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Fourier Dissection of Early-Type Galaxy Bars R
The Astronomical Journal, 132:1859Y1876, 2006 November # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. FOURIER DISSECTION OF EARLY-TYPE GALAXY BARS R. Buta,1 E. Laurikainen,2 H. Salo,2 D. L. Block,3 and J. H. Knapen4 Received 2006 May 4; accepted 2006 July 14 ABSTRACT This paper reports on a near-infrared survey of early-type galaxies designed to provide information on bar strengths, bulges, disks, and bar parameters in a statistically well-defined sample of S0YSa galaxies. Early-type galaxies have the advantage that their bars are relatively free of the effects of dust, star formation, and spiral structure that com- plicate bar studies in later type galaxies. We describe the survey and present results on a detailed analysis of the rela- tive Fourier intensity amplitudes of bars in 26 early-type galaxies. We also evaluate the ‘‘symmetry assumption’’ of these amplitudes with radius, used recently for bar-spiral separation in later type galaxies. The results show a wide variety of radial Fourier profiles of bars, ranging from simple symmetric profiles that can be represented in terms of a single Gaussian component to both symmetric and asymmetric profiles that can be represented by two overlapping Gaussian components. More complicated profiles than these are also found, often due to multiple barlike features including extended ovals or lenses. Based on the gravitational bar torque indicator Qb, double-Gaussian bars are stronger on average than single-Gaussian bars, at least for our small sample. We show that published numerical simulations in which the bar transfers a large amount of angular momentum to the halo can account for many of the observed profiles. -
John J. Cowan Date of Birth: April 3, 1948 Place of Birth: Washington, D.C
VITA NAME: John J. Cowan Date of Birth: April 3, 1948 Place of Birth: Washington, D.C. EDUCATION: 1970 B.A. George Washington University, Washington, D.C. 1972 M.S. Case Institute of Technology, Cleveland, OH 1976 Ph.D. University of Maryland, College Park, MD PROFESSIONAL EXPERIENCE: 2002–present David Ross Boyd Professor, University of Oklahoma, 2002–2002 Research Fellow, University of Texas, Austin, TX 1998–2002 Samuel Roberts Noble Foundation Presidential Professor, University of Oklahoma, Norman, OK 1997–1998 Big XIIFaculty Fellow,University ofOklahoma 1991–1992 Visiting Professor, Department of Astronomy, Columbia University, New York, NY 1989–present Professor, Department of Physics and Astronomy, University of Oklahoma, Norman, OK 1988–1994 Consultant and Participating Guest, Lawrence Livermore National Laboratory, Livermore, CA 1987–1988 Visiting Research Associate, Harvard-Smithsonian Center for Astrophysics, Harvard University, Cambridge, MA 1984–1989 Associate Professor, University of Oklahoma 1979–1984 Assistant Professor, University of Oklahoma 1976–1979 Postdoctoral Research Fellow, Harvard-Smithsonian Center for Astrophysics, Harvard University PROFESSIONAL AND HONORARY SOCIETIES: American Astronomical Society International Astronomical Union Phi Beta Kappa RESEARCH INTERESTS: Stellar evolution, supernovae, nucleosynthesis and abundances Radio observations of supernovae and galaxies JOHN J. COWAN Page 2 PUBLICATIONS J. J. Cowan and W. K. Rose, “Production of 17O and 18O by Means of the Hot CNO Tri-Cycle,” Astrophys. J. (Letters) 201, L45 (1975) J. J. Cowan, M. Kafatos, and W. K. Rose, “Sources of Excitation of the Interstellar Gas and Galactic Structure,” Astrophys. J. 195, 47 (1975) M. F. A’Hearn and J. J. Cowan, “Molecular Production Rates in Comet Kohoutek,” As- tron. -
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. -
198 7Apj. . .312L. .11J the Astrophysical Journal, 312:L11-L15
.11J The Astrophysical Journal, 312:L11-L15,1987 January 1 .312L. © 1987. The American Astronomical Society. All rights reserved. Printed in U.S.A. 7ApJ. 198 INTERSTELLAR DUST IN SHAPLEY-AMES ELLIPTICAL GALAXIES M. Jura and D. W. Kim Department of Astronomy, University of California, Los Angeles AND G. R. Knapp and P. Guhathakurta Princeton University Observatory Received 1986 August 11; accepted 1986 September 30 ABSTRACT We have co-added the IRAS survey data at the positions of the brightest elliptical galaxies in the Revised Shapley-Ames Catalog to increase the sensitivity over that of the IRAS Point Source Catalog. More than half of 7 8 the galaxies (with Bj< \\ mag) are detected at 100 /xm with flux levels indicating, typically, 10 or 10 M0 of cold interstellar matter. The presence of cold gas in ellipticals thus appears to be the rule rather than the exception. Subject headings: galaxies: general — infrared: sources I. INTRODUCTION infrared emission from the elliptical galaxy in the line of sight. The traditional view of early-type galaxies is that they are Our criteria for a real detection are as follows: essentially free of interstellar matter. However, with advances 1. The optical position of the galaxy and the position of the in instrumental sensitivity, it has become possible to observe IRAS source agree to better than V. (The agreement is usually 21 cm emission (Knapp, Turner, and Cunniffe 1985; Wardle much better than T.) and Knapp 1986), optical dust patches (Sadler and Gerhard 2. The flux is at least 3 times the r.m.s. noise. -
The Local Galaxy Volume
11-1 How Far Away Is It – The Local Galaxy Volume The Local Galaxy Volume {Abstract – In this segment of our “How far away is it” video book, we cover the local galaxy volume compiled by the Spitzer Local Volume Legacy Survey team. The survey covered 258 galaxies within 36 million light years. We take a look at just a few of them including: Dwingeloo 1, NGC 4214, Centaurus A, NGC 5128 Jets, NGC 1569, majestic M81, Holmberg IX, M82, NGC 2976,the unusual Circinus, M83, NGC 2787, the Pinwheel Galaxy M101, the Sombrero Galaxy M104 including Spitzer’s infrared view, NGC 1512, the Whirlpool Galaxy M51, M74, M66, and M96. We end with a look at the tuning fork diagram created by Edwin Hubble with its description of spiral, elliptical, lenticular and irregular galaxies.} Introduction [Music: Johann Pachelbel – “Canon in D” – This is Pachelbel's most famous composition. It was written in the 1680s between the times of Galileo and Newton. The term 'canon' originates from the Greek kanon, which literally means "ruler" or "a measuring stick." In music, this refers to timing. In astronomy, "a measuring stick" refers to distance. We now proceed to galaxies more distant than the ones in our Local Group.] The Local volume is the set of galaxies covered in the Local Volume Legacy survey or LVL, for short, conducted by the Spitzer team. It is a complete sample of 258 galaxies within 36 million light years. This montage of images shows the ensemble of galaxies as observed by Spitzer. The galaxies are randomly arranged but their relative sizes are as they appear on the sky. -
Luminous Blue Variables
Review Luminous Blue Variables Kerstin Weis 1* and Dominik J. Bomans 1,2,3 1 Astronomical Institute, Faculty for Physics and Astronomy, Ruhr University Bochum, 44801 Bochum, Germany 2 Department Plasmas with Complex Interactions, Ruhr University Bochum, 44801 Bochum, Germany 3 Ruhr Astroparticle and Plasma Physics (RAPP) Center, 44801 Bochum, Germany Received: 29 October 2019; Accepted: 18 February 2020; Published: 29 February 2020 Abstract: Luminous Blue Variables are massive evolved stars, here we introduce this outstanding class of objects. Described are the specific characteristics, the evolutionary state and what they are connected to other phases and types of massive stars. Our current knowledge of LBVs is limited by the fact that in comparison to other stellar classes and phases only a few “true” LBVs are known. This results from the lack of a unique, fast and always reliable identification scheme for LBVs. It literally takes time to get a true classification of a LBV. In addition the short duration of the LBV phase makes it even harder to catch and identify a star as LBV. We summarize here what is known so far, give an overview of the LBV population and the list of LBV host galaxies. LBV are clearly an important and still not fully understood phase in the live of (very) massive stars, especially due to the large and time variable mass loss during the LBV phase. We like to emphasize again the problem how to clearly identify LBV and that there are more than just one type of LBVs: The giant eruption LBVs or h Car analogs and the S Dor cycle LBVs. -
The Distribution of Absorbing Column Densities Among Seyfert 2 Galaxies
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server The distribution of absorbing column densities among Seyfert 2 galaxies G. Risaliti Dipartimento di Astronomia e Scienza dello Spazio, Univerit`a di Firenze, L. E. Fermi 5, I-50125, Firenze, Italy R. Maiolino and M. Salvati Osservatorio Astrofisico di Arcetri, L. E. Fermi 5, I-50125 Firenze, Italy ABSTRACT We use hard X-ray data for an “optimal” sample of Seyfert 2 galaxies to derive the distribution of the gaseous absorbing column densities among obscured active nuclei in the local Universe. Of all Seyfert 2 galaxies in the sample, 75% are heavily obscured 23 2 24 2 (NH > 10 cm− ) and about half are Compton thick (NH > 10 cm− ). Intermediate type 1.8–1.9 Seyferts are characterized by an average NH much lower than “strict” Seyfert 2s. No correlation is found between NH and the intrinsic luminosity of the nuclear source. This NH distribution has important consequences for the synthesis of the cosmic X-ray background. Also, the large fraction of Compton thick objects implies that most of the obscuring gas is located within a radius of a few 10 pc from the nucleus. Subject headings: Galaxies: active — Galaxies: nuclei — Galaxies: Seyfert — X-rays: galaxies 1. Introduction According to the so-called unified model (Antonucci 1993) the same engine is at work in all Active Galactic Nuclei (AGNs). The differences between type 1 and type 2 AGNs are ascribed solely to orientation effects: our line of sight to the nucleus may (type 2) or may not (type 1) be obstructed by optically thick material, perhaps distributed in a toroidal geometry. -
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”. -
Exors and the Stellar Birthline Mackenzie S
A&A 600, A133 (2017) Astronomy DOI: 10.1051/0004-6361/201630196 & c ESO 2017 Astrophysics EXors and the stellar birthline Mackenzie S. L. Moody1 and Steven W. Stahler2 1 Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA e-mail: [email protected] 2 Astronomy Department, University of California, Berkeley, CA 94720, USA e-mail: [email protected] Received 6 December 2016 / Accepted 23 February 2017 ABSTRACT We assess the evolutionary status of EXors. These low-mass, pre-main-sequence stars repeatedly undergo sharp luminosity increases, each a year or so in duration. We place into the HR diagram all EXors that have documented quiescent luminosities and effective temperatures, and thus determine their masses and ages. Two alternate sets of pre-main-sequence tracks are used, and yield similar results. Roughly half of EXors are embedded objects, i.e., they appear observationally as Class I or flat-spectrum infrared sources. We find that these are relatively young and are located close to the stellar birthline in the HR diagram. Optically visible EXors, on the other hand, are situated well below the birthline. They have ages of several Myr, typical of classical T Tauri stars. Judging from the limited data at hand, we find no evidence that binarity companions trigger EXor eruptions; this issue merits further investigation. We draw several general conclusions. First, repetitive luminosity outbursts do not occur in all pre-main-sequence stars, and are not in themselves a sign of extreme youth. They persist, along with other signs of activity, in a relatively small subset of these objects. -
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. -
The Impact of the Astro2010 Recommendations on Variable Star Science
The Impact of the Astro2010 Recommendations on Variable Star Science Corresponding Authors Lucianne M. Walkowicz Department of Astronomy, University of California Berkeley [email protected] phone: (510) 642–6931 Andrew C. Becker Department of Astronomy, University of Washington [email protected] phone: (206) 685–0542 Authors Scott F. Anderson, Department of Astronomy, University of Washington Joshua S. Bloom, Department of Astronomy, University of California Berkeley Leonid Georgiev, Universidad Autonoma de Mexico Josh Grindlay, Harvard–Smithsonian Center for Astrophysics Steve Howell, National Optical Astronomy Observatory Knox Long, Space Telescope Science Institute Anjum Mukadam, Department of Astronomy, University of Washington Andrej Prsa,ˇ Villanova University Joshua Pepper, Villanova University Arne Rau, California Institute of Technology Branimir Sesar, Department of Astronomy, University of Washington Nicole Silvestri, Department of Astronomy, University of Washington Nathan Smith, Department of Astronomy, University of California Berkeley Keivan Stassun, Vanderbilt University Paula Szkody, Department of Astronomy, University of Washington Science Frontier Panels: Stars and Stellar Evolution (SSE) February 16, 2009 Abstract The next decade of survey astronomy has the potential to transform our knowledge of variable stars. Stellar variability underpins our knowledge of the cosmological distance ladder, and provides direct tests of stellar formation and evolution theory. Variable stars can also be used to probe the fundamental physics of gravity and degenerate material in ways that are otherwise impossible in the laboratory. The computational and engineering advances of the past decade have made large–scale, time–domain surveys an immediate reality. Some surveys proposed for the next decade promise to gather more data than in the prior cumulative history of astronomy. -
Stellar Population Gradient in Lenticular Galaxies: NGC 1023, NGC 3115 and NGC 4203
A&A 410, 803–812 (2003) Astronomy DOI: 10.1051/0004-6361:20031261 & c ESO 2003 Astrophysics Stellar population gradient in lenticular galaxies: NGC 1023, NGC 3115 and NGC 4203 M. Bassin1 and Ch. Bonatto1 Universidade Federal do Rio Grande do Sul, Instituto de F´ısica, CP 15051, Porto Alegre CEP 91501-970, RS, Brazil Received 11 March 2003 / Accepted 2 July 2003 Abstract. We investigate the stellar population content in the lenticular galaxies NGC 1023, NGC 3115 and NGC 4203 applying a population synthesis method based on a seven component spectral basis with different ages – 2.5 106,10 106,25 106,75 106, 200 106,1.2 109 and older than 1010 years, and metallicity in the range 1.3 ×[Z/Z ] × 0.2. This× study employs× two-dimensional× × STIS spectra in the range λλ2900–5700 Å, obtained from the Hubble− ≤ Space Telescope ≤− public archives. We extracted one-dimensional spectra in adjacent windows 100 pc wide (projected distance) from the nuclear regions up to 300–400 pc. The largest contribution, both in λ5870 Å flux and mass fraction, comes from old stars (age > 1010 years). We verified the possible existence of circumnuclear bursts (CNBs) in NGC 3115 and NGC 4203. Key words. galaxies: elliptical and lenticular, cD – galaxies: stellar content – galaxies: nuclei 1. Introduction the purpose of determining the star formation history in galax- ies based on integrated properties. A precise determination of properties of the stellar content of Two main approaches have been considered: evolutionary galaxies is clearly an important issue, since they are related synthesis, a technique to study the spectrophotometric evolu- to the galaxy formation and evolution.