Difference between revisions of "Triggers:GRBs"
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| − | == Gamma-Ray Burst Optical Afterglows == | + | === Gamma-Ray Burst Optical Afterglows === |
| − | [[File:GRB-schematic_lightcurve.png|350px|right]] | + | [[File:GRB-schematic_lightcurve.png|350px|border|right]] |
| − | Gamma-ray bursts (GRBs) are extremely energetic, brief and unpredictable explosions | + | Gamma-ray bursts (GRBs) are extremely energetic, brief and unpredictable explosions occurring on cosmological distances. They represent the most luminous events in the gamma-ray part of the electromagnetic spectrum known in the universe. Often, the prompt gamma-ray emission is followed by an afterglow emitted at longer wavelengths (from X-rays to radio), which can last for several days. Comprehensive review on GRBs and their physics can be found in [http://adsabs.harvard.edu/abs/2004RvMP...76.1143P Piran 2004] or [http://adsabs.harvard.edu/abs/2006RPPh...69.2259M Meszaros 2006]. |
| − | GRB explosions are believed to be collimated, rather than spherical [http://adsabs.harvard.edu/abs/2007RMxAC..27..140G Granot 2007]. Thus the material, ejected by the explosion, is expanding in the form of a bimodal jet, characterized by an initial half-opening angle | + | GRB explosions are believed to be collimated, rather than spherical [http://adsabs.harvard.edu/abs/2007RMxAC..27..140G Granot 2007]. Thus the material, ejected by the explosion, is expanding in the form of a bimodal jet, characterized by an initial half-opening angle [[File:theta.png]]. The shape of the light curve depends on the relative position of the observer's line-of-sight and the axis of the jet cone. We can describe that with an angle [[File:thetaobs.png]] between both directions. We talk about an on-axis GRB and a 'regular' optical afterglow when [[File:theta1.png]]. In the case of [[File:theta2.png]], we can not observe the prompt gamma-ray emission. Due to the beaming effect, we could still observe the so called orphan afterglow (details in [http://adsabs.harvard.edu/abs/2007RMxAC..27..140G Granot 2007] or ). A schematic afterglow light curves for different jet half-opening angles and viewing angles are shown in figure on the right. |
| − | [[File:kann.png|350px|left]] | + | [[File:kann.png|thumb|350px|border|left|A large sample of regular (on-axis) optical afterglow light curves, corrected for Galactic extinction [http://adsabs.harvard.edu/abs/2010ApJ...720.1513K Kann et al. 2010].]] |
| − | A large sample of observed optical | + | A large sample of observed optical light curves of regular 'on-axis' afterglows is shown in figure on the left ([http://adsabs.harvard.edu/abs/2010ApJ...720.1513K Kann et al. 2010]). |
Observations made by the Swift satellite imply that there are approximately 300 on-axis GRBs per year for which we could observe an optical afterglow. | Observations made by the Swift satellite imply that there are approximately 300 on-axis GRBs per year for which we could observe an optical afterglow. | ||
| − | [[File:Color-oa.png|325px|right]] | + | [[File:Color-oa.png|thumb|325px|border|right|Color-color (B-V vs. V-R) diagram of optical afterglows of long GRBs [http://adsabs.harvard.edu/abs/2001A%26A...377..450S Šimon et al. 2001] [http://adsabs.harvard.edu/abs/2004AIPC..727..487S Šimon et al. 2004]..]] |
Even though orphan afterglows have not been conclusively detected yet, they have been studied a great deal over the last 15 years and various estimations on their detectability have been made ([http://adsabs.harvard.edu/abs/2007RMxAC..27..140G Granot 2007] and references therein). | Even though orphan afterglows have not been conclusively detected yet, they have been studied a great deal over the last 15 years and various estimations on their detectability have been made ([http://adsabs.harvard.edu/abs/2007RMxAC..27..140G Granot 2007] and references therein). | ||
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It has been observed, that the color indices (R - I), (V -R) and (B - V) of a sample of observed afterglows are roughly constant in the first 10 days of observation, i.e. their time evolution is negligible. This property could serve as a mean to recognize an afterglow and to distinguish it from other possible sources [http://adsabs.harvard.edu/abs/2001A%26A...377..450S Šimon et al. 2001] [http://adsabs.harvard.edu/abs/2004AIPC..727..487S Šimon et al. 2004]. Color-color (B-V vs. V-R) diagram of optical afterglows of long GRBs is shown in figure on the right. All the color indices were corrected for the Galactic reddening. Multiple indices of the same optical afterglow are connected by lines for convenience. Optical afterglows of the ensemble are denoted by open red circles. The mean colors (centroid) of the whole ensemble, including the standard deviations, are marked by the large cross. The outlying optical afterglow of GRB 060218 (closed blue circles) is not included in the calculation of the centroid. The representative reddening paths for E(B-V) = 0.5 mag are shown; they show how much and where the observed data point would move without proper correction (even erroneous correction would thus shift the point only slightly and in predictable direction). Adapted from [http://adsabs.harvard.edu/abs/2001A%26A...377..450S Šimon et al. 2001] [http://adsabs.harvard.edu/abs/2004AIPC..727..487S Šimon et al. 2004] where a detailed information can be found. | It has been observed, that the color indices (R - I), (V -R) and (B - V) of a sample of observed afterglows are roughly constant in the first 10 days of observation, i.e. their time evolution is negligible. This property could serve as a mean to recognize an afterglow and to distinguish it from other possible sources [http://adsabs.harvard.edu/abs/2001A%26A...377..450S Šimon et al. 2001] [http://adsabs.harvard.edu/abs/2004AIPC..727..487S Šimon et al. 2004]. Color-color (B-V vs. V-R) diagram of optical afterglows of long GRBs is shown in figure on the right. All the color indices were corrected for the Galactic reddening. Multiple indices of the same optical afterglow are connected by lines for convenience. Optical afterglows of the ensemble are denoted by open red circles. The mean colors (centroid) of the whole ensemble, including the standard deviations, are marked by the large cross. The outlying optical afterglow of GRB 060218 (closed blue circles) is not included in the calculation of the centroid. The representative reddening paths for E(B-V) = 0.5 mag are shown; they show how much and where the observed data point would move without proper correction (even erroneous correction would thus shift the point only slightly and in predictable direction). Adapted from [http://adsabs.harvard.edu/abs/2001A%26A...377..450S Šimon et al. 2001] [http://adsabs.harvard.edu/abs/2004AIPC..727..487S Šimon et al. 2004] where a detailed information can be found. | ||
| + | == Detecting GRBs with Gaia == | ||
| + | |||
| + | [[File:F5.png|thumb|400px|border|right|GRB on-axis and OAs detection rate in five years of Gaia's operation as a function of limiting magnitudes. In the case of OAs, the results are given for two different circumburst environments.]] | ||
| + | |||
| + | [[File:F6.png|thumb|400px|border|right|Distribution of magnitudes, which are associated with detected afterglows (black), same magnitudes at the time of the first detection (grey) and magnitudes of afterglows detected by the second telescope (red) in the case of on-axis simulation. The results are given for a time of five years.]] | ||
| + | |||
| + | In order to predict the number of optical afterglow detections with Gaia in five years of it's time of operation, a simulation was performed. The simulation took into account a scanning law of Gaia, it's field of view, etc. It consists of two parts: one for regular 'on-axis' afterglows and the other for orphan afterglows. In the former the observational data were used to constrain the parameters needed in the simulation (i.e. initial afterglow magnitude distribution, number of afterglows occurring in five years, etc.), while in the latter the parameters were obtained from theoretical predictions. Details on the simulation are given in [[#Simulation references|simulation references]]. | ||
| + | |||
| + | Number of detections in respect to limiting magnitude are shown on the the right in the top figure for the case of on-axis and orphan afterglows. The average GRB orphan-afterglow detection rate has been simulated for two different circumburst environments. | ||
| + | |||
| + | Bottom, right figure shows initial magnitude distribution of detected on-axis afterglows (black), same distribution at the time of the first detection (gray) and the distribution of detections with the second telescope. Similar plot for orphan afterglows is given in [[#Simulation references|references]]. | ||
| − | == | + | Since GRB afterglows are initially rapidly fading and they will be observed for 4.4 seconds by each CCD camera, the change of magnitude in that time could in principle be observable. For all detected afterglows in our simulations, we therefore calculated the change of magnitude in 4.4 s, corresponding to observations by two successive CCDs, and also for observations lasting as long as a specific afterglow is in the telescope's field of view. The distribution of the change of magnitude for both cases is shown in the bottom figure on the left. Since the expected photometric error of Gaia at $M_{\rm lim} = 20$ mag will be 10 mmag at best (though it will be smaller for brighter sources [http://www.rssd.esa.int/index.php?project=GAIA&page=index ESA]), the chances of observing the change in magnitudes will be small. |
| + | |||
| + | To summarize: the number of expected GRB optical afterglow detections with Gaia satellite during it's five years of expected operation is of the order of a few tens. Most of the expected detections are of the orphan afterglows, while the possibility of an on-axis afterglow detection is small (less than 10). The problem of afterglow recognition and poor time sampling of the light curve, in addition to the small number of expected detections, makes the study of GRB optical afterglows with Gaia difficult. On the other hand, since orphan afterglows have not been conclusively detected yet, a possible detection would provide valuable new data. | ||
| + | |||
| + | [[File:F10.png|thumb|400px|border|center|Left: Distribution of the change in magnitude in 4.4 s (corresponding to an observation with 2 successive CCDs) (black) and the change of magnitude in the time in which an afterglow is in the entire field of view (red) for the on-axis case. Right: Distribution of the change in magnitude in the time in which an orphan afterglow is in the field of view. Black distribution corresponds to detection after the peak in a light curve while red distribution corresponds to detection before the peak.]] | ||
| + | |||
| + | == Simulation references == | ||
| − | + | *J. Japelj, A. Gomboc, Gaia Alerts Workshop 2011, [http://www.ast.cam.ac.uk/~wyrzykow/GAIA/GSAW2011/Talks/gaia_alerts_japelj.pdf presentation] and [http://www.ast.cam.ac.uk/~wyrzykow/GAIA/GSAW2011/Movies/Japelj-GRBs.mov video recording] of the talk: The detectability of GRB optical counterparts with Gaia | |
| + | *J. Japelj, A. Gomboc, 2011, [http://arxiv.org/abs/1107.2858 arXiv:1107.2858] | ||
| − | |||
| − | |||
| − | + | [[User:Jure.Japelj|Jure.Japelj]] 11:18, 15 July 2011 (BST) | |
Latest revision as of 09:34, 8 September 2011
Gamma-Ray Burst Optical Afterglows
Gamma-ray bursts (GRBs) are extremely energetic, brief and unpredictable explosions occurring on cosmological distances. They represent the most luminous events in the gamma-ray part of the electromagnetic spectrum known in the universe. Often, the prompt gamma-ray emission is followed by an afterglow emitted at longer wavelengths (from X-rays to radio), which can last for several days. Comprehensive review on GRBs and their physics can be found in Piran 2004 or Meszaros 2006.
GRB explosions are believed to be collimated, rather than spherical Granot 2007. Thus the material, ejected by the explosion, is expanding in the form of a bimodal jet, characterized by an initial half-opening angle 
. The shape of the light curve depends on the relative position of the observer's line-of-sight and the axis of the jet cone. We can describe that with an angle 
between both directions. We talk about an on-axis GRB and a 'regular' optical afterglow when 
. In the case of 
, we can not observe the prompt gamma-ray emission. Due to the beaming effect, we could still observe the so called orphan afterglow (details in Granot 2007 or ). A schematic afterglow light curves for different jet half-opening angles and viewing angles are shown in figure on the right.
A large sample of observed optical light curves of regular 'on-axis' afterglows is shown in figure on the left (Kann et al. 2010).
Observations made by the Swift satellite imply that there are approximately 300 on-axis GRBs per year for which we could observe an optical afterglow.
Even though orphan afterglows have not been conclusively detected yet, they have been studied a great deal over the last 15 years and various estimations on their detectability have been made (Granot 2007 and references therein).
It has been observed, that the color indices (R - I), (V -R) and (B - V) of a sample of observed afterglows are roughly constant in the first 10 days of observation, i.e. their time evolution is negligible. This property could serve as a mean to recognize an afterglow and to distinguish it from other possible sources Šimon et al. 2001 Šimon et al. 2004. Color-color (B-V vs. V-R) diagram of optical afterglows of long GRBs is shown in figure on the right. All the color indices were corrected for the Galactic reddening. Multiple indices of the same optical afterglow are connected by lines for convenience. Optical afterglows of the ensemble are denoted by open red circles. The mean colors (centroid) of the whole ensemble, including the standard deviations, are marked by the large cross. The outlying optical afterglow of GRB 060218 (closed blue circles) is not included in the calculation of the centroid. The representative reddening paths for E(B-V) = 0.5 mag are shown; they show how much and where the observed data point would move without proper correction (even erroneous correction would thus shift the point only slightly and in predictable direction). Adapted from Šimon et al. 2001 Šimon et al. 2004 where a detailed information can be found.
Detecting GRBs with Gaia
In order to predict the number of optical afterglow detections with Gaia in five years of it's time of operation, a simulation was performed. The simulation took into account a scanning law of Gaia, it's field of view, etc. It consists of two parts: one for regular 'on-axis' afterglows and the other for orphan afterglows. In the former the observational data were used to constrain the parameters needed in the simulation (i.e. initial afterglow magnitude distribution, number of afterglows occurring in five years, etc.), while in the latter the parameters were obtained from theoretical predictions. Details on the simulation are given in simulation references.
Number of detections in respect to limiting magnitude are shown on the the right in the top figure for the case of on-axis and orphan afterglows. The average GRB orphan-afterglow detection rate has been simulated for two different circumburst environments.
Bottom, right figure shows initial magnitude distribution of detected on-axis afterglows (black), same distribution at the time of the first detection (gray) and the distribution of detections with the second telescope. Similar plot for orphan afterglows is given in references.
Since GRB afterglows are initially rapidly fading and they will be observed for 4.4 seconds by each CCD camera, the change of magnitude in that time could in principle be observable. For all detected afterglows in our simulations, we therefore calculated the change of magnitude in 4.4 s, corresponding to observations by two successive CCDs, and also for observations lasting as long as a specific afterglow is in the telescope's field of view. The distribution of the change of magnitude for both cases is shown in the bottom figure on the left. Since the expected photometric error of Gaia at $M_{\rm lim} = 20$ mag will be 10 mmag at best (though it will be smaller for brighter sources ESA), the chances of observing the change in magnitudes will be small.
To summarize: the number of expected GRB optical afterglow detections with Gaia satellite during it's five years of expected operation is of the order of a few tens. Most of the expected detections are of the orphan afterglows, while the possibility of an on-axis afterglow detection is small (less than 10). The problem of afterglow recognition and poor time sampling of the light curve, in addition to the small number of expected detections, makes the study of GRB optical afterglows with Gaia difficult. On the other hand, since orphan afterglows have not been conclusively detected yet, a possible detection would provide valuable new data.
Simulation references
- J. Japelj, A. Gomboc, Gaia Alerts Workshop 2011, presentation and video recording of the talk: The detectability of GRB optical counterparts with Gaia
- J. Japelj, A. Gomboc, 2011, arXiv:1107.2858
Jure.Japelj 11:18, 15 July 2011 (BST)
