18-40 cm (7″-15.5″); Bushy, Black often with White Tip or Fringe.
Black with 2 broad White Stripes on back meeting in cap on head and shoulders; thin White Facial Stripe.
Five in front (3-4.5 cm long); five in back (5-9 cm long).
Variable shape, dark, cylindrical, sometimes segmented.
Many residents of Toronto and the Greater Toronto Area (GTA) do not realize that in addition to spraying smelly skunk odour, skunks carry many diseases which can be transferred to cats and dogs, as well as humans. Skunks are family oriented animals and usually live with other skunks and babies. Skunks will bite if approached and threatened. Therefore you have to be very careful when removing skunks from your property.
Pestend Pest Control Toronto specializes in skunk removal services. We will take care of the dirty work and remove any skunks that are on your property or near by. We have the tools and experience to humanely remove the skunks without harming them. This gives them a chance to start a new life with their families far away from your home or business.
Skunks are a well known group of fur bearers belonging to the weasel family (Mustelidae). Since they are not particularly disturbed by human presence and activities, they will frequently move in from their native habitat and take up residency beneath buildings. The striped skunk is about the size of an adult house cat. Skunks are often found in wooded areas, close to stream banks and irrigation levees. Litters of 4 to 7 young are born late spring or early summer. Some females may produce a second litter the same year.
Skunks are most commonly known for their scent glands, which can spray a powerful liquid for 2-3.5 meters. The skunk is capable of spraying 5-6 times in a row and even when held aloft by its tail. Skunks are also omnivorous. Their diet includes grubs and various species of mature insects, small rodents, snakes, frogs, bird eggs, nestlings, decaying flesh, as well as fruit, berries, mushrooms and garbage, when convenient.
Although they occasionally dig dens in a fresh-cut bank, skunk dens are usually enlarged vacant burrows dug by other animals. Rock, wood and brush piles or out-cropping are also used in some areas, as are hollow logs. When no natural shelter is available, skunks may create their dens underneath a house or other structure if they can enter by way of porches, steps and crawl spaces that open to the outside. Although uncommon, more than one family of skunks may occupy the same den.
The skunk's odour may be strong or only faintly evident at inhabited dens. Occupied dens will often show signs of fresh digging, at least in spring. Wondering if Toronto raccoon removal is needed, droppings will be evident and usually contain numerous insect fragments. Hair and rub marks can also be found. Skunks are nocturnal. Their occasional presence may go unnoticed around buildings temporarily, until they take up occupancy beneath a building or have a confrontation with some other animal, leaving the telltale reminder of their presence.
Skunks are primary carriers of rabies. We need to cautious around any skunk you see during daylight hours. Skunks are also carriers of ticks, mites and fleas. Skunks have also been known to carry Leptospirosis and distemper, a disease which can be fatal to dogs. Call Pestend Pest Control Toronto to immediately remove all skunks from your property.
Rabies is a viral infection that is usually always fatal. It is transmitted through a bite by an animal infected with the disease. Rabies can spread when the saliva of an infected animal enters an open wound although this is a rare occurrence. Receiving a rabies vaccine promptly after exposure to the virus is the best way to prevent the disease in humans. This is why raccoon removal in Toronto is important.
The presence of skunk odour on anything touched by the fluid is hard to remove and can linger for days. Carbolic soap is useful for cleaning skin and ammonia or tomato juice is helpful for clothing. Commercial products to offset skunk odour on dogs are available from Vet and Pet Supply stores. A popular home remedy that combines one quart of 3 percent hydrogen peroxide, 1/4 cup baking soda and one tsp. liquid laundry or dishwashing soap can help to neutralize the smell of skunk spray on a dog's skin (be careful to avoid contact with eyes). Apply mixture on the dog outdoors wearing rubber gloves and rinse with water after 10 minutes. Repeat procedure if necessary.
Use mixture immediately after combining ingredients and do no store in a closed container. The oxygen gas contained in the mixture could release and burst through the container. Note the strength of this mixture can also bleach fur and hair colour. If eyes come in contact with the mixture, flush with cold water to temporarily relieve discomfort and consult with your doctor about proper treatment.
Keep garbage cans inside garage or shed until pick-up day or use locking or secured lids outside.
Keep shed and garage door close all the time.
Remove wood and rock piles around property.
Secure elevated sheds, openings under concrete slabs and porches, and access to crawl spaces under houses.
Block pet doors or any other passageway to prevent skunks entering your home.
Safely clean the areas on your property where these animals urinate and defecate, also known as skunk latrines, being careful not to touch skunk droppings.
Skunk urine can contaminate water, soil and surrounding vegetation so direct contact should be avoided.
You should always contact a company experienced in wildlife control services when you need help removing skunks from your property.
Lawns, especially newer ones are usually heavily watered and worms and grubs that live just underneath the sod attract skunks. Skunks normally dig 1-3-inch deep holes only where a grub is located. Using pesticides to kill lawn grubs and worms is not recommended because of their toxic effect on the environment.
If you don't know what type of wild animal is nesting inside a structure, the concerned person should be present when the technician arrives to share his or her concerns. A technician may require complete interior and exterior access of the property to indentify your wildlife problem.
Every wildlife job is unique and getting rid of skunks requires special skills, knowledge, tools, materials and methods. Pestend skunk removal technicians specialize in removal of wild animals from attics, chimneys, walls, crawl spaces beneath buildings, sheds, and other hard to reach locations. We provide customized skunk removal solutions in Toronto, North York, Oakville, Brampton, Mississauga, Markham, Scarborough, Thornhill, Richmond Hill, and Vaughan.
Call us for Toronto skunk removal services!


Are you interested in ways to improve your health and enhance your fitness routine? There are many ways to improve your performance, but one tried and true method seems to be protein powder; vegan protein powder, to be exact. Vegan protein powder is designed to help you recover more quickly after workouts, as well as improve your body and your health. It allows you to push yourself further in your fitness routine by keeping your body fueled with an extra supply of protein. You can also use vegan protein powder to manage your weight.
Vegan protein powder comes in many forms, flavors and brands. So how can you be sure to choose the best vegan protein powder that is right for your body, as well as the best tasting vegan protein powder? In this article, you'll be able to learn about a few different brands and types of vegan protein powder currently on the market. You'll discover what makes each one stand out. In addition, we will share ways you can incorporate vegan protein powder into your diet. By the time you finish reading this article, you'll be able to make a well-informed decision about which vegan protein powder to try.
Why Purchase Vegan Protein Powder?
Why is everyone suddenly interested in vegan protein powder? What's the difference between regular old protein powder and vegan protein powder? Does it really make any difference which kind of protein powder you use?
Vegan protein powder uses no animal products whatsoever. It is entirely plant based and uses many types of plants to provide the complete amount of protein that your body needs. Due to the large amount of plants that are included in vegan protein powder, there are a lot more vitamins and nutrients in it, as compared to regular whey protein.
Vegan protein powder is also more easily digestible, since it is entirely plant based. It contains fiber and digestive enzymes that are gentler on your stomach. Other kinds of protein powders contain lactose, which is a harder ingredient to digest for many people.
Now that you understand the difference between vegan protein powder and other kinds of protein powder, which kind of vegan protein powder should you choose? There are many different varieties and brands of vegan protein powder on the market, making it difficult to narrow down which one is best.
There are traditional powders, spirulina powders, raw powders and organic powders. Below is a list of some of the most popular types and brands of vegan protein powder, and our recommendations for the best of each kind.
There are so many options for Vegan Protein Powder, including organic protein powder and raw vegan protein powder. They range in price and amount of protein per serving size. Many are offered in different flavors, such as vanilla, chocolate or coffee flavored. Here are a few of the most popular vegan protein powders.
Coming from Hawaii, this vegan protein powder offers high levels of protein per serving and is the only spirulina based protein powder to be produced in a bio-secure zone, making it the purest and healthiest form of spirulina based protein on the market.
Nutrex Hawaii, a Hawaiian healthy supplement company. You can buy directly through the company's website, as well as nutritional shops such as The Vitamin Shoppe. You can also purchase it through Amazon.
This protein powder has excellent reviews online. It is one of the most popular traditional vegan protein powders and is currently ranked as #2. It contains 55 to 70 percent digestible protein per serving, making it easier on the stomach. It is also the only spirulina to be produced in a bio secure zone, making it completely free of herbicides, pesticides and industrial pollutants. It is reasonably priced and is free of pesticides.
This vegan protein powder offers one of the largest flavor varieties and can also be purchased in on-the-go packs. It's formulated with athletes in mind and is Informed Choice certified for sports.
Vega, a nutrition company that produces a wide variety of health supplements and shakes. This product can be found through big box stores such as Wal-Mart and Target.
This protein powder has fantastic reviews. It is one of the more cheaply priced protein powders, and boasts great flavor choices. It is available in 4 flavors: mocha, berry, chocolate and vanilla.
This protein powder goes a step further, offering an organic, plant based choice in a wide variety of flavors. As one of the top ranked choices, it's a great choice for those who prefer organic protein powder.
Orgain makes this organic vegan protein powder. It can be purchased online through many sites, including Amazon. It can also be purchased in stores such as Market Street.
This is one of the more reasonably priced organic vegan protein powders. From the reviews, it appears to be one of the best tasting vegan protein powders. It also blends well in shakes and is free of any harmful chemicals or additives, due to it being organic. This protein boasts 21 grams of organic protein and 5 grams of organic fiber per serving.
To be called a 'raw' protein, a protein powder cannot be exposed to heat above 42C / 107F at any time during processing. This manufacturing process seals in all the vital nutrients and enzymes that allow us to efficiently digest the protein – meaning that your product gets to work exactly where it is needed.
This is why many people are interested in raw vegan protein powders. Here are a couple of the top raw protein powders.
This raw vegan protein powder is made of 44 superfoods that provide a high level of organic plant based protein per serving, and it also contains probiotics for improved digestive health.
Garden of Life, a company that focuses on organic healthy supplements, makes this raw vegan protein powder. It can be purchased online, as well as other online stores. It can also be purchased in brick and mortar grocery stores, such as Market Street.
If it is important to you to purchase a protein powder that is not only vegan and organic, but is also considered to be raw, then this product is a great choice. However, according to the reviews, many people aren't fond of the flavor and the distinct powdery texture. Yet many continue to use it and praise it as having helped them in obtaining weight loss goals and feeling more energized.
Made with a special 5-protein blend and available in two basic flavors, this raw organic vegan protein powder is manufactured using a more environmentally friendly process.
KOS is the company responsible for this product. This raw vegan protein powder can be purchased online. It can also be found online through the company's website.
This raw vegan protein powder is another great option. It has great reviews and boasts a good flavor, especially the vanilla flavor. In fact, it appears that the absolute best thing about this protein powder is the taste, which everyone seems to rave about in the reviews. Several reviews share that this protein powder is also gentle on the stomach.
As you can see, there are many options when it comes to vegan protein powders. You can find it in several flavors, from chocolate, to mocha, to vanilla to spirulina. So now that you are aware of the huge variety of vegan protein powders you can find, including traditional, to spirulina, to raw, to organic protein powders, how do you use vegan protein powder?
You will want to read the directions carefully on any protein powder you choose, because each one has different amounts of protein per serving. Follow the nutritional guidelines and do not take more vegan protein powder than the container recommends in a day. Be sure to properly measure the amount of protein you mix into your drink or shake, according to the directions on the packaging. Do not let the mixed protein powder sit out in the open for too long. You want to drink it fairly quickly after you have mixed the powder into your drink. Be sure to also properly store your dry protein powder, according to the package directions. Most say to keep in a dry and cool location.
Health Supplement: Protein powder is an easy and helpful way to boost your body's health by adding a properly measured amount to your water or smoothie. Have some for an energy boost midday, or as an afternoon snack.
Post-Workout:After a grueling workout, it is great to have a protein shake to help keep your muscles healthy. After you have finished your exercise routine, have a protein drink within the hour for optimal results. Protein powder can aid in muscle building as well.
Meal-Replacement: Many vegan protein powders can be used as meal replacements for losing weight. Be sure to carefully follow the meal replacement instructions found on the packaging.
Weight Gain: For those with high metabolism, or who find it difficult to gain weight, the addition of a protein shake can be helpful. Mix your vegan powder into some water or a smoothie and drink it as an additional meal during the day.
There are many ways you can incorporate your vegan protein powder into different drinks, smoothies and shakes. Here is a delicious smoothie recipe. Try this refreshing, satisfying and protein packed smoothie, that has a tangy twist to it, after a long workout.
There are many different types and brands of protein powders to choose from, and they all offer different benefits. Each type of vegan protein powder is made up of its own special blend of nutrients and proteins. They each have different textures, flavors and unique positive features.
For some people, being completely free of harmful pesticides, additives, artificial preservatives and flavors is very important. Many believe that makes a protein powder much healthier. In addition, being Non-GMO, gluten free and soy free is often a big plus. If these benefits are important to you, then you will want to choose an organic vegan protein powder.
Taking it one step further, those in support of raw vegan protein powder, or raw organic vegan protein powder, believe that the temperature of the protein powder is also important, and that the manufacturing process is also a critical factor in regards to which protein they ingest. If this feature is important to you, then a raw organic vegan protein powder may be the best choice.
Many people have to deal with digestive issues on a regular basis, and a protein powder with probiotics could help you have a healthier gut. Digestive issues or lactose intolerance is another reason vegan protein powder can be a better choice.
If flavor matters to you, there are several to choose from, and it all depends on what you prefer. Texture plays a big role too, as far as how well a protein powder can mix into your water, or smoothies. Often, it takes trying out a few different types of vegan protein powders to figure out which one you prefer, taste-wise.
Aside from personal preference and your health, price may play a big role in your decision-making process. Although most vegan protein powders fall around the same price ranges, there is still a difference. So, make sure to stay within your budget. There is no need to pay more money. More expensive does not always mean it's the best. All of the above protein powders appear to be excellent choices.
Lastly, when it comes to finally making a decision, all of the protein powders we've discussed today have great reviews. They boast good flavors, great textures, healthy benefits and energy enhancing nutrients. Pick the one that stands out to you, and then see if you feel great after using it. Again, it is good to try a few different kinds out, until you determine which one you like the best, based on your increased energy level, and how you feel overall. Once you find the one that is absolutely best for you, stick with it.
Do you have a vegan protein powder you absolutely love and recommend? Or perhaps you have made a homemade protein powder yourself? Tell us about your favorite protein powder and why you like it in the comments below.
Vegan protein powder no doubt uses no animal products, making it entirely plant-based. It uses many types of plants to provide the complete amount of protein that our body needs and that is why I always tell people to pick it over the regular one. Though I've only tested a few of the products here, u still believe that they are all great products and works well.
Do these vegan protein powders also come with side effects? Most plant foods contain purines which break down into uric acid and can badly affect gout, kidney stones and various digestive disorders which can lead to problems. Vegan protein powder is also known to be high in sodium which can be problematic for people who suffer from heart related issues such as high blood pressure.


Banasiewicz, H. (1973) Impulse response computer. Doctoral thesis, University of Surrey (United Kingdom)..
The Thesis describes the design of a small, portable computer for on-line system identification. The machine generates its own test sequence, monitors, averages and data logs a system's response. On a further command it computes the Cross-correlation Function and displays it on a CRT. Under favourable conditions a valid identification may be obtained in approximately 3 sequence periods. Typical results are given for ideal and real systems.
Thesis (M.Phil.)--University of Surrey (United Kingdom), 1973.


Shawn Flower is the Principal Researcher and sole proprietor at Choice Research Associates. Her primary mission is to conduct criminal justice research with a focus on program evaluation and female offenders including recidivism research, needs assessment, and re-entry into the community. She has been using Remark Office OMR since the Fall of 2002 when she began working as a graduate student at the University of Maryland, College Park. After she completed her education, she purchased a copy of Remark for use with her clients in her consulting company.
She uses Remark Office OMR for pen and pencil self-report surveys and to create forms to monitor day to day program activities (e.g., intake forms, adherence to curriculum, client progress reports). One of her most interesting and largest surveys was a 16 page survey for 200 men detained in jail. The men completed a survey that contained 182 questions on broad areas including criminal history, employment, education, relationships, leisure time, neighborhood safety, life skills, health including substance use history and interest in treatment. Shawn also used Remark Office OMR for a series of inter-related forms for an evaluation of Community Mediation Maryland (CMM) Re-Entry Program. CMM is a state-wide program that offers mediation services to those imprisoned in 10 correctional facilities around the state of Maryland. It is a rare opportunity for those returning to the community to have important and necessary conversations with those they care about and to plan for their return. When all information from all of the forms from different stages of the program is combined, the merged data captures both the administrative process and information required for an assessment of the program's effectiveness. One of the challenges of evaluating this program is that CMM's Executive Director assists independent local mediation centers in providing these services – but in the past, each center used their own forms and processes. Working collaboratively with CMM, Shawn was able to unify the process for this program by using the forms with Remark. This ensures the integrity of data captured both between the centers and from year to year, when staff turnover occurs given the program utilizes one-year contracted volunteers in this work.
When asked about her favorite features of Remark Office OMR, Shawn says, "the flexibility of the software – it is incredibly powerful." As a researcher with such critical projects, she also appreciates the ability to translate the data directly into SPSS for analysis. Retaining the value and variable labels eliminates a lot of coding of syntax and/or getting the data ready for the analysis work. As Shawn says, "just set it up when you do the form – and presto! There you are – ready to crunch numbers." She says it "sounds geeky" but for us, it's music to our ears. We thank Shawn for her continued support of the Remark software through her samples and suggestions.


This course is designed for those individuals who have been charged with the responsibility of writing an application to the annual Assistance to Firefighters Grant Program offered by FEMA. It does not matter if you have never written a grant in your life or if you have won 3-4 AFG's already; this course is taught in plain, easy-to-comprehend language that you will understand. The corse will give you the knowledge and skill sets needed to develop, write and submit an application to the Assistance to Firefighter's Grant Program.
Know what steps are needed to properly prepare for this grant application in advance of the application period.
Know how to describe the problem your department is trying to resolve and how to properly explain your proposed solution to that problem.
Understand the rules and regulations about the program and submitting your request.


text:
Home » Niacin Plus Statins For Low HDL
Niacin Plus Statins For Low HDL
Statins Plus Niacin: Safe?
Statin plus niacin or ezetimibe?
Combination of Simvastatin Plus Vitamin D Offers New Hope for Migraine Prevention
Spinal Manipulative Therapy for Acute Low Back Pain
Medication for Acute Low Back — A Randomized Clinical Trial
Abstract & Commentary
Synopsis: The addition of niacin to patients with known CAD on statins raised HDL cholesterol and reduced atherosclerosis progression.
Source: Taylor AJ, et al. Circulation. 2004;110: 3512-3517.
Although good at lowering LDL cholesterol, statins do not raise HDL enough in many patients. Niacin is the most effective therapy for low HDL, but little information exists about combination niacin and statin therapy on cardiovascular outcomes. Thus, the Arterial Biology for the Investigation of the Treatment Effects of Reducing Cholesterol (ARBITER 2) study was conducted at Walter Reed Army Medical Center to evaluate the effect of adding niacin to statins on carotid intima-media thickness (CMT) in patients with known coronary artery disease (CAD). This was a double-blind, randomized, placebo-controlled study in 167 patients with CAD documented by myocardial infarction or coronary revascularization. Patients on statins with LDL < 130 and HDL < 45, and no known contraindication to niacin, were randomized to placebo or extended-release niacin starting at 500 mg for 30 days, then 1000 mg for 11 months. Only 4 patients had their statin dose changed during the study. The primary end point of CMT change at 1 year was increased in the placebo group by 0.044 mm (P <.001 and was unchanged in the niacin group>P = 0.23. LDL was 89 at baseline and was unchanged by niacin therapy. HDL averaged 39 in the niacin group at baseline and increased to 47 (P < .001); there were no changes in the placebo group. Triglycerides also decreased in the niacin group (164 to 134; P < .01), but fasting glucose increased (107 to 123; P = 0.017). CRP measures were unchanged by niacin. Patients without insulin resistance (diabetes or metabolic syndrome) on niacin had the lowest progression rate of CMT. Cardiovascular events occurred in 3 niacin patients and in 7 placebo patients (P = NS). Study drug adherence was > 90%, and not different between placebo and niacin. No patient had liver tests > 3 times the upper normal limit, and none had myositis. The majority of patients on niacin noted skin flushing. Taylor et al concluded that the addition of niacin to patients with known CAD on statins raised HDL cholesterol and reduced atherosclerosis progression.
Comment by Michael H. Crawford, MD
Although it is well-known that niacin raises HDL levels, the value of this effect, in addition to statins and its tolerability, has been poorly defined. The coronary drug project evaluated niacin monotherapy and showed a reduction in nonfatal myocardial infarction and 15-year mortality, but other studies employing niacin included it with other agents, making it difficult to tease out the effects of niacin alone. This is the first study of moderate-dose niacin added to statins in a systematic, controlled fashion. The study was not powered for clinical outcomes, but rather used CMT as a surrogate. Despite an average duration of statin therapy of about 5 years and average LDL levels of 85 to 90, the placebo group showed progression in CMT. There are several explanations for this: The low HDLs, high triglycerides (average > 150), or failure to drive the LDL below 80 in all the statin patients. Niacin addressed the first 2 issues and showed a lack of progression, thus, indirectly supporting the value of raising HDL and lowering triglycerides. These results are also concordant with the results of a small study of the effect on vessel walls of infusing man-made HDL.
Niacin seemed to be well-tolerated at this dose. Although most patients had skin flushing, few discontinued therapy. Also, liver tests were not alarmingly elevated (> 3 times the upper limit), but the report did not give the actual liver function test data. So elevations < 3 times the upper limit probably were observed. No muscle problems were reported.
Thus, this long-acting niacin preparation given at bedtime in moderate doses seems like a reasonable approach to those with low HDL on adequate statin therapy.
Since most of the subjects were on simvastatin, we do not know if more potent statins with greater LDL-lowering would have worked just as well. Also, the role of fibrates, which also increase HDL and reduce triglycerides, either alone or in combination with statins, is unclear. However, the fibrate statin combination probably has more potential for adverse effects. Finally, the suggestion that patients with diabetes or the metabolic syndrome do not do as well on the statin and niacin combination requires more study.
Dr. Crawford, Professor of Medicine, Chief of Clinical Cardiology University of California San Francisco, is Editor of Clinical Cardiology Alert.
Clinical Cardiology Alert
Clinical Cardiology Alert 2005-02-01
Statins, Rhabdomyolysis, and the FDA
Left Ventricular Remodeling With Chronic Right Ventricular Apical Pacing
A New Novel Anti-Arrhythmic Agent
Clinical Briefs in Primary Care Supplement
Pharmacology Watch: Statins and the Incidence of Rhabdomyolysis

redpajama_set_name: RedPajamaCommonCrawl


text:
Q: How can I make mockito change the content of a method argument? Consider the following Java classes
public class SomeClass {

 public void validateSomething(List<String> exceptions) {
  //Nothing here
 }
}

public class AnotherClass {

 public SomeClass someClass;

 public void validate() {
 List<String> exceptions = new List<>();
 someClass.validateSomething(exceptions);

 if(exceptions.length > 0)
  //do something
 }
}

How can I use mockito to mock SomeClass and make it add an item to the exceptions list so the code path where exceptions.length > 0 will execute for AnotherClass?

A: The Answer interface allows your mock to perform any action you desire when a method is called.  In your case, simply take the argument and do with it as you wish.

redpajama_set_name: RedPajamaStackExchange


text:
Q: Most Efficient Sorting Algorithm for Generated Data I have the following formula: A=(x+x0)^.5 * (y+y0) * (z+z0)^.5
x0, y0, and z0 are constant for a given run, but may change between runs of the program.  x, y, and z are randomly generated for an item and are uniform integers in [0, 15].  This means there are 16^3=4096 possible combinations.
I am trying to find the most efficient way to get the percentile of a given A value (x0, y0, and z0 will be given as well).  I have two questions:

*

*Is there a way to create an analytic formula that will solve for percentile directly, without generating all possible As and sorting them?

*If not, what is the most efficient way to sort this data, given that I have some information about how it will be structured?

I kind of assumed the answer to #1 is "no" but will be pleasantly surprised if someone can come up with an analytic solution.  Proceeding with #2, here is my current progress:
Data will be generated via 3 nested loops:
For x = 0 to 15
   For y = 0 to 15
       For z = 0 to 15
          array(n) = A(x,y,z)
          n=n+1
       Next z
   Next y
Next x

We know (at least) 3 things about this data:

*

*array(0) < array(1) < array(2)...

*array(0) < array(16) < array(32) ...

*array(0) < array(256) < array(512)...

So far my best working algorithm is a mergesort that starts with list size 16.  However this ignored 2) and 3) above.
Note: My question is about efficiency.  I have a solution, that is slow, but works, so what I'm looking for is the most efficient way to do this.
EDIT: Here is a solution I started to come up with, which feels like it would be the most efficient, but it doesn't work.  I'm not sure if it can be salvaged.
Put your values in a 3-dimensional array (x, y, z).  Start with (0,0,0) which must be the minimum.  The next value must be (1,0,0), (0,1,0), or (0,0,1).  Test and add.  Let's say it was (1,0,0).  Then the next value must be (2,0,0), (0,1,0), or (0,0,1).  Continue until you've added all the values in O(n) time.
FLAW: The number of possibilities isn't always constrained to 3.  I can't figure out a way to tell the computer which cells are possibilities without killing the efficiency gain.  There may be a way, but I just haven't thought of it.
Edit 2: I am still interested in the most efficient sorting algorithm for values generated from a monotonic function, since it is theoretically an interesting question.  However, since I asked first if there was a shortcut to getting percentile, I have select the strikingly simple "count the number less than A" as the answer.

A: If all you need to know is the position of A in the sorted list of possibilities, there is actually no need to sort the possibilities (O(n log n)). It's sufficient to count the number of possibilities less than or equal to A (O(n)).
In this case, where the function is monotonic, you can reduce the work even further: given some definite values x' and z', you can solve for y' in A = f(x', y', z'). Then you know that there are max(0, min(16, floor(y') + 1)) triples <x', y, z'> whose value is less than or equal to A.
That solution is quite simple. Given
A=(y' + y0) * ((x'+x0) * (z'+z0))^.5

we have
y' = A / ((x'+x0) * (z'+z0))^.5 - y0

Python (which could be considered pseudocode):
def gmean(x, y):
    return (x * y) ** 0.5

def count_le(A, x0, y0, z0):
    count = 0
    for x in range(16):
        for z in range(16):
            gm = gmean(x + x0, z + z0)
            if gm == 0:
                count += 16
            else:
                y = A / gm - y0
                if y >= 0:
                    count += min(16, 1 + int(y))
    return count

To turn the result of count_le into a percentile, you'd have to multiply it by 100/4096.

A: Interesting problem!
Here's one idea, which may or may not be the most efficient.
Initialize a min-heap with A(0, 0, 0)
numItems = 0
While True:
    A(x, y, z) = pop minimum from heap
    numItems = numItems + 1
    If A(x, y, z) matches given A value:
        break
    else:
        Add to heap A(x + 1, y, z)
        Add to heap A(x, y + 1, z)
        Add to heap A(x, y, z + 1)

Note that you need to maintain a set of flags to ensure that no duplicates are added to the heap. This can be done in O(1) time e.g. Flags[x][y][z] = True when A(x,y,z) is added to the heap. Also another minor note to perform some boundary checks when adding to the heap.
Pop minimum takes O(logn) time. Adding to the heap takes O(logn) time. Thus the worst case time complexity is still O(nlogn).
The advantages are:

*

*You can stop as soon as the given A value is found. i.e. you don't need to calculate all possible A values, and you certainly don't need to sort them all.

*If the given A value is large, you can work with a max-heap.


It's time for a talk.
I appreciate the concern shown here and through social media. The comic has been absent for almost a month and I owe all of you an explanation. Both Elisa and I have fallen on some hardships that have monopolized all our time and caused us to break contract with you, the reader.
Yes, I'll be discontinuing Carbon Dating updates.
The hardcover collection is an achievement that I am very proud of, and one that I couldn't have made without your support through Patreon and Kickstarter. However, comics demand a lot of uncompensated hours that we just couldn't keep up with anymore – even if these characters meant a lot to me.
I plan on finishing personalized comics for supporters who have been waiting way too long to see them. After that, we'll be wrapping things up and replacing the old black and white archive with the colored versions that appeared in the book.
Sometimes writing comics can feel like shouting into the void of the internet, but I've gotten to know many of you over the years through comments and interactions at conventions – and I hope that we can stay in touch. I do have some science communication projects on the horizon that I'm looking forward to sharing with you.


text:
One Song A Day Keeps The Evil Away…
Longer Reads
Artist Guides
20/04/2018: "Rock The Casbah" by The Clash
I will generally try to keep politics out of this blog. It can be incendiary, alienating people needlessly when all I'm trying to do is promote my favourite music. However, it must be said, music and politics, as with all culture, can interact and overlap in various ways, to varying degrees. At its best, music can inspire people and bring them together.
Perhaps not many genres are more overtly political than punk rock, and The Clash were undoubtedly a politically aware band. "Rock The Casbah" is about an Arab dictator trying to ban rock music, with his people revolting and listening anyway.
"By order of the prophet
We ban that boogie sound"
The none-too-subtle video satirises countries like Saudi Arabia, and was inspired partly by the Islamic Revolution in Iran in 1979, which resulted in very socially conservative values being imposed in Iran. I do think that any attempt to ban music is just very uncool. The band even perform in front of an oil well to hammer home their point.
The video seems to suggest that the Israel-Palestine conflict could be solved through a shared love of fast food and funky music, which at this point has got to be worth a try…
The song was released in 1982 as the third single from their album, Combat Rock. It was basically written just by their drummer, with the lyrics added by the singer. I can only say that, really, The Clash had a very talented set of musicians.
The bass part is very lively on this one, with a crazily catchy riff played on the guitar and piano. The chorus is very catchy as well, giving the whole thing a real riotous joy.
The funk is just irrepressible!
CategoriesPunk TagsFunk, Party, Political Songs, The Clash
Previous PostPrevious 19/04/2018: "Memory Lane (Sittin' In Da Park)" by Nas
Next PostNext 21/04/2018: "Funkytown" by Lipps Inc.
Find Something New
Pick Your Poison Select Category Afro-Beats Blues Classical Country Dance Bass Music Breakbeat Disco Drum and Bass Dubstep Electro Garage House Techno Trance Dancehall Dub Electronica Film Soundtracks Folk Funk Grime Highlife Hip Hop Jazz Bossa Nova Pop R'n'B Reggae Rocksteady Rock Heavy Metal Punk Ska Soul Uncategorized
The Music365 Playlist
Open in Spotify


text:
Q: Web scraping 40+ websites in search of opportunities in python I am trying to automate the task of searching for opportunities (tenders) in 40+ websites, for a company. The opportunities are usually displayed in table format. They have a title, date published, and a clickable link that takes you to a detailed description of what the opportunity is.
One website example is:
http://www.eib.org/en/about/procurement/index.htm
The goal would be to retrieve the new opportunities that are posted everyday and that fit specific criteria. So I need to look at specific keywords within the opportunities' title. These keywords are the fields and regions in which the company had previous experience.
My question is: After I extract these tables, with the tenders' titles, in a dataframe format,  how do I search for the right opportunities and sort them by relevance (given a list of keywords)? Do I use NLP in this case and turn the words in the titles into binary code (0s and 1s)? Or are there other simpler methods I should be looking at?
Thanks in advance!

A: To sort the tenders by relevance, you need define the relevance.
In this case you could count the number of occurrence of your keywords in the tender and this would be your relevance score. You can then only keep the ones that have at least one appearing keyword.
This is a first try, you can improve this by adding keywords, or assign a higher score if the keyword is in the title rather than in the detailed description...
The task you might be trying to solve here is information retrieval:  rank documents (the tenders) given their relevance to a query (your keyword).
So then you can use weighing schemes like Tf-Idf or BM25, etc... But it depends on your needs, maybe counting the keyword is more than enough !


text:
\section{Introduction}
Low mass X-ray binaries (LMXBs) with orbital periods of less than one hour are known as ultra-compact X-ray binaries. Their short orbital periods
imply orbits that are so tight that only an evolved compact donor could fit (e.g. \citealt{1984ApJ...283..232R}; \citealt*{1986ApJ...311..226N}).
Therefore, they must consist of a white dwarf  or a
helium star that has filled its Roche lobe and is accreting onto
a neutron star \citep*[e.g.][]{1993ARep...37..411T, 1995ApJS..100..233I, 1995xrbi.nasa..457V, 2003ApJ...598.1217D, 2005ApJ...624..934D}.

X-ray radiation from LMXBs usually consists of a primary and a reflected component \citep[e.g.][and references therein]{2010LNP...794...17G}. Primary
radiation is most likely created in a hot optically thin corona, the disk itself or -- in the case of a neutron star accretor --
in the boundary layer that forms on the surface of the star.
The reflected component is produced when primary radiation is reprocessed  by the optically thick Shakura - Sunyaev accretion disk and by the surface of the
donor star facing the compact object. X-ray reflection spectra originating in normal LMXBs with main sequence or red giant
donors are characterized by a bright iron  $\rm K{\rm\alpha}$ emission
line at $\approx 6.4-6.9$\,keV with an equivalent width (EW) typically of the order of $\approx100$\,eV  \citep[e.g.][]{2010ApJ...720..205C}.

The composition of the accreting material in UCXBs is  expected to be significantly different from the solar
composition accretion disks of typical LMXBs with main sequence or red giant donors.
Due to the nature of their compact donor,
their chemical composition is expected to be consistent with the ashes of H burning (mostly He and $\rm ^{14}N$),
He burning (mostly C/O) or carbon burning (mostly O/Ne).
Depending on initial parameters and the environment (e.g. being part of a globular cluster) of UCXB progenitors they
will follow different evolutionary channels, resulting in a variety of
donors ranging from non-degenerate He stars to C-O or O-Ne-Mg white dwarfs \citep*[e.g.][]{1986A&A...155...51S,2002ApJ...565.1107P,2002A&A...388..546Y, 2004ApJ...607L.119B}.
Due to the fact that the different UCXB formation channels lead to degenerate donors of similar mass,
determining the chemical composition of the disk (and therefore the donor star) in UCXBs can provide valuable insights
into the evolutionary path that created each system.

In principle, a straight forward determination of the chemical composition of the disk and donor star in these systems could be achieved
using optical spectroscopy. A He-rich object could be identified by the presence of strong He lines in its spectrum
\citep[e.g][]{2006MNRAS.370..255N}, while a C/O-rich object can be inferred by the lack of H and He lines combined with the presence
of strong C and O lines \citep[e.g.][]{2004MNRAS.348L...7N, 2006A&A...450..725W}. However, due to their small sized accretion disks
\citep{1994A&A...290..133V} the optical counterparts of UCXBs are quite faint, with V-band absolute magnitudes that are usually larger than
$\approx$5 with distances ranging from $\approx$3-12\,kpc \citep[e.g.][]{2004MNRAS.348L...7N, 2006MNRAS.370..255N}.
Therefore, ensuring definitive proof of the donor star composition -- using optical spectroscopy -- is a difficult task
that can only be attempted using the latest generation of $>$8m telescopes.

In the case of X-ray spectroscopy the presence of O and Ne emission features --
that appear in the spectra of reprocessed emission from the accretion disk and
white dwarf surface --  \cite[e.g.][]{2010MNRAS.407L..11M} and K-edges stemming from
absorbing material in the vicinity of the disk \cite[e.g.][]{2010ApJ...725.2417S}
could also provide direct indication of a C/O or O/Ne-rich disk and donor star.
However, due to increased interstellar absorption below 1\,keV and
contamination of the reflected component by the primary emission, detection of these features with sufficient
accuracy, often proves to be difficult.
On the other hand, in \cite{2013MNRAS.432.1264K}, we demonstrated that
the most striking and readily observable consequence of an anomalous C/O abundance
involves the iron $\rm K{\rm\alpha}$ line located at 6.4\,keV. In particular, for a source of moderate
luminosity (${\rm L}\rm_X\lesssim$ a few $10^{37}\rm erg\,s^{-1}$) we predicted a strong
suppression of the Fe $\rm K{\rm\alpha}$ line in the case of a C/O or O/Ne/Mg WD donor. This translates to a more than an order of magnitude
decrease of the EW of the line.
On the other hand, in the case of a He-rich donor the iron line is expected to remain unaffected
with its EW similar to that observed in LMXBs with main sequence or red giant donors. As was demonstrated in Koliopanos et al.
these results are luminosity dependent. Namely,
for luminosities exceeding $\rm LogL\rm_X\approx 37.5 $, we expect C, O and Ne to be fully ionized in the inner parts of
the disk and thus canceling their screening effect on the iron line.

In addition to spectroscopic analysis, one could indirectly infer the accretion disk and donor star composition by
studying a system's bursting activity. Gradual accumulation of H and/or He on the surface of an accreting neutron star can
eventually result in the ignition of the accumulated shell, producing a thermonuclear flash that is known as a type I X-ray burst
(e.g. \citealt{1976ApJ...205L.127G}; \citealt{1975ApJ...195..735H} and for a detailed review \citealt{2006csxs.book..113S}). Half of the
total population of known UCXBs have exhibited bursting activity, ranging from a few sporadic bursts to frequent bursting activity with a recurrence
time extending from a few hours to a few weeks. Sporadic bursts could be due to trace amounts of H and He in an otherwise C/O-rich accreted material.
Frequent bursting activity, on the other hand, would require copious amounts of H and/or He to refuel the bursts. Consequently,
such an activity would support arguments in favor of a He-rich donor in a particular UCXB.
This is illustrated by the detection of frequent burster \citep{2008ApJS..179..360G} 4U 1916-05 (discussed in this paper)
which is also an optically confirmed He-rich source
\citep{2006MNRAS.370..255N}. On other hand the same approach can yield conflicting results as is the case of
4U 0614+091 (also discussed in this work) whose bursting activity \citep{2010A&A...514A..65K, 2012ApJ...760..133L} seems to be inconsistent
with the strong evidence in favor of a C/O-rich donor \citep{2004MNRAS.348L...7N, 2006A&A...450..725W}.

In the present paper we investigate the chemical composition of the accretion disk in five UCXBs using X-ray spectroscopy.
In particular we analyze {\it XMM-Newton} spectra of these sources and compare our results with the findings of
Koliopanos et al. in order to put a constraint on the
chemical composition of  their accretion disks and donor star. We also analyze the spectra
of two normal LMXBs, which we use as a control sample. In Section 2
we present the sample of UCXBs and LMXBs chosen for our analysis.
We describe the details of data extraction, report on the specifics of each
observation and present our data analysis where we look
for the existence and strength of a potential iron $\rm K{\rm\alpha}$ line at $\approx 6.4$\,keV.
The analysis is followed by discussion and conclusions in Sections 3 and 4.

\section{OBSERVATIONS, DATA ANALYSIS AND results}

\begin{table*}
 \centering
 \begin{minipage}{115mm}
 \caption{List of {\it XMM-Newton} observations}
 \label{tab:obs}
 \begin{tabular}{@{}lcccc}
  \hline
   Object & obsID  & Date &Duration$^{1}$ (s)  &  Net count rate$^{2}$ (c/s) \\
     \hline
  UCXBs      &    &    &  \\
 \hline
 4U 0513-40       & 0151750101  &  2003-04-01  & 16420 & $35.40\pm0.05$\\
 4U 0614+091      & 0111040101  &  2001-03-13  & 13140 & $252.1\pm0.17$\\
 2S 0918-549      & 0061140101  &  2001-05-05  & 38070 & $60.47\pm0.06$\\
 XTE J1807-294    & 0157960101  &  2003-03-22  & 9293 & $35.42\pm0.11$\\
 4U 1916-05       & 0085290301  &  2002-09-25  & 14820 & $55.47\pm0.11$\\
      \hline
 LMXBs       &    &    & & \\
 \hline
 4U 1705-44       & 0402300201  &  2006-08-26  & 34130 & $27.23\pm0.05$\\
 SAX J1808.4-3658 & 0560180601  &  2008-10-01  & 45050 & $300.3\pm0.09$ $^{3}$\\
  \hline
\end{tabular}

 \medskip
{$^{1}$Duration of filtered pn observation.\\
 $^{2}$Full bandpass.\\
 $^{3}$Count rate after treatment for pile-up. Initial count rate was $689\pm0.1$}

\end{minipage}
\end{table*}

There are 14 confirmed UCXBs with measured orbital periods of less than one hour
\citep[e.g. see][for a comprehensive list of candidate and confirmed UCXBs]{2012A&A...543A.121V}.
The majority of these sources has been observed by multiple X-ray observatories.
The present work focuses on {\it XMM-Newton} observations.

After analyzing all {\it XMM} observations of confirmed UCXBs, we have selected five sources for further analysis.
The details of these observations are summarized in Table~\ref{tab:obs}.
The five sources were selected due to their simple, power law dominated spectrum above 2.5\,keV.
Due to calibration uncertainties, as well as features inherent in the source emission, most of the sources
in our sample display increasing spectral complexity below 2-2.5\,keV. Since the focus of our investigation lies
in the high energy part of the spectrum and a detailed  description of the spectral continuum is beyond the scope of this paper,
we have chosen to ignore all energy channels below 2.5\,keV.
This configuration allows for a more reliable detection of the Fe $\rm K{\rm\alpha}$ line.
The only exception to this treatment is SAX J1808.4-3658
where a thermal component is strongly required by the fit, despite our channel selection.
As a result -- for SAX J1808.4-3658 -- we decided to exclude only energy channels below 1\,keV and include the additional spectral component in our model.
The two LMXBs that constitute our control sample feature similar hard-state spectra.
They have been chosen in order to verify our data analysis procedures in the full range of count rates, spanned by our UCXB sample.

Data reduction was performed using the {\it XMM-Newton} Data Analysis software SAS version 13.5.0.
The present work focuses on the hard (above 1 keV) part of the spectrum and particularly the presence or absence of iron
emission features at $\approx 6-7$\,keV. The effective area of EPIC-pn at $\approx 7$\,keV is approximately five times higher than
that of MOS. Furthermore, during all observations analyzed below, at least one of the MOS detectors was operated in imaging mode. Due to the brightness
of our sources, most of the observations taken in this mode were suffering from severe pile-up.
 On the other hand -- with the exception of 4U 0513-40 -- pn was operating in timing mode during all observations analyzed in this work.
In this mode, photon coordinates are resolved only in one dimension, along the column axis, allowing for high speed CCD read out.
Apart from offering high time resolution, the timing mode is particularly suited for observing bright sources, since it  allows
for a higher non-piled up count rate.
For these reasons our work is based exclusively on pn data.

Source photons for all pn observations, taken in timing mode, were extracted
for RAWX from 25 to 50 and background for RAWX from 3 to 5, where RAWX is the coordinate
along the column axis.
For 4U 0513-40, where pn was operating in imaging mode,
we extracted the source spectrum from a 27\arcsec circle centered at the source. Background was extracted according to
latest EPIC calibration notes\footnote{http://xmm2.esac.esa.int/docs/documents/CAL-TN-0018.pdf}
from a source-free region at the same {\small{RAWY}} position as the source region.
In all cases we extract photons with pixel pattern less than 5.
All pn observations were checked for pile-up, using the SAS task \texttt{epatplot}. With the exception of
SAX J1808.4-3658 no signatures of pile-up were found for any of the sources in our samples.
Due to the high count rate of SAX J1808.4-3658 the pn data suffered from pile-up.
To minimize pile-up effects we removed the three central columns from our extraction region.
A subsequent \texttt{epatplot} test
confirms that pile-up effects have been adequately treated.
Lastly, event files for all sources observed in timing mode were treated with \texttt{ epfast}.
This SAS tool is a default setting in SAS 13.5 and corrects possible Charge Transfer Inefficiency (CTI) effects, due to high count rate.

Analysis is done using the {\small {XSPEC}} spectral fitting package, version 12.8.0
\citep{1996ASPC..101...17A}. Prior to analysis, all spectra were re-binned to ensure a minimum of 25 counts per energy channel.
All spectra are fitted with a simple power law, with exception of SAX J1808.4-3658 where an additional
thermal black body component was required.
The iron line was modeled with a Gaussian and when not detected an upper limit on its EW was calculated at 90\% confidence.
Best-fit parameters for the spectral continuum of all objects along with their distances and
luminosities calculated in the 2.5-10\,keV range are summarized in Table \ref{tab:cont}.
Best-fit parameters and EWs for Fe $\rm K{\rm\alpha}$ emission lines (or upper limits in the case of non detection) are presented in Table \ref{tab:lines}.

\begin{table*}
 \centering
 \begin{minipage}{157mm}
  \caption{Best-fit parameters for spectral continuum. All uncertainties are $1\,{\rm \sigma}$. }
\label{tab:cont}
  \begin{tabular}  {lccccc}
  \hline
 Sources   &    &   Power Law & &Luminosity&Distance\\
 \cline{1-6}
 \hline
          &            $ {\rm \Gamma}$ &Norm                                        &   $\rm{{\chi_{\nu}}^{2}}$(d.o.f)   &Lx$^{1}$&\\
          &                &($10^{-2}\,{\rm ph\,keV^{-1}\,cm^{-2}\,s^{-1}}$)  &   &($10^{36}{\rm \,erg\,s^{-1}}$)&(kpc)\\
  \hline
  With faint or no Fe $\rm K{\rm\alpha}$ line\\
  \hline
4U 0513-40    & $2.04_{-0.01}^{+0.02}$  & $2.29 _{-0.04}^{+0.09}$& 1.05(1065)&0.9&12.2$^{2}$\\
2S 0918-549   & $2.19\pm0.05$  & $5.93\pm0.05$   &1.01(1470)&0.4&4.8$^{3}$\\
XTE J1807-294 & $2.07 \pm0.02$  & $7.22\pm0.3$   &1.00(1265)&1.1&8.3\\
\hline
  With bright Fe $\rm K{\rm\alpha}$ line\\
  \hline
4U 0614+091        & $2.28\pm0.01$  & $32.91 _{-0.7}^{+0.8}$      &1.01(1490)&0.6& 3.2$^{4}$\\
4U 1916-05   &  $1.84\pm0.02$  & $6.22\pm0.20$  &1.07(1413)&1.6&8.9$^{5}$\\
\hline
Control sample\\
  \hline
4U 1705-44         &  $1.91\pm0.01$  & $8.85\pm0.16$  &1.05(1493)&1.5&7.4$^{6}$\\
SAX J1808.4-3658   &  $2.19\pm0.01$  & $76.5\pm0.01$  &1.30(1795)&2.0&3.5$^{7}$\\
\hline
\end{tabular}

\medskip

{The models used are: \texttt{phabs$\cdot$powerlaw} (4U 0513-40, 2S 0918-549, XTE J1807-294),
\texttt{phabs$\cdot$(powerlaw+gaussian)} (4U 0614+091, 4U 1705-44), \texttt{phabs$\cdot$(powerlaw+gaussian)$\cdot$gabs$\cdot$gabs} (4U 1916-05)
and \texttt{phabs$\cdot$(blackbody+powerlaw+gaussian)} (SAX J1808.4-3658). Here \texttt{phabs} is the XSPEC model for photoelectric absorption
and \texttt{gabs} is the XSPEC model for a Gaussian absorption line.
The paramaters of the black body component in SAX J1808.4-3658 are kT=$0.23\pm0.003$ and norm=0.007$\pm0.0002$.

$^{1}$ Calculated in the 2.5-10\,keV range.
$^{2}$ \cite{2003A&A...399..663K}
$^{3}$ \cite{2004MNRAS.354..355J}
$^{4}$ \cite{2010A&A...514A..65K}
$^{5}$ \cite{2008ApJS..179..360G}
$^{6}$ \cite{2008ApJS..179..360G}
$^{7}$ \cite{2009ApJ...694L..21C, 2009A&A...493L..39P}}

\end{minipage}
\end{table*}

\begin{figure}
  \centering
\includegraphics[trim=0cm 1.20cm 0cm 0cm, clip=true, width=0.5\textwidth, angle=-90]{combined_II.eps}
\caption{Ratio of the data to continuum model vs energy (keV) for three UCXB systems where no Fe line was detected.
Best-fit parameters of the continuum models and upper limits on Fe line flux and EW are listed in Tables~\ref{tab:cont} and~\ref{tab:lines}, respectively.}

\label{fig:noline}
\end{figure}

\subsection{4U 0513-40}
4U 0513-40 is located at a distance of $\approx12.2$\,kpc \citep{2003A&A...399..663K} and has an observed orbital period of 17\,min \citep{2011MNRAS.414L..41F}.
It has been observed by {\it BeppoSAX} , {\it Chandra}, {\it INTEGRAL}, {\it RXTE} and {\it XMM-Newton}.
{\it XMM-Newton} observations have been analyzed by \cite{2005ApJ...627..926J}, where they report no significant emission or absorption features in the spectrum.
No constraints on the donor composition -- based on optical spectroscopy -- have been reported.

At least nine thermonuclear X-ray bursts have been reported for 4U 0513-40. Two of them have been observed
by Chandra and BeppoSAX \citep[][respectively]{2001ApJ...550L.155H, 2011MNRAS.414L..41F}, and another 7 by
RXTE \citep{2008ApJS..179..360G}. The latter have been detected after analyzing more than ten years of
RXTE observations.

{\it XMM-Newton} observed 4U 0513-40 on 2003 April 1 for 24 ks.  All EPIC-cameras were working
in imaging mode with MOS1 and MOS2 suffering from considerable pile-up.
The net source count rate is $35.40\pm0.05\,{\rm c/s}$.

The spectrum of 4U 0513-40 above 2.5\,keV, was adequately described by an absorbed power law.
No Fe $\rm K{\rm\alpha}$ emission line was detected in the spectrum.
An upper limit for the EW of the iron line was calculated by including a Gaussian with a fixed width
of 0.5\,keV, centered between 6.4-6.9\,keV. The source has a moderate luminosity.

\subsection{4U 0614+091}
4U 0614+091 lies close to the galactic plane, at a distance of $\approx3.2$\,kpc \citep{2010A&A...514A..65K}
and has a measured optical period of $\approx50$\,min
\citep{2008PASP..120..848S}. It has been observed by {\it ASCA}, {\it BeppoSAX}, {\it Chandra},
{\it RXTE}, {\it  Swift} and {\it XMM-Newton}.
Numerous authors report the detection of a broad emission-like feature near 0.7\,keV
\citep[e.g.][]{1994ApJ...422..791C, 1999A&A...349L..77P,
2010MNRAS.407L..11M, 2010ApJ...725.2417S}. Nevertheless, using data taken with the  {\it Chandra}
 {\it Low-Energy Transmission Grating Spectrometer} (LETGS),  \cite{2001ApJ...546..338P} failed to detect the feature.
They do, however report an unusually high Ne/O abundance ratio based on absorption edges. Furthermore,
\cite{2001ApJ...560L..59J}, analyzing archival {\it ASCA} data, argue that the broad line-like feature,
reported by previous authors, can be explained by neon overabundance, attributed to neon-rich material local to
the binary. \cite{2010ApJ...725.2417S} analyzing data taken with the {\it High-Energy Transmission Grating Spectrometer}
(HETGS) on board {\it Chandra}, confirm the existence of
excess optical depth near the Ne K edge. They also detect an extremely broadened O{\small VIII} $\rm Ly{\rm\alpha}$
emission feature, which they attribute to emission by highly ionized material in the inner parts of the disk.
In order to account for the line broadening, the authors need to invoke the effects of
gravitational broadening. Fitting a Laor profile  \citep{1991ApJ...376...90L}
to the residuals reveals an inclination angle of the order of $\approx88^{\rm{o}}$.
However, there is no compelling evidence suggesting an edge-on inclination for 4U 0614+091
and there have been no dips observed in its light curve. To overcome this problem,
\cite{2010MNRAS.407L..11M}, suggest that a similar broad emission feature -- this time detected in
{\it XMM-Newton} RGS observations -- is due to a gravitationally broadened
O{\small VIII} emission line, that is the result of reflection of the source's primary spectrum off a C/O-rich disk. In this scenario,
line broadening is partly due to effects of Compton scattering and their fit does not require such
a high inclination angle. \citeauthor{2010MNRAS.407L..11M} also report the absence of an iron emission line
in their analysis of MOS2 data of the same observation. They propose that
this could also be attributed to non solar composition of the accretion disk. Nevertheless \cite{2010A&A...522A..96N},
analyzing pn data of the same {\it XMM-Newton} observation, report a broad emission feature at $\approx6.8\,\rm{keV}$ with an
EW of the order of $\approx160$\,eV. In a more recent publication, \cite{2014arXiv1403.1432M} reanalyze
RGS observations of 4U 0614+091, this time using a modified version of the {\small{XIILVER}} reflection model \citep{2010ApJ...718..695G, 2013ApJ...768..146G}.
{\small{XIILVER}} is adjusted to mimic a C/O-rich disk by increasing the abundances of carbon and oxygen relative to hydrogen by more than a hundredfold.
This produces a disk reflection spectrum featuring a strong O{\small{VIII}} emission line which is then used to model RGS observations of 4U 0614+091.
The authors conclude that the broad positive residuals at $\approx$0.7\,keV are due to a relativistically broadened O{\small{VIII}} emission line
caused by reflection off a C/O-rich disk.

Absence of H or He lines, along with the presence of C{\small{I-IV}} and O{\small{I-III}} emission lines in optical
spectra of 4U 0614+091, taken with {\it VLT}, suggest a C/O-rich accretion disk and donor star \citep{2004MNRAS.348L...7N, 2006A&A...450..725W}.
In particular, \citeauthor{2006A&A...450..725W} use synthetic spectra, generated by a non-LTE accretion disk model,
to place an upper limit of 10\% on the abundance of H and/or He present in the accretion disk.
These conclusions seem to be at odds with the fact that 4U 0614+091 is a source
of multiple X-ray bursts, with a measured recurrence time ranging from once every few weeks to once every $\approx10\,$days
\citep{2010A&A...514A..65K, 2012ApJ...760..133L}. Namely, \citeauthor{2010A&A...514A..65K} --
based on archival data collected from multi-instrument observations -- calculate an average burst recurrence rate of about once every one to
two weeks. \citeauthor{2012ApJ...760..133L} use data collected with
the Gamma-ray Burst Monitor (GBM) aboard the {\it Fermi Gamma-ray Space Telescope} to calculate
a burst recurrence time of $\approx12$\,d, with the closest burst pair recorded within 2.8\,d. Furthermore, by creating ignition
models for type I X-ray bursts, following the work of \cite{2001ApJ...559L.127C}, \citeauthor{2010A&A...514A..65K}
demonstrate that a H or He amount, substantially larger than the inferred
upper limit of 10\%, is required to simulate the characteristics of the observed bursts.

{\it XMM-Newton} observed 4U 0614+091 on 2001 March 13. There were two subsequent observations
for $\approx11$\,ks and  $\approx17$\,ks. The MOS1, MOS2 and pn detectors
were only active during the second observation, therefore we focus on the second observation only.
The net source count rate is $252.1\pm0.17\,{\rm c/s}$.

Modeling 4U 0614-091 with an absorbed power law leaves increased positive residuals
in the 6-7\,keV range (Fig.~\ref{fig:lines}). We account for these by adding a Gaussian to our initial model.
This reveals a bright and broad Fe $\rm K{\rm\alpha}$ emission line and improves our fit by a $\Delta\chi^2$ of
89, which corresponds to a more than 4$\sigma$ significance for 3 d.o.f..
The line is centered at $\approx6.64$\,keV with an EW of $\approx111$\,eV
and a width of  $\approx0.7$\,keV.

\subsection{2S 0918-549}
2S 0918-549 has a measured orbital period of 17.4\,min \citep{2011ApJ...729....8Z} and lies at a distance of $\approx4.8$\,kpc \citep{2004MNRAS.354..355J}. It has been observed
by {\it ASCA}, {\it BeppoSAX}, {\it Chandra}, {\it RXTE}, {\it XMM-Newton} and {\it VLT}. \cite{2001ApJ...560L..59J}
analyzed archival {\it ASCA}  observations of 2S 0918-549.
They suggested an O/Ne chemical composition of the accreting material based on an unusual Ne/O number ratio compared to what is
expected for the interstellar medium. This non-solar relative abundance of Ne was attributed to enrichment of the local ISM by the donor material.
However further examination \citep{2003ApJ...599..498J, 2005ApJ...627..926J}
revealed that the Ne/O ratio varies between different  {\it Chandra}, {\it XMM-Newton} and
{\it ASCA} observations of 2S 0918-549. This variability, combined with a tenfold decrease in flux
between the  {\it Chandra} and {\it XMM-Newton} observations and the earlier one by {\it ASCA},
led to the conclusion that the unusual Ne/O ratio maybe due to ionization effects and is not proof of the donor composition.
In their analysis of 2S 0918-549, \cite{2003ApJ...599..498J} do not comment on the existence or absence of the iron  $\rm K{\rm\alpha}$ emission line.
{\it VLT} data, analyzed by \cite{2004MNRAS.348L...7N} tentatively suggest a C/O-rich chemical composition of the accretion disk and donor star.

2S 0918-549 is also known to produce sporadic X-ray bursts. At least six type I X-ray bursts have been reported
for this binary between 1996 and 2004. Two have been observed by \cite{2001ApJ...553..335J} and \cite{2002A&A...392..885C} and another
four by \cite{2005A&A...441..675I}. \citeauthor{2005A&A...441..675I} in contrast to what is suggested by optical data,
suggest the possibility of a He-rich donor, based on the system's bursting activity.

{\it XMM-Newton} observed 2S 0918-549  on 2001 May 5 for 40 ks. MOS1 and pn cameras were operated in timing mode, while the MOS2 camera was operated in imaging mode.
The net source count rate is $60.47\pm0.06\,{\rm c/s}$.

Similarly to 4U 0513-40, 2S 0918-549 has a moderate luminosity and is adequately modeled with an absorbed power law. No emission feature was required by the fit.

\subsection{XTE J1807-294}
XTE J1807-294 is a transient, accreting  millisecond pulsar.
\cite{2003ATel..127....1M}, using {\it Chandra} observations, detected the source in the direction of the galactic bulge,
suggesting a distance of  $\approx8.3$\,kpc. X-ray pulsations observed
using {\it RXTE}  give an orbital period of $\approx 17$\,min \citep{2003ATel..127....1M}. {\it XMM-Newton} observations
were analyzed by \cite{2003ApJ...594L..39C}. No emission or absorption features were detected, and an upper limit of 18-25\,eV is placed on
the EW of the iron line. Similarly, simultaneous {\it INTEGRAL}, {\it XMM-Newton} and {\it RXTE}  observations by \cite{2005A&A...436..647F}
revealed no evidence of emission or absorption features in the source continuum.
{\it VLT} observations by \cite{2009A&A...508..297D} failed to detected the source's optical counterpart.
No type I X-ray bursts have been reported for this system.

{\it XMM-Newton} observed XTE J1807-294 on 2003 March 22 for $\approx 17$\,ks during an outburst.
MOS1 and MOS2 were operating on imaging mode and both suffered from pile-up.
The net source count rate is $35.42\pm0.11\,{\rm c/s}$.

Again, the spectrum was modeled with an absorbed power law and no Fe $\rm K{\rm\alpha}$ emission line was detected.
The data-to-model ratio vs energy plot for XTE J1807-294 is presented in Fig.~ \ref{fig:noline} along with those of
4U 0513-40, 2S 0918-549 for which also no iron line was detected.

\subsection{4U 1916-05}
4U 1916-05 is a dipping source (its light curve exhibits periodic intensity dips),
with an orbital period of 50\,min \citep{1982ApJ...253L..67W} and a distance of
$\approx8.9$\,kpc  \citep{2008ApJS..179..360G}. The characteristics of the source's dipping behavior
indicate that it is viewed at a large inclination angle, with $\rm i\ge60{}^\circ$ \citep{1988MNRAS.232..647S}.
{\it ASCA} observations of 4U 1916-05 were analyzed by \cite{2000ApJS..131..571A}. They report a broad emission feature at 5.9\,keV with an
EW of $\approx$87\,eV. The presence of an emission feature in the unusual energy of 6.0\,keV is also reported by \cite{2004A&A...418.1061B} in their
analysis of the {\it XMM-Newton} observation of 4U 1916-05. However this feature was not further investigated as it was not the focus of their paper.
On the other hand, they report the detection of two narrow absorption lines at 6.65 and 6.95\,keV that are consistent with resonant absorption
from Fe{\small XXV} and Fe{\small XXVI} ions, respectively. This detection is repeated in {\it Chandra} observations analyzed by \cite{2006ApJ...646..493J}.
The authors also report the existence of narrow absorption lines, due to the presence of H-like neon, magnesium, silicon, and sulfur. In addition to X-rays,
optical observations by {\it VLT}, found prominent lines from He{\small I}, He{\small II}, N{\small II} and N{\small III},
consistent with a He-rich accretion disk \citep{2006MNRAS.370..255N}.

4U 1916-05 is also a known X-ray burster. It exhibits short bursts that are consistent with moderate to high accretion rates, and have
a recurrence time of $\approx$6.2\,hr \citep{2008ApJS..179..360G}.

{\it XMM-Newton} observations of 4U 1916-05, analyzed in this work, were performed on September 25, 2002 for 17 ks. All
EPIC cameras were operating in timing mode. The net source count rate is $55.47\pm0.11\,{\rm c/s}$.

Fitting the spectrum of 4U 1916-05 with an absorbed power law revealed a complex structure
with both positive and negative residuals between $\approx6-7$\,keV (Fig.~\ref{fig:lines}).
As has been suggested before \citep[e.g.][]{2004A&A...418.1061B}, the negative residuals could be interpreted as
absorption lines at $\approx6.65$ and $\approx6.95$\,keV, due to resonant absorption by Fe{\small XXV} and Fe{\small XXVI} ions.
To account for these features, we add two narrow Gaussian absorption lines to our model. The first one -- corresponding to absorption due to He-like iron --
is centered at $\approx6.66$\,keV and improves our fit by a $\Delta\chi^2$ of 40 for 3 d.o.f..
The second -- corresponding to absorption due to H-like iron --
is centered at $\approx6.92$\,keV and reduces the $\chi^2$ value by 20 for 3 d.o.f..
The two absorption lines  are strongly required by the fit and are of high (more than 3$\sigma$) significance.
They can be attributed to highly ionized plasma in the vicinity of the accretion disk.

The remaining positive residuals suggest a complex broad emission feature in the 5-7\,keV range.
Fitting this feature with a Gaussian reveals a broad emission
``line'' at the unexpected energy of $\approx5.46$\,keV with a width of $\approx1.64$\,keV.
The EW of this feature is $\approx595$\,eV. Adding the Gaussian line to our model,
 improves our fit massively,  by a $\Delta\chi^2$  of 187 for 3 d.o.f..
However, the unusual values of the line parameters and the fact that this is a dipping source,
could indicate that this feature is an artifact resulting from our extraction of a
single spectrum for the entire observation, during both dipping and persistent phases.
To investigate this possibility, we extracted two additional spectral sets. One taken from events that
were recorded only during the persistent phase and a second one during the dipping phase.
The results are qualitatively identical to the ones obtained for the full observation.
All three spectra (dipping, persistent and combined) show strong evidence of a broad emission feature
located at $\approx5.5-6$\,keV.
Obviously this feature is too complex to be fitted with a simple Gaussian.
Hence the parameters obtained have no physical meaning.
Nevertheless, in the framework of our model, the statistical significance of a strong iron emission line
in the 6-7\,keV range is beyond doubt.
Further examination of the detailed spectral shape of the emission line is beyond the scope of this paper.
If we fix the line energy at 6.4\,keV and the line width at 0.5\,keV
we obtain an emission line with an EW of $\approx95$\,eV with more than $4{\rm\sigma}$ significance.

\begin{figure}
\centering
\includegraphics[trim=0cm 1.20cm 0cm 0cm, clip=true, width=0.5\textwidth, angle=-90]{combi_line_II.eps}
\caption{Ratio of the data to continuum model vs energy for 4U 1916-05 and 4U 0614-091 whose spectra feature a bright iron line.
Best-fit parameters of the continuum models are listed in Table~\ref{tab:cont}. Fe line flux and EW for Gaussian
are listed in Table~\ref{tab:lines}.}
\label{fig:lines}
\end{figure}

\subsection{Control Sample}

\subsubsection{4U 1705-44}
4U 1705-44 is a typical LMXB containing a neutron star accretor with a weak magnetic field.
Its distance is measured at $\approx 7.4$\,kpc \citep{2008ApJS..179..360G}. The source exhibits frequent type I
X-ray bursts \citep[e.g.][]{1989ApJ...339.1044G} and has been observed during hard and soft states. In both states its
spectrum features a bright broad iron $\rm K{\rm\alpha}$ emission line
\citep[e.g][]{2005ApJ...623L.121D, 2009MNRAS.398.2022D, 2010ApJ...720..205C, 2013A&A...550A...5E}.
Multiple observations of 4U 1705-44 have been performed by all major X-ray telescopes. 4U 1705-44 is a frequent burster
with a recurrence time of $\approx0.91$\,hr \citep{2008ApJS..179..360G}.

In the present work we reanalyze {\it XMM-Newton} observations performed on September 26, 2006 during a hard state.
Only pn and RGS were active during the observation with pn operating in timing mode. The net source count rate is $27.23\pm0.05\,{\rm c/s}$.

As expected for the LMXBs in our control sample, we detect
strong positive residuals in the 6-7\,keV range (Fig. \ref{fig:control}), characteristic of a strong iron line.
Fitting the emission feature  with a Gaussian yields an emission line with an EW of $\approx52$\,eV (for details see Table~\ref{tab:lines}).

 \subsubsection{SAX J1808.4-3658}
SAX J1808.4-3658 is a transient LMXB with an orbital period of $\approx2.01$\,hrs \citep{1998Natur.394..346C}.
Its distance is measured at $\approx 3.5$\,kpc \citep{2009ApJ...694L..21C, 2009A&A...493L..39P}.
It was the first millisecond pulsar discovered \citep{1998Natur.394..344W}. The source's quiescent periods are
interrupted by short outbursts approximately every 2.5 years. SAX J1808.4-3658 has been observed by
{\it ASCA}, {\it BeppoSAX}, {\it Chandra}, {\it INTEGRAL}, {\it  Swift}, {\it RXTE} and  {\it XMM-Newton}
during both quiescent and bursting periods. {\it VLT} observations have also been performed during its 2008 September-October
outburst. Analysis of source spectra during outbursts, have revealed the existence of a Fe $\rm K{\rm\alpha}$ emission line
\citep[e.g][]{1998A&A...338L..83G, 2009ApJ...694L..21C, 2009A&A...493L..39P}. Lastly, the source is a
burster with a recurrence time of  $\approx21$\,hr \citep{2008ApJS..179..360G}.

We reanalyze  the 63\,ks  {\it XMM-Newton} observation of October 1st 2008 during outburst. The MOS1 camera operated in imaging mode
while MOS2 and pn in timing mode.
The net source count rate is $300.3\pm0.09\,{\rm c/s}$.

SAX J1808.4-3658 is fitted using a black body and a power law spectrum.
Examination of the data-to-model ratio of our fit, reveals a strong emission feature at the 6-7\,keV range (Fig. \ref{fig:control}). Fitting this
feature with a Gaussian reveals a broad emission line centered at $\approx6.61$\,keV with a width of $\approx1.13$\,keV
and an EW of $\approx246$\,eV. The emission feature is characteristic of the iron $\rm K{\rm\alpha}$ emission line
expected in X-ray reflection spectra originating in typical LMXBs with main sequence or red giant donors.
The broadness of the line obviously justifies further inquiry on different possible mechanisms
that would explain it. However, such a task has already been accomplished by \cite{2009A&A...493L..39P} and is not the focus of the present work.

\begin{figure}
  \centering
\includegraphics[trim=0cm 1.20cm 0cm 0cm, clip=true, width=0.5\textwidth, angle=-90]{LMXB_combi_2.5keV.eps}
\caption{Ratio of the data to continuum model vs energy for the two LMXBs in our control sample.
Best-fit parameters of the continuum models are listed in Table~\ref{tab:cont}.
Fe line flux and EWs are listed in Table~\ref{tab:lines}.}
\label{fig:control}
\end{figure}

\begin{table*}
 \centering
 \begin{minipage}{143mm}
  \caption{Best-fit parameters of iron $\rm K{\rm\alpha}$ emission line.
  In case of no detection an upper limit at $90\%$ confidence level is given. All errors are 1$\rm \sigma$.}
\label{tab:lines}
  \begin{tabular}  {lccccl}
  \hline

 Sources &  & Gaussian&  &&Bursts\\
 \cline{1-6}
 \hline
        &Norm             &  LineE      & ${\rm \sigma}$     &EW     &Rec. Time$^{1}$\\
        & ($10^{-5}\,{\rm ph\,cm^{-2}\,s^{-1}}$)     &  (keV)      & (keV)              &   (eV)&\\
  \hline
  With faint or no Fe $\rm K{\rm\alpha}$ line\\
  \hline
4U 0513-40        & $<0.92$ & 6.4-6.9& 0.5$^{2}$&$<20$&9 bursts\\
2S 0918-549       & $<0.63$ & 6.4-6.9& 0.5$^{2}$&$<7 $&6 bursts\\
XTE J1807-294     & $<1.25$ & 6.4-6.9& 0.5$^{2}$&$<10$&0 bursts\\
  \hline
  With Fe $\rm K{\rm\alpha}$ line\\
  \hline
4U 0614+091        &$32.9_{-7.4}^{+7.9}$  & $6.64\pm0.08$  & 0.67$_{-0.08}^{+0.10}$&$111.1_{-17}^{+20}$&$\approx$10\,d\\
4U 1916-05   &$27.7\pm2.47$&6.4$^{2}$&0.5$^{2}$  &$95\pm12$&$\approx$6.2\,hr\\
  \hline
Control sample\\
  \hline
4U 1705-44        & $13.2_{-1.82}^{+1.95}$ & $6.53\pm0.05$&$0.34\pm0.05$&$51.7_{-12}^{+13}$&$\approx$0.91\,hr\\

SAX J1808.4-3658  & $173\pm27$ & $6.40\pm0.07$&$0.83_{-0.11}^{+0.10}$&$131\pm20$&$\approx$21\,hr\\
\hline
\end{tabular}
\medskip

{$^{1}$ Recurrence time when available. Otherwise total number of recorded bursts. All references regarding bursting activity are given in Section 2.

$^{2}$ The parameter was fixed.}

\end{minipage}
\end{table*}

\section{Discusssion}
We have analyzed the spectra of 5 confirmed UCXBs with H-poor donors and low to moderate luminosities. Specifically, we investigated the existence of a
Fe $\rm K{\rm\alpha}$ line in their spectra. Three objects in our sample --
namely 2S 0918-549, XTE J1807-294, 4U 0513-40 -- display no obvious emission features in the energy range
between 6 and 7\,keV. This result is in agreement with the works of previous authors \citep[e.g.][]{2003ApJ...594L..39C, 2005ApJ...627..926J}.
On the other hand, systems 4U 0614+091 and 4U 1916-05 display a bright iron $\rm K{\rm\alpha}$ line. This emission feature is broad and more complex than
a simple Guassian would describe, but there is no doubt that strong iron emission is evident in both sources.
The spectra of 4U 0614+091 and 4U 1916-05 are similar (e.g. see the ratio plots in figures~\ref{fig:lines} and~\ref{fig:control})
to the spectra of typical LMXBs like 4U 1705-44 and SAX J1808.4-3658, also analyzed in this work.

\begin{figure}
  \centering
\includegraphics[trim=0.2cm 0cm 0cm 0cm, clip=true, width=0.52\textwidth, angle=0]{Graph2_MC_II.eps}
\caption{ Dependence of Fe $\rm K{\rm\alpha}$ line EW (eV) on O/Fe ratio, given in units of its solar value.
The curves were calculated for an incident spectrum with power law spectral shape with an index of 2.2. The solid curve is calculated for
a face-on configuration ($0^{{\rm o}}$ inclination) and the dotted line for an $\approx$edge-on configuration ($80^{{\rm o}}$ inclination).}
\label{fig:code}
\end{figure}

\subsection{X-ray diagnostics}
In Koliopanos et al. (2013) we showed that non-solar composition of the accretion disks in UCXBs can have a powerful effect on
fluorescent emission lines appearing in their spectra. Namely, the bright iron $\rm K{\rm\alpha}$ line, typically found in
spectra of LMXBs with main sequence or red giant donors, is expected to be severely suppressed in the case of UCXBs with  C/O or O/Ne/Mg WD donors.
This is due to screening by oxygen in the C/O or O/Ne dominated material.
On the other hand, due to the lower ionization threshold of He,
the iron line in spectra of UCXBs with He star or He WD donors, is expected to retain its nominal strength, mostly determined by iron abundance.
Ionization of the disk material at high mass accretion rates may lead to luminosity dependence of this behavior.
Specifically, line suppression due to screening by oxygen, is expected to
take effect in objects with moderate luminosities (${\rm L}\rm_X\lesssim$ a few $10^{37}\rm erg\,s^{-1}$).

\subsubsection{Sources with no Fe $\rm K{\rm\alpha}$ emission line}
Using results of our Monte Carlo simulation from Koliopanos et al. (2013)
we can place constraints on the O/Fe ratio of the accretion disk in the three sources
for which an iron line was not detected. The code simulates reflection off a homogeneous slab of infinite optical depth
that is comprised of cold and neutral material . For this example, the primary, incident radiation has a power law shaped spectrum with a
spectral index of 2.2 and is emitted isotropically from a point source above the disk surface.
In order to study the whole range of possible configurations,
from face-on to $\approx$edge-on view, we run two sets of calculations, where the reflection spectrum is registered
at two distinct viewing angles of $0^{\rm o}$ and $80^{\rm o}$ respectively.
Since there are no dips in the light curves of the three systems, we do not investigate a viewing angle larger than $80^{\rm o}$.
The code simulates fluorescence $\rm K{\rm\alpha}$ and $\rm K{\rm\beta}$ lines for elements from Z=3 to 30
and reports their EWs with respect to the total emission, which is a mixture of both the primary and reflected emission
(for details see Appendix A in Koliopanos et al. 2013).

We generate a grid of EW values of the Fe $\rm K{\rm\alpha}$ fluorescence line at 6.4\,keV, calculated for a sequence of
increasing C/O abundance, starting with solar-like material. Abundances of H and He are reduced along the sequence, thus conserving the total number of nucleons.
Similarly to Koliopanos et al. mass fractions of all other elements remain fixed at their solar values, as well as the abundance ratio of carbon
and oxygen. The position along this sequence is given in terms of O/Fe ratio, in units of its solar value.
Obviously, as H and He are ``converted'' to C and O, O/Fe ratio will increase. The maximum value of the O/Fe ratio that
corresponds to a C/O-rich disk -- in which all hydrogen and helium has been replaced by carbon and oxygen -- is $\approx77$ times its solar value.
Solar abundances for elements with Z=1-30 were adopted from \cite{1992PhyS...46..202F}, elements not listed in
this tabulation were taken from \cite{1998SSRv...85..161G}.
The resulting dependencies of EW on the O/Fe ratio are presented in Fig.~\ref{fig:code}.

As is evident from the plot, even in the marginal case of a system viewed $\approx$edge-on,
an EW value of 20\,eV -- the highest upper limit measured for the three sources -- corresponds to an O/Fe
ratio that is more than $\approx$10 times higher than the solar value.
The EW upper limits of 7 and 10\,eV -- for 2S 0918-549 and XTE J1807-294 -- correspond to  O/Fe
ratios exceeding $\approx$37 and $\approx$20 times the solar value, respectively. Since there are no indications (e.g. a dipping light curve)
of a large inclination angle for these three sources, the real lower limits are probably higher. These results
place a strong constraint on the chemical composition of these systems.
Namely, we conclude that the lack of an iron emission line in the spectra of 2S 0918-549, XTE J1807-294 and 4U 0513-40
is the result of a C/O or O/Ne/Mg-rich accretion disk and donor star in these systems.

A final point of interest regarding  Fig.~\ref{fig:code} is the fact that in this example, our calculations predict
a maximum Fe $\rm K{\rm\alpha}$ EW value of $\approx$100\,eV. This value is in agreement with the values
obtained by the fits of 4U 0614+091 and 4U 1705-44 but it is relatively smaller than the value obtained for SAX J1808.4-3658
and significantly smaller than the one obtained for 4U 1916-05.
This apparent discrepancy is mostly due to the fact that a simple Gaussian profile was used to fit broad emission features that
have a more complicated shape than a Gaussian can describe. This is particularly evident in 4U 1916+091
which is a confirmed edge-on viewed system with a dipping light curve. Implementation of more sophisticated models
such a Laor profile or XSPEC model \texttt{diskline} \citep{1989MNRAS.238..729F} yields smaller,
more realistic EW values in the $\approx100$\,eV range.
Additionally, alternative modeling of the underlying spectral continuum -- especially when the full energy range is considered --
can result in different values for the EW of the line. For instance a different choice of the spectral continuum
of SAX J1808.4-3658 in \cite{2010A&A...522A..96N} resulted in an EW of  $\approx$30\,eV for the iron line. A value much smaller than
the one derived in this work ($\approx130$\,eV) and in that of \cite{2009A&A...493L..39P} ($\approx120$\,eV).
However, a detailed investigation of the emission line profiles and the shape of the spectral continuum was beyond the scope of this work, where we are only
interested in the fact of the existence of the line.
Therefore, energies below 2.5\,kev were ignored and an absorbed power law and a simple Gaussian model were used to model the spectral continuum and the emission lines.

\subsubsection{Sources with Fe $\rm K{\rm\alpha}$ emission line}
The  presence of a strong Fe $\rm K{\rm\alpha}$ line in the spectra of two remaining sources in our sample, 4U 1916-05 and 4U 0614+091
is an indication of a He-rich accretion disk and donor star in these systems. Namely, according to our model, the presence of a strong iron line,
in the spectrum of a moderately luminous object, requires an O/Fe ratio that is close to the solar value.
In the context of UCXBs, this would point towards a He-rich donor.

\subsection{Optical spectra and X-ray bursts}
Out of the three systems for which no emission line was detected, only 2S 0918-549 has been studied by means of optical spectroscopy.
The analysis of \cite{2004MNRAS.348L...7N} tentatively suggests a C/O-rich rich donor. This is in agreement with our own conclusions.
On the other hand, systems 2S 0918-549 and 4U 0513-40 have exhibited sporadic bursting activity during the previous decades
(see Table~\ref{tab:lines} and relevant subsections).
The characteristics of some of the bursts are compatible with helium burning, a fact that led \cite{2005A&A...441..675I} to suggest
the possibility of a He-rich donor in 2S 0918-549. Nevertheless, over the span of $\approx10$years,
just a handful of bursts has been reported for these two systems \citep[e.g.][]{2005A&A...441..675I, 2008ApJS..179..360G}
and therefore they cannot provide definitive proof of donor composition. It is certainly plausible that small amounts of H and/or He in an
otherwise C/O-rich disk could fuel sporadic bursts.

The strong Fe $\rm K{\rm\alpha}$ line in the spectrum of 4U 1916-05, which is an UCXB system with an optically confirmed He-rich donor \citep{2006MNRAS.370..255N}
is also  in complete agreement with the theoretical predictions presented in Koliopanos et al.. Furthermore, the system's frequent bursting activity
reinforces the arguments in favor of a He-rich donor.
Perhaps more interestingly, however, our argument in favor of a He-rich donor star in 4U 0614+091 is at odds with
the fact that the system has been classified as C/O rich, based on optical spectroscopy  \citep{2004MNRAS.348L...7N, 2006A&A...450..725W}.
On the other hand, our estimation readily explains the source's repeated bursting activity as reported by \cite{2010A&A...514A..65K} and \cite{2012ApJ...760..133L}
and is in complete agreement with the conclusions reached by these authors.

Nevertheless, the lack of He lines in the optical spectrum of 4U 0614+091 \citep{2004MNRAS.348L...7N, 2006A&A...450..725W} and particularly the
upper limit of 10\% He abundance in the disk material, placed by \citeauthor{2006A&A...450..725W} are strong arguments in favor of a C/O rich donor.
This upper limit is calculated for a disk ${\rm T_{\rm eff}}$ of 28000\,K at a distance of 2000 stellar radii. For this
temperature the dominant ionization stage of helium at $\tau=1$ is He{\small II} \citep[][Figure 6]{2006A&A...450..725W}.
Therefore, according to the \citeauthor{2006A&A...450..725W} model, an accretion disk with a helium abundance of more than 10\%,
would produce stronger He emission lines than the observed upper limits.
However, their model ignores disk illumination and authors acknowledge that
introducing disk irradiation from the NS surface and the comptonizing corona would affect the ionization structure of the disk.
Namely, if ${\rm T_{\rm eff}}$ is high enough, helium could be fully ionized even in the outer parts of the disk. Such a scenario would promptly
reconcile the lack of He-lines in the optical spectrum, the system's bursting activity
and the presence of a strong iron line in the reflection spectrum.

\section{Summary and conclusions}
We searched for the iron ${\rm K\alpha}$ in the spectra of five UCXBs with H-deficient donors.
Based on the non-detection of a Fe line and the predictions of \cite{2013MNRAS.432.1264K},
we have concluded that the accretion disk material of three of the objects in our sample (2S 0918-549, XTE J1807-294 and 4U 0513-40)
has an O/Fe ratio that is at least $\approx$10\,times higher than the solar value. In the context of UCXBs this
suggests a C/O or O/Ne/Mg-rich donor.
Furthermore, the presence of a strong Fe ${\rm K\alpha}$ line in the spectra of the
remaining two systems (4U 0614+091 and 4U 1916-05) indicates a He-rich donor.
In the case of 2S 0918-549 and 4U 1916-05 our findings are also supported by results obtained through optical spectroscopy.
On the other hand, our suggestion of a He-rich donor in 4U 0614+091 contradicts arguments in favor of a C/O-rich donor,
but is consistent with the source's regular bursting activity.

\section*{Acknowledgements}
The authors would like to thank Dr. Mikhail Revnivtsev for crucial comments and valuable advice.
We also thank Pierre Maggi for frequent helpful discussions.
This work was supported by the National Science Foundation under
grants PHY 11-25915 and AST 11-09174.

\bibliographystyle{mn2e}

redpajama_set_name: RedPajamaArXiv


After years of being in prison, I didn't know what to expect at Dismas House. I was scared of failing there: I've had no day to day responsibilities for a long time. But, I have one responsibility that is with me for life: my beautiful daughter Ashley.
In prison, I learned to be very cautious, and aware of my surroundings. I also become a little judgmental. When I was told that Dismas had a way that my daughter could come to visit, my reaction was "no way". I couldn't imagine any situation there that I would want her exposed to "in that kind of environment".
Well, when I got to Dismas, I found things were different than I had imagined. They made me feel as much as possible that this was my home. The people here are people just like me, who want someone to give them a chance.
And I felt comfortable when I found out what I had to do to have my daughter visit. At first, there is a lot of paperwork, and discussions with Parole and Probation, her mother, Dismas, and me.
I think Ashley was uncomfortable at first, but everyone was so good to her that she enjoys coming here now. She comes here twice a week now, every week. She really likes sitting down at the table with us and eating dinner like a family.
I'm really glad I gave Dismas a chance because it has brought my family and me together. Being with my daughter is the best possible situation for us both. I'm very grateful to the Dismas community for ensuring that my child and I can spend time together each week. It means more than you know.


This is a placeholder page for Dallas Kowalski, which means this person is not currently on this site. We do suggest using the tools below to find Dallas Kowalski.
You are visiting the placeholder page for Dallas Kowalski. This page is here because someone used our placeholder utility to look for Dallas Kowalski. We created this page automatically in hopes Dallas Kowalski would find it. If you are not Dallas Kowalski, but are an alumni of East Jordan High School, register on this site for free now.


text:
Nearly 10 pct of American adults with a record of angry behavior have access to guns: study
WASHINGTON Apr 08, 2015 - 12:00 am GMT+3
| AP Photo
by French Press Agency - AFP Apr 08, 2015 12:00 am
Around nine percent of American adults who have a record of impulsive and angry behavior have access to guns, says a study out Wednesday.
These researchers also reported that 1.5 percent of adults acknowledge feeling impulsive anger and carrying guns outside their home.
These people are usually young or middle aged men who sometimes lose their temper, break things or get into fights, said the study, co-authored by psychiatrists at Duke, Harvard and Columbia universities.
The study was published in the journal Behavioral Sciences and the Law.
"As we try to balance constitutional rights and public safety regarding people with mental illness, the traditional legal approach has been to prohibit firearms from involuntarily-committed psychiatric patients," said Jeffrey Swanson, a professor in psychiatry and behavioral sciences at Duke University in North Carolina and lead author of the study.
"But now we have more evidence that current laws don't necessarily keep firearms out of the hands of a lot of potentially dangerous individuals," he wrote.
The researchers looked at data from 5,563 face-to-face interviews conducted in the National Comorbidity Study Replication, or NCS-R. This is a nationally representative survey of mental disorders in America that was led by Harvard University in the early 2000s.
The study concluded there was little overlap between participants with serious mental illnesses and those with a history of impulsive, angry behavior and access to firearms.
The researchers found that anger-prone people with guns were at higher risk for a range of fairly common psychiatric conditions such as personality disorders, alcohol abuse, anxiety and post-traumatic stress. But only a very small fraction suffered from acute symptoms of major disorders such as schizophrenia.
"Very few people in this concerning group suffer from the kinds of disorders that often lead to involuntary commitment and which would legally prohibit them from buying a gun," said Ronald Kessler, a professor of health care policy at Harvard and principal investigator of the NCS-R survey.
He and other co-authors argued that a more effective way to prevent gun violence would be to examine a prospective gun buyer's record of misdemeanor convictions, including violent offenses and multiple convictions for impaired driving, rather than screening based on mental health treatment history.
In 2012, a total of 11,622 people were killed by firearms in the United States, according to federal statistics.
Muslims around the world celebrate Ramadan Bayram


Tesco's finance boss Laurie McIlwee is reportedly due to leave the business as soon as next week, with profits expected to fall again.
Tesco is expected to announce another sharp decline in profits next week when it reports its 2013-14 results on April 16, the Financial Times reported, and the pressure is mounting on the grocer to improve its performance in the UK and Europe.
McIlwee is also reported to have disagreed with chief executive Philip Clarke over some areas of strategy.
McIlwee attracted negative attention from investors in October when Tesco surprised the markets with a fall in profits in its central European operations, which the finance chief had not flagged.
Tesco FD Laurie McIlwee: "Market contracted more than we anticipated in December"
Tesco chief financial officer Laurie McIlwee said the grocer was "too optimistic" at the beginning of December and the market contracted more than it thought over the key Christmas trading period, leading to "disappointing" results.


Roast chicken and pork sage & onion stuffing with seasoned mayonnaise on malted bread. Chicken and seasoned mayonnaise with tomato, cos lettuce and cucumber on malted bread. Chicken breast and smoke flavoured bacon with seasoned mayonnaise on malted bread.
Malted Bread (Wheat Flour (fortified with calcium carbonate, iron, niacin and thiamin), Water, Malted Wheat Flakes, Wheat Bran, Wheat Gluten, Yeast, Salt, Muscovado Sugar, Spirit Vinegar, Barley Malt Flour, Emulsifiers: E471, E472(e), E481, Palm Oil, Rapeseed Oil), Chicken (15%) (Chicken Breast, Water, Salt), Seasoned Mayonnaise (11%) (Water, Rapeseed Oil, Pasteurised Egg Yolk, Cornflour, Spirit Vinegar, Sugar, Dijon Mustard (Water, Mustard Seeds, Spirit Vinegar, Salt), White Wine Vinegar, Salt, Black Pepper), Roast Chicken (9%) (Chicken Breast, Water, Salt, Brown Sugar), Pork Sage & Onion Stuffing (6%) (Water, Pork, Bread Crumbs (Wheat Flour (fortified with calcium carbonate, iron, niacin and thiamin), Yeast, Salt), Onion, Rusk (Wheat Flour (fortified with calcium carbonate, iron, niacin and thiamin), Salt, Water), Rolled Oats, Seasoning (Salt, Wheat Flour (fortified with calcium carbonate, iron, niacin and thiamin), Dextrose, Pepper, Sage, Parsley), Pork Back Fat, Sage, Parsley), Smoke Flavoured Bacon (6%) (Pork Belly, Water, Salt, Sugar, Emulsifier: E451(i), Smoke Flavouring, Preservative: E250), Tomato (2%), Blended Spread (Palm Oil, Rapeseed Oil, Water, Butter (Milk), Buttermilk (Milk) Powder, Salt, Emulsifier: E322, Colour: E160(a)), Cucumber, Lettuce, Red Onion.