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26 April 2024 |
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Identification of twenty-three accreting binaries in the Galactic Bulge Survey | | M.A.P. Torres
; P.G. Jonker
; C.T. Britt
; C.B. Johnson
; R.I. Hynes
; S. Greiss
; D. Steeghs
; T.J. Maccarone
; F. Ozel
; C. Bassa
; G. Nelemans
; | | Date: |
1 Oct 2013 | | Abstract: | (Abridged:) We present the identification of optical counterparts to 23
Galactic Bulge Survey X-ray sources. We report their accurate coordinates and
optical spectra acquired at the VLT and Magellan. All sources are classified as
accreting binaries according to their emission line characteristics. To
distinguish accreting binaries from chromospherically active objects we develop
and explain criteria based on Halpha and HeI 5786,6678 emission line properties
available in the literature. The spectroscopic properties and photometric
variability of all the objects are discussed and a classification of the source
is given where possible. Among the 23 systems, at least 9 of them show an
accretion-dominated optical spectrum (CX28, CX63, CX70, CX128, CX142, CX207,
CX522, CX794, CX1011) and another 6 show photospheric lines from a late-type
donor star in addition to accretion disc emission (CX44, CX93, CX137, CX154,
CX377 and CX1004) indicating that they are probably accreting binaries in
quiescence or in a low accretion rate state. Two sources are confirmed to be
eclipsing: CX207 and CX794. CX207 shows a broad asymmetric Halpha profile
blue-shifted by >300 km/s. Such line profile characteristics are consistent
with a magnetic (Polar) CV. CX794 is an eclipsing nova-like CV in the period
gap. Time-resolved photometry and the large broadening of the Halpha emission
lines in CX446 (2100 km/s FWHM) suggest that this is also an eclipsing or
high-inclination accreting binary. Finally, the low-accretion rate source
CX1004 shows a double-peaked Halpha profile with a FWHM of 2100 km/s. This
supports a high inclination or even eclipsing system. Whether the compact
object is a white dwarf in an eclipsing CV or a black hole primary in a
high-inclination LMXB remains to be established. | | Source: | arXiv, 1310.0224 | | Services: | Forum | Review | PDF | Favorites | |
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