论文标题
观察麦哲伦电晕
Observations of a Magellanic Corona
论文作者
论文摘要
大小的麦哲伦云（LMC/SMC）是银河系中最接近的主要卫星星系。他们很可能是在通向我们的星系的轨道上的第一次通道（Besla等，2007），并追踪本地群体的持续动态（D'Onghia＆Fox 2016）。 LMC高质量的最新测量（M_HALO = 10^（11.1-11.4）太阳能； Penarrubia等人2016，Erkal等人，2018年，2019年，Kallivayalil等人，Kallivayalil等人，2018年），暗示LMC应该是LMC的岩浆Corona：一个碰撞的温度，3. 3. 3. 3. 5. 3. gaseous not 5。 k）最初延伸到病毒半径（100-130 kpc）。这样的电晕本来会塑造麦哲伦流的形成（Lucchini etal。2020），这是一种潮汐气体结构，在天空中延伸了200度以上（D'Onghia＆Fox 2016，Besla等人，2012年，Nidever等人，2010年），它将金属贫气的可怜气体带到了乳Metal的含量（Fox etal。2014）。先前没有发表过有关这种扩展电晕的观察证据，其检测高度电离气体仅在直接向LMC方向上报告，其中来自LMC磁盘的风可能占主导地位（Deboer＆Savage 1980，Wakker等，1998）。在这里，我们在高度离子化的氧（O^+5）中展示了该麦芽岩电晕的证据，并通过三重离子化的碳和硅在高度离子化的氧气中有潜在的直接检测，在紫外线吸收中可见于朝着背景类星体的紫外线吸收中。 We find that the Magellanic Corona is part of a pervasive multiphase Magellanic circumgalactic medium (CGM) seen in many ionization states with a declining projected radial profile out to at least 35 kpc from the LMC and a total ionized CGM mass of log_10(M_HII;CGM/solar masses) = 9.1 +/- 0.2.麦哲伦电晕的证据是向麦哲伦群体及其与当地群体嵌套的进化来表征的至关重要的一步。
The Large and Small Magellanic Clouds (LMC/SMC) are the closest major satellite galaxies of the Milky Way. They are likely on their first passage on an infalling orbit towards our Galaxy (Besla et al. 2007) and trace the ongoing dynamics of the Local Group (D'Onghia & Fox 2016). Recent measurements of a high mass for the LMC (M_halo = 10^(11.1-11.4) solar masses; Penarrubia et al. 2016, Erkal et al. 2018, 2019, Kallivayalil et al. 2018) imply the LMC should host a Magellanic Corona: a collisionally ionized, warm-hot gaseous halo at the virial temperature (10^(5.3-5.5) K) initially extending out to the virial radius (100-130 kpc). Such a Corona would have shaped the formation of the Magellanic Stream (Lucchini et al. 2020), a tidal gas structure extending over 200 degrees across the sky (D'Onghia & Fox 2016, Besla et al. 2012, Nidever et al. 2010) that is bringing in metal poor gas to the Milky Way (Fox et al. 2014). No observational evidence for such an extended Corona has been published previously, with detections of highly ionized gas only reported in directions directly toward the LMC, where winds from the LMC disk may dominate (deBoer & Savage 1980, Wakker et al. 1998). Here we show evidence for this Magellanic Corona with a potential direct detection in highly ionized oxygen (O^+5), and indirectly via triply-ionized carbon and silicon, seen in ultraviolet absorption toward background quasars. We find that the Magellanic Corona is part of a pervasive multiphase Magellanic circumgalactic medium (CGM) seen in many ionization states with a declining projected radial profile out to at least 35 kpc from the LMC and a total ionized CGM mass of log_10(M_HII;CGM/solar masses) = 9.1 +/- 0.2. The evidence for the Magellanic Corona is a crucial step forward in characterizing the Magellanic Group and its nested evolution with the Local Group.
