Table 1.
Values of observable quantities for models of stellar populations including stripped stars.
| Time | log10 Q0, pop | log10 Q1, pop | log10Q2, pop | log10ξion, 0 | log10ξion, 1 | log10ξion, 2 | log10 Lν(1500 Å) | log10U | β |
|---|---|---|---|---|---|---|---|---|---|
| [Myr] | [s−1] | [s−1] | [s−1] | [erg−1 Hz] | [erg−1 Hz] | [erg−1 Hz] | [erg s−1 Hz−1] | ||
| Section | 5 | 5 | 5 | 6.1.1 | 6.1.1 | 6.1.1 | 6.1.1 | 6.1.2 | 6.2 |
| Co-eval stellar population (106 M⊙, Z = 0.014) | |||||||||
| 2 | 52.6 {−} (52.6) | 51.7 {−} (51.7) | 47.3 {−} (47.3) | 25.6 (25.6) | 24.7 (24.7) | 20.3 (20.3) | 27.0 (27.0) | −2.0 (−2.0) | −2.97 (−2.97) |
| 3 | 52.3 {−} (52.3) | 51.4 {−} (51.4) | 41.7 {−} (41.7) | 25.2 (25.2) | 24.3 (24.3) | 14.6 (14.6) | 27.1 (27.1) | −2.1 (−2.1) | −2.5 (−2.5) |
| 5 | 51.7 {−} (51.7) | 50.3 {−} (50.3) | 39.9 {−} (39.9) | 24.9 (24.9) | 23.5 (23.5) | 13.1 (13.1) | 26.8 (26.8) | −2.3 (−2.3) | −2.41 (−2.41) |
| 7 | 50.8 {−} (50.8) | 48.0 {−} (48.0) | 37.5 {−} (37.5) | 24.3 (24.3) | 21.5 (21.5) | 11.0 (11.0) | 26.5 (26.5) | −2.6 (−2.6) | −2.41 (−2.41) |
| 11 | 50.9 {50.9} (49.8) | 50.7 {50.7} (46.0) | 48.7 {48.7} (−) | 24.8 (23.6) | 24.5 (19.9) | 22.6 (−) | 26.2 (26.2) | −2.6 (−3.0) | −2.32 (−2.31) |
| 20 | 50.3 {50.3} (48.6) | 50.1 {50.1} (43.4) | 47.7 {47.7} (−) | 24.5 (22.8) | 24.3 (17.6) | 21.9 (−) | 25.8 (25.8) | −2.8 (−3.4) | −2.21 (−2.2) |
| 30 | 50.0 {49.9} (47.9) | 49.6 {49.6} (41.5) | 46.7 {46.7} (−) | 24.3 (22.3) | 24.0 (15.9) | 21.1 (−) | 25.6 (25.6) | −2.9 (−3.6) | −2.02 (−2.01) |
| 50 | 49.5 {49.5} (46.7) | 49.1 {49.1} (39.8) | 45.5 {45.5} (−) | 24.2 (21.4) | 23.8 (14.4) | 20.1 (−) | 25.3 (25.3) | −3.0 (−4.0) | −1.83 (−1.82) |
| 100 | 48.9 {48.9} (44.9) | 48.3 {48.3} (37.7) | 43.2 {43.2} (−) | 24.0 (19.9) | 23.4 (12.8) | 18.3 (−) | 24.9 (24.9) | −3.2 (−4.6) | −1.51 (−1.49) |
| 200 | 48.2 {48.2} (42.8) | 46.9 {46.9} (−) | 40.3 {40.3} (−) | 23.7 (18.3) | 22.4 (−) | 15.8 (−) | 24.5 (24.5) | −3.5 (−5.3) | −1.2 (−1.17) |
| 300 | 47.4 {47.4} (41.5) | 46.1 {46.1} (−) | 40.7 {40.7} (−) | 23.3 (17.4) | 22.0 (−) | 16.6 (−) | 24.1 (24.1) | −3.8 (−5.7) | −0.4 (−0.31) |
| 500 | 45.9 {45.9} (39.6) | 43.4 {43.4} (−) | 37.6 {37.6} (−) | 22.6 (16.3) | 20.1 (−) | 14.3 (−) | 23.3 (23.3) | −4.3 (−6.4) | 1.78 (2.54) |
| 800 | 44.7 {44.7} (36.7) | 41.6 {41.6} (−) | 34.5 {34.5} (−) | 22.8 (15.3) | 19.7 (−) | 12.6 (−) | 22.0 (21.4) | −4.6 (−7.3) | 4.5 (9.73) |
| 1000 | 44.2 {44.2} (35.7) | 40.8 {40.8} (−) | 33.8 {33.8} (−) | 22.5 (15.2) | 19.1 (−) | 12.1 (−) | 21.7 (20.5) | −4.8 (−7.6) | 4.8 (11.97) |
| Continuous star-formation (1 M⊙/year, Z = 0.014) | |||||||||
| 500 | 53.1 {51.9} (53.1) | 52.3 {51.6} (52.2) | 49.4 {49.3} (48.3) | 25.1 (25.1) | 24.4 (24.3) | 21.4 (20.4) | 28.0 (28.0) | −1.8 (−1.9) | −2.27 (−2.27) |
Notes. We use curly brackets to show values for only the stripped stars in the population and regular parentheses to show the values for single star populations (predicted by STARBURST99, Leitherer et al. 1999, 2010). The presented quantities are the following. First, the emission rates of H I-, He I-, and He II-ionizing photons, which we refer to as Q0, pop, Q1, pop, and Q2, pop, respectively (Sect. 5). Then, the production efficiencies of H I-, He I-, and He II-ionizing photons, labeled ξion, 0, ξion, 1, and ξion, 2, respectively (Sect. 6.1.1). For calculating the production efficiencies, the UV luminosity of the following column was used (see (2) and also Sect. 6.2). The next column displays the ionization parameter, U (Sect. 6.1.2), and the last column the slope of the UV continuum, β (Sect. 6.2). We assume the gas density to be nH = 100 cm−3 when calculating the ionization parameter. Snapshots for which no ionizing radiation was published are marked with “–”.
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