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Pos(EVN 2014)001 Ante Portas

Pos(EVN 2014)001 Ante Portas

PoS(EVN 2014)001 ante portas. http://pos.sissa.it/ † [email protected] abc , is a collaboration of the major astronomical institutes in ‡ and Eduardo Ros a ∗ azensus@mpifr-.mpg.de Speaker. The authors are grateful to R.W. Porcas forThe careful reading European of VLBI the manuscript Network and is useful comments a and joint suggestions. facility of European, Chinese, South African and other radio The European VLBI Network Europe, Asia, and Puertostantly Rico. improved Established its four performance decades in ago, terms sincewith made then improvements using it in resolution, has data performance, con- bit-rate and and theThe image addition EVN fidelity of provides new open stations skies and accesscontribution observing we and capabilities. discuss has the over present time status become anding a environment, perspectives especially for common-user in the facility. the array era In of in ALMA this a and continuously with chang- the ∗ † ‡ Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. Max-Planck-Institut für Radioastronomie Observatori Astronòmic, Universitat de València Departament d’Astronomia i Astrofísica, Universitat de València c

institutes funded by their national research councils. Auf dem Hügel 69, D-53121 Bonn, C. Catedrático José Beltrán 2, E-46980 Paterna, València, Spain C. Dr. Moliner 50, E-46100 Burjassot,E-mail: València, Spain 12th European VLBI Network Symposium and7-10 Users October Meeting 2014 Cagliari, Italy J. Anton Zensus European VLBI Network: Present and Future c a b PoS(EVN 2014)001 ] 3 ] ]. Ini- 6 2 , , 5 1 J. Anton Zensus ] ]. 8 , 13 7 ]. 10 303 [ ◦ including JIVE. Overall EVN policy is ] 1 9 2 . ] 4 ], and feedback in the jet of the radio loud 4C +12.50 [ 12 , 11 http://www.evlbi.org/contact/ See Since 1980 many stations have been added to the network: Medicina (1984), Wettzell (1995), Data were initially correlated at the MPIfR processing centre in Bonn. The Joint Institute for The addressed by EVN observations has covered a broad range of topics with a high At present the EVN comprises 14 major institutes After successful VLBI observations using European in the late 1960s and intra- 1 a study of a sample of radio [ investigation of methanol masers (a uniqueimaging EVN of capability gravitational for lenses many such years) as [ B0218+35.7 [ examining the dynamics of the compact symmetric objects 0710+439 and 0108+388 [ imaging of radio jets in galactic objects such as LS I +61 the properties of compact steep-spectrum sources using radio observations at different scales [ • • • Recent publications with the largest number ofMilky citations Way [ per month report astrometric studies of the • • Noto (1989), Shanghai, Metsähovi andTorun-32m Cambridge-32m (1996), (1990), Arecibo Yebes-14m and andwork: Hartebeesthoek Urumqi (1994), (2001), Svetloe, Yebes-40m Zelenchukskaya (2008), andTamna (2014). the Badary The KVAZAR Sardinia-64m (2009), net- and and Tianma-65m will recently start the regular participation KVN: in 2015. Yonsei,VLBI Ulsan in Europe, and established inand 1993, EVN is currently user tasked support. with Abeen data new correlation replaced correlator and by was postprocessing a dedicated software insince correlator, 1998, foundation, SFXC. both and in The in terms EVN recent of antenna has yearsby performance constantly this the and data improved has Mk bit-rate, II its now from system capabilities thebackends. in 4 Mbps 1980 provided to the plans for 2 Gbps inscientific 2015 impact. using Several the hundred Mk refereed V papersmost system make cited use with works of digital include: observations from the network; the • tially it was a 4-station network (Dwingeloo/Westerbork,very Effelsberg, Jodrell beginning and a Onsala). program From committee the posals (the submitted EVNPC) 3 was times established per and year.and reviewed A this observing scheduler task pro- to was coordinatetook observations performed this was by over appointed in different in 2014. individuals 1982, at the MPIfR until Alastair Gunn (Jodrell) 2. Present EVN set by the Consortium Boardinvestigations of of Directors. high EVN brightness-temperature science objects topics emitting cover non-thermal a radiation, broad range; atomic they and include European observations in the earlyAfter 1970s, several discussions meetings about a the European Europeanfounding array radio VLBI date astronomy Network back institutes was to (MPIfR, formally IRA, 1975. description ASTRON, of established OSO, the in and early Jodrell 1980 times Bank). with of A five the detailed network has been published in recent conferences [ EVN: Present & Future 1. A very short history of the EVN PoS(EVN 2014)001 J. Anton Zensus ]. Additionally, the desire . For observations at 3.5 mm, 14 3 . . . ]. EVN as a ground array is a key element 16 3 . The status of the telescopes, receiver availability, ob- 2 ] in this conference). 17 has the same collecting area as two 30-m dishes. The first results . 4 Spektr-R ] and currently RadioAstron [ In its early days VLBI was confined to centimetre wavelengths where observing 15 The EVN performs observations with disk recording (standard EVN, three sessions As mentioned above the KVN recently joined the EVN. Its 3 antennas (with separa- http://www.evlbi.org/user_guide/EVNstatus.txt http://www.evlbi.org/proposals/call.txt http://www3.mpifr-bonn.mpg.de/div/vlbi/globalmm/ See See See 3 2 4 2.1 Recent highlights Technical for longer baselines has pushed VLBIin to the have late elements in 1990s Earth [ orbit, first with the VSOP project Observing of three weeks each perof-session year) scheduling or has in been realto introduced time a recently (e-VLBI, maximum in of 10 144 blocks sessionsregular hours per of sessions. per Observations year, up year), are each possible to for at of specific 12 92,length. 24h). purposes 49, hours 30, which Joint 21, of Out- justify observations 18, duration observations 13, with 6, outside (up also the 5, of include Very 3.6, the Long 1.3, Green and Baseline Bank 0.7 Array cm Telescopecan wave- and (VLBA), the currently (’Global’ phased use proposals) up can Very Large topossible Array. as 1 Global Gbps well. proposals Following data the bit Korean2014, VLBI rate. it Network is joining Joint the planned observationswith EVN that as the somestarting an joint RadioAstron associate in time project member with 2015, in are the creating Australianare Long a announced Baseline real Array in global will every be array. call available, for The proposals details and updatesastronomers can of use the the EVN Global performance IRAM, Millimetre Onsala VLBI and Array NRAO (GMVA), operated jointly by the MPIfR, supporting RadioAstron observations. Thethe small use dish of onboard areported large are dish spectacular such (see e.g., as [ Effelsberg together with serving modes, etc., is maintained by JIVE in the EVN status tables EVN: Present & Future molecular processes, synchrotron radiation andthe large emission. collecting The area high of sensitivityof many provided faint of by objects its such elements as makes young the radio supernovae. EVN especiallyEVN in suitable context for the study systems made it feasible; shorterlow wavelengths performance of suffered receivers, from and longer short wavelengths coherenceby were steadily affected times by increasing and the radio ionosphere relatively frequency and interference. plagued the Recent technical parameter developments space have expanded inand radio “software astronomy. telescopes” have Progress pushed insors towards processing longer of data wavelengths, the with from Square pathfinders thousandsin and Kilometre of detector precur- Array dipoles techniques (SKA), and suchshort-wavelength increasing telescopes, as the bandwidths LOFAR. recently have dedicated At Atacama triggeredray the Large (ALMA) the Millimetre/sub-millimetre same being Ar- advent time, the of most improvements as important. new-generation, an It element is in plannedof millimetre that ALMA, the VLBI as immediate arrays, a neighbourhood notably phasedthe of with array, will the nearby the observe super-massive galaxy aim black of M 87 holes investigating – at the the the morphology so-called Galactic Event Centre Horizon and in [ PoS(EVN 2014)001 11 . 5 . simulta- 15 coverage. ) Framework RadioNet v , rd u J. Anton Zensus ( RadioNet3 , in FP6 with , it continued in FP4 with 6 10 Access to the EVN of radio , Ref. 261525, programme FP7- and and currently 7 ]. It can also provide a very short 14 19 FARADAY , Ref. HPRI-CT-2001-50031, programme FP5- , Ref. HPRI-CT-1999-00045, programme FP5- and 9 , Ref. 026642, programme FP6-IST, funding scheme I3 - 4 RadioNet-FP7 , , Ref. 505818, programme FP6-INFRASTRUCTURES, subpro- 13 The and origin of the most compact cosmic radio , Ref. 227290, programme FP7-INFRASTRUCTURES, subprogramme , Ref. 283393, programme FP7-INFRASTRUCTURES, subprogramme EVN-ACCESS NEXPReS . The European VLBI network of radio telescopes The EVN is an excellent example of international cooperation in science. This , and in FP7 with 12 , in FP5 with the projects 8 http://goo.gl/Ca0dJH observations are possible at 13, 7, 3.5, and 2 mm wavelength; 13 and 7 mm are offered by Advanced in Europe Advanced Radio Astronomy in Europe NEXPReS- Novel EXplorations Pushing Robust e-VLBI Services RadioNet: Advanced Radio Astronomy in Europe EXPReS: a production astronomy e-VLBI infrastructure Focal-plane arrays for radio astronomy; design, access and yield See Ref. CHGE920011, programme FP3-HCM. Code FMGE980101, programme FP4-TMR. Code FMGE950012, programme FP4-TMR, subprogramme 0201 - Access for researchers, fundingEuropean scheme vlbi 0201 network via the joint institute for vlbi in europe As mentioned above the Tianma 65-m telescope will be available for EVN observations in In September 2014 the radome of the 20m-Onsala telescope was renewed. The top cap of 50 RadioAstron has performed joint observations with the EVN since early 2012,Recently combining a the new correlator developed at JIVE (UniBoard project, supported by RadioNet3, see Additional funding for EVN research activities was provided by programs such as the coop- EXPReS 5 6 7 8 9 ]) has successfully demonstrated 4 Gbps operation. When brought into operation the correlator 14 15 13 11 12 10 18 INFRASTRUCTURES, subprogramme INFRA-2010-1.2.3 - Virtual Research Communities. INFRA-2008-1.1.1 - Bottom-up approach: Integrating Activities in all scientific and technologicalINFRA-2011-1.1.21. fields. - Research Infrastructures for advanced radio astronomy. Research Infrastructure-Integrated Infrastructure Initiative. HUMAN POTENTIAL. gramme INFRASTR-2.1 - Integrating activities combiningprojects. cooperation networks with transnational access and research HUMAN POTENTIAL. - Access for researchers. 2015. It will operate with adaptiveFirst optics in fringes all with the the bands offered EVN by were the EVN obtained from in 21 cm March to 2014 7 mm. [ panels was replaced in one piece, and the remaining 570 elements were changed one by one will support 32 stations with 64 MHzresolution bandwidth, up integration times to of 15.625 0.022 kHz. s to 1 s, and a frequency high resolution provided by space VLBI with the high sensitivity of the[ EVN (see above). eration with the former Soviet Union by EVN: Present & Future tions up to 480 km) at theAn easternmost interesting edge feature of of the network these enhance telescopesneous remarkably is the their novel high-frequency capabilities,the since EVN for joint observations. baseline together with the Seshan 25-m telescope. EU Support collaborative aspect has been boostedCommission over via the different last funding instruments. twentyProgram years Following (FP3) by from with the support support inderEnhancing the of the 3 the European European VLBItelescopes Network of Radio Telescopes and PoS(EVN 2014)001 , 17 ]. 21 32 m × ], in setting 22 ) by building a J. Anton Zensus 22 also contributes to . 20 AstroNet ], or in the imaging of the 23 RadioNet3 . ESTRELA RADIO- 21 and , Ref. 19669, programme FP6-MOBILITY, , Ref. FMRX960034, programme FP4-TMR, 19 , Ref. FMRX960071, programme FP4-TMR, subpro- ANGLES , 5 , Ref. 505183, programme FP6-MOBILITY, subprogramme 18 . . CERES includes a transnational access programme (which supports ]. Methanol masers can be probed at 5 cm wavelength, and these , geodesy-related projects such as 20 16 Six dishes were recently added to the network (KVAZAR with 3 21 m in 2014). The telescopes in Sardinia (64-m) and Tianma (65-m) RadioNet3 × ]. Synergies with observations from telescopes at the very highest frequencies are 24 The future has now become the present, since the European Commission decided in ]. As reported above, the EVN has produced hundreds of scientific publications in several 25 http://www.astronet-eu.org/ http://www.radionet-eu.org/ See See Ref. INTAS-94-4010. Measurement of vertical crustal motion in Europe by VLBI The at high redshift and the of active galaxies fromAstrophysics multi-wave length Network studies for of Galaxy compact Lensing ra- Studies Early stage training site for European long-wavelength Astronomy The present I3 project 22 21 16 17 18 19 20 subprogramme MOBILITY-1.2 - Marie Curie Host Fellowships - Early stage research training (EST). 3. The future JIV-ERIC the course of writing this contribution toConsortium, allow initially JIVE with to four become member a countries European (TheFrance). Research Netherlands, In Infrastructure United addition, Kingdom, research Sweden councils and andGermany institutes and in other China countries – – will Italy, Spain,planned contribute South for to Africa, April JIVE 2015. as well. The official dedicationExpanding of the network the JIV-ERIC is are a reality and will increasingly participate in EVN observations in 2015. Further in the future dio sources - consortium for European research on extragalactic surveys The high sensitivity shows its full powerupper in the limits study of to ultraluminous the X-ray sources emission [ from radio supernovae, e.g.,possible, SN as 2014 in [ the casethe of EVN the [ blazar IC 310 in the Perseus cluster, studied jointly by MAGIC and in 2009 and KVN with 3 gramme 1.4.1.-3.1S4 - Environment and Geosciences. subprogramme 1.4.1.-3.1S7 - Physics. MOBILITY-1.1 - Marie Curie Research Training Networks (RTN). astrometric results complement astrometric studies performed at 1 cm with water masers, see [ EVN: Present & Future sources known in the Universe Crab nebula [ and research training networks such as EVN observations and data analysis), networkingthis activities conference), (which, and amongst joint other reseach things,tronomical activities support facilities to support in research Europe, anddescription including development of JIVE at the project the and and radio several itsthe as- goals EVN implementation is radio of provided the in telescopes. strategic its plan webpage A for European complete radio astronomy ( sustainable radio astronomical research community. Scientific areas; highlights are shown regularly onuseful the for EVN webpages. global Its experiments high andhelical fidelity for imaging features observations is in of especially 0836+710 complex [ jet structures, e.g., in the study of PoS(EVN 2014)001 J. Anton Zensus (2010) (2010) (2010) . Even when other facilities are threatened with 6 (2014) GAIA (2012) (2014) PoS(EVN 2014)020 PoS(10th EVN Symposium)053 PoS(10th EVN Symposium)011 PoS(10th EVN Symposium)098 In the future the EVN will continue being a key instrument in radio astronomy, PoS(RTS2012)005 ´ n. Furthermore, a beam-formed MeerKAT telescope would be an excellent addition to the http://goo.gl/5N7M6u [3] Fanti, R., et al., A&A[4] 231, 333-346Giovannini, (1990) G., et al., ApJ[5] 552, 508–526Owsianki, (2001) I. & Conway, J.E.,[6] A&A 337,Owsianik, 69–79 I., (1998) Conway, J.E., &[7] Polatidis, A.G.,Minier, A&A V., Booth, 336, R.S., L37 & (1998b) [8] Conway, J.E., A&ABeuther, 362, H., 1093–1108 et (2000) al., A&A[9] 390, 289–298Patnaik, (2002) A.R., et al., MNRAS 261, 435–444 (1993) [1] Porcas, R.W., [2] Booth, R.S., [15] Hirabayashi, H., et al., Science[16] 281, 1825Kardashev, N.S., (1998) et al., Astron.[17] Rep. 57,Kovalev, et Y.Y., 153–194 al., (2013) [18] Szomoru, A., [20] Perucho, M., et al., ApJ[21] 749, 55Rygl, (2012) K.L.J., et al., A&A[22] 539, A79Mezcua, (2012) M., et al., MNRAS[23] 436, 1546–1554Pérez-Torres, M.A., (2013) et al., ApJ[24] 792, 38Lobanov, (2014) A.P., et al., A&A[25] 533, A10 (2011) Aleksic, J., et al., Science 346, 1080–1084 (2014) [10] Massi, M., et al., A&A[11] 414, L1-L4Reid, (2004) M.J., et al., ApJ[12] 738, 130Xu, (2014) Y., et al., ApJ[13] 769, 15Morganti, (2013) R., et al., Science[14] 341, 1082Doeleman, (2013) S.D., [19] Shen, Z.Q., in 3rd China-U.S. Workshop on Radio Astronomy Science and Technology, see EVN: Present & Future are the planned 110-m telescopewhich in could Qitai, join near EVN observations, Urumqi, and andof also the Toru a FAST 70-m 500-m class telescope telescope in innetwork Poland to China, (RT90) the to South, the north withan a African short VLBI baseline array to are Hartebeesthoek alsoat being and centimetre developed, with and wavelengths, high this to sensitivity. would boost yield Plans radioKilometre an for Array. astronomy unprecendented coverage in the next years, complementing theNew Square frontiers complementing multi-messenger campaigns, in the study ofand transients, astrometric enhancing precision, its complementing image millimetre- fidelity and space-VLBI,for and astrometric as measurements a match in in the thefunding era radio cuts, of one of the strengthsflexible facility of for the many EVN years is in its the international future. nature, makingReferences a sustainable and

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