scholarly journals Discovery of a supernova remnant with a central X-ray source: AX J184453.3-025642 in G 29.6+0.1

2000 ◽  
Vol 177 ◽  
pp. 707-708
Author(s):  
E. V. Gotthelf ◽  
G. Vasisht ◽  
B. Gaensler ◽  
K. Torii
Keyword(s):  
Supernova Remnant ◽  
Dramatic Reduction ◽  
X Ray ◽  
Preliminary Results ◽  
The Third ◽  
Error Circle

AbstractWe report preliminary results from our follow-up X-ray and radio study of AX J1845–0258, the 7-s X-ray pulsar whose characteristics are similar to those found for the anomalous X-ray pulsars (AXPs). We have located a faint X-ray source within the pulsar’s error circle implying a dramatic reduction in flux, however, the source is too faint to provide a confirmation of the expected pulsations. Centered on this X-ray source is a newly discovered supernova remnant, evident in both radio and X-ray emission. This is the third example of an AXP-like object associated with a supernova remnant.

Rostral Leucotomy: a Report on 240 Cases Personally Followed Up After ½ to 5 Years

1955 ◽  
Vol 101 (425) ◽  
pp. 756-773 ◽  
Author(s):  
John Pippard
Keyword(s):  
Standard Technique ◽  
Similar Technique ◽  
Preliminary Results ◽  
The Third ◽  
Follow Up Study ◽  
Major Operation ◽  
Initial Impressions

Cortical undercutting, as an alternative to standard leucotomy and to the major operation of topectomy, was devised by three surgeons independently. Scoville (1949) published his preliminary results soon after McKissock had begun to do rostral leucotomies. Both have continued to use this type of operation (Scoville et al., 1951; Scoville, 1954) but Ferey (1950), the third to develop a similar technique, was disappointed with the results and soon abandoned it (Ferey, 1953). McKissock (1951) reported the initial impressions of the results in 100 cases and by the end of 1952 had operated on 240 cases. During 1953–54, 1½ to 5 years after operation, I followed up these patients, visiting 175 of them in their homes, and 35 in hospital. Personal follow up was refused or for some reason impracticable in 17 cases, including 4 whose case notes had been destroyed; 13 others had died before the survey was made.Partridge (1950) reported a follow up study of 300 cases operated on by the same surgeon by his “standard” technique (McKissock, 1943); he had the advantage, which I had not, of being able to see his patients before operation. I have had to work retrospectively, and the case notes available, whilst often excellent, had usually not been made with the idea that they would be needed for follow-up purposes. I have not, therefore, thought it right to draw more than broad conclusions from this study.

scholarly journals Optical Follow-Up Observations of ASCA Lynx Deep Survey

1998 ◽  
Vol 188 ◽  
pp. 471-472
Author(s):  
K. Ohta ◽  
M. Akiyama ◽  
K. Nakanishi ◽  
T. Yamada ◽  
K. Hayashida ◽  
...  
Keyword(s):  
Energy Density ◽  
Energy Band ◽  
X Ray ◽  
Preliminary Results ◽  
Deep Survey ◽  
X Ray Background

Since the bulk of the energy density of the Cosmic X-ray Background (CXB) resides in the harder energy band than that of the ROSAT band (0.5-2 keV) and since the X-ray sources identified in the ROSAT band have X-ray spectra softer than that of the CXB, investigation of nature of the X-ray sources at the harder energy band is indispensable to solve the origin of the CXB. However, only 2-3% of the CXB in the hard band (2-10 keV) had been resolved into discrete sources (Piccinotti et al. 1982, ApJ 253, 485). We present our preliminary results of optical follow-up observations of the ASCA Lynx deep survey.

scholarly journals Searching for X-ray counterparts of Fermi Gamma-ray pulsars in Suzaku observations

2011 ◽  
Vol 7 (S279) ◽  
pp. 317-318 ◽  
Author(s):  
Yu Aoki ◽  
Takahiro Enomoto ◽  
Yoichi Yatsu ◽  
Nobuyuki Kawai ◽  
Takeshi Nakamori ◽  
...  
Keyword(s):  
Gamma Ray ◽  
Thermal Emission ◽  
Flux Ratio ◽  
Radio Pulsars ◽  
Pulsar Wind Nebulae ◽  
X Ray ◽  
Absorbed Power ◽  
Pulsar Wind ◽  
Error Circle

AbstractWe report the Suzaku follow-up observations of the Gamma-ray pulsars, 1FGL J0614,13328, J1044.55737, J1741.82101, and J1813.31246, which were discovered by the Fermi Gamma-ray observatory. Analysing Suzaku/XIS data, we detected X-ray counterparts of these pulsars in the Fermi error circle and interpreted their spectra with absorbed power-law functions. These results indicate that the origin of these X-ray sources is non-thermal emission from the pulsars or from Pulsar Wind Nebulae (PWNe) surrounding them. Moreover we found that J1741.82101 exhibits a peculiar profile: spin-down luminosity vs flux ratio between X- and gamma-rays is unusually large compared to usual radio pulsars.

scholarly journals The nature of the unassociated 2FGL sources

2014 ◽  
Vol 10 (S313) ◽  
pp. 91-92
Author(s):  
T. Pursimo ◽  
R. Ojha ◽  
E. Ferrara ◽  
F. Acero ◽  
H. Johnston ◽  
...  
Keyword(s):  
Spectral Energy Distribution ◽  
Low Frequency ◽  
Spectral Energy ◽  
High Frequency Peak ◽  
X Ray ◽  
Frequency Peak ◽  
Inverse Compton ◽  
Multi Wavelength ◽  
Error Circle

AbstractThe majority of Fermi-LAT detected (2FGL) sources are AGN, mostly blazars. However, the second largest category in the 2FGL are unassociated sources (~30% or 575 sources), whose multi-wavelength counterpart is either inconclusive or absent. Follow-up observations and archival data at X-ray, optical, and radio frequencies suggest that many unassociated 2FGL sources are strong candidates to be AGN. Typical observed characteristics of 2FGL detected AGN include variability at all frequencies and a spectral energy distribution (SED) with two “bumps”; a low-frequency synchrotron peak in the radio to optical/X-ray region and a high-frequency peak, possibly due to synchrotron self-Compton or Inverse Compton processes, that extends up to TeV energies. We present optical follow-up observations of a sample of Fermi unassociated sources with one or more potential X-ray counterparts detected within the LAT error circle.

scholarly journals N49: The Site of a Gamma-ray Burst. Preliminary Results from X-ray Observations

1983 ◽  
Vol 101 ◽  
pp. 573-577
Author(s):  
G. Pizzichini ◽  
T. L. Cline ◽  
U. D. Desai ◽  
B. J. Teegarden ◽  
W. D. Evans ◽  
...  
Keyword(s):  
High Resolution ◽  
Supernova Remnant ◽  
Gamma Ray ◽  
Large Magellanic Cloud ◽  
X Rays ◽  
Radio Image ◽  
Gamma Ray Burst ◽  
X Ray ◽  
Preliminary Results ◽  
Einstein Observatory

The error box of the unusual Gamma-Ray Burst of March 5, 1979 falls completely inside the optical and radio image of the Supernova Remnant N49 in the Large Magellanic Cloud. This region was observed twice in x-rays with the High Resolution Imager of the Einstein Observatory, six weeks and nearly two years after the Gamma-Ray Burst. We show the comparison between the two observations.

THE PUZZLING JET AND PULSAR WIND NEBULA OF IGR J11014-6103

2014 ◽  
Vol 28 ◽  
pp. 1460172 ◽  
Author(s):  
LUCIA PAVAN ◽  
POL BORDAS ◽  
GERD PÜHLHOFER ◽  
MIROSLAV D. FILIPOVIC ◽  
AIN DE HORTA ◽  
...  
Keyword(s):  
Neutron Star ◽  
Supernova Remnant ◽  
Helical Structure ◽  
Core Collapse ◽  
Radio Observations ◽  
X Ray ◽  
Core Collapse Supernova ◽  
The Core ◽  
Pulsar Wind

IGR J11014-6103 is a hard X-ray source discovered by INTEGRAL. Follow-up X-ray and radio observations revealed an elongated pulsar wind nebula formed by a neutron star escaping supersonically its parent supernova remnant SNR MSH 11-61A. The pulsar also emits highly collimated jets extending perpendicularly to the direction of motion. The jet has a continuous helical structure extending up to more than 10 parsecs. IGR J11014-6103 is a laboratory to study jet ejection in the wind of a pulsar and to constrain the core collapse supernova mechanism responsible for the observed pulsar kick velocity in excess of 1000 km/s.

scholarly journals Spin-Resolved Hα Spectroscopy and Photometry of the Intermediate Polar RXJ0558+5353

1996 ◽  
Vol 158 ◽  
pp. 177-178
Author(s):  
S. R. Duck ◽  
M. D. Still ◽  
A. Allan ◽  
K. Horne ◽  
R. W. Hilditch
Keyword(s):  
Optical Spectroscopy ◽  
Orbital Period ◽  
X Ray ◽  
Preliminary Results ◽  
Spin Period ◽  
Spin Modulation ◽  
Sky Survey

RXJ0558+5353 was discovered and classified as an intermediate polar during the ROSAT all-sky survey and subsequent optical follow up programme (Haberl et al. 1994). A further pointed ROSAT observation revealed a spin periodicity of 272.74 s and a soft X-ray component well represented by an absorbed 57 eV blackbody, the spin modulation being due principally to intensity variations of the component (rather than variable absorption). Optical spectroscopy showed the orbital period to be 4.15 h. In this paper we show the true spin period to be 545.4555(8) s (Allan, Horne & Hilditch 1995), twice the published X-ray period, and also discuss preliminary results of the first spin-resolved spectroscopy of RXJ0558+5353.

scholarly journals Swift-XRT follow-up of gravitational wave triggers during the third aLIGO/Virgo observing run

2020 ◽  
Vol 499 (3) ◽  
pp. 3459-3480
Author(s):  
K L Page ◽  
P A Evans ◽  
A Tohuvavohu ◽  
J A Kennea ◽  
N J Klingler ◽  
...  
Keyword(s):  
Gravitational Wave ◽  
X Ray ◽  
Binary Neutron Star ◽  
The Third ◽  
Mass Gap ◽  
Binary Black Hole ◽  
Sky Survey ◽  
Upper Limits ◽  
Transient Sources

ABSTRACT The Neil Gehrels Swift Observatory followed up 18 gravitational wave (GW) triggers from the LIGO/Virgo collaboration during the O3 observing run in 2019/2020, performing approximately 6500 pointings in total. Of these events, four were finally classified (if real) as binary black hole (BH) triggers, six as binary neutron star (NS) events, two each of NSBH and Mass Gap triggers, one an unmodelled (Burst) trigger, and the remaining three were subsequently retracted. Thus far, four of these O3 triggers have been formally confirmed as real gravitational wave events. While no likely electromagnetic counterparts to any of these GW events have been identified in the X-ray data (to an average upper limit of 3.60 × 10−12 erg cm−2 s−1 over 0.3–10 keV), or at other wavelengths, we present a summary of all the Swift-XRT observations performed during O3, together with typical upper limits for each trigger observed. The majority of X-ray sources detected during O3 were previously uncatalogued; while some of these will be new (transient) sources, others are simply too faint to have been detected by earlier survey missions such as ROSAT. The all-sky survey currently being performed by eROSITA will be a very useful comparison for future observing runs, reducing the number of apparent candidate X-ray counterparts by up to 95 per cent.

The use of self-expanding metallic Wallstents (SMW) in ab-extrinsic ureteral obstructions: Preliminary results

1995 ◽  
Vol 62 (3) ◽  
pp. 380-382
Author(s):  
B. Rovereto ◽  
P. Quaretti ◽  
F. La Marca ◽  
A. Tronci ◽  
D. Cappelli ◽  
...  
Keyword(s):  
Retroperitoneal Fibrosis ◽  
Uterine Cancer ◽  
The Other ◽  
Use Of Self ◽  
Preliminary Results ◽  
The Third ◽  
First Case ◽  
Limited Experience ◽  
Pelvic Relapse

We report the preliminary results of ureteral obstruction treatment with self-expanding metallic Wallstents (SMWs) in 3 women. The causes of the obstructions were: in the first case pelvic relapse of an ovario carcinoma, in the second retroperitoneal fibrosis, and in the third pelvic fibrosis due to uterine cancer radiotherapy. In one patient only one SMW was placed, while in the other two, two SMWs were placed in the same ureter. At follow-up sonography, urography, and CT scan the ureters showed no sign of obstruction. In our limited experience, the SMW device is effective, easy to insert and minimally invasive.

Electron Microscopy of Human Gallstones

1971 ◽  
Vol 29 ◽  
pp. 296-297
Author(s):  
C. Wolpers ◽  
R. Blaschke
Keyword(s):  
Electron Microscopy ◽  
Room Temperature ◽  
Bile Pigment ◽  
X Ray Diffraction ◽  
Triclinic Crystal System ◽  
X Ray ◽  
Follow Up Study ◽  
Infra Red ◽  
Main Components

Scanning microscopy was used to study the surface of human gallstones and the surface of fractures. The specimens were obtained by operation, washed with water, dried at room temperature and shadowcasted with carbon and aluminum. Most of the specimens belong to patients from a series of X-ray follow-up study, examined during the last twenty years. So it was possible to evaluate approximately the age of these gallstones and to get information on the intensity of growing and solving.Cholesterol, a group of bile pigment substances and different salts of calcium, are the main components of human gallstones. By X-ray diffraction technique, infra-red spectroscopy and by chemical analysis it was demonstrated that all three components can be found in any gallstone. In the presence of water cholesterol crystallizes in pane-like plates of the triclinic crystal system.

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