A spatially resolved study of ionized regions in galaxies at different ...
A spatially resolved study of ionized regions in galaxies at different ... A spatially resolved study of ionized regions in galaxies at different ...
β[H 84 3 • IFS of a GEHR in NGC 6946 ◦A−1 ) s−1 Flux (erg cm−2 1e−15 2.4 2.0 1.6 1.2 0.8 0.4 [OII]3727 Knot C 4000 4500 5000 5500 6000 6500 1e−15 HδHγ OIII]4959 [OIII]5007 HeI 5876 [SII] 6717,6731 Hα ◦A−1 ) 1.5 s−1 Flux (erg cm−2 1.0 0.5 [ArIII] 7136 [OII] 7319,7330 [SIII]9069 0.0 7000 7500 8000 8500 9000 Wavelength (◦A) 1e−15 1.0 ◦A−1 ) s−1 Flux (erg cm−2 0.8 0.6 0.4 0.2 [OII]3727 Knot D 0.0 4000 4500 5000 5500 6000 6500 1e−16 Hγ Hβ[OIII]4959 [OIII]5007 HeI 5876 [SII] 6717,6731 Hα ◦A−1 ) s−1 Flux (erg cm−2 2.4 1.8 1.2 0.6 [ArIII] 7136 0.0 7000 7500 8000 8500 9000 Wavelength (◦A) [SIII]9069 Figure 3.24: Blue and red spectra for the knots C and D.
3.4. Results 85 ◦A−1 ) s−1 Flux (erg cm−2 1e−14 2.8 2.4 2.0 1.6 1.2 0.8 0.4 [OII]3727 PPak-field 4000 4500 5000 5500 6000 6500 1e−14 HδHγ Hβ[OIII]4959 [OIII]5007 HeI 5876 [SII] 6717,6731 Hα ◦A−1 ) s−1 Flux (erg cm−2 1.6 1.4 1.2 1.0 0.8 0.6 0.4 0.2 0.0 7000 7500 8000 8500 9000 Wavelength (◦A) [ArIII] 7136 [OII] 7319,7330 [SIII]9069 Figure 3.25: Blue and red spectra for the whole PPak-field. pointing of the knots A and B, and C and D, respectively. Their ratios, as compared with the ones obtained from the mosaic exposure are, again, in good agreement. Thus, we only show the measured line intensities coming from the first pointing exposure. In Tables 3.5 and 3.6 the total reddening-corrected Hβ intensity (I tot (Hβ)) measured in the mosaic is also given. As it can be appreciated, the total flux is between a factor of 2 or 3 higher than the value measured in the one single pointing. The Hβ flux of the emission knots amounts to about 50% of the total PPak field-ofview flux, with knot A, B, C, and D contributing 38%, 2%, 7%, and 3% to the total flux, respectively. Knot A is the brightest of them and provides 75% of the combined flux from the four knots. Electron densities and temperatures The physical conditions of the ionized gas, including electron temperature and electron density, have been derived using the five-level statistical equilibrium atom approximation in the task temden of the STSDAS package of the software IRAF. For details of the equations involved, the reader is referred to Appendix B. We have taken as sources of error the uncertainties associated with the measurement of the emission-line fluxes and the reddening
- Page 54 and 55: 34 2 • The star formation history
- Page 56 and 57: 36 2 • The star formation history
- Page 58 and 59: 38 2 • The star formation history
- Page 60 and 61: 40 3 • IFS of a GEHR in NGC 6946
- Page 62 and 63: 42 3 • IFS of a GEHR in NGC 6946
- Page 64 and 65: 44 3 • IFS of a GEHR in NGC 6946
- Page 66 and 67: 46 3 • IFS of a GEHR in NGC 6946
- Page 68 and 69: 48 3 • IFS of a GEHR in NGC 6946
- Page 70 and 71: 50 3 • IFS of a GEHR in NGC 6946
- Page 72 and 73: 52 3 • IFS of a GEHR in NGC 6946
- Page 74 and 75: 54 3 • IFS of a GEHR in NGC 6946
- Page 76 and 77: 56 3 • IFS of a GEHR in NGC 6946
- Page 78 and 79: 58 3 • IFS of a GEHR in NGC 6946
- Page 80 and 81: 60 3 • IFS of a GEHR in NGC 6946
- Page 82 and 83: 62 3 • IFS of a GEHR in NGC 6946
- Page 84 and 85: 64 3 • IFS of a GEHR in NGC 6946
- Page 86 and 87: 66 3 • IFS of a GEHR in NGC 6946
- Page 88 and 89: 68 3 • IFS of a GEHR in NGC 6946
- Page 90 and 91: 70 3 • IFS of a GEHR in NGC 6946
- Page 92 and 93: 72 3 • IFS of a GEHR in NGC 6946
- Page 94 and 95: 74 3 • IFS of a GEHR in NGC 6946
- Page 96 and 97: 76 3 • IFS of a GEHR in NGC 6946
- Page 98 and 99: 78 3 • IFS of a GEHR in NGC 6946
- Page 100 and 101: 80 3 • IFS of a GEHR in NGC 6946
- Page 102 and 103: 82 3 • IFS of a GEHR in NGC 6946
- Page 106 and 107: 86 3 • IFS of a GEHR in NGC 6946
- Page 108 and 109: 88 3 • IFS of a GEHR in NGC 6946
- Page 110 and 111: 90 3 • IFS of a GEHR in NGC 6946
- Page 112 and 113: 92 3 • IFS of a GEHR in NGC 6946
- Page 114 and 115: 94 3 • IFS of a GEHR in NGC 6946
- Page 116 and 117: 96 3 • IFS of a GEHR in NGC 6946
- Page 118 and 119: 98 3 • IFS of a GEHR in NGC 6946
- Page 120 and 121: 100 3 • IFS of a GEHR in NGC 6946
- Page 122 and 123: 102 3 • IFS of a GEHR in NGC 6946
- Page 124 and 125: 104 3 • IFS of a GEHR in NGC 6946
- Page 126 and 127: 106 4 • Long-slit spectrophotomet
- Page 128 and 129: 108 4 • Long-slit spectrophotomet
- Page 130 and 131: 110 4 • Long-slit spectrophotomet
- Page 132 and 133: 112 4 • Long-slit spectrophotomet
- Page 134 and 135: 114 4 • Long-slit spectrophotomet
- Page 136 and 137: Hδ 116 4 • Long-slit spectrophot
- Page 138 and 139: 118 4 • Long-slit spectrophotomet
- Page 140 and 141: 120 4 • Long-slit spectrophotomet
- Page 142 and 143: 122 4 • Long-slit spectrophotomet
- Page 144 and 145: Table 4.4 continued SDSS J1657 Knot
- Page 146 and 147: 126 4 • Long-slit spectrophotomet
- Page 148 and 149: 128 4 • Long-slit spectrophotomet
- Page 150 and 151: 130 4 • Long-slit spectrophotomet
- Page 152 and 153: 132 4 • Long-slit spectrophotomet
β[H<br />
84 3 • IFS <strong>of</strong> a GEHR <strong>in</strong> NGC 6946<br />
◦A−1<br />
)<br />
s−1<br />
Flux (erg cm−2<br />
1e−15<br />
2.4<br />
2.0<br />
1.6<br />
1.2<br />
0.8<br />
0.4<br />
[OII]3727<br />
Knot C<br />
4000 4500 5000 5500 6000 6500<br />
1e−15<br />
HδHγ<br />
OIII]4959<br />
[OIII]5007<br />
HeI 5876<br />
[SII] 6717,6731<br />
Hα<br />
◦A−1<br />
)<br />
1.5<br />
s−1<br />
Flux (erg cm−2<br />
1.0<br />
0.5<br />
[ArIII] 7136<br />
[OII] 7319,7330<br />
[SIII]9069<br />
0.0<br />
7000 7500 8000 8500 9000<br />
Wavelength (◦A)<br />
1e−15<br />
1.0<br />
◦A−1<br />
)<br />
s−1<br />
Flux (erg cm−2<br />
0.8<br />
0.6<br />
0.4<br />
0.2<br />
[OII]3727<br />
Knot D<br />
0.0<br />
4000 4500 5000 5500 6000 6500<br />
1e−16<br />
Hγ<br />
Hβ[OIII]4959<br />
[OIII]5007<br />
HeI 5876<br />
[SII] 6717,6731<br />
Hα<br />
◦A−1<br />
)<br />
s−1<br />
Flux (erg cm−2<br />
2.4<br />
1.8<br />
1.2<br />
0.6<br />
[ArIII] 7136<br />
0.0<br />
7000 7500 8000 8500 9000<br />
Wavelength (◦A)<br />
[SIII]9069<br />
Figure 3.24: Blue and red spectra for the knots C and D.
Change language