C. Yan - HKS - JLab E05-115 and E01-001 - Collaborations

C. Yan
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C. Yan
HKS - JLab E05-115 and E01-001 - Collaborations

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Astrophysics of Galaxies (10)
Cosmology and Nongalactic Astrophysics (10)
Nuclear Experiment (8)
Instrumentation and Methods for Astrophysics (7)
Mathematics - Combinatorics (5)
High Energy Astrophysical Phenomena (5)
Solar and Stellar Astrophysics (4)
High Energy Physics - Theory (2)
Mathematics - Classical Analysis and ODEs (2)
Physics - Optics (1)
Mathematics - Optimization and Control (1)
Mathematics - Numerical Analysis (1)
Physics - Instrumentation and Detectors (1)
Mathematics - Probability (1)
Physics - Classical Physics (1)
Mathematics - Mathematical Physics (1)
Physics - Materials Science (1)
Physics - Computational Physics (1)
Mathematical Physics (1)
High Energy Physics - Experiment (1)
High Energy Physics - Phenomenology (1)
Physics - Fluid Dynamics (1)
Computer Science - Computer Vision and Pattern Recognition (1)
Physics - Mesoscopic Systems and Quantum Hall Effect (1)
Nuclear Theory (1)
Computer Science - Databases (1)
Computer Science - Learning (1)
Quantitative Biology - Quantitative Methods (1)
Computer Science - Software Engineering (1)
Computer Science - Performance (1)
General Relativity and Quantum Cosmology (1)

Publications Authored By C. Yan

In the context of the Bank-Fishler-Shenker-Susskind Matrix theory, we analyze a spherical membrane in light-cone M theory along with two asymptotically distant probes. In the appropriate energy regime, we find that the membrane behaves like a smeared Matrix black hole; and the spacetime geometry seen by the probes can become non-commutative even far away from regions of Planckian curvature. This arises from non-linear Matrix interactions where fast matrix modes lift a flat direction in the potential -- akin to the Paul trap phenomenon in atomic physics. Read More

We present the results of transport measurements in a hybrid system consisting of an arch-shaped quantum point contact (QPC) and a reflector; together, they form an electronic cavity in between them. On tuning the arch-QPC and the reflector, asymmetric resonance peak in resistance is observed at the one-dimension to two-dimension transition. Moreover, a dip in resistance near the pinch-off of the QPC is found to be strongly dependent on the reflector voltage. Read More

In this paper, a novel neural network architecture is proposed attempting to rectify text images with mild assumptions. A new dataset of text images is collected to verify our model and open to public. We explored the capability of deep neural network in learning geometric transformation and found the model could segment the text image without explicit supervised segmentation information. Read More

The role of surface tension and wettability in the dynamics of air-liquid interfaces during immiscible fluid displacement flows in capillary tube driven by pressure has been investigated. The contact angle and capillary number drive the force wetting processes which is controlled by the balance between the capillary and the viscous lubrication forces. The dynamic wetting condition with the critical capillary number is studied analytically and validated experimentally, which demonstrates that the critical capillary number is associated with the contact angle, slip length and capillary radius. Read More

Results from the RHIC and LHC experiments show, that in relativistic heavy ion collisions, a new state of matter, a strongly interacting perfect fluid is created. Accelerating, exact and explicit solutions of relativistic hydrodynamics allow for a simple and natural description of this medium. A finite rapidity distribution arises from these solutions, leading to an advanced estimate of the initial energy density of high energy collisions. Read More

Classical Gon\v{c}arov polynomials are polynomials which interpolate derivatives. Delta Gon\v{c}arov polynomials are polynomials which interpolate delta operators, e.g. Read More

Authors: Naoyuki Tamura, Naruhisa Takato, Atsushi Shimono, Yuki Moritani, Kiyoto Yabe, Yuki Ishizuka, Akitoshi Ueda, Yukiko Kamata, Hrand Aghazarian, Stephane Arnouts, Gabriel Barban, Robert H. Barkhouser, Renato C. Borges, David F. Braun, Michael A. Carr, Pierre-Yves Chabaud, Yin-Chang Chang, Hsin-Yo Chen, Masashi Chiba, Richard C. Y. Chou, You-Hua Chu, Judith G. Cohen, Rodrigo P. de Almeida, Antonio C. de Oliveira, Ligia S. de Oliveira, Richard G. Dekany, Kjetil Dohlen, Jesulino B. dos Santos, Leandro H. dos Santos, Richard S. Ellis, Maximilian Fabricius, Didier Ferrand, Decio Ferreira, Mirek Golebiowski, Jenny E. Greene, Johannes Gross, James E. Gunn, Randolph Hammond, Albert Harding, Murdock Hart, Timothy M. Heckman, Christopher M. Hirata, Paul Ho, Stephen C. Hope, Larry Hovland, Shu-Fu Hsu, Yen-Shan Hu, Ping-Jie Huang, Marc Jaquet, Yipeng Jing, Jennifer Karr, Masahiko Kimura, Matthew E. King, Eiichiro Komatsu, Vincent Le Brun, Olivier Le Fevre, Arnaud Le Fur, David Le Mignant, Hung-Hsu Ling, Craig P. Loomis, Robert H. Lupton, Fabrice Madec, Peter Mao, Lucas S. Marrara, Claudia Mendes de Oliveira, Yosuke Minowa, Chaz N. Morantz, Hitoshi Murayama, Graham J. Murray, Youichi Ohyama, Joseph Orndorff, Sandrine Pascal, Jefferson M. Pereira, Daniel J. Reiley, Martin Reinecke, Andreas Ritter, Mitsuko Roberts, Mark A. Schwochert, Michael D. Seiffert, Stephen A. Smee, Laerte Sodre Jr., David N. Spergel, Aaron J. Steinkraus, Michael A. Strauss, Christian Surace, Yasushi Suto, Nao Suzuki, John Swinbank, Philip J. Tait, Masahiro Takada, Tomonori Tamura, Yoko Tanaka, Laurence Tresse, Orlando Verducci Jr., Didier Vibert, Clement Vidal, Shiang-Yu Wang, Chih-Yi Wen, Chi-Hung Yan, Naoki Yasuda

PFS (Prime Focus Spectrograph), a next generation facility instrument on the 8.2-meter Subaru Telescope, is a very wide-field, massively multiplexed, optical and near-infrared spectrograph. Exploiting the Subaru prime focus, 2394 reconfigurable fibers will be distributed over the 1. Read More

Most modern database-backed web applications are built upon Object Relational Mapping (ORM) frameworks. While ORM frameworks ease application development by abstracting persistent data as objects, such convenience often comes with a performance cost. In this paper, we present CADO, a tool that analyzes the application logic and its interaction with databases using the Ruby on Rails ORM framework. Read More

Structure functions, as measured in lepton-nucleon scattering, have proven to be very useful in studying the quark dynamics within the nucleon. However, it is experimentally difficult to separately determine the longitudinal and transverse structure functions, and consequently there are substantially less data available for the longitudinal structure function in particular. Here we present separated structure functions for hydrogen and deuterium at low four--momentum transfer squared, Q^2< 1 GeV^2, and compare these with parton distribution parameterizations and a k_T factorization approach. Read More

Particle picking is a time-consuming step in single-particle analysis and often requires significant interventions from users, which has become a bottleneck for future automated electron cryo-microscopy (cryo-EM). Here we report a deep learning framework, called DeepPicker, to address this problem and fill the current gaps toward a fully automated cryo-EM pipeline. DeepPicker employs a novel cross-molecule training strategy to capture common features of particles from previously-analyzed micrographs, and thus does not require any human intervention during particle picking. Read More

We introduce the sequence of generalized Gon\v{c}arov polynomials, which is a basis for the solutions to the Gon\v{c}arov interpolation problem with respect to a delta operator. Explicitly, a generalized Gon\v{c}arov basis is a sequence $(t_n(x))_{n \ge 0}$ of polynomials defined by the biorthogonality relation $\varepsilon_{z_i}(\mathfrak d^{i}(t_n(x))) = n! \;\! \delta_{i,n}$ for all $i,n \in \mathbf N$, where $\mathfrak d$ is a delta operator, $\mathcal Z = (z_i)_{i \ge 0}$ a sequence of scalars, and $\varepsilon_{z_i}$ the evaluation at $z_i$. We present algebraic and analytic properties of generalized Gon\v{c}arov polynomials and show that such polynomial sequences provide a natural algebraic tool for enumerating combinatorial structures with a linear constraint on their order statistics. Read More

Supermassive binary black holes (BBHs) are unavoidable products of galaxy mergers and are expected to exist in the cores of many quasars. Great effort has been made during the past several decades to search for BBHs among quasars; however, observational evidence for BBHs remains elusive and ambiguous, which is difficult to reconcile with theoretical expectations. In this paper, we show that the distinct optical-to-UV spectrum of Mrk 231 can be well interpreted as emission from accretion flows onto a BBH, with a semimajor axis of ~590AU and an orbital period of ~1. Read More


The Prime Focus Spectrograph (PFS) is an optical/near-infrared multifiber spectrograph with 2394 science fibers distributed across a 1.3-deg diameter field of view at the Subaru 8.2-m telescope. Read More

Background: Measurements of forward exclusive meson production at different squared four-momenta of the exchanged virtual photon, $Q^2$, and at different four-momentum transfer, t, can be used to probe QCD's transition from meson-nucleon degrees of freedom at long distances to quark-gluon degrees of freedom at short scales. Ratios of separated response functions in $\pi^-$ and $\pi^+$ electroproduction are particularly informative. The ratio for transverse photons may allow this transition to be more easily observed, while the ratio for longitudinal photons provides a crucial verification of the assumed pole dominance, needed for reliable extraction of the pion form factor from electroproduction data. Read More


The Prime Focus Spectrograph (PFS) is an optical/near-infrared multi-fiber spectrograph with 2394 science fibers, which are distributed in 1.3 degree diameter field of view at Subaru 8.2-meter telescope. Read More

The Prime Focus Spectrograph (PFS) is a new optical/near-infrared multi-fiber spectrograph designed for the prime focus of the 8.2m Subaru telescope. The metrology camera system of PFS serves as the optical encoder of the COBRA fiber motors for the configuring of fibers. Read More

Authors: L. Tang1, C. Chen2, T. Gogami3, D. Kawama4, Y. Han5, L. Yuan6, A. Matsumura7, Y. Okayasu8, T. Seva9, V. M. Rodriguez10, P. Baturin11, A. Acha12, P. Achenbach13, A. Ahmidouch14, I. Albayrak15, D. Androic16, A. Asaturyan17, R. Asaturyan18, O. Ates19, R. Badui20, O. K. Baker21, F. Benmokhtar22, W. Boeglin23, J. Bono24, P. Bosted25, E. Brash26, P. Carter27, R. Carlini28, A. Chiba29, M. E. Christy30, L. Cole31, M. M. Dalton32, S. Danagoulian33, A. Daniel34, R. De Leo35, V. Dharmawardane36, D. Doi37, K. Egiyan38, M. Elaasar39, R. Ent40, H. Fenker41, Y. Fujii42, M. Furic43, M. Gabrielyan44, L. Gan45, F. Garibaldi46, D. Gaskell47, A. Gasparian48, E. F. Gibson49, P. Gueye50, O. Hashimoto51, D. Honda52, T. Horn53, B. Hu54, Ed V. Hungerford55, C. Jayalath56, M. Jones57, K. Johnston58, N. Kalantarians59, H. Kanda60, M. Kaneta61, F. Kato62, S. Kato63, M. Kawai64, C. Keppel65, H. Khanal66, M. Kohl67, L. Kramer68, K. J. Lan69, Y. Li70, A. Liyanage71, W. Luo72, D. Mack73, K. Maeda74, S. Malace75, A. Margaryan76, G. Marikyan77, P. Markowitz78, T. Maruta79, N. Maruyama80, V. Maxwell81, D. J. Millener82, T. Miyoshi83, A. Mkrtchyan84, H. Mkrtchyan85, T. Motoba86, S. Nagao87, S. N. Nakamura88, A. Narayan89, C. Neville90, G. Niculescu91, M. I. Niculescu92, A. Nunez93, Nuruzzaman94, H. Nomura95, K. Nonaka96, A. Ohtani97, M. Oyamada98, N. Perez99, T. Petkovic100, J. Pochodzalla101, X. Qiu102, S. Randeniya103, B. Raue104, J. Reinhold105, R. Rivera106, J. Roche107, C. Samanta108, Y. Sato109, B. Sawatzky110, E. K. Segbefia111, D. Schott112, A. Shichijo113, N. Simicevic114, G. Smith115, Y. Song116, M. Sumihama117, V. Tadevosyan118, T. Takahashi119, N. Taniya120, K. Tsukada121, V. Tvaskis122, M. Veilleux123, W. Vulcan124, S. Wells125, F. R. Wesselmann126, S. A. Wood127, T. Yamamoto128, C. Yan129, Z. Ye130, K. Yokota131, S. Zhamkochyan132, L. Zhu133
Affiliations: 1HKS - JLab E05-115 and E01-001 - Collaborations, 2HKS - JLab E05-115 and E01-001 - Collaborations, 3HKS - JLab E05-115 and E01-001 - Collaborations, 4HKS - JLab E05-115 and E01-001 - Collaborations, 5HKS - JLab E05-115 and E01-001 - Collaborations, 6HKS - JLab E05-115 and E01-001 - Collaborations, 7HKS - JLab E05-115 and E01-001 - Collaborations, 8HKS - JLab E05-115 and E01-001 - Collaborations, 9HKS - JLab E05-115 and E01-001 - Collaborations, 10HKS - JLab E05-115 and E01-001 - Collaborations, 11HKS - JLab E05-115 and E01-001 - Collaborations, 12HKS - JLab E05-115 and E01-001 - Collaborations, 13HKS - JLab E05-115 and E01-001 - Collaborations, 14HKS - JLab E05-115 and E01-001 - Collaborations, 15HKS - JLab E05-115 and E01-001 - Collaborations, 16HKS - JLab E05-115 and E01-001 - Collaborations, 17HKS - JLab E05-115 and E01-001 - Collaborations, 18HKS - JLab E05-115 and E01-001 - Collaborations, 19HKS - JLab E05-115 and E01-001 - Collaborations, 20HKS - JLab E05-115 and E01-001 - Collaborations, 21HKS - JLab E05-115 and E01-001 - Collaborations, 22HKS - JLab E05-115 and E01-001 - Collaborations, 23HKS - JLab E05-115 and E01-001 - Collaborations, 24HKS - JLab E05-115 and E01-001 - Collaborations, 25HKS - JLab E05-115 and E01-001 - Collaborations, 26HKS - JLab E05-115 and E01-001 - Collaborations, 27HKS - JLab E05-115 and E01-001 - Collaborations, 28HKS - JLab E05-115 and E01-001 - Collaborations, 29HKS - JLab E05-115 and E01-001 - Collaborations, 30HKS - JLab E05-115 and E01-001 - Collaborations, 31HKS - JLab E05-115 and E01-001 - Collaborations, 32HKS - JLab E05-115 and E01-001 - Collaborations, 33HKS - JLab E05-115 and E01-001 - Collaborations, 34HKS - JLab E05-115 and E01-001 - Collaborations, 35HKS - JLab E05-115 and E01-001 - Collaborations, 36HKS - JLab E05-115 and E01-001 - Collaborations, 37HKS - JLab E05-115 and E01-001 - Collaborations, 38HKS - JLab E05-115 and E01-001 - Collaborations, 39HKS - JLab E05-115 and E01-001 - Collaborations, 40HKS - JLab E05-115 and E01-001 - Collaborations, 41HKS - JLab E05-115 and E01-001 - Collaborations, 42HKS - JLab E05-115 and E01-001 - Collaborations, 43HKS - JLab E05-115 and E01-001 - Collaborations, 44HKS - JLab E05-115 and E01-001 - Collaborations, 45HKS - JLab E05-115 and E01-001 - Collaborations, 46HKS - JLab E05-115 and E01-001 - Collaborations, 47HKS - JLab E05-115 and E01-001 - Collaborations, 48HKS - JLab E05-115 and E01-001 - Collaborations, 49HKS - JLab E05-115 and E01-001 - Collaborations, 50HKS - JLab E05-115 and E01-001 - Collaborations, 51HKS - JLab E05-115 and E01-001 - Collaborations, 52HKS - JLab E05-115 and E01-001 - Collaborations, 53HKS - JLab E05-115 and E01-001 - Collaborations, 54HKS - JLab E05-115 and E01-001 - Collaborations, 55HKS - JLab E05-115 and E01-001 - Collaborations, 56HKS - JLab E05-115 and E01-001 - Collaborations, 57HKS - JLab E05-115 and E01-001 - Collaborations, 58HKS - JLab E05-115 and E01-001 - Collaborations, 59HKS - JLab E05-115 and E01-001 - Collaborations, 60HKS - JLab E05-115 and E01-001 - Collaborations, 61HKS - JLab E05-115 and E01-001 - Collaborations, 62HKS - JLab E05-115 and E01-001 - Collaborations, 63HKS - JLab E05-115 and E01-001 - Collaborations, 64HKS - JLab E05-115 and E01-001 - Collaborations, 65HKS - JLab E05-115 and E01-001 - Collaborations, 66HKS - JLab E05-115 and E01-001 - Collaborations, 67HKS - JLab E05-115 and E01-001 - Collaborations, 68HKS - JLab E05-115 and E01-001 - Collaborations, 69HKS - JLab E05-115 and E01-001 - Collaborations, 70HKS - JLab E05-115 and E01-001 - Collaborations, 71HKS - JLab E05-115 and E01-001 - Collaborations, 72HKS - JLab E05-115 and E01-001 - Collaborations, 73HKS - JLab E05-115 and E01-001 - Collaborations, 74HKS - JLab E05-115 and E01-001 - Collaborations, 75HKS - JLab E05-115 and E01-001 - Collaborations, 76HKS - JLab E05-115 and E01-001 - Collaborations, 77HKS - JLab E05-115 and E01-001 - Collaborations, 78HKS - JLab E05-115 and E01-001 - Collaborations, 79HKS - JLab E05-115 and E01-001 - Collaborations, 80HKS - JLab E05-115 and E01-001 - Collaborations, 81HKS - JLab E05-115 and E01-001 - Collaborations, 82HKS - JLab E05-115 and E01-001 - Collaborations, 83HKS - JLab E05-115 and E01-001 - Collaborations, 84HKS - JLab E05-115 and E01-001 - Collaborations, 85HKS - JLab E05-115 and E01-001 - Collaborations, 86HKS - JLab E05-115 and E01-001 - Collaborations, 87HKS - JLab E05-115 and E01-001 - Collaborations, 88HKS - JLab E05-115 and E01-001 - Collaborations, 89HKS - JLab E05-115 and E01-001 - Collaborations, 90HKS - JLab E05-115 and E01-001 - Collaborations, 91HKS - JLab E05-115 and E01-001 - Collaborations, 92HKS - JLab E05-115 and E01-001 - Collaborations, 93HKS - JLab E05-115 and E01-001 - Collaborations, 94HKS - JLab E05-115 and E01-001 - Collaborations, 95HKS - JLab E05-115 and E01-001 - Collaborations, 96HKS - JLab E05-115 and E01-001 - Collaborations, 97HKS - JLab E05-115 and E01-001 - Collaborations, 98HKS - JLab E05-115 and E01-001 - Collaborations, 99HKS - JLab E05-115 and E01-001 - Collaborations, 100HKS - JLab E05-115 and E01-001 - Collaborations, 101HKS - JLab E05-115 and E01-001 - Collaborations, 102HKS - JLab E05-115 and E01-001 - Collaborations, 103HKS - JLab E05-115 and E01-001 - Collaborations, 104HKS - JLab E05-115 and E01-001 - Collaborations, 105HKS - JLab E05-115 and E01-001 - Collaborations, 106HKS - JLab E05-115 and E01-001 - Collaborations, 107HKS - JLab E05-115 and E01-001 - Collaborations, 108HKS - JLab E05-115 and E01-001 - Collaborations, 109HKS - JLab E05-115 and E01-001 - Collaborations, 110HKS - JLab E05-115 and E01-001 - Collaborations, 111HKS - JLab E05-115 and E01-001 - Collaborations, 112HKS - JLab E05-115 and E01-001 - Collaborations, 113HKS - JLab E05-115 and E01-001 - Collaborations, 114HKS - JLab E05-115 and E01-001 - Collaborations, 115HKS - JLab E05-115 and E01-001 - Collaborations, 116HKS - JLab E05-115 and E01-001 - Collaborations, 117HKS - JLab E05-115 and E01-001 - Collaborations, 118HKS - JLab E05-115 and E01-001 - Collaborations, 119HKS - JLab E05-115 and E01-001 - Collaborations, 120HKS - JLab E05-115 and E01-001 - Collaborations, 121HKS - JLab E05-115 and E01-001 - Collaborations, 122HKS - JLab E05-115 and E01-001 - Collaborations, 123HKS - JLab E05-115 and E01-001 - Collaborations, 124HKS - JLab E05-115 and E01-001 - Collaborations, 125HKS - JLab E05-115 and E01-001 - Collaborations, 126HKS - JLab E05-115 and E01-001 - Collaborations, 127HKS - JLab E05-115 and E01-001 - Collaborations, 128HKS - JLab E05-115 and E01-001 - Collaborations, 129HKS - JLab E05-115 and E01-001 - Collaborations, 130HKS - JLab E05-115 and E01-001 - Collaborations, 131HKS - JLab E05-115 and E01-001 - Collaborations, 132HKS - JLab E05-115 and E01-001 - Collaborations, 133HKS - JLab E05-115 and E01-001 - Collaborations

Since the pioneering experiment, E89-009 studying hypernuclear spectroscopy using the $(e,e^{\prime}K^+)$ reaction was completed, two additional experiments, E01-011 and E05-115, were performed at Jefferson Lab. These later experiments used a modified experimental design, the "tilt method", to dramatically suppress the large electromagnetic background, and allowed for a substantial increase in luminosity. Additionally, a new kaon spectrometer, HKS (E01-011), a new electron spectrometer, HES, and a new splitting magnet were added to produce precision, high-resolution hypernuclear spectroscopy. Read More

Affiliations: 1The Jefferson Lab Fpi Collaboration, 2The Jefferson Lab Fpi Collaboration, 3The Jefferson Lab Fpi Collaboration, 4The Jefferson Lab Fpi Collaboration, 5The Jefferson Lab Fpi Collaboration, 6The Jefferson Lab Fpi Collaboration, 7The Jefferson Lab Fpi Collaboration, 8The Jefferson Lab Fpi Collaboration, 9The Jefferson Lab Fpi Collaboration, 10The Jefferson Lab Fpi Collaboration, 11The Jefferson Lab Fpi Collaboration, 12The Jefferson Lab Fpi Collaboration, 13The Jefferson Lab Fpi Collaboration, 14The Jefferson Lab Fpi Collaboration, 15The Jefferson Lab Fpi Collaboration, 16The Jefferson Lab Fpi Collaboration, 17The Jefferson Lab Fpi Collaboration, 18The Jefferson Lab Fpi Collaboration, 19The Jefferson Lab Fpi Collaboration, 20The Jefferson Lab Fpi Collaboration, 21The Jefferson Lab Fpi Collaboration, 22The Jefferson Lab Fpi Collaboration, 23The Jefferson Lab Fpi Collaboration, 24The Jefferson Lab Fpi Collaboration, 25The Jefferson Lab Fpi Collaboration, 26The Jefferson Lab Fpi Collaboration, 27The Jefferson Lab Fpi Collaboration, 28The Jefferson Lab Fpi Collaboration, 29The Jefferson Lab Fpi Collaboration, 30The Jefferson Lab Fpi Collaboration, 31The Jefferson Lab Fpi Collaboration, 32The Jefferson Lab Fpi Collaboration, 33The Jefferson Lab Fpi Collaboration, 34The Jefferson Lab Fpi Collaboration, 35The Jefferson Lab Fpi Collaboration, 36The Jefferson Lab Fpi Collaboration, 37The Jefferson Lab Fpi Collaboration, 38The Jefferson Lab Fpi Collaboration, 39The Jefferson Lab Fpi Collaboration, 40The Jefferson Lab Fpi Collaboration, 41The Jefferson Lab Fpi Collaboration, 42The Jefferson Lab Fpi Collaboration, 43The Jefferson Lab Fpi Collaboration, 44The Jefferson Lab Fpi Collaboration, 45The Jefferson Lab Fpi Collaboration, 46The Jefferson Lab Fpi Collaboration, 47The Jefferson Lab Fpi Collaboration, 48The Jefferson Lab Fpi Collaboration, 49The Jefferson Lab Fpi Collaboration, 50The Jefferson Lab Fpi Collaboration, 51The Jefferson Lab Fpi Collaboration, 52The Jefferson Lab Fpi Collaboration, 53The Jefferson Lab Fpi Collaboration, 54The Jefferson Lab Fpi Collaboration, 55The Jefferson Lab Fpi Collaboration, 56The Jefferson Lab Fpi Collaboration, 57The Jefferson Lab Fpi Collaboration, 58The Jefferson Lab Fpi Collaboration, 59The Jefferson Lab Fpi Collaboration, 60The Jefferson Lab Fpi Collaboration, 61The Jefferson Lab Fpi Collaboration, 62The Jefferson Lab Fpi Collaboration, 63The Jefferson Lab Fpi Collaboration, 64The Jefferson Lab Fpi Collaboration, 65The Jefferson Lab Fpi Collaboration, 66The Jefferson Lab Fpi Collaboration, 67The Jefferson Lab Fpi Collaboration, 68The Jefferson Lab Fpi Collaboration, 69The Jefferson Lab Fpi Collaboration, 70The Jefferson Lab Fpi Collaboration, 71The Jefferson Lab Fpi Collaboration, 72The Jefferson Lab Fpi Collaboration, 73The Jefferson Lab Fpi Collaboration, 74The Jefferson Lab Fpi Collaboration, 75The Jefferson Lab Fpi Collaboration, 76The Jefferson Lab Fpi Collaboration, 77The Jefferson Lab Fpi Collaboration, 78The Jefferson Lab Fpi Collaboration, 79The Jefferson Lab Fpi Collaboration, 80The Jefferson Lab Fpi Collaboration, 81The Jefferson Lab Fpi Collaboration, 82The Jefferson Lab Fpi Collaboration, 83The Jefferson Lab Fpi Collaboration, 84The Jefferson Lab Fpi Collaboration, 85The Jefferson Lab Fpi Collaboration, 86The Jefferson Lab Fpi Collaboration, 87The Jefferson Lab Fpi Collaboration, 88The Jefferson Lab Fpi Collaboration

The study of exclusive $\pi^{\pm}$ electroproduction on the nucleon, including separation of the various structure functions, is of interest for a number of reasons. The ratio $R_L=\sigma_L^{\pi^-}/\sigma_L^{\pi^+}$ is sensitive to isoscalar contamination to the dominant isovector pion exchange amplitude, which is the basis for the determination of the charged pion form factor from electroproduction data. A change in the value of $R_T=\sigma_T^{\pi^-}/\sigma_T^{\pi^+}$ from unity at small $-t$, to 1/4 at large $-t$, would suggest a transition from coupling to a (virtual) pion to coupling to individual quarks. Read More

It was proved by Rubey that the number of fillings with zeros and ones of a given moon polyomino that do not contain a northeast chain of size $k$ depends only on the set of columns of the polyomino, but not the shape of the polyomino. Rubey's proof is an adaption of jeu de taquin and promotion for arbitrary fillings of moon polyominoes. In this paper we present a bijective proof for this result by considering fillings of almost-moon polyominoes, which are moon polyominoes after removing one of the rows. Read More

Sub-parsec binary massive black holes (BBHs) are long anticipated to exist in many QSOs but remain observationally elusive. In this paper, we propose a novel method to probe sub-parsec BBHs through microlensing of lensed QSOs. If a QSO hosts a sub-parsec BBH in its center, it is expected that the BBH is surrounded by a circum-binary disk, each component of the BBH is surrounded by a small accretion disk, and a gap is opened by the secondary component in between the circum-binary disk and the two small disks. Read More

The surface of a topological crystalline insulator (TCI) carries an even number of Dirac cones protected by crystalline symmetry. We epitaxially grew high quality Pb$_{1-x}$Sn$_x$Te(111) films and investigated the TCI phase by in-situ angle-resolved photoemission spectroscopy. Pb$_{1-x}$Sn$_x$Te(111) films undergo a topological phase transition from trivial insulator to TCI via increasing the Sn/Pb ratio, accompanied by a crossover from n-type to p-type doping. Read More

Transshipment problem is one of the basic operational research problems. In this paper, our first work is to develop a biologically inspired mathematical model for a dynamical system, which is first used to solve minimum cost flow problem. It has lower computational complexity than Physarum Solver. Read More

A fluorescence system is developed by using several light emitting diodes (LEDs) with different wavelengths as excitation light sources. The fluorescence detection head consists of multi LED light sources and a multimode fiber for fluorescence collection, where the LEDs and the corresponding filters can be easily chosen to get appropriate excitation wavelengths for different applications. By analyzing fluorescence spectra with the principal component analysis method, the system is utilized in the classification of four types of green tea beverages and two types of black tea beverages. Read More

The Prime Focus Spectrograph (PFS) of the Subaru Measurement of Images and Redshifts (SuMIRe) project has been endorsed by Japanese community as one of the main future instruments of the Subaru 8.2-meter telescope at Mauna Kea, Hawaii. This optical/near-infrared multi-fiber spectrograph targets cosmology with galaxy surveys, Galactic archaeology, and studies of galaxy/AGN evolution. Read More

In this paper, we will present a new approach for solving Laplace equations in general 3-D domains. The approach is based on a local computation method for the DtN mapping of the Laplace equation by combining a deterministic (local) boundary integral equation method and the probabilistic Feynman-Kac formula of PDE solutions. This hybridization produces a parallel algorithm where the bulk of the computation has no need for data communications. Read More

Affiliations: 1HKS, 2HKS, 3HKS, 4HKS, 5HKS, 6HKS, 7HKS, 8HKS, 9HKS, 10HKS, 11HKS, 12HKS, 13HKS, 14HKS, 15HKS, 16HKS, 17HKS, 18HKS, 19HKS, 20HKS, 21HKS, 22HKS, 23HKS, 24HKS, 25HKS, 26HKS, 27HKS, 28HKS, 29HKS, 30HKS, 31HKS, 32HKS, 33HKS, 34HKS, 35HKS, 36HKS, 37HKS, 38HKS, 39HKS, 40HKS, 41HKS, 42HKS, 43HKS, 44HKS, 45HKS, 46HKS, 47HKS, 48HKS, 49HKS, 50HKS, 51HKS, 52HKS, 53HKS, 54HKS, 55HKS, 56HKS, 57HKS, 58HKS, 59HKS, 60HKS, 61HKS, 62HKS, 63HKS, 64HKS, 65HKS, 66HKS, 67HKS, 68HKS, 69HKS, 70HKS, 71HKS, 72HKS, 73HKS, 74HKS, 75HKS, 76HKS, 77HKS, 78HKS, 79HKS, 80HKS, 81HKS, 82HKS, 83HKS, 84HKS, 85HKS, 86HKS, 87HKS, 88HKS, 89HKS, 90HKS, 91HKS, 92HKS, 93HKS

An experiment with a newly developed high-resolution kaon spectrometer (HKS) and a scattered electron spectrometer with a novel configuration was performed in Hall C at Jefferson Lab (JLab). The ground state of a neutron-rich hypernucleus, He 7 Lambda, was observed for the first time with the (e,e'K+) reaction with an energy resolution of ~0.6 MeV. Read More

FS Tau B is one of the few T Tauri stars that possess a jet and a counterjet as well as an optically-visible cavity wall. We obtained images and spectra of its jet-cavity system in the near-infrared H and K bands using Subaru/IRCS and detected the jet and the counterjet in the [Fe II] 1.644 \mu m line for the first time. Read More

Using a sample of BzK-selected galaxies at z~2 identified from the CFHT/WIRCAM near-infrared survey of GOODS-North, we discuss the relation between star formation rate (SFR), specific star formation rate (SSFR), and stellar mass (M_{*}), and the clustering of galaxies as a function of these parameters. For star-forming galaxies (sBzKs), the UV-based SFR, corrected for extinction, scales with the stellar mass as SFR ~ M_{*}^{alpha} with alpha = 0.74+/-0. Read More

It has been suggested that the high metallicity generally observed in active galactic nuclei (AGNs) and quasars originates from ongoing star formation in the self-gravitating part of accretion disks around the supermassive black holes. We designate this region as the star forming (SF) disk, in which metals are produced from supernova explosions (SNexp) while at the same time inflows are driven by SNexp-excited turbulent viscosity to accrete onto the SMBHs. In this paper, an equation of metallicity governed by SNexp and radial advection is established to describe the metal distribution and evolution in the SF disk. Read More

We observed the Sh 2-233IR (S233IR) region with better sensitivity in near-infrared than previous studies for this region. By applying statistical subtraction of the back- ground stars, we identified member sources and derived the age and mass of three distinguishable sub-groups in this region: Sh 2-233IR NE, Sh 2-233IR SW, and the "distributed stars" over the whole cloud. Star formation may be occurring sequentially with a relatively small age difference (\sim 0. Read More

Authors: G0 Collaboration, D. Androic, D. S. Armstrong, J. Arvieux, R. Asaturyan, T. D. Averett, S. L. Bailey, G. Batigne, D. H. Beck, E. J. Beise, J. Benesch, F. Benmokhtar, L. Bimbot, J. Birchall, A. Biselli, P. Bosted, H. Breuer, P. Brindza, C. L. Capuano, R. D. Carlini, R. Carr, N. Chant, Y. -C. Chao, R. Clark, A. Coppens, S. D. Covrig, A. Cowley, D. Dale, C. A. Davis, C. Ellis, W. R. Falk, H. Fenker, J. M. Finn, T. Forest, G. Franklin, R. Frascaria, C. Furget, D. Gaskell, M. T. W. Gericke, J. Grames, K. A. Griffioen, K. Grimm, G. Guillard, B. Guillon, H. Guler, K. Gustafsson, L. Hannelius, J. Hansknecht, R. D. Hasty, A. M. Hawthorne Allen, T. Horn, T. M. Ito, K. Johnston, M. Jones, P. Kammel, R. Kazimi, P. M. King, A. Kolarkar, E. Korkmaz, W. Korsch, S. Kox, J. Kuhn, J. Lachniet, R. Laszewski, L. Lee, J. Lenoble, E. Liatard, J. Liu, A. Lung, G. A. MacLachlan, J. Mammei, D. Marchand, J. W. Martin, D. J. Mack, K. W. McFarlane, D. W. McKee, R. D. McKeown, F. Merchez, M. Mihovilovic, A. Micherdzinska, H. Mkrtchyan, B. Moffit, M. Morlet, M. Muether, J. Musson, K. Nakahara, R. Neveling, S. Niccolai, D. Nilsson, S. Ong, S. A. Page, V. Papavassiliou, S. F. Pate, S. K. Phillips, P. Pillot, M. L. Pitt, M. Poelker, T. A. Porcelli, G. Quemener, B. P. Quinn, W. D. Ramsay, A. W. Rauf, J. -S. Real, T. Ries, J. Roche P. Roos, G. A. Rutledge, J. Schaub, J. Secrest, T. Seva, N. Simicevic, G. R. Smith, D. T. Spayde, S. Stepanyan, M. Stutzman, R. Suleiman, V. Tadevosyan, R. Tieulent, J. van de Wiele, W. T. H. van Oers, M. Versteegen, E. Voutier, W. F. Vulcan, S. P. Wells, G. Warren, S. E. Williamson, R. J. Woo, S. A. Wood, C. Yan, J. Yun, V. Zeps

In the G0 experiment, performed at Jefferson Lab, the parity-violating elastic scattering of electrons from protons and quasi-elastic scattering from deuterons is measured in order to determine the neutral weak currents of the nucleon. Asymmetries as small as 1 part per million in the scattering of a polarized electron beam are determined using a dedicated apparatus. It consists of specialized beam-monitoring and control systems, a cryogenic hydrogen (or deuterium) target, and a superconducting, toroidal magnetic spectrometer equipped with plastic scintillation and aerogel Cerenkov detectors, as well as fast readout electronics for the measurement of individual events. Read More

We give a complete proof of a set of identities (7) proposed recently from calculation of high-energy string scattering amplitudes. These identities allow one to extract ratios among high-energy string scattering amplitudes in the fixed angle regime from high-energy amplitudes in the Regge regime. The proof is based on a signless Stirling number identity in combinatorial theory. Read More

(Abridged) High redshift galaxies are undergoing intensive evolution of dynamical structure and morphologies. We incorporate the feedback into the dynamical equations through mass dropout and angular momentum transportation driven by the SNexp-excited turbulent viscosity. We numerically solve the equations and show that there can be intensive evolution of structure of the gaseous disk. Read More

Self-gravitating accretion disks collapse to star-forming(SF) regions extending to the inner edge of the dusty torus in active galactic nuclei (AGNs). A full set of equations including feedback of star formation is given to describe the dynamics of the regions. We explore the role of supernovae explosion (SNexp), acting to excite turbulent viscosity, in the transportation of angular momentum in the regions within 1pc scale. Read More

We present a near-infrared extinction study of nine dense cores at evolutionary stages between starless to Class I. Our results show that the density structure of all but one observed cores can be modeled with a single power law rho \propto r^p between ~ 0.2R-R of the cores. Read More

Affiliations: 1The Tibet ASgamma Collaboration, 2The Tibet ASgamma Collaboration, 3The Tibet ASgamma Collaboration, 4The Tibet ASgamma Collaboration, 5The Tibet ASgamma Collaboration, 6The Tibet ASgamma Collaboration, 7The Tibet ASgamma Collaboration, 8The Tibet ASgamma Collaboration, 9The Tibet ASgamma Collaboration, 10The Tibet ASgamma Collaboration, 11The Tibet ASgamma Collaboration, 12The Tibet ASgamma Collaboration, 13The Tibet ASgamma Collaboration, 14The Tibet ASgamma Collaboration, 15The Tibet ASgamma Collaboration, 16The Tibet ASgamma Collaboration, 17The Tibet ASgamma Collaboration, 18The Tibet ASgamma Collaboration, 19The Tibet ASgamma Collaboration, 20The Tibet ASgamma Collaboration, 21The Tibet ASgamma Collaboration, 22The Tibet ASgamma Collaboration, 23The Tibet ASgamma Collaboration, 24The Tibet ASgamma Collaboration, 25The Tibet ASgamma Collaboration, 26The Tibet ASgamma Collaboration, 27The Tibet ASgamma Collaboration, 28The Tibet ASgamma Collaboration, 29The Tibet ASgamma Collaboration, 30The Tibet ASgamma Collaboration, 31The Tibet ASgamma Collaboration, 32The Tibet ASgamma Collaboration, 33The Tibet ASgamma Collaboration, 34The Tibet ASgamma Collaboration, 35The Tibet ASgamma Collaboration, 36The Tibet ASgamma Collaboration, 37The Tibet ASgamma Collaboration, 38The Tibet ASgamma Collaboration, 39The Tibet ASgamma Collaboration, 40The Tibet ASgamma Collaboration, 41The Tibet ASgamma Collaboration, 42The Tibet ASgamma Collaboration, 43The Tibet ASgamma Collaboration, 44The Tibet ASgamma Collaboration, 45The Tibet ASgamma Collaboration, 46The Tibet ASgamma Collaboration, 47The Tibet ASgamma Collaboration, 48The Tibet ASgamma Collaboration, 49The Tibet ASgamma Collaboration, 50The Tibet ASgamma Collaboration, 51The Tibet ASgamma Collaboration, 52The Tibet ASgamma Collaboration, 53The Tibet ASgamma Collaboration, 54The Tibet ASgamma Collaboration, 55The Tibet ASgamma Collaboration, 56The Tibet ASgamma Collaboration, 57The Tibet ASgamma Collaboration, 58The Tibet ASgamma Collaboration, 59The Tibet ASgamma Collaboration, 60The Tibet ASgamma Collaboration, 61The Tibet ASgamma Collaboration, 62The Tibet ASgamma Collaboration, 63The Tibet ASgamma Collaboration, 64The Tibet ASgamma Collaboration, 65The Tibet ASgamma Collaboration, 66The Tibet ASgamma Collaboration, 67The Tibet ASgamma Collaboration, 68The Tibet ASgamma Collaboration, 69The Tibet ASgamma Collaboration, 70The Tibet ASgamma Collaboration, 71The Tibet ASgamma Collaboration, 72The Tibet ASgamma Collaboration, 73The Tibet ASgamma Collaboration, 74The Tibet ASgamma Collaboration, 75The Tibet ASgamma Collaboration, 76The Tibet ASgamma Collaboration, 77The Tibet ASgamma Collaboration, 78The Tibet ASgamma Collaboration, 79The Tibet ASgamma Collaboration, 80The Tibet ASgamma Collaboration, 81The Tibet ASgamma Collaboration, 82The Tibet ASgamma Collaboration, 83The Tibet ASgamma Collaboration, 84The Tibet ASgamma Collaboration

Using the Tibet-III air shower array, we search for TeV gamma-rays from 27 potential Galactic sources in the early list of bright sources obtained by the Fermi Large Area Telescope at energies above 100 MeV. Among them, we observe 7 sources instead of the expected 0.61 sources at a significance of 2 sigma or more excess. Read More

We present new near-IR H2, CO J=2-1, and CO J = 3-2 observations to study outflows in the massive star forming region IRAS 05358+3543. The Canada-France-Hawaii Telescope H2 images and James Clerk Maxwell Telescope CO data cubes of the IRAS 05358 region reveal several new outflows, most of which emerge from the dense cluster of sub-mm cores associated with the Sh 2-233IR NE cluster to the northeast of IRAS 05358. We used Apache Point Observatory (APO) JHK spectra to determine line of sight velocities of the outflowing material. Read More

Affiliations: 1The Tibet AS gamma Collaboration, 2The Tibet AS gamma Collaboration, 3The Tibet AS gamma Collaboration, 4The Tibet AS gamma Collaboration, 5The Tibet AS gamma Collaboration, 6The Tibet AS gamma Collaboration, 7The Tibet AS gamma Collaboration, 8The Tibet AS gamma Collaboration, 9The Tibet AS gamma Collaboration, 10The Tibet AS gamma Collaboration, 11The Tibet AS gamma Collaboration, 12The Tibet AS gamma Collaboration, 13The Tibet AS gamma Collaboration, 14The Tibet AS gamma Collaboration, 15The Tibet AS gamma Collaboration, 16The Tibet AS gamma Collaboration, 17The Tibet AS gamma Collaboration, 18The Tibet AS gamma Collaboration, 19The Tibet AS gamma Collaboration, 20The Tibet AS gamma Collaboration, 21The Tibet AS gamma Collaboration, 22The Tibet AS gamma Collaboration, 23The Tibet AS gamma Collaboration, 24The Tibet AS gamma Collaboration, 25The Tibet AS gamma Collaboration, 26The Tibet AS gamma Collaboration, 27The Tibet AS gamma Collaboration, 28The Tibet AS gamma Collaboration, 29The Tibet AS gamma Collaboration, 30The Tibet AS gamma Collaboration, 31The Tibet AS gamma Collaboration, 32The Tibet AS gamma Collaboration, 33The Tibet AS gamma Collaboration, 34The Tibet AS gamma Collaboration, 35The Tibet AS gamma Collaboration, 36The Tibet AS gamma Collaboration, 37The Tibet AS gamma Collaboration, 38The Tibet AS gamma Collaboration, 39The Tibet AS gamma Collaboration, 40The Tibet AS gamma Collaboration, 41The Tibet AS gamma Collaboration, 42The Tibet AS gamma Collaboration, 43The Tibet AS gamma Collaboration, 44The Tibet AS gamma Collaboration, 45The Tibet AS gamma Collaboration, 46The Tibet AS gamma Collaboration, 47The Tibet AS gamma Collaboration, 48The Tibet AS gamma Collaboration, 49The Tibet AS gamma Collaboration, 50The Tibet AS gamma Collaboration, 51The Tibet AS gamma Collaboration, 52The Tibet AS gamma Collaboration, 53The Tibet AS gamma Collaboration, 54The Tibet AS gamma Collaboration, 55The Tibet AS gamma Collaboration, 56The Tibet AS gamma Collaboration, 57The Tibet AS gamma Collaboration, 58The Tibet AS gamma Collaboration, 59The Tibet AS gamma Collaboration, 60The Tibet AS gamma Collaboration, 61The Tibet AS gamma Collaboration, 62The Tibet AS gamma Collaboration, 63The Tibet AS gamma Collaboration, 64The Tibet AS gamma Collaboration, 65The Tibet AS gamma Collaboration, 66The Tibet AS gamma Collaboration, 67The Tibet AS gamma Collaboration, 68The Tibet AS gamma Collaboration, 69The Tibet AS gamma Collaboration, 70The Tibet AS gamma Collaboration, 71The Tibet AS gamma Collaboration, 72The Tibet AS gamma Collaboration, 73The Tibet AS gamma Collaboration, 74The Tibet AS gamma Collaboration, 75The Tibet AS gamma Collaboration, 76The Tibet AS gamma Collaboration, 77The Tibet AS gamma Collaboration, 78The Tibet AS gamma Collaboration, 79The Tibet AS gamma Collaboration, 80The Tibet AS gamma Collaboration, 81The Tibet AS gamma Collaboration, 82The Tibet AS gamma Collaboration, 83The Tibet AS gamma Collaboration, 84The Tibet AS gamma Collaboration, 85The Tibet AS gamma Collaboration

We develop a model anisotropy best-fitting to the two-dimensional sky-map of multi-TeV galactic cosmic ray (GCR) intensity observed with the Tibet III air shower (AS) array. By incorporating a pair of intensity excesses in the hydrogen deflection plane (HDP) suggested by Gurnett et al., together with the uni-directional and bi-directional flows for reproducing the observed global feature, this model successfully reproduces the observed sky-map including the "skewed" feature of the excess intensity from the heliotail direction, whose physical origin has long remained unknown. Read More

We establish a stronger symmetry between the numbers of northeast and southeast chains in the context of 01-fillings of moon polyominoes. Let $\M$ be a moon polyomino with $n$ rows and $m$ columns. Consider all the 01-fillings of $\M$ in which every row has at most one 1. Read More

Motivated by Genzel et al.'s observations of high-redshift star-forming galaxies, containing clumpy and turbulent rings or disks, we build a set of equations describing the dynamical evolution of gaseous disks with inclusion of star formation and its feedback. Transport of angular momentum is due to "turbulent" viscosity induced by supernova explosions in the star formation region. Read More

The growth of supermassive black holes (BHs) located at the centers of their host galaxies comes mainly from accretion of gas, but how to fuel them remains an outstanding unsolved problem in quasar evolution. This issue can be elucidated by quantifying the radiative efficiency parameter ($\eta$) as a function of redshift, which also provides constraints on the average spin of the BHs and its possible evolution with time. We derive a formalism to link $\eta$ with the luminosity density, BH mass density, and duty cycle of quasars, quantities we can estimate from existing quasar and galaxy survey data. Read More

Tracing the star formation history in circumnuclear regions (CNRs) is a key step towards understanding the starburst-AGN connection. However, bright nuclei outshining the entire host galaxy prevent the analysis of the stellar populations of CNRs around type-I AGNs. Obscuration of the nuclei by the central torus provides an unique opportunity to study the stellar populations of AGN host galaxies. Read More

We propose a major index statistic on 01-fillings of moon polyominoes which, when specialized to certain shapes, reduces to the major index for permutations and set partitions. We consider the set F(M, s; A) of all 01-fillings of a moon polyomino M with given column sum s whose empty rows are A, and prove that this major index has the same distribution as the number of north-east chains, which are the natural extension of inversions (resp. crossings) for permutations (resp. Read More

Affiliations: 1nee Rohe, 2nee Rohe, 3nee Rohe, 4nee Rohe, 5nee Rohe, 6nee Rohe, 7nee Rohe, 8nee Rohe, 9nee Rohe, 10nee Rohe, 11nee Rohe, 12nee Rohe, 13nee Rohe, 14nee Rohe, 15nee Rohe, 16nee Rohe, 17nee Rohe, 18nee Rohe, 19nee Rohe, 20nee Rohe, 21nee Rohe, 22nee Rohe, 23nee Rohe, 24nee Rohe, 25nee Rohe, 26nee Rohe, 27nee Rohe, 28nee Rohe, 29nee Rohe, 30nee Rohe, 31nee Rohe, 32nee Rohe, 33nee Rohe, 34nee Rohe, 35nee Rohe, 36nee Rohe, 37nee Rohe, 38nee Rohe, 39nee Rohe, 40nee Rohe, 41nee Rohe, 42nee Rohe, 43nee Rohe, 44nee Rohe, 45nee Rohe, 46nee Rohe, 47nee Rohe, 48nee Rohe, 49nee Rohe, 50nee Rohe, 51nee Rohe, 52nee Rohe

We have extracted QCD matrix elements from our data on double polarized inelastic scattering of electrons on nuclei. We find the higher twist matrix element \tilde{d_2}, which arises strictly from quark- gluon interactions, to be unambiguously non zero. The data also reveal an isospin dependence of higher twist effects if we assume that the Burkhardt-Cottingham Sum rule is valid. Read More

Cross sections for the reaction ${^1}$H($e,e'\pi^+$)$n$ were measured in Hall C at Thomas Jefferson National Accelerator Facility (JLab) using the CEBAF high-intensity, continous electron beam in order to determine the charged pion form factor. Data were taken for central four-momentum transfers ranging from $Q^2$=0.60 to 2. Read More