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arXiv 2017年

作者： Meadows, Victoria S. Reinhard, Christopher T. Arney, Giada N. Parenteau, Mary N. Schwieterman, Edward W. Domagal-Goldman, Shawn D. Lincowski, Andrew P. Stapelfeldt, Karl R. Rauer, Heike DasSarma, Shiladitya Hegde, Siddharth Narita, Norio Deitrick, Russell Lyons, Timothy W. Siegler, Nicholas Lustig-Yaeger, Jacob University of Washington Astronomy Department SeattleWA United States NASA Astrobiology Institute Virtual Planetary Laboratory Team SeattleWA United States School of Earth and Atmospheric Sciences Georgia Institute of Technology AtlantaGA United States NASA Astrobiology Institute Alternative Earths Team RiversideCA United States Planetary Systems Laboratory NASA Goddard Space Flight Center 8800 Greenbelt Road GreenbeltMD20771 United States NASA Ames Research Center Exobiology Branch Mountain ViewCA94035 United States Department of Earth Sciences University of California RiversideCA United States NASA Postdoctoral Program Universities Space Research Association ColumbiaMD United States NASA Astrobiology Institute Alternative Earths Team RiversideCA United States Blue Marble Space Institute of Science SeattleWA United States Planetary Environments Laboratory NASA Goddard Space Flight Center 8800 Greenbelt Road GreenbeltMD20771 United States NASA Exoplanet Exploration Program Jet Propulsion Laboratory 4800 Oak Grove Drive PasadenaCA91109 German Aerospace Center Institute of Planetary Research Extrasolar Planets and Atmospheres Rutherfordstraße 2 Berlin12489 Department of Microbiology and Immunology University of Maryland School of Medicine Institute of Marine and Environmental Technology University System of Maryland MD21202 United States Carl Sagan Institute Cornell University IthacaNY14853 United States Cornell Center for Astrophysics and Planetary Science Cornell University IthacaNY14853 United States Astrobiology Center National Institutes of Natural Sciences 2-21-1 Osawa Mitaka Tokyo181-8588 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109-8099 United States

Here we review how environmental context can be used to interpret whether O2 is a biosignature in extrasolar planetary observations. This paper builds on the overview of current biosignature research discussed in Schwieterman et al. (2017), and provides an in-depth, interdisciplinary example of biosignature identification and observation that serves as a basis for the development of the general framework for biosignature assessment described in Catling et al., (2017). O2 is a potentially strong biosignature that was originally thought to be an unambiguous indicator for life at high-abundance. In exploring O2 as a biosignature, we describe the coevolution of life with the early Earth’s environment, and how the interplay of sources and sinks in the planetary environment may have resulted in suppression of O2 release into the atmosphere for several billion years, a false negative for biologically generated O2. False positives may also be possible, with recent research showing potential mechanisms in exoplanet environments that may generate relatively high abundances of atmospheric O2 without a biosphere being present. These studies suggest that planetary characteristics that may enhance false negatives should be considered when selecting targets for biosignature searches. Similarly our ability to interpret O2 observed in an exoplanetary atmosphere is also crucially dependent on environmental context to rule out false positive mechanisms. We describe future photometric, spectroscopic and time-dependent observations of O2 and the planetary environment that could increase our confidence that any observed O2 is a biosignature, and help discriminate it from potential false positives. The rich, interdisciplinary study of O2 illustrates how a synthesis of our understanding of life’s evolution and the early Earth, scientific computer modeling of star-planet interactions and predictive observations can enhance our understanding of biosignatures and guide and inform the developm

关键词： Extrasolar planets

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OGLE-2016-BLG-1045: A test of cheap space-based microlens parallaxes

arXiv

引用

arXiv 2017年

作者： Shin, I.-G. Udalski, A. Yee, J.C. Calchi Novati, S. Christie, G. Poleski, R. Mróz, P. Skowron, J. Szymanski, M.K. Soszynski, I. Pietrukowicz, P. Kozlowski, S. Ulaczyk, K. Pawlak, M. Natusch, T. Pogge, R.W. Gould, A. Han, C. Albrow, M.D. Chung, S.-J. Hwang, K.-H. Ryu, Y.-H. Jung, Y.K. Zhu, W. Lee, C.-U. Cha, S.-M. Kim, D.-J. Kim, H.-W. Kim, S.-L. Lee, Y. Lee, D.-J. Park, B.-G. Beichman, C. Bryden, G. Carey, S. Gaudi, B.S. Henderson, C.B. Shvartzvald, Y. Harvard-Smithsonian Center for Astrophysics 60 Garden St. CambridgeMA02138 United States Warsaw University Observatory Al. Ujazdowskie 4 Warszawa00-478 Poland Department of Physics University of Warwick Gibbet Hill Road CoventryCV4 7AL United Kingdom Auckland Observatory Auckland New Zealand AUT University Auckland New Zealand Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-Gu Daejeon34055 Korea Republic of Korea University of Science and Technology 217 Gajeong-ro Yuseong-gu Daejeon34113 Korea Republic of University of Canterbury Department of Physics and Astronomy Private Bag 4800 Christchurch8020 New Zealand School of Space Research Kyung Hee University Giheung-gu Yongin Gyeonggi-do17104 Korea Republic of Department of Physics Chungbuk National University Cheongju28644 Korea Republic of IPAC Mail Code 100-22 California Institute of Technology 1200 E. California Boulevard PasadenaCA91125 United States NASA Exoplanet Science Institute California Institute of Technology PasadenaCA91125 United States Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States Spitzer Science Center MS 220-6 California Institute of Technology PasadenaCA United States Department of Astronomy Ohio State University 140 W. 18th Ave. ColumbusOH43210 United States Max-Planck-Institute for Astronomy Königstuhl 17 Heidelberg69117 Germany OGLE Collaboration µFUN Collaboration KMTNet Group Spitzer Team NASA Postdoctoral Program Fellow

Microlensing is a powerful and unique technique to probe isolated objects in the Galaxy. To study the characteristics of these interesting objects based on the microlensing method, measurement of the microlens parallax is required to determine the properties of the lens. Of the various methods to measure microlens parallax, the most routine way is to make simultaneous ground- and space-based observations, i.e., by measuring the space-based microlens parallax. However, space-based campaigns usually require "expensive" resources. Gould & Yee (2012) proposed an idea called the "cheap space-based microlens parallax" that can measure the lens-parallax using only two or three space-based observations of high-magnification events (as seen from Earth). This cost-effective observation strategy to measure microlens parallaxes could be used by space-borne telescopes to build a complete sample for studying isolated objects. This would enable a direct measurement of the mass function including both extremely low-mass objects and high-mass stellar remnants. However, to adopt this idea requires a test to check how it would work in actual situations. Thus, we present the first practical test of this idea using the high-magnification microlensing event OGLE-2016-BLG-1045, for which a subset of Spitzer observations fortuitously duplicate the prescription of Gould & Yee (2012). From the test, we confirm that the measurement of the lens-parallax adopting this idea has sufficient accuracy to determine the physical properties of the isolated lens. Copyright © 2017, The Authors. All rights reserved.

关键词： Geometrical optics

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Erratum: 'Evolution of Intrinsic Scatter in the SFR–Stellar Mass Correlation at 0.5

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The Astrophysical Journal Letters 2018年第2期864卷

作者： Peter Kurczynski Eric Gawiser Viviana Acquaviva Eric F. Bell Avishai Dekel Duilia F. de Mello Henry C. Ferguson Jonathan P. Gardner Norman A. Grogin Yicheng Guo Philip F. Hopkins Anton M. Koekemoer David C. Koo Seong-Kook Lee Bahram Mobasher Joel R. Primack Marc Rafelski Emmaris Soto Harry I. Teplitz Department of Physics and Astronomy Rutgers University Piscataway NJ 08854 USA New York City College of Technology Brooklyn NY 11201 USA Department of Astronomy University of Michigan Ann Arbor MI 48109 USA Center for Astrophysics and Planetary Science Racah Institute of Physics The Hebrew University Jerusalem 91904 Israel Laboratory for Observational Cosmology Astrophysics Science Division Code 665 Goddard Space Flight Center Greenbelt MD 20771 USA Department of Physics The Catholic University of America Washington DC 20064 USA Space Telescope Science Institute 3700 San Martin Drive Baltimore MD 21218 USA UCO/Lick Observatory Department of Astronomy and Astrophysics University of California Santa Cruz CA USA TAPIR Mailcode 350-17 California Institute of Technology Pasadena CA 91125 USA Department of Astronomy and Theoretical Astrophysics Center University of California Berkeley Berkeley CA 94720 USA Center for the Exploration of the Origin of the Universe Department of Physics and Astronomy Seoul National University Seoul 151-742 Republic of Korea Department of Physics and Astronomy University of California Riverside CA USA Department of Physics University of California Santa Cruz CA 95064 USA NASA Postdoctoral Program Fellow. Infrared Processing and Analysis Center MS 100-22 Caltech Pasadena CA 91125 USA

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OGLE-2015-BLG-1482L: THE FIRST ISOLATED LOW-MASS MICROLENS IN THE GALACTIC BULGE

arXiv

引用

arXiv 2017年

作者： Chung, S.-J. Zhu, W. Udalski, A. Lee, C.-U. Ryu, Y.-H. Jung, Y.K. Shin, I.-G. Yee, J.C. Hwang, K.-H. Gould, A. Albrow, M. Cha, S.-M. Han, C. Kim, D.-J. Kim, H.-W. Kim, S.-L. Kim, Y.-H. Lee, Y. Park, B.-G. Pogge, R.W. Poleski, R. Mróz, P. Pietrukowicz, P. Skowron, J. Szymanski, M.K. Soszynski, I. Kozlowski, S. Ulaczyk, K. Pawlak, M. Beichman, C. Bryden, G. Novati, S. Calchi Carey, S. Fausnaugh, M. Gaudi, B.S. Henderson, Calen B. Shvartzvald, Y. Wibking, B. Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-Gu Daejeon34055 Korea Republic of Korea Universit of Science and Technolo 217 Gajeon -ro Yuseon Daejeon34113 Department of Astronomy Ohio State University 140 W 18th Ave ColumbusOH43210 United States Warsaw University Observatory AI Ujazdowskie 4 Warszawa00-478 Poland Harvard-Smithsonian Center for Astrophysics 60 Garden St. CambridgeMA02138 United States Max-Planck-Institute for Astronomy Königstuhl 17 Heidelberg69117 Germany Department of Physics and Astronomy University of Canterbury Private Bag 4800 Christchurch New Zealand School of Space Research Kyung Hee University Giheung-gu Yongin Gyeonggi-do17104 Korea Republic of Department of Physics Chungbuk National University Cheongju361-763 Korea Republic of De artment of Ph sics Uni ersit of War ick Gibbet Hill Road Co entrCV4 7AL United Kingdom NASA Exoplanet Science Institute MS 100-22 California Institute of Technology PasadenaCA91125 United States Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States IPAC Mail Code 100-22 Caltech 1200 E California Blvd PasadenaCA91125 United States 84084 Italy Spitzer Science Center MS 220-6 California Institute of Technology PasadenaCA United States NASA Postdoctoral Program Fellow KMTNet Collaboration The OGLE Collaboration Spitzer Team

We analyze the single microlensing event OGLE-2015-BLG-1482 simultaneously observed from two ground-based surveys and from Spitzer. The Spitzer data exhibit finite-source effects due to the passage of the lens close to or directly over the surface of the source star as seen from Spitzer. Such finite-source effects generally yield measurements of the angular Einstein radius, which when combined with the microlens parallax derived from a comparison between the ground-based and the Spitzer light curves, yields the lens mass and lens-source relative parallax. From this analysis, we find that the lens of OGLE-2015-BLG-1482 is a very low-mass star with the mass 0.10±0.02 M or a brown dwarf with the mass 55±9 MJ, which are respectively located at DLS = 0.80±0.19 kpc and DLS = 0.54±0.08 kpc, where DLS is the distance between the lens and the source, and thus it is the first isolated low-mass microlens that has been decisively located in the Galactic bulge. The degeneracy between the two solutions is severe (∆χ2 = 0.3). The fundamental reason for the degeneracy is that the finite-source effect is seen only in a single data point from Spitzer and this single data point gives rise to two solutions for ρ, the angular size of the source in units of the angular Einstein ring radius. Because the ρ degeneracy can be resolved only by relatively high cadence observations around the peak, while the Spitzer cadence is typically ∼ 1 day−1, we expect that events for which the finite-source effect is seen only in the Spitzer data may frequently exhibit this ρ degeneracy. For OGLE-2015-BLG-1482, the relative proper motion of the lens and source for the low-mass star is µrel = 9.0 ±1.9 mas yr−1, while for the brown dwarf it is µrel = 5.5 ± 0.5 mas yr−1. Hence, the degeneracy can be resolved within ∼ 10 yrs from direct lens imaging by using next-generation instruments with high spatial resolution. Keywords: brown dwarfs - gravitational lensing: micro - stars: fundamental parameters Copyright

关键词： Geometrical optics

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Eddies spatial variability at Makassar Strait – Flores Sea

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IOP Conference Series: Earth and Environmental science 2017年第1期54卷

作者： F Nuzula M L Syamsudin L P S Yuliadi N P Purba Martono Bachelor Degree Marine Science Program Faculty of Fisheries and Marine Science Padjadjaran University Jl. Raya Bandung-Sumedang Km. 21 Jatinangor West Java 45363 Indonesia Department of Marine Science Padjadjaran University Jl. Raya Bandung-Sumedang Km. 21 Jatinangor West Java 45363 Indonesia Science Technology and Atmosphere Center National Institute of Aeronautics and Space (LAPAN) Jl. Doktor Djunjunan No. 133 Padjadjaran Cicendo Bandung City West Java 40173 Indonesia

This study was aimed to get the distribution of eddies spatially and temporally from Makassar Waters (MW) to Flores Sea (FS), as well as its relations with the upwelling, the downwelling, and chlorophyll-a concentration. The study area extends from 115º–125º E to 2.5º–8º S. The datasets were consisted of monthly geostrophic currents, sea surface heights, sea surface temperatures, and chlorophyll-a from 2008 – 2012. The results showed that eddies which found at Makassar Strait (MS) has the highest diameter and speed of 255.3 km and 21.4 cm/s respectively, while at the southern MW has 266.4 km and 15.6 cm/s, and at FS has 182.04 km and 11.4 cm/s. From a total of 51 eddies found, the majority of eddies type was anticyclonic. At MS and FS, eddies formed along the year, whereas at southern MW were found missing in West Season. Moreover, the chlorophyll-a concentration was consistently higher at the eddies area. Even though, the correlation among eddies and the upwelling downwelling phenomena was not significantly as shown by sea surface temperatures value.

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Galaxy clusters selected via the Sunyaev-Zel’dovich effect in the SPTpol 100-Square-Degree survey

arXiv

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arXiv 2019年

作者： Huang, N. Bleem, L.E. Stalder, B. Ade, P.A.R. Allen, S.W. Anderson, A.J. Austermann, J.E. Avva, J.S. Beall, J.A. Bender, A.N. Benson, B.A. Bianchini, F. Bocquet, S. Brodwin, M. Carlstrom, J.E. Chang, C.L. Chiang, H.C. Citron, R. Corbett Moran, C. Crawford, T.M. Crites, A.T. de Haan, T. Dobbs, M.A. Everett, W. Floyd, B. Gallicchio, J. George, E.M. Gilbert, A. Gladders, M.D. Guns, S. Gupta, N. Halverson, N.W. Harrington, N. Henning, J.W. Hilton, G.C. Holder, G.P. Holzapfel, W.L. Hrubes, J.D. Hubmayr, J. Irwin, K.D. Khullar, G. Knox, L. Lee, A.T. Li, D. Lowitz, A. McDonald, M. McMahon, J.J. Meyer, S.S. Mocanu, L.M. Montgomery, J. Nadolski, A. Natoli, T. Nibarger, J.P. Noble, G. Novosad, V. Padin, S. Patil, S. Pryke, C. Reichardt, C.L. Ruhl, J.E. Saliwanchik, B.R. Saro, A. Sayre, J.T. Schaffer, K.K. Sharon, K. Sievers, C. Smecher, G. Stark, A.A. Story, K.T. Tucker, C. Vanderlinde, K. Veach, T. Vieira, J.D. Wang, G. Whitehorn, N. Wu, W.L.K. Department of Physics University of California BerkeleyCA94720 United States High Energy Physics Division Argonne National Laboratory 9700 S. Cass Avenue ArgonneIL60439 United States Kavli Institute for Cosmological Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States LSST 950 N Cherry Ave TucsonAZ United States Cardiff University CardiffCF10 3XQ United Kingdom Kavli Institute for Particle Astrophysics and Cosmology Stanford University 452 Lomita Mall StanfordCA94305 United States Department of Physics Stanford University 382 Via Pueblo Mall StanfordCA94305 United States SLAC National Accelerator Laboratory 2575 Sand Hill Road Menlo ParkCA94025 United States Fermi National Accelerator Laboratory MS209 P.O. Box 500 BataviaIL60510 United States NIST Quantum Devices Group 325 Broadway Mailcode 817.03 BoulderCO80305 United States Department of Astronomy and Astrophysics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States School of Physics University of Melbourne ParkvilleVIC3010 Australia Department of Physics Ludwig-Maximilians-Universität Scheinerstr. 1 München81679 Germany Department of Physics and Astronomy University of Missouri 5110 Rockhill Road Kansas CityMO64110 United States Department of Physics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Enrico Fermi Institute University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Department of Physics McGill University 3600 Rue University MontrealQCH3A 2T8 Canada School of Mathematics Statistics & Computer Science University of KwaZulu-Natal Durban South Africa University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States TAPIR Walter Burke Institute for Theoretical Physics California Institute of Technology 1200 E California Blvd PasadenaCA91125 United States California Institute of Technology MS 249-17 1216 E. California Blvd. PasadenaCA91125

We present a catalog of galaxy cluster candidates detected in 100 square degrees surveyed with the SPTpol receiver on the South Pole Telescope. The catalog contains 89 candidates detected with a signal-to-noise ratio greater than 4.6. The candidates are selected using the Sunyaev-Zel’dovich effect at 95 and 150 GHz. Using both space- and ground-based optical and infrared telescopes, we have confirmed 81 candidates as galaxy clusters. We use these follow-up images and archival images to estimate photometric redshifts for 66 galaxy clusters and spectroscopic observations to obtain redshifts for 13 systems. An additional 2 galaxy clusters are confirmed using the overdensity of near-infrared galaxies only, and are presented without redshifts. We find that 15 candidates (18% of the total sample) are at redshift of z ≥ 1.0, with a maximum confirmed redshift of zmax = 1.38 ± 0.10. We expect this catalog to contain every galaxy cluster with M500c > 2.6×1014M☉h−701 and z > 0.25 in the survey area. The mass threshold is approximately constant above z = 0.25, and the complete catalog has a median mass of approximately M500c = 2.7 × 1014M☉h−701. Compared to previous SPT works, the increased depth of the millimeter-wave data (11.2 and 6.5 µK-arcmin at 95 and 150 GHz, respectively) makes it possible to find more galaxy clusters at high redshift and lower mass. Copyright © 2019, The Authors. All rights reserved.

关键词： Infrared devices

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Combining spitzer parallax and Keck II adaptive optics imaging to measure the mass of a solar-like star orbited by a cold gaseous planet discovered by microlensing

arXiv

引用

arXiv 2017年

作者： Beaulieu, J.-P. Batista, V. Bennett, D.P. Marquette, J.-B. Blackman, J.W. Cole, A.A. Coutures, C. Danielski, C. Dominis-Prester, D. Donatowicz, J. Fukui, A. Koshimoto, N. Lončaric, C. Morales, J.C. Sumi, T. Suzuki, D. Henderson, C. Shvartzvald, Y. Beichman, C. School of Physical Sciences University of Tasmania Private Bag 37 HobartTAS7001 Australia Sorbonne Universités UPMC Université Paris 6 CNRS UMR 7095 Institut dAstrophysique de Paris 98 bis bd Arago Paris75014 France Laboratory for Exoplanets and Stellar Astrophysics NASA/Goddard Space Flight Center GreenbeltMD20771 United States Laboratoire d’Astrophysique de Bordeaux Univ. Bordeaux CNRS B18N allée Geoffroy Saint-Hilaire Pessac33615 France GEPI Observatoire de Paris Section de Meudon 5 place Jules Janssen Meudon92195 France Department of Physics University of Rijeka Radmile Matejčić 2 Rijeka51000 Croatia Technische Universitt Wien Karlsplatz 13 Wien1040 Austria Okayama Astrophysical Observatory National Astronomical Observatory of Japan Asakuchi Okayama719-0232 Japan Department of Earth and Space Science Graduate School of Science Osaka University 1-1 Machikaneyama Toyonaka Osaka560-0043 Japan Campus UAB Carrer de Can Magrans s/n Cerdanyola del VallsE-08193 Spain Jet Propulsion Laboratory California Institute of Technology 4800 Oak Grove Drive PasadenaCA91109 United States NASA Exoplanet Science Institute California Institute of Technology Jet Propulsion Laboratory PasadenaCA91125 United States PAC/NExScI Mail Code 100-22 Caltech 1200 East California Boulevard PasadenaCA91125 NASA Postdoctoral Program

To obtain accurate mass measurements for cold planets discovered by microlensing, it is usually necessary to combine light curve modeling with at least two lens mass-distance relations. Often, a constraint on the Einstein ring radius measurement is obtained from the caustic crossing time: This is supplemented by secondary constraints such as precise parallax measurements and/or measures of the lens luminosity using high angular resolution observations. In the discovery paper of the planetary system OGLE-2014-BLG-0124Lb, the OGLE ground-based observations were combined with simultaneous Spitzer observations, providing good measurements of the mass ratio and projeced separation of the planetary system. The parallax was also well-measured, but the photometric data failed to tightly constrain the Einstein ring radius, ΘE. As a consequence, the physical parameters are therefore poorly constrained in the original study. We resolved the source+lens star from subarcsecond blends in H band using adaptive optics (AO) observations with NIRC2 mounted on Keck II telescope. We identify additional flux, coincident with the source to within 160 mas. We estimate the potential contributions to this blended light (chance-aligned star, additional companion to the lens or to the source) and find that 85% of of the NIR flux is due to the lens star at HL = 16.63 ± 0.06 and KL = 16.46 ±0.06. We combined the parallax constraint and the AO constraint to derive the physical parameters of the system. The lensing system is composed of a mid-late type G main sequence star of ML = 0.89 ± 0.05 Mo located at DL = 3.6 ± 0.3 kpc in the Galactic disk. Taking the mass ratio and projected separation from the original study leads to a planet of Mp = 0.64 ± 0.044 MJupiter at 3.48 ± 0.22 AU. Excellent parallax measurement from simultaneous ground-space observations have been obtained on the microlensing event OGLE-2014-BLG-0124, but it is only when they are combined with ∼ 30 min of Keck II AO observations

关键词： Geometrical optics

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Erratum to: An Update of Non-iterative Solutions for Surface Fluxes Under Unstable Conditions

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Boundary-Layer Meteorology 2016年第1期161卷 225-228页

作者： Li, Yubin Gao, Zhiqiu Li, Dan Chen, Fei Yang, Yuanjian Sun, Liang Collaborative Innovation Center on Forecast and Evaluation of Meteorological Disasters School of Geography and Remote Sensing Nanjing University of Information Science and Technology Nanjing China State Key Laboratory of Atmospheric Boundary Layer Physics and Atmospheric Chemistry Institute of Atmospheric Physics Chinese Academy of Sciences Beijing China Program of Atmospheric and Oceanic Sciences Princeton University Princeton USA National Center for Atmospheric Research Boulder USA Key Laboratory of Atmospheric Sciences and Satellite Remote Sensing of Anhui Province Anhui Institute of Meteorological Sciences Hefei China School of Earth and Space Sciences University of Science and Technology of China Hefei China

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Erratum to: Vol. 35 No. 1 Publisher’s Erratum

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Chinese Journal of Oceanology and Limnology 2017年第2期35卷 466-467页

作者： Shuangyan He Mingxia He Jürgen Fischer Dongliang Yuan Peng Xu Tengfei Xu Xianping Yang Leonid Sokoletsky Xiaodao Wei Fang Shen Juhong Zou Maohua Guo Songxue Cui Wu Zhou Dalu Gao Guangzhen Jin Xianqing Lü Fuwen Qiu Wendong Fang Aijun Pan Jing Cha Shanwu Zhang Jiang Huang Tao Wang Yongzhou Cheng Xiaoyan Chen Zhaopu Liu Xiaohua Long Zhishuai Hou Haishen Wen Jifang Li Feng He Qun Liu Jinhuan Wang Biao Guan Qinglong Wang Md. Shahjahan Md. Farajul Kabir Kizar Ahmed Sumon Lipi Rani Bhowmik Harunur Rashid Shu Li Kefu Yu Jianxin Zhao Yuexing Feng Tianran Chen Shun Zhou Yichao Ren Christopher M. Pearce Shuanglin Dong Xiangli Tian Qinfeng Gao Fang Wang Liming Liu Rongbin Du Xiaoling Zhang Shichun Sun Song Feng Jianing Lin Song Sun Fang Zhang Zhipeng Zhang Xuexi Tang Haitian Tang Jingjing Song Jian Zhou Hongjun Liu Qixiang Wang Kuimei Qian Xia Liu Yuwei Chen Chengjun Sun Fenghua Jiang Wei Gao Xiaoyun Li Yanzhen Yu Xiaofei Yin Yong Wang Haibing Ding Zhongmin Sun Yongqiang Wang Pengcheng Yan Hui Guo Jianting Yao Jiro Tanaka Hiroshi Kawai Na Song Muyan Chen Tianxiang Gao Takashi Yanagimoto Xia Lu Sheng Luan Jie Kong Longyang Hu Yong Mao Shengping Zhong Yan Liu Weihong Zhao Caiyan Li Hui Miao Ocean Remote Sensing Institute Ocean University of China Qingdao China Institute for Space Sciences Freie Universität Berlin Berlin Germany Ocean College Zhejiang University Hangzhou China Key Laboratory of Ocean Circulation and Waves (KLOCAW) Institute of Oceanology Chinese Academy of Sciences Qingdao China Qingdao Collaborative Innovation Center of Marine Science and Technology Qingdao China University of Chinese Academy of Sciences Beijing China First Institute of Oceanography State Oceanic Administration Qingdao China State Key Laboratory of Estuarine and Coastal Research East China Normal University Shanghai China National Satellite Ocean Application Service Beijing China Key Laboratory of Space Ocean Remote Sensing and Application SOA Beijing China Key Laboratory of Physical Oceanography (Ocean University of China) Ministry of Education Qingdao China Key Lab of Marine Science and Numerical Modeling First Institute of Oceanography SOA Qingdao China Third Institute of Oceanography State Oceanic Administration Xiamen China State Key Laboratory of Tropical Oceanography South China Sea Institute of Oceanology Chinese Academy of Sciences Guangzhou China Jiangsu Provincial Key Laboratory of Marine Biology College of Resources and Environmental Sciences Nanjing Agricultural University Nanjing China Fisheries College Ocean University of China Qingdao China Key Laboratory of Mariculture Ministry of Education Ocean University of China Qingdao China Department of Fisheries Management Bangladesh Agricultural University Mymensingh Bangladesh Sado Marine Biological Station Faculty of Science Niigata University Sado Niigata Japan Department of Aquatic Ecology and Water Quality Management Wageningen University Wageningen University and Research Centre Amsterdam The Netherlands Science and Math Program Asian University for Women Chittagong Bangladesh Key laboratory of Marginal Sea Geology South China Sea Institute of Oceanology Chinese Academy of Sciences

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Concurrent starbursts in molecular gas disks within a pair of colliding galaxies at z = 1.52

arXiv

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arXiv 2018年

作者： Silverman, J.D. Daddi, E. Rujopakarn, W. Renzini, A. Mancini, C. Bournaud, F. Puglisi, A. Rodighiero, G. Liu, D. Sargent, M. Arimoto, N. Béthermin, M. Fensch, J. Hayward, C.C. Kartaltepe, J. Kashino, D. Koekemoer, A. Magdis, G. McCracken, H.J. Nagao, T. Sheth, K. Smolčić, V. Valentino, F. Kavli Institute for the Physics and Mathematics of the Universe University of Tokyo Kashiwa277-8583 Japan Laboratoire AIM CEA/DSM-CNRS-Universite Paris Diderot Irfu/Service d'Astrophysique CEA Saclay Department of Physics Faculty of Science Chulalongkorn University 254 Phayathai Road Pathumwan Bangkok10330 Thailand Don Kaeo Mae Rim Chiang Mai50180 Thailand Kavli Institute for the Physics and Mathematics of the Universe Todai Institutes for Advanced Study University of Tokyo Kashiwa277-8583 Japan Instituto Nazionale de Astrofisica Osservatorio Astronomico di Padova v.co dell'Osservatorio 5 PadovaI-35122 Italy Dipartimento di Fisica e Astronomia Universita di Padova vicolo Osservatorio 3 Padova35122 Italy Astronomy Centre Department of Physics and Astronomy University of Sussex BrightonBN1 9QH United Kingdom Astronomy Program Department of Physics and Astronomy Seoul National University 599 Gwanak-ro Gwanak-gu Seoul151-742 Korea Republic of Subaru Telescope 650 North A'ohoku Place Hilo Hawaii96720 United States European Southern Observatory Karl-Schwarzschild-Str. 2 Garching85748 Germany European Southern Observatory Karl-Schwarzschild-Str. 2 Garching bei München85748 Germany Center for Computational Astrophysics Flatiron Institute 162 Fifth Avenue New YorkNY10010 United States School of Physics and Astronomy Rochester Institute of Technology 84 Lomb Memorial Drive RochesterNY14623 United States Institute of Astronomy ETH Zürich Wolfgang-Pauli-Strasse 27 ZürichCH-8093 Switzerland Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Cosmic DAWN Centre Niels Bohr Institute University of Copenhagen Juliane Mariesvej 30 Copenhagen2100 Denmark Institut d'Astrophysique de Paris CNRS UMR 7095 and UPMC 98bis boulevard Arago ParisF-75014 France Graduate School of Science and Engineering Ehime University 2-5 Bunkyo-cho Matsuyama790-8577 Japan NASA Headquaters 300 E. St SW WashingtonDC2054

We report on the discovery of a merger-driven starburst at z = 1:52, PACS-787, based on high signal-to-noise ALMA observations. CO(5-4) and continuum emission (850μm) at a spatial resolution of 0.3" reveal two compact (r1/2 ∼ 1 kpc) and interacting molecular gas disks at a separation of 8.6 kpc thus indicative of an early stage in a merger. With a SFR of 991 Mo yr-1, this starburst event should occur closer to final coalescence, as usually seen in hydrodynamical simulations. From the CO size, inclination, and velocity profile for both disks, the dynamical mass is calculated through a novel method that incorporates a calibration using simulations of galaxy mergers. Based on the dynamical mass, we measure (1) the molecular gas mass, independent from the CO luminosity, (2) the ratio of the total gas mass and the CO(1 - 0) luminosity (αCO ≡ Mgas/L'CO1-0), and (3) the gas-to-dust ratio, with the latter two being lower than typically assumed. We find that the high star formation, triggered in both galaxies, is caused by a set of optimal conditions: a high gas mass/fraction, a short depletion time (τdepl = 85 and 67 Myrs) to convert gas into stars, and the interaction of likely counter-rotating molecular disks that may accelerate the loss of angular momentum. The state of interaction is further established by the detection of di_use CO and continuum emission, tidal debris that bridges the two nuclei and is associated with stellar emission seen by HST/WFC3. This observation demonstrates the power of ALMA to study the dynamics of galaxy mergers at high redshift. Copyright © 2018, The Authors. All rights reserved.

关键词： Galaxies

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