How to Choose a Model¶
The dust_extinction package provides a suite of dust extinction models.
Which model to use can depend on the wavelength range of interest, the expected
type of extinction, or some other property.
Average Models¶
Simple Average Curves¶
These are straightforward averages of observed extinction curves. They are the
simplest models and include models for the MW
(RL85_MWGC,
RRP89_MWGC,
B92_MWAvg,
I05_MWAvg,
CT06_MWLoc,
CT06_MWGC,
GCC09_MWAvg,
F11_MWGC,
G21_MWAvg;
D22_MWAvg;
Note the different valid wavelength ranges), the LMC
(G03_LMCAvg,
G03_LMC2) and the SMC
(G03_SMCBar).
One often used alternative to these straight average models is to use one of the parameter dependent models with the average R(V) value. For the Milky Way, the usual average used is R(V) = 3.1. See the next section.
Model |
x range [1/micron] |
wavelength range [micron] |
galaxy |
|---|---|---|---|
B92_MWAvg |
1.3 - 2.9 |
0.34 - 0.78 |
MW |
I05_MWAvg |
0.13 - 0.8 |
1.24 - 7.76 |
MW |
GCC09_MWAvg |
0.3 - 10.96 |
0.0912 - 3.3 |
MW |
G21_MWAvg |
0.3125 - 1 |
1 - 32 |
MW |
D22_MWAvg |
0.2 - 1.25 |
0.8 - 4 |
MW |
CT06_MWLoc |
0.037 - 0.8 |
1.24 - 27.0 |
MW (Local) |
RL85_MWGC |
0.08 - 0.8 |
1.25 - 13.0 |
MW (GCenter) |
RRP89_MWGC |
0.08 - 1.25 |
0.8 - 13.0 |
MW (GCenter) |
CT06_MWGC |
0.037 - 0.8 |
1.24 - 27.0 |
MW (GCenter) |
F11_MWGC |
0.05 - 0.8 |
1.28 - 19.1 |
MW (GCenter) |
G03_LMCAvg |
0.3 - 10.0 |
0.1 - 3.3 |
LMC |
G03_LMC2 |
0.3 - 10.0 |
0.1 - 3.3 |
LMC (30 Dor) |
G03_SMCBar |
0.3 - 10.0 |
0.1 - 3.3 |
SMC |
Parameter Dependent Average Curves¶
The models that are dependent on parameters provide average curves that account for overall changes in the extinction curve shapes. For example, the average behavior of Milky Way extinction curves has been shown to be dependent on R(V) = A(V)/E(B-V). R(V) roughly tracks with the average dust grain size.
For MW type extinction, the
G23 model should be considered as it
spectroscopically covers the far-ultraviolet (912 A) to mid-infrared (32 micron)
and is based on the spectroscopic extinction curves used for the
GCC09,
F19,
G21_MWAvg, and
D22 studies.
For those who wish to bypass the python implementation of the
G23 model, tables for the range
of valid R(V) values with 0.1 steps are available.
A more general model is G16 as this
model encompasses the average measured behavior of extinction curves in the MW,
LMC, and SMC. But it only covers wavelengths between 1150 A and 3 micron.
The G16 model reduces
to the F99 model with fA=
1.0.
Model |
Parameters |
x range [1/micron] |
wavelength range [micron] |
galaxy |
|---|---|---|---|---|
CCM89 |
R(V) |
0.3 - 10.0 |
0.1 - 3.3 |
MW |
O94 |
R(V) |
0.3 - 10.0 |
0.1 - 3.3 |
MW |
F99, F04 |
R(V) |
0.3 - 10.0 |
0.1 - 3.3 |
MW |
VCG04 |
R(V) |
3.3 - 8.0 |
0.125 - 0.31 |
MW |
GCC09 |
R(V) |
3.3 - 11.0 |
0.0912 - 0.31 |
MW |
M14 |
R_5495 |
0.3 - 3.3 |
0.31 - 3.3 |
MW, LMC |
G16 |
R(V)_A, f_A |
0.3 - 10.0 |
0.1 - 3.3 |
MW, LMC, SMC |
F19 |
R(V) |
0.3 - 8.7 |
0.115 - 3.3 |
MW |
D22 |
R(V) |
0.2 - 1.25 |
0.8 - 5.0 |
MW |
G23 |
R(V) |
0.032 - 11.0 |
0.0912 - 32.0 |
MW |
Notes¶
The M14 models focus on refining
models in the optical, and use the
CCM89 models for the NIR and the UV.
The M14 models use
R_5495 = A(5485)/E(4405-5495), the spectroscopic equivalent to
band-integrated R(V); see the paper for discussion. Because of a spurious
feature in the near UV caused by smoothly tying their optical to the
CCM89 UV, only the NIR and
optical portions of the M14
models are provided here.
Grain Models¶
The models are based on dust grain models that are calculated based on dust size, composition, and shape distributions. The distributions are constrained by observations of dust extinction, abundances, emission, and polarization (usually a subset, not all). One use of these models is to provide extinction measurements at wavelengths not accessible observationally (e.g., in the extreme UV below 912 A).
Model |
x range [1/micron] |
wavelength range [micron] |
galaxy |
|---|---|---|---|
DBP90 MWRV31 |
0.00001 - 10.9 |
0.0918 - 100000 |
MW R(V)=3.1 |
WD01 MWRV31 |
0.0001 - 100 |
0.01 - 10000 |
MW R(V)=3.1 |
WD01 MWRV40 |
0.0001 - 100 |
0.01 - 10000 |
MW R(V)=4.0 |
WD01 MWRV55 |
0.0001 - 100 |
0.01 - 10000 |
MW R(V)=5.5 |
WD01 LMCAvg |
0.0001 - 100 |
0.01 - 10000 |
LMC |
WD01 LMC2 |
0.0001 - 100 |
0.01 - 10000 |
LMC2 Region |
WD01 SMCBar |
0.0001 - 100 |
0.01 - 10000 |
SMC |
D03 MWRV31 |
0.0001 - 10000 |
0.0001 - 10000 |
MW R(V)=3.1 |
D03 MWRV40 |
0.0001 - 10000 |
0.0001 - 10000 |
MW R(V)=4.0 |
D03 MWRV55 |
0.0001 - 10000 |
0.0001 - 10000 |
MW R(V)=5.5 |
ZDA04 MWRV31 |
0.0001 - 1000 |
0.001 - 10000 |
MW R(V)=3.1 |
C11 MWRV31 |
0.00001 - 25 |
0.04 - 100000 |
MW R(V)=3.1 |
J13 MWRV31 |
0.00001 - 25 |
0.04 - 100000 |
MW R(V)=3.1 |
HD23 MWRV31 |
0.000033 - 10 |
0.1 - 30000 |
MW R(V)=3.1 |
Shape Models¶
The models that focus on describing the full extinction curve shape are usually
used to fit measured extinction curves. These models allow features in the
extinction curve to be measured (e.g., 2175 A bump or 10 micron silicate
feature). The P92 is the most
general as it covers the a very broad wavelength range. The
FM90 model covers the UV wavelength range
and has been extensively shown to fit all known UV extinction curves.
The FM90_B3 model provides a variant
of the FM90 model that uses B3 instead of C3 as B3 = explicit 2175 A
bump height = C3/gamma^2.
G21 model focuses on the NIR/MIR
wavelength range from 1-40 micron.
Model |
x range [1/micron] |
wavelength range [micron] |
# of parameters |
|---|---|---|---|
FM90 |
3.13 - 11.0 |
0.0912 - 0.32 |
6 |
FM90_B3 |
3.13 - 11.0 |
0.0912 - 0.32 |
6 |
P92 |
0.001 - 1000 |
0.001 - 1000 |
19 (24 possible) |
G21 |
0.025 - 1 |
1 - 40 |
10 |