The Galactic Bulge Survey: Outline and X-Ray Observations

Jonker, P. G.; Bassa, C. G.; Nelemans, G.; Steeghs, D.; Torres, M. A. P.; Maccarone, Thomas J.; Hynes, R. I.; Greiss, S.; Clem, James L.; Dieball, A.; Mikles, V. J.; Britt, C. T.; Gossen, L.; Collazzi, A. C.; Wijnands, Rudy; Zand, J. J. M. in ’t; Méndez, Mariano; Rea, N.; Kuulkers, E.; Ratti, E. M.; Haaften, L. M. van; Heinke, C. O.; Özel, Feryal; Groot, P.; Verbunt, F.

doi:10.1088/0067-0049/194/2/18

Cited by 74 publications

(106 citation statements)

References 74 publications

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“…Our XRT position of AX J1738.4-2902 is only 0.2 away from the ROSAT source 1RXS J173826.7-290140 (Sidoli et al 2001), which has an accurate Chandra localisation (Evans et al 2010;Jonker et al 2011) and is associated with the infrared object 2MASS J17382620-2901494. This object is classified as a pre-main sequence star of spectral type K0V (Skiff 2009).…”

Section: Ax J17384-2902 and Ax J18461-0239mentioning

confidence: 78%

Swiftfollow-up observations of unclassified ASCA sources

Degenaar

Starling

Evans

et al. 2012

A&A

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We present Swift follow-up observations of a sample of 35 unclassified faint X-ray sources drawn from the ASCA Galactic centre and Galactic plane surveys. Our short, pointed XRT observations allow detections down to a limiting 0.3-10 keV flux of F X ∼ 10 −13 erg cm −2 s −1 , which translates into a luminosity of L X ∼ 10 33 erg s −1 for an assumed distance of D = 8 kpc. The brightest source in our sample reaches a maximum 0.3-10 keV luminosity of L X ∼ 2 × 10 36 (D/8 kpc) 2 erg s −1 during our Swift observations. We detect 16 (46%) of the ASCA sources with the XRT, while 19 were not detected during our program. Since we are probing the faint end of the ASCA source populations, we expect a large fraction of the non-detections to be due to the Eddington bias. This is strengthened by the fact that we find the observed XRT count rates to be predominantly lower than expected based on the reported ASCA intensities. Nevertheless, investigation of the ASCA properties and any possible long-term X-ray variability leads us to conclude that the nondetections likely include two spurious ASCA detections and three objects that are highly variable or transient X-ray sources. For the 16 XRT-detected sources we obtain positional accuracies of ∼2−4 , which significantly improves upon their ASCA uncertainties of ∼1 . We use the X-ray spectra and variability to characterise these objects. Most appear to be faint, persistent X-ray emitters that have highly absorbed spectra. Based on their X-ray properties we identify three accreting compact objects: one confirmed (AX J1754.2-2754) and one candidate (AX J1538.3-5541) X-ray binary, and one possible magnetically accreting white dwarf (AX J1620.1-5002). Furthermore, we use the improved positions of XRT-detected sources to search for counterparts in simultaneously obtained Swift/UVOT images and possible associations with catalogued sources at various wavelengths. This reveals three possible main sequence stars amongst our sample. The other sources remain unclassified, but our improved XRT positions provide good prospects for dedicated follow-up observations that have the potential to elucidate the nature of these faint, unclassified ASCA sources.

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Section: Ax J17384-2902 and Ax J18461-0239mentioning

confidence: 78%

Swiftfollow-up observations of unclassified ASCA sources

Degenaar

Starling

Evans

et al. 2012

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“…For the LMXBs, the uncertanties for L br and α 1 might be reduced by factor of two if all detected LMXBs are identified. However, this is unlikely to be the case, as the source identification is a major challenge for low-luminosity LMXBs, which are easily confused with cataclysmic variables (Jonker et al 2011;Torres et al 2014).…”

Section: Resultsmentioning

confidence: 99%

Population of the Galactic X-ray binaries and eRosita

Doroshenko

Ducci

Santangelo

et al. 2014

A&A

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The population of the Galactic X-ray binaries has been mostly probed with moderately sensitive hard X-ray surveys so far. The eRosita mission will provide for the first time a sensitive all-sky X-ray survey in the 2−10 keV energy range, where the X-ray binaries emit most of the flux and discover the still unobserved low-luminosity population of these objects. In this paper, we briefly review the current constraints for the X-ray luminosity functions of high-and low-mass X-ray binaries and present our own analysis based the INTEGRAL 9-year Galactic survey, which yields improved constraints. Based on these results, we estimate the number of new XRBs to be detected in the eRosita all-sky survey.

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“…Furthermore, we adopt the total extinction in the V filter band from Nelemans et al (2004), which is based on Sandage's extinction law (Sandage 1972). We assume the Galactic scale height of the dust to be 120 pc (Jonker et al 2011). To evaluate the magnitude of extinction in the different bands of the ugrizphotometric system, we use the conversion of Schlegel et al (1998), which are based on the extinction laws of Cardelli et al (1989) and O'Donnell (1994) with R V = 3.1.…”

Section: Magnitudesmentioning

confidence: 99%

The effect of common-envelope evolution on the visible population of post-common-envelope binaries

Toonen

Nelemans

2013

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Context. An important ingredient in binary evolution is the common-envelope (CE) phase. Although this phase is believed to be responsible for the formation of many close binaries, the process is not well understood. Aims. We investigate the characteristics of the population of post-common-envelope binaries (PCEB). As the evolution of these binaries and their stellar components are relatively simple, this population can be directly used to constraint CE evolution. Methods. We use the binary population synthesis code SeBa to simulate the current-day population of PCEBs in the Galaxy. We incorporate the selection effects in our model that are inherent to the general PCEB population and that are specific to the SDSS survey, which enables a direct comparison for the first time between the synthetic and observed population of visible PCEBs. Results. We find that selection effects do not play a significant role on the period distribution of visible PCEBs. To explain the observed dearth of long-period systems, the α-CE efficiency of the main evolutionary channel must be low. In the main channel, the CE is initiated by a red giant as it fills its Roche lobe in a dynamically unstable way. Other evolutionary paths cannot be constrained more. Additionally our model reproduces well the observed space density, the fraction of visible PCEBs amongst white dwarf (WD)-main sequence (MS) binaries, and the WD mass versus MS mass distribution, but overestimates the fraction of PCEBs with helium WD companions.

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The Galactic Bulge Survey: Outline and X-Ray Observations

Cited by 74 publications

References 74 publications

Swiftfollow-up observations of unclassified ASCA sources

Swiftfollow-up observations of unclassified ASCA sources

Population of the Galactic X-ray binaries and eRosita

The effect of common-envelope evolution on the visible population of post-common-envelope binaries

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