Sterrenstelsels en Cosmologie. Dates of the courses. on Monday, 11:15-13:00 Jan 26 - June 1, room 414, (exceptions April 8 and June 1)

Size: px

Start display at page:

Download "Sterrenstelsels en Cosmologie. Dates of the courses. on Monday, 11:15-13:00 Jan 26 - June 1, room 414, (exceptions April 8 and June 1)"

Gregory Montgomery
5 years ago
Views:

1 see franx/college/ mf-sts-2015-c see franx/college/ mf-sts-2015-c01-2 Sterrenstelsels en Cosmologie Docent: M. Franx, kamer 425 College assistenten: Margot Brouwer, kamer 541, Marijke Segers, kamer 436 Dates of the courses on Monday, 11:15-13:00 Jan 26 - June 1, room 414, (exceptions April 8 and June 1) Two books are relevant for this course. None are obligatory: Binney and Tremaine: Galactic Dynamics (B&T) (2nd edition) (69 euro bol.com) Introduction into theory of galaxy dynamics, i.e. potential theory, orbits, distribution functions, equilibria, disks, mergers, etc. QUESTION HOURS: generally 13:45, Thursday BEFORE next course (except May 13). room 207 (except May 6, 14 room 106) Extragalactic Astronomy and Cosmology Peter Schneider, edition 2 76 euro bij bol These books are not obligatory. Their level is very high (advanced Master course), but this means they remain useful throughout your career. 1 other book is also sometimes used: Binney and Merrifield: Galactic Astronomy (indicated with BM ) Het cijfer voor het college wordt voor 66% bepaald door het tentamen, en voor 33% door de ingeleverde huiswerk opgaven. Een minimum cijfer van een 6 voor de huiswerk opgaves is nodig om deel te kunnen De huiswerk opgaven moeten voor het begin van het volgende college worden g d naar: skassistenten@strw.leidenuniv.nl (scannen kan bij de kopieerapparaten). Te laat inleveren betekent het cijfer 0. De vragen uurtjes geven specifiek de mogelijkheid om hulp te krijgen bij het maken van het huiswerk.

2 see franx/college/ mf-sts-2015-c see franx/college/ mf-sts-2015-c01-4 Brief content of the course 1) Introduction What is a galaxy? Classifications Photometry, exponentials, r1/4 profiles, luminosity function 2) Keeping a galaxy together: Gravity Potentials 3) Galactic Dynamics Equilibrium collisions, Virial Theorem Universe expansion 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) Observing galaxy formation High redshift galaxies from HST Fair samples of galaxies at high redshift 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 neighborhood, Oort limit Elliptical galaxies and hot gas Clusters of galaxies, the universe Candidate dark matter particles 8) Galaxy formation

3 see franx/college/ mf-sts-2015-c see franx/college/ mf-sts-2015-c General Introduction Content Handout 1: i) What is a galaxy? Optical Radio X-Ray Dark Matter (halo) ii) Why do we study galaxies? iii) Optical Photometry iv) Surveys and Selection Effects v) Luminosity Function Study material from B&M: 4.1, (4.1.2), to page 165, (4.1.4) 4.2, (4.2.2), not , to page , (not 4.4.2), to page , to page 244 (4.6.2) subsection in brackets means for reading only i) What is a galaxy? Galaxies emit in many wavelengths [See the multiwavelength color show franx/ college/sterrenstelsels15/galaxies.pdf ] Radio: Continuum emission follows spiral arms Compact emission regions - supernova remnants Active nuclei produce jets, radio lobes... Line emission: HI 21 cm, CO, molecular lines Infrared: Continuum emission by dust Star forming regions, active nuclei Near Infrared: Red super giants, some extinction Optical-UV: Visible stars, dust absorbtion Emission lines Blue active nuclei X-Ray: (Double) stars, neutron stars, star forming regions Very hot gas active nuclei

4 see franx/college/ mf-sts-2015-c see franx/college/ mf-sts-2015-c01-8 Active Nuclei produce emission at all wavelengths at all lengthscales: from very close to the nucleus ( pc) to the largest scale (> 10 kpc) Conclusion a Galaxy consists of several components: stars: -bulge red, old (?) r 1/4 law -disk blue or red spiral arms, rings, bars exponential profile gas: -disk -extended H I gas H 2 gas dust Hot Gas active nucleus: center black hole Dark Halo: large, dominant unknown particles

5 see franx/college/ mf-sts-2015-c see franx/college/ mf-sts-2015-c01-10 Why study galaxies? What are the main questions? What is the structure of galaxies? What is their equilibrium? What are they made off? What is their mass distribution? How do they evolve in time? How have they formed? Homework Questions: 1) Why is the name sterrenstelsel bad? In what component is most of the mass? 2) What telescope would you use to measure the emission of Andromeda at a frequency of (i) hz, (ii) hz, (iii) hz. First calculate the wavelengths of this emission. 3) Give an estimate from literature of the total mass of the Milky Way, and the total stellar mass. Give the relevant source (i.e., mention where you got these estimates from)

23-1-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c01-11 23-1-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c01-12 Optical images of galaxies and classification See the pdf file on the web for nice pictures http://www.

6 see franx/college/ mf-sts-2015-c see franx/college/ mf-sts-2015-c01-12 Optical images of galaxies and classification See the pdf file on the web for nice pictures franx/ college/sterrenstelsels15/galaxies.pdf All classification systems are idealizations. Independent of true size of the galaxy and Luminosity! Often used systems: 1. Hubble-Sandage 2. de Vaucouleurs or Numerical types T (based on de Vaucouleurs) were often used Disadvantages of ALL classifications Only based on optical image > independent of true size! Galaxies vary in more than one dimension Many galaxies are peculiar, i.e. inclassifiable We first highlight the classifications from the RSA (Revised Shapley Ames Catalogue, Sandage)

23-1-2015see http://www.strw.leidenuniv.

7 see franx/college/ mf-sts-2015-c see franx/college/ mf-sts-2015-c01-14 Normal Spirals are classified from Sa to Sd. Along this sequence the following properties change: 1) degree of central concentration (or Bulge-to-disk ratio). (decreasing from Sa to Sd) 2) angle of the spiral arm (increasing from Sa to Sd) 3 degree of resolution of spiral arms into individual clumps (from smooth to clumpy from Sa to Sd).

23-1-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c01-15 23-1-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c01-16 Bars occur at all types.

8 see franx/college/ mf-sts-2015-c see franx/college/ mf-sts-2015-c01-16 Bars occur at all types. Their strength can be used as another dimension in the classification. These galaxies have rings

9 see franx/college/ mf-sts-2015-c see franx/college/ mf-sts-2015-c01-18 De Vaucouleurs introduced a classification scheme which was slightly different, classifying into ring and s-shaped, and bars. He also introduced a numerical type t running from -5 to 10. These are peculiar galaxies (Arp et al, 1987). These galaxies are generally mergers (collisions between galaxies).

10 see franx/college/ mf-sts-2015-c see franx/college/ mf-sts-2015-c01-20 van den Bergh introduced yet another scheme: Currently, these classifications have become less important. We now have distances to most galaxies, and multi-wavelength information. We characterize galaxies by their stellar mass, age, star formation rate, metallicity, and halo mass (or environment). Homework Questions: 4) Why are galaxy classifications problematic? 5) Describe in your own words 3 criteria which are used to classify spirals into Sa, Sb to Sd. 6) What is the type of the Milky Way? Motivate your answer 7) Why don t we classify the Magellanic Clouds as ellipticals? They don t have spiral arms. 8) What is the type of the galaxy on the cover of BM? Give the reasons for your classification 9) How do you recognize mergers?

11 see franx/college/ mf-sts-2015-c see franx/college/ mf-sts-2015-c01-22 Quantitative photometry of galaxies In the past: photographic plates: Limited dynamic range Now: CCDs (= very sensitive TV camera s) Sizes 2048x2048 pixels Quantum efficiency 90 % Very good dynamic range Photometry > Imaging galaxies and measuring their brightness distribution As can be seen, the galaxy does not really stop! How to measure average surface brightness profile? Measure the intensity on ellipses of (nearly) constant surface brightness In practice, our images stop when there might still be very faint galaxy light. This would not be a problem, but we also have the much brighter light from the night sky. We have to estimate this, and we make systematic errors in the profiles if we estimate it too low or too high Big technical problem: galaxies are really large, and have low surface brightness wings. See the beautiful image of M31

12 see franx/college/ mf-sts-2015-c see franx/college/ mf-sts-2015-c01-24 Resulting profiles: Ellipticals: King profile de Vaucouleurs law (r 1/4 ) Spirals: Disks: exponential profile Bulges: r 1/4 For elliptical galaxies we often find the r 1/4 law: I(R) = I e exp( 7.67[(R/R e ) 1/4 1]) where R e is the half light radius: half the light is emitted inside R e. Because of uncertainties in the background subtraction, we never know the exact half light radius. The parameter I e is the surface brightness at R = R e. No galaxy follows the r 1/4 law exactly! On the next page, some examples are shown. The profiles can change systematically from bright galaxies to faint elliptical galaxies.

23-1-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c01-25 23-1-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c01-26 An exponential disk has I(R) = I 0 exp( R/R d ) where R d is the disk scalelength.

13 see franx/college/ mf-sts-2015-c see franx/college/ mf-sts-2015-c01-26 An exponential disk has I(R) = I 0 exp( R/R d ) where R d is the disk scalelength. You can see that the outer parts of the galaxies shown above show a straight profile - hence have an exponential profile. The inside shows an upturn, and that is modeled as a separate component. This is the bulge. Many galaxies are modelled well by fitting an r 1/4 law to the bulge and an exponential model to the disk.

14 see franx/college/ mf-sts-2015-c01-27 Surveys and Catalogs of galaxies most catalogs based on optical surveys Currently used: Sloan Digital Sky Survey: Data Release 7 covers sq degrees > 300 million objects (galaxies, stars,...) spectra over 9380 sq degrees: 1.6 million spectra of galaxies, quasars, stars! Many optical surveys over smaller areas (GAMA, BOSS, ) see franx/college/ mf-sts-2015-c01-28 Selection effects in optical catalogs Consider galaxy with certain luminosity If galaxy too small: misclassified as star if galaxy too big: surface brightess is too low > not detected! Near-IR: 2MASS (imaging, all sky) Mid-IR: Wise (all sky) X-Ray: ROSAT All-Sky Survey OLDER Revised Shapley-Ames Catalog Sandage and Tammann Third Reference Catalogue of Bright Galaxies de Vaucouleurs et al e.g.: Very important were Palomar Sky Survey Plates, these have been used for systematische surveys UGC: northern galaxies ESO catalog: southern galaxies Lauberts, Lauberts en Valentijn

15 see franx/college/ mf-sts-2015-c see franx/college/ mf-sts-2015-c01-30 Luminosity Function Φ(L) = (Φ 0/L )(L/L ) α exp( L/L ) Typical values: Φ = (1.6±0.3) 10 2 h 3 Mpc 3 M B = 19.7±0.1+5logh α = 1.07±0.07 L B = (1.2±0.1) h L Sun where H 0 = h100km/s The number of galaxies with a luminosity larger than L is given by N(> L) = L Φ(L )dl = N 0 Γ(1+α,L/L ) Here we used the following definition for the incomplete gamma function Γ(α,x) = x t(α 1) e t dt Total amount of light produced SDSS Luminosity function from Blanton 2005 Determine for each galaxy the intrinsic luminosity from apparent luminosity and distance. Correct for bandpass, internal absorbtion and absorbtion by the Milky Way. The luminosity function is defined by ΦdM = number density of galaxies in magnitude range (M,M + dm) l tot = 0 Φ(L )L dl = Φ L Γ(2+α) = Φ L for α = 1 Hence, huge numbers of low luminosity galaxies expected, but finite luminosity. Most of the luminosity comes from galaxies with L = L. A simple approximation is that the universe is filled with L galaxies with a density Φ The distribution of luminosities is given by a Schechter function

16 see franx/college/ mf-sts-2015-c see franx/college/ mf-sts-2015-c01-32 Homework questions 10) Given a galaxy with an exponential profile I(R) = I 0 exp( R/R d ) a) what is the total emount of light emitted? (Express in terms of I 0 and R d.) (Hint: integrate the light emitted as a function of radius, where radius runs from 0 to infinity) b) what is the half light radius? (i.e., the radius in which half the light is emitted) (Hint: use the integral from 10a, now to Re instead of infinity) 16) Find the website of a catalogue with more than galaxies (and NOT the Sloan Digital Sky Survey or GAMA ). Give the full reference. 11) How can we attempt to classify galaxies automatically (i.e., by computer)? 12) What is the luminosity function? 13) Given a Schechter Luminosity function, what is the luminosity at which half of the total luminosity density is emitted by galaxies brighter than that luminosity? Assume α = 1. 14) What is the luminosity of a typical galaxy in terms of solar luminosities? Motivate your answer, and give a full reference if you take a value from a source. 15) The Schechter function implies that the total number of galaxies per volume element is infinite if the Schechter luminosity function extends to luminosity 0. Derive that this is the case for a simple Schechter luminosity function with α = 1. How can it be that the total amount of light is finite, despite the fact that the number of galaxies is infinite? (per volume element?)

Dates of the courses. Sterrenstelsels en Cosmologie. Docent: M. Franx, kamer 425. Usually on Monday, 11:15-13:00, but also on Thursdays 13:45-15:30

Dates of the courses. Sterrenstelsels en Cosmologie. Docent: M. Franx, kamer 425. Usually on Monday, 11:15-13:00, but also on Thursdays 13:45-15:30 1-2-2013see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2013-c01-1 1-2-2013see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2013-c01-2 Sterrenstelsels en Cosmologie Docent: M. Franx, kamer