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Benitez JY, Franzen KY, Hodgkinson A, Lyneis CM, Strohmeier M, Thullier T, Todd D, Xie D. Production of high intensity 48Ca for the 88-Inch Cyclotron and other updates. Rev Sci Instrum 2014; 85:02A961. [PMID: 24593540 DOI: 10.1063/1.4854896] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/03/2023]
Abstract
Recently the Versatile ECR for NUclear Science (VENUS) ion source was engaged in a 60-day long campaign to deliver high intensity (48)Ca(11+) beam to the 88-Inch Cyclotron. As the first long term use of VENUS for multi-week heavy-element research, new methods were developed to maximize oven to target efficiency. First, the tuning parameters of VENUS for injection into the cyclotron proved to be very different than those used to tune VENUS for maximum beam output of the desired charge state immediately following its bending magnet. Second, helium with no oxygen support gas was used to maximize the efficiency. The performance of VENUS and its low temperature oven used to produce the stable requested 75 eμA of (48)Ca(11+) beam current was impressive. The consumption of (48)Ca in VENUS using the low temperature oven was checked roughly weekly, and was found to be on average 0.27 mg/h with an ionization efficiency into the 11+ charge state of 5.0%. No degradation in performance was noted over time. In addition, with the successful operation of VENUS the 88-Inch cyclotron was able to extract a record 2 pμA of (48)Ca(11+), with a VENUS output beam current of 219 eμA. The paper describes the characteristics of the VENUS tune used for maximum transport efficiency into the cyclotron as well as ongoing efforts to improve the transport efficiency from VENUS into the cyclotron. In addition, we briefly present details regarding the recent successful repair of the cryostat vacuum system.
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Affiliation(s)
- J Y Benitez
- Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
| | - K Y Franzen
- Mevion Medical Systems, 300 Foster St., Littleton, Massachusetts 01460, USA
| | - A Hodgkinson
- Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
| | - C M Lyneis
- Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
| | - M Strohmeier
- Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
| | - T Thullier
- Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
| | - D Todd
- Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
| | - D Xie
- Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
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Benitez JY, Franzen KY, Hodgkinson A, Loew T, Lyneis CM, Phair L, Saba J, Strohmeier M, Tarvainen O. Recent progress on the superconducting ion source VENUS. Rev Sci Instrum 2012; 83:02A311. [PMID: 22380158 DOI: 10.1063/1.3662119] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/31/2023]
Abstract
The 28 GHz Ion Source VENUS (versatile ECR for nuclear science) is back in operation after the superconducting sextupole leads were repaired and a fourth cryocooler was added. VENUS serves as an R&D device to explore the limits of electron cyclotron resonance source performance at 28 GHz with its 10 kW gryotron and optimum magnetic fields and as an ion source to increase the capabilities of the 88-Inch Cyclotron both for nuclear physics research and applications. The development and testing of ovens and sputtering techniques cover a wide range of applications. Recent experiments on bismuth demonstrated stable operation at 300 eμA of Bi(31+), which is in the intensity range of interest for high performance heavy-ion drivers such as FRIB (Facility for Rare Isotope Beams). In addition, the space radiation effects testing program at the cyclotron relies on the production of a cocktail beam with many species produced simultaneously in the ion source and this can be done with a combination of gases, sputter probes, and an oven. These capabilities are being developed with VENUS by adding a low temperature oven, sputter probes, as well as studying the RF coupling into the source.
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Affiliation(s)
- J Y Benitez
- Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA.
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Abbott B, Abbott R, Adhikari R, Agresti J, Ajith P, Allen B, Allen J, Amin R, Anderson SB, Anderson WG, Araya M, Armandula H, Ashley M, Aulbert C, Babak S, Balasubramanian R, Ballmer S, Barish BC, Barker C, Barker D, Barton MA, Bayer K, Belczynski K, Betzwieser J, Bhawal B, Bilenko IA, Billingsley G, Black E, Blackburn K, Blackburn L, Bland B, Bogue L, Bork R, Bose S, Brady PR, Braginsky VB, Brau JE, Brown DA, Buonanno A, Busby D, Butler WE, Cadonati L, Cagnoli G, Camp JB, Cannizzo J, Cannon K, Cardenas L, Carter K, Casey MM, Charlton P, Chatterji S, Chen Y, Chin D, Christensen N, Cokelaer T, Colacino CN, Coldwell R, Cook D, Corbitt T, Coyne D, Creighton JDE, Creighton TD, Dalrymple J, D'Ambrosio E, Danzmann K, Davies G, DeBra D, Dergachev V, Desai S, DeSalvo R, Dhurandar S, Díaz M, Di Credico A, Drever RWP, Dupuis RJ, Ehrens P, Etzel T, Evans M, Evans T, Fairhurst S, Finn LS, Franzen KY, Frey RE, Fritschel P, Frolov VV, Fyffe M, Ganezer KS, Garofoli J, Gholami I, Giaime JA, Goda K, Goggin L, González G, Gray C, Gretarsson AM, Grimmett D, Grote H, Grunewald S, Guenther M, Gustafson R, Hamilton WO, Hanna C, Hanson J, Hardham C, Harry G, Heefner J, Heng IS, Hewitson M, Hindman N, Hoang P, Hough J, Hua W, Ito M, Itoh Y, Ivanov A, Johnson B, Johnson WW, Jones DI, Jones G, Jones L, Kalogera V, Katsavounidis E, Kawabe K, Kawamura S, Kells W, Khan A, Kim C, King P, Klimenko S, Koranda S, Kozak D, Krishnan B, Landry M, Lantz B, Lazzarini A, Lei M, Leonor I, Libbrecht K, Lindquist P, Liu S, Lormand M, Lubinski M, Lück H, Luna M, Machenschalk B, MacInnis M, Mageswaran M, Mailand K, Malec M, Mandic V, Marka S, Maros E, Mason K, Matone L, Mavalvala N, McCarthy R, McClelland DE, McHugh M, McNabb JWC, Melissinos A, Mendell G, Mercer RA, Meshkov S, Messaritaki E, Messenger C, Mikhailov E, Mitra S, Mitrofanov VP, Mitselmakher G, Mittleman R, Miyakawa O, Mohanty S, Moreno G, Mossavi K, Mueller G, Mukherjee S, Myers E, Myers J, Nash T, Nocera F, Noel JS, O'Reilly B, O'Shaughnessy R, Ottaway DJ, Overmier H, Owen BJ, Pan Y, Papa MA, Parameshwaraiah V, Parameswariah C, Pedraza M, Penn S, Pitkin M, Prix R, Quetschke V, Raab F, Radkins H, Rahkola R, Rakhmanov M, Rawlins K, Ray-Majumder S, Re V, Regimbau T, Reitze DH, Riesen R, Riles K, Rivera B, Robertson DI, Robertson NA, Robinson C, Roddy S, Rodriguez A, Rollins J, Romano JD, Romie J, Rowan S, Rüdiger A, Ruet L, Russell P, Ryan K, Sandberg V, Sanders GH, Sannibale V, Sarin P, Sathyaprakash BS, Saulson PR, Savage R, Sazonov A, Schilling R, Schofield R, Schutz BF, Schwinberg P, Scott SM, Seader SE, Searle AC, Sears B, Sellers D, Sengupta AS, Shawhan P, Shoemaker DH, Sibley A, Siemens X, Sigg D, Sintes AM, Smith J, Smith MR, Spjeld O, Strain KA, Strom DM, Stuver A, Summerscales T, Sung M, Sutton PJ, Tanner DB, Taylor R, Thorne KA, Thorne KS, Tokmakov KV, Torres C, Torrie C, Traylor G, Tyler W, Ugolini D, Ungarelli C, Vallisneri M, van Putten M, Vass S, Vecchio A, Veitch J, Vorvick C, Vyachanin SP, Wallace L, Ward H, Ward R, Watts K, Webber D, Weiland U, Weinstein A, Weiss R, Wen S, Wette K, Whelan JT, Whitcomb SE, Whiting BF, Wiley S, Wilkinson C, Willems PA, Willke B, Wilson A, Winkler W, Wise S, Wiseman AG, Woan G, Woods D, Wooley R, Worden J, Yakushin I, Yamamoto H, Yoshida S, Zanolin M, Zhang L, Zotov N, Zucker M, Zweizig J. Upper limits on a stochastic background of gravitational waves. Phys Rev Lett 2005; 95:221101. [PMID: 16384203 DOI: 10.1103/physrevlett.95.221101] [Citation(s) in RCA: 7] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/30/2005] [Indexed: 05/05/2023]
Abstract
The Laser Interferometer Gravitational-Wave Observatory has performed a third science run with much improved sensitivities of all three interferometers. We present an analysis of approximately 200 hours of data acquired during this run, used to search for a stochastic background of gravitational radiation. We place upper bounds on the energy density stored as gravitational radiation for three different spectral power laws. For the flat spectrum, our limit of omega0 < 8.4 x 10(-4) in the 69-156 Hz band is approximately 10(5) times lower than the previous result in this frequency range.
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Affiliation(s)
- B Abbott
- LIGO-California Institute of Technology, Pasadena, California 91125, USA
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Abbott B, Abbott R, Adhikari R, Ageev A, Allen B, Amin R, Anderson SB, Anderson WG, Araya M, Armandula H, Ashley M, Asiri F, Aufmuth P, Aulbert C, Babak S, Balasubramanian R, Ballmer S, Barish BC, Barker C, Barker D, Barnes M, Barr B, Barton MA, Bayer K, Beausoleil R, Belczynski K, Bennett R, Berukoff SJ, Betzwieser J, Bhawal B, Bilenko IA, Billingsley G, Black E, Blackburn K, Blackburn L, Bland B, Bochner B, Bogue L, Bork R, Bose S, Brady PR, Braginsky VB, Brau JE, Brown DA, Bullington A, Bunkowski A, Buonanno A, Burgess R, Busby D, Butler WE, Byer RL, Cadonati L, Cagnoli G, Camp JB, Cantley CA, Cardenas L, Carter K, Casey MM, Castiglione J, Chandler A, Chapsky J, Charlton P, Chatterji S, Chelkowski S, Chen Y, Chickarmane V, Chin D, Christensen N, Churches D, Cokelaer T, Colacino C, Coldwell R, Coles M, Cook D, Corbitt T, Coyne D, Creighton JDE, Creighton TD, Crooks DRM, Csatorday P, Cusack BJ, Cutler C, D'Ambrosio E, Danzmann K, Daw E, DeBra D, Delker T, Dergachev V, DeSalvo R, Dhurandhar S, Di Credico A, Díaz M, Ding H, Drever RWP, Dupuis RJ, Edlund JA, Ehrens P, Elliffe EJ, Etzel T, Evans M, Evans T, Fairhurst S, Fallnich C, Farnham D, Fejer MM, Findley T, Fine M, Finn LS, Franzen KY, Freise A, Frey R, Fritschel P, Frolov VV, Fyffe M, Ganezer KS, Garofoli J, Giaime JA, Gillespie A, Goda K, González G, Gossler S, Grandclément P, Grant A, Gray C, Gretarsson AM, Grimmett D, Grote H, Grunewald S, Guenther M, Gustafson E, Gustafson R, Hamilton WO, Hammond M, Hanson J, Hardham C, Harms J, Harry G, Hartunian A, Heefner J, Hefetz Y, Heinzel G, Heng IS, Hennessy M, Hepler N, Heptonstall A, Heurs M, Hewitson M, Hild S, Hindman N, Hoang P, Hough J, Hrynevych M, Hua W, Ito M, Itoh Y, Ivanov A, Jennrich O, Johnson B, Johnson WW, Johnston WR, Jones DI, Jones L, Jungwirth D, Kalogera V, Katsavounidis E, Kawabe K, Kawamura S, Kells W, Kern J, Khan A, Killbourn S, Killow CJ, Kim C, King C, King P, Klimenko S, Koranda S, Kötter K, Kovalik J, Kozak D, Krishnan B, Landry M, Langdale J, Lantz B, Lawrence R, Lazzarini A, Lei M, Leonor I, Libbrecht K, Libson A, Lindquist P, Liu S, Logan J, Lormand M, Lubinski M, Lück H, Lyons TT, Machenschalk B, MacInnis M, Mageswaran M, Mailand K, Majid W, Malec M, Mann F, Marin A, Márka S, Maros E, Mason J, Mason K, Matherny O, Matone L, Mavalvala N, McCarthy R, McClelland DE, McHugh M, McNabb JWC, Mendell G, Mercer RA, Meshkov S, Messaritaki E, Messenger C, Mitrofanov VP, Mitselmakher G, Mittleman R, Miyakawa O, Miyoki S, Mohanty S, Moreno G, Mossavi K, Mueller G, Mukherjee S, Murray P, Myers J, Nagano S, Nash T, Nayak R, Newton G, Nocera F, Noel JS, Nutzman P, Olson T, O'Reilly B, Ottaway DJ, Ottewill A, Ouimette D, Overmier H, Owen BJ, Pan Y, Papa MA, Parameshwaraiah V, Parameswariah C, Pedraza M, Penn S, Pitkin M, Plissi M, Prix R, Quetschke V, Raab F, Radkins H, Rahkola R, Rakhmanov M, Rao SR, Rawlins K, Ray-Majumder S, Re V, Redding D, Regehr MW, Regimbau T, Reid S, Reilly KT, Reithmaier K, Reitze DH, Richman S, Riesen R, Riles K, Rivera B, Rizzi A, Robertson DI, Robertson NA, Robison L, Roddy S, Rollins J, Romano JD, Romie J, Rong H, Rose D, Rotthoff E, Rowan S, Rüdiger A, Russell P, Ryan K, Salzman I, Sandberg V, Sanders GH, Sannibale V, Sathyaprakash B, Saulson PR, Savage R, Sazonov A, Schilling R, Schlaufman K, Schmidt V, Schnabel R, Schofield R, Schutz BF, Schwinberg P, Scott SM, Seader SE, Searle AC, Sears B, Seel S, Seifert F, Sengupta AS, Shapiro CA, Shawhan P, Shoemaker DH, Shu QZ, Sibley A, Siemens X, Sievers L, Sigg D, Sintes AM, Smith JR, Smith M, Smith MR, Sneddon PH, Spero R, Stapfer G, Steussy D, Strain KA, Strom D, Stuver A, Summerscales T, Sumner MC, Sutton PJ, Sylvestre J, Takamori A, Tanner DB, Tariq H, Taylor I, Taylor R, Taylor R, Thorne KA, Thorne KS, Tibbits M, Tilav S, Tinto M, Tokmakov KV, Torres C, Torrie C, Traylor G, Tyler W, Ugolini D, Ungarelli C, Vallisneri M, van Putten M, Vass S, Vecchio A, Veitch J, Vorvick C, Vyachanin SP, Wallace L, Walther H, Ward H, Ware B, Watts K, Webber D, Weidner A, Weiland U, Weinstein A, Weiss R, Welling H, Wen L, Wen S, Whelan JT, Whitcomb SE, Whiting BF, Wiley S, Wilkinson C, Willems PA, Williams PR, Williams R, Willke B, Wilson A, Winjum BJ, Winkler W, Wise S, Wiseman AG, Woan G, Wooley R, Worden J, Wu W, Yakushin I, Yamamoto H, Yoshida S, Zaleski KD, Zanolin M, Zawischa I, Zhang L, Zhu R, Zotov N, Zucker M, Zweizig J, Kramer M, Lyne AG. Limits on gravitational-wave emission from selected pulsars using LIGO data. Phys Rev Lett 2005; 94:181103. [PMID: 15904354 DOI: 10.1103/physrevlett.94.181103] [Citation(s) in RCA: 8] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/29/2004] [Indexed: 05/02/2023]
Abstract
We place direct upper limits on the amplitude of gravitational waves from 28 isolated radio pulsars by a coherent multidetector analysis of the data collected during the second science run of the LIGO interferometric detectors. These are the first direct upper limits for 26 of the 28 pulsars. We use coordinated radio observations for the first time to build radio-guided phase templates for the expected gravitational-wave signals. The unprecedented sensitivity of the detectors allows us to set strain upper limits as low as a few times 10(-24). These strain limits translate into limits on the equatorial ellipticities of the pulsars, which are smaller than 10(-5) for the four closest pulsars.
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Affiliation(s)
- B Abbott
- LIGO-California Institute of Technology, Pasadena, CA 91125, USA
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