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首页> 外文期刊>The Astrophysical journal >Low-mass X-ray Binaries And Globular Clusters In Early-type Galaxies. I. Chandra Observations
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Low-mass X-ray Binaries And Globular Clusters In Early-type Galaxies. I. Chandra Observations

机译：早期型星系中的低质量X射线双星和球状星团。 I.钱德拉的观察

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We present a Chandra survey of LMXBs in 24 early-type galaxies. Correcting for detection incompleteness, the X-ray luminosity function (XLF) of each galaxy is consistent with a power law with negative logarithmic differential slope, β～2.0. However, β strongly correlates with incompleteness, indicating the XLF flattens at low-Z x. The composite XLF is well fitted by apower law withabreak at (2.21_(-0.56)~(+0.65))×10~(38) ergs s~(-1) and β = 1.40_(-0.13)~(+0.10) and 2.84_(-0.30)~(+0.39) below and above it, respectively. The break is close to the Eddington limit for a 1.4 M_☉ neutron star, but the XLF shape rules out its representing the division between neutron star and black hole systems. Although the XLFs are similar, we find evidence of some variation between galaxies. The high-L_X XLF slope does not correlate with age, but may correlate with [α/Fe]. Considering only LMXBs with L_X > 10~(37) ergs s~(-1), matching the LMXBs with globular clusters (GCs) identified in HST observations of 19 of the galaxies, we find the probability a GC hosts an LMXB is proportional to L_(GC)~α where α = 1.01 ± 0.19 and 7 = 0.33 ±0.11. Correcting for GC luminosity and color effects, and detection incompleteness, we find no evidence that the fraction of LMXBs with L_X > 10~(37) ergs s~(-1) in GCs (40%), or the fraction of GCs hosting LMXBs (～6.5%) varies between galaxies. The spatial distribution of LMXBs resembles that of GCs, and the specific frequency of LMXBs is proportional to the GC specific luminosity, consistent with the hypothesis that all LMXBs form in GCs. If the LMXB lifetime is Τ_L, and the duty cycle is F_d, our results imply ～1.5(Τ_L/10~8 yr)~(-1)F_d~(-1) LMXBs are formed per gigayear per GC, and we place an upper limit of one active LMXB in the field per 3.4×10~9 L_☉ of V-band luminosity.
机译：我们提出了一项Chandra对24个早期类型星系中LMXB的调查。校正检测不完备性后，每个星系的X射线光度函数（XLF）均与对数微分斜率为β〜2.0为负的幂律一致。但是，β与不完全性密切相关，表明XLF在低Z x时变平。复合XLF通过幂定律很好地拟合，在（2.21 _（-0.56）〜（+0.65））×10〜（38）ers s〜（-1）且β= 1.40 _（-0.13）〜（+0.10） ）和下方和上方的2.84 _（-0.30）〜（+0.39）。该断裂接近1.4M_☉中子星的爱丁顿极限，但XLF形状排除了它代表中子星与黑洞系统之间的距离的可能性。尽管XLF相似，但我们发现了星系之间某些差异的证据。 L_X XLF的高斜率与年龄无关，但可能与[α/ Fe]相关。仅考虑L_X> 10〜（37）erg s〜（-1）的LMXB，将LMXB与在19个星系的HST观测中确定的球状星团（GC）匹配，我们发现GC承载LMXB的概率与L_（GC）〜α其中α= 1.01±0.19和7 = 0.33±0.11。校正GC的光度和颜色效果以及检测不完整性，我们没有发现证据表明L_X> 10〜（37）ers s〜（-1）的LMXB在GC中所占的比例（40％），或承载LMXB的GC中所占的比例（〜6.5％）在星系之间变化。 LMXB的空间分布类似于GC，并且LMXB的比频率与GC的特定光度成正比，这与所有LMXB在GC中形成的假设相一致。如果LMXB的寿命为Τ_L，占空比为F_d，则我们的结果表明，每GC的每千兆年形成〜1.5（Τ_L/ 10〜8 yr）〜（-1）F_d〜（-1）个LMXB，我们将每个V波段光度的3.4×10〜9 L_ one范围内一个活动LMXB的上限。

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