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Low-momentum direct photon measurement in Cu+Cu collisions at √sNN = 200 GeV

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arXiv 2018年

作者： Adare, A. Afanasiev, S. Aidala, C. Ajitanand, N.N. Akiba, Y. Al-Bataineh, H. Alexander, J. Alfred, M. Aoki, K. Aphecetche, L. Armendariz, R. Aronson, S.H. Asai, J. Atomssa, E.T. Averbeck, R. Awes, T.C. Azmoun, B. Babintsev, V. Bagoly, A. Baksay, G. Baksay, L. Baldisseri, A. Barish, K.N. Barnes, P.D. Bassalleck, B. Bathe, S. Batsouli, S. Baublis, V. Bazilevsky, A. Belikov, S. Belmont, R. Bennett, R. Berdnikov, A. Berdnikov, Y. Bickley, A.A. Boer, M. Boissevain, J.G. Bok, J.S. Borel, H. Boyle, K. Brooks, M.L. Bryslawskyj, J. Buesching, H. Bumazhnov, V. Bunce, G. Butsyk, S. Campbell, S. Canoa Roman, V. Chang, B.S. Charvet, J.-L. Chernichenko, S. Chi, C.Y. Chiba, J. Chiu, M. Choi, I.J. Chujo, T. Chung, P. Churyn, A. Cianciolo, V. Cleven, C.R. Cole, B.A. Comets, M.P. Connors, M. Constantin, P. Csanád, M. Csörgo, T. Dahms, T. Danley, T.W. Das, K. David, G. Deaton, M.B. Dehmelt, K. Delagrange, H. Denisov, A. D'Enterria, D. Deshpande, A. Desmond, E.J. Dietzsch, O. Dion, A. Do, J.H. Donadelli, M. Drapier, O. Drees, A. Dubey, A.K. Durham, J.M. Durum, A. Dzhordzhadze, V. Efremenko, Y.V. Egdemir, J. Ellinghaus, F. Emam, W.S. Enokizono, A. En'yo, H. Esumi, S. Eyser, K.O. Fan, W. Feege, N. Fields, D.E. Finger, M. Finger, M. Fleuret, F. Fokin, S.L. Fraenkel, Z. Frantz, J.E. Franz, A. Frawley, A.D. Fujiwara, K. Fukao, Y. Fusayasu, T. Gadrat, S. Gallus, P. Garg, P. Garishvili, I. Ge, H. Glenn, A. Gong, H. Gonin, M. Gosset, J. Goto, Y. Granier de Cassagnac, R. Grau, N. Greene, S.V. Grosse Perdekamp, M. Gunji, T. Gustafsson, H.-Å. Hachiya, T. Hadj Henni, A. Haegemann, C. Haggerty, J.S. Hamagaki, H. Han, R. Harada, H. Hartouni, E.P. Haruna, K. Hasegawa, S. Haseler, T.O.S. Haslum, E. Hayano, R. He, X. Heffner, M. Hemmick, T.K. Hester, T. Hiejima, H. Hill, J.C. Hill, K. Hobbs, R. Hodges, A. Hohlmann, M. Holzmann, W. Homma, K. Hong, B. Horaguchi, T. Hornback, D. Hoshino, T. Hotvedt, N. Huang, J. Abilene Christian University AbileneTX79699 United States Department of Physics Augustana University Sioux FallsSD57197 United States Department of Physics Banaras Hindu University Varanasi221005 India Baruch College City University of New York New YorkNY10010 United States Collider-Accelerator Department Brookhaven National Laboratory UptonNY11973-5000 United States Physics Department Brookhaven National Laboratory UptonNY11973-5000 United States University of California-Riverside RiversideCA92521 United States Charles University Ovocný trh 5 Praha 1 Prague116 36 Czech Republic Chonbuk National University Jeonju561-756 Korea Republic of Science and Technology on Nuclear Data Laboratory China Institute of Atomic Energy Beijing102413 China Center for Nuclear Study Graduate School of Science University of Tokyo 7-3-1 Hongo Bunkyo Tokyo113-0033 Japan University of Colorado BoulderCO80309 United States Columbia University New YorkNY10027 United States Nevis Laboratories IrvingtonNY10533 United States Czech Technical University Zikova 4 Prague 6166 36 Czech Republic Dapnia CEA Saclay Gif-sur-YvetteF-91191 France Debrecen University Egyetem tér 1 DebrecenH-4010 Hungary ELTE Eötvös Loránd University Pázmány P. s. 1/A BudapestH-1117 Hungary Eszterházy Károly University Károly Róbert Campus Mátrai út 36 GyöngyösH-3200 Hungary Florida Institute of Technology MelbourneFL32901 United States Florida State University TallahasseeFL32306 United States Georgia State University AtlantaGA30303 United States Hiroshima University Kagamiyama Higashi-Hiroshima739-8526 Japan Department of Physics and Astronomy Howard University WashingtonDC20059 United States IHEP Protvino State Research Center of Russian Federation Institute for High Energy Physics Protvino142281 Russia University of Illinois at Urbana-Champaign UrbanaIL61801 United States Institute for Nuclear Research Russian Academy of Sciences prospekt 60-letiya Okt

We have measured direct photons for pT √sNN = 200 GeV. The e+e− contribution from quasi-real direct virtual photons has been determined as an excess over the known hadronic contributions in the e+e− mass distribution. A clear enhancement of photons over the binary scaled p+p fit is observed for pT ch/dη observed in Au+Au at the same collision energy. Copyright © 2018, The Authors. All rights reserved.

关键词： Germanium alloys

Construction of KAGRA: An underground gravitational wave observatory

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arXiv 2017年

作者： Akutsu, T. Ando, M. Araki, S. Araya, A. Arima, T. Aritomi, N. Asada, H. Aso, Y. Atsuta, S. Awai, K. Baiotti, L. Barton, M.A. Chen, D. Cho, K. Craig, K. DeSalvo, R. Doi, K. Eda, K. Enomoto, Y. Flaminio, R. Fujibayashi, S. Fujii, Y. Fujimoto, M.-K. Fukushima, M. Furuhata, T. Hagiwara, A. Haino, S. Harita, S. Hasegawa, K. Hasegawa, M. Hashino, K. Hayama, K. Hirata, N. Hirose, E. Ikenoue, B. Inoue, Y. Ioka, K. Ishizaki, H. Itoh, Y. Jia, D. Kagawa, T. Kaji, T. Kajita, T. Kakizaki, M. Kakuhata, H. Kamiizumi, M. Kanbara, S. Kanda, N. Kanemura, S. Kaneyama, M. Kasuya, J. Kataoka, Y. Kawaguchi, K. Kawai, N. Kawamura, S. Kawazoe, F. Kim, C. Kim, J. Kim, J.C. Kim, W. Kimura, N. Kitaoka, Y. Kobayashi, K. Kojima, Y. Kokeyama, K. Komori, K. Kotake, K. Kubo, K. Kumar, R. Kume, T. Kuroda, K. Kuwahara, Y. Lee, H.-K. Lee, H.-W. Lin, C.-Y. Liu, Y. Majorana, E. Mano, S. Marchio, M. Matsui, T. Matsumoto, N. Matsushima, F. Michimura, Y. Mio, N. Miyakawa, O. Miyake, K. Miyamoto, A. Miyamoto, T. Miyo, K. Miyoki, S. Morii, W. Morisaki, S. Moriwaki, Y. Muraki, Y. Murakoshi, M. Musha, M. Nagano, K. Nagano, S. Nakamura, K. Nakamura, T. Nakano, H. Nakano, M. Nakano, M. Nakao, H. Nakao, K. Narikawa, T. Ni, W.-T. Nonomura, T. Obuchi, Y. Oh, J.J. Oh, S.-H. Ohashi, M. Ohishi, N. Ohkawa, M. Ohmae, N. Okino, K. Okutomi, K. Ono, K. Ono, Y. Oohara, K. Ota, S. Park, J. Peña Arellano, F.E. Pinto, I.M. Principe, M. Sago, N. Saijo, M. Saito, T. Saito, Y. Saitou, S. Sakai, K. Sakakibara, Y. Sasaki, Y. Sato, S. Sato, T. Sato, Y. Sekiguchi, T. Sekiguchi, Y. Shibata, M. Shiga, K. Shikano, Y. Shimoda, T. Shinkai, H. Shoda, A. Someya, N. Somiya, K. Son, E.J. Starecki, T. Suemasa, A. Sugimoto, Y. Susa, Y. Suwabe, H. Suzuki, T. Tachibana, Y. Tagoshi, H. Takada, S. Takahashi, H. Takahashi, R. Takamori, A. Takeda, H. Tanaka, H. Tanaka, K. Tanaka, T. Tatsumi, D. National Astronomical Observatory of Japan Tokyo181-8588 Japan Graduate School of Science University of Tokyo Tokyo113-0033 Japan Department of Physics Graduate School of Science University of Tokyo Tokyo113-0033 Japan Ibaraki305-0801 Japan Earthquake Research Institute University of Tokyo Tokyo113-0032 Japan Department of Physics Graduate School of Science Osaka City University Osaka558-8585 Japan Graduate School of Science and Technology Hirosaki University Aomori036-8561 Japan Department of Physics Graduate School of Science and Engineering Tokyo Institute of Technology Tokyo152-8551 Japan Institute for Cosmic Ray Research University of Tokyo Chiba277-8582 Japan Institute for Cosmic Ray Research University of Tokyo Gifu506-1205 Japan Graduate School of Science Osaka University Osaka560-0043 Japan Department of Physics Sogang University Seoul121-742 Korea Republic of University of Sannio at Benevento BeneventoI-82100 Italy Sezione di Napoli NapoliI-80126 Italy University of Toyama Toyama930-8555 Japan Department of Physics Graduate School of Science Kyoto University Kyoto606-8502 Japan Institute of Physics Academia Sinica Taipei11529 Taiwan University of Toyama Toyama930-8555 Japan Yukawa Institute for Theoretical Physics Kyoto University Kyoto606-8502 Japan Albert-Einstein-Institut Max-Planck-Institut für Gravitationsphysik HannoverD-30167 Germany Department of Physics and Astronomy Seoul National University Seoul151-742 Korea Republic of Daejeon34055 Korea Republic of Department of Physics Myongji University Yongin449-728 Korea Republic of Department of Computer Simulation Inje University Gimhae-shi50834 Korea Republic of Daejeon34047 Korea Republic of Department of Physical Science Graduate School of Science Hiroshima University Hiroshima903-0213 Japan Department of Applied Physics Graduate School of Science Fukuoka University Fukuoka814-0180 Japan Graduate School of Science and Engineer

Major construction and initial-phase operation of a second-generation gravitational-wave detector KAGRA has been completed. The entire 3-km detector is installed underground in a mine in order to be isolated from background seismic vibrations on the surface. This allows us to achieve a good sensitivity at low frequencies and high stability of the detector. Bare-bones equipment for the interferometer operation has been installed and the first test run was accomplished in March and April of 2016 with a rather simple configuration. The initial configuration of KAGRA is named iKAGRA. In this paper, we summarize the construction of KAGRA, including the study of the advantages and challenges of building an underground detector and the operation of the iKAGRA interferometer together with the geophysics interferometer that has been constructed in the same tunnel. Copyright © 2017, The Authors. All rights reserved.

关键词： Interferometers

Collapse and nonlinear instability of AdS with angular momenta

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arXiv 2017年

作者： Choptuik, Matthew W. Dias, Óscar J.C. Santos, Jorge E. Way, Benson Department of Physics and Astronomy University of British Columbia 6224 Agricultural Road VancouverB.C.V6T 1W9 Canada CIFAR Cosmology and Gravity Program 180 Dundas St W Suite 1400 TorontoONM5G 1Z8 Canada STAG research centre and Mathematical Sciences University of Southampton United Kingdom Department of Applied Mathematics and Theoretical Physics University of Cambridge Wilberforce Road CambridgeCB3 0WA United Kingdom

We present a numerical study of rotational dynamics in AdS5 with equal angular momenta in the presence of a complex doublet scalar field. We determine that the endpoint of gravitational collapse is a Myers-Perry black hole for high energies and a hairy black hole for low energies. We investigate the timescale for collapse at low energies E, keeping the angular momenta J ∝ E in AdS length units. We find that the inclusion of angular momenta delays the collapse time, but retains a t ∼ 1/E scaling. We perturb and evolve rotating boson stars, and find that boson stars near AdS appear stable, but those sufficiently far from AdS are unstable. We find that the dynamics of the boson star instability depend on the perturbation, resulting either in collapse to a Myers-Perry black hole, or development towards a stable oscillating solution. Copyright © 2017, The Authors. All rights reserved.

关键词： Stars

Constraints on core-collapse supernova progenitors from explosion site integral field spectroscopy

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arXiv 2017年

作者： Kuncarayakti, H. Anderson, J.P. Galbany, L. Maeda, K. Hamuy, M. Aldering, G. Arimoto, N. Doi, M. Morokuma, T. Usuda, T. University of Turku Väisäläntie 20 Piikkiö21500 Finland Tuorla Observatory Department of Physics and Astronomy University of Turku Väisäläntie 20 Piikkiö21500 Finland Millennium Institute of Astrophysics Casilla 36-D Santiago Chile Departamento de Astronomía Universidad de Chile Casilla 36-D Santiago Chile European Southern Observatory Alonso de Córdova 3107 Casilla 19001 Vitacura Santiago Chile PITT PACC Department of Physics and Astronomy University of Pittsburgh PittsburghPA15260 United States Department of Astronomy Graduate School of Science Kyoto University Sakyo-ku Kyoto606-8502 Japan University of Tokyo 5-1-5 Kashiwanoha Kashiwa Chiba277-8583 Japan Physics Division Lawrence Berkeley National Laboratory 1 Cyclotron Road BerkeleyCA94720 United States Astronomy Program Department of Physics and Astronomy Seoul National University 599 Gwanak-ro Gwanak-gu Seoul151-742 Korea Republic of Subaru Telescope National Astronomical Observatory of Japan National Institutes of Natural Sciences 650 North A'ohoku Place HiloHI96720 United States Institute of Astronomy Graduate School of Science University of Tokyo 2-21-1 Osawa Mitaka Tokyo181-0015 Japan Research Center for the Early Universe Graduate School of Science University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan

Context. Observationally, supernovae are divided into subclasses pertaining to their distinct characteristics. This diversity naturally reflects the diversity in the progenitor stars. It is not entirely clear however, how different evolutionary paths leading massive stars to become a supernova are governed by fundamental parameters such as progenitor initial mass and metallicity. Aims. This paper places constraints on progenitor initial mass and metallicity in distinct core-collapse supernova subclasses, through a study of the parent stellar populations at the explosion sites. Methods. Integral field spectroscopy (IFS) of 83 nearby supernova explosion sites with a median distance of 18 Mpc has been collected and analysed, enabling detection and spectral extraction of the parent stellar population of supernova progenitors. From the parent stellar population spectrum, the initial mass and metallicity of the coeval progenitor are derived by means of comparison to simple stellar population models and strong-line methods. Additionally, near-infrared IFS was employed to characterise the star formation history at the explosion sites. Results. No significant metallicity differences are observed among distinct supernova types. The typical progenitor mass is found to be highest for supernova type Ic, followed by type Ib, then types IIb and II. Type IIn is the least associated with young stellar populations and thus massive progenitors. However, statistically significant differences in progenitor initial mass are observed only when comparing supernovae IIn with other subclasses. Stripped-envelope SN progenitors with initial mass estimate lower than 25 Moare found;these are thought to be the result of binary progenitors. Confirming previous studies, these results support the notion that core-collapse supernova progenitors cannot arise from single-star channel only, and both single and binary channels are at play in the production of core-collapse supernovae. Near-infrared IFS s

关键词： Supernovae

Gaia17biu/SN 2017egm IN NGC 3191: THE CLOSEST HYDROGEN-POOR SUPERLUMINOUS SUPERNOVA TO DATE IS IN A "NORMAL", MASSIVE, METAL-RICH SPIRAL GALAXY

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arXiv 2017年

作者： Bose, Subhash Dong, Subo Pastorello, A. Filippenko, Alexei V. Kochanek, C.S. Mauerhan, Jon Romero-Cañizales, C. Brink, Thomas G. Chen, Ping Prieto, J.L. Post, R. Ashall, Christopher Grupe, Dirk Tomasella, L. Benetti, Stefano Shappee, B.J. Stanek, K.Z. Cai, Zheng Falco, E. Lundqvist, Peter Mattila, Seppo Mutel, Robert Ochner, Paolo Pooley, David Stritzinger, M.D. Villanueva, S. Zheng, WeiKang Beswick, R.J. Brown, Peter J. Cappellaro, E. Davis, Scott Fraser, Morgan de Jaeger, Thomas Elias-Rosa, N. Gall, C. Gaudi, B. Scott Herczeg, Gregory J. Hestenes, Julia Holoien, T.W.-S. Hosseinzadeh, Griffin Hsiao, E.Y. Hu, Shaoming Jaejin, Shin Jeffers, Ben Koff, R.A. Kumar, Sahana Kurtenkov, Alexander Lau, Marie Wingyee Prentice, Simon Reynolds, T. Rudy, Richard J. Shahbandeh, Melissa Somero, Auni Stassun, Keivan G. Thompson, Todd A. Valenti, Stefano Woo, Jong-Hak Yunus, Sameen Kavli Institute for Astronomy and Astrophysics Peking University Yi He Yuan Road 5 Hai Dian District Beijing100871 China INAF-Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 PadovaI-35122 Italy Department of Astronomy University of California BerkeleyCA94720-3411 United States Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Department of Astronomy Ohio State University 140 W. 18th Avenue ColumbusOH43210 United States Ohio State University 191 W. Woodruff Avenue ColumbusOH43210 United States Millennium Institute of Astrophysics Santiago Chile Núcleo de Astronomía de la Facultad de Ingeniería y Ciencias Universidad Diego Portales Av. Ej ército 441 Santiago Chile Post Observatory LexingtonMA02421 Department of Physics Florida State University 77 Chieftain Way TallahasseeFL32306 United States Department of Earth and Space Science Morehead State University 235 Martindale Dr. MoreheadKY40351 United States Carnegie Observatories 813 Santa Barbara Street PasadenaCA91101 United States Hubble Fellow Carnegie-Princeton Fellow UCO/Lick Observatory University of California at Santa Cruz Santa CruzCA95064 United States Harvard-Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States Department of Astronomy and The Oskar Klein Centre AlbaNova University Center Stockholm University StockholmSE-10691 Sweden Tuorla Observatory Department of Physics and Astronomy University of Turku Vislntie 20 PiikkiFI-21500 Finland Department of Physics and Astronomy University of Iowa Trinity University Department of Physics & Astronomy One Trinity Place San AntonioTX78212 United States Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Jodrell Bank Centre for Astrophysics & e-MERLIN School of Physics and Astronomy University of Manchester ManchesterM13 9PL United Kingdom George P. and Cynthia Woods Mitchell Insti

Hydrogen-poor superluminous supernovae (SLSNe-I) have been predominantly found in low-metallicity, star-forming dwarf galaxies. Here we identify Gaia17biu/SN 2017egm as an SLSN-I occurring in a "normal" spiral galaxy (NGC 3191) in terms of stellar mass (several times 1010 M) and metallicity (roughly Solar). At redshift z = 0.031, Gaia17biu is also the lowest redshift SLSN-I to date, and the absence of a larger population of SLSNe-I in dwarf galaxies of similar redshift suggests that metallicity is likely less important to the production of SLSNe-I than previously believed. With the smallest distance and highest apparent brightness for an SLSN-I, we are able to study Gaia17biu in unprecedented detail. Its pre-peak near-ultraviolet to optical color is similar to that of Gaia16apd and among the bluest observed for an SLSN-I while its peak luminosity (Mg = −21 mag) is substantially lower than Gaia16apd. Thanks to the high signal-to-noise ratios of our spectra, we identify several new spectroscopic features that may help to probe the properties of these enigmatic explosions. We detect polarization at the ∼ 0.5% level that is not strongly dependent on wavelength, suggesting a modest, global departure from spherical symmetry. In addition, we put the tightest upper limit yet on the radio luminosity of an SLSN-I with 26 erg s−1 Hz−1 at 10 GHz, which is almost a factor of 40 better than previous upper limits and one of the few measured at an early stage in the evolution of an SLSN-I. This limit largely rules out an association of this SLSNe-I with known populations of gamma-ray burst (GRB) like central engines. Copyright © 2017, The Authors. All rights reserved.

关键词： Luminance

Structure of the Milky Way stellar halo out to its outer boundary with blue horizontal-branch stars

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arXiv 2017年

作者： Fukushima, Tetsuya Chiba, Masashi Homma, Daisuke Okamoto, Sakurako Komiyama, Yutaka Tanaka, Masayuki Tanaka, Mikito Arimoto, Nobuo Matsuno, Tadafumi Astronomical Institute Tohoku University Aoba-ku Sendai980-8578 Japan Shanghai Astronomical Observatory 80 Nandan Road Shanghai200030 China National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Graduate University for Advanced Studies Osawa 2-21-1 Mitaka Tokyo181-8588 Japan Astronomy Program Department of Physics and Astronomy Seoul National University 599 Gwanak-ro Gwanaku-gu Seoul151-742 Korea Republic of

We present the structure of the Milky Way stellar halo beyond Galactocentric distances of r = 50 kpc traced by blue horizontal-branch (BHB) stars, which are extracted from the survey data in the Hyper Suprime-Cam Subaru Strategic program (HSC-SSP). We select BHB candidates based on (g,r, i,z) photometry, where the z-band is on the Paschen series and the colors that involve the z-band are sensitive to surface gravity. About 450 BHB candidates are identified between r=50 kpc and 300 kpc, most of which are beyond the reach of previous large surveys including the Sloan Digital Sky Survey. We find that the global structure of the stellar halo in this range has substructures, which are especially remarkable in the GAMA15H and XMM-LSS fields in the HSC-SSP. We find that the stellar halo can be fitted to a single power-law density profile with an index of α 3.3 (3.5) with (without) these fields and its global axial ratio is q 2.2 (1.3). Thus, the stellar halo may be significantly disturbed and be made in a prolate form by halo substructures, perhaps associated with the Sagittarius stream in its extension beyond r ∼ 100 kpc. For a broken power-law model allowing different power-law indices inside/outside a break radius, we obtain a steep power-law slope of α ∼ 5 outside a break radius of 100 kpc (200 kpc) for the case with (without) GAMA15H and XMM-LSS. This radius of 200 kpc might be as close as a halo boundary if there is any, although larger BHB sample is required from further HSC-SSP survey to increase its statistical significance. Copyright © 2017, The Authors. All rights reserved.

关键词： Stars

AKARI mid-infrared slitless spectroscopic survey of star-forming galaxies at z < 0.5

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arXiv 2018年

作者： Ohyama, Y. Wada, T. Matsuhara, H. Takagi, T. Malkan, M. Goto, T. Egami, E. Lee, H.-M. Im, M. Kim, J.-H. Pearson, C. Inami, H. Oyabu, S. Usui, F. Burgarella, D. Mazyed, F. Imanishi, M. Jeong, W.-S. Miyaji, T. Tello, J. Díaz Nakagawa, T. Serjeant, S. Takeuchi, T.T. Toba, Y. White, G.J. Hanami, H. Ishigaki, T. Academia Sinica Institute of Astronomy and Astrophysics 11F of Astronomy-Mathematics Building AS/NTU No. 1 Sec. 4 Roosevelt Rd. Taipei10617 Taiwan Institute of Space and Astronautical Science Japan Aerospace Exploration Agency 3-1-1 Yoshinodai Chuo-ku Sagamihara Kanagawa252-5210 Japan Japan Space Forum Shin-Ochanomizu Urban Trinity Bldg. 2F 3-2-1 Kandasurugadai Chiyoda-ku Tokyo101-0062 Japan Division of Astronomy and Astrophysics University of California Los Angeles 430 Portola Plaza Box 951547 Los AngelesCA90095-1547 United States Dark Cosmology Centre Niels Bohr Institute University of Copenhagen Juliane Maries Vej 30 Copenhagen Ø2100 Denmark National Tsing hua University No. 101 Section 2 Kuang-Fu Road Hsinchu30013 Taiwan Steward Observatory University of Arizona 933 N. Cherry Ave TucsonAZ85721 United States Astronomy Program Department of Physics and Astronomy Seoul National University Shillim-Dong Kwanak-Gu Seoul151-742 Korea Republic of Subaru Telescope National Astronomical Observatory of Japan 650 North Aòhoku Place HiloHI96720 United States RAL Space STFC Rutherford Appleton Laboratory Chilton Didcot OxfordshireOX11 0QX United Kingdom Department of Physics and Astronomy Open University Walton Hall Milton KeynesMK7 6AA United Kingdom Oxford Astrophysics Denys Wilkinson Building University of Oxford Keble Rd OxfordOX1 3RH United Kingdom National Optical Astronomy Observatory 950 North Cherry Avenue TucsonAZ85719 United States CRAL Observatoire de Lyon 9 avenue Charles André Saint Genis Laval69561 France Graduate School of Science Nagoya University Furo-cho Chikusa-ku Nagoya Aichi464-8602 Japan Graduate School of Science University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan Center for Planetary Science Graduate School of Science Kobe University 7-1-48 Minatojima-Minamimachi Chuo-Ku Kobe650-0047 Japan Laboratoire d’Astrophysique de Marseille Pôle de l’Étoile Site de Château-Gombert 38 rue F

Context. Deep mid-infrared (MIR) surveys have revealed numerous strongly star-forming galaxies at redshift z . 2. Their MIR fluxes are produced by a combination of continuum and Polycyclic Aromatic Hydrocarbon (PAH) emission features. The PAH features can dominate the total MIR flux, but are difficult to measure without spectroscopy. Aims. We aim to study star-forming galaxies by using a blind spectroscopic survey at MIR wavelengths to understand evolution of their star formation rate (SFR) and specific SFR (SFR per stellar mass) up to z ' 0.5, by paying particular attention to their PAH properties. Methods. We conducted a low-resolution (R ' 50) slitless spectroscopic survey at 5–13 µm of 9 µm flux-selected sources (> 0.3 mJy) around the North Ecliptic Pole with the Infrared Camera (IRC) onboard AKARI. After removing 11 AGN candidates by using the IRC photometry, we identified 48 PAH galaxies with PAH 6.2, 7.7, and 8.6 µm features at z Copyright © 2018, The Authors. All rights reserved.

关键词： Polycyclic aromatic hydrocarbons

A multiline study of a high-mass young stellar object in the small magellanic cloud with alma: The detection of methanol gas at 0.2 solar metallicity

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arXiv 2018年

作者： Shimonishi, Takashi Watanabe, Yoshimasa Nishimura, Yuri Aikawa, Yuri Yamamoto, Satoshi Onaka, Takashi Sakai, Nami Kawamura, Akiko Frontier Research Institute for Interdisciplinary Sciences Tohoku University Aramakiazaaoba 6-3 Aoba-ku Sendai Miyagi980-8578 Japan Astronomical Institute Tohoku University Aramakiazaaoba 6-3 Aoba-ku Sendai Miyagi980-8578 Japan Faculty of Pure and Applied Sciences University of Tsukuba 1-1-1 Tennodai Tsukuba Ibaraki305-8577 Japan Tomonaga Center for the History of the Universe University of Tsukuba Tsukuba Ibaraki305-8571 Japan Institute of Astronomy University of Tokyo 2-21-1 Osawa Mitaka Tokyo181-0015 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Department of Astronomy Graduate School of Science University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan Department of Physics University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan Research Center for the Early Universe University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan RIKEN 2-1 Hirosawa Wako Saitama351-0198 Japan

We report the results of subparsec-scale submillimeter observations towards an embedded high-mass young stellar object in the Small Magellanic Cloud (SMC) with ALMA. Complementary infrared data obtained with the AKARI satellite and the Gemini South telescope are also presented. The target infrared point source is spatially resolved into two dense molecular cloud cores;one is associated with a high-mass young stellar object (YSO core), while another is not associated with an infrared source (East core). The two cores are dynamically associated but show different chemical characteristics. Emission lines of CS, C33S, H2CS, SO, SO2, CH3OH, H13CO+, H13CN, SiO, and dust continuum are detected from the observed region. Tentative detection of HDS is also reported. The first detection of CH3OH in the SMC has a strong impact on our understanding of the formation of complex organic molecules in metal-poor environments. The gas temperature is estimated to be ∼10 K based on the rotation analysis of CH3OH lines. The fractional abundance of CH3OH gas in the East core is estimated to be (0.5-1.5) × 10-8, which is comparable with or marginally higher than those of similar cold sources in our Galaxy despite a factor of five lower metallicity in the SMC. This work provides observational evidence that an organic molecule like CH3OH, which is largely formed on grain surfaces, can be produced even in a significantly lower metallicity environment compared to the solar neighborhood. A possible origin of cold CH3OH gas in the observed dense core is discussed. Copyright © 2018, The Authors. All rights reserved.

关键词： Astrophysics

Violations of a Bell inequality for entangled SU(1,1) coherent states based on dichotomic observables

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Physical Review A 2016年第4期93卷 042104-042104页

作者： Edwin E. Hach, III Paul M. Alsing Christopher C. Gerry School of Physics and Astronomy Rochester Institute of Technology 85 Lomb Memorial Drive Rochester New York 14623 USA Air Force Research Lab Rome New York 13441 USA Department of Physics and Astronomy Lehman College The City University of New York Bronx New York 10468-1589 USA Physics Program The Graduate Center CUNY New York New York 10016 USA

We study the violation of the Bell-Clauser-Horne-Shimony-Holt (Bell-CHSH) inequality for entangled SU(1,1) coherent states of the form proposed by Perelomov. Specifically, we examine Bell-CHSH violations by such states in the case in which distant observers Alice and Bob perform local, noncompact, SU(1,1) transformations characterized by hyperbolic angles on each of the subsystems and subsequently measure dichotomic observables, namely SU(1,1) parity operators. We find significant violations over a broad range of hyperbolic angles.

关键词： Nonlocality