The Late-time Afterglow Evolution of Long Gamma-Ray Bursts GRB 160625B and GRB 160509A

Kangas, T.; Fruchter, A.; Cenko, S. Bradley; Corsi, A.; Postigo, A. de Ugarte; Pe’er, Asaf; Vogel, S. N.; Cucchiara, Antonino; Gompertz, B.; Graham, John F.; Levan, A. J.; Misra, Kuntal; Perley, D.; Racusin, J. L.; Tanvir, N. R.

doi:10.3847/1538-4357/ab8799

Cited by 18 publications

(11 citation statements)

References 77 publications

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“…Using radio observations at ∼12.7 days (Ho et al 2020c), for the case where ν m < ν radio < ν c < ν X−rays we find that ν c ∼ 6.3 × 10 16 Hz for p = 2 (see Fig. 4), which is consistent with the behavior observed for GRB afterglows at late times (see, e.g., Kangas et al 2020) and it is also consistent with the radio SED presented in Fig. 5 in Ho et al (2020c).…”

Section: Discussionsupporting

confidence: 87%

Broad-line type Ic SN 2020bvc

Izzo

Auchettl

Hjorth

et al. 2020

A&A

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Long-duration gamma-ray bursts (GRBs) are almost unequivocally associated with very energetic, broad-line supernovae of Type Ic-BL. While the gamma-ray emission is emitted in narrow jets, the SN emits radiation isotropically. Therefore, it has been hypothesized that some SN Ic-BL not associated with GRBs arise from events with inner engines such as off-axis GRBs or choked jets. Here we present observations of the nearby (d = 120 Mpc) SN 2020bvc (ASAS-SN 20bs) that support this scenario. Swift-UVOT observations reveal an early decline (up to two days after explosion), while optical spectra classify it as a SN Ic-BL with very high expansion velocities (≈70 000 km s−1), similar to that found for the jet-cocoon emission in SN 2017iuk associated with GRB 171205A. Moreover, the Swift X-Ray Telescope and CXO X-ray Observatory detected X-ray emission only three days after the SN and decaying onward, which can be ascribed to an afterglow component. Cocoon and X-ray emission are both signatures of jet-powered GRBs. In the case of SN 2020bvc, we find that the jet is off axis (by ≈23 degrees), as also indicated by the lack of early (≈1 day) X-ray emission, which explains why no coincident GRB was detected promptly or in archival data. These observations suggest that SN 2020bvc is the first orphan GRB detected through its associated SN emission.

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Section: Discussionsupporting

confidence: 87%

Broad-line type Ic SN 2020bvc

Izzo

Auchettl

Hjorth

et al. 2020

A&A

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“…Because of the short delay between the detection and the observations, a possible contamination of the afterglow cannot be excluded. Kangas et al (2020) showed that the remaining afterglow at 35.3 days is very weak (H F160W = 26.07 mag) compared to the host galaxy. We conclude (for this object) that the HST observations considered are not strongly affected by the GRB afterglow and that the host galaxy is assumed dominant.…”

Section: Sample Selectionmentioning

confidence: 99%

Are the host galaxies of long gamma-ray bursts more compact than star-forming galaxies of the field?

Schneider

Floc’h

Arabsalmani

et al. 2022

A&A

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Context. Long Gamma-Ray Bursts (GRBs) offer a promising tool to trace the cosmic history of star formation, especially at high redshift where conventional methods are known to suffer from intrinsic biases. Previous studies of GRB host galaxies at low redshift showed that high surface densities of stellar mass and star formation rate (SFR) can potentially enhance the GRB production. Evaluating the effect of such stellar densities at high redshift is therefore crucial to fully control the ability of long GRBs for probing the activity of star formation in the distant Universe. Aims. We assess how the size, the stellar mass and star formation rate surface densities of distant galaxies affect their probability to host a long GRB, using a sample of GRB hosts at z > 1 and a control sample of star-forming sources from the field. Methods. We gather a sample of 45 GRB host galaxies at 1 < z < 3.1 observed with the Hubble Space Telescope WFC3 camera in the near-infrared. Our subsample at 1 < z < 2 has cumulative distributions of redshift and stellar mass consistent with the host galaxies of already-known unbiased GRB samples, while our GRB host selection at 2 < z < 3.1 has lower statistics and is probably biased to the high end of the stellar mass function. Using the GALFIT parametric approach, we model the GRB host light profile with a Sérsic component and derive the half-light radius for 35 GRB hosts, which we use to estimate the star formation rate and stellar mass surface densities of each object. We compare the distribution of these physical quantities to the SFR-weighted properties of a complete sample of star-forming galaxies from the 3D-HST deep survey at comparable redshift and stellar mass. Results. We show that, similarly to z < 1, GRB hosts are smaller in size and they have higher stellar mass and star formation rate surface densities than field galaxies at 1 < z < 2. Interestingly, this result is robust even when considering separately the hosts of GRBs with optically-bright afterglows and the hosts of dark GRBs, as the two subsamples share similar size distributions. At z > 2 though, GRB hosts appear to have sizes and stellar mass surface densities more consistent with those characterizing the field galaxies. This may reveal an evolution with redshift of the bias between GRB hosts and the overall population of star-forming sources, although we cannot exclude that our result at z > 2 is also affected by the prevalence of dark GRBs in our selection. Conclusions. In addition to a possible trend toward low metallicity environment, other environmental properties such as stellar density appears to play a role in the formation of long GRBs, at least up to z ∼ 2. This might suggest that GRBs require special environments to be produced.

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“…An interesting result is found towards the end of the light curve. After removing the potential constant component, the combination of a late break and an early shallow decay makes the afterglow of this burst the most luminous ever detected for a certain time span, before the shallower post-break decay of the afterglow of GRB 160625B (which itself had a very late jet break, Kangas et al 2020) makes the latter the most luminous known at very late times again (Kann et al 2022c, in prep.). This provides further evidence for the extremely energetic nature of GRB 210905A.…”

Section: The Optical/nir Afterglow In Contextmentioning

confidence: 99%

A blast from the infant Universe: The very high-zGRB 210905A

Rossi

Frederiks

Канн

et al. 2022

A&A

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We present a detailed follow-up of the very energetic GRB 210905A at a high redshift of z = 6.312 and its luminous X-ray and optical afterglow. Following the detection by Swift and Konus-Wind, we obtained a photometric and spectroscopic follow-up in the optical and near-infrared (NIR), covering both the prompt and afterglow emission from a few minutes up to 20 Ms after burst. With an isotropic gamma-ray energy release of E iso = 1.27 +0.20 −0.19 × 10 54 erg, GRB 210905A lies in the top ∼ 7% of gamma-ray bursts (GRBs) in the Konus-Wind catalogue in terms of energy released. Its afterglow is among the most luminous ever observed, and, in particular, it is one of the most luminous in the optical at t 0.5 d in the rest frame. The afterglow starts with a shallow evolution that can be explained by energy injection, and it is followed by a steeper decay, while the spectral energy distribution is in agreement with slow cooling in a constant-density environment within the standard fireball theory. A jet break at ∼ 46.2 ± 16.3 d (6.3 ± 2.2 d rest-frame) has been observed in the X-ray light curve; however, it is hidden in the H band due to a constant contribution from the host galaxy and potentially from a foreground intervening galaxy. In particular, the host galaxy is only the fourth GRB host at z > 6 known to date. By assuming a number density n = 1 cm −3 and an efficiency η = 0.2, we derived a half-opening angle of 8.4 • ± 1.0 • , which is the highest ever measured for a z 6 burst, but within the range covered by closer events. The resulting collimation-corrected gamma-ray energy release of 1 × 10 52 erg is also among the highest ever measured. The moderately large half-opening angle argues against recent claims of an inverse dependence of the half-opening angle on the redshift. The total jet energy is likely too large to be sustained by a standard magnetar, and it suggests that the central engine of this burst was a newly formed black hole. Despite the outstanding energetics and luminosity of both GRB 210905A and its afterglow, we demonstrate that they are consistent within 2σ with those of less distant bursts, indicating that the powering mechanisms and progenitors do not evolve significantly with redshift.

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The Late-time Afterglow Evolution of Long Gamma-Ray Bursts GRB 160625B and GRB 160509A

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Cited by 18 publications

References 77 publications

Broad-line type Ic SN 2020bvc

Broad-line type Ic SN 2020bvc

Are the host galaxies of long gamma-ray bursts more compact than star-forming galaxies of the field?

A blast from the infant Universe: The very high-zGRB 210905A

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