Black Holes at the IceCube Neutrino Telescope

If the fundamental Planck scale is about a TeV and the cosmic neutrino flux is at the Waxman-Bahcall level, quantum black holes are created daily in the Antarctic ice-cap. We re-examine the prospects for observing such black holes with the IceCube neutrino-detection experiment. To this end, we first revise the black hole production rate by incorporating the effects of inelasticty, i.e., the energy radiated in gravitational waves by the multipole moments of the incoming shock waves. After that we study in detail the process of Hawking evaporation accounting for the black hole's large momentum in the lab system. We derive the energy spectrum of the Planckian cloud which is swept forward with a large, O (10^6), Lorentz factor. (It is noteworthy that the boosted thermal spectrum is also relevant for the study of near-extremal supersymmetric black holes, which could be copiously produced at the LHC.) In the semiclassical regime, we estimate the average energy of the boosted particles to be less than 20% the energy of the neutrino-progenitor. Armed with such a constraint, we determine the discovery reach of IceCube by tagging on "soft" (relative to what one would expect from charged current standard model processes) muons escaping the electromagnetic shower bubble produced by the black hole's light descendants. The statistically significant 5-sigma excess extends up to a quantum gravity scale ~ 1.3 TeV.Comment: Matching version to be published in Phys. Rev.

Non-gaussianities and the Stimulated creation of quanta in the inflationary universe

Cosmological inflation generates a spectrum of density perturbations that can seed the cosmic structures we observe today. These perturbations are usually computed as the result of the gravitationally-induced spontaneous creation of perturbations from an initial vacuum state. In this paper, we compute the perturbations arising from gravitationally-induced stimulated creation when perturbations are already present in the initial state. The effect of these initial perturbations is not diluted by inflation and survives to its end, and beyond. We consider a generic statistical density operator $\rho$ describing an initial mixed state that includes probabilities for nonzero numbers of scalar perturbations to be present at early times during inflation. We analyze the primordial bispectrum for general configurations of the three different momentum vectors in its arguments. We find that the initial presence of quanta can significantly enhance non-gaussianities in the so-called squeezed limit. Our results show that an observation of non-gaussianities in the squeezed limit can occur for single-field inflation when the state in the very early inflationary universe is not the vacuum, but instead contains early-time perturbations. Valuable information about the initial state can then be obtained from observations of those non-gaussianities.Comment: 25 page

Revising the observable consequences of slow-roll inflation

We study the generation of primordial perturbations in a (single-field) slow-roll inflationary universe. In momentum space, these (Gaussian) perturbations are characterized by a zero mean and a non-zero variance $\Delta^2(k, t)$. However, in position space the variance diverges in the ultraviolet. The requirement of a finite variance in position space forces one to regularize $\Delta^2(k, t)$. This can (and should) be achieved by proper renormalization in an expanding universe in a unique way. This affects the predicted scalar and tensorial power spectra (evaluated when the modes acquire classical properties) for wavelengths that today are at observable scales. As a consequence, the imprint of slow-roll inflation on the CMB anisotropies is significantly altered. We find a non-trivial change in the consistency condition that relates the tensor-to-scalar ratio $r$ to the spectral indices. For instance, an exact scale-invariant tensorial power spectrum, $n_t=0$, is now compatible with a non-zero ratio $r\approx 0.12\pm0.06$, which is forbidden by the standard prediction ($r=-8n_t$). The influence of relic gravitational waves on the CMB may soon come within the range of planned measurements, offering a non-trivial test of the new predictions.Comment: 24 page

Performance of the CMS Regional Calorimeter Trigger

The CMS Regional Calorimeter Trigger (RCT) receives eight-bit energies and a data quality bit from the HCAL and ECAL Trigger Primitive Generators (TPGs). The RCT uses these trigger primitives to find e/γ candidates and calculate regional calorimeter sums that are sent to the Global Calorimeter Trigger (GCT) for sorting and further processing. The RCT hardware consists of one clock distribution crate and 18 double-sided crates containing custom boards, ASICs, and backplanes. The RCT electronics have been completely installed since 2007. The RCT has been integrated into the CMS Level-1 Trigger chain. Regular runs, triggering on cosmic rays, prepare the CMS detector for the restart of the LHC. During this running, the RCT control is handled centrally by CMS Run Control and Monitor System communicating with the Trigger Supervisor. Online Data Quality Monitoring (DQM) evaluates the performance of the RCT during these runs. Offline DQM allows more detailed studies, including trigger efficiencies. These and other results from cosmicray data taking with the RCT will be presented

Enhanced local-type inflationary trispectrum from a non-vacuum initial state

We compute the primordial trispectrum for curvature perturbations produced during cosmic inflation in models with standard kinetic terms, when the initial quantum state is not necessarily the vacuum state. The presence of initial perturbations enhances the trispectrum amplitude for configuration in which one of the momenta, say $k_3$, is much smaller than the others, $k_3 \ll k_{1,2,4}$. For those squeezed configurations the trispectrum acquires the so-called local form, with a scale dependent amplitude that can get values of order $\epsilon ({k_1}/{k_3})^2$. This amplitude can be larger than the prediction of the so-called Maldacena consistency relation by a factor $10^6$, and can reach the sensitivity of forthcoming observations, even for single-field inflationary models.Comment: 11 pages, 1 figure. References added, typos corrected, minor change

Long-term survival after liver transplantation in children with metabolic disorders

Background: Liver transplantation for inherited metabolic disorders aims to save the patient's life when the disorder is expected to progress to organ failure, and to cure the underlying metabolic defect. Methods : We retrospectively analyzed 146 pediatric liver transplants (28 metabolic; 118 non-metabolic) performed between 1986 and 2000. Results : Twenty-eight transplants were performed in 24 children with metabolic disease (8 females; 16 males; age range 3 months to 17 yr). Indications included α−1-antitrypsin deficiency (n = 8), two cases each of hyperoxaluria type 1, Wilson's disease, hereditary tyrosinemia type I, citrullinemia, methylmalonic acidemia, and one case each of propionic acidemia, Crigler–Najjar syndrome type I , neonatal hemachromatosis, hemophilia B, Niemann–Pick disease type B, and cystic fibrosis. Eighteen transplants were whole organ grafts and 10 were lobar or segmental. Auxiliary liver transplants were performed in two patients and three received combined liver-kidney transplants. There were three deaths from sepsis, two from chronic rejection, and one from fulminant hepatitis. Seven of 10 patients currently of school age are within 1 yr of expected grade and three who had pretransplant developmental delay have remained in special education. Actuarial survival rates at 5 and 10 yr are 78% and 68%, respectively, with mean follow-up in excess of 5 yr. These results compare favorably to 100 pediatric patients transplanted for non-metabolic etiologies (65% and 61%, respectively) (p= NS). Conclusions : Pediatric liver transplantation for metabolic disorders results in excellent clinical and biochemical outcome with long survival and excellent quality of life for most recipients.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/72583/1/j.1399-3046.2002.02009.x.pd

Revising the predictions of inflation for the cosmic microwave background anisotropies

We point out that if quantum field renormalization is taken into account, and the counterterms are evaluated at the Hubble-radius crossing time or few e-foldings after it, the predictions of slow-roll inflation for both the scalar and tensorial power spectrum change significantly. This leads to a change in the consistency condition that relates the tensor-to-scalar amplitude ratio with spectral indices. A reexamination of the potentials $\bf{\phi^2, \phi^4}$, shows that both are compatible with five-year WMAP data. Only when the counterterms are evaluated at much larger times beyond the end of inflation one recovers the standard predictions. The alternative predictions presented here may soon come within the range of measurement of near-future experiments.Comment: 4 pages, 1 figure. Expanded version. To appear in Phys. Rev. Let

Determining the main-sequence mass of Type II supernova progenitors

We present radiation-hydrodynamics simulations of core-collapse supernova (SN) explosions, artificially generated by driving a piston at the base of the envelope of a rotating or non-rotating red-supergiant progenitor star. We search for trends in ejecta kinematics in the resulting Type II-Plateau (II-P) SN, exploring dependencies with explosion energy and pre-SN stellar-evolution model. We recover the trivial result that larger explosion energies yield larger ejecta velocities in a given progenitor. However, we emphasise that for a given explosion energy, the increasing helium-core mass with main-sequence mass of such Type II-P SN progenitors leads to ejection of core-embedded oxygen-rich material at larger velocities. We find that the photospheric velocity at 15d after shock breakout is a good and simple indicator of the explosion energy in our selected set of pre-SN models. This measurement, combined with the width of the nebular-phase OI6303-6363A line, can be used to place an upper-limit on the progenitor main-sequence mass. Using the results from our simulations, we find that the current, but remarkably scant, late-time spectra of Type II-P SNe support progenitor main-sequence masses inferior to ~20Msun and thus, corroborate the inferences based on the direct, but difficult, progenitor identification in pre-explosion images. The narrow width of OI6303-6363A in Type II-P SNe with nebular spectra does not support high-mass progenitors in the range 25-30Msun. Combined with quantitative spectroscopic modelling, such diagnostics offer a means to constrain the main-sequence mass of the progenitor, the mass fraction of the core ejected, and thus, the mass of the compact remnant formed.Comment: accepted to MNRA