The case for a high-redshift origin of GRB 100205A

Chrimes, A. A.; Levan, A. J.; Stanway, Elizabeth R.; Berger, E.; Bloom, J.; Cenko, S. Bradley; Cobb, B. E.; Cucchiara, Antonino; Fruchter, A.; Gompertz, B. P.; Hjorth, J.; Jakobsson, P.; Lyman, J.; O’Brien, P. T.; Perley, D.; Tanvir, N. R.; Wheatley, P. J.; Wiersema, K.

doi:10.1093/mnras/stz1811

Cited by 5 publications

(3 citation statements)

References 60 publications

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“…Furthermore, the burst lay behind a complex region of Galactic dust, making the foreground extinction for this event high but also poorly determined (Tanvir et al 2006). Then, Chrimes et al (2019) report on observations of GRB 100205A, which had an afterglow that was yet again significantly fainter than that of GRB 090429B, and no reasonably precise photo-z could be determined, but it could lie at up to z ≈ 8.…”

Section: The High-redshift Samplementioning

confidence: 99%

“…We therefore conclude there is no evidence for significant afterglow luminosity evolution between z ≳ 6 to 1.4 < z ≲ 6. Now, the problem that arises is that most z ≳ 6 GRB afterglows have only been observed, and have only really been observable, by large ( / ⃝ ≳ 2 m) telescopes with NIR capabilities, such as the 2.2 m MPG/GROND, the 3.8 m United Kingdom InfraRed Telescope (UKIRT)/Wide Field Infrared Camera (WFCAM; Casali et al 2007), and "big glass" such as the 8.2 m VLT/(ISAAC or HAWKI), 8.1 m Gemini/NIRI, and 10.0 m Keck/MOSFIRE (Chrimes et al 2019). This implies that few high-z GRB afterglows (specifically the aforementioned, very luminous GRBs 050904, 130606A, as well as, with some extrapolation, GRBs 080913, 210905A) have actually been detected during the time after trigger that Gamow will be attaining its first finding chart; and this sample is very clearly biased toward the most luminous high redshift events as only those have been detectable by rapidly slewing telescope robots of small aperture.…”

Section: The High-redshift Samplementioning

confidence: 99%

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Fires in the deep: The luminosity distribution of early-time gamma-ray-burst afterglows in light of the Gamow Explorer sensitivity requirements

Kann,

White,

Ghirlanda

et al. 2024

A&A

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Gamma-ray bursts (GRBs) are ideal probes of the Universe at high redshift ($z$), pinpointing the locations of the earliest star-forming galaxies and providing bright backlights with simple featureless power-law spectra that can be used to spectrally fingerprint the intergalactic medium and host galaxy during the period of reionization. Future missions such as Gamow Explorer (hereafter )\ are being proposed to unlock this potential by increasing the rate of identification of high-$z$ ($z>5$) GRBs in order to rapidly trigger observations from $6-10$ m ground telescopes, the James Webb Space Telescope (JWST), and the upcoming Extremely Large Telescopes (ELTs). was proposed to the NASA 2021 Medium-Class Explorer (MIDEX) program as a fast-slewing satellite featuring a wide-field lobster-eye X-ray telescope (LEXT) to detect and localize GRBs with arcminute accuracy, and a narrow-field multi-channel photo-$z$ infrared telescope (PIRT) to measure their photometric redshifts for $>80<!PCT!>$ of the LEXT detections using the Lyman-alpha dropout technique. We use a large sample of observed GRB afterglows to derive the PIRT sensitivity requirement. We compiled a complete sample of GRB optical--near-infrared (optical--NIR) afterglows from 2008 to 2021, adding a total of 66 new afterglows to our earlier sample, including all known high-$z$ GRB afterglows. This sample is expanded with over 2837 unpublished data points for 40 of these GRBs. We performed full light-curve and spectral-energy-distribution analyses of these afterglows to derive their true luminosity at very early times. We compared the high-$z$ sample to the comparison sample at lower redshifts. For all the light curves, where possible, we determined the brightness at the time of the initial finding chart of at different high redshifts and in different NIR bands. This was validated using a theoretical approach to predicting the afterglow brightness. We then followed the evolution of the luminosity to predict requirements for ground- and space-based follow-up. Finally, we discuss the potential biases between known GRB afterglow samples and those to be detected by We find that the luminosity distribution of high-$z$ GRB afterglows is comparable to those at lower redshift, and we therefore are able to use the afterglows of lower-$z$ GRBs as proxies for those at high $z$. We find that a PIRT sensitivity of $15\ (21 mag AB) in a 500 s exposure simultaneously in five NIR bands within 1000s of the GRB trigger will meet the mission requirements. Depending on the $z$ and NIR band, we find that between 75<!PCT!> and 85<!PCT!> of all afterglows at $z>5$ will be recovered by at $5 detection significance, allowing the determination of a robust photo-$z$. As a check for possible observational biases and selection effects, we compared the results with those obtained through population-synthesis models, and find them to be consistent. and other high-$z$ GRB missions will be capable of using a relatively modest 0.3m onboard NIR photo-$z$ telescope to rapidly identify and report high-$z$ GRBs for further follow-up by larger facilities, opening a new window onto the era of reionization and the high-redshift Universe.

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Section: The High-redshift Samplementioning

confidence: 99%

Section: The High-redshift Samplementioning

confidence: 99%

Fires in the deep: The luminosity distribution of early-time gamma-ray-burst afterglows in light of the Gamow Explorer sensitivity requirements

Kann,

White,

Ghirlanda

et al. 2024

A&A

View full text Add to dashboard Cite

show abstract

“…With the rapid slewing capabilities of Swift, observations with Swift/UVOT have enabled us to rule out these dark GRBs as being due to factors such as a lack of sensitivity, late observation times, and rapid temporal decays [173]. The low detection rate or "darkness", could however, be due to one or more of the following: a high background due to a small Sun-to-field angle [174], a large galactic extinction (e.g., [174,175]), a high circumburst extinction (e.g., [176][177][178]), intrinsic faintness [177], and Lyα damping due to high redshift (e.g., [176,177,179]). Several studies, including those using Swift/UVOT observations (e.g., [72]), have suggested that high circumburst extinction and high-redshift are the two main causes for why GRBs are 'dark' [67,172,173,180].…”

Section: Dark Grbsmentioning

confidence: 99%

Swift/UVOT: 18 Years of Long GRB Discoveries and Advances

Oates

2023

Universe

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The Neil Gehrels Swift Observatory (Swift) has been in operation for 18 years. The Ultra-Violet/Optical Telescope (UVOT) onboard Swift was designed to capture the earliest optical/UV emission from gamma-ray bursts (GRBs), spanning the first few minutes to days after the prompt gamma-ray emission. In this article, we provide an overview of the long GRBs (whose prompt gamma-ray duration is >2 s) observed by the Swift/UVOT, and review the major discoveries that have been achieved by the Swift/UVOT over the last 18 years. We discuss where improvements have been made to our knowledge and understanding of the optical/UV emission, particularly the early optical/UV afterglow.

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Detecting the near-infrared afterglows of high-redshift gamma-ray bursts using CAGIRE

Fortin,

Atteia,

Nouvel de la Flèche

et al. 2024

A&A

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Transient sky astronomy is entering a new era with the advent of the Space Variable Objects Monitor mission (SVOM), successfully launched on 22 June 2024. The primary goal of SVOM is to monitor the hard X-ray sky searching for gamma-ray bursts (GRBs). On top of its on-board follow-up capabilities, SVOM will be backed by its ground segment composed of several facilities, including the near-infrared (NIR) imager CAGIRE. Mounted on the robotic telescope COLIBRI, it will be a unique instrument capable of performing fast follow-up of GRB afterglows in the J and H bands, ideal for capturing high-redshift (z$>$6) and/or obscured GRBs. This paper is aimed at estimating the performances of CAGIRE for GRB NIR afterglow detection based on the characteristics of the detector and the specificities of the COLIBRI telescope. Quickly fading GRB afterglows pose challenges that should be addressed by adapting observing strategies to the capabilities of CAGIRE. We used an end-to-end image simulator to produce realistic CAGIRE images, taking into account the results from the characterisation of the ALFA detector used by CAGIRE. We implemented a GRB afterglow generator that simulates infrared light curves and spectra based on published observation of distant GRBs (z$>$6). We retrieved the photometry of nine GRB afterglows in various scenarios covered by CAGIRE. Capturing afterglows as early as one minutes after the burst allows for the identification of a NIR counterpart in the brightest four events. When artificially redshifted even further away, these events remain detectable by CAGIRE up to z=9.6 in the J band and z=13.3 in H band, indicating the pioneering potential of CAGIRE in identifying the most distant GRBs to date.

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The case for a high-redshift origin of GRB 100205A

Cited by 5 publications

References 60 publications

Fires in the deep: The luminosity distribution of early-time gamma-ray-burst afterglows in light of the Gamow Explorer sensitivity requirements

Fires in the deep: The luminosity distribution of early-time gamma-ray-burst afterglows in light of the Gamow Explorer sensitivity requirements

Swift/UVOT: 18 Years of Long GRB Discoveries and Advances

Detecting the near-infrared afterglows of high-redshift gamma-ray bursts using CAGIRE

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