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Measure the Sky 2nd Edition Chromey Solutions Manual

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Measure the Sky 2nd Edition Chromey Solutions Manual.

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Measure the Sky 2nd Edition Chromey Solutions Manual

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ISBN-10 ‏ : ‎ 9781107572560
ISBN-13 ‏ : ‎ 978-1107572560
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The second edition of this popular text provides undergraduates with a quantitative yet accessible introduction to the physical principles underlying the collection and analysis of observational data in contemporary optical and infrared astronomy. The text clearly links recent developments in ground- and space-based telescopes, observatory and instrument design, adaptive optics, and detector technologies to the more modest telescopes and detectors that students may use themselves. Beginning with reviews of the most relevant physical concepts and an introduction to elementary statistics, students are given the firm theoretical foundation they need. New topics, including an expanded treatment of spectroscopy, Gaia, the Large Synoptic Survey Telescope, and photometry at large redshifts bring the text up to date. Historical development of topics and quotations emphasize that astronomy is both a scientific and a human endeavour, while extensive end-of-chapter exercises facilitate the students’ practical learning experience.

Table contents:

Chapter 1 Light
1.1 The story
1.2 Models for the behavior of light
1.2.1 Electromagnetic waves
1.2.2 Quantum mechanics and light
1.2.3 A geometric approximation: light rays
1.3 Measurements of light rays
1.3.1 Luminosity and brightness
1.3.2 The inverse square law of brightness
1.3.3 Surface brightness
1.4 Spectra
1.4.1 Monochromatic flux
1.4.2 Flux within a band
1.4.3 Spectrum analysis
The Fraunhofer spectrum
The Kirchhoff–Bunsen results
Blackbody spectra
1.4.4 Spectra of stars
1.5 Magnitudes
1.5.1 Apparent magnitudes
1.5.2 Absolute magnitudes
1.5.3 The bolometric correction
1.5.4 Apparent magnitudes from images
1.5.5 Example problem
Exercises
Chapter 2 Uncertainty
2.1 Accuracy and precision
2.1.1 An example
2.1.2 Accuracy and systematic error
2.1.3 Precision and random error
2.1.4 Uncertainty
2.1.5 Digitizing effects
2.1.6 Significant digits
2.2 Describing populations
2.2.1 Descriptive statistics of a finite population
Measures of the central value
Measures of dispersion
2.2.2 Estimating population statistics
2.3 Probability distributions
2.3.1 The random variable
2.3.2 The Poisson distribution
2.3.3 The Gaussian, or normal, distribution
2.3.4 The standard normal distribution
2.3.5 Other distributions
2.4 Estimating uncertainty
2.4.1 The central limit theorem
2.4.2 Reducing uncertainty
2.5 Propagation of uncertainty
2.5.1 Combining several variables
2.5.2 General rule
2.5.3 Several measurements of a single variable
2.6 Additional topics
Exercises
Chapter 3 Place, time, and motion
3.1 Astronomical coordinate systems
3.1.1 Three-dimensional coordinates
3.1.2 Coordinates on a spherical surface
3.1.3 Terrestrial latitude and longitude
3.1.4 The altitude–azimuth system
3.1.5 The equatorial system: definition of coordinates
3.1.6 The relation between the equatorial and the horizon systems
3.1.7 Measuring equatorial coordinates
3.1.8 Precession and nutation
3.1.9 Barycentric coordinates
3.1.10 The ICRS
3.1.11 The ecliptic coordinate system
3.1.12 The Galactic coordinate system
3.1.13 Transformation of coordinates
3.2 The third dimension
3.2.1 The astronomical unit
3.2.2 Stellar parallax
3.3 Time
3.3.1 Atomic time
3.3.1 Solar time
3.4 Motion
3.4.1 Space motion
3.4.2 Proper motion
3.4.3 Radial velocity
Precise radial velocities
Large redshifts
Exercises
Chapter 4 Names, catalogs, and databases
4.1 Star names
4.1.1 Proper names
4.1.2 Bayer designations
4.1.3 Flamsteed designations
4.1.4 Double stars, exoplanets, and variables
4.1.5 Durchmusterung numbers
4.1.6 The nomenclature problem
4.1.7 Other stellar catalogs
4.2 Non-stellar objects outside the Solar System
4.2.1 Bright objects
4.2.2 Faint non-stellar objects
4.3 Objects at non-optical wavelengths
4.4 Atlases, finding charts, and sky surveys
4.5 Solar System objects
4.6 Websites and other computer resources
Exercises
Chapter 5 Optics for astronomy
5.1 Principles of geometrical optics
5.1.1 Rays and wavefronts in dielectric media
5.1.3 Reflection and transmission coefficients
5.1.4 Reflecting materials
5.1.5 Transmitting materials
5.1.6 Thin film coatings
5.1.7 Cleaning
5.1.8 Reflection at a spherical surface
5.1.9 Refraction at a spherical surface
5.2 Lenses, mirrors, and simple optical configurations
5.2.1 Thick lenses
5.2.2 Thin lenses
5.2.3 Graphical ray tracing
5.2.4 Multiple lenses
5.2.5 The thick plane-parallel plate
5.2.6 Refraction by an atmosphere
5.2.7 Optical fibers
5.2.8 Prisms
5.3 Simple telescopes
5.3.1 Telescopes as single-element cameras
5.3.2 Image scale and image size
5.3.3 Focal ratio and image brightness
5.3.4 Telescopes with oculars
5.4 Image quality: telescopic resolution
5.4.1. The diffraction limit
5.4.2 Rayleigh refused: atmospheric seeing and optical aberrations
5.5 Aberrations
5.5.1 Chromatic aberration
5.5.2 Classification of monochromatic wavefront aberrations
5.5.3 Shapes of optical surfaces
5.5.4 Spherical aberration
5.5.5 Coma
5.5.6 Astigmatism
5.5.7 Field curvature
5.5.8 Distortion
5.5.9 Other aberrations and ray tracing in practice
Exercises
Chapter 6 Astronomical telescopes
6.1 Telescope mounts and drives
6.1.1 Altazimuth and equatorial mounts
6.1.2 Telescope mounts in space
6.2 Reflecting telescope optics
6.2.1 Prime focus and Newtonian focus
6.2.2 Cassegrain and Gregorian reflectors
6.2.3 Aplanatic two-mirror telescopes
6.2.4 Nasmyth and coudé foci
6.2.5 Three-mirror telescopes
6.2.6 Schmidt telescopes
6.2.7 Other catadioptric telescopes
6.3 Telescopes in space
6.3.1 Advantages of space telescopes
Resolution
Detection limits
Background
Atmospheric transmission
Access to sky
Perturbing forces and environment
6.3.2 Disadvantages of space telescopes
6.3.3 Airborne telescopes
6.3.4 The James Webb Space Telescope
6.4 The current revolution in ground-based observing
6.4.1 Large mirrors
6.4.2 Observatory engineering
6.4.3 Computers
6.5 Atmospheric blur
6.5.1 Atmospheric wavefront (WF) distortion
6.5.2 High resolution on short exposures
6.5.3 Quantifying wavefront distortion
6.6 Adaptive optics
6.6.1 The idea of adaptive optics
6.6.2 The Greenwood time delay
6.6.3 Anisoplanatism
6.6.4 Guide stars
6.6.5 Wavefront correctors
6.6.6 Wavefront sensors
6.6.7 A simple AO system
6.6.8 Advanced AO systems
6.7 Extremely large telescopes
Exercises
Chapter 7 Matter and light
7.1 Isolated atoms
7.1.1 Atomic energy levels
7.1.2 Absorption of light by atoms
7.1.3 Emission of light by atoms
7.1.4 Collisions and thermal excitation
7.1.5 Specification of energy levels
7.2 Isolated molecules
7.3 Solid-state crystals
7.3.1 Bonds and bands in silicon
7.3.2 Conductors, semiconductors, and insulators
7.3.3 Intrinsic semiconductors
Semiconductor crystals
Conductivity and temperature
7.3.4 Intrinsic photo-absorbers
7.3.5 Extrinsic semiconductors
7.4 Photoconductors
7.4.1 Simple photoconductors
7.4.2 The blocked impurity band photoconductor
7.5 The MOS capacitor
7.6 The p–n junction
7.6.1 Generation and recombination
7.6.2 p–n junction diodes
7.6.3 Light detection in diodes
7.6.4 Variations on the junction diode
7.7 The vacuum photoelectric effect
7.8 Superconductivity
7.8.1 The superconductor band gap
7.8.2 Light detection in an SIS junction
7.8.3 Light detection in kinetic induction devices
Exercises
Chapter 8 Detectors
8.1 Detector characterization
8.1.1 Detection modes
8.1.2 Efficiency and yield
8.1.3 Noise
8.1.4 Spectral response and discrimination
8.1.5 Linearity and dynamic range
8.1.6 Stability
8.1.7 Response time
8.1.8 Physical size and pixel count
8.1.9 Image sampling and degradation
8.2 The CCD
8.2.1 General operation
8.2.2 Channel stops, blooming, full well, and gain
8.2.3 Readout time, read noise, and bias
8.2.4 Dark current, cooling, and vacuum enclosures
8.2.5 Charge transfer efficiency
8.2.6 The buried channel CCD
8.2.7 The MPP CCD
8.2.8 CCD variations
8.2.9 CCD sensitivity issues
Frontside options
Backthinning
Anti-reflection coatings
8.2.10 Drift scanning and time delayed integration
8.3 CMOS arrays
8.4 Infrared arrays
8.4.1 Detectors at different wavelengths
Silicon IR and SWIR (0.72–1.1 and 0.9–2.5 μm)
Thermal infrared
8.4.2 Infrared detector construction
8.5 Photo-emissive devices
8.5.1 The photomultiplier tube
8.5.2 The microchannel plate
8.5.3 Image intensifiers and the ICCD
8.6 Thermal detectors
Exercises
Chapter 9 Digital images from arrays
9.1 Arrays
9.1.1 Pixels and pixel response
9.1.2 Digital images
9.1.3 CCD gain
9.1.4 Pictures lie
9.2 Digital image manipulation
9.2.1 Basic image arithmetic
9.2.2 Image dimensions and color
9.2.3 Image functions
9.2.4 Image convolution and filtering
9.3 Preprocessing array data: bias, linearity, dark, flat, and fringe
9.3.1 Bias frames
9.3.2 Overscan and reference pixels
9.3.3 Dark current
9.3.4 Detector linearity
9.3.5 Flat field
Twilight flats
Dark-sky flats
Dome flats
Space telescope flats
Computing simple flats
Compound flats
9.3.6 Preprocessing data frames
9.3.7 Fringing
9.4 Combining images
9.4.1 Where is it? The centroid
9.4.2 Where is it, again? PSF fitting
9.4.3 Aligning images: shift, canvas, and trim
9.4.4 Aligning images: geometric transformations
9.4.5 Interpolation
9.4.6 Resampling, interlace, and drizzle
9.4.7 Cleaning images
9.5 Digital aperture photometry
9.5.1 Digital apertures and PSF fits
9.5.2 Measuring the sky
9.5.3 Signal and noise in an aperture
9.5.4 The CCD equation
Exercises
Chapter 10 Photometry
10.1 Introduction: a short history
10.2 The photometric response function
10.2.1 Types of photometry
Single-band photometry
Broadband multicolor photometry
Narrow- and intermediate-band photometry
10.2.2 Magnitudes
10.2.3 Response function implementation
10.2.4 Response function description
10.2.5 Color indices
10.2.6 Line and feature indices
10.3 The idea of a photometric system
10.4 Common photometric systems
10.4.1 Visual and photographic systems
10.4.2 The UBVRI system
10.4.3 The SDSS ugriz(y) system
10.4.4 The broadband infrared systems: ZYJHKLMNQ
10.4.5 The intermediate-band Strömgren system: uvbyβ
10.4.6 Other systems
10.5 Absorption by the atmosphere
10.5.1 Atmospheric windows
10.5.2 Absorption by a plane-parallel slab
10.5.3 Bouguer’s law
10.5.4 Sources of extinction
Rayleigh scattering by molecules
Absorption by ozone
Scattering by aerosols
Molecular-band absorption
10.5.5 Heterochromatic extinction
10.5.6 Compensating for extinction: theory
10.5.7 Compensating for extinction: practice
Case 1: assume a mean extinction
Case 2: use known outside-the-atmosphere magnitudes
Case 3: draw the Bouguer line from observations
Case 4: variable extinction
Case 5: use all the data
10.5.8 Indices or magnitudes?
10.6 Transformation to a standard system
10.7 Absorption outside the atmosphere
10.7.1 The interstellar medium
10.7.2 Interstellar absorption and reddening
10.7.3 The interstellar reddening law
10.7.4 Spectroscopic parallax
10.8 Wavelength changes
10.8.1 Redshift and photometry
10.8.2 The K correction
10.8.3 Absorption outside our Galaxy
Exercises
Chapter 11 Spectroscopy
11.1 Dispersive spectrometry
11.2 Dispersing optical elements
11.2.1 Prisms
11.2.2 The diffraction grating
11.2.3 Blazed gratings
11.2.4 Echelles
11.2.5 Volumetric phase gratings
11.2.6 Grating manufacture
11.3 Spectrometers without slits
11.3.1 The objective prism
11.3.2 The non-objective prism and grism
11.4 Basic slit and fiber spectrometers
11.5 Single-object spectrometer design for astronomy
11.5.1 An example configuration
11.5.2 Slit orientation and spectrum widening
11.5.3 Getting light in
11.6 Multiplexed spectrometers
11.6.1 Spectra without dispersion – energy-resolving detectors
11.6.2 Long-slit spectrometers
11.6.3 Integral field spectrometers
Image slicers
Fiber mosaics
Lenslet arrays
11.6.4 Multi-object spectrometers
11.6.5 Refinements
11.7 Spectrometer stability and mounting
11.8 Data acquisition and reduction
11.8.1 Observing practices
11.8.2 Spectrum extraction
11.8.3 Wavelength calibration
11.8.4 Flux calibration
11.8.5 Other calibrations
11.9 Interpreting spectra
11.9.1 Classification of stellar spectra
11.9.2 Spectra of gaseous nebulae
11.9.3 Measuring line strength
11.9.4 Line profiles
Natural broadening
Instrumental broadening
Rotational broadening
Thermal broadening
Microturbulence
Pressure broadening
Abundances
11.9.5 The redshift parameter
11.9.6 Determination of masses
11.9.7 Exoplanets
11.9.8 Galaxies and the universe
The Hubble law
Determining the value of H0
High z supernovae and dark energy
Exercises
Appendices
Appendix A General reference data
A1 The Greek alphabet
A2 Metric system prefixes and symbols
A3 Physical constants
A4 Astronomical constants
A5 Conversions
Appendix B Light
B1 Photon properties
B2 The strongest Fraunhofer lines
B3 Sensitivity of human vision
B4 The visually brightest stars
Appendix C
C1 The standard normal distribution
Appendix D
D1 The nearest stars
D2 The equation of time
D3 Coordinate transformations and relations
D4 Atmospheric refraction
D5 Astrometric catalogs
D6 Days and years
Appendix E
E1 The constellations
E2 Some named stars
E3 Naming small bodies in the Solar System
Minor planets
Comets
Natural satellites of the major and minor planets
Appendix F
F1 A timeline for optical telescopes
Appendix G
G1 Websites
G2 Largest optical telescopes (2015)*
G3 Large Schmidt telescopes
Appendix H
H1 The hydrogen atom
H2 Some common semiconductors
Appendix I
I1 Characteristics of some commercial CCDs for astronomy
I2 Manufacturers of sensors and cameras for astronomy
Appendix J
J1 The point-spread function
Appendix K
K1 Intrinsic broadband colors for various spectral types
References
Index

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