Delta Sco
Periastron
campaign 2011
July 22, 2011 update
The periastron time is predicted for the first days of July 2011 (July 6, +/-2). High quality spectroscopic radial velocity (RV) observations are very encouraged during 2011 year - see Anatoly Miroshnichenko webpage's: http://www.uncg.edu/~a_mirosh/Delta_Sco/. Amateur spectroscopic RV data can substantially improve the uncertainties of the predicted date of the periastron, but high precision is required, better then 10 km/s. The radial velocity expected variation is about 40 km/s during a period of +/-1 month relative to the date of periastron.
Example of usefull amateur instruments for the campaign are Lhires III (2400 l/mm configuration - typical resolution power of R=15000) and echelle spectrographe eShel (precise ThorAr spectral calibration, R=11000). Extensive information and recommendations about spectroscopic observations of Delta Sco are given in Anatoly Miroshnichenko's pages. See also http://www.stsci.de/convento/pdf/deltaSco2011.pdf (ConVento group page).The periastron passage can also produce high interaction between the secondary and the circumstellar matter of the primary, so a Ha morphologie spectral profile survey is also welcome.
The present page is a compilation of amateur Delta Scopii spectra specially dedicated to the present 2011 periastron campaign. The data are available to professional community for anaysis and publications. See also the Be stars database BeSS for an enlarged compilation (pro/am) of Delta Sco spectra (many years of observation), and remember to submit your spectra to BeSS.
About recent Delta Scorpii orbit and periastron time prediction see the reference (C. Tycner & all paper): http://arxiv.org/abs/1101.5152
LOG OF OBSERVATIONS
# |
Date (DD/MM/YYYY) |
Observer |
Instrument |
Exposure |
Resolution |
Range (nm) |
fits files Heliocentric velocity not corrected |
dat files Heliocentric velocity corrected |
Notes |
1 |
10.245/01/2011 |
C. Buil |
C11 + eShel |
11 x 300 s |
11000 |
430-710 |
1 |
||
2 |
20.232/01/2011 |
C. Buil |
C11 + eShel |
9 x 300 s |
11000 |
430-710 |
1 |
||
3 |
23.225/01/2011 |
C. Buil |
C11 + eShel |
12 x 300 s |
11000 |
430-710 |
1 | ||
4 |
9.209/02/2011 |
C. Buil |
C11 + eShel |
17 x 180 s |
11000 |
430-710
|
1 |
||
5 |
6.196/03/2011 |
C. Buil |
C11 + eShel |
17 x 180 s |
11000 |
430-710 |
1 |
||
6 |
25.100/03/2011 |
C. Buil |
C11 + eShel |
16 x 300 s |
11000 |
430-710 |
1 |
||
7 |
16.050/04/2011 |
C. Buil |
C11 + eShel |
11 x 300 s |
11000 |
430-710 |
1 |
||
8 |
16.080/04/2011 |
J. Ribeiro |
C14 + Lhires III (2400) |
3740 s |
16000 |
458 - 483 |
1 |
||
9 |
28.059/04/2011 |
C. Buil |
C11 + eShel |
15 x 180 s |
11000 |
430-710 |
1 |
||
10 |
3.991/05/2011 |
C. Buil |
C11 + eShel |
15 x 180 s |
11000 |
430-710 |
1 |
||
11 |
11.011/05/2011 |
C. Buil |
C11 + eShel |
10 x 300 s |
11000 |
430-710 |
1 |
||
12 |
22.925/05/2011 |
C. Buil |
C11 + eShel |
7 x 300 s |
11000 |
430-710 |
1 |
||
13 |
28.048/05/2011 |
C. Buil |
C11 + eShel |
7 x 300 s |
11000 |
430-710 |
1 |
||
14 |
28.878/05/2011 |
C. Buil |
C11 + eShel |
9 x 300 s |
11000 |
430-710 |
1 |
||
15 |
13.960/06/2011 |
C. Buil |
C11 + Lhires III (2400) |
6 x 180 s |
10000 |
458-473 |
1 |
||
16 |
14.919/06/2011 |
C. Buil |
C11 + eShel |
11 x 180 s |
11000 |
430-710 |
1 |
||
17 |
15.931/06/2011 |
C. Buil |
C11 + eShel |
13 x 180 s |
11000 |
430-710 |
1 |
||
18 |
18.896/06/2011 |
C. Buil |
C11 + eShel |
8 x 180 s |
11000 |
430-710 |
1 |
||
19 |
26.859/06/2011 |
C. Buil |
C11 + eShel |
7 x 240 s |
11000 |
430-710 |
1 |
||
20 |
1.874/07/2011 |
C. Buil |
C11 + eShel |
10 x 240 s |
11000 |
430-710 |
1 |
||
21 |
2.976/07/2011 |
C. Buil |
C11 + eShel |
10 x 240 s |
11000 |
430-710 |
1 |
||
22 |
4.858/07/2011 |
C. Buil |
C11 + eShel |
8 x 240 s |
11000 |
430-710 |
1 |
||
23 |
5.949/07/2011 |
C. Buil |
C11 + eShel |
8 x 240 s |
11000 |
430-710 |
1 |
||
24 |
8.850/07/2011 |
C. Buil |
C11 + eShel |
16 x 150 s |
11000 |
430-710 |
1 |
||
25 |
9.854/07/2011 |
C. Buil |
C11 + eShel |
16 x 180 s |
11000 |
430-710 |
1 |
||
26 |
10.856/07/2011 |
C. Buil |
C11 + eShel |
7 x 180 s |
11000 |
430-710 |
1 |
||
27 |
10.893/07/2011 |
C. Buil |
C11 + eShel |
8 x 180 s |
11000 |
430-710 |
1 |
||
28 |
11.848/07/2011 |
C. Buil |
C11 + eShel |
16 x 240 s |
11000 |
430-710 |
1 |
||
29 |
17.870/07/2011 |
C. Buil |
C11 + eShel |
11 x 240 s |
11000 |
430-710 |
1 |
||
30 |
20.859/07/2011 |
C. Buil |
C11 + eShel |
16 x 180 s |
11000 |
430-710 |
1 |
||
31 |
21.923/07/2011 |
C. Buil |
C11 + eShel |
10 x 180 s |
11000 |
430-710 |
1 |
Note: For the .dat spectra, the telluric lines are removed and heliocentric velocity is corrected.
# |
JD0 - 2450000 |
Rectified continuum (He II region) |
Relative radial velocity |
Relative radial velocity |
Absolute radial
velocity based on 4686 A line |
Reference |
5585.000 |
|
|
-11.46 km/s |
|
1 |
5571.741 |
-4.0 |
-5.6 |
-16.26 km/s |
|
2 |
5581.729 |
+0.0 |
-0.6 |
-12.06 km/s |
|
3 |
5584.722 |
+2.0 |
+2.0 |
-11.76 km/s |
|
4 |
5601.708 |
+2.0 |
+0.2 |
-10.36 km/s |
|
5 |
5626.697 |
-5.0 |
-5.1 |
-16.51 km/s |
|
6 |
5645.603 |
-4.0 |
-3.6 |
-15.26 km/s |
|
7 |
5667.555 |
+2.0 |
+2.8 |
-9.06 km/s |
|
8 |
5667.667 |
+3.0 |
+5.6 |
-7.16 km/s |
|
9 |
5679.564 |
-10.0 |
-9.9 |
-21.41 km/s |
|
10 |
5685.496 |
+0.0 |
+0.1 |
-11.41 km/s |
|
11 |
5692.517 |
-5.0 |
+1.0 |
-13.46 km /s |
|
12 |
5704.431 |
-7.0 |
-6.1 |
-18.01 km/s |
|
13 |
5709.554 |
-9.0 |
-8.1 |
-20.01 km/s |
|
14 |
5710.383 |
-10.0 |
-7.9 |
-20.41 km/s |
|
15 |
5726.465 |
-13.0 |
-10.7 |
-23.31 km/s |
|
16 |
5727.424 |
-16.0 |
-12.9 |
-25.91 km/s |
|
17 |
5728.436 |
-17.0 |
-14.7 |
-27.31 km/s |
|
18 |
5731.401 |
-31.0 |
-29.3 |
-41.61 km/s |
|
19 |
5739.364 |
-28.0 |
-28.2 |
-39.56 km/s |
|
20 |
5744.379 |
-35.0 |
-37.1 |
-47.51 km/s |
|
21 |
5745.481 |
-35.0 |
-37.7 |
-47.81 km/s |
|
22 |
5747.362 |
-36.0 |
-34.6 |
-46.76 km/s |
|
23 |
5748.453 |
-37.0 |
-37.1 |
-48.51 km/s |
|
24 |
5751.354 |
-22.0 |
-22.5 |
-33.71 km/s |
|
25 |
5752.358 |
-25.0 |
-28.9 |
-38.41 km/s |
|
26 |
5753.360 |
-32.0 |
-35.9 |
-45.42 km/s |
|
27 |
5753.397 |
-38.0 |
-21.6 |
-41.26 km/s |
|
28 |
5754.352 |
-32.0 |
-31.2 |
-43.01 km/s |
|
29 |
5760.373 |
-23.0 |
-23.0 |
-34.46 km/s |
|
30 |
5763.363 |
-14.0 |
-12.2 |
-24.56 km/s |
|
31 |
5764.426 |
-16.0 |
-11.5 |
-25.22 km/s |
Note: The reference spectrum is
the mean of #1, #2, #3 and #4 individual spectra. Radial velocity is measured
relative to the reference spectrum.
The gaussien fit center of 4686 A line
on reference spectrum give position 4685.503 A (RV=-11.460 km/s relative
to admited rest wavelength of 4685.682 A).
2011 STATUS
Time
evolution of HeII 4686 A line - Shift of 0.05 intensity unit is applied for
clarity.
Time
evolution of Ha -
Shift of 0.3 intensity unit is applied for clarity.
Dynamic
Halpha line evolution.
Radial
velocity (HeII 4686 A reference). Typical measure error is +/- 3 km/s (1-sigma) - Positive radial: object move toward observer.
SUMMARY OF 2010 ACTIVITY
C11 telescope (D = 0.28 m) + eShel spectrographe (echelle R = 11000) - C. Buil - Castanet-Tolosan observatory.
Typical
high resolution Ha
profile at R = 25600 (date 05/07/2010). No correction by heliocentricity or waterlines.
By Lothar Shanne.
LINES IDENTIFICATION
C11 telescope (D = 0.28 m) + eShel spectrographe (echelle R = 11000) - C. Buil - Castanet-Tolosan observatory. Note: Orbital radial velocity measure from Ha profile is not easy because the high sensibility to circumstellar activity. He I lines are also variables because part of them form in a region above the photosphere, near the inner boundary of the disk. Therefore, they are affected by the densest circumstellar matter that is reflected in their changing radial velocities. A. Miroshnichenko suggest use of He II for good RV measurements. These lines form in the photosphere and are not affected by circumstellar medium. There are only two He II in the optical spectrum of Delta Sco at 4686 A (see below) and at 5411 A (very weak). |
The He II l4686 A line position time stability.
Conditions for use of data in
publications
Note
there is no precise validation check prior to adding spectra to this table.
Users should verify the quality of the spectra with the observers
concerned.
Use of these data in research publications is encouraged subject to the
following conditions: The observers concerned should be contacted
to confirm the particular acquisition and data reduction procedures
used.