scholarly journals 30. Commission des Vitesses Radiales Stellaires

1936 ◽  
Vol 5 ◽  
pp. 188-196
Author(s):  
M. J. S. Plaskett ◽  
MM. Adams ◽  
Campbell ◽  
Frost ◽  
Guthnick ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Pacific Coast ◽  
Radial Velocities ◽  
University Of Michigan ◽  
University Of Texas ◽  
University Of Toronto ◽  
Visual Magnitude ◽  
Under Construction ◽  
The University

The three years that have elapsed since the Harvard meeting of the Union have witnessed steady progress in the determination of radial velocities. While the three large Pacific Coast Observatories have naturally been able to make the greatest additions to radial velocity work, the Yerkes Observatory, the Simeiz Observatory and the Observatory of the University of Michigan have also made valuable contributions. It is a pleasure to report that there will soon be three major accessions to the list of observatories capable of determining radial velocities. The David Dunlap Observatory of the University of Toronto with its 74-inch telescope, which should be in operation soon after the meeting, will have radial velocities as a prominent feature of its programme. The McDonald Observatory of the University of Texas with an 80-inch telescope now under construction should be ready to commence operations in 1936 and will undertake an extensive radial velocity programme. The Radcliffe Observatory at Oxford has now been granted permission by the Courts to remove to Pretoria, South Africa, and will establish there a 74-inch reflecting telescope, which will also be largely employed in the determination of the urgently needed radial velocities of the southern stars fainter than 5.5 visual magnitude. The Commission may, I believe, congratulate itself that substantial assistance in the preliminary steps leading to this permission of removal was provided by our action at the last meeting in presenting a resolution to the Union, duly passed by the General Assembly, pointing out the urgent need for additional radial velocities in the southern sky, and strongly supporting the project of the Radcliffe Observatory to establish a large telescope at Pretoria.

scholarly journals 30. Commission des Vitesses Radiales Stellaires

1933 ◽  
Vol 4 ◽  
pp. 178-189
Author(s):  
M. J. S. Plaskett ◽  
MM. Adams ◽  
W. W. Campbell ◽  
Frost ◽  
Hamy ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Radial Velocities ◽  
University Of Michigan ◽  
International Astronomical Union ◽  
Short Summary ◽  
International Astronomical ◽  
Ann Arbor ◽  
The University

The four years that have elapsed since the last meeting of the International Astronomical Union have witnessed steady progress in the determination of radial velocities, principally at the Mt Wilson Observatory, Pasadena, Cal., the Lick Observatory, Mt Hamilton, Cal., the Yerkes Observatory, Williams Bay, Wis., the Dominion Astrophysical Observatory, Victoria, B.C., the Observatory of the University of Michigan, Ann Arbor, Mich., and the Simeis Observatory in Russia. It will be useful, for the members of the Commission, to give a short summary of the radial velocity work completed and in progress since the last meeting.

Introduction

1984 ◽  
Vol 88 ◽  
pp. 3-3
Author(s):  
A.G. Davis Philip
Keyword(s):  
Financial Support ◽  
National Science Foundation ◽  
Radial Velocities ◽  
University Of Toronto ◽  
New Methods ◽  
Photoelectric Measurements ◽  
The University ◽  
Lead Article ◽  
Made In

The last meeting on the determination of radial velocities was held at the University of Toronto, June 20 - 2A 1966, eighteen years ago. Five of the participants of this meeting were present at that meeting; Abt, Batten, Bertiau, Fehrenbach and Griffin. The lead article was “Photoelectric Measurements of Radial Velocities” by Griffin, followed by “Radial Velocities From Image Tube Spectra” by Rubin, Ford and Christy. These were the major new methods of determining radial velocities.This meeting was planned to discuss the major advances made in the accuracy with which radial velocities can now be measured, and the applications of these methods to astronomical problems. I made a formal proposal at the Commission 30 meetings in Patras, Greece, to hold such a meeting in 1984 and the members of the commission ratified the idea. Subsequently, proposals were made to the Executive Committee of the IAU for sponsorship and to the National Science Foundation for financial support. Union College provided the first financial support and agreed to act as host for the meeting. The result of these activities is the presence of all of you in Schenectady for this meeting. I trust that it will be a productive meeting and I wish you all success with your deliberations.

scholarly journals Mm CO observation of the old nova NQ Vul

1990 ◽  
Vol 122 ◽  
pp. 199-199
Author(s):  
J. S. Albinson ◽  
A. Evans
Keyword(s):  
Interstellar Medium ◽  
Rotational Transition ◽  
Millimetre Wave ◽  
University Of Texas ◽  
Evolutionary Phase ◽  
Mass Estimate ◽  
The University ◽  
Nova Outbursts ◽  
Broad Feature

AbstractWe have observed the old nova NQ Vul in the J = 2 → 1 rotational transition of 12CO at 230.5 GHz at the University of Texas Millimetre Wave Observatory. The spectrum shows narrow features which clearly arise in the local interstellar medium. However these local features are superimposed on a broad feature which peaks at ~ 63 mK. This feature is centred on velocity VLSR ≃ 26 ± 9 km s−1–consistent with that expected for NQ Vul–and has FWHM 80 ± 20 km s−1. The peak antenna temperature corresponds to an integrated flux of 3.2 × 10−15 erg s−1 cm−2.Assuming LTE and a distance of 1.2 kpc the mass of CO is ~ 10−6M⊙ if the line is optically thin. The CO mass is comparable with the total mass ejected in 1976 (4) so the CO we detect at millimetre wavelengths has nothing to do with the 1976 outburst. If the CO/H ratio in the emitting material is similar to that in the interstellar medium (2), the total mass is ~ 0.6 M⊙.The CO mass rules out an origin both in the 1976 outburst and in the post-outburst phase: the CO must have originated in material ejected by the NQ Vul system prior to the 1976 outburst. There are two possibilities. First, the CO may have formed in material accumulated following a large number of nova outbursts. Second, the CO may have been present, or formed, in material ejected by the NQ Vul system during a previous evolutionary phase. The deduced mass is comparable to the mass of CO seen around planetary nebulae (3); the outflow velocity (~ 40 km s−1) would also be in line with this interpretation.In either case, the above mass estimate of 0.6 M⊙ (based on the interstellar CO/H ratio) is likely to be an upper limit as we would expect an enhancement of heavy elements in any ejected material. A determination of 12C/13C and other isotopic ratios would be valuable to pin down the origin of the CO.

scholarly journals Study of Spectroscopic Binaries with the Objective Prism Method

1983 ◽  
Vol 62 ◽  
pp. 104-107
Author(s):  
Frank Gieseking
Keyword(s):  
Radial Velocity ◽  
Frequency Distribution ◽  
Radial Velocities ◽  
Spectroscopic Binaries ◽  
Steep Decrease ◽  
Visual Magnitude ◽  
Objective Prism ◽  
The Individual ◽  
Large Telescopes

The frequency distribution of SB’s over apparent visual magnitude emerging from the catalogue of Batten et. al. (1978) shows a very steep decrease of the number of spectroscopically detected SB’s already for such bright stars of magnitude 7. Considering the number of all stars in the individual magnitude intervals, we find a kind of completeness parameter of the spectroscopic surveys: If we scale it somewhat optimistically at 100% between 0 and 3 mag, we see a 50% decrease of the completeness of our knowledge of stellar radial velocities already for stars fainter than 4.5 mag.This situation is mainly due to the fact that the measurement of radial velocities with conventional slit spectrographs is extremely laborious, requiring long exposure times at large telescopes for the exposure of only one spectrum at a time. – Therefore more efficient methods for radial velocity determinations of fainter stars are urgently needed.

Minutes of the Board of Directors Meeting (Summary)

1973 ◽  
Vol 7 (2) ◽  
pp. 48-48
Keyword(s):  
New York ◽  
Middle East ◽  
Board Of Directors ◽  
Annual Meeting ◽  
University Of Michigan ◽  
University Of Texas ◽  
The Board Of Directors ◽  
Chicago Circle ◽  
The University ◽  
Middle East Studies

The Board of Directors met for its fourteenth meeting at New York on 16 February 1973. The Board approved the Association’s co-sponsorship of Hamline University’s summer project on the Middle East as an encouragement to small institutions and new programs to undertake the kind of activity proposed by the Image Committee and Center Directors. The Board decided to hold the 1974 annual meeting in Boston under the sponsorship of universities in the area, coordinated by Harvard, and also to look into the possibilities of Madrid and New York City for later meetings. The Board approved a proposal to Be submitted by the University of Michigan to the National Science Foundation for an automated data project on the Middle East, as originally envisaged by the Library Committee. The Board also approved the proposal for a translation project submitted jointly by MESA, the University of Texas and AUC to the Office of Education. In accordance with the current Ford grant, the Board designated visiting scholars and alternates to be invited to attend the 1973 annual meeting and to remain in the country for 3 to 6 weeks travelling and lecturing at American and Canadian institutions. The Board reviewed the matters of federal funding of non-academic markets for graduates in Middle East studies and of the State of the Art Conference. It appointed the following Nominating Committee: Professor John Masson Smith, University of California, Berkeley, Chairman, and Professors Frank Tachau, University of Illinois at Chicago Circle, Carolyn Killean, University of Chicago, Michael Lorraine, University of Washington and President Issawi.

scholarly journals The Texas High-Precision Radial-velocity Programs

1999 ◽  
Vol 170 ◽  
pp. 113-120
Author(s):  
William D. Cochran ◽  
Artie P. Hatzes
Keyword(s):  
High Resolution ◽  
Radial Velocity ◽  
High Precision ◽  
Line Profile ◽  
Planetary Systems ◽  
Profile Measurement ◽  
European Southern Observatory ◽  
University Of Texas ◽  
The University ◽  
Search Program

AbstractSeveral different high-precision radial-velocity programs are now underway at The University of Texas. This paper discusses the aspects of these programs that are related to the problem of detection of extrasolar planetary systems. This includes the McDonald Observatory Planetary Search program on the McDonald 2.7-m Harlan Smith Telescope, an accompanying program of high-resolution stellar line profile measurement, the European Southern Observatory planetary search program, the Keck Hyades survey, and the Hobby∙Eberly Telescope planet surveys. Here, we summarize each of these programs, and present recent results from each.

Preparation of Benzene Derivatives: The Yu/Baran Synthesis of (+)-Hongoquercin A

2017 ◽  
Author(s):  
Douglass F. Taber
Keyword(s):  
Electrophilic Aromatic Substitution ◽  
University Of Michigan ◽  
Aromatic Substitution ◽  
Blocking Group ◽  
University Of Texas ◽  
University Of Houston ◽  
National University ◽  
Reformatsky Reagent ◽  
The University

Lutz Ackermann of the Georg-August-Universität Göttingen oxidized (Org. Lett. 2013, 15, 3484) the anisole derivative 1 to the phenol 2. Melanie S. Sanford of the University of Michigan devised (Org. Lett. 2013, 15, 5428) complementary condi­tions for either para acetoxylation of 3, illustrated, to give 4, or meta acetoxylation. Lukas J. Goossen of the Technische Universität Kaiserlautern developed (Synthesis 2013, 45, 2387) conditions for the cascade alkoxylation/decarboxylation of 5 to give 6. Cheol-Hong Cheon of Korea University showed (J. Org. Chem. 2013, 78, 12154) that the boronic acid of 7 could act as a blocking group during electrophilic aromatic substitution or, as illustrated, as an ortho directing group. It could then be removed by protodeboronation, leading to 8. Jun Wu of Zhejiang University coupled (Synlett 2013, 24, 1448) the phenol 9 with the bromo amide 10 to give an ether that, on exposure to KOH at elevated temperature, rearranged to the intermediate amide, that was then hydrolyzed to 11. Dong-Shoo Shin of Changwon National University reported (Tetrahedron Lett. 2013, 54, 5151) a similar protocol (not illustrated) to prepare unsubsti­tuted anilines. Guangbin Dong of the University of Texas, Austin used (J. Am. Chem. Soc. 2013, 135, 18350) a variation on the Catellani reaction to add 13 to the ortho bromide 12 to give the meta amine 14. Kei Manabe of the University of Shizuoka found (Angew. Chem. Int. Ed. 2013, 52, 8611) that the crystalline N-for­myl saccharin 16 was a suitable CO donor for the carbonylation of the bromide 15 to the aldehyde 17. John F. Hartwig of the University of California, Berkeley described (J. Org. Chem. 2013, 78, 8250) the coupling of the zinc enolate of an ester (Reformatsky reagent), either preformed or generated in situ, with an aryl bromide 18 to give 19. Olafs Daugulis of the University of Houston developed (Org. Lett. 2013, 15, 5842) conditions for the directed ortho phenoxylation of 20 with 21 to give 22. Yao Fu of the University of Science and Technology of China effected (J. Am. Chem. Soc. 2013, 135, 10630) directed ortho cyanation of 23 with 24 to give 25.

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