Table 1.
Characteristics of the samples associated with the different spectral classes used in this analysis.
| Type | Lines or features | Sample | Observed by | N. of objects | References |
|---|---|---|---|---|---|
| [NeVI]7.7 μm | heterogeneous | ISO-SWS | 8 | Sturm et al. (2002) | |
| MIR lines in the 10–35 μm range | 12MGS | Spitzer-IRS HR | 88 | Tommasin et al. (2008, 2010) | |
| AGN | including H2 rotational lines | ||||
| PAH features | 12MGS | Spitzer-IRS LR | 103 | Wu et al. (2009) | |
| FIR lines in the 50–205 μm range | heterogeneous | Herschel-PACS and SPIRE | 149 | Fernández-Ontiveros et al. (2016) | |
| MIR lines in the 10–35 μm range | GOALS sample | 153 | Inami et al. (2013) | ||
| + heterogeneous | Spitzer-IRS HR | 10 | Bernard-Salas et al. (2009) | ||
| + heterogeneous | 28 | Goulding & Alexander (2009) | |||
| H2 rotational lines | GOALS sample | 153 | Stierwalt et al. (2014) | ||
| SFG | + heterogeneous | Spitzer-IRS HR | 10 | Bernard-Salas et al. (2009) | |
| + heterogeneous | 28 | Goulding & Alexander (2009) | |||
| PAH features | GOALS sample | Spitzer-IRS LR | 179 | Stierwalt et al. (2014) | |
| + heterogeneous | 12 | Brandl et al. (2006) | |||
| FIR lines in the 50–205 μm range | GOALS sample | Herschel-PACS | 153 | Díaz-Santos et al. (2017) | |
| + heterogeneous | Herschel-PACS and SPIRE | 20 | Fernández-Ontiveros et al. (2016) | ||
| + heterogeneous | ISO-LWS | 23 | Negishi et al. (2001) | ||
| LMG | MIR lines in the 10–35 μm range | DGS | Spitzer-IRS HR and LR | 40 | Cormier et al. (2015) |
| FIR lines in the 50–158 μm range | DGS | Herschel-PACS | 40 | Cormier et al. (2015) | |
Notes. For each class we list: the different lines and features considered, the samples (heterogeneous indicates that the sources do not belong to a specific well-defined sample of galaxies), the facilities and instruments used in the observations, the number of objects in each sample, and the corresponding references.
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