Field and globular cluster low-mass X-ray binaries in NGC 4278

Fabbiano, G.; Brassington, N. J.; Lentati, L.; Angelini, L.; Davies, R. L.; Gallagher, J.; Kalogera, V.; Kim, D. W.; King, A. R.; Kundu, A.; Pellegrini, S.; Richings, A. J.; Trinchieri, G.; Zezas, A.; Zepf, S.

Abstract

We report a detailed spectral analysis of the population of low-massX-ray binaries (LMXBs) detected in the elliptical galaxy NGC 4278 with Chandra. Seven luminous sources were studied individually, four in globular clusters (GCs) and three in the stellar field. The range of (0.3-8 keV) LX for these sources is ∼(3-8) × 10^38 erg s^-1, suggesting that they may be black hole binaries (BHBs). Fitting the data with either single thermal accretion disk or power-law (PO) models results in best-fit temperatures of ∼0.7-1.7 keV and Λ ∼ 1.2-2.0, consistent with those measured in Galactic BHBs. Comparison of our results with simulations allows us to discriminate between disk and power-lawdominated emission, pointing to spectral/luminosity variability, reminiscent of Galactic BHBs. The BH masses derived from a comparison of our spectral results with the LX ≥ T in^4 relation of Galactic BHBs are in the 5-15M⊙ range, as observed in the Milky Way. The analysis of joint spectra of sources selected in three luminosity ranges (LX ≥ 1.5 × 10^38 erg s^-1, 6 × 10^37 erg s^-1 ≤ LX < 1.5 × 10^38 erg s^-1, and LX < 6 × 10^37 erg s^-1) suggests that while the high-luminosity sources have prominent thermal disk emission components, power-law components are likely to be important in the mid- and low-luminosity spectra. Comparing low-luminosity average spectra, we find a relatively larger NH in the GC spectrum; we speculate that this may point to either a metallicity effect or to intrinsic physical differences between field and GC accreting binaries. Analysis of average sample properties uncovers a previously unreported L X-RG correlation (where RG is the galactocentric radius) in the GC-LMXB sample, implying richer LMXB populations in more central GCs. No such trend is seen in the field LMXB sample. We can exclude that the GC LX-RG correlation is the by-product of a luminosity effect and suggest that it may be related to the presence of more compact GCs at smaller galactocentric radii, fostering more efficient binary formation. © 2010. The American Astronomical Society. All rights reserved.

Citation

Fabbiano, G., Brassington, N. J., Lentati, L., Angelini, L., Davies, R. L., Gallagher, J., Kalogera, V., Kim, D. W., King, A. R., Kundu, A., Pellegrini, S., Richings, A. J., Trinchieri, G., Zezas, A., & Zepf, S. (2010). Field and globular cluster low-mass X-ray binaries in NGC 4278. The Astrophysical journal, 725(2), 1824-1847. https://doi.org/10.1088/0004-637X/725/2/1824

• Journal Article Type: Article
• Acceptance Date: Oct 11, 2010
• Online Publication Date: Dec 2, 2010
• Publication Date: Dec 20, 2010
• Deposit Date: Aug 23, 2023
• Journal: Astrophysical Journal
• Print ISSN: 0004-637X
• Electronic ISSN: 1538-4357
• Publisher: American Astronomical Society
• Peer Reviewed: Peer Reviewed
• Volume: 725
• Issue: 2
• Pages: 1824-1847
• DOI: https://doi.org/10.1088/0004-637X/725/2/1824
• Keywords: Galaxies: individual (NGC 4278); X-rays: binaries; X-rays: galaxies
• Public URL: https://hull-repository.worktribe.com/output/4132581
• Publisher URL: https://iopscience.iop.org/article/10.1088/0004-637X/725/2/1824