CHI-3 is an ASA 1000, a 39 inch (100 cm) telescope with a Ritchey Chretien design, situated in the Rio Hurtado valley, Chile. It is equipped with a set of Astrodon astrophotography filters. This large aperture telescope is an excellent choice for both scientific applications and astrophotography of deep sky objects.
The position angle of images acquired with CHI-3 varies depending on the guiding star used for each request. The guiding star is selected automatically each time, and we are therefore not able to predict the position angle for your target. However, you can make sure that separate requests of the same object use the same guiding star, and position angle, by using exactly the same target name and coordinates (RA, Dec) during submission. You can do this by using the Resubmit request functionality. Find out more.
- 3.3 credits/min
- NGC 3603, Halpha, 600 sec. Download.
- Aperture: 1000 mm (39 inches)
- Focal Length: 6800 mm
- F-ratio: 6.8
- Mount: ASA Alt-Az Direct Drive Mount
- Minimum elevation: 30 degrees
- Model: FLI PL 16803 (spec sheet)
- Pixel Size: 9 μm
- Pixel Array: 4096 x 4096
- Pixel Resolution: 0.27 arcsec/pixel
- Field of View: 19 x 19 arcmin
- Filters(50mm square): Astrodon LRGB 2GEN, Ha (3nm), SII (3nm), OIII (3nm), Sloan r, Sloan g, Sloan i
- Available binning: 1, 2
- Position angle: Can vary depending on which guide star is used. Find out more.
- Allowed exposure times (in seconds): 180, 300, 600, 1200, 1800
- Automated calibration: Yes, the images will be provided fully calibrated in FITS format
- Observatory name: El Sauce Observatory
- Location: Río Hurtado, Coquimbo Region, Chile
- Coordinates: 30.4725° S, 70.7631° W (Google maps)
- Elevation: 1525 m
- Average seeing: 1.5'' - 2''
- MPC code: X02
This large 1 m telescope is an Alt-Az instrument equipped with de-rotators in both focuses. The field of view of guider sensor is very small, so in 90% of cases there is no guiding star on the sensor.
To deal with this we use a routine to find the suitable guiding star. The system takes a test frame, plate solves it and finds the nearest guiding star. Then it rotates the field to put the star on the guider sensor. So the Position Angle (PA) is determined by the nearest guiding star position.