Discovery of very high energy gamma-ray emission in the W 28 (G6.4-0.1) region, and multiwavelength comparisons

H.E.S.S. observations of the old-age (>10^4yr; ~0.5deg diameter) composite supernova remnant (SNR) W 28 reveal very high energy (VHE) gamma-ray emission situated at its northeastern and southern boundaries. The northeastern VHE source (HESS J1801-233) is in an area where W 28 is interacting with a dense molecular cloud, containing OH masers, local radio and X-ray peaks. The southern VHE sources (HESS J1800-240 with components labelled A, B and C) are found in a region occupied by several HII regions, including the ultracompact HII region W 28A2. Our analysis of NANTEN CO data reveals a dense molecular cloud enveloping this southern region, and our reanalysis of EGRET data reveals MeV/GeV emission centred on HESS J1801-233 and the northeastern interaction region.Comment: 4 pages, 3 figures, proceedings of the 30th ICRC, Merida, Mexico, 200

XMM-Newton observations of HESS J1813-178 reveal a composite Supernova remnant

We present X-ray and 12CO(J=1-0) observations of the very-high-energy (VHE) gamma-ray source HESS J1813-178 with the aim of understanding the origin of the gamma-ray emission. Using this dataset we are able to undertake spectral and morphological studies of the X-ray emission from this object with greater precision than previous studies. NANTEN 12CO(J=1-0) data are used to search for correlations of the gamma-ray emission with molecular clouds which could act as target material for gamma-ray production in a hadronic scenario. The NANTEN 12CO(J=1-0) observations show a giant molecular cloud of mass 2.5 10^5 M_{\sun} at a distance of 4 kpc in the vicinity of HESS J1813-178. Even though there is no direct positional coincidence, this giant cloud might have influenced the evolution of the gamma-ray source and its surroundings. The X-ray data show a highly absorbed non-thermal X-ray emitting object coincident with the previously known ASCA source AX J1813-178 showing a compact core and an extended tail towards the north-east, located in the centre of the radio shell-type Supernova remnant (SNR) G12.82-0.2. This central object shows morphological and spectral resemblance to a Pulsar Wind Nebula (PWN) and we therefore consider that the object is very likely to be a composite SNR. We discuss the scenario in which the gamma-rays originate in the shell of the SNR and the one in which they originate in the central object. We demonstrate, that in order to connect the core X-ray emission to the VHE gamma-ray emission electrons have to be accelerated to energies of at least 1 PeV.Comment: Submitted to A&

CO J=1-0 observations of molecular gas interacting with galactic supernova remnants G5.4-1.2, G5.55+0.32 and G5.71-0.08

The field just West of the galactic supernova remnant W28 (l=6.4\degr, b=-0.2\degr) harbors 3 of 5 newly-discovered 1720 OH maser spots and two recently-discovered candidate supernova candidates (one of which is a $\gamma$-ray source), as well as several compact and classical HII regions. Here, we analyze a datacube of CO J=1-0 emission having 1\arcmin and 1 \kms resolution, made with on-the-fly mapping over the region 5\degr \le l \le 6\degr, -1\degr \le b \le 0.5\degr}. {Extended and often very bright CO emission was detected at the velocities of the 1720 MHz OH masers and around the supernova remnant G5.55+0.32 which lacks a maser. A new bipolar outflow which is marginally resolved at 1\arcmin resolution and strong in CO (12K) was detected at the periphery of G5.55+0.32, coincident with an MSX source; there is also a bright rim of CO just beyond the periphery of the radio remnant. The OH maser near G5.71-0.08 lies on a shell of strongly-emitting molecular gas (up to 20K) . At the -21 \kms velocity of G5.4-1.2, CO covers much of the field but is weak (3 K) and undisturbed near the remnant. The extended molecular gas around the compact H II region and outflow in G5.89-0.39 (W28A2) is shown for the first time.}Comment: 6 Pages, 3 figures submitted to A&A 4 May 200

Chandra Observations of A Galactic Supernova Remnant Vela Jr.: A New Sample of Thin Filaments Emitting Synchrotron X-Rays

A galactic supernova remnant (SNR) Vela Jr. (RX J0852.0$-$4622, G266.6$-$1.2) shows sharp filamentary structure on the north-western edge of the remnant in the hard X-ray band. The filaments are so smooth and located on the most outer side of the remnant. We measured the averaged scale width of the filaments ($w_u$ and $w_d$) with excellent spatial resolution of {\it Chandra}, which are in the order of the size of the point spread function of {\it Chandra} on the upstream side and 49.5 (36.0--88.8) arcsec on the downstream side, respectively. The spectra of the filaments are very hard and have no line-like structure, and were well reproduced with an absorbed power-law model with $\Gamma =$2.67 (2.55--2.77), or a {\tt SRCUT} model with $\nu_{rolloff}$ = 4.3 (3.4--5.3)$\times 10^{16}$ Hz under the assumption of $p=0.3$. These results imply that the hard X-rays are synchrotron radiation emitted by accelerated electrons, as mentioned previously. Using a correlation between a function ${\cal B} \equiv \nu_{rolloff}/w_d^2$ and the SNR age, we estimated the distance and the age of Vela Jr.: the estimated distance and age are 0.33 (0.26--0.50) kpc and 660 (420--1400) years, respectively. These results are consistent with previous reports, implying that ${\cal B}$--age relation may be a useful tool to estimate the distance and the age of synchrotron X-ray emitting SNRs.Comment: 19 pages, 8 figures, ApJ, in pres

Nonthermal X-radiation of SNR RX J1713.7-3946: The Relations to a Nearby Molecular Cloud

The recent X-ray and CO observations of RX J1713.7-3946 show that a significant fraction of the nonthermal X-ray emission of this unique supernova remnant associates, in one way or another, with a molecular cloud interacting with the west part of the shell. This adds a new puzzle in the origin of X-ray emission which cannot be easily explained within the standard model in accordance of which X-rays are result of synchrotron radiation of multi-TeV electrons accelerated by supernova shock waves. We explore an alternative origin of the X-ray emission assuming that it is produced by secondary electrons resulting from high energy hadronic interactions in the molecular gas. Such a scenario could explain in a quite natural way the apparent correlation between the X-ray and CO morphologies. However, the TeV gamma-ray emission recently reported by H.E.S.S. significantly constrains the parameter space of this model. Namely, this mechanism cannot reproduce the bulk of the observed X-ray flux unless one postulates existence of a PeV cosmic-ray component penetrating with an unusually hard spectrum into the dense cloud.Comment: 6 pages, 3 figures, to appear in Proc. of Int. Symp. on High Energy Gamma-ray Astronomy, Heidelberg (July 2004

A religiosidade no processo de viver envelhecendo

This study aimed to identify how religious and spiritual practices are experienced at different ages during the aging process. The study was cross-sectional and observational and conducted in the city of Chapecó, SC, from July 2008 to January 2009. The sample included 2,160 individuals with 720 individuals interviewed in each age group. The analysis was univariate and obtained the absolute and relative frequency of each variable. The final data obtained were statistically analyzed with SPSS 13.0 software. It was observed that 77.6% of the respondents were Catholic and that the older individuals were more religious. A total of 50.6% of the respondents prayed once a day, 38.3% of them to offer thanks and 30.4% in the supine position. We conclude that religiosity is a valuable resource in coping with the crises of everyday life and positively affects physical and mental health, particularly in the elderly.Se objetivó identificar cómo son experimentadas la religiosidad y las prácticas espirituales en las diferentes fajas etarias durante el proceso de envejecimiento. Estudio observacional, de tipo transversal, realizado en Chapecó-SC, de julio 2008 a enero 2009. Muestra de 2160 personas, con 720 individuos entrevistados en cada faja etaria. Se utilizó análisis descriptivo univariado, con obtención de frecuencias simples y relativas para cada variable. Los datos finales recibieron tratamiento estadístico por software SPSS 13.0. Se observó que: 77,6% de los entrevistados eran católicos, que a mayor edad correspondió mayor religiosidad, 50,6% de los entrevistados reza una vez al día, 38,3% de ellos reza para agradecer y 30,4% reza acostado. Se concluye en que la religiosidad es un recurso valioso para enfrentar las crisis cotidianas y un factor que interfiere positivamente en la salud física y mental, principalmente entre las personas ancianas.Este estudo teve o objetivo identificar como a religiosidade e as práticas espirituais são vivenciadas nas diferentes faixas etárias durante processo de envelhecimento. Foi um estudo observacional do tipo transversal, realizado na cidade de Chapecó-SC, no período de Julho de 2008 a Janeiro de 2009. A amostra foi de 2160 pessoas com 720 indivíduos entrevistados em cada faixa etária. A análise foi descritiva univariada, com a obtenção das frequências simples e relativas para cada variável. Os dados finais receberam tratamento estatístico com o software SPSS 13.0. Observou-se que 77,6% dos pesquisados eram católicos, que quanto mais velhos mais religiosos; 50,6% dos pesquisados rezam uma vez por dia, 38,3% destes rezam para agradecer e 30,4% rezam na posição deitada. Concluiu-se que a religiosidade é um recurso valioso no enfrentamento das crises da vida cotidiana e um fator que interfere de maneira positiva na saúde física e mental, principalmente das pessoas idosas