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"abstract": "Spectro-Photometer for the History of the Universe, Epoch of Reionization, and Ices Explorer (SPHEREx), a NASA Explorer satellite launched on 2025 March 11, is carrying out the first all-sky near-infrared spectral survey. The satellite observes in 102 spectral bands from 0.75 to 5.0 μm with a resolving power ranging from λ/Δλ = 35–130 in 6.\"2 pixels. The observatory obtains a 5σ depth of 19.5–19.9 AB mag for 0.75 < λ < 3.8 μm with λ/Δλ ∼ 40 and 17.8–18.8 AB mag for 3.8 < λ < 5.0 μm with λ/Δλ ∼ 120 after mapping the full sky four times over two years. Scientifically, SPHEREx will produce a large galaxy redshift survey over the full sky to constrain the amplitude of inflationary non-Gaussianity. The observations will produce two deep spectral maps near the ecliptic poles that use intensity mapping to probe the evolution of galaxies over cosmic history. By mapping the depth of infrared absorption features over the Galactic plane, SPHEREx will comprehensively survey the abundance and composition of water and other biogenic ice species in the interstellar medium. The project will release initial data rapidly in the form of spectral images, and specialized data products over the life of the mission as the surveys proceed. The science team will also produce spectral catalogs of planet-bearing and low-mass stars, solar system objects, and galaxy clusters three years after launch. We describe the design of the instrument and spacecraft, which flow from the core science requirements. Finally, we present an initial evaluation of the satellite’s in-flight performance and key characteristics.
",
"doi": "10.3847/1538-4357/ae2be2",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2026-03-01",
"series_number": "1",
"volume": "999",
"issue": "1",
"pages": "139"
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"orcid": "0000-0002-5215-6993"
},
{
"family_name": "Kefeli",
"given_name": "S.",
"clpid": "Kefeli-S"
},
{
"family_name": "Kovac",
"given_name": "J. M.",
"orcid": "0009-0003-5432-7180"
},
{
"family_name": "Kuo",
"given_name": "C."
},
{
"family_name": "Lasko",
"given_name": "K.",
"orcid": "0000-0002-4540-1495"
},
{
"family_name": "Lau",
"given_name": "K.",
"orcid": "0000-0002-6445-2407",
"clpid": "Lau-King"
},
{
"family_name": "Lautzenhiser",
"given_name": "M."
},
{
"family_name": "Lennox",
"given_name": "A."
},
{
"family_name": "Liu",
"given_name": "T.",
"orcid": "0000-0001-5677-5188"
},
{
"family_name": "Mackey",
"given_name": "S."
},
{
"family_name": "Maher",
"given_name": "N."
},
{
"family_name": "Megerian",
"given_name": "K. G.",
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},
{
"family_name": "Minutolo",
"given_name": "L.",
"orcid": "0000-0002-4876-112X",
"clpid": "Minutolo-Lorenzo"
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{
"family_name": "Moncelsi",
"given_name": "L.",
"orcid": "0000-0002-4242-3015",
"clpid": "Moncelsi-Lorenzo"
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{
"family_name": "Nakato",
"given_name": "Y."
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
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{
"family_name": "O'Brient",
"given_name": "R.",
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{
"family_name": "Paine",
"given_name": "S. N.",
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},
{
"family_name": "Patel",
"given_name": "A.",
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{
"family_name": "Petroff",
"given_name": "M. A.",
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{
"family_name": "Polish",
"given_name": "A. R.",
"orcid": "0000-0002-7822-6179"
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{
"family_name": "Prouve",
"given_name": "T."
},
{
"family_name": "Pryke",
"given_name": "C.",
"orcid": "0000-0003-3983-6668"
},
{
"family_name": "Reintsema",
"given_name": "C. D."
},
{
"family_name": "Richter",
"given_name": "S."
},
{
"family_name": "Romand",
"given_name": "T.",
"orcid": "0009-0000-7421-8908",
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{
"family_name": "Salatino",
"given_name": "M."
},
{
"family_name": "Schillaci",
"given_name": "A.",
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{
"family_name": "Schmitt",
"given_name": "B."
},
{
"family_name": "Schwarz",
"given_name": "R."
},
{
"family_name": "Sheehy",
"given_name": "C. D."
},
{
"family_name": "Singari",
"given_name": "B.",
"orcid": "0000-0001-7387-0881"
},
{
"family_name": "Soliman",
"given_name": "A.",
"clpid": "Soliman-A"
},
{
"family_name": "St Germaine",
"given_name": "T."
},
{
"family_name": "Steiger",
"given_name": "A.",
"orcid": "0000-0003-0260-605X",
"clpid": "Steiger-Aaron"
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{
"family_name": "Steinbach",
"given_name": "B.",
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{
"family_name": "Sudiwala",
"given_name": "R."
},
{
"family_name": "Teply",
"given_name": "G. P.",
"clpid": "Teply-G-P"
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{
"family_name": "Thompson",
"given_name": "K. L."
},
{
"family_name": "Tucker",
"given_name": "C.",
"orcid": "0000-0002-1851-3918"
},
{
"family_name": "Turner",
"given_name": "A. D.",
"clpid": "Turner-A-D"
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{
"family_name": "Verg\u00e8s",
"given_name": "C.",
"orcid": "0000-0002-3942-1609"
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{
"family_name": "Vieregg",
"given_name": "A. G."
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{
"family_name": "Wandui",
"given_name": "A.",
"orcid": "0000-0002-8232-7343",
"clpid": "Wandui-Albert"
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{
"family_name": "Weber",
"given_name": "A. C.",
"clpid": "Weber-A-C"
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{
"family_name": "Willmert",
"given_name": "J.",
"orcid": "0000-0002-6452-4693"
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{
"family_name": "Wong",
"given_name": "C. L."
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{
"family_name": "Wu",
"given_name": "W. L. K.",
"orcid": "0000-0001-5411-6920",
"clpid": "Wu-Wai-Ling-Kimmy"
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{
"family_name": "Yang",
"given_name": "H."
},
{
"family_name": "Yu",
"given_name": "C.",
"orcid": "0000-0002-8542-232X"
},
{
"family_name": "Zeng",
"given_name": "L.",
"orcid": "0000-0001-6924-9072"
},
{
"family_name": "Zhang",
"given_name": "C.",
"orcid": "0000-0001-8288-5823"
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{
"family_name": "Zhang",
"given_name": "S.",
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{
"literal": "(BICEP/Keck Collaboration)"
}
],
"abstract": "We present component-separated polarization maps of the cosmic microwave background (CMB) and Galactic thermal dust emission, derived using data from the BICEP/Keck experiments through the 2018 observing season and Planck. By employing a maximum-likelihood method that utilizes observing matrices, we produce unbiased maps of the CMB and dust signals. We outline the computational challenges and demonstrate an efficient implementation of the component map estimator. We show methods to compute and characterize power spectra of these maps, opening up an alternative way to infer the tensor-to-scalar ratio from our data. We compare the results of this map-based separation method with the baseline BICEP/Keck analysis. Our analysis demonstrates consistency between the two methods, finding an 84% correlation between the pipelines.
",
"doi": "10.3847/1538-4357/ae3e53",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2026-03-01",
"series_number": "1",
"volume": "999",
"issue": "1",
"pages": "89"
},
{
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"type": "article",
"title": "The SPHEREx Sky Simulator: Science Data Modeling for the First All-sky Near-infrared Spectral Survey",
"author": [
{
"family_name": "Crill",
"given_name": "Brendan P.",
"orcid": "0000-0002-4650-8518",
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{
"family_name": "Bach",
"given_name": "Yoonsoo P.",
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{
"family_name": "Bryan",
"given_name": "Sean A.",
"orcid": "0000-0003-4607-9562"
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{
"family_name": "Choppin de Janvry",
"given_name": "Jean",
"orcid": "0009-0008-8066-446X",
"clpid": "Choppin-de-Janvry-Jean"
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{
"family_name": "Cukierman",
"given_name": "Ari J.",
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"clpid": "Cukierman-Ari-J"
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{
"family_name": "Dowell",
"given_name": "C. Darren",
"orcid": "0009-0002-0098-6183",
"clpid": "Dowell-C-Darren"
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{
"family_name": "Everett",
"given_name": "Spencer W.",
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{
"family_name": "Fazar",
"given_name": "Candice",
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{
"family_name": "Goldina",
"given_name": "Tatiana",
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{
"family_name": "Huai",
"given_name": "Zhaoyu",
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{
"family_name": "Hui",
"given_name": "Howard",
"orcid": "0000-0001-5812-1903",
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{
"family_name": "Jeong",
"given_name": "Woong-Seob",
"orcid": "0000-0002-2770-808X"
},
{
"family_name": "Kang",
"given_name": "Jae Hwan",
"orcid": "0000-0002-3470-2954",
"clpid": "Kang-Jae-Hwan"
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{
"family_name": "Korngut",
"given_name": "Phillip M.",
"orcid": "0009-0003-8869-3365",
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{
"family_name": "Lee",
"given_name": "Jae Joon",
"orcid": "0000-0003-0894-7824"
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{
"family_name": "Masters",
"given_name": "Daniel C.",
"orcid": "0000-0001-5382-6138",
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{
"family_name": "Nguyen",
"given_name": "Chi H.",
"orcid": "0000-0001-9368-3186",
"clpid": "Nguyen-Chi-H"
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{
"family_name": "Pyo",
"given_name": "Jeonghyun",
"orcid": "0000-0001-9937-8270"
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{
"family_name": "Symons",
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{
"family_name": "Tolls",
"given_name": "Volker",
"orcid": "0000-0003-1841-2241"
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{
"family_name": "Yang",
"given_name": "Yujin",
"orcid": "0000-0003-3078-2763"
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{
"family_name": "Zemcov",
"given_name": "Michael",
"orcid": "0000-0001-8253-1451",
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{
"family_name": "Akeson",
"given_name": "Rachel",
"orcid": "0000-0001-9674-1564",
"clpid": "Akeson-Rachel"
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{
"family_name": "Ashby",
"given_name": "Matthew L. N.",
"orcid": "0000-0002-3993-0745"
},
{
"family_name": "Bock",
"given_name": "James J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
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{
"family_name": "Chang",
"given_name": "Tzu-Ching",
"orcid": "0000-0001-5929-4187",
"clpid": "Chang-Tzu-Ching"
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{
"family_name": "Cheng",
"given_name": "Yun-Ting",
"orcid": "0000-0002-5437-0504",
"clpid": "Cheng-Yun-Ting"
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{
"family_name": "Chiang",
"given_name": "Yi-Kuan",
"orcid": "0000-0001-6320-261X"
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{
"family_name": "Cooray",
"given_name": "Asantha",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
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{
"family_name": "Dore",
"given_name": "Olivier P.",
"orcid": "0000-0001-7432-2932",
"clpid": "Dor\u00e9-O"
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{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Feder",
"given_name": "Richard M.",
"orcid": "0000-0002-9330-8738",
"clpid": "Feder-Richard-M"
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{
"family_name": "Werner",
"given_name": "Michael W.",
"orcid": "0000-0003-4990-189X",
"clpid": "Werner-Michael-W"
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],
"abstract": "We describe the SPHEREx Sky Simulator (henceforth the Simulator), a software tool designed to model science data for NASA’s SPHEREx mission that will carry out a series of all-sky spectrophotometric surveys at ∼6″ spatial resolution in 102 spectral channels spanning 0.75–5 μm. The Simulator software implements models for astrophysical emission, instrument characteristics, and survey strategy to generate realistic infrared sky scenes as they will be observed by SPHEREx. The simulated data include a variety of realistic noise and systematic effects that are estimated using up-to-date astrophysical measurements and information from prelaunch instrument characterization campaigns. Through the preflight mission phases, the Simulator has been critical in predicting the impact of various effects on SPHEREx science performance and has played an important role in guiding the development of the SPHEREx data analysis pipeline. In this paper, we describe the Simulator architecture, preflight instrument, and sky models, and summarize high-level predictions from the Simulator, including a prelaunch prediction for the 5σ point source sensitivity of SPHEREx, which we estimate to be mAB 18.5–19 from 0.75 to 3.8 μm and mAB 16.6–18 from 3.8 to 5 μm, with the sensitivity limited by the zodiacal light background at all wavelengths. In the future, on-orbit data will be used to improve the Simulator, which will form the basis of a variety of forward-modeling tools that will be used to model myriad instrumental and astrophysical processes to characterize their systematic effects on our final data products and analyses.
",
"doi": "10.3847/1538-4365/ae04cc",
"issn": "0067-0049",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2025-11",
"series_number": "1",
"volume": "281",
"issue": "1",
"pages": "10"
},
{
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"type": "article",
"title": "The Potential of the SPHEREx Mission for Characterizing Polycyclic Aromatic Hydrocarbon 3.3 \u03bcm Emission in Nearby Galaxies",
"author": [
{
"family_name": "Zhang",
"given_name": "Edward",
"orcid": "0009-0003-1284-3507",
"clpid": "Zhang-Edward"
},
{
"family_name": "Faisst",
"given_name": "Andreas L.",
"orcid": "0000-0002-9382-9832",
"clpid": "Faisst-Andreas-L"
},
{
"family_name": "Crill",
"given_name": "Brendan P.",
"orcid": "0000-0002-4650-8518",
"clpid": "Crill-Brendan-P"
},
{
"family_name": "Inami",
"given_name": "Hanae",
"orcid": "0000-0003-4268-0393"
},
{
"family_name": "Lai",
"given_name": "Thomas",
"orcid": "0000-0001-8490-6632",
"clpid": "Lai-Thomas"
},
{
"family_name": "Ohyama",
"given_name": "Youichi",
"orcid": "0000-0001-9490-3582"
},
{
"family_name": "Pyo",
"given_name": "Jeonghyun",
"orcid": "0000-0001-9937-8270"
},
{
"family_name": "Akeson",
"given_name": "Rachel",
"orcid": "0000-0001-9674-1564",
"clpid": "Akeson-Rachel"
},
{
"family_name": "Ashby",
"given_name": "Matthew L. N.",
"orcid": "0000-0002-3993-0745"
},
{
"family_name": "Bock",
"given_name": "James J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cheng",
"given_name": "Yun-Ting",
"orcid": "0000-0002-5437-0504",
"clpid": "Cheng-Yun-Ting"
},
{
"family_name": "Chiang",
"given_name": "Yi-Kuan",
"orcid": "0000-0001-6320-261X"
},
{
"family_name": "Cooray",
"given_name": "Asantha",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Dor\u00e9",
"given_name": "Olivier",
"orcid": "0000-0001-7432-2932",
"clpid": "Dor\u00e9-O"
},
{
"family_name": "Feder",
"given_name": "Richard M.",
"orcid": "0000-0002-9330-8738"
},
{
"family_name": "Kim",
"given_name": "Yongjung",
"orcid": "0000-0003-1647-3286"
},
{
"family_name": "Lee",
"given_name": "Bomee",
"orcid": "0000-0003-1954-5046"
},
{
"family_name": "Masters",
"given_name": "Daniel",
"orcid": "0000-0001-5382-6138",
"clpid": "Masters-Daniel"
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{
"family_name": "Melnick",
"given_name": "Gary",
"orcid": "0000-0002-6025-0680"
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{
"family_name": "Paladini",
"given_name": "Roberta",
"orcid": "0000-0002-5158-243X",
"clpid": "Paladini-Roberta"
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{
"family_name": "Werner",
"given_name": "Michael W.",
"orcid": "0000-0003-4990-189X",
"clpid": "Werner-Michael-W"
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],
"abstract": "Together with gas, stars, and supermassive black holes, dust is crucial in stellar and galaxy evolution. Hence, understanding galaxies’ dust properties across cosmic time is critical to studying their evolution. In addition to photometric constraints on the absorption of blue light and its reemission at infrared wavelengths, dust grain properties can be explored spectroscopically via polycyclic aromatic hydrocarbon (PAH) emission bands in the mid-IR. The new SPHEREx space telescope conducts an all-sky spectrophotometric survey of stars and galaxies at wavelengths of 0.75–5 μm, making it ideal for studying the widespread presence of the 3.3 μm PAH emission across galaxy populations out to z ∼ 0.4. In this paper, we simulated galaxy spectra to investigate SPHEREx's capability to study PAH emission in such galaxies. We find that for the all-sky survey the PAH 3.3 μm emission band flux can be measured to 30% accuracy at log (M/M\u2299) > 9.5 and star formation rate (SFR) > 1 M\u2299 yr\u207b¹ at z = 0.1, log (M/M\u2299) > 10.5 and SFR > 10 M\u2299 yr\u207b¹ at z = 0.2–0.3, and log (M/M\u2299) > 11 and SFR > 100 M\u2299 yr\u207b¹ at z = 0.4. For deep SPHEREx fields, a factor of ∼10 deeper sensitivity limits can be reached. Overall, SPHEREx will enable the measurement of the 3.3 μm PAH band emission in several hundred thousand galaxies across the sky, providing a population study of the smallest dust grains (“nano grains”) and radiation properties in massive galaxies in the nearby Universe.
",
"doi": "10.3847/1538-4357/adfd5a",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2025-10-10",
"series_number": "1",
"volume": "992",
"issue": "1",
"pages": "3"
},
{
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"type": "article",
"title": "The Cosmic Infrared Background Experiment-2: An Intensity-mapping Optimized Sounding-rocket Payload to Understand the Near-IR Extragalactic Background Light",
"author": [
{
"family_name": "Zemcov",
"given_name": "Michael",
"orcid": "0000-0001-8253-1451",
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{
"family_name": "Bock",
"given_name": "James J.",
"orcid": "0000-0002-5710-5212",
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{
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"given_name": "Asantha",
"orcid": "0000-0002-3892-0190",
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{
"family_name": "Matsuura",
"given_name": "Shuji",
"orcid": "0000-0002-5698-9634"
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{
"family_name": "Lee",
"given_name": "Dae-Hee"
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{
"family_name": "Fazar",
"given_name": "Candice",
"orcid": "0000-0001-9925-0146"
},
{
"family_name": "Feder",
"given_name": "Richard M.",
"orcid": "0000-0002-9330-8738"
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{
"family_name": "Heaton",
"given_name": "Grigory",
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{
"family_name": "Hashimoto",
"given_name": "Ryo"
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{
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{
"family_name": "Matsumoto",
"given_name": "Toshio"
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{
"family_name": "Nguyen",
"given_name": "Chi H.",
"orcid": "0000-0001-9368-3186",
"clpid": "Nguyen-Chi-H"
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{
"family_name": "Noda",
"given_name": "Kazuma",
"orcid": "0000-0002-5756-5964"
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{
"family_name": "Park",
"given_name": "Won-Kee",
"orcid": "0000-0002-8292-2556"
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{
"family_name": "Sano",
"given_name": "Kei",
"orcid": "0000-0002-6468-8532"
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{
"family_name": "Takimoto",
"given_name": "Kohji",
"orcid": "0000-0002-8405-9549"
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{
"family_name": "Arai",
"given_name": "Toshiaki"
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{
"family_name": "Bang",
"given_name": "Seung-Cheol"
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{
"family_name": "Bangale",
"given_name": "Priyadarshini",
"orcid": "0000-0002-3886-3739"
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{
"family_name": "Furutani",
"given_name": "Masaki"
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{
"family_name": "Hristov",
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{
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{
"family_name": "Kida",
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{
"family_name": "Kojima",
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{
"family_name": "Lanz",
"given_name": "Alicia",
"orcid": "0000-0003-2565-1558"
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{
"family_name": "Matsumi",
"given_name": "Chika"
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{
"family_name": "Mercado",
"given_name": "Dale",
"orcid": "0000-0002-7485-7563"
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{
"family_name": "Nakagawa",
"given_name": "Shunsuke"
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{
"family_name": "Nakagawa",
"given_name": "Tomoya"
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{
"family_name": "Nakahata",
"given_name": "Shuta"
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{
"family_name": "Ohta",
"given_name": "Ryo"
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{
"family_name": "Patru",
"given_name": "Dorin",
"orcid": "0009-0008-5671-9061"
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{
"family_name": "Shirahata",
"given_name": "Mai"
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{
"family_name": "Suzuki",
"given_name": "Hiroko"
},
{
"family_name": "Takahashi",
"given_name": "Aoi",
"orcid": "0000-0003-3881-3202"
},
{
"family_name": "Tamai",
"given_name": "Momoko"
},
{
"family_name": "Tramm",
"given_name": "Serena",
"orcid": "0009-0002-8148-7502",
"clpid": "Tramm-Serena"
},
{
"family_name": "Tsumura",
"given_name": "Kohji",
"orcid": "0000-0001-7143-6520"
},
{
"family_name": "Yamada",
"given_name": "Yasuhiro"
},
{
"family_name": "Wang",
"given_name": "Shiang-Yu",
"orcid": "0000-0001-6491-1901"
}
],
"abstract": "\n
The background light produced by emission from all sources over cosmic history is a powerful diagnostic of structure formation and evolution. At near-infrared wavelengths, this extragalactic background light (EBL) is comprised of emission from galaxies stretching all the way back to the first-light objects present during the Epoch of Reionization. The Cosmic Infrared Background Experiment 2 (CIBER-2) is a sounding-rocket experiment designed to measure both the absolute photometric brightness of the EBL over 0.5–2.0 μm and perform an intensity-mapping measurement of EBL spatial fluctuations in six broad bands over the same wavelength range. CIBER-2 comprises a 28.5 cm, 80 K telescope that images several square degrees to three separate cameras. Each camera is equipped with an HAWAII-2RG detector covered by an assembly that combines two broadband filters and a linear-variable filter, which perform the intensity mapping and absolute photometric measurements, respectively. CIBER-2 has flown three times: an engineering flight in 2021, a terminated launch in 2023, and a successful science flight in 2024. In this paper, we review the science case for the experiment; describe the factors motivating the instrument design; review the optical, mechanical, and electronic implementation of the instrument; present preflight laboratory characterization measurements; and finally assess the instrument’s performance in flight.
\n
Precise, unbiased measurements of extragalactic background anisotropies require careful treatment of systematic effects in fluctuation-based, broadband intensity mapping measurements. In this paper, we detail improvements in methodology for the Cosmic Infrared Background Experiment (CIBER), concentrating on flat field errors and source masking errors. In order to bypass the use of field differences, which mitigate flat field errors but reduce sensitivity, we characterize and correct for the flat field on pseudopower spectra, which includes both additive and multiplicative biases. To more effectively mask point sources at 1.1 and 1.8 μm, we develop a technique for predicting masking catalogs that utilizes optical and near-infrared photometry through random forest regression. This allows us to mask over 2 Vega mag deeper than the completeness limits of Two Micron All Sky Survey alone, with errors in the shot noise power remaining below <10% at all masking depths considered. Through detailed simulations of CIBER observations, we validate our formalism and demonstrate unbiased recovery of the sky fluctuations on realistic mocks. We demonstrate that residual flat field errors comprise <20% of the final CIBER power spectrum uncertainty with this methodology.
",
"doi": "10.3847/1538-4357/adfa1a",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2025-09-20",
"series_number": "1",
"volume": "991",
"issue": "1",
"pages": "87"
},
{
"id": "authors:4hzkp-zt112",
"collection": "authors",
"collection_id": "4hzkp-zt112",
"cite_using_url": "https://authors.library.caltech.edu/records/4hzkp-zt112",
"type": "article",
"title": "BICEP/Keck XVIII: Measurement of BICEP3 polarization angles and consequences for constraining cosmic birefringence and inflation",
"author": [
{
"family_name": "Ade",
"given_name": "P.\u2009A.\u2009R.",
"orcid": "0000-0002-5127-0401"
},
{
"family_name": "Ahmed",
"given_name": "Z.",
"orcid": "0000-0002-9957-448X"
},
{
"family_name": "Amiri",
"given_name": "M."
},
{
"family_name": "Barkats",
"given_name": "D.",
"orcid": "0000-0002-8971-1954"
},
{
"family_name": "Basu Thakur",
"given_name": "R.",
"orcid": "0000-0002-3351-3078",
"clpid": "Basu-Thakur-Ritoban"
},
{
"family_name": "Bischoff",
"given_name": "C.\u2009A."
},
{
"family_name": "Beck",
"given_name": "D."
},
{
"family_name": "Bock",
"given_name": "J.\u2009J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Boenish",
"given_name": "H."
},
{
"family_name": "Buza",
"given_name": "V."
},
{
"family_name": "Cheshire",
"given_name": "J.\u2009R.",
"orcid": "0000-0002-1630-7854",
"clpid": "Cheshire-James-R"
},
{
"family_name": "Connors",
"given_name": "J."
},
{
"family_name": "Cornelison",
"given_name": "J.",
"orcid": "0000-0002-2088-7345"
},
{
"family_name": "Crumrine",
"given_name": "M."
},
{
"family_name": "Cukierman",
"given_name": "A.\u2009J."
},
{
"family_name": "Denison",
"given_name": "E."
},
{
"family_name": "Duband",
"given_name": "L."
},
{
"family_name": "Eiben",
"given_name": "M.",
"orcid": "0009-0007-6718-1730"
},
{
"family_name": "Elwood",
"given_name": "B.\u2009D."
},
{
"family_name": "Fatigoni",
"given_name": "S.",
"orcid": "0000-0002-3790-7314",
"clpid": "Fatigoni-S"
},
{
"family_name": "Filippini",
"given_name": "J.\u2009P."
},
{
"family_name": "Fortes",
"given_name": "A."
},
{
"family_name": "Gao",
"given_name": "M.",
"clpid": "Gao-M"
},
{
"family_name": "Giannakopoulos",
"given_name": "C."
},
{
"family_name": "Goeckner-Wald",
"given_name": "N."
},
{
"family_name": "Goldfinger",
"given_name": "D.\u2009C."
},
{
"family_name": "Grayson",
"given_name": "J.\u2009A."
},
{
"family_name": "Greathouse",
"given_name": "A."
},
{
"family_name": "Grimes",
"given_name": "P.\u2009K.",
"orcid": "0000-0001-9292-6297"
},
{
"family_name": "Hall",
"given_name": "G."
},
{
"family_name": "Halal",
"given_name": "G.",
"orcid": "0000-0003-2221-3018"
},
{
"family_name": "Halpern",
"given_name": "M."
},
{
"family_name": "Hand",
"given_name": "E."
},
{
"family_name": "Harrison",
"given_name": "S.\u2009A."
},
{
"family_name": "Henderson",
"given_name": "S."
},
{
"family_name": "Hubmayr",
"given_name": "J."
},
{
"family_name": "Hui",
"given_name": "H.",
"orcid": "0000-0001-5812-1903",
"clpid": "Hui-Howard"
},
{
"family_name": "Irwin",
"given_name": "K.\u2009D.",
"orcid": "0000-0002-2998-9743"
},
{
"family_name": "Kang",
"given_name": "J.\u2009H.",
"clpid": "Kang-J-H"
},
{
"family_name": "Karkare",
"given_name": "K.\u2009S."
},
{
"family_name": "Kefeli",
"given_name": "S.",
"clpid": "Kefeli-S"
},
{
"family_name": "Kovac",
"given_name": "J.\u2009M.",
"orcid": "0009-0003-5432-7180"
},
{
"family_name": "Kuo",
"given_name": "C.",
"orcid": "0000-0003-4895-5247"
},
{
"family_name": "Lau",
"given_name": "K.",
"clpid": "Lau-K"
},
{
"family_name": "Lautzenhiser",
"given_name": "M."
},
{
"family_name": "Lennox",
"given_name": "A."
},
{
"family_name": "Liu",
"given_name": "T.",
"orcid": "0000-0001-5677-5188"
},
{
"family_name": "Megerian",
"given_name": "K.\u2009G."
},
{
"family_name": "Minutolo",
"given_name": "L.",
"orcid": "0000-0002-4876-112X",
"clpid": "Minutolo-Lorenzo"
},
{
"family_name": "Moncelsi",
"given_name": "L.",
"orcid": "0000-0002-4242-3015",
"clpid": "Moncelsi-Lorenzo"
},
{
"family_name": "Nakato",
"given_name": "Y."
},
{
"family_name": "Nguyen",
"given_name": "H.\u2009T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "O'brient",
"given_name": "R.",
"orcid": "0000-0002-4987-6375",
"clpid": "O'brient-Roger"
},
{
"family_name": "Patel",
"given_name": "A."
},
{
"family_name": "Petroff",
"given_name": "M.\u2009A."
},
{
"family_name": "Polish",
"given_name": "A.\u2009R."
},
{
"family_name": "Prouve",
"given_name": "T."
},
{
"family_name": "Pryke",
"given_name": "C.",
"orcid": "0000-0003-3983-6668"
},
{
"family_name": "Reintsema",
"given_name": "C.\u2009D."
},
{
"family_name": "Romand",
"given_name": "T.",
"orcid": "0009-0000-7421-8908",
"clpid": "Romand-Thibault"
},
{
"family_name": "Salatino",
"given_name": "M."
},
{
"family_name": "Schillaci",
"given_name": "A.",
"orcid": "0000-0002-0512-1042",
"clpid": "Schillaci-Alessandro"
},
{
"family_name": "Schmitt",
"given_name": "B."
},
{
"family_name": "Singari",
"given_name": "B."
},
{
"family_name": "Sjoberg",
"given_name": "K."
},
{
"family_name": "Soliman",
"given_name": "A.",
"clpid": "Soliman-A"
},
{
"family_name": "St Germaine",
"given_name": "T."
},
{
"family_name": "Steiger",
"given_name": "A."
},
{
"family_name": "Steinbach",
"given_name": "B.",
"orcid": "0000-0001-6544-7469",
"clpid": "Steinbach-Bryan"
},
{
"family_name": "Sudiwala",
"given_name": "R."
},
{
"family_name": "Thompson",
"given_name": "K.\u2009L."
},
{
"family_name": "Tsai",
"given_name": "C."
},
{
"family_name": "Tucker",
"given_name": "C.",
"orcid": "0000-0002-1851-3918"
},
{
"family_name": "Turner",
"given_name": "A.\u2009D.",
"clpid": "Turner-A-D"
},
{
"family_name": "Verg\u00e8s",
"given_name": "C.",
"orcid": "0000-0002-3942-1609"
},
{
"family_name": "Vieregg",
"given_name": "A.\u2009G."
},
{
"family_name": "Wandui",
"given_name": "A.",
"orcid": "0000-0002-8232-7343",
"clpid": "Wandui-Albert"
},
{
"family_name": "Weber",
"given_name": "A.\u2009C.",
"clpid": "Weber-A-C"
},
{
"family_name": "Willmert",
"given_name": "J."
},
{
"family_name": "Wu",
"given_name": "W.\u2009L.\u2009K."
},
{
"family_name": "Yang",
"given_name": "H."
},
{
"family_name": "Yu",
"given_name": "C."
},
{
"family_name": "Zeng",
"given_name": "L."
},
{
"family_name": "Zhang",
"given_name": "C.",
"orcid": "0000-0001-8288-5823",
"clpid": "Zhang-Cheng"
},
{
"family_name": "Zhang",
"given_name": "S."
},
{
"literal": "BICEP/Keck Collaboration"
}
],
"abstract": "We use a custom-made calibrator to measure individual detectors’ polarization angles of BICEP3, a small aperture telescope observing the cosmic microwave background (CMB) at 95 GHz from the South Pole. We describe our calibration strategy and the statistical and systematic uncertainties associated with the measurement. We reach an unprecedented precision for such measurement on a CMB experiment, with a repeatability for each detector pair of 0.02°. We show that the relative angles measured using this method are in excellent agreement with those extracted from CMB data. Because the absolute measurement is currently limited by a systematic uncertainty, we do not derive cosmic birefringence constraints from BICEP3 data in this work. Rather, we forecast the sensitivity of BICEP3 sky maps for such analysis. We investigate the relative contributions of instrument noise, lensing, and dust, as well as astrophysical and instrumental systematics. We also explore the constraining power of different angle estimators, depending on analysis choices. We establish that the BICEP3 2-year dataset (2017–2018) has an on-sky sensitivity to the cosmic birefringence angle of \ud835\udf0e\ud835\udefc =0.07\u20628°, which could be improved to \ud835\udf0e\ud835\udefc =0.05\u20625° by adding all of the existing BICEP3 data (through 2023). Furthermore, we emphasize the possibility of using the BICEP3 sky patch as a polarization calibration source for CMB experiments, which with the present data could reach a precision of 0.035°. Finally, in the context of inflation searches, we investigate the impact of detector-to-detector variations in polarization angles as they may bias the tensor-to-scalar ratio \ud835\udc5f. We show that while the effect is expected to remain subdominant to other sources of systematic uncertainty, it can be reliably calibrated using polarization angle measurements such as the ones we present in this paper.
",
"doi": "10.1103/physrevd.111.063505",
"issn": "2470-0010",
"publisher": "American Physical Society",
"publication": "Physical Review D",
"publication_date": "2025-03-03",
"series_number": "6",
"volume": "111",
"issue": "6",
"pages": "063505"
},
{
"id": "authors:zrg1z-qv096",
"collection": "authors",
"collection_id": "zrg1z-qv096",
"cite_using_url": "https://authors.library.caltech.edu/records/zrg1z-qv096",
"type": "article",
"title": "Improving H2RG Performance in SPHEREx Brassboard Model",
"author": [
{
"family_name": "Nguyen",
"given_name": "Chi H.",
"orcid": "0000-0001-9368-3186",
"clpid": "Nguyen-Chi-H"
},
{
"family_name": "Korngut",
"given_name": "Phillip",
"clpid": "Korngut-Philip-M"
},
{
"family_name": "Dowell",
"given_name": "C. Darren"
},
{
"family_name": "Bock",
"given_name": "James",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Burnham",
"given_name": "Jill",
"clpid": "Burnham-Jill-A"
},
{
"family_name": "Condon",
"given_name": "Samuel",
"orcid": "0000-0003-4255-3650",
"clpid": "Samuel-Condon"
},
{
"family_name": "Cook",
"given_name": "Walter",
"clpid": "Cook-Walter-Richardson-III"
},
{
"family_name": "Heaton",
"given_name": "Grigory",
"orcid": "0009-0003-5681-2956",
"clpid": "Heaton-Grigory-J"
},
{
"family_name": "Hui",
"given_name": "Howard",
"orcid": "0000-0001-5812-1903",
"clpid": "Hui-Howard"
},
{
"family_name": "Kecman",
"given_name": "Branislav",
"clpid": "Kecman-Branislav"
},
{
"family_name": "Miyasaka",
"given_name": "Hiromasa",
"orcid": "0000-0002-8074-4186",
"clpid": "Miyasaka-Hiromasa"
},
{
"family_name": "Manatt",
"given_name": "Kenneth"
},
{
"family_name": "Nguyen",
"given_name": "Hien T."
},
{
"family_name": "Padin",
"given_name": "Stephen",
"orcid": "0009-0001-9993-4393",
"clpid": "Padin-Stephen"
},
{
"family_name": "Viero",
"given_name": "Marco",
"orcid": "0000-0003-0545-4872",
"clpid": "Viero-Marco"
}
],
"abstract": "Spectro-Photometer for the History of the Universe, Epoch of Reionization, and Ices Explorer is an upcoming NASA satellite mission to study the physics of inflation, the history of galaxy formation, and the abundance of biogenic ices in the Milky Way, obtaining the first all-sky spectroscopic survey at infrared wavelengths 0.75–5.0 μm. The instrument implements HAWAII-2RG (H2RG) detectors and custom-built Video8 electronics with multiple sampling features to optimize the H2RG noise performance, including nonsequential row reads, voltage monitoring, multiple visits to optically dark reference pixels, as well as onboard slope fitting and cosmic-ray removal. We report here the performance of a single H2RG with the readout electronics. We focus on the effectiveness of multiple reference samplings to reduce 1/f noise most relevant to the galaxy formation analysis, in particular the noise on large angular scales k <0.13 [pix−1] (∼5''–20'') where the imprints of galaxy clustering will be measured. Our characterization confirms that increased sampling of reference pixels successfully reduces the 1/f noise by ∼50% at these scales. However, the effectiveness of multiple reference reads is limited by irreducible per-pixel telegraph noise. Further noise reduction can be achieved by using optical pixels in addition to the reference pixels to remove common-mode signal offsets in each channel. Additionally, we observe that the gain of optical pixels is consistently ∼90% that of the reference pixels, prompting additional correction steps in the data reduction pipeline.
",
"doi": "10.3847/1538-4365/ad97bd",
"issn": "0067-0049",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Supplement Series",
"publication_date": "2025-02",
"series_number": "2",
"volume": "276",
"issue": "2",
"pages": "43"
},
{
"id": "authors:z5b92-16p28",
"collection": "authors",
"collection_id": "z5b92-16p28",
"cite_using_url": "https://authors.library.caltech.edu/records/z5b92-16p28",
"type": "article",
"title": "Analysis of Polarized Dust Emission Using Data from the First Flight of SPIDER",
"author": [
{
"family_name": "Ade",
"given_name": "P. A. R."
},
{
"family_name": "Amiri",
"given_name": "M."
},
{
"family_name": "Benton",
"given_name": "S. J.",
"orcid": "0000-0002-4214-9298"
},
{
"family_name": "Bergman",
"given_name": "A. S."
},
{
"family_name": "Bihary",
"given_name": "R."
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bond",
"given_name": "J. R.",
"orcid": "0000-0003-2358-9949"
},
{
"family_name": "Bonetti",
"given_name": "J. A."
},
{
"family_name": "Bryan",
"given_name": "S. A."
},
{
"family_name": "Chiang",
"given_name": "H. C."
},
{
"family_name": "Contaldi",
"given_name": "C. R.",
"orcid": "0000-0001-7285-0707"
},
{
"family_name": "Dor\u00e9",
"given_name": "O.",
"orcid": "0000-0001-7432-2932",
"clpid": "Dor\u00e9-O"
},
{
"family_name": "Duivenvoorden",
"given_name": "A. J.",
"orcid": "0000-0003-2856-2382"
},
{
"family_name": "Eriksen",
"given_name": "H. K."
},
{
"family_name": "Filippini",
"given_name": "J. P.",
"orcid": "0000-0001-8217-6832"
},
{
"family_name": "Fraisse",
"given_name": "A. A."
},
{
"family_name": "Freese",
"given_name": "K."
},
{
"family_name": "Galloway",
"given_name": "M."
},
{
"family_name": "Gambrel",
"given_name": "A. E."
},
{
"family_name": "Gandilo",
"given_name": "N. N."
},
{
"family_name": "Ganga",
"given_name": "K."
},
{
"family_name": "Gourapura",
"given_name": "S.",
"orcid": "0000-0002-8149-0632"
},
{
"family_name": "Gualtieri",
"given_name": "R.",
"orcid": "0000-0003-4245-2315"
},
{
"family_name": "Gudmundsson",
"given_name": "J. E.",
"orcid": "0000-0003-1760-0355"
},
{
"family_name": "Halpern",
"given_name": "M."
},
{
"family_name": "Hartley",
"given_name": "J.",
"orcid": "0009-0006-9861-9718"
},
{
"family_name": "Hasselfield",
"given_name": "M."
},
{
"family_name": "Hilton",
"given_name": "G."
},
{
"family_name": "Holmes",
"given_name": "W."
},
{
"family_name": "Hristov",
"given_name": "V. V.",
"orcid": "0009-0008-9575-7538",
"clpid": "Hrostov-Viktor-V"
},
{
"family_name": "Huang",
"given_name": "Z.",
"orcid": "0000-0002-1506-1063"
},
{
"family_name": "Irwin",
"given_name": "K. D.",
"orcid": "0000-0002-2998-9743"
},
{
"family_name": "Jones",
"given_name": "W. C.",
"orcid": "0000-0002-3636-1241"
},
{
"family_name": "Karakci",
"given_name": "A."
},
{
"family_name": "Kuo",
"given_name": "C. L."
},
{
"family_name": "Kermish",
"given_name": "Z. D."
},
{
"family_name": "Leung",
"given_name": "J. S.-Y.",
"orcid": "0000-0001-7116-3710"
},
{
"family_name": "Li",
"given_name": "S.",
"orcid": "0000-0002-8896-911X"
},
{
"family_name": "Mak",
"given_name": "D. S. Y."
},
{
"family_name": "Mason",
"given_name": "P. V.",
"orcid": "0000-0002-7963-7420",
"clpid": "Mason-Peter-Vroman"
},
{
"family_name": "Megerian",
"given_name": "K."
},
{
"family_name": "Moncelsi",
"given_name": "L.",
"orcid": "0000-0002-4242-3015",
"clpid": "Moncelsi-Lorenzo"
},
{
"family_name": "Morford",
"given_name": "T. A.",
"clpid": "Morford-T-A"
},
{
"family_name": "Nagy",
"given_name": "J. M.",
"orcid": "0000-0002-2036-7008"
},
{
"family_name": "Netterfield",
"given_name": "C. B."
},
{
"family_name": "Nolta",
"given_name": "M."
},
{
"family_name": "O'Brient",
"given_name": "R."
},
{
"family_name": "Osherson",
"given_name": "B."
},
{
"family_name": "Padilla",
"given_name": "I. L.",
"orcid": "0000-0002-0024-2662"
},
{
"family_name": "Racine",
"given_name": "B."
},
{
"family_name": "Rahlin",
"given_name": "A. S.",
"orcid": "0000-0003-3953-1776"
},
{
"family_name": "Reintsema",
"given_name": "C."
},
{
"family_name": "Ruhl",
"given_name": "J. E.",
"orcid": "0000-0001-5875-4751"
},
{
"family_name": "Runyan",
"given_name": "M. C.",
"orcid": "0000-0002-9554-5710",
"clpid": "Runyan-Marcus-Christian"
},
{
"family_name": "Ruud",
"given_name": "T. M.",
"orcid": "0000-0002-7615-1900"
},
{
"family_name": "Shariff",
"given_name": "J. A."
},
{
"family_name": "Shaw",
"given_name": "E. C.",
"orcid": "0000-0001-5644-8750"
},
{
"family_name": "Shiu",
"given_name": "C.",
"orcid": "0000-0002-6635-5950"
},
{
"family_name": "Soler",
"given_name": "J. D."
},
{
"family_name": "Song",
"given_name": "X."
},
{
"family_name": "Trangsrud",
"given_name": "A.",
"clpid": "Trangsrud-Amy-Ruth"
},
{
"family_name": "Tucker",
"given_name": "C."
},
{
"family_name": "Tucker",
"given_name": "R. S.",
"clpid": "Tucker-Rebecca-Suzanne"
},
{
"family_name": "Turner",
"given_name": "A. D."
},
{
"family_name": "van der List",
"given_name": "J. F."
},
{
"family_name": "Weber",
"given_name": "A. C."
},
{
"family_name": "Wehus",
"given_name": "I. K.",
"orcid": "0000-0003-3821-7275"
},
{
"family_name": "Wiebe",
"given_name": "D. V."
},
{
"family_name": "Young",
"given_name": "E. Y."
},
{
"literal": "Spider Collaboration"
}
],
"abstract": "Using data from the first flight of Spider and from the Planck High Frequency Instrument, we probe the properties of polarized emission from interstellar dust in the Spider observing region. Component-separation algorithms operating in both the spatial and harmonic domains are applied to probe their consistency and to quantify modeling errors associated with their assumptions. Analyses of diffuse Galactic dust emission spanning the full Spider region demonstrate (i) a spectral energy distribution that is broadly consistent with a modified-blackbody (MBB) model with a spectral index of βd = 1.45 ± 0.05 (1.47 ± 0.06) for E (B)-mode polarization, slightly lower than that reported by Planck for the full sky; (ii) an angular power spectrum broadly consistent with a power law; and (iii) no significant detection of line-of-sight polarization decorrelation. Tests of several modeling uncertainties find only a modest impact (∼10% in σr) on Spider's sensitivity to the cosmological tensor-to-scalar ratio. The size of the Spider region further allows for a statistically meaningful analysis of the variation in foreground properties within it. Assuming a fixed dust temperature Td = 19.6 K, an analysis of two independent subregions of that field results in inferred values of βd = 1.52 ± 0.06 and βd = 1.09 ± 0.09, which are inconsistent at the 3.9σ level. Furthermore, a joint analysis of Spider and Planck 217 and 353 GHz data within one subregion is inconsistent with a simple MBB at more than 3σ, assuming a common morphology of polarized dust emission over the full range of frequencies. This evidence of variation may inform the component-separation approaches of future cosmic microwave background polarization experiments.
",
"doi": "10.3847/1538-4357/ad900c",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2025-01-01",
"series_number": "2",
"volume": "978",
"issue": "2",
"pages": "130"
},
{
"id": "authors:1ax8j-1cp24",
"collection": "authors",
"collection_id": "1ax8j-1cp24",
"cite_using_url": "https://authors.library.caltech.edu/records/1ax8j-1cp24",
"type": "article",
"title": "The Universe SPHEREx Will See: Empirically Based Galaxy Simulations and Redshift Predictions",
"author": [
{
"family_name": "Feder",
"given_name": "Richard M.",
"orcid": "0000-0002-9330-8738",
"clpid": "Feder-Richard-M"
},
{
"family_name": "Masters",
"given_name": "Daniel C.",
"orcid": "0000-0001-5382-6138",
"clpid": "Masters-Daniel-C"
},
{
"family_name": "Lee",
"given_name": "Bomee",
"orcid": "0000-0003-1954-5046"
},
{
"family_name": "Bock",
"given_name": "James J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Chiang",
"given_name": "Yi-Kuan",
"orcid": "0000-0001-6320-261X"
},
{
"family_name": "Dor\u00e9",
"given_name": "Olivier",
"orcid": "0000-0001-7432-2932",
"clpid": "Dor\u00e9-Olivier"
},
{
"family_name": "Hemmati",
"given_name": "Shoubaneh",
"orcid": "0000-0003-2226-5395",
"clpid": "Hemmati-Shoubaneh"
},
{
"family_name": "Ilbert",
"given_name": "Olivier",
"orcid": "0000-0002-7303-4397"
}
],
"abstract": "\n
We simulate galaxy properties and redshift estimation for SPHEREx, the next NASA Medium Class Explorer. To make robust models of the galaxy population and test the spectrophotometric redshift performance for SPHEREx, we develop a set of synthetic spectral energy distributions based on detailed fits to COSMOS2020 photometry spanning 0.1–8 μm. Given that SPHEREx obtains low-resolution spectra, emission lines will be important for some fraction of galaxies. Here, we expand on previous work, using better photometry and photometric redshifts from COSMOS2020 and tight empirical relations to predict robust emission-line strengths and ratios. A second galaxy catalog derived from the GAMA survey is generated to ensure the bright (mAB < 18 in the i band) sample is representative over larger areas. Using template fitting to estimate photometric continuum redshifts, we forecast the recovery of 19 million galaxies over 30,000 deg2 with redshifts better than σz < 0.003(1 + z), 445 million with σz < 0.1(1 + z), and 810 million with σz < 0.2(1 + z). We also find through idealized tests that emission-line information from spectrally dithered flux measurements can yield redshifts with accuracy beyond that implied by the naive SPHEREx channel resolution, motivating the development of a hybrid continuum–line redshift estimation approach.
\n
We describe a technique for measuring focus errors in a cryogenic, wide-field, near-infrared space telescope. The measurements are made with a collimator looking through a large vacuum window, with a reflective cold filter to reduce the background thermal infrared loading on the detectors and optics. The vacuum window and cold filter introduce a wavefront error that we characterize using an autocollimating microscope. For the 200 mm diameter aperture f/3 space telescope SPHEREx, we achieve a focus position measurement with a ∼15µm systematic and a ∼5µm statistical error.
",
"doi": "10.1364/ao.514784",
"issn": "1559-128X",
"publisher": "Optica Publishing Group",
"publication": "Applied Optics",
"publication_date": "2024-05-01",
"series_number": "13",
"volume": "63",
"issue": "13",
"pages": "3453"
},
{
"id": "authors:rez6n-4zx12",
"collection": "authors",
"collection_id": "rez6n-4zx12",
"cite_using_url": "https://authors.library.caltech.edu/records/rez6n-4zx12",
"type": "article",
"title": "Design and Performance of a 30/40 GHz Diplexed Focal Plane for the BICEP Array",
"author": [
{
"family_name": "Shiu",
"given_name": "Corwin",
"orcid": "0000-0002-6635-5950",
"clpid": "Shiu-Corwin"
},
{
"family_name": "Soliman",
"given_name": "Ahmed",
"orcid": "0009-0007-9335-1326",
"clpid": "Soliman-Ahmed"
},
{
"family_name": "O'Brient",
"given_name": "Roger",
"orcid": "0000-0002-4987-6375",
"clpid": "O'Brient-Roger-C"
},
{
"family_name": "Steinbach",
"given_name": "Bryan",
"orcid": "0000-0001-6544-7469",
"clpid": "Steinbach-Bryan-A"
},
{
"family_name": "Bock",
"given_name": "James J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Frez",
"given_name": "Clifford F.",
"clpid": "Frez-Clifford-F"
},
{
"family_name": "Jones",
"given_name": "William C.",
"orcid": "0000-0002-3636-1241",
"clpid": "Jones-William-C"
},
{
"family_name": "Megerian",
"given_name": "Krikor. G.",
"clpid": "Megerian-Krikor-G"
},
{
"family_name": "Moncelsi",
"given_name": "Lorenzo",
"orcid": "0000-0002-4242-3015",
"clpid": "Moncelsi-Lorenzo"
},
{
"family_name": "Schillaci",
"given_name": "Alessandro",
"orcid": "0000-0002-0512-1042",
"clpid": "Schillaci-Alessandro"
},
{
"family_name": "Turner",
"given_name": "Anthony D.",
"clpid": "Turner-Anthony-D"
},
{
"family_name": "Weber",
"given_name": "Alexis C.",
"clpid": "Weber-Alexis-C"
},
{
"family_name": "Zhang",
"given_name": "Cheng",
"orcid": "0000-0001-8288-5823",
"clpid": "Zhang-Cheng"
},
{
"family_name": "Zhang",
"given_name": "Silvia",
"clpid": "Zhang-Silvia"
}
],
"abstract": "\n
We demonstrate a wideband diplexed focal plane suitable for observing low-frequency foregrounds that are important for cosmic microwave background polarimetry. The antenna elements are composed of slotted bowtie antennas with 60% bandwidth that can be partitioned into two bands. Each pixel is composed of two interleaved 12 × 12 pairs of linearly polarized antenna elements forming a phased array, designed to synthesize a symmetric beam with no need for focusing optics. The signal from each antenna element is captured in-phase and uniformly weighted by a microstrip summing tree. The antenna signal is diplexed into two bands through the use of two complementary, six-pole Butterworth filters. This filter architecture ensures a contiguous impedance match at all frequencies, and thereby achieves minimal reflection loss between both bands. Subsequently, out-of-band rejection is increased with a bandpass filter and the signal is then deposited on a transition-edge sensor bolometer island. We demonstrate the performance of this focal plane with two distinct bands, 30 and 40 GHz, each with a bandwidth of ∼20 and 15 GHz, respectively. The unequal bandwidths between the two bands are caused by an unintentional shift in diplexer frequency from its design values. The end-to-end optical efficiency of these detectors is relatively modest, at 20%–30%, with an efficiency loss due to an unknown impedance mismatch in the summing tree. Far-field beam maps show good optical characteristics, with edge pixels having no more than ∼5% ellipticity and ∼10%–15% peak-to-peak differences for A–B polarization pairs.
\n
We report measurements of the fluctuations in atmospheric emission (atmospheric noise) above Mauna Kea recorded with Bolocam at 143 and 268 GHz from the Caltech Submillimeter Observatory. The 143 GHz data were collected during a 40 night observing run in late 2003, and the 268 GHz observations were made in early 2004 and early 2005 over a total of 60 nights. Below \u22430.5 Hz, the data time-streams are dominated by atmospheric noise in all observing conditions. The atmospheric noise data are consistent with a Kolmogorov–Taylor turbulence model for a thin wind-driven screen, and the median amplitude of the fluctuations is 280 mK2 rad−5/3 at 143 GHz and 4000 mK2 rad−5/3 at 268 GHz. Comparing our results with previous ACBAR data, we find that the normalization of the power spectrum of the atmospheric noise fluctuations is a factor of \u224380 larger above Mauna Kea than above the South Pole at millimeter wavelengths. Most of this difference is due to the fact that the atmosphere above the South Pole is much drier than the atmosphere above Mauna Kea. However, the atmosphere above the South Pole is slightly more stable as well: the fractional fluctuations in the column depth of precipitable water vapor are a factor of \u2243√2 smaller at the South Pole compared to Mauna Kea. Based on our atmospheric modeling, we developed several algorithms to remove the atmospheric noise, and the best results were achieved when we described the fluctuations using a low-order polynomial in detector position over the 8' field of view. However, even with these algorithms, we were not able to reach photon-background-limited instrument photometer performance at frequencies below \u22430.5 Hz in any observing conditions. We also observed an excess low-frequency noise that is highly correlated between detectors separated by \u2272(f/#)λ; this noise appears to be caused by atmospheric fluctuations, but we do not have an adequate model to explain its source. We hypothesize that the correlations arise from the classical coherence of the electromagnetic field across a distance of \u2243(f/#)λ on the focal plane.
",
"doi": "10.1088/0004-637X/708/2/1674",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2010-01-10",
"series_number": "2",
"volume": "708",
"issue": "2",
"pages": "1674-1691"
},
{
"id": "authors:62a8a-grz27",
"collection": "authors",
"collection_id": "62a8a-grz27",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100106-132419629",
"type": "article",
"title": "The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) 2006: Calibration and Flight Performance",
"author": [
{
"family_name": "Truch",
"given_name": "Matthew D. P",
"clpid": "Truch-M-D-P"
},
{
"family_name": "Ade",
"given_name": "Peter A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Bock",
"given_name": "James J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Chapin",
"given_name": "Edward L.",
"clpid": "Chapin-E-L"
},
{
"family_name": "Devlin",
"given_name": "Mark J.",
"clpid": "Devlin-M-J"
},
{
"family_name": "Dicker",
"given_name": "Simon R.",
"clpid": "Dicker-S-R"
},
{
"family_name": "Griffin",
"given_name": "Matthew",
"clpid": "Griffin-M"
},
{
"family_name": "Gundersen",
"given_name": "Joshua O.",
"clpid": "Gundersen-J-O"
},
{
"family_name": "Halpern",
"given_name": "Mark",
"orcid": "0000-0002-1760-0868",
"clpid": "Halpern-M"
},
{
"family_name": "Hargrave",
"given_name": "Peter C.",
"orcid": "0000-0002-3109-6629",
"clpid": "Hargrave-P-C"
},
{
"family_name": "Hughes",
"given_name": "David H.",
"clpid": "Hughes-D-H"
},
{
"family_name": "Klein",
"given_name": "Jeff",
"clpid": "Klein-J"
},
{
"family_name": "Marsden",
"given_name": "Gaelen",
"clpid": "Marsden-Gaelen"
},
{
"family_name": "Martin",
"given_name": "Peter G.",
"orcid": "0000-0002-5236-3896",
"clpid": "Martin-P-G"
},
{
"family_name": "Mauskopf",
"given_name": "Philip",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "Moncelsi",
"given_name": "Lorenzo",
"orcid": "0000-0002-4242-3015",
"clpid": "Moncelsi-Lorenzo"
},
{
"family_name": "Netterfield",
"given_name": "C. Barth",
"clpid": "Netterfield-C-B"
},
{
"family_name": "Olmi",
"given_name": "Luca",
"orcid": "0000-0002-1162-7947",
"clpid": "Olmi-L"
},
{
"family_name": "Pascale",
"given_name": "Enzo",
"orcid": "0000-0002-3242-8154",
"clpid": "Pascale-E"
},
{
"family_name": "Patanchon",
"given_name": "Guillaume",
"clpid": "Patanchon-G"
},
{
"family_name": "Rex",
"given_name": "Marie",
"clpid": "Rex-M"
},
{
"family_name": "Scott",
"given_name": "Douglas",
"orcid": "0000-0002-6878-9840",
"clpid": "Scott-Douglas"
},
{
"family_name": "Semisch",
"given_name": "Christopher",
"clpid": "Semisch-C"
},
{
"family_name": "Thomas",
"given_name": "Nicholas E.",
"clpid": "Thomas-Nicholas-E"
},
{
"family_name": "Tucker",
"given_name": "Carole",
"clpid": "Tucker-C-E"
},
{
"family_name": "Tucker",
"given_name": "Gregory S.",
"orcid": "0000-0002-6954-6947",
"clpid": "Tucker-G-S"
},
{
"family_name": "Viero",
"given_name": "Marco P.",
"clpid": "Viero-M-P"
},
{
"family_name": "Wiebe",
"given_name": "Donald V.",
"clpid": "Wiebe-D-V"
}
],
"abstract": "The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) operated successfully during a 250 hr flight over Antarctica in 2006 December (BLAST06). As part of the calibration and pointing procedures, the red hypergiant star VY CMa was observed and used as the primary calibrator. Details of the overall BLAST06 calibration procedure are discussed. The 1\u03c3 uncertainty on the absolute calibration is accurate to 9.5%, 8.7%, and 9.2% at the 250, 350, and 500 \u03bcm bands, respectively. The errors are highly correlated between bands resulting in much lower errors for the derived shape of the 250-500 \u03bcm continuum. The overall pointing error is < 5'' rms for the 36'', 42'', and 60'' beams. The performance of optics and pointing systems is discussed.",
"doi": "10.1088/0004-637X/707/2/1723",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2009-12-20",
"series_number": "2",
"volume": "707",
"issue": "2",
"pages": "1723-1728"
},
{
"id": "authors:0qqt9-kx166",
"collection": "authors",
"collection_id": "0qqt9-kx166",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100106-113854541",
"type": "article",
"title": "BLAST Observations of Resolved Galaxies: Temperature Profiles and the Effect of Active Galactic Nuclei on FIR to Submillimeter Emission",
"author": [
{
"family_name": "Wiebe",
"given_name": "Donald V.",
"clpid": "Wiebe-D-V"
},
{
"family_name": "Ade",
"given_name": "Peter A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Bock",
"given_name": "James J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Chapin",
"given_name": "Edward L.",
"clpid": "Chapin-E-L"
},
{
"family_name": "Devlin",
"given_name": "Mark J.",
"clpid": "Devlin-M-J"
},
{
"family_name": "Dicker",
"given_name": "Simon",
"clpid": "Dicker-S-R"
},
{
"family_name": "Griffin",
"given_name": "Matthew",
"clpid": "Griffin-M"
},
{
"family_name": "Gundersen",
"given_name": "Joshua O.",
"clpid": "Gundersen-J-O"
},
{
"family_name": "Halpern",
"given_name": "Mark",
"orcid": "0000-0002-1760-0868",
"clpid": "Halpern-M"
},
{
"family_name": "Hargrave",
"given_name": "Peter C.",
"orcid": "0000-0002-3109-6629",
"clpid": "Hargrave-P-C"
},
{
"family_name": "Hughes",
"given_name": "David H.",
"clpid": "Hughes-D-H"
},
{
"family_name": "Klein",
"given_name": "Jeff",
"clpid": "Klein-J"
},
{
"family_name": "Marsden",
"given_name": "Gaelen",
"clpid": "Marsden-Gaelen"
},
{
"family_name": "Martin",
"given_name": "Peter G.",
"orcid": "0000-0002-5236-3896",
"clpid": "Martin-P-G"
},
{
"family_name": "Mauskopf",
"given_name": "Philip",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "Netterfield",
"given_name": "Calvin B.",
"clpid": "Netterfield-C-B"
},
{
"family_name": "Olmi",
"given_name": "Luca",
"orcid": "0000-0002-1162-7947",
"clpid": "Olmi-L"
},
{
"family_name": "Pascale",
"given_name": "Enzo",
"orcid": "0000-0002-3242-8154",
"clpid": "Pascale-E"
},
{
"family_name": "Patanchon",
"given_name": "Guillaume",
"clpid": "Patanchon-G"
},
{
"family_name": "Rex",
"given_name": "Marie",
"clpid": "Rex-M"
},
{
"family_name": "Scott",
"given_name": "Douglas",
"orcid": "0000-0002-6878-9840",
"clpid": "Scott-Douglas"
},
{
"family_name": "Semisch",
"given_name": "Christopher",
"clpid": "Semisch-C"
},
{
"family_name": "Thomas",
"given_name": "Nicholas E.",
"clpid": "Thomas-Nicholas-E"
},
{
"family_name": "Truch",
"given_name": "Matthew D. P.",
"clpid": "Truch-M-D-P"
},
{
"family_name": "Tucker",
"given_name": "Carole",
"clpid": "Tucker-C-E"
},
{
"family_name": "Tucker",
"given_name": "Gregory S.",
"orcid": "0000-0002-6954-6947",
"clpid": "Tucker-G-S"
},
{
"family_name": "Viero",
"given_name": "Marco P.",
"clpid": "Viero-M-P"
}
],
"abstract": "Over the course of two flights, the Balloon-borne Large Aperture Submillimeter Telescope (BLAST) made resolved maps of seven nearby (<25 Mpc) galaxies at 250, 350, and 500 \u03bcm. During its 2005 June flight from Sweden, BLAST observed a single nearby galaxy, NGC 4565. During the 2006 December flight from Antarctica, BLAST observed the nearby galaxies NGC 1097, NGC 1291, NGC 1365, NGC 1512, NGC 1566, and NGC 1808. We fit physical dust models to a combination of BLAST observations and other available data for the galaxies observed by Spitzer. We fit a modified blackbody to the remaining galaxies to obtain total dust mass and mean dust temperature. For the four galaxies with Spitzer data, we also produce maps and radial profiles of dust column density and temperature. We measure the fraction of BLAST detected flux originating from the central cores of these galaxies and use this to calculate a \"core fraction,\" an upper limit on the \"active galactic nucleus fraction\" of these galaxies. We also find our resolved observations of these galaxies give a dust mass estimate 5-19 times larger than an unresolved observation would predict. Finally, we are able to use these data to derive a value for the dust mass absorption coefficient of \u03ba = 0.29 \u00b1 0.03 m^2 kg^(\u20131) at 250 \u03bcm. This study is an introduction to future higher-resolution and higher-sensitivity studies to be conducted by Herschel and SCUBA-2.",
"doi": "10.1088/0004-637X/707/2/1809",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2009-12-20",
"series_number": "2",
"volume": "707",
"issue": "2",
"pages": "1809-1823"
},
{
"id": "authors:6evdf-h2j43",
"collection": "authors",
"collection_id": "6evdf-h2j43",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100107-142047477",
"type": "article",
"title": "The Blast Survey of the Vela Molecular Cloud: Physical Properties of the Dense Cores in Vela-D",
"author": [
{
"family_name": "Olmi",
"given_name": "Luca",
"orcid": "0000-0002-1162-7947",
"clpid": "Olmi-L"
},
{
"family_name": "Ade",
"given_name": "Peter A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Angl\u00e9s-Alc\u00e1zar",
"given_name": "Daniel",
"orcid": "0000-0001-5769-4945",
"clpid": "Angl\u00e9s-Alc\u00e1zar-D"
},
{
"family_name": "Bock",
"given_name": "James J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Chapin",
"given_name": "Edward L.",
"clpid": "Chapin-E-L"
},
{
"family_name": "De Luca",
"given_name": "Massimo",
"clpid": "De-Luca-M"
},
{
"family_name": "Devlin",
"given_name": "Mark J.",
"clpid": "Devlin-M-J"
},
{
"family_name": "Dicker",
"given_name": "Simon",
"clpid": "Dicker-S-R"
},
{
"family_name": "Elia",
"given_name": "Davide",
"clpid": "Elia-D"
},
{
"family_name": "Fazio",
"given_name": "Giovanni G.",
"orcid": "0000-0002-0670-0708",
"clpid": "Fazio-G-G"
},
{
"family_name": "Giannini",
"given_name": "Teresa",
"clpid": "Giannini-T"
},
{
"family_name": "Griffin",
"given_name": "Matthew",
"clpid": "Griffin-M"
},
{
"family_name": "Gundersen",
"given_name": "Joshua O.",
"clpid": "Gundersen-J-O"
},
{
"family_name": "Halpern",
"given_name": "Mark",
"orcid": "0000-0002-1760-0868",
"clpid": "Halpern-M"
},
{
"family_name": "Hargrave",
"given_name": "Peter C.",
"orcid": "0000-0002-3109-6629",
"clpid": "Hargrave-P-C"
},
{
"family_name": "Hughes",
"given_name": "David H.",
"clpid": "Hughes-D-H"
},
{
"family_name": "Klein",
"given_name": "Jeff",
"clpid": "Klein-J"
},
{
"family_name": "Lorenzetti",
"given_name": "Dario",
"clpid": "Lorenzetti-D"
},
{
"family_name": "Marengo",
"given_name": "Massimo",
"orcid": "0000-0001-9910-9230",
"clpid": "Marengo-M"
},
{
"family_name": "Marsden",
"given_name": "Gaelen",
"clpid": "Marsden-Gaelen"
},
{
"family_name": "Martin",
"given_name": "Peter G.",
"orcid": "0000-0002-5236-3896",
"clpid": "Martin-P-G"
},
{
"family_name": "Massi",
"given_name": "Fabrizio",
"clpid": "Massi-F"
},
{
"family_name": "Mauskopf",
"given_name": "Philip",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "Netterfield",
"given_name": "Calvin B.",
"clpid": "Netterfield-C-B"
},
{
"family_name": "Patanchon",
"given_name": "Guillaume",
"clpid": "Patanchon-G"
},
{
"family_name": "Rex",
"given_name": "Marie",
"clpid": "Rex-M"
},
{
"family_name": "Salama",
"given_name": "Alberto",
"clpid": "Salama-A"
},
{
"family_name": "Scott",
"given_name": "Douglas",
"orcid": "0000-0002-6878-9840",
"clpid": "Scott-Douglas"
},
{
"family_name": "Semisch",
"given_name": "Christopher",
"clpid": "Semisch-C"
},
{
"family_name": "Smith",
"given_name": "Howard A.",
"clpid": "Smith-H-A"
},
{
"family_name": "Strafella",
"given_name": "Francesco",
"clpid": "Strafella-F"
},
{
"family_name": "Thomas",
"given_name": "Nicholas E.",
"clpid": "Thomas-Nicholas-E"
},
{
"family_name": "Truch",
"given_name": "Matthew D. P",
"clpid": "Truch-M-D-P"
},
{
"family_name": "Tucker",
"given_name": "Carole",
"clpid": "Tucker-C-E"
},
{
"family_name": "Tucker",
"given_name": "Gregory S.",
"orcid": "0000-0002-6954-6947",
"clpid": "Tucker-G-S"
},
{
"family_name": "Viero",
"given_name": "Marco P.",
"clpid": "Viero-M-P"
},
{
"family_name": "Wiebe",
"given_name": "Donald V.",
"clpid": "Wiebe-D-V"
}
],
"abstract": "The Balloon-borne Large-Aperture Submillimeter Telescope (BLAST) carried out a 250, 350, and 500 \u03bcm survey of the galactic plane encompassing the Vela Molecular Ridge, with the primary goal of identifying the coldest dense cores possibly associated with the earliest stages of star formation. Here, we present the results from observations of the Vela-D region, covering about 4 deg^2, in which we find 141 BLAST cores. We exploit existing data taken with the Spitzer MIPS, IRAC, and SEST-SIMBA instruments to constrain their (single-temperature) spectral energy distributions, assuming a dust emissivity index \u03b2 = 2.0. This combination of data allows us to determine the temperature, luminosity, and mass of each BLAST core, and also enables us to separate starless from protostellar sources. We also analyze the effects that the uncertainties on the derived physical parameters of the individual sources have on the overall physical properties of starless and protostellar cores, and we find that there appear to be a smooth transition from the pre- to the protostellar phase. In particular, for protostellar cores we find a correlation between the MIPS24 flux, associated with the central protostar, and the temperature of the dust envelope. We also find that the core mass function of the Vela-D cores has a slope consistent with other similar (sub)millimeter surveys.",
"doi": "10.1088/0004-637X/707/2/1836",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2009-12-20",
"series_number": "2",
"volume": "707",
"issue": "2",
"pages": "1836-1851"
},
{
"id": "authors:rjnzs-xej41",
"collection": "authors",
"collection_id": "rjnzs-xej41",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091105-090201427",
"type": "article",
"title": "Improved Measurements of the Temperature and Polarization of the Cosmic Microwave Background from QUaD",
"author": [
{
"family_name": "Brown",
"given_name": "M. L.",
"clpid": "Brown-M-L"
},
{
"family_name": "Ade",
"given_name": "P.",
"clpid": "Ade-P"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bowden",
"given_name": "M.",
"clpid": "Bowden-M"
},
{
"family_name": "Cahill",
"given_name": "G.",
"clpid": "Cahill-G"
},
{
"family_name": "Castro",
"given_name": "P. G.",
"clpid": "Castro-P-G"
},
{
"family_name": "Church",
"given_name": "S.",
"clpid": "Church-S"
},
{
"family_name": "Culverhouse",
"given_name": "T.",
"clpid": "Culverhouse-T"
},
{
"family_name": "Friedman",
"given_name": "R. B.",
"clpid": "Friedman-R-B"
},
{
"family_name": "Ganga",
"given_name": "K.",
"clpid": "Ganga-K"
},
{
"family_name": "Gear",
"given_name": "W. K.",
"clpid": "Gear-W-K"
},
{
"family_name": "Gupta",
"given_name": "S.",
"clpid": "Gupta-S"
},
{
"family_name": "Hinderks",
"given_name": "J.",
"clpid": "Hinderks-J"
},
{
"family_name": "Kovac",
"given_name": "J.",
"clpid": "Kovac-J"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Leitch",
"given_name": "E.",
"clpid": "Leitch-E"
},
{
"family_name": "Melhuish",
"given_name": "S. J.",
"clpid": "Melhuish-S-J"
},
{
"family_name": "Memari",
"given_name": "Y.",
"clpid": "Memari-Y"
},
{
"family_name": "Murphy",
"given_name": "J. A.",
"clpid": "Murphy-J-A"
},
{
"family_name": "Orlando",
"given_name": "A.",
"clpid": "Orlando-A"
},
{
"family_name": "O' Sullivan",
"given_name": "C.",
"clpid": "O'Sullivan-C"
},
{
"family_name": "Piccirillo",
"given_name": "L.",
"clpid": "Piccirillo-L"
},
{
"family_name": "Pryke",
"given_name": "C.",
"clpid": "Pryke-C"
},
{
"family_name": "Rajguru",
"given_name": "N.",
"clpid": "Rajguru-N"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Schwarz",
"given_name": "R.",
"clpid": "Schwarz-R"
},
{
"family_name": "Taylor",
"given_name": "A. N.",
"clpid": "Taylor-A-N"
},
{
"family_name": "Thompson",
"given_name": "K. L.",
"clpid": "Thompson-K-L"
},
{
"family_name": "Turner",
"given_name": "A. H.",
"clpid": "Turner-A-H"
},
{
"family_name": "Wu",
"given_name": "E. Y. S.",
"clpid": "Wu-E-Y-S"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
},
{
"literal": "The QUaD collaboration"
}
],
"abstract": "We present an improved analysis of the final data set from the QUaD experiment. Using an improved technique to remove ground contamination, we double the effective sky area and hence increase the precision of our cosmic microwave background (CMB) power spectrum measurements by ~30% versus that previously reported. In addition, we have improved our modeling of the instrument beams and have reduced our absolute calibration uncertainty from 5% to 3.5% in temperature. The robustness of our results is confirmed through extensive jackknife tests, and by way of the agreement that we find between our two fully independent analysis pipelines. For the standard six-parameter \u039bCDM model, the addition of QUaD data marginally improves the constraints on a number of cosmological parameters over those obtained from the WMAP experiment alone. The impact of QUaD data is significantly greater for a model extended to include either a running in the scalar spectral index, or a possible tensor component, or both. Adding both the QUaD data and the results from the Arcminute Cosmology Bolometer Array Receiver experiment, the uncertainty in the spectral index running is reduced by ~25% compared to WMAP alone, while the upper limit on the tensor-to-scalar ratio is reduced from r < 0.48 to r < 0.33 (95% c.l.). This is the strongest limit on tensors to date from the CMB alone. We also use our polarization measurements to place constraints on parity-violating interactions to the surface of last scattering, constraining the energy scale of Lorentz violating interactions to <1.5 \u00d7 10^(\u201343) GeV (68% c.l.). Finally, we place a robust upper limit on the strength of the lensing B-mode signal. Assuming a single flat band power between \u2113 = 200 and \u2113 = 2000, we constrain the amplitude of B-modes to be <0.57 \u03bcK^2 (95% c.l.).",
"doi": "10.1088/0004-637X/705/1/978",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2009-11-01",
"series_number": "1",
"volume": "705",
"issue": "1",
"pages": "978-999"
},
{
"id": "authors:t5akv-mvr98",
"collection": "authors",
"collection_id": "t5akv-mvr98",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091104-144315878",
"type": "article",
"title": "The Warm Molecular Gas around the Cloverleaf Quasar",
"author": [
{
"family_name": "Bradford",
"given_name": "C. M.",
"orcid": "0000-0001-5261-7094",
"clpid": "Bradford-C-M"
},
{
"family_name": "Aguirre",
"given_name": "J. E.",
"orcid": "0000-0002-4810-666X",
"clpid": "Aguirre-J-E"
},
{
"family_name": "Aikin",
"given_name": "R.",
"clpid": "Aikin-R"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Earle",
"given_name": "L.",
"clpid": "Earle-L"
},
{
"family_name": "Glenn",
"given_name": "J.",
"orcid": "0000-0001-7527-2017",
"clpid": "Glenn-J"
},
{
"family_name": "Inami",
"given_name": "H.",
"orcid": "0000-0003-4268-0393",
"clpid": "Inami-Hanae"
},
{
"family_name": "Maloney",
"given_name": "P. R.",
"clpid": "Maloney-P-R"
},
{
"family_name": "Matsuhara",
"given_name": "H.",
"clpid": "Matsuhara-Hideo"
},
{
"family_name": "Naylor",
"given_name": "B. J.",
"clpid": "Naylor-B-J"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
},
{
"family_name": "Zmuidzinas",
"given_name": "J.",
"orcid": "0000-0002-3330-5439",
"clpid": "Zmuidzinas-J"
}
],
"abstract": "We present the first broadband \u03bb = 1 mm spectrum toward the z = 2.56 Cloverleaf quasar, obtained with Z-Spec, a grating spectrograph on the 10.4 m Caltech Submillimeter Observatory. The 190-305 GHz observation band corresponds to the rest frame 272-444 \u03bcm, and we measure the dust continuum as well as all four transitions of carbon monoxide (CO) lying in this range. The power-law dust emission, F_\u03bd = 14 mJy(\u03bd/240 GHz)^(3.9) is consistent with the published continuum measurements. The CO J = 6 \u2192 5, J = 8 \u2192 7, and J = 9 \u2192 8 measurements are the first, and now provide the highest-J CO information in this source. Our measured CO intensities are very close to the previously published interferometric measurements of J = 7 \u2192 6, and we use all available transitions and our ^(13)CO upper limits to constrain the physical conditions in the Cloverleaf molecular gas disk. We find a large mass (2-50 \u00d7 10^9 M_\u2299) of highly excited gas with thermal pressure nT > 10^6 K cm^(\u20133). The ratio of the total CO cooling to the far-IR dust emission exceeds that in the local dusty galaxies, and we investigate the potential heating sources for this bulk of warm molecular gas. We conclude that both UV photons and X-rays likely contribute, and discuss implications for a top-heavy stellar initial mass function arising in the X-ray-irradiated starburst. Finally, we present tentative identifications of other species in the spectrum, including a possible detection of the H_2O 2_(0,2) \u2192 1_(1,1) transition at \u03bb_(rest) = 303 \u03bcm.",
"doi": "10.1088/0004-637X/705/1/112",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2009-11-01",
"series_number": "1",
"volume": "705",
"issue": "1",
"pages": "112-122"
},
{
"id": "authors:jfmk9-yg253",
"collection": "authors",
"collection_id": "jfmk9-yg253",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090928-115957244",
"type": "article",
"title": "A Bright Submillimeter Source in the Bullet Cluster (1E0657-56) Field Detected with Blast",
"author": [
{
"family_name": "Rex",
"given_name": "Marie",
"clpid": "Rex-M"
},
{
"family_name": "Ade",
"given_name": "Peter A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Aretxaga",
"given_name": "Itziar",
"orcid": "0000-0002-6590-3994",
"clpid": "Aretxaga-I"
},
{
"family_name": "Bock",
"given_name": "James J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Chapin",
"given_name": "Edward L.",
"clpid": "Chapin-E-L"
},
{
"family_name": "Devlin",
"given_name": "Mark J.",
"clpid": "Devlin-M-J"
},
{
"family_name": "Dicker",
"given_name": "Simon R.",
"clpid": "Dicker-S-R"
},
{
"family_name": "Griffin",
"given_name": "Matthew",
"clpid": "Griffin-M"
},
{
"family_name": "Gundersen",
"given_name": "Joshua O.",
"clpid": "Gundersen-J-O"
},
{
"family_name": "Halpern",
"given_name": "Mark",
"orcid": "0000-0002-1760-0868",
"clpid": "Halpern-M"
},
{
"family_name": "Hargrave",
"given_name": "Peter C.",
"orcid": "0000-0002-3109-6629",
"clpid": "Hargrave-P-C"
},
{
"family_name": "Hughes",
"given_name": "David H.",
"clpid": "Hughes-D-H"
},
{
"family_name": "Klein",
"given_name": "Jeff",
"clpid": "Klein-J"
},
{
"family_name": "Marsden",
"given_name": "Gaelen",
"clpid": "Marsden-Gaelen"
},
{
"family_name": "Martin",
"given_name": "Peter G.",
"orcid": "0000-0002-5236-3896",
"clpid": "Martin-P-G"
},
{
"family_name": "Mauskopf",
"given_name": "Philip",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "Monta\u00f1a",
"given_name": "Alfredo",
"orcid": "0000-0003-4229-381X",
"clpid": "Monta\u00f1a-A"
},
{
"family_name": "Nettefield",
"given_name": "Calvin B.",
"clpid": "Netterfield-C-B"
},
{
"family_name": "Olmi",
"given_name": "Luca",
"orcid": "0000-0002-1162-7947",
"clpid": "Olmi-L"
},
{
"family_name": "Pascale",
"given_name": "Enzo",
"orcid": "0000-0002-3242-8154",
"clpid": "Pascale-E"
},
{
"family_name": "Patanchon",
"given_name": "Guillaume",
"clpid": "Patanchon-G"
},
{
"family_name": "Scott",
"given_name": "Douglas",
"orcid": "0000-0002-6878-9840",
"clpid": "Scott-Douglas"
},
{
"family_name": "Semisch",
"given_name": "Christopher",
"clpid": "Semisch-C"
},
{
"family_name": "Thomas",
"given_name": "Nicholas E.",
"clpid": "Thomas-Nicholas-E"
},
{
"family_name": "Truch",
"given_name": "Matthew D. P",
"clpid": "Truch-M-D-P"
},
{
"family_name": "Tucker",
"given_name": "Carole",
"clpid": "Tucker-C-E"
},
{
"family_name": "Tucker",
"given_name": "Gregory S.",
"orcid": "0000-0002-6954-6947",
"clpid": "Tucker-G-S"
},
{
"family_name": "Viero",
"given_name": "Marco P.",
"clpid": "Viero-M-P"
},
{
"family_name": "Wiebe",
"given_name": "Donald V.",
"clpid": "Wiebe-D-V"
}
],
"abstract": "We present the 250, 350, and 500 \u03bcm detection of bright submillimeter emission in the direction of the Bullet Cluster measured by the Balloon-borne Large-Aperture Submillimeter Telescope (BLAST). The 500 \u03bcm centroid is coincident with an AzTEC 1.1 mm point-source detection at a position close to the peak lensing magnification produced by the cluster. However, the 250 \u03bcm and 350 \u03bcm centroids are elongated and shifted toward the south with a differential shift between bands that cannot be explained by pointing uncertainties. We therefore conclude that the BLAST detection is likely contaminated by emission from foreground galaxies associated with the Bullet Cluster. The submillimeter redshift estimate based on 250-1100 \u03bcm photometry at the position of the AzTEC source is z_(phot) = 2.9^(+0.6)_(\u20130.3), consistent with the infrared color redshift estimation of the most likely Infrared Array Camera counterpart. These flux densities indicate an apparent far-infrared (FIR) luminosity of L_(FIR) = 2 \u00d7 10^(13) L_\u2609 . When the amplification due to the gravitational lensing of the cluster is removed, the intrinsic FIR luminosity of the source is found to be L_(FIR) \u2264 10^(12) L_\u2609, consistent with typical luminous infrared galaxies.",
"doi": "10.1088/0004-637X/703/1/348",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2009-09-20",
"series_number": "1",
"volume": "703",
"issue": "1",
"pages": "348-353"
},
{
"id": "authors:x9txv-h8838",
"collection": "authors",
"collection_id": "x9txv-h8838",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090910-142750424",
"type": "article",
"title": "Subdegree Sunyaev-Zel'dovich Signal from Multifrequency BOOMERANG Observations",
"author": [
{
"family_name": "Veneziani",
"given_name": "M.",
"clpid": "Veneziani-M"
},
{
"family_name": "Amblard",
"given_name": "A.",
"clpid": "Amblard-A"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Piacentini",
"given_name": "F.",
"orcid": "0000-0002-5444-9327",
"clpid": "Piacentini-F"
},
{
"family_name": "Pietrobon",
"given_name": "D.",
"clpid": "Pietrobon-D"
},
{
"family_name": "Serra",
"given_name": "P.",
"clpid": "Serra-P"
},
{
"family_name": "Ade",
"given_name": "P. A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bond",
"given_name": "J. R.",
"orcid": "0000-0003-2358-9949",
"clpid": "Bond-J-R"
},
{
"family_name": "Borrill",
"given_name": "J.",
"clpid": "Borrill-J"
},
{
"family_name": "Boscaleri",
"given_name": "A.",
"clpid": "Boscaleri-A"
},
{
"family_name": "Cabella",
"given_name": "P.",
"clpid": "Cabella-P"
},
{
"family_name": "Contaldi",
"given_name": "C. R.",
"clpid": "Contaldi-C-R"
},
{
"family_name": "Crill",
"given_name": "B. P.",
"orcid": "0000-0002-4650-8518",
"clpid": "Crill-B-P"
},
{
"family_name": "de Bernardis",
"given_name": "P.",
"orcid": "0000-0001-6547-6446",
"clpid": "de-Bernardis-P"
},
{
"family_name": "De Gasperis",
"given_name": "G.",
"clpid": "De-Gasperis-G"
},
{
"family_name": "de Oliveira-Costa",
"given_name": "A.",
"clpid": "de-Oliveira-Costa-A"
},
{
"family_name": "De Troia",
"given_name": "G.",
"clpid": "De-Troia-G"
},
{
"family_name": "di Stefano",
"given_name": "G.",
"clpid": "di-Stefano-G"
},
{
"family_name": "Ganga",
"given_name": "K. M.",
"clpid": "Ganga-K-M"
},
{
"family_name": "Hivon",
"given_name": "E.",
"clpid": "Hivon-E"
},
{
"family_name": "Jones",
"given_name": "W. C.",
"clpid": "Jones-W-C"
},
{
"family_name": "Kisner",
"given_name": "T. S.",
"clpid": "Kisner-T-S"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "MacTavish",
"given_name": "C. J.",
"clpid": "MacTavish-C-J"
},
{
"family_name": "Masi",
"given_name": "S.",
"orcid": "0000-0001-5105-1439",
"clpid": "Masi-S"
},
{
"family_name": "Mauskopf",
"given_name": "P. D.",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "Melchiorri",
"given_name": "A.",
"clpid": "Melchiorri-A"
},
{
"family_name": "Montroy",
"given_name": "T. E.",
"clpid": "Montroy-T-E"
},
{
"family_name": "Natoli",
"given_name": "P.",
"clpid": "Natoli-P"
},
{
"family_name": "Netterfield",
"given_name": "C. B.",
"clpid": "Netterfield-C-B"
},
{
"family_name": "Pascale",
"given_name": "E.",
"orcid": "0000-0002-3242-8154",
"clpid": "Pascale-E"
},
{
"family_name": "Polenta",
"given_name": "G.",
"clpid": "Polenta-G"
},
{
"family_name": "Ricciardi",
"given_name": "S.",
"clpid": "Ricciardi-S"
},
{
"family_name": "Romeo",
"given_name": "G.",
"clpid": "Romeo-G"
},
{
"family_name": "Ruhl",
"given_name": "J. E.",
"clpid": "Ruhl-J-E"
},
{
"family_name": "Santini",
"given_name": "P.",
"clpid": "Santini-P"
},
{
"family_name": "Tegmark",
"given_name": "M.",
"clpid": "Tegmark-M"
},
{
"family_name": "Vittorio",
"given_name": "N.",
"clpid": "Vittorio-N"
}
],
"abstract": "The Sunyaev-Zel'dovich (SZ) effect is the inverse Compton-scattering of cosmic microwave background (CMB) photons by hot electrons in the intervening gas throughout the universe. The effect has a distinct spectral signature that allows its separation from other signals in multifrequency CMB data sets. Using CMB anisotropies measured at three frequencies by the BOOMERANG 2003 flight we constrain SZ fluctuations in the 10 arcmin to 1 deg angular range. Propagating errors and potential systematic effects through simulations, we obtain an overall upper limit of 15.3 \u03bcK (2\u03c3) for rms SZ fluctuations in a broad bin between multipoles of 250 and 1200 at the Rayleigh-Jeans (RJ) end of the spectrum. The resulting upper limit on the local universe normalization of the density perturbations with BOOMERANG SZ data alone is \u03c3^(SZ)_8 < 1.14 at the 95% confidence level. When combined with other CMB anisotropy and SZ measurements, we find \u03c3^(SZ)_8 < 0.92 (95% c.l.).",
"doi": "10.1088/0004-637X/702/1/L61",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2009-09-01",
"volume": "702",
"pages": "L61-L65"
},
{
"id": "authors:7t8sj-0bt04",
"collection": "authors",
"collection_id": "7t8sj-0bt04",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090825-104125123",
"type": "article",
"title": "Cosmological Parameters from the QUaD CMB Polarization Experiment",
"author": [
{
"family_name": "Castro",
"given_name": "P. G.",
"clpid": "Castro-P-G"
},
{
"family_name": "Ade",
"given_name": "P.",
"clpid": "Ade-P"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bowden",
"given_name": "M.",
"clpid": "Bowden-M"
},
{
"family_name": "Brown",
"given_name": "M. L.",
"clpid": "Brown-M-L"
},
{
"family_name": "Cahill",
"given_name": "G.",
"clpid": "Cahill-G"
},
{
"family_name": "Church",
"given_name": "S.",
"clpid": "Church-S"
},
{
"family_name": "Culverhouse",
"given_name": "T.",
"clpid": "Culverhouse-T"
},
{
"family_name": "Friedman",
"given_name": "R. B.",
"clpid": "Friedman-R-B"
},
{
"family_name": "Ganga",
"given_name": "K.",
"clpid": "Ganga-K"
},
{
"family_name": "Gear",
"given_name": "W. K.",
"clpid": "Gear-W-K"
},
{
"family_name": "Gupta",
"given_name": "S.",
"clpid": "Gupta-S"
},
{
"family_name": "Hinderks",
"given_name": "J.",
"clpid": "Hinderks-J"
},
{
"family_name": "Kovac",
"given_name": "J.",
"clpid": "Kovac-J"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Leitch",
"given_name": "E.",
"clpid": "Leitch-E"
},
{
"family_name": "Melhuish",
"given_name": "S. J.",
"clpid": "Melhuish-S-J"
},
{
"family_name": "Memari",
"given_name": "Y.",
"clpid": "Memari-Y"
},
{
"family_name": "Murphy",
"given_name": "J. A.",
"clpid": "Murphy-J-A"
},
{
"family_name": "Orlando",
"given_name": "A.",
"clpid": "Orlando-A"
},
{
"family_name": "Pryke",
"given_name": "C.",
"clpid": "Pryke-C"
},
{
"family_name": "Schwarz",
"given_name": "R.",
"clpid": "Schwarz-R"
},
{
"family_name": "O'Sullivan",
"given_name": "C.",
"clpid": "O'Sullivan-C"
},
{
"family_name": "Piccirillo",
"given_name": "L.",
"clpid": "Piccirillo-L"
},
{
"family_name": "Rajguru",
"given_name": "N.",
"clpid": "Rajguru-N"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Taylor",
"given_name": "A. N.",
"clpid": "Taylor-A-N"
},
{
"family_name": "Thompson",
"given_name": "K. L.",
"clpid": "Thompson-K-L"
},
{
"family_name": "Turner",
"given_name": "A. H.",
"clpid": "Turner-A-H"
},
{
"family_name": "Wu",
"given_name": "E. Y. S.",
"clpid": "Wu-E-Y-S"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
},
{
"literal": "The QUaD collaboration"
}
],
"abstract": "In this paper, we present a parameter estimation analysis of the polarization and temperature power spectra from the second and third season of observations with the QUaD experiment. QUaD has for the first time detected multiple acoustic peaks in the E-mode polarization spectrum with high significance. Although QUaD-only parameter constraints are not competitive with previous results for the standard six-parameter \u039bCDM cosmology, they do allow meaningful polarization-only parameter analyses for the first time. In a standard six-parameter \u039bCDM analysis, we find the QUaD TT power spectrum to be in good agreement with previous results. However, the QUaD polarization data show some tension with \u039bCDM. The origin of this 1\u03c3-2\u03c3 tension remains unclear, and may point to new physics, residual systematics, or simple random chance. We also combine QUaD with the five-year WMAP data set and the SDSS luminous red galaxies 4th data release power spectrum, and extend our analysis to constrain individual isocurvature mode fractions, constraining cold dark matter density, \u03b1_(cdmi) < 0.11 (95% confidence limit (CL)), neutrino density, \u03b1_(ndi) < 0.26 (95% CL), and neutrino velocity, \u03b1_(nvi) < 0.23 (95% CL), modes. Our analysis sets a benchmark for future polarization experiments.",
"doi": "10.1088/0004-637X/701/2/857",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2009-08-20",
"series_number": "2",
"volume": "701",
"issue": "2",
"pages": "857-864"
},
{
"id": "authors:a7kcf-fx758",
"collection": "authors",
"collection_id": "a7kcf-fx758",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090808-142505714",
"type": "article",
"title": "The Spitzer Deep, Wide-field Survey",
"author": [
{
"family_name": "Ashby",
"given_name": "M. L. N.",
"orcid": "0000-0002-3993-0745",
"clpid": "Ashby-M-L-N"
},
{
"family_name": "Stern",
"given_name": "D.",
"orcid": "0000-0003-2686-9241",
"clpid": "Stern-D"
},
{
"family_name": "Brodwin",
"given_name": "M.",
"orcid": "0000-0002-4208-798X",
"clpid": "Brodwin-M"
},
{
"family_name": "Griffith",
"given_name": "R.",
"clpid": "Griffith-R"
},
{
"family_name": "Eisenhardt",
"given_name": "P.",
"clpid": "Eisenhardt-P-R-M"
},
{
"family_name": "Kozlowski",
"given_name": "S.",
"clpid": "Kozlowski-S"
},
{
"family_name": "Kochanek",
"given_name": "C. S.",
"orcid": "0000-0001-6017-2961",
"clpid": "Kochanek-C-S"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Borys",
"given_name": "C.",
"clpid": "Borys-C-J-K"
},
{
"family_name": "Brand",
"given_name": "K.",
"clpid": "Brand-K"
},
{
"family_name": "Brown",
"given_name": "M. J. I.",
"orcid": "0000-0002-1207-9137",
"clpid": "Brown-M-J-I"
},
{
"family_name": "Cool",
"given_name": "R.",
"clpid": "Cool-R-J"
},
{
"family_name": "Cooray",
"given_name": "A.",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Croft",
"given_name": "S.",
"clpid": "Croft-S-K"
},
{
"family_name": "Dey",
"given_name": "A.",
"orcid": "0000-0002-4928-4003",
"clpid": "Dey-A"
},
{
"family_name": "Eisenstein",
"given_name": "D.",
"clpid": "Eisenstein-D-J"
},
{
"family_name": "Gonzalez",
"given_name": "A. H.",
"orcid": "0000-0002-0933-8601",
"clpid": "Gonzalez-A-H"
},
{
"family_name": "Gorjian",
"given_name": "V.",
"clpid": "Gorjian-V"
},
{
"family_name": "Grogin",
"given_name": "N. A.",
"clpid": "Grogin-N-A"
},
{
"family_name": "Ivison",
"given_name": "R. J.",
"orcid": "0000-0001-5118-1313",
"clpid": "Ivison-R-J"
},
{
"family_name": "Jacob",
"given_name": "J.",
"clpid": "Jacob-J-C"
},
{
"family_name": "Jannuzi",
"given_name": "B. T.",
"orcid": "0000-0002-1578-6582",
"clpid": "Jannuzi-B-T"
},
{
"family_name": "Mainzer",
"given_name": "A.",
"clpid": "Mainzer-A-K"
},
{
"family_name": "Moustakas",
"given_name": "L. A.",
"orcid": "0000-0003-3030-2360",
"clpid": "Moustakas-L-A"
},
{
"family_name": "R\u00f6ttgering",
"given_name": "H. J. A.",
"clpid": "R\u00f6ttgering-H-J-A"
},
{
"family_name": "Seymour",
"given_name": "N.",
"orcid": "0000-0003-3506-5536",
"clpid": "Seymour-N"
},
{
"family_name": "Smith",
"given_name": "H. A.",
"clpid": "Smith-H-A"
},
{
"family_name": "Stanford",
"given_name": "S. A.",
"clpid": "Stanford-S-A"
},
{
"family_name": "Stauffer",
"given_name": "J. R.",
"orcid": "0000-0003-3595-7382",
"clpid": "Stauffer-J-R"
},
{
"family_name": "Sullivan",
"given_name": "I.",
"orcid": "0000-0003-0632-4607",
"clpid": "Sullivan-Ian"
},
{
"family_name": "van Breugel",
"given_name": "W.",
"clpid": "van-Breugel-W"
},
{
"family_name": "Willner",
"given_name": "S. P.",
"orcid": "0000-0002-9895-5758",
"clpid": "Willner-S-P"
},
{
"family_name": "Wright",
"given_name": "E. L.",
"orcid": "0000-0001-5058-1593",
"clpid": "Wright-E-L"
}
],
"abstract": "The Spitzer Deep, Wide-Field Survey (SDWFS) is a four-epoch infrared survey of 10 deg^(2) in the Bootes field of the NOAO Deep Wide-Field Survey using the IRAC instrument on the Spitzer Space Telescope. SDWFS, a Spitzer Cycle 4 Legacy project, occupies a unique position in the area-depth survey space defined by other Spitzer surveys. The four epochs that make up SDWFS permit-for the first time-the selection of infrared-variable and high proper motion objects over a wide field on timescales of years. Because of its large survey volume, SDWFS is sensitive to galaxies out to z ~ 3 with relatively little impact from cosmic variance for all but the richest systems. The SDWFS data sets will thus be especially useful for characterizing galaxy evolution beyond z ~ 1.5. This paper explains the SDWFS observing strategy and data processing, presents the SDWFS mosaics and source catalogs, and discusses some early scientific findings. The publicly released, full-depth catalogs contain 6.78, 5.23, 1.20, and 0.96 x 10^(5) distinct sources detected to the average 5 sigma, 4\"-diameter, aperture-corrected limits of 19.77, 18.83, 16.50, and 15.82 Vega mag at 3.6, 4.5, 5.8, and 8.0 mu m, respectively. The SDWFS number counts and color-color distribution are consistent with other, earlier Spitzer surveys. At the 6 minute integration time of the SDWFS IRAC imaging, > 50% of isolated Faint Images of the Radio Sky at Twenty cm radio sources and > 80% of on-axis XBootes sources are detected out to 8.0 mu m. Finally, we present the four highest proper motion IRAC-selected sources identified from the multi-epoch imaging, two of which are likely field brown dwarfs of mid-T spectral class.",
"doi": "10.1088/0004-637X/701/1/428",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2009-08-10",
"series_number": "1",
"volume": "701",
"issue": "1",
"pages": "428-453"
},
{
"id": "authors:89192-3ag63",
"collection": "authors",
"collection_id": "89192-3ag63",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090819-153500287",
"type": "article",
"title": "Small Angular Scale Measurements of the Cosmic Microwave Background Temperature Power Spectrum From QUaD",
"author": [
{
"family_name": "Friedman",
"given_name": "R. B.",
"clpid": "Friedman-R-B"
},
{
"family_name": "Ade",
"given_name": "P.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bowden",
"given_name": "M.",
"clpid": "Bowden-M"
},
{
"family_name": "Brown",
"given_name": "M. L.",
"clpid": "Brown-M-L"
},
{
"family_name": "Cahill",
"given_name": "G.",
"clpid": "Cahill-G"
},
{
"family_name": "Castro",
"given_name": "P. G.",
"clpid": "Castro-P-G"
},
{
"family_name": "Church",
"given_name": "S.",
"clpid": "Church-S"
},
{
"family_name": "Culverhouse",
"given_name": "T.",
"clpid": "Culverhouse-T"
},
{
"family_name": "Ganga",
"given_name": "K.",
"clpid": "Ganga-K"
},
{
"family_name": "Gear",
"given_name": "W. K.",
"clpid": "Gear-W-K"
},
{
"family_name": "Gupta",
"given_name": "S.",
"clpid": "Gupta-S"
},
{
"family_name": "Hinderks",
"given_name": "J.",
"clpid": "Hinderks-J"
},
{
"family_name": "Kovac",
"given_name": "J.",
"clpid": "Kovac-J"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Leitch",
"given_name": "E.",
"clpid": "Leitch-E"
},
{
"family_name": "Melhuish",
"given_name": "S. J.",
"clpid": "Melhuish-S-J"
},
{
"family_name": "Memari",
"given_name": "Y.",
"clpid": "Memari-Y"
},
{
"family_name": "Murphy",
"given_name": "J. A.",
"clpid": "Murphy-J-A"
},
{
"family_name": "Orlando",
"given_name": "A.",
"clpid": "Orlando-A"
},
{
"family_name": "O'Sullivan",
"given_name": "C.",
"clpid": "O'Sullivan-C"
},
{
"family_name": "Piccirillo",
"given_name": "L.",
"clpid": "Piccirillo-L"
},
{
"family_name": "Pryke",
"given_name": "C.",
"clpid": "Pryke-C"
},
{
"family_name": "Rajguru",
"given_name": "N.",
"clpid": "Rajguru-N"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Schwarz",
"given_name": "R.",
"clpid": "Schwarz-R"
},
{
"family_name": "Taylor",
"given_name": "A. N.",
"clpid": "Taylor-A-N"
},
{
"family_name": "Thompson",
"given_name": "K. L.",
"clpid": "Thompson-K-L"
},
{
"family_name": "Turner",
"given_name": "A. H.",
"clpid": "Turner-A-H"
},
{
"family_name": "Wu",
"given_name": "E. Y. S.",
"clpid": "Wu-E-Y-S"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We present measurements of the cosmic microwave background (CMB) radiation temperature anisotropy in the multipole range 2000 < \u2113 < 3000 from the QUaD telescope's second and third observing seasons. After masking the brightest point sources our results are consistent with the primary \u039bCDM expectation alone. We estimate the contribution of residual (un-masked) radio point sources using a model calibrated to our own bright source observations, and a full simulation of the source finding and masking procedure. Including this contribution slightly improves the \u03c7^2. We also fit a standard Sunyaev-Zel'dovich (SZ) template to the bandpowers and see no strong evidence of an SZ contribution, which is as expected for \u03c3_8 \u2248 0.8.",
"doi": "10.1088/0004-637X/700/2/L187",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2009-08-01",
"series_number": "2",
"volume": "700",
"issue": "2",
"pages": "L187-L191"
},
{
"id": "authors:zyed2-2t624",
"collection": "authors",
"collection_id": "zyed2-2t624",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090831-110123089",
"type": "article",
"title": "High-Resolution CMB Power Spectrum from the Complete ACBAR Data Set",
"author": [
{
"family_name": "Reichardt",
"given_name": "C. L.",
"clpid": "Reichardt-C-L"
},
{
"family_name": "Ade",
"given_name": "P. A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bond",
"given_name": "J. R.",
"orcid": "0000-0003-2358-9949",
"clpid": "Bond-J-R"
},
{
"family_name": "Brevik",
"given_name": "J. A.",
"clpid": "Brevik-J-A"
},
{
"family_name": "Contaldi",
"given_name": "C. R.",
"clpid": "Contaldi-C-R"
},
{
"family_name": "Daub",
"given_name": "M. D.",
"clpid": "Daub-M-D"
},
{
"family_name": "Dempsey",
"given_name": "J. T.",
"clpid": "Dempsey-J-T"
},
{
"family_name": "Goldstein",
"given_name": "J. H.",
"clpid": "Goldstein-J-H"
},
{
"family_name": "Holzapfel",
"given_name": "W. L.",
"clpid": "Holzapfel-W-L"
},
{
"family_name": "Kuo",
"given_name": "C. L.",
"clpid": "Kuo-Chia-Lam"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Lueker",
"given_name": "M.",
"clpid": "Lueker-M"
},
{
"family_name": "Newcomb",
"given_name": "M.",
"clpid": "Newcomb-M"
},
{
"family_name": "Peterson",
"given_name": "J. B.",
"clpid": "Peterson-J-B"
},
{
"family_name": "Ruhl",
"given_name": "J. E.",
"clpid": "Ruhl-J-E"
},
{
"family_name": "Runyan",
"given_name": "M. C.",
"clpid": "Runyan-M-C"
},
{
"family_name": "Staniszewski",
"given_name": "Z.",
"clpid": "Staniszewski-Z"
}
],
"abstract": "In this paper, we present results from the complete set of cosmic microwave background (CMB) radiation temperature anisotropy observations made with the Arcminute Cosmology Bolometer Array Receiver (ACBAR) operating at 150 GHz. We include new data from the final 2005 observing season, expanding the number of detector hours by 210% and the sky coverage by 490% over that used for the previous ACBAR release. As a result, the band-power uncertainties have been reduced by more than a factor of two on angular scales encompassing the third to fifth acoustic peaks as well as the damping tail of the CMB power spectrum. The calibration uncertainty has been reduced from 6% to 2.1% in temperature through a direct comparison of the CMB anisotropy measured by ACBAR with that of the dipole-calibrated WMAP5 experiment. The measured power spectrum is consistent with a spatially flat, \u039bCDM cosmological model. We include the effects of weak lensing in the power spectrum model computations and find that this significantly improves the fits of the models to the combined ACBAR+WMAP5 power spectrum. The preferred strength of the lensing is consistent with theoretical expectations. On fine angular scales, there is weak evidence (1.1\u03c3) for excess power above the level expected from primary anisotropies. We expect any excess power to be dominated by the combination of emission from dusty protogalaxies and the Sunyaev-Zel'dovich effect (SZE). However, the excess observed by ACBAR is significantly smaller than the excess power at \u2113 > 2000 reported by the CBI experiment operating at 30 GHz. Therefore, while it is unlikely that the CBI excess has a primordial origin; the combined ACBAR and CBI results are consistent with the source of the CBI excess being either the SZE or radio source contamination.",
"doi": "10.1088/0004-637X/694/2/1200",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2009-04-01",
"series_number": "2",
"volume": "694",
"issue": "2",
"pages": "1200-1219"
},
{
"id": "authors:scehr-qvk60",
"collection": "authors",
"collection_id": "scehr-qvk60",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090831-141710879",
"type": "article",
"title": "QUaD: A High-Resolution Cosmic Microwave Background Polarimeter",
"author": [
{
"family_name": "Hinderks",
"given_name": "J. R.",
"clpid": "Hinderks-J-R"
},
{
"family_name": "Ade",
"given_name": "P.",
"clpid": "Ade-P"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bowden",
"given_name": "M.",
"clpid": "Bowden-M"
},
{
"family_name": "Brown",
"given_name": "M. L.",
"clpid": "Brown-M-L"
},
{
"family_name": "Cahill",
"given_name": "G.",
"clpid": "Cahill-G"
},
{
"family_name": "Carlstrom",
"given_name": "J. E.",
"orcid": "0000-0002-2044-7665",
"clpid": "Carlstrom-J-E"
},
{
"family_name": "Castro",
"given_name": "P. G.",
"clpid": "Castro-P-G"
},
{
"family_name": "Church",
"given_name": "S.",
"clpid": "Church-S"
},
{
"family_name": "Culverhouse",
"given_name": "T.",
"clpid": "Culverhouse-T"
},
{
"family_name": "Friedman",
"given_name": "R.",
"clpid": "Friedman-R"
},
{
"family_name": "Ganga",
"given_name": "K.",
"clpid": "Ganga-K"
},
{
"family_name": "Gear",
"given_name": "W. K.",
"clpid": "Gear-W-K"
},
{
"family_name": "Gupta",
"given_name": "S.",
"clpid": "Gupta-S"
},
{
"family_name": "Harris",
"given_name": "J.",
"clpid": "Harris-J"
},
{
"family_name": "Haynes",
"given_name": "V.",
"clpid": "Haynes-V"
},
{
"family_name": "Keating",
"given_name": "B. G.",
"clpid": "Keating-B-G"
},
{
"family_name": "Kovac",
"given_name": "J.",
"clpid": "Kovac-J"
},
{
"family_name": "Kirby",
"given_name": "E.",
"orcid": "0000-0001-6196-5162",
"clpid": "Kirby-E-N"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Leitch",
"given_name": "E.",
"clpid": "Leitch-E"
},
{
"family_name": "Mallie",
"given_name": "O. E.",
"clpid": "Mallie-O-E"
},
{
"family_name": "Melhuish",
"given_name": "S.",
"clpid": "Melhuish-S"
},
{
"family_name": "Memari",
"given_name": "Y.",
"clpid": "Memari-Y"
},
{
"family_name": "Murphy",
"given_name": "A.",
"clpid": "Murphy-A"
},
{
"family_name": "Orlando",
"given_name": "A.",
"clpid": "Orlando-A"
},
{
"family_name": "Schwarz",
"given_name": "R.",
"clpid": "Schwarz-R"
},
{
"family_name": "O'Sullivan",
"given_name": "C.",
"clpid": "O'Sullivan-C"
},
{
"family_name": "Piccirillo",
"given_name": "L.",
"clpid": "Piccirillo-L"
},
{
"family_name": "Pryke",
"given_name": "C.",
"clpid": "Pryke-C"
},
{
"family_name": "Rajguru",
"given_name": "N.",
"clpid": "Rajguru-N"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Taylor",
"given_name": "A. N.",
"clpid": "Taylor-A-N"
},
{
"family_name": "Thompson",
"given_name": "K. L.",
"clpid": "Thompson-K-L"
},
{
"family_name": "Tucker",
"given_name": "C.",
"clpid": "Tucker-C"
},
{
"family_name": "Turner",
"given_name": "A. H.",
"clpid": "Turner-A-H"
},
{
"family_name": "Wu",
"given_name": "E. Y. S.",
"clpid": "Wu-E-Y-S"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "We describe the QUaD experiment, a millimeter-wavelength polarimeter designed to observe the cosmic microwave background (CMB) from a site at the South Pole. The experiment comprises a 2.64 m Cassegrain telescope equipped with a cryogenically cooled receiver containing an array of 62 polarization-sensitive bolometers. The focal plane contains pixels at two different frequency bands, 100 GHz and 150 GHz, with angular resolutions of 5' and 35, respectively. The high angular resolution allows observation of CMB temperature and polarization anisotropies over a wide range of scales. The instrument commenced operation in early 2005 and collected science data during three successive Austral winter seasons of observation.",
"doi": "10.1088/0004-637X/692/2/1221",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2009-02-24",
"series_number": "2",
"volume": "692",
"issue": "2",
"pages": "1221-1246"
},
{
"id": "authors:zynqx-y1196",
"collection": "authors",
"collection_id": "zynqx-y1196",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090924-141617154",
"type": "article",
"title": "Second and Third Season QUaD Cosmic Microwave Background Temperature and Polarization Power Spectra",
"author": [
{
"family_name": "Pryke",
"given_name": "C.",
"clpid": "Pryke-C"
},
{
"family_name": "Ade",
"given_name": "P.",
"clpid": "Ade-P"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bowden",
"given_name": "M.",
"clpid": "Bowden-M"
},
{
"family_name": "Brown",
"given_name": "M. L.",
"clpid": "Brown-M-L"
},
{
"family_name": "Cahill",
"given_name": "G.",
"clpid": "Cahill-G"
},
{
"family_name": "Castro",
"given_name": "P. G.",
"clpid": "Castro-P-G"
},
{
"family_name": "Church",
"given_name": "S.",
"clpid": "Church-S"
},
{
"family_name": "Culverhouse",
"given_name": "T.",
"clpid": "Culverhouse-T"
},
{
"family_name": "Friedman",
"given_name": "R.",
"clpid": "Friedman-R"
},
{
"family_name": "Ganga",
"given_name": "K.",
"clpid": "Ganga-K"
},
{
"family_name": "Gear",
"given_name": "W. K.",
"clpid": "Gear-W-K"
},
{
"family_name": "Gupta",
"given_name": "S.",
"clpid": "Gupta-S"
},
{
"family_name": "Hinderks",
"given_name": "J.",
"clpid": "Hinderks-J"
},
{
"family_name": "Kovac",
"given_name": "J.",
"clpid": "Kovac-J"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Leitch",
"given_name": "E.",
"clpid": "Leitch-E"
},
{
"family_name": "Melhuish",
"given_name": "S. J.",
"clpid": "Melhuish-S-J"
},
{
"family_name": "Memari",
"given_name": "Y.",
"clpid": "Memari-Y"
},
{
"family_name": "Murphy",
"given_name": "J. A.",
"clpid": "Murphy-J-A"
},
{
"family_name": "Orlando",
"given_name": "A.",
"clpid": "Orlando-A"
},
{
"family_name": "Schwarz",
"given_name": "R.",
"clpid": "Schwarz-R"
},
{
"family_name": "\u00d3 Sullivan",
"given_name": "C.",
"clpid": "\u00d3-Sullivan-C"
},
{
"family_name": "Piccirillo",
"given_name": "L.",
"clpid": "Piccirillo-L"
},
{
"family_name": "Rajguru",
"given_name": "N.",
"clpid": "Rajguru-N"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Taylor",
"given_name": "A. N.",
"clpid": "Taylor-A-N"
},
{
"family_name": "Thompson",
"given_name": "K. L.",
"clpid": "Thompson-K-L"
},
{
"family_name": "Turner",
"given_name": "A. H.",
"clpid": "Turner-A-H"
},
{
"family_name": "Wu",
"given_name": "E. Y. S.",
"clpid": "Wu-E-Y-S"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
},
{
"literal": "QUaD Collaboration"
}
],
"abstract": "We report results from the second and third seasons of observation with the QUaD experiment. Angular power spectra of the cosmic microwave background are derived for both temperature and polarization at both 100 GHz and 150 GHz, and as cross-frequency spectra. All spectra are subjected to an extensive set of jackknife tests to probe for possible systematic contamination. For the implemented data cuts and processing technique such contamination is undetectable. We analyze the difference map formed between the 100 and 150 GHz bands and find no evidence of foreground contamination in polarization. The spectra are then combined to form a single set of results which are shown to be consistent with the prevailing LCDM model. The sensitivity of the polarization results is considerably better than that of any previous experiment\u2014for the first time multiple acoustic peaks are detected in the E-mode power spectrum at high significance.",
"doi": "10.1088/0004-637X/692/2/1247",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2009-02-20",
"series_number": "2",
"volume": "692",
"issue": "2",
"pages": "1247-1270"
},
{
"id": "authors:9y6zr-qw224",
"collection": "authors",
"collection_id": "9y6zr-qw224",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:SAYapj09",
"type": "article",
"title": "A Search for Cosmic Microwave Background Anisotropies on Arcminute Scales with Bolocam",
"author": [
{
"family_name": "Sayers",
"given_name": "J.",
"orcid": "0000-0002-8213-3784",
"clpid": "Sayers-Jack"
},
{
"family_name": "Golwala",
"given_name": "S. R.",
"orcid": "0000-0002-1098-7174",
"clpid": "Golwala-S-R"
},
{
"family_name": "Rossinot",
"given_name": "P.",
"clpid": "Rossinot-P"
},
{
"family_name": "Ade",
"given_name": "P. A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Aguirre",
"given_name": "J. E.",
"orcid": "0000-0002-4810-666X",
"clpid": "Aguirre-J-E"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Edgington",
"given_name": "S. F.",
"clpid": "Edgington-S-F"
},
{
"family_name": "Glenn",
"given_name": "J.",
"orcid": "0000-0001-7527-2017",
"clpid": "Glenn-J"
},
{
"family_name": "Goldin",
"given_name": "A.",
"clpid": "Goldin-A-L"
},
{
"family_name": "Haig",
"given_name": "D.",
"clpid": "Haig-D"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Laurent",
"given_name": "G. T.",
"clpid": "Laurent-G-T"
},
{
"family_name": "Mauskopf",
"given_name": "P. D.",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "Nguyen",
"given_name": "H. T.",
"clpid": "Nguyen-Hien-Trong"
}
],
"abstract": "We have surveyed two science fields totaling 1 deg2 with Bolocam at 2.1 mm to search for secondary Cosmic Microwave Background (CMB) anisotropies caused by the Sunyaev-Zel'dovich effect (SZE). The fields are in the Lynx and Subaru/XMM SDS1 fields. Our survey is sensitive to angular scales with an effective angular multipole of \u2113eff = 5700 with FWHM\u2113 = 2800 and has an angular resolution of 60 arcsec FWHM. Our data provide no evidence for anisotropy. We are able to constrain the level of total astronomical anisotropy, modeled as a flat-band power in C_\u2113, with most frequent 68%, 90%, and 95% CL upper limits of 590, 760, and 830 μK2CMB. We statistically subtract the known contribution from primary CMB anisotropy, including cosmic variance, to obtain constraints on the SZE anisotropy contribution. Now including flux calibration uncertainty, our most frequent 68%, 90%, and 95% CL upper limits on a flat-band power in C_\u2113 are 690, 960, and 1000 μK2CMB. When we instead employ the analytical spectrum suggested by Komatsu and Seljack in 2002, and account for the non-Gaussianity of the SZE anisotropy signal, we obtain upper limits on the average amplitude of their spectrum weighted by our transfer function of 790, 1060, and 1080 μK2CMB. We obtain a 90% CL upper limit on σ8, which normalizes the power spectrum of density fluctuations, of 1.57. These are the first constraints on anisotropy and σ8 from survey data at these angular scales at frequencies near 150 GHz.
",
"doi": "10.1088/0004-637X/690/2/1597",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2009-01-10",
"series_number": "2",
"volume": "690",
"issue": "2",
"pages": "1597-1620"
},
{
"id": "authors:xx8ca-ywd87",
"collection": "authors",
"collection_id": "xx8ca-ywd87",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090524-204222732",
"type": "article",
"title": "Spider optimization: probing the systematics of a large-scale B-mode experiment",
"author": [
{
"family_name": "MacTavish",
"given_name": "C. J.",
"clpid": "MacTavish-C-J"
},
{
"family_name": "Ade",
"given_name": "P. A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Battistelli",
"given_name": "E. S.",
"orcid": "0000-0001-5210-7625",
"clpid": "Battistelli-E-S"
},
{
"family_name": "Benton",
"given_name": "S.",
"clpid": "Benton-S"
},
{
"family_name": "Bihary",
"given_name": "R.",
"clpid": "Bihary-R"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bond",
"given_name": "J. R.",
"orcid": "0000-0003-2358-9949",
"clpid": "Bond-J-R"
},
{
"family_name": "Brevik",
"given_name": "J.",
"clpid": "Brevik-J"
},
{
"family_name": "Bryan",
"given_name": "S.",
"clpid": "Bryan-S"
},
{
"family_name": "Contaldi",
"given_name": "C. R.",
"clpid": "Contaldi-C-R"
},
{
"family_name": "Crill",
"given_name": "B. P.",
"orcid": "0000-0002-4650-8518",
"clpid": "Crill-B-P"
},
{
"family_name": "Dor\u00e9",
"given_name": "O.",
"orcid": "0000-0001-7432-2932",
"clpid": "Dor\u00e9-O"
},
{
"family_name": "Fissel",
"given_name": "L.",
"orcid": "0000-0002-3242-8154",
"clpid": "Fissel-Laura-M"
},
{
"family_name": "Golwala",
"given_name": "S. R.",
"orcid": "0000-0002-1098-7174",
"clpid": "Golwala-S-R"
},
{
"family_name": "Halpern",
"given_name": "M.",
"orcid": "0000-0002-1760-0868",
"clpid": "Halpern-M"
},
{
"family_name": "Hilton",
"given_name": "G.",
"clpid": "Hilton-G"
},
{
"family_name": "Holmes",
"given_name": "W.",
"clpid": "Holmes-W"
},
{
"family_name": "Hristov",
"given_name": "V. V.",
"clpid": "Hristov-V-V"
},
{
"family_name": "Irwin",
"given_name": "K.",
"clpid": "Irwin-K"
},
{
"family_name": "Jones",
"given_name": "W. C.",
"clpid": "Jones-W-C"
},
{
"family_name": "Kuo",
"given_name": "C. L.",
"clpid": "Kuo-Chia-Lam"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Lawrie",
"given_name": "C.",
"clpid": "Lawrie-C"
},
{
"family_name": "Martin",
"given_name": "T. G.",
"clpid": "Martin-T-G"
},
{
"family_name": "Mason",
"given_name": "P.",
"clpid": "Mason-P"
},
{
"family_name": "Montroy",
"given_name": "T. E.",
"clpid": "Montroy-T-E"
},
{
"family_name": "Netterfield",
"given_name": "C. B.",
"clpid": "Netterfield-C-B"
},
{
"family_name": "Riley",
"given_name": "D.",
"clpid": "Riley-D"
},
{
"family_name": "Ruhl",
"given_name": "J. E.",
"clpid": "Ruhl-J-E"
},
{
"family_name": "Runyan",
"given_name": "M.",
"clpid": "Runyan-M"
},
{
"family_name": "Trangsrud",
"given_name": "A.",
"clpid": "Trangsrud-Amy-R"
},
{
"family_name": "Tucker",
"given_name": "C.",
"clpid": "Tucker-C"
},
{
"family_name": "Turner",
"given_name": "A.",
"clpid": "Turner-A"
},
{
"family_name": "Viero",
"given_name": "M.",
"clpid": "Viero-M-P"
},
{
"family_name": "Wiebe",
"given_name": "D.",
"clpid": "Wiebe-D"
}
],
"abstract": "Spider is a long-duration, balloon-borne polarimeter designed to measure large-scale cosmic microwave background (CMB) polarization with very high sensitivity and control of systematics. The instrument will map over half the sky with degree angular resolution in the I, Q, and U Stokes parameters in four frequency bands from 96 to 275 GHz. Spider's ultimate goal is to detect the primordial gravity-wave signal imprinted on the CMB B-mode polarization. One of the challenges in achieving this goal is the minimization of the contamination of B-modes by systematic effects. This paper explores a number of instrument systematics and observing strategies in order to optimize B-mode sensitivity. This is done by injecting realistic-amplitude, time-varying systematics into a set of simulated time streams. Tests of the impact of detector noise characteristics, pointing jitter, payload pendulations, polarization angle offsets, beam systematics, and receiver gain drifts are shown. Spider's default observing strategy is to spin continuously in azimuth, with polarization modulation achieved by either a rapidly spinning half-wave plate or a rapidly spinning gondola and a slowly stepped half-wave plate. Although the latter is more susceptible to systematics, the results shown here indicate that either mode of operation can be used by Spider.",
"doi": "10.1086/592732",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2008-12-20",
"series_number": "2",
"volume": "689",
"issue": "2",
"pages": "655-665"
},
{
"id": "authors:6z9x1-c3692",
"collection": "authors",
"collection_id": "6z9x1-c3692",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200130-074148107",
"type": "article",
"title": "An AzTEC 1.1 mm survey of the GOODS-N field \u2013 I. Maps, catalogue and source statistics",
"author": [
{
"family_name": "Perera",
"given_name": "T. A.",
"clpid": "Perera-T-A"
},
{
"family_name": "Chapin",
"given_name": "E. L.",
"clpid": "Chapin-E-L"
},
{
"family_name": "Austermann",
"given_name": "J. E.",
"clpid": "Austermann-J-E"
},
{
"family_name": "Scott",
"given_name": "K. S.",
"clpid": "Scott-K-S"
},
{
"family_name": "Wilson",
"given_name": "G. W.",
"clpid": "Wilson-G-W"
},
{
"family_name": "Halpern",
"given_name": "M.",
"orcid": "0000-0002-1760-0868",
"clpid": "Halpern-M"
},
{
"family_name": "Pope",
"given_name": "A.",
"orcid": "0000-0001-8592-2706",
"clpid": "Pope-Alexandra"
},
{
"family_name": "Scott",
"given_name": "D.",
"orcid": "0000-0002-6878-9840",
"clpid": "Scott-Douglas"
},
{
"family_name": "Yun",
"given_name": "M. S.",
"orcid": "0000-0001-7095-7543",
"clpid": "Yun-Min-S"
},
{
"family_name": "Lowenthal",
"given_name": "J. D.",
"clpid": "Lowenthal-J-D"
},
{
"family_name": "Morrison",
"given_name": "G.",
"clpid": "Morrison-G-E"
},
{
"family_name": "Aretxaga",
"given_name": "I.",
"orcid": "0000-0002-6590-3994",
"clpid": "Aretxaga-I"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Coppin",
"given_name": "K.",
"clpid": "Coppin-K-E-K"
},
{
"family_name": "Crowe",
"given_name": "M.",
"clpid": "Crowe-M"
},
{
"family_name": "Frey",
"given_name": "L.",
"clpid": "Frey-L"
},
{
"family_name": "Hughes",
"given_name": "D. H.",
"clpid": "Hughes-D-H"
},
{
"family_name": "Kang",
"given_name": "Y.",
"clpid": "Kang-Y"
},
{
"family_name": "Kim",
"given_name": "S.",
"clpid": "Kim-S"
},
{
"family_name": "Mauskopf",
"given_name": "P. D.",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
}
],
"abstract": "We have conducted a deep and uniform 1.1 mm survey of the Great Observatories Origins Deep Survey-North (GOODS-N) field with AzTEC on the James Clerk Maxwell Telescope. Here, we present the first results from this survey including maps, the source catalogue and 1.1 mm number counts. The results presented here were obtained from a 245 arcmin\u00b2 region with a near uniform coverage to a depth of 0.96\u20131.16 mJy beam\u207b\u00b9. Our robust catalogue contains 28 source candidates detected with S/N \u2265 3.75, only \u223c1\u2013 2 of which are expected to be spurious detections. Of these source candidates, eight are also detected by Submillimetre Common-User Bolometer Array (SCUBA) at 850 \u03bcm in regions where there is a good overlap between the two surveys. The major advantage of our survey over that with SCUBA is the uniformity of coverage. We calculate number counts using two different techniques: the first using a frequentist parameter estimation and the second using a Bayesian method. The two sets of results are in good agreement. We find that the 1.1 mm differential number counts are well described in the 2\u20136 mJy range by the functional form dN/dS=N\u2032(S\u2032/S) exp(\u2212S/S\u2032) with fitted parameters S\u2032= 1.25 \u00b1 0.38 mJy and dN/dS= 300 \u00b1 90 mJy\u207b\u00b9deg\u207b\u00b2 at 3 mJy.",
"doi": "10.1111/j.1365-2966.2008.13902.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2008-12",
"series_number": "3",
"volume": "391",
"issue": "3",
"pages": "1227-1238"
},
{
"id": "authors:r6fmg-dwf28",
"collection": "authors",
"collection_id": "r6fmg-dwf28",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:HOLao08",
"type": "article",
"title": "Initial test results on bolometers for the Planck high frequency instrument",
"author": [
{
"family_name": "Holmes",
"given_name": "Warren A.",
"clpid": "Holmes-W-A"
},
{
"family_name": "Bock",
"given_name": "James J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Crill",
"given_name": "Brendan P.",
"orcid": "0000-0002-4650-8518",
"clpid": "Crill-B-P"
},
{
"family_name": "Koch",
"given_name": "Timothy C.",
"clpid": "Koch-T-C"
},
{
"family_name": "Jones",
"given_name": "William C.",
"clpid": "Jones-W-C"
},
{
"family_name": "Lange",
"given_name": "Andrew E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Paine",
"given_name": "Christopher G.",
"clpid": "Paine-C-G"
}
],
"abstract": "We summarize the fabrication, flight qualification, and dark performance of bolometers completed at the Jet Propulsion Laboratory for the High Frequency Instrument (HFI) of the joint ESA/NASA Herschel/Planck mission to be launched in 2009. The HFI is a multicolor focal plane which consists of 52 bolometers operated at 100 mK. Each bolometer is mounted to a feedhorn-filter assembly which defines one of six frequency bands centered between 100-857 GHz. Four detectors in each of five bands from 143-857 GHz are coupled to both linear polarizations and thus measure the total intensity. In addition, eight detectors in each of four bands (100, 143, 217, and 353 GHz) couple only to a single linear polarization and thus provide measurements of the Stokes parameters, Q and U, as well as the total intensity. The measured noise equivalent power (NEP) of all detectors is at or below the background limit for the telescope and time constants are a few ms, short enough to resolve point sources as the 5 to 9 arc min beams move across the sky at 1 rpm.",
"doi": "10.1364/AO.47.005996",
"issn": "0003-6935",
"publisher": "Optical Society of America",
"publication": "Applied Optics",
"publication_date": "2008-11-10",
"series_number": "32",
"volume": "47",
"issue": "32",
"pages": "5996-6008"
},
{
"id": "authors:ezapb-gvz38",
"collection": "authors",
"collection_id": "ezapb-gvz38",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090514-172906404",
"type": "article",
"title": "The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) 2005: calibration and targeted sources",
"author": [
{
"family_name": "Truch",
"given_name": "M. D. P.",
"clpid": "Truch-M-D-P"
},
{
"family_name": "Ade",
"given_name": "P. A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Chapin",
"given_name": "E. L.",
"clpid": "Chapin-E-L"
},
{
"family_name": "Devlin",
"given_name": "M. J.",
"clpid": "Devlin-M-J"
},
{
"family_name": "Dicker",
"given_name": "S.",
"clpid": "Dicker-S-R"
},
{
"family_name": "Griffin",
"given_name": "M.",
"clpid": "Griffin-M"
},
{
"family_name": "Gundersen",
"given_name": "J. O.",
"clpid": "Gundersen-J-O"
},
{
"family_name": "Halpern",
"given_name": "M.",
"orcid": "0000-0002-1760-0868",
"clpid": "Halpern-M"
},
{
"family_name": "Hargrave",
"given_name": "P. C.",
"orcid": "0000-0002-3109-6629",
"clpid": "Hargrave-P-C"
},
{
"family_name": "Hughes",
"given_name": "D. H.",
"clpid": "Hughes-D-H"
},
{
"family_name": "Klein",
"given_name": "J.",
"clpid": "Klein-J"
},
{
"family_name": "Marsden",
"given_name": "G.",
"clpid": "Marsden-Gaelen"
},
{
"family_name": "Martin",
"given_name": "P. G.",
"orcid": "0000-0002-5236-3896",
"clpid": "Martin-P-G"
},
{
"family_name": "Mauskopf",
"given_name": "P.",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "Netterfield",
"given_name": "C. B.",
"clpid": "Netterfield-C-B"
},
{
"family_name": "Olmi",
"given_name": "L.",
"orcid": "0000-0002-1162-7947",
"clpid": "Olmi-L"
},
{
"family_name": "Pascale",
"given_name": "E.",
"orcid": "0000-0002-3242-8154",
"clpid": "Pascale-E"
},
{
"family_name": "Patanchon",
"given_name": "G.",
"clpid": "Patanchon-G"
},
{
"family_name": "Rex",
"given_name": "M.",
"clpid": "Rex-M"
},
{
"family_name": "Scott",
"given_name": "D.",
"orcid": "0000-0002-6878-9840",
"clpid": "Scott-Douglas"
},
{
"family_name": "Semisch",
"given_name": "C.",
"clpid": "Semisch-C"
},
{
"family_name": "Tucker",
"given_name": "C. E.",
"clpid": "Tucker-C-E"
},
{
"family_name": "Viero",
"given_name": "M. P.",
"clpid": "Viero-M-P"
},
{
"family_name": "Wiebe",
"given_name": "D. V.",
"clpid": "Wiebe-D-V"
},
{
"family_name": "Tucker",
"given_name": "G. S.",
"orcid": "0000-0002-6954-6947",
"clpid": "Tucker-G-S"
}
],
"abstract": "The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) operated successfully during a 100 hr flight from northern Sweden in 2005 June (BLAST05). As part of the calibration and pointing procedures, several compact sources were mapped, including solar system, Galactic, and extragalactic targets, specifically Pallas, CRL 2688, LDN 1014, IRAS 20126+4104, IRAS 21078+5211, IRAS 21307+5049, IRAS 22134+5834, IRAS 23011+6126, K3-50, W75N, and Mrk 231. One additional source, Arp 220, was observed and used as our primary calibrator. Details of the overall BLAST05 calibration procedure are discussed here. The BLAST observations of each compact source are described, flux densities and spectral energy distributions are reported, and these are compared with previous measurements at other wavelengths. The 250, 350, and 500 \u03bcm BLAST data can provide useful constraints to the amplitude and slope of the submillimeter continuum, which in turn may be useful for the improved calibration of other submillimeter instruments.",
"doi": "10.1086/588542",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2008-07-01",
"series_number": "1",
"volume": "681",
"issue": "1",
"pages": "415-427"
},
{
"id": "authors:jrj46-11v83",
"collection": "authors",
"collection_id": "jrj46-11v83",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090517-205138563",
"type": "article",
"title": "SANEPIC: a mapmaking method for time stream data from large arrays",
"author": [
{
"family_name": "Patanchon",
"given_name": "G.",
"clpid": "Patanchon-G"
},
{
"family_name": "Ade",
"given_name": "P. A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Chapin",
"given_name": "E. L.",
"clpid": "Chapin-E-L"
},
{
"family_name": "Devlin",
"given_name": "M. J.",
"clpid": "Devlin-M-J"
},
{
"family_name": "Dicker",
"given_name": "S.",
"clpid": "Dicker-S-R"
},
{
"family_name": "Griffin",
"given_name": "M.",
"clpid": "Griffin-M-J"
},
{
"family_name": "Gundersen",
"given_name": "J. O.",
"clpid": "Gundersen-J-O"
},
{
"family_name": "Halpern",
"given_name": "M.",
"orcid": "0000-0002-1760-0868",
"clpid": "Halpern-M"
},
{
"family_name": "Hargrave",
"given_name": "P. C.",
"orcid": "0000-0002-3109-6629",
"clpid": "Hargrave-P-C"
},
{
"family_name": "Hughes",
"given_name": "D. H.",
"clpid": "Hughes-D-H"
},
{
"family_name": "Klein",
"given_name": "J.",
"clpid": "Klein-J"
},
{
"family_name": "Marsden",
"given_name": "G.",
"clpid": "Marsden-Gaelen"
},
{
"family_name": "Martin",
"given_name": "P. G.",
"orcid": "0000-0002-5236-3896",
"clpid": "Martin-P-G"
},
{
"family_name": "Mauskopf",
"given_name": "P.",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "Netterfield",
"given_name": "C. B.",
"clpid": "Netterfield-C-B"
},
{
"family_name": "Olmi",
"given_name": "L.",
"orcid": "0000-0002-1162-7947",
"clpid": "Olmi-L"
},
{
"family_name": "Pascale",
"given_name": "E.",
"orcid": "0000-0002-3242-8154",
"clpid": "Pascale-E"
},
{
"family_name": "Rex",
"given_name": "M.",
"clpid": "Rex-M"
},
{
"family_name": "Scott",
"given_name": "D.",
"orcid": "0000-0002-6878-9840",
"clpid": "Scott-Douglas"
},
{
"family_name": "Semisch",
"given_name": "C.",
"clpid": "Semisch-C"
},
{
"family_name": "Truch",
"given_name": "M. D. P.",
"clpid": "Truch-M-D-P"
},
{
"family_name": "Tucker",
"given_name": "C.",
"clpid": "Tucker-C-E"
},
{
"family_name": "Tucker",
"given_name": "G. S.",
"orcid": "0000-0002-6954-6947",
"clpid": "Tucker-G-S"
},
{
"family_name": "Viero",
"given_name": "M. P.",
"clpid": "Viero-M-P"
},
{
"family_name": "Wiebe",
"given_name": "D. V.",
"clpid": "Wiebe-D-V"
}
],
"abstract": "We describe a mapmaking method that we have developed for the Balloon-borne Large Aperture Submillimeter Telescope (BLAST) experiment, but which should have general application to data from other submillimeter arrays. Our method uses a maximum likelihood-based approach, with several approximations, which allows images to be constructed using large amounts of data with fairly modest computer memory and processing requirements. This new approach, Signal and Noise Estimation Procedure Including Correlations (SANEPIC), builds on several previous methods but focuses specifically on the regime where there are a large number of detectors sampling the same map of the sky, and explicitly allowing for the possibility of strong correlations between the detector time streams. We provide real and simulated examples of how well this method performs compared with more simplistic mapmakers based on filtering. We discuss two separate implementations of SANEPIC: a brute-force approach, in which the inverse pixel-pixel covariance matrix is computed, and an iterative approach, which is much more efficient for large maps. SANEPIC has been successfully used to produce maps using data from the 2005 BLAST flight.",
"doi": "10.1086/588543",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2008-07-01",
"series_number": "1",
"volume": "681",
"issue": "1",
"pages": "708-725"
},
{
"id": "authors:19gys-4eh43",
"collection": "authors",
"collection_id": "19gys-4eh43",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090517-211252065",
"type": "article",
"title": "The Balloon-borne Large Aperture Submillimeter Telescope: BLAST",
"author": [
{
"family_name": "Pascale",
"given_name": "E.",
"orcid": "0000-0002-3242-8154",
"clpid": "Pascale-E"
},
{
"family_name": "Ade",
"given_name": "P. A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Chapin",
"given_name": "E. L.",
"clpid": "Chapin-E-L"
},
{
"family_name": "Chung",
"given_name": "J.",
"clpid": "Chung-J"
},
{
"family_name": "Devlin",
"given_name": "M. J.",
"clpid": "Devlin-M-J"
},
{
"family_name": "Dicker",
"given_name": "S.",
"clpid": "Dicker-S-R"
},
{
"family_name": "Griffin",
"given_name": "M.",
"clpid": "Griffin-M"
},
{
"family_name": "Gundersen",
"given_name": "J. O.",
"clpid": "Gundersen-J-O"
},
{
"family_name": "Halpern",
"given_name": "M.",
"orcid": "0000-0002-1760-0868",
"clpid": "Halpern-M"
},
{
"family_name": "Hargrave",
"given_name": "P. C.",
"orcid": "0000-0002-3109-6629",
"clpid": "Hargrave-P-C"
},
{
"family_name": "Hughes",
"given_name": "D. H.",
"clpid": "Hughes-D-H"
},
{
"family_name": "Klein",
"given_name": "J.",
"clpid": "Klein-J"
},
{
"family_name": "MacTavish",
"given_name": "C. J.",
"clpid": "MacTavish-C-J"
},
{
"family_name": "Marsden",
"given_name": "G.",
"clpid": "Marsden-Gaelen"
},
{
"family_name": "Martin",
"given_name": "P. G.",
"orcid": "0000-0002-5236-3896",
"clpid": "Martin-P-G"
},
{
"family_name": "Martin",
"given_name": "T. G.",
"clpid": "Martin-T-G"
},
{
"family_name": "Mauskopf",
"given_name": "P.",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "Netterfield",
"given_name": "C. B.",
"clpid": "Netterfield-C-B"
},
{
"family_name": "Olmi",
"given_name": "L.",
"orcid": "0000-0002-1162-7947",
"clpid": "Olmi-L"
},
{
"family_name": "Patanchon",
"given_name": "G.",
"clpid": "Patanchon-G"
},
{
"family_name": "Rex",
"given_name": "M.",
"clpid": "Rex-M"
},
{
"family_name": "Scott",
"given_name": "D.",
"orcid": "0000-0002-6878-9840",
"clpid": "Scott-Douglas"
},
{
"family_name": "Semisch",
"given_name": "C.",
"clpid": "Semisch-C"
},
{
"family_name": "Thomas",
"given_name": "N.",
"clpid": "Thomas-Nicholas-E"
},
{
"family_name": "Truch",
"given_name": "M. D. P.",
"clpid": "Truch-M-D-P"
},
{
"family_name": "Tucker",
"given_name": "C.",
"clpid": "Tucker-C-E"
},
{
"family_name": "Tucker",
"given_name": "G. S.",
"orcid": "0000-0002-6954-6947",
"clpid": "Tucker-G-S"
},
{
"family_name": "Viero",
"given_name": "M. P.",
"clpid": "Viero-M-P"
},
{
"family_name": "Wiebe",
"given_name": "D. V.",
"clpid": "Wiebe-D-V"
}
],
"abstract": "The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) is a suborbital surveying experiment designed to study the evolutionary history and processes of star formation in local galaxies (including the Milky Way) and galaxies at cosmological distances. The BLAST continuum camera, which consists of 270 detectors distributed between three arrays, observes simultaneously in broadband (30%) spectral windows at 250, 350, and 500 \u03bcm. The optical design is based on a 2 m diameter telescope, providing a diffraction-limited resolution of 30'' at 250 \u03bcm. The gondola pointing system enables raster mapping of arbitrary geometry, with a repeatable positional accuracy of ~30''; postflight pointing reconstruction to \u227e5'' rms is achieved. The onboard telescope control software permits autonomous execution of a preselected set of maps, with the option of manual override. In this paper we describe the primary characteristics and measured in-flight performance of BLAST. BLAST performed a test flight in 2003 and has since made two scientifically productive long-duration balloon flights: a 100 hr flight from ESRANGE (Kiruna), Sweden to Victoria Island, northern Canada in 2005 June; and a 250 hr, circumpolar flight from McMurdo Station, Antarctica, in 2006 December.",
"doi": "10.1086/588541",
"issn": "0004-637X",
"publisher": "University of Chicago Press",
"publication": "Astrophysical Journal",
"publication_date": "2008-07-01",
"series_number": "1",
"volume": "681",
"issue": "1",
"pages": "400-414"
},
{
"id": "authors:4yx1j-rfr69",
"collection": "authors",
"collection_id": "4yx1j-rfr69",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090618-202204043",
"type": "article",
"title": "The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) 2005: A 4 deg2 Galactic Plane Survey in Vulpecula (ell = 59\u00b0)",
"author": [
{
"family_name": "Chapin",
"given_name": "E. L.",
"clpid": "Chapin-E-L"
},
{
"family_name": "Ade",
"given_name": "P. A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Brunt",
"given_name": "C.",
"clpid": "Brunt-C"
},
{
"family_name": "Devlin",
"given_name": "M. J.",
"clpid": "Devlin-M-J"
},
{
"family_name": "Dicker",
"given_name": "S.",
"clpid": "Dicker-S-R"
},
{
"family_name": "Griffin",
"given_name": "M.",
"clpid": "Griffin-M"
},
{
"family_name": "Gunderson",
"given_name": "J. O.",
"clpid": "Gunderson-J-O"
},
{
"family_name": "Halpern",
"given_name": "M.",
"orcid": "0000-0002-1760-0868",
"clpid": "Halpern-M"
},
{
"family_name": "Hargrave",
"given_name": "P. C.",
"orcid": "0000-0002-3109-6629",
"clpid": "Hargrave-P-C"
},
{
"family_name": "Hughes",
"given_name": "D. H.",
"clpid": "Hughes-D-H"
},
{
"family_name": "Klein",
"given_name": "J.",
"clpid": "Klein-J"
},
{
"family_name": "Marsden",
"given_name": "G.",
"clpid": "Marsden-Gaelen"
},
{
"family_name": "Martin",
"given_name": "P. G.",
"orcid": "0000-0002-5236-3896",
"clpid": "Martin-P-G"
},
{
"family_name": "Mauskopf",
"given_name": "P. D.",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "Netterfield",
"given_name": "C. B.",
"clpid": "Netterfield-C-B"
},
{
"family_name": "Olmi",
"given_name": "L.",
"orcid": "0000-0002-1162-7947",
"clpid": "Olmi-L"
},
{
"family_name": "Pascale",
"given_name": "E.",
"orcid": "0000-0002-3242-8154",
"clpid": "Pascale-E"
},
{
"family_name": "Patanchon",
"given_name": "G.",
"clpid": "Patanchon-G"
},
{
"family_name": "Rex",
"given_name": "M.",
"clpid": "Rex-M"
},
{
"family_name": "Scott",
"given_name": "D.",
"orcid": "0000-0002-6878-9840",
"clpid": "Scott-Douglas"
},
{
"family_name": "Semisch",
"given_name": "C.",
"clpid": "Semisch-C"
},
{
"family_name": "Truch",
"given_name": "M. D. P.",
"clpid": "Truch-M-D-P"
},
{
"family_name": "Tucker",
"given_name": "C.",
"clpid": "Tucker-C-E"
},
{
"family_name": "Tucker",
"given_name": "G. S.",
"orcid": "0000-0002-6954-6947",
"clpid": "Tucker-G-S"
},
{
"family_name": "Viero",
"given_name": "M. P.",
"clpid": "Viero-M-P"
},
{
"family_name": "Wiebe",
"given_name": "D. V.",
"clpid": "Wiebe-D-V"
}
],
"abstract": "We present the first results from a new 250, 350, and 500 \u03bcm Galactic plane survey taken with the Balloon-borne Large-Aperture Submillimeter Telescope (BLAST) in 2005. This survey's primary goal is to identify and characterize high-mass protostellar objects (HMPOs). The region studied here covers 4 deg^2 near the open cluster NGC 6823 in the constellation Vulpecula (\u2113 = 59\u00b0). We find 60 compact sources (<60'' diameter) detected simultaneously in all three bands. Their SEDs are constrained through BLAST, IRAS, Spitzer MIPS, and MSX photometry, with inferred dust temperatures spanning ~12-40 K assuming a dust emissivity index \u03b2 = 1.5. The luminosity-to-mass ratio, a distance-independent quantity, spans ~0.2-130 L_\u2609 M^(\u22121)_\u2609. Distances are estimated from coincident ^(13)CO(1\u2192 0) velocities combined with a variety of other velocity and morphological data in the literature. In total, 49 sources are associated with a molecular cloud complex encompassing NGC 6823 (distance ~2.3 kpc), 10 objects with the Perseus arm (~8.5 kpc), and one object is probably in the outer Galaxy (~14 kpc). Near NGC 6823, the inferred luminosities and masses of BLAST sources span ~40-10^4 L_\u2609 and ~15-700 M_\u2609, respectively. The mass spectrum is compatible with molecular gas masses in other high-mass star-forming regions. Several luminous sources appear to be ultracompact H II regions powered by early B stars. However, many of the objects are cool, massive gravitationally bound clumps with no obvious internal radiation from a protostar, and hence excellent HMPO candidates.",
"doi": "10.1086/588544",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2008-07-01",
"series_number": "1",
"volume": "681",
"issue": "1",
"pages": "428-452"
},
{
"id": "authors:p79xp-2e929",
"collection": "authors",
"collection_id": "p79xp-2e929",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090423-201108516",
"type": "article",
"title": "The AzTEC mm-wavelength camera",
"author": [
{
"family_name": "Wilson",
"given_name": "G. W.",
"clpid": "Wilson-G-W"
},
{
"family_name": "Austermann",
"given_name": "J. E.",
"clpid": "Austermann-J-E"
},
{
"family_name": "Perera",
"given_name": "T. A.",
"clpid": "Perera-T-A"
},
{
"family_name": "Scott",
"given_name": "K. S.",
"clpid": "Scott-K-S"
},
{
"family_name": "Ade",
"given_name": "P. A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Glenn",
"given_name": "J.",
"orcid": "0000-0001-7527-2017",
"clpid": "Glenn-J"
},
{
"family_name": "Golwala",
"given_name": "S. R.",
"orcid": "0000-0002-1098-7174",
"clpid": "Golwala-S-R"
},
{
"family_name": "Kim",
"given_name": "S.",
"clpid": "Kim-S"
},
{
"family_name": "Kang",
"given_name": "Y.",
"clpid": "Kang-Y"
},
{
"family_name": "Lydon",
"given_name": "D.",
"clpid": "Lydon-D"
},
{
"family_name": "Mauskopf",
"given_name": "P. D.",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "Predmore",
"given_name": "C. R.",
"clpid": "Predmore-C-R"
},
{
"family_name": "Roberts",
"given_name": "C. M.",
"clpid": "Roberts-C-M"
},
{
"family_name": "Souccar",
"given_name": "K.",
"clpid": "Souccar-K"
},
{
"family_name": "Yun",
"given_name": "M. S.",
"orcid": "0000-0001-7095-7543",
"clpid": "Yun-Min-S"
}
],
"abstract": "AzTEC is a mm-wavelength bolometric camera utilizing 144 silicon nitride micromesh detectors. Here, we describe the AzTEC instrument architecture and its use as an astronomical\ninstrument. We report on several performance metrics measured during a three-month observing campaign at the James Clerk Maxwell Telescope and conclude with our plans for AzTEC as a facility instrument on the Large Millimetre Telescope.",
"doi": "10.1111/j.1365-2966.2008.12980.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2008-05-11",
"series_number": "2",
"volume": "386",
"issue": "2",
"pages": "807-818"
},
{
"id": "authors:khfry-9a133",
"collection": "authors",
"collection_id": "khfry-9a133",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090423-212245434",
"type": "article",
"title": "AzTEC millimetre survey of the COSMOS field \u2013 I. data reduction and source catalogue",
"author": [
{
"family_name": "Scott",
"given_name": "K. S.",
"clpid": "Scott-K-S"
},
{
"family_name": "Austermann",
"given_name": "J. E.",
"clpid": "Austermann-J-E"
},
{
"family_name": "Perera",
"given_name": "T. A.",
"clpid": "Perera-T-A"
},
{
"family_name": "Wilson",
"given_name": "G. W.",
"clpid": "Wilson-G-W"
},
{
"family_name": "Aretxaga",
"given_name": "I.",
"orcid": "0000-0002-6590-3994",
"clpid": "Aretxaga-I"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Hughes",
"given_name": "D. H.",
"clpid": "Hughes-D-H"
},
{
"family_name": "Kang",
"given_name": "Y.",
"clpid": "Kang-Y"
},
{
"family_name": "Kim",
"given_name": "S.",
"clpid": "Kim-S"
},
{
"family_name": "Mauskopf",
"given_name": "P. D.",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "Sanders",
"given_name": "D. B.",
"orcid": "0000-0002-1233-9998",
"clpid": "Sanders-D-B"
},
{
"family_name": "Scoville",
"given_name": "N.",
"orcid": "0000-0002-0438-3323",
"clpid": "Scoville-N-Z"
},
{
"family_name": "Yun",
"given_name": "M. S.",
"orcid": "0000-0001-7095-7543",
"clpid": "Yun-Min-S"
}
],
"abstract": "We present a 1.1mm wavelength imaging survey covering 0.3 deg^2 in the COSMOS field. These data, obtained with the AzTEC continuum camera on the James Clerk Maxwell Telescope, were centred on a prominent large-scale structure overdensity which includes a rich X-ray cluster at z \u2248 0.73. A total of 50 mm-galaxy candidates, with a significance ranging from 3.5 to 8.5\u03c3, are extracted from the central 0.15 deg^2 area which has a uniform sensitivity of \u223c1.3 mJy beam^\u22121. 16 sources are detected with S/N \u2265 4.5, where the expected false detection rate is zero, of which a surprisingly large number (9) have intrinsic (deboosted) fluxes \u22655 mJy at 1.1 mm. Assuming the emission is dominated by radiation from dust, heated by a massive population of young, optically obscured stars, then these bright AzTEC sources have far-infrared luminosities >6 \u00d7 10^(12)L_\u2609 and star formation rates \u22651100M_\u2609 yr^(\u22121). Two of these nine bright AzTEC sources are found towards the extreme peripheral region of the X-ray cluster, whilst the remainder are distributed across the larger scale overdensity. We describe the AzTEC data reduction pipeline, the source-extraction algorithm, and the characterization of the source catalogue, including the completeness, flux deboosting correction, false-detection rate and the source positional uncertainty, through an extensive set of Monte Carlo simulations. We conclude with a preliminary comparison, via a stacked analysis, of the overlapping MIPS 24-\u03bcm data and radio data with this AzTEC map of the COSMOS field.",
"doi": "10.1111/j.1365-2966.2008.12989.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2008-04-21",
"series_number": "4",
"volume": "385",
"issue": "4",
"pages": "2225-2238"
},
{
"id": "authors:qxnd5-ztk79",
"collection": "authors",
"collection_id": "qxnd5-ztk79",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:ADEapj08",
"type": "article",
"title": "First season QUaD CMB temperature and polarization power spectra",
"author": [
{
"family_name": "Ade",
"given_name": "P.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Bock",
"given_name": "J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bowden",
"given_name": "M.",
"clpid": "Bowden-M"
},
{
"family_name": "Brown",
"given_name": "M. L.",
"clpid": "Brown-M-L"
},
{
"family_name": "Cahill",
"given_name": "V.",
"clpid": "Cahill-V"
},
{
"family_name": "Carlstrom",
"given_name": "J. E.",
"orcid": "0000-0002-2044-7665",
"clpid": "Carlstrom-J-E"
},
{
"family_name": "Castro",
"given_name": "P. G.",
"clpid": "Castro-P-G"
},
{
"family_name": "Church",
"given_name": "S.",
"clpid": "Church-S"
},
{
"family_name": "Culverhouse",
"given_name": "T.",
"clpid": "Culverhouse-T"
},
{
"family_name": "Friedman",
"given_name": "R.",
"clpid": "Friedman-R"
},
{
"family_name": "Ganga",
"given_name": "K.",
"clpid": "Ganga-K"
},
{
"family_name": "Gear",
"given_name": "W. K.",
"clpid": "Gear-W-K"
},
{
"family_name": "Hinderks",
"given_name": "J.",
"clpid": "Hinderks-J"
},
{
"family_name": "Kovac",
"given_name": "J.",
"clpid": "Kovac-J"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Leitch",
"given_name": "E. M.",
"clpid": "Leitch-E-M"
},
{
"family_name": "Melhuish",
"given_name": "S. J.",
"clpid": "Melhuish-S-J"
},
{
"family_name": "Murphy",
"given_name": "J. A.",
"clpid": "Murphy-J-A"
},
{
"family_name": "Orlando",
"given_name": "A.",
"clpid": "Orlando-A"
},
{
"family_name": "Schwarz",
"given_name": "R.",
"clpid": "Schwarz-R-B"
},
{
"family_name": "O'Sullivan",
"given_name": "C.",
"clpid": "O'Sullivan-C"
},
{
"family_name": "Piccirillo",
"given_name": "L.",
"clpid": "Piccirillo-L"
},
{
"family_name": "Pryke",
"given_name": "C.",
"clpid": "Pryke-C"
},
{
"family_name": "Rajguru",
"given_name": "N.",
"clpid": "Rajguru-N"
},
{
"family_name": "Rusholme",
"given_name": "B.",
"orcid": "0000-0001-7648-4142",
"clpid": "Rusholme-B"
},
{
"family_name": "Taylor",
"given_name": "A. N.",
"clpid": "Taylor-A-N"
},
{
"family_name": "Thompson",
"given_name": "K. L.",
"clpid": "Thompson-K-L"
},
{
"family_name": "Wu",
"given_name": "E. Y. S.",
"clpid": "Wu-E-Y-S"
},
{
"family_name": "Zemcov",
"given_name": "M.",
"orcid": "0000-0001-8253-1451",
"clpid": "Zemcov-M"
}
],
"abstract": "QUaD is a bolometric CMB polarimeter sited at the South Pole, operating at frequencies of 100 and 150 GHz. In this paper we report preliminary results from the first season of operation (austral winter 2005). All six CMB power spectra are presented derived as cross spectra between the 100 and 150 GHz maps using 67 days of observation in a low foreground region of approximately 60 deg^2. These data are a small fraction of the data acquired to date. The measured spectra are consistent with the \u039bCDM cosmological model. We perform jackknife tests that indicate that the observed signal has negligible contamination from instrumental systematics. In addition, by using a frequency jackknife we find no evidence for foreground contamination.",
"doi": "10.1086/524922",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2008-02-10",
"series_number": "1",
"volume": "674",
"issue": "1",
"pages": "22-28"
},
{
"id": "authors:etqdy-8y960",
"collection": "authors",
"collection_id": "etqdy-8y960",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091202-122207165",
"type": "article",
"title": "Searching for Non-Gaussian Signals in the BOOMERANG 2003 CMB Maps",
"author": [
{
"family_name": "De Troia",
"given_name": "G.",
"clpid": "De-Troia-G"
},
{
"family_name": "Ade",
"given_name": "P. A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bond",
"given_name": "J. R.",
"orcid": "0000-0003-2358-9949",
"clpid": "Bond-J-R"
},
{
"family_name": "Borrill",
"given_name": "J.",
"clpid": "Borrill-J"
},
{
"family_name": "Boscaleri",
"given_name": "A.",
"clpid": "Boscaleri-A"
},
{
"family_name": "Cabella",
"given_name": "P.",
"clpid": "Cabella-P"
},
{
"family_name": "Contaldi",
"given_name": "C. R.",
"clpid": "Contaldi-C-R"
},
{
"family_name": "Crill",
"given_name": "B. P.",
"orcid": "0000-0002-4650-8518",
"clpid": "Crill-B-P"
},
{
"family_name": "de Bernardis",
"given_name": "P.",
"orcid": "0000-0001-6547-6446",
"clpid": "de-Bernardis-P"
},
{
"family_name": "De Gasperis",
"given_name": "G.",
"clpid": "De-Gasperis-G"
},
{
"family_name": "de Oliveira-Costa",
"given_name": "A.",
"clpid": "de-Oliveira-Costa-A"
},
{
"family_name": "Di Stefano",
"given_name": "G.",
"clpid": "Di-Stefano-G"
},
{
"family_name": "Ferreira",
"given_name": "P. G.",
"clpid": "Ferreira-P-G"
},
{
"family_name": "Hivon",
"given_name": "E.",
"clpid": "Hivon-E"
},
{
"family_name": "Jaffe",
"given_name": "A. H.",
"clpid": "Jaffe-A-H"
},
{
"family_name": "Kisner",
"given_name": "T. S.",
"clpid": "Kisner-T-S"
},
{
"family_name": "Kunz",
"given_name": "M.",
"clpid": "Kinz-M"
},
{
"family_name": "Jones",
"given_name": "W. C.",
"clpid": "Jones-W-C"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Liguori",
"given_name": "M.",
"clpid": "Liguori-M"
},
{
"family_name": "Masi",
"given_name": "S.",
"orcid": "0000-0001-5105-1439",
"clpid": "Masi-S"
},
{
"family_name": "Matarrese",
"given_name": "S.",
"clpid": "Matarrese-S"
},
{
"family_name": "Mauskopf",
"given_name": "P. D.",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "MacTavish",
"given_name": "C. J.",
"clpid": "MacTavish-C-J"
},
{
"family_name": "Melchiorri",
"given_name": "A.",
"clpid": "Melchiorri-A"
},
{
"family_name": "Montroy",
"given_name": "T. E.",
"clpid": "Montroy-T-E"
},
{
"family_name": "Natoli",
"given_name": "P.",
"clpid": "Natoli-P"
},
{
"family_name": "Netterfield",
"given_name": "C. B.",
"clpid": "Netterfield-C-B"
},
{
"family_name": "Pascale",
"given_name": "E.",
"orcid": "0000-0002-3242-8154",
"clpid": "Pascale-E"
},
{
"family_name": "Piacentini",
"given_name": "F.",
"orcid": "0000-0002-5444-9327",
"clpid": "Piacentini-F"
},
{
"family_name": "Pogosyan",
"given_name": "D.",
"clpid": "Pogosyan-D"
},
{
"family_name": "Polenta",
"given_name": "G.",
"clpid": "Polenta-G"
},
{
"family_name": "Prunet",
"given_name": "S.",
"clpid": "Prunet-S"
},
{
"family_name": "Ricciardi",
"given_name": "S.",
"clpid": "Ricciardi-S"
},
{
"family_name": "Romeo",
"given_name": "G.",
"clpid": "Romeo-G"
},
{
"family_name": "Ruhl",
"given_name": "J. E.",
"clpid": "Ruhl-J-E"
},
{
"family_name": "Santini",
"given_name": "P.",
"clpid": "Santini-P"
},
{
"family_name": "Tegmark",
"given_name": "M.",
"clpid": "Tegmark-M"
},
{
"family_name": "Veneziani",
"given_name": "M.",
"clpid": "Veneziani-M"
},
{
"family_name": "Vittorio",
"given_name": "N.",
"clpid": "Vittorio-N"
}
],
"abstract": "We analyze the BOOMERANG 2003 (B03) 145 GHz temperature map to constrain the amplitude of a non-Gaussian, primordial contribution to CMB fluctuations. We perform a pixel-space analysis restricted to a portion of the map chosen in view of high-sensitivity, very low foreground contamination and tight control of systematic effects. We set up an estimator based on the three Minkowski functionals which relies on high-quality simulated data, including non-Gaussian CMB maps. We find good agreement with the Gaussian hypothesis and derive the first limits based on BOOMERANG data for the nonlinear coupling parameter f_(NL) as -300 < f_(NL) < 650 at 68% CL and -800 < f_(NL) < 1050 at 95% CL.",
"doi": "10.1086/524402",
"issn": "2041-8205",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal Letters",
"publication_date": "2007-12-01",
"series_number": "2",
"volume": "670",
"issue": "2",
"pages": "L73-L76"
},
{
"id": "authors:natpy-dv072",
"collection": "authors",
"collection_id": "natpy-dv072",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:JONapj06",
"type": "article",
"title": "A Measurement of the Angular Power Spectrum of the CMB Temperature Anisotropy from the 2003 Flight of BOOMERANG",
"author": [
{
"family_name": "Jones",
"given_name": "W. C.",
"clpid": "Jones-W-C"
},
{
"family_name": "Ade",
"given_name": "P. A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bond",
"given_name": "J. R.",
"orcid": "0000-0003-2358-9949",
"clpid": "Bond-J-R"
},
{
"family_name": "Borrill",
"given_name": "J.",
"clpid": "Borrill-J"
},
{
"family_name": "Boscaleri",
"given_name": "A.",
"clpid": "Boscaleri-A"
},
{
"family_name": "Cabella",
"given_name": "P.",
"clpid": "Cabella-P"
},
{
"family_name": "Contaldi",
"given_name": "C. R.",
"clpid": "Contaldi-C-R"
},
{
"family_name": "Crill",
"given_name": "B. P.",
"orcid": "0000-0002-4650-8518",
"clpid": "Crill-B-P"
},
{
"family_name": "de Bernardis",
"given_name": "P.",
"orcid": "0000-0001-6547-6446",
"clpid": "de-Bernardis-P"
},
{
"family_name": "De Gasperis",
"given_name": "G.",
"clpid": "De-Gasperis-G"
},
{
"family_name": "de Oliveira-Costa",
"given_name": "A.",
"clpid": "de-Oliveira-Costa-A"
},
{
"family_name": "De Troia",
"given_name": "G.",
"clpid": "De-Troia-G"
},
{
"family_name": "di Stefano",
"given_name": "G.",
"clpid": "di-Stefano-G"
},
{
"family_name": "Hivon",
"given_name": "E.",
"clpid": "Hivon-E"
},
{
"family_name": "Jaffe",
"given_name": "A. H.",
"clpid": "Jaffe-A-H"
},
{
"family_name": "Kisner",
"given_name": "T. S.",
"clpid": "Kisner-T-S"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "MacTavish",
"given_name": "C. J.",
"clpid": "MacTavish-C-J"
},
{
"family_name": "Masi",
"given_name": "S.",
"orcid": "0000-0001-5105-1439",
"clpid": "Masi-S"
},
{
"family_name": "Mauskopf",
"given_name": "P. D.",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "Melchiorri",
"given_name": "A.",
"clpid": "Melchiorri-A"
},
{
"family_name": "Montroy",
"given_name": "T. E.",
"clpid": "Montroy-T-E"
},
{
"family_name": "Natoli",
"given_name": "P.",
"clpid": "Natoli-P"
},
{
"family_name": "Netterfield",
"given_name": "C. B.",
"clpid": "Netterfield-C-B"
},
{
"family_name": "Pascale",
"given_name": "E.",
"orcid": "0000-0002-3242-8154",
"clpid": "Pascale-E"
},
{
"family_name": "Piacentini",
"given_name": "F.",
"orcid": "0000-0002-5444-9327",
"clpid": "Piacentini-F"
},
{
"family_name": "Pogosyan",
"given_name": "D.",
"clpid": "Pogosyan-D"
},
{
"family_name": "Polenta",
"given_name": "G.",
"clpid": "Polenta-G"
},
{
"family_name": "Prunet",
"given_name": "S.",
"clpid": "Prunet-S"
},
{
"family_name": "Ricciardi",
"given_name": "S.",
"clpid": "Ricciardi-S"
},
{
"family_name": "Romeo",
"given_name": "G.",
"clpid": "Romeo-G"
},
{
"family_name": "Ruhl",
"given_name": "J. E.",
"clpid": "Ruhl-J-E"
},
{
"family_name": "Santini",
"given_name": "P.",
"clpid": "Santini-P"
},
{
"family_name": "Tegmark",
"given_name": "M.",
"clpid": "Tegmark-M"
},
{
"family_name": "Veneziani",
"given_name": "M.",
"clpid": "Veneziani-M"
},
{
"family_name": "Vittorio",
"given_name": "N.",
"clpid": "Vittorio-N"
}
],
"abstract": "We report on observations of the cosmic microwave background (CMB) obtained during the 2003 January flight of BOOMERANG. These results are derived from 195 hr of observation with four 145 GHz polarization-sensitive bolometer (PSB) pairs, identical in design to the four 143 GHz Planck High Frequency Instrument (HFI) polarized pixels. The data include 75 hr of observations distributed over 1.84% of the sky with an additional 120 hr concentrated on the central portion of the field, which represents 0.22% of the full sky. From these data we derive an estimate of the angular power spectrum of temperature fluctuations of the CMB in 24 bands over the multipole range 50 \u2264 l \u2264 1500. A series of features, consistent with those expected from acoustic oscillations in the primordial photon-baryon fluid, are clearly evident in the power spectrum, as is the exponential damping of power on scales smaller than the photon mean free path at the epoch of last scattering (l \u2273 900). As a consistency check, the collaboration has performed two fully independent analyses of the time-ordered data, which are found to be in excellent agreement.",
"doi": "10.1086/505559",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2006-08-20",
"series_number": "2",
"volume": "647",
"issue": "2",
"pages": "823-832"
},
{
"id": "authors:4m1yp-yj755",
"collection": "authors",
"collection_id": "4m1yp-yj755",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110629-150937119",
"type": "article",
"title": "A Measurement of the CMB Spectrum from the 2003 Flight of BOOMERANG",
"author": [
{
"family_name": "Montroy",
"given_name": "T. E.",
"clpid": "Montroy-T-E"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Crill",
"given_name": "B. P.",
"orcid": "0000-0002-4650-8518",
"clpid": "Crill-B-P"
},
{
"family_name": "Hivon",
"given_name": "E.",
"clpid": "Hivon-E"
},
{
"family_name": "Jones",
"given_name": "W. C.",
"clpid": "Jones-W-C"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
}
],
"abstract": "We report measurements of the CMB polarization power spectra from the 2003 January Antarctic flight of BOOMERANG. The primary results come from 6 days of observation of a patch covering 0.22% of the sky centered near R.A. = 82\u00b0.5, decl. = -45\u00b0. The observations were made using four pairs of polarization-sensitive bolometers operating in bands centered at 145 GHz. Using two independent analysis pipelines, we measure a nonzero signal in the range 201 < l < 1000 with a significance of 4.8 \u03c3, a 2 \u03c3 upper limit of 8.6 \u03bcK^2 for any contribution, and a 2 \u03c3 upper limit of 7.0 \u03bcK^2 for the spectrum. Estimates of foreground intensity fluctuations and the nondetection of and signals rule out any significant contribution from Galactic foregrounds. The results are consistent with a \u039bCDM cosmology seeded by adiabatic perturbations. We note that this is the first detection of CMB polarization with bolometric detectors.",
"doi": "10.1086/505560",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2006-08-20",
"series_number": "2",
"volume": "647",
"issue": "2",
"pages": "813-822"
},
{
"id": "authors:xmx8s-16493",
"collection": "authors",
"collection_id": "xmx8s-16493",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100629-095444366",
"type": "article",
"title": "A Measurement of the Polarization-Temperature Angular Cross-Power Spectrum of the Cosmic Microwave Background from the 2003 Flight of BOOMERANG",
"author": [
{
"family_name": "Piacentini",
"given_name": "F.",
"orcid": "0000-0002-5444-9327",
"clpid": "Piacentini-F"
},
{
"family_name": "Ade",
"given_name": "P. A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bond",
"given_name": "J. R.",
"orcid": "0000-0003-2358-9949",
"clpid": "Bond-J-R"
},
{
"family_name": "Borrill",
"given_name": "J.",
"clpid": "Borrill-J"
},
{
"family_name": "Boscaleri",
"given_name": "A.",
"clpid": "Boscaleri-A"
},
{
"family_name": "Cabella",
"given_name": "P.",
"clpid": "Cabella-P"
},
{
"family_name": "Contaldi",
"given_name": "C. R.",
"clpid": "Contaldi-C-R"
},
{
"family_name": "Crill",
"given_name": "B. P.",
"orcid": "0000-0002-4650-8518",
"clpid": "Crill-B-P"
},
{
"family_name": "de Bernardis",
"given_name": "P.",
"orcid": "0000-0001-6547-6446",
"clpid": "de-Bernardis-P"
},
{
"family_name": "De Gasperis",
"given_name": "G.",
"clpid": "De-Gasperis-G"
},
{
"family_name": "de Oliveira-Costa",
"given_name": "A.",
"clpid": "de-Oliveira-Costa-A"
},
{
"family_name": "De Troia",
"given_name": "G.",
"clpid": "De-Troia-G"
},
{
"family_name": "di Stefano",
"given_name": "G.",
"clpid": "di-Stefano-G"
},
{
"family_name": "Hivon",
"given_name": "E.",
"clpid": "Hivon-E"
},
{
"family_name": "Jaffe",
"given_name": "A. H.",
"clpid": "Jaffe-A-H"
},
{
"family_name": "Kisner",
"given_name": "T. S.",
"clpid": "Kisner-T-S"
},
{
"family_name": "Jones",
"given_name": "W. C.",
"clpid": "Jones-W-C"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Masi",
"given_name": "S.",
"orcid": "0000-0001-5105-1439",
"clpid": "Masi-S"
},
{
"family_name": "Mauskopf",
"given_name": "P. D.",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "MacTavish",
"given_name": "C. J.",
"clpid": "MacTavish-C-J"
},
{
"family_name": "Melchiorri",
"given_name": "A.",
"clpid": "Melchiorri-A"
},
{
"family_name": "Montroy",
"given_name": "T. E.",
"clpid": "Montroy-T-E"
},
{
"family_name": "Natoli",
"given_name": "P.",
"clpid": "Natoli-P"
},
{
"family_name": "Netterfield",
"given_name": "C. B.",
"clpid": "Netterfield-C-B"
},
{
"family_name": "Pascale",
"given_name": "E.",
"orcid": "0000-0002-3242-8154",
"clpid": "Pascale-E"
},
{
"family_name": "Pogosyan",
"given_name": "D.",
"clpid": "Pogosyan-D"
},
{
"family_name": "Polenta",
"given_name": "G.",
"clpid": "Polenta-G"
},
{
"family_name": "Prunet",
"given_name": "S.",
"clpid": "Prunet-S"
},
{
"family_name": "Ricciardi",
"given_name": "S.",
"clpid": "Ricciardi-S"
},
{
"family_name": "Romeo",
"given_name": "G.",
"clpid": "Romeo-G"
},
{
"family_name": "Ruhl",
"given_name": "J. E.",
"clpid": "Ruhl-J-E"
},
{
"family_name": "Santini",
"given_name": "P.",
"clpid": "Santini-P"
},
{
"family_name": "Tegmark",
"given_name": "M.",
"clpid": "Tegmark-M"
},
{
"family_name": "Veneziani",
"given_name": "M.",
"clpid": "Veneziani-M"
},
{
"family_name": "Vittorio",
"given_name": "N.",
"clpid": "Vittorio-N"
}
],
"abstract": "We present a measurement of the polarization-temperature angular cross power spectra, and , of the cosmic microwave background. The result is based on ~200 hr of data from eight polarization-sensitive bolometers operating at 145 GHz during the 2003 flight of BOOMERANG. We detect a significant TE correlation in the l-range between 50 and 950 with a statistical significance of >3.5 \u03c3. Contamination by polarized foreground emission and systematic effects are negligible in comparison with statistical uncertainties. The spectrum is consistent with previous detections and with the \"concordance model\" that assumes adiabatic initial conditions. This is the first measurement of polarization-temperature angular cross-power spectra using bolometric detectors.",
"doi": "10.1086/505557",
"issn": "0004-637X",
"publisher": "American Astronomical Society",
"publication": "Astrophysical Journal",
"publication_date": "2006-08-20",
"series_number": "2",
"volume": "647",
"issue": "2",
"pages": "833-839"
},
{
"id": "authors:tyxew-qea43",
"collection": "authors",
"collection_id": "tyxew-qea43",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110727-112202154",
"type": "article",
"title": "MAXIMA: A balloon-borne cosmic microwave background anisotropy experiment",
"author": [
{
"family_name": "Rabii",
"given_name": "B.",
"clpid": "Rabii-B"
},
{
"family_name": "Winant",
"given_name": "C. D.",
"clpid": "Winant-C-D"
},
{
"family_name": "Collins",
"given_name": "J. S.",
"clpid": "Collins-J-S"
},
{
"family_name": "Lee",
"given_name": "A. T.",
"clpid": "Lee-Adrian-T"
},
{
"family_name": "Richards",
"given_name": "P. L.",
"clpid": "Richards-P-L"
},
{
"family_name": "Abroe",
"given_name": "M. E.",
"clpid": "Abroe-M-E"
},
{
"family_name": "Hanany",
"given_name": "S.",
"clpid": "Hanany-S"
},
{
"family_name": "Johnson",
"given_name": "B. R.",
"clpid": "Johnson-B-R"
},
{
"family_name": "Ade",
"given_name": "P.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Balbi",
"given_name": "A.",
"clpid": "Balbi-A"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Borrill",
"given_name": "J.",
"clpid": "Borrill-J"
},
{
"family_name": "Stompor",
"given_name": "R.",
"clpid": "Stompor-R"
},
{
"family_name": "Boscaleri",
"given_name": "A.",
"clpid": "Boscaleri-A"
},
{
"family_name": "Pascale",
"given_name": "E.",
"orcid": "0000-0002-3242-8154",
"clpid": "Pascale-E"
},
{
"family_name": "de Bernardis",
"given_name": "P.",
"orcid": "0000-0001-6547-6446",
"clpid": "de-Bernardis-P"
},
{
"family_name": "Ferreira",
"given_name": "P. G.",
"clpid": "Ferreira-P-G"
},
{
"family_name": "Hristov",
"given_name": "V. V.",
"clpid": "Hristov-V-V"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Jaffe",
"given_name": "A. H.",
"clpid": "Jaffe-A-H"
},
{
"family_name": "Netterfield",
"given_name": "C. B.",
"clpid": "Netterfield-C-B"
},
{
"family_name": "Smoot",
"given_name": "G. F.",
"clpid": "Smoot-George-F"
},
{
"family_name": "Wu",
"given_name": "J. H. P.",
"clpid": "Wu-J-H-P"
}
],
"abstract": "We describe the Millimeter wave Anisotropy eXperiment IMaging Array (MAXIMA), a balloon-borne experiment which measured the temperature anisotropy of the cosmic microwave background (CMB) on angular scales of 10\u2032 to 5\u00b0. MAXIMA mapped the CMB using 16 bolometric detectors in spectral bands centered at 150, 240, and 410\u2004GHz, with 10\u2032 resolution at all frequencies. The combined receiver sensitivity to CMB anisotropy was ~40\u2004\u03bcK \u221as. The bolometric detectors, which were cooled to 100\u2004mK, were a prototype of the detectors which will be used on the Planck Surveyor Satellite of the European Space Agency. Systematic parasitic contributions were controlled by using four uncorrelated spatial modulations, thorough cross-linking, multiple independent CMB observations, heavily baffled optics, and strong spectral discrimination. Pointing reconstruction was accurate to 1\u2032, and absolute calibration was better than 4%. Two MAXIMA flights with more than 8.5\u2004h of CMB observations have mapped a total of 300\u2004deg^2 of the sky in regions of negligible known foreground emission. MAXIMA results have been released in previous publications and shown to be consistent with the Wilkinson Microwave Anisotropy Probe. MAXIMA I maps, power spectra, and correlation matrices are publicly available at http://cosmology.berkeley.edu/maxima.",
"doi": "10.1063/1.2219723",
"issn": "0034-6748",
"publisher": "American Institute of Physics",
"publication": "Review of Scientific Instruments",
"publication_date": "2006-07",
"series_number": "7",
"volume": "77",
"issue": "7",
"pages": "Art. No. 071101"
},
{
"id": "authors:tjs1w-t4x15",
"collection": "authors",
"collection_id": "tjs1w-t4x15",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110120-144321793",
"type": "article",
"title": "The cosmic infrared background experiment",
"author": [
{
"family_name": "Bock",
"given_name": "James",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Battle",
"given_name": "John",
"clpid": "Battle-J"
},
{
"family_name": "Cooray",
"given_name": "Asantha",
"orcid": "0000-0002-3892-0190",
"clpid": "Cooray-A"
},
{
"family_name": "Kawada",
"given_name": "Misunobu",
"clpid": "Kawada-Misunobu"
},
{
"family_name": "Keating",
"given_name": "Brian",
"clpid": "Keating-B"
},
{
"family_name": "Lange",
"given_name": "Andrew",
"clpid": "Lange-A-E"
},
{
"family_name": "Lee",
"given_name": "Dae-Hea",
"clpid": "Lee-Dae-Hea"
},
{
"family_name": "Matsumoto",
"given_name": "Toshio",
"orcid": "0000-0001-6066-5221",
"clpid": "Matsumoto-Toshio"
},
{
"family_name": "Matsuura",
"given_name": "Shuji",
"orcid": "0000-0002-5698-9634",
"clpid": "Matsuura-Shuji"
},
{
"family_name": "Pak",
"given_name": "Soojong",
"clpid": "Pak-Soojong"
},
{
"family_name": "Renbarger",
"given_name": "Tom",
"clpid": "Renbarger-T"
},
{
"family_name": "Sullivan",
"given_name": "Ian",
"clpid": "Sullivan-I"
},
{
"family_name": "Tsumura",
"given_name": "Kohji",
"clpid": "Tsumura-Kohji"
},
{
"family_name": "Wada",
"given_name": "Takehiko",
"clpid": "Wada-Takehiko"
},
{
"family_name": "Watabe",
"given_name": "Toyoki",
"clpid": "Watabe-Toyoki"
}
],
"abstract": "The extragalactic background, based on absolute measurements reported by DIRBE and IRTS at 1.2 and 2.2 \u00b5m, exceeds the brightness\nderived from galaxy counts by up to a factor 5. Furthermore, both DIRBE and the IRTS report fluctuations in the near-infrared sky\nbrightness that appear to have an extra-galactic origin, but are larger than expected from local (z = 1\u20133) galaxies. These observations\nhave led to speculation that a new class of high-mass stars or mini-quasars may dominate primordial star formation at high-redshift\n(z ~ 10\u201320), which, in order to explain the excess in the near-infrared background, must be highly luminous but produce a limited\namount of metals and X-ray photons. Regardless of the nature of the sources, if a significant component of the near-infrared background\ncomes from first-light galaxies, theoretical models generically predict a prominent near-infrared spectral feature from the redshifted\nLyman cutoff, and a distinctive fluctuation power spectrum.\nWe are developing a rocket-borne instrument (the Cosmic Infrared Background ExpeRiment, or CIBER) to search for signatures of\nprimordial galaxy formation in the cosmic near-infrared extra-galactic background. CIBER consists of a wide-field two-color camera, a\nlow-resolution absolute spectrometer, and a high-resolution narrow-band imaging spectrometer.\nThe cameras will search for spatial fluctuations in the background on angular scales from 7\" to 2\u00b0, where a first-light galaxy signature\nis expected to peak, over a range of angular scales poorly covered by previous experiments. CIBER will determine if the fluctuations\nreported by the IRTS arise from first-light galaxies or have a local origin. In a short rocket flight CIBER has sensitivity to probe fluctuations\n100x fainter than IRTS/DIRBE, with sufficient resolution to remove local-galaxy correlations. By jointly observing regions of\nthe sky studied by Spitzer and ASTRO-F, CIBER will build a multi-color view of the near-infrared background, accurately assessing the\ncontribution of local (z = 1\u20133) galaxies to the observed background fluctuations, allowing a deep and comprehensive survey for first-light\ngalaxy background fluctuations.\nThe low-resolution spectrometer will search for a redshifted Lyman cutoff feature between 0.8 and 2.0 \u00b5m. The high-resolution\nspectrometer will trace zodiacal light using the intensity of scattered Fraunhofer lines, providing an independent measurement of the\nzodiacal emission and a new check of DIRBE zodiacal dust models. The combination will systematically search for the infrared\nexcess background light reported in near-infrared DIRBE/IRTS data, compared with the small excess reported at optical\nwavelengths.",
"doi": "10.1016/j.newar.2005.11.034",
"issn": "1387-6473",
"publisher": "Elsevier",
"publication": "New Astronomy Reviews",
"publication_date": "2006-03",
"series_number": "1-3",
"volume": "50",
"issue": "1-3",
"pages": "215-220"
},
{
"id": "authors:v4wa5-25m84",
"collection": "authors",
"collection_id": "v4wa5-25m84",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200130-075505900",
"type": "article",
"title": "Scientific optimization of a ground-based CMB polarization experiment",
"author": [
{
"family_name": "Bowden",
"given_name": "M.",
"clpid": "Bowden-M"
},
{
"family_name": "Taylor",
"given_name": "A. N.",
"clpid": "Taylor-A-N"
},
{
"family_name": "Ganga",
"given_name": "K. M.",
"clpid": "Ganga-K-M"
},
{
"family_name": "Ade",
"given_name": "P. A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Cahill",
"given_name": "G.",
"clpid": "Cahill-G"
},
{
"family_name": "Carlstrom",
"given_name": "J. E.",
"orcid": "0000-0002-2044-7665",
"clpid": "Carlstrom-J-E"
},
{
"family_name": "Church",
"given_name": "S. E.",
"clpid": "Church-S-E"
},
{
"family_name": "Gear",
"given_name": "W. K.",
"clpid": "Gear-W-K"
},
{
"family_name": "Hinderks",
"given_name": "J. R.",
"clpid": "Hinderks-J-R"
},
{
"family_name": "Hu",
"given_name": "W.",
"clpid": "Hu-W"
},
{
"family_name": "Keating",
"given_name": "B. G.",
"clpid": "Keating-B-G"
},
{
"family_name": "Kovac",
"given_name": "J.",
"clpid": "Kovac-J"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Leitch",
"given_name": "E. M.",
"clpid": "Leitch-E-M"
},
{
"family_name": "Maffei",
"given_name": "B.",
"clpid": "Maffei-B"
},
{
"family_name": "Mallie",
"given_name": "O. E.",
"clpid": "Mallie-O-E"
},
{
"family_name": "Melhuish",
"given_name": "S. J.",
"clpid": "Melhuish-S-J"
},
{
"family_name": "Murphy",
"given_name": "J. A.",
"clpid": "Murphy-J-A"
},
{
"family_name": "Pisano",
"given_name": "G.",
"clpid": "Pisano-G"
},
{
"family_name": "Piccirillo",
"given_name": "L.",
"clpid": "Piccirillo-L"
},
{
"family_name": "Pryke",
"given_name": "C.",
"clpid": "Pryke-C"
},
{
"family_name": "Rusholme",
"given_name": "B. A.",
"clpid": "Rusholme-B-A"
},
{
"family_name": "O'Sullivan",
"given_name": "C.",
"clpid": "O'Sullivan-C"
},
{
"family_name": "Thompson",
"given_name": "K.",
"clpid": "Thompson-K"
}
],
"abstract": "We investigate the science goals achievable with the upcoming generation of ground-based cosmic microwave background polarization experiments, focusing on one particular experiment, QUaD [QUEST (Q and U Extragalactic Submillimetre Telescope) and DASI (Degree Angular Scale Interferometer)], a proposed bolometric polarimeter operating from the South Pole. We calculate the optimal sky coverage for this experiment, including the effects of foregrounds and gravitational lensing. We find that an E-mode measurement will be sample-limited, whereas a B-mode measurement will be detector-noise-limited. We conclude that a 300 deg\u00b2 survey is an optimal compromise for a 2-yr experiment to measure both E and B modes, and that a ground-based polarization experiment can make an important contribution to B-mode surveys. QUaD can make a high significance measurement of the acoustic peaks in the E-mode spectrum, over a multipole range of 25 < \u2113 < 2500, and will be able to detect the gravitational lensing signal in the B-mode spectrum. Such an experiment could also directly detect the gravitational wave component of the B-mode spectrum if the amplitude of the signal is close to current upper limits. We also investigate how QUaD can improve constraints on the cosmological parameters. We estimate that combining two years of QUaD data with the 4-yr Wilkinson Microwave Anisotropy Probe (WMAP) data can improve constraints on \u03a9_bh\u00b2, \u03a9_mh\u00b2, h, r and n_s by a factor of 2. If the foreground contamination can be reduced, the measurement of r can be improved by up to a factor of 6 over that obtainable from WMAP alone. These improved accuracies will place strong constraints on the potential of the inflaton field.",
"doi": "10.1111/j.1365-2966.2004.07506.x",
"issn": "1365-2966",
"publisher": "Oxford University Press",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2004-03",
"series_number": "1",
"volume": "349",
"issue": "1",
"pages": "321-335"
},
{
"id": "authors:0m8p5-wqy33",
"collection": "authors",
"collection_id": "0m8p5-wqy33",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:YUNjvstb04",
"type": "article",
"title": "Microfabrication of silicon\u2013nitride micromesh bolometric detectors for Planck high frequency instrument",
"author": [
{
"family_name": "Yun",
"given_name": "Minhee",
"clpid": "Yun-Minhee-H"
},
{
"family_name": "Bock",
"given_name": "Jamie",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Holmes",
"given_name": "Warren",
"clpid": "Holmes-W"
},
{
"family_name": "Koch",
"given_name": "Tim",
"clpid": "Koch-T"
},
{
"family_name": "Mulder",
"given_name": "Jerry",
"clpid": "Mulder-J"
},
{
"family_name": "Vasquez",
"given_name": "Richard P.",
"clpid": "Vasquez-R-P"
},
{
"family_name": "Wild",
"given_name": "Larry",
"clpid": "Wild-L"
},
{
"family_name": "Lange",
"given_name": "Andrew",
"clpid": "Lange-A-E"
}
],
"abstract": "The high frequency instrument (HFI) on the National Aeronautics and Space Administration/European Space Agency Planck Surveyor, scheduled for launch in 2007, will map the entire sky in six frequency bands ranging from 100 to 857 GHz to probe cosmic microwave background anisotropy and polarization with angular resolution ranging from 9[prime] to 5[prime]. The HFI focal plane will contain 48 silicon\u2013nitride micromesh bolometers operating from a 100 mK heat sink. Four detectors in each of the six bands will detect unpolarized radiation. An additional four pairs of detectors will provide sensitivity to linear polarization of emissions at 143, 217, and 353 GHz. We have fabricated and developed sensitive Si3N4 micromesh spider-web bolometers for submillimeter observation using microelectromechanical system techniques. The spiderweb architecture in this research provides high infrared absorption with minimal heat capacity and volume.",
"doi": "10.1116/1.1642644",
"issn": "1071-1023",
"publisher": "American Vacuum Society",
"publication": "Journal of Vacuum Science and Technology B",
"publication_date": "2004-01",
"series_number": "1",
"volume": "22",
"issue": "1",
"pages": "220-225"
},
{
"id": "authors:pw47r-bk102",
"collection": "authors",
"collection_id": "pw47r-bk102",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:WOOao03",
"type": "article",
"title": "Predicting the response of a submillimeter bolometer to cosmic rays",
"author": [
{
"family_name": "Woodcraft",
"given_name": "Adam L.",
"clpid": "Woodcraft-A-L"
},
{
"family_name": "Sudiwala",
"given_name": "Rashmi V.",
"clpid": "Sudiwala-R-V"
},
{
"family_name": "Ade",
"given_name": "Peter A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Griffin",
"given_name": "Matthew J.",
"clpid": "Griffin-M-J"
},
{
"family_name": "Wakui",
"given_name": "Elley",
"clpid": "Wakui-Elley"
},
{
"family_name": "Bhatia",
"given_name": "Ravinder S.",
"clpid": "Bhatia-R-S"
},
{
"family_name": "Lange",
"given_name": "Andrew E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Bock",
"given_name": "James J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Turner",
"given_name": "Anthony D.",
"clpid": "Turner-A-D"
},
{
"family_name": "Yun",
"given_name": "Minhee H.",
"clpid": "Yun-Minhee-H"
},
{
"family_name": "Beeman",
"given_name": "Jeffrey W.",
"clpid": "Beeman-J-W"
}
],
"abstract": "Bolometers designed to detect. submillimeter radiation also respond to cosmic, gamma, and x rays. Because detectors cannot be fully shielded from such energy sources, it is necessary to understand the effect of a photon or cosmic-ray particle being absorbed. The resulting signal (known as a glitch) can then be removed from raw data. We present measurements using an Americium-241 gamma radiation source to irradiate a prototype bolometer for the High Frequency Instrument in the Planck Surveyor satellite. Our measurements showed no variation in response depending on where the radiation was absorbed, demonstrating that the bolometer absorber and thermistor thermalize quickly. The bolometer has previously been fully characterized both electrically and optically. We find that using optically measured time constants underestimates the time taken for the detector to recover from a radiation absorption event. However, a full thermal model for the bolometer, with parameters taken from electrical and optical measurements, provides accurate time constants. Slight deviations from the model were seen at high energies; these can be accounted for by use of an extended model.",
"issn": "0003-6935",
"publisher": "Optical Society of America",
"publication": "Applied Optics",
"publication_date": "2003-09-01",
"series_number": "25",
"volume": "42",
"issue": "25",
"pages": "5009-5016"
},
{
"id": "authors:2jqq5-43m96",
"collection": "authors",
"collection_id": "2jqq5-43m96",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200130-080407664",
"type": "article",
"title": "The trispectrum of the cosmic microwave background on subdegree angular scales: an analysis of the BOOMERanG data",
"author": [
{
"family_name": "De Troia",
"given_name": "G.",
"clpid": "De-Troia-G"
},
{
"family_name": "Ade",
"given_name": "P. A. R.",
"orcid": "0000-0002-5127-0401",
"clpid": "Ade-P-A-R"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Bond",
"given_name": "J. R.",
"orcid": "0000-0003-2358-9949",
"clpid": "Bond-J-R"
},
{
"family_name": "Boscaleri",
"given_name": "A.",
"clpid": "Boscaleri-A"
},
{
"family_name": "Contaldi",
"given_name": "C. R.",
"clpid": "Contaldi-C-R"
},
{
"family_name": "Crill",
"given_name": "B. P.",
"orcid": "0000-0002-4650-8518",
"clpid": "Crill-B-P"
},
{
"family_name": "de Bernardis",
"given_name": "P.",
"orcid": "0000-0001-6547-6446",
"clpid": "de-Bernardis-P"
},
{
"family_name": "Ferreira",
"given_name": "P. G.",
"clpid": "Ferreira-P-G"
},
{
"family_name": "Giacometti",
"given_name": "M.",
"clpid": "Giacometti-M"
},
{
"family_name": "Hivon",
"given_name": "E.",
"clpid": "Hivon-E"
},
{
"family_name": "Hristov",
"given_name": "V. V.",
"clpid": "Hristov-V-V"
},
{
"family_name": "Kunz",
"given_name": "M.",
"clpid": "Kunz-M"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Masi",
"given_name": "S.",
"orcid": "0000-0001-5105-1439",
"clpid": "Masi-S"
},
{
"family_name": "Mauskopf",
"given_name": "P. D.",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "Montroy",
"given_name": "T.",
"clpid": "Montroy-T-E"
},
{
"family_name": "Natoli",
"given_name": "P.",
"clpid": "Natoli-P"
},
{
"family_name": "Netterfield",
"given_name": "C. B.",
"clpid": "Netterfield-C-B"
},
{
"family_name": "Pascale",
"given_name": "E.",
"orcid": "0000-0002-3242-8154",
"clpid": "Pascale-E"
},
{
"family_name": "Piacentini",
"given_name": "F.",
"orcid": "0000-0002-5444-9327",
"clpid": "Piacentini-F"
},
{
"family_name": "Polenta",
"given_name": "G.",
"clpid": "Polenta-G"
},
{
"family_name": "Romeo",
"given_name": "G.",
"clpid": "Romeo-G"
},
{
"family_name": "Ruhl",
"given_name": "J. E.",
"clpid": "Ruhl-J-E"
}
],
"abstract": "The trispectrum of the cosmic microwave background can be used to assess the level of non-Gaussianity on cosmological scales. It probes the fourth-order moment, as a function of angular scale, of the probability distribution function of fluctuations and has been shown to be sensitive to primordial non-Gaussianity, secondary anisotropies (such as the Ostriker\u2013Vishniac effect) and systematic effects (such as astrophysical foregrounds). In this paper we develop a formalism for estimating the trispectrum from high-resolution sky maps that incorporates the impact of finite sky coverage. This leads to a series of operations applied to the data set to minimize the effects of contamination due to the Gaussian component and correlations between estimates at different scales. To illustrate the effect of the estimation process, we apply our procedure to the BOOMERanG data set and show that it is consistent with Gaussianity. This work presents the first estimation of the cosmic microwave background trispectrum on subdegree scales.",
"doi": "10.1046/j.1365-8711.2003.06665.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2003-07",
"series_number": "1",
"volume": "343",
"issue": "1",
"pages": "284-292"
},
{
"id": "authors:0c6c7-x3c03",
"collection": "authors",
"collection_id": "0c6c7-x3c03",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170215-134941436",
"type": "article",
"title": "High Spatial Resolution Mid-Infrared Observations of Three Seyfert Galaxies",
"author": [
{
"family_name": "Soifer",
"given_name": "B. T.",
"orcid": "0000-0002-8112-1132",
"clpid": "Soifer-B-T"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Marsh",
"given_name": "K.",
"orcid": "0000-0003-0107-7803",
"clpid": "Marsh-K-A"
},
{
"family_name": "Neugebauer",
"given_name": "G.",
"clpid": "Neugebauer-G"
},
{
"family_name": "Matthews",
"given_name": "K.",
"clpid": "Matthews-Keith-Astronomy"
},
{
"family_name": "Egami",
"given_name": "E.",
"clpid": "Egami-Eichi"
},
{
"family_name": "Armus",
"given_name": "L.",
"orcid": "0000-0003-3498-2973",
"clpid": "Armus-L"
}
],
"abstract": "Images at 12.5 \u03bcm of nuclei of three nearby Seyfert galaxies\u2014NGC 1275, NGC 4151, and NGC 7469\u2014have been obtained with the 10 m Keck Telescope. NGC 7469 is resolved and deconvolution delineates a structure (<0farcs04) \u00d7 0farcs08, or less than 13 \u00d7 26 pc at a position angle of 135\u00b0. From a comparison with structure seen at millimeter wavelengths, this structure is interpreted as a disk aligned with the molecular gas in the central few hundred parsecs of the galaxy. NGC 1275 and NGC 4151 are not resolved; limits on the sizes of these nuclei are 0farcs08 and 0farcs16, corresponding to physical spatial scales of 28 and 10 pc. The lower limits to the brightness temperatures implied by these size limits and the measured flux densities are within ~50 K of the 12\u201325 \u03bcm color temperatures of these systems, as inferred from IRAS observations. The angular size limits are within a factor of 2 of the sizes required to spatially resolve thermal emission from dust heated by a central luminosity source. These sizes preclude significant contributions to the nuclear infrared emission from star-forming regions.",
"doi": "10.1086/375647",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2003-07",
"series_number": "1",
"volume": "126",
"issue": "1",
"pages": "143-152"
},
{
"id": "authors:frkd8-hn452",
"collection": "authors",
"collection_id": "frkd8-hn452",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180207-112040907",
"type": "article",
"title": "Cosmological constraints from Archeops",
"author": [
{
"family_name": "Beno\u00eet",
"given_name": "A.",
"clpid": "Beno\u00eet-A"
},
{
"family_name": "Bhatia",
"given_name": "R. S.",
"clpid": "Bhatia-R-S"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Ganga",
"given_name": "K.",
"clpid": "Ganga-K"
}
],
"abstract": "We analyze the cosmological constraints that Archeops (Beno\u00eet et al. 2003) places on adiabatic cold dark matter models with passive power-law initial fluctuations. Because its angular power spectrum has small bins in \u2113 and large \u2113 coverage down to COBE scales, Archeops provides a precise determination of the first acoustic peak in terms of position at multipole l_(peak) = 220 \u00b1 6, height and width. An analysis of Archeops data in combination with other CMB datasets constrains the baryon content of the Universe, \u03a9_bh^2 = 0.022^(+0.003)_(-0.004), compatible with Big-Bang nucleosynthesis and with a similar accuracy. Using cosmological priors obtained from recent non-CMB data leads to yet tighter constraints on the total density, e.g. \u03a9_(tot) = 1.00^(+0.03)_(-0.02) using the HST determination of the Hubble constant. An excellent absolute calibration consistency is found between Archeops and other CMB experiments, as well as with the previously quoted best fit model. The spectral index n is measured to be 1.04^(+0.10)_(-0.12) when the optical depth to reionization, \u03c4, is allowed to vary as a free parameter, and 0.96^(+0.03)_(-0.04) when \u03c4 is fixed to zero, both in good agreement with inflation.",
"doi": "10.1051/0004-6361:20021722",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy & Astrophysics",
"publication_date": "2003-02-14",
"volume": "399",
"pages": "L25-L30"
},
{
"id": "authors:vw0jk-0vt32",
"collection": "authors",
"collection_id": "vw0jk-0vt32",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20180207-131552158",
"type": "article",
"title": "The cosmic microwave background anisotropy power spectrum\n measured by Archeops",
"author": [
{
"family_name": "Beno\u00eet",
"given_name": "A.",
"clpid": "Beno\u00eet-A"
},
{
"family_name": "Bhatia",
"given_name": "R. S.",
"clpid": "Bhatia-R-S"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Ganga",
"given_name": "K.",
"clpid": "Ganga-K"
}
],
"abstract": "We present a determination by the Archeops experiment of the angular power spectrum of the cosmic microwave background anisotropy in 16 bins over the multipole range \u2113 = 15-350. Archeops was conceived as a precursor of the Planck HFI instrument by using the same optical design and the same technology for the detectors and their cooling. Archeops is a balloon\u2013borne instrument consisting of a 1.5 m aperture diameter telescope and an array of 21 photometers maintained at mK that are operating in 4 frequency bands centered at 143, 217, 353 and 545 GHz. The data were taken during the Arctic night of February 7, 2002 after the instrument was launched by CNES from Esrange base (Sweden). The entire data cover ~30% of the sky. This first analysis was obtained with a small subset of the dataset using the most sensitive photometer in each CMB band (143 and 217 GHz) and 12.6% of the sky at galactic latitudes above 30 degrees where the foreground contamination is measured to be negligible. The large sky coverage and medium resolution (better than 15 arcmin) provide for the first time a high signal-to-noise ratio determination of the power spectrum over angular scales that include both the first acoustic peak and scales probed by COBE/DMR. With a binning of \u2113\u0394 = 7 to 25 the error bars are dominated by sample variance for \u2113 below 200. A companion paper details the cosmological implications.",
"doi": "10.1051/0004-6361:20021850",
"issn": "0004-6361",
"publisher": "EDP Sciences",
"publication": "Astronomy & Astrophysics",
"publication_date": "2003-02-14",
"series_number": "3",
"volume": "399",
"issue": "3",
"pages": "L19-L23"
},
{
"id": "authors:sjd1x-r2p16",
"collection": "authors",
"collection_id": "sjd1x-r2p16",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20111102-141515126",
"type": "article",
"title": "Numerical optimization of integrating cavities for diffraction-limited millimeter-wave bolometer arrays",
"author": [
{
"family_name": "Glenn",
"given_name": "Jason",
"orcid": "0000-0001-7527-2017",
"clpid": "Glenn-J"
},
{
"family_name": "Chattopadhyay",
"given_name": "Goutam",
"orcid": "0000-0001-7942-5025",
"clpid": "Chattopadhyay-G"
},
{
"family_name": "Edgington",
"given_name": "Samantha F.",
"clpid": "Edgington-S-F"
},
{
"family_name": "Lange",
"given_name": "Andrew E.",
"clpid": "Lange-A-E"
},
{
"family_name": "Bock",
"given_name": "James J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Mauskopf",
"given_name": "Philip D.",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "Lee",
"given_name": "Adrian T.",
"clpid": "Lee-Adrian-T"
}
],
"abstract": "Far-infrared to millimeter-wave bolometers designed to make astronomical observations are typically encased in integrating cavities at the termination of feedhorns or Winston cones. This photometer combination maximizes absorption of radiation, enables the absorber area to be minimized, and controls the directivity of absorption, thereby reducing susceptibility to stray light. In the next decade, arrays of hundreds of silicon nitride micromesh bolometers with planar architectures will be used in ground-based, suborbital, and orbital platforms for astronomy. The optimization of integrating cavity designs is required for achieving the highest possible sensitivity for these arrays. We report numerical simulations of the electromagnetic fields in integrating cavities with an infinite plane-parallel geometry formed by a solid reflecting backshort and the back surface of a feedhorn array block. Performance of this architecture for the bolometer array camera (Bolocam) for cosmology at a frequency of 214 GHz is investigated. We explore the sensitivity of absorption efficiency to absorber impedance and backshort location and the magnitude of leakage from cavities. The simulations are compared with experimental data from a room-temperature scale model and with the performance of Bolocam at a temperature of 300 mK. The main results of the simulations for Bolocam-type cavities are that (1) monochromatic absorptions as high as 95% are achievable with <1% cross talk between neighboring cavities, (2) the optimum absorber impedances are 400 \u03a9/sq, but with a broad maximum from ~150 to ~700 \u03a9/sq, and (3) maximum absorption is achieved with absorber diameters \u22651.5\u03bb. Good general agreement between the simulations and the experiments was found.",
"doi": "10.1364/AO.41.000136",
"issn": "0003-6935",
"publisher": "Optical Society of America",
"publication": "Applied Optics",
"publication_date": "2002-01-01",
"series_number": "1",
"volume": "41",
"issue": "1",
"pages": "136-142"
},
{
"id": "authors:nn2m8-cee25",
"collection": "authors",
"collection_id": "nn2m8-cee25",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170208-103123393",
"type": "article",
"title": "High Spatial Resolution Imaging of NGC 1068 in the Mid-Infrared",
"author": [
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Neugebauer",
"given_name": "G.",
"clpid": "Neugebauer-G"
},
{
"family_name": "Matthews",
"given_name": "K.",
"clpid": "Matthews-K"
},
{
"family_name": "Soifer",
"given_name": "B. T.",
"orcid": "0000-0002-8112-1132",
"clpid": "Soifer-B-T"
},
{
"family_name": "Becklin",
"given_name": "E. E.",
"clpid": "Becklin-E-E"
},
{
"family_name": "Ressler",
"given_name": "M.",
"clpid": "Ressler-M-E"
},
{
"family_name": "Marsh",
"given_name": "K.",
"orcid": "0000-0003-0107-7803",
"clpid": "Marsh-K-A"
},
{
"family_name": "Werner",
"given_name": "M. W.",
"clpid": "Werner-M-W"
},
{
"family_name": "Egami",
"given_name": "E.",
"clpid": "Egami-Eichi"
},
{
"family_name": "Blandford",
"given_name": "R.",
"orcid": "0000-0002-1854-5506",
"clpid": "Blandford-R-D"
}
],
"abstract": "Mid-infrared observations of the central source of NGC 1068 have been obtained with a spatial resolution in the deconvolved image of 0.\"1 (~7 pc). The central source is extended by ~1'' in the north-south direction but appears unresolved in the east-west direction over most of its length. About 2/3 of its flux can be ascribed to a core structure that is itself elongated north-south and does not show a distinct unresolved compact source. The source is strongly asymmetric, extending significantly farther to the north than to the south. The morphology of the mid-infrared emission appears similar to that of the radio jet and has features which correlate with the images in [O III]. Its 12.5\u201324.5 \u03bcm color temperature ranges from 215 to 260 K and does not decrease smoothly with distance from the core. Silicate absorption is strongest in the core and to the south and is small in the north. The core, apparently containing 2/3 of the bolometric luminosity of the inner 4'' diameter area, may be explained by a thick, dusty torus near the central active galactic nucleus (AGN) viewed at an angle of ~65\u00b0 to its plane. There are, however, detailed difficulties with existing models, especially the narrow east-west width of the thin extended mid-infrared \"tongue\" to the north of the core. We interpret the tongue as reprocessed visual and ultraviolet radiation that is strongly beamed and that originates in the AGN.",
"doi": "10.1086/316871",
"issn": "0004-6256",
"publisher": "American Astronomical Society",
"publication": "Astronomical Journal",
"publication_date": "2000-12",
"series_number": "6",
"volume": "120",
"issue": "6",
"pages": "2904-2919"
},
{
"id": "authors:f60py-b9y39",
"collection": "authors",
"collection_id": "f60py-b9y39",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BLAmnras00",
"type": "article",
"title": "Millimetre/submillimetre-wave emission-line searches for high-redshift galaxies",
"author": [
{
"family_name": "Blain",
"given_name": "A. W.",
"orcid": "0000-0001-7489-5167",
"clpid": "Blain-A-W"
},
{
"family_name": "Frayer",
"given_name": "D. T.",
"orcid": "0000-0003-1924-1122",
"clpid": "Frayer-D-T"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Scoville",
"given_name": "N. Z.",
"orcid": "0000-0002-0438-3323",
"clpid": "Scoville-N-Z"
}
],
"abstract": "The redshifted spectral line radiation emitted from both atomic fine-structure and molecular rotational transitions in the interstellar medium (ISM) of high-redshift galaxies can be detected in the centimetre, millimetre and submillimetre wavebands. Here we predict the counts of galaxies detectable in an array of molecular and atomic lines. This calculation requires a reasonable knowledge of both the surface density of these galaxies on the sky, and the physical conditions in their ISM. The surface density is constrained using the results of submillimetre-wave continuum surveys. Follow-up OVRO Millimeter Array observations of two of the galaxies detected in the dust continuum have provided direct measurements of CO rotational line emission at redshifts of 2.56 and 2.81. Based on these direct high-redshift observations and on models of the ISM that are constrained by observations of low-redshift ultraluminous infrared galaxies, we predict the surface density of line-emitting galaxies as a function of line flux density and observing frequency. We incorporate the sensitivities and mapping speeds of existing and future millimetre/submillimetre-wave telescopes and spectrographs, and so assess the prospects for blank-field surveys to detect this line emission from gas-rich high-redshift galaxies.",
"doi": "10.1046/j.1365-8711.2000.03287.x",
"issn": "0035-8711",
"publisher": "Royal Astronomical Society",
"publication": "Monthly Notices of the Royal Astronomical Society",
"publication_date": "2000-04-11",
"series_number": "3",
"volume": "313",
"issue": "3",
"pages": "559-570"
},
{
"id": "authors:0y9df-nab56",
"collection": "authors",
"collection_id": "0y9df-nab56",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20120130-075759922",
"type": "article",
"title": "Composite infrared bolometers with Si_3N_4 micromesh absorbers",
"author": [
{
"family_name": "Mauskopf",
"given_name": "P. D.",
"orcid": "0000-0001-6397-5516",
"clpid": "Mauskopf-P-D"
},
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Del Castillo",
"given_name": "H.",
"clpid": "Del-Castillo-H"
},
{
"family_name": "Holzapfel",
"given_name": "W. L.",
"clpid": "Holzapfel-W-L"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
}
],
"abstract": "We report the design and performance of 300-mK composite bolometers that use micromesh absorbers and support structures patterned from thin films of low-stress silicon nitride. The small geometrical filling factor of the micromesh absorber provides 20\u00d7 reduction in heat capacity and cosmic ray cross section relative to a solid absorber with no loss in IR-absorption efficiency. The support structure is mechanically robust and has a thermal conductance, G < 2 \u00d7 10^(\u221211) W/K, which is four times smaller than previously achieved at 300 mK. The temperature rise of the bolometer is measured with a neutron transmutation doped germanium thermistor attached to the absorbing mesh. The dispersion in electrical and thermal parameters of a sample of 12 bolometers optimized for the Sunyaev\u2013Zel'dovich Infrared Experiment is \u00b17% in R (T), \u00b15% in optical efficiency, and \u00b14% in G.",
"doi": "10.1364/AO.36.000765",
"issn": "0003-6935",
"publisher": "Optical Society of America",
"publication": "Applied Optics",
"publication_date": "1997-02-01",
"series_number": "4",
"volume": "36",
"issue": "4",
"pages": "765-771"
},
{
"id": "authors:6e2ka-zrs61",
"collection": "authors",
"collection_id": "6e2ka-zrs61",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BOCao95a",
"type": "article",
"title": "Performance of a low-pass filter for far-infrared wavelengths",
"author": [
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
}
],
"abstract": "We describe a low-pass filter that provides high in-band transmittance and excellent rejection at nu > 100 cm^-1. The transmittance of the filter components was measured at liquid-helium temperatures from 10 to 10,000 cm^-1. The total transmittance is > 50% for nu < 50 cm^-1 and is calculated to be < 10^-9 for nu > 300 cm^-1. The filter was successfully used in a liquid-helium-cooled, rocketborne, far-infrared absolute photometer.",
"issn": "0003-6935",
"publisher": "Optical Society of America",
"publication": "Applied Optics",
"publication_date": "1995-11-01",
"series_number": "31",
"volume": "34",
"issue": "31",
"pages": "7254-7257"
},
{
"id": "authors:ajjdf-h7q06",
"collection": "authors",
"collection_id": "ajjdf-h7q06",
"cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:BOCao95b",
"type": "article",
"title": "Emissivity measurements of reflective surfaces at near-millimeter wavelengths",
"author": [
{
"family_name": "Bock",
"given_name": "J. J.",
"orcid": "0000-0002-5710-5212",
"clpid": "Bock-J-J"
},
{
"family_name": "Parikh",
"given_name": "M. K.",
"clpid": "Parikh-M-K"
},
{
"family_name": "Fischer",
"given_name": "M. L.",
"orcid": "0000-0001-7956-2361",
"clpid": "Fischer-M-L"
},
{
"family_name": "Lange",
"given_name": "A. E.",
"clpid": "Lange-A-E"
}
],
"abstract": "We have developed an instrument for directly measuring the emissivity of reflective surfaces at near-millimeter wavelengths. The thermal emission of a test sample is compared with that of a reference surface, allowing the emissivity of the sample to be determined without heating. The emissivity of the reference surface is determined by one's heating the reference surface and measuring the increase in emission. The instrument has an absolute accuracy of \u0394e = 5 x 10^-4 and can reproducibly measure a difference in emissivity as small as \u0394e = 10^-4 between flat reflective samples. We have used the instrument to measure the emissivity of metal films evaporated on glass and carbon fiber-reinforced plastic composite surfaces. We measure an emissivity of (2.15 \u00b1 0.4) x 10^-3 for gold evaporated on glass and (2.65 \u00b1 0.5) x 10^-3 for aluminum evaporated on carbon fiber-reinforced plastic composite.",
"issn": "0003-6935",
"publisher": "Optical Society of America",
"publication": "Applied Optics",
"publication_date": "1995-08-01",
"series_number": "22",
"volume": "34",
"issue": "22",
"pages": "4812-4816"
}
]