deletions | additions       diff --git a/Proposed HI Observations.tex b/Proposed HI Observations.tex  index a4b45bc..af0aa1e 100644  --- a/Proposed HI Observations.tex  +++ b/Proposed HI Observations.tex 
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\section{Proposed HI Observations}  Reines Reins  et al.~(2013) identified al. (2013) indentified  151 low mass galaxies with optical signs of AGN activity. Of these, xx 39  sources are unambigous AGN displaying either broad emission lines or xx. have been identified as AGN in the BPT diagram.  Of these xx 39  sources, yy 27  are observable with Arecibo in the Spring. We have identified 29 45  primary targets for an estimated total of 13 33  hours required for high signal-to-noise observations. Our primary targets include all spring BPT AGN candidates, all broad-line or isolated BPT composites and one BPT star forming galaxy that has a high likelyhood of being an AGN.  We have also identified 65 41  secondary targets that include the remaining BPT composites  for anestimated total of 28 hours of observing time. We have included 4  additional tertiary targets for 2 57  hours of observing time. time, in case our gas fractions are underestimated.  We request a total of 43 33  hours with the Arecibo telescope to observe 98 45 primary  low mass AGN candidates.Our targets are described in the Target Selection List below.  Given our prior experience, we are confident that we will obtain high quality, high signal-to-noise spectra for our proposed observations. We will observe our target dwarf galaxy AGN candidates in the L-band wide receiver, with the spectrometer in 9 level sampling mode with 4096 channels and a 12.5 MHz bandwidth. This yields a velocity resolution of 0.66 km/s which we will center on the redshifted 21-cm line using the SDSS optically measured recession velocity. All of our target galaxies have recession velocities less than 5000 km s−1 and are unresolved by the Arecibo beam. We chose the L-band over the ALFA receiver as it has a higher sensitivity and minimizes side-lobe contamination. To mitigate any baselines issues, we will perform an associated off observation (position switching) of equal integration time for each target.  We request primarily night-time observing only in order to avoid standing waves due to solar interference which make estimating accurate baselines difficult. Using recently obtained HI data for low mass isolated galaxies, we have calibrated the relation of HI gas mass to stellar mass. Using this relation with the distances determined from SDSS redshifts, we have determined estimated integration times for all of our targets.   We have recently completed a fully automated set of reduction and measurement scripts for 21-cm emission spectra obtained at Arecibo. We will therefore reduce our new observations and measure the HI parameters of the emission lines within days of completing our observations. This expedited and automated pipleline will enable us to quickly meet our science objectives and publish our analysis and results.