Chandra X - Ray CenterMIT Kavli Institute
نویسنده
چکیده
Some observations are adversely affected by bias-parity errors. To explore the properties of these errors, 16,304 bias-parity error files were obtained from the archive for the interval from the beginning of the mission through July 8, 2010. Figure 1 shows histograms of the total number and the “valid” number (see sec. 1.5) of errors for each file. The results for the valid errors are also listed in Table 1. The results below the horizontal line in the middle of the table are the results for the twelve files that contain errors associated with the “FEP0 problem.” The number of errors, if any, per frame of data is typically very small (Fig. 2 and Table 2). The only bias-parity error files that have more than 10 errors per frame are the twelve files associated with the FEP0 problem. As shown in Figure 3, the number of bias-parity errors varies with time. There is a correlation between the number of errors and the number of pixels on which the errors occur (Fig. 4). Of the 16,304 files, there are only seven where the number of valid errors is not equal to the number of pixels affected by the errors. Six of these seven files are ones associated with FEP0 problem for which the number of errors is comparable to or greater than 262,144, the maximum number of pixels that can be affected by the problem. The seventh file is for OBS ID 7649, where all but one of the 7,439 errors are reported for the pixel (CCD ID, CHIPX, CHIPY) = (8, 786, 356). The distribution of the valid errors in chip coordinates is shown in Figure 5. Inspection of this figure suggests that there is a periodic pattern every 32 pixels in CHIPX. Figures 6 and 7 confirm the existence of a periodic pattern. As shown in Figure 8, there is a similar, but much less pronounced, 32-pixel periodicity in the CHIPX values of the errors associated with the FEP0 problem. A much more prominent feature of the FEP0 errors is that they only occur in columns with odd values of CHIPX (Fig. 9) and in rows with values of CHIPY ≥ 513 (Fig. 8). The remainder of this spec describes how the tool acis build badpix handles bias-parity error files.
منابع مشابه
Chandra Observations of the X - ray Environs of SN 1998 bw / GRB 980425
We report X-ray studies of the environs of SN 1998bw and GRB 980425 using the Chandra X-Ray Observatory 1281 days after the GRB. Eight X-ray point sources were localized, three and five each in the original error boxes S1 and S2 assigned for variable X-ray counterparts to the GRB by BeppoSAX. The sum of the discrete X-ray sources plus continuous emission in S2 observed by CXO on day 1281 is wit...
متن کاملJ ul 2 00 9 X - ray and Optical Study of Low Core Density Globular Clusters NGC 6144 and E 3
We report on the Chandra X-ray Observatory and Hubble Space Telescope observation of two low core density globular clusters, NGC6144 and E3. By comparing the number of X-ray sources inside the half-mass radius to those outside, we found 6 X-ray sources within the half-mass radius of NGC6144, among which 4 are expected to be background sources; 3 X-ray sources are also found within the half-mass...
متن کاملVariability of Nineteen Millisecond Pulsars in 47 Tucanae with CHANDRA/HRC-S
We present results from our 830 ksec observation of the globular cluster 47 Tucanae with the Chandra X-ray Observatory’s High Resolution Camera-S. We limit our analysis here to the 19 previously known, localized millisecond pulsars (MSPs) in the cluster. This work more than doubles the sample of X-ray-detected MSPs observed with sensitivity to rotational variability; it is also the first survey...
متن کاملEvidence for a Canonical GRB Afterglow Light Curve in the Swift XRT Data
We present new observations of the early X-ray afterglows of the first 27 gamma-ray bursts (GRBs) well-observed by the Swift X-ray Telescope (XRT). The early X-ray afterglows show a canonical behavior, where the light curve broadly consists of three distinct power law segments: (i) an initial very steep decay (∝ t with 3 . α1 . 5) , followed by (ii) a very shallow decay (0.5 . α2 . 1.0), and fi...
متن کاملChandra X-ray Observation of a Mature Cloud-Shock Interaction in the Bright Eastern Knot Region of Puppis A
We present Chandra X-ray images and spectra of the most prominent cloudshock interaction region in the Puppis A supernova remnant. The Bright Eastern Knot (BEK) has two main morphological components: (1) a bright compact knot that lies directly behind the apex of an indentation in the eastern X-ray boundary and (2) lying 1 westward behind the shock, a curved vertical structure (bar) that is sep...
متن کامل