A Deep Search for Planets in the Inner 15 au around Vega

被引：6
|
作者：
Meshkat, Tiffany [1 ,2 ]
Nilsson, Ricky [3 ,4 ]
Aguilar, Jonathan [5 ]
Vasisht, Gautam [2 ]
Oppenheimer, Rebecca [4 ]
Su, Kate Y. L. [6 ]
Cady, Eric [2 ]
Lockhart, Thomas [2 ]
Matthews, Christopher [2 ]
Dekany, Richard [3 ]
Leisenring, Jarron [6 ]
Ygouf, Marie [1 ]
Mawet, Dimitri [2 ,3 ]
Pueyo, Laurent [7 ]
Beichman, Charles [1 ,2 ]
机构：
[1] CALTECH, IPAC, M-C 100-22,1200 East Calif Blvd, Pasadena, CA 91125 USA
[2] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA
[3] CALTECH, Dept Astron, 1200 East Calif Blvd,MC 249-17, Pasadena, CA 91125 USA
[4] Amer Museum Nat Hist, Astrophys Dept, Cent Pk West & 79th St, New York, NY 10024 USA
[5] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA
[6] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA
[7] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA
来源：
ASTRONOMICAL JOURNAL | 2018年 / 156卷 / 05期
关键词：
circumstellar matter; planets and satellites: detection; stars: individual (Vega); techniques: high angular resolution; ADAPTIVE OPTICS; EVOLUTIONARY MODELS; GIANT PLANETS; BROWN DWARFS; DEBRIS DISK; MASS; SPECTROSCOPY; DISCOVERY; EXOPLANET; IMAGES;
D O I：
10.3847/1538-3881/aae14f
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We present the results of a deep high-contrast imaging search for planets around Vega. Vega is an ideal target for high-contrast imaging because it is bright, nearby, and young with a face-on two-belt debris disk that may be shaped by unseen planets. We obtained J- and H-band data on Vega with the coronagraphic integral-field spectrograph Project 1640 (P1640) at Palomar Observatory. Two nights of data were obtained in 2016, in poor seeing conditions, and two additional nights in more favorable conditions in 2017. In total, we obtained 5.5 hours of integration time on Vega in moderate to good seeing conditions (< 1 ''.5). We did not detect any low-mass companions in this system. Our data present the most sensitive contrast limits around Vega at very small separations (2-15 au) thus far, allowing us to place new constraints on the companions that may be sculpting the Vega system. In addition to new constraints, as the deepest data obtained with P1640, these observations form the final legacy of the now decommissioned instrument.
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页数：5
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