HRS (decommissioned) Configurations

N.B., this information applies to the original HRS, which has been decommissioned and will be replaced by HRS-2 at a time to be determined.

HRS
See the HRS Configurations Check to see if a configuration is valid or not

HRS_ResPower_echelle_CrossDisp_fiber_skyfibers_slicer_gascell_binning

ResPower = 15k, 30k, 60k, or 120k These values set the slit width for resolving powers of 15,000, 30,000, 60,000, and 120,000, respectively
If you wish to use higher resolution modes below 4000 Å then consider using the special K configuration. This configuration has its best focus at the Ca K line. If you are interested in the higher resolution modes above 4400 Å then we suggest you don't use the special K version of the cross disperser.

echelle = blue, central, red These values set the echelle rotation angle for changing the position of the orders on the CCD, primarily to move spectral features of interest off CCD defects.
Central: Default value. It is intended to center the orders on the CCD, and yield the (theoretical) wavelengths given below in the CrossDisp table. In practice, the blaze peaks are slightly to the red side of the CCD.
Blue: Causes the wavelength approximately at the blue end of the orders to be moved to the center of the CCD. The blaze peak of the order (peak efficiency) moves near the red edge of the CCD.

Red: Causes the wavelength approximately at the red end of the orders to be moved to the center of the CCD. The blaze peak of the order (peak efficiency) moves near the blue edge of the CCD.

CrossDisp

Wavelength (Å) Wavelength (Å)

CrossDisp Begin Central End Orders CrossDisp Begin Central End Orders

316g4931K see NOTE below## *3057 4931 6793 200 124 90 600g4739K *3751 4739 5732 163 129 106

316g4931 see NOTE below## *3057 4931 6793 200 124 90 600g4739 *3751 4739 5732 163 129 106

316g5936 4076 5936 7838 150 103 78 600g5271 4275 5271 6263 143 116 97

316g6948 5095 6948 8860 120 88 69 600g5822 4814 5822 6793 127 105 90

316g7940 6114 7940 9861 100 77 61 600g6302 5316 6302 7278 115 97 84

316g8991 7109 8991 **10917 86 68 56 600g6869 5879 6869 7838 104 89 78

316g10022 8152 10022 **11757 76 61 52 600g7366 see NOTE ### 6369 7366 8375 96 83 73

600g7940 see NOTE ### 6948 7940 8861 88 77 69

600g8375 see NOTE ### 7456 8375 9406 82 73 65

600g8990 see NOTE ### 7940 8990 9861 77 68 62

600g9405 see NOTE ### 8491 9405 10362 72 65 59

*HRS+HET flux below 4000 Å drops sharply but the focus also degrades. If you wish to use higher resolution modes below 4000 Å then consider using the special K configuration. This configuration has its best focus at the Ca K line. If you are interested in the higher resolution modes above 4400 Å then we suggest you don't use the special K version.
**HRS+HET delivers very little flux above 10400 Å

## For the bluest settings of the 316g the orders get very close together and the PI is strongly urged to use the 600g which has wider order spacing and higher blue throughput!!

### The g600 grating does not have as good throughput in the red as the g316 grating. It is not advised to use this grating far out in the red.
These values set the rotation of the cross disperser to:

select which orders fall on the CCD
set how much inter-order space there is for sky fibers
The three wavelengths given above for each value of CrossDisp are the blaze (central) wavelengths of the blue-most order, the central order that falls between the two CCDs, and the red-most order.
The wavelengths given are for the echelle=central setting.
The longest wavelength observable is approximately 1050nm due to the drop in the CCD quantum efficiency.
The central wavelength of any order can be calculated from any other order of known central wavelength and order number (eg. those in the table) by using the relationship:
lambda * order = constant
eg. for 316g4931, where lambda=4931 and order=124, the central wavelength of order 150 is (4931*124)/150=4076.
The spectral coverage of a given order (its FSR or Free Spectral Range) is lambda/order number. eg. 316g4931: for order 124, lambda=4931 so FSR=39.8 Å
A filter is always used for rejecting the 2nd order of the cross disperser, and it is selected automatically.

fiber = 2as or 3as (as=arcsecond) Angular diameter on the sky of the fiber to be used for feeding light from the telescope to the spectrometer.
An important consideration for observing faint objects is that the 3as fiber collects 225% more "sky" than the 2as fibers.

skyfibers = 0sky, 1sky, 2sky The maximum number of sky fibers that can be used without order overlap depends upon the values of "CrossDisp" and "fiber". The limiting wavelengths are:
316g and 2as: 4000+ for 0sky, 5880+ for 2sky
316g and 3as: 4000+ for 0sky, 5880+ for 1sky, 7100+ for 2sky
600g and 2as: 4000+ for 0sky, 4200+ for 2sky
600g and 3as: 4000+ for 0sky, 4200+ for 1sky, 5100+ for 2sky

slicer = IS0 or IS1
0 = no slicer

1 = image slicer #1
Available when fiber=3as, skyfibers=0sky, and ResPower is one of30k, 60k, or 120k. The increase in throughput verses the 3as fiber is 41%. Or ders overlap depending upon "CrossDisp" as follows:
all 316g settings: orders overlap below 5880 Å
all 600g settings: orders overlap below 4200 Å

gascell = GC0 or GC1
0 = iodine gas cell out of beam

1 = iodine gas cell in beam

binning = 2x1, 2x2, 2x3, 2x4, 2x5, 2x6 (or 1xN) The format is (column binning)x(row binning), where
column binning is in the cross dispersion dimension
row binning is in the echelle dispersion dimension
Typical binnings for each "ResPower" are:

ResPower Binnings Recommended Binning(s)
(pixels per resolution element)

120k 2x1 (or 1x1) 2x1 (2.0)

60k 2x1 2x2 (or 1xN) 2x1 or 2x2 (4.0 or 2.0)

30k 2x2 2x3 2x4 (or 1xN) 2x3 (2.7)

15k 2x4 2x5 2x6 (or 1xN) 2x5 (3.2)

The width of the orders as a function of "fiber" is
for fiber = 2as: 13 pixels for column binning = 1
for fiber = 3as: 20 pixels for column binning = 1
NOTE: YOU PROBABLY SHOULD NOT USE COLUMN BINNING OF 1 BECAUSE YOUR READ NOISE WILL GROW TO BE SIGNIFICANT
The number of pixels per resolution element can be calculated as

(240,000)/(Resolving power)/(row binning)
Note that this value varies along the orders.

NOTE: YOU SHOULD PROBABLY USE OUR SUGGESTED BINNING; IF YOU OVER-RESOLVE THE LINE YOU WILL NOT GAIN ANY INFORMATION DUE TO FIBER SCRAMBLING; YOU WILL JUST HAVE A SQUARE PSF WITH MORE READNOISE
Example: with 2x3 binning and ResPower=30k (30,000), there are approximately 2.7 pixels per resolution element.

Example HRS configurations:
HRS_15k_central_316g7940_3as_2sky_IS0_GC0_2x5
HRS_30k_central_600g5271_2as_2sky_IS0_GC0_2x3
HRS_60k_central_316g5936_3as_0sky_IS0_GC0_2x1
HRS_120k_central_316g6948_3as_0sky_IS0_GC0_2x1

Clarifications or bug reports:

Contact Phillip MacQueen at pjm@astro.as.utexas.edu or (512) 471-1470.