bluuebunny/crossref_metadata_2025 huggingface dataset:
“Putrid Boils and Sores, and Burning Wounds in the Body”: The Valorization of Health and Illness in Late Antique Manichaeism
Authors: Baker-Brian Nicholas
Published: July 2016

Recent publications concerned with attitudes to the human body in the religion of Mani have revealed a complex spectrum of ideas. A reading of the “Manichaean body” informed by a gnostic polarity of flesh versus spirit has been largely rejected, and a more complex, ambivalent portrayal of the body, shaped by specific cosmological and theological readings of its origin and purpose, has come to light. New interpretive tools and approaches have changed perceptions of classical texts and revealed how the “subjugated, perfected [Manichaean body was] put into use in the process of salvation.” For example, rereading chapter 70 of the Coptic work theKephalaia of the Teacher, we encounter a complex lesson that betrays the Manichaeans’ understanding of the dual heritage of the human body. Here the Mani of theKephalaiainstructs his disciples about the correspondences that exist between the fleshly body and the universe and formulates them in a manner that suggests a simultaneous patterning of the two forms: “Mani says to his disciples: ‘This whole universe, above and below, reflects the pattern of the human body; as the formation of this body of flesh accords to the pattern of the universe’” (70.169.28–170.1). The organs and limbs of the body resemble specific astral structures and elements in the universe, and both body and universe are afflicted by a range of competing powers. Chapter 70 offers a melothesiac reading of these archontic powers as zodiacal signs fused with the organs, bones, and sinews of the body (cf. chapter 69). As archons they exercise a malevolent influence over the flesh. However, they are also constantly in conflict with each other, and the cause of bodily sickness lies in their “creeping, and moving within the body. . . [where] they shall beset and destroy one another. . . they shall erupt from the body of the person who will die; and make putrid boils and sores and burning wounds in the body” (70.175.12–14, 16–18). Leaving such colorful descriptions of lesions aside, chapter 70 also indicates that human beings, specifically the Manichaean elect, possess enormous potential as the ones who are able to facilitate the release of the “light” by subduing the activities of the “five camps” (i.e., the face, heart, genitalia, stomach, and ground).
Chronological Framework for the Early Talayotic Period in Menorca: The Settlement of Cornia Nou
Authors: Anglada Montserrat , Ferrer Antoni , Plantalamor Lluís , Ramis Damià , van Strydonck Mark , De Mulder Guy
Published: July 2016

The prehistoric site of Cornia Nou (Menorca) features a number of well-preserved architectural structures belonging to the Talayotic culture. Over the last 6 yr, a team linked to the Museum of Menorca has conducted an archaeological excavation project of a large rectangular building attached to the south side of a substantial and massivetalayot, which is considered the westerntalayot.The main objective of this paper is to present the chronological framework of this building, specifying the period of use and the time of abandonment of the building, as well as the dating of the different phases of its construction. A total of 2714C analyses were obtained from samples of the stratigraphic layers and architectonic structures inside the South Building (SB). This research has provided new insights concerning the early stages of the Talayotic culture. The14C dates allow us to place the first recorded occupation phase of the SB in an interval dated within 1100–900 BC (phase 4). A second phase in the occupation of the SB dates to ∼900–800 BC (phase 5). A final occupation phase could be situated between 800–600 BC (phase 6). However, this record provides evidence to suggest that the construction of the westtalayotmay pertain to a time before the beginning of the 1st millennium cal BC.
Puzzling Radiocarbon Dates for the Upper Paleolithic Site of Sungir (Central Russian Plain)
Authors: Kuzmin Yaroslav V , van der Plicht Johannes , Sulerzhitsky Leopold D
Published: July 2016

A summary is presented of more than a decade-long study of direct radiocarbon dating for one of the most important human burials in Eurasia, the Sungir site in eastern Europe. Eighteen14C dates were produced before early 2014 on three skeletons (Sungir 1–3), and there is still no consistency in the results. In the absence of other independent methods to establish the antiquity of Sungir, a careful analysis is performed of the site's stratigraphy, paleoenvironment, and14C dates run on animal bones from the same layer as the burials. Although the conclusions of this work cannot be guaranteed to be absolutely correct, we suggest that at the present stage of research the age range of ∼26,000–27,210 BP is the most probable time for the creation of the elaborate human burials at the Sungir site.
Challenging the Traditional Chronological Framework of Funerary Rituals in the Meuse-Demer-Scheldt Region: 14C Results from the Site of Lummen-Meldert (Belgium)
Authors: De Mulder Guy , Creemers Guido , Van Strydonck Mark
Published: July 2016

Archaeologists tend to use typochronological frameworks to date their sites. These are based on the appearance of certain cultural markers such as grave types or houseplans. In the Meuse-Demer-Scheldt region, a chronological framework is used for the cremation cemeteries from the Middle Bronze Age until the Late Iron Age based on the size, number, and presence of different types of cremation graves. Radiocarbon dating of cremated bone from the small cemetery at Lummen-Meldert dates this site to the Late Bronze Age. These results challenge the hypothesis that small cremation cemeteries with mostly “unurned” graves date to the Middle Iron Age. The cremation graves without an urn and grave goods are a specific category that has to be dated by absolute dating methods such as14C. The results also suggest a connection with the funerary traditions in the Atlantic region.
A New Database Program Installed at the SUERC Radiocarbon Laboratory
Authors: Tripney Brian G , Naysmith Philip , Cook Gordon T
Published: July 2016

The SUERC Radiocarbon Dating Laboratory has recently replaced its spreadsheet-based record keeping with a new database program, custom designed to help laboratory staff manage the high throughput of nearly 5000 cathodes in the past year. The system can accept data from a variety of sources in addition to manual entry; experimental results can be uploaded from spreadsheets, while integration with graphitization lines means that graphite yields are automatically recorded. The system is able to pass14C results directly to OxCal v 4 for calibration, with the resulting plots incorporated into the dating certificates issued to submitters. There are also benefits to submitters, with electronic sample submission both eliminating transcription errors and speeding up the logging-in process, which keeps turnaround times down. For bone samples, data on collagen yields are now stored electronically and are more readily obtainable from the laboratory. The new SUERC Radiocarbon Dating Laboratory database will make a significant contribution to maintaining the high quality of results produced by the laboratory, aiding staff in tracking sample progress, and monitoring quality assurance (QA) samples going through the laboratory, eliminating transcription errors, and making communication easier between laboratory staff and sample submitters.
Dating Late Paleolithic Harpoons from Lake Lubāns, Latvia
Authors: Meadows John , Eriksen Berit V , Zagorska Ilga , Dreves Alexander , Simpson Joanna
Published: July 2016

Over 3000 prehistoric bone and antler artifacts, collected in the late 1930s from the former lakebed of Lake Lubāns, are held by the National History Museum of Latvia. This collection is remarkable not only as one of the largest known assemblages of bone implements in northern Europe, but also in terms of diversity of forms. The most elaborately worked objects include harpoons, often with two rows of barbs and spade-shaped bases, which are believed to date to the Late Paleolithic, and to be among the oldest organic artifacts ever found in Latvia. Four broken specimens were sampled in 2011 for accelerator mass spectrometry (AMS) dating, stable isotope analysis, and taxonomic attribution by ZooMS. The results support the interpretation that these artifacts were made from large cervid bones, and date all four objects to the early Preboreal (mid-10th millennium cal BC). The Lake Lubāns harpoons therefore fall in the same period as similar harpoons from Denmark, northern Germany, and Poland, although only a handful of these have been dated directly.
14C Dating of Historical Buildings in Japan
Authors: Nakao Nanae , Sakamoto Minoru , Imamura Mineo
Published: July 2016

The radiocarbon dating method was applied to the study of Japanese traditional wooden buildings. The traditional Japanese architecture studied includes the Main Hall of Banna-ji Temple (Buddhist building), Sekisui-in of Kozan-ji Temple (noble house), Hakogi-ke house (farmhouse), and Kawai-ke house (townhouse).14C dating proved useful as a research method to better understand the history of these buildings and Japanese architecture as a whole.
Vegetation Changes Viewed from Pollen Analysis in Rarotonga, Southern Cook Islands, Eastern Polynesia
Authors: Fujiki Toshiyuki , Okuno Mitsuru , Moriwaki Hiroshi , Nakamura Toshio , Kawai Kei , McCormack Gerald , Cowan George , Maoate Paul T
Published: July 2016

This study presents accelerator mass spectrometry (AMS) radiocarbon dates and pollen assemblages of 400-cm core sediments collected from the Karekare Swamp in Rarotonga, Southern Cook Islands, to investigate vegetation changes on the island, in particular those induced by human impacts. Eight14C dates of charcoal and higher plant fragment samples indicate that the sediments accumulated since ∼6.0 cal kBP, with an apparent interruption of deposition (hiatus) from 130 to 132 cm in depth, corresponding to ∼2.8 to 0.7 cal kBP. The appearance of Chenopodiaceae pollen from upland weeds, and Cucurbitaceae andVignapollen grains from cultivated plants suggest that human influence existed in core sediments above 130 cm in depth. The increased abundance ofPandanuspollen and monolate-type fern spores also implies the existence of human activity.
Wood Pretreatment Protocols and Measurement of Tree-Ring Standards at the Oxford Radiocarbon Accelerator Unit (ORAU)
Authors: Staff Richard A , Reynard Linda , Brock Fiona , Ramsey Christopher Bronk
Published: July 2016

This article presents the pretreatment protocols for wood samples processed at the Oxford Radiocarbon Accelerator Unit (ORAU), including recent implementation of a purification method to α-cellulose for non-routine samples. We examine the long-term reproducibility of measurement on wood samples at ORAU through the >100014C determinations made on known-age tree-ring standards processed in each AMS wheel since our present High Voltage Engineering Europa (HVEE) AMS system came on-line in September 2002. A discussion of background measurements is also provided.
Shepsi, the Oldest Dolmen with Port-Hole Slab in the Western Caucasus
Authors: Trifonov V A , Zaitseva G I , van der Plicht J , Kraineva A A , Sementsov A A , Kazarnitsky A , Burova N D , Rishko S A
Published: July 2016

The dolmen known as Shepsi was accidentally discovered on the Black Sea coast (Tuapse region, Russia). Radiocarbon dates show that the classic trapezoidal construction of the Caucasian dolmens with a port-hole appeared in the region as early as 3250 BC. The distinctive structural characteristic for dolmens of that time was a floor slab laid between the side slabs, which were embedded in the ground. The material complex and14C dates show that this type of dolmen coexisted with the Novosvobodnaya-type of the Maikop culture, located on the northern slope of the main Caucasus ridge. This leads to a new hypothesis concerning the regional origin and further development of the megalithic structures in the western Caucasus.
Radiocarbon Distance Between Calendar Dates
Authors: Walanus Adam , Nalepka Dorota
Published: July 2016

The calibration procedure, and especially the nonlinear shape of the calibration curve, makes analyzing a possible dating result a far from straightforward process. This is especially so if the goal is to distinguish between two relatively close events. Proposed herein is a calculator, or alternatively a graph, which enables reading of the difference between two radiocarbon ages corresponding to their expected calendar ages. The result may surprise the less experienced14C users. Such a calculation also indicates the time periods with high or low potential for application of the wiggle-matching method.
Radiocarbon Dating, Mineralogy, and Isotopic Composition of Hackberry Endocarps from the Neolithic Site of Aşikli Höyük, Central Turkey
Authors: Quade Jay , Li Shanying , Stiner Mary C. , Clark Amy E. , Mentzer Susan M. , Özbaşaran Mihriban
Published: July 2016

Carbonate is abundant in many Neolithic tells and is a potentially useful archive for dating and climate reconstruction. In this paper, we focus on the mineralogy, radiocarbon dating, and stable isotope systematics of carbonate in hackberry endocarps. Hackberry fruits and seeds are edible in fresh and stored forms, and they were consumed in large quantities in many Neolithic sites in the Near East, including the site of our study, Aşıkli Höyük in central Anatolia, an Aceramic Neolithic tell occupied from about 9.4 to > 10.3 BP (7.4 to > 8.3 BCE). Detailed14C age control provided by archaeological charcoal permits a test of the fidelity in14C dating of hackberry endocarps. Modern endocarps and leaves yield fraction modern14C values of 1.050–1.066, consistent with levels present in the atmosphere when sampled in 2009. On the other hand, archaeological endocarps yield consistently younger ages than associated charcoal by ca. 13014C years (ca. 220 calendar years) for samples about 10,000 years old. We speculate this is caused by the slight addition of calcite or recrystallization to calcite in the endocarp, as detected by scanning electron microscopy. Subtle addition or replacement of calcite by primary aragonite is not widely recognized in the14C community, even though similar effects are reported from other natural carbonates such as shell carbonate. This small (but consistent) level of contamination supports the usefulness of endocarps in dating where other materials like charcoal are lacking. Before dating, however, hackberries should be carefully screened for mineralogical preservation and context. We examined the carbon and oxygen isotopic systematics of the fossil endocarps to try to establish potential source areas for harvesting. Most of the hackberries are enriched in18O compared to local water sources, indicating that they were drawing on highly evaporated soil water, rather than the local (perched and regional) water table sampled in our study. Isotopic evidence therefore suggests that most but not all of the hackberries were harvested from nearby mesas well above the local streams and seeps fed by the water table.
Dendrochronological Dating in Egypt: Work Accomplished and Future Prospects
Authors: Kuniholm Peter Ian , Newton Maryanne , Sherbiny Hend , Bassir Hussein
Published: July 2016

We assess the state of and potential for expansion of dendroarchaeological research in Egypt. We also report previously unpublished findings, which we hope will assist with the new effort in constructing tree-ring chronologies in Egypt. In doing so, we explain briefly some of the problems and potential of the future enterprise.
1.9. Globular clusters within 5° of the Galactic center
Authors: Barbuy B. , Bica E. , Ortolani S.
Published: July 2016

The knowledge of age and spatial distribution of stars in the Galactic bulge require observational constraints to establish whether its stellar population is very old (Larson 1990) or is a younger, disk-like component (Raha et al. 1992), and if its shape is spherical or extended, or perhaps a bar (Blitz & Spergel 1991). Yet other possibilities are a flattened bulge or a disk-like system (Zinn 1985; Armandroff 1989; Ortolani et al. 1993; Minniti 1995).
1.13. Structural characteristics of spiral bulges
Authors: Byun Yong-Ik
Published: July 2016

Recently it has been suggested that some bulges are really disks (Kormendy 1993). He argues that some bulges are not spheroidal components of steep luminosity distribution like elliptical galaxies but actually parts of flat disks, whose central luminosity profiles are steeper than the inward extrapolation of an exponential fit to the outer parts. The existence of disk-like bulges strongly supports the idea of disk secular evolution.
1.15. J- and H-band observations of the Galactic bulge by PANIC
Authors: Matsumoto Shigeru , Nakada Yoshikazu , Glass Ian S.
Published: July 2016

Nine regions in the Galactic bulge were observed at J and H bands with a PtSi 1040×520 array camera which is named the PtSi Astronomical Near Infrared Camera (PANIC). These regions were centered at l=(–5°,0°,+5°) b=(–6°,0°,+6°) respectively. Each region was covered with nine frames each of which spanned 30′ by 30′ square arcmin. Observations were carried out at the South African Astronomical Observatory, Cape Town, from 1995 to 1997 using a 40cm f/5 Newtonian telescope. A bolometric correction (Frogel and Whitford 1987) was given to the observed stars by using J-H values of reference RGB stars (Frogel et al 1990).
1.16. 4.5 to 11.7 microns spectrophotometric observations of the Galactic bulge by the MIRS/IRTS
Authors: Chan Kin-Wing , Roellig T. L. , Onaka T. , Yamamura I. , Tanabé T.
Published: July 2016

Using the Mid-Infrared (MIRS) on board the Infrared Telescope in Space (IRTS) we obtained the 4.5 to 11.7 μm spectra of the stellar populations and diffuse interstellar medium in the Galactic bulge (l ≈ 8.7°, b ≈ 2.9, 4.0, 4.7, and 5.7°). Below galactic latitute of 4.0° the mid-infrared background spectra in the bulge are similar to the spectrum of M and K giants. The UIR bands (6.2, 7.7, 8.6, and 11.3 μm) are also detected in these regions and they are likely arising from the diffuse interstellar medium in the bulge. Above galactic latitude of 4.0°, the mid-infrared background spectra are similar to the spectrum of those evolved stars with high mass-loss rate detected by IRAS. One likely interpretation is that this background emission arises predominantly from these stars with very low luminosities that have not been detected by IRAS. The main-sequence life time for such low luminosity evolved stars is at least 10 Gyr, even in the metal poor cases. If these low luminosity evolved stars are metal-rich then the age would be much older. Thus, the existence of a large number (~ 75) of such low luminosity evolved stars in a small region (8′ × 8′) in the bulge would have significant impact on our understanding of the stellar content and the age of the Galactic bulge.
1.20. The color-magnitude relation of bulges
Authors: Itoh Nobunari , Ichikawa Takashi
Published: July 2016

One of the main aims with respect to the evolution of spiral galaxies is to clarify how the disk and bulge were formed. The study of bulges has usually been focused on how bulges resemble to elliptical galaxies. For the study of the evolution of elliptical galaxies, the color-magnitude relation (C-M relation) gives us a clue to understanding the formation and evolution of ellipticals. In fact, the tight C-M relation of ellipticals (Bower et al. 1992) was interpreted as the sequence of the metallicity difference (Kodama and Arimoto 1997). On the contrary, there are few observations for the C-M relation of bulges. On the analogy of elliptical galaxies, the C-M relation of bulges, if it exists, may be one of the most important clues to understanding the formation process of bulges. The main goal of the present study is to investigate the C-M relation of bulges.
2.4. Collisional stellar dynamics around a central galactic black hole
Authors: Freitag Marc , Benz Willy
Published: July 2016

Massive but invisible black holes (BH) are often assumed to lurk in the center of many galaxies but definitive proof of their existence has not yet been established. However, in the surrounding stellar cluster stars are unavoidably being destroyed by tidal disruptions and stellar collisions liberating of order 1M⊙ in each event. The subsequent accretion of this gas by the BH could bring it back to “life” and reveal its presence.
2.5. Stellar Mg abundances in the Galactic center
Authors: Ramirez S. V. , Sellgren K. , Terndrup D. M. , Carr J. S. , Balachandran S. , Blum R. D.
Published: July 2016

Star formation in the Galactic Center (GC) happens under unusual conditions, which include high gas temperatures, high velocity dispersions, and strong tidal shear (Spergel & Blitz 1992; Blitzet al.1993). All these conditions may lead to an initial mass function (IMF) dominated by massive stars (Morris & Serabyn 1996). A history of chemical evolution dominated by massive stars is expected to result in enhancements ofα-elements (Mg, Si, Ca, Ti) relative to Fe (Wheeleret al.1989). This argument is the main motivation to study the abundance of Fe and Mg in GC stars.
2.11. Oscillation of a stellar system by a central massive object
Authors: Taga M.
Published: July 2016

We investigated the oscillation of a dense stellar system which harbours a massive object, presumably a supermassive black hole, in its center. The central mass moves in response to the oscillation of the stellar system. This phenomenon may explain the asymmetric structure observed in M31 (Lauer et al., 1993), or NGC4486B (Lauer et al., 1996). Moreover, the motion of the central massive black hole may well induce the accretion of gas onto the black hole itself and ignite the activity in galactic nuclei. We first investigated the stability of a fluid disk around a massive object by linear modal analysis. Next, we performed N-body simulations for spherically symmetric, rotating, particle systems with a central mass.
2.13. Optical and X-ray variability in NGC 4395
Authors: Lira P. , Lawrence A.
Published: July 2016

The spectrum of the dwarf Seyfert 1 nucleus in NGC 4395 was first reported about a decade ago (Filippenko & Sargent 1989), showing high ionization narrow emission lines and broad permitted lines. The later detection of radio and X-ray compact nuclear sources and of a featureless UV continuum gave support to the idea that NGC 4395 is a genuine low luminosity AGN (Sramek 1992; Filippenko, Ho & Sargent 1993). However, it has been claimed that, unlike classic Seyferts, NGC 4395 does not vary at all (Shields & Filippenko 1992).
3.1. Long-term star formation at the Galactic center and its effect on the stellar population
Authors: Serabyn E.
Published: July 2016

Star formation presently occurs in our Galactic nucleus at a rate of several 10−1 M⊙ yr−1. If this value represents the long-term average, some 109 M⊙ of stars should have been generated in our Galaxy's central few hundred parsec volume over the Milky Way's lifetime. As the expected stellar yield is actually in rough agreement with the mass of our Galaxy's bright near-infrared “central r−2 cluster”, it is possible to hypothesize that this massive “nuclear” cluster is in fact the product of long-term nuclear star-formation, rather than being a remnant of the Galaxy's formation epoch. Several lines of evidence supporting this hypothesis are laid out in Serabyn and Morris (1996), to which the reader is referred for a complete discussion and reference list; here only a brief summary of the main arguments is presented.
3.2. ISO spectroscopy of the Galactic center and starburst nuclei
Authors: Lutz D.
Published: July 2016

Since its launch in November 1995, the Infrared Space Observatory ISO has converted mid-infrared spectroscopy into a mature tool. Due to its proximity, brightness, and the wealth of complementary information, the center of our Galaxy remains a unique testbed for studies of galactic nuclei. A first analysis of the 2.4-45μm spectrum obtained with ISO-SWS (Fig. 1) has been presented by Lutz et al. (1996a). One of the surprises is a determination of the mid-infrared extinction law from comparison of the Galactic center hydrogen recombination line fluxes and case B expectations: The extinction law clearly lacks the deep minimum near 7μm expected for standard graphite/silicate mixes. External galaxies are less close to the ideal ‘screen’ case and cannot provide the detail of the GC recombination line spectrum needed to derive an extinction law. However, simple ratios of the strongest recombination lines are inconsistent with a classical extinction law and any dust configuration.
3.6. AGN variability studies: an agenda for the next millenium?
Authors: Ulrich M.-H.
Published: July 2016

Data which are obtained today can be re-acquired better and faster in the future. Their only enduring value, after they have been interpreted, is as historical markers. With electronic archiving one can envision archives covering decades, centuries and even longer periods of observations of selected objects or classes of objects. Such a data base would allow the study of phenomena with low temporal frequencies, and of rare events.

First hints of such phenomena in AGN have been discovered recently: 1) The Seyfert 1s, the best studied AGN at present, exhibit flux variations on time scales ranging from hours to several years (see Ulrich et al. 1997). The faster variations (up to months) have been extensively observed, and they are best understood as being caused by magnetic flares in the corona above the central part of the accretion disk (Blandford and Payne 1982). The origin of the long term and large amplitude UV/optical flux variations (factor 20 in several years as observed in NGC4151 and F9), however, remain essentially unknown.
3.9. Intranight variability of NGC 1275 nucleus in optics implying its central activity
Authors: Pronik I. , Merkulova N. , Metik L.
Published: July 2016

NGC 1275 is one of the enigmatic blazars. The nature of central sources of blazars is open to discussion. Variability measurement of continuum is a major touchstone in the understanding of the nature of central sources of AGNs. Below we examine the intranight optical variability of NGC 1275 nucleus using our observations in 1982-1994.
3.10. X-ray constraints on accretion and starburst processes in galactic nuclei
Authors: Ptak A. , Serlemitsos P. , Yaqoob T. , Mushotzky R. , Terashima Y. , Kunieda H.
Published: July 2016

Although the galaxies in our sample are heterogenous in their optical classifications (LLAGN: M51, NGC 3147, NGC 4258; LINER: NGC 3079, NGC 3310, NGC 3998, NGC 4579, NGC 4594; starburst: M82, NGC 253, NGC 3628, NGC 6946), they are fit well by a “canonical” spectrum with a hot, optically-thin thermal component with T ~ 8 × 106 K and an absorbed (NH ~ 1022 cm−2) power-law with an energy index α ~ 0.7–0.8. Both the “soft” component, most likely due to SN or superwind-heated ISM, and the “hard” power-law, most likely due to a micro-AGN and/or blackhole candidates, appear to be common in low-activity galaxies. If the soft component is associated with a superwind outflow, than ~ 10% of the X-ray emission is due to “swept-up” ISM rather than superwind emission. The abundance of Fe relative to α-process elements tends to be sub-solar, possibly due to dust-depletion and/or type-II SN enrichment. The lack of short-term variability in the hard component suggests that if it is due to an AGN, then the mode of accretion is probably fundamentally different from “normal” Seyfert galaxies.
3.16. Bar-driven spiral density waves and accretion of gas-dominated central disks
Authors: Yuan Chi
Published: July 2016

In this short paper, we report the main results of a comprehensive theory of bar-driven spiral density waves. The theory offers explanations of the morphological difference of the spirals observed in the gas-dominated central disks as well as the different patterns of isovelocity curves distorted by the waves. It also gives reliable estimates of the induced mass flux to fuel the AGNs and starburst ring activities and hence the lifespan of the central disks. In particular, we compare our results with the CO and HCN observations of NGC1068 and M100. Based on these results, we can speculate the possible origin of the central bars and will propose two critical observational tests of the theory.
3.17. MACHO RR Lyrae stars in the Galactic bulge: the spatial distribution
Authors: Minniti D. , Alcock C. , Alves D. , Cook K. , Marshall S. , Allsman R. , Axelrod T. , Freeman K. , Peterson B. , Rodgers A. , Griest K. , Lehner M. , Vandehei T. , Becker A. , Pratt M. , Stubbs C. , Tomaney A. , Quinn P. , Bennett D. , Sutherland W. , Welch D.
Published: July 2016

We have analyzed a sample of 1150 type ab, and 550 type c RR Lyrae stars found in 24 of 94 bulge fields of the MACHO database. These fields cover a range in Galactocentric distances from 0.3 to 1.6 kpc. In combination with the data on the outer bulge fields of Alard (1997) and Wesselink (1987), here we present the surface density distribution of bulge RR Lyrae between 0.3 and 3 kpc.
3.21. Atomic ISM in the nuclear starburst regions of M82 & NGC 253
Authors: Yun M. S. , Ho P. T. P. , Lo K. Y.
Published: July 2016

M82 (NGC 3034) is a nearby (D = 3.3 Mpc) “prototypical” starburst galaxy which emits most of its luminosity in the infrared (LIR = 3×1010L⊙, see Rieke et al. 1980). M82 is also a strong radio source 3C 231, with numerous compact knots which are thought to be young SNR's (Kronberg et al., 1981; Muxlow et al., 1994). Its strong 1.4 GHz radio continuum is extended over the entire 500 pc nuclear starburst region, and the HI absorption is easily mapped at 2″ (30 pc) resolution using the VLA. The resulting velocity integrated optical depth (τΔV) map can be converted to HI column density map if HI spin temperature (Tsp) is known.
3.22. Star formation properties of barred galaxies
Authors: Kandalyan Rafik , Kalloghlyan Arsen
Published: July 2016

The main results of this study can be summarized in the following:

(a)

Magnitude-limited complete sample of barred galaxies was constructed. Space density of barred and unbarred galaxies at low luminosity range (M >-20) almost the same. At the high (M<-20) luminosity range about 30% of the galaxies are barred ones.

(b)

Bars do not have obvious influence on active nuclei. Presence or absence of bars does not related with the large scale galaxy environment.

(c)

Barred spirals, on average, have significantly higher relative star formation rate than that do unbarred galaxies.

(d)

Barred spirals exhibit tight correlations between FIR, radio and X-ray luminosities, while for unbarred spirals these luminosities do not correlated, which indicates on enhanced star formation activity in barred galaxies.

(f)

Group and non-group barred galaxies may differ by star formation activity.
3.24. Nuclear fueling by radiative avalanche induced by starbursts
Authors: Umemura M. , Fukue Jun , Mineshige Shin
Published: July 2016

Recently, as a solid physical mechanism which links circumnuclear starbursts to AGN fueling, Umemura, Fukue, & Mineshige (1997a) have proposed a radiative avalanche which is the black hole accretion driven by intensive radiation from circumnuclear starbursts of ≲ 100 pc.
3.30. Tridimensional spectroscopy of ionized gases surrounding the low luminosity Seyfert 2 nucleus of NGC2273
Authors: Hayashi T. , Ohtani H. , Sugai H. , Ishigaki T. , Ozaki S. , Hattori T. , Sasaki M. , Aoki K. , Yoshida M.
Published: July 2016

Seyfert galaxies often have extended emission line regions around their nucleus. We started an observation program of optical tridimensional spectroscopy for circumnuclear regions of nearby Seyfert galaxies to investigate the ionization source of the gas of just vicinity(typically several hundred pc) of nucleus.
3.31. Tri-dimensional observation of the superbubble in the starburst galaxy NGC 2782
Authors: Yoshida M.
Published: July 2016

We present results of an optical tri-dimensional observation of the central 2′ × 12″ region of the starburst galaxy NGC 2782. The circumnuclear Hα emission lines consist of broad (δv ~ 300 km s−1), blue-shifted component and narrow (δv < 100 km s−1) component and we first revealed the two-dimensional spatial distribution of those two components. The broad Hα emitting region is extended to 6″ (> 1 kpc) south from the nucleus and the emission-line ratios indicates that shock heating may be the main excitation mechanism of the ionized gas in the region. We conclude that this region is a superbubble outflowing from the nuclear starburst region.
4.2. The Galactic center region filled by molecular shells
Authors: Tsuboi Masato , Miyazaki Atsushi
Published: July 2016

The kinematics and structures of the molecular clouds probably give us key information for activities in the Galactic center region. CS lines are good tracers of dense molecular clouds. In addition, the lines are expected to be nearly free from the strong contamination of disk molecular clouds because of high critical density, n(H2) ≃ 104cm−3. Thus, we have made survey observations of the Galactic center region in the CS J=1-0 line with the Nobeyama 45-m telescope (Tsuboi, Handa, and Ukita 1997). The beamsize is 34″ and the achieved noise was Trms = 0.25 K/1.6 km s−1 in TMB. Then, we detected the molecular mass of M(H2)CS, thin = (3 − 8) × 107 M⊙ in the Galactic center molecular zone (CMZ), assuming of optically thin, Tex = 30 − 80 K (Güsten 1989), and X(CS) = 1 × 10−8 (Irvine et al. 1987).
4.4. The Sagittarius C region mapped in CS(2→1) and (3→2) by the IRAM 30m telescope
Authors: Kramer C. , Staguhn J. , Ungerechts H. , Sievers A.
Published: July 2016

We study the interaction of a dense giant molecular cloud with the HII region Sagittarius C, and a prominent nonthermal filament (NTF). For this purpose, we mapped the CS(2→1) and (3→2) transitions simultaneously with the IRAM 30m radio telescope, using the on-the-fly observing mode, and covering a 20pc×37pc (8′ × 15′) region. The high spatial resolution, 0.7pc (16″) at 147 GHz, allows for the first time to analyze in detail the morphology and kinematics of the molecular material and its relation to the ionized gas.
4.7. The CO 2–1/1–0 ratio in the disk and center of the Milky Way Galaxy
Authors: Hasegawa Tetsuo , Morino Jun-Ichi , Sawada Tsuyoshi , Handa Toshihiro , Sato Kumiko , Oka Tomoharu , Sakamoto Seiichi , Sorai Kazuo , Seta Masumichi , Hayashi Masahiko , Bronfman Leonardo , May Jorge , Booth Roy , Nyman Lars-Åke , Shaver Peter
Published: July 2016

We are conducting a survey of the CO J=2-1 line emission in the southern Milky Way (the Tokyo-Onsala-ESO-Calán Galactic CO survey), using the 60-cm radio telescope (VST2) in La Silla, Chile. It is combined with the northern survey made with the identical telescope (VST1) at Nobeyama (e.g., Sakamoto et al. 1995), and is directly comparable with the Columbia survey of the CO J=1-0 emission (e.g., Dame et al. 1987).
4.12. A molecular cloud interacting by the vertical filaments of the Galactic center radio arc
Authors: Oka Tomoharu , Hasegawa Tetsuo , Sato Fumio , Tsuboi Masato , Miyazaki Atsushi
Published: July 2016

Surely the most striking radio feature in the Galactic center may be a sheaf of straight vertical filaments (VFs, e.g., Yusef-Zadeh, Morris, & Chance 1984) of the radio arc. The VFs are believed to be the manifestations of strong magnetic field lines (≥1mG) which have been illuminated by some local relativistic particle source.
4.13. A high velocity molecular cloud near the center of the Galaxy
Authors: Oka Tomoharu , Hasegawa Tetsuo , White Glenn J. , Sato Fumio , Tsuboi Masato , Miyazaki Atsushi
Published: July 2016

Molecular clouds in the Galactic center region are characterised by their large velocity widths and physical conditions which differ from clouds in the Galactic disk (e.g., Morris 1996). These clouds may not be gravitationally bound, but in equilibrium with the high external pressure in the Galactic bulge (Spergel & Blitz 1992, Oka et al. 1997a).
5.6. Mapping the nucleus of NGC1068 in CO(2-1)
Authors: Baker A.J. , Scoville N.Z.
Published: July 2016

Molecular gas in active galactic nuclei (AGN) may play multiple roles: it can fuel a massive black hole, collimate jets, and/or obscure a broad-line region from most viewing angles. In order to understand the physical state and kinematics of molecular gas in AGN, we are using the Owens Valley Millimeter Array to map several nearby active galxies at high resolution in the CO(2–1) line. Our first target is NGC 1068, which hosts an obscured broad-line Seyfert nucleus as well as an extended starburst. We acquired data from 35 baselines out to 242 m, with 10.4 km s−1 resolution. After calibration with MMA (Scoville et al. 1992), we subtracted a 23 mJy nuclear continuum source from the visibility data and made CLEAN maps with AIPS. The resulting sensitivity in each line channel is 32 mJy per 1.8″ × 1.5″ robustly-weighted beam (1″ = 70 pc at 14.4 Mpc).
5.8. Molecular hydrogen emission from ultraluminous infrared galaxies
Authors: Van der Werf P.P.
Published: July 2016

Ultraluminous infrared galaxies (ULIRGs) are major mergers of gas-rich galaxies and are characterized by a molecular interstellar medium that is concentrated in the central kpc, where it forms a dynamically significant, or perhaps dominant, component (Scoville et al., 1991). Sanders et al. (1988) proposed that ULIRGs might harbour, or evolve into, dust-enshrouded quasars, formed in their obscured centers.
5.9. Gas dynamics in the central part of the Sy 1 galaxies: III Zw 2 and Mrk 817
Authors: Popović L. Č. , Vince I. , Kubičela A. , Salim S.
Published: July 2016

Spectra of Active Galactic Nuclei (AGN) indicate that in their central parts a composite motion of emission gas exists. An analysis of broad as well as narrow lines of active galaxies can give information about gas dynamics in central part of these objects (see e.g. Netzer 1990, Osterbrock 1990). Here we present the investigation of the Hβ and O III[4959,5007] line shapes of the two Sy 1 galaxis: Mrk 817 and III Zw2.
5.10. Peculiar CO distribution in active spiral galaxies: NCG4258 and Circinus
Authors: Krause M. , Neininger N. , Elmouttie M. , Jones K.L. , Haynes R.F.
Published: July 2016

NGC4258 and Circinus are both nearby spiral galaxies with active galactic nuclei which show high velocity water maser emission and Seyfert 2 characteristics. Both show radio emission perpendicular to the normal spiral arms which seem to be related to the nuclear activity (van der Kruit et al., 1972; Harnett et al., 1990). In NGC 4258 they coincide with the inner part of the rapidly rotating nuclear disk as expected for nuclear jets. Due to the strong misalignment of the nuclear disk plane with the galaxy's disk plane the jets pass the galactic disk. Molecular gas in NGC 4258 has only been detected in the nucleus and along the Hα jets up to a distance of 2 kpc from the nucleus (Krause et al., 1990).
5.11. Dense molecular gas in nearby galaxies
Authors: Gao Y. , Solomon P.M.
Published: July 2016

HCN, one of the most abundant high dipole-moment molecules (traces molecular gas at densities ≳ 3 × 104 cm−3 whereas CO traces at ∼ 500 cm−3), has only been detected in ∼ 25 galaxies, primarily towards the galactic nuclei (Solomon et al. 1992; Nguyen-Q-Rieu et al. 1992; Helfer & Blitz 1993; Aalto et al. 1995). Dense molecular gas properties in “normal” galactic disks, as compared to the centers of “normal” spirals, starbursts, and luminous IR galaxies are not clear. As part of a large HCN survey in 60 galaxies (Gao 1996; Gao & Solomon 1997), we present here HCN observations in central regions of a few nearby galaxies. HCN was mapped at least along the major axes in the inner disks to determine the total HCN luminosity, the distribution with radius of HCN emission, and of the surface brightness ratio of SBR ≡ IHCN/ICO.
5.12. High-resolution CO (1-0) observations of the ringed galaxy NGC 4736
Authors: Wong Tony , Helfer Tamara , Blitz Leo
Published: July 2016

It is well known that the radial distributions of atomic and molecular gas differ markedly in spiral galaxies, including our own (e.g. Burton & Gordon 1978, Sofue et al. 1995). We have recently begun a program to obtain multifrequency observations of several nearby galaxies in order to determine whether H I is needed to replenish the H2 consumed by star formation and, if so, how this might be accomplished. Here we present initial results on the nearby RSab galaxy NGC 4736, known for its bright ring of H II regions and recently shown to have a central stellar bar (Möllenhoff et al. 1995). We have mapped the distribution of CO (1-0) emission within r=1′ (1.8 kpc at D=6.2 Mpc) with the BIMA interferometer at ~5″ resolution, and added data from the NRAO 12-m telescope to recover zero-spacing information.
5.16. CO mapping of barred spiral galaxies
Authors: Kuno N. , Nakai N. , Nishiyama K. , Sorai K. , Handa T. , Iga T.
Published: July 2016

We have made CO mapping observations of nearby barred spiral galaxies (NGC253, NGC3504, NGC4303, NGC4321, NGC6951, M83) with the Nobeyama 45-m telescope using the 2×2 SIS focal-plane array receiver. The purpose of this project is to investigate distribution and kinematics of molecular gas in barred spiral galaxies and the relation between star formation and them. We present some of the results (NGC3504 and NGC6951).
5.19. A high resolution CO map of the inner region of M51
Authors: Aalto S. , Hüttemeister S. , Scoville N. , Thaddeus P.
Published: July 2016

M51, the Whirlpool Galaxy, at a distance of ≈ 9,6 Mpc and a systemic velocity of 465 km s−1, is the closest “Grand Design” spiral galaxy. Its low inclination (20°) makes it an excellent target for structural studies, e.g. the formation of arms in response to a spiral density wave causing gas streaming motions. We have obtained a high resolution, sensitive map of the inner 2.5′ of M51 using the Caltech six-element OVRO array. The map consists of a 19-field mosaic, taken using three different telescope configurations. The resolution is 2.5″, (corresponding to 115 pc linear size) and 3.5” for the robustly and naturally weigthed maps, respectively.
5.20. Molecular cloud properties in the barred galaxy NGC 7479
Authors: Aalto S. , Hüttemeister S. , Das M. , Wall W.F.
Published: July 2016

Bars are considered to be an important fueling mechanism for nuclear starburst activity, and are believed to be a dynamical result of gravitational interactions and merging. Furthermore, in a recent study, Das & Jog (1995) suggest that the dynamical impact of a bar will also have important consequences for cloud properties in the bar and nucleus. NGC 7479 is a barred galaxy with an unusually long and strong bar. At a distance of D=32 Mpc the bar length is ≈10 kpc. We selected NGC 7479 for a study of cloud properties in bars because of its proximity and because molecular gas is distributed along the whole length of the bar (e.g. Quillen et al. 1995).
6.2. Efficiency in nuclear fueling
Authors: Noguchi M.
Published: July 2016

Starburst phenomena in interacting and merging galaxies have been one of the most widely investigated subjects in today's galactic astronomy. On the theoretical side, a large body of numerical studies have been performed in order to interpret available observational data. Numerical simulations have been advanced to the point where they can include interstellar medium (ISM) and star formation process.
6.5. Hydrodynamical simulations as probes for the structure of the galactic center
Authors: Wada K. , Minezaki T. , Sakamoto K. , Fukuda H.
Published: July 2016

Numerical modeling of the interstellar gas in galaxies is an effective approach to infer galactic gravitational structure. This is because the dynamical behavior of gas is very sensitive to the background gravitational potential. Since the dynamical resonances depend closely on the mass distribution and the pattern speed of the non-axisymmetric component, it is possible to determine these dynamical parameters by comparison of numerical simulations and gas observations.
6.7. Dynamics of the asymetries at galactic centers
Authors: Masset F. , Tagger M.
Published: July 2016

Bars in galaxies are frequently found to be off-centered, so that the center of the bar does not coincide with the center of rotation, with a difference which typically amounts to several tens of parsecs. This is clearly seen in the distribution of the gas and the rotation curves at the center of the Milky Way, and in nearby barred galaxies (Blitz, these proceedings, and del Burgo et al., these proceedings).
6.12. Microlensing and dynamics of the Galactic bulge
Authors: Zhao H.S.
Published: July 2016

Microlensing (μ—lensing) towards the bulge started out as a unique technique of detecting dark objects in the Galactic disc (brown dwarfs) by measuring a rare transient brightening of one star among millions of stars in the Galactic bulge (Paczyński 1991). More than 200 events have been detected towards the Bulge since 1993 by the DUO, MACHO, OGLE etc. survey teams. But where are the lenses? Are they truly dark objects or merely faint stars? I show the results on the mass function, spatial distribution and dynamics of these observed lenses based on a dynamical model of the Galactic bar.
7.6. Dust composition, energetics, and morphology of the Galactic center
Authors: Chan Kin-Wing , Moseley S. H. , Casey S. , Harrington J. P. , Dwek E. , Loewenstein R. , Városi F. , Glaccum W.
Published: July 2016

Spectra at 16 - 45 μm of several regions within the central 80″ of the Galaxy have been obtained at 20″ resolution using the Goddard Cryogenic Grating Spectrometer No. 2 on the Kuiper Airborne Observatory. A broad band of excess emission extending from 24 to 45 μm is present in the spectra at positions covering the “tongue” and the inner edge of the circumnuclear disk. A similar dust emission feature has been observed in some carbon-rich evolved stars and in a nitrogen-rich evolved massive star. The observations reported here are the first detection of this dust emission feature in the interstellar medium. After considering several possible candidates of the carrier for this 30 μm dust feature, we find that MgS is the best owing to its good fit to the observed spectra. The origin of this ~ 30 μm feature in the Galactic center is unknown. Based on the theoretical results of dust condensation and elemental abundances in a supernova, we find that the supernovae in the central 500 pc could provide the amount of MgS dust, which we proposed as the carrier of the 30 μm dust feature, observed in the central 3 pc.
7.7. A search for [Ne II] 12.8 micron line emission from Galactic ultracompact H II regions
Authors: Matsuhara H. , Takahashi H. , Watarai H.
Published: July 2016

Starburst galaxies are powered by newly formed massive stars, and are heavily obscured by dust, prohibiting the UV and optical studies. A fine-structure line from Ne+ ion ([Ne II] 12.8 μm) is usually the brightest mid-infrared(MIR) line emitted from starburst galaxies. The [Ne II] line suffers from far less dust extinction than the optical line does, and hence it is often used as a probe for starburst properties of galaxies(Achtermann & Lacy, 1995; Roche et al., 1991). However, the [Ne II] line should not be used as the physical probe unless the relationship between Ne+ abundance and spectral type of the ionizing star is established for very dusty H II regions. To study this, we started the [Ne II] line survey toward dusty ultracompact(UC) H II regions in our Galaxy. The UC H II regions are powered by newly formed early-type stars whose spectral type can be inferred from their radio and far-infrared(FIR) properties.