Scientific role of ACA for low-mass star-formation study     

Shigehisa Takakuwa  Daisuke Iono  Baltasar Vila-Vilaro  Tomohiko Sekiguchi  Ryohei Kawabe 《Astrophysics and Space Science》2008,313(1-3):169-173

We discuss the scientific role of the Atacama Compact Array (ACA), the Japanese contribution to the ALMA project, for low-mass star-formation study. Our recent observations of several low-mass protostellar envelopes in the submillimeter CS (J=7–6) and HCN (J=4–3) lines with the SMA and ASTE have revealed that these submillimeter emissions are more extended than ∼2000 AU and show different velocity structures from those traced by millimeter lines. These results suggest the importance of taking short-spacing informations the ACA can offer. Our comprehensive imaging simulations of these protostellar envelopes, as well as prestellar cores and debris disks, unprecedentedly demonstrate the scientific importance of ACA.  相似文献   

Ambient air measurements of six bifunctional carbonyls in a suburban area     

Ricardo Ortiz  Hiroyuki Hagino  Kazuhiko Sekiguchi  Qingyue Wang  Kazuhiko Sakamoto   《Atmospheric Research》2006,82(3-4):709

Low-molecular-weight carbonyl compounds, generated by photochemical reactions in the atmosphere and found in the exhaust of motor vehicles, have recently come to the attention of researchers because some of them are suspected carcinogens or mutagens. Six bifunctional carbonyl compounds were detected and measured in a suburban site 30 km northwest of the Tokyo metropolitan area. Samples were taken on five sunny days between 2 August and 11 August 2003 with a low-volume denuder and three-filter tandem system using O-(2,3,4,5,6-pentafluorobenzyl)hydroxylamine (PFBHA) as a sorbent. Bifunctional carbonyls were measured by gas chromatography–mass spectrometry after two derivatization processes with PFBHA and N,O-bis(trimethylsilyl)-trifluoroacetamide (BSTFA). The average total (gas plus particle) concentrations were 162.8 ng m^− 3 for pyruvic acid, 113.7 ng m^− 3 for methylglyoxal, 36.0 ng m^− 3 for glycolaldehyde and 58.6 ng m^− 3 for glyoxal.  相似文献   

Virtual velocity of sand transport in water          下载免费PDF全文

Anthony John Parsons  James Cooper  John Wainwright  Tomohiro Sekiguchi 《地球表面变化过程与地形》2018,43(3):755-761

Using the 160‐m‐long flume at Tsukuba University we undertook an experiment to provide a first estimate of the virtual velocity of sand in the size range 0.5–2.0 mm. For the flow velocity used in our experiment this sediment‐size range would conventionally be regarded as suspended sediment. The virtual velocity was found to be 37–41% of the flow velocity. Paradoxically, virtual velocity decreases as particle size decreases. Such a lower virtual velocity of finer sediment is not inconceivable. First, trapping of the sediment appears to be a function of bed roughness, and there is a probable relationship between bed roughness and trapping efficiency for particles of different sizes. Second, finer particles are more likely to find sheltered positions on a rough bed and thus experience lower mobility, relative to the more exposed coarser grains, as observed for bedload transport. Third, the virtual velocity of particles undergoing bedload transport has been found, in some instances, to be lower for finer clasts. We combine our data with previous studies of virtual velocity of bedload to develop, for the first time, a hypothesis for a holistic analysis of sediment movement in rivers. Copyright © 2017 John Wiley & Sons, Ltd.  相似文献   

Probing the evolution of early-type galaxies using multicolour number counts and redshift distributions     

Fumiaki Nakata  Kazuhiro Shimasaku  Mamoru Doi  Nobunari Kashikawa  Wataru Kawasaki  Yutaka Komiyama  Sadanori Okamura  Maki Sekiguchi  Masafumi Yagi  Naoki Yasuda 《Monthly notices of the Royal Astronomical Society》1999,309(4):L25-L29

We investigate pure luminosity evolution models for early-type (elliptical and S0) galaxies (i.e. no number density change or morphological transition), and examine whether these models are consistent with observed number counts in the B , I and K bands, and redshift distributions of two samples of faint galaxies selected in the I and K bands. The models are characterized by the star formation time-scale τ _SF and the time t _gw when the galactic wind starts to blow, in addition to several other conventional parameters. We find that the single-burst model ( τ _SF=0.1 Gyr and t _gw=0.353 Gyr), which is known to reproduce the photometric properties of early-type galaxies in clusters, is inconsistent with the redshift distributions of early-type galaxies in the field environment, owing to overpredictions of the number of galaxies at z ≳1.4 even with strong extinction which is at work until t _gw. In order for dust extinction to be more effective, we treat τ _SF and t _gw as free parameters, and find that models with τ _SF≳0.5 Gyr and t _gw>1.0 Gyr can be made consistent with both the observed redshift distributions and the number counts, if we introduce strong extinction [ E ( B − V )≥1 as a peak value]. These results suggest that early-type galaxies in the field environment do not have the same evolutionary history as described by the single-burst model.  相似文献   

Large-scale structure of galaxies in the Ophiuchus region     

Takashi Hasegawa  †  Ken-ichi Wakamatsu  ‡  Matthew Malkan  ‡  Kazuhiro Sekiguchi  John W. Menzies  Quentin A. Parker  Jun Jugaku  Hiroshi Karoji  Sadanori Okamura 《Monthly notices of the Royal Astronomical Society》2000,316(2):326-344

The large-scale structure around the Ophiuchus cluster of galaxies in the vicinity of the Galactic Centre ( l =05, b =95, cz =8500 km s⁻¹) is investigated on the basis of a galaxy survey and spectroscopic observations made for a 12°×17° area. The galaxy survey was performed using six ESO/SERC Sky Survey Atlas films, and 4021 galaxies were detected in total. Recession velocities were newly obtained for 179 galaxies to make the total number of galaxies in the survey area with known velocities 219.
In the distribution of bright galaxies, we identified seven new clumps of galaxies. Comparing the surface number density of bright galaxies with the Galactic extinction, which is estimated from the 100‐μm flux density in the IRAS Sky Survey Atlas, we demonstrate that the seven clumps are not spurious as a result of the inhomogeneity of the Galactic extinction. Among the seven clumps, two are found to be clusters and four to be groups on the basis of the histogram of recession velocities and the number of member galaxies. The Ophiuchus cluster, two newly identified clusters, and four groups are all concentrated at 9000 km s⁻¹. Field galaxies are also distributed centred at 8500 km s⁻¹. Hence field galaxies occupy a common three-dimensional region with galaxies in the clusters and groups, and altogether they form a large-scale structure of supercluster size. As opposed to the overdensity in the supercluster region, the mean number density of galaxies in the velocity range 0–5000 km s⁻¹ is only 25 per cent of the mean number density of the Universe, comparable with the density of the well-known Böotes void. Hence this nearby three-dimensional region in Ophiuchus is a void of galaxies also.  相似文献   

A unified model for bedform development and equilibrium under unidirectional,oscillatory and combined‐flows     

Mauricio M. Perillo  James L. Best  Miwa Yokokawa  Tomohiro Sekiguchi  Tomohiro Takagawa  Marcelo H. Garcia 《Sedimentology》2014,61(7):2063-2085

The development of bedforms under unidirectional, oscillatory and combined‐flows results from temporal changes in sediment transport, flow and morphological response. In such flows, the bedform characteristics (for example, height, wavelength and shape) change over time, from their initiation to equilibrium with the imposed conditions, even if the flow conditions remain unchanged. These variations in bedform morphology during development are reflected in the sedimentary structures preserved in the rock record. Hence, understanding the time and morphological development in which bedforms evolve to an equilibrium stage is critical for informed reconstruction of the ancient sedimentary record. This article presents results from a laboratory flume study on bedform development and equilibrium development time conducted under purely unidirectional, purely oscillatory and combined‐flow conditions, which aimed to test and extend an empirical model developed in past work solely for unidirectional ripples. The present results yield a unified model for bedform development and equilibrium under unidirectional, oscillatory and combined‐flows. The experimental results show that the processes of bedform genesis and growth are common to all types of flows, and can be characterized into four stages: (i) incipient bedforms; (ii) growing bedforms; (iii) stabilizing bedforms; and (iv) fully developed bedforms. Furthermore, the development path of bedform; growth exhibits the same general trend for different flow types (for example, unidirectional, oscillatory and combined‐flows), bedform size (for example, small versus large ripples), bedform shape (for example, symmetrical or rounded), bedform planform geometry (for example, two‐dimensional versus three‐dimensional), flow velocities and sediment grain sizes. The equilibrium time for a wide range of bed configurations was determined and found to be inversely proportional to the sediment transport flux occurring for that flow condition.  相似文献   

Rocket observations of atomic oxygen density and airglow emission rate in the WAVE2000 campaign     

N. Iwagami  T. Shibaki  T. Suzuki  H. Sekiguchi  N. Takegawa  W. H. Morrow 《Journal of Atmospheric and Solar》2003,65(16-18):1349-1360

Atomic oxygen density and airglow volume emission rate profiles measured in the rocket experiment S-310-29 carried out as a part of the Waves in Airglow Structures Experiment over Kagoshima in 2000 (WAVE2000) campaign are presented, and the excitation processes of the atomic oxygen 557.7 nm line and the molecular oxygen atmospheric band airglow emissions are discussed. The volume emission rate profiles calculated from the measured atomic oxygen densities using the methods and parameters proposed by the ETON campaign (EATON model) are found to well represent the shapes of measured twin-peak emission rate profiles seen during this campaign suggesting that the EATON model is valid for a perturbed atmosphere. There is some discrepancy in the modeled absolute values for the emissions. Applying the model to the current O density measurements results in predicted emission rates that are a factor of 3.2 and 1.5 too high for the 557.7 nm line and Atmospheric band, respectively. This suggests either that the atomic oxygen densities of the present campaign are too large by a factor of 1.2 (=1.5^1/2) to 1.5 (=3.2^1/3), or that those of the ETON campaign were too small by the same factor or that the combined errors in both campaigns can account for the discrepancy (the modeled volume emission rates of the 557.7 nm line and atmospheric band are roughly in proportion to [O]³ and [O]², respectively). Our present data findings do not favor the 2-step more than the 1-step excitation process for the atmospheric band because a calculation of the quantum efficiency based on the observed O density does not show a steep gradient around 100 km.  相似文献   

Study of variable stars in the MOA data base: long-period red variables in the Large Magellanic Cloud – II. Multiplicity of the period–luminosity relation     

S. Noda  M. Takeuti  F. Abe  I. A. Bond  R. J. Dodd  J. B. Hearnshaw  M. Honda  M. Honma  J. Jugaku  Y. Kan-ya  Y. Kato  P. M. Kilmartin  Y. Matsubara  K. Masuda  Y. Muraki  T. Nakamura  K. Ohnishi  M. Reid  N. J. Rattenbury  To. Saito  Y. Saito  H. Sato  M. Sekiguchi  J. Skuljan  D. J. Sullivan  T. Sumi  R. Yamada  T. Yanagisawa  P. C. M. Yock  M. Yoshizawa 《Monthly notices of the Royal Astronomical Society》2004,348(4):1120-1134

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Wide Field Imaging of Ion Tail of Comet C/Hale–Bopp     

Kinoshita  D.  Watanabe  J.  Fukushima  H.  Sekiguchi  T.  Yamamoto  N.  Abe  S. 《Earth, Moon, and Planets》1997,77(3):265-269

A sequential imaging observation of the ion tail of Comet C/Hale-Bopp 1995O1 was carried out in February–March 1997 with a wide-field CCD imaging camera using narrow band filters for two ion species; CO⁺ and H₂O⁺ along with those for blue and red continuum. From the surface photometry of the ion tail of two species, we derived a relationship between plasma density and distance from the nucleus. The local velocity of the ion flow as a function of the distance from the nucleus was also estimated on the basis of some assumptions. We report preliminary results of our analysis, and discuss some characteristics of cometary plasma and its interaction with interplanetary magnetic field (IMF). May the source be with you! This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

A medium-deep Chandra and Subaru survey of the 13-h XMM/ROSAT deep survey area     

I. M. MHardy  K. F. Gunn  A. M. Newsam  K. O. Mason  M. J. Page  T. Takata  K. Sekiguchi  T. Sasseen  F. Cordova  L. R. Jones  N. Loaring 《Monthly notices of the Royal Astronomical Society》2003,342(3):802-822

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