Criminal Profiling vs Racial Profiling

Criminal Profiling versus Racial Profiling Racial profiling is a social issue that has emitted all through the nation. Numerous areas, urban areas, social gatherings, and scholastics have contemplated racial profiling and how race and ethnicity may have an influence in police examinations. Charges of racial profiling have been around for a considerable length of time, and still is a subject that makes a great deal on media promotion and debate encompassing police and their collaboration with minorities. In Toronto, there have been various paper and TV articles blaming the Toronto Police Service for methodical bigotry (Canadian Race Relations Foundations, 2005). Racial profiling ought not be mistaken for criminal profiling, since they are two distinct things (Mucchetti, 2006, pp. 1-32). Racial profiling isn't explicit to one race or one nation. As a matter of fact being racially profiled can transpire whenever regardless of what race or sex or nation they live in. This paper will analyze racial profiling and criminal profiling by police and clarifying how the distinctive sociological viewpoints; functionalist, strife, interactionist, and women's activist points of view see it. The paper will likewise endeavor to contend if there is orderly racial profiling by the Toronto Police. My postulation is the Toronto Police doesn't methodicallly racially profile, rather they deliberately criminally profile. So as to analyze racial profiling and criminally profiling one must comprehend the contrasts between the two. In spite of the fact that there is no reasonable or all inclusive meaning of racial profiling, there is a typical part in the entirety of the definitions (Ontario Human Rights Commission, 2009). This paper characterizes racial profiling as the act of focusing on racial minorities for criminal examination exclusively or, to some degree, based on their skin shading (Court of Appeal for Ontario, 1999). As indicated by the Harvard Latino Law Review, criminal profiling includes: The utilization of racial or ethnic qualities by police divisions in halting an individual since their depiction coordinates that of a real suspect. In this sense, race capacities as what could be compared to hair shading or stature, which would then be able to be utilized in mix with different variables to paint an increasingly precise picture of a speculated criminal. Accordingly, summed up thoughts of criminal affinity are not anticipated onto an individual on account of that people enrollment in a specific racial or ethnic gathering (Mucchetti, 2006, pp. 1-32). The term racial profiling started during the 1980s, when the Drug Enforcement Agency (DEA) in the United States created and utilized basic attributes to profile sedate messengers as a major aspect of the offices war on drugs (Harris, 2006, pp. 213-239). At the point when network individuals started to gripe about police examinations and their activities towards minorities the employments of the profiling strategy developed to be named as racial profiling (Ibid). Functionalist, strife, interactionist, and women's activist viewpoints all accept racial profiling is one of separation, weight and control of subordinate gatherings with the goal that the prevailing gathering can practice their social class, race, and sexual predominance over others (Banks, Eberhardt, Ross, 2006, pp. 1169-1190). Preference in racial profiling is brought about by mental and socially built impacts, where people are affected by their environmental factors to despise another gravely dependent on their race (Guimond, Dambrun, Michinov, Duarte, 2003, pp. 697-721). The functionalist viewpoint accepts society is separated into two gatherings, the prevailing and subordinate. What's more, that these gatherings are a characteristic piece of society (Kendall, Nygaard, Thompson, 2011). Functionalist likewise accept society isn't adjusted regarding race, since it is normal for one gathering of individuals to be better over the other and that racial fairness will lessen the command bunch power on subordinate gathering (Kimberle Williams Crenshaw, 1988, pp. 1331-1387). In this way, functionalist see racial profiling as being framed by overwhelm gatherings to make the subordinate gatherings feel substandard, so they can have their own jobs in the public arena since it is the means by which society expected it to be. Strife point of view accept that all gatherings in the public arena are occupied with a persistent force battle in light of the fact that the predominant gatherings who have social, political and conservative force, battle to keep up their advantaged position over the subordinate gatherings (Kendall, Nygaard, Thompson, 2011). Strife scholars likewise accept everybody is equivalent, in spite of their race, sex or business, restricted to the functionalist hypothesis (Ibid). They additionally accept racialized and ethnic imbalance is caused because of financial definition (Ibid). The overwhelm bunch figures out what laws ought to be implemented and what punishments are to be managed. They additionally figure out what subordinate gathering will be focused on, captured and rebuffed unjustifiably so as to keep up their situations in an entrepreneur society. The police are utilized as an instrument by the command gathering to keep up their situation in the public eye. Racial profiling by po lice is just one of the techniques utilized by police to implement the standards of the rule class. Representative interactionist point of view can be utilized to clarify officials conduct which is situated in social brain science (Kendall, Nygaard, Thompson, 2011). The social elements including the cooperation among official and resident may impact officials conduct and cause them to racially profile. The interactionist approach stresses how racialized socialization adds to sentiments of solidarity with ones own racialized or ethnic gathering and antagonistic vibe towards others (Ibid) which could make residents challenge officials authority on the off chance that they felt their characters were being tested, their common freedoms were being limited, or the official was acting in an impolite conduct. Albeit emblematic interactionist point of view doesn't legitimately clarify why police at first stop minorities, it clarifies the social communication between the official and resident and how it could bring about the resident sentiment of being racially profiled if the officials asso ciation was proficient. Women's activist point of view depends on basic clash viewpoint (Kendall, Nygaard, Thompson, 2011). A women's activist view on racial profiling is about sexual orientation and race contrasts, and the confinements related with conventional male-predominance in the public eye. There is nobody women's activist point of view that can clarify a social issue, for example, racial profiling since all are speculations of mistreatment, contrasts, and disparity (Ibid). Social extremist gatherings alongside minority bunches cases of efficient racial profiling by the Toronto Police Service exists and allude to distributed articles to help their cases, for example, the 2002 arrangement of paper articles composed by the Toronto Star, and the absence of racial measurements aggregated by the Toronto Police Service. In these articles, the Toronto Star articles utilized experimental information gathered from the Toronto Police Services Criminal Information Processing System (CIPS) database. As per the paper articles that inspected 480,000 documents contained inside the database, identifying with capture and traffic stops, guarantee Blacks captured by Toronto Police are dealt with more brutally than white, and an unbalanced number of dark drivers are tagged for infringement that lone surface after a traffic stop. As per common libertarians, network pioneers and criminologists, the distinction could propose that police utilize racial profiling in concluding whom to pull over (Toronto Star Newspaper, 2009, p. A01). Social and minority bunches likewise bolster their cases of precise racial profiling by the Toronto Police Service, as the Service doesn't gather or discharge race base insights. They contend One feelings of trepidation that the main explanation the Police Board will not discharge this information is to guarantee that general society doesn't get refreshed data on racial profiling (Toronto Police Accountability Coalition, 2008). This paper yields that racial profiling may exist on an individual premise (small scale level) inside the Toronto Police Service. This was affirmed by Chief Blair of the Toronto Police Service who was talking a decent variety meeting and stated: Racism is a human fizzling. Racial profiling can happen. Weve recognized that front and center (Doolittle, 2009). As a cop, clearly there are mistakes in the Toronto Stars ends. The Toronto Star assembled its information utilizing the documents contained in the CIPS database, which just contained records identifying with capture and tickets gave to people. The issue utilizing just this database is that it doesn't consider the quantity of individuals the police really research where there were no capture or tickets gave, or the way that the CIPS framework prohibits data on section 1 Provincial Offenses tickets; for example safety belt, speeding and so forth as it just incorporates section 3 Provincial offences tickets (progressively genuine offences). By just choosing the CIPS database and not the genuine number of people halted by police slanted the conclusive outcomes. Teacher Edward B. Harvey, a PhD, from the University of Toronto affirmed this reality that the Toronto Police database, which was not intended for research purposes, contains such a large number of blemishes that its uses in rese arch is constrained (Harvey, 2003). The information assortment by the Toronto Star was additionally contested by Allan Gold dependent on the qualification among receptive and proactive policing (2003, pp. 391-399). Gold contends receptive policing could ascribe to cases of racial profiling while proactive policing won't. With regards to the assortment of information, the Toronto Start utilizes the two styles of policing which defective their decision (Ibid). It is very notable that any and each technique in the sociologies is available to analysis and assault (May, 2001). Max Weber a spearheading humanist and social specialist focuses on the significance of appropriate technique in social examination in looking at any s

Siren Song

In â€Å"Homer’s Odyssey† and â€Å"Siren Song† both show the shortcomings of individuals. Additionally it uncovers people discover something so alluring that they are unequipped for withstanding it. In â€Å"Homer’s Odyssey† Homer makes a dream that the alarms are perilous animals, not at all like Atwood’s sonnet, â€Å"Siren Song. † Atwood’s sonnet anyway shows a distress originating from the alarms. In â€Å"Homer’s Odyssey† the sonnet is told from Odysseus perspective. He depicts the Sirens as puzzling and luring.Circes prompts Odysseus that the Sirens â€Å"spellbind any man alive, whoever comes their direction. † Gaining this information, Odysseus made his mariners plug their ears with beeswax so they would abstain from hearing the exciting melodies of the Sirens. Odysseus was resolved to hear the excellent melodies of the Sirens, despite the fact that he knew about the outcomes. This uncovers keeps an eye on narrow-mindedness by having Odysseus take the necessary steps to hear the melody. Odysseus arranges his men to secure him on the pole to guarantee his survival.Odysseus hears the Siren's tune and begins to respond to it, his men â€Å"flung themselves to the oars† and â€Å"sprung up on the double to tie him quicker with ropes. † This shows how impelling the alarms were to men. In â€Å"Homer’s Odyssey† a man’s keen is appeared, and depicts how enticement will consistently be a piece of life. Not at all like â€Å"Homer’s Odyssey†, Atwood’s sonnet â€Å"Siren Song† is told from the Sirens perspective. The alarms are depicted as overpowering animals that cause men to totally lose all self control.One of the Sirens states â€Å"I don’t appreciate it here,† in â€Å"Homer’s Odyssey† all the alarms appear to be attached to singing their outstanding melodies. In Atwood’s sonnet a Sir en is asking for help; â€Å"Help me, no one but you can. † Unfortunately nobody can help on the grounds that once the music of the Sirens contacts the ear; they capitulate to the intensity of the Sirens. The Sirens have a specific edginess to be liberated from their disagreeable life on the island. â€Å"Will you get me out of this winged animal suit? † shows that the Sirens in Atwood’s sonnet have personalities, inverse of â€Å"Homer’s Odyssey†.There is no data in The Odyssey that surmises that the alarms have a character. In the two sonnets the Sirens voices demonstrate a compelling draw to men. The reasons that the Sirens sings contrast from every sonnet. In† Homer’s Odyssey,† Odysseus feels like they are focusing on him, anyway in Atwood’s sonnet the Sirens are basically singing for themselves. The Sirens appear to be sympatric to the men who bounce over the edge, yet unfit to prevent themselves from calling the men to their island.The sonnets â€Å"Homer’s Odyssey† and â€Å"Siren Song† have numerous similitudes in how the Sirens are depicted and yet they vary in a wide range of parts of the sonnets. The â€Å"Sirens Song† Sirens utilize the men’s own common interest to carry the men to them. The â€Å"Odyssey† Sirens use charm and the guarantee of energy to get the men to come. In any case, the Sirens uncover how precarious and shrewd they are with their otherworldly melodies. In any case, the Sirens could simply be attempting to torment men for their own diversion or they could be attempting to connect for help.

Video case report Essay Example | Topics and Well Written Essays - 1000 words

Video case report - Essay Example Anyway on this day, to everyone’s awe, calls, messages and letters began flooding in, with each client communicating disappointment on different regions, for example, item disappointments, administration conveyance, the speed of the reaction and consideration offered to the clients towards their objections. The outcomes were definitely influencing each division inside the firm, for example, decrease on the business, disturbance on our creation and excusal of different specialists. To give a perpetual arrangement, the firm needed to place different factors in to account by spreading out vital measures to control that event regularly rehashing itself. As per (Meredith 2010), a client makes the business run and there is no specific firm that can pursue away clients eagerly; however the straightforward mix-ups that different firms ordinarily make, might be acts that bring about pursuing ceaselessly clients in camouflage. In each firm the same number of agents consistently put it, the â€Å"customer is the king† however perhaps this is the thing that our firm didn’t set up or didn’t have set up. ... As indicated by (Zairi 2000), â€Å"Customers are the fundamental reason for running a firm, in addition to as opposed to them contingent upon the firm, the firm relies upon them†. This demonstrates the significance of a delicate connection between the firm and the clients. For (Hansemark and Albinsson 2004), they characterized fulfillment as â€Å"overall client disposition towards a specialist co-op or the enthusiastic response on what clients envision according to what they get on their ideal needs†. As per (Anderson 2000), client devotion is really the aftereffect of an association making an air helpful for clients turning out to be rehash customers with the goal that they can keep up or increment deals. Client steadfastness must be accomplished by giving and conveying what the clients want and anticipate. Likewise (Oliver 1997), named client unwaveringness as that profound responsibility to re-buy a specific favored item or administration reliably later on regardle ss of changes or impacts with plausibility of causing an adjustment in the promoting conduct. Hokanson {1995), clarifies different elements that influence the degree of consumer loyalty. This incorporates: employees’ information on the item, cordiality, respectful and accommodating staff, serious evaluating, great estimation of the item, charging clearness, practicality and exactness and fast assistance conveyance. The most influenced region as portrayed in our firm by the disappointment of the clients was on the productivity. As per (Hoyer 2001), fulfilled clients give the establishment of each fruitful business association as it prompts rehash buys and reliability on the brands enhanced by a positive informal. As per different researchers’, disappointment of clients prompts

A Sub-Subtle College Essay

<h1>A Sub-Subtle College Essay</h1><p>A shallow school paper is one that is expected to quantify an understudy's capacity recorded as a hard copy instead of requesting that an individual build a significant book. At the point when progressed nicely, a shallow exposition can fill in as a keen investigation of the subtext of a theme, accordingly permitting a person to reveal their own remarkable thoughts and comprehension of the subject matter.</p><p></p><p>When composing a shallow school article, there are numerous things to mull over, for example, when it will be utilized, where it will be distributed, the length of the paper, and even who will understand it. It's critical to consider the individual who will peruse your work, regardless of whether they are a business, regardless of whether they are taking the class for individual, and regardless of whether they will be the one evaluating it.</p><p></p><p>First, we shou ld understand that you won't be allowed the chance to talk about all the potential points before an underlying judgment has been made on the piece. There are numerous ways that a shallow exposition can be composed, and it would be dependent upon you to choose which of these thoughts will best serve your requirements. In the event that you are uncertain of your own considerations regarding the matter, don't hesitate to think carefully, and investigate any way that will permit you to communicate your thoughts.</p><p></p><p>For model, if you somehow happened to compose an article on Asperger's Syndrome for a college class that was occurring in June, an assessment of your composing style would be hard to have right now. By and large, an assessment of a solitary page of composing could take a while. If you somehow happened to finish this activity before the beginning of the semester, it would be increasingly helpful to have a strong structure with the main page of the exposition saying the general thought, trailed by a presentation and a conclusion.</p><p></p><p>Since so much can change through the span of a semester, this procedure of composing a first draft of the article is only the start. There are numerous potential points that could be examined, numerous potential inquiries that could be posed, and even various strategies for composing which can truly assist with making your last item outstanding.</p><p></p><p>Remember that you may at present have a lot of inquiries in regards to the material and hence it is enthusiastically suggested that the primary draft of the article to be caught up with ensuing drafts. By having the chance to talk with individuals inside the class, it is likewise prescribed that you have the chance to pose inquiries, this assists with ensuring that your paper has been arranged and furnishes you with the opportunity to address botches that may have been made during t he first draft.</p><p></p><p>An person's school exposition won't be acknowledged without a decent establishment, accordingly your initial step ought to be to accumulate data so as to build up the best method to build up a firm establishment for your content. When the right data has been accumulated, you can start building up your underlying draft, from that point you can start utilizing your thinking capacities to build up your content and make your own one of a kind masterpiece.</p>

Just Mercy Essay Samples

<h1>Just Mercy Essay Samples</h1><p>Why have such a significant number of individuals been composing just benevolence and other comparable kindness terms in their fair leniency paper? A typical explanation is on the grounds that the data isn't anything but difficult to track down. Particularly the presentation or 'source of inspiration' ought to be similarly as simple to access as the proposition explanation or end. Above all, however, it ought to be as short as conceivable to shield from stalling the progression of the essay.</p><p></p><p>Another reason individuals are finding these terms in only a basic structure is a direct result of the unpredictability of that specific point. Numerous individuals might be hindered by the subject, yet be not able to discover data about just benevolence. Then again, the individuals who are sufficiently sure to compose the paper will need it to be concise.</p><p></p><p>Writing the pr esentation of your exposition is just the initial step. You likewise need to realize where to discover just benevolence and other such terms. There are various spots online that give just benevolence paper tests. Coming up next is a rundown of the spots where you can discover such article samples.</p><p></p><p>Willowtree.com. This site is a basic and compelling asset for pretty much any kind of composing. Simply take a gander at its models for tests on just kindness, Christian just leniency, and different themes. There are articles on only 'kindness' just as different terms you will be writing.</p><p></p><p>WriteInJustMercy.com. This site is for authors who need to find out about just kindness. The website incorporates an inquiry and answer highlight where the author can pose inquiries about only leniency, just as other such terms.</p><p></p><p>Just Mercy Blog. Composing a fair leniency article includes a great deal of examination. This blog, however, might be useful to the individuals who don't wish to visit a few sites so as to realize exactly writing just leniency. It has various articles on only 'benevolence' with connections to different sites to get more information.</p><p></p><p>Just Mercy Radio. This online radio show has essayists of numerous kinds who are prepared to share exactly what they think about just benevolence. They likewise at times give just 'kindness' citations to the network. Guests to the website can likewise follow the visitor's web journals or take an interest in gathering discussions.</p><p></p><p>Justmercy.org. This site is like Willowtree.com, however it additionally gives test expositions. These examples are appropriate for perusers who are new to simply 'benevolence' terms and who need to become familiar with just mercy.</p>

Why Are Cause-Related Essays Such A Tough Sell?

<h1>Why Are Cause-Related Essays Such A Tough Sell?</h1><p>Have you at any point asked why causation articles will in general have such an extreme time getting acknowledged by far most of schools? The truth of the matter is that understudies invest most of their energy perusing and reading for their general school or college selection test, which is commonly the SAT or the ACT. On the off chance that you are taking a shot at a theory or some sort of article and you have to get into a school to do as such, your most logical option is to go with the least demanding subject that you can work with.</p><p></p><p>Causation composing is perhaps the simplest theme to work with. It is simple enough for understudies to see, however it is additionally pertinent. This implies, in the event that you accomplish something like propose that somebody had an impact on their parent's separation, odds are that you won't burn through much time chipping away at yo ur paper, since individuals will as of now have the option to comprehend what you are attempting to convey.</p><p></p><p>Another motivation behind why causality papers neglect to get acknowledged is that there is no genuine reason. There is no genuine direct reason, but instead various components that added to the activities of an individual that lead to a specific outcome. For instance, an individual may get fixated on a specific measure of chocolate in their life, and this will likely prompt changes in their dietary patterns that make them increasingly inclined to overeat.</p><p></p><p>As a self evident reality, causality article subjects are probably the hardest thing to compose. They are commonly exceptionally subject to the peruser, in light of the fact that they depend on close to home translation, and they regularly depend on various kinds of information to fit into a specific example. This regularly implies understudies need to look at a wide assortment of thoughts, so as to show up at a conclusion.</p><p></p><p>So, understudies frequently wind up examining a few things, before going to a last answer. This can frequently make contentions emerge, particularly when another understudy says that the examination of the information utilized for the situation was broken, or that the subject was never a primary concern of the case by any means. In such cases, understudies will wind up returning their contention to the educator and ask for clarification.</p><p></p><p>Causation papers likewise make some hard memories getting acknowledged in light of the fact that understudies have an exceptionally troublesome time getting a handle on the legitimacy of the information used to build up the case. Their own relationship with the other two gatherings can regularly assume a huge job in whether they accept that their motivation has any legitimacy, and commonly, the translati on of the information is very arbitrary.</p><p></p><p>In different words, causation points are frequently hard for understudies to comprehend, just as they are hard to decipher. To exacerbate the situation, they additionally will in general be difficult to get acknowledged, as understudies are not constantly effective in aiding themselves.</p>

The New Angle On Term Paper Writers Just Released

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The History of Term Essay Papers Research Paper Teenage Pregnancy Refuted

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Writing a Persuasive Essay for 7th Graders

Writing a Persuasive Essay for 7th GradersTo write a persuasive essay for 7th graders is to write an essay that makes you different. It is not a simple task. If you would like to succeed, you will need to work on your essay writing skills before hand and learn how to create the right scene in your essay.A persuasive essay must provide the reader with some of the most powerful reasons for understanding and agreeing with your point of view. You must be able to use your full argumentative capacity to force your ideas to the top of the student's mind. As a writer, it is important to practice your persuasive writing skills as much as possible. There are many ways to improve your ability to persuade your readers. Here are some good persuasive essay topics for 7th graders.A long essay is boring. Sometimes, you need to have a short answer that is easy to remember. It is best to make it short and simple, but if you do have a lengthy topic, do not do the whole thing in one sentence. Sometimes, it is easier to create a simple sentence, say, 'Sugar's pizza has amazing pepperoni.'An effective persuasive essay for 7th graders should contain two basic parts. The first part should be full of arguments. The second part should be simple and easy to remember. For example, you could begin your second part by saying something like, 'Just because you believe this doesn't mean you have to act on it.' The reason why you want to tell the reader these two sentences is so they can easily follow your ideas and you do not have to re-invent the wheel each time you try to persuade them.A persuasive essay for 7th graders must also address an important issue or argument. In your opinion, what would be the best way to solve the problem of homelessness? A persuasive essay for 7th graders should never address the problem of homelessness in the abstract. You must provide the reader with examples of how homeless people have been helped by their circumstances, but this does not mean that you are adv ocating for the solution.A persuasive essay for 7th graders must address all sides of the issue. You do not want to provide an opinion. Readers do not want to read an opinion in a persuasive essay. They want to be convinced that you are making a case for one side or the other.In conclusion, it is important to think about all the issues that you would like to discuss in a persuasive essay for 7th graders. If you know what the problem is, then you will have more ideas to think about. When you have enough ideas, it is important to write the essay. Practice makes perfect!

Variable Star XX Andromeda - Free Essay Example

A Study on the Variable Star XX Andromeda Abstract We present the results of a month long V-Band study on the RRab type variable star XX Andromeda. 4526 data points are used to plot a light curve, with 3 maxima observed and added to data from the GEOS database to create an O-C diagram. Three methods of estimating the pulsation period are used, including two Phase Dispersion Minimisation methods and an O-C method, resulting in a best estimate of the period of days. This value is in excellent agreement with the literature values for the period of XX And, from both the Hipparcos catalogue and the GCVS. The distance to XX And is estimated to be pc using a main sequence fitting method to estimate the absolute magnitude, and the mean radius is estimated to be . A flatfielding improvement to the photom.py pipeline is suggested to combat dust artefacts on the CCD. Physical reasons are discussed for the distinctive features present in the light curve, namely the Hump and the Bump. I. Introduction In 1893 Solon I Bailey started a program of globular cluster study[i]. He noticed that some clusters (e.g Centuri) were extremely rich in variable stars with similar properties they had periods of less than a day, and light curve amplitudes of around 1 mag. The mean value of apparent magnitude of these stars in a particular cluster was also approximately the same across the sky. Bailey named these Cluster Type Variables. However an increasing number of stars with these properties were being found outside of clusters indeed the brightest star of this type ever found was a field variable, RR Lyrae (after which the class is now named). Discoveries then began to come thick and fast, and it is currently estimated that over 85000 exist in the Milky Way alonei. RR Lyrae variables have also been observed in the Andromeda Galaxy, the Large Magellanic Cloud and other Local Group dwarf galaxies[ii]. Measuring the properties of these variables has become increasingly important to astronomers, as it was realised that they could be used to gauge astronomical distances through a period-luminosity (P-L) relation, in a similar way to Cepheids. Various catalogues have studied their properties, for example the General Catalogue of Variable Stars[iii] or the more recent Hipparchos Catalogue[iv]. Until recently however, no distinct P-L relation had been found, and instead astronomers had to use a relation between metallicity and visual magnitude or the Baade-Wesselink method, the drawbacks of which are discussed later. Currently there is still no P-L relation for V-band observations, although there are now relations for most of the infrared spectral bands[v]. RR Lyrae variables are also of importance for the study of the population of both the Galactic Bulge (via Baades Window for example) and the Galactic Halo. Their advanced age and low metallicity combined with distinctive pulsation properties provides an excellent tracer for the development of the Milky Way in its early stages, as well as current kinematic analysis[vi]. They have also been used as a means of quantifying the interstellar reddening caused by dust in the galactic plane, thanks to the fact that the colour excess is a function of minimum (V-I) colour only[vii]. Using this reddening data with other distance indicators (for example red clump stars in the bulge[viii]), a meaningful approximation of the distance to the centre of the bulge can be obtained. Clearly then the study of RR Lyrae variables is useful for the understanding of the evolution of both the Milky Way and the rest of the Local Group. The star to be observed in this study is XX Andromeda (abbr. XX And), an F2 spectral class RRab type variable, located in the constellation of Andromeda at RA: 1h 17m 27.4145s, Dec: +3857 02.026 (see 1). Its moderately high position in the sky at Durham means that it is circumpolar, whilst not exceeding the +65 limit for the telescope fork mount, resulting in minimal atmospheric interference and the maximum possible observing time. The GCVS lists a period of. It is also known to exhibit the Blazhko effect, a long-period modulation of the amplitude of an RR Lyrae star (the cause of which is currently under investigation), with a period ofiii, and has an [Fe/H] value of -1.94. II. Theory Observational Theory CCD Theory Perhaps the most important advance in astronomy in the last 20 years has been the widespread use of Charge-Coupled Devices (CCDs) to replace photographic plates. Invented in 1969 at Bell Labs by Boyle and Smith, CCDs are a thin piece of semiconductor material (e.g. silicon) upon which lies an grid-like array of metal-oxide semiconductor (MOS) capacitors[x]. During an exposure, if a photon impacts on the silicon an electron/hole pair can be produced, as an electron is pushed up into a higher energy state. The MOS capacitors act as deep potential wells (pixels), which hold the electrons until the exposure is finished. The charge is then read-out to an amplifier at one edge, in a specific order so that that the position of the original pixel can be identified, and related to the magnitude of the detected charge. The charge is converted from a raw number of electrons into ADUs (analogue to digital units), the conversion factor of which is the gain of the CCD[xi]. They are preferred to photographic plates in modern astronomical photometry for several reasons: * High quantum efficiency (QE) for each incident photon there is upwards of 90% certainty[1] that an pair will be produced. On the other hand, with photographic plates one can achieve (at best) an efficiency of 3%[xii], so using CCDs will increase the likelihood of detection of distant objects. * Large dynamic range, allowing them to detect objects with a range of magnitudes in the sky in the same exposure. * Strong linearity up to the saturation point, so that for longer exposure times the number of electrons produced is proportional to the integration time, whereas photographic plates will experience a drop in their efficiency. Their linearity will also mean that the magnitude of charge in each pixel is linearly proportional to the luminosity of the object. CCDs have also brought some inherent problems however, for example the noise associated with each image. Because photons obey Gaussian statistics for large counts, there will be a shot noise (uncertainty in the count rate) for each pixel of whereis the number of photons detected. Error in an image also stems from both the bias of the CCD, and the dark current present. The bias of a CCD is a systematic voltage offset across the whole CCD to prevent digital underflow during analogue to digital (A-D) conversion. It includes the read-out noise, a result of the manipulation of the pixel charge values during the A-D process and any charge-loss which occurs during the transfer[xiii]. A CCDs dark current is an unwanted flow of electrons which have been released from the surface of the semiconductor by thermal excitation, and is purely dependant on the surface temperature, rather than being a function of illumination. For this reason the CCD was cooled by both the Peltier method (electrically ) and with an active assisting fan[xiv], to around 35C below ambient temperature, as the thermal current is approximately halved for each 7C reduction in CCD temperaturexii. To remove noise from an image, a set of calibration images may be taken alongside each raw exposure. These are called bias and dark frames. The bias frame is a zero-time exposure which will include both bias and read-out noise. A dark frame can be found by leaving the shutter on the camera closed and taking an exposure seconds long. It can be expressed as , [xv](2) whereis the dark current, andis the thermal noises statistical variation. Ideally one would be taken before each exposure, as temperature routinely varies slightly with time. A master dark frame can be found by taking the average of a large number of dark frames, and will include the equivalent of a master bias. This master dark can then be subtracted from each image to leave a final, processed image with as low a random error as possible. The Automated Photometry Process Since the experiment involved a large number of images, the photometry processes were automated using several Python scripts and FORTRAN routines. The script all.py was used to iterate the photom.py script over a range of images within a directory and print a string detailing which file was currently being processed. photom.py was the main script run, and was used to call several other processes which ran the photometry calculations, among other things. Firstly, it read in the file specified, and split the filename into the file and the extension, by using the find function to search for the full stop as the delimiter. i=file_name.find(.) Using the extension to determine the file type, the script then either subtracted the master_dark.sdf frame (if it was a FITS file, and hence a DRACO output file) or converted it to a FITS file (if it was an ST9 file, and hence 14-inch, which had already had the dark frame removed). The conversion is achieved using two separate routines: sbig2ndf, a routine from the SBIG python module which converts compressed output ST9 files created in CCDOPS into NDF files, and ndf2fits, which is a routine from the convert set of variables that converts the NDF files to FITS images. The subtraction of the dark frame is made using the kappa package from Starlink. photom.py then reads the variable star position from a user-created var_sky_position file. Using this, the script runs find_astrom.py. This attempts to match the stars in the image to the USNOA2 catalogue, and produce a new FITS file with the derived header solution. Firstly it takes the given star position as the centre of the image, and runs sextractor to find all the objects in the image. Next, it runs the WCS Tools routine scat at that RA and Dec to attempt to find any known objects in the region from the catalogue and prints it to a new file, usnoa_ref.cat: commands.getoutput(scat+ -d -c ua2 -n 200 -m 17 r 600 +ra+ +dec+ j2000 usnoa_ref.cat) The pixel scale is taken from the directorys automag_driver file, and used by Andrew Pickles starfit script to match each object found by sextractor to the catalogues objects. This is achieved by the matching of triangles created between sets of objects in the sky to similar triangles created from the catalogues objects. Starlinks astrom routine is then used to correct the solution: out=commands.getoutput(/star/bin/astrom fits=asc) print astrom returns:, out Finally, find_astrom.py edits the header keys using pyfits to reflect the newly derived solution, and creates a new FITS image with the file ending _ast.fits. photom.py then runs sextractor again, to product a new catalogue of the objects from the image, complete with their RA and Dec. The script then performs the aperture photometry using automag.py. This measures the relative aperture magnitudes for the objects defined in the new object catalogue, by taking the number of counts within the specified aperture radius from the driver, and applying the formula: (3) Here is a constant offset defined in the driver, is the number of counts within the aperture (which is pixels in size) minus the background, and is the integration time. Background errors are calculated by measuring the counts within the two sky aperture radii to find the mean and rms sky-counts over pixels,and, and firstly deriving the signal to noise ratio for the star, by applying Equation (4) below[xvi]. (4) In the above equation, is the gain of the CCD. By using the flux based definition of the magnitude difference and manipulating the logarithm equation, the signal to noise value can be used to find the error on a measured magnitude, as shown in Equation (5). (5) These instrumental magnitudes are appended to the catalogue file, next to each object. auto_mag2list.py is subsequently run to pull the calibration stars from the catalogue, by matching the RA and Dec to those in the cal_sky_positions. The variable stars data, as well as the calibration stars data and the observation time in Modified Julian Days (MJD) are then appended to a file called summary.obs. Once photom.py completes, the raw2dif routine can then be run to perform the differential magnitude calculation. This routine takes each line from the summary.obs file and subtracts the average of the two comparison stars instrumental magnitudes from the variable stars instrumental magnitude, . A zero-point constant is then added to put the differential magnitude on the standard scale. This can be measured by taking images of photometric standard stars (from the Tycho catalogue for example), and comparing their instrumental magnitudes to their known apparent magnitudes, as described in the next section. (6) raw2dif outputs simply the observation time, variable stars standardised magnitude, and the error on the magnitude to a user-defined file. Magnitude Zero-point Measurement The zero-point is found by measuring the magnitudes of photometric stars with the telescopes, and comparing these to the values found for the stars in the Tycho catalogue. This catalogue uses a separate magnitude system, which can be converted into standard V-band magnitudes using the following formula: (7) The difference in these catalogue magnitudes and the observed values can then be used to show the difference that the specific equipment has made. This is the zero-point magnitude. Period Determination Two programs are used for the period determination, the routine bforce and PDM win 3.0[xvii]. bforce uses a brute force method to find the period of the variability. It attempts to fit the data onto a user generated model of the light curve (with a phase resolution of 0.1), and wrap (or fold) it around a suggested period. The routine then splits the data into a series of bins and estimates the variance in each, as follows; , (8) for observations in each bin. If the trial period is incorrect, there will be a large scatter of magnitudes in each bin, i.e. a large variance. This is compared to the variance of the data set as a whole using an F-test, which is achieved by finding the ratioof bin variance (the explained variance) to total variance (the unexplained variance). For an incorrect estimate of the period 1, whereas for the correct period 1. The routine will use a new trial period and re-compute the variances, repeating this until a minimumvalue is obtained. The PDM program works in a similar, if more refined way, implementing some of the recent changes in the accepted way of calculating a phase dispersion minimisation period. While still using a variation-based method, it finds the period using a beta-distribution method (designated PDM*) rather than an F-test, as this has been shown to be the correct probability distribution to use[xviii]. It also utilises a GUI with a series of user-set options, for example variable phase resolution. RR Lyrae Theory Subclasses of RR Lyrae Variables From his observations, Bailey noticed three separate subclasses of variable, which have subsequently been compacted into two subclasses (as subclasses a b were very similar). The following is paraphrased from Baileys original description[xix]: * Subclass ab: Very rapid increase of magnitude, with a moderately rapid decrease in mag. Nearly constant mag for approx one half of the full period. Amplitude of roughly one mag and a period of between 12 and 20 hours. * Subclass c: Magnitude always changing, with moderate rapidity. Range generally half a magnitude, with a period of 8 to 10 hours. As our study concerns an RRab type variable, this class shall be primarily discussed. Typical characteristics of RRab stars RR Lyrae stars are large red stars with a low mass, occupying the area of the instability strip on the H-R Diagram (see Fig. 1) between -Scuti and Cepheid variables, where it intersects the horizontal branch. They are in the core helium burning stage of their evolution, having exhausted their core hydrogen fuel. Mean physical properties of these variables are under some contention, but a summary of current approximations is provided in Table 1. Period 0.2 1.1 days Mv 0.78 0.02 Te 6404 12 K [Fe/H] -1.56 0.25 Mass 0.55 0.01 M Radius 5 1 R Table 1. Typical properties of RRab variables. All values are mean values of 335 variable stars[xxi], except period which is a typical rangei. Evolutionary theory It is thought that the progenitor of an RR Lyrae star was a typical low-mass main sequence star, with M* 0.8M. For the first 15 Gyr of its life, the star burns core hydrogen, fusing it into helium. Once the hydrogen supply in the core is exhausted, the star expands to become a red giant, moving off the main sequence and up the giant branch of the Hertzprung-Russell diagram (see Fig. 1), and shell-burning of hydrogen now occurs around an inert helium core. The helium core eventually collapses, becoming electron degenerate, and increases in temperature until the helium in the core ignites using the triple - process, causing the helium flash. The cores degeneracy is lost and the star moves off the giant branch asymptotically, down towards the instability strip. At this point it can develop the pulsational properties of an RR Lyrae star, although this will be dependent on its mass, its chemical composition, and its temperaturei. Once the helium core is also used up after around 0.1 Gyr, the star begins to expand and cool again, fuelled only by shell burning of hydrogen and helium. The core never becomes hot enough for the fusion of heavier elements. Eventually all the usable fuel is expended and the star will jettison off its outer layers of material to leave a white dwarf star, shining only through the radiation of internal thermal energy. Pulsation theory The study of pulsation theory owes much to Arthur Eddington, who wrote a series of papers detailing a mathematical description of the properties of stars. Having realised that a radial pulsation in a static star would have a decay time of around 8000 years (much shorter than the length of time stars spend in the instability strip), he proposed that stars behaved as thermodynamic heat engines, using some valve mechanism to regulate energy flow[xxii]. In order to fulfil pulsation, this valve would need to make the star more thermally opaque as the star was compressed, and less opaque as it expanded. Effectively this would cause energy to build up when the star was compressed, forcing the star to swell in size until some turning point was reached and the opacity was small enough that energy could escape, leading to the star contracting again. The Rosseland mean opacity shows the overall opacity of a stellar region, and is defined as follows, (9) where is a constant, is the density of the region, and is temperature. Eddington was unable to come up with a particular material that would possess these properties in a star, particularly as during his time it was not believed that hydrogen or helium made up significant proportions of the inside of stars. It is also the case that neutral hydrogen or helium regions cannot be the valve region, as for these regions and i.e. as increases will decrease. This would lead to the pulsation dying out extremely quickly as all the radiative pressure was lost during contraction. However in 1953 Sergei Zhevakin found that regions of doubly ionised helium would provide an area wherebecomes small or negative, resulting in the desired properties for the gas. It was later shown by R. F. Christy[xxiii] that hydrogen ionisation can play a smaller, but still important, role in the mechanism. Ionisation zones can make another possible contribution to the valve in a star. If the energy from fusion processes cause ionisation in gas regions instead of raising their temperature, then the gas will absorb heat during compression stages, causing a pressure maximum near the minimum volume and thus aiding pulsation. This is known as the mechanism. Different classes of RR Lyrae variable pulsate with different modes. For instance RRab stars all vary in the fundamental mode, whilst RRc stars are pulsating in the first overtone. This is one of the reasons that types a and b can be separated from type c as a separate class. A third class of variables has also been observed, termed RRd type stars, which have a double-mode pulsation, pulsating in the fundamental and first overtone modes simultaneously. However, some RRab stars show a long-timescale second periodicity, known as the Blazhko effect. This is an overarching period that can be anywhere between 30 days and several years. The cause of this effect is unclear, but is believed to come from either a nonlinear resonance effect between the radial fundamental mode and some non-radial mode, or a cyclical rotating magnetic field that deforms the main radial mode of pulsation[xxiv]. Estimation of Absolute Magnitude and Distance RR Lyrae stars are useful for the determination of astronomical distances, especially to regions such as clusters in the Halo, and the Bulge. However, unlike for Cepheids, accurate parallax measurements of distance do not exist for RR Lyrae variables (with the exception of a very few the star RR Lyrae itself for example[xxv]), as the majority of stars are simply too far away for resolution currently[2]. Instead, astronomers look to alternative measurement tools, for example main sequence fitting or the Baade-Wesselink method. Main sequence fitting is the process of determining the distance to a cluster by fitting its colour-magnitude diagram to that of nearby main sequence stars which have a parallax-determined distance. This has produced a wide variety of relations over the last twenty years, but a general relation (that is within error of the majority of current estimates) is given by H. Smithi: (10) The currently favoured method of finding the metallicity is to use the relation, described by Jurcsik Kovcs in their seminal paper Determination of [Fe/H] from the light curves of RR Lyrae stars[xxvi]. This used a sixth order Fourier decomposition of the light curve to find multiple properties of an RR Lyrae star. When they plotted the data they found the following linear relation: (11) This allows the metallicity to be determined accurately, and then used in the main sequence fitting method to find an accurate absolute magnitude for a star. Finding the absolute magnitudeis important, because it allows for the use of the magnitude equation to determine distance to an object, taking into account the galactic extinction in the direction of the object due to dust and gas in the galactic plane, : (12) The Baade-Wesselink method, originally applied to Cepheid variables, was based on the assumption that a star will have the same surface temperature and brightness at all points of equal colour on the ascending and descending sides of the light curve. This implies that any luminosity variation between two half-phases can be said to be the result of radial differences in the star. Thus a fractional radius change can be measured as. If a radial velocity curve is also plotted for the star, the radius change over the period can be directly measured, and through the combination of these two results a value for the luminosity of the star can be found. This can be used to show the distance to an RR Lyrae star through the relation (13) whereis Stefans Constant, andis the stars effective temperature. However RR Lyrae variables do not behave exactly like Cepheids; for example during stellar expansion the surface gravity is much greater than when the star is contracting, leading to flux redistribution across the surface. This, combined with shock waves permeating through the stellar atmosphere causing distorted radial velocity curves, means that V band photometry is unfortunately useless for applying the Baade-Wesselink method to RR Lyrae stars. The procedure must instead be carried out in (V-H) or (V-K) colours for example, as infra-red wavelengths are less sensitive to the expansion phase distortions[xxvii]. Estimation of Radius Marconi et alxxv have published an equation relating the period of a fundamental mode RR Lyrae star to its average radius; (14) whereis the mean radius (in units of solar radii), is the period (in days), and is the heavier-than-iron metallicity of the star, defined as; xxi, (15) whereis the alpha-enhancement with respect to iron, and is taken to be equal to 1. This is derived from their theoretical predictions of the radial oscillations of a metal poor RR Lyrae, and applies to stars with helium abundances of between (0.24 and 0.28). III. Experimental Methods Preparing the experiment Inital sessions were spent becoming aquainted with the computers Linux-based operating systems, understanding the basics of photometry and exploring the provided software. Several rooftop sessions were attended to gain knowledge of the telescopes provided, and to learn safety procedures associated with the use of the equipment. Due to initial poor weather, previous years data was analysed in order to improve understanding of the provided scripts. A list of RRab targets from the NSVS catalogue[xxviii] was examined to find a suitable object, with a magnitude range visible on the telsecopes available, a period of less than a day, and a high position in the sky. Table 2. Properties of the Telescope and CCD combinations for each dome. Both telescopes were fitted with the same model of V-band filter. Background information on the chosen star (XX And) was found using the SIMBAD database[xxix], and examined to find previous studies, including estimates of period, metallicity, and star type, as well as dates of previously observed maxima. A plot of the field around the star was taken, and used to identify two calibration stars for the photometry ( 3): The calibration stars used were USNOA2.0 numbers 1275-00765817 (cal-star 1) and 1275-00761527 (cal-star 2). They were searched for in various catalogues to verify that they were not known to be variable. The best exposure time for our field was estimated to be 30 seconds with the 14-inch telescope, and 60 seconds with DRACO, so as not to saturate the image. By taking some sample images and viewing them in GAIA, suitable sizes for the apertures were chosen for each telescope. The sizes of the apertures were chosen to enclose the whole star, whilst giving the minimum error. These were then converted from scaled values to numbers of pixels, and entered into seperate automag_driver files for each telescope, along with the specific pixel scale, gain and read-out noise. Telescope Star Sky Inner Sky Outer 14-inch 4.7 14.9 21.4 DRACO 7 25.7 35.1 Table 3. The aperture radii (in pixels) used for each telescope. Firstly, the convert variables were set up. XX Ands RA and Dec in decimal degrees were inserted into a file called var_sky_position, and photom.py was run on the first frame (called for example filename.fits). This produced an output file called amag.out which contained the positions of all the recognised stars in the image, as well as a calibrated image dfilename_ast.fits. By comparing the (x,y) pixel locations in GAIA for the two calibration stars with the data in amag.out the RA and Dec of the calibration stars were noted, and inserted into a text file named cal_sky_positions. Observation of the Variable Observations of the field containing XX And were then taken over a period of 1 month, using both the 14-inch Far East and the 10-inch DRACO telescopes. For the 14-inch, the observing process was as follows: The object was located using the Earth Centre Universe program, the telescope synched and set to track, and the CCD programmed to take around 30 images per sequence at 30 seconds each, with an 8 second dark frame before each new image. For DRACO, the object was found using the provided G.U.I., with care taken to place the variable star and both comparison stars away from dust grains on the CCD. The telescope was set to track, and programmed to take a large number of images with a 60 second exposure. For each new observing session a seperate file was created, containing all the images and the scripts required for automated photometry. For DRACO processing, a master dark file was also copied from the archive. The file all.py was then amended to iterate over all the images in the dir ectory, and set running. Once the photometry had completed, the raw2dif routine was run, and the results viewed by running qplot. The data were adjusted to Heliocentric Julian Days by running the cor2hjd routine, and the final tables were copied across to a main results directory to be added to the full table of data. bfplot was run on the full dataset using an estimate for the period, and the phase values from the output file fort.30 were killed out and yanked into the dataset file using EMACS. This table was viewed in TOPCAT, and a light curve created. Any clear and accountable anomalies were removed in TOPCAT. To gain a value for the absolute magnitude of XX And, rather than simply an instrumental magnitude, a series of observations were made of photometric stars which had known magnitudes. These are shown in table 4 below: Photometric Star RA Dec Apparent V-band Magnitude 1 1h 18m 20.581s 38 55 38.23 9.847 2 1h 14m 50.729s 38 29 55.80 9.961 3 1h 15m 12.229s 38 49 10.95 9.048 4 1h 16m 39.436s 39 09 38.64 9.735 Table 4: Properties of photometric stars used in the magnitude calibration of XX And. This gave a value for the correction which had to be made to all the observed values for each telescope. The corrections were then applied to the full dataset. An O-C diagram was constructed using the data from the Hipparcos mission, the GEOS RR Lyrae Survey, and also archive data from the GEOS database[xxxi]. The period used was the Hipparcos estimate. Since the newly observed data used HJD, and the archive data was in modified HJD, an addition of 0.5 HJD has to be made to the new data in order to be comparable. The newly observed data was then added to the diagram, and the input period was altered to give the flattest line possible, thus providing a new estimate of the period. The error on the period is given by the slope of the line[xxxii]. Any historical period changes were searched for in the line of the O-C plot. The fast_solve routine was run on all of the summary.obs files, and the comparison stars were checked to see whether or not they were varying. The output model file from fast_solve was edited to include estimates of bin values where there was no actual observational data, and then used in the routine bforce. This was run using the period quoted in the Hipparcos catalogue as the initial period to give an estimate of the new period and its error. The period was also estimated using PDMwin, using an output table from TOPCAT. Errors in the period-finding were estimated using the Jackknife method on both the PDM and bforce programs. This was achieved by recomputing the period, but leaving out one observation at a time from the dataset. The standard deviation of the results produced by this method will be the standard error on the period. Using the new estimates of the period, the dataset was folded using bfplot, and the corrected phase for each datapoint extracted from the output file fort.30. By reading the period-corrected data into TOPCAT a new light curve was plotted. Estimates of the absolute magnitude and average radius of XX And were then computed, as well as its approximate distance from Earth. IV. Results 4: Folded and doubled light curve to show period of XX And pulsation, plotted in TOPCAT, with erroneous data points removed. The colours represent the date on which the observations were taken. Notice the distinct bump at phase 0.1 0.3, and also the hump along the near vertical part of the curve, between phases 0.45 0.55. The curve is doubled to emphasize these features, the causes of which are discussed in Section V. The period of XX And was determined using three methods, the results of which are shown below: 1. The bforce routine: days 2. PDM Win 3.0: days 3. O-C flattening: days These errors represent a precision of the order of 1 second in the estimation of the period. 5: O-C plot for XX And using archive data from the GEOS RR Lyrae database. The plot was calculated using a temporal zero-point constant of 0.0554042 and a minimised to period of 0.72275 days. The newly added points are the ones with error bars. From this it can be seen that no significant period change has occured over the observing history of this star, as a period change would be reflected in a broken line type plot, clearly not present here. The results from the fast_solve routine showed that the comparison stars did not significantly vary in magnitude, i.e. were good candidates for comparison stars (s 6 7). s 6 and 7: Plots created by fast_solve to show the change in the differential magnitude between the two comparison stars, over the course of an observation taken on the 14-inch telescope ( 6) and on DRACO ( 7). It can be seen that the stars retain a near constant differential magnitude throughout both observations. These are shown as an example of the plots produced, and the full set are attached in the appendix. The maximum apparent magnitude of XX And was found to be 9.3814, and the mean apparent magnitude to beusing TOPCAT. From Equation (10), the estimated mean absolute magnitude of XX And was calculated to be 0.512, so using Equation (12) and the observed mean apparent magnitude we can estimate the distanceto XX And to be; pc, using an estimate from the NASA Extragalactic Database extinction calculator for the interstellar extinction in the direction of XX And due to the galactic plane of 0.147 mag[xxxiii]. From Equation (14) the size of XX Ands average radius can be estimated to be: V. Discussion Image Quality During the initial few weeks of the study, the observing conditions were not suitable for collecting data. However whilst this delayed the initial training process, a prolonged spell of good conditions meant that there was ample opportunity for observation of the target star with completely clear skies. The high declination of XX And meant that atmospheric extinction was as low as possible, and did not affect the images significantly. Some image degradation occurred due to dew building up on the lens of the telescope, but these were cropped from the data set. The pipeline script photom.py was able to weed out poor quality images, as they could not be matched to a known field from a catalogue by the starfit routine. The script would then return an error, append nothing to the summary.obs file, and move onto the next image. This helped to remove images with a high background, caused for example by stray clouds across them, as well as smeared images. Whilst the 14-inch telescope provided excellent data over the runs we carried out, DRACO had some slight complications. Dust grains have built up over time on its CCD or on the mirror, and these create small dark patches on a non-flatfielded image. Also, due to small errors in the gears of DRACOs tracking motor, images were noted to jump a few arcseconds at irregular intervals. The jump itself resulted in a smear of light across the image from the objects, and so those frames were unusable for photometry. Fortunately the volume of data taken with DRACO was such that this was of no great consequence. However, the tracking problems caused a slightly more serious problem as well. Whilst care was taken to view the field in such a way that the necessary stars were not located near dust grains on the CCD, the jumping of the tracking system occasionally moved Cal Star 1 into the region of a dust grain. This was initially not caught as an error, until examination of the following light curve ( 9) gave reason to investigate several data runs. 9: Light curve (not adjusted for standard magnitude) of XX And produced using TOPCAT, emphasising the variance in the data caused by the passage of one calibration star across a dust grain region. The blue, green and gray data points were the observations which gave grounds for concern. All three were observing runs from different dates. The reason for the error became apparent after viewing the output plots from fast_solve for the comparison stars ( 10); there was a sharp rise in the difference in magnitudes between the two comparison stars, and as they had been determined to be non-variable, it seemed likely to be caused by an experimental error. This was confirmed when the original images from the runs were examined, and the calibration star was noted to be passing into a darker, dust grain region ( 11). For future studies with DRACO, an automated flat-fielding process would be introduced to the DRACO observing script, as well as the photom.py script. Flat-fielding is a process whereby the differences in quantum efficiency of the pixels across the CCD are measured, and used to account for differences in the gain of the CCD, the goal being to produce a uniform output response to a uniform illumination. In this case it would help to account for the presence of a dust grain on the CCD. A flatfield image taken with the telescope would be combined with the master dark frame to produce a master thermal frame, which could then be subtracted from each raw image using a call to Starlinks Kappa package from within the pipeline. Notes on processing and period determination Since one of our calibration stars (Cal Star 2) had another (~14th magnitude) star very close to it on the image, small aperture sizes had to be set on the 14-inch telescope to ensure that this did not affect our background calculations. DRACO did not have this problem, as it has a smaller resolving power, so larger apertures could be used. During one set of image processing it was noted that Starlink was no longer matching any objects to the field in the image. After much discussion it was realised that the source of the error was a recent change in the standard way of defining the keys in a FITS header, and a conflict was arising as the routine attempted to extract the date from the header. This was solved by editing the header creation script in the DRACO control software source code. The program TOPCAT was found to be extremely useful for the processing and consolidation of large tables of data when in ascii form, where Excel struggled to format them correctly. The plotting tools available in TOPCAT were also more suitable to the experiment, containing options such as auxiliary axes. EMACS was also found to be of use for the killing and yanking of data into new files. From our data, no conclusions can be made in relation to XX Ands Blazhko period, which the literature quotes as 36 days. Although 3 maxima were observed, and all were of slightly different magnitude, the differences can easily be explained simply by statistical variance, and is not indicative of a long overarching period. Further work would attempt to span a much longer timescale, for example 4 or 5 months, in order to capture at least 4 Blazhko periods, and confirm this feature of XX And. PDM Win 3.0 was found to be a preferable method to the bforce routine for period finding, for a number of reasons already discussed in section II, but a major benefit of this method is that it allows the user to manually choose the minimumvalue using a plot ofagainst. bforce on the other hand simply finds the minimum value of , but ignores the possibility of multiple small statistical oscillations around the minimum. This is best demonstrated in 12 below: 12: Screenshot of the GUI of PDM Win 3.0, showing the point in the process where the user is able to pick the point that best represents the minimum of the plot, to give the most accurate value for the period. It can be seen that were simply the lowest value of to be used, the period found could be multiple values in the range 0.72268 to 0.72275 days. For future studies, a more comprehensive investigation of the light curve would be undertaken, and specifically a Fourier analysis would be performed using the Python module Numpys FFT function. The Fourier decomposition of the light curve would allow the use of Equation (11) to accurately determine both the metallicity of the variable star, and its period. This would be extremely helpful in determining a more accurate value for both the distance to XX And, and the radius. During this study an attempt was made to transform the light curve, but no sensible results were obtained. The main code used was based around creating an array containing the phase and magnitude data by reading the ascii data file, in and performing a Fast Fourier Transform on the data: arr=numpy.array([]) a=open(data,r) b=[] for line in a.readlines(): data_a, data_b= (line.split(,)) data_a = float(data_a) data_b = float(data_b) b.append(data_a) b.append(data_b) x=len(b) arr=numpy.array(b) arr.shape=(x/2),2 FFT=fft(arr) y=len(arr) print Zero-frequency Term = , FFT[0] print Positive-frequency Terms = , FFT[1:y/2+1] print Negative -frequency Terms = , FFT[y/2+1:] The coefficients produced were around one order of magnitude too high, caused possibly by sampling rates being too low, and so the process was discarded from the main experimental method. Refinement of this process would be a priority for any further study. The Hump and the Bump From examination of the full light curve for XX And, it became apparent that there were distinct features to the minimum point and along the rising edge. As noted in Section IV these were termed the Hump and the Bump of the light curve by Christyxxiii. They are apparent in over 82% of RRab stars, for example RX Eri, and RR Lyrae itself[xxxiv]. The sources of these increases in magnitude have been considered in many papers, and are still under some contention. These features are considered to be the result of two separate shockwaves emanating from within the stars photospheric layer. The Hump is postulated to be the result of the main shockwave, and is characterised by a standstill on the light curve where the magnitude increases very rapidly to a point, and then increases more slowly up to the maximum. It is followed by a line doubling of the H emission from the star and accompanied by an extreme spike in the ultra violet emission in the stars spectrum. It is postulated that the shockwave occurs when the photosphere of the star reaches its minimum radius, and experiences a very rapid acceleration towards the surface, as a result of the opacity mechanism (see Equation (9)). This collides with higher atmospheric layers, splitting them into two one moving towards the core and the other moving outwards. This is the source of the doubling of the H linesi. The Bump is a small increase in magnitude which occurs as the star is approaching its minimum radius, followed by a weak spike in ultra violet emission from the star, but with no H line doubling. Two competing theories have been proposed: * The Infall Theory Having been pushed to maximum radius by the previous pulsation, material falls towards the core in freefall. It collides with the slower moving photosphere as it approached minimum radius, and a shockwave is caused by the rapid deceleration. * The Echo Theory As the star contracts, a compression wave reaches the stellar core at high speed and is reflected, causing a shockwave in the other infalling matter. Originally the Echo model was rejected in favour of the Infall model, as the outward moving shockwave would be expected to produce the same line doubling phenomenon as seen in the Hump. However, recent studies[xxxv] on cluster RRab variables have noted that the delay time for the Bump is larger for stars with greater radii, as would be expected from a echo-produced shockwave. Also, it has been postulated that the magnitude increase during the Bump is actually sourced in the heating of material caused by the speed of infall[xxxvi]. Investigations are continuing into the source of this magnitude increase. VI. Conclusions The study of RR Lyrae stars is still extremely important in modern astronomy. These variables are still poorly understood in many areas, especially their typical properties, their pulsation mechanisms (specifically in Blazhko variables) and the reasons for shock waves occurring deep within the star. They are vital for the estimation of distances both within our own galaxy and out into the Local Group, since they are more abundant than Cepheids and occur in areas (globular clusters for example) where Cepheids are not found. This study of XX Andromeda focussed on estimating the properties of said star, an RRab type variable. Observations taken over a month were reduced using an automated photometry pipeline, and 4526 data points were used to plot a light curve for XX And. The target star was found to have a fundamental mode pulsation period ofdays, estimated using three methods, two PDM based routines and an O-C plot minimisation. This was in excellent agreement with the literature period found in the GCVS of 0.722747 days. An estimate of the distance to XX And of pc was made using a main sequence fit and a literature value for the metallicity. An estimate for the radius of XX And was also made, and found to be. This value is in agreement with the generally accepted range of RR Lyrae type variable radii, as quoted in Section I. The two comparison stars were confirmed to be non-variable, and thus suitable for the photometry process. An improvement to the pipeline was suggested, namely the addition of automated flatfielding in DRACO images, to remove the possibility of dust grains on the surface of the detector interfering with photometry, especially (in this case) differential photometry. Reasons are suggested for the Hump and Bump features of the light curve, specifically that they are the result of shockwaves occurring at different points during the pulsation process. In conclusion, despite initial bad weather and some data processing problems, this study has resulted in a high quality light curve and several good estimates of the properties XX Andromeda. Appendix Error on the distance comes from taking the standard error of the mean apparent magnitude, and propagating this through Equation (12): Error on the radius is from the propagation of the error on the period through Equation (14) as follows: Jackknifing The jackknife technique was used to estimate the errors on both the bforce and PDM Win 3.0 programs. This was achieved by recomputing the period, but leaving out one observation at a time from the dataset. The error on the total period will then be the standard deviation of these results: Calibration Stars used: Calibration Stars USNOA2.0 Cat Number RA Dec 1 1275-00761527 1:16:55.68 38 55 36.1 2 1275-00765817 1:17:20.69 39 00 38.7 Photometric Stars Photometric Star RA Dec BT mag VT mag V 1 1:18:20.581 38 55 38.23 9.967 9.856 9.847 2 1:14:50.729 38 29 55.80 10.301 9.989 9.961 3 1:15:12.229 38 49 10.95 9.564 9.091 9.048 4 1:16:39.436 39 09 38.64 11.028 9.842 9.735 Table A.2: Photometric Stars Focussing Star Focussing Star RA Dec 1 01:36:47.8 41.405549 Table A.3: Focussing Star Observing Times Date Time On Time Off Telescope Conditions 04/11/09 18:30 20:30 14-inch Cloudy 05/11/09 21:10 22:15 14-inch Cloudy 06/11/09 21:02 22:52 14-inch Clear 06/11/09 21:20 01:15 DRACO Clear 08/11/09 20:00 23:00 14-inch Clear 09/11/09 18:30 22:02 DRACO Clear 14/11/09 18:24 00:20 DRACO Clear 15/11/09 17:05 00:13 DRACO Clear (data taken by JRL) 20/11/09 17:14 00:05 DRACO Clear 20/11/09 20:46 22:09 14-inch Clear 23/11/09 17:51 22:35 DRACO Clear 23/11/09 21:04 21:44 14-inch Clear 25/11/09 18:29 00:26 DRACO Clear (data taken by JRL) 26/11/09 16:58 00:53 DRACO Clear Table A.4: Observing times VIII. 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Percy, 2007, Cambridge University Press [xxxiii] NED Galactic extinction estimator, https://nedwww.ipac.caltech.edu/forms/calculator.html, data originally from Maps of Dust Infrared Emission for Use in Estimation of Reddening and Cosmic Microwave Background Radiation Foregrounds, D. Shlegel et al, 1998, ApJ, 500, 595. [xxxiv] Bump, hump and shock waves in the RR Lyrae stars X Ari and RR LYR, Gillet, D. Crowe, R. A., 1988, AA, 199, 242-254. [xxxv] Carney et al, 1992, ApJ, 386, 663 [xxxvi] Gillet et al, 1989, AA, 225, 445 [xxxvii] https://www.dur.ac.uk/physics.astrolab/

Preparing Students For Their AP Language and Composition Test

<h1>Preparing Students For Their AP Language and Composition Test</h1><p>Learning talk is about more than retaining the guidelines of sentence structure. There are numerous aptitudes and procedures you can exploit when you decide to procure your Rhetoric and Composition degree. This will help set you up for a vocation in talk or composition.</p><p></p><p>As a starting necessity, understudies more likely than not finished and passed their AP language and sythesis test. This test tests an understudy's information on composing the test inquiries with diagnostic abilities and dynamic aptitudes. Understudies additionally probably taken two school level English classes that include composing expositions and perusing abstract works.</p><p></p><p>As an essential for a serious access to graduate school, understudies must finish a temporary job or occupation arrangement in a scholastic foundation just as complete one semester of separation learning classes or online guidance in their picked territory of study. This remembers culmination of four online courses for one semester, with the staying four semesters spent on the web or in grounds study halls. These online courses are essential to procuring a graduate degree in the territory of decision and taking their Graduate Record Examination (GRE).</p><p></p><p>Students ought to likewise be acquainted with the Rhetoric and Composition educational program as it considers showing the understudies the standards behind the law of incongruity, social standards, and the American political scene. A nature with the Rhetoric and Composition educational plan can likewise assist understudies with increasing a more profound comprehension of these parts of the American instructive framework. Understudies will pick up the capacity to comprehend the conventional structure of factious composition by being encouraged a couple of significant fundamental s and working with perusing material that has been concentrated from the oral, composed, and insightful perspectives.</p><p></p><p>Most online degree programs offer the understudies test prospectuses, especially those that don't charge educational cost. Now and again, understudies may even have the chance to make and present their own course schedule using intelligent showing apparatuses, for example, white sheets and video. They can likewise gain from different understudies by requesting investigates, requesting help with a class conversation, and taking an interest in conversations with friends and educators in the online classroom.</p><p></p><p>Students will have the option to perceive how powerful utilization of intuitive apparatuses and on-request criticism encourages them to rehearse and build up the fundamental methods and methodologies of compelling article composing. These would then be able to be utilized to plan for the GRE assessment. The entirety of this will assist understudies with pushing forward in their scholarly professions and improve their general instructive experience.</p><p></p><p>As an essential to acquiring a degree in Rhetoric and Composition, understudies more likely than not taken their AP assessment. To get to the most state-of-the-art data on AP directions, understudies should contact their school or college's expert counselor.</p>