199 research outputs found
Optical Imaging and Spectroscopic Observation of the Galactic Supernova Remnant G85.9-0.6
Optical CCD imaging with H and [SII] filters and spectroscopic
observations of the galactic supernova remnant G85.9-0.6 have been performed
for the first time. The CCD image data are taken with the 1.5m Russian-Turkish
Telescope (RTT150) at TUBITAK National Observatory (TUG) and spectral data are
taken with the Bok 2.3 m telescope on Kitt Peak, AZ.
The images are taken with narrow-band interference filters H, [SII]
and their continuum. [SII]/H ratio image is performed. The ratio
obtained from [SII]/H is found to be 0.42, indicating that the
remnant interacts with HII regions. G85.9-0.6 shows diffuse-shell morphology.
[SII] average flux ratio is calculated from the
spectra, and the electron density is obtained to be 395 . From
[OIII]/H ratio, shock velocity has been estimated, pre-shock density of
, explosion energy of ergs,
interstellar extinction of , and neutral hydrogen column density
of are reported.Comment: 20 pages, 4 tables, 4 figures. Accepted for publication in
Astrophysics & Space Scienc
The first optical light from the supernova remnant G182.4+4.3 located in the Galactic anti-centre region
We report the discovery of optical filamentary and diffuse emission from
G182.4+4.3 using 1.5-m Russian-Turkish telescope. We present the optical CCD
images obtained with Halpha filter revealing the presence of mainly filamentary
structure at the northwest, filamentary and diffuse structure at the centre,
south and north regions of the remnant. The bright optical filaments located in
northwest and south regions are well correlated with the prominent radio shell
of the remnant strongly suggesting their association. From the flux-calibrated
CCD imaging, the average [SII]/Halpha ratio is found to be ~0.9 and ~1.1 for
south and northwest regions, which clearly indicates that the emission
originates from the shock heated gas. We also present the results of X-ray data
obtained from XMM-Newton that show diffuse emission with a very low luminosity
of ~7.3x10^31 erg s^-1 at a distance of 3 kpc in 0.3-10 keV energy band.
Furthermore, we find a surprisingly young age of ~4400 yr for this remnant with
such a large radius of ~22 pc.Comment: 9 pages, 6 figures and 1 table, Accepted for publication in MNRA
A deep X-ray observation of supernova remnant G304.6+0.1 (Kes 17) with Suzaku
In this paper, we present the analysis of a deep (99.6 ks) observation of
G304.6 + 0.1 with the X-ray Imaging Spectrometer on board {\it Suzaku}
satellite. The X-ray spectral data are well-fitted with a plasma model
consisting of a thermal component in collisional ionization equilibrium and a
non-thermal component. The thermal emission is well fitted with VMEKAL model
with an electron temperature of keV, a high absorbing
column density of and near/lower
solar abundances which indicate that the X-ray emitting plasma of G304.6 + 0.1
is dominated by swept-up ambient medium. The non-thermal component is well
fitted with a power-law model with photon index of . We found
a relatively high electron density cm, age
yr, and X-ray emitting mass {M\sun} at an adopted distance of d=10 kpc. Using the morphological
and spectral X-ray data, we confirm that the remnant is a new member of
mixed-morphology supernova remnants.Comment: 8 pages, 4 figures, 2 table
Ejecta detection in the middle-aged Galactic supernova remnant G296.1-0.5 observed with Suzaku
In this paper, we report the detection of ejecta in the middle-aged Galactic
supernova remnant G296.1-0.5 with the X-ray Imaging Spectrometer onboard the
Suzaku satellite. The spectra of three lobes, north, southeast and southwest
and inter-lobe regions, consist of soft (0.3-2.0 keV) emission originated from
non-equilibrium ionization plasma. In north, southeast and inter-lobe regions,
the thermal emission can be represented by a one-component, in southwest region
it can be represented by two- component non-equilibrium ionization (VNEI)
model. The spectra of studied regions have lines of N, O, Ne, Mg and Si
elements. Si emission from this remnant is shown for the first time in this
work. Enhanced abundances of Ne, Mg and Si elements obtained show the ejecta
contribution in all regions. Assuming that the remnant is in Sedov phase, we
obtained ambient density n0 ~ 0.45 cm-3, age t ~ 2.8 x 104 yr, shock velocity
Vs ~ 320 km s-1, shock temperature Ts ~ 1.2 x 106 K, and swept-up mass Msw ~
340 M at an adopted distance of d=3 kpc.Comment: 9 pages, 5 figures, 2 table
Suzaku Observations of Ejecta-Dominated Galactic Supernova Remnant G346.6-0.2
We present here the results of the X-ray analysis of Galactic supernova
remnant G346.6-0.2 observed with {\it Suzaku}. K-shell emission lines of Mg,
Si, S, Ca and Fe are detected clearly for the first time. Strong emission lines
of Si and S imply that X-ray emission nature of G346.6-0.2 is ejecta-dominated.
The ejecta-dominated emission is well fitted with a combined model consisting
of thermal plasma in non-equilibrium ionization and a non-thermal component,
which can be regarded as synchrotron emission with a photon index of
. Absorbing column density of is obtained from the best-fitting implying a high-density medium,
high electron temperature of keV, and ionization timescale
of indicating that this
remnant may be far from full ionization equilibrium. The relative abundances
from the ejecta show that the remnant originates from a Type Ia supernova
explosion.Comment: 7 pages, 4 figur
{\it Suzaku} observation of Galactic supernova remnant CTB 37A (G348.5+0.1)
We present here the results of the observation of CTB 37A obtained with the
X-ray Imaging Spectrometer onboard the {\it Suzaku} satellite. The X-ray
spectrum of CTB 37A is well fitted by two components, a single-temperature
ionization equilibrium component (VMEKAL) with solar abundances, an electron
temperature of keV, absorbing column density of and a power-law component with photon
index of . The X-ray spectrum of CTB 37A is characterized by
clearly detected K-shell emission lines of Mg, Si, S, and Ar. The plasma with
solar abundances supports the idea that the X-ray emission originates from the
shocked interstellar material. The ambient gas density, and age of the remnant
are estimated to be and
yr, respectively. The center-filling X-ray emission
surrounded by a shell-like radio structure and other X-ray properties indicate
that this remnant would be a new member of mixed-morphology supernova remnant
class
HPV testing on self collected cervicovaginal lavage specimens as screening method for women who do not attend cervical screening: cohort study
Objective To determine whether offering self sampling of cervicovaginal material for high risk human papillomavirus (HPV) testing is an effective screening method for women who do not attend regular cervical screening programmes
The contribution of HPV18 to cervical cancer is underestimated using high-grade CIN as a measure of screening efficiency
In one geographical area, 14 high-risk human papillomavirus types in cervical intraepithelial neoplasia (CIN2/3; n=139) and cervical squamous cell carcinoma (SCC; n=84) were analysed. HPV18 was more prevalent in SCC than CIN2/3 (OR 9.8; 95% confidence interval: 2.5–39). Other high-risk types prevalences corresponded in CIN2/3 and SCC. Evaluations using CIN2/3 as a measure of efficiency underestimate the contribution of HPV18 to SCC
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