Spectral models for low-luminosity active galactic nuclei in LINERs

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. <br>For more info about the data, please open the README.md file included.<br>DOI for paper: 10.1093/mnras/stt2388<br>This notation applies to all files:<br>- 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<br><br># PDF files<br>The spectral energy distribution (SED) plots published in the paper, in the PDF format.<br># Spectral models: accretion flow and jet<br>ASCII files with the models for each galactic nucleus, with two columns: <br>1. log10(nu / Hz)2. log10(nu * L_nu / erg/s)<br>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`).<br>`ad` refers to an ADAF-dominated model, `jd` refers to a jet-dominated model.<br># Spectral model: stellar population<br>The file `Sed_Mar05_Z_0.02_Age_10.00000000.popstar` corresponds to a stellar population spectrum based on the Bruzual &amp; 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.<br># Observations<br>ASCII files containing the observed SED data points for each galaxy. These files end with extensions `.dat`.<br>Each column in he data files is the following:<br>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)<br>`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.<br>