论文标题
ERASST J040515.6-745202，麦哲伦桥的X射线泡
eRASSt J040515.6-745202, an X-ray burster in the Magellanic Bridge
论文作者
论文摘要
在第三次全套调查（ERASS3）期间，Erosita，Spectrum-Roentgen-Gamma上的软X射线仪器，在麦哲伦桥的方向上检测到了新的硬X射线瞬态，Erasst J040515.6-745202。我们安排了后续观察，并搜索了档案数据以揭示瞬态的性质。使用XMM-Newton，NoT和Swift的X射线观测，我们研究了源的时间和光谱行为，大约10天以上。从XMM-Newton观测中获得的X射线光曲线，暴露于28 kS，显示出I型X射线爆发，峰值侧冲亮度至少为1.4E37 ERG/s。爆发的能量与麦芽岩桥距离的伯斯特的位置一致。 70 s爆发的相对较长的指数衰减时间表明它在H丰富的环境中被点燃。在ERASS3之前的十二六个月和六个月之前，在其他EROSITA调查期间，源的未检测表明，在持续排放中达到2.6e36 ERG/s的中度爆发中发现了爆发。在更好的观察过程中，源显示出与XMM-Newton观察期间高水平的交替通量状态。这种行为可能是由于XMM-Newton观察的最后一个小时所见，可能是由下降引起的。 21.8小时的倾角复发的证据表明，ERASST J040515.6-745202是一种低质量X射线二元（LMXB）系统，其积聚盘几乎可以看到。我们在XMM-Newton上的光学/UV监视器和Cerro Tololo Intererican Intererican Intererican Perservatory上的光学/UV监视器获得的UVW1和G，R，I和Z图像中确定了与X射线源的多波长对应物。 （缩写）
During the third all-sky survey (eRASS3), eROSITA, the soft X-ray instrument aboard Spectrum-Roentgen-Gamma, detected a new hard X-ray transient, eRASSt J040515.6-745202, in the direction of the Magellanic Bridge. We arranged follow-up observations and searched for archival data to reveal the nature of the transient. Using X-ray observations with XMM-Newton, NICER, and Swift, we investigated the temporal and spectral behaviour of the source for over about 10 days. The X-ray light curve obtained from the XMM-Newton observation with an 28 ks exposure revealed a type-I X-ray burst with a peak bolometric luminosity of at least 1.4e37 erg/s. The burst energetics are consistent with a location of the burster at the distance of the Magellanic Bridge. The relatively long exponential decay time of the burst of 70 s indicates that it ignited in a H-rich environment. The non-detection of the source during the other eROSITA surveys, twelve and six months before and six months after eRASS3, suggests that the burst was discovered during a moderate outburst which reached 2.6e36 erg/s in persistent emission. During the NICER observations, the source showed alternating flux states with the high level at a similar brightness as during the XMM-Newton observation. This behaviour is likely caused by dips as also seen during the last hour of the XMM-Newton observation. Evidence for a recurrence of the dips with a period of 21.8 hr suggests eRASSt J040515.6-745202 is a low-mass X-ray binary (LMXB) system with an accretion disk seen nearly edge on. We identify a multi-wavelength counterpart to the X-ray source in UVW1 and g, r, i, and z images obtained by the optical/UV monitor on XMM-Newton and the Dark Energy Camera at the Cerro Tololo Inter-American Observatory. (abbreviated)
