Experimental Astronomy最新文献

{"title":"The discovery space of ELT-ANDES. Stars and stellar populations","authors":"Ian U. Roederer,&nbsp;Julián D. Alvarado-Gómez,&nbsp;Carlos Allende Prieto,&nbsp;Vardan Adibekyan,&nbsp;David S. Aguado,&nbsp;Pedro J. Amado,&nbsp;Eliana M. Amazo-Gómez,&nbsp;Martina Baratella,&nbsp;Sydney A. Barnes,&nbsp;Thomas Bensby,&nbsp;Lionel Bigot,&nbsp;Andrea Chiavassa,&nbsp;Armando Domiciano de Souza,&nbsp;J. I. González Hernández,&nbsp;Camilla Juul Hansen,&nbsp;Silva P. Järvinen,&nbsp;Andreas J. Korn,&nbsp;Sara Lucatello,&nbsp;Laura Magrini,&nbsp;Roberto Maiolino,&nbsp;Paolo Di Marcantonio,&nbsp;Alessandro Marconi,&nbsp;José R. De Medeiros,&nbsp;Alessio Mucciarelli,&nbsp;Nicolas Nardetto,&nbsp;Livia Origlia,&nbsp;Celine Peroux,&nbsp;Katja Poppenhäger,&nbsp;Ansgar Reiners,&nbsp;Cristina Rodríguez-López,&nbsp;Donatella Romano,&nbsp;Stefania Salvadori,&nbsp;Patrick Tisserand,&nbsp;Kim Venn,&nbsp;Gregg A. Wade,&nbsp;Alessio Zanutta","doi":"10.1007/s10686-024-09938-8","DOIUrl":"10.1007/s10686-024-09938-8","url":null,"abstract":"<div><p>The ArmazoNes high Dispersion Echelle Spectrograph (ANDES) is the optical and near-infrared high-resolution echelle spectrograph envisioned for the Extremely Large Telescope (ELT). We present a selection of science cases, supported by new calculations and simulations, where ANDES could enable major advances in the fields of stars and stellar populations. We focus on three key areas, including the physics of stellar atmospheres, structure, and evolution; stars of the Milky Way, Local Group, and beyond; and the star-planet connection. The key features of ANDES are its wide wavelength coverage at high spectral resolution and its access to the large collecting area of the ELT. These features position ANDES to address the most compelling questions and potentially transformative advances in stellar astrophysics of the decades ahead, including questions which cannot be anticipated today.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-04-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140586721","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Evaluation of the performance of a CdZnTe-based soft (gamma )-ray detector for CubeSat payloads","authors":"Kees de Kuijper,&nbsp;Rishank Diwan,&nbsp;Partha Sarathi Pal,&nbsp;Andreas Ritter,&nbsp;Pablo M. Saz Parkinson,&nbsp;Andy C. T. Kong,&nbsp;Quentin A. Parker","doi":"10.1007/s10686-024-09936-w","DOIUrl":"10.1007/s10686-024-09936-w","url":null,"abstract":"<div><p>The low-energy <span>(varvec{gamma })</span>-ray (0.1-30 MeV) sky has been relatively unexplored since the decommissioning of the COMPTEL instrument on the Compton Gamma-Ray Observatory (CGRO) satellite in 2000. However, the study of this part of the energy spectrum (the “MeV gap”) is crucial for addressing numerous unresolved questions in high-energy and multi-messenger astrophysics. Although several large MeV <span>(varvec{gamma })</span>-ray missions like AMEGO and e-ASTROGAM are being proposed, they are predominantly in the developmental phase, with launches not anticipated until the next decade at the earliest. In recent times, there has been a surge in proposed CubeSat missions as cost-effective and rapidly implementable “pathfinder” alternatives. A MeV CubeSat dedicated to <span>(varvec{gamma })</span>-ray astronomy has the potential to serve as a demonstrator for future, larger-scale MeV payloads. This paper presents a <span>(varvec{gamma })</span>-ray payload design featuring a CdZnTe crystal calorimeter module developed by IDEAS. We report the detailed results of simulations to assess the performance of this proposed payload and compare it with those of previous <span>(varvec{gamma })</span>-ray instruments.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-03-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-024-09936-w.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140199639","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The first cut is the cheapest: optimizing Athena/X-IFU-like TES detectors resolution by filter truncation","authors":"M. Teresa Ceballos,&nbsp;Nicolás Cardiel,&nbsp;Beatriz Cobo,&nbsp;Stephen J. Smith,&nbsp;Michael C. Witthoeft,&nbsp;Philippe Peille,&nbsp;Malcolm S. Durkin","doi":"10.1007/s10686-024-09930-2","DOIUrl":"10.1007/s10686-024-09930-2","url":null,"abstract":"<div><p>The X-ray Integral Field Unit (X-IFU) instrument on the future ESA mission Athena X-ray Observatory is a cryogenic micro-calorimeter array of Transition Edge Sensor (TES) detectors designed to provide spatially-resolved high-resolution spectroscopy. The onboard reconstruction software provides energy, spatial location and arrival time of incoming X-ray photons hitting the detector. A new processing algorithm based on a truncation of the classical optimal filter and called <i>0-padding</i>, has been recently proposed aiming to reduce the computational cost without compromising energy resolution. Initial tests with simple synthetic data displayed promising results. This study explores the slightly better performance of the <i>0-padding</i> filter and assess its final application to real data. The goal is to examine the larger sensitivity to instrumental conditions that was previously observed during the analysis of the simulations. This <i>0-padding</i> technique is thoroughly tested using more realistic simulations and real data acquired from NASA and NIST laboratories employing X-IFU-like TES detectors. Different fitting methods are applied to the data, and a comparative analysis is performed to assess the energy resolution values obtained from these fittings. The <i>0-padding</i> filter achieves energy resolutions as good as those obtained with standard filters, even with those of larger lengths, across different line complexes and instrumental conditions. This method proves to be useful for energy reconstruction of X-ray photons detected by the TES detectors provided proper corrections for baseline drift and jitter effects are applied. The finding is highly promising especially for onboard processing, offering efficiency in computational resources and facilitating the analysis of sources with higher count rates at high resolution.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-024-09930-2.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140199636","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Forward modelling low-spectral-resolution Cassini/CIRS observations of Titan","authors":"Lucy Wright,&nbsp;Nicholas A. Teanby,&nbsp;Patrick G. J. Irwin,&nbsp;Conor A. Nixon","doi":"10.1007/s10686-024-09934-y","DOIUrl":"10.1007/s10686-024-09934-y","url":null,"abstract":"<div><p>The Composite InfraRed Spectrometer (CIRS) instrument onboard the Cassini spacecraft performed 8.4 million spectral observations of Titan at resolutions between 0.5–15.5 cm<span>(^{varvec{-1}})</span>. More than 3 million of these were acquired at a low spectral resolution (SR) (13.5–15.5 cm<span>(^{varvec{-1}})</span>), which have excellent spatial and temporal coverage in addition to the highest spatial resolution and lowest noise per spectrum of any of the CIRS observations. Despite this, the CIRS low-SR dataset is currently underused for atmospheric composition analysis, as spectral features are often blended and subtle compared to those in higher SR observations. The vast size of the dataset also poses a challenge as an efficient forward model is required to fully exploit these observations. Here, we show that the CIRS FP3/4 nadir low-SR observations of Titan can be accurately forward modelled using a computationally efficient correlated-<span>(varvec{k})</span> method. We quantify wavenumber-dependent forward modelling errors, with mean 0.723 nW cm<span>(^{varvec{-2}},)</span>sr<span>(^{varvec{-1}})</span>/cm<span>(^{varvec{-1}})</span> (FP3: 600–890 cm<span>(^{varvec{-1}})</span>) and 0.248 nW cm<span>(^{varvec{-2}},)</span>sr<span>(^{varvec{-1}},)</span>/ cm<span>(^{varvec{-1}})</span> (FP4: 1240–1360 cm<span>(^{varvec{-1}})</span>), that can be used to improve the rigour of future retrievals. Alternatively, in cases where more accuracy is required, we show observations can be forward modelled using an optimised line-by-line method, significantly reducing computation time.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-024-09934-y.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140199563","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Outdoor fibre link between two telescopes and the lab of the CHARA array at 810 nm. Demonstration of the optical path servo control","authors":"Magri Julie,&nbsp;Grossard Ludovic,&nbsp;Reynaud François,&nbsp;Fabert Marc,&nbsp;Delage Laurent,&nbsp;Krawczyk Rodolphe,&nbsp;Le Duigou Jean-Michel","doi":"10.1007/s10686-024-09935-x","DOIUrl":"10.1007/s10686-024-09935-x","url":null,"abstract":"<div><p>In the framework of the ALOHA (Astronomical Light Optical Hybrid Analysis) project, dedicated to high resolution imaging in the L-band using optical fibre and nonlinear optics, we have implemented a servo controlled hectometric outdoor fibre link between two telescopes and the recombination beam facility of the CHARA telescope array. A two-stage servo system using optical fibre modulator, fibre delay line, and a metrology laser at 1064 nm allows to stabilise the optical path difference within 3 nm RMS over a 3000 s record. Using an internal source at 810 nm, the signal-to-noise ratio of the fringe modulation peak is enhanced by a factor better than two when the servo control is switched on. This study can be also considered as a seminal work towards very long base fibre linked telescope arrays and allows to scale the perturbative environment of an outdoor fibre link.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-03-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140126401","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"How many random observations are needed for good phase coverage of a periodic source?","authors":"Chris Koen","doi":"10.1007/s10686-024-09931-1","DOIUrl":"10.1007/s10686-024-09931-1","url":null,"abstract":"<div><p>The specific problem considered is the number of radial velocity measurements required to obtain good estimates of physical parameters of binary star. It is assumed that observations are made at random binary phases. The loss of information due to poor phase coverage is explored, and a suggested limit on the largest acceptable gap introduced. The statistical distribution of maximum gap lengths can then be used to specify the minimum number of velocity measurements to obtain good phase coverage with a specified confidence limit. The effects of non-zero orbital eccentricity are discussed, as are the ramifications of having multiple binary targets. The theory is also applicable to the characterisation of the radial velocity curves induced by exoplanets on their host stars, provided that the periods and eccentricities are known (from e.g. transit observations).</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-03-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-024-09931-1.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140097359","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Modeling the effects of power efficient approximate multipliers in radio astronomy correlators","authors":"A. B. J. Kokkeler,&nbsp;G. A. Gillani,&nbsp;A. J. Boonstra","doi":"10.1007/s10686-024-09921-3","DOIUrl":"10.1007/s10686-024-09921-3","url":null,"abstract":"<div><p>Large scale Radio Telescopes for Radio Astronomy highly depend on the availability of large (digital) processing capacities for imaging. Estimates concerning power efficiency for future Radio Telescopes lead to anticipated power consumption numbers beyond feasibility. To reduce the power budget, the use of approximate multipliers within the correlator is explored. A baseband equivalent executable model of a radio synthesis telescope is constructed to assess the effects of approximate multipliers. Besides ideal multipliers with floating point accuracy, the use of accurate 8-bit multipliers and 4 different types of approximate multipliers is explored. For each of these multipliers, the energy efficiency of an individual multiplier is known and used to determine the energy efficiency improvement of a correlator when using approximate multipliers. The effects of approximation are quantified by 3 metrics (Signal-to-Noise-Ratio (SNR), Spurious-Free-Dynamic-Range (SFDR) and Root-Mean-Square (RMS) level) derived from maps constructed by the executable model based on an empty sky with only a single point source. This is considered to be the worst case scenario. For illustration purposes, a more realistic input is processed by the model as well. The metrics have been determined based on different SNR levels at the input of each antenna element. For input SNR levels up to 10 dB, all types of approximate multipliers used in this paper can be exploited to improve energy efficiency of correlators, leading to a maximum energy reduction of 19 %. For input SNR values up to 30 dB an energy improvement up to 12 % can be achieved. These percentages are based on implementations in a 40nm low power IC technology at 1 GHz.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-03-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-024-09921-3.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140056563","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Ground calibration result of the Lobster Eye Imager for Astronomy","authors":"Huaqing Cheng,&nbsp;Zhixing Ling,&nbsp;Chen Zhang,&nbsp;Xiaojin Sun,&nbsp;Shengli Sun,&nbsp;Yuan Liu,&nbsp;Yanfeng Dai,&nbsp;Zhenqing Jia,&nbsp;Haiwu Pan,&nbsp;Wenxin Wang,&nbsp;Donghua Zhao,&nbsp;Yifan Chen,&nbsp;Zhiwei Cheng,&nbsp;Wei Fu,&nbsp;Yixiao Han,&nbsp;Junfei Li,&nbsp;Zhengda Li,&nbsp;Xiaohao Ma,&nbsp;Yulong Xue,&nbsp;Ailiang Yan,&nbsp;Qiang Zhang,&nbsp;Yusa Wang,&nbsp;Xiongtao Yang,&nbsp;Zijian Zhao,&nbsp;Weimin Yuan","doi":"10.1007/s10686-024-09932-0","DOIUrl":"10.1007/s10686-024-09932-0","url":null,"abstract":"<div><p>We report on results of the on-ground X-ray calibration of the Lobster Eye Imager for Astronomy (LEIA), an experimental space wide-field (18.6 <span>(times )</span> 18.6 square degrees) X-ray telescope built from novel lobster eye micro-pore optics. LEIA was successfully launched on July 27, 2022 onboard the SATech-01 satellite. To achieve full characterisation of its performance before launch, a series of tests and calibrations have been carried out at different levels of devices, assemblies and the complete module. In this paper, we present the results of the end-to-end calibration campaign of the complete module carried out at the 100-m X-ray Test Facility at the Institute of High-energy Physics, Chinese Academy of Sciences (CAS). The Point Spread Function (PSF), effective area and energy response of the detectors were measured in a wide range of incident directions at several characteristic X-ray line energies. Specifically, the distributions of the PSF and effective areas are roughly uniform across the FoV, in large agreement with the prediction of lobster-eye optics. The mild variations and deviations from the prediction of idealized, perfect lobster-eye optics can be understood to be caused by the imperfect shapes and alignment of the micro-pores as well as the obscuration of incident photons by the supporting frames, which can be well reproduced by Monte Carlo simulations. The spatial resolution of LEIA defined by the full width at half maximum (FWHM) of the focal spot ranges from <span>(textbf{4})</span> to <span>(textbf{8})</span> arc minutes with a median of <span>(mathbf{5.7})</span> arcmin. The measured effective areas are in range of <span>(mathbf{2-3}~mathbf {cm^2})</span> at <span>(mathbf{sim })</span>1.25 keV across the entire FoV, and its dependence on photon energy is also in large agreement with simulations. The gains of the four complementary metal-oxide semiconductor (CMOS) sensors are in range of <span>(mathbf{6.5-6.9}~mathbf {eV/DN})</span>, and the energy resolutions in the range of <span>(mathbf{sim 120 - 140})</span> eV at <span>(mathbf{1.25})</span> keV and <span>(mathbf{sim 170-190})</span> eV at <span>(mathbf{4.5})</span> keV. These calibration results have been ingested into the first version of calibration database (CALDB) and applied to the analysis of the scientific data acquired by LEIA. This work paves the way for the calibration of the Wide-field X-Ray Telescope (WXT) flight model modules of the Einstein Probe (EP) mission.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-03-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140056565","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Improvements in digital meteor spectra reduction","authors":"Marko Šegon,&nbsp;Vlastimil Vojáček,&nbsp;Jiří Borovička","doi":"10.1007/s10686-024-09933-z","DOIUrl":"10.1007/s10686-024-09933-z","url":null,"abstract":"<div><p>This study addresses the complexity and importance of developing a method of calibrating digital observations of meteor spectra with all-sky cameras. It aims to present novel approaches to spectral sensitivity, atmospheric extinction and flat-field corrections. Images of a known line emission spectrum were captured at various positions within the field of view using a camera with a fish-eye lens and plastic holographic grating. The flat-field correction was separated into a wavelength-independent and wavelength-dependent component, both dependent on the position of the spectral line in the field of view (FoV). Total profile intensities of spectra obtained from the images were compared throughout the spectral range at different positions in the FoV. The flat-field was constructed by fitting those dependencies with high-degree polynomial functions. Using a simplified atmospheric model, a novel approach was constructed to determine the atmospheric extinction curve throughout the spectral range, allowing it to be separately considered from the spectral sensitivity which was previously not the case. A comparison of the newly developed and previously used methodology was tested on several meteor spectra of the same meteor captured from different stations of the European Fireball Network. It revealed a significantly improved correspondence of the analysed spectra in the part of the spectral range unaffected by the limitations imposed by the newly developed methodology. Failing to follow the correct calibration methodology precisely may introduce varying degrees of uncertainty in computations of elemental abundances and other physical properties, depending on the equipment’s specific effect magnitude.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-03-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-024-09933-z.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140045830","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Design and characterization of a 90 GHz CMB TES bolometer","authors":"Yu Xu,&nbsp;Zhengwei Li,&nbsp;Yongping Li,&nbsp;Yifei Zhang,&nbsp;Xufang Li,&nbsp;Xuefeng Lu,&nbsp;Guofu Liao,&nbsp;Qingchen Li,&nbsp;Fangjun Lu,&nbsp;Laiyu Zhang,&nbsp;Yudong Gu,&nbsp;Zhouhui Liu,&nbsp;Shibo Shu,&nbsp;Zhi Chang,&nbsp;Guofeng Wang,&nbsp;Yongjie Zhang,&nbsp;He Gao,&nbsp;Aimei Zhang,&nbsp;Daikang Yan,&nbsp;Congzhan Liu","doi":"10.1007/s10686-024-09927-x","DOIUrl":"10.1007/s10686-024-09927-x","url":null,"abstract":"<div><p>The transition-edge sensor (TES) as a type of low-temperature superconducting detector offers superior sensitivity due to its low thermal noise. In this work, we present a prototype TES bolometer designed for cosmic microwave background (CMB) polarization measurements. This TES is made of aluminum doped with a low concentration of manganese (2000 ppm by atomic percentage), and is deposited on the SiNx membrane which connects to the silicon substrate via narrow legs. In order to calculate its electrothermal parameters we have performed dark characterizations, which include measuring voltage-current (IV) curve at different bath temperatures, square-wave time response at various bias voltages, and noise level. This TES bolometer shows a noise equivalent power (NEP) of about <span>(5times 10^{-17})</span> W/<span>(sqrt{textrm{Hz}})</span>, which meets the requirement of CMB observation. However, its saturation power is smaller and time constant is larger than what are expected. We have analyzed the reasons and will make corresponding improvements in our future work.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 2","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-03-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140019868","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}