基于NiosⅡ嵌入式软核处理器的天文用IRFPA图像采集系统

介绍了一套自主研制的用于地基天文望远镜的，基于IRFPA（红外焦平面阵列）图像采集系统，以及所使用的IRFPA原理、性能特点，着重介绍了IRFPA图像采集系统中以NiosⅡ处理器为核心的电子系统的框架结构方案以及软硬件的设计思想。最后给出了初步的图像采集成像结果。     

可用于近红外太阳观测的几种红外探测器阵列

总结了天文用近红外焦平面阵列（ＩＲＦＰＡ）的发展历程，阐述了ＩＲＦＰＡ的结构，重点介绍了ＩｎＳｂ、ＨｇＣｄＴｅ和ＰｔＳｉ三种近红外探测器阵列，结合目前正在筹建的红外太阳塔计划，对其各项性能指标作了详细比较     

可用于近红外太阳观测的几种红外探测器阵列

总结了天文用近红外焦平面阵列（ＩＲＦＰＡ）的发展历程，阐述了ＩＲＦＰＡ的结构，重点介绍了ＩｎＳｂ，ＨｇＣｄＴｅ和ＰｔＳｉ三种近红外探测器阵列，结合目前在筹建的红外太阳塔计划，对其各项性能指标作了详细比较。]     

红外波段太阳观测技术方法研究

1m红外太阳塔是我国未来重点发展的地面太阳观测设备 ,本文的所有工作均围绕着与此相关的红外波段太阳观测技术方法展开。1 .针对望远镜实验平台—云台太阳光谱仪 ,建立了光谱仪分光流量模型 ,并用多种实验手段验证了其可靠性。利用该模型计算了FeⅠ 1 .56μm红外太阳光谱的分光流量 ,分析了实验观测的可行性及改进方案。2 .针对探测器实验平台—PtSi红外焦平面阵列相机 ,建立了FeⅠ 1 .56μm光谱观测信噪比模型 ,模拟了各种噪声对观测的影响。在此基础上 ,在国内首次成功进行了FeⅠ1 .56μm红外太阳光谱的面阵观测实验。3 .在红外观测实验所处的高背景低对比度条件下 ,讨论了红外太阳光谱观测的图像处理方法 ,分析了观测中出现的干涉条纹的来源及解决办法 ,初步建立起了一整套红外太阳光谱与成像的定标方法和图像处理方法。4 .首次利用PVA材料 ,设计研制了一套FeⅠ 1 .56μm近红外Stokes参量偏振仪 ,并将该偏振仪安装在美国国立天文台McMath望远镜上进行了观测实验。针对一太阳黑子 ,通过扫描进行了二维的Stokes参量观测。同时建立了一套从Stokes参量反演磁矢量场的方法 ,并将反演的结果与怀柔太阳磁场望远镜的观测结果进行了比对。5.针对 1m红外太阳塔的太阳光谱仪系统 ,给出了垂直多波段光谱仪和红外     

红外阵列成象器件在天文上的应用

本文描述了红外阵列探测器件的基本性能要求、分类特征及其利弊。专门介绍了一个具有典型代表意义的InSb-CID阵列的原理及设计构造,还扼要介绍了目前世界各国红外阵列探测技术在天文上的应用动态,最后阐述了今后红外CCD可做的天文课题。     

红外波段太阳观测技术方法研究

1m红外太阳塔是我国未来重点发展的地面太阳观测设备，本文的所有工作均围绕着与此相关的红外波段太阳观测技术方法展开。1．针对望远镜实验平台－云台太阳光谱仪，建立了光谱仪分光流量,工用多种实验手段验证了其可靠性。利用该模型计算了Fe Ⅰ1.56μm红外太阳光 谱的分光流量，分析了实验观测的可行性及改进方案。2．针对探测器实验平台－PtSi红外焦平面阵列相机，建立了FeⅠ1.56μm光谱观测信噪比模型，模拟了各种噪声对观测的影响。在此基础上，在国内首次成功进行了FeⅠ1.56μm红外太阳光谱的面阵观测实验。3．在红外观测实验所处的高背景低对比度条件下，讨论了红外太阳光谱观测的图像处理方法，分析了观测中出现的干涉条纹的来源及解决办法，初步建立起了一整套红外太阳光谱与成像的定标方法和图像处理方法。4．首次利用PVA材料，设计研制了一套FeⅠ1.56μm近红外Stokes参量偏振仪，并将该偏振仪安装在美国国立天文台McMath望远镜上进行了观测实验。针对一太阳黑子，通过扫描进行了二维的Stokes参量观测。同时建立了一套从Stokes参量反演磁矢量场的方法，并将反演的结果与怀柔太阳磁场望远镜的观测结果进行了比对。5．针对1m红外太阳塔的太阳光谱仪系统，给出了垂直多波段光谱仪和红外大色散光谱仪的光、机初步设计。6．针对1m红外太阳塔的科学目标，提出了多波段光谱仪探测器系统方案，对红外大色散光谱仪所使用的红外探测器也进行了初步方案设计。     

日本早期的空间红外天文学

与前几期所介绍的那些大个头空间望远镜相比,今天将要出场的主人公无疑是一个小字辈,它是日本的第一个空间红外设备——空间红外望远镜（Infrared Telescope in Space,IRTS）。可能大家都注意到了,很多空间设备的名字都很相似,比如先前讲过的红外天文卫星（IRAS）、红外空间天文台（ISO）以及今天将要提到的空间红外望远镜（IRTS）,它们的名字都是大同小异。     

年轻星天体喷流的近红外成像观测进展

分子氢的红外振动发射线是显现年轻星质量外流的重要谱线之一。自Gautier等人1976年在猎户座发现年轻星质量外流的分子氢发射开始,人们在银河系内几乎所有的恒星形成区都发现了这种线发射。研究表明,分子氢发射与年轻星周围的其它活动现象（如分子外流和光学喷流）之间有着非常密切的联系。红外和光学喷流代表了年轻星剧烈活动的两个侧面,是喷流与周围介质相互作用强弱不同的表现,这种作用还拖带周围介质,产生分子外流,光学、红外喷流和分子外流组成了恒星形成区壮观的景象,它们是恒星形成活动的重要标志。随着红外探测技术的飞速发展,对年轻星外流活动现象的观测越来越丰富的详细,使人们对这种现象的本质越来越了解。在20世纪90年代NICMOS等大阵列红外探测器投入使用后,红外成像观测有了长足的进步。目前已在70个左右的区域里发现了H2发射,这一数字还在迅速增加,今后的研究主要可能向两个方向发展。其一是高分辨观测,进一步了解H2发射的结构以及与光学喷流和分子外流之间的关系;其二是天观测,了解银河系内的恒星形成H2区发射的大尺度结构和恒星形成的统计分布规律。     

AIMS望远镜8～10微米成像终端系统装调检测方法

针对用于太阳磁场精确测量的中红外观测系统(Accurate Infrared Magnetic field Measurements of the Sun,AIMS)望远镜8～10μm真空制冷成像终端系统的高精度装调需求,提出了一种基于中红外可调谐激光光源的宽谱段干涉检测和装调方法.首先,采用泰曼-格林干涉仪,利用参考...     

矩尺天区的近红外天体

利用Ｒ（红）－Ｉ（近红外）两色照相测光方法，搜寻银道带天区的红外超天体，并证认ＩＲＡＳ点源的红外超对应体。本文是一组系列文章的第四篇。在矩尺天区发现了１９５个红外超天体，并证认出其中２２个是ＩＲＡＳ点源的对应体。     

Conversion Gain and Interpixel Capacitance of Cmos Hybrid Focal Plane Arrays

The conversion gain of optical and infrared focal plane CMOS hybrid arrays is a fundamental parameter, whose value computes into the derivation of other parameters characterizing the performance of a detector. The widespread “noise squared versus signal” method used to obtain the conversion gain can overestimate the nodal capacitance of the detector pixel by more than 20% for infrared arrays and by more than 100% for Si-PIN diode arrays. This is because this method does not take account of the capacitive coupling between neighboring pixels. A simple technique has been developed to measure the nodal capacitance directly by comparing the voltage change of an external calibrated capacitor with the voltage change on the nodal capacitor of the detector pixel. The method is elaborated in detail and has been verified with a Si-PIN diode array hybridized to a Hawaii-2RG multiplexer using an Fe ⁵⁵ X-ray source. It is also in good agreement with a stochastic method based on 2D autocorrelation.     

The Be/X-ray transient V0332+53: evidence for a tilt between the orbit and the equatorial plane?

We present optical and infrared observations of BQ Cam, the optical counterpart to the Be/X-ray transient system V0332+53. BQ Cam is shown to be an O8–9Ve star, which places V0332+53 at a distance of ∼7 kpc. H α spectroscopy and infrared photometry are used to discuss the evolution of the circumstellar envelope. Owing to the low inclination of the system, parameters are strongly constrained. We find strong evidence for a tilt of the orbital plane with respect to the circumstellar disc (presumably on the equatorial plane). Even though the periastron distance is only ≈10 R _*, during the present quiescent state the circumstellar disc does not extend to the distance of periastron passage. Under these conditions, X-ray emission is effectively prevented by centrifugal inhibition of accretion. The circumstellar disc is shown to be optically thick at optical and infrared wavelengths, which, together with its small size, is taken as an indication of tidal truncation.     

The geometric calibration of the Planck satellite using solar system objects

The geometric calibration of the Planck satellite using the planetary transits is investigated, together with the reconstruction of any offsets from the nominal layout of the focal plane. The methods presented here may be applied to a single focal plane transit of a planet, to find the values of the geometric-calibration parameters at the epoch of the transit or all the transits over the course of the mission. The pointing requirements are easily met, with the pointing reconstruction being dominated by the errors due to the star tracker.     

Infrared instruments for the Gemini 8-M telescopes

The Gemini Telescopes are being built to exploit the splendid infrared sites of Mauna Kea in Hawaii and Cerro Pachon in Chile. Both telescopes are being designed to deliver 0.1 arcsecond images at 2.2 m to the focal plane. This image size includes all tracking and enclosure effects. To exploit the superb infrared characteristics of the sites and telescopes we will require a new generation of IR instruments which will challenge both instrument designers and infrared array technologies.     

Infrared interferometry with single telescopes

We examine the merits of three basic interferometric techniques using two-dimensional infrared arrays: speckle interferopmetry, pupil plane interferometry, and speckle holography.Paper presented at the Symposium on the JNLT and Related Engineering Developments, Tokyo, November 29–December 2, 1988.     

Orion: A 1–5 Micron Focal Plane for the 21st Century

The Orion program is a project to develop a 2K × 2K infrared focal plane using InSb p-on-n diodes for detectors. It is the natural follow-up to the successful Aladdin 1K × 1K program started in the early 90's. The work is being done at the Raytheon Infrared Operations Division (RIO, previously known as the Santa Barbara Research Center) by many of the same people who created the Aladdin focal plane. The design is very similar to the successful Aladdin design with the addition of reference pixels, whole array readout (no quadrants), two-adjacent-side buttability, and a packaging design that includes going directly to the ultimate focal plane size of 4K × 4K. So far we have successfully made a limited number of hybrid modules with InSb detectors. In this paper we will describe the design features and test data taken from some of these devices. This revised version was published online in July 2006 with corrections to the Cover Date.     

Properties of optical fibres at cryogenic temperatures

A perhaps surprising property of optical fibres is that they remain flexible at cryogenic temperatures. This implies that they may be used for multiple-object and integral field spectroscopy in the thermal infrared in cryogenic instrumentation. In this paper the results of performance tests of optical fibres (silica and zirconium fluoride) at cryogenic temperatures are presented. By mounting the fibres in glass tubes with the appropriate adhesive, it was found that only negligible focal ratio degradation occurs when the fibre is cooled to 77 K.     

Possible formation scenarios for the giant H i envelope around the NGC 4490/4485 system

We present observations of H i in the nearby interacting galaxies NGC 4490 and 4485 made with the VLA in both C and D arrays. The galaxies are embedded in an extensive envelope of neutral hydrogen which is elongated in a direction approximately perpendicular to the plane of NGC 4490, with an extent of about 56 kpc. We argue that this distribution of neutral hydrogen can best be explained by a galactic-scale bipolar outflow of H  i driven by supernovae in NGC 4490. The flow from the disc appears to be reasonably well collimated and has probably persisted for approximately 6 × 10⁸ yr. The implications for galaxy evolution when such mass loss occurs are briefly discussed.     

Simulated performance of dedicated Ge-strip Compton telescopes as γ-lens focal plane instrumentation

With focusing of gamma rays in the nuclear-line energy regime starting to establish itself as a feasible and very promising approach for high-sensitivity γ-ray (line) studies of individual sources, optimizing the focal plane instrumentation for γ-ray lens telescopes is a prime concern. Germanium detectors offer the best energy resolution available at ∼2 keV FWHM at 1 MeV and thus constitute the detector of choice for a spectroscopy mission in the MeV energy range. Using a Compton detector focal plane has three advantages over monolithic detectors: additional knowledge about (Compton) events enhances background rejection capabilities, the inherently finely pixellated detector naturally allows the selection of events according to the focal spot size and position, and Compton detectors are inherently sensitive to γ-ray polarization. We use the extensive simulation and analysis package assembled for the ACT vision mission study to explore achievable sensitivities for different Ge Compton focal plane configurations as a first step towards determining an optimum configuration.CBW thanks the Townes Fellowship at UCB and NASA Grant NNG05WC28G for Support.     

SCUBA-2 CCD-STYLE IMAGING FOR THE JCMT

SCUBA-2 will replace SCUBA (Submillimetre Common User Bolometer Array) on the James Clerk Maxwell Telescope in 2006 and will be the first CCD-style camera for submillimetre astronomy. The instrument will simultaneously image at 850 and 450 microns using two focal plane arrays of 5120 pixels each. SCUBA-2 will map the submillimetre sky 1000 times faster than SCUBA to the same signal-to-noise ratio. This paper introduces the detector technology and the challenges faced in reading out a detector array cooled to ～120 mK.