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2012Novechelle.log 27-Nov-2012 20:44 11K
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gaia_echelle.tar.gz 27-Nov-2012 22:02 318M
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оригинального документа
: http://www.mso.anu.edu.au/~bessell/FTP/gaia/
Дата изменения: Unknown Дата индексирования: Sun Feb 3 09:14:17 2013 Кодировка: Поисковые слова: п п п п п п п п п п п п п п п п п п п |
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.
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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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