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

Wiersema, K.; Horst, A. J. van der; Канн, Д. А.; Rol, E.; Starling, R. L. C.; Curran, P. A.; Gorosabel, J.; Levan, A. J.; Fynbo, J. P. U.; Postigo, A. de Ugarte; Wijers, R. A. M. J.; Castro-Tirado, A. J.; Guziy, S.; Hornstrup, A.; Hjorth, J.; Jelínek, M.; Jensen, B. L.; Kidger, M.; Martín-Luis, F.; Tanvir, N. R.; Tristram, P. J.; Vreeswijk, P. M.

doi:10.1051/0004-6361:20078050

Cited by 23 publications

(13 citation statements)

References 71 publications

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“…For the hosts of GRB 051016B, 051117B, 060814 and 070318 we calculated the SFR UV from V -, B-, and R-band fluxes, respectively, reported by Ovaldsen et al (2007) and Malesani et al (2012), which correspond to the rest-frame UV emission at the redshifts of the hosts. For the hosts of GRB 040924 and 061021 there are no UV continuum data available, so we calculated SFR [O II] from the flux reported by Wiersema et al (2008) and Jakobsson et al (2012), respectively, applying the conversion of Kewley et al (2004, their equation (4)).…”

Section: Resultsmentioning

confidence: 99%

THE OPTICALLY UNBIASED GRB HOST (TOUGH) SURVEY. VI. RADIO OBSERVATIONS ATz≲ 1 AND CONSISTENCY WITH TYPICAL STAR-FORMING GALAXIES

Michałowski

Kamble

Hjorth

et al. 2012

ApJ

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The objective of this paper is to determine the level of obscured star formation activity and dust attenuation in a sample of gamma-ray burst (GRB) hosts; and to test the hypothesis that GRB hosts have properties consistent with those of the general star-forming galaxy populations. We present a radio continuum survey of all z < 1 GRB hosts in The Optically Unbiased GRB Host (TOUGH) sample supplemented with radio data for all (mostly pre-Swift) GRB-SN hosts discovered before 2006 October. We present new radio data for 22 objects and have obtained a detection for three of them (GRB 980425, 021211, 031203; none in the TOUGH sample), increasing the number of radio-detected GRB hosts from two to five. The star formation rate (SFR) for the GRB 021211 host of ∼ 825 M ⊙ yr −1 , the highest ever reported for a GRB host, places it in the category of ultraluminous infrared galaxies. We found that at least ∼ 63% of GRB hosts have SFR < 100 M ⊙ yr −1 and at most ∼ 8% can have SFR > 500 M ⊙ yr −1 . For the undetected hosts the mean radio flux (< 35 µJy 3σ) corresponds to an average SFR < 15 M ⊙ yr −1 . Moreover, 88% of the z 1 GRB hosts have ultraviolet dust attenuation A UV < 6.7 mag (visual attenuation A V < 3 mag). Hence we did not find evidence for large dust obscuration in a majority of GRB hosts. Finally, we found that the distributions of SFRs and A UV of GRB hosts are consistent with those of Lyman break galaxies, Hα emitters at similar redshifts and of galaxies from cosmological simulations. The similarity of the GRB population with other star-forming galaxies is consistent with the hypothesis that GRBs, a least at z 1, trace a large fraction of all star formation, and are therefore less biased indicators than once thought.

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Section: Resultsmentioning

confidence: 99%

THE OPTICALLY UNBIASED GRB HOST (TOUGH) SURVEY. VI. RADIO OBSERVATIONS ATz≲ 1 AND CONSISTENCY WITH TYPICAL STAR-FORMING GALAXIES

Michałowski

Kamble

Hjorth

et al. 2012

ApJ

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“…GRB 040924 was a short burst with duration T 90 = 2.39 ± 0.24 s. It was located at z = 0.858 ( D L ∼ 1.7 × 10 28 cm) (Wiersema et al 2005). The peak energy of the time‐integrated spectrum obtained by Konus–Wind was E p = 67 ± 6 keV.…”

Section: Case Study and A Comparison Of The Different Methodsmentioning

confidence: 99%

“…The gamma‐ray isotropic equivalent energy was ∼1.5 × 10 52 erg (Fan et al 2005). The first optical observations was taken at ∼1000 s (Wiersema et al 2005), which yields an upper limit of decelerating time. As the parameters are not firmly determined (Fan et al 2005), we choose the typical parameters (with HETE‐II limit: f ν,lim ∼ 1.2 × 10 −27 erg cm −2 Hz −1 s −1 ).…”

Section: Case Study and A Comparison Of The Different Methodsmentioning

confidence: 99%

Lorentz factor constraint from the very early external shock of the gamma-ray burst ejecta

Zou

Piran

2010

Monthly Notices of the Royal Astronomical Society

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While it is generally agreed that the emitting regions in gamma‐ray bursts move ultra‐relativistically towards the observer, different estimates of the initial Lorentz factors, Γ0, lead to different at times conflicting estimates. We show here that the quiet periods in which the signals goes down below the instrumental thresholds put strong upper limits on the values of Γ0. According to the standard internal–external shock model, an external shock should develop during the prompt stage. This external shock radiates in the hard X‐rays to soft gamma‐rays bands and this emission should be seen as a smooth background signal. The observed deep minima indicate that this contribution is negligible. This limits, in turn, Γ0. We obtain upper limits on Γ0 for several bursts with typical values around hundreds. We compare these values with those obtained by the other methods, which typically yield lower limits. The results are marginally consistent leaving only a narrow range of allowed values for Γ0.

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“…Due to a similar shape of all standard extinction and attenuation curves between 0.275 μm and V-band, our A V estimate would only be ∼10% higher if we used the LMC or the Milky Way extinction curves (Gordon et al 2003), and ∼20% higher with the Calzetti et al (2000) attenuation curve. Up to date 89 long-GRB hosts have been targeted in the radio continuum (Berger et al 2001Vreeswijk et al 2001;Fox et al 2003;Frail et al 2003;van der Horst et al 2005;Wiersema et al 2008;Michałowski et al 2009Michałowski et al , 2012bStanway et al 2010Stanway et al , 2014Watson et al 2011;Perley et al 2015b), and only 15 (∼17%) were detected: the hosts of GRB 980425 (Michałowski et al 2009), 980703 (Berger et al 2001), 000418, 010222, , 021211 (Michałowski et al 2012b), 031203 (Stanway et al 2010;Watson et al 2011;Michałowski et al 2012b), 051022, 080207, and 090404 ; 051006, 060814, 061121, 070306, (Perley et al 2015b), 080517 (Stanway et al 2015a), 100621A (Stanway et al 2014); with the addition of the hosts of short (duration <2 s) GRBs 071227 (Nicuesa Guelbenzu et al 2014), and 120804A (Berger et al 2013). The map for the GRB 111005A host is not shown, as we use archival data with poor spatial resolution (Sect.…”

Section: Radio Continuummentioning

confidence: 99%

Massive stars formed in atomic hydrogen reservoirs: H I observations of gamma-ray burst host galaxies

Michałowski

Gentile

Hjorth

et al. 2015

A&A

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Long gamma-ray bursts (GRBs), among the most energetic events in the Universe, are explosions of massive and short-lived stars, so they pinpoint locations of recent star formation. However, several GRB host galaxies have recently been found to be deficient in molecular gas (H 2 ), believed to be the fuel of star formation. Moreover, optical spectroscopy of GRB afterglows implies that the molecular phase constitutes only a small fraction of the gas along the GRB line of sight. Here we report the first ever 21 cm line observations of GRB host galaxies, using the Australia Telescope Compact Array, implying high levels of atomic hydrogen (H i), which suggests that the connection between atomic gas and star formation is stronger than previously thought. In this case, it is possible that star formation is directly fuelled by atomic gas (or that the H i-to-H 2 conversion is very efficient, which rapidly exhaust molecular gas), as has been theoretically shown to be possible. This can happen in low-metallicity gas near the onset of star formation because cooling of gas (necessary for star formation) is faster than the H i-to-H 2 conversion. Indeed, large atomic gas reservoirs, together with low molecular gas masses, stellar, and dust masses are consistent with GRB hosts being preferentially galaxies which have very recently started a star formation episode after accreting metal-poor gas from the intergalactic medium. This provides a natural route for forming GRBs in low-metallicity environments. The gas inflow scenario is also consistent with the existence of the companion H i object with no optical counterpart ∼19 kpc from the GRB 060505 host, and with the fact that the H i centroids of the GRB 980425 and 060505 hosts do not coincide with optical centres of these galaxies, but are located close to the GRB positions.

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

Cited by 23 publications

References 71 publications

THE OPTICALLY UNBIASED GRB HOST (TOUGH) SURVEY. VI. RADIO OBSERVATIONS ATz≲ 1 AND CONSISTENCY WITH TYPICAL STAR-FORMING GALAXIES

THE OPTICALLY UNBIASED GRB HOST (TOUGH) SURVEY. VI. RADIO OBSERVATIONS ATz≲ 1 AND CONSISTENCY WITH TYPICAL STAR-FORMING GALAXIES

Lorentz factor constraint from the very early external shock of the gamma-ray burst ejecta

Massive stars formed in atomic hydrogen reservoirs: H I observations of gamma-ray burst host galaxies

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