ABSTRACT PAUCam is an innovative optical narrow-band imager mounted at the William Herschel Telescope built for the Physics of the Accelerating Universe Survey (PAUS). Its set of 40 filters results in images that are complex to calibrate, with specific instrumental signatures that cannot be processed with traditional data reduction techniques. In this paper, we present two pipelines developed by the PAUS data management team with the objective of producing science-ready catalogues from the uncalibrated raw images. The Nightly pipeline takes care of entire image processing, with bespoke algorithms for photometric calibration and scatter-light correction. The Multi-Epoch and Multi-Band Analysis pipeline performs forced photometry over a reference catalogue to optimize the photometric redshift (photo-z) performance. We verify against spectroscopic observations that the current approach delivers an inter-band photometric calibration of 0.8 per cent across the 40 narrow-band set. The large volume of data produced every night and the rapid survey strategy feedback constraints require operating both pipelines in the Port d’Informació Cientifica data centre with intense parallelization. While alternative algorithms for further improvements in photo-z performance are under investigation, the image calibration and photometry presented in this work already enable state-of-the-art photo-z down to iAB = 23.0.

PAUCam is an innov ati ve optical narro w-band imager mounted at the William Herschel Telescope built for the Physics of the Accelerating Universe Survey (PAUS). Its set of 40 filters results in images that are complex to calibrate, with specific instrumental signatures that cannot be processed with traditional data reduction techniques. In this paper, we present two pipelines developed by the PAUS data management team with the objective of producing science-ready catalogues from the uncalibrated raw images. The N IGHTLY pipeline takes care of entire image processing, with bespoke algorithms for photometric calibration and scatter-light correction. The Multi-Epoch and Multi-Band Analysis pipeline performs forced photometry o v er a reference catalogue to optimize the photometric redshift (photo-z) performance. We verify against spectroscopic observations that the current approach delivers an inter-band photometric calibration of 0.8 per cent across the 40 narrow-band set. The large volume of data produced every night and the rapid survey strategy feedback constraints require operating both pipelines in the Port d’Informaci ´o Cientifica data centre with intense parallelization. While alternative algorithms for further impro v ements in photo-z performance are under investigation, the image calibration and photometry presented in this work already enable state-of-the-art photo-z down to i AB = 23.0.

The Silicon Vertex Detector of Belle II is a state-of-the-art tracking and vertexing system based on double-sided silicon strip sensors, designed and fabricated by a large international collaboration in the period 2012–2018. Since 2019 it has been in operation providing high quality data with a small number of defective channels (<1%), a large hit-finding efficiency (>99%), a good signal-to-noise ratio (well in excess of 10 for all sensor configurations and tracks). Together with the good control over the alignment, these are all essential factors to achieve good tracking reconstruction and physics performance. In this extended paper we try to document all the aspects of the SVD challenges and achievements, in the spirit of providing information to the broader community and help the development of high quality detector systems, which are essential tools to carry out physics research.

Vera C. Rubin Observatory is a ground-based astronomical facility under construction, a joint project of the National Science Foundation and the U.S. Department of Energy, designed to conduct a multipurpose 10 yr optical survey of the Southern Hemisphere sky: the Legacy Survey of Space and Time. Significant flexibility in survey strategy remains within the constraints imposed by the core science goals of probing dark energy and dark matter, cataloging the solar system, exploring the transient optical sky, and mapping the Milky Way. The survey's massive data throughput will be transformational for many other astrophysics domains and Rubin's data access policy sets the stage for a huge community of potential users. To ensure that the survey science potential is maximized while serving as broad a community as possible, Rubin Observatory has involved the scientific community at large in the process of setting and refining the details of the observing strategy. The motivation, history, and decision-making process of this strategy optimization are detailed in this paper, giving context to the science-driven proposals and recommendations for the survey strategy included in this Focus Issue.

PAUCam is an innovative optical narrow-band imager mounted at the William Herschel Telescope built for the Physics of the Accelerating Universe Survey (PAUS). Its set of 40 filters results in images that are complex to calibrate, with specific instrumental signatures that cannot be processed with traditional data reduction techniques. In this paper we present two pipelines developed by the PAUS data management team with the objective of producing science-ready catalogues from the uncalibrated raw images. The Nightly pipeline takes care of all image processing, with bespoke algorithms for photometric calibration and scatter-light correction. The Multi-Epoch and Multi-Band Analysis (MEMBA) pipeline performs forced photometry over a reference catalogue to optimize the photometric redshift performance. We verify against spectroscopic observations that the current approach delivers an inter-band photometric calibration of 0.8% across the 40 narrow-band set. The large volume of data produced every night and the rapid survey strategy feedback constraints require operating both pipelines in the Port d'Informació Cientifica data centre with intense parallelization. While alternative algorithms for further improvements in photo-z performance are under investigation, the image calibration and photometry presented in this work already enable state-of-the-art photometric redshifts down to iAB=23.0.

This paper shows the hardware and the procedure utilized to test all components of the readout system (cables, FADC boards, junction boards) of the Belle II Silicon Vertex Detector after the series production. For the FADC board special testing hardware and firmware were designed and created to check all digital and analog inputs and outputs as well as all data interconnections on the board. The main FPGA on the FADC board generates digital signals which are converted to periodic analog differential alternating voltages up to 40 MHz on the FADC board tester, which then are fed into the analog inputs of the FADC board. Histograms and scans of the samples are recorded by using random equivalent-time sampling or sequential equivalent-time sampling, allowing to characterize the behavior of the system with a much higher bandwidth than the ADCs could do with conventional measurements. Small changes of parameters of the assembly (like using a cable of different length) lead to significant changes of the measured values, creating a sensitive testing instrument. The shapes of the distributions are analyzed and compared to references by software which then decides if a test is passed or not. The commissioning setup of the whole readout chain, with all the final components including the final detector, has been tested in three phases. The respective graphs of the signal-to-noise ratios of the strips of a detector module and histograms of the noise development of the whole detector show very high consistency of the SVD readout system.

The Belle II Silicon Vertex Detector (SVD) was installed recently and has been prepared for physics run at SuperKEKB factory, Tsukuba, Japan. For a reliable operation and data taking of the SVD, a sophisticated and robust run and slow control system has been implemented, which utilizes the Experimental Physics and Industrial Control System (EPICS) framework. EPICS uses client/server and publish/subscribe techniques to communicate between the various sub-systems and computers. The information exchange between the different pieces of software and computers is done by process variables (PVs). These PVs are provided by input/output controllers (IOCs), which communicate and interface with the hardware components. The Belle II SVD slow and run control comprises five groups of subsystems, which are SVD DAQ controller, Flash ADC controller, environmental monitors and interlocks, power supplies and EPICS infrastructure services. In this paper we describe the tasks and the implementation of the individual sub-systems, the interaction between them and the global Belle II run and slow control as well as the first experience from commissioning and initial operation of the SuperKEKB accelerator.

The Belle II experiment at the SuperKEKB collider of KEK (Japan) will accumulate 50 ab−1 of e+e- collision data at an unprecedented instantaneous luminosity of 8⋅ 1035 cm−2s−1, about 40 times larger than its predecessor. The Belle II vertex detector plays a crucial role in the rich Belle II physics program, especially for time-dependent measurements. It consists of two layers of DEPFET-based pixels and four layers of double sided silicon strip sensors (SVD detector). We report here results of the standalone commissioning of the SVD and highlights from the first cosmic runs acquired in Belle II. We also report on reconstruction performances of a reduced-scale version of the SVD operated during the accelerator commissioning in 2018.

T. Bilka∗†d , F. Abudinénn, K. Ackermannn, P. Ahlburge, H. Aiharaac, M. Albalawin, O. Alonsoai, L. Andriceko, R. Ayadah, T. Azizu, V. Babuh, S. Bacherag, S. Bahinipatip, Y. Baim, E. Barberioa, Ti. Baroncellia, To. Baroncellia, A. K. Basithq, G. Batignaniv,w, A. Bauerb, P. K. Beheraq, V. Bertacchiv,w, S. Bettariniv,w, B. Bhuyanr, R. Blanco j, F. Bosiw, M. Boronatak, L. Bosisiox,y, A. Bozekag, F. Buchsteinerb, C. Camienh, A. Caldwelln, G. Cariaa, G. Casarosav,w, M. Ceccantiw, D. Červenkovd , V. Chekeliann, T. Czankab, N. Dashp, M. De Nucciov,w, B. Deschampse, A. Dieguezai, J. Dingfeldere, Z. Doležald , D. Esperanteak, P. Fischeri, F. Fortiv,w, M. Frasn, A. Freyg, M. Friedlb, J. Fusterak, M. Gabrieln, K. Gadowh, U. Gebauerg, L. Germice, T. Gessler f , D. Getzkow f , L. Gioin, A. Glazovh, B. Gobboy, P. Gomisak, J. A. M. Grimaldoac, K. Haraad , M. Heck j, T. Hempereke, M. Henselo, T. Higuchiz, M. Hoekk, C. Irmlerb, A. Ishikawaab, I. Jaegleal,H. B. Jeonae, C. Jooz, M. Kaletaag, J. Kandrad , N. Kambaraad , K. H. Kangae, P. Kapustaag, C. Kieslingn, B. Kisielewskiag, D. Kittlingern, D. Kloseo, P. Kodyšd , C. Koffmaneo, T. Kohrikiad , S. KoikeC,ad , I. Komarovy, I. Konorovm, S. Krivokucao, H. Krügere, T. Kuhrl, W. Kühn f , M. Kumars, R. Kumart , P. Kvasničkad , C. La Licatax,y, C. Lacastaak, K. Lalwanis, L. Lancerix,y, J. S. Lange f , K. Lautenbach f , J. Y. Leea f , S. C. Leeae, U. Leisn, P. Leitln, D. Levitm, Y. Lian, J. Libbyq, G. Liemanno, Z. Liuc, T. Lueckv,w, F. Lüttickee, L. Macharskih, P. Mamminiw, C. Mariñase, A. Martiniv,w, S. N. Mayekaru, S. Mccarneyn, G. B. Mohantyu, T. Moriiz, H. G. Mosern, D. Moyaa j, F. J. Muellerh, F. Müllern, D. Münchow f , K. R. Nakamuraad , H. Nakayamaad ,Z. Natkaniecag, C. Niebuhrh, J. Ninkovico, Y. Onukiac, W. Ostrowiczag, U. Packheiserh, A. Paladinoz, E. Paoloniv,w, H. Parkae, B. Paschene, S. Paulm, I. Peric j, F. Poblotzkih, K. Prasanthu, C. Prazh, A. Profetiw, A. Rabusovm, I. RashevskayaA,y, K. K. Raou, S. P. Reiter f , Resmi P. K.q, R. Richtero, M. Ritterl, M. Ritzerti, G. Rizzov,w, M. Rozanskaag, S. Rummell, D. Sahoou, J. G. Sancheza j, L. Santeljam, J. Sasakiac, N. Satoad , B. Scavinok, G. Schallero, M. Schneckeo, F. Schoppero, H. Schreeckg, S. Schultschikb, C. Schwandab, B. Schwenkerg, R. Sedlmeyern, C. Sfientik, F. Simonn, S. Skambraksn, Y. Solovievh, B. Spruckk, R. Steverh, U. Stolzenbergg, J. Stypulaag, J. Suzukiad , E. Tafelmayero, M. Takahashih, S. Tanakaad , H. Tanigawaac, G. N. Taylora, R. Thalmeierb, T. Tsuboyamaad , P. Urquijoa, I. Vilaa j, A. L. Virtoa j, L. Vitalex,y, S. Vogtn, M. Vosak, K. Wanac, C. Wangc, S. Watanukiab, M. WatanabeC,aa, I. J. Watsonac, J. Webba, N. Wermese, C. Wessele, J. Wiechczynskiag, P. Wieduwiltg, S. Williamsa, H. Windeln, H. Yeh, H. Yinb, L. Zaniv,w, J. Zhaoc

Commodity cloud computing makes it possible for science projects to easily procure highly-reliable data management infrastructure on demand. In this paper we argue that astronomy should outsource our data management needs to the commercial cloud thereby allowing us to focus on our core competencies of data calibration and science exploitation.

At the High Energy Accelerator Research Organization (KEK) in Tsukuba, Japan, the double-sided silicon strip sub-detector of the Belle II experiment is read out by 1748 APV25 chips. FPGAs perform several calculations on the digitized signals. One of them will be "Hit Time Finding": the determination of the time and amplitude of the signal peaks of each event in real time using pre-programmed neural networks. This work analyses the possibility, precision and reliability of these calculations depending on various parameters.

The construction of the new accelerator at the Super Flavor Factory in Tsukuba, Japan, has been finalized and the commissioning of its detector (Belle II) has started. This new e$^{+}$e$^{-}$ machine (SuperKEKB) will deliver an instantaneous luminosity of $8\times10^{35}\mathrm{~cm}^{-2}\mathrm{s}^{-1}$, which is 40 times higher than the world record set by KEKB. In order to be able to fully exploit the increased number of events and provide high precision measurements of the decay vertex of the B meson systems in such a harsh environment, the Belle II detector will include a new 6 layer silicon vertex detector. Close to the beam pipe, 2 pixel and 4 double-sided strip detector layers will be installed. During its first data taking period in 2018, the inner volume of the Belle II detector was only partially equipped with the final vertex detector technologies. The remaining volume was covered with dedicated radiation monitors, collectively called BEAST II, in order to investigate the particle and synchrotron radiation backgrounds near the interaction point. In this note, the milestones of the commissioning of the Belle II vertex detector and BEAST II are reviewed and the detector performance and selected background measurements will be presented.

The Belle II experiment at the SuperKEKB collider in Japan will search for new sources of CP violation and indirectly probe new physics by studying the suppressed decays of beauty mesons, charm mesons and tau leptons. In these pursuits, the spatial resolution of the Belle II Silicon Vertex Detector (SVD) will play a key role. We report herein the spatial resolution of the SVD using simulated data for a simplified version of the Belle II detector.

The Belle II experiment comes with a substantial upgrade of the Belle detector and will operate at the SuperKEKB energy-asymmetric e(+)e(-) collider with energies tuned to Y(4S) resonance root s = 10.588 GeV. The accelerator has successfully completed the first phase of commissioning in 2016 and the first electron-positron collisions in Belle II took place in April 2018. Belle II features a newly designed silicon vertex detector based on DEPFET pixel and double-sided strip layers. Currently, a subset of the vertex detector is installed (Phase 2 of the experiment). Installation of the full detector (Phase 3) will be completed by the end of 2018. This paper describes the Phase 2 arrangement of the Belle II silicon vertex detector, with focus on the interconnection of detectors and their integration with the software framework of Belle II. Alignment issues are discussed based on detector simulations and first acquired data.

B. Schwenker∗g, F. Abudinénn, K. Ackermannn, P. Ahlburge, H. Aiharaac, M. Albalawin, O. Alonsoai, L. Andriceko, R. Ayadah, T. Azizu, V. Babuh, S. Bacherag, S. Bahinipatip, Y. Baim, E. Barberioa, Ti. Baroncellia, To. Baroncellia, A. K. Basithq, G. Batignaniv,w, A. Bauerb, P. K. Beheraq, V. Bertacchiv,w, S. Bettariniv,w, B. Bhuyanr, T. Bilkad , R. Blanco j, F. Bosiw, M. Boronatak, L. Bosisiox,y, A. Bozekag, F. Buchsteinerb, C. Camienh, A. Caldwelln, G. Cariaa, G. Casarosav,w, M. Ceccantiw, D. Červenkovd , V. Chekeliann, T. Czankab, N. Dashp, M. De Nucciov,w, B. Deschampse, A. Dieguezai, J. Dingfeldere, Z. Doležald , D. Esperanteak, P. Fischeri, F. Fortiv,w, M. Frasn, A. Freyg, M. Friedlb, J. Fusterak, M. Gabrieln, K. Gadowh, U. Gebauerg, L. Germice, T. Gessler f , D. Getzkow f , L. Gioin, B. Gobboy, P. Gomisak, J. A. M. Grimaldoac, K. Haraad , M. Heck j, T. Hempereke, M. Henselo, T. Higuchiz, M. Hoekk, C. Irmlerb, A. Ishikawaab, I. Jaegleal,H. B. Jeonae, C. Jooz, M. Kaletaag, J. Kandrad , N. Kambaraad , K. H. Kangae, P. Kapustaag, C. Kieslingn, B. Kisielewskiag, D. Kittlingern, D. Kloseo, P. Kodyšd , C. Koffmaneo, T. Kohrikiad , S. KoikeC,ad , I. Komarovy, I. Konorovm, S. Krivokucao, H. Krügere, T. Kuhrl, W. Kühn f , M. Kumars, R. Kumart , P. Kvasničkad , C. La Licatax,y, C. Lacastaak, K. Lalwanis, L. Lancerix,y, J. S. Lange f , K. Lautenbach f , J. Y. Leea f , S. C. Leeae, U. Leisn, P. Leitln, D. Levitm, Y. Lian, J. Libbyq, G. Liemanno, Z. Liuc, T. Lueckv,w, F. Lüttickee, L. Macharskih, P. Mamminiw, C. Mariñase, A. Martiniv,w, S. N. Mayekaru, S. Mccarneyn, G. B. Mohantyu, T. Moriiz, H. G. Mosern, D. Moyaa j, F. J. Muellerh, F. Müllern, D. Münchow f , K. R. Nakamuraad , H. Nakayamaad ,Z. Natkaniecag, C. Niebuhrh, J. Ninkovico, Y. Onukiac, W. Ostrowiczag, U. Packheiserh, A. Paladinoz, E. Paoloniv,w, H. Parkae, B. Paschene, S. Paulm, I. Peric j, F. Poblotzkih, K. Prasanthu, A. Profetiw, A. Rabusovm, I. RashevskayaA,y, K. K. Raou, S. P. Reiter f , Resmi P. K.q, R. Richtero, M. Ritterl, M. Ritzerti, G. Rizzov,w, M. Rozanskaag, S. Rummell, D. Sahoou, J. G. Sancheza j, L. Santeljam, J. Sasakiac, N. Satoad , B. Scavinok, G. Schallero, M. Schneckeo, F. Schoppero, H. Schreeckg, S. Schultschikb, C. Schwandab, R. Sedlmeyern, C. Sfientik, F. Simonn, S. Skambraksn, Y. Solovievh, B. Spruckk, R. Steverh, U. Stolzenbergg, J. Stypulaag, J. Suzukiad , E. Tafelmayero, M. Takahashih, S. Tanakaad , H. Tanigawaac, G. N. Taylora, R. Thalmeierb, T. Tsuboyamaad , P. Urquijoa, I. Vilaa j, A. L. Virtoa j, L. Vitalex,y, S. Vogtn, M. Vosak, K. Wanac, C. Wangc, S. Watanukiab, M. WatanabeC,aa, I. J. Watsonac, J. Webba, N. Wermese, C. Wessele, J. Wiechczynskiag, P. Wieduwiltg, S. Williamsa, H. Windeln, H. Yeh, H. Yinb, L. Zaniv,w, J. Zhaoc

The “chip-on-sensor” concept of this detector minimizes the distance of the signal propagation from the double-sided silicon detector strips to the readout chips and thus reduces noise from strip capacitance. One half of the detector is built, the second half is being assembled at the time of writing. Prototypes have been tested in several test beams as well as in the so-called Phase 2 setup inside the detector structure. First results from a commissioning run of the Belle-II prototype SVD detector are presented. The measured signal-to-noise and timing performance are found to be according to design specifications.

The Silicon Vertex Detector of the Belle II Experiment at KEK in Tsukuba, Japan, consists of 172 double-sided strip sensors. They are read out by 1748 APV25 chips, and the analog data are sent out of the radiation zone to 48 modules which convert them to digital. FPGAs then compensate line signal distortions using digital finite impulse response filters and detect data frames from the incoming stream. Then they perform pedestal subtraction, common mode correction and zero suppression, as well as calculate the peak timing and amplitude of each event from a set of data samples using a neural network.

The Silicon Vertex Detector (SVD) is one of the main detectors in the Belle II experiment at KEK, Japan.In combination with a pixel detector, the SVD determines precise decay vertices and performs low-momentum track reconstruction.The SVD ladders are being developed at several institutes.For the development of the tracking algorithm as well as the performance estimation of the ladders, beam tests for the ladders were performed.We report an overview of the SVD development, its performance measured in the beam tests, and the prospect of its assembly and commissioning until installation.

The Silicon Vertex Detector of Belle II will be fundamental not only for the reconstruction of B meson vertices, but also for the reconstruction of neutral particles like K shorts, and the tracking of low-pt particles like slow pions associated with the decays of the abundant D* mesons. As a consequence great importance is given to the performance of the software that deals with the simulation and reconstruction of the SVD events. The Belle II experiment is the successor to Belle, one of the two experiments that first observed CP violation in the decay of B mesons. The SuperKEKB collider will deliver 40 times more luminosity than its predecessor KEKB, which requires major upgrades to the detector hardware. This also poses new challenges not only for the data collection and storage, but also for the software framework which is used to process and analyse the experimental data. In this article we present in detail the SVD software framework together with its development for the test of the Vertex Detector system, which took place at DESY in April 2016 using an electron beam.

We describe the selection of galaxies targeted in eight low-redshift clusters (APMCC0917, A168, A4038, EDCC442, A3880, A2399, A119 and A85; 0.029 < z < 0.058) as part of the Sydney-AAO Multi-Object Integral field spectrograph Galaxy Survey (SAMI-GS). We have conducted a redshift survey of these clusters using the AAOmega multi-object spectrograph on the 3.9-m Anglo-Australian Telescope. The redshift survey is used to determine cluster membership and to characterize the dynamical properties of the clusters. In combination with existing data, the survey resulted in 21 257 reliable redshift measurements and 2899 confirmed cluster member galaxies. Our redshift catalogue has a high spectroscopic completeness (similar to 94 per cent) for r(petro) <= 19.4 and cluster-centric distances R < 2R(200). We use the confirmed cluster member positions and redshifts to determine cluster velocity dispersion, R-200, virial and caustic masses, as well as cluster structure. The clusters have virial masses 14.25 = log(M-200/M-circle dot) <= 15.19. The cluster sample exhibits a range of dynamical states, from relatively relaxed-appearing systems, to clusters with strong indications of merger-related substructure. Aperture-and point spread function matched photometry are derived from Sloan Digital Sky Survey and VLT Survey Telescope/ATLAS imaging and used to estimate stellar masses. These estimates, in combination with the redshifts, are used to define the input target catalogue for the cluster portion of the SAMI-GS. The primary SAMI-GS cluster targets have R < R-200, velocities vertical bar v(pec)vertical bar < 3.5 sigma(200) and stellar masses 9.5 <= log(M*(approx)/M-circle dot) <= 12. Finally, we give an update on the SAMI-GS progress for the cluster regions.