DOCSLIB.ORG

中國天文學會 2006 年研討會論文摘要 Abstracts of CAST Symposium 2006

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

臺北天文館學報 JTAM Vol.4 中國天文學會 2006 年研討會論文摘要 Abstracts of CAST Symposium 2006 SMA Observations of Star Forming Regions [Oral 1-1] Sheng-Yuan Liu ASIAA The SMA Team Abstract The Submillimeter Array (SMA) located atop of Mauna Kea in Hawaii is a collaborative project of the Smithsonian Astrophysical Observatory (SAO) and the Academia Sinica Institute of Astronomy and Astrophysics (ASIAA). With its coverage over the submillimeter regime of the EM spectrum, the SMA best probes in high angular resolution the dense and warm material (including both gas and dust) particularly associated with the dynamical and often energetic processes in the formation of stars and planetary systems. This presentation gives recent results obtained with the SMA in the area of star formation. These studies covers phenomena associated with low- and high-mass young stellar objects such as dense cores, circumstellar disks, jet and outflows, as well as the complex chemical processes within. ASIAA-SMA Seyfert Survey [Oral 1-2] Matsushita, S. Inst. of Astronomy and Astrophysics, Academia Sinica, Taiwan ASIAA-SMA Extragalactic Group Abstract Seyfert activity is believed to be powered by a supermassive black hole, and the fuel for the activity is believed to be supplied from dusty disk/torus surrounding the supermassive black hole. In addition, a broadly accepted model (unified scheme) suggests that the type of the Seyfert (type 1 and 2) can be explained with the viewing angle of the circumnuclear dusty disk/torus (whether it obscures the supermassive black hole or not). Molecular gas in submillimeter-wave, such as higher-J CO lines, can trace warmer and denser molecular gas selectively, and therefore it is suitable to study the distributions, kinematics, and physical conditions of the circumnuclear disk/torus, and the relation between the Seyfert activities and also the large-scale strucutres. Here, we present the current status of the ASIAA-SMA Seyfert Survey. So far, we observed one Seyfert 1 galaxy and three Seyfert 2 galaxies. Most of the galaxies (three out of four) show possible molecular gas concentrations with rotating features at the nuclei, and multi-line CO studies show these central components are warm and dense. We will discuss more details in the talk. Instrumentation and Science with the CFHT [Oral 1-3] Jeremy Lim ASIAA Abstract Taiwan astronomers have access to the Canadian-France-Hawaii Telescope (CFHT) through participation in the Wide Field Infrared Camera (WIRCam) project. Here I give an overview of the telescope, focussing in particular on the instruments that are especially competitive or unique, and examples of the science being conducted with these instruments. I also briefly review the process of applying and allocating time on the telescope. The CFHT provides an opportunity to develop a broader optical/IR community in Taiwan, and we hope this review will encourage more Taiwan astronomers to conduct research with this telescope. - 45 - 中國天文學會 2006 年研討會論文摘要 Abstracts of CAST Symposium 2006 CFHT Megacam I and z Survey of DEEP2 Field [Oral 1-4] Hsieh, B. C. Inst. of Astronomy and Astrophysics, Academia Sinica, Taiwan Lin, Lihwai Inst. of Physics, National Taiwan Univ., Taiwan Abstract The photometric redshift technique is a good utility for extragalactic studies. However, the redshift limitations of most published photometric redshift catalogs are less than 0.7. Although there are few catalogs containing objects with redshift higher than 1.0, the templates for these photometric redshift estimations are inadequate to derive accurate photometric redshifts for high-z objects. The DEEP2 project provides tens of thousands spectroscopic redshifts up to z=1.5, which is an excellent template for the photometric redshift method to estimate the redshift at high-z. Therefore, we proposed the CFHT Megacam observation of DEEP2 field for filter i and z for 21 hours. By combining the data with the B, R, I observation of DEEP2 field, a photometric redshift catalog for DEEP2 field is generated. The catalog is ideal for studies of large scale structure, galaxy formation/evolution, and galaxy cluster/group/pair finding. In this talk, we will present the latest results of our studies. Iapetus and Enceladus as seen from Cassini [Oral 1-5] Wing-Huen Ip Inst. of Astronomy and Space Science, National Central Univ., Taiwan Wei-Ling Tseng Inst. of Astronomy, National Central Univ., Taiwan Lily Lin Inst. of Space Science, National Central Univ., Taiwan Jinnee Wang Inst. of Astronomy, National Central Univ., Taiwan Abstract While Titan remains to be the central focus of the Cassini-Huygens mission, two rising stars have been found. They are Iapetus and Enceladus, respectively. Iapetus is interesting because of the remarkable dichotomy in its surface brightness distribution with the albedo on the leading emisphere a factor of ten darker than the trailing hemisphere. The origin of such albedo asymmetry is still to be explained satisfactorily. But recent Cassini observations by the imaging SSI experiment onboard has shown that this medium-sized satellite (radius ~ 720 km) has a slightly ellipsoidal shape which might be indicative of an unusual tidal despinning history. In addition, Iapetus equator is lined up with a curious mountain ridge system probably as old as the satellite itself. The formation of this equatorial ridge system could be related to the tectonic process accompanying the tidal despinning or the collisional imprint of a primordial ring system. Iapetus is thus a representation of the satellite formation process in the days long gone. On the contrary, the small icy satellite Enceladus (radius ~ 250 km) displays an amazing level of outgassing activity. The recent Cassini SSI report of possible presence of liquid water on its surface is even more of a shock to planetary science. In this talk some of these interesting results will be summarized. AMiBA Science [Oral 2-1] Jiun-Huei Proty Wu Dept. of Phys. NTU, Taiwan Abstract The Array for Microwave Background Anisotropy (AMiBA) is a Taiwanese project to observe the Cosmic Microwave Background (CMB). It is led by a joint effort from the Academic Sinica Institute of Astronomy and Astrophysics (ASIAA) and the Institute of Astrophysics at National Taiwan University (IoAp, NTU). I will give an overview on the science goals of the project, with particular emphasis on the Sunyaev-Zel'dovich effect, the CMB polarization, and the cosmic strings. We expect the project to enhance not only our understanding of the universe, but also the competitiveness of Taiwan in the - 46 - 臺北天文館學報 JTAM Vol.4 international cosmology community. Ultra-Wideband Digital Correlator of Upgraded AMiBA [Oral 2-2] H.H. Li, S.K. Wong & T. Chiueh Institute of Astrophysics & Department of Physics, National Taiwan University Abstract In the upgraded AMiBA to begin operation in early 2007, the bandwidth will increase from 18Ghz to 35Ghz so as to compensate for the sensitivity loss of a 13-element array compared with the original 19-element array. In addition, to circumvent the 50% efficiency loss of analog correlation present in the current version of AMiBA due to its wide band, a world fastest digital correlator, able to process signals of 10Ghz bandwidth, is being developped. We report the design and progress of this digital correlator. SZ Effect from Secondary Electrons in Clusters of Galaxies [Oral 2-3] Hwang, Chorng-Yuan Graduate Institute of Astronomy, National Central University, Taiwan Abstract Secondary electrons will be produced in interactions between cosmic rays and thermal plasma. This process in galaxy clusters will continuously last longer than a Hubble time because the cosmic ray protons contained within the galaxy clusters have a lifetime longer than the age of the cluster. These secondary particles in the galaxy clusters will scatter the cosmic micro-wave background photons and produce a non-thermal SZ effect in addition to the thermal SZ effect caused by the thermal plasma in the clusters. We derive the non-thermal SZ effect from the secondary electrons under a variety of scenarios and discuss our findings in relation to observations. X-shaped sources: An unusual result at low radio frequency [Oral 2-4] Lal, D.V. Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan, R.O.C. Rao, A.P. National Centre for Radio Astrophysics, TIFR, Pune, India. Abstract Lal & Rao (2005) reported an unusual result for 3C~223.1, an X-shaped radio source, i.e., the wings (or the low-surface-brightness jets) have flatter spectral indices with respect to the high-surface-brightness (active) jets, using low frequency data from Giant Metrewave Radio Telescope (GMRT). This clearly shows the value of mapping the sample of X-shaped radio sources at low frequencies to understand the formation scenario of these sources. We have now obtained GMRT data for almost all of the X-shaped radio sources, performed in a uniform way. Here, we will present our results from the GMRT radio images at 240 and 610 MHz for these sources with an aim to test the formation models of these sources. Dynamical History of Galaxy Encounters [Oral 2-5] Sun, W.H. Institute of Astronomy, National Central University Abstract I will review the several cases of interacting galaxies in which low surface brightness extension around the galaxies and/or faint, diffuse emission have been detected. Multi-wavelength observations of these galaxies reveal the fact that often the diffuse emission are both gaseous and stellar in nature. By studying the spectral energy distributions of the stellar components and comparing to that of the member galaxies, - 47 - 中國天文學會 2006 年研討會論文摘要 Abstracts of CAST Symposium 2006 as we have done using the BATC archive, the origin of the scattered stars can be studied, which allows us to trace back and delineate the interacting process among the participating galaxies. Structure and Kinematics of CO 2-1 Emission in the Central Region of NGC4258 [Oral 2-6] Sawada-Satoh, S.
Recommended publications
  • Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1

    Aqueous Alteration on Main Belt Primitive Asteroids: Results from Visible Spectroscopy1

    Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 1 LESIA, Observatoire de Paris, CNRS, UPMC Univ Paris 06, Univ. Paris Diderot, 5 Place J. Janssen, 92195 Meudon Pricipal Cedex, France 2 Univ. Paris Diderot, Sorbonne Paris Cit´e, 4 rue Elsa Morante, 75205 Paris Cedex 13 3 Department of Physics and Astronomy of the University of Padova, Via Marzolo 8 35131 Padova, Italy Submitted to Icarus: November 2013, accepted on 28 January 2014 e-mail: [email protected]; fax: +33145077144; phone: +33145077746 Manuscript pages: 38; Figures: 13 ; Tables: 5 Running head: Aqueous alteration on primitive asteroids Send correspondence to: Sonia Fornasier LESIA-Observatoire de Paris arXiv:1402.0175v1 [astro-ph.EP] 2 Feb 2014 Batiment 17 5, Place Jules Janssen 92195 Meudon Cedex France e-mail: [email protected] 1Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 062.S-0173 and 064.S-0205 (PI M. Lazzarin) Preprint submitted to Elsevier September 27, 2018 fax: +33145077144 phone: +33145077746 2 Aqueous alteration on main belt primitive asteroids: results from visible spectroscopy1 S. Fornasier1,2, C. Lantz1,2, M.A. Barucci1, M. Lazzarin3 Abstract This work focuses on the study of the aqueous alteration process which acted in the main belt and produced hydrated minerals on the altered asteroids. Hydrated minerals have been found mainly on Mars surface, on main belt primitive asteroids and possibly also on few TNOs. These materials have been produced by hydration of pristine anhydrous silicates during the aqueous alteration process, that, to be active, needed the presence of liquid water under low temperature conditions (below 320 K) to chemically alter the minerals.
  • Cumulative Index to Volumes 1-45

    Cumulative Index to Volumes 1-45

    The Minor Planet Bulletin Cumulative Index 1 Table of Contents Tedesco, E. F. “Determination of the Index to Volume 1 (1974) Absolute Magnitude and Phase Index to Volume 1 (1974) ..................... 1 Coefficient of Minor Planet 887 Alinda” Index to Volume 2 (1975) ..................... 1 Chapman, C. R. “The Impossibility of 25-27. Index to Volume 3 (1976) ..................... 1 Observing Asteroid Surfaces” 17. Index to Volume 4 (1977) ..................... 2 Tedesco, E. F. “On the Brightnesses of Index to Volume 5 (1978) ..................... 2 Dunham, D. W. (Letter regarding 1 Ceres Asteroids” 3-9. Index to Volume 6 (1979) ..................... 3 occultation) 35. Index to Volume 7 (1980) ..................... 3 Wallentine, D. and Porter, A. Index to Volume 8 (1981) ..................... 3 Hodgson, R. G. “Useful Work on Minor “Opportunities for Visual Photometry of Index to Volume 9 (1982) ..................... 4 Planets” 1-4. Selected Minor Planets, April - June Index to Volume 10 (1983) ................... 4 1975” 31-33. Index to Volume 11 (1984) ................... 4 Hodgson, R. G. “Implications of Recent Index to Volume 12 (1985) ................... 4 Diameter and Mass Determinations of Welch, D., Binzel, R., and Patterson, J. Comprehensive Index to Volumes 1-12 5 Ceres” 24-28. “The Rotation Period of 18 Melpomene” Index to Volume 13 (1986) ................... 5 20-21. Hodgson, R. G. “Minor Planet Work for Index to Volume 14 (1987) ................... 5 Smaller Observatories” 30-35. Index to Volume 15 (1988) ................... 6 Index to Volume 3 (1976) Index to Volume 16 (1989) ................... 6 Hodgson, R. G. “Observations of 887 Index to Volume 17 (1990) ................... 6 Alinda” 36-37. Chapman, C. R. “Close Approach Index to Volume 18 (1991) ..................
  • The Minor Planet Bulletin (Warner Et Al., 2015)

    The Minor Planet Bulletin (Warner Et Al., 2015)

    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 42, NUMBER 3, A.D. 2015 JULY-SEPTEMBER 155. ROTATION PERIOD DETERMINATION period lightcurve with a most likely value of 30.7 days (737 FOR 1220 CROCUS hours). He noted that periods of 20.47 and 15.35 days (491 hours and 368 hours, respectively) were also compatible with his data. Frederick Pilcher His lightcurves of 1984 Feb 7-9 showed a second period of 7.90 Organ Mesa Observatory hours with an amplitude 0.15 magnitudes. Jacobson and Scheeres 4438 Organ Mesa Loop (2011) describe how, following rotational spin-up and fissioning, Las Cruces, NM 88011 USA an asteroid binary system can evolve by angular momentum [email protected] transfer into a system in which the primary acquires a long rotation period and the satellite has a long orbital revolution period around Vladimir Benishek the primary and short rotation period. Warner et al. (2015) list Belgrade Astronomical Observatory 1220 Crocus as one of eight systems in which a slowly rotating Volgina 7, 11060 Belgrade 38, SERBIA primary may have a satellite. The several authors of this paper agreed to collaborate in a search to confirm the existence of the Lorenzo Franco short period and obtain a reliable value for the large amplitude Balzaretto Observatory (A81), Rome, ITALY long period. A. W. Harris Observers Vladimir Benishek at Sopot Observatory, Lorenzo More Data! Franco at Balzaretto Observatory, Daniel Klinglesmith III and La Canada, CA USA Jesse Hanowell at Etscorn Campus Observatory, Caroline Odden and colleagues at Phillips Academy Observatory, and Frederick Daniel A.
  • The Minor Planet Bulletin It Would Be Very Helpful to Have Clearly More Realistic Period

    The Minor Planet Bulletin It Would Be Very Helpful to Have Clearly More Realistic Period

    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 34, NUMBER 1, A.D. 2007 JANUARY-MARCH 1. A ROTATION PERIOD FOR 1493 SIGRID -0.2 Colin Bembrick 1493 SIGRID Mt Tarana Observatory -0.1 PO Box 1537, Bathurst, NSW, Australia 0 [email protected] 0.1 Jeff Byron 0.2 Cecil Sayers Observatory 22-Jul 0.3 18 Albuera Rd, Epping, NSW, Australia 26-Jul 27-Jul 0.4 29-Jul (Received: 9 October Revised: 30 October) 1-Aug 0.5 6-Aug 7-Aug 0.6 22-Aug Minor planet 1493 Sigrid was observed over 8 nights in 0.7 2006. The synodic period was found to be 0.0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1.0 43.296±0.048hr with a peak-to-peak amplitude of at least 0.6 magnitudes. The axial ratio a/b implied by the peak to peak variation is 1.74. compared with most asteroids of less than 50km diameter, which have mean rotation rates of 2-3 revs/day (Binzel et al, 1989). Minor planet 1493 Sigrid was observed over a period of 32 days References from two sites in NSW, Australia, Mt Tarana Observatory (S 33d 26.1m E 149d 45.4m +880m) and Cecil Sayers Observa- Barbera, R. (2004). “AVE” Analisis de Variabilidad Estelar, tory (S 33d 46.9m E 151d 05.1m +80m). The Cecil Sayers version 2.51. Grup d’Estudis Astronomics.
  • The British Astronomical Association Handbook 2016

    The British Astronomical Association Handbook 2016

    THE HANDBOOK OF THE BRITISH ASTRONOMICAL ASSOCIATION 2016 2015 October ISSN 0068–130–X CONTENTS CALENDAR 2016 . 2 PREFACE . 3 HIGHLIGHTS FOR 2016 . 4 SKY DIARY . .. 5 VISIBILITY OF PLANETS . 6 RISING AND SETTING OF THE PLANETS IN LATITUDES 52°N AND 35°S . 7-8 ECLIPSES . 9-15 TIME . 16-17 EARTH . 18 SUN . 19-21 LUNAR LIBRATION . 22 MOON . 23 MOONRISE AND MOONSET . 24-27 SUN’S SELENOGRAPHIC COLONGITUDE . 28 LUNAR OCCULTATIONS . 29-35 GRAZING LUNAR OCCULTATIONS . 36-37 APPEARANCE OF PLANETS . 38 MERCURY . 39-40 VENUS . 41 MARS . 42-43 ASTEROIDS . 44-49 ASTEROID OCCULTATIONS .. 50-53 ASTEROIDS: FAVOURABLE OBSERVING OPPORTUNITIES . 54-56 NEO CLOSE APPROACHES TO EARTH . 57 JUPITER . .. 58-62 SATELLITES OF JUPITER . 62-66 JUPITER ECLIPSES, OCCULTATIONS AND TRANSITS . 67-76 SATURN . 77-80 SATELLITES OF SATURN . 81-84 URANUS . 85 NEPTUNE . 86 TRANS–NEPTUNIAN & SCATTERED DISK OBJECTS . 87 DWARF PLANETS . 88-91 COMETS . 92-96 METEOR DIARY . 97-99 VARIABLE STARS (RZ Cassiopeiae; Algol; λ Tauri) . 100-101 MIRA STARS . 102 VARIABLE STAR OF THE YEAR (Z Andromedæ) . .. 103-105 EPHEMERIDES OF VISUAL BINARY STARS . 106-107 BRIGHT STARS . 108 ACTIVE GALAXIES . 109 PLANETS – EXPLANATION OF TABLES . 110 ELEMENTS OF PLANETARY ORBITS . 111 ASTRONOMICAL AND PHYSICAL CONSTANTS . 112-113 INTERNET RESOURCES . 114-115 GREEK ALPHABET . 115 ACKNOWLEDGEMENTS / ERRATA . 116 Front Cover: The previous Transit of Mercury - as taken through a Hydrogen Alpha telescope on 08 November 2006 at 08:19-22UT (D.C.Parker) British Astronomical Association HANDBOOK FOR 2016 NINETY–FIFTH
  • Proceedings of Ceres 2001 Workshop

    Proceedings of Ceres 2001 Workshop

    Proceedings of Ceres 2001 Workshop October 9-12, 2001 Paris, France Institut de Mécanique Céleste et de Calcul des Ephémérides Observatoire de Paris Dépôt légal : février 2004 ISBN : 2-91015-43-2 © IMC Editions Foreword You will find herewith the proceedings of the workshop Ceres 2001 organized in honour of the bicentenary of the discovery of Ceres by Piazzi and dedicated to astrometry and physics of asteroids thanks to observational networks. We are glad to present here these proceedings : the contributions of the participants covered all the topics of the workshop. They deal with celestial mechanics and physics of the asteroids and also with theoretical and observational studies. The progress of our knowledge on aste- roids needs to investigate simultaneously these topics. The efficiency of the observational networks has been put into light and the need of an improved astrometric accuracy was demonstrated as a necessary step for new discoveries. The determination of the masses of the asteroids, the interpretation of the observations of occultations, will be improved thanks to high accurate astrometric observations, together with photometric measurements. Then we will be able to reach information on what are the asteroids and what are the composition and the evolution of the solar system. We hope that discussions have been helpful for the participants and that collaborations have started among them. 3 Acknowledgements We wish to thank here all of those who contributed to the success of the workshop, and in particular the scientific organizing committee and the local organizing committee : Mrs Baron, Derouazi, Martinez, Raoult, Simon, MM. Mulo, Renaudineau, Vaubaillon for the organization of the meeting and Mrs S.