Spectral models for low-luminosity active galactic nuclei in LINERs

2016-10-25T21:56:47Z (GMT) by Rodrigo Nemmen
Spectral energy distribution data from the paper Nemmen et al. 2014, "Spectral models for low-luminosity active galactic nuclei in LINERs: the role of advection-dominated accretion and jets", published in MNRAS. This dataset includes the observational data and model SEDs published in the paper. 

For more info about the data, please open the README.md file included.

DOI for paper: 10.1093/mnras/stt2388

This notation applies to all files:

- Each filename begins with the name of the galaxy
- `ad` in the filename refers to an ADAF-dominated model
- `jd` in the filename refers to a jet-dominated model
- Extensions `.adaf`, `.ssd`, `.jet` or `.sum` refer to model SEDs
- Extension `.dat` refer to observational data
- Extension `.popstar` refer to the stellar population spectrum

# PDF files

The spectral energy distribution (SED) plots published in the paper, in the PDF format.

# Spectral models: accretion flow and jet

ASCII files with the models for each galactic nucleus, with two columns: 

1. log10(nu / Hz)
2. log10(nu * L_nu / erg/s)

The spectral model files end with one of the following extensions: `.adaf`, `.ssd`, `.jet` or `.sum`. Each extension refers to the physical component of the flow which is considered: ADAF (`adaf`), thin accretion disk (`ssd`), relativistic jet (`jet`) or the sum of all components (`sum`).

`ad` refers to an ADAF-dominated model, `jd` refers to a jet-dominated model.

# Spectral model: stellar population

The file `Sed_Mar05_Z_0.02_Age_10.00000000.popstar` corresponds to a stellar population spectrum based on the Bruzual & Charlot models which we plotted with every SED. We fit this spectrum to the optical-UV data for each galaxy, hence deriving the stellar mass.

# Observations

ASCII files containing the observed SED data points for each galaxy. These files end with extensions `.dat`.

Each column in he data files is the following:

1. Frequency (Hz)  
2. Observed nu*L_nu (erg/s)  
3. nu*L_nu (erg/s) 
4. Fractional Uncertainty (Variability) 
5. Upper limit? (1-yes, 0-no)

`NGC3998 old.dat` includes a high-frequency UV data point which as suggested by Mike Eracleous I ended up discarding. Please read the paper for more info.



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