The Bright X-Ray Source in NGC 3413

被引：0
作者：
Sonbas, E. [1 ,2 ]
Dhuga, K. S. [2 ]
Gogus, E. [3 ]
机构：
[1] Adiyaman Univ, Dept Phys, TR-02040 Adiyaman, Turkey
[2] George Washington Univ, Dept Phys, Washington, DC 20052 USA
[3] Sabanci Univ, TR-34956 Istanbul, Turkey
来源：
ASTROPHYSICAL JOURNAL | 2018年 / 865卷 / 02期
关键词：
galaxies: dwarf; methods: data analysis; stars: black holes; X-rays: binaries; BLACK-HOLE; ULTRALUMINOUS STATE; ACCRETION DISKS; GALAXIES; MASS; VARIABILITY; POPULATION; EMISSION;
D O I：
10.3847/1538-4357/aadba2
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
The emission-line dwarf galaxy NGC 3413 is known to host a bright X-ray source near its optical center. The 0.3-10 keV luminosity of this source is estimated to be approximately 10(39) erg s(-1), potentially qualifying it as an ultraluminous X-ray source (ULX). A recent X-ray Multi-Mirror Mission-Newton observation suggests that the source is not point-like, and instead is more likely a composite of point-like sources with extended and/or diffuse emission. The spectral and temporal features of the bright region are similar to those associated with the so-called broadened disk state of ULXs. Based on a multicolor blackbody spectral fit, we estimate the mass of the bright source to be in the range 3-20M(circle dot). Potential optical counterparts are also explored with the aid of available Sloan Digital Sky Survey and PanStars data.
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页数：6
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