PoS(ICRC2019)593 http://pos.sissa.it/ ∗ † [email protected], [email protected] Speaker. A footnote may follow. The current generation of experimentsspace devoted platforms. to study extreme Recent energycomplex satellite than cosmic missions previous rays models. have will Therefore, shown be thatthe the at upper the observation atmosphere of UV will transient light be luminous important. background eventsvery TLEs is fast Information at about events more may the time need tothe and largest be space focus recorded, depth. evolution this of The impose this simplest requirementsThis optical of pinhole design, a a pinhole wide camera field have fulfills aimages of this of multianode view characteristics. TLEs photomultiplier and of about 8x8 milliseconds. , Infrom that this Sierra allow Negra work us Volcano we in present to Mexico the and register shape its 2d of capabilities some in events order recorded to use it as a monitoring device. † ∗ Copyright owned by the author(s) under the terms of the Creative Commons c Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). 36th International Cosmic Ray Conference -ICRC2019- July 24th - August 1st, 2019 Madison, WI, U.S.A. S. Hernandez, E. Ponce E-mail: UV Transient Luminous Events observed withterrestrial a pinhole Autonomous University of Puebla, Mexico. 4 sur 104 Col. Centro C.P. 72000, Puebla, Mexico. PoS(ICRC2019)593 E. Ponce =300-400 λ ], it is possible to 3 =300 nm. For estimate of the λ . In our case the design and construction of the 2 1 ] for EAS Cherenkov light observations. A scheme of 1 ]. We plan to operate it onboard a space mission satellite ) with uniform intensity over the circle. So the total UV 1 1 =300-400 nm and decreases below λ ] and taking the TLE UV intensity and time duration from [ 2 One of the important phenomena in night atmosphere, related to ultraviolet light background The detector is the one of best optical imaging designs due to their nm. To improve the detection ofTLE TLEs, whole for area this is project we observedand by time considered all is the pixels, obtained configuration in as where this it the the was setup designed suggested a camera in detailed [ obscura image it of is the shown UV in flash figure in space energy Euv radiated by the TLE correspond to the number of photons of camera obscura was made withmodel the H7546B following (Hamamatsu) technical a parameters: matrixhave one of the 8 photo same by receivers size, 8 MaPMT pixels theof focal with the distance a f camera considered size obscure is of detector, f=75 2x2 as mm. mm. a In the first The test stage, pinhole and we developing process have performed several measurements at the planed to orbit theeventual earth creation at of 700 Km perturbationsperturbation height. near was to The considerated the camera event obscuraparticle. that as The it high may background will brightness of should be noise TLE trigger usedthe may in allow image some us the in to to TLE’s. pixels use tracking of explore the UV of simplest This the the detector. pinhole hole the The size optimal cosmic for imaging measuring is quality ray equal inalso original to a the the pinhole temporal detector camera pixel is profile size. achieved offast if Our the photo aim image detector is is with to available measure time only notnumber as only of resolution a the pixels. Multi-Anode of TLE The Photomultiplier image about size Tube but milliseconds. ofequal (MaPMT) the to with Today pixel this such in size some a MaPMT [ isestimate of the about signals 2-3 in mm. the Assuming pixelsaround the of 20% camera the for hole pinhole camera. Efficiency of the MaPMT pixels to UV is measurement, are TLE (transientup luminous to events) 0.1-1 characterized MJ)flashes by were short very done (duration bright by two (energy of artificialUniversitetskii–Tat’yana in 1-300 microsatellites and UV designed Universitetskii–Tat’yana ms) for 2; scientific flashes. recently, and continueof educational with UV purposes the radiation The observations (300-400 firstexperiment nm global on-board wavelength) measurements bursts in of Lomonosov theconstructed UV satellite. night at atmosphere of the These the MSU scientific Skobeltsyn Earthwe Institute Earth with present of a TUS satellites Nuclear method were of (SINP) TLE designedcamera (Moscow). measurement In and by this is the project planned imaging pinhole foracceleration camera. operation in The in the presented space pinhole atmosphere, experimentsatmosphere devoted from the to electric magnetosphere study discharges among of others. and processes relativistic of electron electron precipitation to the 2. Pinhole camera wide field of view and large deep field [ TLEs 1. Introduction TLE image signals the lateralthat distribution UV of flash UV images intensity during covertypical the a TLE event circular is by area needed. video of We , assume some figure tens of km diameter (as it was measure in a PoS(ICRC2019)593 E. Ponce . 3 the electronic board used to 2 2 , shows the block diagram and at center of figure 3 Camera obscura: 1 Photo receiver. 3 pinhole. 2 Electronic Board, all main electrinic parts at Some transient luminous events measured by video cameras. The images correspond to an elve The figure 3. Camera electronics Figure 2: center and at right shows the tx-rx data and commands of the camara obscura board and a PC. red sprite, blue jet and micrometorites. the signal processing of MaPMTprocessor when a FPGA Xilinx a series. luminous This64 event FPGA analog will control signals appears. from the each The MaPMT. multiplexingMaPMT Also board and in control has the order and digitalization as to monitored of protect a the it the high main iffiguration voltage a bright and supplied or operation to long parameters lasting the from eventcommand appears. the controls PC The of and FPGA FPGA stores communicate are all it the definedWith thru con- the by comunication same port. software the The we user construct byThe a software data 64 graphic base programmable pixels in interface. order of tomultiplexers MAPMT process of and are plot digitalized type with the ADG706, registeredaccording only where events. to one each digital multiplexer ADC. values selects applied For 1 forboards this signal control we we from obtain use and multiplexing. its process an 16 Then every input with array signal signals, the from of array MAPMT four as of shows 4 in multiplexer figure Figure 1: TLEs Sierra Negra Volcano in Puebla-Mexico, atdue a to height the of small 4200 light meters pollution above and sea less level approximately atmospheric absorption. PoS(ICRC2019)593 E. Ponce s. Amplitude of each pixel at lefth. At µ ], and use it to convert the signal to physical 4 3 Form of process all the 64 MaPMT’s analog signals. At lefth, multiplexing module. at right UV TLE registered with pinhole camera in a frame of 64 As a first step in the calibration process of the Camera Oscura, it is necessary to measure the right TLE’s image, the numbers corresond to the pixel. Figure 4: response to a single photo-electron by the MaPMT [ Figure 3: electronic block diagram. 4. Camera testing photon flux. To obtainvoltage the for single the MaPMT photoelectron used. response, Toa do we function this, have of we found supplied obtained voltage the theage. with single From photo optimal the electron a operative analysis (SPE) controlled of spectrum LED as photo pulse. some electron thousands We response events, selected we and 950V found as the theafter operative SPE mean calibrated, volt- charge was pulse produced tested amplitude by at distribution. a mountainheight single Sierra The of Negra 4200 designed in meters Puebla-Mexico pinhole located above camera geographically seafigures. at level a approximately, some results obtained are shown in the next TLEs PoS(ICRC2019)593 E. Ponce 4 Possible micrometeorite trajectory observed during one second in the pinhole’s field of view, in UV TLE registered with pinhole camera in a frame of 32 milliseconds. At lefth, amplitud of each Figure 6: four frames of .25 seconds each one. Amplitude of each pixel, upper. TLE’s bright, down. pixel. At center, amplitude distributed in an array of 8x8. TLE’s bright, at right. Figure 5: TLEs PoS(ICRC2019)593 . E. Ponce 564 J. Phys. G: Nucl. , Journal of , Printed in the UK. 21 5 J. Phys. G: Nucl. Part. Phys. Nuclear Instruments and Methods in physics research A , , 1994]. . 115 Camera obscura network: an array for registration of EAS Cerenkov radiation in the Program of transient UV event research at TATIANA-2 satellite Printed in the UK [ Camera obscura for observation of EAS images in Cerenkov light Performance of a multi-anode photomultiplier employing a weak electrostatic focusing 20 Geophysical Research A system (Hamamatsu R8900 series) presence of high-intensity sky noise Part. Phys. The pinhole camera design has shown to be a fruitful configuration for studies of background [3] Garipov G.K., [4] Y. Kawasaki., [2] G. K. Garipov, [1] G K. Garipov, References light level distribution presented inMexican mountain the Pico atmosphere. de Orizaba The andconfidence calibration Sierra and la TLE Negra performance and shows UV test that background at its light. possible the to detect with high TLEs 5. Conclusions