J/ApJ/862/156 High-z galaxy candidates in the HFF cluster fields (Leung+, 2018)
Magnification bias of distant galaxies in the Hubble Frontier Fields: testing
wave versus particle dark matter predictions.
Leung E., Broadhurst T., Lim J., Diego J.M., Chiueh T., Schive H.-Y.,
Windhorst R.
<Astrophys. J., 862, 156 (2018)>
=2018ApJ...862..156L 2018ApJ...862..156L
ADC_Keywords: Clusters, galaxy; Gravitational lensing; Galaxies, photometry;
Redshifts; Photometry, HST; Photometry, infrared; Ultraviolet
Keywords: cosmology: observations ; dark matter ; galaxies: abundances ;
galaxies: evolution ; galaxies: high-redshift ;
gravitational lensing: strong
Abstract:
Acting as powerful gravitational lenses, the strong lensing galaxy
clusters of the deep Hubble Frontier Fields (HFF) program permit
access to lower-luminosity galaxies lying at higher redshifts than
hitherto possible. We analyzed the HFF to measure the volume density
of Lyman-break galaxies at z>4.75 by identifying a complete and
reliable sample up to z∼10. A marked deficit of such galaxies was
uncovered in the highly magnified regions of the clusters relative to
their outskirts, implying that the magnification of the sky area
dominates over additional faint galaxies magnified above the flux
limit. This negative magnification bias is consistent with a slow
rollover at the faint end of the UV luminosity function and it
indicates a preference for Bose-Einstein condensate dark matter with a
light boson mass of mB∼10-22eV over standard cold dark matter. We
emphasize that measuring the magnification bias requires no correction
for multiply-lensed images (with typically three or more images per
source), whereas directly reconstructing the luminosity function will
lead to an overestimate unless such images can be exhaustively matched
up, especially at the faint end that is only accessible in the
strongly lensed regions. In addition, we detected a distinctive
downward transition in galaxy number density at z≳8, which may be
linked to the relatively late reionization reported by Planck. Our
results suggests that JWST will likely peer into an "abyss" with
essentially no galaxies detected in deep NIR imaging at z>10.
Description:
We analyzed all of the 12 completed fields of the HFF program,
comprising six pairs of cluster field and a parallel "blank" (or
control) field. Seven HST bandpass filters spanning from optical (with
ACS/WFC) to near-IR (with WFC3/IR) were employed in the observations,
with a total of up to 140 HST orbits devoted to each pair of cluster
and parallel fields. The 5σ point-source limiting AB magnitude
reached for each cluster and its accompanying parallel field is
∼28.6-29.1.
Throughout this research, we adopted the standard cosmological
parameters in concordance cosmology for distance determinations,
i.e., ΩM=0.3, ΩΛ=0.7, and H0=70km/s/Mpc.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table11.dat 113 679 Detailed information of individual galaxy candidates
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See also:
VII/4 : Abell and Zwicky Clusters of Galaxies (Abell+ 1974)
VII/110 : Rich Clusters of Galaxies (Abell+ 1989)
J/ApJS/150/1 : VV29 and NGC 4676 HST photometry (Benitez+, 2004)
J/AJ/132/926 : Galaxies in the Hubble Ultra Deep Field (Coe+, 2006)
J/ApJS/199/25 : CLASH sources for MACS1149.6+2223 (Postman+, 2012)
J/MNRAS/432/2696 : Galaxy luminosity function at z = 7-9 (McLure+, 2013)
J/ApJ/793/115 : UV-continuum slopes beta for z∼4-8 galaxies (Bouwens+, 2014)
J/MNRAS/444/268 : HST Frontier Fields clusters (Richard+, 2014)
J/ApJ/803/34 : z∼4-10 galaxies from HST legacy fields (Bouwens+, 2015)
J/ApJ/810/71 : UV mag of cand. galaxies at 3~<z~<8.5 (Finkelstein+, 2015)
J/MNRAS/452/1437 : Abell 2744 strong-lensing analysis (Jauzac+, 2015)
J/ApJ/819/114 : Strong lensing mass modeling of 4 HFF cl. (Kawamata+, 2016)
J/A+A/600/A90 : MACS J0416.1-2403 redshift catalogue (Caminha+, 2017)
J/ApJ/835/113 : Gal. ≳6 from the Hubble Frontier Fields (Livermore+, 2017)
Byte-by-byte Description of file: table11.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Cluster HFF target cluster
10- 17 A8 --- Type Field type ("cluster" or "parallel"=control)
19- 21 I3 --- ID [1/112] Galaxy ID
23- 33 F11.7 deg RAdeg Right Ascension, decimal degrees (J2000)
35- 45 F11.7 deg DEdeg Declination, decimal degrees (J2000)
47- 51 F5.3 --- zphot [4.7/9.9] Bayesian Photometric redshift
53- 57 F5.3 --- e_zphot [0.03/7] Lower uncertainty,
95% confidence interval (1)
59- 63 F5.3 --- E_zphot [0.03/3.5] Upper uncertainty,
95% confidence interval (1)
65- 69 F5.2 mag omag [24/28.5] Observed AB magnitude in Filt
71- 74 F4.2 mag e_omag [0.01/3.2] Uncertainty in omag
76- 80 A5 --- Filt HFF Filter (F105W (Y), F814W (I), F125W (J),
F140W (JH) or F160W (H))
82- 82 A1 --- u_mu Uncertainty flag on mu
84- 89 F6.2 --- mu [1/100] Magnification factor (2)
91- 96 F6.2 --- e_mu [0.1/100]? Uncertainty in mu (3)
98-103 F6.2 mag UVMag [-22.5/-14.4] Inferred UV 1500Å absolute
AB magnitude (4)
105-108 F4.2 mag e_UVMag [0.02/1.5] Lower uncertainty in UVMag
110-113 F4.2 mag E_UVMag [0.02/2.5] UPper uncertainty in UVMag
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Note (1): For the A370 cluster and parallel fields, the uncertainties in
photometric redshifts are assumed to be 0.05(1+zphot), i.e. 5% errors.
Note (2): For the cluster fields, the magnification values were computed
from the free-form lens models described in Section 3 using Equation
(1), assuming the quoted zphot estimates.
Note (3): Magnification uncertainties were assumed to be 10% if mu(lens)<10
as are usually obtained in the low-mu regime. In contrast, when the
galaxies are fairly close to the model critical curves, i.e. mu(lens)≳10,
we roughly estimated the magnification uncertainties to be
emu(lens)~µ0_(1"/θ)2∼0.01mu(lens)2. On the other hand,
we assumed a fiducial 5% magnification throughout all the parallel
fields (i.e. mu(fiducial)=1.05), considering that they would not be
completely free of any lensing effect from their cluster counterparts.
Note (4): Determined using Equation (8), with uncertainties estimated by
taking into account the uncertainties in the photo-z's (e_zphot)
(both explicitly through Equation (8) and implicitly through the
magnification factor mu(theta,z), the UV continuum slope B(z,MUV), and the
luminosity distance DL(z)), the uncertainties in the apparent magnitudes
(e_omag), and the systematic uncertainties in the magnification
factors (e_mu).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 31-Jul-2019