It's July, and were this a rightful world "Mad Men" would be gracing our televisions on Sunday nights. But it's not, and we'll have to wait until early 2012 for the return of my (and maybe your?) favorite show. But in the meantime, we can note with approval that "Mad Men" received 19 Emmy nominations this morning — more than any other series. This included acting nods for Jon Hamm, Elisabeth Moss, Christina Hendricks, John Slattery, Robert Morse and first-timers Cara Buono, who played Dr. Faye Miller, and Randee Heller, the truly awe-inspiring Miss Blankenship. (Let's pause for a moment of silence for the late, lamented Miss Blankenship, who will be making no further guest appearances.) "The Suitcase," one of the show's best episodes, was nominated in three different categories. So, what would Don Draper say to all of this?
Meanwhile, "Mildred Pierce" led the pack with 21 nominations (I have to say, beautiful as it was, I couldn't bring myself to watch the whole thing), and also scoring high were "Boardwalk Empire," "Modern Family," "Saturday Night Live," "Game of Thrones," and two more personal favorites of mine, "30 Rock" and "Downton Abbey." Even "The Killing" squeaked out five nominations, though to my mind they were the wrong ones: Why nominate Mireille Enos and not her rather more interesting partner, Joel Kinnaman? You can read the whole list here; should you wish.


text:
Andrea Temesvári
This article includes a list of references, related reading or external links, but its sources remain unclear because it lacks inline citations. Please help to improve this article by introducing more precise citations. (February 2016) (Learn how and when to remove this template message)
Andrea Temesvári (born 26 April 1966) is a former professional tennis player from Hungary. She won the Italian Open at age sixteen, but injuries would later hamper her career.
French Open 2011 Trophée des Légendes
(1966-04-26) 26 April 1966 (age 53)
Right-handed (two-handed backhand)
No. 7 (23 January 1984)
3R (1982, 1983, 1984, 1989)
No. 13 (21 December 1986)
Grand Slam Doubles results
W (1986)
QF (1985, 1989)
The native form of this personal name is Temesvári Andrea. This article uses Western name order when mentioning individuals.
PersonalEdit
Temesvári was born in Budapest, Hungary. She began playing tennis at age nine. She was coached by her father, Otto Temesvári, and Ferenc Polyak.
Temesvári joined the WTA Tour in 1981. She received the Most Improved Player Award by WTA Tour and TENNIS Magazine in 1982. She reached a high of World No. 7. in 1983. After several injuries, she made a comeback after dropping out of Top 25 for first time since 1983 in 1986. At the 1986 French Open she won the women's doubles title with Martina Navratilova.
She returned to the tour at start of 1989 after a 20-month layoff due to ankle and shoulder injuries. She had two operations on ankle in March and September 1987 and then arthroscopic surgery on right shoulder in April 1988. She played for the Hungarian Fed Cup Team from 1983 to 1986, 1989 to 1990, and 1992. She was also a member of the Hungarian Olympic Team in 1996. She retired in 1997. During her career she won a total of five singles titles and seven doubles titles.
Major finalsEdit
Grand Slam finalsEdit
Doubles: 1 (1 title, 0 runners-up)Edit
Winner 1986 French Open Clay
Gabriela Sabatini 6–1, 6–2
WTA career finalsEdit
Singles: 7 (5–2)Edit
Winner — Legend
Grand Slam tournaments (0–0)
WTA Tour Championships (0–0)
Tier I (0–0)
Tier II (0–0)
Tier III (0–0)
Tier IV (0–1)
Tier V (0–0)
Virginia Slims, Avon, Other (5–1)
Titles by Surface
Winner 1. 1 March 1982 Hershey Hard (I)
Catherine Tanvier 6–4, 6–2
Runner-up 1. 10 May 1982 Lugano Clay
Chris Evert-Lloyd 0–6, 3–6
Winner 2. 2 May 1983 Perugia Clay
Bonnie Gadusek 6–1, 6–0
Winner 3. 4 July 1983 Hittfeld Clay
Eva Pfaff 6–4, 6–2
Winner 4. 1 August 1983 Indianapolis Clay
Zina Garrison 6–2, 6–2
Winner 5. 22 July 1985 Indianapolis Clay
Zina Garrison 7–6(7–0), 6–3
Runner-up 2. 14 August 1989 Mahwah Hard
Steffi Graf 5–7, 2–6
Doubles: 10 (7–3)Edit
Winner 1. 29 October 1984 Zürich Carpet (I)
Andrea Leand
Claudia Kohde-Kilsch
Hana Mandlíková 6–1, 6–3
Hana Mandlíková
Helena Suková 6–4, 3–6, 7–5
Winner 3. 31 March 1986 Marco Island Clay
Elise Burgin 7–5, 6–2
Runner-up 1. 12 May 1986 Berlin Clay
Helena Suková 5–7, 2–6
Winner 4. 26 May 1986 French Open Clay
Winner 5. 17 April 1989 Tampa Clay
Brenda Schultz
Elise Burgin
Rosalyn Fairbank 7–6(8–6), 6–4
Runner-up 2. 9 April 1990 Amelia Island Clay
Regina Rajchrtová
Mercedes Paz
Arantxa Sánchez Vicario 6–7(5–7), 4–6
Winner 6. 17 May 1993 Strasbourg Clay
Shaun Stafford
Jill Hetherington
Kathy Rinaldi 6–7(5–7), 6–3, 6–4
Runner-up 3. 14 February 1994 Paris Carpet (I)
Mary Pierce
Sabine Appelmans
Laurence Courtois 4–6, 4–6
Winner 7. 24 July 1995 Maria Lankowitz Clay
Silvia Farina Elia
Alexandra Fusai
Wiltrud Probst 6–2, 6–2
Grand Slam singles performance timelineEdit
W F SF QF #R RR Q# A NH
(W) Won; (F) finalist; (SF) semifinalist; (QF) quarterfinalist; (#R) rounds 4, 3, 2, 1; (RR) round-robin stage; (Q#) qualification round; (A) absent; (NH) not held. SR=strike rate (events won/competed)
Career SR
Australian Open A A A 3R A NH A A 3R 2R A A 2R A A 1R A 0 / 5
French Open 1R 3R 4R 2R 1R 2R A A 2R 3R 2R A 1R A 1R 2R A 0 / 12
Wimbledon A 3R 3R 4R 2R A A A 1R 1R 1R A 1R A 2R A A 0 / 9
US Open A 3R 3R 3R 2R 2R A A 3R 1R 1R 1R A 1R 1R A A 0 / 11
SR 0 / 1 0 / 3 0 / 3 0 / 4 0 / 3 0 / 2 0 / 0 0 / 0 0 / 4 0 / 4 0 / 3 0 / 1 0 / 3 0 / 1 0 / 3 0 / 2 0 / 0 0 / 37
Year End Ranking 146 33 11 14 16 43 NR NR 43 116 157 71 153 132 90 181 942
Andrea Temesvári at the Women's Tennis Association
Andrea Temesvári at the International Tennis Federation
Andrea Temesvári at the Fed Cup
Pálma Balogh Hungarian Sportswoman of The Year
Mária Ábrahám
Sabina Simmonds WTA Most Improved Player
Retrieved from "https://en.wikipedia.org/w/index.php?title=Andrea_Temesvári&oldid=884996802"

redpajama_set_name: RedPajamaCommonCrawl


text:
The forgotten massacre
https://michaelfreund.org/9198/the-forgotten-massacre
This past week marked the 500th anniversary of one of the most horrific, and least remembered, massacres of Jews ever to have taken place on the streets of a major European capital. For three days beginning on April 19, 1506, a bloodthirsty mob goaded on by Dominican preachers roamed throughout Lisbon, the Portuguese capital, hunting down their victims and butchering them with unrestrained glee.
Their prey were the Cristaos Novos ("New Christians"), the thousands of Portuguese Jews who had been forcibly converted to Catholicism by order of King Manuel just a decade before. Some were beaten to death, others were beheaded. Many more were dragged through the streets and tossed alive into burning pyres that had been erected at the Rossio, Lisbon's main square. Anyone who looked Jewish, or was known to have had dealings with Jews, quickly found themselves a target of the murderous throng as well.
The orgy of violence reportedly began after one of the "New Christians" expressed doubt about a miracle that allegedly had taken place in a local church. He was immediately taken outside and butchered, along with his brother.
Then, according to a contemporary account written by Solomon Ibn Verga, a number of Dominican friars "went to the main avenue of the city and proclaimed: 'Anyone who kills the seed of Israel shall be granted one hundred days of absolution for the world to come!'"
The rabble took its cue, and proceeded to break into Jewish homes across the city and commit atrocities, which included tossing pregnant women out of windows onto spears held aloft by the crowd at ground level.
Aware of the mayhem taking place in the city, German, Dutch and French sailors based on ships in Lisbon's harbor are said to have come ashore - not in order to stop the bloodshed, but to join in on it instead.
All told, it is estimated that 2,000 to 4,000 Jews were slain in the massacre, underlining the hostility which they continued to face even after being compelled to abandon their faith and join the Church.
BUT DESPITE its ghastly nature, and the terrible toll it claimed in life and limb, the Lisbon massacre has been all but forgotten by much of the Jewish world, with few even aware that it took place.
Sure, prominent historians such as Heinrich Graetz and Meyer Kayserling wrote about it, as has Columbia University's Yosef Haim Yerushalmi. But outside of academic circles, the entire incident has been all but overlooked.
And while members of Lisbon's Jewish community held a small memorial ceremony last week, virtually nothing was done outside of Portugal to recall this dark moment in our people's history.
So the question remains: why has the Lisbon massacre, whose ferocity foreshadowed subsequent anti-Jewish carnage in Europe, been so thoroughly overlooked? And, no less crucial, does it really matter?
Of course, for a people who have experienced so much horror in the intervening centuries, it is only somewhat natural that our collective memory has grown dimmer with each additional blow that we suffered. To commemorate every massacre and pogrom, every expulsion and blood libel, would fill the calendar to overflowing with dates of sadness and despair.
Moreover, the proximity of the Holocaust, its unparalleled uniqueness, and the vast devastation that it wrought, clearly overshadow all that came before it.
Nonetheless, I don't think that excuses us from our responsibility to bear witness to our people's past. If we allow events such as the Lisbon massacre to fade into obscurity, we will be committing an unforgivable act of historical injustice, not only to those who were killed, but also to ourselves.
It is precisely by keeping alive the memory of these events that we gain a better understanding of our place both in the past and the present, as well as in the future. If we disregard that which came before us, we ultimately deny ourselves the opportunity to learn from history and to absorb its lessons.
In Zakhor, his classic work on Jewish history and Jewish memory, Yosef Haim Yerushalmi writes that, "hardly any Jew today is without some Jewish past. Total amnesia is still relatively rare. The choice for Jews, as for non-Jews, is not whether or not to have a past, but rather - what kind of past shall one have."
I for one choose to remember.
The writer is chairman of Shavei Israel, a Jerusalem-based group which assists "lost Jews" seeking to return to the Jewish people. www.shavei.org


(National Sentinel) Respectful: Former Republican senator from Kansas and presidential nominee Bob Dole, who is 94 and bound to a wheelchair, sent the NFL a not-so-subtle message on Wednesday when he was honored on Capitol Hill.
Dole, who is also a U.S. Army World War II veteran, was wounded so badly by German machine gun fire in 1945 he permanently lost the use of his right arm. Nevertheless, after a slow and painful recovery, he went to law school and spent more than four decades in politics, rising to the position of Senate Minority and Senate Majority Leader.
The long-serving senator received the Congressional Gold Medal in a ceremony that included Republican and Democratic leaders, as well as President Donald J. Trump and Vice President Mike Pence.
The former Kansas Senator was also honored for being particularly instrumental in the commissioning of the World War II Veterans Memorial.
Though he can no longer walk and remained in his wheelchair for the majority of the ceremony, when the Color Guard walked in hoisting the American flag and the flags of the military services, Dole was seen on camera waiving for an aide.
A young man responded and then helped Dole stand so that he could properly honor the American flag.
"In an America where standing for the national anthem is a controversial act, Bob Dole should be an example to us all," The Daily Caller reported.
NBC is broadcasting this year's Super Bowl. Executives said they planned to show any kneeling, protesting players during the broadcast.


Music Theme Park: Watch: Eric Clapton inducts The Band into the Rock & Roll Hall of Fame in 1994.
Watch: Eric Clapton inducts The Band into the Rock & Roll Hall of Fame in 1994.
Eric Clapton inducts The Band into the Rock & Roll Hall of Fame in 1994.


Excellent low noise miniature electret mic. A lower cost alternative to the DPA4060, with almost the same noise level, though max SPL is specified as 120dB.
Note HF peak of 4dB@15kHz (less than Beyer show in their graphs and of little consequence).
Noise levels shown are not true (power amp noise). MCE60 measured -62dB ie 38dB SPL 468-wtd. This is in line with the specified figure of 26dB SPL A-wtd.
Blue plot is Lindos MM3 reference, Red is MCE60.
Alignment level is 100dBSPL approx.


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When it's time to place your order for an octagon picnic table, our representatives are always available by phone or online to chat with you and help you select the equipment that is right for you. Get a free quote now to get started!


Excellent THREE DOUBLE BEDROOM furnished second floor flat, located on Moulsecoomb Way and within easy reach of Lewes Road and both Brighton & Sussex universities.
The door to the flat opens in to the entrance hallway which all the rooms run off. As you walk in on your left you will find 2 bedrooms and on your right you will find the kitchen and the bathroom. Also on your right you will find the 3rd and final bedroom which has the added benefit of having direct access to the balcony.
Please quote the property reference 6704584 when enquiring.


As if a workshop and a short talk wasn't enough, I also decided to submit a poster to LILAC 2017! The poster looked at the Supporting Researchers in the 21st Century programme at Cambridge which aims to upskill library staff in the area of scholarly communication. We are very much hoping to offer this training to a wider audience in some form so keep your eyes open!
In the meantime my poster can be found below and further details of the programme are available here.


f you are passionate about computer technology and eager to develop a career in technology sales, Dell is the place to be. Within our Commercial Sales Team, we are looking for an Account Executive to work as part of a team based in Jordan .With more than 100,000 team members globally, Dell promotes an environment that is rooted in the entrepreneurial spirit in which the company was founded.As we continue to grow our business in EMEA we are looking for sales people with a proven track record who are passionate about technology.You will be joining a collaborative and energetic team that welcomes creativity and different perspectives. In return Dell offers the training, development and support for you to develop your career and fulfil your ambitions and potential.
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text:
Q: Simulink math operations on 2 bus signals I need to make a Simulink block which receives a concatenation of a number of bus signals and performs the same math operations on the signals contained in the bus for each pair of consequent buses. The bus signals are of the same type and are non-virtual.
For the sake of the question, let's assume to have a concatenation of 4 simple buses, each containing a x and a y field. A bus of signals composed of a=x1+x2 and b=y1-y2 need to be made out of buses inputs 1,2 and 3,4. So, the output of the block should be a concatenation of 2 buses, the first containing information from the first pair of input buses, and the second one from the second pair.
An hard-to-scale way to do it is the following.

Are there any built-in Buses Math operations possibilities, or better ways to implement this? I could not find anything in Mathworks documentation, and simple operations block generate incompatibility errors.

A: You need to use For Each Subsystem Block. As shown in this example. Note that I called the bus BusTest and made the dimension and datatype of signals visible:

Now set the Signal Width parameter of that block to two so it divides input array into chunks of length 2:

Then move your logic into that block:

redpajama_set_name: RedPajamaStackExchange


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text:
\section{INTRODUCTION}

Globular Clusters (GCs) are the most populous, old and dense stellar aggregates in the Galaxy.
They are formed by millions of stars, whose age, distance and chemical composition can be
determined with great accuracy. For this reason GCs
play a crucial role in the current understanding
of stellar and dynamical evolution and they represent the ideal target
to constrain the interplay between the ``environment'' and the evolution of stars.

The average age of Galactic GCs (GGCs; $<t>\sim 12$ Gyr) is typically significantly larger
than the time-scales in which the internal dynamical processes occur (Meylan \& Heggie 1997).
During their evolution, GCs can survive the early expansion
triggered by primordial gas expulsion and mass loss due to stellar evolution, then
their evolution is mainly driven by two-body relaxation
thus reaching higher central
concentrations and eventually the core collapse, while loosing stars through the boundary set by
the tidal field of their host galaxy
(see for example Heggie \& Hut 2003).

Two-body relaxation drives the long-term dynamical evolution of GCs.
Because of this physical process, heavier objects tend to sink toward the
cluster centers (mass segregation), while less massive stars are forced towards more
external orbits.
The typical time-scale in which two-body relaxation occurs scales
with the number of stars (Spitzer 1987) and it is typically of the order of 1-2 Gyr in GCs (Meylan \& Heggie 1997).
The internal dynamics of stellar aggregates affect objects of any mass and it can be efficiently
probed by means of massive
test particles, like Blue Straggler Stars (BSSs), binaries and Millisecond Pulsars (e.g. Ferraro et al. 2001, 2003).
Among them, BSSs
have been successfully used for this purpose, since they are numerous and relatively easy to measure.
Indeed, Ferraro et al. (2012) have shown that the BSS radial distribution can be
efficiently used to rank clusters according to their dynamical age.
Using this approach, evidence of mass segregation has been observed in all GCs studied so far,
with only very few exceptions: $\omega$ Centauri, NGC~2419, Palomar~14, Terzan~8 and Arp~2,
where the BSS radial distribution has been found to be indistinguishable from that of any
other population
(Ferraro et al. 2006; Dalessandro et al. 2008b; Beccari et al. 2011; Salinas et al. 2012).
In general, for clusters that haven't reached relaxation yet, the radial distribution of stars of any mass is
expected to be the same (apart from possible primordial dissimilarities).
The lack of mass segregation in NGC~2419 has been confirmed by Bellazzini et al. (2012)
studying the the radial variation of the luminosity function (LF) of Main Sequence (MS) stars
at different radii\footnote{The same result has been obtained by Baumgardt et al. (2009) who performed
detailed comparison between velocity dispersion
profiles and theoretical models.}, while it has been questioned for Palomar~14 by Frank et al. (2014) who observed
an increase of the slope of the stellar mass function for increasing distance from the cluster center,
as expected for relaxed systems.

As a part of a large observational campaign aimed at deriving the binary fraction in the external regions
of GGCs,
we present results about the dynamical state of the low mass ($M_V=-6.94$; Harris 1996- 2010 edition)
GC NGC~6101. This is an old ($t\sim 13$ Gyr, Dotter et al. 2010), metal poor ($[Fe/H]=-1.98$; Carretta et al. 2009)
Galactic halo GC, with a low concentration ($c=0.80$; Harris 1996).
A recent analysis of its RRLyrae content (Cohen et al. 2011) revealed that NGC~6101 is an Oosterhoff type II
cluster. This is consistent with the metallicity of the cluster, but it is  unusual
for its kinematical properties. In fact NGC~6101 is one of the very few metal-poor GCs in
the Galaxy  with a retrograde motion. Because of its peculiar kinematical properties it has been possibly
connected
(Martin et al. 2004) to the Canis Major dwarf galaxy.
The stellar content of NGC~6101 has been studied by
Sarajedini \& Da Costa (1991) and later on by Marconi et al. (2001; hereafter M01).
In particular M01
performed a detailed analysis of the radial distributions of different stellar populations of NGC~6101.
They found that Horizontal Branch (HB) stars and BSS are more centrally concentrated than MS-Turn Off
stars. They interpreted
this behavior as evidence of mass segregation among different populations.

In this study  we investigate the dynamical state of NGC~6101 by using three diagnostics:
the radial distribution of {\it (i)}  BSSs, {\it (ii)} MS binaries,
and {\it (iii)} genuine MS stars with different masses.
According to these three indicators, and at odds with the results of M01, we find that NGC~6101 does not show
evidence of mass segregation.
We compare
this observational fact with theoretical expectations and the new dynamical
timescale estimates obtained from the newly derived structural parameters.

The paper is structured as follows: in Section~2 we present the details of our observations and the adopted data
reduction procedures; in Section~3 we derive the main structural parameters of the cluster; in Section~4 the BSS
radial distribution is analyzed and compared to that of the reference populations; in Section~5 we study the binary
content of NGC~6101 at different distances from the center and in Section~6 we analyze the radial variations
of the luminosity and mass function of MS stars. The main results of the paper are summarized and discussed in
Section~7.

\section{OBSERVATIONS AND DATA ANALYSIS}

The data set used in this paper consists of a combination of images obtained
with both the Hubble Space Telescope (HST) and ground based facilities (see Figure~1).

For the analysis of the BSS radial distribution (see Section~4), we used two publicly available catalogs.
The first is the HST Advanced Camera for Survey/Wide Field Camera (ACS/WFC) catalog
published by Sarajedini et al. (2007; see also Anderson et al. 2008) in the context of
the ``ACS Survey of Galactic Globular Clusters''.
This catalog samples the innermost $\sim120\arcsec$ of the cluster.
We will refer to this sample as the {\it ACS} data set. The $(V, V-I)$ color magnitude diagram (CMD)
obtained by using the Johnson-Cousin $V_{\rm ground}$ and $I_{\rm ground}$ magnitudes, is shown in Figure~2.
The second public data set used in this work consists of the B, V and I catalog published and
fully described by M01 and obtained with the 1.54 mt
Danish telescope at ESO/La Silla. In the following we will refer to this sample as the
{\it Danish} sample. The corresponding CMD is shown in Figure~3.

The binary fraction analysis (Section~5) has been performed by using deep $V_{\rm HIGH}$ and
$I_{\rm BESSEL}$  images obtained with the
the FOcal Reducer/low dispersion Spectrograph 2 (FORS2) at the Very Large Telescope (Prop ID: 091.D-0562; PI: Dalessandro).
The $2k\times4k$ pixels MIT Red- optimized CCD mosaic in the standard resolution mode
($\sim0.25\arcsec pixel^{-1}$) was adopted for these observations,
thus to sample the largest possible field of view (FOV; $\sim 6.8\arcmin \times 6.8\arcmin$).
Three pointings complementary to the {\it ACS} sample have been set up (see Figure~1) starting from $r\sim150\arcsec$
(and reaching $r\sim750\arcsec$) from the center of the cluster.
For each pointing, eight images in the
$I_{\rm BESSEL}$ band with exposure time $t_{\rm exp}=240$ sec each and four in $V_{\rm HIGH}$
with $t_{\rm exp}=510$ sec, have been obtained. A dither pattern of few arcsec has been adopted
to allow a better reconstruction of the Point Spread Function (PSF) and avoid CCD blemishes and artifacts.
Master bias and flat-fields have been obtained by using a large number of calibration frames.
Scientific images have been corrected for bias and flat-field by using
standard procedures and tasks contained in the Image Reduction and Analysis Facility
(IRAF)\footnote{Astronomy Observatory,
which is operated by the Association of Universities fro Research in Astronomy, Inc., under the cooperative
agreement with the National Science Foundation.}.
The photometric analysis has been performed independently for each image
and chip (see for example Dalessandro et al. 2014) by using \texttt{DAOPHOT{\sc II}} (Stetson 1987).
For each frame we selected several tens of bright, not saturated and relatively isolated stars to model the PSF,
which turned out to be well reproduced by a Moffat function (Moffat 1969).
The parameters ($\sigma$, $\beta$) describing the PSF model have been allowed to vary
with a third order polynomial as a function of the instrumental coordinates $(x,y)$ within the frame.
For each chip, the best PSF model was then applied to all sources at $2\sigma$ above the
background by using \texttt{DAOPHOT{\sc II}/ALLSTAR}. We then created a master list of stars composed by sources
detected in at least four frames. In the single frames, at the corresponding positions of the stars present
in the master-list,
a fit was forced with \texttt{DAOPHOT{\sc II}/ALLFRAME}.
For each star different magnitude estimates in each filter were homogenized and their weighted mean and standard
deviation were finally adopted as star magnitude and photometric error (see for example Ferraro et al. 1991, 1992).
We used the stars in common with the Stetson photometric secondary standard catalog (Stetson 2000) to report
the instrumental magnitudes to the $V$ and $I$ Johnson bands.
Instrumental coordinates (x, y) have been reported to the absolute ($\alpha$, $\delta$) system by using
the stars in common with the GSC2.3 catalog and the cross-correlation tool \texttt{CataXcorr}\footnote{CataXcorr is
a code aimed at cross-correlating catalogs and finding solutions, developed by P. Montegriffo at INAF -
Osservatorio Astronomico di Bologna, and successfully used by our group for the past 10 years.}.
At this stage the catalogs obtained for each chip are on the same photometric and astrometric system.
They have been combined to form a single catalog that we defined {\it FORS2} sample.
Stars in common between different pointings have been used
to check for the presence of residuals in the calibration procedure.

Both the {\it FORS2} and the {\it ACS} catalogs have been corrected for differential reddening
using the approach described by Milone et al. (2012). We recall the reader to this paper for details on the procedure.
For each star, we used the 50 closest neighbors to compute the corresponding average differential color excess
$\delta[E(B-V)]$. We adopted extinction coefficients from Cardelli et al. (1989). Over the FOV covered
by the three pointings, the total variation of $E(B-V)$ amounts to only 0.06 mag.
The resulting $(V, V-I)$ CMDs are shown in Figure~2.

Since the {\it FORS2} data set saturates at $V\sim18$ and does not provide a complete area coverage (see Figure~1),
we complemented it with images obtained with the Wide Field Imager (WFI) mounted at the MPG/ESO 2.2 m telescope to
homogeneously analyze the density profile of NGC~6101 (Section~3).
We used six long exposure images: three in the
$B_{\rm NEW}$ band with $t_{\rm exp}=120$ sec (Prop ID: 069.D-0582, PI: Ortolani) and three in $V/89_{ESO843}$
with $t_{\rm exp}=60$ sec (Prop ID: 068.D-0265, PI: Ortolani). Both the pre-reduction and the photometric analysis have
been performed as described above for the {\it FORS2} data set. Also the instrumental magnitudes have
been reported to the Johnson
system by using the stars in common with the catalog by Stetson (2000). A color equation was adopted
to calibrate the $B_{\rm NEW}$ band, while a zeropoint was enough for the $V/89_{ESO843}$ band.
Instrumental coordinates have been reported to the absolute system for each of the eight WFI chips using the stars
in common with GSC2.3,
as done before. The resulting $(V, B-V)$ CMD is shown in the right panel of Figure~3.

We emphasize that for all catalogs, the magnitudes are in the Johnson-Cousin photometric system.
To avoid confusion, in the following we will refer to them as $``B''$, $``V''$ and $``I''$.

\section{DENSITY PROFILE AND CLUSTER PARAMETERS}

We used the {\it ACS} and {\it WFI} data sets to compute the density profile of NGC~6101 from direct star counts.
In particular, the sample is composed of all stars in the {\it ACS} catalog and
those in the complementary {\it WFI} data-set.
We used stars with $13.5\leq V\leq 19.5$ to avoid incompleteness and saturation problems.
As done in other works (see for example Dalessandro et al. 2013a), we divided the FOV in 17 concentric annuli
(five of them are in the {\it ACS} FOV)
centered on the center of gravity (C$_{grav}$), which we have adopted to be the one reported by Goldsbury at al.
(2010; $R.A.=16^h:25^m:48^s.12$, $Dec.=-72^{\circ}:12\arcmin:07\arcsec.9$).
Each annulus has been then split in an adequate number of sub-sectors (ranging from two to four)
according to the local density of stars and the angular coverage in the {\it WFI} FOV.
Number counts have been calculated in each subsector and the corresponding densities were obtained dividing them by the
sampled area. Particular attention has been paid to incomplete area coverage of the {\it WFI} data set starting from
$r\sim1000\arcsec$ and to the inter-chip gaps.
The stellar density of each annulus was then defined as the average of the subsector densities, and its standard
deviation was computed from the variance among the subsectors.
We made sure to guarantee some radial overlap between the two samples in order to homogenize the two portions of the
density profile.
The resulting surface density profile is shown in Figure~4.
We estimated the contribution of the Galactic field background by averaging the densities of the five outermost measures,
corresponding to $r>400\arcsec$. We obtain an average background density of $\log(\rho_{\rm bck})\sim-2.7$ stars
arcsec$^{-2}$. We have verified that the observed background density is fully consistent with that obtained
by using the Besancon Galaxy model simulation (Robin et
al. 2003) covering an area of $1^{\circ}\times 1^{\circ}$ centered on the position of NGC~6101 and for stars in the same
magnitude limit used to build the density profile. This density has been subtracted to the observed density profile to obtain a ``decontaminated"
density distribution (solid symbols in Figure~4).
As apparent from the figure, the background in the external regions of NGC~6101 does not appear
to be constant at odds with what expected, but it mildly increases as a function of the distance.
This behavior introduces some uncertainties
on the background density estimate. However we have checked that variations of the
background density within intervals compatible with the observations do not affect significantly
the density distribution.

We fit the radial density profile by using an isotropic single-mass King model (King 1966) following
the procedure fully
described in Miocchi et al. (2013). The model best-fitting the observed density profile has a concentration
$c=1.3^{+0.15} _{-0.16}$ and core radius $r_c=61.3\arcsec ^{+6.9} _{-5.4}$, which yield a tidal radius
$r_t=1200\arcsec ^{+390} _{-250}$. We also derive the projected half light radius (effective radius)
$r_h=128.2\arcsec ^{+16} _{-7.6}$.
The newly determined structural parameters are in partial disagreement with those found in
the literature and they make NGC~6101 more concentrated and extended than previously thought.
In particular, $r_c$ is compatible within the errors with the one listed by Harris
(1996, $r_c=58.5\arcsec$), while the values of $c$
(and as a consequence $r_t$) and $r_h$ are much larger than in Harris (1996; $c=0.80$ and $r_h=63\arcsec$).
The same result comes out also from the comparison with the values obtained by McLaughlin \& van der Marel (2005),
who quote $c=0.60$, $r_c=59.2\arcsec$ and $r_h=63.6\arcsec$.
We argue that the difference between our parameters and the literature is mainly due to the fact
that both Harris
(1996) and McLaughlin \& van der Marel (2005) made use of non homogeneous surface brightness profiles that are limited
to the innermost $\sim100\arcsec$ from the center not allowing for an appropriate background subtraction.

We have estimated the distance modulus and reddening of NGC~6101 by comparing its CMD to that
of M~30 (NGC~7099). M~30 can be used as a template for this analysis since it has a similar metallicity
($[Fe/H]=-2.33\pm0.2$; Carretta et al. 2009) and its distance has been
robustly determined because of its proximity.
To guarantee homogeneity, we compared the {\it ACS} sample of NGC~6101 with the CMD of M~30 obtained with the same
instrument within the same survey (Sarajedini et al. 2007).

We reported the CMD of M~30 in the absolute plane $M_V, (V-I)_0$ by adopting as distance modulus $(m-M)=14.80$ and reddening
$E(B-V)=0.03$ (Ferraro et al. 2009).
To overlap the CMDs and align all the main evolutionary sequences in the absolute plane (see Figure~5),
we needed to adopt $(m-M)_V=16.20\pm0.10$ and reddening $E(B-V)=0.12\pm0.02$ for NGC~6101, which yield to a true
(unreddened) distance modulus $(m-M)_0=15.83\pm0.12$ and thus to a distance $d=14.6\pm0.8$ Kpc.
We used these values throughout the paper.

These values are slightly larger than those obtained in the literature, but in most cases they are still compatible within the
errors. In particular, Harris (1996) report $(m-M)_V=16.07\pm0.1$ and $E(B-V)=0.05$,
Sarajedini \& Da Costa (1991) found
$(m-M)_V=16.12\pm0.1$ and $E(B-V)=0.06$, M01 obtained $(m-M)_V=16.12\pm0.03$ $E(B-V)=0.1$, while Cohen et al. (2011)
estimated $(m-M)_V=16.00\pm0.03$ $E(B-V)=0.1$
from the average luminosity of RRLyrae stars and ZAHB fit.

\section{THE BSS RADIAL DISTRIBUTION}

BSSs in GCs are commonly defined as those stars located along an extrapolation of the MS,
in a region brighter and bluer than the Turn-Off (TO) point in the optical CMD (Sandage 1962).
Their location suggests that they are more massive than the current cluster population (see for example Ferraro et al.
2006; Lanzoni et al. 2007a).
Indeed observational evidence
(Shara et al. 1997; Gilliland et al. 1998; Fiorentino et al. 2014) showed that BSSs have masses
of $M\sim 1.2 - 2.0 M_{\odot}$ compared to a mass of $\sim0.8 M_{\odot}$ for stars at the MS-TO of an old stellar system.

Because of their mass, BSSs are heavily affected by dynamical friction and thus they can be used as natural
test particles to probe the internal dynamics of stellar aggregates. In particular, their radial distribution has been
found to probe the efficiency of dynamical friction (Mapelli et al. 2006; Alessandrini et al. 2014; Miocchi et
al. 2015).
Ferraro et al. (2012) suggested that the BSS radial distribution can be used to define the so called {\it dynamical clock}
which is a powerful indicator of the cluster
dynamical age. In this picture GCs with a flat BSS radial distribution
are dynamically young stellar systems and they are defined as {\it Family I} GCs, clusters with a
bimodal radial distribution have intermediate dynamical ages ({\it Family II}), while
those with a centrally peaked and
monotonically decreasing BSS distribution are dynamically old ({\it Family III}).

The BSS population of NGC~6101 has been studied by Sarajedini \& Da Costa (1991) and M01.
In particular M01 studied also the BSS radial distribution by using a combination of HST Wide Field Planetary Camera 2
(defined {\it ``hst'' sample}) and ground based data ({\it ``ground'' sample})
corresponding to the {\it Danish} sample defined in Section~2.
By using cumulative radial distributions and Kolmogorov-Smirnov tests,
they concluded that BSSs have a large probability (84$\%$) to have
been extracted from the same parent population as HB, while HB and Tip RGB stars being more
centrally concentrated than MS-TO stars. They interpreted these results as evidence of mass segregation.

\subsection{Population selections}

We studied the BSS population of NGC~6101 by using the {\it ACS} and {\it Danish} data sets.
In detail, the final sample consists of stars in the {\it ACS} catalog and those present in the
{\it Danish} data set and complementary to the {\it ACS} FOV (see Figure~1).
In this way the central region of NGC~6101
is homogeneously covered up to a distance $r\sim250\arcsec$ (corresponding to about $4\times r_c$) from
$C_{grav}$.
While the {\it WFI} data set
covers a larger FOV and ensures a complete sampling of the cluster up to $r_t$, we preferred this combination of
catalogs for the BSS analysis because of the better photometric quality of the data (see Figures~2 and 3).

As done in previous works (see for example Ferraro et al. 1997, 2004; Lanzoni et al. 2007a,b;
Dalessandro et al. 2008a and reference therein),
in order to study the BSS radial distribution, we need a homogeneous selection of BSSs
and at least one reference stellar population. For the case of NGC~6101 we selected HB, RGB and MS-TO
stars as reference.

BSSs have been selected following the definition of stars bluer and brighter than TO.
The selection box shown in Figure~6 follows the well defined BSS sequence brighter than $V=20$. An additional
constraint on the color ($(V-I)<0.5$) has been adopted to avoid contamination and blends from MS and SGB stars.
In this way we selected 52 BSSs, 33 in the {\it ACS} FOV and 19 in the complementary {\it Danish} sample.
Because of the more conservative selection criteria adopted in this work, the BSS sample is smaller
than the one obtained by M01, who identified 73 BSS adopting different magnitude and color selections.
As for the reference populations, we selected RGB stars along the RGB and having $13.5<V<18.7$.
With these limits we selected a total of 510 RGB
stars, 328 in the {\it ACS} sample and 182 in the {\it Danish} one.
We selected HB stars following their well defined sequence for $(V-I)<0.5$ to minimize the impact
of field contamination. In fact, as apparent from Figure~6, the Galactic field describes a vertical sequence
in the color range $0.7<(V-I)<0.9$. The HB selection box is shown in Figure~6 and encloses 137 stars.
By using the list of known RRlyrae stars (Liller 1981; Cohen et al. 2011; Fitzgerald et al. 2012),
we identified 11 stars in common, seven in the {\it ACS} and four in the {\it Danish} FOVs.
The RRLyrae falling outside the HB selection were added to the HB sample.
In this way we count 102 and 42 HB stars in the {\it ACS} and {\it Danish} samples respectively.
In order to provide a direct comparison with M01, we used also MS-TO stars as additional reference population.
They have been selected approximately within the limits $0.65<(V-I)<0.80$ and $20.2<V<20.9$.
It is worth noting that in this magnitude range, MS stars have a completeness of $100\%$
both in the {\it ACS} (see Section~5.1) and in the complementary data-set (M01).
We count 3125 MS-TO stars in total, 2375 in the {\it ACS} and 750 in the complementary {\it Danish} FOVs.

We obtained an estimate of the Galaxy field contamination by using the Besancon Galaxy
model simulation (see Section~3). We counted the number of stars lying in the adopted $(V, V-I)$ selection boxes.
We find 125 and 455 Galactic field MS-TO and RGB stars respectively, yielding densities
$\rho_{bck} ^{MS}\sim 1\times 10^{-4}$ stars arcsec$^{-2}$ and $\rho_{bck} ^{RGB}\sim 3.5\times 10^{-4}$ stars arcsec$^{-2}$.
We don't find any field star falling in the boxes adopted to select HB and BSS stars.

\subsection{Radial distributions}

We first compared the BSS cumulative radial distribution to
those of the reference populations. As done in Dalessandro et al. (2013b), we took into account the effect of
Galactic field contamination by statistically decontaminating the RGB and MS populations. We divided the FOV into
four concentric annuli centered on $C_{grav}$ and for each of them we randomly subtracted
a number of stars corresponding to the average field densities quoted above.
The decontaminated cumulative radial distributions are shown in Figure~7.
As apparent, the four populations show very similar behaviors.
Indeed when a KS test is applied, we obtain probabilities $P_{\rm BSS/RGB}\sim18\%$, $P_{\rm BSS/HB}\sim20\%$
and $P_{\rm BSS/MS}\sim 65\%$ that they are extracted from a different parent population.
Since they are well below the canonical probability limit of $95\%$, we can conclude that in all cases
the differences in the observed radial distributions are not significant. Also, we obtain that the radial distributions of
the parent populations (HB, RGB and MS) are consistent with all being extracted from the same parent distribution.
These results are in good agreement with what found by M01 as far as the analysis is limited to HB, RGB and BSS stars,
while a different behavior is observed for MS stars.
In fact, M01 found the BSS population to be significantly more centrally segregated than MS stars.
In order to compare more accurately our results with M01,
we used also their {\it ``hst'' sample} and selected stellar populations using the same boxes defined above.
Also in this case, we do not find any significant difference among the radial distribution of RGB, HB and BSS
and that of MS stars.

We also analyzed the radial distribution of the specific frequencies $N_{\rm BSS}/N_{\rm RGB}$,
$N_{\rm BSS}/N_{\rm HB}$ and $N_{\rm BSS}/N_{\rm MS}$, where $N_{\rm POP}$ is the number of stars in the corresponding
population. We divided the FOV into four concentric annuli
centered on $C_{grav}$ and in each of them we counted the number of BSS and that of the reference population stars.
Galaxy field contamination has been accounted as described above.
The radial distributions of the specific frequencies are shown in Figure~8. In all cases, and in agreement with what
observed from the cumulative radial distributions,  we find that these ratios are almost constant over
the entire extension of the {\it ACS} + {\it Danish} FOV ($r<250\arcsec$).

We computed also the double normalized ratio ($R_{\rm POP}$\footnote{$R_{\rm POP}=(N_{\rm POP}/N_{\rm POP}^{\rm tot})/(L^{\rm
samp}/L^{\rm samp}_{tot})$, where POP = RGB and BSS. $L^{\rm samp}$ is the luminosity sampled in each annulus and estimated by using
the best-fit King model, distance modulus and reddening derived in Section~3, $L^{\rm samp}_{tot}$ is instead
the luminosity sampled in the entire field of view.}; Ferraro et al. 1993) for BSS and RGB stars.
In particular, for the same annuli used before, we estimated the sampled luminosity using the best-fit King model
discussed in Section~3, a distance modulus $(m-M)_{\rm V}=16.20 \pm 0.1$ and reddening
$E(B-V)=0.12$. We find that the $R_{\rm POP}$ is constant for both RGB stars and BSSs
as expected for any post-MS population (Renzini \& Fusi Pecci 1988).
The same result is obtained when HB and MS stars are considered.

Although this analysis does not cover the entire extension of NGC~6101 (it is limited to $\sim2 r_h$),
we note that the considered data-sets sample about
the $70\%$ of the total luminosity of the cluster. On the basis of what observed
in tens of GCs (Ferraro et al. 2012), we do not expect any significant deviation
from the general behavior at larger distances.
Therefore we can safely conclude that the BSS radial distribution of NGC~6101 is flat (i.e., indistinguishable from that of the
reference populations). Such a distribution
is not common for GCs and it has been observed only in few other cases so far ($\omega$
Centauri - Ferraro et al. 2006; NGC~2419 - Dalessandro et al. 2008b; Palomar~14 - Beccari et al. 2011; Ter~8 and Arp~2
- Salinas et al. 2012).
As for those GCs, a flat BSS radial distribution is a strong indication of the absence of
mass segregation in NGC~6101.

\section{THE BINARY FRACTION RADIAL DISTRIBUTION}

The fraction of binaries is an essential component of the formation and evolutionary processes of stellar systems.
In dynamically active aggregates as GCs, binaries are thought to promote the formation of
exotic objects like BSSs, X-ray sources and Millisecond Pulsars (see e.g. Mc Crea et al. 1964,
Paresce et al. 1992; Ferraro et al. 2006b, 2009; Heinke et al. 2003; Pooley \& Hut 2006; Xin et al. 2015).
Binaries are typically more massive than the average single star mass in GCs ($<m>\sim0.3 M_{\odot}$),
therefore they tend to sink towards the center of GCs
because of dynamical friction. As a consequence, also their radial distribution can be an useful tool to constrain the
dynamical state of GCs.

Up to now, three main techniques have been used to measure the binary fraction:
{\it (i)} radial velocity variability (e.g. Mathieu \& Geller 2009), {\it (ii)} search for eclipsing binaries
(e.g. Mateo 1996; Cote et al. 1996), and {\it (iii)} studies of the distribution of stars along the cluster MS in CMDs
(Romani \& Weinberg 1991; Bellazzini et al. 2002).
In this paper we used the latter approach by following the method described by Bellazzini et al. (2002;
see also Sollima et al. 2007; Dalessandro et al. 2011; Beccari et al. 2013).
The basic idea is that the magnitude of the binary system corresponds
to the luminosity of the primary star (more massive) increased by that of the companion.
Stars on the MS obey a mass-luminosity relation, hence the luminosity of the binary system is a function of the
mass ratio $q=m_2/m_1$ of the two components (where $m_1$ and $m_2$ are the masses of the primary and secondary, respectively).
Since $q$ can assume any value between $0$ and $1$, in CMDs binaries describe a ``secondary MS'' in the CMD, i.e. they generate
a broadening of the single stars MS, toward higher luminosities.

The binary fraction ($\xi$) of the central regions of NGC~6101 has been estimated by Sollima et al.
(2007) and  Milone et al. (2012).
In this work, we recomputed the central binary fraction by using the {\it ACS} sample for homogeneity,
and we extended the analysis to the cluster peripheries by using the {\it FORS2} data set.

\subsection{Artificial stars experiment and Galaxy contamination.}

In order to estimate the binary fraction by analyzing the ``secondary MS'', a number of spurious effects should be considered.
First, the Galactic field contamination should be properly taken into account.
Then, a robust measures of source of broadening, like blending and photometric errors, should be considered.
These factors are related to the quality of the data and can be properly studied through artificial stars experiments.

For the {\it ACS} sample, we used the artificial star catalog provided with the real stars catalog and available at the
``ACS Survey of Galactic Globular Clusters'' web page\footnote{http://www.astro.ufl.edu/$\sim$ata/public
$\textunderscore$hstgc/}. For the {\it FORS2} sample
we performed a large number of artificial stars experiments. We followed
the method described by Bellazzini et al. (2002; see also Dalessandro et al. 2011).
We generated a catalog of simulated stars with an I-band input magnitude ($I_{\rm in}$) magnitude extracted from a
LF modeled to reproduce the
observed luminosity function (LF) in that band and extrapolated beyond the limiting magnitude. Then to each star
extracted from the LF we assigned a $V_{\rm in}$ magnitude by means of an interpolation along the mean ridge line of the
cluster.

Artificial stars were added to real images by using the \texttt{DAOPHOT{\sc II}/ADDSTAR} software. In order to avoid
``artificial crowding'', stars were placed into the images following a regular grid composed by $35\times35$ pixels
cells
(corresponding approximately to 8-9 times the usual FWHM of stars for these images) in which only one artificial star for
each run was allowed to lie.  More than 250,000 stars have been simulated for the entire FOV covered by the {\it FORS2} sample.
The photometric reduction process used for the artificial star experiments is exactly the same as described in
Section~2. Those stars recovered after the photometric analysis have also values of $V_{\rm out}$
and $I_{\rm out}$.
As already noticed in Dalessandro et al. (2011; see also Milone et al. 2012), the MSs of the artificial stars
CMDs are narrower than
the observed ones. One possible reason for this effect, is that the formal photometric errors of the artificial-star catalogs
systematically underestimate the true observational uncertanties. Another possibility is that the broadening of the
observed data is due to some physical effects, as the presence of multiple populations along the MS.
Irrespective of the origin and as done in Dalessandro et al. (2011) we increased the formal artificial-star catalog errors thus to
reproduce the observed error distribution as a function of magnitude.
The curves of photometric completeness ($C$), defined as the ratio between the number of stars recovered at the
end of the procedure and the total number of stars actually simulated, are shown in Figure~9 for different radial bins.

For a proper measurement of the binary fraction we performed a detailed study of the field contamination,
using the same
Besancon Galaxy model catalog described in Section~4.

\subsection{The binary fractions}

The high photometric quality and the spatial coverage provided by the combination of the {\it ACS} and {\it FORS2} data sets,
allow us to study the binary fraction radial distribution from the core to up $600\arcsec$ from the cluster center.\footnote{
While the {\it FORS2} data set extends out to $r\sim800\arcsec$, we preferred to limit the analysis at $r\sim600\arcsec$ where the fraction of
covered area coverage is more complete and the number of detected stars is appropriate for an accurate analysis of the binary population.}
We divided the FOV in four concentric annuli roughly corresponding to $0.0-1.0$ $r_h$, $1.0-2.0$ $r_h$, $2.0-3.5$ $r_h$ and
$3.5-5 r_h$, and we estimated both the minimum ($\xi_{\rm min}$)  and
the global binary fractions ($\xi_{\rm TOT}$) following the approach described by Bellazzini et al. (2002).
The analysis was performed for stars with $19\leq I\leq 22$, where the completeness parameter ($C$)
is safely larger than $50\%$.
This interval corresponds to a mass range $0.55<m/M_{\odot}<0.80$ for a single star along the MS, according to
an isochrone of 12 Gyr and $Z=0.003$ (Bressan et al. 2012).

First, we measured $\xi_{\rm min}$, which is the fraction of binaries with a mass ratio $q_{\rm min}$
large enough to make them clearly distinguishable from single MS stars. The value of $q_{\rm min}$ depends on
the photometric errors: we considered a color range equal to
three times the photometric error
from the MS ridge line (see Figure~3 in Dalessandro et al. 2011);
in the considered magnitude interval and for the entire sample such a color difference corresponds to $q_{\rm min}\sim0.4$.
The contamination from blended sources and non member stars has been accounted by means of the artificial star
catalogs and the Besancon model simulation (Section~5.1).
The radial distribution of $\xi_{\rm min}$ is shown in Figure~10. As already observed for BSSs, binaries
show no significant evidence of mass segregation. In fact, their radial distribution
is almost flat around a mean value $\xi_{\rm min}=(6.2\pm 0.4)\%$.
Such a value is slightly larger than what obtained by Milone et al. (2012) only in the central regions
($q_{\rm min}=4.8\pm 0.3\%$). It is important to note, however, that Milone et al. (2012)
considered only binaries with a mass ratio larger than ours ($q>0.5$).

As a second step of the analysis, we estimated also $\xi_{\rm TOT}$.
To this aim we created hundreds of synthetic CMDs including
single and binary stars for different input values of the global binary fraction
($\xi_{\rm IN}$), for each run.
To simulate the binaries we randomly extracted $N_{\rm bin}$ values of the mass of the primary from a Kroupa (2002)
initial mass
function and $N_{\rm bin}$  values of the mass of the primary component from the Fisher et al. (2005)
mass ratio distribution, $f(q)$, which is one of the unknowns in this kind of analysis.
The impact of adopting different
mass ratio distributions has been discussed in Sollima et al. (2007) and Dalessandro et al. (2011).
To generate the sample of single MS stars we adopted the best fit to the observed mass function (MF),
which is discussed in detail in Section~6.
In Dalessandro et al. (2011) we have verified that the adoption of different present day
mass functions to simulate MS stars has a negligible impact on the final result.
$\xi_{\rm TOT}$ was then determined from the comparison between the artificial and the observed CMDs:
the value of $\xi_{\rm IN}$ providing the best match between the two CMDs is adopted as global
binary fraction $\xi_{\rm TOT}$. In particular, from the simulated catalog we computed the ratio
$r_{\rm sim} = N_{\rm bin}^{sim}/N_{\rm MS}^{sim}$ between the number of
binary stars defined as before and that of the synthetic MS population. The same was done for the observed CMD,
thus obtaining $r_{\rm sim} = N_{\rm bin}^{obs}/ N_{\rm MS}^{obs}$. For different values of $\xi_{IN}$
we computed the penalty function $\chi^2(\xi_{IN})$
defined as the summation of $(r_{\rm sim}-r_{\rm obs})^2$ and the relative probability $P(\chi^2)$ was derived (Figure~11).
The mean of the best-fitting Gaussian is adopted ad best fit value of the global binary fraction $\xi_{\rm TOT}$.
The radial distribution of $\xi_{\rm TOT}$ is shown in Figure~10.
Similarly to the minimum binary fraction, also $\xi_{\rm TOT}$ shows no variation as a function of
the distance from the center in the FOV covered in this analysis.
This results confirms that NGC~6101 has not experienced complete relaxation yet and does not show any evidence of mass segregation
among its populations.

The mean value of the global binary fraction is $\xi_{\rm TOT}=(14.4\pm 0.9)\%$.
This value is in good agreement with the one obtained by Sollima et al. (2007) in the {\it ACS} FOV
($\xi_{\rm TOT}=15.6\pm 1.3\%$), while it is significantly larger than the one estimated by
Milone et al. (2012; $\xi_{\rm TOT}=9.6\pm0.6 \%)$. Note however that Milone et al. (2012) determined the value of
$\xi_{\rm TOT}$ assuming that it is twice the value of $\xi_{\rm min}$.

\section{LUMINOSITY AND MASS FUNCTION RADIAL VARIATIONS}

To further investigate the mass segregation phenomenon in NGC~6101,
we analyzed the radial
variation of the luminosity function (LF) of MS stars. LFs give information about the effect of cluster internal
dynamics on stars in a wide range of masses, including the faint-end of the MS where most of the cluster mass lies.
In relaxed stellar systems, the slope of the LFs is expected to vary as a function of the distance from the cluster center,
with indexes decreasing as the distance increases, because of the differential effect of mass segregation.

To study the LF of NGC~6101 we used the {\it ACS} and {\it FORS2} samples. We selected a sample of bona-fide stars along the MS,
defined as those stars located within $3\sigma$ from the mean ridge line,
where $\sigma$ is the combined photometric uncertainty in the $V$ and $I$ bands.
We used the same radial bins defined in Section~5 for the binary fraction analysis.
For each radial interval we obtained the completeness-corrected
LF for stars fainter than $V=18$ and reaching the magnitude limit where
the completeness parameter $C$ is $50\%$.
Completeness has been derived by means of the artificial star catalog described in Section~5.1 (see Figure~9).
The LFs obtained in the four radial bins are shown in Figure~12.
We took the LF corresponding to the innermost radial bin as reference for comparison with the LFs in the other radial ranges.
The line connecting the points of the reference LF is plotted as a solid line in Figure~12. As apparent,
it  well reproduces the behavior observed in the more external radial bins after a proper normalization.
The key result of Figure~12 is that, in the range of magnitude and radial extension ($0<r<5 r_h$) covered by our analysis,
the shape of the different LF is clearly the same and any subtle
difference lies well within the combined uncertainty of the LFs and of the adopted normalization.

We derived the mass function (MF) of the same bona-fide stars used for the LF and within the same magnitude limits.
Masses have been obtained by using the Baraffe et al. (1997) mass-luminosity relation.
The MFs obtained in the same radial bins as the LFs are shown in Figure~13. The MF obtained in the {\it ACS} sample
goes down to $m\sim0.15 M_{\odot}$, while it reaches at most $m\sim0.35 M_{\odot}$ in the {\it FORS2} data set.
As done before, we used the MF of the innermost radial bin as reference, and we normalized the more external ones
to this by using number counts in the mass range $(0.5 <m/M_{\odot}<0.7)$. As apparent from Figure~13,
and in agreement with what obtained from the analysis of
the LFs, all MFs are virtually indistinguishable.

\section{DISCUSSION}

Three distinct indicators, namely the radial distribution of BSSs, binaries stars and
the LF of MS stars have been investigated to study the mass segregation in NGC~6101.
We have traced this effect by using stars in a wide range of masses, going from $\sim0.35 M_{\odot}$, corresponding
to the lowest mass MS stars, up to $\sim1.4M_{\odot}$ reached by the highest mass BSSs and binaries.
The results clearly indicate that the cluster  do not show evidence of mass segregation
up to $r\sim600\arcsec$ ($\sim5r_h$) from the cluster center.

Only few other GGCs are known to be in such a dynamical state:
massive systems ($M_{\rm V}<-10$), namely $\omega$~Centauri (Ferraro et al. 2006a) and
NGC~2419 (Dalessandro et al. 2008b), and three GCs that are at the low mass end distribution ($M_{\rm V}\sim-5$),
namely Palomar~14 (Beccari et al. 2011), Ter~8 and Arp~2 (Salinas et al. 2012).
Similarly to these clusters, NGC~6101 can be considered dynamically young.

Starting from the new structural parameters obtained in Section~3,
we derived the central ($t_{\rm rc}$) and half mass radius ($t_{\rm rh}$)
relaxation times following the formulae by Spitzer (1987). We adopted the same values of
$(m-M)_V$ and $E(B-V)$ used in Section~4.2,
 which yield a distance from the Sun $d=14.6\pm 0.8$ Kpc (see Section 3). We estimated the total
cluster mass $M_t$ by adopting an integrated V magnitude $V_t=9.2$ (Harris 1996) and a
mass-to-light ratios $M/L_V=3.17$ and 2.07 (Maraston et al. 1998),
appropriate for a Salpeter and Kroupa IMF respectively, and for a population of metallicity $[Fe/H]=-2.25$
and age $t=13$ Gyr.
We obtained $M_t=1.2-1.7\times10^5 M_{\odot}$ which gives a central mass density
$\rho_{M,0}=68.5 M_{\odot}$ pc$^{-3}$. We thus obtained $t_{rc}\sim1.3$ Gyr and $t_{rh}\sim5.4-6.3$ Gyr.
The value of $t_{rc}$ is consistent with what reported
by Harris (1996), while $t_{rh}$ is about three times larger than the Harris value ($t_{rh}\sim1.7$ Gyr) and more
than five times larger than the one
derived by McLaughlin \& van der Marel 2005 ($t_{rh}\sim0.9$ Gyr). This is qualitatively in agreement with
$r_h$ being larger than previous estimates reported in the literature.

We note however that both $t_{rc}$ and $t_{rh}$ are significantly smaller than the age of NGC~6101
($t_{\rm age}=13\pm 1$ Gyr; Dotter et al. 2010).
Therefore some evidence of mass segregation should be visible, at odds with the observed flat
distribution of BSS and binaries, and the constant slope of the MF LFs.
In the cases of NGC~2419 and Palomar~14, $t_{\rm rh}$ has been estimated to be $\sim 20$ Gyr
(Dalessandro et al. 2008b; Sollima et al. 2011), in good agreement with the observational evidence
of a lack of mass segregation, at least in the external regions.
However also for NGC~2419,
the central relaxation time is significantly smaller ($t_{\rm rc}\sim6$ Gyr) than the age of the cluster ($t=12$ Gyr)
and Ferraro et al. (2006) found for $\omega$~Centauri
a relatively short relaxation time ($t_{\rm rh}\sim 5$ Gyr), as for NGC~6101.
In the case of $\omega$~Centauri a number of possibilities to understand this apparent disagreement between
observations and theoretical results were examined.
Cluster rotation can play a role. In fact angular momentum
tends to keep stars out of the core, balancing the effect of mass segregation (Spurzem 2001).
Another possibility is that $\omega$ Centauri could have been hundreds of time more massive in the past
than observed today. Indeed
it has been suggested to be the relic of a partially disrupted galaxy (Bekki \& Freeman 2003; Tsuchiya et al. 2004).
The same argument can be applied to
NGC~2419 (van den Bergh \& Mackey 2004; Mackey \& van den Bergh 2005) and the extended tidal tails observed around Palomar~14 (Sollima et al. 2011) would suggest that
it experienced quite recent and efficient tidal stripping events.

For the case of NGC~6101 no evidence of internal rotation are known.
However we may speculate that NGC~6101 could have experienced a quite complex dynamical
history.
By means of dynamical simulations,
Martin et al. (2004) suggested that NGC~6101 can be associated to the Canis Major dwarf galaxy
accreted to the Galactic halo after an encounter between the dwarf and the dark matter halo of the Milky Way.
Indeed the kinematical properties of  NGC~6101 are atypical for systems with its metallicity and age.
In fact it is one of the very few metal-poor and old GGCs
with a retrograde motion (Geisler et al. 1995; Rutledge et al. 1997).
Mackey \& Gilmore (2004) suggested that the existence of old GCs with large cores in a
relative proximity to the Galactic center (as for the case of NGC~6101) can be explained by the fact that they follow
wide orbits in which they spend little time close to the Galactic center.
Alternatively, they could have been accreted only recently by the Galactic halo.

In this respect it is interesting to note that a linear fit to the MFs in Figure~12 limited to the stars
with $m<0.75 M_{\odot}$ gives a power-law index $\alpha\sim-0.9$.
With such a value and with the new estimate of the central concentration obtained in Section~3 ($c=1.3$),
NGC~6101 would nicely fit the correlation found by De Marchi, Paresce \& Pulone (2007) according to which less concentrated GCs
tend to have flatter MFs.
This behavior was interpreted by the authors as an indication of a more efficient loss of low mass stars
via evaporation and tidal stripping in less concentrated clusters. To support this possibility, evidence of tidal arms and
distortions should be searched for this cluster.

On the other hand, the observational facts collected in the case of NGC~2419, $\omega$ Cen and NGC~6101
suggest that the current theoretical estimates of the central relaxation time are extremely rough and must be used (at
least in absolute terms) with caution.
On the other side the nice agreement among the different mass segregation indicators used in the case of NGC~6101
provides additional support to the use of the radial distribution of BSS (the so called ``dynamical clock'')
as a powerful indicator of the dynamical evolution of stellar systems (Ferraro et al. 2012).
In fact, among the adopted mass-segregation indicators, BSSs are significantly brighter than the others (MS stars and
binaries), their analysis is simpler and less prone to observational bias (as completeness) and assumptions.
Hence the BSS radial distribution represents the clearest indicator
of mass segregation in stellar systems.

\acknowledgements
This research is part of the project COSMIC-LAB (http://www.cosmic-lab.eu) funded by the European Research Council
(under contract ERC-2010-AdG-267675).

\newpage

redpajama_set_name: RedPajamaArXiv


text:
Album Title Includes:
Robin Bigwood
Philip Salmon
Philip Potter
Margaret Eales
Artist's Name Includes:
Composer's Name Includes:
Any format CD CD Single SACD DVD Audio Vinyl: All LP 7" Single (45 RPM) 12" Single 78 RPM Cassette 8-Track Minidisc Reel-to-Reel
Label Name Includes:
11 Matching Classical Music Titles for
Artist: David Knight
J.S. Bach: Brandenburg Concertos 1-6 (1995)
performed by Anthony Randall (horn), Carmel Kaine (violin), Christopher Hogwood (continuo), David Mason (trumpet), Emanuel Hurwitz (violin), English Chamber Orchestra (chamber ensemble), Ifor James (horn), Nicholas Kraemer (continuo), Norman Knight (flute)
composed by Johann Sebastian Bach
Classic Kennedy (2000)
performed by Andrew Crowley (trumpet), Charles Tunnell (cello), David C. Heath (flute), David Thomas (oboe), Doug Boyle (guitar), Fabio Zanon (guitar), Greg Knowles (cimbalom), Greg Knowles (hand percussion), Harold Lester (harpsichord), Janice Knight (oboe)
composed by Antonio Vivaldi, Charles Gounod, Claude Debussy, English Traditional, Erik Satie, Frédéric Chopin, George Frederick Handel, George Gershwin, Irish Traditional, Johann Sebastian Bach, Johannes Brahms, Joni Mitchell, Jules Massenet, Nigel Kennedy
More Music Like This | Add to Wishlist
James MacMillan: Tenebrae Responsories (2013)
performed by Alexander Hopkins (treble), Andrew Crowley (trumpet), Daniel Newell (trumpet), David Knight (tenor), London Brass (brass ensemble), Peter Stevens (organ), William Gaunt (bass), Westminster Cathedral Choir (choir, chorus), Martin Baker (conductor)
composed by Gregorian Chant, James MacMillan
Gilbert & Sullivan: The Yeoman of the Guard & Trial by Jury [1964 Recordings] (1989)
performed by Ann Hood (vocals), Anthony Raffell (vocals), David Palmer (vocals), Donald Adams (vocals), Elizabeth Harwood (vocals), Gillian Knight (vocals), John Reed (vocals), Kenneth Sandford (vocals), Margaret Eales (vocals), Philip Potter (vocals)
composed by Arthur Sullivan
Christmas at St. John's (2006)
performed by Alexander Robarts (treble), Christopher Robinson (descant), David Hill (descant), George Humphreys (baritone), Jonathan Knight (tenor), Lester Lardenoye (counter tenor), Paul Provost (organ), Peter Morgan (cantor), Quintin Beer (treble)
composed by Christmas Traditional, Edward Woodall Naylor, Gregorian Chant, Gustav Holst, Herbert Howells, John Francis Wade, John Rutter, Judith Bingham, Morten Lauridsen, Otto Goldschmidt, Peter Warlock, Plainchant, Recorded Sound
Bach: Brandenburg Concertos 1-4 (1998)
performed by David Mason (trumpet), Emanuel Hurwitz (violin), Ifor James (horn), Norman Knight (flute), Peter Graeme (oboe), Philip Ledger (harpsichord), Richard Adeney (flute), English Chamber Orchestra, Benjamin Britten (conductor)
Robert Docker: Legend; Tabarinage (2000)
performed by David Presley (oboe), William Davies (piano), William Davis (piano), RTÉ Concert Orchestra, Barry Knight (conductor)
composed by Robert Docker
Ave Maria (2008)
performed by David Clegg (vocals), David Knight (vocals), David Terry (organ), John Biddle (vocals), John Biddle (chant), Laurence Carroll (vocals), Philip Bell (chant), Philip Salmon (chant), Philip Salmon (vocals), Simon Biazeck (vocals)
composed by Anton Bruckner, Charles Gounod, David Terry, Edward Elgar, Franz Biebl, Franz Schubert, Giovanni Pierluigi da Palestrina, Jacobus Clemens Non Papa, Josquin Des Prez, Matthew Martin, Robert Parsons, Roxanna Panufnik, Simon Biazeck, Tomás Luis de Victoria
Gordon Jacob: Chamber Music with Recorder
performed by Annabel Knight (recorder), David Angel (violin), Giuliano Fontanella, Maggini Quartet, Michal Kaznowski (cello), Robin Bigwood (harpsichord), Robin Bigwood (piano)
composed by Gordon Jacob, Jacob van Eyck
Beyond Imagination (2002)
performed by David Hartley (piano), Frank Ricotti (percussion), Ivor Goldberg (guitar), Jeff Bova (keyboards), John Parricelli (guitar), Jon Cohen (piano), Jon Cohen (keyboards), Juan Martín (guitar), Karen England (mezzo-soprano), Kodo (drums), Laurence Lottle (bass)
composed by Alfredo Catalani, Antonin Dvorák, Carl Orff, Edvard Grieg, Ennio Morricone, Felix Mendelssohn, Franz Schubert, George Forrest / Robert Wright, Georges Bizet, Giacomo Puccini, Giuseppe Verdi, Jacques Offenbach, Léo Delibes, Ludwig van Beethoven
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Kenneth Sandford
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John Biddle
Ifor James


Do you love Rocket League but wish it featured super-powered mecha instead of cars and focused exclusively on American football? If so, then allow me to introduce Touchdown: Armor League.
Touchdown: Armor League is a competitive, arena-based title which pits two teams of six against one another in the most frantic game of football ever. Each player gets control of a hulking power suit equipped with customized skills to suit their tastes.
If you want to learn more about the game, then check out its newly launched Kickstarter. Touchdown: Armor League needs $50,000 in funding for the developers to score a touchdown of their own.


Jewbelation is finally 21! No fake IDs or over-limit ABVs and legal in all 50 states! Genesis 21 narrates the birth of Isaac, meaning "He who laughs," born to 100 year-old parents who still circumcised him on day 8. The day I turned 21 (4/24/90) drinking birra alla spina in Florence (unlikely to say 21 letters in Italian backwards that night), the Hubble Telescope launched to seek the deepest views and true age of the universe.


text:
Schenkl is an Austro-Bavarian surname. Notable people with the surname include:

 Maurus von Schenkl (1749–1816), German Benedictine theologian and canon law jurist
 Karl Schenkl (1827–1900), Austrian classical philologist
 Emilie Schenkl (1910–1996), Austrian-Indian leader in the Indian Independence Movement

See also
 Schenk
 Schenck

redpajama_set_name: RedPajamaWikipedia


We are Independent Agents in Butler, Pennsylvania, free to choose the best carrier for your insurance needs. We do not work for an insurance company; we work for you. We work on your side when you have a loss and follow through to see that you get fair, prompt payment and service. John E. Hollock Insurance Agency represents a carefully selected group of financially strong, reputable insurance companies. Therefore, we are able to offer you the best coverage at the most competitive price.


Some family recipes go back generations, like the tea cake recipe that dates back to pre-Civil War days in an African-American family.
As young Tosh's grandmother mixes her tea cake batter, she tells him that the story behind the recipe that dates many generations back to their Grandma Ida, a cook and slave at a Southern plantation.
But as his grandmother's memory starts to suffer, Tosh picks up the mantle of family storyteller and cook.
E.B. Lewis's lovely illustrations carry an internal glow that reflects this story's sentimental heart. And there's a recipe for tea cakes!


text:
Q: Commands in /usr/bin don't work anymore I am fairly new to Ubuntu and Oracle and was following instructions to install Oracle 12c when I accidently deleted the file /lib64/ld-linux-x86-64.so.2 Now all of the commands from /usr/bin have stopped working. For every command I type, No such file or directory shows up, for eg: if I run
sudo
bash: /usr/bin/sudo: No such file or directory
My $PATH variable is fine.
The output of echo $PATH is
/home/houdini/bin:/home/houdini/.local/bin:/usr/local/sbin:/usr/local/bin:/usr/sbin:/usr/local/android-studio/bin:/usr/bin:/sbin:/bin:/usr/games:/usr/local/games:/snap/bin

I don't know what file it was and some suggest complete reinstallation, I'm hoping maybe copying somebody else's /lib64/ld-linux-x86-64.so.2 running ubuntu 16.04 LTS might solve the problem. Would it? If yes, can someone send me one. Or do i have to reinstall?


text:
No Bail For Aryan Khan, Court Decision On Wednesday
Leave a Comment / Mix Bag / By Our Team
The decision came after the Narcotics Control Bureau told the court that Aryan Khan is a regular consumer of drugs during the hearing.
Aryan Khan was arrested earlier this month by the NCB in the drugs-on-cruise case.
Mumbai: Bollywood superstar Shah Rukh Khan's 23-year-old son Aryan Khan did not get bail in the drugs-on-cruise case yesterday from a Mumbai Sessions Court that reserved the order till Wednesday, sending him back to jail. The decision meant that Aryan Khan, who has spent 12 days in jail since his arrest, has been left with no legal options till the order is announced.
The court's move came after the Narcotics Control Bureau said that Aryan Khan is a regular consumer of drugs, as the bail hearing resumed for the second day over an hour late since Additional Solicitor General Anil Singh, representing the central agency, came in late.
Mr Singh referred to on-record statements to claim to the court that "he (Aryan Khan) used to consume it for the last few years".
Arguing against giving Aryan Khan bail, Mr Singh also threw in dramatic appeals for good measure, telling the court "this is the land of Mahatma Gandhi… this (drug) abuse is affecting young boys".
In response, senior advocate Amit Desai, arguing for Aryan Khan, said that the WhatsApp chats the agency was relying on heavily can often appear suspicious given the kind of language young people use today.
"Please bear in mind one other reality. Today's generation have a means of communication, which is English… not the Queen's English.. it's sometimes what the older generation will call a torture. The way they communicate is very different," he said.
"Conversions on chats can often be misunderstood. WhatsApp chats are supposed to be private conversations. But I am told there are no messages or conversations on the mobile about the rave party," Mr Desai said.
"There is always a possibility that casual conversations between friends on WhatsApp may appear suspicious," he added.
Mr Desai acknowledged the dangers of drugs, particularly on younger people, but stressed "whatever action is taken, it should be within the ambit of the law".
"… very important to remember we fought for freedom, we fought for the Constitution, to maintain freedom of people and their rights. We can't ignore rights and can't take action without law," he said.
Mr Desai said that under the NDPS there were provisions for both "severe punishment for illegal trafficking" and "reformative approach for those people who are addicted".
"I am not saying my client is (an) addict… I am just reading that document. I am not saying anything personally but I am talking about the Supreme Court, the legislature and the government, and they have accepted that provision of punishment will be decided on basis of quantity," he said.
The defence's case is that Aryan Khan did not have drugs on him when he was arrested, he did not have money to purchase drugs and neither was he caught consuming them.
Mr Desai also reminded the court (this was in response to ASG Anil Sinha calling for strict action against celebrities and influencers) that the Bombay High Court hat said "… everyone is equal before the law (and) each case has to be decided in its own merit, despite the status of the accused".
On the question of WhatsApp chats recovered from Aryan Khan's phone, he said conversations between friends can often appear suspicious given the kind of language young people use today.
Earlier in the day ASG Anil Singh said: "Aryan Khan is not taking drugs only once… the statement that has been received shows he used to consume it for the last few years. Drugs have been found from Arbaaz Merchant (Aryan's friend, from whom six grams of charas were seized) … Aryan was with him."
"When the IO (investigating officer) asked if he had drugs, Arbaaz said he had drugs in his shoes… Arbaaz admitted that both (he and Aryan Khan) were going to consume it on the cruise."
"This is not what our freedom fighters had in mind. This is the land of Mahatma Gandhi and Buddha. The investigation is at preliminary stage, this is not the stage for grant of bail," he said.
He referred to eight previous judgments, including the Supreme Court in 'State of Orissa v Mahimananda Mishra', to say that in a conspiracy case "there can only be circumstantial evidence".
"In conspiracy there cannot be direct evidence because only conspirator will know the conspiracy. So Supreme Court has said there can only be circumstantial evidence," he said.
The ASG also told the court statements to a NCB officer under NDPS Act – referring to Aryan Khan's statements, which the defence has claimed was forced – is "admissible until proven wrong".
"In this case 15 to 20 people are involved and there is talk of conspiracy… if commercial quantity has also come to the fore," he said, in reference to claims Aryan "indulged in illicit drug trafficking".
In response to no drugs being found on Aryan Khan, he said: "If drugs were not found from you but, in the same case, if drugs in commercial quantity is found from others, action can be taken on that basis."
"My submission is that bail cannot be granted in this case," ASG Anil Singh had said.
In yesterday's hearing Aryan Khan's lawyers underlined the fact the NCB had found no drugs on their client or any evidence that suggested he was about to use banned substances.
On the NCB claim that Aryan Khan had "admitted he was about to use charas that was found on Arbaaz Merchant", the defence said the admissions were forced.
Aryan Khan was arrested hours after the anti-drugs agency's officers raided a Mumbai cruise ship party in disguise on October 2. Seven others, including Arbaaz Merchant, were arrested on October 3.
137CommentsAryan Khan has been in Mumbai's Arthur Road Jail since then; this morning he and five other accused were shifted from the quarantine block after their mandatory Covid tests returned negative.
Chalgenius: Come Promote Your Start-ups For Free
Sumit Challenges Cerebral Palsy to script Success


text:
Mega Man Battle Network Legacy Collection Japan Collector's Edition Announced
The Japanese branch of Capcom has announced the collector's edition for the upcoming Mega Man Battle Network Legacy Collection. Costing ¥10,989 for both PlayStation 4 and Nintendo Switch, this package includes the physical game alongside "two shot glasses, two acrylic coasters, and a special E-Capcom exclusive Battle Chip keychain."
View our announcement coverage containing screenshots.
Online NetBattling and Chip Trading are being worked on.
Check out 7 minutes of gameplay.
Steam Updates
Second Official Trailer, New Features & More
Thanks to Rockman's Corner for sharing and translating this edition's information. They also stated that, unfortunately, there are currently no plans for an English collector's edition. The writer, Protodude, is reliable with Mega Man news.
An image of the collector's edition is viewable below:
In case you missed it, Mega Man 11 recently became the highest-selling game in the franchise.
Mega Man Battle Network Legacy Collection will be the next release for the franchise. It was initially announced for Nintendo Switch digitally with a 2023 release window. Over 1,000 illustrations and over 150 songs from across the series will be included. PlayStation 4 and PC versions via Steam were also officially announced soon after.
The physical release will include all 10 games, while the digital releases will be separated across 2 volumes.
The following titles are included:
Mega Man Battle Network
Mega Man Battle Network 2
Mega Man Battle Network 3 White
Mega Man Battle Network 3 Blue
Mega Man Battle Network 4 Red Sun
Mega Man Battle Network 4 Blue Moon
Mega Man Battle Network 5 Team Protoman
Mega Man Battle Network 5 Team Colonel
Mega Man Battle Network 6 Cybeast Gregar
Mega Man Battle Network 6 Cybeast Falzar
Mega Man Battle Network Legacy Collection will launch for PlayStation 4, Nintendo Switch, and PC via Steam on April 14, 2023.
Resident Evil Village Reveals New Winters' Expansion Trailer; Third-Person Mode Demo Today
Resident Evil Village Receiving Free Accessibility Update October 2022; Subtitle Customization, Permanent Reticle & More
July 28, 2022 Orpheus Joshua
Street Fighter 6 Reveals New Character, Kimberly & The Return of Fan-Favorite Juri


One of the things that I like about human resources is the variety. Not just from the standpoint of the many different HR functions: recruiting and onboarding, training and development, compensation, etc. but from the variety of backgrounds that transition into HR careers. Organizations have an opportunity to harness the variety of experiences for the benefit of the workforce.
For instance, I know marketing and operations professionals that have moved into HR. Another area is actuarial science. Now you might be saying – actuarial science?! Yes, it's true. I recently had the chance to chat with Dean Aloise, global HR consulting leader for Xerox HR Services, overseeing career, health, wealth, engagement, and knowledge practices. Before becoming a human resources professional, he was the operations leader for a major actuarial firm.
I was so intrigued with Dean's professional journey that I asked if he would share his story and insights about human resources with us. Luckily, he said yes.
Dean, I was immediately intrigued by your background, particularly your experience with an actuarial firm. How did that experience translate to working in the human resources field?
[Aloise] Actuarial science, particularly as it relates to valuing the liabilities of a pension plan, is a critical need in managing the retirement benefit programs for many organizations that sponsor a defined benefit pension plan. For some organizations, this is a key component of their benefits package, thus it's an important part of the overall employee value proposition. So, while being a pension actuary is how I got into the HR field, as I gained exposure to other areas of HR, my interests and activities expanded into all other aspects of HR, which led to my career advancement.
You mentioned defined benefits plans. I know one of your areas of expertise is in the area of retirement planning. There are lots of articles these days on the topic of retirement – ranging from whether people are actually retiring (versus transitioning to an encore career) to the financial considerations of retirement. How do you see the retirement conversation having an impact on strategic HR?
[Aloise] This is indeed a critical area for employees these days, and HR must lead the way in helping their employees achieve the best possible outcome for themselves and for their organization. HR needs to approach this strategically, understanding that the changing dynamics of retirement (employees are working longer, living longer, and seeking various ways to phase into retirement) should be embraced. By supporting their employees in this changing dynamic, HR will be in the best position to properly succession plan, but also do right by their people in helping them to achieve a successful retirement outcome.
Thinking about and planning for retirement can have a huge impact on well-being. Should HR consider retirement planning a part of their well-being programs? And if so, what would help employees better prepare for retirement?
[Aloise] Well-being must be thought of as TOTAL well-being, which includes the health, wealth (retirement), and career development of employees, as well as community and social engagement, and even spiritual elements. Traditional wellness or well-being programs initially were primarily focused on only one aspect of well-being—physical health—and this likely explains why many employers haven't achieved the results they seek. The well-being programs of the future will achieve greater results by focusing on all five of the elements I mentioned.
Looking more closely at my area of initial focus—wealth—up until now we have focused exclusively, or nearly exclusively on accumulating wealth to fund a traditional retirement. But today, given the dramatic economic and social changes that have impacted the workplace, HR should be expanding beyond assisting employees with retirement planning and instead help them achieve greater levels financial well-being.
This is a great time of year to have this conversation. In many organizations, it's the start of operational planning and budgeting. HR has the opportunity to educate senior management on trends in retirement and planning. What trends are you seeing that HR needs to keep on their radar?
[Aloise] Adding a meaningful financial well-being program into employees' benefit offerings is a key trend. HR should be looking for what vendors are offering in this area, issuing requests for proposal (RFPs) and taking different programs for a test drive. Another trend that has been with us for a while now, but that continues to gain momentum thanks to continuing advances in technology, is supporting employees—and their families—in making more informed decisions about their benefits, not just when it's time to choose their benefits but year-round, when they actually are using those benefits to meet their physical and financial well-being needs.
I'm curious. Are the conversations and trends we see in the U.S. about retirement and well-being the same conversations that are happening globally?
[Aloise] The nuances around retirement readiness and financial well-being vary by country, as social security programs, employer and individual practices vary significantly. Some countries like France have fairly robust programs that lessen the severity of the retirement readiness issue, while other countries like the U.K. share fully in the 'grey tsunami' risks and concerns such that the U.S. is seeing in the very near future. The dynamics of individual, company-provided and social security retirement programs overlaps come into play in a big way when looking at retirement issues globally.
At this time, we are finalizing the results of the seventh edition of our global wellness survey, Working Well—only this year we have dubbed it the Global Survey of Workplace Well-Being Strategies, reflecting the trends I discussed earlier. Among our survey's findings is that implementing a global well-being strategy is challenging, due to the variability in culture, laws and practices across regions. This holds true not just for retirement plans, as I mentioned above, but also for physical wellness and financial well-being programs.
What is consistent around the world are the reasons for supporting employees' well-being: improving worker performance and productivity and attracting and retaining employees. Clearly, employers believe that the well-being of their employees is critical to the organization's success.
I want to thank Dean for sharing his expertise with us. I believe organizations will have to start viewing retirement as more than just a program they offer employees. And, as an increasing number of organizations adopt a global business strategy, it will be important to understand well-being in a global context.
P.S. We hope you can join us on Tuesday, December 13, 2016 at 9a Eastern for a Google Hangout with Dean and Scot Marcotte, managing director of talent and HR solutions, to talk about global well-being and retirement strategies. You can also follow @XeroxHRInsights on Twitter for details. It's sure to be a thought provoking conversation about the future of HR that you just won't want to miss.
P.S.S. Google just released an update to Hangouts, so be sure to check it out beforehand.
I think companies or organization should start creat a value for employees like share holders do get. He/she is not not only a factor production, he is a wealth creator. And as ethical point of view he/she is human being and not a lifeless mechine to discard. Must be provided safty after retirement life with medical and living source.


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