bluuebunny/crossref_metadata_2025_split huggingface dataset:
Microwave Spectroscopy of Astrophysical Molecules
Authors: Irvine William M. 
Published: June 2019

ABSTRACTRecent detections of new molecules in dense interstellar clouds, first detections of certain chemical elements in interstellar molecules, and new information on isotopic fractionation of hydrogen in the interstellar medium are discussed in the context of the need for new laboratory data on transition rest frequencies, reaction rates, and branching ratios.
Atmospheres of Planets and their Satellites
Authors: Strobel Darrell F. 
Published: June 2019

ABSTRACTA general review of the chemistry of planetary atmospheres was given with the emphasis on the outer planets and their satellites. The impact of the scientific findings of the Voyager Mission on our understanding of the chemistry and composition of the Jovian, Saturnian, and Uranian atmospheres was highlighted. Hydrocarbon photochemistry will be treated in the context of comparative planetary atmospheres and illustrated by important similarities and differences. The interesting chemistry of satellites with significant atmospheres, Titan, Triton, and Io was explored in the evolutionary context and the impact on the magnetospheres of their parent planet.
The Far-Infrared (IRAS) Excess in Roberts 22 and Related Objects
Authors: Parthasarathy M. 
Published: June 2019

ABSTRACTFrom an analysis of the IRAS data of Roberts 22,Ml-92,M2-9,OH 231.8+4.2,M1-91,MWC 922,Hen 401,Mz-3,OH 19.2-1.0 and OH 26.5+0.6 it is found that the characteristics of the dust shells or disks around these objects are similar to that observed in planetary nebulae. These ten objects may be described as transition objects evolving from the tip of AGB towards left in the HR diagram. The bipolar and disk geometry of the dust envelopes around these objects may be the result of large angular momentum of the progenitor star or the central objects may be evolved binary systems embedded in thick disks formed from severe mass loss.
The Next Generation: An 8-16 M Space Telescope
Authors: Illingworth Garth D. 
Published: June 2019

The Hubble Space Telescope is to be a long-lived observatory with wide-ranging spectroscopic and imaging capability in the UV and the visible, and in the near-IR as the second-generation instruments are implemented. HST will have a dramatic impact on our view of the universe. However, it is by no means premature to address the issue of its successor, even though HST has not yet been launched. We must look ahead with the realistic view that HST will degrade and will need to be replaced. The question that we must then address is:What is the UV-Visible-IR Observatory that will follow HST?I will make the case for this being an 8-16 m class telescope.
Molecules in Galaxies: Results from Bell Laboratories
Authors: Stark A. A. 
Published: June 2019

AbstractA decade of galaxy observations at the Crawford Hill 7 m antenna are summarized. Significant results include the mapping of spiral arms in CO, the demonstration that gas in many spiral galaxies is roughly half atomic and half molecular, the detection of extragalactic HCO+, CS, 13CO and C18O, and the observation of molecular material in the halo of M82.
Joint Commission Meeting 5, JCM5: Spectroscopy of Individual Stars in Globular Clusters and the Early Chemical Evolution of our Galaxy
Authors: de Strobel G. Cayrel 
Published: June 2019

The Proceedings of these two meetings will be edited by G.. Cayrel de Strobel, M. Spite and T. Lloyd-Evans and published by the printing office of Paris Observatory.We present here an overview of what has been discussed during these meetings.
Analytical Approximations of Long-Exposure Point Spread Functions and their Use
Authors: Bendinelli O. , Parmeggiani G. , Zavatti F. 
Published: June 2019

AbstractThe observed light distribution in long exposure star images (PSF) may be fitted equally well by a variety of models. But dealing with undersainpled star images, only the use of the multi-Gaussian model allows the correct model parameters estimation, taking into account integration on pixel surface, image off-centering and background behaviour. It is also shown that the convolution of a spherical source with the multi-Gaussian and Moffat’s models gives in practice the same result.
The Microwave Background Radiation: Recent Advances and New Problems
Authors: de Zotti G. , Toffolatti L. 
Published: June 2019

AbstractThe substantially improved intensity measurements at wavelengths longward of the intensity peak of the microwave background are fully consistent with a Planck spectrum. The most precise data disagree with non-relativistic comptonization models for the large submillimeter excess observed by the Nagoya-Berkeley collaboration. The interpretation of such excess as dust emission at high redshifts also faces severe difficulties. Reported anisotropies on scales of several degrees and of tens of arcsec may be contributed, at least in part, by discrete sources. Just because the best experiments at cm wavelengths nave already got close to the source confusion limit, they also provide interesting information on the large scale distribution of radio sources. Polarimetry may be decisive in clarifying the origin of observed fluctuations.
Relativistic Aspects of Reference Systems and Time Scales
Authors: Brumberg V.A. 
Published: June 2019

Mindful of the fact that any time and space coordinates of General Relativity Theory (GRT) are not, in general, physically meaningful and measurable quantities, one may choose between three possibilities in applying GRT to ephemeris astronomy:
1)avoid coordinates completely, i.e., construct coordinate-independent theories of light propagation and solar system body motion involving the removal of all coordinate-dependent quantities from the present system of astronomical constants;2)use any coordinate system to describe observational procedures and to solve dynamics problems, provided that one and the same coordinates be used for both the kinematics and dynamics of a specific problem;3)adopt IAU recommendations specifying reference systems and time scales to be used in ephemeris astronomy.
X-ray Morphology of Clusters of Galaxies
Authors: Böhringer H. , Schwarz R.A. , Briel U.G. , Ebeling H. , Voges W. 
Published: June 2019

AbstractThe ROSAT observatory with its high spatial resolution X-ray telescope is an ideal instrument for the study of clusters of galaxies. In the first part of the mission an All Sky X-ray Survey was conducted with ROSAT. Here we present first results of observations of Virgo, Perseus and some other clusters of galaxies from the All Sky Survey. These data illustrate the capabilities of the ROSAT observatory for studies of the morphological structure and physical properties of galaxy clusters.
Observation of the Cosmic Microwave Background Anisotropy
Authors: Smoot George F. 
Published: June 2019

AbstractRecent precise observations of the cosmic microwave background (CMB) isotopy and experiments in progress are summarized. The current measurements on all angular scales are approaching sensitivities of the order of ΔT/T ≈ 10-5. Nearly all experiments are observing positive detections. Most assume the detection to be due to galactic emission or other foregrounds or systematics and not due to primordial anisotropies in the CMB. The context and significance of these observations are discussed.
The Microwave Background Radiation: An Alternative View
Authors: Narlikar Jayant V. 
Published: June 2019

Why do we need to think about any alternatives when the primordial interpretation of the microwave background radiation (MBR) has been accepted by so many for so long? The answer is that the primordial interpretation, in spite of its successes has manifest shortcomings in spite of attempts to remove them by so many for so long. To mention a few:
a)Why is the MBR temperature 2.7 K? The value is taken as a parameter in all early universe calculations; it is not predicted by the hot big bang theory with or without inflation.b)There are other astrophysical processes of comparable energy density and other radiation backgrounds that have no primordial origin; why should MBR alone stand out as the odd one out just at this epoch?c)Why are there no signatures of structure formation on the MBR; why is it so smooth?d)The hot big bang model relates to the universe in the first three minutes while the MBR is observed in the more recent past; are we not making too long a jump across from the one to the other?
Deuterium in the Solar System
Authors: Owen T. 
Published: June 2019

AbstractValues of D/H measured in the methane on the giant planets and Titan indicate the presence of two distinct reservoirs of deuterium in the outer solar system. The dominant reservoir is in hydrogen gas, the second, multi-component reservoir is found in the hydrogen that is bound in condensed compounds. Both reservoirs appear to have originated in the interstellar medium. In contrast, the values of D/H in water vapor on Mars and Venus (especially) exhibit a large enrichment from the “condensed matter” starting value. Interpretation of this enrichment may illuminate the history of water on these two planets.
Solar System Objects in the HIPPARCOS Programme
Authors: Bec-Borsenberger A. 
Published: June 2019

AbstractForty eight minor planets and two planetary satellites have been retained in the Hipparcos programme. The observations of minor planets will be used to try to determine the dynamical equinox and the rotation of the Hipparcos reference system (S. Söderhjelm and Lindegren, 1982); they can be also used to determine some physical properties of minor planets. As for the observations of planetary satellites, they will allow to obtain accurate ephemendes of these objects and to improve those of the primary planets. The inclusion of minor planets and satellites in the observing programme raises very specific problems: owing to their motion, positions of these objects are given in the Input Catalogue using ephemerides; preparatory astrometric work needed for improving these ephemerides (ground-based observations and improvement of orbital elements) has been described in Bec-Borsenberger (1989, 1991a). To be sure that the ephemerides are sufficient to get the 1 arcsecond predictability needed for Hipparcos, a reduced programme of ground-based observations will last all along the Hipparcos campaign (with the automatic meridian circles of Bordeaux and La Palma observatories). Presently, an annual update is adequate in order to ensure this precision. The improved orbital elements and predicted ephemerides for years 1991 and 1992 are published (Bec-Borsenberger, 1990, 1991b): the residuals obtained from the last set of improved elements with the meridian observations made for the Hipparcos programme givermsin right ascension and declination between 0.19 and 0.38 arcsecond for all Hipparcos minor planets. Since the launch of Hipparcos, the two satellites have been observed and about a third of the minor planets of the programme have been found; the previsions allow to hope to observe this year about ten more minor planets.
On-Ground Attitude Determination in the HIPPARCOS Mission
Authors: Donati F. , Canuto E. , Falin J.L. , Froeschlè M. , Kovalevsky J. 
Published: June 2019

AbstractAn accurate on-ground reconstitution of the satellite three-axes attitude from the downlinked star mapper photon counts is an essential factor in the final accuracy of the Hipparcos Astrometric Catalogue. The reconstitution method developed by the FAST Consortium and currently on use to process Hipparcos data is the concern of this paper. After on outline of the main reconstitution models and algorithms, an accuracy assessment of the estimates, attitude and star coordinates, coming out from the first year data reduction, is presented; the assessment shows that attitude root mean square errors are already around the mission target of 0.1 arcseconds.
Tycho Astrometry and Photometry
Authors: Høg E. 
Published: June 2019

AbstractIn the Tycho project astrometric and photometric data of about 1 000 000 stars to a limit of B = 12 mag will be derived. The brightest 500 000 stars will obtain magnitudes in two colours BT and VT, the fainter 500 000 usually only one broad-band magnitude T. There is confidence that an accuracy will be achieved about 0.03 arcsec for positions and 0.03 mag for magnitudes, at B = 10.5 mag. The results are obtained by appropriate treatment of the continuous data records generated by the Hipparcos satellite’s star mapper (which provide simultaneous measurements in two spectral channels), based on predicted star transits using its own ‘Tycho Input Catalogue’. The data treatment is carried out by the Tycho Data Analysis Consortium (TDAC), using calibration and satellite attitude information from the two Hipparcos data reduction consortia. An overview of the data reductions is given. Raw observation data and their numerical treatment are described. This assessment is based on a small data set, i.e. 12 weeks spread over the first 8 months of the Tycho ‘revised mission’ where the satellite is in the elliptical transfer orbit, instead of the intended geostationary orbit.
Double Star Recognition
Authors: Frœschle M. , Mignard F. , Falin J.L. 
Published: June 2019

AbstractHipparcos observations provide a wealthy source of discovery of new double and multiple stars. We have developed adequate procedures to recognize in the signal parameters the multiplicity of the stellar source passing through the Hipparcos field of view. These procedures are outlined together with the design of the statistical tests employed. Sampling on real data indicates that about 6000 new double stars will be detected at the mission completion.
A Comparison of the Southern Optical and Radio Astrometric Reference Frames
Authors: White Graeme L. , Jauncey D.L. , Reynolds J.E. , Lestrade J.-F. , Malin D.F. , Russell J. , Johnston K.J. , Vegt C. de , Nicolson G. 
Published: June 2019

AbstractA comparison of accurate optical and radio positions is presented for 25 southern compact radio objects. There is a systematic “S” shaped trend indicating a zonal bias in the Perth 70 optical catalogue.
Proposal for a Second HIPPARCOS
Authors: Høg E. , Chubey M.S. 
Published: June 2019

AbstractAn improved astrometric space mission similar to Hipparcos is proposed for launch ten years after the present Hipparcos. The new mission should provide positions, parallaxes and annual proper motions with an accuracy about one milli-arcsecond for some 400 000 stars. The positions from the two missions would give proper motions for the 120 000 common stars with an accuracy about 0.2 milli-arcsecond per year, ten times less than expected for the first mission. The improvements of the satellite relate e.g. to: larger telescope aperture, smooth attitude motion, enhanced star mapper for four-colour observations (B V U R) of two million stars. The proposal resulted from discussions with members of the Pulkovo Observatory and the Hipparcos Science Team, and it is being considered by the Mission Control Centre, Moscow.
GHRS Observations of the Bp Star, chi Lupi
Authors: Leckrone David S. 
Published: June 2019

AbstractHigh resolution, high S/N ultraviolet observations of the ultra-sharp-lined Bp star chi Lupi, obtained with the Goddard High Resolution Spectrograph, reveal an unprecedented level of spectroscopic detail. Spectral synthesis of the Hg II λ1942 resonance line confirms the extreme isotope abundance anomaly of mercury in this star. The data also provide the first positive detections of Ru II and Zr III, and tentative detections of As I and Ge II.
Atomic and Molecular Data Needed for Analysis of Infrared Spectra from ISO and Sirtf
Authors: Bernath P.F. 
Published: June 2019

AbstractThe satellites ISO and SIRTF are cryogenically-cooled infrared observatories. These telescopes will provide a tremendous increase in sensitivity and will, therefore, require new laboratory data to support their missions. A survey of some of the necessary atomic and moelcular data is presented.
A Unified Picture of Large-Scale Structure
Authors: Bahcall Neta A. 
Published: June 2019

AbstractA consistent picture of large-scale structure appears to be emerging from different types of observations including the spatial distribution of galaxies, clusters of galaxies, narrow pencil-beam surveys, and quasars. I describe these observations below. A network of large-scale superclusters, up to ~ 150 Mpc in scale, is suggested. The supercluster network surrounds low-density regions of similar scales, suggesting a “cellular” structure of the universe. (Ho = 100 km /s/ Mpc is used).
Archiving of Current Observational Data on Variable Stars
Authors: Dubois P. 
Published: June 2019

The first question is : which types of data should we archive for variable stars?Let us consider the three following types of data : (i) raw data (output of the telescope, time…); (ii) reduced data (flux, magnitude…); (iii) processed data (light curve…).We generally need the third one and use the reduced data only when we have trouble with the processed data or when we could obtain better processed data. We never quite go back to the raw data. The situation could evolve with raw data obtained with the CCD frame where the reduction procedure is more complex than with electronic counts. Then, at first sight, we have first to archive the processed data, then make an effort on reduced data and raw data.
Student Projects using Astronomical Data Bank
Authors: Gerbaldi M. , Dupré J. 
Published: June 2019

There are several ways to use a computer with students for teaching Astronomy. Among many others we can list the following : to emulate and to explain the phenomena as with a planetarium, to visualise some astronomical properties such as the motions in a binary-stars system, or to simulate some observations with a telescope. We shall present here a different approach : the use of a computer to compute and to analyse the content of an astronomical data bank.The projects developed with the students, in this context, allow them to have access to real astronomical data obtained by professional astronomers and then to make an analysis of the data based on their own knowledge.
On [Tibullus] III, 19 (IV, 13)
Authors: Lee A. G. 
Published: June 2019

In considering whether or not this poem is genuine Tibullus we have only internal evidence to go on. Internal evidence is often not conclusive enough. It is difficult to assess, and the assessment usually involves a subjective element. The ideal is to reduce this subjective element to a minimum, to appeal to logic in the way a textual critic does when he chooses one MS reading rather than another or decides to admit an emendation of the text. The textual critic's choice of reading or the truth of his emendation cannot be proved in the way a madiematical theorem can be proved, but none the less we can know that the critic is right or wrong on grounds of probability, which in this field is the only available criterion.I want now to point to the kind of internal evidence I shall appeal to: it is literary reminiscence, or imitation. Most often no deductions at all about priority can be drawn from parallel passages in different authors; one simply notes them and that is that. But sometimes a deduction about priority can be made. Under what conditions? And precisely how? To answer these questions I shall quote an example from English poetry, because it is particularly instructive to see ‘imitation’ at work in one's own language.
Inconsistency of Plot and Character in Aeschylus
Authors: Dawe R. D. 
Published: June 2019

The plays of Aeschylus contain many contradictions, and much recent criticism of the dramatic technique of this author has been directed at attempts to extract from these contradictions a unified picture of what the poet really intended us to understand in the case of each particular play. Within the last few years no less than four major articles have been devoted to giving a logically consistent interpretation of the Seven, and if one extends the range to, say, the last thirty years, one can find that all the plays of Aeschylus have been subjected to criticism of a similar kind.All this may seem entirely praiseworthy; and yet, as we come to read more and more of these books and articles, the sensation may grow upon some of us that we are not so much learning about Aeschylus as witnessing the transactions of a private club: transactions conducted with admirable propriety, but according to a system of rules which has been left unrevised for too long, untouched even after the notorious affair of the Suppliants. Although the members of this club are willing to challenge each others' view-points, they are all agreed that no gentleman would venture to call in question the one great assumption that underlies all their discussions: namely that Aeschylus could not possibly have constructed plays in which such contradictions were deliberately intended; and only seldom can he be allowed to have contradicted himself by oversight.
A Type of Hyperbaton in Latin Prose
Authors: Adams J. N. 
Published: June 2019

False generalisations have often been made about the use of hyperbaton in Latin prose. According to Hofmann-Szantyr, for instance, ‘die klass. Prosa geht im Gebrauch des Hyperbatons…kaum über die Praxis des Aldateins hinaus'. The same scholars also imply that even when Cicero and Caesar do separate a substantive from its attribute, the separating word is seldom a verb. Again, E. Fraenkel, while showing that long disjunctions are common in Cicero, has maintained that hyperbaton ‘vielmehr ist… in der Umgangssprache zuhause’.E. Skard has recendy pointed out the frequency with which Cornelius Nepos uses hyperbaton of the kind which comprises a substantive separated from its attribute by a verb. Since Skard accepts the above assertions of Hofmann-Szantyr, he is led to suggest that Nepos must have been following a Greek master. The favoured candidate is Dionysius of Halicarnassus. Dionysius not only has hyperbaton more often than any earlier Greek prose author; his work περὶ ἐνδόξων ἀνδρῶν may have been a source for some of Nepos' biographies.It is the purpose of this paper to discuss the history of one type of hyperbaton in Latin prose, that consisting of a verb standing between a substantive and its adjective (henceforth for convenience referred to as ‘verbal hyperbaton’). It will be demonstrated that, however easy disjunction might seem in a synthetic language, our device was artistic rather than natural to ordinary speech. The statements of Hofmann-Szantyr mentioned above will be shown to be inaccurate, and Skard's hypothesis to be unnecessary.
The ‘Dirae’
Authors: Goodyear F. R. D. 
Published: June 2019

Battare, cycneas repetamus carmine uoces, diuisas iterum sedes et rura canamus, rura quibus diras indiximus, impia uota:ante lupos rapient haedi, uituli ante leones, delphini fugient pisces, aquilae ante columbas, et conuersa retro rerum discordia gliscet — multa prius fient quam non mea libera auena montibus et siluis dicat tua facta, Lycurge. impia Trinacriae sterilescant gaudia uobis nec fecunda, senis nostri felicia rura, semina parturiant segetes, non pascua colles, non arbusta nouas fruges, non pampinus uuas, ipsae non siluae frondes, non flumia montes.
Understanding the Consumer
Authors: Lamb C 
Published: June 2019

We can produce the tenderest, tastiest, highest welfare beef, pork and lamb in the world but if the consumer wants to buy chicken and fish, so what!The changes that have taken place in what consumers can purchase and what and where they eat are nothing short of phenomenal and on-going.In the 1950s families ate at least one cooked meal together every day, as they had for most of the century. The focus of this meal, lunch, dinner, tea or evening meal, depending on where you lived, was meat and two veg. All of this was cooked from scratch by the housewife, who had probably bought all the ingredients freshly that day.