J/MNRAS/474/3700 Gravitational lens candidates models (Kung+, 2018)
Models of gravitational lens candidates from Space Warps CFHTLS.
Kung R., Saha P., Ferreras I., Baeten E., Coles J., Cornen C.,
Macmillan C., Marshall P., More A., Oswald L., Verma A., Wilcox J.K.
<Mon. Not. R. Astron. Soc., 474, 3700-3713 (2018)>
=2018MNRAS.474.3700K 2018MNRAS.474.3700K (SIMBAD/NED BibCode)
ADC_Keywords: Gravitational lensing ; Models
Keywords: gravitational lensing: strong - galaxies: general -
galaxies: stellar content - dark matter
Abstract:
We report modelling follow-up of recently discovered
gravitational-lens candidates in the Canada France Hawaii Telescope
Legacy Survey. Lens modelling was done by a small group of specially
interested volunteers from the Space Warps citizen-science
community who originally found the candidate lenses. Models are
categorized according to seven diagnostics indicating (a) the image
morphology and how clear or indistinct it is, (b) whether the mass map
and synthetic lensed image appear to be plausible, and (c) how the
lens-model mass compares with the stellar mass and the
abundance-matched halo mass. The lensing masses range from ∼1011 to
>1013M{sun|. Preliminary estimates of the stellar masses show a
smaller spread in stellar mass (except for two lenses): a factor of a
few below or above ∼1011M☉. Therefore, we expect the
stellar-to-total mass fraction to decline sharply as lensing mass
increases. The most massive system with a convincing model is
J1434+522 (SW 05). The two low-mass outliers are J0206-095
(SW 19) and J2217+015 (SW 42); if these two are indeed lenses,
they probe an interesting regime of very low star formation
efficiency. Some improvements to the modelling software
(SpaghettiLens), and discussion of strategies regarding scaling to
future surveys with more and frequent discoveries, are included.
Description:
We report on a first set of mass distributions and follow-up
diagnostics for the Space Warps lens candidates created with a novel
approach that aims to be scalable by orders of magnitude to prepare
for the many thousands of lenses the next generation of wide-field
surveys will yield (e.g. Euclid and WFIRST).
Table 1 is a summary of our results. It characterizes each modelled
system with seven diagnostics, indicating (a) the image morphology and
how clear or indistinct it is, (b) whether the mass map and synthetic
lensed image appear to be plausible, and (c) how the model mass
compares with the estimated stellar and full-halo masses. Missing
entries are due unavailable imaging data, whereas missing rows are due
to models that were not created for this particular candidate.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 160 59 Diagnostics of the selected models for each
Space Warps candidate (see Section 6)
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- SWID SW designation, SWNN,
[MVM2016] SWNN in Simbad
6- 15 A10 --- ZooID Zoo designation
17- 32 A16 --- CFHTLS CFHTLS designation (JHHMMSS.s+DDMMSS)
34- 37 F4.2 --- zlens ?=- Lens redshift
39 A1 --- Unbled [Y-N] Unblended image
41 A1 --- Alldis [Y-N] All images discernible
43 A1 --- Isolens [Y-N] Isolated lens
45- 46 A2 --- Mtype Image morphology (1)
48 A1 --- SyntI [Y-N] Synthetic image reasonable
50 A1 --- Mmap [Y-N] Mass map reasonable
52- 61 E10.5 [Msun] log10Mstel ? Stellar mass
63- 72 E10.5 [Msun] log10Mlens ? Lens mass
74- 78 F5.3 --- H ? Halo-matching index H
80- 89 E10.5 Msun Mstel ? Stellar mass
91-100 E10.5 Msun Mlens ? Lens mass
102-111 E10.5 Msun Mmoster ? Moster et al. (2010ApJ...710..903M 2010ApJ...710..903M) mass
113-122 E10.5 Msun Mstel-yr ? Stellar mass yr
(not explained in the paper)
124-133 E10.5 Msun Mstel-sr ? Stellar mass sr
(not explained in the paper)
135-144 E10.5 Msun Mlens-min ? Minimum lens mass
146-155 E10.5 Msun Mlens-max ? Maximum lens mass
157-160 F4.2 arcsec REins ? Einstein radius
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Note (1): Image morphology code as follows:
D = source at larger transverse distance tend to produce doubles
Q = source close to being dead-centre behind a lens tend to produce quads
LQ = source is inferred as displaced along the long axis of the lens
SQ = displaced along the short axis
IQ = inclined to both axes
CQ = only very little or no displacement is evident
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 26-Feb-2021