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\@writefile{lof}{\contentsline {figure}{\numberline {1}{\ignorespaces  M33 mapped in HI line emission with Half Mile Telescope. K. Newton, 1980}}{6}}
\@writefile{lof}{\contentsline {figure}{\numberline {2}{\ignorespaces \relax \fontsize  {10.95}{13.6}\selectfont  \abovedisplayskip 11\p@ plus3\p@ minus6\p@ \abovedisplayshortskip \z@ plus3\p@ \belowdisplayshortskip 6.5\p@ plus3.5\p@ minus3\p@ \def \leftmargin \leftmargini \parsep 5\p@ plus2.5\p@ minus\p@ \topsep 10\p@ plus4\p@ minus6\p@ \itemsep 5\p@ plus2.5\p@ minus\p@ {\leftmargin \leftmargini \topsep 9\p@ plus3\p@ minus5\p@ \parsep 4.5\p@ plus2\p@ minus\p@ \itemsep \parsep }\belowdisplayskip \abovedisplayskip \baselineskip 1.5\baselineskip \relax  M33 velocity field mapped in HI line emission with Half Mile Telescope}}{7}}
\@writefile{lof}{\contentsline {figure}{\numberline {3}{\ignorespaces  M81 and M82 mapped in HI line emission with Half Mile Telescope. G. Cottrell, 1977}}{8}}
\@writefile{lof}{\contentsline {figure}{\numberline {4}{\ignorespaces Allen Telescope Array 2000-2011. 42 antennas, with 4 simultaneous RF bands in the range 0.7 to 11 GHz. 4 100 MHz bandwidth, 1000 channel correlators, 3 beamformers. Used for radio surveys, HI in spiral galaxies, radio transient surveys, SETI.}}{9}}
\@writefile{lof}{\contentsline {figure}{\numberline {5}{\ignorespaces M31 HI distribution imaged with the Allen Telescope Array. 7-pointing mosaic with 8 hours per pointing. Garrett Keating, UCB.}}{10}}
\@writefile{lof}{\contentsline {figure}{\numberline {6}{\ignorespaces \relax \fontsize  {10.95}{13.6}\selectfont  \abovedisplayskip 11\p@ plus3\p@ minus6\p@ \abovedisplayshortskip \z@ plus3\p@ \belowdisplayshortskip 6.5\p@ plus3.5\p@ minus3\p@ \def \leftmargin \leftmargini \parsep 5\p@ plus2.5\p@ minus\p@ \topsep 10\p@ plus4\p@ minus6\p@ \itemsep 5\p@ plus2.5\p@ minus\p@ {\leftmargin \leftmargini \topsep 9\p@ plus3\p@ minus5\p@ \parsep 4.5\p@ plus2\p@ minus\p@ \itemsep \parsep }\belowdisplayskip \abovedisplayskip \baselineskip 0.85\baselineskip \relax  The CARMA 23-element interferometer at Cedar Flat. Heterogeneous array with six 10 m, nine 6 m, and eight 3.5 m antennas providing projected antenna spacings from 3.5 m to 2 km. Receivers at 1cm, 3mm, and 1.3 mm. 4 GHz bandwidth correlator providing 16 spectral windows. Used for imaging star formation regions, galaxies, planets, protoplanetary disks, molecular clouds, galaxy clusters. Recent 1.3 mm VLBI using telescopes in Arizona, California and Hawaii with phased arrays at CARMA and SMA detected 30 microarcsec structure in the 4 million solar mass Black hole at the Galactic center.}}{11}}
\@writefile{lof}{\contentsline {figure}{\numberline {7}{\ignorespaces CO images of nearby spiral galaxies observed with CARMA by Koda et al. Most were observed with a 19 point mosaic, providing a field of view of 2.3 arcmin and a resolution of 3 arcsec.}}{12}}
\@writefile{lof}{\contentsline {figure}{\numberline {8}{\ignorespaces HCN, OH, NH3 emission in the Galactic center. BIMA and VLA 19 point mosaic images}}{13}}
\@writefile{lof}{\contentsline {figure}{\numberline {9}{\ignorespaces 1.3 mm continuum map of Orion-KL, with spectra of Source I and BN. Red contours (18--320 mJy/beam) show a $0.25''$ resolution map; halftone image is with $0.85''$ resolution. The H30$\alpha $ recombination line is prominent in the spectrum of BN, but isn't detected toward Source\nobreakspace  {}I. A vibrationally excited transition of water is, however, detected in Source\nobreakspace  {}I for the first time.}}{14}}
\@writefile{lof}{\contentsline {figure}{\numberline {10}{\ignorespaces  Paired Antenna Calibration System using 3.5 m antennas at 30 GHz. The 3.5\nobreakspace  {}m antennas are paired with 6.1 and 10.4\nobreakspace  {}m antennas making science observations at millimeter wavelengths. The 3.5\nobreakspace  {}m antennas simultaneously observe calibration sources in the 1 cm band. For calibration sources within a few degrees, the millimeter wavelength observations of the science target source, and the observations of the calibrator at 1cm, sample similar atmospheric phase fluctuations, allowing us to correct for the atmospheric phase fluctuations on long baselines at millimeter wavelengths.}}{15}}