Minor-Axis Velocity Gradients in Spirals and the Case of Inner Polar Disks?,??
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Infrared Spectroscopy of Nearby Radio Active Elliptical Galaxies
The Astrophysical Journal Supplement Series, 203:14 (11pp), 2012 November doi:10.1088/0067-0049/203/1/14 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. INFRARED SPECTROSCOPY OF NEARBY RADIO ACTIVE ELLIPTICAL GALAXIES Jeremy Mould1,2,9, Tristan Reynolds3, Tony Readhead4, David Floyd5, Buell Jannuzi6, Garret Cotter7, Laura Ferrarese8, Keith Matthews4, David Atlee6, and Michael Brown5 1 Centre for Astrophysics and Supercomputing Swinburne University, Hawthorn, Vic 3122, Australia; [email protected] 2 ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) 3 School of Physics, University of Melbourne, Melbourne, Vic 3100, Australia 4 Palomar Observatory, California Institute of Technology 249-17, Pasadena, CA 91125 5 School of Physics, Monash University, Clayton, Vic 3800, Australia 6 Steward Observatory, University of Arizona (formerly at NOAO), Tucson, AZ 85719 7 Department of Physics, University of Oxford, Denys, Oxford, Keble Road, OX13RH, UK 8 Herzberg Institute of Astrophysics Herzberg, Saanich Road, Victoria V8X4M6, Canada Received 2012 June 6; accepted 2012 September 26; published 2012 November 1 ABSTRACT In preparation for a study of their circumnuclear gas we have surveyed 60% of a complete sample of elliptical galaxies within 75 Mpc that are radio sources. Some 20% of our nuclear spectra have infrared emission lines, mostly Paschen lines, Brackett γ , and [Fe ii]. We consider the influence of radio power and black hole mass in relation to the spectra. Access to the spectra is provided here as a community resource. Key words: galaxies: elliptical and lenticular, cD – galaxies: nuclei – infrared: general – radio continuum: galaxies ∼ 1. INTRODUCTION 30% of the most massive galaxies are radio continuum sources (e.g., Fabbiano et al. -
Radio Identification and Continuum Spectra of Decameter-Wavelength
Astronomy Reports, Vol. 47, No. 2, 2003, pp. 110–118. Translated from Astronomicheski˘ı Zhurnal, Vol. 80, No. 2, 2003, pp. 130–139. Original Russian Text Copyright c 2003 by Verkhodanov, Verkhodanova, Andernach. Radio Identification and Continuum Spectra of Decameter-Wavelength Sources O.V. Verkhodanov1, N. V. Verkhodanova1,andH.Andernach2 1Special Astrophysical Observatory, Russian Academy of Sciences, Nizhni ˘ı Arkhyz, Karachaevo-Cherkesskaya Republic, 357169 Russia 2University of Guanajuato, Department of Astronomy, Apdo Postal 144, Guanajuato, GTO, CP36000, Mexico´ Received March 22, 2002; in final form, June 26, 2002 Abstract—The paper describes a method for the radio identification of decameter-wavelength sources based on their continuum spectra and analysis of their coordinates in relatively large error boxes sur- rounding a specified position on the sky. The distribution of continuum spectra and identifications in other wavelength ranges are analyzed for the resulting radio catalog. Using identifications with the FIRST and NVSS surveys, the statistics of the spectral index–size and spectral index–fluxdensity distributions for steep-spectrum sources have been studied, and a catalog of ultrasteep-spectrum (α<−1.2) decameter- wavelength sources has been compiled. c 2003MAIK “Nauka/Interperiodica”. 1. INTRODUCTION 40 × 40cosecδ window obtained from a cross iden- tification with the CATS database [7]. We addressed The catalog of 1822 radio sources obtained with this problem via interactive processing of the radio the UTR telescope (Kharkov) by Braude et al.[1–5] spectra [8] obtained through a cross-identification at 10, 12.6, 14.7, 16.7, 20, and 25 MHz covers about of the UTR objects with sources from the CATS 30% of the sky and is the lowest-frequency catalog database using a 40 identification window. -
Observing Galaxies in Pegasus 01 October 2015 23:07
Observing galaxies in Pegasus 01 October 2015 23:07 Context As you look towards Pegasus you are looking below the galactic plane under the Orion spiral arm of our galaxy. The Perseus-Pisces supercluster wall of galaxies runs through this constellation. It stretches from RA 3h +40 in Perseus to 23h +10 in Pegasus and is around 200 million light years away. It includes the Pegasus I group noted later this document. The constellation is well placed from mid summer to late autumn. Pegasus is a rich constellation for galaxy observing. I have observed 80 galaxies in this constellation. Relatively bright galaxies This section covers the galaxies that were visible with direct vision in my 16 inch or smaller scopes. This list will therefore grow over time as I have not yet viewed all the galaxies in good conditions at maximum altitude in my 16 inch scope! NGC 7331 MAG 9 This is the stand out galaxy of the constellation. It is similar to our milky way. Around it are a number of fainter NGC galaxies. I have seen the brightest one, NGC 7335 in my 10 inch scope with averted vision. I have seen NGC 7331 in my 25 x 100mm binoculars. NGC 7814 - Mag 10 ? Not on observed list ? This is a very lovely oval shaped galaxy. By constellation Page 1 NGC 7332 MAG 11 / NGC 7339 MAG 12 These galaxies are an isolated bound pair about 67 million light years away. NGC 7339 is the fainter of the two galaxies at the eyepiece. I have seen NGC 7332 in my 25 x 100mm binoculars. -
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, -
Nuclear Activity in Circumnuclear Ring Galaxies
International Journal of Astronomy and Astrophysics, 2016, 6, 219-235 Published Online September 2016 in SciRes. http://www.scirp.org/journal/ijaa http://dx.doi.org/10.4236/ijaa.2016.63018 Nuclear Activity in Circumnuclear Ring Galaxies María P. Agüero1, Rubén J. Díaz2,3, Horacio Dottori4 1Observatorio Astronómico de Córdoba, UNCand CONICET, Córdoba, Argentina 2ICATE, CONICET, San Juan, Argentina 3Gemini Observatory, La Serena, Chile 4Instituto de Física, UFRGS, Porto Alegre, Brazil Received 23 May 2016; accepted 26 July 2016; published 29 July 2016 Copyright © 2016 by authors and Scientific Research Publishing Inc. This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/ Abstract We have analyzed the frequency and properties of the nuclear activity in a sample of galaxies with circumnuclear rings and spirals (CNRs), compiled from published data. From the properties of this sample a typical circumnuclear ring can be characterized as having a median radius of 0.7 kpc (mean 0.8 kpc, rms 0.4 kpc), located at a spiral Sa/Sb galaxy (75% of the hosts), with a bar (44% weak, 37% strong bars). The sample includes 73 emission line rings, 12 dust rings and 9 stellar rings. The sample was compared with a carefully matched control sample of galaxies with very similar global properties but without detected circumnuclear rings. We discuss the relevance of the results in regard to the AGN feeding processes and present the following results: 1) bright companion galaxies seem -
Astronomy Magazine 2011 Index Subject Index
Astronomy Magazine 2011 Index Subject Index A AAVSO (American Association of Variable Star Observers), 6:18, 44–47, 7:58, 10:11 Abell 35 (Sharpless 2-313) (planetary nebula), 10:70 Abell 85 (supernova remnant), 8:70 Abell 1656 (Coma galaxy cluster), 11:56 Abell 1689 (galaxy cluster), 3:23 Abell 2218 (galaxy cluster), 11:68 Abell 2744 (Pandora's Cluster) (galaxy cluster), 10:20 Abell catalog planetary nebulae, 6:50–53 Acheron Fossae (feature on Mars), 11:36 Adirondack Astronomy Retreat, 5:16 Adobe Photoshop software, 6:64 AKATSUKI orbiter, 4:19 AL (Astronomical League), 7:17, 8:50–51 albedo, 8:12 Alexhelios (moon of 216 Kleopatra), 6:18 Altair (star), 9:15 amateur astronomy change in construction of portable telescopes, 1:70–73 discovery of asteroids, 12:56–60 ten tips for, 1:68–69 American Association of Variable Star Observers (AAVSO), 6:18, 44–47, 7:58, 10:11 American Astronomical Society decadal survey recommendations, 7:16 Lancelot M. Berkeley-New York Community Trust Prize for Meritorious Work in Astronomy, 3:19 Andromeda Galaxy (M31) image of, 11:26 stellar disks, 6:19 Antarctica, astronomical research in, 10:44–48 Antennae galaxies (NGC 4038 and NGC 4039), 11:32, 56 antimatter, 8:24–29 Antu Telescope, 11:37 APM 08279+5255 (quasar), 11:18 arcminutes, 10:51 arcseconds, 10:51 Arp 147 (galaxy pair), 6:19 Arp 188 (Tadpole Galaxy), 11:30 Arp 273 (galaxy pair), 11:65 Arp 299 (NGC 3690) (galaxy pair), 10:55–57 ARTEMIS spacecraft, 11:17 asteroid belt, origin of, 8:55 asteroids See also names of specific asteroids amateur discovery of, 12:62–63 -
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 -
Optical Surface Photometry of a Sample of Disk Galaxies. II
A&A manuscript no. ASTRONOMY (will be inserted by hand later) AND Your thesaurus codes are: 3 (11.19.2; 11.19.5; 11.19.7) ASTROPHYSICS Optical Surface Photometry of a Sample of Disk Galaxies. II Structural Components M. Prieto1, J. A. L. Aguerri1,2,A. M. Varela1 & C. Mu˜noz-Tu˜n´on1 1.- Instituto de Astrof´ısica de Canarias, E-38200 La Laguna, Tenerife, Spain 2.- Astronomisches Institut der Universitat Basel, CH-4102 Binningen, Switzerland Received ; accepted Abstract. This work presents the structural decomposi- In general, the B/D relation has very little reliability due tion of a sample of 11 disk galaxies, which span a range to these above-mentioned reasons and also because the of different morphological types. The U, B, V , R, and I bulge scale length is sometimes smaller than the seeing photometric information given in Paper I (color and color- disk. Perhaps the most reliable decompositions are those index images and luminosity, ellipticity, and position-angle for galaxies with a very well defined disk. This means, well profiles) has been used to decide what types of components sampled and free from other emission features. form the galaxies before carrying out the decomposition. In recent decades much work has been done in or- We find and model such components as bulges, disks, bars, der to improve the methods for ascertaining the principal lenses and rings. (bulge and disk) components of disk galaxies from their optical photometric profiles. Kormendy (1977), Boroson’s (1981), Shombert & Bothum (1987), Kent (1987), Capac- Key words: Galaxies: optical photometry, galaxies: cioli, Held, & Nieto (1987), Andredakis & Sanders (1994), structure, galaxies: fundamental parameters, galaxies: spi- De Jong (1996), Moriondo, Giovanardi, & Hunt (1997). -
Counterrotation in Galaxies 3
COUNTERROTATION IN GALAXIES F. BERTOLA AND E.M. CORSINI Dipartimento di Astronomia, Universit`adi Padova vicolo dell’Osservatorio 5, I-35122 Padova, Italy 1. Introduction The phenomenon of counterrotation is observed when two galaxy compo- nents have their angular momenta projected antiparallel onto the sky. It follows that if the two components rotate around the same axis, the counter- rotation is intrinsic. On the contrary the counterrotation is only apparent if the rotation axes are misaligned and the line-of-sight lies in between the two vectors or their antivectors. In the case of intrinsic counterrotation the two components can be superimposed or radially separated. As far as the two components are concerned, stars are observed to coun- terrotate with respect to other stars or gas. The counterrotation of gas ver- sus gas has been also detected. Up to now, the number of galaxies exhibiting these phenomena are ∼ 60, the morphological type of which ranges from ellipticals to S0’s and to spirals. Previous reviews about counterrotation are those of Rubin (1994b) and Galletta (1996). When a second event occurs in a galaxy, such as the acquisition of ma- terial from outside, it is likely that the resulting angular momentum of the acquired material is decoupled from the angular momentum of the preex- arXiv:astro-ph/9802314v1 24 Feb 1998 isting galaxy. Counterrotation is therefore a general signature of material acquired from outside the main confines of the galaxy. Good examples of such cases are ellipticals with a dust lane or gaseous disk along the minor axis and polar ring galaxies, where the angular momenta are perpendicular. -
A Complete Redshift Survey to the Zwicky Catalog Limit in a 2-Hour by 15-Degree Region Around 3C
A Complete Redshift Survey to the Zwicky Catalog Limit in a 2h × 15◦ Region Around 3C 273 Norman A. Grogin, Margaret J. Geller, and John P. Huchra Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 E-mail: ngrogin, mgeller, [email protected] ABSTRACT We compile 1113 redshifts (648 new measurements, 465 from the literature) for Zwicky catalogue galaxies in the region (−3◦.5 ≤ δ ≤ 8◦.5, 11h.5 ≤ α ≤ 13h.5). We include redshifts for 114 component objects in 78 Zwicky catalogue multiplets. The redshift survey in this region is 99.5% complete to the Zwicky catalogue limit, mZw = 15.7. It is 99.9% complete to mZw = 15.5, the CfA Redshift Survey (CfA2) magnitude limit. The survey region is adjacent to the northern portion of CfA2, overlaps the northernmost slice of the Las Campanas Redshift Survey, includes the southern extent of the Virgo Cluster, and is roughly centered on the QSO 3C 273. As in other portions of the Zwicky catalogue, bright and faint galaxies trace the same large-scale structure. Subject headings: cosmology: observations — galaxies: distances and redshifts — galaxies: interactions 1. Introduction arXiv:astro-ph/9807067v1 7 Jul 1998 The Center for Astrophysics Redshift Survey (hereafter CfA2, Geller & Huchra 1989) of galaxies from Zwicky’s Catalogue of Galaxies and Clusters of Galaxies (Zwicky et al. 1961–1968, hereafter CGCG) still remains one of the best re- sources for the study of the nearby galaxy distribution. In a recent paper (Gro- gin & Geller 1998), we used CfA2 to investigate the connection between local −1 (cz ∼< 10000 km s ) Lyman-alpha absorption systems observed with HST (Bah- call et al. -
Near-IR Photometry of Disk Galaxies: Search for Nuclear Isophotal Twist
A&A manuscript no. (will be inserted by hand later) ASTRONOMY AND Your thesaurus codes are: ASTROPHYSICS 04 (11.16.1; 11.19.2; 11.06.2; 11.19.6) 17.6.2021 Near-IR photometry of disk galaxies: search for nuclear isophotal twist and double bars Bruno Jungwiert1,2, Fran¸coise Combes1 and Dave J. Axon3 1 DEMIRM, Observatoire de Paris, 61 Avenue de l’Observatoire, 75 014 Paris, France 2 Astronomical Institute, Academy of Sciences of the Czech Republic, Boˇcn´ıII 1401, 141 31 Prague 4, Czech Republic 3 ESA secondment, Space Telescope Science Institute, Baltimore, MD 21218, USA Received 29 November 1996 / Accepted 21 January 1997 Abstract. We present a near-IR, mainly H band, pho- medium (ISM) into the nuclear region. Numerous obser- tometry of 72 nearby (d < 40 Mpc) disk galaxies. The vations complete the picture by showing that various kinds main goal of the survey was to search for isophotal twist of central activity, like Seyfert nuclei (e.g. Hummel et al. inside their nuclear regions. As the twist can be due in 1987), LINERs and starbursts (e.g. Devereux 1989, Tele- some cases to projection effects, rather than resulting from sco et al. 1993) are often correlated with the presence a dynamical phenomenon, we deproject – under the sim- of bars (note however counter-examples of many Seyferts plifying assumption of a 2D geometry – all galaxies whose (McLeod & Rieke 1995), as well as galaxies with strong disk position angle and inclination are known, the latter IR excess (Pompea & Rieke 1990), that do not show any not exceeding 75o.