bluuebunny/crossref_metadata_2025_split huggingface dataset:
Searching for Near-Earth Asteroids with the UK Schmidt Telescope at the AAO
Authors: Steel D. I. , McNaught R. H. , Garradd G. J. , Russell K. S. , Asher D. J. 
Published: July 2016

AbstractSince 1990 we have operated a program in which all plates and films exposed at the 1.2 m U.K. Schmidt Telescope (UKST) are searched for suspicious trails that may represent fast-moving (Earth-approaching) objects. When a possible near-Earth asteroid is discovered, we obtain follow-up astrometric positions using photography on either the UKST (if the object is faint) or the 0.5 m Uppsala Southern Schmidt at the same site. Further astrometric positions, once a reasonable ephemeris is available, are obtained with a large-format CCD on the 40 inch telescope of the Siding Spring Observatory (SSO).In the near term we plan to extend our use of the UKST making use of time near bright-of-moon when the telescope is currently underused. We will conduct photographic searching by taking dedicated films in pairs of 5-10 minutes exposure, with 30-60 minutes gaps between. These will then be inspected using electronically blinked video cameras to scan the films and look for objects that have moved between the exposures. We believe that we can better than triple our current discovery rate (which is about 8-10 near-Earth asteroids per year) in this way.In the longer term clearly the installation of a mosaic of CCDs covering some reasonable fraction of the UKST focal surface is a desideratum, and this is under consideration.
An attempt to Derive the Proper Motion for Blanco Cluster 1
Authors: Hidayat Bambang , Wiyanto Paulus 
Published: July 2016

In order to establish the probability of physical membership of open clusters by means of astrometrical methods, two criteria are used: the position distribution of stars in the sky and their proper motions. Proper motion methods have shown validity from a practical point of view; but are difficult to apply where there is a high ratio of cluster-to-field stars, and in crowded fields of the Milky Way.As a test we have selected the nearby (170–190 pc) Blanco Cluster 1 (1 = 16°, b = −73°) in order to avoid complications arising from crowded fields. Photometric data however, suggests that the diameter of the cluster is rather extended (~ 120 arcsec). This will require a large-field solution, rather than a small-field solution which can be obtained with greater accuracy using Schmidt astrometry (Fresneau 1978; Nakamura & Sekiguchi 1993).
Astrometric Programmes of the Abastumani Observatory
Authors: Chanturiya Soso M. , Inasaridze Raguli I. , Kiladze Rolan I. , Kurtanidze Omar M. 
Published: July 2016

AbstractAstrometric investigations undertaken with the 70 cm meniscus and 40 cm double astrograph telescopes are considered. We describe the determination of accurate positions for minor planets, giant-planet satellites, late-type stars, extragalactic radio-sources, optically discovered quasars and compact extragalactic objects in the Second Byurakan Survey.
The Tautenburg Schmidt Telescope and Galactic Proper Motion Studies
Authors: Schilbach E. , Scholz R.-D. , Hirte S. 
Published: July 2016

AbstractThe combination of Tautenburg plates and automatic measuring machines provides a powerful tool to obtain photometry and proper motions of a great number of stars for statistical investigations of our Galaxy. Photographic photometry with an accuracy of about 0.07 mag can be obtained provided two plates of the same colour and a sufficient number of photometric standards are available. With two plate pairs and a 20 years baseline, a proper motion accuracy better than 4 mas/year can be achieved for stars over a wide range of magnitudes. Outside the Galactic plane proper motions are determined with respect to hundreds of background galaxies.
The Edinburgh-Cape Blue Object Survey
Authors: Stobie R. S. , Kilkenny D. , O’Donoghue D. , Chen A. 
Published: July 2016

AbstractThe Edinburgh-Cape Blue Object Survey is a major survey to discover blue stellar objects brighter than B ∼ 18 in the southern sky. It covers an area of sky of 10,000 square degrees with |b| > 30° and δ < 0°. The blue stellar objects are selected by automatic techniques from U and B pairs of UK Schmidt Telescope plates scanned with the COSMOS measuring machine. Follow-up photometry and spectroscopy are being obtained with the SAAO telescopes to classify objects brighter than B = 16.5. This paper describes the survey, the techniques used to extract the blue stellar objects, the photometric accuracy, and the completeness of the survey.
Aitoff Projection Plots and Other Statistical Results for Stars in Volumes 1–4 of the Michigan Catalogue of MK Types for the HD Stars
Authors: Houk N. , Sowell J. , Austin S. 
Published: July 2016

AbstractThe approximately 130,000 HD stars between declinations −90° and −12° have been classified on the MK system. This large, consistently classified database has been used to examine the distribution of the stars in galactic coordinates by using Aitoff equal area plots. Both normal stars, grouped by similar temperature and luminosity types, and peculiar stars of various types, will be displayed. The plots will be published in the Astronomical Journal, rather than in these Colloquium Proceedings.
A Near–IR Survey of the Southern Galactic Plane
Authors: MacConnell D. Jack , Wing Robert F. , Edgardo Costa H. 
Published: July 2016

AbstractWe describe a long term project to find faint, heavily-reddened, cool supergiants and carbon stars and to classify IRAS Point Sources within 6° of the southern galactic plane. Many new supergiants and carbon stars have been found, and thousands of IRAS Point Sources have had their spectral types determined.
A Large Number of Herbig-Haro Candidates Found by the Contrast Enhancement and Unsharp Masking Technique
Authors: Ogura Katsuo 
Published: July 2016

AbstractAbout 1300, 60 and 70 Herbig-Haro candidates have been picked up in the Ori A/L1641, Ori B/L1630 and NGC 2264/Mon OBI regions, respectively, on deep Schmidt plates. The contrast enhancement and unsharp masking technique has been applied simultaneously. Unsharp masking applied to an objective-prism Schmidt plate for the Carina Nebula region has yielded the detection of 38 Hα emission stars, of which 13 are new findings.
Measurement of Rose Indices on a Kiso 4-Degree Objective Prism Plate
Authors: Lee S.-G. 
Published: July 2016

AbstractIn order to check the utilisation of 4-degree objective prism spectra for the deep spectroscopic galactic structure study, Rose’s (1984) seven indices between 3500 Å and 4400 Å for 19 Hyades stars were measured on a Kiso Schmidt prism plate, L3496. By comparison with those of Rose (1984), it is found that his spectral indices, Hδ/FeI, Hγ/P(4325), and P(3912)/P(CN) measured on these low dispersion spectra, are still usable. This result gives good prospects for a deep spectroscopic galactic structure program with the 4-degree objective prism and narrow band interference filters.
A Deep Spectral Survey of Peculiar A-Type Stars
Authors: Kurtanidze Omar M. , Nikolashvili Miriam G. 
Published: July 2016

AbstractWe are conducting a long-term deep spectral survey to investigate the distribution of Ap and Am stars in selected fields of the Milky Way and in open star clusters of different ages. The spectral survey is based on objective prism spectra obtained with an eight degree prism attached to the 70/98 cm meniscus telescope (f/3, 135 Å mm−1at Hδ) at the Abastumani Observatory. Kodak IIIa-J emulsions hypersensitized by baking in nitrogen gas are used in combination with a 500 Å FWHM filter centered on Hδ. A limiting magnitude ofmB= 14 was reached in an exposure time of 120 m. Study of the objective prism plates is still in a very early stage. Observations of the central part of the same field taken with a CCD resulted in a limiting magnitudemB= 16. On the basis of spectral material obtained, a wide range of spectra may be classified in the MK system.
Studies of Extended Southern Galactic Clusters and Loose Star Groupings using the Bosscha Schmidt Telescope
Authors: Wiramihardja S. D. , Hidayat B. , Tejawijaya I. , Hakim  , Malasan L. 
Published: July 2016

One of the programs conducted with the Bosscha Schmidt telescope is the study of loose star groupings and extended galactic clusters in the southern hemisphere (The 1963; Hidayat & Wiramihardja 1978; Hidayat et al. 1994). The aims of the study are, in short, to:
1.investigate or to confirm the physical reality of the loose groupings.2.study the relationship between extended clusters or loose groupings with their environment.3.derive their physical parameters which ultimately can be used to construct the luminosity functions of the objects.The purpose of the present paper is to present one of our results for the extended cluster OCL 1104-584 (NGC 3532). The results of studies of loosegrouping objects taken from the list of Loden (1979) will be presented elsewhere.
The Stellar Structure of the Orion Spiral ARM in Selected Directions. I. The Galactic Anticenter
Authors: Kvernadze Teimuraz M. 
Published: July 2016

To investigate the spatial distribution of various stellar groups in the Hertzsprung-Russell diagram, it is necessary to have homogeneous observational data of MK spectral classification and photometry. This enables us to perform some statistical analyses with sufficient accuracy.This paper reports BV photographic photometry of about 700 stars complete to mV = 12, in the direction of galactic anticenter with (l,b) = (169°, −12.4°), (178°, −2.4°), (184°, 8.9°). For the MK spectral data we used the catalogue by Bartaya and Kharadze (1992), which contains spectral and luminosity classes of 6042 stars in Kapteyn Areas Nos. 44–67. The observational data for this catalogue were obtained using the Abastumani Astrophysical Observatory 70 cm meniscus telescope and an 8°objective prism with dispersion 166 Åmm−1 near Hγ. The errors in classification are equal to ± 0.6 spectral subclasses and ± 0.5 luminosity classes, with a limiting magnitude of mV = 12.5.
Surveys for Hα Emission-Line Stars using the Bosscha Schmidt Telescope
Authors: Hidayat Bambang , Ogura Katsuo , Shinohara Masao 
Published: July 2016

According to McCarthy (1984) the objects detected in objective prism surveys for Hα emission line are a ”most unnatural“ group. Of course they consist of many natural groupings whose identities or other peculiarities could become apparent after observing them with higher dispersion and resolution spectroscopy. In some cases, however, their galactic locations and associations with other known populations, can provide a clue to their population types.The aims of the objective prism surveys using the Bosscha Schmidt telescope can be broadly categorised as follows:
1.Searches for galactic planetary nebulae in the region 240° < l < 360 °; |b| ≤ 10°, initiated by The (1968).2.Searches for T-Tauri stars in some southern dark clouds (Shinohara, Ogura & Hidayat 1989).3.Searches for variations in Hα intensities and luminous emission stars in some selected galactic regions, such as in the Puppis and Carina regions.
The Study of Stellar Populations and Dynamics in the Small Magellanic Cloud using the UKST
Authors: Hatzidimitriou D. 
Published: July 2016

AbstractThe combination of the wide field of Schmidt telescope photographic plates with fast measuring machines such as COSMOS and APM, had a major impact on the study of the global properties of the Magellanic Clouds. Results (based on UKST data) regarding the stellar populations and dynamics of the Small Magellanic Cloud are described here in some detail. The stellar content and kinematics of the intercloud region are also outlined, with particular emphasis on the importance of this region in understanding the interaction between the Magellanic Clouds.
Multi-Wavelength Imaging of Galaxies – using Kiso Schmidt CCD Photometry
Authors: van Driel Wim 
Published: July 2016

AbstractEquipping the 105 cm Kiso Observatory Schmidt telescope with large CCD cameras has initiated a new phase for galaxy photometry studies performed with the telescope. As part of multi-wavelength studies deep multi-colour CCD images were obtained of various types of individual galaxies, as well as pairs and groups of galaxies.
Rotation Curves of 38 Galaxies in Clusters from Scanning Fabry-Perot observations
Authors: Amram P. , Marcelin M. , Balkowski C. , Boulesteix J. , Coarer E. le , Cayatte V. , Sullivan W. 
Published: July 2016

AbstractA major astrophysical problem is related to the fact that rotation curves (RCs)) of galaxies are flat. The presence of a dark halo is most often invoked to explain that. Some controversies exist concerning the existence of a dark halo for galaxies in very hostile environments like in center of clusters. Using a scanning Fabry-Perot interferometer, we have observed Hα velocity fields of a sample of 38 galaxies located in 7 different clusters of galaxies. From this sample, our conclusion is that spirals located in the central part of clusters do not have decreasing RCs within the optical radius.
Results of the Hα Survey of the Small Magellanic Cloud
Authors: Rosado Margarita , le Coarer Etienne , Georgelin Yvon 
Published: July 2016

AbstractWe present the results of a kinematic survey of the Small Magellanic Cloud, performed with a scanning FP interferometer mainly at Hα. These data allow us to study the overall dynamics of the ionized hydrogen of this galaxy as well as the kinematics of classes of objects. In this presentation we exemplify how the availability of data in several wavelengths can be very useful in establishing the nature of large nebular complexes of the Small Magellanic Cloud. Our kinematic study allows us to discriminate faint shocked nebulae (such as supernova remnants) inside bright HII regions. This is confirmed by recently available radio and X-ray data.
Hα Survey of the Large Magellanic Cloud
Authors: Laval A. , le Coarer E. , Georgelin Y.P. , Marcelin M. , Amram P. , Goldes G. , Carranza G. , Rosado M. 
Published: July 2016

AbstractThe LMC is being surveyed in the Hα emission line with a scanning Fabry-Perot interferometer, attached to the 36 cm telescope of the Observatoire de Marseille. The present results concern the kinematical mapping of bright nebulae; it shows that the kinetic energy involved in the gas motion is closely related to the evolutionary stage of the embedded stars. In particular, in the 30 Dor nebula, a few one-peaked line profiles remain at the boundaries of the shells, among the numerous split areas. The 50-100 pc shells exhibit a relatively usual spherical expansion, with velocities in the same range at the boundaries. On the contrary, the 10-20 pc shells of the central core show different velocities of the one-peak sides of the shells.
Three-Dimensional Fabry-Perot Imaging Spectroscopy of the Crab Nebula
Authors: Lawrence Stephen S. , MacAlpine Gordon M. , Uomoto Alan , Gelderman Richard , Woodgate Bruce E. , Brown Larry W. 
Published: July 2016

AbstractA three-dimensional model of the [O III] λ5007 line-emitting gas in the Crab Nebula has been developed from imaging spectroscopy taken with the Goddard Fabry-Perot Imager mounted on the McGraw-Hill 1.3m telescope of Michigan-Dartmouth-MIT Observatory. Several interesting morphological features revealed in three-dimensional isophotal displays are discussed.
Hybrid 3-D Spectrophotometry of Emission-Line Nebulae at Ohio State
Authors: Pogge Richard W. , Lame Nancy Joanne 
Published: July 2016

AbstractA program of 3-D spectrophotometry of emission nebulae being carried out at the Ohio State University will be described. We have had considerable success combining Fabry-Perot imaging, long-slit spectroscopy, and narrowband filter imaging into a hybrid 3-D spectroscopic approach that we have used to obtain detailed spectrophotometric maps of the density, temperature, extinction, and ionization in HII regions and Planetary Nebulae. The centerpiece instrument of this effort, the OSU Imaging Fabry-Perot Spectrograph (IFPS), will be described, and scientific results illustrative of our work will be presented.
Astronomical Observations of Comets and the Io Torus Using Fabry-Perot-Interferometry
Authors: Jockers Klaus 
Published: July 2016

AbstractFabry-Perot interferometers have been applied in a focal reducer to observe radiation from atoms and molecules in comets and in the Io torus. Tunable Fabry-Perot interferometers have been used as narrowband filters, and an etalon with fixed airgap in classical arrangement was employed for the measurement of Doppler shifts and for narrow-line photometry.
A Two-Dimensional Spectrometer for Solar Observation and its recent modifications
Authors: Bendlin Cornelia 
Published: July 2016

AbstractThe instrument presented here is based on the combined use of a Universal Birefringent Filter (UBF) and a Fabry-Perot Interferometer (FPI) to obtain narrow-band filtergrams with a CCD. Scanning through a Fraunhofer line with a sufficient number of wavelength settings is accomplished within a few seconds by tuning only the FPI. The two-dimensional spectrometer in the German Vacuum Tower Telescope (VTT)/Tenerife was used to take observations of high spatial, spectral, and temporal resolution, yielding a wide range of results. Since recently, additional information on the solar magnetic field is obtained with it.
An Infrared Multiobject Fiber–Fed Spectrograph for the Calar Alto Observatory
Authors: Herbst T. M. , Pitz E. , Reuther C. M. 
Published: July 2016

AbstractWe report the first use of a near infrared multiobject spectrograph that can acquire 1–2.5µm spectra of up to 35 objects in a 1000 arcsecond field.
Near-Infrared Spectroscopy of the Surface of Mars Derived from TIGER Spectro-Imaging Data
Authors: Martin P. , Pinet P.C. , Bacon R. , Rousset A. 
Published: July 2016

AbstractHigh spectral and spatial resolution telescopic observations of the western hemisphere of Mars, using the integral field spectrograph TIGER at 0.8-1.1 µm, are described.
A Review of Fabry and Perot discoveries
Authors: Georgelin Y.P. , Amram P. 
Published: July 2016

It is a great pleasure for us, daily Fabry-Perot interferometer (hereafter referred to as FP) users, to pay homage to the genius inventors of the FP. Each day we are still bewildered by the power of this instrument which mainly consists of two pieces of half-silvered glass. Even if equations of physics are perfectly able to describe multiple-beam interferences (hereafter referred to as MBI), something magic remains in our mind.We will tackle this paper from a historical point of view. As any discovery, the invention of the FP did not occur just by chance from nowhere. As pointed out by Connes (1986) the invention of the multiple-beam interferometer may be understood as having proceeded from the fortunate convergence of two independent developments: (i) During 2 centuries, MBI has been observed and even computed but its specific and pregnant feature, the fringe sharpening, was not understood before Fabry’s thesis, (ii) A long production of mirrors, leading to the semi-transparent silver film.
Interstellar Wind-Blown Bubbles
Authors: Dyson J. E. 
Published: July 2016

Summary‘Classical’ stellar wind-driven bubbles are either energy or momentum driven, and evolve in smooth media containing only radial density gradients. Real bubbles are produced from winds from moving stars and which blow into non-homogeneous media. The resulting mixing of clump material can produce a variety of thermal, dynamical and chemical effects. In this review we discuss some of the modifications to classical bubbles which ensue, using observational examples where appropriate.
Supernova Remnants
Authors: Falle S.A.E.G. 
Published: July 2016

Abstract.In this review I will concentrate on older remnants, by which I mean those in which radiative cooling is important somewhere and the swept up mass is sufficiently large for the details of the initial explosion not to matter. For such remnants it is the optical emission which is crucial since it allows us to deduce a great deal about the physical state of the emitting gas provided we are careful about how we interprete it. Without discussing any particular remnant in detail, I will consider how large and small scale density variations in the ambient medium affect the appearance and energetics of such remnants.
Dust Condensation in the Ejecta of SN 1987A
Authors: Lucy L.B. , Danziger I.J. , Gouiffes C. , Bouchet P. 
Published: July 2016

AbstractAn asymmetry of optical emission lines that appeared in Sept. 1988 is interpreted as evidence of dust condensation within the metal-rich ejecta of SN 1987A. A quantitative analysis of this spectroscopic effect is given and shown to be compatible with the photometric record. Moreover, observational and theoretical estimates of the bolometric light curve come into agreement when the far-IR excess is interpreted as thermal emission by grains in the ejecta. A grain population comprising small silicate grains with an admixture of graphite or amorphous carbon particles is suggested by the data. The relevance of this discovery to suggestions that supernovae are major sources of interstellar dust is briefly discussed.
Infrared Environment of the BE Star 6 Cephei: Interaction of Stellar and Interstellar Winds
Authors: Kun M. 
Published: July 2016

Abstract:Several arclike structures are seen on the high resolution IRAS images (processes via GEISHA system of Groningen) centred on the Be star 6 Cephei, among others an extended bow shock which indicates the rapd motion of the star and the interstellar matter relative to each other. 6 Cephei is embedded in a giant infrared-emitting shell which is thougth to be a three million year old supernova remnant, therefore in this case the presence of the bow shock around the star shows the interaction of a supernova blast wave with the stellar wind of a Be star. In this paper an attempt is made to reveal the history of the interactions of the star with its surroundings during different periods of its life which are recorded on the infrared maps. Some aspects of the formation and evolution of 6 Cephei can be inferred also from its infrared environment.
Near-Infrared Images of the Serpens Molecular Cloud Core
Authors: Eiroa C. , Casali M. 
Published: July 2016

ABSTRACT:Near-infrared images of the Serpens molecular cloud core have been carried out at UKIRT (Mauna Kea Observatory) using the infrared array camera, IRCAM. A large-scale diffuse nebulosity extending over the central part of the core is observed. Over 100 K-sources are detected in the 30 arc min2 cloud core. Some of them are PMS objects which were previously unknown. For the first time, a near-infrared counterpart of the far-infrared source Seroens FIRS1 has been detected. The 2.2 µm source appears as a point like object at the apex of an extended knotty, jet-like nebulosity oriented towards the northwest. In addition, a group of 11 stellar objects is seen in the position of the IR/radio source SVS4. These objects are embedded in a very faint nebulosity and form one of the densest clustering of young stars found in dark clouds.
The Shaping of the Optical Jet of the Galaxy NGC 4258
Authors: Martin P. , Roy J.-R. , Noreau L. , Lo K.-Y. 
Published: July 2016

SUMMARY.Hα + [NII] and red continuum CCD images as well as high resolution aperture synthesis CO maps were obtained in order to study the optical jet of the barred spiral galaxy NGC 4258. The CO observations show two clouds near the center of the galaxy; these clouds outline a channel and the Hα jet follows this channel. The observations are consistent with the jet being in or making a small angle with the galaxy plane. It is concluded that the interstellar medium may play an important role in making jets detectable optically and in shaping their forms.