Epsilon Aurigae Aurigae College of San Mateo Science Center & Planetarium College of San Mateo Science Center & Planetarium Lunar eclipse 10-27-07.

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Presentation transcript:

Epsilon Aurigae Aurigae

College of San Mateo Science Center & Planetarium College of San Mateo Science Center & Planetarium Lunar eclipse

Imaging : Deep sky PlanetaryPhotometrySpectroscopyVideo Imaging : Deep sky PlanetaryPhotometrySpectroscopyVideo

Equipment: Losmandy G-11-excellent tracking. -good signal -5 min. exp. ST7-XME CCD -SGS matched, guide chip. SBIG-SGS A/pix x765. -Oriented E/W

Software: TheSky 6 -accurate mount control CCDSoft -image acquisition Maxim DL -image reduction (darks) Iris, Vspec, IRAF -spectra processing

Calibration spectra: Calibration spectra: Blue=mercury 4358, px. 236 Blue=mercury 4358, px. 236 Red=neon 6402, px. 332 ( SGS micrometer) Red=neon 6402, px. 332 ( SGS micrometer) Exp.=Merc=180s Neon=90s(autodarks) Exp.=Merc=180s Neon=90s(autodarks)

Imaging: 2 Stars: eps Aur & HR1544 ConnectST7 SyncSky6 Focusmanual Calibrateguider Testexposure

Imaging: Imaging: 1st calibration spectra: red or blue. Image 1st star: eps Aur or 1544, 5 min. Slew/image 2nd star: same wavelength. 2nd cal. spectra: re-image both stars. All images: x2 Dark frames: x10

Processing: IRAF Starting point for analysis: Raw eps Aur / red. Intensity level vs. pixel number.

Raw HR1544 / red. Standard star, used to flux calibrate eps Aur. -Taken the same night. Processing: IRAF

Flux calibrated epsilon Aurigae in red. Intensity vs. wavelength.

Magnified view of the hydrogen alpha line of Almaaz. March 30, 2009

Epsilon Aurigae - A Spectral Investigation. Summer 2009 Citizen Sky Workshop

Red Blue3-2-09