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- W3100488140 abstract "We present an empirical parameterization of the [NII]/H$alpha$ flux ratio as a function of stellar mass and redshift valid at 0 < z < 2.7 and 8.5 < log(M) < 11.0. This description can easily be applied to (i) simulations for modeling [NII]$lambda6584$ line emission, (ii) deblend [NII] and H$alpha$ in current low-resolution grism and narrow-band observations to derive intrinsic H$alpha$ fluxes, and (iii) to reliably forecast the number counts of H$alpha$ emission-line galaxies for future surveys, such as those planned for Euclid and the Wide Field Infrared Survey Telescope (WFIRST). Our model combines the evolution of the locus on the Baldwin, Phillips & Terlevich (BPT) diagram measured in spectroscopic data out to z = 2.5 with the strong dependence of [NII]/H$alpha$ on stellar mass and [OIII]/H$beta$ observed in local galaxy samples. We find large variations in the [NII]/H$alpha$ flux ratio at a fixed redshift due to its dependency on stellar mass; hence, the assumption of a constant [NII] flux contamination fraction can lead to a significant under- or overestimate of H$alpha$ luminosities. Specifically, measurements of the intrinsic H$alpha$ luminosity function derived from current low-resolution grism spectroscopy assuming a constant 29% contamination of [NII] can be overestimated by factors of ~8 at log(L) > 43.0 for galaxies at redshifts z = 1.5. This has implications for the prediction of H$alpha$ emitters for Euclid and WFIRST. We also study the impact of blended H$alpha$ and [NII] on the accuracy of measured spectroscopic redshifts." @default.
- W3100488140 created "2020-11-23" @default.
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- W3100488140 date "2018-03-16" @default.
- W3100488140 modified "2023-10-01" @default.
- W3100488140 title "Empirical Modeling of the Redshift Evolution of the $[{rm{N}},{rm{II}}]$/H<i>α</i> Ratio for Galaxy Redshift Surveys" @default.
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- W3100488140 cites W1851823814 @default.
- W3100488140 cites W1943306457 @default.
- W3100488140 cites W1967876247 @default.
- W3100488140 cites W1969881452 @default.
- W3100488140 cites W1975780632 @default.
- W3100488140 cites W1985952407 @default.
- W3100488140 cites W1996267430 @default.
- W3100488140 cites W1996738326 @default.
- W3100488140 cites W2008877686 @default.
- W3100488140 cites W2011654732 @default.
- W3100488140 cites W2013575191 @default.
- W3100488140 cites W2015295900 @default.
- W3100488140 cites W2019103948 @default.
- W3100488140 cites W2067242485 @default.
- W3100488140 cites W2067857092 @default.
- W3100488140 cites W2071433262 @default.
- W3100488140 cites W2073262056 @default.
- W3100488140 cites W2074094455 @default.
- W3100488140 cites W2076051966 @default.
- W3100488140 cites W2080927107 @default.
- W3100488140 cites W2089947188 @default.
- W3100488140 cites W2096147217 @default.
- W3100488140 cites W2121173473 @default.
- W3100488140 cites W2125977823 @default.
- W3100488140 cites W2128759530 @default.
- W3100488140 cites W2129760210 @default.
- W3100488140 cites W2143480379 @default.
- W3100488140 cites W2150995848 @default.
- W3100488140 cites W2153305744 @default.
- W3100488140 cites W2157917411 @default.
- W3100488140 cites W2166365370 @default.
- W3100488140 cites W2303330669 @default.
- W3100488140 cites W2397592981 @default.
- W3100488140 cites W2516977061 @default.
- W3100488140 cites W2524194729 @default.
- W3100488140 cites W2621381271 @default.
- W3100488140 cites W2763659440 @default.
- W3100488140 cites W2794983349 @default.
- W3100488140 cites W2949306268 @default.
- W3100488140 cites W3098337129 @default.
- W3100488140 cites W3098362140 @default.
- W3100488140 cites W3098784892 @default.
- W3100488140 cites W3099390633 @default.
- W3100488140 cites W3099438994 @default.
- W3100488140 cites W3100024326 @default.
- W3100488140 cites W3100235861 @default.
- W3100488140 cites W3100366211 @default.
- W3100488140 cites W3100494980 @default.
- W3100488140 cites W3100601682 @default.
- W3100488140 cites W3100971600 @default.
- W3100488140 cites W3101580377 @default.
- W3100488140 cites W3102074255 @default.
- W3100488140 cites W3102144907 @default.
- W3100488140 cites W3102538720 @default.
- W3100488140 cites W3102836929 @default.
- W3100488140 cites W3103415621 @default.
- W3100488140 cites W3103727617 @default.
- W3100488140 cites W3103868583 @default.
- W3100488140 cites W3104206875 @default.
- W3100488140 cites W3104214999 @default.
- W3100488140 cites W3104477111 @default.
- W3100488140 cites W3104499440 @default.
- W3100488140 cites W3104628793 @default.
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- W3100488140 doi "https://doi.org/10.3847/1538-4357/aab1fc" @default.
- W3100488140 hasPublicationYear "2018" @default.
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