@article{karoumpis_cii_2021,
	title = {[{CII}] line intensity mapping the epoch of reionization with the {Prime}-{Cam} on {FYST}},
	url = {http://arxiv.org/abs/2111.12847},
	abstract = {We predict the three-dimensional intensity power spectrum (PS) of the [CII] 158\${\textbackslash},{\textbackslash}mu\$m line throughout the epoch of (and post) reionization at redshifts from \${\textbackslash}approx\$ 3.5 to 8. We study the detectability of the PS in a line intensity mapping (LIM) survey with the Fred Young Submillimeter Telescope (FYST). We created mock [CII] tomographic scans in redshift bins at \$z{\textbackslash}approx\$ 3.7, 4.3, 5.8, and 7.4 using the Illustris TNG300-1 \${\textbackslash}Lambda\$CDM simulation and adopting a relation between the star formation activity and the [CII] luminosity (\$L\_\{[CII]\}\$) of galaxies. A star formation rate (SFR) was assigned to a dark matter halo in the Illustris simulation in two ways: (i) we adopted the SFR computed in the Illustris simulation and, (ii) we matched the abundance of the halos with the SFR traced by the observed dust-corrected ultraviolet luminosity function of high-redshift galaxies. The \$L\_\{[CII]\}\$ is related to the SFR from a semi-analytic model of galaxy formation, from a hydrodynamical simulation of a high-redshift galaxy, or from a high-redshift [CII] galaxy survey. The [CII] intensity PS was computed from mock tomographic scans to assess its detectability with the anticipated observational capability of the FYST. The amplitude of the predicted [CII] intensity power spectrum varies by more than a factor of 10, depending on the choice of the halo-to-galaxy SFR and the SFR-to-\$L\_\{[CII]\}\$ relations. In the planned \$4{\textasciicircum}\{{\textbackslash}circ\} {\textbackslash}times 4{\textasciicircum}\{{\textbackslash}circ\}\$ FYST LIM survey, we expect a detection of the [CII] PS up to \$z {\textbackslash}approx\$ 5.8, and potentially even up to \$z {\textbackslash}approx \$ 7.4. The design of the envisioned FYST LIM survey enables a PS measurement not only in small ({\textless}10 Mpc) shot noise-dominated scales, but also in large ({\textgreater}50 Mpc) clustering-dominated scales making it the first LIM experiment that will place constraints on the SFR-to-\$L\_\{[CII]\}\$ and the halo-to-galaxy SFR relations simultaneously.},
	urldate = {2021-12-17},
	journal = {arXiv:2111.12847 [astro-ph]},
	author = {Karoumpis, C. and Magnelli, B. and Romano-Díaz, E. and Haslbauer, M. and Bertoldi, F.},
	month = nov,
	year = {2021},
	note = {arXiv: 2111.12847},
	keywords = {Astrophysics - Astrophysics of Galaxies},
}

{"_id":"Yj9fCvZzwz5E4v7bM","bibbaseid":"karoumpis-magnelli-romanodaz-haslbauer-bertoldi-ciilineintensitymappingtheepochofreionizationwiththeprimecamonfyst-2021","author_short":["Karoumpis, C.","Magnelli, B.","Romano-Díaz, E.","Haslbauer, M.","Bertoldi, F."],"bibdata":{"bibtype":"article","type":"article","title":"[CII] line intensity mapping the epoch of reionization with the Prime-Cam on FYST","url":"http://arxiv.org/abs/2111.12847","abstract":"We predict the three-dimensional intensity power spectrum (PS) of the [CII] 158\\${\\textbackslash},{\\textbackslash}mu\\$m line throughout the epoch of (and post) reionization at redshifts from \\${\\textbackslash}approx\\$ 3.5 to 8. We study the detectability of the PS in a line intensity mapping (LIM) survey with the Fred Young Submillimeter Telescope (FYST). We created mock [CII] tomographic scans in redshift bins at \\$z{\\textbackslash}approx\\$ 3.7, 4.3, 5.8, and 7.4 using the Illustris TNG300-1 \\${\\textbackslash}Lambda\\$CDM simulation and adopting a relation between the star formation activity and the [CII] luminosity (\\$L_\\{[CII]\\}\\$) of galaxies. A star formation rate (SFR) was assigned to a dark matter halo in the Illustris simulation in two ways: (i) we adopted the SFR computed in the Illustris simulation and, (ii) we matched the abundance of the halos with the SFR traced by the observed dust-corrected ultraviolet luminosity function of high-redshift galaxies. The \\$L_\\{[CII]\\}\\$ is related to the SFR from a semi-analytic model of galaxy formation, from a hydrodynamical simulation of a high-redshift galaxy, or from a high-redshift [CII] galaxy survey. The [CII] intensity PS was computed from mock tomographic scans to assess its detectability with the anticipated observational capability of the FYST. The amplitude of the predicted [CII] intensity power spectrum varies by more than a factor of 10, depending on the choice of the halo-to-galaxy SFR and the SFR-to-\\$L_\\{[CII]\\}\\$ relations. In the planned \\$4{\\textasciicircum}\\{{\\textbackslash}circ\\} {\\textbackslash}times 4{\\textasciicircum}\\{{\\textbackslash}circ\\}\\$ FYST LIM survey, we expect a detection of the [CII] PS up to \\$z {\\textbackslash}approx\\$ 5.8, and potentially even up to \\$z {\\textbackslash}approx \\$ 7.4. The design of the envisioned FYST LIM survey enables a PS measurement not only in small (\\textless10 Mpc) shot noise-dominated scales, but also in large (\\textgreater50 Mpc) clustering-dominated scales making it the first LIM experiment that will place constraints on the SFR-to-\\$L_\\{[CII]\\}\\$ and the halo-to-galaxy SFR relations simultaneously.","urldate":"2021-12-17","journal":"arXiv:2111.12847 [astro-ph]","author":[{"propositions":[],"lastnames":["Karoumpis"],"firstnames":["C."],"suffixes":[]},{"propositions":[],"lastnames":["Magnelli"],"firstnames":["B."],"suffixes":[]},{"propositions":[],"lastnames":["Romano-Díaz"],"firstnames":["E."],"suffixes":[]},{"propositions":[],"lastnames":["Haslbauer"],"firstnames":["M."],"suffixes":[]},{"propositions":[],"lastnames":["Bertoldi"],"firstnames":["F."],"suffixes":[]}],"month":"November","year":"2021","note":"arXiv: 2111.12847","keywords":"Astrophysics - Astrophysics of Galaxies","bibtex":"@article{karoumpis_cii_2021,\n\ttitle = {[{CII}] line intensity mapping the epoch of reionization with the {Prime}-{Cam} on {FYST}},\n\turl = {http://arxiv.org/abs/2111.12847},\n\tabstract = {We predict the three-dimensional intensity power spectrum (PS) of the [CII] 158\\${\\textbackslash},{\\textbackslash}mu\\$m line throughout the epoch of (and post) reionization at redshifts from \\${\\textbackslash}approx\\$ 3.5 to 8. We study the detectability of the PS in a line intensity mapping (LIM) survey with the Fred Young Submillimeter Telescope (FYST). We created mock [CII] tomographic scans in redshift bins at \\$z{\\textbackslash}approx\\$ 3.7, 4.3, 5.8, and 7.4 using the Illustris TNG300-1 \\${\\textbackslash}Lambda\\$CDM simulation and adopting a relation between the star formation activity and the [CII] luminosity (\\$L\\_\\{[CII]\\}\\$) of galaxies. A star formation rate (SFR) was assigned to a dark matter halo in the Illustris simulation in two ways: (i) we adopted the SFR computed in the Illustris simulation and, (ii) we matched the abundance of the halos with the SFR traced by the observed dust-corrected ultraviolet luminosity function of high-redshift galaxies. The \\$L\\_\\{[CII]\\}\\$ is related to the SFR from a semi-analytic model of galaxy formation, from a hydrodynamical simulation of a high-redshift galaxy, or from a high-redshift [CII] galaxy survey. The [CII] intensity PS was computed from mock tomographic scans to assess its detectability with the anticipated observational capability of the FYST. The amplitude of the predicted [CII] intensity power spectrum varies by more than a factor of 10, depending on the choice of the halo-to-galaxy SFR and the SFR-to-\\$L\\_\\{[CII]\\}\\$ relations. In the planned \\$4{\\textasciicircum}\\{{\\textbackslash}circ\\} {\\textbackslash}times 4{\\textasciicircum}\\{{\\textbackslash}circ\\}\\$ FYST LIM survey, we expect a detection of the [CII] PS up to \\$z {\\textbackslash}approx\\$ 5.8, and potentially even up to \\$z {\\textbackslash}approx \\$ 7.4. The design of the envisioned FYST LIM survey enables a PS measurement not only in small ({\\textless}10 Mpc) shot noise-dominated scales, but also in large ({\\textgreater}50 Mpc) clustering-dominated scales making it the first LIM experiment that will place constraints on the SFR-to-\\$L\\_\\{[CII]\\}\\$ and the halo-to-galaxy SFR relations simultaneously.},\n\turldate = {2021-12-17},\n\tjournal = {arXiv:2111.12847 [astro-ph]},\n\tauthor = {Karoumpis, C. and Magnelli, B. and Romano-Díaz, E. and Haslbauer, M. and Bertoldi, F.},\n\tmonth = nov,\n\tyear = {2021},\n\tnote = {arXiv: 2111.12847},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n","author_short":["Karoumpis, C.","Magnelli, B.","Romano-Díaz, E.","Haslbauer, M.","Bertoldi, F."],"key":"karoumpis_cii_2021","id":"karoumpis_cii_2021","bibbaseid":"karoumpis-magnelli-romanodaz-haslbauer-bertoldi-ciilineintensitymappingtheepochofreionizationwiththeprimecamonfyst-2021","role":"author","urls":{"Paper":"http://arxiv.org/abs/2111.12847"},"keyword":["Astrophysics - Astrophysics of Galaxies"],"metadata":{"authorlinks":{}}},"bibtype":"article","biburl":"https://bibbase.org/zotero/polyphant","dataSources":["7gvjSdWrEu7z5vjjj"],"keywords":["astrophysics - astrophysics of galaxies"],"search_terms":["cii","line","intensity","mapping","epoch","reionization","prime","cam","fyst","karoumpis","magnelli","romano-díaz","haslbauer","bertoldi"],"title":"[CII] line intensity mapping the epoch of reionization with the Prime-Cam on FYST","year":2021}