- 2016B Programs and Schedule Announced
- Gemini Home
- Telescopes and Sites
- Science Visitors at Gemini
- Observing With Gemini
- Retired Instruments
- Status and Availability
- Nod and Shuffle
- Spectroscopy Overview
- Long-slit Spectroscopy
- Multi-Object Spectroscopy
- Integral Field Spectroscopy
- ITC, Sensitivity and Overheads
- Guiding Options
- Observation Preparation
- Data Format and Reduction
- Visiting Instrument Policy
- Visiting Instrument Telescope Interfaces
- DSSI Speckle Camera
- TEXES (North)
- Integration Time Calculators
- Magnitudes and Fluxes
- Near-IR Resources
- Mid-IR Resources
- Observing Condition Constraints
- Performance Monitoring
- SV/Demo Science
- Future Instrumentation & Current Development
- Queue and Schedules
- Data and Results
- Gemini Research Staff
Change page style:
Defining a N&S Observation
In this section we outline a few definitions and features of a GMOS Nod & Shuffle observation.
Cycle: A Nod & Shuffle cycle is defined as the smallest useful quantity in the Nod & Shuffle exposure. In theory, this is one exposure in the target position and one exposure in the sky position.
A = B: The exposure time in the target position during one cycle is defined as A. The exposure time in the sky position during one cycle is defined as B. For Nod & Shuffle observations with GMOS the exposure time A will always be equal to B.
A is even: Because of the slightly uneven performance of the GMOS blade-type shutter, Nod & Shuffle exposures are always taken in pairs in order to preserve photometry. Therefore, the exposure time A must be an even integer number of seconds.
B/2, A/2, A/2, B/2: In order to obtain the best sky subtraction, the sky exposure brackets the target exposure. Therefore, each Nod & Shuffle cycle with exposure time A is composed of 4 equal length sub-exposures taken in the following order - sky, object, object, sky.
Observation: A Nod & Shuffle observation is defined to have a set number of cycles, each with observing time A. Therefore, the total observing time (total open shutter time) for a Nod & Shuffle observation with a number of cycles C is equal to 2 × A × C.
Shuffle distance: The shuffle distance defines the height of the bands (or the length of the slits for micro-shuffling). Normally, the shuffle distance is a positive number, the sign determines whether the charge is shuffled up or down for the sky exposures. The object is always observed with the charge in the normal (no shuffling) configuration. For a positive shuffle, the resulting spectral images will have the sky spectrum located beneath the object spectrum with a separation equal to the shuffle distance. The shuffle distance is always specified in unbinned pixels, regardless of whether or not the spectral data is binned in the y-direction. For example, for a single-band Nod & Shuffle observation the shuffle distance is +1536 pixels (for e2v at GN) and +1392 pixels (for Hamamatsu at GS); for a micro-shuffled image with 1 arcsec slits the shuffle distance is 14 pixels (GN) and 12 pixels (GS). However, if the spectral data is binned in the y-direction, one must make sure that the shuffle distance is a multiple of the binning (e.g., one cannot have a shuffle distance of 21 pixels if binning by 2 in the y-direction, but a shuffle distance of 20 or 22 pixels would be acceptable).
Hamamatsu CCDs: charge traps are not an issue. It is no longer necessary to use these type of Darks with these detectors for charge traps removal.
E2V CCDs: The presence of local defects (charge traps) in GMOS detectors #2 and #3 lead to low-level horizontal stripes in Nod & Shuffle spectral images. There are two approaches to minimizing the effects of these defects. Since semester 2003B we have provided a special kind of dark exposure for Nod & Shuffle. Taking these dark exposures is very time consuming, and they are therefore only guaranteed to be made available for the following Nod & Shuffle configurations:
- A=60, 15 cycles, shuffle distance=31 pixels, CCD binned 2x1
- A=60, 15 cycles, shuffle distance=70 pixels, CCD binned 2x1
- A=60, 15 cycles, shuffle distance=1536, CCD binned 2x1
Any Nod & Shuffle darks defined by PIs in their Phase II proposals other than the above configurations will be taken on a best-effort basis. The Nod & Shuffle darks are effective for correcting for most of the effect of the defects. However, for very deep observations it is recommended to also translate the detector between Nod & Shuffle observations by ± a few pixels in the y-direction. This allows the defects to be removed in the data reduction stage via a suitable rejection algorithm. Nod & Shuffle programs that aim to go very deep should have their observations split into at least three dithered exposures. The translation of the detector must be defined by the PI in the OT using a GMOS sequence to change the DTA-X offset.
Baseline calibrations: For Nod & Shuffle programs all baseline calibrations are taken in exactly the same manner as for classical long-slit and MOS spectroscopy programs. Additional calibrations or calibrations taken in Nod & Shuffle mode must be requested explicitly in Phase I and Phase II proposals and Nod & Shuffle Darks must be defined by the PI in their Phase II OT program.