%0 Generic %1 gong2016intensity %A Gong, Yan %A Cooray, Asantha %A Silva, Marta B. %A Zemcov, Michael %A Feng, Chang %A Santos, Mario G. %A Dore, Olivier %A Chen, Xuelei %D 2016 %K intensity line mapping %T Intensity mapping of H-alpha, H-beta, OII and OIII lines at z<5 %U http://arxiv.org/abs/1610.09060 %X Intensity mapping is now becoming a useful tool to study the large-scale structure of the universe through spatial variations in the integrated emission from galaxies and the intergalactic medium. We study intensity mapping of the H-alpha6563A, OIII5007A, OII3727A and H-beta4861A lines at 0.8<z<5.2. The mean intensities of these four emission lines are estimated using the observed luminosity functions (LFs), cosmological simulations, and the star formation rate density (SFRD) derived from observations at z<5. We calculate the intensity power spectra and consider the foreground contamination of other lines at lower redshifts. We use the proposed NASA small explorer SPHEREx (the Spectro-Photometer for the History of the Universe, Epoch of Reionization, and Ices Explorer) as a case study for the detectability of the intensity power spectra of the four emission lines. We also investigate the cross correlation with the 21-cm line probed by CHIME (the Canadian Hydrogen Intensity Mapping Experiment), Tianlai experiment and SKA (the Square Kilometer Array) at 0.8<z<2.4. We find both the auto and cross power spectra can be well measured for the four lines at z<3, especially for the H-alpha, OIII and OII lines. Finally, we estimate the constraint on the SFRD from intensity mapping, and find we can reach accuracy higher than 7% at z<4, which is better than usual measurements using the LFs of galaxies.

@misc{gong2016intensity, abstract = {Intensity mapping is now becoming a useful tool to study the large-scale structure of the universe through spatial variations in the integrated emission from galaxies and the intergalactic medium. We study intensity mapping of the H-alpha6563A, [OIII]5007A, [OII]3727A and H-beta4861A lines at 0.8<z<5.2. The mean intensities of these four emission lines are estimated using the observed luminosity functions (LFs), cosmological simulations, and the star formation rate density (SFRD) derived from observations at z<5. We calculate the intensity power spectra and consider the foreground contamination of other lines at lower redshifts. We use the proposed NASA small explorer SPHEREx (the Spectro-Photometer for the History of the Universe, Epoch of Reionization, and Ices Explorer) as a case study for the detectability of the intensity power spectra of the four emission lines. We also investigate the cross correlation with the 21-cm line probed by CHIME (the Canadian Hydrogen Intensity Mapping Experiment), Tianlai experiment and SKA (the Square Kilometer Array) at 0.8<z<2.4. We find both the auto and cross power spectra can be well measured for the four lines at z<3, especially for the H-alpha, [OIII] and [OII] lines. Finally, we estimate the constraint on the SFRD from intensity mapping, and find we can reach accuracy higher than 7% at z<4, which is better than usual measurements using the LFs of galaxies.}, added-at = {2016-10-31T09:31:18.000+0100}, author = {Gong, Yan and Cooray, Asantha and Silva, Marta B. and Zemcov, Michael and Feng, Chang and Santos, Mario G. and Dore, Olivier and Chen, Xuelei}, biburl = {https://www.bibsonomy.org/bibtex/25a2daac7c12bc6966aa9a4defabc5eb3/miki}, description = {[1610.09060] Intensity mapping of H-alpha, H-beta, [OII] and [OIII] lines at z&lt;5}, interhash = {d3c542af2078043f326e51c297c08731}, intrahash = {5a2daac7c12bc6966aa9a4defabc5eb3}, keywords = {intensity line mapping}, note = {cite arxiv:1610.09060Comment: 14 pages, 9 figures, 4 tables}, timestamp = {2016-10-31T09:31:18.000+0100}, title = {Intensity mapping of H-alpha, H-beta, [OII] and [OIII] lines at z<5}, url = {http://arxiv.org/abs/1610.09060}, year = 2016 }