Search for Gamma-Ray Spectral Lines from Dark Matter Annihilation up to 100 TeV toward the Galactic Center with MAGIC.

Linelike features in TeV γ rays constitute a "smoking gun" for TeV-scale particle dark matter and new physics. Probing the Galactic Center region with ground-based Cherenkov telescopes enables the search for TeV spectral features in immediate association with a dense dark matter reservoir at a sensitivity out of reach for satellite γ-ray detectors, and direct detection and collider experiments. We report on 223 hours of observations of the Galactic Center region with the MAGIC stereoscopic telescope system reaching γ-ray energies up to 100 TeV. We improved the sensitivity to spectral lines at high energies using large-zenith-angle observations and a novel background modeling method within a maximum-likelihood analysis in the energy domain. No linelike spectral feature is found in our analysis. Therefore, we constrain the cross section for dark matter annihilation into two photons to ⟨σv⟩≲5×10^{-28} cm^{3} s^{-1} at 1 TeV and ⟨σv⟩≲1×10^{-25} cm^{3} s^{-1} at 100 TeV, achieving the best limits to date for a dark matter mass above 20 TeV and a cuspy dark matter profile at the Galactic Center. Finally, we use the derived limits for both cuspy and cored dark matter profiles to constrain supersymmetric wino models.

Bounds on Lorentz Invariance Violation from MAGIC Observation of GRB 190114C.

On January 14, 2019, the Major Atmospheric Gamma Imaging Cherenkov telescopes detected GRB 190114C above 0.2 TeV, recording the most energetic photons ever observed from a gamma-ray burst. We use this unique observation to probe an energy dependence of the speed of light in vacuo for photons as predicted by several quantum gravity models. Based on a set of assumptions on the possible intrinsic spectral and temporal evolution, we obtain competitive lower limits on the quadratic leading order of speed of light modification.

Periprosthetic femoral fractures after hemiarthroplasty. An analysis of 17 cases.

PURPOSE: To describe the characteristics of patients with periprosthetic femoral fractures after hemiarthroplasty and analyze their treatment. MATERIAL AND METHOD: An observational, longitudinal, retrospective study was conducted on a series of 17 patients with periprosthetic femoral fractures after hip hemiarthroplasty. Fourteen fractures were treated surgically. The characteristics of patients, fractures and treatment outcomes in terms of complications, mortality and functionality were analyzed. RESULTS: The large majority (82%) of patients were women, the mean age was 86 years and with an ASA index of 3 or 4 in 15 patients. Ten fractures were type B. There were 8 general complications, one deep infection, one mobilization of a non-exchanged hemiarthroplasty, and 2 non-unions. There were 85% consolidated fractures, and only 5 patients recovered the same function prior to the injury. At the time of the study 9 patients had died (53%). DISCUSSION: Periprosthetic femoral fractures after hemiarthroplasty will increase in the coming years and their treatment is difficult. CONCLUSION: Periprosthetic femoral fractures after hemiarthroplasty are more common in women around 90 years-old, and usually occur in patients with significant morbidity. Although the Vancouver classification is reliable, simple and reproducible, it is only a guide to decide on the best treatment in a patient often fragile. The preoperative planning is essential when deciding a surgical treatment.

Black hole physics. Black hole lightning due to particle acceleration at subhorizon scales.

Supermassive black holes with masses of millions to billions of solar masses are commonly found in the centers of galaxies. Astronomers seek to image jet formation using radio interferometry but still suffer from insufficient angular resolution. An alternative method to resolve small structures is to measure the time variability of their emission. Here we report on gamma-ray observations of the radio galaxy IC 310 obtained with the MAGIC (Major Atmospheric Gamma-ray Imaging Cherenkov) telescopes, revealing variability with doubling time scales faster than 4.8 min. Causality constrains the size of the emission region to be smaller than 20% of the gravitational radius of its central black hole. We suggest that the emission is associated with pulsar-like particle acceleration by the electric field across a magnetospheric gap at the base of the radio jet.

[Solitary proximal end of femur osteochondroma. An indication and result of the en bloc resection without hip luxation]. / Osteocondromas solitarios del extremo proximal del fémur. Indicación y resultados de la resección en bloque sin luxación de la cadera.

OBJECTIVE: To review the indication of surgical treatment of solitary proximal end of femur osteochondromas, and present our experience as regards the approach for a complete and safe resection. MATERIAL AND METHOD: A retrospective study of a series of 6 symptomatic solitary proximal end of femur osteochondromas treated by en bloc resection by means of a single anterior or posterior-lateral approach. The patients were followed up routinely, as well as contacted by telephone to find out their current status. The functional assessment was made using the Musculoskeletal Tumour Society (MSTS) scale. The main limitation of the study was the its low level of recommendation. RESULTS: There were no post-operative complications and, after a mean follow of 8 years (rang:2-21 years), the clinical result was excellent or good in all cases, and there were no recurrences of the tumour. DISCUSSION: Although some authors have proposed femur head subluxation or luxation to expose the whole of the femur neck and head to facilitate the resection of the osteochondroma and the joint exploration, in our experience, this can be avoided in the majority of cases. CONCLUSIONS: Surgical treatment of solitary proximal end of femur osteochondromas is mandatory, as is the detailed pre-operative study of each case. Depending on their implantation and extension, en bloc resection can be performed by a single wide approach without the need for hip luxation.

Observation of pulsed gamma-rays above 25 GeV from the Crab pulsar with MAGIC.

One fundamental question about pulsars concerns the mechanism of their pulsed electromagnetic emission. Measuring the high-end region of a pulsar's spectrum would shed light on this question. By developing a new electronic trigger, we lowered the threshold of the Major Atmospheric gamma-ray Imaging Cherenkov (MAGIC) telescope to 25 giga-electron volts. In this configuration, we detected pulsed gamma-rays from the Crab pulsar that were greater than 25 giga-electron volts, revealing a relatively high cutoff energy in the phase-averaged spectrum. This indicates that the emission occurs far out in the magnetosphere, hence excluding the polar-cap scenario as a possible explanation of our measurement. The high cutoff energy also challenges the slot-gap scenario.

Very-high-energy gamma rays from a distant quasar: how transparent is the universe?

The atmospheric Cherenkov gamma-ray telescope MAGIC, designed for a low-energy threshold, has detected very-high-energy gamma rays from a giant flare of the distant Quasi-Stellar Radio Source (in short: radio quasar) 3C 279, at a distance of more than 5 billion light-years (a redshift of 0.536). No quasar has been observed previously in very-high-energy gamma radiation, and this is also the most distant object detected emitting gamma rays above 50 gigaelectron volts. Because high-energy gamma rays may be stopped by interacting with the diffuse background light in the universe, the observations by MAGIC imply a low amount for such light, consistent with that known from galaxy counts.

Variable very-high-energy gamma-ray emission from the microquasar LS I +61 303.

Microquasars are binary star systems with relativistic radio-emitting jets. They are potential sources of cosmic rays and can be used to elucidate the physics of relativistic jets. We report the detection of variable gamma-ray emission above 100 gigaelectron volts from the microquasar LS I 61 + 303. Six orbital cycles were recorded. Several detections occur at a similar orbital phase, which suggests that the emission is periodic. The strongest gamma-ray emission is not observed when the two stars are closest to one another, implying a strong orbital modulation of the emission or absorption processes.