Mauvais - French Expressions

Mauvais - French Expressions The French word mauvais literally means bad and is also used in many idiomatic expressions. Learn how to say mean trick, weed, ill repute, and more with this list of expressions with mauvais. French Expressions Using Mauvais avoir mauvaise mine to look unhealthy La balle est mauvaise. (tennis) The ball is out. faire un mauvais coup to play a mean trick (on someone) se faire du mauvais sang to worry en mauvais tat in bad condition un mauvais contact faulty connection un mauvais coucheur awkward customer une mauvaise excuse poor excuse la mauvaise graine bad seed, bad lot une mauvaise herbe weed une mauvaise langue a gossip un mauvais lieu place of ill repute le mauvais il evil eye Les mauvais ouvriers ont toujours de mauvais outils. (proverb) A bad workman always blames his tools. mauvais rapport qualit-prix poor value le mauvais temps bad weather regarder lil mauvais to look threatening, to fix someone with a threatening look recevoir un mauvais coup to get a nasty blow

The media and American politics Essay Example | Topics and Well Written Essays - 6000 words

The media and American politics - Essay Example US media has been often criticised as being manipulated by the government and ends up serving biased and distorted news to the general people. My article will examine the role of the US media in the political scenario, in the context of the 2000/2004 elections, and will examine to find out as to whether the media does really have a slant/bias, and whether it really acts as a propaganda vehicle for the political party in power. The Media and American politics 1 Introduction â€Å"Balanced coverage [is what] plagues American journalism and ...leads to utterly spineless reporting with no edge. The idea seems to be that journalists are allowed to go out to report, but when it comes time to write, we are expected to turn our brains off and repeat the spin from both sides..."Balanced" is not fair, it's just an easy way of avoiding real reporting...and shirking our responsibility to inform readers† (Ken Silverstein, 2008). ... esidential speeches, various TV ads, press meetings, or even through the normal routine daily news, which creates a form of ‘virtual reality’ for its viewers. Though the results, as have been observed in the various elections, are quite far from being virtual, and are indeed real and turning out to be critical too, for the political parties. In the context of conducting political campaigns, the magnitude and scale of the US elections in the recent years, is something which would have been unimaginable even 60 years back. These transformations in the political field can be to a large extent laid at the door of the media and press coverage of the political policies.. John Zaller summarily defines this slowly evolving new process in the arena of US media and politics as, â€Å"the attempt to govern on the basis of words and images that diffuse through the mass media† (2009, 389). There is no denying the fact that in this twenty first century modern world, the news me dia does indeed play a pivotal role in the functioning of the political regimes, and the shaping of a nation’s democracy. In a modern democratic country, the right to information forms a vital criterion for its citizens to assess the functioning of the political party in power, and to receive this information they rely on different various news distributing agents like the television, newspapers, amongst many others. This free access to the media for information related to the actions of the political leaders, in terms of various policies and legislations and their consequential aspects, are essential for the proper functioning of a democratic country. â€Å"It ensures that citizens make responsible, informed choices... [While] information serves a â€Å"checking function† by ensuring that elected

Facilitating Learning and Teaching Essay Example | Topics and Well Written Essays - 4000 words

Facilitating Learning and Teaching - Essay Example Reflection is a way in which professionals can bridge the theory-practice gap, based on the potential of reflection to uncover knowledge in and on action (Schon, 1983 cited in Taylor, 2006). (Taylor, 2006) in his book defined reflection in more broad way, Reflection is the throwing back of thoughts and memories, in cognitive acts such as thinking, contemplation, meditation and any other form of attentive consideration, in order to make sense of them, and to make contextually appropriate changes if they are required. When we use reflection it enable us to explore what is beyond the line of vision and to look around and find out what is behind. Reflection in nursing education allows students to express their learning which occurred in the clinical placement (Kuiper & Pesut, 2004). The reflection can confirm and correct actions. Doing that equips you translate strategies successfully in the new situations and continue development. Also when problems exist it enables you to avoid using t he previous solutions in the new similar situations and try another new ways of actions (Jones, 2010:11) Reflection is divided in to two types, reflection in action and reflection on action, identified by Donald Schon (1983) Cited by Jasper (2003). Reflection in action is the way that people think and theorise about practice while they are doing it. It is an automatic activity occurs during situation in the practice in every day practice. Reflection on action involves us in consciously exploring experience and thinking about practice after it has occurred to discover the knowledge used in the situation. This occurs through analysis, interpretation, and the recombination of information about the experience so that the new perspectives are found about that what has happened. It is an active process that changes the experience to knowledge by thinking, analyzing and describing the situation. In this paper work I am going to reflect on a lecture given by me for midwives’ students and will use reflection on action through following Gibbs reflection framework (Rolf et al,2001:18 & Jasper 2003:6). This reflection framework model is developed by Graham Gibbs in 1998. It consists of six stages that guide you through the process of reflection by asking a set of question divided in the cycle stages. The stages are description, feelings, evaluation, analysis, conclusion and action plan (Jasper, 2003:78). Description Meeting with the lecturer was made two week before the lecture day, which gave enough time to read, plan and prepare for the lecture. The lecture subject and the time were discussed between me and the module lecturer. The topic was about kidney and urine formation, covering anatomy and pathophysiology. It was the last session on a Friday and the students are eager to go home and start their weekend; I arrived one hour before the session, to meet the lecturer and to show here the material, the case studies related to the subject and the multiple choice q uestions. After that we discussed the session plan and she suggested to amend one multiple choice question and it was done. We arrived in the class room and the lecturer introduced me and my colleague and informed the student that we are going to give today’s lectures. My colleague started her lecture that was about body fluids. I sat on the side to take some notes that will be useful to include in my session. After my colleague

No Day of Triumph Essay Example | Topics and Well Written Essays - 750 words

No Day of Triumph - Essay Example While being American brings about an idea of inclusion and equality, being black creates a sense of being an outsider and being separated from the mainstream. This dichotomy means that African Americans have to deal with the perception of others as well as a self-perception that could be colored by how others see them. In this respect, relationships become critical for the African Americans described in the stories since family, the idea of being connected to family values and the need to pass on the family heritage to the children is very important for the characters. While family supports and shapes the African American identity, in some ways it can also be a hindrance to the personal liberty and drive of an individual who seeks a different path. These act as the remnants of the slavery era in which freedom and being able to choose your destiny were not the options available to every African American. In fact, slavery also affects the viewpoints of white and Caucasian individuals described in the story since the idea of whites being the masters and blacks being slaves continues to reside in the cultural subconscious of the southern states where the story takes place. Perhaps the worse situation is experienced by the Mulatto who is neither black nor accepted by the whites as being a part of them. Even amongst African Americans, there is a level of awareness about being darker and thus more African than others and this difference is also reflected in the socioeconomic situation an African American can find himself in when the educated black person has to bear the burden of being better than others so that s/he can present a positive face for his/her race. These differences carry on with the love of religion which poor black people show in greater strength compared to those who are economically their betters. The

RPS in Galaxy Clusters Analysis

RPS in Galaxy Clusters Analysis Jellyfish:  A  spectroscopic  study  of  ram-pressure  stripping  in  massive  galaxy  clusters* ABSTRACT We continue our exploration of ram-pressure stripping (RPS) in massive galaxy clusters at z>0.3 by assessing the spectroscopic properties of RPS candidates selected previously based on their morphological appearance in Hubble Space Telescope images. We confirm cluster membership for 55 of our candidates, thereby tripling the number of RPS candidates known at z>0.2. Although many of these systems are too faint and too distant for the kind of in-depth investigation required to unambiguously confirm or refute the presence of RPS, the ensemble properties of our sample are consistent with increased star formation, and many of the selected galaxies exhibit visible debris trails. Specifically, about two thirds of all galaxies exhibit line emission ([OII]ÃŽÂ »3727AËÅ ¡ , HÃŽÂ ², and, where observationally accessible, HÃŽÂ ±) consistent with ro- bust star-formation rates that significantly exceed those expected for systems on the galaxy main sequence. We find no significant depe ndence of either the presence of line emission or the inferred star-formation rate on the relaxation state of the host cluster. Although we caution that our sample may contain not only galaxies undergoing RPS by the diffuse intra-cluster medium (ICM), but also minor mergers located at the low-density cluster outskirts and merely projected onto the cluster cores, we expect our results to facilitate and inform realistic process models of the stripping process by providing the first statistically significant sample of RPS candidates in truly massive clusters. While extremely rapid removal of the intrastellar medium is not ruled out by our findings, extended periods of triggered star formation are clearly an integral component of the physics of ICM-galaxy interaction in massive clusters. INTRODUCTION Spiral and elliptical galaxies are both commonly observed in the universe but inhabit (and dominate) very different environments. The inverse correlation between spiral fraction and density of the environment has long been established based on both galaxy mor- phology and colour (Dressler 1980; Baldry et al. 2006) and is so pronounced as to suggest causation. Since the preponderance of red, elliptical galaxies is not limited to the densest environments (i.e., the cores of massive galaxy clusters) but is notable already in groups of galaxies (Blanton Moustakas 2009), several phys- ical mechanisms may be responsible for the observed segregation of galaxy types and appear to be have been at work for several Gyr, as evinced by the steady increase in the dominance of ellipticals in  clusters from zà ¢Ã‹â€ Ã‚ ¼1.5 to the present day (Scoville et al. 2013). * Most of the data presented herein were obtained at the W.M. Keck Ob- servatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aero- nautics and Space Administration. The observatory was made possible by the generous finical support of the W.M. Keck Foundation. Although simulations have indicated that elliptical galaxies can form directly through spherical collapse of dark-matter halos in high-density environments (e.g. Navarro Benz 1991), it is widely accepted that transformations of galaxies from late to early types are central to the creation of the Hubble sequence. These occur in a range of environments and, most likely, over a range of character- istic timescales. While slow-acting gradual effects such as galaxy harassment (Moore et al. 1996, 1998) are bound to contribute, more violent interactions have been shown to be highly effective in turning disk galaxies into spheroids. In modestly dense environ- ments with commensurately modest relative galaxy velocities, i.e., in galaxy groups and at the outskirts of more massive galaxy clus- ters, galaxy mergers as predicted by Holmberg (1941) and explored in numerical simulations (e.g., Toomre Toomre 1972; Barnes Hernquist 1992, 1996; Mihos Hernquist 1996) can create a wide range of remn ants, including spheroidal galaxies (Toomre 1977; Hammer et al. 2009). By contrast, at the extreme opposite end of the density range where galaxies move too fast to have a signif- icant cross section for merging, ram-pressure stripping (RPS) by the diffuse intra-cluster medium (ICM) has been predicted (Gunn   Gott 1972), simulated (e.g., Farouki Shapiro 1980; Vollmer et   al. 2001; Roediger Hensler 2005; Domainko et al. 2006; Kron- berger et al. 2008; Bekki 2009; Tonnesen Bryan 2010), and ob- served across a wide range of wavelengths. Numerous studies have established that RPS is capable of rapidly displacing and removing gas from spirals falling into galaxy clusters (e.g., White et al. 1991; Rangarajan et al. 1995; Veilleux et al. 1999; Vollmer et al. 2008; Sun et al. 2010). We here present new results from an observational study de- signed to identify and characterise RPS events in massive clusters at intermediate redshift. Our project is motivated by the fact that, while RPS has been well studied in the local Universe (e.g., Sun et al. 2006; Sun, Donahue Voit 2007; Merluzzi et al. 2013; Fuma- galli et al. 2014; Poggianti et al. 2016), work at higher redshift has advanced more slowly, due to the obvious challenges in attaining commensurate signal and spatial resolution (but see Poggianti et al. 2004; Cortese et al. 2007; Moran et al. 2007; Owers et al. 2012). It is only at z>0.2, however, that the volume probed by any clus- ter survey becomes large enough to contain a significant number of truly massive clusters (systems more massive than Coma), i.e., clusters that allow us to study RPS over the full range of environ- ments, from the only mildly overdense cluster outskirts to extreme densities in the core regions that are never reached in local cluster s like Virgo. In this paper we examine the spectroscopic properties of galaxies tentatively identified as undergoing RPS in massive galaxy clusters at z>0.3. All clusters considered for this work were iden- tified by their X-ray emission and optically confirmed in the course of the Massive Cluster Survey (MACS; Ebeling et al. 2001, 2007, 2010; Mann Ebeling 2012). Potential stripping events were se- lected based on the morphology of galaxies in images of MACS cluster cores obtained with the Advanced Camera for Surveys (ACS) aboard the Hubble Space Telescope (HST) (see Repp Ebeling, in preparation, for an overview of this dataset). In Ebel- ing et al. (2014, hereafter E14) we presented a first sample of six textbook cases of RPS identified visually in these data and, ow- ing to their appearance, referred to as jellyfish (Fig. 1). Our sec- ond paper (McPartland et al. 2016, hereafter M16) defined a cus- tomized set of morphological selection criteria used to compile a larger sample of 223 potential RPS candidates and examined the spatial distribution and apparent projected direction of motion of the most plausible candidates. In this third paper, we present, dis- cuss, and interpret the results of extensive spectroscopic follow-up observations of the M16 sample. Our paper is organised as follows: After a brief introduction in  §1,  §2 describes the setup and execution of our spectroscopic  follow-up observations of RPS candidates, the data reduction, as well as our criteria to assess cluster membership for any given  galaxy. In  §3 we derive fundamental spectral properties of the con-firmed cluster members, infer star-formation rates, and estimate their stellar mass.  §4 compares the properties of RPS candidates  with those of the general population of star-forming galaxies, dis- cusses physical triggering mechanisms, and investigates correla- tions between the star-formation rate of RPS candidates and the relaxation state of the host cluster. We summarise our findings in  Ãƒâ€šÃ‚ §5. Throughout this paper we adopt the concordance ΆºCDM cos-mology, characterised by à ¢Ã¢â‚¬Å¾Ã‚ ¦m= 0.3, à ¢Ã¢â‚¬Å¾Ã‚ ¦ÃƒÅ½Ã¢â‚¬ º = 0.7, and H0 = 70 km sà ¢Ã‹â€ Ã¢â‚¬â„¢1 Mpcà ¢Ã‹â€ Ã¢â‚¬â„¢1. Figure1.HST/ACS snapshot image of MACSJ0451-JFG1, a textbook case of ram-pressure stripping from the E14 sample. The red and yellow arrows mark the inferred direction of motion in the plane of the sky and the di- rection to the cluster centre, respectively. Note that the tell-tale jellyfish morphology of this z=0.43 galaxy is readily discernible only thanks to the superb resolution of HST/ACS. (Reproduced from E14) SPECTROSCOPIC OBSERVATIONS AND DATA REDUCTION The targets of our spectroscopic follow-up observations were drawn from the set of 223 galaxies tentatively identified by M16 as undergoing ram-pressure stripping. We refer to M16 for a detailed discussion of the morphological criteria applied to select these can- didates from a master catalogue of over 15,000 galaxies detected in short HST/ACS exposures in the F606W and F814W bands of 63 MACS clusters in the redshift range of 0.30.7. A comprehen- sive description of the HST observations used by M16 is provided by Repp Ebeling (in preparation). Since most of the RPS candidates from the list of 223 were targeted by us in spectroscopic observations of MACS clusters that supported several complementary research projects, compromises had to be made in the design of the observations. In order to max- imise scientific returns, clusters that feature large numbers of tar- gets for each of the different projects were given priority, resulting in a bias in favour of clusters with multiple RPS candidates. In ad- dition, the simultaneous focus on many targets made it impossible to optimise the orientation of individual slits or even the position angle of the entire mask for the study of RPS candidates. Keck/DEIMOS observations All spectroscopic data for this work were obtained with the Deep Imaging Multi-Object Spectrograph (DEIMOS; Faber et al. 2003) on the Keck II 10m telescope on Maunakea. All multi-object spec- troscopy (MOS) masks used 1//-wide slits of at least 8//length, i.e., long enough to allow sky subtraction from in-slit data. Spectra were obtained using the 600 l/mm Zerodur grating set to a central wavelength of 6300AËÅ ¡ ; the GG455 blocking filter was employed to prevent second-order contamination at ÃŽÂ »>9000AËÅ ¡ . Exposure times  ranged from 3ÃÆ'-600 to 3ÃÆ'-1200 seconds. The seeing during these  observations was typically 0.8//. All data were reduced with the DEIMOS DEEP2 pipeline (Cooper et al. 2012; Newman et al. 2013), creating sky-subtracted and wavelength-calibrated one- and two-dimensional spectra. Redshifts were determined from the one- dimensional spectra using elements of the SpecPro software pack- age (Masters Capak 2011). Overall 110 RPS candidates were observed in 26 MACS clus-ters. Cluster membership We establish (likely) cluster membership by comparing the differ- ence between an RPS candidates redshift and the systemic redshift of the cluster with the cluster velocity dispersion. The latter is com- puted from all galaxy redshifts measured for the respective cluster in the course of the extensive spectroscopic follow-up work per- formed by the MACS team; a description of the underlying data and of the procedure employed to determine robust velocity dispersions for MACS clusters is provided by Repp Ebeling (in preparation). Although it is possible that some of the galaxies for which we rule out cluster membership are in fact still undergoing RPS within their local environment in the fore- or background of the respective MACS cluster, the majority of such non-cluster members are more likely to owe their disturbed optical morphology (and thus their selection in M16) to merger events or to gravitational lensing. In the following, we thus limit the term RPS candidates to galaxies classified as likely cluster members based on their radial velocity within the comoving cluster rest frame. Spectral corrections and flux calibration The reduced spectra created with the DEEP2 pipeline are wave- length-calibrated and thus allow redshift measurements that are ac- curate to within the limits set by the instrumental setup and the pre- cision of the dispersion solution. The determination of line fluxes and, in particular, line-flux ratios across a significant wavelength range, however, require flux-calibrated spectra. In addition, flux lost during the data-reduction process (due to CCD defects, non- optimal definition of spectral apertures, and, importantly, the finite slit width) needs to be recovered, if the measured line fluxes are to be interpreted as characteristics of the observed galaxy as a whole. Whereas corrections for missing flux are fairly straightforward to apply, flux calibration is notoriously difficult for multi-object spec- trographs (especially when the respective observations were not performed at the parallactic angle), owing to spatial variations in the instrument response across the field of vie w covered by the slit mask. Before flux calibration is performed, we visually inspect the two-dimensional spectra of all RPS candidates classified as likely cluster members. We manually mask out the spectral traces of non- target sources falling serendipitously into a slit, fill in bad detector columns, and re-extract the target spectra within an aperture that maximizes the object flux at all wavelengths. We then resort to external means to calibrate these spectra by tying the latter at two wavelengths to the photometry obtained for the respective galaxy with HST/ACS in the F606W and F814W passbands. To this end, we convolve the HST images in these two filters with a Gaussian whose full width at half maximum is matched to the average seeing during our DEIMOS observations and then integrate the flux within the DEIMOS slit (Fig. 2). The re- sulting linear calibration, illustrated in Fig. 3, achieves two goals: it Figure2.Example of the procedure applied to obtain accurate absolute photometry for the flux entering a slit on our MOS masks. Left: HST/ACS image of an RPS candidate in the F606W filter; overlaid are isophotal flux contours (green) and the slit as positioned during the DEIMOS observation. Right: As left, but convolved with a Gaussian kernel that mimics the seeing of the groundbased observation and rotated to align the slit with the image axes. 80 3000 250060 2000 40 1500 1000 20 500 00 40005000600070008000900010000 wavelength (A) Figure 3.DEIMOS spectrum of one of our RPS candidates before and af- ter flux calibration and slit size correction. The green and red lines show the throughput (in arbitrary units) of the ACS/F606W and F814W filters, respectively, used to anchor the flux calibration. (1) crudely corrects for wavelength-dependent variations in the to- tal throughput of our observational setup; and (2) extrapolates the spectrum actually observed through the slit to the spectrum of the entire galaxy. Note that the validity of the latter correction rests on the implicit assumption that the spectrum recorded within the slit is representative of that of the galaxy as a whole. Although this as- sumption is not necessarily well justified, it is widely applied and ensures consistency and comparability between line fluxes (and de- rived properties like star-formation rates) obtained in studies using different instrumental setups and observational strategies. PHYSICAL PROPERTIES OF RPS CANDIDATES Stellar mass In order to establish the locus of our RPS candidates within the general population of star-forming galaxies, we need to ensure that comparisons are made only between galaxies of comparable stellar mass. While the stellar mass of galaxies in our sample cannot re- liably be determined from only the HST/ACS data in the F606W  and F814W used for their original selection by M16, or from the optical spectroscopy within the à ¢Ã‹â€ Ã‚ ¼5000 à ¢Ã‹â€ Ã¢â‚¬â„¢9000AËÅ ¡ range described in Section 2, photometry across a wider spectral range that extends into the near-infrared (NIR) regime is well suited to constrain the spectral-energy distribution (SED) of galaxies and thus their stel- lar masses. For a significant fraction (QUANTIFY) of our cluster fields, the required data are available thanks to imaging observa- tions of MACS clusters with the NIR channel of HSTs Wide-Field Camera 3 (WFC3) performed for the CLASH project (Postman et al. 2012) and the MACS SNAPshot programs GO-12188 and -12884 (PI: Ebeling) described in Repp Ebeling (in preparation). The resulting photometry in the XXX passbands (CLASH) for 15 of our RPS candidates, and in the F606W, F814W, F110W, and F140W filters (SNAPshot programs) for an additional 17 galaxies, is fit with synthetic spectral templates using LePhare (Arnouts et al. 1999; Ilbert et al. 2006), an SED modeling code developed pri- marily for the determination of photometric redshifts of galaxies in the COSMOS field. Emission-line fluxes and star-formation rates 3.2.1   Extinctioncorrection DISCUSSION BPT diagram RPS candidates and the galaxy main sequence Properties of the host clusters CONCLUSIONS ACKNOWLEDGEMENTS We thank Elke Roediger for helpful discussions on the latest in nu- merical simulations of ram-pressure stripping and how to further constrain them via imaging and spectroscopic observations. Most of the data presented herein were obtained at the W. M. Keck Ob- servatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The observa- tory was made possible by the generous finical support of the W. 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Philosophy as a Contributor to Well-Being :: Paideia Philosophers Essays

Philosophy as a Contributor to Well-Being ABSTRACT: In this essay, I sketch five complementary arenas of concern are set forth as candidates for a cogent contemporary theory of paideia. First, a searching, goal setting form of reflection is central to paideia today even as it was in Hellenistic times. A second contributor to paideia is critical reflection. But, third, reasoning is also connected to embodied activity through feeling. Thus, sensitivity to existential meaning helps people determine what they really want and believe, and it also joins them to the persons, things, and events that matter most to them. Fourth, use of the moral point of view safeguards individuals against wallowing in mere self-indulgence heedless of the welfare of others or of the world as a whole. Finally, only by being open to the complex challenges of the world can a person be receptive to the mysterious dimension of life and discern ultimate priorities. I claim that persons guiding themselves by the five-leveled notion of paideia articulated he re will again experience the power of philosophy to confer well-being upon themselves and the world. The main theme of the Twentieth World Congress of Philosophy, "Paideia: Philosophy Educating Humanity," challenges philosophers to assess what impact philosophy is having and should be having in the world today. The use in the title of the classical term paideia suggests that conference organizers believe that philosophy should have both an beneficial and a broad impact. For implicit in the notion of paideia is the idea that philosophy is a boon bestowing enterprise; in enlightening persons, it improves their well-being. The breadth of impact is suggested by this definition of paideia from Webster's Third New International Dictionary: "The training of the physical and mental faculties in such a way as to produce a broad enlightened mature outlook harmoniously combined with maximum cultural development." I submit that this classical notion remains a worthy ideal expressive of the gifts philosophy can bring humanity. Paideia is cognate to notions of education found in Asian philosophy. Philosophy practiced in the spirit of paideia can indeed be a contributor to human well-being. However, the world today is a vastly different place than the classical world in which the notion of paideia took root. A challenge facing any interpreter of paideia now is to locate considerations which have arisen in the course of philosophical history which deserve to be incorporated into a contemporary theory of paideia.

Bags of Reactions Lab Essay

* Problem/Purpose * Background Information: The Law of Conservation of Mass was created by Antoine Lavoisier in the 18th century. This law stated that mass could matter could neither be created nor destroyed. During a reaction the bonds of the reactants are broken and form new substances. As stated in the Law of Conservation, matter can neither be created nor destroyed; because of this the products should have the same number and type of atoms as seen in the reactants. * Purpose: Test the Law of Conservation of Mass. * Hypothesis: If we weight the mass of the materials before and after the reaction, then we can prove if the Law of Conservation of Mass is true. * Materials: * Goggles * 25mL graduated cylinder * 2 resealable bags * Scale * Antacid tablet * Scoopula * CaCl2 , Calcium Chloride * NaHCO3 , Sodium Hydrogen Carbonate * Universal Indicator * Procedure Part A 1. Measure 25mL of water and put into a resealable bag. Flatten air out of the bag and seal it. Record the mass in Table 1. 2. Record the mass of the antacid tablet in Table 1 3. Tip the bag sideways, and while holding the bag this way, add the tablet and water so not mix. Do not trap any extra air in the bag. Reseal the bag. 4. Let the tablet drop into the water. Observe the reaction until it comes to a complete stop. Record the observations. 5. When the reaction is complete, record the mass of the bag and its contents in Table 1. Part B 6. Add two scoops of CaCl2 to the second bag 7. Add one scoop of NaHCO3 to the bag and shake gently to mix. 8. Determine the mass of the bag and its contents. Record in Table 2. 9. Measure 25mL of water in a graduated cylinder. Add 10 drops of Universal Indicator to the water. 10. Tip the bag sideways, and while holding the solids in the upper part of the bag, pour the water into the bag so the solids don’t mix. 11. Keeping the trapped air to a minimum, reseal the bag. Hold the bag and let the liquid move from one end of the bag to the other until the contents are mixed. 12. Observe the reaction until it comes to a complete stop. Record your observations 13. Record the mass of the unopened bag in Table 2. Clean up your work and wash your hands before leaving the laboratory. * Data/Results Table 1: Antacid and Water| Mass of bag and water| 27.085g| Mass of tablet| 3.21g| Mass of bag and reactants| 30.305g| Mass of bag and products| 28.14g| Table 2: CaCl2, NaHCO3, and Water| Mass of bag and dry reactants| 4.09g| Volume of water| 25mL| Mass of water| 24.925g| Total mass of bag and reactants| 29.015g| Mass of bag and products| 27.37g| * Analysis/Conclusion A. Analysis Questions: 1. How do the values for the total mass before and after each reaction demonstrate the law of conservation of mass? The values seem to be in the same general value 2. What were three observations you made that indicated a reaction had occurred in part A? The tablet started to fizz, the bag began to fill with gas, and you could hear the tablet reacting with the water. 3. An indicator changes color when the acidity of a solution changes. What evidence is there that such change occurred in Part B? The universal indicator changed to a yellowish orange color 4. Did the reaction in Part B become more acidic or basic? More acidic B. Conclusion: The lab showed us that the Law of Conservation of Mass is correct. I feel that there were some mistakes in the lab. The size of the scale we were using was not large enough to fit the entire bag on for weighing. I feel that this affected the results we recorded for mass. If I were to redo this experiment I would be sure to use a bigger scale. I feel the data was also affected by extra air left in the bag. The results are close enough to show that the Law of Conservation of Mass is possible though when you take into accounts the problem we had with the lab.

Push and Pull Factors in the Tourism Industry Essay

Gogo (formerly known as Aircell), is an innovation company, becoming leaders in providing inflight connectivity. The company began in 1991, when they began creating telephone systems for aircrafts, they progressed from this and in 2006 began creating a broadband network for aircraft. In 2008, they launched this new system into commercial flights and since then they have been offering this service for various American airlines including US Airways, Virgin America and American Airlines (Gogo 2013). The purpose of this paper is to discuss the recent experience of using Gogo Wi-Fi on an American Airlines flight, and investigate the strategy of Gogo, with reference to the innovation dilemmas when creating this new service. The experience occurred on an American Airlines flight from San Francisco to Los Angeles, although the technology had been available for a few years, this was the first time the consumer had experienced Wi-Fi whilst flying. Although the consumer had no need for the Internet on their flight and only purchase it to update their Facebook status, they recognised the benefits of having the internet on long haul flights, this included people being able to check emails and stay in touch with people and it also provides people with the ability to download entertainment from online sources and no longer be limited to the selection provided by the airline. Due to the nature of the Airline industry, at the core level it can be viewed as a generic offering across the industry. This resulting in airlines often creating a differentiation strategy, in order to gain a competitive advantage as they seek to increase the value of the product/service on offer to the consumer (Hooley et al, 2012). The Gogo Company acknowledged that their innovation could provide a service to Airlines that will enable them to differentiate themselves. This can be identified on the Gogo website, as it states ‘By differentiating your airline and providing a memorable passenger experience, you stand to gain loyalty among your valued flyers†¦lets you custom wrap the video portal, so your brand is consistently comes forth whenever passengers are connected’ (Gogo 2013). In 2009, American Airlines announced it would be using Gogo services on their domestic flights, costing the airline $100 000 to install (Semuels, 2009). This therefore shows that American Airlines have recognised the benefits and the increase ticket sales and revenue they could receive by advertising Gogo Internet is now a part of inflight entertainment. When innovation occurs within a company, they must consider the following innovation dilemmas, whether the product or service is a technology push or market pull, product or process innovation, open or closed innovation and finally a technological or business-model innovation. Technology push is when innovation is pushed by technologist or scientist who pass this information onto the company, from there they will manage, promote and distribute this new innovation. This can be compared to market push, this is when companies create innovation based on what the ‘lead users’ are doing in that particular industry (Johnson et al, 2011). One aspect that has enable Gogo to overcome this dilemma, is by listening to what the market wants and ensuring they are up to date with the current market technological tends. Product Innovation is when emphasis on innovation is placed on the finally product, whereas in process innovation is when innovation is focused on the production and distribution (Johnson et al, 2011). At the beginning Gogo was focused on the product innovation, but as the company has grown, they have shifted to process innovation. This can be identified on the Gogo website stating that ‘1 in 4 people consider their laptop, tablet or IPad an essential carry on item’ (Gogo 2013), therefore Gogo has had to ensure its innovation is compatible across the multiple devices. Open innovation is when companies improve their innovation through gaining ideas through internal and external personnel. This can be compared to closed innovation, when innovation is based on internal personnel (Johnson et al, 2011). Gogo tend to go for closed innovation to ensure they remain leaders in the industry however ensuring they are receiving feedback from their clients to ensure they are meeting their needs. Technological or business-model innovation, technological innovation is when innovation is relied on new science or technology, whereas business-model innovation emphasises on creating new models that will bring stakeholders together in a new method (Johnson et al, 2011). Gogo began as a technological innovation, however has become a business-model innovation for companies using Gogo products and service, as it changes the way they sell and promote their airline company. Overall, Gogo are the market leaders and innovators in inflight communications services. And from reviewing the company’s current strategy, it can be recognised that will continue to be market leaders as they are aware of the demands from today’s consumers, and are constantly updating, innovating and meeting these demands. Although by company innovating new products or services, it dose propose the risk of innovation dilemmas, Gogo has proven that they can overcome these dilemmas and continue to lead and grow.