根据SPIRITS巡天的明亮河外红外瞬变和变星的哈勃空间望远镜成像
Hubble Space Telescope Imaging of Luminous Extragalactic Infrared Transients and Variables from the SPIRITS Survey
摘要：
SPIRITS-斯皮策红色密集瞬变调查-从2014年到2019年，使用温暖的斯皮策望远镜在3.6和4.5微米处搜索近200个附近星系的发光红外（IR）瞬变和变量。在SPIRITS变量中，有一些红外明亮的物体在地面光学测量中无法检测到。我们将它们分为（1）瞬变，（2）周期性变量和（3）不规则变量。瞬变现象包括“SPRITE“（特别是红色的中等亮度瞬变事件），其最大亮度比超新星微弱，红色的红外颜色，以及广泛的爆发持续时间（几天到几年）。在这里，我们报告深光学和近红外成像与哈勃太空望远镜（HST）的21个SPIRITS变量。它们最初被认为是SPRITE瞬变，但随着更多数据的收集，许多最终被证明是周期性或不规则的变量。哈勃望远镜的图像显示，大多数这些冷而尘埃的变星都与晚型星系中的恒星形成区有关，这意味着它们起源于大质量恒星。两个SPRITE在爆发前的HST图像中缺乏光学祖细胞;然而，在J和H的爆发期间检测到一个，表明有效温度为~1050 K的尘埃物体。一颗微弱的SPRITE被证明是一颗尘埃弥漫的经典新星。大约一半的HST目标被证明是周期变星，脉动周期为670-2160天;它们可能是质量约为5-10 Msun的尘埃渐近巨星分支（AGB）恒星。其中一些足够温暖，可以在深度HST帧中检测到，但大多数都太冷了。在六颗不规则变星中，有两颗是红超巨星，在HST的影像中有光学对应物;有四颗因为太过遮蔽而无法被HST侦测到。
英文摘要：
SPIRITS--the SPitzer InfraRed Intensive Transients Survey--searched for luminous infrared (IR) transients and variables in nearly 200 nearby galaxies from 2014 to 2019, using the warm Spitzer telescope at 3.6 and 4.5 microns. Among the SPIRITS variables are IR-bright objects that are undetected in ground-based optical surveys. We classify them as (1) transients, (2) periodic variables, and (3) irregular variables. The transients include "SPRITE"s (eSPecially Red Intermediate-luminosity Transient Events), having maximum luminosities fainter than supernovae, red IR colors, and a wide range of outburst durations (days to years). Here we report deep optical and near-IR imaging with the Hubble Space Telescope (HST) of 21 SPIRITS variables. They were initially considered SPRITE transients, but many eventually proved instead to be periodic or irregular variables as more data were collected. HST images show most of these cool and dusty variables are associated with star-forming regions in late-type galaxies, implying an origin in massive stars. Two SPRITEs lacked optical progenitors in deep pre-outburst HST images; however, one was detected during eruption at J and H, indicating a dusty object with an effective temperature of ~1050 K. One faint SPRITE turned out to be a dusty classical nova. About half the HST targets proved to be periodic variables, with pulsation periods of 670-2160 days; they are likely dusty asymptotic-giant-branch (AGB) stars with masses of ~5-10 Msun. A few of them were warm enough to be detected in deep HST frames, but most are too cool. Out of six irregular variables, two were red supergiants with optical counterparts in HST images; four were too enshrouded for HST detection.
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