Discovery's new global headquarters, located in Sandton Central, now holds the honour of being the first new build project to receive a 5-Star Green rating by the Green Building Council of South Africa. It is a project that's become a joint venture by two of the country's top property companies, Zenprop Property Holdings and Growthpoint Limited.
The beautiful new 112,000sqm building is a resource effective and cost efficient, eco-friendly endeavour. It is also the largest single phase commercial office development on the continent. From its inception, the design to construction and operation, the sustainable development has been a key priority to both the property companies and to Discovery.
Zenprop Property Holdings CEO, James Tannenberger is of the opinion that it's a significant milestone for Zenprop, specifically since their long history of delivering environmentally conscious and sustainable buildings across all sectors of the property market is so well known.
GBCSA Executive Director: Certifications, Manfred Braune, says it is the largest new building certified as Green Star to date in South Africa, which makes it an incredible achievement. It continues to be a testament to the advancement and innovation achievable in South Africa, as it leads the continent in sustainable and eco-friendly constructions.


text:
Lo Oracle Challenger Series - Newport Beach 2019 è stato un torneo di tennis giocato su campi in cemento all'aperto. È stata la seconda edizione del torneo, che fa parte del WTA Challenger Tour 2019 femminile e dell'ATP Challenger Tour maschile. Il torneo si è giocato a Newport Beach dal 21 al 27 gennaio 2019.

Partecipanti ATP Challenger

Teste di serie

* Ranking al 14 gennaio 2019.

Altri partecipanti
I seguenti giocatori hanno ricevuto una wild card per il tabellone principale:
  Ulises Blanch
  Taylor Fritz
  Marcos Giron
  Patrick Kypson
  Roy Smith

Il seguente giocatore è entrato nel tabellone principale come alternate:
  Collin Altamirano

I seguenti giocatori sono passati dalle qualificazioni:
  Maxime Cressy
  Evan Song

Il seguente giocatore è entrato nel tabellone principale come lucky loser:
  Alafia Ayeni

Partecipanti WTA

Teste di serie

* Ranking al 14 gennaio 2019.

Altre partecipanti
Le seguenti giocatrici hanno ricevuto una wild card per il tabellone principale:
  Hanna Chang
  Haley Giavara
  Elizabeth Halbauer
  Maegan Manasse

Le seguenti giocatrici sono passate dalle qualificazioni:
  Giuliana Olmos
  Katie Volynets

La seguente giocatrice è entrata in tabellone come alternate:
  Anna Danilina

Campioni

Singolare maschile

 Taylor Fritz ha sconfitto in finale  Brayden Schnur con il punteggio di 7–67, 6–4.

Singolare femminile

 Bianca Andreescu ha sconfitto in finale  Jessica Pegula con il punteggio di 0–6, 6–4, 6–2.

Doppio maschile

 Robert Galloway /  Nathaniel Lammons hanno sconfitto in finale  Romain Arneodo /  Andrei Vasilevski col punteggio di 7–5, 7–61.

Doppio femminile

 Hayley Carter /  Ena Shibahara hanno sconfitto in finale  Taylor Townsend /  Yanina Wickmayer col punteggio di 6–3, 7–61.

Collegamenti esterni

redpajama_set_name: RedPajamaWikipedia


Essential oils are volatile liquids that contain highly concentrated compounds from a specific plant variety. Although they are called oils, they are not oily to the touch. In fact, many of them are colorless while some assume a yellow or amber coloration. The color of an essential oil largely depends on the plant from which it is made from.
Essential oils are made by extracting liquids from a specific plant species. These oils can be extracted from different plant parts, such as seeds, flowers, stem, root, leaves, and the wood. More so, there are several different types of extraction methods while the most common one is steam distillation.
Essential oils can either be sold in its pure form (i.e. made from only one plant) or as a blend form (i.e. made from the aggregation of two or more plants species). Also, these blending usually have a specific formula depending on the target purpose of the oil.
Buying blended oil saves you the headache of having to look around for different oil types. Likewise, buying oils differently can be a little bit costly. Hence, buying blends can be more affordable and as well save you from unnecessary headaches.
There are different purposes by with which essential oils can be used. One of these purposes is growing of beard hair. Essential oils have been investigated to facilitate the growth of beard hair. Covered in this article are the major types of essential oils and the uses of the homemade beard growth oil.
As earlier stated, essential oils play an important role in the growth of beard hair. More still, beard hair needs a boost in order to keep it fresh and shinning. The best way to enhance your hair growth and keep it physically upright is through the use of essential oils. I recommend Growther Beard Growth Oil by Beard Farmer (click here to see current pricing).
There are several sources of essential oils but for the sake of this article, we will highlight only a few of them.
Olive oil is an excellent ingredient you can use to treat your hair. It adds a bit of nourishment to the hair and this, on the overall, makes the hair more attractive and well developed. Generally, olive oil has the essential ability to nourish and condition the hair which improves the structural strength and elasticity the hair.
You can decide to buy a blended pack of olive oil or decide to create a homemade formula yourself. To do this, you will need a half cup of olive oil, 5 drops of any favorite essential oil, and a plastic container for storing the formula over a long period of time. Simple mix the oils and allow it to cool overnight.
To use the formula, first, rinse your beard hair with warm water. If you have a slight scruff or no beard, clean your chin surface with warm water using a hand towel. Pour a small bit of oil on your palm and gently rub through your shin skin in a circular motion using your fingertips. Continue this process until the whole surface is touched.
If you have hair already, rub the ends of your hair as well. Protect your beard with a plastic bag and allow the oil to remain on your hair for at least, 30 minutes. This will make it soak properly. After this time duration, remove the covering and rinse the oil away with running water. For an extra touch, you can shampoo the hair and allow your beard to dry.
Castor oil is known for several different functions. For instance, it is known for quality medicinal use and excellent beauty product constituent. More so, castor oil is an effective substance used for treating various forms of acne and deep scars. And, more importantly, castor oil has a number of benefits for the hair. It nourishes the hair, keeps it shinning, and promotes the growth of new hair.
Castor oil contains ricinoleic acid that helps to protect the scalp and shin against hair loss. More so, this oil also contains Omega 9 fatty acids which keep the hair moist and prevent dandruff. Castor oil is popularly used due to its ability to produce thick and lustrous beard hair. Castor oil is highly beneficial to people with thin hair or hair loss problems.
Furthermore, castor oil is a humectant. This means that it can draw more moisture to the hair. Applying castor oil to the beard on a regular weekly basis can help to enhance a quality beard hair growth.
Almond oil is another source of essential oils for beard growth. Generally, almond oil has a lot of health and beauty benefits and has been used for many years to improve beard growth and strength. It is also a natural treatment for over processed and dry hair. Almond oil contains magnesium and vitamin E where both are great for improving hair luster and strength. Moreover, almond oil also helps to control hair loss by providing essential nourishment to the hair follicles.
Rosemary oil is known for its ability to stimulate hair growth and has been widely used over years for this same purpose. The oil is believed to induce a rapid cell division and dilate the blood vessels which help to stimulate the hair follicles for beard hair growth.
Lavender is a natural anti-inflammatory substance that helps to maintain a healthy beard skin surface. It also helps to improve blood circulation which stimulates rapid beard hair growth.
Hair follicles can become weaken when there is an insufficient supply of blood. However, Cedarwood oil helps to stimulate rapid blood circulation to the beard follicles Cedarwood oils also contains anti-fungal properties that prevent infections that can induce hair loss.
Other notable essential oils for inducing beard growth include the carrot root oil, peppermint oil, and coconut oil. Carrot oil is known for its ability to stimulate and regenerate hair follicles. Coconut beard oil is gotten from coconut fruit and is also useful for inducing beard growth. Likewise, you can also make use of the peppermint oil for beard growth.
Generally, you can blend all these oils together in order to achieve a more effective essential oil blend solution. There are several formulae for preparing hair growth recipe.
One of the best, safe, natural, and most effective ways of promoting healthy hair growth and prevent hair loss is through the use of essential oils. There are several essential oils for beard growth available on the market today. Some of them are available raw while some are sold in their blended form. In any case, we hope the above guide will help you in making a wise decision.


text:
package org.apache.geode.internal;

import static org.apache.geode.distributed.ConfigurationProperties.ENABLE_CLUSTER_CONFIGURATION;
import static org.apache.geode.distributed.ConfigurationProperties.LOCATORS;
import static org.apache.geode.distributed.ConfigurationProperties.MCAST_PORT;
import static org.apache.geode.distributed.ConfigurationProperties.START_LOCATOR;
import static org.junit.Assert.assertEquals;
import static org.junit.Assert.assertNotNull;

import java.io.File;
import java.io.IOException;
import java.nio.file.Files;
import java.util.Collection;
import java.util.List;
import java.util.Properties;
import java.util.concurrent.CopyOnWriteArrayList;

import org.junit.Test;
import org.junit.experimental.categories.Category;

import org.apache.geode.cache.Cache;
import org.apache.geode.cache.CacheFactory;
import org.apache.geode.cache.DiskStoreFactory;
import org.apache.geode.cache.Region;
import org.apache.geode.cache.RegionFactory;
import org.apache.geode.cache.RegionShortcut;
import org.apache.geode.internal.cache.DiskStoreImpl;
import org.apache.geode.pdx.PdxInstance;
import org.apache.geode.pdx.PdxReader;
import org.apache.geode.pdx.PdxSerializable;
import org.apache.geode.pdx.PdxWriter;
import org.apache.geode.pdx.internal.EnumInfo;
import org.apache.geode.pdx.internal.PdxInstanceImpl;
import org.apache.geode.pdx.internal.PdxType;
import org.apache.geode.test.dunit.Host;
import org.apache.geode.test.dunit.LogWriterUtils;
import org.apache.geode.test.dunit.SerializableCallable;
import org.apache.geode.test.dunit.VM;
import org.apache.geode.test.dunit.cache.internal.JUnit4CacheTestCase;
import org.apache.geode.test.junit.categories.SerializationTest;

@Category({SerializationTest.class})
public class PdxRenameDUnitTest extends JUnit4CacheTestCase {

  final List<String> filesToBeDeleted = new CopyOnWriteArrayList<String>();

  @Test
  public void testPdxRenameVersioning() throws Exception {
    final String DS_NAME = "PdxRenameDUnitTestDiskStore";
    final String DS_NAME2 = "PdxRenameDUnitTestDiskStore2";
    final int[] locatorPorts = AvailablePortHelper.getRandomAvailableTCPPorts(2);
    final File f = new File(DS_NAME);
    f.mkdir();
    final File f2 = new File(DS_NAME2);
    f2.mkdir();
    this.filesToBeDeleted.add(DS_NAME);
    this.filesToBeDeleted.add(DS_NAME2);

    final Properties props = new Properties();
    props.setProperty(MCAST_PORT, "0");
    props.setProperty(LOCATORS,
        "localhost[" + locatorPorts[0] + "],localhost[" + locatorPorts[1] + "]");
    props.setProperty(ENABLE_CLUSTER_CONFIGURATION, "false");

    Host host = Host.getHost(0);
    VM vm1 = host.getVM(0);
    VM vm2 = host.getVM(1);

    vm1.invoke(new SerializableCallable() {
      @Override
      public Object call() throws Exception {
        disconnectFromDS();
        props.setProperty(START_LOCATOR, "localhost[" + locatorPorts[0] + "]");
        final Cache cache =
            (new CacheFactory(props)).setPdxPersistent(true).setPdxDiskStore(DS_NAME).create();
        DiskStoreFactory dsf = cache.createDiskStoreFactory();
        dsf.setDiskDirs(new File[] {f});
        dsf.create(DS_NAME);
        RegionFactory<String, PdxValue> rf1 =
            cache.createRegionFactory(RegionShortcut.REPLICATE_PERSISTENT);
        rf1.setDiskStoreName(DS_NAME);
        Region<String, PdxValue> region1 = rf1.create("region1");
        region1.put("key1", new PdxValue(1));
        return null;
      }
    });

    vm2.invoke(new SerializableCallable() {
      @Override
      public Object call() throws Exception {
        disconnectFromDS();
        props.setProperty(START_LOCATOR, "localhost[" + locatorPorts[1] + "]");
        final Cache cache = (new CacheFactory(props)).setPdxReadSerialized(true)
            .setPdxPersistent(true).setPdxDiskStore(DS_NAME2).create();
        DiskStoreFactory dsf = cache.createDiskStoreFactory();
        dsf.setDiskDirs(new File[] {f2});
        dsf.create(DS_NAME2);
        RegionFactory rf1 = cache.createRegionFactory(RegionShortcut.REPLICATE_PERSISTENT);
        rf1.setDiskStoreName(DS_NAME2);
        Region region1 = rf1.create("region1");
        Object v = region1.get("key1");
        assertNotNull(v);
        cache.close();
        return null;
      }
    });

    vm1.invoke(new SerializableCallable() {
      @Override
      public Object call() throws Exception {
        Cache cache = CacheFactory.getAnyInstance();
        if (cache != null && !cache.isClosed()) {
          cache.close();
        }
        return null;
      }
    });

    vm1.invoke(new SerializableCallable() {
      @Override
      public Object call() throws Exception {
        Collection<Object> renameResults =
            DiskStoreImpl.pdxRename(DS_NAME, new File[] {f}, "apache", "pivotal");
        assertEquals(2, renameResults.size());

        for (Object o : renameResults) {
          if (o instanceof PdxType) {
            PdxType t = (PdxType) o;
            assertEquals("org.pivotal.geode.internal.PdxRenameDUnitTest$PdxValue",
                t.getClassName());
          } else {
            EnumInfo ei = (EnumInfo) o;
            assertEquals("org.pivotal.geode.internal.PdxRenameDUnitTest$Day", ei.getClassName());
          }
        }
        return null;
      }
    });

    vm1.invoke(new SerializableCallable() {
      @Override
      public Object call() throws Exception {
        props.setProperty(START_LOCATOR, "localhost[" + locatorPorts[0] + "]");
        final Cache cache =
            (new CacheFactory(props)).setPdxPersistent(true).setPdxDiskStore(DS_NAME).create();
        DiskStoreFactory dsf = cache.createDiskStoreFactory();
        dsf.setDiskDirs(new File[] {f});
        dsf.create(DS_NAME);
        RegionFactory<String, PdxValue> rf1 =
            cache.createRegionFactory(RegionShortcut.REPLICATE_PERSISTENT);
        rf1.setDiskStoreName(DS_NAME);
        Region<String, PdxValue> region1 = rf1.create("region1");
        return null;
      }
    });

    vm2.invoke(new SerializableCallable() {
      @Override
      public Object call() throws Exception {
        disconnectFromDS();
        props.setProperty(START_LOCATOR, "localhost[" + locatorPorts[1] + "]");
        final Cache cache = (new CacheFactory(props)).setPdxReadSerialized(true)
            .setPdxPersistent(true).setPdxDiskStore(DS_NAME2).create();

        DiskStoreFactory dsf = cache.createDiskStoreFactory();
        dsf.setDiskDirs(new File[] {f2});
        dsf.create(DS_NAME2);
        RegionFactory rf1 = cache.createRegionFactory(RegionShortcut.REPLICATE_PERSISTENT);
        rf1.setDiskStoreName(DS_NAME2);
        Region region1 = rf1.create("region1");
        PdxInstance v = (PdxInstance) region1.get("key1");
        assertNotNull(v);
        assertEquals("org.pivotal.geode.internal.PdxRenameDUnitTest$PdxValue",
            ((PdxInstanceImpl) v).getClassName());
        cache.close();
        return null;
      }
    });

    vm1.invoke(new SerializableCallable() {
      @Override
      public Object call() throws Exception {
        Cache cache = CacheFactory.getAnyInstance();
        if (cache != null && !cache.isClosed()) {
          cache.close();
        }
        return null;
      }
    });
  }

  @Override
  public void preTearDownCacheTestCase() throws Exception {
    for (String path : this.filesToBeDeleted) {
      try {
        Files.delete(new File(path).toPath());
      } catch (IOException e) {
        LogWriterUtils.getLogWriter().error("Unable to delete file", e);
      }
    }
    this.filesToBeDeleted.clear();
  }

  enum Day {
    Sunday, Monday, Tuesday, Wednesday, Thursday, Friday, Saturday;
  }

  class PdxValue implements PdxSerializable {
    private int value;
    public Day aDay;

    public PdxValue(int v) {
      this.value = v;
      aDay = Day.Sunday;
    }

    @Override
    public void toData(PdxWriter writer) {
      writer.writeInt("value", this.value);
      writer.writeObject("aDay", aDay);
    }

    @Override
    public void fromData(PdxReader reader) {
      this.value = reader.readInt("value");
      this.aDay = (Day) reader.readObject("aDay");
    }
  }
}

redpajama_set_name: RedPajamaGithub


Excellent mechanical design engineer and project manager with 10 years of solid experience and extensive knowledge in mechanical design of consumer electronics products and electronics devices. Major strengths include design product using 3D CAD software such as Pro/Engineer and Solid works, manage tooling development with local and overseas vendors and provide technical support for pilot run activity in local or worldwide facilities. Special abilities in prioritizing project schedule, managing multiple projects simultaneously and outstanding team building and interpersonal skills. A hardworking, target oriented person with leadership and bilingual communication skill in fluent English and Chinese.
lExpert user of Pro/Engineer, Solid works and AutoCAD for 10 years.
lProficient in designingplastic, sheet metal and casting parts and related molding technology.
lUnderstanding of EMI/EMC,thermal flow safety requirements for mechanical design.
lDFx, (Design for MFG, Cost, Assembly, Test, Logistics…etc).
lDFMEA, (Design Failure Mode Effects Analysis).
Patents acquired since 2002 as following.
project. Consistently complete project on time and on budget with highest team satisfaction.
lDesign to reduce cost or improve interchangeability of the product. Cost reduction exceeding $100K.
l100% improved the performance of touch screen with Acoustic Pulse Recognition (APR) touch technology by modifying the circuit trace and redefining the bonding methodology with plastic bezel.
lPlayed a key role in managing the entire tooling development process from vendor selection and RFQ review. Tooling cost saving 20% per project.
lSuccessfully established mechanical development SOP and mechanical design check list. Performed DFMEA review before tooling development result in about 30% reduction of tooling turnover rate.
l Developd fixture for production to reduce 30% of the manufacture time.
R&D team for HannsG brand projects development.
lBuilt engineering support team in China to handle tooling development process to reduce travelling frequency and save 60% the travelling expense in 2006.
lSuccessfully led and completed 6 HannsG brand projects from concept design to mass production in 3 months in tight budget from 2006~2007.100% hit the project goal.
lKept on implementing cost effective substitute material for existing products result in 10% BOM cost reduction for each project. 5million NTD ($150K) cost down per year.
Supervised 5 mechanical engineers and managed the day to day mechanical design activity.
Worked with key customers, Medion and Westing house as a team for mechanical design.
lTrained engineers in the use of Pro-Engineer resulting in a 50% saving of mechanical design hours.
lSuccessfully resolve "Buzz" issue by designing elastic member to improve the Yield Rate from 30% to 100%. This design awarded patent in 2005.
lCollaborated with process personnel to develop fixture to reduce 30% of the manufacturing time.
lSuccessfully established mechanical design guideline. Effectively improved the design lead time from 4 weeks to 3 weeks.
lSuccessfully led and completed 5 Hannspree brand projects from concept design to mass production in 3 months in tight budget from 2002~2003. No more than 3 months for each project.
lAwarded 5 patents for LCD monitor design from 2002 to 2004.
design with vendors, also modified designs based on vendor's feedback to reduce overall costs.
Generated drawings with detail dimensions and tolerances and maintained documentation.
lCompleted 5 projects for Sharp on time and on budget with the highest degrees of their satisfaction.
lEffectively saved shipping cost by designing the optimum product packing size to add 50% loading quantities for 1 container.
head. Generated drawings with detail dimensions and tolerances and maintained documentation.
lResearched thermal solution by testing different thermal pad and thermal glue and implementing for 100% improving the performance.
lResolved resonance issue in CD-ROM product by changing the thickness of enclosure and adding sponge inside the chassis to meet 100% of customer satisfaction.


text:
Soccer-A-League to kick off with Bolt question left hanging
Reuters Wed, 17 Oct 2018 Wed, 17 Oct 2018
FILE PHOTO: Soccer Football - Central Coast Mariners v Central Coast Select - Central Coast Stadium, Gosford, Australia - August 31, 2018 Central Coast Mariners' Usain Bolt applauds the fans after the match REUTERS
MELBOURNE : Usain Bolt's mission to win a professional football contract in Australia has dominated the A-League's pre-season and could prove an intriguing sideshow throughout a championship that has lacked superstar glamour in recent years.
Bolt, trying to make his mark at Central Coast Mariners, netted twice in a trial match last week, generating headlines around the world but failing to remove doubts about the eight-time Olympic gold medallist's chances of making the grade.
However, Bolt's mere presence at Central Coast has given the sleepy region north of Sydney its time in the limelight, drawing thousands to warm-up games that would normally struggle to lure a few hundred spectators.
Football Federation Australia (FFA) has said it would not raid a special fund set up to lure marquee players to the league if the Mariners decide 32-year-old Bolt is worth the risk.
But it would likely move heaven and earth to keep the Jamaican Down Under, for his marketing value if not his footballing quality.
Adding another element of intrigue, Maltese champions Valletta FC have declared their interest in signing Bolt, dangling a two-year deal in front of him.
What is certain is that Bolt will not be turning out for the Mariners when they open their season at Brisbane Roar on Sunday, and most probably not until the New Year at the earliest.
The league's next registration period does not open until Jan. 3, which could leave him a mere cheerleader for the first half of a season tipped to be one of the most open in years.
With Bolt cooling his heels, former Japan midfielder Keisuke Honda will feel the burden of expectation as the league's highest profile recruit in its most dominant team, Melbourne Victory.
Honda is arguably the league's biggest signing since Sydney FC lured Italy great Alessandro del Pierro for a couple of seasons in 2012, and he could prove key to the Kevin Muscat-coached Victory's hopes of extending the champions' record to five titles.
Sydney FC and Newcastle Jets, beaten in the championship decider by Victory last season, are also expected to figure prominently in the post-season but Perth Glory may be set to make the biggest move up the table.
Glory finished eighth in the 10-team league last year but the recruitment of manager Tony Popovic, who guided the Western Sydney Wanderers to the Asian Champions League title in 2014, has helped trigger an influx of quality signings.
They now boast three former Australia internationals in a defence that leaked far too many goals last season.
The A-League will also kick off without a governance war raging in the background for the first time in years after FFA's Congress voted in a reform package earlier this month to end a long-running dispute.
The political wrangling delayed the selection of new expansion sides but FFA CEO David Gallop said on Wednesday the league still planned for new teams to join the A-League in the 2019/20 season.

redpajama_set_name: RedPajamaCommonCrawl


Panaji: April 27,2018 … Minister for Art and Culture Shri Govind Gaude recently graced the prize distribution ceremony of Marathi Drama 'A' and 'B' Group competition, Konkani Drama Competition and One Act Play competition (High School and Higher Secondary/College Level organized by Kala Acdemy at Dinanath Mangeshkar Kala Mandir, Kala Academy Complex Panaji .
Shri Raju Nayak, Editor of Lokmat was the Guest of Honour for the ceremony.
Shri Gaude addressing the gathering congratulated the winners and lauded the efforts of the awardees for their hard work in showcasing their talent and making the competition such a success. Criticism play a very important role in an individual's life and one has to accept it as a challenge to achieve the goal he added.
Shri.Gurudas Pilarnekar, Director, Directorate of Art and Culture welcome the gathering Shri Pradeep Gaonkar compered the function while Shri Dattaguru Amonkar proposed the vote of thanks.


text:
Opposition grows ahead of 'cheese wedges' planning decision
PUBLISHED: 06:00 19 October 2019
Katy Sandalls
Opposition to the cheese wedges has been growing ahead of the planning meeting Picture: CLAIRE PADFIELD
Opponents to a controversial new housing project have been stepping up their campaign against the site ahead of an important council decision next week.
Mrs Padfield said it was important to make people aware of the planning meeting Picture: CLAIRE PADFIELD
New posters have gone up in Woodbridge in protest ahead of a meeting about the future of the former Suffolk Coastal District Council offices on Melton Hill.
An application for 100 new homes - known locally as the cheese wedges but officially as King's View - is set to go before East Suffolk District Council next week.
MORE: Cheese wedge homes could FINALLY get the go-ahead
Planning officers have recommended that councillors approve the application made by developers Active Urban Woodbridge Limited.
New posters opposing the cheese wedges have been put up in Woodbridge Picture: CLAIRE PADFIELD
Claire Padfield, who lives close to the site, has put up a number of posters outside her property to remind people of next week's meeting.
"The reason I had the posters up is to warn local people. Unless you are following the planning application you don't know," said Mrs Padfield.
"It's a communication to those members of the community who care and will have been bothered to file letters of objection three times."
Alan Vaughan, chair of the Woodbridge Society Picture: ANDREW PARTRIDGE
She added: "My objection is that this is totally wrong for the site; it's out of character and overdeveloped."
Alan Vaughan, chairman of the Woodbridge society has also raised further concerns about the proposal, including how it fits with the latest government advice on housing.
"Their argument seems to be that they like the design and the complete absence of local support should be ignored.
"Since the earlier applications, the National Planning Policy Framework has been changed. As the Council's Conservation Officer acknowledges, it gives more weight to developments fitting in with their surroundings. The proposed Cheese Wedges do not and will harm their neighbours.
"This is a new planning committee for a new council.
"They must take this opportunity to end this sorry saga so that a new proposal which command popular support can be put forward."
Active Urban Woodbridge Limited were contacted for comment.
East Suffolk Council's planning committee will meet to discuss the application on Tuesday.
'It was cheaper to smash a window' – Town striker Norwood has to break into own car to make training
Welterweight title on the line at stacked Contenders 29


This is a presentation that I gave to a great group of folks at Thomson Reuters who graciously invited me to Keynote at their internal DevOps event. Thomson Reuters is making great strides in adopting DevOps so I wanted to provide them with some bullet points that they can use to help build a solid foundation.
Tom Duffield Tom Duffield is a software engineer for Chef Software based out of Austin, TX.


text:
Getting Curiosity on Mars
Why inoperative plane sensors can leave pilots helpless.
The perfect reptile-bird hybrid definitely looks the part
Archeopteryx had strong feathers, bony jaws and teeth, and a tail with a line of bone running down its legs. Physically, it was exactly half-reptile, half-bird. (2:11)
The P-38 almost single-handedly drove back the Germans as they attempted to keep their North Africa armies supplied. In just one month, the Allies shot down over 400 German planes, while losing only 36.
Germany suffered big losses at the hands of the P-38 (3:24)
Henry Ford spent the majority of the war as a pacifist. By 1917, however, his state-of-the-art assembly line was churning out vital engine parts to feed the war machine.
How Henry Ford went from pacifist to major supplier of World War I (2:56)
On May 18, 1980, Mount St. Helens became the largest and most destructive volcanic eruption in U.S. history. By the end of its cycle of fire and fury, 57 people had died.
Footage of the 1980 Mount St. Helens eruption (3:47)
By 1953, six years after the Bell X-1 first went supersonic, that airplane and others were routinely flying at more than twice the speed of sound. On December 17, 1953the 50th anniversary of the Wright brothers first powered flight at Kitty HawkMajor Yeager sat down at the Pentagon for an informal press briefing to discuss his own Mach 2.43 flight in the X-1 five days earlier. Video: Department of Defense, Courtesy National Archives and Records Administration
Chuck Yeager Press Conference, 1953 (2:41)
This ordinary small town holds extraordinary significance for aviation: its home to Elvis private jet, an airplane demolition yard, and the most famous aircraft that no ones ever seen.
Roswell's Bizarre Aircraft Boneyard (2:17)
Just one minute away from landing, both of this planes engines suddenly fail.
How to Land a Boeing 777 Without Any Engines (3:58)
This rare footage shot during the Vietnam War shows the Douglas A-26 Invader operating at England Air Force Base in Louisiana and at Nakhon Phanom RTAFB in Thailand. The final scenes at the Vintage Flying Museum at Meacham Field in Fort Worth, Texas, show the last airworthy A-26A, "Special K," now owned and being restored by the Pacific Prowler organization chaired by Jim Terry. Video: Nolan Schmidt/Franklin Poole/Pacific Prowler Organization
Truck Killer:The A-26A (4:34)


text:
WWW . GODDARD . GRAPHICS
Sussex Scenes
Normandy, France
Bosham
(Click on the image for a large view)
A small attractive village on one of the small inlets of Chichester harbour, Bosham (pronounced 'Bozzum') has played an important part in the history of this country over the centuries.
Inhabited by the Romans, Bosham was the sixth most important town in Sussex in the 8th century. Legend has it that the Danish King Canute sat on a chair surrounded by his courtiers and commanded the waves to go back – they did not, an exercise which showed that even the great Canute was mortal; he got his feet wet! King Canute's eight year old daughter was drowned in the Brook Stream and is buried in Bosham Church in a Saxon coffin at the foot of the chancel steps.
It was from Bosham that Harold II set forth in 1064 to negotiate with William of Normandy, a voyage that led to William the Conqueror's return in 1066; Bosham features in the Bayeaux Tapestry.
Today Bosham is both picturesque and a thriving centre for sailing. Chichester harbour is a sanctuary for migrating wildfowl, shellduck, wigeon, Brent geese, waders and many more, and offers great walks along the sea shore.
A favourite haunt for artists and photographers, this picturesque village offers something to suit all tastes; those with a sense of history, artists, photographers, walkers, cyclists, sailors and weekenders all love the place.
BUY A CARD
English French Italian


Southern California City Mourns in Wake of Borderline Bar Massacre - Jago Times "English Edition"
Hundreds of people gathered Thursday evening to remember the dozen people shot and killed by a Marine veteran at the packed Borderline Bar & Grill the night before. It was a scene of horror enacted in many places around the country in recent months, but never before in Thousand Oaks.
Terrified patrons who had gathered for the weekly Wednesday night line dancing and college night hurled barstools through windows to escape or threw their bodies protectively on top of friends as shots erupted. Twelve people were killed including Ventura County sheriff's Sgt. Ron Helus, a 29-year veteran nearing retirement who responded to reports of shots fired and was gunned down as he entered the bar.
The community, already reeling from the mass shooting, is also facing the devastation of wildfires that broke out later Thursday and destroyed homes. Tens of thousands of homes remain threatened by the Woolsey and Hill fires.
Those killed in the shooting included a man who had survived last year's massacre in Las Vegas, Telemachus Orfanos, 22.


text:
\section{Introduction} \label{sec:intro}

The Galactic black hole candidate MAXI J1820$+$020/\\ASASSN-18ey,
discovered in optical by the All-Sky Automated Survey for
SuperNovae (ASSAS-SN) project \citep{sha14}
on 2018 March 6 \citep{tuc18} and in X-rays with
{\maxi} \citep{mat09} on 2018 March 11 \citep{kaw18a},
has been an ideal target to probe black hole accretion
flows and jets over a wide range of mass accretion rates.
Thanks to its relatively small distance ($3 \pm 1$ kpc, \citealt{gan18b})
and low Galactic extinction ($N_\mathrm{H} = 1.5 \times 10^{21}$ cm$^{-2}$,
\citealt{utt18}), the source
has been intensively observed at various wavelengths, with
different methods (photometry, spectroscopy, and polarimetry),
and on various time resolutions, from ms to $\gtrsim$day
\citep[][and many other reports in the Astronomer's
Telegram]{ken18a,ken18b,ken18c,bag18a,bri18a,lit18,vel18,
utt18,bah18,gar18,sak18,del18,pai18,gan18a,tru18}.

\begin{figure*}[th!]
\plotone{./fig1_new3.eps}
\caption{\maxi/GSC light curves of MAXI J1820$+$070 in 2--6 keV,
6--20 keV, their hardness ratio, and \swift/BAT light curve
in 15--50 keV downloaded from the ``BAT Transient Monitor''
website \citep[][\url{http://swift.gsfc.nasa.gov/docs/swift/results/transients}]{kri13},
from top to bottom. The grey and red points show
the data with orbital time bins ($\sim$92 min) and
the binned data, respectively. The error bars indicate
1$\sigma$ statistical errors. The periods
"LH", "IM", "HS" represent the low/hard, intermediate,
and high/soft state periods, respectively. The spectra
in the bin (a)--(i) indicated with stars
and thin vertical lines are plotted in Fig.~\ref{fig:MAXIBATspec}.
\label{fig:LC_longterm}}
\end{figure*}

Since its discovery, the source stayed in the low/hard state
for more than 3 months, and then exhibited a rapid X-ray spectral
softening in 2018 July \citep{hom18a}. This indicates that
the source made the state transition from the so-called
low/hard state, in which a strong hard X-ray component is
observed in the X-ray spectrum, to the high/soft
state, where the soft X-ray emission from the
standard accretion disk \citep{sha73} dominates the
X-ray flux. The source exhibited strong radio
flares at the beginning of the transition \citep{bri18b}.
During the transition, the radio to infrared flux decreased,
suggesting quenching of the jet \citep{tet18,cas18}.
By contrast, the optical flux behaved in an opposite
way \citep{tuc18}.
In September, an X-ray spectral hardening was observed,
indicating that the source returned to the low/hard
state \citep{neg18,mot18,hom18b}.

In \citet{shi18} (hereafter S18), we studied the
X-ray properties of {MAXI J1820$+$070 } using
the {\maxi} and {\swift} \citep{geh04} data obtained
during the low/hard state before the state transition in July.
The X-ray spectrum in this period was well explained by
Comptonization of soft X-ray photons from the standard
disk, in the hot ($\gtrsim$ several ten keV), radiatively inefficient
inner flow or the corona above the disk. We also analyzed a
simultaneous multi-wavelength spectral energy distribution taken in late
March and found that the synchrotron emission from the jet
was likely to contribute to the optical and
near-infrared wavelengths, whereas in the X-ray band,
its contribution, as well as the contributions of
synchrotron self-Comptonization and external
Comptonization, were likely to be negligible.

In this article, we investigate the
long-term X-ray spectral evolution over the entire
outburst from March to October, using the \maxi/Gas
Slit Camera (GSC)
and \swift/Burst Alert Telescope (BAT) data.
We also combine the optical photometric data
acquired with the MITSuME 50 cm telescope
in Akeno Observatory, to study long-term optical
flux evolution and correlation with the X-ray flux.
We adopt the solar abundance table
given by \citet{wil00} for the spectral analysis
described below. Errors represent the 90\% confidence
ranges for one parameter, unless otherwise stated.

\if0
\begin{figure}[th!]
\plotone{./MAXIJ1820_LC_trans.eps}
\caption{Same as Fig.~\ref{fig:LC_longterm}, around the soft X-ray
flux peak on MJD$\sim$58306. \label{fig:LC_trans}}\end{figure}
\fi

\begin{figure}[th!]
\plotone{./fig2_2.eps}
\caption{Hardness intensity diagram of MAXI J1820$+$070,
created from the MAXI data in Fig.~\ref{fig:LC_longterm}.
The error bars indicate 1$\sigma$ statistical errors. \label{fig:HID}}\end{figure}

\section{X-ray Data Reduction and Analysis}
\label{sec:ana}
We reduced the $\maxi$/GSC event data
and $\swift$/BAT survey data from 2018 March
to October, utilizing the $\maxi$ analysis
tools \citep{nak13} and the HEAsoft version 6.23,
and produced the light curves and spectra of
MAXI J1820$+$070. We adopted the same
procedures of the data reduction
as those in S18.

\subsection{Light Curves and Hardness Ratio}
\label{sec:lc}
Figure~\ref{fig:LC_longterm} shows the \maxi/GSC
2--6 keV and 6--20 keV light curves of MAXI J1820$+$020,
and the {\swift}/BAT light curve in 15--50 keV
during the 2018 outburst,
with a time bin size of their orbital periods
($\sim$92 minutes; grey points). The hardness
ratio (HR) calculated from these two {\maxi}
light curves is also plotted.
Using the MAXI data in Fig.~\ref{fig:LC_longterm},
we have also plotted the hardness intensity
diagram (HID) of MAXI J1820$+$070 in Figure~\ref{fig:HID}.
To improve statistics, we combined the GSC data
taken in each 1--85 adjacent orbits with similar
fluxes into one bin (red points in Fig.~\ref{fig:LC_longterm}).

\begin{figure*}[ht!]
\epsscale{1.2}
\plotone{./fig3_new2.eps}
\caption{Unfolded \maxi/GSC (cross) and \swift/BAT (open square)
spectra, obtained at the epochs (a)--(i) indicated
in Fig.~\ref{fig:LC_longterm} and Fig.~\ref{fig:HID}, with their best-fit models (top),
and the data versus model ratios (bottom).
The unscattered and scattered components are plotted in pink
dashed and blue dotted lines, respectively, for the high/soft state and
and intermediate state spectra.
\label{fig:MAXIBATspec}}
\end{figure*}

The source showed a rapid flux rise and
then a slower decay in all energy bands,
in the first $\sim$3 months after the
discovery on 2018 March 11. In this period,
the HR was kept almost constant. A re-brightening
in the 15--50 keV band was detected with the \swift/BAT
in the middle of June (MJD $\sim$58290), whereas
the soft X-ray data could not be obtained with
the {\maxi} from the beginning to the end of June,
because the source was out
of its field of view. In early July,
{\maxi} detected a rapid increase of the soft X-ray flux
in 2--6 keV, to the peak level of $\sim$10 photons s$^{-1}$
cm$^{-2}$, corresponding to $\sim$4 Crab. Meanwhile,
the hard X-ray flux above 6 keV decreased rapidly
a few days before the soft X-ray peak, and the HR
thereby dropped.

Since the second flux peak, the soft X-ray flux below
6 keV has been decreasing gradually, whereas the
harder X-ray flux increased again from late September
to the beginning of October (MJD 58380--58393).
Consequently, the HR increased again to the initial
level before the re-brightening in June to July.
The overall evolution of the fluxes and HR
provided a counter-clockwise track in the HID,
like typical Galactic transient
black hole binaries in their outburst.

Considering the behavior of the HR,
we classified the whole outburst period into
the canonical three spectral states of black hole X-ray binaries
\citep[e.g.,][for details]{don07}:
the low/hard state, the high/soft state, and the intermediate
state (which is the transitional state between the former two states).
\begin{description}
\item[low/hard state] {until MJD 58303.5 and from MJD 58393.0}, in which the HR was at the highest level, $\gtrsim$0.4. \item[intermediate state] {MJD 58303.5--58310.7 and MJD 58380.0--58393.0}, in which the HR was rapidly decreasing/increasing between 0.04--0.4.
\item[high/soft state] {MJD 58310.7--58380.0}, in which the HR was lower than $\sim 0.04$.
    \end{description}
This classification is confirmed to be valid
in the following sections, on the basis of the X-ray
spectral profile.

\begin{deluxetable*}{cccCCCCCCC}[ht!]
\tablecaption{Best-fit
parameters for the representative spectra \label{tab:fit}}
\tablecolumns{10}
\tablenum{2}
\tablewidth{0pt}
\tablehead{
\colhead{ID\tablenotemark{a}} & \colhead{state} &
\colhead{model\tablenotemark{b}\tablenotemark{c}} & \colhead{$\Gamma$} & \colhead{$kT_\mathrm{e}$} & \colhead{$F_\mathrm{scat}$} &
\colhead{$kT_\mathrm{in}$} & \colhead{$r_\mathrm{in}$\tablenotemark{d}}
& \colhead{$\chi^2/\mathrm{dof}$} & \colhead{$F_X$\tablenotemark{e}} \\
\colhead{} &
\colhead{} &
\colhead{} &
\colhead{} &
\colhead{keV} &
\colhead{} &
\colhead{keV} &
\colhead{km} &
\colhead{} &
\colhead{$10^{-8}$ erg s$^{-1}$ cm$^{-2}$}
}
\startdata
(a) &
low/hard & {\tt nthcomp} & 1.55 \pm 0.08 & >42 & -
& 0.1~\mathrm{(fixed)} & - & 29/28 & 1.6^{+0.4}_{-0.3} \\
(b) &
low/hard & {\tt nthcomp} & 1.72 \pm 0.05 & 41^{+11}_{-7} & -
& 0.1~\mathrm{(fixed)} & - & 27/27 & 14 \pm 1 \\
(c) &
low/hard & {\tt nthcomp} & 1.74^{+0.08}_{-0.07} & 61^{+139}_{-22} & -
& 0.1~\mathrm{(fixed)} & - & 80/72 & 5.0^{+0.6}_{-0.5} \\
(d) &
intermediate & {\tt simpl*diskbb} & 2.20 \pm 0.08  & - & 0.4^{+0.1}_{-0.2}
& 0.5 \pm 0.2 & 81^{+190}_{-40} & 18/23 & 7.5^{+1.1}_{-0.7} \\
(e) &
intermediate & {\tt simpl*diskbb} &  2.4 \pm 0.2 & - & 0.10^{+0.03}_{-0.02}
& 0.67^{+0.06}_{-0.05} & 67^{+17}_{-12} & 75/80 & 10.0^{+0.7}_{-0.8} \\
 (f) &
high/soft & {\tt simpl*diskbb} &  2.5~\mathrm{(fixed)} & - & 0.022 \pm 0.004
& 0.70 \pm 0.01 & 61 \pm 2  & 118/115 & 8.5 \pm 0.2 \\
 (g) &
high/soft & {\tt simpl*diskbb} &  2.5~\mathrm{(fixed)} & - & 0.01 \pm 0.05
& 0.64 \pm 0.02 & 66 \pm 5  & 99/89 & 5.9 \pm 0.2 \\
 (h) &
 intermediate & {\tt simpl*diskbb} &  2.1 \pm 0.2 & - & 0.12 \pm 0.04
& 0.45 \pm 0.08 & 73^{+61}_{-27} & 88/80 & 2.5^{+0.4}_{-0.3}\\
 (i) &
 low/hard & {\tt nthcomp} & 1.83 \pm 0.08 & >84 & -
& 0.1~\mathrm{(fixed)} & - & 69/77 & 1.1 \pm 0.1 \\
\enddata
\tablenotetext{a}{Data IDs in Fig~\ref{fig:MAXIBATspec}.}
\tablenotetext{b}{The {\tt TBabs} model was combined for all models, with $N_\mathrm{H}$ of $1.5 \times 10^{21}$, to account for the interstellar absorption.}
\tablenotetext{c}{The seed spectrum for the Comptonization component was assumed to be a disk blackbody.}
\tablenotetext{d}{Inner radius estimated from the total photons of the disk blackbody emission, including the Comptonized photons. A distance and
an inclination angle of 3 kpc and 60$^\circ$ are assumed, respectively.
The color-temperature correction and the correction of the inner boundary
condition are not considered here.}
\tablenotetext{e}{Unabsorbed 1--100 keV flux.}
\end{deluxetable*}

\subsection{Spectral Analysis}
\label{sec:spec}

We studied X-ray spectral evolution of {MAXI J1820$+$070 }
using the \maxi/GSC and \swift/BAT survey data.
We produced {\maxi} spectra in the individual
bins presented in Fig.~\ref{fig:LC_longterm} as
red points. Following S18, we then matched them
with the BAT survey spectra of the individual
continuous scans. We thus obtained 93
simultaneous \maxi/GSC and \swift/BAT spectra
covering from 2 keV to $\sim$200 keV over the
whole outburst. We presented
9 representative spectra in Figure~\ref{fig:MAXIBATspec}.

The simultaneous \maxi/GSC and \swift/BAT spectra were
systematically analyzed on XSPEC version 12.10.0.
We varied the cross-normalization factor of the BAT data
with respect to the GSC data, to take into account
an uncertainty in the instrumental
cross-calibration and that caused by flux variation due
to the slight differences of the observation periods
between the \maxi/GSC and \swift/BAT.
We adopted a canonical spectral
model for black hole binaries in outbursts:
disk blackbody emission and its thermal or non-thermal
Comptonization component.
The {\tt TBabs} model \citep{wil00} was also employed
to account for the interstellar absorption. We
fixed the equivalent hydrogen column density
$N_\mathrm{H}$ at $1.5 \times 10^{21}$ cm$^{-2}$,
which was determined from the data of
{\it the Neutron star
Interior Composition Explorer} ({\it NICER}, \citealt{utt18}).

As investigated in S18, before the spectral
softening, the source showed a typical spectral profile
of black bole binaries in the low/hard state: a hard
power-law shaped spectrum with a photon index of
$<2$, often accompanying an exponential cutoff (see
Fig.~\ref{fig:MAXIBATspec}a--c). A similar spectrum
was observed after the spectral hardening around
MJD 58380--58390 (see Fig.~\ref{fig:MAXIBATspec}i).
We applied the same model as S18,
{\tt TBabs*nthcomp} to the spectra in
these periods.
The {\tt nthcomp} model calculates thermal
Comptonization spectrum using a photon index
and an electron temperature \citep{zyc99}.
Following S18, the seed spectrum
was assumed to be a disk blackbody, with
a fixed inner temperature of 0.1 keV, as
it cannot be determined with the MAXI$+$BAT data
covering only above 3 keV.
The results do not depend on this value,
as all the parameters we obtain
remain within their 90\% error ranges,
even when $T_\mathrm{in} =  0.5$ keV and
0.05 keV are adopted. We ignored
the direct disk blackbody component in $P_\mathrm{H}$.

In the high/soft state, the spectrum of {MAXI J1820$+$070 } was dominated by the
soft X-rays (see Fig.\ref{fig:MAXIBATspec}f and g)
likely originating in the thermal emission
from the standard accretion disk \citep{sha73}. We used {\tt diskbb}
\citep{mit84} to model this component.
A weak power-law tail was also often observed
above $\sim$10 keV, without a significant cutoff.
To account for this component, we employed {\tt simpl}
\citep{ste09},
assuming the non-thermal Comptonization of the disk
emission as the origin of the hard tail. Thus, the
model applied for the high/soft state periods
was expressed as {\tt TBabs*simpl*diskbb}.
The {\tt simpl} model makes a fraction of an input seed
spectrum scatter into a power-law component, using a
scattered fraction $F_\mathrm{scat}$ and a photon index
$\Gamma$ as the free parameters. We fixed $\Gamma$ at 2.5,
a typical value for the high/soft state \citep[e.g.,][]{ebi94,mcc06},
because we were unable to constrain it, due to the low statistics
of the \swift/BAT data. We extended the energy range
over which the model spectrum is calculated on XSPEC,
from those in the \maxi/GSC and \swift/BAT response
matrix files to 0.1--500 keV, for accurate calculation
of the convolution model {\tt simpl}.

The spectrum changed drastically during the intermediate states,
as shown in Fig.~\ref{fig:MAXIBATspec}(c)--(e) and (h).
We applied the same model as that used for the
spectrum in the high/soft state.
{\tt TBabs*simpl*diskbb}, varying the photon index.
We note that the {\tt simpl} model does
not consider the radial dependence of the
scattering fraction.
This means that it assumes a specific geometry
(a disk-like geometry) for the Comptonized region,
and its parameters may become unreliable when a
different geometry is considered, such as a spherical
electron cloud inside a highly truncated standard disk.
We have also tested the disk and its thermal Comptonization model,
{\tt TBabs*(diskbb+nthcomp)}, linking the inner disk
temperatures of {\tt diskbb} and {\tt nthcomp},
and have obtained equally good fit with parameter
values similar to {\tt TBabs*simpl*diskbb}. The spectral
cutoff was not detected significantly and only a lower limit
of the electron temperature was obtained ($kT\mathrm{e} \gtrsim$ 50 keV).

These models successfully described the wide-band
{\maxi}/GSC and {\swift}/BAT X-ray spectra in the
individual states. The best-fit models
for the 9 representative spectra and their
parameters are presented in Figure~\ref{fig:MAXIBATspec}
and Table~\ref{tab:fit},respectively.
Figure~\ref{fig:trend_fitpars} shows the trend of
the fit parameters over the entire outburst.
As found by S18,
the photon index and the electron temperature slightly
increased and decreased, respectively, during the
flux rise at the beginning of the outburst.
In the second flux rise from MJD$\sim$58300,
the {\tt diskbb} component emerged from the low edge
of the {\maxi} energy band and it contributed more to the X-ray
spectrum as the source became brighter. In the high/soft state,
the total X-ray flux varied by a
factor of $\sim 5$ and the inner disk temperature varied
between $\sim$ 0.4 and $\sim$ 0.7, whereas the inner disk
radius was fairly constant at $\sim$60 ($D$/3 kpc)
($\cos i/\cos 60^\circ$) km, where $D$ and $i$ are
the distance and the inclination angle.

\begin{figure*}[ht!]
\plotone{./fig4_new3.eps}
\caption{Time variations of the parameters in the best-fit
models. The unabsorbed 1--100 keV flux
(in units of $10^{-8}$ erg s$^{-1}$ cm$^{-2}$, estimated
by adopting the normalization of the \maxi/GSC data),
the photon index, the electron temperature (keV),
the fraction of the Comptonization component, the inner
disk temperature (keV), the inner disk radius (km) estimated by
assuming a distance of 3 kpc and an inclination angle of
$60^\circ$, and the reduced chi-squared,
from top to bottom. \label{fig:trend_fitpars}}
\end{figure*}

The iron K$\alpha$ emission line, often seen in
other sources during the low/hard state and the intermediate
state, was not detected significantly in any of the above spectra.
This is most likely because of statistics and energy resolution
of the MAXI/GSC. Fitting the spectrum (b) in Fig.~\ref{fig:MAXIBATspec}
with the {\tt tbabs*nthcomp} model plus a Gaussian component,
which represents the iron line, we estimated the upper
limit on the equivalent width of the line as $\sim$300 eV.
This is consistent with the typical values in the low/hard
state $\lesssim 100$ eV \citep[e.g.,][]{mak08,kol14}.
In this fit, the line-center
energy and the width were fixed to $6.4$ keV and $100$ eV,
respectively, referring to the values obtained in
GX 339$-$4 \citep{shi11b}. The results were confirmed to
be unaffected, even when the line center energy is changed to
6.9 keV, corresponding to the H-like iron, and when the line
width is varied by a factor of 5.

\if0
Using the best-fit models, we estimated the inner disk radius $r_\mathrm{in}$,
assuming the conservation of the number of photons from the disk
after Compton scattering.
For the {\tt simpl*diskbb} model, we calculated it from the
normalization of {\tt diskbb}, which is given by
$\frac{r_\mathrm{in}^2 \cos i}{(D/ 10~\rm{kpc})^2}$, where
$i$ and $D$ are the inclination angle and the distance.
For models employing {\tt nthcomp}, we estimated the radius
from the photon fluxes of the direct disk
component ({\tt diskbb}) and the Comptonized component ({\tt nthcomp}),
via the equation given in \citep{kub04}:
\begin{eqnarray*}
P_\mathrm{d} + P_{c} \cdot 2 \cos i = 0.0165 \left[ \frac{r_\mathrm{in}^2 \cos i}{(D/ 10~\rm{kpc})^2} \right] \left( \frac{kT_\mathrm{in}}{1~\rm{keV}} \right)^3
\\~ \rm{Photons~s^{-1}~{cm}^{-2}},
\end{eqnarray*}
(where $P_\mathrm{c}$ and $P_\mathrm{d}$ are 0.01--100 keV photon fluxes of
the Comptonization component and the direct disk component, respectively),
by assuming a spherical geometry of the Comptonization component.
\fi

\section{Optical Data Reduction and Analysis}

Optical photometric observations of MAXI J1820$+$070
in the $g'$ band were performed with the MITSuME 50\,cm telescope
in Akeno Observatory, Yamanashi, Japan
\citep{kotani2005,yatsu2007,shimokawabe2008}, based on a
Target-of-Opportunity program in the Optical and
Infrared Synergetic Telescopes for Education and
Research (OISTER). We reduced the $g$'-band data
following standard procedures including
bias and dark subtraction, flat fielding, and bad pixel masking,
and then performed photometry of {MAXI J1820$+$070 } using IRAF.
Magnitude calibration was carried out by using the magnitudes
of nearby reference stars, which were taken from the UCAC4 catalog \citep{2013AJ....145...44Z}.
The source was also observed
through several different optical and near-IR filters,
with telescopes involved in the OISTER. The complete
datasets and their analysis will be presented by
Adachi et al. (in preparation).

Figure~\ref{fig:xoptlc} shows the unabsorbed 2--10 keV light
curve obtained from the best-fit models in Section~\ref{sec:spec},
and the optical $g'$-band light curve from the MITSuME telescope.
The optical data were dereddened
with the reddening factor $A_{g'} = 0.98$. This value was obtained
by using the extinction law given in \citet{car89} and the
reddening factor in the $V$-band, $A_V = 0.84$, which was
derived from the absorption column $N_\mathrm{H} = 1.5 \times 10^{21}$
cm$^{-2}$ via the $N_\mathrm{H}$ vs. $A_V$ relation in \citet{pre95}.
The errors of the magnitudes include both the statistical
photometric errors of MAXI J1820$+$070 and the systematic errors
of the reference star magnitudes (typically $\sim$0.034 mag in total).
Overall, the optical flux increased (decreased) with increasing
(decreasing) X-ray flux, although a weak optical re-brightening took
place just after the soft-to-hard transition during the X-ray decay (MJD $\sim$58400),
as was reported by \citet{bag18b}.
A remarkable point is that the $g'$-band flux at the first peak
on MJD $\sim$58202 is higher than that at the second peak on
MJD $\sim$58306 by $\sim 1$ mag (by a factor of $\sim 2.5$ in
the flux unit), whereas the X-ray flux at the first peak is
slightly lower than that at the second peak.

To investigate a flux correlation between
the X-ray and optical bands, we also plotted the
optical vs. X-ray luminosity diagram in
Figure~\ref{fig:xoptcor} using the simultaneous
data in Fig.~\ref{fig:xoptlc}.
The optical magnitudes were converted to fluxes,
and multiplied by the central frequency of the
$g'$-band filter, $\nu = 6.25 \times 10^{14}$
Hz, following \citet{rus06}, to obtain the fluxes in the $\nu F_\nu$ units. Using these extinction/absorption-corrected
optical and X-ray fluxes, we estimated the optical and
X-ray luminosities, $L_\mathrm{opt}$ and $L_\mathrm{2-10~keV}$,
respectively, assuming an isotropic radiation at a distance of 3 kpc.
As is noticed in this figure, the data points are more highly
scattered and $L_\mathrm{opt}$ with respect to $L_\mathrm{2-10~keV}$
is somewhat higher in the low/hard state than in
the intermediate state and the high/soft states. The
data points in the latter two states can be
described with a power-law function.
Fitting the data of the two states in Fig.~\ref{fig:xoptcor}
together, we obtained the best-fit model of $L_\mathrm{opt} \propto
L_\mathrm{2-10~keV}^{0.51 \pm 0.03}$.

\begin{figure}[ht!]
\plotone{./maxij1820_xunabs_gband7.eps}
\caption{X-ray 2--10 keV (top) and optical $g'$-band (bottom)
light curves of MAXI J1820$+$070. The X-ray light curve was
obtained from the best-fit model in Section~\ref{sec:spec}
and corrected for the interstellar absorption.
The optical magnitudes were corrected for reddening
and are expressed in the AB system.
The error bars of the optical light curves include both
the statistical photometric errors of MAXI J1820+070
and the systematic errors of the reference star magnitudes
($\sim$ 0.034 mag in total).
\label{fig:xoptlc}}
\end{figure}

\begin{figure}[ht!]
\plotone{./lumi_xout_norm1e36_4.eps}
\caption{Correlation of X-ray and optical luminosities of
MAXI J1820$+$070. Blue circles, black squares, and red triangles
indicate the data taken in the low/hard state, the intermediate state,
and the high/soft state, respectively. The dashed lines are
the best-fit power-law function for the data points
in the latter two states,
$L_\mathrm{opt} \propto
L_\mathrm{2-10~keV}^{0.51 \pm 0.03}$.
\label{fig:xoptcor}}
\end{figure}

\section{Discussion}
\subsection{Interpretation of the Long-term X-ray Evolution} \label{sec:discussion_lcspec}

We have monitored {MAXI J1820$+$070 } in 2--200 keV during its outburst
using \maxi/GSC and \swift/BAT. In the soft X-ray band below
6 keV, it showed two ``rapid rise and slow decay''-type
long-term flux evolutions (hereafter we call them
as the first/second sub-outbursts). This profile
is often seen in X-ray light curves of
transient black hole X-ray binaries.
The two big sub-outbursts suggest that, in this outburst,
the source
exhibited two discrete increases in
its mass accretion rate through the disk. Re-flares in the outburst
decay have been observed in many other black hole X-ray
binaries, and they usually occur after 50--100 days
from the first flux peak \citep[e.g.,][]{che93, nak14}.
This interval is similar to that of the two sub-outbursts
in MAXI J1820$+$070.

Such re-flares were often
interpreted by the enhancement of the mass
accretion rate from the donor star, which
was inflated due to the X-ray irradiation
\citep{che93,min94}.
This could also explain the second sub-outburst
of MAXI J1820$+$070, as was discussed in S18.
However, the re-flares in other sources are
usually much weaker than their main
outbursts, having $\sim$1 order of magnitude
lower peak luminosities than those of
the main outbursts. Why such a strong
re-brightening took place in MAXI J1820$+$070
is an open question, but maybe it is because
the source stayed in the low/hard state during
the first sub-outbursts, and the strong hard
X-rays heated the companion star more efficiently
than other sources with re-flares, which often
show state transitions in their main outbursts.

The HR was almost constant at a high level
during the first sub-outburst, whereas
its rapid decrease was observed in
the second sub-outburst. This indicates that the state
transition from the low/hard state to the
high/soft state (the hard-to-soft transition)
took place only in the second
sub-outburst. Interestingly, the 1--100 keV fluxes
were almost the same (different only by $\sim$10\%)
at the flux peaks in the two sub-outbursts.
If the radiation efficiency was constant
during the outburst,
this suggests that the mass accretion rates were
the same in the two peaks, and that the hard-to-soft
transition is not determined the mass accretion rate
alone. We note that, however, in reality, the radiation
efficiency most likely varies, depending
on the properties of the accretion flow and outflows
\citep[e.g.,][and references therein]{mal04,kat08}.
Hence, the same X-ray luminosity does not necessarily
mean the same mass accretion rate, and it is difficult
to completely rule out, using our results alone,
the possibility that the mass accretion rate at
the beginning of the hard-to-soft transition
was higher than that at the first X-ray peak.

More direct evidence that something
other than the mass accretion rate plays a
role to trigger the hard-to-soft transitions,
has been found in previous observations.
As was observed in other sources such as GX 339$-$4,
the hard-to-soft transitions actually took place
at different luminosities in different outbursts
of the same sources \citep[e.g.,][]{dun08}.
What made the difference in the two sub-outbursts
of {MAXI J1820$+$070 } is still unclear, but it may be related
to the magnetic fields in the inner disk region,
considering previous theoretical studies of
the accretion flows in the hard-to-soft transition
\citep{mat06, beg14}. Perhaps, in the first sub-outburst,
strong magnetic fields were present in the inner disk
region for some unknown reasons,
and prevented from developing the standard disk inwards.

Although the low/hard state period before the hard-to-soft
transition was unusually long,
the combination of two sub-outburst provided a normal ``q''-shaped
track in the HID, like other black hole binaries.
The hysteretic behavior in the HID, where the hard-to-soft
transition occurs at higher luminosity than that of the
transition from the high/soft state back to the low/hard
state (the soft-to-hard transition),
is seen not only in black hole binaries but
also neutron star low mass X-ray binaries \citep{mun14}.
However, MAXI J1820$+$070 is unlikely to harbor
a neutron star.
Typical soft X-ray spectra of neutron star
low-mass X-ray binaries at high luminosities
show a thermal emission component with a temperature
of $\sim 1$ keV and a comparably strong Comptonization
component located at slightly higher energies than
the thermal component, and these two components are
considered to originate in the blackbody emission of the
neutron star surface and a Comptonized disk emission
\citep{mit89}, respectively, or the disk blackbody emission
and a Comptonized neutron star blackbody emission \citep{chu95},
respectively. By contrast, all the high/soft-state spectra
of MAXI J1820$+$070 below 10 keV were successfully described by a
single disk blackbody model with $T_\mathrm{in} \lesssim 1$ keV.
We have confirmed that the fit of the spectrum (f) in
Fig.~\ref{fig:MAXIBATspec} is not improved when
{\tt nthcomp} with $kT_\mathrm{e} = 5$ keV (a typical value
for the Comptonization component of neutron star X-ray binaries) is
added to the {\tt simpl*diskbb} model. These results support
that its compact object is not a neutron star but a black hole.

The all-time monitoring and the wide coverage
provided by the combination of the \maxi/GSC and
\swift/BAT, have enabled us to simultaneously
determine the levels of the disk and Comptonization
components in the X-ray spectrum of MAXI J1820$+$070,
and study their long-term variations in the outburst.
We discuss the evolution of the structure
of the accretion flow, based on the results
from our spectral analysis.

In the low/hard state, the spectrum was well described
with a thermal Comptonization
component with $\Gamma < 2.0$ and $kT_\mathrm{e} \gtrsim$
40 keV. We detected a gradual increase of
$\Gamma$ and decrease of $kT_\mathrm{e}$
during the rapid flux increase in the first sub-outburst
(see Tab.~\ref{tab:fit} and Fig.~\ref{fig:trend_fitpars}).
As discussed in S18, this could be explained
by the disk truncation model, in which the
standard disk is truncated in the
beginning of the outburst, and it develops
inward as the X-ray flux increases
\citep[e.g.,][for more details]{don07}.
The seed photons for Compton scattering
increases as the standard disk extends
inward, which would cause a more effective
cooling of the hot inner flow or corona.

In the intermediate state, where the spectral
softening/hardening took place, the inner disk temperature
rapidly increased as the total X-ray flux increased,
while the fraction of the Comptonization component
in the total X-ray flux dropped
and the photon index increased up to $\sim$ 2.5.
The rapid change of the X-ray spectrum
is typical of black hole X-ray binaries
in the intermediate state. In this phase, $r_\mathrm{in}$
was not well constrained, due to uncertainties
in the inner disk temperature and the normalization
of the direct disk component, whose contribution
to the total X-ray flux was smaller than that
in the high/soft state.

After the hard-to-soft transition, the contribution of
the Comptonization component decreased down to less than
a few \%, a typical value in the high/soft state.
During the high/soft state,
the inner radius was almost constant
at $r_\mathrm{in} \sim 60$ ($D$/3 kpc) ($\cos i/\cos 60^\circ$)$^{-1/2}$ km,
even though the 1--100 keV flux decreased
by a factor of $\sim$ 5. This indicate that the
standard disk extended stably down to the innermost
stable circular orbit (ISCO) in this period.

\begin{figure}[th!]
\plotone{./M_vs_i.eps}
\caption{Constraints on the black hole mass
and the inclination angle of MAXI J1820$+$020,
in the case of a non-spinning black hole. The
horizontal and vertical lines
present the lower limit of the mass imposed
by the luminosity at the soft-to-hard
transition, and the lower limit of the
inclination angle at which the dips
are observed, respectively.
The solid curve shows the relations
obtained from the constant inner radius
in the high/soft state, and the
dashed ones separating the
shadowed region are its upper/lower
limits considering the errors of
the inner disk radius and the distance.
\label{fig:M_i}}\end{figure}

\subsection{Estimation of System Parameters} \label{sec:discussion_mass}

We have attempted to constrain the black hole mass
using the results of our spectral analysis.
\citet{mac03} suggested that the soft-to-hard
transition occurs at 1-4 \% Eddington luminosity
($L_\mathrm{Edd}$). The 0.01--100 keV flux
at the beginning of the soft-to-hard transition is
estimated to be $\sim 5 \times 10^{-8}$ erg cm$^{-2}$
s$^{-1}$ from the best-fit model, which
can be converted to a luminosity of $\sim 5 \times
10^{37}$ ($D$/3 kpc)$^2$ erg s$^{-1}$, if an isotropic
emission is assumed.
Considering the uncertainties in the transition
luminosity and the distance ($\approx 3 \pm 1$ kpc; \citealt{gan18b}),
the lower limit of the black hole mass ($M_\mathrm{BH}$)
of {MAXI J1820$+$070 } is calculated as 4 $M_\sun$, when
$D=2$ kpc and the transition
luminosity of $4$\% $L_\mathrm{Edd}$ are adopted.
This value justifies that the source has a black hole accretor.

Another constraint is given
from the inner disk radius in the high/soft state,
which is considered to be identical the radius of
the ISCO. We derive $r_\mathrm{in} = 66.0 \pm 0.8$
($D$/3 kpc) ($\cos i/\cos 60^\circ$)$^{-\frac{1}{2}}$
km as a weighted average of the inner radii estimated
in the high/soft state.
Applying the combined correction factor of 1.18,
for the stress-free boundary
condition and the color-temperature correction
\citep[see e.g.,][]{kub98},
we obtain $R_\mathrm{in} = 77.9 \pm 1.0$
($D$/3 kpc) ($\cos i/\cos 60^\circ$)$^{-\frac{1}{2}}$ km.
In Figure~\ref{fig:M_i}, we plot the constraint
obtained by equating this radius to that of the ISCO,
as a shaded region on the $M_\mathrm{BH}$
versus $i$ plane. Here, we have assumed a non-rotating
black hole, in which case th radius of the ISCO
is 6 $GM_\mathrm{BH}/c^2$
(where $G$ and $c$ are the gravitational constant and
the light speed, respectively).

In the beginning of the outburst, {\it NICER} detected a
strong absorption dips \citep{hom18c}, which are often seen
in X-ray binaries with high inclination angles
above $\sim 70^\circ$ \citep[e.g.,][and references therein]{boi03, hom05}.
If {MAXI J1820$+$070 } has a high inclination angle similar to other dipping
sources, a lower limit of $M_\mathrm{BH}$, $\sim
7 M_\sun$, is obtained from Fig.~\ref{fig:M_i}.
The origin of the dips in {MAXI J1820$+$070 } is not yet fully
understood, however; the dips have not been detected
after the flux peak in the first sub-outburst,
Also, ionized absorption lines from disk winds,
also often observed in high inclination sources,
have never been detected in the outburst. The allowed
range of $M_\mathrm{BH}$ becomes lower if the
source has a smaller inclination angle than other
X-ray binaries with dips and ionized absorption lines.
\if0
A constraint on the
inclination angle, $\lesssim 70^\circ$, would also
be imposed because no absorption dips have been
detected in the X-ray light curves, nor ionized
absorption lines from the disk winds.
Combining these constraints, we obtain $4-xx M_\sun$
as a realistic value of $M_\mathrm{BH}$.
\fi

If the black hole of {MAXI J1820$+$070 } is a Kerr (rotating)
black hole, the $M_\mathrm{BH}$ values
become larger (by up to a few to several
times in the case of the maximum spin) than
those in the zero-spin case,
primarily because the ISCO radius decreases
from 6 $GM_\mathrm{BH}/c^2$ up to $\sim 1 GM_\mathrm{BH}/c^2$,
as the black hole spin becomes higher
(see \citealt{dav11} for more detailed discussion and
\citealt{dav11, shi11a, wan18} for comparisons of
the constraints on $M_\mathrm{BH}$ among different spin parameters).
In the case of a highly spinning black hole,
the strong relativistic effects,
including gravitational redshift and light
bending in the vicinity of the black hole,
and the Doppler beaming due to the disk rotation,
modifies the observed disk spectrum from that obtained
with the simple {\tt diskbb} model, and hence
disk emission models considering these effects,
instead of the simple multi-color disk model,
must be employed to describe the spectra and to determine
$M_\mathrm{BH}$ accurately.
However, the {\maxi} spectra do not have statistics
and soft X-ray coverage sufficient to apply such
relativistic disk emission models. For further studies,
we need data from soft X-ray detectors like $NICER$, with high
sensitivity but free from the pile-up effects,
This is beyond the scope of this work and we
leave it as a future work.

Also, the common transition luminosity estimated
by \citet{mac03} may not always be applicable;
an exception has recently been found in the
outburst of MAXI J1535$-$571 \citep{nak18},
which stayed in the high/soft state even after
the X-ray flux decreased $\sim$ 3 orders of
magnitude from the luminosity of the hard-to-soft
transition. To derive more accurate $M_\mathrm{BH}$
and to test the argument on the transition
luminosity, determination of the mass function
of {MAXI J1820$+$070 } is required via optical spectroscopy
in the quiescence phase.

\subsection{Optical and X-ray Correlation}

In most of the outburst period, the optical flux
increased/decreased with the X-ray flux
rise/decay, although in the optical band,
the second sub-outburst
was weaker than the first
sub-outburst, unlike those in the X-ray
band; in 2--10 keV, the second peak flux
was twice higher than that of the first peak.
Consequently, the $L_\mathrm{opt}/L_\mathrm{2-10~keV}$
ratio in the intermediate state and the high/soft state
is relatively small compared with that in
$P_\mathrm{H}$ (see Fig.~\ref{fig:xoptcor}).
Similar trend was found in other BHBs
\citep{rus06}. The difference in the
$L_\mathrm{opt}/L_\mathrm{2-10~keV}$
value can be explained by the contribution
of the jet in the optical band during the low/hard
state. Indeed, S18 found that the jet emission
can substantially contribute to the optical
flux but not significantly to the X-ray flux of
MAXI J1820$+$070 during the low/hard state.
A smaller $L_\mathrm{opt}/L_\mathrm{2-10~keV}$
value would be obtained if the jet in
suppressed in the other states, as suggested
by \citet{tet18,cas18}.
We note, however, that the synchrotron emission
from a magnetized hot inner accretion flow
could also considerably contribute to the optical
flux and its variation in the low/hard state,
as suggested by \citet{vel18}.
It is difficult to separate the contributions of
the jets and the hot inflow, because they
can have similar SED profiles and variability
properties \citep{vel13, vel18}.

We have found a tight correlation between
the X-ray and optical luminosities in the
intermediate state and the high/soft state,
which is well reproduced by a power-law model
as $L_\mathrm{opt} \propto
L_\mathrm{2-10~keV}^{0.51 \pm 0.03}$,
whereas the data points in the low/hard state
are strongly scattered. Considering that
our optical and X-ray observations were
not exactly simultaneous, the scatter
in the low/hard state
could be produced
by the strong flux variations in both
optical and X-ray bands on timescales of
$<$day, which are likely to originate in
synchrotron radiation from the jets
or the hot inflow, and Comptonization of
the disk photons in
the hot inflow/corona, respectively
(e.g., \citealt{gan18a}; \citealt{tuc18}; S18).
By contrast, appearance of the strong X-ray-optical
correlation in the intermediate state and the high/soft state
would indicate the suppression of such variability
in these states, and this could be explained if
the jets were quenched and the standard disk
was developed close to the ISCO, replacing the
hot inner flow.

When the variable emission components are suppressed,
the blackbody emission from the companion star, and/or
the reprocessed emission from the outer disk
irradiated by strong X-rays,
are the possible origins of the the optical flux.
The former possibility is unlikely in MAXI J1820$+$070,
because its optical magnitude in quiescence was
found to be $\gtrsim 18$ mag,
much lower than those during the outburst (S18).
Hence, the observed correlation
in the intermediate state and the high/soft state
would be produced by variation of the disk emission.
If the optical band is located in the Rayleigh-Jeans (RJ)
part of the disk spectrum,
$L_\mathrm{opt}$ should be proportional to
$L_\mathrm{X}^{1/4}$. If it is located
in the flat part of the irradiated disk
spectrum, which is produced at higher
frequencies than the RJ part by the
reprocessing of the X-rays \citep{gie09},
$L_\mathrm{opt} \propto L_\mathrm{X}$
is realized \citep[e.g.,][]{cor09,shi11b}.
The index of the correlation that we obtained,
$0.51 \pm 0.03$, is larger than that expected in the RJ part
and smaller than that of the flatter part, and therefore
the $g'$-band frequency of MAXI J1820$+$070
may correspond to the transition region
between the RJ and flat parts, somewhere around
the peak frequency of the blackbody emission
of the outer disk edge.

If the above discussion is correct, the
$g'$ band approximately corresponds to the
peak of the blackbody emission from the irradiated
outer disk edge, and this
gives the outer disk temperature, $T_\mathrm{out,eff} \sim 0.1$ eV.
The total flux generated at the outer edge,
$\sigma T_\mathrm{out,eff}^4$ (where $\sigma$ is
the Stefan-Boltzmann constant) is determined by the sum of
the intrinsic disk flux at the outer edge,
$\sigma T_\mathrm{in}^4 \left(\frac{R_\mathrm{out}}{R_\mathrm{in}} \right)^{-3}$
(where $R_\mathrm{out}$ is the outer disk radius),
and the illuminating X-ray flux that is thermalized
at $R_\mathrm{out}$. Assuming the irradiated disk model
constructed by \citet{gie09}, where the illuminating
X-ray flux decreases in proportion to $r^{-2}$
and a fraction $f_\mathrm{out}$ of it is thermalized,
the total flux at $R_\mathrm{out}$ is expressed as
\begin{equation}
    \sigma T_\mathrm{out,eff}^4 = \sigma T_\mathrm{in}^4 \left(\frac{R_\mathrm{out}}{R_\mathrm{in}} \right)^{-3} + f_\mathrm{out}
    \sigma T_\mathrm{in}^4 \left(\frac{R_\mathrm{out}}{R_\mathrm{in}} \right)^{-2}.
\end{equation}
In the high/soft state, the second term is usually
dominant and $f_\mathrm{out}$ is typically $\sim 10^{-3}$ \citep[e.g.,][]{gie09}.
Adopting $T_\mathrm{in} \sim 0.7$ keV, a typical value
of MAXI J1820$+$070 in the high/soft state, we obtain
$R_\mathrm{out} \sim 10^6 R_\mathrm{in} \sim 10^7$ km.
Application of this value to the Keplar's third law
gives a lower limit on the orbital period,
$\sim 2~((M_\mathrm{BH}+M_\mathrm{c})/10 M_\sun)^{-1/2}$ day,
where $M_\mathrm{c}$ is the mass of the companion star.
The above calculation is just a rough order-of-magnitude
estimation based on some assumptions, and should be tested in
the future by e.g., modeling spectral energy distribution
from optical to X-ray bands, and measuring orbital modulations
of emission/absorption lines through optical spectroscopy.

\section{Summary}
We have studied the nature of {MAXI J1820$+$070 }
and the evolution of its accretion
disk structure, using the {\maxi}/GSC
and {\swift}/BAT data obtained in
almost the entire period of the 2018 outburst.
The behavior in the hardness intensity diagram,
the basic properties of the X-ray spectra, and
the constraints on accretor's mass obtained
from our spectral analysis, indicate that the
source is a black hole binary.
We found that the outburst is composed of two
``fast rise and slow decay''-type flux evolutions,
with almost the same total X-ray luminosity at the
peaks, although the state transition only took place
in the second flux rise and decay. This implies
that the mass accretion rate is not the unique
factor to trigger the transition to the high/soft
state. The X-ray spectrum was well described with
the standard disk emission and its Comptonization,
and its long-term variation can be explained
in terms of the disk truncation model. The
optical-X-ray luminosity correlation suggests
that in the low/hard state the optical flux
was substantially contributed by emission
from the jets, which was likely to be suppressed
in the intermediate and high/soft state.

\acknowledgments

We acknowledge the use of {\maxi} data provided by RIKEN, JAXA
and the {\maxi} team, and of public data from the {\swift}
data archive. Part of this work was financially supported
by Grants-in-Aid for Scientific Research 16K17672 (MS),
17H06362 (NK, YU, HN), and 16K05301 (HN)
from the Ministry of Education, Culture, Sports,
Science and Technology (MEXT) of Japan.
This work was supported by Optical and Near-Infrared Astronomy
Inter-University Cooperation Program and the joint research program
of the Institute for Cosmic Ray Research (ICRR).

\vspace{5mm}
\facilities{\maxi(GSC), \swift(BAT)}

redpajama_set_name: RedPajamaArXiv


text:
Q: Having variable issue I'm having trouble with a variable being update. Below, my Main document function has my level equaling 1 and generating multiple tiles. It does equal 1, but I have the if statement saying to go up a level if a var equals true.
    public var enemiesDefeated:Boolean = false;
    addChild(level);
    //START THE GAME AT LEVEL 1//
    level.levelNumber = 1;
    if (enemiesDefeated == true){
        level.levelNumber += 1;
    }
    var tileh:int = 60;

    for (var Y:int=0; Y<floor.length; Y++)
    {
        for (var X:int=0; X<floor[Y].length; X++)
        {
                var cell:MovieClip = new Tile(X,Y);
            cell.gotoAndStop(floor[Y][X]);
            cell.x = ((X-Y)*tileh)+365;
            cell.y = ((X+Y)*tileh/2)+70;
            addChild(cell);

            cell.addEventListener(MouseEvent.CLICK, mouseclick);
            cell.addEventListener(Event.ENTER_FRAME, onGame);
            cell.addEventListener(Event.ADDED_TO_STAGE, addEnemy);
        }
    }

The variable enemiesDefeated is turned to true in my onGame function if I destroy all the enemies, however, the level is staying at level 1 after enemiesDefeated equals true.
function onGame(event:Event){

    ...

    if (enemy.enemyHP <= 0)
        {
             removeChild(enemy);
             enemy.enemyDead = true;
             enemiesDefeated = true;
             trace("Dead", enemy.enemyDead);
        }
}

Is there a way to fix this?

redpajama_set_name: RedPajamaStackExchange


A case of selective application?
The first thing that came to mind when an arrest was made regarding the recent hoax call to the George FL Charles Airport at Vigie was how quick the police had traced the culprit.
One always knew the technology existed and is available across the Caribbean to allow service providers to trace every phone call made, so one also always wondered why, to one's knowledge, no one had previously been traced, arrested and charged for this criminal offense.
There've been dozens of such incidents (reported and unreported) here and across the region in which workers have been forced to vacate buildings and assemble safely elsewhere while the police take the necessary time to properly search.
Over time, affected workers here and elsewhere started becoming fed-up with the repeated interruptions of their day's work schedule, resulting in the collective loss of thousands of working hours — each and every time.
Many here would have liked to have been able to just sit at their desks and continue working while others 'waste their time', but have had to accept — each time — that while all previous calls had been pranks resulting in mere scares, one can never tell when 'the real thing' will happen.
Considering the hundreds of thousands of working hours and the resulting losses in earnings, incomes, payments and other forms of business, one would have thought there would have been, by now, some determination somewhere to more readily use the available technology to trace, catch and prosecute pranksters.
Given how quick the alleged culprit in the airport case was caught, one also expected that by yesterday (never mind All Fools Day) the police would just as quickly have traced those whose calls closed down Castries last Friday.
But the charging of someone in the airport matter certainly has not resulted in perpetrators lessening their will to continue doing the same — and even more, as they targeted at least five local banking and financial institutions, all in one day — and within much less than one square mile in the city's centre.
Interestingly, more prank calls were made on Friday than in the airport case, but investigators have (so far) been less able to as quickly trace the calls.
And then there's the case of a local boat captain who claimed persons were impersonating him by falsely claiming and receiving monies in his name.
After six months of complaints, the Rodney Bay-based captain says, he made the impersonators' telephone numbers available to the Gros Islet police and actually invited them to make an arrest after the individuals were identified — but to no avail.
He says he eventually arranged a sting operation to ensnare the impersonators, leading to their eventual arrest last week – by City Police officers on patrol.
One would like to believe there are reasons why the airport prank call was traced so quickly, while no other like calls have (so far) been traced, with arrests.
But the silence of the investigators is so deafeningly loud that no one can even hear — far less see or imagine — what such reasons could be, allowing for those not in the know to feel and (just as loudly) claim there may be some selectivity in application of the tech and the law when it comes to tracing and prosecuting perpetrators of this criminal practice.
There's need for some clarification here, I would think, if only to prove that's not the case.


text:
Q: how to create new column on the basis of word matched how to add a new column on the basis searched item like if dataframe column contain BX-- then in new column it should replace it with BOX as there are more than 30 short form
i think dictionary would be best option for replacement
 mapping= {
'BX': 'BOX',
'CS': 'CASE',
'EA': 'EACH',
'PK': 'PACK',
'None': None
  }
  import pandas as pd
   lst = ['BX', 'EA', 'EA', 'PK', 'BG','CS']
  df = pd.DataFrame(lst)
      df.map(mapping)

somehow i am not able to do it

A: You can do this as follows.
# first define a mapping
mapping= {
    'BX': 'BOX',
    'CS': 'CASE',
    'EA': 'EACH',
    'PK': 'PACK',
    'None': None
}

# then apply it with map (assuming your abbreviations are
# stored in column short and the result should be stroed
# in long)
df['long']=df['short'].map(mapping)

With the following test dataframe
lst = ['BX', 'EA', 'EA', 'PK', 'BG','CS']
df = pd.DataFrame(dict(short=lst))
df['short'].map(mapping)

It outputs:
Out[447]:
  short  long
0    BX   BOX
1    EA  EACH
2    EA  EACH
3    PK  PACK
4    BG   NaN
5    CS  CASE


Lyrics catalog with ability to integrate the application with iTunes Library.
Now lyrics of russian artists are in your iPhone. You can use this app being on a party with friends or alone, reading your favorite texts.
Integration with iTunes Library. You can bind a song from library to composition lyrics and sing together with your favorite artists.


Join the International Orphan Relief Foundation, in partnership with The Streets of Brentwood, to sponsor one of many scheduled activities, at Family Fun Day on March 24th, as part of Spring Fling @ The Streets.
.All vendors are responsible for bringing their own tents, tables, chairs etc.
Vendor check in time before 9am.
Please return your sponsorship request by March 15, 2018.
jstatonprod@aol.com. if you have any questions, or if you would like to volunteer to assist with this event or donate goods or services, please contact Johnny Staton, Committee Chairperson at (925)516-4518 or by email to jstatonprod@aol.com.
Thank you for supporting the International Orphan Relief Foundation.


text:
Police latest after 14 month old boy found alone in Plymouth street
Devon and Cornwall Police have issued an update
Police at the scene of an incident (Image: Penny Cross)
Police have issued an update after a toddler was found alone in a Plymouth street.
Devon and Cornwall Police were alerted to the incident at around 6pm on Thursday after the 14-month-old was found outside on his own.
Two hours later, officers, including armed response units, were dispatched to reports of people with weapons at a property, making threats to the occupants.
Today – Friday – a spokesperson for Devon and Cornwall Police confirmed that a 31-year-old woman and a 41-year-old man were arrested on suspicion of neglect.
Police searching for assault suspect after police helicopter incident
Harry Tangye finally reveals his future plans when he leaves the police
The spokesperson said: "A 31-year-old woman and a 41-year-old man have been arrested on suspicion of child neglect after an 14-month-old boy was found wandering around outside alone [in] Plymouth, last night, Thursday 16 April, at around 6pm.
"The child is safe and well and is under the care of social services."
The man and woman have now been released pending further investigation.
Officers are investigating reports that threats were made and enquiries are ongoing at this time.
The force spokesperson added: "Police, including fire arms officers, were called to a residential address [in] Plymouth, last night, Thursday, 16 April, at around 8pm following reports that a group of people were making threats to the occupants of the address, armed with weapons.
"Any persons involved had fled the scene when police arrived.
"Police are investigating the incident."


text:
EM Microelectronic, basé à Marin, à La Tène près de Neuchâtel en Suisse, est un développeur et fabricant de semi-conducteurs spécialisé dans la conception et la production de circuits intégrés à très faible puissance et basse tension pour les applications alimentées par batterie dans les secteurs grand public, automobile et industriel. EM Microelectronic SA est une filiale du Swatch Group depuis 1985 .

Filiales
EM Microelectronic dispose d'un centre de design à son siège social à Marin, en Suisse près de la ville de Neuchâtel.

EM dispose de filiales et de centres de conception supplémentaires:

 EM Microelectronic - US Inc., située à Colorado Springs, Colorado, États-Unis.

 ASICentrum sro  est un centre de design situé à Prague, en République tchèque. Il participe à la conception de circuits intégrés numériques, analogiques et mixtes.

Technologie

EM Microelectronic se spécialise dans la conception et la production de circuits intégrés à très faible puissance et basse tension pour les applications alimentées par batterie et sur site dans les produits grand public, automobiles et industriels.  Elle dispose d'installations de fabrication de semi-conducteurs en interne et utilise également des fonderies externes.

Produits
Les produits d'EM Microelectronic comprennent des circuits RFID, des circuits intégrés pour cartes à puce, des microcontrôleurs à très faible puissance, la récupération d'énergie, la gestion de l'alimentation, des pilotes et écrans LCD, des capteurs optiques et des circuits intégrés d'interface de capteur. EM fabrique non seulement des circuits standard et des ASIC, mais également des systèmes et des modules pour des applications telles que le contrôle d'accès, l'identification par radiofréquence, les téléphones mobiles, les appareils grand public, les systèmes d'alarme et de sécurité, les compteurs de services publics et de chauffage, le traitement du signal des capteurs, le contrôle, l'immobilisation des voitures, les sous-systèmes électroniques automobiles et bien d'autres.

BLE et sans fil 2,4 GHz
EM Microelectronic conçoit et développe des produits Bluetooth Low Energy tels que l'EM9304, destinés aux applications à faible encombrement et à faible consommation d'énergie. EM est membre associé du Bluetooth SIG et contribue par le biais de plusieurs groupes de travail à améliorer les spécifications et l'expertise mondiales en matière de conception à très faible consommation d'énergie pour la technologie sans fil Bluetooth à faible consommation d'énergie. EM Micro dispose également d'une famille de produits de liaison propriétaire avec des solutions 1Mbits, 2Mbit / s et longue portée.

RFID
EM a commencé son activité RFID dans les années 1980 et son portefeuille comprend des produits RFID passifs, semi-actifs et actifs, dans des gammes de fréquences comprenant LF, HF et UHF.

La popularité de la gamme EM Microelectronic de ~ 125 Les appareils RFID kHz ont conduit à des produits d'autres fabricants annoncés comme "compatibles EM4100", bien que cela puisse simplement signifier que le dispositif actif intégré dans l'étiquette / la carte RFID est un produit EM Microelectronic.

EM Microelectronic a développé des circtuis intégrés RFID UHF au début des années 1990 et a lancé le premier déploiement de grande distribution en 2003, avec Marks & Spencer.

En 2008, EM avait expédié 250 millions de circuits intégrés UHF dans le projet Marks & Spencer.

En 2015, EM Microelectronic a lancé em | echo, une gamme de puces combinant la communication RFID UHF et HF, ou RAIN RFID et NFC, une combinaison qu'elle appelle «RAINFC». Ce concept permet d'utiliser la même étiquette RFID pour la logistique et l'interaction du consommateur avec un produit. En 2020, EM a lancé la deuxième génération de cette famille, em | echo-V, récompensée «Meilleur nouveau produit» par RFID Journal

Voir également
 Circuit intégré spécifique à l'application
 Bluetooth basse énergie
 Microcontrôleur
 RFID

Notes et références

Liens externes
 Site Web de l'entreprise EM Microelectronic-Marin
 Description du protocole EM4100 (récupéré le 20 janvier 2013)]

Entreprise d'électronique ayant son siège en Suisse


Over 8000 people attend the suburban All Saints Catholic parish each week. Wester, 62, also teaches homiletics, aka the art of preaching, at Kenrick-Glennon Seminary. His preaching inspiration comes from Martin Luther King, Jr., Walter Brueggemann, and of course, he adds, the simple teachings of Jesus.
I've found in my 36 years preaching that silence is often the greatest reverence for anything. Take a few moments to silently live with our reactions. Are you feeling scared like you want to hide and never want to be with people again? Are you feeling angry? Helpless, like what could I do in the face of such great evil? Then, out of our silence—even if we don't have words—what will our response be to the choice someone made to do evil? Will that response be governed by evil, or by virtue returned? If we are the people who we say we are, and follow the footsteps of someone who was nailed to a tree and forgave those who hurt him, what will be our response?
My other thought is a very Catholic-centered message that the cross is the centerpiece of our faith. There is no mistaking that this is one of those moments of the cross. Just like in the crucifixion of Jesus, the main thing we do is seek where there is love in the midst of this destruction. You can invite people to say, what are you looking at, what are the images that are filling your mind and heart? Are they the blood and limbs laying on the street, or are they the guys who tied the tourniquets to save people from bleeding to death, or the surgeons who worked to save peoples lives, or the families who took people in while they are waiting for loved ones?
Somehow it says to us again that our strength is in our gathering. Our fear, our anger might cause us to want to run and hide. But the strength you see today is in the gathering of the people. It is the strength we gather from each other and with each other.
People that are anxiety ridden anyway, something like this triggers that in them. People who are depressed or cynical about humanity, this triggers it in us. Wherever our Achilles heel is, this triggers that in us. The violence has the ability of triggering that in us unless we counter it with some other truth.
The Biblical passage this week is on Jesus the good shepherd from John's gospel. Jesus says, They are mine, they are in my hands and no one has the power to take them from me. That message will be tied in somewhere in the hopeful part of my homily. That is the promise we live out of, the promise that takes flesh in how we take care of other people.


text:
Susana Baca: Live in Concert 2005
Susana Baca, the Peruvian vocalist who became internationally renowned with "Maria Lando," a track in the 1995 David-Byrne-produced CD The Soul of Black Peru, has often been compared to Cesaria Evora, from Cabo Verde. It's not surprising; both women have found rich material in folk traditions of their countries, and both sing songs that are rooted in gloomy emotions: pain, nostalgia, longing.
Susana Baca: Live in Concert-2005
Susana Baca, the Peruvian vocalist who became internationally renowned with "Maria Lando," a track in the 1995 David-Byrne-produced CD The Soul of Black Peru, has often been compared to Cesaria Evora, from Cabo Verde. It's not surprising; both women have found rich material in folk traditions of their countries, and both sing songs that are rooted in gloomy emotions: pain, nostalgia, longing. Susana Baca is not only one of the greatest divas in South America, she is a tireless researcher, and is largely responsible for the revival of many forms of Afro-Peruvian folklore. She is also the founder of the "Centro Experimental de Música Negrocontinuo" (Institute of the Black Continuum), a cultural center dedicated to the study of Afro-Peruvian music and dance. Won a GRAMMY AWARD in 2002.
Permanent URL: http://hdl.handle.net/2333.1/4j0zpcfz
Date: Thursday, March 17, 2005
Website: www.susanabaca.com
Encuentro Location: Palacio das Artes -- Grande Teatro
https://hemisphericinstitute.org/en/enc05-performances/item/1397-enc05-susana-baca.html#sigProIdb232195ef6
« Guillermo Gómez-Peña, James Luna, and Violeta Luna Grupo de Teatro de Bonecos Giramundo: Cobra Norato »
link-arrow Created with Sketch.
Help secure the future of our fearless artists, scholars, and activists from across the Americas. Support the work of the Hemispheric Institute.
The Hemispheric Institute connects artists, scholars, and activists from across the Americas and creates new avenues for collaboration and action. Focusing on social justice, we research politically engaged performance and amplify it through gatherings, courses, publications, and archives. Our dynamic, multilingual network traverses disciplines and borders and is grounded in the fundamental belief that artistic practice and critical reflection can spark lasting cultural change.
Never Miss an Event or Exhibition Again! Sign up for our mailing list to receive regular updates on events, publications, and exhibitions.
Made with in New York City. Copyright © 2020 Hemispheric Institute of Performance and Politics
Accessibility | Privacy


text:
Part IV CRIMES, PUNISHMENTS AND PROCEEDINGSIN CRIMINAL CASES
Title I CRIMES AND PUNISHMENTS
Chapter 272 CRIMES AGAINST CHASTITY, MORALITY, DECENCY AND GOOD ORDER
Section 53A Engaging in sexual conduct for a fee; engaging in sexual conduct with child under age 18 for a fee; penalties
Section 53A
Go Directly to a General Law
Go to General Law
Section 53A: Engaging in sexual conduct for a fee; engaging in sexual conduct with child under age 18 for a fee; penalties
Section 53A. (a) Whoever engages, agrees to engage or offers to engage in sexual conduct with another person in return for a fee, shall be punished by imprisonment in the house of correction for not more than 1 year or by a fine of not more than $500, or by both such imprisonment and fine, whether such sexual conduct occurs or not.
(b) Whoever pays, agrees to pay or offers to pay another person to engage in sexual conduct, or to agree to engage in sexual conduct with another person, shall be punished by imprisonment in the house of correction for not more than 2 and one-half years or by a fine of not less than $1,000 and not more than $5,000, or by both such imprisonment and fine, whether such sexual conduct occurs or not.
(c) Whoever pays, agrees to pay or offers to pay any person with the intent to engage in sexual conduct with a child under the age of 18, or whoever is paid, agrees to pay or agrees that a third person be paid in return for aiding a person who intends to engage in sexual conduct with a child under the age of 18, shall be punished by imprisonment in the state prison for not more than 10 years, or in the house of correction for not more than 2 and one-half years and by a fine of not less than $3,000 and not more than $10,000, or by both such imprisonment and fine, whether such sexual conduct occurs or not; provided, however, that a prosecution commenced under this section shall not be continued without a finding or placed on file.