An EXOSAT observation of CTB 80

Angelini, L.; White, N. E.; Parmar, A. N.; Smith, A. D.; Stevens, M.

doi:10.1086/185201

Cited by 3 publications

(3 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The EXOSAT observation confirmed the nonthermal nature of the X-ray spectrum but inferred a smaller photon index of 1.9±0.5 (Angelini et al 1988). Safi-Harb et al (1995) studied CTB 80 and PSR B1951+32 with the Position Sensitive Proportional Counter (PSPC) and the High Resolution Imager (HRI) onboard ROSAT.…”

Section: Introductionmentioning

confidence: 90%

“…The Einstein observations show a central filled X-ray source with a nonthermal X-ray spectrum (photon index ¼ 3:8 þ0:2 À0:3 ), and the morphology of the source has been interpreted as resulting from the relativistic jets energized by the central pulsar (Becker et al 1982;Wang & Seward 1984). The European X-Ray Observatory Satellite (EXOSAT ) observation confirmed the nonthermal nature of the X-ray spectrum but inferred a smaller photon index of 1:9 AE 0:5 (Angelini et al 1988). Safi-Harb et al (1995) studied CTB 80 and PSR B1951+32 with the Position Sensitive Proportional Counter (PSPC) and the High Resolution Imager (HRI ) on board Röntgensatellit (ROSAT ).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

X‐Ray Spectroscopy of PSR B1951+32 and Its Pulsar Wind Nebula

2005

ApJ

View full text Add to dashboard Cite

We present spatially resolved X-ray spectroscopy of PSR B1951+32 and its pulsar wind nebula ( PWN ) in supernova remnant (SNR) CTB 80 from a Chandra observation. The Chandra X-ray map clearly reveals various components of a ram-pressure-confined PWN embedded in the SNR ejecta: a point source representing the pulsar, X-ray emission from the bow shock, a luminous X-ray tail, a 30 00 diameter plateau whose northwestern part is absent, and the more diffuse outer X-ray emission. The plateau is closely surrounded by the radio, [O iii], [S ii], and [N ii] shells, and the outer diffuse emission is mostly within the H shells. While the spectra of all the features are well fitted with power-law models, a power-law plus blackbody model can fit the spectrum of the pulsar significantly better than using a power-law model alone. Generally, the spectra of these components obey the trend of steepening from the inside to the outside. However, the edge of the plateau probably has a harder spectrum than the central region of the plateau. The cause of the apparent hard spectrum of the plateau edge is unclear, but we speculate that it might be due to a shock between the PWN and the SNR ejecta. The possible blackbody radiation component from the pulsar has a temperature of 0:13 AE 0:02 keV and an equivalent emitting radius of 2:2 þ1:4 À0:8 (d/2 kpc) km, and is thus probably from the hot spots on the pulsar. We also show in this paper that the blackbody temperature of the entire surface of PSR B1951+32 is much lower than those predicted by the standard neutron star cooling models.

show abstract

Section: Introductionmentioning

confidence: 90%

Section: Introductionmentioning

confidence: 99%

X‐Ray Spectroscopy of PSR B1951+32 and Its Pulsar Wind Nebula

2005

ApJ

View full text Add to dashboard Cite

show abstract

“…Search for X-ray pulsation from this source with EXOSAT yielded inconclusive evidence for pulsation (confidence level of 97%, byÖgelman & Buccheri 1987, and 93% by Angelini et al 1988). The pulsed emission was detected by ROSAT at a 99% confidence level (Safi-Harb, Ogelman & Finley 1995), which shows a single peak roughly consistent in phase with the radio emission.…”

Section: Introductionmentioning

confidence: 95%

[ITAL]RXTE[/ITAL] Observation of PSR B1951+32

Chang

1997

The Astrophysical Journal

View full text Add to dashboard Cite

We report results of RXTE observations of PSR B1951+32 using the PCA instrument for 19k seconds during 1996 March 24th. We applied the contemporaneous radio ephemeris and various statistical tests to search for evidence of pulsation. These analyses yield intriguing yet inconclusive evidence for the presence of the pulsation in the time series: confidence level for the presence of pulsation is 94.5% in the 2.0-4.8 keV band and 97.6% in the 4.8-6.3 keV band based on the H-test. Under the premise of non-detection of pulsation, we derive estimated 2-σ upper limits for the pulsed flux to be 3.3 × 10 −6 cm −2 s −1 keV −1 in the 2.0-4.8 keV band, 2.7 × 10 −6 cm −2 s −1 keV −1 in the 4.8-8.5 keV band, and 2.0 × 10 −6 cm −2 s −1 keV −1 in the 8.5-13.0 keV band.These upper limits are consistent with the trend of spectral turn-over from high-energy gamma-ray emission as suggested by the OSSE upper limit. Such turn-over strongly suggests the outer magnetosphere as the emission site for pulsed gamma-rays. These RXTE upper limits for X-ray pulsation are, on the other hand, not consistent with the extrapolation of reported power-law spectra from the point source observed by ROSAT in the 0.1-2.4 keV band, assuming a constant pulse fraction: The pulsed soft X-ray emission detected by ROSAT must follow a much softer spectrum than that of the overall point source.

show abstract

Evidence of pulsed X-ray emission from radio pulsar PSR1951+32

Liu

Sun

et al. 1994

Astrophys Space Sci

View full text Add to dashboard Cite

An EXOSAT observation of CTB 80

Cited by 3 publications

References 0 publications

X‐Ray Spectroscopy of PSR B1951+32 and Its Pulsar Wind Nebula

X‐Ray Spectroscopy of PSR B1951+32 and Its Pulsar Wind Nebula

[ITAL]RXTE[/ITAL] Observation of PSR B1951+32

Evidence of pulsed X-ray emission from radio pulsar PSR1951+32

Contact Info

Product

Resources

About