A stylish and contemporary four double bedroom family home occupying a generous South Westerly aspect garden plot situated on the outskirts of the village. The well presented accommodation benefits from a versatile layout having three separate reception rooms, in addition to the generous open plan kitchen/dining room which has bi-folding doors opening onto the patio. A useful utility room and cloakroom completes the ground floor. On the first floor there are four bedrooms generous double bedrooms and a family bathroom, three bedrooms have built in wardrobes and the two largest rooms feature contemporary en-suite shower rooms. The high specification of this property includes; zoned under floor heating throughout the ground floor and a solar assisted hot water system, top quality 'Siemens' kitchen appliances, and 'Villeroy and Boch' sanitary ware with chrome 'Hansgrohe' fittings. We highly recommend arranging a viewing to fully appreciate this quality home.
From our office turn right into the High Street towards Guildford continuing straight over two mini roundabouts and taking the second exit at the next roundabout signposted to Guildford. Continue down this road for approximately 1 mile and the property will be found on the left hand side.
The property is situated on the edge of Cranleigh village which is a large, attractive and vibrant village on the edge of the beautiful Surrey Hills, midway between Guildford and Horsham. It has a fantastic mix of shops, pubs, restaurants and cafes, from independent retailers to well known brands including M&S Food Hall and Sainsburys, as well as a weekly market. The village boasts a huge array of clubs and societies to suit many tastes as well as a leisure centre, arts centre, library, children's playgrounds, a choice of golf courses and a number of churches. Cranleigh is popular with families, with an excellent range of nurseries and well regarded private and state schools. The nearby towns of Guildford, Godalming and Horsham offer mainline train services to London.
Tiled floor, understairs storage cupboard.
Contemporary 'Villeroy and Boch' suite comprising wash hand basin and concealed cistern WC, part tiled walls and floor.
Bay window, front aspect, selection of bespoke fitted cupboards and shelves.
Feature fireplace with stone surround and granite hearth, solid fuel burning stove, Bi-folding doors opening onto rear patio.
Selection of base and wall mounted units, stainless steel sink with mixer tap, space and plumbing for washing machine and tumble drier, barn style back door.
Velux window, large boarded loft accessed via ladder. Linen cupboard housing hot water cylinder with solar assistance.
Double bedroom, featuring a generous selection of fitted wardrobe cupboards. Rear aspect.
Contemporary 'Villeroy and Boch' suite with 'Hansgrohe' fittings comprising fully tiled walk-in shower enclosure thermostatic shower, tiled vanity unit with 'His and Hers' wash hand basins, close coupled WC, wall mounted mirrored storage cupboards, chrome heated towel rail.
Spacious double bedroom, bay window with front aspect, built-in double wardrobe cupboard.
Contemporary 'Villeroy and Boch' suite with 'Hansgrohe' fittings comprising fully tiled shower enclosure with thermostatic shower, glass sliding door, close coupled WC and wash hand basin with mixer tap and storage drawer under, part tiled walls and tiled floor, chrome heated towel rail.
Spacious double bedroom, built-in double wardrobe cupboard, further eaves storage cupboard, front aspect.
Double bedroom, eaves storage cupboard, rear aspect.
Contemporary Villeroy and Boch white suite with comprising bath with mixer tap and shower attachment over with glass and chrome shower screen, wash hand basin with mixer tap and storage drawer under, close coupled WC, part tiled walls to wet areas, chrome heated towel rail.
The property is approached via a gravelled driveway which proceeds through the five bar gate into a parking area for several vehicles leading to double garage. Access to side of the property leads to the fantastic rear garden with the total plot measuring approximately ¼ of an acre in size and benefitting from a South Westerly rear aspect with mature hedge and close board fencing boundaries. Furthermore there is a generous area of paved patio with brick edging providing a lovely outside entertaining area.
Electronically operated up and over door, power and light points, wall mounted gas fired boiler for heating and hot water.


iPage, founded in 1998, is a US-based web host with an aim to provide hosting for personal websites and small online businesses. The hosting is of top quality and to compensate for the energy they're consuming iPage purchase renewable energy credits.
The hosting itself is affordable, qualitative and green. The plans include great features such as unlimited diskspace, add-on domains and a free domain name. The support team is professional and you can get in contact with thtem 24/7 via phone, email and live chat.


This is a two-day course that will focus on NeuroKinetic manual strategies of myofascial therapy. The course will focus on orthopedic and fascial anatomy assessment along with massage therapy and bodywork techniques that fit appropriate strategies of care. This course will allow the attendee to incorporate current manual therapy skills with new strategies of care supported by additional understanding of kinesiology and fascial anatomy.
After completing this course participants will be able to: Perform appropriate assessment utilizing special myofascial tests.
Determine, based on their assessment and clinical impression, proper soft tissue therapy management including immediate care, long term treatment, and/or referral.
Understand other health care techniques for management of myofascial dysfunction.
Utilize the latest manual therapy and soft tissue techniques for non-surgical challenges and contribute to the restoration of proper biomechanical function and reduction / elimination of pain.
Utilize specific myofascial stretching techniques to enhance extensibility and function of skeletal.
This course will focus on functional hands-on applications that can be incorporated immediately into a massage or bodywork session. The format will include lecture, demonstration, and practice with question—answer periods to ensure understanding and facilitation of information presented. There will be generous periods of learning-by-doing. All categories of soft tissue conditions will be covered, i.e. strains, sprains, and adhesions.
This course is designed for the massage therapist, and other professionals who possess fundamental massage therapy skills who are interested in predictable outcomes.


The second day of negotiations has begun, and the Scottish delegation has been busy both in and out of the conference room.
The day started with our daily ICAN meeting, which noted that attendees were generally pleased with the discussions of the previous day, and also mentioned the positive discussions that were had between delegates, wishing to strengthen the treaty where possible. 103 states participated in the negotiations which is an improvement on the number at the beginning of the previous discussions, and it is expected that others could join or participate in due course. Despite remarking positively on the negotiations, it was still agreed that there could be a greater emphasis on Human Rights law as well as Environmental Law with the draft treaty moving forward.
Not long into the morning session, where delegates continued their discussions on the Preamble, our colleagues at the World Council of Churches received confirmation of a meeting from the UK Mission office across from the United Nations. Keen to discuss the UK's position on the ban treaty as well as the UK's notable absence at the negotiations, Dagmar, Flavia, Janet and I joined, along with Dave from UK CND and Tim, from Quakers UK, while Andy remained in the negotiations room to take attendance of participating countries and to take notes on the continued proceedings.
While Chatham House Rule applies for the discussions had and we were aware there would be little room for manoeuvre, the group were able to discuss their differing views on the relationship between the Nuclear Proliferation Treaty to the Nuclear Ban Treaty, as well as the perceived security that nuclear weapons hold.
Journeying back to the United Nations in time for lunch, we attended the Side Event by Pugwash Conferences, where a panel discussed the challenges of being a host state to other nuclear weapon states. This was a particularly pertinent and interesting discussion for our Scottish team, because whilst Scotland's position of hosting nuclear weapons for the UK is quite unique, it holds some resemblance to that of host states who hold these weapons for nuclear states, but have little control. Whilst there was discussion on all of the host states in this situation, there was a greater discussion on the Netherlands position, as they are the only host state attending these negotiations. It was noted that whilst they made strong opening remarks yesterday about their allegiance and priorities to NATO as a pre-requisite of signing a treaty, their attendance here should still be commended, which shows an honesty and willingness on their part, to make progress.
Moving to the afternoon negotiations shortly after, the floor was opened to a variety of civil society representatives who gave their thoughts on the preamble. They highlighted a variety of issues, including the obligation to assist victims of nuclear weapons, the need for recognition of the disproportionate effects on indigenous people and the reminder of the long-lasting humanitarian consequences of nuclear weapons.
The official book launch of 'Disarming the Nuclear Argument: the truth about nuclear weapons', written by Tim Wallis was the next item on the agenda for the Scottish team. Janet, along with Dave Webb, Chair of UK CND, and Dr Rebecca Johnson, of the Acronym Institute, joined Tim in an open discussion session where they spoke about the arguments and importantly the rebuttals that can come from discussions with opponents to the ban treaty. A free copy of this book will be offered to all 130 delegates at the negotiations where it is hoped that this will give delegates greater information and answers to the common questions and queries surrounding disarmament. In attendance and contributing to the discussion were nuns Sister Ardath Platte and Sister Carol Gilbert, who have both served prison sentences for poring their own blood on a nuclear warhead.
Our Scottish team split up for the last part of our day, as Flavia, Dagmar and I attended the 'Student and Young People' Sign Making event for the march tomorrow, whilst Andy and Janet took part in the Sign Making event for the 'slightly older' generation. Momentum is certainly building for the march tomorrow, with it being widely discussed by many and we are hoping this is the case for the partner marches that will be going on throughout the world also. We hope that there will be a great turnout for the events worldwide, and that we are able to spread the word- 'Ban the Bomb'!


For many, the beard and moustache are a symbol of masculinity. Because the Needle technique leaves no scars, neither in the donor area nor in the receptor area, it is optimal for constructing or reconstructing facial hair. The hairline is the frame of the face. For a male with a desire to enhance his look, a natural beard can be achieved, even if Mother Nature has not been so generous. That is when hair transplant in Istanbul, Turkey can be the best option.
As the hair implant is done using the natural angles to the grafts, the outcome is a completely natural look.
Especially in the hair frontline, for the most natural results, it is the most appropriate technique.
The circular grafts are transplanted in circular holes, leaving a natural healing process with invisible scars.
Cost: The average cost of Beard Transplantation in Istanbul, Turkey is around €2,090/$2,395.
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text:
package namespace

import (
	"github.com/m3db/m3/src/metrics/metric/id"
)

// NewTestID creates a new ID for testing that always returns the namespace for TagValue.
func NewTestID(id, namespace string) id.ID {
	return &testID{
		id: []byte(id),
		ns: []byte(namespace),
	}
}

type testID struct {
	id []byte
	ns []byte
}

func (t testID) Bytes() []byte {
	return t.id
}

func (t testID) TagValue(_ []byte) ([]byte, bool) {
	return t.ns, true
}

redpajama_set_name: RedPajamaGithub


text:
Meet the 2013 Douglas Tweedale Fellows
Hassel Fallas Lopez
Media Organization: La Nación newspaper
Hassel Fallas Lopez is an editor and journalist with over a decade of experience in media and corporate communications in Costa Rica and Latin America. She holds a Masters in Digital Journalism from the University of Alcalá de Henares in Spain. For most of her career, she has focused on the areas of Economics and Business. Currently, she is working as a data-driven journalist in the Investigative Unit at La Nación newspaper. She is dedicated to analyzing databases and producing investigative reports, apps, and multimedia products about her findings. Her skills include a broad vision of national and international realities, team work, leadership, and capacity for decision-making. She is creative, organized, and has a passion for her job. She enjoys challenges and has the ability to learn quickly and obtain the required acumen to develop projects.
Vanessa Dezem
Media Organization: Valor Economico
Vanessa Dezem is a journalist and holds degrees in Journalism and Economics. She has six years of experience in writing articles for economics sections. She specializes in economic journalism but is proficient with multimedia production skills, printed newspapers, online publications, news agencies, broadcast TV, and radio shows. She is currently working as reporter in one of the biggest newspapers of Latin America - Valor Economico, in São Paulo, Brazil- with expertise in gathering information, breaking news, connecting subjects, and integrating media. She recently completed a Masters-level Digital Journalism program in Madrid, Spain. The program is well recognized as innovative in the area of new media; spreading the knowledge of news production platform integration and the development of new business models in the journalism field. She speaks Portuguese, English, German, and Spanish.
The Douglas Tweedale Memorial Fellowship
Becas Douglas Tweedale

redpajama_set_name: RedPajamaCommonCrawl


Fun, color and action were keys to creating interesting, informative and inviting nutrition choices for the students. From menus and aprons to truck signage, the desire was for fresh, cool and fun food choices—an image carried across all aspects of the program. Kids themselves were involved in selecting images integral to the program, guaranteeing the success of the program from the first tray to the last!


text:
package com.google.security.zynamics.binnavi.API.disassembly;

import static org.junit.Assert.assertEquals;
import static org.junit.Assert.assertNull;

import com.google.security.zynamics.binnavi.API.disassembly.CouldntSaveDataException;
import com.google.security.zynamics.binnavi.API.disassembly.Tag;
import com.google.security.zynamics.binnavi.API.disassembly.TagType;
import com.google.security.zynamics.binnavi.Database.MockClasses.MockSqlProvider;
import com.google.security.zynamics.binnavi.Tagging.CTag;
import com.google.security.zynamics.zylib.types.trees.ITreeNode;
import com.google.security.zynamics.zylib.types.trees.TreeNode;
import org.junit.Test;
import org.junit.runner.RunWith;
import org.junit.runners.JUnit4;

@RunWith(JUnit4.class)
public final class TagTest {
  private final ITreeNode<CTag> tagNode = new TreeNode<CTag>(new CTag(1, "Tag Name",
      "Tag Description", com.google.security.zynamics.binnavi.Tagging.TagType.NODE_TAG, new MockSqlProvider()));

  private final Tag tag = new Tag(tagNode);

  @Test
  public void testConstructor() {

    assertEquals("Tag 'Tag Name'", tag.toString());
    assertEquals("Tag Description", tag.getDescription());
    assertNull(tag.getParent());
    assertEquals(0, tag.getChildren().size());
    assertEquals(TagType.NodeTag, tag.getType());
  }

  @Test
  public void testSetDescription() throws CouldntSaveDataException,
      com.google.security.zynamics.binnavi.Database.Exceptions.CouldntSaveDataException {
    final MockTagListener listener = new MockTagListener();

    tag.addListener(listener);

    tag.setDescription("D1");

    assertEquals("D1", tag.getDescription());
    assertEquals("D1", tagNode.getObject().getDescription());
    assertEquals("changedDescription;", listener.events);

    tagNode.getObject().setDescription("D2");

    assertEquals("D2", tag.getDescription());
    assertEquals("D2", tagNode.getObject().getDescription());
    assertEquals("changedDescription;changedDescription;", listener.events);

    tag.removeListener(listener);
  }

  @Test
  public void testSetName() throws CouldntSaveDataException,
      com.google.security.zynamics.binnavi.Database.Exceptions.CouldntSaveDataException {
    final MockTagListener listener = new MockTagListener();

    tag.addListener(listener);

    tag.setName("N1");

    assertEquals("N1", tag.getName());
    assertEquals("N1", tagNode.getObject().getName());
    assertEquals("changedName;", listener.events);

    tagNode.getObject().setName("N2");

    assertEquals("N2", tag.getName());
    assertEquals("N2", tagNode.getObject().getName());
    assertEquals("changedName;changedName;", listener.events);

    tag.removeListener(listener);
  }
}


This is said to be one of the most special Hilton hotels in the world. Why? It had to be built in the style of the rest of the Castle area, and also with the ruins of the monastery from the 15th century that has been built into the hotel. The placement makes it a part of the Castle district which is on the World Heritage list of Unesco.
The hotel is not in the city center, but with a taxi you can easily reach it, or you can walk for 20 minutes, and you will be in the Vaci Street. You can also use the Castle Bus that will take you to Moszkva Square, and from there you can go with the red metroline.


text:
Crassula umbella is a succulent plant species in the genus Crassula. It is endemic to the Cape Provinces of South Africa.

Distribution
Crassula umbella is found from the Richtersveld and western Karoo through to the Little Karoo to Humansdorp.

Conservation status
Crassula umbella is classified as Least Concern as it is widespread and not in decline.

References

External links

Endemic flora of South Africa
Flora of South Africa
Flora of the Cape Provinces
umbella

redpajama_set_name: RedPajamaWikipedia


The committee of European Parliament on environmental issues supported the ban of disposable plastic tableware in the European Union since 2021.
is said About it in the statement on the website of the European Parliament.
will Be forbidden disposable plastic products, such as: tableware, ear sticks, plates, tubules, mixers for drinks and holders of balloons, products from plastic which decay under the influence of oxygen, thin plastic bags, products from plastic. 51 members of the committee voted for it, 10 acted against, 3 refrained.
Use of some other the products which do not have an alternative, to member states suggest to reduce to 2025. Disposable boxes for burgers, food containers for fruit, vegetables, desserts or ice cream belong to such objects.
Member states will develop national plans for encouragement of use of the products suitable for repeated use and also reuse and processing.
Other plastic products, such as bottles for drinks, it will be necessary to collect separately and to overwork of 90% till 2025.
the Problem of plastic waste - global. Such objects do not decay and litter the habitat. In August to the Mexican resort took out from the ocean of ton of plastic.


text:
This Will Be 'The Next Big Thing,' According to Richard Branson
BYBloomberg
Supersonic jetliner travel, which ended more than a decade ago with the Concorde, will make a comeback and transform the aviation industry in coming years, according to billionaire Richard Branson.
"The next big thing, hopefully in my lifetime, will be supersonic travel coming back and people traveling around the world in next to no time," Branson told Bloomberg Television in an interview in Washington Tuesday. "And hopefully in a relatively environmentally friendly way."
Branson's Virgin Galactic is already working with Boom Technology Inc. on its supersonic jet, and Japan Airlines Co. in December took an option to buy as many as 20 of the aircraft from the Colorado startup.
To read more about the return of supersonic travel, click here
Boom is planning to build a 45- to 55-seat aircraft that cruises at Mach 2.2 (about 1,500 miles per hour) — capable of whisking passengers between New York and London in about three hours. The Concorde, flown by British Airways and Air France, retired in 2003 after almost three decades in service as customers, weighed down by hefty operating costs, abandoned the jets.


An American style wheat beer made with pure Wisconsin honey. This cloudy looking hefe style (unfiltered) beer has a yeasty tone layered with a honey sweetness which makes this a refreshingly light brew.
This classic German-style pilsner is golden-straw in color and is well hopped with noble type hops that give this brew a nice crisp flavor profile. A bit of residual malt sweetness can be detected in the nose as well as the flavor.
Our owner Tom's homebrew recipe brought up to the big scale. Brewed with barley, wheat, corn, oats, rye and rice, you can expect this easy-drinking English ale to have a complex malt profile and be complimented with a nice hop balance.
An English-style India Pale Ale aimed to accent the hops used throughout the brewing process. The malt produces a biscuity flavor while a medium hop bite adds a flowery sharpness that finishes smooth.
A caramel sweet beer with a malty profile. This amber toned beer has low but apparent hops. Small hints of smokiness may be found throughout this well balanced brew.
This is a traditional oatmeal stout. Expect this, our darkest beer, to have a pleasant, full flavor and a smooth profile that may include coffee, chocolate and caramel notes. Bitterness is moderate and rounds out beautifully in the finish.
An English-Style stout with high-grade pure vanilla added during brewing. This sweeter flavored beer is vanilla forward but finishes with flavors of smooth chocolate, caramel, and coffee. It is a perfect end of night dessert-like beer.
An American Pale Ale filled with Citra and Cascade hops for a wonderfully fresh hop aroma.
We always have at least one specialty beer on tap. We brew numerous seasonal favorites as well as a few select new specialties every year to fill in the gaps.
Stone Arch brews its own line of gourmet sodas. Each recipe uses pure cane sugar and contains no artifical sweetners. Always available is Stone Arch Root Beer – a lighter colored, all-natural root beer, directly from the tap. Other selections are rotated for a greater variety.
Flavors: Blue Raspberry, Bubblegum, Cinnamon, Ginger Ale, Grape, Orange Cream, Vanilla Cream, Green Apple, and Wild Cherry.


text:
New Foundation Trustee Announced
Dame Kiri Te Kanawa has announced the appointment of Robert Wiremu as a new trustee for the Kiri Te Kanawa Foundation.
"I have enjoyed an association with Robert that spans more than 20 years so I was delighted when he accepted the invitation to join our dedicated and highly regarded Trustees and we know that his knowledge, expertise and holistic approach will be invaluable in our support of young New Zealand opera singers, particularly as the world we are now experiencing is and will continue to be a "moving feast" for these singers.
Well known in music circles as an experienced baritone, chorister, soloist and recording artist Robert is in constant demand as a teacher, repertoire coach, vocal consultant, adjudicator and artistic advisor – all the skills that will be so necessary in his new trustee role.
I'm really looking forward to working with him - he joins a marvellous group of trustees all with professional experience and expertise in a wide range of related areas. Most of whom have been with me since the Foundation was created in 2004."
Further details from Paul Gleeson, Foundation Administrator, 0275 944534
Joanna Foote to attend french music course19 Dec 2013
Messages from our foundation singers - Edward Laurenson22 Dec 2016
Singers to listen for22 Dec 2016
Kawiti Waetford reports from Cardiff18 Dec 2014


Brother Printer Support Number is an independent online service provider of remotely access technical support for third party products and services. All of we using third party trademarks, brand name, product and services is only referential.
Electronic industry is bursting with products of regional as well as global brands. Consumers normally go for the company that has a renowned name in the industry. Furthermore, they look for characteristics, quality along with the cost of the commodity. Smart consumers normally tend to purchase such products that give them the biggest of perks along with a reasonable price tag. In regards to printers, people usually go for Brother Printers because it possesses all that you require in the printer.
3.	It performs many tasks such as scanning, printing, and copying.
Being the most famous name in the Printer industry, Brother company concentrates on providing top-notch products and services to their precious consumers. Printers delivered by the company meet every requirement and needs of the home as well as office, small sized and medium sized companies along with extensive business corporations respectively. It is one of the most favored printers across the globe. You can perform various processes at the same time. These are the essential reasons which will surely convince you to get Brother printer. But, if you still have any apprehension or inquiry related to the features as well as functions of Brother printers, you should connect with the Brother Printer support.
Setup Brother Printer on a Wireless Network: Before getting to it, one needs to comprehend the prevailing wireless network setting which includes network name and the network key. Now, you only have to follow the process mentioned below. When you have gone through the process, you can setup Brother Printer on a wireless network.
1.	The very first thing to do is to connect your Brother printer to the power supply.
2.	After that, Tap the Menu button. Press the Up or Down buttons to select the Network and after that hit on the OK button.
3.	With the help of Up and Down keys, choose WLAN and then press the OK button.
4.	Then, select the Setup Wizard with the help of Up and Down keys and click on the OK button.
5.	The printer will begin to look for the network.
6.	A list of Service Set Identifiers will show up now.
7.	After that, pick the Service Set Identifier you wish to connect to and then click on the OK button.
- Type in the Network key only when you are applying an authentication method which needs a network key and after that give the WEP key and click on OK.
- Instead of determining an authentication method, if you have picked an open system method which has no encryption mode, then your Brother printer will get connected to the wireless device on its own.
- If the WLAN access router which is being used by the user supports WPS, then it will come up automatically.
- For connecting it to your device, hit the WPS button and thereafter hit the UP arrow key two times.
8. If neither of the steps mentioned above work, then review the status if it is now revealing "Connected" on the LCD of the Brother printer or not.
1.	Go to the official website of Brother Company.
2.	Click on the Downloads section.
4.	After that, submit the necessary information such as Printer model details, etc.
5.	Click on the button for Download.
1.	When the download process is over, you should just power off the Brother Printer and detach it from the computer it is connected to.
2.	After that, wait for a minimum duration of sixty seconds and then connect your Brother printer to the computer.
3.	Now, double-click on the driver setup file from the downloads folder.
4.	Select your language of preference.
Follow the directions displayed on the screen to finish the installation process. After you have successfully performed each of the steps mentioned above, you will be able to setup and install the Printer drivers in the computer very conveniently. Check that you have approved the auto-update mode as the computer as well as the drivers need to be updated from time to time.
How to Get Brother Printer Support?
Brother company always considers consumer comfort and ease. Therefore it offers the users fantastic Brother printer customer support service. The staff at Brother printer customer service consists of highly-trained professionals who are perpetually available to assist you in case of any obstacle or concern. To get on-the-spot support, you should dial the Brother Printer customer support number +1-800-295-0961 (US/Canada) (Toll-free). To go through the steps of standard errors and to know more about Brother printers and to get updates, you can go through the blog. The Brother customer support phone number is toll-free, and the lines are open day and night.
Prompt assistance with the Brother printer setup.
Troubleshooting Brother printer errors such as error 27.
Fixing overheating of Brother printers.
Download and installation of Brother printer software.


text:
Column: Padres should learn from success of A's and Rays
Oakland Athletics' Marcus Semien celebrates with Matt Olson after hitting a home run against the Texas Rangers last month in Oakland.
(ASSOCIATED PRESS)
Petco Park is good for revenues and franchise valuation, but hasn't led to on-field success of low-budget A's and Rays
By Tom Krasovic
A baseball rhyme is A's-Rays-Padres, and a baseball riddle is this:
Why do the A's and Rays continue to achieve much more baseball success than the Padres, despite the Padres playing in a palace while the A's and Rays slum it?
The A's and Rays will meet today in the American League's wild-card game after winning 97 and 96 games, respectively, this year.
The Padres, who've exceeded 92 victories just once in their 51 years, are coming off their ninth consecutive losing season.
The simple answer to the riddle is A's and Rays braintrusts are smart and nimble, which isn't to say the Pads are dummies.
Not even John Moores, for one, saw the A's being able to beat tall odds as often as they do.
Moores, in days as Padres owner, heaped praise on the A's braintrust of Sandy Alderson and Billy Beane — and later hired Alderson — but in the months before Petco Park opened in 2004, Moores also said this of the A's:
"I don't think they can keep it up."
Moores said a new ballpark would allow teams of less economic means, like the A's, Rays and Padres, to muster more than sporadic success.
While he never promised any World Series titles for the Pads because of a new ballpark, Moores said the venue that would open in the East Village would make the Padres more competitive on the field.
He wasn't alone. Team CEO Larry Lucchino, smooth broadcaster Ted Leitner and Padres players spun the "competitive" pitch over and over.
The logic made sense: A new ballpark enhances team revenues and thus greater investments in Padres baseball, to some degree.
The A's and Rays, meantime, were unable to get voter approval for a massive ballpark subsidy. They remained in venues that were inferior to Petco Park and many others, both in amenities and ability to increase revenues.
I wrote in August that Pads leaders should study the Rays, who probably get more from the revenue dollar than any big-league franchise.
As for the A's, what I heard this week from MLB sources is winning 97 games each of the past two season was worthy of a standing ovation.
The MLB folks ticked off common traits between the A's and Rays. A "what do we have to lose" approach, which is encouraged by underdog status. A nucleus of leaders who've stayed together a long time, headed in Oakland by executives Billy Beane, David Forst and Billy Owens (and much-praised manager Bob Melvin). A resolve to zig when the industry is zagging. A habit of buying low on talent, and moving on from players in question a year early, instead of a year later. A belief in constant flux at the bottom of the roster, to give low-cost players a chance to emerge.
As for current A's stars, the team's "traditional" scouting, more so than analytics, earned gold stars for the first-round draft selections of Matt Olson and Matt Chapman, the latter a Brooks Robinson-type defender. Both have hit better than a lot of the thinking at the time of their draft selection.
There was praise for the work former A's infield coach Ron Washington (now the third-base coach in Atlanta) did with shortstop Marcus Semien, a MVP contender acquired in a 2014 trade with the White Sox, and for the A's being patient with Semien, which dovetailed with their "what do we have to lose" approach.
Circa 2003 Moores was right about the A's in one important aspect: The A's were unable to maintain their torrid pace of the early 2000s, when they reached the playoffs from 2000-03.
But staying in the Coliseum, which is like the Jack Murphy Stadium of Oakland, only with a history of sewage-line ruptures, doesn't seem to have overly tied their hands. Perhaps it even fostered some innovation.
In the 16-year Petco Era, the A's have logged eight winning seasons and six playoff berths.
While they've reached no World Series in that span and probably won't get there this month, that's the kind of competitiveness the Pads implied they'd muster if San Diegans voted them a ballpark subsidy. It hasn't worked out that way (five winning seasons, two playoff berths).
Thankfully, Petco Park delivered on other pitches from its advocates. And in 2020, the target year of team ownership for a playoff push, we'll see if the Pads can finally play like the less-wealthy A's and Rays.
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Tom Krasovic
Chargers/Rams
Column: New Chargers coach Brandon Staley raises hopes — and concerns
Rise of Rams, Bills, Browns rise could bode well for Staley; Urban Meyer wasn't a fit for Los Angeles team
Column: Patrick Mahomes doesn't finish Chiefs victory, but don't count out Andy Reid's team
Chiefs boss showed what it means to coach to win, sending K.C. to third straight AFC title game
Column: Packers' Aaron Rodgers getting better bounces in latest Super Bowl quest
"San Diego guy" leads Packers past Rams in Green Bay, reaches fifth NFL championship game
Column: Cleveland Browns' road playoff victory takes USD coach back to '69
Dale Lindsey was the middle linebacker on previous Browns team to win a road game in the playoffs
Column: Packers, Chiefs see playoff odds improve, thanks to first-round upsets by Rams, Browns
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text:
\section{Introduction}
\label{1}
The H.E.S.S. Galactic Plane Survey (HGPS) has recently completed nine years of continuum observations in the 250$^\circ$-65$^\circ$ longitude range for latitudes $\rvert$\textit{b}$\rvert$ $\leq$ 3$^\circ$ \citep{HESS18a}. Observations towards the region containing the known pulsar wind nebula (PWN) HESS~J1825$-$137 show a new source named HESS~J1826$-$130, which emerges towards the north of HESS~J1825$-$137 and whose origin is still unknown (see Fig.~\ref{Figure1}).

HESS~J1825$-$137 is one of the brightest and most extensive PWN detected at very high energies (VHEs) \citep{HESS2018d}. It has been proposed that this TeV source is powered by the high spin-down luminosity ($\dot{E}$ = 2.8~$\times~10^{36}$ erg s$^{-1}$) pulsar \object{PSR~J1826$-$1334} \citep{Manchester05}. This pulsar is located at a distance of $\sim$4~kpc based on dispersion measurements \citep{Cordes02} and its spin-down age is $\sim$20~kyr. The pulsar is about 10\m~offset from the peak of HESS~J1825$-$137. This TeV source was the first to exhibit an energy dependent morphology characterized by a spectral steeping with increasing distance from the pulsar. In the GeV range, observations made with {\it Fermi}-LAT showed both morphological similarity and spectrum continuity with the H.E.S.S. data \citep{Grondin11}.

{\XMM} observations towards PSR~J1826$-$1334 show a bright and elongated core that is $\sim$30$^{\prime\prime}$ in size  with a hard photon index ($\Gamma$~$\sim$~$1.6$), which is embedded in a fainter diffuse component of emission that extends $\sim$$5^{\prime}$ with a softer photon index ($\Gamma$~$\sim$~$2.3$) and is located on the southern side of the pulsar \citep{Gaensler03}. This spectral behaviour is remarkably similar to that observed in $\gamma$-rays, except that the spatial scales are different (few arcmin in X-rays, fraction of a degree in $\gamma$-rays). Inside the compact nebula, {\Chandra} data reveal a small component ($\sim$7$^{\prime\prime}\times3^{\prime\prime}$) elongated in the NE-SW direction. The extended X-ray emission is detected in these observations up to at least $2^{\prime}.4$ south of the pulsar \citep{Pavlov08}.

The offset and asymmetrical nature of the emission in the X-ray and $\gamma$-ray ranges have been explained by \citet{Gaensler03} and \citet{Aharonian2006a} using the scenario known as ``crushed PWN'' \citep{Blondin01}. In this framework, the supernova remnant (SNR) blastwave expands into an inhomogeneous interstellar medium (ISM). Consequently, an asymmetric reverse shock is generated, which returns from higher density regions first, reaching one side of the PWN sooner than the other side, then pushing the X-ray and TeV emission mainly towards regions of lower ambient density.

In the radio band, the region around PSR~J1826$-$1334 has been explored at 8.3~GHz by \citet{Frail97} and at 1.4~GHz by \citet{Gaensler00} using the Very Large Array (VLA). However, in both cases the observations failed to detect nebular emission down to the respective sensitivity limits (rms noise levels of 0.2 and 0.5~mJy~beam$^{-1}$ at 8.3 and 1.4~GHz, respectively).

\begin{figure*}
\center
\vspace{1cm}
 \includegraphics[width=0.7\textwidth]{Figure1_low-res.eps}
\caption{HESS~J1825$-$137 and HESS~J1826$-$130 $\gamma$-ray excess map ($E$ $>$ 0.2~TeV) extracted from the on-line material of the HGPS \citep{HESS18a}.{\protect\footnotemark} The wedge is shown in units of $\mathbf{10^{-13}}$~ph~cm$^{-2}$~s$^{-1}$ the TeV flux. The plus signs indicate the position of the pulsars PSR~J1826$-$1334 and PSR~J1826$-$1256, and the diamonds the best-fit position of the TeV sources.}
\label{Figure1}
\end{figure*}
\footnotetext{\url{https://www.mpi-hd.mpg.de/hfm/HESS/hgps/}. The image corresponds to the file {\itshape hgps\_map\_significance\_0.1deg\_v1.fits.gz}.}

Regarding HESS~J1826$-$130, it is a new unidentified extended TeV source previously hidden in the emission from the bright nearby PWN HESS~J1825$-$137 \citep{HESS18a}. Fitting the excess map with a 2D symmetric Gaussian, \citet{anguner17} estimated the best fit-position of HESS~J1826$-$130 to be R.A.=18\hh 26\mm 0\ss.2, Dec.=$-$13\d 02\m $1^{\prime\prime}.8$~(J2000) with an extension of {0.17\d} $\pm$ $0.02^\circ_\mathrm{stat} \pm 0.05^\circ_\mathrm{sys}$.

Based on their spatial coincidence, HESS~J1826$-$130 has been associated with the \object{PWN~G18.5$-$0.4} (also known as `Eel' PWN), which is a diffuse and weak non-thermal X-ray nebula detected with {\Chandra} \citep{Roberts07}. This PWN is probably powered by the pulsar PSR~J1826$-$1256, which lies within the VHE emission region $5^{\prime}.4$ offset from its centroid, and now is notable for being one of the brightest radio-quiet $\gamma$-ray pulsars \citep{Acero15}. Nevertheless, within the extension of HESS~J1826$-$130 there are other potential sources of energetic particles capable to power the TeV emission, such as radio SNRs and HII regions \citep{paron13}, and this fact hampers a decisive conclusion on the origin of the $\gamma$-rays.

In this paper we report on new high-resolution and high-sensitivity radio observations carried out with the Karl G. Jansky Very Large Array (JVLA)\footnote{The Very Large Array of the National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.} towards PSR~J1826$-$1334 with the aim to detect the radio counterpart of the PWN detected at high and VHEs. In addition, we present a new X-ray study carried out with archival data acquired with the {\XMM} satellite of the PWN~G18.5$-$0.4 to investigate its connection with HESS~J1826$-$130 and shed light on the origin of this TeV source.

\section {Observations and data reduction}
\subsection {New radio observations}
We carried out observations centred on PSR~J1826$-$1334 using the B and C configurations of the JVLA
\footnote{Further information on the JVLA array configurations is reported at \url{https://science.nrao.edu/facilities/vla/docs/manuals/propvla/array_configs}.}
The data were taken at L band using the wide-band 1 GHz receiver system centred at 1.4 GHz, which consists in 16 spectral windows with a bandwidth of 64 MHz each, spread into 64 channels. These observations are under the project 12A-166, which was intended to carry out deep full-synthesis imaging of intensity of the nebular radio emission from the vicinity of the scientific target source.

The observing details are summarized in Table~\ref{data}. All the data were reduced using the capabilities within the CASA software infrastructure.

\begin{table}[h!]
\centering
\caption{Summary of JVLA observations}
\label{data}
\begin{tabular}{ccc}\hline\hline
  Date           &   Config.  &  Integration time [min]  \\ \hline
  2012 ~Feb. 05  &      C     &         90               \\
  2012 ~Feb. 18  &      C     &         90               \\
  2012 ~Jun. 20  &      B     &         90               \\
  2012 ~Jun. 21  &      B     &         60               \\ \hline
\end{tabular}
\end{table}

After an initial data inspection and editing, the calibration was done according a standard procedure separately for each of the four observing dates. This includes determinations of antenna position and delay corrections, as well as complex antenna gains and bandpass solutions. For the four datasets observations of the primary flux density calibrator \object{3C~286} were used, in reference to a model of the flux distribution of the calibrator source, to calculate the antenna-based gain (amplitude and phase) corrections and to derive the flux of the phase calibrator \object{J1834$-$1237}. The source 3C~286 was also used to correct the bandpass.

After the calibration was applied, the data of the scientific target PSR~J1826$-$1334 was split out from all of the observations listed in Table~\ref{data} and the individual files were imaged together using the capability incorporated in the CASA task tclean. Two rounds of phase-only self-calibration were performed to improve the dynamic range. It was found that a further amplitude calibration iteration was not necessary as it showed very little additional improvements on the image results. The self-cal process was made with a multi-scale technique with three different scale sizes and a robust parameter of 0.5. A wide-field imaging technique based on the W-projection algorithm was also applied during the imaging process to take account the non-coplanar nature of the JVLA baselines as a function of the distance from the phase centre.

The synthesized beam of the final L-band image after combining the four datasets described in Table~\ref{data} and including primary beam corrections is 9.$^{\prime\prime}$24$\times$6.$^{\prime\prime}$43 with a position angle PA=0$^{\circ}$.05. The sensitivity achieved in the L-band image, without primary beam corrections applied, is 0.24~mJy~beam$^{-1}$.

\subsection {X-Ray data}
We reprocessed unpublished archival {\XMM} data (obs. ID \#0744420101) towards \object{PSR~J1826$-$1256} to analyse the properties of the extended X-ray emission. The EPIC-pn camera was operated in the small-window mode, which partially covers the extent of the PWN around PSR~J1826$-$1256. On the other hand, EPIC-MOS1 and MOS2 cameras were set in the full-frame mode and hence mapped the full extension of the nebula. We employed the two EPIC-MOS cameras for the analysis of the X-ray emission of the PWN and the three cameras for the spectral study of the pulsar.

We reduced the observation and extracted the scientific products using the software packages SAS 16.1.0 and Heasoft 6.22.1,
following standard procedures described in the SAS Sciences Threads.\footnote{\url{https://www.cosmos.esa.int/web/xmm-newton/sas-threads}.} After obtaining calibrated event files using the latest current calibration files (CCF), we constructed a light curve in the high-energy band ($> 10$~keV) to filter periods of high count-rate. We applied FLAG = 0 and PATTERN $\leq 12$ and 4 for MOS and pn cameras, respectively.
We obtained filtered event files with 124, 128, and 91 ks for the MOS1, MOS2, and pn cameras, respectively. We constructed individual images from MOS1 and MOS2 cameras in the 1-7~keV band, the energy range where we detect emission, and combined these into a mosaicked and exposure-corrected image with a spatial scale of 3\s/pix. The final image was smoothed by convolving it with a 2D Gaussian function with $\sigma = 3$ pixel.

\section{Results and discussion}
\subsection{HESS~J1825$-$137}
The main panel of Fig.~\ref{Figure2} shows the new JVLA radio image at 1.4 GHz centred on the position of PSR~J1826$-$1334. As the primary beam of the interferometer at the mentioned frequency is about 30$^{\prime}$, the data only cover the northern half of the source HESS~J1825$-$137. Especially prominent is the emission from two objects in the surveyed field. One of these sources, with its brightness peak at R.A.=18\hh 26\mm 1\ss.7, Dec.=$-$13\d 38\m 14$^{\prime\prime}$.6~(J2000),  is in positional coincidence with the HII region G017.928$-$0.677 and most likely represents thermal emission associated with ionized gas \citep{anderson11}. The catalogued kinematical distance to this thermal source is $\sim$13~kpc, based on recombination-line emission detected at $\sim$39~km~s$^{-1}$ with the NRAO Green Bank 140-foot telescope \citetext{\citealt{anderson11}, see also \citealt{roman-duval09}}. The emission centred at R.A.=18\hh 25\mm 37\ss.5, Dec.=$-$13\d 36\m 41$^{\prime\prime}$~(J2000) is catalogued as NVSS~ J182538$-$133637 in the 1.4~GHz NRAO VLA Sky Survey \citep{condon98} and referred to as source ``C'' in \citet{Pavlov08}. To the best of our knowledge, the literature does not contain a counterpart that helps to discern its nature.

A zoomed view of the region surrounding  PSR~J1826$-$1334 is shown in the upper left corner of Fig~\ref{Figure2}. This image shows, for the first time, emission from a bright region  around the pulsar with a size of about 20\s, in good agreement with the size of the X-ray compact component of the PWN reported by \citet{Gaensler03}. We estimated the total flux density of this structure, detected at 4$\sigma$ above the noise level, in $\sim$4~mJy. The brightest central portion of the compact radio component, which is comparable in size to the angular resolution of our observations,  harbours the pulsar. Its contribution to the flux calculated over all the compact component is about 3~mJy. We highlight that this result is largely consistent with the flux density determination for PSR~J1826$-$1334 reported by \citet{kijak07}, on the basis of the total on-pulse energy measured over the pulse period around 1~GHz using the Giant Metrewave Radio Telescope \citetext{see also the compatible estimates presented in \citet{jankowski18} and references therein}.

The enlargement included in the new image at 1.4~GHz (Fig.~\ref{Figure2}) also shows, at 2$\sigma$ above the noise, a feature extending to the north of the pulsar position. Even though the detection occurs at a low level, the internal structure of this faint feature suggests that it could be real. If it were, we are likely observing part of the X-ray PWN. To confirm this, further observations with higher sensitivity are required. In addition, further polarization and spectrum studies are needed since a high degree of polarization ($\gtrsim 10\% $) and a flat radio spectral index ($ -0.3 \leq \alpha \leq 0$, S $\propto \nu^{\alpha}$,  where $S$ is the flux density, $\nu$ the frequency and $\alpha$ the radio spectral index) are two unmistakable properties of PWNe in the radio band \citep{Gaensler06}.

\begin{figure*}
\center
\vspace{1cm}
\includegraphics[width=0.7\textwidth]{Figure2_low-res.eps}
\caption{Main panel shows the radio continuum image at 1.4 GHz of the region surrounding the pulsar PSR J1826$-$1334 constructed using B and C arrays of the JVLA. The intensity scale is based on a square root relation in units of mJy beam$^{-1}$. The final beam size, shown in the bottom left corner, is 9.$^{\prime\prime}$24$\times$6.$^{\prime\prime}$43 while the rms noise level is 0.24~mJy~beam$^{-1}$ without considering attenuation of the primary beam. The catalogued HII region G017.928$-$00.677 is also labelled \citep{anderson11}. The inset shows the radio continuum emission on the region surrounding the PSR J1826$-$1334, whose position is marked by a black plus sign.}
\label{Figure2}
\end{figure*}

The non-detection in the radio band of a PWN detected at high energies is not an unusual result. Indeed, there are a large number of pulsars for which the search of radio PWNe yielded negative results \citep [e.g.][]{Gaensler00,Giacani14,cas2016}. In most of these cases, the failure to detect the nebular emission has been explained as a consequence of  either  a high magnetic field of the pulsar that inhibits the production of synchrotron radiation at longer wavelengths, or  severe adiabatic losses that occur in young and energetic pulsars producing under luminous radio PWNe if they evolve in a very low ambient density ($\sim$0.003~cm$^{-3}$).
Nevertheless, neither of the two conditions are satisfied for PSR~J1826$-$1334. On one hand, taking into account the parameters of the pulsar ($P$ = 101~ms and $\dot{P}$ = 7.52 $\times$ 10$^{-14}$~s~s$^{-1}$, \citet{Clifton98}), we estimated its magnetic field strength in about 2.8~$\times$~10$^{12}$~G, a value typical of young pulsars in SNRs. On the other side, the requirement of an ambient of very low density is not consistent with the presence of several dense molecular regions in the vicinity of the pulsar at its kinematic distance \citep{voisin16}.

Even though the two conditions invoked to account for the lack of an associated radio nebula fail to explain the case for PSR~J1826$-$1334, we can quantify our non-detection. To do this, we characterized the luminosity integrated between 10$^{7}$~Hz and 10$^{11}$~Hz of the putative radio PWN by L$_{\mathrm{R}} \equiv \epsilon\,\dot{\rm E}$~erg~s$^{-1}$, where $\dot{\rm E}$ is the associated spin-down luminosity of the pulsar and $\epsilon$ is the efficiency of conversion of $\dot{\rm E}$ in radio emission. Assuming that typical values for the efficiency ($\epsilon$$\simeq$10$^{-4}$) and the spectral index ($\alpha$=$-$0.3) measured in radio PWNe \citep{Gaensler06} are also valid for the case of PSR~J1826$-$1334, we obtained an upper limit for the flux density at 1.4~GHz of $\sim$400~mJy; this upper limit is calculated using the relation $S= 2.15 \times 10^{5} \epsilon \dot{\rm E}_{34}$ $d^{-2}$~mJy, where $d$ is the distance to the pulsar in kpc and $\dot{\rm E}_{34}$ is in units of 10$^{34}$~erg. If the extension of the supposed PWN were at least the same as that of the X-ray nebula observed with {\XMM} satellite (ellipsoid $\sim$5$^\prime$ $\times$ 4$^\prime$ in size), then the limit of the detection would be $\sim$0.3~mJy~beam$^{-1}$, i.e. of the order of the rms noise level of our radio observations. Morever, in the case in which the size of the radio PWN were comparable to that observed in $\gamma$ rays, the corresponding limit for its detection in radio would be even one order of magnitude lower.

\subsection{HESS~J1826$-$130}

\subsubsection{X-ray imaging and spectral analysis}
\label{X_spec}
Figure~\ref{Figure3}a shows the X-ray emission towards PSR~J1826$-$1256 in the 1-7~keV energy band with overlaid contours of the TeV emission from HESS~J1826$-$130, for reference, while panel b of Fig.~\ref{Figure3} indicates a brightness profile. This profile was constructed from a mosaicked image using data from the MOS1 and MOS2 cameras with a spatial scale of $1.5^{\prime\prime}/\rm{pix}$. No exposure correction and smoothing was applied.
We defined rectangular boxes of $130^{\prime\prime}\times 14^{\prime\prime}$  placed along the most intense X-ray emission. For the background, we used rectangular regions of $60^{\prime\prime}\times 14^{\prime\prime}$ orientated in the same way as the source boxes and placed outside the diffuse emission. We defined the box containing the pulsar J1826$-$1256 as the reference position to measure boxes distances.

The large-exposure {\XMM} observation allows us to identify some morphological features not detected in previous imaging studies performed with {\Chandra}. Indeed, the asymmetric and non-uniform distribution of the X-ray emitting gas around PSR~J1826$-$1256 is shown in Fig.~\ref{Figure3}. Bright emission is observed ahead of the pulsar up to a distance of $\sim$$1^{\prime}$ (Fig.~\ref{Figure3}b). We notice, however, that this emission may be due to projection effects. An enlargement showing the detailed X-ray morphology is presented in Fig.~\ref{Figure4}a.
The bulk of the emission comes from an elongated feature with an elliptical shape of $\sim$$6^{\prime}\times2^{\prime}$ (major $\times$ minor-axis), which appears brighter around the pulsar and extends towards the southwest in the direction of the TeV source. We refer to this feature as the ``bar'' and we associate it with the ``tail'' identified by \citet{Roberts07} in the {\Chandra} image. These authors suggested that the shape of the X-ray PWN could be caused by the motion of the pulsar which leaves behind a high-energy trailing nebula. The bar is surrounded by faint and diffuse emission that is more prominent towards the southeast. PSR~J1826$-$1256 appears slightly displaced from the apparent axis of the bar (indicated with a green line in Fig.\ref{Figure4}a).

Several point-source candidates are seen in the field in the {\Chandra} Source Catalog (CSC; \citealt{eva10}) and in the {\XMM} Serendipitous Source Catalog (3XMM DR8; \citealt{Rosen16}). We identified the brightest sources that appear over the bar (indicated with red circles in Fig.\ref{Figure4}a) and excluded these from the spectral analysis. To obtain the overall properties of the PWN, we extracted the spectrum of the bar from the ellipse shown in Fig. \ref{Figure4}a. The background was chosen from a circular region free of diffuse emission and excluding the point sources over it. We obtained individual spectra for MOS1 and MOS2 with minimum of 30 cts/bin. Inspection and fitting of the spectra was done using Xspec 12.9.1. The spectra are hard and show a continuum with no hint of emission lines (see Fig.~\ref{Figure4}b).
We simultaneously fitted the MOS1 and MOS2 spectra in the 1-7~keV energy band with an absorbed power-law model ($wabs \times powerlaw$). The results are shown in Table \ref{tab_X1}. The reported flux was calculated in the 0.5-8.0~keV energy band and this flux is\ used in Sect.~\ref{hess} to analyse the possible connection between the X-ray PWN and HESS~J1826$-$130.

\begin{figure*}[ht!]
\centering
\includegraphics[width=0.90\linewidth]{Figure3_low-res.eps}
\caption{\bf a. \rm  X-ray emission towards PSR~J1826$-$1256 in the 1-7~keV energy band. Cyan contours correspond to 9.5, 10.5, and 12 counts/pixel. The position of the pulsar is indicated with a plus sign. Green contours trace the TeV emission from HESS~J1826$-$130 at levels of (1.5, 1.8, and 2.1)~$\times$~$10^{-13}$~ph~cm$^{-2}$~s$^{-1}$. \bf b. \rm A brightness profile along the PWN (solid line) and the adjacent background (dashed line). The rectangular box in the inset image  indicates the regions from which the radial profile was extracted.}
\label{Figure3}
\end{figure*}

\begin{figure*}[ht!]
\centering
\includegraphics[width=0.9\linewidth]{Figure4_low-res.eps}
\caption{\bf a. \rm Regions used for the spatially resolved spectral analysis. Red circles are likely point sources excluded from the extraction regions. The circle inside box 1 was used to exclude the emission of the pulsar from the surrounding diffuse emission. \bf b. \rm MOS1 (black) and MOS2 (red) spectra of the bar in the 1-7~keV band. The solid lines represent the best fit for an absorbed power-law model.  }
\label{Figure4}
\end{figure*}

\begin{table*}[ht!]
\caption{Spectral analysis parameters of the diffuse emission from the PWN and the pulsar PSR~J1826$-$1256. For the PWN we used MOS1 and MOS2 cameras, while data from the pn camera was also considered for analysing the emisson from the pulsar. Spectral fitting with an absorbed power law was performed in the 1-7~keV energy band. The symbol ($^{*}$) indicates that the parameter was fixed during the fitting process. The value $F$ is the absorption corrected flux calculated in the 0.5-8.0~keV energy band. Quoted errors correspond to the 90\% confidence range.}
\label{tab_X1}
\small
\centering
\setlength{\extrarowheight}{5pt}
\begin{tabular}{cccccc}
\hline\hline
Region        & Total counts & $\chi^{2}_{\nu}$ (d.o.f.) & $N_\mathrm{H}$        & $\Gamma_X$       & $F$~(0.5-8.0~$\rm{keV})$            \\
              &              &                           & [$10^{22}$ cm$^{-2}$] &                  & [$10^{-13}$~erg~s$^{-1}$ cm$^{-2}$] \\\hline
Bar (ellipse) & 24600        & 1.02 (212)                & $1.89 \pm 0.26$       & $1.79 \pm 0.17$  & $13.4 \pm 0.4$                      \\
Pulsar        & 3300         & 1.05 (156)                & $1.89^*$              & $1.42 \pm 0.12 $ & $1.22 \pm 0.06$                     \\
Pulsar        & 3300         & 1.04 (155)                & $1.59 \pm 0.42$       & $1.26 \pm 0.25 $ & $1.14 \pm 0.06$                     \\\hline
\end{tabular}
\end{table*}

Taking advantage of the high number of counts of the {\XMM} observations, we performed a spatially resolved spectral analysis to look for variations of the photon index $\Gamma_X$ along the diffuse emission. We extracted individual spectra from nine rectangular boxes located along the bar (see Fig.~\ref{Figure4}a) from MOS1 and MOS2 cameras excluding the point sources. We defined the distance $r$ among boxes as the separation between their centres and the centre of box 1, which contains the pulsar J1826$-$1256. This is indicated in Fig.~\ref{Figure4}a with a green arrow. Spectra were binned to a minimum of 30 cts/bin. For each box, the two spectra are simultaneously fitted with a power-law model in the 1-7~keV energy band, keeping the hydrogen column density frozen to the best-fit value obtained for the whole diffuse emission, namely $N_\mathrm{H}=1.89\times10^{22}$~cm$^{-2}$.
The results are summarized in Table~\ref{tab_X2} and plotted in Fig.~\ref{Figure5}. The top panel in Fig.~\ref{Figure5} shows the variation of the photon index variation $\Gamma_X$ with respect to $r$. The softening of the spectrum is remarkable, where $\Gamma_X$ increases from $\sim$1.6 around the pulsar (boxes 0-2) up to $\sim$ 2.7 in the outer regions (boxes 7 and 8). This behaviour has been observed in several Galactic PWNe, such as G0.9+0.1 \citep{porquet03}, 3C~58 \citep{bocchino01a}, and G21.5$-$0.9 \citep{safi01}, among others. The spectral softening is a consequence of the underlying synchrotron radiation mechanism responsible for the non-thermal emission in the keV band. Highly energetic electrons cool faster than low energetic electrons after having travelled a short distance from the powering pulsar while they diffuse throughout the pulsar wind.
On the other hand, the surface brightness {\SB}, which is defined as the ratio of the absorption corrected flux in the 1-7~keV band and the area of the corresponding region, decreases with increasing distance to the powering pulsar, as shown  in the bottom panel of Fig.~\ref{Figure5}. This is a consequence of the synchrotron radiation mechanism responsible for the X-ray emission from PWNe \citep{holler12}.

For the spectral study of the pulsar PSR~J1826$-$1256 we used the three cameras (MOS1, MOS2, and pn) and extracted the corresponding spectra from a circular region of radius $14^{\prime\prime}$. Spectra were binned to a minimum of 15 cts/bin. For the background, we defined an annular region with inner and outer radii of $20^{\prime\prime}$ and $80^{\prime\prime}$, respectively. X-ray emission from pulsars may correspond to black-body (BB) emission from the neutron star surface and/or to non-thermal synchrotron emission from the magnetosphere. To look for non-thermal emission from the pulsar, we fitted the spectra with an absorbed power-law model. Letting $N_\mathrm{H}$ to vary freely or freezing it to the best-fit value of the diffuse emission ($N_\mathrm{H} = 1.89\times 10^{22}$ cm$^{-2}$) gives statistically acceptable fits ($\chi^{2}_{\nu} \simeq 1.05$) and model parameters that agree within the uncertainties (see Table \ref{tab_X1}).
Fitting the spectra with an absorbed BB ($wabs \times blackbody$) and $N_\mathrm{H}$ fixed to $1.89\times 10^{22}$ cm$^{-2}$ yields a statistically poorer fit ($\chi^{2}_{\nu} \simeq 1.45$), which fails to model the low-energy part of the spectra ($E<3$~keV). Letting $N_\mathrm{H}$ to vary freely results in a better fit ($\chi^{2}_{\nu} \simeq 1.03$) but a hydrogen column density of $\sim$0.2$\times 10^{22}$ cm$^{-2}$ is obtained in this case, which is about an order of magnitude lower than the column density for the diffuse emission. If PSR~J1826$-$1256 is powering the PWN, we would expect a similar ISM absorption. Moreover, the obtained BB temperature ($\sim$1.6~keV) is higher than expected for young pulsars, which usually have BB temperatures $\lesssim$$\,0.5$~keV \citep{mereghetti11}. We therefore conclude that the model which better fits the X-ray emission from PSR~J1826$-$1256 is a power law with the hydrogen column density similar to that obtained towards the PWN, as expected if they are associated sources.

\begin{table*}[ht!]
\caption{Parameters of spatially resolved spectral analysis of the bar feature. We used MOS1 and MOS2 cameras. The value $r$ is the distance between the centre of each box and box 1 (see Fig.~\ref{Figure4}a), where PSR~J1826$-$1256 appears projected. Spectral fitting with an absorbed power law was performed in the 1-7~keV energy band, keeping $N_\mathrm{H}$ frozen to $1.89 \times 10^{22}$~cm$^{-2}$. Quoted errors indicate the 90\% confidence level uncertainties.}
\label{tab_X2}
\small
\centering
\setlength{\extrarowheight}{5pt}
\begin{tabular}{ccccccc}
\hline\hline
Box &  $r$      & area           & Counts & $\chi^{2}_{\nu}$ (d.o.f.) & $\Gamma_X$       & {\SB}~(1-7~$\rm{keV})$                           \\
    &  [arcmin] & [arcsec$^{2}$] &        &                           &                  & [$10^{-17}$~erg~s$^{-1}$~cm$^{-2}$~arcsec$^{-2}$]\\\hline
0   &  $-0.62$  & 1650           & 1242   & 1.04 (39)                 & $1.66 \pm 0.34$  & $2.28 \pm 0.31$                                  \\
1   &  $0$      & 3160           & 2646   & 1.04 (84)                 & $1.54 \pm 0.18$  & $2.73 \pm 0.22$                                  \\
2   &  $0.74$   & 5100           & 4128   & 1.15 (129)                & $1.58 \pm 0.15$  & $2.65 \pm 0.18$                                  \\
3   &  $1.48$   & 5100           & 3967   & 0.96 (124)                & $1.70 \pm 0.16$  & $2.36 \pm 0.17$                                  \\
4   &  $2.21$   & 4833           & 3602   & 1.05 (111)                & $1.86 \pm 0.21$  & $1.96 \pm 0.18$                                  \\
5   &  $2.93$   & 5080           & 3782   & 0.90 (116)                & $1.95 \pm 0.19$  & $2.11 \pm 0.18$                                  \\
6   &  $3.66$   & 5080           & 3616   & 1.07 (113)                & $2.16 \pm 0.22$  & $1.88 \pm 0.18$                                  \\
7   &  $4.39$   & 5100           & 3501   & 0.87 (168)                & $2.70 \pm 0.31$  & $1.75 \pm 0.19$                                  \\
8   &  $5.27$   & 5534           & 2739   & 0.99 (86)                 & $2.71 \pm 0.37$  & $1.27 \pm 0.16$                                  \\\hline
\end{tabular}
\end{table*}

\begin{table*}[h]
\caption{Parameters of PSR~J1826$-$1256, the X-ray PWN and HESS~J1826$-$130 for distances of 4.6 and 11.4~kpc. References are (1) this work, (2) \citet{abdo10}, and (3) \citet{HESS2018d}. Some of the parameters referred to this work were derived using parameters of Ref. 2 and/or 3.}
\label{table_disc}
\small
\centering
\setlength{\extrarowheight}{5pt}
\begin{tabular}{lccll}
\hline
 Parameter                                      & $D = 4.6$~kpc         & $D=11.4$~kpc          &                                                       & Ref.  \\\hline
 $\dot{E}$ [erg~s$^{-1}$]                       & \multicolumn{2}{c}{$3.60\times 10^{36}$}      & Pulsar's spin-down power                              & (2)   \\
 $\tau_c$ [yr]                                  & \multicolumn{2}{c}{$1.4\times10^4$}           & Pulsar's characteristic age                           & (2)   \\
 $\Gamma_{\mathrm{X}}^{\mathrm{PSR}}$           & \multicolumn{2}{c}{$1.42$}                    & Photon index of the pulsar in the keV band            & (1)   \\
 $L_{\mathrm{X}}^{\mathrm{PSR}}$ [erg s$^{-1}$] & $2.3 \times 10^{32}$  &  $1.7 \times 10^{33}$ & Pulsar luminosity in the 0.5-8.0~keV band             & (1)   \\\hline
 $\Gamma_{\mathrm{X}}$                          & \multicolumn{2}{c}{$1.79$}                    & Photon index of the PWN in the keV band               & (1)   \\
 $L_{\mathrm{X}}$ [erg s$^{-1}$]                & $3.4 \times 10^{33}$  &  $2.0 \times 10^{34}$ & PWN luminosity in the 0.5-8.0~keV band                & (1)   \\
 $\eta_{\mathrm{X}}$                            & $9.4 \times 10^{-4}$  &  $5.8 \times 10^{-3}$ & Pulsar's efficiency in the keV band                   & (1)   \\\hline
 $\Gamma_{\mathrm{TeV}}$                        & \multicolumn{2}{c}{$2.04$}                    & TeV spectral index                                              & (3)   \\
 $L_{\mathrm{TeV}}$ [erg s$^{-1}$]              & $1.0 \times 10^{34}$  &  $6.5 \times 10^{34}$ & Luminosity of HESS~J1826$-$130 in the 1-10 TeV band   & (3)   \\
 $\eta_{\mathrm{TeV}}$                          & $2.9 \times 10^{-3}$  &  $1.8 \times 10^{-2}$ & Pulsar's efficiency in the TeV band                   & (1,3) \\\hline
\end{tabular}
\end{table*}

\subsubsection{Origin of TeV emission}
\label{hess}
In a search for counterparts to HESS~J1826$-$130, the X-ray PWN driven by the PSR~J1826$-$1256 appears to be the most plausible candidate. In a leptonic scenario the TeV emission is expected to arise from inverse Compton (IC) scattering between the ambient low energetic photons and the same population of electron producing synchrotron radiation in the keV band. In our analysis of the spectral behaviour (see Sect.~\ref{X_spec}), we found that the photon index $\Gamma_\mathrm{X}$ of the extended X-ray PWN is $1.8 \pm 0.2$, close to the value $\Gamma_{\mathrm{TeV}}=2.0 \pm 0.1$ of the TeV spectrum of HESS~J1826$-$130 \citep{HESS18a}. This fact suggests a scenario in which the X-ray and TeV emissions arise from the same population of electrons \citep{pav08}. Based on our X-ray results and assuming that the softening of the spectrum with the distance from the pulsar is due to cooling effects, we estimated the magnetic field $B$ in the nebula from the relation $\tau_{\mathrm{sync}}\sim 38B_{\mu\rm{G}}^{-3/2} E^{-1/2}_{\mathrm{keV}}$~kyr, where $B_{\mu\rm{G}}$ is the magnetic field expressed in $\mu \rm{G}$ and $E_{\mathrm{keV}} = E_{\mathrm{sync}}/ (1~\rm{keV})$ being $E_{\mathrm{sync}}$ the energy of photons produced in the synchrotron radiation. As a consequence of the radiative cooling, the synchrotron cooling time $\tau_{\mathrm{sync}}$ should be smaller than the age of the PWN, which we roughly  approximated to the pulsar's characteristic age $\tau_c \sim 14$~kyr. The condition $\tau_{\mathrm{sync}} < \tau_\mathrm{c}$, gives $B > 2$ $\mu\rm{G}$ for $E_{\mathrm{sync}} = 1.5$~keV (the peak of the X-ray spectrum shown in Fig.~\ref{Figure4}a). The corresponding energy of the electrons is $E_\mathrm{e} \sim 160E_{\mathrm{keV}}^{1/2}B_{\mu\rm{G}}^{-1/2}$~TeV. For $E_{\mathrm{sync}}=1.5$~keV and $B > 2$~$\mu$G, we constrained the energy of the synchrotron emitting electrons to be $E_\mathrm{e} < 150$~TeV.

The population of relativistic electrons analysed in the paragraph above, with energy $E_\mathrm{e}$, can also interact with background photons of energy $\epsilon$ via IC scattering producing $\gamma$-ray photons in the TeV band, revealed as the VHE counterpart to the X-ray PWN. Hence, we estimated the energy of the TeV photons through the relation $E_{\mathrm{IC}} \sim 4 (E_\mathrm{e}/\rm{TeV})^2 \epsilon_{\mathrm{eV}}$~TeV, where $\epsilon_{\mathrm{eV}} = \epsilon / (1~\rm{eV})$. If the cosmic microwave background is the main source of background photons with $T \sim 3$~K, then $\epsilon \sim 3 \times 10^{-4}$~eV. Using $E_\mathrm{e} < 150$~TeV, we found that the energy of the photons produced by the IC scattering is $E_{\mathrm{IC}} < 30$~TeV. This analysis shows that the VHE counterpart to the X-ray nebula around PSR J1826$-$1256 is expected to radiate IC photons with energies up to a few tens of TeV. This result is largely compatible with the detection of $\gamma$ rays in the 0.5-40~TeV range from  HESS~J1826$-$130 \citep{anguner17}.

Another approach to analyse  the possible connection between PSR~J1826$-$1256, its PWN, and HESS~J1826$-$130, is to compare the high-energy properties of the system with those observed in others PWNe. To do this, we used the luminosities $L_{\mathrm{X}}$ and $L_{\mathrm{TeV}}$  to estimate the efficiency of pulsar's energy conversion in the keV and TeV bands as $\eta_{\mathrm{X}} = L_{\mathrm{X}} / \dot{E}$ and $\eta_{\mathrm{TeV}} = L_{\mathrm{TeV}} / \dot{E}$, where  $L_{\mathrm{X}}$ and $L_{\mathrm{TeV}}$ are the luminosities of the PWN in the 0.5-8.0 keV and 1-10 TeV energy bands, respectively.
From Table~\ref{tab_X1}, the flux of the PWN in the 0.5-8.0~keV band is $F_{X}\sim 13.4\times 10^{-13}$~erg~s$^{-1}$~cm$^{-2}$. This translates into a luminosity $L_{\mathrm{X}}\sim 1.60\times 10^{32} D_{\mathrm{kpc}}^{2}$~erg~s$^{-1}$, where $D_{\mathrm{kpc}}$ is the distance in kpc. Using the $\gamma$-ray flux reported by \citet{anguner17}, the luminosity in the 1-10 TeV band is $L_{\mathrm{TeV}}\sim 5.01\times 10^{32} D_{\mathrm{kpc}}^{2}$~erg~s$^{-1}$. From the obtained luminosities, together with the pulsar spin-down power $\dot{E}=3.60\times 10^{36}$ erg s$^{-1}$, we calculated the efficiency of pulsar's energy conversion $\eta_{\mathrm{keV}} \sim 4.5 \times 10^{-5} D_{\mathrm{kpc}}^{2}$ and $\eta_{\mathrm{TeV}} \sim 1.4\times 10 ^{-4} D_{\mathrm{kpc}}^{2}$ as a function of the distance.
In the case of PSR~J1826$-$1256 its distance is not well known. \citet{Wang11} suggested a distance to the pulsar of about 1.2~kpc, based on the correlation found between the efficiency in the GeV band and other pulsar parameters in a sample of $\gamma$-ray pulsars detected by {\it Fermi}-LAT. However, from a molecular study of a wide region containing the source HESS~J1826$-$ 130, \citet{voisin16} reported the presence of molecular gas in spatial coincidence with it at kinematical velocities between 60 and 80~km~s$^{-1}$ that correspond to intermediate near/far distances of about 4.6/11.4~kpc. Besides, the authors pointed out that a distance of 1.2~kpc to the pulsar implies a TeV $\gamma$-ray efficiency lower than the typical values. Thus, by adopting in our calculations the distances reported by \citet{voisin16} for the PSR-PWN-HESS source system, we compared their properties  with the population of Galactic PWNe and listed them in Table~\ref{table_disc}. Photon indexes $\Gamma$, in both keV and TeV bands, are in good agreement with those measured for other PWNe, and the obtained efficiencies $\eta_\mathrm{X}$ and $\eta_{\mathrm{TeV}}$ show that PSR~J1826$-$1256 has a spin-down energy sufficient to power the observed nebulae in X- and $\gamma$-rays \citep{kargal13, HESS2018d}.

\begin{figure}[h!]
\centering
\includegraphics[width=0.85\linewidth]{Figure5_low-res.eps}
\caption{Variation of the X-ray photon index $\Gamma_X$ (top) and the surface brightness {\SB} (bottom) with respect to the distance $r$ to box 1 (labelled in Fig.~\ref{Figure4}a). The {\SB} is expressed in units of $10^{-17}$~erg~s$^{-1}$~cm$^{-2}$~arcsec$^{-2}$.}
\label{Figure5}
\end{figure}

We also mention that a number of HII regions, OB stars, and high-mass star-forming regions are located in the vicinity of the TeV source at a distance of $\sim$4~kpc \citep{paron13}. These objects are able to accelerate particles to multi-TeV energy via hadronic interactions with dense material \citep[e.g,][]{araudo08,br10}. At the distance of 4~kpc, \citet{voisin16} reported the presence of molecular gas overlapping the TeV source, thus the contribution to the $\gamma$-ray emission via a hadronic process cannot be completely ruled out.

\section{Summary}
In this paper we presented the highest angular resolution and sensitivity radio continuum emission image from JVLA observatory at 1.4 GHz towards the pulsar PSR~J1826$-$1334. We sought to search for the radio counterpart to the PWN HESS~J825$-$137, which has been also detected in the X-ray band. The new radio data allowed us to detect an extended bright radio source with the pulsar located in its centre, in positional coincidence, and with a size similar to that of the compact component of the X-ray PWN. Although with the available radio data it is not possible to go deeper in the analysis of the origin of the observed emission, we suggest that it could be the radio counterpart of the PWN detected in the X- and $\gamma$-ray spectral regimes. Regarding the diffuse emission of the X-ray PWN, its radio counterpart was not detected in the 1-2~GHz band with an rms noise of 0.24~mJy~beam$^{-1}$.

We also reported the analysis of unpublished archival X-ray observations performed with {\XMM} towards PSR~J1826$-$1256. The new image revealed an elongated nebula, brighter around the pulsar with the emission in  the direction of the peak of the TeV source HESS~J1826$-$130. The spectral analysis demonstrated a non-thermal origin for the X-ray emission and a photon index $\Gamma$ softening with the distance to the pulsar. This study shows that the most plausible origin for HESS~J1826$-$130 is due to the IC mechanism within the PWN powered by PSR~J1826$-$1256.

\begin{acknowledgements}
The authors wish to thank the anonymous referee since his/her comments greatly improved our manuscript.
This work is based on observations done with the {\XMM}, an ESA science mission with instruments and contributions directly funded by ESA Member States and the US (NASA).
This research was partially funded by Argentina Grants awarded by ANPCYT (PICT 0571/11) and University of Buenos Aires (UBACYT 20020150100098BA).
G. C, E. G. and A. P. are Members of the Carrera del Investigador Cient{\'\i}fico of CONICET, Argentina. L. D. and L. S. are fellows of CONICET, Argentina.
\end{acknowledgements}

\bibliographystyle{aa}

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text:
Орден Круне је орден који је 5. априла 1930. основао краљ Александар I под називом Орден Југословенске круне у спомен на промену званичног назива Краљевине Срба, Хрвата и Словенаца у Краљевину Југославију. Орден који је додељиван у Краљевини Југославији а данас га додељује старешина краљевског дома Карађорђевића. Назив ордена је преложен још 1911. године. Ордену је 2002. године враћен првобитни назив који је први предложен.

Историја
Пред почетак Балканских ратова 1911. године, председник владе Никола Пашић сачинио је прелог закона о оснивању ордена. Тај пројекат је реализован тек деветнаест година касније. Краљ Александар I оснивач ордена, био је регент Краљевине Србије од 1914, регент Краљевине Срба, Хрвата и Словенаца од 1918, а на престо је ступио 1921. Током 1929. године политичке кризе и растући снажни сепаратистички покрети у земљи натерали су Краља да привремено суспендује Устав и подстакне национално јединство, што је најзад довело до промене назива земље.
Орден је организован у 5 степени, а био је додељиван грађанима који су предњачили у раду на остваривању националног јединства и сарадње, или за заслуге према Круни, држави и нацији у јавним службама, као и страним држављанима, претежно за дипломатске заслуге. Орден (Југословенске) круне био је старији од Ордена Светог Саве, а носио се о тамно плавој траци. Орден је додељивала Круна. Орденске инсигније су израђивали Артис Бертран у Паризу (Француска) и Браћа Игенен у Ле Локлу (Швајцарска).

Данас орден поново додељује старешина краљевског дома Карађорђевића.

Ликовну инспирацију по узору на Орден југословенске круне имају одликовања у Аргентини и Чилеу.

Изглед ордена

Одликовани од 1930. до 1945.
 Краљ Александар I Карађорђевић, Орден Југословенске круне 1. реда, 1930.
 Краљица Марија Карађорђевић, Орден Југословенске круне 1. реда, 1930.
 Краљ Петар II Карађорђевић, Орден Југословенске круне 1. реда, 1930.
 Принц Томислав Карађорђевић, Орден Југословенске круне 1. реда, 1930.
 Принц Андреј Карађорђевић, Орден Југословенске круне 1. реда, 1930.
 Кнез Арсен Карађорђевић, Орден Југословенске круне 1. реда, 1930.
 Кнез Павле Карађорђевић, Орден Југословенске круне 1. реда, 1930.
 Петар Бојовић, Орден Југословенске круне 1. реда, 1930.
 Емило Белић, Орден Југословенске круне 2. реда, 1930.
 Виктор Викерхаузер, Орден Југословенске круне 2. реда, 1930.
 Ђура Докић, Орден Југословенске круне 2. реда, 1930.
 Миливоје Зечевић, Орден Југословенске круне 2. реда, 1930.
 Данило Калафатовић, Орден Југословенске круне 2. реда, 1930.
 Милан Недић, Орден Југословенске круне 2. реда, 1930.
 Петар Пешић, Орден Југословенске круне 2. реда, 1930.
 Божидар Терзић, Орден Југословенске круне 2. реда, 1930.
 Милош Васић, Орден Југословенске круне 3. реда, 1930.
 Панта Драшкић, Орден Југословенске круне 3. реда, 1930.
 Владимир Кондић, Орден Југословенске круне 3. реда, 1930.
 Петар Косић, Орден Југословенске круне 3. реда, 1930.
 Љубомир Марић, Орден Југословенске круне 3. реда, 1930.
 Михаило Рашић, Орден Југословенске круне 3. реда, 1930.
 Душан Симовић, Орден Југословенске круне 3. реда, 1930.
 Душан Стефановић, Орден Југословенске круне 3. реда, 1930.
 Радисав Станојловић, Орден Југословенске круне 3. реда, 1930.
 Душан Трифуновић, Орден Југословенске круне 3. реда, 1930.
 Боривоје Мирковић, Орден Југословенске круне 4. реда, 1930.
 Леон Рупник, Орден Југословенске круне 4. реда, 1930.
 Никола Тесла, Орден Југословенске круне 1. реда 1931.
 Коча Поповић, Орден Југословенске круне 5. реда, 1931.
 Иван Мохорич, Орден Југословенске круне 1. реда, 1932.
 Ристо Ђурић, Орден Југословенске круне 5. реда, 1932.
 Ђорђе Стефановић, Орден Југословенске круне 5. реда, 1934.
 Јосиф Костић, Орден Југословенске круне 1. реда, 1936.
 Пантелија Јуришић, Орден Југословенске круне 1. реда, 1936.
 Војислав Томић, Орден Југословенске круне 1. реда, 1936.
 Богољуб Илић, Орден Југословенске круне 2. реда, 1936.
 Јеврем Дамјановић, Орден Југословенске круне 2. реда, 1936.
Иван Докић, Орден Југословенске круне 2. реда, 1936.
 Ратко Ракетић, Орден Југословенске круне 2. реда, 1936.
 Петар Арачић, Орден Југословенске круне 2. реда, 1937.
 Љубомир Велебит, Орден Југословенске круне 3. реда, 1937.
 Јован Дучић, Орден Југословенске круне 1. реда, 1937.
 Патријарх српски Гаврило, Орден Југословенске круне 1. реда, 1938.
 Блажо Врбица, Орден Југословенске круне 2. реда, 1938.
 Гојко Ђурић, Орден Југословенске круне 2. реда, 1938.
 Валтер фон Браухич, Орден Југословенске круне 1. реда 1939.
 Драгутин Протић, Орден Југословенске круне 1. реда, 1939.
Урош Тешановић, Орден Југословенске круне 3. реда, 1939.
 Виктор фон Херен, Орден Југословенске круне 1. реда 1939.
 Хајнрих Химлер, Орден Југословенске круне 1. реда 1939.
 Балдур фон Ширах, Орден Југословенске круне 1. реда 1939.
 Артур Флепс, Орден Југословенске круне 2. реда 1939.
 Иван Шубашић, Орден Југословенске круне 1. реда 1939.
 Слободан Јовановић, Орден Југословенске круне 1. реда, 1940.
 Драгиша Пандуровић, Орден Југословенске круне 2. реда, 1940.
 Жарко Рувидић, Орден Југословенске круне 2. реда, 1940.
 Арсо Јовановић, Орден Југословенске круне 5. реда 1940.
Коста Илић - Турчин, Орден Југословенске круне 4. реда, 1940.
 Роман Дембицки, Орден Југословенске круне 1. реда, 1942.
 Густав Пашкијевић, Орден Југословенске круне 3. реда, 1942.
 Краљица Александра Карађорђевић, Орден Југословенске круне 1. реда, 1944.
Престолонаследник Александар Карађорђевић, Орден Југословенске круне 1. реда, 1945.

Одликовани од 1945. до 2002.
 Бранко Терзић, Орден Југословенске круне 2. реда, 1976.
 Принц Петар Карађорђевић, Орден Југословенске круне 1. реда, 1980.
 Принц Филип Карађорђевић, Орден Југословенске круне 1. реда, 1982.
 Принц Александар Карађорђевић, Орден Југословенске круне 1. реда, 1982.

Одликовани од 2002.
 Никола Тасић, Орден Круне 1. реда, 2007.
 Миленко Зебић, Орден Круне 1. реда, 2009.
 Бора Драгашевић, Орден Круне 1. реда, 2012.
 Оливер Антић, Орден Круне 1. реда, 2013.
 Радош Бајић, Орден Круне 3. реда, 2015.
 Марко Бумбаширевић, Орден круне 1. реда 2017.
 Владимир Гајић, Орден круне 1. реда 2017.
 Љубодраг Грујић, Орден круне 1. реда 2017.
 Драгослав Мицић, Орден круне 1. реда 2017.
 Војислав Миловановић, Орден круне 1. реда 2017.
 Миладин Милошевић, Орден круне 1. реда 2017.
 Момчило Павловић, Орден круне 1. реда 2017.
 Мирко Петровић, Орден круне 1. реда 2017.
 Милорад Савићевић, Орден круне 1. реда 2017.
 Димитрије Стефановић, Орден круне 1. реда 2017.
 Зоран Трифуновић, Орден круне 1. реда 2017.

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The Dragon Ball universe has evolved into a familiar, well-loved world filled with vibrant, memorable characters over the years, thanks to series' creator Akira Toriyama — but sometimes traditions are meant to be broken. Dragon Ball Xenoverse — the newest addition to the Dragon Ball legacy — delivers a new-world setup and new gameplay design, incorporating familiar elements from the Dragon Ball universe with new, exciting possibilities and features. Explore an enigmatic city shrouded in mystery in Dragon Ball Xenoverse.
A clock that once had stopped will start to tick again in Dragon Ball Xenoverse, which is set in an all-new futuristic city. Engage in epic encounters between Goku and his fiercest foes, including Vegeta, Frieza and Cell. With improved gameplay, you'll be able to unleash destruction on opponents in the form of fast-paced, savage battles, as well as transforming in real-time. Who's that new fighter? Reveal the identity of an unheard-of figure that appears with a uniform, cape and scouter. Your favorite manga will never be the same again after being depicted on the PlayStation 4 console for the first time ever. Rebirth the hostility between Goku and his enemies in Dragon Ball Xenoverse.


Today on the blog, we're talking about lasers. While we at WEFPS love doing surgery, we also love less invasive ways of helping our patients look better. Previously we discussed intense pulsed light or IPL treatments as a way of reversing sun damage. While IPL is great at getting rid of brown spots and background redness, it really doesn't do well for fine lines and wrinkles. For those, we actually have a lot of solutions!
While IPL uses very bright white light to achieve its effects, lasers take one specific frequency of light to do a task. Laser resurfacing technology uses lasers to rejuvenate the more superficial layers of your skin. It comes in a lot of different flavors.
Older lasers would use a literal laser beam to zap off the outer layers of your skin. This is Star Wars kind of stuff. While the effects were awesome, there were some significant disadvantages- your entire face would get red and icky and would stay that way for weeks to months! Think about getting a really severe sunburn- it was kind of like that.
Stormtroopers can be cute, but don't let them resurface your face.
In the mid-2000's, laser resurfacing technology changed. Instead of a solid beam of light vaporizing the top layers of your skin, the beam started to get broken up or fractionated. So instead of one big beam, you would get treated with hundreds to thousands of little tiny beams. The advantage was that areas of intact skin were left behind which greatly accelerated healing times. Instead of being red and icky for months, you were only red for a week or two. The effects were still good, but the recovery was a lot easier. However, it still hurt A LOT. We would frequently combine laser resurfacing with a facelift because the patient was under anesthesia and rarely did it otherwise simply because it required anesthesia!
Here at WEFPS, we offer a fractionated laser resurfacing technology that is not ablative. What does that mean? There's no vaporizing. Your skin remains intact, so there's minimal redness and it goes away in a few hours. Our laser works by stimulating collagen production in the deeper layers of your skin. It can hurt, so we use topical numbing cream and the laser head is cooled which is nice.
Now, the effects aren't as dramatic as you would get with a laser that vaporizes the outer layers of your skin, so there is a trade off. We usually recommend three treatments spaced out about six weeks apart to get the best effect, but you will see an effect with just one treatment.
This gentleman had his eyes done and had full face laser resurfacing at the same time using our kinder, gentler laser. He had no significant redness after his treatment. And you can see a nice change.
For more on our laser-based treatments, check out this link!


As much as we'd love to write all of the words, sometimes it's not practical and sometimes it's not the most sustainable approach for our clients. That's why we offer a range of tone of voice and copywriting training courses to equip your team with solid writing skills. We can provide this training in the form of ongoing, online consultations or intensive, in-person sessions designed to educate groups of key stakeholders on how to maintain tone, voice and messaging for your brand.


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Thursday, May 14, 2020 | History
7 edition of The World of the Early Sienese Painter found in the catalog.
The World of the Early Sienese Painter
by Hayden B. J. Maginnis
Published November 2000 by Pennsylvania State University Press .
European history: c 500 to c 1500,
History of art: c 500 CE to c 1400,
Painting & paintings,
Social history,
c 1000 CE to c 1500,
Gothic Art,
History - Renaissance,
Arte dei pittori (Siena),
Historiography,
Contributions Gabriele Erasmi (Translator), Arte Dei Pittori (Corporate Author)
Sacro occipital technic
study of selectivity in the reactions of unsymmetrical trialkylboron compounds
Techniques in store location research
The International Handbook of Convertible Securities
Summary of charges for telecommunications services.
Proceedings of the 5th Meeting of the AcademicSociety for Large Animal Veterinary Medicine, held at the University of Glasgow Veterinary School, September 8-9, 1980.
Customs tariff of Virgin Islands, British West Indies
Orville Horwitz, trustee, &c.
Effectiveness measurement study
The 2000 Import and Export Market for Lubricating Petroleum Oils and Other Heavy Petroleum Oils in China (World Trade Report)
Disinfection by Sodium Hypochlorite
Memorial of the Republican members of the Legislature of Alabama, asking the enactment of stringent laws for the protection of all citizens of the United States.
Report of Hon. T. Butler King, on California.
Frommers New Orleans 2008 (Frommers Complete)
Charter no. 176; a short account of the origins and history of the First National Bank of Peoria, 1863-1963.
Get Going (GETG)
Principal Purchase Inspector
The sage senator delineated, or, A discourse of the qualifications, endowments, parts, external and internal, office, duty and dignity of a perfect politician
Insects and human welfare
The World of the Early Sienese Painter by Hayden B. J. Maginnis Download PDF EPUB FB2
The World of the Early Sienese Painter is the second volume of a trilogy Maginnis began with Painting in the Age of Giotto (). The third volume will turn from the broad social and cultural history of the present book to a history of early Sienese by: 5.
Get this from a library. The world of the early Sienese painter. [Hayden B J Maginnis; Gabriele Erasmi; Arte dei pittori (Siena).] -- "Siena of the thirteenth and fourteenth centuries was one of the great cities of Europe and its artists - Duccio, Simone Martini, and Ambrogio and Pietro Lorenzetti - were among those who reshaped.
Hayden B.J. Maginnis. The World of the Early Sienese Painter (With a Translation of the Sienese Breve dell'Arte dei Pittori by Gabriele Erasmi) University Park, Pennsylvania: Pennsylvania State University Press, xxiv + pp.
+ 16 color and b/w pls. $ ISBN: This volume is the second in a trilogy by Maginnis. The World of the Early Sienese Painter is the second volume of a trilogy Maginnis began with Painting in the Age of Giotto (). The third volume will turn from the broad social and cultural history of the present book to a history of early Sienese painting.5/5(2).
The World of the Early Sienese Painter is the second volume of a trilogy Maginnis began with Painting in the Age of Giotto (). The third volume will turn from the broad social and cultural history of the present book to a history of early Sienese : Find helpful customer reviews and review ratings for The World of the Early Sienese Painter at Read honest and unbiased product reviews from our users.5/5.
The World of the Early Sienese Painter is the second volume of a trilogy Maginnis began with Painting in the Age of Giotto (). The third volume will turn from the broad social and cultural history of the present book to a history of early Sienese painting.
mpcs.online - The World of the Early Sienese Painter book © 2020


The position of a prominent or well-known object in a particular landscape.
An event marking a unique or important historical change of course or one on which important developments depend. Synonyms: turning point, watershed.
A mark showing the boundary of a piece of land.
An anatomical structure used as a point of origin in locating other anatomical structures (as in surgery) or as point from which measurements can be taken.