Issue |
A&A
Volume 515, June 2010
|
|
---|---|---|
Article Number | A94 | |
Number of page(s) | 6 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361/200913795 | |
Published online | 15 June 2010 |
No evidence for dust extinction in GRB 050904 at 
T. Zafar1 - D. J. Watson1 - D. Malesani1 - P. M. Vreeswijk1 - J. P. U. Fynbo1 - J. Hjorth1 -
A. J. Levan2 - M. J. Michaowski1,3
1 - Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen,
Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark
2 - Department of Physics, University of Warwick, Coventry, CV4 7AL, UK
3 - Scottish Universities Physics Alliance, Institute for
Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, EH9
3HJ, UK
Received 3 December 2009 / Accepted 22 February 2010
Abstract
Context. Gamma-ray burst (GRB) afterglows are excellent and
sensitive probes of gas and dust in star-forming galaxies at all
epochs. It has been posited that dust in the early Universe must be
different from dust at lower redshifts. To date two reports in the
literature directly support this contention, one of which is based on
the spectral shape of the afterglow spectrum of GRB 050904 at z=6.295.
Aims. Here we reinvestigate the afterglow of GRB 050904 to
understand cosmic dust at high redshift. We address the claimed
evidence for unusual (supernova-origin) dust in its host galaxy by
simultaneously examining the X-ray and optical/near-infrared
spectrophotometric data of the afterglow.
Methods. We derived the intrinsic spectral energy distribution
(SED) of the afterglow at three different epochs, 0.47, 1.25, and
3.4 days after the burst. We reduced again the Swift X-ray data, the 1.25 days FORS2 z-Gunn photometric data, the spectroscopic and -band photometric data at
3 days from the Subaru telescope, as well as the critical UKIRT Z-band photometry at 0.47 days, upon which the claim of dust detection largely relies.
Results. We find no evidence of dust extinction in the SED at any time. We computed flux densities at
directly from the observed counts at all epochs. In the earliest epoch,
0.47 days, where the claim of dust is strongest, the Z-band suppression is found to be weaker (
mag) than previously reported and statistically insignificant (
). Furthermore, we find that the photometry of this band is unstable and difficult to calibrate.
Conclusions. From the afterglow SED we demonstrate that there is
no evidence of dust extinction in GRB 050904 - the SED at all
times can be reproduced without dust, and at 1.25 days in
particular, significant extinction can be excluded, with
mag
at 95% confidence using the supernova-type extinction curve. We
conclude that there is no evidence of any extinction in the afterglow
of GRB 050904 and that the presence of supernova-origin dust in
the host of GRB 050904 must be viewed skeptically.
Key words: galaxies: high-redshift - dust, extinction - gamma-ray burst: individual: GRB 050904
1 Introduction
Gamma-ray bursts (GRBs) can be detected up to the onset of reionization (e.g. Salvaterra et al. 2009; Tanvir et al. 2009) due to their brightness in the first few hours after the explosion (Lamb & Reichart 2000). GRBs are transient sources followed by long lasting afterglows, emitting energy intensely across the full range of the electromagnetic spectrum. GRB afterglows are effective and informative probes for the detailed study of cosmic dust at high redshifts due to their simple power-law spectra, high luminosities and locations in star-forming environments.
Interstellar dust has a crucial significance in the appearance and
evolution of star formation in the early Universe. It is still under
debate whether interstellar dust properties have evolved as a function
of redshift. At high redshift (z
> 5-6) it has been suggested that dust might originate in sources
other than the evolved asymptotic giant branch stars that are the
dominant source of dust production in the local Universe (Gehrz 1989; Dwek et al. 2007). Previous studies reported that dust in cosmological objects at z
> 6 is predominantly produced in the ejecta of core-collapse
supernovae (SNe), rather than the evolved stars which are missing on
short timescales (Morgan & Edmunds 2003; Todini & Ferrara 2001; Hirashita et al. 2005; Marchenko 2006; Dwek et al. 2007; Nozawa et al. 2003). Recently, however, Valiante et al. (2009)
calculated that the most massive asymptotic giant branch (AGB) stars
could produce dust on time scales short enough to dominate dust
production by .
Observationally, Maiolino et al. (2004) found an unusual extinction curve in the most distant known broad absorption line quasar (BAL QSO) at redshift z = 6.2, consistent with what could be expected from dust produced in core-collapse SNe.
The progenitors of long-duration GRBs are known to be short-lived massive stars (Malesani et al. 2004; Stanek et al. 2003; Hjorth et al. 2003b; Galama et al. 1998). GRB 050904 at z =6.295 was a long duration GRB. It was extremely luminous and is the third most distant known GRB to date. GRB 050904 was detected by Swift on 2005 September 4 at t0= 01:51:44 UT (Cummings et al. 2005). Substantial multi-wavelength follow-up was carried out simultaneously for GRB 050904 with several ground based facilities. Previous analysis of the rest-frame UV afterglow found no evidence of dust (Haislip et al. 2006; Gou et al. 2007; Kann et al. 2007; Tagliaferri et al. 2005). Later Stratta et al. (2007) re-examined the afterglow SED at different epochs and claimed the detection of dust absorptiontion with an extinction curve consistent with that used to explain the spectrum of the highest redshift BAL QSO, but inconsistent with the dust typical of the local Universe.
The claim of detection of SN-origin dust in GRB 050904 is of fundamental importance to the question of the origin of dust in the early Universe, a very vexed problem for high redshift sub-mm galaxies (see, e.g. the discussion in Michaowski et al. 2010). It was the first only direct observational evidence of dust from SNe in a high redshift star-forming environment. In this paper we review the relevant data to test whether dust is required by these observations and if so, what kind of dust is needed. The outline of the paper is as follows: In Sect. 2 we describe the detailed multi-band spectral analysis of the afterglow of GRB 050904 at different epochs. In Sect. 3 we present results from the SED of the afterglow. In Sect. 4 we discuss possible scenarios. In Sect. 5 we provide our conclusions.
2 Multi-wavelength observations of the afterglow
2.1 X-ray analysis
Swift's X-ray Telescope (XRT) localized the afterglow of GRB 050904. The XRT data (in the 0.3-10.0 keV energy range) were extracted and reduced using the HEAsoft software (version 6.4). We computed the X-ray spectra at three epochs, specifically 0.47, 1.25 and 3.4 days post-burst, chosen as the epochs with the best spectroscopic and photometric optical/near-infrared coverage. X-ray spectra at three epochs were created in a standard way using the most recent calibration files.For our analysis, it is important to obtain an accurate estimate of
the absolute flux for these X-ray spectra. The X-ray lightcurve is
extremely variable, exhibiting long lasting flaring activity (Gendre et al. 2006; Cusumano et al. 2006; Watson et al. 2006b).
The flares suggest two separate components, which may be due to a
number of causes, possibly activity of the GRB central engine (e.g. Burrows et al. 2007). At late times the X-ray count rate is very low (see Fig. 2),
therefore, we aim to get an accurate estimation of the flux which
includes the uncertainty due to the flares. We fitted the afterglow
lightcurve by assuming a smoothly broken power-law (Beuermann et al. 1999) to get an approximate overall X-ray lightcurve. The fit to the afterglow lightcurve results in at most a 30-40
scatter around this fit at all epochs. We then normalized the X-ray
spectra to the lightcurve fit at the relevant SED epoch. The procedure
results in X-ray spectra with the best estimate of the slope and flux
at the relevant SED epoch, and with an additional overall 30-40
uncertainty on their absolute flux levels.
2.2 Near-IR and optical imaging
Several telescopes obtained photometric observations of the afterglow in the optical and near-infrared bands (Haislip et al. 2006; Price et al. 2006; Tagliaferri et al. 2005). For a comprehensive investigation of the SED, we gathered optical and near-infrared photometry at three epochs. Stratta et al. (2007) suggested unusual dust particularly on the basis of the Z-band observation at

At 1.25 days z-band photometry was obtained with the 8.2 m ESO Very Large Telescope (VLT) by using the FOcal Reducer and low dispersion Spectrograph 2 (FORS2) z-Gunn filter. The object is detected with high signal to noise and using aperture photometry we could significantly reduce the error reported by Tagliaferri et al. (2005), which was likely mostly due to calibration issues.
At 3.3 days after the burst, -band photometry was carried out with the 8.2 m Subaru telescope (Iye et al. 2004) using the Faint Object Camera and Spectrograph (FOCAS; Kashikawa et al. 2002). We re-analysed the photometric data using aperture photometry. We compared our FOCAS
result with the Gemini South GMOS
value at 3.16 days obtained by Haislip et al. (2006). Correcting for the time difference between the two observations using a broken power-law with
,
,
days (Tagliaferri et al. 2005), we found these photometric measurements to be consistent within the statistical uncertainties.
Other photometric data were taken from the literature (Haislip et al. 2006; Tagliaferri et al. 2005) when available at a time close to our nominal SED epochs (J-band at 0.49 days). All H and
data as well as J at 1.25 and 3.4 days were derived from the best-fit lightcurves of Haislip et al. (2006) and Tagliaferri et al. (2005). At 1.25 days we used the Y-band photometry from the lightcurve computed in this band (Haislip et al. 2006).
We corrected the observed magnitudes for extinction in the Milky Way (MW) using the Schlegel et al. (1998) maps with RV=3.1 and
E(B-V)=0.081 mag along the line of sight of
the burst. Potential systematic uncertainties in the Galactic
extinction correction have no significant effect on our results. The
independent analysis of Dutra et al. (2003) confirms the Schlegel et al. (1998) maps for low E(B-V). For the z-bands
considered here, even assuming a 30% uncertainty in the Galactic value
would correspond to an extinction uncertainty of 0.03 mag which is
smaller than the statistical uncertainties we find for the extinction
in the host galaxy (see Table 1). Effects in the J, H, and
bands will be smaller still. An under-estimate of the Galactic
extinction would lead to a smaller host galaxy extinction than we find
in the current analysis.
The z-Gunn, FOCAS ,
GMOS
and Sloan Digital Sky Survey (SDSS
; Fukugita et al. 1996) z filters have almost the same profile across the whole band and extend much redder than the UKIRT Z filter. It should be noted that since the Ly
absorption
occurs in these bands, the filter wavelength coverage affects the
observed magnitude significantly (see Sect. 3.2). Unless
explicitly mentioned, in the rest of the paper we use the term ``z-band" to denote all of the three z filters, i.e. UKIRT Z, FORS2 z-Gunn and FOCAS
.
2.3 Grism spectroscopy
The optical spectrum of the afterglow was obtained with FOCAS at the
Subaru telescope and the spectroscopic data were retrieved from the
SMOKA science archive facility (Baba et al. 2002).
The afterglow was observed on 7 September 2005 for 4.0 h. The
exposure mid-time was 12:05 UT, corresponding to 3.4 days after
the burst trigger (Totani et al. 2006; Kawai et al. 2006).
The spectra were flux calibrated using the spectrophotometric standard
star BD+28D4211 obtained on the same night. Individual spectra were
combined following standard data reduction techniques using IRAF. The
spectrum exhibits no flux below
,
consistent with a break due to Ly
absorption at redshift
and the Ly
forest. The spectrum shows a flat continuum at the red wavelength end,
revealing a series of metal absorption lines arising from different
atomic species at z=6.295, and an intervening
system at z=4.84 (Kawai et al. 2006). The observed spectrum was corrected for Galactic extinction by assuming the Cardelli et al. (1989) extinction curve and as explained in Sect. 2.2 above.
We implemented Voigt profile fitting to the 3.4 day Subaru spectrum using the FITLYMAN package in MIDAS (Fontana & Ballester 1995). We measure a hydrogen column density of
(cm-2)
,
consistent with the value reported by Totani et al. (2006). It should be noted that
-band photometry and spectroscopy of the afterglow were obtained with FOCAS at 3.3 and 3.4 days, respectively.
3 SED analysis
Stratta et al. (2007) studied the optical-UV rest-frame SED of the afterglow of GRB 050904 at 0.5, 1 and 3 day epochs and found a deficit in the z-band at 0.5 and 1 days, and (less significantly) at 3 days, compared to the JHK power-law extrapolation, claiming that dust reddening could explain the flux deficit. This required a SN-type extinction curve.
3.1 Afterglow compound SED
Knowledge of the SED can address the z-band flux suppression issue, therefore, we computed the near-infrared to X-ray SED of GRB 050904 at three epochs, i.e. 0.47, 1.25 and 3.4 days. To facilitate comparison of the z-band flux, the SED at all epochs was normalized to the H-band flux, using the smoothly broken power-law presented by Tagliaferri et al. (2005). The normalized near-infrared photometry is generally consistent, but the X-ray spectra are much brighter at 0.47 and 1.25 days due to the intense afterglow flaring activity at these times. The consistency of the X-ray flux with the NIR SED extrapolation suggests that the X-ray afterglow at 3.4 days was relatively unaffected by flares. The composite SED of the afterglow of GRB 050904 at three different epochs is shown in Fig. 2.
3.2 Comparing the z-band filter responses
Since the z-band photometry is strongly affected by the Ly
absorption, we performed spectro-photometric analysis by utilizing the
total effective filter transmission functions including detector
responses (Fig. 1). We use the following method that allows for a clean comparison of the different z-band magnitudes of the afterglow, taken at 0.47, 1.25, and 3.4 days after the burst, with the filters UKIRT Z, VLT z-Gunn, and Subaru
,
respectively. The method essentially constructs the SEDs of stars in
the field and uses these to make a direct comparison of the afterglow
magnitudes at each epoch.
First, in each afterglow image we select several non-saturated
reference stars with known SDSS and Two Micron All Sky Survey (2MASS; Skrutskie et al. 2006) magnitudes. Using the 2MASS J-band, and the SDSS z and i, we construct a rudimentary SED for each reference star, where we convert the magnitudes to flux densities (in
)
at the central wavelength of the SDSS and 2MASS filters. We connect
these flux densities with a linear interpolation, and integrate the
reference star SED convolved with the filter response curve relevant to
that image, retrieving the band-integrated flux in
.
Second, from the image we measure the counts for the reference stars
using aperture or PSF photometry, determining the conversion factor
between counts and flux. Using this factor, we eventually compute the
(band-integrated) afterglow flux from its measured counts. We used
several comparison stars to evaluate the accuracy of the procedure. At
0.47, 1.25, and 3.3 days, we find a scatter of 0.02, 0.04, and
0.02 mag using 8, 10, and 5 reference stars, respectively. The
small scatter confirms the robustness of our method.
![]() |
Figure 1:
Filter transmission curves of SDSS z, FOCAS |
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![]() |
Figure 2:
Near-infrared to X-ray spectral energy distribution of the afterglow of
GRB 050904 at 0.47 (red triangles), 1.25 (blue squares) and
3.4 days (black circles) after the burst. The SED at 0.47 and
1.25 days is scaled to the H-band at 3.4 days. The solid grey curve represents the median-filtered optical spectrum at t0+3.4 days.
The black dashed line corresponds to a power-law fit to the
near-infrared to the X-ray data at 3.4 days with a spectral index
|
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In the deep FORS2 and FOCAS z-band images, the brightest
stars are heavily saturated, and suitable reference stars are lacking
since the fainter stars have large uncertainties in the SDSS and 2MASS
catalogues. Therefore, we calibrated a set of faint stars using the
UKIRT J and z-band images, based on the 2MASS and SDSS catalogs. For the z
band, due to the difference in the UKIRT and SDSS filters, appropriate
color terms were taken into account, achieving a photometric accuracy
of
mag. Given the higher sensitivity of the SDSS in the i band,
suitable calibrators for the VLT and Subaru images were available
directly from the SDSS catalog. Note that our calibration is entirely
based on the SDSS and 2MASS catalogs, therefore, our analysis is not
dependent on the sky conditions when the data have been acquired.
The third and final step is to convolve the relative afterglow
spectral shape (as measured from the Subaru spectrum that was obtained
at 3.4 days) with the three different z-band filter response curves, where the spectrum is rescaled in absolute terms to recover the band-integrated flux (in
)
determined for each epoch (see above). We note that this method does
not rely on the absolute flux calibration of the Subaru spectrum; it
merely uses the photometry to rescale it, and therefore the errors only
include the errors in the aperture/PSF photometry, the error from the
conversion factor, and the Subaru noise error when convolving it with
the filter response curves. After rescaling of the spectrum, the
afterglow flux density (in
)
can be compared at any pivot wavelength, after the H-band normalization. At all epochs we computed the flux density at
,
which was selected since it is close to the peak of all the involved filter transmission curves (see Fig. 1), and is separated from the metal absorption lines visible in the spectrum (Kawai et al. 2006).
Table 1: Best fit parameters of the SED at different epochs.
The single but important assumption in this method is that the spectral
shape of the afterglow is not changing from 0.47 to 3.4 days. This
is in some sense the null hypothesis that we are trying to test: dust
destruction would produce a change in the relative spectral shape, and
would therefore produce a change in the z-band brightness relative to the H-band normalization. Other effects, such as a variable
column, or a change in the spectral slope due to e.g. the cooling frequency crossing the z-band, could also in principle cause such a change. However, if the resulting afterglow z-band brightness (normalized to the H-band)
between 0.47 and 3.4 days does not show a significant change, then
this would provide strong support for the null hypothesis that the
spectral shape is not changing.
Following the above procedure, we find the afterglow to have a flux density at
of
,
and
Jy at 0.47, 1.25 and 3.3 days, respectively. We find that the normalized 0.47 day UKIRT Z-band brightness is
mag fainter than the FOCAS
-band brightness at 3.3 days. At 1.25 days, the normalized FORS2 z-Gunn brightness is brighter by
mag compared to the FOCAS
-band
brightness at 3.3 days. The uncertainties here also include the
uncertainties in the normalization, i.e. the errors in the H-band photometry (0.06 mag). Therefore, there is no evidence for variability of the spectral shape around the z band.
In particular, after taking into account the appropriate filter shapes
and color effects, there is no significant deficiency of flux in the z-band flux at 0.47 days compared to later epochs (Haislip et al. 2006; Stratta et al. 2007).
4 Discussion
At 0.47 days post-burst, we find a flux deficit in the UKIRT Z-band compared to the 3.3 days Subaru photometry that is only significant at <
4.1 Dust in the GRB 050904 host galaxy
The claim of SN-type dust in GRB 050904 is important because of the possibility of observing the evolution of cosmic dust at high redshift. Stratta et al. (2007) suggested SN-type dust extinction in the host galaxy of GRB 050904 with an extinction curve inferred for a BAL QSO at z=6.2 (Maiolino et al. 2004). The unusual extinction curve is rather flat at longer wavelengths and steeply rises at




It is clear from our broad-band SED at 3.4 days (see Fig. 2)
that the extrapolation of the near-infrared power-law is consistent
with a single power-law to the X-ray spectrum, i.e. consistent with
both the slope and flux level of the X-ray spectrum at that time. We
can also clearly see that there is no evidence in the flux-calibrated
optical/near-infrared spectrum at 3.4 days for any extinction -
the continuum just redward of the Ly
absorption is consistent with the single JHK
power-law. Both facts mean that there is no evidence for dust
extinction at 3.4 days. We fitted a dust-attenuated power-law
using a dust model for the Small Magellanic Cloud (SMC, RV=2.93; Pei 1992) and the SN-origin extinction model of Maiolino et al. (2004) to the 0.47, 1.25 and 3.4 day
data (from the z-band, we compute the flux density at
Å). The best fit parameters are reported in Table 1. With our revised z-band photometry, extinction at the level suggested by Stratta et al. (2007) can be ruled out at all three epochs (see Fig. 3). In no case the computed absorption is significant at more than 1.5
level.
Extinction-correcting the 1.25 day SED at the level fitted by Stratta et al. (2007) makes its extrapolation overshoot the X-ray spectrum, hinting that 1 mag of extinction at 3000 Å is not required. More importantly, the Y-band photometry, with a central wavelength of 1400 Å in the rest-frame, at 1.25 days (Haislip et al. 2006), is consistent with the near-infrared power-law extrapolation. Such consistency would not be expected in the Stratta et al. (2007) dust hypothesis since
is about 1.75 times the
in the Maiolino et al. (2004) model, and the Y-band photometry should therefore lie a factor of 2 below a power-law extrapolation, while it does not (Fig. 3), though its error is large. As it can be seen in the middle panel of Fig. 3,
the SED at 1 day follows a simple power-law and provides strong
constraints on dust absorption. Again, it seems likely that not only is
there no evidence for SN-type extinction in GRB 050904 after
1.25 days, but that there is no evidence for any dust extinction
at all at
1 day or later.
There are also strong arguments against a SN-origin dust interpretation
at 0.47 days. While dust reddening has been unequivocally observed
in lower redshift GRBs (e.g. Kann et al. 2006; Fynbo et al. 2009; GRB 050401: Watson et al. 2006a; GRB 991216: Vreeswijk et al. 2006; GRB 050408: Foley et al. 2006; de Ugarte Postigo et al. 2007; GRB 070802: Elíasdóttir et al. 2009; GRB 080607: Prochaska et al. 2009),
so far SN-origin dust has never been seen before in any GRB host.
Moreover there is no compelling evidence of dust extinction in any GRB
beyond z=5. A possible exception is GRB 071025 (which has a photometric redshift
4.4 < z < 5.2 Perley et al. 2009),
which shows indications of a significant dust column. Notable are the
two bursts at higher redshift than GRB 050904, i.e.
GRB 080913 at z=6.7 (Greiner et al. 2009), and GRB 090423 at z=8.2 (Salvaterra et al. 2009; Tanvir et al. 2009), neither of which show any sign of extinction. Second, given that dust can be excluded at t>1 day, having non-zero absorption at t
= 0.47 days would require time-varying dust extinction, which has
never been observed in any burst. If due to dust destruction, we would
expect reddening variations to be associated with intense episodes of
emission, while there is no optical flaring or any significant feature
in the restframe-UV lightcurve in this period that could be responsible
for such dust destruction (see Haislip et al. 2006; Tagliaferri et al. 2005), and most dust destruction scenarios sublimate dust on timescales of only a few minutes after the burst at most (Fruchter et al. 2001; Perna et al. 2003). Stratta et al. (2007)
suggested that varying extinction may also indicate that the emitting
region had become larger than the obscuring cloud. While this cannot be
excluded, such a geometry requires some tuning of the cloud and
fireball parameters. The claim of dust in the host galaxy of
GRB 050904, with an unusual extinction curve, relying principally
on a smaller (0.3 mag) and <
flux deficit in a photometric observation, is not the most likely
explanation. The most likely hypothesis is simply systematic
uncertainties related to the Z-band calibration.
It is worth noting however that time-variable dust with an unusual extinction curve is not even the simplest explanation even if the original analysis had been reliable. Given that we know from the optical spectrum that a large quantity of gas is present in the system, a variability in the gas column density at early times is a less tortured hypothesis.
![]() |
Figure 3: Near-infrared spectral energy distribution of the afterglow of GRB 050904 at 0.47 (top panel), 1.25 (middle panel) and 3.4 days (bottom panel) after the burst. The observed data are corrected for Galactic extinction (Sect. 2.2). The corresponding bands are identified in the bottom panel. The solid, dashed, and dotted lines represent the best fit with a power-law, a power-law with SN dust, and a power-law with SMC dust, respectively. At 1.25 days, the three lines almost overlap. |
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4.2 X-ray absorption
The X-ray spectral analysis suggests a high metal column density in the afterglow of GRB 050904 (Campana et al. 2007; Watson et al. 2006b). Time-resolved X-ray spectroscopy reveals that the column density of metals within the first few hours is highly variable (Campana et al. 2007; Gendre et al. 2006; Cusumano et al. 2006).
Due to the rapid changes in the X-ray spectrum this apparently variable
column may be an artifact of the changing intrinsic spectrum resulting
in a downturn at soft energies that disappears at later times (see Butler et al. 2006).
However, even if the change in the soft X-rays is really due to a
variable column density, i.e. due to increasing ionization of the
metals, this effect occurs at early times (103 s)
and cannot support the idea of dust destruction after 0.5 days.
Indeed, a varying metal column density at <1000 s argues
against dust destruction at 0.5 days. If the varying metal column
density is a real effect, destruction of any dust associated with the
high metal column should have been completed long before 0.5 days.
As a more general point, the optical and X-ray fluxes are at least one
to two orders of magnitude lower after 0.5 days than before
1000 s. It is difficult to construct a scenario in which
significant dust destruction occurs in the interval 0.5-3 days
that did not occur before in the absence of a huge flare in the
UV-X-ray, something which is not observed.
4.3 Gas-to-dust ratio
GRBs typically occur in host galaxies with high gas to dust ratios (e.g. Galama & Wijers 2001; Jensen et al. 2001; Stratta et al. 2004; Elíasdóttir et al. 2009; Hjorth et al. 2003a). The H I column density of the host of GRB 050904 is very large while AV is small. Using our limit on (SMC-type) dust at 1.25 days,
mag at
confidence, leads to a high gas-to-dust ratio N(H I)/
cm-2 mag-1. The Galactic relation between H I column density and dust reddening is N(H I)/
cm-2 mag-1 (Diplas & Savage 1994). Correcting for metallicity at 3.4 days (
;
Kawai et al. 2006), this implies an N(H I)/AV ratio limit 5 times the Galactic value. A comparison with the SMC (Gordon et al. 2003),
which has a similar metallicity to the environment of GRB 050904,
yields a gas-to-dust ratio which is also more than 5-10 times larger in
the host of GRB 050904.
4.4 The origin of dust in the early Universe
In the local Universe, the major sources of interstellar dust are AGB stars, the lower mass ranges of which require 1 Gyr to evolve to produce dust (Dwek et al. 2007). It has been suggested that for sources with large dust masses such as sub-mm galaxies, due to the short time available at
,
an alternative source of dust is required and that core-collapse SNe could dominate dust formation at these times (Morgan & Edmunds 2003; Todini & Ferrara 2001; Hirashita et al. 2005; Marchenko 2006; Dwek et al. 2007; Nozawa et al. 2003).
However, more complete theoretical models including dust destruction by
supernova shock or grain growth/destruction in the interstellar medium
obtain yields that are
0.01
per SN (Bianchi & Schneider 2007), consistent with almost all observations of nearby SNe (Elmhamdi et al. 2003; Sakon et al. 2009; Wooden et al. 1993; Meikle et al. 2006; Blair et al. 2007). This is too little to produce the quantities of dust observed at high redshift. Recently Valiante et al. (2009)
argued that on short timescales massive AGB stars could form much of
the dust, depending on the assumed initial stellar metallicity and star
formation history. The galaxy-SED modelling of sub-mm-selected galaxies
of Michaowski et al. (2010) suggests dust-formation timescales of order tens of millions of years in a few cases at
,
which would clearly preclude even high-mass AGB dust-formation. While
intriguing, these cases may be affected by active galactic nuclei (AGN)
contamination and must be treated cautiously.
Observationally, after our analysis here of the afterglow of GRB 050904, the detection of a peculiar extinction curve in a BAL QSO spectrum at z = 6.2 (Maiolino et al. 2004) remains the only direct evidence for dominant SN-origin dust in the early Universe (but see recent work by Perley et al. 2009). While the observational analysis of Maiolino et al. (2004) is carefully done, the relatively narrow wavelength coverage, the presence of strong, broad absorption and emission lines that dominate over the continuum at the blue end of the spectrum, and the use of composite QSO spectra, leave the result awaiting further confirmation. Furthermore, it is difficult to exclude that the dust is affected by the central AGN itself (Perna et al. 2003), so that the extinction curve may not tell us a lot about the origin of that dust.
5 Conclusions
In this work we reinvestigated the afterglow of GRB 050904 at 0.47, 1.25 and 3.4 day epochs to understand stellar environments and interstellar dust at high redshift. We find that the afterglow SED can be reproduced at all epochs without any dust extinction. The previous finding of dust extinction requiring a SN-type extinction curve by Stratta et al. (2007) relies mostly on a Z-band photometric point at 0.47 days which we find has calibration difficulties and with our new accurate analysis technique we find the flux deficit to be both smaller and less significant than reported by previous studies. We can reasonably exclude the presence of substantial quantities of any type of dust in this GRB host galaxy at all epochs. We therefore conclude that there is no significant evidence of dust extinction in the afterglow of GRB050904.
AcknowledgementsThe Dark Cosmology Centre is funded by the Danish National Research Foundation. Based in part on data collected at Subaru Telescope and obtained from the SMOKA archive, which is operated by the Astronomy Data Center, National Astronomical Observatory of Japan. Our special thanks to Giorgos Leloudas for helpful discussions. We are grateful to Tomonori Totani, Kentaro Aoki and Takashi Hattori for helping us in the Subaru data re-reduction. The authors thank the referee for very positive and constructive comments.
Note added post-submission: A recent paper by Perley et al. (2009) reports significant SN-origin dust extinction in GRB 071025 at z
5 (Perley et al. 2009). We note that Perley et al. (2009)
also independently attempted to model the dust profile of
GRB 050904 and found that the data are consistent with no
extinction at all.
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Footnotes
- ... (SDSS
- http://www.sdss.org/
- ... facility
- http://smoka.nao.ac.jp/
- ... (2MASS
- http://www.ipac.caltech.edu/2mass/
All Tables
Table 1: Best fit parameters of the SED at different epochs.
All Figures
![]() |
Figure 1:
Filter transmission curves of SDSS z, FOCAS |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
Near-infrared to X-ray spectral energy distribution of the afterglow of
GRB 050904 at 0.47 (red triangles), 1.25 (blue squares) and
3.4 days (black circles) after the burst. The SED at 0.47 and
1.25 days is scaled to the H-band at 3.4 days. The solid grey curve represents the median-filtered optical spectrum at t0+3.4 days.
The black dashed line corresponds to a power-law fit to the
near-infrared to the X-ray data at 3.4 days with a spectral index
|
Open with DEXTER | |
In the text |
![]() |
Figure 3: Near-infrared spectral energy distribution of the afterglow of GRB 050904 at 0.47 (top panel), 1.25 (middle panel) and 3.4 days (bottom panel) after the burst. The observed data are corrected for Galactic extinction (Sect. 2.2). The corresponding bands are identified in the bottom panel. The solid, dashed, and dotted lines represent the best fit with a power-law, a power-law with SN dust, and a power-law with SMC dust, respectively. At 1.25 days, the three lines almost overlap. |
Open with DEXTER | |
In the text |
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