An Optical/Near-infrared Investigation of HD 100546 b with the Gemini Planet Imager and MagAO
An Optical/Near-infrared Investigation of HD 100546 b with the Gemini Planet Imager and MagAO
复制标题
使用 Gemini 行星成像仪和 MagAO 对 HD 100546 b 进行光学/近红外研究
DOI：
10.3847/1538-3881/aa6cae
复制
发表时间：
2017
期刊：
影响因子：
--
通讯作者：
S. Wiktorowicz
中科院分区：
文献类型：
--
作者：
J. Rameau;K. Follette;K. Follette;L. Pueyo;C. Marois;C. Marois;B. Macintosh;M. Millar;Jason J. Wang;David Vega;R. Doyon;D. Lafreniére;E. Nielsen;E. Nielsen;V. Bailey;J. Chilcote;L. Close;T. Esposito;J. Males;S. Metchev;S. Metchev;K. Morzinski;J. Ruffio;S. Wolff;S. Wolff;S. Ammons;T. Barman;J. Bulger;T. Cotten;R. J. Rosa;G. Duchêne;G. Duchêne;M. Fitzgerald;S. Goodsell;J. Graham;A. Greenbaum;P. Hibon;L. Hung;P. Ingraham;P. Kalas;Q. Konopacky;J. Larkin;J. Maire;F. Marchis;R. Oppenheimer;D. Palmer;J. Patience;M. Perrin;L. Poyneer;A. Rajan;F. Rantakyrö;M. Marley;D. Savransky;A. Schneider;A. Sivaramakrishnan;I. Song;R. Soummer;Sandrine Thomas;J. Wallace;K. Ward;S. Wiktorowicz
我们给出了用双子星成像仪和麦哲伦可见声光相机获得的HD 100546的H带光谱和Hα光度观测结果。我们在原行星HD 100546 b的位置探测到了H带发射，但数据处理参数的选择强烈地影响了这个源的形态。在一些激进的减少中，它看起来像点状，但在大多数其他情况下，它重新加入了扩展的磁盘结构。此外，我们还证明了这一辐射在4.6年的时间尺度上是稳定的，在2σ水平上与圆盘平面上59Au的开普勒顺时针轨道不一致。发射的H波段光谱与任何类型的低有效温度天体或吸积原行星盘都不一致。它强烈地暗示了散射光的起源，因为这与恒星的光谱以及在圆盘中其他位置提取的光谱是一致的。假设原行星位于一个没有消光的空隙中，在5σ能级的HD 100546 b处没有被探测到，这是一个上限，它的吸积光度为1.7x10−4 L⊙和1RJup。这些极限与T-Tauri星或LkCa15b的吸积光度和吸积率相当。综合起来，这些证据表明，HD 100546 b位置的H带源不是由行星光球或吸积的环行星盘发出的，而是由点扩展函数减去过程增强的盘特征。这种未检测到的情况与早期研究中报告的K带未检测到的情况是一致的，但不排除HD 100546 b被深度嵌入的可能性。
We present H band spectroscopic and Hα photometric observations of HD 100546 obtained with the Gemini Planet Imager and the Magellan Visible AO camera. We detect H band emission at the location of the protoplanet HD 100546 b, but show that the choice of data processing parameters strongly affects the morphology of this source. It appears point-like in some aggressive reductions, but rejoins an extended disk structure in the majority of the others. Furthermore, we demonstrate that this emission appears stationary on a timescale of 4.6 years, inconsistent at the 2σ level with a Keplerian clockwise orbit at 59 au in the disk plane. The H band spectrum of the emission is inconsistent with any type of low effective temperature object or accreting protoplanetary disk. It strongly suggests a scattered-light origin, as this is consistent with the spectrum of the star and the spectra extracted at other locations in the disk. A non-detection at the 5σ level of HD 100546 b in differential Hα imaging places an upper limit, assuming the protoplanet lies in a gap free of extinction, on the accretion luminosity of 1.7 × 10−4 L⊙ and for 1 RJup. These limits are comparable to the accretion luminosity and accretion rate of T-Tauri stars or LkCa 15 b. Taken together, these lines of evidence suggest that the H band source at the location of HD 100546 b is not emitted by a planetary photosphere or an accreting circumplanetary disk but is a disk feature enhanced by the point-spread function subtraction process. This non-detection is consistent with the non-detection in the K band reported in an earlier study but does not exclude the possibility that HD 100546 b is deeply embedded.