Circumnuclear Keplerian Disks in Galaxies
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Stellar Tidal Streams As Cosmological Diagnostics: Comparing Data and Simulations at Low Galactic Scales
RUPRECHT-KARLS-UNIVERSITÄT HEIDELBERG DOCTORAL THESIS Stellar Tidal Streams as Cosmological Diagnostics: Comparing data and simulations at low galactic scales Author: Referees: Gustavo MORALES Prof. Dr. Eva K. GREBEL Prof. Dr. Volker SPRINGEL Astronomisches Rechen-Institut Heidelberg Graduate School of Fundamental Physics Department of Physics and Astronomy 14th May, 2018 ii DISSERTATION submitted to the Combined Faculties of the Natural Sciences and Mathematics of the Ruperto-Carola-University of Heidelberg, Germany for the degree of DOCTOR OF NATURAL SCIENCES Put forward by GUSTAVO MORALES born in Copiapo ORAL EXAMINATION ON JULY 26, 2018 iii Stellar Tidal Streams as Cosmological Diagnostics: Comparing data and simulations at low galactic scales Referees: Prof. Dr. Eva K. GREBEL Prof. Dr. Volker SPRINGEL iv NOTE: Some parts of the written contents of this thesis have been adapted from a paper submitted as a co-authored scientific publication to the Astronomy & Astrophysics Journal: Morales et al. (2018). v NOTE: Some parts of this thesis have been adapted from a paper accepted for publi- cation in the Astronomy & Astrophysics Journal: Morales, G. et al. (2018). “Systematic search for tidal features around nearby galaxies: I. Enhanced SDSS imaging of the Local Volume". arXiv:1804.03330. DOI: 10.1051/0004-6361/201732271 vii Abstract In hierarchical models of galaxy formation, stellar tidal streams are expected around most galaxies. Although these features may provide useful diagnostics of the LCDM model, their observational properties remain poorly constrained. Statistical analysis of the counts and properties of such features is of interest for a direct comparison against results from numeri- cal simulations. In this work, we aim to study systematically the frequency of occurrence and other observational properties of tidal features around nearby galaxies. -
ARRAKIS: Atlas of Resonance Rings As Known in The
Astronomy & Astrophysics manuscript no. arrakis˙v12 c ESO 2018 September 28, 2018 ARRAKIS: atlas of resonance rings as known in the S4G⋆,⋆⋆ S. Comer´on1,2,3, H. Salo1, E. Laurikainen1,2, J. H. Knapen4,5, R. J. Buta6, M. Herrera-Endoqui1, J. Laine1, B. W. Holwerda7, K. Sheth8, M. W. Regan9, J. L. Hinz10, J. C. Mu˜noz-Mateos11, A. Gil de Paz12, K. Men´endez-Delmestre13 , M. Seibert14, T. Mizusawa8,15, T. Kim8,11,14,16, S. Erroz-Ferrer4,5, D. A. Gadotti10, E. Athanassoula17, A. Bosma17, and L.C.Ho14,18 1 University of Oulu, Astronomy Division, Department of Physics, P.O. Box 3000, FIN-90014, Finland e-mail: [email protected] 2 Finnish Centre of Astronomy with ESO (FINCA), University of Turku, V¨ais¨al¨antie 20, FI-21500, Piikki¨o, Finland 3 Korea Astronomy and Space Science Institute, 776, Daedeokdae-ro, Yuseong-gu, Daejeon 305-348, Republic of Korea 4 Instituto de Astrof´ısica de Canarias, E-38205 La Laguna, Tenerife, Spain 5 Departamento de Astrof´ısica, Universidad de La Laguna, E-38200, La Laguna, Tenerife, Spain 6 Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487 7 European Space Agency, ESTEC, Keplerlaan 1, 2200 AG, Noorwijk, the Netherlands 8 National Radio Astronomy Observatory/NAASC, 520 Edgemont Road, Charlottesville, VA 22903, USA 9 Space Telescope Science Institute, 3700 San Antonio Drive, Baltimore, MD 21218, USA 10 European Southern Observatory, Casilla 19001, Santiago 19, Chile 11 MMTO, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA 12 Departamento de Astrof´ısica, -
Making a Sky Atlas
Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it. -
Ngc Catalogue Ngc Catalogue
NGC CATALOGUE NGC CATALOGUE 1 NGC CATALOGUE Object # Common Name Type Constellation Magnitude RA Dec NGC 1 - Galaxy Pegasus 12.9 00:07:16 27:42:32 NGC 2 - Galaxy Pegasus 14.2 00:07:17 27:40:43 NGC 3 - Galaxy Pisces 13.3 00:07:17 08:18:05 NGC 4 - Galaxy Pisces 15.8 00:07:24 08:22:26 NGC 5 - Galaxy Andromeda 13.3 00:07:49 35:21:46 NGC 6 NGC 20 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 7 - Galaxy Sculptor 13.9 00:08:21 -29:54:59 NGC 8 - Double Star Pegasus - 00:08:45 23:50:19 NGC 9 - Galaxy Pegasus 13.5 00:08:54 23:49:04 NGC 10 - Galaxy Sculptor 12.5 00:08:34 -33:51:28 NGC 11 - Galaxy Andromeda 13.7 00:08:42 37:26:53 NGC 12 - Galaxy Pisces 13.1 00:08:45 04:36:44 NGC 13 - Galaxy Andromeda 13.2 00:08:48 33:25:59 NGC 14 - Galaxy Pegasus 12.1 00:08:46 15:48:57 NGC 15 - Galaxy Pegasus 13.8 00:09:02 21:37:30 NGC 16 - Galaxy Pegasus 12.0 00:09:04 27:43:48 NGC 17 NGC 34 Galaxy Cetus 14.4 00:11:07 -12:06:28 NGC 18 - Double Star Pegasus - 00:09:23 27:43:56 NGC 19 - Galaxy Andromeda 13.3 00:10:41 32:58:58 NGC 20 See NGC 6 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 21 NGC 29 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 22 - Galaxy Pegasus 13.6 00:09:48 27:49:58 NGC 23 - Galaxy Pegasus 12.0 00:09:53 25:55:26 NGC 24 - Galaxy Sculptor 11.6 00:09:56 -24:57:52 NGC 25 - Galaxy Phoenix 13.0 00:09:59 -57:01:13 NGC 26 - Galaxy Pegasus 12.9 00:10:26 25:49:56 NGC 27 - Galaxy Andromeda 13.5 00:10:33 28:59:49 NGC 28 - Galaxy Phoenix 13.8 00:10:25 -56:59:20 NGC 29 See NGC 21 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 30 - Double Star Pegasus - 00:10:51 21:58:39 -
Structure, Mass and Distance of the Virgo Cluster from a Tolman-Bondi
A&A manuscript no. ASTRONOMY (will be inserted by hand later) AND Your thesaurus codes are: 03(11.03.4; 11.04.1; 11.05.1; 11.06.2; 11.19.2; 12.04.3) ASTROPHYSICS Structure, mass and distance of the Virgo cluster from a Tolman-Bondi model Pascal Fouqu´e1,2, Jos´eM. Solanes3, Teresa Sanchis4, and Chantal Balkowski5 1 Observatoire de Paris-Meudon DESPA, F-92195 Meudon CEDEX, France 2 European Southern Observatory, Casilla 19001, Santiago 19, Chile email: [email protected] 3 Departament d’Enginyeria Inform`atica i Matem`atiques, Escola T`ecnica Superior d’Enginyeria, Universitat Rovira i Virgili, Carretera de Salou, s/n; E–43006 Tarragona, Spain email: [email protected] 4 Departament d’Astronomia i Meteorologia, Facultat de F´ısiques, Universitat de Barcelona C/ Mart´ı i Franqu´es 1; E– 08028 Barcelona, Spain email: [email protected] 5 Observatoire de Paris-Meudon DAEC, F-92195 Meudon CEDEX, France email: [email protected] Received / Accepted Abstract. We have applied a relativistic Tolman-Bondi 1. Introduction model of the Virgo cluster to a sample of 183 galaxies with measured distances within a radius of 8 degrees from M 87. In 1990, Fouqu´eet al. (1990) derived an unbiased dis- We find that the sample is significantly contaminated by tance to the Virgo cluster, based on a complete sample background galaxies which lead to too large a cluster mean of 178 spiral galaxies, using the B-band Tully-Fisher re- distance if not excluded. The Tolman-Bondi model predic- lation (Tully & Fisher 1977). -
University of Groningen Diffuse Neutral Hydrogen in the Local
University of Groningen Diffuse neutral hydrogen in the Local Universe Popping, Attila 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: 2010 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Popping, A. (2010). Diffuse neutral hydrogen in the Local Universe. [s.n.]. 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). Take-down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. Downloaded from the University of Groningen/UMCG research database (Pure): http://www.rug.nl/research/portal. For technical reasons the number of authors shown on this cover page is limited to 10 maximum. Download date: 24-09-2021 6 The WSRT Virgo H i Filament Survey II: Cross Correlation Data ABSTRACT — In this chapter the cross-correlation product is described of the Westerbork Virgo Filament Survey (WVFS). This data was acquired simultaneously with the total-power data. By observing at very extreme hour angles, a filled aperture is sim- ulated of 300 25 meters in size, that has the typical collecting power and sensitivity of a single dish telescope,× but the well defined bandpass characteristics of an interferometer. -
The SLUGGS Survey: New Evidence for a Tidal Interaction Between the Early Type Galaxies NGC 4365 and NGC 4342
Mon. Not. R. Astron. Soc. 000, 000{000 (0000) Printed 16 October 2018 (MN LATEX style file v2.2) The SLUGGS Survey: New evidence for a tidal interaction between the early type galaxies NGC 4365 and NGC 4342 Christina Blom,1? Duncan A. Forbes,1 Caroline Foster;2;3 Aaron J. Romanowsky4;5 and Jean P. Brodie5 1Centre for Astrophysics and Supercomputing, Swinburne University, Hawthorn, VIC 3122, Australia 2Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia 3European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago 19001, Chile 4Department of Physics and Astronomy, San Jos´eState University,1 Washington Square, San Jose, CA 95192, USA 5University of California Observatories, 1156 High St., Santa Cruz, CA 95064, USA ? Email: [email protected] 16 October 2018 ABSTRACT We present new imaging and spectral data for globular clusters (GCs) around NGC 4365 and NGC 4342. NGC 4342 is a compact, X-ray luminous S0 galaxy with an unusually massive central black hole. NGC 4365 is another atypical galaxy that dominates the W 0 group of which NGC 4342 is a member. Using imaging from the MegaCam instrument on the Canada-France-Hawaii Telescope (CFHT) we identify a stream of GCs between the two galaxies and extending beyond NGC 4342. The stream of GCs is spatially coincident with a stream/plume of stars previously identified. We find that the photometric colours of the stream GCs match those associated with NGC 4342, and that the recession velocity of the combined GCs from the stream and NGC 4342 match the recession velocity for NGC 4342 itself. -
The Globular Cluster System of NGC 4365
The Globular Cluster System of NGC 4365 Christina Blom Presented in fulfillment of the requirements of the degree of Doctor of Philosophy May 2013 Faculty of Information and Communication Technology Swinburne University i Abstract This thesis presents a study of the globular cluster (GC) system of NGC 4365 and the GCs associated with the W 0 group of galaxies, of which NGC 4365 is the dominant galaxy. We use the analysis of these GC systems to investigate the evolutionary history of NGC 4365 as well as the ongoing interactions within the W 0 group. To analyse the photometric properties of NGC 4365's GC system we combined three filter imaging from the SuprimeCam instrument on the 8m Subaru telescope with eight, two filter, pointings from the Advanced Camera for Surveys on the Hubble Space Tele- scope. To analyse the kinematic properties of NGC 4365's GC system we obtained spectra for over 250 GCs around NGC 4365 from the DEep Imaging Multi-Object Spectrograph (DEIMOS) on the Keck II telescope. The photometric properties of the group GCs were analysed with square degree, three filter imaging from the MegaCam instrument on the Canada-France-Hawaii Telescope. We confirmed that NGC 4365 hosts three GC subpopulations, the usual blue and red GC subpopulations plus an additional subpopulation at intermediate colour: the green subpopulation. Photometric analysis showed that the three subpopulations have distinct radial and azimuthal distributions, different median sizes and mass distributions drawn from different populations. Using recession velocities calculated from GC spectra we also determined that each GC subpopulation rotates about the galaxy in a different direction. -
Spitzer/Infrared Array Camera Near-Infrared Features in the Outer Parts of S4G Galaxies
University of Louisville ThinkIR: The University of Louisville's Institutional Repository Faculty Scholarship 11-2014 Spitzer/Infrared Array Camera near-infrared features in the outer parts of S4G galaxies. Seppo Laine Spitzer Science Center Johan H. Knapen Universidad de La Laguna Juan Carlos Munoz-Mateos National Radio Astronomy Observatory Taehyun Kim Seoul National University Sebastien Comeron University of Oulu See next page for additional authors Follow this and additional works at: https://ir.library.louisville.edu/faculty Part of the Astrophysics and Astronomy Commons Original Publication Information Laine, Seppo, et al. "Spitzer/Infrared Array Camera Near-Infrared Features in the Outer Parts of S4G Galaxies." 2014. Monthly Notices of the Royal Astronomical Society 444(4): 3015-3039. This Article is brought to you for free and open access by ThinkIR: The University of Louisville's Institutional Repository. It has been accepted for inclusion in Faculty Scholarship by an authorized administrator of ThinkIR: The University of Louisville's Institutional Repository. For more information, please contact [email protected]. Authors Seppo Laine, Johan H. Knapen, Juan Carlos Munoz-Mateos, Taehyun Kim, Sebastien Comeron, Marie Martig, Benne W. Holwerda, E. Athanassoula, Albert Bosma, Peter H. Johansson, Santiago Erroz-Ferrer, Dimitri A. Gadotti, Armando Gil de Paz, Joannah Hinz, Jarkko Laine, Eija Laurikainen, Karin Menendez- Delmestre, Trisha Mizusawa, Michael Regan, Heikki Salo, Kartik Sheth, Mark Seibert, Ronald J. Buta, Mauricio Cisternas, Bruce G. Elmegreen, Debra M. Elmegreen, Luis C. Ho, Barry F. Madore, and Dennis Zaritsky This article is available at ThinkIR: The University of Louisville's Institutional Repository: https://ir.library.louisville.edu/ faculty/189 MNRAS 444, 3015–3039 (2014) doi:10.1093/mnras/stu1642 Spitzer/Infrared Array Camera near-infrared features in the outer parts of S4G galaxies Seppo Laine,1‹ Johan H. -
Box-And Peanut-Shaped Bulges: I. Statistics
A&A manuscript no. ASTRONOMY (will be inserted by hand later) AND Your thesaurus codes are: ASTROPHYSICS 11 (11.05.2; 11.19.2; 11.19.7; 11.19.6) November 9, 2018 Box- and peanut-shaped bulges ⋆ I. Statistics R. L¨utticke, R.-J. Dettmar, and M. Pohlen Astronomisches Institut, Ruhr-Universit¨at Bochum, D-44780 Bochum, Germany email: [email protected] Received 11 May 2000; accepted 14 June 2000 Abstract. We present a classification for bulges of a com- External cylindrically symmetric torques (May et al. plete sample of ∼ 1350 edge-on disk galaxies derived from 1985) or mergers of two disk galaxies (Binney & Petrou the RC3 (Third Reference Catalogue of Bright Galaxies, 1985, Rowley 1988) as origins of b/p bulges require very de Vaucouleurs et al. 1991). A visual classification of the special conditions (Bureau 1998). Therefore such evolu- bulges using the Digitized Sky Survey (DSS) in three types tionary scenarios can explain only a very low frequency of of b/p bulges or as an elliptical type is presented and sup- b/p bulges. Accretion of satellite galaxies is a formation ported by CCD images. NIR observations reveal that dust process of b/p bulges (Binney & Petrou 1985, Whitmore & extinction does almost not influence the shape of bulges. Bell 1988), which could produce a higher frequency of b/p There is no substantial difference between the shape of bulges. However, an oblique impact angle of the satellite bulges in the optical and in the NIR. Our analysis reveals is needed for the formation of a b/p bulge and a mas- that 45% of all bulges are box- and peanut-shaped (b/p). -
Kinematic Disturbances in Optical Rotation Curves Among 89 Virgo
KINEMATIC DISTURBANCES IN OPTICAL ROTATION CURVES AMONG 89 VIRGO DISK GALAXIES Vera C. Rubin1,2 Department of Terrestrial Magnetism, Carnegie Institution of Washington 5241 Broad Branch Road N.W., Washington, D.C. 20015 [email protected] Andrew H. Waterman3 Montgomery Blair High School, Silver Spring, MD and Jeffrey D. P. Kenney1,2 Astronomy Department, P.O. Box 208101, Yale University, New Haven, CT. 06520 Received ; accepted arXiv:astro-ph/9904050v1 3 Apr 1999 1Visiting Astronomer, Kitt Peak National Observatory, which is operated by AURA, Inc. under contract to the National Science Foundation. 2Observations at Palomar Observatory were made as part of a collaborative agreement between the California Institute of Technology and the Carnegie Institution of Washington. 3present address: Stanford University, Stanford, CA. –2– ABSTRACT For 89 galaxies, mostly spirals, in the Virgo cluster region, we have obtained optical long-slit major axis spectra of the ionized gas. We find: (1) One-half of the Virgo galaxies we observed have regular rotation patterns, while the other 50% exhibit kinematic disturbances ranging from mild to major. Velocity complexities are generally consistent with those resulting from tidal encounters or accretion events. Since kinematic disturbances are expected to fade within ∼109 years, many Virgo galaxies have experienced several significant kinematic disturbances during their lifetimes. (2) There is no strong correlation of rotation curve complexity with Hubble type, with galaxy luminosity, with local galaxy density, or with HI deficiency. (3) A few Virgo galaxies have ionized gas of limited extent, with velocities exceptionally low for their luminosities. In these galaxies the gas must be not rotationally supported. -
A Nearby Galaxy Perspective on Dust Evolution. Scaling Relations And
Astronomy & Astrophysics manuscript no. manuscript ©ESO 2021 January 5, 2021 A Nearby Galaxy Perspective on Dust Evolution Scaling relations and constraints on the dust build-up in galaxies with the DustPedia? and DGS samples Frédéric Galliano1, Angelos Nersesian2; 4, Simone Bianchi3, Ilse De Looze4; 5, Sambit Roychowdhury6; 7; 8, Maarten Baes4, Viviana Casasola9, Letizia, P. Cassara´10, Wouter Dobbels4, Jacopo Fritz11, Maud Galametz1, Anthony P. Jones6, Suzanne C. Madden1, Aleksandr Mosenkov12; 13, Emmanuel M. Xilouris2, and Nathalie Ysard6 1 AIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris Cité, F-91191 Gif-sur-Yvette, France e-mail: [email protected] 2 National Observatory of Athens, Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing, Ioannou Metaxa and Vasileos Pavlou GR-15236, Athens, Greece 3 INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125, Florence, Italy 4 Sterrenkundig Observatorium, Ghent University, Krijgslaan 281 - S9, 9000 Gent, Belgium 5 Dept. of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT, UK 6 Université Paris-Saclay, CNRS, Institut d’Astrophysique Spatiale, 91405 Orsay, France 7 International Centre for Radio Astronomy Research (ICRAR), M468, University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia 8 ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia 9 INAF – Istituto di Radioastronomia, Via P. Gobetti 101, 40129 Bologna, Italy 10 INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica, Via Alfonso Corti 12, 20133, Milan, Italy 11 Instituto de Radioastronomía y Astrofísica, UNAM, Antigua Carretera a Pátzcuaro # 8701, Ex-Hda. San José de la Huerta, 58089 Morelia, Michoacán, Mexico 12 Central Astronomical Observatory of RAS, Pulkovskoye Chaussee 65/1, 196140 St.