Hard X-ray Emission Clumps in the gamma-Cygni Supernova Remnant: an INTEGRAL-ISGRI View

Spatially resolved images of the galactic supernova remnant G78.2+2.1 (gamma-Cygni) in hard X-ray energy bands from 25 keV to 120 keV are obtained with the IBIS-ISGRI imager aboard the International Gamma-Ray Astrophysics Laboratory INTEGRAL. The images are dominated by localized clumps of about ten arcmin in size. The flux of the most prominent North-Western (NW) clump is (1.7 +/- 0.4) 10^{-11} erg/cm^2/s in the 25-40 keV band. The observed X-ray fluxes are in agreement with extrapolations of soft X-ray imaging observations of gamma-Cygni by ASCA GIS and spatially unresolved RXTE PCA data. The positions of the hard X-ray clumps correlate with bright patches of optical line emission, possibly indicating the presence of radiative shock waves in a shocked cloud. The observed spatial structure and spectra are consistent with model predictions of hard X-ray emission from nonthermal electrons accelerated by a radiative shock in a supernova interacting with an interstellar cloud, but the powerful stellar wind of the O9V star HD 193322 is a plausible candidate for the NW source as well.Comment: 5 pages, 5 figures, Astronomy and Astrophysics Letter

Polycyclic aromatic hydrocarbons in the dwarf galaxy IC 10

Infrared observations from the Spitzer Space Telescope archive are used to study the dust component of the interstellar medium in the IC~10 irregular galaxy. Dust distribution in the galaxy is compared to the distributions of H$\alpha$ and [SII] emission, neutral hydrogen and CO clouds, and ionizing radiation sources. The distribution of polycyclic aromatic hydrocarbons (PAH) in the galaxy is shown to be highly non-uniform with the mass fraction of these particles in the total dust mass reaching 4%. PAHs tend to avoid bright HII regions and correlate well with atomic and molecular gas. This pattern suggests that PAHs form in the dense interstellar gas. We propose that the significant decrease of the PAH abundance at low metallicity is observed not only globally (at the level of entire galaxies), but also locally (at least, at the level of individual HII regions). We compare the distribution of the PAH mass fraction to the distribution of high-velocity features, that we have detected earlier in wings of H$\alpha$ and SII lines, over the entire available galaxy area. No conclusive evidence for shock destruction of PAHs in the IC~10 galaxy could be found.Comment: Accepted for publication in Astronomy Report

Gas Emission Spectrum in the Irr Galaxy IC 10

Spectroscopic long-slit observations of the dwarf Irr galaxy IC 10 were conducted at the 6-m Special Astrophysical Observatory telescope with the SCORPIO focal reducer. The ionized-gas emission spectra in the regions of intense current star formation were obtained for a large number of regions in IC 10. The relative abundances of oxygen, N+, and S+ in about twenty HII regions and in the synchrotron superbubble were estimated. We found that the galaxy-averaged oxygen abundance is 12 + log(O/H) = 8.17 +- 0.35 and the metallicity is Z = 0.18 +- 0.14 Z_sun. Our abundances estimated from the strong emission lines are found to be more reliable than those obtained by comparing diagnostic diagrams with photoionization models.Comment: Abridged; accepted in Astronomy Letter

Detailed Kinematic Study of the Ionized and Neutral Gas in the Complex of Star Formation in the Galaxy IC 1613

We carried out detailed kinematic studies of the complex of multiple HI and HII shells that represent the only region of ongoing star formation in the dwarf irregular galaxy IC 1613. We investigated the ionized-gas kinematics by using Fabry--Perot H-alpha observations with the 6-m Special Astrophysical Observatory telescope and the neutral-gas kinematics by using VLA 21-cm radio observations. We identified three extended (300-350 pc) neutral shells with which the brightest HII shells in the complex of star formation are associated. The neutral-gas kinematics in the complex has been studied for the first time and the H~I shells were found to expand at a velocity of 15--18 km/s. We constructed velocity ellipses for all HII shells in the complex and refined (increased) the expansion velocities of most of them. The nature of the interacting ionized and neutral shells is discussed.Comment: 14 pages, 9 EPS-figure

New Studies of the Pulsar Wind Nebula in the Supernova Remnant CTB 80

We investigated the kinematics of the pulsar wind nebula (PWN) associated with PSR B1951+32 in the old supernova remnant CTB 80 using the Fabry-Perot interferometer of the 6m Special Astrophysical Observatory telescope. In addition to the previously known expansion of the system of bright filaments with a velocity of 100-200km/s, we detected weak high-velocity features in the H-alpha line at least up to velocities of 400-450km/s. We analyzed the morphology of the PWN in the H-alpha, [SII], and [OIII] lines using HST data and discuss its nature. The shape of the central filamentary shell, which is determined by the emission in the [OIII] line and in the radio continuum, is shown to be consistent with the bow-shock model for a significant (about 60 degrees) inclination of the pulsar's velocity vector to the plane of the sky. In this case, the space velocity of the pulsar is twice higher than its tangential velocity, i.e., it reaches ~500 km/s, and PSR B1951+32 is the first pulsar whose line-of-sight velocity (of about 400 km/s) has been estimated from the PWN observations. The shell-like H-alpha-structures outside the bow shock front in the east and the west may be associated with both the pulsar's jets and the pulsar-wind breakthrough due to the layered structure of the extended CTB 80 shell.Comment: to appear in Astronomy Letters, 12 pages, 6 postscript figures, two in colour; for a version with high resolution figures see http://www.sao.ru/hq/grb/team/vkom/CTB80_fine.pd

Polarization Observations of 1720 MHz OH Masers toward the Three Supernova Remnants W28, W44, and IC443

(abridged) - We present arcsecond resolution observations from the VLA of the satellite line of the hydroxyl molecule (OH) at 1720.53 MHz toward three Galactic supernova remnants: W28, W44 and IC443. All of our observations are consistent with a model in which the OH(1720 MHz) is collisionally excited by H2 molecules in the postshock gas heated by a non-dissociative shock. Supernova remnants with OH(1720 MHz) maser emission may be promising candidates to conduct high energy searches for the sites of cosmic ray acceleration.Comment: ApJ Let (accepted). Hardcopies available from [email protected]

Multi-wavelength study of a new Galactic SNR G332.5-5.6

We present compelling evidence for confirmation of a Galactic supernova remnant (SNR) candidate, G332.5-5.6, based initially on identification of new, filamentary, optical emission line nebulosity seen in the arcsecond resolution images from the AAO/UKST HAlpha survey. The extant radio observations and X-ray data which we have independently re-reduced, together with new optical spectroscopy of the large-scale fragmented nebulosity, confirms the identification. Optical spectra, taken across five different, widely separated nebula regions of the remnant as seen on the HAlpha images, show average ratios of [NII]/HAlpha =2.42, [SII]/HAlpha = 2.10, and [SII] 6717/6731 = 1.23, as well as strong [OI] 6300, 6364A and [OII] 3727A emission. These ratios are firmly within those typical of SNRs. Here, we also present the radio-continuum detection of the SNR at 20/13cm from observations with the Australia Telescope Compact Array (ATCA). Radio emission is also seen at 4850 MHz, in the PMN survey (Griffith and Wright 1993) and at 843 MHz from the SUMSS survey (Bock, Large and Sadler 1999). We estimate an angular diameter of ~30 arcmin and obtain an average radio spectral index of alpha = -0.6 +- 0.1 which indicates the non-thermal nature of G332.5-5.6. Fresh analysis of existing ROSAT X-ray data in the vicinity also confirms the existence of the SNR. The distance to G332.5-5.6 has been independently estimated by Reynoso and Green (2007) as 3.4 kpc based on measurements of the HI lambda21 cm line seen in absorption against the continuum emission. Our cruder estimates via assumptions on the height of the dust layer (3.1 kpc) and using the Sigma-D relation (4 kpc) are in good agreement.Comment: 14 pages, 18 figures. Accepted for publishing in the MNRA

Synchrotron superbubble in the galaxy IC10: the ionized gas structure, kinematics, and emission spectrum

We have investigated the structure, kinematics, and emission spectrum of the ionized gas in the synchrotron superbubble in the irregular galaxy IC 10 based on observations with the 6-m Special Astrophysical Observatory telescope with the SCORPIO focal reducer in three modes: direct imaging in the [SII](6717+6731)A lines, long-slit spectroscopy, and spectroscopy with a scanning Fabry--Perot interferometer. We have identified a bright (in the [SII] lines) filamentary optical shell and determined its expansion velocity, mass, and kinetic energy. The nature of the object is discussed.Comment: 12 pages, 9 EPS figure

Hymecromone Administration in Real Clinical Practice: Results of the Prospective Multicentre Observational Study in the Republic of Kazakhstan

Introduction. This multicentre prospective non-interventional observational study was conducted to obtain additional data about Odeston efficacy and safety in routine clinical practice. The objectives of the study included collection of clinical characteristics of patients, evaluation of Odeston effects in treatment of biliary pain and changes in the gallbladder emptying, evaluation of compliance to therapy, and treatment effect satisfaction.Materials and methods. The study was conducted from July 2020 to April 2021 at the premises of 60 study sites in 4 cities of the Republic of Kazakhstan. Patients having indications for Odeston administration according to the patient leaflet were enrolled. The study included 2 patient visits and an intermediate telephone contact. A visual analogue scale and RAPID questionnaire were used to characterise biliary pain; severity of associated symptoms, bowel habit and a quality of life according the SF-12 were also assessed. A rate of a ≥50 % reduction in symptom severity was used as a primary efficacy criterion; a rate of a ≥10 improvement in the SF-12 quality of life score was used as a secondary efficacy criterion. Compliance to treatment was evaluated using a number of days on Odeston. Treatment satisfaction was assessed using 5 grades.Results. 877 patients, 68.2 % of females and 31.8 % of males, were included in the study; the mean age was 46.0 ± 14.9 years. Primary functional biliary disorder was diagnosed in 65.3 % of patients, chronic non-calculous cholecystitis — 51.4 %, uncomplicated gallbladder disease — in 8.9 %, biliary sludge — 38.4 %, sphincter of Oddi functional disorder — 5.3 % of patients. A dose of Odeston was prescribed at the discretion of the physician. Group A patients received 600 mg (n = 89), group B received 1200 mg of Odeston a day (n = 788). In group B, an incidence of pronounced pain interference with daily living activities was higher. In both groups, the mean VAS scores were reduced to 1 point on treatment, a primary efficacy criterion was achieved in 77.3 % of patients in group A and in 79.8 % of patients in group B, р < 0.05. In both groups, a reduction in the incidence of constipation and diarrhea (р < 0,001) and an increase in the mean scores of physical and mental functioning were noted (р < 0.001, though a secondary efficacy criterion was not achieved (a ≥10 change in the SF-12 score). A prevalence of ultrasonographic sings of biliary sludge was reduced, and an increased gallbladder emptying was observed (p < 0.001). 77.4 % of patients in a total group of patients reported about drug administration for 21 days. A number of patients who were completely satisfied with treatment was higher in group B (p = 0.027).Conclusions. It was found that biliary pain interfered with daily living activities and commonly accompanied by other symptoms of gastrointestinal dysmotility. Odeston effectively reduces the severity of biliary pain, corrects dyspeptic disorders and normalizes stool pattern in patients with functional and organic diseases of the biliary system. Treatment satisfaction was higher with a dose of 1200 mg a day, particularly in more pronounced interference of pain with daily living activities

MAGIC J0616+225 as delayed TeV emission of cosmic-rays diffusing from SNR IC 443

We present a theoretical model that explains the high energy phenomenology of the neighborhood of SNR IC 443, as observed with the Major Atmospheric Gamma Imaging Cherenkov (MAGIC) telescope and the Energetic Gamma-Ray Experiment Telescope (EGRET). We interpret MAGIC J0616+225 as delayed TeV emission of cosmic-rays diffusing from IC 443 and interacting with a known cloud located at a distance of about 20 pc in the foreground of the remnant. This scenario naturally explains the displacement between EGRET and MAGIC sources, their fluxes, and their spectra. We compare this model with others recently presented, and discuss how it can be tested with observations by the Gamma-ray Large Area Telescope (GLAST).Comment: Accepted for publication in MNRAS Letter