Midterm Distribution 31 A’s, 37 B’s, 26 C’s, 21 D’s, 17 F’s.

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Midterm Distribution 31 A’s, 37 B’s, 26 C’s, 21 D’s, 17 F’s

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Transcript of Midterm Distribution 31 A’s, 37 B’s, 26 C’s, 21 D’s, 17 F’s.

Page 1: Midterm Distribution 31 A’s, 37 B’s, 26 C’s, 21 D’s, 17 F’s.

Midterm Distribution

31 A’s, 37 B’s, 26 C’s, 21 D’s, 17 F’s

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Common Mistakes

Do the algebra first! Units, Units, Units Does your answer make sense? Using ratios

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Lecture 18:

Telescopes

and

Observational Astronomy

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There are two kinds of telescopes

RefractingRefracting: a lens is used to focus the light from distant objects.

ReflectingReflecting: a primary mirror is used to gather and focus light.

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A Refracting Telescope

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A Reflecting Telescope

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Alternative designs for reflecting telescopes

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Charge Coupled Devices (CCD)

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Fundamental Telescope Properties

Light collecting area (diameter of primary mirror or lens)

angular resolution (smallest angular distance that can be resolved clearly) limited by effects of Earth’s atmosphere

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Angular Separation

= 360o . s /(2d)

“small angle formula”

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Angular Resolution

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Diffraction

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The Diffraction Limitdiffraction limit = 2.5 x 105 x wavelength of light(arcsec) diameter of telescope

Find the diffraction limit of the 2.4 m Hubble Space Telescope for visible light (500 nm).

d.l. = 2.5 x 105 (500 x 10-9 m/2.4 m) = 0.05 arcsec

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Where to put your telescope high and dry – to minimize the blurring

effects of the Earth’s atmosphere and emission/absorption from water vapor

away from light pollution with roads, electricity, and other support

systems nearby

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The Summit of Mauna Kea

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The Keck Telescopes

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The Magellan Telescopes

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Basic Functions of Telescopes

Imaging/photometryaccurate measurement of light intensity filters can be used to separate into different

colors spectroscopy

light spread out using a diffraction grating time sequence

how an object’s brightness changes with time

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A Basic Spectrograph

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Spectral Resolution

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Telescopes across the spectrum

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Hubble Space Telescope

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Infra-red Telescopes

SOFIA

SIRTF

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Radio Telescopes

Arecibo

Very Large Array (VLA)

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Interferometry

An array of smaller telescopes can be used together

the light gathering power is equal to the sum of all the areas

the angular resolution is greatly improved

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X-ray Telescopes

grazing incidence mirror

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Chandra X-ray Observatory

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Compton Gamma-ray Observatory

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Images of non-visible light

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Radio

CO

FIR

NIR

vis.

X-ray

gammaray


My B F F’S

My B F F’S

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3 B’s B4 Me

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