Predicting Future Space Near-Ir Grism Surveys Using the Wfc3 Infrared Spectroscopic Parallels Survey

Colbert, James; Teplitz, Harry I.; Atek, Hakim; Bunker, Andrew J.; Rafelski, Marc; Ross, Nathaniel; Scarlata, Claudia; Bedregal, A. G.; Domínguez, A.; Dressler, Alan; Henry, Alaina; Malkan, M.; Martin, Crystal L.; Masters, Dan; McCarthy, Patrick J.; Siana, Brian

doi:10.1088/0004-637x/779/1/34

Cited by 92 publications

(249 citation statements)

References 54 publications

Supporting

Mentioning

208

Contrasting

Order By: Relevance

“…As mentioned in Section 3.1, Colbert et al (2013) and Mehta et al (2015) Fig. 6 shows, for both cases, the cumulative number counts obtained when adopting the optical depth that minimises the reduced χ 2 statistic.…”

Section: Examination Of [Nii] Contaminationmentioning

confidence: 89%

“…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.…”

Section: Comparison To Observed Number Countsmentioning

confidence: 99%

“…Due to the resolution of the WFC3 grisms, WISP is unable to resolve the [NII] doublet and de-blend it from the Hα line. In their analysis, Colbert et al (2013) and Mehta et al (2015) The coloured pixels show the logarithm base-10 of the median line ratio for the galaxies in that M vs. sSFR bin. In the left-hand panel we show the distribution for the SDSS galaxies in the catalogue presented in Masters et al (2016).…”

Section: Modelling [Nii] Contaminationmentioning

confidence: 99%

“…The optical depth parameters that yield this minimum value for χ 2 /ν are reported along with an estimate of their uncertainties. The uncertainties correspond to ±1σ and are estimated by identifying for each parameter the range of values for which ∆χ 2 = 1 for the Ferrara et al (1999) and Calzetti et al (2000) The observed counts reported by Colbert et al (2013) and Mehta et al (2015) are shown by the symbols. For the three dust methods we assume values for the optical depths as stated in Table 1. for χ 2 min /ν, this could also suggest that the ISM attenuation set by the galaxy properties is too strong and that further calibration of GALACTICUS is required in the future.…”

Section: Chi-squared Minimisationmentioning

confidence: 99%

“…Therefore, knowledge of the number density of different galaxies, as a function of redshift, is crucial in both the planning and evaluation of a survey strategy. As such, much effort has been invested in using existing emission line galaxy surveys to estimate the number of Hα emitters that Euclid and WFIRST are likely to observe (for example, Colbert et al 2013;Mehta et al 2015;Pozzetti et al 2016;Valentino et al 2017).…”

Section: Introductionmentioning

confidence: 99%

See 4 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

View full text Add to dashboard Cite

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.

show abstract

Section: Examination Of [Nii] Contaminationmentioning

confidence: 89%

Section: Comparison To Observed Number Countsmentioning

confidence: 99%

Section: Modelling [Nii] Contaminationmentioning

confidence: 99%

Section: Chi-squared Minimisationmentioning

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

View full text Add to dashboard Cite

show abstract

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

Pozzetti

Hirata

Geach

et al. 2016

A&A

106

155

View full text Add to dashboard Cite

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.

show abstract

Euclidpreparation

Gabarra¹,

Mancini²,

Muñoz³

et al. 2023

A&A

View full text Add to dashboard Cite

This work focusses on the pilot run of a simulation campaign aimed at investigating the spectroscopic capabilities of the Euclid Near-Infrared Spectrometer and Photometer (NISP), in terms of continuum and emission line detection in the context of galaxy evolutionary studies. To this purpose, we constructed, emulated, and analysed the spectra of 4992 star-forming galaxies at 0.3 ≤ z ≤ 2.5 using the NISP pixel-level simulator. We built the spectral library starting from public multi-wavelength galaxy catalogues, with value-added information on spectral energy distribution (SED) fitting results, and stellar population templates from Bruzual & Charlot (2003, MNRAS, 344, 1000). Rest-frame optical and near-IR nebular emission lines were included using empirical and theoretical relations. Dust attenuation was treated using the Calzetti extinction law accounting for the differential attenuation in line-emitting regions with respect to the stellar continuum. The NISP simulator was configured including instrumental and astrophysical sources of noise such as the dark current, read-out noise, zodiacal background, and out-of-field stray light. In this preliminary study, we avoided contamination due to the overlap of the slitless spectra. For this purpose, we located the galaxies on a grid and simulated only the first order spectra. We inferred the 3.5σ NISP red grism spectroscopic detection limit of the continuum measured in the H band for star-forming galaxies with a median disk half-light radius of 0.″4 at magnitude H = 19.5 ± 0.2 AB mag for the Euclid Wide Survey and at H = 20.8 ± 0.6 AB mag for the Euclid Deep Survey. We found a very good agreement with the red grism emission line detection limit requirement for the Wide and Deep surveys. We characterised the effect of the galaxy shape on the detection capability of the red grism and highlighted the degradation of the quality of the extracted spectra as the disk size increased. In particular, we found that the extracted emission line signal-to-noise ratio (S/N) drops by ~45% when the disk size ranges from 0.″25 to 1″. These trends lead to a correlation between the emission line S/N and the stellar mass of the galaxy and we demonstrate the effect in a stacking analysis unveiling emission lines otherwise too faint to detect.

show abstract

Predicting Future Space Near-Ir Grism Surveys Using the Wfc3 Infrared Spectroscopic Parallels Survey

Cited by 92 publications

References 54 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

Euclidpreparation

Contact Info

Product

Resources

About