text:
OtherShort Communication
EVALUATION OF INHIBITORY POTENCIES FOR COMPOUNDS INHIBITING P-GLYCOPROTEIN BUT WITHOUT MAXIMUM EFFECTS: F2 VALUES
Johanna Weiss and Walter Emil Haefeli
Drug Metabolism and Disposition February 2006, 34 (2) 203-207; DOI: https://doi.org/10.1124/dmd.105.007377
Johanna Weiss
Walter Emil Haefeli
In cell culture systems with aqueous buffers, concentration-response curves to lipophilic inhibitors are difficult to establish because plateau effects (Imax) are often not reached because of limited drug solubility. Consequently, the inhibitory potency of a compound will not be definable using IC50 values (concentration exerting 50% of Imax). Since alternative potency measures f2 values, the concentrations required to double baseline signals have been proposed. Using both methods, we reevaluated the concentration-response curves of calcein assays with 78 compounds in three different cell culture systems and found a close correlation between both methods (rs = 0.93–0.99, p ≤ 0.0028). These findings suggest that f2 values are a valuable alternative to define rank orders of highly lipophilic inhibitors as a basis for the prediction of pharmacological interaction properties in clinical settings. Although it was only tested for inhibition of P-glycoprotein, it seems likely that this method may be transferred to other assays with other proteins.
Article, publication date, and citation information can be found at http://dmd.aspetjournals.org.
doi:10.1124/dmd.105.007377.
ABBREVIATIONS: ABC, ATP-binding cassette; f1.5, f2, f3, and f4, concentration needed to increase baseline fluorescence by a factor of 1.5, 2, 3, and 4, respectively; rS, Spearman rank correlation coefficient; DMSO, dimethyl sulfoxide; LY335979, zosuquidar; GG918, elacridar; IC50, concentration leading to 50% of Imax; Imax, maximum effect; Imin, minimum effect; pBCEC, porcine brain capillary endothelial cell; P-gp, P-glycoprotein; SDZ-PSC833, valspodar.
Accepted November 2, 2005.
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Drug Metabolism and Disposition February 1, 2006, 34 (2) 203-207; DOI: https://doi.org/10.1124/dmd.105.007377
Preincubation Effects on Inhibition of OCT1 by CsA
Carbamazepine Metabolite and Hypersensitivity Reactions
SULT4A1 Preserves Mitochondrial Function
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The central question in this empirical study is the impact of women's land ownership on existing power relations in the household, the family and society. What factors facilitate or constrain women's ownership of land? Do women who own land have more power, especially to challenge and change unequal gender and class relations? These questions, inspired by Bina Agarwal's A Field of One's Own (1994), have been examined in the specific context of unequal gender and class relations and processes of economic and social transformation in rural Bangladesh through an extensive (re)study of the village "Jhagrapur" (see: Jenneke Arens & Jos van Beurden, 1977, Jhagrapur: Poor Peasant and Women in a Village in Bangladesh). The concepts of agency and empowerment have been extensively discussed. The study provides a deeper insight into various issues that play a role (such as Islam, moral norms and values, dowry, education, women's reproductive rights, microfinance) and makes an argument for the importance of women's control over their land for social transformation of gender and class relations. The study indicates that control over land is an essential prerequisite for women's empowerment. The specific gender division of labour, the lack of recognition of women's productive role, and patriarchal gender norms are identified as the main obstacles for women's control over land. These insights are valuable for anyone committed to a more just and equitable society in which people, in particular women, have control over their own lives and communities.


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Make sure that you will follow through a guide when hiring an MA plumber. It is a must that you will carefully lay out a guide that will set everything out, so that you will get the best outcome of the works that you can expect from the plumber. You can trust that the word of mouth is something that you can fully trust so that you will be lead to the best plumber that you can find around, and that it is an important consideration to see to it that you are having your friends recommend someone that you can fully work out well. It is also an important thing that you will look at the local business listings that are necessary for you to have a good check so that you will really be able to ensure that you are getting the best people to work for you.
Another thing that you can look out to is that of trade associations as well as unions, and that it would be important that you are going to be looking at such so that you will see who are the best people in the profession. It would also be an imperative thing that you will check on the online reviews as to the best MA plumber that are found on the net, so that you can fully gauge what will be the kind of work that they are going to give to you. On the other hand, you can actually check out on the estate agents so that you will really be able to see to it that you are provided with a good list of plumbers that are really up for any challenges of the job.
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Marek Antosiewicz graduated in Mathematics from the University of Warsaw and in Economics from the Warsaw School of Economics. Since 2012, he has been a PhD student at the WSE Collegium of Economic Analysis. In his PhD thesis, he develops methods of solving heterogeneous-agent macroeconomic models and applies them in labour market analysis.
At the Institute for Structural Research, he is responsible for the construction of macroeconomic models used to analyse climate change mitigation and energy policies. Participated in both national and international research projects such as National Science Centre grants, consultancy for Polish Ministries, MAPS Chile, DYNAMIX or TRANSrisk.
At the TRANSrisk workshop in Santiago (Chile) Marek Antosiewicz gave a presentation about simulating the macroeconomic effects of climate change mitigation policies (24.08.).
What is the short and long run response of energy demand to price changes? Presentations of Jan Witajewski-Baltvilks and Marek Antosiewicz at IEW 2018 & CEF 2018 (19-21.06.).
Green innovation, economic growth and renewable energy sources were the topics of Jan Witajewski-Baltvilks and Marek Antosiewicz presentations at WCERE conference and EMEE workshop.
The main objective of this research project is to better understand the impact of climate policies, in particular environmental taxes, on unemployment and wages.


text:
Is This The Root Cause Of Welcome To Plathville's Olivia And Ethan's Marriage Troubles?
NEWS EXCLUSIVES ENTERTAINMENT BEAUTY HEALTH ROYALS LOVE FOOD STYLE LIVING POLITICS FEATURES
By Haley Van Horn/Sept. 16, 2021 2:17 pm EST
One of TLC's most popular reality shows centered around a family unit, "Welcome to Plathville," gives viewers an inside look at what growing up in an incredibly religious lifestyle looks like. The Plath family consists of nine children, but only eight are a part of the filming process (via Distractify).
According to Screen Rant, the family consists of children who follow the strict lifestyle their parents have forced upon them, and a few who have rebelled to form their own opinions and lifestyles. One of the daughters got a tattoo and started dating, which is a big deal for this family.
Of all the children, Ethan Plath and his wife Olivia are the villains in the eyes of the family. The Plath parents have attempted to bar their other children from hanging out with Ethan and Olivia. Of course, the ongoing family tension has put a strain on the couple's marriage.
If you're keeping up with the show, you've seen Ethan and Olivia struggle through marital problems. While the drama has unfolded publicly, what exactly is the root of their strained marriage?
The couple are seeking therapy to solve their marriage problems
While Ethan and Olivia are seen as the most rebellious of the two, one way they are breaking the norms of their religion is by seeking therapy for their marital problems (via Us Weekly). Olivia shared, "Growing up in a very religious world, there's so much stigma surrounding therapy," Plath says, "You know, 'You should just pray more or read your bible more' or 'It's not a real thing.' But there comes a time in your life when you're an adult and you come to say, 'I choose to recognize that I need help and it doesn't make me weaker for it.'"
That seems like a rather mature decision to make, right? They've come a long way since Olivia attempted to dismiss rumors of their struggling marriage (per Screen Rant). During these therapy sessions, it seems they are digging in deep and finding the root of their marital woes.
It turns out the issues between the Plath's might be centered around Olivia's change and Ethan"s wish for things to stay the same. Plath told Us Weekly, "He has a really hard time with me changing. The one underlying thing he says is I'm not the person he married and if he had known I was going to be like this, he wouldn't have married me." She believes change is at the root of their issues, but so is dealing with childhood trauma, something that is incredibly difficult to overcome even as an adult.

redpajama_set_name: RedPajamaCommonCrawl


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Todays Though > News > Ravens sign veteran linebacker, former Gilman standout Brandon Copeland to practice squad – Boston Herald
Ravens sign veteran linebacker, former Gilman standout Brandon Copeland to practice squad – Boston Herald
Margaret Rood
posted on Sep. 21, 2022 at 7:54 pm
The Ravens announced Wednesday that they've signed veteran linebacker and former Gilman standout Brandon Copeland to the practice squad.
Copeland has spent time with six teams in his NFL career, totaling 158 tackles, seven sacks and 21 quarterback hits in 82 games. He was a member of the Atlanta Falcons in 2021, playing in 16 games (three starts) while recording 39 tackles and two quarterback hits.
The 31-year-old is a familiar face for the Ravens, as the Sykesville native signed with Baltimore as an undrafted free agent out of the University of Pennsylvania in 2013 before being released during final roster cuts. He didn't play his first NFL game until 2015 as a member of the Detroit Lions.
Copeland, the grandson of former Baltimore Colts defensive end Roy Hilton, has also been recognized for his community work. He was named the 2020 Alan Page Community Award winner, the NFL Players Association's highest honor, for his annual "December to Remember" event, which hosted shopping sprees in seven cities, including Baltimore.
Copeland has a chance to get immediate playing time as the Ravens are thin at outside linebacker. Veteran Steven Means is out for the season after suffering a torn Achilles tendon in Sunday's loss to the Miami Dolphins, while Tyus Bowser and rookie David Ojabo are recovering from the same injury.
Margaret Rood September 21, 2022
Ravens QB Lamar Jackson wearing sleeve on throwing arm at practice; CB Marlon Humphrey among 5 missing – Boston Herald
PnB Rock UPDATE: LAPD Sources Say Fatal Shooting Might Have Been A Planned Hit & Not Random Robbery
LeBron James reaches 4th all-time in assists, inches closer to points record in 129-123 win over Knicks – Boston Herald
Eastern Massachusetts high school roundup, scoreboard – Boston Herald
Clemson was ranked No. 20.
Heat score statement road victory in pushing past Cavaliers 100-97 – Boston Herald
North Quincy beats Scituate 53-39 – Boston Herald
Two years after ending the rebuild with the trade for Nikola Vučević, are the Chicago Bulls running in place? – Boston Herald
Do You Know What the Best Way of Shipping A Car is?


text:
Sport and Outdoor
Bredon School
Bredon appears as top-ranking specialist dyslexia school in A Level league table
Bredon School appears as the highest-ranking specialist dyslexia school for A Level results in a league table published by The Times newspaper (27 August 2018). Over one third (36.4%) of Bredon's A Level results were either an A* or A grade, which means Bredon School has a higher ranking than any other specialist dyslexia school in the UK.
The Times compiled its table based on A Level, IB and Pre-U results supplied by the Independent Schools Council. Bredon School is ranked 126th out of all independent co-educational schools across the UK, appearing as the top-ranking specialist dyslexia school for A Level attainment.
Bredon School's Headteacher Koen Claeys comments: "As a specialist school for dyslexic pupils and other additional learning needs, these academic results provide a great endorsement for our distinct and tailored approach to teaching and learning. It is wonderful to see our pupils achieving such impressive results."
100% of pupils taking A Levels at Bredon School achieved grade A* to C, with 63% of students gaining an A* to B grade, which is an increase of nearly 20% compared to last year.
Mr Claeys added: "We believe our small classes, specialist teaching and very broad curriculum combining traditional academic and vocational study options set us apart. We provide every pupil with their own Google Chromebook to use in class and we harness assistive technologies and voice recognition software to make curriculums accessible to everyone. All subjects are taught with dyslexic-friendly practices in mind."
Furthermore, according to this year's The Daily Telegraph's league table of independent schools with small sixth forms (under 25 students) for 2018 A Level results, Bredon ranks 19th in the UK compared to other schools with similarly sized sixth forms.
Mr Claeys concludes: "As a small, specialist school we can get to know our students on an individual basis. Our tailored approach enables all our students to make progress in a way best suited to their individual learning style, whether that's traditional A Levels or BTECs and vocational CACHE qualifications."
"We also offer an on-site CISCO Academy IT programme leading the way to apprenticeship employment. Our range of courses mean that the widest career options are available to our students when they leave us for employment or further education."
GCSE Results: Bredon School Pupils Achieve Full Potential
Bredon School adopts BSA COVID-Safe Charter
A Level and BTEC Results: Bredon School Students Celebrate Outstanding Achievements
Bredon School is a part of the Cavendish Education Group.
Bredon School Ltd is registered in England and Wales. No 04399845
Registered office: 14 Waterloo Place, London SW1Y 4AR
www.cavendisheducation.com
Copyright ©2020 Cavendish Education Ltd
By EPG Design


text:
\section{Introduction}

\hii\ regions have long served as a primary indicator of
high-mass star formation, both in the Milky Way and in external
galaxies.  The luminosity function of \hii\ regions (\hlf)
is therefore a vital probe of the present global star
formation properties in individual galaxies.
In recent years, the number and accuracy of compiled
\hlf s for nearby galaxies has increased substantially, extending
the use of this tool to greater distances.

The differential \hlf\ is usually parameterized as a power law:
\begin{equation}
N(L)\ dL = A\ L^{-a}\ dL \quad ,
\end{equation}
where $N(L)\ dL$ is the number of nebulae with luminosities in the range
$L$ to $L + dL$.  Some interesting patterns have emerged regarding the
form of the \hlf:
\begin{enumerate}
\item[1.]
A large number of galaxies show a break in slope of the \hlf\,
with the fainter \hii\ regions showing a shallower slope compared to
the high-luminosity objects (\eg Kennicutt, Edgar, \& Hodge 1989,
hereafter KEH; Rand 1992; Walterbos \& Braun 1992; Rozas, Beckman, \&
Knapen 1996a;)

\item[2.]
The \hlf\ for arm and interarm regions of spiral galaxies
sometimes show steeper slopes in the interarm regions (e.g., KEH;
Banfi {\etal}1993; Rand 1992).  However, there are also many
instances where no difference is found (e.g., Rozas
{\etal}1996a; Knapen {\etal}1993; Knapen 1997)

\item[3.]
The slope of the \hlf\ is correlated with galactic Hubble type, such
that early-type galaxies show steeper slopes than late-types.  The
power-law index $a \sim 2.0$ for Sb -- Sc galaxies, compared to $a\sim
1.7$ for Sc -- Im galaxies (KEH; Banfi {\etal}1993).  It is even
steeper in Sa galaxies, with $a\sim 2.6$ (Caldwell {\etal}1991).
\end{enumerate}
These differences in the \hlf\ have usually been interpreted as
resulting from corresponding differences in star formation properties.
For example, the break in slope (Point 1, above) has been suggested to
be caused by a physical transition between normal \hii\ regions and
the class of
supergiant \hii\ regions such as 30 Doradus in the Large Magellanic Cloud
(KEH).  Likewise, the difference in slope for arm vs. interarm
regions, and among various Hubble types (Points 2 and 3), have been
attributed to differences in gasdynamics and molecular cloud mass
spectrum (\eg Thronson, Rubin, and Ksir 1991; Rand 1992; KEH).
However, we feel that it may be premature to draw a direct connection
between the form of the \hlf\ and details of star forming
environment such as these.  There are other effects that can influence
the form of the \hlf, that have not been adequately explored.

One important effect, in particular, is the influence of simple
evolution in the ionizing clusters, and hence, luminosity of the host
\hii\ regions.  There are several empirical factors that suggest that
nebular luminosity evolution is an important effect in the form of the
\hlf.  The steeper slopes seen in interarm regions of spiral galaxies
(Point 2, above) have been identified by von Hippel \& Bothun (1990)
as evidence of an aging effect in those populations.
Assuming star formation takes place primarily in the spiral density waves
delineated by the arm regions, then the interarm regions should
exhibit a typically older population of nebulae in the wake of this
star formation activity.
In addition, von Hippel \& Bothun cite the behavior of \Ha\ equivalent
widths as
further compelling evidence of the importance of luminosity evolution.
As a cluster ages, its associated \Ha\ emission decreases, while
that of the underlying red stellar continuum increases, thereby
reducing the \Ha\ equivalent width as a function of time.  They
demonstrate that for the \hii\ regions in NGC 628, there is indeed a
clear decrease in \Ha\ equivalent width with decreasing \Ha\
luminosity, indicating higher numbers of evolved nebulae among the
fainter populations.  Finally, Knapen {\etal}(1993) and Rozas, Knapen,
\& Beckman (1996b) show that the slope
of the nebular luminosity vs. volume relation is slightly flatter in the
interarm regions of five galaxies as compared to the arm regions.  As
emphasized by the authors, this may be caused by observational
selection effects, but if real, we suggest that it is consistent with a higher
tendency for shell-like geometries in the interarm nebulae, as would
be expected for an older population.

All of these arguments suggest that evolved nebulae will be an
important population in the \hlf.  Von Hippel \& Bothun (1990) carried
out the first detailed investigation of the evolutionary effect on the
\hlf.  They constructed two models to reproduce the observed slope for
NGC 628:  one with zero evolution, in which the power-law slope of the
luminosity function is due entirely to the cluster mass spectrum; and one
in which the distribution in nebular luminosity is due entirely to a
different age and number distribution of objects with the same
initial cluster mass.  The \hlf\ resulting from the evolutionary model
is sensitive to the stellar initial mass function (IMF), since the relative
numbers of stars at a given ionizing luminosity become important when
these stars become the dominant contributor to the nebular luminosity.
Recognizing this, von Hippel \& Bothun oriented their study toward exploring the use of
the \hlf\ to place constraints on the IMF.  As a result, they did not
explicitly examine the consequences of aging on the form of the \hlf\
itself.  In addition, their assumption of uniform initial cluster
masses in the evolutionary model is of only limited use, since actual
initial cluster masses apparently have a power-law distribution (e.g., Oey
\& Clarke 1997; see below).  Therefore, we will here investigate
the effect of cluster aging on the form of the \hlf\ itself.

\section{Saturated Population}

We have carried out a preliminary investigation of this problem as
part of a different study (Oey \& Clarke 1997), and
review the important relevant issues here.  A first critical
point is the fact that not all clusters have the
same relative contribution to ionizing luminosity from the various
stellar masses.  Such a situation is true for rich clusters that sample
the IMF well, but breaks down for sparse
clusters in which small-number statistics determine the relative
ionizing contribution of different stellar masses.  We shall refer to
the rich clusters with good stellar statistics as ``saturated'' with
respect to the IMF, and those with poor statistics as ``unsaturated.''
The importance of this fundamental difference in the dominant ionizing
contributors between the saturated and unsaturated clusters is
demonstrated by a break in the predicted slope of the unevolved \hlf.
This change in slope was clearly demonstrated by McKee \& Williams
(1997; hereafter MW97), who performed Monte Carlo simulations of
clusters drawn from a truncated power-law
distribution in the numbers of member stars $N_*$, and a
Scalo (1986) IMF.  Since $L\propto N_*$ for the saturated objects,
the \hlf\ slope is the same as the parent slope in
$N_*$; but for unsaturated populations, the \hlf\ slope is
distinctly flatter.  This flattening is caused by the increased
scatter in the $L$'s contributed by a bin of
given $N_*$.  The unsaturated condition occurs when this scatter is
large compared to the mean $L$ at the given $N_*$, hence the slope of
the \hlf\ flattens.  MW97 observed that in their
simulations, this change in slope occurs at $\lsat=\lup$, the luminosity
contributed by a single star at the upper-mass limit $m_{\rm up}$, of
the IMF.  Stellar models currently suggest that
$\lup$ is in the range $38.0 \lesssim\log \lup\lesssim
38.5$ (Schaerer \& de Koter 1997; Vacca, Garmany, \& Shull 1996;
Panagia 1973).  We caution however, that the slope break $\lsat$ in
the \hlf\ does not necessarily occur at $\lup$, as we show in \S 4.3.

Investigation of evolutionary effects on the \hlf\ should therefore
consider the differences in stellar ionizing populations between the
saturated and unsaturated regime.
We examined the behavior of the saturated case analytically in Oey \&
Clarke (1997).  We considered two extremes in the formation of
ionizing clusters:  a single-burst scenario, in which all objects are
created at the same time; and a continuous-creation scenario.
In what follows, we will also assume a constant IMF throughout.

For the case of the single burst, it is apparent that, since
all objects follow the same luminosity evolution, the initial slope of
the \hlf\ is simply preserved.

\begin{figure*}
\vspace*{-1.7 truein}
\hspace*{0.8 truein}
\epsfbox{Oey.fig1.ps}
\vspace*{-10 pt}
\caption{
Evolution of ionizing photon emission rate $q_0$ (sec$^{-1}$) from
Schaerer \& de Koter (1997).  The stellar models are, from bottom, 20,
25, 40, 60, 85, and 120$\msol$.
\label{stellev}}
\end{figure*}

However, in the case of continuous creation, such a conclusion is not
obvious.  We described the luminosity evolution of the
\hii\ regions in terms of a fading function $f(t)$ (Oey \& Clarke 1997):
\begin{equation}
L = L_0\ f(t) \quad ,
\end{equation}
where $L_0$ is the zero-age nebular luminosity.  Stellar population
synthesis work (\eg Leitherer \& Heckman 1995; Beltrametti,
Tenorio-Tagle, \& Yorke 1982) suggests that the tail of the fading
function $f(t)$ is well-described by a power-law in time $t$, so that
\begin{equation}\label{f}
f = \left\{ \begin{array}{ll}
	1 ~~, & \quad t < t_{\rm ms} \\
	& \\
	\Bigl(t/t_{\rm ms}(\mup)\Bigr)^{-\eta} ~~, & \quad t \geq t_{\rm ms}(\mup)
	\end{array} \right.
\end{equation}
For saturated objects, the onset time, $t_{\rm ms}(\mup)$, for the
fading is the same for all objects.  Nebular fading causes initially
bright objects to
contribute to lower-$L$ bins at later ages, thus if the epoch of
fading dominates over the epoch of zero-age luminosity, we would
expect the observed \hlf\ to be steeper than the unevolved one.
We found that for $f(t)$ of the form in equation~\ref{f}, and
reasonable ranges for $m_{\rm up}$, $t_{\rm ms}(\mup)$,
and $\eta$, that essentially no change in \hlf\ slope is expected.
There is an exception for initially shallow slopes of $ <
\eta^{-1}+1$, for which the observed slope indeed steepens to a value
$a = \eta^{-1}+1$.  This critical value of the slope is probably in the range
1.2 -- 1.4, which is lower than most measured \hlf\ slopes, hence it
is likely that this effect is unimportant.
These effects are described in further detail in Oey \& Clarke (1997).
Thus in the saturated regime, no change in \hlf\ slope
is reasonably expected.

\section{Monte Carlo Models}

The statistical uncertainties that dominate the unsaturated clusters
render an analytic investigation of these objects unfeasible.  This is
due primarily to the fact that many different combinations of stellar
masses can contribute to any given luminosity, and there is no
simple way to relate the total nebular luminosity to the stellar
composition, and hence, luminosity evolution.  We have therefore
modeled the \hlf\ with Monte Carlo simulations to investigate its
behavior in the unsaturated regime.

Our model draws the integer number of ionizing stars from a power-law
distribution, so that $N(N_*)\ dN_*$ is the number of clusters with
quantities of stars in the range $N_*$ to $N_* + dN_*$:
\begin{equation}\label{N*}
N(N_*)\ dN_* = N_*^{-\beta}\ dN_* \quad .
\end{equation}
We consider ``clusters'' containing a minimum of one star, with the
probability of larger clusters decreasing with $N_*$ according to the
exponent $\beta$.
Our models use the RAN1 portable random number generator described by
Press {\etal}(1986), to generate the random deviate $x$, having values
between 0 and 1.  The distribution in $N_*$ given by equation~\ref{N*}
is then obtained by
\begin{equation}
N_* = \Bigl[-x \Bigl(1-\beta\Bigr)\Bigr]^{1/(1-\beta)}\quad ,
\end{equation}
where $N_*$ is assigned to the nearest integer.
Since the saturated end of the \hlf\ does not
change slope, as
outlined in the previous section, we adopt $\beta = 2$ as a
typical value found for \hlf s in nearby galaxies (\eg KEH).
Unlike MW97, we do not consider
a distribution that is truncated at an upper limit in $N_*$ for our
default models, although this condition is relaxed in \S~3.3.

For each cluster, we then draw $N_*$ stars from a stellar mass
distribution truncated above a mass limit $\mup$:
\begin{equation}\label{imf}
n(m)\ dm\propto \biggl[\Bigl(\frac{m}{\mup}\Bigr)^{-\gamma} - 1\biggl]
	\ dm \quad ,
\end{equation}
where $n(m)\ dm$ is the number of stars in the range $m$ to $m+dm$.
These are generated with an algorithm analogous to that for $N_*$.
Equation~\ref{imf} describes a power-law for $m\ll\mup$, and is the same
analytic form used by MW97 for their $N_*$
distribution and IMF; we refer to this form as a truncated power-law,
following their nomenclature.  We use a Salpeter (1955) power-law
slope of $\gamma = 2.35$, and adopt an upper-mass limit $m_{\rm
up}=100\msol$.  We include stars down to a lower-mass limit $m_{\rm
lo}=17\msol$ (see below).  The \Ha\ luminosity
$l$ associated with individual stars is dependent on the mass and
main-sequence lifetime $t_{\rm ms}$, for which we also use power law
parameterizations:
\begin{equation}\label{ml}
m\propto l^\delta \quad ,
\end{equation}
normalized so that $l_{\rm up}\equiv l(m_{\rm up}) = 3\times
10^{38}\ergs$; and
\begin{equation}\label{mti}
m\propto t_{\rm ms}^{-d} \quad ,
\end{equation}
normalized so that $t_{\rm ms}(m_{\rm up}) = 2.8$ Myr (Schaerer
{\etal}1993).  For stars in the range $17 < m < 100\msol$,
we find a value of $d=0.7$ from Schaerer {\etal}(1993).
We caution the reader that the power-law representations of
equations~\ref{ml} and \ref{mti} are approximations; the relations
steepen significantly toward lower masses.  As discussed below, larger
values of $\delta$ imply a greater sensitivity of $l$ to $m$, thereby
increasing the range of $L$ in the unsaturated regime, for a given
range of $m$.  We adopt $\delta \sim 1.5$, which yields a reasonable
$\log\ l_{\rm lo} \sim 37.3$ for $m_{\rm lo}=17\msol$.
For illustrative purposes, it is helpful to
show a larger dynamic range of unsaturated objects, though we caution
that in reality the range of these objects is likely to be
somewhat smaller for our mass limits, since the $m - l$ relation
flattens toward higher masses (\eg Leitherer 1990).
We have adopted the value
of $m_{\rm lo}$ to coincide roughly with the value at which the $l-m$
relation turns over more steeply, since stars below $\sim 17\msol$
do not contribute strongly to the ionizing fluxes.  There is also
a relative increase in $t_{\rm ms}(m)$ at lower masses, but not as
significant as the change in $l(m)$.  It is useful to bear in mind
that the representative values of $\delta$ and $d$ will increase
toward lower masses.

We consider two different formulations for the stellar ionizing
rate $q_0$ with time.  The first simply approximates that
$q_0$ remains constant until $t_{\rm ms}$ and is zero thereafter.
The second formulation accounts for evolution of $q_0$ during the
stellar main-sequence phase.  Figure~\ref{stellev}
shows $q_0$ for stars of different initial masses as a
function of time, from the models of Schaerer \& de Koter (1997).
These models suggest that $l$ remains fairly constant until a
time after which it decreases roughly along the relation,
\begin{equation}\label{stelleveq}
l = \lup\ \biggl(\frac{t}{t_{\rm ms}(m_{\rm up})}\biggr)^{-\zeta} \quad ,
\end{equation}
where $\zeta\sim 5$, and $t$ is the age from birth.  Given the
uncertainties in massive star evolution and ionizing fluxes, we adopt
the crude approximation of constant $l$ until the time of intersection
with equation~\ref{stelleveq}, after which we adopt $l$ from that
relation.  One consequence of this formulation is that stars with
initially different luminosities can have the same $l$ during certain of their
fading periods.  Figure~\ref{stellev} suggests that this may not be
far from reality.  We caution that the assumption of coeval star
formation within individual nebulae is likely to be an
oversimplification, and that the stellar age spread is typically
similar to the main-sequence lifetime of the most massive stars (\eg
Massey {\etal}1995).  Therefore, the early nebular luminosity evolution
could potentially increase somewhat before the onset of fading.
Specific modeling of star formation scenarios would be necessary to
investigate this effect.

Our adopted lower-mass cutoff introduces artificial fluctuations
that can be seen in all our models at low $L$.  The quantized nature
of the stellar ionizing sources, combined with the truncation
of stellar masses below $m_{\rm lo}$, causes artificial kinks in the
distribution of nebular luminosities at low $L$.  For example, the
most prominent of these features appears at $\log L = 37.6$ in our
models, or 0.3 dex above the lower-$L$ cutoff of $\log l_{\rm lo} =
37.3$.  This dip results from the fact that all nebulae at $L\lesssim
37.6$ contain single stars, selected according to the IMF, whereas
two-star nebulae begin to contribute above this luminosity.
To more clearly demonstrate the features in the \hlf, we
therefore include $10^4$ clusters in our simulations, although this
number is higher than is seen in most nearby galaxies.  Finally, we
truncate our model \hlf s below the minimum luminosity $l_{\rm lo}$,
which is that due to a single star of mass $m_{\rm lo}$.  Although
objects originating at higher $L$ evolve to luminosities below $l_{\rm
lo}$ for cases incorporating main-sequence evolution, the omission of
objects originating below $l_{\rm lo}$ renders the
model populations incomplete below that value.

\subsection{Single Burst}

Figure~\ref{unsat} shows two models for the evolution of an \hii\
region population created in a single burst, with $\delta = 1.5$,
$d=0.7$, and $17<m<100 \msol$.  The left column of Figure~\ref{unsat}
(panels $a-c$) shows model A1, with constant $l$ during the main-sequence;
while the right column (panels $d-f$) shows model A2, with $l(t)$
as described above, to include main-sequence fading.  The zero-age
\hlf s are given in the top panels, with the middle and bottom panels
showing ages of 4 and 7 Myr, respectively.  Note that the two zero-age
models (top panels) are statistically identical.  To aid comparison of
the models, the dotted line corresponding to $\lsat = 3\times 10^{38}\
\ergs$ is shown for reference.

\begin{figure*}
\vspace*{-0.8 truein}
\hspace*{-0.25 truein}
\epsfbox{Oey.fig2.ps}
\caption{Model \hlf s for a single burst.  Model A1 (panels $a-c$)
considers constant $l$ over main sequence lifetimes; Model A2 (panels
$d-f$) considers main sequence fading of $l$ as described in
\S 3.  The dotted line marks $\lsat=3\times 10^{38}\ \ergs$.  Ages of 0,
4, and 7 Myr are shown from top to bottom, respectively.  The dip
near $\log L \sim 37.6$ is a quantization artifact induced by the
lower-mass cutoff.  [Note that the slope of $\log N(\log L)$
vs. $\log L$ is $1-\beta$.]
\label{unsat}}
\end{figure*}

\begin{figure*}
\vspace*{-0.25 truein}
\hspace*{-0.25 truein}
\epsfbox{Oey.fig3.ps}
\vspace*{-6.25 truein}
\caption{\hlf\ Model B1, for continuous creation, with
constant $l$ over main sequence lifetimes.  Panel $a$ shows
an age of 6 Myr after the onset of continuous creation, before
steady-state is achieved.  Panel $b$ shows the steady-state form.
(The dip near $\log\ L\sim 37.6$ is the same quantization artifact seen
in Figure~\ref{unsat}.)
\label{unsatcc}}
\end{figure*}

As found in the simulations of MW97, the zero-age
models in Figure~\ref{unsat} (top panels) show a flattening of the
\hlf\ slope below a saturation luminosity.  For the adopted stellar
parameters, this transition from saturated to unsaturated populations
occurs at $\log\lsat=\log\lup=38.5$.  Equation~\ref{ml} shows
that the extent of this unsaturated regime is determined
by $\delta$:  a larger $\delta$ implies a greater
sensitivity of $l$ to $m$, thereby increasing the
range in $L$ of this population, for a given
range of $m$.  This effect also causes the slope in the
unsaturated regime ($L < \lsat$) to be dependent on $\delta$ because
the scatter in $L$ contributed by individual stars is larger for large
$\delta$, and this scatter determines the flattening in slope.  Hence,
larger values of $\delta$ will induce a flatter slope.  As mentioned
above, our adopted value of $\delta=1.5$ is an
overestimate for the more massive stars in the IMF, hence the
unsaturated slope should be somewhat steeper near $\lsat$ than
is seen in our models.

\hii\ regions with $L > \lsat$ are not sensitive to the $m - l$
relation since statistical effects are unimportant in this regime.
The slope of the \hlf\ in the saturated regime is $\beta$, the same as
that of the parent distribution in $N_*$ (equation~\ref{N*}), as
described in \S 2.

Figures~\ref{unsat}$b$ and $c$ show Model A1 at ages of 4
and 7 Myr respectively.  These ages should not be regarded too
literally, since the evolutionary state at a given age is dependent on
equation~\ref{mti}, which is an approximate parameterization, as well
as equations~\ref{imf} and \ref{ml}.  For reference, $t_{\rm
ms}(m_{\rm lo})=9.7$ Myr for our adopted $d=0.7$.  It is immediately
apparent that the inflection in slope
moves toward progressively lower luminosities with age.  This is
primarily a reflection of the group evolution of the saturated
population to lower luminosities; the entire distribution at $L>\lsat$ in
Figure~\ref{unsat}$a$ is moving toward lower luminosities in
Figures~\ref{unsat}$b$ and $c$.
For cases such as this, in which the zero-age $\lsat=\lup$, the
slope inflection at later ages now corresponds to $l$ of the most
massive star still present in these objects.  More generally, the rate
at which the saturated objects fade in $L$ has a dependence of
$t^{\delta/d}$, as determined by equations~\ref{ml} and \ref{mti}.

Model A2 includes main-sequence evolution of the ionizing fluxes.  We
caution that the models including the main-sequence evolution should
be interpreted qualitatively, owing to the crude parameterization
of the stellar evolution.  The principal feature is that Model A2
clearly evolves much faster than Model A1.  The other important effect
is that noticeable, sharp structure in the \hlf\ becomes apparent near the
transition from saturated to unsaturated objects, as seen in
Figure~\ref{unsat}$e$ as contrasted to Figure~\ref{unsat}$b$.  This
results from the fact that
clusters dominated by a few, high-mass stars are now capable of evolving
to lower $L$ than clusters dominated by many, unevolved, low-mass stars.
In other words, stellar evolution allows the low-$L$ end of the
saturated population to overtake, toward lower luminosities, the
high-$L$ end of the unsaturated population.  The details of this
structure in the \hlf\ are dependent on the details of the
main-sequence luminosity evolution.

\subsection{Continuous Creation}

Figure~\ref{unsatcc} shows simulations for a population where the
\hii\ regions are being continuously created (Model B1).  This model is the
same as that in the single burst case with no main-sequence
luminosity evolution (Model A1), but now with each new cluster
formed at a uniform incremental time after its predecessor.  The total
distribution of initial luminosities, $\log L_0$, of all the objects,
which represents the parent, unevolved \hlf, is the same as the
zero-age distributions in Models~A1 and A2 (Figures~\ref{unsat}$a$ and
$d$).  Figure~\ref{unsatcc}$a$ shows the
distribution at an age of 6 Myr after the onset of continuous creation, but
before the population has achieved its steady-state form.  The
steady-state \hlf, which occurs at $t > t_{\rm ms}(m_{\rm lo})$, is shown
in the Figure~\ref{unsatcc}$b$.

We may consider the \hlf\ for continous creation to be a sum of
individual bursts with a continuous age distribution.  Since the
single burst \hlf\ evolves predominantly as a progression of the
saturated objects, with slope $\beta$, to the lower luminosities of
the unsaturated regime, we therefore expect that the
slope in the region $L<\lsat$ will be intermediate between
its flatter value in the unevolved case and $\beta$.
Figure~\ref{unsatcc}$b$ shows that this is indeed the case.  We can
also see in Figure~\ref{unsatcc}$a$, that the intermediate
evolutionary stage shows
the region of steepening moving in from higher luminosities,
since the low-luminosity bins are not yet affected by saturated,
evolved objects.  We also generated a Model B2, incorporating main sequence
luminosity evolution, analogous to Model A2.  The steady-state form of
that model also shows an intermediate-value slope at $L <
\lsat$, but slightly flatter than its analog in
Model B1 because of the structure present at $L<\lsat$
in the burst case (Model A2).

\subsection{Unsaturated Population}

\begin{figure*}
\vspace*{-2.0 truein}
\hspace*{-0.25 truein}
\epsfbox{Oey.fig4.ps}
\vspace*{-3.1 truein}
\caption{Models with the same parameters as in Figures~\ref{unsat}
and \ref{unsatcc}, but for populations with $N_*\leq 10$. $(a)$
Unevolved population; $(b)$ steady-state, continuous creation; $(c)$
single burst at age 4 Myr; $(d)$ single burst at age 7 Myr.  To aid
comparison, these models are plotted on the same scale as
Figures~\ref{unsat} and \ref{unsatcc}.
\label{unsatonly}}
\end{figure*}

In Figure~\ref{unsatonly}, we show models for a population of only
unsaturated clusters.  These are drawn from the same power law
distribution in $N_*$ (equation~\ref{N*}) as the previous models, but
only for $N_* \leq 10$.  For our default stellar parameters with
$17<m<100 \msol$, the saturation transition in $N_*$ is roughly
between 10 and 20 stars.  We use the same stellar parameters as in the
previous models, now with a total of 3000 clusters.
The left side of Figure~\ref{unsatonly} shows the simulation for
the unevolved population ($a$), and continuous creation ($b$);
while the right side shows the single burst case at ages 4 Myr ($c$)
and 7 Myr ($d$).  These models do not include main sequence
luminosity evolution, whose consequences are analogous to those
discussed for Models A2 and B2 above.

It is apparent in Figure~\ref{unsatonly} that the primary difference
in the \hlf\ between this population and the complete power-law
sampling in $N_*$, is that the high-$L$ tail of the unsaturated
objects falls off very steeply.
The highest-luminosity, unsaturated clusters result from a chance
assemblage containing a disproportionate number of high-mass
stars.  Therefore, the
distribution of these objects must fall more
steeply than that of a saturated population, owing largely to the
scarcity of the high-mass stars.  The actual slope in this
regime is once again determined by the detailed statistics of the
cluster compositions, and equations~\ref{imf} and \ref{ml}.

At $L<\lsat$, the behavior of these unsaturated populations
is identical to that seen in the models with a full distribution in $N_*$,
since, as discussed above, this range in $L$ is
dominated by the unsaturated objects.
It is only at the high-$L$ limit itself, in the evolved case of
Figure~\ref{unsatonly}$d$, that the sudden drop due to
sheer lack of objects, effectively generates a steep slope.
Note that at luminosities below this high-$L$ drop-off, the \hlf\
in this model recovers a slope of $\beta$, analogous to
Figure~\ref{unsat}$c$.

\section{Observed \hlf s}

The features and behavior found in the simulated
\hlf s can provide a useful interpretation of the patterns found in
observed \hlf s.

\subsection{Arm and Interarm \hlf s}

In Figure~\ref{arms}, we reproduce the published \hlf s for arm and
interarm populations in six grand design spirals.  The solid
histograms show the arm \hlf s, and the dot-dashed lines show the
interarm \hlf s.  In each case, the peak of the interarm
\hlf\ occurs at a fainter luminosity than that for the arm regions,
suggesting that the interarm \hlf\ mirrors that of the arms at
lower $L$.  This shift in peak occurs despite the smaller total
numbers of \hii\ regions in the interarm areas.  Owing to
incompleteness effects, we might otherwise expect the smaller numbers
to induce a turnover at, if anything, higher $L$.  We do caution
that blending of nebulae (Deharveng et al. 1988; KEH) in the more
crowded arm populations could also introduce a flattening in the
observed \hlf\ at lower $L$.  However, as pointed
out previously (Rand 1992; Knapen {\etal}1993; KEH), the highest-$L$
objects in the interarm regions are apparently always fainter than
those in the arms.  This is again consistent with a group shift in
luminosity.

\begin{figure*}
\vspace*{-0.8 truein}
\epsfbox{Oey.fig5.ps}
\caption{Observed \hlf s for arm (solid lines) and interarm
(dot-dashed lines) populations in grand design spirals:  M51 (Rand
1992); NGC 6814 (Knapen {\etal}1993); NGC 157, NGC 3631, and NGC 6951
(Rozas {\etal}1996a); M100 (Knapen 1997).
\label{arms}}
\end{figure*}

These features exhibit the behavior of our model \hlf s
for the burst scenario.  This is consistent with the expectation that
the arm nebulae are largely coeval, and are undergoing a current burst of
cluster formation; whereas the interarm regions represent, on average,
an older population remaining from previous star formation.  As
seen in Figure~\ref{unsat}, the inflection in
the \hlf\ occurs at progressively lower values with age.
Note that even if incompleteness affects the location of the peak for
the arm objects, which we take to reflect the unevolved population,
the relative shift in the peak for the interarm objects is still
consistent with evolution, owing to the steeper slope at lower $L$.
This is because the low-$L$ bins are more robust to incompleteness for a
steep slope than for a shallow one, since the proportion of missing
objects is the same in each case.  Therefore,
while the absolute location, or existence, of the \hlf\ peak may be
suspect due to observational limitations, the observed shift in peak
for the interarm regions is fully consistent with our model because a
steeper slope is expected at low $L$ (cf. Figure~\ref{unsat}$d$ and
$f$).   Indeed, given that the
\hlf\ peak is often substantially lower in $\log N (\log L)$ for the interarm
regions, this suggests that the actual peak of the distribution has
moved to luminosities much lower than the empirical completeness
limit, as is illustrated, for example, in Figure~\ref{unsat}$f$.

The aging effect can also explain the steeper \hlf\ slopes that
are sometimes reported for the interarm regions as compared
to the arm regions of spiral galaxies (Point~2 in \S 1).
If the actual nebular luminosity function conforms to the two-slope
shape seen in the models, and if the two slopes are not fitted separately,
then the net effect is that the measured slope will be
intermediate between the two.  In our single burst model, the location
of the break moves to lower $L$.  Therefore,
over a fixed range of $L$, the contribution of the shallower slope to
the composite, measured \hlf\ slope will be less for an evolved
burst population, than for an unevolved one.  As is apparent in
Figure~\ref{arms}, it is difficult to pinpoint the location of the
slope change.  We mention once again that our simulations show
a flatter slope in the unsaturated regime than would be expected,
owing to the parameterization of equation~\ref{ml}.
Furthermore, the observed location of $\lsat$ will
also vary with galactic internal extinction, which most \hlf s,
including the ones in Figure~\ref{arms}, do not take into account.
With these difficulties, we suggest that the slopes of the interarm regions
do appear to be the same as those in the saturated regime of the arm
populations.

Thus the differences observed in the \hlf s for arm
and interarm regions are not necessarily due to changes in star
formation environment, but are likely to be affected by evolution.
The time scale between the passage of spiral density waves is of order
$\sim40$ Myr (\eg Rand 1993) at any given location in the disk, which is
much longer than the observable life expectancy of the \hii\ regions.
Thus, the spatial and luminosity distribution of
nebulae between the arms does imply that there is at least a certain
amount of bona fide interarm star formation taking place.  However,
based on the arguments presented in \S 1, we feel that an aging
population is likely to be an important component in the interarm
regions, and that the behavior of the \hlf\ is consistent with this
interpretation.  With the present data and the observational
uncertainties mentioned above, combined with uncertainties in
predicted $q_0$ and its evolution, we have not attempted to place
meaningful age constraints on the evolved population.  However, it will
be interesting to re-examine the data more closely, and search for an
evolutionary progression in the \hlf\ with distance behind the leading
edge of the spiral arms.  We hope to carry out such an investigation
in the near future.

\subsection{The Hubble Sequence}

The correlation of earlier type galaxies with steeper slopes (Point 3 in
\S 1) can be explained by systematically lower cutoffs in $N_*$ in
those clusters.  KEH have shown compelling evidence that
these galaxies have fewer stars per cluster, since
the mean nebular luminosities in the early type spirals
are substantially lower than those in late types, despite the larger
total numbers of \hii\ regions in the earlier types.  Therefore,
unless the stellar ionizing population varies drastically, it is
probable that the
size of the parent clusters must themselves be smaller on average in
the earlier type galaxies.  The same conclusion has been found for Sa
galaxies (Caldwell {\etal}1991), although the total numbers of \hii\
regions are again smaller in those galaxies.

\begin{figure*}
\vspace*{-0.25 truein}
\hspace*{-0.25 truein}
\epsfbox{Oey.fig6.ps}
\vspace*{-6.25 truein}
\caption{($a$)  Model for $3<m<100 \msol$; and ($b$)  model for
$17<m<300 \msol$.  The location of $\bar{l}$ and $\lup$ are indicated
in each case.
\label{trans}}
\end{figure*}

The decrease in typical $N_*$ per cluster with Hubble type (KEH) could
easily result from a decrease in the upper cutoff of the $N_*$ power-law.
The earliest type galaxies would have populations composed only of
unsaturated objects, as would correspond to Sa galaxies,
where the maximum $\log L$ is typically in the range $38.0 - 38.5$
(Caldwell {\etal}1991).  This is the same range in values as the
estimates for $\lup$, as mentioned earlier, hence it is indeed the regime of
unsaturated objects.  As seen in \S 3.3, the models that
describe this population show a steeper high-luminosity tail above
$\lsat$, than do the populations with saturated objects.  Indeed, the
slopes in Sa galaxies have been found to be even steeper than those
for Sb -- Sc types:  the typical \hlf\ slope $a\sim2.6$ for Sa
galaxies (Caldwell {\etal}1991), as compared to $a\sim 2.0$ for Sb --
Sc galaxies (KEH; Banfi {\etal}1993).  The model in
Figure~\ref{unsatonly}$b$, for continuous creation of unsaturated objects,
would therefore be the most appropriate of our simulations to describe
the Sa \hlf s.  The form of the Sa \hlf s shown in
Figure~5 of Caldwell {\etal}(1991) show a consistent resemblance with
our models in Figure~\ref{unsatonly}.  Thus, ironically, although
these nebulae are dominated by unsaturated objects whose
characteristic slope is flatter than the saturated case, the high-$L$
drop-off will induce a steeper measured slope in these populations.

The Sb -- Sc galaxies would then show a slope intermediate between the
Sa and Im types (cf. Figures~4$b$ and 3$b$), as the upper cutoff in
$N_*$ approaches the exclusively
unsaturated regime.  Indeed, KEH suggest that the \hlf\ in Sb -- Sc
galaxies is truncated at an upper-$L$ limit.  This is quantitatively
supported by MW97, who also find evidence for a
truncated \hlf\ in the Milky Way and Sb--Sc galaxies, but not in
irregular galaxies.  Since this limit is still
at $L$ above the regime of unsaturated objects, these findings are
consistent with our interpretation of a progressively lower
upper-$N_*$ cutoff with earlier Hubble type.  There may be exceptions
caused by temporarily enhanced star formation, in which large numbers
of saturated clusters are formed.  This scenario can explain the
larger range in \hlf\ slope seen in earlier type galaxies (KEH).
Indeed, a slope steepening at high $L$ reported in some earlier type
galaxies could well correspond to a cutoff; indeed, KEH note that it
is often impossible to distinguish such a turnover from a cutoff.
Thus the steepening in slope for disk galaxies across the Hubble
sequence can be explained by a simple trend in upper cutoff of the
$N_*$ distribution, and need not invoke a change in the parent
slope $\beta$ of $N_*$.

\subsection{The Slope Transition}

In \S 3, we denoted the luminosity of the slope break in the
initial \hlf\ by $\lsat$ and noted that, as in the models of MW97,
this often corresponds to the luminosity
contributed by most luminous star in the IMF, $\lup$.  We
however caution that this correspondence is dependent on the stellar
parameters.  As an example,
Figure~\ref{trans} exhibits the \hlf\ resulting from two models with
identical IMF slope and $m-l$ relation, but with different stellar
mass limits.  Figure~\ref{trans}$a$, with $3<m<100 \msol$, exhibits an \hlf\
that more closely resembles in form the simulation by MW97.
There are two principal slope breaks apparent:  one near
$\lup$; and one near $\bar{l}$, below which the slope appears quite flat.
The existence of a minimum cluster membership number, $N_*=1$, causes
this flattening, or in some cases even positive slope, for
luminosities below the expectation value of $L$ containing single
stars, i.e., the average stellar luminosity $\bar{l}$.
At $\bar{l}<L<\lup$, there is an intermediate slope in the \hlf\ that
joins the flat regime to the saturated regime of slope $\beta$.
A small transition region of $\lesssim 0.3$ dex is noticeable in this
intermediate-slope region near both $\bar{l}$ and $\lup$, which
results from the form of the IMF adopted in equation~\ref{imf}.  With
instead a sharp IMF truncation at $\mup$, the slope breaks would occur cleanly
at $\bar{l}$ and $\lup$.

One can now see that certain stellar mass ranges and values of $\delta$
can change the relative location of the two breaks such that one or
the other could disappear.  The model in Figure~\ref{trans}$b$, with
$17<m<300 \msol$, shows an example where the $\lup$ slope break is
virtually undetectable at $\log \lup=39.2$.  The smaller difference
between $\bar{l}$ and ${\lup}$ has compressed the intermediate-slope
range in $L$-space, thereby steepening its slope to a value closer to
$\beta$, which represents the maximum slope possible in this regime.
An observed \hlf\ similar to Figure~\ref{trans}$b$ would
most likely be measured to have only one slope in the regime $L>\bar{l}$.
Note that the models in Figure~\ref{trans} are probably
unrealistic, since $\delta=1.5$ is not representative over such large
mass ranges, and we only show these for illustrative purposes.
However, these examples demonstrate that breaks in observed \hlf s
should be interpreted with caution, and may only provide a lower limit
to the most luminous star in the IMF.
Furthermore, the tendency of the highest-mass stars to approach
similar ionizing emission rates $q_0$ (\eg Leitherer 1990), compounds the
insensitivity of $\lup$ to $\mup$.  We therefore conclude that,
unfortunately, the \hlf\ is not a useful probe of $\mup$.

However, the insensitivity of $\lup$ to $\mup$ suggests that
the high-$L$ end of the \hlf\ should be a reliable indicator of
$\beta$ for saturated nebular populations, since it diminishes the
likelihood of a varying $\mup$
as an explanation for the observed variations in the \hlf.
The principal caveat is that a truncation at maximum $N_*$ not be
confused with a steep slope of $\beta$, as may have been done for Sa
galaxies in the past (see above).
It is also apparent that, since the form of the \hlf\ is sensitive to
the stellar parameters, that demonstrable variations in the
unsaturated regime of the zero-age or continuous creation \hlf\
could possibly indicate substantial variations in the stellar
parameters of the hottest stars.

We note that stochastic variations in $\mup$ within a galaxy will not
change the location of the break if the distribution of $\mup$ is
gaussian.  We confirmed this by drawing $\mup$ from a parent normal
distribution of $\sigma = 15\msol$ and the same mean value of
100$\msol$.  The resulting \hlf\ is indistinguishable from that with a
constant $\mup$.

Empirically, a flattening at lower
$L$ is often seen in many galaxies (Point 1 in \S 1), but at varying critical
luminosities.  While the models for a single burst show that the
transition point is not necessarily fixed, $\lsat$ cannot be greater
than $\lup.$
At present, the value of $\lup$, the \Ha\ luminosity associated with
$\mup$, is not well-determined.  Our models have adopted a value of
$\lup = 3 \times 10^{38}\ \ergs$, which is uncertain within a factor
of a few, and is a high estimate.  Most published \hlf s are not
corrected for internal extinction within the galaxies, which
will affect the location of the break.  As can be seen in Figure~8$b$
of Walterbos \& Braun (1992), extinction correction for the
highly-inclined case of M31 can shift the location of the apparent
turnover by
an order of magnitude.  It is also important to distinguish between
a real slope change and artificial slope flattening induced by
limitations such as incompleteness, and the more insidious problem of
object blending, mentioned above, for more distant galaxies.
In view of the difficulty in pinpointing the location of a slope
change, and the variations induced by reddening and possible aging
effects, we suggest that the published \hlf\ slopes are thus far
consistent with our models.

We note that KEH modeled the lower-$L$ end of the \hlf\ by
combining the $m - l$ relation with the IMF for single-star
\hii\ regions.  This representation is somewhat different from ours,
since we include multiple-star, low-$L$ objects that will contribute
to the same luminosity bins occupied by bright, single-star nebulae.
Our slope in this regime will therefore tend to be slightly flatter
(more positive) than theirs.  This will affect estimates for the
fraction of total galactic ionizing emission due to faint \hii\
regions below empirical completeness limits, such that those using the
KEH model are an upper limit for similar stellar parameters.

Additional models of the \hlf\ by Feinstein (1997) came to our
attention during the refereeing process.  These models consider only
nebular populations with luminosities scaled from objects with a
saturated IMF, but with $m_{\rm lo}$ extending down to $5\msol$.  We
emphasize that, since unsaturated clusters are not considered, the
slope turnover seen in those models is therefore
{\it not} caused by the same mechanism seen in our work, or
that of KEH and MW97.  Rather, the slope break seen in Feinstein's
models result from the adopted lower cutoff in the $L$ distribution,
combined with an extended creation period.  The zero-age, saturated
\hlf\ is described by the power-law $\beta$, which simply shifts to
lower luminosity with advancing age, as exhibited by the saturated
tail of our models in Figure~\ref{unsat}.  Feinstein's continuous
creation models are therefore a superposition of many power-laws with
a continuous range of ages.  The lower-$L$ cutoff seen in those models
therefore induces a flattening in the \hlf\ below that luminosity.
This is best illustrated in the right panel of Feinstein's Figure~3,
which varies the lower-$L$ cutoff according to assumed total stellar
mass, for continuous creation.  The slope break occurs at
the lower-$L$ cutoff, hence, as pointed out by the author,
this parameter determines the location of the break.  We caution,
however, that the lower-$L$ cutoffs used in Feinstein's models are
necessarily artificial, owing to the consideration of only saturated
\hii\ regions.  Therefore, the slope breaks seen in these models must
be regarded as artificial to the same extent.  If, however, nebular
creation scenarios exist with such a strong lower-$L$ cutoff,
Feinstein's models demonstrate another mechanism which can also induce
a slope break.

Previous work has sometimes suggested an empirical slope change
at high luminosities of $\log L\sim 38.6$ or even higher (Rozas
{\etal}1996a; Rand 1992; KEH).  If a break at these high luminosities
is real, it is unlikely to result from the stochastic effect below $\lsat$.
However, if the high-$L$ slope is steep enough, it could well be a
manifestation of the maximum $N_*$ cutoff in those galaxies, which is
expected to vary in the scenario we presented in \S 4.2.  It could
also result from a change in $\lsat$, although this appears unlikely,
as argued above.  But factors other than those that we have considered
can affect the form of the \hlf\ as well.  For example, Rozas
{\etal}(1996a,b) suggest that such a break at high $L$ results from
a transition between radiation-bounded nebulae at fainter
luminosities, to density-bounded objects at brighter luminosities.
Another potentially
important effect is a differential extinction pattern among the nebular
population, and of course, the usual differences in IMF slope and star
forming conditions.  Given the currently available data, the
systematic presence of an additional, high-luminosity slope change
at a fixed $L$ remains controversial.

\section{Conclusion}

We have modeled the \hlf\ with Monte Carlo simulations that draw $N_*$
for each cluster from a power-law distribution of constant slope, and
for each cluster, $m$ from a Salpeter IMF truncated at
$\mup=100\msol$.  As found by MW97, this produces
shallower slopes corresponding to the population dominated by
unsaturated objects, and a steeper, high-$L$ side dominated by
saturated ones.  The saturated slope is $\beta$, the slope of the
$N_*$ distribution (equation~\ref{N*}).  The transition
luminosity $\lsat$ in the unevolved \hlf\ may correspond to $\lup$, the
\Ha\ luminosity due to a single star of mass $\mup$, but this depends
on the assumed stellar parameters.  The observed \hlf s do often show
flatter slopes at lower luminosities that are consistent with the
transition at $\lsat$ (\eg Walterbos \& Braun 1992; Scowen, Dufour, \&
Hester 1992).

We have hitherto not discussed the form of the \hlf\ below $l_{\rm
lo}$, which is unexplored in our models.  Since the slope $\delta$ of
the $m - l$ relation (equation~\ref{ml}) steepens, the \hlf\ will
continue to grow flatter for the same $N_*$ power law, extending to
lower luminosities.  At $\log L
\lesssim 36$, contamination from planetary nebulae may become
important (Walterbos \& Braun 1992), while confusion and background
diffuse \Ha\ emission will undoubtedly limit the \hlf\ in this regime.

Our simulations show that for a single-burst case, the slope transition
moves to lower $L$ as the population ages and the saturated objects
grow fainter (Figure~\ref{unsat}).  Hence, the
steady-state model for continuous creation shows a slope in the
region $L<\lsat$ that is intermediate between its value in the unevolved
\hlf\ and the slope $\beta$ of the saturated objects
(Figure~\ref{unsatcc}).  Models that
include main-sequence evolution for stellar ionizing luminosities show
a faster evolution than those that do not, with a noticeable peak
around the transition between saturated and unsaturated populations
(Figure~\ref{unsat}$e$).
The steady-state model for continuous creation
incorporating stellar evolution yields a slightly shallower slope than
that for the case without stellar evolution, but still steeper than
the unevolved case.  Models for a population of only
unsaturated clusters with $N_*\leq 10$ show a much steeper drop-off at
$L> \lsat$ (Figure~\ref{unsatonly}), where the \hlf\ is normally
dominated by saturated objects.  The behavior at $L<\lsat$ is generally
the same as that for the models with fully populated $N_*$, with the
exception of a high-$L$ drop-off in an evolving burst.

The patterns seen in observed \hlf s in nearby galaxies can be
explained by the behavior of these models.  If \hii\ regions in spiral
arms of galaxies represent a current burst of coeval star formation,
then the steeper slopes seen in interarm vs. arm regions can be
explained as an aging burst compared to a current burst population.
Since single slope measurements will yield a composite of the
saturated and unsaturated slopes, the zero-age \hlf\ will show a
flatter slope owing to the larger range of unsaturated objects.  The
lower peak $L$ and maximum $L$ seen in the interarm regions are also consistent
with a dominant contribution from an aging population.

The steeper slopes seen in earlier galactic Hubble types can be
explained by the lower cutoff in maximum $N_*$.  As seen in the models for
populations of only unsaturated clusters (Figure~\ref{unsatonly}), the
high-$L$ tail is much steeper than in populations with higher $N_*$.
A truncation at the high end of the \hlf\ has been suggested by
KEH and MW97.
Since the mean $N_*$ does apparently decrease in earlier type galaxies
to the values in unsaturated clusters (KEH; Caldwell {\etal}1991), the
steeper \hlf\ slopes are likely to simply result from a lower maximum $N_*$.
A slope dropoff therefore may also be seen at $L$ corresponding to the
maximum $N_*$.

Thus, we suggest that the current data are consistent
with evolutionary effects and the upper-$N_*$ cutoff being the primary
determinants of the shape of the \hlf.
Indeed, it may be unnecessary to invoke
any other parameters for the nebular and cluster properties to
explain the behavior of the \hlf\ as described in \S 1.
If this is true, it is rather remarkable, for example, that grand design
spirals with strong star formation induced by tidal interactions, would
show the same power-law distribution in $N_*$ as those found in normal
disk and irregular galaxies.  However, we
again acknowledge that other, unexplored effects, such as
gas density bounding, differential
reddening, and variations in IMF and other stellar parameters, can
influence the form of the \hlf.  Nor can we rule out suggested
environmental influence like variations in slope of the molecular
cloud mass spectrum.  But thus far, it appears that the power-law
slope $\beta$ of $N_*$ might vary even less than was suggested by the
observed slopes of the \hlf, even though the rate and total star formation
can vary by one to two orders of magnitude.  Further detailed
observations of the \hlf, and re-examination of those in the
literature, are of great interest in evaluating
the possibility of a universal $\beta\sim 2$.  Suggestively, Caldwell
{\etal}(1991) find that the luminosity function of knots seen in the
$B$ continuum of four of their Sa galaxies do show such a power-law
exponent $\sim 2$.

As is done with the luminosity functions of distant galaxies,
it may thus be possible to use the form of the \hlf\ to understand
features in the most recent star formation history ($\lesssim 10$ Myr)
of their host galaxies, since
individual bursts can leave their imprint on the \hlf.  Our models,
for example, show that an aged burst population is distinguishable
from continuous creation of low-$N_*$ clusters
(cf. Figures~\ref{unsat}$c$,$f$ and \ref{unsatonly}$b$).
Feinstein (1997) also demonstrates effects of different creation
histories.  At present,
it is difficult to make useful quantitative constraints, owing to present
constraints on stellar and cluster parameters, but it is at least
possible gain qualitative insight on the recent star formation history.

\acknowledgments

We thank Rob Kennicutt, Johan Knapen, and the referee, Carlos
Feinstein, for comments on the manuscript.  We also thank
Johan Knapen for access to data for M100 in advance of publication,
and John Beckman for an interesting discussion.

redpajama_set_name: RedPajamaArXiv


text:
Als Inseln über dem Winde, auch Inseln vor dem Wind oder Inseln im Wind (in nicht-deutschsprachigen Kartenwerken oder in solchen mit internationaler Beschriftung auch , , ,  oder ), bezeichnet man im Deutschen die windzugewandte, meist östliche Hälfte größerer Inselgruppen in tropischen Meeresregionen. Diese Benennung entstammt der historischen Seefahrt und liegt darin begründet, dass über den tropischen Meeren die Passatwinde wehen, die vorzugsweise aus östlichen Richtungen kommen. Die windabgewandten, meist westlichen Hälften dieser Inselgruppen heißen entsprechend Inseln unter dem Winde.

Als Inseln über dem Winde werden folgende Inselgruppen bezeichnet:

Inselgruppe
Choronym

redpajama_set_name: RedPajamaWikipedia


text:
Robbie Williams >
Robbie Williams signs publishing deal and will release new...
Robbie Williams signs publishing deal and will release new album in 2019
By Bang Showbiz in Music / Festivals on 05 November 2019
Follow Robbie Williams
Robbie Williams Bryan Adams
Robbie Williams has inked a global publishing deal with Universal Music Publish Group which will see him release his 13th studio album by the end of 2019.
Robbie Williams has signed a new deal with Universal Music Publishing Group (UMPG) which will see him release his 13th studio album this year.
The 'Rock DJ' hitmaker has recently confirmed his debut Christmas album, 'The Christmas Present', will be released on November 22, and now it's been announced that as part of his new contract with the music label, his follow-up to 2016's 'The Heavy Entertainment Show' will be out before the end of 2019 as well.
The global administration deal with Robbie's own publishing company, Farrell Music, includes all of his existing and future works.
UMPG UK's Managing Director, Mike McCormack said: ''It's such a pleasure to be reunited with Robbie and his management team at ie: music after so many years.
''I first signed Robbie as a young, fresh faced member of Take That back in the early 90s when I was at Virgin Music and even then, he was a huge personality and a pleasure to work with. He's gone on to become a global superstar and an incredible songwriter - so it's a privilege to represent all these great songs and the new material he will be writing in the future.''
Robbie's upcoming festive record features debuts with Tyson Fury, Bryan Adams, Sir Rod Stewart, his dad and his young daughter Teddy.
The 45-year-old singer asked the 31-year-old boxer to sing on 'Bad Sharon', a song about a ''boozy office party'', and he said the heavyweight ''smashed it'' in the recording studio.
He said of the track: ''That makes sense in some sort of universe! I got my residency in Vegas and while I was out there Tyson was fighting and he invited me into his dressing room, is it called a dressing room when you fight? I don't know.
''And I asked him and he said yes and the song itself, 'Bad Sharon', is basically a boozy office party somewhere in the Midlands and it makes sense for Tyson, in that moment in my head, and to be fair he's smashed it.''
Robbie was also delighted to have both Bryan and Rod record songs for the album because they have always been inspirations to him.
He said of the pair: ''People that I know, people that I like and people that I've got captive audience with that can't say no in that moment when you ask them to do it. It's easier on emails to say no.
''That was like two years ago and they'd forgotten but I hadn't...' me again'. They're both really lovely chaps, incredibly nice people, incredibly nice with me and I look up to them and they're the people I've gone, 'Right OK, what happens to your career when you get older, where do you go? How do you do it?' And I watch them for inspiration.''
The 'Angels' singer - who will perform a festive show at the SSE Arena, Wembley, in support of the record on December 16, and is also playing Hits Live Manchester on November 17 and Magic of Christmas at the London Palladium on November 24 - teamed up with his father Pete Conway on 'A Wonderful Life' and his daughter Teddy, seven, has a small part on the track 'Home'.
Robbie Williams: Monogamy is my greatest achievement
Robbie Williams: I still love working
Robbie Williams met Ayda Field after sleeping with drug dealer
Robbie Williams wants to hire detective to find Jason Orange
Robbie Williams says daughter is destined for music career
Robbie Williams jokes Ayda Field didn't make the cut for Christmas duet
Robbie Williams: Middle age makes for boring songs
Robbie Williams and Ayda Field to hire social club to renew vows
Robbie Williams: 'I don't like myself very much'
Robbie Williams cancels plans for Liam Gallagher boxing match
Robbie Williams is hopeful he and Britney Spears will record festive duet
Robbie Williams praises supportive Sir Elton John
Robbie Williams thinks Oasis reunion would fail to live up to Take That comeback hype
Robbie Williams struggled to live up to huge record deal
De-Lovely Movie Review
"This is one of those avant-garde things, is it?" says a droll, dubious and dying...


Upset about the UMass Amherst - Mt. Ida deal? The underfunding of our Boston campus? The disrespect being shown to us by the UMass Board of Trustees?
You should have received the following notice (see below) from the Administration about joint UMB and MTA retirement workshops being held tomorrow and Wednesday of this week, along with additional UMB HR retirement workshops starting May 1st. We encourage you to attend.
If you are an FSU/MTA union member in good standing and are unable to attend one of the sessions below please contact us so that we may put you in touch with Ed McCourt, the MTA retirement specialist, for further consultation.


Zynga (NASDAQ:ZNGA) said Monday afternoon it plans to cut about 18% of its workforce as it moves to cut costs amid a shift toward mobile games.
Shares were briefly halted on the Nasdaq Stock Market in afternoon trading ahead of Zynga's announcement. The stock closed Monday down 12% at $2.99.
The maker of online games will lay off 520 workers by August and close several office locations, taking pre-tax charges of $24 million to $26 million this quarter and about $5 million in the third quarter. Zynga expects to cut expenses by as much as $80 annually.
While the company reaffirmed its prior outlook for revenue and per-share earnings this quarter, Zynga now expects to post a loss of $28.5 million to $39 million versus its prior estimate of $26.5 million to $36.5 million.
"None of us ever expected to face a day like today, especially when so much of our culture has been about growth," founder and CEO Mark Pincus said in a note to employees that was posted on the company's blog.
The San Francisco-based company has struggled to capitalize on the rise of mobile gaming, losing much of the momentum it gained from its popular social games. It also relied upon Facebook (NASDAQ:FB) for attracting users but has seen less exposure on the site.
Zynga posted a surprise profit in the first quarter in the wake of other cost-cutting moves. In October, the company announced it would cut 145 positions, or about 5% of its workforce, closing studios in Boston, Japan and the U.K. Then in February, Zynga shut its doors in Baltimore and reduced the number of New York offices to slash its workforce by another 1%.
All Things Digital first reported news of the layoffs, citing a source as saying Zynga is now closing offices in New York and Los Angeles.
With the cuts announced Monday, Zynga has reduced its workforce by about 24% over the last eight months. As of March 31, 2012, Zynga had about 2,916 employees.


April 20, 2018 - With SecurityBridge, Pilz is expanding its product range to include the area of Industrial Security. The Pilz SecurityBridge protects the connections between the programming/configuration tools and the hardware controllers from manipulation by detecting unauthorised changes to the automation project, for example. The SecurityBridge acts as a firewall. However they do not need complex configuration; thanks to application-specific default settings they use the plug-and-play principle.
Pilz also develops products from the perspective of security, within a TÜV-certified process in accordance with IEC 62443-4-1. Aspects such as threat scenarios, strengths and weaknesses of protocols or encryption methods are taken into consideration from the outset.
The same applies for both security and safety: To ensure that technical measures can work, these must be accompanied by organisational measures such as handling instructions, procedures and training. The Pilz Academy therefore offers training courses on the topic of industrial security.


text:
Illumination is the fourth studio album by the Scottish band The Pastels, originally released via Domino Recording Company in 1997. The album shows the group honing in on a warmer, gentler and more subdued sound compared to their previous work. It is their last studio album to feature longtime member Annabel "Aggi" Wright as a full member before she left to concentrate on her career as an illustrator in 2000. Whilst The Pastels continued to release music, Illumination would be their last proper studio album for 16 years, until the release of Slow Summits in 2013.

Reception
Stephen Thomas Erlewine of AllMusic gave the album 3.5 stars out of 5, saying, "Scaling back the snappy production and crisp guitars of their earlier releases, the group crafts a collection of subdued, lovely melodies in the vein of the Velvet Underground's third album." He added, "While the Pastels lack Lou Reed's lyricism or the Velvets' assured experimentalism, the hushed ambience and sighing melodies of Illumination make it a charming listen." Angela Lewis of The Independent said, "The patron saints of Scottish indie pop retain their love of gently poignant lyrics and mellow guitar rustlings with their umpteenth album in 10 years; but now there's a new electronic edge, adding curiosity value."

Track listing

Personnel
Credits adapted from liner notes.
 Stephen Pastel – guitar, vocals, keyboards
 Aggi Wright – bass guitar, vocals, melodica
 Katrina Mitchell – drums, vocals, keyboards, melodica, violin, arrangement
 Jonathan Kilgour – guitar
 Gerard Love – guitar
 Norman Blake – guitar, vocals
 Dean Wareham – guitar, vocals
 Bill Wells – piano, arrangement
 Sarah Ward – flute
 Isobel Campbell – cello
 Dawn Kelly – French horn
 Gregor Reid – percussion

References

External links

1997 albums
The Pastels albums
Domino Recording Company albums


Wildlife, Mammals, Birds, Nature,Interesting Facts and much much more! 'Life' from the South African Bush.
With five species of 'Roller' in South Africa the European Roller (Coracias garrulus) is quite common but is one of the largest of the 'Rollers' species. The European Roller is a summer migrant from Europe which is called here in South Africa a 'Paleartic Migrant'. Being a bird of warmer climes the European Roller will in the next few weeks start heading back to North Africa/Europe/Middle East.
All images and text are copyright of © Tony Sparkes. Simple theme. Powered by Blogger.


text:
Home›World›What is the secret of the equipment in which Messi performed at the World Cup?
What is the secret of the equipment in which Messi performed at the World Cup?
After the 2022 World Cup final, the meaning of the traditional Qatari outfit of Argentina captain Lionel Messi was revealed.
Argentina won the 2022 FIFA World Cup hosted by Qatar after 36 years, beating France on penalties in a final that ended 2-2 in regular time and 3-3 in extra time. At the end of the match, captain Lionel Messi, who stepped onto the podium to present the trophy, was dressed as the Emir of Qatar. "Bisht" The traditional dress is called
BIST PRESENTS ARAB CULTURE
It has come to light that Bisht, also known as Besht, was actually used by Qatari men and symbolized Arab culture. Bisht, which is used especially on formal occasions and ceremonies, is made from this fine fabric, which is preferred by the Arabs in the Gulf countries and comes in various colors such as grey, black, brown, white and beige.
During the awards ceremony, the Emir of Qatar, Sheikh Tamim bin Hamed Al Sani, and FIFA President Infantino made a historic pose, dressing Messi in local clothes.
On the other hand, Lionel Messi won his first title in the second World Cup final of his career.
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The opening track is the Phantasy for Viola and Piano Op.54 from 1914 by the English composer York Bowen. It's a simply gorgeous work which perfectly showcases the warmth, lightness and agility of Lipman's playing as well as the top-notch contribution from Kramer. The standard never drops throughout the world premiere recording of Assad's two-part Metamorfose or Robert Schumann's four Märchenbilder Op.113.
Fuga libre by the Irish violist and composer Garth Knox is the only solo viola work on the CD. Written in 2008 for the Tokyo International Viola Competition, it uses some really interesting effects, including quite fascinating harmonic glissandi.
Shostakovich's very brief (at 1:56) Impromptu for Viola and Piano Op.33, written in 1931 but not discovered until 2017, is another world premiere recording, Lipman having managed to obtain a pre-publication transcript of the score from the DSCH Publishing House. A viola arrangement of Franz Waxman's virtuosic Carmen Fantasie brings an outstanding CD to a close, Lipman's flawless technique, beautiful tone and consummate musicianship making for viola playing as fine as any you will hear.
It's difficult to think of a more exciting duo than violinist Alina Ibragimova and her long-time pianist partner Cédric Tiberghien. Their 3-CD live recital set of the complete Beethoven violin sonatas contained some electrifying performances, and they bring the same level of playing to their latest CD, Vierne & Franck: Violin Sonatas, a recital of works that pay homage in their own ways to 19th-century musical thinking, their fairly dense textures and serious nature being qualities that would be rejected in post-WWI Paris (Hyperion CDA68204 hyperion-records.co.uk).
The Poème élégiaque Op.12 by Eugène Ysaÿe opens the CD – and what an opening it is! Published in the piano version in 1893 and the first of Ysaÿe's nine Poèmes for string instruments and orchestra, it was inspired by the death and funeral scenes from Shakespeare's Romeo and Juliet and employs scordatura tuning for darker colour, the low G string being tuned down to F. It's a rhapsodic, passionate work that perfectly showcases this duo's strengths: tone, nuance, intelligence, passion, commitment, and flawless technical assurance.
César Franck's Violin Sonata in A Major was written in 1886 as a wedding present for Ysaÿe; it's been popular for so long that hearing it again is like revisiting an old and treasured friend, and the visit here is a truly lovely one. The connections between the works on the disc continue with Louis Vierne's outstanding Violin Sonata in G Minor Op.23. Vierne was a pupil of Franck, and this sonata was written at Ysaÿe's request and premiered by him in 1908. It's a sweeping work much in the style of the Franck, and deserves to be much better known.
The brief Nocturne from 1911 by the 18-year-old Lili Boulanger, Nadia's younger sister, acts as a light dessert after the richness that has preceded it, and ends a CD of music-making of the highest order.
Whenever there's another CD from the always wonderful Steven Isserlis in the new releases, you just know you're in for something special, and so it proves yet again with Shostakovich & Kabalevsky Cello Sonatas, Isserlis being joined by his recital partner of over 30 years, pianist Olli Mustonen (Hyperion CDA68239 hyperion-records.co.uk).
The Shostakovich Sonata in D Minor Op.40, written in 1934 when the composer was in his late 20s, sets the tone for the whole CD, Isserlis displaying his usual full-blooded and passionate, yet always sensitive and musically intelligent playing, especially in the opening movement and the fiendish and demonic second. Mustonen is his equal in every respect.
There's no doubting the strength and quality of Kabalevsky's Sonata in B-flat major Op.71, written for Rostropovich in 1962. Isserlis notes that this is a work that should really be heard more often, and his performance here makes an even stronger case.
Three short works round out the CD. Shostakovich's brief (at 2:31) Moderato was only published in 1986 after being discovered in a Moscow archive alongside the manuscript of the Cello Sonata. It's believed to be from the same period, but its real provenance remains unknown. Prokofiev's Adagio – Cinderella and the Prince is a 1944 arrangement of a section from his ballet Cinderella. Kabalevsky's Rondo in memory of Prokofiev Op.79 was the third of three test-piece Rondos he wrote for the Tchaikovsky Competition in Moscow – one for piano in 1958, one for violin in 1962 and this one in 1965. It's quite substantial, with more than a hint of Prokofiev's music, especially the wispy "wind-in-the-graveyard" effect from the first violin sonata.
In his usual outstanding booklet notes Isserlis includes his customary exact timing references to salient points in the works, adding an extra touch of class to a simply outstanding CD.
In his introductory booklet notes to Bach: The Cello Suites (Hyperion CDA68261 hyperion-records.co.uk) the German cellist Alban Gerhardt reveals that, like so many others, he was reluctant to even try recording these challenging works before turning 50 – which he does this coming May. He is also aware that any recording can never be a final word.
He consequently uses vibrato "with great care and control" and aims for "a seemingly effortless articulation with as much depth to the sound as possible." Add Gerhardt's 1710 Matteo Gofriller cello and the results are simply beautiful. It's a set that easily holds its own in a very competitive field.
With the BIS Super Audio CD Tan Dun: Fire Ritual – Violin Concertos we enter the distinctive sound world of the Chinese composer Tan Dun, now in his early 60s. The Norwegian violinist Eldbjørg Hemsing has been collaborating with the composer since 2010, a relationship which resulted in the creation of both of the works on the CD: the violin concertos Rhapsody and Fantasia and Fire Ritual. Tan Dun conducts the Oslo Philharmonic Orchestra (BIS-2406 bis.se).
An early version of the Rhapsody and Fantasia was originally written over a decade ago, but the work is heard here in the 2018 revision for Hemsing. The two movements, each of three parts, have their roots in ancient Peking opera melody, Tan Dun having been a conductor of a travelling Peking Opera troupe in his teens.
Fire Ritual was written for Hemsing and premiered by her in Oslo in September 2018. Subtitled A music ritual for the Victims of War, it unfolds from – and stays centred on – the single note D, using its status as "Re" on the solfège scale as a prefix meaning "again," as in the Renewal, Resurrection, Return and Rebirth of souls who were lost in wars.
Both concertos have a similar sound, with little Western melodic (or harmonic, for that matter) material, prominent percussion sections (four players with at least 20 mainly Chinese percussion instruments) and a distinctly Chinese flavour to the solo violin writing. Hemsing is outstanding in what must be considered definitive performances.
Formed in 2002 for a concert tour of Taiwan, the Formosa Quartet celebrates its members' Taiwanese heritage on From Hungary to Taiwan, a project that pairs treatments of folk music from the two countries and explores their similarities (Bridge Records 9519 bridgerecords.com).
Dana Wilson's Hungarian Folk Songs was commissioned by the quartet as "a sort of entrée" into Béla Bartók's quartets. Wilson says that he tried to capture key aspects of the traditional music itself and not just write his own music inspired by it, and he certainly succeeded. The Formosa Quartet perfectly captures his remarkable folk music effects and nuances.
In Song Recollections, another work written for the group, Chinese composer Lei Liang studies Taiwan's art, songs and people. His settings of five songs from four native tribes are mostly quiet and atmospheric, with a distinctly Chinese feel.
Béla Bartók's String Quartet No.4 from 1928, constructed as a five-movement symmetrical arch with the Night Music slow movement at its heart, is the major work on the CD.
Another Formosa Quartet commission, Wei-Chieh Lin's Four Taiwanese Folk Songs from 2017 ends the disc. These clearly popular and much-loved melodies, two of them written in the 1930s, are given lush, Romantic treatment, and draw rich, warm and evocative playing from the quartet.
A bonus track, Spring Breeze, is available only through an online link; it turns out to be the first of Five – not Four – Taiwanese Folk Songs, so its omission from the CD is a bit odd. Still, it's a gorgeous piece, and you can watch the quartet performing the complete set on YouTube. It's well worth watching, and well worth a listen.
The Juilliard String Quartet has been around since 1946, and although founding first violinist Robert Mann lasted for an astonishing 51 years and two subsequent members for over 40 years each, the ensemble has had a total of 17 members during its existence. The 2017 lineup (first violin Joseph Lin left in 2018) is featured on Juilliard String Quartet: Beethoven, Davidovsky, Bartók, a CD recorded as part of the group's 70th anniversary celebrations (Sony Classical 19075 88454 2 sonymusicmasterworks.com).
The quartet's longstanding commitment to both the classic repertoire and new contemporary works is fully evident here. A suitably tense and energetic performance of Beethoven's String Quartet in F Minor Op.95 "Serioso" opens the disc, and the centrepiece is Mario Davidovsky's Fragments, String Quartet No.6 from 2016, written on a commission for the Juilliard. Davidovsky explains that the title refers to broken and scattered parts that, "moved and processed by some creative force, can aggregate to become something." It certainly gives you a good idea of what the quite brief work sounds like as it moves from a fairly abrasive start to a more integrated ending.
A passionate and powerful performance of Bartók's String Quartet No.1 ends the CD. It's a work with a distinct post-Romantic feel, and no hint of the Night Music of the later quartets – more an indication of where the composer has come from than where he is going.
The playing throughout is of the exceptionally high standard we have come to expect from this ensemble.


Tools/Items needed: Ratchet (2 if possible) and socket set from 12mm-17mm, allen wrenches, open end wrench for the shock bolt, thin masking tape, spring compressor, jack, jackstands.
Step 2: We'll start with the rear. It's best to remove the interior parts first so you don't get the fabrics dirty after handling the suspension parts. Start by removing the rear bench cushion. Reach under the front part of the cushion on either ends and yank up to pop the cushion loose. There are two. Next, there is one bolt holding it down in the back crevice between the 2 seat belt latches.
Step 3: Fold the rear seats down (Place a towel underneath the seat so it doesn't contact the floor directly).
Step 4: Remove the two side cushions on either end. They are held in place by one bolt at the base. Once the bolt is removed, slide the seat cushion up to unlatch the hook.
Step 5: Remove the plastic cover to gain access to the top mounts of the shock. The plastic cover is held in place at 4 points. 2 of the points are held by plastic retainers which simply pop out by reaching in the back and tugging upward. They're located about 1/4 way in from each end. Once they are popped out, hold the plastic up and slide it forward towards the front of the car.
Step 6: Remove the bolts holding the shock in place.
Step 7: Removal of the suspension. 1st, remove the swaybar endlink bolt that's connected to the lower arm. Next remove the bottom bolt of the shock. Carefully remove the suspension (you might need to press down on the control arms) If you have a second person, have him press it down with his foot.
Step 8: Compress the springs using a spring compressor (in many places, auto parts stores offer these tools as loaners). While the springs are adequately compressed, remove the top mount using an open ended wrench and an allen wrench holding the strut rod still. *Keep track of how the washers and other components are placed once the top mount is removed.
**If you're switching to coilovers, you will only be reusing the top mount unless yours includes one. The pic below are the components of the suspension.
Step 9: If you're reusing the stock bump stop, saw it in half with a hacksaw, knife, etc. When using aftermarket springs, you normally do not need to use a spring compressor. you should be able to put the top mount on and push down on the spring to get the nut back into place. From there you can just tighten the nut. It should be fairly tight, but not to the point where you burst a vein.
Step 10: Reinstall the assembled suspension. Torque specs: bottom shock bolt - 43 ft. lbs.; swaybar endlink - 29 ft. lbs.; top mount bolts - 37 ft. lbs. You should put the interior back together after the front and rear installation is done and a test drive was taken. This way you can make adjustments if needed without removing everything again.
Step 11: The front side. Jack the front up **Jackpoints** and support the front on jackstands.
Step 12: Loosen the top mount bolts and brace bolts, but do not remove them completely.
Step 13: Remove the 2 bolts for the brake line support.
Step15: Using 2 ratchets (on both sides of the bolt/nut), remove the bolt holding the fork part of the suspension. Slide the fork off the bottom of the shock.
Step 16: Remove the bolts from the top mount. Hold the suspension (or have someone else hold it) before removing the last nut so it doesn't drop.
Step 17: Most likely the suspension will be difficult to remove completely. Jack the lower control arm up a little and you should be able to remove the suspension.
Step 18: **IMPORTANT - IMPORTANT - IMPORTANT** NOTE: IF YOU ARE CHANGING JUST THE SPRINGS AND PLAN ON RE-USING THE FACTORY SHOCKS, PAY CLOSE ATTENTION, OTHERWISE SKIP TO THE NEXT STEP. If you notice on the bottom of the spring perch, there are metal tabs protruding on each end. This must be perfectly aligned with the top mount when you reassemble the suspension. This is where the thin masking tape comes in. Run the masking tape straight from one of the tabs to the bottom of the shock. Next, run the masking tape across the top of the mount so when you look straight down from the top, you will see a line going straight down all the way to the bottom.
Step 19: As with the rear suspension, compress the springs and remove the top bolt holding the assembly together.
Step 20: Reassemble everything making sure the align the top mount with the tabs on the bottom of the spring perch (masking tape). Torque specs: Bottom fork bolt - 47 ft. lbs, Top damper fork bolt - 32 ft. lbs., Top mount bolts - 37 ft. lbs, Strut brace bolts - 12 ft. lbs.


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