J/A+A/686/A4 Powerful lens galaxy cluster PLCK G287.0+32.9 (D'Addona+, 2024)
The powerful lens galaxy cluster PLCK G287.0+32.9 (thetaE∼43").
Redshift catalog and new lens model using MUSE observations.
D'Addona M., Mercurio A., Rosati P., Grillo C., Caminha G., Acebron A.,
Angora G., Bergamini P., Bozza V., Granata G., Annunziatella M.,
Gargiulo A., Gobat R., Tozzi P., Girardi M., Lombardi M., Meneghetti M.,
Schipani P., Tortorelli L., Vanzella E.
<Astron. Astrophys. 686, A4 (2024)>
=2024A&A...686A...4D 2024A&A...686A...4D (SIMBAD/NED BibCode)
ADC_Keywords: Gravitational lensing ; Clusters, galaxy ; Spectroscopy ;
Redshifts
Keywords: gravitational lensing: strong - galaxies: clusters: general -
galaxies: clusters: individual: PLCK G287.0+32.9 - dark matter
Abstract:
We present a new high-precision strong-lensing model of PLCK
G287.0+32.9, a massive lens galaxy cluster at z=0.383, with the
aim of obtaining an accurate estimation of its effective Einstein
radius and total mass distribution. We also present a spectroscopic
catalog containing accurate redshift measurements for close to 500
objects up to redshift z=6, including multiply lensed sources
and cluster member galaxies.
We exploited high-quality spectroscopic data from the Multi Unit
Spectroscopic Explorer (MUSE), covering a central 3arcmin2 region
of the cluster. We supplemented the spectroscopic catalog by including
redshift measurements from VIsible MultiObject Spectrograph (VIMOS)
and DEep Imaging Multi-Object Spectrograph (DEIMOS). We identified 129
spectroscopic cluster member galaxies with redshift values of
0.360≤z≤0.405, and mF160W≤21. We complemented this galaxy cluster
member sample with 24 photometric members identified with a
convolutional neural network (CNN) approach. We also identified 114
multiple images from 28 background sources, of which 84 images from 16
sources are new and the remaining ones have already been identified in
previous works. From these, we extracted 'golden sample' of 47
secure multiple images and used them, together with the selected
cluster member, to build and optimize several strong-lensing models
with the software lenstool.
The best-fitting lens model shows a root mean square (RMS) separation
value between the predicted and observed positions of the multiple
images of 0.75". Using its predictive power, we found three new
multiple images and we confirm the configuration of three systems of
multiple images that were not used for the optimization of the model.
For a source at a redshift of zs=2, we found a cluster with an
Einstein radius of thetaE=43.4±0.1". This value is in
agreement with previous estimates and corresponds to a total mass
enclosed in the critical curve of
ME=3.33-0.07+0.02x1014M☉.
The combined application of ancillary Hubble Space Telescope (HST)
imaging, VIMOS and DEIMOS data, and the new MUSE spectroscopic
observations allowed us to build a new lens model of the galaxy
cluster PLCK G287.0+32.9, with an improvement in terms of
reconstructing the observed positions of the multiple images of a
factor of 2.5 with respect to previous models. The derived total mass
distribution confirms this cluster to be a very prominent
gravitational lens, with an effective Einstein radius of
thetaE∼43". We were also able to construct an extensive
spectroscopic catalog containing 490 objects, of which 153 are bright
cluster members with mF160W≤21, and 114 are multiple images.
Description:
We present a new high-precision strong lensing model of
PLCK G287.0+32.9, a massive lens galaxy cluster at z=0.383. We exploit
high-quality spectroscopic data from the Multi Unit Spectroscopic
Explorer (MUSE), redshift measurements from VIsible Multi-Object
Spectrograph (VIMOS) and DEep Imaging Multi-Object Spectrograph
(DEIMOS), and ancillary Hubble Space Telescope (HST) imaging. We
identify 124+24 spectroscopic+photometric member galaxies, 114
multiple images from 28 multiply-lensed background sources (of which
84 images from 16 sources are new and the remaining ones were
previously identified in Zitrin et al. (2017ApJ...839L..11Z 2017ApJ...839L..11Z, Cat.
J/ApJ/839/L11). We extract a Golden Sample of 47 secure multiple
images that we use to build and optimize out strong lensing model
using the pipeline lenstool (Kneib et al., 1996ApJ...471..643K 1996ApJ...471..643K), Jullo
et al., 2007NJPh....9..447J 2007NJPh....9..447J, Jullo & Kneib (2009MNRAS.395.1319J 2009MNRAS.395.1319J).
This catalog contains spectroscopic redshifts for more than 600
objects from MUSE observations of the galaxy cluster PLCK G287.0+32.9
(P.I.: Amata Mercurio, ESO program 0102.A-0640(A)): spectra have been
extracted with python-spex and the redshifts have been measured using
pandora.ez v3.1.10761. For objects outside the area covered by MUSE,
redshift measurements are taken from observations made with VIMOS
(P.I.: Mario Nonino, period 094.A-0529(B)) and DEIMOS (Golovich et
al., 2019ApJS..240...39G 2019ApJS..240...39G, Cat. J/ApJS/240/39 and 2019ApJ...882...69G 2019ApJ...882...69G,
Cat. J/ApJ/882/69). Cluster members having a Kron magnitude in HST
WFC3 band F160W≤21 are also reported: spectroscopic members have been
selected using the redshift interval 0.360-0.405, while photometric
members have been identified using the Convolutional Neural Network
technique from Angora et al., 2020A&A...643A.177A 2020A&A...643A.177A, Cat.
J/A+A/643/A177.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablec1.dat 89 148 Catalog of multiple images
tabled1.dat 45 153 Selected galaxy cluster members catalog
tablee1.dat 169 639 Full spectroscopic redshifts catalog
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See also:
https://github.com/mauritiusdadd/python-specex : python-specex
https://pandora.lambrate.inaf.it : pandora.ez
https://projets.lam.fr/projects/lenstool : lenstool
Byte-by-byte Description of file: tablec1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Name Names of the multiple images (1)
8- 11 I4 --- ID ?=-99 The unique ID of the objects
13- 22 F10.6 deg RAdeg Right ascension (ICRS, J2000)
24- 33 F10.6 deg DEdeg Delcination (ICRS, J2000)
35- 42 F8.4 --- zspec ?=-99 Spectroscopic redshift (2)
44- 46 I3 --- QF [1/9]?=-99 Redshift quality flag (3)
48 A1 --- GOLD Golden Sample flag (4)
50- 53 F4.2 --- zmodel ? Redshift from the lens model (5)
55 A1 --- --- [(]
56- 59 F4.2 --- b_zmodel ? Redshift from the lens model
16th percentile (5)
60 A1 --- --- [-]
61- 64 F4.2 --- B_zmodel ? Redshift from the lens model
84th percentile (5)
65 A1 --- --- [)]
67- 72 A6 --- Arc-ID Image name (6)
74- 77 F4.2 --- zphot ? Photometric redshift (6)
79 A1 --- --- [(]
80- 83 F4.2 --- b_zphot ? Photometric redshift 16th percentile (6)
84 A1 --- --- [-]
85- 88 F4.2 --- B_zphot ? Photometric redshift 84th percentile (6)
89 A1 --- --- [)]
--------------------------------------------------------------------------------
Note (1): The names of multiple images in column NAME are in the format X.Yk,
where X indicates the multiply-lensed background source, Y indicates
the clump/substructure and k differentiates among the various
counter-images. -99 when no name.
Note (2): Objects without a redshift measurement either are outside the area
covered by MUSE or the Signal-to-Noise ration of their spectra is too
low to measure the redshift.
Note (3): QF values meaning as follows:
1 = UNCERTAIN (do not trust these values)
2 = LIKELY (∼80% reliability)
3 = SECURE (100% reliability)
9 = SINGLE-LINE (>90% reliability)
Note (4): GOLD values meaning as follows:
y = the image has been used to optimize the cluster lens model
Note (5): zmodel reports the median redshift z estimated using the best
fitting lens model, along with the 16th and 84th percentiles.
Note (6): Columns Arc-ID, zphot, b_zphot and B_zphot are taken, for comparison,
from Zitrin et al., 2027, Cat. J/ApJ/839/L11
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tabled1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- ID The unique ID of the objects
6- 16 F11.7 deg RAdeg Right ascension (ICRS, J2000)
18- 28 F11.7 deg DEdeg Delcination (ICRS, J2000)
30 A1 --- Source [mvdc] Origin membership identification (1)
32- 39 F8.4 --- zspec ?=-99 Spectroscopic redshift
41- 45 F5.2 mag F160Wmag Kron magnitude in HST-WFC3 band F160W
--------------------------------------------------------------------------------
Note (1): SOURCE values meaning as follows:
m = MUSE [85 objects]
v = VLT-VIMOS [ 9 objects]
d = KECK-DEIMOS [35 objects]
c = CNN [24 objects]
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablee1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- ID The unique ID of the objects
6- 16 F11.7 deg RAdeg Right ascension (ICRS, J2000)
18- 28 F11.7 deg DEdeg Delcination (ICRS, J2000)
30 A1 --- Source [mvd] Origin of the redshift estimation (1)
32- 39 F8.4 --- zspec Spectroscopic redshift
41- 43 I3 --- QF [1/9] Redshift quality flag (2)
45-169 A125 --- Comments Comments (3)
--------------------------------------------------------------------------------
Note (1): SOURCE values meaning as follows:
m = MUSE [581 objects]
v = VLT-VIMOS [ 11 objects]
d = KECK-DEIMOS [ 47 objects]
Note (2): QF values meaning as follows:
1 = UNCERTAIN (do not trust these values) [ 57 objects]
2 = LIKELY (∼80% reliability) [ 44 objects]
3 = SECURE (100% reliability) [402 objects]
9 = SINGLE-LINE (>90% reliability) [136 objects]
Note (3): contains information on visible emission or absorption lines,
the presence of contamination, etc.
--------------------------------------------------------------------------------
History:
From Maurizio D'Addona, mdaddona(at)unisa.it
Acknowledgements:
This work is based on observations taken by the RELICS Treasury
Program (GO 14096) with the NASA/ESA HST, which is operated by the
Association of Universities for Research in Astronomy, Inc., under
NASA contract NAS5-26555. Based on observations collected at the
European Southern Observatory under ESO programme(s) 0102.A-0640(A)
and/or data obtained from the ESO Science Archive Facility with DOI(s)
under https://doi.org/10.18727/archive/41. We acknowledge financial
support through grants PRIN-MIUR 2017WSCC32 and 2020SKSTHZ.
AM acknowledges financial support through grant NextGenerationEU" RFF
M4C2 1.1 PRIN 2022 project 2022ZSL4BL INSIGHT. AA has received funding
from the European Union's Horizon 2020 research and innovation
programme under the Marie Sklodowska-Curie grant agreement No
101024195 - ROSEAU.
The data published in this paper have been obtained using the
pandora.ez software developed by INAF IASF-Milano. This research made
use of Photutils, an Astropy package for the detection and photometry
of astronomical sources (Bradley et al., 2023,
https://github.com/astropy/photutils).
(End) Patricia Vannier [CDS] 05-Feb-2024