Photometric calibrations and characterization of the 4K$$\times $$4K CCD imager, the first-light axial port instrument for the 3.6m DOT

Kumar, Amit; Singh, Avinash; Yadav, R. K. S.; Reddy, B.K.; Nanjappa, Nandish; Yadav, Shobhit; Srinivasan, R.

doi:10.1007/s12036-022-09798-8

Cited by 8 publications

(7 citation statements)

References 18 publications

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“…3.6 m DOT: We performed the optical observations of the afterglow of GRB 201015A starting on 2020 October 16 at 13:09:07.2 UT (∼0.6 day post burst) using 3.6 m DOT located at the Devasthal observatory, which is part of the Aryabhatta Research Institute of Observational Sciences (ARIES), India. We acquired multiple frames in the B, V, R, and I filters (with an exposure time of 10 minutes in each) using the 4K × 4K CCD IMAGER (Kumar et al 2022b) mounted on the main port of 3.6 m DOT. In stacked DOT images, we clearly detect the optical afterglow of GRB 201015A consistent with the error region of NOT observations Malesani et al (2020).…”

Section: Optical Afterglows Of Grb 201015a and Grb 201216cmentioning

confidence: 99%

“…Table B7 Magnitudes of 13 Secondary Standard Stars in the Vicinity of GRB 201015A, Calibrated against the Landolt Standard Field PG 0231Note. Observations were obtained using the 4K × 4K CCD Imager(Kumar et al 2022b), the first light instrument on the axial port of 3.6 m DOT. The quoted magnitude values are in the AB system and are not corrected for foreground extinction.Note.…”

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confidence: 99%

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Prompt Emission and Early Optical Afterglow of Very-high-energy Detected GRB 201015A and GRB 201216C: Onset of the External Forward Shock

Ror

Gupta

Jelínek

et al. 2023

ApJ

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We present a detailed prompt emission and early optical afterglow analysis of the two very-high-energy (VHE) detected bursts GRB 201015A and GRB 201216C, and their comparison with a subset of similar bursts. Time-resolved spectral analysis of multistructured GRB 201216C using the Bayesian binning algorithm revealed that during the entire duration of the burst, the low-energy spectral index (α pt) remained below the limit of the synchrotron line of death. However, statistically some of the bins supported the additional thermal component. Additionally, the evolution of spectral parameters showed that both the peak energy (E p) and α pt tracked the flux. These results were further strengthened using the values of the physical parameters obtained by synchrotron modeling of the data. Our earliest optical observations of both bursts using the F/Photometric Robotic Atmospheric Monitor Observatorio del Roque de los Muchachos and Burst Observer and Optical Transient Exploring System robotic telescopes displayed a smooth bump in their early optical light curves, consistent with the onset of the afterglow due to synchrotron emission from an external forward shock. Using the observed optical peak, we constrained the initial bulk Lorentz factors of GRB 201015A and GRB 201216C to Γ0 = 204 and Γ0 = 310, respectively. The present early optical observations are the earliest known observations constraining outflow parameters and our analysis indicate that VHE detected bursts could have a diverse range of observed luminosity within the detectable redshift range of present VHE facilities.

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Section: Optical Afterglows Of Grb 201015a and Grb 201216cmentioning

confidence: 99%

mentioning

confidence: 99%

Prompt Emission and Early Optical Afterglow of Very-high-energy Detected GRB 201015A and GRB 201216C: Onset of the External Forward Shock

Ror

Gupta

Jelínek

et al. 2023

ApJ

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“…The late-time optical observations of the two events, i.e., GRB 171010A/SN 2017htp and GRB 171205A/SN 2017iuk were obtained using the 4K×4K CCD Imager mounted at the 3.6m DOT (Pandey et al, 2018;Kumar et al, 2022), finding charts are shown in Figures 2 and 3, respectively. Observations of GRB/SNe cases presented in this study were acquired with 2×2 binning, a gain of 5 e − /ADU, and a readout speed of 1 MHz, having readout noise of ∼10 e − .…”

Section: Optical Observations and Analysismentioning

confidence: 99%

“…Calibrated magnitudes of the secondary standard stars in the field of GRB 171010A/SN 2017htp observed using the 4K×4K CCD Imager mounted at the axial port of the 3.6m DOT (Pandey et al, 2018;Kumar et al, 2022)…”

Section: Table A1mentioning

confidence: 99%

“…This article presents the prompt emission data analysis of GRB 171010A and GRB 171205A, late-time optical observations and the semi-analytical light-curve modelling of SN 2017htp and SN 2017iuk (along with SLSN 2011kl) to investigate the underlying physical mechanisms behind such rare events and to constrain some of the physical parameters. The optical observations of the above-discussed GRB-SNe are acquired using the first light instrument called 4K×4K CCD Imager mounted at the axial port of the recently commissioned 3.6m Devasthal Optical Telescope (3.6m DOT; Pandey et al, 2018;Kumar et al, 2022). The longitudinal advantage of India and specifically the 3.6m DOT at Nainital is crucial, having a significant temporal gap with its site in the middle of the longitude belt of 180 • between Eastern Australia (160 • E) and the Canary Islands (20 • W), vital for transient studies at optical-NIR frequencies (Kumar et al, 2018;Pandey et al, 2018;Sagar et al, 2019;Kumar et al, 2020bKumar et al, , 2021a.…”

Section: Introductionmentioning

confidence: 99%

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Tale of GRB 171010A/SN 2017htp and GRB 171205A/SN 2017iuk: Magnetar origin?

Kumar,

Pandey,

Gupta

et al. 2022

Preprint

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We present late-time optical follow-up observations of GRB 171010A/SN 2017htp ( = 0.33) and low-luminosity GRB 171205A/SN 2017iuk ( = 0.037) acquired using the 4K×4K CCD Imager mounted at the 3.6m Devasthal Optical Telescope (3.6m DOT) along with the prompt emission data analysis of these two interesting bursts. The prompt characteristics (other than brightness) such as spectral hardness, 90 , and minimum variability time-scale are comparable for both the bursts. The isotropic -ray and kinetic energies of the plateau phase of GRB 171205A are found to be less than the maximum energy budget of magnetars, supporting magnetar as a central engine powering source. The new optical data of SN 2017htp and SN 2017iuk presented here, along with published ones, indicate that SN 2017htp is one of the brightest and SN 21017iuk is among the faintest GRB associated SNe (GRB-SNe). Semianalytical light-curve modelling of SN 2017htp, SN 2017iuk and only known GRB associated superluminous supernova (SLSN 2011kl) are performed using the MINIM code. The model with a spin-down millisecond magnetar as a central engine powering source nicely reproduced the bolometric light curves of all three GRB-SNe mentioned above. The magnetar central engines for SN 2017htp, SN 2017iuk, and SLSN 2011kl exhibit values of initial spin periods higher and magnetic fields closer to those observed for long GRBs and H-deficient SLSNe. Detection of these rare events at such late epochs also demonstrates the capabilities of the 3.6m DOT for deep imaging considering longitudinal advantage in the era of time-domain astronomy.

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Pathway to Devasthal astronomical observatory, ARIES

Sagar,

Gopal-Krishna

2024

Indian J Hist. Sci.

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Photometric calibrations and characterization of the 4K$$\times $$4K CCD imager, the first-light axial port instrument for the 3.6m DOT

Cited by 8 publications

References 18 publications

Prompt Emission and Early Optical Afterglow of Very-high-energy Detected GRB 201015A and GRB 201216C: Onset of the External Forward Shock

Prompt Emission and Early Optical Afterglow of Very-high-energy Detected GRB 201015A and GRB 201216C: Onset of the External Forward Shock

Tale of GRB 171010A/SN 2017htp and GRB 171205A/SN 2017iuk: Magnetar origin?

Pathway to Devasthal astronomical observatory, ARIES

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