bluuebunny/crossref_metadata_2025 huggingface dataset:
Extract from A Wrack Behind: Frank Whittle
Authors: Norton Lord Kings
Published: July 2016

Whittle is one of the great engineers of the century, perhaps the greatest if judged by the scale of the consequences of his invention. Only the discoverer of the properties of the silicon chip could claim comparable importance.

Jet propulsion was first demonstrated by Hero of Alexandria in AD 60. The gas turbine was patented by Barber of Nuneaton in 1791. Whittle patented a design for an aircraft engine in 1930 in which propulsion was to be achieved by a jet produced by a gas turbine. By combining the thoughts of two men separated in time by over 1,700 years he made an engine which revolutionised world air transport.
Lord Kings Norton and the Air Registration Board, Part 1
Authors: Cropper Graham
Published: July 2016

The association of Harold Roxbee Cox with the Air Registration Board began in 1938 (the year following its formation) with his appointment as its first chief technical officer — a post to which he was eminently suited by virtue of his experience and already formidable reputation in a wide range of technical aspects of aviation. Interrupted by the war, his service to the ARB was renewed first as consultant and member of the board, later (as Sir Harold Roxbee Cox) as its vice chairman and finally (as Lord Kings Norton) as its chairman.
Extract from A Wrack Behind
Authors: Lord Kings Norton
Published: July 2016

In 1943, with the world still at war, a great discussion on the future of aeronautical education was held by the Royal Aeronautical Society. Not only would the war years, however many were still to come, demand more well-qualified aeronautical engineers, but the longed for peace years, with engineers turning swords into ploughshares, would want more. The discussion was in two parts. One took place on 25 June and the other on 23 July. Many of the leading figures in British aeronautics took part and in the chair on both occasions was Dr Roxbee Cox, a vice-president of the society. The discussion culminated in a resolution based on a proposal by Marcus Langley. That resolution and the discussion which led to it resulted in the recommendation by the Aeronautical Research Committee that a post-graduate college of aeronautical science should be established. This was followed by governmental action. Sir Stafford Cripps, then the minister responsible for aircraft production, set up a committee presided over by Sir Roy Fedden to make specific proposals, and the committee recommended in its 1944 report that such a college should be a new and independent establishment. In 1945 the government created the College of Aeronautics board of governors under the chairmanship of Air Chief Marshal Sir Edgar Ludlow-Hewitt to bring the college into existence and govern it. The first meeting of this board took place on 28 June 1945 and there were present:

Sir Edgar Ludlow Hewitt, Dr W. Abbot, Mr Hugh Burroughs, Sir Roy Fedden, Mr J. Ferguson, Sir Harold Hartley, Sir William Hil-dred, Sir Melvill Jones, Dr E.B. Moullin, Mr J.D. North, Sir Frederick Handley Page, Mr E.F. Relf, Dr H. Roxbee Cox, Air Marshal Sir Ralph Sovley, Rear Admiral S.H. Troubridge and Mr W.E.P. Ward. Sir William Stanier, who had been appointed, was not present.
Extract from A Wrack Behind: Myself, when old
Authors: Norton Lord Kings
Published: July 2016

I am not quite sure when I became old, but I think I must date it in my seventies when I retired from a variety of activities and settled into a more sedentary style of life. I retired from Dowty Rotol and Bergers (and so Hoechst UK) in 1975, from the Royal Institution in 1976, from Ricardo’s and British Printing Corporation in 1977 and sold Withers Estates, very profitably for the Withers family, in 1981.

I was left with the chairmanships of two tiny companies, Land-speed and Cotswold Research. While Landspeed has not served its purpose, Cotswold Research has its place in history. Both companies are concerned with the inventions of Professor Eric Laithwaite, who demonstrated in model and prototype form tracked hovercraft powered by the linear motor. Landspeed failed to develop this, through lack of funds, to a commercially viable transport system, though the Japanese appear to have done so. Cotswold Research, however, made a success of an adaptation of the linear motors to the separation of aluminium from scrap material and for their work, which ended in profitable industrial apparatus and a big saving in manpower, Mr A.P. Bird and I received the Prince of Wales Award in 1986.
The evidence for open and closed exocytosis as the primary release mechanism
Authors: Ren Lin , Mellander Lisa J. , Keighron Jacqueline , Cans Ann-Sofie , Kurczy Michael E. , Svir Irina , Oleinick Alexander , Amatore Christian , Ewing Andrew G.
Published: July 2016

Exocytosis is the fundamental process by which cells communicate with each other. The events that lead up to the fusion of a vesicle loaded with chemical messenger with the cell membrane were the subject of a Nobel Prize in 2013. However, the processes occurring after the initial formation of a fusion pore are very much still in debate. The release of chemical messenger has traditionally been thought to occur through full distention of the vesicle membrane, hence assuming exocytosis to be all or none. In contrast to the all or none hypothesis, here we discuss the evidence that during exocytosis the vesicle-membrane pore opens to release only a portion of the transmitter content during exocytosis and then close again. This open and closed exocytosis is distinct from kiss-and-run exocytosis, in that it appears to be the main content released during regular exocytosis. The evidence for this partial release via open and closed exocytosis is presented considering primarily the quantitative evidence obtained with amperometry.
Absolute Chronology for the Beaker Culture Site of Coval Simó (Mallorca, Balearic Islands)
Authors: Coll Jaume , Ramis Damià
Published: July 2016

This contribution of the absolute chronology for the Beaker culture presents the results of archaeological research that took place at Coval Simó (Mallorca) between 1998 and 2008. Coval Simó is a rockshelter situated at the summit of one of the mountains that forms part of the northern mountain range of the Serra de Tramuntana. The site provided an exceptional undisturbed context, shielding a small space of only 25 m2. Thin sedimentary layers were deposited in a short timespan and later were sealed off by large blocks due to a rockslide falling from the top of the rockshelter. This site has offered significant information related to the occupation of a human group linked to the Bell Beaker culture, and users of other distinctive undecorated pottery vessels. Direct evidence of early island metallurgy was also obtained: smelting slags from local copper minerals. Regarding the methodology used for analysis, short-lived samples were chosen for radiocarbon dating, consisting of bone fragments identified and classified taxonomically. The samples were submitted alternately to two different14C laboratories and the obtained results point to a clear horizon for the early human occupation of the site, ranging between about 2300 and 1900 cal BC.
14C Analysis and Sample Preparation at the New Bern Laboratory for the Analysis of Radiocarbon with AMS (LARA)
Authors: Szidat Sönke , Salazar Gary A , Vogel Edith , Battaglia Michael , Wacker Lukas , Synal Hans-Arno , Türler Andreas
Published: July 2016

The University of Bern has set up the new Laboratory for the Analysis of Radiocarbon with AMS (LARA) equipped with an accelerator mass spectrometer (AMS) MICADAS (MIni CArbon Dating System) to continue its long history of14C analysis based on conventional counting. The new laboratory is designated to provide routine14C dating for archaeology, climate research, and other disciplines at the University of Bern and to develop new analytical systems coupled to the gas ion source for14C analysis of specific compounds or compound classes with specific physical properties. Measurements of reference standards and wood samples dated by dendrochronology demonstrate the quality of the14C analyses performed at the new laboratory.
An Archaeological Mystery Revealed by Radiocarbon Dating of Cross-Flow Nanofiltrated Amino Acids Derived from Bone Collagen, Silk, and Hair: Case Study of the Bishops Baldwin I and Radbot II from Noyon-Tournai
Authors: Boudin Mathieu , Boeckx Pascal , Vandenabeele Peter , van Strydonck Mark
Published: July 2016

Excavations in the cathedral of Tournai revealed two sepultures, which were identified by the excavators as those of bishops because of their special location in the cathedral. One burial was assigned to Baldwin I, who died in AD 1068, because (1) a ring with the inscription “BAL” was found and (2) a funeral stone with text was present on top of the grave mentioning the name Baldewinus. The second burial probably belongs to Radbot II, who was the successor of Baldwin I, and died in AD 1098. Both burials contained textiles (silk), the skeleton, a wooden pastoral staff, and human hair was still present on the skull of what was presumed to be Radbot II. All the protein-containing materials were degraded and/or contaminated. Standard sample pretreatment methods were not able to remove all the contaminants. Single and double cross-flow nanofiltration of the hydrolyzed protein-containing materials were performed. The sample quality for radiocarbon dating was improved and14C data revealed interesting and surprising results. The14C dates of the wooden pastoral staff and permeate femur confirm that the skeleton and tomb belong to bishop Baldwin I. The14C dates of hair and permeate skull indicate that the skeleton may indeed belong to bishop Radbot II. The younger14C dates of the wooden pastoral staff and silk samples indicate a postburial disturbance of the site burial during the 12th–13th century.
19 Years of Mortar Dating: Learning from Experience
Authors: Ringbom Åsa , Lindroos Alf , Heinemeier Jan , Sonck-Koota Pia
Published: July 2016

Since 1994, our team has gained extensive experience applying accelerator mass spectrometry (AMS) radiocarbon analysis for mortar dating, totaling over 465 samples and 1800+ measured CO2fractions. Several samples have been analyzed repeatedly. The research covers both Medieval and Classical archaeology. We therefore believe our experience can be helpful when developing preparation procedures for different kinds of mortars in different areas and in varying chronologies. So far, the main areas of interest have been (a) the churches of the Åland Islands (in the archipelago between Finland and Sweden); (b) the churches in the Åboland Archipelago (SW Finland); (c) sites in the Iberian Peninsula including Torre de Palma (a Roman village in Portugal); and (d) Rome, Pompeii, and Herculaneum (Italy). Most of the analyses before 2000 were hydrolized in only two CO2fractions per sample, and reliability criteria were defined on the basis of how well the ages of the two fractions agree with each other. These criteria have proved most helpful in determining the reliability of14C mortar analyses. Different types of mortar have been investigated, including lime mortars made both from limestone and marble, pozzolana mortars, fire-damaged mortars, and mortars based on burnt shells. Most importantly, separate lime lumps sampled from these mortars have been analyzed sporadically and recently more systematically. The research also includes different types of hydrolysis applied in the pretreatment. In addition to using 85% phosphoric acid (H3PO4), the experimental research includes tests with smaller concentrations of phosphoric acid, and tests based on 2–3% hydrochloric acid (HCl) dissolutions. To characterize the dissolution process, results are presented as age profiles of 2–5 CO2fractions. In our experience, pozzolana mortars have been difficult to date, and HCl dissolution should be used only in special cases and in complementary tests.
The 1st Millennium AD Mediterranean Shipbuilding Transition at Dor/Tantura Lagoon, Israel: Dating the Dor 2001/1 Shipwreck
Authors: Lorentzen Brita , Manning Sturt W , Kahanov Yaacov
Published: July 2016

During the 1st millennium AD, a fundamental set of changes in ship design, building methods, and sequence of construction took place in the Mediterranean. This process is known as the “Transition in Construction.” Before the Transition, ship hull design was based longitudinally on the ship's strakes (“shell-first”). By about the mid-1st millennium AD, the concept and construction of ship hulls had changed and were based on the ship's frames (“frame-based”). The Transition was a complex, nonlinear evolution. High-precision dating of the construction and service period of ships built during the 1st millennium is essential for elucidating the Transition process. Such dating precision is possible using radiocarbon wiggle-matching and Bayesian analysis techniques. The following study uses these techniques to determine the construction, launch, and final voyage (wrecking) dates of Dor 2001/1, a Byzantine shipwreck from northern Israel that was built based on frames. The results indicate that Dor 2001/1 was likely constructed and launched in the first third of the 6th century AD and was wrecked no later than AD 540. This is one of the earliest frame-based ships found in the Mediterranean so far. Dor 2001/1 is therefore an important shipwreck in understanding the Transition, since it provides evidence that frame-based hulls were already being built by the mid-1st millennium AD, about 500 yr earlier than has been commonly accepted.
The Neolithization of Siberia and the Russian Far East: Major Spatiotemporal Trends (the 2013 State-of-the-Art)
Authors: Kuzmin Yaroslav V
Published: July 2016

The updated chronology of the earliest pottery-containing complexes in Siberia and the Russian Far East is presented herein. The appearance of pottery (i.e. the process of Neolithization) in this vast region of Eurasia is discussed based on a model that represents a simple approximation of calendar ages between key sites as isolines. No clear spatiotemporal patterns for the origin and spread of pottery in northern Asia can be observed because pottery-making (unlike agriculture) could have emerged in different parts of the Old World at various times. Before modeling of pottery dispersal is conducted, careful evaluation of typology and technology of ceramics and stone artifacts should be done, in order to avoid the confusing situation when the results of modeling contradict the basic archaeological information.
Synchronizing a Late Glacial Abrupt Cooling Event with Paleoenvironmental and Population Changes: Case Study of the Moervaart Paleolake Area (NW Belgium)
Authors: Crombé Philippe , Robinson Erick , van Strydonck Mark
Published: July 2016

Sum probability and Bayesian modeling of a substantial series of radiocarbon dates from a former extensive lake area in NW Belgium, known as the Moervaart area, allow important hydrological changes to be synchronized with Greenland Interstadial lb (or Intra-Allerød Cold Period). It is postulated that the disappearance of nearly all open water systems (Moervaart lake, anastomosing gullies, and dune-slacks) in response to this short but abrupt cooling event was responsible for a nearly total retreat of hunter-gatherers already some centuries before the start of Greenland Stadial 1 (Younger Dryas).
1.6. Are the Galactic bulge and bar the same?
Authors: Ng Yuen Keong
Published: July 2016

An overview is given of the results obtained about Galactic Structure studies towards the Galactic Centre from star counts. The results indicate the presence of an old metal-rich population (Z = 0.005–0.08; t = 13–15 Gyr), presumably the old Galactic Bulge. In addition, a younger, less metal-rich population was found (Z = 0.005-0.03; t = 8–9 Gyr), likely related to the tri-axial bar found in other studies. In Baade's Window a ratio bulge/bar stars of approximately 1/2 was obtained from star counts.
1.8. Evolutionary population synthesis of AGN host galaxy spectra
Authors: Kollatschny W. , Goerdt A.
Published: July 2016

We compute the stellar population of nearby Seyfert host galaxies and non-active galaxies using population and evolutionary synthesis methods. We find indication of enhanced star formation rates in the host-galaxies of AGN - especially in the circumnuclear regions of Seyfert 2 galaxies.
1.14. Stellar sources in a field at l ≃ −45°, B ≃ 0° of the ISOGAL survey (ISOCAM 7 and 15 microns observations)
Authors: Ojha D.K. , Omont A. , Simon G.
Published: July 2016

ISOGAL is a survey at 15 and 7 μm with ISOCAM of the inner Galactic disk. The survey covers ∼ 18 deg2 in selected areas of the central l = ±30 deg of the Galactic plane, all complemented by 0.8-2.2 μm DENIS data. Combined with the near infrared IJK data of the DENIS survey, it is mainly aimed at the study of the cold stellar populations of the most obscured regions of the inner Galaxy and the corresponding Galactic structure.
1.18. Nuclear rise of rotation curves of galaxies
Authors: Sofue Y. , Tutui Y. , Honma M. , Tomita A.
Published: July 2016

Rotation curves of spiral galaxies have been thought to rise rigidly in the central a few kpc, while they are flat in the outer regions (Rubin et al 1982; Persic 1996). On the other hand, CO-line and recent Hα observations have revealed steeply rising rotation curves near the nucleus (Sofue 1996,1997; Sofue et al 1997a,b; Rubin et al 1997).
2.2. The stellar content of the Quintuplet cluster
Authors: Figer Donald F. , McLean Ian S. , Morris Mark , Najarro Francisco
Published: July 2016

The Quintuplet cluster contains over two dozen post main sequence descendants of massive O-stars, including Wolf-Rayet and OBI stars.

The five Quintuplet-proper members (QPMs) may be dusty late-type Wolf-Rayet carbon stars (DWCLs), and the Pistol star may have a very high luminosity, ≈ 106.7±0.5 L⊙. Coupled with its rather cool temperature, 12–23 kK, the Pistol Star is well in violation of the Humphreys–Davidson limit. We argue that the surrounding “Pistol” nebula was ejected from the star a few thousand years ago.

The cluster stars imply the following approximate cluster properties: tage ∼ 2 to 7 Myrs, M ∼ 104 M⊙, L ∼ 107.3±0.2 L⊙, and NLy,c > 1049.9 s−1. The “Sickle” (G0.18–0.04) radio feature and the mid-IR ring (seen in MSX images) may naturally be explained by the presence of a young cluster and a nearby molecular cloud.
2.3. Mosaic-mapping of very extended objects in (sub)millimetre and near-infrared
Authors: Philipp Sabine , Zylka Robert
Published: July 2016

The details of current and past star formation episodes and the stellar content of the central parsecs of our galaxy are still not very well known (Mezger et al., 1996). We have therefore begun an observing program to study star formation processes in the nuclear bulge. Here we discuss the technical aspects of this program, while the scientific goals are presented by Zylka et al. (1997).
2.7. Chemically decoupled nuclei in disk galaxies
Authors: Sil'chenko O.K.
Published: July 2016

In 1993 I have started an observational program to search for decoupled galactic nuclei with the Multi-Pupil Field Spectrograph (MPFS) of the 6m telescope (Afanasiev et al. 1990); a list of 34 northern candidate galaxies with photometrically distinct red nuclei (Sil'chenko 1994) is used.
2.8. Two dimensional decomposition of the luminosity distribution of the spiral galaxies : ESO598-G009, NGC1515 and NGC7456
Authors: Choi Young-Jun , Park Byeong-Gon , Yoon Tae Seog , Ann Hong Bae
Published: July 2016

Because it is inevitable to lose some information in the process of one dimensional luminosity profile extraction, we developed a two dimensional luminosity decomposition method in order to examine the structure of galaxy such as bulge, bar and spiral arms.
2.9. Microlens mapping of disks in active galactic nuclei
Authors: Yonehara A. , Mineshige S. , Fukue J. , Umemura M. , Turner E.L.
Published: July 2016

Generally, it is believed that there is a supermassive black hole and a surrounding accretion disk in a central region of active galactic nuclei (AGN). However, it is quite difficult to obtain direct information about the center of AGN, because the accretion disk size is far too small to resolve.
2.12. Strong gravitational slingshot effect in centra parts of stellar and galactic systems
Authors: Anosova J.
Published: July 2016

We study numerically the dynamical evolution of models of stellar systems which contain two heavy centers of gravity and extended shells inside and around orbits of these binaries. Initially the binary components surrounded by numerous small-mass particles on shells with small initial velocities. It is shown that at some moment of time there is a collapse of these particles on to the heavier component of the binary. We have the strong interactions of bodies at this time. Frequently, the ‘gravitational slingshot’ effect occurs. Further in time, some part of particles which initially were outside the binary orbit escape from the system. Other particles are captured by binary components forming in the center a ‘dumb-bell’ bar. During evolution of our models different kinds of structures of systems often are very similar to the observed structures of galaxies: spiral and elliptical galaxies, interacting galaxies, different kinds of flows and jets. Totally systems are expanding. Formation of different kinds of structures of galaxies depends on motions of particles with respect to the line of apses of the nuclear binary: 1. in the case of almost orthogonal motion (the gravitational slingshot effect), these particles escape from systems and before an escape form open expanding spirals; 2. in the alternative case (small angles of motion of the particles with respect to this line), these particles are captured by the binary components; 3. in the intermediate cases, particles form different kinds of flows like jets, rings, close spirals etc.
3.4. Molecular hydrogen emission in galaxies: the case of NGC 6240
Authors: Egami E.
Published: July 2016

The ISO SWS spectrometer has enabled us to detect for the first time the emission lines from the pure rotational transitions of molecular hydrogens (H2). We have been investigating the physical conditions and the excitation mechanisms of H2 in bright IR galaxies. Here, we present the preliminary results for NGC 6240, which is probably the most interesting object in our sample because of its largest known H2 luminosity.
3.7. Diffraction-limited IR speckle masking observations of the central regions of Seyfert galaxies
Authors: Wittkowski M. , Balega Y. , Beckert T. , Duschl W.J. , Hofmann K.-H. , Weigelt G.
Published: July 2016

We present speckle masking observations of Seyfert galaxies with the Russian 6 m telescope. Diffraction-limited resolution of 76 mas in the K-band was obtained for the first time. This resolution is similar to the resolution of recent MERLIN and VLA observations of galactic centers, thus allowing us to study the radio-IR spectrum of the same structures. Figure 1 shows the decreasing K-band visibility function of NGC 1068 and the contour plot of our reconstructed image. The results show that NGC 1068 is resolved with a FWHM diameter of 30 mas or 2 pc for an assumed Gaussian flux distribution. The image is elongated in northern direction, which is approximately the direction of the radio jet. In the right panel of figure 1 the observed flux values at 5,15 and 22 GHz (from) are plotted together with our K-band flux. The spectral index between 5 GHz and the K-band is approximately 1/3. This spectrum can be explained by synchrotron emission of quasi-monoenergetic relativistic electrons (as for our Galactic Center by). Assuming that the observed flux is mainly nuclear light (from, for example, scattering lobes above and below a torus, without absorption and re-emission) we use the same synchrotron model as has been used for the Galactic Center to explain our data. With this model, we find a source radius of R ∼ 1015 cm, a magnetic field of B ∼ 11 G, a electron number density of ne ∼ 1.1103 cm−3 and a mean electron energy of ∼ 2.7 GeV. The corresponding model spectrum is shown in the right panel of fig. 1. The observed flux value at 2.2 μm lies slightly above the model spectrum. This could be caused by flux contributions from additional components, for example, a central stellar cluster, an accretion disk or thermal radiation from a dusty torus. We have also observed the central regions of other galaxies. For example, for NGC 4151, we found a dominant central core, which is not resolved, and therefore has a diameter of < 20 mas.
3.8. Are the stellar populations in starbursts, LINERs and Seyfert galaxies similar?
Authors: Joly M. , Boisson C. , Pelat D. , Roos M. Serote , Ward M.J.
Published: July 2016

It is well known that about 10% of galaxies harbour an Active Galactic Nuclei (AGN). A debated question is whether the activity influences the stellar population, or inversely, whether the level of activity is induced by the stellar population. By inspection of AGN spectra of low activity level, it is obvious that starlight contributes to a substantial fraction of the light.
3.11. Resolved structure in the nuclear region of the ultraluminous infrared galaxy Mrk 273
Authors: Knapen J.H. , Laine S. , Yates J.A. , Robinson A. , Richards A.M.S. , Doyon R. , Nadeau D.
Published: July 2016

As an example of the power of near-infrared (NIR) Adaptive Optics imaging in the detailed study of central regions of galaxies, we present high-resolution K-band imaging of Mrk 273, in combination with interferometric radio continuum data.
3.12. High-resolution NIR imaging of circumnuclear regions in barred galaxies
Authors: Pérez-Ramírez D. , Knapen J.H.
Published: July 2016

We present preliminary results of our ongoing programme to obtain subarcsec resolution near-infrared (NIR) images and colour maps of the central regions of a sample of barred galaxies with circumnuclear starbursts, using the CFHT. In those cases where structure is seen in the broad band images, the NIR colour index maps confirm the location of dust lanes and regions of star formation. In those galaxies where the NIR broad band images appear featureless, the colour maps do show evidence for tightly wound spiral or ring structure, as hinted at in the optical.
3.13. Outflow in the Seyfert galaxy NGC 7319
Authors: Aoki K. , Kosugi G. , Yoshida M. , Ohtani H. , Wilson A.S.
Published: July 2016

Aoki et al. (1996) found outflowing gas in the Seyfert galaxy NGC 7319. The velocity of the outflow comes up to 500 km s−1 and its extent is 4 kpc. This outflow is one of the largest outflowing phenomenon that have ever been found in Seyfert galaxies. The radio emission found by van der Hulst & Rots (1981) aligns the outflowing gas. It suggests the radio emission has relation to the outflow. We have made higher resolution radio imaging of NGC 7319 with VLA to study in detail relation of radio emission to outflowing gas. These radio images have been compared to Hubble Space Telescope (HST) archival broad-band WFPC2 image. The systemic velocity 6740 km s−1 (Aoki et al. 1996) gives a distance of 90 Mpc for NGC 7319 assuming a Hubble constant H0=75 km s−1 Mpc−1. Thus 1″ corresponds to 450 pc.
3.18. Observational data implying the NGC 1275 nucleus complexity
Authors: Pronik I.
Published: July 2016

The central unresolved source of the galaxy NGC 1275 in red has a dimension of about 8″, but in blue its bright part is about of 0.″5. HST observations, obtained with the filter λ 2200Å cannot reveal the structure of the source inside 0.″26. Now we have collected the observed features of NGC 1275 nucleus in optics and radio domains, which are possibly associated with the complex structure of the nucleus.
3.19. ROSAT HRI observations of the young starburst galaxy NGC 5253
Authors: Strickland D. K. , Stevens I. R.
Published: July 2016

Large numbers of Wolf-Rayet stars in the nearby (4.1 Mpc) star-bursting dwarf galaxy NGC 5253 indicate the starburst is only ~ 5 million years old (Schaerer et al. 1997). This makes NGC 5253 an ideal object for studying the early phases of starburst activity, in particular superbubbles blown by supernovae and winds from massive stars.

Previous low resolution observations suggested the observed X-ray emission was due to a superbubble. We use the enhanced resolution available with a long ROSAT High Resolution Imager (HRI) observation and find that the X-ray emission arises from several unresolved sources associated with the young star clusters seen in the optical. We discuss the possible origins of the point-like emission, and find that they could be small superbubbles blown by the individual clusters of massive stars.
3.23. The centre of the LMC bar
Authors: Ardeberg A. , Linde P. , Snel R. , Gustafsson B. , Nissen P. E.
Published: July 2016

We study star formation and chemical evolution in the LMC Bar centre with the HST PC and uvby photometry. For all bands, mean turn off star data have σ around 0.015 mag. Present data have zero points from stars in M67. b-y of these stars coincides with target turn off. All measurement bands have zero point accuracy better than 0.010 mag.
3.25. Radiative avalanche driven by a circumnuclear starburst torus
Authors: Ohsuga Ken , Umemura Masayuki
Published: July 2016

Recently, a novel mechanism for fueling active galactic nuclei (AGNs) has been proposed by Umemura et al. (1997a, b). That is a radiative avalanche, in which a rotating gas disk sheds angular momentum due to the radiation drag force exerted by starlight from circumnuclear starbursts, so that the mass accretion onto nuclei is driven. Originally, a thin ring of a starburst region has been assumed for simplicity. However, recent observations have revealed that circumnuclear starburst rings have radial extension of ∼ 10pc up to kpc, and they often consist of compact star clusters of < 10pc Thus, the ratio of the half thickness to curvature radius of the ring can be minimally less than one tenth when all the star clusters are aligned on a plane of an inner gas disk, while the ratio could be larger if the distributions of star clusters are extended due to some velocity dispersions.
3.26. Molecular gas in the nuclear region and the bar of NGC 253
Authors: Sorai K. , Nakai N. , Kuno N. , Nishiyama K.
Published: July 2016

In order to study relationship between molecular gas and star-forming activities, we have made observations of the barred spiral galaxy NGC 253 in 12CO(J = 1–0), 13CO(J = 1–0), and HCN(J = 1–0) emission lines with the Nobeyama 45-m radio telescope. NGC 253 is located in a distance of 2.5 M pc(Mauersbergeretal.(1996)) and has an inclination angle of 78°.5 (Pence 1980). This galaxy has a starburst nuclear region and is suggested in an early stage of a starburst (Rieke, Lebofsky, & Walker (1988)).
3.29. Radio recombination lines from starburst galaxies
Authors: Anantharamaiah K.R.
Published: July 2016

Starburst activity is often heavily obscured by dust. To see through the dust and measure the full extent, power and dynamics of the starburst, we are surveying hydrogen radio recombination lines (RRLs) from famous nearby starburst galaxies. Exploiting the improved sensitivity and dynamic range of aperture synthesis arrays such as the VLA and the AT and millimeter-wave telescopes such as SEST and the IRAM-30m telescope, we have searched for RRLs in about 25 starburst galaxies. RRLs have been detected in 14 galaxies. The observations were made variously at 1.4, 4.9, 8.4, 86, 135 and 232 GHz (Anantharamaiah et al 1993, Zhao et al 1996, 1997, Phookun et al 1997). Table 1 summarizes the observations. In all the cases the detected line originates in the nuclear starburst region and the emission region is resolved with a beam of 1–3″.
3.33. A close look at NGC1068 by adaptive optics: dust torus and micro-spiral structure
Authors: Rouan Daniel , Lai Olivier , Alloin Danielle , Rigaut Francois
Published: July 2016

As the closest Seyfert nucleus, NGC 1068 is a key object to establish on firm grounds the model of active galactic nuclei (AGN). Two important questions relative to AGNs are : i) can we actually see the parsec-scale torus of dust and molecular gas around the central engine predicted by the popular Unified Model model (e.g. Antonucci, 1993)?; ii) how the gas is brought down to the parsec scale to feed the monster, and, in particular, is there a micro spiral/bar system that could produce the required torque ? Adaptive Optics in the near-IR has potential advantages to make a significant progress in those two questions : the low dust opacity and the excellent angular resolution.
4.3. A large-scale CO imaging of the Galactic center by the Nobeyama 45-m telescope: shell statistics and star formation history
Authors: Hasegawa Tetsuo , Oka Tomoharu , Sato Fumio , Tsuboi Masato , Yamazaki Atsushi
Published: July 2016

As a key program of the 45-m telescope at Nobeyama Radio Observatory, we have made high-resolution CO images of the Galactic center region with the 2×2 focal plane array receiver. The data consist of 44,000 12CO and 13,000 13CO spectra taken with 16″ beams spaced by 34″. The 12CO image covers roughly −1.5° ≤ l ≤ +3.4° and −0.6° ≤ b ≤ +0.6° (Oka et al. 1997b)
4.6. Structure of the molecular cloud and star-forming activity in the Sagittarius B2 region
Authors: Sato Fumio , Hasegawa Tetsuo , Whiteoak John B. , Miyawaki Ryosuke
Published: July 2016

Sgr B2 is one of the most active star-forming complexes in our Galaxy located ~100 pc from the Galactic center. Whiteoak et al. (1987) found that groups of the OH and H2CO masers and the compact HII regions are aligned in a north-south line, and suggested that star formation there is being triggered by a single large-scale event such as an interaction between molecular clouds. In order to investigate the total molecular cloud distribution and the triggering mechanism of the active massive-star formation in the Sgr B2 region, we mapped it in the 13CO and C18O (J = 1–0) lines with the Nobeyama 45 m telescope in 1988 March and May. In the 13CO line, an area was mapped of 345″ in right ascension and 495″ in declination covering the whole Sgr B2 molecular cloud at a grid spacing of 15″. In the C18O line, more restricted area was observed at 7.5″ or 15″ spacing. The HPBW of the 45 m telescope was 16″ at 110 GHz. Full description of the observations will be given elsewhere (Whiteoak et al. 1997).
4.8. Distribution of C18O and HNCO emission in the Sagittarius B2 molecular cloud
Authors: Sato Fumio , Hasegawa Tetsuo , Whiteoak John B. , Shimizu Masayoshi
Published: July 2016

Sgr B2, located at a distance of ∼100 pc from the Galactic center, is one of the most active, recent massive-star formation regions in the Galaxy. Based on the 13CO (J = 1–0) line data taken with the Nobeyama 45 m telescope, we presented a cloud collision scenario as the triggering mechanism of the burst of massive-star formation there (Hasegawa et al. 1994). In order to obtain further evidence supporting our model, we observed the Sgr B2 molecular cloud in various molecular lines with the 45 m telescope in 1992 February. Twelve points each with 20″ spacings were observed along several strips 3.67′ long at constant galactic longitudes through the major HII region complexes. Here we report the results of the two lines in the 110 GHz band, C18O (J = 1–0) and HNCO (50,5–40,4). Full description of the observations will be given elsewhere (Sato et al. 1997).
4.11. 3 μm spectroscopy of galactic nuclei
Authors: Imanishi M. , Terada H. , Goto M. , Maihara T.
Published: July 2016

We have carried out spectroscopic observations at 3 μm, where extinction is small, of active galaxies to study the obscured emitting regions with LEWIS(Imanishi et al. 1996) mounted on the Steward Observatory 60 and 61 inch telescopes.
4.15. Dynamics of the Galactic center molecular clouds
Authors: Lee C. W. , Lee H. M. , Ann H.B. , Kwon K.H.
Published: July 2016

We have performed Smoothed Particle Hydrodynamics (SPH) simulations in order to understand the dynamical structures of Galactic Center molecular clouds. In our study it was found that the structures of GC molecular clouds could be induced by the combined effects of a gravitational perturbation by rotating bar potential and the hydrodynamic collisions between the clouds.
5.2. Molecular gas and nuclear outflows
Authors: Irwin Judith A.
Published: July 2016

There is now overwhelming evidence that spiral galaxies can experience nuclear outflows, from radio lobes perpendicular to the disks of edge-on galaxies (Hummel et al. 1983), to optical ionization cones (see list in Wilson and Tsvetanov 1994), to spectacular X-ray emission extending many kpc beyond the disk (e.g. Dahlem et al. 1996). These observations indicate that hot and/or energetic components of the ISM can escape away from the plane of the galaxy from their origin in the nuclear vicinity.
5.13. High-density-and-temperature circumnuclear molecular torus in M51
Authors: Matsushita S. , Kohno K. , Vila-Vilaro B. , Kawabe R. , Tosaki T.
Published: July 2016

It is very important to know the physical conditions of circumnuclear molecular gas in order to understand the nature of Active Galactic Nuclei (AGN), since the circumnuclear molecular gas in active galaxies might be directly affected by or is affecting the activity of nucleus. To investigate the physical conditions of the molecular clouds in detail, multi-line observations with millimeter arrays are essential.
5.15. Star formation and molecular gas in NGC 404
Authors: Cepa J. , Vila B. , Nakai N. , Kohno K. , Kawabe R.
Published: July 2016

The last decade has brought about a completely different picture of elliptical galaxies. The once considered completely inert systems have revealed the presence of fair amount of dust, cool and cold gas, and undergoing star formation. The current statistics is that 80% of elliptical galaxies have detectable cool gas components, and as many as 60% have ionized gas (Knapp et al. 1989, Goudfrooij et al. 1994). Several single-dish CO surveys have been reported in the literature, allowing the deduction of several general properties of the molecular gas in early-type galaxies (Sage & Wrobel 1989, Lees et al. 1991, Wiklind et al. 1995).
5.17. The NRO CO survey of nearby spiral galaxies
Authors: Nishiyama K. , Nakai N.
Published: July 2016

Our survey observation is high spatial resolution (16″) by NRO observatory 45 m antenna and have many galaxies of sample. This high resolution observations (16″ = 1.6 kpc at 20 Mpc) could be to resolve the some characteristic structure, typical molecular gas disk, arm - interarm and optical bar.
5.21. Molecular gas in the center of the elliptical galaxy NGC759
Authors: Wiklind T. , Combes F. , Henkel C. , Wyrowski F.
Published: July 2016

Elliptical galaxies are traditionally defined as gas–free, inert stellar systems. Observations of continuum emission in the far–infrared (FIR) and sub–mm wavelength bands have, however, shown that a large fraction of all ellipticals, ~50% (Jura et al. 1987), contain a dust component. The infrared emission is due to warm dust, in many cases associated with star formation and/or weak AGN activity, while cold dust dominates the long wavelength continuum emission (e.g. Wiklind & Henkel 1995). Some elliptical galaxies also contain a molecular gas component, as seen through CO emission (Lees et al. 1991; Wiklind et al. 1995; Knapp & Rupen 1996). The dust and molecular gas are believed to be associated with each other, but it is not clear what powers the emission: star formation activity and/or AGN activity. Both the molecular gas mass and the FIR luminosity are on average lower in ellipticals than in spiral galaxies of similar luminosities. However, the LFIR/MH2 ratio is larger for the elliptical galaxies. If this ratio is a measure of the star formation efficiency, this suggests that gas is being used up more efficiently in elliptical galaxies than in normal spirals (e.g. Wiklind et al. 1995). Other possibilities is that the FIR dust emission is not only powered by UV–light from young stars, but from other sources as well, or that some dust is not spatially associated with the molecular gas.
6.1. Non-axisymmetric dynamics in galaxy centers
Authors: Combes F.
Published: July 2016

Our Galaxy is representative of the majority of spiral galaxies, which are highly non-axisymmetric, developping bars (m= 2 perturbations), but also lopsidedness and off-centering (m= 1), and superposed higher order perturbations. Recent high-resolution N-body and gas-dynamical simulations have considerably improved our knowledge on the nature and formation of these features. Contrary to previous beliefs, they are not long-lived, but fade away and can be reformed continuously, provided enough gas is supplied to the center, to maintain gravitational instability. The dynamical mechanisms involved are reviewed and discussed, and in particular the new features brought by the dissipative gas component. The role of these axisymmetries in the galaxy evolution, mass concentration, together with nucleus fueling are described, and typical time-scales discussed in particular for confrontation to the Milky Way observations.
6.6. The galactic bar and spiral arms
Authors: Gerhard O.E. , Englmaier P.
Published: July 2016

The inner Galaxy light distribution recovered non-parametrically from the COBE/DIRBE surface brightness data shows an elongated bulge set in a highly non-axisymmetric disk. Gas flows computed in the potential of the COBE bar/bulge and disk have been compared with HI and CO line observations. For the best values of the NIR mass-to-light ratio and pattern speed a good match to the tangent point locations of the inner Galactic spiral arms is obtained.
7.2. 12.5μ imaging of Sgr A West with the Keck Telescope
Authors: Becklin E. E. , Morris M. , Figer D. F. , Ghez A. M. , Puetter R. , Jones B.
Published: July 2016

We have used the 10-meter Keck I telescope and the camera mode of the long wavelength spectrometer to observe the central region of the Galaxy at 12.5 μm. The 96×70 As:Si array used had a scale of 0.114 arcsec per pixel. The filter was centered at 12.5 μm and had a bandwidth of about 1 μm. The array was flat-fielded using sky flats from the background. We observed the central 20×20 arcsec region (about 1pc × 1pc) by using a mosaic pattern of the 11×8 arcsec array in approximately half-array steps. The position of the array was determined after the fact by using structure in the flux in the overlap regions. The accuracy of the positioning was better than 0.1 arcsec. The resultant spatial resolution of the final map was about 0.7 arcsec FWHM based on the size of IRS 7 and IRS 3. The demonstrated diffraction limit of the phased Keck telescope at 12.5 microns is just over 0.3 arcsec FWHM, so that the final resolution is a result of atmospheric seeing and chopper smear. The final map is shown in Figure 1. The map is similar, but of much higher angular resolution, to the 12.5 μm map of Gezari (1992, The Center, Bulge and Disk of the Galaxy, ed. Blitz, Dordrecht: Kluwer, 23).
7.5. Tentative detection of far infrared excess in Arp 220
Authors: Chan Kin-Wing , Moseley S. H. , Dwek E. , Roellig T. L. , Casey S. , Loewenstein R.
Published: July 2016

We report 36 to 50 μm observations of Arp 220 by the Goddard Cryogenic Grating Spectrometer on the Kuiper Airborne Observatory in May 1994. In this measurement, we find the galaxy to be four times brighter than in the measurements of Joy et al. (1986). If both of the observations are correct, this large far infrared luminosity increasing in a short time scale between the two observations suggests that the infrared emission in Arp 220 consists mostly of nonthermal synchrotron radiation which originates from the active nucleus.
7.9. Far-infrared emission and gas to dust ratio in discs and central regions of galaxies
Authors: Mayya Y.D. , Rengarajan T.N.
Published: July 2016

We study the radial profiles of radio comtinuum (RC) and far-infrared (FIR) emissions and also the gas to dust ratio for a sample of 22 spiral galaxies. For this, we use the data from IRAS HiRES FIR maps, available VLA 20 cm maps and radial profile data available on neutral hydrogen (H) and molecular hydrogen (H2, derived from velocity integrated CO intensity). In order to have enough resolution with the 1-1.5 arcminute IRAS beam, the galaxies chosen were large sized and had a 60 μm flux density of more than 5 Jy. The sample consists of: NGC 628, NGC 2403, NGC 2841, NGC 2903, NGC 3079, NGC 3198, NGC 3627, NGC 3628, NGC 4192, NGC 4254, NGC 4303, NGC 4321, NGC 4501, NGC 4535, NGC 4569, NGC 4656, NGC 4736, NGC 5033, NGC 5055, NGC 6503, NGC 6946 and NGC 7331. For 13 of these galaxies information is also available on metallicity (z) and V band CCD maps.
7.10. Confirmation of a MIR source near Sgr A∗
Authors: Cotera A. S. , Werner M. W. , Plavchan P. P.
Published: July 2016

The nature of the nonthermal source Sgr A∗ has been the subject of extensive debate, with evidence mounting that it is in fact a ~ 2 × 106 M⊙ black hole (e.g. Eckart & Genzel 1997). Although previous Mid-Infrared (MIR, ~5-40 μm) observations (Gezari 1992; Telesco, Davidson & Werner 1996) have estabished upper limits on the flux of a potential source at Sgr A∗, they were unable to differentiate a point source at the location of Sgr A∗ from the background. Stolovy et al. (1996) reported the first detection of a compact source coincident with Sgr A∗ to ±0.3″, which they measured to have a flux value of 25±5 mJy. The existence of this source, and a better understanding of its flux and spectral characteristics are needed. We present here confirmation of a MIR source near Sgr A∗.
7.12. The Galactic center – a laboratory for AGN
Authors: Duschl Wolfgang J.
Published: July 2016

In this short note, we summarize recent developments of the understanding of the physics of the Galactic Center. For a much more detailled compilation, we refer to our review paper (Mezger, Duschl & Zylka 1996, A&AR 7, 289) and to Beckert & Duschl (1997, A&A, in press).
7.13. The Sgr A East HII complex and associated features
Authors: Uchida Keven I. , Morris Mark R. , Serabyn Gene , Fong David , Meseroll Thomas
Published: July 2016

The Sgr A East H ii complex consists of 4 compact H ii regions situated just east of and following, in an arc pattern, the edge of the Sgr A East nonthermal shell. Located between the arc of H ii regions and the nonthermal shell is a dense molecular ridge – presumably compressed – known as the “50 km/s cloud”. The hypothesis that these H ii regions delineate massive star formation provoked by the rapid expansion of Sgr A East into the molecular cloud is problematical because of the mismatch of the shell expansion and star formation time scales. We therefore examine the alternative hypothesis that Sgr A East is a quasi-static or slowly expanding structure fed from within by the release of relativistic particles from sources at or near the nucleus. The elongation of SgrA East along the Galactic plane is ascribed to the shear inherent in the velocity field this close to the Galactic center (GC). In this proceeding we discuss our ongoing efforts to model the effects of shear in detail, using the elongation of Sgr A East to constrain its expansion time scale.