text:
package org.wso2.developerstudio.eclipse.gmf.esb.diagram.edit.policies;

import org.eclipse.draw2d.ColorConstants;
import org.eclipse.draw2d.Figure;
import org.eclipse.draw2d.FigureListener;
import org.eclipse.draw2d.Graphics;
import org.eclipse.draw2d.IFigure;
import org.eclipse.draw2d.Label;
import org.eclipse.draw2d.RectangleFigure;
import org.eclipse.draw2d.geometry.Rectangle;
import org.eclipse.gef.editpolicies.SelectionEditPolicy;
import org.eclipse.gmf.runtime.draw2d.ui.figures.WrappingLabel;
import org.eclipse.gmf.tooling.runtime.edit.policies.labels.IRefreshableFeedbackEditPolicy;

/**
 * @generated
 */
public class EsbTextSelectionEditPolicy extends SelectionEditPolicy implements
		IRefreshableFeedbackEditPolicy {

	/**
	 * @generated
	 */
	private IFigure selectionFeedbackFigure;

	/**
	 * @generated
	 */
	private IFigure focusFeedbackFigure;

	/**
	 * @generated
	 */
	private FigureListener hostPositionListener;

	/**
	 * @generated
	 */
	protected void showPrimarySelection() {
		if (getHostFigure() instanceof WrappingLabel) {
			((WrappingLabel) getHostFigure()).setSelected(true);
			((WrappingLabel) getHostFigure()).setFocus(true);
		} else {
			showSelection();
			showFocus();
		}
	}

	/**
	 * @generated
	 */
	protected void showSelection() {
		if (getHostFigure() instanceof WrappingLabel) {
			((WrappingLabel) getHostFigure()).setSelected(true);
			((WrappingLabel) getHostFigure()).setFocus(false);
		} else {
			hideSelection();
			addFeedback(selectionFeedbackFigure = createSelectionFeedbackFigure());
			getHostFigure().addFigureListener(getHostPositionListener());
			refreshSelectionFeedback();
			hideFocus();
		}
	}

	/**
	 * @generated
	 */
	protected void hideSelection() {
		if (getHostFigure() instanceof WrappingLabel) {
			((WrappingLabel) getHostFigure()).setSelected(false);
			((WrappingLabel) getHostFigure()).setFocus(false);
		} else {
			if (selectionFeedbackFigure != null) {
				removeFeedback(selectionFeedbackFigure);
				getHostFigure().removeFigureListener(getHostPositionListener());
				selectionFeedbackFigure = null;
			}
			hideFocus();
		}
	}

	/**
	 * @generated
	 */
	protected void showFocus() {
		if (getHostFigure() instanceof WrappingLabel) {
			((WrappingLabel) getHostFigure()).setFocus(true);
		} else {
			hideFocus();
			addFeedback(focusFeedbackFigure = createFocusFeedbackFigure());
			refreshFocusFeedback();
		}
	}

	/**
	 * @generated
	 */
	protected void hideFocus() {
		if (getHostFigure() instanceof WrappingLabel) {
			((WrappingLabel) getHostFigure()).setFocus(false);
		} else {
			if (focusFeedbackFigure != null) {
				removeFeedback(focusFeedbackFigure);
				focusFeedbackFigure = null;
			}
		}
	}

	/**
	 * @generated
	 */
	protected Rectangle getFeedbackBounds() {
		Rectangle bounds;
		if (getHostFigure() instanceof Label) {
			bounds = ((Label) getHostFigure()).getTextBounds();
			bounds.intersect(getHostFigure().getBounds());
		} else {
			bounds = getHostFigure().getBounds().getCopy();
		}
		getHostFigure().getParent().translateToAbsolute(bounds);
		getFeedbackLayer().translateToRelative(bounds);
		return bounds;
	}

	/**
	 * @generated
	 */
	protected IFigure createSelectionFeedbackFigure() {
		if (getHostFigure() instanceof Label) {
			Label feedbackFigure = new Label();
			feedbackFigure.setOpaque(true);
			feedbackFigure
					.setBackgroundColor(ColorConstants.menuBackgroundSelected);
			feedbackFigure
					.setForegroundColor(ColorConstants.menuForegroundSelected);
			return feedbackFigure;
		} else {
			RectangleFigure feedbackFigure = new RectangleFigure();
			feedbackFigure.setFill(false);
			return feedbackFigure;
		}
	}

	/**
	 * @generated
	 */
	protected IFigure createFocusFeedbackFigure() {
		return new Figure() {

			protected void paintFigure(Graphics graphics) {
				graphics.drawFocus(getBounds().getResized(-1, -1));
			}
		};
	}

	/**
	 * @generated
	 */
	protected void updateLabel(Label target) {
		Label source = (Label) getHostFigure();
		target.setText(source.getText());
		target.setTextAlignment(source.getTextAlignment());
		target.setFont(source.getFont());
	}

	/**
	 * @generated
	 */
	protected void refreshSelectionFeedback() {
		if (selectionFeedbackFigure != null) {
			if (selectionFeedbackFigure instanceof Label) {
				updateLabel((Label) selectionFeedbackFigure);
				selectionFeedbackFigure.setBounds(getFeedbackBounds());
			} else {
				selectionFeedbackFigure.setBounds(getFeedbackBounds().expand(5,
						5));
			}
		}
	}

	/**
	 * @generated
	 */
	protected void refreshFocusFeedback() {
		if (focusFeedbackFigure != null) {
			focusFeedbackFigure.setBounds(getFeedbackBounds());
		}
	}

	/**
	 * @generated
	 */
	public void refreshFeedback() {
		refreshSelectionFeedback();
		refreshFocusFeedback();
	}

	/**
	 * @generated
	 */
	private FigureListener getHostPositionListener() {
		if (hostPositionListener == null) {
			hostPositionListener = new FigureListener() {
				public void figureMoved(IFigure source) {
					refreshFeedback();
				}
			};
		}
		return hostPositionListener;
	}
}


The Code of Ethics for the Tandem Group (TTG) has been adopted to promote and maintain the highest standards of service and personal conduct within this agency. Adherence to these standards is required and serves to assure industry confidence in the integrity and service or The Tandem Group Sale Representative.
-Use every opportunity to improve public understanding of The Tandem Group Inc., our suppliers, Manufacturers' Representatives and their positive impact on our industry.


Raytheon Co. – Integrated Defense System, Tewksbury, Massachusetts, has been awarded a $15,150,728 modification (P00029) to previously awarded contract FA8730-15-C-0002 for the Qatar Air and Missile Defense Operation Center. This modification provides for the procurement of the Qatar Alternate ADOC Prime Mission Equipment and software. This modification involves 100 percent foreign military sales to Qatar. Air Force Life Cycle Management Center, Hanscom Air Force Base, Massachusetts, is the contracting activity.


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Homeward Bound Renovates Women's Unit
Dallas, February 5, 2009 – Homeward Bound in Dallas changes lives for clients struggling with addiction to drugs and alcohol. Thanks to multiple donors, women at the Center will now enjoy a warm, welcoming and more comfortable environment while undergoing intensive treatment for their addictions.
The Center recently announced the completion of the renovation of its women's unit renovation, made possible by donations of goods and services from multiple organizations and a grant from The Boone Family Foundation. This renovation involved a month-long effort by volunteers and staff to improve the therapeutic environment with the installation of new furniture and flooring, fresh paint and other improvements.
"The renovation is quite simply a miracle — a wonderful, beautiful, tangible miracle," said Renee Breazeale, Program Director, Homeward Bound. "When we walk off the elevator now it feels like a welcoming home, so warm and comforting." She added that the newly-renovated women's unit "is a place of light and hope, a place of healing and compassion, a place of respect and honor, a place of safety and concern and a place where all women can feel nurtured, special, and cherished. The renovation is a transformative event that will impact many women's lives to come."
Garrett Boone of the The Boone Family Foundation praised the collaboration of businesses and volunteers that made the renovation a success.
"We are thrilled by the response from the businesses who contributed to make this renovation even more spectacular," said Mr. Boone. "The depth of the coordination involving many people was inspiring to me all the while maintaining a consistent focus to keep the women comfortable."
Among the improvements:
*Sherwin-Williams and 400 volunteers from the Volunteer Center of North Texas painted the interiors, brightening the unit with fresh pastel colors.
* Specified Floor Designs installed an ivory vinyl tile floor to replace the dark carpeting.
* The rooms were updated with new mattresses donated from Sleep Experts Rest Assured Foundation and beautiful bed linens donated by Peacock Alley.
* The Container Store donated Elfa drawer units.
* New blinds from Kensington Window Expressions, along with new chairs, blankets, pillows and shower caddies accessorized the newly-renovated rooms.
"We are honored to join with other local organizations that share the Boone Foundation's passionate commitment to family and community," said Mary Ella Gabler, founder and chief executive officer of Peacock Alley. "We can help create a safe comfortable haven, which is a powerful thing."
"Sleep Experts is honored to support the efforts of Homeward Bound in helping families overcome abuse," said Christine Cook, president of Sleep Experts. "We are dedicated to helping out in any way we can to share the comfort of a good night's sleep with families who need it most. We are truly humbled to be a part of such an inspiring effort. "
"The renovation was a complete transformation of our old women's unit to one that is light and bright and uplifting for patients and staff alike," said Diane Burns, Development Director, Homeward Bound. "The women in the unit were touched by the volunteers who came and put everything together. It is beautiful to see and it is beautiful to know that so many care about women who are striving to improve their lives."
Founded in 1866, The Sherwin-Williams Company is a global leader in the manufacture, development, distribution, and sale of coatings and related products to professional, industrial, commercial, and retail customers. The company manufactures products under well-known brands such as Sherwin-Williams®, Dutch Boy®, Krylon®, Minwax®, Thompson's®, WaterSeal® and many more.
With global headquarters in Cleveland, Ohio, and Southwest Division headquarters in Dallas, Sherwin-Williams(R) branded products are sold exclusively through a chain of more than 3,300 company-operated stores and facilities across the country, while the company's other brands are sold through leading mass merchandisers, home centers, independent paint dealers, hardware stores, automotive retailers, and industrial distributors. For more information, visit www.sherwin.com.
VCNT
The Volunteer Center of North Texas (VCNT) is a 37-year old nonprofit whose mission is "making volunteerism a part of everyday life." The VCNT connects people to causes by providing volunteers to more than 1,700 nonprofit agencies in North Texas.
Sleep Experts
Sleep Experts is a third-generation mattress retailer servicing the Dallas/Fort Worth Metroplex and offering a broad selection of traditional and specialty sleep brand names, including Simmons, Beautyrest, Spring Air, Back Supporter, Tempur-Pedic, ComforPedic and Air Number. Sleep Experts is an Inc. 5000 company that has been chosen by D/FW consumers as the "Consumers' Choice for Business Excellence" for mattress retailers for 2007 and 2008. Sleep Experts utilizes a portion of proceeds from every mattress sale toward helping families in need. Through its Community Connection Program "Rest Assured," Sleep Experts recycles customers' old mattresses for donation to area nonprofits in need, which also reduces landfill bulk. Sleep Experts has 33 locations. For more information, visit www.sleepexperts.com or call 1-888-55-SLEEP.
Peacock Alley is a premier manufacturer and importer of luxury linens for the bed and bath, known for impeccable quality and attention to detail. For fine linen and bath consumers, Peacock Alley products are a smart indulgence with high quality standards, classic and contemporary designs, soothing colors and the versatility to mix and match for personal expression-all with sharp attention to detail and long-lasting value. Peacock Alley is based in Dallas and was founded in 1973 by Mary Ella Gabler, Chief Executive Officer. Visit us online at www.peacockalley.com
The Container Store currently has 46 locations across the country. The Container Store offers free closet design services every day in its stores and online using Elfa, the premiere shelving and drawer system. Visit www.containerstore.com for more information about store locations, the product collection and services offered. Sales for fiscal year 2008 are projected at $650 million. The Container Store is privately held.
The Boone Family Foundation
The Boone Family Foundation is a resource for social change and innovation. Grants are primarily focused in Texas and support programs in three areas: advancing equity for women and girls; improving quality of life for children; and promoting environmental stewardship.

redpajama_set_name: RedPajamaCommonCrawl


Scripture selection is Day 5 Period I.
for May 2nd are Sorrowful.
years to deliver this message.
are deeply intimate with God.
is their marriage to Jesus.
Mary is the perfect handmaid.
games to give his hate to God.
and hatred in their hearts.
holy love in their hearts.
the soul – who gives in.
to allow satan to use him.
amends for their wrong doing.
And in Him is no darkness.


Sale High School does it again!
Sale High School is pleased to announce record-breaking results once again. The school has exceeded even its own high expectations against all key measures. Students comfortably met the demands of the new specifications and new grading system in all subjects. The school saw particularly high achievement in English, Maths, Science, P.E., Art and Modern Foreign Languages. This year 75% of students achieved grade 4+ in English, 71% grade 4+ in Maths and 100% grade 4+ in triple science. 69% of students achieved 5 GCSE passes including English and Maths, placing the school well above last year's national average. Headteacher Jayne O'Grady is delighted with the results and has been hugely impressed by the hard work and dedication of students throughout her first year in post, "Faced with the rigours of the new examination system at KS4, Sale High School students have demonstrated, yet again, that through hard work and commitment anything is possible". Particular praise goes to Alan, Gionata, Chris, Natasha and Wiktoria who are celebrating 16 grade 9s between them! Ms O'Grady would like to publicly thank and acknowledge the amazing hard work of the Sale High School staff. These results clearly show why Sale High School is the school of choice for the community.


text:
Q: Filter Navision WebService in Android for ReadMultiple Method I have called navision web service succesfully by authenticating it through the use of NTML authentication protocol. And i also got the full, Proper data for all the Method but i have issue in calling READ MULTIPLE METHOD with Filter. i have passed filter in below manner.
CustomerList_Filter customFilter = new CustomerList_Filter();
customFilter.field = CustomerList_Fields.Name;
customFilter.criteria = "B*";
VectorCustomerList_Filter vfilter = new VectorCustomerList_Filter();
vfilter.add(customFilter);
custService.ReadMultipleAsync(vfilter, null,0);

Eventhough i passes Filter to get Customer name Record  starting with B letter still it shows all customer. & custService is an object of CustomerList_Service class.Please help.

A: It is said that first parameter of ReadMultiple is array. Is VectorCustomerList_Filter an array? Maybe you should write custService.ReadMultipleAsync(vfilter.ToArray(), null,0);
Also you can try to put code the way in this answer. salesOrdersService.ReadMultiple(new SalesOrders_Filter[] { filter }, null, 0);
If this not helps then try to catch output XML message that is sent as request to web service. You'll be able to find error by analyzing it.

redpajama_set_name: RedPajamaStackExchange


text:
After Hours: 39.69 0 0.00% 19:58 01/27 EST
JDE Peet's NV: A True Comeback Story
Mizuho picks its top stocks for 2023
Benzinga's Most Accurate Analysts Say Buy These 3 Defensive Stocks Delivering High-Dividend Yields
Analysts Offer Insights on Consumer Goods Companies: Colgate-Palmolive (CL) and Kraft Heinz (KHC)
TipRanks · 4d ago
3 January Buffett Dividend Dog Buys Plus 5 To Watch
Kraft Heinz: It's Not Just About Being Recession-Proof
UPDATE 1-Tesco boss in 'parallel universe' over price rises, says UK farmers' chief
Reuters · 6d ago
Americanas' billionaire shareholders say they were unaware of accounting problems
About KHC
The Kraft Heinz Company (KHC) is a global food and beverage company. The Company's segments geographic include United States, International, and Canada. KHC manufactures and markets food and beverage products, including dairy products, meat products, coffee beans, soybean and vegetable oils, sugar and other sweeteners, tomatoes, potatoes, corn products, wheat products, nuts, and cocoa products. The Company's products are sold through its own sales organizations and through independent brokers, agents, and distributors to chain, wholesale, cooperative and independent grocery accounts, convenience stores, drug stores, value stores, bakeries, pharmacies, mass merchants, club stores and institutions. KHC's products are also sold online through various e-commerce platforms and retailers. KHC offers its products under various brands, such as Kraft, Oscar Mayer, Heinz, Philadelphia, Lunchables, Velveeta, Maxwell House, Kool-Aid, Ore-Ida, Jell-O, Master, Quero, Golden Circle and Wattie's.
Webull offers kinds of Kraft Heinz Co stock information, including NASDAQ:KHC real-time market quotes, financial reports, professional analyst ratings, in-depth charts, corporate actions, KHC stock news, and many more online research tools to help you make informed decisions.
You can practice and explore trading KHC stock methods without spending real money on the virtual paper trading platform.


text:
Our Projects in 2015 – a review
Our Projects in 2015 – a reviewPhotoVoiceJanuary 11, 2016 March 4, 2022
Becky Warnock, Projects Manager for PhotoVoice, reflects on her views on PhotoVoice's projects over the course of 2015.
I'm writing this post in a hotel in Jakarta, having completed our second trip working with Indonesian women migrant workers, in partnership with MAMPU. It's been an incredible two weeks, full of contrasting experiences and surprises, ranging from the stunning and welcoming remote island of Lembata, the more developed and dynamic Lombok, to the sheer size and density of cosmopolitan Jakarta.
It would be so simple to make the assumption that all migrant workers in Indonesia are united by a common aspiration, or that their desires for employment are the same. But they aren't; and each group is so different in their identities. You can read more about this in our project update post here.
It has reinforced to me that the strength of PhotoVoice's methodology in its capacity to be flexible, to respond to the group, meeting each individual where they are at, and allowing that the outcome be defined by them.
It was this same creativity and artistic value that strengthened our work with Sense UK this year too; despite being such a short pilot project, the images from the participants we worked with are beautiful, and unusual, standing out even from the log of images in the PhotoVoice database.
Sean/TouchBase/Sense/PhotoVoice/2015
The photos are special in that they each capture the unique perspectives of the participants and their experiences of deafblindness. We are hopeful that 2016 might bring further activities with Sense, and look forward to being challenged to creatively develop new ideas for sensory photography and how this might provide an outlet and expression for participants' identities.
Earlier in the year, we provided Christian Aid with the evaluation report for our partnership My Pharm, a monitoring and evaluation project supporting the development of subsistence farmers in rural Ghana. The report contained a section titled Unintended Outcomes, which detailed stories of moments where our trained Community Monitors were able to take complete agency over their new roles and photographic skills; one using them to create warning posters about the dangers of swimming in certain areas, the other using his photos of a badly burnt young boy to ensure that he was able to receive life saving healthcare.
Apam Apamlea 2014 / YHFG / Christian Aid / PhotoVoice
We could never have anticipated the role that images might have played in these situations, but we can certainly celebrate the initiative and inspiration that these participants displayed.
We are continuing work with Christian Aid through a new project in Ethiopia, building skills with the local partners to support resilience around climate change. This year we will support the community to further embed their role as community monitors and better manage the resources provided as part of the climate intervention; ensuring that they have the capacity and training to do so.
Another major project in 2015 was our work in the UK with young people who are affected by or at risk of sexual exploitation, as part of our project Having Our Say3. We were struck by the need for, and importance of, a caring, nurturing environment in which the young people feel safe. So many of the young people we have met and worked with have reflected on the importance of workers taking the time to be with them, get to know them as people, as opposed to processing their situations on a conveyor belt system.
Zarin/HOS3/NWG/PhotoVoice/2015
With one of our partners on this project, NSPCC Croydon, it was clear that the staff care deeply about their clients and have managed to find the time to create meaningful relationships with each young person. For our partners at The Men's Room in Manchester, despite their small team, there is the sense that staff don't just try to solve a young persons' situation of unemployment by focusing on just getting them any job, instead working with them to think about their aspirations, their hopes, and what might be holding them back from these. These stories and experiences make us hopeful for our future work on the project, but more importantly, for the futures of the young people themselves and what these experiences might empower them to achieve.
This year will see PhotoVoice build further on these experiences. We are excited to complete our next phase of workshop delivery for Having Our Say 3, share our learnings and report with MAMPU, and also host a panel event on How to Encourage Diversity in Photography at London Art Fair on the 20th January. These different events will target a variety of changes at various levels, both for individuals, organisations and sectors, but also continue to expand our development as a charity and methodology too.
In the meantime, we would like to thank everyone who has supported us up till now, and wish you a very happy 2016.
GhanaHavingOurSaySensoryPhotography
PhotoVoice Fieldwork – Zimbabwe DiaryPhotoVoiceFebruary 14, 2017 March 4, 2022
February 14, 2017 March 4, 2022 |BY PhotoVoicePhotoVoice Fieldwork – Zimbabwe Diary
Kate Watson, Projects Manager at PhotoVoice is currently working with 14 community members in Lower...
A thousand more words on the photographs of Alan Kurdi, one year onKate WatsonSeptember 5, 2016 March 4, 2022
September 5, 2016 March 4, 2022 |BY Kate WatsonA thousand more words on the photographs of Alan Kurdi, one year on
12 months ago, Russell Watkins, a PhotoVoice trustee wrote 'A thousand words on the photographs...
Wrap on Workshop Phase of Having Our Say 3PhotoVoiceAugust 11, 2016 March 4, 2022
August 11, 2016 March 4, 2022 |BY PhotoVoiceWrap on Workshop Phase of Having Our Say 3
11/08/2016 For young people who have experienced or are at risk of sexual exploitation; defining,...


The Orange County Society of Ophthalmology (OCSO), a non-profit voluntary organization, was founded in the early 1960's. It is designed to promote the science and art of ophthalmology, the protection of public health, and the betterment of the profession. The membership of OCSO is composed of physicians holding a medical degree and trained in the subspecialty of ophthalmology. All members are required to be certified or eligible for certification by the American Board of Ophthalmology. OCSO is a component of the Orange County Medical Association and the California Medical Association.


text:
Frogmore to submit planning permission for new hotel in Southwark following £14m loan from OakNorth
By Bridging Loan Directory - 12th May 2017
OakNorth – the bank for entrepreneurs, by entrepreneurs – has lent £14.4m to Frogmore, the UK-focussed, fully integrated real estate investment manager which has invested and sold over £6bn of real estate since its founding in 1995.
The capital has been used to acquire a cleared site on Ufford Street, adjacent to the LeSoCo College, and submit planning permission to develop a hotel. The site is less than a 10 minute walk from both Waterloo and Southwark stations and is in close proximity to other popular attractions, including: The Young Vic, The Old Vic, The London Eye, The London Dungeon, Sea Life, Southbank Centre and the Royal Festival Hall, making it an ideal spot for tourists. In addition to this, there are a number of Michelin star restaurants such as Gordon Ramsey's Union Street and Mark Hix's Hixter located nearby. Whilst there are a number of hotel projects and schemes currently under construction in Southwark – Hilton's Hampton, Marriott's Autograph, and Park Plaza's Art'otel – the area still has one of the lowest levels of hotel bedroom supply amongst key Central London boroughs. This is especially noticeable when compared to neighbouring Waterloo where a number of established hotel brands – Novotel, Ibis, Hilton, Holiday Inn Express, Park Plaza, Premier Inn and Travelodge – all have a presence.
Established in 1961, Frogmore has transacted over £6bn of projects since 1995. Currently it owns assets such as: The Notting Hill Gate Estate, Stratford Shopping Centre, and Weston House in Holborn. Previously, Frogmore developed the South Place Hotel, an 80 bedroom boutique hotel with restaurant, brasserie and private dining facilities. The hotel is let to D&D Restaurants Limited and was completed in 2012. Earlier this year, South Place Hotel was sold to Chinese Investors.
Commenting on the deal, Jo Allen, Chief Executive of Frogmore, said:
"Southwark has been experiencing a shortage in hotel room supply for several years. In Kensington and Chelsea, there are three times as many hotel rooms. In Westminster, there are more than seven times. Our hope is that we can secure planning permission to build a hotel here and help fill this gap with a new 275 bedroom hotel on the site.
"It was a pleasure working with OakNorth on this deal – we're no strangers to securing debt finance for large-scale projects, but this experience was one of the simplest and most stress-free transactions we've concluded."
Ben Barbanel, pictured, Head of Debt Finance and Damien Hughes, Property Finance Director at OakNorth Bank, commented:
"Southwark's regeneration in recent years has put this south London borough on the map and made it a prime location for homes; international tourism and business.
"We're very proud to have been selected by Frogmore for this deal – the business has an incredibly strong track-record spanning more than five decades. Frogmore's last project in the hotel space – the South Place Hotel – was a huge success and we have no doubt that this one will be too. We look forward to working with Frogmore on future projects and hopefully celebrating their planning permission approval very soon."


Fluid Transitions by Sara Beaman is an excellent DVD for dancers looking to work on movement transitions and Fusion combinations. Sara's dancing is really beautiful, her breakdowns of movements and exercises were clear, and the content was original and informative. The DVD was well thought out, nicely structured, and the pacing and flow of the exercises felt good. I enjoyed the combinations and thought she had some great ideas for transitional movements. The one thing I would have liked to see different on this DVD would have been to extend the combinations practice flow. Sara did a great job creating a professional product. The graphic design, filming, and editing are all lovely. The one glitch I encountered was scrolling through the menu items. I couldn't scroll through them in the order they appeared.
The DVD consists of a warm up, isolation drills, isolation practice flow, combinations, and a cool down. Sara faces the camera standing at an angle so that the view from the back is reflected in the mirror. The mirrors aren't full length so you can't see her feet but it doesn't detract from the instruction since the transitions are all fairly stationary. All instruction is done via voice overs. Basic isolations such as chest circles and undulations are assumed for the warm up but broken down in the isolation drills section. There are 6 combinations, each consisting of 2-4 moves done back to back to work on the transitions between them. Sara does a great job of showing the movements from front and side views and drills each side evenly for movements which can be done on the right or left. Each combination is broken down and then drilled at 3 speeds. For each of the three speeds the combination is done at half time and full time (so in effect it gets practiced at 6 speeds). Combinations 1-4 are later added together as a practice flow to show how to transition between them. The flows aren't drilled as long as the individual combinations and are presented at only one speed. While the flows were enjoyable I ended up wishing that they were drilled for a little longer. Combinations 5-6 involve movement layering and are more difficult then combinations 1-4.
In addition to the regular chapters of the DVD, Sara has included 4 shorter practice play lists. I thought this was a really great addition. Each play list is about 20-30 minutes long and these would be perfect for when you can only fit in a short practice. They each have a warm up, cool down, and a few of the combination drills. They allow you to do a short self contained practice which would make it more likely for dancers to do a complete practice session then if you had to click through the menu to do each of those sections separately. I know how hard it is to have discipline when doing DVDs and for myself I would be likely to skip warm up or cool down, or to get distracted by something when going to switch between menu items and stop practicing, so I appreciate that this was included.
Who would get the most from this DVD?
The video description recommends it for dancers at the advanced beginner level and I completely agree. Advanced beginners who are looking to smooth out their movement transitions or learn new Fusion style combinations will get the most from this content although I think intermediate and advanced dancers would enjoy the exercises as well. The isolations used are broken down so that beginners could use the DVD as well, but I think dancers who have some background in basic isolations will get the most out of the entirety of the instruction on this DVD; true beginners might end up slightly overwhelmed especially with the layering combinations. If you are a dancer who specializes in another style but want to work on Fusion combinations and stylizations I think this DVD is an excellent choice for cross training. This is what I was hoping to use it for and have found it to be a perfect fit.
Disclosure: I received this DVD as a review copy from Sara.


As if we didn't see it coming. Last night at the 91st Annual Academy Awards when it came time to announce the winner for 'Best Actor', Rami Malek won the award for his stunning portrayal of Freddie Mercury in 'Bohemian Rhapsody' beating out Christian Bale, Bradley Cooper, Willem Dafoe, and Viggo Mortensen.
For this role, Rami also took home a Golden Globe, a BAFTA, and a SAG award. Rami's win last night was surely expected, but that didn't make it any less amazing when his name was called to the stage.
'Bohemian Rhapsody's' road to its massive success surely didn't come without its roadblocks. Believe it or not, this film was actually roughly 10 years in the making and is the passion project of Queen guitarist Brian May and drummer Roger Taylor. They had planned to make the film before with actor Sacha Baron Cohen directing the biopic and starring in the film as Freddie Mercury, himself.
Fast forward to present day, the band struck gold with Rami Malek. However, the film still encountered its struggles with director Bryan Singer being fired from the project just weeks before the end of principle photography. However, they would finish and produce a movie that wowed audiences all over the world.
Rami gave arguably the most gracious acceptance speech in the Academy's history. He thanked everyone he possibly could and hardly a single participant in the film went unmentioned. It's clear from his wavering voice that he feels as strongly about Freddie, the band, and film as we do.
Watch this heartfelt speech below and have some tissues ready.


text:
A war over a 'sanctuary' mirage?
Ruben Navarrette
Washington Post Writers Group
Immigration has always made President Trump a bit loony. No rational person would say the United States is hurt by accepting risk-takers from "shithole" countries, paint immigrants as violent criminals and claim Mexico is sending us its worst people. Just to scare up a few votes?
But now, the issue seems to have finally driven him and his entire administration stark raving mad. How else can we explain Attorney General Jeff Sessions suing California over a phony "sanctuary" law that only has the power to offend conservatives and make liberals feel morally superior?
Sessions is not the right person to defend federal supremacy. He's a career politician from Alabama, which seceded from the union in the 1860s and defied federal civil rights laws in the 1960s. He sides with gun zealots who think they have the duty to overthrow a tyrannical federal government, and he thinks local police departments accused of civil rights violations should escape federal oversight.
It's absurd. To make sense of it all, keep in mind the three F's: foil, fraud and flip.
Foil: With a modern-day P.T. Barnum at the helm, the Trump administration has a knack for finding a sucker every minute by creating a foil so as to deflect attention away from whatever is going wrong — a fractured and backbiting White House in chaos, a looming trade war over 19th century-style tariffs, the resignation of top advisers, questions about payoffs to a porn star, etc. During the campaign, amid a cascade of gaffes and scandals, Trump shifted the conversation to trade and made a foil out of China. A few weeks ago, when the topic was school safety, Trump pointed his finger at violent movies and video games. Now that the subject has turned to immigration, the convenient foil is California.
Fraud: When railing against so-called sanctuaries, the administration keeps contradicting itself. One minute, it says that California is preventing Immigration and Customs Enforcement agents from doing their jobs; the next, it announces with great fanfare that it's business as usual and that raids are on the way. So much for not being able to do their jobs, eh? No matter who declares what, the federal government doesn't take orders from local and state officials in California. But nor do local officials like Oakland Mayor Libby Schaff – whom Sessions called out for spilling the beans about an ICE raid – take orders from the federal government. By the way, not for nothing, but Republicans like Sessions have for decades gone to Central California to milk contributions from conservative farmers who would lose everything and see their crops rot on the vine without illegal immigrant laborers to pick them.
Flip: Remember when conservatives ranted and raved about local control? When local school officials wanted to skirt federal education accountability requirements under No Child Left Behind, or a local county clerk declared that her Christian beliefs prohibited her from issuing marriage licenses to same-sex couples, or the state of Arizona insisted that it had the right to deputize its local and state law enforcement officers to enforce federal immigration law, who did all these people go to for support? The Republican Party, that's who. In all those cases, and too many others to mention, conservatives argued for states' rights and local autonomy. Part of the reason for that is their healthy suspicion of an overbearing federal government. Where did those people go? We could use a few of them in California to help us fight off the overbearing – and hypocritical – Trump administration.
Think about the spectacle on the left coast, and how surreal it has become.
California Gov. Jerry Brown says the administration has declared "war" against his state. And what exactly are we going to war over? A con job. A mirage. A so-called sanctuary that offers no safe harbor.
In the new California, as in the old one, local police still cooperate with ICE agents, who still have access to prisoners in jail. People still get deported. Very little has changed.
But those are facts, and politics has no interest in facts. People will believe what they want to believe.
On behalf of the Golden State, this carnival act of an administration can believe this: We'll see you in court.
Email Ruben Navarrette' at ruben@rubennavarrette.com.


text:
Бетюн (фр. Béthune) — многозначный термин.

 Бетюн — город во французском департаменте Па-де-Кале, на старинной дороге из Дуэ и Арраса на Сент-Омер и Кале.
 Бетюн — округ во Франции, один из округов в регионе Нор-Па-де-Кале.
 Клан Бетюн — один из горных кланов Шотландии.

См. также
 Бетюн-Нор — кантон во Франции, находится в регионе Нор-Па-де-Кале, департамент Па-де-Кале.
 Бетюн-Сюд — кантон во Франции, находится в регионе Нор-Па-де-Кале, департамент Па-де-Кале.
 Бетюн-Эст — кантон во Франции, находится в регионе Нор-Па-де-Кале, департамент Па-де-Кале.
 Сюлли, Максимильен де Бетюн (1560—1641) — глава французского правительства при короле Генрихе IV.

redpajama_set_name: RedPajamaWikipedia


Sport Pro-Motion is pleased to present the new medal of Lago Maggiore Half Marathon.
The medal will be put on the neck of all the finishers of the tenth edition of the most important half marathon on Lake Maggiore, both for the participants in the 21k, and the participants in the competitive 10k.
The new medal is characterized by a square in the center of which stands the LMHM logo and Lake Maggiore.
The tenth edition of the Lago Maggiore Half Marathon will start from Verbania Sunday, March 5th, 2017 and it is already possible to register!
Visit our section dedicated to events to find out the detailed program of the event.


The U.S. Court of Appeals for the First Circuit recently held that, under Massachusetts law, a borrower's right to rescind a mortgage loan was not extended where the lender provided a borrower with only one copy of the Notice of Right to Cancel.
A copy of the opinion is available at http://www.ca1.uscourts.gov/cgi-bin/getopn.pl?OPINION=11-1650P.01A.
When a borrower defaulted on her home loan for a property located in Massachusetts, the lending bank (the "bank") successfully foreclosed using the "limited judicial procedure" permitted under Massachusetts law. The bank then informed the borrower of its intention proceed with a foreclosure sale. The borrower responded by asserting a right to rescind the mortgage, and sued to stop the foreclosure sale. The borrower's right to rescind was premised on her allegation that (1) the bank had provided her with one copy of the notice of right to cancel, rather than two; and (2) that the bank understated the finance charge.
The lower court granted a preliminary injunction preventing the bank from selling the home. The bank then moved to remove the matter to federal court, contending that jurisdiction was appropriate given the borrower's federal claims, as well as diversity of citizenship. In the federal district court, the bank's motion to dismiss the borrower's complaint for failure to state a claim was granted. The borrower filed a motion for reconsideration, which was denied. The borrower then appealed.
On appeal, the First Circuit first considered whether the federal district court had subject matter jurisdiction to consider the matter. This analysis was complicated by the fact that although the borrower's claims were styled as arising under state law, the bank's primary assertion in motioning to removing the matter was that the claims raised federal questions. The First Circuit noted that "unsettled questions as to what federal rights are displaced and what others remain where...the Federal Reserve has exempted a state from various [of] TILA's provisions" where, as here, state law establishes requirements substantially similar to those of TILA. However, the Court found resolving those questions to be unnecessary, given that under the facts at issue here, "removal can be supported by diversity jurisdiction..."
Turning to the merits of the matter, the First Circuit examined the borrower's two central claims: (1) that the bank could no longer foreclosure, because it was not the holder of the note; and (2) that the borrower had the right to rescind the loan.
The Court found for the bank in both instances. It began by noting that the Supreme Judicial Court of Massachusetts recently held that a foreclosing entity must demonstrate that it holds both the mortgage and the note. Eaton v. Federal National Mortgage Association, 969 N.E. 2d 1118, 1129-31 (2012) ("Eaton"). However, that same opinion provided that the rule would apply only to foreclosures where the notice of sale was given after the date of the opinion. Id. at 1133. Therefore, the First Circuit held that Eaton provided the borrower with no protection, and accordingly found the borrower's related contentions to be without merit.
Next, the Court turned to the borrower's right of rescission claim, which were brought under the Massachusetts Consumer Credit Cost Disclosure Act ("MCCCDA"), which as you may recall is substantially similar to the federal Truth in Lending Act. Like TILA, under the MCCCDA, the right of rescission is extended where the borrower is not provided with certain disclosures.
Here, the borrower alleged that she received only one copy of her "Notice of Right to Cancel," rather than two as required by statute. The lower court held that where a borrower receives one such notice, the rescission period is not extended. The Court agreed, noting that although the MCCCDA says "nothing about the lack of multiple copies being a basis for rescission," the language concerning the extension of the rescission period refers to "written notice," which the Court observed was singular rather than plural. Therefore, the Court held that "lack of notice, not the number of copies" is the "predicate for rescission."
Finally, the Court examined the borrower's claims that the closing attorney overcharged her for title insurance, and therefore that the bank underdisclosed the cost of the transaction in violation of Massachusetts law. The Court affirmed the lower court's dismissal of this claim as well, finding that "[n]othing in [the borrower's] complaint provided any...factual basis" for that claim. The Court therefore deemed the borrower's allegations "wholly conclusory."


You can personalise this notebook with a name up to 12 characters and an additional line up to 20 characters long (These will both appear inside the record). Lines 3 & 4 have a character limit of 20 characters per line (which will appear at the bottom of the notebook.All personalisation entered will appear in UPPERCASE.
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text:
\section{Introduction}\label{sec:one}

One of the most important scientific features of planetary microlensing is that it is
sensitive to cold planets lying at around or beyond the snow line. Detecting these
planets is important because, according to the core-accretion theory of the planet
formation \citep{Laughlin2004}, there are abundant solid grains at around the snow line
to be accreted into planetesimals that will eventually evolve into gas giants  by accreting
gas residing in the surrounding disk. It is, in general, difficult to detect these cold
planets using other major planet detection methods such as the radial-velocity and
transit methods because of the long orbital periods of the planets. Hence, the microlensing
method is essential for the demographic studies that encompass planets distributed throughout
a wide region of planetary systems \citep{Gaudi2012}.

For the complete demographics of planets, it is important to accurately estimate the
planet detection efficiency. The efficiency of microlensing planets is calculated as
the ratio of the number of detected planets to the total number of lensing events. If
a fraction of planets are missed despite their signals being above a detection threshold,
then their frequency would be underestimated, and this would lead to an erroneous
evaluation of planet properties.

Strong planetary signals appearing in lensing light curves covered with high cadences
and good photometric precision, for example, OGLE-2018-BLG-1269 \citep{Jung2020a} and
KMT-2019-BLG-0842 \citep{Jung2020b}, can be readily identified. However, identifying planetary
signals for a subset of lensing events is difficult caused by various reasons, such as very
short durations of signals, low photometric precision due to the faintness of the source or
the occurrence of planetary signals during low lensing magnifications, weakness of signals
due to their non-caustic-crossing nature, and relatively sparse coverage of signals for
events detected in low-cadence fields and (or) in the wings of the observing season.  In
some cases of events produced by high-mass planets lying in the vicinity of the Einstein
ring, the planet-induced caustics have a resonant form.  In this case, the planetary signals
can significantly deviate from the typical form of a short-term anomaly \citep{GouldLoeb1992},
and this also makes it difficult to immediately identify the planetary signals. Therefore,
finding unidentified planetary signals in the data of lensing surveys is important for the
accurate estimation of planet frequency.

Searches for unidentified microlensing planets in the data collected by the Korea Microlensing
Telescope Network \citep[KMTNet:][]{Kim2016} survey have been carried out in two major channels.
The first channel is a systematic investigation of the residuals in lensing light curves from
the single-lens single-source (1L1S) fits. This approach has been applied to the KMTNet
prime-field data obtained in the 2018 and 2019 seasons, leading to the discoveries of dozens
of planets: 1 planet (OGLE-2019-BLG-1053Lb) published in \citet{Zang2021}, 6 planets
(OGLE-2018-BLG-0977Lb, OGLE-2018-BLG-0506Lb, OGLE-2018-BLG-0516Lb, OGLE-2019-BLG-1492Lb,
 KMT-2019-BLG-0253Lb, KMT-2019-BLG-0953Lb) published in \citet{Hwang2022}, 1 planet
(OGLE-2018-BLG-0383Lb) published in \citet{Wang2022}, 3 planets (KMT-2019-BLG-1042Lb,
KMT-2019-BLG-1552Lb, KMT-2019-BLG-2974Lb) published in \citet{Zang2022}, and 8 planets
(OGLE-2018-BLG-1126Lb, KMT-2018-BLG-2004Lb, OGLE-2018-BLG-1647Lb, OGLE-2018-BLG-1367Lb,
OGLE-2018-BLG-1544Lb, OGLE-2018-BLG-0932Lb, OGLE-2018-BLG-1212Lb, and KMT-2018-BLG-2718Lb)
published in \citet{Gould2022}.  This approach  is being expanded to the data obtained from
the other fields and to those acquired in other seasons, and 6 planets (KMT-2018-BLG-0030Lb,
KMT-2018-BLG-0087Lb, KMT-2018-BLG-0247Lb, OGLE-2018-BLG-0298Lb, KMT-2018-BLG-2602Lb,
OGLE-2018-BLG-1119Lb)  were recently reported from the investigation of the 2018
sub-prime-field data \citep{Jung2022}.

The second approach for exhuming missing planets is visually inspecting planetary signals.
\citet{Han2020} found 4 microlensing planets (KMT-2016-BLG-2364Lb, KMT-2016-BLG-2397Lb,
OGLE-2017-BLG-0604Lb, and OGLE-2017-BLG-1375Lb) from visually inspecting faint-source events
found during the 2016 and 2017 seasons. \citet{Han2021a} inspected anomalies with no
caustic-crossing features and identified 3 planets (KMT-2018-BLG-1976Lb, KMT-2018-BLG-1996,
and OGLE-2019-BLG-0954). \citet{Han2021b} additionally identified 3 planets (KMT-2017-BLG-2509Lb,
OGLE-2017-BLG-1099Lb, and OGLE-2019-BLG-0299Lb) detected via resonant-caustic channels.
\citet{Han2022} reexamined high-magnification microlensing events in the 2018 season data
and found 1 planet (KMT-2018-BLG-1988Lb) with a very short-duration planetary signal.

This independent visual search for planetary signals complements the AnomalyFinder search
and provides a verification sample for evaluating the effectiveness of the AnomalyFinder
algorithm. The visual search requires modeling a large number of anomalous events to isolate
the ones of interest. The output of the AnomalyFinder is then compared to this modeling to
verify that the anomalies have been correctly classified and vet for ambiguous events, such
as those that suffer from various types of degeneracy. In addition, planets discovered by-eye
but not recovered by the AnomalyFinder search provide important insight into false negatives
in that search.

In this work, we report the discovery of a planet (KMT-2017-BLG-0673Lb) and a planet candidate
(KMT-2019-BLG-0414Lb).  These were both identified from the visual inspection of the KMTNet
data obtained in the peripheral fields, toward which the observational cadences are
substantially lower than that of the prime fields, and thus planetary signals were sparsely
covered. KMT-2019-BLG-0414Lb was also identified by the AnomalyFinder search.  However,
while the anomaly in KMT-2017-BLG-0673 was found by the algorithm, it was rejected by the
operator because the peak data appeared to be ``noisy'', which, in fact, was due to the
planetary signal. This event demonstrates the importance and complementarity of such by-eye
searches.

To present the analyses of the planetary events, we organize the paper as follows. In
Section~\ref{sec:two}, we describe the observations of the planetary lensing events and
the procedure of data reduction.  In Section~\ref{sec:three}, we describe the detailed
features of the observed anomalies, and present analyses of the lensing events conducted
to explain the anomalies.  In particular, we show that there is an alternate,
non-planetary, solution for KMT-2019-BLG-0414, in which the anomaly is explained by an
orbiting companion of the source (xallarap) and which is disfavored by only $\Delta\chi^2=4.2$.
We explain the procedure of modeling and present the lensing parameters constrained by the
modeling. In Section~\ref{sec:four}, we specify the source stars of the events and estimate
angular Einstein radii. In Section~\ref{sec:five}, we estimate the physical lens parameters
by conducting Bayesian analyses of the events.  In Section~\ref{sec:six}, we discuss how
future adaptive optics (AO) observations on 30~m class telescopes can resolve the
planet-xallarap degeneracy for KMT-2019-BLG-0414.  We summarize the results found from
the analyses in Section~\ref{sec:seven}.

\begin{figure}[t]
\includegraphics[width=\columnwidth]{f1.eps}
\caption{
KMTNet fields and cadences.  The locations of the events KMT-2017-BLG-0673 and
KMT-2019-BLG-0414 are indicated by cross marks.
}
\label{fig:one}
\end{figure}

\section{Observations}\label{sec:two}

Observations of the KMTNet survey are being carried out in different cadences depending on
the fields. Six prime fields (KMT01, KMT02, KMT03, KMT41, KMT42, and KMT43) are visited with
a 0.5~hr cadence. Each pair of the fields KMT01-KMT41, KMT02-KMT42, KMT03-KMT43 overlaps but
are shifted to cover the gaps between chips in one of the two fields (about 15\% of the total
region) and thus most region of the prime fields are covered with a 0.25~hr cadence.
For the other fields, the cadences are lower than that of the prime fields with 1.0~hr cadence
for 7 fields (KMT04, KMT14, KMT15, KMT17, KMT18, KMT19, and KMT22), 2.5~hr cadence for 11 fields
(KMT11, KMT16, KMT20, KMT21, KMT31, KMT32, KMT33, KMT34, KMT35, KMT37, and KMT38), and 5~hr
cadence for 3 fields (KMT12, KMT13, and KMT36).  Figure~\ref{fig:one} shows the fields covered
by the KMTNet survey and the observational cadences of the individual fields.

The two planetary events KMT-2017-BLG-0673 and KMT-2019-BLG-0414 were found in the KMT13
and KMT38 fields, toward which observations were conducted with 5~hr and 2.5~hr cadences,
respectively. The equatorial coordinates of the individual events are (RA, DEC)$=$(17:39:01.69,
-33:48:28.91), which correspond to the Galactic coordinates $(l, b)=(-4^\circ\hskip-2pt .882,
-1^\circ\hskip-2pt.373)$, for KMT-2017-BLG-0673, and (RA, DEC)$=$(17:55:24.70, -21:53:43.94),
which correspond to $(l, b)=(7^\circ\hskip-2pt .179, 1^\circ\hskip-2pt .709)$, for
KMT-2019-BLG-0414.  In Figure~\ref{fig:one}, we mark the positions of the two lensing events.

Both events were found solely by the KMTNet survey, and there are no data from the other
currently working surveys of the Optical Gravitational Lensing Experiment
\citep[OGLE:][]{Udalski2015} and the Microlensing Observations in Astrophysics survey
\citep[MOA:][]{Bond2001}.  The event KMT-2017-BLG-0673 occurred before the development
of the KMTNet AlertFinder algorithm \citep{Kim2018b}, which began operation in the 2018 season,
and thus it was identified from the post-season investigation of the data using the KMTNet
EventFinder algorithm \citep{Kim2018a}.  On the other hand, the event KMT-2019-BLG-0414
was found using the AlertFinder system in the early stage of the event on 2019 April 16
(HJD$^\prime \sim 8589.5$), when the apparent source flux was brighter than the baseline
by $\sim 0.15$~mag.

Observations of both events were done using the three KMTNet telescopes. The individual KMTNet
telescopes are located in three sites of the Southern Hemisphere: Cerro Tololo Interamerican
Observatory in Chile (KMTC), the South African Astronomical Observatory in South Africa (KMTS)
and the Siding Spring Observatory in Australia (KMTA). Each of these telescopes has a 1.6~m
aperture and is equipped with a camera yielding 4~deg$^2$ field of view. Images from the survey
were obtained primarily in the $I$ band, and about 9\% of images were acquired in the $V$
band for the source color measurement.

Reductions of images and photometry of the events were carried out utilizing the automatized
pipeline of the KMTNet survey developed by \citet{Albrow2009}. For a subset of the KMTC data
sets, additional photometry were conducted using pyDIA code \citep{Albrow2017} to measure the
source colors of the events. The detailed procedure of the source color measurement will be
discussed in Sect.~\ref{sec:three}. For the data used in the analysis, we readjusted the error
bars estimated from the photometry pipeline using the method of \citet{Yee2012} so that the
data are consistent with their scatter and $\chi^2$ per degree of freedom for each data set
is unity.

\section{Light curve analyses}\label{sec:three}

By inspecting the data of the lensing events detected in the peripheral KMTNet fields covered
with observational cadences $\geq 1 $~hours during the 2017--2019 seasons, we found that
KMT-2017-BLG-0673 and KMT-2019-BLG-0414 exhibit subtle deviations from the 1L1S models.
In Figure~\ref{fig:two}, we present the light curves of the two events.  From a brief glimpse,
the light curves of both events appear to be well described by 1L1S models, which are drawn
over the data points. However, a thorough inspection reveal that there exist weak short-term
anomalies. We mark the regions of the anomalies for the individual events with grey boxes
drawn over the light curves, and the enlarged views of the anomaly regions are shown in
Figure~\ref{fig:three} for KMT-2017-BLG-0673 and in Figure~\ref{fig:four} for KMT-2019-BLG-0414.

In the following subsections, we present analyses of both events conducted to explain the observed
anomalies in the lensing light curves. As will be discussed, the anomalies are well described by a
binary-lens (2L1S) model, in which the mass ratio between the lens components ($M_1$ and $M_2$) is
very small.

\begin{figure}[t]
\includegraphics[width=\columnwidth]{f2.eps}
\caption{
Microlensing light curves of KMT-2017-BLG-0673 and KMT-2019-BLG-0414. The curve drawn over
the data points of each light curve is a 1L1S model, and the box indicates the region of the
anomaly.  The enlarged views of the anomaly regions are shown in Fig.~\ref{fig:three} for
KMT-2017-BLG-0673 and in Fig.~\ref{fig:four} for KMT-2019-BLG-0414.  Colors of data points
are set to match those of the telescopes marked in the legend.
}
\label{fig:two}
\end{figure}

The 2L1S modeling procedure commonly applied to both events are as follows. In the modeling of
each event, we  search for a lensing solution, which represents a set of lensing parameters describing
the observed lensing light curve.  Under the approximation that the relative lens-source motion
is rectilinear, a 2L1S event light curve is described by 7 basic parameters. The first three of
these parameters $(t_0, u_0, t_{\rm E})$ characterize the encounter between the lens and source, and
the individual parameters denote the time of the closest lens-source approach, the separation
at that time (impact parameter) normalized to the angular Einstein radius $\theta_{\rm E}$, and the
event time scale, respectively. The event time scale is defined as the time for the source to
cross the angular Einstein radius, that is, $t_{\rm E} = \theta_{\rm E}/\mu$, where $\mu$
represents the relative lens-source proper motion. The next three parameters $(s, q, \alpha)$
define the binary lens, and the first two parameters represent the projected separation (scaled to
$\theta_{\rm E}$) and mass ratio between $M_1$ and $M_2$, respectively, and the third parameter indicates
the source trajectory angle defined as the angle between the relative source motion and
the binary axis of the lens. The last parameter $\rho$ (normalized source radius), which is
defined as the ratio of the angular source radius $\theta_*$ to $\theta_{\rm E}$, characterizes the
deformation of a lensing light curve by finite-source effects, which occur during the crossing of
a source over the caustic formed by a binary lens.

The searches for the the best-fit lensing parameters were carried out in two steps. In the first
step, we divided the lensing parameters into two groups, and the binary parameters $(s, q)$ in
the first group were searched for via a grid approach with multiple initial values of $\alpha$
evenly divided in the [0 -- 2$\pi$] range, and the other parameters were found via a downhill
approach using a Markov Chain Monte Carlo (MCMC) algorithm. We then construct $\chi^2$ maps on
the $\log s$--$\log q$--$\alpha$ planes, and identify local solutions on the $\chi^2$ maps.  In
the second step, we refine the individual local solutions by letting all parameters, including
$s$ and $q$, vary. If the degeneracies among different local solutions are severe, we present
 multiple solutions, and otherwise we present a single global solution.

\begin{figure}[t]
\includegraphics[width=\columnwidth]{f3.eps}
\caption{
Enlargement of the anomaly region in the lensing light curve of KMT-2017-BLG-0673.  The
solid and dotted curves drawn over the data points are the 2L1S and 1L1S models, respectively.
The residuals from the individual models are shown in the lower two panels. The inset in the
top panel shows the lens system configuration, in which the source trajectory (line with an
arrow) with respect to the caustic (red figures) is shown.  The curve drawn in the bottom
panel is the difference between the 2L1S and 1L1S models.
}
\label{fig:three}
\end{figure}

\subsection{KMT-2017-BLG-0673}\label{sec:three-one}

The anomaly feature of KMT-2017-BLG-0673, shown in Figure~\ref{fig:three}, is characterized by
a single strong anomaly point at HJD$^\prime\sim 7963.9$ ($t_{\rm anom}$) surrounded by weak
positive deviations around $t_{\rm anom}$ during the relatively short time range of $7960\lesssim
{\rm HJD}^\prime \lesssim 7967$. The light curve variation at $t_{\rm anom}$ is discontinuous,
and this suggests that the anomaly point was produced by the source crossing over a caustic,
although the detailed structure of the caustic-crossing feature could not be delineated due to
the sparse coverage of the anomaly caused by the low observational cadence of the field.

Considering that the anomaly appears in the peripheral part of the light curve, it is likely
that the anomaly was generated by a planetary caustic lying at around the planet-host axis
with a separation of $u_{\rm anom}\sim s-1/s$ from the host \citep{Griest1998, Han2006}.  In
this case, the planet-host separation can be heuristically estimated as \begin{equation} s =
{1\over 2} \left[(u_{\rm anom}^2 +4)^{1/2} \pm u_{\rm anom}\right], \label{eq1} \end{equation}
where $u_{\rm anom}=(\tau_{\rm anom}^2+u_0^2)^{1/2}$, $\tau_{\rm anom}=(t_{\rm anom}-t_0)/t_{\rm E}$,
and $t_{\rm anom}\sim 7964$ represents the time of the anomaly.  With the values of $t_0\sim
7973.3$, $u_0\sim 0.12$, and $t_{\rm E} \sim 22$~days obtained from the 1L1S modeling conducted by
excluding the data points around the anomaly, we find two values of $s_{\rm close}\sim 0.81$
and $s_{\rm wide}\sim 1.24$, which correspond to the separations of the close ($s<1.0$) and wide
($s>1.0$) solutions, respectively.

From the 2L1S modeling, we found a unique solution without any degeneracy. In Table~\ref{table:one},
we list the lensing parameters of the solution and the model curve corresponding to the solution
is drawn over the data points in Figure~\ref{fig:three}. It was found that the 2L1S model improved
the fit by $\Delta\chi^2=584.7$ with respect to the 1L1S model. As expected, the anomaly was
produced by a low-mass companion with the binary parameters of $(s, q)\sim (0.81, 5.6\times
10^{-3})$. We note that the planet-host separation matches well the value that was heuristically
estimated from the location of the anomaly in the lensing light curve.

\begin{table}[t]
\small
\caption{Lensing parameters of KMT-2017-BLG-0673\label{table:one}}
\begin{tabular*}{\columnwidth}{@{\extracolsep{\fill}}lllcc}
\hline\hline
\multicolumn{1}{c}{Parameter}    &
\multicolumn{1}{c}{Value }       \\
\hline
$\chi^2$                &   $452.0             $      \\
$t_0$ (HJD$^\prime$)    &   $7973.264 \pm 0.049$      \\
$u_0$                   &   $0.121 \pm  0.006  $      \\
$t_{\rm E}$ (days)            &   $22.36 \pm  0.63   $      \\
$s$                     &   $0.813 \pm  0.005  $      \\
$q$ ($10^{-3}$)         &   $5.58 \pm  1.22    $      \\
$\alpha$ (rad)          &   $3.179 \pm 0.032   $      \\
$\rho$ ($10^{-3}$)      &   $7.56 \pm  2.32    $      \\
\hline
\end{tabular*}
\tablefoot{ ${\rm HJD}^\prime = {\rm HJD}- 2450000$.  }
\end{table}

\begin{table*}[t]
\small
\caption{Lensing parameters of KMT-2019-BLG-0414\label{table:two}}
\begin{tabular}{llllll}
\hline\hline
\multicolumn{1}{c}{Parameter}   &
\multicolumn{2}{c}{2L1S (Sol 1)}  &
\multicolumn{2}{c}{2L1S (Sol 2)}  &
\multicolumn{1}{c}{Xallarap}    \\
\multicolumn{1}{c}{}            &
\multicolumn{1}{c}{Close}       &
\multicolumn{1}{c}{Wide}        &
\multicolumn{1}{c}{Close}       &
\multicolumn{1}{c}{Wide}        &
\multicolumn{1}{c}{}        \\
\hline
$\chi^2$                &  $585.8             $   &  $585.8             $   & $585.9             $  &  $586.0             $  &  $590.0              $     \\
$t_0$ (HJD$^\prime$)    &  $8611.332 \pm 0.005$   &  $8611.330 \pm 0.005$   & $8611.333 \pm 0.005$  &  $8611.335 \pm 0.005$  &  $8611.362 \pm 0.015 $     \\
$u_0$ ($10^{-3}$)       &  $4.33 \pm 0.52     $   &  $4.31 \pm 0.49     $   & $4.48 \pm 0.53     $  &  $4.26 \pm 0.56     $  &  $4.84 \pm    0.63   $     \\
$t_{\rm E}$ (days)            &  $71.32 \pm 7.80    $   &  $71.31 \pm 7.70    $   & $70.77 \pm 7.50    $  &  $74.65 \pm 8.17    $  &  $72.28 \pm     4.48 $     \\
$s$                     &  $0.347 \pm 0.066   $   &  $2.803 \pm 0.599   $   & $0.416 \pm 0.078   $  &  $2.714 \pm 0.376   $  &  --                        \\
$\log q$                &  $-2.23 \pm 0.26    $   &  $-2.26 \pm 0.25    $   & $-2.60 \pm 0.28    $  &  $-2.56 \pm 0.26    $  &  --                        \\
$\alpha$ (rad)          &  $2.986 \pm 0.064   $   &  $3.003 \pm 0.056   $   & $0.783 \pm 0.067   $  &  $0.784 \pm 0.068   $  &  --                        \\
$\rho$ ($10^{-3}$)      &  $< 5               $   &  $< 5               $   & $< 5               $  &  $< 5               $  &  --                        \\
$P$ (day)               &                         &                         &                       &                        & $ 0.9 \pm 0.1        $     \\
$\xi_N$ ($10^{-3}$)     &                         &                         &                       &                        & $  0.84 \pm    0.16  $     \\
$\xi_E$ ($10^{-3}$)     &                         &                         &                       &                        & $  0.00 \pm    0.12  $     \\
$\phi$ (deg)            &                         &                         &                       &                        & $  326.72 \pm   15.39$     \\
$i$ (deg)               &                         &                         &                       &                        & $  11.83 \pm   12.24 $     \\
\hline
\end{tabular}
\end{table*}

The lens system configuration, showing the source motion with respect to the caustic, is
presented in the inset of the top panel in Figure~\ref{fig:three}.  It shows that the anomaly
was generated by the source passage through one of the two planetary caustics induced
by a close planet with $s<1.0$. To be noted among the parameters is that the normalized
source radius $\rho =(7.56\pm 2.32)\times 10^{-3}$ is measured despite the fact that
only a single point covered the caustic. This is possible because the data points lying
adjacent to the caustic point provide an extra constraint on the source radius.

A short-term anomaly can also be produced if a source is a binary \citep{Gaudi1998}.  We
checked this possibility by additionally conducting a binary-source (1L2S) modeling of the
light curve. From this modeling, it was found that the 1L2S model yielded a poorer fit to the
anomaly than the 2L1S model by $\Delta\chi^2 =30.7$, especially in the peripheral region of
the anomaly. We, therefore, exclude the 1L2S interpretation of the anomaly.  We also checked
the feasibility of detecting higher-order effects, including the microlens-parallax effect
\citep{Gould1992} and lens-orbital effect \citep{Batista2011, Skowron2011} induced by the
orbital motion of Earth and the binary lens, respectively.  We found that it was difficult
to securely constrain the lensing parameters defining these higher-order effects not only
because the event time scale was not long enough but also because the photometry was not
sufficiently precise.

\subsection{KMT-2019-BLG-0414}\label{sec:three-two}

The event KMT-2019-BLG-0414 reached a very high magnification at the peak: $A_{\rm peak} >
200$.  The anomaly, whose features are shown in Figure~\ref{fig:four}, occurred near the peak,
and the deviation from the 1L1S model was subtle without any strong signatures, such as would
be generated by a caustic crossing. From the inspection of the residual from the 1L1S model,
presented in the bottom panel, the feature of the anomaly is characterized by two KMTA points
at the peak (HJD$^\prime =8611.11$ and 8611.22) with positive deviations and those around the
peak exhibiting slight negative deviations that lasted for about 2.5 days.

\begin{figure}[t]
\includegraphics[width=\columnwidth]{f4.eps}
\caption{
Enlarged view around the anomaly region in the lensing light curve of KMT-2019-BLG-0414.
Drawn over the data points are the 1L1S model considering finite-source effects (FSPL),
the two 2L1S (solutions~1 and 2) models, and   the binary-source model considering xallarap
effects (xallarap).  The model curves of the two 2L1S models are difficult to be resolved
within the line width due to the severe degeneracy between the models. The four bottom panels
show the residuals from the individual models.  The two left insets in the top panel show
the lens-system configurations of the two 2L1S solutions,  and the right inset shows the
configuration of the xallarap model.  The blue and red curves in the bottom panel represent
the differences of the 2L1S solutions 1 and 2 from the FSPL model, respectively.
}
\label{fig:four}
\end{figure}

\begin{table*}[t]
\small
\caption{Source properties\label{table:three}}
\begin{tabular}{lllll}
\hline\hline
\multicolumn{1}{c}{Quantity}             &
\multicolumn{1}{c}{KMT-2017-BLG-0673}    &
\multicolumn{1}{c}{KMT-2019-BLG-0414}    \\
\hline
$(V-I, I)_{\rm S}$        &  $(3.728 \pm 0.063, 17.291\pm 0.006)  $    &  $(2.603 \pm 0.029, 21.476 \pm 0.003)$      \\
$(V-I, I)_{\rm RGC}$      &  $(3.693, 17.517)                     $    &  $(2.966, 17.435)                    $      \\
$(V-I, I)_{\rm RGC,0}$    &  $(1.060, 14.377)                     $    &  $(1.060, 14.239)                    $      \\
$(V-I, I)_{\rm 0,S}$      &  $(1.096 \pm 0.063, 14.150 \pm 0.006) $    &  $(0.697 \pm 0.029, 18.280\pm 0.003) $      \\
$\theta_*$ ($\mu$as)      &  $7.29 \pm 0.70                       $    &  $0.68\pm 0.05                       $      \\
\hline
\end{tabular}
\end{table*}

From the 2L1S modeling of the light curve, we found 2 sets of planetary solutions with source
trajectory angles of $\alpha \sim 3.00$ (in radian) and $\sim 0.78$.  We refer to the solutions
as  2L1S ``solution~1'' and ``solution~2'', respectively. For each solution, we identified
a pair of solutions resulting from the close-wide degeneracy \citep{Griest1998, Dominik1999},
and thus there are 4 solutions in total. Regardless of the solution, the estimated mass ratios
between the lens components are in the range of [3.3 -- 4.7]$\times 10^{-3}$, indicating that
the companion to the lens is a planet. The fit improvement of the 2L1S models with respect to
a 1L1S model conducted with the consideration of finite-source effects is $\Delta\chi^2= 90.8$,
indicating that the planetary signal is securely detected.

In Table~\ref{table:two}, we list the lensing parameters of the 4 degenerate planetary 2L1S
solutions along with the $\chi^2$ values of the fits. The degeneracies among the solutions
are very severe with $\Delta\chi^2 <0.2$. In Figure~\ref{fig:four}, we present the model
curves and residuals of solutions~1 and 2. The lens system configurations of the solutions~1
and 2 are shown in the left and right insets inserted in the top panel of Figure~\ref{fig:four},
respectively, where the presented configurations are for the close solutions. Despite the large
difference in the source trajectory angle, $\alpha\sim 3.00$ for solutions~1 and $\sim 0.78$ for
solution~2, the planet parameters, $(s, q)\sim (0.35/2.8, 4.7\times 10^{-3})$ for solution~1 and
$(0.42/2.7, 3.3\times 10^{-3})$ for solution~2, are similar to each other, and thus the caustics
of both solutions appear to be similar to each other. For both solutions, the anomaly was produced
by the source approach close to the central caustic induced by a planetary companion. The two points
with positive deviations appeared when the source approached the cusp of the caustic.  Although the
normalized source radius cannot be measured because the source did not cross the caustic, the
modeling yields an upper limit of $\rho_{\rm max}\sim  5 \times  10^{-3}$.

We additionally checked the binary-source origin the anomaly.  Under the static 1L2S
interpretation without the orbital motion of the source, we found that the anomaly could
not be explained by the model because the light curve exhibited both positive and negative
deviations, while the 1L2S model could produce only positive deviations.  However, a negative
deviation can be produced by a xallarap effect, in which a faint source companion induces
a variation of the primary source motion by the orbital motion \citep{Griest1992, Han1997}.
Following the parameterization of \citet{Dong2009}, we thus carried out a xallarap modeling
by adding 5 extra parameters of ($\xi_{{\rm E},N}, \xi_{{\rm E},E}$, $P$, $\phi$, $i$) to
those of the 1L1S model.  Here $(\xi_{{\rm E},N}, \xi_{{\rm E},E})$ are the north and east
components of the xallarap vector $\mbox{\boldmath $\xi$}_{{\rm E}}$, $P$ denotes the orbital period,
$\phi$ is the phase angle, and $i$ represents the inclination of the source orbit.  From
this modeling, we found a xallarap solution that approximately explained the observed anomaly.
We list the lensing parameters of the best-fit xallarap solution in Table~\ref{table:two},
and present the model curve, its residual, and the lens system configuration in
Figure~\ref{fig:four}.  According to the model, the source is accompanied by a close faint
companion inducing a very short orbital period of $\sim 1$~day.  Although the xallarap fit
is not preferred over the the 2L1S solutions, the $\chi^2$ difference is minor with $\Delta
\chi^2\sim 4.2$.  We, therefore, consider the xallarap solution as a viable interpretation of
the event.  Had the Einstein radius of the lens system been measured, the minimum mass of the
source companion could be constrained by the relation of $M_{S_2,{\rm min}}=(\xi_{\rm E}
\hat{r}_{\rm E}/{\rm AU})^3/(P/{\rm yr})^2$ to judge the validity of the xallarap solution,
but this constraint could not be applied to the lens system because the normalized source
radius could not be measured.  Here $\hat{r}_{\rm E}=D_{\rm S}\theta_{\rm E}$ denotes the physical
Einstein radius projected on the source plane.  We note that the model curves of the the 2L1S
and xallarap solutions differ from each other in the region not covered by data points,
indicating that the degeneracy between the solutions could have been resolved if the event
had more continuous coverage. In particular, the two models differ by $\sim 0.1$~mag during
the KMTC observing window centered on HJD$^\prime \sim 8610.75$. Unfortunately, KMTC was
weathered out on that night.

\section{Source stars and Einstein radii}\label{sec:four}

In this section, we characterize the source stars of the events.  Characterizing the source
star is important not only to fully describe the event but also to measure the Einstein
radius, which is related to the lensing parameter of the normalized source radius by
\begin{equation}
\theta_{\rm E} = {\theta_* \over \rho},
\label{eq2}
\end{equation}
where the angular source radius can be deduced from the source type. See below for the detailed
procedure of the $\theta_*$ estimation. Measurement of the Einstein radius is important because it
is related to the mass $M$ and distance to the lens $D_{\rm L}$ as $\theta_{\rm E}=(\kappa M\pi_{\rm rel})^{1/2}$,
and thus $\theta_{\rm E}$ can provide an extra constraint on the mass and distance to the lens in addition
to the basic observable of the event time scale.  Here $\kappa\equiv 4 G/c^2\,{\rm AU}\simeq
8.14\,{\rm mas}/M_\odot$ and $\pi_{\rm rel}$ represents the relative lens-source parallax, that is,
$\pi_{\rm rel}={\rm AU}(D_{\rm L}^{-1} - D_{\rm S}^{-1})$, where $D_{\rm S}$ is the distance to the
source.   We specified the source stars of the events by measuring their color and brightness.  In
order to estimate the extinction- and reddening-corrected (de-reddened) color and magnitude of the
source, $(V-I, I)_{\rm S,0}$, from the instrumental values, $(V-I, I)_{\rm S}$, we applied the
\citet{Yoo2004} routine. In this routine, the centroid of the red giant clump (RGC) in the
color-magnitude diagram (CMD) with its known de-reddened color and magnitude \citep{Bensby2013,
Nataf2013} was used as a reference for the calibration of the source color and brightness.

\begin{figure}[t]
\includegraphics[width=\columnwidth]{f5.eps}
\caption{
Source locations with respect to the centroids of red giant clump (RGC) in the instrumental
color-magnitude diagrams of stars lying in the neighborhood of the source of KMT-2017-BLG-0673
and KMT-2019-BLG-0414 constructed using the pyDIA photometry of KMTC data set. Also marked are
the positions of the blend.
}
\label{fig:five}
\end{figure}

Figure~\ref{fig:five} shows the CMDs of stars lying in the neighborhood of the source stars
of the two events constructed with the photometry data processed using the pyDIA code
\citep{Albrow2017}. In each CMD, we mark the positions of the source and RGC centroid by a
blue dot and a red dot, respectively.  Also marked is the position of a blend, which is marked
by a green dot, indicating that the blended fluxes of both events are dominated by bright disk
stars. We will discuss the nature the blend in the following section. For the estimation of the
source position in the CMD, we measured the $I$- and $V$-band magnitudes of the source by regressing
the data of the individual passbands processed using the pyDIA photometry code with the variation
of the lensing magnification. By measuring the offsets in color and magnitude between the source
and RGC centroid in the CMD, $\Delta (V-I, I) = [(V-I, I)_{\rm S} - (V-I, I)_{\rm RGC}]$, then
the de-reddened color and magnitude of the source  were estimated as
\begin{equation}
(V-I, I)_{\rm S,0} = (V-I, I)_{\rm RGC,0} + \Delta (V-I, I).
\label{eq3}
\end{equation}
In Table~\ref{table:three}, we list the values of $(V-I, I)_{\rm S}$, $(V-I, I)_{\rm RGC}$,
$(V-I, I)_{\rm RGC,0}$, and $(V-I, I)_{\rm 0,S}$ for the two lensing events. According to the
measured color and magnitude, it was found that the source of KMT-2017-BLG-0673 was a K-type
giant and the source of KMT-2019-BLG-0414 was a G-type main-sequence star.

We estimated the source radii of the events by first converting $V-I$ into $V-K$ using the
color-color relation of \citet{Bessell1988}, and then derived
$\theta_*$ from the
$(V-K, V)$--$\theta_*$ relation of \citet{Kervella2004}.  The estimated angular radii of the
source stars are
\begin{equation}
\theta_* =
\begin{cases}
(7.29 \pm 0.70)~\mu{\rm as}, & \textrm{for KMT-2017-BLG-0673}, \\
(0.68 \pm 0.05)~\mu{\rm as},  & \textrm{for KMT-2019-BLG-0414}.
\end{cases}
\label{eq4}
\end{equation}
From the relation in Equation~(\ref{eq2}), it is estimated that the angular Einstein radii of
the two events are
\begin{equation}
\theta_{\rm E} =
\begin{cases}
(0.96 \pm 0.31)~{\rm mas}, & \textrm{for KMT-2017-BLG-0673}, \\
> 0.14~{\rm mas},          & \textrm{for KMT-2019-BLG-0414}.
\end{cases}
\label{eq5}
\end{equation}
With the values of the event time scales, the relative lens-source proper motions,
$\mu=\theta_{\rm E}/t_{\rm E}$, are estimated as
\begin{equation}
\mu =
\begin{cases}
(15.74 \pm 5.05)~{\rm mas/yr}, & \textrm{for KMT-2017-BLG-0673}, \\
> 0.7~{\rm mas/yr},            & \textrm{for KMT-2019-BLG-0414}.
\end{cases}
\label{eq6}
\end{equation}
For KMT-2019-BLG-0414, we present the lower limits of $\theta_{\rm E}$ and $\mu$ because only an
upper limit on $\rho$ is obtained for this event.

\begin{table*}[t]
\small
\caption{Physical lens parameters\label{table:four}}
\begin{tabular}{lccccc}
\hline\hline
\multicolumn{1}{c}{Quantity}               &
\multicolumn{1}{c}{KMT-2017-BLG-0673}      &
\multicolumn{4}{c}{KMT-2019-BLG-0414}      \\
\multicolumn{1}{c}{}                       &
\multicolumn{1}{c}{}                       &
\multicolumn{2}{c}{Solution 1}             &
\multicolumn{2}{c}{Solution 2}             \\
\multicolumn{1}{c}{}                       &
\multicolumn{1}{c}{}                       &
\multicolumn{1}{c}{Close}                  &
\multicolumn{1}{c}{Wide}                   &
\multicolumn{1}{c}{Close}                  &
\multicolumn{1}{c}{Wide}                   \\
\hline
$M_{\rm h}$ ($M_\odot$)      &  $0.63^{+0.37}_{-0.35}$   &  $0.74^{+0.43}_{-0.38}$   & $\leftarrow          $  &  $\leftarrow          $  &  $\leftarrow           $ \\  [0.7ex]
$M_{\rm p}$ ($M_{\rm J}$)    &  $3.67^{+2.17}_{-2.07}$   &  $4.57^{+3.74}_{-2.06}$   & $4.26^{+3.32}_{-1.87}$  &  $1.95^{+1.76}_{-0.93}$  &  $2.14^{+1.75}_{-0.96} $ \\  [0.7ex]
$D_{\rm L}$ (kpc)                  &  $5.08^{+1.22}_{-1.59}$   &  $4.41^{+1.79}_{-1.93}$   & $\leftarrow          $  &  $\leftarrow          $  &  $\leftarrow           $ \\  [0.7ex]
$a_\perp$ (AU)               &  $2.34^{+0.56}_{-0.74}$   &  $1.16^{+0.47}_{-0.51}$   & $9.42^{+3.83}_{-4.12}$  &  $1.40^{+0.57}_{-0.61}$  &  $9.12^{+3.71}_{-3.99} $ \\  [0.7ex]
disk/bulge                   &  $63\%/37\%           $   &  $73\%/27\%           $   & $\leftarrow          $  &  $\leftarrow          $  &  $\leftarrow           $ \\  [0.7ex]
\hline
\end{tabular}
\end{table*}

\begin{figure}[t]
\includegraphics[width=\columnwidth]{f6.eps}
\caption{
Bayesian posteriors of the host mass for the planetary systems KMT-2017-BLG-0673L (upper panel) and
KMT-2019-BLG-0414L (lower panel). The vertical line in each panel represents the median value and the
two dotted vertical lines indicate the 1$\sigma$ range of the distribution. The curves drawn in blue
and red represent the contributions of the disk and bulge lens populations, respectively.
}
\label{fig:six}
\end{figure}

\section{Physical lens parameters}\label{sec:five}

The physical parameters of the lens mass and distance are constrained by the lensing observables
of $t_{\rm E}$, $\theta_{\rm E}$, and $\pi_{\rm E}$, which are related to the physical parameters.  The basic parameter
of the event time scale was securely measured for both events, the Einstein radius was measured for
KMT-2017-BLG-0673, while only a lower limit was obtained for KMT-2019-BLG-0414.  However, the microlens
parallax could not be measured for either event.  Although the partial measurements of the lensing
observables make it difficult to uniquely determine $M$ and $D_{\rm L}$ from the relations \citep{Gould2000}
\begin{equation}
M= {\theta_{\rm E} \over \kappa\pi_{\rm E}};\qquad
D_{\rm L} ={{\rm AU} \over \pi_{\rm E}\theta_{\rm E} + \pi_{\rm S}},
\label{eq7}
\end{equation}
it is still possible to constrain the physical parameters with the measured observables of the
individual events from a Bayesian analysis.

\begin{figure}[t]
\includegraphics[width=\columnwidth]{f7.eps}
\caption{
Bayesian posteriors of the distance to the planetary system. Notations are same as those in
Fig.~\ref{fig:six}.
}
\label{fig:seven}
\end{figure}

In the Bayesian analysis, we first produced a large number ($10^7$) of lensing events by conducting
a Monte Carlo simulation based on a Galactic model. The Galactic model defines the matter density,
motion, and mass function of Galactic objects. From the physical parameters of the simulated events,
we computed the lensing observables of $t_{{\rm E},i}=D_{\rm L} \theta_{\rm E}/v_\perp$ and $\theta_{{\rm E},i}
=(\kappa M \pi_{\rm rel})^{1/2}$.  Here $v_\perp$ represents the transverse speed between the lens
and source.  We then constructed Bayesian posteriors of the lens mass and distance
with a weight assigned to each simulated event computed by $w_i=\exp(-\chi^2/2)$, where $\chi^2=
(t_{{\rm E},i}-t_{\rm E})^2/\sigma({t_{\rm E}})^2+(\theta_{{\rm E},i}-\theta_{\rm E})^2/\sigma(\theta_{\rm E})^2$, $\sigma(t_{\rm E})$
and $\sigma(\theta_{\rm E})$ represent the uncertainties of $t_{\rm E}$ and $\theta_{\rm E}$ estimated from the modeling,
respectively. In the simulation of lensing events, we used the \citet{Jung2021} Galactic model.

In Figures~\ref{fig:six} and \ref{fig:seven}, we present the posteriors of the host mass and distance
to the planetary systems, respectively. For each distribution, the solid vertical line denotes the
median value, and the two dotted vertical lines represent the 1$\sigma$ range estimated as 16\% and
84\% of the distribution. We separately mark posterior distributions of the disk and bulge lens
populations with blue and red curves, respectively. In Table~\ref{table:four}, we summarize the
estimated masses of the host ($M_{\rm h}$) and planet ($M_{\rm p}$), distances, and projected
planet-host separations ($a_\perp=sD_{\rm L}\theta_{\rm E}$) for the two planetary systems. For KMT-2019-BLG-0414,
we present four sets of parameters corresponding to the four degenerate solutions. We note that the
primary mass and distance of KMT-2019-BLG-0414L estimated from the degenerate solutions are alike
regardless of the solution because the constraint given by the lower limit of $\theta_{\rm E}$ is very weak
and the other constraint of the event time scales of the degenerate solutions are nearly identical.

It is found that the two planetary systems are very similar to each other in many aspects. First,
both systems have planets heavier than the Jupiter of the Solar system with masses $M_{\rm p}\sim
3.7~M_{\rm J}$ and $\sim [2.0$--$4.5]~M_{\rm J}$ for KMT-2017-BLG-0673L and KMT-2019-BLG-0414L,
respectively. Second, the masses of the planet hosts, $M_{\rm h}\sim 0.6~M_\odot$ and $\sim
0.7~M_\odot$ for the individual lenses, are also similar to each other. Third, the distances to
the systems, $D_{\rm L}\sim 5.1$~kpc and $\sim 4.4$~kpc, indicate that both planetary systems are likely
to be in the disk. According to the Bayesian estimation, the probability for the planetary system
to be in the disk is $\sim 63\%$ for KMT-2017-BLG-0673L and $\sim 73\%$ for
KMT-2019-BLG-0414L.

Prompted by the facts that the lenses of both events are likely to be in the disk and the blended
fluxes come from disk stars, we inspected the possibility of the lenses of the events to be the
main sources of the blended flux. For this inspection, we examined the reference images taken
before the lensing magnification and the difference image taken during the lensing magnification.
For KMT-2017-BLG-0673, there exists a star even brighter than the source of a bulge giant at a
location with a separation of $\sim 2.2$~arcsec from the source, and this degrades the photometry
and astrometry of the event together with the high extinction, $A_I\sim 3.1$~mag, toward the field.
Nevertheless, we identified a blend lying at a separation of $\sim 0.65$~arcsec from the source with
a brightness corresponding to the blend. This indicates that the lens is not the main source of the
blended flux. For KMT-2019-BLG-0414, the astrometric offset between the centroid of baseline object
measured on the reference image, $\theta_{\rm ref}=[(f_s/f_b)\theta_s+\theta_b]/(f_s/f_b+1)$, and
the source position measured on the difference image, $\theta_s$, is $\Delta\theta=|\theta_{\rm ref}
-\theta_s|=(79.2\pm 59.2)$~mas.  Here $f_s$ and $f_b$ represent the flux values of the source and
blend, respectively.  In the case of KMT-2019-BLG-0414, $f_b\gg f_s$, and thus the centroid shift
can be approximated as $\Delta\theta\sim |\theta_b-\theta_s|$.  Considering that the measured
astrometric offset is only 1.3 times greater than the uncertainty, it is difficult to firmly
exclude the possibility that the lens is the major source of blended light based on the argument
of the measurement uncertainty.

\section{Resolution of KMT-2019-BLG-0414 Degeneracy}\label{sec:six}

In this section, we discuss the possibility of resolving the degeneracy between the 2L1S and
xallarap solutions of KMT-2019-BLG-0414 by means of AO observations on 30~m class telescopes,
which may see first light in about 2030.  We give a brief synopsis of the decision tree governing
these observations.

In the 2L1S model, $\rho<0.005$ at $3\,\sigma$ confidence, which implies, $\mu>0.7$~mas~yr$^{-1}$
(see Equation~(\ref{eq6})). If $\mu$ is really at the threshold of this limit, then several
decades would be required to separately resolve the lens and source. However, typical lens-source
relative proper motions are substantially higher than this, and therefore, most likely, 30~m-class
AO imaging in 2030 will resolve them. This will yield a heliocentric proper motion measurement.
One must be careful to correct from heliocentric to geocentric proper motion using
\begin{equation}
\mbox{\boldmath $\mu$}_{\rm geo} = \mbox{\boldmath $\mu$}_{\rm hel} - {{\bf v}_{\oplus,\perp}\over {\rm AU}}\pi_{\rm rel},
\label{eq8}
\end{equation}
where ${\bf v}_{\oplus,\perp}(N,E) = (-0.7,+21.6)~{\rm km~s}^{-1}$ is the projected velocity
of Earth at the peak of the event. However, we ignore this correction in the following
simplified treatment. Because $t_{\rm E} \simeq {\rm yr}/5$ is well measured in both models, such
a proper motion measurement will immediately yield a determination of the Einstein radius:
$\theta_{\rm E} \simeq 0.6~{\rm mas}~(\mu/3\,{\rm mas}~{\rm yr}^{-1})$.

Within the context of the xallarap model, this will yield the semi-major axis of the orbit of
the primary, i.e., $a_{\rm primary}=\xi\theta_{\rm E} D_{\rm S}=1.25~R_\odot~(\mu/3~{\rm mas~yr}^{-1})$,
where we have assumed a source distance of $D_{\rm S}=8$~kpc. Combined with the period measurement
$P=0.9$~day, a source-mass estimate of $M_{\rm S} \simeq 1\,M_\odot$ and Kepler's Third Law, this
will yield the mass of the source companion. For example, for $\mu=3~{\rm mas~yr}^{-1}$,
$M_{\rm companion}\sim 0.4\,M_\odot$ (which would account for its lack of photometric signature).
However, if $\mu$ were measured to be sufficiently large, this might imply photometric signatures
from a luminous orbiting companion and (or) eclipses, which might rule out the xallarap scenario.

Assuming that xallarap solutions survive this test, there remains a radial-velocity (RV) test
of the xallarap hypothesis. The amplitude of the RV signature would be $v\sin i = 2\pi (a_{\rm
primary}/P) \sin i = 70~{\rm km~s}^{-1} (\mu/3~{\rm mas~yr}^{-1})\sin i$.  The source is
$I_{\rm S} \sim 21.5$ ($K_{\rm S} \sim 18.0$), so RV signatures of amplitude $\ll 1~{\rm km~s}^{-1}$
should be detectable with 30~m-class AO spectroscopy. If these signatures are not detected, then
the xallarap model would become highly implausible because it would require an almost perfectly
face-on orbit.  For completeness, we note that {\it Gaia} DR3 reports a parallax and proper
motion for the baseline object of $\pi_{\rm base} = (1.1\pm 0.4)$~mas and $\mbox{\boldmath $\mu$}_{\rm base}(E,N)
= (-0.4\pm 0.4,-2.3\pm 0.3)~{\rm mas~yr}^{-1}$. As shown in Figure~\ref{fig:five}, the baseline
object is dominated by the blend.  While the parallax error is large, the low proper motion is
also consistent with the blend being a nearby object. This object is most likely dominated by
the host or a companion to the host. By the time 30~m-class AO is available, the parallax error
will likely be reduced by a factor $\sim 1.7$, so Gaia astrometry may substantially aid the
interpretation of the AO images.

\section{Summary}\label{sec:seven}

We presented analyses of two microlensing events KMT-2017-BLG-0673 and KMT-2019-BLG-0414, for
which the presence of planets in the lenses were found from the inspection of the microlensing
data collected by the KMTNet survey during the 2017--2019 seasons in the peripheral Galactic
bulge fields.  The planetary signal of KMT-2017-BLG-0673 had been previously missed because of
the relatively sparse coverage of the event, and the signal of KMT-2019-BLG-0414 had not been
identified due to the weakness of the signal caused by its non-caustic-crossing nature.  The
detections of the planets indicate the need for thorough investigations of non-prime-field
lensing events for the complete census of microlensing planet samples.

For KMT-2017-BLG-0673, we identified a unique planetary solution with lensing parameter of $(s, q)
\sim  (0.81, 5.6\times 10^{-3})$.  It was found that the planetary signal was generated by the
source passage through one of the two tiny planetary caustics induced by a planet lying inside
the Einstein ring of the planetary system.

For KMT-2019-BLG-0414, on the other hand, we identified two pairs of solutions, for each of which
there were two solutions caused by the close-wide degeneracy.  Despite the fact that the incidence
angles of the two sets of solutions differed from each other, the planet parameters of the projected
planet-host separations and mass ratios were similar to each other.  Although slightly less favored,
the anomaly could also be explained by a model, in which a single lens mass magnified a rapidly
orbiting binary source with a faint companion. In Section~\ref{sec:six}, we discussed how the
planet/xallarap degeneracy might one day be resolved by AO observations on 30~m class telescopes.
Pending such resolution, KMT-2019-BLG-0414Lb should not be included in catalogs of
``known planets.''

From the physical parameters estimated by conducting Bayesian analyses based on the observables of
the events, it was found that the two planetary systems were similar to each other in many aspects.
For both planetary systems, the hosts of the planets are stars with masses lower than the Sun, and
they host planets heavier than the Jupiter of the Solar system.  Furthermore, both planetary systems
reside in the disk of the Galaxy.

\begin{acknowledgements}
Work by C.H. was supported by the grants of National Research Foundation of Korea
(2020R1A4A2002885 and 2019R1A2C2085965).
This work was financially supported by the Research Year of Chungbuk National University in 2021.
This research has made use of the KMTNet system operated by the Korea Astronomy and Space
Science Institute (KASI) and the data were obtained at three host sites of CTIO in Chile,
SAAO in South Africa, and SSO in Australia.
J.C.Y.  acknowledges support from NSF Grant No. AST-2108414.
W.Z. and H. Y. acknowledge the support by the National Science Foundation of China (Grant
No. 12133005).
\end{acknowledgements}

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