DOCSLIB.ORG

Sterrenstelsels En Kosmologie

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Sterrenstelsels En Kosmologie Sterrenstelsels en Kosmologie Docent: Huub Röttgering, kamer 465, email: [email protected] College assistent: Chael Kruip, kamer 401, email: [email protected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ijfer 1. Mondeling tentamen 2. Opgaven moeten worden ingeleverd bij het volgende college. Antwoorden tellen mee voor 30 % voor tentamen cijfer, indien tentamen wordt afgelegd voor 1 augustus 2010 Brief content of the course 1) Introduction What is a galaxy ? What is an active galaxy? Classifications, multiwavelength observations, luminosity functions 2) Keeping a galaxy together: Gravity, Potentials 3) Galactic Dynamics Equilibrium, Collisions, Virial Theorem 4) Galactic Dynamics continued Timescales, Orbits 5) Collisionless Boltzmann Equation equilibrium, phase mixing derivation of distribution function 6) Velocity Moments Jeans equations comparison to observations 7) Mass distribution and dark matter Evidence for dark matter from rotation curves Solar neighbourhood, Oort limit Elliptical galaxies and hot gas Candidate dark matter particles 8) Galaxy formation Universe expansion Cosmic microwave background Growth of galaxies by gravity Galaxy scaling relations 9) Galaxy formation - forming the stars Gas cooling and star formation formation of disks dynamical friction and mergers tidal tails in mergers 10) Clusters and Large scale structure 11) Active Galaxies Classification Building blocks Feedback mechanisms Overview • Our galaxy (PS 1.1 - 1.2.3) • History of early galaxy studies (PS. p. 87) • Optical classification and galaxy profiles (PS. 3.1.1, 3.2.1,3.2.2,3.3.2) • Multi-wavelength view • Luminosity functions (PS 3.7 intro, 3.7.1) • Active galactic nuclei (a bit of 5.1.1-3, 5.2) • Main questions Our galaxy (PS 1.1 - 1.2.3) • A panorama of the Milky Way, as seen from Death Valley, 2005. • see: http://en.wikipedia.org/wiki/Milky_Way ZF8%Y>[> YY ZF8%Y>[> • =QD%*6/0",%@K]%.%@K]%/$'6*)9%@?%N;'%/#%[?%O;' • IJ%#(*4%U/4%5:$%0/1/.7,% – 5:$%4:)%/#%]K?%N;'9% – 5$L*2)0%/#%V>>?%N6T49% – #/N*)0%>[?%6*11*5)%7"/$4 • L$*0(#%L1:"%N)5#4,%75:)0%4#/$4 • $"+%015U,%51+%4#/$49%6/*)17%*)%#("%L:10" • 0/1/.7%#5%#("%1"^,%+*4#5$#"+%'56;/)*5)%0/1/.7 Y> NGC 4013 Y[ ZF8%_?Y[ • 5L4"$R"+%"+0"<5)%L7%`:LL1" • +*4N%5L4':$"+%L7%+:4# • '")#$/1%L:10" Y_ a:$%0/1/.7 Y\ D("%F/1/.7 • #(*)%+*4N%5J%75:)0%4#/$4%/)+%0/4%U*#(%/%$/+*:4% 5J%>?%N;'%/)+%/%4'/1"%("*0(#%5J%[??%;'K% • V%Y%N;'%#(*'N%+*4N%U(*'(%'5)#/*)4%/)%51+"$% 4#"11/$%;5;:1/25)%'56;/$"+%#5%#("%#(*)%+*4N • /%'")#$/1%L:10"%5J%51+%4#/$4% • 4;("$*'/1%(/15%'5)#/*)*)0%654#%5J%#("%015L:1/$% '1:4#"$4%/)+%456"%5J%#("%51+"4#%4#/$4% Y@ b5#/25)%/)+%+/$N%6/S"$ Yc • b5#/25)%R"15'*#7, GM(r0) V0 = R0 • R*4*L1"%6/S"$%0*R"4%J5$%#("%4:)%/#%b5%d%]%N;'% Y@?%N6T4% • e"%6"/4:$"%>>?%N6T4%+:"%#5%E+/$N%6/S"$H • Z/#:$"%5J%6/S"$%:)N)5U)K – U"/N17%*)#"$/'2)0%;/$2'1"4f – J$""%g5/2)0%$5'N4f Y] History of early galaxy studies (PS. p. 87) Messier (1730-1817) compiled his ”Catalogue des Nébuleuses et des John Dreyerʼs AY]\><Yh>@B% Amas d’Étoiles” (“Catalogue of Nebulae contribution was the monumental and Star Clusters”) New General Catalogue of Nebulae and Clusters of Stars >? 1920: Great debate on the nature of galaxies between Slipher and in Curtis. Vesto Melvin Slipher Are the nebulae in or (1875 - 1969) outside our galaxy? demonstrated that galaxies rotate >Y %%%%%()*&+,-.//'$ Yh>\,% !"$*5+%1:6*)54*#7%$"1/25)% J5$%8";("*+4%*)%/)+$56"+/, O[Y%/#%/%+*4#/)'"%5J%>]\% N;'%AJ/'#5$%[%#55%46/11B >> `*4#5$7 • O"44*"$%AYc[?<Y]YcB%1*4#4%Y?[%+*i:4"%5Lj"'#4 – O[Y,%3)+$56"+/%)"L:1/ • X5()%G$"*"$%AY]\><Yh>@B,%Z"U%F")"$/1%'/#/150:" – ]???%5Lj"'#4 • YhY>,%="4#5%&1*;("$%6"/4:$"+%#(/#%4;*$/1%)"L:1/"%/$"% $5#/2)0 • Yh>?,%F$"/#%+"L/#"%L"#U"")%&(/;1"7%/)+%8:$24 – /$"%)"L:1/"%*)4*+"%5$%5:#4*+"%#("%0/1/.7f% • Yh>\,%!"$*5+%1:6*)54*#7%$"1/25)%J5$%8";("*+4%*)% /)+$56"+/ – O[Y%/#%/%+*4#/)'"%5J%>]\%N;'%AJ/'#5$%[%#55%46/11B% >[ Optical classification and galaxy profiles (PS. 3.1.1, 3.2.1,3.2.2, 3.3.2) Optical images of galaxies and classification All classification systems are idealisations. Independent of true size of the galaxy ! Classifications problems: Galaxies ‘’look’’ different depending on Depth of image Projection effects Band observed / redshift Often used system: Hubble-Sandage tuning fork diagram >@ M94 - Sa M81 - Sb M101 - Sc M95 - SBa NGC 1300 - SBb NGC 7741 - SBc >] The S0 or lenticular galaxy NGC 3115 QO8%<%I$$%I% %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%O]>%<%I$$%II [? Hubble tuning fork diagram Left: ‘early types’, right: `late types’ Elliptical galaxies ellipical isophotes: vary from round to highly elongated En, where n=10[1-(b/a)], with b/a apparent axial radio (note projection effects) Subdivision cD galaxies: central cluster galaxies, M=10^13-10^14 solar mass Giant ellipticals (gE’s) Normal ellipticals -23 < M_B < -15, M=10^8-10^13M Dwarf ellipticals (dE’s), Blue compact dwarf galaxies: bluer than normal, relatively gas-rich Dwarf spheroidals: low luminosity and surface brightness, M=10^7-10^9 M Spirals S: without bar, SB with bar a, ab, b, bc, c, cd, d, from ``early’’ type to ``late’’ type L_bulge/L_tot ~0.3 for a, ~0.13 for b and ~0.05 for c opening angles ~6 deg for a, ~12 deg for b and ~18 deg for c S0 or Lenticular galaxies: ‘ellipticals with signs of disks’’ SB0 or Barred Lenticular galaxies: ‘ellipticals with signs of barred disks’’ Irregulars: Irr I : some regular structure (extension of Sd) Irr II: weak regular structure -11*;2'/1%0/1/.*"4,% L$*0(#)"44%;$5P1" Elliptical galaxies normally follow an r 1/4 law: 1/4 I(R) = Ie exp(!7.67[(R/Re) ! 1]), The constant is chosen so that where Re is the half light radius: half the light is emitted inside Re. Because of uncertainties in the background subtraction, we never know the exact half light radius. The parameter Ie is the surface brightness at R = Re. No galaxy follows the r 1/4 law exactly ! [> C$*0(#)"44%;$5P1"%4;*$/1%0/1/.*"4 In general, the brightness profile of spirals galaxies can be modelled as the sum of (i) an exponential disk for the outer regions I(R) = I0 exp(!R/Rd), where Rd is the disk scale-length. (ii) an r 1/4 law to the bulge Multi-wavelength view: Galaxies emit over the entire electromagnetic spectrum M31 RADIO CONTINUUM EMISSION AT 6 CM 21 CM LINE EMISSION (WSRT) [c Spitzer 24 micron Hot dust Galex UV image Radio cold dust hot dust Optical UV X-ray (center) Galaxies emit in many wavelengths Radio: • Smooth continuum emission following spiral arms: free-free emission due to warm gas • Compact emission regions identified as supernova remnants • Line emission: HI 21 cm, CO, molecular lines from cold gas Infrared: • Continuum emission from dust, heated by young stars in starforming regions Near Infrared: • Red super giants, modest extinction Optical-UV: • Visible stars, dust absorption • Emission lines from hot (10^4 K) gas • Stellar absorption lines •X-Ray: •( Double) stars, neutron stars • Very hot gas Luminosity functions (PS 3.7 intro, 3.7.1) Catalogs of galaxies most catalogs based on optical surveys, e.g.: Revised Shapley-Ames Catalog Sandage and Tammann: Third Reference Catalogue of Bright Galaxies de Vaucouleurs et al Sloan Digital Sky Survey 1 million galaxies + spectra (!) Very important were Palomar Sky Survey Plates, these have been used for systematic surveys UGC: northern galaxies ESO catalog: southern galaxies Selection effects in optical catalogs Consider galaxy with certain luminosity If galaxy too small: misclassified as star if galaxy too big: surface brightness is too low ! > not detected ! Luminosity Function The luminosity function is defined by " dM = number density of galaxies in magnitude range (M,M + dM) ∞ The total density of galaxies is then: ν = Φ(M)dM −∞ Equivalently, "(L)dL is the number density of galaxies in the range (L,L+dL) The distribution of luminosities is well approximated by a Schechter Function #: slope of LF at the faint end, L*: characteristic Luminosity above which the number density drops sharply, "* overall normalization of galaxy density Typical values: where H0 = h 100 km/s The number of galaxies with a luminosity larger than L is given by Total amount of light produced Hence, huge numbers of low luminosity galaxies expected, but finite luminosity. Most of the luminosity comes from galaxies with L=L䌫. A simple approximation is that the universe is filled with L䌫 galaxies with a density "䌫 In practice determining LF is non-trivial: - a large sample of galaxies is needed with well determined absolute luminosities corrected for bandpass, internal absorption and absorption by the Milky Way.
Load more

Recommended publications
  • Libro Resumen Sea2016v55 0.Pdf
    2 ...................................................................................................................................... 4 .................................................................................................. 4 ........................................................................................................... 4 PATROCINADORES .................................................................................................................... 5 RESUMEN PROGRAMA GENERAL ............................................................................................ 7 PLANO BIZKAIA ARETOA .......................................................................................................... 8 .......................................................................................... 9 CONFERENCIAS PLENARIAS ................................................................................................... 14 ............................................................................................. 19 ................................................................................................ 21 ............... 23 CIENCIAS PLANETARIAS ......................................................................................................... 25 - tarde ....................................................................................................... 25 - ............................................................................................ 28 - tarde ................................................................................................
    [Show full text]
  • Galactic Astronomy 1 File
    INTRODUCTION TO SPACE 16.11.2020 The Galaxy I: Magnitude systems Structure, rotation, spiral arms Evolution Galactic continuum Galactic centre Boris Dmitriev 23.11. The Galaxy II: stars, gas, dust 30.11. Extragalactic & cosmology 8.12. Exam BASICS OF ASTRONOMY? • Observational Coordinate systems techniques • Feasibility • Source Emission spectrum mechanisms • Source properties • What kind of ELEC-E4530 Radio Astronomy Astronomy sources? ELEC-E4220 Space Instrumentation (galactic & extragalactic) • What kind of science? Why do we study astronomy on this course Needed on other space courses, and by anyone who wishes to continue in astronomical research. The astronomy part on this course consists of coordinate systems, emission mechanisms, and the basics of celestial objects, such as galactic and extragalactic sources. REMINDER: LUMINOSITY The luminosity emitted by a source (= the total radiated energy) L = 4r2 σT4 can be divided into two parts: L = 4r2F F = σT4 (Stefan-Boltzmann law) Luminosity is proportional to the size and the fourth power of the temperature High luminosity → the source is hot or large in size, or both Effective temperature = the temperature of a black body that would emit the same total amount of electromagnetic radiation BRIGHTNESS OF STARS? MAGNITUDE SYSTEMS Describe the optical brightness of celestial objects Logarithmic 2 Apparent magnitude: m = –2.5 lg F/F0 [F]=W/m m1 – m2 = –2.5 lg F1/F2 Bolometric magnitude at all wavelengths: mbol=mv- BC Visual magnitude mv corresponds to the sensitivity of the eye Absolute magnitude M (= the apparent m at a distance of 10pc): m – M = 5 lg (r/10pc) Absolute bolometric magnitude: Mbol – Mbol, = –2.5 lg L/L BC = Bolometric correction, zero for sun-like emission.
    [Show full text]
  • Annual Report ESO Staff Papers 2018
    ESO Staff Publications (2018) Peer-reviewed publications by ESO scientists The ESO Library maintains the ESO Telescope Bibliography (telbib) and is responsible for providing paper-based statistics. Publications in refereed journals based on ESO data (2018) can be retrieved through telbib: ESO data papers 2018. Access to the database for the years 1996 to present as well as an overview of publication statistics are available via http://telbib.eso.org and from the "Basic ESO Publication Statistics" document. Papers that use data from non-ESO telescopes or observations obtained with hosted telescopes are not included. The list below includes papers that are (co-)authored by ESO authors, with or without use of ESO data. It is ordered alphabetically by first ESO-affiliated author. Gravity Collaboration, Abuter, R., Amorim, A., Bauböck, M., Shajib, A.J., Treu, T. & Agnello, A., 2018, Improving time- Berger, J.P., Bonnet, H., Brandner, W., Clénet, Y., delay cosmography with spatially resolved kinematics, Coudé Du Foresto, V., de Zeeuw, P.T., et al. , 2018, MNRAS, 473, 210 [ADS] Detection of orbital motions near the last stable circular Treu, T., Agnello, A., Baumer, M.A., Birrer, S., Buckley-Geer, orbit of the massive black hole SgrA*, A&A, 618, L10 E.J., Courbin, F., Kim, Y.J., Lin, H., Marshall, P.J., Nord, [ADS] B., et al. , 2018, The STRong lensing Insights into the Gravity Collaboration, Abuter, R., Amorim, A., Anugu, N., Dark Energy Survey (STRIDES) 2016 follow-up Bauböck, M., Benisty, M., Berger, J.P., Blind, N., campaign - I. Overview and classification of candidates Bonnet, H., Brandner, W., et al.
    [Show full text]
  • Astr 323/423 Hw #1
    ASTR 323/423 HW #1 Note: running python/astropy, most of the datafiles can be easily loaded by saying: from astropy.io import ascii # load the file data=ascii.read('http://burro.case.edu/Academics/Astr323/HW/HW1/<filename>') # look at data column names print(data.colnames) # plot data plt.scatter(data['<some_column>'],data['<some_other_column>' 1. Galaxy classification (courtesy Heather Morrison) Sandage's "The Hubble Atlas of Galaxies" (on reserve in the library, or available online, although the online version is hard to read) gives a detailed description of the traditional Hubble classification. Read pages 7-26 of the Hubble Atlas to familiarize yourself with the classification scheme. Then go to the Sloan Digital Sky Survey and look at galaxy images using the Navigator function to classify the galaxies in the table below. In each case, write a short paragraph explaining why you chose this classification. You should include comparison galaxies in the Hubble atlas which you used to classify each galaxy. Note any difficulties you had applying Sandage's rules. It may be helpful for you to type the NGC numbers of some of the Hubble Atlas galaxies into Navigator so you can see, for example, what HII regions look like in color images, etc. # RA Dec 1 221.546 –0.223 2 145.514 +0.336 3 39.849 +1.094 4 36.907 –1.155 5 152.110 +12.300 6 161.957 +12.582 7 Another galaxy of your choice near one of these galaxies. Give RA and Dec and include a color image 2. Adopt-A-Galaxy (courtesy Matt Bershady, UWisc) You have been assigned a galaxy to adopt (see table below).
    [Show full text]
  • Astro-Ph/0211002V1 1 Nov 2002 Aayi Nipratpoet Htms Eex- Be Must That Property Important an Is Galaxy Introduction 1
    The Ringed Spiral Galaxy NGC 4622. I. Photometry, Kinematics, and the Case for Two Strong Leading Outer Spiral Arms1 Ronald J. Buta2 and Gene G. Byrd Department of Physics & Astronomy Department, University of Alabama, Tuscaloosa, AL 35487, USA and Tarsh Freeman Bevill State Community College, Fayette, AL, USA ABSTRACT The intriguing nearly face-on southern ringed spiral galaxy NGC 4622, the first galaxy defini- tively shown to have leading spiral structure, is revisited in this paper with new images from the Hubble Space Telescope’s WFPC2, together with ground-based optical and near-IR imaging, and a Fabry-Perot Hα velocity field. The data provide new information on the disk/bulge/halo mix, rotation curve, star formation in the galaxy, and the sense of winding of its prominent spiral arms. Previously, we suggested that the weaker, inner single arm most likely has the leading sense, based on a numerical simulation. Now, taking advantage of HST resolution and using de Vaucouleurs’ standard extinction and reddening technique to determine the near side of the galaxy’s slightly tilted disk, we come to the more surprising conclusion that the two strong outer arms have the leading sense. We suggest that this highly unusual configuration may be the result of a past minor merger or mild tidal encounter. Possible evidence for a minor merger is found in a short, central dust lane, although this is purely circumstantial and an unrelated interaction with a different companion could also be relevant. The leading arms may be allowed to persist because NGC 4622 is dark halo-dominated (i.e., not “maximum disk” in the inner regions) and displays a significantly rising rotation curve.
    [Show full text]
  • Hubble Heritage
    VOL 18 ISSUE 03 Space Telescope Science Institute HubbleHubble Heritage:Heritage: Scowen and Brian Moore (ASU) NASA, (SCSU), Paul Donald Walter FromFrom InspirationInspiration toto RealizationRealization Keith Noll, [email protected] hances are you’ve seen some of our images. They are popping up support. More than a year of planning and team-building later, Hubble everywhere in textbooks, magazines, and online. Perhaps you’ve Heritage unveiled its first four images on October 21, 1998. In the first month used them in a lecture or maybe pinned one on your bulletin board. thereafter, our new web site recorded 14 million hits from people coming to You may be one of the 200,000 people who view our web site each view our images of the “Fried Egg” Seyfert Galaxy NGC 7742, a colorful field C of stars in Sagittarius near the center of the Milky Way, the wisps of the month or the millions more who see our monthly images in other venues. You may have even noticed an image credit to NASA/Hubble Heritage and Bubble Nebula, and Saturn’s classic rings. (http://heritage.stsci.edu) wondered briefly what that signified. Early on in our project, we settled on the pace of producing one new image Hubble Heritage is many things. It is an idea—an idea born in a holiday each month. We have attempted to include as broad and representative a conversation with relatives who wanted to know if I had worked on “that selection of astronomical objects as possible. We use both public, archival picture from Hubble”—Jeff Hester’s image of the Eagle Nebula, M16.
    [Show full text]
  • The Chemically Distinct Nucleus and Structure of the S0 Galaxy NGC 80 O
    Astronomy Reports, Vol. 47, No. 2, 2003, pp. 88–98. Translated from Astronomicheski˘ı Zhurnal, Vol. 80, No. 2, 2003, pp. 107–117. Original Russian Text Copyright c 2003 by Sil’chenko, Koposov, Vlasyuk, Spiridonova. The Chemically Distinct Nucleus and Structure of the S0 Galaxy NGC 80 O. K. Sil’chenko1,S. E. Koposov 1,V. V. Vlasyuk 2,andO.I.Spiridonova2 1Sternberg Astronomical Institute, Universitetski ˘ı pr. 13, Moscow, 119992 Russia 2Special Astrophysical Observatory, Russian Academy of Sciences, pos. Nizhni˘ı Arkhyz, Karacha ˘ı -Cherkessia, Russia Received April 3, 2002; in final form, May 23, 2002 Abstract—The giant lenticular galaxy NGC 80, which is the brightest member of a rich group, possesses a central evolutionarily-distinct region: the stars in the nucleus and in a circumnuclear ring of radius 5t–7 have a mean age of only 7 Gyr, whereas the stellar population of the bulge is older than 10 Gyr. The nucleus of NGC 80 is also chemically distinct: it is a factor of 2–2.5 richer in metals than its immediate neighborhood and is characterized by a high magnesium-to-iron abundance ratio [Mg/Fe] ≈ +0.3.The global stellar disk of NGC 80 has a two-tiered structure: its outer part has an exponential scale length of 11 kpc and normal surface density, while the inner disk, which is also exponential and axisymmetric, is more compact and brighter. Although the two-tiered structure and the chemically distinct nucleus obviously have a common origin and owe their existence to some catastrophic restructuring of the protogalactic gaseous disk, the origin of this remains unclear, since the galaxy lacks any manifestations of perturbed morphology or triaxiality.
    [Show full text]
  • Atlante Grafico Delle Galassie
    ASTRONOMIA Il mondo delle galassie, da Kant a skylive.it. LA RIVISTA DELL’UNIONE ASTROFILI ITALIANI Questo è un numero speciale. Viene qui presentato, in edizione ampliata, quan- [email protected] to fu pubblicato per opera degli Autori nove anni fa, ma in modo frammentario n. 1 gennaio - febbraio 2007 e comunque oggigiorno di assai difficile reperimento. Praticamente tutte le galassie fino alla 13ª magnitudine trovano posto in questo atlante di più di Proprietà ed editore Unione Astrofili Italiani 1400 oggetti. La lettura dell’Atlante delle Galassie deve essere fatto nella sua Direttore responsabile prospettiva storica. Nella lunga introduzione del Prof. Vincenzo Croce il testo Franco Foresta Martin Comitato di redazione e le fotografie rimandano a 200 anni di studio e di osservazione del mondo Consiglio Direttivo UAI delle galassie. In queste pagine si ripercorre il lungo e paziente cammino ini- Coordinatore Editoriale ziato con i modelli di Herschel fino ad arrivare a quelli di Shapley della Via Giorgio Bianciardi Lattea, con l’apertura al mondo multiforme delle altre galassie, iconografate Impaginazione e stampa dai disegni di Lassell fino ad arrivare alle fotografie ottenute dai colossi della Impaginazione Grafica SMAA srl - Stampa Tipolitografia Editoria DBS s.n.c., 32030 metà del ‘900, Mount Wilson e Palomar. Vecchie fotografie in bianco e nero Rasai di Seren del Grappa (BL) che permettono al lettore di ripercorrere l’alba della conoscenza di questo Servizio arretrati primo abbozzo di un Universo sempre più sconfinato e composito. Al mondo Una copia Euro 5.00 professionale si associò quanto prima il mondo amatoriale. Chi non è troppo Almanacco Euro 8.00 giovane ricorderà le immagini ottenute dal cielo sopra Bologna da Sassi, Vac- Versare l’importo come spiegato qui sotto specificando la causale.
    [Show full text]
  • Super-Massive Black Hole Scaling Relations and Peculiar Ringed Galaxies
    SUPER-MASSIVE BLACK HOLE SCALING RELATIONS AND PECULIAR RINGED GALAXIES A DISSERTATION SUBMITTED TO THE FACULTY OF THE GRADUATE SCHOOL OF THE UNIVERSITY OF MINNESOTA BY BURCIN MUTLU IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY MARC S. SEIGAR June, 2017 c BURCIN MUTLU 2017 ALL RIGHTS RESERVED Acknowledgements There are several people who I would like to acknowledge for directly or indirectly contributing to this dissertation. First and foremost, I would like to acknowledge the guidance and support of my ad- visor, Marc S. Seigar. I am thankful to him for his continuous encouragement, patience, and kindness. I appreciate all his contributions of knowledge, expertise, and time, which were invaluable to my success in graduate school. He has set an example of excellence as a researcher, mentor, and role model. In addition, I would like to thank my dissertation committee, Liliya L. R. Williams, M. Claudia Scarlata, and Robert Lysak, for their insightful input, constructive criticism and direction during the course of this dissertation. I have crossed paths with many collaborators who have influenced and enhanced my research. Patrick Treuthardt has been a collaborator for most of the work during my dissertation. The addition of his scientific point of view has improved the quality of the work in this dissertation tremendously. Our discussions have always been stimulating and rewarding. I am thankful to him for mentoring me and being a dear friend to me. I would also like to thank Benjamin L. Davis for numerous helpful advice and inspiring discussions. He has directly involved with many aspects of Chapter 1.
    [Show full text]
  • The NGC 7742 Star Cluster Luminosity Function: a Population Analysis
    Research in Astron. Astrophys. Vol.0 (201x) No.0, 000–000 Research in http://www.raa-journal.org http://www.iop.org/journals/raa Astronomy and (LATEX: n7742.tex; printed on December 4, 2017; 1:18) Astrophysics The NGC 7742 star cluster luminosity function: A population analysis revisited Richard de Grijs1,2,3 and Chao Ma1,2 1 Kavli Institute for Astronomy & Astrophysics, Peking University, Yi He Yuan Lu 5, Hai Dian District, Beijing 100871, China; [email protected] 2 Department of Astronomy, Peking University, Yi He Yuan Lu 5, Hai Dian District, Beijing 100871, China 3 International Space Science Institute–Beijing, 1 Nanertiao, Zhongguancun, Hai Dian District, Beijing 100190, China Abstract We re-examine the properties of the star cluster population in the circumnuclear starburst ring in the face-on spiral galaxy NGC 7742, whose young cluster mass func- tion has been reported to exhibit significant deviations from the canonical power law. We base our reassessment on the clusters’ luminosities (an observational quantity) rather than their masses (a derived quantity), and confirm conclusively that the galaxy’s starburst-ring clusters—and particularly the youngest subsample, log(t yr−1) ≤ 7.2—show evidence of a turnover in the cluster luminosity function well above the 90% completeness limit adopted to ensure the reliability of our results. This confirmation emphasizes the unique conundrum posed by this unusual cluster population. Key words: globular clusters: general – galaxies: evolution – galaxies: individual (NGC 7742) – galaxies: star clusters: general – galaxies: star formation 1 RAPID STAR CLUSTER EVOLUTION Until recently, neither theoretical predictions nor prior observational evidence indicated that the power- law cluster luminosity functions (CLFs) and the equivalent cluster mass functions (CMFs) commonly found for very young star cluster systems could transform into the lognormal distributions characteristic of old globular clusters on timescales as short as a few ×107 yr.
    [Show full text]
  • I. Personal Information
    Curriculum Vitae Notarization. I have read the following and certify that this curriculum vitae is a current and accurate statement of my professional record. Signature_ Sylvain Veilleux____ Date___03/12/20___________________ • Please organize your CV using the headings and sub-headings in this template. • In general, do not list a work or activity more than once. • Certain sections with numerous sub-categories include a special sub-category for Historical data in which you can group, for convenience, all items from 10+ years ago. I. Personal Information I.A. UID, Last Name, First Name, Middle Name, Contact Information Include mailing address, email, URL • UID: 104987658 • Last name: Veilleux • First name: Sylvain • Mailing address: Department of Astronomy, Physical Science Complex, Stadium Drive, University of Maryland, College Park 20742 USA • Email: [email protected] • URL: http://www.astro.umd.edu/~veilleux I.B. Academic Appointments at UMD Include specific dates • 07/01/2005 – present Professor • 07/01/2003 – present Optical Director • 07/01/2000 – 06/30/2005 Associate Professor • 07/01/1995 – 06/30/2000 Assistant Professor I.C. Administrative Appointments at UMD Include specific dates I.D. Other Employment Include specific dates • 12/01/2019 – … Clare Hall Lifetime Membership, U. Cambridge, U.K. • 02/01/2009 – … Visiting Professor, MPE, Germany. • 01/01/2019 – 08/15/2019 Sackler Distinguished Visitor, Institute of Astronomy, U.K. • 01/01/2019 – 08/15/2019 Kavli Lecturer, Kavli Institute for Cosmology, Cambridge (KICC), U.K. • 01/01/2019 – 08/15/2019 Clare Hall Visiting Fellow, U. Cambridge, U.K. • 01/01/2015 – 06/30/2015 Guggenheim Fellow, U.
    [Show full text]
  • A Classical Morphological Analysis of Galaxies in the Spitzer Survey Of
    Accepted for publication in the Astrophysical Journal Supplement Series A Preprint typeset using LTEX style emulateapj v. 03/07/07 A CLASSICAL MORPHOLOGICAL ANALYSIS OF GALAXIES IN THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G) Ronald J. Buta1, Kartik Sheth2, E. Athanassoula3, A. Bosma3, Johan H. Knapen4,5, Eija Laurikainen6,7, Heikki Salo6, Debra Elmegreen8, Luis C. Ho9,10,11, Dennis Zaritsky12, Helene Courtois13,14, Joannah L. Hinz12, Juan-Carlos Munoz-Mateos˜ 2,15, Taehyun Kim2,15,16, Michael W. Regan17, Dimitri A. Gadotti15, Armando Gil de Paz18, Jarkko Laine6, Kar´ın Menendez-Delmestre´ 19, Sebastien´ Comeron´ 6,7, Santiago Erroz Ferrer4,5, Mark Seibert20, Trisha Mizusawa2,21, Benne Holwerda22, Barry F. Madore20 Accepted for publication in the Astrophysical Journal Supplement Series ABSTRACT The Spitzer Survey of Stellar Structure in Galaxies (S4G) is the largest available database of deep, homogeneous middle-infrared (mid-IR) images of galaxies of all types. The survey, which includes 2352 nearby galaxies, reveals galaxy morphology only minimally affected by interstellar extinction. This paper presents an atlas and classifications of S4G galaxies in the Comprehensive de Vaucouleurs revised Hubble-Sandage (CVRHS) system. The CVRHS system follows the precepts of classical de Vaucouleurs (1959) morphology, modified to include recognition of other features such as inner, outer, and nuclear lenses, nuclear rings, bars, and disks, spheroidal galaxies, X patterns and box/peanut structures, OLR subclass outer rings and pseudorings, bar ansae and barlenses, parallel sequence late-types, thick disks, and embedded disks in 3D early-type systems. We show that our CVRHS classifications are internally consistent, and that nearly half of the S4G sample consists of extreme late-type systems (mostly bulgeless, pure disk galaxies) in the range Scd-Im.
    [Show full text]