Request PDF on ResearchGate | XTE J+ | Goddard Space Flight Center reports the serendipitous The best-fit position is R.A. 19h 08m 50s, Decl. IAUC cf; cg; cc; XTE J+ The following SN cf is located at R.A. = 12h54m31s, Decl. = o51’24”.8 (equinox ) . The best-fit position is R.A. = 19h08m50s, Decl. seen between and Hz. The authors conclude that XTE J+ is a new blackhole candidate.
By 4may02 the southern source seems to have faded by 2sigmathough it is marginally present peaking at 0.
Central Bureau for Astronomical Telegrams
In several observations the two overlap and you can only see a solid dot. The big circle in the 0. Please do not use these results without first contacting M. On 23apr02 and 1may02 the 8.
XTE J+ Radio Observations
These are based on inverted-parabola fits to find the peak, and may be biased for extended sources. As to the southern dot: 0944 is however an argument for a deeper, HRC observation Unfortunately those data were taken in a narrower bandwidth mode to allow imaging the large initial X-ray error circle, resulting in lower sensitivity.
There’s also the simple statistical dec, for sources which are only sigma; with a beam of x mas on 1may02, this corresponds to mas.
Please send any questions, comments, or suggestions to Michael Rupen at the e-mail address given below.
The open circles represent the peak flux density; the solid dot show the integrated flux density over a small region including roughly a half-beam “guard radius” around the regions of clearly-real emission. These are naturally-weighted images, which bring out the southern component in particular more strongly.
[Bug 2084] R-094: Issues with identity constraints and derivation by restriction
I give two versions of the 4may02 image, the first with the same contours as the previous images, the second using the lower noise level of the 4may02 observations, so that one can see some negative contours. The upper limits correspond to 3-sigma.
We are continuing to observe the source every few days, but will soon 6may02 begin to lose spatial resolution as the VLA antennas are moved to the next-smaller configuration BnA. The two vecl crosses to the south represent the southern component as measured on those same days.
in src/SynTree – Cforall
If it’s not, given the rather high noise level of the initial maps, the southern dot could conceivably have been there forever, hiding below the noise floor. These results are preliminary, and provided here primarily to aid other observers.
The two other northern crosses are the xecl of the northern component from 23apr02 and 1may02; these agree perfectly within the small 09 with the 4may02 position. The positional agreement between those and the slight southern extension hinted at on 4may02 makes me think that that extension is real.
I am currently re-analyzing the earlier data to see whether there is any similar indication of an extension. This is partly because an offset would be so intrinsically interesting that believing it would require fairly overwhelming evidence.
In both cases I’ve superposed some interesting positions. My reading of the Chandra position is that it is basically coincident with the radio source.