LSU Digital Commons LSU Digital Commons A close look into the carbon disk at the core of the planetary A close look into the carbon disk at the core of the planetary nebula CPD-56°8032 nebula CPD-56°8032
LSU Digital Commons LSU Digital Commons A close look into the carbon disk at the core of the planetary A close look into the carbon disk at the core of the planetary nebula CPD-56°8032 nebula CPD-56°8032
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路易斯安那州立大学数字共享 路易斯安那州立大学数字共享 近距离观察行星状星云核心的碳盘 近距离观察行星状星云核心的碳盘 CPD-56°8032 星云 CPD-56°8032
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通讯作者：
D. Spini
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作者：
G. Elcheroth;S. Penić;R. Fasel;F. Giudici;S. Glaeser;D. Joye;Jean;D. Morselli;D. Spini
目标。我们给出了用Wolf-Rayet中心星Cpd-56◦8032对行星星云尘埃核心的高空间分辨率观测，HST/SIT观测发现了其致密盘的迹象。方法：研究方法。这些观测是使用中红外干涉仪VLTI/MIDI进行的，在成像模式下提供典型的300毫安分辨率，并在干涉模式下使用UT2-UT3 47m基线提供典型的空间分辨率20毫安。我们还利用了F435W和F606WfiLter中未发表的HST/ACES图像。结果。可见的HST图像显示了一个复杂的多全局几何图形，以微弱的叶为主。最远的结构位于距离恒星7(Cid：3)(Cid：3)处。Cpd-56◦8032的中红外环境以紧凑源为主，仅用一台UT望远镜在8.7umfilter(∆λ=1.6微米，受多环芳烃排放污染)。从−5◦到51◦的三个40-45m的投影基线几乎完全分辨了红外核，但在光谱分散的能见度中检测到了低层平滑的振荡条纹。这个清晰的信号被解释为一种环状结构，它将fiNe赤道盘明亮的内缘。几何模型使我们能够推导出圆盘的主要几何参数。例如，对于半径为97±11 AU、倾角为28±7◦、长轴为345◦±7◦的消色差和椭圆截断的高斯光束，可以获得相当好的PART t。此外，我们还进行了一些辐射传输模拟，目的是通过考虑MIDI弥散可见度、光谱和源的大口径SED来进一步限制圆盘的几何和质量含量。这些模型表明，该圆盘在N波段大部分是光学上很薄的，并且具有很高的fl。由于复杂的flUX分布，数据不排除边缘倾斜。
Aims. We present high spatial resolution observations of the dusty core of the Planetary Nebula with Wolf-Rayet central star CPD-56 ◦ 8032, for which indications of a compact disk have been found by HST / SITS observations. Methods. These observations were taken with the mid-infrared interferometer VLTI / MIDI in imaging mode providing a typical 300 mas resolution and in interferometric mode using UT2-UT3 47m baseline providing a typical spatial resolution of 20 mas. We also made use of unpublished HST / ACS images in the F 435 W and F 606 W filters. Results. The visible HST images exhibit a complex multilobal geometry dominated by faint lobes. The farthest structures are located at 7 (cid:3)(cid:3) from the star. The mid-IR environment of CPD-56 ◦ 8032 is dominated by a compact source, barely resolved by a single UT telescope in a 8.7 µ m filter ( ∆ λ = 1 . 6 µ m, contaminated by PAH emission). The infrared core is almost fully resolved with the three 40–45 m projected baselines ranging from − 5 ◦ to 51 ◦ but smooth oscillating fringes at low level have been detected in spectrally dispersed visibilities. This clear signal is interpreted in terms of a ring structure which would define the bright inner rim of the equa- torial disk. Geometric models allowed us to derive the main geometrical parameters of the disk. For instance, a reasonably good fit is reached with an achromatic and elliptical truncated Gaussian with a radius of 97 ± 11 AU, an inclination of 28 ± 7 ◦ and a PA for the major axis at 345 ◦ ± 7 ◦ . Furthermore, we performed some radiative transfer modeling aimed at further constraining the geometry and mass content of the disk, by taking into account the MIDI dispersed visibilities, spectra, and the large aperture SED of the source. These models show that the disk is mostly optically thin in the N band and highly flared. As a consequence of the complex flux distribution, an edge-on inclination is not excluded by the data.