bluuebunny/crossref_metadata_2025_split huggingface dataset:
An Observatory Publications Reclassification Project
Authors: Cummins Marlene 
Published: July 2016

In our library we define observatory publications as all materials disseminated in serial form and on its own behalf, by an observatory, astronomical institute or university department. Included are annual reports, research reports, reprints, newsletters, and monograph series. Preprints, though fitting the description, are handled separately. Excluded and catalogued separately are individual monographs and users manuals. Sometimes items such as catalogues and atlases are catalogued and shelved elsewhere with a dummy left in the appropriate place.Traditionally, libraries have shelved observatory publications alphabetically according to the city or town in which the observatory is located. Reference tools such as Astronomy and Astrophysics Abstracts and the Bibliography of Non-commercial Publications have used that arrangement too. One of the problems of this system is that without a number, it does not provide a single, unique, identifier for observatories with many locations. The same holds true in cases where there are many observatories in one location. In addition, the location may not be known or the library’s arrangement may have idiosyncracies.
Session 3 Overview: Management of Astronomical Pecularities
Authors: Hutchins Carol 
Published: July 2016

Session 3 on “Handling and Use of Special Format Materials” dealt with diverse items which are of unique importance in astronomical libraries.Preprints and reprints are important in several ways. Libraries’ collection and dissemination of information about pre-publication journal and conference papers boosts the astronomer’s awareness of current research in a timely fashion. Individual libraries’ practices range from very basic—the receipt and physical display of preprints—to the more elaborate activities including production of lists, gathering of subsequent publication information about the papers themselves, construction of local databases listing preprints, and electronic network exchange of listings.There was a consensus that the sending of reprint series is far less important than it was in years past.We heard a call for formal recognition or designation of a central clearinghouse for information about astronomy preprints.
The AAVSO and its Variable Star Data Bank
Authors: Mattei Janet Akyuz 
Published: July 2016

AbstractThe American Association of Variable Star Observers (AAVSO) is the largest organization of variable star observers in the world that coordinates observations, and evaluates, compiles, processes, publishes, and disseminates them to the astronomical community. The organizational structure of the AAVSO, i t s visual and photoelectric observing programs, data management, publications, and services to the astronomical community are discussed.
Organized Observations of Night-Sky Brightness in Japan
Authors: Kosai Hiroki , Isobe Syuzo 
Published: July 2016

ABSTRACTObservations of the night-sky brightness were organized at 106 places in Japan by a promotion of the Environmental Agency with the help of many local governments. Two kinds of measurements were carried out: 1) Number of stars were counted in a region of triangle formed by Alpha Lyr, Epsilon Lyr, and Zeta Lyr by at least 10 contributors at each point. 2) Photographs of a star field at the zenith at each point were taken with the same type of camera and film. These results gave us a good idea on distribution of night-sky brightness in Japan.
Protection of Passive Bands in Australia, India, and Japan
Authors: Robinson B.J. 
Published: July 2016

ABSTRACTThe problems of protecting passive bands in Australia, India, and Japan reflect the variety of research activities and radio telescopes in those countries, colored by the degree of user friendliness of the frequency management authorities.In India, it is important to protect frequencies below 1400 MHz (for high redshift hydrogen line absorption or emission) and continuum bands at 327 MHz and 150 MHz (the latter currently allocated to cordless phones, paging systems, and rural communication).In Japan, protection from harmful interference has been sought and refused at 4.8 and 5 GHz (microwave network), 10 and 15 GHz (mobile relay service), and 22 GHz (mobile data relay service). But extensive radio astronomy usage of mm to sub-mm bands has established priority for their use and allocation.In Australia, there are major problems at 408 MHz (telephone links), 1.6 GHz (GLONASS, RDSS, and Land Mobile Service), 4.9 to 5 GHz (RDSS), and 22 GHz (satellite broadcasting and high definition TV service).The degree of user friendliness of the frequency management administration appears to rate: 1. Australia, 2. India, 3. Japan on a diminishing scale of cooperation and concern. This affects the awareness of the radio astronomy community of conflicting allocations and the level of input into CCIR and the WARC.
RFI Survey for the Giant Metrewave Radio Telescope in India
Authors: Swarup G. , Venkatasubramani T.L. 
Published: July 2016

ABSTRACTA Giant Meterwave Radio Telescope (GMRT) is being set up at Khodad about 80 km north of Pune in India for operation in the frequency range of about 30 to 1500 MHz. It is to be completed by 1992 and is being designed to investigate many outstanding problems in the fields of galactic and extragalactic astronomy. We present here measurements of man-made radio frequency interference (RFI) conducted at the GMRT site in 1985 and 1988. It is seen that highly sensitive radio astronomy observations can still be made at selected bands in the above frequency range because of the relatively low level of RFI in India. However, this advantage may not remain for more than a decade or two.
Plinian eruptions à la Eta Carinae
Authors: Davidson Kris 
Published: July 2016

Eta Carinae is at once ourmost notableLBV but also adoubtfulLBV, because its Great Eruption observed 150 years ago was so unique. Since that event exceeded other major LBV outbursts by orders of magnitude in ejected mass and energy, we are not certain that it really was an example of S Dor, P Cyg, R127-type behavior. But even if it turns out to be a freak,ηCar has provided either the original example or one of the earliest hints for several facets of the LBV phenomenon,e.g.:--Visual-wavelength brightening with little change in luminosity during each major mass-loss event;--The idea of a modified Eddington limit causing instability in a critical range of surface temperature;--CNO-processed surface material;--Bipolar structure in the ejecta.
The B[e] stars
Authors: Zickgraf F.-J. 
Published: July 2016

AbstractB[e] supergiants show evidence for a non-spherical two-component stellar wind. The general appearance and the physical properties of the suggested disk-like configuration are discussed. The high mass-loss rates, the surprisingly large number and the location in the H-R diagram make these stars important for the understanding of the post-main-sequence evolution of massive stars.
High resolution coronographic imaging of AG Carinae
Authors: Nota Antonella , Paresce Francesco 
Published: July 2016

AbstractWe present the first high resolution observations of the ring nebula around the galactic LBV AG Car obtained through broad band B, V, R, I filters with the STScI coronograph on the ESO 2.2 m. telescope. Highly anisotropic continuum emission in all these bands is clearly detected, in the shape of a bipolar structure elongated along the NE-SW direction extending from a few arcsecs from the star out to ⋍ 15 arcsecs corresponding to a projected linear distance of ⋍ 0.5 parsecs, with a surface brightness in the range 17.9-19.4 mag/arcsec2. Its essentially neutral color with respect to the star Δ(V-I) = −0.07) suggests that the observed radiation is starlight scattered by dust grains of diameter &gt; 1μ.
Infrared observations of circumstellar ejecta around Luminous Blue Variables
Authors: McGregor Peter J. 
Published: July 2016

AbstractRecent infrared spectroscopy and imaging of LBVs lead to the following results. CO overtone emission at 2.3μm has been found in 13 LBVs in the Galaxy and the LMC. This emission is collisionally excited in warm (3000 – 5000 K), dense (NH&gt; 1010cm-3) circumstellar material. Circumstellar disks offer favorable conditions for the formation and excitation of CO molecules and are very likely the location of the observed emission. It is proposed that the LBVs showing 2.3 μm CO overtone emission possess the highest density circumstellar disks.A group of eight LBVs has been identified in the LMC with He I 2.058 μm emission stronger than H I Brγ. This group includes the CO emission star HD 37836. Helium is over-abundant in these stars withN(He)/N(H) ranging from 0.2 to &gt;0.5. Remarkably five of the helium strong stars belong to the small class of Ofpe/WN9 stars and a further two are probably related to this class.Slit scans of the galactic LBV AG Car have resolved the far-infrared emission from this star, clearly showing it to originate from cool dust in the circumstellar ring structure. Thermal equilibrium considerations require large grains in the ring in order to match the measured grain temperature and radial distance. Similar slit scans of the galactic B[e] star HD 87643 fail to resolve the far-infrared emission from this star at the 10″ level.
Close binary models for Luminous Blue Variable stars
Authors: Gallagher J. S. 
Published: July 2016

AbstractThe evolution of massive close binary stars inevitably involves mass exchange between the two stellar components as well as mass loss from the system. A combination of these two processes could produce the stellar wind-modulated behavior seen in LB Vs. The possibility that LBVs are powered by accretion is examined, and does not appear to be a satisfactory general model. Instead, identification of LBVs with close binaries in high mass-loss rate or common envelope evolutionary phases shows promise.
Morphological Type Correlation between Nearest Neighbor Pairs of Galaxies
Authors: Yamagata Tomohiko 
Published: July 2016

Although the morphological type of galaxies is one of the most fundamental properties of galaxies, its origin and evolutionary processes, if any, axe not yet fully understood. It has been established that the galaxy morphology strongly depends on the environment in which the galaxy resides (e.g. Dressler 1980).Galaxy pairs correspond to the smallest scales of galaxy clustering and may provide important clues to how the environment influences the formation and evolution of galaxies. Several investigators pointed out that there is a tendency for pair galaxies to have similar morphological types (Karachentsev and Karachentseva 1974, Page 1975, Noerdlinger 1979).We analyzed morphological type correlation for 18,364 nearest neighbor pairs of galaxies identified in the magnetic tape version of the Center for Astrophysics Redshift Catalogue (Huchra 1987, hereafter CfA Catalog).
What is the Number of Spiral Galaxies in Compact Groups?
Authors: Tikhonov N. A. 
Published: July 2016

AbstractThe distribution of morphological types of galaxies in compact groups is studied on plates from the 6 m telescope. In compact groups there are 57% galaxies of late morphological types (S + Irr), 23% lenticulars (SO) and 20% ellipical galaxies. The morphological content of compact groups is very nearly the same as in loose groups. There is no dependence of galaxy morphology on density in all compact groups (and possibly in loose groups). Genuine compact groups form only 60% if Hickson’s list.
HI Studies of the Sculptor Group Galaxies
Authors: Carignan Claude , Puche Daniel 
Published: July 2016

AbstractResults from large-scale mapping of the HI gas in the Sculptor group are presented. From our kinematic analysis, a mean global (M/LB) ⋍ 9 M⊙/L⊙ (at the last observed velocity point) is found for the individual galaxies. This is only a factor ~ 10 smaller than the (M/LB)dyn ⋍ 90 M⊙/L⊙ derived from a dynamical study of the whole group. The parameters derived from the mass models suggest that most of the unseen matter has to be concentrated around the luminous galaxies. Under the assumption that the Sculptor group is a virialized system and that all the mass is associated with the galaxies, an upper limit of ~ 40 kpc is derived for the size of the dark halos present in the five late-type spirals of the group.
HI and Mass Distribution of GR8
Authors: Beaulieu Sylvie , Carignan Claude 
Published: July 2016

AbstractThe dwarf irregular galaxy GR8, which is at the extreme faint end of the luminosity and mass functions, is studied using optical photometry and 21cm HI line observations. It is shown that rotation is only important to the gravitational support of the system in the inner parts (r < 250 pc). GR8 is one of the very few non-elliptical systems known (with M81dwA) where the random motions provide essentially all the support in the outer parts (r ≥ 500 pc). The Gaussian nature of the HI distribution and the isothermal distribution of the HI velocity dispersion implies M α R3 in the outer regions of GR8 (ie the stellar disk and the HI lie in the approximately uniform density core of the dark halo).
Tidal Events and Galactic Activity
Authors: Hutchings J.B. , Neff S.G. 
Published: July 2016

SummaryWe report some results from recent and ongoing work which relate to the connection between nuclear activity and tidal interactions. We suggest that tidal events are in general a necessary but not sufficient condition for nuclear activation. We also suggest that nuclear activity generally develops at a ‘late stage’ of a tidal encounter, following star-formation and dust evaporation, and when the most obvious morphological disturbances may have disappeared.
Paired and Interacting Galaxies: Conference Summary
Authors: Norman Colin A. 
Published: July 2016

This has been an excellent conference with a very international component and a rich and wide ranging diversity of views on the topical subject of paired and interacting galaxies. The southern hospitality shown to us by our hosts Jack Sulentic and Bill Keel has been most gracious and the general growth of the astronomy group at the University of Alabama is most impressive.The conference began with the presentation of the basic data sets on pairs, groups, and interacting galaxies with the latter being further discussed with respect to both global properties and properties of the galactic nuclei. Then followed the theory, modelling and interpretation using analytic techniques, simulations and general modelling for spirals and ellipticals, starbursts and active galactic nuclei. Before the conference I had written down the three questions concerning pairs, groups and interacting galaxies that I hoped would be answered at the meeting: (1) How do they form? including the role of initial conditions, the importance of subclustering, the evolution of groups to compact groups, and the fate of compact groups; (2) How do they evolve? including issues such as relevant timescales, the role of halos and the problem of overmerging, the triggering and enhancement of star formation and activity in the galactic nuclei, and the relative importance of dwarf versus giant encounters; and (3) Are they important? including the frequency of pairs and interactions, whether merging and interactions are very important aspects of the life of a normal galaxy at formation, during its evolution, in forming bars, shells, rings, bulges etc., and in the formation and evolution of active galaxies. In what follows I shall summarize the meeting and where possible focus on these three central issues. Since this is a conference summary my references are all to papers presented at this meeting.
Surveys of Spectroscopic Binaries at the Center for Astrophysics
Authors: Latham D.W. 
Published: July 2016

Abstract For more than a decade we have been measuring stellar radial velocities with three almost identical digital speedometers on telescopes in Arizona and Massachusetts. By now we have accumulated nearly 100,000 measurements with a typical precision of better than 1 km s-1. One of the main scientific applications has been surveys of binaries in several different stellar environments, to study the frequency and orbital characteristics of binaries in a variety of stellar populations. A main goal is to confront theories of binary formation and evolution with observational results. With various collaborators we have investigated the binary populations among pre-main-sequence stars, in the Hyades and M67 open clusters, and in the Carney-Latham proper-motion sample. Thus, we have data for coeval samples of binaries covering a wide range of ages. One result is clear evidence for evolution of binary orbits. The orbital period at which there is a transition from circular to eccentric orbits gets longer for older samples of binaries, presumably due to tidal circularization. Another result is that the frequency of binaries does not seem to depend on the stellar population. Binaries are just as common among the oldest stars in the halo of our Galaxy as among the younger stars in the disk.
The Combination of Spectroscopic and Astrometric Data in the Analysis of Orbital Motions in Binary Star Systems
Authors: Morbey Christopher 
Published: July 2016

AbstractEven though various types of data for binary stars are being obtained in unprecedented quantities there is still a lack of completeness. Because the reduction of combinations of these data adds to the fundamental concepts in astronomy it is advantageous to have available a general self-consistent method whereby all the elements of the orbits of a binary or multiple system may be solved simultaneously. Such a method is reviewed in this paper and an emphasis is placed on the specification of meaningful errors attached to the orbital elements.
High-Precision Radial Velocities of Southern Solar-Type Stars
Authors: Murdoch Kaylene , Hearnshaw J.B. 
Published: July 2016

AbstractWith a small telescope and conventional techniques we have achieved external radial-velocity errors for bright stars of only ±50 m/s by using an optical fibre feed between telescope and spectrograph. In a search for low-mass companions to solar-type dwarf stars, intrinsic radial-velocity variability was detected in some IAU radial-velocity standard stars but no convincing evidence was found of the presence of low-mass companions to the dwarfs.
The Companions of the Classical Cepheid FF Aql
Authors: Evans Nancy Remage , Udalski Andrej 
Published: July 2016

AbstractWe have obtained CCD photometry of the classical Cepheid FF Aql and the companion 6″ away to determine whether they are likely to be physically associated. Because the Cepheid is 5 magnitudes brighter than the companion, the measurements are difficult. The values we find for the companion are V = 11.14 ± 0.07 mag, B – V = 0.60 ± 0.05 mag and V – R = 0.39 ± 0.04 mag. If the companion were at the same distance as the Cepheid, its absolute magnitude would be MV = 2.58 mag, corresponding a spectral type of approximately A8 V. The observed (B – V)0 corresponds to a spectral type of F4 V to F5 V. The observed color and spectral type are incompatible with a ZAMS magnitude of the companion at the distance of the Cepheid.Positional measures indicate that there may be relative motion between the two stars, which would be too large to be orbital motion. We conclude that the 6″.8 companion is not a member of the FF Aql system. Information about the four stars in the direction of FF Aql is summarized.
Methods of HIPPARCOS Double Star Parameter Estimation for Relative and Absolute Astrometry within the FAST Consortium
Authors: Bernstein H.-H. , Hering R. , Badiali M. , Cardini D. , Emanuele A. 
Published: July 2016

AbstractThis paper outlines the details of astrometric parameter determination of double stars from HIPPARCOS observations as prepared in the FAST consortium. Methods of parameter estimation are developed for relative astrometry and absolute astrometry. The capability of the procedures will be demonstrated using simulated observations, in describing the particular steps of a Monte Carlo simulation which have been executed at the Istituto di Astrofisica Spaziale (IAS) and at the Astronomisches Rechen–Institut (ARI).
Double and Multiple Star Speckle Observations at the 6-m Telescope
Authors: Balega I.I. , Balega Y.Y. , Vasyuk V.A. , McManus J.J. 
Published: July 2016

During the last 15 years more than 9,000 speckle interferometric measurements of binary stars have been collected using large optical telescopes (McAlister & Hartkopf 1988). Among them a significant contribution to the world speckle data has been made by the 6-m telscope near Zelenchuk. Up to now this instrument provides the maximal spatial resolution for single–aperture telescopes. First speckle images of the binary Capella were recorded at the telescope in 1977 (Balega & Tikhonov 1977), but we spent 5 more years to create special television techniques for photon counting and digital means for image processing before we started the regular interferometric program of binary observations in the wide range of stellar magnitudes. At first, the measurements were conducted in cooperation with French astronomers from the Centre d’Etudes et de Recherches Geodynamiques et Astronomiques using the optical camera and the television detector developed by Blazit et al. (1977). Since 1983 our equipment has been in use. The program of observations was oriented upon the traditional problems of multiple star speckle interferometry:1.Determination of stellar distances and masses for different types of binaries whose orbital elements can be derived. This includes already known fast visual and astrometric pairs with undetermined orbits, spectroscopic binaries that can be resolved directly, and newly discovered interferometric pairs which show fast orbital motion. The main attention was devoted to the late–type dwarfs in the vicinity of the Sun.2.Search for the secondary components whose existence could explain anomalies of stellar spectra or photometry (stars with composite spectra, occultation binaries, etc.)3.Study of unusual binaries (symbiotic stars, binaries with relativistic components, such as SS 433, etc.)
Photometric Observations of Three Double Stars by the Occultation Method — Comparison with Interferometric Results and with Preliminary Results of HIPPARCOS
Authors: Froeschlé M. , Meyer C. 
Published: July 2016

AbstractWe first briefly recall the geometry of the occultation of a double star by the Moon’s edge. Then we give a short description of the principle of the formation of the diffraction pattern. We present the results for three double stars and compare them with those obtained by other methods.
Multicolour Photometric System for Investigation of the Galaxy Population
Authors: Straižys V. 
Published: July 2016

AbstractMany photometric systems for classification of stars have been proposed. However, not all of them are equally suitable for investigation of distant and reddened stars without additional information from their spectra. Earlier it was shown that the Vilnius photometric system is optimum for purely photometric classification of stars in spectral types, luminosities, metallicities and peculiarity types, when interstellar reddening is present. When realized with a CCD detector, the system permits to classify stars down to 17 mag with a 1.5 m class telescope or down to 20 mag with a 4 m telescope. A possibility of realizing the system with the WF camera of the Hubble Space Telescope is investigated. The problem of unification of broad-band and medium-band photometric systems is discussed.