[ { "id": "authors:whsm0-1bc09", "collection": "authors", "collection_id": "whsm0-1bc09", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201015-152733092", "type": "book_section", "title": "Cryogenic W-Band SiGe BiCMOS Low-Noise Amplifier", "book_title": "2020 IEEE/MTT-S International Microwave Symposium (IMS)", "author": [ { "family_name": "Varonen", "given_name": "Mikko", "orcid": "0000-0002-6515-5092", "clpid": "Varonen-Mikko" }, { "family_name": "Sheikhipoor", "given_name": "Nima", "clpid": "Sheikhipoor-Nima" }, { "family_name": "Gabritchidze", "given_name": "Bekari", "clpid": "Gabritchidze-B" }, { "family_name": "Cleary", "given_name": "Kieran", "orcid": "0000-0002-8214-8265", "clpid": "Cleary-K-A" }, { "family_name": "Forst\u00e9n", "given_name": "Henrik", "orcid": "0000-0003-1841-9769", "clpid": "Forst\u00e9n-Henrik" }, { "family_name": "R\u00fccker", "given_name": "Holger", "orcid": "0000-0001-7407-959X", "clpid": "R\u00fccker-Holger" }, { "family_name": "Kaynak", "given_name": "Mehmet", "clpid": "Kaynak-Mehmet" } ], "abstract": "In this paper we present the design, modeling, and on-wafer measurement results of an ultra- wideband cryogenically cooled SiGe low-noise amplifier covering at least 71 to 116 GHz. When cryogenically cooled to 20 K and measured on wafer the SiGe amplifier shows 95-116-K noise temperature from 77 to 116 GHz. This means 6 to 7 times improvement in noise temperature compared to room temperature noise. The measured gain is around 20 dB for frequency range of 71 to 116 GHz with unprecedented low power consumption of 2.8 mW. To the best of authors' knowledge, this is the highest frequency cryogenic SiGe low-noise amplifier and lowest noise performance for silicon amplifiers for W-band reported to date.", "doi": "10.1109/ims30576.2020.9223922", "isbn": "9781728168159", "publisher": "IEEE", "place_of_publication": "Piscataway, NJ", "publication_date": "2020-08", "pages": "185-188" }, { "id": "authors:z4mth-xd005", "collection": "authors", "collection_id": "z4mth-xd005", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190108-110437676", "type": "book_section", "title": "The STRIP instrument of the Large Scale Polarization Explorer: microwave eyes to map the Galactic polarized foregrounds", "book_title": "Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy IX", "author": [ { "family_name": "Franceschet", "given_name": "Cristian", "clpid": "Franceschet-C" }, { "family_name": "Cleary", "given_name": "Kieran A.", "clpid": "Cleary-K-A" }, { "family_name": "Kangaslahti", "given_name": "Pekka", "clpid": "Kangaslahti-P" }, { "family_name": "Soria", "given_name": "Mary", "clpid": "Soria-M" } ], "contributor": [ { "family_name": "Zmuidzinas", "given_name": "Jonas", "clpid": "Zmuidzinas-J" }, { "family_name": "Gao", "given_name": "Jian-Rong", "clpid": "Gao-Jian-Rong" } ], "abstract": "In this paper we discuss the latest developments of the STRIP instrument of the \"Large Scale Polarization Explorer\" (LSPE) experiment. LSPE is a novel project that combines ground-based (STRIP) and balloon-borne (SWIPE) polarization measurements of the microwave sky on large angular scales to attempt a detection of the \"B-modes\" of the Cosmic Microwave Background polarization. STRIP will observe approximately 25% of the Northern sky from the \"Observatorio del Teide\" in Tenerife, using an array of forty-nine coherent polarimeters at 43 GHz, coupled to a 1.5 m fully rotating crossed-Dragone telescope. A second frequency channel with six-elements at 95 GHz will be exploited as an atmospheric monitor. At present, most of the hardware of the STRIP instrument has been developed and tested at sub-system level. System-level characterization, starting in July 2018, will lead STRIP to be shipped and installed at the observation site within the end of the year. The on-site verification and calibration of the whole instrument will prepare STRIP for a 2-years campaign for the observation of the CMB polarization.", "doi": "10.1117/12.2313558", "isbn": "9781510619692", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2018-07-09", "pages": "Art. No. 107081G" }, { "id": "authors:4ktgt-4mg12", "collection": "authors", "collection_id": "4ktgt-4mg12", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181212-160922767", "type": "book_section", "title": "Cryogenic Millimeter-Wave CMOS Low-Noise Amplifier", "book_title": "2018 IEEE/MTT-S International Microwave Symposium", "author": [ { "family_name": "Varonen", "given_name": "Mikko", "clpid": "Varonen-M" }, { "family_name": "Cleary", "given_name": "Kieran", "clpid": "Cleary-K-A" }, { "family_name": "Karaca", "given_name": "Denizhan", "clpid": "Karaca-D" }, { "family_name": "Halonerr", "given_name": "Kari A. I.", "clpid": "Halonerr-K-A-I" } ], "abstract": "In this paper we report a cryogenically cooled CMOS amplifier covering at least 75 to 115 GHz frequency range. The amplifier chip was fabricated in 2S-nm FD SOI CMOS technology. When cryogenically cooled to 20 K and measured on-wafer the CMOS amplifier shows lOS-ISS K noise temperature from 75 to 115 GHz. This means 6 to 8 times improvement in noise temperature compared to room temperature noise. The measured small-signal gain is around 20 dB. To the best of authors' knowledge, these are the first cryogenic measurements of millimeter-wave CMOS amplifiers and lowest CMOS LNA noise temperatures for W-Band reported to date.", "doi": "10.1109/mwsym.2018.8439505", "isbn": "978-1-5386-5067-7", "publisher": "IEEE", "place_of_publication": "Piscataway, NJ", "publication_date": "2018-06", "pages": "1503-1506" }, { "id": "authors:fsd4x-a8t37", "collection": "authors", "collection_id": "fsd4x-a8t37", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161114-151435470", "type": "book_section", "title": "Sideband-separating MMIC receivers for observation in the 3-mm band", "author": [ { "family_name": "Lamb", "given_name": "James W.", "clpid": "Lamb-J-W" }, { "family_name": "Cleary", "given_name": "Kieran A.", "clpid": "Cleary-K-A" }, { "family_name": "Gawande", "given_name": "Rohit S.", "clpid": "Gawande-R-S" }, { "family_name": "Kooi", "given_name": "Jacob W.", "orcid": "0000-0002-6610-0384", "clpid": "Kooi-J-W" }, { "family_name": "Laxen", "given_name": "Michael P.", "clpid": "Laxen-M-P" }, { "family_name": "Plambeck", "given_name": "Richard L.", "clpid": "Plambeck-R-L" }, { "family_name": "Reeves", "given_name": "Rodrigo A.", "orcid": "0000-0001-5704-271X", "clpid": "Reeves-R-A" }, { "family_name": "Kangaslahti", "given_name": "Pekka P.", "clpid": "Kangaslahti-P-P" }, { "family_name": "Varonen", "given_name": "Mikko", "clpid": "Varonen-M" } ], "contributor": [ { "family_name": "Holland", "given_name": "Wayne S.", "clpid": "Holland-W-S" }, { "family_name": "Zmuidzinas", "given_name": "Jonas", "clpid": "Zmuidzinas-J" } ], "abstract": "Wideband receivers for the 3-mm band were developed for CARMA, the Combined Array for Research in Millimeterwave Astronomy. Three cryogenic MMIC (monolithic microwave integrated circuit) amplifiers manufactured in InP 35- nm technology are combined in a block with waveguide probes and gain equalizers to cover the 80\u2013116 GHz band. These are followed by a sideband-separating mixer that has two 17 GHZ wide outputs, for upper and lower sidebands. Each receiver has a feed horn followed by a circular-to-linear polarizer and orthomode transducer. The two polarizations are amplified by the cryogenic MMICs, and the outputs downconverted in sideband separating mixers, resulting in four 1\u201318 GHz channels that can be simultaneously correlated. The first receiver was tested in the lab, and on-sky tests conducted at CARMA. Measured noise temperatures were in the range 40\u201370 K, with a sideband rejection of about 15 dB.", "doi": "10.1117/12.2233106", "publisher": "Society of Photo-Optical Instrumentation Engineers (SPIE)", "publication_date": "2016-07-19" }, { "id": "authors:s2c38-5t682", "collection": "authors", "collection_id": "s2c38-5t682", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170123-172732524", "type": "book_section", "title": "Argus: A W-band 16-pixel focal plane array for the Green Bank Telescope", "book_title": "2014 United States National Committee of URSI National Radio Science Meeting (USNC-URSI NRSM)", "author": [ { "family_name": "Devaraj", "given_name": "Kiruthika", "clpid": "Devaraj-K" }, { "family_name": "Church", "given_name": "Sarah", "clpid": "Church-S" }, { "family_name": "Cleary", "given_name": "Kieran", "clpid": "Cleary-K-A" }, { "family_name": "Frayer", "given_name": "David", "orcid": "0000-0003-1924-1122", "clpid": "Frayer-D-T" }, { "family_name": "Gawande", "given_name": "Rohit", "clpid": "Gawande-R" }, { "family_name": "Goldsmith", "given_name": "Paul", "orcid": "0000-0002-6622-8396", "clpid": "Goldsmith-P-F" }, { "family_name": "Gundersen", "given_name": "Joshua", "clpid": "Gundersen-J-O" }, { "family_name": "Harris", "given_name": "Andrew", "clpid": "Harris-A" }, { "family_name": "Kangaslahti", "given_name": "Pekka", "clpid": "Kangaslahti-P" }, { "family_name": "Readhead", "given_name": "Anthony", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Reeves", "given_name": "Rodrigo", "clpid": "Reeves-R" }, { "family_name": "Samoska", "given_name": "Lorene", "clpid": "Samoska-L" }, { "family_name": "Sieth", "given_name": "Matthew", "clpid": "Sieth-M" }, { "family_name": "Voll", "given_name": "Patricia", "clpid": "Voll-P" } ], "abstract": "We are building Argus, a 16-pixel square-packed focal plane array that will cover the 75-115.3 GHz frequency range on the Robert C. Byrd Green Bank Telescope (GBT). The primary research area for Argus is the study of star formation within our Galaxy and nearby galaxies. Argus will map key molecules that trace star formation, including carbon monoxide (CO) and hydrogen cyanide (HCN). An additional key science area is astrochemistry, which will be addressed by observing complex molecules in the interstellar medium, and the study of formation of solar systems, which will be addressed by identifying dense pre-stellar cores and by observing comets in our solar system. Argus has a highly scalable architecture and will be a technology path finder for larger arrays. The array is modular in construction, which will allow easy replacement of malfunctioning and poorly performing components.", "doi": "10.1109/USNC-URSI-NRSM.2014.6928110", "isbn": "978-1-4799-3120-0", "publisher": "IEEE", "place_of_publication": "Piscataway, NJ", "publication_date": "2014-01", "pages": "1" }, { "id": "authors:ef71v-5cn84", "collection": "authors", "collection_id": "ef71v-5cn84", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180828-122924115", "type": "book_section", "title": "Using Spinning Dust Emission To Constrain The Evolution Of Dust Grains In Cold Clumps", "author": [ { "family_name": "Tibbs", "given_name": "C. T.", "clpid": "Tibbs-C-T" }, { "family_name": "Paladini", "given_name": "R.", "orcid": "0000-0002-5158-243X", "clpid": "Paladini-Roberta" }, { "family_name": "Cleary", "given_name": "K.", "clpid": "Cleary-K-A" }, { "family_name": "Grainge", "given_name": "K. J. B.", "clpid": "Grainge-K-J-B" }, { "family_name": "Muchovej", "given_name": "S. J. C.", "clpid": "Muchovej-Stephen-J-C" }, { "family_name": "Pearson", "given_name": "T. J.", "orcid": "0000-0001-5213-6231", "clpid": "Pearson-T-J" }, { "family_name": "Perrott", "given_name": "Y. C.", "clpid": "Perrott-Y-C" }, { "family_name": "Rumsey", "given_name": "C.", "clpid": "Rumsey-C" }, { "family_name": "Scaife", "given_name": "A. M. M.", "clpid": "Scaife-A-M-M" }, { "family_name": "Stevenson", "given_name": "M. A.", "clpid": "Stevenson-M-A" }, { "family_name": "Villadsen", "given_name": "J.", "orcid": "0000-0003-3924-243X", "clpid": "Villadsen-J" } ], "abstract": "Within many molecular clouds in our Galaxy there are cold, dense regions known as cold clumps in which stars form. These dense environments provide a great location in which to study dust grain evolution. Given the low temperatures (\u223c10\u201315 K) and high densities (\u223c10^5 cm^(\u22123)), these environments are dark at mid-infrared (IR) wavelengths and emit strongly at wavelengths \u2265160 \u00b5m. The lack of mid-IR emission can be attributed to one of two reasons: i) a deficit of the small dust grains that emit stochastically at mid-IR wavelengths; or ii) small dust grains are present, but due to the high densities, the stellar photons cannot penetrate deep enough into the clumps to excite them. Using mid-IR observations alone it is impossible to distinguish between these two scenarios. However, by using spinning dust emission at cm wavelengths it is possible to break this degeneracy, because if small dust grains are present in these clumps, then even though stellar photons cannot excite them to emit at mid-IR wavelengths, these dust grains will be spun-up by collisions and hence emit spinning dust radiation. If spinning dust were detected in these clumps it would prove that there are small dust grains present and that the lack of mid-IR emission is due to a lack of stellar photons. Conversely, a lack of spinning dust emission would indicate a deficit of small dust grains in these clumps. Since small dust grains require harsh radiation fields to be destroyed, a lack of small dust grains is likely a result of dust grain coagulation. With this in mind, we present preliminary results illustrating our method of using spinning dust observations to determine the evolution of small dust grains in these environments.", "doi": "10.22323/1.207.0064", "publisher": "SISSA", "publication_date": "2013-11" }, { "id": "authors:qrff0-rzc34", "collection": "authors", "collection_id": "qrff0-rzc34", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180525-073555253", "type": "book_section", "title": "A 75\u2013116-GHz LNA with 23-K noise temperature at 108 GHz", "book_title": "2013 IEEE MTT-S International Microwave Symposium (IMS)", "author": [ { "family_name": "Varonen", "given_name": "Mikko", "clpid": "Varonen-M" }, { "family_name": "Reeves", "given_name": "Rodrigo", "orcid": "0000-0001-5704-271X", "clpid": "Reeves-R-A" }, { "family_name": "Kangaslahti", "given_name": "Pekka", "clpid": "Kangaslahti-P" }, { "family_name": "Samoska", "given_name": "Lorene", "clpid": "Samoska-L" }, { "family_name": "Akgiray", "given_name": "Ahmed", "orcid": "0000-0002-7373-4158", "clpid": "Akgiray-A" }, { "family_name": "Cleary", "given_name": "Kieran", "clpid": "Cleary-K-A" }, { "family_name": "Gawande", "given_name": "Rohit", "clpid": "Gawande-R" }, { "family_name": "Fung", "given_name": "Andy", "orcid": "0000-0003-4849-759X", "clpid": "Fung-Andy-K" }, { "family_name": "Gaier", "given_name": "Todd", "clpid": "Gaier-T" }, { "family_name": "Weinreb", "given_name": "Sander", "clpid": "Weinreb-S" }, { "family_name": "Readhead", "given_name": "Anthony C. S.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" }, { "family_name": "Lawrence", "given_name": "Charles", "clpid": "Lawrence-C" }, { "family_name": "Sarkozy", "given_name": "Stephen", "clpid": "Sarkozy-S" }, { "family_name": "Lai", "given_name": "Richard", "clpid": "Lai-Richard" } ], "abstract": "In this paper we present the design and measurement results, both on-wafer and in package, of an ultra-low-noise and wideband monolithic microwave integrated circuit (MMIC) amplifier in the frequency range of 75 to 116 GHz. The three-stage amplifier packaged in a WR10 waveguide housing and fabricated using a 35-nm InP HEMT technology achieves a record noise temperature of 23 K at 108 GHz when cryogenically cooled to 27 K. The measured gain is 22 to 27 dB for frequency range of 75 to 116 GHz. Furthermore, the amplifier utilizes four-finger devices with a total gate width of 60 \u03bcm resulting in higher output power. Therefore, we consider that this amplifier achieves state-of-the-art performance in terms of bandwidth, noise temperature, gain, and linearity so far reported for cryogenically cooled amplifiers around W-band.", "doi": "10.1109/MWSYM.2013.6697595", "isbn": "978-1-4673-6176-7", "publisher": "IEEE", "place_of_publication": "Piscataway, NJ", "publication_date": "2013-06", "pages": "1-3" }, { "id": "authors:x9cz5-94531", "collection": "authors", "collection_id": "x9cz5-94531", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20161028-133133809", "type": "book_section", "title": "Development of MMIC receivers for cosmic microwave background interferometry", "book_title": "Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy V", "author": [ { "family_name": "Sieth", "given_name": "Matthew", "clpid": "Sieth-M" }, { "family_name": "Lau", "given_name": "Judy M.", "clpid": "Lau-Judy-M" }, { "family_name": "Voll", "given_name": "Patricia", "clpid": "Voll-P" }, { "family_name": "Church", "given_name": "Sarah", "clpid": "Church-S" }, { "family_name": "Kangaslahti", "given_name": "Pekka", "clpid": "Kangaslahti-P" }, { "family_name": "Samoska", "given_name": "Lorene", "clpid": "Samoska-L-A" }, { "family_name": "Soria", "given_name": "Mary", "clpid": "Soria-M" }, { "family_name": "Gaier", "given_name": "Todd", "clpid": "Gaier-T" }, { "family_name": "Van Winkle", "given_name": "Dan", "clpid": "Van-Winkle-D" }, { "family_name": "Neilson", "given_name": "Jeffrey", "clpid": "Neilson-J" }, { "family_name": "Tantawi", "given_name": "Sami", "clpid": "Tantawi-S" }, { "family_name": "Cleary", "given_name": "Kieran", "clpid": "Cleary-K-A" }, { "family_name": "Readhead", "given_name": "Anthony C. S.", "orcid": "0000-0001-9152-961X", "clpid": "Readhead-A-C-S" } ], "contributor": [ { "family_name": "Holland", "given_name": "Wayne S.", "clpid": "Holland-W-S" }, { "family_name": "Zmuidzinas", "given_name": "Jonas", "clpid": "Zmuidzinas-J" } ], "abstract": "We report on the development of some of the key technologies that will be needed for a large-format Cosmic Microwave Background (CMB) interferometer with many hundreds of wideband W-band (75-110 GHz) receivers. A scalable threebaseline prototype interferometer is being assembled as a technology demonstration for a future ground- or space-based instrument. Each of the prototype heterodyne receivers integrates two InPMonolithic Microwave Integrated Circuit (MMIC) low-noise amplifiers, a coupled-line bandpass filter, a subharmonic balanced diode mixer, and a 90\u00b0 local oscillator phase switch into a single compact module that is suitable for mass production. Room temperature measurements indicate bandaveraged receiver noise temperatures of 500 K from 85-100 GHz. Cryogenic receiver noise temperatures are expected to be around 50 K.", "doi": "10.1117/12.857830", "isbn": "978-0-81948-231-0", "publisher": "Society of Photo-Optical Instrumentation Engineers", "place_of_publication": "Bellingham, WA", "publication_date": "2010-07-15", "pages": "Art. No. 77412I" }, { "id": "authors:60tj2-yaz46", "collection": "authors", "collection_id": "60tj2-yaz46", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110328-110301502", "type": "book_section", "title": "Coherent polarimeter modules for the QUIET experiment", "book_title": "Millimeter, Submillimeter, and Far-infrared Detectors and Instrumentation for Astronomy V", "author": [ { "family_name": "Cleary", "given_name": "Kieran A.", "orcid": "0000-0002-8214-8265", "clpid": "Cleary-K-A" }, { "literal": "QUIET Collaboration" } ], "abstract": "The Q/U Imaging Experiment (QUIET) is an experimental program to make very sensitive measurements of the Cosmic Background Radiation (CMB) polarization from the ground. A key component of this project is the ability to produce large numbers of detectors in order to achieve the required sensitivity. Using a breakthrough in mm-wave packaging at JPL, a polarimeter-on-a-chip has been developed which lends itself to the mass-production techniques used in the semiconductor industry. We describe the design, implementation and performance of these polarimeter modules for QUIET Phase I and briefly discuss the plans for further module development.", "doi": "10.1117/12.857673", "isbn": "978-0-81948-231-0", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2010-07-15", "pages": "Art. No. 77412H" } ]