|created: 30 Dec. 2008|
updated: 12 Jan. 2009
This web page summarizes some further analyses of the Chandra LETG-ACIS observations of the planetary nebula BD+30 3639. See Yu et al. 2009 and references therein for more information on the observations.
This page is a beginning, some further questions/items are:
- Why is the Eastern region bright ? Due to N_H variation? Temp? Interaction with denser material?
- Implement a spatially-varying N_H "screen" in the model and simulate line-images due to it.
- Is there significant ionized absorption that would modify the X-ray spectrum ?
- Use a tri-axial ellipsoid in the model; this may not change the projected image very much but would be more similar to Li et al. 2002..
- Better determine the absolute coordinates in the data/model to locate the WC star and other emssion relative to the X-ray.
- Put these analyses into context of other BD+30 papers/results.
Absorption: Ionized and/or Multi-N_H
Two effects may complicate the simple "wabs" model of X-ray absorption: i) ioniztion and ii) spatial variation.
3D Spheroid images and the Li+ 2002 ellipsoid
As a starting point a simple model was made with a fixed arc of emsission (as suggested in Fig.6 of Kastener+ 2002) plus an adjustable spheroid of emission. Note that the "origin" of the model is x-ray center determined by tgdetect applied to the zeroth-order data; this is why the model appears off-center (image at right). Here are some diagrams sketched in Keynote using rotated 3D images from this "K02fig6nocrop" model:
MCMC Fitting Plots for "K02fig6nocrop" model parameters
An MCMC "exploration" (e2d_mcmc_explore) was carried out to determine the best-fit parameter values of the model. The low-Chi^2 range in parameter space, as well as parameter correlations, are shown in the plots from the MCMC process below.
Using the simple "K02fig6nocrop" model, it is possible to compare simulated dispersed line images with the actual data. Because the number of counts in the dispersed line-images is low (50 to 290) it is useful to combine the roll sets and focus primarilly on any differences between data and model in the bright (Eastern arc) region versus the more extended region. Because the "center" of the data/model is near the bright X-ray region, different rolls will have their bright region events overlap while the more extended emission will be separated. As an example, the three images below show the O VIII (~ 19A) line image as seen in the LEG+1 image for each roll angle and for their combination.
LEG+1, roll ~ +53 deg.
LEG+1, roll ~ -25 deg.
LEG+1, Combined rolls
The table below gives line-images for 12 lines in the BD+30 spectra and the C VI RRC region (25.0 to 25.7 A, see Nordon et al. 2009, arXiv:0901.1039). These are generally from the combined LEG+1 orders because of their greater sensitivity ("dat15" is in the filename of their 1d plots.) In four cases the combination of all 4 LEG spectra ("dat17") were used and for the C VI 33.73 A line the LEG-1 orders were used.
Besides the images, plots of 1D projections along the two axes, wavelength and cross-dispersion ("TG_D" in arc seconds), are given as well. Note that the data and model have been finely binned and smoothed, this helps show the individual events in the images.
The second plot, below the projection, is a K-S test plot showing the cummulative fraction of data and model events; the smoothing is not applied here. The "p-value" shows the chance that these are from the same underlying distribution and is generally greater than 0.1, suggesting that the data and model agree to the level of the statistics.
Looking at the images and K-S p-values, there are some images where the data (yellow dots) appear to have a significantly different distribution from the model (green):
These analyses/plots were made with
|Mg XI r |
||Ne IX He-beta |
|Ne X Ly-alpha |
|Ne IX r |
|Ne IX f |
|O VIII Ly-beta |
|O VII He-beta |
|O VIII Ly-alpha |
|O VII r |
|O VII f |
|C VI RRC |
|C VI Ly-beta |
|C VI Ly-alpha|
Extended view of the RRC and the Lyman series limit
To get a better perspective on the 25.5 A events near the C VI RRC,
the images and plots below cover from 24.3 A (left) to 26.6 A (right);
the RRC is just left-of-center.
The data events are shown as yellow dots and the (higher-density) predicted MC model events are in green.
The highest Lyman series line in the model, Ly-delta, is near the right edge (n=5 --> n=1, ~ 26.35 A).
Data from the two rolls (see O VIII example above) are shown separately - because the 25.5 A events show up at each roll this rules out that they are due to a single contaminating source.
The 25.5 A events corespond to n ~ 11 --> n=1 transitions and the n=11 level is about 3000 A from the series limit.
Roll +53, LEG +1, C VI RRC region (90 cts)||
Roll -25, LEG +1, C VI RRC region (84 cts)|
These analyses/plots were made with Event-2D s/w using the files: analysis_rrc.sl, bd30_model_wRRC.sl, and bd30_data.sl .