NIRSPEC Calibration Lamp Exposures

Note: this page is obsolete and here only for legacy reference. The EFS gui and CAT gui take care of exposure times.

This table documents the exposure times used in the EFSgui when in "Obs. Mode - Lamps". Users who wish to take customized calibration exposure sets can use this table as a basis for exposures.

Notes:
  1. The brightness of the NIRSPEC flat lamp fluctuates on long time scales. Integration times you used a few months ago may not apply. Please test your integration times.
  2. Even the shortest itime (0.25 seconds) exposure on the arc lamps can cause persistence on SPEC. Please see the troubleshooting page for methods of avoiding and recovering from charge persistence.
  3. The terminology below is (itime(s) x coadds).
  4. The pre-defined exposure sequences are:
    • Low-resolution: Flatfield, test(flush), Off(at flat exposure level), Ne, Ar, test(flush).
    • High-resolution: Flatfield, test(flush), Off(at flat exposure level), Ne+Ar+Xe+Kr, test(flush).

Filter Low Resolution High Resolution
Flatfield Ne,Ar Flatfield Ne,Ar,Xe,Kr
NIRSPEC-1 29 x 3 0.25 x 10 59 x 3 0.25 x 10
NIRSPEC-2 29 x 3 0.25 x 10 59 x 3 0.25 x 10
NIRSPEC-3 1.9 x 7 0.25 x 10 39 x 3 0.25 x 10
NIRSPEC-4 1.3 x 7 0.25 x 10 17 x 5 0.25 x 10
NIRSPEC-5 1.5 x 7 0.25 x 10 17 x 5 0.25 x 10
NIRSPEC-6 0.25 x 10 0.25 x 10 1.5 x 7 0.25 x 10
NIRSPEC-7 0.25 x 10 0.25 x 10 3.5 x 7 0.25 x 10
BR-GAMMA(2.16) 0.25 x 10 0.25 x 10 2 x 7 0.25 x 10
CO(2.3) 0.25 x 10 0.25 x 10 2 x 7 0.25 x 10
K 0.25 x 10 0.25 x 10 3.5 x 7 0.25 x 10
K-PRIME 0.25 x 10 0.25 x 10 3.5 x 7 0.25 x 10
L-PRIME 0.25 x 10 0.25 x 10 1 x 10 0.25 x 10
M-PRIME 0.25 x 10 0.25 x 10 1 x 10 0.25 x 10
KL 0.25 x 10 0.25 x 10 1 x 10 0.25 x 10
HeI(1.08) 10 x 5 0.25 x 10 120 x 1 0.25 x 10
PA-BETA(1.28) 10 x 5 0.25 x 10 120 x 1 0.25 x 10
FeII(1.64) 1 x 10 0.25 x 10 12 x 5 0.25 x 10
H2(2.12) 0.25 x 10 0.25 x 10 2 x 7 0.25 x 10
M-WIDE 0.25 x 10 0.25 x 10 1 x 10 0.25 x 10
Last modified: 04/04/2012 01:43
Send questions or comments to:NIRSPEC Support

The information on this page is the property of the W. M. Keck Observatory. The contents of this page or any part thereof shall not be copied or otherwise reproduced or transferred to other documents or used or disclosed to others for any purpose other than observing support at the W. M. Keck Observatory and the subsequent analysis and publication of scientific data obtained from observations conducted at the W. M. Keck Observatory. All rights reserved. © W. M. Keck Observatory.