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Obtain the sky brightness in optical B, V, and R photometric bands above Dome A site

Gattini-DomeA Goals of experiment. Obtain the sky brightness in optical B, V, and R photometric bands above Dome A site To measure the cloud cover extent during the 2009 and 2010 winter seasons Extended to 2011 by NSF To provide aurora and airglow statistics

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Obtain the sky brightness in optical B, V, and R photometric bands above Dome A site

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  1. Gattini-DomeA Goals of experiment • Obtain the sky brightness in optical B, V, and R photometric bands above Dome A site • To measure the cloud cover extent during the 2009 and 2010 winter seasons • Extended to 2011 by NSF • To provide aurora and airglow statistics • Photometry of bright target stars in field with unprecedented window function • Meet budget of ~$50k (NSF OPP/AST award) excluding logistical costs • All logistical costs provided by PRIC/China collaboration

  2. Camera, Data • 90oFoV transit camera + Optic ‘IFW’ filter wheel (B, V, R, >650nm) • Apogee Alta ‘U4000’ 2kx2k interline CCD with 7.4 micron pixels • AF DX Fisheye-Nikkor 10.5mm f/2.8G ED results in ~2.4arcmin/pix, aperture ~few mm • Continuous observations: • 100s B 30s B • 100s V 30s V • 100s R 30s R • 100s OH 30s OH • 100s dark • BIAS frame • REPEAT

  3. V sky brightness, whole season

  4. CAUTION: more work needed to assess effect of imperfect baffling (are we measuring true sky brightness or instrument performance?)

  5. Photometry

  6. ‘Cloud’ cover • Strongly suspect “cloud” equals local snow obscuration lifted by wind in many cases

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