Reply to the comment by S. Dannefaer et al. on the paper of H. E. Schaefer et al. on ?amorphous hydrogenated silicon studied by positron lifetime spectroscopy?

Schaefer, H.; Würschum, Roland; Schwarz, R.; Slobodin, D.; Wagner, S.

doi:10.1007/bf00635186

Cited by 35 publications

(31 citation statements)

References 14 publications

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“…The latter non-detections are in agreement with the upper limits reported by ROTSE-III (Schaefer et al 2005) and ART (Torii et al 2005).…”

Section: Resultssupporting

confidence: 90%

“…The prompt dissemination (55.0 s) of the GRB position by HETE-2 enabled rapid responses by automated and robotic telescopes like ROTSE-III (Schaefer et al 2005) and ART (Torii et al 2005), although no prompt optical afterglow was detected. Swift slewed and started data acquisition (about 3.5 h after the event) and fading X-ray emission was detected by the XRT, which can be considered as the first clear detection of the afterglow from GRB 051022 (Racusin et al 2005a).…”

Section: +37mentioning

confidence: 99%

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The dark nature of GRB 051022 and its host galaxy

Castro-Tirado

Bremer

McBreen

et al. 2007

A&A

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Aims. We present multiwavelength (X-ray/optical/near-infrared/millimetre) observations of GRB 051022 between 2.5 h and ∼1.15 yr after the event. It is the most intense gamma-ray burst (∼10 −4 erg cm −2 ) detected by HETE-2, with the exception of the nearby GRB 030329. Methods. Optical and near infrared observations did not detect the afterglow despite a strong afterglow at X-ray wavelengths. Millimetre observations at Plateau de Bure (PdB) detected a source and a flare, confirming the association of this event with a moderately bright (R = 21.5) galaxy. Results. Spectroscopic observations of this galaxy show strong [O II], Hβ and [O III] emission lines at a redshift of 0.809. The spectral energy distribution (SED) of the galaxy implies A V (rest frame) = 1.0 and a starburst occuring ∼25 Myr ago, during which the star-forming-rate reached ∼50 M /yr. In conjunction with the spatial extent (∼1 ) it suggests a very luminous (M V = −21.8) blue compact galaxy, for which we also find Z ∼ Z . The X-ray spectrum shows evidence of considerable absorption by neutral gas with N H,X−ray = 3.47 +0.48 −0.47 × 10 22 cm −2 (rest frame). Absorption by dust in the host galaxy at z = 0.809 certainly cannot account for the non-detection of the optical afterglow, unless the dust-to-gas ratio is quite different than that seen in our Galaxy (i.e. large dust grains). Conclusions. It is likely that the afterglow of the dark GRB 051022 was extinguished along the line of sight by an obscured, dense star forming region in a molecular cloud within the parent host galaxy. This galaxy is different from most GRB hosts being brighter than L * by a factor of 3. We have also derived a SFR ∼ 50 M /yr and predict that this host galaxy will be detected at sub-mm wavelengths.

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“…The latter non-detections are in agreement with the upper limits reported by ROTSE-III (Schaefer et al 2005) and ART (Torii et al 2005).…”

Section: Resultssupporting

confidence: 90%

Section: +37mentioning

confidence: 99%

The dark nature of GRB 051022 and its host galaxy

Castro-Tirado

Bremer

McBreen

et al. 2007

A&A

View full text Add to dashboard Cite

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“…The detection significance of the source is 4.5 aD(SIS)/4.8 aD(GIS), and the source is localized to be at R.A. = 12 h15ml1 s, Dec. = -10 0 18' 21'' (J 2000) with a 90% confidence error radius of 1'. This location coincides with an X-ray source detected with the ROBAT All-Sky Survey, which is claimed to be associated with HR4657, an F-type star ofV=6.1 mag at D=34pc [6]. If the extremely intense GRB930131 carne from the normal star HR4657, how was the burst energy produced?…”

Section: Grb930131supporting

confidence: 57%

Possible X-Ray Counterparts to Gamma-Ray Bursts, GRB930131 and GRB940217

Shibata

Murakami

Ueda

et al. 1998

Symp. - Int. Astron. Union

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We made a search of quiescent X-ray counterparts of two Gamma-R.ay Bursts (GRBs), GRB930131 and GRB940217. These GRBs were detected with BATSE, EGRET, COMPTEL on board CGRO together with the GRB detector on Ulysses spacecraft, then they were localized in small error regions, These observations showed that the bursts were remarkably bright accompanying delayed high energy gamma-rays. ASCA observations have fOU11d a single X-ray source for each GRB on the possible location determined with the above instruments,

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“…We immediately detected a bright afterglow candidate (Filgas et al 2010) in all seven optical to NIR bands (i.e. ; g , r , i , z , J, H, K s ) at the coordinate reported by Schaefer et al (2010). GROND continued observing GRB 100814A during the first night as long as it was observable from La Silla (∼23 ks) and then densely covered the light curve evolution for the following three weeks for a total of about 200 individual observations for each band.…”

Section: Observations and Data Reductionmentioning

confidence: 76%

Afterglow rebrightenings as a signature of a long-lasting central engine activity?

Nardini

Elliott

Filgas

et al. 2014

A&A

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Context. In the past few years the number of well-sampled optical to near-infrared (NIR) light curves of long gamma-ray bursts (GRBs) has greatly increased, particularly due to simultaneous multi-band imagers such as GROND. Combining these densely sampled ground-based data sets with the Swift UVOT and XRT space observations unveils a much more complex afterglow evolution than what was predicted by the most commonly invoked theoretical models. GRB 100814A represents a remarkable example of these interesting well-sampled events, showing a prominent late-time rebrightening in the optical to NIR bands and a complex spectral evolution. This represents a unique laboratory to test the different afterglow emission models. Aims. Here we study the nature of the complex afterglow emission of GRB 100814A in the framework of different theoretical models. Moreover, we compare the late-time chromatic rebrightening with those observed in other well-sampled long GRBs. Methods. We analysed the optical and NIR observations obtained with the seven-channel Gamma-Ray burst Optical and Near-infrared Detector (GROND) at the 2.2 m MPG/ESO telescope together with the X-ray and UV data detected by the instruments onboard the Swift observatory. The broad-band afterglow evolution, achieved by constructing multi-instrument light curves and spectral energy distributions, is discussed in the framework of different theoretical models. Results. We find that the standard models that describe the broad-band afterglow emission within the external shock scenario fail to describe the complex evolution of GRB 100814A, and therefore more complex scenarios must be invoked. The analysis of the very well sampled broad-band light curve of GRB 100814A allowed us to deduce that models invoking late-time activity of the central engine in the observed afterglow emission are the preferred ones for all the different observed features. This late-time activity most likely has the form of a delayed reactivation of the ejecta emission process. However, a more detailed modelling of the radiative mechanisms associated with these scenarios is necessary to arrive at a firm conclusion on the nature of the optical rebrightenings that so often are detected in long GRBs.

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Reply to the comment by S. Dannefaer et al. on the paper of H. E. Schaefer et al. on ?amorphous hydrogenated silicon studied by positron lifetime spectroscopy?

Cited by 35 publications

References 14 publications

The dark nature of GRB 051022 and its host galaxy

The dark nature of GRB 051022 and its host galaxy

Possible X-Ray Counterparts to Gamma-Ray Bursts, GRB930131 and GRB940217

Afterglow rebrightenings as a signature of a long-lasting central engine activity?

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