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Characterizing the Radial Oxygen Abundance Distribution in Disk Galaxies? I
A&A 623, A7 (2019) Astronomy https://doi.org/10.1051/0004-6361/201834364 & c ESO 2019 Astrophysics Characterizing the radial oxygen abundance distribution in disk galaxies? I. A. Zinchenko1,2, A. Just2, L. S. Pilyugin1,2, and M. A. Lara-Lopez3 1 Main Astronomical Observatory, National Academy of Sciences of Ukraine, 27 Akademika Zabolotnoho St., 03680 Kyiv, Ukraine e-mail: [email protected] 2 Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr. 12–14, 69120 Heidelberg, Germany 3 Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark Received 2 October 2018 / Accepted 13 January 2019 ABSTRACT Context. The relation between the radial oxygen abundance distribution (gradient) and other parameters of a galaxy such as mass, Hubble type, and a bar strength, remains unclear although a large amount of observational data have been obtained in the past years. Aims. We examine the possible dependence of the radial oxygen abundance distribution on non-axisymmetrical structures (bar/spirals) and other macroscopic parameters such as the mass, the optical radius R25, the color g − r, and the surface brightness of the galaxy. A sample of disk galaxies from the third data release of the Calar Alto Legacy Integral Field Area Survey (CALIFA DR3) is considered. Methods. We adopted the Fourier amplitude A2 of the surface brightness as a quantitative characteristic of the strength of non- axisymmetric structures in a galactic disk, in addition to the commonly used morphologic division for A, AB, and B types based on the Hubble classification. To distinguish changes in local oxygen abundance caused by the non-axisymmetrical structures, the multiparametric mass–metallicity relation was constructed as a function of parameters such as the bar/spiral pattern strength, the disk size, color index g−r in the Sloan Digital Sky Survey (SDSS) bands, and central surface brightness of the disk. -
Galaxies with Rows A
Astronomy Reports, Vol. 45, No. 11, 2001, pp. 841–853. Translated from Astronomicheski˘ı Zhurnal, Vol. 78, No. 11, 2001, pp. 963–976. Original Russian Text Copyright c 2001 by Chernin, Kravtsova, Zasov, Arkhipova. Galaxies with Rows A. D. Chernin, A. S. Kravtsova, A. V. Zasov, and V. P. Arkhipova Sternberg Astronomical Institute, Universitetskii˘ pr. 13, Moscow, 119899 Russia Received March 16, 2001 Abstract—The results of a search for galaxies with straight structural elements, usually spiral-arm rows (“rows” in the terminology of Vorontsov-Vel’yaminov), are reported. The list of galaxies that possess (or probably possess) such rows includes about 200 objects, of which about 70% are brighter than 14m.On the whole, galaxies with rows make up 6–8% of all spiral galaxies with well-developed spiral patterns. Most galaxies with rows are gas-rich Sbc–Scd spirals. The fraction of interacting galaxies among them is appreciably higher than among galaxies without rows. Earlier conclusions that, as a rule, the lengths of rows are similar to their galactocentric distances and that the angles between adjacent rows are concentrated near 120◦ are confirmed. It is concluded that the rows must be transient hydrodynamic structures that develop in normal galaxies. c 2001 MAIK “Nauka/Interperiodica”. 1. INTRODUCTION images were reproduced by Vorontsov-Vel’yaminov and analyze the general properties of these objects. The long, straight features found in some galaxies, which usually appear as straight spiral-arm rows and persist in spite of differential rotation of the galaxy 2. THE SAMPLE OF GALAXIES disks, pose an intriguing problem. These features, WITH STRAIGHT ROWS first described by Vorontsov-Vel’yaminov (to whom we owe the term “rows”) have long escaped the To identify galaxies with rows, we inspected about attention of researchers. -
SAC's 110 Best of the NGC
SAC's 110 Best of the NGC by Paul Dickson Version: 1.4 | March 26, 1997 Copyright °c 1996, by Paul Dickson. All rights reserved If you purchased this book from Paul Dickson directly, please ignore this form. I already have most of this information. Why Should You Register This Book? Please register your copy of this book. I have done two book, SAC's 110 Best of the NGC and the Messier Logbook. In the works for late 1997 is a four volume set for the Herschel 400. q I am a beginner and I bought this book to get start with deep-sky observing. q I am an intermediate observer. I bought this book to observe these objects again. q I am an advance observer. I bought this book to add to my collect and/or re-observe these objects again. The book I'm registering is: q SAC's 110 Best of the NGC q Messier Logbook q I would like to purchase a copy of Herschel 400 book when it becomes available. Club Name: __________________________________________ Your Name: __________________________________________ Address: ____________________________________________ City: __________________ State: ____ Zip Code: _________ Mail this to: or E-mail it to: Paul Dickson 7714 N 36th Ave [email protected] Phoenix, AZ 85051-6401 After Observing the Messier Catalog, Try this Observing List: SAC's 110 Best of the NGC [email protected] http://www.seds.org/pub/info/newsletters/sacnews/html/sac.110.best.ngc.html SAC's 110 Best of the NGC is an observing list of some of the best objects after those in the Messier Catalog. -
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. -
Nearby Supernova Host Galaxies from the CALIFA Survey: II. SN
Astronomy & Astrophysics manuscript no. IFU_P2_v10 c ESO 2018 June 17, 2018 Nearby supernova host galaxies from the CALIFA Survey: II. SN environmental metallicity L. Galbany1, 2, V. Stanishev3, A. M. Mourão3, M. Rodrigues4, 5, H. Flores5, C. J. Walcher6, S. F. Sánchez7, R. García-Benito8, D. Mast9, C. Badenes10, R. M. González Delgado8, C. Kehrig8, M. Lyubenova11, R. A. Marino12, 13 M. Mollá14, S. Meidt15, E. Pérez8, G. van de Ven15, J. M. Vílchez8 (Affiliations can be found after the references) Received December 26th / Accepted ————- ABSTRACT The metallicity of a supernova progenitor, together with its mass, is one of the main parameters that can rule their outcome. We present the second study of nearby supernova (SN) host galaxies (0.005 < z < 0.03) using Integral Field Spectroscopy (IFS) from the CALIFA survey. We analyze the metallicity of 115 galaxies, which hosted 132 SNe within and 10 SNe outside the field-of-view (FoV) of the instrument. Further 18 galaxies, which hosted only SNe outside the FoV were also studied. Using the O3N2 calibrator from Marino et al. (2013) we found no statistically significant differences between the gas-phase metallicities at the locations of the three main SN types – Ia, Ib/c and II, all having 12 + log(O/H) ≃ 8.50 within 0.02 dex. The total galaxy metallicities are also very similar and we argue that this is because our sample consists only of SNe discovered in massive galaxies (log(M/M⊙) > 10 dex) by targeted searches. We also found no evidence that the metallicity at the SN location differs from the average metallicity at the galactocentric distance of the SNe. -
Dynamics of Barred Galaxies
Reports on Progress in Physics 56 (1993) 173-255 Dynamics of Barred Galaxies J A Sellwood1,2 and A Wilkinson3 1Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 2Department of Physics and Astronomy, Rutgers University, PO Box 849, Piscataway, NJ 08855-0849, USA 3Department of Astronomy, The University, Manchester M13 9PL, England Abstract Some 30% of disc galaxies have a pronounced central bar feature in the disc plane and many more have weaker features of a similar kind. Kinematic data indicate that the bar constitutes a major non-axisymmetric component of the mass distribution and that the bar pattern tumbles rapidly about the axis normal to the disc plane. The observed motions are consistent with material within the bar streaming along highly elongated orbits aligned with the rotating major axis. A barred galaxy may also contain a spheroidal bulge at its centre, spirals in the outer disc and, less commonly, other features such as a ring or lens. Mild asymmetries in both the light and kinematics are quite common. We review the main problems presented by these complicated dynamical systems and sum- marize the effort so far made towards their solution, emphasizing results which appear secure. Bars are probably formed through a global dynamical instability of a rotationally supported galactic disc. Studies of the orbital structure seem to indicate that most stars in the bar follow regular orbits but that a small fraction may be stochastic. Theoretical work on the three-dimensional structure of bars is in its infancy, but first results suggest that bars should be thicker in the third dimension than the disc from which they formed. -
The Extragalactic Distance Scale Sidney Van Den Bergh
THE EXTRAGALACTIC DISTANCE SCALE SIDNEY VAN DEN BERGH Dominion Astrophysical Observatory National Research Council of Canada 5071 West Saanich Road Victoria, British Columbia V8X 4M6, Canada - 2 - ABSTRACT Cepheid variables are used to derive a Virgo cluster distance of 16.0 ± 1.5 Mpc. In conjunction with the Coma velocity and the well-established -1 Coma/Virgo distance ratio, this yields a Hubble parameter Ho = 81 ± 8 km s Mpc-1. By combining this value with an age of the Universe / 16.8 ± 2.1 Gyr, that is derived from the metal-poor globular cluster M92, one obtains f (S, 7) / 1.39 ± 0.22. This value is only marginally consistent with an Einstein-de Sitter universe with S = 0 and 7 = 0, which has f = 1. An Einstein-de Sitter universe with S = 1 and 7 = 0, for which f = b , appears to be excluded at the 3F level. It is shown that some recent small values of Ho resulted from the large intrinsic dispersion in the linear diameters of galaxies, and from the fact that well-observed supernovae of Type Ia exhibit a luminosity range of ~30 at maximum light. - 3 - 1. INTRODUCTION Seventy-six years ago Curtis (1921) and Shapley(1921) met in this auditorium to present their differing views on the nature of the nebulae. Shapley believed that our Milky Way galaxy was a vast continent surrounded by small island nebulae. On the other hand, Curtis advocated the view that spiral nebulae were very distant objects with dimensions similar to that of our own Milky Way System. -
The Duality of Spiral Structure, and a Quantitative Dust Penetrated Morphological Tuning Fork at Low and High Redshift
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server Galaxy Disks and Disk Galaxies ASP Conference Series, Vol. 3 108, 2000 J.G. Funes S.J., and E.M. Corsini,× eds. The Duality of Spiral Structure, and a Quantitative Dust Penetrated Morphological Tuning Fork at Low and High Redshift D. L. Block, I. Puerari and R. J. Buta Department of Computational and Applied Mathematics, University of the Witwatersrand, Johannesburg, South Africa R. Abraham Department of Astronomy, University of Toronto, Toronto, Canada M. Takamiya Gemini Observatory, Hilo, HI A. Stockton Institute for Astronomy, University of Hawaii, Honolulu, HI Abstract. In the near-infrared, the morphology of older star-dominated disks indicates a simple classification scheme (1) Hm where m is the dom- inant harmonic, (2) a pitch angle (derived from the Fourier spectra) as- sociated with the rate of shear A/ω in the stellar disk and (3) a ‘bar strength’ parameter, robustly derived from the gravitational potential or torque of the bar. A spiral galaxy may present two radically different morphologies in the optical and near-infrared regime; there is no cor- relation between our quantitative dust penetrated tuning fork and that of Hubble. Applications of our z 0 Fourier template to the HDF are discussed using L and M band simulations∼ from an 8-m NGST; the rest- wavelength IR morphology of high-z galaxies should probably be a key factor in deciding the final choice of instruments for the NGST. 1. Introduction There is a fundamental limit in predicting what an evolved stellar disk might look like (Block et al. -
Clues from NGC 922
A&A 371, 393–403 (2001) Astronomy DOI: 10.1051/0004-6361:20010081 & c ESO 2001 Astrophysics Dust-penetrated morphology in the high-redshift universe: Clues from NGC 922 D. L. Block1, I. Puerari2, M. Takamiya3, R. Abraham4,A.Stockton5, I. Robson6, and W. Holland6 1 Dept. of Computational and Applied Mathematics, University of the Witwatersrand, Private Bag 3, WITS 2050, South Africa 2 Instituto Nacional de Astrof´ısica, Optica y Electr´onica, Calle Luis Enrique Erro 1, 72840 Tonantzintla, Puebla, M´exico 3 Gemini Observatory, 670 North Aohoku Place, Hilo, HI 96720, USA 4 Department of Astronomy, University of Toronto, 60 St. George Str., Toronto, ON M5S 3H8, Canada 5 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 6 Joint Astronomy Centre, Univ. Park, 660 North Aohoku Place, Hilo, HI 96720, USA Received 16 November 2000 / Accepted 4 January 2001 Abstract. Results from the Hubble Deep Field (HDF) North and South show a large percentage of high-redshift galaxies whose appearance falls outside traditional classification systems. The nature of these objects is poorly understood, but sub-mm observations indicate that at least some of these systems are heavily obscured (Sanders 2000). This raises the intriguing possibility that a physically meaningful classification system for high-redshift galaxies might be more easily devised at rest-frame infrared wavelengths, rather than in the optical regime. Practical realization of this idea will become possible with the advent of the Next Generation Space Telescope (NGST). In order to explore the capability of NGST for undertaking such science, we present NASA-IRTF and SCUBA observations of NGC 922, a chaotic system in our local Universe which bears a striking resemblance to objects such as HDF 2-86 (z =0.749) in the HDF North. -
Galaxy Morphology Ronald J
Secular evolution of galaxies XXIII Canary Islands Winter School of Astrophysics Edited by J. Falc´on-Barroso and J. H. Knapen arXiv:1304.3529v1 [astro-ph.CO] 12 Apr 2013 Galaxy morphology Ronald J. Buta Department of Physics and Astronomy, University of Alabama Box 870324, Tuscaloosa, AL 35487, USA [email protected] Abstract Galaxy morphology has many structures that are suggestive of various processes or stages of secular evolution. Internal perturbations such as bars can drive secular evolution through gravity torques that move gas into the central regions and build up a flattened, disk-like central bulge, or which may convert an open spiral pseudoring into a more closed ring. Interaction between individual components of a galaxy, such as between a bar and a dark halo, a bar and a central mass concentration, or between a perturbation and the basic state of a stellar disk, can also drive secular transformations. In this series of lectures, I review many aspects of galaxy morphology with a view to delineating some of the possible evolutionary pathways between different galaxy types. 2.1 Introductory remarks A principal goal of extragalactic studies has been to understand what drives the morphology of galaxies. It is important to determine the dynamical and evolutionary mechanisms that underlie the bewildering array of forms that define the various galaxy classification schemes used today (e.g., Sandage & Bedke 1994; Buta et al. 2007), because this will allow us to establish the relationships, if any, between different galaxy types. Physical -
Index of Objects
Cambridge University Press 978-1-107-00054-4 - Dynamics of Galaxies: Second Edition Giuseppe Bertin Index More information Index of objects Galaxies NGC 3198, 31, 36, 175–6, 178, 255, 276, 283, NGC 221 (= M32), 20, 321, 350 285, 287, 293 NGC 224 (= M31), 4–5, 48, 80, 282–3, 289, NGC 3344, 264 321, 350, 381 NGC 3377, 321 NGC 309, 258, 265, 288 NGC 3379, 32–3, 314, 342, 344, 347, 371, 373, NGC 598 (= M33), 223–4, 381 376, 379, 385–6 NGC 628 (= M74), 23, 174, 259, 261, 265 NGC 3521, 36 NGC 720, 375, 377 NGC 3741, 259 NGC 801, 36, 284 NGC 3923, 386 NGC 821, 379 NGC 3938, 264 NGC 3998, 159 NGC 891, 24, 177, 180, 182 NGC 4013, 276 NGC 936, 264 NGC 4038, 75 NGC 1035, 284 NGC 4039, 75 NGC 1058, 259 NGC 4244, 27 NGC 1068, 445–6 NGC 4254 (= M99), 223–4, 256, 258, 261, 264 NGC 1300, 13, 225, 254, 256 NGC 4258 (= M106), 294, 321–2, 350, 445 NGC 1316, 386 NGC 4278, 378 NGC 1344, 387 NGC 4321 (= M100), 23, 224, 254, 264–5 NGC 1365, 225 NGC 4374, 33, 373, 387, 405–6 NGC 1379, 410–1 NGC 4406, 386 NGC 1399, 351, 373, 376, 379, 385–6, NGC 4472 (= M49), 347, 349–50, 370–3, 375–6, 405–6 379, 385–6, 405–6 NGC 1404, 373, 405–6 NGC 4486 (= M87), 5, 8, 20, 72, 80, 321, 350–1, NGC 1407, 388 376, 379, 385–6 NGC 1549, 22 NGC 4494, 379 NGC 1566, 21 NGC 4550, 37 NGC 1637, 265, 288 NGC 4552, 33, 410–1 NGC 2300, 382 NGC 4559, 177 NGC 2403, 28, 31, 177 NGC 4565, 27 = NGC 2599 ( UGC 4458), 36 NGC 4594 (= M104), 321 NGC 2663, 37 NGC 4596, 264 NGC 2683, 36 NGC 4622, 223, 254, 256–7, 288 NGC 2685, 159 NGC 4636, 5, 373, 375, 379, 385–6, 405–6 NGC 2841, 22 NGC 4649 (= M60),