L. Gyori, T. Baranyi, G. Csepura, O. Gerlei and A. Ludmany
abstract Full postscript version of paper JAD6_2.ps
S. Stefl, L.A. Balona and C. Aerts
A. Stankov, G. Handler, D. E. Mkrtichian, E. B. Janiashvili, A. V.
Kusakin, N. I. Dorokhov, T. N. Dorokhova, M. Breger
Klaus Staubermann, PhD Dissertation
A collection of papers on the History of Photometry. Edited by C.
STERKEN and K.B. STAUBERMANN .Published by VUB UNIVERSITY PRESS,
Waversesteenweg 1077, 1160 Brussels. 2000 ISBN 90 5487 254 3
Peter Kroll, Constanze la Dous and Hans-Juergen Brauer (Eds.)
Debrecen Photoheliographic Data for 1987 with
The present catalogue is the second volume of the Debrecen Photoheliographic Data (DPD). The DPD is a catalogue of daily positions and areas of sunspots compiled by using white-light full-disk observations taken at the Heliophysical Observatory (Debrecen, Hungary) and its Gyula Observing Station as well as at some other observatories. In 1987 the contributing observatories were: Abastumani Astrophysical Observatory (Georgia), Ebro Observatory (Spain), Kiev University Observatory (Ukraine), Kislovodsk Observing Station of Pulkovo Observatory (Russia), Kodaikanal Solar Observatory (India) and Tashkent Observatory (Uzbekistan). The material is divided in two parts. The numerical part contains the measured data and the other part contains the CCD scans of all the active regions that were found on the photographic plates. Every measured spot is marked with the same number in the picture as in the numerical catalogue. The images along with the measured data allow more complex analyses, morphological studies and comparison with magnetic, Halpha and other observations.
Radio spectroscopy of long-term 22~GHz
observations of water maser outbursts in W49N
High signal-to-noise spectroscopic results are presented for the powerful water maser cluster W49N, obtained with the Metsahovi radio telescope from a 2.5 year long monitoring period. Gaussian line parameters of 108 maser outburst features as function of time are presented (108 electronic tables in ASCII format). These contain in total some 1740 Gaussian fits of the masing water line at 22 GHz. The flux density curves of 168 maser outbursts have been ordered as function of time and are displayed in 11 electronically available figures. Correlated outburst events are briefly discussed.
Simultaneous photometry and spectroscopy of the
Be star 28 (omega) CMa - III. Original data
For the bright southern Be star 28 CMa, we publish 275 He I line profiles of high spectral and temporal resolution obtained mostly in January 1996 as well as more than 600 original photometric observations in the Stroemgren and Geneva photometric system. We summarize our analysis and modeling published in two MNRAS papers.
Time-series photometry of the delta Scuti star
This paper introduces the presentation of all the time-series photometry of the delta Scuti star XX Pyx ever acquired for asteroseismological purposes. This represents approximately 900 hr of monitoring, or more than 24000 data points. In addition, the data of the primary comparison star and the observations of two new variable stars discovered during the observations are also supplied. Descriptions of the experiment, and the resuklting data, are given in JAD6,4 B-J).
[JAD 6, 4B]
Measurements from McDonald Observatory
We present the observations for the DSN campaign on XX Pyx in 1998 carried out at McDonald Observatory. The data were acquired with a two-channel photoelectric photometer on the 2.1-m and the 0.9-m telescopes. We describe the observations and several steps of data reduction which are non-standard, such as observations in the presence of bright moonlight and correction for thin clouds, which allows one to obtain accurate relative photometry even under marginal conditions. We also compare the data quality depending on the photometric conditions and telescope used. Finally, we evaluate the reliability of the amplitudes and phases determined in the initial study of the star's amplitude and frequency variability. The discussions of all these aspects are accompanied by the reduced McDonald Observatory time series.
[JAD 6, 4C]
ESO CCD observations
We present our contribution of CCD--based observations to the 1998 multisite campaign on \xx \newline (Handler et al. 2000). The data were obtained during 26 nights in early 1998, using the Dutch~91~cm telescope at ESO, La Silla, Chile. We describe the observations and the reductions, and we present the resulting photometric light~curves. We perform and compare Fourier and wavelet frequency analysis, and we compare the results with those found by Handler et al. (2000). From our dataset, which constitute a little less than 20 percent of the campaign dataset, we are able to detect 11 of the 22 independent frequencies detected by Handler et al. (2000). \newline \xx~is a difficult object due to a very high frequency content in a small frequency band. Our analysis demonstrates some of the problems of analysing even extented single--site observations of multiperiodic variable stars, and the need for multi--site campaigns on such objects. \newline We publish the table of magnitudes obtained for XX Pyx, and the 5411 bias--corrected and flatfielded CCD images.
[JAD 6, 4D]
We present the photoelectric observations of XX Pyx carried out at the South African Astronomical Observatory for the 17th DSN campaign on this star in 1998 January - March. The data were acquired as single-channel measurements on the 0.75-m and 1-m telescopes of SAAO. We discuss the reduction methods used and present the reduced SAAO time series.
[JAD 6, 4E]
Photoelectric observations from Siding Spring Observatory
The XX Pyx observations acquired from Siding Spring Observatory for the 17th DSN campaign are presented. We give an introduction to the telescope and instrument used, which are among only a few left in a professional environment for stellar photometry in the Southern Hemisphere. We then give a description of the observations and reductions as well as some assessment of the impact of our observations on the whole campaign. Finally, the reduced time series of our measurements is presented.
[JAD 6, 4F]
Photoelectric observations from the Perth and Vainu Bappu Observatories
This paper publishes the time series of the XX Pyx observations obtained at the Perth and Vainu Bappu Observatories. The two sites are briefly introduced and the observations described. We then discuss some aspects of data reduction important for the measurements from these sites and we present the reduced time series of our measurements.
[JAD 6, 4G]
SARA 0.9m CCD observations
We present the CCD--based observations obtained at the SARA Observatory as part of the 1998 multisite campaign on \xx\ (Handler et al. 2000, Paper 4). The data were obtained during 12 nights in Jan-Feb 1998, using the SARA 0.9-m telescope at Kitt Peak National Observatory, Arizona, USA. In this paper, we present the observations and data reduction procedure. We publish the table of magnitudes obtained for XX Pyx, and the 2137 bias-, dark- and flat-corrected CCD images.
[JAD 6, 4H]
SAAO CCD observations
We refer to the paper by Handler et al. published elsewhere in this volume of The Journal of Astronomical Data for a general introduction to the 1998 multisite campaign on the low-amplitude, multiperiodic delta Scuti star XX Pyx. In the present paper we outline the XX Pyx observations obtained at SAAO, Sutherland, South Africa in early February 1998.
[JAD 6, 4J]
Measurements from Wise Observatory
We present the observations for the DSN campaign on XX Pyx in 1998 carried out at Wise Observatory. The data were acquired with the CCD camera on the 1.0-m telescope of the observatory. We explain briefly why we resort to this observational technique rather than performing photoelectric photometry, which is the common mode of observations of WET and of DSN. We describe the observations and the atmospheric and the technical conditions prevailing during our observing run. Based on the experience gained at the WO in similar CCD photometry measurements, we estimate the accuracy of stellar photometry that can be achieved by applying well known reduction techniques to our image frames.
The multiperiodic delta Scuti star 4 CVn: 1997
We present the data of the evolved delta Scuti star 4 CVn obtained during the multisite campaign 1997 at the Asian observatories of Abastumani, Mt. Dushak-Erekdag and Tien-Shan. 4 CVn was observed photometrically for 35 nights and 195 hours of data could be obtained. We show the light curves of 4 CVn and compare the data with the 34-frequency solution which was derived with the previously published set of data of the 1996 Delta Scuti Network campaign (Breger et al. 1999, hereafter called Paper I). There is a good agreement between the measurements and the independently derived fit. This paper also includes other data (tables 7 to 16) from this campaign which was used in Paper I as well as data from Breger & Hiesberger (1999) using the Automatic Photoelectric Telescope (APT).
Using my training as an astronomer and drawing on resources such as museums, instrument collections, and archives, I have rebuilt Zoellner's astro-photometer designed by Zoellner in the late 1850s when he was working for his doctoral thesis at Basel University. The photometer was designed to compare an artificial star with a real star by means of a half-transparent screen which allowed simultaneously observation of the two together. The brightness and colour of the artificial star could be matched those of the real star by means of polarisation. After completing his instrument Zoellner observed with it at Berlin for almost two years. I have both replicated the instrument and carried out observations following Zoellner's own records. The replication of the instrument included all its optical components, the brass and wooden parts and the town gas used to produce the artificial star. This dissertation will follow the line of investigation of historical practice. The beginnings of nineteenth-century photometry will be presented, followed by a description of the Zoellner photometer, its replication and the observations carried out with the replica. I will contextualize my work based on my insights with the photometer, and then trace its career through the second half of the nineteenth century.
This book results from presentations and discussions of a group of astronomers and historians during a one-day workshop held at Archenhold Observatory, Berlin-Treptow, on April 4, 1997. This meeting was the first forum in a series dedicated to historical aspects of observational astrophysics in the nineteenth and early twentieth century. The basic principle of these meetings is to reflect during one or more days on the work and personality of a single individual or of a group of persons, at the same time avoiding the really dominant figures that typify the age. By focusing on key people who epitomize a way of thinking and working that has formed many of the ideas by which we do astrophysical research today, we also attempt to evoke the scientific spirit of the era under consideration. In 1858, the German physicist Karl Friedrich Zoellner introduced a new type of astronomical photometer which became a bestseller in the second half of the nineteenth century and which led him to the first German professorship in astrophysics. His type of photometer allowed most accurate photometric measurements and was used at several observatories for almost half a century. This book outlines four major themes. The first part describes the observing instruments that were used by Zoellner and his contemporaries: photometers and spectrographs that complemented his original design, but also competed with his most versatile prototype photometer. The description also includes an account of technical aspects associated with the replication of such a photometer today. The second part analyses the astrophysical data that were obtained with Zoellner's tools, and extracts information hidden in the published data --- scientific information as well as diverse aspects related to the observer himself. These nineteenth-century data are now published for the first time on a modern magnitude scale and are directly accessible in tabular form, and are thus fully applicable to archeophotometric studies. The third part of the book illustrates some aspects of Zoellner's personal life, his correspondence, and the relationship to his direct colleagues. It follows Zoellner during the last years of his life when he experienced severely strained relationships with the scientific establishment of his time. The last part reviews a number of scientific studies made on the most enigmatic personality that Zoellner certainly was, and also gives a bibliography of all works by Karl Friedrich Zoellner which were published during his lifetime or which appeared posthumously.
[JAD 6, 8] BOOK REVIEW: Treasure-Hunting in Astronomical Plate Archives. Proceedings of the international workshop held at Sonneberg Observatory, March 4-6, 1999. Peter Kroll, Constanze la Dous and Hans-Juergen Brauer (Eds.) This book consists of the proceedings of a conference on the exploration of the invaluable scientific treasure present in astronomical plate archives worldwide. The book incorporates fifty scientific papers covering almost 250 pages. There are several most useful papers, such as, for example, an introduction to the world's large plate archives that serves the purpose of a guide for the beginning user of plate archives. It includes a very useful list of twelve mayor archives with many details on their advantages (completeness, number of plates, classification system and homogeneity of time coverage) and their limitations (plate quality, access, electronic catalogues, photographic services, limiting magnitudes, search software and cost to the user). Other topics cover available contemporary digitization machines, the applications of commercial flatbed scanners, technical aspects of plate consulting, astrophysical applications and astrometric uses, data reduction, data archiving and retrieval, and strategies to find astrophysically useful information on plates. The astrophysical coverage is very broad: from solar-system bodies to variable stars, sky surveys and sky patrols covering the galactic and extragalactic domain and even gravitational lensing. The book concludes by an illuminating paper on ALADIN, the reference tool for identification of astronomical sources. This work can be considered as a kind of field guide, and is recommended reading for anyone who wishes to undertake small- or large-scale consulting of photographic plate material. A shortcoming of the proceedings is the fact that very few papers have abstracts.