Search with UVES and X-Shooter for signatures of the low-mass secondary in the post common-envelope binary AA Doradus

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Volume 578 (June 2015)

A&A, 578 (2015) A125

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Issue		A&A Volume 578, June 2015


Article Number		A125
Number of page(s)		26
Section		Stellar atmospheres
DOI		https://doi.org/10.1051/0004-6361/201526229
Published online		16 June 2015

Online material

	Fig. 2 UVES spectrum (blue, start time 2001-01-08T00-27-37.434 UT). Identified lines of the primary are marked. ISM denotes interstellar lines.
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	Fig. 3 X-Shooter spectrum (blue, start time 2014-01-08T02-03-37.877 UT) taken in the UVB arm compared with our final model of the primary (red). Identified lines of the primary are marked. ISM denotes interstellar lines.
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	Fig. 4 X-Shooter spectrum (blue, start time 2014-01-08T02-03-43.068 UT) taken in the VIS arm compared with our final model of the primary (red). Identified lines of the primary are marked.
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	Fig. 5 X-Shooter spectrum (blue, start time 2014-01-08T02-03-45.7348) UT) taken in the NIR arm compared with our final model of the primary (red). Identified lines of the primary are marked.
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	Fig. 9 Detection limit for s-curves. A synthetic line profile (phase-dependently shifted with K_sec = 230 km s^-1) at three strengths (equivalent widths of W_λ = 122,15,and 3 mÅ, from left to right) is shown for S/N = 50, 25 (approximately our UVES data value), and 10 (top to bottom). All panels show the same wavelength and phase intervals.
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Appendix A: TLISA

As a part of the Tübingen contribution to the GAVO project, the TLISA tool is generally designed in VO-compliant form. In particular, its menu navigation is fully intuitive, i.e., no profound knowledge of the background software by a VO user is necessary for an astronomically worthwhile usage. The TLISA tool is provided as a registered GAVO tool.

The TLISA tool is a module-based analyzer (like a Content-Management-System for websites), written in the programming language Java, which allows the user to develop a lot of modules and tools to analyze and modify spectra. For this purpose, the program provides many methods and classes (like a data container for FITS files).

The first module, which was developed for TLISA, is SEFOBS (SEarch for Faint Objects in Binary Systems). The module is divided into three parts. The data provider and the data analyzers for the primary and the secondary. The data provider allows the user to choose data and save path. The data can be a single FITS file, several FITS files or a directory, but can only contain files of the same object and the same wavelength interval.

The SEFOBS reads the data and saves it into the internally used variables. It arranges the data by its observation time and indicates the most important information.

In the second part, the user has the option to either calculate the system parameters of the primary by SEFOBS or to enter individual parameters (Fig. A.1).

The analyzer windows (Figs. A.2, A.3) are divided into two panels. The left panel with the spectrum and the right panel with the s-curve plot.

The s-curve plot has a width of 500 pixels. Every other pixel is a data point, i.e., we have 250 data points. With a wavelength step of 0.2 Å, we cover an interval of 50 Å. Thus, the spectrum is divided into 50 Å-wide intervals. With the two buttons at the bottom on the right panel and also with the input field, the user can navigate through the spectrum.

With the slider at the right panel, the user can choose an individual spectrum at a specific observation time. It is not possible to switch between MJD and phase because SEFOBS needs the system parameters to calculate the phase from MJD.

The SEFOBS assigns each flux value an equivalent color value. The SEFOBS contains a lot more options to manipulate the s-curve plot. The first option is the selection of the background color, that is given every other pixel. This is very important because it is a graphical analysis where we need high contrast between background and spectrum. For example, the wings of an absorption line have a higher flux value compared to the line core. A higher flux value means a brighter color (default: from black to white), i.e., the line core is black and the line wings may be very diffuse. A black background will therefore sharpen the line. Vice versa, this works for an emission line.

	Fig. A.1 TLISA. SEFOBS input window.
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	Fig. A.2 TLISA. SEFOBS analyzer window for the primary.
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	Fig. A.3 TLISA. SEFOBS analyzer window for the secondary.
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Appendix B: TLISA s-curve plots and secondary spectra from UVES data

	Fig. B.1 Same as Fig. 10, for 3870 Å ≤ λ ≤ 3910 Å.
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	Fig. B.2 Same as Fig. 10, for 3900 Å ≤ λ ≤ 3940 Å.
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	Fig. B.3 Same as Fig. 10, for 3935 Å ≤ λ ≤ 3975 Å.
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	Fig. B.4 Same as Fig. 10, for 3950 Å ≤ λ ≤ 3990 Å.
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	Fig. B.5 Same as Fig. 10, for 4080 Å ≤ λ ≤ 4120 Å.
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	Fig. B.6 Same as Fig. 10, for 4105 Å ≤ λ ≤ 4145 Å.
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	Fig. B.7 Same as Fig. 10, for 4165 Å ≤ λ ≤ 4205 Å.
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	Fig. B.8 Same as Fig. 10, for 4295 Å ≤ λ ≤ 4335 Å.
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	Fig. B.9 Same as Fig. 10, for 4320 Å ≤ λ ≤ 4360 Å.
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	Fig. B.10 Same as Fig. 10, for 4395 Å ≤ λ ≤ 4435 Å.
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	Fig. B.11 Same as Fig. 10, for 4580 Å ≤ λ ≤ 4620 Å.
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	Fig. B.12 Same as Fig. 10, for 4625 Å ≤ λ ≤ 4665 Å.
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	Fig. B.13 Same as Fig. 10, for 4650 Å ≤ λ ≤ 4690 Å.
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	Fig. B.14 Same as Fig. 10, for 4680 Å ≤ λ ≤ 4720 Å.
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	Fig. B.15 Same as Fig. 10, for 4840 Å ≤ λ ≤ 4880 Å.
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Appendix C: TLISA s-curve plots and secondary spectra from X-Shooter UVB data

	Fig. C.1 Top: section of the phase-dependent X-Shooter UVB spectra (3780 Å ≤ λ ≤ 3820 Å). Bottom: is the spectrum taken at 2014-01-08T06-56-55.408 UT , the average of all spectra in the secondary’s rest frame in the respective wavelength interval.
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	Fig. C.2 Same as Fig. C.1, for 3815 Å ≤ λ ≤ 3855 Å.
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	Fig. C.3 Same as Fig. C.1, for 3870 Å ≤ λ ≤ 3910 Å.
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	Fig. C.4 Same as Fig. C.1, for 3900 Å ≤ λ ≤ 3940 Å.
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	Fig. C.5 Same as Fig. C.1, for 3950 Å ≤ λ ≤ 3990 Å.
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	Fig. C.6 Same as Fig. C.1, for 4010 Å ≤ λ ≤ 4050 Å.
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	Fig. C.7 Same as Fig. C.1, for 4050 Å ≤ λ ≤ 4090 Å.
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	Fig. C.8 Same as Fig. C.1, for 4080 Å ≤ λ ≤ 4120 Å.
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	Fig. C.9 Same as Fig. C.1, for 4130 Å ≤ λ ≤ 4170 Å.
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	Fig. C.10 Same as Fig. C.1, for 4245 Å ≤ λ ≤ 4285 Å.
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	Fig. C.11 Same as Fig. C.1, for 4300 Å ≤ λ ≤ 4340 Å.
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	Fig. C.12 Same as Fig. C.1, for 4320 Å ≤ λ ≤ 4360 Å.
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	Fig. C.13 Same as Fig. C.1, for 4395 Å ≤ λ ≤ 4435 Å.
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	Fig. C.14 Same as Fig. C.1, for 4580 Å ≤ λ ≤ 4620 Å.
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	Fig. C.15 Same as Fig. C.1, for 4625 Å ≤ λ ≤ 4665 Å.
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	Fig. C.16 Same as Fig. C.1, for 4840 Å ≤ λ ≤ 4880 Å. Bottom spectrum taken at 2014-01-08T07-00-19.465 UT.
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	Fig. C.17 Same as Fig. C.1, for 4905 Å ≤ λ ≤ 4945 Å.
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	Fig. C.18 Same as Fig. C.1, for 4920 Å ≤ λ ≤ 4960 Å.
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Appendix D: TLISA s-curve plots and secondary spectra from X-Shooter VIS data

	Fig. D.1 Top: section of the phase-dependent X-Shooter VIS spectra (5855 Å ≤ λ ≤ 5895 Å). Bottom: is the spectrum taken at 2014-01-08T06-57-01.888 UT − the average of all spectra in the secondary’s rest frame in the respective wavelength interval.
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	Fig. D.2 Same as Fig. D.1, for 6130 Å ≤ λ ≤ 6170 Å.
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	Fig. D.3 Same as Fig. D.1, for 6545 Å ≤ λ ≤ 6585 Å.
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	Fig. D.4 Same as Fig. D.1, for 6560 Å ≤ λ ≤ 6600 Å.
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	Fig. D.5 Same as Fig. D.1, for 6770 Å ≤ λ ≤ 6810 Å.
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	Fig. D.6 Same as Fig. D.1, for 7045 Å ≤ λ ≤ 7085 Å.
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	Fig. D.7 Same as Fig. D.1, for 8540 Å ≤ λ ≤ 8580 Å.
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Appendix E: TLISA s-curve plots and secondary spectra from X-Shooter NIR data

	Fig. E.1 Top: section of the phase-dependent X-Shooter VIS spectra (17590 Å ≤ λ ≤ 17710 Å). Bottom: is the spectrum taken at 2014-01-08T06:57:05.083 UT − the average of all spectra in the secondary’s rest frame in the respective wavelength interval.
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© ESO, 2015

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