Structural Comparisons of the Semantic Interface of the Top Cosmetic Brands on the Web by Network Analysis

Web presentations of consumer products serve as an interface between businesses and consumers. The present paperfocused on the verbal information on the webs of the top two skincare brands in Japan. Term by context matrices createdfrom the texts were truncated by SVD to construct graphs that represented high similarities among terms. In pursuit ofessential terms and the networks surrounding them, the primary clusters were decomposed in to communities in whichthe core nodes and their neighborhoods were identified. Though the brands differed greatly in concentrations of clusters,communities and neighborhoods, they showed similarities in the properties of cores. Of particular interest was the coreterm "plump" that appeared in both brands. Probably, this reflected the shared business awareness of the central concernabout skincare among the Japanese consumers. In lieu of conclusions, our plan of further inquiries were stated

Molecular clouds towards RCW 49 and Westerlund 2; Evidence for cluster formation triggered by cloud-cloud collision

We have made CO(J=2-1) observations towards the HII region RCW 49 and its ionizing source, the rich stellar cluster Westerlund 2 (hereafter Wd2), with the NANTEN2 sub-mm telescope. These observations have revealed that two molecular clouds in velocity ranges of -11 to +9 km/s and 11 to 21 km/s respectively, show remarkably good spatial correlations with the Spitzer IRAC mid-infrared image of RCW 49, as well a velocity structures indicative of localized expansion around the bright central regions and stellar cluster. This strongly argues that the two clouds are physically associated with RCW 49. We obtain a new kinematic distance estimate to RCW 49 and Wd2 of 5.4^{+ 1.1}_{- 1.4} kpc, based on the mean velocity and velocity spread of the associated gas. We argue that acceleration of the gas by stellar winds from Wd2 is insufficient to explain the entire observed velocity dispersion of the molecular gas, and suggest a scenario in which a collision between the two clouds ~4 Myrs ago may have triggered the formation of the stellar cluster.Comment: A version with higher resolution figures is available from http://www.a.phys.nagoya-u.ac.jp/~naoko/research/apjl2009/fur09_rev_highreso.pd

A Detailed Observational Study of Molecular Loops 1 and 2 in the Galactic Center

Fukui et al. (2006) discovered two huge molecular loops in the Galactic center located in (l, b) ~ (355 deg-359 deg, 0 deg-2 deg) in a large velocity range of -180-40 km s^-1. Following the discovery, we present detailed observational properties of the two loops based on NANTEN 12CO(J=1-0) and 13CO(J=1-0) datasets at 10 pc resolution including a complete set of velocity channel distributions and comparisons with HI and dust emissions as well as with the other broad molecular features. We find new features on smaller scales in the loops including helical distributions in the loop tops and vertical spurs. The loops have counterparts of the HI gas indicating that the loops include atomic gas. The IRAS far infrared emission is also associated with the loops and was used to derive an X-factor of 0.7(+/-0.1){\times}10^20 cm^-2 (K km s^-1)^-1 to convert the 12CO intensity into the total molecular hydrogen column density. From the 12CO, 13CO, H I and dust datasets we estimated the total mass of loops 1 and 2 to be ~1.4 {\times} 106 Msun and ~1.9 {\times} 10^6 Msun, respectively, where the H I mass corresponds to ~10-20% of the total mass and the total kinetic energy of the two loops to be ~10^52 ergs. An analysis of the kinematics of the loops yields that the loops are rotating at ~47 km s-1 and expanding at ~141 km s^-1 at a radius of 670 pc from the center. Fukui et al. (2006) presented a model that the loops are created by the magnetic flotation due to the Parker instability with an estimated magnetic field strength of ~150 {\mu}G. We present comparisons with the recent numerical simulations of the magnetized nuclear disk by Machida et al. (2009) and Takahashi et al. (2009) and show that the theoretical results are in good agreements with the observations. The helical distributions also suggest that some magnetic instability plays a role similarly to the solar helical features.Comment: 40 pages, 22 figures, submitted to publication in PAS

Discovery of Molecular Loop 3 in the Galactic Center: Evidence for a Positive-Velocity Magnetically Floated Loop towards L=355∘−359∘L=355^\circ-359^\circ

We have discovered a molecular dome-like feature towards $355^{\circ} \leq l \leq 359^{\circ}$ and $0^{\circ} \leq b \leq 2^{\circ}$. The large velocity dispersions of 50--100 km s$^{-1}$ of this feature are much larger than those in the Galactic disk and indicate that the feature is located in the Galactic center, probably within $\sim1$ kpc of Sgr A$^{*}$. The distribution has a projected length of $\sim600$ pc and height of $\sim300$ pc from the Galactic disk and shows a large-scale monotonic velocity gradient of $\sim130$ km s $^{-1}$ per $\sim600$ pc. The feature is also associated with HI gas having a more continuous spatial and velocity distribution than that of $^{12}$CO. We interpret the feature as a magnetically floated loop similar to loops 1 and 2 and name it "loop 3". Loop 3 is similar to loops 1 and 2 in its height and length but is different from loops 1 and 2 in that the inner part of loop 3 is filled with molecular emission. We have identified two foot points at the both ends of loop 3. HI, $^{12}$CO and $^{13}$CO datasets were used to estimate the total mass and kinetic energy of loop 3 to be \sim3.0 \times 10^{6} \Mo and $\sim1.7 \times 10^{52}$ ergs. The huge size, velocity dispersions and energy are consistent with the magnetic origin the Parker instability as in case of loops 1 and 2 but is difficult to be explained by multiple stellar explosions. We argue that loop 3 is in an earlier evolutionary phase than loops 1 and 2 based on the inner-filled morphology and the relative weakness of the foot points. This discovery indicates that the western part of the nuclear gas disk of $\sim1$ kpc radius is dominated by the three well-developed magnetically floated loops and suggests that the dynamics of the nuclear gas disk is strongly affected by the magnetic instabilities.Comment: 30 pages, 10 figures. High resolution figures are available at http://www.a.phys.nagoya-u.ac.jp/~motosuji/fujishita09_figs

The Second Survey of the Molecular Clouds in the Large Magellanic Cloud by NANTEN I: Catalog of Molecular Clouds

The second survey of the molecular clouds in 12CO (J = 1-0) was carried out in the Large Magellanic Cloud by NANTEN. The sensitivity of this survey is twice as high as that of the previous NANTEN survey, leading to a detection of molecular clouds with M_CO > 2 x 10^4 M_sun. We identified 272 molecular clouds, 230 of which are detected at three or more observed positions. We derived the physical properties, such as size, line width, virial mass, of the 164 GMCs which have an extent more than the beam size of NANTEN in both the major and minor axes. The CO luminosity and virial mass of the clouds show a good correlation of M_VIR propto L_CO^{1.1 +- 0.1} with a Spearman rank correlation of 0.8 suggesting that the clouds are in nearly virial equilibrium. Assuming the clouds are in virial equilibrium, we derived an X_CO-factor to be ~ 7 x 10^20 cm^-2 (K km s^-1)^-1. The mass spectrum of the clouds is fitted well by a power law of N_cloud(>M_CO) proportional to M_CO^{-0.75 +- 0.06} above the completeness limit of 5 x 10^4 M_sun. The slope of the mass spectrum becomes steeper if we fit only the massive clouds; e.g., N_cloud (>M_CO) is proportional to M_CO^{-1.2 +- 0.2} for M_CO > 3 x 10^5 M_sun.Comment: 54 pages in total, 18 figures (21 files) and 4 tables, to appear in Astrophysical Journal Supplement Series. A full color version with higher resolution figures is available at http://www.a.phys.nagoya-u.ac.jp/~kawamura/research/NANTEN_LMC_1_preprint_highres.pd

The Second Survey of the Molecular Clouds in the Large Magellanic Cloud by NANTEN. II. Star Formation

We studied star formation activities in the molecular clouds in the Large Magellanic Cloud. We have utilized the second catalog of 272 molecular clouds obtained by NANTEN to compare the cloud distribution with signatures of massive star formation including stellar clusters, and optical and radio HII regions. We find that the molecular clouds are classified into three types according to the activities of massive star formation; Type I shows no signature of massive star formation, Type II is associated with relatively small HII region(s) and Type III with both HII region(s) and young stellar cluster(s). The radio continuum sources were used to confirm that Type I GMCs do not host optically hidden HII regions. These signatures of massive star formation show a good spatial correlation with the molecular clouds in a sense they are located within ~100 pc of the molecular clouds. Among possible ideas to explain the GMC Types, we favor that the Types indicate an evolutionary sequence; i.e., the youngest phase is Type I, followed by Type II and the last phase is Type III, where the most active star formation takes place leading to cloud dispersal. The number of the three types of GMCs should be proportional to the time scale of each evolutionary stage if a steady state of massive star and cluster formation is a good approximation. By adopting the time scale of the youngest stellar clusters, 10 Myrs, we roughly estimate the timescales of Types I, II and III to be 6 Myrs, 13 Myrs and 7 Myrs, respectively, corresponding to a lifetime of 20-30 Myrs for the GMCs with a mass above the completeness limit, 5 x 10^4 Msun.Comment: accepted to the Astrophysical Journal Supplement Series. 20 figures and 4 tables. Higher resolution color PDF is found at http://www.a.phys.nagoya-u.ac.jp/~kawamura/research/NANTEN_LMC_2_preprint.pdf (47 pages,32MB

アサガオ ノ カンサツ カラ マナベル コト ショウガクセイ ノ カンサツ キロク オ リカ ノ ガクシュウ ニイカス

小学生によるアサガオの観察記録を理科の学習に活用するため， 科学的活動や後で学ぶこととの繋がりといった視点で分析した． 測定・ナンバリング・観察の視点の変更・内部構造を観察するための操作・原因の考察といった科学の営みが， 簡単な方法ながら行われていた． さらに， 植物の一生を通して観察されているため， 植物の構造や機能や生き方など， 高学年や中学生以降に学ぶ内容との繋がりもあり， 低学年での観察記録を， 後々， 理科の学習に活用できる可能性もある

イノチ ノ ナカマド アンケート ニ ミル ダイガクセイ ノ セイブツカン ト セイブツ キョウイク ノ カダイ

大学生の生物観を掴み，特に小学校教師や保育士を目指している大学生に対する生物教育の課題を考えるために，「命の仲間度アンケート」 を実施した．それぞれの生物に対して，命あるものとして自分の仲間と感じる度合いを，ヒトを 100 として 0 から 100 までの数値で記入してもらい，併せて，命のあるものとはどんなものだと思うかと質問したものである．仲間度をそれぞれの生物ごと，生物の自然分類群ごと，あるいは人為分類群ごとに集計した．また，同時に実施した 「食べものと生物アンケート」 では，食べたものの原材料が生物に由来するか否かで分類することを試みたところ，生物由来のものをそうではないとした人たち （A 群） と水と塩以外は生物とした人たち （B 群） とはほぼ半数ずついたが，A 群は B 群に比べて，すべての分類群で仲間度が低かった．これらを分析し，生物教育の課題について考察した．To consider the problems in biological education for college students, I investigated their degree of affinity for a variety of organisms. The samples of degree of affinity were analyzed according to each student, organism, or group of natural and artificial classification. In addition, I asked students to classify raw materials used in preparing food on the basis of whether or not the materials are obtained from organisms. Half the students did not classify vegetables and grains as materials obtained from organisms. This half was found to be lower in the degree of affinity for a variety of organisms in comparison with the other half

ショクブツ オ イキテイル ト オモエル ニハ ダイガクセイ ノ セイブツカン カラ カンガエル セイブツ キョウイク ノ カダイ

植物を生物と思えるようになるには， 生物教育として何が重要かを探るため， 昨年度 （水野 2013） と同じように 「命の仲間度アンケート」 と 「食べものと生物アンケート」 を実施した． 今年度は， 約 3 分の 2 の学生たちが， 食べものの原材料である植物を生物と思っていなかった． しかし， それらの学生たちも植物の構造や機能についての知識は， 植物を生物と思った学生たちと違いがみられなかった． また， 小学校から高校までの過程で， 全員， 授業の一環として植物を栽培した経験があった． 植物栽培の体験もあり知識もあるのに， 植物を生物と思えていない学生が多い． 小学校教師を目指す学生たちが受講する 「理科研究」 のレポートから， この現状を打開する方法を探ってみた．To consider the problems in biological education, I asked students to classify the raw materials used to prepare food on the basis of whether or not the materials are obtained from organisms. Two-thirds of the students did not classify vegetables and grains as organic materials. This was despite the fact that these students are as familiar with the structure and function of plants as the rest of their peers. Moreover, all students have experience in plant cultivation. They have observed the life cycle of plants. I considered the factors that are necessary for students to recognize plants as organisms by examining students\u27 reports that expressed fascination for microscopic observation of plant tissues or cells and for observation of underground organisms