version sent to whole committee

Author: Martin Beroiz

thesis.tex

@@ -213,7 +213,7 @@ \chapter{Introduction}
 
 In February 2016, celebrating the centenary anniversary of Albert Einstein's first paper on gravitational 
 waves\footnote{``Approximate integration of the field equations of gravitation'' - A. Einstein. (1916)} (\citet{1916SPAW.......688E}), 
-the LVC collaboration announced the first ever direct detection of a gravitational wave, named GW150914.
+the LVC collaboration announced the first ever direct detection of a gravitational wave.
 With this, a new window of the universe for the purely relativistic astronomical phenomena was opened. 
 
 The history of gravitational waves (GWs) was not without controversies. 
@@ -314,8 +314,8 @@ \section{Gravitational Waves}
 Nautilus is a cryogenic, high Q-factor bar at a temperature of 0.1 K.
 This bar has already reached a strain sensitivity of $10^{-21}$ Hz${}^{-1/2}$ in the kHz region. (\citet{1997APh.....7..231A})
 
-A whole other category of GW detectors are those based on Michelson interferometry using lasers running along two kilometer long, or greater, arms.
-Interferometer GW detectors transduce a GW warp in space to the shrinking and stretching of relative distances of masses put far apart in two or more --mostly perpendicular-- long interferometers. 
+A whole other category of GW detectors are those based on Michelson interferometry using lasers running along two kilometric-long arms.
+Interferometer GW detectors transduce a GW warp in space to the shrinking and stretching of relative distances of masses put far apart in two or more --mostly perpendicular-- interferometers. 
 In the case of Earth based observatories, each interferometer is one arm several kilometers long, of an L-shaped facility.
 The test masses are the end mirrors on each arm that reflect a laser beam pointed in each arm direction. 
 On normal circumstances, the beams from two different arms can be set to be (`locked') on a dark or bright fringe of the interferometer diffraction pattern.
@@ -471,7 +471,7 @@ \section{Observable Sources by LIGO}
 Soft Gamma Repeaters (\citet{2007PhRvD..76f2003A}) 
 or instabilities in Neutron Stars (\citet{2016PhRvD..93l2008A}). 
 These type of sources are difficult to model because of the complicated physics of the progenitor.
-This typically demands a non-parametric un-modeled filter search on the GW time series, 
+This typically demands a non-parametric or un-modeled filter search on the GW time series, 
 either searching for excess of flux or using generic sine-Gaussian signals templates.
 
 {\bf Stochastic Background} is the collection of all the unresolved GW signals.
@@ -514,7 +514,6 @@ \chapter{The Transient Universe}
 Transients are most often unpredictable, but some of them are recurring, with or without predictability of the next event; they lack periodic variability; 
 and some of them are only a one-time occurrence and will only last for a relatively short period of time.
 This makes it necessary to study them in the field of time domain astronomy.
-% 'time domain' astronomy?
 
 Nonetheless, time domain astronomy poses at least two big main challenges.
 The first one deals with the huge amount of data, and the process of recovering interesting transients from it. 
@@ -1966,13 +1965,6 @@ \section{Target Selection}
 \label{fig:pointings}
 \end{figure}
 
-%\begin{figure}
-%\centering
-%\includegraphics[scale=0.5]{figures/pointings}
-%\caption{cWB, LIB, BYST, LALinf Sky-maps re-scaled regions that mark TOROS targets (red dots).}
-%\label{fig:pointings}
-%\end{figure}
-
 The algorithm utilized for the cWB estimations produces reasonably accurate maps for BBH signals, but underestimates the extent of high-confidence regions (\citet{2015ApJ...800...81E}). 
 As seen in figure \ref{fig:pointings}), the adoption of maps from alternative algorithms (not available at the time our observations started) 
 significantly reduced the fraction of the high-confidence region probed by our small field of view.