Inclusive K0 production in e+e− annihilation for 9.3&lt;√s&lt; 31.6 GeV

Berger, Ch.; Genzel, H.; Grigull, R.; Lackas, W.; Raupach, F.; Klovning, A.; Lillestøl, Egil; Skard, J. A.; Ackermann, H.; Alexander, G.; Burger, J. D.; Criegee, L.; Eskreys, A.; Franke, G.; Gabriel, W.; Gerke, Ch.; Knies, G.; Lehmann, E.; Mertiens, H.D.; Michelsen, U.; Pape, K. H.; Reich, H.; Scarr, J. M.; Stella, B.; Timm, U.; Wagner, W.; Winter, G. G.; Zimmermann, W.; Achterberg, O.; Blobel, V.; Boesten, L.; Hepp, V.; Kapitza, H.; Koppitz, B.; Lewendel, B.; Lührsen, W.; Staa, R. van; Spitzer, H.; Chang, C. Y.; Glasser, R. G.; Kellogg, R. G.; Lau, K.; Polvado, R. O.; Sechi-Zorn, B.; Skuja, A.; Welch, G. E.; Zorn, G. T.; Bäcker, A.; Barreiro, F.; Brandt, Siegmund; Derikum, K.; Grupen, C.; Neumann, B.; Rost, M.; Zech, G.; Daum, H. J.; Meyer, H.; Meyer, Olivier; Rößler, M.; Schmidt, D.; Wacker, K.

doi:10.1016/0370-2693(81)90859-5

Cited by 33 publications

(11 citation statements)

References 28 publications

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“…Our dataset also includes Swift /UVOT data 26 and we have retrieved and analyzed public Gemini archival data 27 of GRB 081007 and GRB 090424, confirming results reported by Berger et al (2008) and Chornock et al (2009).…”

Section: Observations and Resultssupporting

confidence: 83%

See 1 more Smart Citation

GRB 081007 and GRB 090424: The Surrounding Medium, Outflows, and Supernovae

Jin

Covino

Valle

et al. 2013

ApJ

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We discuss the results of the analysis of multi-wavelength data for the afterglows of GRB 081007 and GRB 090424, two bursts detected by Swift. One of them, GRB 081007, also shows a spectroscopically confirmed supernova, SN 2008hw, which resembles SN 1998bw in its absorption features, while the maximum magnitude may be fainter, up to 0.7 mag, than observed in SN 1998bw. Bright optical flashes have been detected in both events, which allows us to derive solid constraints on the circumburst-matter density profile. This is particularly interesting in the case of GRB 081007, whose afterglow is found to be propagating into a constant-density medium, yielding yet another example of a gamma-ray burst (GRB) clearly associated with a massive star progenitor which did not sculpt the surroundings with its stellar wind. There is no supernova component detected in the afterglow of GRB 090424, likely because of the brightness of the host galaxy, comparable to the Milky Way. We show that the afterglow data are consistent with the presence of both forward-and reverse-shock emission powered by relativistic outflows expanding into the interstellar medium. The absence of optical peaks due to the forward shock strongly suggests that the reverse-shock regions should be mildly magnetized. The initial Lorentz factor of outflow of GRB 081007 is estimated to be Γ ∼ 200, while for GRB 090424 a lower limit of Γ > 170 is derived. We also discuss the prompt emission of GRB 081007, which consists of just a single pulse. We argue that neither the external forward-shock model nor the shock-breakout model can account for the prompt emission data and suggest that the single-pulse-like prompt emission may be due to magnetic energy dissipation of a Poynting-flux-dominated outflow or to a dissipative photosphere.

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Section: Observations and Resultssupporting

confidence: 83%

“…Gemini-South took two 900 s spectra, starting 73 minutes after the burst. Two absorption lines at 6016.7 and 6070.3Å and an emission line at 5700.9Å were identified as Ca II H, K and [O II] 3727Å lines respectively at z = 0.5295 ± 0.0001 (Berger et al 2008, see also figure 1).…”

Section: Introductionmentioning

confidence: 95%

GRB 081007 and GRB 090424: The Surrounding Medium, Outflows, and Supernovae

Jin

Covino

Valle

et al. 2013

ApJ

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“…If the optical-depth distribution of absorbers in not smooth (e.g., bimodal) the resulting metal column densities can be underestimated (see Prochaska 2006, for a detailed discussion of this caveat). However, we note that the b value derived from SiII is small compared to previous measurements in GRB afterglow spectra (e.g., Savaglio & Fall 2004;Berger et al 2006;Vreeswijk et al 2006). In a cloud with N HI > 10 20 cm −2 , the ionization level of the gas is low and the ionization correction can be neglected (Meiring et al 2009).…”

Section: Afterglow Spectrumcontrasting

confidence: 56%

A VERY METAL-POOR DAMPED LYMAN-α SYSTEM REVEALED THROUGH THE MOST ENERGETIC GRB 090926A

Rau

Savaglio

Krühler

et al. 2010

ApJ

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We present VLT/FORS2 spectroscopy and GROND optical/near-IR photometry of the afterglow of the bright Fermi/LAT GRB 090926A. The spectrum shows prominent Lyman-α absorption with N HI = 10 21.73±0.07 cm −2 and a multitude of metal lines at a common redshift of z = 2.1062 ± 0.0004, which we associate with the redshift of the GRB. The metallicity derived from SII is log(Z/Z ⊙ ) ≈ −1.9, one of the lowest values ever found in a GRB Damped Lyman-α (DLA) system. This confirms that the spread of metallicity in GRB-DLAs at z ≈ 2 is at least two orders of magnitude. We argue that this spread in metallicity does not require a similar range in abundances of the GRB progenitors, since the neutral interstellar medium probed by the DLA is expected to be at a significant distance from the explosion site. The hydrogen column density derived from Swift/XRT afterglow spectrum (assuming log(Z/Z ⊙ ) ≈ −1.9) is approx. ≈ 100 times higher than the N HI obtained from the Lyman-alpha absorptions. This suggests either a large column density of ionized gas or a higher metallicity of the circum-burst medium compared to the gas traced by the DLA. We also discuss the afterglow light curve evolution and energetics. The absence of a clear jet-break like steeping until at least 21 days post-burst suggests a beaming corrected energy release of E γ > 3.5 × 10 52 erg, indicating that GRB 090926A may have been one of the most energetic bursts ever detected.

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“…However, we can also set an upper limit on the metallicity from the non-detection of S II lines. Sulfur has proven useful in previous studies of GRB host galaxies at high redshift (e.g., Kawai et al 2006;Berger et al 2006;Price et al 2007) because the weak S II lines near 1250Å are not likely to be saturated and sulfur does not deplete onto dust grains (Savage & Sembach 1996). An unidentified absorption line near 8703Å in the blue wing of Si II λ1260 is near the expected position of S II λ1259.52 at the redshift of GRB 130606A, but formally the centroid is more than 10σ away from the correct wavelength, so we regard it as a non-detection.…”

Section: Z=5913mentioning

confidence: 99%

GRB 130606A AS A PROBE OF THE INTERGALACTIC MEDIUM AND THE INTERSTELLAR MEDIUM IN A STAR-FORMING GALAXY IN THE FIRST Gyr AFTER THE BIG BANG

Chornock

Berger

Fox

et al. 2013

ApJ

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We present high signal-to-noise ratio Gemini and MMT spectroscopy of the optical afterglow of the gamma-ray burst (GRB) 130606A at redshift z=5.913, discovered by Swift. This is the first high-redshift GRB afterglow to have spectra of comparable quality to those of z ≈ 6 quasars. The data exhibit a smooth continuum at near-infrared wavelengths that is sharply cut off blueward of 8410Å due to absorption from Lyα at redshift z ≈ 5.91, with some flux transmitted through the Lyα forest between 7000−7800Å. We use column densities inferred from metal absorption lines to constrain the metallicity of the host galaxy between a lower limit of [Si/H] −1.7 and an upper limit of [S/H] −0.5 set by the non-detection of S II absorption. We demonstrate consistency between the dramatic evolution in the transmission fraction of Lyα seen in this spectrum over the redshift range z = 4.9 to 5.85 with that previously measured from observations of high-redshift quasars. There is an extended redshift interval of ∆z=0.12 in the Lyα forest at z=5.77 with no detected transmission, leading to a 3σ upper limit on the mean Lyα transmission fraction of 0.2% (or τ eff GP (Lyα)>6.4). This is comparable to the lowest-redshift Gunn-Peterson troughs found in quasar spectra. Some Lyβ and Lyγ transmission is detected in this redshift window, indicating that it is not completely opaque, and hence that the IGM is nonetheless mostly ionized at these redshifts. We set a 2σ upper limit of 0.11 on the neutral fraction of the IGM at the redshift of the GRB from the lack of a Lyα red damping wing, assuming a model with a constant neutral density. GRB 130606A thus for the first time realizes the promise of GRBs as probes of the first galaxies and cosmic reionization.

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Inclusive K0 production in e+e− annihilation for 9.3<√s< 31.6 GeV

Cited by 33 publications

References 28 publications

GRB 081007 and GRB 090424: The Surrounding Medium, Outflows, and Supernovae

GRB 081007 and GRB 090424: The Surrounding Medium, Outflows, and Supernovae

A VERY METAL-POOR DAMPED LYMAN-α SYSTEM REVEALED THROUGH THE MOST ENERGETIC GRB 090926A

GRB 130606A AS A PROBE OF THE INTERGALACTIC MEDIUM AND THE INTERSTELLAR MEDIUM IN A STAR-FORMING GALAXY IN THE FIRST Gyr AFTER THE BIG BANG

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