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Seeing Stars
Here is the output from a CCD Camera from a star tracker, identify as many stars as you can! (in image reference coordinates) Note: The camera prints pixels in the following order (x,y): (0,0), (1,0), (2,0)... (0,1), (1,1), (2,1)…
Present this ticket when connecting to the challenge:
Don't share your ticket with other teams.
Connect to the challenge on stars.satellitesabove.me:5013 . Using netcat, you might run nc stars.satellitesabove.me 5013
Your team's flag for this challenge will look something like flag{victor624juliet:a bunch of unguessable stuff} .
Flag: flag{…} Statistics
Stellar CCD aperture photometry is the technique of extracting information about the brightness of stars from a series of images collected over time. The light curve of a variable star can reveal useful information about the physics of the star, including a measure of its intrinsic brightness. Light curve analysis can yield information about eclipsing binary systems, and also lead to exoplanet discoveries when a planet alters the brightness of a star by crossing its disk as viewed from Earth.
In CCD photometry, we want to be able to determine a measure of the amount of radiation coming from a given star arriving on our CCD detector. Plotted as a function of time, this measurement can reveal important information about the star or star system.
We must make some assumptions about the images in order to compare them against each other. We calibrate the image frames by doing the following:
Subtracting dark frames (removes thermal noise) Subtracting flat frames (removes illumination variation) Aligning image frames (allows photometric comparison across multiple images) These steps allow us to compare different stars across a CCD field and get accurate magnitude comparisons. Bias noise associated with reading the CCD array is automatically subtracted out by the main photometry computation.
Technique First, divide the area around our star into three regions:
Solution: kandi3kan3
ticket{victor624juliet:GLokOngLOluXVb4dQizz9cmvj8s-3UVmrjWWG0sb8v19OKnXs8ZCc4El6KqEDs8byQ}
8,12
44,25
47,43
46,78
49,96
53,123
72,98
88,106
111,74
123,49
12,90
31,41
42,88
44,60
69,48
78,90
77,110
88,45
98,29
117,60
27,51
49,29
64,6
66,76
79,42
82,113
95,36
97,87
102,104
113,36
13,49
17,32
29,9
29,56
42,36
48,56
55,82
65,23
87,15
100,99
5,36
16,85
15,123
28,62
35,100
52,104
91,92
110,44
115,7
123,85
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