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Posted on August 21, 2017	by Ametia
Happy Monday, 3 Chics Family & Friends!
This entry was posted in #BlackGirlMagic, Arts, Human Rights, Institutional Racism, Media, Movies, Open Thread, Politics, prejudice, Racial Bias, Racism and tagged 2017 Sundance Institute Vanguard Award, Ava DuVernay, Dee Rees, Justin Chon. Bookmark the permalink.
Amy Goodman's entire show today (after headlines) was about Dick Gregory. Video at the link…
Dick Gregory In His Own Words: Remembering the Pioneering Comedian and Civil Rights Activist
https://www.democracynow.org/2017/8/21/dick_gregory_in_his_own_words
Research from the @splcenter shows most Confederate statues went up during times of civil rights tension https://t.co/NEzGrx4gAG
— NPR Politics (@nprpolitics) August 21, 2017
Moon trolls sun on Twitter in solar cyber spat https://t.co/pkz1MlGdHu pic.twitter.com/3OWCyHkJD2
— Reuters Top News (@Reuters) August 21, 2017
First time in history Jeff Sessions has cheered something getting blacker. pic.twitter.com/vZOHZEQsE2
— Schooley (@Rschooley) August 21, 2017
*DEAD*
#SolarEclipse2017 edition pic.twitter.com/VSkfHnTs9I
— Jeffrey Guterman (@JeffreyGuterman) August 21, 2017
Early America had school choice. The Founding Fathers rejected it.
They believed public schools were the foundation of a virtuous republic.
By Johann N. Neem
August 20 at 10:29 AM
Education Secretary Betsy DeVos has been a loyal proponent of school choice. In her home state of Michigan, DeVos advocated both public school choice and vouchers to empower parents to send their children to private and religious schools. As secretary, she argues that "parents no longer believe that a one-size-fits-all model of learning meets the needs of every child." They "know other options exist, whether magnet, virtual, charter, home, faith-based or any other combination."
Now President Trump is proposing devoting unprecedented amounts of federal money to expand school choice nationally. Both Trump and DeVos argue that families, not the public, should choose their schools. As DeVos recently proclaimed, "School choice is about recognizing parents' inherent right to choose what is best for their children. That's the manifestation of expanding human liberty in America."
But this conception of public education ignores our collective interests as a society. America's public schools developed because after the Revolution, Americans realized that leaving education to parental whims and pocketbooks created vast inequalities and could not ensure an educated citizenry. A return to this type of system threatens to exacerbate educational inequality, which already plagues modern America and weakens our democracy. The Founding Fathers saw freedom as the cornerstone of the nation and public schools as essential vehicles to secure it. Guided by their vision, we should work to fix America's public schools, not abandon them.
The Revolution transformed how some Americans thought about education. These Americans agreed with Thomas Jefferson that the future of the republic depended on an educated citizenry. They also believed that the opportunities offered by schooling should be available to rich and poor alike. Many state constitutions included clauses like Georgia's in 1777: "Schools shall be erected in each county, and supported at the general expense of the State." But how to execute this directive? The best way, American leaders ultimately concluded, was to encourage local public schools and to limit the growth of academies.
The Brilliance of Buy-in: The Private Market and States Won't Let Obamacare Collapse
Spandan Chakrabarti
When Donald Trump lost the popular vote by the biggest margin of anyone who'd ever won the presidency, his assent to the White House with a unified Republican Congress was seen as doomsday for their primary and first target: the Affordable Care Act. I was worried. Everyone I know was worried. The news of a unified right wing government in Washington was not – and still is not – good news for health care.
But one person who had never had much patience for the dramatics said he thought Obamacare would survive. That man was, in fact, President Obama.
Each time Trump was faced with the failure of Obamacare repeal, he comes back to the old refrain: some version of "Obamacare is collapsing, we'll let it collapse, and then come back and force Democrats to compromise on repeal!"
That Obamacare-is-collapsing argument, backed nearly universally by national Republicans, is dependent on a singular factor: that many health insurers are now refusing to offer any plans at all in the ACA exchanges for many (mostly rural) counties. Setting aside the fact that this is primarily a phenomenon faced by states originally (and in many cases, still) resistant to Obamacare, the entire basis behind that argument has now, well, collapsed.
There is now just one county – with 334 private exchange enrollees – left without an insurer.
You read that right. Not 80 counties, not 50 counties, just one. And even that county might end up being covered by the time open enrollment starts in November.
That's right. Insurers are jumping in to cover previously uncovered counties as state officials spring into action to make it happen for their constituents. As a result, as of now, all but one of the 81 counties that were at risk of losing all ACA private insurance options now have them.
The reason they are doing so is even more detrimental to Republican narrative of a collapsing Obamacare market: it's profitable. The CEO of Centene, the company that signed up more than half of the "bare" counties, had this to say in an investor call: "For 2018, we intend to grow this profitable segment of our business."
Dan PfeifferVerified account
@danpfeiffer
Dan Pfeiffer Retweeted HowardKurtz
We should all prepare now for the punditocracy to gush when Trump reads from a teleprompter without saying anything pro-Nazi
Here is Trump's plan for Afghanistan: a privatized military that makes MORE money for his inner circle. pic.twitter.com/VTm7YJ3e6q #morningjoe
— Girls Really Rule. (@girlsreallyrule) August 21, 2017
MUST WATCH This holocaust survivor's message for neo-nazis and white supremacists in the US. #MorningJoe pic.twitter.com/kI4jMyxGIM
— #LaquanMcDonald (@ifuaskmee) August 21, 2017
yahtzeebutterfly says:
Everyone across America should watch this video.
Farmers' Crops Are Rotting in the Fields Thanks To Trump. (We should make him eat the stuff.) https://t.co/VDf7oDlYwu
— Peggy Stuart (@PeggyStuart) August 21, 2017
Trump has caused such fear in experiencedMexican farm workers that they are not showing up for the harvest.
I think that's what Reagan understood and why he allowed Mexican people who were here without proper papers to receive citizenship.
Thirty-five years ago, during a primary debate between Ronald Reagan and George H.W. Bush, both former presidents spoke with compassion about immigrants living in the United States when they were asked whether the U.S. should allow the children of undocumented immigrants to go to public schools.
"Today, if those people are here, I would reluctantly say I think they would get whatever it is, you know, that society is giving to their neighbors," Bush said at the time, calling immigrants "good people, strong people."
"Because, as we have made illegal some kinds of labor that I'd like to see legal, we're doing two things. We're creating a whole society of really honorable, decent, family-loving people that are in violation of the law and secondly we're exacerbating relations with Mexico," Bush added.
Reagan responded in kind, stating in part, "Rather than talking about putting up a fence, why don't we work out some recognition of our mutual problems?" "Open the borders both ways," he added.
From https://thinkprogress.org/you-will-not-believe-how-reagan-talked-about-immigration-during-the-1980-gop-presidential-debate-c46400a2b47c/
WATCH: Atlanta students get a heartfelt welcome on their first day of school as mentors line up to cheer them on. pic.twitter.com/r4EXrvNpg3
— NBC News (@NBCNews) August 20, 2017
Check your email, ladies
The #SolarEclipse has officially hit the continental U.S. per @AP. We're about 1.5 hours away in #Charleston! #chseclipse #chsnews pic.twitter.com/aisCWlfmlh
— The Post and Courier (@postandcourier) August 21, 2017
First glimpse of #SolarEclipse2017 totality in Oregon! Take a look here and watch our live stream for more: https://t.co/cOKssim1bY pic.twitter.com/g9zEbWFXfk
— NASA (@NASA) August 21, 2017
THIS IS HAPPENING! You are witnessing the corona phase of the #SolarEclipse2017! WATCH LIVE ON TV OR HERE: https://t.co/lKcmbueTi3 pic.twitter.com/4O0KlwgFUv
— ABC13 Houston (@abc13houston) August 21, 2017
#SolarEclipse2017 Totality in Oregon – LIVE on C-SPAN https://t.co/yDCozcEbHp #SolarEclipse #Eclipse pic.twitter.com/0I8dF9iZ4Y
— CSPAN (@cspan) August 21, 2017
GQ story on Dylann Roof. His dad called the story….fake news! Wow!
A Most American Terrorist: The Making of Dylann Roofhttps://t.co/jjqgs23eK0
— 3ChicsPolitico (@3ChicsPolitico) August 21, 2017
This is a really good article. It's long, I had to print it, but definitely a good read.
SUNDAY, AUG 13, 2017 06:30 PM CDT
Want to understand white privilege? Look at college golf teams like mine
It's time we talked about how colleges let affluent white students be supported by African-American student labor
ANYA ALVAREZ
More and more discussion has become centered around what white privilege is. But very little dialogue has taken place around white privilege in college sports and the labor of African-American athletes on the football and basketball teams who make it possible for other sports to exist at universities.
For a good 20 years of my life, I was a competitive golfer. I played on a full athletic scholarship and eventually turned pro, playing a short while on the LPGA and developmental tours.
While it is no secret golf is made up of a majority of white men, I never fully recognized the privilege I had to play on a golf scholarship, and this realization came to me after reading a Facebook post from another white woman who I used to play on tour with: "If college is free for everyone, then it will be equivalent to a high school degree," she lamented.
My first reaction was, "But you went to school for free on an athletic scholarship . . . also, your parents are millionaires."
Then I wondered, "How do golf programs exist at universities?"
In 2011, when Washington's football program went 0-11 for the season, the football program made a profit of close to $15 million. The basketball program, which did very well that year, pocketed around $6 million.
The cost of playing on the women's golf team included my equipment, travel to tournaments, physical therapy and insurance on me. In total, my time at the university cost the school around $424,000.
When I asked how the school could afford to have a golf program, without hesitation she responded, "Well, the football and basketball program, of course."
Knowing this I quickly realized that in essence I was the freeloader that America loathes, the one we hear about so often in elections, one of those who takes advantage of a system set up to make people feel entitled.
In particular, other university sports like tennis, golf, swimming and gymnastics (mostly made up of white athletes) ride off the backs of mostly African-American athletes. According to a study conducted by University of Pennsylvania researcher Shaun R. Harper, black men only make up 2.5 percent of undergraduate students, but comprise 56 percent of college football teams and 61 percent of college basketball teams.
As Trump controversies intensify, Mar-a-Lago faces cancellations
08/21/17 10:40 AM—UPDATED 08/21/17 11:15 AM
In D.C., Donald Trump's response to Charlottesville became so politically toxic, there was a sudden exodus from several White House advisory panels, with private-sector members deciding they no longer wanted to be associated with this president.
But about 1,000 miles to the south, Trump World faced a slightly different kind of problem stemming from the same controversy. The New York Times reported:
With its ornate 20,000-square-foot ballroom and manicured lawns, President Trump's Mar-a-Lago Club in Palm Beach, Fla., is often the site of elaborate fund-raisers, drawing big charities – and big dollars.
But several organizations are having a change of heart since Mr. Trump blamed "both sides" for the violence in Charlottesville, Va., after a white nationalist rally and an attack by a driver that left a woman dead. There were "very fine people on both sides," Mr. Trump said.
Over the weekend, the Preservation Foundation of Palm Beach and the Palm Beach Zoo and Conservation Society became the latest nonprofit groups to cancel galas at Mar-a-Lago.
Exact tallies vary, but I believe that was the 10th cancellation of the 16 big-ticket events scheduled at Mar-a-Lago for the upcoming "social season."
The Secret Service confronts unique challenges in the Trump era
A couple of years ago, the U.S. Secret Service struggled with a series of damaging controversies, including some important security breakdowns, prompting a congressional investigation and a bipartisan report about an "agency in crisis." Among other things, lawmakers identified budget cuts one of the "primary causes" of the agency's difficulties.
And while the Secret Service has tried to turn things around since the release of that report, the agency is now facing another daunting challenge: Donald Trump's presidency.
The relationship between the Secret Service and the Republican president's team has already faced some difficulties. A leading Trump attorney, for example, tried to blame the agency for last year's infamous meeting in Trump Tower with a Kremlin-linked attorney, prompting the Secret Service to make a rare entry into a political debate in order to defend the agents' actions. That was soon followed by a leasing dispute between the agency and the New York building the president still owns.
But USA Today goes a step further this morning, highlighting a different kind of problem.
The Secret Service can no longer pay hundreds of agents it needs to carry out an expanded protective mission – in large part due to the sheer size of President Trump's family and efforts necessary to secure their multiple residences up and down the East Coast.
Secret Service Director Randolph "Tex" Alles, in an interview with USA TODAY, said more than 1,000 agents have already hit the federally mandated caps for salary and overtime allowances that were meant to last the entire year.
The agency has faced a crushing workload since the height of the contentious election season, and it has not relented in the first seven months of the administration. Agents must protect Trump – who has traveled almost every weekend to his properties in Florida, New Jersey and Virginia – and his adult children whose business trips and vacations have taken them across the country and overseas.
The Daily 202: The elites strike back — getting under Trump's skin
By James Hohmann
August 21 at 7:07 AM
Seven months into President Trump's reign, the elites are striking back. From Wall Street to West Palm Beach and West Hollywood, the past week has been a turning point, perhaps even a tipping point. Since Trump abdicated his moral leadership after Charlottesville, the well-connected have used their leverage — like checkbooks and celebrity — to send a message about what truly makes America great.
The growing number of groups canceling galas, stars boycotting ceremonies and chief executives resigning from advisory boards is further isolating Trump.
People in his orbit say the president has been in a sour mood about all of this. He stormed the barricades, but now he's the one under siege. Unlike most of the criticism he's engendered since taking office, the past week has actually impacted his bottom line. The value of the Trump "brand," which he once said is worth billions, has taken a bath since he declared that some "fine people" were protesting alongside the neo-Nazis and white supremacists at the University of Virginia.
— The White House announced on Saturday that neither the president nor first lady Melania Trump will attend the annual Kennedy Center Honors in December. For the first time since the award was created in 1978, they also will not invite the honorees over for a reception beforehand.
That came after three of the five honorees — television producer Norman Lear, singer Lionel Richie and dancer Carmen de Lavallade — said they would or may boycott the traditional reception. "As for the other two, rapper LL Cool J had not said whether he would attend, and Cuban American singer Gloria Estefan said she would go to try to influence the president on immigration issues," per David Nakamura, Amy B Wang and Peter Marks.
As an alpha male, Trump seems to take special satisfaction when people who are richer, cooler and better looking than him kowtow. It seems silly to have to write this, but it's true: Having his ring kissed seems to be one of Trump's favorite parts of the job. But there's not been very much ring-kissing lately.
In 1825, Nat Turner's 2nd vision: "I saw white spirits and black spirits engaged in battle, and the sun was darkenedhttps://t.co/7xO4210fEs
On August 21, 2017, the anniversary of Nat Turner's rebellion, there will be a total solar eclipse.
— Sean Diddy Combs (@diddy) August 19, 2017
#SolarEclipse2017 is streaming live on Twitter from 12-4pm ET. https://t.co/xMfnagg50H
— Women's March (@womensmarch) August 21, 2017
The Long-Term Effects of Trump Will Be Disastrous for the GOP
Trump and the alt right will be a curse on the GOP for decades to come.
by David Atkins
It may be a bit odd, at a time when the Republican Party dominates all branches of the federal government as well as most governor's mansions and state legislatures, to declare it a political party in dire peril. From one perspective, Trump seems to have saved the GOP from the brink of disaster and infused it with new energy. But the danger signs are flashing brightly nonetheless, and the cure may well be worse than the disease.
While it's true that a combination of district-level gerrymandering, voter suppression and newfound white-working-class appeal has helped sustain Republican majorities and launch Donald Trump into the White House despite a popular vote loss, the demographic tide remains squarely set against the GOP. And even though minority voters did shift slightly to Trump from Romney per exit polling, people of color have nonetheless been shifting sharply away from the GOP over the last two decades. Millennials, too, despite a similar slight shift to Trump from Romney in 2016, remain the most progressive generation in American politics. Even conservative young people are more liberal on a host of issues than their parents.
These trends have forced Republicans to become much more aggressive in their gerrymandering and suppression efforts to retain statehouses and congressional seats. They have also been the chief reason that Republican presidential candidates have failed to earn a popular vote majority in 6 of the last 7 presidential elections. Only the anti-majoritarian Electoral College has saved the GOP from near annihilation in White House contests over the last 30 years.
These trends are still working aggressively against the Republican Party. Even if Republicans manage to maintain the white working class voters who switched from Obama to Trump in the last election cycle—and that's a big if given Trump's precipitous decline in the polls and the large boost Democrats have received against their baseline numbers in recent special elections—it won't be enough to save Republicans from the slow-rising tsunami of the emerging Democratic majority.
The day the sun disappears is here.
Read: https://t.co/JwV2ZUx97r
Watch: https://t.co/pEm9iUW8i8#SolarEclipse2017 pic.twitter.com/ZsqiuxKsbr
— CNN (@CNN) August 21, 2017
Prepare Yourself For Talk of Another Trump Pivot
There has always been a sort of manic/depressive quality to Trump's presidency. I'm not suggesting that the president should be diagnosed with bipolar disorder. That would require a more up-close examination of his daily routines. But we've witnessed periods where he seems to go off the deep end emotionally, only to be followed by times when his behavior is actually described as "presidential."
Last week brought us one of those cycles as it unfolded over a couple of days. Trump's immediate response to the events in Charlottesville was to suggest that in altercations between white supremacists and counter-protesters, there were "many sides" to blame. Then his handlers got hold of things and scripted a speech in which he condemned racism, only to be followed the next day by unscripted remarks at a press conference where he reverted to his original statement.
Yesterday we learned that Trump will give a speech tonight in which he is expected to lay out a plan for this administration's strategy in Afghanistan. Based on what we've seen from this president over the last few months, we can expect that to be a very well scripted affair and the media will respond by doing a logical analysis of what he has to say. While it grows increasingly difficult to buy into the charade, there might even be some who will suggest that his remarks were "presidential." If so, you'll be able to hear a sigh of relief in their voices that signals the hope that all of this ugliness we've witnessed over the past week is finally behind us. I'm sure that is exactly what Chief of Staff John Kelly and his other handlers had in mind when they decided to schedule this speech tonight.
After that, the president is off to Phoenix for a campaign-style speech in which it is very possible that he will announce a pardon for convicted Sheriff Joe Arpaio—a hero to white nationalists. His staff will have their hands full in trying to keep him on script at this kind of event. As we watched throughout the 2016 election, Trump tends to feed off the crowd, which will be stacked with his most loyal supporters.
Dear Lord today, #SolarEclipse2017 pic.twitter.com/FLypSwS8Fm
— ruh-mel (@itsRamel) August 21, 2017
Jared Kushner's firm seeks arrest of Maryland tenants to collect debt
Doug Donovan
The real estate company owned by Jared Kushner, son-in-law and top adviser to President Donald Trump, has been the most aggressive in Maryland in using a controversial debt-collection tactic: getting judges to order the arrest of people who owe his company money.
Since 2013, the first full year in which the Kushner Cos. operated in Maryland, corporate entities affiliated with the firm's 17 apartment complexes in the state have sought the civil arrest of 105 former tenants for failing to appear in court to face allegations of unpaid debt, The Baltimore Sun has found.
That's more than any other landlord in the state over that time, an analysis of Maryland District Court data shows. Court records show that 20 former Kushner tenants have been detained.
Industry professionals say such arrests, called body attachments, can be the only way to get tenants to pay the money they owe. Kushner Cos. officials say the New York-based firm employs the tactic as a last resort, and follows industry standards and state law.
It's amazing to see references to today's eclipse alongside news reports about WWI troop movements. https://t.co/SokSqaDHkd pic.twitter.com/1KqnIOz3Yq
— Philip Bump (@pbump) August 21, 2017
In 1932, the Times wrote about today's eclipse (alongside a dog who won an award). https://t.co/SokSqaDHkd pic.twitter.com/ZmJGxPfLg7
Get them outta there!
PHOTOS: Confederate statues removed from University of Texas at Austin campus in dead of night https://t.co/pJD1grEaAE #UTAustin pic.twitter.com/C4ZOuZqn1C
— Austin Statesman (@statesman) August 21, 2017
University of Texas Removes Four Confederate Statues Overnight https://t.co/r2O2YsabeO
— deray mckesson (@deray) August 21, 2017
The #Confederate statues have been removed from the University of Texas at Austin campus
More: https://t.co/oEkLklYT9h #UTAustin #Texas pic.twitter.com/EOqESuLZnE
— ANTONIO ARELLANO (@AntonioArellano) August 21, 2017
TAKE ALL THEM BITCHES DOWN
Nat Turner's rebellion started on this day 186 years ago. He began planning in February of that year when he saw a solar eclipse.
— Vann R. Newkirk II (@fivefifths) August 21, 2017
"The roots of American Christian nationalism—including flavors that insist on white supremacy—stretch back decades" https://t.co/IKy4u7IUZH
— Judd Legum (@JuddLegum) August 21, 2017
As others flee, Trump's top evangelical ally comes to his defense
After Donald Trump publicly defended racist activists, to the delight of prominent white supremacists, the White House hoped the president's Republican allies would rally to his defense. That clearly didn't happen.
Last week, bookers and producers for a variety of news programs – including colleagues of mine at MSNBC – reached out to dozens of GOP officials about appearing on camera to defend Trump's comments, and Republicans simply weren't interested. That continued yesterday: in an exceedingly rare sight, there were no elected GOP officials on any of the Sunday shows.
In an interesting twist, when ABC News' "This Week" asked the White House for a spokesperson willing to appear as a guest, officials directed the show's producers to, of all people, Jerry Falwell Jr., the president of Liberty University and a member of the White House's Evangelical Advisory Board. Falwell was one of the few people to defend Trump last week, and he did so again yesterday with ABC's Martha Raddatz.
RADDATZ: [Trump] said, there were "very fine people" on both sides. Do you believe there were very fine people on both sides?
FALLWELL: He has inside information that I don't have. I don't know if there were historical purists there who were trying to preserve some statues. I don't know. But he had information I didn't have. And I believe that he spoke what was…
RADDATZ: What made you think he knew that…
FALLWELL: I think he saw videos of who was there. I think he was talking about what he had seen, information that he had that I don't have.
White Supremacist Leader Loses Job As Electrician After Being ID'd At Virginia Rally – https://t.co/GZDPSwCiqG
— zellie (@zellieimani) August 21, 2017
Are you ready for #Eclipse2017? Our live coverage starts at 11, followed by @ABC's The Great American Eclipse news special at noon. #ABC13 pic.twitter.com/5q0or0DQla
GOP base comfortable with Trump's racially inflammatory posture
More than a few political observers, hopeful that American politics was still driven by decency and principle, saw last week as a deal-breaker of sorts for Donald Trump. The amateur president could spend months testing the limits of the fabric that holds the country together, the argument went, but he couldn't expect to get away with offering a tacit defense of white supremacists.
And yet, here we are. The Washington Post reported yesterday:
A GOP strategist working campaigns in red and purple states said that while support for Trump generally declined slightly since Charlottesville, support rose among his base, after a decline last month because of the failure on health care and revelations about the Russia investigation. This strategist said many Trump supporters applaud the president's continuing desire to shake up Washington, favor his economic priorities and admire his willingness to speak his mind.
So, yes, Trump praised the "very fine people" among the racist activists in Charlottesville, and faced an immediate backlash, but to assume that much of the Republican base was troubled by any of this is to lose sight of what made Trump appealing to those voters in the first place.
When the president fought to take away their health care benefits, the GOP base minded, When he fought with the media and blamed "both sides" for racist violence, these voters liked what they saw.
There's no accounting for these people. They are lost. All we can do is stop them for destroying the country and the future.
Sen. Claire McCaskill spends August recess trekking through Republican strongholds in rural Missouri https://t.co/jVwTOnSsru pic.twitter.com/hlH0lmMYzX
— CBS News (@CBSNews) August 21, 2017
The Power of Privilege: Why Charlottesville Has Succeeded Where Charleston Failed
Trevor LaFauci August 21, 2017
Few remember the name Clementa Pinckney.
Even the most progressive among us may not recall who this person was or what they did. We can add the title of State Senator to his name and most people will still draw a blank. We can even add the title of Reverend, which may have a couple additional people recognize the name, but most still won't be able to recall this person. It is not until we add the geographic location of Charleston, South Carolina that people begin to remember the name. Reverend Clementa Pinckney was, in fact, the person eulogized by President Obama after the murder of nine African-American churchgoers by White supremacist Dylan Roof in Charleston in June of 2015.
Despite the moving eulogy by our then president, the needless deaths of Reverend Pinckney and eight others did very little to affect public policy in this country. Yes, the Confederate flag was removed from the South Carolina statehouse. However, gun laws in this country remained unchanged. Many AME churches had to hire additional security for their church services and Bible study groups. Hate groups ups like the ones Roof idolized not only faced zero repercussions for their influence but actually were able to prosper in the wake of the Charleston shooting. Roof himself was not only kept alive after committing mass murder but was kindly provided lunch by local law enforcement. Even with the public outcry at the time, the murder of Reverend Clementa Pinckney and eight other members of the Emanuel African Methodist Episcopal Church proved to move the needle very little in terms of addressing the problem of White supremacy in this country.
Now, compare what happened in Charleston to what happened in Charlottesville these past ten days.
In short, public policy has dramatically shifted more in ten days after Charlottesville than in two years after Charleston.
Why has there now been a wide-scale effort to take down Confederate monuments and statues? Why have business leaders and artists now chosen to spoke out? Why are web-hosting sites now all of a sudden concerned about providing Nazis with a platform? Why are people in Boston and throughout the country now feeling compelled to leave their homes, take to the streets, and let it be known that we are not a nation that supports Nazis?
The answer to all these questions is, quite simply, White privilege.
Charlottesville did what Charleston could not because the events in that city directly affected White people. This wasn't simply something that happened in an historically African-American church in a deep-red state. This was a something that happened an affluent, middle-class community with a prominent public university in a purple state that has been trending blue in recent elections. In other words, it was something that could have happened anywhere. People choose to live in and around Charlottesville because they feel safe. Ten days ago, an army of torch-wielding, violent Nazis entered their town, weapons in hand. When on Saturday, three people died including activist Heather Heyer, the community felt threatened as if their own very lives were at stake. For those in the community who grew up in privilege, it was the first time in their lives they had felt this way and for them it was terrifying.
TRUTH! Those NAZI MOFOs rolled up into their towns and killed and plowed down a white woman.
Exclusive: Secret Service depletes funds to pay agents because of Trump's frequent travel, large family
Kevin Johnson, USA TODAY Published 5:00 a.m. ET Aug. 21, 2017
WASHINGTON — The Secret Service can no longer pay hundreds of agents it needs to carry out an expanded protective mission – in large part due to the sheer size of President Trump's family and efforts necessary to secure their multiple residences up and down the East Coast.
If it's time for Republicans to find courage & stand up to Trump, give us a sign! Like blot out the sun.
🌒
— Rep. Eric Swalwell (@RepSwalwell) August 20, 2017
In response to my question about the USS John S. McCain collision @POTUS at @WhiteHouse South Portico replies "that's too bad." pic.twitter.com/G6CK0E8y8Y
— Steve Herman (@W7VOA) August 21, 2017
BREAKING: U.S. Navy says 10 sailors are missing, five injured after USS John S. McCain collided with merchant ship.
— The Associated Press (@AP) August 21, 2017
Virginia is renaming Jefferson Davis Highway and asking the internet for suggestions https://t.co/sKcYODGvSt pic.twitter.com/LGJwJ82VmK
— Jalopnik (@Jalopnik) August 20, 2017
Dear @ArlingtonVA,
Respectfully, I recommend the highway be named after John Punch, America's First Slave. https://t.co/wi3VNhSJC0
— Bobfr (@Our4thEstate) August 21, 2017
There is nothing more American than voting. Don't let anyone take that away from us pic.twitter.com/oCCCIpymPf #TW #VotingRights4All
— Action2getherNetwork (@Action2getherUS) August 21, 2017
398 years ago today, the first enslaved Africans arrived in Jamestown, VA. Today, we mourn their suffering, and that of all slaves.
— Rep. Terri A. Sewell (@RepTerriSewell) August 20, 2017
Prayers being sent out to SG2'S daughter and grandson. May they both heal and get stronger every day 👶🙌💓🏥🚼😇
Sending WAVES of love to SG2, and her family.
Good morning! Thank you all for your prayers and love. Karson will be moving to level 2, he's breathing on his own. God is so good. Thank you Lord, for answered prayers.
how much does he weigh, SG2?
He's breathing on his own!!! That is such good news.
I'm excited.
I don't know how much he weighs right now but at birth he was 3.8 lbs. But he's moving to level 2. Whoo Hoo! Thank you, God! Last night the kids faced timed me while they were in NICU and I said Hi Karson, Hi sweet baby and he was trying so hard to open his eyes and finally opened them big for a few seconds. He heard my voice.
So good to learn that he is breathing on his own!
Good Morning, Everyone 😐😐😐


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How to solve this error ?

redpajama_set_name: RedPajamaStackExchange


text:
\section{Introduction} \label{introduction}

Over the last decades, rapid advances in technology and the resulting increasing number of large-scale digital sky surveys have helped to propel astronomy into a new data-rich era \citep{djorgovski13}. This development necessitated the invention of novel ways to deal with the amount of incoming data produced by the petabyte-scale sky surveys, and algorithmic advances in the automated handling of massive and complex data sets have become of great importance.

The field of variable star research is no exception and has greatly benefited from the increasing amount of available photometric time-series data, which are often made available in real time. The number of known variable stars has increased by several magnitudes over the last decade alone, with recent variable star catalogues containing hundreds of thousands of entries (e.g. \citealt{heinze18,ZTFvars}) and the International Variable Star Index (VSX; \citealt{VSX}) of the American Association of Variable Star Observers (AAVSO), the most coherent and up-to-date database of variable stars, cataloging more than 2,100,000 objects at the time of this writing (June 2021). Automated classification routines are of essential importance to sort the vast number of newly discovered variable stars into astrophysically meaningful classes. However, with the development of new and improved algorithms and classification networks, new (meta)classes are constantly developed, and it is not easy to keep track with this steadily growing body of nomenclature.

In agreement with the general trend, an increasingly large number of photometrically variable chemically peculiar (CP) stars have been identified during the past decades \citep[e.g.][]{paunzen98,wraight12,bernhard15b,bernhard15a,huemmerich16,bowman18,huemmerich18,david_uraz19,sikora19}. CP stars are upper main-sequence objects, which are generally found between spectral types early B to early F and characterised by peculiar surface abundances. The observed peculiarities are thought to have their origin in the interplay between radiative levitation and gravitational settling (atomic diffusion) in the calm outer layers of slowly rotating stars (e.g. \citealt{michaud70,richer00}). Several types of CP stars exist, such as the metallic-line or Am/CP1 stars, the magnetic Ap/CP2 stars, the HgMn/CP3 stars, and the He-peculiar stars, which are composed of the CP4/He-weak stars and the He-rich stars \citep{preston74}. Relevant to the present investigation are the CP2 and the He-pec stars, which generally exhibit strong and globally organised magnetic fields and atmospheres selectively enriched in elements such as Si, Cr, Sr, or Eu. These objects are frequently grouped together under the term of magnetic chemically peculiar (mCP) stars, which, for convenience, we will adhere to in the present study.

Magnetic CP stars usually present a non-uniform surface distribution of chemical elements (chemical spots or belts). Flux is redistributed in these structures via line and continuum blanketing (e.g. \citealt{lanz96,shulyak10}), which results in strictly periodic light and spectral variations with the rotation period. After their bright prototype, photometrically variable mCP stars are also referred to as $\alpha^{2}$ Canum Venaticorum (ACV) variables. Observed amplitudes of the photometric variability are generally of the order of several hundredth of a magnitude in the optical region, occasionally reaching up to about 0.2\,mag ($V$). In the 'zoo' of variable stars, ACV variables constitute a rather obscure class and, in automated classification systems, are often combined with other rotational variables under generic types, such as 'ROT' (i.e. spotted stars not classified into a particular class), or get largely ignored.

Here we show that the 'upside-down CBH variables'\footnote{For convenience, in the text, these objects are hereafter referred to as ud-CBH variables.}, identified through the analysis of data from the Asteroid Terrestrial-impact Last Alert System (ATLAS) and proposed by \citet{heinze18} in the ATLAS variable star Data Release One (ATLAS DR1) catalogue as a potentially new class of variable stars, are, at least to a high percentage, made up of ACV variables with distinct double-wave light curves. Using suitable selection criteria, we identified 264 candidate ACV variables in the ATLAS DR1 catalogue. 62 of these stars could be confirmed as mCP stars (53 new discoveries) using spectra from the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) and were classified on the MK system.

Data sources, motivation and the process of target selection are detailed in Section~\ref{datasources}. Spectral classifications are described and presented in Section \ref{spectral_classification}. The magnitude, period and space distributions of our sample stars are investigated in Section~\ref{space_distribution}, while Section \ref{parameters} explores the ages and masses of our sample stars. We conclude in Section~\ref{conclusions}.

\section{Data sources, motivation and target selection} \label{datasources}

\subsection{The Asteroid Terrestrial-impact Last Alert System (ATLAS)}

The Asteroid Terrestrial-impact Last Alert System (ATLAS) is a NASA-funded sky survey developed by the University of Hawaii with the main aim of discovering potentially hazardous near-Earth asteroids (NEAs). It currently consists of two telescopes, which are situated on Haleakala and Mauna Loa and equipped with f/2.0 0.5-m DFM custom Wright Schmidt telescopes and STA-1600 10.5x10.5k CCD detectors. The telescopes command a field of view with a diameter of 7\fdg4, and observations are procured through two broadband filters: the cyan filter ('$c$'; 420$-$650\,nm), which is employed during the two weeks surrounding the new Moon, and the orange filter ('$o$'; 560$-$820\,nm), which is used in lunar bright time. Both filters are linked via colour transformations to the Pan-STARRS $g$, $r$, and $i$ bands. More information on the ATLAS sky survey is found in \citet{tonry18}.

\subsection{The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST)} \label{LAMOST}

The LAMOST telescope \citep{lamost1,lamost2}, also called the Guo Shou Jing\footnote{Guo Shou Jing (1231$-$1316) was a Chinese astronomer, hydraulic engineer, mathematician, and politician of the Yuan Dynasty.} Telescope, is a reflecting Schmidt telescope located at the Xinglong Observatory in Beijing, China. It boasts an effective aperture of 3.6$-$4.9\,m and a field of view of 5$\degr$. Thanks to its unique design, LAMOST is able to take 4000 spectra in a single exposure with spectral resolution R\,$\sim$\,1800, limiting magnitude r\,$\sim$\,19\,mag and wavelength coverage from 3700\,\AA\ to 9000\,\AA. LAMOST is therefore particularly suited to survey large portions of the sky and is dedicated to a spectral survey of the entire available northern sky. LAMOST data products are released to the public in consecutive data releases and can be accessed via the LAMOST spectral archive.\footnote{\url{http://www.lamost.org}} With about 10 million stellar spectra contained in data release (DR) 6, the LAMOST archive constitutes a real treasure trove for researchers. The present study uses spectra from LAMOST DR4 \citep{DR4}.

\subsection{ATLAS variable star Data Release One (ATLAS DR1) and the 'upside-down CBH variables'}

Using data from the first two years of operation of the Haleakala telescope (observations up to the end of June 2017), \citet{heinze18} published the ATLAS DR1 catalogue. Analysing observations for approximately 142 million stars between declinations of about $-$30$^{\circ}$\,$\le$\,$\delta$\,$\le$\,+60$^{\circ}$ in the magnitude range of about 11\,<\,$r$\,<\,19, they produced a major catalogue containing $\sim$430,000 confirmed variable stars (among which are $\sim$300,000 new discoveries) and 4.7 million candidate variable stars. The observations consisted of four to six 30-s exposures of each field per night; the provided data sets boast a median time span of about 620\,d, the median number of observations is $N$\,=\,208 \citep{heinze18}. Subsequent data releases are planned, which are expected to greatly enhance the number of identified variables and available measurements.

\begin{figure}
	\includegraphics[width=\columnwidth,bb=0 0 500 400]{LC_overview.pdf}
    \caption{Phase plots of (from top to bottom) the 'upside-down CBH variables' ATO J074.9570+40.2063 and ATO J084.9321+37.2119, based on ATLAS data, and the known ACV variables HD 77314 and HD 26792, based on MASCARA data. The amplitude of the light variations appears reduced in the filterless MASCARA data.}
    \label{fig:LC_overview}
\end{figure}

\citet{heinze18} calculated an extensive set of 169 variability features for each object, 70 of which were employed as input for sorting the stars into broad, astrophysically meaningful variability classes based on light curve morphology, such as CBF = 'Close binary, full period'; CBH = 'Close binary, half period'; MIRA = 'High-amplitude, long-period red variable'; PULSE = 'Pulsating variable' etc. A complete overview of the variability classes is provided in Table 2 of \citet{heinze18}.

In the context of the present study, the class of CBH = 'Close binary, half period' is of importance, which consists of close eclipsing binaries for which a period equal to half the true orbital period was selected by the employed period search algorithm. In analogy to this group of objects, and in want of a better expression, \citet{heinze18} coined the term ud-CBH variables to refer to a particular set of light curves that look almost exactly like the inverted light curves of CBH stars -- that is, instead of the minima (eclipses) in the light curves of CBH binaries, they show narrow symmetrical maxima (cf. Figure \ref{fig:LC_overview}, upper panels). About 70 such objects were manually identified, most of which were sorted into the PULSE class by the classification algorithm. However, the authors note that many more can probably be found in the final catalogue.

\citet{heinze18} briefly consider the astrophysical nature of the ud-CBH variables, which occupy a well-defined region in period-amplitude space (amplitudes of up to 0.2\,mag, period distribution peaks around 2\,d; cf. Figure 23 of \citealt{heinze18}). In particular, they rule out contact binaries (GCVS-type EW; \citealt{GCVS}) and binary stars with strong reflection effects (GCVS-type R) on the grounds of light curve morphology and argue against 'ordinary' rotating variables with classical starspots and binary systems with an accreting compact object because of the consistency of the observed light curves. In summary, the authors were unable to properly classify these stars and present them as a potentially new type of (pulsating?) variables, whose astrophysical nature is unclear.

\subsection{Motivation and target selection} \label{motivation_and_target_section}

The present study was conceived after we noticed the strong similarity of the light curves of the ud-CBH variables illustrated in \citealt{heinze18} (their Figure 23) to the light curves of a certain subset of ACV variables. Unlike stars with classical starspots, these spotted rotators show simple and remarkably consistent light curves that remain stable in shape and amplitude over decades and more \citep[e.g.][]{huemmerich18}. As has been expanded upon in Section \ref{introduction}, the light variations of ACV variables are due to the presence of chemical spots. They generally show simple light curves that can be well described by a sine wave and its first harmonic (e.g. \citealt{north84,mathys85,bernhard15b}). Depending on the inclination of the rotational axis and the number of spots that come into view during the rotation cycle, most ACVs show either single-wave or double-wave light curves \citep[e.g.][]{maitzen80,jagelka19}. In the case of two dominant spots of different sizes or photometric properties on opposing hemispheres of the star, a double-wave light curve with maxima of different heights is to be expected, in agreement with the light curves of the ud-CBH variables. This variability pattern is fairly unique among early-type stars and, according to our experience \citep{bernhard15b,bernhard15a,huemmerich16}, a tell-tale sign of ACV variables. According to the study of \citet{jagelka19}, roughly one third of ACV variables are expected to show double-wave light curves, with half of these stars exhibiting maxima of different height.

\begin{figure}
	\includegraphics[width=\columnwidth,bb=0 0 500 300]{colourcolourdiagram.pdf}
    \caption{Near-/mid-infrared colour-colour diagram of all stars selected via the criteria outlined in Section \ref{motivation_and_target_section}. Note the 'red tail' of objects with $(J-K_{s})$\,$>$\,0.6\,mag.}
    \label{fig:colourcolourdiagram}
\end{figure}

Furthermore, the characteristics of the ud-CBH variables given in \citet{heinze18} -- low-amplitude ($<$0.2\,mag) variability;  periods in the range of about 1\,<\,$P(d)$\,<\,5, with a peak around 2\,d -- are in agreement with the majority of ACV variables, which mostly exhibit rotational periods in the above mentioned period range, with a well-known peak around 2\,d \citep[e.g.][]{RM09,bernhard15a}. A comparison of the light curves of two ud-CBH variables from the list of \citet{heinze18} to the light curves of two double-waved ACV variables taken from \citet{bernhard20} is provided in Figure \ref{fig:LC_overview}. While the amplitude of the light variations appears reduced in the filterless data from the Multi-site All-Sky CAmeRA (MASCARA; \citealt{MASCARA1,MASCARA2}), the general variability pattern is the same. As an initial test of our hypothesis, we investigated the LAMOST DR4 spectra of several ud-CBH stars, which confirmed our suspicion that these objects are indeed mCP (mostly CP2) stars.

For the final target selection process, several considerations had to be taken into account. As 'ud-CBH stars' is not one of the final adopted variability classes, these objects cannot be simply queried via the interface to the ATLAS DR1 catalogue.\footnote{More information on how to query the ALTAS DR1 catalogue is available at \url{https://archive.stsci.edu/prepds/atlas-var/}.} \citet{heinze18} comment that most ud-CBH variables were sorted into the category PULSE by the classification algorithm. Apart from that, we consider the CBH and SINE groups the most promising targets for discovering ACV variables among the remaining variability classes. The SINE group ('Pure sine was fit with small residuals') was chosen because most ACV stars (roughly 50\,\% of the sample of \citealt{jagelka19}) show symmetric single-wave light curves that can be well fitted by a sine wave. All other variability groups were ruled out as primary targets on grounds of the covered period and amplitude ranges, the occurrence of multiple periods, irregular variability, or, as ACV variables show remarkably stable light curves, the indication of large residuals to the sine fit (class NSINE = 'Noisy sine: pure sine was fit, but residuals are large or nonrandom').

On grounds of these considerations, and after some initial testing regarding the feasibility of our intended approach, we decided to investigate objects from the PULSE, CBH, and SINE groups with the following requirements: (i) 0.5\,<\,$P(d)$\,<\,10, (ii) peak-to-peak variability amplitude in the $c$ band of amp($c$)\,$<$\,0.3\,mag, and (iii) phase offset $\phi{_2}$\,$-$\,$\phi{_1}$ of the first two Fourier terms between 60$^{\circ}$ and 110$^{\circ}$. The imposed cuts form a compromise between an effective identification of mCP stars and the need to keep the sample down to a manageable size. The period (i) and phase offset (iii) requirements were enforced to exclude $\delta$ Scuti (GCVS-type DSCT) stars or other short period pulsators and W UMa variables. Item (iii) was chosen according to the results of \citet{heinze18}, who find that most ud-CBH stars have phase offsets near 90$^{\circ}$ (cf. in particular their Figure 23). We note that while there exist mCP stars with rotation periods in excess of the chosen limit, their incidence drops significantly towards longer rotational periods (e.g. \citealt{RM09}); more importantly, the number of suitable light curves in the ATLAS DR1 catalogue diminishes rapidly at $P$\,>\,10\,d. The peak-to-peak variability cut-off (ii) was set deliberately high in order not to per se exclude any high-amplitude ACV variables. Although most ACV stars show amplitudes smaller than 0.2\,mag ($V$), we noticed several stars with amplitudes approaching this limit in the $c$ band (cf. Figure \ref{fig:LC_overview}).

Frequency spectra of all objects selected via these criteria were calculated using \textsc{Period04} \citep{period04}. Light curves and frequency spectra were then visually inspected. Obviously multiperiodic objects, such as slowly pulsating B (GCVS-type SPB) stars and $\gamma$ Doradus (GCVS-type GDOR) variables, were discarded; mono-periodic objects (that is, objects with frequency spectra indicative of a single significant frequency or a single significant frequency plus corresponding harmonics) with stable light curves typical of ACV variables were chosen for further consideration.

Although spot configurations in late-type stars are much more unstable, we expect contamination by late-type rotational variables such as BY Draconis (GCVS-type BY) or RS Canum Venaticorum (GCVS-type RS) stars that, at least in the investigated time-span, did not show significant changes in spot sizes and distribution and therefore exhibited appreciably stable light curves. For this reason, as an initial check, the remaining objects were plotted in a near-/mid-infrared colour-colour diagram (Figure \ref{fig:colourcolourdiagram}) in order to identify red stars. To this end, we employed photometry from the 2MASS \citep{2MASS} and WISE \citep{WISE} catalogues. Considering the faintness of the investigated objects and the unknown amount of reddening in the line-of-sight, this will only have a limited predictive value as regards the intrinsic colours of the stars. However, there is an obvious red tail of objects with ($J-K_{s}$)\,$>$\,0.6\,mag, which likely corresponds to late-type rotational variables. For several of these objects, LAMOST DR4 spectra are available, which indeed confirmed this assumption. Three exemplary spectra are shown in Figure \ref{fig:showcase_red_stars}. As expected, all objects show signs of increased chromospheric activity, which is typical of late-type rotational variables. We therefore felt justified in excluding objects with ($J-K_{s}$)\,$>$\,0.6\,mag from further consideration.

264 stars passed the imposed selection criteria, which, for convenience, are hereafter referred to as the 'final sample'. The full list of parameters for these objects is provided in Table \ref{table_master_part1} in the Appendix (Section \ref{essentialdata}). A sample page illustrating the light curves of the first 16 stars from our sample is also provided in the Appendix (Figure \ref{LC_sample_page}). The full set of light curves is obtainable online.

\begin{figure*}
	\includegraphics[width=2.0\columnwidth,bb=0 0 600 400]{showcase_red_stars.pdf}
    \caption{Spectra of late-type rotational variables from the 'red tail' with $(J-K_{s})$\,$>$\,0.6\,mag, showing signs of increased chromospheric activity. Identifiers and spectral types (derived in this study) are indicated in the plot. The spectrum of J070728.85+410115 shows emission in the H alpha line (not shown in the plot).}
    \label{fig:showcase_red_stars}
\end{figure*}

\section{Spectral classification} \label{spectral_classification}

The final sample was cross-matched with the LAMOST DR4 VizieR online catalogue\footnote{\url{http://cdsarc.u-strasbg.fr/viz-bin/cat/V/153}} \citep{DR4}, requiring S/N\,$\ge$\,25 in the Sloan $g$ band. In this manner, spectra for 62 stars could be procured. If more than one spectrum was available for a single object, only the spectrum with the highest $g$ band S/N was considered.

Spectral classification was performed in the framework of the refined MK classification system following the methodology outlined in \citet{gray87,gray89a,gray89b,gray94} and \citet{gray09}. For a precise classification and to identify peculiarities, the blue-violet (3800$-$4600\,\AA) spectral region was compared visually to, and overlaid with, MK standard star spectra and a set of synthetic spectra.

The standard star spectra were taken from the \textit{libr18} and \textit{libnor36} libraries that are distributed with the MKCLASS code\footnote{\url{http://www.appstate.edu/~grayro/mkclass/}}, a computer program written to classify stellar spectra on the MK system \citep{gray14}, and the \textit{liblamost} library, which is a preliminary set of suitable LAMOST spectra compiled by \citet{huemmerich20}. The synthetic spectra were calculated using the program SPECTRUM\footnote{\url{http://www.appstate.edu/~grayro/spectrum/spectrum.html}} \citep{SPECTRUM} and ATLAS9 model atmospheres \citep{ATLAS9}, assuming log g = 4.0, [M/H] = 0.0 and a microturbulent velocity of 2 km\,s$^{-1}$. The spectra were then subsequently smoothed to a resolution of 3.0\,\AA\ to provide a good match to the LAMOST spectra.

\begin{figure*}
	\includegraphics[width=2.1\columnwidth,bb=0 0 650 400]{showcase_ATLAS.pdf}
    \caption{Blue-violet region of the LAMOST DR4 spectra of (from top to bottom) the CP2 stars LAMOST J054513.97+111502.4 (ATO J086.3082+11.2506), LAMOST J033258.73+442605.0 (ATO J053.2447+44.4347), LAMOST J054613.28+402902.7 (ATO J086.5553+40.4840), and LAMOST J061457.97+412840.8 (ATO J093.7415+41.4780). Some prominent lines of interest are identified.}
    \label{fig:showcase_ATLAS}
\end{figure*}

mCP stars exhibit several peculiarities related to traditional classification criteria, which need to be taken into account when assigning a spectral type to these objects. They often show weak, unusually broad or otherwise peculiar \ion{Ca}{ii} K line profiles, weak \ion{Mg}{ii} 4481\,\AA\ lines and are markedly He deficient \citep{gray09,ghazaryan18}. The latter characteristic resulted in the classification of many of the hotter (late B-type) mCP stars as A-type stars because of the lack of, or the occurrence of only very weak, \ion{He}{i} lines in their spectra \citep{gray09}. Furthermore, mCP stars generally show enhanced and peculiar metallic lines. In general, therefore, the hydrogen-line profile is the most accurate indicator of the actual temperature of these objects \citep{gray09}.

We have determined spectral types based on the \ion{Ca}{ii} K line strength (the k-line type) and the hydrogen-line profile (the h-line type) \citep{osawa65}. Spectral types based on the strength of the \ion{He}{i} lines were not determined for all stars but only in the case of the He-weak/CP4 stars and where they were unambiguously visible in the spectra. Most late B-type stars in our sample appear noticeably He weak.

The metallic lines of most mCP stars are so peculiar that they cannot be used for luminosity classification. Luminosity types, therefore, were based on the wings of the hydrogen lines. In this respect, it is important to note that a considerable number of mCP stars shows narrow or unusual hydrogen-line profiles \citep[e.g.][]{faraggiana87,gray94,ghazaryan18} which are best matched by the profiles of high-luminosity objects like giants or even bright giants (luminosity classes III and II, respectively). This also holds true for many stars of our sample, although, apart from the hydrogen-line profile, other high-luminosity indicators are mostly absent from their spectra. It is well known that the vast majority of mCP stars are in fact main-sequence objects (\citealt{netopil17} and references therein) and our results from the colour-magnitude diagram (CMD) (Section \ref{parameters}) fully support this finding. Non-LTE effects may be at the root of this obvious discrepancy between the luminosities derived from the hydrogen-line profiles and other indicators \citep{gray94}. Perhaps the influence of the strong magnetic fields results in unusual atmospheric structures; however, this remains as yet unsolved.

Main chemical peculiarities are given in order of importance. Parantheses and a double pair of parantheses have been employed to indicate that a peculiarity is, respectively, weakly or only marginally present \citep{gray87,gray89a,gray89b,gray94}. Likewise, the notation ``metallic lines'' is used to indicate a faint background of metallic lines due to other atomic species than iron, titanium, or their ions \citep{gray87}. This notation may also appear in parantheses or a double pair of parantheses.

For several objects, only spectra of low S/N (S/N < 40) are available. Spectral types based on these spectra should be regarded as estimates only. For instance, the difference between the hydrogen-line profiles of a B8 III star and a B5 V star gets blurred in low S/N spectra \citep{gray94}. As mCP stars often show weak He lines, this leads to corresponding uncertainties in the spectral classification.

Example spectra are provided in Figure \ref{fig:showcase_ATLAS}; final spectral types and remarks are presented in Table \ref{table_SpT}. We also investigated the 4800$-$5600\,\AA\ spectral region to check for the presence and morphology of the flux depression around 5200\,\AA, which is a characteristic of mCP stars \citep{kodaira69,kupka03,khan07} and readily visible at LAMOST resolution \citep{huemmerich20}. Unless indicated otherwise in the remarks, all objects show a clearly visible 5200\,\AA\ feature in their spectra, as expected.

Nine of the spectroscopically confirmed mCP stars are contained in the sample of \citet{huemmerich20}; the remaining 54 stars are here presented as mCP stars for the first time. Our classifications agree well with the automatically derived classifications from the aforementioned study. \citet{huemmerich20} did not specify k-line types for all objects; however, the h-line types, the most important temperature-type criterion in mCP stars, agree very well: the differences amount to 0.0 spectral subclasses in the case of six objects, 0.5 spectral subclasses in the case of two stars, and 2.0 spectral subclasses in the case of one star (one spectral subclass being the difference between, for instance, A0 and A1). The main spectral peculiarities have been correctly identified by \citet{huemmerich20}; using manual classification, we can in some cases add weak peculiarities that have been missed by their code and, in two cases, are able to resolve the generic 'bl4077' (strong 4077\,\AA\ blend) and 'bl4130' (strong 4130\,\AA\ blend) types into their contributing ions. For instance, in the case of J072338.12+003848.5, 'bl4077' resolves into \ion{Si}{II} 4076\,\AA\ and \ion{Sr}{II} 4077\,\AA, and 'bl4130' into \ion{Si}{II} 4128$-$30\,\AA\ and \ion{Eu}{II} 4130\,\AA. Classifications from \citet{huemmerich20}, where available, are also provided in Table \ref{table_SpT}.

\begin{table*}
\caption{Spectral types of the mCP stars identified in the present study. The columns denote: (1) ATLAS object identifier. (2) LAMOST identifier. (3) Sloan $g$ band S/N ratio of the analysed spectrum. (4) Spectral type, as derived in this study. (5) Remark. 'H20' denotes spectral types from the study of \citet{huemmerich20}.}
\label{table_SpT}
\begin{center}
\begin{adjustbox}{max width=0.9\textwidth}
\begin{tabular}{lllll}
\hline
\hline
(1) & (2) & (3) & (4) & (5) \\
\hline
ID\_ATO	&	ID\_LAMOST	&	S/N\,$g$	&	SpT\_final	&	remark	\\
\hline
\hline
J046.2665+57.4649	&	J030503.98+572753.7	&	33	&	kA0 hB7 HeB8 V Si(Sr:)	&	no 5200\,\AA\ flux depression visible	\\
J046.9585+53.9453	&	J030750.05+535643.2	&	98	&	kA0 hA0: III-IV (Si)	&	$\lambda$4481 weak	\\
J047.5021+53.3159	&	J031000.50+531857.3	&	30	&	kA1 hA3 III SiCrEu	&		\\
J050.9303+44.3793	&	J032343.27+442245.4	&	108	&	kA0 hA0 II EuSi	&	$\lambda$4481 weak; H20: A0 Ib-II EuSi	\\
J053.2447+44.4347	&	J033258.73+442605.0	&	69	&	kB9.5 hB9 III SiEuCr	&	$\lambda\lambda$4172-9 strong	\\
J057.4910+58.7724	&	J034957.85+584620.8	&	57	&	kA0 hB9.5 III Si(Cr)Eu	&	$\lambda$4481 weak	\\
J060.7275+46.2448	&	J040254.59+461441.4	&	45	&	kA1 hB9: II: SiEuSr	&	$\lambda$4481 weak	\\
J060.7480+45.3172	&	J040259.53+451902.0	&	113	&	kA1 hA1 III SiEu((Cr))	&	$\lambda$4481 weak	\\
J063.5805+46.9075	&	J041419.32+465427.1	&	42	&	knA1 hA5 III EuCrSr(Si)	&	$\lambda$4481 weak	\\
J064.2611+46.2848	&	J041702.66+461705.5	&	65	&	kA0 hA0 III-IV Si	&	$\lambda$4481 weak	\\
J065.7038+47.6938	&	J042248.93+474138.0	&	308	&	kA0 hA0 II EuSiCr	&	$\lambda$4481 weak; H20: A0 II Eu	\\
J066.9854+44.3739	&	J042756.51+442226.2	&	67	&	kB9.5 hB8 IV Si	&	$\lambda$4481 weak	\\
J067.4887+38.9535	&	J042957.29+385712.5	&	58	&	knB9 hB5 V Si	&		\\
J072.5642+39.5294	&	J045015.40+393146.0	&	78	&	kA1 hA5 III SiCr	&		\\
J074.4268+43.8711	&	J045742.44+435216.0	&	30	&	kA0 hA5 III-IV SiEuSr	&	$\lambda$4481 weak	\\
J074.9570+40.2063	&	J045949.68+401222.8	&	83	&	kA0 hB9 III-IV SiEu	&	$\lambda$4481 broad and shallow	\\
J074.9889+42.2979	&	J045957.34+421752.6	&	31	&	kA0 hB9 III SiEuCr	&		\\
J076.4023+45.6101	&	J050536.57+453636.6	&	59	&	kA1 hB9 III EuSi	&	Eu very strong; $\lambda$4481 broad and shallow	\\
J077.0867+36.5911	&	J050820.81+363528.0	&	41	&	kB9.5 hB8 V (Si) ((metallic lines))	&	very weak 5200\,\AA\ flux depression	\\
J081.9629+42.4325	&	J052751.11+422557.3	&	92	&	kB9.5 hB9.5 III Si	&	$\lambda$4481 weak	\\
J082.5579+33.1925	&	J053013.91+331133.3	&	31	&	kA0 hB9: III: SiCr:Eu:	&	$\lambda$4481 weak	\\
J082.6115+29.6992	&	J053026.78+294157.2	&	84	&	kA0 hB9 III Si	&	$\lambda$4481 weak	\\
J082.6322+21.1693	&	J053031.74+211009.4	&	103	&	kB9 hB7 HeB9 V ((metallic lines))	&		\\
J084.9321+37.2119	&	J053943.72+371243.0	&	59	&	knA0 hB9 V SiEu((Cr))	&	$\lambda$4481 broad and shallow	\\
J086.1147+31.8873	&	J054427.54+315314.3	&	28	&	kA1 hB9 IV Si:Cr:Eu:	&		\\
J086.1972+24.3919	&	J054447.34+242331.1	&	52	&	kB9 hB7 HeB8 V ((Si)) (metallic lines)	&		\\
J086.3082+11.2506	&	J054513.97+111502.4	&	232	&	kB8 hB8 V Si	&	$\lambda$4481 weak	\\
J086.4762+23.3391	&	J054554.30+232021.0	&	47	&	kA0 hB9 III SrCrEuSr	&	$\lambda$4481 slightly weak	\\
J086.5553+40.4840	&	J054613.28+402902.7	&	98	&	kA0 hB9 IV Si(SrCr)	&	$\lambda$4481 weak	\\
J087.1757+29.1833	&	J054842.18+291059.9	&	35	&	kA0 hB9: V: SiEuCr	&	$\lambda$4481 weak	\\
J087.2218+29.4548	&	J054853.23+292717.3	&	26	&	kB9 hA0: III: SiCrEu	&	$\lambda$4481 weak	\\
J088.2315+38.6528	&	J055255.56+383910.1	&	47	&	kB9 hB7 HeB9 V Si (metallic lines)	&	$\lambda$4481 weak	\\
J090.0237+21.9017	&	J060005.70+215406.3	&	40	&	kA0 hB9 V CrSiEu	&	\\
J090.7455+31.0548	&	J060258.92+310317.1	&	37	&	kB9 hB9: II: SiCrSr	&	$\lambda$4481 weak	\\
J091.1746+24.8696	&	J060441.92+245210.8	&	26	&	kB9: hB9: III: Si	&	$\lambda$4481 weak	\\
J091.9664+24.5688	&	J060751.94+243407.9	&	95	&	kB9 hB5 HeB9 IV (Si) (metallic lines)	&		\\
J093.7415+41.4780	&	J061457.97+412840.8	&	112	&	kA1 hA5 V Eu	&	$\lambda\lambda$4172-9 strong	\\
J093.9930+13.8659	&	J061558.32+135157.3	&	148	&	kB9 hB5 HeB9 V (SiSr)Ti?	&	H20: B5 III-IV bl4130 (He-wk)	\\
J094.3323+15.5243	&	J061719.74+153127.5	&	86	&	kB9.5 hB7 HeB9 V Si	&		\\
J094.7507+19.5193	&	J061900.18+193109.6	&	76	&	knA0 hA0: II-III SiEuCr	&	$\lambda$4481 weak	\\
J095.0108+01.8715	&	J062002.59+015217.4	&	41	&	kA0 hB9 IV SiCrSrEu	&	$\lambda$4481 weak	\\
J095.4959+23.6564	&	J062159.02+233923.1	&	42	&	knB9 hB8 HeB9 V SiCr	&		\\
J096.8934+14.9451	&	J062734.41+145642.6	&	37	&	kA1 hA3: III: Cr:Si:	&	$\lambda$4481 weak	\\
J097.1763+16.4813	&	J062842.31+162852.9	&	168	&	kB9.5 hB9.5 III EuSi((Cr))	&	$\lambda$4481 weak; H20: B9.5 II-III EuSi	\\
J097.4242+24.5808	&	J062941.80+243450.9	&	155	&	kB9 hB7 HeB8 V 	&		\\
J097.6873+03.0070	&	J063044.96+030025.3	&	61	&	kB9 hB7 HeB9: V 	&		\\
J098.5904+17.0987	&	J063421.70+170555.6	&	83	&	knA0 hB9 III Si	&	$\lambda$4481 weak	\\
J098.6389+19.1051	&	J063433.34+190618.6	&	26	&	kA0 hB8 IV SiCr:Eu:	&	$\lambda$4481 weak	\\
J099.0745+18.8221	&	J063617.89+184919.6	&	28	&	kB9 hB9 IV SiEuCr	&		\\
J099.6853+17.3396	&	J063844.48+172022.5	&	162	&	kA0 hB9 III Si(Sr)((Cr))	&	$\lambda$4481 weak; H20: B9 III-IV Si	\\
J100.3063+00.9026	&	J064113.52+005409.4	&	43	&	kA0 hB8 IV SiCr	&	$\lambda$4481 weak	\\
J101.1743+21.6307	&	J064441.84+213750.5	&	132	&	kA0 hA0 II EuSi((Cr))	&	$\lambda$4481 weak; H20: A0 II EuSi	\\
J101.3758+01.7599	&	J064530.19+014535.8	&	97	&	kB9 hB8 V SiEu((Cr))	&	$\lambda$4481 weak	\\
J103.3079+10.5510	&	J065313.89+103303.3	&	119	&	kA0 hA0 III EuSi	&	$\lambda$4481 weak; H20: kA0hA2mA5 Eu	\\
J103.8576-00.4954	&	J065525.82-002943.4	&	71	&	kA0 hB5 V (metallic lines)	&		\\
J105.0327+06.1169	&	J070007.86+060701.0	&	50	&	kA1 hA1 II: EuCrSi	&	$\lambda$4481 weak	\\
J106.4471-03.7806	&	J070547.31-034650.2	&	80	&	kB9.5 hB9 III: (metallic lines)	&	\\
J106.5580+18.8987	&	J070613.94+185355.6	&	63	&	kA0 hB9 III Si	&	H20: B9.5 II-III Si	\\
J110.2675-03.2520	&	J072104.20-031507.4	&	142	&	kA0 hB9 III SiSrEu	&	$\lambda$4481 weak; H20: B9.5 II-III bl4077 bl4130	\\
J110.9088+00.6468	&	J072338.12+003848.5	&	94	&	knB9 hB9 IV-V SiSrCrEu	&	$\lambda$4481 weak; very broad Ca II K line blend	\\
J306.9801+45.3863	&	J202755.24+452311.0	&	99	&	kA0 hB9 IV Si(EuSr)	&	$\lambda$4481 weak	\\
J350.3833+56.4514	&	J232132.00+562705.2	&	57	&	kA0 hA3 III EuSi	&	$\lambda$4481 weak	\\
\hline
\end{tabular}
\end{adjustbox}
\end{center}                                                    \end{table*}

\section{Magnitude, period and space distribution} \label{space_distribution}

The upper panel of Figure \ref{histograms} illustrates the histogram of the $G$ magnitudes of the spectroscopically confirmed mCP stars ($N$\,=\,62) and the mCP star candidates ($N$\,=\,202) of our final sample. The magnitude distribution peaks around 14th magnitude. For comparison, the stars in the catalogues of \citet{RM09} and \citet{huemmerich20} peak at 9th magnitude and between 11th and 12th magnitude, respectively. With this work, we therefore extend the search for new mCP stars to even fainter magnitudes.

The period histogram is presented in the lower panel of Figure~\ref{histograms}. All periods were extracted from \citet{heinze18} and are presented, together with other parameters, in Table \ref{table_master_part1}. The period distribution is fully in agreement with the observed rotational periods of mCP stars, which generally cluster at around a period value of 2 days \citep[e.g.][]{RM09,bernhard15a}. We recall the here imposed period cut-off (0.5\,<\,$P(d)$\,<\,10), which was chosen to exclude short-period pulsators and because the number of suitable light curves in the ATLAS DR1 catalogue diminishes rapidly at $P$\,>\,10\,d (cf. Section \ref{motivation_and_target_section}). Any mCP stars with rotation periods longer than 10 days will therefore have been missed by our approach.

\begin{figure}
        \includegraphics[width=\columnwidth,bb=0 0 550 400]{histogram_mag.pdf}
        \includegraphics[width=\columnwidth,bb=0 0 550 400]{histogram_P.pdf}
    \caption{Histograms of the $G$ magnitudes (upper panel) and photometric periods (lower panel) of the spectroscopically confirmed mCP stars ($N$\,=\,62) and the mCP star candidates ($N$\,=\,202) of our final sample.}
		\label{histograms}
\end{figure}

The coordinates in the Galactic [XYZ] plane were obtained via the conversion of spherical Galactic coordinates (latitude and longitude) to Cartesian coordinates using the distance $d$ from \citet{2021AJ....161..147B}. Only objects with absolute parallax errors less than 25\,\% ($N$\,=\,257) were considered. The positive X-axis is towards the Galactic centre, the positive Y-axis is in the direction of the Galactic rotation, and the positive Z-axis is towards the north Galactic pole.

Our results are shown in the Appendix in Figure \ref{map_3D}. Most sample stars classify as either members of the thin disk (scale height of 350\,pc) or the thick disk (1200\,pc). The corresponding scale heights were adopted from \citet{2001MNRAS.322..426O} and \citet{2017MNRAS.470.2113A}. Interestingly, four stars (ATO J265.2024+10.6314, ATO J072.9129-07.0638, ATO J005.5419+15.5369, and ATO J310.1614-15.1051) are situated more than 1200\,pc above or below the [XY] plane and thus qualify as members of the halo population. This is of considerable interest as only very few halo CP2 stars are known \citep{huemmerich20}.

\section{Mass and age distribution} \label{parameters}

For generating a colour-magnitude diagram (CMD), we employed the homogeneous Gaia DR2 photometry of \citet{2018A&A...616A..17A} and the photogeometric distances of \citet{2021AJ....161..147B}, which are based on the Gaia EDR3 \citep{2021A&A...649A...3R}. As most of our sample stars are members of the Galactic disk and situated within a mean distance of 2500\,pc from the Sun, interstellar reddening is significant and needs to be taken into account. To estimate the absorption in the line-of-sight, we interpolated the reddening map of \citet{2018MNRAS.478..651G} using the Gaia EDR3 photogeometric distances. Reddening values were transformed using the relations
\begin{equation}
E(B - V) = 0.76E(BP - RP) = 0.40A_G,
\end{equation}
which take into account the coefficients listed in \citet{2018MNRAS.478..651G}.

The Gaia DR2 photometry was corrected as suggested by \citet{2018A&A...619A.180M}. The PARSEC isochrones \citep{2012MNRAS.427..127B} for solar metallicity [Z]\,=\,0.02\,dex and the filter curves from \citet{2018A&A...619A.180M}
were used for further analysis.
For the estimation of the stellar mass and logarithmic ages, the Stellar Isochrone Fitting Tool\footnote{\url{https://github.com/Johaney-s/StIFT}} was used, which searches for the best-fit evolutionary track within a model grid box. The four grid points closest to the input value are determined, from which the output parameters are derived by bilinear interpolation following the methodology described by \citet{2010MNRAS.401..695M}.

The CMD (Figure \ref{fig:CMD}) shows that our sample contains no young stars near the zero-age main sequence (ZAMS). This allowed a corresponding restriction of the tracks in the models to increase the accuracy of the estimates. Parameters could not be determined for five stars of our sample (ATO J076.1702+08.2581, ATO J115.0928-10.6198, ATO J117.8237-09.5101, ATO J308.7048+45.8077, and ATO J321.3283+53.8969) because they did not fit into the grid of models.

Figure~\ref{histograms2} shows the mass and age distribution of our sample stars, the complete list of parameters is given in Appendix~\ref{essentialdata}. Derived masses range from 1.4\,\(\textup{M}_\odot\) (a spectral type of about F3) to 5\,\(\textup{M}_\odot\) (B5). However, half of our sample stars have masses between 2 and 2.4\,\(\textup{M}_\odot\) (A2 to B9), which is in line with the spectral classifications presented in Section \ref{spectral_classification}. There is only a single outlier with a mass of 4.8\,\(\textup{M}_\odot\). The derived ages are in agreement with the results from the CMD; the vast majority of our sample stars are main-sequence objects situated rather close to the terminal-age main sequence (TAMS).

\begin{figure}
	\includegraphics[width=\columnwidth]{CMD.pdf}
    \caption{$(BP - RP)_0$ versus $M_{\mathrm{G,0}}$ diagram of our sample stars. Also indicated are PARSEC isochrones for solar metallicity [Z]\,=\,0.02\,dex. Ages are given in logarithmic units of years.}
    \label{fig:CMD}
\end{figure}

\begin{figure}
	\includegraphics[width=\columnwidth,bb=0 0 550 400]{histogram_M.pdf}
	\includegraphics[width=\columnwidth,bb=0 0 550 400]{histogram_logt.pdf}
    \caption{Histograms of the estimated masses (upper panel) and the logarithmic ages (lower panel) of our sample stars.}
    \label{histograms2}
\end{figure}

\section{Conclusions} \label{conclusions}

Instigated by the similarity of the light curves, periods and amplitudes of the 'upside-down CBH variables' shown in \citet{heinze18} to the parameters of the class of ACV variables, we carried out a search for ACV variables in the ATLAS DR1 catalogue. Our main results are summarised in the following.

\begin{itemize}
	\item Using suitable selection criteria (0.5\,<\,$P(d)$\,<\,10; amp($c$)\,$<$\,0.3\,mag; phase offset $\phi{_2}$\,$-$\,$\phi{_1}$ of the first two Fourier terms between 60$^{\circ}$ and 110$^{\circ}$; stable light curves; monoperiodicity; suitable near-/mid-infrared colours), we identified 264 candidate ACV variables.
	\item 62 of these objects could be spectroscopically confirmed as mCP stars with LAMOST spectra and were classified on the MK system. Nine of these objects are included in the sample of \citet{huemmerich20}; the other 54 stars are new discoveries. The remaining 202 stars are here presented as ACV star candidates that require further observations.
	\item We present basic stellar parameters for all sample stars. Derived masses range from 1.4\,\(\textup{M}_\odot\) to 5\,\(\textup{M}_\odot\), with half our sample stars being situated in the range from 2 \,\(\textup{M}_\odot\) to 2.4 \,\(\textup{M}_\odot\). These results are in good agreement with our spectral classifications. As expected, the majority of our sample stars are main-sequence objects.
	\item Most of our sample stars are members of the thin and thick disk. Four objects (ATO J265.2024+10.6314, ATO J072.9129-07.0638, ATO J005.5419+15.5369, and ATO J310.1614-15.1051) classify as members of the halo population.
	\item With a peak magnitude distribution at around 14th magnitude, the here presented mCP stars and candidates are situated at the faint end of the known Galactic mCP star population.
\end{itemize}

While ACV variables have been included into automated classification routines with good success in the past (e.g. \citealt{sitek14}), several of the more recent, massive variability catalogues, such as \citet{heinze18} and \citet{ZTFvars}, do not specifically consider this class of variable stars. Nevertheless, ACV variables are characterised by a distinct set of parameters in period, amplitude and colour spaces as well as concerning their light curve morphology (monoperiodicity, light curve stability, characteristic phase offset), and should therefore be well suited for automated classification attempts.

Our study shows that a dedicated search for ACV variables in catalogues that do not consider this class is a good starting point for the identification of further members of this group of variables. In general, we expect that the advent of high-precision, multi-colour and spectroscopic surveys will open up a multitude of possibilities to identify new ACV variables, and hence increase the sample size of know mCP stars, in the future.

\section*{Acknowledgements}

We thank the referee for his/her comments that helped to improve the paper. EP acknowledges support by the Erasmus+ programme of the European Union under grant number 2020-1-CZ01-KA203-078200. The Guo Shou Jing Telescope (the Large Sky Area Multi-Object Fiber Spectroscopic Telescope, LAMOST) is a National Major Scientific Project built by the Chinese Academy of Sciences. Funding for the project has been provided by the National Development and Reform Commission. LAMOST is operated and managed by National Astronomical Observatories, Chinese Academy of Sciences. This work presents results from the European Space Agency (ESA) space mission Gaia. Gaia data are being processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC is provided by national institutions, in particular the institutions participating in the Gaia MultiLateral Agreement (MLA). The Gaia mission website is https://www.cosmos.esa.int/gaia. The Gaia archive website is https://archives.esac.esa.int/gaia.

\section*{Data Availability}

The data underlying this article will be shared on reasonable request to the corresponding author.

\bibliographystyle{mnras}

redpajama_set_name: RedPajamaArXiv


text:
PORTLAND RY., LIGHT & POWER CO. v. RAILROAD COM'N OF OREGON
PORTLAND RY., LIGHT & POWER CO. v. RAILROAD COM'N OF OREGON(1913)
Argued: Decided: June 10, 1913
Messrs. Franklin T. Griffith, Joseph S. Clark, and Frederick V. Holman for plaintiff in error.
Mr. A. M. Crawford, Attorney General of Oregon, and Messrs. Cylde B. Aitchison, R. M. Sewell, and R. R. Giltner for defendant in error.
Mr. Justice Day delivered the opinion of the court:
The Oak Park Improvement Association, a voluntary organization of persons residing in and about the stations on the Oregon City division of the plaintiff in error, the Portland Railway, Light & Power Company, known as the Oak Grove district, and comprising Milwaukie Heights, Courtney, Oak Grove, Center, and Risley, sought by complaint filed with the railroad commission of Oregon to have the commission fix reasonable fares, and to order their substitution for those found to be unreasonable and unjustly discriminatory. The commission, upon hearing, found that the rate of fare of 15 cents charged [229 U.S. 414, 415] by the railway company between the city of Portland and the Oak Grove district was unreasonable and unjustly discriminatory, and ordered the railway company to charge in lieu thereof a 10 cent fare, and to give the same transfer privileges to passengers traveling between Portland and the Oak Grove district that were accorded to passengers on the Mt. Scott division of the plaintiff in error. The supreme court of Oregon, relying upon the conclusions reached by it in the Milwaukie Case (Portland R. Light & P. Co. v. Railroad Commission, 56 Or. 468, 105 Pac. 709, 109 Pac. 273), decided this day by this court, and reported at 229 U.S. 397 , 57 L. ed. --, 33 Sup. Ct. Rep. 820, affirmed the decree of the circuit court, confirming the order of the commission (57 Or. 126, 105 Pac. 715), and the case is here on writ of error.
The findings of fact in the present case are practically identical with those in the Milwaukie Case, ante, 820, except the exclusion of facts applying to Milwaukie alone, and the substitution of facts pertinent to the Oak Grove district, and show that the circumstances and conditions under which the plaintiff in error transports passengers between Portland and certain stations named for a fare of 10 cents, with transfer privileges, are substantially the same as the circumstances and conditions under which the plaintiff in error transports passengers between Portland and the Oak Grove district, except as to the rate of fare and the giving of transfers, and that, while the charges of the railway company upon the Oregon City division are not in themselves unreasonable, they are 'unjust and unreasonable, discriminatory, and give undue preference.'
This case, denominated the Oak Grove Case, and the Milwaukie Case, were heard together in the supreme court of Oregon, and have been presented together in this court. The contentions asserted in this case are the same contentions set up in the Milwaukie Case, and the opinion in the latter case (ante, 820) has dealt with the controversy [229 U.S. 414, 416] here presented. In view of the conclusions reached in that case, we see no reason to disturb the judgment of the Supreme Court of Oregon in the present case, and it is accordingly affirmed.

redpajama_set_name: RedPajamaCommonCrawl


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Frixo › Sportsbook › Articles › What Are Forecasts?
Primarily associated with racing, "Forecast" refers to a class of bets made on a single event, in which the bettor attempts to predict (forecast) the correct finishing order of two or more entries. Among the various types of Forecasts available at most tracks are Straight Forecasts, Tricasts and others, as defined below.
A basic Forecast requires wagering of only one unit, typically no more than £2 at most U.K. racecourses or $2 in North America. It is possible to wager on multiple forecasts in a single race, creating "Reverse Forecasts" or "Combination Forecasts," although these usually require stakes of multiple units.
The returns on correctly predicted finishing orders are calculated by official industry sources using computer software that takes into account the starting prices of all participants in the event, the number of runners and other factors. Payouts are announced as the return per unit wagered.
Straight Forecast – In horse or greyhound racing, a bet on two selections (A & B) in a single event that yields a return if they finish first and second in the exact order indicated (e.g., AB if A wins and B is runner-up); also known as a "Perfecta" or "Exacta" in the United States or the "Exactor" in Canada. The term "computer straight forecast" (CSF) is sometimes used in conjunction with this bet, too. A Straight Forecast wager requires a bet of a single unit, typically £2 at racecourses in the U.K.
Reverse Forecast – In horse and greyhound racing, a combination of two Straight Forecast bets, allowing for a return if both selections (A & B) finish first and second in either order—AB or BA; also known as "Reverse Action," "Reversed Forecast," "Boxed Exacta," or "Boxed Perfecta." It requires two units to be staked. Where available, the "Quinella" replaces this type of bet—a single unit bet on two selections in a single event that yields a return as long as they finish in the first two places in any order.
Tricast – In horse and greyhound racing, a bet on three selections in a single event that yields a return if they finish first, second and third in the exact order indicated; also known as a "Trifecta" in the United States, "Triactor" in Canada or "Tiercé" in France. This wager requires a stake of one unit. Most horse racing courses in the U.K. require that at least six of eight declared starters must actually run in a race for the Tricast to be valid. In dog racing, the requirement may be reduced to five runners.
Combination Tricast – In horse and greyhound racing, this is most commonly made up of bets on three selections (A, B & C), including six Tricast wagers—ABC, ACB, BAC, BCA, CAB and CBA. If the three selections come in first, second and third in any order, a return will be received. In North America, the phrase "Boxed Trifecta" is used. Combination Tricasts may also be placed on more than three selections, in which case the number of wagers required (w) is expressed by the equation w = n(n-1)(n-2) where "n" is the number of selections.


Adam Lallana ensured Sam Allardyce's reign as England manager got off to a dramatic winning start with a strike deep into injury time against Slovakia.
Allardyce had looked as though he would have to settle for a deeply uninspiring stalemate in Trnava – the hosts having held firm in the World Cup Group F qualifier despite Martin Skrtel's sending-off after a nasty stamp on Harry Kane.
However Lallana picked a perfect moment to break his international duck and seal a 1-0 success. The Liverpool forward had already clattered a post when the ball broke for him inside the area, with seconds of the four added minutes left.
He showed neat footwork and got his shot away, then turned away in celebration as keeper Matus Kozacik let the ball squirm between his legs and over the line.
Also in Group F alongside England, Scotland made a winning start as a hat-trick from Hull's Robert Snodgrass helped secure a 5-1 victory in Malta.
Snodgrass' over-hit cross flew into the far top corner to give Gordon Strachan's side a ninth-minute lead but Alfred Effiong quickly headed an equaliser.
Chris Martin restored Scotland's lead just after half-time before a harsh red card for home defender Jonathan Caruana. Snodgrass scored from the resulting penalty and a Steven Fletcher header extended the lead.
Snodgrass tapped in for his hat-trick after a Fletcher shot had struck the crossbar, and Malta finished with nine men after Luke Gambin was sent off for a hack at Snodgrass.
The other game in Group F saw Slovenia fight back from two goals down to draw in Lithuania. Quick-fire goals from Fedor Cernych and Vykintas Slivka had the hosts in control at half-time but headed goals from Rene Krhin and Bostjan Cesar – the latter in injury time – earned Slovenia a point.
In Group C, world champions Germany began with a 3-0 win in Norway as Joshua Kimmich scored in between two goals from Thomas Muller.
Ruslan Gurbanov's goal just before half-time saw Azerbaijan get their campaign off to a winning start with a 1-0 victory over 10-man San Marino, who had Cristian Brolli sent off early in the second half, and the Czech Republic drew 0-0 with Northern Ireland.
Denmark were the only team to make a winning start in Group E thanks to Christian Eriksen's first-half strike against Armenia in Copenhagen, as Kazakhstan and Poland drew 2-2 and Romania and Montenegro shared the points in a 1-1 draw.
Bartosz Kapustka's strike and a Robert Lewandowski penalty had Poland in control but a quick-fire double from Sergei Khizhnichenko early in the second half earned an impressive 2-2 draw for the hosts.
Late drama in Romania saw Stevan Jovetic's 87th-minute header cancel out Adrian Popa's goal for the hosts just two minutes previously, before Nicolae Stanciu put a penalty over the crossbar in the seventh minute of injury time.


LIKES : fame and recognition, personal privacy, rainbows, dreams, magic, change for its own sake, eccentricity, surprises, and living within their means despite the many temptations which constantly surround them every waking moment.
DISLIKES : emotion and intimacy, people who show off, being taken for granted, being pinned down, violence and fighting, and senseless or purposeless extravagance of any sort.
You are generally without prejudice and quite tolerant of others' point of view. They are good listeners, and care deeply for their friends. To people they are not close to however, they can be somewhat detached. The Aquarius sun sign is true blue and loyal. They are one of the first to sign up to server their country, and will give their lives defending her. A typical Aquarius has the attribute of intense desire to communicate.
You are a bit tactless and rude if you don't learn to moderate your constant broadcasting around those whose opinions may be a bit more on the conservative side. You are interesting and attractive. You can be shy, sensitive, gentle and patient or enthusiastic and lively with a tendency to be exhibitionists. Both types are strong willed and forceful in its own way.
You are very opinionated with strong convictions and fight for what you believe. You are farsighted and innovative. They can be counted on to come up with original ideas. They make good designers and inventors as well as musicians. These intellectuals excel in the arts as well as the technical trades.
You cherish and guard your independence and are a strange mixture of caring concern and cool detachment. You will go out of your way to help when needed but will never get emotionally involved.
You are truly humane and known to be frank and outspoken. You are refined and idealistic, romantic and practical, personable and likable person. Being quick in mind and responding, you love activity and are quite reasonable in that.
It can be pure in color or may contain secondary minerals. If the matrix forms a pattern of interlocking polygons it is called "spider:web" turquoise.
The beautiful Turquoise is STAR GEMS of Aquarius. The name comes from the French "turquoise", which means "Turkey".
It is the symbol of total independence and asserts the freedom of an individual from all restriction and restraint. It is a breakthrough planet and indicates talent, originality and genius in a horoscope.
Uranus is the RULING PLANET of Aquarius an air sign. It brings a new way of looking at things and its approach is best met with an expanded consciousness. Uranus rules unexpected change, upheaval, revolution.
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KIM, JUHAN;PARK, CHANGBOM;L'HUILLIER, BENJAMIN;HONG, SUNGWOOK E.
The Horizon Run 4 is a cosmological N-body simulation designed for the study of coupled evolution between galaxies and large-scale structures of the Universe, and for the test of galaxy formation models. Using 63003 gravitating particles in a cubic box of Lbox = 3150 h−1Mpc, we build a dense forest of halo merger trees to trace the halo merger history with a halo mass resolution scale down to Ms = 2.7 × 1011h−1M⊙. We build a set of particle and halo data, which can serve as testbeds for comparison of cosmological models and gravitational theories with observations. We find that the FoF halo mass function shows a substantial deviation from the universal form with tangible redshift evolution of amplitude and shape. At higher redshifts, the amplitude of the mass function is lower, and the functional form is shifted toward larger values of ln(1/σ). We also find that the baryonic acoustic oscillation feature in the two-point correlation function of mock galaxies becomes broader with a peak position moving to smaller scales and the peak amplitude decreasing for increasing directional cosine μ compared to the linear predictions. From the halo merger trees built from halo data at 75 redshifts, we measure the half-mass epoch of halos and find that less massive halos tend to reach half of their current mass at higher redshifts. Simulation outputs including snapshot data, past lightcone space data, and halo merger data are available at http://sdss.kias.re.kr/astro/Horizon-Run4.