%0 Generic %1 vallini2013emission %A Vallini, Livia %A Gallerani, Simona %A Ferrara, Andrea %A Baek, Sunghye %D 2013 %K CII alma ir lines simulation %T FIR line emission from high redshift galaxies %U http://arxiv.org/abs/1305.2202 %X By combining high resolution, radiative transfer cosmological simulations of z~6 galaxies with a sub-grid multi-phase model of their interstellar medium we derive the expected intensity of several far infrared (FIR) emission lines (C II 158 micron, O I 63 micron, and N II 122 micron) for different values of the gas metallicity, Z. For Z = Z_sun the C II spectrum is very complex due to the presence of several emitting clumps of individual size < 3 kpc; the peak is displaced from the galaxy center by ~100 km/s. While the O I spectrum is also similarly displaced, the N II line comes predominantly from the central ionized regions of the galaxy. When integrated over ~500 km/s, the C II line flux is 185 mJy km/s; 95% of such flux originates from the cold (T~250 K) H I phase, and only 5% from the warm (T~5000 K) neutral medium. The O I and N II fluxes are ~6 and ~90 times lower than the C II one, respectively. By comparing our results with observations of Himiko, the most extended and luminous Lyman Alpha Emitter (LAE) at z = 6.6, we find that the gas metallicity in this source must be sub-solar. We conclude that the C II line from z~6 galaxies is detectable by the ALMA full array in 1.9 < t_ON < 7.7 hr observing time, depending on Z.

@misc{vallini2013emission, abstract = {By combining high resolution, radiative transfer cosmological simulations of z~6 galaxies with a sub-grid multi-phase model of their interstellar medium we derive the expected intensity of several far infrared (FIR) emission lines ([C II] 158 micron, [O I] 63 micron, and [N II] 122 micron) for different values of the gas metallicity, Z. For Z = Z_sun the [C II] spectrum is very complex due to the presence of several emitting clumps of individual size < 3 kpc; the peak is displaced from the galaxy center by ~100 km/s. While the [O I] spectrum is also similarly displaced, the [N II] line comes predominantly from the central ionized regions of the galaxy. When integrated over ~500 km/s, the [C II] line flux is 185 mJy km/s; 95% of such flux originates from the cold (T~250 K) H I phase, and only 5% from the warm (T~5000 K) neutral medium. The [O I] and [N II] fluxes are ~6 and ~90 times lower than the [C II] one, respectively. By comparing our results with observations of Himiko, the most extended and luminous Lyman Alpha Emitter (LAE) at z = 6.6, we find that the gas metallicity in this source must be sub-solar. We conclude that the [C II] line from z~6 galaxies is detectable by the ALMA full array in 1.9 < t_ON < 7.7 hr observing time, depending on Z.}, added-at = {2013-05-13T11:38:04.000+0200}, author = {Vallini, Livia and Gallerani, Simona and Ferrara, Andrea and Baek, Sunghye}, biburl = {https://www.bibsonomy.org/bibtex/2c5ebfeae0e968e7047906170f004214c/miki}, description = {[1305.2202] FIR line emission from high redshift galaxies}, interhash = {c9ad49cc76a040f7bdefc5a18525e8d4}, intrahash = {c5ebfeae0e968e7047906170f004214c}, keywords = {CII alma ir lines simulation}, note = {cite arxiv:1305.2202Comment: 7 pages, 3 figures, accepted for publication in MNRAS}, timestamp = {2013-05-13T11:38:14.000+0200}, title = {FIR line emission from high redshift galaxies}, url = {http://arxiv.org/abs/1305.2202}, year = 2013 }