Index of /~bessell/FTP/gaia

 Name                    Last modified      Size  Description
 Parent Directory                             -   
 2012Novechelle.log      27-Nov-2012 20:44   11K  
 gaia_echelle.tar.gz     27-Nov-2012 22:02  318M  

All the program stars were observed. 

The setup provides  11 orders with the 79 gr/mm echelle from 35 to 25.
Halpha is in the second order from the top (#34).
The Ca triplet is in the order second from the bottom (#26).
The arc is ThAr.
The spectrum is reversed left to right.

The log file is 2012Novechelle.log

16-22 are for FF lamp attached to instrument
26-28 are for twilight sky
72-91 are for FF lamp attached to instrument
92 - 100 are dome flats - low intensity not useful
109 - 124 dome flats long exposures OK
205 - 223 dome flats long exposures OK

I also did two exposures of spectrophotometric standards,
some fast rotating hots stars as "smooth spectrum" stars
and some radial velocity standards.

"HR1757"   05 19 59.0 -12 18 54   ! HR1757 "smooth" fast rotator
"HR8858"   23 17 54.1 -09 10 50   ! HR8858 "smooth" fast rotator
"HR1829"   05 28 14.7 -20 45 34   ! V=2.84 RV std -13.5 G5II
"HR3145"   08 02 15.9 +02 20 04   ! V=4.39 RV std +70.9 K2III
"HR911"    03 02 17.0  +4 05 17   ! V=2.53 RV std 
"BS7950"   20 47 40.5  -9 29 45   ! A1V 3.778 -0.001  0.029 -0.005 -0.010 ep Aqr
"BS1544"   04 50 36.7  08 54 01   !A1Vn 4.355  0.02  -0.03   0.014  0.039 pi Ori
 
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There is significant fringing in the order containing the Ca triplet.
I had not realised that it was so bad as I had not worked this red before.
There is a lot of scattered light in the instrument, especially visible 
between the orders in the flat fields. You will need to remove this to
flat field correctly. The internal lamp did not seem to remove the fringes 
very well. The dome flat did a better job. However I did not remove the 
scattered before dividing so that step should produce a better result.
The total counts per pixel from the 15 dome flats was about 35000.

------------------------------------------------------------------------------
Starting line IDs
Line identification in order 26 (x reversed)
      Channel   Wavelength   Calculated  Discrepancy  Line#
     166.3593    8478.3584    8478.3613       0.0029      1    
     258.5106    8490.3066    8490.3213       0.0146      2    
     500.5818    8521.4385    8521.3926      -0.0459      3    
     912.9249    8573.1211    8573.1758       0.0547      4    
    1178.5211    8605.7764    8605.7803       0.0039      5    
    1299.3500    8620.4600    8620.4209      -0.0391      6    
    1698.4974    8667.9404    8667.9492       0.0088      7 

line identification in order 34 (x reversed)
      Channel   Wavelength   Calculated  Discrepancy  Line#
      63.3921    6490.7373    6490.7119      -0.0254      1    
     627.3649    6538.1118    6538.3472       0.2354      2    
     795.5715    6554.1602    6553.9297      -0.2305      3    
    1111.7754    6583.9058    6583.8257      -0.0801      4    
    1161.6134    6588.5396    6588.5420       0.0024      5    
    1193.3696    6591.4844    6591.5410       0.0566      6    
    1708.8270    6638.2212    6638.3521       0.1309      7    
    1725.9540    6639.7402    6639.8115       0.0713      8    
    1770.6957    6643.6982    6643.5845      -0.1138      9    
    1983.1193    6660.6758    6660.6016      -0.0742     10    
    2003.7838    6662.2686    6662.1689      -0.0996     11    
    2030.5995    6664.0508    6664.1772       0.1265     12    
  
line identification in order 33 (x reversed)
      Channel   Wavelength   Calculated  Discrepancy  Line#
      51.6319    6677.2822    6677.2461      -0.0361      1    
     120.2989    6684.2930    6684.3345       0.0415      2    
     466.0633    6719.1997    6719.2119       0.0122      3    
     806.2533    6752.8340    6752.7690      -0.0649      4    
     947.4620    6766.6118    6766.6602       0.0483      5    
    1960.1033    6871.2891    6871.2881      -0.0010      6    
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