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47 results on '"Takeuchi, T."'

1. Characterization of a novel Entamoeba histolytica strain from Burkina Faso, Africa, possessing a unique hexokinase-2 gene

Author

Suzuki J., Kobayashi S., Imada M., Tolba M.E., and Takeuchi T.

Subjects
Entamoeba histolytica, isoenzyme, hexokinase, genetic variation, isoelectric focusing, Infectious and parasitic diseases, RC109-216
Abstract

An Entamoeba histolytica strain (BF-841 cl1) that originated from Burkina Faso, Africa presented with novel, polymorphic genotypes of the serine-rich E. histolytica protein and the anodic hexokinase-2 (HXK-2) isoenzyme band, which showed less electrophoretic mobility than that of an E. histolytica reference strain [HM-1:IMSS cl6 (zymodeme (Z)-II)] by starch gel electrophoresis and isoelectric focusing (IEF). The HXK-2 gene of BF-841 cl1 had amino acid variations at four positions compared to the sequence of HM-1: IMSS cl6. These variations were absent from the sequences of four other E. histolytica strains with different zymodemes [KU27 (Z-II), SAW1627 (Z-IIα-), SAW755CR clB (Z-XIV), and KU2 (Z-XIX)]. The results of IEF showed no difference in the substrate specificity of HXK (HXK-1 and HXK-2) between BF-841 cl1 and the three reference E. histolytica strains (HM-1:IMSS cl6, SAW755 clB, and KU27). It was also confirmed that BF-841 cl1 was able to form liver abscesses in Syrian hamsters.

Published
2011
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2. Establishment of a continuous culture system for Entamoeba muris and analysis of the small subunit rRNA gene

Author

Kobayashi S., Suzuki J., and Takeuchi T.

Subjects
Entamoeba muris, Entamoeba coli, dixenic culture, Balamuth’s egg yolk infusion medium, SSU-rRNA gene, phylogenetic analysis, Infectious and parasitic diseases, RC109-216
Abstract

We established a culture system for Entamoeba muris (MG-EM-01 strain isolated from a Mongolian gerbil) using a modified Balamuth’s egg yolk infusion medium supplemented with 4% adult bovine serum and Bacteroides fragilis cocultured with Escherichia coli. Further, encystation was observed in the culture medium. The morphological characteristics of E. muris are similar to those of Entamoeba coli (E. coli); moreover, the malic isoenzyme electrophoretic band, which shows species-specific electrophoretic mobility, of E. muris had almost the same mobility as that observed with the malic isoenzyme electrophorectic band of E. coli (UZG-EC-01 strain isolated from a gorilla). We determined the small subunit rRNA (SSU-rRNA) gene sequence of the MG-EM-01 strain, and this sequence was observed to show 82.7% homology with that of the UZG-EC-01 strain. Further, the resultant phylogenetic tree for molecular taxonomy based on the SSU-rRNA genes of the 21 strains of the intestinal parasitic amoeba species indicated that the MG-EM-01 strain was most closely related to E. coli.

Published
2009
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3. Growth-promoting effect on iron-sulfur proteins on axenic cultures of Entamoeba dispar

Author

Khalifa S.A.M., Imai E., Kobayashi S., Haghighi A., Hayakawa E., and Takeuchi T.

Subjects
growth, mitochondria, hydrogenosomes, chloroplasts, iron-sulphur protein, Entamoeba dispar, Infectious and parasitic diseases, RC109-216
Abstract

A growth-promoting factor (GPF) that promotes the growth of Entamoeba dispar under axenic culture conditions was found in fractions of mitochondria (Mt), hydrogenosomes (Hg) and chloroplasts (Cp) obtained from cells of six different protozoan, mammalian and plant species. We were able to extract the GPF from the Cp-rich leaf cells of a plant (spiderwort: Commelina communis L.) in an acetone-soluble fraction as a complex of chlorophyll with low molecular weight proteins (molecular weight [MW] approximately 4,600). We also found that on treatment with 0.6 % complexes of 2-mercapthoethanol (2ME), complexes of chlorophyll-a with iron-sulphur (Fe-S) proteins (e.g., ferredoxins [Fd] from spinach and Clostridium pasteurianum) and noncomplex rubredoxin (Rd) from C. pasteurianum have a growth-promoting effect on E. dispar. These findings suggest that E. dispar may lack a sufficient quantity of some essential components of Fe-S proteins, such as Fe-S center.

Published
2006
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5. The fate of the interstellar medium in early-type galaxies

Author

Michałowski, M. J., primary, Hjorth, J., additional, Gall, C., additional, Frayer, D. T., additional, Tsai, A.-L., additional, Hirashita, H., additional, Rowlands, K., additional, Takeuchi, T. T., additional, Leśniewska, A., additional, Behrendt, D., additional, Bourne, N., additional, Hughes, D. H., additional, Spring, E., additional, Zavala, J., additional, and Bartczak, P., additional

Published
2019
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6. AKARI mid-infrared slitless spectroscopic survey of star-forming galaxies at z ≲ 0.5

Author

Ohyama, Y., primary, Wada, T., additional, Matsuhara, H., additional, Takagi, T., additional, Malkan, M., additional, Goto, T., additional, Egami, E., additional, Lee, H.-M., additional, Im, M., additional, Kim, J.H., additional, Pearson, C., additional, Inami, H., additional, Oyabu, S., additional, Usui, F., additional, Burgarella, D., additional, Mazyed, F., additional, Imanishi, M., additional, Jeong, W.-S., additional, Miyaji, T., additional, Díaz Tello, J., additional, Nakagawa, T., additional, Serjeant, S., additional, Takeuchi, T. T., additional, Toba, Y., additional, White, G. J., additional, Hanami, H., additional, and Ishigaki, T., additional

Published
2018
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7. The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Author

Siudek, M., primary, Małek, K., additional, Pollo, A., additional, Krakowski, T., additional, Iovino, A., additional, Scodeggio, M., additional, Moutard, T., additional, Zamorani, G., additional, Guzzo, L., additional, Garilli, B., additional, Granett, B. R., additional, Bolzonella, M., additional, de la Torre, S., additional, Abbas, U., additional, Adami, C., additional, Bottini, D., additional, Cappi, A., additional, Cucciati, O., additional, Davidzon, I., additional, Franzetti, P., additional, Fritz, A., additional, Krywult, J., additional, Le Brun, V., additional, Le Fèvre, O., additional, Maccagni, D., additional, Marulli, F., additional, Polletta, M., additional, Tasca, L. A.M., additional, Tojeiro, R., additional, Vergani, D., additional, Zanichelli, A., additional, Arnouts, S., additional, Bel, J., additional, Branchini, E., additional, Coupon, J., additional, De Lucia, G., additional, Ilbert, O., additional, Haines, C. P., additional, Moscardini, L., additional, and Takeuchi, T. T., additional

Published
2018
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8. The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Author

Krywult, J., primary, Tasca, L. A. M., additional, Pollo, A., additional, Vergani, D., additional, Bolzonella, M., additional, Davidzon, I., additional, Iovino, A., additional, Gargiulo, A., additional, Haines, C. P., additional, Scodeggio, M., additional, Guzzo, L., additional, Zamorani, G., additional, Garilli, B., additional, Granett, B. R., additional, de la Torre, S., additional, Abbas, U., additional, Adami, C., additional, Bottini, D., additional, Cappi, A., additional, Cucciati, O., additional, Franzetti, P., additional, Fritz, A., additional, Le Brun, V., additional, Le Fèvre, O., additional, Maccagni, D., additional, Małek, K., additional, Marulli, F., additional, Polletta, M., additional, Tojeiro, R., additional, Zanichelli, A., additional, Arnouts, S., additional, Bel, J., additional, Branchini, E., additional, Coupon, J., additional, De Lucia, G., additional, Ilbert, O., additional, McCracken, H. J., additional, Moscardini, L., additional, and Takeuchi, T. T., additional

Published
2017
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10. The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Author

Siudek, M., primary, Małek, K., additional, Scodeggio, M., additional, Garilli, B., additional, Pollo, A., additional, Haines, C. P., additional, Fritz, A., additional, Bolzonella, M., additional, de la Torre, S., additional, Granett, B. R., additional, Guzzo, L., additional, Abbas, U., additional, Adami, C., additional, Bottini, D., additional, Cappi, A., additional, Cucciati, O., additional, De Lucia, G., additional, Davidzon, I., additional, Franzetti, P., additional, Iovino, A., additional, Krywult, J., additional, Le Brun, V., additional, Le Fèvre, O., additional, Maccagni, D., additional, Marchetti, A., additional, Marulli, F., additional, Polletta, M., additional, Tasca, L. A. M., additional, Tojeiro, R., additional, Vergani, D., additional, Zanichelli, A., additional, Arnouts, S., additional, Bel, J., additional, Branchini, E., additional, Ilbert, O., additional, Gargiulo, A., additional, Moscardini, L., additional, Takeuchi, T. T., additional, and Zamorani, G., additional

Published
2017
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12. Clustering of the AKARI NEP deep field 24μm selected galaxies

Author

Solarz, A., primary, Pollo, A., additional, Takeuchi, T. T., additional, Małek, K., additional, Matsuhara, H., additional, White, G. J., additional, Pȩpiak, A., additional, Goto, T., additional, Wada, T., additional, Oyabu, S., additional, Takagi, T., additional, Ohyama, Y., additional, Pearson, C. P., additional, Hanami, H., additional, Ishigaki, T., additional, and Malkan, M., additional

Published
2015
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13. Environmental dependence of 8 μm luminosity functions of galaxies at z ~ 0.8: Comparison between RXJ1716.4+6708 and the AKARI NEP-deep field

Author

Goto, T., Koyama, Y., Wada, T., Pearson, C., Matsuhara, H., Tagaki, T., Shim, H., Im, M., Lee, M. G., Inami, H., Malkan, M., Okamura, S., Takeuchi, T. T., Serjeant, S., Kodama, T., Nakagawa, T., Oyabu, S., Ohyama, Y., Lee, H. M., Hwang, N., Hanami, H., Imai, K., and Ishigaki, T.

Abstract

Aims. We aim to reveal environmental dependence of infrared luminosity functions (IR LFs) of galaxies at z ~ 0.8 using the AKARI satellite. AKARI’s wide field of view and unique mid-IR filters help us to construct restframe 8 μm LFs directly without relying on SED models. Methods. We construct restframe 8 μm IR LFs in the cluster region RXJ1716.4+6708 at z = 0.81, and compare them with a blank field using the AKARI north ecliptic pole deep field data at the same redshift. AKARI’s wide field of view (10' × 10') is suitable to investigate wide range of galaxy environments. AKARI’s 15 μm filter is advantageous here since it directly probes restframe 8 μm at z ~ 0.8, without relying on a large extrapolation based on a SED fit, which was the largest uncertainty in previous work. Results. We have found that cluster IR LFs at restframe 8 μm have a factor of 2.4 smaller L^∗ and a steeper faint-end slope than that of the field. Confirming this trend, we also found that faint-end slopes of the cluster LFs becomes flatter and flatter with decreasing local galaxy density. These changes in LFs cannot be explained by a simple infall of field galaxy population into a cluster. Physics that can preferentially suppress IR luminous galaxies in high density regions is required to explain the observed results.

Published
2010

14. Discovery of very high energy gamma-ray emission coincident with molecular clouds in the W 28 (G6.4-0.1) field

Author

Aharonian, F., Akhperjanian, A.G., Bazer-Bachi, A.R., Behera, B., Beilicke, M., Benbow, W., Berge, D., Bernlöhr, K., Boisson, C., Bolz, O., Borrel, V., Braun, I., Brion, E., Brown, A.M., Bühler, R., Bulik, T., Büsching, I., Boutelier, T., Carrigan, S., Chadwic, P.M., Chounet, L.-M., Clapson, A.C., Coignet, G., Cornils, R., Costamante, L., Degrange, B., Dickinson, H.J., Djannati-Ataï, A., Domainko, W., Drury, L.O'C., Dubus, G., Dyks, J., Egberts, K., Emmanoulopoulos, D., Espigat, P., Farnier, C., Feinstein, F., Fiasson, A., F¨orster, A., Fontaine, G., Fukui, Y., Funk, Seb., Funk, S., Füssling, M., Gallant, Y.A., Giebels, B., Glicenstein, J.F., Glück, B., Goret, P., Hadjichristidis, C., Hauser, D., Hauser, M., Heinzelmann, G., Henri, G., Hermann, G., Hinton, J.A., Hoffmann, A., Hofmann, W., Holleran, M., Hoppe, S., Horns, D., Jacholkowska, A., de Jager, O.C., Kendziorra, E., Kerschhagg, M., Khélifi, B., Komin, Nu., Kosack, K., Lamanna, G., Latham, I.J., Le Gallou, R., Lemière, A., Lemoine-Goumard, M., Lenain, J.-P., Lohse, T., Martin, J.M., Martineau-Huynh, O., Marcowith, A., Masterson, C., Maurin, G., Mccomb, T.J.L., Moderski, R., Moriguchi, Y., Moulin, Emmanuel, de Naurois, M., Nedbal, D., Nolan, S.J., Olive, J.-P., Orford, K.J., Osborne, J.L., Ostrowski, M., Panter, M., Pedaletti, G., Pelletier, G., Petrucci, P.-O., Pita, S., P¨uhlhofer, G., Punch, M., Ranchon, S., Raubenheimer, B.C., Raue, M., Rayner, S.M., Reimer, O., Renaud, M., Ripken, J., Rob, L., Rolland, L., Rosier-Lees, S., Rowell, G., Rudak, B., Ruppel, J., Sahakian, V., Santangelo, A., Saugé, L., Schlenker, S., Schlickeiser, R., Schroder, R., Schwanke, U., Schwarzburg, S., Schwemmer, S., Shalchi, A., Sol, H., Spangler, D., Stawarz, &#321., Steenkamp, R., Stegmann, C., Superina, G., Takeuchi, T., Tam, P.H., Tavernet, J.-P., Terrier, R., van Eldik, C., Vasileiadis, G., Venter, C., Vialle, J.P., Vincent, P., Vivier, M., Volk, H.J., Volpe, F., Wagner, S.J., Ward, M., 10859748 - Holleran, Mathew, 12006653 - Venter, Christo, 10179240 - Raubenheimer, Barend Christoffel, 10065857 - De Jager, Ocker Cornelis, 13235176 - Büsching, Ingo, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), APC - Astrophysique des Hautes Energies (APC - AHE), Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), AstroParticule et Cosmologie (APC (UMR_7164)), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), HESS, Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, 010303 astronomy & astrophysics, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Molecular cloud, Local standard of rest, Astrophysics (astro-ph), Gamma ray, observations [gamma rays], Astronomy and Astrophysics, Galactic plane, Particle acceleration, 13. Climate action, Space and Planetary Science, Open cluster
Abstract

We observed the W28 field (for ~40 h) at Very High Energy (VHE) gamma-ray energies (E>0.1 TeV) with the H.E.S.S. Cherenkov telescopes. A reanalysis of EGRET E>100 MeV data was also undertaken. Results from the NANTEN 4m telescope Galactic plane survey and other CO observations have been used to study molecular clouds. We have discovered VHE gamma-ray emission (HESSJ1801-233) coincident with the northeastern boundary of W28, and a complex of sources (HESSJ1800-240A, B and C) ~0.5 deg south of W28, in the Galactic disc. The VHE differential photon spectra are well fit by pure power laws with indices Gamma~2.3 to 2.7. The NANTEN ^{12}CO(J=1-0) data reveal molecular clouds positionally associating with the VHE emission, spanning a ~15 km s^{-1} range in local standard of rest velocity. The VHE/molecular cloud association could indicate a hadronic origin for HESSJ1801-233 and HESSJ1800-240, and several cloud components in projection may contribute to the VHE emission. The clouds have components covering a broad velocity range encompassing the distance estimates for W28 (~2 kpc), and extending up to ~4 kpc. Assuming a hadronic origin, and distances of 2 and 4 kpc for cloud components, the required cosmic ray density enhancement factors (with respect to the solar value) are in the range ~10 to ~30. If situated at 2 kpc distance, such cosmic ray densities may be supplied by a SNR like W28. Additionally and/or alternatively, particle acceleration may come from several catalogued SNRs and SNR candidates, the energetic ultra compact HII region W28A2, and the HII regions M8 and M20 along with their associated open clusters. Further sub-mm observations would be recommended to probe in detail the dynamics of the molecular clouds at velocites >10 km s^{-1}, and their possible connection to W28., 10 pages, 4 figures. Accepted for publication in Astronomy & Astrophysics. (Abstract shortened)

Published
2008

15. [Ultra] luminous infrared galaxies selected at 90 μm in the AKARI deep field: a study of AGN types contributing to their infrared emission.

Author

Małek, K., Bankowicz, M., Pollo, A., Buat, V., Takeuchi, T. T., Burgarella, D., Goto, T., Malkan, M., and Matsuhara, H.

Subjects
ACTIVE galactic nuclei, SPECTRAL energy distribution, LUMINOSITY, FIELD research, STELLAR evolution
Abstract

Aims. The aim of this work is to characterize physical properties of ultra luminous infrared galaxies (ULIRGs) and luminous infrared galaxies (LIRGs) detected in the far-infrared (FIR) 90 μm band in the AKARI Deep Field-South (ADF-S) survey. In particular, we want to estimate the active galactic nucleus (AGN) contribution to the LIRGs and ULIRGs' infrared emission and which types of AGNs are related to their activity. Methods. We examined 69 galaxies at redshift ≥0.05 detected at 90 μm by the AKARI satellite in the ADF-S, with optical counterparts and spectral coverage from the ultraviolet to the FIR. We used two independent spectral energy distribution fitting codes: one fitting the SED from FIR to FUV (CIGALE) (we use the results from CIGALE as a reference) and gray-body + power spectrum fit for the infrared part of the spectra (CMCIRSED) in order to identify a subsample of ULIRGs and LIRGs, and to estimate their properties. Results. Based on the CIGALE SED fitting, we have found that LIRGs and ULIRGs selected at the 90 μm AKARI band compose ~56% of our sample (we found 17 ULIRGs and 22 LIRGs, spanning over the redshift range 0.06

Published
2017
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16. Gas-to-dust mass ratios in local galaxies over a 2 dex metallicity range

Author

Rémy-Ruyer, A., primary, Madden, S. C., additional, Galliano, F., additional, Galametz, M., additional, Takeuchi, T. T., additional, Asano, R. S., additional, Zhukovska, S., additional, Lebouteiller, V., additional, Cormier, D., additional, Jones, A., additional, Bocchio, M., additional, Baes, M., additional, Bendo, G. J., additional, Boquien, M., additional, Boselli, A., additional, DeLooze, I., additional, Doublier-Pritchard, V., additional, Hughes, T., additional, Karczewski, O. Ł., additional, and Spinoglio, L., additional

Published
2014
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18. Clustering of the AKARI NEP deep field 24 µm selected galaxies.

Author

Solarz, A., Pollo, A., Takeuchi, T. T., Małek, K., Matsuhara, H., White, G. J., Pępiak, A., Goto, T., Wada, T., Oyabu, S., Takagi, T., Ohyama, Y., Pearson, C. P., Hanami, H., Ishigaki, T., and Malkan, M.

Subjects
GALAXIES, DARK matter, REDSHIFT, SUPPORT vector machines, STATISTICAL correlation
Abstract

Aims. We present a method of selection of 24 μm galaxies from the AKARI north ecliptic pole (NEP) deep field down to 150 μJy and measurements of their two-point correlation function. We aim to associate various 24 μm selected galaxy populations with present day galaxies and to investigate the impact of their environment on the direction of their subsequent evolution. Methods. We discuss using of Support Vector Machines (SVM) algorithm applied to infrared photometric data to perform star-galaxy separation, in which we achieve an accuracy higher than 80%. The photometric redshift information, obtained through the CIGALE code, is used to explore the redshift dependence of the correlation function parameter (r0) as well as the linear bias evolution. This parameter relates galaxy distribution to the one of the underlying dark matter. We connect the investigated sources to their potential local descendants through a simplified model of the clustering evolution without interactions. Results. We observe two different populations of star-forming galaxies, at zmed ~ 0.25, zmed ~ 0.9. Measurements of total infrared luminosities (LTIR) show that the sample at zmed ~ 0.25 is composed mostly of local star-forming galaxies, while the sample at zmed ~ 0.9 is composed of luminous infrared galaxies (LIRGs) with LTIR ~ 1011.62 Lʘ.We find that dark halo mass is not necessarily correlated with the LTIR: for subsamples with LTIR = 1011.15 Lʘ at zmed ~ 0.7 we observe a higher clustering length (r0 = 6.21 ± 0.78 [h-1Mpc]) than for a subsample with mean LTIR = 1011.84 Lʘ at zmed ~ 1.1 (r0 = 5.86 ± 0.69 h-1Mpc). We find that galaxies at zmed ~ 0.9 can be ancestors of present day L* early type galaxies, which exhibit a very high r0 ~ 8 h-1 Mpc. [ABSTRACT FROM AUTHOR]

Published
2015
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20. The North Ecliptic Pole Wide survey of AKARI: a near- and mid-infrared source catalog

Author

Kim, S. J., primary, Lee, H. M., additional, Matsuhara, H., additional, Wada, T., additional, Oyabu, S., additional, Im, M., additional, Jeon, Y., additional, Kang, E., additional, Ko, J., additional, Lee, M. G., additional, Takagi, T., additional, Pearson, C., additional, White, G. J., additional, Jeong, W.-S., additional, Serjeant, S., additional, Nakagawa, T., additional, Ohyama, Y., additional, Goto, T., additional, Takeuchi, T. T., additional, Pollo, A., additional, Solarz, A., additional, and Pȩpiak, A., additional

Published
2012
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21. Star-galaxy separation in the AKARI NEP deep field

Author

Solarz, A., primary, Pollo, A., additional, Takeuchi, T. T., additional, Pȩpiak, A., additional, Matsuhara, H., additional, Wada, T., additional, Oyabu, S., additional, Takagi, T., additional, Goto, T., additional, Ohyama, Y., additional, Pearson, C. P., additional, Hanami, H., additional, and Ishigaki, T., additional

Published
2012
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25. Environmental dependence of 8 μm luminosity functions of galaxies atz~ 0.8

Author

Goto, T., primary, Koyama, Y., additional, Wada, T., additional, Pearson, C., additional, Matsuhara, H., additional, Takagi, T., additional, Shim, H., additional, Im, M., additional, Lee, M. G., additional, Inami, H., additional, Malkan, M., additional, Okamura, S., additional, Takeuchi, T. T., additional, Serjeant, S., additional, Kodama, T., additional, Nakagawa, T., additional, Oyabu, S., additional, Ohyama, Y., additional, Lee, H. M., additional, Hwang, N., additional, Hanami, H., additional, Imai, K., additional, and Ishigaki, T., additional

Published
2010
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27. Evolution of infrared luminosity functions of galaxies in the AKARI NEP-deep field

Author

Goto, T., primary, Takagi, T., additional, Matsuhara, H., additional, Takeuchi, T. T., additional, Pearson, C., additional, Wada, T., additional, Nakagawa, T., additional, Ilbert, O., additional, Le Floc'h, E., additional, Oyabu, S., additional, Ohyama, Y., additional, Malkan, M., additional, Lee, H. M., additional, Lee, M. G., additional, Inami, H., additional, Hwang, N., additional, Hanami, H., additional, Im, M., additional, Imai, K., additional, Ishigaki, T., additional, Serjeant, S., additional, and Shim, H., additional

Published
2010
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31. SPICA Deep Cosmological Survey: From AKARI to SPICA

Author

Shirahata, M., primary, Matsuura, S., additional, Matsuhara, H., additional, Takagi, T., additional, Oyabu, S., additional, Wada, T., additional, Nakagawa, T., additional, Kawada, M., additional, Takeuchi, T. T., additional, Hatsukade, B., additional, Kohno, K., additional, Pearson, C. P., additional, Serjeant, S., additional, and White, G., additional

Published
2009
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34. Ultraviolet-to-far infrared properties of Lyman break galaxies and luminous infrared galaxies at z ~ 1

Author

Burgarella, D., primary, Pérez-González, P. G., additional, Tyler, K. D., additional, Rieke, G. H., additional, Buat, V., additional, Takeuchi, T. T., additional, Lauger, S., additional, Arnouts, S., additional, Ilbert, O., additional, Barlow, T. A., additional, Bianchi, L., additional, Lee, Y.-W., additional, Madore, B. F., additional, Malina, R. F., additional, Szalay, A. S., additional, and Yi, S. K., additional

Published
2006
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45. Properties of star forming galaxies in AKARI Deep Field-South.

Author

Buat, V., Burgarella, D., Giovannoli, E., Kurek, A., Małek, K., Malkan, M., Matsuura, S., Pollo, A., and Takeuchi, T. T.

Subjects
STAR formation, GALACTIC redshift, ASTRONOMICAL photometry, GALACTIC evolution, SPECTRAL energy distribution, INFRARED spectroscopy
Abstract

Aims. The main aim of this work is the characterization of physical properties of galaxies detected in the far-infrared (FIR) in the AKARI Deep Field-South (ADF-S) survey. Methods. Starting from a catalog of the 1000 brightest ADF-S sources in the WIDE-S (90 μm) AKARI band, we constructed a subsample of galaxies with spectral coverage from the ultraviolet to the FIR. We then analyzed the multiwavelength properties of this 90 μm selected sample of galaxies. For galaxies without known spectroscopic redshifts we computed photometric redshifts using the codes Photometric Analysis for Redshift Estimate (Le PHARE) and Code Investigating GALaxy Emission (CIGALE), tested these photometric redshifts using spectroscopic redshifts, and compared the performances of both codes. To test the reliability of parameters obtained by fitting spectral energy distributions, a mock catalogue was generated. Results. We built a large multiwavelength catalog of more than 500 ADF-S galaxies. We successfully fitted spectral energy distributions of 186 galaxies with Χ2 min < 4, and analyzed the output parameters of the fits. We conclude that our sample consists mostly of nearby actively star-forming galaxies, and all our galaxies have a relatively high metallicity. We estimated photometric redshifts for 113 galaxies from the whole ADF-S sample. Comparing the performance of Le PHARE and CIGALE, we found that CIGALE gives more reliable redshift estimates for our galaxies, which implies that including the IR photometry allows for substantial improvement of photometric redshift estimation. [ABSTRACT FROM AUTHOR]

Published
2014
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47. The North Ecliptic Pole Wide survey of AKARI: a nearand mid-infrared source catalog.

Author

Kim, S. J., Lee, H. M., Matsuhara, H., Wada, T., Oyabu, S., Im, M., Jeon, Y., Kang, E., Ko, J., Lee, M. G., Takagi, T., Pearson, C., White, G. J., Jeong, W.-S., Serjeant, S., Nakagawa, T., Ohyama, Y., Goto, T., Takeuchi, T. T., and Pollo, A.

Subjects
PHOTOMETRY, TELESCOPES, INFRARED radiation, COSMIC rays, IONIZING radiation
Abstract

We present a photometric catalog of infrared (IR) sources based on the North Ecliptic Pole Wide field (NEP-Wide) survey of AKARI, which is an infrared space telescope launched by Japan. The NEP-Wide survey covered 5.4 deg² area, a nearly circular shape centered on the NEP, using nine photometric filter-bands from 2-25 μm of the Infrared Camera (IRC). Extensive efforts were made to reduce possible false objects due to cosmic ray hits, multiplexer bleeding phenomena around bright sources, and other artifacts. The number of detected sources varied depending on the filter band: with about 109 000 sources being cataloged in the near-infrared (NIR) bands at 2-5 μm, about 20 000 sources in the shorter parts of the mid-infrard (MIR) bands between 7-11 μm, and about 16 000 sources in the longer parts of the MIR band, with ∼4000 sources at 24 μm. The estimated 5σ detection limits are approximately 21 mag (mag) in the 2-5 μm bands, 19.5-19 mag in the 7-11 μm, and 18.8-18.5 mag in the 15-24 μm bands in the AB magnitude scale. The completenesses for those bands were evaluated as a function of magnitude: the 50% completeness limits are about 19.8 mag at 3 μm, 18.6 mag at 9 μm, and 18 mag at 18 μm band, respectively. To construct a reliable source catalog, all of the detected sources were examined by matching them with those in other wavelength data, including optical and ground-based NIR bands. The final band-merged catalog contains about 114 800 sources detected in the IRC filter bands. The properties of the sources are presented in terms of the distributions in various color-color diagrams. [ABSTRACT FROM AUTHOR]

Published
2012
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