Collision Unit¶

How to Use Collision Unit

Collision Unit has the API functions for plasma diagnostics and abundance analysis of collisionally excited lines. Here are some examples of using Collision Unit:

Temperature:

In [1]:

s2=obj_new('collision')
s2->set,['s','ii']
upper_levels='1,2,1,3/'
lower_levels='1,5/'
density = double(2550)
line_flux_ratio=double(10.753)
temperature=s2->calc_temperature(line_flux_ratio=line_flux_ratio, density=density, $
                                 upper_levels=upper_levels, lower_levels=lower_levels)
print, "Electron Temperature:", temperature

Electron Temperature:       7920.2865

Density:

In [2]:

s2=obj_new('collision')
s2->set,['s','ii']
upper_levels='1,2/'
lower_levels='1,3/'
temperature=double(7000.0);
line_flux_ratio=double(1.506);
density=s2->calc_density(line_flux_ratio=line_flux_ratio, temperature=temperature, $
                         upper_levels=upper_levels, lower_levels=lower_levels)
print, "Electron Density:", density

Electron Density:       2312.6164

Ionic Abundance:

In [3]:

o3=obj_new('collision')
o3->set,['o','iii']
levels5007='3,4/'
temperature=double(10000.0)
density=double(5000.0)
iobs5007=double(1200.0)
Abb5007=o3->calc_abundance(temperature=temperature, density=density, $
                      line_flux=iobs5007, atomic_levels=levels5007)
print, 'N(O^2+)/N(H+):', Abb5007

N(O^2+)/N(H+):   0.00041256231

Emissivity:

In [4]:

o3=obj_new('collision')
o3->set,['o','iii']
levels5007='3,4/'
temperature=double(10000.0)
density=double(5000.0)
iobs5007=double(1200.0)
emis=o3->calc_emissivity(temperature=temperature, density=density, $
                    atomic_levels=levels5007)
print, 'Emissivity(O III 5007):', emis

Emissivity(O III 5007):   3.6041012e-21

Atomic Level Population:

In [5]:

s2=obj_new('collision')
s2->set,['s','ii']
density = double(1000)
temperature=double(10000.0);
Nlj=s2->calc_populations(temperature=temperature, density=density)
print, 'Populations:', Nlj

Populations:      0.96992796    0.0070037404     0.023062517   2.6594158e-06
   3.1277593e-06

Critical Density:

In [6]:

s2=obj_new('collision')
s2->set,['s','ii']
temperature=double(10000.0)
N_crit=s2->calc_crit_density(temperature=temperature)
print, 'Critical Densities:', N_crit

Critical Densities:       0.0000000       5007.8396       1732.8414
       1072685.0       2220758.1

All Ionic Level Information:

In [7]:

o3=obj_new('collision')
o3->set,['o','iii']
temperature=double(10000.0)
density=double(5000.0)
o3->print_ionic, temperature=temperature, density=density

Temperature =   10000.0 K
Density =    5000.0 cm-3

Level    Populations   Critical Densities
Level 1:   1.556E-01   0.000E+00
Level 2:   4.269E-01   4.908E+02
Level 3:   4.172E-01   3.419E+03
Level 4:   2.221E-04   6.853E+05
Level 5:   1.522E-08   2.547E+07

 2.597E-05  
     88.34um 
    (2-->1) 
 4.986E-23  

 0.000E+00   9.632E-05  
     32.66um      51.81um 
    (3-->1)     (3-->2) 
 0.000E+00   3.081E-22  

 2.322E-06   6.791E-03   2.046E-02  
   4932.60A    4960.29A    5008.24A 
    (4-->1)     (4-->2)     (4-->3) 
 4.153E-25   1.208E-21   3.604E-21  

 0.000E+00   2.255E-01   6.998E-04   1.685E+00  
   2315.58A    2321.67A    2332.12A    4364.45A 
    (5-->1)     (5-->2)     (5-->3)     (5-->4) 
 0.000E+00   5.875E-24   1.815E-26   2.335E-23  

H-beta emissivity: 1.239E-25 N(H+) Ne  [erg/s]

Recombination Unit¶

How to Use Recombination Unit

Recombination Unit has the API functions for plasma diagnostics and abundance analysis of recombination lines. Here are some examples of using Recombination Unit:

He+ Ionic Abundance:

In [8]:

he1=obj_new('recombination')
he1->set,['he','ii'] ; He I
temperature=double(10000.0)
density=double(5000.0)
he_i_4471_flux= 2.104
linenum=10; 4471.50
Abund_he_i=he1->calc_abundance(temperature=temperature, density=density, $
                              linenum=linenum, line_flux=he_i_4471_flux)
print, 'N(He^+)/N(H^+):', Abund_he_i

N(He^+)/N(H^+):     0.040848391

He++ Ionic Abundance:

In [9]:

he2=obj_new('recombination')
he2->set,['he','iii'] ; He II
temperature=double(10000.0)
density=double(5000.0)
he_ii_4686_flux = 135.833
Abund_he_ii=he2->calc_abundance(temperature=temperature, density=density, $
                                line_flux=he_ii_4686_flux)
print, 'N(He^2+)/N(H^+):', Abund_he_ii

N(He^2+)/N(H^+):      0.11228817

C++ Ionic Abundance:

In [10]:

c2=obj_new('recombination')
c2->set,['c','iii'] ; C II
temperature=double(10000.0)
density=double(5000.0)
wavelength=6151.43
c_ii_6151_flux = 0.028
Abund_c_ii=c2->calc_abundance(temperature=temperature, density=density, $
                              wavelength=wavelength, line_flux=c_ii_6151_flux)
print, 'N(C^2+)/N(H+):', Abund_c_ii

N(C^2+)/N(H+):   0.00063404650

C3+ Ionic Abundance:

In [11]:

c3=obj_new('recombination')
c3->set,['c','iv'] ; C III
temperature=double(10000.0)
density=double(5000.0)
wavelength=4647.42
c_iii_4647_flux = 0.107
Abund_c_iii=c3->calc_abundance(temperature=temperature, density=density, $
                                wavelength=wavelength, line_flux=c_iii_4647_flux)
print, 'N(C^3+)/N(H+):', Abund_c_iii

N(C^3+)/N(H+):   0.00017502840

N++ Ionic Abundance:

In [12]:

n2=obj_new('recombination')
n2->set,['n','iii'] ; N II
wavelength=4442.02
n_ii_4442_flux = 0.017
Abund_n_ii=n2->calc_abundance(temperature=temperature, density=density, $
                              wavelength=wavelength, line_flux=n_ii_4442_flux)
print, 'N(N^2+)/N(H+):', Abund_n_ii

N(N^2+)/N(H+):   0.00069297542

N3+ Ionic Abundance:

In [13]:

n3=obj_new('recombination')
n3->set,['n','iv'] ; N III
wavelength=4640.64
n_iii_4641_flux = 0.245
Abund_n_iii=n3->calc_abundance(temperature=temperature, density=density, $
                                wavelength=wavelength, line_flux=n_iii_4641_flux)
print, 'N(N^3+)/N(H+):', Abund_n_iii

N(N^3+)/N(H+):   6.3366174e-05

O++ Ionic Abundance:

In [14]:

o2=obj_new('recombination')
o2->set,['o','iii'] ; O II
wavelength=4613.68
o_ii_4614_flux = 0.009
Abund_o_ii=o2->calc_abundance(temperature=temperature, density=density, $
                              wavelength=wavelength, line_flux=o_ii_4614_flux)
print, 'N(O^2+)/N(H+):', Abund_o_ii

N(O^2+)/N(H+):    0.0018886330

Ne++ Ionic Abundance:

In [15]:

ne2=obj_new('recombination')
ne2->set,['ne','iii'] ; Ne II
wavelength=3777.14
ne_ii_3777_flux = 0.056
Abund_ne_ii=ne2->calc_abundance(temperature=temperature, density=density, $
                                wavelength=wavelength, line_flux=ne_ii_3777_flux)
print, 'N(Ne^2+)/N(H+):', Abund_ne_ii

N(Ne^2+)/N(H+):   0.00043376850

He I Emissivity:

In [16]:

he1=obj_new('recombination')
he1->set,['he','ii'] ; He I
temperature=double(10000.0)
density=double(5000.0)
linenum=10; 4471.50
emiss_he_i=he1->calc_emissivity(temperature=temperature, density=density, $
                                linenum=linenum)
print, 'He I Emissivity:', emiss_he_i

He I Emissivity:   6.3822830e-26

He II Emissivity:

In [17]:

he2=obj_new('recombination')
he2->set,['he','iii'] ; He II
temperature=double(10000.0)
density=double(5000.0)
emiss_he_ii=he2->calc_emissivity(temperature=temperature, density=density)
print, 'He II Emissivity:', emiss_he_ii

He II Emissivity:   1.4989134e-24

C II Emissivity:

In [18]:

c2=obj_new('recombination')
c2->set,['c','iii'] ; C II
temperature=double(10000.0)
density=double(5000.0)
wavelength=6151.43
emiss_c_ii=c2->calc_emissivity(temperature=temperature, density=density, $
                               wavelength=wavelength)
print, 'C II Emissivity:', emiss_c_ii

C II Emissivity:   5.4719511e-26

C III Emissivity:

In [19]:

c3=obj_new('recombination')
c3->set,['c','iv'] ; C III
temperature=double(10000.0)
density=double(5000.0)
wavelength=4647.42
emiss_c_iii=c3->calc_emissivity(temperature=temperature, density=density, $
                                wavelength=wavelength)
print, 'C III Emissivity:', emiss_c_iii

C III Emissivity:   7.5749632e-25

N II Emissivity:

In [20]:

n2=obj_new('recombination')
n2->set,['n','iii'] ; N II
wavelength=4442.02
emiss_n_ii=n2->calc_emissivity(temperature=temperature, density=density, $
                               wavelength=wavelength)
print, 'N II Emissivity:', emiss_n_ii

N II Emissivity:   3.0397397e-26

N III Emissivity:

In [21]:

n3=obj_new('recombination')
n3->set,['n','iv'] ; N III
wavelength=4640.64
emiss_n_iii=n3->calc_emissivity(temperature=temperature, density=density, $
                                wavelength=wavelength)
print, 'N III Emissivity:', emiss_n_iii

N III Emissivity:   4.7908644e-24

O II Emissivity:

In [22]:

o2=obj_new('recombination')
o2->set,['o','iii'] ; O II
wavelength=4613.68
emiss_o_ii=o2->calc_emissivity(temperature=temperature, density=density, $
                               wavelength=wavelength)
print, 'O II Emissivity:', emiss_o_ii

O II Emissivity:   5.9047319e-27

Ne II Emissivity:

In [23]:

ne2=obj_new('recombination')
ne2->set,['ne','iii'] ; Ne II
wavelength=3777.14
emiss_ne_ii=ne2->calc_emissivity(temperature=temperature, density=density, $
                                 wavelength=wavelength)
print, 'Ne II Emissivity:', emiss_ne_ii

Ne II Emissivity:   1.5996881e-25

Reddening Unit¶

How to Use Reddening Unit

Reddening Unit has the API functions for estimating logarithmic extinctions at H-beta and dereddening observed fluxes based on reddening laws and extinctions. Here are some examples of using Reddening Unit:

Reddening Law Function:

In [24]:

ext=obj_new('reddening')
wavelength=6563.0
R_V=3.1
fl=ext->redlaw(wavelength, rv=R_V, ext_law='GAL')
print, 'fl(6563):', fl

fl(6563):     -0.32013816

Galactic Reddening Law Function based on Seaton (1979), Howarth (1983), & CCM (1983):

In [25]:

ext=obj_new('reddening')
wavelength=6563.0
R_V=3.1
fl=ext->redlaw_gal(wavelength, rv=R_V)
print, 'fl(6563):', fl

fl(6563):     -0.32013816

Galactic Reddening Law Function based on Savage & Mathis (1979):

In [26]:

ext=obj_new('reddening')
wavelength=6563.0
fl=ext->redlaw_gal2(wavelength)
print, 'fl(6563):', fl

fl(6563):     -0.30925984

Reddening Law Function based on Cardelli, Clayton & Mathis (1989):

In [27]:

ext=obj_new('reddening')
wavelength=6563.0
R_V=3.1
fl=ext->redlaw_ccm(wavelength, rv=R_V)
print, 'fl(6563):', fl

fl(6563):     -0.29756615

Galactic Reddening Law Function based on Whitford (1958), Seaton (1977), & Kaler(1976):

In [28]:

ext=obj_new('reddening')
wavelength=6563.0
fl=ext->redlaw_jbk(wavelength)
print, 'fl(6563):', fl

fl(6563):     -0.33113684

Reddening Law Function based on Fitzpatrick & Massa (1990), Fitzpatrick (1999), Misselt (1999):

In [29]:

ext=obj_new('reddening')
wavelength=6563.0
R_V=3.1
fmlaw='AVGLMC'
fl=ext->redlaw_fm(wavelength, fmlaw=fmlaw, rv=R_V)
print, 'fl(6563):', fl

fl(6563):     -0.35053034

Reddening Law Function for the Small Magellanic Cloud:

In [30]:

ext=obj_new('reddening')
wavelength=6563.0
fl=ext->redlaw_smc(wavelength)
print, 'fl(6563):', fl

fl(6563):     -0.22659261

Reddening Law Function for the Large Magellanic Cloud:

In [31]:

ext=obj_new('reddening')
wavelength=6563.0
fl=ext->redlaw_lmc(wavelength)
print, 'fl(6563):', fl

fl(6563):     -0.30871187

Dereddening Relative Flux:

In [32]:

ext=obj_new('reddening')
wavelength=6563.0
m_ext=1.0
flux=1.0
ext_law='GAL'
R_V=3.1
flux_deredden=ext->deredden_relflux(wavelength, flux, m_ext, ext_law=ext_law, rv=R_V)
print, 'dereddened flux(6563)', flux_deredden

dereddened flux(6563)      0.47847785

Dereddening Absolute Flux:

In [33]:

ext=obj_new('reddening')
wavelength=6563.0
m_ext=1.0
flux=1.0
ext_law='GAL'
R_V=3.1
flux_deredden=ext->deredden_flux(wavelength, flux, m_ext, ext_law=ext_law, rv=R_V)
print, 'dereddened flux(6563)', flux_deredden

dereddened flux(6563)       4.7847785

In [ ]: