text:
Стангерія пухнастонога (Stangeriaceae) — вид голонасінних рослин класу саговникоподібні (Cycadopsida).

Опис
Зростає кущем, менш ніж 2 м у висоту. Форми моркви підземне стебло до 20 см у поперечнику. Зріле листя 0,3–2 м в довжину, перисте, папоротеподібне, прямовисне або дугове, темно-зелене. Чоловічі шишки 10–25 см × 3–4 см, вузько циліндричні, поодинокі, вкриті короткими срібними волосками коли молоді, жовтувато-коричневі при дозріванні. Жіночі шишки 8–35 см × 6–10 см, від яйцюватих до еліпсоїдних, покриті сріблястими волосками коли молоді, темно-зелені й менш волохаті при дозріванні. Насіння 3–3,5 см × 2–2,5 см, від яйцюватої до обернено-яйцюватої форми, саркотеста (плід як у граната) пурпурно-червона при дозріванні.

Поширення, екологія
Країни проживання: Мозамбік; ПАР (капська провінція, Квазулу-Наталь). Записаний на висотах від 10 до 750 м над рівнем моря, на широтах від 26 до 33 градусів південної широти. Середньорічна кількість опадів від 750 до 1000 мм. Росте на відкритих, сухих луках, у легкій тіні під деревами в прибережній парковій зоні, або в щільних вологих низовинних лісах. Знайдено на піщаних ґрунтах (отриманих з пісковику) або іноді в гранітних або важких чорних глинах, всі злегка кислі, росте у 50 км зоні від океану.

Використання
Використовується для традиційної медицини, є також декоративне використання.

Загрози та охорона
На чисельність вплинув надмірний збір для медицини та декоративного використання. Величезна кількість рослин була знищена вздовж узбережжя провінції Квазулу-Наталь та Капської задля промисловості цукрової тростини і ананаса. Середовище проживання швидко деградує через вирубку лісів і розширення землеробства. Цей вид, перелічений у Додатку I СІТЕС. Вид зустрічається, принаймні, в 5 заказниках.

Галерея

Примітки

Джерела
 The Gymnosperm Database

Саговникоподібні
Флора Мозамбіку
Флора Південно-Африканської Республіки


Cellular mobile phone consumers could quickly be ready to select and change telcos in an immediate.
Getting a new SIM card and migrating to a new provider stays a barrier for a lot of complacent buyers who cannot be bothered switching to conserve.
But the arrival of eSIM able telephones could quickly let consumers to hook up to a rival community with out demanding a actual physical SIM card.
The most recent Apple iphone units which includes the XS and XS Max the two let a nano-SIM and eSIM to run.
The latter allows consumers to activate a program with out possessing to insert a SIM card.
But Australians telcos are nevertheless to assist this technological innovation, regardless of eSIMs presently doing work on some smartwatch units which includes the Apple View four and Samsung's Galaxy View.
The buyer watchdog, the Australian Opposition and Buyer Fee, stated intently it is observing the motion of telcos in signing up for forces with mobile phone firms to empower this new technological innovation.
"E-SIMs have the prospective to drastically market competitors in the cellular sector by facilitating buyer switching and the ACCC is checking the use of eSIMS in Australia," an ACCC spokesman stated.
Cellular mobile phone consumers use a nano-SIM — a actual physical SIM card — but to change carriers they need to have to insert yet another nano-SIM from their new provider just before generating any modifications.
Increase Cellular founder Peter Adderton questioned why mobile phone consumers even now essential a actual physical SIM card.
"The carriers do not assist eSIM due to the fact that places the energy into consumers' fingers and the buyers can go away with out possessing do to a SIM swap," he stated.
"Subscribers must be ready to transfer, if you do the ideal task and offer you the ideal program and the ideal community and give great client provider you must maintain that client.
Cellular mobile phone portability also makes it possible for consumers to maintain the exact same quantity when they change carriers.
More compact carriers make up the remaining 11 for every cent.
Telco comparison internet site WhistleOut's spokesman Joseph Hanlon stated eSIM abilities could have a drastic influence in the Australian telco market place and in the long run conserve buyers funds.
"It will truly ramp up people's consciousness of what is in the market place and who the smaller sized companies are," he stated.
Vodafone's main professional officer Ben McIntosh stated they would function with mobile phone companies to produce the eSIM functionality to market place.
"New technological innovation that presents men and women a lot more decision and adaptability is in the long run a great factor for buyers," he stated.


text:
import syntax_tree as ast
from   collections import OrderedDict

_global_symbol_table = None

class SymbolTable(object):
    """ SymbolTable contains the mapping of identifiers to types
        it can contain point to one of
        function or type
    """
    def __init__(self, parent = None):
        #TODO: remove this ugly hack
        global _global_symbol_table
        init_global_symbol_table()

        self.data     = OrderedDict()
        if parent:
            parent.children.append(self)

        self.parent   = parent if parent else _global_symbol_table
        self.children = []

    def __getitem__(self, key):
        try:
            return self.data[key]
        except KeyError as e:
            if self.parent:
                return self.parent[key]
            raise

    def __setitem__(self, key, value):
        assert(isinstance(value, (ast.Function, ast.Type, ast.Struct)))
        assert(isinstance(key, ast.Identifier))
        if key in self.data.keys():
            raise KeyError()
        self.data[key] = value

    def set_parent(self, parent):
        assert isinstance(parent, SymbolTable)
        self.parent = parent

    def __str__(self):
        out = ""
        if self.parent:
            out = str(self.parent)
        out += str(self.data) + "\n"
        return out

class ParamTable(SymbolTable):
    pass

class SubTable(SymbolTable):
    pass

def dummy_function(name, return_type_name, *args):
    return_type = ast.Type(ast.Identifier(return_type_name))
    params = []
    for i, j in enumerate(args):
        param_name = "param_{}".format(i)
        params.append(ast.Decl(ast.Type(j),
                               ast.Identifier(param_name),
                               None))

    return ast.Function(ast.Identifier(name),
                        ast.ParamList(*params),
                        return_type,
                        ast.StatementList())

def add_dummy_function(name, return_type, *args):
    _global_symbol_table[ast.Identifier(name)] = \
                dummy_function(name, return_type, *args)
def init_global_symbol_table():
    global _global_symbol_table
    if not _global_symbol_table:
        _global_symbol_table = True
        _global_symbol_table = SymbolTable()
        _global_symbol_table.parent = None
        add_dummy_function("print", "void", "int")
        add_dummy_function("prints", "void", "string")
        add_dummy_function("putc", "void", "int")

redpajama_set_name: RedPajamaGithub


It's *occasionally* been remarked upon that I tend to talk a lot. (Or, as I like to put it, why use a few words when dozens will do?) Sometimes, this is a nuisance – not only for those listening to/reading what I have to say (because there are only so many hours in a day, I get it), but also because my brain simply does not think in small phrases. One of the reasons I have yet to Tweet – despite having a Twitter account so I can follow random celebrities (especially of Harry Potter movies fame *ahem*; also Ken Jennings and Eric Stonestreet are hilarious) – is that I absolutely cannot condense anything into 140 characters. Even ordering a pizza takes me a good while.
On the other hand, being overly loquacious has sometimes come in handy, like when I'm teaching and need to fill the last few minutes of a class with anything to keep the kids occupied. I might have even won several Talk-Offs (you know, those "competitions" where you and an opponent are given random topics to discuss and whoever stops talking first loses. The word "competitions" is in quotes because, people, please), and I carry a certain swagger in my step as a result of those definitive victories.
He would write me cards for all sorts of occasions – birthdays, milestone events, just because – and, rather than gloss over them because of their lack of expanded prose, I began to see them as perfectly him: direct; to the point; honest. I called them "Dad Cards" and saved every one, tucking some of my favorites into scrapbooks and diaries.
His penmanship is not quite as clear as his message, but it all evens out in the end.
Somehow, this looks like it was Photoshopped – very weird!
The cards continued all through high school, college, and beyond, with more and more arriving for no reason at all other than that he wanted to let me know I was on his mind. A cute card, a few words (unlike the paragraphs I would write to my friends). Each time I received one, it was like a smile coming through the mail.
Just as often, he'll forward me an article from the Wall Street Journal with no preamble or additional writing at all. Although I usually understand why he's forwarded me the story (Ah, yes, a discussion of Disney Cruises), I'll sometimes have no idea if the article was meant as an encouragement or an admonishment (Wait, does he think I should be drinking Starbucks beverages daily, or is this a subtle hint that maybe I've got a problem?).
No matter, the underlying message remains the same: You're on my mind. You're awesome. And I love you.
My dad and I do talk a lot more these days than we used to when I was growing up – like, actual, for real, back-and-forth conversations. Admittedly, I'm probably responsible for 85% of the words used between us, and his responses are still short and sweet – but hey, old habits die hard. At least there's dialogue.
Still, despite our increased discourse, some of my very favorite communications – not just from my father, but from anyone on the planet – are the brief cards, emails, and voicemail messages from him that are so perfectly Dad. There's no one (at least, no one I know) who doesn't enjoy being remembered, being thought of. Far harder (for me, anyway) is actually taking the time to reach out and let that person know that they're on your mind.
I know this is a day late, Dad, but I'm thinking about you.
I am undoubtedly getting ready to say something to him.
This entry was posted in good life, thinking and talking and tagged dad, family, Father's Day, love, parenthood by missemtoo. Bookmark the permalink.


text:
Back to Press Release
New World Group and its 20 group companies are awarded as Caring Companies
Dedicated to becoming model corporate citizens
New World Development Company Limited ( "NWD", "New World Group" or the "Group", Hong Kong stock code : 17) and its 20 group companies are awarded the 2010/11 Caring Company Logo by the Hong Kong Council of Social Service today, recognizing their contribution to and outstanding performance in corporate social responsibility during the past year.
The group companies receiving the distinction are:
New World Development Company Limited
NWS Holdings Limited
K11 Concepts Limited
New World Strategic Investment Limited
New World Telecommunications Limited
New World TMT Limited
Grand Hyatt Hong Kong
Renaissance Harbour View Hotel
Hyatt Regency Hong Kong, Tsim Sha Tsui
Hong Kong Convention and Exhibition Centre (Management) Limited
Sky Connection Limited
Anway Limited
Hip Hing Construction Limited
Vibro (HK) Limited
Barbican Construction Company Limited
New World First Bus Limited
Citybus Limited
New World First Ferry Services Limited
New World First Ferry Services (Macau) Limited
CiF Solutions Limited
Urban Parking Limited
New World Group has been paying full effort in contributing to the society and actively participating in and supporting various activities of environmental protection, youth development and cultural exchange between Mainland China and Hong Kong, dedicated to building a harmonious society and cultivating talents for the community.
Since 2008, the Group has shown its continual support to "New Youth New World" Summer Internship Programme jointly organized by Hong Kong United Youth Association and more than 20 other organizations. Around 600 students were granted the opportunities to work as interns in Mainland China since then. In 2010, the Group fully supported the first "New Youth New World" Exchange Programme furthering its persistence in nurturing young talents. Exchange opportunities were provided to over 70 outstanding Mainland students to experience the Hong Kong life and culture. Besides, to encourage academic breakthrough of Mathematics students, the Group fully supported the second "New World Mathematics Awards" with an aim to encourage outstanding mathematics undergraduates, masters and PhD students of Chinese descendant to continue doing academic researches.
As a responsible corporate citizen, New World Group actively contributes to environmental protection. The Group has established the Group Environmental Committee, leading various group companies to actively formulate environmental targets and implement green measures in business. To coincide with United Nations World Environment Day on 5 June, the Group organized the first "New World Green Week" in 2010 with "carbon reduction" as the theme, dedicated to raising the environmental awareness of public and the staff. The Group also demonstrates its commitment to carbon reduction and environmental protection through continual support to "Earth Hour" organized by WWF. Various properties of the Group in Hong Kong and Mainland China turned off the lightings for an hour during the event.
To serve our community and the nation, the Group has established three volunteer teams in Hong Kong and Mainland China. Established in 2010, the "Green New World Volunteers" aims at encouraging staff members to focus on environmental issues and build an ideal community together. The Group has also organized sports and recreational activities as well as training programmes regularly to create a harmonious and ideal working environment for its staff.
K11 ATELIER King's Road Cements a New Landmark in Island East, Redefining the Design, Purpose & Culture of Workplaces
Biggest-ever New World Harbour Race to be held on 27 October 4,000 swimmers to cross Victoria Harbour on brand-new route

redpajama_set_name: RedPajamaCommonCrawl


BrainRush is a collection of fast-paced learning activities. It adapts to the individual users, providing information at just the right level to learn quickly without boredom. The mastery meter shows progress along the way, and BrainRush states "When you finish playing a BrainRush, you know the material, guaranteed." Browse the library to choose from hundreds of topics in categories including all academic subjects as well as sports and Spanish. Future improvements to the site include the promise to create your own BrainRushes. Account creation using your email and a password is required to play BrainRush games. Many activities have audio.
Share this site with students to practice and learn classroom material as well as topics they choose. Join the site yourself to share it on your interactive whiteboard or projector. Share with ESL/ELL and Special Education teachers as a resource for their students. Create a link to specific BrainRushes on your class website or blog for students to complete at home. Any student creating an account requires an email address. Read tips for safely managing email registrations here.
Learn English or Spanish through news stories. Use this site to become more fluent in Spanish or English (for ESL/ELL learners). Start by registering (with email or Facebook). Choose the language you wish to learn at the top of the screen ("English please"). Adjust other settings in your profile. You may have to click to "try" the premium version. No charge is collected for trying it, and the tools seem to all work for free. Read or listen to news articles about engaging topics. Select the type of news of interest to you. Use the audio button to listen to the story while reading. With a mouse over, a translation pops up. After learning more and more language, less translation will be necessary. Create flashcards by clicking on any difficult word. Select the level of difficulty for each word so that the word will reappear until you learn it. Stories may be in narrative or dialogue form. You can change the speed of the oral reading with a simple click. The site also offers review questions.
Encourage ESL/ELL students and Spanish learners to increase their fluency by selecting news articles that appear interesting. Have one student prepare a story each week by having him or her preview the reading, prepare the flash cards, and also write additional comprehension questions. If permitted by your administration, students can log in with Facebook (or email) and make comments about the site and/or the stories there. Be sure to review good Netiquette about online commenting.


However, Savannah proved to be full of culture.
To celebrate how far they've come, The Royal Noise has put together their debut album, "Keep on Moving," on sale now, and are having a weekend-long CD release bash, kicking things off at Huc-A Poos on Thursday, then onto their home-away-from-home Live Wire on Friday, with special guests Sincerely, Iris and Wormsloew. Then they'll wrap up the weekend with a show Saturday at Congress Street Social Club.
Harvey and his bandmates are continuing to ride the good vibes of 2011. They don't plan on slowing down any time soon.
Find out more at www.theroyalnoise.com.
Shawndra Russell can be reached via Twitter @ShawndraRussell or her blog www.shawndrarussell.blogspot.com.


text:
Елеонора Анна Джорджі (;  ) — італійська легкоатлетка, яка спеціалузіється в спортивній ходьбі, , рекордменка Європи на цій дистанції.

Спортивні досягнення

Бронзова призерка чемпіонату світу у ходьбі на 50 км (2019).

Срібна призерка (в командному заліку) командного чемпіонату світу з ходьби на дистанції 20 км (2018).

Переможниця (в командному заліку) та срібна призерка (в особистому заліку) командного чемпіонату Європи з ходьби на дистанції 35 км (2021).

Переможниця (в особистому заліку) та бронзова призерка (в командному заліку) Кубка Європи з ходьби на дистанції 50 км (2019).

Срібна призерка (в особистому та командному заліку) Кубка Європи з ходьби на дистанції 20 км (2015).

Рекордсменка Європи та Італії у дисциплінах ходьби.

Виступи на основних міжнародних змаганнях

Примітки

Джерела

 Елеонора Джорджі  — профіль на сайті Федерації легкої атлетики Італії

Італійські спортивні ходоки
Італійські легкоатлетки
Легкоатлети на літніх Олімпійських іграх 2016
Призери чемпіонатів світу з легкої атлетики
Срібні призери командних чемпіонатів світу зі спортивної ходьби
Переможці командних чемпіонатів Європи зі спортивної ходьби
Призери командних чемпіонатів Європи зі спортивної ходьби
Рекордсмени Європи з легкої атлетики
Чемпіони Італії з легкої атлетики

redpajama_set_name: RedPajamaWikipedia


text:
\section{Introduction}
 Supernovae (SNe), the core-collapse of massive stars or the thermonuclear disruption of white dwarfs,
 are rare events, occurring on average every 50 years in the Galaxy \citep{2008MNRAS.391.2009K}. However,
 only 7 Galactic SNe have been observed with historical records in the past two thousand years --
 SN 185 (RCW 86), SN 386 (G11.2--0.3), SN 1006, SN 1181 (3C58), Crab SN, Tycho SN and the Kepler SN.
 Several other records of guest stars by ancient Chinese astronomers exists. However, no solid
 identification with a known supernova remnant (SNR) has been possible for most of them so far
 \citep{2003LNP...598....7G}. Most Galactic SNe go unobserved owing to visible-band extinction by
 interstellar dust. For example SN Cas A may belong to this group. No widespread reports of Cas A exist
 in the literature of the 17th century (cf.~Hartmann et al., 1997). A more recent example is the
 youngest supernova known in our Galaxy, G1.9+0.3, which was totally missed by optical observatories
 about 100 years ago \citep{2008ApJ...680L..41R}. The majority of supernova remnants
 which have been identified so far were found in radio surveys in which the observations are
 unhampered by interstellar dust \citep[and references therein]{2009BASI...37...45G}.
 Nevertheless, the radio band is not free of selection effects. SNRs with a diameter of $<3'$ are
 difficult to identify. Only three of the 274 remnants listed in the Green catalogue fall into
 this category. In addition, most searches for SNRs focus on the Galactic plane, leaving remnants
 located at a higher galactic attitude underrepresented. Only 5 supernova remnants with $|b|>7^\circ$
 are listed in Greens catalogue. Hence, small remnants at high attitude are easily missed in
 radio surveys.

 Most SNRs emit thermal radiation when the SN blast wave expands into the surrounding interstellar
 medium (ISM), forms a shock wave at the shock front which then ionizes the atoms and increases the
 temperature to $10^6 - 10^7$ K. Therefore, the successful completion of the ROSAT All-Sky Survey (RASS)
 in the X-ray regime provided a new window for both finding SNRs and the compact objects
 that may reside within them.  The seven X-ray detected and radio-quiet Central Compact Objects which
 were associated with SNRs \citep[see][for a review]{2008AIPC..983..320G} are a good example for the
 impact on pulsar and SN science of X-ray observatories. Additionally, X-ray observations of SNRs at
 moderate spectral resolution can determine remnant properties such as shock velocities, post-shock gas
 densities and temperature as well as swept-up shell mass and overall morphology.

 The ROSAT All-Sky survey has demonstrated the potential power for finding new SNRs
 \citep{1996rftu.proc..267P, 1996rftu.proc..239B, 1994A&A...284..573A, 1996rftu.proc..233A,
 1996rftu.proc..247E,  1996rftu.proc..253F}. This has motivated \citet{1998PhDTBusser} and
 \citet{2002ASPC..271..391S} to investigate the all-sky survey data more systematically in order to
 search for unidentified supernova remnants. They analyzed RASS data in a systematic search
 for extended ($\ge 5'$) X-ray sources at Galactic latitudes ($b \le \pm 15^\circ$) by correlating
 them with databases like SIMBAD, NED, NVSS, SUMSS, DSSII, NRAO, ATNF, Parkes and Effelsberg
 radio survey data. From their candidate list several sources have been confirmed meanwhile as SNR, e.g.
 \citep{2008ApJ...674..936J, 2012MNRAS.419.2623R, 2008ApJ...681..320R, 2007MNRAS.381..377S, 2010ApJ...712..790T}.
 These identifications suggest that many of their SNR candidates are indeed radio-under-luminous, explaining
 why past radio surveys could not detect or identify them before.

 In \citet{2003PhDTSchaudel} 9 sources are listed which appear to be very
 promising SNR candidates. One of them is G308.4--1.4 designated with G308.3--1.4 in
 \citet{2002ASPC..271..391S,2003PhDTSchaudel}. Since the RASS had only an average exposure time of $\sim 400$s for sources in
 the Galactic plane the available ROSAT data do not support a detailed spectral and spatial analysis of
 these sources. However, G308.4--1.4 appears in the RASS data as a spherical center-filled X-ray source whereas
 in the Sydney University Molonglo Sky Survey (SUMSS) two radio arcs have been detected which partly overlap
 with the RASS data (see Fig. \ref{fig.rass_most}). Moreover, G308.4--1.4 is listed in the MOST supernovae
 remnant catalogue as possible SNR candidate \citep{1996A&AS..118..329W}.

\begin{figure}
  \resizebox{\hsize}{!}{\includegraphics[angle=-90, clip]{g308.4_RASS_SUMSS_1.eps}}
  \caption{ROSAT RASS $30'\times 30'$ image of G308.4--1.4 (0.1-2.4 keV) overlaid with the SUMSS image at 843 MHz
  (contour lines at 4, 8, 12, 16 and 25 mJy). The half-power beam-width of the telescope is $43''$.
  The RASS image is binned with $0.75'$ per pixel and smoothed by a Gaussian kernel of $\sigma \approx 2'$.}
  \label{fig.rass_most}
\end{figure}

 In this paper we report on the identification of G308.4--1.4 as SNR using archival data from Chandra, SWIFT,
 ATCA and WISE observatories. The results of the spatial and spectral analysis of the X-ray and radio data are
 presented in \S \ref{kap:obs_x-ray} and \S \ref{kap:obs_radio}, respectively. In \S \ref{kap:obs_multi}
 we report on data of G308.4--1.4 in other wavelength regimes. A concluding discussion about the
 identification of G308.4--1.4 and its central sources is given in \S \ref{kap:discus_concl}. Furthermore, in the
 same section we use the inferred spectral parameters of the SNR to derive an estimate for the age, the radius and the
 expansion velocity as well as the distance to the remnant. Paragraph \ref{kap:Summary} provides a summary.

\section{X-ray observations and data analysis}\label{kap:obs_x-ray}

 The SNR candidate G308.4--1.4 was observed with the Advanced CCD Imaging Spectrometer (ACIS-I) on board the Chandra X-ray
 observatory on 26th and 27th of June 2010 (obs.ID. 11249) for $\approx 15.1$ ks. All data were uncontaminated by
 soft proton flares. After dead-time correction we were left with 14.9 ks of good data. Standard processed
 data were used with up-to-date calibration applied. The reduction of the data was done with
 the Chandra Interactive Analysis software CIAO, version 4.3. For the spectral fitting we used the
 X-Ray Spectral Fitting Package (XSPEC) developed by NASA, version 12.7.0.

 In addition to Chandra we made use of the SWIFT observatory to analyze X-ray point sources detected in the central
 region of the remnant. G308.4--1.4 was observed three times with the Swift X-ray Telescope (XRT) on 17th of June 2011
 (obs.ID 00032030001), 7th (obs.ID 00032030002) and 11th of August 2011 (obs.ID 00032030003) for 3.5 ks, 4.2 ks
 and 1.3 ks, respectively. These data were reduced with the HEASOFT software package, version 6.11. For the spatial
 and spectral analysis we used the high resolution Chandra data as it contains five times more counts of G308.4--1.4.

 To calculate the error in the X-ray flux we used a public available XSPEC
 tool\footnote{\sffamily fluxerror.tcl\normalfont, see \url{http://heasarc.nasa.gov/xanadu/xspec/fluxerror.html}}.
 For the spectral analysis of the extended source emission we restricted the energy range to $0.5-4.0$
 keV as the count rate detected at higher energies is too sparse for a meaningful spectral analysis.
 Below 0.5 keV the detector and telescope response is not well established.
 In all other cases the energy range was restricted to 0.1--5 keV. All errors in this publication represent the
 1$\sigma$ confidence range for one parameter of interest, unless stated otherwise.

\subsection{Spatial analysis}\label{kap:spatial}

 Inspecting Fig.\ref{fig.chandra_rgb}, the X-ray image of G308.4--1.4 shows strong emission in the eastern part. This region has a circular shape with a diameter
 of $\sim 8.4'$. The radiation is fading towards the geometrical center of the
 source. The coordinate of the circle center is RA$_c = 13^\mathrm{h} 41^\mathrm{m} 23.9^\mathrm{s}\pm 0.7^\mathrm{s}$,
 DEC$_c = -63^\circ 43' 08''\pm 04''$ which was obtained by fitting an annulus to the outer skirts of the extended
 emission.

 Searching for point sources in a $12'\times 12'$ box around G308.4--1.4 using a wavelet source detection algorithm
 (CIAO-tool \sffamily wavdetect\normalfont) yielded a list of 21 sources.  Their position, positional error and signal-to-noise ratio
 is listed in Table \ref{tab:point_src}. The sources itself are marked in Fig. \ref{fig.chandra_rgb}. Cross-correlating
 the sources with the help of the VizieR online tool\footnote{\url{http://vizier.u-strasbg.fr/viz-bin/VizieR}} we found seven matches.
 They are included with their positional error in Table \ref{tab:point_src}.

 Eight of the detected sources are located within the extended emission of G308.4--1.4 and two of them (\# 1 and \# 10) are within
 $\approx 1$ arcmin of the geometrical center of the SNR candidate.  Source 1 is the brightest
 among all detected point sources and its designation is CXOU J134124.22--634352.0. Its position is coincident with
 2MASS J13412422--6343520. In the optical source catalogs this source has no information about its proper motion.
 Hence we cannot put better constraints on the positional coincidence of source \# 1 and the 2MASS object.
 Source 10 has no optical counterpart and is designated with CXOU J134127.12--634327.7.

\begin{table*}
\begin{footnotesize}
\caption{Detected sources in a $12'\times 12'$ box around G308.4--1.4. The sources are denoted as in Fig. \ref{fig.chandra_rgb}.}
\label{tab:point_src}
\begin{tabular}{ccccccc}
\hline\hline \\[-2ex]
Source 	& RA (J2000) 	& DEC (J2000) 	& $\delta$ RA 	& $\delta$ DEC 	& $S/N$ & optical counterpart (positional discrepancy) \\ \hline
	& h:m:s		& d:m:s		& arcsec	& arcsec	& $\sigma_G$\tablefootmark{\alpha} & \\ \hline
1	& 13:41:24.217 & -63:43:52.04 & 0.41 & 0.40 & 63.0 & 2MASS J13412422--6343520 (0.07$'$)\\
2	& 13:40:50.534 & -63:38:03.12 & 0.45 & 0.42 & 2.7 & \\
3	& 13:41:24.203 & -63:47:24.47 & 0.70 & 0.42 & 3.1 & \\
4	& 13:41:21.634 & -63:47:05.63 & 0.44 & 0.43 & 25.5 & 2MASS J13412162--6347053 (0.27$'$)\\
5	& 13:40:38.921 & -63:46:38.83 & 0.54 & 0.45 & 3.3 & 2MASS 13403887--6346384 (0.48$'$)\\
6	& 13:41:05.585 & -63:46:25.89 & 0.47 & 0.42 & 4.9 &\\
7	& 13:41:10.742 & -63:45:36.11 & 0.52 & 0.42 & 4.9 & \\
8	& 13:41:04.580 & -63:44:56.66 & 0.52 & 0.42 & 6.7 & \\
9	& 13:40:44.230 & -63:44:29.50 & 0.65 & 0.41 & 2.4 & \\
10	& 13:41:27.121 & -63:43:27.72 & 0.56 & 0.44 & 3.8 & \\
11	& 13:41:14.267 & -63:39:45.91 & 0.57 & 0.43 & 9.7 & 3UC 053--222814 (0.02$'$)\\
12	& 13:40:38.666 & -63:39:04.77 & 0.61 & 0.43 & 9.0 & 2MASS J13403862--6339044 (0.41$'$)\\
13	& 13:41:02.437 & -63:38:00.00 & 0.56 & 0.44 & 0.8 & \\
14	& 13:40:36.217 & -63:45:57.41 & 0.47 & 0.44 & 2.0 & \\
15	& 13:41:01.308 & -63:43:23.50 & 0.40 & 0.40 & 2.9 & \\
16	& 13:41:11.249 & -63:39:44.07 & 0.76 & 0.44 & 4.7 & \\
17	& 13:41:54.767 & -63:39:20.68 & 0.91 & 0.67 & 6.7 & 2MASS J13415473--6339207 (0.22$'$)\\
18	& 13:41:18.147 & -63:37:01.87 & 1.31 & 0.53 & 3.8 & \\
19	& 13:41:14.934 & -63:48:38.00 & 0.67 & 0.54 & 3.2 & \\
20	& 13:41:49.497 & -63:46:23.59 & 1.06 & 0.65 & 4.1 & \\
21	& 13:41:43.058 & -63:38:38.10 & 1.24 & 0.50 & 5.4 & 2MASS J13414304--6338371 (0.93$'$)\\
\hline\\[-1ex]
\end{tabular}
\tablefoot{
\tablefoottext{\alpha}{$\sigma_G=1+\sqrt{c_\mathrm{bg}+0.75}$, where $c_\mathrm{bg}$ are the background counts.}
}
\end{footnotesize}
\end{table*}

\begin{figure}
  \resizebox{\hsize}{!}{\includegraphics[clip]{g308.3-1.4_rgb_clip.eps}}
  \caption{Chandra ACIS-I color image of G308.4--1.4 (red 0.1-1.0 keV, green 1-1.5 keV and blue 1.5-5 keV).
  The images are binned with $1''$ per pixel and smoothed by a Gaussian kernel of $\sigma = 3''$.
  20 point sources were detected on the $12'\times 12'$ area around the center of G308.4--1.4 (c.f. Table \ref{tab:point_src}).}
  \label{fig.chandra_rgb}
\end{figure}

\subsection{Spectral analysis of G308.4--1.4}\label{kap:spec_whole_remnant}

To extract the spectra of the SNR candidate we first removed all point like
sources and then selected all photons in a circular sector with a radius of
$4.2'$ and opening angle of $\approx 136^\circ$ (see Fig. \ref{fig.chandra_rgb}).
The background spectrum was derived from all photons in an annular sector with
the same opening angle as the circular one but with the radii 5.5$'$ and 7.2$'$.
After subtraction of the background contribution (0.054 cts/pix) we were left with
11\,752 counts for the spectral analysis of the whole remnant-candidate. Additionally, the emission region of
G308.4--1.4 was divided into four separate regions which are illustrated in Fig. \ref{fig.chandra_rgb}.
The net counts are 4095 for the inner sector and 7658 for the outer shell,
as well as 4499 for the northern part of the outer shell and 3158
for the southern part. The spectrum of every single region was binned with at least
50 counts per bin. Only the spectra of the southern and northern parts of the outer rim were
binned with at least 75 counts per bin.

To fit the X-ray spectrum of G308.4--1.4 we tried various one- and two-component spectral
models. However, only a model of an absorbed collisional plasma which is in non-equilibrium and
allows a temperature evolution \citep{2001ApJ...548..820B} reproduces the energy distribution
of the extended source. In XSPEC this model is implemented as \sffamily VGNEI\normalfont.
To improve the goodness of the fit and to obtain the abundance of metals in the plasma we thawed
the parameter of every single metal and monitored the improvement of the fit statistic.

\begin{figure}
\begin{center}
\includegraphics[width=0.375\textwidth,angle=-90,clip]{remnant_spec_clip.eps}
\caption{Spectrum and fitted model of the X-ray emission of the whole remnant.}
\label{fig:spec_remnant}
\end{center}
\end{figure}

The analysis results in a best fit model with a reduced $\chi^2$ of 1.03 for 95 degrees of freedom (d.o.f.)
and a hydrogen column density $n_\mathrm{H}=1.02\pm 0.04\times 10^{22}$ cm$^{-2}$. The value for $n_\mathrm{H}$ is smaller than
the integrated hydrogen column density towards G308.4--1.4 which is $1.31\times 10^{22}$ cm$^{-2}$ \citep{2005A&A...440..775K}
and $1.45\times 10^{22}$ cm$^{-2}$ \citep{1990ARA&A..28..215D}. These values are based on HI emission line measurements at 21 cm and
therefore refer to the entire hydrogen column density in the line of sight.
The temperature of the plasma is found to be $6.3_{-0.7}^{+1.2}$ million Kelvin. The best fit was obtained when thawing the abundance in
Neon, Magnesium, Sulfur and Iron which differs significantly from the solar values: $\mathrm{Ne}=(0.72\pm 0.14)$ $\mathrm{Ne}_{\odot}$,
$\mathrm{Mg}=0.70_{-0.08}^{+0.09}$ $\mathrm{Mg}_{\odot}$, $\mathrm{S}=2.3_{-0.8}^{+0.7}$ $\mathrm{S}_{\odot}$ and $\mathrm{Fe}=0.70_{-0.12}^{+0.14}$
$\mathrm{Fe}_{\odot}$. The ionization timescale $\tau_0=t_0 N_\mathrm{e}$ ($t_0$ is the remnant's age and $N_\mathrm{e}$ the post-shock
electron number density)  is $2.7\times 10^{10}$ s/cm$^3$ and the ionization timescale-averaged temperature
$\langle kT \rangle=\int_{t_\mathrm{s}}^{t_0}T(t)N_\mathrm{e}(t)\mathrm{dt}/\tau=1.2_{-0.4}^{+2.2}$ keV ($t_\mathrm{s}$ is
the age of the shock). Thus, the unabsorbed flux of G308.4--1.4 in the energy band $0.5 - 4.0$ keV is $f_X=1.61_{-0.23}^{+0.15}\times 10^{-10}$
ergs cm$^{-2}$s$^{-1}$. The model fit and the raw spectrum are shown in Fig. \ref{fig:spec_remnant}. The fitted
parameters are listed in Table \ref{tab:spec_param}.

Adding a second plasma component which is in non-equilibrium results in $\chi^2_{red}=1.06$ for 91 d.o.f. and hence
is no improvement over a single component model. The other models we have fitted to the spectral distribution
are a hot diffuse gas model (\sffamily VMEKAL\normalfont, $\chi^2_{red}=2.92$ for 96 d.o.f.), a model for a
collisionally-ionized diffuse gas (\sffamily VAPEC\normalfont, $\chi^2_{red}=2.34$ for 96 d.o.f.)
and a thermal bremsstrahlung model ($\chi^2_{red}=7.7$ for 101 d.o.f.). Non of these models can reproduce
the spectrum of G308.4--1.4. However, all three model fits result in $n_\mathrm{H}\approx 1\times 10^{22}$ cm$^{-2}$ and a plasma
temperature of $\sim 0.5$ keV.

\subsubsection{The inner sector and the outer rim}\label{kap:part_remnant}

As mentioned in chapter \ref{kap:spec_whole_remnant} the extended source was divided into four regions. This was done
to investigate the spatial variation of the hot plasma. For the extraction of
the background spectra of the inner sector and the outer rim we used the same area on the detector as for the whole remnant.
The northern and southern region of the outer rim were analyzed separately. For the background we used only the part of this annular
sector which has the same opening angle as the source region.

First we fitted the plasma model with free $n_\mathrm{H}$. In every of the four spectral fits we found a hydrogen
column density which is in good agreement with the $n_\mathrm{H}$ of the whole remnant. Second we fitted
the spectra with a $n_\mathrm{H}$ fixed to the value of the whole remnant. The fitted value for $n_\mathrm{H}$ and
the results of the fits with a fixed column density are summarized in Table \ref{tab:spec_param}.
The spectra with the respective fits are shown in Fig. \ref{fig:spec_regions}.

\begin{table*}
\renewcommand{\arraystretch}{1.25}
\begin{footnotesize}
\caption{Spectral parameters of the best fit model for different parts of SNR G308.4--1.4.}
\label{tab:spec_param}
\begin{tabular}{cccccc}
\hline\hline \\[-2ex]
				& Whole remnant		& Inner rim		& Outer rim		& Outer rim north 	& Outer rim south \\ \hline
$n_\mathrm{H}$ [$10^{22}$cm$^{-2}$]& $1.02\pm 0.04$	&$1.05_{-0.09}^{+0.11}$ & $1.00\pm 0.05$	& $1.02\pm 0.09$	& $0.99 \pm 0.09$\\
$k_\mathrm{B}T$ [keV]		& $0.54_{-0.06}^{+0.10}$&$0.55_{-0.10}^{+0.08}$	& $0.54_{-0.05}^{+0.08}$& $0.50_{-0.06}^{+0.12}$& $0.57\pm 0.08$\\
Ne\tablefootmark{\alpha} [Ne$_{\odot}$]		& $0.72\pm 0.14$	&$0.7\pm 0.3$		& $0.73_{-0.14}^{+0.15}$& $0.5\pm 0.2$		& $0.8\pm 0.2$\\
Mg\tablefootmark{\alpha} [Mg$_{\odot}$]		& $0.70_{-0.08}^{+0.09}$&$0.80_{-0.17}^{+0.20}$	& $0.67_{-0.09}^{+0.10}$& $0.83_{-0.13}^{+0.14}$& $0.62_{-0.12}^{+0.14}$\\
S\tablefootmark{\alpha} [S$_{\odot}$]			& $2.3_{-0.8}^{+0.7}$	&$3.0_{-1.0}^{+1.9}$	& $1.7_{-0.7}^{+0.8}$	& $2.4_{-1.0}^{+1.3}$	& $-$\\
Fe\tablefootmark{\alpha} [Fe$_{\odot}$]		& $0.70_{-0.12}^{+0.14}$&$0.9\pm 0.3$		& $0.64_{-0.12}^{+0.14}$& $-$			& $0.45_{-0.15}^{+0.19}$	\\
$\tau$\tablefootmark{\beta} [$10^{10}$ s/cm$^3$]	& 2.7			& 8.1			& 2.1			& 5.2			& 2.0\\
$\langle kT \rangle$\tablefootmark{\gamma} [keV]			& $1.2_{-0.4}^{+2.2}$	& $0.72_{-0.12}^{+0.75}$& $1.4_{-0.5}^{+1.6}$	& $0.81_{-0.15}^{+0.76}$& $1.1_{-0.4}^{+1.4}$\\
Norm\tablefootmark{\delta} [10$^{-2}$ cm$^{-5}$]	& $3.3\pm0.9$		& $0.9_{-0.2}^{+0.5}$	& $2.4\pm 0.5$		& $1.4\pm 0.4$		& $1.0\pm 0.3$\\
$\chi^2$			& 98.19			& 57.54 		& 76.81			& 38.74			& 18.55\\
d.o.f.				& 95			& 57			& 77			& 38			& 27\\
$f_X$\tablefootmark{\epsilon} [$10^{-10}$ ergs cm$^{-2}$s$^{-1}$]&$1.61_{-0.23}^{+0.15}$&$0.30_{-0.02}^{+0.01}$&$1.25_{-0.09}^{+0.08}$&$0.55_{-0.04}^{+0.02}$&$0.56_{-0.06}^{+0.07}$\\
\\[-2ex] \hline\\[-1ex]
\end{tabular}
\tablefoot{
\tablefoottext{\alpha}{abundance with respect to solar value}
\tablefoottext{\beta}{ionization timescale}
\tablefoottext{\gamma}{ionization timescale-averaged temperature}
\tablefoottext{\delta}{Norm=$\frac{10^{-14}}{4 \pi [D_\mathrm{A}(1+z)]^2} \int N_\mathrm{e} N_\mathrm{H} \mathrm{dV}$, where $D_\mathrm{A}$ is the angular diameter distance to
the source in cm, $N_\mathrm{e}$ and $N_\mathrm{H}$ are the post-shock electron and hydrogen densities in cm$^{-3}$, respectively.}
\tablefoottext{\epsilon}{X-ray flux in the energy range 0.5 to 4.0 keV}
}
\end{footnotesize}
\end{table*}

\begin{figure*}[!]
\begin{center}
\includegraphics[width=0.33\textwidth,angle=-90,clip]{inner_rim_spec_clip.eps}
\includegraphics[width=0.33\textwidth,angle=-90,clip]{outer_rim_spec_clip.eps}

\includegraphics[width=0.33\textwidth,angle=-90,clip]{outer_north_spec_smaller_bg_clip.eps}
\includegraphics[width=0.33\textwidth,angle=-90,clip]{outer_south_spec_smaller_bg_clip.eps}
\caption{Spectrum and fitted model of the X-ray emission of the various regions.
{\it Upper left}: inner part of the remnant, {\it upper right}: outer rim, {\it
lower left}: outer rim north and {\it lower right}: outer rim south.}
\label{fig:spec_regions}
\end{center}
\end{figure*}

Within the statistical uncertainties, all regions turned out to have
a similar temperature. Only the ionization timescale-averaged temperature was varying.
The large statistical uncertainty also prevents us from concluding on a
temperature evolution with the distance to the expected center of the remnant.
No variation of the Neon and Magnesium abundance over the surface of the remnant is
detectable. The only noticeable change
in abundance is in Sulfur and Iron in the outer rim. The spectrum in the northern rim shows
an abundance in Iron comparable with the solar value. In the southern rim no significant
deviation from the solar value was found in the abundance of Sulfur. Furthermore, the ionization
timescale varies with distance from the remnant's center and the direction of the expanding
shock wave into the ISM. The highest values for $\tau$ were found for the inner sector
($8.1 \times 10^{10}$ s/cm$^3$) and the lower one in the southern part of the rim
($2.0 \times 10^{10}$ s/cm$^3$) which implies a different post-shock electron number
density in the inner and outer regions of the SNR candidate.

\subsection{The central sources}

As mentioned above, two point sources were detected close to the presumed center of the remnant,
source \# 1 (CXOU J134124.22--634352.0) and \# 10 (CXOU J134127.12--634327.7). For the spectral analysis of source \# 1 we used all
photons within a circular region of radius 10 arcsec centered on the source position. The background
was extracted from an annulus with radii $15''$ and $20''$. After background correction we were left
with 195 source counts in the energy band between 0.5 and 10.0 keV. We used the CIAO tool \sffamily psextract
\normalfont to compute the response matrices which are necessary to compensate for the changing spectral response
of the CCD and the telescope with energy and off-axis angle. The spectrum was binned with at least 20 counts per bin.

A single absorbed blackbody or a single absorbed power law model for fitting the spectral distribution
gives poor results. In the case of a blackbody spectrum the reduced $\chi^2=2.67$ for 6 degrees of
freedom is unacceptably large. The power law model fit results in a reduced $\chi^2$ of 0.94
(6 d.o.f.). However, the post-fit residuals show systematic derivations between the data points
and the fitted model. Therefore, we used a two-component absorbed blackbody model which results in
$\chi^2= 1.62$ (4 d.o.f.) and a $n_\mathrm{H}=1.34^{+1.80}_{-1.31} \times 10^{22}$ cm$^{-2}$. To better
constrain the spectral parameters we fixed $n_\mathrm{H}$ to the hydrogen column density
obtained from fits to G308.4--1.4. This gave a reasonable fit with $\chi^2=1.96$ for 5 d.o.f. (see Fig.
\ref{fig.spec_src1}). The temperatures of the two blackbodies are $T_1=1.3_{-0.2}^{+0.3}\times 10^6$ K
and $T_2=6.4_{-1.4}^{+2.8}\times 10^6$ K. The normalization factors of the two blackbodies are $K_1= 7_{-5}^{+21}\times 10^{-5}$
and $K_2= (1.3\pm +0.4)\times 10^{-6}$. Using these values and the distance to the source $D_{10}$ in
units of 10 kpc we estimated the emitting source radius $R$ as follows:

\begin{equation}\label{equ.Remit_vs_D}
R_i=\sqrt{\frac{K_i \times 10^{39}}{4 \pi \sigma_B D^2_{10} T^4}}~\mathrm{[m]},
\end{equation} where $\sigma_B$ is the Stefan-Boltzmann constant. As we do not know the distance to
G308.4--1.4 we considered the emitting radius as function of the distance to the source. This is illustrated
in Fig. \ref{fig.R_vs_d}. The result for the second blackbody is $R_2=340_{-158}^{+302} D^{-1}_{10}$ m.
The unabsorbed flux in the energy band 0.5 to 10 keV is $f_X=2.2_{-1.9}^{+0.5}\times 10^{-12}$
ergs cm$^{-2}$s$^{-1}$ and in the energy band 0.3 to 3.5 $f_X=(4\pm 2)\times 10^{-12}$ ergs cm$^{-2}$s$^{-1}$.

\begin{figure}
  \resizebox{\hsize}{!}{\includegraphics[clip]{r_emit_vs_d.eps}}
  \caption{Dependence of the blackbody emitting radius $R_1$ of the first blackbody in the double blackbody spectral fit
on the distance to source \# 1 in kpc (equation \ref{equ.Remit_vs_D}). The error range is gray shaded and
the green line indicates the upper limit on the radius of a neutron star.}
  \label{fig.R_vs_d}
\end{figure}

Additionally, we tried a model composed of a blackbody and a power law with the same fixed $n_\mathrm{H}$ as before.
This gives a reasonable fit with $\chi^2=2.17$ (5 d.o.f.). The photon index is $2.4_{-1.2}^{+1.0}$ and the blackbody
temperature is $(1.3\pm 0.3)\times 10^6$ K. With the normalization of $K_1=9_{-7}^{+53}\times 10^{-5}$ the
emitting radius is $73_{-45}^{+216} D^{-1}_{10}$ km.
The unabsorbed flux in the energy band 0.5 to 10 keV is $f_X=2.5_{-2.3}^{+0.5}\times 10^{-12}$ ergs cm$^{-2}$s$^{-1}$

\begin{figure}
  \resizebox{\hsize}{!}{\includegraphics[clip,angle=-90]{cco_spec_bb_bb.eps}}
  \caption{Spectrum of source \# 1 fitted with a double blackbody spectrum.}
  \label{fig.spec_src1}
\end{figure}

As mentioned in section \ref{kap:spatial} the position of source \# 1 is consistent with 2MASS J13412422--6343520,
a star with a magnitude of $B=19.7$, $R=19.6$, $J=14.0$, $H=13.3$ and $K=13.1$. This implies an X-ray-to-visual
flux ratio of $\log(f_X/f_V)=\log(f_X) + V/2.5 + 5.37=1.55$ \citep{1988Maccacaro}. Here $f_X$ is the X-ray flux in
the $0.3-3.5$ keV band in ergs cm$^{-2}$ s$^{-1}$, $V$ is the visual magnitude and we assumed that $V\approx R$.

In addition we tried to fit various plasma models to the source spectrum. The only reasonable fit
was found when using a collisionally-ionized diffuse gas model (\sffamily APEC \normalfont).
The goodness of fit which we found for 6 d.o.f. was $\chi^2_{red}=0.78$
for the following spectral parameters: $n_\mathrm{H} < 0.47 \times 10^{22}$ cm$^{-2}$, $ T=3.1^{+1.7}_{-1.4} \times 10^7$ K.
For this model the flux in the 0.3 to 3.5 keV range is $f_X=1.1^{+0.2}_{-0.1}\times 10^{13}$ ergs cm$^{-2}$s$^{-1}$.
Thus, the X-ray-to-visual flux ratio is $\log(f_X/f_V)=0.25$.
Again no variation in the spectral parameters between the flaring and quiescence epoch are detectable.
All fitted models and their inferred spectral parameters are listed in Table \ref{tab:point_src_spec}.

\begin{table*}
\linespread {1.25}\selectfont
\begin{footnotesize}
\caption{Spectral fit results of the central source \# 1.}
\label{tab:point_src_spec}
\begin{tabular}{cccccccc}
\hline\hline \\[-2ex]
Model			& $\chi^2$/d.o.f.& $n_\mathrm{H}$		& $\Gamma$/$kT_1$ 	& $K_1$ 				&
$kT_2$ 		& $K_2$ 				& $f_X^{0.5-10}$/$f_X^{0.3-3.5}$ \\
			&		& $10^{22}$ cm$^{-2}$	& -/keV			& 	& keV		& 	& $10^{-12}$ergs cm$^{-2}$ s$^{-1}$ 	\\ \hline
BB\tablefootmark{\alpha,\delta}	& 16.00/6	& $1.2\times10^{-4}$	& $0.44$& $9.9\times10^{-7}$	&
--&--& $-$/$-$\\
PL\tablefootmark{\alpha,\gamma}	& 5.62/6	& $<0.33$		& $2.2_{-0.4}^{+0.9}$	& $3.9_{-0.9}^{+4.3}\times 10^{-5}$	&
--&--& $0.16_{-0.02}^{+0.03}$/$0.16_{-0.03}^{+0.04}$\\
BB+BB\tablefootmark{\beta}	& 1.96/5	& $1.34_{-1.31}^{+1.80}$& $0.11_{-0.02}^{+0.03}$	& $7_{-5}^{+21}\times 10^{-5}$	&
$0.55_{-0.12}^{+0.24}$&$(1.3 \pm -0.4) \times 10^{-6}$& $2.2_{-1.9}^{+0.5}$/$4\pm 2$ \\
PL+BB\tablefootmark{\beta,\gamma}	& 2.74/5	& $<3.8$		& $2.4_{-1.2}^{+1.0}$	& $7_{-5}^{+11}\times 10^{-5}$	&
$0.11\pm 0.03$&$9_{-7}^{+53}\times 10^{-5}$& $2.5_{-2.3}^{+0.5}$/$5_{-4}^{+3}$ \\
APEC		& 4.66/6	& $<0.47$	& $2.7_{-1.2}^{+1.5}$				& $9.0_{-1.5}^{+3.0}\times 10^{-5}$	&
--&--& $0.13_{-0.02}^{+0.03}$/$0.11_{-0.03}^{+0.04}$\\
BREMS\tablefootmark{\alpha,\delta}	& 6.98/6& $1.8\times10^{-9}$& $2.1_{-0.8}^{+2.1}$		& $5.1_{-1.3}^{+2.3}\times 10^{-5}$	&
--&--& $-$/$-$\\
RAYMOND\tablefootmark{\alpha}	& 5.70/6	& $<0.21$	& $2.8_{-1.1}^{+2.0}$			& $8.9_{-0.8}^{+1.8}\times 10^{-5}$	&
--&--& $0.13\pm-0.02$/$0.11_{-0.01}^{+0.02}$\\
\\[-2ex]\hline \\[-1ex]
\end{tabular}
\linespread {1.0}\selectfont
\tablefoot{
\tablefoottext{\alpha}{fit shows systematic derivations between the data points and the fitted model.}
\tablefoottext{\beta}{the spectral parameters are calculated with $n_\mathrm{H}$ fixed to the value obtained in the fit to the spectrum of G308.4--1.4.}
\tablefoottext{\gamma}{Power law norm in photons keV$^{-1}$cm$^{-2}$s$^{-1}$ at 1 keV.}
\tablefoottext{\delta}{some errors could not be calculated.}
}
\end{footnotesize}
\end{table*}

\subsubsection{Temporal analysis of source \# 1}

In order to search for any temporal variability we binned the photon time of arrivals with
400 s per bin (see Fig. \ref{fig.flaring_src1}). The data show clearly a flare in the
first kilo-seconds of the observation. The spectral parameter of the double blackbody in the flaring
and quiescence epoch match the overall spectrum within the error bars. Varying only the
normalizations of the two blackbodies the flux in the quiescence epoch is with $f_X^{0.5-10}=
(1.9\pm 0.3)\times 10^{-12}$ ergs cm$^{-2}$s$^{-1}$ slightly lower than the flux in the total
exposure. However, the flux in the time interval when the source was flaring is
$f_X^{0.5-10}= (5.2 \pm 1.5)\times 10^{-12}$ ergs cm$^{-2}$s$^{-1}$, three times the
quiescence flux. However, the sparse photon statistics lead to large uncertainties in the
derived errors of the quiescence and flaring fluxes and thus they are only rough estimates.
Merging the SWIFT observations we cannot detect a source at the position of source \# 1.
In the merged image a total of 4 counts were recorded within a circle with radius 15 arcsec
(equals an encircled energy of 70~\%) centered on the position of source \# 1 . The
total exposure time of the source was 8344 s. Hence, the $3\sigma$ upper limit for the
counting rate is approximately $8.6\times 10^{-4}$ cts/s. Using the mission count
rate simulator for X-ray observatories WebPIMMS\footnote{\url{http://heasarc.nasa.gov/Tools/w3pimms.html}} with the SWIFT
response and the spectral parameters derived for a double blackbody spectrum the upper limit
on the flux is  $\approx 5.3\times 10^{-13}$ ergs cm$^{-2}$ s$^{-1}$. For the \sffamily APEC \normalfont model the
upper limit is $\approx 2.3\times 10^{-14}$ ergs cm$^{-2}$ s$^{-1}$. These limits are less
than 25 \% of the average flux in the Chandra observation, clearly indicating that the
source flux is variable on time scales of at least several hours to weeks.

\begin{figure}
  \resizebox{\hsize}{!}{\includegraphics[clip]{lc_flux_flaring_star.eps}}
  \caption{Flux variation of source \# 1 in the Chandra observation binned with
  400 s per bin and scaled with the mean flux in the whole exposure.
The red arrow indicates the 3$\sigma$ upper limit derived with the SWIFT observations.}
  \label{fig.flaring_src1}
\end{figure}

\subsubsection{Extent of source \# 1}

With the help of a one-dimensional distribution of the counts per $0.5''$ bin along a
vertical line in the Chandra image around source \# 1 we checked if the source
is extended. The resulting diagram was obtained by integrating all counts within
$5''\times 0.5''$ rectangular apertures moving along the western direction with
$0.5''$ steps. We compared this with the count distribution of a point source
simulated with MARX\footnote{MARX is a software which can be used to simulate the
performance of the Chandra X-ray observatory; see \url{http://space.mit.edu/cxc/marx/}}.
However, no excess emission of point source \# 1 could be detected.

For source \# 10, the other source located close to the center of the remnant,
we detected only 8 net counts. Hence, the count rate is $(5.1\pm 1.9)\times 10^{-4}$
cts/s, but no spectral analysis is possible by the limited statistics.

\section{Radio observation and data analysis}\label{kap:obs_radio}
The source G308.4--1.4 was observed for 11.25 hours with the Australia Telescope
Compact Array, a synthesis telescope near Narrabri, New South Wales on 11th
January 2002 at 1.432 and 2.448 GHz with 13 channels per band.
The single pointing continuum observations of the source G308.4--1.4 was
carried out with the array configuration 0.75C (maximal baseline length is 750 m).
All four Stokes parameters have been recorded.

The flux density calibration was performed through observations of
PKS B1934--638, which is the standard primary calibrator for ATCA observations.
Phases were calibrated using observations of secondary calibrating sources
PKS 1329--665. Since the primary beam response is frequency dependent we did not
merge the data from two observing bands before imaging and cleaning. Every single
observing run and each of the two observing bands were calibrated separately
following the standard procedures for ATCA observations.

The reduction was carried out using the ATNF release of the Multichannel
Image Reconstruction, Image Analysis and Display \citep[MIRIAD,][]{1995ASPC...77..433S}.
A number of steps in the reduction process (i.e. ``flagging``) were done interactively.

   Because of the bad phase stability during the observation, the scalar
averaging of gains over the interval of 5 min (the length of secondary
calibrator's scan) was performed. Then, a total-intensity continuum image square
region was formed using multi-frequency synthesis, uniform weighting and a cell
size of 10 arcsec. At the stage of the dirty map production all the correlations
with 6th baseline were excluded to obtain images with better signal-to-noise
ratio. The next step was to de-convolved both images using the standard CLEAN algorithm
\citep{1980A&A....89..377C} with 10\,000 iterations. The resulting images were restored and
corrected for the mean primary beam response of the ATCA antennas.
The final images have synthesized beam sizes of $63.6''\times 53.2''$ and $35.2''\times 29.3''$
for the 1.384 GHz and 2.496 GHz band, respectively.

In both frequency bands the images show two radio arcs (see Fig. \ref{fig:becker}).
The eastern arc matches the X-ray emission region. For the western arc no counterpart is visible in the X-ray regime.
There are also two radio bright knots within the arcs which do neither have a counterpart in
X-rays (see Fig. \ref{fig.chandra_radio}) nor in the optical band (dss2red). No difference
can be seen to the morphology of the extended source in the SUMSS 843 MHz map.

\begin{figure*}[!]
\begin{center}
\resizebox{0.8\hsize}{!}{\includegraphics[clip]{g308_ss_v2.eps}}
\caption{Grey-scale image of SNR G308.4--1.4. The left image displays the SNR at 1.4 GHz and on the right the same
region at 2.5 GHz. The 1.4 GHz image is smoothed with a beam of $63.6''\times 53.2''$ and the 2.5 GHz with a beam of $35.2''\times 29.3''$.}
\label{fig:becker}
\end{center}
\end{figure*}

The flux density of G308.4--1.4 without the two bright knots are 235, 174 and 110 mJy at
843, 1384 and 2496 MHz, respectively. These values were
obtained by integrating the emission within multiple polygons enclosing the remnant. The 843 MHz flux
density was deduced from the SUMSS image. The bright southern knot has a flux density of 110,
75 and 70 mJy at 843, 1384 and 2496 MHz. Whereas for the northern knot we measured a flux density of 96, 76 and 56 mJy
at 843, 1384 and 2496 MHz. In all cases we assumed a conservative error in the flux density of $20\%$.

The rms noise levels are 0.28 mJy beam$^{-1}$ and
0.05 mJy beam$^{-1}$ for the 1.384 GHz and 2.496 GHz image. The levels were measured by integrating over
nearby source-free regions. The spectral indices were computed using the total flux density measurements
in all available frequencies (0.843, 1.384 and 2.496 GHz). Fitting the data with a
power law $S_\nu \propto \nu^\alpha$, we obtained a spectral index for the northern knot
$\alpha=-0.50\pm0.14$ and for the southern $\alpha=-0.49\pm0.16$, respectively. The radio
emission of the two arcs, however, have a spectral index $\alpha=-0.7\pm0.2$.
No significant polarized radio emission could be detected.

\begin{figure}
  \resizebox{\hsize}{!}{\includegraphics[angle=-90, clip]{g308_xray_radio.eps}}
  \caption{Chandra $15'\times 15'$ image of G308.4--1.4 overlaid with the ATCA data at 1.4 GHz.
  The contour levels are 4, 8, 12, 16 and 24 mJy beam$^{-1}$. The radio image has a full width at half maximum (FWHM)
  of $ 63.6''\times 53.2''$ and the X-ray image is binned with $1''$ per pixel.} \label{fig.chandra_radio}
\end{figure}

\section{Observations in other wavelength regimes}\label{kap:obs_multi}
The region around G308.4--1.4 was observed in the four infrared bands 3, 5, 12 and 22 $\mu$m during the
Wide-field Infrared Survey \citep[WISE,][]{2010AJ....140.1868W}. With the 22 $\mu$m filter an extended
infrared emission, overlapping with the radio and X-ray emission regions, is detectable (see Fig. \ref{fig:infrared}).
After subtraction of the background contribution the intensity image in the 22 $\mu$m band was converted into a flux
image using the explanatory Supplement to the WISE All-Sky Data Release
Products\footnote{\url{http://wise2.ipac.caltech.edu/docs/release/allsky/expsup/sec2_3f.html}}. We did not apply color correction as the
emission mechanism in the infrared regime is uncertain. In addition, the integrated flux is not corrected for extinction.
To compare the infrared with the 1.4 GHz image the flux density in the 22 $\mu$m observation was scaled to Jy/beam, where beam is $63.6 \times 53.2$ arcsec$^2$.
Using the region of infrared emission which is clearly associated with the remnant the integrated flux of G308.4--1.4 in the 22 $\mu$m band
is $\approx 1.7$ Jy.

\begin{figure}
  \resizebox{\hsize}{!}{\includegraphics[angle=-90,clip]{g308_IR_radio_xray_v2.eps}}
  \caption{$10'\times 10'$ WISE image around G308.4--1.4 at 22 micron with the radio contour lines in white
at 3, 8, 12, 16 and 24 mJy and the X-ray contours in black.}
  \label{fig:infrared}
\end{figure}

The shock wave of a SN which is running into the interstellar medium can interact with adjacent
molecular clouds and produce $\gamma$-rays via decays of $\pi^0$ \citep{2011ApJ...734...28A}.
We therefore checked the archive of the Fermi Large-Area Telescope for a $\gamma$-ray source at the
position of G308.4--1.4. The Fermi $\gamma$-ray satellite monitors the sky continuously since August 2008.
However, no source has been detected close to G308.4--1.4 in the Fermi-LAT Second Source Catalog
\citep{2012ApJS..199...31N} and investigating the images ourselves we found no $\gamma$-ray
emission matching the X-ray morphology.

\section{Discussion and Conclusion}\label{kap:discus_concl}

Comparing the fitted $n_\mathrm{H}$ with the integrated hydrogen column density towards the source of \citet{2005A&A...440..775K}
and \citet{1990ARA&A..28..215D} places G308.4--1.4 within our Galaxy.

The plasma model which is used to fit the energy spectrum of G308.4--1.4 was especially designed to improve
the modeling of X-ray spectra of SNR. Other plasma models assume ionization equilibrium and are therefore not
able to reproduce the spectra of young SNRs which are not old enough to reach ionization equilibrium
\citep{2001ApJ...548..820B}. Furthermore, the temperature of the plasma of approximately 6 million Kelvin
is in the typical range for SNRs \citep{1987soap.conf..226M}.

The analysis of the archival ATCA radio data revealed non-thermal emission with a spectral index of
$\approx -0.7$, which is typical for young to middle-aged SNRs \citep{1991supe.conf..675D}. The spectral index has a
large error due to the noise in the 2.5 GHz observation but is still in agreement with the expected value  of 0.4 to 0.5 for
middle-aged SNR.

Infrared radiation from SNRs is expected to come either from thermal emission
of dust grains in the hot plasma which are heated through collision or from the forbidden
lines of elements such as Neon, Oxygen and Iron \citep{2008PASJ...60S.453S}. Several authors could
show that by comparing the infrared and radio emission it is possible to distinguish between SNRs and HII-regions
\citep{1987A&AS...71...63F, 1989MNRAS.237..381B, 2011AJ....142...47P}. Moreover, in the work by
\citet{2011AJ....142...47P} the ratio between the flux density in the MIPSGAL 24-$\mu$m
\citep{2009PASP..121...76C} and the 1.4-GHz band was used. They find that the ratio is $\leq 10$ for SNR and larger than
30 for HII-regions. In the case of SNR G308.4--1.4 the 22 $\mu$m band
was observed which covers roughly the wavelength range from 20 $\mu$m to 27 $\mu$m.
Thus, the band is comparable with the MIPSGAL 24 $\mu$m band which is sensitive for infrared emission in the range from
20 $\mu$m to 30 $\mu$m \citep{2011AJ....142...47P}. The 22-$\mu$m
to 1.4-GHz ratio for G308.4--1.4 is $\approx 10$. Hence, the infrared emission matching the radio and
X-ray morphology and the measured 22-$\mu$m to 1.4-GHz ratio gives further support for G308.4--1.4 being a SNR.

The lack of $\gamma$-ray emission from G308.4--1.4 can be explained by the poor spatial resolution of the
Fermi-LAT telescope ($\sim 1^\circ$ at 1 GeV), which makes it hard to distinguish faint
extended sources from the diffuse emission of the Galactic plane.
From the 274 known SNRs only 7 have been detected by Fermi-LAT so far \citep{2012ApJS..199...31N}.

There are various physical scenarios to cause a plasma to emit X-rays. However, the two emission
models for hot diffuse \citep[\sffamily MEKAL\normalfont,][]{1986A&AS...65..511M} and collisionally-ionized diffuse gas
\citep[\sffamily APEC\normalfont,][]{2001ApJ...556L..91S} which
are often used to describe the X-ray emission of Galaxy Clusters (ClGs)  cannot
reproduce the spectrum of G308.4--1.4. Moreover, the temperature of ClGs is normally several $10^7$ K \citep{2010A&ARv..18..127B},
one order of magnitude higher than the fitted value. Thus, we can conclude that G308.4--1.4 is not a ClG.
In addition, the possibility of G308.4--1.4 being a planetary nebula (PN) can be ruled out as the X-ray flux
of G308.4--1.4 is three orders of magnitude higher than the flux of the brightest PN detected in
X-rays, which is at a distance of $\approx 1$ kpc \citep{2006ESASP.604...85G} and the small 22-$\mu$m
to 1.4-GHz flux ratio. Furthermore, the temperature of G308.4--1.4 is a factor of two higher than the highest measured
temperature of the hotter, type 2 PNe \citep{2000ApJS..129..295G}.

Based on these results we conclude that G308.4--1.4 is indeed a supernova remnant. Only the eastern part of the remnant
can be seen in the radio, infrared and X-ray regime which is is not unusual for SNR \citep[e.g.,][]{2011ApJ...734...86C}. A reason
for that could be that its shock wave is expanding in more dense ISM in the east or the emission in the western part is absorbed by ISM
which is in front of the SNR. Looking at Fig.\ref{fig:infrared} it can be seen that there is an extended and infrared bright region
in the north-western part of the SNR whose emission is no correlated with the SNR.

Using the inferred spectral parameters we can estimate fundamental
characteristics of the remnant, such as the distance from earth and its age.

\subsection{Distance} \label{chap.distance}

To derive a rough estimate for the distance to SNR G308.4--1.4 we use a method described by various authors
\citep{1999ApJ...511..274S,2001ApJ...561..308S,2003ApJ...591L.143G}: From the distribution of mean color excess
$\langle E_\mathrm{B-V}\rangle$ per kiloparsec derived by \citet{1978A&A....64..367L} we found
$\langle E_\mathrm{B-V}\rangle= (0.3\pm 0.1)$ mag kpc$^{-1}$. Using the fitted hydrogen column density
for the whole remnant $n_\mathrm{H}=(1.02\pm 0.04) \times 10^{22}$ cm$^{-2}$, the relation between the
hydrogen column density $n_\mathrm{H}$ and the visual extinction $A_\mathrm{V}$ of \citet{1995A&A...293..889P}
$n_\mathrm{H}=(1.79\pm 0.03)\times 10^{21}$ cm$^{-2} A_\mathrm{V}$  and adopting the relation between
$A_\mathrm{V}$ and the color excess $A_\mathrm{V}/\langle E_\mathrm{B-V}\rangle=(3.2\pm 0.2) $
\citep{2007hsaa.book.....Z} the distance to G308.4--1.4 is $d=5.9\pm 2.0$ kpc. We note, that
this distance is a lower boundary of the real distance. This is due to the fact that the mean
color excess $\langle E_\mathrm{B-V}\rangle$ which we used was derived for reddening layer up
to 2 kpc. In the case of distance estimates for Galactic PNe the reddening inferred distances
are mostly significantly smaller than distances derived with other methods \citep{2006RMxAA..42..229P}.
This leads us to assume that $d\approx 6$ kpc is the lower bound limit for the distance to SNR G308.4--1.4.

Another approach to determine the distance to G308.4--1.4 uses the fact that the radius of the remnant $R_\mathrm{s}$ can be determined in two
ways, where $R_\mathrm{s}$ depends on the distance $d$ with different exponents. The first equation is a result of the Sedov analysis discussed in the next chapter
(equation \ref{eq.Rs1}) and depends on $d^{1/6}$. The second equation to determine $d$ is simply the comparison of the radius of the remnant in
pc ($R_\mathrm{s}$) and in arcmin ($\theta$), $d=R_\mathrm{s}/\theta$, which depends linearly on the distance unit $d$.
Using this dependencies we derive
\begin{equation}
 d=7420 \cdot (\theta~[\mathrm{arcmin}])^{-3/5}\left(\frac{E_{51}}{T_\mathrm{s}[\mathrm{K}]}\right)^{2/5}\left(\frac{f}{\mathrm{Norm}}
\right)^{1/5}=9.8^{+0.9}_{-0.7}~\mathrm{kpc},
\end{equation}
where $T_\mathrm{s}$ is the post-shock temperature and $E_{51}$ the SN explosion released kinetic energy in units
of $10^{51}$ ergs.

Furthermore, with the help of the ATCA radio observations and the public available HI data from the Southern Galactic Plane Survey
\citep[SGPS;][]{2005ApJS..158..178M} it is possible to constrain the distance using the Galactic rotation model of
\citet{1989ApJ...342..272F}. For the region around G308.4--1.4 the SGPS archive provides ATCA data observed with a beam size of
$130''\times 130''$ and a $1\sigma$ sensitivity of $\sim 1.6$ K. However, the data covers only the northern part of the remnant.
In the SGPS archive there are also Parkes data covering the region around the SNR, but with an angular resolution of $15'$.
This beam is twice the size of the remnants diameter. Therefore, we choose to use the ATCA data for the further analysis.

First, we convolved the radio continuum image at 1.4 GHz to the same beam size as the SGPS data. We assumed that the emission of the
remnant is not varying significantly across the emission region. Second, the convolved image was used to generate an on-source spectrum
of SNR G308.4--1.4 by averaging the HI emission for every velocity bin in the HI data cube where the radio continuum emission was above
5 mJy. The off-source spectrum was computed by taking the average of the emission in the surrounding of the on-source region of the remnant.
These two profiles as well as the difference plot between these two profiles are shown in Fig. \ref{fig:hi}.
The difference profile is dominated by drifts in the zero level. This is due to the fact that the source is at the border of the
image and as we are using public data the pointing is not perfect for the method applied. In addition to the drifts we detect one
absorption feature with a significance of $>3\sigma$ at $V_r\sim 30$ km/s. With the standard IAU parameter for the distance to
the center of the Galaxy $R_0=8.5$ kpc and the solar orbit velocity of $V_0=220$ km/s derived by \citet{1986MNRAS.221.1023K} and the already
mentioned Galactic rotation model we deduce a distance to G308.4--1.4 of $2.0\pm0.6$ kpc and $12.5\pm0.7$ kpc. For the error estimate
we assume a uncertainty in the velocity-to-distance conversion of 7 km/s as suggested by various authors \citep[e.g.,][]{1988ApJ...333..332C} and
we use the FWHM of the feature as the uncertainty in the velocity determination. Based on the calculated lower limit for the distance
of the remnant we can rule out the lower value as unreasonable. The low significance of the absorption feature leads to
the conclusion that the Sedov-analysis based distance approximation is the more reliable estimate for the distance to SNR G308.4--1.4.
Thus, in the following all important quantities are given in units of $d_{9.8}=d/9.8$ kpc.
Using the flux values deduced for G308.4--1.4 we compute its X-ray luminosity to
be $L_X^{0.5-4}=1.8_{-0.2}^{+0.3}\times 10^{36}~d_{9.8}^{-2}$ erg/s.

\begin{figure}
  \resizebox{\hsize}{!}{\includegraphics{hi_velocity_G308_ATCA_bin2.eps}}
  \caption{Top: HI spectrum on- and off-source (continuous and dotted line, respectively) in the direction of SNR G308.4--1.4.
Bottom: Difference profile with the $3\sigma$ level indicated by a dotted vertical line.}
  \label{fig:hi}
\end{figure}

\subsection{Age of SNR G308.4--1.4}

First we had to deduce the post-shock hydrogen density $N_\mathrm{H}$. Using the normalization constant derived in the
model fit of a collisional plasma which is in non-equilibrium (\sffamily VGNEI\normalfont) and assuming that the
hydrogen and electron densities are constant over
the volume $V$ of the emission region we derived the following relation:
$N_\mathrm{e}N_\mathrm{H}=Norm \cdot \frac{\pi D_A^2}{10^{-14} V}$ cm$^{-6}$. $V$ can be approximated by a sphere with radius
$r\approx \frac{4.2'\pi}{180}\cdot D$ of which only a fraction of $\sim \frac{136}{360}$ is bright enough to
be detected in the X-ray regime. Therefore, the volume is $V=1.14\times 10^{54}~(r[\mathrm{arcmin}])^3 d^3_{kpc} \mathrm{cm}^3=7.98\times 10^{58}
d^3_{9.8} \mathrm{cm}^3$. Here $d_{kpc}$ is the distance to G308.4--1.4 in kpc. For a fully ionized
plasma with cosmic abundances ($\approx 10\%$ He) the ratio between hydrogen and electron density can be estimated
by $N_\mathrm{H}/N_\mathrm{e}\approx 0.8$. Thus, the post-shock hydrogen density $N_\mathrm{H}=(0.77 \pm 0.11)~d^{-1/2}_{9.8}$ cm$^{-3}$
and the corresponding swept-up mass  $M=1.4N_\mathrm{H}m_\mathrm{H}V \sim 71.7 d^{5/2}_{9.8} M_\odot$ \citep{2002ApJ...580..904S}.

The age of the remnant can be approximated by \citep{1987soap.conf..226M}
\begin{equation}
t=2.71\times 10^9 \left(\frac{E_{51}}{N_\mathrm{H}}\right)^\frac{1}{3} T_\mathrm{s}^{-\frac{6}{5}}d_{9.8}^\frac{1}{6}~\mathrm{yrs}.
\end{equation}
Assuming that the explosion energy is equal to the canonical
value of $10^{51}$ ergs and the fitted temperature is approximately $T_\mathrm{s}$, the derived value for the hydrogen
density suggests an age of $\approx 5000 - 7500$ years for SNR G308.4--1.4. Using this result we can calculate the theoretical
radius of the remnant \citep{1977ASSL...66...29C}
\begin{equation}\label{eq.Rs1}
R_\mathrm{s} = 0.34 \left(\frac{E_{51}}{N_\mathrm{H}}\right)^\frac{1}{5} t^\frac{2}{5}~\mathrm{pc} = 11.9^{+1.9}_{-1.8} d_{9.8}^\frac{1}{6}~\mathrm{pc}
\end{equation}
and the shock velocity \citep{1959sdmm.book.....S}
\begin{equation}
v_\mathrm{s}=\frac{2}{5} \frac{R_\mathrm{s}}{t} = 730^{+190}_{-160}~\mathrm{km/s},
\end{equation}
which is independent on the assumed distance. The age for the transition from the Sedov-phase
into the radiative phase is about 29 kyrs \citep{1998ApJ...500..342B}. The fact that the age of G308.4--1.4 is
much lower than the transition time scale suggest that G308.4--1.4 is in the Sedov-phase. Furthermore, the energy
spectrum of the remnant is in agreement with G308.4--1.4 being in the Sedov-phase.

However, the derived parameters should only be seen as rough estimates as we could not determine whether
a full temperature equilibrium is already established. If not, a generally higher ion temperature which
determines the SNR dynamics would lead to a higher shock velocity and subsequently to an e.g.~overestimation of the remnant's age.

\subsection{The central sources CXOU J134124.22--634352.0 and CXOU J134127.12--634327.7}\label{kap.dis_point_src}

No radio counterpart for CXOU J134124.22--634352.0 has been detected in the ATCA and SUMSS observations
of G308.4--1.4. An explanation could be that the variable source is also
variable in the radio band and therefore the source was missed in all previous observations of this region. To decide
if this is the case new observations are needed.

Additionally, CXOU J134124.22--634352.0 has no compact/extended X-ray emission as seen in other young and powerful pulsars. Its best fit
spectral model consists of two blackbodies. Thus, source \# 1 shows some properties
which have been also seen in central compact objects \citep[CCO, see][for a review]{2008AIPC..983..320G}.
CCOs are young neutron stars which are located in SNRs having an age of less than 10 kyrs. They have X-ray luminosities
between $10^{32}$ and $10^{33}$ erg/s in the energy range 0.5-10 keV. No CCO has a detected counterpart in the
radio and optical band so far. For one member of the CCO group, 1E 161348--5055 in RCW 103, flares have been detected
in which the flux varies between 0.8 and $60 \times 10^{-12}$ ergs cm$^{-2}$ s$^{-1}$. This is
comparable to source \# 1 where the maximal flux is $\approx 10^{-11}$ ergs cm$^{-2}$ s$^{-1}$
and the upper limit derived from the SWIFT observations is $\approx 5 \times 10^{-13}$ ergs cm$^{-2}$ s$^{-1}$.

Using the distance derived in chapter \ref{chap.distance} the luminosity of CXOU J134124.22--634352.0 is
$L_X^{0.5-10}=2.5_{-0.6}^{+1.2}\times 10^{34}~d_{9.8}^{-2}$ erg/s. This is slightly higher than the derived luminosity
for the normal population of CCO \citep[p.121]{2009Becker}, only the flaring CCO in RCW 103 has a comparable luminosity of
$0.1-8 \times 10^{34}$ erg/s \citep{2008AIPC..983..311D}.

In the ROSAT All-Sky Survey \citet{1999Krautter} found for all X-ray bright stars
with an optical counterpart a ratio of $\log(f_X/f_V)=-2.46 \pm 1.27$.
Therefore, the X-ray-to-visual flux ratio of 1.55 and the fitted $n_\mathrm{H}$, which is in
the order of what has been observed for G308.4--1.4, suggest a CCO interpretation
for source \#~1.

Assuming that the source is indeed the compact remnant we can derive the proper motion of the object
$\mu=\sqrt{(RA_c-RA_{\# 1})^2+(DEC_c-DEC_{\# 1})^2}/t = (45\pm 4)''/t$ using the inferred center and the age of the SNR. We
deduce the proper motion to be  $\mu=7 \pm 2$ mas/yr $= 320 \pm 100$ km/s. The upper limit on $\mu$ is higher than
the mean two-dimensional proper motion of pulsars in SNRs of $\sim 227$ km/s \citep{2005MNRAS.360..974H}, but
would not be an exception. For example, the CCO RX J0822-4300 in the SNR Puppis A has a 2d proper
motion of $672 \pm 115$ km/s \citep{2012arXiv1204.3510B}.

Nevertheless, the lower limit of the inferred emitting radius of the blackbody in the double blackbody or the
power law-blackbody spectral fit is in the order of the expected value for the neutron star radius of 10 to 20 km only
if the source is at a distance larger than 14.5 kpc (see Fig. \ref{fig.R_vs_d}). Moreover, we found
an infrared and optical source which position is consistent with source \# 1. The spectral distribution of the
source allows us to fit a collisionally-ionized diffuse gas model (\sffamily APEC\normalfont) which
\citet{2005ApJ...621..398O} used to model the energy distribution in the X-ray band of the M dwarf flare star
EV Lacertae. In addition, the fitted hydrogen column density is consistent to that of a nearby star and the X-ray-to-visual flux ratio
is 0.25, only $2\sigma$ higher than the value for stars derived by \citet{1999Krautter}.

Using the stellar density in direction of G308.4--1.4 we can derive the chance association of the observed 2MASS source with
the compact remnant candidate. The chance association is given by
$P_{coin}=\frac{N}{l_{RA} l_{Decl.}} \pi~ \delta RA~ \delta DEC$, where $N$ is the number of sources detected within
a rectangular region of length $l_{RA}$ and width $l_{Decl.}$ and $\delta RA$, $\delta DEC$ are the errors in the position
of the source. The 2MASS catalog contains 2206 point-like sources
in a box with side length of 5 arcmin around the center of the remnant and the chance association is 1.3\%.
Thus, the possibility of a false association between the X-ray and the 2MASS source cannot be excluded.

Until now, we did not discuss the western radio arc which has no counterpart in the X-ray and infrared image. The arc could
be interpreted as a relativistic radio jet of a source at the geometrical center of the SNR. If so, the central source
is either a black hole of stellar mass or a neutron star in a binary system \citep[~and reference therein]{1999ARA&A..37..409M}.
Especially the possibility that the central source is a black hole is an interesting speculation which, if proven, would
mean that G308.4--1.4 is the remnant of a Type II core-collapse SN. Thus, would be the first one known which left over a black hole.

To obtain a rough estimate of the source flux of the other source in the center of the remnant, source \# 10, we assumed that the
source is a CCO, should have at least a spectrum with a blackbody of temperature 2.6 million Kelvin as the CCO in
Puppis-A \citep[cf. Table 6.4,][]{2009Becker}. Using the WebPIMMS
tool with the source count rate and the fitted $n_\mathrm{H}$ of the SNR
the flux in the $0.3-3.5$ keV range is $f_X \approx 2.2\times 10^{-14}$ ergs cm$^{-2}$s$^{-1}$ and
in the $0.5-10$ keV range is $f_X \approx 1.9\times 10^{-14}$ ergs cm$^{-2}$s$^{-1}$. The normalization
of a blackbody with this flux, temperature and $n_\mathrm{H}$ is $2.5\times 10^{-5}$ which corresponds to
an emitting radius of the source of $\approx 9 d_{9.8}^{-1}$ km. This value is in perfect agreement with the expected
value for the neutron star radius. The corresponding luminosity in the energy band $0.5-10$ keV is
$L_X^{0.5-10}=2.1\times 10^{32}~d_{9.8}^{-2}$ erg/s, a typical value for CCOs. Furthermore, the X-ray-to-visual
flux ratio is $\log(f_X/f_V)>0.11$ taking into account that no optical source was detected in the USNO-B1.0
catalog and the limiting magnitude of this catalog is 21 \citep{2003AJ....125..984M}.
Thus, no clear evidence for the origin of the emission of source \# 10 could be found.

Finally we mention that the detector support structure of Chandra covers the
central part of G308.4--1.4 (see Fig. \ref{fig.chandra_rgb}). It is therefore not
excluded from our observations that other faint X-ray point sources are located
at this position. However, the non-detection of a source in the SWIFT data
at the assumed position of the remnant's expansions center sets a strict upper limit of
$5 \times 10^{-13}$ ergs cm$^{-2}$ s$^{-1}$ on the flux of such an object.

\section{Summary}\label{kap:Summary}

The high resolution imaging and spectroscopic capability of Chandra revealed that the X-ray emission of
the source is an extended plasma and G308.4--1.4 is indeed a supernova remnant. The emission region is spherically
symmetric with a diameter of 8.4 arc-minutes and an excess emission towards the east.

The radio morphology at 0.843, 1.384 and 2.496 GHz is characterized by two arcs. The eastern arc matches well with the X-ray and
infrared contours. The second arc which is bending in the west and decreasing brightness towards the center of G308.4--1.4 has no
counterpart in other wavelengths. The remnant without the two bright knots has a spectral index of $\alpha=-0.7\pm0.2$

\begin{table}
\renewcommand{\arraystretch}{1.25}
\begin{footnotesize}
\caption{Fundamental parameters of SNR G308.4--1.4.}
\label{tab:imp_para}
\begin{tabular}{cc}
\hline\hline
SNR & \\ \hline
distance & $9.8^{+0.9}_{-0.7}$ kpc\\
age & $5000-7500$ yrs\\
radius & $\sim 4.2'$/ $11.9^{+1.9}_{-1.8} d_{9.8}^{1/6}$ pc \\
expansion velocity & $730^{+190}_{-160}$ km/s\\
\\[-2ex]\hline\\[-1ex]
\end{tabular}
\end{footnotesize}
\end{table}

The Sedov analysis lead to the conclusion that the SNR is about 6200 years old and is expanding with a velocity in the order
of $\approx 730$ km/s. All fundamental parameters of the SNR are summarized in Table \ref{tab:imp_para}.

The X-ray point-like source CXOU J134124.22--634352.0, located close to the geometrical center of the SNR
G308.4--1.4, is seen to exhibit variable and flaring X-ray emission. However, no certain conclusion on the origin of this
source and the other central source CXOU J134127.12--634327.7 could be drawn. Deeper observations of the central part of SNR G308.4--1.4 are
needed to resolve the obvious ambiguities.

\begin{acknowledgements}
 T.P. acknowledges support from and participation in the International Max-Planck
Research School on Astrophysics at the Ludwig-Maximilians University. The authors acknowledge
discussions with M.~D. {Filipovi{\'c}}.
\end{acknowledgements}

\bibliographystyle{aa}

redpajama_set_name: RedPajamaArXiv


2012-01-18T17:42:00-05:00https://images.c-span.org/Files/694/303746-04-m.jpgMembers spoke briefly about their reaction to President Obama's decision to reject the Keystone oil pipeline.
Members spoke briefly about their reaction to President Obama's decision to reject the Keystone oil pipeline.
Telephone lines were open for viewer comments on President Obama's decision to reject the Keystone pipeline project.
Amy Harder was interviewed about the Obama's administration to reject the Keystone oil pipeline.


text:
Q: Как настроить в .properties log4j путь к логам внутри проекта? Как настроить в .properties log4j путь к логам внутри проекта?
То есть что бы после пула с гита путь был всегда октуален.
log4j.properties
# Root logger option
log4j.rootLogger=INFO,infoLogfile, errorLogFile, stdout

#Error Logger option
log4j.logger.com.testNgExample.tests=errorLogFile

# Direct log messages to a log file
log4j.appender.infoLogfile=org.apache.log4j.RollingFileAppender
log4j.appender.infoLogfile.File=/Users/mu/Dev/Auto_test/my_example/src/test/log/Log.txt
log4j.appender.infoLogfile.threshold=INFO
log4j.appender.infoLogfile.MaxFileSize=1MB
log4j.appender.infoLogfile.MaxBackupIndex=10
log4j.appender.infoLogfile.layout=org.apache.log4j.PatternLayout
log4j.appender.infoLogfile.layout.ConversionPattern=line:%L - [%-5p][%d{yyyy-MM-dd HH:mm:ss}] %c{1}: - %m%n

# Direct logError messages to a log file
log4j.appender.errorLogFile=org.apache.log4j.RollingFileAppender
log4j.appender.errorLogFile.File=/Users/mu/Dev/Auto_test/my_example/src/test/log/logError.txt
log4j.appender.errorLogFile.threshold=ERROR
log4j.appender.errorLogFile.MaxFileSize=1MB
log4j.appender.errorLogFile.MaxBackupIndex=10
log4j.appender.errorLogFile.layout=org.apache.log4j.PatternLayout
log4j.appender.errorLogFile.layout.ConversionPattern=line:%L - [%-2p][%d{yyyy-MM-dd HH:mm:ss}] [%t] %c{5}.%M.%F.%M: - %m%n

# Direct log messages to stdout
log4j.appender.stdout=org.apache.log4j.ConsoleAppender
log4j.appender.stdout.threshold=INFO
log4j.appender.stdout.Target=System.out
log4j.appender.stdout.layout=org.apache.log4j.PatternLayout
log4j.appender.stdout.layout.ConversionPattern=line:%L - [%-5p][%d{yyyy-MM-dd HH:mm:ss}] %c{1}: - %m%n

A: Из пути надо убрать лишнее
log4j.appender.infoLogfile.File=log/Log.txt

тогда лог будет создаваться в папке log относительно текущей папки.

redpajama_set_name: RedPajamaStackExchange


Brandon Williams (born 1984), better known by his stage name Urban Mystic, is an American Hip hop soul singer. He is currently signed to the record label SoBe Entertainment.
Williams was born the son of a church minister in 1984 in Fort Lauderdale where he was also raised. In his early years, he developed an interest for music at his father's church. He attended Dillard High School in Fort Lauderdale where he sang at every pep rally, show and event that was held in order to get noticed. He even performed at the local "Sistrunk Historical Festival" held every year in honor of Dr. James Sistrunk, one of the first African-American Physicians in Broward County, Florida. He was looking forward to pursuing a musical career with support from his brother Christopher. He grew more familiar with the music industry and became active as songwriter and producer.
In 2003, Williams gave himself the moniker Urban Mystic which reflects both his street mentality and his singing talent. In 2004, hip-hop producer Scott Storch offered Williams a deal with both The Roots and Stack$, a.k.a. Yannique Barker, for SoBe Entertainment, the label he is still signed to. His debut album, Ghetto Revelations, released on November 30, 2004, included the Billboard R&B hit single "Where Were You", produced by KayGee. He also had worked with Red Spyda and El DeBarge on the album. The first single from his second album, "It's You", was released in 2005 and featured Paul Wall. In the same year, Williams joined the newfangled Spitkicker collective. His second studio album, Ghetto Revelations 2 was released on March 21, 2006 and produced by Scott Storch, KayGee and Terence "Tramp-Baby" Abney. It reached #10 in the Heatseekers albums chart. The second single, "I Refuse", produced by Scott Storch and released in 2006, reached #36 in the Billboard Hot R&B/Hip-Hop Songs chart. His third studio album, titled GRIII: Old School 2 Nu Skool, was released in 2009. The album featured a genre mix of Neo soul and Contemporary R&B. Urban Mystic is currently working on his fourth studio album entitled Love Intervention, the first single off his album is called "Name On It" It was released on April 3, 2012 via iTunes. Urban Mystic released his second single "I Promise" on October 9, 2012 on iTunes, His album "Love Intervention" will be released sometime in 2013.
"Best Part of the Day"