Table 1 - uploaded by Andy Shearer
Content may be subject to copyright.
Source publication
Using time-resolved two-dimensional aperture photometry we have put upper limits on the pulsed emission from two proposed optical counterparts for PSR B1951+32. Our pulsed upper limits of m_{vpulsed}>23.3, m_{bpulsed}>24.4$, for the first candidate and m_{vpulsed}>23.6$, m_{bpulsed}>24.3 for the second, make it unlikely that either of these is, in...
Contexts in source publication
Context 1
... observations were made with standard B and V filters and are summarised in Table 1. In all, a total of 19,456 seconds of B-band data and 8,173 seconds of V- band data were collected. ...
Context 2
... 4 shows the extension along with a another Fig. 2. B-band image of the core region of CTB 80. The image was made from the B-band observations listed in Table 1, and is equivalent to a total exposure of 16,456 seconds. The star identifications refer to those listed in Blair & Schild (1985). ...
Similar publications
We present X-ray imaging, timing, and phase-resolved spectroscopy of the anomalous X-ray pulsar 1E 2259+586 using the Chandra X-Ray Observatory. The spectrum is well described by a power-law plus blackbody model with Γ = 3.6(1), kTBB = 0.412(6) keV, and NH = 0.93(3) × 1022 cm-2; we find no evidence for spectral features (0.5-7.0 keV). We derive a n...
Citations
The scientific performance evaluation of a photon countingimaging system is presented. The detector is constituted by an ICCD camera with RbTe photocathode(optimized for UV radiation), and dedicated electronics for the acquisition and analysis ofthe events. For each photon event on the CCD, a real-time centroid calculation is performed, inorder to reach spatial resolution down to 25 m FWHM. The system has been tested usingthe 182 cm telescope of the Asiago Observatory.A standard stars field through U Johnson filter,and the Crab pulsar (PSR 0531+21) were observed. From the photometric data, relative magnitudes of the standard stars have been derived, showing a goodlinearity of the detector in the range of flux under consideration, as expected fromprevious laboratory measurements.The pulsar's data have been processed by FFT and epoch foldingtechniques to testthe detector's timing performances in the highest resolutionmode (4.512 ms).These observations show that a space resolved time analysis ofperiodic sources can be performed with 10-7 s accuracy.
There remain several definitive gamma-ray pulsars that are as yet undetected in the optical regime. A classic case is the pulsar PSR B1951+32, associated with the complex CTB 80 SNR. Previous ground based high speed 2-d optical studies have ruled out candidates to V ~ 24. Hester (2000a) has reported an analysis of archival HST/WFPC2 observations of the CTB 80 complex which suggest a compact synchrotron nebula coincident with the pulsar's radio position. Performing a similar analysis, we have identified a possible optical counterpart within this synchrotron nebula at V ~ 25.5 - 26, and another optical counterpart candidate nearby at V ~ 24.5. We assess the reality of these counterpart candidates in the context of existing models of pulsar emission. Comment: 7 pages, 5 figures, Accepted for publication in Astronomy & Astrophysics
