G. Cugno, J. Leisenring, Kevin R. Wagner, Camryn Mullin, Roubing Dong, Tom Greene, Doug Johnstone, Michael R. Meyer, S. Wolff, C. Beichman, Martha Boyer, Scott Horner, K. Hodapp, Doug Kelly, Don McCarthy, Thomas L. Roellig, G. Rieke, Marcia J. Rieke, J. Stansberry, Erick Young
{"title":"JWST/NIRCam 对年轻恒星天体的成像。II.对 SAO 206462 周围螺旋盘外巨行星和一颗候选行星的深度约束","authors":"G. Cugno, J. Leisenring, Kevin R. Wagner, Camryn Mullin, Roubing Dong, Tom Greene, Doug Johnstone, Michael R. Meyer, S. Wolff, C. Beichman, Martha Boyer, Scott Horner, K. Hodapp, Doug Kelly, Don McCarthy, Thomas L. Roellig, G. Rieke, Marcia J. Rieke, J. Stansberry, Erick Young","doi":"10.3847/1538-3881/ad1ffc","DOIUrl":null,"url":null,"abstract":"\n We present JWST/NIRCam F187N, F200W, F405N, and F410M direct imaging data of the disk surrounding SAO 206462. Previous images show a very structured disk, with a pair of spiral arms thought to be launched by one or more external perturbers. The spiral features are visible in three of the four filters, with the nondetection in F410M due to the large detector saturation radius. We detect with a signal-to-noise ratio of 4.4 a companion candidate that, if on a coplanar circular orbit, would orbit SAO 206462 at a separation of ∼300 au, 2.25σ away from the predicted separation for the driver of the eastern spiral. No other companion candidates were detected. At the location predicted by simulations of both spirals generated by a single massive companion, the NIRCam data exclude objects more massive than ∼2.2 M\n J assuming the BEX evolutionary models. In terms of temperatures, the data are sensitive to objects with T\n eff ∼ 650–850 K, when assuming planets emit like blackbodies (R\n p between 1 and 3R\n J). From these results, we conclude that if the spirals are driven by gas giants, these must be either cold or embedded in circumplanetary material. In addition, the NIRCam data provide tight constraints on ongoing accretion processes. In the low extinction scenario we are sensitive to mass accretion rates of the order \n \n\n\n \n \n \n M\n \n \n ̇\n \n \n ∼\n \n \n 10\n \n \n −\n 9\n \n \n \n \n M\n \n \n J\n \n \n \n \n yr−1. Thanks to the longer wavelengths used to search for emission lines, we reach unprecedented sensitivities to processes with \n \n\n\n \n \n \n M\n \n \n ̇\n \n \n ∼\n \n \n 10\n \n \n −\n 7\n \n \n \n \n M\n \n \n J\n \n \n \n \n yr−1 even toward highly extincted environments (A\n V ≈ 50 mag).","PeriodicalId":424210,"journal":{"name":"The Astronomical Journal","volume":"15 2","pages":""},"PeriodicalIF":0.0000,"publicationDate":"2024-01-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"JWST/NIRCam Imaging of Young Stellar Objects. II. Deep Constraints on Giant Planets and a Planet Candidate Outside of the Spiral Disk Around SAO 206462\",\"authors\":\"G. Cugno, J. Leisenring, Kevin R. Wagner, Camryn Mullin, Roubing Dong, Tom Greene, Doug Johnstone, Michael R. Meyer, S. Wolff, C. Beichman, Martha Boyer, Scott Horner, K. Hodapp, Doug Kelly, Don McCarthy, Thomas L. Roellig, G. Rieke, Marcia J. Rieke, J. Stansberry, Erick Young\",\"doi\":\"10.3847/1538-3881/ad1ffc\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"\\n We present JWST/NIRCam F187N, F200W, F405N, and F410M direct imaging data of the disk surrounding SAO 206462. Previous images show a very structured disk, with a pair of spiral arms thought to be launched by one or more external perturbers. The spiral features are visible in three of the four filters, with the nondetection in F410M due to the large detector saturation radius. We detect with a signal-to-noise ratio of 4.4 a companion candidate that, if on a coplanar circular orbit, would orbit SAO 206462 at a separation of ∼300 au, 2.25σ away from the predicted separation for the driver of the eastern spiral. No other companion candidates were detected. At the location predicted by simulations of both spirals generated by a single massive companion, the NIRCam data exclude objects more massive than ∼2.2 M\\n J assuming the BEX evolutionary models. In terms of temperatures, the data are sensitive to objects with T\\n eff ∼ 650–850 K, when assuming planets emit like blackbodies (R\\n p between 1 and 3R\\n J). From these results, we conclude that if the spirals are driven by gas giants, these must be either cold or embedded in circumplanetary material. In addition, the NIRCam data provide tight constraints on ongoing accretion processes. In the low extinction scenario we are sensitive to mass accretion rates of the order \\n \\n\\n\\n \\n \\n \\n M\\n \\n \\n ̇\\n \\n \\n ∼\\n \\n \\n 10\\n \\n \\n −\\n 9\\n \\n \\n \\n \\n M\\n \\n \\n J\\n \\n \\n \\n \\n yr−1. Thanks to the longer wavelengths used to search for emission lines, we reach unprecedented sensitivities to processes with \\n \\n\\n\\n \\n \\n \\n M\\n \\n \\n ̇\\n \\n \\n ∼\\n \\n \\n 10\\n \\n \\n −\\n 7\\n \\n \\n \\n \\n M\\n \\n \\n J\\n \\n \\n \\n \\n yr−1 even toward highly extincted environments (A\\n V ≈ 50 mag).\",\"PeriodicalId\":424210,\"journal\":{\"name\":\"The Astronomical Journal\",\"volume\":\"15 2\",\"pages\":\"\"},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2024-01-05\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"The Astronomical Journal\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/10.3847/1538-3881/ad1ffc\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"The Astronomical Journal","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.3847/1538-3881/ad1ffc","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
引用次数: 0
摘要
我们展示了 JWST/NIRCam F187N、F200W、F405N 和 F410M 对 SAO 206462 周围圆盘的直接成像数据。之前的图像显示了一个结构非常清晰的圆盘,其中有一对螺旋臂被认为是由一个或多个外部扰动器发射的。在四个滤光片中的三个滤光片中都能看到螺旋特征,F410M滤光片中未发现螺旋特征是由于探测器饱和半径过大造成的。我们以 4.4 的信噪比探测到了一个候选伴星,如果它处于共面环形轨道上,那么它将在距离 SAO 206462 ∼ 300 au 的地方绕其运行,与东螺旋驱动的预测距离相差 2.25σ。没有发现其他候选伴星。在模拟由单个大质量伴星产生的两个螺旋所预测的位置,NIRCam数据排除了质量大于∼2.2 M J(假设BEX演化模型)的天体。在温度方面,假定行星像黑体一样发射(R p 在 1 到 3R J 之间),数据对 T eff ∼ 650-850 K 的天体很敏感。从这些结果中,我们得出结论,如果螺旋是由气体巨行星驱动的,那么这些气体巨行星必须是低温的,或者嵌入了环行星体物质。此外,NIRCam 数据还对正在进行的吸积过程提供了严格的约束。在低消光情况下,我们对 M ∼ 10 - 9 M J yr-1 数量级的质量吸积率非常敏感。由于使用了更长的波长来搜索发射线,我们对 Ṁ ∼ 10 - 7 M J yr-1 的过程达到了前所未有的敏感度,甚至对高度消光环境(A V ≈ 50 mag)也是如此。
JWST/NIRCam Imaging of Young Stellar Objects. II. Deep Constraints on Giant Planets and a Planet Candidate Outside of the Spiral Disk Around SAO 206462
We present JWST/NIRCam F187N, F200W, F405N, and F410M direct imaging data of the disk surrounding SAO 206462. Previous images show a very structured disk, with a pair of spiral arms thought to be launched by one or more external perturbers. The spiral features are visible in three of the four filters, with the nondetection in F410M due to the large detector saturation radius. We detect with a signal-to-noise ratio of 4.4 a companion candidate that, if on a coplanar circular orbit, would orbit SAO 206462 at a separation of ∼300 au, 2.25σ away from the predicted separation for the driver of the eastern spiral. No other companion candidates were detected. At the location predicted by simulations of both spirals generated by a single massive companion, the NIRCam data exclude objects more massive than ∼2.2 M
J assuming the BEX evolutionary models. In terms of temperatures, the data are sensitive to objects with T
eff ∼ 650–850 K, when assuming planets emit like blackbodies (R
p between 1 and 3R
J). From these results, we conclude that if the spirals are driven by gas giants, these must be either cold or embedded in circumplanetary material. In addition, the NIRCam data provide tight constraints on ongoing accretion processes. In the low extinction scenario we are sensitive to mass accretion rates of the order
M
̇
∼
10
−
9
M
J
yr−1. Thanks to the longer wavelengths used to search for emission lines, we reach unprecedented sensitivities to processes with
M
̇
∼
10
−
7
M
J
yr−1 even toward highly extincted environments (A
V ≈ 50 mag).