Observational Studies of the Galaxy Peculiar Velocity Field
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Nuclear Star Formation in NGC 6240
A&A 415, 103–116 (2004) Astronomy DOI: 10.1051/0004-6361:20034183 & c ESO 2004 Astrophysics Nuclear star formation in NGC 6240 A. Pasquali1,2,J.S.Gallagher3, and R. de Grijs4 1 ESO/ST-ECF, Karl-Schwarzschild-Strasse 2, 85748 Garching bei M¨unchen, Germany 2 Institute of Astronomy, ETH H¨onggerberg, 8093 Z¨urich, Switzerland 3 University of Wisconsin, Department of Astronomy, 475 N. Charter St., Madison WI 53706, USA e-mail: [email protected] 4 University of Sheffield, Department of Physics and Astronomy, Hicks Building, Hounsfield Road, Sheffield S3 7RH, UK e-mail: [email protected] Received 12 August 2003 / Accepted 6 November 2003 Abstract. We have made use of archival HST BVIJH photometry to constrain the nature of the three discrete sources, A1, A2 and B1, identified in the double nucleus of NGC 6240. STARBURST99 models have been fitted to the observed colours, under the assumption, first, that these sources can be treated as star clusters (i.e. single, instantaneous episodes of star formation), and subsequently as star-forming regions (i.e. characterised by continuous star formation). For both scenarios, we estimate ages as young as 4 million years, integrated masses ranging between 7 106 M (B1) and 109 M (A1) and a rate of 1 supernova per × 1 year, which, together with the stellar winds, sustains a galactic wind of 44 M yr− . In the case of continuous star formation, 1 a star-formation rate has been derived for A1 as high as 270 M yr− , similar to what is observed for warm Ultraluminous 3 Infrared Galaxies (ULIRGs) with a double nucleus. -
XIII Publications, Presentations
XIII Publications, Presentations 1. Refereed Publications E., Kawamura, A., Nguyen Luong, Q., Sanhueza, P., Kurono, Y.: 2015, The 2014 ALMA Long Baseline Campaign: First Results from Aasi, J., et al. including Fujimoto, M.-K., Hayama, K., Kawamura, High Angular Resolution Observations toward the HL Tau Region, S., Mori, T., Nishida, E., Nishizawa, A.: 2015, Characterization of ApJ, 808, L3. the LIGO detectors during their sixth science run, Classical Quantum ALMA Partnership, et al. including Asaki, Y., Hirota, A., Nakanishi, Gravity, 32, 115012. K., Espada, D., Kameno, S., Sawada, T., Takahashi, S., Ao, Y., Abbott, B. P., et al. including Flaminio, R., LIGO Scientific Hatsukade, B., Matsuda, Y., Iono, D., Kurono, Y.: 2015, The 2014 Collaboration, Virgo Collaboration: 2016, Astrophysical Implications ALMA Long Baseline Campaign: Observations of the Strongly of the Binary Black Hole Merger GW150914, ApJ, 818, L22. Lensed Submillimeter Galaxy HATLAS J090311.6+003906 at z = Abbott, B. P., et al. including Flaminio, R., LIGO Scientific 3.042, ApJ, 808, L4. Collaboration, Virgo Collaboration: 2016, Observation of ALMA Partnership, et al. including Asaki, Y., Hirota, A., Nakanishi, Gravitational Waves from a Binary Black Hole Merger, Phys. Rev. K., Espada, D., Kameno, S., Sawada, T., Takahashi, S., Kurono, Lett., 116, 061102. Y., Tatematsu, K.: 2015, The 2014 ALMA Long Baseline Campaign: Abbott, B. P., et al. including Flaminio, R., LIGO Scientific Observations of Asteroid 3 Juno at 60 Kilometer Resolution, ApJ, Collaboration, Virgo Collaboration: 2016, GW150914: Implications 808, L2. for the Stochastic Gravitational-Wave Background from Binary Black Alonso-Herrero, A., et al. including Imanishi, M.: 2016, A mid-infrared Holes, Phys. -
Evidence of Enhanced Star Formation Efficiency in Luminous And
Astronomy & Astrophysics manuscript no. main c ESO 2018 October 24, 2018 Evidence of enhanced star formation efficiency in luminous and ultraluminous infrared galaxies⋆ J. Graci´a-Carpio1,2, S. Garc´ıa-Burillo2, P. Planesas2, A. Fuente2, and A. Usero2,3 1 FRACTAL SLNE, Castillo de Belmonte 1, Bloque 5 Bajo A, E-28232 Las Rozas de Madrid, Spain 2 Observatorio Astron´omico Nacional (OAN), Observatorio de Madrid, Alfonso XII 3, E-28014 Madrid, Spain 3 Centre for Astrophysics Research, University of Hertfordshire, College Lane, AL10 9AB, Hatfield, UK e-mail: [email protected], [email protected], [email protected], [email protected], [email protected] Received 4 July 2007; accepted 4 December 2007 ABSTRACT We present new observations made with the IRAM 30m telescope of the J=1–0 and 3–2 lines of HCN and HCO+ used to probe the dense molecular gas content in a sample of 17 local luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs). These observations have allowed us to derive an updated version of the power law describing the correlation between the FIR luminosity ′ (LFIR) and the HCN(1–0) luminosity (LHCN(1−0)) of local and high-redshift galaxies. We present the first clear observational evidence ′ that the star formation efficiency of the dense gas (SFEdense), measured as the LFIR/LHCN(1−0) ratio, is significantly higher in LIRGs and ULIRGs than in normal galaxies, a result that has also been found recently in high-redshift galaxies. This may imply a statistically 11 significant turn upward in the Kennicutt-Schmidt law derived for the dense gas at LFIR ≥ 10 L⊙. -
1. Introduction
THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 122:109È150, 1999 May ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. GALAXY STRUCTURAL PARAMETERS: STAR FORMATION RATE AND EVOLUTION WITH REDSHIFT M. TAKAMIYA1,2 Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637; and Gemini 8 m Telescopes Project, 670 North Aohoku Place, Hilo, HI 96720 Received 1998 August 4; accepted 1998 December 21 ABSTRACT The evolution of the structure of galaxies as a function of redshift is investigated using two param- eters: the metric radius of the galaxy(Rg) and the power at high spatial frequencies in the disk of the galaxy (s). A direct comparison is made between nearby (z D 0) and distant(0.2 [ z [ 1) galaxies by following a Ðxed range in rest frame wavelengths. The data of the nearby galaxies comprise 136 broad- band images at D4500A observed with the 0.9 m telescope at Kitt Peak National Observatory (23 galaxies) and selected from the catalog of digital images of Frei et al. (113 galaxies). The high-redshift sample comprises 94 galaxies selected from the Hubble Deep Field (HDF) observations with the Hubble Space Telescope using the Wide Field Planetary Camera 2 in four broad bands that range between D3000 and D9000A (Williams et al.). The radius is measured from the intensity proÐle of the galaxy using the formulation of Petrosian, and it is argued to be a metric radius that should not depend very strongly on the angular resolution and limiting surface brightness level of the imaging data. It is found that the metric radii of nearby and distant galaxies are comparable to each other. -
On the Relation Between Circular Velocity and Central Velocity Dispersion in High and Low Surface Brightness Galaxies1 A
The Astrophysical Journal, 631:785–791, 2005 October 1 A # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. ON THE RELATION BETWEEN CIRCULAR VELOCITY AND CENTRAL VELOCITY DISPERSION IN HIGH AND LOW SURFACE BRIGHTNESS GALAXIES1 A. Pizzella,2 E. M. Corsini,2 E. Dalla Bonta`,2 M. Sarzi,3 L. Coccato,2 and F. Bertola2 Received 2005 January 5; accepted 2005 March 24 ABSTRACT In order to investigate the correlation between the circular velocity Vc and the central velocity dispersion of the spheroidal component c , we analyzed these quantities for a sample of 40 high surface brightness (HSB) disk galaxies, eight giant low surface brightness (LSB) spiral galaxies, and 24 elliptical galaxies characterized by flat À1 À1 rotation curves. Galaxies have been selected to have a velocity gradient 2kms kpc for R 0:35R25.Weused these data to better define the previous Vc-c correlation for spiral galaxies (which turned out to be HSB) and elliptical galaxies, especially at the lower end of the c values. We find that the Vc-c relation is described by a linear À1 law out to velocity dispersions as low as c 50 km s , while in previous works a power law was adopted for À1 galaxies with c > 80 km s . Elliptical galaxies with Vc based on dynamical models or directly derived from the H i rotation curves follow the same relation as the HSB galaxies in the Vc-c plane. On the other hand, the LSB galaxies follow a different relation, since most of them show either higher Vc or lower c with respect to the HSB galaxies. -
Comprehensive Broadband X-Ray and Multiwavelength Study of Active Galactic Nuclei in Local 57 Ultra/Luminous Infrared Galaxies Observed with Nustar And/Or Swift/BAT
Draft version July 26, 2021 Typeset using LATEX twocolumn style in AASTeX631 Comprehensive Broadband X-ray and Multiwavelength Study of Active Galactic Nuclei in Local 57 Ultra/luminous Infrared Galaxies Observed with NuSTAR and/or Swift/BAT Satoshi Yamada ,1 Yoshihiro Ueda ,1 Atsushi Tanimoto ,2 Masatoshi Imanishi ,3, 4 Yoshiki Toba ,1, 5 Claudio Ricci ,6, 7, 8 and George C. Privon 9 1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan 2Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan 3National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, Japan 4Department of Astronomical Science, Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan 5Research Center for Space and Cosmic Evolution, Ehime University, 2-5 Bunkyo-cho, Matsuyama, Ehime 790-8577, Japan 6N´ucleo de Astronom´ıade la Facultad de Ingenier´ıa,Universidad Diego Portales, Av. Ej´ercito Libertador 441, Santiago, Chile 7Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, People's Republic of China 8George Mason University, Department of Physics & Astronomy, MS 3F3, 4400 University Drive, Fairfax, VA 22030, USA 9National Radio Astronomy Observatory, 520 Edgemont Rd, Charlottesville, VA 22903, USA (Received April 13, 2021; Revised June 11, 2021; Accepted Jul, 2021) ABSTRACT We perform a systematic X-ray spectroscopic analysis of 57 local ultra/luminous infrared galaxy systems (containing 84 individual galaxies) observed with Nuclear Spectroscopic Telescope Array and/or Swift/BAT. Combining soft X-ray data obtained with Chandra, XMM-Newton, Suzaku and/or Swift/XRT, we identify 40 hard (>10 keV) X-ray detected active galactic nuclei (AGNs) and con- strain their torus parameters with the X-ray clumpy torus model XCLUMPY (Tanimoto et al. -
Bias Mitigation in Galaxy Zoo Using Machine Learning Techniques
UC Irvine UC Irvine Electronic Theses and Dissertations Title Bias Mitigation in Galaxy Zoo Using Machine Learning Techniques Permalink https://escholarship.org/uc/item/7241p065 Author Silva do Nascimento Neto, Pedro Publication Date 2019 License https://creativecommons.org/licenses/by/4.0/ 4.0 Peer reviewed|Thesis/dissertation eScholarship.org Powered by the California Digital Library University of California UNIVERSITY OF CALIFORNIA, IRVINE Bias Mitigation in Galaxy Zoo Using Machine Learning Techniques DISSERTATION submitted in partial satisfaction of the requirements for the degree of DOCTOR OF PHILOSOPHY in Computer Science by Pedro Silva do Nascimento Neto Dissertation Committee: Professor Wayne Hayes, Chair Professor Aaron Barth Professor Eric Mjolsness 2019 c 2019 Pedro Silva do Nascimento Neto DEDICATION To my beloved wife, Elise. ii TABLE OF CONTENTS Page LIST OF FIGURES v LIST OF TABLES x LIST OF ALGORITHMS xii ACKNOWLEDGMENTS xiii CURRICULUM VITAE xv ABSTRACT OF THE DISSERTATION xvii 1 Introduction 1 2 Spiral Galaxy Recognition Using Arm Analysis and Random Forests 4 2.1 Introduction . 5 2.1.1 Related Work . 8 2.1.2 Regression, Not Classification, Because Galaxy Morphology Is Contin- uous, Not Discrete . 11 2.2 Methods . 13 2.3 Results . 17 2.3.1 Features, Trees, and Forests . 17 2.3.2 Adding SpArcFiRe Features . 18 2.3.3 Feature Quality . 26 2.3.4 Comparison with Other Regression Methods . 28 2.4 Conclusions . 30 3 The Chirality Bias in Galaxy Zoo 1 32 3.1 Introduction . 33 3.2 Nature of the bias . 36 3.2.1 More S-wise than Z-wise spins for all values of \spirality" . -
In IAU Symp. 193, Wolf-Rayet Phenomena in Stars and Starburst
Synthesis Models for Starburst Populations with Wolf-Rayet Stars Claus Leitherer Space Telescope Science Institute1, 3700 San Martin Drive, Baltimore, MD 21218 Abstract. The prospects of utilizing Wolf-Rayet populations in star- burst galaxies to infer the stellar content are reviewed. I discuss which Wolf-Rayet star features can be detected in an integrated stellar pop- ulation. Specific examples are given where the presence of Wolf-Rayet stars can help understand galaxy properties independent of the O-star population. I demonstrate how populations with small age spread, such as super star clusters, permit observational tests to distinguish between single-star and binary models to produce Wolf-Rayet stars. Different synthesis models for Wolf-Rayet populations are compared. Predictions for Wolf-Rayet properties vary dramatically between individual models. The current state of the models is such that a comparison with starburst populations is more useful for improving Wolf-Rayet atmosphere and evo- lution models than for deriving the star-formation history and the initial mass function. 1. Wolf-Rayet Signatures in Young Populations The central 30 Doradus region has the highest concentration of Wolf-Rayet (WR) stars in the LMC. Parker et al. (1995) classify 15 stars within 2000 (or 5 pc) of R136 as WR stars, including objects which may appear WR-like due to very dense winds (de Koter et al. 1997). This suggests that about 1 out of 10 ionizing stars around R136 is of WR type. The WR stars can be seen in an ultraviolet (UV) drift-scan spectrum of the integrated 30 Dor population obtained by Vacca et al. -
Emissão Infra - Vermelha De Galáxias Iras
UNIVERSIDADE FEDERAL DO RIO GRANDE DO SUL INSTITUTO DE FÍSICA EMISSÃO INFRA - VERMELHA DE GALÁXIAS IRAS Charles José Bonatto Tese realizada sob a orientação da Dra. Miriani G. Pastoriza e apresentada ao Instituto de Física da UFRGS, em preenchi- mento parcial dos requisitos para a obtenção do título de Doutor em Física. Porto Alegre 1992 *Trabalho financiado pelo Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq). Aos meus pais, irmãos e cunhados. Agradecimentos À Miriani Pastoriza por sua orientação e confiança; À Sebastian Lípari por ter fornecido as observações de CASLEO; A todo o pessoal do Departamento de Astronomia, pelos bons momentos que têm sido proporcionados; Ao pessoal da Biblioteca, em especial à Zuleika e à Ana; A todas as pessoas que direta ou indiretamente contribuíram para este trabalho; Ao CNPq, pelo financiamento deste trabalho; À FAPERGS, pelo apoio financeiro em um dos turnos em Tololo. Resumo Galáxias ativas emitem fortemente no infra-vermelho. Grãos de poeira, aquecidos por fótons Ultra-Violeta e ópticos absorvem estes fótons e os re-emitem no infra-vermelho. Atualmente, esta é a interpretação mais provável para esta emissão no infra-vermelho. Neste trabalho, desenvolvemos um modelo para a emissão e distribuição espacial dos graõs de poeira, incluindo a contribuição de uma lei-de-potência. Usamos galáxias com observações no óptico e no infra-vermelho, separando-as em Seyfert tipo 1 e 2, para analisar as relações entre luminosidades de linhas de emissão no óptico e a luminosidade no infra-vermelho (LIR). Contando o número de galáxias com L r.. dentro de um determinado intervalo, mostramos que as distribuições de LIR de Seyferts tipo 1 e 2 são quase idênticas. -
Classification of Galaxies Using Fractal Dimensions
UNLV Retrospective Theses & Dissertations 1-1-1999 Classification of galaxies using fractal dimensions Sandip G Thanki University of Nevada, Las Vegas Follow this and additional works at: https://digitalscholarship.unlv.edu/rtds Repository Citation Thanki, Sandip G, "Classification of galaxies using fractal dimensions" (1999). UNLV Retrospective Theses & Dissertations. 1050. http://dx.doi.org/10.25669/8msa-x9b8 This Thesis is protected by copyright and/or related rights. It has been brought to you by Digital Scholarship@UNLV with permission from the rights-holder(s). You are free to use this Thesis in any way that is permitted by the copyright and related rights legislation that applies to your use. For other uses you need to obtain permission from the rights-holder(s) directly, unless additional rights are indicated by a Creative Commons license in the record and/ or on the work itself. This Thesis has been accepted for inclusion in UNLV Retrospective Theses & Dissertations by an authorized administrator of Digital Scholarship@UNLV. For more information, please contact [email protected]. INFORMATION TO USERS This manuscript has been reproduced from the microfilm master. UMI films the text directly from the original or copy submitted. Thus, some thesis and dissertation copies are in typewriter face, while others may be from any type of computer printer. The quality of this reproduction is dependent upon the quality of the copy submitted. Broken or indistinct print, colored or poor quality illustrations and photographs, print bleedthrough, substandard margins, and improper alignment can adversely affect reproduction. In the unlikely event that the author did not send UMI a complete manuscript and there are missing pages, these will be noted. -
Understanding the H2/HI Ratio in Galaxies 3
Mon. Not. R. Astron. Soc. 394, 1857–1874 (2009) Printed 6 August 2021 (MN LATEX style file v2.2) Understanding the H2/HI Ratio in Galaxies D. Obreschkow and S. Rawlings Astrophysics, Department of Physics, University of Oxford, Keble Road, Oxford, OX1 3RH, UK Accepted 2009 January 12 ABSTRACT galaxy We revisit the mass ratio Rmol between molecular hydrogen (H2) and atomic hydrogen (HI) in different galaxies from a phenomenological and theoretical viewpoint. First, the local H2- mass function (MF) is estimated from the local CO-luminosity function (LF) of the FCRAO Extragalactic CO-Survey, adopting a variable CO-to-H2 conversion fitted to nearby observa- 5 1 tions. This implies an average H2-density ΩH2 = (6.9 2.7) 10− h− and ΩH2 /ΩHI = 0.26 0.11 ± · galaxy ± in the local Universe. Second, we investigate the correlations between Rmol and global galaxy properties in a sample of 245 local galaxies. Based on these correlations we intro- galaxy duce four phenomenological models for Rmol , which we apply to estimate H2-masses for galaxy each HI-galaxy in the HIPASS catalog. The resulting H2-MFs (one for each model for Rmol ) are compared to the reference H2-MF derived from the CO-LF, thus allowing us to determine the Bayesian evidence of each model and to identify a clear best model, in which, for spi- galaxy ral galaxies, Rmol negatively correlates with both galaxy Hubble type and total gas mass. galaxy Third, we derive a theoretical model for Rmol for regular galaxies based on an expression for their axially symmetric pressure profile dictating the degree of molecularization. -
The NGC 1614 Interacting Galaxy Molecular Gas Feeding a “Ring of fire”
A&A 553, A72 (2013) Astronomy DOI: 10.1051/0004-6361/201220453 & c ESO 2013 Astrophysics The NGC 1614 interacting galaxy Molecular gas feeding a “ring of fire” S. König1,2,S.Aalto3, S. Muller3,R.J.Beswick4, and J. S. Gallagher III5 1 Institut de Radioastronomie Millimétrique, 300 rue de la Piscine, Domaine Universitaire, 38406 Saint-Martin d’Hères, France e-mail: [email protected] 2 Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark 3 Chalmers University of Technology, Department of Radio and Space Science, Onsala Space Observatory, 43992 Onsala, Sweden 4 University of Manchester, Jodrell Bank Centre for Astrophysics, Oxford Road, Manchester, M13 9PL, UK 5 Department of Astronomy, University of Wisconsin, 475 N Charter Street, Madison, WI, 53706, USA Received 27 September 2012 / Accepted 1 March 2013 ABSTRACT Minor mergers frequently occur between giant and gas-rich low-mass galaxies and can provide significant amounts of interstellar matter to refuel star formation and power active galactic nuclei (AGN) in the giant systems. Major starbursts and/or AGN result when fresh gas is transported and compressed in the central regions of the giant galaxy. This is the situation in the starburst minor merger NGC 1614, whose molecular medium we explore at half-arcsecond angular resolution through our observations of 12CO (2−1) emission using the Submillimeter Array (SMA). We compare our 12CO (2−1) maps with optical and Paα, Hubble Space Telescope and high angular resolution radio continuum images to study the relationships between dense molecular gas and the NGC 1614 starburst region.