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首页> 外文期刊>The Astrophysical journal >MULTIWAVELENGTH MONITORING OF THE DWARF SEYFERT 1 GALAXY NGC 4395. Ⅰ. A REVERBERATION-BASED MEASUREMENT OF THE BLACK HOLE MASS
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MULTIWAVELENGTH MONITORING OF THE DWARF SEYFERT 1 GALAXY NGC 4395. Ⅰ. A REVERBERATION-BASED MEASUREMENT OF THE BLACK HOLE MASS

机译：DWARF SEYFERT 1 GALAXY NGC 4395的多波长监测。基于孔率的黑洞质量测量

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摘要

A reverberation-mapping program on NGC 4395, the least luminous known Seyfert 1 galaxy, undertaken with the Space Telescope Imaging Spectrograph on the Hubble Space Telescope yields a measurement of the mass of the central black hole M_(BH) = (3.6 ± 1.1) x 10~5 solar mass. The observations consist of two visits of five orbits each, in 2004 April and July. During each of these visits, the UV continuum varied by at least 10% (rms), and only C IV λ1549 showed corresponding variations large enough to reliably determine the emission-line lag, which was measured to be of order 1 hr for both visits. The size of the C IV-emitting region is about a factor of 3 smaller than expected if the slope of the broad-line region radius-luminosity relationship is identical to that for the Hβ emission line. NGC 4395 is under-luminous even for its small black hole mass; the Eddington ratio of ～ 1.2 x 10~(-3) is lower than that of any other active galactic nucleus for which a black hole mass measurement has been made by emission-line reverberation.
机译：在哈勃太空望远镜上使用太空望远镜成像光谱仪在NGC 4395（最小发光的塞舌尔1星系）上进行的混响映射程序产生了中心黑洞质量的测量值M_（BH）=（3.6±1.1） x 10〜5太阳质量观测包括2004年4月和7月的两次访问，每次访问有五个轨道。在每次访问中，UV连续性变化至少10％（rms），并且只有C IVλ1549显示出足够大的相应变化，才能可靠地确定发射线延迟，两次访问的测量值约为1小时。如果宽线区域的半径-光度关系的斜率与Hβ发射线的斜率相同，则C IV发射区的大小大约比预期小3倍。 NGC 4395即使是较小的黑洞质量也不会发光。 〜1.2 x 10〜（-3）的爱丁顿比率低于通过发射线混响测量黑洞质量的任何其他活动银河核的比率。

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