PREDICTING THE REDSHIFT 2 H<i>α</i>LUMINOSITY FUNCTION USING [O iii] EMISSION LINE GALAXIES

Mehta, Vihang; Scarlata, Claudia; Colbert, James; Dai, Y. Sophia; Dressler, Alan; Henry, Alaina; Malkan, M.; Rafelski, Marc; Siana, Brian; Teplitz, Harry I.; Bagley, Micaela; Beck, Mélanie; Ross, Nathaniel; Rutkowski, Michael J.; Wang, Yun

doi:10.1088/0004-637x/811/2/141

Cited by 53 publications

(147 citation statements)

References 39 publications

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“…In this section we will therefore compare the GALACTICUS counts to the observed counts from the WISP survey, as presented by Colbert et al (2013) and Mehta et al (2015). In particular we will focus on comparing to the most recent results from Mehta et al (2015) over the redshift range 0.7 < z < 1.5. We remind the reader that due to the upper wavelength limit of the HST WFC3 G141 grism, 1.2-1.7 microns, the Hα line is only directly detectable with WFC3 out to z 1.5.…”

Section: Comparison To Observed Number Countsmentioning

confidence: 99%

“…The galaxy counts presented by Mehta et al (2015) have not been corrected for dust attenuation or for contamination from [NII]. Due to the resolution of the WFC3 grisms, WISP is unable to resolve the [NII] doublet and de-blend it from the Hα line.…”

Section: Modelling [Nii] Contaminationmentioning

confidence: 99%

“…Note that neither Colbert et al (2013) nor Mehta et al (2015) made any flux corrections for dust attenuation or contamination due to the [NII] (6548Å + 6584Å) doublet. Using 29 separate WISP fields covering a combined area of 0.037 square degrees, Colbert et al (2013) estimated a number density of 6,700 deg −2 for Hα-emitting galaxies above a Hα + [NII] blended flux limit of 2 × 10 −16 erg s −1 cm −2 .…”

Section: Introductionmentioning

confidence: 99%

“…In their analysis, Mehta et al (2015) also estimated the WISP Hα counts out to z < 2 by firstly measuring the bivariate Hα-[OIII] line luminosity function for 0.7 < z < 1.5 and then using the observed correlation between the Hα and [OIII] luminosities to predict the Hα counts from the [OIII]-only line luminosity function (see Mehta et al 2015 for further details). Over the redshift range 0.7 < z < 2 Mehta et al (2015) find the number density of Hα-emitters to be approximately 11,000 deg −2 for a Hα + [NII] blended flux limit of 2 × 10 −16 erg s −1 cm −2 and approximately 32,000 deg −2 for a limit of 1 × 10 −16 erg s −1 cm −2 (again they made no correction for dust attenuation).…”

Section: Introductionmentioning

confidence: 99%

“…Over the redshift range 0.7 < z < 2 Mehta et al (2015) find the number density of Hα-emitters to be approximately 11,000 deg −2 for a Hα + [NII] blended flux limit of 2 × 10 −16 erg s −1 cm −2 and approximately 32,000 deg −2 for a limit of 1 × 10 −16 erg s −1 cm −2 (again they made no correction for dust attenuation).…”

Section: Introductionmentioning

confidence: 99%

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Predicting Hα emission-line galaxy counts for future galaxy redshift surveys

Merson

Wang

Benson

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Knowledge of the number density of Hα emitting galaxies is vital for assessing the scientific impact of the Euclid and WFIRST missions. In this work we present predictions from a galaxy formation model, GALACTICUS, for the cumulative number counts of Hα-emitting galaxies. We couple GALACTICUS to three different dust attenuation methods and examine the counts using each method. A χ 2 minimisation approach is used to compare the model predictions to observed galaxy counts and calibrate the dust parameters. We find that weak dust attenuation is required for the GALACTICUS counts to be broadly consistent with the observations, though the optimum dust parameters return large values for χ 2 , suggesting that further calibration of GALACTICUS is necessary. The model predictions are also consistent with observed estimates for the optical depth and the Hα luminosity function. Finally we present forecasts for the redshift distributions and number counts for two Euclid-like and one WFIRST-like survey. For a Euclid-like survey with redshift range 0.9 z 1.8 and Hα + [NII] blended flux limit of 2 × 10 −16 erg s −1 cm −2 we predict a number density between 3900-4800 galaxies per square degree. For a WFIRST-like survey with redshift range 1 z 2 and blended flux limit of 1 × 10 −16 erg s −1 cm −2 we predict a number density between 10400-15200 galaxies per square degree.

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Section: Comparison To Observed Number Countsmentioning

confidence: 99%

Section: Modelling [Nii] Contaminationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Predicting Hα emission-line galaxy counts for future galaxy redshift surveys

Merson

Wang

Benson

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Modelling the number density of Hαemitters for future spectroscopic near-IR space missions

Pozzetti

Hirata

Geach

et al. 2016

A&A

101

155

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Context. The future space missions Euclid and WFIRST-AFTA will use the Hα emission line to measure the redshifts of tens of millions of galaxies. The Hα luminosity function at z > 0.7 is one of the major sources of uncertainty in forecasting cosmological constraints from these missions. Aims. We construct unified empirical models of the Hα luminosity function spanning the range of redshifts and line luminosities relevant to the redshift surveys proposed with Euclid and WFIRST-AFTA. Methods. By fitting to observed luminosity functions from Hα surveys, we build three models for its evolution. Different fitting methodologies, functional forms for the luminosity function, subsets of the empirical input data, and treatment of systematic errors are considered to explore the robustness of the results. Results. Functional forms and model parameters are provided for all three models, along with the counts and redshift distributions up to z ∼ 2.5 for a range of limiting fluxes (F Hα > 0.5−3 × 10 −16 erg cm −2 s −1 ) that are relevant for future space missions. For instance, in the redshift range 0.90 < z < 1.8, our models predict an available galaxy density in the range 7700-130 300 and 2000-4800 deg −2 respectively at fluxes above F Hα > 1 and 2×10 −16 erg cm −2 s −1 , and 32 000-48 0000 for F Hα > 0.5×10 −16 erg cm −2 s −1 in the extended redshift range 0.40 < z < 1.8. We also consider the implications of our empirical models for the total Hα luminosity density of the Universe, and the closely related cosmic star formation history.

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The MUSE-Wide Survey: A determination of the Lymanαemitter luminosity function at 3 <z< 6

Herenz

Wisotzki

Saust

et al. 2019

A&A

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We investigate the Lyman α emitter (LAE) luminosity function (LF) within the redshift range 2.9 ≤ z ≤ 6 from the first instalment of the blind integral field spectroscopic MUSE-Wide survey. This initial part of the survey probes a region of 22.2 arcmin2 in the CANDELS/GOODS-S field (24 MUSE pointings with 1h integrations). The dataset provided us with 237 LAEs from which we construct the LAE LF in the luminosity range 42.2 ≤ log LLyα[erg s−1] ≤ 43.5 within a volume of 2.3 × 105 Mpc3. For the LF construction we utilise three different non-parametric estimators: the classical 1/Vmax method, the C− method, and an improved binned estimator for the differential LF. All three methods deliver consistent results, with the cumulative LAE LF being Φ(log L Lyα[erg s−1] = 43.5) ≃ 3 × 10−6 Mpc−3 and Φ(log L Lyα[erg s−1] = 42.2) ≃ 2 × 10−3 Mpc−3 towards the bright and faint end of our survey, respectively. By employing a non-parametric statistical test, and by comparing the full sample to subsamples in redshift bins, we find no supporting evidence for an evolving LAE LF over the probed redshift and luminosity range. Using a parametric maximum-likelihood technique we determine the best-fitting Schechter function parameters α = 1.84+04.2−0.41 and L∗[erg s−0.1] = 42.2−0.16+0.22 with the corresponding normalisation logϕ*[Mpc−3]= − 2.71. However, the dynamic range in Lyα luminosities probed by MUSE-Wide leads to a strong degeneracy between α and L*. Moreover, we find that a power-law parameterisation of the LF appears to be less consistent with the data compared to the Schechter function, even so when not excluding the X-Ray identified AGN from the sample. When correcting for completeness in the LAE LF determinations, we take into account that LAEs exhibit diffuse extended low surface brightness halos. We compare the resulting LF to one obtained by applying a correction assuming compact point-like emission. We find that the standard correction underestimates the LAE LF at the faint end of our survey by a factor of 2.5. Contrasting our results to the literature we find that at 42.2 ≤ log LLyα[erg s−1] ≲ 42.5 previous LAE LF determinations from narrow-band surveys appear to be affected by a similar bias.

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PREDICTING THE REDSHIFT 2 HαLUMINOSITY FUNCTION USING [O iii] EMISSION LINE GALAXIES

Cited by 53 publications

References 39 publications

Predicting Hα emission-line galaxy counts for future galaxy redshift surveys

Predicting Hα emission-line galaxy counts for future galaxy redshift surveys

Modelling the number density of Hαemitters for future spectroscopic near-IR space missions

The MUSE-Wide Survey: A determination of the Lymanαemitter luminosity function at 3 <z< 6

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