TY - JOUR
T1 - UVUDF
T2 - UV Luminosity Functions at the Cosmic High Noon
AU - Mehta, Vihang
AU - Scarlata, Claudia
AU - Rafelski, Marc
AU - Gburek, Timothy
AU - Teplitz, Harry I.
AU - Alavi, Anahita
AU - Boylan-Kolchin, Michael
AU - Finkelstein, Steven
AU - Gardner, Jonathan P.
AU - Grogin, Norman
AU - Koekemoer, Anton
AU - Kurczynski, Peter
AU - Siana, Brian
AU - Codoreanu, Alex
AU - De Mello, Duilia F.
AU - Lee, Kyoung Soo
AU - Soto, Emmaris
N1 - Publisher Copyright:
© 2017. The American Astronomical Society. All rights reserved.
PY - 2017/3/20
Y1 - 2017/3/20
N2 - We present the rest-1500 Å UV luminosity functions (LF) for star-forming galaxies during the cosmic high noon- the peak of cosmic star formation rate at 1.5 < z < 3. We use deep NUV imaging data obtained as part of the Hubble Ultra-Violet Ultra Deep Field (UVUDF) program, along with existing deep optical and NIR coverage on the HUDF. We select F225W, F275W, and F336W dropout samples using the Lyman break technique, along with samples in the corresponding redshift ranges selected using photometric redshifts, and measure the rest-frame UV LF at z ∼ 1.7, 2.2, 3.0, respectively, using the modified maximum likelihood estimator. We perform simulations to quantify the survey and sample incompleteness for the UVUDF samples to correct the effective volume calculations for the LF. We select galaxies down to MUV = -15.9, -16.3, -16.8 and fit a faint-end slope of α = -1.20-0.13+0.10,-1.32+0.100.14, 1.39+0.08-0.12 at 1.4 < z < 1.9, 1.8 < z < 2.6, and 2.4 < z < 3.6, respectively. We compare the star formation properties of z ∼ 2 galaxies from these UV observations with results from Hα and UV +IR observations. We find a lack of high-SFR sources in the UV LF compared to the Hα and UV+IR, likely due to dusty SFGs not being properly accounted for by the generic IRX-β relation used to correct for dust. We compute a volume-averaged UV-to-Hα ratio by abundance matching the rest-frame UV LF and Hα LF. We find an increasing UV-to-Hα ratio toward low-mass galaxies (M∗ ≲ 5 ×109 M⊙). We conclude that this could be due to a larger contribution from starbursting galaxies compared to the high-mass end.
AB - We present the rest-1500 Å UV luminosity functions (LF) for star-forming galaxies during the cosmic high noon- the peak of cosmic star formation rate at 1.5 < z < 3. We use deep NUV imaging data obtained as part of the Hubble Ultra-Violet Ultra Deep Field (UVUDF) program, along with existing deep optical and NIR coverage on the HUDF. We select F225W, F275W, and F336W dropout samples using the Lyman break technique, along with samples in the corresponding redshift ranges selected using photometric redshifts, and measure the rest-frame UV LF at z ∼ 1.7, 2.2, 3.0, respectively, using the modified maximum likelihood estimator. We perform simulations to quantify the survey and sample incompleteness for the UVUDF samples to correct the effective volume calculations for the LF. We select galaxies down to MUV = -15.9, -16.3, -16.8 and fit a faint-end slope of α = -1.20-0.13+0.10,-1.32+0.100.14, 1.39+0.08-0.12 at 1.4 < z < 1.9, 1.8 < z < 2.6, and 2.4 < z < 3.6, respectively. We compare the star formation properties of z ∼ 2 galaxies from these UV observations with results from Hα and UV +IR observations. We find a lack of high-SFR sources in the UV LF compared to the Hα and UV+IR, likely due to dusty SFGs not being properly accounted for by the generic IRX-β relation used to correct for dust. We compute a volume-averaged UV-to-Hα ratio by abundance matching the rest-frame UV LF and Hα LF. We find an increasing UV-to-Hα ratio toward low-mass galaxies (M∗ ≲ 5 ×109 M⊙). We conclude that this could be due to a larger contribution from starbursting galaxies compared to the high-mass end.
KW - galaxies: evolution
KW - galaxies: high-redshift
KW - galaxies: luminosity function, mass function
KW - galaxies: star formation
UR - http://www.scopus.com/inward/record.url?scp=85016571086&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85016571086&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/aa6259
DO - 10.3847/1538-4357/aa6259
M3 - Article
AN - SCOPUS:85016571086
SN - 0004-637X
VL - 838
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 29
ER -