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Kinematic properties of the field elliptical NGC?7507

机译:椭圆椭圆场NGC?7507的运动学特性

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The dark matter (DM) halos of field elliptical galaxies have not been well-studied and their properties appear controversial in the literature. While some galaxies appear to be nearly devoid of DM, others show clear evidence of its presence. Furthermore, modified Newtonian dynamics (MOND), which has been found to have predictive power in the domain of disk galaxies, has not yet been investigated for isolated elliptical galaxies. We study the kinematics of the isolated elliptical NGC?7507, which has been claimed as a clear example of DM presence in early-type galaxies. We obtained major and minor axis long-slit spectroscopy of NGC?7507 using the Gemini South telescope and deep imaging in Kron-Cousins R and Washington C using the CTIO/MOSAIC camera. Mean velocities, velocity dispersion and higher order moments of the velocity distribution are measured out to ?~90′′. The galaxy, although almost circular, has significant rotation along the minor axis and a rapidly declining velocity dispersion along both axes. The velocity dispersion profile is modeled in the context of a spherical Jeans analysis. Models without DM provide an excellent representation of the data with a mass-to-light ratio (M/L) of 3.1 (R-band). The most massive Navarro-Frenk-White (NFW) halo the data allow has a virial mass of only 3.9-2.1+3.1×1011 M⊙, although the data are more consistent with models that have a slight radial anisotropy, which implies the galaxy has an even lower DM halo mass of 2.2-1.2+2.0×1011 M⊙. Modeling of the h4 Gauss-Hermite coefficient is inconclusive but seems to be consistent with mild radial anisotropy. A cored logarithmic DM halo with parameters r0?=?7 kpc and v0?=?100?km?s-1 can also reproduce the observed velocity dispersion profile. The MOND predictions overestimate the velocity dispersion. In conclusion, we cannot easily reproduce the previous findings of a predominance of DM in NGC?7507 within a simple spherical model. DM may be present, but only in conjunction with a strong radial anisotropy, for which there are some indications.
机译:野外椭圆星系的暗物质(DM)光晕尚未得到充分研究,其性质在文献中也引起争议。尽管有些星系似乎几乎不含DM,但另一些星系清楚地表明了它的存在。此外,还没有对孤立的椭圆星系研究改进的牛顿动力学(MOND),该改进的牛顿动力学在盘状星系领域具有预测能力。我们研究了孤立的椭圆形NGC?7507的运动学,该运动被认为是早期类型星系中DM存在的明显例子。我们使用Gemini South望远镜获得了NGC?7507的长轴和短轴长缝光谱,并使用CTIO / MOSAIC相机在Kron-Cousins R和Washington C中获得了深成像。测得的平均速度,速度弥散和速度分布的高阶矩约为90°。尽管银河系几乎是圆形的,但它沿短轴具有明显的自转,并且沿两个轴具有迅速下降的速度色散。速度色散曲线是在球形Jeans分析的背景下建模的。没有DM的模型以3.1(R波段)的质光比(M / L)很好地表示了数据。数据允许的最大质量的纳瓦罗·弗兰克·怀特(NFW)光晕的病毒质量只有3.9-2.1 + 3.1×1011M⊙,尽管该数据与具有轻微径向各向异性的模型更为一致,这暗示了星系具有甚至更低的DM晕质量为2.2-1.2 + 2.0×1011M⊙。 h4 Gauss-Hermite系数的模型尚无定论,但似乎与轻微的径向各向异性一致。参数为r0θ=?7 kpc和v0?=?100?km?s-1的有芯对数DM光晕也可以重现观察到的速度色散分布。 MOND预测高估了速度色散。总之,我们不能轻易地在简单的球形模型中重现NGC?7507中DM占优势的先前发现。可能存在DM,但仅与强烈的径向各向异性结合存在,对此有一些迹象。

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