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Illinois—Where Astronomical Photometry Grew Up
Beaman and Svec, JAAVSO Volume 40, 2012 141 Illinois—Where Astronomical Photometry Grew Up Barry B. Beaman 6804 Alvina Road, Rockford, IL 61101; [email protected] Michael T. Svec Furman University, Department of Education, 3300 Poinsett Highway, Greenville SC 29613; Internet: [email protected] Presented at the 100th Annual Meeting of the AAVSO, October 7, 2011; received January 21, 2012; revised February 2, 2012; accepted February 6, 2012 Abstract In 1903 Dr. Joel Stebbins joined the University of Illinois faculty as an astronomy instructor and Director of the University of Illinois Observatory. In 1905 he and F. C. Brown began experimenting with selenium sell photometry and developed the equipment and many of the photometric practices used then. Those practices formed the foundation on which present day photometry processes are based. This paper will trace the history of Stebbins’ career and his development of photoelectric photometry from 1903 to 1922. This story explains how Stebbins’ wife, May, caused a change in astronomical observing that continues today. 1. Introduction The prairies of central Illinois may seem an unlikely place to begin a photometric revolution. Illinois is a flat land state with only about 100 clear nights per year, the average elevation is only 600 feet above sea level, and the highest point is only at 1,500 feet. Yet, Illinois has produced its share of prominent and innovative astronomers. George Ellery Hale built his Kenwood Observatory in the heart of Chicago. Edwin Hubble spent his teen years in the Chicago suburbs and was educated at University of Chicago. Grote Reber built the World’s first parabolic-steerable radio telescope. -
Refining the UW–Madison Campus Dan Okoli, NCARB, AIA University Architect
Beneficent Beauty: Refining the UW–Madison Campus Dan Okoli, NCARB, AIA University Architect WISCAPE – Presentation 10.27.08 Campus Design Guide University of Wisconsin-Madison An Approach to a Functional and Pleasing Composition QUESTION 3 What should our campus look and feel like in the near and long term? GOOD EXAMPLES OF WHAT NOT TO DO 4 McFadden Hall, 1919 GOOD EXAMPLES OF WHAT NOT TO DO 5 McFadden Hall, 1919 After 1960’s Renovation Schear Hall,1960’s Addition GOOD EXAMPLES OF WHAT NOT TO DO 6 McFadden Hall, 1919 After 1960’s Renovation 2008 Renovation GREAT CAMPUS PLACES 7 Memorial Union Terrace Memorial Union Terrace Memorial Union Memorial Union Interior Bascom Hill Memorial Union Interior Bascom Hall Bascom Hill Bascom Hall GREAT CAMPUS PLACES 8 Bascom Hill Bascom Hall Memorial Union Terrace Agricultural Hall Library Mall Allen Centennial Gardens Lakeshore Path BascomScience Hill Hall and Bascom Hill School of Education NOT SO GREAT CAMPUS PLACES 9 NOT SO GREAT CAMPUS PLACES 1 0 Old Ogg Hall Van Vleck Plaza Engineering Research Building Van Hise Hall Humanities Building Peterson Building Social Sciences Building Union South Biotron Laboratory EDUCATION BUILDING EXAMPLE 1 1 Selected Design Option Open Space North of Education Building North Elevation of Education Building Interior Atrium BIOCHEMISTRY I EXAMPLE 1 2 BIOCHEMISTRY II EXAMPLE 1 3 BIOCHEMISTRY I 1 4 BIOCHEMISTRY COMPLEX 1 5 WISCONSIN INSTITUTES FOR DISCOVERY 1 6 WISCONSIN INSTITUTES FOR DISCOVERY 1 7 WISCONSIN INSTITUTES FOR DISCOVERY 1 8 WISCONSIN INSTITUTES FOR DISCOVERY -
Investigations of the Interstellar Medium at Washburn Observatory, 1930-58
Journal of Astronomical History andheritage 7(2):85-94 2004 Investigations of the interstellar medium at Washburn Observatory, 1930-58 David S Liebl* University of Wisconsin- College of Engineering, 432 North Lake Street, Rm. 311, Madison, Wisconsin 53706, USA E-mail: [email protected] Christopher Fluke Centre for Astrophysics and Supercomputing, Swinbume University ofTeclmo/ogy, PO Box 218, Victoria 3122, Australia E-mail: [email protected] Abstract Behveen 1930 and 1958, the Washburn Observatory of the University of Wisconsin-Madison was home to pioneering photometric research into the interstellar medium by Joel Stebbins and Albert Whitford. Between 1933 and 1941, Stebbins and Whitford published seminal research on the photometry of stellar reddening, using the Washburn 15-inch refractor and the 60- and 100-inch reflectors at Mount Wilson Observatory. Many factors were responsible for the Washburn Observatory's pre-eminence in this area. l11is paper reviews their research on interstellar dust during the years 1922 58, the observational teclmology and scientific methods that were developed at the Washburn Observatory during that time and the scientific discoveries that originated there. We discuss the factors that enabled WashburnObservatory to become a leader in photometry during the first half of the twentieth century. We also draw on the recollections of past and present Washburn Observatory scientists1 to understand how Washburn's standing led to a subsequent programme of research into the interstellar medium at the University of Wisconsin-Madison. The resulting portrayal of Washburn Observatory provides insights into the evolution of astronomical research in America, from the beginning of the hventieth cenh1ry until today. -
Long-Range Transportation Plan
DRAFT JUNE 2007 2005 LONG RANGE TRANSPORTATION PLAN AND TRANSPORTATION DEMAND MANAGEMENT PLAN UNIVERSITY OF WISCONSIN-MADISON I. THE PLANNING PROCESS AND PURPOSE OF THE PLAN This Long Range Transportation Plan (LRTP) has been developed in coordination with and as an element of the 2005 Campus Master Plan of the University of Wisconsin- Madison. It both responds to and helps shape the overall development plan for the campus over the next 20 years and beyond. Unlike most municipal or regional plans, this transportation plan does not call for any new roadway capacity or additional parking. It does include plans for intersection improvements—mostly to help pedestrian movement—and road realignments to boost connectivity. Parking will remain capped at its current level of approximately 13,000 spaces and virtually all of the specific improvements and program changes called for in this plan are strategies designed to make travel without a private motor vehicle safer and more convenient. For that reason, this long range plan is also the University’s Transportation Demand Management (TDM) Plan. The University has long demonstrated its commitment to TDM and has created TDM plans for specific building projects, notably the Kohl Center and Camp Randall. In 2006 the United States Environmental Protection Agency recognized the University of Wisconsin-Madison with an award for being a Best Employer for Commuters. However, it has never had a formal and comprehensive transportation demand management plan for the University as a whole. This plan will act as a guide to the University’s own goals for improving an already stellar TDM program, and respond to a new City of Madison ordinance requiring TDM plans in association with major developments. -
Introduction to Astronomical Photometry, Second Edition
This page intentionally left blank Introduction to Astronomical Photometry, Second Edition Completely updated, this Second Edition gives a broad review of astronomical photometry to provide an understanding of astrophysics from a data-based perspective. It explains the underlying principles of the instruments used, and the applications and inferences derived from measurements. Each chapter has been fully revised to account for the latest developments, including the use of CCDs. Highly illustrated, this book provides an overview and historical background of the subject before reviewing the main themes within astronomical photometry. The central chapters focus on the practical design of the instruments and methodology used. The book concludes by discussing specialized topics in stellar astronomy, concentrating on the information that can be derived from the analysis of the light curves of variable stars and close binary systems. This new edition includes numerous bibliographic notes and a glossary of terms. It is ideal for graduate students, academic researchers and advanced amateurs interested in practical and observational astronomy. Edwin Budding is a research fellow at the Carter Observatory, New Zealand, and a visiting professor at the Çanakkale University, Turkey. Osman Demircan is Director of the Ulupınar Observatory of Çanakkale University, Turkey. Cambridge Observing Handbooks for Research Astronomers Today’s professional astronomers must be able to adapt to use telescopes and interpret data at all wavelengths. This series is designed to provide them with a collection of concise, self-contained handbooks, which covers the basic principles peculiar to observing in a particular spectral region, or to using a special technique or type of instrument. The books can be used as an introduction to the subject and as a handy reference for use at the telescope, or in the office. -
Lick Observatory Records: Correspondence UA.036.Ser.01
http://oac.cdlib.org/findaid/ark:/13030/c8dj5m3f No online items Guide to the Lick Observatory Records: Correspondence UA.036.Ser.01 Alix Norton University of California, Santa Cruz 2015 1156 High Street Santa Cruz 95064 [email protected] URL: http://guides.library.ucsc.edu/speccoll Guide to the Lick Observatory UA.036.Ser.01 1 Records: Correspondence UA.036.Ser.01 Language of Material: English Contributing Institution: University of California, Santa Cruz Title: Lick Observatory Records: Correspondence Creator: Lick Observatory Identifier/Call Number: UA.036.Ser.01 Physical Description: 148.5 Linear Feet257 boxes and 54 microfilm reels Date (inclusive): 1833-2009 Date (bulk): 1870-1960 Access Collection is open for research. The physical copybooks are restricted due to the fragile nature of the material. All use is directed to the microfilm of these volumes. The microfilm reels can be accessed by requesting them from Special Collections via the Library Catalog. Historical note The Lick Observatory was completed in 1888 and continues to be an active astronomy research facility at the summit of Mount Hamilton, near San Jose, California. It is named after James Lick (1796-1876), who left $700,000 in 1875 to purchase land and build a facility that would be home to "a powerful telescope, superior to and more powerful than any telescope yet made". The completion of the Great Lick Refractor in 1888 made the observatory home to the largest refracting telescope in the world for 9 years, until the completion of the 40-inch refractor at Yerkes Observatory in 1897. Since its founding in 1887, the Lick Observatory facility has provided on-site housing on Mount Hamilton for researchers, their families, and staff, making it the world's oldest residential observatory. -
The Origin of Nonradiative Heating/Momentum in Hot Stars
NASA Conference Publication 2358 NASA-CP-2358 19850009446 The Origin of Nonradiative Heating/Momentum in Hot Stars Proceedings of a workshop held at NASA Goddard Space Flight Center Greenbelt, Maryland June 5-7, 1984 NI_SA NASA Conference Publication 2358 The Origin of Nonradiative Heating/Momentum in Hot Stars Edited by A. B. Underhill and A. G. Michalitsianos Goddard Space Flight Center Greenbelt, Maryland Proceedings of a workshop sponsored by the National Aeronautics and Space Administration, Washington, D.C., and the American Astronomical Society, Washington, D.C., and held at NASA Goddard Space Flight Center Greenbelt, Maryland June 5-7, 1984 N/LS/X NationalAeronautics and SpaceAdministration ScientificandTechnical InformationBranch J 1985 TABLE OF CONTENTS ORGANIZING COMMITTEE v LIST OF PARTICIPANTS vi OPENING REMARKS A.B. Underhill I SESSION I. - EVIDENCE FOR NONRADIATIVE ACTIVITY IN STARS EVIDENCE FOR NONRADIATIVE ACTIVITY IN HOT STARS J.P. Cassinelli (Invited review) 2 EVIDENCE FOR NON-RADIATIVE ACTIVITY IN STARS WITH Tef f < i0,000 K Jeffrey L. Linsky (Invited review) 24 OBSERVATIONS OF NONTHERMAL RADIO EMISSION FROM EARLY TYPE STARS D.C. Abbott, J.H. Bieging and E. Churehwell 47 NONRADIAL PULSATION AND MASS LOSS IN EARLY B STARS G. Donald Penrod and Myron A. Smith 53 NARROW ABSORPTION COMPONENTS IN Be STAR WINDS C.A. Grady 57 LIGHT VARIATIONS OF THE B-TYPE STAR HD 160202 Gustav A. Bakos 62 ULTRAVIOLET SPECTRAL MORPHOLOGY OF 0-TYPE STELLAR WINDS Nolan R. Walborn 66 NONTHERMAL RADIO EMISSION AND THE HR DIAGRAM D.M. Gibson 70 X-RAY ACTIVITY IN PRE-MAIN SEQUENCE STARS Eric D. Feigelson 75 ACTIVE PHENOMENA IN THE PRE-MAIN SEQUENCE STAR AB AUR F. -
University of Wisconsin-Madison - WI - Final Report - 4/26/2019
University of Wisconsin-Madison - WI - Final Report - 4/26/2019 University of Wisconsin-Madison - WI HLC ID 1713 OPEN PATHWAY: Reaffirmation Review Visit Date: 3/25/2019 Ms. Rebecca Blank President Jeffrey Rosen Cheryl Murphy Katie Clauson HLC Liaison Review Team Chair Federal Compliance Reviewer Sheila Craft-Morgan Lisa Hinchliffe Nancy Middlebrook Team Member Team Member Team Member Mary Pomatto William Ray Eric Schwarze Team Member Team Member Team Member Randy Smith Team Member Page 1 University of Wisconsin-Madison - WI - Final Report - 4/26/2019 Context and Nature of Review Visit Date 3/25/2019 Mid-Cycle Reviews include: The Year 4 Review in the Open and Standard Pathways The Biennial Review for Applying institutions Reaffirmation Reviews include: The Year 10 Review in the Open and Standard Pathways The Review for Initial Candidacy for Applying institutions The Review for Initial Accreditation for Applying institutions The Year 4 Review for Standard Pathway institutions that are in their first accreditation cycle after attaining initial accreditation Scope of Review Reaffirmation Review Federal Compliance On-site Visit Multi-Campus Visit (if applicable) Federal Compliance 2018 Institutional Context Purpose of the Visit An eight-member team conducted a comprehensive evaluation of the University of Wisconsin-Madison (UW- Madison) for continued institutional accreditation. The visit did not include review of any Change Requests. Organizational Context The University of Wisconsin-Madison is a land-grant institution that serves as the flagship campus of the University of Wisconsin System. The institution is strongly influenced by the principal of the Wisconsin Idea which states that education should influence people's lives beyond the boundaries of the classroom. -
NATIONAL ACADEMY of SCIENCES Volume 20 February 15, 1934 Number 2
PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES Volume 20 February 15, 1934 Number 2 THE DIAMETER OF THE ANDROMEDA NEBULA By JOEL STEBBINS AND ALBERT E. WHITFORD* MOUNT WILSON OBSERVATORY, CARNEGIE INSTITUTION OF WASHINGTON Communicated January 12, 1934 During recent summers, beginning in 1930, the brightness and colors of several scores of extra-galactic nebulae have been measured with a photoelectric photometer attached to the large reflectors at Mount Wilson. One of the conclusions resulting from this study is that the diameters of a number of these objects are greater than those seen at first sight on photographs. This extension of size is not surprising, as usually each nebula fades from a relatively bright center gradually outward until the outline is lost in the foreground of the sky. Any increase in the known size of extra-galactic nebulae is of course important in a comparison with the dimensions of our own galaxy. When the photoelectric amplifier using the FP-54 tube was perfected at Madison, our attention was directed to the possibility of detecting light in the outer regions of the Andromeda nebula, M 31, which should be a favorable object for such a test. Trial measures were made in the spring of 1933 with the amplifier on the 15-inch refractor, but it was soon decided to wait until the summer, when the outfit was to be used with the 100-inch reflector at Mount Wilson. The details of the installation on the 100-inch will be published elsewhere. For measures of the An- dromeda nebula a focal diaphragm of 8 mm. -
President's Column Continued Copyright Updates for AAS Journals Conduct with Regards to Other People Is Also Simple, but Not Chris Biemesderfer Easy
May/June 2009 Issue 146 A Publication for the members of the American Astronomical Society 3 President’s Column AAS Council John Huchra, [email protected] Recognizes As we prepare for Pasadena, I would like to touch on a topic of interest to many members of our Henrietta Leavitt Society. In my last column, I noted that at our January Council meeting we had agreed to work on an AAS ethics statement. No other comment of mine has sparked as much e-mail! Every note addressed the need for more guidelines for our Society and there are even Decadal Survey white papers on 5 the subject. Although somewhat unexpected, on further thought this is not surprising—ethics in its various forms touches every member of our Society. Our statement is still under construction, but let AAS Member me enumerate some of the ethical issues we face. I will also note that a large part of our problem lies in training. How many of you have had any training in the conduct of research or general professional Anniversaries conduct with respect to peers, students and employees? And if you did, do you remember it? There are five basic areas we need to worry about: research conduct, authorship (publications) and peer review, conflicts of interest, professional conduct with respect to people, and societal responsibility. I list these 6 in approximate order of difficulty. Using the The conduct of research is perhaps the easiest. When I was a whippersnapper (read undergraduate) Job Center at we were required as part of our undergraduate physics lab to read E. -
Observatory Hill
Observatory Hill Cultural Landscape Inventory December 2005 (Revisions January 2010) Quinn Evans|Architects University of Wisconsin-Madison Department of Landscape Architecture, College of Agricultural and Life Sciences Division of Facilities Planning and Management ©2010, Board of Regents of the University of Wisconsin System University of Wisconsin-Madison Cultural Landscape Inventory Observatory Hill DEFINITIONS What is a “cultural landscape”? The following document is based on concepts and techniques developed by the National Park Service. The NPS has produced a series of manuals for identifying, describing, and maintaining culturally significant landscapes within the national park system.1 The National Park Service defines a cultural landscape as a geographic area, including both cultural and natural resources and the wildlife or domestic animals therein[,] associated with a historic event, activity, or person, or [one] that exhibits other cultural or aesthetic values.2 In 1925, geographer Carl Sauer (1889-1975) summarized the process that creates cultural landscapes: “Culture is the agent, the natural area is the medium, the cultural landscape the result.” 3 Similarly, the writer J. B. Jackson (1909-1996) looked upon the landscape as a composition of spaces made or modified by humans “to serve as infrastructure or background for our collective existence.”4 What is a “cultural landscape inventory”? 5 This cultural landscape inventory for Observatory Hill is one of eight such studies completed as part of the UW-Madison Cultural Landscape Resource Plan. Each inventory defines the boundaries of a distinct cultural landscape on campus, summarizes its history, describes its current condition, and makes recommendations about its treatment. In addition to these eight cultural landscape inventories, two companion documents address the archaeology and overall history of the campus. -
SOME PROBLEMS in STELLAR PHOTOMETRY by Joel Stebbins ASTRONOMICAL OBSERVATORY, UNIVERSITY of ILLINOIS Readbefore Tbe Aadmy, April20, 1915
PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES Volume 1 MAY 15, 1915 Number 5 SOME PROBLEMS IN STELLAR PHOTOMETRY By Joel Stebbins ASTRONOMICAL OBSERVATORY, UNIVERSITY OF ILLINOIS Readbefore tbe Aadmy, April20, 1915. Recired, Arl 1, 1915 It is the purpose of this note to point out some of the researches which have been made possible by the development of the selenium and photo-electric photometers. The first advantage of these electrical de- vices is a considerable increase in accuracy over what is possible by vis- ual and photographic methods. Perhaps the best field for immediate investigation lies in the study of the eclipsing variables, which give us the only direct clue to the actual diameters of stars. Nearly one hun- dred of these systems are now known, and new ones are continually being found. In the various studies which have been made, there is one line of reasoning which seems to have been overlooked, as follows. Among the systems discovered, some are constant in light for a large fraction of the period, while others have relatively long times of varia- tion, and are thus easier of discovery and observation. If P be the total period, and D the time of duration of the eclipse, the probability that a star will be faint when observed at any time is D/P. It seems plausi- ble to assume that if we take the number of discovered stars of each class and multiply by P/D we shall get numbers representing the rela- tive occurrence of such objects which are actually visible and might be discovered.