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Paper text:
gamma - ray bursts ( grb ) are bursts of gamma - rays that arguably signal the birth of a black hole somewhere in the universe . based on the duration and spectrum , two classes of bursts
have been observed  @xcite : those that last less than two seconds and have on the average hard spectra ( short grbs ) , and those that last longer than two seconds and are spectrally softer ( long grbs ) . the exact nature of the grb progenitors is unknown , although it is possible that long grbs come from the collapse of massive , rapidly rotating stars  @xcite and short grbs result from the merger of compact objects  @xcite .
regardless of the progenitor system , accretion onto the resulting compact object is thought to create a highly relativistic jet .
the prompt gamma - ray emission from the grbs may arises from the internal shocks due to collisions of faster shells with slower ones ejected earlier by the central engine .
the subsequent softer multi - wavelength emission , referred to as the afterglow , may be due to the collision of the fireball with the extra - stellar material  @xcite .
our understanding of grbs progressed very rapidly after the detection of multi - wavelength afterglows .
well localized , favorably positioned grbs get fairly good multi - wavelength afterglow coverage .
currently , the leading grb afterglow detection mission is @xmath0 which detects 90100 grbs annually .
most of the @xmath0 grbs get observed by various instruments around the world because of its rapid arc - minute localization capability .
compared to @xmath0 , @xmath1 gamma - ray burst monitor ( gbm ) detects about 250 burst per year but with poor localization . the error circle ( ec ) of @xmath1 gbm detected bursts
is too large for a single telescope to observe effectively .
the typical statistical uncertainty of the gbm burst location is about 3.3 degrees .
however , when combined with the systematic uncertainty of 3.8 degrees  @xcite , the total burst location uncertainty is @xmath2 5.0 degrees ( i.e. , 5.0 degree error radius ) .
naturally , a brighter burst will have a smaller gbm ec than a weaker burst .    even though the localization is poor , gbm detected bursts have very good timing and spectral information including crucial @xmath3 measurements ( @xmath3 is the peak energy of the grb @xmath4 spectrum ) . if there is a method to localize gbm detected grbs to a few arc - seconds uncertainty , then large telescopes can do deeper follow  up observations to determine the redshift of the burst and also potentially identify any emerging supernova . in addition , @xmath0 can also slew quickly to the gbm burst in order to observe the x - ray afterglow and obtain its light curve in x - ray wavelengths .
based on @xmath0 observations about @xmath2 60% of grbs have optical counterparts  @xcite .
these optical counterparts are detected by various observatories with r magnitudes ranging from 14 to 22 within few hours after the burst  @xcite .
thus , it is reasonable to assume about 60% of the gbm detected grbs also have optical counterparts with similar brightness distribution . if we were able to cover the entire gbm ec within about 24 hours after the burst it is conceivable that we would be able to find optical afterglows of @xmath2150 grbs per year , which is more than the total number of burst @xmath0 detects per year .    due to the small energy range ( 15 - 150 kev ) of the @xmath0 burst alert telescope ( bat )
, @xmath0 measurements alone can not constrain the @xmath3 of all bat detected bursts  @xcite . in contrast , due to the wide energy range ( 8 kev - 40 mev ) of gbm , all grbs detected by gbm have fairly good @xmath3 measurements . hence
, addition of possibly another @xmath2100 bursts per year with good @xmath5 and redshift measurements may allow us to explore the validity of various grb luminosity relations and to conduct detailed grb hubble diagram studies .
we have investigated the feasibility of using a system to do coordinated monitoring of the bat field - of - view ( fov ) for prompt optical emission from grbs  @xcite .
the study showed that with the current instrumentation , performing such a coordinated monitoring is not practical mainly due to the bat s very large fov .
however , a similar coordinated observing campaign can be used to find the optical afterglow of gbm detected bursts .
the gbm ec is much smaller than the bat fov and observers do not need to continuously monitor the field to detect the optical afterglow .
this enables a given observatory to perform multiple observations inside the gbm ec and thereby increase the chance of a afterglow detection .
the basic proposal is to design a system to facilitate scanning of the gbm ec for optical emission from grb afterglows .
this observing program will be specially aimed at amateur astronomers around the world .
proliferation of amateur telescopes with high quality ccd cameras has opened a new avenue to study optical emission from grbs .
the basic objective of the system is to coordinate a significant number of ground based telescopes to scan different patches of the gbm ec in order to find the location of the optical afterglow . unlike the gcn system  @xcite which sends notices to large number of recipients ,
this system will send customized targeted messages to individual registered telescopes .
these individual messages will be sent via email or socket connections and they will have one or more assigned pointing locations for each telescope .
the target telescopes can be either robotic or non - robotic .
the selection of various patches in the gbm ec will be done based on the number of available telescopes , individual telescopes physical location , field of view ( fov ) and sensitivity .
it is also reasonable to assume that these telescopes can observe multiple patches of the gbm ec , which will increase the chances of detection significantly .
some of the important impacts of the proposed project are :    1 .
the project will significantly enhance the value of gbm as a grb discovery instrument .
2 .   potentially increase the number of burst with good timing , spectral and redshift measurements .
the project will allow and attract the participation of amateur astronomers and their telescopes .            in order to investigate the feasibility of the project
, we performed a monte carlo simulation to study the probability of detection of optical afterglows from @xmath1 gbm grbs .
we assumed that gbm detects about 150 grbs with optical afterglows ( total rate is 250 per year ) per year distributed isotropically in the sky and throughout the year .
we have distributed telescopes in such a way that they roughly trace the major cities in the world .
then for each burst we tracked the path of the sun and selected a set of telescopes away from the sun and within few hours from the burst location to scan the gbm ec .
we also calculated the illuminated fraction of the moon s disk ( @xmath6 ) at the time of each burst .
the probability , @xmath7 , of finding a grb was estimated by @xmath8 here @xmath9 is the total number of independent attempts to observe , with probability of success , @xmath10 . in this case
@xmath9 is equal to the product of number of available telescopes and number of patches each telescope can observe .
we calculated the probability of success , i.e. , the probability of detecting a given burst afterglow per observation using the following equation .
@xmath11 note that typically the one @xmath12 gbm ec is @xmath13 .
we repeated this procedure for every simulated burst , while changing the total number of telescopes participating in the program , the fov of telescopes , and total number of patches a given telescope can cover .
the results of our simulation are shown in figure  [ sim_results01 ] and figure  [ sim_results02 ] .
for these particular simulations we have assumed that all the telescopes have the same fov and all telescopes can cover some constant number of patches in the gbm ec .
furthermore , we assumed that these telescopes will be able to observe assigned sky patches within a few hours after the burst .
hence , in the simulation we used only telescopes which are within a few hours ( @xmath2 6 hours ) of the burst location .
the number of participating telescopes in the observing program was varied from 20 to 100 .
figure  [ sim_results01 ] shows the number of localized bursts ( @xmath14 total number of bursts ) as a function of the fov of participating telescopes .
here we have fixed the number of participating telescopes to 25 .
various curves correspond to different number of patches that each telescopes can observe .
figure  [ sim_results02 ] shows the number of localized bursts as a function of number of participating telescopes in the program assuming that each telescope can observe 20 patches .
the six curves shown in the plot correspond to various field of views . according to the simulation , with 60 telescopes participating
it is possible to detect about 40 grb optical afterglows per year using telescopes with fov of @xmath15 .
this value is close to the value of a typical fov of an amateur telescope .
it is also interesting to note that if we have about 10 telescopes participating with fov of @xmath16 , then it is possible to detect about 25 grb afterglows per year . in order to put these values into perspective we point out that thus far , no one has managed to observe optical afterglow of a grb based only on a gbm localization ( the gbm has been detecting grbs for more than three years ) .
it is also worth noting that not all the gbm locations will have a statistical error of 3.3 degrees . about a third of the grbs
will have a statistical error less than this value .
about 10% will have error of 1 degree or less .
in such cases the gbm ec radius will be less than 5 degrees and may be as small as 4 degrees . obviously , for those cases we have a much higher chance of detecting the afterglow .    a schematic block diagram of a potential software system is shown in the figure  [ diagram ]
the system has two components : 1 ) a scheduling system that will assign various observing patches to participating telescopes , and 2 ) a online system that will let observers to upload their images and search for candidate transients .
the algorithms in the scheduling system will check the gbm ec observability of each participating telescope and assign them to different parts of the gbm ec . in doing this
the algorithm will consider individual telescopes fov , sensitivity and local weather conditions .
in addition , it will also assign more than one patch for each astronomer .
on average an amateur astronomer may receive about 40 notices per year .
the exposure time for each patch depends on many factors such as aperture , seeing , type of ccd camera etc and typically may vary from 1 to 30 mins .
the probability of success depends on the telescope configuration ( fov , sensitivity ) , local weather and sky conditions , and the number of patches observed .
however , every amateur observer who submits an observation to the system will get credit for their effort by being a co - author of the subsequent gcn notice that results from a successful detection .
the online system is envisioned to have a web interface where the participants can submit their observations .
it will also have online tools that will compare the submitted observations with existing catalogs and search for the optical afterglow of the grb .
if one of the observations has a positive detection then the system will initiate a follow up observation to establish whether the candidate source is fading .
if the candidate is found to be fading ( telltale signature of a grb afterglow ) then the magnitudes of the two images will be determined and a gcn circular will be sent .
we investigate the feasibility of implementing a system that will coordinate ground based telescopes ( both amateur and professional ) to scan the gbm ec in order to localize gbm bursts .
unlike the gcn system , proposed system will send individual customized messages to telescopes to observe certain patches in the gbm ec .
the scientific objective of the system is by localizing gbm detected burst , we will be able to increase the number of gbm bursts with mutil - wavelength followups potentially with redshifts measurements .
these measurements are scientifically very important because there are hints that gbm bursts may represent significantly different burst population . based on our simulation
, we can detect about 25 grb afterglows per year using just 10 telescopes with @xmath16 field - of - view . with more telescopes participating in the program
, we should be able to detect many more afterglows and study a potentially interesting burst population that is currently inaccessible to the grb community .
we investigate the feasibility of implementing a system that will coordinate ground - based optical telescopes to cover the fermi gbm error circle ( ec ) . 
 the aim of the system is to localize gbm detected grbs and facilitate multi - wavelength follow - up from space and ground . 
 this system will optimize the observing locations in the gbm ec based on individual telescope location , field of view ( fov ) and sensitivity . 
 the proposed system will coordinate gbm ec scanning by professional as well as amateur astronomers around the world . 
 the results of a monte carlo simulation to investigate the feasibility of the project are presented .