Data Set Overview
  =================
    Data
    -----
    The H-band (1.65 micron) data, consisting of 1,535 images, were obtained
    through the PISCES near-infrared camera (McCarthy et al. 2001) using 80x80
    pixel frames (14.4 arcsec on a side) at a rate of 2.5 Hz with a duty cycle
    of 70%. Analysis of the infrared dataset can be found in McCarthy et al.
    2008. Long-wavelength Density Fluctuations Resolved in Pluto's High
    Atmosphere. Astron. J. 136, 1519-1522.
 
    The visible band (unfiltered, approximately 0.24-1.24 micron) data,
    consisting of 19,200 images (contained within datacubes of 5 minute
    intervals), were obtained through the POETS (Portable Occultation,
    Eclipse, and Transit Systems; Souza et al. 2006; Gulbis et al. 2008)
    camera at a rate of 4 Hz. Analysis of the visible dataset can be found in
    Person et al. 2008. Waves in Pluto's Upper Atmosphere. Astron. J. 136,
    1510-1518.
 
    Both datasets have been bias subtracted and flatfield calibrated.
 
    Images from the other observing sites (The Large Binocular Telescope
    Observatory, USNO Flagstaff Station, Magdalena Ridge Observatory and
    Fremont Peak Observatory), for this event are not contained within this
    dataset, however lightcurve tables are included in the tables directory.
 
    Telescope and Instrument/Observation Information
    ------------------------------------------------
    MMT Observatory (originally the Multiple Mirror Telescope, but now a
    single large mirror)
    Telescope Diameter: 6.5 m
    Location: -110 53 04, 31 41 19, 2.61 km
    Instrument: PISCES, 1.65 microns (H filter), cadence ~2 Hz, S/N=490 and
    POETS, 0.24-1.24 micron (unfiltered), cadence 4 Hz, S/N=336
    Data included in this dataset: Images and lightcurve tables.
 
    Large Binocular Telescope Observatory (LBTO)
    Telescope Diameter: 8.4m
    Location: -109 53 31, 32 42 04, 3.19 km
    Instrument: Guide Camera, 0.64 microns (r' filter), cadence ~0.2 Hz, S/N =
    88
    Data included in this dataset: lightcurve table only.
 
    United States Naval Observatory, Flagstaff Station (USNO, FS)
    Telescope Diameter: 1.66m
    Location: -111 44 23, 35 11 02, 2.31 km
    Instrument: POETS, 0.24-1.24 micron (unfiltered), cadence 2 Hz, S/N=70
    Data included in this dataset: lightcurve table only.
 
    Magdalena Ridge Observatory (MRO)
    Telescope Diameter: 2.4m
    Location: -107 11 05, 33 58 36, 3.18 km
    Instrument: POETS, 0.24-1.24 micron (unfiltered), cadence 2 Hz, S/N=45
    Data included in this dataset: lightcurve table only.
 
    Fremont Peak Observatory (FPO)
    Telescope Diameter:0.32m
    Location: -121 29 55, 36 45 37, 0.84 km
    Instrument: SBIG ST-10XME, 0.79 microns (I filter), cadence 0.25 Hz, S/N=8
    Data included in this dataset: lightcurve table only.
 
    Note: The S/N in the time that the shadow moves a distance of 60 km
    (approximately one pressure scale height). This was calculated from a
    portion of the light curves outside the occultation.
 
    Lightcurve Table file descriptions
    -----------------------------------
    The columns for each of the following tables are:
    (1) Exposure midtime in seconds from 2007 March 18 10:30:00 UT
    (2) Normalized stellar flux (normalized by a portion of the light curves
    outside the occultation)
    (3) Standard error on the normalized stellar flux
 
    lbt_visible.tab is a lightcurve table generated from data acquired at the
    LBT.
 
    usno_visible.tab is a lightcurve table generated from data acquired at the
    USNO, Flagstaff station.
 
    magdalenaridge_visible.tab is a lightcurve table generated from data
    acquired at MRO.
 
    fremontpeak_visible.tab is a lightcurve table generated from data acquired
    at the FPO.
 
    mmt_infrared.tab is a lightcurve table generated from data acquired at the
    MMT in the infrared.
 
    mmt_visible.tab is a lightcurve table generated from data acquired at the
    MMT in the visible.
 
    Additional Table file descriptions
    -----------------------------------
    The columns for each of the following tables are:
    (1) Image filename
    (2) Approximate x-position on the image of P445.3 in pixel space.
    (3) Approximate y-position on the image of P445.3 in pixel space.
 
    mmt_infrared_positions.tab is a table of approximate positions on the MMT
    infrared images.
 
    mmt_visible_positions.tab is a table of approximate positions on the MMT
    visible images.
 
 
    References
    -----------
    Gulbis, A. A. S., J. L. Elliot, M. J. Person, B. A. Babcock, J. M.
    Pasachoff, S. P. Souza, & C. A. Zuluaga, 2008, in The Universe at
    Sub-Second Timescale, High Time Resolution Astrophysics, Recent Stellar
    Occultation Observations Using High-Speed, Portable Camera Systems, ed. D.
    Phelan, O. Ryan, & A. Shearer (Edinburgh: American Institute of Physics),
    91.
 
    McCarthy, D.,  J. Ge, J. Hinz, R. Finn, & R. de Jong, R. 2001, PISCES: A
    Wide-Field, 1-2.5 micron Camera for Large-Aperture Telescopes. PASP, 115,
    353.
 
    McCarthy D. W., C. A. Kulesa, W. B. Hubbard, S. D. Benecchi, M. J. Person,
    J. L. Elliot, A. A. S. Gulbis. 2008, Long-wavelength Density Fluctuations
    Resolved in Pluto's High Atmosphere. Astron. J. 136, 1519-1522.
 
    Souza, S. P., B. A. Babcock, J. M. Pasachoff, A. A. S. Gulbis, J. L.
    Elliot, M. J. Person, & J. W. Gangestad, 2006, POETS: Portable
    Occultation, Eclipse, and Transit System. PASP, 118, 1550.
 
    Person, M. J., J. L. Elliot, A. A. S. Gulbis, C. A. Zuluaga, B. A.
    Babcock, A. J. McKay, J. M. Pasachoff, S. P. Souza, W. B. Hubbard, C. A.
    Kulesa, D. W. McCarthy, S. D. Benecchi, S. E. Levine, A. S. Bosh, E. V.
    Ryan, W. H. Ryan, A. Meyer, J. Wolf, and J. Hill 2008, Waves in Pluto's
    Upper Atmosphere. Astron. J. 136, 1510-1518.

Confidence Level Overview
  =========================
    The data were obtained at airmass (~3). The S/N in the time that the
    shadow moves a distance of 60 km (approximately one pressure scale height)
    is 490 for the IR dataset and 336 for the visible dataset. This was
    calculated from a portion of the light curves outside the occultation. The
    lightcurve datatables have been normalized to correct for trends in the
    data that are specifically background related.