► Studies on noise level and transient noise in South Pole ice with the South Pole Acoustic Test Setup (SPATS). ► Acoustic noise level in South Pole ice estimated to be smaller than 20
mPa in 10–50
...kHz frequency range. ► Refreezing of IceCube holes and Rodriguez wells observed acoustically. ► Upper limit on the flux of ultra high energy neutrinos.
The detection of acoustic signals from ultra-high energy neutrino interactions is a promising method to measure the flux of cosmogenic neutrinos expected on Earth. The energy threshold for this process depends strongly on the absolute noise level in the target material. The South Pole Acoustic Test Setup (SPATS), deployed in the upper part of four boreholes of the IceCube Neutrino Observatory, has monitored the noise in Antarctic ice at the geographic South Pole for more than two years down to 500
m depth. The noise is very stable and Gaussian distributed. Lacking an in situ calibration up to now, laboratory measurements have been used to estimate the absolute noise level in the 10–50
kHz frequency range to be smaller than 20
mPa. Using a threshold trigger, sensors of the South Pole Acoustic Test Setup registered acoustic events in the IceCube detector volume and its vicinity. Acoustic signals from refreezing IceCube holes and from anthropogenic sources have been used to test the localization of acoustic events. An upper limit on the neutrino flux at energies
E
ν
>
10
11
GeV is derived from acoustic data taken over eight months.
We report on a search with the IceCube detector for high-energy muon neutrinos from GRB 080319B, one of the brightest gamma-ray bursts (GRBs) ever observed. The fireball model predicts that a mean of ...0.1 events should be detected by IceCube for a bulk Lorentz boost of the jet of 300. In both the direct on-time window of 66 s and an extended window of about 300 s around the GRB, no excess was found above background. The 90% CL upper limit on the number of track-like events from the GRB is 2.7, corresponding to a muon neutrino fluence limit of 9.5 X 10-3 erg cm-2 in the energy range between 120 TeV and 2.2 PeV, which contains 90% of the expected events.
Most of the matrix metalloproteinases (MMP) are not expressed in normal intact skin but they are upregulated in inflamed or diseased skin. The recently cloned MMP-19 is one of the few MMP members ...that are also expressed in healthy epidermis. In this study, we found that MMP-19 is generally coexpressed with cytokeratin 14 that is confined to keratinocytes of the stratum basale. MMP-19 was also detected in hair follicles, sebaceous glands, and eccrine sweat glands. Its expression, however, changed in cutaneous diseases exhibiting increased alternations of epidermal proliferation, such as psoriasis, eczema, and tinea. In the affected area, MMP-19 was also found in suprabasal and spinous epidermal layers. We also studied the regulation of MMP-19 expression at the protein level, as well as by using a promoter assay. The constitutive expression of MMP-19 was upregulated with phorbol myristate acetate and downregulated with retinoic acid and dexamethasone. Tumor necrosis factor-α, interleukin (IL)-6, TGF-β, IL-15, IL-8, and RANTES as well as the bacterial compounds lipopolysaccharide and lipoteichoic acid did not show any profound effect in HaCaT cells. In contrast, type IV and type I collagens upregulated MMP-19 significantly. The dysregulation of MMP-19 expression in epidermis suggests its possible involvement in the perpetuation of cutaneous infections and proliferative disorders such as psoriasis.
SN 2008D, a core collapse supernova at a distance of 27 Mpc, was serendipitously discovered by the Swift satellite through an associated X-ray flash. Core collapse supernovae have been observed in ...association with long gamma-ray bursts and X-ray flashes and a physical connection is widely assumed. This connection could imply that some core collapse supernovae possess mildly relativistic jets in which high-energy neutrinos are produced through proton-proton collisions. The predicted neutrino spectra would be detectable by Cherenkov neutrino detectors like IceCube. A search for a neutrino signal in temporal and spatial correlation with the observed X-ray flash of SN 2008D was conducted using data taken in 2007–2008 with 22 strings of the IceCube detector. Events were selected based on a boosted decision tree classifier trained with simulated signal and experimental background data. The classifier was optimized to the position and a “soft jet” neutrino spectrum assumed for SN 2008D. Using three search windows placed around the X-ray peak, emission time scales from 100–10 000 s were probed. No events passing the cuts were observed in agreement with the signal expectation of 0.13 events. Upper limits on the muon neutrino flux from core collapse supernovae were derived for different emission time scales and the principal model parameters were constrained. While no meaningful limits can be given in the case of an isotropic neutrino emission, the parameter space for a jetted emission can be constrained. Future analyses with the full 86 string IceCube detector could detect up to ~100 events for a core-collapse supernova at 10 Mpc according to the soft jet model.
We have measured the speed of both pressure waves and shear waves as a function of depth between 80 and 500
m depth in South Pole ice with better than 1% precision. The measurements were made using ...the South Pole Acoustic Test Setup (SPATS), an array of transmitters and sensors deployed in the ice at the South Pole in order to measure the acoustic properties relevant to acoustic detection of astrophysical neutrinos. The transmitters and sensors use piezoceramics operating at ∼5–25
kHz. Between 200
m and 500
m depth, the measured profile is consistent with zero variation of the sound speed with depth, resulting in zero refraction, for both pressure and shear waves. We also performed a complementary study featuring an explosive signal propagating vertically from 50 to 2250
m depth, from which we determined a value for the pressure wave speed consistent with that determined for shallower depths, higher frequencies, and horizontal propagation with the SPATS sensors. The sound speed profile presented here can be used to achieve good acoustic source position and emission time reconstruction in general, and neutrino direction and energy reconstruction in particular. The reconstructed quantities could also help separate neutrino signals from background.
We report on the search for electromagnetic and hadronic showers (“cascades”) produced by a diffuse flux of extraterrestrial neutrinos in the AMANDA neutrino telescope. Data for this analysis were ...recorded during 1001
days of detector livetime in the years 2000–2004. The observed event rates are consistent with the background expectation from atmospheric neutrinos and muons. An upper limit is derived for the diffuse flux of neutrinos of all flavors assuming a flavor ratio of
ν
e
:
ν
μ
:
ν
τ
=
1:1:1 at the detection site. The all-flavor flux of neutrinos with an energy spectrum
Φ
∝
E
−2 is less than 5.0
×
10
−7
GeV
s
−1
sr
−1
cm
−2 at a 90% C.L. Here, 90% of the simulated signal would fall within the energy range 40
TeV to 9
PeV. We discuss flux limits in the context of several specific models of extraterrestrial and prompt atmospheric neutrino production.
We have noticed some mistakes in formulae (A2) and (A5) in the appendix of our paper. The errors are not present in the code used in the analysis and hence none of the plots or results is affected. ...The correct formulae are below.
A measurement of the atmospheric muon neutrino energy spectrum from 100 GeV to 400 TeV was performed using a data sample of about 18 000 up-going atmospheric muon neutrino events in IceCube. Boosted ...decision trees were used for event selection to reject misreconstructed atmospheric muons and obtain a sample of up-going muon neutrino events. Background contamination in the final event sample is less than 1%. This is the first measurement of atmospheric neutrinos up to 400 TeV, and is fundamental to understanding the impact of this neutrino background on astrophysical neutrino observations with IceCube. The measured spectrum is consistent with predictions for the atmospheric nu(mu) + (nu) over bar (mu) flux.
Self-annihilating or decaying dark matter in the Galactic halo might produce high energy neutrinos detectable with neutrino telescopes. We have conducted a search for such a signal using 276 days of ...data from the IceCube 22-string configuration detector acquired during 2007 and 2008. The effect of halo model choice in the extracted limit is reduced by performing a search that considers the outer halo region and not the Galactic Center. We constrain any large-scale neutrino anisotropy and are able to set a limit on the dark matter self-annihilation cross section of h <sigma(A)nu > similar or equal to 10(-22) cm(3) s(-1) for weakly interacting massive particle masses above 1 TeV, assuming a monochromatic neutrino line spectrum.
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