Fair Dealing and Online Content Curation: Can I do it?
Online Content Curation: Can I do it?
The internet is a platform for collating, collaborating and curating. Just think of all the major social networks and news aggregators and imagine just how much of their content is actually their own. Many online businesses in Australia are building their ideas on models that follow the same strategy. If you are following this track, this article will run through some of the legal aspects of this business model including aggregation, fair dealing and licensing.
You can base an entire website on the automatic aggregation of other people's information. Essentially, a website can exist without having produced a piece of original work, but rather by aggregating from various other content creators. This system often exists without permission from the original creators.
For a website that builds their model on aggregation, they may face the issue of copyright infringement. However, infringement could be countered with the argument that use of the content was "fair".
"Fair Dealing" is a legal term describing the ability to use content without permission. For businesses who thrive on the creation of original content, aggregation websites are a threat because external parties can monetise on the content the business has created.
The clause relating to Fair Dealing in the Copyright Act 1968 (Cth) runs through the situations where the use of copyright material would be authorised even without the permission of the copyright owner. This becomes relevant as one of the fair dealing provisions allows for the use of content for the purpose of reporting the news. For other websites that don't aggregate information for the purpose of reporting the news, it would be difficult to rely on the Fair Dealing provision.
An option for many organisations is to strike a deal with the content creator. This can take the form of a Licence Agreement that allows the aggregator to use copyright content for a royalty fee. As the interests of the aggregator and content creator may conflict, this is essentially a question of commercial negotiation.
Content curation and aggregation is a developing area of law that is usually played out between many of the larger online businesses. Despite major cases involving search engines, larger news organisations and subscription-based information providers, small businesses intending to operate similar business models may also face these issues. Our team of specialist online lawyers can provide you with advice on your business plans and guide you through the potential legal issues you need to consider.


This morning, I was driving my son to daycare and I had to drive through the area around CBC at 7:30 am. If you have ever had to try to drive by CBC at this time you know it is almost impossible. The city of Pasco needs to do something about this and I have a simple solution.
The main problem is that all the traffic from the exit on the west side of New Horizons all the way to the airport has to go one way. There is no easy way to 395 unless you go all the way back to road 68 or back down to the Pasco Red Lion past CBC. This causes huge traffic problems from all the students and staff from both campuses arriving at the same time. I went to a major university and I never saw traffic like this at any time of the day. All they need is to add an exit out to 395 off the west side of New Horizons and to expand the road to 3 lanes behind CBC. The extra lane would allow for a turn lane into campus and allow the through traffic to go around people turning in.
Maybe I should run for office!


What is the Trend for "WLFC" Stock?
Short Term : "WLFC" is trading above the Weekly Pivot at 0. Short term trend is Up.
Medium Term : "WLFC" is trading below the Monthly Pivot at N/A. Medium term trend is Down.
Long Term : "WLFC" is trading below the Yearly Pivot at N/A. Long term trend is Down.
What Can We Learn From Willis Lease Finance Corporation's (NASDAQ:WLFC) Investment Returns?


text:
Two experienced experts at the helm of RAMPF Machine Systems
Wangen (near Göppingen), 10/20/17.
RAMPF Machine Systems, an international development partner and system supplier for complete machine bed solutions and machine systems, is being led by a strong team comprising managing directors Thomas Altmann and Dirk Haumann.
Thomas Altmann (48) has held managerial positions in machine sales for more than 17 years and was Director of Sales and Marketing at RAMPF Machine Systems in Wangen from April to September 2017. He graduated in mechanical engineering from Esslingen University of Applied Sciences, majoring in production systems. His areas of responsibility are:
Design and development / engineering
Over the past 22 years, Dirk Haumann (54) has held managerial positions at the Fraunhofer Society, automotive suppliers, consultancies, and mechanical / plant engineering companies.
During this time, he has gathered extensive international experience in the fields of operational excellence, lean management, and developing innovative production concepts. The University of Stuttgart mechanical engineering graduate is also a qualified mechanic.
His areas of responsibility are:
Operational business
Purchasing and materials management / supply chain
Chemical laboratory and chemical development
"We're delighted that in Thomas Altmann and Dirk Haumann we have two highly competent and experienced executives at the helm of RAMPF Machine Systems," says Michael Rampf, CEO of RAMPF Holding. "In the years ahead, we'll be further expanding the product and service portfolio for highly dynamic production engineering and pressing ahead with our internationalization," he adds.
RAMPF Machine Systems supplies its customers worldwide with innovative system solutions, basic machinery, and positioning / moving systems based on machine beds and machine bed components made of high-performance materials such as mineral casting, ultra-high performance concrete, natural hard stone, and fiber composites. The company forms part of the international RAMPF Group and is the world's largest mineral casting manufacturer.
01/15/22 RAMPF makes design dreams come true
01/30/18 High-performance material with outstanding ecological credentials

redpajama_set_name: RedPajamaCommonCrawl


Find a reliable and flexible partner in Condor Heavy Services, an integral link in the logistical process of offshore windmill construction. We facilitate your needs with our climate-controlled warehouse, located in the heart of the Port of Rotterdam.
The logistical process of offshore windmill construction is full of different complex challenges. For every individual aspect, you will want a solution that is a perfect fit and partners who are reliable. Where storage, transshipment and assembly of wind turbines and related engineering are concerned, Condor Heavy Services will facilitate you with a fully equipped climate-controlled warehouse.
An area of 12500 m2, including a container spreader capacity of 500 TUE.
Feel free to come by and discover for yourself how our high-quality storage, transshipment and assembly facilities supporting offshore windmill construction can benefit you. You can download the specifications of the warehouse or contact us for more information.
With our indoor storage facilities, we offer support for part of your logistical process. We are happy to adapt to your process at every turn, so you stay in control of the way in which you choose to run the process. For example, you would be able to store part of your goods at another location or communicate specific times at which your technicians and engineers need to be able to gain access to the warehouse. We will organize and equip our heated warehouse to perfectly fit your wishes, possibilities and logistics.
Supporting offshore windmill construction requires a versatile working environment. Your demands will naturally and justly be high, and we will undoubtedly be able to fulfill all of them. Our offshore engineering assembly area offers the newest high-end technology certified in accordance with the highest of quality standards, such as ISO 9001, ISPS and OHSAS 18001, by Bureau Veritas. We also raise the bar when it comes to cooperation, by employing short lines of communication and keeping agreements clear and concise.
Judge our vision on reliable partnership in a conversation, by calling 0031 10-303 7000 or dropping by, you're very welcome to do so!


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N.C. NIELSEN'S SPECIALISED MACHINE MOVES Trolly Carts IN BUNDLES
Press releases N.C. Nielsen now launches the new specialised machine NCN Trolly Cart which is a converted Linde pallet truck which can move up to 30 trolly carts with two long and particularly robust "fingers". This is good news for busy distribution centres, terminals and big industrial warehouses, where trolly carts can easily create bottlenecks.
Trolly carts are used for the distribution of groceries to the retailers where they are on-loaded and off-loaded day and night. The filled trolly carts are transported in the truck, emptied on their destination and subsequently returned to the distribution centre in order to get filled for the next delivery.
CONSTANT FLOW OF TROLLY CARTS
The NCN Trolly Cart solves a common problem, i.e. the need to transport a lot of trolly carts over long distances. It therefore makes sense to gather the empty trolly carts in bundles and move them together, in order to handle new tasks in the warehouse. The specialised machine does this instantly by placing the long fingers underneath the trolly carts, lifting them up and attaching them with upper clip pliers and drive on:
– We have developed a reliable and robust specialised machine. The different distribution centres are very busy, and the machines need to be versatile. We have built a very robust specialised machine which makes it easier to handle several trolly carts at a time and transport them over long distances in the big distribution centres, explains technical director Per T. Nielsen from N.C. Nielsen.
CUSTOMISED FORKS
The specialised machine has been constructed as a converted Linde T20AP with new forks at two levels that are 3.5 metres long. The forks are specially built to be placed underneath two rows of 15 trolly carts each which are lifted up, attached by the upper clip pliers and transported to their destination. This manoeuvre takes place very quickly, and the trolly carts then move on to their next stop.
– We have focused on the lift itself, and the need for the operator to keep the full overview from the platform. The operator is well-protected in the operating position and does not need to step down from the machine to handle the trolly carts. The visibility is good both when moving forward and backward, and the machine can drive quickly, keeping the load stable over long distances, explains Per T. Nielsen from N.C. Nielsen.
Would you like to know more about our specialised NCN Trolly Cart, please contact technical director Per T. Nielsen
Per T. NielsenDirector teqnique and production
Tlf. +45 99 83 83 41 Mobil +45 40 55 15 08ptn@nc-nielsen.dk


This article is meant to assist users of Cloud Application Manager willing to access Cloud Application Manager billing section to review billing details.
The user should be at the organization level scope to access the Billing option in the left side menu.
When you click on Billing in the left side menu you will land into a dashboard page, where a bar graph with the billed amount for the previous months will be shown. You can change the range of months being shown in the bars graph by selecting a different value in the date filter and you can also select the consumption categories you want to display with the consumption category type filter.
When you click on Usage History option under the Billing left menu item, you will be able to review your detailed billing information.
When you enter this page, you can see a list with the previous months billing summary, including the period of usage and the total credit and debit amounts for each month.
When you click on a line, the details for that month appears on the bottom of the page, showing the line-items you may encounter in your invoice, including for example your Application Lifecycle charges, your support charges as well as your discounts.
Each line item on the below table includes additional information such as region (where applicable), quantity, cost and total.
Some items have a dropdown icon at the beginning, meaning that you can click on it to drill down and see further details on that item appearing below.
For more information about the usage history details see detailed billing report.
When you click on Pricing option under the Billing left menu item, you will be able to see the Cloud Application Manager default pricing of the different Cloud Application Manager products and services, including the billing type and the hourly or monthly price, depending on the type and the setup fee if any is required.


Portable grill with all the accessories? Definitely make sure you've got that!
Although just about every American town hosts its own Fourth of July celebration, many campers see 4th of July as the perfect excuse to take one of many summer getaways or last-minute vacations. And why not? Pretty much anywhere you go, the weather's going to be gorgeous, and the kids are off school anyhow.
If you're looking for 4th of July travel deals, don't forget about the savings you can find when you rent an RV through RVshare. The peer-to-peer market offers substantial discounts off of traditional dealership prices!
If you're an avid camper, you might also want to invest in a Passport America membership — and not only because of its thematically-appropriate moniker. This discount camping club is the only one that'll get you 50% off your campsite accommodation fees at almost 1900 campgrounds across the country, which spells a whole lot of savings over time. After all, it's less than $50 for a full year's membership!
So, where should you pack up and head this Independence Day? Here are some of our favorite options.
Where better to celebrate America's birthday than the capitol? Washington, DC is well-known to be one of the country's best (and most popular) 4th of July destinations, and better yet, most of its museums and cultural attractions are free year round — including the Fourth of July.
Click here to find RVshare rentals in the Washington, DC area.
If those hiking boots and trekking poles of yours are itching for a workout, you already have ample reason to head to Sedona, one of the most scenic hiking areas in the country. And if you head there in time for the Fourth of July, you'll enjoy a host of totally free events including fireworks and a laser show — as if the town needed any more visual amazement.
Click here to find RVshare rentals in Sedona, Arizona.
Just on the border of the Ouachita National Forest, this destination town hosts a beautiful Fourth of July fireworks display on the shores of Lake Catherine State Park.
Click here to find RVshare rentals in Hot Springs, Arkansas.
Touting itself as the largest fireworks show in the west — which is a tall order — Idaho Falls' Melaleuca Freedom Celebration will once again take place at Snake River Landing this year.
Fun fact: last year's show, the 25th annual, launched more than 20,000 fireworks, weighing over 17,000 pounds, in a 31-minute spectacular production.
Click here to find RVshare rentals in Idaho Falls, Idaho.
The gateway town to the stunning Acadia National Park, Bar Harbor boasts a Fourth of July show good enough to have earned the #1 ranking by the Today Show. And hey, even if it's too cloudy for pyrotechnics, who can beat that coastal Maine view? Click here to read more about Bar Harbor's Independence Day celebration.
Click here to find RVshare rentals in Bar Harbor, Maine.
Whitefish Lake is already high on many campers' travel bucket lists, and if you're looking for a great Fourth of July event, this might just be the ideal time. Better still: the town's stunning, shoreside fireworks display is absolutely free of charge. Click here for full details.
Click here to find RVshare rentals in Whitefish, Montana.
Where better to enjoy your favorite annual 4th of July activities than in the watchful shadow of Mount Rushmore? Several different spots in the Black Hills host fun, free activities for the whole family — click here to learn more.
Click here to find RVshare rentals in the Black Hills area.
The most happening town at the heart of it all goes all out for Independence Day, calling it "America's Biggest Birthday Party." This year, St. Louis is hosting events both on the 4th of July proper — which falls on a Wednesday — as well as all throughout the following weekend. Click here for the deets.
Click here to find RVshare rentals in St. Louis, Missouri.
They don't call themselves "America's Fourth of July City" for nothing!
The small town of Seward, Nebraska has been hosting an all-out Independence Day bash since all the way back in 1868, so you can rest assured they know a thing or two about how to host a great patriotic celebration. From classics like fireworks and a parade to novelties like car and craft shows, Seward's event truly offers something for everyone — click here for full details.
Click here to find RVshare rentals in Seward, Nebraska.
But if hosting the ultimate RV barbecue party is in your plans this year, don't light that charcoal without checking out our ultimate grillmaster's guide.
There's no denying it: they call it America the Beautiful for a reason.
And if you've just gotta get out there and experience a celebration, simply search for "free fourth of July events near me" to see what cost-free patriotic fun is going on in your area.
Click here to find RVshare rentals near you.
Happy Independence Day, campers! Enjoy exploring the land of the free and the home of the brave.


DREAMING ABOUT THE RV LIFESTYLE?
In this entry I'll talk about the various types of recreational vehicles, how to choose one for the kind of TV lifestyle you are considering, and the reasons for our decision to travel and live in a 5th-wheel coach on an almost full-time basis.
I use the term "RVing" in a broad sense that includes traveling in all types of motorized and towable rigs from pop-up tent campers to bus-like Class A motorhomes. All of them provide mobile living quarters -- they are literally "rolling residences."
Motorhomes, which combine a motor vehicle chassis and living quarters in one unit, include Class A, B, and C rigs (L-R in diagrams below). Full-timers often choose a Class A or C motorhome for their convenience, features, and interior space. They appear to be the most expensive RVs -- until you realize that you need a motorized vehicle to tow all the other types of campers!
Sometimes it's hard to tell the difference between a Class B and a Class C motorhome. Both are built on a van chassis but the Class C typically has a sleeping area over the cab. To confuse things even further, at least one manufacturer has a new, short Class A motorhome (Winnebago Via, shown below) built on a Sprinter chassis that looks like an longer-than-usual Class B. The Mercedes-built Sprinter chassis has pretty much revolutionized the motorhome industry in recent years. A variety of RV manufacturers now offer more fuel-efficient diesel Class As, Bs, and Cs.
Note that the picture of the Class B van in the middle is too large in proportion to the Class A on the left and Class C on the right. Some bus-like Class As are 45 feet long. Class Cs are usually shorter than As but almost always longer than the van-like Bs.
These pictures are also out of proportion, with the two on the right being too large in comparison to the two on the left. Trailers and 5th-wheels typically stretch from about 20 to 40 feet.
Depending on their size, some travel trailers and pop-ups can be pulled by a truck, SUV, van, or car. These units hitch to the tow vehicle's bumper. We've even seen some tiny pop-ups that can be towed by a motorcycle. You need a pick-up truck to haul a 5th-wheel coach or truck camper. Fifth-wheels attach to a large hitch in the bed of the truck.
Note that all or most of these recreational vehicles can be called by several names: RV, camper, rig, coach, unit, and probably some more I can't think of right now. I'll be using all of them in this series.
I went into excruciating detail about purchasing an RV in a series I wrote early last year. Check out the 2010 journal for those entries. The next section focuses more on choosing the best type of RV if you plan to travel and live in it full-time or for extended periods of time.
WHAT TYPE OF RV IS BEST FOR ME?
Figuring that out can be fun if you have a laid-back Type B personality. If you're too O-C about it, you might just drive yourself nuts!
There are many considerations, including cost to purchase and operate the unit, how much space you need/want, and what you want your RV lifestyle to be. Keep in mind that the smaller the RV, the more places you can park it and probably the better your fuel mileage will be. The downside is lack of space in the smaller units.
Let's start with the smallest RVs in size and work up to larger ones.
We don't know anyone who lives for extended periods of time in a pop-up tent camper, even ones with solid and not canvas sides. Some people might do this but it's too primitive for most.
Truck camper tops don't have wheels per se; they slide onto the bed of pick-ups. With some effort, the camper top can be removed at the campsite and used on its own, with the truck detached.
Although Jim and I can't imagine spending much time in one of those, we've known several retired runners who travel all over the country to marathons and ultras in them. I think most of the men still have a home base but they are driving to and from races the majority of the time. Some have done the 50 States & DC marathon/ultra circuit in one year and/or multiple times over a number of years.
I personally think it'd be a recipe for disaster if two people tried to live in one of those for any length of time! YMMV.
L - R: Class B, Class C (I think), and truck camper. They belong to ultra running friends of ours.
We know several couples and individuals who are quite content to travel around in rather small Class B (van-like) and Class C motorhomes, however. Most of these units do not have slide-outs that can be opened while parked to give more interior space. WYSIWYG.
One of the better known couples is prolific 100-miler Hans-Dieter Weisshaar and his wife Susi. Although they own houses in both Germany and Mexico, Hans has spent considerable time traveling to races all around the U.S. during the past decade, often accompanied by Susi and their dog in an older German-made Class C motorhome they shipped over here in the early 2000s. It's the small van-like RV shown in the middle above. Many Class Cs are larger than this one.
Another one of our friends purchased a very nice used Class B Airstream motorhome based on the Sprinter chassis a couple of years ago. It's the van on the left in the photo above. He enjoys traveling in it so much that he sold his house last year and RVs full time in it now.
Many folks who full-time need/want more space than that and purchase larger Class A and C motorhomes, travel trailers, and 5th-wheels.
Class As and Cs can be even longer than that and are often seen with a "toad" behind them (smaller, more fuel-efficient towed vehicle to drive when the motorhome is parked at a campground).
I was invited into the Dynamax shown above for a tour. I loved the attractive interior, which "lives" as large as many Class As -- and is more expensive than many of them. I noted, however, that it didn't have as much room as our old 34-foot HitchHiker 5th-wheel with three slides! Our Cameo is two feet longer and has three slides that are bigger than the HitchHiker -- at a much lower cost, even with the cost of a tow vehicle.
Many of these larger RVs have one to five slide-outs to offer additional living space. Materials used to construct them can range from quite basic to very luxurious -- with price tags to match. Some motorhomes end up costing more than sticks-and-bricks houses. In fact, in the most depressed housing markets right now, there are many "real" houses that cost less than most new Class A and C rigs! An average Class A coach can run you over $200,000, a luxury one well over $600,000.
Their "toads" are usually Jeeps so they can drive around the multitude of 4WD roads in the area.
One younger couple we know who still work at least part of the year to earn income to maintain their active lifestyle (ultra and adventure races) have a "toy hauler" in which they live.
We've also heard of some people who've turned the storage space of toy haulers into work space (office, workshop, etc.). More and more people are finding a way to make a living while traveling in their RV.
If you've never had an RV you'll have to start from scratch in your research for a suitable rig. You're miles ahead, so to speak, if you've already had some experience with one or more of the types of campers and have a better idea of their advantages and disadvantages.
So much depends on your budget, your space requirements, and how you want to travel and live in your RV.
If you'll be traveling by yourself, you don't need as much space as a couple with two big dogs, for example. If you want to fit into just about any campsite out there, particularly little ones in public campgrounds or at trailheads, you'll need a smaller rig. If you love to cook and want to prepare meals like you make in your house, you'll need a kitchen with adequate counter/storage space and appliances (refrigerator, range, oven, microwave). If you want the convenience of moving from the passenger seat to the bathroom in transit without getting out of your RV, or you don't want the bother of hooking/unhooking from a tow vehicle, you'll want a motorhome instead of a trailer or 5th-wheel.
Those are just a few examples of some of the decisions that should be made prior to choosing a particular type or model of RV for extended use. I guarantee you the consequences are greater the more time you plan to live in it!
I'm going to open a can of worms here . . .
From what I've read, it appears that full-timers are pretty evenly split between owning motorhomes (especially Class As) and 5th-wheel coaches. Each has advantages and disadvantages. Your task is to figure out which type of RV will suit you the best. Good luck!
Most folks we know who are living in Class A, B, or C motorhomes wouldn't trade them for a 5th-wheel. Most people we know who are full-timing in 5th-wheels wouldn't trade them for a motorhome.
Neither Jim nor I have ever owned a motorhome so we can't speak as knowledgeably as people who have traveled and lived extensively in them. Over the years we have gradually gotten larger and larger towable campers to accommodate our lifestyle. The last three were 5th-wheel coaches of 27 feet, then 34 feet (we thought until a few days before trading it in that it was only 32!), and now 36 feet long.
The advantage of the larger models is more comfort. The disadvantages are more weight to haul, lower fuel mileage, higher costs in general, and fewer options of where to park.
Each time we've knowingly chosen comfort over all that! After all this time, we know ourselves pretty well. We'd be miserable constantly tripping over each other or our dog(s), having inadequate space in the kitchen or bathroom, or being scrunched against the walls in the bedroom.
When we traded our 34-foot NuWa HitchHikerII 5th-wheel a year ago we purchased a new 36-foot Carriage Cameo 5th-wheel coach. (See five-part series starting January 29, 2010.) Even though we aren't technically full-timing yet we worked hard to find a sturdier, better insulated -- and yes, more comfortable -- camper because we want to use it eight to nine months of the year and aspire to be full-timers.
We didn't realize until we were looking for the new rig that only two companies at that time warranted their fivers for full-time use. That came as a surprise to us; we verified that information and focused on products made only by those two companies: Carriage, Inc. and DRV.
of our 5th-wheel, and another 12-foot slide-out on the door side ; that one is deeper (three feet).
The dry weight of the Cameo is about 2,000 pounds heavier than the old HitchHiker but our fuel mileage hasn't significantly deteriorated. One reason is that we started driving slower when we got the Cameo, usually 60 MPH now on freeways instead of 65-70. That makes a big difference. We also try to carry less weight in the camper, particularly less fresh, grey, or black water in our tanks when we're in transit (only enough for the nights we'll be boondocking somewhere like WalMart) and fewer heavy items like canned goods (we wait until we get to our next destination to buy what we need for a few days).
We average 11-12 MPG in mountainous terrain and up to 14-15 MPG on flatter ground -- especially heading back east, which is more downhill and with a prevailing tailwind! That's not too terrible for a camper that weighs 14,000 to 15,000 pounds loaded.
I don't know if Jim and I will ever get a Class A or Class C motorhome (Bs are too small for us). They are considerably more expensive, don't offer any more living area (usually less) than what we have, and require a different "toad" than what we already own. In our opinion, well-built 5th-wheel coaches have the most room and features for the money.
Most satisfied motorhome owners will quibble with that, however. You have to figure out what's best for you.
Do plenty of research if you haven't already purchased an RV to accommodate your intended lifestyle. Check out the series of entries I wrote last January, search the internet for other buying tips, go look at all the different categories of rigs at RV shows and dealerships, learn as much as you can about different features, investigate the companies whose products you prefer, and maybe rent one or more types of campers for short trips to see how they drive and "live."
It can be a long process to find what you want at an affordable price but everything you learn along the way will help you select the right RV for you.
Next topic in this series: endless camping options -- how in the world do we figure out where to stay??


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\section{Introduction}

The number of known magnetic hot stars has steadily increased thanks dedicated campaigns (e.g., MiMeS, \citealt{2016MNRAS.456....2W}; the BOB campaign, \citealt{2015IAUS..307..342M}; and the BRITE spectropolarimetric survey, \citealt{2016arXiv161103285N}) using the latest generation of high-resolution spectropolarimeters.  Magnetic fields are found to occur in about 10\,\% of hot stars, are stable over long time scales, have a simple geometry (often dipolar), and are considered to be of fossil origin \citep[e.g.,][]{2007MsT..........1P, 2015IAUS..305...61N, 2016sf2a.conf..199V, 2017arXiv171202811S}.  Yet, we still do not understand the impact of such large-scale magnetic fields on the deep stellar interior or on stellar evolution.  Theory and numerical simulations indicate that the large-scale magnetic field should enforce a uniform rotation within the radiative envelope of hot stars \citep[e.g.,][]{1937MNRAS..97..458F, 1992MNRAS.257..593M, 1999A+A...349..189S, 2005A+A...440..653M, 2011IAUS..272...14Z}.  This affects the amount of material that is able to overshoot from the convective core to the surrounding radiative layers in these stars \citep[e.g.,][]{1981ApJ...245..286P, 2004ApJ...601..512B}.  However, observational evidence of this effect remains rare.

Asteroseismology, the study of non-radial oscillations in stars, remains the sole method to reliably observe the conditions within stars \citep{2010aste.book.....A}.  Depending on the type of stellar oscillations, classified on the basis of their dominant restoring force of the pulsation modes, the driving mechanism, and the global stellar parameters, these oscillations probe different regions within the stellar interior.  Gravity modes (g modes) probe the deep interior and the near-core region, while pressure modes (p modes) are mostly sensitive to the stellar envelope.  The detection and modelling of oscillation modes has been successfully exploited for only two hot magnetic OB stars, namely V2052\,Oph \citep{2012A+A...537A.148N, 2012MNRAS.424.2380H,   2012MNRAS.427..483B} and $\beta$\,Cep \citep{2000ApJ...531L.143S}, at the level of magneto-asteroseismology.  This is the combination of magnetometry and asteroseismology to study how the large-scale magnetic field of these magnetic hot stars influences their deep interior.  \citet{2012MNRAS.427..483B} determined that the magnetic field of V2052\,Oph was responsible for the low amount of convective-core overshooting required to successfully model the observed $\beta$\,Cep p-mode oscillations when, comparised to a star with similar oscillations but no detected large-scale magnetic field.

Unfortunately, the number of known magnetic pulsating hot stars with a complete characterization of their large-scale magnetic field and sufficient data to perform asteroseismic modelling remains limited.  This is in part due to the brightness limitation for ground-based high-resolution spectropolarimetry ($V = 7 - 10$\,mag is the typical limit for moderately rotating hot stars) and in part because few intrinsically bright hot stars were observed by photometric space missions, such as \textit{Kepler} or CoRoT.  The K2 space mission \citep{2014PASP..126..398H} has partly filled this niche, since its field of view changes on the sky every ${\sim}90$\,days, and monitors stars that are accessible with modern high-resolution spectropolarimetry.  As such, we are able to search for and investigate the periodic variability in photometry caused by oscillations and rotational modulation, while also measuring the strength of the large-scale magnetic field.

For this current study, we selected a sample of candidate magnetic hot stars, based on their peculiar chemical surface composition, to be observed with both K2 and ESPaDOnS, with the aim to find optimal targets for magneto-asteroseismology.

We describe the sample selection in Sect.\,\ref{sec:sample}.  Section\,\ref{sec:data} discusses the observations and their respective data treatments.  The periodic variability in the K2 photometry is investigated in Sect.\,\ref{sec:photometry}, estimates on the stellar parameters are determined in Sect.\,\ref{sec:spectroscopy}, and in Sect.\,\ref{sec:magnetic} we examine the high-resolution spectropolarimetry for the presence of a large-scale magnetic field.  Section\,\ref{sec:discussion} discusses the results, and a summary and conclusions are provided in Sect.\,\ref{sec:conclusions}.

\section{Sample selection}
\label{sec:sample}
For each observing campaign of the K2 space mission, we selected the CP-2 stars(also known as Ap/Bp stars) and the He weak/strong stars from the \citet{2009A+A...498..961R} catalogue, which contains a list of stars known to have peculiar chemical photospheric abundances.  The Ap/Bp stars are typically slow rotators with strong large-scale magnetic fields, which cause stratification in their atmospheres and create long-term chemical spots on the stellar surface \citep[e.g.,][]{1950MNRAS.110..395S, 1970ApJ...160..641M}.  The He strong stars are also assumed to host large-scale magnetic fields (e.g., \citealt{1979ApJ...228..809B}, with $\sigma$\,Ori\,E as the best studied example, \citealt{2015MNRAS.451.2015O}).  The He weak stars (CP-4 stars) are of a different nature and do not form a homogeneous group \citep[which was already noted by e.g.,][]{1964ARA+A...2..297S, 1971ApJS...23..213N, 1974VA.....16..131J}.  Some CP-4 stars exhibit intense Si, or Ti and Sr lines, and are considered a hot extension of the magnetic Ap/Bp stars (examples of magnetic He weak stars are 3\,Sco \citep{1979MNRAS.188..609L}, HD\,176582 \citep{2011AJ....141..169B}, and HR\,2949 \citep{2015MNRAS.449.3945S}).  Others show overabundances of P and Ga, typically noted for HgMn stars (CP-3 stars), and could thus be related to these non-magnetic HgMn stars.

In total, over 60 of these anticipated magnetic stars have been selected and monitored by the K2 space mission, in its campaigns C00 up to C15.  From this sample, we selected 16 of the brightest and/or slowest rotating stars to be observed with high-resolution spectropolarimetry, with the aim to detect and/or confirm the presence of a stable large-scale magnetic field.  The combined analysis of the photometric and spectro-polarimetric data of this sub-sample forms the basis   of the current paper.  The individual stars and their properties are presented in Table\,\ref{tab:sample}.  The photometric variability of the complete sample of 60 stars is analysed and presented in \citet[][submitted]{Bowman2018}.

Two stars of the sample are the primary components of long-period binary systems.  HD\,134759 is part of a hierarchical system, for which the shortest orbital period is 23.42\,yr \citep{1982A+AS...47..569H}.  HD\,158596 has an angular separation of ${\sim}0.3$\,arcsec according to its Hipparcos data \citep{1997ESASP1200.....E}.  One star is part of a short-period binary system, namely HD\,139160.  \citet{1987ApJS...64..487L} indicated an orbital orbit of 5.28\,d and an eccentricity of $0.33 \pm 0.02$.  Yet, substantial scatter remains between their spectroscopic observations and orbital solution.

\begin{table*}
\caption{Ap/Bp stars observed with K2 and ESPaDOnS.  Spectral types are retrieved from \citet{2009A+A...498..961R} and confirmed binary systems in the literature are indicated (see text).  Values for the effective temperature $T_{\mathrm{eff}}$ and surface gravity $\log g$ were determined in this work by fitting synthetic spectra to the H$\beta$ and H$\gamma$ lines.  The values for the projected rotational velocity $v\sin i$ and the non-rotational line broadening $v_{\rm NR}$ were determined from a fit to an unblended metal line.}
\centering
\tabcolsep=6pt
\begin{tabular}{lllrrrr}
\hline
\hline
Star		& V 		& SpT		& $T_{\mathrm{eff}}	$& $\log g	$& $v\sin i$& $v_{\rm NR}$\\
		& [mag]	&			& [K]				& [dex] 		& [km s$\mathrm{^{-1}}$]& [km s$\mathrm{^{-1}}$]\\
\hline
HD97859	&	9.35	&	B9 Si		&$	13750	\pm	300	$&$	3.85	\pm	0.10	$&$	83	\pm	1	$&$	42	\pm	5	$\\
HD107000	&	8.02	&	A2 Sr		&$	7850		\pm	200	$&$	3.20	\pm	0.15	$&$	20	\pm	5	$&$	41	\pm	6	$\\
HD134759	&	4.54	&	Bp Si + ...	&$	11900	\pm	200	$&$	3.80	\pm	0.10	$&$	60	\pm	2	$&$	33	\pm	4	$\\
HD139160	&	6.19	&	B7 He wk.	&$	13200	\pm	400	$&$	4.05	\pm	0.10	$&$	20	\pm	5	$&$	35	\pm	5	$\\
HD152366	&	8.08	&	B8 Si		&$	10250	\pm	450	$&$	3.30	\pm	0.30	$&$	23	\pm	2	$&$	17	\pm	3	$\\
HD152834	&	8.83	&	A0 Si		&$	10100	\pm	500	$&$	3.40	\pm	0.30	$&$	13	\pm	1	$&$	10	\pm	2	$\\
HD155127	&	8.38	&	B9 Eu Cr Sr	&$	8050		\pm	150	$&$	3.45	\pm	0.15	$&$	37	\pm	3	$&$	35	\pm	5	$\\
HD158596	&	8.94	&	B9 Si + ...	&$	11200	\pm	400	$&$	3.90	\pm	0.20	$&$	60	\pm	3	$&$	40	\pm	4	$\\
HD164224	&	8.49	&	B9 Eu Cr		&$	8850		\pm	250	$&$	3.45	\pm	0.10	$&$	22	\pm	4	$&$	40	\pm	7	$\\
HD165972	&	8.96	&	B9 Si		&$	12700	\pm	250	$&$	3.85	\pm	0.10	$&$	29	\pm	4	$&$	50	\pm	5	$\\
HD166804	&	8.88	&	B9 Si		&$	12900	\pm	250	$&$	4.00	\pm	0.10	$&$	45	\pm	3	$&$	29	\pm	4	$\\
HD173406	&	7.43	&	B9 Si		&$	13150	\pm	250	$&$	4.05	\pm	0.10	$&$	38	\pm	2	$&$	33	\pm	5	$\\
HD173657	&	7.41	&	B9 Si Cr		&$	10750	\pm	500	$&$	3.80	\pm	0.20	$&$	91	\pm	5	$&$	47	\pm	15	$\\
HD177013	&	9.04	&	A2 Eu Cr Sr	&$	11700	\pm	400	$&$	4.40	\pm	0.20	$&$	24	\pm	6	$&$	41	\pm	8	$\\
HD177562	&	7.38	&	B8 Si		&$	12200	\pm	300	$&$	3.65	\pm	0.10	$&$	15	\pm	1	$&$	13	\pm	3	$\\
HD177765	&	9.15	&	A5 Eu Cr Sr	&$	8600		\pm	200	$&$	4.50	\pm	0.10	$&$	5	\pm	2	$&$	8	\pm	2	$\\

\hline
\end{tabular}
\label{tab:sample}
\end{table*}

\subsection{Previous inference of large-scale magnetic fields}
For some of the stars in our sample, the presence of a large-scale magnetic field has been investigated from previous observations.  However, in several cases it was not clearly confirmed that the star hosts a large-scale magnetic field.  These observations are either from a photometric estimation of the `surface' magnetic field \citep[e.g.,][]{1980A+AS...41..111C}, medium resolution circular spectropolarimetry of metal or Balmer lines \citep[e.g.,][]{2014AstBu..69..427R}, or from the directly observed Zeeman splitting of absorption lines \citep{1997A+AS..123..353M}.

The photometric $Z$ index based on the Geneva photometric system and calibrated on Kurucz models \citep{1979ApJS...40....1K} can indicate the presence of a (large-scale) magnetic field for hot stars \citep[with a spectral type ranging from B1 to A2;][]{1979A+A....78..305C, 1980A+A....88..135C}.  This method was employed by \citet{1980A+AS...41..111C} to indicate that HD\,134759 and HD\,139160 should host a large-scale magnetic field with a strength of more than 1\,kG.  \citet{1984A+AS...58..387N} continued this analysis and determined a magnetic field strength of 1\,kG, 2.7\,kG, 4.1\,kG, 2.4\,kG, and 1.2\,kG for HD\,134759, HD\,155127, HD\,164224, HD\,165972, and HD\,173406, respectively.

Low to medium resolution circular spectropolarimetry was utilized to detect and measure the strength of the large-scale magnetic fields of three stars in our sample.  \citet{1975ApJ...201..624L} investigated HD\,134759 and obtained a longitudinal magnetic field value of $-600\pm 700$\,G, which the authors did not claim as a definite detection.  HD\,97859 was observed and discussed by \citet{1998CoSka..27..452E}, who obtained a longitudinal magnetic field of $-400$\,G.  No errorbars were provided, but it can be assumed to be of the order of the measured value, as HD\,97859 had the largest $v \sin i$ of all stars in their sample, with typical uncertainties ranging from 100\,G to 500\,G for stars with a $v \sin i < 20$\,km\,s$\mathrm{^{-1}}$.  Lastly, HD\,107000 was monitored by \citet{2008AstBu..63..139R, 2014AstBu..69..427R, 2015AstBu..70..444R}, who measured longitudinal magnetic field values ranging from $-240\pm30$\,G up to $320\pm50$\,G that vary with a period of about 2.4\,d.

\citet{1997A+AS..123..353M} and \citet{2017A+A...601A..14M} noted that HD\,177765 hosts a sufficiently strong large-scale magnetic field causing Zeeman splitting of several absorption lines.  By measuring the strength of the splitting, the authors determined a mean magnetic field modulus of approximately 3.4\,kG, with little variation between the various observations.

Given this overview, we conclude that only HD\,107000 and HD\,177765 have a firmly detected large-scale magnetic field, albeit not with modern high-resolution spectropolarimetry.

\section{Observations}
\label{sec:data}
\subsection{K2 photometry}

To construct the K2 light curves, we retrieved the target pixel files from the Mikulski Archive for Space Telescopes (MAST).  For each (sub)-campaign and each star, we determined custom non-circular apertures from the stacked images.  These were sufficiently large to accommodate the pixel drifts due to the thruster fires \citep{2014PASP..126..398H} and did not change during a given data set.  Next, the mean background per frame was subtracted to create raw background corrected photometry.  This was subsequently passed through the \textsc{k2sc} package \citep{2015MNRAS.447.2880A, 2016MNRAS.459.2408A, 2017MNRAS.471..759A} to correct for the pixel drifts, and their associated instrumental effects, by means of Gaussian processes.  Subsequently, an outlier rejection was applied to the corrected photometry of each (sub)-campaign and another (long-term) instrumental detrending was performed.  During this detrending step, we accounted for the high-amplitude rotational modulation signal (see Sect.\,\ref{sec:photometry_rotation}).  Finally, we combined the different (sub)-campaigns for a given star to one light curve.  Details on the K2 photometry are given in Table\,\ref{tab:photometry}.

Reduced K2 light curves were constructed for 14 stars of the sample, while reductions for HD\,134759 and HD\,139160 were still ongoing at the time of writing.  A significant fraction of the flux of HD\,177562 was lost outside the subraster, causing the light curve to be of poor quality. Therefore, only 13 light curves were used in the remaining of this paper.

\begin{table}
\caption{Logs of the the K2 photometric observations.  We provide the EPIC ID, the K2 campaign number, C, during which observations were taken, the total duration of the observations, and the total number of datapoints in the light curve, N.  $^{a}$ Light curve not yet fully reduced at the time of submission.  $^{b}$ Light curve has a significant time gap in between the two campaigns.  $^{c}$ Light curve of poor quality due to flux loss outside the sub-raster.}
\centering
\tabcolsep=6pt
\resizebox{\columnwidth}{!}{
\begin{tabular}{lllccc}
\hline
\hline
Star		& EPIC ID		& C& Time length	& N & Notes\\
		&&&[d]\\
\hline
HD\,97859	&	201777342	&	01	&	80.07	&	3345	&$		$\\
HD\,107000	&	201667495	&	10	&	47.89	&	1907	&$		$\\
HD\,134759	&	249657024	&	15	&			&		&$	^{a}	$\\
HD\,139160	&	249152551	&	15	&			&		&$	^{a}	$\\
HD\,152366	&	203749199	&	02, 11&	822.59	&	4209	&$	^{b}	$\\
HD\,152834	&	232176043	&	11	&	69.43	&	2925	&$		$\\
HD\,155127	&	232284277	&	11	&	69.45	&	2876	&$		$\\
HD\,158596	&	225990054	&	09, 11&	221.99	&	5831	&$	^{b}	$\\
HD\,164224	&	226241087	&	09	&	68.64	&	2824	&$		$\\
HD\,165972	&	224206658	&	09	&	68.64	&	2822	&$		$\\
HD\,166804	&	227373493	&	09	&	68.64	&	2812	&$		$\\
HD\,173406	&	218676652	&	07	&	65.79	&	2624	&$		$\\
HD\,173657	&	213786701	&	07	&	81.28	&	3361	&$		$\\
HD\,177013	&	219198038	&	07	&	81.24	&	3289	&$		$\\
HD\,177562	&	214133870	&	07	&	81.80	&	3494	&$	^{c}	$\\
HD\,177765	&	214503319	&	07	&	78.78	&	3331	&$		$\\
\hline
\end{tabular}}
\label{tab:photometry}
\end{table}

\subsection{ESPaDOnS spectropolarimetry}

Each star was observed at least once by the Echelle SpectroPolarimetric Device for the Observations of Stars \citep[ESPaDOnS,][]{2006ASPC..358..362D} mounted at the Canada France Hawaii Telescope (CFHT) on Mauna Kea in Hawaii.  Standard settings were used for the spectropolarimeter in circular polarisation mode (Stokes\,V).  The spectropolarimetric sequences consisted of four consecutive sub-exposures, for which the exposure times were tailored to the spectral type, brightness, and anticipated $v\sin i$, to be able to detect a dipolar field of 600\,G or higher.  The observations were reduced with the \textsc{libre-esprit} \citep{1997MNRAS.291..658D} and \textsc{upena} softwares available at CFHT.  The data span from 3\,700\,\AA\ to 10\,500\,\AA\ and have an average resolving power R\,=\,65\,000.  The spectropolarimetric data were normalized to unity per spectral order with the interactive spline fitting tool \textsc{spent} \citep{2018MNRAS.475.1521M}.  Details on the spectropolarimetric observations are given in Table\,\ref{tab:magnetometry}.

\section{Photometric variability}
\label{sec:photometry}

\begin{figure*}
\centering
\includegraphics[width=\textwidth, height = 0.33\textheight]{hd107000}%
\caption{The K2 light curve of HD\,107000 is shown in the \textit{top left} panel and its corresponding Lomb-Scargle periodogram in the \textit{middle left} panel.  \textit{Top right}: K2 photometry (black) phase-folded with the rotation period, as well as a fourth-order sine model (red).  Rotation phases where ESPaDOnS spectropolarimetry were taken are marked by the black dashed lines.  \textit{Bottom left}: Lomb-Scargle periodogram of the residual K2 photometry, after removal of the rotational modulation signal.  Instrumental frequencies related to the thruster firing are indicated by the gray solid lines.  \textit{Bottom right}:  LSD profiles of the ESPaDOnS spectropolarimetry where the Stokes\,V, the diagnostic null, and the Stokes\,I profiles are shown, with an offset for increased visibility.  Integration limits for the determination of the FAP and longitudinal magnetic field are indicated by the dashed vertical lines.}
\label{fig:hd107000}
\end{figure*}

\subsection{Rotational modulation}
\label{sec:photometry_rotation}
We computed a Lomb-Scargle periodogram \citep{1976Ap+SS..39..447L, 1982ApJ...263..835S} for each of the 13 K2 light curves.  The dominant variability for all 13 light curves occurs in the low-frequency regime, which consists of a few significant frequency harmonics.  These periodograms are indicated in the top and middle panels of the left column of Fig.\,\ref{fig:hd107000} (similar figures for the other stars are depicted in Appendix\,\ref{sec:appendix}).  We attribute this variability to rotational modulation, due to surface abundance inhomogeneities.  Instead of iteratively prewhitening this variability, we performed a Least-Squares (LS) fit to the light curve with a fourth-order sine model:
\begin{equation}
M(t) = C + \sum\limits_{n=1}^{4} A_n \cdot \sin \left(2 \pi (n f_{\mathrm{rot}} t + \phi_n)\right) \, \mathrm{,}
\label{eq:rotmodel}
\end{equation}
\noindent where $A_n$ and $\phi_n$ are the amplitude and phase of the $n$th harmonic and $C$ is a constant offset.  This fitting procedure has the advantage that the exact rotation frequency, $f_{\rm rot}$, and its (higher) frequency harmonics are simultaneously enforced.  We truncated the series at the fourth order, because this was the highest frequency harmonic encountered in the periodograms.  The fitting process was a two-step approach.  First, $f_{\mathrm{rot}}$ was kept fixed to the estimated value from a ten times oversampled Lomb-Scargle periodogram to estimate $A_n$, $\phi_n$, and $C$.  In the second step, all parameters, including $f_{\mathrm{rot}}$, were set as free fitting parameters, where $f_{\rm rot}$ was allowed to vary within the Rayleigh resolution limit.  We show the final fit to the K2 light curve in the top right panel of Fig.\,\ref{fig:hd107000} for HD\,107000 and provide all 13 determined rotation periods in Table\,\ref{tab:rotation}.  We propagated the Rayleigh limit as a conservative uncertainty for each $P_{\mathrm{rot}}$.

Several of the stars in our sample have previously been monitored to investigate their periodic variability.  We compared the literature values for the rotation period with the values derived in this work (see Table\,\ref{tab:rotation}). Most agreed well with only two exceptions.  For HD\,107000, we recovered twice the literature value.  This may occur if \citet{2012MNRAS.420..757W} performed a frequency extraction instead of fitting a high-order sine model to the \textsc{stereo} light curve in the time domain.  Our value for the rotation period of HD\,107000 offers a better fit to the K2 light curve.  The other exception is HD\,177765, for which \citet{2017A+A...601A..14M} indicated a rotation period longer than 5\,years due to the lack of variability in the mean magnetic field modulus.  The variability in the K2 light curve has a small amplitude and does not contain two full cycles of the derived rotation period (56\,days). We cannot exclude that this photometric variability has a different (possibly instrumental) origin other than rotation.

\begin{table}
\caption{Rotation periods from photometric modulation.  Values determined in this work were calculated from the K2 photometry. $^{a}$ \citet{2006SASS...25...47W},  $^{b}$ \citet{2012MNRAS.420..757W}, $^{c}$ \citet{2015A+A...581A.138B}, $^{d}$ \citet{2016AJ....152..104H}, $^{e}$ \citet{2017A+A...601A..14M}, $^{*}$ Length of the K2 light curve  is smaller than twice the rotation period.}
\centering
\tabcolsep=6pt
\begin{tabular}{lccl}
\hline
\hline
Star		& $P_{\mathrm{rot}}$ [d] 	&  $P_{\mathrm{rot}}$ [d]  	& Note 		\\
		& This work					&  Literature 				&		 	\\
\hline
HD\,97859	&$	0.792	\pm	0.008	$&$	0.7921	\pm	0.0002	$&$^{	b	}$\\
HD\,107000	&$	5.6	\pm	0.7	$&$	2.8187	\pm	0.0002	$&$^{	b	}		$\\
HD\,134759	&$				$&$	3.099	\pm	0.001	$&$^{	b	}		$\\
HD\,139160	&$				$&$	6.62	\pm	0.02	$&$^{	b	}				$\\
HD\,152366	&$	3.23	\pm	0.01	$&$				$&$^{		}				$\\
HD\,152834	&$	4.4	\pm	0.3	$&$	4.2928	\pm	0.0003	$&$^{	d	}		$\\
HD\,155127	&$	5.5	\pm	0.4	$&$	5.5243	\pm	0.0004	$&$^{	d	}		$\\
HD\,158596	&$	2.02	\pm	0.02	$&$	2.02206	\pm	0.00005	$&$^{	c	}		$\\
HD\,164224	&$	0.73	\pm	0.01	$&$				$&$^{		}				$\\
HD\,165972	&$	2.8	\pm	0.1	$&$	2.7596	\pm	0.0001	$&$^{	d	}		$\\
HD\,166804	&$	3.7	\pm	0.2	$&$	3.7035	\pm	0.0002	$&$^{	d	}		$\\
HD\,173406	&$	4.6	\pm	0.3	$&$	5.095			$&$^{	a	}			$\\
HD\,173657	&$	1.94	\pm	0.05	$&$	1.93789	\pm	0.00005	$&$^{	d	}		$\\
HD\,177013	&$	4.9	\pm	0.3	$&$	4.873			$&$^{	a	}			$\\
HD\,177562	&$				$&$				$&$^{		}				$\\
HD\,177765	&$	56	\pm	40	$&$	\gg 5$\,years&$^{	e, *	}				$\\
\hline
\end{tabular}
\label{tab:rotation}
\end{table}

\subsection{Remaining periodic variability}

By removing the rotation signal from the K2 photometry, we drastically reduced the power in the Lomb-Scargle periodograms (e.g., the bottom left panel of Fig.\,\ref{fig:hd97859}).  The strongest remaining signal within the periodogram of the residuals falls within one of the following categories:

\begin{itemize}
\item Low-frequency power excess related to imperfectly reduced and corrected K2 photometry.  This might have been caused by stitching different K2 (sub)-campaigns together into one light curve or because of an incomplete removal of long-term instrumental variability. HD\,152834 and HD\,165792 show examples of this power excess in the periodogram of the residuals.

\item Remaining aliasing structure around the ${\sim}$6\,h K2 thruster fire frequency (or its harmonics) or at the harmonics of the ${\sim}$6\,h thruster fire frequency itself.  A clear example of the former was observed for HD\,173657.

\item Remaining structure around the rotation frequency or its frequency harmonics.  This is observed, for example, for HD\,155127, HD\,158596, or HD\,166804.  The surface abundance inhomogeneities are anticipated to be stable over the time scale of the light curves, as they are linked to the stable large-scale magnetic fields.  However, spot migration could have occurred, but is considered to be unlikely.
\end{itemize}

Three stars are exceptions to these results with significant power in their residual periodograms.  Both HD\,158596 and HD\,177765 show a clear, isolated frequency peak at $17.001 \pm 0.005$\,d$^{-1}$ and $11.76 \pm 0.01$\,d$^{-1}$, respectively.  These could be Nyquist aliases of unresolved, high-frequency pulsation modes in the rare subgroup of roAp stars \citep{1982MNRAS.200..807K}.  \citet{2012MNRAS.421L..82A} discussed the detection of a 61.01\,d$^{-1}$ roAp pulsation in the spectroscopy of HD\,177765, supporting the hypothesis that we may indeed be dealing with an alias in the photometry.  We cannot exclude that the frequency peak for HD\,158596 originates in the fainter secondary component.  Finally, we note that HD\,164224 reveals a low-frequency power excess, which could be due to unresolved g-mode pulsation frequencies or internal gravity waves, which are predicted in stars with convective cores \citep[e.g.,][]{2015ApJ...806L..33A}.

We did not find evidence of frequency peaks related to stellar oscillations driven by the $\kappa$-mechanism for any of the 13 targets.

\section{Estimation of stellar parameters}
\label{sec:spectroscopy}

To perform the magnetometric analysis, we required estimates for the effective
temperature, $T_{\mathrm{eff}}$, and the surface gravity, $\log g$, to construct
average spectra with the Least-Squares Deconvolution (LSD) technique
\citep{1997MNRAS.291..658D}.  This method drastically increased the S/N of a
possible Zeeman signature in the (LSD) Stokes\,V profile.

As a first step, we deduced the projected rotational velocity $v\sin i$ and the radial velocity for each star by fitting a rotation profile \citep[see e.g.,][]{2005oasp.book.....G} convolved with a Gaussian profile to an unblended \textsc{Fe} or \textsc{Si} line.  The Gaussian profile captures the non-rotational broadening $v_{\rm NR}$ acting upon the absorption line, due to macro-turbulence, micro-turbulence, waves, etc.  We followed the goodness-of-fit approach by \citet{2014A+A...562A.135S} to derive the values and confidence intervals for $v\sin i$ and $v_{\rm NR}$ and report the results in Table\,\ref{tab:sample}, keeping in mind that these two parameters are correlated.

Next, we determined $T_{\mathrm{eff}}$ and $\log g$ for each star by fitting pre-computed \textsc{syntv} local thermodynamical equilibrium synthetic spectra \citep{1996ASPC..108..198T} for \textsc{llmodels} atmosphere models \citep{2004A+A...428..993S} using the Grid Search in Stellar Parameters \citep[\textsc{gssp},][]{2015A+A...581A.129T} software to the observations.  Because of the significant chemical peculiarities for these stars, we performed the fitting simultaneously to the H$\beta$ and H$\gamma$ lines, while keeping the overall metallicity fixed at [M/H]\,=\,0.0 and the micro-turbulent velocity at $v_{\rm micro} = 2.0$\,km\,s$^{-1}$.   Moreover, both the line broadening and the radial velocity were fixed at the values in Table\,\ref{tab:sample}.  The grid of stellar parameters for \textsc{gssp} spanned from $T_{\mathrm{eff}}$ = 6000\,K up to 15000\,K, with steps of 500\,K, and $\log g$ from 3.0\,dex up to 4.5\,dex, with a step of 0.1\,dex.  The determined values for $T_{\mathrm{eff}}$ and $\log g$, as well as their statistical uncertainties, are also listed in Table\,\ref{tab:sample}.  These errors on $T_{\mathrm{eff}}$ and $\log g$ should be considered as a lower limit of the confidence intervals, because Ap stars are known to have a core-wing anomaly for their hydrogen lines \citep[see e.g.,][]{2001A+A...367..939C, 2002ApJ...578L..75K}.  For the stars with unresolved binary components, the values given may have contributions from both stars.  However, the difference in $T_{\mathrm{eff}}$ as a result of this would not significantly affect our conclusions.

Although the secondary components of HD\,134759, HD\,139160, and HD\,158596 should be well within the fiber area of ESPaDOnS, we did not find a clear indication of the presence of the secondary in the spectra. Therefore, we also fitted their respective observations with a single-star synthetic spectrum to estimate the stellar parameters.

\section{Magnetometry}
\label{sec:magnetic}

\begin{table*}
\caption{Magnetometric properties of the sample.  We provide the HJD at the middle of the spectropolarimetric sequence, as well as the total exposure time.  Furthermore, we indicate the $T_{\mathrm{eff}}$ and $\log g$ of the \textsc{vald3} line mask, the S/N in the LSD Stokes\,I profile, the Land\'{e} factor $g$, the mean wavelength $\lambda$, the integration range around the line centroid used for the longitudinal field calculation and FAP analysis, the detection status of a Zeeman signature (DD for definite detection, ND for non-detection and MD for marginal detection), and the measured longitudinal magnetic field.}
\centering
\tabcolsep=6pt
\begin{tabular}{lllrrrrrrcr}
\hline
\hline
Star		& HJD		& $t_{\mathrm{exp}}$ & $T_{\mathrm{eff}}$& $\log g$ 	& S/N	&$g$	&$\lambda$ &  int. range& Det.	& $B_l$\\
		& -2450000&& \multicolumn{2}{c}{line mask}\\
		& [d]				& [s]	& [K]		& [dex]				&		& &	[nm]&	[km s$\mathrm{^{-1}}$]	&	& [G]\\
\hline
HD97859		&	2457881.78364	&$4 \times 	1272	$&	14000	&	4.0	&	4829	&	1.192	&	519.13	&$\pm	150	$&	DD	&$	570	\pm	122	$\\
HD107000		&	2457475.92214	&$4 \times 	338	$&	7750	&	3.5		&	2836	&	1.210	&	519.94	&$\pm	50	$&	DD	&$	250	\pm	10	$\\
			&	2457497.87935	&$4 \times 	338	$&		&			&	3047	&	1.210	&	518.95	&$			$&	DD	&$	162	\pm	12	$\\
HD134759		&	2457799.17433	&$4 \times 	37	$&	12000	&	4.0	&	4941	&	1.183	&	520.89	&$\pm	70	$&	DD	&$	305	\pm	30	$\\
			&	2457801.17550	&$4 \times 	37	$&		&			&	5056	&	1.183	&	521.12	&$			$&	DD	&$	364	\pm	31	$\\
HD139160		&	2457820.00404	&$8 \times 	22	$&	13000	&	4.0	&	3133	&	1.177	&	520.43	&$\pm	45	$&	ND	&$	42	\pm	50	$\\
primary		&				&		&		&		&		&		&&$\pm	25	$&	ND	&$	-2	\pm	30	$\\
secondary	&				&		&		&		&		&		&&$\pm	35	$&	ND	&$	49	\pm	116	$\\
HD152366		&	2457818.06147	&$4 \times 	599	$&	10000	&	3.5	&	2843	&	1.196	&	518.52	&$\pm	40	$&	DD	&$	-82	\pm	14	$\\
HD152834		&	2457818.08468	&$4 \times 	267	$&	10000	&	3.5	&	1769	&	1.188	&	511.72	&$\pm	25	$&	DD	&$	228	\pm	20	$\\
HD155127		&	2457818.10943	&$4 \times 	676	$&	8000		&	3.5	&	1812	&	1.201	&	511.06	&$\pm	40	$&	DD	&$	-435	\pm	7	$\\
HD158596		&	2457818.15110	&$4 \times 	1060	$&	11000	&	4.0	&	2744	&	1.182	&	525.24	&$\pm	110	$&	DD	&$	610	\pm	46	$\\
HD164224		&	2457817.15008	&$4 \times 	1089	$&	8750		&	3.5	&	1373	&	1.197	&	515.58	&$\pm	50	$&	DD	&$	580	\pm	27	$\\
HD165972		&	2457905.94729	&$4 \times 	517	$&	13000	&	4.0	&	3144	&	1.185	&	518.54	&$\pm	60	$&	DD	&$	-326	\pm	50	$\\
HD166804		&	2457883.11294	&$4 \times 	443	$&	13000	&	4.0	&	3095	&	1.180	&	517.88	&$\pm	55	$&	DD	&$	-476	\pm	50	$\\
			&	2457886.92179	&$4 \times 	443	$&			&		&	3066	&	1.180	&	518.47	&$			$&	DD	&$	-520	\pm	50	$\\
			&	2457890.13132	&$4 \times 	443	$&			&		&	2468	&	1.180	&	519.00	&$			$&	DD	&$	-429	\pm	67	$\\
HD173406		&	2457500.13798	&$4 \times 	214	$&	13000	&	4.0	&	1882	&	1.174	&	519.73	&$\pm	70	$&	ND	&$	-44	\pm	45	$\\
HD173657		&	2457554.98727	&$4 \times 	226	$&	11000	&	4.0	&	3631	&	1.164	&	508.96	&$\pm	120	$&	ND	&$	-79	\pm	84	$\\
HD177013		&	2457905.96915	&$4 \times 	310	$&	12000	&	4.5	&	963	&	1.163	&	511.23	&$\pm	45	$&	MD	&$	217	\pm	59	$\\
HD177562		&	2457553.02367	&$4 \times 	262	$&	13000	&	3.5	&	4572	&	1.176	&	524.93	&$\pm	30	$&	ND	&$	16	\pm	18	$\\
HD177765		&	2457554.99870	&$4 \times 	120	$&	8500		&	4.5	&	1001	&	1.204	&	513.89	&$\pm	25	$&	DD	&$	1067	\pm	21	$\\
\hline
\end{tabular}
\label{tab:magnetometry}
\end{table*}

To boost the signal-to-noise ratio (S/N) of the possible Zeeman signatures in the Stokes\,V spectrum, we constructed an average line profile using the LSD technique.  A precomputed \textsc{vald3} line mask \citep{2015PhyS...90e4005R} with parameters close to the estimated stellar parameters was used for each star, and is listed in Table\,\ref{tab:magnetometry}.  All hydrogen lines and all spectral lines blended with hydrogen lines, telluric features, and known diffuse interstellar bands were removed from the line masks.  Furthermore, the depths of the lines in the masks were adjusted to match the observations \citep[a process so-called ``tweaking'', see e.g.,][]{2017MNRAS.465.2432G}.  The resulting LSD profiles are shown in the bottom right panel of Fig.\,\ref{fig:hd107000} for HD\,107000 and in Appendix\,\ref{sec:appendix} for the other stars.

Most of the LSD Stokes\,I profiles show some sort of distortion.  We attributed this profile variability to the surface abundance inhomogeneities, because the corresponding K2 photometry displays rotational modulation.

\subsection{Zeeman signature}
The False Alarm probability \citep[FAP;][]{1992A+A...265..669D,   1997MNRAS.291..658D} was utilized to determine the presence of a Zeeman signature in the LSD Stokes\,V profile.  Non-detections (NDs) have been assigned for a FAP\,$ > 10^{-1}\,\%$, definite detections (DDs) for FAP\,$ < 10^{-3}\,\%$, and marginal detections correspond to $10^{-3}\,\% <$\,FAP\,$ < 10^{-1}\,\%$.  Using these criteria, eleven stars have a DD, while four have a ND and one a MD.  We mark the detection status in Table\,\ref{tab:magnetometry}.

For each spectropolarimetric observation, we also determined the longitudinal magnetic field \citep{1979A+A....74....1R} as:
\begin{equation}
B_l = -2.14 \cdot 10^{11} \frac{\int v V(v) \mathrm{d}v}{\lambda g c \int[1-I(v)] \mathrm{d}v} \, \mathrm{,}
\label{eq:longfield}
\end{equation}
\noindent where $V(v)$ and $I(v)$ are the LSD Stokes\,V and I profiles, respectively, for a given velocity $v$ in km s$\mathrm{^{-1}}$. The mean Land\'{e} factor, $g$, and the mean wavelength (in nm), $\lambda$, result from the LSD technique.  The speed of light, $c$, is given in km s$\mathrm{^{-1}}$ and the longitudinal magnetic field, $B_l$, in Gauss.  The integration range spans the full width of the Zeeman signature and the mean absorption line profile.  We report the values for $\lambda$, $g$, the integration range, and the calculated longitudinal magnetic field in Table\,\ref{tab:magnetometry}.

The determined $B_l$ values are well in line with the expectations for magnetic hot stars with a polar strength of at least several 100\,G \citep[where the polar strength is at least 3.5 times the measured longitudinal magnetic field;][]{1967ApJ...150..547P}.  Stars for which we obtained a ND also have a measured $B_l$ compatible with zero within the 2$\sigma$ confidence interval. In addition, Zeeman splitting is observed in individual lines (Stokes\,I) of HD\,177765 \citep[as already clearly indicated in Figure\,4 of][]{1997A+AS..123..353M}, confirming that the star hosts a strong field of several kG.  This strong magnetic field agrees with the long rotation period for the star (out of the studied sample) when considering magnetic braking.

Nearly all of the detected Zeeman profiles have a typical appearance for large-scale magnetic fields with a simple geometry (dominantly dipolar), where the exact shape depends on the rotation phase and on the unknown inclination and obliquity angles.  Distortions of the Zeeman signature due to the distorted LSD Stokes\,I profile did occur for several stars, such as HD\,166804.  However, the signature was sufficiently clear that these distortions did not cause any issues with the detection.  Moreover, the rotation periods are sufficiently long compared to the total exposure time of the spectropolarimetric sequence, so that the measured $B_l$ values were not affected by these distortions.

\subsection{Binary systems}
\label{sec:magnetic_binaries}
As mentioned earlier, three stars of our sample are part of binary systems.  A component of two of these (i.e., HD\,134759 and HD\,158596) clearly host a large-scale magnetic field. The spectropolarimetric sequence of HD\,139160, however, led to a ND.  Here, we consider several explanations.

\begin{itemize}
\item  The ND could be caused by the binary nature of HD\,139160.  The distortions in the LSD Stokes\,I profile could be due to the presence of the nearby companion, classifying HD\,139160 as SB2 system, instead of the previously claimed surface abundance inhomogeneities.  By means of LS fitting, we described the LSD Stokes\,I profile with two Gaussian functions to represent the individual components (see Fig.\,\ref{fig:hd139160}).  After subtracting either one of the Gaussian profiles, we isolated the individual components in the Stokes\,I profile.  We then used these two profiles to redetermine the FAP for a Zeeman signature (in the LSD Stokes\,V) and recomputed the longitudinal magnetic field (see Table\,\ref{tab:magnetometry}).  Again, we did not detect a signature of a large-scale magnetic field for the individual components.  Hence, the binary nature is probably not the cause of the ND.

\item HD\,139160 has a rather short orbital period of 5.28\,d, according to the modelling efforts of \citet{1987ApJS...64..487L}  to the measured radial velocities.  As magnetic hot stars seem to be less common in binary systems with short orbital periods \citep[as inferred from the BinaMIcS results,][]{2015IAUS..307..330A}, this could explain the ND.  Yet, spectropolarimetric data with a much higher S/N are needed to exclude the possibility of a weak magnetic field.

\item As indicated earlier, two sub-groups of He-weak stars exist.  The He-weak stars related to the HgMn stars do not host a large-scale magnetic field.  We compared the Stokes\,I spectrum with the synthetic \textsc{syntv} + \textsc{llmodels} (with solar abundances) spectrum, but did not find clear evidence of strong P or Ga absorption lines, which would associate HD\,139160 to this non-magnetic sub-group of He-weak stars.  We did, however, note the substantially weaker He\,\textsc{I} lines.  Thus, HD\,139160 may host a large-scale magnetic field, but that is weaker than our detection threshold.

\end{itemize}

\section{Discussion}
\label{sec:discussion}
\subsection{Rotation period}
\begin{figure}
\centering
\includegraphics[width=0.45\textwidth, height = 0.33\textheight]{Prot_vsiniv3}%
\caption{Rotation frequency $f_{\mathrm{rot}}$ versus $v\sin i$ (dots).  The colour of the symbols indicates the magnetic detection (black for a DD, blue for a MD, red for a ND).  The symbol relates to the measured $T_{\mathrm{eff}}$, with squares for A-type stars and dots for B-type stars. Solid lines represent the anticipated rotation frequency for the labelled stellar radius, inclination angle, and measured $v\sin i$.  Solid lines are for $i=90\,^{\circ}$ and dashed lines for $i=20\,^{\circ}$.  Anticipated rotation frequencies at a given $v\sin i$ decrease for increasing model radii ($2R_{\odot}$, $3R_{\odot}$, $4R_{\odot}$, and $5R_{\odot}$, respectively). We indicate the confidence intervals for both $f_{\mathrm{rot}}$ and $v\sin i$, where we added the errors of $v\sin i$ and of $v_{\rm NR}$ in quadrature given the correlated nature of these two parameters.}
  \label{fig:prot_vsini}
\end{figure}

The determined rotation periods indicate that all stars are slow to moderate rotators.  This result was expected because of a known bias introduced in the sample star selection since we required to obtain high S/N, high-resolution spectropolarimetry with reasonable exposure times. Nevertheless, rotation periods of a few days are typical of Ap/Bp stars.  We compare the determined rotation frequencies with the derived values for $v\sin i$ in Fig.\,\ref{fig:prot_vsini}.  No strict relation is present, as expected due to differences in stellar radii and the anticipated random distribution of inclination angles.  HD\,97859 and HD\,164224 seem closer to (rotation) pole-on than the others, as they are situated in the upper part of the diagram.  The two probable roAp stars do not reside in a particular region of Fig.\,\ref{fig:prot_vsini}.  The variety in the inclination angle $i$, and the obliquity angle $\beta$, is further supported by the different shapes of the rotational modulation in the K2photometry.

\subsection{Magnetic detections and non-detections}

Out of the 16 expected magnetic stars in our sample, we directly detected the presence of a strong, large-scale magnetic field for 11 stars.  This is the first firm detection for 9 of these stars and the first for all 11 stars employing high-resolution spectropolarimetry.  We have a 69\,\% detection rate in our sample, with no obvious correlation with the stellar properties for the detection status.  The spectropolarimetric measurements for the four stars with a ND and the one MD are of similar quality as the other 11 stars with detected magnetic fields.  Moreover, it seems unlikely that the NDs/MDs were due to particularly unfavourable rotation phases where the field is seen in a cross-over configuration (see top right panels of Figures in Appendix\,\ref{sec:appendix}).

Two of the stars with a ND, namely HD\,173406 and HD\,173657, show stable rotational modulation over the duration of their K2 light curves.  Because of the poor quality light curve of HD\,177562, we could not confirm the presence of rotational modulation for this star with a ND.  Yet, the comparison of the ESPaDOnS spectra with their respective synthetic spectra suggests chemical peculiarities, as claimed by the \citet{2009A+A...498..961R} catalogue.  Therefore, it is likely that these three stars are indeed Ap/Bp stars with expected, stable surface abundance inhomogeneities, and thus host a large-scale magnetic field.  It may be that these stars host a weaker large-scale magnetic field than what is typically anticipated for Ap/Bp stars, which is in agreement with the increased number of detections of such weak large-scale magnetic fields \citep[e.g., HD\,5550;][]{2016A+A...589A..47A}.  These weaker magnetic fields could be an evolutionary consequence if the stars have burned a considerable amount of their hydrogen, while still undergoing hydrogen core burning, leading to an increased stellar radius and assuming magnetic flux conservation \citep[e.g.,][]{2008A+A...481..465L}.  This scenario could be further enhanced if magnetic field decay has occurred \citep[as determined by][for the most massive magnetic stars]{2016A+A...592A..84F}.

The distortions of the LSD Stokes\,I profile of HD\,173657 (see bottom right panel of Fig.\,\ref{fig:hd173657}) could be due to a resolved SB2 system, instead of surface abundance inhomogeneities.  However, this star is not known to be a binary system and we only obtained one observation.  More spectroscopic observations are needed to corroborate this hypothesis.

We also did not detect the presence of a large-scale magnetic field for the He-weak star HD\,139160.  We explored the possibility of a large-scale magnetic field in the individual components of the binary system, but again obtained a ND for both components.  Since we did not note any strong P or Ga lines in the spectroscopic observations, HD\,139160 is inferred to be unrelated to be related to the non-magnetic HgMn stars.  Thus, the presence of a large-scale magnetic field is anticipated, that is likely weaker than what was expected when computing the exposure time for the spectropolarimetric sequences.

\subsection{Lack of heat-driven stellar oscillations}

We found no evidence for the presence of stellar oscillations produced by the $\kappa$ mechanism in any of the Ap/Bp stars studied in this work. Some of our target stars do reside in the theoretical $\kappa$-driven instability regions. Although only a small fraction of the stars in these regions are known to have observable oscillations at current detection thresholds, the fact that none of our targets show such pulsations is significant.  These results provide support for the theoretical predictions that strong large-scale magnetic fields change the nature of waves and may even completely suppress them \citep{2017MNRAS.466.2181L}.

Two stars in our sample (HD\,158596 and HD\,177765) show statistically-significant peaks in their periodograms with strong evidence that there are Nyquist aliases of high-frequency roAp pulsations.  Furthermore, HD\,164224 shows a significant low-frequency power excess that is unlikely to be explained by instrumental effects and could be caused by unresolved g-mode pulsation modes or internal gravity waves.  Extended observations of all these candidate pulsators will be extremely useful in characterising the exact nature of their observed variability in the K2 photometry.

Several pulsating magnetic hot stars are known, such as $\beta$\,Cep \citep{2000ApJ...531L.143S, 2013A+A...555A..46H}, V2052\,Oph \citep{2012A+A...537A.148N, 2012MNRAS.424.2380H, 2012MNRAS.427..483B}, $\xi^1$\,CMa \citep{2017MNRAS.471.2286S}, HD\,43317 \citep{2012A+A...542A..55P, 2013A+A...557L..16B, 2017A+A...605A.104B}, HD\,188774 \citep{2015MNRAS.454L..86N}, $\beta$\,Cen\,Ab \citep{2011A+A...536L...6A, 2016A+A...588A..55P}, and $\rho$\,Pup \citep{2017MNRAS.468L..46N}. However, all these stars host a rather weak magnetic field. The only strongly magnetic star exhibiting variations interpreted as $\kappa$-driven pulsations known at present is the He-strong star HD\,96446, with a dipolar field strength of about 5\,kG \citep{2012A+A...546A..44N, 2017MNRAS.464L..85J}.

\section{Summary and conclusions}
\label{sec:conclusions}

We observed 16 chemically peculiar hot stars with space-based high-precision photometry to study their periodic variability, and with modern high-resolution optical spectropolarimetry to detect the signatures of a large-scale magnetic field.  The investigated stars are all slow to moderate rotators, with large-scale magnetic fields being easier to detect from spectropolarimetry in slowly-rotating stars compared to fast rotators. Although our sample of stars was biased towards slow rotators, the observed rotation periods are typical of Ap/Bp stars.  It is known that gravity-mode oscillations are easier to detect in slowly-rotating OB-type stars \citep{2003SSRv..105..453A, 2017ApJ...847L...7A}. Therefore, our sample bias should favour the detection of such oscillations.

In our sample, 13 stars have a high-quality K2 light curve and all of them show evidence of rotational modulation.  We detected a large-scale magnetic field for 69\% of our sample stars and found no obvious correlation between this detection and the stellar parameters, such as binarity, rotation rate, or occurrence of possible stellar pulsations.  All four non-magnetic stars, HD\,139160, HD\,173406, HD\,173657, and HD\,177562 show either rotational modulation, peculiar chemical surface abundances, or both, and therefore likely host an undetected weak large-scale magnetic field.

No $\kappa$-driven oscillations were detected in any of the targets in oursample. Two stars, namely HD\,158596 and HD\,177765, show an isolated high-frequency peak in their periodogram, which we interpret as the Nyquist alias of high-frequency roAp pulsations.  One star, HD\,164224, shows a significant low-frequency power excess in its periodogram which could be evidence of convectively-driven internal gravity waves.  Further observations and analyses of these candidate pulsators are needed to fully test these hypotheses, since we are too limited by the length and cadence of the K2 space photometry.

We conclude that, after major efforts with the K2 mission and modern spectropolarimetry, the best stars to try and perform in-depth magneto-asteroseismic modelling are those with a moderate magnetic field which does not suppress $\kappa$-driven modes. The best target for this is and remains the CoRoT target HD\,43317, for which a series of gravity modes with consecutive radial order has been found in the CoRoT photometry \citep{2012A+A...542A..55P, 2013A+A...557L..16B} and whose magnetic field detection and modelling led to fully consistent results between the seismically and magnetically derived rotation frequency of the star \citep{2017A+A...605A.104B}.

\section*{Acknowledgements}
B.B. would like to thank Dr. Andrew Tkachenko for the useful discussions on GSSP.

This work has made use of the VALD database, operated at Uppsala University, the Institute of Astronomy RAS in Moscow, and the University of Vienna. This research has made use of the SIMBAD database operated at CDS, Strasbourg (France), and of NASA's Astrophysics Data System (ADS). Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Part of the research leading to these results has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement N$^\circ$670519: MAMSIE) and from the Research Foundation Flanders (FWO, grant agreement G.0B69.13).

\bibliographystyle{mnras}

redpajama_set_name: RedPajamaArXiv


text:
The Bigs
Lee las noticias de Al Bat en tu idioma aquí
Jose Bautista to the Houston Astros?
No one expected this!
By Gabriel Delgado March 23 2018 - 10:56 HS
José Bautista | AP
The Jose Bautista saga has yet another episode and now, rumor has it that an unexpected team is now after the sign of Jose Bautista. And this could be a huge signing if the rumors are true.
According to a Mexican reporter, the World Series Champions, the Houston Astros, were in pursuit for Jose Bautista and were close to signing a deal. But the rumor quickly began to spread on the U.S.
The Astros are not signing Jose Bautista.
— Brian McTaggart (@brianmctaggart) 23 de marzo de 2018
This Friday MLB.com's reporter, Brian McTaggart, rejected these rumors as he explained that there was no such deal, but he didn't offer some further information, or whether negotiations were taking place or at least if there was an interest from the Astros.
Even though, the idea of the Champions acquiring Bautista is kind of strange, as the Astros don't have the necessity of bringing a player like him, having plenty of options on the outfield and for the designated hitter spot like Evan Gattis.
In previous weeks, it was reported that Bautista was considering retirement due to the lack of good offers for him, but his agent came and said that these rumors were not true at all.
Continue reading (*)
Rays and Cardinals with BIG TRADE involving Jose Martinez and TOP pitching prospect
Dallas Keuchel and White Sox finalize $55 million dollar deal
Yankees lose another player, Edwin Encarnación signs with White Sox
Dellin Betances stays in New York, but not with Yankees
Anthony Rendón and Angels finalize $245 million dollar deal
Stephen Strasburg signs RECORD deal at Winter Meetings


text:
ARCHITECT Magazine
Restoring the Phoenix Naval Stores in Turkey Creek
When commercial development threatened the historic Gulf Coast community, activist and educator Derrick Evans and unabridged Architecture transformed a condemned structure into a space to remember.
By MADELEINE D'ANGELO Posted on: February 28, 2022
In 2001, Derrick Evans, a successful Boston-based historian and educator, returned to his native Turkey Creek in Gulfport, Miss., to spend the winter holidays with family. While he was home, Evans couldn't stop thinking about pervasive coastal sprawl. He'd spent years watching new runways constructed at the Gulfport-Biloxi International Airport just south of Turkey Creek, the widening of the state's busiest highway to the west, and the creeping casino- and tourism-driven coastal development leeching from central Gulfport to the south. "I mean, hideous coastal sprawl," Evans recalls.
Meanwhile, stalwart examples of coastal architecture, some featuring Mediterranean and Arabic influences, had been boarded up and forgotten as the city focused economic resources on "whatever development could be plunked into the wetlands adjacent to the interstate exits," Evans says. "My whole world was being redeveloped grotesquely."
Twenty years on, Evans has helped secure parts of Turkey Creek against this sprawl through preservation projects including the newly opened Phoenix Naval Stores. The museum lies on northern edge of the Turkey Creek community in Gulfport, Miss., welcoming residents and visitors into the historic area, founded by formerly enslaved people in 1866. The project is the result of a determined restoration collaboration between the Evans and the Bay St. Louis firm Unabridged Architecture to transform the building, a former paymaster's office, which had been abandoned for decades and on the brink of demolition, into a site of community gathering and remembrance, marking a new chapter in the building's century-long life.
The process began in the early aughts when Evans, fearing that the redevelopment could wind its way through Turkey Creek as the area underwent a comprehensive 25 year planning process, took action, writing a brief paper on the community's historical significance and rich identity as a historically Black community. His work succeeded: Turkey Creek is now on the National Register of Historic Places. "Turkey Creek Community Historic District … represents a surviving example of a local community established by newly emancipated African Americans during the Reconstruction Era," states the registration. "Unlike many other such communities, the Turkey Creek Community largely retains its historic geographic boundaries, residential nature, architectural heritage, and sense of community."
But Evans wanted to do more. He began arranging to leave behind his rich life as an professor and landlord in Boston and reinvesting his savings back into Turkey Creek, buying up strategic parcels of marshlands that would buffer the community from "some developer who's gonna come in and haul in a bunch of impervious red clay from north Mississippi, fill in a swamp, and put up a hotel," Evans says.
One of those parcels included a termite-ridden structure overgrown with vines and surrounded by pine trees. The building, was so decrepit that its foundation had cracked, slowly sinking the structure into the marshy ground. Evans forgot about the building, which, along with most of Turkey Creek, flooded during Hurricane Katrina. Then in 2015, Evans was faced with a choice to tear the building down or take action, so he began researching the property's history and original design with historian Jeff Rosenberg and Unabridged Architecture, aiming to restore the structure with funding from a National Parks Service 2018 Civil Rights Grant.
Originally constructed circa 1920, the building housed the paymaster's office for the Yaryan Naval Stores Co., a manufacturing plant where workers boiled pine tree stumps in gasoline to extract creosote and turpentine, materials often used to waterproof naval ships of the era.
It was dangerous work and, in 1943, an explosion rocked the plant, killing 11 men, including nine Black Turkey Creek residents, bringing tragedy to the community. Miraculously, the paymaster's office survived the explosion due to "its unique fireproof construction" of "3/4-inch-thick concrete plaster wrapped its sturdy, pine-framed walls, soffit, and roof, which was topped with metal for water resistance," says unabridged principal Allison Anderson. "We had never encountered this method of construction before, and had to learn more about the original materials, such as Hy-Rib Metal Lath," Anderson says.
After the explosion, the paymaster's office was moved to a different location in Turkey Creek, about 1,000 feet from its original site, and transformed into a residential structure by local carpenter Thomas Benton Evans, Sr. The building served that purpose until the late 1990s, falling into disuse until Evans purchased the structure in 2003 and officially began the restoration in 2018.
There was little existing information about the building's design so the restoration team, which included the local contractor Rip Daniels, learned by investigating structure itself. "There were no original windows remaining," Anderson says. "We had to make educated guesses about the porch and the windows based on building conventions from the period of the structure and the remaining evidence embedded in the structure."
Their attention also offered insight into the mastery and the craftsmanship behind the original building. "This building wasn't built from a blueprint," Evans explains. "Whatever went into this thing, the first time it was built was like someone's mom's best gumbo in that there's no written recipe."
In order to save the building's foundation, the restorers lifted the building from the mud and guessed "at the original floor elevation of the structure," Anderson says. "The building had to be shored up and raised incrementally, one-quarter inch at a time, at all four corners."
Although the structure's interior had been lost to time, the team uncovered more details embedded in the framing, including indications of an original wraparound porch. Some of the details, such as two original entry door frames—markers of segregated entrances for Black and white workers—were more sobering. The restorers worked painstakingly to restore the interior following 1920s conventions, celebrating when they found a trove of original beaded board in a shed tucked into the rear of the property. "It was like finding a treasure," Anderson says.
In spite of the building's mysteries, the team was intentional with the scope of their restoration work. "We reused almost every scrap of the remaining building materials, and retained many of the building's imperfections and scars as part of the narrative," Anderson says. "As a result, the building does not appear 'new' but as a part of the community fabric."
After three years of work, the completed Phoenix Naval Stores building opened its doors in December to community members and visitors alike. In addition to serving as a l gathering place for many community elders, the humble structure creates a visual link between Turkey Creek and some of its surrounding industrial landscape. "It brings coherence to the community and its environments, which includes this toxic, contaminated industrial wasteland that some of which is currently inactive," Evans says.
The Phoenix Naval Stores is also a community anchor where individuals can, quite literally, reflect on Turkey Creek as they watch the community from chairs on the porch, Evans notes. "I would hope that architects would value those kinds of things—anchoring a community, giving a community and a space, a reflection back on itself—as opposed to the new thing that I just plunk down here because we could do it."
2022 AIA Architecture Award
Marine Education Center at the University of Southern Mississippi Architect: Lake|Flato...
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text:
2021 Mr. and Ms. Wrestler of the Year – TOP 7
Fareway Stores, Inc. and Body Armor present the Dan Gable Mr. and Ms. Wrestler of the Year Awards in coordination with IAwrestle and IWCOA.
The IWCOA accepted nominations from high school coaches for student athletes in each of the three state wrestling classes for the men and combined all classes for the women's award, regardless of their year in school and weight class. A committee selected by the IWCOA recently provided IAwrestle with a list of 7 semi-finalist candidates for public input.
Fans have the ability to vote once per day for their top wrestler in each category until February 8th, where it will be narrowed down to the top 3. (Top voted wrestler receives a nomination)
Another round of voting will take place to determine the three finalists by February 8th. The fan votes will count as ONE vote towards the IWCOA's committee votes in EACH round. (For example: Wrestler A received enough fan votes to place second in the poll but that does not guarantee them to move on to the next round. IWCOA has selected 12 coaches and officials for this committee. The fan vote, this poll, is the 13th vote to break up any ties.)
The two runner-up student athletes in each class will each receive finalist award plaques. A duplicate Wrestler of the Year trophy and duplicate Wrestler of the Year runner-up plaques will be provided to each high school where finalists attend, for permanent placement in the high school trophy case.
VOTE ONCE EVERY 24 HOURS. WAIT A FULL 24 HOURS. (FOR EXAMPLE: YOU CAN'T VOTE MONDAY AT 8PM AND THEN TUESDAY AT 8AM BECAUSE IT IS A NEW DAY. 24 HOURS MEANS 24 HOURS)
MS. WRESTLER OF THE YEAR
MR. WRESTLER OF YEAR
IWCOA Girls State Wrestling Seeds vs Rankings
Kirk Hageman Memorial Wrestling Scholarship
2 thoughts on "2021 Mr. and Ms. Wrestler of the Year – TOP 7"
Vote For MARIAH WEBBSTER From Colfax-MINGO!!!!!!!!!!!!!!!!!!!!!!!!!!!! SKOWHAT
VOTE MARIAH FROM COLFAX!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!1


text:
Volume 24, No. 2 Buffalo County Historical Society March-April, 2001
A vignette is a short scene or incident. Historical vignettes are like short poems or story fragments that may seem incomplete but suggest an internal story or a micro-history that can be appreciated for their own value to inform or amuse while they may also inspire consideration and reflection of larger themes and events. Historical Vignette: The Tea Pot Told to Leroy A. Walker by John Nutter in the 1920's
This story has to do with the Nutter family of Gibbon and it happened before the Colony arrived - in fact, before the railroad was built in 1866.
The Nutter family lived in a log house, just north of where the eight-sided Nutter house now stands. The Nutters came from England and like all good Englishmen, liked their tea. In fact, they had two tea pots - identical tea pots, sitting on the shelf. But through habit and convenience, only one of the tea pots was used daily. The other one just sat there waiting its turn.
Came the day when the supply of tea ran out. There was no store to buy more closer than Grand island - a day's journey away by ox team. These two-day shopping trips were not taken without real necessity. Day after day without tea soon became the real necessity. So, Mr. Nutter left for Grand Island. On the afternoon of the second day, one of the children was sent to the top of the log house so he could more easily spot the returning father - with the tea. As soon as he was sighted as a speck on the horizon a child was sent to get the tea and hurry back with it. A child could run faster than an ox team could plod, and the tea could be made and ready for drinking the very minute Mr. Nutter came to the cabin. This was done. Never had tea tasted better. So refreshing. It was only when the tea pot was being washed that it was discovered that in the haste to make the tea, that the second tea pot had been used - the tea pot in which the rattle snake rattles had been stored.
[Special thanks to Leroy Walker for this Historical Vignette. If you would like to contact Leroy his address is P.O. Box 116, Gibbon, NE 68840.]
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Edited 3/14/2003


text:
Brendan Philip Reidy (born 13 September 1968 in Wellington) is a New Zealand-born Samoan rugby union player. He plays as a prop.

Career
He spent his club career first with the Saracens between 1997 and 1999, then with Rugby Rovigo for two years, and later, with AS Montferrand from 2000 to 2002, when he retired from the playing career. He was part of the 1995 and 1999 Rugby World Cup rosters, where he played for Samoa. He also played the National Provincial Championship in New Zealand for Wellington.

References

External links

Brendan P. Reidy international statistics

1968 births
Living people
Samoan rugby union coaches
Samoan rugby union players
Rugby union players from Wellington City
Samoa international rugby union players
ASM Clermont Auvergne players
Rugby union props
Samoan people of New Zealand descent
New Zealand sportspeople of Samoan descent

redpajama_set_name: RedPajamaWikipedia


On 11 December 2018, East Lothian Council approved the proposal to close Prestonpans Infant School and Prestonpans Primary School and to establish a new school in the town. As stated within the Council's proposal the decision to close both schools and establish a new school required to be ratified by Scottish Ministers. I can now confirm that Scottish Ministers have determined that they will not be calling in this proposal and that the Education Service can proceed with closing both schools and establishing a new school. The education service will work closely with both Head Teachers and the Chairs of both Parent Councils to recruit a Head Teacher for the newly established school. Education Officers will also work closely with staff, parents and pupils in both schools to progress the establishment of a new primary school and will also work closely with the community given the differing views expressed during the consultation process.
Click on the link below for more information from East Lothian First Response Service.
P1A had a lovely time at our Christmas Party. We danced, played games and had a visit from Santa . It was great fun.
We had a wonderful time at our Christmas Lunch on Monday. The food was yummy!
We have been learning about Christianity. We had some lovely visitors from Prestongrange Church who told us about Christian beliefs and we acted out the story of Christmas. We had good fun.


The Finnish term "sauna" indicates a room that is heated to a high temperature in which people sweat. The stone steam bath, the forerunner of today's sauna, is a very old cultural artefact of humanity and goes back to the Stone Age. Taking a sauna builds up the body, purifies it and increases the sense of wellbeing. Taking a sauna is also a social event that enables people to spend quality time together. In terms of separation of the sexes and clothing, there are considerable national differences.
In German-speaking countries and Scandinavia people go naked into the sauna whereas in other countries, above all in Latin countries, taking saunas naked is unusual or even forbidden.
The operating principle of a sauna is simple: raising the body temperature to up to 39 °C (artificial fever point) causes germs within the body to be destroyed. The subsequent cold bath relaxes the muscles and lowers blood pressure, stimulates the circulation, immune system and breathing.
Through thorough but gentle cleansing of the body the sauna also slows aging of the skin. Modern saunas come in a wide variety of different versions that basically differ from one another through the temperature and air humidity.
You will find herbal saunas, Finnish saunas and others at us at Leitlhof - Dolomiten. Please ask us for details without any obligation.