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The Remarkable Ladies of Christmas
Posted on February 14, 2019 January 12, 2020 by admin
Hey there, hi there, ho there. This month, I wanted to share some thoughts on just how important women are to our Christmas performing art form. And coincidentally, just how much they have helped shape the Holiday as we've come to know it.
Mrs Claus Saves the Day (artwork by Vanessa Ellis)
First, let's ponder some not so imponderables. Consider the following.
Who generally teaches children about Christmas?
Who does most of the Christmas decorating in homes?
Who does most of the wrapping?
Who does most of the baking?
Who plans most social gatherings?
Who does most of the bookings for Christmas characters?
When you see lines for photos with Santa, who stays with the kids?
Who does most of the Christmas shopping (that $465 billion annual industry)?
See a pattern developing? But let's get more specific. In the Christmas Performing industries,
Who are most of the agents? Women.
Who creates most of the costuming? Women.
Who have been some of our first trainers? Women.
And for those of us lucky enough to have Manager/Handlers in our lives, they tend to be: Women (surprise!). They help us make the magic possible (big shout out to my "Manny," Ms. Cat).
The simple truth, gents, is that we Santas are essentially the furry hood ornament on the front of the sleigh that is the Christmas Industry. This is a profession that owes so much to the ladies. We should do everything we can to support them.
There's so much irony in all this. Mrs. Claus of legend and lore is sometimes considered pretty anonymous as a character. Most people cannot tell you her first name or give you any specifics beyond, "she's a nice old lady who makes cookies." That's rather sad. It's also much like real life where women are still getting paid only 70% on the dollar that men make, plus putting in longer hours to boot. Most female Christmas performers (with a few exceptions) have to fight to get paid as much as their male colleagues. Often they are not hired for many gigs simply because, "Mrs. Claus just isn't in the budget."
As professional Christmas Performers, we know there are incredibly talented female performers who have amazing chops, can work their magic with crying babies and groups of children, sing from the stage, or enthrall with a puppet like few Santas can.
Ladies Who Influenced Christmas History
Before Mrs. Claus ever appeared in print, the esteemed Thomas Nast described Saint Nick getting his dance on with Mother Goose. And while Mother Goose may not have been the prettiest of ladies, she did come with some real advantages. She was bundled with a pantheon of stories, songs, and characters that Saint Nick fit into, amid a body of lore that went back centuries. Nast was not only a brilliant illustrator, he was pretty darn clever, associating Santa in a rich story tradition, just like the clever move placing St. Nick at the apolitical North Pole.
Mrs. Claus (Finally in Print)
Mother Goose dances with Santa Claus (Thomas Nast)
The traditional St. Nicholas—a religious figure, a bishop, and reputably a long-term bachelor—went through several transformations before the Jolly Old Elf we know today. To make him a bit more trustworthy and retool him for domesticity, along came Santa's wife. Mrs. Claus was likely already part of the tradition when she was first mentioned in a short story called, "A Christmas Legend," written by James Rees in 1849.
Then in 1878, a children's book was published titled, "Lill's Travels in Santa Claus Land and Other Stories." Young Lill on her adventures meets, "a lady sitting by a golden desk writing in a large book,"—the Naughty and Nice book. From this time on, Mr. and Mrs. Claus become an item (sorry, Ms. Goose).
As we look at the histories of women in Christmas traditions, remember that in many of these eras, it was uncommon for women to receive a formal education. Many of these women were not allowed to own property, could not vote, and often published their writing under a male pseudonym.
Sarah Josepha Hale was the editor of "Godey's Lady's book"—one of the most influential periodicals before the Civil War, with a circulation of 150,000. This brilliant and self-taught woman was also the author of, "Mary Had a Little Lamb." She also helped establish many of the traditions of Thanksgiving and fought to make it a national holiday.
Sarah Josepha Hale, editor of "Godey's Lady's book"
Sara held Queen Victoria as a role model (another powerful woman) who had her own influence on Christmas. Queen Victoria started the tradition of Christmas Trees in the palace, via a German/Hanover connection. After the popularity of prints produced in the U.S. depicting this tradition, Christmas trees were everywhere shortly after.
Mary Mapes Dodge, the editor of the St. Nicholas Magazine, which solicited some of the best writers of the time to contribute to the body of lore about Christmas. She wrote Hans Brinker and nurtured some of the greatest authors of her age: Mark Twain, Louisa May Alcott, Robert Louis Stevenson, Tennyson, Longfellow, and scores of others. In fact, she convinced Kipling to write some children's stories, the result of which was "The Jungle Book." Many of these authors wrote for the St. Nicholas Magazine, which ran for over thirty years and had a circulation over 70,000 (phenomenal for its time). These two periodicals, The Godey's Lady's Book and St. Nicholas Magazine, were very influential on what we call Christmas today.
Mary Mapes Dodge, editor of the St. Nicholas Magazine
Finally, Katharine Lee Bates, a woman truly ahead of her time, wrote the lyrics for America the Beautiful, which is still sung today. In 1889, this social activist, poet, author, and professor wrote, "Goody Santa Claus on a Sleigh Ride." (She also had a long term, 25-year relationship with her equally brilliant partner, Katharine Coman.) While not well known today, her "Goody Santa Claus" poem has some truly remarkable features.
Katharine Lee Bates, author of "Goody Santa Claus on a Sleigh Ride"
Ms. Claus finally has a name! "Goody," which derives from Good-Wife, was a name of respect for a woman who is brilliant at domestic management.
Mrs. Claus has a voice and opinions. And what will become a trope, she wants to guide the sleigh and deliver presents, which she does.
Goody complains that she does most of the work and Santa gets most of the credit. (Hmm, we've never seen that before.)
Finally, the poem has some really amazing fantasy elements.
She tends a forest where there are trees that grows candy and toys.
She raises the Thanksgiving Turkeys and the Rainbow Chickens, which give the Easter bunny his colorful eggs.
She reminds Santa of how they fled the Fairy Realm together on their wedding day.
She is truly concerned that EVERYONE gets a present, even the poorest of the poor, starving poets, and orphans.
She can darn a sock with an icicle needle and thread made of moonlight, and she gives gifts like a paint box filled the colors of autumn.
And yes, she can control the reindeer and go down a chimney (although her bonnet does get a bit sooty).
Here's the link to the poem itself: https://en.wikisource.org/wiki/Goody_Santa_Claus_on_a_Sleigh_Ride
Is it any surprise that in an era when women had to tread carefully, Mrs. Claus became an advocate for human rights, a suffragist, and a promoter of child welfare and domesticity? And true to form, the women in the Christmas Performing field today, whether off stage or on, have helped grow it into the art form and industry it is. For that, we owe not only thanks, but active and real support. Speaking of which, if you get a chance, check out Santa Nana's Holiday University, the first roving school with an emphasis on Female Christmas Performers!


Hear from Shobana Jeyasingh, choreographer of Contagion, and Professor John Oxford, leader in the field of vaccine and anti-viral clinical trials, to find out more about the Spanish Flu and its influence on the choreography and audiovisual experience in Contagion.
You can watch the performance of Contagion at Imperial War Museum North at midday, then we'll walk over together to Ziferblat MediaCityUK for the talk or you can meet us there at 1pm.
Departing from IWMN reception at 12.45pm.
Free (refreshments included). No need to book.


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Diary of a Wimpy Kid: The Long Haul (Book 9) and over 2 million other books are available for Amazon Kindle . Learn more
The Long Haul (Diary of a Wimpy Kid book 9)
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A family road trip is supposed to be a lot of fun . . . unless, of course, you're the Heffleys.
The journey starts off full of promise, then quickly takes several wrong turns. Gas station bathrooms, crazed seagulls, a fender bender, and a runaway pig-not exactly Greg Heffley's idea of a good time. But even the worst road trip can turn into an adventure-and this is one the Heffleys won't soon forget.
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This item:The Long Haul (Diary of a Wimpy Kid book 9) by Jeff Kinney Paperback Rs. 249.00
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Diary of a Wimpy Kid: Hard Luck by Jeff Kinney Paperback Rs. 236.00
Diary of a Wimpy Kid: Old School (Book 10) by Jeff Kinney Paperback Rs. 249.00
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Diary of a Wimpy Kid: Hard Luck
Double Down (Diary of a Wimpy Kid Book 11)
Diary of a Wimpy Kid: Old School (Book 10)
Diary of a Wimpy Kid: The Getaway (book 12)
Diary of a Wimpy Kid - 6: Cabin Fever
Diary of a Wimpy Kid: The Ugly Truth
Jeff Kinney is a #1 New York Times bestselling author and a five-time Nickelodeon Kids' Choice Award winner for Favorite Book. Jeff has been named one of Time magazine's 100 Most Influential People in the World. He is also the creator of Poptropica, which was named one of Time magazine's 50 Best Websites. He spent his childhood in the Washington, D.C., area and moved to New England in 1995. Jeff lives with his wife and two sons in Massachusetts, where they own a bookstore, An Unlikely Story.
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Reading level: 16.00+ years
Publisher: Puffin; 1, 2015 edition (4 June 2015)
Amazon Bestsellers Rank: #2,578 in Books (See Top 100 in Books)
#116 in Classic Fiction (Books)
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Diary of a Wimpy Kid - 7: The Third Wheel
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Surya narayanan
5.0 out of 5 stars About the LONG HAUL book.
Format: PaperbackVerified Purchase
This book was so funny and miserable. And I think the HEFFLEYS had the most miserable haul or journey in the world . In this book the HEFFLEYS went for a long journey which totally floped, just because Greg's mom followed the instruction in the weekly family magazine . In the middle I was a bit when Greg's parents supported Manny (Greg's younger brother.). In this book a new family member joins with the HEFFLEYS. 'SO READ THE BOOK TO FIND IT'.And by the way the book was so good . I loved it .
Anita Bist
5.0 out of 5 stars Great fan of wimpy kid😂😁
Awesome book ..Most hilarious ..Great trip which turned out to be somewhat of disaster for gerg ..Love it 😂😁👍👌😃 one should buy it
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5.0 out of 5 stars Good Choice
Again the book was for my kids and they really loved it. A perfect companion for holidays and leisure.
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5.0 out of 5 stars Kids books
My granddaughter was thrilled with this gift of books pack. This gift was her birthday present. She has now a complete set of Wimpy boojs
5.0 out of 5 stars Nice, but not great
Its Just Nice, can't say its up to the mark of the other Wimpy kid books though. The humor wasn't there like the other books. I would recommend you Roderick Rules or Old school.
5.0 out of 5 stars Good Purchase at best price
My kid loves these books and getting it at a good price was an additional advantage. Arrived early too. A good buy
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5.0 out of 5 stars BEST BOOK!
THE FIRST BOOK THAT I READ OF THE WIMPY KID SERIES WAS "THE THIRD WHEEL" BUT AFTER READING IT THERE WAS NO LOOKING BACK AND NOW I HAVE READ ALL THE PARTS OF THE WIMPY KID...
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Wedding Wednesday - Roy F Shackford and Alice Savage (Blog 32)
"SAVAGE-SHACKFORD. Percy's Clerks Unexpectedly Assist at Quiet Wedding.
Roy F Shackford and Miss Alice F Savage were married Monday forenoon at 9:30 o'clock at the residence of the bride's uncle, Benjamin F Savage, High St.
The wedding ceremony was primarily intended only for the eyes and ears of the immediate families but the clerks of the D T Percy & Sons store where
the bride formerly worked heard about the event and of course a delegation was hustled up over the hill to see that proper usage was given to the bride and groom. They arrived before the ceremony was completed, not stopping to knock and immediately as the knot was tied by the Rev George D Stanley of the Beacon St Church did things to the bride and groom, filling the house with confetti and rice. The bride was pretty in a traveling gown of dove colored cloth with a becoming hat.
Mr and Mrs Shackford were taken away in a hack properly decorated. Other friends were at the station when the hack drew up. The hack was driven around the square several times in order that the tie at the train would be short but the friends there made up for all lost time when Mr and Mrs Shackford stepped forth. The car in the vicinity of their seat had been decorated when the train pulled out of the station.
Mrs Shackford is the daughter of James Savage and is a graduate of the Bath High School She has been a popular clerk in the D T Percy & Sons store for several years. Mr Shackford is the son of Mrs J B Shackford of Waterville and has been employed several years as a candy maker for J F Clary. He is a member of the Colonial Club. Both Mr and Mrs Shackford have a host of friends and nothing but best wishes for a happy and prosperous married life follow them on their honeymoon. They will visit Springfield Mass and make a trip to Vermont before returning to Bath. They will reside at 618 High St.
Among the out of town guests at the wedding were Mrs J B Shackford, mother of the groom, and Miss Meverett, Margaret and Ruth Shackford, sisters of the groom, all of Waterville."
Roy F Shackford (1881-1948) was the son of Albert Eugene Shackford and Jennie Bessie Sparks and the grandson of Nathaniel Shackford and Emeline E Lovering.
All posts on this website are a work in progress. We'd love to learn of any corrections or additions to the information shared. Also we'd love it if you'd like the post here or at http://www.facebook.com/shackfordgenealogy) as that helps share the post with others. Thanks!
"SAVAGE-SHACKFORD. Percy's Clerks Unexpectedly Assist at Quiet Wedding. Roy F Shackford and Miss Alice F Savage were married Monday forenoon at 9:30 o'clock at the residence of the bride's uncle, Benjamin F Savage, High St.
Copyright 2018 Joanne Shackford Parkes (sharing a link to this post is appreciated but please do not copy this material and paste it elsewhere)


The passing of poet and civil rights activist Maya Angelou has triggered a flood of articles highlighting her most famous quotes. The quotes are moving and inspiring, but there's one in particular that can radically improve the way you do business if you put it into action.
I think about Angelou's perceptive observation nearly every time I interview leaders for this column who have turned businesses into customer service champions. In fact, some have even quoted Angelou to make their point. Brands that excel in service focus on making people feel good about the relationship with the product, service, or employees.
For example, I've written several articles on AT&T's renewed focus on making its stores the customer service leader in its category. It now has two J.D. Power customer service awards to show for it. AT&T conducted focus group research to develop its "10 feet or 10 seconds" method of greeting a customer. One focus group was greeted within 10 feet or 10 seconds of entering the store. The second group was not greeted nor told how long they would have to wait for service. Each group waited exactly three minutes to be served, and not a second more. Controlling for all other factors, AT&T consistently found that the first group had a significantly better perception of the brand because they "felt" recognized and acknowledged.
According to Virgin Group founder Richard Branson, "Customers shouldn't think of your business as a place to buy a product or use a service. It should be a fun place to be!" Branson is a master of making his employees feel good and, when employees feel as though work is a "fun place to be," they spread their enthusiasm to customers. Branson is constantly thinking about how people—employees and customers—should feel about the brand. When I interviewed Branson for this story, I realized that public praise plays a major role in how he motivates employees. "Praise people and people flourish; criticize and they shrivel up," Branson once said.
Let's turn to Howard Schultz, the CEO of Starbucks. Schultz' vision for Starbucks wasn't about the coffee as much as it was about the experience—the feeling—that Schultz wanted people to have when they walked in. Schultz had never planned to build a store that just sold coffee beans. Schultz traveled to Italy and had "an epiphany," a feeling he couldn't shake. Pay attention to the words Schultz uses in a recent interview with Oprah Winfrey about how he felt in an Italian cafe: "I was out of my mind. I walked in and saw a symphony of activity and the romance and the theater of coffee, coffee at the center of conversation and the sense of community. That's what spoke to me." Schultz didn't want to bring the coffee back from Italy, but the feeling of the experience.
When I first interviewed Howard Schultz, I was the one who first brought up the word 'coffee.' Schultz doesn't sell coffee; he sells an experience. He's focused on how people feel when they enter a store. Everything in a Starbucks store— design, smells, sounds—is created to evoke a feeling of community and conversation.
When former Apple Store executive, George Blankenship, built out the first retail experiences for Tesla Motors, he told me his mission was not to "sell cars," but to put a smile on people's faces. I looked back at this Forbes.com article I wrote two years ago about the Tesla dealerships and customer service. Blankenship said, "We're not selling you anything. We want you to feel differently when you leave the store." When people learn something new in a relaxed setting where they are made to 'feel' better, they have a much stronger connection and more pleasurable connection to the brand.
Blankenship received the best training in customer service from his previous boss, Steve Jobs. The Apple Store grew into the most profitable retailer in America because Jobs and his team had decided in 2001 to reimagine the entire retail experience. They started by asking the question, "How do we want customers to feel when they walk into the store?" By focusing on "feelings" before profits, the Apple Store went on to become America's most profitable retailer. Apple, Tesla, Starbucks, Virgin and many other great customer service brands have learned the lesson in Maya Angelou's quote—people will never forget how you made them feel.
Carmine Gallo is the communication coach for the world's most admired brands, a popular keynote speaker, and author of Talk Like TED and The Apple Experience; Secrets To Building Insanely Great Customer Loyalty.


April 5th 2018 meeting – Fruit trees and getting your seeds started.
The membership meeting in April will have two speakers.
Sylvain Alie, our chair, will talk about getting our seeds started and will answer your seedling related questions. On his farm. Stella Raven, he and his wife Royann start 100's of seedlings every year and have surely learnt the do's and don'ts the hard way.
Rod Heitzmann from Creekside Commons has agreed to do a presentation on growing heritage apple trees in the Comox Valley.
He has planted and cared for the apple trees at Creekside for the last 10 years. He will answer questions not only about apple trees but blueberries etc.
The meeting will begin at 7.00 and will be followed by some snacks from Sonja, a bit of Eduardo's chili left over from Seedy Saturday and some of Linda's freshly made cornbread.
All are welcome. Members pay nothing and anyone else is by donation.


We make every effort to schedule an appointment at a time that is convenient for you.
As a courtesy to others who may require our services, we ask that you provide 24 hours notice when canceling an appointment.
You do not need a physician referral to be seen by our physicians.
Often it is helpful for family members or caregivers to come in with patients who are very debilitated or have significant memory impairment.
Please work closely with the staff regarding the medications you are taking as well as any allergies or adverse reactions you have with medications. We are happy to provide a list of your medications from your electronic chart.


My cat, whose name is Two, looks so handsome in this photo, I just couldn't crop him out. Plus, we're nicely coordinated today, don't you think?
Over at theproject333.com, Courtney has issued a challenge: Using your capsule wardrobe, wear and share 33 different outfits for 33 days. It began on October 1st, so I'm a little late in writing about it, but I am doing it! It's surprisingly easy to create a lot of different outfits from a few items of clothing. I actually made a little chart so I can keep track of my outfits and try to avoid repeats. So far on this blog, I have shared 33 unique outfits, and I will keep coming up with new combinations through the end of Courtney's challenge - and hopefully for the full 91 days of the fall season. I think I can do it.
What about you? Would you try a capsule wardrobe just for 33 days? It could be fun, and interesting, and help you make your closet more streamlined and relevant (what do you want to wear right now, this season?). You don't even have to get rid of anything - just pack up the extra stuff, or designate a section of your closet for your capsule wardrobe and move everything else aside. But you might end up getting rid of some clothes that you don't wear or don't like. Why not jump in this weekend? You can start any time!


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Daily Dawg Chow: Browns news (9/12/17)
By Jon Stinchcomb@JonDBN Sep 12, 2017, 6:30am EDT
Share All sharing options for: Daily Dawg Chow: Browns news (9/12/17)
Cleveland Browns:
"Kenny Britt's starting job in jeopardy" (Plain Dealer) - "The drop came at a crucial point in the game, with the Browns trailing 21-10 and Derrick Kindred just having picked off Ben Roethliberger to breathe new life into the Browns."
"Garrett Vows Not To Return Too Soon From High Ankle Sprain" (92.3) - "Garrett remains in a walking boot on his right leg still waiting for his opportunity to show the NFL why he was the top pick in the draft."
"Schobert making his mark in Year 2" (OBR) - "Long before Tank Carder went down with a season-ending knee injury, Joe Schobert was closing in on the starting middle linebacker position."
"Browns face another tough test next in Ravens" (MJ) - "Flacco was crushed on a hit up high by Bengals defensive end Carlos Dunlap. He was evaluated for a concussion and was allowed to continue."
"Injuries: Colts rule Andrew Luck out for Week 2" (NFL.com) - "Rapoport reported Monday morning that Orlando Scandrick broke his hand in Sunday night's dominant win over the division-rival Giants and will have surgery."
"NFL moving quickly to reverse halt on Elliott's 6-game ban" (AP) - "The NFL moved quickly Monday in hopes of reversing a federal judge's decision that has blocked the league's six-game suspension..."
"Rams sign Johnny Hekker to two-year extension, $10M guaranteed" (ESPN) - "Four more years was apparently not enough for Johnny Hekker, quite possibly the game's best punter."
"Patriots replacing new turf at Gillette Stadium after embarrassing loss to Chiefs" (CBS) - "ESPN's Mike Reiss reported that the Patriots are replacing their turf at Gillette Stadium even though it was installed in May..."


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package org.apache.hadoop.hbase.filter;

import java.io.IOException;
import java.util.ArrayList;
import java.util.Objects;
import org.apache.hadoop.hbase.Cell;
import org.apache.hadoop.hbase.CellUtil;
import org.apache.hadoop.hbase.CompareOperator;
import org.apache.hadoop.hbase.PrivateCellUtil;
import org.apache.hadoop.hbase.exceptions.DeserializationException;
import org.apache.hadoop.hbase.util.Bytes;
import org.apache.yetus.audience.InterfaceAudience;

import org.apache.hbase.thirdparty.com.google.common.base.Preconditions;
import org.apache.hbase.thirdparty.com.google.protobuf.InvalidProtocolBufferException;
import org.apache.hbase.thirdparty.com.google.protobuf.UnsafeByteOperations;

import org.apache.hadoop.hbase.shaded.protobuf.ProtobufUtil;
import org.apache.hadoop.hbase.shaded.protobuf.generated.FilterProtos;
import org.apache.hadoop.hbase.shaded.protobuf.generated.HBaseProtos;

/**
 * Different from {@link SingleColumnValueFilter} which returns an entire row when specified
 * condition is matched, {@link ColumnValueFilter} return the matched cell only.
 *

 * This filter is used to filter cells based on column and value. It takes a
 * {@link org.apache.hadoop.hbase.CompareOperator} operator (<, <=, =, !=, >, >=), and and a
 * {@link ByteArrayComparable} comparator.
 */
@InterfaceAudience.Public
public class ColumnValueFilter extends FilterBase {
  private final byte[] family;
  private final byte[] qualifier;
  private final CompareOperator op;
  private final ByteArrayComparable comparator;

  // This flag is used to speed up seeking cells when matched column is found, such that following
  // columns in the same row can be skipped faster by NEXT_ROW instead of NEXT_COL.
  private boolean columnFound = false;

  public ColumnValueFilter(final byte[] family, final byte[] qualifier, final CompareOperator op,
    final byte[] value) {
    this(family, qualifier, op, new BinaryComparator(value));
  }

  public ColumnValueFilter(final byte[] family, final byte[] qualifier, final CompareOperator op,
    final ByteArrayComparable comparator) {
    this.family = Preconditions.checkNotNull(family, "family should not be null.");
    this.qualifier = qualifier == null ? new byte[0] : qualifier;
    this.op = Preconditions.checkNotNull(op, "CompareOperator should not be null");
    this.comparator = Preconditions.checkNotNull(comparator, "Comparator should not be null");
  }

  /**
   * n
   */
  public CompareOperator getCompareOperator() {
    return op;
  }

  /** Returns the comparator */
  public ByteArrayComparable getComparator() {
    return comparator;
  }

  /** Returns the column family */
  public byte[] getFamily() {
    return family;
  }

  /** Returns the qualifier */
  public byte[] getQualifier() {
    return qualifier;
  }

  @Override
  public void reset() throws IOException {
    columnFound = false;
  }

  @Override
  public boolean filterRowKey(Cell cell) throws IOException {
    return false;
  }

  @Override
  public ReturnCode filterCell(Cell c) throws IOException {
    // 1. Check column match
    if (!CellUtil.matchingColumn(c, this.family, this.qualifier)) {
      return columnFound ? ReturnCode.NEXT_ROW : ReturnCode.NEXT_COL;
    }
    // Column found
    columnFound = true;
    // 2. Check value match:
    // True means filter out, just skip this cell, else include it.
    return compareValue(getCompareOperator(), getComparator(), c)
      ? ReturnCode.SKIP
      : ReturnCode.INCLUDE;
  }

  /**
   * This method is used to determine a cell should be included or filtered out.
   * @param op         one of operators {@link CompareOperator}
   * @param comparator comparator used to compare cells.
   * @param cell       cell to be compared.
   * @return true means cell should be filtered out, included otherwise.
   */
  private boolean compareValue(final CompareOperator op, final ByteArrayComparable comparator,
    final Cell cell) {
    if (op == CompareOperator.NO_OP) {
      return true;
    }
    int compareResult = PrivateCellUtil.compareValue(cell, comparator);
    return CompareFilter.compare(op, compareResult);
  }

  /**
   * Creating this filter by reflection, it is used by {@link ParseFilter},
   * @param filterArguments arguments for creating a ColumnValueFilter
   * @return a ColumnValueFilter
   */
  public static Filter createFilterFromArguments(ArrayList<byte[]> filterArguments) {
    Preconditions.checkArgument(filterArguments.size() == 4, "Expect 4 arguments: %s",
      filterArguments.size());
    byte[] family = ParseFilter.removeQuotesFromByteArray(filterArguments.get(0));
    byte[] qualifier = ParseFilter.removeQuotesFromByteArray(filterArguments.get(1));
    CompareOperator operator = ParseFilter.createCompareOperator(filterArguments.get(2));
    ByteArrayComparable comparator =
      ParseFilter.createComparator(ParseFilter.removeQuotesFromByteArray(filterArguments.get(3)));

    if (comparator instanceof RegexStringComparator || comparator instanceof SubstringComparator) {
      if (operator != CompareOperator.EQUAL && operator != CompareOperator.NOT_EQUAL) {
        throw new IllegalArgumentException("A regexstring comparator and substring comparator "
          + "can only be used with EQUAL and NOT_EQUAL");
      }
    }

    return new ColumnValueFilter(family, qualifier, operator, comparator);
  }

  /** Returns A pb instance to represent this instance. */
  FilterProtos.ColumnValueFilter convert() {
    FilterProtos.ColumnValueFilter.Builder builder = FilterProtos.ColumnValueFilter.newBuilder();

    builder.setFamily(UnsafeByteOperations.unsafeWrap(this.family));
    builder.setQualifier(UnsafeByteOperations.unsafeWrap(this.qualifier));
    builder.setCompareOp(HBaseProtos.CompareType.valueOf(this.op.name()));
    builder.setComparator(ProtobufUtil.toComparator(this.comparator));

    return builder.build();
  }

  /**
   * Parse a serialized representation of {@link ColumnValueFilter}
   * @param pbBytes A pb serialized {@link ColumnValueFilter} instance
   * @return An instance of {@link ColumnValueFilter} made from bytes
   * @throws DeserializationException if an error occurred
   * @see #toByteArray
   */
  public static ColumnValueFilter parseFrom(final byte[] pbBytes) throws DeserializationException {
    FilterProtos.ColumnValueFilter proto;
    try {
      proto = FilterProtos.ColumnValueFilter.parseFrom(pbBytes);
    } catch (InvalidProtocolBufferException e) {
      throw new DeserializationException(e);
    }

    final CompareOperator compareOp = CompareOperator.valueOf(proto.getCompareOp().name());
    final ByteArrayComparable comparator;
    try {
      comparator = ProtobufUtil.toComparator(proto.getComparator());
    } catch (IOException ioe) {
      throw new DeserializationException(ioe);
    }

    return new ColumnValueFilter(proto.getFamily().toByteArray(),
      proto.getQualifier().toByteArray(), compareOp, comparator);
  }

  @Override
  public byte[] toByteArray() throws IOException {
    return convert().toByteArray();
  }

  /**
   * Returns true if and only if the fields of the filter that are serialized are equal to the
   * corresponding fields in other. Used for testing.
   */
  @Override
  boolean areSerializedFieldsEqual(Filter o) {
    if (o == this) {
      return true;
    } else if (!(o instanceof ColumnValueFilter)) {
      return false;
    }
    ColumnValueFilter other = (ColumnValueFilter) o;
    return Bytes.equals(this.getFamily(), other.getFamily())
      && Bytes.equals(this.getQualifier(), other.getQualifier())
      && this.getCompareOperator().equals(other.getCompareOperator())
      && this.getComparator().areSerializedFieldsEqual(other.getComparator());
  }

  @Override
  public boolean isFamilyEssential(byte[] name) throws IOException {
    return Bytes.equals(name, this.family);
  }

  @Override
  public String toString() {
    return String.format("%s (%s, %s, %s, %s)", getClass().getSimpleName(),
      Bytes.toStringBinary(this.family), Bytes.toStringBinary(this.qualifier), this.op.name(),
      Bytes.toStringBinary(this.comparator.getValue()));
  }

  @Override
  public boolean equals(Object obj) {
    return obj instanceof Filter && areSerializedFieldsEqual((Filter) obj);
  }

  @Override
  public int hashCode() {
    return Objects.hash(Bytes.hashCode(getFamily()), Bytes.hashCode(getQualifier()),
      getCompareOperator(), getComparator());
  }
}

redpajama_set_name: RedPajamaGithub


The Iowa Department of Natural Resources (DNR) manages fish and wildlife programs, ensures the health of Iowa's forests and prairies, and provides recreational opportunities in Iowa's state parks. Just as importantly, the DNR carries out state and federal laws that protect air, land and water through technical assistance, permitting and compliance programs. The DNR also encourages the enjoyment and stewardship of natural resources among Iowans through outreach and education.
See how Iowa is working to improve public health and the environment.
Learn about programs from Iowa related to streamlining and improving the way they operate and administer their environmental programs.


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DY11 Postcode district consists of 1028 postcode units (also known as Inward codes). Currently there 794 active inward codes in DY11 postal district.
As per 2011 Census data from Office for National Statistics, DY11 Postcode district has a population of 30311 spread across 13054 households.


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The 8310 walkie pallet jack is a durable workhorse designed to load and unload trailers with ease in heavy-duty applications. With ergonomic controls, sturdy forks and durable construction throughout, your operators will move pallets with ease. Customize with extreme environment and cold storage packages.
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text:
Willbros Wins Final Dismissal
Willbros Group, Inc. said in an SEC filing that the FCPA charges against it were formally dismissed this month.
After the three-year deferred prosecution agreement and monitorship expired on March 30, the DOJ asked the federal court in Houston to dismiss the criminal charges.… Continue Reading
The Fugitive Report 2010
Frerik Pluimers, the only FCPA fugitive with his own wanted poster.About a year ago, we compiled our original list of fugitives — people facing FCPA-related criminal charges but still at large.… Continue Reading
Tillery's 'Extraction'
A report this week from Nigeria said FCPA fugitive James "Ken" Tillery has been seized by the FBI in Lagos and is being held by American authorities. But another report on Wednesday said the Nigerian high court had halted the extradition at least until the end of the month because due process wasn't followed.… Continue Reading
Prison For Ex-Willbros Execs
FCPA violations: The Justice Department is targeting individuals who pay bribes to foreign officials. Photo by Ken MayerTwo former Willbros managers on Thursday were given jail time for conspiracy to violate the Foreign Corrupt Practices Act.… Continue Reading
Novak Pleads Guilty
A former consultant for a subsidiary of Houston-based Willbros Group Inc. pleaded guilty on November 12 to paying $6 million in bribes to officials who worked in the Nigerian government, in government-owned companies, and in a political party there.… Continue Reading
The FCPA's Most Wanted
People charged with a Foreign Corrupt Practices Act-related offense either cop a plea or fight the case in court. Except for those who choose the third option. They run. If they're living outside the U.S.… Continue Reading
On The Subject Of Resources
We've mentioned before Dan Newcomb's FCPA Digest, calling it the most definitive publicly-available catalog of FCPA prosecutions, enforcement actions and disclosed investigations. So it's great to see the release of the March 2009 version, available here.… Continue Reading
Two More Ex-Willbros Workers Charged
The Justice Department's aggressive enforcement of the Foreign Corrupt Practices Act against individuals continues. On Friday, a former executive and an ex-consultant of Willbros International Inc., a subsidiary of Houston-based Willbros Group Inc.,… Continue Reading


The announcement of the European Union's General Data Protection Regulation has meant that companies of all sizes should be starting to think about their data privacy and data protection obligations. The new rules will provide a uniform framework for companies that hold and manage customer data. However, while the rules that are being put in place should help every organization to act as if they are on a level playing field, the challenge will be making sure that this approach makes it through to the real world.
This real world environment is increasingly becoming "mobile first" as people work outside the office across more devices. Rather than being tied to the "beige boxes" that traditionally powered enterprises, people have much more flexibility in how they make use of IT assets. This freedom does have its drawbacks, though. Increasingly, IT teams are being cut out of procurement decisions as line of business departments buy their own kit and Cloud services; users can also enable themselves to run their applications on their own devices as well.
This problem has hit the music and other content industries as downloading MP3s moved from being the province of those with technical knowledge and awareness of where to search for files through to being something that anyone could do using paid-for and legal services. Now, the growth of streaming services has meant that there is even less of a footprint for data on devices.
What does this have to do with Enterprise IT and data privacy? Well, it illustrates something originally termed the "Smart Cow Problem" - it only takes one smart user to unlock the gate and everyone else will follow. Just as physical media was replaced by downloads, so enterprise IT users can now make and consume their own data sets using their choice of applications without being aware of the impact.
The risk here is that there is a distinct lack of safeguards around the data. While users are smart, they may not know or care enough about the necessary encryption and data protection steps that are being put in place by IT for the needs of the business. The likelihood of these users recognizing that their activities could breach data privacy requirements are even less.
The response from IT here also has to mirror the latter days of the music industry, rather than the beginning. Rather than trying to lock down services and preventing users from working in ways that suit them, the approach has to be based on making the user experience seamless and smarter. In music, the rise of iTunes for legal music purchases led the way, while new streaming services that make huge catalogues of songs available on-demand have started to grow rapidly. Meeting a user need in a smarter way led to greater potential revenues for music and content businesses where people were happy to pay.
In the same way, data privacy and control can be put back in place through smarter use of automation, so that the user experience is better compared to any workarounds that individuals might put in place. This proactive approach to data protection, privacy and compliance can ensure that both central IT and end-users benefit.
For example, tracking the use of personally identifiable information (PII) should be a key part of ensuring that customer data is protected and secure. However, any time a new file is created, that PII could be re-used and added to. Couple this with files being created and stored on mobile devices without oversight by IT, and this could lead to a breach in customer data protection rules.
Instead, tracking the creation of new files and automatically scanning them for PII can help ensure that the IT team knows what is being created. These files can then be automatically added to data protection processes so that they are copied and sent back to the central IT repository, whether this is on the company's own IT infrastructure or on a secure public Cloud instance. By tracking the creation of new PII records by employees in the background, and then ensuring that the right security and data protection processes are in place, IT can ensure that the company is meeting its compliance requirements in a proactive manner.
At the same time, this user experience is far better than one that either locks down IT services to only run on central IT devices, or relies on manual intervention to remain compliant. This approach ensures that employees can carry on working in flexible ways while also keeping data secure and protected.
Now, there are more in-depth considerations around how people create data to consider. For example, companies with operations in multiple countries will have to track the creation of data on mobile endpoints in different ways to ensure that data protection regulations are met.
As an example, employees in Germany will have to be treated very differently to those in the UK or outside the EU. For German employees, any personal data on a laptop or phone that an employee creates on their device should be left alone, while company data and files that use PII on behalf of the organization can and should be protected.
This level of data privacy means that there is a fine line to be considered on how data from these mobile devices is protected. Understanding these local nuances and requirements is important to ensure compliance with privacy regulations, both for the protection of customer data and for the privacy of employees as well.
For IT teams, the coming of EU GDPR is both a challenge and an opportunity. The challenge comes as more data is being created outside the control of IT – as much as 40 per cent of company data can live outside the network. However, the need for compliance can drive a rethink around the role of data protection within the business too. This opportunity can help IT design and deliver services that fit with the needs of employees as well as meeting the privacy requirements. By thinking "mobile first" IT can get ahead of the privacy problem, rather than reacting to problems caused by smarter users.
Jaspreet Singh , CEO, Druva is an accomplished entrepreneur. Prior to founding Druva, Jaspreet was a member of the storage foundation group at Veritas. He also held a number of engineering specific roles at Ensim Corporation.


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

Stellar systems that are both young and nearby are of importance for a range of present-day scientific topics, not least for the purpose of direct imaging of exoplanets \citep[e.g.][]{marois2008,macintosh2015,chauvin2017} and disks \citep[e.g.][]{schneider2009,thalmann2013,boccaletti2015}. This has led to an increased interest in young moving groups (YMGs), which are associations of stars that are unbound but clustered in phase space, and thus are expected to have originated from a mutual birth cluster \citep[e.g.][]{torres2008}. One such group that is particularly close, and thus particularly useful for many purposes, is the AB Dor Moving Group (ABMG) \citep[e.g.][]{zuckerman2004}. While ABMG is clearly older than 5--20~Myr, which is the approximate age of the youngest YMGs such as the TW Hya or $\beta$~Pic associations \citep[e.g.][]{bell2015}, its specific age has remained uncertain, with different studies suggesting age ranges from a lower limit of 30~Myr \citep{close2005} all the way to an upper limit of 200~Myr \citep{bell2015}.

The defining member of the ABMG, AB~Dor itself, is a complex and intriguing system. The primary AB Dor A is a K-type star, which has long been known to share a common proper motion with the M-type secondary AB Dor B \citep{rossiter1955} at a separation of $\sim$10$^{\prime \prime}$. However, more recently it has been discovered that A and B can each be resolved into tight stellar pairs. AB Dor C is a $\sim$90$M_{\rm jup}$ star near the hydrogen burning limit in a 11.75-year orbit around AB Dor A \citep{guirado1997,close2005,azulay2017b}. AB Dor B is in fact a nearly equal-mass stellar pair \citep{janson2007} designated as AB Dor Ba and Bb. The Ba/Bb pair has been the subject of particular attention in several studies, due to its particular properties. Both stars are M5--M6 type stars, which means that unlike earlier-type stars, they still reside in the pre-main sequence (PMS) phase at the age of the ABMG. Furthermore, orbital monitoring of the system \citep[e.g.][hereafter W14 and A15, respectively]{wolter2014,azulay2015} has shown that the orbital period is only $\sim$1 year, which benefits the determination of precise stellar masses and ages. \citet{azulay2015} estimate masses of 0.28$\pm$0.05~$M_{\rm sun}$ and 0.25$\pm$0.05~$M_{\rm sun}$ for the Ba and Bb components, respectively. This implies a total mass 23\% lower than the 0.69~$M_{\rm sun}$ derived by W14, although the two estimates are consistent within the errors. Given that the observations of both previous studies largely cluster around the apoapsis of the orbit where the binary spends most of its time, these parameters can be further constrained by targeting previously unobserved orbital phases. The A15 study is based on radio interferometry using a quasar as phase reference, and could therefore also produce an absolute parallax of 66.4$\pm$0.5~mas, corresponding to a distance of 15.06$\pm$0.11~pc. This is consistent within the errors with the Hipparcos parallax for AB Dor A of 66.92$\pm$0.54~mas \citep{perryman1997} and marginally consistent with the Gaia DR2 parallax of AB Dor B of 67.03$\pm$0.09~mas \citep{brown2018}, which has a better formal precision. However, here we adopt the A15 parallax for AB for Ba/Bb because the Gaia measurement may conceivably be affected by the Ba/Bb orbit (and likewise, the AB Dor A component could be affected by the A/C orbit).

 M dwarfs remain for a long time in the pre-main sequence phase, and  dynamical masses allow for direct comparison between observational data and isochronal models, which make M-dwarf binaries in YMGs an important sample for astrophysical calibrations \citep{janson2017}. In this context, AB Dor Ba and Bb are of particularly high priority, given their short orbital period, which makes them promising for calibrating theoretical models of young stars, as well as for potentially constraining the age of the system if well matching isochrones are found. This could in turn have implications for the entire ABMG. Independent of any model uncertainties, dynamic and photometric/spectroscopic data of the binary can also be used to define an empirical isochrone, which through comparison with other binaries in ABMG or other YMGs can provide precise information about the relative ages of different YMGs, or the age spread within individual YMGs. Thus, we have performed a dedicated study of the astrometry for this system with the goal of further constraining the orbital properties by adding data over a larger orbital phase coverage and with higher precision than has been previously available with near-infrared imaging. Here, we present the results of this study.

The article is organized as follows. In section \ref{s:obs}, we outline the observations and reduction of the data included in this study. This data is used for astrometric extraction, which is described in Sect. \ref{s:astro}, and which in turn is used for orbit fitting to constrain the AB Dor Ba/Bb orbital parameters, as discussed in Sect. \ref{s:orbit}. Since the main aim of the study is isochronal analysis in mass-luminosity space, we also need to derive bolometric luminosities, which is the topic of Sect. \ref{s:lbol}. The isochronal analysis itself is  described in Sect. \ref{s:iso}, where we relate our result to other results of YMG binaries in the literature in order to build a framework for empirical isochrones in mass versus luminosity. Finally, the results are summarized in Sect. \ref{s:summary}.

\section{Observations and data reduction}
\label{s:obs}

This study considers both archival and newly acquired data for the purpose of constraining the AB Dor Ba/Bb orbit. The archival data includes NACO\footnote{NAOS-CONICA \citep{lenzen2003,rousset2003}.} images from various programmes compiled by W14, and VLBI radio interferometric data presented in A15. Our new data includes Sparse Aperture Masking (SAM) observations with NACO, offering a higher angular resolution than archival NACO images, and a sequence of images from the ZIMPOL\footnote{Zurich Imaging Polarimeter \citep{thalmann2008}.} arm of the SPHERE \footnote{Spectro-Polarimetric High-contrast Exoplanet Research \citep{beuzit2008}.} instrument. ZIMPOL enables a rather high Strehl ratio (often in excess of 50\%) even for wavelengths as short as R-band, and thus provides unparalleled angular resolution for full aperture imaging.

The ZIMPOL observations are the most recent (from 2016--2017, apart from a test epoch taken during SVT\footnote{Science Verification Time}), and their scheduling was informed by the previously acquired astrometry for the system. Since the period was known to be very close to one year, the ZIMPOL scheduling was spread out over one year, with denser sampling during phases of the orbit that were not previously well covered. At $-65$ deg latitude, AB Dor B is effectively circumpolar, but from approximately late April to mid July, the airmass for AB Dor B as seen from Paranal is too high ($>$1.8) to acquire a sufficient image quality during night time. Thus, the ZIMPOL observations are restricted to a $\sim$9-month window during the year. Since two of the requested observations could not be executed by the observatory within their required time windows, our total coverage was in practice limited to 6 months. Still, the observations cover a significant fraction of the orbital phase that had previously not been probed. All observations are summarized in Table \ref{t:log}. In principle, another NACO epoch from 2008.65 exists, as presented in W14. However, that data point is a special case where only a marginal PSF extension was seen in the NACO image. The fitting performed in W14 for this epoch also provided a flux ratio that was inconsistent with their other values. They therefore concluded that the derived separation of 19 mas should merely be regarded as an upper limit to the separation. Here, we note that 19 mas corresponds to only $\sim$0.3~$\lambda / D$ for the VLT in $K_{\rm s}$ band, so the measurement would be challenging even for a perfectly diffraction-limited PSF. With the imperfect Strehl ratio and stability of the NACO PSF, we estimate that there is a risk that the measured extension could be substantially affected by PSF imperfections. We thus opt to omit the 2008.65 data point in our analysis.

\begin{table}[htb]
\caption{Archival and new observations of AB Dor Ba/Bb}
\label{t:log}
\centering
\begin{tabular}{lll}
\hline
\hline
Date & Facility & Reference \\
\hline
2004-02-03      & NACO   & W14 \\
2005-01-07      & NACO   & W14 \\
2005-11-28      & NACO   & W14 \\
2007-11-11      & VLBI   & A15 \\
2008-11-08      & NACO   & W14 \\
2008-12-19      & NACO   & W14 \\
2009-01-01      & NACO   & W14 \\
2009-02-17      & NACO   & W14 \\
2010-10-25      & VLBI   & A15 \\
2012-11-26      & NACO-SAM       & This paper \\
2012-12-20      & NACO-SAM       & This paper \\
2013-01-28      & NACO-SAM       & This paper \\
2013-08-16      & VLBI   & A15 \\
2014-12-11      & ZIMPOL         & This paper \\
2016-10-08      & ZIMPOL         & This paper \\
2017-01-13      & ZIMPOL         & This paper \\
2017-02-16      & ZIMPOL         & This paper \\
2017-03-06      & ZIMPOL         & This paper \\
\hline
\end{tabular}
\end{table}

All the NACO-SAM observations were obtained with the same setting: the $K_s$ filter, the S27 camera (27 mas pixel scale), and the seven-hole mask \citep{tuthill2010}. Observations of AB Dor Ba/Bb were interspersed with several observations of three different calibrators: HD\,35936, HD\,37364, and HD\,271187. To speed up the process, we used the star-hopping technique where the calibrator is reached by means of a simple offset of the telescope, without re-optimization of the AO system. Each individual exposure is composed of eight individual data cubes of 151 0.3-second frames, dithered over the four quadrants of the detector. Each detector quadrant is sky subtracted using the six data cubes where no source is present.

With the exception of the SVT epoch, all ZIMPOL data were taken with the same observational settings. We used the $N_R$ filter with a central wavelength of 645.9~nm and bandwidth of 56.7~nm since this allows for an efficient distribution of light between the science camera and the wavefront sensor using the dichroic beamsplitter. Twenty-five frames were acquired per epoch, with two readouts per frame and 55 seconds per readout. We also had originally intended  for the SVT run to be executed with the $N_R$ filter, but during execution the $H_{\alpha}$-NB filter was mistakenly used instead, leading to much lower fluxes than intended in the images. However, the data were still of sufficient quality to derive reasonably precise astrometry for this epoch. The SVT observations encompassed five frames with five readouts per frame and 50 seconds per readout. All observations were acquired in service mode, with the constraint that the seeing had to remain below 0.8$^{\prime \prime}$. This was mostly fulfilled, except in the January epoch where the seeing fluctuated considerably during the run.  However, since some of the data were of sufficient quality, this epoch could still be used for precise astrometry. All data were acquired in field stabilized mode.

ZIMPOL pixels have a tentative pixel scale of 3.601$\pm$0.005 mas/pixel \citep{schmid2017}, but only every other row is read out on the sky in each individual frame. In order to acquire an equal and uniform sampling in the $x$ and $y$ directions without interpolations, we simply downsampled to an effective pixel scale of 7.202 mas/pixel in both directions. We performed bias correction on individual rows and in individual image quadrants based on the reference values given in the edges of the frames, and corrected for flat-field effects using a lamp flat. An example ZIMPOL frame is shown in Fig. \ref{f:img}

During the ZIMPOL programme, we also observed GJ~3323 in one epoch to serve as a point spread function (PSF) reference star. However, GJ 3323 was spatially extended in the images, possibly as a result of previously unresolved binarity. As a result, and as originally intended as another approach for this purpose, we instead used archival ZIMPOL PSF reference stars, which are regularly observed as part of the standard ZIMPOL calibration package. We used three $N_R$ `flux standard' images from 29 October 2015, 30 April 2016, and 7 May 2016 for this purpose. The PSF standards were reduced in the same way as for the science data as described above.

\begin{figure*}[htb]
\centering
\includegraphics[width=18cm]{f1.eps}
\caption{Series of images of the AB Dor Ba/Bb system from ZIMPOL taken from Oct 2016 to Mar 2017. While the two stellar components were only partially resolvable with previous generations of AO systems, the high Strehl ratio and high spatial resolution of ZIMPOL allows  the components to be clearly resolved.}
\label{f:img}
\end{figure*}

\section{Astrometric extraction}
\label{s:astro}

The astrometric extraction from the SAM data is performed using the closure phases of the interferometric pattern. Complex visibilities are retrieved using the SAMP pipeline \citep{lacour2011}: bad pixels are flagged, the sky is subtracted, frames are centred, and the fringe pattern is fitted using a theoretical diffraction pattern of the seven-hole mask. The 21 complex visibilities of AB Dor Ba/Bb are then calibrated using the 21 complex visibilities of the calibrators. Calibrators are cross-calibrated to check that they are indeed single stars. Finally, the astrometric fit is done after computation of the closure phase using a two-component (binary) model. Errors are normalized to achieve a residual chi-square of one. True north correction and pixel scale were calculated in the same way as in \citet{chauvin2012} on the calibration target $\theta_1$~Ori~C, which was observed on 28 January 2013, yielding a pixel scale of 27.03$\pm$0.18 mas/pixel and a true north correction of 0.43$\pm$0.30 deg.

For  the ZIMPOL data, we used an iterative PSF fitting scheme to account for the partially overlapping PSFs of the AB Dor Ba and Bb components. This is the same procedure as previously developed for the AstraLux M-dwarf multiplicity survey \citep{janson2012,janson2014a}. In brief, a rough initial estimation is made for the locations and brightnesses of the two stars. A model system is then built using two copies of a PSF reference star. The positions and brightnesses of the two components are then iteratively varied until a minimum residual solution (relative to the target image) is found. For AB Dor Ba/Bb, we run this procedure for all individual readouts for each epoch in order to check the scatter among individual images. Furthermore, the procedure is run with each of the three different PSF references in order to evaluate the error resulting from PSF matching imperfections. Due to the relative faintness of AB Dor B at visible wavelengths (R$\sim$11 mag), the adaptive optics correction is sometimes unstable, so in order to sort out low-quality frames, we only perform fits to those frames in which the brightness within a 10-pixel radius aperture from the photocentre of the binary exceeds 50\% of the corresponding value in the brightest frame.

A PSF that is affected by the atmosphere is effectively a superposition of two components: A diffraction-limited core, and a seeing-limited halo. Diffraction is independent of ambient conditions while seeing is not, so the shape of the halo will vary much more strongly with time than the shape of the core. Thus, to benefit the matching of a PSF reference star to a target PSF, it is often useful to filter out the halo with high-pass filtering (e.g. unsharp masking) so that the fit is made almost exclusively on the core component. Thus, unsharp masking using a broad Gaussian kernel is a standard procedure for Lucky Imaging data \citep[e.g.][]{bergfors2010}. For ZIMPOL, the Strehl ratio is rather high, such that a large fraction of the light is already concentrated into the core, making the benefit from usage of unsharp masking less immediately obvious. Thus, we performed a test with two identical fitting procedures for all stars, with the exception that one underwent unsharp masking using a Gaussian kernel of full width at half maximum (FWHM) of 15 pixels, while the other did not. The results were fully consistent within the error bars with no signs of any systematic differences. However, the unsharp masking data had slightly smaller errors (as expected), hence we used them for the analysis in the following.

The PSF fitting procedure outputs differential coordinates $\delta x$ and $\delta y$, and the differential brightness $\delta m$ between AB Dor Ba and AB Dor Bb, with uncertainties represented by the standard errors from frame-to-frame scatter and PSF-to-PSF reference scatter added in quadrature. These results are in pixels, so to convert into sky coordinates we apply two times the tentative pixel scale of 3.601$\pm$0.005 mas/pixel (since our data are rebinned by a factor of 2), and the true north correction of -2.0$\pm$0.5 deg \citep{schmid2017}. We note that the true north correction here refers to the angle of the vertical axis relative to north; for example, an angle of  90 deg relative to the vertical axis corresponds to an angle of 88 deg relative to north. The derived astrometric quantities are summarized in Table \ref{t:astro}. We show them along with the literature data in Fig. \ref{f:astro}. The various classes of data are broadly consistent, although some interesting trends can be seen, for example  the projected separation in the literature NACO data appear to have a larger average projected separation than the NACO-SAM data, which in turn seem to have a larger average separation than the ZIMPOL data. This is probably due to systematic effects in the astrometric calibration, although we also discuss alternative interpretations in Sect. \ref{s:nonkeplerian}.

\begin{figure*}[htb]
\sidecaption
\includegraphics[width=12cm]{f2.eps}
\caption{Astrometric data of AB Dor Bb relative to AB Dor Ba, collected with ZIMPOL (brown) and NACO-SAM (red), along with literature data from W14 (green) and A15 (blue), labeled with the epochs of each observation. The black circle indicates the fixed location of AB Dor Ba.}
\label{f:astro}
\end{figure*}

\begin{table}[htb]
\caption{Astrometric results.}
\label{t:astro}
\centering
\begin{tabular}{llll}
\hline
\hline
Date & Sep. (mas) & PA (deg) & Instrument \\
\hline
2012-11-26      & 64$\pm$2 & 248.8$\pm$1.0 & NACO-SAM \\
2012-12-20      & 62$\pm$2 & 242.8$\pm$1.0 & NACO-SAM \\
2013-01-28      & 55$\pm$2 & 231.8$\pm$1.0 & NACO-SAM \\
2014-12-11      & 58.0$\pm$0.6 & 242.86$\pm$0.69 & ZIMPOL \\
2016-10-08      & 62.3$\pm$0.6 & 256.02$\pm$0.51 & ZIMPOL \\
2017-01-13      & 49.9$\pm$0.7 & 228.69$\pm$0.97 & ZIMPOL \\
2017-02-16      & 42.5$\pm$1.1 & 213.81$\pm$0.88 & ZIMPOL \\
2017-03-06      & 37.9$\pm$1.6 & 202.53$\pm$0.82 & ZIMPOL \\
\hline
\end{tabular}
\end{table}

\section{Orbital constraints}
\label{s:orbit}

We  performed orbital fitting to the relative Ba/Bb astrometry for the ZIMPOL and NACO-SAM data in combination with the literature data using on one hand the procedure developed and described in \citet{kohler2008,kohler2012} based on the Levenberg-Marquardt algorithm \citep{press1992}, and on the other hand a routine described in \citet{chauvin2012} based on a Markov chain Monte Carlo (MCMC) Bayesian analysis technique \citep{ford2005,ford2006}. The two routines give consistent best-fit values, but the errors are larger in the MCMC fit. We consider the MCMC procedure more conservative in this regard since it accounts for a wide range of correlations among the parameters, and use its output for all the  analyses in the following.

The resulting fit is shown in Fig. \ref{f:orbit}, the posteriors on the orbital parameters and their mutual correlations are shown in Fig. \ref{f:posteriors}, and the best-fit parameters are listed in Table \ref{t:stdorbit}. Most of the parameters are consistent with those reported in A15 within the mutual error bars but with considerably smaller errors in our fit, as expected considering the new and precise astrometric data points provided in Sect. \ref{s:astro}. The semi-major axis is also consistent with that in A15; however, in this case, the error is  larger in our fit. The reason for this is most likely our use of MCMC for the fitting, which is more robust to parameter correlations than the Levenberg-Marquardt algorithm used in A15. Another reason may be that A15 use the 2008.65 NACO data point from W14 in their analysis, which we omit as discussed in Sect. \ref{s:obs}. The larger error in semi-major axis also leads  to a larger error in mass than in A15. Our derived mass is consistent with both W14 and A15 within error bars. The total system mass is derived as 0.66$\pm$0.12~$M_{\rm sun}$.

\begin{figure*}[htb]
\sidecaption
\includegraphics[width=12cm]{f3.eps}
\caption{Resulting orbit of AB Dor Ba/Bb from our orbital fitting.}
\label{f:orbit}
\end{figure*}

\begin{figure*}[htb]
\centering
\includegraphics[width=16cm]{f4.eps}
\caption{Posterior distributions of our fitted parameters, along with their mutual correlations.}
\label{f:posteriors}
\end{figure*}

Thanks to the long baseline relative to the orbit and the precise measurements, the period can now be constrained to significantly better precision than 1 day, and has a fractional error of $\sim$0.1\%. Of the three components that play a  role in deriving a total system mass (angular semi-major axis $\alpha$, distance $d$, and period $P$), $P$ has the weakest exponent and the smallest fractional error, so it is now  constrained closely enough to have a negligible impact on the system mass uncertainty. Of the two remaining parameters, which in combination yield the physical semi-major $a$, $\alpha$ has a fractional error of $\sim$6\% and the parallax-based distance has 0.7\%. Hence, $\alpha$ is the limiting factor in the mass determination, and any future attempts to further constrain the orbit are best focused on placing tighter constraints on this parameter, particularly by collecting data even closer to periastron.

\begin{table}
\caption{Parameters of the best orbital solution.}
\label{t:stdorbit}
\renewcommand{\arraystretch}{1.3}
\begin{center}
\begin{tabular}{lr@{}l}
\noalign{\vskip1pt\hrule\vskip1pt}
Orbital Element                         & \multicolumn{2}{c}{Value} \\
\noalign{\vskip1pt\hrule\vskip1pt}
Date of periastron $T_0$ (yr)                   & $2003.713$ & $\pm 0.015$\\
                                                & (2003 Aug 16)\span\\
Period $P$ (yr)                         & $0.9856$ & $\pm 0.0009$\\
Period $P$ (d)                          & $359.98$ & $\pm 0.33$\\
Angular semi-major axis $\alpha$ ($^{\prime \prime}$)                       & $0.0571$ & $\pm 0.0034$\\
Semi-major axis $a$ (AU)                        & $0.86$ & $\pm 0.05$\\
Eccentricity $e$                                & $0.669$ & $\pm0.039$\\
Argument of periastron $\omega$ ($^\circ$)      & $68.0$ & $\pm 3.5$\\
P.A. of ascending node $\Omega$ ($^\circ$)      & $96.8$ & $\pm 2.2$\\
Inclination $i$ ($^\circ$)                      & $114.9$ & $\pm 1.9$\\
System mass $M_{\rm S}$ ($M_{\rm sun}$)                   & $0.66$ & $\,^{+0.12}_{-0.12}$\\
\noalign{\vskip1pt\hrule\vskip1pt}
\end{tabular}
\end{center}
\end{table}

\subsection{Non-Keplerian alternatives}
\label{s:nonkeplerian}

In a previous section we noted that there are indications for small but consistent offsets between different data sets, which we interpreted as residual systematic errors. However, it is also relevant to evaluate whether there could be an actual physical effect at play in the observed system to cause these offsets. In particular, the orbit fitting described above assumes that the AB Dor Ba/Bb system consists of two bodies in a closed Keplerian orbit, but if any third body in the system has a sufficiently large gravitational impact on the pair, this assumption breaks down. In this context, it is especially relevant to note that around apastron, the W14 data points (2004--2009) have a larger mean separation than the NACO-SAM points (2012--2013), which in turn have a higher mean separation than the ZIMPOL points (2014--2017). This could in principle be interpreted as continuous orbital evolution over $\sim$1~yr timescales.

To evaluate this scenario, we first turn our attention to the known additional component of the system,   the AB Dor A/C pair, which is dominated in mass by the A component. At a present-day separation of at least 150~AU from AB Dor Ba/Bb, it is clear that AB Dor A cannot impose dynamical changes on a 1~yr timescale. Even at large separations, it can impose Kozai-Lidov \citep{kozai1962,lidov1962} oscillations on the Ba/Bb pair, if it is sufficiently inclined to the Ba/Bb orbital plane. However, the timescale for Kozai-Lidov oscillations is proportional to $P_{A/B}^2 / P_{Ba/Bb}$ \citep[e.g.][]{antognini2015}, where $P_{Ba/Bb}$ is close to 1~yr as determined in our orbital fitting, and $P_{A/B}^2$ is of order $10^6$ yr$^2$ or more at 150~AU projected separation, so it is highly unlikely that it could have any impact on the timescales we are considering here.

Next we consider additional components within the AB Dor Ba/Bb system,   i.e. unresolved companions around either star. Such companions could cause an impact on the observed Ba/Bb orbit either through three-body dynamical interactions, forcing the orbit of the visible components to evolve over time, or through simply shifting the photocentre of its host star during its orbit. The latter can again be excluded on the basis of the timescale. The orbital period of such an unseen companion would have to be much shorter than the 360~d orbit of Ba/Bb, so we would expect its astrometric effects to manifest itself as  scatter on short timescales, such as within the ZIMPOL 2016--2017 arc, rather than a consistent offset between the ZIMPOL and NACO-SAM arcs. The lack of scatter within these arcs may also be a problem for the three-body dynamics hypothesis, although in this case the solution may be fine-tuned by assigning a small mass to the unseen companion such that it has a negligible impact on the photocentre on the component it orbits, but still has close enough encounters with the other component that it inflicts a large dynamical disturbance. However, such a configuration should be extremely short-lived since the less massive perturber should be rapidly ejected from the system, so it is an unlikely scenario for that reason. Taking all these arguments into account, we thus argue that non-Keplerian solutions are very improbable, and that the small remaining offsets seen in the data are instrumental effects rather than any physical mechanism at play in the AB Dor system.

\section{Luminosity constraints}
\label{s:lbol}

By relating the dynamical mass of our stellar components to a quantity that is expected to evolve with time, we can perform an isochronal analysis to either produce a model-dependent age estimate, or conversely, to test the accuracy of the isochronal models with an independent age estimate. The bolometric luminosity $L_{\rm bol}$ is particularly useful in this context. For the purpose of estimating $L_{\rm bol}$, we first acquire unresolved photometry from the literature at a range of wavelengths. The \textit{Gaia} $G$ filter \citep{prusti2016} is used for the visible wavelength range, since it covers a wide band with a small photometric error. For the near-infrared regime we use 2MASS \citep{skrutskie2006} $JHK$ bands, and for the mid-infrared we use the WISE \citep{wright2010} $W1$--$W4$ bands. Furthermore, we measure differential photometry in the $N_R$ and $K$ bands in our data. We then construct a grid of theoretical binaries based on the BT-SETTL models \citep{allard2014}. Each artificial component is given a mass in the range of 0.1--1~$M_{\rm sun}$ and an age in the range of 50--150~Myr, and every possible pairing of components is used to produce a prediction of the total brightness and differential brightness in the bands listed above. If a given artificial pair matches the observations within uncertainties, then the predicted $L_{\rm bol}$ values of the individual components are considered to be part of the set of bolometric luminosities that accurately represent the real values. The mean and scatter of these sets then represent the adopted $L_{\rm bol}$ for the two components. All the photometric values and derived luminosities are summarized in Table \ref{t:mag}. The advantage of this method is that it uses photometric information across a wide range of wavelengths, sampling a large fraction of the stars' total bolometric outputs. In this way, it effectively averages over all different atmospheric and physical properties that could potentially represent the system, making the result quite insensitive to specifics among these effects (e.g. the degree of atmospheric absorption within a given photometric band).

\begin{table}[htb]
\caption{Photometry and luminosity of AB Dor Ba/Bb}
\label{t:mag}
\centering
\begin{tabular}{lll}
\hline
\hline
Quantity &Value & Reference \\
\hline
Combined $G$ (mag)      & 11.159$\pm$0.002       & \textit{Gaia} \\
Combined $J$ (mag)      & 8.171$\pm$0.018        & 2MASS \\
Combined $H$ (mag)      & 7.659$\pm$0.042        & 2MASS \\
Combined $K$ (mag)      & 7.341$\pm$0.031        & 2MASS \\
Combined $W1$ (mag)     & 7.038$\pm$0.191        & WISE \\
Combined $W2$ (mag)     & 6.897$\pm$0.103        & WISE \\
Combined $W3$ (mag)     & 6.852$\pm$0.043        & WISE \\
Combined $W4$ (mag)     & 6.744$\pm$0.094        & WISE \\
$\delta N_R$ (mag)      & 0.33$\pm$0.05  & This paper \\
$\delta K$ (mag)                & 0.24$\pm$0.14  & This paper \\
$\log{L_{\rm bol, Ba} / L_{\rm sun}}$   & -2.02$\pm$0.02         & This paper \\
$\log{L_{\rm bol, Bb} / L_{\rm sun}}$   & -2.11$\pm$0.02         & This paper \\
\hline
\end{tabular}
\end{table}

One of the scientific aims of this study is to compare the results for AB Dor Ba/Bb with other low-mass YMG binaries in the literature;  therefore, we have collected the relevant isochronal quantities for all low-mass components in YMG binaries with good individual dynamical mass constraints that we are aware of. Masses, and in some cases luminosities, come from \citet{close2007} and \citet{azulay2017b} for AB Dor AC; \citet{montet2015} for GJ 3305 AB; \citet{kohler2013} and \citet{kohler2018} for TWA 5 AB; \citet{nielsen2016} for V343 Nor B; \citet{calissendorff2017} for 2MASS J10364483+1521394 BC (hereafter J1036); \citet{azulay2017a} for HD 160934 AC; and \citet{rodet2018} for GJ 2060 AB. For V343 Nor B and J1036 BC, no $L_{\rm bol}$ was available, and for HD160934 AC, the value quoted in \citet{hormuth2007} is based on the distance from the original Hipparcos reduction, which is inconsistent with newer values such as the VLBI parallax in \citet{azulay2017a}; for these cases we calculated an $L_{\rm bol}$ in the same way as described for AB Dor Ba/Bb above, with small variations depending on which unresolved and resolved photometric data points were available for each target.  We find $\log{L_{\rm bol} / L_{\rm sun}}$ of -1.56$\pm$0.07 for V 343 Nor B, -0.97$\pm$0.02 for HD 160934 A, -1.40$\pm$0.03 for HD 160934 C, and -2.49$\pm$0.02 for both J1036 B and C.

\section{Isochronal analysis}
\label{s:iso}

The masses and luminosities of AB Dor Ba and Bb are plotted in Fig. \ref{f:iso}, along with the corresponding measurements from relevant binaries in the literature. Individual masses for the two components are presented in A15, but this predicts a lower total mass than we find in our fitting of the relative orbit. Thus, we show two separate individual masses for each component in Fig. \ref{f:iso}, where one corresponds to the exact masses in A15 and the other  to the same mass ratio as A15 but scaled to account for the difference in total mass. As discussed previously, the total masses are consistent within the errors. Also plotted are the corresponding measurements from relevant binaries in the literature. By now, a sufficiently large sample of these stars is emerging to  start building a framework of empirical isochrones. In general,  stars of a common age are expected to fall approximately along a line in a mass--luminosity diagram, and thus constitute an empirical isochrone. This isochrone could be fit with theoretical isochrones, which can provide an age estimate for the stars based on which isochrone fits the best or, conversely, can be used to calibrate the theoretical isochrones, for example by distinguishing which out of a set of different theories provides the best fit or by identifying parameter ranges in which the models fit comparatively poorly. However, empirical isochrones of different populations of stars can also be useful completely irrespective of theoretical models since it provides a framework for determining model-free relative ages. For example, the isochrones of two kinematically distinct YMGs can be used to evaluate which one is younger, and the scatter around an isochrone within a YMG can provide clues about the degree of age spread within the group. Among the sample we have included in Fig. \ref{f:iso}, TWA 5 is associated with the TW Hya (TWA) YMG with an age of $\sim$5--10~Myr; GJ 3305 and V343 Nor B are associated with the $\beta$ Pic moving group (BPGM) with an age of $\sim$20--30~Myr; AB Dor and GJ 2060 are associated with the AB Dor moving group (ABMG) with an age of $\sim$50--150~Myr; and J1036 has been identified as an UMa moving group (UMaMG) member with an age in the range of 300--500~Myr \citep[e.g.][]{brandt2015,jones2015}. HD 160934 has been identified as an ABMG member \citep{lopez2006}; this classification has varied substantially in the literature \citep[see e.g.][]{azulay2017a} and across different versions of the BANYAN tool \citep[e.g.][]{gagne2014,gagne2018},  and we thus consider it  an unclear case. The M-dwarf pair TWA~22 also has a tight system mass constraint \citep{bonnefoy2009,rodet2018}, but we do not include it in this analysis since the mass ratio is not yet determined.

\begin{figure*}[htb]
\sidecaption
\includegraphics[width=12cm]{f5.eps}
\caption{Isochronal analysis of AB Dor Ba/Bb and other low-mass YMG binaries with known orbits. Brown symbols denote TWA members (TWA 5 AB), red are BPMG members (diamonds: GJ 3305 AB, triangle: V343 Nor B), blue are ABMG members (asterisks: AB Dor system, circles: GJ 2060 AB), and magenta are UMaMG members (J1036 BC; the two stars appear as one point since they have equal derived properties). Black symbols denote unclear YMG membership (HD 160934 AC). For AB Dor Ba/Bb, the original A15 masses are plotted as grey asterisks, while the masses scaled for the total mass derived in this work are plotted in blue. Also plotted are BCAH15 isochrones going from 10 Myr (top) through 30, 50, 100, and 300 Myr (bottom). The last (300 Myr) is already close to the main sequence at these masses, and thus largely indistinguishable from older ages.}
\label{f:iso}
\end{figure*}

Several interesting trends emerge in Fig. \ref{f:iso}. The first thing to note is that there is a general trend that qualitatively agrees very well with the expected behaviour of stars in the PMS phase: the TWA stars are systematically brighter than the BPMG stars at any given mass, and the BPMG stars are in turn brighter than the ABMG stars which are marginally brighter than the UMaMG stars. HD 160934 appears more consistent with a BPMG age than an ABMG. We note that HD 160934 is kinematically distinct from the BPMG, with a 0\% membership probability according to the BANYAN tools, so it is highly unlikely that it is an actual BPMG member. Another clear trend in the figure is that there is considerable consistency within the different pairs of stars; e.g. stars in pairs with similar masses also have similar luminosities. Also plotted in Fig. \ref{f:iso} is an example set of isochrones from ages from 10 Myr to 300 Myr. Above 300 Myr, there is very little further evolution expected since the main sequence is generally reached by then. In Fig. \ref{f:iso}, the BCAH15 \citep{baraffe2015} isochrones are used, but we have tested a broad set of isochrones including PARSEC \citep{bressan2012} and MIST \citep{choi2016}, which all give quite similar results. All TWA and BPMG stars match  the expected theoretical isochrones well for their respective ages, perhaps with the  exception of GJ 3305 B, which appears marginally too old for the BPMG. However, for the older ABMG and UMaMG stars in this analysis, the situation is slightly more complicated. AB Dor C fits to isochrones in the $\sim$50--100 Myr range, which is consistent with the ABMG age. AB Dor A is too massive to provide meaningful constraints, but is also consistent with such an interpretation. On the other hand, GJ 2060 A, GJ 2060 B, AB Dor Ba, AB Dor Bb, J1036 B, and J1036 C all have best-fit values below these tracks, effectively placing most of them even below the expected main sequence. The GJ 2060 pair still appears consistent with $\sim$100~Myr ages in the figure, but we note that the large error bars for those components are primarily caused by the large fractional error in the mass ratio (24\%). The fractional error in total mass is much smaller (9\%), so while it would be possible for either one of the components to be individually consistent with a 100 Myr isochrone, it would not be possible for both components simultaneously. This is shown more clearly in \citet{rodet2018}, where an isochronal analysis is performed for the GJ 2060 pair as a whole.

Many different potential explanations exist for why a data point may deviate from the isochronal expectation, but in this population analysis several of them  appear unlikely. For the case of J1036, an incorrectly estimated distance could cause it to deviate from the theoretical expectation, but this explanation would not work for AB Dor, where component C is consistent with the expectations, while Ba and Bb are not. An incorrect age estimation is another general factor of importance, but it cannot explain the most deviant cases here, since they are below the main sequence and would not fit  an existing theoretical isochrone of any age. A high mass relative to the observed brightness could also in principle be caused by unresolved additional components in the systems. However, for GJ 2060 A, the B component is already clearly impacting the radial velocity of its stellar lines, and any closer companion of similar mass would impose an even greater velocity amplitude except in the case of pathological inclinations, so it would be very difficult to hide additional companions to GJ 2060 A. Furthermore, both the AB Dor Ba/Bb and J1036 BC pairs have internally similar luminosities and masses, so if we hide a companion to one component, we must in principle also hide a similar companion to the other in order to conserve the consistency between the observed components. This seems to be an overly complicated solution. The isochrones assume roughly solar composition, so a significantly different metallicity could cause a deviation from these isochrones, but this is not expected in the solar neighbourhood, and for example does not explain  the case of J1036 BC, where a range of metallicities were tested in the models \citep{calissendorff2017}. One possible explanation is missing physics in the isochronal models, which might impose incorrect slopes or offsets in the isochrones. For example, it is certainly possibly to imagine an ad hoc line in Fig. \ref{f:iso} that would function as a satisfactory isochrone for all of the ABMG members. Another hypothesis, as argued in e.g. \citet{azulay2017a}, is that the high stellar activity for low-mass stars alters the radii and effective temperatures of the components from the theoretical expectations. In this scenario, however, it is somewhat surprising that the deviation from the isochrones is largest among the oldest stars in our sample, even though such stars are statistically the least active.

\section{Summary and conclusions}
\label{s:summary}

We have presented an orbital analysis  of the AB Dor Ba/Bb pair based on several new epochs of astrometry from NACO-SAM and ZIMPOL, which have been added to existing literature astrometry. This allows us to set significantly tighter constraints on all orbital parameters than has previously been possible. Much like several other YMG binaries analysed in the literature, we find that the stars are more massive than  would have been predicted based on their brightnesses from isochronal analysis. We further address this peculiar trend by uniformly plotting all known low-mass YMG binaries with known individual stellar masses in mass--luminosity space. The targets in TWA and BPMG appear to be reasonably internally consistent, and can be matched by sensible theoretical isochrones for their expected ages. For ABMG and older targets, there is a similar internal consistency, but they generally do not match   their theoretical isochrones well.

Using mass and bolometric luminosity as the fundamental parameters for isochronal analysis is a comparatively straightforward and model-free approach, and thus avoids many uncertainties that can otherwise arise, such as uncertainty in the SpT-$T_{\rm eff}$ relation if $T_{\rm eff}$ is used as an observable. The prospects for this kind of analysis is improving rapidly with time, for several reasons. Firstly, \textit{Gaia} will provide precise distances to all M dwarfs in the solar neighbourhood. This will improve error bars in both dynamical mass and bolometric luminosity. Furthermore, the \textit{Gaia} astrometry will improve YMG membership assessments, and probably identify new members suitable for isochronal analysis. In addition, many M-dwarf binaries have now been monitored for well over a decade with high-resolution imaging \citep{janson2014b}, which means that orbital constraints will soon become available even for moderately wide binaries of $\sim$40~yr orbital periods. The fact that many of these young binaries are also significantly radio emitting \citep{azulay2017a} is another factor that brings additional potential since it allows for closer pairs to be resolved with VLBI than is possible at visible/infrared wavelengths and can provide absolute astrometry allowing for mass ratio determinations and independent parallax estimations. Furthermore, VLBI imaging is relatively insensitive to day-night cycles, and could thus potentially reach orbital epochs that are unattainable to visible/infrared imaging during the times of the year when the target is on the dayside of Earth. This is particularly relevant for a case such as AB Dor Ba/Bb, with a period only 5 days shorter than an Earth year, such that certain parts of its orbital phase are hidden from visible light imaging continuously for over a decade.

\begin{acknowledgements}
M.J. gratefully acknowledges funding from the Knut and Alice Wallenberg Foundation. The authors thank J. Guirado and R. Azulay for useful discussion, and the anonymous referee for useful comments. We also thank the ESO staff for their efficient support. This study made use of the CDS services SIMBAD and VizieR, and the SAO/NASA ADS service.
\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


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jacdac
"We'll need to draft a fake set of orders," Wahlman said.
Wahlman had chosen a generic-looking four-door sedan, a black one that closely resembled some of the official government vehicles he'd seen at the research facility, and he'd driven it back down to the Myrtle Beach area and had checked into the same place he'd stayed at previously. He used one of the desktop computers in the lobby to create a fake set of orders for the fake flag officer he was planning to become, knowing that the paperwork wouldn't pass any sort of rigorous inspection process and pretty much betting his life that it wouldn't have to. He bought some dark brown hair dye at a nearby pharmacy and a dark brown mustache at a nearby costume shop, and he bought an audio recording device about the size of a quarter at a nearby electronics.
Source: The Jack Reacher Experiment by Jude Hardin
Context: Wahlman is looking to infiltrate a top security government site.
What does a set of orders refer to? insignia?
Official papers that order him to do certain things or to be in certain places at certain times. For example, Navy orders might tell him to be on board a specific aircraft carrier in the port of San Diego no later than 1000 hours (10 am) on Tuesday, June 18.
RM1(SS)
English - US (Midwest)
Egmont said:
Navy orders might tell him to be on board a specific aircraft carrier in the port of San Diego no later than 1000 hours (10 am) on Tuesday, June 18.
Still laughing about the last set of fake orders we drew up....