Cosmic Star-Formation History Measured at 1.4 GHz. Matthews, A. M., Condon, J. J., Cotton, W. D., & Mauch, T. arXiv e-prints, 2104:arXiv:2104.11756, April, 2021.
Paper abstract bibtex We matched the 1.4 GHz local luminosity functions of star-forming galaxies (SFGs) and active galactic nuclei to the 1.4 GHz differential source counts from \$0.25 {\textbackslash} {\textbackslash}mu{\textbackslash}mathrm\{Jy\}\$ to 25 Jy using combinations of luminosity and density evolution. We present the most robust and complete local far-infrared (FIR)/radio luminosity correlation to date in a volume-limited sample of \${\textbackslash}approx 4.3 {\textbackslash}times 10{\textasciicircum}3\$ nearby SFGs, finding that it is very tight but distinctly sub-linear: \$L_{\textbackslash}mathrm\{FIR\} {\textbackslash}propto L_{\textbackslash}mathrm\{1.4{\textbackslash},GHz\}{\textasciicircum}\{0.85\}\$. If the local FIR/radio correlation does not evolve, the evolving 1.4 GHz luminosity function of SFGs yields the evolving star-formation rate density (SFRD) \${\textbackslash}psi (M_{\textbackslash}odot {\textbackslash} {\textbackslash}mathrm\{year\}{\textasciicircum}\{-1\} {\textbackslash} {\textbackslash}mathrm\{Mpc\}{\textasciicircum}\{-3\}\$) as a function of time since the big bang. The SFRD measured at 1.4 GHz grows rapidly at early times, peaks at "cosmic noon" when \$t {\textbackslash}approx 3 {\textbackslash} {\textbackslash}mathrm\{Gyr\}\$ and \$z {\textbackslash}approx 2\$, and subsequently decays with an \$e\$-folding time scale \${\textbackslash}tau = 3.2 {\textbackslash} {\textbackslash}mathrm\{Gyr\}\$. This evolution is similar to, but somewhat stronger than, SFRD evolution estimated from UV and FIR data.
@article{matthews_cosmic_2021,
title = {Cosmic {Star}-{Formation} {History} {Measured} at 1.4 {GHz}},
volume = {2104},
url = {http://adsabs.harvard.edu/abs/2021arXiv210411756M},
abstract = {We matched the 1.4 GHz local luminosity functions of star-forming galaxies (SFGs) and active galactic nuclei to the 1.4 GHz differential source counts from \$0.25 {\textbackslash} {\textbackslash}mu{\textbackslash}mathrm\{Jy\}\$ to 25 Jy using combinations of luminosity and density evolution. We present the most robust and complete local far-infrared (FIR)/radio luminosity correlation to date in a volume-limited sample of \${\textbackslash}approx 4.3 {\textbackslash}times 10{\textasciicircum}3\$ nearby SFGs, finding that it is very tight but distinctly sub-linear: \$L\_{\textbackslash}mathrm\{FIR\} {\textbackslash}propto L\_{\textbackslash}mathrm\{1.4{\textbackslash},GHz\}{\textasciicircum}\{0.85\}\$. If the local FIR/radio correlation does not evolve, the evolving 1.4 GHz luminosity function of SFGs yields the evolving star-formation rate density (SFRD) \${\textbackslash}psi (M\_{\textbackslash}odot {\textbackslash} {\textbackslash}mathrm\{year\}{\textasciicircum}\{-1\} {\textbackslash} {\textbackslash}mathrm\{Mpc\}{\textasciicircum}\{-3\}\$) as a function of time since the big bang. The SFRD measured at 1.4 GHz grows rapidly at early times, peaks at "cosmic noon" when \$t {\textbackslash}approx 3 {\textbackslash} {\textbackslash}mathrm\{Gyr\}\$ and \$z {\textbackslash}approx 2\$, and subsequently decays with an \$e\$-folding time scale \${\textbackslash}tau = 3.2 {\textbackslash} {\textbackslash}mathrm\{Gyr\}\$. This evolution is similar to, but somewhat stronger than, SFRD evolution estimated from UV and FIR data.},
urldate = {2021-04-29},
journal = {arXiv e-prints},
author = {Matthews, A. M. and Condon, J. J. and Cotton, W. D. and Mauch, T.},
month = apr,
year = {2021},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
pages = {arXiv:2104.11756},
}
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We present the most robust and complete local far-infrared (FIR)/radio luminosity correlation to date in a volume-limited sample of \\${\\textbackslash}approx 4.3 {\\textbackslash}times 10{\\textasciicircum}3\\$ nearby SFGs, finding that it is very tight but distinctly sub-linear: \\$L_{\\textbackslash}mathrm\\{FIR\\} {\\textbackslash}propto L_{\\textbackslash}mathrm\\{1.4{\\textbackslash},GHz\\}{\\textasciicircum}\\{0.85\\}\\$. If the local FIR/radio correlation does not evolve, the evolving 1.4 GHz luminosity function of SFGs yields the evolving star-formation rate density (SFRD) \\${\\textbackslash}psi (M_{\\textbackslash}odot {\\textbackslash} {\\textbackslash}mathrm\\{year\\}{\\textasciicircum}\\{-1\\} {\\textbackslash} {\\textbackslash}mathrm\\{Mpc\\}{\\textasciicircum}\\{-3\\}\\$) as a function of time since the big bang. The SFRD measured at 1.4 GHz grows rapidly at early times, peaks at \"cosmic noon\" when \\$t {\\textbackslash}approx 3 {\\textbackslash} {\\textbackslash}mathrm\\{Gyr\\}\\$ and \\$z {\\textbackslash}approx 2\\$, and subsequently decays with an \\$e\\$-folding time scale \\${\\textbackslash}tau = 3.2 {\\textbackslash} {\\textbackslash}mathrm\\{Gyr\\}\\$. 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We present the most robust and complete local far-infrared (FIR)/radio luminosity correlation to date in a volume-limited sample of \\${\\textbackslash}approx 4.3 {\\textbackslash}times 10{\\textasciicircum}3\\$ nearby SFGs, finding that it is very tight but distinctly sub-linear: \\$L\\_{\\textbackslash}mathrm\\{FIR\\} {\\textbackslash}propto L\\_{\\textbackslash}mathrm\\{1.4{\\textbackslash},GHz\\}{\\textasciicircum}\\{0.85\\}\\$. If the local FIR/radio correlation does not evolve, the evolving 1.4 GHz luminosity function of SFGs yields the evolving star-formation rate density (SFRD) \\${\\textbackslash}psi (M\\_{\\textbackslash}odot {\\textbackslash} {\\textbackslash}mathrm\\{year\\}{\\textasciicircum}\\{-1\\} {\\textbackslash} {\\textbackslash}mathrm\\{Mpc\\}{\\textasciicircum}\\{-3\\}\\$) as a function of time since the big bang. 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