University of Hertfordshire

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By the same authors

Modelling the number density of H$ emitters for future spectroscopic near-IR space missions

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Modelling the number density of H$ emitters for future spectroscopic near-IR space missions. / Pozzetti, L.; Hirata, C.~M.; Geach, J.~E.; Cimatti, A.; Baugh, C.; Cucciati, O.; Merson, A.; Norberg, P.; Shi, D.

In: Astronomy & Astrophysics, Vol. 590, A3, 01.06.2016.

Research output: Contribution to journalArticlepeer-review

Harvard

Pozzetti, L, Hirata, CM, Geach, JE, Cimatti, A, Baugh, C, Cucciati, O, Merson, A, Norberg, P & Shi, D 2016, 'Modelling the number density of H$ emitters for future spectroscopic near-IR space missions', Astronomy & Astrophysics, vol. 590, A3. https://doi.org/10.1051/0004-6361/201527081

APA

Pozzetti, L., Hirata, C. M., Geach, J. E., Cimatti, A., Baugh, C., Cucciati, O., Merson, A., Norberg, P., & Shi, D. (2016). Modelling the number density of H$ emitters for future spectroscopic near-IR space missions. Astronomy & Astrophysics, 590, [A3]. https://doi.org/10.1051/0004-6361/201527081

Vancouver

Author

Pozzetti, L. ; Hirata, C.~M. ; Geach, J.~E. ; Cimatti, A. ; Baugh, C. ; Cucciati, O. ; Merson, A. ; Norberg, P. ; Shi, D. / Modelling the number density of H$ emitters for future spectroscopic near-IR space missions. In: Astronomy & Astrophysics. 2016 ; Vol. 590.

Bibtex

@article{683cb5ce2b724f84a26d50b014aed860,
title = "Modelling the number density of H$ emitters for future spectroscopic near-IR space missions",
abstract = "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 (FHα> 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 1 and 2 × 10-16 erg cm-2 s-1, and 32 000–48 0000 for FHα> 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.",
keywords = "galaxies: evolution, galaxies: high-redshift, galaxies: star formation, galaxies: luminosity function, mass function, cosmology: observations",
author = "L. Pozzetti and C.~M. Hirata and J.~E. Geach and A. Cimatti and C. Baugh and O. Cucciati and A. Merson and P. Norberg and D. Shi",
note = " Reproduced with permission from Astronomy & Astrophysics, {\textcopyright} ESO",
year = "2016",
month = jun,
day = "1",
doi = "10.1051/0004-6361/201527081",
language = "English",
volume = "590",
journal = "Astronomy & Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",

}

RIS

TY - JOUR

T1 - Modelling the number density of H$ emitters for future spectroscopic near-IR space missions

AU - Pozzetti, L.

AU - Hirata, C.~M.

AU - Geach, J.~E.

AU - Cimatti, A.

AU - Baugh, C.

AU - Cucciati, O.

AU - Merson, A.

AU - Norberg, P.

AU - Shi, D.

N1 - Reproduced with permission from Astronomy & Astrophysics, © ESO

PY - 2016/6/1

Y1 - 2016/6/1

N2 - 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 (FHα> 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 1 and 2 × 10-16 erg cm-2 s-1, and 32 000–48 0000 for FHα> 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.

AB - 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 (FHα> 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 1 and 2 × 10-16 erg cm-2 s-1, and 32 000–48 0000 for FHα> 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.

KW - galaxies: evolution, galaxies: high-redshift, galaxies: star formation, galaxies: luminosity function, mass function, cosmology: observations

U2 - 10.1051/0004-6361/201527081

DO - 10.1051/0004-6361/201527081

M3 - Article

VL - 590

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 0004-6361

M1 - A3

ER -