Table 4
Selected variable SFH models, with physical properties derived from fitting with the BC03 library.
| ID | Model |
|
A V | Age [Gyr] | M⋆ [1010M⊙] | Lbol [1011L⊙] | SFRBC[M⊙ yr-1] |
|
|
|||||||
| A68/C0∗ | Calz+neb+decl | 0.72 | 1.6 (1.1−2.0) | 0.18 (0.05−1.4) | 2.1 (0.9−3.9) | 2.97 (1.3−7.8) | 35.5 (13.9−117.5) |
| A68/C0 | SMC+decl | 1.02 | 0.5 (0.4−0.7) | 3.4 (2.3−3.5) | 4.1 (3.3−4.8) | 0.6 (0.4−1.0) | 10.6 (8.1−16.1) |
| A68/h7∗ | Calz+neb+decl | 3.67 | 0.3 (0.2−1.4) | 0.36 (0.18−0.36) | 18.5 (17.2−21.8) | 1.71 (0.98−24.7) | 3.6 (2.8−174.1) |
| A68/h7 | SMC+neb+decl | 1.86 | 0.5 (0.4−0.6) | 0.36 (0.25−2.0) | 17.4 (13.6−27.4) | 6.35 (3.8−9.4) | 73.8 (20.1−155.8) |
| A68/HLS115∗ | Calz+neb+decl | 1.65 | 1.7 (1.5−1.9) | 0.09 (0.05− 0.13) | 1.0(0.7−1.5) | 4.4 (2.9−6.1) | 57.8 (30.3−98.5) |
| A68/HLS115 | SMC+neb+decl | 2.5 | 0.5 (0.5−0.6) | 3.5 (2.6−3.5) | 3.0 (2.7−3.6) | 0.6 (0.5−0.8) | 10.9 (9.1−13.6) |
| A68/nn4∗ | SMC+decl | 0.85 | 1.9 (1.8−2.0) | 0.033 (0.03−0.039) | 5.7(5.3−6.2) | 64.3 (57.3−73.8) | 1265 (1069−1518) |
| A68/nn4 | Calz+neb+decl | 4.68 | 2.8 (2.2− 2.9) | 0.017 (0.013−0.18) | 4.9 (4.4−18.9) | 109 (35.3−131) | 2400 (343.8−3183) |
| MACS0451∗ | Calz+neb+decl | 6.3 | 1.1 (1.0−1.1) | 0.015 (0.013−0.02) | 0.15 (0.15−0.16) | 3.7 (3.1−3.8) | 101.6 (82.3−105.1) |
| MACS0451 | SMC+neb+decl | 8.5 | 0.2 (0.2−0.2) | 0.72 (0.72−0.72) | 0.78 (0.77−0.85) | 0.42 (0.42−0.43) | 13.4 (12.9−13.6) |
| cB58∗ | SMC+neb+decl | 1.57 | 0.3 (0.3−0.4) | 0.09 (0.05−0.09) | 0.63 (0.4−0.72) | 1.63 (1.5−2.65) | 37.9 (30.9−65.1) |
| cB58 | Calz+neb+decl | 2.86 | 0.5 (0.3−0.6) | 0.128 (0.09−0.18) | 1.03 (0.8−1.3) | 1.36 (0.62−2.05) | 21.7(9.8−413) |
| Cosmic Eye∗ | Calz+neb†+decl | 1.35 | 0.6 (0.5−0.7) | 0.18 (0.18−0.25) | 4.03(3.6−4.6) | 3.83(2.84−5.04) | 57.1 (47.8−85.8) |
| Cosmic Eye | Calz+neb+decl | 1.52 | 0.6 (0.5−0.7) | 0.18 (0.13−0.25) | 3.86 (3.4−4.4) | 3.92 (2.9−5.0) | 66.1 (47.6−84.7) |
| Cosmic Eye | SMC+neb+decl | 1.65 | 0.2 (0.2−0.2) | 1.7 (1.7−2.0) | 6.68 (6.3−7.2) | 1.56 (1.52−1.59) | 47.3 (46−48.8) |
Notes. Values are corrected for lensing. Lbol stands for the absorbed luminosity in the [912 Å−3 μm] for the given extinction, and is used as a proxy to predict LIR. In parenthesis are given the values for the 68% confidence levels derived from our MC runs. Asterisks show the favored scenarios, in general they coincide with the lowest , except for h7, in which case our considerations discussed in Sect. 5.1.2 made us favor the Calzetti-based solution. The results listed for MACS0451 come from the integrated photometry of the entire arc, and a scaling factor of 0.4 can be applied to estimate the properties of the northern part separately (see Sect. 5.1.5). We do not show results of our rising SFH models as they do not provide more insight to our sample nor better fits.
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