Observations. The Evaluator’s first observation of the Educator should take place by November 15. Observations required by the Educator Plan should be completed by May 15th. The Evaluator may conduct additional observations after this date. The Evaluator is not required nor expected to review all the indicators in a rubric during an observation.
Observations. As a component of the FFMP, AstraZeneca U.S. compliance personnel shall conduct observations of sales representatives to assess whether the messages delivered and materials distributed to HCPs are consistent with applicable legal requirements and with AstraZeneca’s Policies and Procedures. These observations shall be full day ride-alongs with sales representatives (Observations), and each Observation shall consist of directly observing all meetings between a sales representative and HCPs during the workday. The Observations shall be scheduled throughout the year, selected by AstraZeneca U.S. compliance personnel both on a risk-based targeting approach and on a sampling approach, include each therapeutic area and actively promoted product, and be conducted across the United States. At the completion of each Observation, AstraZeneca U.S. compliance personnel shall prepare a report which includes:
Observations. The Evaluator’s first observation of the Educator should take place by November 15th, unless the Educator is on a self-directed plan. Observations required by the Educator Plan should be completed by May 15th. The Evaluator is not required nor expected to review all the indicators in a rubric during an observation. However, every effort will be made to observe for a period of time sufficient to observe as many indicators as possible.
Observations. OY Car was observed using XMM-Newton on 29–30 June 2000 and again on 7 Aug. 2000. Optical observations from Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20000039 G. Ramsay et al.: XMM-Newton timing studies of OY Car L289 Table 1. The duration of the EPIC observations and the mean background subtracted count rates DatePNorbit 121 0.56 ct/s 0.17 ct/s 0.19 ct/s ∼∼∼∼∼ ∼the AAVSO (Mattei 2000a) indicate that OY Car was in outburst on 24–25 June (reaching 12 mag) and had faded below 15 mag by 27 June. Observations taken using the OM indicate that V 16.0–16.2 mag on 29 June, indicat- ing that it had faded rapidly after outburst. On 7 Aug., OM observations gave B 15.7–15.9 mag. A series of 5 optical spectra were also taken at the South African Astronomical Observatory on 7 Aug. The spectra imply V 15.8–16.5 and B 15.6–16.8, indicating that, in the optical, OY Car was at a similar brightness compared to the June observation.Outbursts of OY Car vary in length. For those that last less than a week, AAVSO observations (Mattei 2000b) show that the next outburst typically occurs 180 days later, so it is unlikely that OY Car experienced another outburst between the two XMM-Newton observations.˚∼∼Data were collected in various observation modes of the OM. These include V band images and fast window mode data in UVW1 ( 2400–3400 A) (all taken in June) and B band images ( 3800–4900 A) and also Grism data (all taken in August). Although OY Car was faint in both the UV and optical Grism observations, an emission line is detected at Hα. Observations were also made with each EPIC camera (PN, MOS1 & MOS2, 0.1–12 keV; Turner et al. 2001). There was a weak detection (0.05 ct s−1 back- ground subtracted) of OY Car in the RGS (0.3–2.1 keV; den Herder et al. 2001).The EPIC exposures were taken in full window mode using the medium filter. In both EPIC observations, the particle background increased significantly towards the end. The data with high background were therefore re- moved from the analysis. The resulting useful exposure and the mean background subtracted count rates are shown in Table 1: in X-rays OY Car faded by a factor of 2.1 between the two observations.In the June observations, 9 eclipses were observed in the EPIC cameras and 2 in the OM UVW1 filter in fast mode. In the August observations, 2 and 3 eclipses were observed in the EPIC PN and MOS cameras respectively and3 eclipses in the OM B filter in fast...
Observations. The Fermi-LAT data included in this paper span seven years, from 2008 August 4 to 2015 August 7. The analysis of the Fermi-LAT data was performed using the Fermi Science Tools,2 10-00-05 release. Events from the “P8 Source” event class (evclass=128) and “FRONT+BACK” 1A Fermi-LAT study of æ with an earlier data release was presented in van Heerden & Meintjes (2015).2http://fermi.gsfc.nasa.gov/ssc/ event type (evtype=3) were selected3. The “Pass 8 R2 V6” instrument response functions (IRFs) were included in the analysis. All photons within an energy range of 100 MeV–300 GeV andwithin a circular region of interest (ROI) of 10◦ radius centered on æ were considered. To reject contaminating gamma rays from the Earth’s limb, we selected events with zenith angle < 90◦.The gamma-ray flux and spectral results presented in this work were calculated by perform- ing a binned maximum likelihood fit using the Science Tool gtlike. The spectral-spatial model constructed to perform the likelihood analysis includes Galactic and isotropic diffuse emission components (“gll iem v06.fits”, Acero et al. 2016, and “iso P8R2 SOURCE V6 v06.txt”, respec-tively4) as well as known gamma-ray sources within 15◦ of æ, based on a preliminary seven yearsource list. The spectral parameters of these sources were fixed at the source list values, except for sources within 3◦ of our target. For these sources, all the spectral parameters were left free. In the phase-related analysis, photons within a specific phase interval are selected. To account for it, theprefactor parameter of the sources were scaled to the width of the phase interval. The test statistic (TS) was employed to evaluate the significance of the gamma-ray fluxes coming from the sources. The Test Statistic is defined as TS=−2 ln(Lmax,0/Lmax,1), where Lmax,0 is the maximum likelihoodvalue for a model without an additional source (the “null hypothesis”) and Lmax,1 is the maximumlikelihood value for a model with the additional source at a specified location. The larger the value of TS the more likely that an additional source is needed. TS > 25 was the threshold for inclusion in the preliminary seven year source list. TS maps in this paper are produced with the Pointlike analysis package (Kerr 2010).For the X-ray timing analysis, we derived X-ray light curves using data from Swift, Suzaku, and NuSTAR. For the Swift/XRT observations included in our analysis, we selected Photon Count- ing (PC) data with event grades 0–12 in the 0.3–10 ...
Observations. A. Formal observations shall be defined as an observation of a minimum of thirty (30) minutes that results in completion of a written observation form and is preceded by a pre- conference and followed by a post conference. A minimum of two (2) observations will be made for all teachers being evaluated. A minimum of three (3) observations will be made for teachers who may be subject to non-renewal. The first observation will be held and the conference completed on or before January 15. The second observation and a third observation (if required) will be held and the conference completed on or before May 1. There will be at least three (3) weeks between the second and third observations. No formal observation will be done within the first week a teacher is with a new class of students. Any teacher who is scheduled for three (3) observations will have the right to request that the third observation be done by a different administrator who also meets the criteria in Section 7.6.9. For each observation, the teacher shall provide a lesson plan to the evaluator at least forty-eight (48) hours prior to the pre-conference. Once the evaluator has reviewed the lesson plan, he/she will prepare a list of no more than six (6) questions drawn from the “OTES Pre-Observation Planning and Lesson Reflection Resource Questions” for the teacher to answer during the pre conference. The teacher may provide written answers to these questions. Additional questions may be asked during the conversations held between the evaluator and the teacher during the conference. The written observation form shall be provided to the teacher after the post- conference information is considered. In general, pre-and post-observation conferences will be no more than one class period in length.
Observations. I certify that: - The information in this document is true and accurate and I assume the responsibility for proving such representations. - I understand that I am liable for any false statements or material omissions made on or in connection with this document. - I agree to maintain, and present upon request, documentation necessary to support this Certificate, and to inform, in writing, all persons to whom the Certificate was given of any changes that would affect the accuracy or validity of this Certificate. - The goods originate in the territory of one or both Parties and comply with the origin requirements specified for those goods in The Korea - United State of America Free Trade Agreement. This Certificate consists of pages, including all attachments. Authorized Signature: Company: Name: Title: Date: YYYY/MM/DD Telephone :Fax:
Observations. Observations shall be both formal and informal. The number 23 of formal observations shall routinely be three (3). With agreement of both evaluatee 24 and evaluator the number may be reduced to two (2) or one (1) in cases of obviously 25 satisfactory performance by permanent employees. Additional observations shall be 26 conducted when deemed necessary by either the evaluatee or evaluator. 27