The nature of the dwarf starforming
galaxy associated   with GRB 060218/SN 2006aj

Wiersema, K.; Savaglio, S.; Vreeswijk, P. M.; Ellison, Sara L.; Ledoux, C.; Yoon, S.C.; Møller, Per; Sollerman, J.; Fynbo, J. P. U.; Pian, E.; Starling, R. L. C.; Wijers, R. A. M. J.

doi:10.1051/0004-6361:20066273

Cited by 87 publications

(125 citation statements)

References 78 publications

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“…XRF 020903 had a late lightcurve and spectrum consistent with a supernova at z = 0.25 (Soderberg et al 2005;Bersier et al 2006). More recently, the nearby (z = 0.0331, Wiersema et al 2007) and unusual burst, XRF 060218, with a very low E peak ∼ 5 keV (Campana et al 2006) showed unambiguous evidence for an associated supernova (e.g., Sollerman et al 2006;Modjaz et al 2006;Pian et al 2006). SN 2006aj associated with XRF 060218 clearly established the close link between SNe, (GRBs) and XRFs.…”

Section: Introductionmentioning

confidence: 78%

The nature of the X-ray flash of August 24 2005

Sollerman

Fynbo

Gorosabel

et al. 2007

A&A

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Aims. Our aim is to investigate the nature of the X-Ray Flash (XRF) of August 24, 2005. Methods. We present comprehensive photometric R-band observations of the fading optical afterglow of XRF 050824, from 11 min to 104 days after the burst. In addition we present observations taken during the first day in the BRIK bands and two epochs of spectroscopy. We also analyse available X-ray data. Results. The R-band lightcurve of the afterglow resembles the lightcurves of long duration Gamma-Ray Bursts (GRBs), i.e., a powerlaw, albeit with a rather shallow slope of α = 0.6 (F ν ∝ t −α ). Our late R-band images reveal the host galaxy. The rest-frame B-band luminosity is ∼0.5 L * . The star-formation rate as determined from the [O II] emission line is ∼1.8 M yr −1 . When accounting for the host contribution, the slope is α = 0.65 ± 0.01 and a break in the lightcurve is suggested. A potential lightcurve bump at 2 weeks can be interpreted as a supernova only if this is a supernova with a fast rise and a fast decay. However, the overall fit still shows excess scatter in the lightcurve in the form of wiggles and bumps. The flat lightcurves in the optical and X-rays could be explained by a continuous energy injection scenario, with an on-axis viewing angle and a wide jet opening angle (θ j > ∼ 10• ). If the energy injections are episodic this could potentially help explain the bumps and wiggles. Spectroscopy of the afterglow gives a redshift of z = 0.828 ± 0.005 from both absorption and emission lines. The spectral energy distribution (SED) of the afterglow has a power-law (F ν ∝ ν −β ) shape with slope β = 0.56 ± 0.04. This can be compared to the X-ray spectral index which is β X = 1.0 ± 0.1. The curvature of the SED constrains the dust reddening towards the burst to A v < 0.5 mag.

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Section: Introductionmentioning

confidence: 78%

The nature of the X-ray flash of August 24 2005

Sollerman

Fynbo

Gorosabel

et al. 2007

A&A

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“…The host galaxy of SN2006aj is a low luminosity, metal-poor star-forming dwarf galaxy (Ferrero et al 2006) with an irregular morphology (Wiersema et al 2007), similar to those of other GRBs associated with SNe (Modjaz et al 2006;Sollerman et al 2006).…”

Section: Grb 060218 -Sn2006ajmentioning

confidence: 96%

GRB 060218 and GRBs associated with supernovae Ib/c

Dainotti¹,

Bernardini²,

Bianco³

et al. 2007

A&A

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Context. The Swift satellite has given continuous data in the range 0.3-150 keV from 0 s to 10 6 s for GRB 060218 associated with SN2006aj. This Gamma-Ray Burst (GRB) which has an unusually long duration (T 90 ∼ 2100 s) fulfills the Amati relation. These data offer the opportunity to probe theoretical models for GRBs connected with Supernovae (SNe). Aims. We plan to fit the complete γ-and X-ray light curves of this long duration GRB, including the prompt emission, in order to clarify the nature of the progenitors and the astrophysical scenario of the class of GRBs associated with SNe Ib/c. Methods. We apply our "fireshell" model based on the formation of a black hole, giving the relevant references. It is characterized by the precise equations of motion and equitemporal surfaces and by the role of thermal emission. Results. The initial total energy of the electron-positron plasma E tot e ± = 2.32 × 10 50 erg has a particularly low value, similar to the other GRBs associated with SNe. For the first time, we observe a baryon loading B = 10 −2 which coincides with the upper limit for the dynamical stability of the fireshell. The effective CircumBurst Medium (CBM) density shows a radial dependence n cbm ∝ r −α with 1.0 < ∼ α < ∼ 1.7 and monotonically decreases from 1 to 10 −6 particles/cm 3 . This behavior is interpreted as being due to a fragmentation in the fireshell. Analogies with the fragmented density and filling factor characterizing Novae are outlined. The fit presented is particularly significant in view of the complete data set available for GRB 060218 and of the fact that it fulfills the Amati relation. Conclusions. We fit GRB 060218, usually considered as an X-Ray Flash (XRF), as a "canonical GRB" within our theoretical model. The smallest possible black hole, formed by the gravitational collapse of a neutron star in a binary system, is consistent with the especially low energetics of the class of GRBs associated with SNe Ib/c. We provide the first evidence for a fragmentation in the fireshell. This fragmentation is crucial in explaining both the unusually large T 90 and the consequently inferred abnormally low value of the CBM effective density.

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“…In the case of GRB 060218/SN 2006aj, using the T e method (see Wiersema et al 2007) measure the oxygen abundance of the host as 12 + log(O/H) = 7.5 but when using the PP04 calibration the host sits at 12 + log(O/H) = 8.1. Given that the moderately low PP04 abundance of the host of SN 2007bg somewhat contradicts its extremely low luminosity, it seems that the abundance has been over-estimated.…”

Section: Host Galaxiesmentioning

confidence: 99%

Two type Ic supernovae in low-metallicity, dwarf galaxies: diversity of explosions

Young¹,

Smartt²,

Valenti³

et al. 2010

A&A

139

132

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Aims. The aim of this paper is to discuss the nature of two type Ic supernovae SN 2007bg and SN 2007bi and their host galaxies. Both supernovae were discovered in wide-field, non-targeted surveys and are found to be associated with sub-luminous blue dwarf galaxies identified in SDSS images. Methods. We present BVRI photometry and optical spectroscopy of SN 2007bg and SN 2007bi and their host galaxies. Their lightcurves and spectra are compared to those of other type Ic SNe and analysis of these data provides estimates of the energetics, total ejected masses and synthesised mass of 56 Ni. Detection of the host galaxy emission lines allows for metallicity measurements. Results. Neither SNe 2007bg nor 2007bi were found in association with an observed GRB, but from estimates of the metallicities of their host-galaxies they are found to inhabit similar low-metallicity environments as GRB associated supernovae. The radio-bright SN 2007bg is hosted by an extremely sub-luminous galaxy of magnitude M B = −12.4 ± 0.6 mag and an estimated oxygen abundance of 12 + log(O/H) = 8.18 ± 0.17 (on the Pettini & Pagel 2004 scale). The early lightcurve evolution of SN 2007bg matches the fastpace decline of SN 1994I giving it one of the fastest post-maximum decline rates of all broad-lined type Ic supernovae known to date and, when combined with its high expansion velocities, a high kinetic energy to ejected mass ratio (E K /M ej ∼ 2.7). We also show that SN 2007bi is possibly the most luminous type Ic known, reaching a peak magnitude of M R ∼ −21.3 mag and displays a remarkably slow decline, following the radioactive decay rate of 56 Co to 56 Fe throughout the course of its observed lifetime. SN 2007bi also displays an extreme longevity in its spectral evolution and is still not fully nebular at approximately one year post-maximum brightness. From a simple model of the bolometric light curve of SN 2007bi we estimate a total ejected 56 Ni mass of M Ni = 3.5−4.5 M , the largest 56 Ni mass measured in the ejecta of a supernova to date. There are two models that could explain the high luminosity and large ejected 56 Ni mass. One is a pair-instability supernova (PISN) which has been predicted to occur for massive stars at low metallicities. We measure the host galaxy metallicity of SN 2007bi to be 12 + log(O/H) = 8.15 ± 0.15 (on the McGaugh 1991 scale) which is somewhat high to be consistent with the PISN model. An alternative is the core-collapse of a C+O star of 20−40 M which is the core of a star of originally 50−100 M .

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The nature of the dwarf starforming galaxy associated with GRB 060218/SN 2006aj

Cited by 87 publications

References 78 publications

The nature of the X-ray flash of August 24 2005

The nature of the X-ray flash of August 24 2005

GRB 060218 and GRBs associated with supernovae Ib/c

Two type Ic supernovae in low-metallicity, dwarf galaxies: diversity of explosions

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