Table 2.
Stellar population synthesis results from BAGPIPES and Prospector.
| Parameter | BAGPIPES(delayed) | BAGPIPES(exp) | Prospector |
|---|---|---|---|
| z_ml | 4.035 | 4.060 | 3.885 |
| z_p | 4.011/4.045/4.079 | 4.013/4.048/4.080 | 3.878/3.908/3.951 |
| mass_p (log(M*/M⊙)) | 10.14/10.17/10.21 | 10.12/10.16/10.20 | 9.81/9.93/10.03 |
| SFR_p (M⊙ yr−1) | 59.27/62.75/70.58 | 53.58/63.25/73.91 | 30.23/36.63/43.37 |
| log(sSFR_p (yr−1)) | −8.48/−8.37/−8.29 | −8.47/−8.36/−8.25 | −8.54/−8.35/−8.19 |
| Av_p | 0.84/0.89/0.94 | 0.84/0.89/0.94 | |
| dust2 (τ) | 0.34/0.40/0.47 | ||
| MWA_p (Gyr) | 0.159/0.199/0.265 | 0.121/0.157/0.205 | 0.176/0.316/0.491 |
Notes. This table shows the SPS properties of Alaknanda derived from fitting two SFHs from BAGPIPES (delayed exponentially decaying SFH and exponentially decaying SFH) and Prospector SPS values from UNCOVER DR4. z_ml is the maximum likelihood redshift obtained by SED modeling. In other rows, we show, in order, the 16th/50th/84th output posterior percentiles of photometric redshift, stellar mass, SFR, logarithm of sSFR, dust extinction (Av), optical depth (τ) and mass-weighted age (MWA). Av and dust2 are BAGPIPES and Prospector outputs, respectively and both are measures of the dust content where Av is the absolute attenuation in the V-band and dust2 (τ) is the optical depth of the diffuse dust.
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