Документ взят из кэша поисковой машины. Адрес оригинального документа : http://jet.sao.ru/hq/lizm/conferences/pdf/1996/1996_p133.pdf Дата изменения: Wed Apr 21 21:00:57 2010 Дата индексирования: Tue Oct 2 08:36:42 2012 Кодировка: Поисковые слова: comet tail

CC D detecto r o f th e Mai n Stella r Spectrograp h
G.A . Chountonov , Yu.V . Glagolevski j
Specia l Astrophysica l Observator y o f th e Russia n AS , Nizhni j Arkhy z 357147 , Russi a

Th e first result s o f usin g a ne w CC D (104 0 X 1160 pixels ) a t th e 6 m telescop e Mai n Stella r Spectrograp h (MSS ) ar e reported . Th e standar d ISD017 A CC D detector , manufacture d b y th e fir m "ELECTRON" , St.Petersburg , ha s a 65 % quantu m efficiency a t 650 0 an d a singl e readou t nois e o f 6 electrons . Th e CC D electroni c syste m wa s designe d i n th e Laborator y o f Advance d Desig n o f th e SA O RAS . Th e CC D wa s teste d for bein g use d i n spectroscop y an d magnetometr y wit h long-focu s camer a I o f MS S whic h ha d bee n use d befor e for obtainin g high-dispersio n norma l photographi c an d Zeema n spectra , an d wher e th e photoelectri c Fabry-Pero t magnetomete r (Chountonov , 1982 ) ha d bee n installed . Unde r a goo d seein g o f abou t 1 " i t wa s possibl e t o obtai n 2 0 mi n exposur e Zeema n spectr a of CV n wit h a spectra l resolutio n o f 0.1 . A series o f suc h spectr a wer e use d for investigatio n o f th e magneti c field structur e o f thi s sta r (Glagolevski j e t al. , 1985) . W e believ e tha t th e installatio n o f th e CC D o n th e long-focu s camer a allowe d u s t o improv e th e accurac y o f spectra l an d Zeema n measurement s an d increas e th e limitin g stella r magnitud e o f th e investigate d stars . Before th e Conferenc e som e spectr a o f brigh t stars , i n particula r o f Arcturus , wer e obtained . Fig . 1 show s par t o f th e spectru m o f thi s sta r wit h a hig h signal-to-nois e rati o an d a spectra l resolutio n o f 0.1 1 . Th e gratin g use d provide d a reciproca l dispersio n o f 2.6 /m m (0.04 4 /pixel) . Ther e ar e som e defect column s o n on e sid e o f th e spectru m (i n Fig . 1 thi s par t i s absent) . Th e vertica l axi s o f th e figur e show s th e numbe r o f th e registere d electron s pe r column . Wit h camer a I a sta r o f 7 for 1 hou r o f exposur e ca n b e recorde d wit h a n accurac y o f 1 % an d a spectra l resolutio n o f 0. 1 time . Fig . 2 show s a spectru m o f th e magneti c sta r Eq u (4. 7 mag ) wit h a spectra l resolutio n o f 0.1 1 . Spectr a wer e recorde d unde r ba d seein g condition s (3.5- 4 arcsec ) wit h a n exposur e tim e o f 3 0 min . Th e left spectra l lin e F e I I 614 9 i s splitte d b y a magneti c fiel d o f 4 kG . Th e first result s obtaine d wit h th e ne w CC D equipmen t sho w tha t i t ca n b e successfull y use d i n spectroscopy , magnetometr y an d spectropolarimetr y o f stars .
m

Acknowledgements . W e wis h t o acknowledg e th e financia l suppor t fro m RFB R N o 94-02-06584 an d "As tronomy " grant s (Russia) .

Reference s
Chountono v G.A. : 1982 , Thesis , SA O USS R AS . Glagolevski j Yu.V. , Piskuno v N.E. , Khokhlov a V.L : 1985 , Pis'm a Astron . Zh. , 11 , 371 .

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