COS exposures may be obtained in either a time-tagged photon-address mode (TIME-TAG
), in which the position, arrival time, and pulse height (for FUV observations) of each detected photon are saved in an event stream, or in accumulation (ACCUM
) mode, in which only the positions of the photon events are recorded.
mode each photon is kept as a separate event in a list in COS memory. Each entry in that list contains the (x, y
) coordinates of the photon together with the pulse height of the charge cloud generated by it (for FUV observations). Time markers are inserted in the list every 32 ms by the instrument electronics. When data are processed by the ground system arrival times are assigned to the events according to the time marker preceding the event.
COS observations should be obtained in TIME-TAG
mode whenever possible because it provides significant opportunities for temporal sampling, exclusion of poor quality data, and, for the FUV, improved thermal correction (by tracking the stim-pulse positions as a function of time) and background removal (by using the pulse-height information). TIME-TAG
mode should always be used for exposures that will generate count rates of 21,000 count/s or less from the entire detector (including both detector segments for the FUV). At count rates between 21,000 and 30,000 count/s, TIME-TAG
may be used to obtain properly flux-calibrated data, but the loss of some continuous time periods within extended exposures will occur (see the discussion of the buffer time in Section 5.4
). At present, TIME-TAG
should not be used for count rates greater than 30,000 count/s. ACCUM
mode should be used for such high count-rate targets.
We recommend that TIME-TAG
mode always be used with FLASH=YES
(the so-called TAGFLASH
mode) unless circumstances prevent it (see Section 5.7.1
In FUV TIME-TAG
mode the pulse height of each photon event is recorded, along with its position and arrival time. Pulse heights are stored as 5-bit words, so their values range from 0 to 31. Post-observation pulse-height screening is useful for rejecting unwanted background events, and can often improve the S/N ratio in the extracted science spectrum. Pulse-height information is not provided by the NUV detector.
mode an image of the detector is stored in a 16-bit memory buffer. As each photon arrives from the detector the location in the buffer at coordinates (x, y)
is incremented by one. Each location can hold at most 65,535 counts; the next event will cause the value to roll over to zero. To conserve memory only a 16,384 ×
128 region of each segment is stored, as well as the regions around each stim pulse. Timing and pulse-height information are not saved, preventing the application of the data-correction techniques available in TIME-TAG
mode is designed for bright targets whose high count rates would fill the on-board buffer memory too rapidly if the data were taken in TIME-TAG
mode. In some instances one may observe a relatively bright object in TIME-TAG
mode by using the BOA instead of the PSA, but the BOA degrades the spectroscopic resolution. Starting in Cycle 23, use of the BOA will be available-but-unsupported (See Section 2.4
for further discussion of BOA usage for FUV science observations). Observers wishing to use ACCUM
mode will be asked to justify doing so when submitting their Phase II program.
images do not include the entire detector. To conserve memory photons are collected only from the stim regions and that portion of the detector actually illuminated by the target (1/8 of the full detector area, or 128 pixels in y
). Each FUV ACCUM
image fills one-half of the total COS memory, so it is possible to acquire two FUV images before dumping the on-board buffer.
images cover the entire detector. Because they are smaller, up to nine of them can be stored in the memory buffer. Unlike TIME-TAG
mode, no data may be acquired during an ACCUM
readout. NUV ACCUM
mode is thus most efficient when repeated identical observations are stored in memory, then read out all at once. (Within APT, the Astronomer’s Proposal Tool
, one may easily schedule multiple iterations of an exposure using the Number_of_Iterations
mode, the COS flight software adjusts the pixel coordinates of detected events to correct for the orbital motion of HST
. The correction (always by an integer number of pixels) is updated whenever HST
’s velocity with respect to the target changes enough to shift the spectrum by an additional pixel. This is done via a small table, computed on the ground, that lists the time of each pixel shift based on the orbital motion and the dispersion of the grating in use.
Note that ACCUM
mode exposures longer than 900 s that use the G130M or G160M gratings may blur the FUV spectra by 1 to 2 pixels (about 1/6 to 1/3 of a resolution element) since shifts are performed in pixel, not wavelength, space.
Some pulse-height information is available for FUV ACCUM
observations. A pulse-height histogram, consisting of 256 bins (128 bins for each detector segment) of 32 bits each, is dumped for every ACCUM
mode image obtained with the FUV detector. (Why 128 bins? In ACCUM
mode individual pulse heights are stored as 7-bit words, so their values range from 0 to 127.) Pulse-height data are not provided for NUV exposures.