To accurately complete the experiment, a computer with internet access was required. Additionally, an account on itelescope.net and AAVSO were needed. To be able to take photos on the telescope you must pay for credits, and certain telescopes require a certain amount of credits to function. To use the photometry tools on AAVSO, you must pay for a membership, which varies in cost. A stargazing guide or searching the internet for extrasolar planet transit times to be able to have accurate data is also necessary. Knowledge on how to navigate the websites is integral. When itelescope.net is logged on to it provides information such as the telescopes listed to a specific location, whether these telescopes are on or in use, the weather in the specific area, and whether it is daytime or night time. Next, the desired telescope is selected. In the first slot, the name of the star or object that you are attempting to photograph and detect must be written. In the right ascension space, one must search the internet or use your stargazer’s guide to find the right ascension of the desired object. Convert this into a decimal number, so it will be properly centered on the image. To do this, keep the hours measurement, but divide the seconds by 60 to determine how many minutes that equals. Add this on to the minutes and divide that by 60 as well, and this will give you the correct right ascension number for this purpose. (i.e. Our right ascension was 17h 52m 07s. 7/60= 0.1166+52= 52.1166/60=0.86861. The final right ascension to be entered into the telescope is 17.86861). To determine the declination, the same process must be completed. To determine the best duration, multiple tests were completed to determine the photo would not be too saturated and that it had enough time to get a good image. It is best to have multiples of 60 seconds. For the filter, the best one for converting to vPHOT and measuring the magnitude is the V filter. The binning should be left at one for this purpose because a higher binning could cause the image to become more pixilated upon enlargement. To begin this research, first understand at variable star photometry and watch tutorials for the program VPHOT (Mogul, Ken screencast.com, 2010) to learn what each gauge and number meant and to become familiar with the technology. Practicing sequencing the magnitudes of variable stars on vPHOT using a variable star, such as S. Leo is extremely helpful. To do this, one must log on to AAVSO and determine which object will be worked with. From here, the photometry report can be viewed which contains all the information that needs to be displayed in one space and comparison stars may be eliminated to help provide a more accurate display of magnitude and other measurements. The comparison stars in red have a high error, which means their magnitudes are not well known. This pollutes the image and makes the magnitude of the measured object different, so getting rid of those stars for the measuring process is best. After a precise measurement is determined, the data was recorded. When our tests of the program were accurate and successful, we chose to focus on detecting the extrasolar planet TrES-3b, which orbits the star TrES-3. Then pictures were taken of TrES-3b. To do this, the right ascension (17.86861) and the declination (37.5461) were calculated using the same process as described previously. Next, the Universal time and Local Sidereal Time were determined, through the internet. Universal time is a standard time kept according to the Greenwich Meridian (longitude zero) (Astronomical Applications Department of the U.S. Naval Observatory, 2011). Local Sidereal Time is the hour angle of the vernal equinox, or a measure of the earth’s rotation in relation to the stars, as opposed to the sun (U.S. Naval Observatory, 2011). These values were entered into the telescope settings on the computer. A Stargazer’s almanac was used to determine the time at night that the right ascension of the extrasolar planet could be seen from the location of the telescope. At the time this was completed, the optimal time was between 1am and 2am Mountain Daylight Time (UTC-7:00). Although this was the most superlative time to view TrES-3b, we could not find any transits at that time. The times of transit for TrES-3b were determined using jefflcoughlin.com/transit.html which is a website that provides educated predictions as to when an extrasolar planet will transit. This website requires the latitude and longitude coordinates of the telescope, which can be found on itelescope.com, and the Julian Date. The Julian dates are a continuous count of days since noon Universal Time on January First, 4713 BCE (on the Julian Calendar) (Astronomical Applications Department of the U.S. Naval Observatory, 2011). After the next transit time was determined, we reserved time on the telescope for July 3rd, 2014 at 10:00 pm Mountain Daylight Time. We used Telescope 24, which is a deep space telescope in Sierra Nevada Mountains, CA, USA. That night three photos of different exposures were taken to test saturation: one that was 120 seconds long, one that was 180 seconds long, and one that was 300 seconds long. Then, 14 photos were taken before and throughout transit. These photos were uploaded to vPHOT using a program called Core FTP. Essentially, the photos taken on the telescope were saved and uploaded to this program that automatically adds the images to vPHOT. Through looking at the saturation levels, this set of photos was inconclusive and contained disadvantageous results. For the next trial, 21 photos of TrES-3b were taken, keeping constant with the exposure tests and photos taken before, throughout, and after transit. This was completed on July 9th, 2014 at 3am Mountain Daylight Time. Once the photos were uploaded, the saturation levels were observed and determined this data set was nearly infallible. Universal time was compared against the magnitudes. The magnitude was taken twice, once with one comparison star, and the second time with one comparison star and one check star. These different magnitudes were entered into separate excel spreadsheets and these were split into three data sets: one before transit, one during transit, and one after transit. These were graphed on the same plane, but in separate colors. The Y values and the R2 values were found and a line of best fit for each before set of data and after set of data was graphed. We then solved for the slope of both of those lines to find the margin of error. The slopes were compared to determine which values were the closest. The graphs were observed to try and determine if the trial was successful and the magnitude dip during transit was detectable. The percentage drop in magnitude was calculated. Then the varying magnitudes were studied and it was asserted that variable star photometry is a viable method for determining the presence of an extrasolar planet in relation to its variable star.