I'm calculating dust corrected luminosities for stellar particles using the model(C) in the paper Nelson+19. But for subhalos without any gas (ex. subhalo id 1572823 in snapshot 99 in tng300-1) do you know how should I implement dust correction model? Thanks
Best,
Hasitha
Dylan Nelson
7 Jan '22
If a subhalo has no gas, then N_H = 0 (in Eqn. 4) by definition. So the "resolved dust" component of Model C would be zero. Note however that this component is in addition to the "unresolved dust" component from Model B, which would still apply (although, if a subhalo has no gas, it likely has no stars younger than 10 Myr, i.e. only the second line of Eqn. 1 would apply).
However, keep in mind that it is somewhat impossible that a subhalo actually has no gas (along a given line of sight). If e.g. you are considering a satellite subhalo, then it is embedded within the gas of its parent FoF halo, which could be used for this calculation. Even if you are considering a central subhalo without gas (e.g. likely a backsplash galaxy), then there would be "IGM" along the line of sight. In both cases, however, it is likely that the resulting N_H would be vanishingly small, and thus that the "resolved dust" contribution would be negligible.
Hi,
I'm calculating dust corrected luminosities for stellar particles using the model(C) in the paper Nelson+19. But for subhalos without any gas (ex. subhalo id 1572823 in snapshot 99 in tng300-1) do you know how should I implement dust correction model? Thanks
Best,
Hasitha
If a subhalo has no gas, then
N_H = 0(in Eqn. 4) by definition. So the "resolved dust" component of Model C would be zero. Note however that this component is in addition to the "unresolved dust" component from Model B, which would still apply (although, if a subhalo has no gas, it likely has no stars younger than 10 Myr, i.e. only the second line of Eqn. 1 would apply).However, keep in mind that it is somewhat impossible that a subhalo actually has no gas (along a given line of sight). If e.g. you are considering a satellite subhalo, then it is embedded within the gas of its parent FoF halo, which could be used for this calculation. Even if you are considering a central subhalo without gas (e.g. likely a backsplash galaxy), then there would be "IGM" along the line of sight. In both cases, however, it is likely that the resulting
N_Hwould be vanishingly small, and thus that the "resolved dust" contribution would be negligible.