J/MNRAS/514/497 HST/MUSE study of galaxies in Abell 370 (Lagattuta+, 2022)
Pilot-WINGS An extended MUSE view of the structure of Abell 370.
Lagattuta D.J., Richard J., Bauer F.E., Cerny C., Claeyssens A., Guaita L.,
Jauzac M., Jeanneau A., Koekemoer A.M., Mahler G., Prieto Lyon G.,
Acebron A., Meneghetti M., Niemiec A., Zitrin A., Bianconi M., Connor T.,
Cen R., Edge A., Faisst A.L., Limousin M., Massey R., Sereno M., Sharon K.,
Weaver J.R.
<Mon. Not. R. Astron. Soc. 514, 497-517 (2022)>
=2022MNRAS.514..497L 2022MNRAS.514..497L (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxies, group ; Infrared ; Optical ;
Spectroscopy ; Photometry ; Positional data ; Redshifts
Keywords: gravitational lensing: strong - techniques: imaging spectroscopy -
galaxies: clusters: individual: Abell 370 -
galaxies: kinematics and dynamics - dark matter -
large-scale structure of Universe
Abstract:
We investigate the strong-lensing cluster Abell 370 (A370) using a
wide Integral Field Unit (IFU) spectroscopic mosaic from the
Multi-Unit Spectroscopic Explorer (MUSE). IFU spectroscopy provides
significant insight into the structure and mass content of galaxy
clusters, yet IFU-based cluster studies focus almost exclusively on
the central Einstein-radius region. Covering over 14 arcmin2, the new
MUSE mosaic extends significantly beyond the A370 Einstein radius,
providing, for the first time, a detailed look at the cluster
outskirts. Combining these data with wide-field, multi-band Hubble
Space Telescope (HST) imaging from the BUFFALO project, we analyse the
distribution of objects within the cluster and along the line of
sight. Identifying 416 cluster galaxies, we use kinematics to trace
the radial mass profile of the halo, providing a mass estimate
independent from the lens model. We also measure radially averaged
properties of the cluster members, tracking their evolution as a
function of infall. Thanks to the high spatial resolution of our data,
we identify six cluster members acting as galaxy-galaxy lenses, which
constrain localized mass distributions beyond the Einstein radius.
Finally, taking advantage of MUSE's 3D capabilities, we detect and
analyse multiple spatially extended overdensities outside of the
cluster that influence lensing-derived halo mass estimates. We stress
that much of this work is only possible thanks to the robust, extended
IFU coverage, highlighting its importance even in less optically dense
cluster regions. Overall, this work showcases the power of combining
HST + MUSE, and serves as the initial step towards a larger and wider
program targeting several clusters.
Description:
We take the first steps at exploring extended cluster regions with IFU
spectroscopy, using a panoramic (14 arcmin2) mosaic of MUSE data, in
conjunction with multiband HST imaging, to investigate the initial
outskirts region of the first-known lensing cluster: Abell 370. These
efforts are a further continuation of two previous studies, Lagattuta
et al. (2017MNRAS.469.3946L 2017MNRAS.469.3946L, Cat. J/MNRAS/469/3946, L17) and Lagattuta
et al. (2019MNRAS.485.3738L 2019MNRAS.485.3738L, Cat. J/MNRAS/485/3738, L19) which
targeted A370 with narrower MUSE fields, respectively, covering
1 arcmin2 and 4 arcmin2 areas around the established centre. With
this wider data set we are, for the first time, able to diversify our
analysis by characterizing the extended cluster structure and probing
colour variations in cluster members, all while continuing to
investigate the total mass profile and thanks to the 3D capabilities
of MUSE search for additional mass components along the expanded line
of sight. This work, which we are calling Pilot-WINGS also sets the
stage for a larger proposed study BUFFALO-WINGS targeting several
clusters out to still greater radii.
For HST, we use multiband HST data observed survey (Lotz et al.
2017ApJ...837...97L 2017ApJ...837...97L) and its successor BUFFALO project (Steinhardt et
al. 2020ApJS..247...64S 2020ApJS..247...64S). The A370 HFF data consist of 160 HST orbits
in seven broad-bands (F435W, F606W, F814W, F105W, F125W, F140W, and
F160W) and are largely stacked over the field of view of a single
instrumental pointing (ACS for the optical bands and WFC3 for the IR
bands). For its part, take the MUSE data obtained in ESO program used
in L17 and L19 (i.e see Fig 1 of the section 2 for MUSE/HST data sky
coverage). Next, as explained in section 2 we proceed to data
reduction before to construct redshift for a 1186 prior sources
(spectroscopically confirmed), a 59 sources muselet and an 5 sources
extern catalogs using SExtractor method for target detection. Thanks
to SExtractor we also extract a spectrum for each object based on the
segmentation map created in the detection step, (i.e see also section
3.2 Inspection and catalogue creation). We present these results in
the master catalogue tablea1.dat with identification IDs, redshifts
and its quality assessments, HST ACS/WF3 apparent magnitudes.
Objects:
----------------------------------------------------------------------------
RA (ICRS) DE Designation(s)
----------------------------------------------------------------------------
02 39 50.50 -01 35 08.0 Abell 370 = ACT-CL J0239.8-0134
----------------------------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 263 1250 The Abell 370 Pilot-WINGS master data catalogue
containing spectroscopic/photometric and spatial
informations
--------------------------------------------------------------------------------
See also:
J/MNRAS/469/3946 : Abell 370 MUSE redshifts (Lagattuta+, 2017)
J/MNRAS/485/3738 : 3D structure in the A370 MUSE Mosaic (Lagattuta+, 2019)
J/A+A/646/A83 : 12 massive lensing clusters MUSE observations
(Richard+, 2021)
J/MNRAS/492/503 : Magnifications in the Hubble Frontier Fields (Raney+, 2020)
J/ApJ/868/129 : Lensing analysis in Abell 370 (Strait+, 2018)
J/MNRAS/371/703 : MILES library of empirical spectra (Sanchez-Blazquez+, 2006)
J/ApJS/199/25 : CLASH sources for MACS1149.6+2223 (Postman+, 2012)
https://archive.stsci.edu/hlsp/buffalo : Buffalo data access
https://astro.dur.ac.uk/~hbpn39/pilot-wings.html : Abell 370 Pilot-WINGS data
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- ID Numerical identifier from SExtractor for each
galaxy (iden) (1)
7- 13 A7 --- IDfrom An indication of how the object was detected
(idfrom) (2)
15- 18 A4 --- Field The data set containing the galaxy (Field) (3)
20- 37 F18.15 deg RAdeg Right Ascension aligned to Gaia DR2 world
coordinate system (J2000) (RA)
39- 57 F19.16 deg DEdeg Declination aligned to Gaia DR2 world
coordinate system (J2000) (DEC)
59- 78 E20.17 --- z The measured redshift of each galaxy (z)
80 I1 --- q_z An assessment of the reliability of the
redshift measurement from low q_z = 1 to high
q_z = 3 (zconf) (4)
82- 91 F10.6 mag F435Wmag ?=99.99 The measured apparent AB magnitude in
the given HST F435W-band (F435W) (5)
93-105 E13.10 mag e_F435Wmag []?=99.99 The measured uncertainty of
F435Wmag (F435W_err)
107-116 F10.6 mag F606Wmag ?=99.99 The measured apparent AB magnitude in
the given HST F606W-band (F606W) (5)
118-129 E12.10 mag e_F606Wmag []?=99.99 The measured uncertainty of
F606Wmag (F606W_err)
131-140 F10.6 mag F814Wmag ?=99.99 The measured apparent AB magnitude in
the given HST F814W-band (F814W) (5)
142-153 E12.10 mag e_F814Wmag []?=99.99 The measured uncertainty of
F814Wmag (F814W_err)
155-164 F10.6 mag F105Wmag ?=99.99 The measured apparent AB magnitude in
the given HST F105W-band (F105W) (5)
166-178 E13.10 mag e_F105Wmag []?=99.99 The measured uncertainty of
F105Wmag (F105W_err)
180-189 F10.6 mag F125Wmag ?=99.99 The measured apparent AB magnitude in
the given HST F125W-band (F125W) (5)
191-203 E13.10 mag e_F125Wmag []?=99.99 The measured uncertainty of
F125Wmag (F125W_err)
205-214 F10.6 mag F140Wmag ?=99.99 The measured apparent AB magnitude in
the given HST F140W-band (F140W) (5)
216-228 E13.10 mag e_F140Wmag []?=99.99 The measured uncertainty of
F140Wmag (F140W_err)
230-239 F10.6 mag F160Wmag ?=99.99 The measured apparent AB magnitude in
the given HST F60W-band (F160W) (5)
241-253 E13.10 mag e_F160Wmag []?=99.99 The measured uncertainty of
F160Wmag (F160W_err)
255-263 A9 --- MULID If the object is part of a multiply-imaged
system it gives a unique identifier for each
image (MUL) (6)
--------------------------------------------------------------------------------
Note (1): Firstly, while individual ID numbers can be repeated between objects
in different datasets or detection methods, a given
(ID + IDfrom + Field) combination is entirely unique for all galaxies
in the catalogue.
Note (2): Secondly, the IDfrom gives an indication of how the object was
detected as follows:
PRIOR = Sources are identified in broadband (HST) images,
1186 sources in our sample
MUSELET = Sources are only seen in the MUSE data,
59 sources in our sample
EXTERN = objects are manually added to the catalogue, in cases
where an object is known but not detected by either method,
e.g a member of a multiply-imaged system that is very faint
or highly contaminated by a bright neighbour,
5 sources in our sample
Note (3): Thirdly, the Field gives the data set containing the galaxy as shown
in the Fig. 1 Data of the Abell 370 of the section 2 as follows:
CORE = Objects are located in the core region of the cluster,
561 sources in our sample
P01 = Objects are located in the 01 shallower outskirt cluster
region, 68 sources in our sample
P02 = Objects are located in the 02 shallower outskirt cluster
region, 73 sources in our sample
P03 = Objects are located in the 03 shallower outskirt cluster
region, 73 sources in our sample
P04 = Objects are located in the 04 shallower outskirt cluster
region, 87 sources in our sample
P05 = Objects are located in the 05 shallower outskirt cluster
region, 68 sources in our sample
P06 = Objects are located in the 06 shallower outskirt cluster
region, 61 sources in our sample
P07 = Objects are located in the 07 shallower outskirt cluster
region, 86 sources in our sample
P08 = Objects are located in the 08 shallower outskirt cluster
region, 39 sources in our sample
P09 = Objects are located in the 09 shallower outskirt cluster
region, 69 sources in our sample
P10 = Objects are located in the 10 shallower outskirt cluster
region, 65 sources in our sample
Note (4): Based on work described in the section 3, the q_z quality measurements
are classified as follows:
1 = The redshift is based on a single ambiguous or low-SNR emission
line, or several low SNR absorption features,
190 sources in our sample
2 = The redshift is based on a single emission line without
additional information, several moderate S/N absorption features,
or a q_z = 1 detection case whose redshift confidence is
increased by the identification of a multiply-imaged system,
204 sources in our sample
3 = The redshift is based on multiple clear spectral features, or
on a single high S/N emission line with additional information,
e.g. an obvious asymmetry in the line profile or aclear
non-detection in HST bands bluewards of the line,
856 sources in our sample
Note (5): Magnitudes that appear as negative numbers are non-detections and
should be treated as upper-limits on the flux estimate.
Note (6): Numbering is taken from the lensing catalogue presented in
Lagattuta et al. 2019MNRAS.485.3738L 2019MNRAS.485.3738L, Cat. J/MNRAS/485/3738.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 31-Mar-2025