shaded regions) adopted for the surface brightness modelling. The residual
maps show the contours of available high-resolution multiwavelength data taken
at two levels corresponding to $\textit{SNR}=5$ and 10 (thick curves), and
five uniformly spaced levels between the $\textit{SNR}=10$ and the maximum SNR
in the multiwavelength image (thin black curves). The images are oriented such
that N is up and E is to the left.

###  4.4 Properties of the lenses

Since $\sim 47\%$ of the modelled lensing galaxies are composed of multiple
components, it is necessary to use a set of parameters that describes the
global properties of the surface brightness distribution and does not depend
on the number and type of components used to model the galaxy. We therefore
use the total effective radius $R_{50}$ (i.e., the radius and surface
brightness of the circularised isophote that contains half of the light of the
galaxy), total effective surface brightness $\mu_{50}$, and total magnitude
$m_{F110W}$. For each galaxy, we sampled $10^{4}$ different combinations of
its components to take into account the uncertainties of the best-fitting
model of the surface brightness distribution. This is done through a set of
truncated normal distributions (one for each component parameter) with central
value being the best-fitting value from the surface brightness model, standard
deviation the uncertainty of the best-fitting value, and ranges $[0,\infty)$
ADU pixel-1, $[0,\infty)$ pixel, $[0.3,10]$, $[0,1]$, and $[0,360]$ deg for
$\mu_{\rm e}$, $R_{\rm e}$, $n$, $q$, and PA, respectively. For all the
combinations, we estimate $R_{50}$ by computing the curve of growth (COG) and
retrieving the radius within which half of the total flux is encircled. The
$\mu_{50}$ value is derived from the surface brightness profile at $R_{50}$,
while the $m_{F110W}$ value is obtained by summing the luminosities of all the
components. For each parameter, we calculate the median and the 16% and 84%
percentiles from the cumulative distribution function. Additionally, we
estimate the $C_{31}=R_{75}/R_{25}$ concentration index (e.g. Watkins et al.,
2022) in order to compare our results with the literature. To derive the
distributions of $R_{25}$ and $R_{75}$, which correspond to the radii
containing 25% and 75% of the total luminosity, respectively, we apply the
same procedure as done for $R_{50}$.

For the edge-on lenses of S_5, S_46, S_53, and S_62, we run ISOFIT on the
model image (Fig. 8) after having deconvolved it with the PSF, and then we use
the result to produce the COG. We also measure the surface brightness radial
profile. We use the COG to estimate the values of $R_{25}$, $R_{50}$, and
$R_{75}$ and to assess their uncertainties, we build a set of $10^{4}$ COGs
for each galaxy. We sample the flux within each circularised radius with a
Gaussian distribution centred on the measured flux value and with standard
deviation being the flux Poisson uncertainty. The circularised radius is
sampled with a Gaussian distribution centred on the measured radius value and
with standard deviation being the uncertainty on the ellipticity as measured
by ISOFIT. We use the surface radial profile to estimate the values of
$\mu_{50}$, and to assess its uncertainty, we build a set of 104 surface
brightness radial profiles. At each radius, we adopt a Gaussian distribution
centred on the measured value of surface brightness, with standard deviation
being the uncertainty measured by ISOFIT.

In Fig. 9, we show the $C_{31}$ distribution of our lenses. The peak at
$C_{31}\simeq 7$ is due to the systems that we model with a de Vaucouleurs
profile and have all the same concentration. We measure a median $\langle
C_{31}\rangle=6.8\pm 0.4$, which is slightly higher than the median value
$\langle C_{31}\rangle=5.2\pm 0.1$ measured by Watkins et al. (2022) for a
sample of nearby ETGs observed with Spitzer at 3.6 $\mu$m. This finding and
the observed morphology of smooth and featureless elliptical systems provide
further evidence that our lenses are mostly ETGs. Lastly, we measure the flux
densities at 1.1 $\mu$m $S_{1.1}$ of the background sources by taking the
aperture photometry in the regions dominated by the lensing features on the
lens subtracted residuals. The uncertainties $\sigma_{S_{1.1}}$ are computed
with $\sigma_{S_{1.1}}^{2}=\sum_{i,j}\sigma_{i,j}^{2}$, where $\sigma_{i,j}$
is the noise map. The values of $S_{1.1}$ and their uncertainties are given in
Tables 8 and 15.

Figure 9: Distribution of the total effective radii $R_{50,0}$ (top left
panel), total effective surface brightnesses $\mu_{50,0}$ (top central panel),
concentrations $C_{31}$ (top right panel), total absolute magnitudes
$M_{F110W}$ (bottom left panel), redshifts $z_{\rm l}$ of the foreground
lenses (bottom central panel), and redshifts $z_{\rm s}$ of the background
sources (bottom right panel). All the foreground lenses and background sources
with a measured redshift are included. The orange line corresponds to the
median of the values of $C_{31}$ of the ETGs sample of Watkins et al. (2022),
while the orange shaded region marks the corresponding $\pm 1\sigma$
confidence interval.

For the 68 lensing foreground galaxies with known photometric or spectroscopic
redshift, we convert the size of the total effective radius from arcsec to kpc
through the angular diameter distance and the total magnitude to absolute
magnitude $M_{F110W}$ through the luminosity distance. We also correct the
total effective surface brightness for cosmological dimming by multiplying the
F110W fluxes by a factor of $(1+z)^{4}$. This is done for the parameter
distributions as derived before. To take into account the uncertainties on the
photometric redshifts, we sample a truncated normal distribution centred on
the redshift measurement, with standard deviation being the uncertainty and
range $[0,\infty)$. When more than one potential lens is present (i.e. for
type 2 and 3 systems), we correct for the redshift only if the secondary
potential lens has a spectroscopic redshift (S_8, S_11, S_15, and S_36) or
none of the lenses dominates the available photometric redshift (S_23, S_28,
and S_33). To denote the parameters corrected for the lens redshifts, we add a
subscript ‘0’. In Table 8, we list the measured values of $m_{F110W}$,
$M_{F110W}$, $R_{50}$, $R_{50,0}$, $\mu_{50}$, $\mu_{50,0}$, and $C_{31}$ for
the five representative systems shown in Fig. 8, while in Table 15 we show the
parameters for the rest of the sample.

Table 8: Derived properties of five representative lensing systems.

No. | IAU Name | $m_{F110W}$ | $\mu_{\rm 50}$ | $R_{\rm 50}$ | $C_{31}$ | $\mu S_{1.1}$
---|---|---|---|---|---|---
|  | [mag] |  [mag arcsec-2] | [arcsec] |  |  [$\mu$Jy]
|  | $M_{F110W}$ | $\mu_{\rm 50,\,0}$ | $R_{\rm 50,\,0}$ |  |
|  | [mag] |  [mag kpc-2] | [kcp] |  |
(1) | (2) | (3) | (4) | (5) | (6) | (7)
S_12 | HERMESJ100144$+$025709 | $19.17^{+0.08}_{-0.08}$ | $21.74^{+0.05}_{-0.05}$ | $0.64^{+0.02}_{-0.02}$ | $9.37^{+0.20}_{-0.20}$ | $10.14^{+0.17}_{-0.17}$
$-20.17^{+0.08}_{-0.08}$ | $18.96^{+0.05}_{-0.05}$ | $5.10^{+0.13}_{-0.13}$
S_11 | HATLASJ083051$+$0132251 | $21.54^{+0.18}_{-0.18}$ | $22.60^{+0.13}_{-0.12}$ | $0.33^{+0.02}_{-0.02}$ | $8.47^{+0.66}_{-0.64}$ | $6.79^{+0.11}_{-0.11}$
$-16.86^{+0.18}_{-0.18}$ | $20.48^{+0.13}_{-0.12}$ | $2.30^{+0.13}_{-0.13}$
HATLASJ083051$+$0132252 | $22.05^{+0.21}_{-0.19}$ | $23.28^{+0.15}_{-0.13}$ | $0.48^{+0.03}_{-0.03}$ | $3.21^{+0.16}_{-0.15}$
$-17.59^{+0.21}_{-0.20}$ | $20.27^{+0.15}_{-0.13}$ | $3.94^{+0.26}_{-0.25}$
S_8 | HERSJ020941.2$+$0015581 | $16.15^{+0.18}_{-0.17}$ | $21.27^{+0.19}_{-0.17}$ | $2.47^{+0.13}_{-0.12}$ | $5.35^{+0.45}_{-0.47}$ | $18.72^{+0.34}_{-0.34}$
$-19.38^{+0.18}_{-0.17}$ | $20.47^{+0.19}_{-0.17}$ | $8.48^{+0.46}_{-0.40}$
HERSJ020941.2$+$0015582 | $19.82^{+0.09}_{-0.09}$ | $20.49^{+0.06}_{-0.06}$ | $0.310^{+0.010}_{-0.009}$ | $5.24^{+0.10}_{-0.10}$
$-15.71^{+0.09}_{-0.09}$ | $19.69^{+0.06}_{-0.06}$ | $1.06^{+0.03}_{-0.03}$
S_5 | HELMSJ005841.2$-$011149 | $18.910^{+0.001}_{-0.001}$ | $20.26^{+0.02}_{-0.02}$ | $0.478^{+0.005}_{-0.006}$ | $3.05^{+0.04}_{-0.04}$ | $14.55^{+0.10}_{-0.10}$
$-18.15^{+0.57}_{-0.48}$ | $18.88^{+0.25}_{-0.24}$ | $2.54^{+0.31}_{-0.35}$
S_50 | HERMESJ021831$-$053131 | $21.55^{+0.19}_{-0.18}$ | $23.60^{+0.13}_{-0.12}$ | $0.51^{+0.03}_{-0.03}$ | $8.95^{+0.71}_{-0.69}$ | $<0.04$
$-18.89^{+0.19}_{-0.18}$ | $19.89^{+0.13}_{-0.12}$ | $4.40^{+0.27}_{-0.26}$

Notes: Col. (1): Source reference number. Col. (2): IAU name of the Herschel
detection. Indices 1 and 2 refer to the two components of the lens candidate.
Col. (3): Apparent magnitude of the model (first row), absolute magnitude of
the model (second row). Col. (4): Total effective radius in arcsec (first row)
and in kpc (second row). Col. (5): Total effective surface brightness before
(first row) and after correcting for cosmological dimming (second row). Col.
(6): Concentration index of the model.

Figure 9 shows the distribution of $R_{50,0}$ in kpc, $\mu_{50,0}$ in mag
arcsec-2, $C_{31}$, $M_{F110W}$ in mag, $z_{\rm l}$ and $z_{\rm s}$. For each
parameter, we stack all the single-system parameter distributions to take into
account the varying uncertainties between different systems. We bin them
together and normalised for the total number of realisations (i.e., $10^{4}$
for each system).

##  5 Lens modelling

For the 34 systems for which we can confidently identify a galaxy acting as
the main lens and the background source in the HST images, we proceed to
estimate the Einstein radius $\theta_{E}$ from the residual images. Depending
on the morphology of the lensing features, we define $\theta_{\rm E}$ as
either the radius of the circle centred on the lens that best fits the
Einstein ring (e.g., S_4), or as half of the separation between the multiple
images (e.g., S_2) following the approach of Amvrosiadis et al. (2018). For
the uncertainty on $\theta_{\rm E}$, we adopt the value corresponding to one-
third of the observed width of the lensing feature. We use these rough
estimates as priors for proper lens modelling.

The lens modelling is performed with PyAutoLens111111PyAutoLens is available
from https://github.com/Jammy2211/PyAutoLens (Nightingale et al., 2018, 2021),
by using a non-linear search trough dynesty (Speagle, 2020)121212dynesty is
available from https://dynesty.readthedocs.io/en/stable/. In order to reduce
the complexity of the lens model, we adopt a singular isothermal ellipsoid
(SIE) for the mass model (see Nightingale et al. 2018 for details). It has
five free parameters, the differences $\delta x_{\rm SIE}$ and $\delta y_{\rm
SIE}$ of the centre coordinates of the mass distribution relative to the
centre coordinates of the lens surface brightness, Einstein radius
$\theta_{\rm E}$, and elliptical components $\epsilon_{\rm SIE,1}=f_{\rm
SIE}\sin(2PA_{\rm SIE})$, $\epsilon_{\rm SIE,2}=f_{\rm SIE}\cos(2PA_{\rm
SIE})$, where $f_{\rm SIE}=(1-q_{\rm SIE})/(1+q_{\rm SIE})$, $PA_{\rm SIE}$ is
the position angle of the mass profile, and $q_{\rm SIE}$ is its flattening.

From the lens-subtracted images and noise maps as obtained in Sec. 4, we set
up the inputs for the lens modelling. We crop the images and we mask the
regions that do not include lensing features in order to reduce the
computation time. To this aim we also crop the PSF to $\sim 5\,{\rm
FWHM}\times\,5\,{\rm FWHM}$ cutouts. We then mask any residual from the lens
subtraction and non-modelled nearby contaminants. We estimate the position of
the lensing features by locating the brightest pixel in $5\,{\rm
pixel}\times\,5\,{\rm pixel}$ boxes encompassing the lensing features. These
estimates are used by PyAutoLens to constrain the location of the background
source in the source plane (see Nightingale et al. 2018 for details).

We proceed with the lens modelling with the following approach. First, we
perform a parametric fit by fitting both the mass model and background source
with parametric functions. We use a single Sérsic component for the parametric
background source. This fit has a total of twelve free parameters: five for
the mass model and seven for the background source. The priors for the mass
model are a Gaussian distribution centred on the cutout centre with
$\sigma=0.1$ arcsec for $\delta x_{\rm SIE}$ and $\delta y_{\rm SIE}$; a
Gaussian distribution centred on the estimated $\theta_{\rm E}$ with $\sigma$
three times its error; a Gaussian distribution centred on 0 with $\sigma=0.3$
for $\epsilon_{\rm SIE,1}$ and $\epsilon_{\rm SIE,2}$, respectively. The
priors for the background source are Gaussian distribution centred on the
cutout centre with $\sigma=0.3$ arcsec for $x_{\rm s}$ and $y_{\rm s}$; a log-
uniform distribution between $10^{-6}$ ADU and $10^{6}$ ADU for
$I_{\rm{s,eff}}$; a uniform distribution between 0 arcsec and 30 arcsec for
$R_{\rm{s,eff}}$; a uniform distribution between 0.8 and 5.0 for $n_{\rm s}$;
a Gaussian distribution centred on 0 with $\sigma=0.3$ for $\epsilon_{\rm
s,1}$ and $\epsilon_{\rm s,2}$ (defined in a similar way as $\epsilon_{\rm
SIE,1}$ and $\epsilon_{\rm SIE,2}$), respectively. As position threshold, we
use a Gaussian distribution centred on the previously identified position with
$\sigma=0.5$ arcsec for all the systems, except for S_41. For the latter, we
adopt $\sigma=0.1$ due to the small angular separation of the lensed images.
We then use the posteriors of the mass model obtained in this parametric fit
and the priors on the position of the background sources on the image plane to
initialize a Voronoi pixelization with a constant regularization coefficient
$\lambda$ (see Nightingale et al. 2018 for details). For the pixelization, we
use as priors a uniform distribution between 20 and 45 pixels for the shape of
the pixelization and a log-uniform distribution between $10^{-6}$ and $10^{6}$
for $\lambda$. We do this pixelized initialization fit by marginalizing the
lens model over the mass model and only fitting the pixelization. In a similar
fashion, we marginalize over the resulting pixelization to fit the mass model
with priors defined by the parametric fit posteriors. We consider this fit as
the best guess for the lens model and source reconstruction.

In the cases of S_6, S_11, S_22, S_24, S_27, and S_31 the SNR of the
background lensed sources is not high enough to produce reliable results. S_2,
S_5, S_25, and S_41 show very complex and/or clumpy lensed background source
morphologies that needed additional information on what is part of the
background source or additional multiple images. Whereas, S_26 shows residuals
related to the lens subtraction that prevent us from building the model. For
S_3, S_19, S_40, the SIE mass model is not sufficient to correctly reproduce
the observations, so we add a shear component, defined, as for the mass model,
through the elliptical components $\epsilon_{\rm shear,\,1}$ and
$\epsilon_{\rm shear,\,2}$. This is done to improve the mass model and not to
model an actual external shear (see Etherington et al. 2023 for details). The
priors for the shear elliptical components are uniform distributions between
$-0.2$ and $0.2$.

For each modelled lens, we extract 500 fits from the lens modelling parameters
posteriors, and, for each fit, we compute the regions of the source plane with
$\textit{SNR}>3$. We compute the magnification by taking the ratio between the
fluxes of the regions on the source plane and the image plane after mapping
them back. We measure the sizes of the source plane by computing the radii of
the circularised regions that we used to compute the magnifications. The
distribution of the physical sizes of our systems is shown in Fig. 10. As
before, the results of the lens modelling for S_7 are shown in Fig. 11, while
the results for the remaining lenses are reported in Table 9 and Fig. 29.

Table 9: Results of the lens modelling.

No. | IAU name | $\delta x$ | $\delta y$ | $\theta_{E}$ | $q$ | $PA$ | $\epsilon_{shear,\,1}$ | $\epsilon_{shear,\,2}$ | $x_{\rm pix}$ | $y_{\rm pix}$ | $\lambda$ | $\mu$ | $R_{\rm bkg,\,circ}$ | $\kappa_{0}$ |
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---
|  | [arcsec] | [arcsec] | [arcsec] |  |  |  |  |  |  |  |  | [arcsec] | [] |
|  | $\delta x_{0}$ | $\delta y_{0}$ | $\theta_{E,\,0}$ |  |  |  |  |  |  |  |  | $R_{\rm bkg,\,circ,\,0}$ | $M$ | $M/L$
|  | [kpc] | [kpc] | [kpc] |  |  |  |  |  |  |  |  | [kpc] |  [$10^{11}$ M⊙] |
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13) | (14) | (15) | (16)
S_1 | HATLASJ000330.6$-$321136 | $-0.13^{+0.03}_{-0.02}$ | $-0.05^{+0.01}_{-0.02}$ | $0.733^{+0.006}_{-0.009}$ | $0.85\pm 0.03$ | $80.11^{+3.78}_{-10.85}$ | – | – | $39^{+3}_{-9}$ | $33^{+8}_{-7}$ | $0.0101^{+0.0011}_{-0.0009}$ | $5.48^{+0.62}_{-0.48}$ | $0.052^{+0.006}_{-0.004}$ | $1.68^{+0.03}_{-0.04}$ | –
$-0.65^{+0.19}_{-0.16}$ | $-0.24^{+0.08}_{-0.12}$ | $3.85^{+0.61}_{-0.85}$ |  |  |  |  |  |  |  |  | $0.41^{+0.04}_{-0.03}$ | $0.92^{+0.23}_{-0.28}$ | $2.93^{+1.65}_{-0.98}$
S_3 | HELMSJ001353.5$-$060200 | $-0.038^{+0.004}_{-0.003}$ | $0.066^{+0.004}_{-0.006}$ | $0.658^{+0.004}_{-0.003}$ | $0.85^{+0.03}_{-0.04}$ | $-49.56^{+8.51}_{-8.32}$ | $0.017^{+0.008}_{-0.010}$ | $0.191\pm 0.009$ | $40\pm 4$ | $31\pm 9$ | $0.0084\pm 0.0006$ | $10.37^{+0.47}_{-0.56}$ | $0.052\pm 0.002$ | $1.49^{+0.02}_{-0.01}$ | –
$-0.26^{+0.05}_{-0.04}$ | $0.45^{+0.07}_{-0.08}$ | $4.56^{+0.50}_{-0.74}$ |  |  |  |  |  |  |  |  | $0.45\pm 0.02$ | $1.48^{+0.52}_{-0.44}$ | $4.19^{+3.00}_{-1.48}$
S_4 | HELMSJ003619.8$+$002420 | $-0.015^{+0.002}_{-0.001}$ | $0.122^{+0.001}_{-0.002}$ | $1.9349^{+0.0017}_{-0.0008}$ | $0.813^{+0.001}_{-0.003}$ | $-79.38^{+0.23}_{-0.21}$ | – | – | $36$ | $40$ | $0.0164^{+0.0009}_{-0.0008}$ | $15.82^{+1.23}_{-0.72}$ | $0.143^{+0.006}_{-0.008}$ | $12.16\pm 0.3$ | –
$-0.063^{+0.007}_{-0.005}$ | $0.504^{+0.006}_{-0.008}$ | $7.977^{+0.007}_{-0.004}$ |  |  |  |  |  |  | $1.25^{+0.06}_{-0.07}$ | $5.234\pm 0.001$ | $3.40^{+0.68}_{-0.54}$ |  |
S_7 | HERSJ012620.5$+$012950 | $-0.006^{+0.015}_{-0.007}$ | $0.14^{+0.01}_{-0.02}$ | $0.766\pm 0.004$ | $0.60^{+0.07}_{-0.03}$ | $52.13^{+0.85}_{-0.58}$ | – | – | $31^{+4}_{-0}$ | $40^{+4}_{-7}$ | $0.0114\pm 0.0006$ | $5.19^{+0.56}_{-0.20}$ | $0.142^{+0.003}_{-0.010}$ | $1.73^{+0.02}_{-0.01}$ | –
$-0.04^{+0.08}_{-0.04}$ | $0.79^{+0.09}_{-0.13}$ | $4.44^{+0.28}_{-0.32}$ |  |  |  |  |  |  |  |  | $1.23^{+0.03}_{-0.08}$ | $1.32^{+0.18}_{-0.17}$ | $2.36^{+0.73}_{-0.54}$
S_8 | HERSJ020941.2$+$001558 | $-0.259^{+0.005}_{-0.010}$ | $0.046^{+0.008}_{-0.002}$ | $2.579^{+0.002}_{-0.003}$ | $0.704^{+0.003}_{-0.004}$ | $-10.81^{+0.55}_{-0.21}$ | – | – | $43$ | $43$ | $0.0093\pm 0.0004$ | $7.29^{+0.30}_{-0.10}$ | $0.158\pm 0.003$ | $18.61^{+0.08}_{-0.19}$ | –
$-0.89^{+0.02}_{-0.03}$ | $0.159^{+0.028}_{-0.006}$ | $8.844^{+0.007}_{-0.011}$ |  |  |  |  |  |  |  |  | $1.30\pm 0.03$ | $5.99^{+0.03}_{-0.06}$ | $4.96^{+0.95}_{-0.77}$
S_9 | HERMESJ032637$-$270044 | $0.024^{+0.009}_{-0.013}$ | $-0.12\pm 0.01$ | $0.981^{+0.005}_{-0.006}$ | $0.87\pm 0.01$ | $-40.54^{+1.64}_{-2.25}$ | – | – | $42^{+0}_{-9}$ | $28^{+11}_{-5}$ | $0.0110^{+0.0010}_{-0.0009}$ | $6.15^{+0.32}_{-0.38}$ | $0.072\pm 0.004$ | $3.01^{+0.03}_{-0.04}$ | –
– | – | – |  |  |  |  |  |  |  |  | – | – | –
S_10 | HERMESJ033732$-$295353 | $0.1754^{+0.0007}_{-0.0005}$ | $0.0576^{+0.0012}_{-0.0008}$ | $1.9718^{+0.0003}_{-0.0006}$ | $0.6495^{+0.0003}_{-0.0006}$ | $-80.49^{+0.04}_{-0.15}$ | – | – | $41$ | $38$ | $0.0057^{+0.0002}_{-0.0003}$ | $6.27^{+0.50}_{-0.05}$ | $0.0801^{+0.0045}_{-0.0002}$ | $11.662^{+0.004}_{-0.007}$ | –
$0.57^{+0.11}_{-0.12}$ | $0.18^{+0.04}_{-0.05}$ | $6.40^{+1.18}_{-1.30}$ |  |  |  |  |  |  |  |  | – | – | –
S_12 | HERMESJ100144$+$025709 | $-0.033^{+0.003}_{-0.004}$ | $0.042^{+0.009}_{-0.003}$ | $0.930\pm 0.002$ | $0.686^{+0.006}_{-0.008}$ | $-16.66^{+0.39}_{-0.56}$ | – | – | $33^{+11}_{-10}$ | $30^{+9}_{-0}$ | $0.0076^{+0.0004}_{-0.0003}$ | $6.33^{+0.15}_{-0.17}$ | $0.094^{+0.002}_{-0.001}$ | $2.63\pm 0.02$ | –
$-0.26^{+0.02}_{-0.03}$ | $0.34^{+0.08}_{-0.02}$ | $7.44^{+0.02}_{-0.01}$ |  |  |  |  |  |  |  | – | – | – |
S_13 | HERMESJ103827$+$581544 | $0.228^{+0.016}_{-0.006}$ | $0.27\pm 0.01$ | $2.408\pm 0.010$ | $0.582\pm 0.007$ | $-70.47^{+0.76}_{-0.47}$ | – | – | $44$ | $44$ | $0.025\pm 0.002$ | $4.29^{+0.15}_{-0.25}$ | $0.17^{+0.02}_{-0.01}$ | $15.68\pm 0.4$ | –
$1.56^{+0.11}_{-0.04}$ | $1.84^{+0.09}_{-0.10}$ | $16.47\pm 0.07$ |  |  |  |  |  |  |  | – | – | – |
S_14 | HERMESJ110016$+$571736 | $-0.324^{+0.007}_{-0.009}$ | $-0.251^{+0.007}_{-0.011}$ | $1.081\pm 0.003$ | $0.71\pm 0.01$ | $11.63^{+1.13}_{-0.88}$ | – | – | $32^{+5}_{-7}$ | $42^{+1}_{-0}$ | $0.0151^{+0.0008}_{-0.0009}$ | $2.43^{+0.03}_{-0.04}$ | $0.211^{+0.004}_{-0.006}$ | $3.56\pm 0.02$ | –
$-2.48^{+0.05}_{-0.07}$ | $-1.92^{+0.05}_{-0.08}$ | $8.28^{+0.02}_{-0.03}$ |  |  |  |  |  |  |  |  | $1.84^{+0.04}_{-0.06}$ | $5.39^{+0.03}_{-0.04}$ | $1.95^{+0.10}_{-0.09}$
S_16 | HATLASJ125126$+$254928 | $-0.40\pm 0.02$ | $0.056^{+0.009}_{-0.014}$ | $1.133^{+0.016}_{-0.007}$ | $0.58^{+0.01}_{-0.02}$ | $20.05^{+2.41}_{-3.88}$ | – | – | $39\pm 3$ | $37^{+5}_{-9}$ | $0.015\pm 0.002$ | $5.10^{+0.37}_{-0.67}$ | $0.052^{+0.006}_{-0.005}$ | $3.73^{+0.13}_{-0.04}$ | –
$-2.75^{+0.24}_{-0.23}$ | $0.38^{+0.08}_{-0.09}$ | $7.94^{+0.50}_{-0.66}$ |  |  |  |  |  |  |  |  | $0.39\pm 0.04$ | $3.20^{+0.45}_{-0.46}$ | $3.29^{+1.07}_{-0.72}$
S_17 | HATLASJ125760$+$224558 | $0.104^{+0.012}_{-0.007}$ | $-0.06^{+0.01}_{-0.04}$ | $0.681^{+0.005}_{-0.006}$ | $0.70^{+0.07}_{-0.02}$ | $60.10^{+1.21}_{-2.50}$ | – | – | $38$ | $43$ | $0.0059\pm 0.0004$ | $4.46^{+0.56}_{-0.52}$ | $0.081^{+0.006}_{-0.005}$ | $1.41^{+0.04}_{-0.03}$ | –
$0.69^{+0.08}_{-0.04}$ | $-0.40^{+0.08}_{-0.30}$ | $4.52^{+0.03}_{-0.04}$ |  |  |  |  |  |  |  |  | $0.70^{+0.05}_{-0.04}$ | $1.43^{+0.22}_{-0.13}$ | $1.74^{+0.28}_{-0.17}$
S_18 | HATLASJ133008$+$245860 | $0.037^{+0.003}_{-0.010}$ | $-0.287^{+0.010}_{-0.005}$ | $1.037^{+0.001}_{-0.002}$ | $0.616^{+0.009}_{-0.007}$ | $-14.02^{+0.61}_{-0.43}$ | – | – | $39^{+2}_{-5}$ | $36^{+7}_{-5}$ | $0.0084\pm 0.0006$ | $12.31^{+1.10}_{-0.72}$ | $0.055\pm 0.003$ | $3.184^{+0.009}_{-0.008}$ | –
$0.21^{+0.02}_{-0.06}$ | $-1.65^{+0.06}_{-0.03}$ | $5.974^{+0.009}_{-0.011}$ |  |  |  |  |  |  |  |  | $0.43\pm 0.02$ | $1.990^{+0.006}_{-0.005}$ | $3.47^{+1.14}_{-0.80}$
S_19 | HATLASJ133846$+$255057 | $0.0905^{+0.0005}_{-0.0028}$ | $-0.1092^{+0.0001}_{-0.0008}$ | $0.6697^{+0.0004}_{-0.0002}$ | $0.895^{+0.002}_{-0.011}$ | $79.56^{+0.59}_{-0.58}$ | $0.281^{+0.008}_{-0.001}$ | $-0.0560^{+0.0024}_{-0.0002}$ | $42$ | $41$ | $0.0046^{+0.0003}_{-0.0002}$ | $3.78^{+0.04}_{-0.02}$ | $0.0963^{+0.0006}_{-0.0008}$ | $1.706^{+0.012}_{-0.002}$ | –
$0.51^{+0.07}_{-0.08}$ | $-0.63^{+0.10}_{-0.08}$ | $3.83^{+0.48}_{-0.62}$ |  |  |  |  |  |  |  |  | $0.80\pm 0.03$ | $1.12\pm 0.26$ | $7.95^{+3.82}_{-2.14}$
S_21 | HERMESJ171451$+$592634 | $-0.23^{+0.05}_{-0.01}$ | $0.21^{+0.03}_{-0.01}$ | $0.976^{+0.006}_{-0.007}$ | $0.72\pm 0.02$ | $-76.63^{+1.34}_{-0.90}$ | – | – | $42^{+1}_{-6}$ | $35^{+5}_{-2}$ | $0.012\pm 0.001$ | $8.40^{+5.93}_{-6.00}$ | $0.053^{+0.053}_{-0.009}$ | $2.46^{+0.02}_{-0.01}$ | –
$-2.01^{+0.39}_{-0.09}$ | $1.80^{+0.27}_{-0.09}$ | $8.35^{+0.05}_{-0.06}$ |  |  |  |  |  |  |  |  | $0.41^{+0.41}_{-0.07}$ | $4.1435\pm 0.0008$ | $2.83^{+0.18}_{-0.17}$

Notes: Col. (1): Source reference number. Col. (2): IAU name of the Herschel
detection. Col. (3) and (4): RA and Dec. offsets in arcsec (first row) and kpc
(second row). Col. (5): Einstein radius in arcsec (first row) and kpc (second
row). Col. (6): Axis ratio of the mass profile. Col. (7): Position angle of
the mass profile. Col. (8) and (9): Shear elliptical components of the mass
profile. Col. (10) and (11): Size of the source plane pixelization. Col. (12):
Regularization coefficient. Col. (13): Magnification computed on the regions
of the source plane with $\textit{SNR}>3$. Col. (14): Circularised radius
equivalent to the regions of the source plane with $\textit{SNR}>3$. Col.
(15): Mass within the Einstein radius. Col. (16): Mass-to-light ratio in
$F110W$ within the Einstein radius.

Table 10: continued No. | IAU name | $\delta x$ | $\delta y$ | $\theta_{E}$ | $q$ | $PA$ | $\epsilon_{shear,\,1}$ | $\epsilon_{shear,\,2}$ | $x_{\rm pix}$ | $y_{\rm pix}$ | $\lambda$ | $\mu$ | $R_{\rm bkg,\,circ}$ | $k_{0}$ |
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---
|  | [arcsec] | [arcsec] | [arcsec] |  |  |  |  |  |  |  |  | [arcsec] | [] |
|  | $dx_{0}$ | $dy_{0}$ | $\theta_{E,\,0}$ |  |  |  |  |  |  |  |  | $R_{\rm bkg,\,circ,\,0}$ | $M$ | $M/L$
|  | [kpc] | [kpc] | [kpc] |  |  |  |  |  |  |  |  | [kpc] |  [$10^{11}$ M⊙] |
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13) | (14) | (15) | (16)
S_29 | HERSJ012041.6$-$002705 | $-0.07\pm 0.01$ | $-0.095^{+0.010}_{-0.011}$ | $0.928^{+0.005}_{-0.006}$ | $0.76^{+0.02}_{-0.01}$ | $-41.77^{+2.16}_{-2.17}$ | – | – | $38^{+5}_{-6}$ | $35\pm 6$ | $0.022\pm 0.002$ | $3.91^{+0.43}_{-0.34}$ | $0.124^{+0.008}_{-0.006}$ | $2.65\pm 0.03$ | –
$-0.55^{+0.08}_{-0.09}$ | $-0.71\pm 0.08$ | $6.94\pm 0.15$ |  |  |  |  |  |  |  |  | – | – | –
S_30 | HATLASJ085112$+$004934 | $0.03406^{+0.00009}_{-0.00014}$ | $0.1967^{+0.0010}_{-0.0002}$ | $1.24359^{+0.00004}_{-0.00003}$ | $0.34221^{+0.00034}_{-0.00007}$ | $-41.033^{+0.008}_{-0.033}$ | $-0.29461^{+0.00011}_{-0.00006}$ | $0.28098^{+0.00005}_{-0.00043}$ | $44$ | $44$ | $0.00112^{+0.00004}_{-0.00005}$ | $27.80^{+0.50}_{-0.59}$ | $0.01863^{+0.00004}_{-0.00009}$ | $4.0578^{+0.0014}_{-0.0003}$ | –
$0.24^{+0.03}_{-0.07}$ | $1.41^{+0.20}_{-0.39}$ | $8.90^{+1.26}_{-2.45}$ |  |  |  |  |  |  |  |  | $0.161^{+0.001}_{-0.004}$ | $4.60^{+3.73}_{-2.22}$ | $1.86^{+2.07}_{-0.72}$
S_32 | HERMESJ104549$+$574512 | $-0.47^{+0.03}_{-0.04}$ | $-0.129^{+0.006}_{-0.009}$ | $2.631^{+0.007}_{-0.012}$ | $0.677^{+0.005}_{-0.003}$ | $18.85^{+0.69}_{-0.23}$ | – | – | $41$ | $40\pm 4$ | $0.014\pm 0.001$ | $8.63^{+0.37}_{-0.21}$ | $0.108\pm 0.002$ | $17.23^{+0.21}_{-0.12}$ | –
$-1.59^{+0.15}_{-0.17}$ | $-0.44\pm 0.04$ | $8.97^{+0.67}_{-0.73}$ |  |  |  |  |  |  |  |  | $0.85\pm 0.02$ | $5.45^{+0.50}_{-0.52}$ | $63.80^{+12.97}_{-10.76}$
S_35 | HATLASJ132630$+$334410 | $0.004^{+0.004}_{-0.006}$ | $-0.057^{+0.009}_{-0.013}$ | $1.684^{+0.005}_{-0.004}$ | $0.577^{+0.008}_{-0.006}$ | $-47.54^{+0.42}_{-0.40}$ | – | – | $42^{+2}_{-4}$ | $34^{+8}_{-2}$ | $0.0095\pm 0.0006$ | $1.89\pm 0.02$ | $0.0938^{+0.0079}_{-0.0004}$ | $8.26^{+0.03}_{-0.02}$ | –
$0.03^{+0.03}_{-0.05}$ | $-0.44^{+0.07}_{-0.10}$ | $12.92^{+0.04}_{-0.03}$ |  |  |  |  |  |  |  |  | $0.743^{+0.063}_{-0.003}$ | $9.09\pm 0.03$ | $3.83^{+0.20}_{-0.19}$
S_38 | HERMESJ142824$+$352620 | $-0.0008^{+0.0065}_{-0.0074}$ | $0.016^{+0.005}_{-0.006}$ | $0.215^{+0.006}_{-0.003}$ | $0.66^{+0.06}_{-0.05}$ | $-5.44^{+5.95}_{-8.75}$ | – | – | $42^{+1}_{-8}$ | $25^{+5}_{-4}$ | $0.0064^{+0.0006}_{-0.0004}$ | $2.64^{+0.15}_{-0.14}$ | $0.090^{+0.003}_{-0.004}$ | $0.137^{+0.010}_{-0.005}$ | –
$-0.007^{+0.054}_{-0.061}$ | $0.13^{+0.04}_{-0.05}$ | $1.78^{+0.05}_{-0.03}$ |  |  |  |  |  |  |  |  | $0.78\pm 0.03$ | $0.58^{+0.04}_{-0.02}$ | $0.98^{+0.11}_{-0.09}$
S_39 | HATLASJ223753.8$-$305828 | $0.19^{+0.02}_{-0.01}$ | $-0.091^{+0.010}_{-0.017}$ | $1.26^{+0.02}_{-0.01}$ | $0.54^{+0.01}_{-0.03}$ | $65.49^{+0.77}_{-0.62}$ | – | – | $44$ | $20$ | $0.0098^{+0.0006}_{-0.0005}$ | $2.65^{+0.04}_{-0.10}$ | $0.1281^{+0.0032}_{-0.0010}$ | $4.53^{+0.07}_{-0.05}$ | –
$1.24^{+0.18}_{-0.20}$ | $-0.60^{+0.11}_{-0.13}$ | $8.28^{+0.90}_{-1.31}$ |  |  |  |  |  |  |  |  | $1.10\pm 0.03$ | $3.88^{+1.15}_{-1.02}$ | $4.00^{+2.08}_{-1.12}$
S_40 | HATLASJ225250.7$-$313657 | $0.182^{+0.012}_{-0.005}$ | $0.08^{+0.01}_{-0.02}$ | $0.605^{+0.008}_{-0.004}$ | $0.633^{+0.020}_{-0.009}$ | $-73.84^{+2.35}_{-0.69}$ | – | – | $41^{+3}_{-9}$ | $40^{+4}_{-14}$ | $0.0031^{+0.0002}_{-0.0003}$ | $3.44^{+0.18}_{-0.11}$ | $0.078^{+0.002}_{-0.003}$ | $1.09^{+0.03}_{-0.01}$ | –
$1.33^{+0.17}_{-0.27}$ | $0.54^{+0.14}_{-0.18}$ | $4.41^{+0.51}_{-0.89}$ |  |  |  |  |  |  |  |  | $0.65\pm 0.02$ | $1.12^{+0.47}_{-0.40}$ | $4.89^{+4.71}_{-1.81}$
S_41 | HELMSJ233633.5$-$032119 | $0.051^{+0.001}_{-0.005}$ | $-0.0851^{+0.0106}_{-0.0004}$ | $1.7281^{+0.0130}_{-0.0007}$ | $0.7347^{+0.0008}_{-0.0196}$ | $-48.44^{+1.47}_{-0.11}$ | – | – | $39$ | $43$ | $0.0084^{+0.0005}_{-0.0004}$ | $12.39^{+2.16}_{-2.48}$ | $0.036^{+0.011}_{-0.005}$ | $9.161^{+0.105}_{-0.006}$ | –
– | – | – |  |  |  |  |  |  |  |  | $0.30^{+0.10}_{-0.05}$ | – | –
Figure 10: Top panel: Distribution of the circularised radius of the
background sources from the lens modelling and taking into account the
uncertainties on the radii. Bottom panel: Circularised radius of the
background sources (blues circles) and HWHM of the PSF of the image corrected
for the lensing magnification (pink line). Figure 11: Left panels: Lens
subtracted image (top left panel), best-fitting background lensed source (top
right panel), SNR residual map (bottom left panel), and ${\rm SNR}>3$ regions
of the source plane lensed back to the image plane of S_7. Each panel shows
the pixel mask (corresponding to the black-shaded regions) adopted for the
lens modelling. The top right panel shows the critical curves (black line).
The bottom right panel show the region of the source plane displayed in the
right panel. Right panel: Source plane reconstruction of the background source
and caustics curves (green line). We highlight with black and blue contour the
$\textit{SNR}>3$ region adopted for computing the lensing magnification and
source size.

A comparison between our Einstein radii and those available in the literature
(Bussmann et al., 2013, 2015; Calanog et al., 2014; Geach et al., 2015; Enia
et al., 2018; Dye et al., 2022; Maresca et al., 2022; Kamieneski et al.,
2023a) is shown in Table 11 and in Fig. 12. Our values are comparable with
what is found in the literature, with only two exceptions: S_38 which Bussmann
et al. (2013) did not resolve with SMA, due to the very low angular separation
of the multiple images and assumed to have Einstein radius of $0.1\pm 0.3$
arcsec; and S_10 for which Calanog et al. (2014) fixed the flattening and
position angle of the mass model to be circular and aligned with the lens.

Table 11: Comparison between our Einstein radii and those available in the
literature in the near-IR and in the sub-mm/mm if available.

No. | IAU Name | $\theta_{\rm{E}}$ | $\theta_{\rm{E,near-IRlit.}}$ | Ref. | $\theta_{\rm{E,sub-mm/mm.lit.}}$ | Ref. | Multiw. | Ref
---|---|---|---|---|---|---|---|---
|  | [arcsec] | [arcsec] |  | [arcsec] |  |  |
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9)
S_8 | HERSJ020941.2$+$001558 | $2.579^{+0.002}_{-0.003}$ | $2.48^{+0.02}_{-0.01}$ | Ge15 | $2.55^{+0.14}_{-0.20}$ | Ka23 | ALMA band 6 | Li22
S_9 | HERMESJ032637$-$270044 | $0.981^{+0.005}_{-0.006}$ | $0.96^{+0.02}_{-0.03}$ | Ca14 | – | – | – | –
S_10 | HERMESJ033732$-$295353 | $1.9718^{+0.0004}_{-0.0005}$ | $1.65^{+0.03}_{-0.054}$ | Ca14 | – | – | – | –
S_12 | HERMESJ100144$-$025709 | $0.930\pm 0.002$ | $0.91\pm 0.01$ | Ca14 | $0.956\pm 0.005$ | Bu15 | ALMA band 7 | Bu15
S_13 | HERMESJ103827$+$581544 | $2.408\pm 0.010$ | $2.40^{+0.01}_{-0.05}$ | Ca14 | $2.0\pm 0.2$ | Bu13 | SMA 340 GHz | Bu13
S_14 | HERMESJ110016$+$571736 | $1.081\pm 0.003$ | $1.14^{+0.04}_{-0.07}$ | Ca14 | – | – | – | –
S_18 | HATLASJ133008$+$24586 | $1.037\pm 0.002$ | $0.944^{+0.002}_{-0.001}$ | Ca14 | $0.88\pm 0.02$ | Bu13 | SMA 340 GHz | Bu13
S_21 | HERMESJ171451$+$592634 | $0.976^{+0.006}_{-0.007}$ | $0.87^{+0.02}_{-0.05}$ | Ca14 | – | – | – | –
S_32 | HERMESJ104549$+$574512 | $2.631^{+0.008}_{-0.012}$ | $2.46\pm 0.01$ | Ca14 | – | – | – | –
S_35 | HATLASJ132630$+$334410 | $1.684^{+0.005}_{-0.004}$ | – | – | $1.80\pm 0.02$ | Bu13 | SMA 340 GHz | Bu13
S_38 | HERMESJ142824$+$35262 | $0.37\pm 0.02$ | – | – | $0.10\pm 0.03$ | Bu13 | SMA 340 GHz | Bu13

Notes: Col. (1): Source reference number. Col. (2): IAU name of the Herschel
detection. Col. (3): Value of the Einstein radii measured in this work. Col.
(4) and (5): Value of the Einstein radii measured in the literature from the
near-IR observations and reference. Col. (6) and (7): Value of the Einstein
radii measured in the literature from the sub-mm/mm observations and
reference. Col. (8) and (9): Multiwavelength observations and reference.

##  6 Discussion

Consistent with expectations (Perrotta et al., 2002; Lapi et al., 2012;
Negrello et al., 2017) our 65 confirmed lenses mostly comprise systems where
the lens is a single galaxy (51). Only 4 are made of spectroscopically
confirmed groups or clusters (S_36, S_48, S_60, and S_61), and 9 systems have
a morphology consistent with a group (S_6, S_15, S_23, S_25, S_28, S_33, S_34,
S_54, and S_63). The lensing galaxies are nearly all ETGs, with the only
exceptions of S_47 and one of the galaxies in the lensing cluster of S_48.
Both of them show a clear spiral structure. The ETG nature of the lensing
galaxies is further confirmed by their concentrations, with $92\%$ of our
sample lenses being more concentrated than expected for an exponential disk.

The mass within the Einstein radii of the foreground lenses ranges between
$9.9\times 10^{10}$ M⊙ (1-st percentile) and $6.4\times 10^{11}$ M⊙ (99-th
percentile). The mass-to-light ratios in the F110W filter within the Einstein
radius range between 1.25 and 8.86 M⊙ L${}_{\odot}^{-1}$. The background
sources host a variety of morphologies, including single compact sources (e.g.
S_12), more diffuse sources (e.g. S_18), and multiple clumps (S_17). We find
that 14 out of 22 reconstructed background sources are single sources, whereas
the remaining 8 are multiple sources. The present analysis alone is not enough
to determine whether these morphologies indicate different populations of
DSFGs or variations in the stellar and/or dust distributions. The physical
sizes of the background sources, measured as the circularised radii of the
circles equivalent to the regions of the source plane with ${\rm SNR}>3$,
range between 0.34 kpc (1-st percentile) and 1.30 kpc (99-th percentile). We
compare our stellar sizes with the dust ones by Enia et al. (2018), who
modelled the SMA sub-mm/mm emission of a sample of 12 lenses similarly
selected and partially included in our sample. They found dust sizes between
1.52 kpc (1-st percentile) and 4.07 kpc (99-th percentile). We can understand
this result by considering that the HST observations, by sampling the
optical/near-UV rest-frame emission, are expected to pick up only the
intrinsically brightest and more compact regions of the background sources
whose light can pass through the dust. This is consistent with an inside-out
growth and later inside-out quenching, a scenario where the central regions of
these DSFGs begin to clear out the dust first, causing the more compact
stellar emission to shine through. Interestingly, the HST sizes are comparable
to bright nuclei and off-nuclear knots in local ULIRGs (Surace et al., 1998;
Farrah et al., 2001). This is somewhat in contrast with previous literature
(e.g., Pantoni et al., 2021) that argued for the dust emission to be more
compact than the stellar one. Although, recently, Kamieneski et al. (2023b)
studied a $z\sim 2.3$ lensed galaxies with properties similar to those of the
lensed DSFGs in our sample and found rest frame near-UV/optical/near-IR
emitting regions comparable or even slightly smaller in size than the ones
measured in the sub-mm, thus providing evidence for an inside-out quenching
scenario. It is worth noticing that Kamieneski et al. (2023b) has also
considered another possible, but less likely, explanation related to
inclination effects and uneven dust distribution. We also want to point out
that the difference in sizes we observe between the stellar emitting region,
as sampled by HST, and the dust emitting region, as probed by SMA, may be
affected by the lower angular resolution of the SMA observations compared to
HST data. In fact, by projecting the half width at half maximum (HWHM) of the
SMA beam to the redshift of the source and then dividing it by the square root
of the total magnification within the $>3\sigma$ regions, we get a physical
resolution (once averaged over the whole sample) of $0.85$ kpc, which is
larger than what we get for near-IR size for about 50 per cent of our sample.
While Enia et al. (2018) sources are resolved ($R_{\rm bkg,\,circ}/{\rm
PSF_{HWHM}}\mathrel{\hbox to0.0pt{\lower 3.0pt\hbox{$\sim$}\hss}\raise
2.0pt\hbox{$>$}}1$), any emission coming from regions smaller than the
projected HWHM would inevitably be broadened. Moreover, the depth of our
observations does not allow us to exclude that other, more obscured and
undetected, star-forming knots are present throughout the disk, implying that
mass buildup could happen disk-wide.

Finally, it is worth mentioning that the optical/near-IR sizes quoted in the
literature are often measured through the effective radius obtained by fitting
a Sérsic profile to the surface brightness distribution of the background
sources. For lensed galaxies, this is usually done directly during the lens
modelling by including a parametric background source (e.g. Calanog et al.,
2014). Such an estimate of size takes into account the concentration of the
source and averages out the surface brightness distribution in the case of
clumpy emission. In comparison, our measure is SNR-dependent and is not
affected by the smoothness of the surface brightness distribution. We remark
that the relation between the observed-frame near-IR sizes and sub-mm ones is
still up to debate and could depend on additional factors we do not discuss
here, like the stellar mass of the galaxy (see, Liu et al., 2023, for details)
or its evolutionary stage. At the same time, we find magnifications ranging
between 2.4 (1-st percentile) and 15.8 (99-th percentile), with a median of
5.5 for our sample. The magnifications by Enia et al. (2018) range between
3.20 (1-st percentile) and 8.35 (99-th percentile) with a median of 5.7. This
comparison suggests a minor, or even negligible, differential magnification.

Figure 12: Comparison between our estimated Einstein radii (blue circles) and
the ones from literature measured either in near-IR (blue triangles) or sub-
mm/mm (red triangles).

We compare the properties of our lenses (i.e., total effective radii, Einstein
radii, and total effective surface brightnesses) to those of the SLACS sample
of confirmed lenses (Bolton et al., 2008). This is the largest available
sample of strong lenses followed up by HST and with lens modelling. The SLACS
lensing candidates were identified from archival SDSS spectroscopic data as
all the systems that show the presence of two separate redshift estimates in
the same spectrum: a lower absorption-line redshift for the foreground lens
and a higher emission-line redshift for the background source. These
candidates were then followed up and confirmed by means of HST ACS/F814W
imaging. We consider the 63 confirmed lenses out of 131 candidates, for which
Bolton et al. (2008) were able to subtract the surface brightness distribution
of the foreground lens and perform the lens modelling. They modelled the
surface brightness distribution of the lens, adopting the de Vaucouleurs
profile. We perform a K-correction of the total effective surface brightness
of all the galaxies of our and SLACS samples with available redshifts. As a
template for the ETG SED, we use the 17 local elliptical galaxies available in
the Brown Atlas (Brown et al., 2014). To estimate the F110W magnitude of the
SLACS lenses, we redshift and normalize the template to match the F814W
magnitude using PySynphot
package131313https://pysynphot.readthedocs.io/en/latest/. Then, we compute the
F110W magnitude of each template at $z=0$ and at the redshift of the
foreground lenses of both samples. Finally, we adopt the F110W magnitude
difference as the K-correction term. This correction does not take into
account possible differences between the SEDs of the templates and the ones of
the lenses. The median K-correction terms for our sample and SLACS are 0.04
mag and 0.03 mag, respectively. From Fig. 13, it is possible to see that our
sample shows different $R_{50}$ and $\theta_{E}$ distributions than SLACS. Our
selection is able to pick up more systems with both smaller or larger values
of $\theta_{E}$. Moreover, at similar Einstein radii, the effective radii of
our lenses are significantly smaller than the SLACS, making our background
sources less contaminated by the emission of the lenses. Figure 14 shows that
the two samples have similar $R_{50,0}$ and absolute magnitude distributions,
although our lenses show a tail for smaller and fainter galaxies. At the same
time, our lenses have lower $\mu_{50,0,{\rm K_{corr}}}$ for the same radii,
which implies that our lenses either are fainter or more concentrated than the
de Vaucouleurs profiles. The increased scatter we find in both the $R_{50,0}$
and $M_{F110W}$, and $R_{50,0}$ and $\mu_{50,0,{\rm K_{corr}}}$ distributions
can be accounted for by considering the variation in concentration and the
wide range of foreground lens redshifts we observed. We can try to further
explain these differences by considering the different selections of the two
samples. The SLACS sample, being constructed from SDSS spectroscopic data and
needing a robust detection of both the foreground lens and background source,
is limited in magnitude to brighter lenses at lower redshift. In particular,
the SLACS spectroscopic selection was done through 3 arcsec diameter fibres
and comprises either local galaxies or massive ETGs at $z\lesssim 0.6$.

Figure 13: Top panel: Normalised distribution of the values of the Einstein
radius of the lenses in our (blue histogram) and in the SLACS samples (orange
histogram). Bottom left panel: Total effective radius as a function of
Einstein radius of the lenses in our (blue symbols) and in the SLACS sample
(orange circles). The blue circles and crosses correspond to systems for which
we derived the Einstein radius from the lens modelling or the separation
between multiple images, respectively. Bottom right panel Normalised
distribution of the values of the total effective radius of the lenses. Figure
14: Top panel: Normalized distribution of the total effective radii in kpc of
our (blue histogram) and SLACS samples (orange histogram). Central left panel:
Absolute magnitude corrected for $K$-correction against the total effective
radii in kpc of the two samples. Central right panel: Normalized distribution
of the absolute magnitude of the two samples with the $K$-correction applied.
Our lensing galaxies are color-coded according to their concentration, with
purple corresponding to the less-concentrated systems and green to the most-
concentrated ones. White marks the concentration of a de Vaucouleurs profile.
Bottom left panel: Kormendy relation of the two samples. Our lensing galaxies
are color-coded according to their concentration. Bottom right panel:
Normalized distribution of the total effective surface brightness of the two
samples with the $K$-correction applied.

##  7 Conclusions

We have carried out a snapshot HST F110W observing campaign to follow-up 281
Herschel-selected candidate strongly lensed galaxies. We visually inspect them
and classify them according to the presence of the background sources,
confirming 25 candidates as strong lenses. We model all the systems where we
identify a suitable lens candidate exploiting three different surface-
brightness modelling algorithms, namely GASP2D, GALFIT, and ISOFIT+CMODEL,
based on the morphology of the foreground lensing galaxies. By combining the
visual inspection, available multi-wavelength follow-ups, and results of the
lens subtraction, we are able to confirm as lensed a total of 65 systems.
Lastly, we perform lens modelling and source reconstruction of all the systems
for which we can confidently identify both a galaxy acting as the main lens
and the background source in the HST images (34 systems). We obtain successful
results for 23 galaxies. The main results of our analysis are the following:

  * •

the overall surface brightness distribution of the lenses and their morphology
follows the relations expected for ETGs; however, the foreground lensing
galaxies often needed multiple surface brightness components, with properties
significantly varying from galaxy to galaxy;

  * •

most of the lensing systems are consistent with single galaxy lenses, with
only $\sim 7\%$ of them being confirmed as a group or cluster lenses;

  * •

the estimated magnifications and Einstein radii are consistent with previous
analysis conducted on data at different wavelengths; however, the inferred
size of the background sources is about 3 times smaller than the ones measured
in the sub-mm/mm with SMA by Enia et al. (2018) for a similarly selected, and
partially overlapping sample. This difference in size between the stellar and
the dust-emitting regions is suggestive of an inside-out quenching scenario;

  * •

the sub-mm selection used to build our sample revealed lensing systems with
fainter lenses and larger Einstein radii than the SLACS survey.

To conclude, we point out that the HST snapshots alone, even after carefully
identifying and subtracting the candidate lenses, might miss some of the
fainter lensed background sources. We argue that this is due to their dust
obscuration and high redshift. This underlines the importance of dedicated,
deeper near-IR observations (e.g., with HST, Keck, Euclid or JWST) and high-
resolution sub-mm observations (e.g., with ALMA and NOEMA) to effectively
determine the nature of the majority of Herschel-selected strong lensing
candidates. This work provides the basis for further detailed analysis of the
background sources by allowing not only more complex lens modelling but also
providing constraints on the stellar content through SED-fitting techniques.

## Acknowledgements

This work benefited from the support of the project Z-GAL ANR-AAPG2019 of the
French National Research Agency (ANR). EB acknowledges the School of Physics
and Astronomy of Cardiff University for hospitality while this paper was in
progress. EB, EMC, and GR are supported by Padua University grants Dotazione
Ordinaria Ricerca (DOR) 2019-2021 and by the Italian Ministry for Education,
University, and Research (MIUR) grant Progetto di Ricerca di Interesse
Nazionale (PRIN) 2017 20173ML3WW-001. EMC is also funded by the Istituto
Nazionale di Astrofisica (INAF) through grant PRIN 2022 C53D23000850006. LM
and MV acknowledge financial support from the Inter-University Institute for
Data Intensive Astronomy (IDIA), a partnership of the University of Cape Town,
the University of Pretoria and the University of the Western Cape, and from
the South African Department of Science and Innovation’s National Research
Foundation under the ISARP RADIOSKY2020 and RADIOMAP+ Joint Research Schemes
(DSI-NRF Grant Numbers 113121 and 150551) and the SRUG Projects (DSI-NRF Grant
Numbers 121291, SRUG22031677 and SRUG2204254729). DW acknowledges support from
program number HST-GO-15242, provided by NASA through a grant from the Space
Telescope Science Institute, which is operated by the Association of
Universities for Research in Astronomy, Incorporated, under NASA contract
NAS5-26555. AA is supported by ERC Advanced Investigator grant, DMIDAS [GA
786910], to C. S. Frenk. PC acknowledges the support of the project Z-GAL ANR-
AAPG2019 of the French National Research Agency (ANR). HD acknowledges
financial support from the Agencia Estatal de Investigación del Ministerio de
Ciencia e Innovación (AEI-MCINN) under grant (La evolución de los cíumulos de
galaxias desde el amanecer hasta el mediodía cósmico) with reference
(PID2019-105776GB-I00/DOI:10.13039/501100011033) and acknowledge support from
the ACIISI, Consejería de Economía, Conocimiento y Empleo del Gobierno de
Canarias and the European Regional Development Fund (ERDF) under grant with
reference PROID2020010107. JGN acknowledges financial support from the PGC
projects PGC2018-101948-B-I00 and PID2021-125630NB-I00 (MICINN, FEDER). SJ is
supported by the European Union’s Horizon Europe research and innovation
program under the Marie Skłodowska-Curie grant agreement No. 101060888. AL is
partly supported by the PRIN MIUR 2017 prot. 20173ML3WW 002 ‘Opening the ALMA
window on the cosmic evolution of gas, stars, and massive black holes’. IPF
acknowledges support from the Spanish State Research Agency (AEI) under grant
number PID2019-105552RB-C43. SS was partly supported by ESCAPE – The European
Science Cluster of Astronomy & Particle Physics ESFRI Research
Infrastructures, which in turn received funding from the European Union’s
Horizon 2020 research and innovation programme under Grant Agreement no.
824064. SS thanks the Science and Technology Facilities Council for support
under grants ST/P000584/1. CY acknowledges the support from the ERC Advanced
Grant 789410.

## Data Availability

The reduced images, models, residuals, and PSF cutouts are available on Zenodo
at the following link https://doi.org/10.5281/zenodo.10007041. Future versions
will be available at https://zenodo.org/doi/10.5281/zenodo.10007040.

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##  Appendix A The Full ‘A’ sample

Figure 15: From left to right panels: Observed HST F110W image, best-fitting
surface-brightness model of the lens, residual obtained after the subtraction
of the lens model from the image, and SNR map of the residuals for the A class
candidates. The contours in the model images are taken at two levels
corresponding to $\textit{SNR}=5$ and 10 (thick curves), and five uniformly
spaced levels between the $\textit{SNR}=10$ and the maximum SNR in the model
image (thin curves). The residual map shows the pixel mask (corresponding to
the black-shaded regions) adopted for the surface brightness modelling. The
residual maps show the contours of available high-resolution multiwavelength
data taken at two levels corresponding to $\textit{SNR}=5$ and 10 (thick
curves), and five uniformly spaced levels between the $\textit{SNR}=10$ and
the maximum SNR in the multiwavelength image (thin black curves). The images
are oriented such that N is up and E is to the left. For S_55, we show the
image and SNR map panels alone since we do not model the lensing galaxy that
is undetected in the HST snapshot. Figure 16: continued Figure 17: continued
Figure 18: continued Figure 19: continued Table 12: Structural parameters of
the systems classified as A obtained from a parametric fit of their surface
brightness distributions.

No. | IAU Name | Type | Components | $\mu_{\rm e}$ | $R_{\rm e}$ | $n$ | $q$ | $PA$ | $m_{\rm PSF}$ | $C/T$ | $\chi^{2}$ | $N_{\rm dof}$
---|---|---|---|---|---|---|---|---|---|---|---|---
|  |  |  |  [mag arcsec-2] | [arcsec] |  |  | [deg] | [mag] |  |  |
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13)
S_1 | HATLASJ000330.6$-$321136 | 1 | Sérsic | $20.69^{+0.12}_{-0.11}$ | $0.36\pm 0.02$ | $4.52^{+0.28}_{-0.27}$ | $0.803\pm 0.009$ | $73.05^{+0.96}_{-0.95}$ | – | $0.71\pm 0.05$ | 1.03 | 35501
Sérsic | $23.39^{+0.15}_{-0.13}$ | $1.17\pm 0.06$ | $0.57\pm 0.05$ | $0.96\pm 0.02$ | $0.003^{+1.933}_{-1.884}$ | – | $0.29\pm 0.05$
S_2 | HATLASJ000912.7$-$300807 | 1 | Sérsic | $21.63^{+0.23}_{-0.20}$ | $1.16^{+0.17}_{-0.18}$ | $3.96\pm 0.27$ | $0.929\pm 0.006$ | $34.92^{+1.39}_{-1.42}$ | – | $0.42^{+0.09}_{-0.10}$ | 1.03 | 135697
Sérsic | $26.24^{+0.14}_{-0.12}$ | $5.24^{+0.19}_{-0.18}$ | $0.80\pm 0.07$ | $0.27\pm 0.03$ | $121.76^{+6.00}_{-6.17}$ | – | $0.018^{+0.005}_{-0.004}$
Sérsic | $23.31^{+0.14}_{-0.12}$ | $3.93\pm 0.11$ | $1.54\pm 0.13$ | $0.78\pm 0.02$ | $139.43^{+3.96}_{-3.97}$ | – | $0.56^{+0.10}_{-0.09}$
S_3 | HELMSJ001353.5$-$060200 | 1 | Sérsic | $21.21^{+0.28}_{-0.22}$ | $0.26^{+0.04}_{-0.03}$ | $4.03\pm 0.60$ | $0.90\pm 0.02$ | $20.44^{+3.85}_{-3.82}$ | – | $0.45\pm 0.11$ | 1.03 | 61093
Exp. disk | $24.41^{+0.22}_{-0.18}$ | $2.02\pm 0.19$ | $[1]$ | $0.66\pm 0.05$ | $2.58^{+4.59}_{-4.42}$ | – | $0.55\pm 0.11$
S_4 | HELMSJ003619.8$+$002420 | 1 | Sérsic | $20.59^{+0.23}_{-0.19}$ | $1.35\pm 0.17$ | $1.26\pm 0.07$ | $0.905\pm 0.005$ | $109.96^{+1.05}_{-1.06}$ | – | $0.46^{+0.08}_{-0.09}$ | 1.01 | 171928
Sérsic | $17.78^{+0.16}_{-0.14}$ | $0.177^{+0.006}_{-0.005}$ | $1.54\pm 0.15$ | $0.90\pm 0.02$ | $159.86^{+2.55}_{-2.57}$ | – | $0.11^{+0.03}_{-0.02}$
Sérsic | $23.65^{+0.14}_{-0.13}$ | $5.68\pm 0.17$ | $0.88^{+0.08}_{-0.07}$ | $0.92\pm 0.02$ | $128.85^{+4.37}_{-4.42}$ | – | $0.42^{+0.08}_{-0.07}$
S_6 | HERSJ011722.3$+$0056241 | 3 | Sérsic | $21.64^{+0.29}_{-0.23}$ | $0.60^{+0.08}_{-0.07}$ | $5.19^{+0.42}_{-0.41}$ | $0.70\pm 0.02$ | $2.90^{+1.96}_{-1.92}$ | – | $0.85^{+0.05}_{-0.07}$ | 1.01 | 55924
Gauss | $24.97^{+0.21}_{-0.17}$ | $1.79\pm 0.16$ | $[0.5]$ | $0.83^{+0.10}_{-0.11}$ | $180.53^{+36.51}_{-36.53}$ | – | $0.15^{+0.07}_{-0.05}$
HERSJ011722.3$+$0056242 | Sérsic | $22.52^{+0.17}_{-0.15}$ | $0.25\pm 0.02$ | $1.12\pm 0.15$ | $0.93\pm 0.03$ | $-0.001^{+3.108}_{-3.000}$ | – | $[1]$ | 1.01 | 56315
S_7 | HERSJ012620.5$+$012950 | 1 | Sérsic | $22.23^{+0.31}_{-0.24}$ | $0.89\pm 0.12$ | $5.86^{+0.48}_{-0.47}$ | $0.70\pm 0.02$ | $13.18^{+1.91}_{-1.92}$ | – | $0.66^{+0.08}_{-0.11}$ | 1.04 | 66653
Gauss | $21.72^{+0.09}_{-0.08}$ | $0.76\pm 0.05$ | $[0.5]$ | $0.88\pm 0.05$ | $74.75\pm 3.74$ | – | $0.34^{+0.11}_{-0.08}$
S_9 |  HERMESJ032637$-$270044 | 1 | Sérsic | $22.70\pm 0.05$ | $1.01^{+0.02}_{-0.03}$ | $5.73\pm 0.11$ | $0.997^{+0.002}_{-0.003}$ | $46.45^{+0.69}_{-0.70}$ | – | $[1]$ | 1.04 | 58583
S_10 | HERMESJ033732$-$295353 | 1 | Sérsic | $20.23^{+0.25}_{-0.21}$ | $0.50\pm 0.09$ | $4.51^{+0.37}_{-0.38}$ | $0.804\pm 0.009$ | $53.64^{+1.65}_{-1.68}$ | – | $0.15^{+0.06}_{-0.05}$ | 1.05 | 177156
Sérsic | $22.12^{+0.13}_{-0.11}$ | $2.96^{+0.08}_{-0.07}$ | $1.73\pm 0.15$ | $0.96\pm 0.02$ | $149.69^{+1.32}_{-1.33}$ | – | $0.71^{+0.05}_{-0.06}$
Sérsic | $20.61^{+0.16}_{-0.14}$ | $0.83\pm 0.03$ | $0.69\pm 0.06$ | $0.90\pm 0.02$ | $54.94^{+2.84}_{-2.94}$ | – | $0.14^{+0.03}_{-0.02}$
S_13 | HERMESJ103827$+$581544 | 1 | Sérsic | $20.25^{+0.10}_{-0.09}$ | $0.47\pm 0.03$ | $1.56\pm 0.07$ | $0.762\pm 0.008$ | $6.07\pm 0.82$ | – | $0.27\pm 0.03$ | 1.02 | 107445
Sérsic | $22.65^{+0.07}_{-0.06}$ | $2.56^{+0.07}_{-0.08}$ | $1.07\pm 0.05$ | $0.74\pm 0.01$ | $12.31^{+1.06}_{-1.07}$ | – | $0.73\pm 0.03$
S_14 |  HERMESJ110016$+$571736 | 1 | Sérsic | $21.76\pm 0.04$ | $1.01\pm 0.02$ | $2.68\pm 0.04$ | $0.807\pm 0.004$ | $120.78^{+0.60}_{-0.59}$ | – | $[1]$ | 1.06 | 46997
S_15 | HATLASJ114638$-$0011321 | 2 | Sérsic | $20.30^{+0.24}_{-0.20}$ | $0.19\pm 0.02$ | $1.36\pm 0.17$ | $0.53\pm 0.03$ | $50.27^{+1.72}_{-1.69}$ | – | $0.58^{+0.08}_{-0.09}$ | 1.03 | 44201
Sérsic | $24.52^{+0.16}_{-0.13}$ | $1.14\pm 0.07$ | $0.45^{+0.07}_{-0.08}$ | $0.81^{+0.05}_{-0.04}$ | $53.88^{+2.83}_{-2.87}$ | – | $0.42^{+0.09}_{-0.08}$
HATLASJ114638$-$0011322 | Sérsic | $21.17^{+0.25}_{-0.21}$ | $0.18\pm 0.02$ | $3.26\pm 0.43$ | $0.81\pm 0.03$ | $128.86^{+1.77}_{-1.75}$ | – | $0.29^{+0.08}_{-0.07}$
Sérsic | $25.49^{+0.14}_{-0.12}$ | $2.29\pm 0.10$ | $1.73^{+0.15}_{-0.14}$ | $0.86\pm 0.03$ | $132.15^{+1.64}_{-1.66}$ | – | $0.71^{+0.07}_{-0.08}$
S_16 |  HATLASJ125126$+$254928 | 1 | Sérsic | $23.11^{+0.06}_{-0.05}$ | $1.50\pm 0.04$ | $7.96\pm 0.16$ | $0.504\pm 0.005$ | $135.36\pm 0.77$ | – | $[1]$ | 1.07 | 50036
S_17 |  HATLASJ125760$+$224558 | 1 | Sérsic | $22.33\pm 0.04$ | $1.13\pm 0.02$ | $4.63\pm 0.08$ | $0.814\pm 0.004$ | $6.39^{+0.58}_{-0.61}$ | – | $[1]$ | 1.07 | 50512
S_18 | HATLASJ133008$+$245860 | 1 | Sérsic | $21.81^{+0.30}_{-0.24}$ | $0.69\pm 0.09$ | $6.34^{+0.49}_{-0.50}$ | $0.80\pm 0.01$ | $81.56^{+1.97}_{-1.95}$ | – | $0.83^{+0.05}_{-0.07}$ | 1.04 | 44862
Gauss | $22.85^{+0.11}_{-0.10}$ | $0.83\pm 0.05$ | $[0.5]$ | $0.91^{+0.05}_{-0.06}$ | $96.76^{+10.85}_{-11.16}$ | – | $0.17^{+0.07}_{-0.05}$
S_19 |  HATLASJ133846$+$255057 | 1 | Sérsic | $23.46^{+0.07}_{-0.06}$ | $1.11\pm 0.04$ | $5.25^{+0.15}_{-0.16}$ | $0.696\pm 0.007$ | $50.61^{+0.87}_{-0.90}$ | – | $[1]$ | 1.04 | 57037
S_21 |  HERMESJ171451$+$592634 | 1 | de Vauc. | $22.05^{+0.05}_{-0.04}$ | $0.45\pm 0.01$ | $[4]$ | $0.55\pm 0.01$ | $144.39^{+1.69}_{-1.64}$ | – | $[1]$ | 1.10 | 31356
S_22 | HERMESJ171545$+$6012381 | 3 | Sérsic | $22.47^{+0.17}_{-0.15}$ | $0.56\pm 0.04$ | $4.43^{+0.33}_{-0.34}$ | $0.992^{+0.006}_{-0.009}$ | $180.00^{+1.08}_{-1.07}$ | – | $0.17^{+0.04}_{-0.03}$ | 1.05 | 55119
PSF | – | – | – | – | – | $[24.97]$ | $0.0023\pm 0.0002$
Sérsic | $24.43\pm 0.08$ | $4.10^{+0.14}_{-0.13}$ | $2.72\pm 0.16$ | $0.69\pm 0.01$ | $96.24^{+1.29}_{-1.27}$ | – | $0.83^{+0.03}_{-0.04}$
HERMESJ171545$+$6012382 | Sérsic | $23.87^{+0.10}_{-0.09}$ | $1.23\pm 0.06$ | $3.76\pm 0.20$ | $0.39\pm 0.01$ | $99.53^{+1.02}_{-0.99}$ | – | $[1]$ | 1.05 | 54970
S_23 |  HATLASJ225844.8$-$2951241 | 2 | Sérsic | $20.69^{+0.07}_{-0.06}$ | $0.44^{+0.01}_{-0.02}$ | $1.84\pm 0.06$ | $0.448\pm 0.008$ | $145.47^{+0.87}_{-0.83}$ | – | $[1]$ | 1.05 | 15053
HATLASJ225844.8$-$2951242 | Sérsic | $22.59^{+0.24}_{-0.20}$ | $0.61\pm 0.07$ | $1.12\pm 0.15$ | $0.39\pm 0.03$ | $58.30\pm 1.77$ | – | $0.10\pm 0.03$
Sérsic | $24.93^{+0.10}_{-0.09}$ | $3.29^{+0.15}_{-0.14}$ | $2.83^{+0.27}_{-0.28}$ | $0.69^{+0.03}_{-0.02}$ | $26.28^{+3.28}_{-3.25}$ | – | $0.90\pm 0.03$
S_24 | HELMSJ232210.3$-$0335591 | 3 | Sérsic | $23.38^{+0.10}_{-0.09}$ | $1.42\pm 0.08$ | $2.25\pm 0.14$ | $0.963^{+0.008}_{-0.009}$ | $80.29^{+0.86}_{-0.89}$ | – | $0.81\pm 0.03$ | 1.08 | 54469
Sérsic | $19.99^{+0.13}_{-0.12}$ | $0.214\pm 0.008$ | $1.29\pm 0.12$ | $0.57\pm 0.03$ | $7.88^{+1.32}_{-1.33}$ | – | $0.19\pm 0.03$
HELMSJ232210.3$-$0335592 | de Vauc. | $21.44\pm 0.06$ | $0.134\pm 0.006$ | $[4]$ | $0.74\pm 0.03$ | $64.64^{+4.21}_{-4.33}$ | – | $[1]$ | 1.07 | 50334

Notes: Col. (1): Source reference number. Col. (2): IAU name of the Herschel
detection. Indices 1 and 2 refer to the two components of the lens candidate.
Col. (3): Type of the system. Col. (4): Adopted model for the lens components.
Col. (5): Effective surface brightness, i.e., the surface brightness at the
effective radius. Col. (6): Effective radius, i.e., the semi-major axis of the
isophote containing half of the light of the component. Col. (7): Sérsic
index. Values fixed in the fit are bracketed. Col. (8): Axial ratio. Col. (9):
Position angle. Col. (10): Magnitude of the unresolved component. Col. (11):
Relative flux of the component $C/T$. Col. (12): Reduced $\chi^{2}$ of the
fit. Col. (13): Number of degrees of freedom of the fit.

Table 13: continued No. | IAU Name | Type | Components | $\mu_{\rm e}$ | $R_{\rm e}$ | $n$ | $q$ | $PA$ | $m_{\rm PSF}$ | $C/T$ | $\chi^{2}$ | $N_{\rm dof}$
---|---|---|---|---|---|---|---|---|---|---|---|---
|  |  |  |  [mag arcsec-2] | [arcsec] |  |  | [deg] | [mag] |  |  |
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13)
S_25 | HATLASJ233037.2$-$3312171 | 3 | Sérsic | $20.79^{+0.23}_{-0.19}$ | $0.25\pm 0.02$ | $7.05^{+0.58}_{-0.57}$ | $0.58\pm 0.02$ | $75.25^{+1.03}_{-1.05}$ | – | $0.32^{+0.07}_{-0.06}$ | 1.05 | 47114
Sérsic | $23.71^{+0.12}_{-0.10}$ | $1.66\pm 0.06$ | $1.44\pm 0.14$ | $0.89\pm 0.03$ | $139.93^{+3.41}_{-3.29}$ | – | $0.68^{+0.06}_{-0.07}$
HATLASJ233037.2$-$3312172 | PSF | – | – | – | – | – | $[23.14]$ | $[1]$
Confirmed after the lens subtraction
S_26 | HELMSJ001626.0$+$042613 | 1 | Sérsic | $19.39\pm 0.05$ | $0.52\pm 0.01$ | $4.23\pm 0.09$ | $0.467\pm 0.004$ | $7.10^{+0.26}_{-0.25}$ | – | $0.59\pm 0.03$ | 1.05 | 55249
Sérsic | $22.22^{+0.09}_{-0.08}$ | $1.83\pm 0.06$ | $1.27\pm 0.08$ | $0.63\pm 0.01$ | $162.98^{+1.24}_{-1.26}$ | – | $0.41\pm 0.03$
S_27 | HATLASJ002624.8$-$341737 | 1 | Sérsic | $21.92^{+0.25}_{-0.20}$ | $0.31\pm 0.03$ | $4.94^{+0.51}_{-0.52}$ | $0.63\pm 0.02$ | $172.06^{+1.73}_{-1.74}$ | – | $0.54^{+0.08}_{-0.09}$ | 1.05 | 52636
Sérsic | $24.33^{+0.13}_{-0.12}$ | $1.08\pm 0.04$ | $0.69^{+0.09}_{-0.08}$ | $0.97^{+0.02}_{-0.03}$ | $180.01\pm 1.36$ | – | $0.46^{+0.09}_{-0.08}$
S_28 | HELMSJ004723.6$+$0157511 | 2 | de Vauc. | $18.60^{+0.30}_{-0.23}$ | $0.09\pm 0.01$ | $[4]$ | $0.84^{+0.04}_{-0.03}$ | $43.47^{+4.28}_{-4.38}$ | – | $0.11^{+0.04}_{-0.03}$ | 1.03 | 58679
Sérsic | $21.92\pm 0.02$ | $1.57\pm 0.02$ | $1.37^{+0.08}_{-0.07}$ | $0.851\pm 0.004$ | $165.60^{+1.09}_{-1.13}$ | – | $0.89^{+0.03}_{-0.04}$
HELMSJ004723.6$+$0157512 | Sérsic | $22.17\pm 0.06$ | $0.80\pm 0.02$ | $3.14\pm 0.07$ | $0.856^{+0.006}_{-0.007}$ | $79.44^{+0.83}_{-0.82}$ | – | $[1]$
S_29 | HERSJ012041.6$-$002705 | 1 | Sérsic | $19.91^{+0.20}_{-0.17}$ | $0.19\pm 0.02$ | $4.39\pm 0.34$ | $0.71\pm 0.01$ | $86.79\pm 1.04$ | – | $0.44\pm 0.07$ | 1.03 | 50744
Sérsic | $23.67^{+0.13}_{-0.12}$ | $1.37^{+0.05}_{-0.06}$ | $1.98\pm 0.18$ | $0.79\pm 0.02$ | $3.03^{+2.85}_{-2.88}$ | – | $0.56\pm 0.07$
S_30 | HATLASJ085112$+$004934 | 1 | Sérsic | $20.24^{+0.41}_{-0.30}$ | $0.27\pm 0.06$ | $4.45^{+0.72}_{-0.71}$ | $0.61\pm 0.02$ | $81.52^{+1.84}_{-1.83}$ | – | $0.25^{+0.12}_{-0.10}$ | 1.06 | 40914
Sérsic | $21.51^{+0.17}_{-0.14}$ | $0.78\pm 0.02$ | $0.44\pm 0.04$ | $0.94\pm 0.03$ | $158.68^{+6.02}_{-6.11}$ | – | $0.37\pm 0.07$
Sérsic | $22.35^{+0.14}_{-0.12}$ | $1.39\pm 0.04$ | $0.72\pm 0.07$ | $0.55\pm 0.02$ | $81.26^{+1.61}_{-1.71}$ | – | $0.38\pm 0.07$
S_31 | HATLASJ085359$+$015537 | 1 | Sérsic | $22.69^{+0.26}_{-0.20}$ | $0.45\pm 0.05$ | $6.78\pm 0.96$ | $0.30\pm 0.03$ | $117.52^{+1.82}_{-1.81}$ | – | $0.30^{+0.08}_{-0.07}$ | 1.13 | 22254
Sérsic | $26.34^{+0.14}_{-0.12}$ | $2.34\pm 0.09$ | $5.14\pm 0.48$ | $0.85\pm 0.03$ | $156.50^{+1.28}_{-1.29}$ | – | $0.70^{+0.07}_{-0.08}$
S_32 | HERMESJ104549$+$574512 | 1 | Sérsic | $19.59^{+0.23}_{-0.19}$ | $0.16\pm 0.02$ | $3.86^{+0.40}_{-0.39}$ | $0.37\pm 0.02$ | $121.59^{+1.47}_{-1.38}$ | – | $0.22^{+0.06}_{-0.05}$ | 1.04 | 60465
Sérsic | $21.54^{+0.12}_{-0.11}$ | $0.64\pm 0.03$ | $1.74\pm 0.17$ | $0.68\pm 0.03$ | $89.59^{+3.16}_{-3.13}$ | – | $0.78^{+0.05}_{-0.06}$
S_33 |  HERMESJ105551$+$5928451 | 2 | Sérsic | $22.62\pm 0.08$ | $0.66\pm 0.03$ | $1.82\pm 0.08$ | $0.762\pm 0.009$ | $92.59\pm 0.85$ | – | $[1]$ | 1.15 | 6328
HERMESJ105551$+$5928452 | Sérsic | $21.85^{+0.15}_{-0.13}$ | $0.28\pm 0.02$ | $1.25\pm 0.12$ | $0.79\pm 0.02$ | $123.08^{+1.84}_{-1.82}$ | – | $[1]$
S_34 | HERMESJ105751$+$5730261 | 2 | Sérsic | $20.36\pm 0.09$ | $0.41\pm 0.02$ | $3.90\pm 0.18$ | $0.752\pm 0.008$ | $91.89^{+0.83}_{-0.84}$ | – | $0.27\pm 0.03$ | 1.11 | 31547
Sérsic | $24.58\pm 0.07$ | $5.16\pm 0.15$ | $2.63^{+0.13}_{-0.12}$ | $0.74\pm 0.01$ | $30.55^{+1.03}_{-1.05}$ | – | $0.73\pm 0.03$
HERMESJ105751$+$5730262 | de Vauc. | $19.30^{+0.27}_{-0.22}$ | $0.10\pm 0.02$ | $[4]$ | $0.37\pm 0.04$ | $32.23^{+4.35}_{-4.53}$ | – | $0.42^{+0.36}_{-0.24}$
Sérsic | $22.80^{+0.67}_{-0.42}$ | $0.43^{+0.23}_{-0.21}$ | $5.95^{+2.42}_{-2.72}$ | $0.76^{+0.12}_{-0.13}$ | $94.68^{+7.37}_{-7.46}$ | – | $0.58^{+0.24}_{-0.36}$
HERMESJ105751$+$5730263 | Sérsic | $20.72^{+0.15}_{-0.13}$ | $0.137\pm 0.009$ | $3.63^{+0.31}_{-0.32}$ | $0.82\pm 0.02$ | $74.54^{+1.82}_{-1.84}$ | – | $[1]$
HERMESJ105751$+$5730264 | de Vauc. | $21.16\pm 0.05$ | $0.220\pm 0.007$ | $[4]$ | $0.61\pm 0.02$ | $100.13^{+2.05}_{-2.07}$ | – | $[1]$
HERMESJ105751$+$5730265 | Sérsic | $20.30^{+0.13}_{-0.12}$ | $0.131^{+0.008}_{-0.007}$ | $3.11\pm 0.23$ | $0.89\pm 0.01$ | $175.89^{+1.42}_{-1.45}$ | – | $[1]$
HERMESJ105751$+$5730266 | PSF | – | – | – | – | – | $[23.60]$ | $[1]$
S_35 |  HATLASJ132630$+$334410 | 1 | Sérsic | $23.80\pm 0.04$ | $2.53\pm 0.05$ | $5.73\pm 0.09$ | $0.595\pm 0.004$ | $72.04^{+0.57}_{-0.59}$ | – | $[1]$ | 1.05 | 39273
S_36 | HATLASJ133543$+$3004041 | 2 | Sérsic | $22.42\pm 0.08$ | $0.65\pm 0.03$ | $0.88\pm 0.04$ | $0.902\pm 0.009$ | $127.84\pm 0.89$ | – | $0.954\pm 0.005$ | 1.03 | 41523
PSF | – | – | – | – | – | $[24.11]$ | $0.046\pm 0.005$
HATLASJ133543$+$3004042 | Sérsic | $21.90^{+0.09}_{-0.08}$ | $0.41\pm 0.02$ | $4.97^{+0.23}_{-0.24}$ | $0.567\pm 0.010$ | $24.77^{+0.94}_{-0.95}$ | – | $[1]$
HATLASJ133543$+$3004043 | Sérsic | $23.50\pm 0.06$ | $1.10\pm 0.03$ | $5.58\pm 0.15$ | $0.844\pm 0.007$ | $64.17^{+0.92}_{-0.94}$ | – | $[1]$
HATLASJ133543$+$3004044 | Sérsic | $23.58^{+0.07}_{-0.06}$ | $1.02\pm 0.04$ | $6.21\pm 0.21$ | $0.609\pm 0.008$ | $165.10^{+0.80}_{-0.84}$ | – | $[1]$
S_37 |  HATLASJ142140$+$000448 | 1 | Sérsic | $21.27^{+0.07}_{-0.06}$ | $0.38\pm 0.01$ | $2.28\pm 0.05$ | $0.925\pm 0.005$ | $0.67\pm 0.77$ | – | $[1]$ | 1.11 | 44658
S_38 |  HERMESJ142824$+$352620 | 1 | Sérsic | $21.47^{+0.08}_{-0.07}$ | $0.49\pm 0.02$ | $2.43^{+0.10}_{-0.09}$ | $0.487\pm 0.008$ | $92.76^{+0.89}_{-0.91}$ | – | $[1]$ | 1.17 | 7204
S_39 |  HATLASJ223753.8$-$305828 | 1 | Sérsic | $21.81\pm 0.05$ | $0.72\pm 0.02$ | $5.03^{+0.10}_{-0.09}$ | $0.940\pm 0.005$ | $87.28^{+0.70}_{-0.71}$ | – | $[1]$ | 1.03 | 63365
S_40 |  HATLASJ225250.7$-$313657 | 1 | Sérsic | $22.23^{+0.12}_{-0.10}$ | $0.40\pm 0.02$ | $6.21\pm 0.40$ | $0.53\pm 0.01$ | $75.70^{+1.21}_{-1.25}$ | – | $[1]$ | 1.04 | 34943
S_41 | HELMSJ233441.0$-$065220 | 1 | Sérsic | $19.47^{+0.20}_{-0.17}$ | $0.28\pm 0.02$ | $1.14\pm 0.09$ | $0.38\pm 0.01$ | $22.16^{+1.00}_{-1.01}$ | – | $0.49^{+0.07}_{-0.08}$ | 1.57 | 35357
Sérsic | $22.59^{+0.15}_{-0.13}$ | $1.00\pm 0.06$ | $0.62\pm 0.06$ | $0.68\pm 0.03$ | $167.72^{+2.29}_{-2.37}$ | – | $0.51^{+0.08}_{-0.07}$
Table 14: continued No. | IAU Name | Type | Components | $\mu_{\rm e}$ | $R_{\rm e}$ | $n$ | $q$ | $PA$ | $m_{\rm PSF}$ | $C/T$ | $\chi^{2}$ | $N_{\rm dof}$
---|---|---|---|---|---|---|---|---|---|---|---|---
|  |  |  |  [mag arcsec-2] | [arcsec] |  |  | [deg] | [mag] |  |  |
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13)
S_42 | HELMSJ233633.5$-$0321191 | 2 | Sérsic | $18.38\pm 0.05$ | $0.332\pm 0.009$ | $2.82\pm 0.06$ | $0.577^{+0.004}_{-0.003}$ | $42.72^{+0.24}_{-0.25}$ | – | $0.34\pm 0.02$ | 1.06 | 58206
Sérsic | $21.94\pm 0.04$ | $2.55^{+0.03}_{-0.04}$ | $1.25\pm 0.04$ | $0.738\pm 0.006$ | $46.04\pm 0.84$ | – | $0.66\pm 0.02$
HELMSJ233633.5$-$0321192 | Sérsic | $23.16^{+0.06}_{-0.05}$ | $1.79\pm 0.04$ | $2.21\pm 0.04$ | $0.723\pm 0.005$ | $160.63^{+0.74}_{-0.75}$ | – | $[1]$
Confirmed through sub-mm/mm follow-up
S_43 | HELMSJ001615.7$+$032435 | 1 | Sérsic | $24.18^{+0.31}_{-0.25}$ | $3.46^{+0.45}_{-0.44}$ | $7.32^{+0.38}_{-0.39}$ | $0.579^{+0.007}_{-0.006}$ | $31.91^{+0.67}_{-0.65}$ | – | $0.86^{+0.04}_{-0.06}$ | 1.09 | 57290
Gauss | $24.61\pm 0.09$ | $3.25\pm 0.21$ | $[0.5]$ | $0.50\pm 0.07$ | $17.05^{+3.68}_{-3.72}$ | – | $0.14^{+0.06}_{-0.04}$
S_44 |  HELMSJ002220.9$-$015524 | 1 | Sérsic | $25.43^{+0.10}_{-0.09}$ | $2.09\pm 0.10$ | $3.77^{+0.19}_{-0.20}$ | $0.58\pm 0.01$ | $98.62\pm 0.99$ | – | $[1]$ | 1.13 | 37251
S_45 |  HELMSJ003814.1$-$002252 | 1 | PSF | – | – | – | – | – | $[22.45]$ | $[1]$ | 1.04 | 18416
S_47 | HELMSJ004714.2$+$032454 | 1 | Sérsic | $20.79^{+0.18}_{-0.15}$ | $0.20\pm 0.02$ | $0.60\pm 0.10$ | $0.75\pm 0.03$ | $103.11^{+4.11}_{-4.17}$ | – | $0.17^{+0.06}_{-0.05}$ | 1.01 | 26442
Exp. disk | $23.42^{+0.19}_{-0.17}$ | $1.47^{+0.14}_{-0.13}$ | $[1]$ | $0.60^{+0.04}_{-0.05}$ | $111.21^{+4.52}_{-4.42}$ | – | $0.83^{+0.05}_{-0.06}$
S_48 | HELMSJ005159.5$+$0622411 | 2 | Sérsic | $18.59^{+0.21}_{-0.17}$ | $0.113^{+0.009}_{-0.010}$ | $2.28\pm 0.18$ | $0.77\pm 0.01$ | $119.44\pm 1.05$ | – | $0.14\pm 0.03$ | 1.03 | 48792
Sérsic | $23.10^{+0.08}_{-0.07}$ | $2.10\pm 0.06$ | $1.95^{+0.10}_{-0.09}$ | $0.96\pm 0.01$ | $9.11^{+1.24}_{-1.22}$ | – | $0.86\pm 0.03$
HELMSJ005159.5$+$0622412 | de Vauc. | $20.48\pm 0.03$ | $0.201\pm 0.004$ | $[4]$ | $0.76\pm 0.01$ | $173.86^{+1.76}_{-1.70}$ | – | $[1]$
HELMSJ005159.5$+$0622413 | Sérsic | $24.00^{+0.07}_{-0.06}$ | $1.92\pm 0.06$ | $1.33\pm 0.04$ | $0.703^{+0.007}_{-0.008}$ | $37.42^{+0.90}_{-0.87}$ | – | $0.899^{+0.008}_{-0.009}$
PSF | – | – | – | – | – | $[22.52]$ | $0.101^{+0.009}_{-0.008}$
S_49 |  HATLASJ005724.2$-$273122 | 1 | Sérsic | $24.83^{+0.07}_{-0.06}$ | $1.46\pm 0.05$ | $9.11\pm 0.30$ | $0.858\pm 0.008$ | $126.93^{+0.84}_{-0.83}$ | – | $[1]$ | 1.05 | 37643
S_51 |  HERMESJ033211$-$270536 | 1 | PSF | – | – | – | – | – | $[23.01]$ | $[1]$ | 1.07 | 9735
S_52 |  HERMESJ044154$-$540352 | 1 | Sérsic | $21.75\pm 0.06$ | $0.54\pm 0.02$ | $7.49\pm 0.17$ | $0.783\pm 0.007$ | $9.27\pm 0.86$ | – | $[1]$ | 1.03 | 44932
S_54 | HATLASJ091841$+$0230481 | 2 | Sérsic | $20.11^{+0.34}_{-0.27}$ | $0.11\pm 0.02$ | $1.83^{+0.30}_{-0.31}$ | $0.69\pm 0.03$ | $152.52^{+1.94}_{-1.93}$ | – | $0.19^{+0.07}_{-0.06}$ | 1.07 | 43760
Sérsic | $25.92^{+0.14}_{-0.12}$ | $2.99\pm 0.14$ | $2.44\pm 0.20$ | $0.76\pm 0.02$ | $70.78^{+1.87}_{-1.88}$ | – | $0.81^{+0.06}_{-0.07}$
HATLASJ091841$+$0230482 | de Vauc. | $21.80\pm 0.06$ | $0.155\pm 0.006$ | $[4]$ | $0.91\pm 0.03$ | $115.92^{+4.12}_{-4.11}$ | – | $[1]$
S_56 |  HATLASJ115433.6$+$005042 | 1 | Sérsic | $21.10^{+0.08}_{-0.07}$ | $0.48\pm 0.02$ | $1.83\pm 0.08$ | $0.337\pm 0.009$ | $169.27^{+0.85}_{-0.87}$ | – | $[1]$ | 1.01 | 34603
S_57 | HATLASJ120127.6$-$014043 | 1 | Sérsic | $25.61^{+0.35}_{-0.26}$ | $1.51\pm 0.23$ | $1.00\pm 0.18$ | $0.74\pm 0.03$ | $42.98^{+1.91}_{-1.83}$ | – | $0.25^{+0.09}_{-0.08}$ | 1.06 | 28398
Sérsic | $19.56^{+0.14}_{-0.12}$ | $0.225\pm 0.009$ | $2.12\pm 0.20$ | $0.27\pm 0.03$ | $20.79^{+1.31}_{-1.29}$ | – | $0.75^{+0.08}_{-0.09}$
S_58 |  HATLASJ131611$+$281220 | 1 | Sérsic | $22.68^{+0.15}_{-0.13}$ | $0.45\pm 0.03$ | $5.08^{+0.44}_{-0.43}$ | $0.40\pm 0.02$ | $1.47^{+1.77}_{-1.73}$ | – | [1] | 1.02 | 28595
S_59 | HATLASJ134429$+$303036 | 1 | Sérsic | $19.44^{+0.37}_{-0.28}$ | $0.20\pm 0.03$ | $2.50\pm 0.29$ | $0.65\pm 0.01$ | $161.16^{+2.23}_{-2.21}$ | – | $0.54^{+0.13}_{-0.14}$ | 1.04 | 48806
Exp. disk | $22.71^{+0.20}_{-0.16}$ | $1.64\pm 0.15$ | $[1]$ | $0.26^{+0.04}_{-0.05}$ | $173.10^{+4.55}_{-4.49}$ | – | $0.46^{+0.14}_{-0.13}$
S_60 | HATLASJ141352$-$0000271 | 3 | Sérsic | $20.47^{+0.18}_{-0.15}$ | $0.51\pm 0.05$ | $3.36^{+0.21}_{-0.22}$ | $0.825\pm 0.006$ | $83.00\pm 1.08$ | – | $0.55^{+0.07}_{-0.08}$ | 1.01 | 73852
Exp. disk | $23.99\pm 0.11$ | $2.87\pm 0.17$ | $[1]$ | $0.96\pm 0.03$ | $-0.01^{+4.33}_{-4.12}$ | – | $0.45^{+0.08}_{-0.07}$
HATLASJ141352$-$0000272 | Sérsic | $21.05\pm 0.08$ | $0.31\pm 0.01$ | $3.64^{+0.17}_{-0.16}$ | $0.536\pm 0.010$ | $148.77^{+0.88}_{-0.89}$ | – | $[1]$ | 1.01 | 63073
HATLASJ141352$-$0000273 | Sérsic | $21.69\pm 0.05$ | $0.68\pm 0.02$ | $4.91\pm 0.10$ | $0.866\pm 0.005$ | $41.57^{+0.79}_{-0.75}$ | – | $[1]$ | 1.01 | 64764
S_61 | HATLASJ142414$+$0223041 | 2 | Sérsic | $24.20^{+0.07}_{-0.06}$ | $1.49\pm 0.05$ | $3.76\pm 0.11$ | $0.910\pm 0.007$ | $15.97^{+0.94}_{-0.89}$ | – | $0.880^{+0.009}_{-0.010}$ | 1.04 | 22914
PSF | – | – | – | – | – | $[22.25]$ | $0.120^{+0.010}_{-0.009}$
HATLASJ142414$+$0223042 | Sérsic | $24.59^{+0.10}_{-0.09}$ | $1.13\pm 0.06$ | $7.02\pm 0.36$ | $0.68\pm 0.01$ | $149.22^{+1.02}_{-0.98}$ | – | $[1]$
S_62 | HATLASJ230815.5$-$343801 | 1 | Sérsic | $22.86^{+0.21}_{-0.17}$ | $0.56\pm 0.05$ | $8.73^{+0.65}_{-0.69}$ | $0.89\pm 0.01$ | $157.26\pm 1.05$ | – | $0.76^{+0.05}_{-0.06}$ | 1.13 | 21244
Sérsic | $22.89^{+0.14}_{-0.13}$ | $0.75\pm 0.03$ | $0.52\pm 0.07$ | $0.56^{+0.03}_{-0.04}$ | $7.75^{+1.49}_{-1.48}$ | – | $0.24^{+0.06}_{-0.05}$
S_63 | HELMSJ232439.5$-$043936 | 1 | Sérsic | $21.14^{+0.22}_{-0.18}$ | $0.27^{+0.02}_{-0.03}$ | $3.26\pm 0.24$ | $0.98\pm 0.01$ | $89.07^{+1.07}_{-1.03}$ | – | $0.67^{+0.06}_{-0.08}$ | 1.06 | 53698
Sérsic | $23.95^{+0.13}_{-0.12}$ | $1.10\pm 0.04$ | $1.61\pm 0.18$ | $0.52\pm 0.03$ | $129.07^{+1.13}_{-1.16}$ | – | $0.33^{+0.08}_{-0.06}$
S_64 | HELMSJ233620.8$-$060828 | 1 | Sérsic | $20.53\pm 0.05$ | $0.64\pm 0.02$ | $4.76^{+0.10}_{-0.09}$ | $0.878\pm 0.004$ | $52.62\pm 0.24$ | – | $0.85\pm 0.02$ | 1.04 | 27656
Sérsic | $22.22^{+0.12}_{-0.10}$ | $0.96\pm 0.04$ | $0.87\pm 0.08$ | $0.73\pm 0.03$ | $127.25^{+3.16}_{-3.17}$ | – | $0.15\pm 0.02$
Table 15: Derived properties of the lensing systems.

No. | IAU Name | $m_{F110W}$ | $\mu_{\rm 50}$ | $R_{\rm 50}$ | $C_{31}$ | $\mu S_{1.1}$
---|---|---|---|---|---|---
|  | [mag] |  [mag arcsec-2] | [arcsec] |  |  [$\mu$Jy]
|  | $M_{F110W}$ | $\mu_{\rm 50,\,0}$ | $R_{\rm 50,\,0}$ |  |
|  | [mag] |  [mag kpc-2] | [kcp] |  |
(1) | (2) | (3) | (4) | (5) | (6) | (7)
S_1 | HATLASJ000330.6$-$321136 | $19.30\pm 0.14$ | $21.49^{+0.21}_{-0.20}$ | $0.56\pm 0.05$ | $7.24^{+0.43}_{-0.40}$ | $1.81\pm 0.06$
$-17.78^{+0.73}_{-0.59}$ | $20.10^{+0.37}_{-0.35}$ | $2.99^{+0.52}_{-0.55}$
S_2 | HATLASJ000912.7$-$300807 | $17.09\pm 0.19$ | $22.18\pm 0.26$ | $2.38^{+0.20}_{-0.17}$ | $5.34^{+0.38}_{-0.40}$ | $45.35\pm 0.12$
$-19.26^{+0.83}_{-0.68}$ | $21.10^{+0.38}_{-0.37}$ | $10.49^{+2.19}_{-2.36}$
S_3 | HELMSJ001353.5$-$060200 | $19.99\pm 0.24$ | $23.16^{+0.41}_{-0.50}$ | $0.90^{+0.25}_{-0.21}$ | $7.26^{+1.15}_{-1.34}$ | $3.00\pm 0.10$
$-18.29^{+0.92}_{-0.72}$ | $21.09^{+0.67}_{-0.64}$ | $5.98^{+1.98}_{-1.57}$
S_4 | HELMSJ003619.8$+$002420 | $16.41\pm 0.18$ | $21.29^{+0.46}_{-0.36}$ | $2.07^{+0.26}_{-0.20}$ | $6.38^{+1.30}_{-0.97}$ | $13.58\pm 0.25$
$-19.72^{+0.18}_{-0.17}$ | $20.29^{+0.46}_{-0.36}$ | $8.55^{+1.06}_{-0.84}$
S_6 | HERSJ011722.3$+$0056241 | $19.45^{+0.34}_{-0.31}$ | $22.10^{+0.47}_{-0.34}$ | $0.67^{+0.08}_{-0.07}$ | $8.68^{+0.74}_{-0.68}$ | $2.23\pm 0.10$
$-19.82^{+0.37}_{-0.36}$ | $19.38^{+0.47}_{-0.37}$ | $5.33^{+0.66}_{-0.55}$
HERSJ011722.3$+$0056242 | $22.87^{+0.23}_{-0.22}$ | $22.52^{+0.17}_{-0.15}$ | $0.24\pm 0.02$ | $2.95\pm 0.18$
– | – | –
S_7 | HERSJ012620.5$+$012950 | $18.86^{+0.29}_{-0.28}$ | $21.22^{+0.13}_{-0.11}$ | $0.74\pm 0.05$ | $4.64^{+1.03}_{-0.76}$ | $5.72\pm 0.09$
$-18.55^{+0.42}_{-0.40}$ | $19.67^{+0.20}_{-0.19}$ | $4.27^{+0.43}_{-0.42}$
S_9 | HERMESJ032637$-$270044 | $19.10\pm 0.07$ | $22.70\pm 0.05$ | $1.01^{+0.02}_{-0.03}$ | $10.12\pm 0.22$ | $3.81\pm 0.13$
– | – | –
S_10 | HERMESJ033732$-$295353 | $16.47^{+0.13}_{-0.12}$ | $21.15^{+0.19}_{-0.20}$ | $1.91\pm 0.16$ | $5.36^{+0.33}_{-0.32}$ | $2.93\pm 0.07$
$-18.89^{+0.68}_{-0.55}$ | $20.40^{+0.25}_{-0.27}$ | $6.15\pm 1.32$
S_13 | HERMESJ103827$+$581544 | $17.86^{+0.09}_{-0.08}$ | $21.95^{+0.12}_{-0.13}$ | $1.53\pm 0.11$ | $4.75^{+0.19}_{-0.20}$ | $10.12\pm 0.23$
$-20.38^{+0.09}_{-0.08}$ | $19.93^{+0.12}_{-0.13}$ | $10.48^{+0.76}_{-0.72}$
S_14 | HERMESJ110016$+$571736 | $18.78\pm 0.06$ | $21.76\pm 0.04$ | $0.91\pm 0.02$ | $4.99\pm 0.06$ | $12.71\pm 0.19$
$-20.19\pm 0.06$ | $19.25\pm 0.04$ | $6.97\pm 0.15$
S_15 | HATLASJ114638$-$0011321 | $21.15^{+0.21}_{-0.20}$ | $21.97^{+1.01}_{-0.70}$ | $0.29^{+0.10}_{-0.05}$ | $7.50^{+0.98}_{-1.17}$ | $6.33\pm 0.14$
$-19.03^{+0.21}_{-0.20}$ | $18.50^{+1.01}_{-0.70}$ | $2.51^{+0.86}_{-0.42}$
HATLASJ114638$-$0011322 | $20.52^{+0.16}_{-0.15}$ | $24.52^{+0.29}_{-0.37}$ | $1.28\pm 0.24$ | $8.90^{+1.82}_{-1.84}$
$-19.66^{+0.16}_{-0.15}$ | $21.05^{+0.29}_{-0.37}$ | $10.90^{+2.06}_{-2.09}$
S_16 | HATLASJ125126$+$254928 | $19.21\pm 0.08$ | $23.11^{+0.06}_{-0.05}$ | $1.07\pm 0.03$ | $15.14^{+0.42}_{-0.41}$ | $4.18\pm 0.15$
$-19.16^{+0.46}_{-0.40}$ | $21.02^{+0.27}_{-0.26}$ | $7.46^{+0.52}_{-0.61}$
S_17 | HATLASJ125760$+$224558 | $18.83\pm 0.06$ | $22.33\pm 0.04$ | $1.02\pm 0.02$ | $8.05\pm 0.13$ | $10.13\pm 0.12$
$-19.25\pm 0.06$ | $20.42\pm 0.04$ | $6.76\pm 0.15$
S_18 | HATLASJ133008$+$245860 | $19.05^{+0.35}_{-0.32}$ | $21.55^{+0.23}_{-0.20}$ | $0.68\pm 0.05$ | $7.33^{+1.09}_{-1.03}$ | $3.54\pm 0.11$
$-18.36^{+0.35}_{-0.32}$ | $20.01^{+0.23}_{-0.20}$ | $3.95\pm 0.31$
S_19 | HATLASJ133846$+$255057 | $20.09^{+0.10}_{-0.09}$ | $23.46^{+0.07}_{-0.06}$ | $0.93\pm 0.03$ | $9.19\pm 0.29$ | $12.23\pm 0.12$
$-17.25^{+0.70}_{-0.55}$ | $21.94^{+0.32}_{-0.30}$ | $5.27^{+0.68}_{-0.84}$
S_21 | HERMESJ171451$+$592634 | $21.03\pm 0.08$ | $22.05^{+0.05}_{-0.04}$ | $0.336^{+0.010}_{-0.009}$ | $6.9887^{+0.0005}_{-0.0003}$ | $7.00\pm 0.13$
$-19.17\pm 0.08$ | $18.56^{+0.05}_{-0.04}$ | $2.87\pm 0.08$
S_22 | HERMESJ171545$+$6012381 | $18.38^{+0.11}_{-0.10}$ | $23.86\pm 0.12$ | $2.68\pm 0.17$ | $6.51^{+0.37}_{-0.35}$ | $6.65\pm 0.14$
$-18.78^{+0.64}_{-0.53}$ | $22.43^{+0.30}_{-0.29}$ | $14.54^{+2.11}_{-2.40}$
HERMESJ171545$+$6012382 | $21.09^{+0.15}_{-0.14}$ | $23.87^{+0.10}_{-0.09}$ | $0.77\pm 0.04$ | $6.60\pm 0.32$
– | – | –

Notes: Col. (1): Source reference number. Col. (2): IAU name of the Herschel
detection. Indices 1 and 2 refer to the two components of the lens candidate.
Col. (3): Apparent magnitude of the model (first row), absolute magnitude of
the model (second row). Col. (4): Total effective radius in arcsec (first row)
and in kpc (second row). Col. (5): Total effective surface brightness before
(first row) and after correcting for cosmological dimming (second row). Col.
(6): $C_{31}$ of the model. Col. (7): Flux density of the background source
uncorrected for the magnification.

Table 16: continued No. | IAU Name | $m_{F110W}$ | $\mu_{\rm 50}$ | $R_{\rm 50}$ | $C_{31}$ | $\mu S_{1.1}$
---|---|---|---|---|---|---
|  | [mag] |  [mag arcsec-2] | [arcsec] |  |  [$\mu$Jy]
|  | $M_{F110W}$ | $\mu_{\rm 50,\,0}$ | $R_{\rm 50,\,0}$ |  |
|  | [mag] |  [mag kpc-2] | [kcp] |  |
(1) | (2) | (3) | (4) | (5) | (6) | (7)
S_23 | HATLASJ225844.8$-$2951241 | $20.37\pm 0.10$ | $20.69^{+0.07}_{-0.06}$ | $0.29\pm 0.01$ | $3.86\pm 0.08$ | $1.41\pm 0.08$
$-18.28^{+0.93}_{-0.69}$ | $18.41^{+0.57}_{-0.49}$ | $2.13^{+0.22}_{-0.33}$
HATLASJ225844.8$-$2951242 | $19.43\pm 0.14$ | $24.60^{+0.12}_{-0.14}$ | $2.32^{+0.19}_{-0.20}$ | $6.47^{+0.56}_{-0.53}$
$-19.18^{+0.92}_{-0.73}$ | $22.33^{+0.56}_{-0.52}$ | $16.60^{+2.34}_{-2.76}$
S_24 | HELMSJ232210.3$-$0335591 | $19.33^{+0.14}_{-0.13}$ | $22.74^{+0.13}_{-0.14}$ | $1.00^{+0.11}_{-0.12}$ | $7.18^{+0.50}_{-0.53}$ | $3.47\pm 0.08$
$-15.46^{+1.76}_{-1.08}$ | $22.13\pm 0.33$ | $2.64^{+1.20}_{-1.30}$
HELMSJ232210.3$-$0335592 | $22.74\pm 0.12$ | $21.44\pm 0.06$ | $0.116^{+0.006}_{-0.005}$ | $6.982^{+0.004}_{-0.001}$
– | – | –
S_25 | HATLASJ233037.2$-$3312171 | $19.45^{+0.14}_{-0.13}$ | $22.91^{+0.19}_{-0.21}$ | $1.08\pm 0.12$ | $6.58^{+1.32}_{-1.03}$ | $19.93\pm 0.21$
$-19.07^{+0.82}_{-0.63}$ | $20.71^{+0.52}_{-0.47}$ | $7.66^{+1.16}_{-1.32}$
HATLASJ233037.2$-$3312172 | $[23.14]$ | – | – | –
$-15.40^{+0.80}_{-0.60}$ | – | –
Confirmed after the lens subtraction |
S_26 | HELMSJ001626.0$+$042613 | $17.63\pm 0.07$ | $20.35\pm 0.11$ | $0.73\pm 0.04$ | $7.11\pm 0.17$ | $1.46\pm 0.08$
$-18.06\pm 0.07$ | $19.50\pm 0.11$ | $2.63^{+0.16}_{-0.15}$
S_27 | HATLASJ002624.8$-$341737 | $20.82^{+0.20}_{-0.19}$ | $23.13^{+0.30}_{-0.31}$ | $0.62^{+0.08}_{-0.07}$ | $6.69^{+0.86}_{-0.94}$ | $0.90\pm 0.03$
$-18.61^{+1.20}_{-0.88}$ | $20.28^{+0.88}_{-0.78}$ | $4.88^{+0.81}_{-0.85}$
S_28 | HELMSJ004723.6$+$0157511 | $18.14\pm 0.06$ | $21.67^{+0.09}_{-0.11}$ | $1.27^{+0.06}_{-0.07}$ | $4.10^{+0.49}_{-0.35}$ | $10.99\pm 0.18$
$-18.86\pm 0.06$ | $20.32^{+0.09}_{-0.11}$ | $6.65^{+0.33}_{-0.38}$
HELMSJ004723.6$+$0157512 | $19.58^{+0.09}_{-0.08}$ | $22.17\pm 0.06$ | $0.74\pm 0.02$ | $5.65\pm 0.10$
– | – | –
S_29 | HERSJ012041.6$-$002705 | $19.59\pm 0.15$ | $21.97^{+0.34}_{-0.37}$ | $0.58^{+0.10}_{-0.09}$ | $9.37^{+0.72}_{-0.85}$ | $2.57\pm 0.10$
$-19.21^{+0.21}_{-0.20}$ | $19.59^{+0.35}_{-0.38}$ | $4.36^{+0.75}_{-0.66}$
S_30 | HATLASJ085112$+$004934 | $18.68^{+0.17}_{-0.19}$ | $20.81^{+0.18}_{-0.20}$ | $0.75\pm 0.06$ | $3.25^{+0.66}_{-0.47}$ | $9.37\pm 0.15$
$-19.86^{+1.58}_{-1.07}$ | $18.60^{+0.88}_{-0.79}$ | $5.27^{+0.91}_{-1.47}$
S_31 | HATLASJ085359$+$015537 | $20.77^{+0.16}_{-0.15}$ | $24.92^{+0.36}_{-0.38}$ | $1.22^{+0.20}_{-0.18}$ | $14.19^{+1.47}_{-1.44}$ | $0.87\pm 0.03$
$-19.26^{+0.58}_{-0.49}$ | $21.58\pm 0.57$ | $10.17^{+1.76}_{-1.54}$
S_32 | HERMESJ104549$+$574512 | $19.69\pm 0.14$ | $20.94^{+0.17}_{-0.18}$ | $0.41\pm 0.04$ | $5.16^{+0.46}_{-0.43}$ | $7.20\pm 0.10$
$-15.81^{+0.29}_{-0.28}$ | $20.15^{+0.18}_{-0.19}$ | $1.39^{+0.17}_{-0.16}$
S_33 | HERMESJ105551$+$5928451 | $20.84\pm 0.12$ | $22.62\pm 0.08$ | $0.58\pm 0.02$ | $3.83\pm 0.10$ | $5.60\pm 0.08$
$-16.26^{+0.85}_{-0.66}$ | $21.22^{+0.37}_{-0.33}$ | $3.09^{+0.51}_{-0.63}$
HERMESJ105551$+$5928452 | $22.06^{+0.21}_{-0.20}$ | $21.86^{+0.15}_{-0.13}$ | $0.25\pm 0.02$ | $3.10\pm 0.14$
– | – | –
S_34 | HERMESJ105751$+$5730261 | $17.82\pm 0.08$ | $23.48^{+0.15}_{-0.17}$ | $2.64\pm 0.24$ | $9.89^{+0.72}_{-0.71}$ | $43.86\pm 0.21$
$-20.47^{+0.20}_{-0.19}$ | $21.43^{+0.19}_{-0.20}$ | $18.16^{+1.76}_{-1.72}$
HERMESJ105751$+$5730262 | $20.98^{+0.70}_{-0.81}$ | $20.67^{+0.99}_{-1.12}$ | $0.16^{+0.19}_{-0.08}$ | $11.33^{+4.02}_{-2.77}$
– | – | –
HERMESJ105751$+$5730263 | $21.93^{+0.22}_{-0.20}$ | $20.72^{+0.15}_{-0.13}$ | $0.124\pm 0.008$ | $6.39\pm 0.49$
– | – | –
HERMESJ105751$+$5730264 | $21.59^{+0.10}_{-0.09}$ | $21.16\pm 0.05$ | $0.172\pm 0.006$ | $6.987^{+0.002}_{-0.001}$
– | – | –
HERMESJ105751$+$5730265 | $21.58^{+0.19}_{-0.18}$ | $20.30^{+0.13}_{-0.12}$ | $0.124\pm 0.007$ | $5.60\pm 0.34$
– | – | –
HERMESJ105751$+$5730266 | $[23.60]$ | – | – | –
– | – | –
S_35 | HATLASJ132630$+$334410 | $18.76\pm 0.06$ | $23.80\pm 0.04$ | $1.95\pm 0.04$ | $10.11^{+0.19}_{-0.18}$ | $1.34\pm 0.06$
$-20.23\pm 0.06$ | $21.28\pm 0.04$ | $15.00^{+0.32}_{-0.31}$
S_36 | HATLASJ133543$+$3004041 | $20.76^{+0.12}_{-0.11}$ | $22.35^{+0.08}_{-0.07}$ | $0.60\pm 0.03$ | $2.88^{+0.06}_{-0.05}$ | $15.09\pm 0.23$
$-18.83^{+0.12}_{-0.11}$ | $19.38^{+0.08}_{-0.07}$ | $4.90\pm 0.22$
HATLASJ133543$+$3004042 | $20.98\pm 0.13$ | $21.90^{+0.09}_{-0.08}$ | $0.31\pm 0.01$ | $8.66^{+0.43}_{-0.42}$
$-18.62\pm 0.13$ | $18.92^{+0.09}_{-0.08}$ | $2.50^{+0.12}_{-0.11}$
HATLASJ133543$+$3004043 | $19.92\pm 0.09$ | $23.50\pm 0.06$ | $1.01\pm 0.03$ | $9.81\pm 0.30$
$-19.67\pm 0.09$ | $20.53\pm 0.06$ | $8.27^{+0.25}_{-0.26}$
HATLASJ133543$+$3004044 | $20.45^{+0.11}_{-0.10}$ | $23.58^{+0.07}_{-0.06}$ | $0.80\pm 0.03$ | $11.10^{+0.45}_{-0.44}$
$-19.18^{+0.11}_{-0.10}$ | $20.58^{+0.07}_{-0.06}$ | $6.56\pm 0.23$
Table 17: continued No. | IAU Name | $m_{F110W}$ | $\mu_{\rm 50}$ | $R_{\rm 50}$ | $C_{31}$ | $\mu S_{1.1}$
---|---|---|---|---|---|---
|  | [mag] |  [mag arcsec-2] | [arcsec] |  |  [$\mu$Jy]
|  | $M_{F110W}$ | $\mu_{\rm 50,\,0}$ | $R_{\rm 50,\,0}$ |  |
|  | [mag] |  [mag kpc-2] | [kcp] |  |
(1) | (2) | (3) | (4) | (5) | (6) | (7)
S_37 | HATLASJ142140$+$000448 | $20.34\pm 0.10$ | $21.27^{+0.07}_{-0.06}$ | $0.36\pm 0.01$ | $4.44\pm 0.10$ | $3.24\pm 0.05$
$-19.62^{+1.19}_{-0.80}$ | $18.00^{+0.91}_{-0.73}$ | $3.08^{+0.17}_{-0.34}$
S_38 | HERMESJ142824$+$352620 | $20.69^{+0.12}_{-0.11}$ | $21.47^{+0.08}_{-0.07}$ | $0.34\pm 0.01$ | $4.64\pm 0.13$ | $1.93\pm 0.05$
$-19.04^{+0.12}_{-0.11}$ | $18.38^{+0.08}_{-0.07}$ | $2.81\pm 0.11$
S_39 | HATLASJ223753.8$-$305828 | $19.09^{+0.08}_{-0.07}$ | $21.81\pm 0.05$ | $0.70\pm 0.02$ | $8.77^{+0.18}_{-0.17}$ | $3.56\pm 0.08$
$-18.92^{+0.79}_{-0.63}$ | $19.93^{+0.43}_{-0.39}$ | $4.55^{+0.53}_{-0.72}$
S_40 | HATLASJ225250.7$-$313657 | $21.31^{+0.17}_{-0.16}$ | $22.23^{+0.12}_{-0.10}$ | $0.29\pm 0.02$ | $11.10^{+0.86}_{-0.81}$ | $2.04\pm 0.03$
$-17.32^{+1.21}_{-0.86}$ | $19.97^{+0.72}_{-0.63}$ | $2.09^{+0.27}_{-0.43}$
S_41 | HELMSJ233441.0$-$065220 | $19.79^{+0.17}_{-0.16}$ | $21.04\pm 0.51$ | $0.38^{+0.08}_{-0.05}$ | $5.13^{+0.39}_{-0.40}$ | $172.09\pm 0.22$
$-18.09^{+0.17}_{-0.16}$ | $19.23\pm 0.51$ | $2.44^{+0.53}_{-0.35}$
S_42 | HELMSJ233633.5$-$0321191 | $16.99^{+0.05}_{-0.04}$ | $20.94\pm 0.08$ | $1.29\pm 0.06$ | $7.24^{+0.28}_{-0.29}$ | $14.41\pm 0.21$
– | – | –
HELMSJ233633.5$-$0321192 | $19.16\pm 0.08$ | $23.16^{+0.06}_{-0.05}$ | $1.53\pm 0.04$ | $4.34\pm 0.06$
– | – | –
Confirmed through sub-mm/mm follow-up |
S_43 | HELMSJ001615.7$+$032435 | $18.24^{+0.36}_{-0.34}$ | $23.64^{+0.18}_{-0.16}$ | $2.54^{+0.24}_{-0.22}$ | $9.16^{+1.47}_{-1.63}$ | $<0.04$
$-20.31^{+0.36}_{-0.34}$ | $21.43^{+0.18}_{-0.16}$ | $18.25^{+1.76}_{-1.62}$
S_44 | HELMSJ002220.9$-$015524 | $21.07^{+0.15}_{-0.14}$ | $25.43^{+0.10}_{-0.09}$ | $1.59\pm 0.08$ | $6.62\pm 0.31$ | $<0.04$
$-18.27^{+0.50}_{-0.44}$ | $22.66^{+0.36}_{-0.34}$ | $12.62^{+0.82}_{-0.90}$
S_45 | HELMSJ003814.1$-$002252 | $[22.45]$ | – | – | – | $<0.04$
$-12.66^{+1.43}_{-0.95}$ | – | –
S_46 | HELMSJ003929.6$+$002426 | $22.398\pm 0.003$ | $22.17^{+0.02}_{-0.01}$ | $0.256\pm 0.003$ | $2.38^{+0.08}_{-0.09}$ | $<0.04$
$-16.34^{+0.99}_{-0.73}$ | $19.83^{+0.61}_{-0.53}$ | $1.90^{+0.18}_{-0.31}$
S_47 | HELMSJ004714.2$+$032454 | $20.25^{+0.24}_{-0.23}$ | $23.07^{+0.17}_{-0.16}$ | $0.92\pm 0.14$ | $4.40^{+0.61}_{-0.60}$ | $<0.04$
$-17.43^{+0.54}_{-0.48}$ | $21.38^{+0.31}_{-0.30}$ | $5.57^{+1.05}_{-1.04}$
S_48 | HELMSJ005159.5$+$0622411 | $18.36\pm 0.09$ | $22.71^{+0.10}_{-0.12}$ | $1.67^{+0.11}_{-0.12}$ | $5.95^{+0.91}_{-0.64}$ | $<0.04$
$-19.94\pm 0.09$ | $20.66^{+0.10}_{-0.12}$ | $11.54^{+0.74}_{-0.80}$
HELMSJ005159.5$+$0622412 | $20.87\pm 0.06$ | $20.48\pm 0.03$ | $0.176\pm 0.004$ | $6.987^{+0.001}_{-0.002}$
– | – | –
HELMSJ005159.5$+$0622413 | $20.03\pm 0.09$ | $23.78\pm 0.05$ | $1.42\pm 0.06$ | $4.08^{+0.13}_{-0.11}$
$-18.24\pm 0.09$ | $21.75\pm 0.05$ | $9.78^{+0.41}_{-0.42}$
S_49 | HATLASJ005724.2$-$273122 | $20.36\pm 0.10$ | $24.83^{+0.07}_{-0.06}$ | $1.35\pm 0.05$ | $18.23^{+0.86}_{-0.84}$ | $<0.05$
$-19.00^{+1.52}_{-0.99}$ | $22.05^{+1.01}_{-0.83}$ | $10.76^{+0.88}_{-2.22}$
S_51 | HERMESJ033211$-$270536 | $[23.01]$ | – | – | – | $<0.03$
– | – | –
S_52 | HERMESJ044154$-$540352 | $19.64^{+0.09}_{-0.08}$ | $21.75\pm 0.06$ | $0.48\pm 0.01$ | $13.98^{+0.40}_{-0.41}$ | $<0.03$
– | – | –
S_53 | HATLASJ083932$-$011760 | $19.992\pm 0.002$ | $21.16\pm 0.01$ | $0.458\pm 0.005$ | $2.18\pm 0.03$ | $<0.03$
$-17.34^{+0.84}_{-0.65}$ | $19.65^{+0.38}_{-0.35}$ | $2.60^{+0.38}_{-0.50}$
S_54 | HATLASJ091841$+$0230481 | $20.48^{+0.17}_{-0.16}$ | $25.27^{+0.24}_{-0.30}$ | $1.85^{+0.30}_{-0.34}$ | $9.93^{+5.55}_{-2.95}$ | $<0.04$
$-18.92^{+1.12}_{-0.80}$ | $22.43^{+0.82}_{-0.71}$ | $14.30^{+2.89}_{-3.32}$
HATLASJ091841$+$0230482 | $22.56\pm 0.11$ | $21.80\pm 0.06$ | $0.148\pm 0.006$ | $6.9849^{+0.0029}_{-0.0010}$
$-16.84^{+1.12}_{-0.80}$ | $18.97^{+0.78}_{-0.67}$ | $1.18^{+0.09}_{-0.17}$
S_56 | HATLASJ115433.6$+$005042 | $20.89\pm 0.13$ | $21.10^{+0.08}_{-0.07}$ | $0.28\pm 0.01$ | $3.83^{+0.10}_{-0.11}$ | $<0.03$
$-17.03^{+0.62}_{-0.51}$ | $19.28^{+0.33}_{-0.31}$ | $1.79^{+0.19}_{-0.23}$
S_57 | HATLASJ120127.6$-$014043 | $20.85\pm 0.19$ | $20.44^{+0.60}_{-0.42}$ | $0.18^{+0.04}_{-0.03}$ | $8.27^{+3.41}_{-1.67}$ | $<0.04$
$-18.43^{+1.34}_{-0.91}$ | $17.81^{+1.06}_{-0.91}$ | $1.37^{+0.36}_{-0.29}$
S_58 | HATLASJ131611$+$281220 | $21.87^{+0.22}_{-0.20}$ | $22.68^{+0.15}_{-0.13}$ | $0.29\pm 0.02$ | $8.86^{+0.84}_{-0.78}$ | $<0.03$
$-17.48^{+0.46}_{-0.42}$ | $19.91^{+0.34}_{-0.33}$ | $2.31^{+0.18}_{-0.19}$
S_59 | HATLASJ134429$+$303036 | $19.57^{+0.32}_{-0.30}$ | $20.85^{+0.73}_{-0.69}$ | $0.38^{+0.14}_{-0.08}$ | $6.09^{+0.69}_{-0.68}$ | $<0.04$
$-19.01^{+0.32}_{-0.30}$ | $18.61^{+0.73}_{-0.69}$ | $2.74^{+1.00}_{-0.58}$
Table 18: continued No. | IAU Name | $m_{F110W}$ | $\mu_{\rm 50}$ | $R_{\rm 50}$ | $C_{31}$ |
---|---|---|---|---|---|---
|  | [mag] |  [mag arcsec-2] | [arcsec] |  |
|  | $M_{F110W}$ | $\mu_{\rm 50,\,0}$ | $R_{\rm 50,\,0}$ |  |
|  | [mag] |  [mag kpc-2] | [kcp] |  |
(1) | (2) | (3) | (4) | (5) | (6) |
S_60 | HATLASJ141352$-$0000271 | $18.19^{+0.18}_{-0.17}$ | $22.11^{+0.43}_{-0.42}$ | $1.22^{+0.23}_{-0.18}$ | $7.67\pm 0.48$ | $<0.04$
$-19.85^{+0.18}_{-0.17}$ | $20.21^{+0.43}_{-0.42}$ | $8.01^{+1.52}_{-1.17}$
HATLASJ141352-0000272 | $20.91^{+0.13}_{-0.12}$ | $21.05\pm 0.08$ | $0.229\pm 0.010$ | $6.40^{+0.27}_{-0.26}$
– | – | –
HATLASJ141352$-$0000273 | $19.18\pm 0.08$ | $21.69\pm 0.05$ | $0.64\pm 0.02$ | $8.56\pm 0.18$
$-18.87\pm 0.08$ | $19.79\pm 0.05$ | $4.20^{+0.10}_{-0.11}$
S_61 | HATLASJ142414$+$0223041 | $19.95^{+0.09}_{-0.08}$ | $23.04\pm 0.09$ | $1.11\pm 0.06$ | $10.30^{+0.64}_{-0.53}$ | $<0.03$
$-18.31\pm 0.09$ | $21.68\pm 0.05$ | $7.65^{+0.39}_{-0.40}$
HATLASJ142414$+$0223042 | $21.05^{+0.15}_{-0.14}$ | $24.59^{+0.10}_{-0.09}$ | $0.93\pm 0.05$ | $12.87^{+0.84}_{-0.80}$
$-17.21^{+0.15}_{-0.14}$ | $22.56^{+0.10}_{-0.09}$ | $6.41^{+0.31}_{-0.30}$
S_62 | HERMESJ142826+345547 | $19.254\pm 0.001$ | $20.801\pm 0.007$ | $0.542\pm 0.003$ | $2.56\pm 0.03$ | $<0.03$
$-18.065\pm 0.001$ | $19.297\pm 0.007$ | $3.07\pm 0.02$
S_63 | HATLASJ230815.5$-$343801 | $20.18^{+0.21}_{-0.20}$ | $22.15^{+0.13}_{-0.11}$ | $0.55^{+0.02}_{-0.03}$ | $7.71^{+1.59}_{-1.35}$ | $<0.04$
$-18.58^{+0.93}_{-0.72}$ | $19.80^{+0.59}_{-0.52}$ | $4.05^{+0.42}_{-0.60}$
S_64 | HELMSJ232439.5$-$043936 | $20.34^{+0.21}_{-0.20}$ | $21.64^{+0.31}_{-0.26}$ | $0.40\pm 0.03$ | $5.96^{+0.32}_{-0.29}$ | $<0.04$
$-18.21^{+1.27}_{-0.89}$ | $19.44^{+0.77}_{-0.67}$ | $2.86^{+0.43}_{-0.65}$
S_65 | HELMSJ233620.8$-$060828 | $17.97\pm 0.07$ | $20.39\pm 0.05$ | $0.66\pm 0.02$ | $6.58^{+0.20}_{-0.19}$ | $<0.04$
$-19.24\pm 0.07$ | $18.94\pm 0.05$ | $3.62\pm 0.09$

##  Appendix B Full candidates table

Below, we present the figures and tables that did not enter the full body of
the paper for the sake of readability.

In Table 19, we summarise the properties for all the systems classified as B,
C and D after the inclusion of the multiwavelength follow-ups and the lens
subtraction. Figure 24 shows the candidates classified as C or D.

Table 19: Properties of the 217 systems classified as B, C and D by visual
inspection

.  No. IAU Name Alt. Name Ref. RA Dec Vis. Class. Multiw. Class. $S_{250}$
$S_{350}$ $S_{500}$ Ref. [h m s] [d m s] [mJy] [mJy] [mJy] (1) (2) (3) (4) (5)
(6) (7) (8) (9) (10) (11) (12) S_66 HELMSJ000215.9$-$012829 HELMS3 Na16
00:02:16 $-$01:28:29.00 B – $643.0\pm 7.0$ $510.0\pm 6.0$ $258.0\pm 7.0$ Na16
S_67 HELMSJ001800.1$-$060235 HELMS21 Na16 00:18:00 $-$06:02:35.00 B –
$206.0\pm 6.0$ $186.0\pm 7.0$ $130.0\pm 7.0$ Na16 S_68 HELMSJ002208.1$+$034044
HELMS38 Na16 00:22:08 $+$03:40:44.00 B – $190.0\pm 6.0$ $157.0\pm 6.0$
$113.0\pm 7.0$ Na16 S_69 HATLASJ002533.5$-$333825 HerBS87 Ba18 00:25:34
$-$33:38:26.00 B – $114.7\pm 5.2$ $127.8\pm 6.1$ $96.0\pm 7.3$ Ba18 S_70
HERMESJ002906$-$421419 HELAISS01 Wa13 00:29:06 $-$42:14:19.00 B – $129.0$
$116.0$ $81.0$ Ca14 S_71 HATLASJ003207.7$-$303724 HerBS56 Ba18 00:32:08
$-$30:37:24.00 B – $80.3\pm 5.0$ $106.2\pm 5.2$ $105.8\pm 6.3$ Ne17 S_72
HERMESJ003824$-$433705 HELAISS02 Ca14 00:38:24 $-$43:37:05.00 B D $115.0\pm
6.0$ $124.0\pm 6.0$ $108.0\pm 6.0$ Bu15 S_73 HELMSJ004747.1$+$061444 HELMS26
Na16 00:47:47 $+$06:14:44.00 B – $85.0\pm 7.0$ $119.0\pm 6.0$ $125.0\pm 8.0$
Na16 S_74 HERSJ010301.2$-$003300 HERS6 Na16 01:03:01 $-$00:33:01.00 B –
$121.0\pm 7.0$ $147.0\pm 6.0$ $130.0\pm 8.0$ Na16 S_75 HERSJ011640.1$-$000454
HERS4 Na16 01:16:40 $-$00:04:54.00 B – $137.5\pm 6.75$ $196.11\pm 6.56$
$189.91\pm 7.81$ Su17 S_76 HATLASJ012415.9$-$310500 HerBS69 Ba18 01:24:16
$-$31:05:00.00 B – $140.4\pm 5.4$ $154.5\pm 5.7$ $100.3\pm 7.0$ Ne17 S_77
HERSJ012521.0$+$011724 HERS13 Na16 01:25:21 $+$01:17:24.00 B – $165.0\pm 8.0$
$153.0\pm 7.0$ $114.0\pm 10.0$ Na16 S_78 HERSJ012546.3$-$001143 HERS12 Na16
01:25:46 $-$00:11:43.00 B – $152.0\pm 8.0$ $135.0\pm 7.0$ $114.0\pm 9.0$ Na16
S_79 HERSJ012754.1$+$004940 HERS3 Na16 01:27:54 $+$00:49:40.00 B – $253.0\pm
6.0$ $250.0\pm 6.0$ $191.0\pm 7.0$ Na16 S_80 HATLASJ012853.0$-$332719 HerBS73
Ba18 01:28:53 $-$33:27:19.00 B – $117.1\pm 6.0$ $129.0\pm 6.2$ $99.6\pm 7.4$
Ba18 S_81 HATLASJ013840.5$-$281855 HerBS14 Ba18 01:38:41 $-$28:18:56.00 B Unc.
$116.3\pm 5.7$ $177.0\pm 6.0$ $179.4\pm 7.1$ Ne17 S_82
HATLASJ013951.9$-$321446 HerBS55 Ba18 01:39:52 $-$32:14:46.00 B – $109.0\pm
4.9$ $116.5\pm 5.3$ $107.1\pm 6.2$ Ne17 S_83 HERSJ021402.6$-$004612 HERS17
Na16 02:14:03 $-$00:46:12.00 B – $110.0\pm 8.0$ $130.0\pm 8.0$ $105.0\pm 9.0$
Na16 S_84 HERSJ021434.4$+$005926 HERS16 Na16 02:14:34 $+$00:59:26.00 B –
$110.0\pm 9.0$ $134.0\pm 8.0$ $109.0\pm 10.0$ Na16 S_85 HERMESJ022017$-$060143
HXMM01 Wa13 02:20:17 $-$06:01:44.00 B Unc. $179.0\pm 7.0$ $188.0\pm 8.0$
$134.0\pm 7.0$ Bu15 S_86 HERMESJ022022$-$015329 HXMM04 Wa13 02:20:22
$-$01:53:29.00 B D $162.0\pm 7.0$ $157.0\pm 8.0$ $125.0\pm 11.0$ Bu15 S_87
HERMESJ022029$-$064846 HXMM09 Wa13 02:20:29 $-$06:48:46.00 B D $129.0\pm 7.0$
$118.0\pm 8.0$ $85.0\pm 7.0$ Bu15 S_88 HERMESJ022135$-$062617 HXMM03 Wa13
02:21:35 $-$06:26:17.00 B Unc. $114.0\pm 7.0$ $134.0\pm 8.0$ $116.0\pm 7.0$
Bu15 S_89 HERMESJ022548$-$041750 HXMM05 Wa13 02:25:48 $-$04:17:50.00 B D
$103.0\pm 7.0$ $118.0\pm 8.0$ $97.0\pm 7.0$ Bu15 S_90 HERMESJ045027$-$524126
HADFS08 Ca14 04:50:27 $-$52:41:26.00 B D $142.0\pm 6.0$ $133.0\pm 6.0$
$90.0\pm 6.0$ Bu15 S_91 HERMESJ045058$-$531654 HADFS03 Ca14 04:50:58
$-$53:16:54.00 B Unc. $119.0\pm 6.0$ $102.0\pm 6.0$ $63.0\pm 6.0$ Bu15 S_92
HATLASJ084933$+$021443 G09-v1.124 08:49:33 $+$02:14:43.14 B D $216.7\pm 7.5$
$248.5\pm 8.2$ $208.6\pm 8.6$ Ne17 HerBS8 Ba18 S_93 HATLASJ084958$+$010713
G09v1.1259 08:49:58 $+$01:07:12.73 B – $81.2\pm 7.3$ $98.9\pm 8.2$ $85.2\pm
8.7$ Ba18 HerBS157 Ba18 S_94 HATLASJ090453.2$+$022017 HerBS183 Ba18 09:04:53
$+$02:20:17.87 B – $87.0\pm 7.2$ $98.2\pm 8.0$ $82.3\pm 8.8$ Ba18 SDP.392 S_95
HATLASJ091331$-$003644 SDP.44 09:13:31 $-$00:36:44.00 B – $175.5\pm 6.5$
$142.2\pm 7.4$ $85.8\pm 7.8$ Va16 S_96 HATLASJ092136$+$000132 HerBS91 Ba18
09:21:36 $+$00:01:31.92 B – $139.2\pm 7.3$ $128.8\pm 8.1$ $95.1\pm 8.6$ Ba18
S_97 HATLASJ092409$-$005018 HerBS185 09:24:09 $-$00:50:18.00 B – $71.8\pm 7.4$
$87.7\pm 8.2$ $82.2\pm 8.5$ Ba18 S_98 HERMESJ103618$+$585454 HLock05 Wa13
10:36:18 $+$58:54:54.36 B – $71.0$ $102.0$ $98.0$ Ca14 S_99
HATLASJ113804$-$011736 HerBS96 Ba18 11:38:04 $-$01:17:36.00 B – $85.1\pm 7.3$
$98.4\pm 8.2$ $94.8\pm 8.8$ Ba18 S_100 HATLASJ113833.3$+$004909 HerBS100 Ba18
11:38:33 $+$00:49:09.68 B – $96.8\pm 7.3$ $106.4\pm 8.1$ $93.4\pm 8.7$ Ba18
S_101 HATLASJ113841$-$020237 – – 11:38:41 $-$02:02:37.00 B – $45.2\pm 7.0$
$72.7\pm 7.7$ $71.7\pm 8.1$ Ma18 S_102 HATLASJ115112$-$012638 HerBS53 Ba18
11:51:12 $-$01:26:38.00 B – $141.2\pm 7.4$ $137.7\pm 8.2$ $108.4\pm 8.8$ Ne17
S_103 HATLASJ115120$-$003322 – – 11:51:20 $-$00:33:22.00 B – $146.9\pm 7.8$
$150.3\pm 8.5$ $88.0\pm 8.8$ Ma18 S_104 HATLASJ120127.8$-$021648 – – 12:01:28
$-$02:16:48.00 B – $207.9\pm 7.3$ $160.9\pm 8.2$ $103.6\pm 8.7$ Ne17 S_105
HATLASJ120319.1$-$011253 HerBS50 Ba18 12:03:19 $-$01:12:54.00 B – $114.3\pm
7.4$ $142.8\pm 8.2$ $110.2\pm 8.6$ Ne17 S_106 HATLASJ121301.5$-$004922 HerBS48
Ba18 12:13:02 $-$00:49:23.00 B – $136.6\pm 6.6$ $142.6\pm 7.4$ $110.9\pm 7.7$
Ne17 S_107 HATLASJ121334.9$-$020323 – – 12:13:35 $-$02:03:23.00 B – $211.0$
$197.9$ $129.9$ Ne17 S_108 HATLASJ121542.7$-$005220 HerBS62 Ba18 12:15:43
$-$00:52:20.00 B – $119.7\pm 7.4$ $135.5\pm 8.2$ $103.4\pm 8.6$ Ne17 S_109
HATLASJ130054$+$260303 HerBS129 Ba18 13:00:54 $+$26:03:02.68 B – $59.4\pm 5.9$
$85.4\pm 5.9$ $89.0\pm 7.0$ Ba18 S_110 HATLASJ131322$+$285836 – – 13:13:22
$+$28:58:35.61 B – $160.8\pm 7.4$ $116.0\pm 8.4$ $68.0\pm 8.8$ Ma18 S_111
HATLASJ134159$+$292833 – – 13:41:59 $+$29:28:32.54 B – $174.4\pm 6.7$
$172.3\pm 7.7$ $109.2\pm 8.1$ Ne17 S_112 HATLASJ141833$+$010212 HerBS110 Ba18
14:18:33 $+$01:02:12.40 B – $66.0$ $106.5$ $92.8$ Ba18 S_113
HERMESJ142201$+$533214 HEGS01 14:22:01 $+$53:32:13.70 B – $74.0$ $98.0$ $89.0$
Ca14 S_114 HATLASJ142318.3$+$013913 – – 14:23:18 $+$01:39:13.80 B – $61.8\pm
7.5$ $83.0\pm 8.2$ $65.1\pm 8.8$ Ma18 S_115 HATLASJ143203$-$005219 – –
14:32:03 $-$00:52:19.00 B – $160.6\pm 7.6$ $125.0\pm 8.3$ $76.1\pm 8.9$ Ma18
S_116 HERMESJ143331$+$345440 HBootes01 14:33:31 $+$34:54:39.60 B Unc. $158.0$
$191.0$ $160.0$ Ca14 S_117 HATLASJ144243$+$015506 HerBS153 Ba18 14:42:43
$+$01:55:05.86 B – $123.2\pm 7.2$ $133.4\pm 8.1$ $85.7\pm 8.8$ Ba18 S_118
HATLASJ144715$-$012114 – – 14:47:15 $-$01:21:14.00 B – $132.7\pm 7.3$
$118.9\pm 8.2$ $74.7\pm 8.6$ Ma18 S_119 HATLASJ222503.7$-$304847 HerBS166 Ba18
22:25:04 $-$30:48:48.00 B D $32.4\pm 7.2$ $50.1\pm 8.5$ $84.3\pm 10.3$ Ba18
UR085S S_120 HATLASJ223942.4$-$333304 HerBS111 Ba18 22:39:42 $-$33:33:04.00 B
– $105.9\pm 6.5$ $115.6\pm 6.2$ $92.7\pm 7.4$ Ba18 S_121
HATLASJ224026.5$-$315154 HerBS148 Ba18 22:40:27 $-$31:51:55.00 B – $120.6\pm
5.0$ $121.2\pm 5.5$ $86.3\pm 6.8$ Ba18 S_122 HATLASJ224759.6$-$310134 HerBS141
Ba18 22:48:00 $-$31:01:35.00 B – $122.1\pm 6.1$ $124.4\pm 6.5$ $87.3\pm 7.5$
Ba18

Notes: Col. (1): Source reference number. Col. (2): IAU name of the Herschel
detection. Cols. (3) and (4): Alternative name and reference. Cols. (5) and
(6): ICRS RA and Dec coordinate (J2000.0) of the Herschel detection. Cols. (7)
and (8): Visual and multiwavelength lens classifications. Col. (9), (10),
(11), and (11): SPIRE flux density at 250 $\mu{\rm m}$, 350 $\mu{\rm m}$, 500
$\mu{\rm m}$ and reference.

Table 20: continued No. | IAU Name | Alt. Name | Ref. | RA | Dec | Vis. Class. | Multiw. Class. | $S_{250}$ | $S_{350}$ | $S_{500}$ | Ref.
---|---|---|---|---|---|---|---|---|---|---|---
|  |  |  | [h m s] | [d m s] |  |  | [mJy] | [mJy] | [mJy] |
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12)
S_123 |  HATLASJ224805.3$-$335820 | HerBS33 | Ba18 | 22:48:05 |  $-$33:58:20.00 | B | – | $122.3\pm 5.7$ | $135.5\pm 6.3$ | $126.9\pm 7.2$ | Ne17
S_124 |  HATLASJ225045.5$-$304719 | HerBS168 | Ba18 | 22:50:46 |  $-$30:47:19.00 | B | – | $65.5\pm 6.1$ | $88.1\pm 6.1$ | $84.0\pm 7.5$ | Na16
S_125 |  HATLASJ230546.2$-$331038 | HerBS49 | Ba18 | 23:05:46 |  $-$33:10:39.00 | B | – | $76.8\pm 5.6$ | $110.9\pm 5.9$ | $110.4\pm 7.0$ | Ne17
S_126 |  HELMSJ231447.5$-$045658 | HELMS44 | Na16 | 23:14:48 |  $-$04:56:58.00 | B | – | $220.0\pm 8.0$ | $141.0\pm 7.0$ | $106.0\pm 8.0$ | Na16
S_127 |  HATLASJ232210.9$-$333749 | HerBS146 | Ba18 | 23:22:11 |  $-$33:37:49.00 | B | – | $122.4\pm 5.2$ | $134.6\pm 5.4$ | $86.6\pm 6.8$ | Ba18
S_128 |  HATLASJ232531.3$-$302235 | HerBS17 | Ba18 | 23:25:31 |  $-$30:22:36.00 | B | – | $175.5\pm 4.3$ | $227.0\pm 4.7$ | $175.7\pm 5.7$ | Ne17
S_129 |  HELMSJ232617.5$-$025319 | HELMS51 | Na16 | 23:26:18 |  $-$02:53:19.00 | B | – | $86.0\pm 6.0$ | $109.0\pm 6.0$ | $104.0\pm 7.0$ | Na16
S_130 |  HELMSJ232831.8$-$004035 | HELMS55 | Na16 | 23:28:32 |  $-$00:40:35.00 | B | – | $95.0\pm 7.0$ | $120.0\pm 6.0$ | $102.0\pm 7.0$ | Na16
S_131 |  HELMSJ232833.6$-$031416 | HELMS48 | Na16 | 23:28:34 |  $-$03:14:16.00 | B | – | $49.0\pm 6.0$ | $104.0\pm 6.0$ | $105.0\pm 8.0$ | Na16
S_132 |  HELMSJ233420.4$-$003458 | HELMS43 | Na16 | 23:34:20 |  $-$00:34:58.00 | B | – | $156.0\pm 7.0$ | $141.0\pm 5.0$ | $109.0\pm 8.0$ | Na16
S_133 |  HELMSJ233721.9$-$064740 | HELMS49 | Na16 | 23:37:22 |  $-$06:47:40.00 | B | – | $173.0\pm 6.0$ | $161.0\pm 7.0$ | $105.0\pm 8.0$ | Na16
S_134 |  HELMS233728.8$-$045106 | HELMS20 | Na16 | 23:37:29 |  $-$04:51:06.00 | B | – | $162.0\pm 6.0$ | $178.0\pm 7.0$ | $132.0\pm 8.0$ | Na16
S_135 |  HELMSJ234314.0$+$012152 | HELMS36 | Na16 | 23:43:14 |  $+$01:21:52.00 | B | – | $115.0\pm 6.0$ | $115.0\pm 6.0$ | $113.0\pm 8.0$ | Na16
S_136 |  HATLASJ234955.7$-$330833 | HerBS184 | Ba18 | 23:49:56 |  $-$33:08:33.00 | B | – | $91.9\pm 5.9$ | $107.6\pm 6.0$ | $82.3\pm 7.1$ | Ba18
S_137 |  HELMSJ235101.7$-$024425 | HELMS50 | Na16 | 23:51:02 |  $-$02:44:26.00 | B | – | $112.0\pm 6.0$ | $124.0\pm 6.0$ | $105.0\pm 7.0$ | Na16
S_138 |  HATLASJ235121.9$-$332902 | HerBS159 | Ba18 | 23:51:22 |  $-$33:29:02.00 | B | Unc. | $92.1\pm 5.9$ | $98.3\pm 5.9$ | $85.0\pm 7.1$ | Ba18
S_139 |  HELMSJ235331.7$+$031717 | HELMS40 | Na16 | 23:53:32 |  $+$03:17:18.00 | B | – | $102.0\pm 6.0$ | $123.0\pm 7.0$ | $111.0\pm 7.0$ | Na16
S_140 |  HATLASJ000455.3$-$330811 | HerBS170 | Ba18 | 00:04:55 |  $-$33:08:12.00 | C | D | $61.9\pm 5.4$ | $78.8\pm 6.0$ | $83.8\pm 7.0$ | Ba18
S_141 |  HATLASJ001030.1$-$330621 | HerBS98 | Ba18 | 00:10:30 |  $-$33:06:22.00 | C | – | $56.3\pm 4.9$ | $51.7\pm 5.0$ | $94.4\pm 6.5$ | Ba18
S_142 |  HELMSJ001226.9$+$020810 | HELMS45 | Na16 | 00:12:27 |  $+$02:08:10.00 | C | – | $107.0\pm 6.0$ | $142.0\pm 6.0$ | $106.0\pm 7.0$ | Na16
S_143 |  HELMSJ001325.7$+$042509 | HELMS56 | Na16 | 00:13:26 |  $+$04:25:09.00 | C | – | $89.0\pm 6.0$ | $98.0\pm 6.0$ | $102.0\pm 7.0$ | Na16
S_144 |  HATLASJ002144.8$-$295217 | HerBS156 | Ba18 | 00:21:45 |  $-$29:52:18.00 | C | – | $103.7\pm 5.7$ | $91.3\pm 6.1$ | $85.4\pm 6.9$ | Ba18
S_145 |  HELMSJ002719.5$+$001204 | HELMS34 | Na16 | 00:27:20 |  $+$00:12:04.00 | C | – | $248.0\pm 6.0$ | $206.0\pm 7.0$ | $116.0\pm 8.0$ | Na16
S_146 |  HERMESJ002854$-$420457 | HELAISS04 | Ca14 | 00:28:54 |  $-$42:04:57.00 | C | – | $131.0$ | $102.0$ | $58.0$ | Ca14
S_147 |  HELMSJ003519.7$+$072806 | HELMS57 | Na16 | 00:35:20 |  $+$07:28:06.00 | C | – | $134.0\pm 7.0$ | $135.0\pm 7.0$ | $101.0\pm 8.0$ | Na16
S_148 |  HATLASJ003728.7$-$284124 | HerBS174 | Ba18 | 00:37:29 |  $-$28:41:25.00 | C | – | $95.6\pm 5.7$ | $84.8\pm 5.9$ | $83.2\pm 7.4$ | Ba18
S_149 |  HELMSJ004622.3$+$073509 | HELMS46 | Na16 | 00:46:22 |  $+$07:35:09.00 | C | – | $82.0\pm 9.0$ | $113.0\pm 9.0$ | $105.0\pm 10.0$ | Na16
S_150 |  HATLASJ005132.8$-$301848 | HerBS45 | Ba18 | 00:51:33 |  $-$30:18:48.00 | C | – | $164.6\pm 5.4$ | $160.2\pm 5.8$ | $113.0\pm 7.2$ | Ne17
S_151 |  HELMSJ005258.6$+$061319 | HELMS10 | Na16 | 00:52:59 |  $+$06:13:19.00 | C | D | $88.0\pm 6.0$ | $129.0\pm 6.0$ | $155.0\pm 7.0$ | Na16
S_152 |  HATLASJ005849.9$-$290122 | HerBS181 | Ba18 | 00:58:50 |  $-$29:01:22.00 | C | – | $92.5\pm 5.7$ | $116.6\pm 6.0$ | $82.6\pm 7.2$ | Ba18
S_153 |  HATLASJ011014.5$-$314813 | HerBS160 | Ba18 | 01:10:15 |  $-$31:48:14.00 | C | Unc. | $48.6\pm 5.6$ | $84.2\pm 6.0$ | $84.8\pm 7.1$ | Ba18
S_154 |  HATLASJ011730.3$-$320719 | HerBS138 | Ba18 | 01:17:30 |  $-$32:07:19.00 | C | – | $120.4\pm 5.8$ | $111.2\pm 6.4$ | $87.4\pm 7.8$ | Ba18
S_155 |  HATLASJ012209.4$-$273824 | HerBS114 | Ba18 | 01:22:09 |  $-$27:38:24.00 | C | – | $81.7\pm 5.9$ | $93.8\pm 6.0$ | $91.8\pm 7.7$ | Ba18
S_156 |  HATLASJ012335.1$-$314618 | HerBS145 | Ba18 | 01:23:35 |  $-$31:46:19.00 | C | D | $54.7\pm 6.0$ | $67.4\pm 6.2$ | $86.8\pm 7.7$ | Ba18
S_157 |  HERSJ013212.2$+$001754 | HERS18 | Na16 | 01:32:12 |  $+$00:17:54.00 | C | – | $176.0\pm 7.0$ | $175.0\pm 6.0$ | $104.0\pm 8.0$ | Na16
S_158 |  HATLASJ013239.9$-$330906 | HerBS40 | Ba18 | 01:32:40 |  $-$33:09:07.00 | C | – | $112.0\pm 5.5$ | $148.8\pm 6.2$ | $117.7\pm 7.0$ | Ne17
S_159 |  HERSJ014057.3$-$010547 | HERS14 | Na16 | 01:40:57 |  $-$01:05:47.00 | C | – | $136.0\pm 8.0$ | $143.0\pm 8.0$ | $112.0\pm 9.0$ | Na16
S_160 |  HATLASJ014520.0$-$313834 | HerBS107 | Ba18 | 01:45:20 |  $-$31:38:35.00 | C | – | $97.3\pm 6.1$ | $99.1\pm 6.4$ | $93.1\pm 7.8$ | Ba18
S_161 |  HERSJ020529.1$+$000501 | HERS19 | Na16 | 02:05:29 |  $+$00:05:01.00 | C | – | $89.0\pm 6.0$ | $112.0\pm 6.0$ | $102.0\pm 8.0$ | Na16
S_162 |  HERMESJ021632$-$053421 | HXMM14 | Ca14 | 02:16:32 |  $-$05:34:21.00 | C | – | $98.0$ | $98.0$ | $78.0$ | Ca14
S_163 |  HERMESJ021837$-$035315 | HXMM13 | Ca14 | 02:18:37 |  $-$03:53:15.00 | C | – | $55.0$ | $88.0$ | $94.0$ | Ca14
S_164 |  HERMESJ021943$-$052433 | HXMM20 | Ca14 | 02:19:43 |  $-$05:24:33.00 | C | D | $85.0$ | $79.0$ | $67.0$ | Ca14
S_165 |  HERMESJ022206$-$070727 | HXMM23 | Ca14 | 02:22:06 |  $-$07:07:27.00 | C | D | $137.0$ | $108.0$ | $57.0$ | Ca14
S_166 |  HERMESJ022213$-$070222 | HXMM28 | Ca14 | 02:22:13 |  $-$07:02:22.00 | C | – | $27.0$ | $47.0$ | $87.0$ | Ca14
S_167 |  HERMESJ022251$-$032414 | HXMM22 | Ca14 | 02:22:51 |  $-$03:24:14.00 | C | D | $101.0\pm 6.0$ | $85.0\pm 6.0$ | $61.0\pm 6.0$ | Bu15
S_168 |  HERMESJ022515$-$024707 | HXMM19 | Ca14 | 02:25:15 |  $-$02:47:07.00 | C | – | $43.0$ | $67.0$ | $70.0$ | Ca14
S_169 |  HERMESJ022518$-$044610 | HXMM27 | Ca14 | 02:25:17 |  $-$04:46:10.00 | C | – | $0.0$ | $48.0$ | $43.0$ | Ca14
S_170 |  HERMESJ023006$-$034153 | HXMM12 | Ca14 | 02:30:06 |  $-$03:41:53.00 | C | Unc. | $98.0\pm 7.0$ | $106.0\pm 8.0$ | $82.0\pm 7.0$ | Bu15
S_171 |  HERMESJ032434$-$292646 | HECDFS08 | Ca14 | 03:24:34 |  $-$29:26:46.00 | C | – | $104.0$ | $67.0$ | $54.0$ | Ca14
S_172 |  HERMESJ032443$-$282134 | HECDFS03 | Ca14 | 03:24:43 |  $-$28:21:34.00 | C | – | $83.0$ | $118.0$ | $113.0$ | Ca14
S_173 |  HERMESJ032713$-$285106 | HECDFS09 | Ca14 | 03:27:13 |  $-$28:51:06.00 | C | – | $77.0$ | $66.0$ | $51.0$ | Ca14
S_174 |  HERMESJ033118$-$272015 | HECDFS11 | Ca14 | 03:31:18 |  $-$27:20:15.00 | C | – | $45.0$ | $52.0$ | $42.0$ | Ca14
S_175 |  HERMESJ043341$-$540338 | HADFS04 | Ca14 | 04:33:41 |  $-$54:03:38.00 | C | Unc. | $74.0\pm 6.0$ | $93.0\pm 6.0$ | $84.0\pm 6.0$ | Bu15
S_176 |  HERMESJ043830$-$541832 | HADFS02 | Ca14 | 04:38:30 |  $-$54:18:32.00 | C | D | $19.0\pm 6.0$ | $39.0\pm 5.0$ | $52.0\pm 6.0$ | Bu15
S_177 |  HERMESJ044947$-$525427 | HADFS09 | Ca14 | 04:49:47 |  $-$52:54:27.00 | C | D | $98.0\pm 6.0$ | $102.0\pm 6.0$ | $72.0\pm 6.0$ | Bu15
S_178 |  HATLASJ083153$+$014014 | – | – | 08:31:53 |  $+$01:40:14.43 | C | D | $69.8\pm 7.3$ | $93.0\pm 8.1$ | $82.0\pm 8.6$ | Va16
S_179 |  HATLASJ083546$+$002804 | – | – | 08:35:46 |  $+$00:28:03.75 | C | – | $86.6\pm 6.6$ | $94.5\pm 7.5$ | $79.5\pm 8.0$ | Va16
S_180 |  HATLASJ083817$-$004134 | HerBS108 | Ba18 | 08:38:17 |  $-$00:41:34.00 | C | – | $84.5\pm 7.4$ | $106.1\pm 8.2$ | $93.0\pm 8.8$ | Ba18
S_181 |  HATLASJ083859.3$+$021325 | HerBS169 | Ba18 | 08:38:59 |  $+$02:13:25.87 | C | – | $95.2\pm 7.5$ | $105.2\pm 8.2$ | $84.0\pm 8.7$ | Ba18
S_182 |  HATLASJ083945$+$021023 | HerBS171 | Ba18 | 08:39:45 |  $+$02:10:22.83 | C | – | $71.3\pm 7.3$ | $97.4\pm 8.1$ | $83.4\pm 8.6$ | Ba18
S_183 |  HATLASJ084259.9$+$024959 | HerBS188 | Ba18 | 08:43:00 |  $+$02:49:59.02 | C | – | $84.2\pm 7.4$ | $101.5\pm 8.1$ | $81.8\pm 8.6$ | Ba18
S_184 |  HATLASJ085033$+$012914 | – | – | 08:50:33 |  $+$01:29:14.10 | C | – | $182.5\pm 6.9$ | $131.6\pm 7.7$ | $74.7\pm 8.0$ | Ma18
S_185 |  HATLASJ085126$+$014638 | – | – | 08:51:26 |  $+$01:46:38.37 | C | – | $66.4\pm 7.4$ | $92.3\pm 8.1$ | $79.1\pm 8.5$ | Va16
S_186 |  HATLASJ085309$-$005727 | HerBS136 | Ba18 | 08:53:09 |  $-$00:57:27.00 | C | – | $68.3\pm 7.5$ | $97.5\pm 8.2$ | $87.7\pm 8.6$ | Ne17
S_187 |  HATLASJ090953$-$010811 | SDP.60 |  | 09:09:53 |  $-$01:08:11.00 | C | – | $152.1\pm 7.2$ | $109.3\pm 8.1$ | $83.5\pm 8.4$ | Va16
S_188 |  HATLASJ091454$-$010357 | HerBS142 | Ba18 | 09:14:54 |  $-$01:03:57.00 | C | D | $69.0\pm 7.3$ | $72.2\pm 8.1$ | $87.2\pm 8.5$ | Ba18
S_189 |  HATLASJ091809$+$001927 | HerBS99 | Ba18 | 09:18:09 |  $+$00:19:27.27 | C | – | $93.2\pm 7.4$ | $116.6\pm 8.2$ | $94.3\pm 8.7$ | Ba18
S_190 |  HATLASJ091857$-$000047 | – | – | 09:18:57 |  $-$00:00:47.00 | C | – | $171.6\pm 6.4$ | $145.7\pm 7.4$ | $85.1\pm 7.7$ | Va16
S_191 |  HATLASJ091949$-$005037 | – | – | 09:19:49 |  $-$00:50:37.00 | C | – | $150.7\pm 7.5$ | $141.4\pm 8.4$ | $90.4\pm 8.7$ | Va16
S_192 |  HATLASJ092141$+$005356 | – | – | 09:21:41 |  $+$00:53:55.58 | C | – | $71.2\pm 7.3$ | $85.4\pm 8.2$ | $79.6\pm 8.8$ | Va16
S_193 |  HERMESJ100057$+$022014 | HCOSMOS02 | Ca14 | 10:00:57 |  $+$02:20:13.70 | C | D | $70.0\pm 6.0$ | $85.0\pm 6.0$ | $71.0\pm 6.0$ | Bu15
|  | COSBO3 |  |  |  |  |  |  |  |  |
Table 21: continued No. | IAU Name | Alt. Name | Ref. | RA | Dec | Vis. Class. | Multiw. Class. | $S_{250}$ | $S_{350}$ | $S_{500}$ | Ref.
---|---|---|---|---|---|---|---|---|---|---|---
|  |  |  | [h m s] | [d m s] |  |  | [mJy] | [mJy] | [mJy] |
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12)
S_194 |  HERMESJ103958$+$563120 | HLock17 | Wa13 | 10:39:58 |  $+$56:31:19.92 | C | – | $62.0$ | $82.0$ | $67.0$ | Ca14
S_195 |  HERMESJ104051$+$560654 | HLock02 | Wa13 | 10:40:51 |  $+$56:06:54.14 | C | – | $53.0$ | $115.0$ | $140.0$ | Ca14
|  | LSW102 |  |  |  |  |  |  |  |  |
S_196 |  HERMESJ104140$+$570859 | HLock11 | Wa13 | 10:41:40 |  $+$57:08:59.42 | C | – | $97.0$ | $112.0$ | $80.0$ | Ca14
S_197 |  HERMESJ105712$+$565458 | HLock03 | Wa13 | 10:57:12 |  $+$56:54:58.25 | C | – | $114.0\pm 7.0$ | $147.0\pm 10.0$ | $114.0\pm 8.0$ | Ca14
S_198 |  HATLASJ113243$-$005109 | HerBS71 | Ba18 | 11:32:43 |  $-$00:51:09.00 | C | – | $68.0\pm 7.0$ | $106.0\pm 8.0$ | $100.0\pm 9.0$ | Ma19
S_199 |  HATLASJ113834$-$014657 | HerBS119 | Ba18 | 11:38:34 |  $-$01:46:57.00 | C | – | $68.5\pm 7.2$ | $85.6\pm 8.1$ | $91.2\pm 8.6$ | Ba18
S_200 |  HATLASJ114753$-$005832 | HerBS85 | Ba18 | 11:47:53 |  $-$00:58:32.00 | C | – | $92.1\pm 6.6$ | $104.2\pm 7.4$ | $96.0\pm 7.7$ | Ba18
S_201 |  HATLASJ115521$-$021332 | HERBS179 |  | 11:55:21 |  $-$02:13:32.00 | C | D | $67.3\pm 7.2$ | $84.9\pm 8.1$ | $75.7\pm 8.9$ | Va16
S_202 |  HATLASJ115820$-$013754 | HerBS66 | Ba18 | 11:58:20 |  $-$01:37:54.00 | C | – | $120.0\pm 7.0$ | $124.0\pm 8.0$ | $101.0\pm 8.0$ | Ma19
S_203 |  HATLASJ120600.7$+$003459 | HerBS74 | Ba18 | 12:06:01 |  $+$00:34:59.51 | C | – | $88.7\pm 7.4$ | $104.1\pm 8.1$ | $98.8\pm 8.7$ | Ba18
S_204 |  HATLASJ120709.2$-$014702 | HerBS51 | Ba18 | 12:07:09 |  $-$01:47:03.00 | C | – | $143.2\pm 7.4$ | $149.2\pm 8.1$ | $110.3\pm 8.7$ | Ne17
S_205 |  HATLASJ121348.0$+$010812 | HerBS116 | Ba18 | 12:13:48 |  $+$01:08:12.59 | C | – | $65.1\pm 7.4$ | $96.6\pm 8.2$ | $93.6\pm 8.5$ | Ba18
S_206 |  HATLASJ121416.3$-$013704 | HerBS164 | Ba18 | 12:14:16 |  $-$01:37:04.00 | C | – | $88.0\pm 6.4$ | $99.3\pm 7.4$ | $84.3\pm 7.7$ | Ba18
S_207 |  HATLASJ121812.8$+$011841 | HerBS83 | Ba18 | 12:18:13 |  $+$01:18:41.67 | C | D | $49.5\pm 7.2$ | $79.7\pm 8.1$ | $94.1\pm 8.8$ | Ba18
S_208 |  HATLASJ122034.2$-$003805 | HerBS197 | Ba18 | 12:20:34 |  $-$00:38:06.00 | C | – | $81.9\pm 7.5$ | $93.8\pm 8.2$ | $84.8\pm 8.7$ | Ba18
S_209 |  HATLASJ122117.0$-$014924 | – | – | 12:21:17 |  $-$01:49:24.00 | C | – | $146.6\pm 7.4$ | $128.9\pm 8.2$ | $87.2\pm 8.3$ | Va16
S_210 |  HATLASJ122158.5$+$003326 | HerBS124 | Ba18 | 12:21:59 |  $+$00:33:26.15 | C | – | $135.7\pm 7.3$ | $116.1\pm 8.2$ | $89.8\pm 8.6$ | Ba18
S_211 |  HATLASJ122407.4$-$003247 | HerBS161 | Ba18 | 12:24:07 |  $-$00:32:47.00 | C | D | $56.5\pm 7.3$ | $75.7\pm 8.1$ | $82.4\pm 8.8$ | Ba18
S_212 |  HATLASJ122459.1$-$005647 | HerBS150 | Ba18 | 12:24:59 |  $-$00:56:47.00 | C | D | $53.6\pm 7.2$ | $81.3\pm 8.3$ | $92.0\pm 8.9$ | Ba18
S_213 |  HATLASJ125105$+$261653 | NGP.2070 |  | 12:51:05 |  $+$26:16:52.62 | C | – | $116.5\pm 5.5$ | $125.3\pm 6.5$ | $81.3\pm 7.7$ | Va16
S_214 |  HATLASJ125653$+$275903 | HerBS31 | Ba18 | 12:56:53 |  $+$27:59:02.98 | C | – | $133.9\pm 7.5$ | $164.1\pm 8.2$ | $131.8\pm 8.9$ | Ne17
S_215 |  HATLASJ125810$+$263710 | – | – | 12:58:10 |  $+$26:37:09.99 | C | – | $131.6\pm 7.3$ | $122.9\pm 8.3$ | $78.8\pm 8.5$ | Ma18
S_216 |  HATLASJ130601$+$231322 | – | – | 13:06:01 |  $+$23:13:21.65 | C | – | $86.0\pm 7.3$ | $88.0\pm 8.2$ | $76.5\pm 8.6$ | Va16
S_217 |  HATLASJ131001$+$264759 | – | – | 13:10:01 |  $+$26:47:59.05 | C | – | $142.1\pm 7.3$ | $124.1\pm 8.2$ | $81.2\pm 8.9$ | Va16
S_218 |  HATLASJ131020$+$253731 | – | – | 13:10:20 |  $+$25:37:31.47 | C | – | $186.4\pm 7.3$ | $158.7\pm 8.1$ | $93.7\pm 8.5$ | Va16
S_219 |  HATLASJ131609$+$254931 | – | – | 13:16:09 |  $+$25:49:31.15 | C | – | $121.4\pm 7.3$ | $108.2\pm 8.1$ | $76.8\pm 8.7$ | Va16
S_220 |  HATLASJ131642$+$251158 | – | – | 13:16:42 |  $+$25:11:58.38 | C | – | $62.7\pm 6.9$ | $71.5\pm 7.7$ | $63.9\pm 8.1$ | Ma18
S_221 |  HATLASJ131805$+$325018 | HerBS173 | Ba18 | 13:18:05 |  $+$32:50:18.05 | C | – | $73.3\pm 5.6$ | $92.7\pm 6.0$ | $83.3\pm 7.2$ | Ba18
S_222 |  HATLASJ132128$+$282023 | HerBS127 | Ba18 | 13:21:28 |  $+$28:20:22.74 | C | – | $110.0\pm 5.5$ | $122.7\pm 6.1$ | $89.5\pm 6.9$ | Ba18
S_223 |  HATLASJ132227$+$300723 | – | – | 13:22:27 |  $+$30:07:22.54 | C | – | $48.0\pm 7.3$ | $78.6\pm 8.2$ | $25.0\pm 8.8$ | Va16
S_224 |  HATLASJ132302$+$341650 | HerBS30 | Ba18 | 13:23:02 |  $+$34:16:49.66 | C | – | $124.2\pm 7.3$ | $144.6\pm 8.2$ | $137.0\pm 8.7$ | Ne17
S_225 |  HATLASJ132419$+$320754 | HerBS43 | Ba18 | 13:24:19 |  $+$32:07:54.43 | C | – | $84.5\pm 6.8$ | $116.0\pm 7.6$ | $115.4\pm 8.0$ | Ne17
S_226 |  HATLASJ132909$+$300958 | HerBS204 | Ba18 | 13:29:09 |  $+$30:09:58.23 | C | – | $57.9\pm 5.5$ | $95.3\pm 6.1$ | $80.1\pm 7.1$ | Ba18
S_227 |  HATLASJ133255$+$265529 | – | – | 13:32:55 |  $+$26:55:29.23 | C | – | $192.5\pm 7.4$ | $167.4\pm 8.1$ | $116.6\pm 8.6$ | Ne17
S_228 |  HATLASJ133256$+$342210 | HerBS44 | Ba18 | 13:32:56 |  $+$34:22:09.50 | C | – | $164.3\pm 7.5$ | $186.8\pm 8.1$ | $114.9\pm 8.7$ | Ne17
|  | NA.v1.267 |  |  |  |  |  |  |  |  |
S_229 |  HATLASJ133440$+$353140 | HerBS134 | Ba18 | 13:34:40 |  $+$35:31:40.17 | C | – | $69.9\pm 5.9$ | $97.3\pm 6.2$ | $87.9\pm 7.3$ | Ba18
S_230 |  HATLASJ133534$+$341837 | HerBS76 | Ba18 | 13:35:34 |  $+$34:18:36.97 | C | – | $108.5\pm 5.9$ | $124.3\pm 6.0$ | $98.5\pm 7.0$ | Ba18
S_231 |  HATLASJ133623$+$343806 | – | – | 13:36:23 |  $+$34:38:05.88 | C | – | $78.8\pm 7.4$ | $83.2\pm 8.3$ | $79.1\pm 8.6$ | Ma18
S_232 |  HATLASJ133715$+$352058 | – | – | 13:37:15 |  $+$35:20:58.04 | C | – | $69.9\pm 7.5$ | $88.1\pm 8.3$ | $69.4\pm 8.8$ | Ma18
S_233 |  HATLASJ133905$+$340820 | – | – | 13:39:05 |  $+$34:08:20.20 | C | – | $59.3\pm 7.3$ | $82.7\pm 8.2$ | $70.1\pm 8.7$ | Va16
S_234 |  HATLASJ134124$+$354007 | – | – | 13:41:24 |  $+$35:40:06.58 | C | – | $62.9\pm 7.3$ | $79.9\pm 8.2$ | $82.2\pm 8.5$ | Va16
S_235 |  HATLASJ134139$+$322837 | – | – | 13:41:39 |  $+$32:28:37.34 | C | – | $39.8\pm 7.4$ | $42.7\pm 8.1$ | $80.1\pm 8.8$ | Va16
S_236 |  HATLASJ134403$+$242627 | HerBS196 | Ba18 | 13:44:03 |  $+$24:26:26.95 | C | – | $86.9\pm 5.7$ | $92.3\pm 6.3$ | $81.0\pm 7.1$ | Ba18
S_237 |  HATLASJ134442$+$240346 | HerBS133 | Ba18 | 13:44:42 |  $+$24:03:46.12 | C | – | $85.4\pm 5.5$ | $98.5\pm 6.1$ | $88.1\pm 7.3$ | Ba18
S_238 |  HATLASJ134654$+$295659 | – | – | 13:46:54 |  $+$29:56:59.06 | C | – | $85.0\pm 7.6$ | $82.0\pm 8.3$ | $77.8\pm 8.6$ | Va16
S_239 |  HATLASJ140422$-$001218 | HerBS206 | Ba18 | 14:04:22 |  $-$00:12:18.00 | C | – | $79.3\pm 7.4$ | $102.6\pm 8.4$ | $80.2\pm 8.8$ | Ba18
S_240 |  HATLASJ141118$-$010655 | HerBS201 | Ba18 | 14:11:18 |  $-$01:06:55.00 | C | D | $52.2\pm 7.2$ | $78.6\pm 8.2$ | $80.5\pm 8.7$ | Ba18
S_241 |  HATLASJ141810.0$-$003747 | HerBS143 | Ba18 | 14:18:10 |  $-$00:37:47.00 | C | – | $77.7\pm 6.5$ | $97.3\pm 7.4$ | $87.1\pm 7.9$ | Ba18
S_242 |  HATLASJ141955.5$-$003449 | – | – | 14:19:56 |  $-$00:34:49.00 | C | – | $76.4\pm 7.5$ | $94.9\pm 8.0$ | $80.2\pm 8.9$ | Va16
S_243 |  HERMESJ142549$+$345024 | – | – | 14:25:49 |  $+$34:50:23.57 | C | – | $48.0\pm 7.4$ | $64.4\pm 8.3$ | $52.9\pm 9.0$ | Ma18
S_244 |  HERMESJ142558$+$332549 | HBootes09 |  | 14:25:58 |  $+$33:25:48.68 | C | – | $69.0$ | $81.0$ | $60.0$ | Ca14
S_245 |  HATLASJ142707$+$002258 | HerBS130 | Ba18 | 14:27:07 |  $+$00:22:57.60 | C | – | $119.4\pm 7.3$ | $118.7\pm 8.1$ | $88.8\pm 8.6$ | Ba18
S_246 |  HATLASJ143403.5$+$000234 | HerBS147 | Ba18 | 14:34:04 |  $+$00:02:34.34 | C | – | $103.3\pm 7.4$ | $103.3\pm 8.1$ | $86.6\pm 8.5$ | Ba18
S_247 |  HERMESJ143544$+$344743 | HBootes12 |  | 14:35:44 |  $+$34:47:43.37 | C | – | $11.0$ | $52.0$ | $21.0$ | Ca14
S_248 |  HERMESJ144030$+$333843 | HBootes07 |  | 14:40:30 |  $+$33:38:42.68 | C | – | $86.0$ | $88.0$ | $72.0$ | Ca14
S_249 |  HATLASJ144556.1$-$004853 | G15v2.481 |  | 14:45:56 |  $-$00:48:53.00 | C | Unc. | $126.7\pm 7.3$ | $132.6\pm 8.4$ | $111.8\pm 8.7$ | Ne17
|  | HerBS46 | Ba18 |  |  |  |  |  |  |  |
S_250 |  HATLASJ144608.6$+$021927 | HerBS38 | Ba18 | 14:46:09 |  $+$02:19:27.01 | C | – | $73.4\pm 7.1$ | $111.7\pm 8.1$ | $122.1\pm 8.7$ | Ne17
S_251 |  HATLASJ145135.2$-$011418 | HerBS126 | Ba18 | 14:51:35 |  $-$01:14:18.00 | C | – | $81.9\pm 7.2$ | $95.9\pm 8.2$ | $89.8\pm 8.8$ | Ba18
S_252 |  HATLASJ145337.2$+$000407 | HerBS137 | Ba18 | 14:53:37 |  $+$00:04:07.94 | C | – | $86.0\pm 7.2$ | $103.6\pm 8.0$ | $87.7\pm 8.6$ | Ba18
S_253 |  HATLASJ145754$+$000017 | HerBS195 | Ba18 | 14:57:54 |  $+$00:00:17.07 | C | – | $70.3\pm 7.3$ | $92.7\pm 8.1$ | $81.0\pm 8.8$ | Ba18
S_254 |  HERMESJ161332$+$544358 | HELAISN01 |  | 16:13:32 |  $+$54:43:57.76 | C | – | $123.0$ | $129.0$ | $88.0$ | Ca14
S_255 |  HERMESJ170508$+$594056 | HFLS07 | Ca14 | 17:05:08 |  $+$59:40:56.32 | C | – | $115.0$ | $92.0$ | $69.0$ | Ca14
S_256 |  HERMESJ170608$+$590921 | HFLS03 | Ca14 | 17:06:08 |  $+$59:09:21.28 | C | – | $98.0$ | $105.0$ | $81.0$ | Ca14
S_257 |  HERMESJ170818$+$582845 | HFLS05 | Ca14 | 17:08:18 |  $+$58:28:45.41 | C | – | $40.0$ | $75.0$ | $74.0$ | Ca14
S_258 |  HERMESJ172222$+$582611 | HFLS10 | Ca14 | 17:22:22 |  $+$58:26:10.82 | C | – | $52.0$ | $50.0$ | $32.0$ | Ca14
S_259 |  HERMESJ172612$+$583742 | HFLS01 | Ca14 | 17:26:12 |  $+$58:37:42.24 | C | – | $107.0$ | $123.0$ | $98.0$ | Ca14
S_260 |  HATLASJ222629.4$-$321111 | HerBS144 | Ba18 | 22:26:29 |  $-$32:11:12.00 | C | – | $98.9\pm 8.4$ | $116.5\pm 8.2$ | $87.0\pm 11.5$ | Ba18
S_261 |  HATLASJ224027.7$-$343134 | HerBS97 | Ba18 | 22:40:28 |  $-$34:31:35.00 | C | – | $96.1\pm 6.0$ | $98.5\pm 6.3$ | $94.4\pm 7.7$ | Ba18
S_262 |  HATLASJ224207.2$-$324159 | HerBS67 | Ba18 | 22:42:07 |  $-$32:41:59.00 | C | Unc. | $73.0\pm 5.5$ | $88.1\pm 6.2$ | $100.8\pm 7.7$ | Ne17
S_263 |  HATLASJ224400.8$-$340030 | HerBS84 | Ba18 | 22:44:01 |  $-$34:00:31.00 | C | – | $105.1\pm 5.9$ | $123.0\pm 6.4$ | $97.0\pm 7.6$ | Ba18
S_264 |  HATLASJ225324.2$-$323504 | HerBS103 | Ba18 | 22:53:24 |  $-$32:35:04.00 | C | – | $126.1\pm 5.3$ | $131.2\pm 5.7$ | $93.5\pm 7.0$ | Ba18
Table 22: continued No. | IAU Name | Alt. Name | Ref. | RA | Dec | Vis. Class. | Multiw. Class. | $S_{250}$ | $S_{350}$ | $S_{500}$ | Ref.
---|---|---|---|---|---|---|---|---|---|---|---
|  |  |  | [h m s] | [d m s] |  |  | [mJy] | [mJy] | [mJy] |
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12)