Observation of faint Be stars
The goal is the survey of faint Be star activity. The target list is extracted from the BeSS data base via ARAS Beam.
The stars selected are faintest than the magnitude V=8.0. The spectra are taken during the 2009 OHP spectroscopic school.
The spectrograph is a Lhires III configured at the minimal spectral resolution (a 150 lines/mm grating) with a 37 microns wide slit. The final spectral resolution power is R=450. The CCD camera is a QSI532 model (KAF3200ME chip, 2184 x 1472 pixels, 6.8 microns, given a spectral dispersion of 2.2 A/pixel). The telescope is an old C8 (D=0.2 m) on a Takahashi EM-200 mount (modified with a FS2 motorization, LX200 protocol). An electronic finder complete the setup (Nikon 135 mm f/2.8 objective lens + Watek 120N video camera). A simple low cost mini-PC control the whole system (model ASUS EeePC 1101HA) via Audela software.
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Left, the equipment (click on the image for enlarge). Right, morning ambiance at Observatoire de Haute Provence spectro "star party". |
Below, a sample of the observed
stars:
For more and global details, consult the BeSS data base.
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Localization
of Be stars HD14422 and HD14605 near the Perseus double cluster. Photo Valérie
Desnoux.
Spectrographic
observations during OHP spectro Star-Party (Valérie Desnoux & Christian
Buil).
Valérie observes with a 5 inch Astrophysics refractor and a Lhires
III 1200 lines/mm grating.
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