text:
Little Alchemy 2 is a game that involves fun yet soothing gameplay.
Its ease of use has made it popular among many, as the gameplay allows players to be creative, making some amazing creations in the process.
Previously, players were free to generate immortal monsters and gods by merging complex and basic elements in games involving a mix of alchemy and elements.
Little Alchemy 2 maximizes these creatures using extraordinary elements, such as Immortality.
In this article, we'll cover more about generating Immortality in Little Alchemy 2, but remember that you can only acquire Immortality if you own a certain pack titled Myths and Monsters.
What Is Immortality In Little Alchemy 2?
Before we can get into how to achieve Immortality, we need to understand what it means within the game.
Essentially, Immortality involves 15 additional elements that can be used to make different items within the game. Some of these are rare or legendary pieces.
However, there's no simple way of attaining the Immortality formula. It can't be crafted, but it can be purchased.
In the following sections, we'll cover how to get hold of Little Alchemy 2 Immortality.
Generate The World On The Correct Device
You'll need the Myths and Monsters content pack to achieve Immortality, but this is only available on iOS and Android-compatible devices.
If you are playing Little Alchemy 2 on a web browser, you need to download the app to a different phone or tablet.
Apple iOS users can find the app in the App Store, while those on Google Android devices can search for the app in Google Play.
PLEASE NOTE that moving to a different compatible device means that you need to start the game over from the beginning.
Little Alchemy 2's developer hasn't yet provided an option to move your online progress between different devices.
Go To The Little Alchemy 2 Store
Players can only currently use the Myths and Monsters content pack if they buy it within the applications store.
Many players believe the pack shouldn't cost any extra, but remember that the developer has already made the actual game and many elements free.
Factoring this in, the content pack's price of $2.99 isn't that much in the grand scheme of things.
The Little Alchemy 2 Store icon will display a line drawing of a brick-and-mortar shop.
You should notice the label 'Store' underneath. This is found at the bottom of the navigation bar or on the left side of the screen.
Add The Content Pack
Unlike other alchemy games, in Little Alchemy 2, you don't need to generate many elements or merges to obtain the Immortality element.
Once you add the Myths and Monsters pack to the main app, you will automatically obtain the Immortality element as a starting item.
This is one of the main building blocks for creating monsters and myths, as well as Monster, Good, and Evil elements.
You add the content pack to the app by tapping the Purchase icon, then following the instructions afterward.
Once you're done, you will have created Immortality!
The Immortality icon looks like a gold infinity sign on a dark background. You'll notice it in your element collection after you've obtained Immortality.
Is Immortality Essential In Little Alchemy 2?
Immortality isn't essential within the game. If you prefer, you can enjoy using the other 720 elements and do without the Myths and Monsters content pack.
However, if you don't have the pack, you won't be able to explore the game fully. The game's educational content and the extra 110 elements in the pack aren't accessible unless you obtain the Immortality element.
Additionally, you won't be able to explore the range of monsters and deities in other guides without the pack and the Immortality element.
In the past, humans would turn to myths and monsters to explain mysterious things in their world. As a result, Immortality depicts the human necessity to comprehend death, as it gives the idea of everlasting existence.
Some believe that particular deities, like gods and goddesses, own the right to be beautiful, live young, and live forever.
Others believe that the soul is immortal and that the soul leaves the human form after death to reach eternal consciousness afterward.
This concept of eternal consciousness is represented within the game.
The Immortality element gives Little Alchemy 2 players access to 15 more elements. They are also connected to the idea of living forever, which is as follows:
Ankh = Immortality and the Mummy
Baast = Immortality and the Cat
Book of the Dead = Immortality and the Book
Tawaret = Immortality and the Hippo
Peach of Immortality = Immortality and the Fruit
Peach of Immortality = Immortality and the Fruit Tree
Sun Wukong = Immortality and the Monkey
Achilles = Immortality and the Hero
Deity = Immortality and the Human
Ouroboros = Immortality and the Dragon
Ouroboros = Immortality and the Snake
Yggdrasil = Immortality and the Tree (see also 'How To Make Tree In Little Alchemy')
Demon = Immortality and Evil
Holy Grail = Immortality and the Cup
Fountain of Youth = Immortality and the Fountain
Elixir of Life = Immortality and the Bottle
Elixir of Life = Immortality and the Container
Elixir of Life = Immortality and Liquid
Philosopher's Stone = Immortality and the Alchemist
Philosopher's Stone = Immortality and the Rock
Philosopher's Stone = Immortality and the Stone
Things The Immortality Element Can Do In Little Alchemy 2
When you use any elements made with Immortality, you can begin learning about several monsters and mythical creatures people once believed had a connection to everlasting life.
For instance, the Peach of Immortality allows you to discover the Chinese Dragon.
Other examples include using the Holy Grail to make a Paladin and, following that, the famed Durendal sword.
Ouroboros lets you create the Midgard Serpent surrounding the Earth and Jörmungandr, Loki's offspring within Viking Norse Legends.
The Deity element allows you to access many mythical figures, including Cupid, Poseidon, Thor, and Zeus. The element also allows you to find famous artifacts like Mjölnir, Pandora's Box, and even Heaven itself.
Now you know how to achieve the Immortality element within Little Alchemy 2!
Remember that you can only access the element by purchasing the Myths and Monsters content pack. This can only be done on Android and iOS-compatible devices, so you must switch to one if you play through an internet browser.
However, switching to these will mean you have to start the game from scratch, so don't switch unless you're prepared to lose your progress.
How To Make Sun In Little Alchemy
How To Make Big In Little Alchemy 2
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Battlefield has fast become one of the most popular game series in the world. With an estimated 30,000 players a month, the Battlefield fad isn't phasing out anytime soon. Although the release of Battlefield 2042 has taken the spotlight away from other games in the series, Battlefield 5 remains an ever-popular installment, with thousands of…
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Video games go through updates all the time. These bring improvements to the game's performance, user experience, and features, but they can also bring new problems, like gameplay glitches and bugs. Among Us, one of the most popular online games of today is one of these games. Among Us received an update in 2021 called…
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The various music abilities available in The Sims 4 are some of the most enjoyable to practice. Piano, guitar, and violin are all instruments that you may learn to play. Writing songs and then licensing them to gain some extra cash is a terrific way to use your musical talents. You might have a sim…
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Civ 6 Best Pantheon List
In this article, we will tell you our Civ 6 best Pantheon list. Our thoughts on them and when you should and shouldn't take them. Everyone has different experiences with Civ 6, and it's a complicated game. Our opinion is that there are only three good pantheons and 86 terrible pantheons, and we will have to sort through them. We're going to have to create middle tiers.
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This blog entry is about moderation or rather my lack of it.
I knit a hat yesterday. A whole hat. The first 90 percent went by really fast, no troubles at all, just straight forward knitting. Then I was almost done. Which is when the problems started and when I just couldn't do what would have been the right thing to do. Have a break, call it a day, just let it be. Instead I went on and on. With tense shoulders, hurting back and fingers that were starting to blister. I decided I didn't like the finishing of the hat and ripped it out again at 10pm. I picked up stitches all around the hat again and fought my way through it. At 11pm. I had to block it as well, it couldn't wait another day.
The result is an ok hat that might or might not be too small even for a newborn. And a feeling that I am again where I shouldn't be - in exaggeration mode. This is not fun, this is pushing myself to go on long after it was fun and I don't know why I always end up here. I guess I have to make myself take a break and find a healthier way to knit.
definitely don't push yourself, you need to take knitting breaks every 20 minutes, a simple stretch of arms a walk for a glass of water. Also experiment with different needles, there's a difference between wooden and metal and how you relax. I like metal for everything but socks and hats I like wooden. Good luck next time!


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So you are planning to buy a new smartphone? However, the availability of numerous options will make you difficult to choose one. Today, many mobile manufacturers are producing different varieties of smartphones. First find out how are smartphones different from regular mobile phones.
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Q: Specifying a custom DateTime format when serializing with Json.Net I am developing an API to expose some data using ASP.NET Web API.
In one of the API, the client wants us to expose the date in yyyy-MM-dd format. I don't want to change the global settings (e.g. GlobalConfiguration.Configuration.Formatters.JsonFormatter) for that since it is very specific to this client. And I do developing that in a solution for multiple clients.
One of the solution that I could think of is to create a custom JsonConverter and then put that to the property I need to do the custom formatting
e.g.
class ReturnObjectA
{
    [JsonConverter(typeof(CustomDateTimeConverter))]
    public DateTime ReturnDate { get;set;}
}

Just wondering if there is some other easy way of doing that.

A: It can also be done with an IsoDateTimeConverter instance, without changing global formatting settings:
string json = JsonConvert.SerializeObject(yourObject,
    new IsoDateTimeConverter() { DateTimeFormat = "yyyy-MM-dd HH:mm:ss" });

This uses the JsonConvert.SerializeObject overload that takes a params JsonConverter[] argument.

A: public static JsonSerializerSettings JsonSerializer { get; set; } = new JsonSerializerSettings()
        {
            DateFormatString= "yyyy-MM-dd HH:mm:ss",
            NullValueHandling = NullValueHandling.Ignore,
            ContractResolver = new LowercaseContractResolver()
        };

Hello,
I'm using this property when I need set JsonSerializerSettings

A: Also available using one of the serializer settings overloads:
var json = JsonConvert.SerializeObject(someObject, new JsonSerializerSettings() { DateFormatString = "yyyy-MM-ddThh:mm:ssZ" });

Or
var json = JsonConvert.SerializeObject(someObject, Formatting.Indented, new JsonSerializerSettings() { DateFormatString = "yyyy-MM-ddThh:mm:ssZ" });

Overloads taking a Type are also available.

A: You are on the right track.  Since you said you can't modify the global settings, then the next best thing is to apply the JsonConverter attribute on an as-needed basis, as you suggested.  It turns out Json.Net already has a built-in IsoDateTimeConverter that lets you specify the date format.  Unfortunately, you can't set the format via the JsonConverter attribute, since the attribute's sole argument is a type.  However, there is a simple solution: subclass the IsoDateTimeConverter, then specify the date format in the constructor of the subclass.  Apply the JsonConverter attribute where needed, specifying your custom converter, and you're ready to go.  Here is the entirety of the code needed:
class CustomDateTimeConverter : IsoDateTimeConverter
{
    public CustomDateTimeConverter()
    {
        base.DateTimeFormat = "yyyy-MM-dd";
    }
}

If you don't mind having the time in there also, you don't even need to subclass the IsoDateTimeConverter. Its default date format is yyyy'-'MM'-'dd'T'HH':'mm':'ss.FFFFFFFK (as seen in the source code).

A: You could use this approach:
public class DateFormatConverter : IsoDateTimeConverter
{
    public DateFormatConverter(string format)
    {
        DateTimeFormat = format;
    }
}

And use it this way:
class ReturnObjectA
{
    [JsonConverter(typeof(DateFormatConverter), "yyyy-MM-dd")]
    public DateTime ReturnDate { get;set;}
}

The DateTimeFormat string uses the .NET format string syntax described here: https://learn.microsoft.com/en-us/dotnet/standard/base-types/custom-date-and-time-format-strings

A: There is another solution I've been using. Just create a string property and use it for json. This property wil return date properly formatted.
class JSonModel {
    ...

    [JsonIgnore]
    public DateTime MyDate { get; set; }

    [JsonProperty("date")]
    public string CustomDate {
        get { return MyDate.ToString("ddMMyyyy"); }
        // set { MyDate = DateTime.Parse(value); }
        set { MyDate = DateTime.ParseExact(value, "ddMMyyyy", null); }
    }

    ...
}

This way you don't have to create extra classes. Also, it allows you to create diferent data formats. e.g, you can easily create another Property for Hour using the same DateTime.

A: With below converter
public class CustomDateTimeConverter : IsoDateTimeConverter
    {
        public CustomDateTimeConverter()
        {
            DateTimeFormat = "yyyy-MM-dd";
        }

        public CustomDateTimeConverter(string format)
        {
            DateTimeFormat = format;
        }
    }

Can use it with a default custom format
class ReturnObjectA
{
    [JsonConverter(typeof(CustomDateTimeConverter))]
    public DateTime ReturnDate { get;set;}
}

Or any specified format for a property
class ReturnObjectB
{
    [JsonConverter(typeof(CustomDateTimeConverter), "dd MMM yy")]
    public DateTime ReturnDate { get;set;}
}

A: Some times decorating the json convert attribute will not work ,it will through exception saying that "2010-10-01" is valid date. To avoid this types i removed json convert attribute on the property and mentioned in the deserilizedObject method like below.
var addresss = JsonConvert.DeserializeObject<AddressHistory>(address, new IsoDateTimeConverter { DateTimeFormat = "yyyy-MM-dd" });

redpajama_set_name: RedPajamaStackExchange


View more >Aim. This article is a report of a study investigating health-related quality of life and its predictors 6 months after hospital discharge in individuals who had experienced moderate to severe injury. Background. Understanding the relationship between individuals' illness representations and health-related quality of life may provide the foundation for strategies to promote recovery after injury. Methods. A longitudinal predictive a survey was undertaken. Questionnaires were administered while patients were in hospital, and telephone interviews were conducted 3 and 6 months after hospital discharge. Data were collected from August 2006 to February 2007. Demographic and clinical data were collected and the Chinese Illness Perception Questionnaire Revised (Trauma) and the Medical Outcomes Study Short Form 36, were used. Simultaneous multiple regressions were used to identify predictors of health-related quality of life. Results. A total of 114 participants completed the 6-month survey. Demographic and clinical characteristics did not predict health-related quality of life. Predictors of 6-month Physical Summary Score were 3-month Physical Summary Score and two illness representation scales: Identity and Timeline (acute/chronic). Predictors of 6-month were 3-month Mental Summary Score, and three illness representation scales: Identity, Emotional representations and Timeline (acute/chronic). Independent variables accounted for 75Ʊ% and 72ƴ% of the variance in Physical and Mental Summary Scores. Conclusion. Assessment of patients' illness representations may help clinicians to understand better how people who have sustained traumatic injury view their health and health-related quality of life and to help patients in their recovery process.


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text:
\section{The {\it Swift} SFXT Project: a review \label{cospar12:intro}}

In the last decade and a half, observations by X--ray satellites
led to the discovery of a new class of high mass X--ray
binaries (HMXBs) with supergiant companions, called
supergiant fast X-ray transients
\citep[SFXTs; ][]{Smith2004:fast_transients,Sguera2005,Negueruela2006:ESASP604}.
The members of this class exhibit periods of enhanced
X--ray activity with durations ranging from a few hours to a few days
and peak luminosities of $10^{36}-10^{37}$~erg~s$^{-1}$.
A distinctive property of SFXTs is the high dynamic range,
spanning three to five orders of magnitude,
with sudden increases in luminosity from $\sim 10^{32}$~erg s$^{-1}$
up to the flare peak luminosity (e.g.\ \citealt{zand2005}).
The X-ray spectra can be described with models typically
used to fit the X-ray emission from pulsars in HMXBs
(see e.g. \citealt{Walter2007}).
We generally distinguish between confirmed and candidate SFXTs
based on the availability of an optical classification of the companion.
We currently have 10 confirmed and about as many candidate SFXTs.

The accretion mechanisms responsible for the fast and high
variability of SFXTs are still poorly known and understood.
They can be divided in two categories:
those models for which the X-ray variability exclusively
depends on the properties of the geometry and inhomogeneity
of the stellar wind from the donor star
(see e.g. \citealt{zand2005}; \citealt{Sidoli2007},
\citealt{Negueruela2008}),
and the accretion mechanisms linking the observed high dynamic ranges
to the properties of the compact object
and assuming only modest variation in the density and/or velocity of the supergiant wind
(see e.g.\ \citealt{Grebenev2007}; \citealt{Bozzo2008}).

Our {\it Swift} SFXT Project
has been performing a systematic investigation of the properties of SFXTs with a strategy that combines
{\it Swift}\footnote{See \citet[][]{Gehrels2004} for a description of the {\it Swift} satellite.}
monitoring programs with outburst fol\-low-up observations.

\subsection{Long term monitoring campaigns\label{cospar12:sec:longterm}}
The initial monitoring sample consisted of 4 confirmed SFXTs, chosen among the 10 or so SFXTs
known in late 2007 and it includes the two prototypes of the class XTE J1739$-$302
and IGR~J17544$-$2619.
The first campaigns ran from 2007 October 26 to 2009 November 3
(MJD 54399 to 55138, shown as part of the grey data in  Fig.~\ref{cospar12:fig:campaigns})
with a regularly sampled pace of 2--3 observations week$^{-1}$ object$^{-1}$, each 1\,ks long,
for a total on-source exposure of 606\,ks divided in 558 observations.
The {\it Swift}/X-ray Telescope \citep[XRT, ][]{Burrows2005:XRT}  was set in AUTO mode,
to best exploit the  XRT automatic mode switching
in response to changes in the observed source intensity.
This has allowed, for the very first time, to study the long term properties of SFXTs
with a pointed, high sensitivity X--ray telescope.

The detailed results of these campaigns can be found in \citet[][]{Sidoli2008:sfxts_paperI} and
\citet[][ and references therein]{Romano2009:sfxts_paperV,Romano2011:sfxts_paperVI}
and they include the discovery, outside their outbursts, of X-ray activity in all four SFXTs,
demonstrating that these transients accrete matter even outside their outbursts.
This emission is highly variable, with timescales ranging from months down to the shortest timescales
we can probe (a few hundred seconds) with a dynamic range in excess of 1 order of magnitude in all four SFXTs.

We also assessed how long each source spends in each state \citep{Romano2011:sfxts_paperVI}
by studying the XRT count rate distributions.
The overall dynamic range reaches then $\sim4$ orders of magnitude  when outbursts,
that only account for 3--5\,\% of the total SFXT phase, are considered.
The most common X-ray flux is $F_{\rm 2-10\,keV}\sim (1$--$2)\times10^{-11}$ erg cm$^{-2}$ s$^{-1}$
(unabsorbed), corresponding to luminosities in the order of a few 10$^{33}$--10$^{34}$~erg~s$^{-1}$,
$\sim 100$ times lower than the bright outbursts \citep{Romano2011:sfxts_paperVI}.
Finally, we calculated that the duty-cycle of inactivity is in the
range $\sim 19$--$55$\,\% \citep[][]{Romano2009:sfxts_paperV,Romano2011:sfxts_paperVI}.
Therefore, differently from what was previously estimated using less sensitive instruments,
true quiescence  (at $\sim 10^{32}$~erg s$^{-1}$)
is a relatively rare state for these transients.

\begin{figure}[t]
\begin{flushleft}
\vspace{-0.5truecm}
\hspace{-0.5truecm}
\centerline{\includegraphics[width=10cm,height=13truecm,angle=0]{figure1.ps}}
\end{flushleft}
\vspace{-2.0truecm}
\caption[XRT campaigns]{{\it Swift}/XRT (0.2--10\,keV) light curves
of our 2007--2009 long-term monitoring program (MJD 54399  to  55138)
and subsequent outbursts and follow-ups.
Each point refers to the average count rate observed
during each observation performed with XRT, except for outbursts
where the data were binned to include at least 20 counts bin$^{-1}$ to best represent the
dynamical range. Downward-pointing arrows are 3-$\sigma$ upper limits.
Upward pointing arrows mark bright outbursts detected
by BAT (and not simultaneously followed by XRT),
or by MAXI (AX~J1841.0$-$0536, MJD~55507).
Data in grey were previously published in
\citet[][]{Romano2009:sfxts_paperV,Romano2011:sfxts_paperVI,Romano2011:sfxts_paperVII,Romano2013:MI50x_sfxts}
and \citet{Farinelli2012:sfxts_paperVIII}. Data in red are presented here for the first time.
}
\label{cospar12:fig:campaigns}
\end{figure}

\subsection{Outbursts and follow-ups\label{cospar12:sec:outburst}}
Many observations were collected during the SFXT outbursts, as these are certainly the
most prominent
manifestation of their activity
\citep[][]{Romano2008:sfxts_paperII,Romano2009:sfxts_paper08408,Sidoli2009:sfxts_paperIII,Sidoli2009:sfxts_paperIV}.
Indeed, {\it Swift} can catch and study them in broad band (0.3--150\,keV) in their early stages,
thanks to the combination of its on-board triggering, autonomous fast slewing and panchromatic capabilities,
thus allowing us to assess the spectroscopic and timing properties of SFXTs when they are in their brightest
phases.
Given the shape of the SFXT spectrum (power law with an exponential cut-off),
the large {\it Swift} energy range allows us to both constrain the
hard-X spectral properties to compare with popular accreting neutron star models
and to obtain a measure of the absorption.

For this project, the Burst Alert Telescope \citep[BAT, ][]{Barthelmy2005:BAT} Team devised
and applied to the whole sample of SFXTs and candidates,
the so called ``BAT special functions'', starting from 2008 September 25.
They are modifications of the on-board triggering
figure of merit that allow SFXTs to trigger the BAT, perform a slew and then observe the source
as if it were a $\gamma$-ray burst, {\it Swift}'s natural target. This ensures that the source obtains
not only coverage with the BAT, but also with the narrow-field instruments, XRT
and the UV/Optical Telescope \citep[UVOT, ][]{Roming2005:UVOT}.
Further `triggers' also came from the BAT Transient Monitor
\citep[][]{Krimm2006_atel_BTM,Krimm2013:BATTM}\footnote{
\href{http://swift.gsfc.nasa.gov/docs/swift/results/transients/}{http://swift.gsfc.nasa.gov/docs/swift/results/transients/} }.
After the initial automated target exposure
we generally follow the decay of the outburst for at least a week with XRT through
target of opportunity  (ToO) observations.

Our strategy has several advantages.
\begin{enumerate}
\item  It quickly tripled the available sets of broad-band data of SFXT outbursts
\citep[e.g.\ ][]{Sidoli2009:sfxts_sax1818,Romano2011:sfxts_paperVI,Romano2011:sfxts_paperVII,Romano2013:MI50x_sfxts,Farinelli2012:sfxts_paperVIII,Mangano2012:Gamma12}.
From launch to the end of 2012, {\it Swift} has detected 42 outbursts, for a total of 45
on-board triggers (5 from candidates),
24 (2) with broad band coverage, 22 of which have been detected thanks to the BAT special functions being applied.
Fig.~\ref{cospar12:fig:campaigns} (red points) shows some of the most recent outbursts of
the 4 monitored SFXTs after the long term monitoring described in Section~\ref{cospar12:sec:longterm} ended
in 2009 November.

\item  The unique \sw\ characteristic of an automated, fast repointing to potentially
any target that triggers the BAT, has allowed the arcsecond localization  for several SFXTs and candidates
whose coordinates were only known to the arcminute level, or to improve upon previously known coordinates,
and consequently help in associating with an optical counterpart.
Such is the case for \src, that we localized when it first went into outburst  \citep{Grupe2009:16328-4726},
and AX~J1845.0$-$0433, whose position we now refine with respect to a previously known {\it XMM-Newton} one.
Both cases are presented in detail below.

\item We have now observed outbursts from most confirmed SFXTs
and followed them with XRT
for days after the outburst (by reaching a few tenths of a $\mu$Crab in 10\,ks),
well after it had become undetectable with monitoring instruments with lower
sensitivity (especially in crowded fields) such as the All-Sky Monitor on board
RXTE (\citealt[][10 mCrab in the 1.5--12\,keV band at 2$\sigma$ level for 1 day average)]{Levine1996:RXTE_ASM}
or MAXI (\citealt[][15\,mCrab in the 0.5--20\,keV band at 5$\sigma$ level for 1 day average)]{MAXI:Matsuoka2009PASJ}.
The simplest piece of information we can derive from the X-ray light curves
is the dynamic range, which is a discriminant \citep[][]{Negueruela2006:ESASP604,Walter2006}
between outbursts of classical supergiant HMXB (sgHMXB, $\lesssim 20$) and SFXT ($\gtrsim100$).
Fig~\ref{cospar12:fig:best_sfxts} shows the best examples of XRT outburst light curves,
and highlights what we have discovered as the common X--ray characteristics of this class:
outburst lengths well in excess of hours (sometimes lasting several days), with a multiple-peaked structure,
and a dynamic range (only including bright outbursts) up to $\sim3$ orders of magnitude.
\end{enumerate}

\subsection{A Physical model for SFXT broad-band spectra\label{cospar12:sec:compmag}.}

As part of our ongoing effort to understand the physical mechanisms responsible for
the bright outbursts, we have recently developed a physical model, {\tt compmag}
in {\tt XSPEC}
\citep[][]{Farinelli2012:compmag},
which includes thermal and bulk Comptonization for cylindrical accretion onto a
magnetized neutron star.
 A full description of the algorithm can be found in \citet[][]{Farinelli2012:compmag};
here we summarize the main characteristics and the results of the first
applications.

\begin{figure}[H]
\begin{flushleft}
\vspace{-3truecm}
\centerline{\includegraphics[width=12cm,angle=0]{figure2.ps}}
\end{flushleft}
\vspace{-2.0truecm}
\caption[XRT light curves]{Light
curves of the better followed-up outbursts of SFXTs
followed by {\it Swift}/XRT with starting times
referred to their respective BAT triggers
(IGR~J11215$-$5952
did not trigger the BAT, so it is referred to MJD 54139.94;
similarly, IGR~J16418$-$4532 is referred to the start of the observation).
Points denote detections, triangles 3$\sigma$ upper limits.
Red data points (panels h and i) refer to observations presented here
for the first time, while grey points to data presented elsewhere.
Vertical dashed lines mark time intervals equal to 1 day, up to a week.
References:
IGR~J08408--4503 \citep[2008-07-05, ][panel a]{Romano2009:sfxts_paper08408};
IGR~J11215$-$5952 \citep[2007-02-09, ][panel b]{Romano2007};
IGR~J16479$-$4514 \citep[2005-08-30, ][panel c]{Sidoli2008:sfxts_paperI};
XTE~J1739$-$302 \citep[2008-08-13, ][panel d]{Sidoli2009:sfxts_paperIV};
IGR~J17544$-$2619 \citep[2010-03-04, ][panel e]{Romano2011:sfxts_paperVII};
SAX~J1818.6$-$1703 \citep[2009-05-06, ][panel f]{Sidoli2009:sfxts_sax1818};
AX~J1841.0$-$0536 \citep[2010-06-05, ][panel g]{Romano2011:sfxts_paperVII};
AX~J1845.0$-$0433 (2012-05-05, this work, panel h);
candidate SFXT IGR~J16328--4726 (2009-06-10, this work, panel i);
candidate SFXT IGR~J16418$-$4532 \citep[2011-02-18, ][panel l]{Romano2012:sfxts_16418}.
}
\label{cospar12:fig:best_sfxts}
\end{figure}

\clearpage

The {\tt compmag}  model considers a blackbody spectrum of photons
as seed for Comptonization of the plasma.
The free parameters are temperature $kT_{\rm bb}$ of the blackbody seed photons,
the electron temperature $kT_{\rm e}$,  and vertical optical depth $\tau$ of the
Comptonization plasma,
the radius of the accretion column $r_{\rm 0}$
and the albedo $A$ at the surface of the neutron star.
The velocity field of the accreting matter can
either be increasing towards the NS surface, in which case further free parameters are
the terminal velocity $\beta_0$ at the NS surface, and the index of the law
$\beta(z) \propto z^{-\eta}$,
or it may be described by an approximately decelerating profile, so that the velocity law
is given by $\beta(\tau) \propto -\tau$.

The {\tt compmag} model was first applied to
the SFXT class prototypes XTE J1739$-$302 and IGR~J17544 $-$2619
\citep[][]{Farinelli2012:sfxts_paperVIII}.
We note that, in general, it is not advisable to keep all the above mentioned parameters free,
when trying to constrain them.
We therefore assumed an increasing velocity of the infalling material towards the NS surface
and set $\eta=0.5$ and $\beta_0= 0.2$ or 0.05.
We also set $r_{\rm 0}= 0.25 $  (in units of the NS Schwarzschild radius) and $A=1$.
Under these assumptions, we found that the XRT+BAT spectra of the
2011 February 22  and 2011 March 24 outbursts of XTE J1739$-$302 and IGR~J17544 $-$2619,
respectively, can be fit well with a single unsaturated Comptonization model such as
 {\tt compmag}. In particular, we showed that the electron density
in the region of the X-ray spectral formation, inferred from the best-fitting parameters
of the {\tt compmag} model, is a about 3 orders of magnitude higher than expected
from the continuity equation at the magnetospheric radius, and we proposed that this might be
explained in terms of a bow shock at the NS magnetosphere.
This effect is currently under investigation via 3D magnetohydrodynamical simulations.

\begin{figure}[t]
\begin{flushleft}
\vspace{-1.5truecm}

\hspace{-0.5truecm}
\centerline{\includegraphics[width=10.5cm,angle=0]{figure3.ps}}
\end{flushleft}
\vspace{-3truecm}
\caption[XRT campaigns]{{\it Swift}/XRT light curves of monitoring programs along
one or more orbital periods.
{\bf Top:} IGR~J18483$-$0311, with orbital period $P_{\rm orb}=12.545$\,d \citep{Levine2011},
observed on 2009 June 11 to July 9, shown at a binning of at least 20 counts bin$^{-1}$
\citep[adapted from][]{Romano2010:sfxts_18483}.
{\bf Middle:} IGR~J16418$-$4532, with  $P_{\rm orb}=3.73886$\,d \citep{Levine2011},
observed on 2011 July 13--30, shown at a binning with a S/N$=3$
\citep[adapted from][]{Romano2012:sfxts_16418}.
{\bf Bottom:} IGR~J17354$-$3255, with  $P_{\rm orb}=8.4474$\,d \citep{Sguera2011:17354},
observed on 2012 July 18--28,  shown at a binning of at least 20 counts bin$^{-1}$
\citep[adapted from][]{Ducci2013:sfxts_17354}.
}
\label{cospar12:fig:campaigns2}
\end{figure}

\subsection{Further monitoring campaigns\label{cospar12:sec:monit2}.}
Further monitoring campaigns featured observations \,
along one or more orbital periods of an SFXT, to study the effects of orbital parameters on the flare distributions.
Such is the case of IGR~J18483\-$-$0311, observed between 2009 June 11 and July 9
\citep[23 daily observations, $\sim2$\,ks each, spread over 28\,d
for a total of 44\,ks; ][see  Fig.~\ref{cospar12:fig:campaigns2} top]{Romano2010:sfxts_18483}
with orbital period $P_{\rm orb}=18.545$\,d \citep{Levine2011},
the candidate SFXT     IGR J16418\-$-$4532,
observed on 2011 July 13--30 \citep[12 observations, $\sim2$--5\,ks each, spread
over 18\,d for a total of 39\,ks; ][see Fig.~\ref{cospar12:fig:campaigns2} middle]{Romano2012:sfxts_16418},
with  $P_{\rm orb}=3.73886$\,d \citep{Levine2011},
and the candidate SFXT  IGR J17354\-$-$3255,
observed on 2012 July 18--28 \citep[22 observations, $~\sim1$\,ks each, spread
over 11\,d for a total of 24\,ks;  ][see Fig.~\ref{cospar12:fig:campaigns2} bottom]{Ducci2013:sfxts_17354},
with  $P_{\rm orb}=8.4474$\,d \citep{Sguera2011:17354}.
These unique datasets allowed us to constrain in these objects the different mechanisms
proposed to explain their nature. In particular, we applied the clumpy wind model for blue supergiants
by \citet[][]{Ducci2009} to the observed X-ray light curve.
By assuming for IGR~J18483\-$-$0311 an eccentricity of $e = 0.4$
and for IGR~J16418\-$-$4532 a circular orbit,
we could explain their X-ray emission in terms of the accretion from a spherically
symmetric clumpy wind, composed of clumps with different masses,
ranging from $10^{18}$ to $5\times10^{21}$\,g for IGR J1848\-$-$0311,
and from $\sim5\times10^{16}$~g to $10^{21}$~g for IGR J16418\-$-$4532.
The soft X-ray light curve of  IGR~J17354$-$3255 shows a moderate orbital
modulation and a dip whose nature we investigated by comparing the X-ray light
curve with the prediction of the Bondi-Hoyle-Lyttleton accretion theory,
assuming both spherical and non spherical symmetry of the outflow from the donor star.
We found that dip cannot be explained with the X-ray orbital modulation.
We propose that an eclipse or the onset of a gated mechanism are the most likely
explanations for the observed light curve.

In the following we present some recent observational results obtained through
our outburst follow-ups.
As fitting examples of the exceptional capabilities of {\it Swift} in catching
bright flares and monitor them panchromatically, we report on the
datasets of the candidate SFXT  IGR J16328\-$-$4726 and the
confirmed SFXT AX J1845.0\-$-$0433,
that went into outburst on 2009 June 10 \citep{Grupe2009:16328-4726}
and 2012 May 05 \citep{Romano2012:atel4095}, respectively.

         \section{Data reduction\label{cospar12:dataredu}}

The new XRT data were processed with standard procedures
({\tt xrtpipeline} v0.12.6), filtering and screening criteria,
within {\tt FTOOLS} in the {\tt HEASOFT} package (v.6.12).
For the monitoring campaigns we generally considered photon-counting (PC) data only,
and selected event grades 0--12 (\citealt{Burrows2005:XRT}); the outburst light
curves generally start off with windowed timing (WT) data, instead,
from which we selected event grades 0--2.
Source events were accumulated within an annular/circular region
(depending on whether pile-up correction was required or not, respectively)
with an outer radius of 20--30 pixels, depending on source brightness;
background events were accumulated from source-free regions.
For our spectral analysis, we extracted events in the same regions as
those adopted for the light curve creation;
ancillary response files were generated with {\tt xrtmkarf},
to account for different extraction regions, vignetting, and PSF corrections.

The BAT data of the outbursts were analysed using the standard BAT analysis
software within {\tt FTOOLS}.
Mask-tagged BAT light curves were created in the standard energy bands
and rebinned to either achieve a signal-to-noise ratio (S/N) of at least 5
or a 50-s integration time.
Survey data products, in the form of Detector Plane
Histograms (DPH), were analysed with the
standard {\tt batsurvey} software.
BAT mask-weighted spectra were extracted during several time intervals;
an energy-dependent systematic error vector was applied and
response matrices were generated with {\tt batdrmgen}.

We derive astrometrically corrected X-ray positions by
using the XRT-UVOT alignment and matching to the
U\-SNO\--B1 catalog \citep[][]{Monet2003:USNO_mn}
as described in
\citet{Goad2007:xrtuvotpostions} and \citet{Evans2009:xrtgrb_mn}\footnote{
\href{http://www.swift.ac.uk//user_objects/}{http://www.swift.ac.uk//user\_objects/}}.

Fig.~\ref{cospar12:fig:campaigns} shows all available data on the 4 SFXT
monitored in 2007--2009 in the 0.2--10\,keV band.
While some were previously published in
\citet[][]{Romano2009:sfxts_paperV,Romano2011:sfxts_paperVI,Romano2011:sfxts_paperVII,Romano2013:MI50x_sfxts}
and \citet{Farinelli2012:sfxts_paperVIII},
the data in red are presented here for the first time, and are updated to the end of 2012.

Fig.~\ref{cospar12:fig:best_sfxts} shows the light curves of the most representative outbursts of
confirmed SFXTs (panels a--h) and candidate SFXTs (panels i--l), that we
followed with {\it Swift}/XRT for a few days after the BAT trigger through ToO observations.
Red data points,
the XRT light curves of outbursts the confirmed SFXT AX~J1845.0-0433 and candidate SFXT IGR~J16328$-$4726
(panels h and i),  refer to observations presented here
for the first time, while grey points indicate data presented elsewhere.

         \section{IGR~J16328$-$4726\label{cospar12:16328}}

\begin{figure}[t]
\begin{center}
\vspace{-0.7truecm}
\centerline{\includegraphics*[angle=0,width=8.5cm]{figure4.ps}}
\end{center}
\vspace{-1.5truecm}
\caption{2009 June 10 outburst of \src: XRT and BAT light curves
of the first day of data, in units of count s$^{-1}$ and count s$^{-1}$ detector$^{-1}$, respectively.
The empty (blue) circles correspond to BAT in event mode data,
filled  (blue) circles to BAT in survey mode data.
}
\label{cospar12:fig:16328lcv_xrtbatbands}
\end{figure}

IGR~J16328$-$4726 \citep{Bird2010:igr4cat,Baumgartner2010:BAT58mos,Cusumano2010:batsur_III}
is considered a candidate SFXT,
based on its history of hard X-ray activity characterized by short flares
lasting up to a few hours \citep{Fiocchi2010:16328-4726}, and a lack of confirmed counterpart,
with an
orbital period of $10.076\pm0.003$\,d \citep{Corbet2010:16328-4726}.

Following the BAT trigger of \src\ on 2009 June 10 at 07:54:27  UT
\citep[image trigger=354542,][]{Grupe2009:16328-4726},
\sw\ executed an immediate slew, so
XRT data are available which are simultaneous with the BAT data.

Using 7818\,s of XRT Photon Counting mode data and 18 UVOT images,
we find an astrometrically corrected X-ray position:
    RA(J$2000)$ = $16^{\rm h} 32^{\rm m} 37\fs87$,
    Dec(J$2000)=-47^{\circ} 23^{\prime} 41\farcs2$
with an uncertainty of 1\farcs4 (90\,\% c.l.).
The XRT position is $0\farcs51$ from 2MASS~J16323791$-$4723409,
the most likely optical counterpart.
This is the best currently available X--ray position for this source.

Fig.~\ref{cospar12:fig:16328lcv_xrtbatbands} shows the 0.3--4\,keV and 4--10\,keV
light curves and the 4--10/0.3--4 hardness ratio of the 2009 June 10 outburst
during the initial bright phase.
The remainder of the XRT data (see Fig.~\ref{cospar12:fig:best_sfxts} panel i)
show that the count rate decreases from about 3 counts s$^{-1}$ (first orbit)
by a factor of 10 during the first 20\,ks of observations.
During the following two days, the source was observed at about
0.1 count s$^{-1}$, thus providing us with a dynamic range of $\approx 40$.
The last two observations only yield 3$\sigma$ upper limits at $1.4 \times 10^{-2}$
counts s$^{-1}$ and $4.5\times10^{-3}$ counts s$^{-1}$, so that the overall dynamic
range reaches at least 650.
While this dynamic range is lower than the 4--5 orders of magnitude observed in ``classical''
\citep{Chaty2010arXiv1012.2318C} SFXTs (such as IGR~J17544$-$2619 and XTE~J1739$-$302),
it nonetheless places \src\ in the typical range for intermediate SFXTs
(e.g., IGR J18483\-$-$0311 and IGR J16418\-$-$4532, \citealt[][]{Romano2010:sfxts_18483,Romano2012:sfxts_16418}).
Fig.~\ref{cospar12:fig:best_sfxts} (panel i) shows several flares, as also typical
of the SFXT behaviour after the initial bright flare.
We note that \citet[][]{Bozzo2012:HMXBs} reported on a 22\,ks \xmm\
observation performed on 2011 February 20, in which they observed the source in
a flux state slightly fainter that the one observed during the outbursts
(unabsorbed $F_{\rm 2-10\,keV}=1.7\times10^{-11}$  erg cm$^{-2}$ s$^{-1}$) also
characterized by luminosity variations by a factor of 10.

 \begin{table}
 \begin{center}
 \caption{Spectral fits of simultaneous XRT and BAT data of \src. POW: absorbed powerlaw. CPL: cutoff powerlaw, energy cutoff E$_{\rm c}$ (keV).
    HCT: absorbed powerlaw, high energy cutoff E$_{\rm c}$ (keV), e-folding energy E$_{\rm f}$ (keV).
Absorbing column density is in units of $10^{22}$ cm$^{-2}$. }
 \label{cospar12:tab:16328broadspec}
 \begin{tabular}{lrrrrr}
 \hline
  \noalign{\smallskip}
Model   & $N_{\rm H}$   &$\Gamma$  &$E_{\rm c}$  &$E_{\rm f}$  &$\chi^{2}_{\nu}$/dof \\
  \noalign{\smallskip}
 \hline
 \noalign{\smallskip}
POW &$12.3_{-1.9}^{+2.3}$ &$1.66_{-0.32}^{+0.32}$ &               &                       &$1.38/51$ \\
CPL &$8.4_{-1.9}^{+2.2}$ &$0.60_{-0.48}^{+0.50}$ &$19_{-7}^{+15}$ &                        & $1.09/50$\\
HCT &$8.8_{-1.8}^{+2.1}$ &$0.93_{-1.79}^{+2.12}$ &$<28$ &$20_{-8}^{+16}$          & $1.09/49$ \\
 \noalign{\smallskip}
  \hline
  \end{tabular}
  \end{center}
  \end{table}

Fig.~\ref{cospar12:fig:16328lcv_xrtbatbands}  also shows
the BAT light curves during the brightest part of the 2009 June 10 outburst
in the 15--25\,keV and 25--50\,keV energy bands.
The source is not detected above $\sim 70$\,keV.

We extracted the mean BAT mask-weighted spectrum
during the first orbit of data of the 2009 June 10 outburst
and fit it in the 15--70\,keV energy band with a simple
power law. We obtained
$\Gamma_{\rm BAT}=2.6\pm0.4$ ($\chi^2_{\nu}=1.235$, 37 degrees of freedom, dof), and
a 20--50\,keV flux of  $7.1\times10^{-10}$ erg cm$^{-2}$ s$^{-1}$.
We extracted the mean XRT spectrum of the brightest X-ray emission
(obs.\ 00354542000, first orbit $T+$404--1036\,s, 632\,s net exposure,
hereafter
`000orb1'), and
fit it in the 0.5--10\,keV energy band with an absorbed power-law model
by adopting \citet{Cash1979} statistics.
We modelled the absorption ({\tt tbabs} in {\tt xspec}) with the abundance
set to the values given by \citet{Wilms2000}.
We obtained a column of $N_{\rm H}=9_{-3}^{+4}\times10^{22}$\,cm$^{-2}$
(in excess of the Galactic one,
$N_{\rm H}^{\rm Gal}=1.54\times 10^{22}$\,cm$^{-2}$; \citealt{LABS}),
a photon index $\Gamma=0.65_{-0.64}^{+0.69}$
(Cash statistics 618.3, 76\,\% of $10^4$ realizations with
statistics in excess of Cstat), and
2--10\,keV observed and unabsorbed fluxes of
$F_{\rm 2-10\,keV}^{\rm obs}=2.9\times10^{-10}$\,erg\,cm$^{-2}$ s$^{-1}$
and $F_{\rm 2-10\,keV}$ $=  4.2\times10^{-10}$\,erg\,cm$^{-2}$ s$^{-1}$, respectively.
Assuming a distance of 10\,kpc
for the luminosity calculation, we obtained $L_{\rm 2-10\,keV}=5\times10^{36}$ erg\,s$^{-1}$.

\begin{figure}[t]
\begin{center}
\vspace{+0.4truecm}
\centerline{\includegraphics[angle=270,width=8.5cm]{figure5.ps}}
\end{center}
\caption{Broad-band spectroscopy of the 2009 June 10 outburst of \src.
		Top: simultaneous XRT/PC (filled red circles) and BAT (empty blue circles) data
			fit with the {\tt cutoffpl} model.
		Bottom: the residuals of the fit (in units of standard deviations). }
\label{cospar12:fig:16328meanspec}
\end{figure}

 Similarly, the mean XRT spectrum, extracted from the whole first observation
(obs.\ 00354542000, $T+$404--18,\,375\,s, 8181\,s net exposure, hereon `000') and
rebinned with a minimum of 20 counts bin$^{-1}$
to allow $\chi^2$ fitting, yielded
$N_{\rm H}=9.0_{-1.8}^{+2.2}\times 10^{22}$ cm$^{-2}$,
and   $\Gamma=0.96_{-0.37}^{+0.41}$
($\chi^2_{\nu}=1.07$, 41 dof).
The 2--10\,keV observed and unabsorbed fluxes are
$F_{\rm 2-10\,keV}^{\rm obs}=(5.6_{-2.7}^{+0.3})\times10^{-11}$ erg cm$^{-2}$ s$^{-1}$
and $F_{\rm 2-10\,keV}=(8.3_{-1.6}^{+0.4})\times10^{-11}$ erg cm$^{-2}$ s$^{-1}$,
respectively; this corresponds to a luminosity
$L_{\rm 2-10\,keV} = 1\times10^{36}$ erg s$^{-1}$.

In order to perform broad-band spectroscopy of the 2009 June 10 outburst,
we matched the BAT spectrum with the `000' XRT one.
We note that the chosen spectra are not strictly simultaneous, as they
span the first and the first 4 orbits of data, respectively.
The XRT `000' spectrum, however, offers the advantage of higher S/N than
the strictly simultaneous `000orb1', and a consistent photon index,
despite a decrease in average flux by a factor of $\sim 5$.
Therefore, constant factors were included in the fitting to allow for
both normalization uncertainties between the two instruments (generally
constrained within 10\,\%) and normalization differences due to the non
strict simultaneity of the XRT and the BAT data.
We considered models that are generally used to describe the X--ray emission
from accreting pulsars in HMXBs. i.e., a simple absorbed power-law,
an absorbed power-law with an exponential cut-off ({\tt cutoffpl} in {\tt xspec}),
and an absorbed power-law with a high energy cut-off ({\tt highecut}).
We performed joint fits in the 0.5--10\,keV, 15--70\,keV
energy bands for XRT and BAT, respectively.
Our results are reported in Table~\ref{cospar12:tab:16328broadspec}.
The simple power-law model yields a clearly unsatisfactory fit.
The absorbed power-law with a high energy cut-off yields a poorly constrained
value of the cut-off energy. The absorbed power-law with an exponential cut-off,
on the other hand, yields a very good fit
($\chi^{2}_{\nu}$/dof$=1.09/50$; see Fig.~\ref{cospar12:fig:16328meanspec}),
with $N_{\rm H}=(8\pm2)\times 10^{22}$ cm$^{-2}$,  $\Gamma=0.60_{-0.48}^{+0.50}$,
and a high-energy cut-off at $E_{\rm c}=19_{-7}^{+15}$ keV.

         \section{AX~J1845.0$-$0436\label{cospar12:18450}}

 \begin{table}
 \begin{center}
 \caption{Spectral fits of simultaneous XRT and BAT data of AX~J1845.0$-$0433.
POW: absorbed powerlaw. CPL: cutoff powerlaw, energy cutoff E$_{\rm c}$ (keV).
    HCT: absorbed powerlaw, high energy cutoff E$_{\rm c}$ (keV), e-folding energy E$_{\rm f}$ (keV).
Absorbing column density is in units of $10^{22}$ cm$^{-2}$.
}
\vspace{9pt}
 \label{cospar12:tab:18450broadspec}
 \begin{tabular}{lrrrrr}
 \hline
  \noalign{\smallskip}
 Model   & $N_{\rm H}$   &$\Gamma$  &$E_{\rm c}$  &$E_{\rm f}$  &$\chi^{2}_{\nu}$/dof \\
  \noalign{\smallskip}
 \hline
 \noalign{\smallskip}
POW & $2.0_{-0.4}^{+0.5}$ & $1.20_{-0.25}^{+0.26}$   &                      &                         & $1.24/78$ \\
CPL  & $1.3_{-0.3}^{+0.4}$  & $0.56_{-0.25}^{+0.26}$  & $17_{-5}^{+8}$ &                        & $0.79/77$\\
HCT & $1.2_{-0.3}^{+0.4}$  & $0.60_{-0.21}^{+0.31}$  &$<19$  & $18_{-5}^{+8}$   & $0.78/76$ \\
 \noalign{\smallskip}
  \hline
  \end{tabular}
  \end{center}
  \end{table}

AX~J1845.0$-$0433/IGR J18450$-$0435
\citep{Bird2010:igr4cat,Baumgartner2010:BAT58mos,Cusumano2010:batsur_III}
was discovered in ASCA data \citep[][]{Yamauchi1995:1845} as a source
variable on timescales of tens of minutes and classified as a SFXT
\citep[][]{Sguera2007:18450} with an O9.5I companion \citep[][]{Coe1996:18450,Zurita2009:1845}.

AX~J1845.0$-$0433 triggered the BAT on 2012 May 05 at 01:44:39 UT\footnote{
Previously, {\it Swift} caught a flare from this source on 2005 November 4
and 2009 June 28 \citep{Romano2009:atel2102}.
The historical light curve from the BAT hard X-ray transient monitor can be found at
\href{http://swift.gsfc.nasa.gov/docs/swift/results/transients/weak/IGRJ18450-0435/}{http://swift.gsfc.nasa.gov/docs/swift/results/transients/weak/}.
}   \citep[image trigger=521567,][]{Romano2012:atel4095}.
\sw\ slewed to the target immediately, so that the XRT began observing the field about
423\,s after the trigger.

To obtain an arcsecond level position of this source,
we used the first 2775\,s PC mode data and, by correcting for the astrometric
errors by utilizing Swift/UVOT data,
we found
    RA(J$2000)=18^{\rm h} 45^{\rm m} 01\fs58$,
    Dec(J$2000)= -04^{\circ} 33^{\prime}  57\farcs4$,
with an estimated error of 1\farcs4 radius (90\,\% c.l.).
The XRT position is $2\farcs2$ from  the most likely optical counterpart proposed by
\citet[][$\sim 1^{\prime\prime}$ error]{Coe1996:18450},
and it is the best currently available X--ray position for this source since
\citet[][ based on {\it XMM-Newton}]{Zurita2009:1845}  reports a localization  with an error of $2^{\prime\prime}$.

We extracted the mean BAT mask-weighted spectrum  (T$-$239 to T$+$963\,s; 1202\,s net exposure)
during the first orbit of data and fit it in the 15--70\,keV energy band with a simple
power law. We obtained
$\Gamma_{\rm BAT}=2.4\pm0.4$ ($\chi^2_{\nu}=0.9$, 24  dof),
and a 15--70\,keV flux of  $1.7\times10^{-9}$ erg cm$^{-2}$ s$^{-1}$.

\begin{figure}[t]
\begin{center}
\vspace{+0.4truecm}
\centerline{\includegraphics[angle=270,width=8.5cm]{figure6.ps}}
\end{center}
\caption{Broad-band spectroscopy of the 2012 May 05 outburst of AX~J1845.0$-$0433.
		Top: XRT/PC (filled red circles) and BAT (empty blue circles) data
			fit with the {\tt cutoffpl} model.
		Bottom: the residuals of the fit (in units of standard deviations). }
\label{cospar12:fig:18450meanspec}
\end{figure}

Figure~\ref{cospar12:fig:best_sfxts} (panel h) shows the XRT light curve that we followed for a total of 18 days.
In the XRT AX J1845.0 $-$0433 reached an initial peak at about 20 count s$^{-1}$ at T$+$1000\,s, immediately
followed by several more flares.
The following day, the source was not detected (3$\sigma$ upper limit at about $2.4\times10^{-2}$ count s$^{-1}$),
and in the following days, it showed several more flares.
The overall dynamic range therefore reaches at least 750 which places AX~J1845.0$-$0436
neatly in the typical SFXT range.
The initial XRT/WT spectrum (T$+$429 to T$+$846\,s; 417\,s net exposure) can be fit with
an absorbed power law, with a photon index of $\Gamma=1.3\pm0.1$, and an absorbing column density
of $N_{\rm H}=(1.8_{-0.2}^{+0.3}\times 10^{22}$ cm$^{-2}$,  in slight excess of the Galactic value
of $1.30\times 10^{22}$ cm$^{-2}$,  \citealt{LABS}).
The mean flux is $F_{\rm 2-10\,keV}=7\times10^{-10}$ erg cm$^{-2}$ s$^{-1}$ (unabsorbed).
The XRT/PC spectrum (T$+$848 to T$+$1891\,s; 1043\,s net exposure)
shows a power law shape with $N_{\rm H}=(1.4_{-0.3}^{+0.4})\times 10^{22}$ cm$^{-2}$,
$\Gamma=0.8\pm0.2$
and an average flux of $F_{\rm 2-10\,keV}=8\times10^{-10}$ erg cm$^{-2}$ s$^{-1}$  (unabsorbed).
These fluxes translate into a luminosity of $L_{\rm 2-10\,keV} = 1\times10^{36}$ erg s$^{-1}$
\citep[assuming the optical counterpart distance of 3.6\,kpc, ][]{Coe1996:18450}, comparable
with the one observed in previous outbursts of this source \citep[][]{Sguera2007:18450,Zurita2009:1845}.

We fit the nearly simultaneous BAT and XRT/PC spectra
in the 0.5--10\,keV and 15--70\,keV energy bands for XRT and BAT, respectively,
with the same models as those used for \src.
Our results are reported in Table~\ref{cospar12:tab:18450broadspec}.
The simple power-law model yields a clearly unsatisfactory fit, showing systematic residuals
that indicate the need for a curved spectrum.
The absorbed power-law with a high energy cut-off yields a poorly constrained
value of the cut-off energy. The absorbed power-law with an exponential cut-off,
on the other hand, yields a better fit
(see Fig.~\ref{cospar12:fig:18450meanspec}),
with $N_{\rm H}=(1.3_{-0.3}^{+0.4})\times 10^{22}$ cm$^{-2}$,  $\Gamma=0.56_{-0.25}^{+0.26}$,
and a high-energy cut-off at $E_{\rm c}=17_{-5}^{+8}$ keV.
These results are consistent with those of \citet[][]{Sguera2007:18450}
and \citet[][]{Zurita2009:1845} both in terms of overall luminosity of the outbursts
and detailed spectral parameters.

\section{Conclusions and Future Perspectives}

In this paper we have given a review of our {\it Swift} SFXT Project, its underlying observing
strategy and its advantages.
Given the shape of the SFXT spectrum,  broad band spectroscopy with {\it Swift} (0.3--150\,keV)
generally allows us to both model the hard-X spectral properties
and to measure the absorption. Furthermore, we can use our detailed light curves to determine the
overall dynamic range, a discriminant between outbursts of classical sgHMXBs and SFXTs.

We used two recent outbursts to highlight the typical results of our activity.
\src\ is considered a candidate SFXT, based on its recorded history of flaring activity
and lack of a confirmed counterpart.
Our evidence, based on \sw\ data, points towards an intermediate SFXT classification.
The temporal and spectroscopic properties of this source,
including the high peak luminosities, the large dynamic range, and the length (days) and flaring
nature of the X--ray outburst are strongly reminiscent of those of the prototypes of the SFXT class.
AX~J1845.0$-$0436, on the other hand, is a confirmed SFXT with a well-known optical companion.
Our \sw\  simultaneous broad band spectroscopy allows us to obtain a good fit with
an absorbed flat power-law with an exponential cut-off at $\sim 18$\,keV,
as is typical for wind-fed HMXBs.
In Fig.~\ref{cospar12:fig:best_sfxts} we draw a comparison among the best light curves
of outbursts of confirmed SFXTs and candidate SFXTs, as caught during
our monitoring campaigns with \sw. Similarly to the observations for
all confirmed SFXTs, the outburst of \src\  (hence, in the SFXT framework,
the length of the accretion phase) lasts a few days.
In particular, we show for the first time, a long monitoring of AX~J1845.0$-$0436
after an outburst, also showing remarkable activity for several days, at least.
Furthermore, in both cases we also observed
the multiple-peak structure of the light curve that can now be considered a defining
characteristic of the SFXT class, which is likely due to inhomogeneities in the accretion flow
\citep[e.g.][]{zand2005}
and/or unstable accretion due to the spin and magnetic field of the compact object
\citep[][]{Grebenev2007,Bozzo2008}.

Currently the Project is catching bright flares at the rate of several per year,
that we follow with XRT for at least one week (often longer if previously not observed in the soft X--rays)
through ToO observations through the {\it Swift} GI program (PI: P.\ Romano) and regular ToOs.
We aim at observing bright flares of the remaining candidate SFXTs in order to localize them to the arcsecond level and
identify their optical/infrared companion,
as well as the remaining SFXTs for which no soft X--ray observations are
available, yet.
At the time of writing long term monitoring campaigns are still ongoing to systematically
study the out-of-outburst behaviour of the whole SFXT class.

\section{Acknowledgements}

We thank the \sw\ team duty scientists and science planners
and the remainder of the \sw\ XRT and BAT teams,
S.\ Barthelmy in particular, for their invaluable help and support.
We also thank D.~Grupe and M.M.~Chester for helpful discussions.
{We also thank the anonymous referees for their insightful comments.
We acknowledge financial contribution from the agreement ASI-INAF I/009/10/0
and from contract ASI-INAF I/004/11/0.
This work made use of the results of the Swift/BAT hard X-ray transient monitor: \\
\href{http://swift.gsfc.nasa.gov/docs/swift/results/transients/}{http://swift.gsfc.nasa.gov/docs/swift/results/transients/} \\
and of data supplied by the UK Swift Science Data Centre at the University of Leicester.

redpajama_set_name: RedPajamaArXiv


Not too short and not too long, we're loving these shorts! Dress them up with a blouse and wedges or dress them down with a tank and flops. Folded hem and patched back pockets. 17" in length with a 9" inseam. Cotton Blend. Imported.


text:
Q: Shooting game Help I'm making a shooting game like Space Invaders. Every time I launched the missile, it's always on the same position. How will I change it depending on the place where the spaceship is.
Here's my codes for now.
class GraphicsApplication
{

    private Form f;
    private PictureBox pb;
    private PictureBox pb1;
    private PictureBox pb2;
    private Boolean bMove;
    Timer Clock = new Timer();
    Timer Missile = new Timer();
    int x = 0;

    public GraphicsApplication()
    {
        f = new Form();

        pb = new PictureBox();
        pb1 = new PictureBox();
        pb2 = new PictureBox();

        bMove = false;
    }

    public void Launch()
    {
        f.Size = new Size(600, 600);
        f.StartPosition = FormStartPosition.CenterScreen;

        f.KeyDown += new KeyEventHandler(f_KeyDown);
        f.KeyPress += new KeyPressEventHandler(f_KeyPress);

        pb.SetBounds(300, 470, 70, 70);
        pb.Image = new Bitmap("spaceship.png");
        pb.SizeMode = PictureBoxSizeMode.StretchImage;
        f.Controls.Add(pb);

        pb1.Image = Image.FromFile("spacedisc.png");
        pb1.SetBounds(20, 20, 130, 80);
        pb1.SizeMode = PictureBoxSizeMode.StretchImage;
        f.Controls.Add(pb1);

        pb2.Image = Image.FromFile("missile.png");
        pb2.SetBounds(pb.Location.X, pb.Location.Y, 25, 40); //pb2 missile //pb spaceship
        pb2.SizeMode = PictureBoxSizeMode.StretchImage;

        Clock = new Timer();
        Clock.Interval = 40;
        Clock.Start();
        Clock.Tick += new EventHandler(Clock_Tick);

        Missile = new Timer();
        Missile.Interval = 40;
        Missile.Tick += new EventHandler(Missile_Tick);
        f.ShowDialog();

    }

    private void f_KeyDown(object sender, KeyEventArgs e)
    {
        if (e.KeyCode == Keys.Space)
        {
            Missile.Start();
        }
    }

    public void Missile_Tick(object sender, EventArgs e)
    {
        if (bMove == true)
        {
            f.Controls.Add(pb2);
            pb2.Top = pb2.Top -= 5;
        }

    }

    private void f_KeyPress(object sender, KeyPressEventArgs e)
    {
        if (e.KeyChar == 'd')
        {
            pb.Left = pb.Left += 5;
        }
        if (e.KeyChar == 'a')
        {
            pb.Left = pb.Left -= 5;
        }
    }

    public void Clock_Tick(object sender, EventArgs e)
    {
        if(x == 400)
        {
           bMove = true;
        }
        else if (x == 30)
        {
            bMove = false;
        }

        if (bMove == false)
        {
            x += 5;
            pb1.Location = new Point(20 + x, 20);
        }
        else
        {
            x -= 5;
            pb1.Location = new Point(x - 20, 20);
        }
    }
 }
 }

A: You probably want something like
pb2.Location.X = pb.Location.X;
pb2.Location.Y = pb.Location.Y;

in your f_KeyDown() function, so that the missile starts in the same location as the spaceship.

A: You have to position your bullets, rockets...etc. relative to your space ship's gun.
Imagine a gun that is mounted on the ship. You could represent this gun with an object.
For example:
public class Gun
{
    private ISpaceshipDesign _spaceshipDesign;

    public Gun(ISpaceshipDesign spaceshipDesign)
    {
        this._spaceshipDesign = spaceshipDesign;
    }

    public void Fire()
    {
        //...
    }
}

Pass in a reference to your spaceship when creating the gun, so that you know onto which spaceship the gun is mounted.
The spaceship should always know where it is in the 2D-plane (X, Y coördinates). It should also know where on the spaceship the gun is mounted.
public interface ISpaceshipDesign
{
    public Point GunLocation { get; }
}

The GunLocation property must return the gun's location relative to the ship's current position. For example:
public Point GunLocation
{
    get
    {
        double x = (double) this.GetValue(Canvas.LeftProperty) + 21;
        double y = (double) this.GetValue(Canvas.TopProperty) + 17;
        return new Point(x, y);
    }
}

You can then access this data in the Gun's Fire() method.
For example:
public void Fire()
{
    Point gunLocation = _spaceshipDesign.GunLocation;

    // Position your missle using the gun's current coördinates (X, Y).
}

About a year ago I wrote a 10-series part about creating a similar game (Asteroids) in Silverlight. One article discusses how to make the gun fire. You can find it here:
https://github.com/geersch/SilverlightAsteroids/blob/master/src/part-6/README.md
You can choose to mount several guns on the ship, one that fires regular bullets, another one for missles...etc. Each gun would have a different location on the ship. You can alter the Fire() method to be triggered by different keys (A = missle, space = bullets).
Hope this helps.


Filipino Librarian: Library Assistant as Murderer?
PRIEST: For five years, Benny's been Professor Chavez's assistant. Usually small things: cleaning, sweeping, keeping the library organized. Benny had an unusual mastery about the Dewey Decimal System.
Benny is also the primary suspect in the murder of Professor Chavez in QWERTY, a 5-minute film by Paolo Dy that has been entered in the new filmmaking reality show "On the Lot."
Dy is a Filipino filmmaker. Watch the film by clicking on the image above, rate it, and tell all your friends about this film that takes a typewriter and a suspect who can't speak, and draws viewers into the mind of the murderer.


text:
Sidecar Coffee Roasters Hitches a Ride into New Digs
Howard Bryman | November 20, 2015
Rendering of the renovated Wonder Bread building. All images courtesy of Sidecar Coffee Roasters.
While foodies today prefer crusty, artisanal breads along with their craft beer and specialty coffee, there's nevertheless a lingering fondness for historic American brands like Wonder Bread, whose cheerful primary-colored packaging continues to bring back memories.
In Waterloo, Iowa, the Wonder Bread building, built in 1928 but left vacant since 2012 following the Hostess company's bankruptcy, is both a beloved monument to this fondness and a fixture of the local cityscape. As part of an urban redevelopment plan undertaken by the city, local beer brewer SingleSpeed Brewing Co. has received grants and other assistance to buy and carefully renovate the building. Sidecar Coffee Roasters, a frequent collaborator with SingleSpeed Brewing, is coming along for the ride.
SingleSpeed Brewing and Sidecar Coffee Roasters were both founded about three years ago. "They opened like within a week of when I opened, back in 2012," Sidecar Coffee Roasters owner Jed Vander Zanden told Daily Coffee News. "I guess they would be called a nano-brewery," said Vander Zanden, who also started his own business nano-style on a Diedrich IR-2.5 that he outgrew in a matter of months. Since then, Sidecar has grown to include two retail cafes and handful of wholesale client cafes and restaurants in the Waterloo/Cedar Falls area. Said Vander Zanden, "We're a small town, so we're able to feed off each other's energy and grow it that way."
Jed Vander Zanden
The roaster and the brewer have collaborated on a number of coffee beers over the years. Some are straightforward, like a brown-and-coffee ale, while others have been a bit more involved, such as an oak-chipped imperial stout that incorporated whiskey barrel-aged coffee. "We always have at least one of the coffee beers on tap at the tap room," said Vander Zanden.
Meanwhile, in the midst of its growth, Sidecar's coffee roasting production has remained inside the same "roasting studio" in which it started, a 600-square-foot space now cramped for the scale of the business. If all goes well, the Sidecar roastery will be relocated and up and running in the Wonder Bread building by the summer of 2016.
Vander Zanden said that while having more space to store larger green coffee orders through Cafe Imports and other importers will facilitate a confident push for more wholesale activity, the growth will continue to take place organically. "For now, the IR-12 is still fine," said Vander Zanden, who said that when the time comes for another upgrade perhaps a year or two from now, he would likely keep the 12 for smaller batches of higher-end coffees in lower demand, and order a new Diedrich IR-25 for general production. "There's enough space for both," said Vander Zanden. "That might not happen for another year or two, or ever. But if I needed extra capacity, it would be an easy fit."
When Hostess was acquired by Flowers Foods, an operational scale-back left various facilities dormant, which resulted in other old buildings being torn down in other towns. "They had plans to do various things, either build condos, or tear it down, make a parking lot," said Vander Zanden of the Wonder Bread building. "But the community really wanted to keep that building there." A public outcry prevented any destruction of the building, which is now poised to enjoy a second life in what Vander Zanden describes as "transitional" neighborhood for which city planners have designs. "Right now there's not a ton of housing or other stuff in that exact neighborhood," said Vander Zanden, "but there's the groundwork for it to become the cultural center of Waterloo."
The Wonder Bread building is central to those revitalization plans. "[SingleSpeed]'s goal is to have the building restored to historical standards," said Vander Zanden of the overall buildout. This will entail the preservation and exposure of original brick work, vintage wood floors and an interesting wood ceiling, restoring window openings, keeping the classic Wonder Bread signage on the outside, and more. At the same time, SingleSpeed Brewing aims to update the building to the highest potential of modern environmental sustainability, aiming for LEED-certification, solar power additions, and more. "It's going to be a cool hybrid," said Vander Zanden. "It's going to feel like a brand new building, but it's going to look back to the traditional old standard of when it was built, which I think is super cool."
Another upcoming upgrade for Sidecar is a new coffee packaging label printer that will open new pathways for communication with consumers. "For me it's sort of a small big deal," said Vander Zanden, as Sidecar's original printers were only capable of a few basic objects like the logo and the name of the coffee, but not much by way of more finely-printed specifics. "It was really an opportunity lost. This is an opportunity to share a heck of a lot more information about the coffee with the customers."
Inside the new space.
The Sidecar portion of the Wonder Bread building will include a casual, open space for seating, with a bar that resembles a scaled down version of the company's other two retail locations. Vander Zanden imagines at least a La Marzocco Linea and a pourover station, along with light grab-and-go pastries. The SingleSpeed Brewery project will involve a full-service brewpub, with an open kitchen and potentially also a bakery—although probably not of the vitamin-enriched, sliced white variety.
Howard Bryman
Howard Bryman is the associate editor of Daily Coffee News by Roast Magazine. He is based in Portland, Oregon.
Tags: beer, breweries, Cedar Rapids, Iowa, Jed Vander Zanden, Sidecar Coffee Roasters, Single Speed Brewing, Waterloo, Wonder Bread


100% cotton. Price is per metre. Hot pink background with darker pink stripes to form a check. The darker pink stripes have little smudges of black dots at various places along the stripe.The Centre of the check (the paler hot pink section) is 5cm, 1 full pattern (hot pink centre plus one dark pink stripe) measures 1 cm. Candy Brights by SSI Studio.


Ascilite's 2015 conference will be held in Perth, Western Australia, and hosted by Curtin University.
See the photos from the ascilite2015 conference dinner.
The conference survey is now closed. Thanks for participating!
Follow ascilite2015 on Facebook, Twitter and Instagram, and tag your conference posts with #ascilite2015.
See registration information for ascilite2015.
See the ascilite 2015 conference schedule, handbook and proceedings.
View the sponsors for ascilite 2015.
The Conference4me smartphone app provides you with the most comfortable tool for planning your participation in ascilite2015. Browse the complete program directly from your phone or tablet and create your very own agenda on the fly. The app is available for Android, iOS, Windows Phone and Kindle Fire devices.
Download the app at http://conference4me.eu/download or type 'conference4me' in Google Play, iTunes App Store, Windows Phone Store or Amazon Appstore.
Once installed, open the app, tap on the 'Available' tab and select ascilite 2015. It will then be accessible under the 'Downloaded' tab.
Ascilite 2015 will be held at Curtin University.
Transperth's bus services 70, 72 and 75 run between the Perth CBD (including Adelaide Terrace and St Georges Terrace) and Curtin University Bus Station. Visit the Transperth website or call Transperth on 13 62 13 for all transport enquiries.
Parking at Curtin University will be free in any Green Zone (A3, A5, B2, C3, D1, D9) during Ascilite2015. Download a campus map with car parks marked [.PDF 3MB].
Accommodation options Perth has plenty of accommodation suitable for a range of budgets.
We have arranged special room rates at the following venues to accommodate a variety of budgets and individual requirements.
Accommodation Bookings are now by request basis only – please email michelle.bye@eecw.com.au with your preferred hotel, check in and check out dates as well as credit card details to secure your booking.
All room rates are in Australian dollars and include GST.
Mounts Bay Waters Apartment Hotel is situated in the secluded Mounts Bay Village; a sanctuary of landscaped gardens complemented by swimming pools, tennis courts and furnished apartments. The village is located between Kings Park and the Swan River and is the perfect vantage point from where to base your stay in Perth. With the free CAT bus service stopping right outside the village, this allows you the freedom to explore the City easily although for those who enjoy the walk, we are only ten minutes from the bustling CBD.
Each apartment has a private balcony or courtyard. All offer a large living area with a fully-equipped kitchen complete with a dishwasher and laundry facilities. The casual Courtside Restaurant is open for breakfast each morning.
One Bedroom Apartment: $220 per night per room only.
The hotel will charge the cost of the first night's accommodation as a non-refundable deposit to individual delegate's cards unless a deposit equal to the cost of the first nights' accommodation is paid to Mounts Bay Waters Apartment Hotel 30 days prior to arrival.
The balance of the cost of the accommodation is to be paid upon check in. Only one account per apartment booked will be issued. There will be no separate billing for individuals sharing an apartment.
A refundable bond or security deposit will be required at check-in and can be paid by credit card or cash.
Whether you are travelling for business or leisure, you can enjoy the convenience of having many of the city's major attractions and offices at your doorstep. The hotel is conveniently located near the greenery of Kings Park and Botanic Garden. St Georges Terrace is just around the corner as well.
Friendly service and a welcoming atmosphere give Rendezvous Hotel Perth Central a personal feel. Choose one of our 103 stylish rooms and apartments to enjoy smart accommodation that has been designed with your needs in mind.
You can expect a hassle-free stay thanks to convenient amenities and services such as 24-hour reception, a restaurant and bar, secure parking, and a gym at this hotel in Perth's CBD.
Guest Room: $175 per night per room only.
A valid credit card is required to hold the room. Any cancellations between 30 and 15 days prior to arrival is subject to 100% of the one night's accommodation charge for each room cancelled. Any cancellations 14 days or less prior to arrival is subject to entire accommodation charge for each room cancelled. No Shows are subject to entire accommodation charge.
Moments away from the river and a short walk from the city's main retail, dining and entertainment precincts, Pan Pacific Perth provides the perfect location for a relaxing and indulgent stay. Our Superior King Rooms are designed to create a refreshing and relaxing space. Stay connected with the convenience of wireless Internet access, or enjoy a good night's rest on our plush, cushion top beds. You will also enjoy complimentary access to our 24-hour Fitness Centre.
Guest Room: $225 per night per room including one breakfast. Includes GST.
A valid credit card is required to hold the room. Any rooms cancelled within 30 days prior to arrival are fully chargeable.
Our guests love the cheery mood brought about by the bright and welcoming ambience in these studio apartments that come with floor-to-ceiling windows and an open floor plan. Fully furnished serviced residence with integrated living, kitchenette and bedroom. Free WiFi, windows that can open and comprehensive entertainment system.
Studio Deluxe: $250 per room per night.
Any cancellations between 14 – 0 days prior to arrival will incur a penalty of 100% of the negotiated rate for the duration of your booking.
From the moment you arrive to the time you check out, you can be assured of the finest quality service and facilities. Comprising of 253 rooms, Novotel Perth Langley provides accommodation to meet your room requirements, including Standard Rooms, One Bedroom Apartments, Jacuzzi and Deluxe Suites both offering sweeping views of the Swan River.
Standard King Room: $239. Includes GST.
A valid credit card is required to hold the room. Cancellation/no show on day of check in will forfeit one night's accommodation deposit.
About Perth The world's most isolated capital city is a vibrant place with plenty of things to see and do.
Perth's culture and lifestyle activities range from sunny outdoor events through to an exciting nightlife complete with clubs, pubs and laneway bars – as well as a vibrant art, theatre and music scene.
In recent years, Perth has become synonymous with quality food and wine. With plenty of cafes and restaurants throughout the city and the beautiful Swan Valley right next door, there's something to satisfy every foodie and wine aficionado.
With stunning natural wonders, stretches of beaches and sunny lifestyle, Perth has something for everyone – whether you're happy to laze around in the sand or experience adrenaline-packed adventures.


A new study has revealed that 99% percent of women wouldn't want to be seen with their partner if they were wearing Speedos.
UK-based beach holiday specialist On the Beach surveyed 100 people and results showed that only one per cent of women would like to see their partner wearing budgie smugglers on the beach. Market research and data analytics firm, YouGov also named the swimming undies UK's most hated piece of clothing, even beating crocs.
Speedos were originally designed in the 1960s to reduce drag and provide freedom of movement. "No matter how ready men's beach bodies are this summer, they might not make too many friends if they stride across the sand in a pair of Speedos."
The swimming undies aren't the only despised items, with leather trousers and Crocs placing second and third for most hated.
The company Speedo has since defended their budgie smugglers, saying: "Originally designed in the 1960s to reduce drag, support and provide freedom of movement for competitive swimmers, the Speedo brief has become an iconic silhouette that transcends both the sports and fashion world."