A GRB Follow-up System at the Xinglong Observatory and Detection of the High-Redshift GRB 060927

Zheng, W.; Deng, J. S.; Zhai, M.; Xin, L. P.; Qiu, Y.; Wang, Jing; Lu, Xiao-Meng; Wei, J. Y.; Hu, Jingyao

doi:10.1088/1009-9271/8/6/08

Cited by 16 publications

(14 citation statements)

References 32 publications

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“…Among the three GRBs whose redshifts are larger than 4, the GFOX observations yielded a successful detection of the afterglow of GRB 060927 which has a redshift as high as 5.6. Details of the GFOX results of this high-redshift GRB can be found elsewhere [5]. Our system also responded well to the peculiar nearby GRB 060218 [3] which, at a redshift of 0.033, was found to be associated with a supernova [6].…”

Section: Gfox Results During 2006-2009supporting

confidence: 65%

“…We summarize all the GRBs observed by the GFOX from Jan. 2008 to Apr. 2009 in Table 1, totaling 17, while the observation log of those before 2008 have been presented elsewhere [5].…”

Section: Gfox Results During 2006-2009mentioning

confidence: 99%

“…The 2.16-m NAOC telescope was also occasionally used. Detailed descriptions of the telescopes and observing program have been presented elsewhere [5].…”

mentioning

confidence: 99%

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Three years’ systematic GRB follow-up at the Xinglong Observatory and the optical afterglow observations of GRB 080330

Xin

Deng

Zheng

et al. 2010

Sci. China Phys. Mech. Astron.

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We present a brief overview of follow-up observations of GRB afterglows made by the 0.8-m TNT and other telescopes at the Xinglong observatory during the last three years. Our system, dedicated to the measurement of early-time optical afterglow emission, responded to 50 GRBs from Jan. 2006 to Apr. 2009. Among them, about 50% have been successfully detected. The fastest response time is 76 sec (GRB 061110A and GRB 090426) after the space-borne GRB detector was triggered. The redshift distribution spans the range from z = 0.033 (GRB 060218) to z = 5.6 (GRB 060927). We also report the optical photometric follow-up of GRB 080330, which is an X-ray flash, as an example of our observations. GRB, afterglow, follow-up observation, TNT, GRB 080330Detection and follow-up photometry of the GRB optical afterglow, since its first discovery in 1997 [1], has brought about a succession of breakthroughs in our understanding of the nature of GRBs. Ground-based observations of optical afterglows can obtain the afterglow light curves, as well as measure GRB redshifts. An optical photometric detection and the subsequent sub-arcsecond afterglow localization are key inputs to big telescopes for their identification and accurate spectroscopic redshift-measurement of the GRB host galaxy.Fast-response observations are required to reach a decent detection rate of optical afterglows. The GRB afterglow is by its nature a transient phenomenon; its emitting flux generally decays quickly with time roughly following a power-law, or f -t −a with a ~1-2. The Swift satellite [2], launched in late 2004, routinely provides GRB alerts and onboard localization information to ground-based telescopes in nearly real time via the Gamma-ray bursts Coordinates Network (GCN). Many robotic telescopes, mostly of relatively small size, have been set up worldwide to receive the Swift alerts to take afterglow photometry as early as possible.However, dedicated GRB follow-up systems were still relatively few in the East Asian region before 2006. This means that the golden chance to detect the optical afterglow would be missed if a GRB happens to occur during the night in the East Asian region.

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Section: Gfox Results During 2006-2009supporting

confidence: 65%

“…We summarize all the GRBs observed by the GFOX from Jan. 2008 to Apr. 2009 in Table 1, totaling 17, while the observation log of those before 2008 have been presented elsewhere [5].…”

Section: Gfox Results During 2006-2009mentioning

confidence: 99%

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Three years’ systematic GRB follow-up at the Xinglong Observatory and the optical afterglow observations of GRB 080330

Xin

Deng

Zheng

et al. 2010

Sci. China Phys. Mech. Astron.

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“…Subsequently, a series of optical multiband follow-up observations were also carried out by Xinglong 0.8 m and 1.0 m telescope in China (Zheng et al 2008), the Lulin One-meter telescope (LOT) in Taiwan Urata et al 2005), and the 0.5 m MITSuME telescope in Japan (Kotani 2005). About one year after the burst, the host galaxy of GRB 071112C was clearly detected with the 3.8 m Canada-France-Hawaii Telescope (CFHT).…”

Section: Optical and X-ray Temporal Analysismentioning

confidence: 99%

GRB 071112c: A Case Study of Different Mechanisms in X-Ray and Optical Temporal Evolution

Huang¹,

Urata²,

Tung³

et al. 2012

ApJ

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We present a study on GRB 071112C X-ray and optical light curves. In these two wavelength ranges, we have found different temporal properties. The R-band light curve showed an initial rise followed by a single power-law decay, while the X-ray light curve was described by a single power-law decay plus a flare-like feature. Our analysis shows that the observed temporal evolution cannot be described by the external shock model in which the X-ray and optical emission are produced by the same emission mechanism. No significant color changes in multi-band light curves and a reasonable value of the initial Lorentz factor (Γ 0 = 275 ± 20) in a uniform interstellar medium support the afterglow onset scenario as the correct interpretation for the early R band rise. The result suggests that the optical flux is dominated by afterglow. Our further investigations show that the X-ray flux could be created by an additional feature related to energy injection and X-ray afterglow. Different theoretical interpretations indicate the additional feature in X-ray can be explained by either late internal dissipation or local inverse-Compton scattering in the external shock.

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“…The R-band optical light curve also starts with a steep decay ( 5.4 a~-by setting the zero time to the BAT trigger time), but it is earlier than the initial steep decay in the X-ray light curve. The first optical data point was obtained during the last pulse of the prompt gamma-rays (from 95 to 115 s post the 9 TNT is a 0.8 m telescope and runs by a custom-designed automation system for GRB follow-up observations (Zheng et al 2008) 13 The slope is obtained by setting the zero time to the BAT trigger. It is physically meaningful only when we know the ejection time associated with the prompt pulse/flare, i.e., its intrinsic zero time (Liang et al 2006).…”

mentioning

confidence: 99%

Multi-Wavelength Observations of GRB 111228a and Implications for the Fireball and Its Environment

Xin

Wang

Lin

et al. 2016

ApJ

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Observations of very early multi-wavelength afterglows are critical to reveal the properties of the radiating fireball and its environment as well as the central engine of gamma-ray bursts (GRBs). We report our optical observations of GRB 111228A from 95 s to about 50 hr after the burst trigger and investigate its properties of the prompt gamma-rays and the ambient medium using our data and the data from the Swift and Fermi missions. Our joint optical and X-ray spectral fits to the afterglow data show that the ambient medium features a low dust-to-gas ratio. Incorporating the energy injection effect, our best fit to the afterglow light curves with the standard afterglow model via the Markov Chain Monte Carlo technique shows that 6.9 0.3 10 e 2 ( )  = ´-, E 7.73 0.62 10 , 6.32 0.86 10 ergThe low medium density likely implies that the afterglow jet may be in a halo or in a hot ISM. A chromatic shallow decay segment observed in the optical and X-ray bands is well explained with the long-lasting energy injection from the central engine, which would be a magnetar with a period of about 1.92 ms inferred from the data. The E p of its time-integrated prompt gamma-ray spectrum is ∼26 KeV. Using the initial Lorentz factor ( 476 0 237) derived from our afterglow model fit, it is found that GRB 111228A satisfies the L E p z iso , 0 --G relation and bridges the typical GRBs and low luminosity GRBs in this relation.

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A GRB Follow-up System at the Xinglong Observatory and Detection of the High-Redshift GRB 060927

Cited by 16 publications

References 32 publications

Three years’ systematic GRB follow-up at the Xinglong Observatory and the optical afterglow observations of GRB 080330

Three years’ systematic GRB follow-up at the Xinglong Observatory and the optical afterglow observations of GRB 080330

GRB 071112c: A Case Study of Different Mechanisms in X-Ray and Optical Temporal Evolution

Multi-Wavelength Observations of GRB 111228a and Implications for the Fireball and Its Environment

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