One of the most frequently asked questions is the existence of planets outside our galaxy, many astronomers answer yes, but it cannot be affirmed until they find one. M51-ULS-1b is the first candidate exoplanet to be found because it produces a complete eclipse. It has a radius more likely to be smaller than Saturn. This planet candidate orbits in one of the most X-ray emitting galaxies, M51. Each galaxy occupies such a small space in the sky that this prevents us from investigating things in more detail. Galaxies have very small numbers of bright X-ray sources (XRS), the XRS of galaxies are binaries (XRB) in which black holes (BH) or neutron stars (NS), the remains of massive stars and matter accretion. M51-ULS-1b is also the first candidate because it blocked the X-rays of the XRB M51-ULS-1 completely for about 30 minutes. There is a lot of excitement to discover new planets in outer galaxies. The identification of X-ray trajectories is the only method for finding planets at great distances, and for the planets discovered by this method we know and can study the system orbited by the star. M51-ULS-1 is an ultra-bright X-ray source. Optical observations detect that the XRB is still young and cannot be compared to a white or brown dwarf star. A search has been carried out with the Chandra space telescope to detect XRS light trails in three different galaxies: M51, M101 and M104. These light corbes were already available because they were studied for another purpose. The exhaustive search through the light corbels of M51, M101 and M104 identified only one transit candidate, which leads to the conclusion that traces can be found or that the profiles of these traces do not have characteristics in common, but the aim was to find a strong candidate in order to submit it to a sequence of further tests. The X-ray source giving the apparent transit is M51-ULS-1, one of the brightest XRS in M51, to give us an idea, it is about 105 or 106 times brighter than the sun at X-ray emission at all wavelengths combined, this rate was large enough to start investigating further. The optical observations of M51 provide clues about the age of M51-ULS-1, a good indicator of the age of M51-ULS1b, since the latter is likely to have been formed with the binari, or at the birth of the binari group. M51-ULS-1b is much younger than can be observed. The X-ray light corbels exhibit variability of many types. Bengals, long Long lasting highs and/or lows are observed, as well as short lasting falls. which are not transients. Therefore, it is important to compare the event with other events We identify ourselves with others, in order to determine whether its characteristics are different from those of others. The characteristics distinguish it from other immersion events. X-ray telescopes not only count the amount of photons received, but also record the energy of each incoming photon, so that we can explore how photons behave. explore how low-energy ("soft") photons behave compared to higher-energy ("soft") photons. In addition to the variations caused by the passage of matter through the XRS, the XRBs exhibit a wide variability. The measurement of an object is a powerful indicator of its nature. The orbit of the transiting mass determines its position relative to the XRB and allows us to assess whether it can survive the flux inflow, as well as whether it would have been possible for the candidate planet to survive the evolution of the XRB so far. The orbit measurement and orbital period are also incorporated into the calculations of the transit detection probability. For a binary orbit, it is easy to determine the value of the velocity, the distance of M51-ULS-1b from the centre of the mass bin at the moment of transit, because the value of velocity is measured from just the short eclipse. The most probable velocity value, the mode of the distribution, is 17 km/s, and the uncertainty limits of 68% are at 8 km/s if 34 km/s. We know that the existence of planets in wide orbits is plausible, because planets with orbits that have half circles larger than the range of tens and hundreds of AU are common among Galactic exoplanets. Although there is little detail on the binary X-rays, M51-ULS-1 had an interesting history. The key elements were discussed and it was concluded that a planet with a wide orbit could survive. M51-ULS-1 underwent an earlier phase of activity during which the star that evolved into today's compact creditor was active. This star may have transferred mass to its companion, but the companion was not compact; less accretion energy would have been released per unit mass than is released today. The evolution of the star would have been even larger, but it would have had consequences for an orbiting planet. What is the likelihood of observing the transit of a small object in the our data set? In answering this question, we can use the detection of M51-ULS-1b to estimate how many objects the size of a planet are likely to be orbiting the X-axis. Orbiting the XRBs, observations of which comprise our data set. In conclusion, it is likely that different groups of researchers will emerge from the discovery that has been made that can provide a new discovery of different characteristics of the exoplanet and also of the orbit in general, and more to the corbels of light. This is very important to develop better statistics. It is up to the current generation of X-ray telescopes to develop information about the population of planets orbiting the XRB and for future generations of XRBs and future generations of instruments to develop a more internal view. The discovery of M51-ULS-1b has established that external galaxies may have planetary candidates and also demonstrates that X-ray studies can reveal the presence of systems that would otherwise be invisible.