The ATLAS3D Project – XIII
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Evidence of Boosted 13CO/12CO Ratio in Early-Type Galaxies in Dense Environments
MNRAS 450, 3874–3885 (2015) doi:10.1093/mnras/stv837 Evidence of boosted 13CO/12CO ratio in early-type galaxies in dense environments Katherine Alatalo,1‹ Alison F. Crocker,2,3 Susanne Aalto,4 Timothy A. Davis,5,6 Kristina Nyland,7 Martin Bureau,8 Pierre-Alain Duc,9 Davor Krajnovic´10 and Lisa M. Young11 1Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA 2Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606, USA 3Department of Physics, Reed College, Portland, OR 97202, USA 4Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Observatory, SE-439 94 Onsala, Sweden 5European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany Downloaded from 6Centre for Astrophysics Research, University of Hertfordshire, Hatfield, Herts AL1 9AB, UK 7Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2, NL-7990 AA Dwingeloo, the Netherlands 8Sub-Department of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK 9Laboratoire AIM Paris-Saclay, CEA/IRFU/SAp – CNRS – Universite´ Paris Diderot, F-91191 Gif-sur-Yvette Cedex, France 10Leibniz-Institut fur¨ Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany 11Physics Department, New Mexico Institute of Mining and Technology, Socorro, NM 87801, USA http://mnras.oxfordjournals.org/ Accepted 2015 April 2. Received 2015 March 27; in original form 2014 October 8 ABSTRACT We present observations of 13CO(1–0) in 17 Combined Array for Research in Millimeter Astronomy ATLAS3D early-type galaxies (ETGs), obtained simultaneously with 12CO(1–0) at California Institute of Technology on October 1, 2015 observations. -
Science Goals and Selection Criteria
University of Groningen The ATLAS(3D) project Cappellari, Michele; Emsellem, Eric; Krajnovic, Davor; McDermid, Richard M.; Scott, Nicholas; Kleijn, G. A. Verdoes; Young, Lisa M.; Alatalo, Katherine; Bacon, R.; Blitz, Leo Published in: Monthly Notices of the Royal Astronomical Society DOI: 10.1111/j.1365-2966.2010.18174.x IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document Version Publisher's PDF, also known as Version of record Publication date: 2011 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Cappellari, M., Emsellem, E., Krajnovic, D., McDermid, R. M., Scott, N., Kleijn, G. A. V., Young, L. M., Alatalo, K., Bacon, R., Blitz, L., Bois, M., Bournaud, F., Bureau, M., Davies, R. L., Davis, T. A., de Zeeuw, P. T., Duc, P-A., Khochfar, S., Kuntschner, H., ... Weijmans, A-M. (2011). The ATLAS(3D) project: I. A volume-limited sample of 260 nearby early-type galaxies: science goals and selection criteria. Monthly Notices of the Royal Astronomical Society, 413(2), 813-836. https://doi.org/10.1111/j.1365- 2966.2010.18174.x Copyright Other than for strictly personal use, it is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license (like Creative Commons). The publication may also be distributed here under the terms of Article 25fa of the Dutch Copyright Act, indicated by the “Taverne” license. -
HST/WFPC2 Imaging of the Circumnuclear Structure of Llagns
HST/WFPC2 imaging of the circumnuclear structure of LLAGNs. I Data and nuclear morphology1 Rosa M. Gonz´alez Delgado1, Enrique P´erez1, Roberto Cid Fernandes2, Henrique Schmitt3, (1) Instituto de Astrof´ısica de Andaluc´ıa(CSIC), P.O. Box 3004, 18080 Granada, Spain ([email protected]; [email protected]) (2) Depto. de F´ısica-CFM, Universidade Federal de Santa Catarina, C.P. 476, 88040-900, Florian´opolis, SC, Brazil ([email protected]) (3) Remote Sensing Division, Naval Research Laboratory, Code 7210, 4555 Overlook Avenue, Washington, DC 20375 ([email protected]) (4) Interferometrics, Inc., 13454 Sunrise Valley Drive, Suite 240, Herndon, VA20171 ABSTRACT In several studies of Low Luminosity Active Galactic Nuclei (LLAGNs), we have characterized the properties of the stellar populations in LINERs and LINER/HII Transition Objects (TOs). We have found a numerous class of galac- tic nuclei which stand out because of their conspicuous 0.1–1 Gyr populations. These nuclei were called ”Young-TOs” since they all have TO-like emission line ratios. To advance our knowledge of the nature of the central source in LLAGNs and its relation with stellar clusters, we are carrying out several imaging projects with the Hubble Space Telescope (HST) at near-UV, optical and near-IR wave- lengths. In this paper, we present the first results obtained with observations of the central regions of 57 LLAGNs imaged with the WFPC2 through any of arXiv:0710.4450v1 [astro-ph] 24 Oct 2007 the V (F555W, F547M, F614W) and I (F791W, F814W) filters that are avail- able in the HST archive. -
Radio Sources in Low-Luminosity Active Galactic Nuclei
A&A 392, 53–82 (2002) Astronomy DOI: 10.1051/0004-6361:20020874 & c ESO 2002 Astrophysics Radio sources in low-luminosity active galactic nuclei III. “AGNs” in a distance-limited sample of “LLAGNs” N. M. Nagar1, H. Falcke2,A.S.Wilson3, and J. S. Ulvestad4 1 Arcetri Observatory, Largo E. Fermi 5, Florence 50125, Italy 2 Max-Planck-Institut f¨ur Radioastronomie, Auf dem H¨ugel 69, 53121 Bonn, Germany e-mail: [email protected] 3 Department of Astronomy, University of Maryland, College Park, MD 20742, USA Adjunct Astronomer, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA e-mail: [email protected] 4 National Radio Astronomy Observatory, PO Box 0, Socorro, NM 87801, USA e-mail: [email protected] Received 23 January 2002 / Accepted 6 June 2002 Abstract. This paper presents the results of a high resolution radio imaging survey of all known (96) low-luminosity active galactic nuclei (LLAGNs) at D ≤ 19 Mpc. We first report new 2 cm (150 mas resolution using the VLA) and 6 cm (2 mas resolution using the VLBA) radio observations of the previously unobserved nuclei in our samples and then present results on the complete survey. We find that almost half of all LINERs and low-luminosity Seyferts have flat-spectrum radio cores when observed at 150 mas resolution. Higher (2 mas) resolution observations of a flux-limited subsample have provided a 100% (16 of 16) detection rate of pc-scale radio cores, with implied brightness temperatures ∼>108 K. The five LLAGNs with the highest core radio fluxes also have pc-scale “jets”. -
April Constellations of the Month
April Constellations of the Month Leo Small Scope Objects: Name R.A. Decl. Details M65! A large, bright Sa/Sb spiral galaxy. 7.8 x 1.6 arc minutes, magnitude 10.2. Very 11hr 18.9m +13° 05’ (NGC 3623) high surface brighness showing good detail in medium sized ‘scopes. M66! Another bright Sb galaxy, only 21 arc minutes from M65. Slightly brighter at mag. 11hr 20.2m +12° 59’ (NGC 3627) 9.7, measuring 8.0 x 2.5 arc minutes. M95 An easy SBb barred spiral, 4 x 3 arc minutes in size. Magnitude 10.5, with 10hr 44.0m +11° 42’ a bright central core. The bar and outer ring of material will require larger (NGC 3351) aperature and dark skies. M96 Another bright Sb spiral, about 42 arc minutes east of M95, but larger and 10hr 46.8m +11° 49’ (NGC 3368) brighter. 6 x 4 arc minutes, magnitude 10.1. Located about 48 arc minutes NNE of M96. This small elliptical galaxy measures M105 only 2 x 2.1 arc minutes, but at mag. 10.3 has very high surface brightness. 10hr 47.8m +12° 35’ (NGC 3379) Look for NGC 3384! (110NGC) and NGC 3389 (mag 11.0 and 12.2) which form a small triangle with M105. NGC 3384! 10hr 48.3m +12° 38’ See comment for M105. The brightest galaxy in Leo, this Sb/Sc spiral galaxy shines at mag. 9.5. Look for NGC 2903!! 09hr 32.2m +21° 30’ a hazy patch 11 x 4.7 arc minutes in size 1.5° south of l Leonis. -
The Newsletter of the Barnard-Seyfert Astronomical Society
March The ECLIPSE 2018 The Newsletter of the Barnard-Seyfert Astronomical Society From the President Next Membership Meeting: Greetings, March 21, 2018, 7:30 pm February 2018 was no friend of BSAS weather wise. Te short Cumberland Valley month of February was not short on rain. We saw 18 or 19 Girl Scout Council Building days with measurable participation. Average monthly rainfall 4522 Granny White Pike in February for Nashville is 3.7 inches. We had just under 11 inches. When it wasn’t raining it was cloudy and windy. Topic: Equipment Tune-up Details on page 6. We had enough bad weather to frustrate almost all attempts to view the winter stars and deep sky objects we believe are still up there. Our public star party at Edwin Warner Park was washed out, as was the private star party on the Natchez In this Issue: Trace at Water Valley Overlook. May we turn the page on that trend? Observing Highlights 2 Tanks to Terry Reeves for his informative and helpful From A Certain Point of View presentation, All About A Messier Marathon, which he gave reviewed by Robin Byrne 3 at this month’s member meeting. We will have a chance to put that information into practice on Saturday, March 17th Deep Sky Daze when BSAS holds a Messier Marathon at Mark Manner’s by Mike Benson 4 Spot Observatory. Just in case, we are planning April 14th as Board Meeting Minutes 8 a backup date. We have that date reserved for a private star February 7, 2018 party at Water Valley Overlook. -
Projekt Ursa Major
12 θ 11 Draco 14 Lynx 7 13 N 15 51 2722 UGC4593 NGC2985 18 NGC3348 NGC3065 47 EW ι NGC3516 49 24NGC2787 6 ρ κ M82 2 S 4 M81 σUGC4687σ2 π NGC3077 1 1 24 19 α 10 2 λ NGC2976 π2 53 6 23 9 7 8 ο 29 3 τ 5 NGC5216 38 35 32 Lyn 23 30 NGC2880 16 NGC5631 NGC5322 22 NGC2742NGC2816 76 NGC2768 NGC4605 47 NGC4041NGC4036 44 NGC5485 NGC5473 α 27 NGC2950 39 M101 NGC3945 υ 17 θ NGC5474 NGC5278 26 86 84 81 75 NGC3809 25 24 ι 83 74 NGC3894 42 38 80ζ 78 70 NGC3610 NGC3757NGC3690BNGC3690A 18 82 ε NGC3838 NGC3613 71 δ68 4139 37 13 NGC3458 NGC2681 73 66 43 NGC2639 β 36 15 33 NGC3898NGC3888 φ NGC3998 M108 NGC4194 NGC3982 26 λ η 44 UGC5720 θ NGC2841 28 NGC3738 M97 24 γ NGC3310UGC5615B 21 M109 ι 34 7 NGC4102 NGC3729NGC3631 31 5 NGC3953 κ 31 NGC4026 NGC4088 NGC3406 11 35 3 NGC3870 UMa NGC4047 NGC3985NGC3928NGC3893 NGC3583 36 NGC3949 χNGC3769 NGC3595 NGC372660 NGC3198 NGC3009 CVn 3332 19 NGC4051 UGC6187UGC6135 23 20 NGC3938 ψ λ 4 67 59 56 42 NGC367558 ω 19 43 9 β NGC3184 25 1715 µ 10 2 38 αα12 47 6 109 32 σ σ 14 57 49 11 2 1 8 α σ 46 NGC3665 38 σ 3 55 UGC613251 13 4 β 7 57 NGC3941 35 21 61 NGC3813 ιι 34 ρ53 9 NGC3694 τ 1 302827 ρ 46 67 2 61 20 37 46 LMi 33 NGC3878 ν 22 15 3 NGC3994 37 75 β 62 15° 41 ξ 42 23 κ ν Bootes 31 24 Cancer 30 43 γ 9 13 Deep Sky•Objekte in Ursa Major (UMa) Object Type RA Dec Mag Size Surf Br Constellation •••••• •••• •• ••• ••• •••• ••••••• ••••••••••••• M101 Galaxy 14h 03m 25.6s +54° 19' 10" 8.2 28.5'x28.3' 14.0 Ursa Major M108 Galaxy 11h 11m 50.1s +55° 38' 39" 10.6 8.6'x2.4' 13.3 Ursa Major M109 Galaxy 11h 57m 54.0s +53° 20' 35" 10.6 7.5'x4.4' -
SUPERMASSIVE BLACK HOLES and THEIR HOST SPHEROIDS III. the MBH − Nsph CORRELATION
The Astrophysical Journal, 821:88 (8pp), 2016 April 20 doi:10.3847/0004-637X/821/2/88 © 2016. The American Astronomical Society. All rights reserved. SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. III. THE MBH–nsph CORRELATION Giulia A. D. Savorgnan Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122, Australia; [email protected] Received 2015 December 6; accepted 2016 March 6; published 2016 April 13 ABSTRACT The Sérsic R1 n model is the best approximation known to date for describing the light distribution of stellar spheroidal and disk components, with the Sérsic index n providing a direct measure of the central radial concentration of stars. The Sérsic index of a galaxy’s spheroidal component, nsph, has been shown to tightly correlate with the mass of the central supermassive black hole, MBH.TheMnBH– sph correlation is also expected from other two well known scaling relations involving the spheroid luminosity, Lsph:theLsph–n sph and the MLBH– sph. Obtaining an accurate estimate of the spheroid Sérsic index requires a careful modeling of a galaxy’s light distribution and some studies have failed to recover a statistically significant MnBH– sph correlation. With the aim of re-investigating the MnBH– sph and other black hole mass scaling relations, we performed a detailed (i.e., bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, that had been imaged at 3.6 μm with Spitzer.Inthispaper,the third of this series, we present an analysis of the Lsph–n sph and MnBH– sph diagrams. -
A Nuclear Molecular Outflow in the Seyfert Galaxy NGC 3227
Astronomy & Astrophysics manuscript no. ALMANGC3227_final c ESO 2019 June 18, 2019 A nuclear molecular outflow in the Seyfert galaxy NGC 3227 A. Alonso-Herrero1, S. García-Burillo2, M. Pereira-Santaella3, R. I. Davies4, F. Combes5, M. Vestergaard6; 7, S. I. Raimundo6, A. Bunker3, T. Díaz-Santos8, P. Gandhi9, I. García-Bernete10, E. K. S. Hicks11, S. F. Hönig8, L. K. Hunt12, M. Imanishi13; 14, T. Izumi13, N. A. Levenson15, W. Maciejewski16, C. Packham17; 13, C. Ramos Almeida18; 19, C. Ricci8; 20, D. Rigopoulou3, P. F. Roche3, D. Rosario21, M. Schartmann22; 4, A. Usero2, and M. J. Ward21 1 Centro de Astrobiología (CAB, CSIC-INTA), ESAC Campus, E-28692 Villanueva de la Cañada, Madrid, Spain e-mail: [email protected] 2 Observatorio de Madrid, OAN-IGN, Alfonso XII, 3, E-28014 Madrid, Spain 3 Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK 4 Max Planck Institut für extraterrestrische Physik Postfach 1312, D-85741 Garching bei München, Germany 5 LERMA, Obs. de Paris, PSL Research Univ., Collége de France, CNRS, Sorbonne Univ., UPMC, Paris, France 6 DARK, The Niels Bohr Institute, University of Copenhagen, Vibenshuset, Lyngbyvej 2, DK-2100 Copenhagen O., Denmark 7 Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, Arizona, USA 8 Núcleo de Astronomía de la Facultad de Ingeniería, Universidad Diego Portales, Av. Ejército Libertador 441, Santiago, Chile 9 Department of Physics & Astronomy, University of Southampton, Hampshire SO17 1BJ, Southampton, UK 10 Instituto de Física de Cantabria, CSIC-Universidad de Cantabria, E-39005 Santander, Spain 11 Department of Physics & Astronomy, University of Alaska Anchorage, AK 99508-4664, USA 12 INAF-Osservatorio Astrofisico di Arcetri, Largo E. -
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. -
Durham Research Online
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Durham Research Online Durham Research Online Deposited in DRO: 22 January 2020 Version of attached le: Published Version Peer-review status of attached le: Peer-reviewed Citation for published item: Babyk, Iu. V. and McNamara, B. R. and Tamhane, P. D. and Nulsen, P. E. J. and Russell, H. R. and Edge, A. C. (2019) 'Origins of molecular clouds in early-type galaxies.', Astrophysical journal., 887 (2). p. 149. Further information on publisher's website: https://doi.org/10.3847/1538-4357/ab54ce Publisher's copyright statement: c 2019. The American Astronomical Society. All rights reserved. Use policy The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that: • a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders. Please consult the full DRO policy for further details. Durham University Library, Stockton Road, Durham DH1 3LY, United Kingdom Tel : +44 (0)191 334 3042 | Fax : +44 (0)191 334 2971 http://dro.dur.ac.uk The Astrophysical Journal, 887:149 (17pp), 2019 December 20 https://doi.org/10.3847/1538-4357/ab54ce © 2019. The American Astronomical Society. All rights reserved. -
Cold Gas in Galaxies a Concise HI Perspective
Cold Gas in Galaxies a concise HI perspective Marc Verheijen Galaxy Formation, 18-22 July 2011 - Durham Characteristics of HI imaging data A limited number of 21cm aperture synthesis imaging telescopes. array dishes Tsys BLmin BLmax configuration " EVLA 27x 25m 35 K 35 m 36 km Y zoomable 1.3” WSRT 14x 25m 27 K 36 m 2.7 km EW moveable 15” GMRT 30x 45m 73 K 100 m 25 km Y fixed 2” ATCA 6x 22m 22 K 31 m 6.0 km EW zoomable 6” Field-of-view : 20’ ! 40’ FWHM Useful resolutions : 5”! 45” x few km s-1 19 22 -2 Column density sensitivities : NHI !10 !10 atoms cm 6 HI mass limits : MHI !10 Msun at D=10 Mpc Maximum redshifts : Z<0.25 Galaxy Formation, 18-22 July 2011 - Durham major HI imaging surveys Targeted Surveys of selected samples: • WHISP (350) northern spirals with F>100 mJy • VIVA (53) SFR-selected Virgo spirals • UMa (85) Ursa Major group with MB< -18.5 • THINGS (34) HI follow-up of SINGS sample • LittleTHINGS (42) Local dIm and BCDs • FIGGS (47) Faint Irregular galaxies • ATLAS3D (166) HI follow-up of northern early-types • HALOGAS (22) the deepest HI survey of spirals • VLA-ANGST (36) HI follow-up of HST/ACS survey Blind Surveys of different environments: • Coma (WSRT) • Perseus-Pisces (VLA) • Ursa Major (VLA) • CVn (WSRT) Galaxy Formation, 18-22 July 2011 - Durham HI science topics • Galactic and galaxy structure & kinematics. - the ISM, warps, lopsidedness, rotation curves, angular momentum, non-circular motions... • Accretion and depletion of gas onto galaxies.