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Design of an Ultra-Wideband Antenna Feed and Reflector for use in Hydrogen Intensity Mapping Interferometers 用于氢强度测绘干涉仪的超宽带天线馈源和反射器的设计
Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-10-27 DOI: 10.1142/s2251171724500041
John Podczerwinski, Peter Timbie
This paper describes the design of a 5.5:1 bandwidth feed antenna and reflector system, intended for use in hydrogen intensity mapping experiments. The system is optimized to reduce systematic effects that can arise in these experiments from scattering within the feed/reflector and cross-coupling between antennas. The proposed feed is an ultra wideband Vivaldi style design and was optimized to have a smooth frequency response, high gain, and minimal shadowing of the reflector dish. This feed can optionally include absorptive elements which reduce systematics but degrade sensitivity. The proposed reflector is a deep parabolic dish with $f/d = 0.216$ along with an elliptical collar to provide additional shielding. The procedure for optimizing these design choices is described.
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引用次数: 0
Low Complexity Radio Frequency Interference Mitigation for Radio Astronomy Using Large Antenna Array 基于大型天线阵列的射电天文学低复杂度射频干扰抑制
Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-10-27 DOI: 10.1142/s225117172450003x
Zaid Bin Tariq, Teviet Creighton, Louis P. Dartez, Naofal Al-Dhahir, Murat Torlak
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引用次数: 0
The Effects of the Local Environment on a Compact Radio Interferometer I: Cross-coupling in the Tianlai Dish Pathfinder Array 局部环境对小型射电干涉仪的影响ⅰ:天来碟探路者阵列的交叉耦合
Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-10-13 DOI: 10.1142/s2251171724500028
Juhun Kwak, John Podczerwinski, Peter Timbie, Reza Ansari, John Marriner, Albert Stebbins, Fengquan Wu, Haotian Cao, Xuelei Chen, Kai He, Jixia Li, Shijie Sun, Jiacong Zhu
The visibilities measured by radio astronomical interferometers include non-astronomical correlated signals that arise from the local environment of the array. These correlated signals are especially important in compact arrays such as those under development for 21,cm intensity mapping. The amplitudes of the contaminated visibilities can exceed the expected 21,cm signal and represent a significant systematic effect. We study the receiver noise radiated by antennas in compact arrays and develop a model for how it couples to other antennas. We apply the model to the Tianlai Dish Pathfinder Array (TDPA), a compact array of 16, 6-m dish antennas. The coupling model includes electromagnetic simulations, measurements with a network analyzer, and measurements of the noise of the receivers. We compare the model to drift-scan observations with the array and set requirements on the level of antenna cross-coupling for 21,cm intensity mapping instruments. We find that for the TDPA, cross-coupling would have to be reduced by TBD orders of magnitude in order to contribute negligibly to the visibilities.
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引用次数: 0
Interferometric determination for cosmological and stellar phenomena 宇宙和恒星现象的干涉测定
IF 1.3 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-09-05 DOI: 10.1142/s2251171724500016
P. B. Lerner, P. H. Cutler, N. Miskovsky, T. E. Sullivan, A. Mayer
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引用次数: 0
DMD based Multi-Object Spectrograph for INdian Spectroscopic and Imaging Space Telescope: INSIST 基于DMD的印度光谱和成像空间望远镜多目标摄谱仪:坚持
IF 1.3 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-08-23 DOI: 10.1142/s2251171723500125
S. Sriram, V. Valsan, A. Hoodati, A. Subramaniam, G. Maheswar
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引用次数: 0
Calibration of Spectropolarimetry Package for Visible Emission Line Coronagraph (VELC) on board Aditya-L1 Mission Aditya-L1任务可见光发射线日冕仪(VELC)分光偏振仪包的校准
IF 1.3 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-08-23 DOI: 10.1142/s2251171723500113
Venkata Suresh Narra, Bhavana S. Hegde, Utkarsha Dasamantarao, Natarajan Venkatasubramanian, Pawan Kumar Somasundaram, Umesh Kamath Padhavu, Raghavendra Prasad Budihal
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引用次数: 0
A compact cryogenic configurable slit unit for a multi-object infrared spectrograph: Design and Development of a prototype at TIFR 用于多目标红外光谱仪的紧凑型低温可配置狭缝装置:TIFR原型的设计和开发
IF 1.3 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-07-28 DOI: 10.1142/s2251171723500101
P. Madhwani, A. Kutty, B. Mookerjea, J. Parmar, V. Kurhade, S. D’costa, P. Manoj, A. Surya
We present a cryogenic configurable slit unit (CSU) for a multi object infrared spectrograph with an effective field of view of 9.1 arcmin x 9.1 arcmin that was completely conceived and designed in the laboratory at TIFR. Several components of the CSU including the controller for the commercially procured piezo-walkers, controlled loop position sensing mechanism using digital slide callipers and a cryogenic test facility for the assembled prototype were also developed in-house. The principle of the CSU involves division of the field of view of the spectrometer into contiguous and parallel spatial bands, each one associated with two opposite sliding metal bars that can be positioned to create a slit needed to make spectroscopic observations of one astronomical object. A three-slit prototype of the newly designed CSU was built and tested extensively at ambient and cryogenic temperatures. The performance of the CSU was found to be as per specifications.
我们提出了一种用于多目标红外光谱仪的低温可配置狭缝单元(CSU),其有效视场为9.1 arcmin x 9.1 arcmin,这是在TIFR实验室中完全构思和设计的。CSU的几个部件,包括商业采购的压电步行器的控制器、使用数字游标卡尺的受控回路位置传感机构以及组装原型的低温测试设施,也在内部开发。CSU的原理包括将光谱仪的视场划分为连续和平行的空间带,每个空间带都与两个相对的滑动金属条相关联,可以定位这些金属条来创建对一个天文物体进行光谱观测所需的狭缝。建造了新设计的CSU的三狭缝原型,并在环境和低温下进行了广泛的测试。CSU的性能符合规范要求。
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引用次数: 1
The Synthesis Convolver 合成卷积器
IF 1.3 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-07-26 DOI: 10.1142/s225117172350006x
J. Bunton
A system, the synthesis convolver, is described that can process the output of an analysis filter bank and: • Reconstruct the analysis filter bank input signal, • Implement continuous convolution on the reconstructed signal, and • Resample the reconstructed signal to different sample rates. The synthesis convolver combines the capabilities of a synthesis filter bank and a continuous convolver. The synthesis convolver is based on earlier work but improves upon it, adding convolution and resampling. As well as reconstructing filterbank data, convolution allows dechirping of pulsar signals and resampling allows synthesized data to conform to the VLBI VDIF standard. The spectral overlap-add approach described, compared to earlier work, reduces errors and is more robust to channel gain errors. The system uses windows with smoothed or apodized edges, with the classical Tukey window being used previously. Here the Tukey window is generalized leading to a class of apodized windows. This class of windows is explored and one is found that is close to optimal in all conditions and can reduce errors by up to 40[Formula: see text]dB compared to an equivalent Tukey window. Achievable aliasing errors are lower than those of a standard polyphase synthesis filter bank. The synthesis convolver provides a high quality and versatile replacement for polyphase synthesis filter banks.
描述了一种系统,即合成卷积器,它可以处理分析滤波器组的输出,并:•重建分析滤波器组的输入信号,•对重建的信号进行连续卷积,以及•将重建的信号重新采样到不同的采样率。合成卷积器结合了合成滤波器组和连续卷积器的功能。合成卷积器是在早期工作的基础上改进的,增加了卷积和重采样。除了重建滤波器组数据外,卷积还可以对脉冲星信号进行解码,重新采样可以使合成数据符合VLBI VDIF标准。与先前的工作相比,所描述的频谱重叠添加方法减少了误差,并且对信道增益误差具有更强的鲁棒性。该系统使用平滑或apoapoed边缘的窗口,而传统的Tukey窗口被使用。在这里,Tukey窗被一般化,引申出一类离形窗。对这类窗口进行了探索,发现在所有条件下都接近最优,与等效的Tukey窗口相比,可以减少高达40 dB的误差。可实现的混叠误差低于标准多相合成滤波器组。合成卷积器为多相合成滤波器组提供了高质量和通用的替代品。
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引用次数: 0
Statistical Prediction of [CII] Observations by Constructing Probability density Functions using SOFIA, Herschel, and Spitzer Observations 利用SOFIA、Herschel和Spitzer观测构建概率密度函数对[CII]观测进行统计预测
IF 1.3 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-07-04 DOI: 10.1142/S2251171723500071
Youngchwa Seo, K. Willacy, U. Rebbapragada
We present a statistical algorithm for predicting the [CII] emission from Herschel and Spitzer continuum images using probability density functions between the [CII] emission and continuum emission. The [CII] emission at 158 $mu$m is a critical tracer in studying the life cycle of interstellar medium and galaxy evolution. Unfortunately, its frequency is in the far infrared (FIR), which is opaque through the troposphere and cannot be observed from the ground except for highly red-shifted sources (z $gtrsim$ 2). Typically [CII] observations of closer regions have been carried out using suborbital or space observatories. Given the high cost of these facilities and limited time availability, it is important to have highly efficient observations/operations in terms of maximizing science returns. This requires accurate prediction of the strength of emission lines and, therefore, the time required for their observation. However, [CII] emission has been hard to predict due to a lack of strong correlations with other observables. Here we adopt a new approach to making accurate predictions of [CII] emission by relating this emission simultaneously to several tracers of dust emission in the same region. This is done using a statistical methodology utilizing probability density functions (PDFs) among [CII] emission and Spitzer IRAC and Herschel PACS/SPIRE images. Our test result toward a star-forming region, RCW 120, demonstrates that our methodology delivers high-quality predictions with less than 30% uncertainties over 80% of the entire observation area, which is more than sufficient to test observation feasibility and maximize science return. The {it pickle} dump files storing the PDFs and trained neural network module are accessible upon request and will support future far-infrared missions, for example, GUSTO and FIR Probe.
我们提出了一种统计算法,用于使用[CI]发射和连续发射之间的概率密度函数预测Herschel和Spitzer连续图像的[CI]辐射。158$mu$m的[CII]发射是研究星际介质生命周期和星系演化的关键示踪剂。不幸的是,它的频率在远红外(FIR)中,远红外在对流层中是不透明的,除了高度红移的源(z$gtrsim$2)外,无法从地面观测到。通常,对较近区域的[CII]观测是使用亚轨道或空间天文台进行的。考虑到这些设施的高成本和有限的可用时间,在最大限度地提高科学回报方面,进行高效的观测/操作是很重要的。这需要精确预测发射线的强度,因此也需要精确预测观测发射线所需的时间。然而,由于缺乏与其他可观测值的强相关性,[CII]排放一直难以预测。在这里,我们采用了一种新的方法,通过将[CII]排放同时与同一地区的几个灰尘排放示踪剂联系起来,来准确预测[CII]的排放。这是使用一种统计方法来完成的,该方法利用[CII]发射、Spitzer IRAC和Herschel PACS/SPIRE图像中的概率密度函数(PDF)。我们对恒星形成区域RCW 120的测试结果表明,我们的方法在整个观测区域的80%范围内提供了不到30%的不确定性的高质量预测,这足以测试观测的可行性并最大限度地提高科学回报。存储PDF和经过训练的神经网络模块的转储文件可应要求访问,并将支持未来的远红外任务,例如GUSTO和FIR Probe。
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引用次数: 0
4K×4K CCD Imager for the 3.6m DOT: Recent up-gradations and results 4K×4K用于360万DOT的CCD成像仪:最近的升级和结果
IF 1.3 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2023-06-23 DOI: 10.1142/s2251171722400098
S. Pandey, Amit Kumar, B. Reddy, S. Yadav, N. Nanjappa, A. Aryan, Rahul Gupta, N. Panwar, R. Yadav
The 4K$times$4K CCD Imager is the first light instrument for the 3.6m Devasthal Optical Telescope and is producing broad-band imaging observations of many Galactic and extra-galactic sources since 2015-2016. Capabilities of the CCD Imager are demonstrated recently through several publications using the well-calibrated multi-band deep photometric results as expected from other similar facilities globally. In this article, we summarize some of the recent up-gradations made to improve the Imager, i.e., mounting the new filter wheel casing, replacing stray light baffles and discussing the fringe pattern corrections in redder filters. Some of the new science initiatives like galaxy-embedded faint point sources including WR stars and the observations of low surface brightness galaxy clusters are also discussed.
4K × 4K CCD成像仪是360米Devasthal光学望远镜的第一台光学仪器,自2015-2016年以来,它正在对许多银河系和星系外源进行宽带成像观测。CCD成像仪的功能最近通过一些出版物展示,这些出版物使用了校准良好的多波段深度光度测量结果,正如全球其他类似设施所期望的那样。在这篇文章中,我们总结了一些最近的升级,以改善成像仪,即安装新的滤光轮壳,更换杂散光挡板,并讨论了条纹图案校正在更红的过滤器。一些新的科学倡议,如星系嵌入的暗点源,包括WR星和低表面亮度星系团的观测也进行了讨论。
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Journal of Astronomical Instrumentation
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