First PANIC results: A stellar burst reveals the formation mechanism of massive stars
Panoramic field of view of 30x30 arcmin
Footprint ideally suited for single large objects
The detector is an array of four Hawaii-2RG detectors. The inter-chip gap between the detectors is only 167 pixels (or 75 arcsec at the 2.2m telescope) and is filled by dithering with sufficient amplitude. For applications which image only 30x30 arcmin this design is ideal.
For full details about the detectors performance and characterization, see this document.
Panic has cold field and pupil stops in order to reduce thermal background.
The HAWAII-2RG detector can be operated with a pixel clock of 100 kHz or 1 MHz.
Furthermore, on fast read-out mode, subwindows frames can be read a higher frame rate, for example:
-> Subwindow of 15''x15'' (34x34px at 2.2m telescope)
34 x 34 x 10µs = 11,56 ms @ 100kHz
34 x 34 x 1µs = 1,156 ms @ 1MHz
And if we spread the window area on two outputs channels, the readout will speed up twice since two AD converters operate in parallel:
17 x 34 x 10µs = 5,78 ms @ 100kHz
17 x 34 x 1µs = 0,578 ms @ 1MHz
PANIC has a pipeline software package (PAPI) with can be run in two modes: one quick which supply the observer with reduced quick-look (PQL) data to judge and optimize the observations, and a science pipeline mode which reduces the data after end of observations with all available calibrations and science data.
|2.2m Telescope||3.5m Telescope|
|FOV||30x30 arcmin||15x15 arcmin|
|Pixel scale||0.45 arcsec||0.225 arcsec|
|Detector||4x4k mosaic of 4 HAWAII-2RG (2x2kx2k)||4x4k mosaic of 4 HAWAII-2RG (2x2kx2k)|
|Standard broad band filters||Z, Y, J, H, Ks||Z, Y, J, H, Ks|
|Narrow band filters||H2, Br-gamma||H2, Br-gamma|
|Intrinsic image quality||80% EE||80% EE|
The following limiting magnitudes are expected (to be finally replaced with real ones) for seeing = 1 arcsec, 1 hour integration time, 5 sigma detection, point sources: