J/A+A/590/A122 Spectra of high-mass X-ray binaries (Reig+, 2016)
Long-term optical variability of high-mass X-ray binaries
II. Spectroscopy.
Reig P., Nersesian A., Zezas A., Gkouvelis L., Coe M.J.
<Astron. Astrophys. 590, A122 (2016)>
=2016A&A...590A.122R 2016A&A...590A.122R (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, X-ray ; Spectroscopy
Keywords: stars: emission-line, Be - stars: massive - X-rays: binaries
Abstract:
High-mass X-ray binaries are bright X-ray sources. The high-energy
emission is caused by the accretion of matter from the massive
companion onto a neutron star. The accreting material comes from
either the strong stellar wind in binaries with supergiant companions
or the circumstellar disk in Be/X-ray binaries. In either case, the
Hα line stands out as the main source of information about the
state of the accreting material.
We present the results of our monitoring program to study the
long-term variability of the Hα line in high-mass X-ray
binaries. Our aim is to characterise the optical variability
timescales and study the interaction between the neutron star and the
accreting material.
We fitted the Hα line with Gaussian profiles and obtained the
line parameters and equivalent width. The peak separation in split
profiles was used to determine the disk velocity law and estimate the
disk radius. The relative intensity of the two peaks (V/R ratio)
allowed us to investigate the distribution of gas particles in the
disk. The equivalent width was used to characterise the degree of
variability of the systems. We also studied the variability of the
Hα line in correlation with the X-ray activity.
Description:
We have been monitoring the Hα line of HMXBs visible from the
northern hemisphere using the 1.3m telescope of the Skinakas
Observatory (SKO) located in the island of Crete (Greece) since 1999.
The targets have also been observed regularly using the 1.5m
telescope of the Fred Lawrence Whipple Observatory (FLWO) at Mt.
Hopkins (Arizona) since 2007.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 130 20 Targets and relevant information
list.dat 53 132 List of spectra
sp/* . 132 Individual fits spectra
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1 A1 --- Spec [*] indicates available spectra
3- 18 A16 --- Name X-ray name
20- 27 A8 -- SpType MK Spectral type
29- 32 F4.1 Msun M Mass (1)
36- 39 F4.1 Rsun Rad Radius (1)
41- 46 F6.2 d Porb ?=- Orbital period
47 A1 --- n_Porb [?*] Note on Porb (3)
50- 53 F4.2 --- e ?=- Ellipticity
55- 58 F4.2 mag E(B-V) Redenning (2)
60- 63 F4.2 mag e_E(B-V) rms uncertainty on E(B-V)
65- 68 F4.1 kpc Dist Distance (2)
70- 72 F3.1 kpc e_Dist rms uncertainty on Dist
74- 76 A3 --- Dloss [yes/no ] Disk loss ?
78-130 A53 --- Ref References for Porb and e
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Note (1): B star masses from Porter (1996MNRAS.280L..31P 1996MNRAS.280L..31P) and O star masses
from Martins et al. (2005A&A...436.1049M 2005A&A...436.1049M),
except for 2S 0114+65 (Reig et al. 1996A&A...311..879R 1996A&A...311..879R).
Note (2): From Reig & Fabregat (2015, Cat. J/A+A/574/A33),
except for X Per (Roche et al. 1997A&A...322..139R 1997A&A...322..139R).
Note (3): *: Based on the time interval between a small number of type I
outbursts and hence uncertain.
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Name X-ray name
18- 27 A10 "date" Obs.Date Observation date
29- 53 A25 --- FileName Filename of spectrum fits file,
in subdirectory sp
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Acknowledgements:
Pablo Reig, pau(at)physics.uoc.gr
(End) Patricia Vannier [CDS] 07-Jun-2016