a particular SFR model,
and therefore do not have to rerun the inference every time we change the SFR model. This is especially helpful
since SFR models are still highly uncertain but strongly impact the local merger rates of BBHs \citep[e.g. ][]{Broekgaarden2021}.
For hyperparameters, we choose parameters that strongly affect
binary evolution in \texttt{COSMIC} for massive stars, including the common envelope
efficiency $\alpha$, the fraction of mass accreted onto the accretor during stable mass transfer $f_{\rm acc}$,
the critical mass ratio which determines whether Roche-overflow mass transfer
proceeds stably or produces a common envelope when the donor star is on the Hertzsprung gap
$q_{\rm crit,3}$, and the root-mean-square of the Maxwellian distribution
employed for CO natal kicks, $\sigma$. For systems which begin a common envelope
with a Hertzsprung-gap donor, we always assume the pessimistic outcome that the two
stars merge since the donor has likely not formed a strong core-envelope boundary
\citep{Ivanova2004, Belczynski2008}.

We show a portion of the joint posterior of the progenitor parameters and
hyperparameters of GW150914 in figure \ref{fig:GW150914_posterior}. Each panel
is colored based on the comparison between progenitor parameters (blue),
hyperparameters (orange), or a mix of the two (green). We find that the choice
for $\sigma$ does not affect the formation of GW150914-like BBHs. This is not
unexpected since we use the \citet{Fryer2012} delayed model which reduces the
natal kick strength at BH formation based on the amount of fallback onto the
proto-CO. In the case of GW150914-like BBHs, the BH progenitors are massive
enough that the fallback reduces the natal kick to zero. Because of this we do
not include $\sigma$ in Figure~\ref{fig:GW150914_posterior}. Similarly, we do
not include the ZAMS orbital period and eccentricity, which are correlated with
one another, but not strongly with the other progenitor parameters or
hyperparameters. We find strong correlations between the ZAMS masses, as well as
strong correlations between $M_{2,\rm{ZAMS}}$ and $f_{\rm{acc}}$, and
$f_{\rm{acc}}$ and $\alpha$. We show scatter plots of each of these combinations
in the upper-right inset of the figure.

The correlations between the ZAMS masses are similar to those found by A21 with
the majority of the population preferring primary and secondary masses between
$60$--$90\,M_{\odot}$. However, we also find some ZAMS masses which extend up to
$150\,M_{\odot}$ which is the limit imposed by our assumptions. We explore the
formation scenarios which lead to successful GW150914-like mergers and those
which fail to produce GW150914-like mergers below in
Figure~\ref{fig:compare_fixed_variable}.

The correlations between $M_{2,\rm{ZAMS}}$ and $f_{\rm acc}$ illustrate the
variety of ways which GW150914-like mergers can be produced. For binaries with
$M_{2,\rm{ZAMS}} < 70\,M_{\odot}$, we find that accretion efficiencies of
$f_{\rm acc} > 0.5$ are preferred. One reason for this is based on the
requirement that the total mass in the binary must remain above the total mass
of GW150914 and strongly non-conservative mass transfer (i.e. $f_{\rm acc} <
0.5$) reduces the total mass of the system. A compounding factor is that as mass
leaves the binary due to non-conservative mass transfer, the evolution of the
binary's orbit is less dramatic and leads to wider binaries on average and thus
fewer mergers in a Hubble time. For binaries with $M_{2,\rm{ZAMS}} \sim
80\,M_{\odot}$, $f_{\rm acc}$ is less constrained. This is because of a
preference for these secondaries to also have primary masses near $
80\,M_{\odot}$ and thus enter a double-core common envelope evolution in which
both stars' envelopes are ejected, leaving behind two stripped helium cores in a
tight orbit. In this case, $f_{\rm acc}$ does not affect the binary evolution
and is thus unconstrained. This effect can also be seen in the ZAMS mass and
$q_{\rm crit, 3}$ panels for masses near $80\,M_{\odot}$ because double-core
common-envelope evolution is triggered in \texttt{COSMIC} when the radii of the
two stars touch due to the rapid expansion of the primary star upon helium
ignition. In this case, the choice for Roche-overflow mass transfer to proceed
stably (as prescribed by $f_{\rm{acc}}$) or unstably (as prescribed by $\alpha$)
using $q_{\rm crit, 3}$ is totally irrelevant, and thus unconstrained. Finally,
for binaries with $M_{2,\rm{ZAMS}} > 80$, we find that $f_{\rm acc}$ is
correlated to decrease with increasing mass. This is due to limits on the total
mass which must be ejected from the binary to produce BH masses that match
GW150914, the reverse situation to $M_{2,\rm{ZAMS}} < 70 \, M_\odot$. Binaries
with both component masses near $150\,M_{\odot}$ must either go through a common
envelope evolution (in which case $f_{\rm acc}$ is unconstrained), or very
non-conservative mass transfer (where $f_{\rm acc}$ is low), to produce BBHs
with the proper mass.

Finally, we find that $\alpha$ and $f_{\rm acc}$ are largely uncorrelated,
though there exist independent trends in each hyper parameter. This is not
totally unexpected since the physical processes which are described by each
hyperparameter, i.e. stable Roche-lobe overflow and common envelope evolution
are two independent channels. Generally, we find that GW150914-like BBHs tend to
prefer larger accretion efficiencies and have common envelope ejection
efficiencies peaking near $\alpha=1$. One shortcoming of our method
implementation is the application of a single hyper parameter for
$f_{\mathrm{acc}}$ and $\alpha$ for each binary, while both the primary and the
secondary star could in principle be defined by their own hyperparameters that
prescribe the outcomes for when each star fills it's Roche lobe. We reserve full
treatment of this for future work but note that this improvement could reveal
correlations between hyperparameters that are not present in our current
analysis.

\begin{figure*}[h]
    \includegraphics[width=\textwidth]{figures/GW150914_corner_zoomed_lowres.png}
    \caption{The posterior for GW150914 in both the progenitor parameter space and hyperparameter space.
    $M_1$ and $M_2$ are the progenitors' masses. $\log{Z}$ is log metallicity at ZAMS.
    $z$ is the redshift at ZAMS.
    $\alpha$ is the common envelope efficiency.
    $f_{\rm acc}$ is the fraction of mass accreted during stable mass transfer.
    $q_{\rm crit, 3}$ is the critical mass ratio on the Hertzsprung Gap.
    The contours correspond to the $68\%$ and $95\%$ confidence intervals.
    Note that the redshift is not fitted during the root finding process or the MCMC process.
    Once we find the evolutionary parameters, we add the delay time to the lookback time of the observed posterior sample,
    then from the total lookback time we can compute the redshift at ZAMS.
    We highlight three panels in the corner plots to show the fine structure of the set of posterior samples in the evolutionary parameter space.
    We also color the posterior in a particular panel according to the type of parameters involved in the corner plot.
    Blue denotes panels that include only progenitor parameters,
    green denotes panels that include a mix of progenitor parameters and hyperparameters,
    and orange denotes panels that include only hyperparameters.
    }
    \label{fig:GW150914_posterior}
    \script{figure1_cornerPlot.py}
\end{figure*}

Once we obtain a set of binaries which successfully map the ZAMS parameters and
hyperparameters to BBH merger masses, we re-evolve the set of ZAMS parameters
with the same physical assumptions as A21, but vary the common envelope
efficiency to explore how keeping a fixed model which only varies one
hyperparameter contrasts to our results.
Figure~\ref{fig:compare_fixed_variable} shows the distribution of ZAMS masses
for three models (first through third columns), each with a different $\alpha$
but the same hyperparameters as A21, as well as the results of our sampling
which allows our hyperparameters to vary (fourth column). We find that holding
the accretion efficiency, $f_{\rm{acc}}$, and common envelope ejection
efficiency, $\alpha$, to fixed values greatly reduces the ZAMS parameter space
that produces GW150914-like mergers. In contrast, by allowing the
hyperparameters to fully span the model uncertainty, we find that there are
distinct ZAMS parameters which produce GW150914-like mergers.

Because we can explore the full evolutionary parameter space, we can also
determine that there are ZAMS parameters which fail to produce GW150914-like
mergers \emph{regardless of our hyperparameter choice.} For primary ZAMS masses
between $\sim95-135\,M_{\odot}$ and secondary ZAMS masses between
$\sim50-95\,M_{\odot}$, we find that there is no combination of accretion
efficiency and common envelope ejection efficiency which produces merging BBHs
that have masses consistent with GW150914's posteriors. In this region, if BBHs
with masses consistent with GW150914's masses are produced through a combination
of $\alpha$ and $f_{\rm{acc}}$, they do not merge in a Hubble time. Conversely,
in the region of the fourth column of Figure~\ref{fig:compare_fixed_variable}
which does produce GW150914-like mergers, the combination of $\alpha$,
$f_{\rm{acc}}$, and the ZAMS masses and orbital separations balance to produce
BHs with the correct masses that merge within a Hubble time.

\begin{figure*}
    \includegraphics[width=0.98\textwidth]{figures/compare_fixed_variable.png}
    \caption{Comparison of ZAMS masses for binaries which produce GW150914-like mergers for three variations of $\alpha$
     with a fixed set of parameter assumptions matching those of A21 (first three columns) and for binaries which produce
     GW150914-like mergers when $\alpha$, $f_{\mathrm{acc}}$, and $q_{crit,3}$ are allowed to vary, (fourth column).}
    \label{fig:compare_fixed_variable}
    \script{figure2_varyAlphaFacc.py}
\end{figure*}

It is interesting to re-project the posterior over progenitor parameters ($\bm{\theta}'$)
and hyperparameters ($\bm{\lambda}$) using fresh random variables ($\bm{X}$) to
the observable space of GW parameters ($\bm{\theta}$).  Agreement between the
observed parameters and the re-projected parameters indicates good exploration
of the random variable space and lack of sensitivity to the details of these
random parameters.  Figure \ref{fig:GW150914_reprojection} shows good agreement
between the re-projected root-finding outputs as well as the re-projected MCMC
draws for our analysis of GW150914.  Unlike \citet{Andrews2021}, we find there
are no regions of observable space inaccessible to our evolutionary models; this
difference arises because we allow the evolutionary hyperparameters
$\bm{\lambda}$ to vary.

\begin{figure}
\includegraphics[width=0.49\textwidth]{figures/GW150914_reprojection.pdf}
\caption{Reprojecting the posterior in evolutionary parameter space of GW150914 to observable space.
The contours correspond to the $68\%$ and $95\%$ confidence intervals.
The blue contour is the reprojected posterior after the root-finding procedure.
The orange contour is the reprojected posterior after the MCMC procedure.
The green contour is the posterior plotted using the original LVK posterior samples.
}
\label{fig:GW150914_reprojection}
\script{figure3_sanityCheck.py}
\end{figure}

To illustrate the potential benefit of using our method on the population level,
we perform the same analysis for all events in GWTC-3.
For events announced in GWTC-1, we use \texttt{Overall\_posterior}, \texttt{PublicationSamples},\texttt{IMRPhenomXPHM\_comoving} and \texttt{C01:Mixed} posterior samples, respectively.
All the data are publicly available from the Gravitational wave Open Science Center \citep{LIGOScientific:2019lzm}.
Plotted in figure
\ref{fig:GWTC-3_f_acc_mass} is the posterior density in the $m_{1,{\rm
GW}}-f_{\rm acc}$ space for most of the events in GWTC-3.
Each contour represents
the $68\%$ credible interval of the posterior density for that particular event.
There is a suggestive trend showing that $f_{\rm acc}$ could increase as the mass of
the progenitor increases. Such a trend implies the stable mass transfer
phase of a less massive binary would be preferentially non-conservative, with
more conservative mass transfer in more massive binary systems.

Note that some events did not pass the KL divergence test we proposed in section
\ref{sec:method}; we do not include these systems in figure
\ref{fig:GWTC-3_f_acc_mass}. Binaries that form low-mass compact objects have
lower amounts of fallback and tend to have correspondingly larger variance in
their random natal kicks. Larger kicks can unbind the progenitor binary, or lead
to wide binaries that do not merge within a Hubble time.  In these cases, the
extra variance during the reprojection can produce a posterior that may not
agree with the original posterior, hence yielding a higher KL divergence.

For high-mass binaries, \texttt{COSMIC} struggles to produce events above the
pair instability supernova mass cutoff, so the posterior in the
evolutionary parameter space only corresponds to part of the posterior in the
observable space below this cutoff, and therefore events beyond the lower edge of the PISN mass
gap also have higher KL divergence.

Events with more extreme mass ratios are hard to produce with \texttt{COSMIC},
and therefore less likely to be accurately recovered by our method \citep[e.g.][]{Zevin2020}. This could
be due to our method assuming a single value for $f_{\rm acc}$ and $\alpha$ as
discussed in Section~\ref{sec:result}.

Merger observations for which \texttt{COSMIC} struggles are likely to be very
informative about formation channels and binary evolution physics, and are
therefore likely worthy of close study.  We anticipate that future work will
follow up these events in detail.

Figure \ref{fig:GWTC-3_f_acc_mass} shows that our method could in principle
reveal the correlation between progenitor parameters and hyperparameters on a
population level. Here we impose a cut to eliminate events with KL divergence larger
than 0.1.
This is a heuristic choice to exclude events that are obviously not compatible with
\texttt{COSMIC}.
A careful treatment of all events in the catalog and
discussion related to the detailed physical implications of figure
\ref{fig:GWTC-3_f_acc_mass} is beyond the scope of this paper.  We defer a
detailed study of the physics related to the population of GW events to future
work.

\begin{figure}
\includegraphics[width=0.49\textwidth]{figures/GWTC3_f_acc_mass.pdf}
\caption{
    The posterior density in the $m_{1,{\rm GW}}-f_{\rm acc}$ space for most of the events in GWTC-3.
    Note that $m_{1,{\rm GW}}$ here refers to the reprojected posterior instead of the posterior released by LIGO.
    Each contour is the $68\%$ credible interval of the posterior density for a particular event.
    At $m_{1,{\rm GW}} \sim 45 M_{\odot}$, the pair instability supernova mechanism prevents \texttt{COSMIC} from producing events that are more massive than this cutoff.
    Therefore, events with the majority of posterior support above this cutoff are not compatible with \texttt{COSMIC}, hence have a large KL divergence and are excluded from this figure.
    On the low mass end, neutron star binaries or neutron star-black hole binaries are subjected to randomness induced by the natal kick,
    also resulting in a larger and fluctuating KL divergences, and therefore are also excluded from the analysis.
}
\label{fig:GWTC-3_f_acc_mass}
\script{figure4_population.py}
\end{figure}

\section{Discussion}
\label{sec:discussion}

We present a new pathway to understand binary evolution with GW events in this
paper. Instead of forward modelling an assumed distribution of initial binaries
to the observed population, we find the corresponding evolutionary parameters
event-by-event. In this first work, we showcase the power of the proposed method
with an application to GW150914. We show the joint posterior of the event's
progenitor parameters and hyperparameters.  Our work is both a more efficient
way to study GW event progenitors, and also allows the possibility of
constraining the astrophysics related to binary evolution, especially by
capturing the correlation between hyperparameters in different systems.

Our results suggest that the accretion efficiency during stable mass transfer
may depend on the primary black hole mass.  In general, our method returns the
joint posterior distribution of progenitor parameters and hyperparameters for
each event, which enables a data-driven way to study the distribution of
hyperparameters.  That is, once we have a catalog of events, each has their own
posterior in the hyperparameter space, and we can employ well-known techniques
such as hierarchical Bayesian analysis to fit a population model to the
distribution of hyperparameters; this avoids making overly-specific assumptions
like fixing the hyperparameters for all types of event.

Working event-by-event as we do permits post-processing application of
arbitrarily complicated models of star formation and metalliticy evolution by
re-weighting the samples we obtain \citep[e.g.][]{VanSon2022}. Once we have
pulled the GW event posterior back from the observable space to the evolutionary
parameter space, we can apply the same hierarchical inference methods currently
used to infer the compact binary population to our progenitor population.  In
particular, we can use our progenitor population to infer the formation rate of
compact binary population progenitor systems over cosmic time without needing to
make artifical and simplistic assumptions about the delay time distribution or
the metallicity-specific star formation rate
\citep{Vitale2019,Ng2021,VanSon2022}.  Comparing the formation rate of
progenitors to the star formation rate provides an avenue to check our
understanding of binary evolution and the relative rate of other formation
channels.

While our method allows data-driven exploration of the hyperparameters space for the first time, there are a number of improvements that can be implemented in future studies.
In this study we use only \texttt{COSMIC} as our evolutionary function, which by design cannot explain all the events in GWTC-3.
For example, events with either of the component mass larger than the lower edge of PISN gap such as GW190521 cannot be explained by \texttt{COSMIC}.
Alternative channels such as dynamical formation might be needed to explain some subset of the events in GWTC-3 \citep{Zevin2021}.
As the sensitivity of GW detectors increases, we expect to see more and more events that are unusual in some way.
Therefore, having a self-consistence population synthesis code that contains multiple formation channels is essential to accommodate the growing catalog of GW events.
In this paper, our main focus is to illustrate the concept of "back-propagating" GW-event posterior samples,
highlighting the capability of our method and motivating the benefits of building population synthesis codes that can work seamlessly with our method.
To avoid cluttering of focus, we discuss the physical implications of the results presented in this work under our specific assumptions (i.e. using \texttt{COSMIC} as our evolutionary function) in a future companion paper.

Due to the implicit definition of random variables in \texttt{COSMIC}, our evolutionary function is stochastic.
This introduces significant inefficiency in our root-finding and sampling algorithm.
The main stochasticity in \texttt{COSMIC} comes from natal kick, which significantly affect the evolutioary pathway of low mass events such as BNS mergers.
The effect of the natal kick is suppressed for heavier mass events due to fallback.
This means events with lighter masses are subject to stochasticity of the function,
where the sampling process for heavier events behaves as if the evolutionary function we use is deterministic.
Due to computational limitation, we only try 1000 different initial guesses per posterior sample in the root-finding process.
This means any posterior sample that has a probability of merging rarer than 1 in 1000 could be missed.
Obviously the problems which comes with the randomness can be alleviated by performing more tries per posterior sample,
but this is not scalable in practice.
On top of limitation in efficiency, some formation channels require explicit control of random variables by construction.
For example, in a dynamical formation scenario such as binaries that form in a globular cluster,
each binary has some probability of undergoing a multi-body encounter with another member in the cluster.
These encounter probability distributions are either studied with direct N-body simulations or semi-analytical methods.
In both cases, each member of the cluster is no longer completely independent of the other members, but coupled through the encounter probability distribution.
By studying the encounter probability distribution, we can infer the properties of the environment which the binary lives in.
This can only be done if we have explicit control over the random variables that characterize the encounter probability distribution.

Another technical note is that we use finite differencing to estimate the gradient of the objective function, which could be a significant source of error near transition points in the evolutionary parameter space.
Also, finite differencing is increasingly inefficient as we increase the dimensionality of the problem.
To improve the accuracy and efficiency in estimating the gradient of the objective function, automatic differentiation is a promising feature that modelers should consider incorporating in their population synthesis codes in the future.

To summarize, we propose a novel method to recover the posterior samples in the evolutionary parameter space for each GW event.
We point out hyperparameters in the usual population synthesis simulation context are not actually parameters related to the population,
but parameters about the evolutionary function.
This means the binary evolution functions can be constrained on an individual event basis.
We "back propagate" the posterior in the observable space to the evolutionary parameter space,
thus allowing us to study hyperparameters and theirs correlations with progenitor parameters in a data-driven manner.
Our method makes less assumptions than the traditional forward modelling approach,
which often fix the hyperparameters across the entire population.
Since we are not limited to the fixed hyperparameters assumptions, we can explore the behavior of the hyperparameters across the population much more efficiently.
While our work lays down a data analysis pathway to understand the population of GW events,
no physics can be learned without a comprehensive physical model.
We hope this letter will motivate the construction of next-generation population synthesis codes that have the following properties:
first, they should retain explicit control over the random variables so marginalizing over random variables can be done precisely and
second, they should be as automatically differentiable as possible so that exploring the evolutionary parameter space is efficient.
By combining the methods presented in this work and future, differentiable population synthesis codes,
we can explore the full parameter space of binary evolution models with future GW data.

\section{Acknowledgement}
The authors are grateful for discussions with the CCA Gravitational Wave Astronomy Group.
The Flatiron Institute is supported by the Simons Foundation.  We thank M. Zevin for helpful comments and suggestions on this manuscript.
This research has made use of data or software obtained from the Gravitational Wave Open Science Center (gw-openscience.org),
a service of LIGO Laboratory, the LIGO Scientific Collaboration, the Virgo Collaboration, and KAGRA.
LIGO Laboratory and Advanced LIGO are funded by the United States National Science Foundation (NSF) as well as
the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS),
and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector.
Additional support for Advanced LIGO was provided by the Australian Research Council. Virgo is funded, through the European Gravitational Observatory (EGO),
by the French Centre National de Recherche Scientifique (CNRS), the Italian Istituto Nazionale di Fisica Nucleare (INFN) and the Dutch Nikhef,
with contributions by institutions from Belgium, Germany, Greece, Hungary, Ireland, Japan, Monaco, Poland, Portugal, Spain.
The construction and operation of KAGRA are funded by Ministry of Education, Culture, Sports, Science and Technology (MEXT),
and Japan Society for the Promotion of Science (JSPS), National Research Foundation (NRF) and Ministry of Science and ICT (MSIT) in Korea,
Academia Sinica (AS) and the Ministry of Science and Technology (MoST) in Taiwan.

\software{
    \texttt{corner}\ \citep{corner};
    \texttt{COSMIC}\ \citep{Breivik2020};
    \texttt{julia}\ \citep{Julia-2017}
    \texttt{matplotlib}\ \citep{matplotlib};
    \texttt{numpy}\ \citep{numpy};
    \texttt{pandas}\ \citep{McKinneyPandas, reback2020pandas};
    \texttt{scipy}\ \citep{scipy}
    \texttt{seaborn}\ \citep{Waskom2021}
    \texttt{showyourwork}\ \citep{Luger2021}
}

redpajama_set_name: RedPajamaArXiv


text:
FDC Foundation Donates $5K to Injured Nebraska Volunteer Firefighter
Brad Elder is a volunteer firefighter in Crete, Nebraska.
He's also a college professor at Doane University, teaching courses on Ecological Botany, Ecological Zoology, among others. He runs the school's Prescribed Burn program.
So he knows something about fire and nature and the unpredictability that emerges when the two forces meet.
On October 23, Elder sustained severe burns over 20% of his body while he was dispatched to help contain wildfires in Lancaster County, Nebraska. He's been hospitalized since, undergoing surgeries and skin grafts, with more on the way. He'll likely remain in the hospital until February.
With Elder's medical bills mounting, one of his friends and fellow firefighters reached out to Fire Dept. Coffee for help.
To help lighten his burden, reduce his expenses and give him a boost on the road to recovery, we were proud to contribute $5,000 to Elder.
"Battling wildfires is incredibly dangerous," Fire Dept. Coffee President and Founder Luke Schneider said. "No matter how much experience or knowledge you have, everything can change in an instant. We're grateful for men like Brad Elder who put themselves in harm's way to protect others, and we're happy to help in any way we can."
'Crawling Through the Fire'
While working to limit the damage from ongoing wildfires in the area of Hallam, Elder and another firefighter noticed that a home was directly in the path of a growing fire. They were setting up a controlled burn in an effort to redirect the fire and save the home, when the fire suddenly shifted.
"So I turn around, just start running. That was my first indication that it had changed direction," Elder told 10/11 Now News from the hospital a week after the event. "I'd actually pulled my glove off, about half a second before I got hit, to open up the valve on the drip torch and just got hit in the face."
He turned to escape, but tripped over his torch.
"Then I was just crawling through the fire," Elder said.
Once he and his fellow firefighter escaped, they called for help. A local sheriff's deputy met them and took them to an ambulance, which rushed them to the hospital.
While the other firefighter suffered less severe injuries, Elder sustained third-degree burns on his hands, legs and back. It required — and continues to require — multiple surgeries and a months-long stay in the hospital.
"It's not as bad as it could be," Elder said. "It could have been a lot worse. If all it takes is 90 days and a little bit of pain to walk away alive, I'll take it."
'A Learning Opportunity'
Elder's spirit of gratitude and optimism have carried him through the harrowing ordeal.
He will return to his role as a volunteer firefighter, he said, and he plans to use his experience as a teaching moment for his students.
"My plan is to address this as a learning opportunity," Elder said. "We're gonna sit down, we're gonna do a lessons learned series on this to look at what happened, how it happened, and then how to prevent things like this in the future."
But first, he must focus on recovery. Our $5,000 contribution will help with his mounting medical bills, and his fellow firefighters are also planning a large fundraiser in February to coincide with Elder's anticipated release from the hospital.
Because of the support from our customers, we are able to play our small role in Elder's recovery. We're thankful for his courageous service — and for the support that his friends, family and fellow firefighters continue to provide every day.
We know he'll be back on the job soon.
Also in Firefighter Support
FDC Foundation Raising Funds in Partnership with the Firefighter Cancer Support Network
In January, Fire Department Coffee customers can choose to make an extra donation to support the Firefighter Cancer Support Network.
Helping a NJ Firefighter Battle Back After a Series of Strokes
Union, New Jersey firefighter Brian Schmitt is working hard to rehabilitate after a series of strokes and, one day, return to work in the fire service.
Partnering with Meijer to Support the GRFD Fire Prevention Foundation
We're thankful for Meijer, the Grand Rapids Fire Department and its Fire Prevention Foundation for working with us to support first responders in overcoming the challenges related to illness or injury.

redpajama_set_name: RedPajamaCommonCrawl


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A growing number of our students have recently gained the Victoria College Junior Bronze Medal and some of the older candidates have been awarded the Associate Diploma in Presentation and Interview Skills. We are pleased to be promoting vcm speech exams once again.
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I am also pleased to get this announcement about the collage exams and it sure seems to be a good thing. One thing is for sure that it has been already decided that we are supposed to bring the change.
We are pleased to write that vcm exams are now available once again.
Day and night are the same length.


The following is a recording of a panel held on Aug. 31, 2014, at DragonCon in Atlanta. At that panel, U.S. Rep. John Lewis discussed his graphic novel memoir March, along with his co-author Andrew Aydin. The panel was moderated by Hogan's Alley editor Tom Heintjes. The recording picks up just as Heintjes asked Rep. Lewis about the genesis of the book.


Hip In Detroit: Detroit Gets Wide Open this Sunday!
When people ask us what makes Detroit special, we always give the same answer, the people. Without the people Detroit is just a bunch of concrete. The spirit of the city can be seen in the artwork and the culture, but you have to come out and be a part of the community to truly understand the city's heart.
Open Streets Detroit recognizes the importance of getting people outside to interact with each other, so they work hard to shut down a 3.5 mile strip of Southwest Detroit for one day every year. During the shutdown they invite everyone out to skate, bike, walk, jog, and have some outdoor fun before the cold weather hits.
This Sunday, October 7th, Open Streets Detroit will close down the streets of Southwest Detroit from noon until 5 p.m. During this time, there will be all sorts of family friendly events including yoga, dance, and basketball. This event is free for all to attend, but parking can be ruff. So if you can avoid driving, they highly recommend that you do.
Many of the stores along the route will be open during this event. This includes places to eat like Slows and Mercury Burger Bar, and places to shop like Eldarado General Store. You can even grab a coffee at Astro while you walk around the streets and see what everyone is up to.
To see the full map of the streets that will be shutdown click here.
Take a second and take a walk around Southwest Detroit this weekend. Experience the city up close and personal by walking it and talking to your neighbors!


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Chris Jericho Status For RAW 25 "Up In The Air", 205 Live Event Attendance, Ricochet At The WWE PC (Video)
Posted By: Ben Jordan Kerin on Jan 21, 2018
- Dave Meltzer revealed on the latest edition of Wrestling Observer Radio that Chris Jericho's status for Monday's 25th Anniversary of Raw is "up in the air" at the moment. He noted that as of the end of last week a deal had not be finalized for Jericho to appear. Meltzer said WWE is desperately trying to negotiate a deal as they have advertised him as appearing for the event.
- Last night's WWE 205 Live house at the Lowell Memorial Auditorium in Lowell, Massachusetts had around between 800 and 1000 fans in attendance. The venue holds at capacity around 2,800 although it is believed to be less for wrestling events due to the setup.
- WWE has posted footage of Trevor "Ricochet" Mann at the WWE Performance Center. In the video below Mann talks about finally joining WWE and the style he can bring to the company and his opponents.
Source: Wrestling Observer Radio Tags: #wwe #chris jericho


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'What a Day': Watch Moment Connecticut Cops Stop Yankees GM Brian Cashman at Gunpoint After Apparent Mix-Up
The confrontation came after police responding to a report of a man with a gun who had been seen driving a white Jeep spotted Brian Cashman's vehicle
Published at 2:00 pm on August 14, 2019
Body-camera footage released Wednesday by CT police show New York Yankees General Manager Brian Cashman getting stopped by cops at gunpoint
Incident was an apparent mix-up involving his own stolen vehicle and a separate report of an armed man at a doctor's office
Cashman told cops he reported the vehicle stolen earlier last week from nearby but the NYPD had recovered the vehicle in the Bronx
Body-camera footage released Wednesday by Connecticut police show New York Yankees General Manager Brian Cashman getting stopped by cops at gunpoint in an apparent mix-up involving his own stolen vehicle and a separate report of an armed man at a doctor's office.
The confrontation came after police responding to a report of a man with a gun who had been seen driving a white Jeep spotted Cashman's vehicle — which incorrectly was still listed as stolen despite having been recovered by New York police days earlier.
Cashman was stopped at a Shell gas station in Darien when he was surrounded by police.
"Driver turn off your car and put your hands up! Put your hands out the window," a Darien police officer is heard yelling on the video, which captures the cop with his gun pointed in Cashman's direction.
The footage shows Cashman -- in a dark T-shirt, white shorts and flip-flops -- exiting his vehicle with his hands in the air. He subsequently makes his way, backwards, following command, toward the officers.
He explains that he reported the vehicle stolen earlier in the week and the NYPD recovered it and returned it to him.
Cashman is allowed to go back to his vehicle to retrieve his identification, at which point the officer tells him, "You look very familiar to me."
"I'm the GM with the New York Yankees," Cashman replies.
"Yeah, I know, I used to see you as Brook Street Bagels when I was an Eastchester cop," the officer says, adding, "I apologize for the embarrassment."
An apparent officer at the scene explained to Cashman that they were responding to an unrelated report of a man who brought a gun at a doctor's office and had reportedly left in a white, Jeep-like vehicle. Then they ran the plates on Cashman's Jeep and found that it had been reported stolen.
"What a day," Cashman could be heard as he wiped his forehead while awaiting next to his vehicle and surrounded by police.
The Yankees' general manager said he reported the vehicle stolen earlier last week from nearby but the NYPD had recovered the vehicle in the Bronx and returned it to him.
It's not clear why his vehicle was not taken off the stolen list.
He was "fully cooperative with all commands and instructions given by the officers conducting the stop and the encounter was quickly, efficiently and properly deescalated," police said in a previous a statement.
"They executed a very tactful interception," Cashman told the NY Post.
"They're clearly very professional and trained and they asked me to turn my car off, exit the vehicle, walk backwards towards them…they were executing their duty."
Officers escorted him to the Norwalk police station, where he was initially driving to in order to have his car processed for evidence because he found items inside that he believed belonged to whomever stole his car.
Police said they later found the patient who had brought a gun to the doctor's office. He had a valid license and wasn't aware he had caused any alarm.


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Sviluška (Tetranychus) je rod roztočů, kterým je obecně věnována velká pozornost pro jejich schopnost vážně poškozovat rostliny. Rod sviluška patří do čeledě sviluškovití (Tetranychidae), řádu sametkovci (Prostigmata).
Velmi rychle se množí, při přemnožení způsobují značné škody a úhyn rostlin. Rod zahrnuje více než 140 druhů, nejznámější je sviluška chmelová (Tetranychus urticae), sviluška ovocná (Panonychus ulmi). Někdy je za svilušku nesprávně považována nápadně červená sametka podzimní (Trombicula autumnalis).

EPPO kód
1TETRG

Zeměpisné rozšíření
Celosvětové.

Popis
Svilušky jsou 0,5–0,7 mm velcí roztoči, většinou bělavě bezbarví nebo červenooranžoví.

Hostitel
Polyfágní rod, některé druhy jsou častější na některých rodech rostlin.

Příznaky
Drobné skvrny způsobené sáním tkání hostitele, obvykle nejdříve na listech. Zavadání, stříbřitý nádech listů (vzduchové bublinky v tkáních) při větším rozvoji populace jemné nebo později husté pavučinky kolem listů nebo jehlic s drobnými, pohybujícími se barevnými tečkami, usychání listů a rostliny. Pavučinky nebo vlákna bývají často v místě, kde stopka listu přiléhá k větvičce nebo stonku. Sviluška ovocná však například pavučinky nevytváří.

Příznaky při případě invazivním průběhu mohou připomínat náhlé vadnutí a bezdůvodné usychání rostlin. Dřeviny mohou zůstat téměř bezlisté nebo s visícími suchými listy. Roztoči sají na spodní straně listu, kde je lze obvykle vidět pomocí lupy.

List
Výrazně světlé, nebo stříbřité zbarvení, žlutavé tečky na listech v místech sání (obvykle hustě), chloróza, spojující se suché nekrotizující plochy, list se svinuje nebo zvedá okraje. Listy obvykle zasychají od špičky nebo okrajů. U travin prosychají, hnědnou a žloutnou tkáně nejdříve mezi žilkami. Rzivé skvrnky na palmových listech. Hostitel se snaží vytvářet nové listy, které jsou okamžitě napadány.

Květy
Hnědnoucí květní oplátky, deformované květy, barevné změny květu, poškozená, zasychající nebo se neotevírající poupata, usychající květy, tečky po sání na plátcích.

Letorosty
Mladé letorosty mohou být poškozeny, zasychají, bývají zřejmé stopy sání.

Plody
Posáté plody se deformují.

Možnost záměny
Saví škůdci.

Význam
V některých letech se svilušky přemnožují. Oslabují rostliny. Dřevo špatně vyzrává. V příštím roce je slabá násada květů.
Může dojít k úhynu rostliny(např. hrnkové rostliny), poškození u pěstovaných rostlin bývá závažnou vadou vzhledu nebo má za následek snížení velikosti a jakosti sklizně.

Biologie
Přezimují samice nebo vajíčka, patogen má mnoho generací během roku a rychle se množí.

Ekologie
Běžný ve všech oblastech. Nejlépe mu vyhovují suché teplé lokality, panelové byty se suchým vzduchem, nejlépe během topné sezóny. Pro vývoj kalamity je ideální vlhké teplé jaro a suché léto téměř bez srážek. Častý patogen skleníkových monokultur.

Ochrana rostlin
Při napadení lze použít přirozené nepřátele (TYPHLODROMUS PYRI, BIOLAAGENS - PP), ale běžně jsou populace svilušek omezovány svými přirozenými nepřáteli ve svém prostředí a kromě přemnožení není zásah nutný.

Prevence
Používat zásadně selektivní insekticidy. Nepřehnojovat dusíkem. Nepěstovat citlivé rostliny v bytech se suchým vzduchem, zimní postřiky proti přezimujícím stádiím.

Chemická ochrana
Insekticidy nebo akaricidy.
 FLORAMITE 240 SC
 Nissorun 10 WP
 PRAKTIK SVILUŠKA STOP (hexytthiazox)
 CAREO Koncentrát proti škůdcům (neselektivní insekticid)
 KARATE se ZEON technologií 5 CS (neselektivní insekticid)
 Omite 570 EW
 Talstar (neselektivní insekticid)
 Magus 200 SC
 Sanmite 20 WP
 Vertimec 1,8 EC

Odkazy

Literatura

Reference

Externí odkazy

 popis, ochrana
 poradna
 sviluška ovocná
 Jak se zbavit svilušek

Choroby a škůdci rostlin
Nespecializovaní patogeni a fyziologické poruchy
Fytofágní hmyz
Sviluškovití

redpajama_set_name: RedPajamaWikipedia


Yes. It can be very hard to live with excessive sweating. You knew that. We knew that. But there's new research documenting the extensive burden hyperhidrosis puts on its sufferers.
The results of a recent study show where important education and advocacy work still needs to be done but that there's hope, too, because people living with hyperhidrosis are not alone in their difficult experiences. The impact of hyperhidrosis on patients' daily life and quality of life: a qualitative investigation was published in the peer-reviewed journal Health and Quality of Life Impacts. To conduct the study, scientists interviewed and surveyed 71 people (mostly in the United Kingdom) who self-identify as having primary hyperhidrosis.
Interestingly, the researchers found that the burden of hyperhidrosis was similar no matter where on the body participants experienced excessive sweating. And, in general, their findings confirm that hyperhidrosis affects many (arguably almost all) aspects of life and can be very challenging to deal with.
69% of study participants said they experience emotional ramifications from hyperhidrosis. Most participants reported being constantly worried about noticeable sweating. Some also said they experience sadness, anger, and hopelessness.
63% of participants said that their sweating interferes with their performance at work or school. The majority regarded this as the most important impact of the condition.
33% reported choosing careers to accommodate their sweating. One participant declined the opportunity to become a policeman "settling for a boring office job" instead.
75% of those in the study said they find it difficult to be in public view. 57% reported difficulties interacting with others. Common situations such as being in a shared office or shared classroom, going to a party, eating at a restaurant, using public transportation, or sitting in a movie theater were reported as challenging. Participants said they often avoid such situations.
Most participants said they are uncomfortable being physically close to others because they are afraid of people's reactions to their sweating. As a result, they avoid touching, holding or shaking hands, sitting next to others, standing in a line, and dancing. Some participants said they are uncomfortable with any physical affection. According to one study member, "I am unable to touch my husband, daughters and grandchildren without first thinking about how to do it without them actually having contact with my skin." Study participants also reported avoiding going out and being in public and, as a result, an inability to nurture important relationships.
40% of study participants said hyperhidrosis is associated with some level of physical discomfort. Individuals said they experience discomfort in relation to "being in wet clothes day in, day out," "having wet feet," and "sweat dripping into the eyes." 17% of patients reported other skin problems that they attribute to constant dampness due to hyperhidrosis. The most common were sore and cracked skin.
61% of patients said that sweating influences their choice of clothing, particularly material, color, and design. Respondents also reported that they cannot enjoy certain recreational activities and are unable to travel to warm-weather destinations.
41% of patients said hobbies are affected by hyperhidrosis including physical as well as non-physical activities such as cycling, exercising in the gym, playing musical instruments, doing yoga, reading books or newspapers, and crocheting/knitting. One patient said, "I don't like exercising on the street or anything like that… people tend to look at me if am really sweaty and that makes me really nervous".
The majority of respondents said hyperhidrosis interferes with general tasks like holding objects, turning door handles, opening jars, working with tools, driving, shopping, and manual work. 33% said they have problems with household chores such as cleaning, cooking, ironing, and caring for young children.
20% of the respondents reported problems using touch technologies including computer keyboards, computer mice, mobile phones, and touch screens.
17% percent of the individuals mentioned doing extra chores in order to stay "clean," such as taking a shower several times a day, changing clothes or shoes often, and using strong antiperspirants.
Most participants said they are not satisfied with the way their condition is being managed in a healthcare setting. In particular, they said they are concerned about poor relationships with physicians, difficulty of obtaining an accurate diagnosis, and lack of (or limited access to) effective treatments as well as negative side effects of treatments. The experience of getting diagnosed was also described as "humiliating" and "belittling." Participants reported that their sweating problems are not taken seriously by clinicians and said they are frustrated by limited coverage for treatments like Botox and iontophoresis and lack of other effective therapies.
Nearly a third of the study participants indicated that they find currently available information on hyperhidrosis inadequate. In particular, participants would like to know what causes hyperhidrosis and what new treatments are in development. Patients also expressed worries about the level of knowledge among healthcare practitioners about the condition. Others said they are concerned about lack of public awareness and said they feel this is why there's not much sympathy for hyperhidrosis. Most of those in the study said they are unaware of the risks of compensatory sweating associated with ETS surgery.
The above results show that the impacts of hyperhidrosis on individuals' lives are far-reaching -- affecting everything from daily household chores and parenting to self-esteem and personal relationships.
From the research results we've discussed here, it's clear that more outreach is needed -- but we can't do it without you!
Spread the word about hyperhidrosis and share SweatHelp.org and this blog widely to help us build greater awareness and concern for the needs of those living with excessive sweating and its myriad detrimental effects. Please also consider making a tax-deductible donation to help us continue our advocacy work.
Remember, the International Hypehidrosis Society speaks up for people with hyperhidrosis around the world and we provide comprehensive information about current hyperhidrosis treatments, new research results, and clinical trials.
We also provide up-to-date training for healthcare providers as well as advocacy and educational opportunities for patients, clinicians, researchers, and the general public.
Watch this blog for important information about our patient-focused hyperhidrosis treatment development meeting this fall in Washington, DC!
You can attend online and be heard.


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Lenovo IdeaCentre K330: Lots of Speed, Little Expandability
By David Murphy
Lenovo IdeaCentre K330
We wish we could throw a few of our favorite $1000-or-less Performance Desktop PCs into a pot and create a stew that combines the best features of each--now that would be a desktop system! Lenovo's IdeaCentre K330 brings some of the bestspeeds we've seen for a system priced at around its level ($999 as of October 11, 2011), but it's not quite as competent in other areas that might have helped this system shine brighter in a home office or gaming den.
Longtime readers may recall the Lenovo IdeaCentre K220--a budget desktop PC from about two years ago. The K330 is so much faster that it doesn't belong in the same category with the K220. An Intel Core i5-2500 processor, clocked at a brisk 3.3GHz, enabled the K330 to scream through our WorldBench 6 test suite. The system's score of 164 doesn't lead the category, but it reflects an excellent price-to-performance ratio for this machine. We also appreciate that the K330 throws 8GB of DDR3 memory into the mix, but we're a little surprised that Lenovo opted for RAM rated at a speed of 667MHz instead of the faster (and more common) DDR3-1333.
The K330 is definitely better suited for general-purpose use than for gaming. Its single Nvidia GeForce GT 440 graphics card delivered lackluster frame rates on our Unreal Tournament 3 benchmark: 33.2 frames per second at 2560 by 2100 resolution and a high quality setting. On the plus side, you don't have to dial the system's resolution too far down to achieve stronger results. We obtained 59 fps on runs conducted at a 1920 by 1080 resolution and high quality--and that's only a hair away from the refresh rate of a typical LCD monitor.
Unique to the K330 is a switch on the system's front that allows the user to alter the system's speeds dynamically by flipping from one to another of three settings--Turbo, Auto, and Cool--which turns part of the system's front panel red, blue, or green, respectively. Don't assume that this feature is some kind of automatic overclocking mechanism that will kick the K330 into high gear. It merely changes some settings in Windows' Power Options menu, most notably the minimum and maximum processor states. In effect, it lets you set the K330's CPU to run at full blast 100 percent of the time, modulate the speed continuously to meet system demands, or run at a consistent reduced speed to conserve power.
Lenovo's inclusion of a Blu-ray combo drive on the system's front is the most exciting thing about that part of the PC. Two USB ports and a multiformat card reader don't deliver much connectivity or diversity on the front panel, but the K330's back panel compensates with six USB ports--though no USB 3.0, regrettably--plus a single eSATA port and a gigabit ethernet port on the motherboard itself, and DVI, VGA, and HDMI ports on the graphics card. The system's integration of 7.1 surround sound is a treat, but we wish Lenovo had included FireWire, an extra eSATA port, some USB 3.0 ports, or DisplayPort.
The wiring inside the system is a smidge messy, but it won't prevent you from installing a new device in the single free 5.25-inch bay or the single free 3.5-inch hard drive bay (a 1TB hard drive occupies the second bay). That's not a lot of free space to work with, even for a midsize tower desktop, but we commend Lenovo for making its upgrading options completely screwless. One free PCI Express x16 port and two free PCI Express x1 ports set aside room for a few add-on cards; they, too, are screwless upgrades.
A generic wired mouse and generic wired keyboard accompany the K330. The rest of the bundle consists of the system's Windows 7 driver CD, hardware replacement guide, and user guide. We had expected a slightly fancier mouse or keyboard with a system that puts processor management front and center on the case.
In general, Lenovo's IdeaCentre K330 feels a bit like a compact PC in a midsize tower case. We love its speeds and its simple add-ons, but we're disappointed that we can't do much internal upgrading (or external device connecting) before running out of room (or ports). The K330 isn't a bad computer by any means; it's just not as well-rounded in its features as a killer $1000 system could be.
You can do a lot with the super-fast speeds on Lenovo's inexpensive PC: You just can't put that much more into this system.
Push-button CPU speed adjustments
Blu-ray support
Great price to performance ratio
Lacks much internal room for upgrades


Many Rosalie residents call Salt their regular spot, whether it be a daily caffeine intake, fast and tasty breakfast, relaxed and enticing lunch, or a delectable dinner.
The menu has been created to reflect what Salt does best, simple yet scrumptious food. No matter what day of the week you dine we aim to uphold consistency.
This is the key to Salt's success … simple consistent food made to please the palate with a homely yet personable service.
We also excel at catering for functions, with a full function package, or custom packages to suit.
All our meals are prepared with the freshest and best quality ingredients.
Falafel |Corn cheese fritters |roast vegetables | mixed bread | aioli | olive oil and balsamic .


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Chapter 20. Drugs Used in Asthma & Chronic Obstructive Pulmonary Disease
Chapter 20. Drugs Used in Asthma & Chronic Obstructive Pulmonary Disease. In: Trevor AJ, Katzung BG, Kruidering-Hall MM, Masters SB. Trevor A.J., & Katzung B.G., & Kruidering-Hall M.M., & Masters S.B.(Eds.),Eds. Anthony J. Trevor, et al.eds. Katzung & Trevor's Pharmacology: Examination & Board Review, 10e. McGraw-Hill; Accessed January 15, 2021. https://accesspharmacy.mhmedical.com/content.aspx?bookid=514&sectionid=41817534
Chapter 20. drugs used in asthma & chronic obstructive pulmonary disease. Trevor AJ, Katzung BG, Kruidering-Hall MM, Masters SB. Trevor A.J., & Katzung B.G., & Kruidering-Hall M.M., & Masters S.B.(Eds.),Eds. Anthony J. Trevor, et al. (2013). Katzung & Trevor's Pharmacology: Examination & Board Review, 10e. McGraw-Hill. https://accesspharmacy.mhmedical.com/content.aspx?bookid=514&sectionid=41817534
"Chapter 20. Drugs Used in Asthma & Chronic Obstructive Pulmonary Disease." Katzung & Trevor's Pharmacology: Examination & Board Review, 10e Trevor AJ, Katzung BG, Kruidering-Hall MM, Masters SB. Trevor A.J., & Katzung B.G., & Kruidering-Hall M.M., & Masters S.B.(Eds.),Eds. Anthony J. Trevor, et al. McGraw-Hill, 2013, https://accesspharmacy.mhmedical.com/content.aspx?bookid=514&sectionid=41817534.
Drugs Used in Asthma & Chronic Obstructive Pulmonary Disease: Introduction
Strategies of Asthma Therapy
Beta-Adrenoceptor Agonists
Skill Keeper: Sympathomimetics in Asthma
Methylxanthines
Muscarinic Antagonists
Cromolyn & Nedocromil
Leukotriene Antagonists
Anti-IgE Antibody
Skill Keeper Answer: Sympathomimetics in Asthma
Drug Summary Table: Bronchodilators & Other Drugs Used in Asthma & COPD
Asthma is a disease characterized by airway inflammation and episodic, reversible bronchospasm. Drugs useful in asthma include bronchodilators (smooth muscle relaxants) and anti-inflammatory drugs. Bronchodilators include sympathomimetics, especially β2-selective agonists, muscarinic antagonists, methylxanthines, and leukotriene receptor blockers. Anti-inflammatory drugs used in asthma include corticosteroids, mast cell stabilizers, and an anti-IgE antibody. Leukotriene antagonists play a dual role. Chronic obstructive pulmonary disease (COPD) is characterized by airflow limitation that is less reversible than in asthma and by a progressive course. However, many of the same drugs are used.
Bronchial hyperreactivity Pathologic increase in the bronchoconstrictor response to antigens and irritants; caused by bronchial inflammation
IgE-mediated disease Disease caused by excessive or misdirected immune response mediated by IgE antibodies. Example: asthma
Mast cell degranulation Exocytosis of granules from mast cells with release of mediators of inflammation and bronchoconstriction
Phosphodiesterase (PDE) Family of enzymes that degrade cyclic nucleotides to nucleotides, for example, cAMP (active) to AMP (inactive); various isoforms, some degrade cGMP to GMP
Tachyphylaxis Rapid loss of responsiveness to a stimulus (eg, a drug)
The immediate cause of asthmatic bronchoconstriction is the release of several mediators from IgE-sensitized mast cells and other cells involved in immunologic responses (Figure 20–1). These mediators include the leukotrienes LTC4 and LTD4. In addition, chemotactic mediators such as LTB4 attract inflammatory cells to the airways. Finally, several cytokines and some enzymes are released, leading to chronic inflammation. Chronic inflammation leads to marked bronchial hyperreactivity to various inhaled substances, including antigens, histamine, muscarinic agonists, and irritants such as sulfur dioxide (SO2) and cold air. This reactivity is partially mediated by vagal reflexes. COPD is often triggered by upper respiratory infection (like asthma) but occurs in older patients (usually long-term smokers) and is poorly reversible with bronchodilators.
Figure 20–1
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Immunologic model for the pathogenesis of asthma. Exposure to antigen causes synthesis of IgE, which binds to and sensitizes mast cells and other inflammatory cells. When such sensitized cells are challenged with antigen, a variety of mediators are released that can account for most of the signs of the early bronchoconstrictor response in asthma. LTC4, D4, leukotrienes C4 and D4; ECF-A, eosinophil chemotactic factor-A; PGD2, prostaglandin D2. (Modified and reproduced, with permission, from Gold WW: Cholinergic pharmacology in asthma. In: Asthma Physiology, Immunopharmacology, and Treatment. Austen KF, Lichtenstein LM, editors. Academic Press, 1974.)
Acute bronchospasm must be treated promptly and effectively with bronchodilators ("reliever" drugs). Beta2 agonists, muscarinic antagonists, and theophylline and its derivatives are available for this indication. Long-term preventive treatment requires control of the inflammatory process in the airways ("controller" drugs). The most important anti-inflammatory drugs in the treatment of chronic asthma are the ...


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It allows you to choose PDF page range or some page to be converted to epub.
It also can convert word document to epub without Office word application installed.
Standalone software, it can do the conversion without Adobe software installed.
Convert multipage tiff file to epub quickly.
Convert scan PDF file to epub correctly.
Difference between a PDF and an EPUB?


Growing up in Southern California, Rachel was raised with a love of Jewish experiential learning and sunshine. She is a proud product of NFTY SOCAL and still consults and staffs for them today. She is a firm believer in the power of summer camp and credits a huge part of her Jewish identity to URJ Kutz Camp and URJ Camp Newman where she spent significant time as a participant and senior staff member. Rachel graduated from UC Davis with a B.S in Human Development and was very active in her campus Hillel. After participating on a MASA program in Israel and working in a variety of Jewish educational environments in the greater LA area, Rachel went on to study at the Rhea Hirsch School of Education at Hebrew Union College. She graduated from HUC with a Masters in Jewish Education.
Rachel is devoted to creating and participating in inclusive Jewish communities that are dedicated to building a more resilient and accessible Jewish future. She is so excited that her love of Jewish camping, fostering Jewish identities and Jewish teachable moments have brought her to the BJE.


The Standby Amplifiers can be interfaced as a slave unit in the Standby CAN-Bus control system or used separately as a standalone amplifier.
Small programmable amplifier built with the latest technology.
All-in-one siren with loudspeaker and amplifier.
Programmable amplifier with integrated control system.
Extra long spiral cable, Police standards. Don´t forget the extension/connection cable between the amplifier and microphone.


Unique, stunning and 100% hand crafted. Available in Crystal & Ice Blue. These beautiful Fish are a great center piece to any table.
The fish is fantastic in quality and I love the crackle effect. Looks so much better in person and am so glad I chose the blue. Again it's just a fantastic item in look and quality.


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redpajama_set_name: RedPajamaGithub


text:
Hispanomeryx is an extinct genus of artiodactyl from the middle to late Miocene epoch, living from 13 to 8 million years ago. Over the years, they have been variously classified as being related to bovids or giraffes, or even belonging to their own unique family, but they are now widely regarded as moschids, relatives of the living musk deer.

Hispanomeryx would have resembled modern musk deer, but was smaller, and some of the teeth in the lower jaw resembled those of bovids, possibly as an adaptation to its diet. Most fossils are known from Spain, but others are known from Turkey to China, most of which are too fragmentary to be assigned to a particular species. Hispanomeryx seems to have been an adaptable species, and to have lived in both subtropical forests and open, relatively arid, savanna.

The following species are known:
 H. duriensis (type) Morales, Moyà-Solà, and Soria, 1981 - Spain
 H. andrewsi Sánchez et al., 2011 - China
 H. aragonensis Azanza, 1986 - Spain
 H. daamsi Sánchez, Domingo, and Morales, 2010 - Spain
 H. lacetanus Sánchez et al., 2019 - Spain

References

Prehistoric musk deer
Miocene even-toed ungulates
Miocene mammals of Europe
Prehistoric even-toed ungulate genera


text:
Argentina's coast guard sinks Chinese trawler
Coast guard of Argentina sunk a Chinese trawler on 15 March after a chase, as it had been fishing illegally in the territorial waters of the country.
Source: Pravda.Ru photo archive
The coast guard had first warned the Chinese ship crew by radio, then made some warning shots. After that there was taken decision to sink the trawler.
"On several occasions, the offending ship performed manoeuvres designed to force a collision with the coast guard, putting at risk not only its own crew but coast guard personnel, who were then ordered to shoot parts of the vessel," the coast guard statement said.
All the sailors, that were on board, have been rescued.
Illegal fishing still remains to be a serious problem in the region. The clash took place despite Argentina's and China's rapprochement during the latest years.
Read article on the Russian version of Pravda.Ru