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the detection of gravitational waves ( gws ) will rank as one of the major scientific achievements of this century . their detection will open up a new observational window to the universe , revealing dynamic sources of strong field relativistic gravity previously inaccessible through conventional astronomical instruments . our understanding of space - time and matter under the most extreme conditions will be transformed . although there has been no direct detection of gws to date , indirect evidence for their existence comes from high precision , nobel - prize winning measurements of the pulsar psr 1913 + 16 and its companion neutron star ( ns ; * ? ? ? * ; * ? ? ? the gw emission that drives the system s orbital decay is in agreement with the predictions of general relativity to better than 1% @xcite . when such binary neutron star ( bns ) systems eventually coalesce , they are predicted to emit copious amounts of gws @xcite . these sources will be prime targets for the new generation of gw detectors , led by advanced ligo ( aligo ; * ? ? ? * ) which is set to begin observing during the second half of 2015 and advanced virgo a year later @xcite . at final sensitivity , these advanced detectors are expected to detect bns mergers at a rate within the range 0.4400 yr@xmath0 @xcite . compact binary coalescences ( cbcs ) consisting of at least one black hole ( bh ) are also targets for gw detectors ; although there is compelling evidence for their existence @xcite , the event rates of these sources for aligo detection is not well known . one realisation in the last decade is that coalescing systems of ns / ns or ns / bh events could be the progenitors of short - hard gamma ray bursts ( sgrbs ) ; transient events routinely observed throughout the electromagnetic ( em ) spectrum @xcite . there exist other types of em , neutrino and cosmic ray emissions that may also be associated with gw events . these include long - duration gamma ray bursts ( lgrbs ; * ? ? ? * ) , short gamma ray repeaters @xcite , supernovae @xcite , fast radio bursts @xcite as well as others . history has already shown that multi - wavelength astronomy can play an important role in unveiling new phenomena . in the last decade , x - ray , optical and radio follow - ups have all transformed and revealed new processes in our understanding of gamma ray bursts ( grbs ) ; combining em observations with those in the gw domain will too provide new insight into the internal engines and mechanisms at play in a multitude of different sources . a new generation of sensitive , wide - field telescopes , advancements in time domain astronomy and upgrades to neutrino and cosmic ray detectors can provide a coordinated network for discovery . the possible simultaneous detection of photons , neutrinos or high energy particles with gws would be a landmark moment for astrophysics , initiating a new era of _ _ multi - messenger _ _ astronomy , for the first time including gw .    maximising the potential offered by gw observations involves the development of a worldwide , multi - messenger network . australian facilities are ideally placed to foster scientific exchanges in this new era and agreements have already been established . to conduct em follow - up of gw triggers , memorandums of understanding ( mous ) have been signed between the ligo / virgo gw collaboration and a number of facilities either based in australia or with strong australian involvement ; these include : the anglo - australian telescope , the australian square kilometer array pathfinder ( askap ; * ? ? ? * ) , the cherenkov telescope array ( cta ; * ? ? ? * ) , the high energy stereoscopic system ( h.e.s.s ; * ? ? ? * ) , icecube @xcite , the murchison widefield array ( mwa ; * ? ? ? * ) , and the skymapper @xcite , the gw optical transient observer ( goto ) and zadko @xcite optical telescopes . in this paper , we focus on the most probable multi - messenger observations from the advanced detector era ; those associated with grbs . whilst doing so , we consider the contribution that the australian facilities can make to the worldwide multi - messenger effort . the structure of this paper is as follows : section 2 describes gw astronomy . sections 3 and 4 introduce sgrbs and lgrbs and describe how co - ordinated gw and multiwavelength observations of these events can provide breakthrough science . section 5 acts as a primer for those unfamiliar with the concepts and terminologies of detection and data analysis often used in the gw domain ; this section is not designed to be exhaustive but to present some of the most important concepts in gw detection and data analysis . section 6 discusses the expected rates and detection ranges for gw sources . the next two sections describe two of the strategies that form the basis for coordinated gw and em observations in the gw era . section 7 discusses em triggered gw searches ; these could likely yield the first coincident gw - em event through archival gw data . section 8 discusses the em follow - up of gw triggers ; this strategy is highly challenging due to the large positional uncertainties of gw observations but the potential rewards for success are without doubt highly significant . section 10 discusses the australian facilities involved in the co - ordinated science programs with aligo / adv and we highlight the areas in which they could contribute in this new frontier . finally , in section 11 we discuss the role neutrino follow - up plays in gw detection . gravitational waves are produced by regions of space - time that are distorted by high velocity bulk motions of matter . the timescale of the motions determine the frequency of the gw emission ; ground based detectors will target systems with masses in the range 110@xmath1 @xmath2 , which emit in the 1  hz10  khz band . this frequency range , covering the audio band , has motivated the characterisation of interferometric gw astronomy as `` listening to the universe '' . instruments capable of achieving detections will begin observations in the second half of 2015 . advanced ligo , a pair of us based interferometric detectors at hanford and livingston ( usa * ? ? ? * ) will have its first observational science run ( o1 ) in late-2015 ; a year later it will be joined by the italian advanced virgo ( adv ; * ? ? ? * ; * ? ? ? * ) for a second observing run ( o2 ) . the `` advanced '' network of interferometric gw detectors will eventually have 10 times the sensitivity of the first generation instruments . the increased sensitivity translates into a factor @xmath3 increase in observed volume , making detections expected rather than plausible . additional instruments are expected to eventually join the network . kagra , a japanese detector , is envisioned to begin operation in 2018 - 19 @xcite and ligo - india is expected to be operational from 2020 , reaching a design sensitivity at the same level as aligo by around 2022  @xcite . the gw observations made by these instruments will differ from most conventional em observations in several ways :    1 . gws are not scattered or obscured by intervening material like dust so provide a window into the densest regions of the universe . as gw detectors observe an amplitude rather than a flux , the measure of detectability follows an inverse relationship with distance rather than the conventional inverse square law . therefore , number counts of a homogeneous distribution of standard - candle sources increases with distance , @xmath4 , as , @xmath5 , rather than , @xmath6 ; 3 .   as gws couple weakly to the detectors , even very local astronomical sources of gws have to be highly energetic emitters of gravitational radiation ; 4 . gw detectors are nearly omnidirectional , with a nearly @xmath7 steradian sensitivity to astrophysical events with a greater than average response over more than 40% of the sky . the first point implies that gw observations can allow us to view astrophysical phenomena inaccessible by other means . the gravitational window can therefore enable frontier explorations in the low to intermediate redshift universe ( @xmath8 ) of sources that are electromagnetically invisible for much , or all , of their lives . the second point means that a factor 2 improvement in the sensitivity of a gw detector results in a factor 8 increase in the volume of the universe being probed . the third point emphasises a detection bias for detecting the most highly energetic astrophysical events . the typical fluxes of gw sources are of order @xmath9 jy , far greater than equivalent fluxes typically observed in the radio domain ( @xmath10jy  jy ) . the final point means that gw detectors are naturally survey instruments over a wide band of frequencies ( 105000 hz ) . there are a number of types of em counterparts that may be associated with gw emissions @xcite . as some of these counterparts are quite speculative , this paper focuses on gw signals associated with grbs . other sources of simultaneous em and gw emission include supernovae as well as multiple emission mechanisms from nss ; for a review of the latter , see the accompanying article in this series @xcite .    in the next few sections we provide a summary of both sgrbs and lgrbs and the type of gw / em associations that could be targeted in the gw era . some of these predictions are based on solid foundations whilst some are more speculative . in considering the latter , we note that when a new window of observation has been opened in the past , the discoveries that transform our understanding of the universe have often been the least expected . +    gravitational waves from the merger of coalescing binary systems of ns / ns and ns / bhs are confidently predicted to have observable em counterparts . this expectation is a result of the connection between these events and sgrbs ( e.g. * ? ? ? * ; * ? ? ? * ; * ? ? ? * ; * ? ? ? the evidence stems from a number of different channels . firstly , the dynamic timescales of discs predicted from the merger of cbcs are consistent with the durations of sgrbs . secondly , em follow - ups of sgrbs have never provided an associated supernova . thirdly , sgrb afterglows have been localised to galaxies harbouring older stellar populations with offsets of order tens of kpc from their galactic centers ; this is consistent with post - natal kick velocities of 100s of km s@xmath0 , and also with the fainter and shorter lived afterglows expected from an ambient interstellar medium at a large offset . finally , as is discussed in  [ kilonova ] , the discovery of a faint em transient called a _ kilonova _ has provided the strongest observational evidence to date of the sgrb / cbc association . conclusive proof of the cbc / sgrb association will be provided through gw observations . coincident em and gw observations of sgrbs could also provide a fascinating insight to the dominant mechanisms at the heart of grbs . low - latency gw pipelines could enable multi - wavelength follow - up measurements of the prompt emission , constraining both the underlying central engines and the emission mechanisms at work . later - time multi - wavelength follow - ups can provide insight through extensive coverage of the sgrb afterglow . a number of em counterparts have been predicted to accompany the inspiral and merger of ns / ns and ns / bh systems . in figure [ fig_mm_scenarios ] we show the likely outcomes of these mergers and in the following sections we will briefly review the most likely em counterparts that could accompany cbcs .      during the final stages of the merger of a compact binary , the system is expected to launch a highly relativistic jet that interacts with itself and the surrounding medium ( the fireball model for grbs ; e.g. * ? ? ? collisions of material moving at different velocities within the jet will lead to internal shocks , giving short - lived bursts of gamma - rays that we detect as the sgrb prompt emission . as the accretion timescale is expected to be @xmath112 seconds @xcite , the grbs associated with compact binary mergers are typically shorter in duration than those associated with core - collapse supernovae ( explaining the observed distribution of grbs ; * ? ? ? . however , the division between these two populations is not easily identifiable from the prompt gamma - ray emission alone ( e.g. * ? ? ? * ; * ? ? ? * ) .    a number of _ fermi_-lat grbs have shown @xmath12gev emission ( even at redshifts as distant as @xmath13 ) . two bursts were observed with gamma - ray photons reaching energies up to 94gev ( grb 130427a ) and 62gev ( grb 131231a )  this supports the suggestion that the photon energies may extend higher than previously assumed @xcite . significantly , these discoveries have not been limited to lgrbs , with sgrbs also showing high energy photons and gev emission often continuing for 10 s of seconds beyond the initial burst . the fact that _ fermi_-lat discovered a photon of energy 31gev during the prompt phase of grb 090510 @xcite is promising for co - ordinated observations between gw detectors and ground - based cherenkov telescope arrays @xcite operating at @xmath12 10 gev . additionally , sgrbs with time - extended emission have recently been cited as promising targets for cherenkov telescope arrays @xcite . one exciting possibility is the observation of prompt optical flashes . so far , these emissions have only been observed in lgrbs @xcite . an early optical emission correlated with the prompt gamma - rays could indicate a common origin related to the internal shocks @xcite . a number of studies have suggested that compact binary mergers could generate prompt coherent radio emission ( e.g. , * ? ? ? such mechanisms include excitation of the plasma surrounding a compact binary merger by gws @xcite , from a dynamically - generated magnetic field after the merger @xcite , or from the onset of the collision of the forward shock with the surrounding medium @xcite . however , the detectability of emission from these processes will be dependent upon the scattering by the surrounding environment @xcite . nonetheless , these studies suggest compact binary mergers are an interesting contender for the progenitors of fast radio bursts ( frbs ; * ? ? ? * ; * ? ? ? * ) , which are currently unknown . plateaus and flares in x - ray light curves following grbs are signatures of ongoing energy injection . this could be caused by late - time accretion onto a central black hole ( unlikely in the compact binary scenario ; see discussion in * ? ? ? * ) , or from ongoing energy injection from the spindown of a newly born neutron star . indeed , recent studies ( e.g. , * ? ? ? * ; * ? ? ? * ; * ? ? ? * ) have shown that the merger of two nss could result in a supramassive ns ; a star with a mass greater than the non - rotating maximum mass but supported from further collapse through rotation @xcite . around 60% of x - ray afterglow light curves of sgrbs observed by the _ swift _ satellite @xcite have shown plateaus lasting 10010000  s after the burst ; these have been attributed to electromagnetic spin - down emissions from protomagnetars @xcite formed via the merger of two neutron stars @xcite . observations of the plateau phase can also be used to constrain the ns equation of state , with gw observations of the inspiral phase significantly aiding this endeavour @xcite    if the post - merger remnant is an ns , early optical afterglow as bright as 17th magnitude in r band ( assuming a distance of @xmath14 mpc ; see  [ section_cbc_ranges ] ) could be produced from dissipation of a wide - beamed protomagnetar wind @xcite . this magnetar wind could launch ejecta at relativistic speeds which would interact with the surrounding medium and produce a bright broadband afterglow from synchrotron radiation @xcite . gravitational wave emission may also accompany an afterglow plateau if a millisecond magnetar is born from the collision . multiple mechanisms for generating such gws exist in nascent neutron stars , including secular bar modes ( e.g. , * ? ? ? * ; * ? ? ? * ; * ? ? ? * ) , @xmath15-modes @xcite , and magnetic - field induced stellar deformations @xcite . such emission could be observable by aligo out to @xmath16 mpc @xcite . in fact , the x - ray light curve itself can be used to constrain the total gw emission from these systems @xcite . some plateaus following sgrbs exhibit an extremely steep decay phase , commonly interpreted as the collapse of the nascent neutron star to a black hole @xcite . such collapse could potentially produce an frb when the magnetic field lines snap as they cross the bh horizon @xcite , which is expected to occur @xmath17 s after the merger @xcite . a low latency gw trigger could enable prompt follow - ups to test this connection @xcite .      as the relativistic jet propagates , it collides with the medium surrounding the progenitor resulting in a forward shock travelling into the surrounding medium , and a reverse shock propagating back up the jet ( e.g. * ? ? ? * ; * ? ? ? these shock fronts produce multi - wavelength synchrotron emission , initially peaking in the x - ray and moving through the different wavelengths to radio as it fades . the typical afterglow of grbs is attributed to the forward shock emission and the brightness of this afterglow is dependent upon a number of parameters , including the density of the surrounding medium . therefore , in a low density environment , the forward shock component is expected to be relatively faint . the multi - wavelength afterglows of sgrbs have been observed and are typically fainter than those of lgrbs @xcite . this is consistent with sgrbs being less energetic than lgrbs and with their locations in lower density environments . the reverse shock has also been observed for sgrb 051221a ( e.g. * ? ? ? * ) . a ` kilonova ' is been predicted to form after the merger of two nss . this faint optical transient is powered by the radioactive decay of the ejected neutron rich matter @xcite and could reach around 21-23 mag in the optical and 21-24 mag in the nir for a source at 200 mpc @xcite . recent optical and near - infrared follow - up observations of grb 130603b have provided the most conclusive evidence to date of this scenario , reinforcing the theory that compact object mergers are the progenitors of sgrbs @xcite . these observations have added significantly to other observational evidence in support of this scenario @xcite . coincident em and gw observations could confirm that sgrbs are indeed the result of coalescing compact binaries . an additional prompt em emission related to the kilonova mechanism has also recently been suggested by @xcite . this has been inspired by studies that suggest a small fraction of the ejected neutron rich matter can expand rapidly enough to avoid r - process capture @xcite . the suggestion is that @xmath18-decay from free neutrons in the outermost layers of this ejecta could power optical emission on a timescale of hours after the merger , peaking at around magnitude 22 in the u - band for a source . for a source at 200 mpc this signal would peak at around magnitude 22 in the u - band and would act as a precursor to a kilonova . lgrbs are amongst the most luminous transient events in the universe in terms of em radiation per unit solid angle . these beamed emissions have been observed to last up to @xmath19 s @xcite and can radiate a total energy equivalent to that of the sun in its entire 10 gyr lifetime . the extreme luminosities allow lgrbs to be seen out to cosmological volumes , making them a probe of the high redshift universe ( @xmath20 ) . the favoured scenario for these bursts is described by the collapsar model @xcite in which the inner part of a wolf - rayet star progenitor collapses to form a rapidly rotating black hole . high angular momentum enables the infalling matter to form an accretion disk , which in turn provides the energy reservoir to power an ultra - relativistic jet that blasts its way through the stellar envelope . the observed radiation is explained through synchrotron and/or inverse compton emission from the accelerated electrons in internal and external shocks . some authors have suggested instead that the central engines may consist of magnetars @xcite . there is observational evidence to support this scenario for at least a proportion of lgrbs @xcite . the connection between lgrbs with the collapse of massive stars @xcite has been supported by afterglow observations in or near dense regions of active star - formation ; predominantly dwarf starburst field galaxies @xcite . as mentioned earlier , their denser environments , as well as their higher emission energies , mean that the multiwavelength afterglows of lgrbs are typically brighter than those that occur from sgrbs @xcite .    in terms of gw emissions from these events , a number of lgrbs have been associated with core - collapse supernova @xcite . modelling the gw emission from these supernovae is very complex , requiring a combination of general relativistic hydrodynamics , magnetic fields , rotation , neutrino transport and nuclear physics @xcite . simulations have so far provided a picture of a very complex and chaotic behavior that includes shock formation and turbulence that create highly complex waveforms with multiple sharp bursts over ms durations . however , most scenarios suggest an event may have to be within tens of kpc for detection . as most lgrbs occur at cosmological distances , the vast majority of their gw signals will be out of reach for advanced detectors .    the requirement for rapid rotation to produce the disc in a grb @xcite allows for alternative emission mechanisms that could produce detectable gws out to 10s of mpc @xcite . fragmentation instabilities could be produced in the core or in the disc @xcite . rapid rotation could also give rise to rotational instabilities in the protoneutron star remnant @xcite    a number of studies have suggested there exists a sub - population of lgrbs known as low - luminosity grbs ( _ _ ll__grbs ) . these events have isotropic equivalent gamma - ray luminosities 2 - 3 orders of magnitude below classical lgrbs @xcite and have only been detected at low-@xmath21 due to their lower energy emissions ( the closest was grb980425 at z = 0.0085 or 36mpc ) . as such their rates have been predicted to be 23 orders of magnitude greater than lgrbs . observations have confirmed that both lgrbs and _ _ ll__grbs produce supernovae , suggesting that the _ _ ll__grbs may just be lower - energy events from the tail of the distribution . this has been a long going debate and attempts to address it have used statistical arguments @xcite , fits to the peak flux distribution @xcite , and simulation @xcite . the suggestion that _ _ ll__grbs could be just normal lgrbs viewed off - axis was discounted based on statistical arguments , as it would produce a far higher local rate density than expected from lgrbs and would require narrower opening angles for lgrbs than determined from the breaks in afterglow lightcurves @xcite .    recently , an analysis of _ _ ll__grb 060218 has suggested that the main difference in the two bursts arises from an extended low - mass envelope in _ _ the existence of such an envelope can smother the jet and drive a mildly relativistic shock resulting in a much lower luminosity than that produced by an ultra - relativistic jet that is able to penetrate through the bare progenitor star . interestingly , the statistical arguments suggesting separate populations put forward by @xcite can also support these two different scenarios . it is therefore possible that gw emission mechanisms could be driven by the same type of engine for both these classes . the output from a single gw detector consists of a time series data stream , @xmath22 , composed of the detector response to a gw signal , @xmath23 , and the detector noise @xmath24 : @xmath25 in general , @xmath23 will be a linear combination of the two orthogonal transverse polarizations , @xmath26 , weighted by the dimensionless detector antenna pattern functions for the two polarizations @xmath27 : @xmath28 which describe the detector sensitivity to radiation of different polarizations , incident from different directions @xcite . the angles , @xmath29 and @xmath30 , represent the direction to the source and @xmath31 is the polarization angle of the wave . a gw detector can follow the phase of a gw signal , so the time series is generally represented in the frequency domain by the strain amplitude spectral density , @xmath32 . this quantity is defined through the power spectral density @xmath33 , with @xmath34 the fourier transform of the time series . similarly , one can define a signal power spectral density , @xmath35 , and a noise power spectral density , @xmath36 . the strain amplitude spectral density is given by : @xmath37 with dimensions of @xmath38 @xcite . this quantity is often used in plots to display the sensitivity of gw interferometers . a single gw detector can not determine the polarization state or source direction of a transient signal . to obtain source localization , a widely separated network of gw detectors is essential . such a network may employ techniques such as _ coincidence analysis _ , in which individual events from different detectors are correlated in time @xcite , or _ coherent analysis _ , in which synchronized detector outputs are merged before searching for a common pattern @xcite . by effectively resolving the different times of arrival of gw events between members of a network , coherent network analysis enables a detector array to become an all - sky monitor with good angular resolution over all source directions .    achieving good directional sensitivity is of paramount importance for gw / em associations . for the sources considered in this review , directional sensitivity is determined through triangulation of arrival times . to maximize the time delays , and hence improve directionality , it is advantageous that a network be as geographically widely separated as possible @xcite and as such , a number of detectors are planned to join the aligo / adv network throughout the next decade . the japanese observatory kagra , should begin operations by around 2018 - 19 @xcite ; at design sensitivity this detector could improve the directional precision of a aligo / adv network by a factor of 1.5 - 2 and the detection rate by a similar factor @xcite . ligo - india operating at aligo sensitivity will be added to the aligo / adv network by 2022  by then bnss will be detectable out to @xmath39200 mpc and up to 400 events are possible per year @xcite . an indian detector will improve the angular resolution sufficiently to increase the percentage of gw sources detected within 5 deg@xmath40 from 3 - 7% to 17% @xcite . it has long been recognized that a gw detector in australia would add the longest baseline to the proposed advanced detector network ( e.g. , * ? ? ? * ; * ? ? ? * ; * ? ? ? for example , adding an australian detector to an aligo / adv three detector network can reduce the error in solid angle to tens of arc - minutes for high signal - to - noise ratio ( snr ) signals @xcite , dramatically improving the ability to localise gw sources for multi - wavelength follow - up observations . this scenario could be realised when third generation observatories such as the ` einstein gravitational wave telescope ' ( et ) become a reality in the next decade @xcite . the optimal site for a detector in the southern hemisphere been shown to be western australia @xcite , the current home to an 80-m baseline prototype gw detector . the false alarm rate ( far ) is the rate that false positives appear above a given snr threshold , and is dependent on the number of glitches ( non - stationary transients ) in the gw data stream . it is a critical measure as it determines whether a candidate should be considered for follow - up . for well modeled sources , the background of false alarms is at a level close to that of gaussian noise . for un - modeled sources typically short duration transients  the data quality has a greater effect on detection confidence . one therefore sets the threshold high enough so that noise generated false alarms are negligible . given that the probability , @xmath41 , of observing an event with an amplitude in the range @xmath42 to @xmath43 is given by a gaussian distribution of standard deviation @xmath44 , the probability of obtaining a far greater than a given threshold , @xmath45 , is : @xmath46    to be 99% confident that a gw has been detected , one can set an snr @xmath47 which is equivalent to a far of 1 in 100 years of observation . to see this one can approximate number of noise instances during that period . if the detector output sampling rate is 1 khz and the output is processed through @xmath48 filters , in 100 years we get @xmath49 , yielding @xmath50 which is our required snr . for a network of three equivalent detectors combined snr , @xmath51 is given as : @xmath52 where @xmath53 represents the snr in the ith detector @xcite . this shows that for a network of 3 equivalent detectors , to dismiss false alarms at a level @xmath54hz requires @xmath55 .     + the expected gw signals from cbcs takes on the well modelled chirp form shown in figure [ fig_chirp ] . the figure shows how the signal increases in both amplitude and frequency towards merger ; as it does so it sweeps across the sensitive bandwidth of advanced gw interferometric detectors .    for such well - modeled signals , the most efficient signal detection method to extract signals from noisy detector data is _ matched filtering _ , in which a _ template _ , representing the predicted waveform as a function of time is correlated with the output of a detector @xcite . a matched signal will produce an output much greater than that expected for pure noise with an optimal snr given as : @xmath56^{1/2}. \label{eq : snr}\ ] ] for well - modelled sources , matched filtering enhances the value of the signal by a factor @xmath57 , where @xmath58 is the number of cycles used in the integration . as inspiralling systems approach merger , even though the rest frame gw amplitude will increase , the number of cycles in each frequency bin , @xmath59 , gets smaller ; therefore the detected signal will decrease . this means that for inspiraling systems , rather than solely base the predicted amplitude of the radiation as a true indicator of the detectability , we include a measure of the observed cycles . the value of @xmath58 increases with the compactness of the system as it approaches merger and if observed from a frequency of 10 hz until merger , could produce @xmath60 cycles  effectively improving the detectability by a factor of 100 . however , to achieve such gains , a gw data - stream would have to be filtered by a large number of templates ( of order @xmath61 in near real time the significant challenges in both theoretical modeling and computational efficiency to achieve this can not be underestimated . one important aspect of well - modeled inspiralling systems is that a detection can be made 10s of seconds before the merger if enough cycles can be detected to boost the snr @xcite . figure 2 illustrates this concept showing a chirp signal 40s before the merger phase . this scenario could allow a low - latency alert to be sent out to em facilities as near real - time as possible to catch a prompt em signature ; the combination of em and gw data in this regime would provide valuable insight into the inner workings of such cataclysmic events . it is also worth noting that gws can provide an independent measure of luminosity distance , @xmath62 @xcite . during the inspiral phase , the gw strain , and the rate of change of gw frequency are given as @xmath63 where @xmath64 is the redshifted chirp mass , @xmath65 , and @xmath66 , @xmath67 are the component masses of the binary . therefore , if one can determine the redshift through , for example , a galaxy association , one can measure the redshift - luminosity distance relation independent of the cosmic distance ladder . a recent series of papers has reinvigorated this topic by introducing novel methods for breaking the redshift - chirp mass degeneracy with future gw observations @xcite . although matched filtering is the optimal strategy for gaussian , stationary noise , high amplitude transients due to instrumental and environmental artifacts can render gw data to be non - stationary and non - gaussian . therefore , one must employ robust methods that can reject instrumental artifacts and retain the true gw events . one such method is the @xmath68 veto that is a powerful consistency test used to reject false alarms @xcite . this method uses the fact that the quantity @xmath45 is an integral over all frequencies and therefore not sensitive to the contributions from different frequency regions of the broadband signal . one can split the signal spectrum into @xmath58 bins of equal snr contribution , and draw a comparison with the expected value in each bin ( based on the model template ) . a true gw event will have power accumulated approximately equally in each of @xmath58 bins ; a noise glitch will have power unevenly distributed and will yield a large @xmath68 value . , b.  l. , abbott , t.  m.  c. , angstadt , r. , et  al . 2012 , in society of photo - optical instrumentation engineers ( spie ) conference series , vol . 8446 , society of photo - optical instrumentation engineers ( spie ) conference series , 11      , d.  w. , price , p.  a. , soderberg , a.  m. , berger , e. , kulkarni , s.  r. , sari , r. , frail , d.  a. , harrison , f.  a. , yost , s.  a. , matthews , k. , peterson , b.  a. , tanaka , i. , christiansen , j. , & moriarty - schieven , g.  h. 2003 , apj , 586 , l5                                                                                                                                                                                                                                                        , r.  m. , dekany , r.  g. , bebek , c. , et  al . 2014 , in society of photo - optical instrumentation engineers ( spie ) conference series , vol . 9147 , society of photo - optical instrumentation engineers ( spie ) conference series , 79                                                                      , r.  d. , barthelmy , s.  d. , denny , r.  b. , graham , m.  j. , & swinbank , j. 2012 , in society of photo - 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the first observations by a worldwide network of advanced interferometric gravitational wave detectors offer a unique opportunity for the astronomical community . at design sensitivity 
 , these facilities will be able to detect coalescing binary neutron stars to distances approaching , and neutron star - black hole systems to . both of these sources 
 are associated with gamma ray bursts which are known to emit across the entire electromagnetic spectrum . 
 gravitational wave detections provide the opportunity for `` multi - messenger '' observations , combining gravitational wave with electromagnetic , cosmic ray or neutrino observations . 
 this review provides an overview of how australian astronomical facilities and collaborations with the gravitational wave community can contribute to this new era of discovery , via contemporaneous follow - up observations from the radio to the optical and high energy . 
 we discuss some of the frontier discoveries that will be made possible when this new window to the universe is opened . 
 binaries : close  gravitational waves  gamma - ray burst : general  methods : observational  supernovae : general  stars : neutron