DIRECT IMAGING CONFIRMATION AND CHARACTERIZATION OF A DUST-ENSHROUDED CANDIDATE EXOPLANET ORBITING FOMALHAUT
DIRECT IMAGING CONFIRMATION AND CHARACTERIZATION OF A DUST-ENSHROUDED CANDIDATE EXOPLANET ORBITING FOMALHAUT
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DOI：
10.1088/2041-8205/760/2/l32
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发表时间：
2012-10
期刊：
影响因子：
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通讯作者：
T. Currie;J. Debes;T. Rodigas;A. Burrows;Y. Itoh;M. Fukagawa;S. Kenyon;M. Kuchner;S. Matsumura
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文献类型：
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作者：
T. Currie;J. Debes;T. Rodigas;A. Burrows;Y. Itoh;M. Fukagawa;S. Kenyon;M. Kuchner;S. Matsumura
我们提出了斯巴鲁/IRCS J波段数据北落师门和档案2004-2006年HST/ACS数据首次提出的Kalas等人（重新）减少。我们确认存在一个候选系外行星，北落师门B，在2004年和2006年的F606 W数据集在一个高的信噪比。此外，我们确认在F814 W的检测，并提出了一个新的检测F435 W。北落师门B的空间运动可能与它处于一个与地球平行的、无碎片的环交叉轨道相一致，尽管需要进行新的天体测量才能得出更确切的结论。我们不能确认北落师门B表现出0.7-0.8等的变化，作为行星吸积或半瞬态尘埃云的证据。新的光谱能量分布和红外上限相结合，证实了北落师门B的发射来自小尘埃散射的星光，但这种尘埃最有可能与一个大质量的天体有关。Subaru和IRAC/4.5 μm的上限意味着M < 2 MJ，仍然与雕刻圆盘所需的北落师门B质量范围一致。北落师门B很可能是“通过直接成像确定的行星”，即使严格来说，它目前的图像并没有显示出来自直接成像行星的热辐射。
We present Subaru/IRCS J-band data for Fomalhaut and a (re)reduction of archival 2004–2006 HST/ACS data first presented by Kalas et al. We confirm the existence of a candidate exoplanet, Fomalhaut b, in both the 2004 and 2006 F606W data sets at a high signal-to-noise ratio. Additionally, we confirm the detection at F814W and present a new detection in F435W. Fomalhaut b's space motion may be consistent with it being in an apsidally aligned, non-debris ring-crossing orbit, although new astrometry is required for firmer conclusions. We cannot confirm that Fomalhaut b exhibits 0.7–0.8 mag variability cited as evidence for planet accretion or a semi-transient dust cloud. The new, combined optical spectral energy distribution and IR upper limits confirm that emission identifying Fomalhaut b originates from starlight scattered by small dust, but this dust is most likely associated with a massive body. The Subaru and IRAC/4.5 μm upper limits imply M < 2 MJ, still consistent with the range of Fomalhaut b masses needed to sculpt the disk. Fomalhaut b is very plausibly “a planet identified from direct imaging” even if current images of it do not, strictly speaking, show thermal emission from a directly imaged planet.