J/PASJ/70/S10 GOLDRUSH I. UV magnitudes (Ono+, 2018)
Great Optically Luminous Dropout Research Using Subaru HSC (GOLDRUSH).
I. UV luminosity functions at z∼4-7 derived with the half-million dropouts on
the 100 deg2 sky.
Ono Y., Ouchi M., Harikane Y., Toshikawa J., Rauch M., Yuma S., Sawicki M.,
Shibuya T., Shimasaku K., Oguri M., Willott C., Akhlaghi M., AkiyamaI M.,
Coupon J., Kashikawa N., Komiyama Y., Konno A., Lin L., Matsuoka Y.,
Miyazaki S., Nagao T., Nakajima K., SilvermaniJ., Tanaka M., Taniguchi Y.,
Wang S.-Y.
<Publ. Astron. Soc. Jap., 70, S10 (2018)>
=2018PASJ...70S..10O 2018PASJ...70S..10O (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, photometry ; Photometry, ultraviolet ; Redshifts
Keywords: galaxies: formation - galaxies: evolution - galaxies: high-redshift
Abstract:
We study the UV luminosity functions (LFs) at z∼4, 5, 6, and 7 based
on the deep large-area optical images taken by the Hyper Suprime-Cam
(HSC) Subaru Strategic Program (SSP). On the 100 deg2 sky of the HSC
SSP data available to date, we take enormous samples consisting of a
total of 579565 dropout candidates at z∼4-7 by the standard color
selection technique, 358 out of which are spectroscopically confirmed
by our follow-up spectroscopy and other studies. We obtain UV LFs at
z∼4-7 that span a very wide UV luminosity range of
∼0.002-100L*UV(-26<MUV←14mag) by combining LFs from our
program and the ultra-deep Hubble Space Telescope legacy surveys. We
derive three parameters of the best-fit Schechter function, Φ*,
MUV, and α, of the UV LFs in the magnitude range where the
active galactic nucleus (AGN) contribution is negligible, and find
that and Φ* decrease from z∼4 to 7 with no significant
evolution of MUV. Because our HSC SSP data bridge the LFs of
galaxies and AGNs with great statistical accuracy, we carefully
investigate the bright end of the galaxy UV LFs that are estimated by
the subtraction of the AGN contribution either aided by spectroscopy
or the best-fit AGN UV LFs. We find that the bright end of the galaxy
UV LFs cannot be explained by the Schechter function fits at >2σ
significance, and require either double power-law functions or
modified Schechter functions that consider a magnification bias due to
gravitational lensing.
Description:
In this study, we use early data products of the HSC SSP that were
obtained in 2014-2016 (Aihara et al., 2018PASJ...70S...8A 2018PASJ...70S...8A).
Specifically, we use the internal data release of S16A, where
additional data taken in 2016 January-April have been merged with
the version of Public Data Release 1.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table4.dat 84 358 Spectroscopically identified galaxies and AGNs
in our dropout samples
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Type [Galaxies AGNs] Type
10- 12 A3 --- --- [HSC]
14- 27 A14 --- HSC HSC designation (JHHMMSS+DDMMSS)
29- 30 I2 h RAh Right ascension (J2000.0)
32- 33 I2 min RAm Right ascension (J2000.0)
35- 39 F5.2 s RAs Right ascension (J2000.0)
41 A1 --- DE- Declination sign (J2000.0)
42- 43 I2 deg DEd Declination (J2000.0)
45- 46 I2 arcmin DEm Declination (J2000.0)
48- 52 F5.2 arcsec DEs Declination (J2000.0)
54- 58 F5.3 --- zsp Spectroscopic redshift
60- 63 F4.1 mag UVmag Apparent UV magnitude
65- 69 F5.1 mag UVMAG Absolute UV magnitude
71 I1 --- Sample [1/4] Sample (1)
73 I1 --- Flag [1/2] Galaxy/AGN flag (1 = galaxy; 2 = AGN)
75- 84 A10 --- r_zsp Reference for spectroscopic redshift (2)
--------------------------------------------------------------------------------
Note (1): The dropout sample in which the source is selected, as follows:
1 = g-dropout
2 = r-dropout
3 = i-dropout
4 = z-dropout
Note (2): References as follows:
S08 = Saito et al. (2008ApJ...675.1076S 2008ApJ...675.1076S)
O08 = Ouchi et al. (2008, Cat. J/ApJS/176/301)
W10 = Willott et al. (2010AJ....140..546W 2010AJ....140..546W)
C12 = Curtis-Lake et al. (2012MNRAS.422.1425C 2012MNRAS.422.1425C)
Mas12 = Masters et al. (2012, Cat. J/ApJ/755/169)
M12 = Mallery et al. (2012, Cat. J/ApJ/760/128)
W13 = Willott et al. (2013AJ....145....4W 2013AJ....145....4W)
L13 = Le Fevre et al. (2013A&A...559A..14L 2013A&A...559A..14L)
K15 = Kashikawa et al. (2015ApJ...798...28K 2015ApJ...798...28K)
Kr15 = Kriek et al. (2015ApJS..218...15K 2015ApJS..218...15K)
W16 = Wang et al. (2016, Cat. J/ApJ/819/24)
T16 = Toshikawa et al. (2016, Cat. J/ApJ/826/114)
Mo16 = Momcheva et al. (2016ApJS..225...27M 2016ApJS..225...27M)
M16 = Matsuoka et al. (2016ApJ...828...26M 2016ApJ...828...26M)
P17 = Paris et al. (2017A&A...597A..79P 2017A&A...597A..79P, Cat. VII/279)
T17 = Tasca et al. (2017, Cat. J/A+A/600/A110)
Y17 = Yang et al. (2017AJ....153..184Y 2017AJ....153..184Y)
Mas17 = Masters et al. (2017, Cat. J/ApJ/841/111)
M17 = Matsuoka et al. (2018PASJ...70S..35M 2018PASJ...70S..35M)
S17 = Shibuya et al. (2018PASJ,,,70S..15S)
H17 = R. Higuchi et al. (in preparation)
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 11-Feb-2019