We installed a new Band10 receiver cartridge (790 − 940 GHz) on ASTE and carried out its Commissioning and Science Verification. We repeated observations toward IRC+10216 with HCN maser line (1110)-(0400), J=10-9, determined the cartridge-specific offsets of sub-reflector position and telescope pointing, and then, obtained beam patterns. The beam size was estimated to be 10.9″ × 10.0″ from the beam patterns. For science verification, we performed observations of an 8′ × 4′ area around Orion-KL of the Orion Molecular Cloud 1 region with CO (J=7-6) line in the on-the-fly method, verified that our images were consistent with past results, and confirmed the capability of ASTE Band10 observations toward bright and extended objects like Giant Molecular Clouds.
{"title":"ASTE BAND10 commissioning and science verification","authors":"T. Kamazaki, S. Ishii, Andrea Silva, S. Asayama","doi":"10.1117/12.2561968","DOIUrl":"https://doi.org/10.1117/12.2561968","url":null,"abstract":"We installed a new Band10 receiver cartridge (790 − 940 GHz) on ASTE and carried out its Commissioning and Science Verification. We repeated observations toward IRC+10216 with HCN maser line (1110)-(0400), J=10-9, determined the cartridge-specific offsets of sub-reflector position and telescope pointing, and then, obtained beam patterns. The beam size was estimated to be 10.9″ × 10.0″ from the beam patterns. For science verification, we performed observations of an 8′ × 4′ area around Orion-KL of the Orion Molecular Cloud 1 region with CO (J=7-6) line in the on-the-fly method, verified that our images were consistent with past results, and confirmed the capability of ASTE Band10 observations toward bright and extended objects like Giant Molecular Clouds.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"9 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"128739710","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}
We present three Monte Carlo models for the propagation of athermal phonons in the diamond absorber of a composite semiconducting bolometer `Bolo 184'. Previous measurements of the response of this bolometer to impacts by $alpha$ particles show a strong dependence on the location of particle incidence, and the shape of the response function is determined by the propagation and thermalisation of athermal phonons. The specific mechanisms of athermal phonon propagation at this time were undetermined, and hence we have developed three models for probing this behaviour by attempting to reproduce the statistical features seen in the experimental data. The first two models assume a phonon thermalisation length determined by a mean free path $lambda$, where the first model assumes that phonons thermalise at the borders of the disc (with a small $lambda$) and the second assumes that they reflect (with a $lambda$ larger than the size of the disc). The third model allows athermal photons to propagate along their geometrical line of sight (similar to ray optics), gradually losing energy. We find that both the reflective model and the geometrical model reproduce the features seen in experimental data, whilst the model assuming phonon thermalisation at the disc border produces unrealistic results. There is no significant dependence on directionality of energy absorption in the geometrical model, and in the schema of this thin crystalline diamond, a reflective absorber law and a geometrical law both produce consistent results.
{"title":"Simulations of athermal phonon propagation in a cryogenic semiconducting bolometer","authors":"S. Stever, F. Couchot, B. Maffei","doi":"10.1117/12.2561969","DOIUrl":"https://doi.org/10.1117/12.2561969","url":null,"abstract":"We present three Monte Carlo models for the propagation of athermal phonons in the diamond absorber of a composite semiconducting bolometer `Bolo 184'. Previous measurements of the response of this bolometer to impacts by $alpha$ particles show a strong dependence on the location of particle incidence, and the shape of the response function is determined by the propagation and thermalisation of athermal phonons. The specific mechanisms of athermal phonon propagation at this time were undetermined, and hence we have developed three models for probing this behaviour by attempting to reproduce the statistical features seen in the experimental data. The first two models assume a phonon thermalisation length determined by a mean free path $lambda$, where the first model assumes that phonons thermalise at the borders of the disc (with a small $lambda$) and the second assumes that they reflect (with a $lambda$ larger than the size of the disc). The third model allows athermal photons to propagate along their geometrical line of sight (similar to ray optics), gradually losing energy. We find that both the reflective model and the geometrical model reproduce the features seen in experimental data, whilst the model assuming phonon thermalisation at the disc border produces unrealistic results. There is no significant dependence on directionality of energy absorption in the geometrical model, and in the schema of this thin crystalline diamond, a reflective absorber law and a geometrical law both produce consistent results.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"142 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"124516215","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}
Sara Salem Hesari, D. Henke, V. Reshetov, F. Jiang, A. Seyfollahi, L. Knee, L. Baker, J. Bornemann, D. Chalmers
A compact front-end system is presented for a dual-linear polarization cryogenic Q-band receiver. This receiver will be used to demonstrate the high frequency performance of the Dish Verification Antenna 2 (DVA-2) composite reflector telescope between 35–50 GHz and is a technology demonstrator with possible application to the National Radio Astronomy Observatory’s Next Generation Very Large Array (ngVLA). A vacuum vessel and a two-stage Gifford-McMahon cryopump system are used for the cryogenic environment. The second stage of the cryostat is cooled to 16 K and includes a small choke ring feed horn, a low-loss noise calibration module (NCM) integrated with orthogonal mode transducer (OMT), and two cryogenically cooled mHEMT MMIC low-noise amplifiers (LNAs). Using a noise diode as the noise source on the 300 K stage inside the cryostat helps to protect the cooled components from signals outside of the cryostat, and also lessen the heat on the second stage since a noise diode normally produce a power dissipation of several hundred mW. The OMT design is an optimized version of the design used in the ALMA Band 1 cartridge with two integrated directional couplers and excellent performance. The cascaded noise analysis of the receiver shows a receiver noise temperature of 19.4 K.
提出了一种紧凑的双线偏振低温q波段接收机前端系统。该接收器将用于演示碟形验证天线2 (DVA-2)复合反射镜望远镜在35-50 GHz之间的高频性能，并且是可能应用于国家射电天文台下一代甚大阵列(ngVLA)的技术演示。真空容器和两级吉福德-麦克马洪低温泵系统用于低温环境。低温恒温器的第二级冷却至16 K，包括一个小扼流环馈电喇叭，一个与正交模式传感器(OMT)集成的低损耗噪声校准模块(NCM)，以及两个低温冷却的mHEMT MMIC低噪声放大器(LNAs)。在低温恒温器内部的300k级上使用噪声二极管作为噪声源有助于保护冷却组件免受低温恒温器外部信号的影响，并且还可以减少第二级的热量，因为噪声二极管通常会产生数百mW的功耗。OMT设计是ALMA Band 1中使用的设计的优化版本，具有两个集成定向耦合器，性能优异。接收机的级联噪声分析表明，接收机噪声温度为19.4 K。
{"title":"Q-band receiver system design for the Canadian DVA-2 radio telescope","authors":"Sara Salem Hesari, D. Henke, V. Reshetov, F. Jiang, A. Seyfollahi, L. Knee, L. Baker, J. Bornemann, D. Chalmers","doi":"10.1117/12.2562751","DOIUrl":"https://doi.org/10.1117/12.2562751","url":null,"abstract":"A compact front-end system is presented for a dual-linear polarization cryogenic Q-band receiver. This receiver will be used to demonstrate the high frequency performance of the Dish Verification Antenna 2 (DVA-2) composite reflector telescope between 35–50 GHz and is a technology demonstrator with possible application to the National Radio Astronomy Observatory’s Next Generation Very Large Array (ngVLA). A vacuum vessel and a two-stage Gifford-McMahon cryopump system are used for the cryogenic environment. The second stage of the cryostat is cooled to 16 K and includes a small choke ring feed horn, a low-loss noise calibration module (NCM) integrated with orthogonal mode transducer (OMT), and two cryogenically cooled mHEMT MMIC low-noise amplifiers (LNAs). Using a noise diode as the noise source on the 300 K stage inside the cryostat helps to protect the cooled components from signals outside of the cryostat, and also lessen the heat on the second stage since a noise diode normally produce a power dissipation of several hundred mW. The OMT design is an optimized version of the design used in the ALMA Band 1 cartridge with two integrated directional couplers and excellent performance. The cascaded noise analysis of the receiver shows a receiver noise temperature of 19.4 K.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"135 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"122565382","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}
N. Cothard, Aamir Ali, J. Austermann, Steve K. Choi, K. Crowley, B. Dober, C. Duell, S. Duff, P. Gallardo, G. Hilton, S. Ho, J. Hubmayr, M. Niemack, Rita F. Sonka, S. Staggs, E. Vavagiakis, Edward J. Wollack, Zhilei Xu
The Simons Observatory (SO) will perform ground-based observations of the cosmic microwave background (CMB) with several small and large aperture telescopes, each outfitted with thousands to tens of thousands of superconducting aluminum manganese (AlMn) transition-edge sensor bolometers (TESs). In-situ characterization of TES responsivities and effective time constants will be required multiple times each observing-day for calibrating time-streams during CMB map-making. Effective time constants are typically estimated in the field by briefly applying small amplitude square-waves on top of the TES DC biases, and fitting exponential decays in the bolometer response. These so-called "bias step" measurements can be rapidly implemented across entire arrays and therefore are attractive because they take up little observing time. However, individual detector complex impedance measurements, while too slow to implement during observations, can provide a fuller picture of the TES model and a better understanding of its temporal response. Here, we present the results of dark TES characterization of many prototype SO bolometers and compare the effective thermal time constants measured via bias steps to those derived from complex impedance data.
{"title":"Comparing complex impedance and bias step measurements of Simons Observatory transition edge sensors","authors":"N. Cothard, Aamir Ali, J. Austermann, Steve K. Choi, K. Crowley, B. Dober, C. Duell, S. Duff, P. Gallardo, G. Hilton, S. Ho, J. Hubmayr, M. Niemack, Rita F. Sonka, S. Staggs, E. Vavagiakis, Edward J. Wollack, Zhilei Xu","doi":"10.1117/12.2575912","DOIUrl":"https://doi.org/10.1117/12.2575912","url":null,"abstract":"The Simons Observatory (SO) will perform ground-based observations of the cosmic microwave background (CMB) with several small and large aperture telescopes, each outfitted with thousands to tens of thousands of superconducting aluminum manganese (AlMn) transition-edge sensor bolometers (TESs). In-situ characterization of TES responsivities and effective time constants will be required multiple times each observing-day for calibrating time-streams during CMB map-making. Effective time constants are typically estimated in the field by briefly applying small amplitude square-waves on top of the TES DC biases, and fitting exponential decays in the bolometer response. These so-called \"bias step\" measurements can be rapidly implemented across entire arrays and therefore are attractive because they take up little observing time. However, individual detector complex impedance measurements, while too slow to implement during observations, can provide a fuller picture of the TES model and a better understanding of its temporal response. Here, we present the results of dark TES characterization of many prototype SO bolometers and compare the effective thermal time constants measured via bias steps to those derived from complex impedance data.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"46 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"126086516","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}
Jose Alberto Rubino Martin, P. Arias, R. Hoyland, M. Aguiar-González, Javier De Miguel Hernandez, R. Génova-Santos, M. F. Gómez-Reñasco, F. Guidi, Patricia Fernández-Izquierdo, M. Fernández-Torreiro, Pablo A. Fuerte Rodriguez, C. Hernandez-Monteagudo, C. López-Caraballo, A. P. D. Taoro, M. Peel, R. Rebolo, Antonio Zamora-Jimenez, Eduardo D. González Carretero, C. Colodro-Conde, Cristina Pérez-Lemus, R. Toledo-Moreo, David Pérez-Lizán, F. Cuttaia, L. Terenzi, C. Franceschet, S. Realini, J. Chluba, Gaizka Murga-Llano, Ruben Sanquirce Garcia
{"title":"The Tenerife Microwave Spectrometer (TMS) experiment: studying the absolute spectrum of the sky emission in the 10-20GHz range","authors":"Jose Alberto Rubino Martin, P. Arias, R. Hoyland, M. Aguiar-González, Javier De Miguel Hernandez, R. Génova-Santos, M. F. Gómez-Reñasco, F. Guidi, Patricia Fernández-Izquierdo, M. Fernández-Torreiro, Pablo A. Fuerte Rodriguez, C. Hernandez-Monteagudo, C. López-Caraballo, A. P. D. Taoro, M. Peel, R. Rebolo, Antonio Zamora-Jimenez, Eduardo D. González Carretero, C. Colodro-Conde, Cristina Pérez-Lemus, R. Toledo-Moreo, David Pérez-Lizán, F. Cuttaia, L. Terenzi, C. Franceschet, S. Realini, J. Chluba, Gaizka Murga-Llano, Ruben Sanquirce Garcia","doi":"10.1117/12.2561309","DOIUrl":"https://doi.org/10.1117/12.2561309","url":null,"abstract":"","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"384 ","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"120879721","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}
Mona Mirzaei, E. Barrentine, B. Bulcha, G. Cataldo, J. Connors, N. Ehsan, T. Essinger-Hileman, L. Hess, S. Moseley, J. Mugge-Durum, O. Noroozian, S. Rodriguez, T. Stevenson, E. Switzer, C. Volpert, Edward J. Wollack
The EXperiment for Cryogenic Large-aperture Intensity Mapping (EXCLAIM) is a cryogenic balloon-borne experiment that will map CO and [CII] line emissions across redshifts from 0 to 3.5. The focal plane will feature six µ-Spec spectrometers. µ-Spec is an integrated grating-analog spectrometer, which uses a superconducting Nb microstrip transmission line on single-crystal Si dielectric to introduce the required phase gradients, and Microwave Kinetic Inductance Detectors (MKIDs). The spectrometers will operate from 420-540 GHz with a resolution R = λ/Δλ = 512. We report the status of spectrometers under development for EXCLAIM, including the design, fabrication development and steps, and preliminary measurements.
{"title":"µ-spec spectrometers for the EXCLAIM instrument","authors":"Mona Mirzaei, E. Barrentine, B. Bulcha, G. Cataldo, J. Connors, N. Ehsan, T. Essinger-Hileman, L. Hess, S. Moseley, J. Mugge-Durum, O. Noroozian, S. Rodriguez, T. Stevenson, E. Switzer, C. Volpert, Edward J. Wollack","doi":"10.1117/12.2562446","DOIUrl":"https://doi.org/10.1117/12.2562446","url":null,"abstract":"The EXperiment for Cryogenic Large-aperture Intensity Mapping (EXCLAIM) is a cryogenic balloon-borne experiment that will map CO and [CII] line emissions across redshifts from 0 to 3.5. The focal plane will feature six µ-Spec spectrometers. µ-Spec is an integrated grating-analog spectrometer, which uses a superconducting Nb microstrip transmission line on single-crystal Si dielectric to introduce the required phase gradients, and Microwave Kinetic Inductance Detectors (MKIDs). The spectrometers will operate from 420-540 GHz with a resolution R = λ/Δλ = 512. We report the status of spectrometers under development for EXCLAIM, including the design, fabrication development and steps, and preliminary measurements.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"23 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"127167200","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}
Y. Yamasaki, S. Masui, Masanari Okawa, Koki Yokoyama, Taisei Minami, Shota Ueda, Yutaka Hasegawa, A. Nishimura, T. Onishi, H. Ogawa, N. Okada, K. Kimura, Álvaro González, T. Kojima, K. Kaneko, R. Sakai
Currently, we are performing a large-scale survey of molecular clouds toward the Galactic Plane in 12CO, 13CO, and C18O(J = 2–1) with the 1.85-m mm-submm telescope from Nobeyama Radio Observatory. In addition, we are proceeding with the preparation of a new project to observe several additional molecular lines including higher transitions of CO isotopes, such as 12CO, 13CO, and C18O(J = 2–1, 3–2) simultaneously with a wideband receiver (210–375 GHz). The optics has a Cassegrain reflector antenna with Nasmyth beam-waveguide feed and is composed of Main-reflector, Sub-reflector, ellipsoidal mirrors, and plane mirrors. New wideband optics will be required to achieve this goal. In order to accomplish the optics, we have designed a corrugated horn with a fractional bandwidth of ∼56 %, and frequency independent optics to couple the beam from the telescope onto the horn. The corrugated horn has a conical profile and the variable corrugation depth. It has been optimized by using CHAMP, our targeting return loss of better than −20 dB, cross-polarization loss of better than −25 dB, and far-field good radiation pattern. The simulation of the corrugated horn results in low return loss, low crosspolarization, and symmetric beam pattern in that frequency band. The simulated aperture efficiency of the designed receiver optics on the 1.85-m telescope is above 0.76 at all frequencies by using GRASP. Recently, we have succeeded in simultaneous observation of 12CO, 13CO, and C18O(J = 2–1 and 3–2) toward Orion KL with the optics for the first time.
{"title":"Optical design of the 1.85-m mm-submm telescope in 210–375 GHz band","authors":"Y. Yamasaki, S. Masui, Masanari Okawa, Koki Yokoyama, Taisei Minami, Shota Ueda, Yutaka Hasegawa, A. Nishimura, T. Onishi, H. Ogawa, N. Okada, K. Kimura, Álvaro González, T. Kojima, K. Kaneko, R. Sakai","doi":"10.1117/12.2561955","DOIUrl":"https://doi.org/10.1117/12.2561955","url":null,"abstract":"Currently, we are performing a large-scale survey of molecular clouds toward the Galactic Plane in 12CO, 13CO, and C18O(J = 2–1) with the 1.85-m mm-submm telescope from Nobeyama Radio Observatory. In addition, we are proceeding with the preparation of a new project to observe several additional molecular lines including higher transitions of CO isotopes, such as 12CO, 13CO, and C18O(J = 2–1, 3–2) simultaneously with a wideband receiver (210–375 GHz). The optics has a Cassegrain reflector antenna with Nasmyth beam-waveguide feed and is composed of Main-reflector, Sub-reflector, ellipsoidal mirrors, and plane mirrors. New wideband optics will be required to achieve this goal. In order to accomplish the optics, we have designed a corrugated horn with a fractional bandwidth of ∼56 %, and frequency independent optics to couple the beam from the telescope onto the horn. The corrugated horn has a conical profile and the variable corrugation depth. It has been optimized by using CHAMP, our targeting return loss of better than −20 dB, cross-polarization loss of better than −25 dB, and far-field good radiation pattern. The simulation of the corrugated horn results in low return loss, low crosspolarization, and symmetric beam pattern in that frequency band. The simulated aperture efficiency of the designed receiver optics on the 1.85-m telescope is above 0.76 at all frequencies by using GRASP. Recently, we have succeeded in simultaneous observation of 12CO, 13CO, and C18O(J = 2–1 and 3–2) toward Orion KL with the optics for the first time.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"30 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"130885274","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}
S. Masui, Taisei Minami, Masanari Okawa, Y. Yamasaki, Koki Yokoyama, Shota Ueda, Yutaka Hasegawa, A. Nishimura, T. Onishi, H. Ogawa, T. Kojima, Álvaro González
{"title":"Development of a wideband waveguide diplexer for simultaneous observation at 210-375 GHz","authors":"S. Masui, Taisei Minami, Masanari Okawa, Y. Yamasaki, Koki Yokoyama, Shota Ueda, Yutaka Hasegawa, A. Nishimura, T. Onishi, H. Ogawa, T. Kojima, Álvaro González","doi":"10.1117/12.2561355","DOIUrl":"https://doi.org/10.1117/12.2561355","url":null,"abstract":"","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"198 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"132623778","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}
S. Dabironezare, K. Karatsu, S. Yates, A. P. Laguna, V. Murugesan, D. Thoen, A. Endo, J. Baselmans, N. Llombart
{"title":"Broadband quasi-optical system for on-chip filter-bank spectrometer operating at sub-mm wavelengths","authors":"S. Dabironezare, K. Karatsu, S. Yates, A. P. Laguna, V. Murugesan, D. Thoen, A. Endo, J. Baselmans, N. Llombart","doi":"10.1117/12.2562383","DOIUrl":"https://doi.org/10.1117/12.2562383","url":null,"abstract":"","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"142 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"123201363","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}
S. Colditz, L. Looney, F. Bigiel, C. Fischer, J. Fischer, S. Hailey-Dunsheath, R. Herrera-Camus, A. Krabbe, H. Leduc, T. Wong, J. Zmuidzinas
We present the initial design, performance improvements and science opportunities for an upgrade to the Field-Imaging Far-Infrared Line Spectrometer (FIFI-LS). FIFI-LS efficiently measures fine structure cooling lines, delivering critical constraints of the interstellar medium and starforming environments. SOFIA provides the only FIR observational capability in the world, making FIFI-LS a workhorse for FIR lines, combining optimal spectral resolution and a wide velocity range. Its continuous coverage from 51-203 microns makes FIFI-LS a versatile tool to investigate a multitude of diagnostic lines within our galaxy and in extragalactic environments. The sensitivity and field-of-view (FOV) of FIFI-LS are limited by its 90s-era photoconductor arrays. These limits can be overcome by upgrading the instrument using the latest developments in Kinetic Inductance Detectors (KIDs). KIDs provide sensitivity gains in excess of 1.4 and allow larger arrays, enabling an increase in pixel count by an order of magnitude. This increase allows a wider FOV and instantaneous velocity coverage. The upgrade provides gains in point source observation speed by a factor <2 and in mapping speed by a factor <3.5, enabled by the improved sensitivity and pixel count. This upgrade has been proposed to NASA in response to the 2018 SOFIA Next Generation Instrumentation call.
{"title":"Upgrading the field-imaging far-infrared line spectrometer for the Stratospheric Observatory for Infrared Astronomy (SOFIA) with KIDs: enabling large sample (extragalactic) surveys","authors":"S. Colditz, L. Looney, F. Bigiel, C. Fischer, J. Fischer, S. Hailey-Dunsheath, R. Herrera-Camus, A. Krabbe, H. Leduc, T. Wong, J. Zmuidzinas","doi":"10.1117/12.2560120","DOIUrl":"https://doi.org/10.1117/12.2560120","url":null,"abstract":"We present the initial design, performance improvements and science opportunities for an upgrade to the Field-Imaging Far-Infrared Line Spectrometer (FIFI-LS). FIFI-LS efficiently measures fine structure cooling lines, delivering critical constraints of the interstellar medium and starforming environments. SOFIA provides the only FIR observational capability in the world, making FIFI-LS a workhorse for FIR lines, combining optimal spectral resolution and a wide velocity range. Its continuous coverage from 51-203 microns makes FIFI-LS a versatile tool to investigate a multitude of diagnostic lines within our galaxy and in extragalactic environments. The sensitivity and field-of-view (FOV) of FIFI-LS are limited by its 90s-era photoconductor arrays. These limits can be overcome by upgrading the instrument using the latest developments in Kinetic Inductance Detectors (KIDs). KIDs provide sensitivity gains in excess of 1.4 and allow larger arrays, enabling an increase in pixel count by an order of magnitude. This increase allows a wider FOV and instantaneous velocity coverage. The upgrade provides gains in point source observation speed by a factor <2 and in mapping speed by a factor <3.5, enabled by the improved sensitivity and pixel count. This upgrade has been proposed to NASA in response to the 2018 SOFIA Next Generation Instrumentation call.","PeriodicalId":393026,"journal":{"name":"Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X","volume":"20 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"133414343","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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