Index of /~bessell/archive

Icon  Name                    Last modified      Size  Description
[DIR] Parent Directory                             -   
[   ] 2011MayWIFESb.log       23-May-2011 14:00   36K  
[   ] 2011mayb3000.tar        23-May-2011 13:17  3.9G  
[   ] 2011mayr7000.tar        23-May-2011 13:11  3.9G  
[   ] arlines_B3000.lis       23-May-2011 13:40  5.0K  
[   ] arlines_R7000.lis       23-May-2011 13:38  3.1K  

23 May 2011

2.3m 16/5/2011-22/5/2011
Partly cloudy most lights. First half of 16 & 17 given to Simon Murphy.
No observing on 22 rain.
Observed ~330 of 370 stars. All priority 1 & 2 + many priority 3 stars done.

Images are 4080x1024. Two images are 4080x2048 by mistake (336, 518)
These images are the same resolution as the other and the columns 1-1024
can be cut off to make them the same as the other images.

The spectra comprise 13 slices. The star usually fell within 3 or 4 slices.
I extracted slices 2 to 9, although 2 to 7 would have been adequate for all 
but the first night's stars. Mostly the star was in slices 3,4,5.

The blue spectra have a "readout" gap in them. This needs to be removed for
continous wavelength coverage. I make a new image with 1:2066 + 2115:4180.
The blue spectra were B3000 spectra. Included are line identifications for
slice 2 (arlines_b3000.lis). 
The red spectra also have a gap but it is smaller. The blue CCD is read out 
through 2 amplifiers, the red CCD through 1 amplifier (the others have died).
The gapless red image is 1:2109 + 2115:4180.

You need to scrunch the individual slices to the same wavelength scale in order
to add up the slices. 
There is significant tilt in the arc lines away from the central slices.
In the red and for faint stars I untilt the lines before doing sky subtraction
but do not bother to do this in the blue as only the [OI] line is in the sky. 

The arc is Fe-Ne-Ar. I include the line list fenear.arc. 
The flat field is a QI lamp so it is OK for the red but not for the blue below
3700A. Be careful with the blue flat fielding in the UV and make good use of 
the smooth spectrum star to remove artifacts of the flat field.  

I did LTT4364 as a smooth spectrum star on 20 and 21. This is a C-rich He white 
dwarf so shows no lines in the red and only weak C2-Swan bands in the blue.
Remove the Swan band absorption bands from the blue spectrum before using it as
a smooth spectrum star.   
The spectrum of EG131 on the 21 was affected by cloud and is too weak to be 
used as a smooth spectrum star.  

Several of your program stars appeared double. I neglected to record which ones 
these were but you should be able to see the duplicity as two overlapping or 
separated spectra.