Spectral models for low-luminosity active galactic nuclei in LINERs NemmenRodrigo 2016 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. <div><br></div><div>For more info about the data, please open the README.md file included.</div><div><br></div><div>DOI for paper: 10.1093/mnras/stt2388</div><div><br></div><div><div>This notation applies to all files:</div><div><br></div><div>- Each filename begins with the name of the galaxy</div><div>- `ad` in the filename refers to an ADAF-dominated model</div><div>- `jd` in the filename refers to a jet-dominated model</div><div>- Extensions `.adaf`, `.ssd`, `.jet` or `.sum` refer to model SEDs</div><div>- Extension `.dat` refer to observational data</div><div>- Extension `.popstar` refer to the stellar population spectrum</div><div><br></div><div><br></div><div># PDF files</div><div><br></div><div>The spectral energy distribution (SED) plots published in the paper, in the PDF format.</div><div><br></div><div># Spectral models: accretion flow and jet</div><div><br></div><div>ASCII files with the models for each galactic nucleus, with two columns: </div><div><br></div><div>1. log10(nu / Hz)</div><div>2. log10(nu * L_nu / erg/s)</div><div><br></div><div>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`).</div><div><br></div><div>`ad` refers to an ADAF-dominated model, `jd` refers to a jet-dominated model.</div><div><br></div><div># Spectral model: stellar population</div><div><br></div><div>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.</div><div><br></div><div># Observations</div><div><br></div><div>ASCII files containing the observed SED data points for each galaxy. These files end with extensions `.dat`.</div><div><br></div><div>Each column in he data files is the following:</div><div><br></div><div>1. Frequency (Hz)  </div><div>2. Observed nu*L_nu (erg/s)  </div><div>3. nu*L_nu (erg/s) </div><div>4. Fractional Uncertainty (Variability) </div><div>5. Upper limit? (1-yes, 0-no)</div><div><br></div><div>`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.</div></div><div><br></div>