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The six articles presented in this journal are: I. Research in Action: The Transfer of Research in Music and Music Education into the Classroom by Jack R. Stephenson; II. Programmed Instruction and Music Education by Douglas L. Turpin; III. Music Education and the Blind by Joan Thief Gagnepain; IV. Improved Teaching Through the Use of the Videotaperecorder by Paul D. Rodabaugh; V. Development of a Methodology for Transcribing the Organ Music of Bach for Band by James M. Burk; and VI. Humanities, Integrated Arts, and Aesthetic Education by William D. Gaver. Dissertation Abstracts listed in chapter VII are as follows: A Basic Method of Group Instruction for Beginning Church Organists by Sister Dorothy Venhouse; An Investigation of the Vibrating Clarinet Reed Utilizing High Speed Cinematography by Roger Dean Coppenbarger; A Study of Interviewing Practices and Techniques Utilized in the Screening of Prospective Music Personnel in Departments of Music in Institutions of Higher Education by Joseph M. Hegstad; A Study of Rehearsal Techniques for Symphonic Band by William N. Vereen, Jr.; A Study of the Application of Creativity in the Teaching of Secondary School Music by Elwood H. Brown; Music Departments of Colleges or Universities and Public Schools--Interrelationships by Jesse Laurence Peterson; and Serial Compositions for Band by Robert Lowell Casey. (LS)

We report the first detection of a credible progenitor system for a Type Ic supernova (SN Ic), SN 2017ein. We present spectra and photometry of the SN, finding it to be similar to carbon-rich, low-luminosity SNe Ic. Using a post-explosion Keck adaptive optics image, we precisely determine the position of SN 2017ein in pre-explosion \hst\ images, finding a single source coincident with the SN position. This source is marginally extended, and is consistent with being a stellar cluster. However, under the assumption that the emission of this source is dominated by a single point source, we perform point-spread function photometry, and correcting for line-of-sight reddening, we find it to have $M_{\rm F555W} = -7.5\pm0.2$ mag and $m_{\rm F555W}-m_{\rm F814W}$=$-0.67\pm0.14$ mag. This source is bluer than the main sequence and brighter than almost all Wolf-Rayet stars, however it is similar to some WC+O- and B-star binary systems. Under the assumption that the source is dominated by a single star, we find that it had an initial mass of $55\substack{+20-15} M_{\odot}$. We also examined binary star models to look for systems that match the overall photometry of the pre-explosion source and found that the best-fitting model is a $80$+$48 M_{\odot}$ close binary system in which the $80 M_{\odot}$ star is stripped and explodes as a lower mass star. Late-time photometry after the SN has faded will be necessary to cleanly separate the progenitor star emission from the additional coincident emission., Comment: 13 pages, 8 figures, published in MNRAS

Since the start of operations in 1993, the twin 10 meter W. M. Keck Observatory telescopes have continued to maximize their scientific impact and to produce transformative discoveries that keep the observing community on the frontiers of astronomical research. Upgraded capabilities and new instrumentation are provided though collaborative partnerships with Caltech and UC instrument development teams. The observatory adapts and responds to the observers’ evolving needs as defined in the observatory’s strategic plan, periodically refreshed in collaboration with the science community. This paper summarizes the performance of recently commissioned infrastructure projects, technology upgrades, and new additions to the suite of instrumentation at the observatory. We will also provide a status of projects currently in the design or development phase, and since we need to keep our eye on the future, we mention projects in exploratory phases that originate from our strategic plan. Recently commissioned projects include telescope control system upgrades, OSIRIS spectrometer and imager upgrades, and deployments of the Keck Cosmic Web Imager (KCWI), the Near-Infrared Echellette Spectrometer (NIRES), and the Keck I Deployable Tertiary Mirror (KIDM3). Under development are upgrades to the NIRSPEC instrument and adaptive optics (AO) system. Major instrumentation in design phases include the Keck Cosmic Reionization Mapper and the Keck Planet Finder. Future instrumentation studies and proposals underway include a Ground Layer Adaptive Optics system, NIRC2 upgrades, the energy sensitive instrument KRAKENS, an integral field spectrograph LIGER, and a laser tomography AO upgrade. Last, we briefly discuss recovering MOSFIRE and its return to science operations.

Motivated by the ever increasing pursuit of science with the transient sky (dubbed Time Domain Astronomy or TDA), we are fabricating and will commission a new deployable tertiary mirror for the Keck I telescope (K1DM3) at the W.M. Keck Observatory. This paper presents the detailed design of K1DM3 with emphasis on the opto-mechanics. This project has presented several design challenges. Foremost are the competing requirements to avoid vignetting the light path when retracted against a sufficiently rigid system for high-precision and repeatable pointing. The design utilizes an actuated swing arm to retract the mirror or deploy it into a kinematic coupling. The K1DM3 project has also required the design and development of custom connections to provide power, communications, and compressed air to the system. This NSF-MRI funded project is planned to be commissioned in Spring 2017., 22 pages; many figures; Published in SPIE

The Keck Observatory began science observations with a laser guide star adaptive optics system, the first such system on an 8-10 m class telescope, in late 2004. This new capability greatly extends the scientific potential of the Keck II Telescope, allowing near-diffraction-limited observations in the near-infrared using natural guide stars as faint as 19th magnitude. This paper describes the conceptual approach and technical implementation followed for this system, including lessons learned, and provides an overview of the early science capabilities.

We describe the goals, guiding principles, and implementation of the Keck Observatory technical operations model and how scientific success is critically dependent on the symbiotic connection with the overall strategy of the observatory. We examine management approaches, organization and staffing that result from this approach. We discuss the choices made at the observatory in balancing regular operations and new scientific and technical capabilities, and the tradeoffs and consequences of these choices. We then elaborate on our plans to evolve operations in the areas of people and processes over the next several years. Finally, we address the applicability of the Keck model to the next generation of telescopes.

In order to validate various assumptions about the operating environment of the Thirty Meter Telescope (TMT), to validate the modeling packages being used to guide the design work for the TMT and to directly investigate the expected operation of several subsystems we have embarked on an extensive campaign of environmental measurements at the Keck telescopes. We have measured and characterized the vibration environment around the observatory floor and at certain locations on the telescope over a range of operating conditions. Similarly the acoustic environment around the telescope and primary mirror has been characterized for frequencies above 2 Hz. The internal and external wind and temperature fields are being measured using combined sonic anemometer and PRT sensors. We are measuring the telescope position error and drive torque signals in order to investigate the wind induced telescope motions. A scintillometer mounted on the telescope is measuring the optical turbulence inside the telescope tube. This experimental work is supplemented by an extensive analysis of telescope and engineering sensor log files and measurements, primarily those of accelerometers located on the main telescope optics, primary mirror segment edge sensor error signals (residuals), telescope structure temperature measurements and the telescope status information.

In this paper we describe both recently completed instrumentation projects and our current development efforts in terms of their role in the strategic plan, the key science areas they address, and their performance as measured or predicted. Projects reaching completion in 2012 include MOSFIRE, a near IR multi-object spectrograph, a laser guide star adaptive optics facility on the Keck I telescope, and an upgrade to the guide camera for the HIRES instrument on Keck I. Projects in development include a new seeing limited integral field spectrograph for the visible wavelength range called the Keck Cosmic Web Imager (KCWI), an upgrade to the telescope control systems on both Keck telescopes, a near-IR tip/tilt sensor for the Keck I adaptive optics system, and a new grating for the OSIRIS integral field spectrograph.

The operations model of the Keck Observatory and the factors that allow it to operate with unprecedented scientific success while maintaining the lowest operating cost to capital ratio of the 8m-10m class of telescopes are examined. We describe matching of resources to operating requirements and steps taken to optimize the effectiveness of the overall operation. We describe how strategic goals, operating philosophy and detailed planning mesh to match science objectives with technological capability. We conclude by examining how operations design drives both long term operating cost and realization of the potential inherent in the initial capital investment.

We examine the factors that drive the size and cost of software for a hypothetical 30 meter telescope and compare those to that of a hypothetical 10 meter telescope. Our goal is to explore methods for developing estimates for such costs. The estimates provided here are intended primarily as examples for these methods, and should not be construed as accurate.

The Keck II telescope control system is a completely new design from the Keck I system. The entire software project, design, implementation and commissioning, has taken 16 months from inception in January 1995 to completion of all major subsystems in April 1996. First light took place in January 1996, and scientific quality images were taken in April 1996. Full operations are planned for October 1996. This paper focuses on the management and software engineering practices and the software tools that made it possible to complete a project of this magnitude with the limited time and resources at our disposal. Areas of potential software sharing and collaboration with other observatories are also discussed.

The experimental physics and industrial control system (EPICS) originated in the high energy physics community and has been used for several years to control accelerators. It is now in use or soon to be in use at several observatories around the world. In 1995, it was decided that Keck II telescope would have a new EPICS-based control system rather than use a copy of the Keck I system. This decision was made because it was felt that EPICS provided a superior software infrastructure to that developed for Keck I, and that it would scale well to encompass adaptive optics and eventual use of the two telescopes for interferometry. The new control system was developed throughout 1995 and the early part of 1996, leading to first light in January 1996, making it the first fully EPICS-controlled telescope control system in the world. This paper describes how EPICS has been used to implement the control system, including a detailed discussion of the axes control, pointing and timing system, and of how they interact with each other.© (1997) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.

The servo design and model of the W. M. Keck telescopes autoguider is presented. Telescope servo models often do not include the guider loop and therefore do not take advantage of traditional control analysis and test techniques to improve performance. Guide camera dynamics, computational and transport lags, and compensation networks are discussed. A means of measuring the actual frequency response characteristics of the guide loop is presented and the results are compared to those predicted by the model. Guide performance as a function of integration time is illustrated. An improved compensation network is developed and its performance examined.© (1997) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.

The achieved pointing and tracking performance of the telescope is presented and compared with the Keck goals. The implications of the current performance on observing are discussed, and planned remedies for deficiencies in pointing and tracking are proposed.© (1994) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.

The computing environment and major components of the Keck telescope control system are discussed. This is followed by a discussion of calibration procedures and a review of current status and problems.

The VLT Survey Telescope (VST) is a cooperative program between the European Southern Observatory (ESO) and the INAF Capodimonte Astronomical Observatory (OAC), Naples, for the study, design, and realization of a 2.6-m wide-field optical imaging telescope to be operated at the Paranal Observatory, Chile. The telescope design. manufacturing and integration are provided and under responsibility of the Technology Working Group (TWO) of OAC. The VST has been specifically designed to carry out stand-alone observations in the UV to I spectral range and to supply target databases for the ESO Very Large Telescope (VLT). The VST control software will operate the telescope, all the auxiliary subsystems and will manage the interfaces toward the instrumentation. The paper will describe the architecture of the software system, including the solutions adopted to be compliant with the ESO standard software environment.

The Galileo National Telescope (TNG) is a 3.6 meter Alt-Az telescope installed at the Astronomical Observatory of the Roque de Los Muchachos in La Palma, Canary Islands (Spain). The Galileo drive and control systems were designed and developed by the Technology Working Group (TWG) of the Capodimonte Astronomical Observatory, Naples (Italy). Apart from a short review of the drive system, the paper describes a novelty in the adaptive preload sub-system.