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Home All issues Volume 497 / No 2 (April II 2009) A&A, 497 2 (2009) 469-480 Full HTML
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Table 1:

Selection of X-ray bursts from GS 1826-24 studied here. For more details, see Galloway et al. (2008).
MJD ObsID Times Active $\Delta^a$
    covered wrt PCUs ($^\prime$)
    burst start    
    time (s)b    
50 971.23019 30054-04-02-01 -2600/+1200 0, 1, 2, 3, 4 0.0
50 971.70032 30054-04-02-000 -2700/+900 0, 1, 2, 3, 4 0.0
50 988.82503 30060-03-01-01 -1700/+1800 0, 1, 2, 3 0.0
51 725.87648 50035-01-02-00 -3000/+200 0, 2, 3, 4 0.5
51 726.71988c,p,t 50035-01-02-02 -1200/+2100 0, 1, 2, 3 0.5
51 728.77338c,p,t 50035-01-02-04 -4000/+2600 0, 1, 2, 3 0.5
51 814.34546c,p,t 50035-01-03-10 -2200/+1500 0, 2 0.5
52 484.41775c,p,t 70044-01-01-000 -4000/+2200 0, 2, 3 0.0
52 484.56684c 70044-01-01-00 -2400/+700 0, 2, 3 0.0
52 485.00672c,p,t 70044-01-01-02 -4000/+2600 0, 2, 3 0.0
52 537.22347 70025-01-01-00 -4000/+2400 0, 1, 2, 3 0.0
52 738.47686c,p,t 80048-01-01-04 -4000/+3200 0, 2, 3 0.0
52 738.74636c,p,t 80048-01-01-07 -4000/+2700 0, 1, 2, 3 0.0
52 820.56256c,p,t 80049-01-01-00 -1100/+2000 0, 2, 3, 4 0.0
52 893.05439 80105-11-01-00 -4000/+3000 0, 2, 3 0.0
53 205.19659c,p,t 70044-01-02-00 -1900/+1500 0, 2, 3 0.0
53 207.07579 90043-01-01-01 -4000/+3600 0, 2 2.5
53 207.21911c 90043-01-01-01 -4000/+1400 0, 2, 3 2.5
53 206.49150c,p,t 90043-01-01-020 -4000/+2800 0, 2, 3 2.5
53 206.63615c,p,t 90043-01-01-02 -4000/+1900 0, 2, 3 2.5
53 956.08413p,t 92031-01-01-000 -4000/+2200 0, 2, 4 13.8
53 956.22695p,t 92031-01-01-000 -2100/+1100 0, 1, 2 13.8
53 957.06785p,t 92031-01-01-010 -4000/+2000 0, 2, 3 13.8
53 957.20458p,t 92031-01-01-010 -1800/+1600 0, 2, 3 13.8
53 959.15478p,t 92031-01-02-000 -4000/+2900 1, 2 13.8
54 167.72354c,p,t 91017-01-01-000 -1900/+1100 1, 2 0.0
54 168.31443c,p,t 91017-01-02-03 -2000/+1600 2 0.0
54 168.75518c,p,t 91017-01-02-010 -4000/+2500 0, 2, 3 0.0
54 168.90229c,p,t 91017-01-02-010 -1900/+1600 0, 2 0.0
a Off-axis angle; b these values are rounded off to an integer times 100 s and may include gaps. c The spectra for these ObsIDs were used to generate average time-resolved spectra (cf., Fig. 4); p data were used to calculate average pre-burst power density spectrum (Fig. 6); t data were used to calculate average tail power density spectrum.

Source LaTeX | All tables | In the text

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