[ { "id": "authors:kbgq2-v7685", "collection": "authors", "collection_id": "kbgq2-v7685", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181211-091513662", "type": "book_section", "title": "TW Hydrae: multi-wavelength interferometry of a transition disk", "book_title": "Exploring the Formation and Evolution of Planetary Systems", "author": [ { "family_name": "Menu", "given_name": "J.", "clpid": "Menu-J" }, { "family_name": "van Boekel", "given_name": "R.", "clpid": "van-Boekel-R" }, { "family_name": "Henning", "given_name": "T.", "clpid": "Henning-T" }, { "family_name": "Benisty", "given_name": "M.", "orcid": "0000-0002-7695-7605", "clpid": "Benisty-M" }, { "family_name": "Chandler", "given_name": "C. J.", "clpid": "Chandler-C-J" }, { "family_name": "Linz", "given_name": "H.", "clpid": "Linz-H" }, { "family_name": "Waelkens", "given_name": "C.", "clpid": "Waelkens-C" }, { "family_name": "Andrews", "given_name": "S. M.", "orcid": "0000-0003-2253-2270", "clpid": "Andrews-S-M" }, { "family_name": "Calvet", "given_name": "N.", "orcid": "0000-0002-3950-5386", "clpid": "Calvet-Nuria" }, { "family_name": "Carpenter", "given_name": "J. M.", "orcid": "0000-0003-2251-0602", "clpid": "Carpenter-J-M" }, { "family_name": "Corder", "given_name": "S. A.", "clpid": "Corder-S" }, { "family_name": "Deller", "given_name": "A. T.", "orcid": "0000-0001-9434-3837", "clpid": "Deller-A-T" }, { "family_name": "Dullemond", "given_name": "C. P.", "clpid": "Dullemond-C-P" }, { "family_name": "Greaves", "given_name": "J. S.", "orcid": "0000-0002-3133-413X", "clpid": "Greaves-J-S" }, { "family_name": "Harris", "given_name": "R. J.", "clpid": "Harris-R-J" }, { "family_name": "Isella", "given_name": "A.", "orcid": "0000-0001-8061-2207", "clpid": "Isella-A" }, { "family_name": "Kwon", "given_name": "W.", "clpid": "Kwon-Woojin" }, { "family_name": "Lazio", "given_name": "J.", "clpid": "Lazio-J" }, { "family_name": "Mundy", "given_name": "L. G.", "clpid": "Mundy-L-G" }, { "family_name": "P\u00e9rez", "given_name": "L. M.", "orcid": "0000-0002-1199-9564", "clpid": "P\u00e9rez-L-M" }, { "family_name": "Ricci", "given_name": "L.", "clpid": "Ricci-L" }, { "family_name": "Sargent", "given_name": "A. I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Storm", "given_name": "S.", "orcid": "0000-0001-9401-1357", "clpid": "Storm-S" }, { "family_name": "Testi", "given_name": "L.", "orcid": "0000-0003-1859-3070", "clpid": "Testi-L" }, { "family_name": "Wilner", "given_name": "D. J.", "orcid": "0000-0003-1526-7587", "clpid": "Wilner-D-J" } ], "contributor": [ { "family_name": "Booth", "given_name": "Mark", "clpid": "Booth-M" }, { "family_name": "Matthews", "given_name": "Brenda C.", "clpid": "Matthews-B-C" }, { "family_name": "Graham", "given_name": "James R.", "clpid": "Graham-J-R" } ], "abstract": "For over a decade, the structure of the inner \"hole\" in the transition disk around TW Hydrae has been a subject of debate. To probe the innermost regions of the protoplanetary disk, observations at the highest possible spatial resolution are required. We present new interferometric data of TW Hya from near-infrared to millimeter wavelengths. We confront existing models of the disk structure with the complete data set and develop a new, detailed radiative-transfer model. This model is characterized by: 1) a spatial separation of the largest grains from the small disk grains; and 2) a smooth inner rim structure, rather than a sharp disk edge.", "doi": "10.1017/s1743921313008016", "isbn": "9781107045200", "publisher": "Cambridge University Press", "place_of_publication": "Cambridge", "publication_date": "2013-06", "pages": "104-108" }, { "id": "authors:3bhr4-hqy53", "collection": "authors", "collection_id": "3bhr4-hqy53", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181121-105912598", "type": "book_section", "title": "Proto-planetary disks with CARMA: sub-arsecond observations at millimeter wavelengths", "book_title": "XXVII IAU General Assembly", "author": [ { "family_name": "Andrea", "given_name": "Isella", "clpid": "Andrea-I" }, { "family_name": "Carpenter", "given_name": "John M.", "orcid": "0000-0003-2251-0602", "clpid": "Carpenter-J-M" }, { "family_name": "P\u00e9rez", "given_name": "Laura", "orcid": "0000-0002-1199-9564", "clpid": "P\u00e9rez-L-M" }, { "family_name": "Sargent", "given_name": "Anneila I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" } ], "contributor": [ { "family_name": "Corbett", "given_name": "Ian F.", "clpid": "Corbett-I-F" } ], "abstract": "Using the Combined Array for Research in Millimeter-wave Astronomy (CARMA) we observed several proto-planetary disks in the dust continuum emission at 1.3 and 2.8 mm (Isella et al. 2009a, 2009b). The observations have angular resolution between 0.15 and 0.7 arcsecond, corresponding to spatial scales spanning from about the orbit of Saturn up to about the orbital radius of Pluto. The observed disks are characterized by a variety of radial profiles for the dust density. We observe inner disk clearing as well as smooth density profiles, suggesting that disks may form, or evolve, in different ways. Despite that, we find that the characteristic disk radius is correlated with the stellar age increasing from 20 AU to 100 AU over about 5 Myr. Interpreting our results in terms of the temporal evolution of a viscous \u03b1-disk, we estimate that (i) at the beginning of the disk evolution about 60% of the circumstellar material was located inside radii of 25-40 AU, (ii) that disks formed with masses from 0.05 to 0.4 solar masses and (iii) that the viscous timescale at the disk initial radius is about 0.1-0.3 Myr. Viscous disk models tightly link the surface density \u03a3(R) with the radial profile of the disk viscosity \u03bd(R)\u221d R\u03b3. We find values of \u03b3 ranging from -0.8 to 0.8, suggesting that the viscosity dependence on the orbital radius can be very different in the observed disks. We demonstrate that the similarity solution for the surface density for \u03b3 < 0 can explain the properties of some \"transitional\" disks without requiring discontinuities in the disk surface density. In the case of LkCa 15, a smooth distribution of material from few stellar radii to about 240 AU can produce both the observed SED and the spatially resolved continuum emission at millimeter wavelengths. For two sources, RY Tau and DG Tau, we observed the dust emission with a resolution as high as 0.15 arcsecond, which corresponds to a spatial scale of 20 AU at the distance of the two stars. The achieved angular resolution is a factor 2 higher than any existing observation of circumstellar disks at the same wavelengths and enable us to investigate the disk structure with unprecedent details. In particular, we present a first attempt to derive the radial profile of the slope of the dust opacity \u03b2. We find mean values of \u03b2 of 0.5 and 0.7 for DG Tau and RY Tau respectively and we exclude that \u03b2 may vary by more than \u00b10.4 between 20-70 AU. This implies that the circumstellar dust has a maximum grain size between 10 \u03bcm and few centimeters.", "doi": "10.1017/S1743921310011270", "isbn": "9781107005334", "publisher": "Cambridge University Press", "place_of_publication": "Cambridge", "publication_date": "2009-11", "pages": "738" }, { "id": "authors:xmv50-yve92", "collection": "authors", "collection_id": "xmv50-yve92", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20100722-073942887", "type": "book_section", "title": "Preliminary physical orbit of the HD 98800 B system", "book_title": "The power of optical/IR interferometry : recent scientfic results and 2nd generation instrumentation", "author": [ { "family_name": "Boden", "given_name": "Andy", "clpid": "Boden-A" }, { "family_name": "Sargent", "given_name": "Anneila", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Akeson", "given_name": "Rachel", "orcid": "0000-0001-9674-1564", "clpid": "Akeson-R-L" }, { "family_name": "Carpenter", "given_name": "John", "clpid": "Carpenter-J" } ], "abstract": "As a part of a larger program to measure physical properties of PMS\nbinary systems, we have observed the PMS quadruple system HD 98800 (aka TW\nHya 4A) with the Keck Interferometer (KI), and resolved the two separate spectroscopic\nbinary components of the system. In particular we have observed the HD\n98800 North (B) binary component on multiple epochs, and integrating our data\nwith the double-lined spectroscopic orbit from Torres et al [15] has allowed us to estimate\na physical orbit for the B system. This orbit in turn yields relatively accurate\n(8%) mass estimates of the component stars, and an independent system distance\nand component luminosity estimates. Comparisons between the estimated physical\nparameters for the low-mass HD 98800 B components with mass-luminosity models\nof PMS stars, and implications for the age of HD 98800 are discussed.", "doi": "10.1007/978-3-540-74256-2_34", "isbn": "978-3-540-74253-1", "publisher": "Springer", "place_of_publication": "Berlin", "publication_date": "2007-10-12", "pages": "281-285" }, { "id": "authors:7j3n0-5y220", "collection": "authors", "collection_id": "7j3n0-5y220", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20110304-110358706", "type": "book_section", "title": "A complete 1.1mm survey of Perseus with Bolocam", "book_title": "Spitzer Space Telescope: New Views of the Cosmos", "author": [ { "family_name": "Enoch", "given_name": "Melissa L.", "clpid": "Enoch-M-L" }, { "family_name": "Sargent", "given_name": "Anneila I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Golwala", "given_name": "Sunil", "orcid": "0000-0002-1098-7174", "clpid": "Golwala-S-R" }, { "family_name": "Evans", "given_name": "Neal J., II", "orcid": "0000-0001-5175-1777", "clpid": "Evans-N-J-II" }, { "family_name": "Young", "given_name": "Kaisa", "clpid": "Young-K-E" }, { "family_name": "Glenn", "given_name": "Jason", "orcid": "0000-0001-7527-2017", "clpid": "Glenn-J" }, { "literal": "c2d Spitzer Legacy Team" }, { "literal": "Bolocam Team" } ], "contributor": [ { "family_name": "Armus", "given_name": "L.", "clpid": "Armus-L" }, { "family_name": "Reach", "given_name": "W. T.", "clpid": "Reach-W-T" } ], "abstract": "We have completed a 7.5 square degree \u03bb=1.1mm map of Perseus\nusing Bolocam. Our map is the largest unbiased survey of Perseus at millimeter wavelengths to date, and covers the same area as the c2d Spitzer IRAC and MIPS maps of Perseus. We find that that the mass function shape is similar to that seen in other clouds and to the local IMF. Despite the large area surveyed, few new sources are found outside the known cluster regions.", "isbn": "978-1-583812-25-9", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "2006", "pages": "137-138" }, { "id": "authors:trpfj-gqa16", "collection": "authors", "collection_id": "trpfj-gqa16", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181207-125031394", "type": "book_section", "title": "Gas evolution in protoplanetary disks", "book_title": "Planetary Systems in the Universe \u2013 Observation, Formation and Evolution", "author": [ { "family_name": "Thi", "given_name": "W. F.", "clpid": "Thi-W-F" }, { "family_name": "van Dishoeck", "given_name": "E. F.", "orcid": "0000-0001-7591-1907", "clpid": "van-Dishoeck-E-F" }, { "family_name": "van Zadelhoff", "given_name": "G. J.", "clpid": "van-Zadelhoff-G-J" }, { "family_name": "Blake", "given_name": "G. A.", "orcid": "0000-0003-0787-1610", "clpid": "Blake-G-A" }, { "family_name": "Mannings", "given_name": "V.", "clpid": "Mannings-V-G" }, { "family_name": "Sargent", "given_name": "A. I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Horn", "given_name": "J.", "clpid": "Horn-J" }, { "family_name": "Becklin", "given_name": "E. E.", "clpid": "Becklin-E-E" }, { "family_name": "van den Ancker", "given_name": "M. E.", "clpid": "van-den-Ancker-M-E" }, { "family_name": "Natta", "given_name": "A.", "clpid": "Natta-A" } ], "abstract": "We present the results of a study of the evolution of the gas and dust in disks around T Tauri, Herbig Ae and Vega-like stars. We observed the two lowest rotational lines of H2 with the ISO-SWS as well as ^(12)CO 3\u20132 and ^(13)CO 3\u20132 with the JCMT, and CO 6\u20135 with the CSO. The H_2 lines trace the warm (\u223d 100 K) inner region whereas the CO lines probe the colder outer disks. Substantial amounts of H_2 have been detected toward T Tauri and Herbig Ae stars, and, surprisingly, also around three Vega-like objects (49 Cet, HD 135344 and \u03b2 Pictoris). In contrast with previous conclusions derived from CO data, a significant mass of warm gas is found to persist up to ages of several tens of Myrs, suggesting that slow formation of gas-rich giant planets is possible.", "doi": "10.1017/s0074180900218317", "isbn": "9781583811764", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "2004", "pages": "378-380" }, { "id": "authors:m2rvc-9ey11", "collection": "authors", "collection_id": "m2rvc-9ey11", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181116-111527568", "type": "book_section", "title": "Techniques of mm/sub-mm Interferometry in Star Formation", "book_title": "Star Formation at High Angular Resolution", "author": [ { "family_name": "Sargent", "given_name": "Anneila I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" } ], "contributor": [ { "family_name": "Burton", "given_name": "Michael G.", "clpid": "Burton-M-G" }, { "family_name": "Jayawardhana", "given_name": "Ray", "clpid": "Jayawardhana-R" }, { "family_name": "Bourke", "given_name": "Tyler L.", "clpid": "Bourke-T-L" } ], "abstract": "Since the earliest stages of star formation occur deep in clouds of gas and dust, they are hidden from optical view. Nevertheless, infrared and millimeter wavelength observations over the last twenty years have enabled increasingly detailed studies of the processes involved in stellar birth. High resolution, aperture synthesis imaging of the millimeter-wave radiation from dust and molecular gas in star-forming clouds has proven particularly effective. On the other hand, there can be pitfalls to be avoided in the use of mm/sub-mm interferometry techniques. Here, we consider what has been learned from currently-operating mm interferometers and the potential of the next generation of arrays.", "doi": "10.1017/S0074180900241417", "isbn": "9781583811610", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "2004", "pages": "19-28" }, { "id": "authors:8k98a-gfy47", "collection": "authors", "collection_id": "8k98a-gfy47", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190115-093812254", "type": "book_section", "title": "Multi-mission operations with the Interferometry Science Center", "book_title": "Observatory Operations to Optimize Scientific Return III", "author": [ { "family_name": "Boden", "given_name": "A. F.", "clpid": "Boden-A-F" }, { "family_name": "Akeson", "given_name": "R. L.", "orcid": "0000-0001-9674-1564", "clpid": "Akeson-R-L" }, { "family_name": "Dehghani", "given_name": "N.", "clpid": "Dehghani-N" }, { "family_name": "Jones", "given_name": "J.", "clpid": "Jones-Jeff" }, { "family_name": "Rengarajain", "given_name": "K.", "clpid": "Rengarajain-K" }, { "family_name": "Sargent", "given_name": "A. I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Sun", "given_name": "Q.", "clpid": "Sun-Quentin" } ], "contributor": [ { "family_name": "Quinn", "given_name": "Peter J.", "clpid": "Quinn-P-J" } ], "abstract": "The Interferometry Science Center (ISC) at the California Institute of Technology (Caltech) is chartered with providing science operations, data analysis support, and data archiving support for the suite of interferometry projects within the NASA Origins theme. Beginning with the Science Operations System (SOS) for the Keck Interferometer (KI), the ISC will design, implement, and operate a multi-mission facility to provide operations and support functions for NASA Origins interferometers and the scientists and engineers that use them. Future Origins interferometry projects such as the Space Interferometry Mission (SIM) will further use and extend the functionality of the ISC's multi-mission base. In this talk I will introduce the functional elements in the KI SOS; describe the common SOS core elements that KI and SIM will share; and provide prospective users of these facilities an introduction to user support model that the ISC is implementing.", "doi": "10.1117/12.460753", "isbn": "9780819446237", "publisher": "Society of Photo-optical Instrumentation Engineers (SPIE)", "place_of_publication": "Bellingham, WA", "publication_date": "2002-01-02", "pages": "164-171" }, { "id": "authors:xxgf0-g4r06", "collection": "authors", "collection_id": "xxgf0-g4r06", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190506-091500837", "type": "book_section", "title": "A Close View on the Protoplanetary Disk in the Bok Globule CB 26", "book_title": "The Origins of Stars and Planets: The VLT View", "author": [ { "family_name": "Launhardt", "given_name": "R.", "clpid": "Launhardt-R" }, { "family_name": "Stecklum", "given_name": "B.", "clpid": "Stecklum-B" }, { "family_name": "Sargent", "given_name": "A. I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" } ], "contributor": [ { "family_name": "Alves", "given_name": "Jo\u00e3o F.", "clpid": "Alves-J-F" }, { "family_name": "McCaughrean", "given_name": "Mark J.", "clpid": "McCaughrean-M-J" } ], "abstract": "We present new sub-arcsecond-resolution near-infrared polarimetric imaging and millimetre interferometry data on the circumstellar disk system in the Bok globule CB26. The data imply the presence of a M \u2265 0.01 M\u2299 edge-on-seen disk of > 400 AU in diameter, being in Keplerian rotation around a young ~0.35 M\u2299 star. The mm dust emission from the inner 200 AU is highly optically thick, but the outer parts are optically thin and made of small dust grains. Planetesimal growth in the inner disk could neither be confirmed nor excluded. We argue that the CB 26 disk is a very young protoplanetary disk and show that it is comparable to the early solar system.", "doi": "10.1007/978-3-662-40277-1_41", "isbn": "978-3-662-39255-3", "publisher": "Springer", "place_of_publication": "Berlin", "publication_date": "2002", "pages": "319-324" }, { "id": "authors:mhqc2-1wj81", "collection": "authors", "collection_id": "mhqc2-1wj81", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20121002-151349410", "type": "book_section", "title": "H_2 Emission From Disks Around Herbig Ae and T Tauri Stars", "book_title": "The Universe as Seen by ISO", "author": [ { "family_name": "Thi", "given_name": "W. F.", "clpid": "Thi-W-F" }, { "family_name": "van Dishoeck", "given_name": "E. F.", "orcid": "0000-0001-7591-1907", "clpid": "van-Dishoeck-E-F" }, { "family_name": "Blake", "given_name": "G. A.", "orcid": "0000-0003-0787-1610", "clpid": "Blake-G-A" }, { "family_name": "van Zadelhoff", "given_name": "G. J.", "clpid": "van-Zadelhoff-G-J" }, { "family_name": "Hogerheijde", "given_name": "M. R.", "clpid": "Hogerheijde-M-R" }, { "family_name": "Mannings", "given_name": "V.", "clpid": "Mannings-V" }, { "family_name": "Sargent", "given_name": "A. I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Becklin", "given_name": "E. E.", "clpid": "Becklin-E-E" }, { "family_name": "Horn", "given_name": "J.", "clpid": "Horn-J" }, { "family_name": "Zuckerman", "given_name": "B.", "clpid": "Zuckerman-B" }, { "family_name": "Koerner", "given_name": "D.", "clpid": "Koerner-D-W" }, { "family_name": "Mundy", "given_name": "L. G.", "clpid": "Mundy-L-G" }, { "family_name": "Waters", "given_name": "L. B. F. M.", "clpid": "Waters-L-B-F-M" }, { "family_name": "Wesselius", "given_name": "P. R.", "clpid": "Wesselius-P-R" }, { "family_name": "van den Ancker", "given_name": "M. E.", "clpid": "van-den-Ancker-M-E" }, { "family_name": "Natta", "given_name": "A.", "clpid": "Natta-A" }, { "family_name": "Waelkens", "given_name": "C.", "clpid": "Waelkens-C" }, { "family_name": "Malfait", "given_name": "K.", "clpid": "Malfait-K" } ], "contributor": [ { "family_name": "Cox", "given_name": "P.", "clpid": "Cox-Pierre" }, { "family_name": "Kessler", "given_name": "M. F.", "clpid": "Kessler-M-F" } ], "abstract": "We present the initial results of a deep ISO-SWS survey\nfor the low J pure rotational emission lines of H2\ntoward a number of Herbig Ae and T Tauri stars.\nThe objects are selected to be as isolated as possible\nfrom molecular clouds, with a spectral energy distribution\ncharacteristic of a circumstellar disk. For most\nof them the presence of a disk has been established\ndirectly by millimeter interferometry. The S (1) line is\ndetected in most sources with a peak flux of 0.3-1 Jy.\nThe S(0) line is definitely seen in 2 objects: GG Tau\nand HD 163296. The observations suggest the presence\nof \"warm\" gas at T_(kin) \u2248 100 K with a mass of a\nfew % of the total gas+ dust mass, derived assuming\na gas-to-dust ratio of 100:1. The S(1) peak flux does\nnot show a strong correlation with spectral type of\nthe central star or continuum flux at 1.3 millimeter.\nPossible origins for the warm gas seen in H_2 are discussed,\nand comparisons with model calculations are\nmade.", "isbn": "9789290927082", "publisher": "European Space Agency", "place_of_publication": "Noordwijk, Netherlands", "publication_date": "1999-03", "pages": "529-532" }, { "id": "authors:9v99g-b6b64", "collection": "authors", "collection_id": "9v99g-b6b64", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20190605-160239913", "type": "book_section", "title": "Dramatic Changes in Molecular Cloud Properties Across the Arp 299 Merger", "book_title": "Galaxy Interactions at Low and High Redshift", "author": [ { "family_name": "Aalto", "given_name": "S.", "orcid": "0000-0002-5828-7660", "clpid": "Aalto-Susanne" }, { "family_name": "Radford", "given_name": "S. J. E.", "clpid": "Radford-S-J-E" }, { "family_name": "Scoville", "given_name": "N. Z.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" }, { "family_name": "Sargent", "given_name": "A. I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" } ], "editor": [ { "family_name": "Barnes", "given_name": "J. E.", "clpid": "Barnes-J-E" }, { "family_name": "Sanders", "given_name": "D. B.", "clpid": "Sanders-D-B" } ], "abstract": "Arp 299 is an IR-luminous (L_(IR) \u2248 8 x 10^(11) L_\u2a00) merger system of two galaxies, IC 694 and NGC 3690, at a distance of 40 Mpc. Its proximity and richness in molecular gas make it suitable for studying the effects of gravitational interactions and starburst activity on molecular cloud distributions, dynamics, and physical conditions. Previous low resolution observations (10 \u2013 30\u2033) indicated that the CO/^(13)CO 1\u20130 intensity ratio is unusually high, > 20, suggesting an unusual population of molecular clouds (Aalto et al. 1991; Casoli et al. 1992).", "doi": "10.1007/978-94-011-4665-4_56", "isbn": "978-0-7923-5833-6", "publisher": "Springer", "place_of_publication": "Dordrecht", "publication_date": "1999", "pages": "231-234" }, { "id": "authors:pqn9q-tyy40", "collection": "authors", "collection_id": "pqn9q-tyy40", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201201-121035964", "type": "book_section", "title": "Protostellar and Protoplanetary Disks", "book_title": "CO: Twenty-Five Years of Millimeter-Wave Spectroscopy", "author": [ { "family_name": "Sargent", "given_name": "Anneila I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" } ], "contributor": [ { "family_name": "Latter", "given_name": "William B.", "clpid": "Latter-W-B" }, { "family_name": "Radford", "given_name": "Simon J. E.", "clpid": "Radford-S-J-E" }, { "family_name": "Jewell", "given_name": "Philip R.", "clpid": "Jewell-P-R" }, { "family_name": "Mangum", "given_name": "Jeffrey G.", "clpid": "Mangum-J-G" }, { "family_name": "Bally", "given_name": "John", "clpid": "Bally-J" } ], "abstract": "It is barely a decade since the first molecular line images of disks around embedded and pre-main sequence stars were published (Beckwith et al., 1986; Mundy et al., 1986; Sargent & Beckwith 1987). In the intervening years there has been steady progress in detecting and analyzing these disks, which are an expected by-product of the star formation process cf. Shu et al., 1987; Shu et al., 1993), and there is now a veritable flood of new and intriguing results as millimeter-wave instrumentation improves (cf. Sargent & Welch 1993).", "doi": "10.1007/978-94-011-5414-7_27", "isbn": "978-0-7923-4284-7", "publisher": "Springer", "place_of_publication": "Dordrecht", "publication_date": "1997", "pages": "151-158" }, { "id": "authors:g5ahj-82b15", "collection": "authors", "collection_id": "g5ahj-82b15", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210125-153052077", "type": "book_section", "title": "Disk observations", "book_title": "Disks and Outflows Around Young Stars", "author": [ { "family_name": "Sargent", "given_name": "Anneila I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" } ], "contributor": [ { "family_name": "Beckwith", "given_name": "Steven V. W.", "clpid": "Beckwith-Steven-V-W" }, { "family_name": "Staude", "given_name": "Jakob", "clpid": "Staude-Jakob" }, { "family_name": "Quetz", "given_name": "Axel", "clpid": "Quetz-Axel" }, { "family_name": "Natta", "given_name": "Antonella", "clpid": "Natta-Antonella" } ], "abstract": "A wide variety of observations suggest that solar mass stars are surrounded by disks of gas and dust for much of their pre-main sequence lifetimes and even beyond. Here, techniques by which the small-scale circumstellar material can be detected are described and evidence for disks is briefly reviewed. Because of the general similarity between the disks around solar-mass stars and the nebula that surrounded the sun as the planets formed, disk properties may have strong bearing on our understanding of solar system evolution. Questions which must be addressed include: How frequently are disks found, and does the fraction vary with environment? What effect do companion stars have? How do disks evolve? Are low infrared fluxes necessarily indicative of disk clearing? Is there evidence of chemical evolution? How long do the disks persist? Are dissipation time-scales different for the gas and dust components? Observations addressing such problems will be summarized and discussed.", "doi": "10.1007/BFb0102623", "isbn": "978-3-540-61389-3", "publisher": "Springer", "place_of_publication": "Berlin", "publication_date": "1996", "pages": "1-23" }, { "id": "authors:2y1r2-82q72", "collection": "authors", "collection_id": "2y1r2-82q72", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181121-083143567", "type": "book_section", "title": "The Owens Valley Millimeter Array", "book_title": "Astronomy with Millimeter and Submillimeter Wave Interferometry", "author": [ { "family_name": "Scoville", "given_name": "N.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" }, { "family_name": "Carlstrom", "given_name": "J.", "orcid": "0000-0002-2044-7665", "clpid": "Carlstrom-J-E" }, { "family_name": "Padin", "given_name": "S.", "clpid": "Padin-S" }, { "family_name": "Sargent", "given_name": "A.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Scott", "given_name": "S.", "clpid": "Scott-S" }, { "family_name": "Woody", "given_name": "D.", "clpid": "Woody-D-P" } ], "contributor": [ { "family_name": "Ishiguro", "given_name": "M.", "clpid": "Ishiguro-M" }, { "family_name": "Welch", "given_name": "Wm. J.", "clpid": "Welch-Wm-J" } ], "abstract": "The present status and projected two year developments for the Owens Valley Millimeter Array are described and a brief summary of the astronomical research is presented.", "doi": "10.1017/S0252921100019023", "isbn": "9780937707784", "publisher": "Astronomical Society of the Pacific", "place_of_publication": "San Francisco, CA", "publication_date": "1994", "pages": "10-17" }, { "id": "authors:4tc2g-1my70", "collection": "authors", "collection_id": "4tc2g-1my70", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181211-093131094", "type": "book_section", "title": "Arp 299 - Two Interacting Galaxies", "book_title": "Dynamics of Galaxies and their Molecular Cloud Distributions", "author": [ { "family_name": "Sargent", "given_name": "A. I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Scoville", "given_name": "N. Z.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" }, { "family_name": "Sanders", "given_name": "D. B.", "orcid": "0000-0002-1233-9998", "clpid": "Sanders-D-B" } ], "contributor": [ { "family_name": "Combes", "given_name": "F.", "clpid": "Combes-F" }, { "family_name": "Casoli", "given_name": "Fabienne", "clpid": "Casoli-F" } ], "abstract": "Arp 299 (Mrk 171), is an interacting system at 42 Mpc, comprising the galaxies IC 694 and NGC 3690. Interferometric CO maps at 6\u2033 resolution (Sargent et al. 1987) showed compact molecular condensations at the nucleus of IC694 and in the overlap region of the galaxy disks [positions A and C \u2013 C in the terminology of Gehrz, Sramek, and Weedman (1983)].", "doi": "10.1017/S0074180900244768", "isbn": "9780792310969", "publisher": "Kluwer", "place_of_publication": "Dordrecht", "publication_date": "1991", "pages": "430" }, { "id": "authors:fba02-bnp76", "collection": "authors", "collection_id": "fba02-bnp76", "cite_using_url": "https://authors.library.caltech.edu/records/fba02-bnp76", "type": "book_section", "title": "Results from 1.4 Millimeter Wavelength Interferometry at the Owens Valley", "book_title": "Submillimetre Astronomy", "author": [ { "family_name": "Mundy", "given_name": "L. G.", "orcid": "0000-0002-8876-0690" }, { "family_name": "Sargent", "given_name": "A. I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Scoville", "given_name": "N. Z.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" }, { "family_name": "Padin", "given_name": "S.", "orcid": "0009-0001-9993-4393", "clpid": "Padin-Stephen" }, { "family_name": "Woody", "given_name": "D. P.", "orcid": "0000-0003-1734-2472", "clpid": "Woody-D-P" } ], "abstract": "
\n
\n

This paper summarizes the first interferometric results in the 1.4 mm band from the Owens Valley Radio Observatory (OVRO) Millimeter Wave Array. Relative to 2.7 mm, observations of thermal dust and molecular emission at 1.4 mm benefit from increased emissivity and brightness temperature sensitivity. For optically thin emir ion in the Rayleigh-Jeans limit, dust emission increases as λ3 to λ-4 assuming λ-1 to λ-2 wavelength dependence for the dust emissivity, while molecular emission increases faster than λ-2 due to the Planck function and the larger statistical weights of higher levels. In the optically thick limit, both increase as λ-2. This λ-2 advantage can also be expressed in terms of the brightness temperature sensitivity; for a given beam size, the rms brightness temperature corresponding to a specific rms flux level is a factor of 4 lower for the 1.4 mm band than for the 2.7 mm band.

\n
\n
", "doi": "10.1007/978-94-015-6850-0_54", "issn": "0067-0057", "isbn": "978-94-015-6852-4", "publisher": "Springer Netherlands", "place_of_publication": "Dordrecht", "publication": "Astrophysics and Space Science Library", "publication_date": "1990-01-31", "volume": "158", "pages": "155-156" }, { "id": "authors:4bfs4-ksv34", "collection": "authors", "collection_id": "4bfs4-ksv34", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201008-112316591", "type": "book_section", "title": "CO(2\u21921) Emission from NGC 3256: An Interacting Pair of Galaxies", "book_title": "Submillimetre Astronomy", "author": [ { "family_name": "Sargent", "given_name": "A. I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Sanders", "given_name": "D. B.", "orcid": "0000-0002-1233-9998", "clpid": "Sanders-D-B" }, { "family_name": "Phillips", "given_name": "T. G.", "clpid": "Phillips-T-G" } ], "contributor": [ { "family_name": "Watt", "given_name": "Graeme D.", "clpid": "Watt-G-D" }, { "family_name": "Webster", "given_name": "Adrian S.", "clpid": "Webster-A-S" } ], "abstract": "At optical wavelengths, characteristic \"tails\" and chaotic nuclear appearance clearly identify NGC 3256 as an interacting system (Toomre 1977; Schweizer 1986). The newly-constructed, 10.4 m diameter, Leighton telescope of the Caltech Submillimeter Observatory (CSO) has been used to acquire observations of this merger in the CO (2\u21921) transition at 230 GHz. The turbulent nature of NGC 3256 is immediately obvious in Figure 1, a high contrast photograph provided by F. Schweizer, where circles representing the beam (30\u2033 FWHM) indicate the positions observed.", "doi": "10.1007/978-94-015-6850-0_82", "isbn": "9789401568524", "publisher": "Springer Netherlands", "place_of_publication": "Dordrecht", "publication_date": "1990", "pages": "221-222" }, { "id": "authors:b4vqb-ebx03", "collection": "authors", "collection_id": "b4vqb-ebx03", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210217-195625774", "type": "book_section", "title": "CO (2-1) Studies of Centaurus A", "book_title": "Submillimetre Astronomy", "author": [ { "family_name": "Phillips", "given_name": "T. G.", "clpid": "Phillips-T-G" }, { "family_name": "Sanders", "given_name": "D. B.", "orcid": "0000-0002-1233-9998", "clpid": "Sanders-David-B" }, { "family_name": "Sargent", "given_name": "A. I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" } ], "contributor": [ { "family_name": "Watt", "given_name": "Graeme D.", "clpid": "Watt-Graeme-D" }, { "family_name": "Webster", "given_name": "Adrian S.", "clpid": "Webster-Adrian-S" } ], "abstract": "Using the Caltech Submillimeter Observatory (CSO), Phillips et al. (1987) detected CO emission from the nearby radio galaxy Centaurus A. They reported emission from the dust lane region and showed that the material rotated very much like a disk galaxy imbedded within the larger elliptical system. They also showed that the heliocentric systemic velocity revealed by the CO observations at 547 (\u00b1 5) km/s was close to the value of 538 (\u00b1 10) km/s found for the elliptical component by Wilkinson et al. (1986).", "doi": "10.1007/978-94-015-6850-0_83", "isbn": "9789401568524", "publisher": "Springer Netherlands", "place_of_publication": "Dordrecht", "publication_date": "1990", "pages": "223-224" }, { "id": "authors:6cvnd-2pt87", "collection": "authors", "collection_id": "6cvnd-2pt87", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20210217-195625533", "type": "book_section", "title": "CO(2\u21921) / CO(1\u21920) observations of luminous infrared galaxies", "book_title": "Submillimetre Astronomy", "author": [ { "family_name": "Sanders", "given_name": "D. B.", "orcid": "0000-0002-1233-9998", "clpid": "Sanders-David-B" }, { "family_name": "Sargent", "given_name": "A. I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Scoville", "given_name": "N. Z.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" }, { "family_name": "Phillips", "given_name": "T. G.", "clpid": "Phillips-T-G" } ], "contributor": [ { "family_name": "Watt", "given_name": "Graeme D.", "clpid": "Watt-Graeme-D" }, { "family_name": "Webster", "given_name": "Adrian S.", "clpid": "Webster-Adrian-S" } ], "abstract": "CO(2\u21921) spectra of several luminous infrared galaxies have been obtained with the Caltech Submillimeter Observatory (CSO). For those galaxies distant enough to be unresolved with the CSO beam, we have compared the CO(2\u21921) profile with the corresponding, unresolved CO(1\u21920) profile in order to investigate the contribution of optically thin CO to the total CO emission.", "doi": "10.1007/978-94-015-6850-0_78", "isbn": "9789401568524", "publisher": "Springer Netherlands", "place_of_publication": "Dordrecht", "publication_date": "1990", "pages": "213-214" }, { "id": "authors:th7f6-qmp59", "collection": "authors", "collection_id": "th7f6-qmp59", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181121-090050084", "type": "book_section", "title": "Molecular Disks Around Young Stars", "book_title": "Structure and Dynamics of the Interstellar Medium", "author": [ { "family_name": "Sargent", "given_name": "Anneila I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Beckwith", "given_name": "Steven V. W.", "clpid": "Beckwith-S-V-W" } ], "contributor": [ { "family_name": "Moles", "given_name": "Mariano", "clpid": "Moles-M" }, { "family_name": "Tenorio-Tagle", "given_name": "Guillermo", "clpid": "Tenorio-Tagle-G" }, { "family_name": "Melnick", "given_name": "Jorge", "clpid": "Melnick-J" } ], "abstract": "There is now a substantial body of evidence that disk-like structures of gas and dust surround many protostars and young stellar objects (e.g. Rodriguez, these proceedings). We are currently studying a number of these disks to establish whether they have properties compatible with those attributed to the proto-solar nebula, in the early stages of evolution of our solar system. The frequency with which such proto-planetary disks are associated with young stars is also being investigated.", "doi": "10.1017/S0252921100023769", "isbn": "9783540519560", "publisher": "Springer", "place_of_publication": "Berlin", "publication_date": "1989", "pages": "215-220" }, { "id": "authors:e5ks6-zp582", "collection": "authors", "collection_id": "e5ks6-zp582", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181119-130439078", "type": "book_section", "title": "High Resolution Studies of Star-Forming Molecular Clouds", "book_title": "Star Forming Regions", "author": [ { "family_name": "Sargent", "given_name": "A. I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Scoville", "given_name": "N.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" }, { "family_name": "Masson", "given_name": "C. R.", "clpid": "Masson-C-R" }, { "family_name": "Lo", "given_name": "K. Y.", "clpid": "Lo-K-Y" }, { "family_name": "Phillips", "given_name": "T. G.", "clpid": "Phillips-T-G" } ], "contributor": [ { "family_name": "Jugaku", "given_name": "Jun", "clpid": "Jugaku-Jun" }, { "family_name": "Peimbert", "given_name": "Manuel", "clpid": "Peimbert-M" } ], "abstract": "Observations of star formation sites in a number of molecular clouds, including NGC 7538, NGC 2071, Cepheus A and K3-50A, have been made using the Owens Valley millimeter wave interferometer. The measurements of ^(12)CO, ^(13)CO, CS and continuum emission are at resolutions of order 7\u2033. Continuum emission at 2.7 mm is detected from all the cloud cores and, in general, the ^(12)CO interferometer maps reveal the presence of high velocity, bipolar outflows within 10\u2033 of these continuum sources. Thus, the origins of the outflows are readily identifiable; the flows themselves appear to remain collimated on scales of less than 10^(17) cm. The orientations of the flows are similar to those seen at lower resolution, except in Cepheus A, where the interferometer is capable of distinguishing between two outflows which are confused in single telescope maps.", "doi": "10.1017/S0074180900095693", "isbn": "9789027723888", "publisher": "D. Reidel", "place_of_publication": "Dordrecht", "publication_date": "1987", "pages": "329-330" }, { "id": "authors:vrtxy-czy95", "collection": "authors", "collection_id": "vrtxy-czy95", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201001-145811098", "type": "book_section", "title": "Radio and Infrared Observations of OH/IR Stars", "book_title": "Mass Loss from Red Giants", "author": [ { "family_name": "Sargent", "given_name": "Anneila I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Baud", "given_name": "Boudewijn", "clpid": "Baud-Boudewijn" } ], "contributor": [ { "family_name": "Morris", "given_name": "Mark", "clpid": "Morris-Mark" }, { "family_name": "Zuckerman", "given_name": "Ben", "clpid": "Zuckerman-B" } ], "abstract": "Combined infrared and OH spectral line observations are essential to understanding the nature of OH/IR stars, the properties of their circumstellar envelopes and the OH maser pump mechanism. We have used the Very Large Array of the National Radio Astronomy Observatory to determine very precise radio positions for a selection of such objects near the tangential point and at the galactic center and have subsequently made simultaneous infrared and OH observations of both samples. From the infrared measurements, luminosities of these stars and masses of the thick dust shells which surround them have been derived, while the double-peaked OH emission line profiles have yielded both the stellar radial velocities, v_R, and the expansion velocities of the envelopes, v_e, as well as the maser luminosities. The selection criteria and the observations are described in detail elsewhere (Baud et al. 1984). The results are consistent with these stars lying at the top of the Asymptotic Giant Branch (AGB) of the Hertzsprung-Russell diagram; the dense circumstellar shells suggest that these objects are evolving rapidly through a phase of high mass loss.", "doi": "10.1007/978-94-009-5428-1_34", "isbn": "9789401088961", "publisher": "Springer Netherlands", "place_of_publication": "Dordrecht", "publication_date": "1985", "pages": "213-214" }, { "id": "authors:f5wak-t5b73", "collection": "authors", "collection_id": "f5wak-t5b73", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20181211-154717976", "type": "book_section", "title": "CO (2\u20131) observations of Maffei 2", "book_title": "The Milky Way Galaxy", "author": [ { "family_name": "Sargent", "given_name": "Anneila I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Sutton", "given_name": "E. C.", "clpid": "Sutton-E-C" }, { "family_name": "Masson", "given_name": "C. R.", "clpid": "Masson-C-R" }, { "family_name": "Phillips", "given_name": "T. G.", "clpid": "Phillips-T-G" }, { "family_name": "Lo", "given_name": "K.-Y.", "clpid": "Lo-K-Y" } ], "abstract": "Maffei 2 is a highly obscured galaxy, probably of type Sbc, at a distance of 5 Mpc (Allen and Raimond 1972; Spinrad et al. 1973). Since it lies close to the Galactic plane, there is considerable confusion in infrared and 21-cm HI observations due to Galactic emission, but investigations of its structure can be carried out at millimeter wavelengths where the Galaxy contribution is confined to a limited velocity range. The high resolution (30\u2033) of our CO J=2\u20131 observations permits both a detailed examination of Maffei 2 and a study of the nature of the gas in its nucleus, through comparison with the CO J=1\u20130 observations.", "doi": "10.1017/S0074180900242411", "isbn": "9789400952911", "publisher": "D. Reidel", "place_of_publication": "Dordrecht", "publication_date": "1985", "pages": "197-198" }, { "id": "authors:3vrhy-n7y56", "collection": "authors", "collection_id": "3vrhy-n7y56", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20201014-153714184", "type": "book_section", "title": "Structure of Star-Forming Regions-The Ages of Subgroups and the Progression of Star Formation", "book_title": "Birth and Evolution of Massive Stars and Stellar Groups", "author": [ { "family_name": "Sargent", "given_name": "Anneila I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" } ], "contributor": [ { "family_name": "Boland", "given_name": "Wilfried", "clpid": "Boland-W" }, { "family_name": "van Woerden", "given_name": "Hugo", "clpid": "van-Woerden-H" } ], "abstract": "The structure of star-forming regions is examined on scales ranging from the few hundred parsecs typical of OB-association/molecular-cloud complexes to the few hundredths of a parsec structure observed in dense cloud cores. Explanations of both the temporal and spatial progress of star formation are reviewed, and factors which may dominate the process on all scales are considered.", "doi": "10.1007/978-94-009-5478-6_2", "isbn": "9789401089197", "publisher": "Springer Netherlands", "place_of_publication": "Dordrecht", "publication_date": "1985", "pages": "5-22" }, { "id": "authors:gnwqg-fd822", "collection": "authors", "collection_id": "gnwqg-fd822", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160421-164244322", "type": "book_section", "title": "Aperture Synthesis Maps of CO Emission from M51", "author": [ { "family_name": "Lo", "given_name": "K. Y.", "clpid": "Lo-K-Y" }, { "family_name": "Berge", "given_name": "G.", "clpid": "Berge-G-L" }, { "family_name": "Claussen", "given_name": "M.", "clpid": "Claussen-M-J" }, { "family_name": "Heiligman", "given_name": "G.", "clpid": "Heiligman-G-M" }, { "family_name": "Keene", "given_name": "J.", "clpid": "Keene-Jocelyn" }, { "family_name": "Masson", "given_name": "C.", "clpid": "Masson-C" }, { "family_name": "Phillips", "given_name": "T.", "clpid": "Phillips-T-G" }, { "family_name": "Sargent", "given_name": "A.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Scoville", "given_name": "N.", "orcid": "0000-0002-0438-3323", "clpid": "Scoville-N-Z" }, { "family_name": "Watson", "given_name": "D.", "clpid": "Watson-D" }, { "family_name": "Woody", "given_name": "D.", "clpid": "Woody-D-P" }, { "literal": "International Union of Radio Science" }, { "literal": "Instituto de Radioastronomia Milimetrica" } ], "abstract": "7\"-resolution maps of CO emission from the central 2' of M51 have been made with the Owens Valley millimeter-wave interferometer. Relative warm gas from giant molecular clouds is seen largely confined to arms coincident with the dust lanes, forming coherent structure on the scale of ~3 Kpc. There is a minimum of CO emission within 400 pc of the center. Integrated CO intensity maps are presented. Non-circular motion of the CO gas is evident from the velocity field.", "publisher": "International Union of Radio Science", "publication_date": "1984" }, { "id": "authors:vnsfy-t1r07", "collection": "authors", "collection_id": "vnsfy-t1r07", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20160421-082902012", "type": "book_section", "title": "The Caltech Millimeter Wave Interferometer", "author": [ { "family_name": "Masson", "given_name": "C. R.", "clpid": "Masson-C-R" }, { "family_name": "Berge", "given_name": "G. L.", "clpid": "Berge-G-L" }, { "family_name": "Claussen", "given_name": "Mark J.", "clpid": "Claussen-M-J" }, { "family_name": "Heiligman", "given_name": "G. M.", "clpid": "Heiligman-G-M" }, { "family_name": "Leighton", "given_name": "R. B.", "clpid": "Leighton-R-B" }, { "family_name": "Lo", "given_name": "K. Y.", "clpid": "Lo-K-Y" }, { "family_name": "Moffett", "given_name": "A. T.", "clpid": "Moffett-A-T" }, { "family_name": "Phillips", "given_name": "T. G.", "clpid": "Phillips-T-G" }, { "family_name": "Sargent", "given_name": "Anneila I.", "orcid": "0000-0002-4633-5098", "clpid": "Sargent-A-I" }, { "family_name": "Scott", "given_name": "S. L.", "clpid": "Scott-S-L" }, { "family_name": "Woody", "given_name": "David P.", "clpid": "Woody-D-P" }, { "family_name": "Young", "given_name": "A.", "clpid": "Young-A" }, { "literal": "International Union of Radio Science" }, { "literal": "Instituto de Radioastronomia Milimetrica" } ], "abstract": "The Caltech Millimeter-Wave Interferometer has recently begun observations at a wavelength of 2.6 mm. We describe the instrument and some of the first results from it.", "publisher": "International Union of Radio Science", "publication_date": "1984" } ]