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Table 1
List of parameters used for interpreting the stellar mass estimation.
| Parameter | Description |
|---|---|
| ma𝑔u, ma𝑔𝑔, ma𝑔r, ma𝑔i, ma𝑔ɀ, ma𝑔W1, ma𝑔W2, ma𝑔W3 | Optical and infrared magnitudes |
| ma𝑔u error, ma𝑔𝑔 error, ma𝑔r error, ma𝑔i error, ma𝑔ɀ error | Optical magnitude errors |
| ma𝑔W1 error, ma𝑔W2 error | Infrared magnitude errors (excluding the W3 band) |
| u – 𝑔, 𝑔 – r, r – i, i – ɀ, ɀ – W1, W1 – W2, W2 – W3 | Optical and infrared colors |
| nu, n𝑔, nr, ru, nɀ | Optical-band Sérsic indices |
| nu/n𝑔, n𝑔/nr, nr/ni, ni/nɀ | Cross-band ratios of Sérsic indices |
| [b/a]u, [b/a]𝑔, [b/a]r, [b/a]i, [b/a]ɀ | Optical-band inclinations based on exponential fits |
| [b/a]u/[b/a]𝑔, [b/a]𝑔/[b/a]r, [b/a]r/[b/a]h [b/a]i/[b/a]ɀ | Cross-band ratios of inclinations |
| R50,u, R50,𝑔, R50,r, R50,i, R50,ɀ | Optical-band Petrosian radii containing 50% of Petrosian fluxes |
| R90,u, R90,𝑔, R90,r, R90,i, R90,ɀ | Optical-band Petrosian radii containing 90% of Petrosian fluxes |
| R90,u/R50,u, R90,𝑔/R50,𝑔, R90,r/R50,r, R90,i/R50,i, R90,ɀ/R50,ɀ | Intra-band ratios of Petrosian radii |
| R90,u – R50,u, R90,𝑔 – R50,𝑔 R90,r – R50,r, R90,i – R50,i, R90,ɀ – R50,ɀ | Intra-band differences of Petrosian radii |
| R50,u/R50,𝑔, R50,𝑔/R50,r, R50,r/R50,i, R50,i/R50,ɀ | Cross-band ratios of Petrosian radii |
| R90,u/R90,𝑔, R90,𝑔/R90,r, R90,r/R90,i, R90,i/R90,ɀ | |
| R90,u/R50,𝑔, R90,𝑔/R50,r, R90,r/R50,i, R90,i/R50,ɀ | |
| ɀspec | Spectroscopic redshift (spec-ɀ) |
| log(SFR) | Star formation rate* |
| M* / Lu, M*/ L𝑔, M* /Lr, M*/ Li, M*/Lɀ | Optical-band mass-to-light ratios** |
| log(sSFR) | Specific star formation rate** |
| Metallicity | Metallicity** |
| Age | Stellarage ** |
| Dust τ1 | Optical depth of dust attenuation around young stars ** |
| Tlook–back | Look-back formation time** |
| PSFu, PSF𝑔, PSFr, PSFi, PSFɀ | FWHMs of optical-band point spread functions |
| E(B – V) | Galactic reddening *** |
Notes. (*)Following the method from Brinchmann et al. (2004) with aperture corrections as described in Salim et al. (2007). (**)Following the method from Conroy et al. (2009). (***)Based on the dust map from Schlegel et al. (1998).
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