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PoS(ICRC2015)675 http://pos.sissa.it/ † ∗ [email protected] [email protected] Speaker. See full list of members of the TRAGALDABAS Colloboration at the end of the article Cosmic Rays are very usefulphenomena as for solar activity, getting magnetic cloud a detection realothers. and the In time high order information to atmosphere improve dynamics, of our among knowledge many ininstalled those Earth’s in fields, two surrounding , singular URAGAN and very in different detectors Moscow(), () have decided and to TRAGALDABAS joint in their S. efforts.have de Although very Compostela they different are performances, based both on different ofcosmic technologies them origin and offer allowing very a good regular and angular coordinatedover resolution a survey for big of muons region the of of arrival of the low north energy hemisphere. cosmic rays ∗ † Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. c

Igor I. Yashin National Research Nuclear University MEPhI (MoscowE-mail: Physics Institute), Moscow I.I. Astapov National Research Nuclear University MEPhI (Moscow Engineering Physics Institute),N.S. Moscow Barbashina National Research Nuclear University MEPhI (Moscow Engineering Physics Institute),A.N. Moscow Dmitriyeva National Research Nuclear University MEPhI (Moscow Engineering Physics Institute),A.A. Moscow Petrukhin National Research Nuclear University MEPhI (Moscow Engineering Physics Institute),V.V. Shutenko Moscow National Research Nuclear University MEPhI (Moscow Engineering Physics Institute), Moscow The 34th International Cosmic Ray Conference, 30 July- 6 August, 2015 The Hague, The Netherlands Juan A. Garzón for the TRAGALDABAS Collaboration URAGAN & TRAGALDABAS: two complementary approaches for the regular survey of Cosmic Rays LabCAF, F. Física. Univ. of Santiago deE-mail: Compostela PoS(ICRC2015)675 show the asymptotic 1 E, 173 m a.s.l.), in Moscow ◦ N, 37.7 ◦ 2 Juan A. Garzón for the TRAGALDABAS Collaboration W, 240 m a.s.l.), in (Spain). ◦ 3557 km, allowing them to look for common effects in ]. ∼ 1 , 8.6 ◦ Aymptotic regions for different arrival angles of cosmic muons for both detectors. Blue contours As a consequence of their complementary performances and the distance existing between the Cosmic Rays of a wide spectrum of energies are permanently arriving to Earth where they In this article present two singular facilities, URAGAN, one of the component of the very regions, covered by both detectors,age for energy and different solar arrival protons. anglesboth As of detectors shown muons would in allow produced to the by improve figure,allowing significantly both the to the discriminate aver- very angular between high resolution common of overlap phenomena the of ofmon tandem interplanetary the phenomena as or acceptances as well solar the of origin as ones and caused uncom- by local changes in the atmosphere conditions, in the magnetic detectors, URAGAN and TRAGALDABAS make upare a very relatively interesting near tandem. in the As both sameities detectors hemisphere, in their the joint study operation of may extraterrestrial open effects plenty related of new with possibil- cosmic rays. Fig. Figure 1: correspond to URAGAN data and the yellow ones correspond to TRAGALDABAS. The distance between both facilitiesthe is arrival of cosmic rays overanylize different those areas effects of in the real Earth’s time. outer space asymptotic directions and interact with the atmosphericthe atoms rate producing and up angular to behaviorat in billions different time of latitudes, of secondary the magnetic particles. most rigidityto common thresholds make Analyzing particles, and a mainly energy regular neutrons cuts and surveyprecise using muons, forecasts of absorbers, for many it those phenomena is phenomena: withgeomagnetic possible storms, interest variations among in others. in the For the this solar humanmonitors purposes activity a and activities wide or muons networks and the of directional to detectors, detection detectors, mainly issue parallel of neutron have and intense been coordinating deployed their efforts over [ the Earth surface working in big NEVOD research complex located at MEPhI ( (55.7 URAGAN & TRAGALDABAS 1. Introduction (Russia), and TRAGALDABAS a newFaculty small of size Physics new generation of tracking the detector USC located (42.9 at the PoS(ICRC2015)675 . The 1 − . ◦ 1300 s . The readout is 2 ∼ 54 s per minute. Every minute three ∼ 3 Juan A. Garzón for the TRAGALDABAS Collaboration ]. It is composed by four super-modules, three of 2 . The track angular resolution is always better than 1 3 . A muon track is recorded if there is a coincidence between at least ◦ we present a joint preliminary analysis of the FD starting at June 22nd. 3 ). A supermodule (SM) is composed by eight planes of 320 streamer tubes with we describe both detectors giving the most interesting features and performances 2 2 The muon hodoscope URAGAN on top of the NEVOD detector. The four Super Modules are The mean counting rate of reconstructed muon tracks of each of the SM is Muon hodoscope URAGAN started taking regular data in 2006 and is a significative compo- In section them are taking data permanentlyposes while (see the Fig. forth one is used for complementary calibrationperformed pur- with a 1.2 cm pitchin by the 320 Y Al oriented electrodes perpendicular in direction. theaccesible The X height zenith oriented of angle planes each of and module 288 75 is Alfour 50 electrodes cm, X being the planes maximum insidebetween a 200 time MeV and 600 ofin MeV 250 a for ns. single the SM different is The zenith shown angles. energy in Fig. The threshold scheme of of the amean detected muon live detection muons time range provided by the acquisition system is of dimensionss 10 mm x10 mm x 3500 mm each. The total of one SM is 11.5 m 2. The detectors 2.1 URAGAN nent of the NEVOD experimental complex [ Figure 2: easily distinguishable. Only threecalibrating of other them detectors. are taking data regularly. The forth one is used for testing and 90x90 cell matrices are storeda with function the of number the following of pairzenith arriving of angle muons variables: and, detected zenith finally, during and the last azimuthal slopes minute angles, of as X the and X Y and projections Y of projections of the zenith angle. These 1-min 2015. of each of them. We alsodetectors. comment the In advantages expected section from the joint analysis of data of both URAGAN & TRAGALDABAS field. PoS(ICRC2015)675 300 ps. All ∼ shows the matrix 4 Example of one minute of data taken with shows an example of the tracking 6 ]. It was developed to better understand and an arrival time resolution better than 4 ]. The detector started to take test data in ◦ 5 Figure 4: three Super Modules of URAGAN 4 Juan A. Garzón for the TRAGALDABAS Collaboration pads each, providing a time resolution of 2 and has a height of 1.8 m. It is composed of three planes of 2 11x11 cm ∼ ), the detector has been working rather smoothly since the end of March 2015. 5 Scheme of a single particle detection in one TRAGALDABAS is a new generation cosmic ray detector based on the RPC (Resistive Plate Starting from the basic 1-min matrices, 5-minute, 60-minute and 24-hour matrices are also It covers a surfaceRPC of cells 1.2x1.5 readout m by 120 this features does allow itray to air reconstruct showers the with time-space an angular microstructure resolution of better the than front 2 of the cosmic capability of the detector. Chamber) technology based on the TRASGO concept [ 2.2 TRAGALDABAS several effects observed in the analysisRPC of ToF wall cosmic of ray the dataSept. taken HADES 2013 during experiment with the at only commissioning the 2 of GSI planeslayout the [ but (see it Fig. has undergone several improvements since then. In its present built for further purposes likeusing solar them, activity all analysis, the atmospheric matrices phenomenaeffects. are and corrected others. After to eliminate the Before both averaging,snapshot pressure of normalization and upper and temperature hemisphere in atmospheric filtering "muon light" procedures,of with every a the certain matrix exposure matrices’ (1, represents 5 anisotropy the orprocesses. 60 provides min). The information analysis about the direction of cosmic ray modulation Figure 3: of the angular distribution of 1-minute of data taken with URAGAN. Super Module of URAGAN 180ps for single tracks.the Another muonic uncommon and performance the is electromagnetic (EM) thatarrival of components the cosmic of detector air the showers is cosmic having sensitive rays only to allowing EM to component. both estimate Fig. the URAGAN & TRAGALDABAS matrices are the basic information formodulation most in of the the heliosphere analysis and related Earth’s with magnetosphere the and processes atmosphere. of Fig. cosmic ray PoS(ICRC2015)675 Jun.16th. Jun.25th.. ∼ ∼ Example of the tracking performances of Figure 6: the TRAGALDABAS detector for aevent. high multiplicity Electromagnetic componentseparated will by software. be partially at four geographic quadrants, where significative 5 shows a muonography giving the arrival angular ) Juan A. Garzón for the TRAGALDABAS Collaboration ◦ 8 50 , ◦ shows the counting rates measured at the acceptance an- 30 10 ( and ) . ◦ ◦ 30 , ◦ 20 ( , ) ◦ 20 , 0 ( shows the counting rate behaviour in the detector for multiplicity M=1 events and for Present layout of the TRAGALDABAS shows the mean rate, corrected by pressure and temperature, measured by URAGAN, 9 7 Jul.1st. Another intriguing feature that should be analyzed in the future is the different shape Waiting for a more detailed analysis, a first glance at the results of both detectors already show Concerning the data taken by TRAGALDABAS, a preliminary analysis has been done using As an example of the joint capabilities provided by both detectors, we present the preliminary Fig. ∼ between both FDs. While in Moscow datathe shows FD two, observed or in perhaps Santiago three, minima de of Compostela the there same is size, a in main minimum taking place at and interesting effects. The FDAlso has both been detectors observed have at been both sensitive locations to more other or small less decreases at that the took same place time. on differences can be observed. approximately the same period. Fig. One of the possible reasons of such a difference is the different rigidity thresholds existing in both starting several days before the FD;was significative produced decrease around is apparent. twodistribution Also days of a muons later. significative arriving replica to the Fig. rate detector of during arrival the muons FD produced minimum. byasymptotic A the direction sizeable solar below screening plasma 45 in cloud the ejected is almost centered in theonly vertical the information of planes 2nd.tion. and Fig. 4th. and, as a consequence, with a limited angulargle resolu- regions: Figure 5: results of data obtained during a biga Forbush big Decrease CME (FD) started (Coronal on Mass Juneby Ejection) 22nd. most held and of produced on the by the neutron Sun monitors and several muon hours detectors before. existing around The the FD world. was observed detector. Starting from the top, only4th. the 1st., planes 2nd. are and electronics. fully Trigger instrumented is with done by the2nd. coincidences read-out and in 4th. planes 3. Example of the joint performances of both detectors URAGAN & TRAGALDABAS PoS(ICRC2015)675 15 Astrophysics and , Angular distribution of muons (muonogra- , GMDN (Global Muon Detector Figure 8: phy) measured by URAGANFD in the in minimum June ofduced 22nd. the in the cosmic rays showing background bycloud. a the solar plasma big screening pro- 6 Juan A. Garzón for the TRAGALDABAS Collaboration 6 GeV at TRAGALDABAS. ∼ http://www.nmdb.eu (2012) P10007. 7 Neutrino water detector on the Earth’s surface (NEVOD) The URAGAN Wide-Aperture Large-Area Muon Hodoscope Inst. Exp. Tech. (1997) 105. TRAGALDABAS: a new RPC based detector for the regular study of cosmic rays J. of Analysis of the space-time microstructure of cosmic ray showers using the HADES 258 2.4 GeV at URAGAN and http://cr0.izmiran.ru/gmdnet/ (2014) C09027. 9 ∼ The URAGAN counting rate behavior during RPC-TOF wall J. of Instrum. (2008) 180-186. Instrum. Network): Space Science Both URAGAN and TRAGALDABAS detectors will survey regularly the arrival of cosmic [4] A. Blanco et al., [5] J. Belver et al. [2] V. M. Aynutdinov et al., [1] NMDB (Neutron Monitor Data Base): [3] N.S. Barbashina et al., Figure 7: the FD in June 22nd. 2015 laboratories: rays with high directional resolution providingsurface. a stereographic A view first of a commonrecently big FD portion and produced of is the as Earth’s under aremove investigation. consequence them of from A the the better solar cosmic surveyatmospheric rays activity or of regular has interplanetary solar flux been origin. allowing events observed a will better allow, study in of the other future, phenomenaReferences from to URAGAN & TRAGALDABAS 4. Summary PoS(ICRC2015)675 ) ◦ 30 , ◦ 20 ( , ) ◦ 20 , 0 ( in the zenith angle and at aproximately ) Counting rate measured by TRAGALD- ◦ 50 , ◦ 30 ( Figure 10: ABAS at the acceptance regions and the four N, E, S and W quadrants. 7 Juan A. Garzón for the TRAGALDABAS Collaboration : 1. Univ. Alcalá /Alcalá de Henares, Spain. 2. CEN-Bordeaux, France. 3. CGUC- The TRAGALDABAS counting rate behavior : H. Alvarez Pol(9) , A. Blanco (4), J.J. Blanco (1), J. Collazo (8), J. Díaz Cortés Figure 9: during the FD in June 22nd. 2015 The TRAGALDABAS Collaboration Members (8), P. Fonte (4),G. D. Kornakov(6), T. García Kurtukian Castro(8), (2), R.A.Morozova J.A. (3), Lorenzo J.C. Garzón (9), Mouriño (8), J.M. (7), M.A. López A.P. Pais (8), Ribeiro (3), Gómez-Tato (3), L. M. (7), M. Palka Lópes Seco (5), (4), M. (9), V. Pérez M.Institutions J. González Muñuzuri Morales Taboada (10), (10). (8), (8), P. Rey(7), Univ. de Coimbra / Coimbra, Portugal./Cracow, . 4. 6. LIP-Coimbra / TU-Darmstadt, Coimbra, Germany.Univ. Portugal. 7. S. 5. de CESGA/ Compostela Jagellionan S. / Univ. de S. Compostela,/ de Spain. Compostela, S. Spain. de 8. Compostela, 9. LabCAF- Spain. Particle Phys. 10. Dept. Meteogalicia-Xunta de Univ. Galicia S. de / Compostela S. de Compostela, Spain. URAGAN & TRAGALDABAS