bluuebunny/crossref_metadata_2025_split huggingface dataset:
Comparison of Polar Motion Data from the 1980 Project Merit Short Campaign
Authors: Mueller Ivan I. , Rajal B. S. , Zhu Y. S. 
Published: July 2016

AbstractPolar motion coordinates obtained during the Merit short campaign by various techniques, as well as their variations, have been compared directly and through a smoothing procedure. In the direct comparison, values at selected dates were differenced in all combinations and the rms values computed. Through the smoothing procedure the amplitudes of the annual and Chandler motions as well as the centers of the polhodes were estimated and compared with predicted values based on the previous six years of polar motion data. The results are somewhat inconclusive, mainly due to the shortness of the campaign and the (practically) real time data reduction techniques. To resolve the issue of possible systematic differences, the proposed MERIT main campaign seems an absolute necessity.
Planetary and Earth Figure Perturbations in the Librations of the Moon
Authors: Eckhardt Donald H. 
Published: July 2016

AbstractComparisons of numeric, semi-analytic and analytic lunar libration models indicate that the planetary and Earth figure perturbations used to supplement the semi-analytic and analytic models are inadequate. Using the ELP-2000 of Chapront and Chapront-Touzé, an improved solution of these perturbations is developed. For the libration in longitude there are numerous terms with periods near that of the free libration; their amplitudes remain ill-defined.
Storing Sky Surveys at NOAO
Authors: Van Atta Cathaleen 
Published: July 2016

At NOAO/Tucson the various sky surveys are not kept in or kept by the Library. Instead, the person who is responsible for their acquisition, care, handling and preservation, is someone whose area of expertise is scientific photography and instrumentation, and he has given me the information that follows.At NOAO we have a very complete set of the sky surveys. In Tucson we have one set of the Palomar survey on print and one on glass, the ESO/SRC southern atlas, red and blue, on glass and film, the SRC infrared atlas on film, the SRC equatorial atlas on glass, the ESO quick blue survey on glass, and original KPNO telescope plates on glass. At the observatory on Kitt Peak there are two sets of the Palomar survey on print. Basically, all of these can be divided by format into three kinds: paper print, film, and glass. I will tell briefly what we do with each.
Handling of Microfiche
Authors: Gómez M. E. 
Published: July 2016

The microficher received at the Library E.S.O. - La Silla, come from different sources: old journals out of print, articles in current journals which often include microfiche for long tables, catalogs and figures not suitable for normal printing, and larger catalogues of data (IUE, IRAS, etc.). These microfiche, coming either in journals or being a publication themselves, are ordered in the same way:
-Every microfiche is assigned a running number.-Three cards are typed: the main one being by author, the second one by title of the article, and the third one by title of the journal. In addition, the running number that identifies the microfiche is typed on the upper right corner of each card. The total amount of microfiche that make up the article or publication is given at the lower center of each card.-The cards are kept in a special catalogue cabinet labeled Microfiche., in strict alphabetical order, where the cards by author, title, and publication are mixed together.-The microfiche themselves are kept in a plastic tray with fiche separators and index dividers with insertable label holders. These label holders are placed at an interval of every five fiche separators. The holders display the running numbers of the microfiche.-In addition, every fiche separator carries on its front side an adhesive label which contains the same information as that found on the main card.
The ESO Archive Project
Authors: Ochsenbein François 
Published: July 2016

AbstractFollowing the Archiving Policy recently defined, observations made at the ESO telescopes will be archived, starting with the large instruments. The Fits format is used extensively for the description of each stored observation, and a Catalogue is built up for retrieval purposes; this Catalogue will be accessible from ESO at Garching and via the existing networks. During the archiving process, special care is taken to homogenize the names of the targets observed.
The Relighting of Kalispell, Montana
Authors: Westpfahl David 
Published: July 2016

ABSTRACTKalispell, Montana, a city of about 20,000 near the Canadian border, has completed major relighting. Aging mercury vapor lamps along U.S. routes #2 and #93 nave been replaced with low pressure sodium (LPS) fixtures. The downtown also has LPS plus turn-of-the-century style cast iron lampposts with low wattage fluorescent lamps, which provide white light on storefronts and curbside parking. The Chamber of Commerce helped with the purchase of these fixtures, which are lit from dusk to midnight and, in the winter, from 6:00 A.M. until sunrise. Most other areas of Kalispell are lit with high pressure sodium in full cut-off fixtures. City and county officials have calculated that the payback time for the LPS relighting was 40 months.
In Defense of Space Art: The Role of the Artist in Space Exploration
Authors: Malina Roger F. 
Published: July 2016

ABSTRACTArtworks will be built in space as the frequency and range of space missions increase. Artists have proposed artworks to be installed in space and have worked with space agencies to begin planning for such projects; a few space art projects have been completed. It is argued that artworks should be reviewed with the same constraints as all other space artifacts. It is unlikely that artworks will ever pose the kind of environmental threat that already exists from scientific, commercial and military activities; the cultural value of creating some space art balances the associated costs and risks. Artworks visible to global audiences can be conceived and have been proposed; it is these proposals that have concerned astronomers. Public space art should be subject to a process of public scrutiny similar to that of earth-based public art works. Most space art will involve interdisciplinary teams of artists, scientists and engineers; these projects offer the possibility of artists providing novel ideas and approaches that will be of interest in other applications. Artists in the past have played crucial roles in promoting space exploration, in literature, film and the plastic arts. They have also explored the negative aspects and risks. In the future it is inevitable and desirable that artmaking be included in planned space activities.
The role of radiation pressure in LBV atmospheres
Authors: Appenzeller I. 
Published: July 2016

AbstractAs LBVs have luminosities close to their Eddington limits, their structure is profoundly influenced by radiation pressure. Radiation pressure effects probably cause the highly extended atmospheres and the extreme mass loss observed during the maximum states of the S Dor variables. An opacity-related instability of the radiative acceleration combined with a delayed thermal readjustement of the sub-atmospheric layers possibly explains the large-amplitude radius variations of these objects.
The ionization and thermal balance in P Cygni’s wind revisited
Authors: Johnson D.R.H. , Drew J.E. 
Published: July 2016

Abstract.The statistical and thermal equilibrium of P Cygni’s wind as a function of radius is investigated using the model of Drew (1985) with an improved treatment of hydrogen. Provisional calculated hydrogen and helium line fluxes are compared with observation. The wind temperature is found to be cooler than observation implies, and a further heating source is tentatively identified.
Triple Galaxies and a Hidden Mass Problem
Authors: Karachentsev I.D. , Karachentseva V.E. , Lebedev V.S. 
Published: July 2016

AbstractWe consider a homogeneous sample of 84 triple systems of galaxies with components brighter than m = 15.7, located in the northern sky and satisfying an isolation criterion with respect to neighboring galaxies in projection. The distributions of basic dynamical parameters for triplets have median values as follows: radial velocity dispersion 133 km/s, mean harmonic radius 63 kpc, absolute magnitude of galaxies MB = —20.38, crossing time τ = 0.04 H−1. For different ways of estimation the median mass-to-luminosity ratio is (20 – 30)f⊙.A comparison of the last value with the ones for single and binary galaxies shows the presence of a virial mass excess for triplets by a factor 4. The mass-to-luminosity ratio is practically uncorrelated with linear size of triplets or with morphological types of their components.We note that a significant part of the virial excess may be explained by the presence of nonisolated triple configurations in the sample, which are produced by debris of more populous groups of galaxies.
Dynamics and Configurations of Galaxy Triplets
Authors: Anosova Joanna P. , Orlov Victor V. , Chernin Arthur D. , Ivanov Alexei V. , Kiseleva Ljudmila G. 
Published: July 2016

AbstractTwo methods are proposed for describing the distributions of the triplet configuration parameters characterizing a tendency to alignment and hierarchy: (1) obtaining a representative sample of configurations and determining its statistical parameters (moments and percentages); and (2) dividing the region of possible configurations of triple systems (Agekian and Anosova, 1967) into a set of segments and finding the probabilities for the configurations to find themselves in each of them.
Numerical Simulations of Interacting Disk Galaxies
Authors: Noguchi Masafumi 
Published: July 2016

Galaxy-galaxy interactions have long attracted many extragalactic astronomers in various aspects. A number of computer simulations performed in the 1970s have successfully reproduced the peculiar morphologies observed in interacting disk galaxies and clarified that tidal deformation explains most of the observed global peculiarities. However, most of these simulations have used test particles in modelling the disk component. Tidal response of a self-gravitating disk remains to be further clarified.Another topic which is intensely discussed at present is the relation between galaxy-galaxy interactoins and activity. Many observations suggest that interactions trigger strong starbursts and possibly active galactic nuclei (AGN). However, the detailed mechanism of triggering is not yet clear. It is vital here to understand the dynamics of interstellar gas.
The Mass–Ratio Distribution of Short–Period Binaries
Authors: Mazeh T. , Goldberg D. 
Published: July 2016

Abstract We present a new algorithm to derive the mass-ratio distribution of an observed sample of spectroscopic binaries. The algorithm replaces each binary of unknown inclination by an ensemble of virtual systems with a distribution of inclinations. We show that contrary to a widely held assumption the orientations of each virtual ensemble should not be distributed randomly in space. A few iterations are needed to find the true mass-ratio distribution. Numerical simulations clearly demonstrate the advantage of the new algorithm over the classical method. We have applied the new algorithm to the recent large sample of G-dwarf spectroscopic binaries, and got a uniform or perhaps a slightly rising linear mass-ratio distribution. This result suggests that the mass-ratio distributions of short-period and long-period binaries are substantially different. It also indicates that the mass distribution of the secondary stars is not the same as that of the single stars.
The Use of Pulsating Stars in Orbit Determination
Authors: Pigulski Andrej 
Published: July 2016

In a double or a multiple system, in which one of the components is a pulsating star, the light-time effect leads to apparent changes of the pulsation period. In some cases, one can obtain much more accurate values of the spectroscopic elements from the fit to the 0 — C diagram than from classical analysis of the radial-velocity data. In addition, in the analysis of the O — C diagram, photometric observations can be used. They are easy to obtain, and therefore are usually more numerous than the spectrographic ones.Below we present the results of a study of three stellar systems, in which the light-time effect is observed. Primaries in all these systems are β Cephei-type pulsating variables.
Biographical and Historical Notes on the Pioneers of Photometry in Ireland
Authors:   The Editors
Published: July 2016

As the circumstances of the early electrical measurements of starlight in Ireland are not widely known we wish to take this opportunity to set down the facts, as far as they are known to us. Corrections or new information will be welcomed.The observations made in Dublin in 1892 were the result of a collaboration between four graduates of Trinity College: George M. Minchin, William H.S. Monck, Stephen M. Dixon and George F. Fitzgerald. The observations in 1895 were made at Daramona Observatory, Co. Westmeath with a 24-inch reflector by Minchin, Fitzgerald and the owner of the telescope, William E. Wilson. In 1875 Minchin was appointed Professor of Applied Mechanics at the Royal Indian Engineering College at Coopers Hill, near Staines in London. In 1877 he started a long series of investigations of photoelectricity using a small optical laboratory at Coopers Hill and the laboratories of University College London. His initial aim was to transmit images electrically but he became skilled in making photovoltaic cells of selenium.By September 1891 Minchin had succeeded in making some working cells and he wished “to test them on the stars”. He contacted his friend Monck who had recently set up an observatory in his back garden in Dublin. Monck in turn asked Fitzgerald for the loan of a galvanometer or electrometer and for advice in its use. As Fitzgerald did not have a suitable instrument, he ordered Clifton’s form of Thomson’s quadrant electrometer, which arrived near the end of the year. It seems that Minchin also sent some of his cells to Dr Boeddicker in the spring of 1892 for trials on the 72-inch telescope but no reports are available.
Crowded Field Photometry using Post-Exposure Image Sharpening Techniques
Authors: Redfern R.M , Shearer A. , Wouts R. , O’Kane P. , O’Byrne C. , Read P.D. , Carter M. , Jordan B.D. , Cullum M. 
Published: July 2016

AbstractThe technique of image sharpening which allows high resolution images to be produced from ground-based telescopes is applied to the problem of photometry in crowded field regions - such as close to the cores of globular clusters. The conditions for image sharpening are discussed and the technique is demonstrated using simple objects (close double stars). Preliminary results from image sharpening of M15 are presented.
Determination of Data Quality and Results from two Mount Hopkins Robotic Telescopes
Authors: Pyper Diane M. , Adelman S.J. , Dukes R.J. , McCook G.P. , Seeds M.A. 
Published: July 2016

AbstractWe present various methods for determining night quality from observations obtained with totally unattended automatic photoelectric telescopes at the Fairborn Observatory site on Mt. Hopkins, AZ. Telescopes are the Phoenix 10-inch (P10) and the Four College 75-cm (CAPT). Filter systems used are Johnson UBV, Kron-Cousins RI and Strömgren uvby. As a preliminary data filter for the P10 “rent-a-star” data, all observations with standard errors of the mean (SEM) above 20 mmag are discarded; a summary of nightly SEM’s, number of aborts and total observing time is sent to each user. The CAPT data are evaluated by standard deviation of magnitudes or counts for photometric groups and for an entire night. The Geneva photometric statistics are computed for these latter data and have proved useful as a preliminary screen for bad data. Various criteria for good and bad groups and nights are discussed. Scientific results are presented for several magnetic CP stars that were observed using both telescopes. Differences in precision of the data and strategies for observing are discussed.
GNAT — A Global Network of Automatic Telescopes
Authors: Crawford D.L. 
Published: July 2016

AbstractAll of us “have-nots” need more telescope time, for ourselves and for our students. There are also many programs where a global linkage is needed to accomplish the objectives. In addition, the world needs more and better science education; astronomy can be a leader if it has adequate facilities to do so. A global network of automatic telescopes can help supply these needs, which are global, spanning all countries. A new non-profit organization (GNAT, Inc.) has been formed to be the catalyst to develop and implement such a concept. We hope that many astronomers and organizations will become “members” of GNAT.
The Simulation and Results of a New Speckle Image Processing Technique
Authors: Cady F. M. , Bates R. H. T. 
Published: July 2016

AbstractA new technique called shift-and-add, which allows nearly diffraction-limited images to be formed of objects viewed through a randomly distorted, turbulent media, has been formulated. True images may be obtained through the earth’s atmosphere when the method is used. It has been shown that this can be achieved even though the telescope may have severe aberration and when using a much wider bandwidth than that used at present in stellar Speckle Interferometry. Results are given for an object of greater extent than simple binary or groups of point sources.
Variable stars in M31 from the MEGA survey
Authors: Alves David R. , Baltz Edward A. , Crotts Arlin , Bergier Alex , Cseresnjes Patrick , Gersch Alan 
Published: July 2016

AbstractThe MEGA microlensing survey is introduced and several topics about variable stars in M31 are discussed. An adopted model population of semiregular (SR) variable stars is presented, and the efficiency to recover these stars in M31 in a specific example MEGA dataset is predicted. The period-flux amplitude relation of the SRs discovered by MEGA could be used to measure the inclination of the M31 disk.
Variable stars from two surveys of microlensing in M31
Authors: Crotts Arlin P.S. , Boyle Richard P. , Corbally Christopher J. ,   the MEGA Collaboration
Published: July 2016

AbstractRecently we completed the VATT/Columbia survey monitoring a portion of M31 for microlensing and stellar variability, and report here on the microlensing result. Also, we have nearly completed a much larger survey (MEGA) covering most of the stars in M31, for which we have started cataloging many tens of thousands of Cepheids, Miras, eclipsing variables and other kinds of variable stars. The microlensing results from these two surveys hint that a significant fraction of the dark matter in M31 is composed of stellar-mass objects in the halo.
Multiperiodic RR Lyrae stars in the Galactic Bulge and the SMC
Authors: Mizerski Tomasz 
Published: July 2016

AbstractI have performed a detailed analysis of multiperiodic RR Lyr stars of the Galactic Bulge and the Small Magellanic Cloud. In the rich OGLE-II database on the Galactic Bulge objects I detected more than 2500 RR Lyr stars, with almost 600 of them exhibiting multiperiodic behavior of various, sometimes unique, kinds. Many of them can only be explained by excitation of nonradial modes. There are two major, striking differences between the two discussed stellar systems: the incidence rate of RRd double mode pulsators is over 30 times higher in the SMC than in the Galactic Bulge, and there are more than twice as many Blazhko stars in the Galactic Bulge as in the SMC.
The distance to the Large Magellanic Cloud from first overtone RR Lyrae variables
Authors: Muzzin A.V. , Clement C.M. , Alves D.R. ,   The MACHO Collaboration
Published: July 2016

AbstractFourier coefficients have been derived for the V and R light curves of 330 bona fide RR Lyrae first-overtone (RR1) pulsators in 16 MACHO fields near the bar of the LMC. We use the Fourier phase parameter ɸ31 and log P values to select a subsample of these stars which are similar to the RR1s in the Galactic globular cluster M5. Assuming that the M5-like stars in the LMC have absolute magnitudes comparable to the HB stars in M5, we use independent studies to derive their mean absolute V magnitude and compute a visual distance modulus of μLMC = 18.43 ± 0.06 (statistical) ±0.16 (systematic). By selecting stars on the basis of their light curve parameters, we are able to derive a distance modulus that does not depend on the somewhat poorly determined Mv – [Fe/H] relation for RR Lyr stars.
β Cephei and SPB stars in the Large Magellanic Cloud
Authors: Kołaczkowski Z. , Pigulski A. , Soszyński I. , Udalski A. , Szymański M. , Kubiak M. , Żebruń K. , Pietrzyński G. , Woźniak P.R. , Szewczyk O. , Wyrzykowski L. ,   the OGLE team
Published: July 2016

AbstractThis is a progress report of the study of pulsating main-sequence stars in the LMC. Using the OGLE-II photometry supplemented by the MACHO photometry, we find 64 β Cephei stars in the LMC. Their periods are generally much longer than observed in stars of this type in the Galaxy (the median value is 0.27 d compared with 0.17 d in the Galaxy). In 20 stars with short periods attributable to the β Cephei-type instability, we also find modes with periods longer than ~0.4d. They are likely low-order g modes, which means that in these stars both kinds of variability, β Cephei and SPB, are observed. We also show examples of the multiperiodic SPB stars in the LMC, the first beyond our Galaxy.
Multisite spectroscopic and photometric observations of the pulsating sdB star PG 1605+072
Authors: O’Toole S.J. , Falter S. , Heber U. , Jeffery C.S. , Dreizier S. , Schuh S.L. ,   the MSST,   WET teams
Published: July 2016

AbstractWe present the first results from the MultiSite Spectroscopic Telescope (MSST) observations of the sdBV star PG 1605+072. Pulsating sdB stars (V361 Hya stars) offer the chance to gain new insights into the formation and evolution of extreme Horizontal Branch stars using the tools of asteroseismology. PG 1605+072 is an outstanding object in its class, with the richest frequency spectrum, the longest periods, and the largest variations. The MSST campaign took place in 2002 May/June and we present here the massive data set, made up of 399 hr of photometry and 151 hr of spectroscopy. The overall aims of the project are to examine light/velocity amplitude ratios and phase differences, changes in equivalent width/line index, and λ-dependence of photometric amplitudes, and to use these properties for mode identification.
Direct detection of multiple periods in variable stars
Authors: Schoenaers C. , Cuypers J. 
Published: July 2016

AbstractIn some observational data sets of variable stars, multiperiodicity was not always recognized as such, and only became apparent when other observational material became available. In other cases, consecutive prewhitening starting with the obviously most significant frequency could lead to a wrong multifrequency solution. A few examples illustrating this are given. Searching directly for a multifrequency solution can often remedy this. Examples are given and the results of applying this technique to a large set of Hipparcos photometric data are communicated. An overview of the multiple periodicities found in β Cephei stars and SPB stars is reported in detail.
Interferometry of pulsating red giants from 0.65 to 3.5 microns
Authors: Ireland Michael , Tuthill Peter , Robertson Gordon , Bedding Timothy , Jacob Andrew , Monnier John , Danchi William 
Published: July 2016

AbstractWe present the results of two multi-wavelength studies of the angular diameters of the Mira-like stars ο Cet, W Hya and R Leo. The MAPPIT experiment was able to deliver diameters of these stars over a continuous wavelength region from 0.65 – 1 micron, while the Keck aperture-masking experiment was able to deliver diameters between 1.2 and 3.5 microns. Strong size variations with wavelength were recorded for all stars, and we discuss the implications for model atmospheres of these stars, and speculate on the necessity of including dust scattering in radiative transfer calculations.