Annual Report ESO Staff Papers 2018
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Chemical Evolution of Protoplanetary Disks-The Effects of Viscous Accretion, Turbulent Mixing and Disk Winds
Draft version June 5, 2018 Preprint typeset using LATEX style emulateapj v. 11/10/09 CHEMICAL EVOLUTION OF PROTOPLANETARY DISKS – THE EFFECTS OF VISCOUS ACCRETION, TURBULENT MIXING AND DISK WINDS D. Heinzeller1 and H. Nomura Department of Astronomy, Graduate School of Science, Kyoto University, Kyoto 606-8502, Japan and C. Walsh and T. J. Millar Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast, BT7 1NN, UK Draft version June 5, 2018 ABSTRACT We calculate the chemical evolution of protoplanetary disks considering radial viscous accretion, vertical turbulent mixing and vertical disk winds. We study the effects on the disk chemical structure when different models for the formation of molecular hydrogen on dust grains are adopted. Our gas- phase chemistry is extracted from the UMIST Database for Astrochemistry (Rate06) to which we have added detailed gas-grain interactions. We use our chemical model results to generate synthetic near- and mid-infrared LTE line emission spectra and compare these with recent Spitzer observations. Our results show that if H2 formation on warm grains is taken into consideration, the H2O and OH abundances in the disk surface increase significantly. We find the radial accretion flow strongly influences the molecular abundances, with those in the cold midplane layers particularly affected. On the other hand, we show that diffusive turbulent mixing affects the disk chemistry in the warm molecular layers, influencing the line emission from the disk and subsequently improving agreement with observations. We find that NH3, CH3OH, C2H2 and sulphur-containing species are greatly enhanced by the inclusion of turbulent mixing. -
Proper Motions of Young Stars in Chamaeleon II
A&A 556, A144 (2013) Astronomy DOI: 10.1051/0004-6361/201321217 & c ESO 2013 Astrophysics Proper motions of young stars in Chamaeleon II. New kinematical candidate members of Chamaeleon I and II Belén López Martí1, Francisco Jiménez-Esteban1,2,3, Amelia Bayo4,5, David Barrado1,6, Enrique Solano1,2, Hervé Bouy1, and Carlos Rodrigo1,2 1 Centro de Astrobiología (INTA-CSIC), Departamento de Astrofísica, PO Box 78, 28261 Villanueva de la Cañada, Madrid, Spain e-mail: [email protected] 2 Spanish Virtual Observatory, 2869 Madrid, Spain 3 Suffolk University, Madrid Campus, C/ Valle de la Viña 3, 28003 Madrid, Spain 4 European Southern Observatory, Alonso de Córdova 3107, Vitacura, Santiago, Chile 5 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany 6 Calar Alto Observatory, Centro Astronómico Hispano-Alemán, C/ Jesús Durbán Remón 2-2, 04004 Almería, Spain Received 1 February 2013 / Accepted 1 July 2013 ABSTRACT Context. The Chamaeleon star-forming region has been extensively studied in the last decades. However, most studies have been confined to the densest parts of the clouds. In a previous paper, we analysed the kinematical properties of the spectroscopically confirmed population of the Chamaeleon I and II clouds. Aims. We want to search for new kinematical candidate members to the Chamaeleon I and II moving groups, extending the studied area beyond the clouds, and to characterize these new populations using available information from public databases and catalogues. We also want to check if the populations of the moving groups are confined to the present dark clouds. Methods. Kinematic candidate members were initially selected on the basis of proper motions and colours using the Fourth US Naval Observatory CCD Astrograph Catalog (UCAC4). -
Source-Plane Reconstruction of the Giant Gravitational Arc in A2667: a Candidate Wolf–Rayet Galaxy At
SOURCE-PLANE RECONSTRUCTION OF THE GIANT GRAVITATIONAL ARC IN A2667: A CANDIDATE WOLF–RAYET GALAXY AT z ∼ 1 Shuo Cao, Giovanni Covone, Eric Jullo, Johan Richard, Luca Izzo, Zong-Hong Zhu To cite this version: Shuo Cao, Giovanni Covone, Eric Jullo, Johan Richard, Luca Izzo, et al.. SOURCE-PLANE RE- CONSTRUCTION OF THE GIANT GRAVITATIONAL ARC IN A2667: A CANDIDATE WOLF– RAYET GALAXY AT z ∼ 1. Astronomical Journal, American Astronomical Society, 2015, 149, pp.8. 10.1088/0004-6256/149/1/3. hal-01109685 HAL Id: hal-01109685 https://hal.archives-ouvertes.fr/hal-01109685 Submitted on 26 Jan 2015 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. The Astronomical Journal, 149:3 (8pp), 2015 January doi:10.1088/0004-6256/149/1/3 C 2015. The American Astronomical Society. All rights reserved. SOURCE-PLANE RECONSTRUCTION OF THE GIANT GRAVITATIONAL ARC IN A2667: A CANDIDATE WOLF–RAYET GALAXY AT z ∼ 1 Shuo Cao1,2, Giovanni Covone2,3, Eric Jullo4, Johan Richard5, Luca Izzo6,7, and Zong-Hong Zhu1 1 Department of Astronomy, Beijing Normal University, 100875 Beijing, China; [email protected] 2 Dipartimento di Scienze Fisiche, Universita` di Napoli “Federico II,” Via Cinthia, I-80126 Napoli, Italy 3 INFN Sez. -
Magnificent Spiral Galaxy Is Being Stretched by Passing Neighbor 27 May 2021, by Ray Villard
Magnificent spiral galaxy is being stretched by passing neighbor 27 May 2021, by Ray Villard animals—the gingham dog and calico cat—who got into a spat and ate each other. It's not so dramatic in this case. The galaxies are only getting a little chewed up because of their close proximity. The magnificent spiral galaxy NGC 2276 looks a bit lopsided in this Hubble Space Telescope snapshot. A bright hub of older yellowish stars normally lies directly in the center of most spiral galaxies. But the bulge in NGC 2276 looks offset to the upper left. What's going on? In reality, a neighboring galaxy to the right of NGC 2276 (NGC 2300, not seen here) is gravitationally tugging on its disk of blue stars, pulling the stars on one side of the galaxy outward to distort the galaxy's normal fried-egg appearance. This sort of "tug of war" between galaxies that pass close enough to feel each other's gravitational pull is not uncommon in the universe. But, like Credit: NASA, ESA, STScI, Paul Sell (University of snowflakes, no two close encounters look exactly Florida) alike. In addition, newborn and short-lived massive stars form a bright, blue arm along the upper left edge of The myriad spiral galaxies in our universe almost NGC 2276. They trace out a lane of intense star all look like fried eggs. A central bulge of aging formation. This may have been triggered by a prior stars is like the egg yolk, surrounded by a disk of collision with a dwarf galaxy. -
Publications for Geraint Lewis 2021 2020
Publications for Geraint Lewis 2021 R., Horner, J., Wright, D., Carter, B., Morton, T., Spina, L., Li, T., Koposov, S., Erkal, D., Ji, A., Shipp, N., Hilmi, T., Bland-Hawthorn, J., Hayden, M., Lewis, G., Sharma, S., Kuehn, K., Pace, A., Lewis, G., Mackey, D., Wan, Z., Bland- Simpson, J., et al (2021). The GALAH Survey: Using galactic Hawthorn, J., Sharma, S., et al (2021). Broken into pieces: archaeology to refine our knowledge of TESS target stars. ATLAS and Aliqa Uma as one single stream. The Astrophysical Monthly Notices of the Royal Astronomical Society, 504(4), Journal, 911(2), 149. <a href="http://dx.doi.org/10.3847/1538- 4968-4989. <a 4357/abeb18">[More Information]</a> href="http://dx.doi.org/10.1093/mnras/stab1052">[More Information]</a> Sharma, S., Hayden, M., Bland-Hawthorn, J., Stello, D., Buder, S., Zinn, J., Kallinger, T., Asplund, M., De Silva, G., D'Orazi, Oliver, W., Elahi, P., Lewis, G., Power, C. (2021). The V., Kos, J., Lewis, G., Lin, J., Zucker, D., Chen, B., Huber, D., hierarchical structure of galactic haloes: Classification and Kafle, P., Khanna, S., et al (2021). Fundamental relations for characterization with halo-optics. Monthly Notices of the Royal the velocity dispersion of stars in the Milky Way. Monthly Astronomical Society, 501(3), 4420-4437. <a Notices of the Royal Astronomical Society, 506(2), 1761-1776. href="http://dx.doi.org/10.1093/mnras/staa3879">[More <a href="http://dx.doi.org/10.1093/mnras/stab1086">[More Information]</a> Information]</a> Arentsen, A., Starkenburg, E., Aguado, D., Martin, N., Placco, Wiseman, P., Sullivan, M., Smith, M., Frohmaier, C., Vincenzi, V., Carlberg, R., Gonz�lez Hern�ndez, J., Hill, V., M., Graur, O., Popovic, B., Armstrong, P., Brout, D., Davis, T., Jablonka, P., Kordopatis, G., Lewis, G., Wan, Z., et al (2021). -
Optical Spectroscopic Monitoring Observations of a T Tauri Star V409 Tau
International Journal of Astronomy and Astrophysics, 2019, 9, 321-334 http://www.scirp.org/journal/ijaa ISSN Online: 2161-4725 ISSN Print: 2161-4717 Optical Spectroscopic Monitoring Observations of a T Tauri Star V409 Tau Hinako Akimoto, Yoichi Itoh Nishi-Harima Astronomical Observatory, Center for Astronomy, University of Hyogo, Hyogo, Japan How to cite this paper: Akimoto, H. and Abstract Itoh, Y. (2019) Optical Spectroscopic Mon- itoring Observations of a T Tauri Star V409 We report the results of optical spectroscopic monitoring observations of a T Tau. International Journal of Astronomy Tauri star, V409 Tau. A previous photometric study indicated that this star and Astrophysics, 9, 321-334. experienced dimming events due to the obscuration of light from the central https://doi.org/10.4236/ijaa.2019.93023 star with a distorted circumstellar disk. We conducted medium-resolution (R Received: July 24, 2019 ~10,000) spectroscopic observations with 2-m Nayuta telescope at Ni- Accepted: September 16, 2019 shi-Harima Astronomical Observatory. Spectra were obtained in 18 nights Published: September 19, 2019 between November 2015 and March 2016. Several absorption lines such as Ca Copyright © 2019 by author(s) and I and Li, and the Hα emission line were confirmed in the spectra. The Ic-band Scientific Research Publishing Inc. magnitudes of V409 Tau changed by approximately 1 magnitude during the This work is licensed under the Creative observation epoch. The equivalent widths of the five absorption lines are Commons Attribution International License (CC BY 4.0). roughly constant despite changes in the Ic-band magnitudes. We conclude http://creativecommons.org/licenses/by/4.0/ that the light variation of the star is caused by the obscuration of light from Open Access the central star with a distorted circumstellar disk, based on the relationship between the equivalent widths of the absorption lines and the Ic-band magni- tudes. -
Small-Scale Structure Is It a Valid Motivation?
Small-scale Structure Is it a valid motivation? Jakub Scholtz IPPP (Durham) Small Scale Structure Problems <—> All the reasons why “CDM is not it” How did we get here? We are gravitationally sensitive to something sourcing T • <latexit sha1_base64="055AcnSYYRkGsBe2aYAe7vH1peg=">AAAB8XicbVDLSgNBEOz1GeMr6tHLYBA8hV0R9Bj04jFCXphdwuxkNhkyM7vMQwhL/sKLB0W8+jfe/BsnyR40saChqOqmuyvOONPG97+9tfWNza3t0k55d2//4LBydNzWqVWEtkjKU9WNsaacSdoyzHDazRTFIua0E4/vZn7niSrNUtk0k4xGAg8lSxjBxkmPzX4eChtKO+1Xqn7NnwOtkqAgVSjQ6Fe+wkFKrKDSEI617gV+ZqIcK8MIp9NyaDXNMBnjIe05KrGgOsrnF0/RuVMGKEmVK2nQXP09kWOh9UTErlNgM9LL3kz8z+tZk9xEOZOZNVSSxaLEcmRSNHsfDZiixPCJI5go5m5FZIQVJsaFVHYhBMsvr5L2ZS3wa8HDVbV+W8RRglM4gwsI4BrqcA8NaAEBCc/wCm+e9l68d+9j0brmFTMn8Afe5w/beZEG</latexit> µ⌫ —> we are fairly certain that DM exists. • An exception is MOND, which has issues of its own. However, the MOND community has been instrumental in pointing out some of the discrepancies with CDM. • But how do we verify the picture? —> NBODY simulations (disclaimer: I have never run a serious body simulation) 2WalterDehnen,JustinI.Read:N-body SimulationsN-body simulations of gravitational dynamics have reached over 106 particles [6], while collisionless calculations can now reach more than 109 particles [7–10]. This disparity reflects the difference in complexity of these rather dissimilar N-body problems. The significant increase in N in the last decade was driven by the usage of parallel computers. In this review, we discuss the state-of-the art software algo- Takerithms N and dark hardware matter improvements -
Arxiv:0808.3207V1 [Astro-Ph] 23 Aug 2008 Nfgr .Nwonsaswr Rtdrcl Icvrdi C in Discovered Directly H first Were and Surroun Stars Variability Area Newborn the of 4
Handbook of Star Forming Regions Vol. II Astronomical Society of the Pacific, 2008 Bo Reipurth, ed. Chamaeleon Kevin L. Luhman Department of Astronomy and Astrophysics The Pennsylvania State University University Park, PA 16802, USA Abstract. The dark clouds in the constellation of Chamaeleon have distances of 160-180pc from the Sun and a total mass of ∼5000 M⊙. The three main clouds, Cha I, II, and III, have angular sizes of a few square degrees and maximum extinctions of AV ∼ 5-10. Most of the star formation in these clouds is occurring in Cha I, with the remainder in Cha II. The current census of Cha I contains 237 known members, 33 of which have spectral types indicative of brown dwarfs (>M6). Approximately 50 members of Cha II have been identified, including a few brown dwarfs. When interpreted with the evolutionary models of Chabrier and Baraffe, the H-R diagram for Cha I exhibits a median age of ∼2 Myr, making it coeval with IC 348 and slightly older than Taurus (∼1 Myr). TheIMF ofChaI reachesa maximumat a massof0.1-0.15 M⊙, and thus closely resembles the IMFs in IC 348 and the Orion Nebula Cluster. The disk fraction in Cha I is roughly constant at ∼ 50% from 0.01 to 0.3 M⊙ and increases to ∼ 65% at higher masses. In comparison, IC 348 has a similar disk fraction at low masses but a much lower disk fraction at M ∼> 1 M⊙, indicating that solar-type stars have longer disk lifetimes in Cha I. 1. Introduction The southern constellation of Chamaeleon contains one of the nearest groups of dark clouds to the Sun (d ∼ 160-180 pc). -
X-Ray and Near-Infrared Spectroscopy of Dim X-Ray Point Sources Constituting the Galactic Ridge X-Ray Emission
Acta Polytechnica CTU Proceedings 1(1): 222{226, 2014 doi: 10.14311/APP.2014.01.0222 222 222 X-Ray and Near-Infrared Spectroscopy of Dim X-Ray Point Sources Constituting the Galactic Ridge X-Ray Emission Kumiko Morihana1, Masahiro Tsujimoto2, Ken Ebisawa2 1Nishiharima Astronomical Observatory, Center for Astronomy, University of Hyogo, 407-2 Nishigaichi, Sayo-cho, Sayo- gun, Hyogo, 679-5313, Japan 2Japan Astrospace Exporation Agency, Institute of Space and Astronautical Science, 3-1-1 Yoshino-dai, Chuo-ku, Sagami- hara, Kanagawa 252-5210, Japan Corresponding author: [email protected] Abstract We present the results of X-ray and Near-Infrared observations of the Galactic Ridge X-ray Emission (GRXE). We extracted 2,002 X-ray point sources in the Chandra Bulge Field (l =0◦.113, b = 1◦.424) down to ∼10−14:8 ergs cm−2 s−1 in 2{8 keV band with the longest observation (∼900 ks) of the GRXE. Based on X-ray brightness and hardness, we classified the X-ray point sources into three groups: A (hard), B (soft and broad spectrum), and C (soft and peaked spectrum). In order to know populations of the X-ray point sources, we carried out NIR imaging and spectroscopy observation. We identified ∼11% of X-ray point sources with NIR and extracted NIR spectra for some of them. Based on X-ray and NIR properties, we concluded that non-thermal sources in the group A are mostly active galactic nuclei and the thermal sources are mostly white dwarf binaries such as cataclysmic variables (CVs) and Pre-CVs. -
The Hot, Warm and Cold Gas in Arp 227 - an Evolving Poor Group R
The hot, warm and cold gas in Arp 227 - an evolving poor group R. Rampazzo, P. Alexander, C. Carignan, M.S. Clemens, H. Cullen, O. Garrido, M. Marcelin, K. Sheth, G. Trinchieri To cite this version: R. Rampazzo, P. Alexander, C. Carignan, M.S. Clemens, H. Cullen, et al.. The hot, warm and cold gas in Arp 227 - an evolving poor group. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2006, 368, pp.851. 10.1111/j.1365- 2966.2006.10179.x. hal-00083833 HAL Id: hal-00083833 https://hal.archives-ouvertes.fr/hal-00083833 Submitted on 13 Dec 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Mon. Not. R. Astron. Soc. 368, 851–863 (2006) doi:10.1111/j.1365-2966.2006.10179.x The hot, warm and cold gas in Arp 227 – an evolving poor group R. Rampazzo,1 P. Alexander,2 C. Carignan,3 M. S. Clemens,1 H. Cullen,2 O. Garrido,4 M. Marcelin,5 K. Sheth6 and G. Trinchieri7 1Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, Italy 2Astrophysics Group, Cavendish Laboratories, Cambridge CB3 OH3 3Departement´ de physique, Universite´ de Montreal,´ C. -
Exoplanet.Eu Catalog Page 1 # Name Mass Star Name
exoplanet.eu_catalog # name mass star_name star_distance star_mass OGLE-2016-BLG-1469L b 13.6 OGLE-2016-BLG-1469L 4500.0 0.048 11 Com b 19.4 11 Com 110.6 2.7 11 Oph b 21 11 Oph 145.0 0.0162 11 UMi b 10.5 11 UMi 119.5 1.8 14 And b 5.33 14 And 76.4 2.2 14 Her b 4.64 14 Her 18.1 0.9 16 Cyg B b 1.68 16 Cyg B 21.4 1.01 18 Del b 10.3 18 Del 73.1 2.3 1RXS 1609 b 14 1RXS1609 145.0 0.73 1SWASP J1407 b 20 1SWASP J1407 133.0 0.9 24 Sex b 1.99 24 Sex 74.8 1.54 24 Sex c 0.86 24 Sex 74.8 1.54 2M 0103-55 (AB) b 13 2M 0103-55 (AB) 47.2 0.4 2M 0122-24 b 20 2M 0122-24 36.0 0.4 2M 0219-39 b 13.9 2M 0219-39 39.4 0.11 2M 0441+23 b 7.5 2M 0441+23 140.0 0.02 2M 0746+20 b 30 2M 0746+20 12.2 0.12 2M 1207-39 24 2M 1207-39 52.4 0.025 2M 1207-39 b 4 2M 1207-39 52.4 0.025 2M 1938+46 b 1.9 2M 1938+46 0.6 2M 2140+16 b 20 2M 2140+16 25.0 0.08 2M 2206-20 b 30 2M 2206-20 26.7 0.13 2M 2236+4751 b 12.5 2M 2236+4751 63.0 0.6 2M J2126-81 b 13.3 TYC 9486-927-1 24.8 0.4 2MASS J11193254 AB 3.7 2MASS J11193254 AB 2MASS J1450-7841 A 40 2MASS J1450-7841 A 75.0 0.04 2MASS J1450-7841 B 40 2MASS J1450-7841 B 75.0 0.04 2MASS J2250+2325 b 30 2MASS J2250+2325 41.5 30 Ari B b 9.88 30 Ari B 39.4 1.22 38 Vir b 4.51 38 Vir 1.18 4 Uma b 7.1 4 Uma 78.5 1.234 42 Dra b 3.88 42 Dra 97.3 0.98 47 Uma b 2.53 47 Uma 14.0 1.03 47 Uma c 0.54 47 Uma 14.0 1.03 47 Uma d 1.64 47 Uma 14.0 1.03 51 Eri b 9.1 51 Eri 29.4 1.75 51 Peg b 0.47 51 Peg 14.7 1.11 55 Cnc b 0.84 55 Cnc 12.3 0.905 55 Cnc c 0.1784 55 Cnc 12.3 0.905 55 Cnc d 3.86 55 Cnc 12.3 0.905 55 Cnc e 0.02547 55 Cnc 12.3 0.905 55 Cnc f 0.1479 55 -
Comprehensive Broadband X-Ray and Multiwavelength Study of Active Galactic Nuclei in Local 57 Ultra/Luminous Infrared Galaxies Observed with Nustar And/Or Swift/BAT
Draft version July 26, 2021 Typeset using LATEX twocolumn style in AASTeX631 Comprehensive Broadband X-ray and Multiwavelength Study of Active Galactic Nuclei in Local 57 Ultra/luminous Infrared Galaxies Observed with NuSTAR and/or Swift/BAT Satoshi Yamada ,1 Yoshihiro Ueda ,1 Atsushi Tanimoto ,2 Masatoshi Imanishi ,3, 4 Yoshiki Toba ,1, 5 Claudio Ricci ,6, 7, 8 and George C. Privon 9 1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan 2Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan 3National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, Japan 4Department of Astronomical Science, Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan 5Research Center for Space and Cosmic Evolution, Ehime University, 2-5 Bunkyo-cho, Matsuyama, Ehime 790-8577, Japan 6N´ucleo de Astronom´ıade la Facultad de Ingenier´ıa,Universidad Diego Portales, Av. Ej´ercito Libertador 441, Santiago, Chile 7Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, People's Republic of China 8George Mason University, Department of Physics & Astronomy, MS 3F3, 4400 University Drive, Fairfax, VA 22030, USA 9National Radio Astronomy Observatory, 520 Edgemont Rd, Charlottesville, VA 22903, USA (Received April 13, 2021; Revised June 11, 2021; Accepted Jul, 2021) ABSTRACT We perform a systematic X-ray spectroscopic analysis of 57 local ultra/luminous infrared galaxy systems (containing 84 individual galaxies) observed with Nuclear Spectroscopic Telescope Array and/or Swift/BAT. Combining soft X-ray data obtained with Chandra, XMM-Newton, Suzaku and/or Swift/XRT, we identify 40 hard (>10 keV) X-ray detected active galactic nuclei (AGNs) and con- strain their torus parameters with the X-ray clumpy torus model XCLUMPY (Tanimoto et al.