text:
In Response to EFF Lawsuit, Government Ordered to Release Secret Surveillance Court Documents Today
Announcement by Mark Rumold
Update: The government released two new FISC opinions this evening, both of which concern the transition of NSA surveillance to the oversight of the FISC in 2007. Neither of the two documents, available here and here, is the Raw Take order or the 2008 FAA order. The government has one additional production deadline in this case on March 2, 2015.
Since 2011, EFF has fought to shed light on the government's secret reinterpretation of federal surveillance laws. Much of our fight has focused on the legal opinions of the Foreign Intelligence Surveillance Court (FISC), the federal court that oversees many of the intelligence community's domestic surveillance programs.
In September, in response to our Freedom of Information Act lawsuit, a federal district court in Washington, D.C. ordered the government to review and produce a series of opinions from the secret court. Today, the government is scheduled to produce some of those documents.
We've sued the government three separate times to force disclosure of significant opinions of the FISC. These lawsuits have produced numerous previously secret FISC decisions, including: opinions showing the government had repeatedly violated court-imposed restrictions on surveillance, unconstitutional surveillance conducted under the FISA Amendments Act, and the transition to FISC oversight over NSA surveillance authorities.
Our third lawsuit sought the disclosure of a number of still-secret and significant FISC opinions. While the government has not indicated which opinion it intends to produce today, two significant opinions remain secret.
First, the so-called "Raw Take" order from 2002. The existence of this opinion was first disclosed in a New York Times article based, in part, off the Snowden disclosures. As the Times described the opinion, it "appears to have been the first substantial demonstration of the court's willingness after Sept. 11 to reinterpret the law to expand government powers." The order, apparently, "weakened restrictions on sharing private information about Americans, according to documents and interviews." Beyond what has been reported in the Times article, not much more is known about the opinion.
The second opinion that remains secret is a 2008 FISC opinion concerning the legality and constitutionality of surveillance under the FISA Amendments Act (FAA). This opinion, described as the "Rosetta Stone" of FAA surveillance by those familiar with it, purportedly represents the FISC's full assessment of the range of legal issues presented by NSA surveillance under Section 702 of the FAA—a provision of law authorizing the government to conduct warrantless surveillance within the United States of overseas targets. Importantly, the opinion likely discusses the constitutionality of the NSA's upstream surveillance operations—currently, the only federal court decision on this topic. Despite this opinion's centrality to understanding FAA surveillance, it has remained secret for nearly 7 years.
Of course, it's possible the government won't release anything today. In fact, in this lawsuit, the government has already claimed that a FISC opinion addressing criminal violations of federal surveillance laws by government officials must remain secret. We fully intend to fight for disclosure of that opinion in court. And, if the government decides to withhold either the Raw Take order or the 2008 FISC order, we promise to fight those withholdings as well. But our hope is that the government will save us all the time and expense of taxpayer dollars, and release the opinions without a lengthy court battle.
The public has a fundamental right to know, read, and understand the decisions of the federal courts. That's true whether the opinions concern national security surveillance or more mundane issues. Secret courts, and secret court opinions, are inimical to our democratic system. Hopefully, today's disclosures will move us one step closer to ending the government's secret surveillance law practices.
may_2007_order.pdf
august_2007_order.pdf
FISC Orders on Illegal Government Surveillance
Deeplinks Blog by Aaron Mackey | January 11, 2022
Court Orders Authorizing Law Enforcement To Track People's Air Travels In Real Time Must Be Made Public
The public should get to see whether a court that authorized the FBI to track someone's air travels in real time for six months also analyzed whether the surveillance implicated the Fourth Amendment, EFF argued in a brief filed this week.In Forbes Media LLC v. United States, the news...
Deeplinks Blog by Kit Walsh | December 30, 2021
Shining a Light on Black Box Technology Used to Send People to Jail: 2021 Year in Review
If you're accused of a crime based on an algorithm's analysis of the evidence, you should have a right to refute the assumptions, methods, and programming of that algorithm. Building on previous wins, EFF and its allies turned the tide this year on the use of these secret programs in...
Deeplinks Blog by Aaron Mackey, Dave Maass | December 17, 2021
EFF Continues Legal Fight to Release Records Showing How Law Enforcement Uses Cell-site Simulators
Four years ago, EFF set out on a mission to chase down the paper trail left behind when cops in California use cell-site simulators. This trail has led us to a California appellate court, where next spring we will face-off with San Bernardino County law enforcement over whether they can...
EFF v. San Bernardino County Superior Court (stingray transparency)
EFF is seeking to make public court records that would show how law enforcement in San Bernardino County, California use cell-site simulators and other invasive surveillance technologies. In 2019, EFF petitioned the San Bernardino County Superior Court to review and unseal 22 search warrants that appear to be sealed in...
EFF, Partners Launch New Edition of Santa Clara Principles, Adding Standards Aimed at Governments and Expanding Appeal Guidelines
San Francisco—The Electronic Frontier Foundation (EFF) and a coalition of civil society organizations and academics today released the second edition of the Santa Clara Principles on Transparency and Accountability In Content Moderation, adding standards directed at government and state actors to beef up due process and expanding guidelines for...
Livestreamed Hearing Monday: EFF Urges Appeals Court to Allow Public Access to Documents in Patent Troll Litigation
WASHINGTON, D.C.— On Monday, December 6, at 10 am ET, the Electronic Frontier Foundation (EFF), standing up for public access to courts and transparency in patent litigation, will urge a panel of judges to unseal documents that a notorious patent troll is trying to hide. At a federal appeals court...
Deeplinks Blog by rainey Reitman | November 16, 2021
EFF's How to Fix the Internet Podcast Offers Optimistic Solutions to Tech Dystopias
Through curious conversations with some of the leading minds in law and technology, we explore creative solutions to some of today's biggest tech challenges. Listen to EFF's podcast, How to Fix the Internet, today.
Deeplinks Blog by Aaron Mackey, Mukund Rathi | September 8, 2021
EFF to Court: FOIA Requires ICE to Release Arrest and Deportation Database Records With Privacy Protections
The Freedom of Information Act requires U.S. Immigration and Customs Enforcement (ICE) to disclose deidentified data that would enable greater public oversight of the agency while protecting the privacy of immigrants and others, EFF argued in an amicus brief filed last month in federal court.The case, ACLU v. ICE,...
Deeplinks Blog by Rory Mir, Cory Doctorow | August 12, 2021
Facebook's Attack on Research is Everyone's Problem
Facebook recently banned the accounts of several New York University (NYU) researchers who run Ad Observer, an accountability project that tracks paid disinformation, from its platform. This has major implications: not just for transparency, but for user autonomy and the fight for interoperable software.Ad Observer is a free/open source...
Press Release | July 27, 2021
EFF Sues U.S. Postal Service For Records About Covert Social Media Spying Program
Washington D.C.—The Electronic Frontier Foundation (EFF) filed a Freedom of Information Act (FOIA) lawsuit against the U.S. Postal Service and its inspection agency seeking records about a covert program to secretly comb through online posts of social media users before street protests, raising concerns about chilling the privacy and...


text:
The Volca Beats is a hybrid drum machine produced by the Japanese music technology manufacturer Korg. It was released in April 2013 along with the Volca Keys and Volca Bass. The Beats uses both analogue synthesis and PCM samples to produce drum sounds.

It is part of Korg's Volca line of affordable synthesizers and drum machines, so has a 16-step sequencer and can run off batteries. It is one of three drum machines/synthesizers in the Volca line, along with the Volca Kick and Volca Drum. The Volca Beats is still being produced, almost 10 years after its initial launch. It retails for around £125.

Release
The Volca Beats was released in April at Musikmesse Frankfurt 2013 alongside the Volca Keys and Volca Bass. It received mixed review, with MusicRadar stating "The balance between functionality, ease of use and playability is great" and others praising it for its "price, size, portability and sheer concentration of functionality". However, criticism was made specifically of its snare circuit, so much so that people developed simple modifications using a single resistor to improve to quality of the sound.

Review ratings
8/10 from MusicTech
4/5 (Excellent) from Vintage Synth Explorer
4.5/5 from MusicRadar
4.3/5 on Thomann
Chosen as one of the best budget drum machines by GearNews

Design
The Volca Beats has a black faceplate, with gold accents and keys; the enclosure is made of black plastic. Its design is partially inspired by the Roland TR-808, TR-606 and Korg's own Electribes.The Volca Beats is compact and lightweight. It features a 16-step sequencer as does all other Volcas, disregarding the Volca Mix. The sequencer has motion sequencing, Korg's version of parameter automation. It also features an "active step" function for fills and build ups. Connection points include 9V DC power, MIDI in, sync in/out and a single stereo output. The Volca can also be powered by AA batteries and has a built in speaker.

Sound engine
The Volca Beats' sound engine consists of two sections, the analogue drum section and the PCM sample section, along with a "stutter" effect. Stutter is a retrigger, with controls over time and depth. It behaves almost like a delay, retriggering either all voices or a single part. Each section is split up into tracks, of which there are 10 in total (6 analogue, 4 PCM). Each track has a different sound, e.g. Hi-hats, Kick.

Analogue section
The analogue section is made up of 6 tracks that Korg say are "common analogue vintage circuits":
Kick - a kick circuit that has been likened to an 808, it has 3 controls over Click (transient), Pitch of the kick and Decay.
Snare - seen as the weak point of the Beats. Controls include Pitch, Decay and "Snappy", which controls the amount of white noise in the snare. Lower levels can stand in for a rimshot.
Toms - The Volca Drum has both high and low toms. They have individual tuning but share a decay envelope.
Hats - There are both closed and open hats on the Volca Beats. Each has an individual decay but shares a Grain control, which controls pitch.

PCM sample section
PCM sample tracks only have control over individual volume and playback speed. There are four different tracks: Clave, Agogo, Clap and Cymbal.

References

External links
https://www.korg-volca.com/en/ - Korg Volca official website
https://www.korg.com/uk/products/dj/volca_beats/ - Official product page
Drum machines
Korg synthesizers
Grooveboxes

redpajama_set_name: RedPajamaWikipedia


text:
//
//  HYScanningView.m
//  QRCodeTest
//
//  Created by yanghaha on 15/12/8.
//  Copyright © 2015年 yanghaha. All rights reserved.
//

#import "HYScanningView.h"
#import <AVFoundation/AVFoundation.h>

@interface CornerView : UIView {
    UIBezierPath *_lefTopCorner;
    UIBezierPath *_rightTopCorner;
    UIBezierPath *_leftBottomCorner;
    UIBezierPath *_rightBottomCorner;
}

/**
 *  边角线的宽度
 */
@property (nonatomic) CGFloat lineWidth;

/**
 *  边角线的长度
 */
@property (nonatomic) CGFloat cornerLength;

@property (strong, nonatomic) UIColor *cornerColor;

@end

@implementation CornerView

- (instancetype)init {
    if (self = [super init]) {
        self.backgroundColor = [UIColor clearColor];
    }

    return self;
}

- (void)drawRect:(CGRect)rect {

    CGPoint originPoint = CGPointMake(CGRectGetMinX(rect), CGRectGetMinY(rect));

    [self.cornerColor set];

    //重绘左上角
    [_lefTopCorner removeAllPoints];
    _lefTopCorner = nil;
    _lefTopCorner = [self newPath];
    [_lefTopCorner moveToPoint:originPoint];
    [_lefTopCorner addLineToPoint:CGPointMake(originPoint.x, originPoint.y+self.cornerLength)];
    [_lefTopCorner moveToPoint:originPoint];
    [_lefTopCorner addLineToPoint:CGPointMake(originPoint.x+self.cornerLength, originPoint.y)];
    [_lefTopCorner stroke];

    originPoint = CGPointMake(CGRectGetMaxX(rect), CGRectGetMinY(rect));
    //重绘右上角
    [_rightTopCorner removeAllPoints];
    _rightTopCorner = nil;
    _rightTopCorner = [self newPath];
    [_rightTopCorner moveToPoint:originPoint];
    [_rightTopCorner addLineToPoint:CGPointMake(originPoint.x-self.cornerLength, originPoint.y)];
    [_rightTopCorner moveToPoint:originPoint];
    [_rightTopCorner addLineToPoint:CGPointMake(originPoint.x, originPoint.y+self.cornerLength)];
    [_rightTopCorner stroke];

    originPoint = CGPointMake(CGRectGetMinX(rect), CGRectGetMaxY(rect));
    //重绘左下角
    [_leftBottomCorner removeAllPoints];
    _leftBottomCorner = nil;
    _leftBottomCorner = [self newPath];
    [_leftBottomCorner moveToPoint:originPoint];
    [_leftBottomCorner addLineToPoint:CGPointMake(originPoint.x, originPoint.y-self.cornerLength)];
    [_leftBottomCorner moveToPoint:originPoint];
    [_leftBottomCorner addLineToPoint:CGPointMake(originPoint.x+self.cornerLength, originPoint.y)];
    [_leftBottomCorner stroke];

    originPoint = CGPointMake(CGRectGetMaxX(rect), CGRectGetMaxY(rect));
    //重绘右下角
    [_rightBottomCorner removeAllPoints];
    _rightBottomCorner = nil;
    _rightBottomCorner = [self newPath];
    [_rightBottomCorner moveToPoint:originPoint];
    [_rightBottomCorner addLineToPoint:CGPointMake(originPoint.x-self.cornerLength, originPoint.y)];
    [_rightBottomCorner moveToPoint:originPoint];
    [_rightBottomCorner addLineToPoint:CGPointMake(originPoint.x, originPoint.y-self.cornerLength)];
    [_rightBottomCorner stroke];

}

#pragma mark - Setter && Getter

- (CGFloat)lineWidth {
    if (_lineWidth < 1) {
        _lineWidth = CGRectGetWidth(self.bounds)/15;
    }

    return _lineWidth;
}

- (CGFloat)cornerLength {
    if (_cornerLength < 5) {
        _cornerLength = CGRectGetWidth(self.bounds)/4;
    }

    return _cornerLength;
}

#pragma mark - Private

- (UIBezierPath *)newPath {
    UIBezierPath *path = [UIBezierPath bezierPath];
    path.lineWidth = self.lineWidth;

    return path;
}

@end

@interface HYScanningView () <AVCaptureMetadataOutputObjectsDelegate> {
    AVCaptureMetadataOutput *_output;
}

@property (nonatomic, strong) UIBezierPath *coverPath;      //
@property (nonatomic, strong) UIBezierPath *boxPath;        //扫描框
@property (nonatomic, strong) CALayer *scanningLineLayer; //扫描线
@property (nonatomic, strong) AVCaptureSession *captureSession; //图像捕获会话
@property (nonatomic, strong) AVCaptureVideoPreviewLayer *videoPreviewLayer;  //预览捕获的图像图层
@property (nonatomic, strong) CAShapeLayer *coverLayer;      //透明覆盖图层
@property (nonatomic, strong) NSTimer *timer;   //定时器

@property (nonatomic, strong) CornerView *cornerView;

@end

@implementation HYScanningView

- (instancetype)init {
    self = [super init];

    if (self) {
        _autoRead = YES;
        _reading = NO;
        [self setupUI];
    }

    return self;
}

- (void)awakeFromNib {
    [super awakeFromNib];

    _autoRead = YES;
    _reading = NO;
    [self setupUI];
}

- (void)layoutSubviews {
    [super layoutSubviews];

    [self updateUI];

    if (self.autoRead) {
        [self startScanning];
    }
}

- (void)drawRect:(CGRect)rect {
    [self updateOutputRectOfInterest];
}

- (void)dealloc {

}

#pragma mark - Setter & Getter

- (CALayer *)scanningLineLayer {
    if (!_scanningLineLayer) {
        _scanningLineLayer = [[CALayer alloc] init];
    }

    return _scanningLineLayer;
}

- (AVCaptureSession *)captureSession {
    if (!_captureSession) {

        _captureSession = [[AVCaptureSession alloc] init];

        NSError *error;

        AVCaptureDevice *captureDevice = [AVCaptureDevice defaultDeviceWithMediaType:AVMediaTypeVideo];
        AVCaptureDeviceInput *input = [AVCaptureDeviceInput deviceInputWithDevice:captureDevice error:&error];
        if (!input) {
            NSLog(@"input初始化失败%@", [error localizedDescription]);
        } else {
            [_captureSession addInput:input];
        }

        _output = [[AVCaptureMetadataOutput alloc] init];

        [_captureSession addOutput:_output];
        [self updateOutputMetadataObjectTypes];
        dispatch_queue_t dispatchQueue = dispatch_queue_create("ScanningQueue", NULL);
        [_output setMetadataObjectsDelegate:self queue:dispatchQueue];
    }

    return _captureSession;
}

- (AVCaptureVideoPreviewLayer *)videoPreviewLayer {
    if (!_videoPreviewLayer) {
        _videoPreviewLayer = [[AVCaptureVideoPreviewLayer alloc] initWithSession:self.captureSession];
        _videoPreviewLayer.videoGravity = AVLayerVideoGravityResizeAspectFill;
    }

    return _videoPreviewLayer;
}

- (CAShapeLayer *)coverLayer {
    if (!_coverLayer) {
        _coverLayer = [CAShapeLayer layer];
        _coverLayer.fillRule = kCAFillRuleEvenOdd;
        _coverLayer.opacity = 0.5;
    }

    return _coverLayer;
}

- (NSTimer *)timer {
    if (!_timer) {
        NSTimeInterval duration = [self timerDuration];
        _timer = [NSTimer scheduledTimerWithTimeInterval:duration target:self selector:@selector(moveScanningLine) userInfo:nil repeats:YES];
    }

    return _timer;
}

- (void)setType:(HYScanningViewType)type {
    _type = type;

    [self updateOutputMetadataObjectTypes];
}

- (UIColor *)coverColor {

    if (!_coverColor) {
        _coverColor = [[UIColor grayColor] colorWithAlphaComponent:.5];
    }

    return _coverColor;
}

- (void)setCornerColor:(UIColor *)cornerColor {
    _cornerColor = cornerColor;

    self.cornerView.cornerColor = _cornerColor;
}

- (CGRect)boxFrame {
    if (CGRectIsEmpty(_boxFrame)) {
        _boxFrame = self.bounds;
    }

    return _boxFrame;
}

- (CornerView *)cornerView {
    if (!_cornerView) {
        _cornerView = [[CornerView alloc] init];
    }

    return _cornerView;
}

#pragma mark - Private

- (void)setupUI {
    [self.layer addSublayer:self.videoPreviewLayer];
    [self.layer addSublayer:self.scanningLineLayer];
    [self.layer addSublayer:self.coverLayer];
    [self addSubview:self.cornerView];
}

- (void)updateUI {
    self.videoPreviewLayer.frame = self.bounds;
    self.coverLayer.frame = self.bounds;
    self.coverLayer.fillColor = self.coverColor.CGColor;

    /*由于下面第一行代码需要在self.videoPreviewLayer完成显示的时候才能获取正确的rect,
     所以此处进行了延迟执行代码 */
    //    CGRect rectOfInterest = [self.videoPreviewLayer metadataOutputRectOfInterestForRect:self.boxFrame];

#if 1
//    [self performSelector:@selector(updateOutputRectOfInterest) withObject:nil afterDelay:1.];
#else
//    [self fixRectOfInterestZero];
#endif
    //    CGRect rectOfInterest = [self.videoPreviewLayer metadataOutputRectOfInterestForRect:self.boxFrame];
    //    NSInvocation *invocation = [NSInvocation invocationWithMethodSignature:[_output methodSignatureForSelector:@selector(setRectOfInterest:)]];
    //    invocation.target = _output;
    //    invocation.selector = @selector(setRectOfInterest:);
    //    [invocation setArgument:&rectOfInterest atIndex:2];
    //    [invocation performSelector:@selector(invoke) withObject:nil afterDelay:1.];

    [self updatePathWithBoxFrame:self.boxFrame];
    self.coverLayer.path = self.coverPath.CGPath;

    CGRect frame = self.boxPath.bounds;
    frame.size.height = 1;
    self.scanningLineLayer.frame = frame;
    self.scanningLineLayer.backgroundColor = self.scanningLineColor.CGColor;

    self.cornerView.frame = self.boxFrame;
}

- (void)updateOutputRectOfInterest {
    CGRect rectOfInterest = [self.videoPreviewLayer metadataOutputRectOfInterestForRect:self.boxFrame];
    _output.rectOfInterest = rectOfInterest;
}

- (void)updateOutputMetadataObjectTypes {

    AVAuthorizationStatus status = [AVCaptureDevice authorizationStatusForMediaType:AVMediaTypeVideo];
    if (status == AVAuthorizationStatusDenied ||
        status == AVAuthorizationStatusRestricted) {
        NSLog(@"请检测相机权限");
        return;
    }
    _output.metadataObjectTypes = [self arrayTranslateType];
}

- (void)updatePathWithBoxFrame:(CGRect)frame {
    [self.boxPath removeAllPoints];
    self.boxPath = nil;
    self.boxPath = [UIBezierPath bezierPathWithRect:frame];

    [self.coverPath removeAllPoints];
    self.coverPath = nil;
    self.coverPath = [UIBezierPath bezierPathWithRect:self.bounds];
    self.coverPath.usesEvenOddFillRule = YES;
    [self.coverPath appendPath:self.boxPath];
}

- (void)moveScanningLine {
    CGRect frame = self.scanningLineLayer.frame;
    CGFloat maxY = CGRectGetMaxY(self.boxFrame);
    if (self.scanningLineLayer.frame.origin.y >= maxY) {
        frame.origin.y = CGRectGetMinY(self.boxFrame);
        self.scanningLineLayer.frame = frame;
    } else {
        frame.origin.y += self.offset;
        NSTimeInterval duration = [self timerDuration];

        [UIView animateKeyframesWithDuration:duration delay:0 options:UIViewKeyframeAnimationOptionCalculationModeLinear animations:^{
            self.scanningLineLayer.frame = frame;
        } completion:nil];
    }
}

-(CGFloat)timerDuration {
    return .2;
}

- (CGFloat)offset {
    return 5;
}

- (NSArray *)arrayTranslateType {
    if (self.type == HYScanningViewTypeQR) {
        return @[AVMetadataObjectTypeQRCode];
    } else if (self.type == HYScanningViewTypeBar) {
        return @[AVMetadataObjectTypeEAN13Code,
                 AVMetadataObjectTypeEAN8Code,
                 AVMetadataObjectTypeCode128Code];
    } else if (self.type == HYScanningViewTypeQRBar) {
        return @[AVMetadataObjectTypeEAN13Code,
                 AVMetadataObjectTypeEAN8Code,
                 AVMetadataObjectTypeCode128Code,
                 AVMetadataObjectTypeQRCode];
    }

    return @[AVMetadataObjectTypeQRCode];
}

//解决AVCaptureVideoPreviewLayer调用metadataOutputRectOfInterestForRect获取RectOfInterest为零的bug
- (void)fixRectOfInterestZero {
    dispatch_async(dispatch_get_global_queue(DISPATCH_QUEUE_PRIORITY_DEFAULT, 0), ^{

        CGRect rectOfInterest = CGRectZero;

        while (CGRectIsEmpty(rectOfInterest)) {
            rectOfInterest = [self.videoPreviewLayer metadataOutputRectOfInterestForRect:self.boxFrame];
        }

        dispatch_async(dispatch_get_main_queue(), ^{
            _output.rectOfInterest = rectOfInterest;
            if (self.autoRead) {
                [self startScanning];
            }
        });
    });
}

#pragma mark - Message

- (void)startScanning {
    AVAuthorizationStatus status = [AVCaptureDevice authorizationStatusForMediaType:AVMediaTypeVideo];
    if (status == AVAuthorizationStatusDenied ||
        status == AVAuthorizationStatusRestricted) {
        NSLog(@"请检测相机权限");
        return;
    }

    if (!self.isReading) {
        self.reading = YES;
        [self.captureSession startRunning];
        self.timer.fireDate = [NSDate date];
    }
}

- (void)stopScanning {

    if (self.reading) {
        self.reading = NO;
        [self.captureSession stopRunning];
        [self.timer invalidate];
        self.timer = nil;
    }
}

#pragma mark - AVCaptureMetadataOutputObjectsDelegate

- (void)captureOutput:(AVCaptureOutput *)captureOutput didOutputMetadataObjects:(NSArray *)metadataObjects fromConnection:(AVCaptureConnection *)connection {
    if (metadataObjects && metadataObjects.count > 0) {
        AVMetadataMachineReadableCodeObject *metadataObj = metadataObjects[0];

        dispatch_async(dispatch_get_main_queue(), ^{
            [self stopScanning];
            if ([self.delegate respondsToSelector:@selector(scanningView:didFinishScanCode:)]) {
                [self.delegate scanningView:self didFinishScanCode:metadataObj.stringValue];
            }
        });
    }
}

@end

redpajama_set_name: RedPajamaGithub


Living in a new country can be a challenging and rewarding experience. Before applying for a homestay, please read the information carefully to be sure that what we offer will suit you.
Details Read all of the information in this web site to be sure our program is right for you. You are responsible for understanding all the details of the site, including the Homestay agreement. Then, decide whether you want the Traditional Homestay or the Bed & Breakfast Homestay.
Details Fill out the Application carefully and completely. The more information you give us, the better placement we can make for you. Read and sign the homestay agreement. Mail your completed and signed paperwork to our office with your check or money order, or fax it to us with your credit card information. You will receive confirmation that we have received your application within ten working days. Applications will not be processed without the fees. Late applications are considered on a case-by-case basis, and you may have to stay in a hotel (at your own expense) if you apply too late.
Details We will send you a biography that describes your homestay hosts. You are welcome to contact your hosts directly by email or phone prior to your arrival. If you are in the area, you will have an opportunity to visit them before you move in. During that meeting, please ask questions to make sure that you will be comfortable in their home. If you are not in the Puget Sound area, your first chance to meet your hosts will be at the airport when you arrive.
Details Contact ABODE to inform us of your arrival information so that we can meet your flight. It is important that you confirm this information as soon as possible. If there are any changes in your flight, or if you miss your flight to Seattle, please call the office to notify us or leave a message (do not email last minute changes). Check Arrival for details on airport pickup. Note: Airport pickup is not guaranteed if you have not informed ABODE of your arrival details at least three working days before your arrival.
Details When you move into your homestay, it is your responsibility to contact ABODE if you have any questions, concerns, or problems.
Important: If you request to move because you are not comfortable with your host, we will place you with a different host at no extra charge during the first six months of your homestay. If you will be attending a school on the academic quarter system, we ask that you stay in homestay for a minimum of three months. If you plan to move to an apartment in your first three months, please do not choose homestay. If you decide to cancel your homestay and move to an apartment in the first 30 days, please read our cancellation policy.


text:
Greece national under-23 football team represents Greece in international football competitions in Olympic Games. The selection is limited to players under the age of 23, except three overaged players. The team is controlled by the Hellenic Football Federation (HFF).

Summer Olympics

Players

Olympic Squads

1920 Summer Olympics
Head coach:  Georgios Kalafatis

1952 Summer Olympics
Head coach:  Antonis Migiakis

2004 Summer Olympics
Head coach:  Stratos Apostolakis

* Overage player.<noinclude>

Overage players in Olympic Games

Olympic match record

Goalscorers

Other appearances
1906 Intercalated Games squads – Greece

Mediterranean Games

See also
Greece national football team
Greece national under-21 football team
Greece national under-20 football team
Greece national under-19 football team
Greece national under-17 football team

External links
 Εθνική U-23
 Rec.Sport.Soccer Statistics Foundation - 1906 Summer Olympics
 FIFA: Men's Olympic Football Tournament 2004
 :el:%CE%9F%CE%BB%CF%85%CE%BC%CF%80%CE%B9%CE%B1%CE%BA%CE%AE %CE%95%CE%B8%CE%BD%CE%B9%CE%BA%CE%AE %CE%BF%CE%BC%CE%AC%CE%B4%CE%B1 %CE%95%CE%BB%CE%BB%CE%AC%CE%B4%CE%B1%CF%82 (%CF%80%CE%BF%CE%B4%CF%8C%CF%83%CF%86%CE%B1%CE%B9%CF%81%CE%BF)

European national under-23 association football teams
Football in Greece
Foot


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\section{Introduction}

A previous analysis of time-series photometry and spectroscopic material of the {\it Hipparcos} variable star HD\,21190 by \citet{2001MNRAS.326..387K} indicated a spectral classification F2\,III~SrEuSi:, making this star the most evolved Ap star known to date. Moreover, they discovered that HD\,21190 shows pulsations of $\delta$~Scuti type, which are unusual among Ap stars. According to the authors, it was also one of the most evolved $\delta$~Scuti stars known. Ultraviolet and Visual Echelle Spectrograph (UVES) high time-resolution observations of HD\,21190 were used by \citet{2008CoSka..38..411G} and \citet{2008MNRAS.384.1140G} to search for pulsational line profile variations. The authors detected in several line profiles three peaks moving smoothly towards the red with a speed of $21$\,km\,s$^{-1}$. Such a behaviour is typical for non-axisymmetric non-radial pulsations. The combination of the cool Ap spectral type and the high-degree $\delta$~Scuti pulsation made HD\,21190 an important target for a more in depth study.

Noteworthy, pulsations of $\delta$~Scuti type among Ap stars are not expected from a theoretical point of view. The models of \citet{2005MNRAS.360.1022S} led to a clear prediction that lower radial overtone pulsation modes typical in $\delta$~Scuti stars are suppressed by the magnetic field in Ap stars. On the other hand, in the Hertzsprung-Russell (H-R) diagram, the coolest members of the Ap stars, the so-called rapidly oscillating Ap stars (roAp stars) with typical pulsation periods between $6$ and $24$\,min appear in the same instability strip as the $\delta$~Scuti stars. According to theoretical considerations, magnetic Ap stars should not be observed to pulsate simultaneously in low radial overtone $p$ modes characteristic for the $\delta$~Scuti stars and high overtone $p$ modes characteristic for the roAp stars. The typical pulsation periods of $\delta$~Scuti stars range from $20$\,min to $0.3$\,d and it is assumed that the $\kappa$~mechanism acting in the second ionization zone of helium is responsible for their pulsational behaviour. Since the pulsation periods of roAp stars and $\delta$~Scuti stars partially overlap, the combination of the cool Ap spectral type and high-degree $\delta$~Scuti pulsations makes HD\,21190 an excellent target for the study of the presence of a magnetic field in its atmosphere.

\citet{2008MNRAS.386.1750K} used the FOcal Reducer low dispersion Spectrograph (FORS\,1; \citealt{Appenzeller1998}) mounted on the $8$\,m Kueyen telescope of the VLT in spectropolarimetric mode with the GRISM 600B and a slit width of $0$\farcs$4$ to achieve a spectral resolution of about $2000$. The analysis of these data revealed the presence of a rather weak longitudinal magnetic field $\left<B_z\right>=47\pm13$\,G. \citet{2016IBVS.6174....1H} re-observed HD\,21190 with FORS\,2 in 2016 March, using the same instrumental setup as \citet{2008MNRAS.386.1750K}, and detected a magnetic field in HD\,21190 at a significance level of more than $4\sigma$ ($\left<B_{\rm z}\right>_{\rm all}= -254\pm59$\,G) using for the measurements the entire spectrum, and at a significance level of more than $3\sigma$ ($\left<B_{\rm z}\right>_{\rm hyd}= -237\pm75$\,G) using the hydrogen lines. This suggests that the magnetic field is variable with rotation, as is typical for Ap stars. However, further observations are necessary to determine the magnetic field geometry and the polar field strength of this star.

We note that there is no other known case of an Ap star with a detected magnetic field that shows $\delta$~Scuti pulsations. \citet{2015MNRAS.454L..86N} recently obtained two spectropolarimetric observations of the {\em Kepler} $\delta$~Sct -- $\gamma$~Dor hybrid candidate HD\,188774. One observation showed a weak signal of about $76$\,G. However, the target did not show any Ap characteristics: the abundance analysis did reveal neither the presence of chemical peculiarity nor of chemical spots. On the other hand, indications that a few Ap stars can show a hybrid $\delta$~Sct -- $\gamma$~Dor variability were reported by several authors, e.g.\ by \cite{2011MNRAS.410..517B} who used {\em Kepler} observations of stars in the $\delta$~Scuti instability strip.

The $\delta$~Scuti star HD\,21190 is so far the only target proven to host a magnetic field along with its $\delta$~Scuti pulsation properties. Up to now, only \cite{2001MNRAS.326..387K} carried out an abundance study for this object, using low-resolution spectra. Obviously, a high-resolution spectroscopic study is necessary to confirm the presence of chemical anomalies typical for cool Ap stars and to improve our understanding of the interplay between the magnetism and the physical processes taking place in the atmospheres of pulsating stars.

In this work, our recent HARPS observations \citep{mayor2003} are used to characterize the abundances of $24$ chemical elements in the atmosphere of HD\,21190. In addition to observations of HD\,21190, we also obtained HARPS observations of the visual nearby companion CPD\,$-$83$^{\circ}$\,64B at an angular distance of about $19$\arcsec{}. The atmospheric parameters and chemical abundances of the companion were also determined. Additionally, the question whether HD\,21190 and CPD\,$-$83$^{\circ}$\,64B have a common proper motion and form a physical wide binary system has not been discussed in the past. In the following sections we present all available astrometric measurements obtained for both stars including those from {\it Hipparcos} and {\it Gaia} to investigate their proper motions and space velocities and discuss the results of our chemical abundance analysis obtained using high-resolution HARPS spectra.

\section{Astrometric measurements}
\label{sect:astro}

The two stars HD\,21190 and CPD\,$-$83$^{\circ}$\,64B are listed in the Washington Double Star (WDS) catalogue \citep{mason01} with a first satisfactory observation of their angular separation ($\sim15$\arcsec{}) in 1835. In the recently published catalogue of $\delta$~Scuti stars in binaries, \citet{liakos16} included CP\,Oct (HD\,21190) as a visual binary with an unspecified orbital period. In the following analysis of available astrometric measurements, we refer to HD\,21190 and CPD\,$-$83$^{\circ}$\,64B as A and B, respectively.

\subsection{Common proper motion}
\label{SubSect_cpm}

\begin{table}
\caption{Proper motions of HD\,21190 (A) and CPD\,$-$83$^{\circ}$\,64B (B).}
\label{table_pm}
\centering
\begin{tabular}{cccl}
\toprule
\multicolumn{1}{c}{Object} &
\multicolumn{1}{c}{$\mu_{\alpha}\cos{\delta}$ (error)} &
\multicolumn{1}{c}{$\mu_{\delta}$ (error)} &
\multicolumn{1}{c}{Source} \\
&
\multicolumn{1}{c}{[mas/year]} &
\multicolumn{1}{c}{[mas/year]} &
\\
\midrule
A & $-8.8$  (2.6) & $+21.5$  (1.0)  & ACT$^{a}$ \\
\smallskip
B & $-6.5$  (1.6) & $+16.4$  (5.2)  & ACT$^{a}$ \\
A & $-8.8$  (2.0) & $+19.2$  (1.8)  & TRC$^{a}$ \\
\smallskip
B & $-7.2$  (2.3) & $+14.9$  (3.6)  & TRC$^{a}$ \\
A & $-8.1$  (1.6) & $+19.4$  (1.6)  & SPM4$^{b}$ \\
\smallskip
B & $-3.6$  (1.2) & $+35.5$  (1.3)  & SPM4$^{b}$ \\
A & $-5.5$  (0.8) & $+19.1$  (0.8)  & UCAC4$^{c}$ \\
\smallskip
B & $-3.4$  (4.5) & $+37.3$  (5.8)  & UCAC4$^{c}$ \\
A & $-6.1$  (2.1) & $+22.4$  (1.4)  & this work$^{d}$ \\
\smallskip
B & $-7.6$  (1.9) & $+19.6$  (1.5)  & this work$^{d}$ \\
\midrule
A & $-4.1$  (0.9) & $+19.9$  (0.9)  & Tycho-2$^{a}$ \\
A & $-4.6$  (0.6) & $+22.4$  (0.7)  & {\it Hipparcos}$^{e,f}$ \\
A & $-5.56$ (0.04)& $+22.15$ (0.05) & TGAS$^{e,g}$ \\
B & $-6.5$  (0.9) & $+21.8$  (0.9)  & UCAC5$^h$ \\
\bottomrule
\end{tabular}
\begin{minipage}{0.45\textwidth}
{\bf Notes:}\\
$^{a}$ {Based on very old photographic plates (AC2000) and Tycho data with a large epoch difference of about 93 years.}\\
$^{b}$ {Combining photographic plates from 1973 and CCD observations from 2007 with the Yale Southern Observatory's double-astrograph.}\\
$^{c}$ {Combining photographic plates from 1973 of Yale Southern Observatory's double-astrograph and modern UCAC CCD observations.}\\
$^{d}$ {Linear solution using the position measurements at three recent epochs only (without photographic plate measurements): Tycho \citep{esa97} from 1991, 2MASS from 1999, and {\it Gaia}  DR1 \citep{gaia16a,gaia16b} from 2015.}\\
$^{e}$ {Determined in combined proper motion and parallax solution.}\\
$^{f}$ {Revised {\it Hipparcos} solution by \citet{vanleeuwen07}.}\\
$^{g}$ {Based on Tycho-2 position from 1991 and the first 14 months of {\it Gaia} observations \citep{gaia16a,gaia16b,lindegren16}.}\\
$^{h}$ {Based on Gaia DR1 and re-reduced UCAC CCD observations using TGAS reference stars.}
\end{minipage}
\end{table}

The question whether A and B share a common proper motion had until recently no clear answer. While both stars can be found in the Tycho catalogue \citep{esa97}, only A has a proper motion in the Tycho-2 catalogue \citep{2000A&A...355L..27H}, which we list in the lower part of Table~\ref{table_pm}. But both A and B were measured on the old photographic plates used for the Astrographic Catalogue (AC2000; \citealt{urban98a}). Consequently, A and B have long-term proper motions in the ACT \citep[Astrographic Catalog/Tycho][]{urban98b} and Tycho Reference Catalogue (TRC; \citealt{hog98}). The ACT and TRC proper motions given in Table~\ref{table_pm} represent two independent reductions of the same AC2000 and Tycho data. Tycho-2 involved not only these data but also intermediate epochs from other ground-based astrometric catalogues. Probably, some of those were problematic for the proper motion solution of B. As one can see, the ACT and TRC proper motion components of A and B agree within the given errors, with B having smaller values and larger errors in declination direction.

On the other hand, the Southern Proper Motion Program (SPM4; \citealt{girard11}) and the Fourth US Naval Observatory CCD Astrograph Catalogue (UCAC4; \citealt{zacharias13}) showed a disagreement in the proper motion components of A and B in declination (see Table~\ref{table_pm}). In these two catalogues, which are only partly independent as both are based on the same first-epoch data, B has a much larger proper motion than A in declination direction. This difference is three times larger than the already relatively large errors given for B. We assume that A and B were well separated and measured with the different modern CCD observations used as second epochs for SPM4 and UCAC4, respectively. The very large and similar proper motion of B in declination may be caused by a centroiding problem on the same photographic plates of the Yale Southern Observatory double-astrograph that served as first epoch data for both catalogues. We also mention that there is a smaller discrepancy seen for the SPM4 proper motion components of A and B in right ascension, which do also not agree within their errors.

To investigate further the questioned common proper motion of A and B, we used the presumably most accurate positional data, excluding any photographic plates, for our own proper motion measurements. The first data release of {\it Gaia}  ({\it Gaia}  DR1; \citealt{gaia16a,gaia16b,lindegren16}) provided the most accurate positions for both A and B. Due to the fact that B was not included in Tycho-2, it has unfortunately no proper motion in the Tycho-{\it Gaia} Astrometric Solution (TGAS) of {\it Gaia} DR1. However, we can combine the {\it Gaia} DR1 positions with those in the Tycho catalogue \citep{esa97} and use in addition the intermediate epoch positions given in the Two Micron All Sky Survey (2MASS; \citealt{skrutskie06}). For object A, we obtained a very similar proper motion as compared to its TGAS measurement (see Table~\ref{table_pm}). Our proper motion of B agrees within the errors with our proper motion of A. Compared to the internal agreement between A and B proper motion components in the ACT and TRC solutions, we achieved an even better agreement. Our A--B difference of the larger component in declination direction is smaller than in all proper motion solutions involving photographic plate measurements. When we included photographic positions from the AC2000 and the Southern Hemisphere Catalogue of Bordeaux \citep{rousseau96} in our proper motion determination, we arrived at values similar to those from the ACT and TRC. Our preferred results for the pair A$+$B, without using any photographic data (Table~\ref{table_pm}), are consistent with a common proper motion of A and B. Interestingly, the new UCAC5 catalogue \citep{2017arXiv170205621Z} provides an accurate proper motion of B that agrees very well with the TGAS proper motion of A (Table\,\ref{table_pm}), whereas the UCAC5 proper motion of A is unreliable (zero number of observations used for mean UCAC5 position).

\subsection{No signs of orbital motion?}
\label{SubSect_orb}

We assume that the common proper motion of A and B indicates a wide binary system. Then we can use the {\it Hipparcos} and {\it Gaia} measurements of the parallax of A to derive a distance and the projected physical separation of the system components. The TGAS parallax of A ($6.07\pm0.29$\,mas) is significantly larger than the almost identical values in the original ($4.16\pm0.63$\,mas; \citealt{esa97}) and revised ($4.17\pm0.60$\,mas; \citealt{vanleeuwen07}) {\it Hipparcos} catalogues, respectively. The formal distance is therefore reduced from about $240$\,pc according to {\it Hipparcos} to about $165$\,pc according to the TGAS. The angular separation of A and B in the TGAS is $19.388$\arcsec{}, corresponding to a projected physical separation of about $3200$~AU.

The apparent magnitudes of A and B ($V=7.604$ and $V=10.815$, respectively; \citealt{kharchenko01}) and the assumed common distance from TGAS lead to absolute magnitudes of about $M_V=1.5\pm0.1$ and $M_V=4.7\pm0.1$, respectively. These values are comparable with those of an A1 main sequence star (Sirius) and the Sun, respectively. With a spectral type of F2\,III SrEuSi: \citep{2001MNRAS.326..387K}, the $\delta$~Scuti star A is expected to be about $0.8$~mag brighter and about $1.3$ times more massive than a normal main sequence star of the same spectral type \citep{starikova79}. Therefore, it should also have a mass similar to that of Sirius. For estimating the orbital period of the system A$+$B, we assume two and one solar masses for the two components, respectively.

\begin{figure*}
\centering
\includegraphics[width=5in]{figure_HD21190_AB_sep_pa.eps}
\caption{Measured separation (bottom) and position angle (top) between A and B over time. Blue symbols and labels mark (with increasing time) data from AC2000, the Catalogue of Components of Double \& Multiple stars (CCDM; \citealt{dommanget00}), Yale observatory (\citealt{lu71} listed in \citealt{wycoff06}), Bordeaux \citep{rousseau96}, UCAC4 double stars \citep{hartkopf13}, SPM4, and the Wide-field Infrared Survey Explorer (WISE; \citealt{wright10}) all-sky catalogue. Red symbols and labels represent the most accurate data from Tycho, 2MASS, and {\it Gaia} (also indicated by the red dotted line). The green lines show the maximum expected effects over a $100$ year baseline (see text). }
\label{fig:sep_pa}
G\end{figure*}

In the simple case of a circular orbit in the plane of the sky, we estimate an orbital period of about 100\,000\,years and a differential proper motion due to orbital motion of B with respect to A of only about $2$~mas/year. This is comparable to our measured difference in the proper motion of A and B in declination but also to our proper motion measurement errors (Table~\ref{table_pm}). Over a time baseline of $100$ years, we would not yet expect to see changes in the separation and/or position angle between A and B, as these are estimated to be smaller than $40$~mas (for an edge-on circular orbit) and $0.7$\,degrees (for a circular orbit in the plane of the sky), respectively. These values are smaller than most pre-{\it Gaia} measurement errors. In Fig.~\ref{fig:sep_pa}, we show all available measurements of the separation and position angle over time (except for the probably most unreliable WDS data from 1835, which fall well outside of the plotted range for the separations and position angles). The expected largest possible effects over $100$ years are shown in green. Error bars were only available for the UCAC4 double star data \citep{hartkopf13}. They should be of similar size (or even larger at early epochs) for all other measurements, except for the presumably most accurate red data points, where they could be comparable to the symbol size. As expected, there is no clear trend but large scatter, especially at early epochs. In particular, the {\it Gaia}, 2MASS, and Tycho data, plotted in red, confirm a constant separation, whereas a constant position angle is in addition supported by the Yale and Bordeaux data.

\subsection{Space velocity}
\label{SubSect_uvw}

The tangential velocity of A is according to the TGAS $17.9\pm0.9$\,km\,s$^{-1}$, which is smaller than the radial velocity measured for B in the 5th data release of the Radial Velocity Experiment (RAVE; \citealt{2017AJ....153...75K}), $+34.0\pm1.3$\,km\,s$^{-1}$. Our own radial velocity measurements (Sect.~\ref{sect:mod}) of $+25\pm3$\,km\,s$^{-1}$ and $+19.0\pm0.5$\,km\,s$^{-1}$, respectively for A and B, are significantly smaller than the RAVE radial velocity of B. We prefer our own radial velocity measurements. The HARPS spectra with the resolution of $115,000$ have much better quality than RAVE spectra that have resolution about $7,500$. The radial velocity of the pulsating primary is not easy to determine accurately using low-resolution RAVE spectra due to the large $v\sin i$ value and spectral variability caused by pulsations. These pulsations have impact on the shape and position of spectral lines. The radial velocity for the primary was calculated using the LSD (Least-Squares Deconvolution) profile in the HARPS Stokes I spectrum. The radial velocity of the secondary was estimated in a similar manner. Using the TGAS parallax measured for A for both components, our own radial velocity, and proper motion measurements for A and B, respectively, we calculated the heliocentric Galactic space velocities $UVW$ according to \citet{johnson87}. These velocity components are defined in a right-handed coordinate system so that they are positive in the direction of the Galactic centre ($U$), of Galactic rotation ($V$), and to the North Galactic Pole ($W$). All three space velocity components of the two stars, $(U,V,W)_A=(-1\pm2,-14\pm3,-28\pm2)$\,km\,s$^{-1}$ and $(U,V,W)_B=(-1\pm1,-9\pm1,-24\pm1)$\,km\,s$^{-1}$, agree to within a few km\,s$^{-1}$. The differences are comparable to or only slightly larger than the individual errors. The relatively large negative $W$-velocity and the Galactic coordinates of $(l,b)\approx(299,-32)$\,degrees indicate a current direction of motion of the pair mainly away from the Galactic plane. According to the TGAS parallax of A, the current distance from the plane is about $87$\,pc. Both kinematics and location fall in the range of the vertical velocity dispersion ($25\pm5$\,km\,s$^{-1}$) and scale height ($300\pm50$\,pc) of the (old) thin disk \citep{BlandHawthorn16}, respectively. To summarize, in spite of the high angular separation between HD\,21190 and CPD\,$-$83$^{\circ}$\,64B, the presented analysis of all available astrometric data indicates that both stars form a physical binary system.

\section{Stellar parameters and abundance determination}
\label{sect:mod}

HARPS observations were carried out on two consecutive nights: the primary HD\,21190 was observed on $2016$ June $15$, while the secondary was observed on $2016$ June $16$. The obtained observations have a signal-to-noise ratio (S/N) of about $100$ for the primary and of about $70$ for the secondary in the Stokes~$I$ spectra and a resolving power of about $R = 115\,000$. They cover the spectral range  $3780-6910$\,\AA{}, with a small gap between $5259$ and $5337$\,\AA{}. The reduction was performed using the HARPS data reduction software available at the $3.6$\,m telescope in Chile.

\begin{figure*}
\centering
\includegraphics[width=7in]{figure-balmerF.ps}
\caption[]{Observed Balmer lines H$\gamma$, H$\beta$, and H$\alpha$ (black) and best fitted synthetic profiles (red) for HD\,21190. The sensitivity of Balmer lines to effective temperature was use to determine ${T}_{\rm eff} = 6900 \pm 100$\,K for this star. }
\label{fig:balmer_f}
\end{figure*}

\begin{figure*}
\centering
\includegraphics[width=7in]{figure-balmerG.ps}
\caption[]{Observed Balmer lines H$\beta$ and H$\alpha$  (black) and best fitted synthetic profiles (red) for CPD\,$-$83$^{\circ}$\,64B. The sensitivity of Balmer lines to effective temperature was use to determine ${T}_{\rm eff} = 5900 \pm 100$\,K for this star.}
\label{balmer_g}
\end{figure*}

\begin{figure}
\centering
\includegraphics[width=3.4in]{figure-strongG.ps}
\caption[]{Observed strong lines (black) and best fitted synthetic profiles (red) for CPD\,$-$83$^{\circ}$\,64B. Lines of \ion{Mg}{i}\,b ($5183.62$\,\AA{}), \ion{Na}{i}\,D1 ($5889.95$\,\AA{}) and D2 ($5895.92$\,\AA{}), and \ion{Ca}{i} ($6162.18$\,\AA{}) used to measure the surface gravity $4.3 \pm 0.1$ of CPD\,$-$83$^{\circ}$\,64B. }
\label{strong_g}
\end{figure}

Different independent sources were used to obtain stellar parameters of both components. Effective temperatures (${T}_{\rm eff}$) and surface gravities ($\log g$) calculated from calibrations of photometric indices and from the spectral energy distribution (SED) were treated as initial parameters for the spectroscopic analysis. Further, a synthesis of hydrogen line profiles as well as the requirement of ionization and excitation equilibria in the Fe lines were used to get ${T}_{\rm eff}$, $\log g$, and microturbulence ($\xi_{\rm t}$) for the F-type primary whereas for the G-type secondary CPD\,$-$83$^{\circ}$\,64B the atmospheric parameters were obtained from Balmer lines, strong \ion{Na}{i}\,D1 ($5889.95$\,\AA{}) and D2 ($5895.92$\,\AA{}), \ion{Ca}{i} ($6162.18$\,\AA{}), \ion{Mg}{i}\,b ($5183.62$\,\AA{}), and \ion{Fe}{i} lines.

To calculate the necessary synthetic spectra, we used atmospheric models (plane-parallel, hydrostatic and radiative equilibrium, 1-dimensional) and synthetic spectra computed with the line-blanketed, local thermodynamical equilibrium (LTE) {\small\sc ATLAS\,9} code \citep{1993KurCD..13.....K}. The grid of atmospheric models was calculated for effective temperatures from $5000$ to $6200$\,K with a step of $50$\,K, and from $6200$ to $12000$\, with a step of 100\,K. Surface gravities from $2.0$ to $4.6$\,dex with a step of $0.1$\,dex, microturbulence velocities between $0.0$ and $6.0$\,km\,s$^{-1}$ with a step of $0.1$\,km\,s$^{-1}$, and metallicities [M/H] equal to $0.0$, $+0.5$ and $+1.0$ were considered for each temperature. Appropriate synthetic spectra were computed with the {\small\sc SYNTHE} code \citep{1993KurCD..18.....K}. Both codes, {\small\sc ATLAS9} and {\small\sc SYNTHE}, were ported to GNU/Linux by \citet{sbordone}. The line list used was that of Robert Kurucz\footnote{http://kurucz.harvard.edu} \citep{2014dapb.book...63K}.

\subsection{Atmospheric parameters of the primary component HD\,21190}

For HD\,21190, Str\"{o}mgren {\it uvby$\beta$} \citep{1998A&AS..129..431H}, Johnson $BV$ \citep{2000A&A...355L..27H}, and 2MASS $JHK$ \citep{2003yCat.2246....0C} photometry is available and was used to determine the initial parameters.

The $uvby\beta$ indices were taken from the General Catalogue of Photometric Data (GCPD) \citep{1998A&AS..129..431H}\footnote{http://obswww.unige.ch/gcpd/gcpd.html}. Atmospheric parameters were determined using the {\small\sc UVBYBETA} code written by \citet{1985MNRAS.217..305M} and corrected by \citet{1993A&A...268..653N}. We obtained the effective temperature $6900 \pm 100$\,K and surface gravity $3.63 \pm 0.17$\,dex. The errors of ${T}_{\rm eff}$ and $\log g$ were calculated taking into account the uncertainties of the photometric indices and the internal error of the method.

To calculate atmospheric parameters from the $(V-K)$ index, knowledge of the interstellar reddening parameter is necessary. The colour excess $E(B-V) = 0.005 \pm 0.003$\,mag was derived using the relation between the equivalent width of the Na\,D$_{2}$ line ($5889.95$\,\AA{}) and the $E(B-V)$\,mag \citep{1997A&A...318..269M}. The $(V-K)$ index was determined on the basis of the $K$ magnitudes from the 2MASS catalogue \citep{2003yCat.2246....0C} and the $V$ magnitudes from the GCPD catalogue. It was used to determine ${T}_{\rm eff}$ from the \citet{2006A&A...450..735M} relation. We used the relation $E(V-K) = 2.72 E(B-V)$ from \citet{1979ARA&A..17...73S}. In the calculations we assumed $\rm{[Fe/H]} = 0.0$ and $\log g = 4.0$. This calibration has only a weak dependence on $\log g$ and metallicity. The obtained effective temperature is equal to $6830 \pm 70$\,K. We determined the uncertainty of ${T}_{\rm eff}$ by changing $\log g$ by $0.2$ and [Fe/H] by $0.2$\,dex.

The stellar effective temperature was also determined from the spectral energy distribution (SED), constructed from the photometry used before ($V$, $uvby$, $2MASS$) supplemented by $B$, $U$, $R$ and $I$ magnitudes adopted from GCPD database. Effective temperatures were determined by fitting \citet{1993KurCD..13.....K} model fluxes to the de-reddened SED. The metallicity [M/H] is poorly constrained by our SED, therefore we fixed [M/H]\,$=0.0$\,dex. The model fluxes were convolved with photometric filter response functions. From this method, we obtained an effective temperature $7100 \pm 200$\,K and $\log g = 3.70 \pm 0.20$. The uncertainties of the derived parameters were estimated taking into account the errors of the photometric colours, $E(B-V)$, and the assumed error $0.1$ for [M/H].

The value of ${T}_{\rm eff} = 6900 \pm 100$\,K was obtained using the sensitivity of the Balmer H$\alpha$, H$\beta$ and H$\gamma$ lines to effective temperature. Hydrogen lines are not good indicators of $\log g$ for effective temperatures lower than about $8000$\,K \citep{2014dapb.book...85S}. Therefore, the surface gravity was assumed to be equal to $4.0$\,dex. We calculated synthetic Balmer lines assuming solar metallicity. We used an iterative approach to minimize the differences between the observed and the synthetic Balmer profiles \citep[see][]{2004A&A...425..641C}. The uncertainties of the derived values were estimated taking into account uncertainties resulting from the validity of the normalisation. Since hydrogen lines in high-resolution HARPS spectra extend over adjacent orders, to improve the normalization, we also used recent FORS\,2 low-resolution observations of HD\,21190. To estimate the error of ${T}_{\rm eff}$, we took into account the differences in the determined ${T}_{\rm eff}$ values from the separate Balmer lines. In Fig.~\ref{fig:balmer_f} we present the observed Balmer lines together with the synthetic profiles.

The photometric methods, SED, and Balmer line analysis provided input atmospheric parameters ${T}_{\rm eff}$ and $\log g$ for the iron line investigation. In the case of HD\,21190, the analysis of individual lines was impossible because of relatively high rotation velocity, hence we assumed that the iron abundances obtained from different spectral regions are the same for the correct ${T}_{\rm eff}$, $\log g$ and $\xi_{\rm t}$ values. We were looking for ${T}_{\rm eff}$ in the range $6700-7200$\,K, $\log g$ from $3.0$ to $3.8$, and $\xi_{\rm t}$ from $1.5$ to $3.5$\,{km\,s}$^{-1}${}. The final effective temperature $6900 \pm 100$\,K, surface gravity $3.6 \pm 0.2$\,dex and microturbulence $2.4 \pm 0.2$\,{km\,s}$^{-1}${} were used for the elemental composition determination of HD\,21190. A moderate $v\sin i = 74 \pm 3$\,{km\,s}$^{-1}${} was measured in the HARPS spectrum.

\begin{table*}
\caption{Atmospheric parameters of HD\,21190 (A) and CPD\,$-$83$^{\circ}$\,64B (B) determined from photometric and spectroscopic methods (see the first column).}
\label{table_atm}
\centering
\begin{tabular}{ll}
\toprule
\multicolumn{2}{c}{HD\,21190} \\
\midrule
Str\"{o}mgren {\it uvby$\beta$}          &${T}_{\rm eff} = 6900 \pm 100$\,K, $\log g = 3.63 \pm 0.17$                \\
2MASS $(V-K)$ index                      &${T}_{\rm eff} = 6830 \pm 70$\,K; $\log g$ and [Fe/H] assumed              \\
SED                                      &${T}_{\rm eff} = 7100 \pm 200$\,K, $\log g = 3.70 \pm 0.20$, [M/H] assumed \\
Balmer H$\alpha$, H$\beta$ and H$\gamma$ &${T}_{\rm eff} = 6900 \pm 100$\,K; $\log g$ and [M/H] assumed              \\
Fe lines                                 &${T}_{\rm eff} = 6900 \pm 100$\,K, $\log g = 3.60 \pm 0.20$,               \\
                                         &$\xi_{\rm t} = 2.4 \pm 0.2$\,{km\,s}$^{-1}$, $v\sin i = 74 \pm 3$\,{km\,s}$^{-1}$\     \\
\midrule
\multicolumn{2}{c}{CPD\,$-$83$^{\circ}$\,64B} \\
\midrule
Balmer H$\beta$ and H$\alpha$                                              & ${T}_{\rm eff} = 5900 \pm 100$\,K; $\log g$ and [M/H] assumed \\
Strong lines: \ion{Na}{i}\,D1 ($5889.95$\,\AA{}) and D2 ($5895.92$\,\AA{}),& $\log g = 4.3 \pm 0.1$, ${T}_{\rm eff}$, $\xi_{\rm t}$, and [M/H] assumed     \\
\ion{Ca}{i} ($6162.18$\,\AA{}), and \ion{Mg}{i}\,b ($5183.62$\,\AA{})      &    \\
Fe lines                                                                   & ${T}_{\rm eff} = 5850 \pm 50$\,K, $\xi_{\rm t} = 1.0\pm0.2$\,{km\,s}$^{-1}$, \\
                                                                           & $v\sin i{} = 3.1 \pm 0.7$\,{km\,s}$^{-1}$; $\log g$ assumed   \\
\bottomrule
\end{tabular}
\end{table*}

\begin{table*}
\centering
\caption{Abundances of chemical elements for both components. An average value is given; the standard deviations were calculated only if the number of analysed lines is greater than two. The number of the analysed lines is also indicated.}
\label{tab:abundances}
\begin{tabular}{lrcrcccrcccc}
\toprule
El. &Atomic & \vline & No. of & Average   & Standard  & \vline & No. of & Average   & Standard  & \vline & Solar  \\
    &number & \vline & lines  & abundance & deviation & \vline & lines  & abundance & deviation & \vline & abundances$^*$ \\
\midrule
 & & \vline & \multicolumn{3}{c}{HD\,21190}&  \vline & \multicolumn{3}{c}{CPD\,$-$83$^{\circ}$\,64B} & \vline \\
\midrule
 C  & $ 6$  & \vline & $ 7 $& $ 8.67 $& $ 0.12 $ & \vline &$   1  $&$  8.71 $&$  -   $ & \vline & $8.43\pm0.05$  \\
 Na & $11$  & \vline & $ 3 $& $ 6.60 $& $ 0.28 $ & \vline &$   9  $&$  6.42 $&$  0.22$ & \vline & $6.21\pm0.04$  \\
 Mg & $12$  & \vline & $ 7 $& $ 7.81 $& $ 0.37 $ & \vline &$   6  $&$  7.62 $&$  0.18$ & \vline & $7.59\pm0.04$  \\
 Si & $14$  & \vline & $14 $& $ 7.68 $& $ 0.21 $ & \vline &$  24  $&$  7.58 $&$  0.25$ & \vline & $7.51\pm0.03$  \\
 S  & $16$  & \vline & $ 4 $& $ 7.61 $& $ 0.01 $ & \vline &$   1  $&$  7.28 $&$  -   $ & \vline & $7.12\pm0.03$  \\
 Ca & $20$  & \vline & $13 $& $ 6.94 $& $ 0.22 $ & \vline &$  36  $&$  6.51 $&$  0.21$ & \vline & $6.32\pm0.03$  \\
 Sc & $21$  & \vline & $ 7 $& $ 3.69 $& $ 0.19 $ & \vline &$   8  $&$  3.10 $&$  0.05$ & \vline & $3.16\pm0.04$  \\
 Ti & $22$  & \vline & $29 $& $ 5.21 $& $ 0.25 $ & \vline &$ 124  $&$  4.90 $&$  0.16$ & \vline & $4.93\pm0.04$  \\
 V  & $23$  & \vline & $ 4 $& $ 4.39 $& $ 0.24 $ & \vline &$  27  $&$  3.92 $&$  0.16$ & \vline & $3.89\pm0.08$  \\
 Cr & $24$  & \vline & $32 $& $ 5.98 $& $ 0.18 $ & \vline &$ 134  $&$  5.68 $&$  0.15$ & \vline & $5.62\pm0.04$  \\
 Mn & $25$  & \vline & $ 8 $& $ 5.09 $& $ 0.21 $ & \vline &$  39  $&$  5.36 $&$  0.15$ & \vline & $5.42\pm0.04$  \\
 Fe & $26$  & \vline & $ 80$& $ 7.71 $& $ 0.13 $ & \vline &$ 599  $&$  7.56 $&$  0.16$ & \vline & $7.47\pm0.04$  \\
 Co & $27$  & \vline & $ 3 $& $ 5.73 $& $ 0.15 $ & \vline &$  27  $&$  4.94 $&$  0.18$ & \vline & $4.93\pm0.05$  \\
 Ni & $28$  & \vline & $44 $& $ 6.82 $& $ 0.16 $ & \vline &$ 134  $&$  6.30 $&$  0.17$ & \vline & $6.20\pm0.04$  \\
 Cu & $29$  & \vline & $ 2 $& $ 4.14 $& $ -    $ & \vline &$   3  $&$  4.13 $&$  0.12$ & \vline & $4.18\pm0.05$  \\
 Zn & $30$  & \vline & $ 2 $& $ 4.46 $& $ -    $ & \vline &$   3  $&$  4.76 $&$  0.08$ & \vline & $4.56\pm0.05$  \\
 Ge & $32$  & \vline & $   $& $      $& $      $ & \vline &$   1  $&$  3.84 $&$   -  $ & \vline & $3.63\pm0.07$  \\
 Sr & $38$  & \vline & $ 1 $& $ 3.97 $& $ -    $ & \vline &$   2  $&$  3.54 $&$   -  $ & \vline & $2.83\pm0.06$  \\
 Y  & $39$  & \vline & $ 7 $& $ 3.08 $& $ 0.42 $ & \vline &$  12  $&$  2.58 $&$  0.22$ & \vline & $2.21\pm0.05$  \\
 Zr & $40$  & \vline & $ 3 $& $ 3.16 $& $ 0.27 $ & \vline &$   4  $&$  2.69 $&$  0.25$ & \vline & $2.59\pm0.04$  \\
 Ru & $44$  & \vline & $   $& $      $& $      $ & \vline &$   1  $&$  1.91 $&$  -   $ & \vline & $1.75\pm0.08$  \\
 Ba & $56$  & \vline & $ 2 $& $ 3.74 $& $ -    $ & \vline &$   5  $&$  2.53 $&$  0.12$ & \vline & $2.25\pm0.07$  \\
 La & $57$  & \vline & $ 3 $& $ 2.09 $& $ 0.17 $ & \vline &$   4  $&$  1.44 $&$  0.11$ & \vline & $1.11\pm0.04$  \\
 Ce & $58$  & \vline & $ 1 $& $ 3.30 $& $ -    $ & \vline &$   7  $&$  1.71 $&$  0.25$ & \vline & $1.58\pm0.04$  \\
 Nd & $60$  & \vline & $13 $& $ 2.29 $& $ 0.26 $ & \vline &$  24  $&$  1.70 $&$  0.27$ & \vline & $1.42\pm0.04$  \\
 Sm & $62$  & \vline & $   $& $      $& $      $ & \vline &$  10  $&$  1.69 $&$  0.28$ & \vline & $0.95\pm0.04$  \\
 Eu & $63$  & \vline & $ 1 $& $ 1.69 $& $ -    $ & \vline &$   1  $&$  0.60 $&$  -   $ & \vline & $0.52\pm0.04$  \\
 Dy & $66$  & \vline & $   $& $      $& $      $ & \vline &$   1  $&$  1.87 $&$  -   $ & \vline & $1.10\pm0.04$  \\
\bottomrule
\end{tabular}
\begin{minipage}{\textwidth}
{\bf Notes:}\\
$^*$ Solar abundances:
C -- \citet{2009ARA&A..47..481A};
Na--Ca -- \citet{2015A&A...573A..25S};
Sc--Ni -- \citet{2015A&A...573A..26S};
Cu--Dy -- \citet{2015A&A...573A..27G}.
\end{minipage}
\end{table*}

\begin{figure*}
\includegraphics[width=7in]{figure_FG.ps}
\caption[]{Chemical abundances of HD\,21190 (upper panel) and CPD\,$-$83$^{\circ}$\,64B (lower panel) compared to solar values, $\log\epsilon({\rm El})-\log\epsilon({\rm El})_\odot$ (see Table~\ref{tab:abundances}). The values determined from more than two lines are shown as filled circles, whereas those with less lines are denoted as open circles. The error bars are standard deviations, calculated in cases where at least three lines or blends were used to determine the abundance of the given element.}
\label{abundances-f}
\end{figure*}

The summary of obtained atmospheric parameters is shown in Table\,\ref{table_atm}. We determined consistent results from every method we use for the atmospheric parameter determination. The $\log g$ parameter is more problematic, as only the {\small\sc UVBYBETA} code and SED analysis give values for the surface gravity. In comparison with the $uvby\beta$ photometry, the SED analysis gives similar value of $\log g = 3.70$. To determine the proper value of $\log g$ from the last method, a well constructed SED is necessary, especially in the region of the Balmer jump. The value $3.60$\,dex obtained from the iron line analysis is consistent with the $\log g$ from the {\small\sc UVBYBETA} code and with the SED investigation.

The obtained atmospheric parameters of HD\,21190 are also consistent with the values obtained in a few previous studies. \citet{2012MNRAS.427..343M} used various surveys to fit the SED and obtained an effective temperature of $6817$\,K. \citet{2011A&A...530A.138C} give ${T}_{\rm eff} = 7030 \pm 120$\,K derived via the InfraRed Flux Method, and $\log g = 3.49$, computed from the fundamental definition involving ${T}_{\rm eff}$, the bolometric flux, and mass. \citet{2001MNRAS.326..387K} derived an effective temperature $6780 \pm 100$\,K and a surface gravity $3.34 \pm 0.15$\,dex using a multidimensional downhill simplex technique developed by \citet{2001AJ....121.2159G}, that simultaneously finds the best fit to the observed spectrum and fluxes determined from photometry from a grid of synthetic spectra and fluxes computed using model atmospheres from the stellar atmosphere program {\small\sc ATLAS\,9} \citep{1993KurCD..13.....K}.

\subsection{Atmospheric parameters of the secondary component CPD\,$-$83$^{\circ}$\,64B}

Only Johnson $BV$ and 2MASS $JHK$ colours are available for the secondary component CPD\,$-$83$^{\circ}$\,64B. These photometries can be used only for effective temperature determination, and require the knowledge of colour excess, surface gravity, and metallicity. Therefore we decided to use various spectral lines to determine atmospheric parameters of secondary component.

A value of ${T}_{\rm eff} = 5900 \pm 100$\,K was obtained using the sensitivity of the Balmer H$\beta$ and H$\alpha$ lines to the effective temperature (see Fig.\,\ref{balmer_g}). The surface gravity was assumed to be equal to $4.0$\,dex, as this parameter has no influence on this analysis. The uncertainties of the derived values were estimated taking into account the uncertainties resulting from the validity of the normalisation. We calculated them taking into account the differences in the determined ${T}_{\rm eff}$ values from the separate Balmer lines.

Strong lines like \ion{Na}{i}\,D1 ($5889.95$\,\AA{}) and D2 ($5895.92$\,\AA{}), \ion{Ca}{i} ($6162.18$\,\AA{}), and \ion{Mg}{i}\,b ($5183.62$\,\AA{}) show strong pressure-broadened wings in the spectra of cool stars, and can be used for $\log g$ determination \citep{gray}. However, the influence of the effective temperature and the abundances have to be taken into account. We assumed ${T}_{\rm eff} = 5900\pm100$\,K as obtained from the Balmer lines, solar metallicity [M/H], and a microturbulence $\xi_{\rm t} = 1.0\pm0.2$\,{km\,s}$^{-1}${}. A surface gravity $4.3 \pm 0.1$ was determined from the strong lines mentioned before. The quality of the fitting can be seen in Figure\,\ref{strong_g}. The uncertainty of $\log g$ was determined by changing the assumed ${T}_{\rm eff}$, [M/H], and $\xi_{\rm t}$ in their error bars.

The final $\log g$ was adopted from the strong line analysis, but the final ${T}_{\rm eff}$ was determined from the dependency of the iron abundance on the excitation potential of the \ion{Fe}{i} lines. Analysing the iron lines, we proceeded according to the following scheme: first, $\xi_{\rm t}$ was adjusted until there was no correlation between iron abundances and line depths for the \ion{Fe}{i} lines; second, ${T}_{\rm eff}$ was changed until there was no trend in the iron abundance versus excitation potential for the \ion{Fe}{i} lines. The obtained value $5850 \pm 50$\,K is consistent with those from the Balmer line investigation and $\xi_{\rm t} = 1.0\pm0.2$\,{km\,s}$^{-1}${} is typical for G type stars. Simultaneously, we obtained $v\sin i{} = 3.1 \pm 0.7$\,{km\,s}$^{-1}${}.

\subsection{Chemical abundances of both components}
\label{subsect:chem}

For both stars, the analysis of all available metal lines lets us derive their chemical compositions. We analysed the metal lines using the spectrum synthesis method, relying on an efficient least-squares optimisation algorithm \citep[for more information see][]{2015MNRAS.450.2764N}. The chosen method allows us a simultaneous determination of various parameters influencing the stellar spectra. The synthetic spectrum depends on ${T}_{\rm eff}$, $\log g$, $\xi_{\rm t}$, $v\sin i$, and the relative abundances of the elements. All these parameters are correlated, hence ${T}_{\rm eff}$, $\log g$, and $\xi_{\rm t}$ were determined before the chemical abundance analysis. The $v\sin i$ values were determined by comparing the shapes of the observed metal line profiles with the computed profiles, as shown by \citet{gray}. Chemical abundances and $v\sin i$ values were determined from many different individual lines or line parts (in case of strong blending) of the spectrum. We took into account all elements that showed lines in the analysed spectral region. Elements that have little or no influence in a given part are assumed to have solar abundances. At the end, we derived the average values of $v\sin i$ and abundances of all chemical elements considered for a given star.

\begin{figure}
\includegraphics[width=3.5in]{figure-specHR.ps}
\caption[]{Position of HD\,21190 (filled red symbol) on the $\log{T}_{\rm eff} - \log g$ diagram. Atmospheric parameters determined in this work are shown with red filled diamod, whereas those taken from \citet{2001MNRAS.326..387K} are plotted with red open diamond. Magnetic Ap stars (black filled circles) discussed in \citet{2000ApJ...539..352H} are shown for comparison. Evolutionary tracks used were taken from \citet{2015MNRAS.450.2764N}. They were calculated with Time Dependent Convection \citep[TDC,][]{2005A&A...434.1055G}, for stars with solar metallicity and $\alpha_{\rm MLT} = 1.8$. The instability strip for $\delta$\,Sct is indicated by black solid lines \citep{2000ASPC..210..215P}.}
\label{hr-diagram}
\end{figure}

In Table~\ref{tab:abundances}, we present the average abundances of both stars together with the solar values of \citet{2009ARA&A..47..481A}, \citet{2015A&A...573A..25S}, \citet{2015A&A...573A..26S}, and \citet{2015A&A...573A..27G}. In Fig.\,\ref{abundances-f} the determined average abundances are compared with the solar abundances. For the primary star, the abundance analysis was carried out for $24$ elements, while abundances for $28$ elements were studied in the spectrum of the secondary.

\citet{2001MNRAS.326..387K} compared a spectrum of HD\,21190 with those of well-known stars and MK standards and classified this star as a chemically peculiar F2\,III\,SrEuSi: object due to the enhancement of the spectral lines \ion{Sr}{ii}\,$4077$\,\AA{}, \ion{Eu}{ii}\,$4205$\,\AA{}, and the \ion{Si}{ii} doublet at $4128-4131$\,\AA{}. In our analysis, all studied heavy and rare-earth elements appear overabundant, confirming the peculiar nature of HD\,21190.

In contrast to the results of \citet{2001MNRAS.326..387K}, the silicon abundance obtained using fourteen lines in the HARPS spectrum is only slightly higher than the solar value. Because of strong blending, we were not able to analyse lines at wavelengths shorter than $4150$\,\AA{}.

The most accurate abundances were derived for elements showing a rich line spectrum. In the case of HD\,21190, these are the elements Si and Ca, and the iron-peak elements Ti, Cr, Fe, and Ni. The iron-peak elements Ti, Cr, and Fe show only slightly higher abundances than solar values, while calcium and nickel are definitely overabundant. The heavy elements Y and Zr, as well as the rare-earth elements are significantly overabundant. Of all these elements, only Y and Nd show enough number of lines for an reliable abundance analysis.

The spectrum of CPD\,$-$83$^{\circ}$\,64B was not analysed before. Since the projected rotation velocity of this star is low, it was possible to carry out an abundance analysis for $28$ elements. With respect to elements with low atomic numbers, Si shows solar abundance, whereas the other considered elements are slightly overabundant. Most lines in the spectrum represent iron-peak elements, from Ca to Cu. All these elements have abundances close to the solar values. All considered heavy and rare-earth elements appear overabundant, but show larger uncertainties. Besides, only for Y, Nd, and Sm ten or more lines were analysed, for the other considered elements only few lines or blends were available. In fact Zr, Ce, and Nd can be solar in the error bars.

To check the reliability of our abundance determinations, we analysed a high S/N day sky solar spectrum taken with HARPS, with a resolving power of about $115\,000$, and covering the spectral range $3780-6860$\,\AA{}. The detailed description of this check is provided in the Appendix.

\section{Discussion}
\label{sect:disc}

Based on a comprehensive astrometric analysis, we show that the stars HD\,21190 and CPD\,$-$83$^{\circ}$\,64B most probably form a physical binary system. The proper motion of CPD\,$-$83$^{\circ}$\,64B agrees within errors with the proper motion of HD\,21190. Using radial velocity values measured in the HARPS spectra and the TGAS parallax measured for HD\,21190, we calculated for both components the heliocentric Galactic space velocities, which agree within a few km\,s$^{-1}$. With our estimated physical separation of a few thousand AU, this wide binary falls well in the range of the new TGAS wide binaries sample of \citet{2017arXiv170407829A}, with similarly small proper motions and relatively bright magnitudes. According to their discussion, our wide binary components are on the one hand not expected to interact over their lifetimes but their separation is also far below the 'tidal limit', where they could not remain gravitationally bound for long in the Galactic tidal field.

Available photometric databases and high-resolution spectroscopic data were used to derive the atmospheric parameters and chemical abundances of both components. For normal stars with similar spectral types nearly solar element abundances are expected. The detection of overabundances of several elements suggest the presence of chemical peculiarities in the atmospheres of HD\,21190. The obtained abundance pattern presented in Table~\ref{tab:abundances} is in good agreement with the previous results of \citet{2001MNRAS.326..387K}, who indicated the presence of chemical peculiarities in HD\,21190.

Two classes of chemically peculiar (CP) stars, the so-called metallic line (Am) stars and magnetic Ap stars, populate the same region in the H-R diagram. The Am stars exhibit overabundances of most iron-peak elements and some heavy elements such as Zn, Sr, Zr, and Ba, and underabundances of Ca and Sc \citep{2009ssc..book.....G}. The majority of Am stars are members of close binary systems.  Chemically peculiar magnetic Ap stars show slight overabundances of iron-peak elements, and stronger overabundances of Sr, Y, Zr, and rare-earth elements (e.g.\ \citealt{2005MNRAS.356.1256C}). The coolest members of the Ap stars, the roAp stars with pulsating periods of $6$ to $24$\,min have effective temperatures in the range of about $6600$ to $8000$\,K \citep{2006MNRAS.370.1274K}. The comparison of the results of our abundance analysis of HD\,21190 listed in Table~\ref{tab:abundances} with diverse abundance analyses presented in the literature indicates a better match with the abundances published for magnetic Ap stars. Whether HD\,21190 can be considered a roAp star is not completely clear yet: \citet{2008MNRAS.384.1140G} obtained for this star $14$ UVES spectra covering about $50$\,min, but no spectral features moving at higher frequencies were identified in the behaviour of the line profiles.

The comparison of the determined atmospheric parameters of HD\,21190, ${T}_{\rm eff} = 6900\pm100$\,K and $\log g = 3.6\pm0.2$, with these of typical magnetic Ap stars presented in Tables\,1 and 2 in the work by \citet{2000ApJ...539..352H} indicates that this star is an evolved magnetic Ap star, even with $\log g$ suggesting less evolved star than it was stated by \citet{2001MNRAS.326..387K}. The position of HD\,21190 in the ${T}_{\rm eff} - \log g$ diagram is shown on Fig.\,\ref{hr-diagram}, together with the positions of Ap stars analysed by \citet{2000ApJ...539..352H}. Evolutionary tracks used were taken from the paper of \citet{2015MNRAS.450.2764N}. They were calculated with Time Dependent Convection \citep[TDC,][]{2005A&A...434.1055G}, for stars with solar metallicity, $\alpha_{\rm MLT} = 1.8$, and cover a range of masses from $1.4$ to $2.8$\,M$_\odot$. The instability strip for $\delta$\,Sct is shown as well \citep{2000ASPC..210..215P}. HD\,21190 is located close to the Terminal Age Main-Sequence and it's position shows that it is the most evolved Ap star among the considered objects, however the error of surface gravity is relatively large. Moreover, the star is located well inside the instability strip of the $\delta$\,Scuti pulsators.

\section*{Acknowledgments}
EN acknowledges the Polish National Science Center grant no. 2014/13/B/ST9/00902.
Calculations have been carried out at the Wroc{\l}aw Centre for Networking and Supercomputing (http://www.wcss.pl), grant No.\,214.
Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs~097.C-0277 and 097.D-0478.

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Inspiral Carpets announce first new material in 16 years
Leonie Cooper Nov 22, 2011 6:25 pm GMT
'You're So Good For Me' is out on CD and vinyl in the new year
Inspiral Carpets have announced the release of 'You're So Good For Me', their first new single in 16 years.
Recorded last month in Manchester, the song is available now on iTunes and will be released on CD and limited edition vinyl on January 3, 2012.
As well as going into the studio to record more new songs, the band will also be heading out on the road for their first UK tour in four years in March 2012. Inspiral Carpets, made up of Clint Boon, Craig Gill, Stephen Holt, Graham Lambert, Martyn Walsh, will play eight shows. They will start off at Bristol Thekla on March 18 and finish up at Manchester HMV Ritz on March 24. Tickets go on sale November 25 at 9am.
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Glasgow O2 ABC (23)
Manchester HMV Ritz (24)
Recently, Clint Boon compared the band's new material with The Vaccines, Kasabian, Interpol and fellow Manchester band Doves.
The keyboardist said the band started writing new songs after reuniting with original singer Stephen Holt. The move comes after singer Tom Hingley left the band over the summer.

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Q: Using Javascript to display current tab in navbar I have a bootstrap side navbar setup on my site. I want to show the user what tabe has been selected by maintaining the active css property. Here is what the side navbar looks like:

            <asp:LinkButton ID="LB_MainPage" CssClass="activeBtn active" runat="server" OnClick="LB_MainPage_Click">Ticket Books Home</asp:LinkButton>

            <asp:LinkButton ID="LB_IssueTicket" CssClass="activeBtn" runat="server" OnClick="LB_IssueTicket_Click">Issue Ticket Book</asp:LinkButton>

            <asp:LinkButton ID="LB_Change_TicketBooks" CssClass="activeBtn" runat="server" OnClick="LB_Change_TicketBooks_Click" >Change Ticket Books</asp:LinkButton>

            <asp:LinkButton ID="LB_TicketBook_Reports" CssClass="activeBtn" runat="server" OnClick="LB_TicketBook_Reports_Click">Search Ticket Books</asp:LinkButton>

            <asp:LinkButton ID="LB_MissingTickets" CssClass="activeBtn" runat="server" OnClick="LB_MissingTickets_Click">Custom Reports</asp:LinkButton>

            <asp:LinkButton ID="LB_AddVoidTicket" CssClass="activeBtn" runat="server" OnClick="LB_AddVoidTicket_Click" >Add Void Ticket</asp:LinkButton>

            <asp:LinkButton ID="LB_VoidTickets" CssClass="activeBtn" runat="server" OnClick="LB_VoidTickets_Click" >Void Tickets</asp:LinkButton>

I am trying to apply the CSS styling as such:
        li .activeBtn {
        cursor: pointer;
    }
    .activeBtn.active {
        color: purple;
        border-bottom: solid;
    }

When a LinkButton is clicked I want to change the LinkButton to active and reset all of the other buttons back to not active. This is the jQuery function that I have in my MasterPage to do so:
$(function () {
          $(".activeBtn").click(function () {
          // remove classes from all
          $(".activeBtn").removeClass("active");
           // add class to the one we clicked
          $(this).addClass("active");
          console.log("this is a test log");
          });
          });

the code is working properly in this jsFiddle. I believe the reason that it is not working because I have a multi-view on my page. When the LinkButton is clicked I change the view in the multi-view.
Any ideas why this would not be working like it is in the jsFiddle?

A: Try this https://jsfiddle.net/hwcgynr0/4/
Add class to clicked element, then find siblings and remove their's active class
$(function () {
    $('body').on('click', '.activeBtn', function () {
        $(this).addClass('active').closest('li').siblings().children().removeClass('active');
    });
});

redpajama_set_name: RedPajamaStackExchange


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Home > News > KTLA Agrees To Broadcast 5 Dodger Games
KTLA Agrees To Broadcast 5 Dodger Games
Scott Andes February 25, 2018 February 25, 2018 News 0
The Dodgers cable television standoff certainly sucks for those that don't have Spectrum. It's been over 4 years now and the Dodgers are only available exclusively on the cable network station sportsnetla, which is only carried by Spectrum. However in order to make a few games nationally available to everyone the club reached an agreement last season with KTLA to televise 10 games on the local station. They eventually added six more games to the schedule at the end of the season to bring the total to 16 games. They are doing it again this season, but this time only 5 games are being broadcast.
The 5 games are all during the first month of the season and will feature three contests against the rival San Francisco Giants. You can also watch the pregame show Access Sportsnet: Dodgers before every game. Check out the list of the five games below so you don't miss anything.
SportsNetLA Dodgers games simulcast on KTLA
Friday, March 30, 7:10 p.m. vs. San Francisco Giants
Saturday, April 7, 1:05 p.m. at San Francisco Giants
Friday, April 13, 7:10 p.m., vs. Arizona Diamondbacks
Saturday, April 21, 6:10 p.m. vs. Washington Nationals
Saturday, April 28, 6:05 p.m. at San Francisco Giants
Dodgers Pound Pale Hose 13-5 in Cactus League Opener
Spring Training Youtube Notebook – The First Weekend
Believe It Or Not, Kershaw's Return Is Around The Corner
Dodgers Finally Announce 2019 Coaching Staff
The Dodgers Opened Their Doors Early and LADR was There


The weather took a turn for the worse as we left Benicàssim, with heavy rain having caused severe flooding in the Valencia area the day before.
Our last night in Benicàssim – está lloviendo a mares!
After stopping to fill up with LPG, we arrived at a very busy Valencia Camper Park. It was the final weekend of the Moto Grand Prix (motorcycling) season at nearby Cheste, so the site was full of Moto GP fans from all over. It's a huge sport in Spain.
The day before we arrived, much of the site had flooded with water knee-deep, but luckily for us it had mostly subsided, with just a few puddles about the place. The rain continued for a few days though, leaving us wishing that the rain in Spain would fall mainly on the plain and not on our van.
Carol went for a wander around the campsite and spotted a guy with a motorhome repair van fixing someone's moho, so I went to see him to get him to look at the tap on our kitchen sink which had packed up for the third time. He couldn't fix it, so we arranged for him to come and fit a new one on Monday, and we now have a fully functioning tap.
On Sunday we took the metro into the city centre. It's a 27 minute ride and costs just €3.20 return each, so terrific value. We went for a wander to re-familiarise ourselves with the old town, and it felt great to be back in a city that we like so much.
Back at the campsite we got chatting to Michelle and Mike from Lincolnshire who happen to have a van that's almost the same as ours, and we spent a fun couple of evenings with them chatting and sharing travel stories.
We returned to town on Monday, and after Carol's appointment at the hairdresser we spent the rest of the day walking around the shopping area and the 'Antiguo Cauce del Río Túria', which is a massive park which was created in the bed of the River Túria after the course of the river was diverted following massive floods in the 1950's. It's a huge green space running through the city, popular with cyclists and runners. After a warm and sunny start, the rain returned later in the afternoon and we headed back to the campsite.
With the weather still hit and miss, we went back into town yesterday and visited the science museum and whiled away a few hours there. When the sun's out it's warm enough to wander around in a t-shirt, and we've been getting funny looks from many locals, who are walking around in puffa jackets, hats and scarves.
Tomorrow both of our daughters will be arriving in Valencia, so we're super excited to be spending a few days with them.
Really great to meet you both. Cracking couple of evenings chewing the fat over a glass of wine….. or two. Enjoy the rest of your tour. Hope you are having a fab weekend with your daughters. Mike & Michele.


Too Much or Too Little Work Causes Stress?
We often think that stress is related to having too much work to do. I recently read that having too little to do at work also can trigger stress. I know for myself when I am overloaded with job tasks that I can feel my blood pressure rise a bit and can become irritable by petty things. On days like this by the end of the day I am exhausted.
When employees do not have enough to do at work they can experience the same stress effects because they are concerned that there is not enough work to keep them employed or maybe they will be perceived as lazy and not pulling their weight. They feel like they need to create things to do to look productive and if asked what they are doing may not have a good answer.
The Occupational Safety and Health Administration (OSHA) declared stress a hazard of the workplace. Stress costs the American industry more than $300 billion annually.
43% of all adults suffer adverse health effects from stress.
75% to 90% of all doctor's office visits are for stress-related ailments and complaints.
Stress is a serious health issue. As a manager and business owner I have noticed when our business is slower, staff seem to "flounder" for things to do. Something that helps is at the beginning of each month to have staff members write down incentive goals with tasks that they can do when they have extra time. By doing this they do not have to "stress" to find things to keep them busy.
Also when we are overly busy I make sure that the staff does not stress about undone tasks, I reassure them there will always be another day and we will catch up over time. This gives them relief and they know I understand the situation and they do not have to stress over it.
Life is just too short to make it shorter.
This entry was posted on Thursday, January 25th, 2018 at 9:00 am by Tina Del Buono, PMAC.
Filed under Business Owner, Health Benefits, Manager Topics, Recommended Websites, Self-improvement. You can follow any responses to this entry through the RSS 2.0 feed. Both comments and pings are currently closed.


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Mini Global Hawk long-range UAV starts test program
A new generation of small, long-range unmanned aerial vehicles (UAVs) took flight 20 June with the maiden voyage of the Scan Eagle, a joint development of The Insitu Group in Bingen, Wash., and Boeing's Unmanned Systems group in St. Louis.
Aug 1st, 2002
by J.R. Wilson
BOARDMAN, Ore. — A new generation of small, long-range unmanned aerial vehicles (UAVs) took flight 20 June with the maiden voyage of the Scan Eagle, a joint development of The Insitu Group in Bingen, Wash., and Boeing's Unmanned Systems group in St. Louis.
In many ways, the Scan Eagle, based on Insitu's Seascan ship-based surveillance aircraft, is a miniature version of the U.S. Air Force Global Hawk, which made UAV history last year with a 22-hour, 7,500-mile flight from Edwards Air Force Base, Calif., to Royal Australian Air Force Base Edinburgh, South Australia.
While Global Hawk has the wingspan of a Boeing 737 jetliner and the length of a Learjet 24E business jet, the Scan Eagle is only four feet long, with a 10-foot wingspan. But it ultimately may have a range as long as 5,000 miles during a three-day flight at speeds as fast as 78 miles per hour.
It its first flight, the Scan Eagle launched from a pneumatic catapult at Insitu's eastern Oregon test facility and flew for 45 minutes at altitudes as high as 1,500 feet. It completed test points using the Global Positioning System and received real-time flight plan updates from its ground station. Retrieval involved Insitu's patented SkyHook technique in which the Scan Eagle snared a rope hanging from a 30-foot pole.
A pilot on the ground radio-controlled take-off and landing, while Scan Eagle's on-board computer autonomously controlled the rest of the flight. In an operational mode, the entire flight could be autonomous.
The test flight was the first in a 15-month agreement with Boeing and Insitu that began in February 2002. Evaluators based its operational performance on a 1998 demonstration by Insitu and the University of Washington, in which a 33-pound Seascan made the first UAV transatlantic flight — a 2,000-mile trip from Newfoundland to Scotland that used only 1.5 gallons of gasoline.
The Scan Eagle effort combines Insitu's aircraft with Boeing systems integration, communications, and payload technologies. "Our goal is to develop low-cost, long-endurance unmanned aerial vehicles offering a high degree of autonomy," Insitu founder and chairman Tad McGeer says.
"We are melding Insitu's expertise and unique capabilities with the best of Boeing to provide an autonomous, low-cost, long-endurance UAV for a wide range of potential customers," notes Charlie Guthrie, Boeing Unmanned Systems director of rapid prototyping and advanced concepts.
Potential applications include military reconnaissance, chemical weapons detection, severe weather monitoring, and border patrol. The aircraft can operate independently or in groups, as well as in an integrated team with other intelligence aircraft.
While neither Boeing nor Insitu has officially disclosed a price, published estimates put Scan Eagle's cost at less than $100,000 per aircraft. In military use, that would make it an inexpensive option for high-risk surveillance missions.
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Kampala — The government yesterday tabled before Parliament a request seeking the approval of the creation of 14 new districts, even as the battle over Bushenyi's split went to court. Local Government State Minister Pereza Ahabwe told MPs that Cabinet had already endorsed the creation of the new districts, which if approved, will bring the total to 111. The new units should be operational by July.
He told MPs that the government considered it necessary to create the new districts "for the effective administration of those areas", and to "bring services closer to the people." The districts to face the blade are Bushenyi, Masaka, Pallisa, Kumi, Amuru and Pader. Masaka is to be split into four units; Kalungu, Bukomansimbi, Lwengo and Masaka.
According to the motion, which Speaker Edward Ssekandi referred to the House's Committee on Public Service and Local Government, Bushenyi will have five new districts. Sheema County now becomes Kibingo District while Buhweju County will now be called Nsiika District. A new Rubirizi District will also be formed, consisting of Bunyaruguru County while Ruhinda County becomes Mitooma District. Bushenyi District will retain Igara County, the request showed.
The other new districts are Gombe District, to be carved out of Mpigi District. Ngora County currently under Kumi District becomes a districtwhile Bokora County becomes Napak District carved out of Moroto. The others are Kibuku District formerly Kibuku County, carved out of Pallisa and Nwoya District formerly Nwoya County currently part of Amuru.
The government also seeks to create Kole District, to be carved out of Apac District and Patongo District to be created out of Pader. Mr Ahabwe said the boundaries of Arua District and another district comprising of Maracha and Terego counties be altered by incorporating Terego County in Arua District and Nyadri District consisting of Maracha County be formed.
But as the minister went about making his proposal, a group of Bushenyi residents were in court seeking to block the split of the western Uganda district. In a petition filed before the Constitutional Court on April 15, Mr Wilberforce Muhangi and four others want the split of the fifth most populous district halted until all residents have been fully consulted and court disposes the petition, which comes up for hearing today.
The petitioners disapprove the notion that smaller administrative units ease development, arguing that the new small districts shall neither sustain themselves nor develop as it shall "drain the national treasury. But Mr Ahabwe last evening said court action would not stop the move. "Going to court doesn't mean anything," he said.