An Astronomical Data Archive System with a Java-Based User Interface

Horaguchi, T.; Nishihara, Eiji; Yoshida, Michitoshi; Aoki, Kentaro; Ito, Takashi; Watanabe, Masaru; Ichikawa, Shinichi; Takata, Tadafumi; Yoshida, S.; Hamabe, M.

doi:10.1093/pasj/51.5.693

Cited by 2 publications

(2 citation statements)

References 2 publications

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“…The regions which have the same labels are adjacent to each other on the sky. 1, 0, 1, 2, 3, 4, 5, 6, {7 and 8}, 9, and 10 in cooperation wich the Japan Association Information Processing in Astronomy (Horaguchi et al 1994;Takata et al 1995). .6…”

Section: Figure Captionsmentioning

confidence: 99%

Photometric Properties of Kiso Ultraviolet‐Excess Galaxies in the Lynx–Ursa Major Region

Takeuchi

Tomita

Nakanishi

et al. 1999

ASTROPHYS J SUPPL S

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We have performed a systematic study of several regions in the sky where the number of galaxies exhibiting star formation (SF) activity is greater than average. We used Kiso ultraviolet-excess galaxies (KUGs) as our SF-enhanced sample. By statistically comparing the KUG and non-KUG distributions, we discovered four KUG-rich regions with a size of ∼ 10 • × 10 • . One of these regions corresponds spatially to a filament of length ∼ 60 h −1 Mpc in the Lynx-Ursa Major region (α ∼ 9 h − 10 h , δ ∼ 42 • − 48 • ). We call this "the Lynx-Ursa Major (LUM) filament". We obtained V (RI) C surface photometry of 11 of the KUGs in the LUM filament and used these to investigate the integrated colors, distribution of SF regions, morphologies, and local environments. We found that these KUGs consist of distorted spiral galaxies and compact galaxies with blue colors. Their star formation occurs in the entire disk, and is not confined to just the central regions. The colors of the SF regions imply that active star formation in the spiral galaxies occurred 10 7−8 yr ago, while that of the compact objects occurred 10 6−7 yr ago. Though the photometric characteristics of these KUGs are similar to those of interacting galaxies or mergers, most of these KUGs do not show direct evidence of merger processes.2. KUGs are preferentially Sb-or later-type spiral galaxies. The KUG fraction changes linearly along the Hubble sequence: it is less than 10 % for E/S0 and more than 50 % for Sd/Sm.3. KUGs are biased toward less luminous galaxies. At around the knee of the luminosity function (LF) where B-luminosity L B ∼ 10 10 L ⊙ , most of the KUGs are spiral galaxies. In the fainter regime of L B < 10 9.3 L ⊙ , the dwarf population dominates. The fraction of the blue population in a survey depends on the depth of the survey.If the survey is volume-limited and deep enough to pick up the bulk of the dwarf population, its fraction would be higher.The distribution of KUGs is inhomogeneous, not only when compared with a uniform distribution but also in comparison with the ambient galaxy distribution. Consequently there are some "KUG-rich regions". This inhomogeneity may be related to environmental effects. Some studies show that a dense environment activates star formation (e.g. Maia et al. 1994;Pastoriza et al. 1994). On the other hand, recent observational studies (e.g. Zabludoff et al. 1996(Z96)) suggest that a low-density environment can enhance star formation. Therefore, the question is unsettled.In this study we statistically analyzed the fraction of KUGs in the whole galaxy population and discovered four KUG-rich regions. Among them was a region which lies in the constellations of Lynx and Ursa Major (α ∼ 9 h − 10 h , δ ∼ 42 • − 48 • ). In this region, there is a galaxy filament with a length of ∼ 60h −1 Mpc (We use H 0 = 100h km s −1 Mpc −1 as the Hubble parameter throughout this paper). We call this structure the Lynx-Ursa Major (hereafter LUM) filament. We obtained V (RI) C surface photometry of eleven KUGs in this region in order to make a q...

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Section: Figure Captionsmentioning

confidence: 99%

Photometric Properties of Kiso Ultraviolet‐Excess Galaxies in the Lynx–Ursa Major Region

Takeuchi

Tomita

Nakanishi

et al. 1999

ASTROPHYS J SUPPL S

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“…‡ You can see the quick look of the raw data of our OAO and KISO observations through Mitaka-Okayama-Kiso data Archival system (MOKA); see http://www.moka.nao.ac.jp/. The MOKA is operated by Astronomical Data Analysis Center, Okayama Astrophysical Observatory (National Astronomical Observatory of Japan), and Kiso Observatory (University of Tokyo) in cooperation with the Japanese Association Information Processing in Astronomy(Horaguchi et al 1994;Takata et al 1995). § In 1995 for January and March runs, in 1996 for April run.…”

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confidence: 99%

Optical and CO Radio Observations of Poor Cluster Zwicky 1615.8+3505

Tomita¹,

Maehara²,

Takeuchi³

et al. 1999

Publications of the Astronomical Society of Japan

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The cluster Zwicky 1615.8+3505 is considered to be a dynamically young poor cluster. To investigate the morphology and star-formation activity of galaxies under the environment of a dynamically young poor cluster, we have performed V , R, and I surface photometry, optical low-resolution spectroscopy, and 12 CO (J = 1 − 0) line observations for member galaxies. Our data show that more than 90% of the observed galaxies show regular morphologies and no star-1 formation activities, indicating that the environment does not affect these galaxy properties.Among sixteen galaxies observed, only NGC 6104 shows a significant star-formation activity, and shows a distorted morphology, indicating a tidal interaction. This galaxy contains double knots, and only one knot possesses Seyfert activity, though the sizes and luminosities are similar to each other; we also discuss this feature.Sports and Culture. † Research fellows of the Japan Society for the Promotion of Science. * The V -band magnitude and V − R and V − I colors within an isophotal ellipsoid of µ R = 23.5 mag arcsec −2 . The errors of measurements were estimated to be 0.02 mag for the magnitudes and colors, except for galaxies Nos. 12 and 14, the errors of which were estimated to be 0.1 mag. † The asymptotic total V -band magnitude and V − R and V − I colors. The errors of measurements were estimated to be 0.03 mag for the magnitudes and colors, except for galaxies Nos. 12 and 14, the errors of which were estimated to be 0.1 mag. ‡ The asymptotic total V -band magnitude and V − R and V − I colors correcting extinction and redshift effects. The errors of measurements were estimated to be 0.1 mag for the magnitudes and colors, except for galaxies Nos. 12 and 14, the errors of which were estimated to be 0.2 mag. 24

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An Astronomical Data Archive System with a Java-Based User Interface

Cited by 2 publications

References 2 publications

Photometric Properties of Kiso Ultraviolet‐Excess Galaxies in the Lynx–Ursa Major Region

Photometric Properties of Kiso Ultraviolet‐Excess Galaxies in the Lynx–Ursa Major Region

Optical and CO Radio Observations of Poor Cluster Zwicky 1615.8+3505

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