RESEARCH FACILITIES Astronomy Observatory JSVXLI7GMIRXM½G'SQQYRMX]
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National Radio RESEARCH FACILITIES Astronomy Observatory JSVXLI7GMIRXM½G'SQQYRMX]
2011
Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array CONTENTS RESEARCH FACILITIES 2011
The NRAO in The Coming Decade ...... 1
Atacama Large Millimeter/submillimeter Array...... 2
Expanded Very Large Array...... 4
Green Bank Telescope ...... 6
Very Long Baseline Array ...... 8
Student & Visitor Programs ...... 10
(above image) The radio emission (orange) detected by the NRAO Very Large Array (VLA) is synchrotron radiation emitted by electrons moving at nearly the speed of light in a GSWQMGQEKRIXMG½IPH8LIWIIPIGXVSRWSVMKMREXIMRIRSVQSYWIRIVK]SYX¾S[WJVSQNIXW fueled by a supermassive black hole at the center of the galaxy NGC 1316 (center, blue- [LMXI 'VIHMX 26%3%9-.19WSR
(cover) 8LMWTERSVEQESJXLI7GYXYQ%UYMPE1MPO];E]MPPYWXVEXIWXLIH]REQMGMRXIVTPE]FIX[IIR the birth and death of massive stars. This image combines 20 cm radio data from the :IV]0EVKI%VVE] VIH [MXLQMHMRJVEVIHHEXEJVSQXLI7TMX^IV7TEGI8IPIWGSTI KVIIR ERHFPYI[LMXI 6IKMSRW[LIVIVEHMSERHMRJVEVIHIQMWWMSREVITVSQMRIRXETTIEV]IPPS[ 'VIHMX (,IPJERH 'SPYQFME 6&IGOIV 9'(EZMW 6;LMXI 787G-
(back cover) 8LISYXP]MRKVIKMSRWSJXLI7SYXLIVR4MR[LIIP+EPE\] 1 EVILMKLPMKLXIHMRXLMW composite image from NASA’s Galaxy Evolution Explorer and the NRAO Very Large Array. The Galaxy Evolution Explorer far- and near-ultraviolet data (blue and green, VIWTIGXMZIP] LMKLPMKLXXLIKEPE\]´WJEVXLIWX¾YRKGPYWXIVWSJ]SYRKWXEVW[LMGLEVIYT to 140,000 light-years from its center. The Very Large Array 21 cm observations (red) LMKLPMKLXXLIL]HVSKIRKEWXLEXGSQTVMWIWXLII\XIRHIHWTMVEPEVQW'VIHMX 2%7%.40 Caltech/NRAO VLA/MPIA The NRAO in the Coming Decade
The research facilities of the National Radio Astronomy Observatory play critical roles across all of modern astrophysics. Radio astronomy probes the earliest, most intense, and optically obscured phases of planet, star, galaxy, and black hole JSVQEXMSRERHVIZIEPWXLIGSSPHIRWIKEWJVSQ[LMGLWXEVWJSVQ6EHMSXIPIWGSTIW EPPS[EWXVSRSQIVWXSQEOITVIGMWMSRGSWQSPSKMGEPQIEWYVIQIRXWXIWXJYRHEQIRXEP TL]WMGW EREP]^I GSQTPI\ QEKRIXMG ½IPHW ERH XLIMV IJJIGXW TVSFI LMKLIRIVK] phenomena, and understand the physics and chemistry of extreme environments.
-RXLIGSQMRKHIGEHIXLI2EXMSREP6EHMS%WXVSRSQ]3FWIVZEXSV][MPPSTIVEXI EWYMXISJXIPIWGSTIWXLEX[MPPIREFPIFVSEHEWXVSTL]WMGEPHMWGSZIV]8LI%XEGEQE 0EVKI1MPPMQIXIVWYFQMPPMQIXIV%VVE] %01% [MPPFIKMR)EVP]7GMIRGIMRPEXI ERHFIJYPP]STIVEXMSREPMRSTIRMRKERI[[MRHS[MRXSXLITL]WMGWSJXLI GSPH9RMZIVWIERHTVSZMHMRKIRSVQSYWMQTVSZIQIRXWMRVIWSPYXMSRWIRWMXMZMX]ERH frequency coverage.
The Expanded Very Large Array (EVLA) leverages existing NRAO infrastructure to GVIEXIERIRXMVIP]RI[VIWIEVGLMRWXVYQIRXERHMQTVSZISYVEFMPMX]XSI\TPSVIXLI 9RMZIVWIEXGIRXMQIXIV[EZIPIRKXLWF]ERSVHIVSJQEKRMXYHI8LI):0%MRMXMEXIH )EVP]7GMIRGISTIVEXMSRWMR1EVGLERH[MPPVIQEMRXLIQSWXTS[IVJYPVEHMS XIPIWGSTIMRXLI[SVPHMRXLMWTSVXMSRSJXLIIPIGXVSQEKRIXMGWTIGXVYQXLVSYKLEX least the next decade.
The Robert C. Byrd Green Bank Telescope has matured into an extremely productive VIWIEVGLXSSP[MXLIZIVMRGVIEWMRKWIRWMXMZMX]IJ½GMIRG]ERHMQEKMRKGETEFMPMXMIWXLEX[MPP WSSRIREFPIHIIT[MHI½IPHWXYHMIWSJXLI+EPE\]ERHFI]SRH8LI26%3ERHMXW MRXIVREXMSREPTEVXRIVWEVIEPWSHIPMZIVMRKWMKRM½GERXP]MQTVSZIHWIRWMXMZMX]EXXLI:IV] 0SRK&EWIPMRI%VVE]IREFPMRKE[MHIVERKISJMRRSZEXMZIWGMIRGIXLEXFIRI½XWJVSQXLI array’s unique precision astrometry and high-resolution imaging capabilities.
8LI26%3MWEPWS[SVOMRK[MXLXLIEWXVSRSQ]GSQQYRMX]XSHIZIPSTXLIWGMIRXM½G and technical concepts for the next generation of research facilities including the *VIUYIRG]%KMPI 7SPEV 6EHMSXIPIWGSTI *%76 XLI 2SVXL%QIVMGER 2ERSLIVX^ Gravitational Observatory (NANOGrav), the Precision Array to Probe the Epoch SJ6IMSRM^EXMSR 4%4)6 ERHXLI7UYEVI/MPSQIXVI%VVE] 7/%
1 Atacama Large Millimeter/ submillimeter Array (ALMA) %PXMTPERSHI'LENRERXSV'LMPI
The Atacama Large Millimeter/submillimeter Array (ALMA) [MPPIREFPIXVERWJSVQEXMSREPVIWIEVGLMRXSXLITL]WMGWSJXLI GSPH9RMZIVWIVIKMSRW[LIVIXLIWO]MWHEVOMRXLIZMWMFPITEVX SJXLIWTIGXVYQFYXWLMRIWFVMKLXP]EXQMPPMQIXIV[EZIPIRKXLW 3TIVEXMRKEX[EZIPIRKXLWJVSQXS QQ%01%[MPPTVSFIXLI½VWXWXEVWERHKEPE\MIWERHHMVIGXP]MQEKIMRXIVWXIPPEVKEWMRXLITVSGIWW SJJSVQMRKRI[TPERIXWXLYWTVSZMHMRKERI[[MRHS[SRGSWQMGSVMKMRW%01%MWFIMRKFYMPXSRXLI'LENRERXSVTPEMRSJXLI'LMPIER%RHIWMR XLIHMWXVMGXSJ7ER4IHVSHI%XEGEQEQEFSZIWIEPIZIP[LIVIXLI)EVXL´WEXQSWTLIVIMWPEVKIP]XVERWTEVIRXEXQMPPMQIXIV[EZIPIRKXLW 9TSRGSQTPIXMSRXLIXIPIWGSTI[MPPFIGSQTSWIHSJEXPIEWXLMKLTVIGMWMSRERXIRREWTVSZMHMRKYRTVIGIHIRXIHWIRWMXMZMX]ERHMQEKMRKXLI WO]EXVIWSPYXMSRWEW½RIEWEVGWIGEJEGXSVSJXIRFIXXIVXLERXLI,YFFPI7TEGI8IPIWGSTI
%01%GSRWXVYGXMSR[MPPFIGSQTPIXIHMRPEXI;LMPIXLIEVVE]MWWXMPPFIMRKEWWIQFPIHWMKRM½GERXSFWIVZMRKXMQI[MPPFIQEHIEZEMPEFPIXS XLIGSQQYRMX]EW)EVP]7GMIRGIFIKMRRMRKMRPEXI%GEPPJSV%01%)EVP]7GMIRGITVSTSWEPW[MPPFIMWWYIHHYVMRKXLI½VWXUYEVXIVSJ [MXLXLITVSTSWEPHIEHPMRIEFSYXXLVIIQSRXLWPEXIV)ZIRHYVMRK)EVP]7GMIRGI%01%[MPPTVSZMHIWMKRM½GERXP]FIXXIVGETEFMPMXMIWXLERSXLIV TVIWIRXHE]QMPPMQIXIVMRXIVJIVSQIXIVW-RMXMEPP]XLIXIPIWGSTI[MPPMRGPYHIEXPIEWXERXIRREWTVSHYGMRKVIWSPYXMSRWEW½RIEWEVGWIGERH XLIGETEFMPMXMIW[MPPMQTVSZIEWXLIXIPIWGSTIETTVSEGLIWJYPPSTIVEXMSRW
ALMA is an international astronomy facility, a partnership SJ )YVSTI .ETER ERH 2SVXL %QIVMGE MR GSSTIVEXMSR [MXL XLI 6ITYFPMG SJ 'LMPI%01% MW JYRHIH MR )YVSTI F]XLI)YVSTIER3VKERM^EXMSRJSV%WXVSRSQMGEP6IWIEVGL MR XLI 7SYXLIVR ,IQMWTLIVI )73 ERH MR .ETER F] the National Institutes of Natural Sciences (NINS) in GSSTIVEXMSR[MXLXLI%GEHIQME7MRMGEMR8EM[ERERHMR 2SVXL%QIVMGEF]XLI972EXMSREP7GMIRGI*SYRHEXMSR 27* MRGSSTIVEXMSR[MXLXLI2EXMSREP6IWIEVGL'SYRGMP of Canada (NRC) and the National Science Council of 8EM[ER 27' %01% GSRWXVYGXMSR ERH STIVEXMSRW EVI PIHSRFILEPJSJ)YVSTIF])73SRFILEPJSJ.ETERF] XLI2EXMSREP%WXVSRSQMGEP3FWIVZEXSV]SJ.ETER 2%3. ERHSRFILEPJSJ2SVXL%QIVMGEF]XLI2EXMSREP6EHMS%WXVSRSQ]3FWIVZEXSV] 26%3 [LMGLMWQEREKIHF]%WWSGMEXIH9RMZIVWMXMIW-RG %9-
The North American ALMA Science Center (NAASC) The North American ALMA Science Center, based at the NRAO headquarters in Charlottesville, Virginia, supports the science use of ALMA by the North American astronomical community, and the research and development for future ALMA upgrades. The NAASC provides a RYQFIVSJOI]WIVZMGIWXSYWIVW8LIWIMRGPYHISVKERM^MRKERHLSWXMRKGSRJIVIRGIWERHXVEMRMRK[SVOWLSTWWYTTSVXMRKYWIVWHYVMRKXLI TVITEVEXMSRERHWYFQMWWMSRSJ%01%TVSTSWEPWERHSFWIVZEXMSRWERHLIPTMRKYWIVWVIHYGIERHEREP]^IXLIMV%01%HEXEFSXLVIQSXIP]ERH XLVSYKLZMWMXWXSXLI2%%7'WMXIMR'LEVPSXXIWZMPPI8LI2%%7'EPWSTVITEVIWERHQEMRXEMRW%01%YWIVHSGYQIRXEXMSRERH[IFWMXIWERH STIVEXIWXLI%01%LIPTHIWO1SVIMRJSVQEXMSRSRXLI2%%7'MWEZEMPEFPIEXLXXT WGMIRGIRVESIHYEPQEMRXVSREEWGWLXQP8LI2%%7'MW STIVEXIHF]26%3MRTEVXRIVWLMT[MXLXLI2EXMSREP6IWIEVGL'SYRGMPSJ'EREHE KEY SCIENCE %01%MWHIWMKRIHXSEGGSQTPMWLEXEQMRMQYQXLVII±0IZIP²WGMIRGIKSEPW HIXIGX'3'MRPIWWXLERLSYVWJVSQERSVQEPKEPE\] PMOIXLI1MPO];E]EXVIHWLMJX^! VIWSPZITVSXSTPERIXEV]HMWOWEVSYRHWXEVWEXEHMWXERGISJTG ERH TVSZMHITVIGMWIMQEKMRKEX WYFQMPPMQIXIV[EZIPIRKXLW[MXLEVGWIGVIWSPYXMSRMR[LMGLXLIWO]FVMKLXRIWWMWEGGYVEXIP]VITVIWIRXIHJSVEPPTSMRXWEFSZI SJXLI
2 TIEO¾Y\MRXLIQET%01%[MPPXLYWFIGETEFPISJLMKL½HIPMX]MQEKMRKFSXLMRXLIGSRXMRYYQERHMRWTIGXVEPPMRIW-X[MPPLEZI[MHIFERH JVIUYIRG]GSZIVEKI +,^MRHYEPTSPEVM^EXMSR ERH[MPPFIGETEFPISJMQEKMRK½IPHWPEVKIVXLERXLITVMQEV]FIEQYWMRKQSWEMGW
%01%[MPPFIEKIRIVEPTYVTSWIVIWIEVGLMRWXVYQIRX-REHHMXMSRXSEGGSQTPMWLMRKXLIWTIGM½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
RECEIVER BANDS
Band # 3 4 5 6 7 8 9 10 Frequency Range (GHz) 84 - 116 125 - 163 163 - 211 211 - 275 275 - 373 385 - 500 602 - 720 Wavelength Range (mm) 2.40 - 1.84 1.84 - 1.42 0.78 - 0.60 0.50-0.42 0.38- 0.32
Early Science Array Completion Antennas * 16 (12 m) At least 54 x 12m & 12 x 7m Bands &ERHW &ERHW 1E\MQYQ&ERH[MHXL +,^ TSP\ +,^ +,^ TSP\ +,^ 'SVVIPEXSV'SR½KYVEXMSRW 5 – 21 GSR½KW OQW Maximum Angular Resolution 0.02” (ƪ /1 mm)(10 km/max baseline) 0.02” (ƪ /1 mm)(10 km/max baseline) Maximum Baseline 250 m (may achieve 500m) 15 km Continuum Sensitivity WIG&ERHW¯ b¯Q.]FIEQ b¯Q.]FIEQ Spectral Line Sensitivity WIGOQWIG&ERHW¯ b¯Q.]FIEQ b¯Q.]FIEQ
Far left: A simulation of an 8-hour ALMA observation at 345 GHz, showing how ALMA will image the gap swept up by the proto-planet, the disk surrounding the star, and the proto-planet itself. Image courtesy S. Wolf, from Wolf & D’Angelo (2005)
Left: An ALMA antenna rides atop a transporter to the 5000m elevation Array Operations Site in northern Chile.
ALMA TIMELINE ALMA on the World Wide Web LXXT WGMIRGIRVESIHYEPQE Call for ALMA Early Science Proposals Early 2011 LXXT [[[EPQESFWIVZEXSV]SVK Early Science Proposal Submission Deadline Mid 2011 Begin Early Science Late 2011 NAASC on the World Wide Web 66 ALMA Antennas Operational 2013 LXXT WGMIRGIRVESIHYEPQEMRXVSREEWGWLXQP
3 © NRAO/AUI & Kristal Armendariz Expanded Very Large Array (EVLA) 7SGSVVS2I[1I\MGS
The Expanded Very Large Array is a radio telescope of unprecedented sensitivity, frequency coverage, and imaging capability that is being GVIEXIHF]QSHIVRM^MRKXLI:IV]0EVKI%VVE]-XWRI[;MHIFERH -RXIVJIVSQIXVMG (MKMXEP %VGLMXIGXYVI ;-(%6 GSVVIPEXSV [LIR HITPS]IHMRJYPP[MPPTVSZMHIWYTIVFWTIGXVEPVIWSPYXMSRERH½HIPMX] SZIVZIV][MHIMRWXERXERISYWJVIUYIRG]FERHWIREFPMRKEWXVSRSQIVW XS QEOI JYPPFIEQ MQEKIW [MXL ZIV] LMKL WTEXMEP VIWSPYXMSR ERH dramatically improved continuum sensitivity. The VLA correlator [EWXYVRIHSJJMR.ERYEV]ERHVITPEGIHF]XLIRI[;-(%6 GSVVIPEXSV%XXLIWEQIXMQIXLIHMVIGXMSRSJXLIEVVE]GSR½KYVEXMSR G]GPI[EWVIZIVWIHXSJEGMPMXEXI;-(%6GSQQMWWMSRMRK8LIWIX[S events marked the beginning of EVLA Early Science in March 2010. )EVP] 7GMIRGI JIEXYVIW X[S TVSKVEQW SJJIVMRK IRLERGIH WGMIRXM½G STTSVXYRMXMIWXSXLIGSQQYRMX] ER3TIR7LEVIH6MWO3FWIVZMRK program for the general user community, and a Resident Shared Risk Observing program. Over time, an increasing range of WIDAR GETEFMPMXMIW[MPPFIQEHIEZEMPEFPIXSXLIWGMIRXM½GGSQQYRMX]XLVSYKL XLIWIX[STVSKVEQW
;LIRGSQTPIXIMRXLI):0%[MPPGSQTPIQIRXRI\XKIRIVEXMSR MRWXVYQIRXWWYGLEW%01%ERHXLI.EQIW;IFF7TEGI8IPIWGSTIERHTVSZMHI
'SRXMRYYQWIRWMXMZMX]MQTVSZIQIRXSZIVXLI:0%F]JEGXSVWSJXS 3TIVEXMSREXER]JVIUYIRG]FIX[IIRERH+,^[MXLYTXS +,^FERH[MHXLTIVTSPEVM^EXMSR MRHITIRHIRXP]XYREFPIWYFFERHTEMVWIEGLTVSZMHMRKJYPPTSPEVM^EXMSRGETEFMPMXMIW %QMRMQYQSJ ERHEQE\MQYQSJ WTIGXVEPGLERRIPWEHNYWXEFPIJVIUYIRG]VIWSPYXMSR FIX[IIR1,^ERH,^ERHI\XIRWMZIGETEFMPMXMIWXSEPPSGEXIGSVVIPEXSVVIWSYVGIW 7TEXMEPH]REQMGVERKI"6JVIUYIRG]H]REQMGVERKI"5[MXLRSMWIPMQMXIHJYPP½IPHMQEKMRKMREPP7XSOIWTEVEQIXIVW (]REQMGWGLIHYPMRKFEWIHSR[IEXLIVEVVE]GSR½KYVEXMSRERHWGMIRGIVIUYMVIQIRXW 6IJIVIRGIMQEKIWEYXSQEXMGEPP]TVSHYGIH[MXLEPPHEXETVSHYGXWEVGLMZIH
8LI):0%4VSNIGXMWJYRHIHF]XLI972EXMSREP7GMIRGI*SYRHEXMSR[MXLEHHMXMSREPGSRXVMFYXMSRWJVSQXLI2EXMSREP6IWIEVGL'SYRGMPMR 'EREHEERHXLI'SRWINS2EGMSREPHI'MIRGME]8IGRSPSKMEMR1I\MGS
EVLA on the World Wide Web LXXT WGMIRGIRVESIHYIZPE
EVLA MILESTONES
Begin Early Science Mar 2010 0EWXERXIRREVIXVS½XXIHXS):0%HIWMKR 1E] Enhanced capabilities offered for Early Science Sep 2011 'SQTPIXIGSQQMWWMSRMRKSJJYPP;-(%6GSVVIPEXSV .ER Last EVLA receiver installed Dec 2012
4 KEY SCIENCE The Magnetic Universe The sensitivity, frequency agility, and spectral capability of the ):0% [MPP EPPS[ EWXVSRSQIVW XS XVEGI XLI QEKRIXMG ½IPHW MR <VE] IQMXXMRK KEPE\] GPYWXIVW MQEKI XLI TSPEVM^IH IQMWWMSR in thousands of spiral galaxies, and map the 3D structure of QEKRIXMG½IPHWSRXLI7YR *PY\HIRWMX]?Q.]A The Obscured Universe ¯ Phenomena such as star formation and accretion onto massive :IPSGMX]SJJWIX?OQWA black holes occur behind dense screens of dust and gas that render optical and infrared observations impossible. The EVLA The CO(2-1) emission [MPPSFWIVZIXLVSYKLXLIWIWGVIIRWXSTVSFIXLIEXQSWTLIVIW from the most distant SJKMERXTPERIXWQIEWYVIXLIVQEPNIXQSXMSRWMR]SYRKWXIPPEV hyper-starburst galaxy SFNIGXW ERH MQEKI XLI HIRWIWX VIKMSRW MR RIEVF] WXEVFYVWX (AzTEC-3), at z = 5.3, galaxies. about 1 billion years after the Big Bang. This EVLA The Transient Universe data shows the cold gas %WXVSRSQMGEP XVERWMIRX WSYVGIW XIRH XS FI GSQTEGX SFNIGXW XLEX IQMX fueling the star formation and indicates more than 1010 solar masses of dense gas synchrotron radiation from high-energy particles, radiation best observed in this still-forming elliptical galaxy (Riechers et al, 2010). EXVEHMS[EZIPIRKXLW8LI):0%[MPPFIMHIEPJSVWXYHMIWSJZEVMEFPIWSYVGIW because of its high sensitivity, ability to observe day and night under most The supernova remnant (SNR) G93.3 at [IEXLIVGSRHMXMSRWERHXLIVETMHVIWTSRWIIREFPIHF]H]REQMGWGLIHYPMRK 5 GHz. Predictions indicate there should 8LI):0%[MPPMQEKIRSZEIERHVIPEXMZMWXMGNIXWER][LIVIMRXLI1MPO];E] be many more Galactic SNRs than are ERHQIEWYVIXLIWM^IWSJQER]XIRWSJKEQQEVE]FYVWXWIEGL]IEV known. SN remnants are typically hidden The Evolving Universe by the Galactic Plane and detectable Radio telescopes can trace the evolution of neutral hydrogen only at radio wavelengths. A single EVLA and molecular gas, and provide extinction-free measurements of observation can provide data on the W]RGLVSXVSR XLIVQEP JVIIJVII ERH HYWX IQMWWMSR 8LI ):0% [MPP IQMWWMSRQIGLERMWQWERHQEKRIXMG½IPH HMWXMRKYMWL HYWX JVSQ JVIIJVII IQMWWMSR MR HMWOW ERH NIXW [MXLMR strengths in these and other radio sources, PSGEP WXEVJSVQMRK VIKMSRW ERH [MPP QIEWYVI XLI WXEVJSVQEXMSR VEXI inside and outside our Galaxy. MVVIWTIGXMZISJHYWXI\XMRGXMSRMRLMKL^KEPE\MIW
CHARACTERISTICS 100 Continuum Sensitivity + in 12 Hours + 2I[HMKMXEPIPIGXVSRMGWERHQSHIVRHMKMXEP[MHIFERHGSVVIPEXSV + MicroJy *YPPJVIUYIRG]GSZIVEKIJVSQXS+,^ VLA
in 10
*MFIVSTXMGXVERWQMWWMSRW]WXIQERHRI[SRPMRIGSRXVSPW]WXIQ + +
Noise + ERXIRREW
6IWSPYXMSR EVGWIG (GSR½KYVEXMSR XSEVGWIG %GSR½KYVEXMSR EX+,^ R.M.S. EVLA -QEKMRK*MIPHSJ:MI[ EVGQMRYXIWEX+,^0EVKIV½IPHWEZEMPEFPIXLVSYKLQSWEMGMRK 1
1 10 Frequency in GHz SPECIFICATIONS Parameter VLA EVLA Continuum sensitivity in 12 hrs. 1Ʊ Ü.] Ü.] 1E\MQYQFERH[MHXL +,^ +,^ 2YQFIVSJJVIUYIRG]GLERRIPWEXQE\MQYQFERH[MHXL 1E\MQYQRYQFIVSJJVIUYIRG]GLERRIPW *VIUYIRG]GSZIVEKI+,^ Number of baselines 351 351 7TEXMEP6IWSPYXMSR +,^ EVGWIG EVGWIG
5 Image courtesy of NRAO/AUIImage courtesy Robert C. Byrd Green Bank Telescope (GBT) Green Bank, West Virginia
The Green Bank Telescope (GBT) is the premier single-dish radio XIPIWGSTI STIVEXMRK EX GIRXMQIXIV ERH QMPPMQIXIV [EZIPIRKXLW -XW VIGIMZIVWI\XIRHJVSQ1,^+,^[MXLETM\IPFSPSQIXIV EVVE]EX +,^MRVSYXMRISTIVEXMSRERHE +,^LIXIVSH]RI receiver under construction for 4mm band spectroscopy. The GBT has EWYMXISJHIXIGXSVWSTXMQM^IHJSVWTIGXVSWGST]TYPWEVSFWIVZEXMSRW continuum, and very long baseline interferometry (VLBI). Located MR XLI 2EXMSREP 6EHMS 5YMIX >SRI XLI +&8 FIRI½XW JVSQ E PS[ radio-frequency interference environment. The GBT surface has an EGGYVEG]SJÜQ]MIPHMRKERETIVXYVIIJ½GMIRG]SJ EX +,^ 3FWIVZEXMSRWEVIWGLIHYPIHH]REQMGEPP]XSQEXGLWGMIRXM½GVIUYMVIQIRXWXSXLI[IEXLIVGSRHMXMSRW
+6))2&%2/8 )0)7'34)'%1)6%():)0341)28463+6%1 8LI26%3MWHIWMKRMRKFYMPHMRKERHGSQQMWWMSRMRKRI[GEQIVEW]WXIQWXLEX[MPPTVSZMHIXLIRI\XUYERXYQPIETMR+&8WGMIRGIGETEFMPMXMIW including conventional feed horn arrays, phased array receivers, and bolometer arrays. The camera development program is a collaboration FIX[IIRXLI26%3ERHQSVIXLERX[IRX]YRMZIVWMX]GSPPIKIERHMRHYWXV]VIWIEVGLKVSYTW
Multiplexed SQUID TES Array at Ninety Gigahertz: MUSTANG Bolometer Array 8LI1978%2+TM\IPFSPSQIXIVEVVE]GSZIVMRK +,^ QQ MWMRVSYXMRIYWIEXXLI+&8ERHEQSVIIJ½GMIRXTM\IPEVVE]MW YRHIVHIZIPSTQIRX1978%2+SRXLI+&8LEWERERKYPEVVIWSPYXMSRSJ EVGWIGSZIVE\EVGWIGJYPP]WEQTPIH½IPHSJZMI[
K-Band Focal Plane Array 8LITM\IPHYEPTSPEVM^EXMSREVVE]SJLIXIVSH]RIVIGIMZIVWJSV +,^ MW RS[ EZEMPEFPI JSV VIKYPEV YWI8LSYKL STXMQM^IH JSV
mapping in the NH3 lines it can be used for other species. Receiver XIQTIVEXYVIWEVIb/EGVSWWXLIFERHKMZMRKXSXEP^IRMXLW]WXIQ XIQTIVEXYVIW EW PS[ EW / MR KSSH [IEXLIV EX ER ETIVXYVI IJ½GMIRG]SJ %RI[WSJX[EVITMTIPMRIEPPS[WRIEVVIEPXMQI data reduction.
W-Band Focal Plane Array 4VIPMQMREV]HIWMKR[SVOMWYRHIV[E]SREPEVKIJSVQEXLIXIVSH]RI focal-plane array for use in the upper end of the 3mm band.
Phased Array Receiver Development 8LI 26%3 MW [SVOMRK [MXL &VMKLEQ=SYRK 9RMZ XLI 9RMZ SJ Massachusetts, and other groups on the development of phased
Early science from the K Band Focal Plane Array. NH3 (1,1) integrated intensity contours EVVE]XIGLRSPSK][MXLXLIKSEPSJFYMPHMRKWIRWMXMZIQYPXMTM\IPEVVE]W are shown on a Spitzer Space Telescope image of the dark cloud surrounding the JSVXLI+&8%TVSXSX]TIFIEQW]WXIQEX+,^MWFIMRKFYMPX I\XVIQIP]]SYRK7IVTIRW7SYXLGPYWXIV8LI½IPHMW \EVGQMR+&8SFWIVZEXMSRW primarily for engineering tests, but it may also be competitive as a probe the cloud’s physical properties at a resolution of 0.06 pc (Friesen et al 2010). pulsar search instrument and for extended HI structure mapping.
6 NEW DIGITAL SIGNAL PROCESSORS 8LI+VIIR&ERO9PXMQEXI4YPWEV4VSGIWWMRK-RWXVYQIRX +944- MWE½IPHTVSKVEQQEFPIKEXIEVVE] *4+% FEWIHTYPWEVTVSGIWWMRKMRWXVYQIRX XLEXTVSZMHIW 1,^FERH[MHXLW[MXL WTIGXVEPGLERRIPWJYPP7XSOIWTEVEQIXIVWERHMRXIKVEXMSRXMQIWEWWLSVXEW ÜWIG8LI+944-GSLIVIRXHIHMWTIVWMSRQSHIWEVIRS[EZEMPEFPI+944-MWEGSPPEFSVEXMSRFIX[IIRXLI26%39'&IVOIPI]9RMZSJ 'MRGMRREXMERH 2);6)')-:)6*3674)'8637'34=%811 %QQHYEPFIEQVIGIMZIVMWFIMRKFYMPXXSGSZIV +,^-XWOI]WGMIRGIHVMZIVMWQSPIGYPEVWTIGXVSWGST]ERH:0&-SFWIVZEXMSRW[MPPEPWS FIWYTTSVXIH'SQQMWWMSRMRK[MXLXLITSWWMFMPMX]SJWLEVIHVMWOWGMIRGISFWIVZEXMSRWMWI\TIGXIHMRPEXI KEY SCIENCE Figure-2: This GBT velocity dispersion map of NH3 lines in a dark cloud WLS[WJSVXLI½VWXXMQIXLIXVERWMXMSR between the supersonic turbulent SYXIVPE]IVWERHXLIWQSSXL¾S[SJ the inner parts as it collapses into new stars (Pineda et al 2010). Fundamental Physics The Structure and Evolution of Galaxy Clusters ;MXL MXW WIRWMXMZMX] [MHI WO] GSZIVEKI ERH WXEXISJXLIEVX 8LI1978%2+QQFSPSQIXIVEVVE]LEWVIZIEPIHLMXLIVXSYRORS[R instrumentation, the GBT is a premier instrument for studying pulsars WXVYGXYVIWMRXLILSXKEWSJKEPE\]GPYWXIVW1978%2+SFWIVZEXMSRW ERHSXLIVGSQTEGXSFNIGXWXLEXTVSFIJYRHEQIRXEPTL]WMGW8LI+&8 of the Sunyaev-Zel’dovich (S-Z) effect reveal the presence of shock- is also vital to the on-going efforts to directly detect gravitational LIEXIHKEWXLEXMWSXLIV[MWIHMJ½GYPXXSHIXIGX7IZIVEPGPYWXIVWWLS[ radiation by timing an array of pulsars around the sky. this distinctive sign of mergers, the remnants of the processes that have formed them. Star Formation With good angular resolution and sensitivity to extended sources, Origin of Life XLI+&8LEWQEHIXLI½VWXHI½RMXMZIHIXIGXMSRSJXLIXVERWMXMSRJVSQ Determining the origin of life on Earth requires research across XYVFYPIRXXSGSLIVIRX¾S[MRXLIHIRWIGSVISJEWXEVJSVQMRKHEVO FMSPSK]GLIQMWXV]TL]WMGWERHEWXVSRSQ]8LI+&8[MPPTPE]EQENSV cloud. By mapping NH3 transitions, Pineda et al (2010) discovered a ERH YRMUYI VSPI MR XLMW [SVO F] QIEWYVMRK MRXIVWXIPPEV GLIQMGEP WLEVTFSYRHEV]FIX[IIRWYTIVWSRMGERHWYFWSRMGXYVFYPIRXQSXMSRW processes and their variation across the Milky Way, determining the XLEXREXYVEPP]HI½RIWEHIRWIGSVIERHWYKKIWXWEWLSGOSVSXLIV characteristics and extent of pre-biotic chemistry in star-forming instability for its origin. regions, and by rapid imaging of the molecular content of comets in our Solar System. GBT on the World Wide Web LXXT WGMIRGIRVESIHYKFX 7 The Very Long Baseline Array (VLBA) is an interferometer of 10 Very Long Baseline Array (VLBA) MHIRXMGEPERXIRREW[MXLFEWIPMRIPIRKXLWYTXS OQ 1EYRE/IE St. Croix, VI Hancock, NH North Liberty, IA ,E[EMMXS7X'VSM\:MVKMR-WPERHW 8LI:0&%MWGSRXVSPPIHVIQSXIP] JVSQXLI7GMIRGI3TIVEXMSRW'IRXIVMR7SGSVVS2I[1I\MGS)EGL Fort Davis, TX Los Alamos, NM :0&%WXEXMSRGSRWMWXWSJEQERXIRREERHEREHNEGIRXGSRXVSP 4MI8S[R21/MXX4IEO%>&VI[WXIV;% FYMPHMRK8LIVIGIMZIHWMKREPWEVIEQTPM½IHHMKMXM^IHERHVIGSVHIH 3[IRW:EPPI]'%1EYRE/IE,- on fast, high capacity recorders. The recorded data are sent from the individual VLBA stations to the correlator in Socorro. 8LI:0&%SFWIVZIWEX[EZIPIRKXLWSJ GQXSQQ +,^XS +,^ MRIMKLXHMWGVIIXFERHWTPYWX[SREVVS[WYFKMKELIVX^FERHW 2I[VIGIMZIVWEVIFIMRKHIZIPSTIHJSVXLI:0&%XLEXEVIGETEFPISJXYRMRKFIX[IIRERH +,^ERHEVII\TIGXIHXSFIEZEMPEFPIMRQMH 8LIEVVE]GERFIWGLIHYPIHH]REQMGEPP]ERHMXWGSRXMRYYQWIRWMXMZMX]GERFIMQTVSZIHWMKRM½GERXP]F]EHHMRKXLI+VIIR&ERO8IPIWGSTI and, soon, the phased Expanded Very Large Array. VLBA on the World Wide Web LXXT WGMIRGIRVESIHYZPFE 8 KEY SCIENCE Precision astrometry is a VLBA science centerpiece. The relative astrometric EGGYVEG]SJbÜEWEGLMIZEFPI[MXLXLI:0&%JSVI\EQTPIMWFIXXIVXLERXLI +EMEWEXIPPMXIMWHIWMKRIHXSEGLMIZIJSVQSWXWXEVWMRMXWGEXEPSK9RPMOI+EMEXLI :0&%GERTVSFIXLI+EPEGXMGTPERI[IPPFI]SRHXLIWSPEVRIMKLFSVLSSHFIGEYWI the radio emission is affected little by extinction. In 2010, the VLBA began a long-term program to determine the 3D structure of XLI 1MPO];E] F] QIEWYVMRK TEVEPPE\IW [MXL ÜEW EGGYVEG] SV FIXXIV XS b high-mass star-formation regions. This program is expected to eventually measure the JYRHEQIRXEP KEPEGXMG VSXEXMSR TEVEQIXIVW [MXL EGGYVEG]LIPTMRK XS UYERXMJ] XLI distribution of luminous and dark matter in the Galaxy. The VLBA is also expected to anchor High Sensitivity Array observations of the center SJ1MRERIJJSVXXSHIXIGXXLIKEPE\]´WRYGPIYW[MXLWMKRM½GERXWMKREPXSRSMWIERH IREFPIE½VWXITSGLTSWMXMSRQIEWYVIQIRX8LIYPXMQEXIKSEPMWXLITVSTIVQSXMSR SJ1VIPEXMZIXSXLI1MPO];E][LMGLWLSYPHLIPTHMWXMRKYMWLFIX[IIRWGIREVMSW proposed for the formation of the Local Group and provide a measurement of the The Bar and Spiral Structure Legacy Survey program (Mark mass of M31 and its dark-matter halo. Reid et al.) will measure accurate distances and proper motions for about 400 high-mass star-forming regions in the 8LI2%7%*IVQM+EQQEVE]7TEGI8IPIWGSTIVIPIEWIHMXW½VWXKEQQEVE]WSYVGI Milky Way between 2010 and 2015. This survey will yield GEXEPSKMR -RXLI:0&%[MPPTEVXMGMTEXIMRWIZIVEPGSSTIVEXMZISFWIVZEXMSREP accurate distances to most of the high-mass star-forming TVSKVEQW[MXL*IVQM8LIWITVSKVEQW[MPPJSGYWSREGXMZIKEPEGXMGRYGPIMSVFPE^EVW regions in our Galaxy that are visible from the northern WIZIVEPXLSYWERHSJ[LMGLWLSYPHFIHIXIGXIHF]*IVQMSZIVXLIRI\XJI[]IEVW hemisphere, as well as very accurate measurements of A long-term VLBA program to study Active Galactic Nuclei containing central H2O fundamental parameters such as the distance to the Galactic QIKEQEWIVW[MPPGSRXMRYI8LMWTVSKVEQLEWX[STVMQEV]WGMIRXM½GKSEPW EGUYMVI center, and the Milky Way rotation velocity and rotation curve. geometric distance measurements that enable an accurate determination of the Credit: IPAC-R. Hurt/CfA-Mark Reid/NRAO/AUI/NSF. ,YFFPI'SRWXERXERHVIPEXIHHEVOIRIVK]TEVEQIXIVW ERH HMVIGXP]QIEWYVIXLI QEWWIWSJGIRXVEPFPEGOLSPIW[MXLEGGYVEGMIWSJEXPIEWX QYGLFIXXIVXLERER]SXLIVXIGLRMUYIYWIHJSVWSYVGIWSYXWMHIXLI1MPO];E] 7)27-8-:-8=)2,%2')1)28463+6%1 %XMXW HIHMGEXMSRXLI:0&%WIRWMXMZMX][EWPMQMXIHF]XLIEZEMPEFPIFERH[MHXL1,^MRHYEPTSPEVM^EXMSR8IGLRSPSK]TVSKVIWWIHLS[IZIV ERHWYFWXERXMEPMRGVIEWIWMRFERH[MHXLERHGSRXMRYYQWIRWMXMZMX]FIGEQIEJJSVHEFPI8LYWWMRGIXLIEVVE]´WHIHMGEXMSRXLI26%3LEWUYEHVYTPIH XLIEZEMPEFPI:0&%FERH[MHXLERHXLI3FWIVZEXSV][MPPUYEHVYTPIMXEKEMRMR8LMWIRLERGIQIRXERHSXLIVWIRWMXMZMX]MQTVSZIQIRXWEVI FIMRKYRHIVXEOIR[MXLSYVMRXIVREXMSREPTEVXRIVWXSTVSZMHIRI[WGMIRXM½GGETEFMPMXMIWJSVXLI:0&%YWIVGSQQYRMX] VLBA MILESTONES 2007:8LI26%3MRGSPPEFSVEXMSR[MXLXLI9'&IVOIPI]'%74)6ERH7SYXL%JVMGER/%8KVSYTWERH[MXL1-8,E]WXEGO 3FWIVZEXSV]MRMXMEXIHHIZIPSTQIRXSJERI[:0&%HMKMXEPFEGOIRHXSHMKMXM^IXLIIRXMVIWTERSJXLIX[SEZEMPEFPI1,^ intermediate frequency channels. 2008:-RTEVXRIVWLMT[MXLXLI1E\4PERGO-RWXMXYXJYV6EHMSEWXVSRSQMIGSQTPIXIHXLI+,^EQTPM½IVVITPEGIQIRXVIWYPXMRKMR WIRWMXMZMX]MQTVSZIQIRX 2010: 'SQTPIXIHGSRZIVWMSRSJXLI:0&%XSLMKLIVFERH[MHXLWSJX[EVIGSVVIPEXSV-RMXMEPHITPS]QIRXSJRI[VIGSVHMRKW]WXIQEX ERXIRREWXEXMSRW-RMXMEXIHGSRZIVWMSRSJ:0&%XSWYFWGVMFIVJEGMPMX][MXLERIQTLEWMWSR/I]7GMIRGI4VSNIGXW 2009-2011:)\TERHHEXEVIGSVHMRKQIHMETSSPERHWSJX[EVIGSVVIPEXSVTVSGIWWSVGPYWXIV'SQTPIXIJYPPGSVVIPEXSVGSQQMWWMSRMRK 2011:'SQTPIXIMQTPIQIRXEXMSRSJ1,^FERH[MHXLGETEFMPMX]ERHRI[:0&%HMKMXEPFEGOIRHW Student & Visitor Programs Summer Student Programs Summer students conduct research at the NRAO under the supervision SJEWGMIRXM½GWXEJJQIQFIVMR7SGSVVS+VIIR&EROSV'LEVPSXXIWZMPPI 8LITVSNIGXQE]MRZSPZIER]EWTIGXSJEWXVSRSQ]ERHSJXIRVIWYPXW MRWGMIRXM½GNSYVREPTYFPMGEXMSRW7XYHIRXWVIGIMZIVIPSGEXMSRWYTTSVX a monthly stipend, and partial support may be available to present summer research results at an American Astronomical Society meeting. Students also participate in an extensive lecture series. 9RHIVKVEHYEXIWXYHIRXW[LSEVI97GMXM^IRWSVTIVQERIRXVIWMHIRXW EVIIPMKMFPIJSVXLI26%36IWIEVGL)\TIVMIRGIWJSV9RHIVKVEHYEXIW 6)9 TVSKVEQ7XYHIRXW[LSHSRSXQIIX6)9KYMHIPMRIWQE]FI IPMKMFPI XS ETTP] JSV XLI 26%3 9RHIVKVEHYEXI 7YQQIV 7XYHIRX Research Assistantship program. First and second year graduate students are eligible to apply for the NRAO Graduate Summer Student Research Assistantship program. Applications are due at the end of January each year. Co-op Program 8LI26%3LEWHIZIPSTIHVIPEXMSRWLMTW[MXLQER]97YRMZIVWMXMIW [MXL WXVSRK IRKMRIIVMRK ERH GSQTYXIV WGMIRGI HITEVXQIRXW )EGL semester the NRAO sponsors one or more paid undergraduate WXYHIRXW8LIWIGSSTWXYHIRXWRSVQEPP]NYRMSVWERHWIRMSVWWTIRHXLVIIEPXIVREXMRKWIQIWXIVW[SVOMRK[MXLER26%3QIRXSV8]TMGEPGS op assignments include engineering tasks related to the design, prototyping, testing, or production of radio astronomical instrumentation or programming tasks related to radio telescope monitor and control. Graduate Student Internships The Graduate Student Internship program is for students in the IEVP]]IEVWSJEKVEHYEXITVSKVEQ[LSEVIMRXIVIWXIHMRVEHMS EWXVSRSQ]SVVIPEXIHVIWIEVGL7XYHIRXW[LSEVI97GMXM^IRWSV TIVQERIRXVIWMHIRXWEVIIRVSPPIHMREREGGVIHMXIH97KVEHYEXI TVSKVEQSV[LSEVISXLIV[MWIIPMKMFPIXS[SVOMRXLI97[MPP receive a stipend. Some travel and housing assistance may also FIEZEMPEFPI%TTSMRXQIRXWQE]FIQEHIJSVTIVMSHWJVSQEJI[ [IIOWXSWM\QSRXLW%R26%3WXEJJQIQFIVWYTIVZMWIWIEGL student. Pre-Doctoral Research Program The NRAO pre-doctoral research program supports upper- PIZIP KVEHYEXI WXYHIRXW [LS LEZI GSQTPIXIH XLIMV EGEHIQMG institution’s requirements for becoming doctoral candidates. Astronomy, engineering, and computer science students are IRGSYVEKIH XS TEVXMGMTEXI 9RHIV XLI NSMRX WYTIVZMWMSR SJ ER 10 26%3WXEJJQIQFIVERHLMWLIVEGEHIQMGEHZMWSVXLIWXYHIRXTYVWYIWVIWIEVGLJYPPXMQIXS[EVHGSQTPIXMSRSJEHSGXSVEPHMWWIVXEXMSR%R 26%3WGMIRXMWXSVEWXYHIRX´WEGEHIQMGEHZMWSVRSQMREXIWXLIQJSVXLITVSKVEQ7XYHIRXWQE]FIWYTTSVXIHJSVWM\QSRXLWXSX[S]IEVWSV PSRKIV[LMPIXLI][SVOEXER26%3WMXI%TTPMGEXMSRWEVIEGGITXIHXLVSYKLSYXXLI]IEVXLSYKLGERHMHEXIWEVIWXVSRKP]IRGSYVEKIHXSWIIO the support of an NRAO scientist before applying. Student Observing Support Program 8SLIPTXVEMRRI[KIRIVEXMSRWSJWGMIRXMWXWXLI26%3WYTTSVXWVIWIEVGLF]KVEHYEXIERHYRHIVKVEHYEXIWXYHIRXWEX97YRMZIVWMXMIWERH colleges. Regular observing time proposals submitted for the GBT, VLBA, and the High Sensitivity Array (HSA) are currently eligible for funding under this program, though regular VLA proposals are not. Large Proposals for the VLBA, GBT, HSA, VLA, and any combination of these telescopes, are also eligible. Visitor Program 8LI:MWMXSV4VSKVEQMWSTIRXS4L(WGMIRXMWXWERHIRKMRIIVWMRVEHMSEWXVSRSQ]ERHVIPEXIH½IPHW[LS[MWLXSZMWMXER26%3WMXIXS GSPPEFSVEXI[MXL3FWIVZEXSV]WXEJJ8LI26%3MWTEVXMGYPEVP]MRXIVIWXIHXSWYTTSVXZMWMXWF]NYRMSVJEGYPX]EXGSPPIKIWERHYRMZIVWMXMIWERHXS IRGSYVEKIGSPPEFSVEXMSRWXLEXGERPIEHXS±½VWXPMKLX²WGMIRGI[MXLRI[MRWXVYQIRXW:MWMXXIVQWEVIRIKSXMEFPIERHXLIMVPIRKXLQE]VERKI JVSQEJI[[IIOWXSWIZIVEPQSRXLW NRAO Student & Visitor Programs on the World Wide Web LXXT WGMIRGIRVESIHYSTTSVXYRMXMIW 11 (above) 8LMWMQEKISJXLIWTMVEPKEPE\]1XLI;LMVPTSSP+EPE\]ERHMXWGSQTERMSR2+' GSQFMRIW SFWIVZEXMSRWSJRIYXVEPL]HVSKIRIQMWWMSREGUYMVIHEXXLI26%3:IV]0EVKI%VVE][MXLSTXMGEPMQEKIW 6& JVSQXLI7IGSRH4EPSQEV3FWIVZEXSV]7O]7YVZI]787G-(MKMXEP7O]7YVZI]8LISTXMGEPHEXEWLS[ the emission of stars and dust in these galaxies, foreground stars in our Galaxy, and some background KEPE\MIW8LIVEHMS[EZIPIRKXLWTIGXVEPPMRISFWIVZEXMSRWSJRIYXVEPEXSQMGL]HVSKIR HITMGXIHF]FPYMWL LYIW MPPYWXVEXIXLIHMWXVMFYXMSRERHOMRIQEXMGWSJXLMWKEW8LIPSRKXMHEPXEMPSJRIYXVEPL]HVSKIR[EWWLEOIR PSSWIF]XLIHERGISJXLIWIX[SKEPE\MIW-RZIWXMKEXSVW %,6SXW 26%3 .1ZERHIV,YPWX +VSRMRKIR 4)7IMHIR -&1 6'/IRRMGYXX 1MRRIWSXE 4''VERI 26%3 %&SWQE 1EVWIMPPI 0%XLEREWWSYPE +VSRMRKIR ERH(1)PQIKVIIR -&1ERH:EWWEV -QEKIGSQTSWMXMSR .19WSR 26%3 (right) Radiation emitted by atomic hydrogen reveals a gas shell surrounding an interstellar bubble, sculpted by XLI[MRHERHVEHMEXMSRJVSQLSXQEWWMZIWXEVWERHXLIWLSGO[EZIWKIRIVEXIHF]WYTIVRSZEI/RS[R EWKEPEGXMGWLIPP+7 XLMWFYFFPIMWEXEHMWXERGISJPMKLX]IEVWERHQIEWYVIWEFSYX F]PMKLX]IEVW8LMWMQEKIWLS[WSRP]EWQEPPTEVXSJEWYVZI]XLEXYWIWXLI26%3:IV]0EVKI Array and the Green Bank Telescope to trace the cool gas in our Galaxy. The gas has been colored TYVTPIFPYIERHKVIIR XLIFVMKLX]IPPS[SVERKIHSXWEVIGPYWXIVWSJ]SYRKQEWWMZIWXEVWWYVVSYRHIH F]LSXKEWPSGEXIHGPSWIVXSYWXLERXLIFYFFPI LIEXIHHYWXMQEKIHMRXLIMRJVEVIHF]XLI1MHGSYVWI 7TEGI)\TIVMQIRX 17< WEXIPPMXIMWWLS[REWVIH-RZIWXMKEXSVW .17XMPERH%68E]PSV 'EPKEV] .1(MGOI] 8EWQERME (;/EZEVW 1MRRIWSXE 4+1EVXMR '-8%8SVSRXS 8%6SXL[IPP 8SVSRXS %-&SSXLVS]H '-8% *IPM\.0SGOQER 26%3 ERH211G'PYVI+VMJ½XLW %YWXVEPME 8IPIWGSTI -QEKIGSQTSWMXMSR .)RKPMWL 1ERMXSFE .17XMPERH%68E]PSV 'EPKEV] 12 13 NRAO Headquarters and North American ALMA Science Center National Radio Astronomy Observatory 520 Edgemont Road 'LEVPSXXIWZMPPI:MVKMRME 211 NRAO - Green Bank National Radio Astronomy Observatory P. O. Box 2 +VIIR&ERO;IWX:MVKMRME 304-456-2011 NRAO - Pete V. Domenici Science Operations Center National Radio Astronomy Observatory P. O. Box 0 7SGSVVS2I[1I\MGS 575-835-7000 NRAO/AUI - Chile 26%3%9- %Z2YIZE'SWXERIVE Suite 502 Vitacura Santiago Chile The National Radio Astronomy Observatory is a facility of the National Science Foundation operated by Associated Universities, Inc.