ISPI Quick reference guide
Updated on July 7, 2021, 10:54 am
The Infrared Side Port Imager ISPI (eye-spy) is a facility imager at the CTIO Blanco 4-m telescope, serving a broad range of science programs through the following capabilities:
- 1-2.4 micron imaging with 2K x 2K HgCdTe HAWAII-2 array
- 0.3 arcsec/pixel sampling matched to f/8 IR image quality of ~0.6 arcsec
- 10.25 x 10.25 arcmin field of view,
- broad band J,H and Ks, as well as a set of narrow band filters.
- A list of available filters can be found on the ISPI filter page.
During the January 2003 engineering night weather permitted us to measure the throughput of ISPI at the telescope, see table. The ISPI throughput is very similar to the throughput of Flamingos at the Kitt Peak 4m. Exposure times and signal-to-noise ratios can be estimated using the exposure time calculator.
for m=15 star
|point source detection limit
5 sigma in
The HAWAII-2 array in ISPI
The array, as set-up in ISPI since May 2003, has the following performance characteristics:
- Gain: 4.25 e-/ADU
- Well depth: 150,000 e-
- Linearity: 1% full frame linear range is ~13,000 ADU's
- Minimum exposure time: 3.227s
NOTE: For data taken prior to May 2003 please consult the ISPI support staff.
Observing with ISPI
ISPI is run through a Graphical User Interface, in which all array control parameters, such as exposure time, number of co-adds, as well as filter, telescope focus and telescope off-set can be set.
The GUI can also initiate a series of observations, to conduct for example a dither sequence, a focus sequence, or a sequence of darks. These sequences are simple ASCII text files, which can be prepared in advance. Examples of such observing sequences are in the following links in H, J and K.
February 13, 2007