Calculation of microscopic nuclear level densities based on covariant density functional theory

A microscopic method for calculating nuclear level density (NLD) based on the covariant density functional theory (CDFT) is developed. The particle-hole state density is calculated by combinatorial method using the single-particle levels schemes obtained from the CDFT. Then the level densities are obtained by taking into account collective effects such as vibration and rotation. Our results are compared with those from other NLD models, including phenomenological, microstatistical, and non-relativistic HFB combinatorial models. The comparison suggests that the general trends among these models are basically the same, except for some deviations from different NLD models. In addition, the NLDs of the CDFT combinatorial method with normalization are compared with experimental data, including the observed cumulative number of levels at low excitation energy and the measured NLDs. Compared with the existing experimental data, the CDFT combinatorial method can give reasonable results.Comment: 9 pages, 8 figure

First detection of GeV emission from an ultraluminous infrared galaxy: Arp 220 as seen with the Fermi Large Area Telescope

Cosmic rays (CRs) in starburst galaxies produce high energy gamma-rays by colliding with the dense interstellar medium (ISM). Arp 220 is the nearest ultra luminous infrared galaxy (ULIRG) that has star-formation at extreme levels, so it has long been predicted to emit high-energy gamma-rays. However, no evidence of gamma-ray emission was found despite intense efforts of search. Here we report the discovery of high-energy gamma-ray emission above 200 MeV from Arp 220 at a confidence level of $\sim 6.3 \sigma$ using 7.5 years of \textsl {Fermi} Large Area Telescope observations. The gamma-ray emission shows no significant variability over the observation period and it is consistent with the quasi-linear scaling relation between the gamma-ray luminosity and total infrared luminosity for star-forming galaxies, suggesting that these gamma-rays arise from CR interactions. As the high density medium of Arp 220 makes it an ideal CR calorimeter, the gamma-ray luminosity can be used to measure the efficiency of powering CRs by supernova (SN) remnants given a known supernova rate in Arp 220. We find that this efficiency is about $4.2\pm2.6\%$ for CRs above 1 GeV.Comment: Accepted by ApJL, 6 pages, 3 figure

Evidence of a spectral break in the gamma-ray emission of the disk component of Large Magellanic Cloud: a hadronic origin?

It has been suggested that high-energy gamma-ray emission ($>100{\rm MeV}$) of nearby star-forming galaxies may be produced predominantly by cosmic rays colliding with the interstellar medium through neutral pion decay. The pion-decay mechanism predicts a unique spectral signature in the gamma-ray spectrum, characterized by a fast rising spectrum and a spectral break below a few hundreds of MeV. We here report the evidence of a spectral break around 500 MeV in the disk emission of Large Magellanic Cloud (LMC), which is found in the analysis of the gamma-ray data extending down to 60 MeV observed by {\it Fermi}-Large Area Telescope. The break is well consistent with the pion-decay model for the gamma-ray emission, although leptonic models, such as the electron bremsstrahlung emission, cannot be ruled out completely.Comment: 11 pages, 4 figures, Accepted by Ap

Detection of gamma-ray emission from the Coma cluster with Fermi Large Area Telescope and tentative evidence for an extended spatial structure

Many galaxy clusters have giant halos of non-thermal radio emission, indicating the presence of relativistic electrons in the clusters. Relativistic protons may also be accelerated by merger and/or accretion shocks in galaxy clusters. These cosmic-ray (CR) electrons and/or protons are expected to produce gamma-rays through inverse-Compton scatterings or inelastic $pp$ collisions respectively. Despite of intense efforts in searching for high-energy gamma-ray emission from galaxy clusters, conclusive evidence is still missing so far. Here we report the discovery of $\ge 200$ MeV gamma-ray emission from the Coma cluster direction with an unbinned likelihood analysis of the 9 years of {\it Fermi}-LAT Pass 8 data. The gamma-ray emission shows a spatial morphology roughly coincident with the giant radio halo, with an apparent excess at the southwest of the cluster. Using the test statistic analysis, we further find tentative evidence that the gamma-ray emission at the Coma center is spatially extended. The extended component has an integral energy flux of $\sim 2\times 10^{-12}{\rm \ erg\ cm^{-2}\ s^{-1}}$ in the energy range of 0.2 - 300 GeV and the spectrum is soft with a photon index of $\simeq-2.7$. Interpreting the gamma-ray emission as arising from CR proton interaction, we find that the volume-averaged value of the CR to thermal pressure ratio in the Coma cluster is about $\sim 2\%$. Our results show that galaxy clusters are likely a new type of GeV gamma-ray sources, and they are probably also giant reservoirs of CR protons.Comment: 10 pages, 10 figures, Accepted by Physical Review D, more spatial models for the gamma-ray emission are used, systematic checks on the results are adde

Retinal nerve fiber layer thickness measured by optical coherence tomography in Chinese teenagers aged from 13 years old to 18 years old

AIM: To establish a reference range of retinal nerve fiber layer(RNFL)thickness by optical coherence tomography(OCT)in Chinese teenagers aged from 13 to 18 years old, and investigate its relationship with age, eye side, gender, and ethnic group.<p>METHODS: A total of 402 eyes from 201 normal Chinese aged from 13 to 18 years old were recruited for this study. Optic disk with 3.4mm diameter circle in different global average, quadrant and part-time bit retinal nerve fiber layer thickness(RNFLT)was measured by RNFL thickness average analysis program. Their RNFLT at different part-time bit, quadrant and global average RNFLT around the disc were measured by OCT with 3.4mm diameter circle, using the RNFL thickness average analysis program. The data was analyzed with SPSS statistical 19.0. The influences of several factors(such as age, eye side, gender, and ethnic group)on RNFLT were also analyzed.<p>RESULTS: The global average RNFLT at 13, 14, 15, 16, 17, 18 years old was 108.32±9.42μm, 109.23±9.67μm, 110.36±11.14μm, 111.27±10.21μm, 109.23±9.67μm, 112.11±8.83μm respectively. RNFLT of right eyes was 109.82±8.93μm and of left eyes was 110.33±9.89μm. All of the male's average RNFLT was 110.14±10.02μm, and all of the female's average RNFLT was 109.96±11.22μm. The average RNFLT of Han nationality was 110.22±9.31μm and of non-Han nationality was 109.87±8.65μm. The average RNFLT of all was 110.02±9.87μm, the RNFLT at the superior, nasal, inferior and temporal quadrant was 146.56 ±18.88μm, 76.49±13.28μm, 136.64±16.29μm, 82.01±12.55μm respectively. There was no significant difference in gender, eye side, and ethnic group(all <i>P</i><0.05), but the difference was significant compared with adult's data of the database. <p>CONCLUSION: This study has established a normal standard reference of RNFLT and its related indexes by OCT in Chinese teenagers aged 13-18 years old. Gender, age, eye side, and ethnic group have no effect on their RNFLT, which has significant difference with adult's data. And for the diagnosis and follow-up of diseases involving in RNFL changes, the adult's data can not be used