J/MNRAS/446/683 Free-form lensing grid solution for A1689 (Diego+, 2015)
A free-form lensing grid solution for A1689 with new multiple images.
Diego J.M., Broadhurst T., Benitez N., Umetsu K., Coe D., Sendra I.,
Sereno M., Izzo L., Covone G.
<Mon. Not. R. Astron. Soc., 446, 683-704 (2015)>
=2015MNRAS.446..683D 2015MNRAS.446..683D (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Gravitational lensing ; Redshifts
Keywords: methods: data analysis - galaxies: clusters: general -
galaxies: clusters: individual: A1689 - dark matter
Abstract:
We examine Abell 1689 non-parametrically, combining strongly lensed
Hubble Space Telescope images and weak distortions from wider
field Subaru imaging. Our model incorporates member galaxies to
improve the lens solution. By adding luminosity-scaled member galaxy
deflections to our smooth grid, we can derive meaningful solutions
with sufficient accuracy to permit the identification of our own
strongly lensed images, so our model becomes self-consistent. We
identify 11 new multiply lensed system candidates and clarify
previously ambiguous cases, in the deepest optical and near-infrared
data to date from Hubble and Subaru. Our improved spatial
resolution brings up new features not seen when the weak and strong
lensing effects are used separately, including clumps and filamentary
dark matter around the main halo. Our treatment means we can obtain an
objective mass ratio between the cluster and galaxy components. We
find a typical mass-to-light ratios of M/LB=21±14 inside the
r<1arcmin region. Our model independence means we can objectively
evaluate the competitiveness of stacking cluster lenses for defining
the geometric lensing-distance-redshift relation in a
model-independent way.
Description:
In this paper, we used public imaging data obtained from the ACS
(filters: F450W and F814W) and the WFC3 (filter F125W), retrieved from
the Mikulski Archive for Space Telescope. The data come from two
different programmes. The F814W (ACS) and F125W (WFC3) data were
obtained within the HST programme 11718 (PI Blakeslee, Cycle 17), from
2010 May 29 to July 8, while the ACS F475W images were obtained within
the programme 9289 (PI Fors, Cycle 11) on 2002 June 16. The total
exposure time is 9500, 75172 and 14367s in the F450W, F814W and F125W
filters, respectively.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 63 165 *Strong lensing (SL) data set
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Note on tablea1.dat: Cut-outs from these images together with additional
information like the magnitudes of the new systems can be found on this
website http://max.ifca.unican.es/diego/FigsA1689/. Also on the same website,
there is a file with useful comments from the referee based on a comparison
between our solution and the model of Limousin et al. (2007,
Cat. J/ApJ/668/643).
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See also:
J/ApJ/621/53 : Multiple arc systems in A1689 (Broadhurst+, 2005)
J/ApJ/668/643 : Multiply imaged gravitational lens systems (Limousin+, 2007)
J/ApJ/723/1678 : LensPerfect A1689 analysis (Coe+, 2010)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/165] Sequential number
4 A1 --- n_Seq [a-n] Note on Seq (1)
6- 9 F4.1 --- ID New system ID following the original notation
of Broadhurst et al. (2005, Cat. J/ApJ/621/53)
10 A1 --- m_ID [a-c] Multiplicity index on ID
12- 15 F4.1 --- B05 ? Original notation (Broadhurst et al. 2005,
Cat. J/ApJ/621/53) (2)
17- 19 A3 --- Ref Previous papers in the literature where that
system was identified (3)
21- 22 I2 h RAh Right ascension (J2000) (4)
24- 25 I2 min RAm Right ascension (J2000) (4)
27- 32 F6.3 s RAs Right ascension (J2000) (4)
34 A1 --- DE- Declination sign (J2000) (4)
35 I1 deg DEd Declination (J2000) (4)
37- 38 I2 arcmin DEm Declination (J2000) (4)
40- 45 F6.3 arcsec DEs Declination (J2000) (4)
47 A1 --- n_z [p] p indicates photometry redshift
48- 51 F4.2 --- z Spectroscopic or photometric (n_z = p)
redshift (5)
53- 57 F5.2 arcsec Dbeta Δβ value derived from our reference
model, see equation (5) of the paper (6)
59- 63 F5.2 arcsec Dtheta Distance between the observed and predicted
positions, Δθ, derived from our
reference model
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Note (1): Notes as follows:
a = System has been re-organized, System 12 in Limousin et al.
(2007, Cat. J/ApJ/668/643)
b = System has been re-organized, System 12 in Limousin et al.
(2007, Cat. J/ApJ/668/643)
c = System 31 in Limousin et al. (2007, Cat. J/ApJ/668/643)
d = System 31 in Limousin et al. (2007, Cat. J/ApJ/668/643)
e = System has been re-organized. New arclet candidate
f = New arclet candidate not used in our primary analysis
g = Original arclet not used in our analysis
h = Original arclet not used in our analysis. Multiple possibilities for
this arclet..
i = New arclet not used in our analysis. Multiple possibilities for this
arclet. 33.2 in Limousin et al. (2007, Cat. J/ApJ/668/643).
Discard (Wrong colour, too bright)..
j = New arclet not used in our primary analysis. Multiple possibilities for
this arclet..
k = New arclet not used in our primary analysis
l = Multiple possibilities for this arclet
m = Multiple possibilities for this arclet
n = 25.2 in Broadhurst et al. (2005, Cat. J/ApJ/621/53)
Note (2): Systems not present in the original paper are left blank.
Note (3): References as follows:
B05 = Broadhurst et al. (2005, Cat. J/ApJ/621/53)
L07 = Limousin et al. (2007, Cat. J/ApJ/668/643)
C10 = Coe et al. (2010, Cat. J/ApJ/723/1678)
D14 = this paper
Note (4): Coordinates of each arclet. Discrepancies with some of the positions
published in Coe et al. (2010, Cat. J/ApJ/723/1678) are corrected in the
present version of the table.
Note (5): redshifts used in our study and are taken from Coe et al.
(2010, Cat. J/ApJ/723/1678). New systems in this work are all assumed to
have z = 2.
Note (6): The standard lens equation is
β=θ-α(θ,S(θ)),
where θ is the observed position of the source, α is the
deflection angle, S(θ) is the surface mass density of the cluster at
the position θ and β is the position of the background source.
The δβ, for a specific arclet i is defined as :
Δβi=|βi-<β>|,
where βi is the predicted position of the arclet in the source plane
when the reference solution is used and <β> is the average of all the
βi for that system.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 29-Jan-2018