Section 4: Spectroscopic Measurements Flashcards

1
Q

what are the quantities we obtain from a spectrum

A

-precise wavelength determination of features ie lines and edges
-spectral energy density of the continuum
-spectral line shape (intensity, width(

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2
Q

quantities obtained from a spectrum are interpreted using

A

physical models for the production of radiation

or laboratory or other standard measurements to derive parameters like density, temperature, velocity etc

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3
Q

most spectrometers in use are based on

A

diffraction gratings or interference filters

(fourier transform spectrometers based on michelson are also used for high spectral-resolution work, especially in the infrared)

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4
Q

Modern spectrometers often imaging spectrometers, called Integral Field Units, giving spectrum for

A

multiple x.y positions in image

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5
Q

grating spectrometer results

A

spectral resolving power
angular dispersion
grating response width

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6
Q

spectral resolving power

A

Rg = λ/delta λ = Ngm

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7
Q

angular dispersion

A

d theta /dλ = m/acos theta

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8
Q

grating response width

A

Wg=λ/Nga

lower limit to the angular width of lines produced by spectrometer

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9
Q

problems with raw spectra

A

usual CCD problems (cosmic ray hits, flatfield…)

spectral lines tilted on detector

no wavelength identification

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10
Q

For ground-based instruments, wavelength calibration for gratings or prisms is sometimes done using

A

absorption lines from the Earth’s atmosphere (telluric lines)

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11
Q

alternative method for ground-based instruments, wavelength calibration is done using

A

reference spectral emission lamp

(the spectrum from the source and from the calibration lamps is imaged onto the same CCD)

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12
Q

standard reference lamps include

A

Thorium/Argon and He/Ne/Ar

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13
Q

x is the position on the CCD, expressed in

A

‘pixel number’

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14
Q

the dispersed reference spectrum or the reference telluric lines provide calibration as follows

A
  1. strong lines/patterns of lines from reference spectrum identified using spectral atlas
  2. fit spectral profile (eg gaussian) on CCD to find x position of central λ of ref lines
  3. a curve is fitted to these identifications, giving λ(x)
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15
Q

CCD-based spectroscopes provide a

A

2D image of the spectrum

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16
Q

the dispersed emission line spectrum consists of

A

multiple images of the spectroscope slit, spread in colour/position along the CCD

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17
Q

ideally, slit images should be as

A

narrow as possible and aligned with CCD columns

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18
Q

to get a spatially integrated spectrum, sum

A

down columns to produce spectrum

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19
Q

In practice, there might be slight mis-alignments of the optics, which
will result

A

in tilted slit images

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20
Q

in a ground-based instrument, tilted slit images could, in principle, be corrected by

A

rotating the detector

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21
Q

in a space-based instrument, tilted slit images need to be correct in the

A

data analysis phase

ie rotation of the spectral lines so they are aligned with the y-axis

however this remapping can cause other issues

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22
Q

what if the remapped pixel values are not integers, how to we assign the counts to actual pixel positions

A

this is done by interpolating the data to the integer pixel positions

(consider the 1D problem and assume that the data follows a piecewise linear cure)

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23
Q

interpolation - the gradient between i1’ and i2’ is

A

m=N(i2’)-N(i1’) / i2’-i1’

(denominator is approx 1)

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24
Q

interpolation - the value of N(i’) at pixel i’ is

A

starting point:
N(i’)=N(i1’) +m(1- deltai’)

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25
Q

interpolation - the counts value at this pixel is the

A

distance weighted mean of the counts at the two neighbouring locations

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26
Q

the distance weighted mean of N(i1’) and N(i2’) gives us

A

N(i’)

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27
Q

linear interpolation is only an example, can also

A

fit a quadratic, or a polynomial through several neighbouring points depending on how rapidly the data is changing from point to point

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28
Q

Sources of instrumental noise should be reasonably well removed by

A

subtracting dark current, flat-fielding etc

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29
Q

even after noise removed, the source of interest will be seen against

A

the background (or foreground) contribution of the sky

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30
Q

if optically thin emission from the source of interest, would have to consider

A

emission from behind

this all has to be removed to get at the source spectrum

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31
Q

usually background is not constant - how to deal with

A

define two background regions, on either side of the feature and then do a linear interpolation using data points in these two regions

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32
Q

let background = Nb(λ) =

A

mλ+c

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33
Q

(background subtraction) the total real counts in the source are

A

sum from λ=λ1 to λ2 of
(N(λ)-Nb(λ))

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34
Q

Whether subtracting background from an image or a spectrum, we deal with errors

A

in the same basic way

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35
Q

Ns+b=

A

Ns +Nb

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36
Q

total counts in the source is, Ns=

A

Ns+b - Nb
=(Ns+Nb)-Nb

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37
Q

the combined errors (assuming poisson noise) are σs^2=

A

σs+b^2 +σb^2
=…
=Ns+2Nb

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38
Q

combined errors assumes gain and quantum efficiency are

A

1
otherwise would need to take into account (see section 2)

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39
Q

uncertainty in N=

A

σ= sqrt (Ng/Q) (Q/g)

=sqrt (NQ/g) [in DN]

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40
Q

The “significance” of an observation is defined as

A

the signal expressed as a number of standard deviations

aka SNR

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41
Q

if Ns is 4 times σs, then this is called

A

a 4σ measurement

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42
Q

if we consider a situation where the background is low compared to the signal then Ns/σs=

A

sqrt (Ns)

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43
Q

if Ns=rate x delta t and rate=const the significance

A

increases as sqrt(delta t)

ie 10x more signficance = 100 x longer exposure time

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44
Q

Properties of spectral lines can be analysed to understand the
conditions in the emitting medium. Because this is done “remotely” without affecting the astronomical
objects, the analysis is said to

A

provide ‘diagnostics’

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45
Q

An absorption line is formed by a

A

cooler less-dense gas overlying a
hotter dense one

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46
Q

In general, the more atoms there
are in the correct state to absorb
the radiation from below, the

A

deeper the (absorption) line profile will be

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47
Q

absorption lines - also have to take into account the effect of

A

convolution with instrumental line profile

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48
Q

The equivalent width 𝑾 is a way to

A

measure the total absorption in a spectral line

W such that the area of rectangular region = area of the spectral line

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49
Q

equivalent width - let the line intensity be described by

A

B_λ which is a function of wavelength

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50
Q

equivalent width - let the continuum intensity be

A

Bc which is taken as a constant

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51
Q

area of absorption line=

A

integral form 0 to inf of (Bc-Bλ)dλ

=WBc

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52
Q

equivalent width, W=

A

integral from - to inf of
Bc-Bλ / Bc dλ

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53
Q

The absorption of photons is described by

A

the optical depth
τ_λ

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54
Q

in the absorption line, photons are taken out of the continuum (in the simplest case) and this is described by

A

Bλ/Bc = e^-τ_λ

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55
Q

if τ_λ is large then

A

Bλ is small relative to Bc (strong absorption)

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56
Q

for a weak spectral line (τ_λ«1), what do you use for expression for W

A

the series expansion for the exponential function to simplify the expression for W

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57
Q

The optical depth is related to

A

the atomic properties of the absorbing
material, and the density of absorbers

58
Q

the atomic properties are encapsulated in the

A

absorption crosssection, 𝝈𝝀, which is a function of wavelength

59
Q

A narrow slab of absorbing gas, with thickness 𝚫𝒔, number density 𝒏 [m-3], has optical depth

A

𝜏𝜆 = 𝑛𝜎𝜆Δ𝑠 = 𝜎𝜆N

60
Q

column density

A

N= 𝑛Δ𝑠

61
Q

But it is clear that from 𝑾 we can obtain the

A

total amount of absorbing matter 𝑵, hence the usefulness of W

62
Q

strong lines

A

𝝉𝝀 ≫1

Wλ prop to sqrt N

63
Q

intermediate lines

A

𝝉𝝀 ≈ 𝟏
wλ prop to sqrt lnN

64
Q

curve of growth

A

shows how the equivalent width varies with density

curve of growth is calculated theoretically and the measured equivalent width can be linked directly to N

65
Q

Spectral lines are produced by

A

a hot, tenuous gas

eg coronae, gas clouds

66
Q

lyman break

A

everything at shorter wavelengths completely absorbed

due to neutral H along LOS in IGM

67
Q

Atomic line diagnostics often involve

A

measuring the ratio of
intensities between two emission lines from the same element

68
Q

The possible transitions in an element are illustrated by diagrams
called

A

Term or Grotrian diagrams

69
Q

Grotrian diagrams for neutral Fe, once-ionised and twice ionised Fe show

A

the richness of spectra from heavy ions

so many possible transitions

70
Q

Most common spectroscopic diagnostics rely on assuming that

A

the radiating gas/plasma is in local thermodynamic equilibrium

71
Q

In local thermodynamic equilibrium (LTE) the matter is

A

in thermal equilibrium in some small neighbourhood around a point in space

can be heating/cooling but doing so slow

matter and radiation do not have to be in equilibrium

72
Q
  • For a gas/plasma, LTE means that the particle distribution function
    𝒇(𝒗) is
A

a Maxwell-Boltzmann distribution

73
Q

LTE also means that the system reaches equilibrium via

A

collisions between particles

74
Q

In many cases we can also assume that interaction with radiation is

A

negligible

the radiation escapes the gas/plasma without interaction -
optically thin approximation

75
Q

most of the collisional excitation is by

A

free electrons

Being faster than ions or atoms at the same temperature, the free
electrons have more interactions per second

76
Q

a collision -

A

a free electron perturbs an orbital electron

77
Q

In LTE, the probability 𝒑𝒊 of finding an atom in state 𝒊 is determined by

A

the boltzmann factor, pi

78
Q

boltzmann factor is proportional to

A

po, gi (degeneracy) and energy

79
Q

what is po in the boltzmann factor

A

constant found by normalising the probability over all possible
states of energy 𝑬𝒊

80
Q

For two levels 𝒊 and 𝒋 (𝒋 = upper level and 𝒊 = lower level) the ratio
of the number of atoms in each level is

A

ni/ni =gi/gi exp (-(Ej-Ei)/kT)

81
Q

Ej-Ei is the

A

transition energy between levels

82
Q

the population ratio of two levels depends on

A

the temperature

83
Q

In an optically thin gas/plasma, the excitation to the upper level is by

A

collisions

84
Q

The average number 𝒏𝒊𝒋 of transitions per second per unit volume,
from state 𝒊 to state 𝒋, due to collisions is

A

nij = ni ne Cij

85
Q

Cij

A

the collisional rate coefficient, and depends on the electron speed,
and the atomic properties

86
Q

ne

A

the number of electrons per unit volume

87
Q

ni

A

the number of atoms in state 𝒊 per unit volume

88
Q

In a true equilibrium, the average state does not change, so for…

A

every upwards transition 𝒊 → 𝒋 must be accompanied somewhere by
a downwards transition 𝒋 → 𝒊.

this is called detailed balance

89
Q

In the case where upwards transitions are collision-dominated, and downward transitions are due to spontaneous radiation (the “coronal approximation”) we have

A

ni ne Cij = nj Aji

90
Q

the coronal approximation

A

the case where upwards transitions are collision-dominated, and
downward transitions are due to spontaneous radiation

91
Q

einstein coefficient

A

the average number of
transitions per second per atom

92
Q

Iji

A

photon emission rate per unit volume

=nj Aji

93
Q

Consider two levels of an atom - call them 1 and 2. Assume that they
are both excited by collisions from the ground level, and decay by
radiation back to the ground state. Then:

A

I2g/I1g = Cg2/Cg1

94
Q

the ratio of intensity of these 2 lines gives a measure of the

A

gas temperature

95
Q

Collisions between fast electrons and atoms in a hot gas can result
in

A

the ejection of a bound electron into a free state (ie collisional ionisation)

96
Q

Atoms with more than one electron can exist in different stages of
ionisation. Removing successive electrons takes

A

increasing amounts of energy

97
Q

ionisation potential

A

the energy required to remove an electron

represented by Chi

98
Q

Consider the situation where the upper level is an ion plus a free
electron with speed 𝒗. The energy of this level is

A

E= X +1/2me v^2

99
Q

To calculate the number of e-i pairs in this ionisation stage, we

A

calculate the number, 𝜟𝒏(𝒗) of states for an ion and a free electron
with velocity 𝒗, and then integrate over all possible v

100
Q

The statistical weight of a particle is

A

the
number of states that it can occupy

101
Q

Electrons
are fermions, so obey

A

Fermi-Dirac statistics

at most only 2 e- per state

102
Q

saha ionisation equation relates

A

the number of ions in ionisation stages r+1 and r

103
Q

population of different ionisation stages of the same species
depends sensitively on

A

the plasma temperature

104
Q

calculations of the saha equation for various ion pairs as a function of temperature results in

A

ionisation balance curves

105
Q

ionisation balance curves

A

ratio will peak at some temp and then fall off

106
Q

contribution function

A

g(t)
calculated from atomic physics and peaks strongly at some T

107
Q

By plotting the ratio of two spectral lines from the same ion, the 𝚺
and 𝒏𝒆 terms

A

cancel and we are left with the ratio of the two g(t) functions

this ratio depends on temperature

108
Q

Assuming emission from isothermal plasma, the temperature can be
determined from

A

the observed intensity ratio

109
Q

contribution function sensitive only over a limited temperature tange, depending on

A

the lines used

110
Q

If we allow also for collisional de-excitation from level 𝒋 to level 𝒊,
then the expression for detailed balance becomes

A

same as before but with an additional njneCij term

111
Q

collisional de-excitation from level j to level i might happen if

A

Aji is very small

ie the natural (radiative) decay time of level j is very long

112
Q

Aji=

A

1/τ

where τ is the radiative lifetime

113
Q

forbidden transition - the upper level is called a

A

metastable level

114
Q

de-population of metastable levels can be largely due to

A

collisions which depend on the electron density

ie this gives diagnostic on electron density

115
Q

intensity of spontaneously de-excited allowed line 2 –> 1

A

I21=n1neC12

116
Q

metastable level m can be depopulated by

A

radiation or by collisions C* either to the ground state or other states

117
Q

n1neC1m=

A

nm Am1 + Σ nm ne C*

the sum is over all possible states accessible by collisions

118
Q

Only that fraction of the excited metastable population that decays by radiation contributes to

A

the line intensity

119
Q

the observed ratio is dependent on

A

electron number density ne

(derivation on slides 150 and 151)

120
Q

The width of the observed spectral line is due to

A

a number of different processes and hence a diagnostic

121
Q

finite lifetime of electron in the excited sates (lorentzian) causes

A

natural broadening and collisional broadening

122
Q

doppler motion on micro or macroscale (gaussian) causes

A

thermal, turbulent and rotational broadening

123
Q

Overall line we observe is a
convolution of

A

these processes

lorentzian * gaussian ==> voigt

(and convolved with the ILP)

124
Q

this course focuses on which types of broadening

A

thermal and turbulent

this keeps everything gaussian

125
Q

The emission lines from a hot gas are broadened due to

A

random particle motions

λ-λ0/λ0 = v/c

126
Q

line profile Φ(λ) is given by

A

Φth(λ) dλ = f(v)dv

127
Q

f(v) is the 1D Maxwellian distribution so Φth is proportional to

A

exp(-mv^2/2kT)

128
Q

Using our other temperature diagnostics (line ratios), we can
determine

A

T and hence the expected thermal line width and vth

129
Q

Sometimes the observed spectral line width exceeds this thermal
value, even once the ILP is removed. One cause of this is

A

the additional speed can be turbulence

i.e. macroscopic motions of different parcels of emitting gas/plasma in
addition to the microscopic thermal motions

130
Q

Let the emitting gas have a distribution of macroscopic speeds

p(vl)dvl=

A

the probability that gas is moving at turbulent LOS speed vl –> vl+dvl

131
Q

Ignoring other broadening for the moment, the shape of the spectral
line profile 𝝓𝒕𝒖𝒓𝒃 𝝀 emitted by this gas is given by:

A

𝜙𝑡𝑢𝑟𝑏 (𝜆) 𝑑𝜆 = 𝑝 (𝑣𝐿) 𝑑𝑣

132
Q

To obtain the overall line profile, we need to evaluate

A

the probability that a particle ahs a total LOS speed vtot=vl+v

133
Q

The functions 𝒑(𝒗𝑳) and 𝒇(𝒗) are both probability density functions
and the LOS speeds 𝒗𝑳 and 𝒗 can be assumed to be

A

independent

134
Q

the probability of obtaining 𝒗𝑻𝑶𝑻 is obtained by

A

multiplying the pdfs and then integrating over all values of 𝒗, subject to 𝒗𝑻𝑶𝑻 = 𝒗𝑳 + v

135
Q

total line profile is thus given
by

A

the convolution of the individual line profiles

136
Q

line emitted by the thermal plasma convolved with turbulent broadening =

A

overall emitted line

137
Q

the total line profile is the convolution of

A

the thermal Gaussian
profile and the turbulent line profile

138
Q

Assume that the turbulent line profile is also Gaussian and define a
“turbulent broadening” such that

A

(Δλturb/λ0)^2 = (vturb/c)^2

139
Q

We can evaluate the resulting overall line profile using

A

the convolution theorem

140
Q

So the total line profile is also a Gaussian, with line width 𝚫𝝀𝑻𝑶𝑻,
from the combined effects of

A

turbulence and thermal broadening