Lecture 12. November 20, 2018 Lab 6
|
|
|
- Ann Palmer
- 5 years ago
- Views:
Transcription
1 Lecture 12 November 20, 2018 Lab 6
2 News Lab 4 Handed back next week (I hope). Lab 6 (Color-Magnitude Diagram) Observing completed; you have been assigned data if you were not able to observe. Due: instrumental color-magnitude diagram: it to me by tomorrow (or whenever you finish it). Whole lab due November 29.
3 Lab 6: Color-Magnitude Diagram Target is the open cluster M34. CMD can determine the cluster distance and age. Will again perform differential photometry by using stars in the field with known standard magnitudes. So the observations can be taken through thin scattered clouds. Will observe in both the B and V filter to get stellar colors, B V. Color measures stellar surface temperature.
4 M34 V 300 sec One field approximately centered on M34.
5 M34a V 300 sec A field with the center offset.
6 M34 1,068 stars
7 Location of the offset field. N E OGS 20-inch RC + SBIG STL-11000M + ST-237
8 907 stars; some are outside plot bounds
9 Offset Field
10 Offset Field Still a few M34 stars? Background red giants or foreground dim red mainsequence stars. Background stars in the Galactic disk (mostly).
11 M34 CMD WIYN 0.9m telescope Green proper motion member Red radial velocity member Blue photometric member Meibom et al. 2011, ApJ, 733, 115
12 Gaia satellite data release 2 photometry. All stars within 0.5 degrees of the cluster center with parallax uncertainty < 10%.
13 Gaia satellite data release proper motions. All stars within 0.5 degrees of the cluster center with parallax uncertainty < 10%.
14 Gaia satellite data release proper motions. All stars within 0.5 degrees of the cluster center with parallax uncertainty < 10%.
15 Gaia data release 2 photometry. All stars within 0.5 degrees of the cluster center with parallax uncertainty < 10%. Blue points are proper motion members.
16 Gaia data release 2 photometry. Use proper motions to change g magnitude to absolute g magnitude. Blue points are proper motion members.
17 Transformation to Standard Magnitudes The simplest transformation would be a simple additive correction, like that for atmospheric extinction, to account for the efficiency of the telescope and detector. However, the passbands defined by our filters and the spectral response of the CCD do not exactly match that of the standard system (which was defined by a 1P21 photomultiplier tube that is no longer made). As the following figures illustrate, the shift in the passband causes the correction to depend on the temperature of the star.
18 The quantum efficiency of the CCD is varying significantly across the V and B bands.
19
20 The effect of a shifted passband will be different for hot and cool stars.
21 Transformation to Standard Magnitudes Thus, the standard transformation equations are: B V = ϕ bv + µ bv (b v) V v = ϕ v + ε (B V) Here, B and V are the standard magnitudes and b and v are the instrumental magnitudes. These can be considered first-order Taylor expansions. We will ignore higher order terms (they are usually unimportant). The µ bv coefficient would be 1.0 and ε would be 0 if our system matched the standard one. Actually differ from these values by
22 Fitting the Transformations B V equation: Calculate a column of Δ B-V = (B V) (ϕ bv + µ bv (b v)) Make another column of (Δ B V ) 2 and sum to form χ 2 = Σ i (Δ B V,i ) 2. Minimize χ 2 by varying ϕ bv and µ bv using solver in excel. V equation: Calculate a column of Δ V = V (v + ϕ v + ε (B V)) Proceed as above to determine ϕ v and ε.
23
24 The smaller range of b-v compared to B-V may arise because the CCD quantum efficiency weights our B band towards long λ s and our V band towards short λ s, thus reducing our wavelength baseline (hence, sensitivity to T). Transformations 2.40 V transformation 1.6 B-V transformation data fit data fit B V b v
25 Interstellar Extinction & Reddening Caused by scattering from dust grains in the interstellar medium. About 1 magnitude of dimming per kiloparsec of distance in the plane of the Galaxy. A major headache. Scattering cross-section is larger at shorter wavelengths (Rayleigh scattering), so light is reddened. also
26 Interstellar Extinction & Reddening Dust grains properties uniform, so there is a (nearly) universal relation between reddening and extinction. Reddening: E(B V) = (B V) (B V) 0 Extinction: A V = V V 0 = 3.1 E(B V) Reddening is not easy to determine. Measure spectral type of stars and use relation between color and type for very nearby stars. For Lab 6 you are given E(B-V) and use it to correct your photometry to V 0 and (B V) 0.
27 Cluster Distance Slide a theoretical zero-age main sequence isochrone vertically until it matches the cluster main sequence. m M = 5 log(d/10 pc) + A V m = M V + 5 log(d/10pc) + A V M V = isochrone absolute magnitudes m = shifted isochrone apparent magnitudes d = cluster distance A V = extinction due to interstellar dus. M_V Isochrones B - V Log Age (yr) = 3.00 Log Age (yr) = 5.00 Log Age (yr) = 6.00 Log Age (yr) = 6.50 Log Age (yr) = 7.00 Log Age (yr) = 7.25 Log Age (yr) = 7.50 Log Age (yr) =7.75 Log Age (yr) = 8.00 Log Age (yr) = 8.25 Log Age (yr) = 8.50 Log Age (yr) = 8.75 Log Age (yr) = 9.00
28 Blue: log(age/yrs) < 7 Green: 7 log(age/yrs) < 8 Black: 8 log(age/yrs) Pre-main-sequence stars
29 Increasing the m M adopted for the isochrone in steps of 0.1. $M34$$(m'M)=8.2$ 6" 7" 8" 9" 10" V_0$ 11" M34" log"age"(yr)"="3.00" 12" 13" 14" 15" 16",0.3",0.1" 0.1" 0.3" 0.5" 0.7" (B'V)_0$ 0.9" 1.1" 1.3" 1.5" 1.7"
30 Increasing the m M adopted for the isochrone in steps of 0.1. $M34$$(m'M)=8.3$ 6" 7" 8" 9" 10" V_0$ 11" M34" log"age"(yr)"="3.00" 12" 13" 14" 15" 16",0.3",0.1" 0.1" 0.3" 0.5" 0.7" (B'V)_0$ 0.9" 1.1" 1.3" 1.5" 1.7"
31 Increasing the m M adopted for the isochrone in steps of 0.1. $M34$$(m'M)=8.4$ 6" 7" 8" 9" 10" V_0$ 11" M34" log"age"(yr)"="3.00" 12" 13" 14" 15" 16",0.3",0.1" 0.1" 0.3" 0.5" 0.7" (B'V)_0$ 0.9" 1.1" 1.3" 1.5" 1.7"
32 Cluster Age Match the main-sequence turnoff. Isochrones M_V B - V 1.50 Log Age (yr) = 3.00 Log Age (yr) = 5.00 Log Age (yr) = 6.00 Log Age (yr) = 6.50 Log Age (yr) = 7.00 Log Age (yr) = 7.25 Log Age (yr) = 7.50 Log Age (yr) =7.75 Log Age (yr) = 8.00 Log Age (yr) = 8.25 Log Age (yr) = 8.50 Log Age (yr) = 8.75 Log Age (yr) = 9.00
33 Isochrones with different $M34$$(m'M)=8.3$ ages and best (m M) 6" 7" 8" 9" 10" V_0$ 11" 12" 13" M34" log"age"(yr)"="3.00" log"age"(yr)"="7.75" log"age"(yr)"="8.00" log"age"(yr)"="8.25" log"age"(yr)"="8.50" log"age"(yr)"="8.75" 14" 15" 16",0.3",0.1" 0.1" 0.3" 0.5" 0.7" (B'V)_0$ 0.9" 1.1" 1.3" 1.5" 1.7"
How to Understand Stars Chapter 17 How do stars differ? Is the Sun typical? Location in space. Gaia. How parallax relates to distance
How to Understand Stars Chapter 7 How do stars differ? Is the Sun typical? Image of Orion illustrates: The huge number of stars Colors Interstellar gas Location in space Two dimensions are easy measure
Chapter 7: From theory to observations
Chapter 7: From theory to observations Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle, predict the evolution of the stellar bolometric luminosity, effective
The magnitude system. ASTR320 Wednesday January 30, 2019
The magnitude system ASTR320 Wednesday January 30, 2019 What we measure: apparent brightness How bright a star appears to be in the sky depends on: How bright it actually is Luminosity and its distance
From theory to observations
Stellar Objects: From theory to observations 1 From theory to observations Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle, give the prediction of the
Lecture Three: Stellar Populations. Stellar Properties: Stellar Populations = Stars in Galaxies. What defines luminous properties of galaxies
Lecture Three: ~2% of galaxy mass in stellar light Stellar Populations What defines luminous properties of galaxies face-on edge-on https://www.astro.rug.nl/~etolstoy/pog16/ 18 th April 2016 Sparke & Gallagher,
AstroBITS: Open Cluster Project
AstroBITS: Open Cluster Project I. Introduction The observational data that astronomers have gathered over many years indicate that all stars form in clusters. In a cloud of hydrogen gas, laced with helium
Hertzprung-Russel and colormagnitude. ASTR320 Wednesday January 31, 2018
Hertzprung-Russel and colormagnitude diagrams ASTR320 Wednesday January 31, 2018 H-R diagram vs. Color- Magnitude Diagram (CMD) H-R diagram: Plot of Luminosity vs. Temperature CMD: Plot of magnitude vs.
Lecture 16 The Measuring the Stars 3/26/2018
Lecture 16 The Measuring the Stars 3/26/2018 Test 2 Results D C B A Questions that I thought were unfair: 13, 18, 25, 76, 77, 80 Curved from 85 to 79 Measuring stars How far away are they? How bright are
Open Cluster Research Project
Open Cluster Research Project I. Introduction The observational data indicate that all stars form in clusters. In a cloud of hydrogen gas, laced with helium and a trace of other elements, something triggers
The Plato Input Catalog (PIC)
The Plato Input Catalog (PIC) Giampaolo Piotto and the WP130000 group Dipartimento di Fisica e Astronomia Universita di Padova Because of the huge size of PLATO field (~2124 sq deg) and the consequent
PART 3 Galaxies. Gas, Stars and stellar motion in the Milky Way
PART 3 Galaxies Gas, Stars and stellar motion in the Milky Way The Interstellar Medium The Sombrero Galaxy Space is far from empty! Clouds of cold gas Clouds of dust In a galaxy, gravity pulls the dust
From theory to observations
Stellar Objects: From theory to observations 1 From theory to observations Update date: December 13, 2010 Given the stellar mass and chemical composition of a ZAMS, the stellar modeling can, in principle,
THE GALAXY. Spitzer Space Telescope Images & Spectra: 3µm - 170µm
THE GALAXY Composite infrared colour image of Galactic Centre region taken at 1.25, 2.2 and 3.5 microns with COBE/DIRBE instrument (NASA/GSFC). GALAXY: A conglomeration of stars, gas + dust Topics: Star
ASTR2050 Spring Please turn in your homework now! In this class we will discuss the Interstellar Medium:
ASTR2050 Spring 2005 Lecture 10am 29 March 2005 Please turn in your homework now! In this class we will discuss the Interstellar Medium: Introduction: Dust and Gas Extinction and Reddening Physics of Dust
3 reasons it was hard to figure out that we are in a Galaxy
Prof. Jeff Kenney Class 10 October 3, 2016 3 reasons it was hard to figure out that we are in a Galaxy 1. it's big -- one needs sensitive telescopes to see (individual stars) across the Galaxy 2. we're
Interstellar Medium by Eye
Interstellar Medium by Eye Nebula Latin for cloud = cloud of interstellar gas & dust Wide angle: Milky Way Summer Triangle (right) α&β Centauri, Coal Sack Southern Cross (below) Dust-Found in the Plane
Remember from Stefan-Boltzmann that 4 2 4
Lecture 17 Review Most stars lie on the Main sequence of an H&R diagram including the Sun, Sirius, Procyon, Spica, and Proxima Centauri. This figure is a plot of logl versus logt. The main sequence is
The Milky Way Galaxy. sun. Examples of three Milky-Way like Galaxies
The Milky Way Galaxy sun This is what our Galaxy would look like if we were looking at it from another galaxy. Examples of three Milky-Way like Galaxies 1. Roughly 100,000 light years across 2. Roughly
The Milky Way. Overview: Number of Stars Mass Shape Size Age Sun s location. First ideas about MW structure. Wide-angle photo of the Milky Way
Figure 70.01 The Milky Way Wide-angle photo of the Milky Way Overview: Number of Stars Mass Shape Size Age Sun s location First ideas about MW structure Figure 70.03 Shapely (~1900): The system of globular
Relativity and Astrophysics Lecture 15 Terry Herter. RR Lyrae Variables Cepheids Variables Period-Luminosity Relation. A Stellar Properties 2
Stellar Properties Relativity and Astrophysics Lecture 15 Terry Herter Outline Spectroscopic Parallax Masses of Stars Periodic Variable Stars RR Lyrae Variables Cepheids Variables Period-Luminosity Relation
Substellar objects: Brown dwarfs and extrasolar planets
Substellar objects: Brown dwarfs and extrasolar planets Basic information Class web site: http://www.mpia-hd.mpg.de/homes/goldman/course/ Material: slides, bibliography, useful links Max-Planck-Institut
Interstellar Dust and Gas
Interstellar Dust and Gas In 1783 William Herschel began a survey of the heavens using an 18 ¾ inch reflector of his own construction. His goal was to discover new star clusters, nebulae, and double stars.
Stars, Galaxies & the Universe Lecture Outline
Stars, Galaxies & the Universe Lecture Outline A galaxy is a collection of 100 billion stars! Our Milky Way Galaxy (1)Components - HII regions, Dust Nebulae, Atomic Gas (2) Shape & Size (3) Rotation of
A New Analysis in the Field of the Open Cluster Collinder 223
Chin. J. Astron. Astrophys. Vol. 4 (2004), No. 1, 67 74 ( http: /www.chjaa.org or http: /chjaa.bao.ac.cn ) Chinese Journal of Astronomy and Astrophysics A New Analysis in the Field of the Open Cluster
Characterization of the exoplanet host stars. Exoplanets Properties of the host stars. Characterization of the exoplanet host stars
Characterization of the exoplanet host stars Exoplanets Properties of the host stars Properties of the host stars of exoplanets are derived from a combination of astrometric, photometric, and spectroscopic
Measurement of the stellar irradiance
Measurement of the stellar irradiance Definitions Specific Intensity : (monochromatic) per unit area normal to the direction of radiation per unit solid angle per unit wavelength unit (or frequency) per
Interstellar Dust and Gas
Interstellar Dust and Gas In 1783 William Herschel began a survey of the heavens using an 18 ¾ inch reflector of his own construction. His goal was to discover new star clusters, nebulae, and double stars.
Astronomy 142 Recitation #7
Astronomy 14 Recitation #7 1 March 01 Formulas to remember Reddening and extinction Magnitude reminder: U = mu, B= mb, = m (apparent magnitudes); B = mb m (color index). isual extinction toward a star:
Stellar Structure and Evolution
Stellar Structure and Evolution Birth Life Death Part I: Stellar Atmospheres Part I: Stellar Atmospheres Jan. 23: Intro and Overview of Observational Data (Chapters 3 and 5) Jan. 28: Basics of Stellar
The Milky Way Galaxy. Sun you are here. This is what our Galaxy would look like if we were looking at it from another galaxy.
The Milky Way Galaxy Sun you are here. This is what our Galaxy would look like if we were looking at it from another galaxy. Examples of three Milky-Way like Galaxies 1. Roughly 100,000 light years across
The Birth Of Stars. How do stars form from the interstellar medium Where does star formation take place How do we induce star formation
Goals: The Birth Of Stars How do stars form from the interstellar medium Where does star formation take place How do we induce star formation Interstellar Medium Gas and dust between stars is the interstellar
Stars: basic observations
Stars: basic observations Basic properties of stars we would like to know in order to compare theory against observations: Stellar mass M Stellar radius R Surface temperature - effective temperature T
Chapter 19 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. Our Galaxy Pearson Education, Inc.
Reading Quiz Clickers The Cosmic Perspective Seventh Edition Our Galaxy 19.1 The Milky Way Revealed What does our galaxy look like? How do stars orbit in our galaxy? Where are globular clusters located
6. Interstellar Medium. Emission nebulae are diffuse patches of emission surrounding hot O and
6-1 6. Interstellar Medium 6.1 Nebulae Emission nebulae are diffuse patches of emission surrounding hot O and early B-type stars. Gas is ionized and heated by radiation from the parent stars. In size,
The HII Regions of Sextans A
Publications of the Astronomical Society of the Pacific 6: 765-769, 1994 July The HII Regions of Sextans A Paul Hodge 1 Astronomy Department, University of Washington, Seattle, Washington 98195 Electronic
Observational Astronomy
Observational Astronomy Photometry...2 Magnitude system...2 Observing procedure...3 Relation magnitude-flux...4 Atmospheric extinction correction...6 Transforming to standard system...6 Photometric System...7
Techniques for measuring astronomical distances generally come in two variates, absolute and relative.
Chapter 6 Distances 6.1 Preliminaries Techniques for measuring astronomical distances generally come in two variates, absolute and relative. Absolute distance measurements involve objects possibly unique
Universe Now. 9. Interstellar matter and star clusters
Universe Now 9. Interstellar matter and star clusters About interstellar matter Interstellar space is not completely empty: gas (atoms + molecules) and small dust particles. Over 10% of the mass of the
Asterseismology and Gaia
Asterseismology and Gaia Asteroseismology can deliver accurate stellar radii and masses Huber et al 2017 compare results on distances from Gaia and asteroseismology for 2200 Kepler stars Asteroseismology
arxiv:astro-ph/ v1 26 Nov 2004
13 Color Photometry of Open Cluster M48 Zhen-Yu Wu, Xu Zhou, Jun Ma, Zhao-Ji Jiang, Jian-Sheng Chen National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, arxiv:astro-ph/0411711v1
The Stars. Background & History The Celestial Sphere: Fixed Stars and the Luminaries
The Stars Background & History The Celestial Sphere: Fixed Stars and the Luminaries The Appearance of Stars on the Sky Brightness and Brightness Variations Atmospheric Effects: Twinkling Variable Stars
Lecture 12: Distances to stars. Astronomy 111
Lecture 12: Distances to stars Astronomy 111 Why are distances important? Distances are necessary for estimating: Total energy released by an object (Luminosity) Masses of objects from orbital motions
Review of stellar evolution and color-magnitude diagrams
Review of stellar evolution and color-magnitude diagrams The evolution of stars can be used to study the properties of galaxies Very characteristic features pinpoint at the age (chemistry) of the stars
Chapter 10: Unresolved Stellar Populations
Chapter 10: Unresolved Stellar Populations We now consider the case when individual stars are not resolved. So we need to use photometric and spectroscopic observations of integrated magnitudes, colors
Chapter 8: Simple Stellar Populations
Chapter 8: Simple Stellar Populations Simple Stellar Population consists of stars born at the same time and having the same initial element composition. Stars of different masses follow different evolutionary
The Giant Branches of Open and Globular Clusters in the Infrared as Metallicity Indicators: A Comparison with Theory
Accepted for publicaton in The Astronomical Journal The Giant Branches of Open and Globular Clusters in the Infrared as Metallicity Indicators: A Comparison with Theory GlennP.Tiede,PaulMartini,&JayA.Frogel
arxiv:astro-ph/ v2 15 Jul 2004
Influence of interstellar and atmospheric extinction on light curves of eclipsing binaries A. Prša and T. Zwitter University of Ljubljana, Dept. of Physics, Jadranska 19, 1000 Ljubljana, Slovenia arxiv:astro-ph/0405314v2
arxiv:astro-ph/ v1 10 Oct 2005
Mon. Not. R. Astron. Soc. 000, 1?? (2005) Printed 5 February 2008 (MN LATEX style file v2.2) CCD photometry of distant open clusters NGC 2425, Haffner 10 and Czernik 29 arxiv:astro-ph/0510274v1 10 Oct
Chapter 10 The Interstellar Medium
Chapter 10 The Interstellar Medium Guidepost You have begun your study of the sun and other stars, but now it is time to study the thin gas and dust that drifts through space between the stars. This chapter
Multi-wavelength study of the Milky Way Galaxy
29 th ASI Meeting ASI Conference Series, 2011, Vol. 3, pp 79 83 Edited by Pushpa Khare & C. H. Ishwara-Chandra Multi-wavelength study of the Milky Way Galaxy Shashikiran Ganesh Physical Research Laboratory,
Measuring stellar distances.
Measuring stellar distances This method can be used to measure distances up to 100pc Some new technology allows measuring distances up to 200pc using this method p= 1/d Stellar Parallax.htm This method
Number of Stars: 100 billion (10 11 ) Mass : 5 x Solar masses. Size of Disk: 100,000 Light Years (30 kpc)
THE MILKY WAY GALAXY Type: Spiral galaxy composed of a highly flattened disk and a central elliptical bulge. The disk is about 100,000 light years (30kpc) in diameter. The term spiral arises from the external
Raven Eyes Elliptical Galaxies and Star Clusters. T. J. Davidge November 24, 2015
Raven Eyes Elliptical Galaxies and Star Clusters T. J. Davidge November 24, 2015 Why Maffei1 and the Glimpse Clusters? Targets were selected at low Galactic latitudes to maximize chances of finding a suitable
Introduction The Role of Astronomy p. 3 Astronomical Objects of Research p. 4 The Scale of the Universe p. 7 Spherical Astronomy Spherical
Introduction The Role of Astronomy p. 3 Astronomical Objects of Research p. 4 The Scale of the Universe p. 7 Spherical Astronomy Spherical Trigonometry p. 9 The Earth p. 12 The Celestial Sphere p. 14 The
Color-Magnitude Diagram Lab Manual
Color-Magnitude Diagram Lab Manual Due Oct. 21, 2011 1 Pre-Lab 1.1 Photometry and the Magnitude Scale The brightness of stars is represented by its value on the magnitude scale. The ancient Greek astronomer
Project for Observational Astronomy 2018/2019: Colour-magnitude diagram of an open cluster
Project for Observational Astronomy 018/019: Colour-magnitude diagram of an open cluster Søren S. Larsen November 9, 018 1 1 Colour-magnitude diagram for an open cluster 1.1 Background The colour-magnitude
OUR DUSTY MILKY WAY: CONSTRAINING THE DUST DISTRIBUTION IN THE DISK OF OUR GALAXY
OUR DUSTY MILKY WAY: CONSTRAINING THE DUST DISTRIBUTION IN THE DISK OF OUR GALAXY Gail Zasowski 1 Advisor: Steven R. Majewski 1 1 Department of Astronomy, University of Virginia, Charlottesville, VA, 22904
Lecture 29. Our Galaxy: "Milky Way"
Lecture 29 The Milky Way Galaxy Disk, Bulge, Halo Rotation Curve Galactic Center Apr 3, 2006 Astro 100 Lecture 29 1 Our Galaxy: "Milky Way" Milky, diffuse band of light around sky known to ancients. Galileo
Project for Observational Astronomy 2017/2018: Colour-magnitude diagram of an open cluster
Project for Observational Astronomy 017/018: Colour-magnitude diagram of an open cluster Søren S. Larsen December 13, 017 1 1 Colour-magnitude diagram for an open cluster 1.1 Background The colour-magnitude
Astronomy 100 Spring 2006 Lecture Questions Twelve Weeks Review
Astronomy 100 Spring 2006 Lecture Questions Twelve Weeks Review 16-1 Fusion in the Sun The solar corona has temperatures roughly the same as temperatures in the Sun's core, where nuclear fusion takes place.
7. Dust Grains & Interstellar Extinction. James R. Graham University of California, Berkeley
7. Dust Grains & Interstellar Extinction James R. Graham University of California, Berkeley Visual Extinction Presence of interstellar gas or nebulae has a long history Existence of absorbing interstellar
Astr 2310 Thurs. March 23, 2017 Today s Topics
Astr 2310 Thurs. March 23, 2017 Today s Topics Chapter 16: The Interstellar Medium and Star Formation Interstellar Dust and Dark Nebulae Interstellar Dust Dark Nebulae Interstellar Reddening Interstellar
Age Dating A SSP. Quick quiz: please write down a 3 sentence explanation of why these plots look like they do.
Color is only a weak function of age after ~3Gyrs (for a given metallicity) (See MBW pg 473) But there is a strong change in M/L V and weak change in M/L K Age Dating A SSP Quick quiz: please write down
Interstellar Dust and Extinction
University of Oxford, Astrophysics November 12, 2007 Outline Extinction Spectral Features Emission Scattering Polarization Grain Models & Evolution Conclusions What and Why? Dust covers a range of compound
Review of stellar evolution and color-magnitude diagrams
Review of stellar evolution and color-magnitude diagrams The evolution of stars can be used to study the properties of galaxies Very characteristic features pinpoint at the age (chemistry) of the stars
Lab 4 Radial Velocity Determination of Membership in Open Clusters
Lab 4 Radial Velocity Determination of Membership in Open Clusters Sean Lockwood 1, Dipesh Bhattarai 2, Neil Lender 3 December 2, 2007 Abstract We used the Doppler velocity of 29 stars in the open clusters
Taurus stars membership in the Pleiades open cluster
Taurus stars membership in the Pleiades open cluster Tadross, A. L., Hanna, M. A., Awadalla, N. S. National Research Institute of Astronomy & Geophysics, NRIAG, 11421 Helwan, Cairo, Egypt ABSTRACT In this
Thirteen-Color Photometry of Open Cluster M48
Publications of the Astronomical Society of the Pacific, 117:32 36, 2005 January 2004. The Astronomical Society of the Pacific. All rights reserved. Printed in U.S.A. Thirteen-Color Photometry of Open
Age Determination of Possible Binary Open Clusters NGC 2383/NGC 2384 and Pismis 6/Pismis 8
Bulg. J. Phys. 33 (6) 68 7 Age Determination of Possible Binary Open Clusters NGC 383/NGC 384 and Pismis 6/Pismis 8 V. Kopchev 1, G. Petrov 1, P. Nedialkov 1 Institute of Astronomy, Bulgarian Academy of
A100 Exploring the Universe: The Milky Way as a Galaxy. Martin D. Weinberg UMass Astronomy
A100 Exploring the Universe: The Milky Way as a Galaxy Martin D. Weinberg UMass Astronomy astron100-mdw@courses.umass.edu November 12, 2014 Read: Chap 19 11/12/14 slide 1 Exam #2 Returned and posted tomorrow
Interstellar Dust Clouds UROP Spring 2013 Chris Nolting Faculty Mentor: Professor Terry Jones 5/17/13
Interstellar Dust Clouds UROP Spring 2013 Chris Nolting Faculty Mentor: Professor Terry Jones 5/17/13 Using infrared observations of L1544, a dark cloud in the Taurus Molecular Complex, density maps were
M31 Color Mag Diagram Brown et al 592:L17-L20!
The physical origin of the form of the IMF is not well understood Use the stellar mass-luminosity relation and present day stellar luminosity function together with a model of how the star formation rate
Galaxies. The majority of known galaxies fall into one of three major classes: spirals (78 %), ellipticals (18 %) and irregulars (4 %).
Galaxies Collection of stars, gas and dust bound together by their common gravitational pull. Galaxies range from 10,000 to 200,000 light-years in size. 1781 Charles Messier 1923 Edwin Hubble The distribution
The Next 2-3 Weeks. Important to read through Chapter 17 (Relativity) before I start lecturing on it.
The Next 2-3 Weeks [27.1] The Extragalactic Distance Scale. [27.2] The Expansion of the Universe. [29.1] Newtonian Cosmology [29.2] The Cosmic Microwave Background [17] General Relativity & Black Holes
Lecture 5. Interstellar Dust: Optical Properties
Lecture 5. Interstellar Dust: Optical Properties 1. Introduction 2. Extinction 3. Mie Scattering 4. Dust to Gas Ratio 5. Appendices References Spitzer Ch. 7, Osterbrock Ch. 7 DC Whittet, Dust in the Galactic
The Milky Way, Our galaxy
The Milky Way, Our galaxy Diffuse Band of light that crosses the Sky in the North Galileo: it s faint stars Early speculation and fleshing out where we are 1 Milky Way from Zuerich Milky Way from Australia
The Hertzsprung-Russell Diagram
The Hertzsprung-Russell Diagram VIREO Virtual Educational Observatory Aims To use the observational + analysis tools of modern astronomy To use the setup that professional astronomers use at large telescopes
Lecture 2: Galaxy types, spectra
Lecture 2: Galaxy types, spectra Galaxies AS 3011 1 Hubble tuning fork this is really just descriptive, but Hubble suggested galaxies evolve from left to right in this picture not unreasonable, perhaps
Lecture 2: Galaxy types, spectra. Galaxies AS
Lecture 2: Galaxy types, spectra Galaxies AS 3011 1 Hubble tuning fork this is really just descriptive, but Hubble suggested galaxies evolve from left to right in this picture not unreasonable, perhaps
Structure & Evolution of Stars 1
Structure and Evolution of Stars Lecture 2: Observational Properties Distance measurement Space velocities Apparent magnitudes and colours Absolute magnitudes and luminosities Blackbodies and temperatures
THE PLEIADES OPEN CLUSTER
THE PLEIADES OPEN CLUSTER G. Iafrate (a), M. Ramella (a) and P. Padovani (b) (a) INAF - Astronomical Observatory of Trieste (b) ESO - European Southern Observatory 1 Introduction Open star clusters are
Extragalactic Astronomy
Extragalactic Astronomy Topics: Milky Way Galaxies: types, properties, black holes Active galactic nuclei Clusters and groups of galaxies Cosmology and the expanding universe Formation of structure Galaxies
Observational properties of brown dwarfs (end)
Polarimetry expectations Observational properties of brown dwarfs (end) Dust in the photosphere produces scattering Non-spherical: Relation eccentricity e angular velocity!: uniform density " uniform rotation
(a) B-V 6 V. (b) B-V
721 TOWARDS AN IMPROVED MODEL OF THE GALAXY Johan Holmberg 1, Chris Flynn 2, Lennart Lindegren 1 1 Lund Observatory, Box 43, SE-22100 Lund, Sweden 2 Tuorla Observatory, Vaisalantie 20, FI-21500 Piikkio,
PHYS133 Lab 7 The HR Diagram
PHYS133 Lab 7 Goals: Measure brightness of various stars in the Pleiades star cluster in two different wavelength bands. Create an HR diagram based on the data taken. Use the distance modulus to determine
LECTURE 1: Introduction to Galaxies. The Milky Way on a clear night
LECTURE 1: Introduction to Galaxies The Milky Way on a clear night VISIBLE COMPONENTS OF THE MILKY WAY Our Sun is located 28,000 light years (8.58 kiloparsecs from the center of our Galaxy) in the Orion
Distance and extinction determination for stars in LAMOST and APOGEE survey
Distance and extinction determination for stars in LAMOST and APOGEE survey 王建岭 (LAMOST, References: NAOC) Wang et al. 2015a, MNRAS, submitted Wang et al. 2015b, In preparation Outline Background: why
X Rays must be viewed from space used for detecting exotic objects such as neutron stars and black holes also observing the Sun.
6/25 How do we get information from the telescope? 1. Galileo drew pictures. 2. With the invention of photography, we began taking pictures of the view in the telescope. With telescopes that would rotate
Fundamental stellar parameters
Fundamental stellar parameters flux received at Earth f º = direct determination of Teff R = radius of the spherical star, D = distance to the star. Luminosity : L = 4π R 2 F º dº T eff 4 = 4π R 2 F =
MSci Astrophysics 210PHY412
MSci Astrophysics 210PHY412 Stellar structure and evolution Dr. Stephen Smartt (Room S039) Department of Physics and Astronomy S.Smartt@qub.ac.uk Online resources - QoL and http://star.pst.qub.ac.uk/~sjs/teaching.html
LAB: Photometry of the Pleiades Cluster
LAB: Photometry of the Pleiades Cluster ASTR 203 - Instructors Olszewski & Rigby Due IN CLASS on Oct. 30 You may work with 1 partner. If you do, only turn in 1 assignment with both your names on it! You
ASTRONOMY 460: PROJECT INTRO - GALACTIC ROTATION CURVE
ASTRONOMY 460: PROJECT INTRO - GALACTIC ROTATION CURVE Snežana Stanimirović, October 6, 2014 1. Introduction This project has two goals: we want to measure the Milky Way (or Galactic) rotation curve by
Astronomical imagers. ASTR320 Monday February 18, 2019
Astronomical imagers ASTR320 Monday February 18, 2019 Astronomical imaging Telescopes gather light and focus onto a focal plane, but don t make perfect images Use a camera to improve quality of images
THE GALACTIC BULGE AS SEEN BY GAIA
143 THE GALACTIC BULGE AS SEEN BY GAIA C. Reylé 1, A.C. Robin 1, M. Schultheis 1, S. Picaud 2 1 Observatoire de Besançon, CNRS UMR 6091, BP 1615, 25010 Besançon cedex, France 2 IAG/USP Departamento de
Lecture 30. The Galactic Center
Lecture 30 History of the Galaxy Populations and Enrichment Galactic Evolution Spiral Arms Galactic Types Apr 5, 2006 Astro 100 Lecture 30 1 The Galactic Center The nature of the center of the Galaxy is
Results better than Quiz 5, back to normal Distribution not ready yet, sorry Correct up to 4 questions, due Monday, Apr. 26
Brooks observing April 19-22: 9:00 PM to at least 10:15 PM Tonight is a go! April 26-29: 9:30 PM to at least 10:45 PM Regular Friday evening public observing after planetarium shows also an option Begins
Deriving stellar masses from SDSS
Deriving stellar masses from SDSS Reference: Bruzual and Charlot 2003MNRAS.344.1000B Kauffmann et al. 2003MNRAS.341.33 Salim et al. 2007ApJS..173..267S Bell et al. 2003ApJS..149..289B Outline! Basic idea!
Observed Properties of Stars ASTR 2120 Sarazin
Observed Properties of Stars ASTR 2120 Sarazin Extrinsic Properties Location Motion kinematics Extrinsic Properties Location Use spherical coordinate system centered on Solar System Two angles (θ,φ) Right
OPEN CLUSTER PRELAB The first place to look for answers is in the lab script!
NAME: 1. Define using complete sentences: Globular Cluster: OPEN CLUSTER PRELAB The first place to look for answers is in the lab script! Open Cluster: Main Sequence: Turnoff point: Answer the following
Astronomy 113. Dr. Joseph E. Pesce, Ph.D. Dr. Joseph E. Pesce, Ph.D.
Astronomy 113 Dr. Joseph E. Pesce, Ph.D. The Nature of Stars 8-2 Parallax For nearby stars - measure distances with parallax July 1 AU d p A A A January ³ d = 1/p (arcsec) [pc] ³ 1pc when p=1arcsec; 1pc=206,265AU=3