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adsnote = {Provided by the SAO/NASA Astrophysics Data System}
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}
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% periodic reference
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@ARTICLE{2005PhRvD..72j2004A,
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author = {{Abbott}, B. and {Abbott}, R. and {Adhikari}, R. and {Ageev}, A. and
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{Agresti}, J. and {Allen}, B. and {Allen}, J. and {Amin}, R. and
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{Anderson}, S.~B. and {Anderson}, W.~G. and et al.},
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title = "{First all-sky upper limits from LIGO on the strength of periodic gravitational waves using the Hough transform}",
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journal = {\prd},
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eprint = {gr-qc/0508065},
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keywords = {Gravitational wave detectors and experiments, Data analysis: algorithms and implementation, data management, Gravitational radiation detectors, mass spectrometers, and other instrumentation and techniques, Pulsars},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
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}
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@ARTICLE{2007PhRvD..76d2001A,
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author = {{Abbott}, B. and {Abbott}, R. and {Adhikari}, R. and {Agresti}, J. and
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{Ajith}, P. and {Allen}, B. and {Amin}, R. and {Anderson}, S.~B. and
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{Anderson}, W.~G. and {Arain}, M. and et al.},
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title = "{Upper limits on gravitational wave emission from 78 radio pulsars}",
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journal = {\prd},
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eprint = {gr-qc/0702039},
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keywords = {Gravitational wave detectors and experiments, Data analysis: algorithms and implementation, data management, Gravitational radiation detectors, mass spectrometers, and other instrumentation and techniques, Pulsars},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
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}
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% GRB search
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@ARTICLE{2005PhRvD..72d2002A,
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author = {{Abbott}, B. and {Abbott}, R. and {Adhikari}, R. and {Ageev}, A. and
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{Allen}, B. and {Amin}, R. and {Anderson}, S.~B. and {Anderson}, W.~G. and
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{Araya}, M. and {Armandula}, H. and et al.},
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title = "{Search for gravitational waves associated with the gamma ray burst GRB030329 using the LIGO detectors}",
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journal = {\prd},
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eprint = {gr-qc/0501068},
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keywords = {Gravitational wave detectors and experiments, Data analysis: algorithms and implementation, data management, Gravitational radiation magnetic fields and other observations, Supernovae},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
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}
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% SGR search
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@ARTICLE{2007PhRvD..76f2003A,
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author = {{Abbott}, B. and {Abbott}, R. and {Adhikari}, R. and {Agresti}, J. and
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{Ajith}, P. and {Allen}, B. and {Amin}, R. and {Anderson}, S.~B. and
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{Anderson}, W.~G. and {Arain}, M. and et al.},
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title = "{Search for gravitational wave radiation associated with the pulsating tail of the SGR 1806-20 hyperflare of 27 December 2004 using LIGO}",
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journal = {\prd},
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eprint = {astro-ph/0703419},
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keywords = {Gravitational wave detectors and experiments, Wave generation and sources, Data analysis: algorithms and implementation, data management, Gravitational radiation magnetic fields and other observations},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
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}
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% Stochastic Background
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@ARTICLE{2014PhRvL.113w1101A,
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author = {{Aasi}, J. and {Abbott}, B.~P. and {Abbott}, R. and {Abbott}, T. and
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{Abernathy}, M.~R. and {Accadia}, T. and {Acernese}, F. and
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{Ackley}, K. and {Adams}, C. and {Adams}, T. and et al.},
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title = "{Improved Upper Limits on the Stochastic Gravitational-Wave Background from 2009-2010 LIGO and Virgo Data}",
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journal = {Physical Review Letters},
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archivePrefix = "arXiv",
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eprint = {1406.4556},
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primaryClass = "gr-qc",
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keywords = {Gravitational radiation magnetic fields and other observations, Gravitational waves: theory, Experimental tests of gravitational theories, Gravitational wave detectors and experiments},
The test masses for LIGO are two massive mirrors at the end of two perpendicular long arms (4 km long.)
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Each mirror weighs about 40 kg and each one of the arms can be thought, for simplicity, as an independent laser interferometer.
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When a GW passes at an angle to this set-up, the arms will stretch and shorten in opposite directions (one arm will stretch as the other shrinks),
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while the laser keeps traveling the arms unaffected.
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This causes minuscule differences in optical paths for the light and this in turn will result in the lasers being out of phase from each other.
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This difference in phase from the `lock' position indicates a change in the relative positions of the mirrors.
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Many other mundane situations can also produce this same effect, the most simple one being seismic activity of almost any strength.
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Additionally, noise from the instrument itself, from the laser beam and electronics, as well as many intrinsic vibration modes of the system complicates the output signal that will be analyzed.
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\end{comment}
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LIGO --the Laser Interferometer Gravitational-Wave Observatory-- (\citet{1992Sci...256..325A}) is an American observatory set to detect the GW predicted by General Relativity.
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It is comprised of two separate observatories, one in Hanford, Washington, called LIGO Hanford, and another one in Livingston, Louisiana, called LIGO Livingston.
%Needs to add: Observables of LIGO, especially Compact Binary Mergers. Rates, etc.
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\begin{comment}
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De Mario:
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EN mi sugerencia 1.1 es como lo tenes, 1.2 es distintas fuentes astrofisica, 1.3 es LIGO y VIRGO y los detectores que convendria que fueran explicados un poco mas tecnicamente (mirar papar de detección) y 1.4 deberia ser una discusion de la deteccion y lo que significa?por ejemplo hay predicciones de rates de fusion de estrellas de neutrones tenes que hablar de eso?mira papers de Belczinski y de Vicki Kalogera?
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\end{comment}
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\begin{comment}
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The successful operation of Advanced LIGO is expected to transform the field from GW detection to GW astrophysics. We illustrate the potential using compact binary coalescences. Detection rate estimates for CBCs can be made using a combination of extrapolations from observed binary pulsars, stellar birth rate estimates and population synthesis models. There are large uncertainties inherent in all of these methods, however, leading to rate estimates that are uncertain by several orders of magnitude. We therefore quote a range of rates, spanning plausible pessimistic and optimistic estimates, as well as a likely rate. For a NS mass of 1.4 sm and a BH mass of 10 sm, these rate estimates for Advanced LIGO are: 0.4 400 yr, with a likely rate of 40 yr for NS???NS binaries; 0.2 300 yr , with a likely rate of 10 yr for NS???BH binaries; 2 4000 yr, with a likely rate of 30 yr for BH-BH binaries.
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LIGO was designed so that its data could be searched for GWs from many different sources. The sources can be broadly characterized as either transient or continuous in nature, and for each type, the analysis techniques depend on whether the gravitational waveforms can be accurately modeled or whether only less specific spectral characterizations are possible. We therefore organize the searches into four categories according to source type and analysis technique.
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(i) Transient, modeled waveforms: the compact binary coalescence search. The name follows from the fact that the best understood transient sources are the final stages of binary inspirals [52], where each component of the binary may be a NS or a BH. For these sources the waveform can be calculated with good precision, and matched-filter analysis can be used.
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(ii) Transient, unmodeled waveforms: the gravitational-wave bursts search. Transient systems, such as core-collapse supernovae [53], BH mergers and NS quakes, may produce GW bursts that can only be modeled imperfectly, if at all, and more general analysis techniques are needed.
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(iii) Continuous, narrow-band waveforms: the continuous wave sources search. An example of a continuous source of GWs with a well-modeled waveform is a spinning NS (e.g. a pulsar) that is not perfectly symmetric about its rotation axis [54].
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(iv) Continuous, broadband waveforms: the gravitational-wave background search. Processes operating in the early universe, for example, could have produced a background of GWs that is continuous but stochastic in character [55].
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The detectors provided unprecedented sensitivity to gravitational waves over a range of frequencies from 30 Hz to several kHz [1],
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which covers the frequencies of gravitational waves emitted during the late inspiral, merger, and ringdown of stellar-mass binary black holes (BBHs).
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In physics, GW detection could provide information about strong-field gravitation, the untested domain of strongly curved space where Newtonian gravitation is no longer even a poor approximation. In astrophysics, the sources of GWs that LIGO might detect include binary NSs (like PSR 1913 + 16 but much later in their evolution); binary systems where a black hole (BH) replaces one or both of the NSs; a stellar core collapse which triggers a type II supernova; rapidly rotating, non-axisymmetric NSs; and possibly processes in the early universe that produce a stochastic background of GWs [3].
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% Use info in EMCounterpartsReview1512.05435v1.pdf for EM counterparts to expected GW sources
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% Add: These detectors are most sensitive to GWs from the late stages of the binary inspiral.
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\end{comment}
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\section{Observable Sources by LIGO}
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Even if it's true that any massive or energetic event with a non-vanishing quadrupole moment will create gravitational waves,
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the sources capable of being detected by Earth-based GW observatories like LIGO will need to be in the design sensitive frequency
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range and be strong enough to be detected potentially tens or hundreds of Mpc away.
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There is extensive research on the many sources that could be potentially discovered by LIGO.
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In the following, we mention the most commonly cited in literature.
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They can broadly be separated into four categories: Compact Binary Coalescence, Continuous or Periodic, Burst, and Stochastic Background (\citet{tjonniethesis}).
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{\bf Compact Binary Coalescence} (CBC) is the best-understood kind of source for LIGO and Virgo.
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This type of source refer to the inspiral merge of compact objects, primarily Black Holes and Neutron Stars.
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Mergers of systems of Binary Neutron Stars, Binary Black Holes, or Neutron Star--Black Hole are the expected sources of GW for compact coalescence.
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These mergers offer a multitude of plausible electromagnetic counterparts and for that reason will be the focus of this thesis.
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The merger rate of binary systems is an area of active research and estimates remain uncertain.
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Compact binaries are formed similarly in stellar field populations of galaxies (\citet{2012LRR....15....8F}).
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Most population synthesis calculations of compact coalescence agree to within 1 to 2 orders of magnitude,
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a result consistent with the typical uncertainties that remain once all possible sources of errors are propagated in the population synthesis models.
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Estimates range from 0.01 to 10 mergers per Mpc${}^{3}$ per Myr.
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For a conservative merge rate of 1 Mpc${}^{-3}$Myr${}^{-1}$, and a projected observable radius of 200 Mpc at the design sensitivity of Advanced LIGO,
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the discovery rate of CBC will be of approximately 40/yr.
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{\bf Continuous or Periodic} sources are those that have roughly constant frequency and amplitude compared to its observation time.
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Primary sources of the continuous kind are rotating Neutron Stars (pulsars) with some non-axisymmetric anisotropy.
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The emitted gravitational wave frequency is twice the rotation frequency, and for many known pulsars, they fall within the LIGO sensitivity band (\citet{1998ApJ...501L..89B}).
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Searches for continuous periodic signals (\citet{2005PhRvD..72j2004A, 2007PhRvD..76d2001A}) involve the integration of large portions of the time series, spanning many cycles of the pulsar,
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correcting for Doppler shift for the motion of the Earth around the Sun, and spin-down of the pulsar, among other effects.
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Although the GW amplitude is generally weaker compared to CBC sources, a longer integration time means that continuous sources may also achieve detectable SNRs.
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{\bf Burst}-type sources are associated with large energy emission in cataclysmic events like Super Nova explosions,
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