McCombs family buys prime real estate near Pearl, next to San Antonio Museum of Art, from CPS Energy
McCombs Family Partners Ltd. purchased 5.9 acres next to the San Antonio Museum of Art for $29.5 million from the city-owned utility this week.
“It’s not something we’re looking at,” Adams said. “We’re not going to rule anything out, but it’s not currently part of our plans.”, 95, started his real estate dealings as a young man in Corpus Christi before coming to San Antonio, Adams said. Its holdings include automotive operations and dealerships, which is the core business; McCombs Energy, which holds oil and natural gas resources; McCombs Properties, which focuses on real estate and development; McCombs Partners, which invests in companies; and a philanthropic foundation, Adams said.
McCombs Properties offered to buy more than the 3.5 acres, envisioning a development that would “create a union” between the museum and Pearl, Adams said.
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Cosmic-Ray Boron Flux Measured from $8.4\text{ }\text{ }\mathrm{GeV}/n$ to $3.8\text{ }\text{ }\mathrm{TeV}/n$ with the Calorimetric Electron Telescope on the International Space StationWe present the measurement of the energy dependence of the boron flux in cosmic rays and its ratio to the carbon flux in an energy interval from $8.4\text{ }\text{ }\mathrm{GeV}/n$ to $3.8\text{ }\text{ }\mathrm{TeV}/n$ based on the data collected by the Calorimetric Electron Telescope (CALET) during $\ensuremath{\sim}6.4\text{ }\text{ }\mathrm{yr}$ of operation on the International Space Station. An update of the energy spectrum of carbon is also presented with an increase in statistics over our previous measurement. The observed boron flux shows a spectral hardening at the same transition energy ${E}_{0}\ensuremath{\sim}200\text{ }\text{ }\mathrm{GeV}/n$ of the C spectrum, though B and C fluxes have different energy dependences. The spectral index of the B spectrum is found to be $\ensuremath{\gamma}=\ensuremath{-}3.047\ifmmode\pm\else\textpm\fi{}0.024$ in the interval $25<E<200\text{ }\text{ }\mathrm{GeV}/n$. The B spectrum hardens by $\mathrm{\ensuremath{\Delta}}{\ensuremath{\gamma}}_{B}=0.25\ifmmode\pm\else\textpm\fi{}0.12$, while the best fit value for the spectral variation of C is $\mathrm{\ensuremath{\Delta}}{\ensuremath{\gamma}}_{C}=0.19\ifmmode\pm\else\textpm\fi{}0.03$. The $\mathrm{B}/\mathrm{C}$ flux ratio is compatible with a hardening of $0.09\ifmmode\pm\else\textpm\fi{}0.05$, though a single power-law energy dependence cannot be ruled out given the current statistical uncertainties. A break in the $\mathrm{B}/\mathrm{C}$ ratio energy dependence would support the recent AMS-02 observations that secondary cosmic rays exhibit a stronger hardening than primary ones. We also perform a fit to the $\mathrm{B}/\mathrm{C}$ ratio with a leaky-box model of the cosmic-ray propagation in the Galaxy in order to probe a possible residual value ${\ensuremath{\lambda}}_{0}$ of the mean escape path length $\ensuremath{\lambda}$ at high energy. We find that our $\mathrm{B}/\mathrm{C}$ data are compatible with a nonzero value of ${\ensuremath{\lambda}}_{0}$, which
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