M. Farris, M. Zandian, L. Fischer, Sam R. Hoffman, Luis Gordillo, W. Strong, Dennis E. Edwall, E. Arkun, A. Chen, Eric Holland, M. Carmody, J. Auyeung, J. Beletic
The Hawaii-4RG-15 (H4RG-15) Sensor Chip Assembly (SCA) is a 4096×4096 pixel sensor with 15 µm pixel pitch. The H4RG-15 is the newest SCA developed by Teledyne for low light level astronomical applications, providing larger format while retaining the low noise and low power of the H1RG and H2RG arrays with additional new features. The SCAs are currently being produced with mercury cadmium telluride (HgCdTe or MCT) detectors having cutoff wavelengths of 1.7 µm for near-infrared (NIR) and 2.5 µm for short-wave infrared (SWIR) applications. SCAs can also be produced with 5.3 µm cutoff wavelength for mid-wave infrared (MWIR) or optimized for visible only applications with hybrid silicon (HyViSI) detectors. Several science grade detectors have been delivered for use in new astronomical instruments. The H4RG-15 sensor has been developed to enable assembly of mosaics with high pixel fill factor, with a new package design that improves the butt-ability of the SCAs. The new package achieves a high level of flatness and is also appropriate for space flight missions, with assembly using flight qualifiable components.
{"title":"Update on the status of H4RG-15 SCA production and testing at Teledyne imaging sensors (Conference Presentation)","authors":"M. Farris, M. Zandian, L. Fischer, Sam R. Hoffman, Luis Gordillo, W. Strong, Dennis E. Edwall, E. Arkun, A. Chen, Eric Holland, M. Carmody, J. Auyeung, J. Beletic","doi":"10.1117/12.2312222","DOIUrl":"https://doi.org/10.1117/12.2312222","url":null,"abstract":"The Hawaii-4RG-15 (H4RG-15) Sensor Chip Assembly (SCA) is a 4096×4096 pixel sensor with 15 µm pixel pitch. The H4RG-15 is the newest SCA developed by Teledyne for low light level astronomical applications, providing larger format while retaining the low noise and low power of the H1RG and H2RG arrays with additional new features. The SCAs are currently being produced with mercury cadmium telluride (HgCdTe or MCT) detectors having cutoff wavelengths of 1.7 µm for near-infrared (NIR) and 2.5 µm for short-wave infrared (SWIR) applications. SCAs can also be produced with 5.3 µm cutoff wavelength for mid-wave infrared (MWIR) or optimized for visible only applications with hybrid silicon (HyViSI) detectors. Several science grade detectors have been delivered for use in new astronomical instruments. The H4RG-15 sensor has been developed to enable assembly of mosaics with high pixel fill factor, with a new package design that improves the butt-ability of the SCAs. The new package achieves a high level of flatness and is also appropriate for space flight missions, with assembly using flight qualifiable components.","PeriodicalId":359588,"journal":{"name":"High Energy, Optical, and Infrared Detectors for Astronomy VIII","volume":"49 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2018-07-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"129670934","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
D. Hall, I. Baker, Vincent Isgar, S. Jacobson, H. Weller
With gain-normalized dark currents reduced below 10 e-/s/pixel, HgCdTe Avalanche Photo-Diode arrays operated in linear mode are now widely accepted as the sensors of choice for adaptive optics wavefront sensing of natural guide stars in the wavelength range 1 to 2.5 um. At lower temperatures the intrinsic dark currents in Leonardo’s SAPHIRA 320 x 256 @ 24um pitch arrays have recently been shown to be four orders of magnitude lower, approaching 0.001 e-/s/pixel. This has opened the way to megapixel class APD arrays offering major advantages for a wide range of low background astronomical observations. We report the status of development of a 1k x 1k @ 15um pixel Read-Out Integrated Circuit (ROIC) for a three-side close-buttable, 16 output, MOVPE HgCdTe array with reference pixels and reference outputs. The design has been optimized for minimum ROIC glow following a detailed investigation of glow sources in the SAPHIRA ME1001 ROIC. This involved precisely overlaying J-band glow images on layout drawings from EDA software to identify all the sources of glow. As of the time of submission of this abstract, the Architecture definition is in its third iteration and the program is on track to produce ROICs around mid-2018. In parallel, Mark 20 SAPHIRAs optimized for very low background operation with the goal of delaying the onset of tunnel-tunnel current to bias voltages producing useful avalanche gain are being characterized along with modified SAPHIRAs with 15um pixels.
随着增益归一化暗电流降低到10 e-/s/像素以下，在线性模式下工作的HgCdTe雪崩光电二极管阵列现在被广泛接受为波长范围为1至2.5 um的自然导星自适应光学波前传感的首选传感器。在较低的温度下，莱昂纳多的sapira 320 x 256 @ 24um间距阵列中的固有暗电流最近被证明降低了四个数量级，接近0.001 e-/s/像素。这为百万像素级APD阵列开辟了道路，为广泛的低背景天文观测提供了主要优势。我们报告了一种1k x 1k @ 15um像素读出集成电路(ROIC)的开发现状，该电路用于具有参考像素和参考输出的三面闭合可开关，16输出，MOVPE HgCdTe阵列。在详细研究了SAPHIRA ME1001 ROIC中的发光源后，该设计已优化为最小ROIC辉光。这包括将j波段辉光图像精确地覆盖在EDA软件的布局图上，以识别所有的辉光源。在提交此摘要时，架构定义处于第三次迭代中，该计划将在2018年中期左右生成roic。与此同时，针对低背景工作优化的Mark 20 safiras，其目标是将隧道-隧道电流的开始延迟到偏置电压，从而产生有用的雪崩增益，与15um像素的改进safiras一起进行了表征。
{"title":"A megapixel class HgCdTe linear mode avalanche photo-diode array for low background astronomy (Conference Presentation)","authors":"D. Hall, I. Baker, Vincent Isgar, S. Jacobson, H. Weller","doi":"10.1117/12.2314897","DOIUrl":"https://doi.org/10.1117/12.2314897","url":null,"abstract":"With gain-normalized dark currents reduced below 10 e-/s/pixel, HgCdTe Avalanche Photo-Diode arrays operated in linear mode are now widely accepted as the sensors of choice for adaptive optics wavefront sensing of natural guide stars in the wavelength range 1 to 2.5 um. At lower temperatures the intrinsic dark currents in Leonardo’s SAPHIRA 320 x 256 @ 24um pitch arrays have recently been shown to be four orders of magnitude lower, approaching 0.001 e-/s/pixel. This has opened the way to megapixel class APD arrays offering major advantages for a wide range of low background astronomical observations.\u0000We report the status of development of a 1k x 1k @ 15um pixel Read-Out Integrated Circuit (ROIC) for a three-side close-buttable, 16 output, MOVPE HgCdTe array with reference pixels and reference outputs. The design has been optimized for minimum ROIC glow following a detailed investigation of glow sources in the SAPHIRA ME1001 ROIC. This involved precisely overlaying J-band glow images on layout drawings from EDA software to identify all the sources of glow.\u0000As of the time of submission of this abstract, the Architecture definition is in its third iteration and the program is on track to produce ROICs around mid-2018. In parallel, Mark 20 SAPHIRAs optimized for very low background operation with the goal of delaying the onset of tunnel-tunnel current to bias voltages producing useful avalanche gain are being characterized along with modified SAPHIRAs with 15um pixels.","PeriodicalId":359588,"journal":{"name":"High Energy, Optical, and Infrared Detectors for Astronomy VIII","volume":"19 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2018-07-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"121071947","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{"title":"Calibrating gain, uniformity, linearity and noise of CCDs in the presence of the brighter-fatter effect (Conference Presentation)","authors":"D. Weatherill","doi":"10.1117/12.2313425","DOIUrl":"https://doi.org/10.1117/12.2313425","url":null,"abstract":"","PeriodicalId":359588,"journal":{"name":"High Energy, Optical, and Infrared Detectors for Astronomy VIII","volume":"28 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2018-07-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"124133154","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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