THE EVOLUTION of the FAINT END of the UV LUMINOSITY FUNCTION during the PEAK EPOCH of STAR FORMATION (1 < z < 3)

Anahita Alavi, Brian Siana, Johan Richard, Marc Rafelski, Mathilde Jauzac, Marceau Limousin, William R. Freeman, Claudia Scarlata, Brant E Robertson, Daniel P Stark, Harry I. Teplitz, Vandana Desai

Research output: Contribution to journalArticle

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Abstract

We present a robust measurement of the rest-frame UV luminosity function (LF) and its evolution during the peak epoch of cosmic star formation at 1 < z < 3. We use our deep near-ultraviolet imaging from WFC3/UVIS on the Hubble Space Telescope and existing Advanced Camera for Surveys (ACS)/WFC and WFC3/IR imaging of three lensing galaxy clusters, Abell 2744 and MACS J0717 from the Hubble Frontier Field survey and Abell 1689. Combining deep UV imaging and high magnification from strong gravitational lensing, we use photometric redshifts to identify 780 ultra-faint galaxies with MUV < -12.5 AB mag at 1 < z < 3. From these samples, we identified five new, faint, multiply imaged systems in A1689. We run a Monte Carlo simulation to estimate the completeness correction and effective volume for each cluster using the latest published lensing models. We compute the rest-frame UV LF and find the best-fit faint-end slopes of a = -1.56 ± 0.04, α = -1.72 ± 0.04, and α = -1.94 ± 0.06 at 1.0 < z < 1.6, 1.6 < z < 2.2, and 2.2 < z < 3.0, respectively. Our results demonstrate that the UV LF becomes steeper from z ∼ 1.3 to z ∼ 2.6 with no sign of a turnover down to MUV = -14 AB mag. We further derive the UV LFs using the Lyman break dropout selection and confirm the robustness of our conclusions against different selection methodologies. Because the sample sizes are so large and extend to such faint luminosities, the statistical uncertainties are quite small, and systematic uncertainties (due to the assumed size distribution, for example) likely dominate. If we restrict our analysis to galaxies and volumes above >50% completeness in order to minimize these systematics, we still find that the faint-end slope is steep and getting steeper with redshift, though with slightly shallower (less negative) values (a = -1.55 ± 0.06, -1.69 ± 0.07, and -1.79 ± 0.08 for z ∼ 1.3, 1.9, and 2.6, respectively). Finally, we conclude that the faint star-forming galaxies with UV magnitudes of -18.5 < MUV < -12.5 covered in this study produce the majority (55%-60%) of the unobscured UV luminosity density at 1 < z < 3.

Original languageEnglish (US)
Article number56
JournalAstrophysical Journal
Volume832
Issue number1
DOIs
StatePublished - Nov 20 2016
Externally publishedYes

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luminosity
completeness
star formation
time measurement
slopes
galaxies
stars

Keywords

  • galaxies: evolution
  • galaxies: high-redshift
  • galaxies: luminosity function, mass function

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

THE EVOLUTION of the FAINT END of the UV LUMINOSITY FUNCTION during the PEAK EPOCH of STAR FORMATION (1 < z < 3). / Alavi, Anahita; Siana, Brian; Richard, Johan; Rafelski, Marc; Jauzac, Mathilde; Limousin, Marceau; Freeman, William R.; Scarlata, Claudia; Robertson, Brant E; Stark, Daniel P; Teplitz, Harry I.; Desai, Vandana.

In: Astrophysical Journal, Vol. 832, No. 1, 56, 20.11.2016.

Research output: Contribution to journalArticle

Alavi, A, Siana, B, Richard, J, Rafelski, M, Jauzac, M, Limousin, M, Freeman, WR, Scarlata, C, Robertson, BE, Stark, DP, Teplitz, HI & Desai, V 2016, 'THE EVOLUTION of the FAINT END of the UV LUMINOSITY FUNCTION during the PEAK EPOCH of STAR FORMATION (1 < z < 3)', Astrophysical Journal, vol. 832, no. 1, 56. https://doi.org/10.3847/0004-637X/832/1/56
Alavi, Anahita ; Siana, Brian ; Richard, Johan ; Rafelski, Marc ; Jauzac, Mathilde ; Limousin, Marceau ; Freeman, William R. ; Scarlata, Claudia ; Robertson, Brant E ; Stark, Daniel P ; Teplitz, Harry I. ; Desai, Vandana. / THE EVOLUTION of the FAINT END of the UV LUMINOSITY FUNCTION during the PEAK EPOCH of STAR FORMATION (1 < z < 3). In: Astrophysical Journal. 2016 ; Vol. 832, No. 1.
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AU - Siana, Brian

AU - Richard, Johan

AU - Rafelski, Marc

AU - Jauzac, Mathilde

AU - Limousin, Marceau

AU - Freeman, William R.

AU - Scarlata, Claudia

AU - Robertson, Brant E

AU - Stark, Daniel P

AU - Teplitz, Harry I.

AU - Desai, Vandana

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N2 - We present a robust measurement of the rest-frame UV luminosity function (LF) and its evolution during the peak epoch of cosmic star formation at 1 < z < 3. We use our deep near-ultraviolet imaging from WFC3/UVIS on the Hubble Space Telescope and existing Advanced Camera for Surveys (ACS)/WFC and WFC3/IR imaging of three lensing galaxy clusters, Abell 2744 and MACS J0717 from the Hubble Frontier Field survey and Abell 1689. Combining deep UV imaging and high magnification from strong gravitational lensing, we use photometric redshifts to identify 780 ultra-faint galaxies with MUV < -12.5 AB mag at 1 < z < 3. From these samples, we identified five new, faint, multiply imaged systems in A1689. We run a Monte Carlo simulation to estimate the completeness correction and effective volume for each cluster using the latest published lensing models. We compute the rest-frame UV LF and find the best-fit faint-end slopes of a = -1.56 ± 0.04, α = -1.72 ± 0.04, and α = -1.94 ± 0.06 at 1.0 < z < 1.6, 1.6 < z < 2.2, and 2.2 < z < 3.0, respectively. Our results demonstrate that the UV LF becomes steeper from z ∼ 1.3 to z ∼ 2.6 with no sign of a turnover down to MUV = -14 AB mag. We further derive the UV LFs using the Lyman break dropout selection and confirm the robustness of our conclusions against different selection methodologies. Because the sample sizes are so large and extend to such faint luminosities, the statistical uncertainties are quite small, and systematic uncertainties (due to the assumed size distribution, for example) likely dominate. If we restrict our analysis to galaxies and volumes above >50% completeness in order to minimize these systematics, we still find that the faint-end slope is steep and getting steeper with redshift, though with slightly shallower (less negative) values (a = -1.55 ± 0.06, -1.69 ± 0.07, and -1.79 ± 0.08 for z ∼ 1.3, 1.9, and 2.6, respectively). Finally, we conclude that the faint star-forming galaxies with UV magnitudes of -18.5 < MUV < -12.5 covered in this study produce the majority (55%-60%) of the unobscured UV luminosity density at 1 < z < 3.

AB - We present a robust measurement of the rest-frame UV luminosity function (LF) and its evolution during the peak epoch of cosmic star formation at 1 < z < 3. We use our deep near-ultraviolet imaging from WFC3/UVIS on the Hubble Space Telescope and existing Advanced Camera for Surveys (ACS)/WFC and WFC3/IR imaging of three lensing galaxy clusters, Abell 2744 and MACS J0717 from the Hubble Frontier Field survey and Abell 1689. Combining deep UV imaging and high magnification from strong gravitational lensing, we use photometric redshifts to identify 780 ultra-faint galaxies with MUV < -12.5 AB mag at 1 < z < 3. From these samples, we identified five new, faint, multiply imaged systems in A1689. We run a Monte Carlo simulation to estimate the completeness correction and effective volume for each cluster using the latest published lensing models. We compute the rest-frame UV LF and find the best-fit faint-end slopes of a = -1.56 ± 0.04, α = -1.72 ± 0.04, and α = -1.94 ± 0.06 at 1.0 < z < 1.6, 1.6 < z < 2.2, and 2.2 < z < 3.0, respectively. Our results demonstrate that the UV LF becomes steeper from z ∼ 1.3 to z ∼ 2.6 with no sign of a turnover down to MUV = -14 AB mag. We further derive the UV LFs using the Lyman break dropout selection and confirm the robustness of our conclusions against different selection methodologies. Because the sample sizes are so large and extend to such faint luminosities, the statistical uncertainties are quite small, and systematic uncertainties (due to the assumed size distribution, for example) likely dominate. If we restrict our analysis to galaxies and volumes above >50% completeness in order to minimize these systematics, we still find that the faint-end slope is steep and getting steeper with redshift, though with slightly shallower (less negative) values (a = -1.55 ± 0.06, -1.69 ± 0.07, and -1.79 ± 0.08 for z ∼ 1.3, 1.9, and 2.6, respectively). Finally, we conclude that the faint star-forming galaxies with UV magnitudes of -18.5 < MUV < -12.5 covered in this study produce the majority (55%-60%) of the unobscured UV luminosity density at 1 < z < 3.

KW - galaxies: evolution

KW - galaxies: high-redshift

KW - galaxies: luminosity function, mass function

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