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--- camera [2024/06/29 11:10] – ↷ Page moved from home:camera to camera tailspin
+++ camera [2025/01/05 06:00] (current) – tailspin
@@ Line 1: / Line 1: @@
 **Seestar Camera**
-(Needs IMX462 color sensitivity curves)
+**Nothing on this page is required Seestar knowledge.** But if you want to geek out on the details of the Seestar’s camera read on.
-**Nothing on this page that is required Seestar knowledge.** But if you want to geek out on the details of the Seestar’s camera read on.
+The Seestar’s camera is at the end of a folded light path that includes two diagonal mirrors ((Source: https://fcc.report/FCC-ID/2a7r3seestar/6801742)).
-The Seestar’s camera uses a sixth generation 2.1 megapixel Sony IMX462MC CMOS sensor with 2.9µm square pixels in a 6.46mm diagonal array. This produces a 1920 x 1080 image. It’s a color camera using a GRBG Bayer matrix.
+{{ :screenshot_2025-01-05_at_5.51.56 am.png?nolink&400 |}}
+The camera uses a sixth generation 2.1 megapixel Sony IMX462MC CMOS sensor with 2.9µm square pixels in a 6.46mm diagonal array. This produces a 1920 x 1080 image. It’s a color camera using a GRBG Bayer matrix.
 {{ :screenshot_2024-06-27_at_8.35.30 am.png?nolink&600 |}}
@@ Line 19: / Line 21: @@
 In a back-illuminated sensor, the sensor is “face down” so the light is allowed to enter the photosensitive surface from the reverse side. In this case, the sensor’s embedded wiring structure is below the photosensitive layer. As a result, more incoming photons strike the photosensitive layer and more electrons are generated and captured in the pixel well. This ratio of photon to electron production is called quantum efficiency. The higher the quantum efficiency the more efficient the sensor is at converting photons to electrons and hence the more sensitive the sensor is to capturing an image of something dim.
 {{ :sensitivitycurve.png?nolink&400 |}}
-The sensitivity curve above shows a UV / IR cut filter which only allows light from about 400 to 700 nm to reach the sensor, cutting out the near infrared, where the camera is very sensitive, which causes star bloat.
-{{ :post-9348-0-75282700-1699478723.jpg?nolink&200|}}The light pollution filter blocks all light except in two narrow bands covering OIII and Ha, both of which are predominant in nebula. Note that a lot of light is blocked, so images collected with this filter require a lot more data collection (exposure) time to produce good results. --- //[[admin@seestar.online|Tom Harnish]] 2024/06/25 10:57//
+The sensitivity curve above shows a UV / IR cut filter which only allows light from about 400 to 700 nm to reach the sensor, cutting out the IR, where the camera is very sensitive snd can causes star bloat. This filter is permanently attached to camera sensor.
+{{ :post-9348-0-75282700-1699478723.jpg?nolink&200 |}}
+The light pollution (LP) filter blocks all light except in two narrow bands covering OIII and Ha, both of which are predominant in nebula. Note that a lot of light is blocked, so images collected with this filter require a lot more data collection (exposure) time to produce good results. The LP filter is automatic selected for emission nebulae, but can be manually controlled.

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