Discovery of a Transient X-Ray Pulsar, AX J1841.0-0536, in the Scutum Arm Region with ASCA

We report on the discovery of a transient X-ray pulsar, AX J1841.0-0536, serendipitously found in the Scutum arm region with the ASCA in two separate observations. The X-ray flux is very faint at the beginning, but exhibits two flares in the second observation. The flare flux increases by a factor 10 within only about 1 hr. Coherent pulsations with a period of 4.7394 plus/minus 0.0008 s were detected in the brightest flare phase. The X-ray spectra in the quiescent and flare phases were fitted with an absorbed power-law model with a photon index about 1 plus a narrow Gaussian line at the center energy of 6.4 keV. The interstellar column density of about 3E22 /cm2 may indicate that AX J1841.0-0536 is located at a tangential point of the Scutum arm at about 10 kpc distance. The coherent pulsations, large flux variability and the spectral shape suggest that AX J1841.0-0536 is a Be/X-ray binary pulsar.Comment: 5 pages, 8 figures, uses pasj00.cls; accepted by Publication of the Astronomical Society of Japa

Image-based quantitative determination of DNA damage signal reveals a threshold for G2 checkpoint activation in response to ionizing radiation

Background: Proteins involved in the DNA damage response accumulate as microscopically-visible nuclear foci on the chromatin flanking DNA double-strand breaks (DSBs). As growth of ionizing radiation (IR)-induced foci amplifies the ATM-dependent DNA damage signal, the formation of discrete foci plays a crucial role in cell cycle checkpoint activation, especially in cells exposed to lower doses of IR. However, there is no quantitative parameter for the foci which considers both the number and their size. Therefore, we have developed a novel parameter for DNA damage signal based on the image analysis of the foci and quantified the amount of the signal sufficient for G2 arrest.Results: The parameter that we have developed here was designated as SOID. SOID is an abbreviation of Sum Of Integrated Density, which represents the sum of fluorescence of each focus within one nucleus. The SOID was calculated for individual nucleus as the sum of (area (total pixel numbers) of each focus) x (mean fluorescence intensity per pixel of each focus). Therefore, the SOID accounts for the number, size, and fluorescence density of IR-induced foci, and the parameter reflects the flux of DNA damage signal much more accurately than foci number. Using very low doses of X-rays, we performed a "two-way" comparison of SOID of Ser139-phosphorylated histone H2AX foci between G2-arrested cells and mitosis-progressing cells, and between mitosis-progressing cells in the presence or absence of ATM or Chk1/2 inhibitor, both of which abrogate IR-induced G2/M checkpoint. The analysis revealed that there was a threshold of DNA damage signal for G2 arrest, which was around 4000~5000 SOID. G2 cells with < 4000 SOID were neglected by G2/M checkpoint, and thus, the cells could progress to mitosis. Chromosome analysis revealed that the checkpoint-neglected and mitosis-progressing cells had approximately two chromatid breaks on average, indicating that 4000~5000 SOID was equivalent to a few DNA double strand breaks.Conclusions: We developed a novel parameter for quantitative analysis of DNA damage signal, and we determined the threshold of DNA damage signal for IR-induced G2 arrest, which was represented by 4000~5000 SOID. The present study emphasizes that not only the foci number but also the size of the foci must be taken into consideration for the proper quantification of DNA damage signal

X-Ray Emission from Supernova Remnants Observed in the ASCA Galactic Plane Survey

X-ray images and spectra of 5 cataloged supernova remnants (SNRs), G12.0-0.1, G346.6-0.2, G348.5+0.1, G348.7+0.3, and G355.6-0.0, observed in the ASCA galactic plane survey are presented. The sizes of X-ray emission from G12.0-0.1, G348.5+0.1, G348.7+0.3, and G355.6-0.0 are comparable to their radio structures, while that of G346.6-0.2 is smaller than the radio structure. The X-ray spectra of all of the SNRs were heavily absorbed by interstellar matter with N_H>10^{22} cm^{-2}. The spectrum of G355.6-0.0 exhibited emission lines, indicating that the X-ray emission has a thin thermal plasma origin, and was well represented by two-temperature thin thermal emission model. On the other hand, no clear emission line features were found in the spectra of the others and the spectra could be represented by either a thin thermal emission model or a power-law model.Comment: Accepted for publication in PAS

High-sensitivity VLBI Observations of the Water Masers in the Seyfert Galaxy NGC 1068

We present observational results of water vapor maser emission with our high-sensitivity 22 GHz VLBI imaging of the Seyfert galaxy NGC 1068. In this galaxy, there are the following four nuclear radio sources; NE, C, S1, and S2. Among them, the S1 component has been identified as the nucleus while the C component has been considered as attributed to the radio jet. In our VLBI observation, we find the following two types of the water maser emission at the S1 component. One is the linearly aligned component that is considered as an edge-on disk with the inner radius of 0.62 pc. The dynamical mass enclosed within the inner radius was estimated to be $1.5\times10^7 M_{\odot}$ by assuming the circular Keplerian motion. Note, however, that the best fit rotation curve shows a sub-Keplerian rotation ($v\propto r^{-0.24\pm0.10}$). The other is the water maser emission distributed around the rotating disk component up to 1.5 pc from the S1 component, suggesting the bipolar outflow from the S1 component. Further, we detected the water maser emission in the C component for the first time with VLBI, and discovered a ring-like distribution of the water maser emission. It is known that a molecular cloud is associated with the C component (both HCN and HCO$^+$ emission lines are detected by ALMA). Therefore, the ring-like maser emission can be explained by the jet collision to the molecular cloud. However, if these ring-like water masing clouds constitute a rotating ring around the C component, it is likely that the C component also has a supermassive black hole with the mass of $\sim 10^6 M_{\odot}$ that could be supplied from a past minor merger of a nucleated satellite galaxy.Comment: 16 pages, 10 figures, accepted for publication in the PAS

Episodic Volunteering in Sport Events : A Seven-Country Analysis

Given its ubiquitous nature, sport events are one of the most popular venues for episodic volunteering around the world. This article explores the rare dataset of volunteering in sport events in seven countries-Finland, Ghana, India, Japan, Switzerland, Tanzania, United States-to overview the differences and similarities identified in demography, volunteers' reactions to hosts' management strategies, satisfaction, and intention to volunteer again. Key findings include differences in the level of satisfaction, where responses among American volunteers were the highest. We also find that although well-organized management strategies such as quality training, communication, and proper appreciation led to higher satisfaction, these factors did not contribute to volunteers' intent to volunteer again. Such management style might be too impersonal with less autonomy on the part of volunteers that they may not feel needed in future events. Somewhat messy management might motivate volunteers to participate again.Peer reviewe