小型IRAIT望远镜:圆顶C的光度测定和星震学

Third Coast Pub Date : 2007-06-01 DOI:10.1553/CIA150S315
G. Tosti
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引用次数: 2

摘要

小型IRAIT是一个25厘米的望远镜,计划于2007年2月在圆顶C安装。它将配备一个CCD,一个滤光轮,两个光电倍增管和一个液晶可调滤光片。小型irit旨在:测试圆顶C的天文测量;利用低闪烁水平和长时间不间断观测的可能性,为星震学提供场地资格和适用性。小型IRAIT将是IRAIT望远镜的前身,后者将在2007 - 2008年南极夏季期间安装。在过去的几年里,人们一直把注意力集中在南极洲作为一个可能的天文地点。极低的温度(夏季-30摄氏度,冬季-80摄氏度),闪烁小,能见度好(至少比在拉西拉,Agabi等人2006年好两倍),极夜持续时间长,是光度测定的有利条件。南极洲似乎是昂贵的空间任务的另一种选择,其巨大的优势是后勤和人员有可能在基地进行实验。意大利和法国合作的康科迪亚基地自2005年以来也在冬季全面投入使用。小型irit望远镜是irit红外望远镜的小兄弟。这台小型望远镜的任务是在irit到来之前进行天文实验。小型IRAIT是一种光学望远镜,直径25厘米,焦距3米。设置在焦平面上的采集单元位于加热的绝缘盒内。它配备了一个自动温度控制器,并通过一个光学窗与外部分离。实验装置的组装遵循两个原则:冗余,以便在故障情况下继续其功能;多用途,以进行不同的天文实验。焦平面配备CCD (MaxCam,带有KAF-0402E/ME, 768× 512像素)、光电倍增管、滤光轮和标准UBVRI滤光片、精密调焦器和液晶干涉滤光片。电子器件包括锁相放大器和调制解调装置。2007年冬季的科学目标小型IRAIT任务将在极夜期间提供第一次天文测量测试。在过去几年中,其他小组也进行了类似的测试,主要致力于大气湍流参数的现场测试和测量(Aristidi等316小型IRAIT望远镜:Dome C等人2005年的光度和星震学,Agabi等人2006年)。小型IRAIT具有多用途焦平面仪器,将提供不同种类的测试。预计将有三个主要目标:•在寒冷的极地冬季进行仪器测试,以检查操作条件,重点是远程控制和通信•现场鉴定,包括测量多波段消光系数、整个夜间的透明度稳定性和冬季夜间不同时间的天空星等(关于先前的研究,请参阅Kenyon等人,2006年)•恒星测光测试,主要用于星震学。对于这个测试,我们计划得到β Hyi (V = 2.8)的时间序列。这将使我们能够测量闪烁,并在大约四周的观测后探测到类似太阳的振荡的能量过剩。我们进一步的目标是获得具有已知变量的开簇的多色时间序列。冬季任务将于2007年2月1日开始,届时望远镜将被安装在康科迪亚基地。致谢我们要感谢意大利和法国极地研究所(PNRA和IPEV)为实验和任务提供的后勤和财政支持。我们要感谢Laszlo Kiss和Tim bedings(澳大利亚悉尼大学)的建设性讨论和建议。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Small IRAIT Telescope: photometry and asteroseismology at Dome C
Small IRAIT is a 25 cm telescope planned to be installed at Dome C during February 2007. It will be equipped with a CCD, a filter wheel, two photomultipliers and a liquid crystal tunable filter. Small IRAIT is intended to: test astronomical measurements from Dome C; provide site qualification and suitability for asteroseismology by taking advantage of the low scintillation level and the possibility for long uninterrupted observations. Small IRAIT will be the forerunner of the IRAIT telescope that will be installed during the Antarctic Summer 2007−2008. Astronomy from Antarctica In the last years attention has been focused towards Antarctica as a possible astronomical site. Extremely low temperatures (-30 C during summer, -80 C during winter), small scintillation and good seeing (at least a factor of two better than at La Silla, Agabi et al. 2006) and the long duration of the polar night are promising ingredients for photometry. Antarctica seems to be an alternative to expensive space missions, with the great advantage of the possibility for logistics and personnel to work on the experiments on the base. Concordia Base, a joint Italian-French cooperation, has been fully operational also in the winter period since 2005. Small IRAIT Telescope Small IRAIT is the little brother of the IRAIT infrared telescope. The task of the small telescope is to perform astronomical experiments before the arrival of IRAIT itself. Small IRAIT is an optical telescope, 25 cm of diameter and with 3 m focal length. The acquisition unit set up on the focal plane is inside a heated, insulated box. It is equipped with an automated temperature controller and is decoupled from the outside by an optical window. The experimental setup has been assembled following two guidelines: redundancy, in order to continue its function even in case of a breakdown, and multipurpose to carry out different astronomical experiments. The focal plane is equipped with a CCD (MaxCam, with KAF-0402E/ME, 768× 512 pixels), photomultipliers, filterwheel and standard UBVRI filters, precision focuser, and liquid crystal interference filters. Electronics include a lock-in amplifier and a modulation and demodulation apparatus. Scientific goal for winter 2007 The Small IRAIT mission will provide a first test of astronomical measurements during the polar night. Similar tests have been performed in the last years by other groups, mainly devoted to site testing and measurements of atmospheric turbulence parameters (Aristidi et 316 Small IRAIT Telescope: photometry and asteroseismology at Dome C al. 2005, Agabi et al. 2006). Small IRAIT, with its multi-purpose focal plane instrumentation, will provide different kinds of tests. Three principal goals are foreseen: • instrumental tests to check operating conditions during the cold polar winter, with emphasis on remote control and communications • site qualification, which includes measurements of multiband extinction coefficients, transparency stability throughout the night, and sky magnitude in winter at different times during the night (for a previous study, refer to Kenyon et al. 2006) • test of stellar photometry, mainly devoted to asteroseismology. For this test we plan to get time series of β Hyi (V = 2.8). This should enable us to measure the scintillation as well as to detect the power excess of solar-like oscillations after roughly four weeks of observation. We further aim to obtain multi-colour time series of an open cluster with known variables. The winter mission will begin on the 1st of February 2007, when the telescope will be installed at Concordia Base. Acknowledgments. We wish to thank the Italian and French Polar Institutes (PNRA & IPEV) for logistics and financial support for the experiment and the mission. We wish to thank Laszlo Kiss and Tim Bedding (Sydney University, Australia) for constructive discussions and suggestions.
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