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NIRI SV Plan

The table below summarises the pool of observations which have been defined for NIRI System Verification. The list encompasses the various NIRI observing modes with a range of observing conditions and is intended to overfill the SV time available for any given mode to provide flexibility when scheduling and in their execution (e.g. with regards to target accessibility or conditions required). As described in the SV Principles, verification will be carried out on a mode by mode basis. Modes that are not being offered in the forthcoming semester (i.e. coronagraphy and polarimetry) will have their SV postponed.

Important note: The proposed observations were developed early in the telescope commissioning phase at a time when the scheduling of NIRI SV was uncertain. The target lists therefore contain objects which may not be observable when SV observations are carried out. The SV plans may also contain observations or targets which are no longer scientifically interesting to the SV team members. Gemini staff will be working with the SV team members to update plans and choose appropriate targets. The observing modes are also overfilled to allow flexibility in executing the SV observations. The presence of a proposed observation in the SV plan does not by any means guarantee that the observation will be executed, and should not deter proposals to observe the same objects as part of the regular semester.

During NIRI commissioning, some tests were performed on targets that may be scientifically interesting. The tests were generally not end-to-end system tests, and did not meet the criteria for normal System Verification. Nevertheless, to make sure that the data are made available, we have assigned them SV numbers and entries appear in the table below (SV programs 20, 24, and 25). The data will be released with the other regular SV programs.

The table links to more information about each program (click on the program number) including specific aspects of the instrument and telescope to be verified, a summary of the possible scientific returns from successful observations, a target list and the members of the assessment team. Each program will link to the SV data and its assessment when available.

Prog. #

Status

Modes

RA (hrs)

Obs conditions2

Low bg Imaging

High bg Imaging

Wide Field Imaging

Grism Spec

Coro1

Pol1

IQ

clds

H20

sky bkg

1

 

0.05; K

         

9-16

50

50

Any

80

2

started L'

 

0.05:L',M'

       

17

20

50

50

50

3

     

1-0 S(1), 2-1 S(1), BrGamma, 3.28um

     

17

50

50

80

80

4

       

0.116;K

   

20

50

50

Any

80

5

       

0.05;H

   

9-13

80

50

Any

80

6

assessment/
released

   

J,Kp

     

16

50

50

Any

80

7

     

H,K

     

18

20

50

Any

80

8

 

0.05; FeII, PaBeta, BrGamma, H2, cont

         

10-14

20

50

Any

80

9

       

0.05 L, M

   

9-10

50

50

50

50

10

       

0.116 L, M

   

19

50

50

50

50

13

         

CH4

 

any

20

80

80

80

14

         

K,M

 

5-15

20

50

20

80

15

       

K

   

any

20

50

80

80

16

           

J,H,K

any

50

50

80

80

18

           

H2,CO,BrG

6

20

80

80

80

19

released

   

J

     

14

50

50

Any

80

20

released

   

J, H, Kp

     

20

50

50

Any

80

24

assessment

J

         

17

80

80

Any

80

25

assessment

   

J

     

13

80

80

Any

80


1 SV observations in these modes not yet scheduled.

2 See the detailed observing condition constraints for the precise meaning of the %-ile categories.


Last update November 1, 2001; Joe Jensen and Phil Puxley