论文标题
h $α$，[oiii]和[oii]发射器的大型3摄氏度$^2 $调查：约束发光功能
A large, deep 3 deg$^2$ survey of H$α$, [OIII], and [OII] emitters from LAGER: constraining luminosity functions
论文作者
论文摘要
We present our measurements of the H$α$, [OIII], and [OII] luminosity functions as part of the Lyman Alpha Galaxies at Epoch of Reionization (LAGER) survey using our samples of 1577 $z = 0.47$ H$α$-, 3933 $z = 0.93$ [OIII]-, and 5367 $z = 1.59$ [OII]-selected单个3度$^2 $ CTIO/BLANCO DECAM指向COSMOS字段中的排放线星系。我们的观察值达到5 $σ$ depths $ 8.2 \ times10^{ - 18} $ erg s $^{ - 1} $ cm $^{ - 2} $和$（1-7）\ times10^{5} $ mpc $^3 $的$（1-7）\ times10^{5} $（1-7）$（1-7）的调查。我们测量观察到的光度函数，并找到$ ϕ^\ star = 10^{ - 3.16 \ pm0.09} $ mpc $^{ - 3} $和$ l^\ star = 10^{41.72 \ pm0.09} $ 10^{ - 2.16^{+0.10} _ { - 0.12}} $ mpc $^{ - 3} $和$ l^\ star = 10^{41.38^{+0.07} _ { - 0.06}} 10^{ - 1.97^{+0.07} _ { - 0.07}} $ mpc $^{ - 3} $和$ l^\ star = 10^{41.66 \ pm0.03} $ 分别。观察到了过量的明亮$> 10^{42} $ erg s $^{ - 1} $ [OIII]发射器，可能是由于AGN污染。假设$ a _ {\ rm {h}α} = 1 $ mag，则应用灰尘更正。我们还使用SDSS DR12数据设计了自己的经验休息框架$ g - r $ $ $校准，对我们的$ z = 0.47 $ h $α$发射器进行测试，$ z $ cosmos $ 1 $ d Spectra，然后以$（g -r）$ -0.8 $ $ -0.8 $ $ -0.8 $和$ 1.3 $ MAG进行校准。灰尘和AGN校正的星形形成率密度（SFRD）被测量为$ \ log_ {10}ρ_{\ rm {\ rm {sfr}}}/（\ rm {m} _ \ odot \ odot \ \ \ \ \ \ \ \ \ \ rm {yr} -1.63 \ pm0.04 $，$ -1.07 \ pm0.06 $和$ -0.90 \ pm0.10 $ for H $α$，[OIII]和[OII]和[OII]。与多波长SFRD相比，我们发现我们的[OIII]和[OII]样品在各自的红移处完全追踪宇宙星形的形成活动，而H $α$样本痕迹$ \ sim 70 $ \ sim 70 $ e z = 0.47 $ sfrd。
We present our measurements of the H$α$, [OIII], and [OII] luminosity functions as part of the Lyman Alpha Galaxies at Epoch of Reionization (LAGER) survey using our samples of 1577 $z = 0.47$ H$α$-, 3933 $z = 0.93$ [OIII]-, and 5367 $z = 1.59$ [OII]-selected emission line galaxies in a single 3 deg$^2$ CTIO/Blanco DECam pointing of the COSMOS field. Our observations reach 5$σ$ depths of $8.2\times10^{-18}$ erg s$^{-1}$ cm$^{-2}$ and comoving volumes of $(1-7)\times10^{5}$ Mpc$^3$ making our survey one of the deepest narrowband surveys. We measure the observed luminosity functions and find best-fits of $ϕ^\star = 10^{-3.16\pm0.09}$ Mpc$^{-3}$ and $L^\star = 10^{41.72\pm0.09}$ erg s$^{-1}$ for H$α$, $ϕ^\star = 10^{-2.16^{+0.10}_{-0.12}}$ Mpc$^{-3}$ and $L^\star = 10^{41.38^{+0.07}_{-0.06}}$ erg s$^{-1}$ for [OIII], and $ϕ^\star = 10^{-1.97^{+0.07}_{-0.07}}$ Mpc$^{-3}$ and $L^\star = 10^{41.66\pm0.03}$ erg s$^{-1}$ for [OII], with $α$ fixed to $-1.75$, $-1.6$, and $-1.3$, respectively. An excess of bright $> 10^{42}$ erg s$^{-1}$ [OIII] emitters is observed and may be due to AGN contamination. Dust corrections are applied assuming $A_{\rm{H}α} = 1$ mag. We also design our own empirical rest-frame $g - r$ calibration using SDSS DR12 data, test it against our $z = 0.47$ H$α$ emitters with $z$COSMOS $1$D spectra, and calibrate it for $(g - r)$ between $-0.8$ and $1.3$ mag. Dust and AGN-corrected star formation rate densities (SFRDs) are measured as $\log_{10}ρ_{\rm{SFR}}/(\rm{M}_\odot\ \rm{yr}^{-1}\ \rm{Mpc}^{-3}) = -1.63\pm0.04$, $-1.07\pm0.06$, and $-0.90\pm0.10$ for H$α$, [OIII], and [OII], respectively. We find our [OIII] and [OII] samples fully trace cosmic star formation activity at their respective redshifts in comparison to multi-wavelength SFRDs, while the H$α$ sample traces $\sim 70$ percent of the total $z = 0.47$ SFRD.
