992 research outputs found
Detection of moisture and moisture related phenomena from Skylab
There are no author-identified significant results in this report
Detection of moisture and moisture related phenomena from Skylab
The author had identified the following significant results. Soil moisture and precipitation variations were not detectable as tonal variations on the S19OA IR B and W photography. Some light tonal areas contained high precipitation .83 inches and high moisture content 21.1% while other light tonal areas contained only .02 inches precipitation and as little as 0.7% moisture. Similar variations were observed in dark tonal areas. This inconsistency may be caused by a lapse of 3 to 4 days from the time precipitation occurred until the photographs were taken and the fact that in the first inch of soil the measured soil moisture was generally less than 5.0%. For overall tonal contrast, the aerial color, color IR and aerial B and W appear to be the best. Cities stand out from the landscape best in the aerial color and color IR, however, to see major street patterns a combination of the two aerial B and W bands and the two IR B and W bands may be desirable. For mapping roads it is best use all 6 bands. For lake detection, the IR B and W bands would be the best but for streams the aerial B and W band would be better. The aerial color, color IR, and the two IR B and W bands are best for distinguishing cultivated and non-cultivated areas, whereas the two aerial B and W bands are better for seeing local relief. Clouds may be best seen in the aerial color and color IR bands
Detection of moisture and moisture related phenomena from Skylab
The author has identified the following significant results. Data from five Skylab passes were combined to give a composite relationship between the S194 antennae temperature and soil moisture content in the surface to one inch layer. The five data sets were comparable and resulted in a correlation coefficient of -0.97. The regression equation was used to predict soil moisture content across the United States for one particular pass on August 5, 1973
Jet emission in NGC1052 at radio, optical, and X-ray frequencies
We present a combined radio, optical, and X-ray study of the nearby LINER
galaxy NGC 1052. Data from a short (2.3 ksec) {\it CHANDRA} observation of NGC
1052 reveal the presence of various jet-related X-ray emitting regions, a
bright compact core and unresolved knots in the jet structure as well as an
extended emitting region inside the galaxy well aligned with the radio
synchrotron jet-emission. The spectrum of the extended X-ray emission can best
be fitted with a thermal model with keV, while the compact
core exhibits a very flat spectrum, best approximated by an absorbed power-law
with . We compare the radio
structure to an optical ``structure map'' from a {\it Hubble Space Telescope}
({\it HST}) observation and find a good positional correlation between the
radio jet and the optical emission cone. Bright, compact knots in the jet
structure are visible in all three frequency bands whose spectrum is
inconsistent with synchrotron emission.Comment: 8 pages, 5 figures (figure 2 in color), image resolution degraded wrt
journal version, needs aa.cls. Accepted for publication in A&
Optical observations of the luminous Type IIn Supernova 2010jl for over 900 days
The luminous Type IIn Supernova (SN) 2010jl shows strong evidence for the
interaction of the SN ejecta with dense circumstellar material (CSM). We
present observations of SN 2010jl for d after its earliest
detection, including a sequence of optical spectra ranging from to
d. We also supplement our late time spectra and the photometric
measurements in the literature with an additional epoch of new, late time
photometry. Combining available photometric and spectroscopic data, we
derive a semi-bolometric optical light curve and calculate a total radiated
energy in the optical for SN 2010jl of erg. We also
examine the evolution of the H emission line profile in detail and find
evidence for asymmetry in the profile for d that is not easily
explained by any of the proposed scenarios for this fascinating event. Finally,
we discuss the interpretations from the literature of the optical and
near-infrared light curves, and propose that the most likely explanation of
their evolution is the formation of new dust in the dense, pre-existing CSM
wind after d.Comment: 14 pages, 10 figures, 5 tables. Full version of Table 3 is included
as an ancillary fil
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