mirror of
https://asciireactor.com/otho/cloudy-agn.git
synced 2025-10-31 20:48:05 +00:00
67 lines
3.3 KiB
Plaintext
67 lines
3.3 KiB
Plaintext
This regards the multiplets about which we currently obtain information from Cloudy, indexed by TOTL. Specifically, the new way these are treated in Cloudy 15.
|
|
|
|
It appears C15 adds a new category of emission lines after "molecules" called "blends". It seems this has largely replaced the TOTL lines we are used to seeing, but there are some exceptions. For example, there is no longer any TOTL line around N III 1750. Here is the readout:
|
|
|
|
Inwd 860.205A 4.359 0.0033
|
|
N 3 1748.65A 6.367 0.3378
|
|
Inwd 1748.65A 6.150 0.2047
|
|
N 3 1753.99A 6.381 0.3489
|
|
Inwd 1753.99A 6.165 0.2118
|
|
N 3 1746.82A 5.099 0.0182
|
|
Inwd 1746.82A 4.866 0.0107
|
|
N 3 1752.16A 5.935 0.1250
|
|
Inwd 1752.16A 5.709 0.0742
|
|
N 3 1749.67A 6.719 0.7598
|
|
Inwd 1749.67A 6.519 0.4794
|
|
N 3 989.799A 6.761 0.8374
|
|
|
|
Instead, presumably, there is a blend line near the relevant wavelength. listed in the blends section. Blended regions can also be accompanied by an inward component. For the N III example I found
|
|
|
|
Blnd 1750.00A 7.040 1.5897
|
|
|
|
In the blends section, Cloudy also outputs lines with more specific labels, often alongside similarly-located blends. For example:
|
|
|
|
Blnd 1657.00A 6.418 0.3794
|
|
C 1R 1656.00A 6.361 0.3329
|
|
Blnd 2326.00A 5.748 0.0811
|
|
Blnd 1335.00A 7.737 7.9093
|
|
C 2R 1335.00A 7.690 7.1108
|
|
C 2P 3920.00A 4.311 0.0030
|
|
Blnd 6580.00A 5.257 0.0262
|
|
|
|
My guess is these are physically-modelled multiplets displayed alongside some sort of continuum blending. I read in the "A Multiplet Table of Astrophysical Interest" about a certain type of blending, but the document is huge and I didn't delve far into it; besides, this could be another type of blend altogether, given what I know.
|
|
|
|
So, I'm not sure how we might make sense of a blend line alongside the thought of the TOTL in C13 (which is that the TOTL should represent the sum of the multiplet values). In the N III example, the sum of the quintuplet's values does match the blend value. For C I, however, it does not.
|
|
|
|
C 1 1656.27A 5.388 0.0354
|
|
Inwd 1656.27A 5.380 0.0348
|
|
C 1 1656.93A 5.390 0.0356
|
|
Inwd 1656.93A 5.374 0.0343
|
|
C 1 1657.01A 5.506 0.0465
|
|
Inwd 1657.01A 5.520 0.0480
|
|
C 1 1657.38A 5.354 0.0327
|
|
Inwd 1657.38A 5.329 0.0310
|
|
C 1 1657.91A 5.390 0.0356
|
|
Inwd 1657.91A 5.374 0.0343
|
|
C 1 1658.12A 5.417 0.0379
|
|
Inwd 1658.12A 5.406 0.0369
|
|
|
|
(Sum = .2237)
|
|
|
|
Blnd 1657.00A 6.418 0.3794
|
|
C 1R 1656.00A 6.361 0.3329
|
|
|
|
|
|
The only places I found where TOTL lines still exist are in the general properties (i.e. TOTL 4861) and the He-like iso-sequence. For example,
|
|
|
|
TOTL 29.0840A 6.811 0.9375
|
|
N 6 29.0840A 6.309 0.2957
|
|
Inwd 29.0840A 6.528 0.4886
|
|
N 6 29.0815A 3.848 0.0010
|
|
Inwd 29.0815A 4.062 0.0017
|
|
N 6 28.7870A 5.941 0.1266
|
|
Inwd 28.7870A 6.062 0.1672
|
|
|
|
|
|
This example does not sum properly, either. So, I really have no idea what's going on, here. But, as we mostly decided before, it shouldn't matter much for our current purposes.
|