Optical Afterglow Observations of the Unusual Short-Duration Gamma-Ray Burst GRB 040924

Huang, K. Y.; Urata, Y.; Filippenko, A. V.; Hu, Jiumei; Ip, W.-H.; Kuo, P. H.; Li, W.; Lin, H. C.; Lin, Z.-Y.; Makishima, Kazuo; Onda, K.; Qiu, Y.; Tamagawa, Toru

doi:10.1086/432612

Cited by 26 publications

(20 citation statements)

References 27 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Zeh et al 2006 for a large sample of optical afterglow parameters). Huang et al (2005) reach similar results qualitatively, but have very different values due to a much smaller dataset. The early data showing this break have only been taken in R band so it is unclear whether this break is achromatic, but after the early break, multi-colour data are available.…”

Section: The Afterglowsupporting

confidence: 53%

Spectroscopy and multiband photometry of the afterglow of intermediate duration γ-ray burst GRB 040924 and its host galaxy

Wiersema¹,

Horst²,

Канн

et al. 2008

A&A

View full text Add to dashboard Cite

Aims. We present optical photometry and spectroscopy of the afterglow and host galaxy of gamma-ray burst GRB 040924. This GRB had a rather short duration of T 90 ∼ 2.4 s, and a well sampled optical afterglow light curve. We aim to use this dataset to find further evidence that this burst is consistent with a massive star core-collapse progenitor. Methods. We combine the afterglow data reported here with those from the literature and compare the host properties with survey data. Results. We find that the global behaviour of the optical afterglow is well fit by a broken power-law, with a break at ∼0.03 days. We determine the redshift z = 0.858 ± 0.001 from the detected emission lines in our spectrum. Using the spectrum and photometry we derive global properties of the host, showing it to have similar properties to other long GRB hosts. We detect the [Ne iii] emission line in the spectrum, and compare the fluxes of this line of a sample of 15 long GRB host galaxies with survey data, showing the long GRB hosts to be comparable to local metal-poor emission line galaxies in their [Ne iii] emission. We fit the supernova bump accompanying this burst, and find that it is similar to other long GRB supernova bumps, but fainter. Conclusions. All properties of GRB 040924 (the associated supernova, the spectrum and SED of host and afterglow) are consistent with an origin in the core-collapse of a massive star.

show abstract

Section: The Afterglowsupporting

confidence: 53%

Spectroscopy and multiband photometry of the afterglow of intermediate duration γ-ray burst GRB 040924 and its host galaxy

Wiersema¹,

Horst²,

Канн

et al. 2008

A&A

View full text Add to dashboard Cite

show abstract

“…We also noted that GRB 090426 shares some similar properties with two other Type II bursts, GRB 040924 and GRB 050416A. The first was a short‐duration (1.2–1.5 s), soft‐spectrum (Huang et al 2005) and a SN 1998bw‐like supernova‐associated burst (Soderberg et al 2006a; Wiersema et al 2008). The second burst also exhibited a soft spectrum and a short duration in the rest frame ( T 90 = 2.4 s, z = 0.6528), which is associated with a SN 1998bw‐like supernova (Soderberg et al 2007), and is located in a circumburst medium with a large density variation.…”

Section: Discussionmentioning

confidence: 62%

Probing the nature of high-z short GRB 090426 with its early optical and X-ray afterglows

Xin¹,

Liang²,

Wei³

et al. 2010

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

GRB 090426 is a short‐duration burst detected by Swift ( s in the observer frame and s in the burst frame at z= 2.609). Its host galaxy properties and some gamma‐ray‐related correlations are analogous to those seen in long‐duration gamma‐ray bursts (GRBs), which are believed to be of a massive star origin (so‐called Type II GRBs). We present the results of its early optical observations with the 0.8‐m Tsinghua University–National Astronomical Observatory of China Telescope (TNT) at Xinglong Observatory and the 1‐m LOAO telescope at Mt Lemmon Optical Astronomy Observatory in Arizona. Our well‐sampled optical afterglow light curve covers from to 104 s after the GRB trigger. It shows two shallow decay episodes that are likely due to energy injection, which end at and 7100 s, respectively. The decay slopes after the injection phases are consistent with each other (). The X‐ray afterglow light curve appears to trace the optical, although the second energy‐injection phase was missed due to visibility constraints introduced by the Swift orbit. The X‐ray spectral index is without temporal evolution. Its decay slope is consistent with the prediction of the forward shock model. Both X‐ray and optical emission are consistent with being in the same spectral regime above the cooling frequency (). The fact that is below the optical band from the very early epoch of the observation provides a constraint on the burst environment, which is similar to that seen in classical long‐duration GRBs. We therefore suggest that death of a massive star is the possible progenitor of this short burst.

show abstract

“…Formal measures of T 90 do not always accurately distinguish long from short, such as in cases where we observe a short hard spike followed by a long, soft tail of emission (e.g., GRB 050724 or GRB 051227; Barthelmy et al 2005bBarthelmy et al , 2005a. Some bursts, notably GRB 040924 and GRB 050925, have short durations but soft emission, hence are likely the tail end of the longduration population (Huang et al 2005;Holland et al 2005). GRB 050911 has a complex BAT γ -ray light curve that may be interpreted as short, but because it is not conclusively in either category (Page et al 2006a), it is not included.…”

Section: Datamentioning

confidence: 99%

A Comparison of the Afterglows of Short- And Long-Duration Gamma-Ray Bursts

Nysewander

Fruchter

Pe’er

2009

ApJ

159

204

View full text Add to dashboard Cite

We present a comparative study of the observed properties of the optical and X-ray afterglows of short-and long-duration γ -ray bursts (GRBs). Using a large sample of 37 short and 421 long GRBs, we find a strong correlation between the afterglow brightness measured after 11 hr and the observed fluence of the prompt emission. Both the optical (R band) and X-ray flux densities (F R and F X ) scale with the γ -ray fluence, F γ . For bursts with a known redshift, a tight correlation exists between the afterglow flux densities at 11 hr (rest frame) and the total isotropic γ -ray energy, E γ,ISO : F R,X ∝ E γ,ISO α , with α 1. The constant of proportionality is nearly identical for long and short bursts, when E γ,ISO is obtained from the Swift data. Additionally, we find that for short busts with F γ 10 −7 erg cm −2 , optical afterglows are nearly always detected by reasonably deep early observations. Finally, we show that the ratio F R /F X has very similar values for short and long bursts. These results are difficult to explain in the framework of the standard scenario, since they require that either (1) the number density of the surrounding medium of short bursts is typically comparable to, or even larger than the number density of long bursts; (2) short bursts explode into a density profile, n(r) ∝ r −2 ; or (3) the prompt γ -ray fluence depends on the density of the external medium. We therefore find it likely that either basic assumptions on the properties of the circumburst environment of short GRBs or else the standard models of GRB emission must be re-examined. We believe that the most likely solution is that the ambient density surrounding typical short bursts is higher than has generally been expected: a typical value of ∼1 cm −3 is indicated. We discuss recent modifications to the standard binary merger model for short bursts which may be able to explain the implied density.

show abstract

Optical Afterglow Observations of the Unusual Short-Duration Gamma-Ray Burst GRB 040924

Cited by 26 publications

References 27 publications

Spectroscopy and multiband photometry of the afterglow of intermediate duration γ-ray burst GRB 040924 and its host galaxy

Spectroscopy and multiband photometry of the afterglow of intermediate duration γ-ray burst GRB 040924 and its host galaxy

Probing the nature of high-z short GRB 090426 with its early optical and X-ray afterglows

A Comparison of the Afterglows of Short- And Long-Duration Gamma-Ray Bursts

Contact Info

Product

Resources

About