# (SHERRY) JCMT-SCUBA2 High rEdshift bRight quasaR surveY - II: the
environment of $z\sim 6$ quasars in sub-millimeter band

Qiong Li Department of Astronomy, School of Physics, Peking University,
Beijing 100871, P. R. China  Kavli Institute for Astronomy and Astrophysics,
Peking University, Beijing, 100871, P. R. China  Jodrell Bank Centre for
Astrophysics, University of Manchester, Oxford Road, Manchester M13 9PL, UK
Ran Wang Department of Astronomy, School of Physics, Peking University,
Beijing 100871, P. R. China  Kavli Institute for Astronomy and Astrophysics,
Peking University, Beijing, 100871, P. R. China  Xiaohui Fan University of
Arizona (Steward Observatory), United States  Xue-Bing Wu Department of
Astronomy, School of Physics, Peking University, Beijing 100871, P. R. China
Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing,
100871, P. R. China  Linhua Jiang Kavli Institute for Astronomy and
Astrophysics, Peking University, Beijing, 100871, P. R. China  Eduardo Bañados
Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117, Heidelberg,
Germany  Bram Venemans Max-Planck-Institut für Astronomie, Königstuhl 17,
D-69117, Heidelberg, Germany  Yali Shao Department of Astronomy, School of
Physics, Peking University, Beijing 100871, P. R. China  Kavli Institute for
Astronomy and Astrophysics, Peking University, Beijing, 100871, P. R. China
Jianan Li Department of Astronomy, School of Physics, Peking University,
Beijing 100871, P. R. China  Kavli Institute for Astronomy and Astrophysics,
Peking University, Beijing, 100871, P. R. China  Jeff Wagg  Square Kilometre
Array Observatory, Lower Withington, Macclesfield, Cheshire SK11 9FT, UK
Roberto Decarli INAF – Osservatorio di Astrofisica e Scienza dello Spazio di
Bologna, via Gobetti 93/3, I-40129, Bologna, Italy.  Chiara Mazzucchelli
European Southern Observatory, Alonso de Cordova 3107, Vitacura, Region
Metropolitana, Chile  Alain Omont Sorbonne Université, UPMC Université Paris 6
and CNRS, UMR 7095, Institut d’Astrophysique de Paris, France  Frank Bertoldi
Universität Bonn (Argelander-Institut für Astronomie), Germany  Sean Johnson
Department of Astronomy, University of Michigan, 311 West Hall, 1085 S.
University Ave, Ann Arbor, MI, 48109-1107, U.S.A.  Christopher J. Conselice
Jodrell Bank Centre for Astrophysics, University of Manchester, Oxford Road,
Manchester M13 9PL, UK

(Received XXX; Revised XXX; Accepted XXX)

###### Abstract

The formation of the first supermassive black holes is expected to have
occurred in some most pronounced matter and galaxy overdensities in the early
universe. We have conducted a sub-mm wavelength continuum survey of 54 $z\sim
6$ quasars using the Submillimeter Common-User Bolometre Array-2 (SCUBA2) on
the James Clerk Maxwell Telescope (JCMT) to study the environments around
$z\sim 6$ quasars. We identified 170 submillimeter galaxies (SMGs) with above
3.5$\sigma$ detections at 450 or 850 $\mu$m maps. Their FIR luminosities are
2.2 - 6.4 $\times$ 10${}^{12}L_{\odot}$, and star formation rates are $\sim$
400 - 1200 M⊙ yr-1. We also calculated the SMGs differential and cumulative
number counts in a combined area of $\sim$ 620 arcmin2. To a $4\sigma$
detection (at $\sim$ 5.5 mJy), SMGs overdensity is $0.68^{+0.21}_{-0.19}$($\pm
0.19$), exceeding the blank field source counts by a factor of 1.68. We find
that 13/54 quasars show overdensities (at $\sim$ 5.5 mJy) of
$\delta_{SMG}\sim$ 1.5 - 5.4. The combined area of these 13 quasars exceeds
the blank field counts with the overdensity to 5.5 mJy of
$\delta_{\rm{SMG}}$$\sim$ $2.46^{+0.64}_{-0.55}$($\pm 0.25$) in the regions of
$\sim$ 150 arcmin2. However, the excess is insignificant on the bright end
(e.g., 7.5 mJy). We also compare results with previous environmental studies
of Lyman alpha emitters (LAEs) and Lyman-Break Galaxies (LBGs) on a similar
scale. Our survey presents the first systematic study of the environment of
quasars at $z\sim 6$. The newly discovered SMGs provide essential candidates
for follow-up spectroscopic observations to test whether they reside in the
same large-scale structures as the quasars and search for protoclusters at an
early epoch.

Quasars (1319), Submillimeter astronomy (1647), Active galaxies (17)

††journal: ApJ

##  1 Introduction

More than 200 quasars at $z>$ 5.6 were discovered in optical and near-infrared
surveys, such as SDSS (e.g. Jiang et al., 2008; Fan et al., 2006), CFHQS (e.g.
Willott et al., 2007, 2010), UKIDSS (e.g. Venemans et al., 2007; Mortlock et
al., 2011), VIKING (e.g. Venemans et al., 2013, 2015), VST-ATLAS (Carnall et
al., 2015), DES (Reed et al., 2015; Yang et al., 2019), HSC (Matsuoka et al.,
2016), Pan-STARRS1 (e.g. PS1; Bañados et al., 2014, 2016; Wang et al., 2019),
etc (e.g. Yang et al. 2021). Galaxy formation simulations and cosmological
models predict that high redshift quasars reside in the most massive dark
matter halos and grow quickly in the galaxy overdensity environments formed by
the hierarchical merging of galaxies (e.g. Romano-Díaz et al., 2011; Costa et
al., 2014). Discovering the overdensities of galaxies associated with $z\sim
6$ quasars will trace mass assembly and probe the evolution of protoclusters
and large-scale structures in the early universe. Hence, it is a chance to
investigate the environment where QSOs hosting SMBHs reside and to search for
galaxy protoclusters close to the end of cosmic reionization.

Over the last twenty years, sub-mm surveys around AGNs and galaxies have
advanced our understanding of the galaxy environment at the cosmic time. The
first one was uncovered by SCUBA (Submillimeter Common-User Bolometre Array)
surveys on JCMT (the James Clerk Maxwell Telescope, Smail et al. 1997).
Subsequently, a series of papers have shown evidence for over-densities of
submillimeter galaxies (SMGs) at $z=2\sim 3$ in the vicinities of luminous
radio galaxies (e.g., De Breuck et al. 2004; Greve et al. 2007) and dust
absorbed QSOs (Stevens et al., 2004; Priddey et al., 2007). The clustering of
SMGs at $z\sim 2$ around luminous QSOs or galaxies indicates evolutionary
scenarios in which powerful starbursts and QSOs occur in the same systems
(Hickox et al., 2012). And Priddey et al. (2008) also reported deep sub-mm
images with a large field of view for three $z>5$ quasars in SCUBA
observations. However, the observational evidence of large-scale structure
close to $z\sim 6$ quasars is elusive, limited by a relatively small quasar
sample size and strong selection biases of quasars.

There are many different approaches for tracing overdense regions around
quasars or galaxies at $z\sim 6$, such as Lyman-Break Galaxies (LBGs) selected
via broad-band optical/NIR colors (Stiavelli et al., 2005; Morselli et al.,
2014) or Lyman alpha emitters (LAEs) selected via narrow/broadband
observations (e.g., Mazzucchelli et al., 2017; Ota et al., 2018). Despite the
huge investment of optical or near-infrared (NIR) telescope time, the galaxy
environments surrounding $z\sim 6$ quasars remain unconstrained. Overdensities
of galaxies were discovered with deep optical imaging around several quasars
at $4<z<6$ (e.g., the $z=6.28$ quasar SDSS J1030+0524 in Stiavelli et al.
2005, and the $z=5.81$ radio-loud quasar SDSS J0836+0054 in Zheng et al. 2006
and Ajiki et al. 2006). However, some works failed to find any significant
galaxy overdensity (e.g., LAEs surrounding PSO J215-16 at $z=5.73$ in
Mazzucchelli et al. 2017, and CFHQS J2329-0301 in Goto et al. 2017). Integral
field spectroscopic investigations at radio/sub-mm wavelengths in quasar
fields both with ALMA (Decarli et al., 2017; Willott et al., 2017; Venemans et
al., 2019) and NOEMA (Wang et al., 2011; Omont et al., 2013) revealed the
presence of close ($<$ 50 kpc, $<$ 1cMpc) companion galaxies in the immediate
proximity of the first massive black holes. It only traces the small-scale
clustering at close separation from the central quasars.

To test whether the companion galaxies identified around some $z\sim 6$
quasars are a small-scale phenomenon or the expression of the long-sought
large-scale overdensities postulated by the models, in 2016-2018 we mapped the
fields around 54 quasars at $z\sim 6$ over a much larger field-of-view
($\sim$15′ in diameter) using SCUBA-2 (Submillimeter Common-User Bolometre
Array-2) on JCMT, named as ‘JCMT-SCUBA2 High rEdshift bRight quasaR surveY’
(‘SHERRY’ survey). SCUBA-2 has a field of view of 64 sq-arcminutes (only 4.3
sq-arcmins for SCUBA) - a factor of 16 times improvement over SCUBA (Chapin et
al., 2013). And it has the fastest mapping speed at 450 $\mu$m and 850 $\mu$m,
which makes searching for SMGs more efficient (Chapin et al., 2013). The
SHERRY survey is the first to build a large, statistical sample of $z\sim 6$
quasars for sub-mm observation, including $\sim 20$% of the $z\sim 6$ quasars
discovered to date.

In the first paper of this survey (SHERRY-I, Li et al. 2020a), we reported
that about 30% (16/54) quasars were detected with a typical 850$\mu$m RMS
sensitivity of 1.2 $\rm mJy\,beam^{-1}$ ($>3.5\sigma$). The broadband SED for
$z\sim 6$ quasars is similar to that at $z\sim 2$, which indicates there is
probably no evolution of quasars’ properties with redshift. The optical/near-
infrared (NIR) spectra of these objects show 11% (6/54) of the sources have
weak ultraviolet (UV) emission line features. The SHERRY survey also indicates
that quasars with sub-mm detections tend to have weaker emission lines than
quasars with non-detections. The weak-line quasar at $z\sim 6$ may be a young
AGN-galaxy system (Li et al., 2020a), in which the broad line region is
starting to develop slowly and have some unusual properties.

In this paper, we present JCMT/SCUBA-2 observations of the environment around
the quasars at $5.6<z<7.1$ and search for galaxy protoclusters close to the
end of cosmic reionization. We describe the SCUBA2 observations and data
reduction in Section 2. In Section 3, we introduce our method to extract SMGs
candidates and calculate the number counts. We present the number counts
results and the discussions in Section 4. Finally, we give a summary of the
main results in Section 5. We adopt a $\Lambda$-model cosmology with
$H_{0}=71$ km s-1 Mpc-1, $\Omega_{M}=0.27$ and $\Omega_{\Lambda}=0.73$
(Spergel et al., 2007) throughout this paper.

Figure 1:  The distrubution of the map depth at 850 and 450 $\mu$m.

##  2 SCUBA2 observations and data reduction

We observed 54 quasars at $5.7<z<7.1$, which have rest-frame 1450 Å absolute
magnitudes of $M_{\rm 1450}\leq-25.4$. The observations were carried out with
the SCUBA2 camera on the JCMT in Hawaii from August 2015 to January 2018
(Program ID: M15BI055, M16AP013, M17AP062, M17BP034). We used ‘the constant
velocity Daisy scan’ observation mode (‘CV DAISY’ mode) with the field of view
of 15′ in diameter. This mode is for small and compact sources of order
3-arcmin or less. The most uniform and best rms region is the central one with
a diameter of about 4′ , corresponding to comoving 9.8 h-1Mpc comoving. This
covers typical protocluster scales at $z\sim 6$ (e.g., Overzier et al. 2009).

SCUBA2 observes two bands, 450 $\mu$m and 850 $\mu$m simultaneously. The main
beam sizes of SCUBA-2 are 7.9″ at 450 $\mu$m and 14.9″ at 850 $\mu$m; with the
spatial resolution of 4″ / pixel and 2″ / pixel, respectively. The
observations were carried out in grade 2 / grade 3 weather conditions with
precipitable water vapor (PWV) of 0.83 - 2.58 mm at zenith (atmospheric
optical depth $0.05\rm<\rm\tau_{225GHz}\rm<0.12$). We observed each target in
four to six $\sim$ 30-minute scans with a total on-source time of 2$-$3 hours
to reach the sensitivity of 1.2 mJy at 850$\mu$m . We present the details of
the observations in Li et al. (2020a). The calibrated sources were observed
before and after the target sources and selected from the James Clerk Maxwell
Telescope (JCMT) calibrator list (Dempsey et al., 2013). Calibration sources
included Mars, Uranus, Neptune, etc.

We reduced the data using the STARLINK SCUBA-2 science pipeline with the
configuration file of ‘dimmconfig blank field.lis’, which is the recipe for
processing maps containing the faint compact sources (Chapin et al., 2013). We
processed each complete observation separately to produce an image and
calibrated it with the flux conversion factors (FCFs) to mJy/beam. We adopted
the default FCFs value of 537$\pm$24 Jy pW-1 beam-1 for 850 $\mu$m map and
491$\pm$67 Jy pW-1 beam-1 for 450 $\mu$m map (Dempsey et al., 2013). We
combined all images for a given source into a single image using inverse-
variance weighting. Using this recipe, we further processed the output map
with a beam-match filtered of a 15″ FWHM Gaussian at 850 $\mu$m band. The S/N
is taken to enhance point sources, which is suitable for searching for SMGs at
$z\sim 6$. The final 850- and 450-$\mu$m maps have typical noise levels of 1.2
and 16.5 $\rm mJy\,beam^{-1}$, shown in Figure 1.

Figure 2: Example SCUBA2 exposure time map. The contours denote the 20, 40,
60% exposure time levels compared to the maximum level on the map. The blue
circle region has a diameter of 4′ and marks the region with uniform and low
RMS for SMG overdensity searches. Figure 3: JCMT-SCUBA2 850$\mu$m images of
the surrounding regions around 54 $z\sim 6$ quasar with a beam size of FWHM =
15″. The selected region is within 2.23 arcmins from the quasar optical
position (which covers typical protocluster scales at $z\sim 6$) and has one
sigma uncertainty of $<$ 1.5 mJy beam-1 for each pixel. The contour levels are
+3, +4, +5, +6, +7$\times$1.5 mJy beam-1 for each map. The star indicates the
quasar optical/NIR position. The star with the blue edge is the sub-mm
detected quasars. The blue circles indicate the selected SMGs (with S/N$>$3.5
at 850um or 450um, see Table 2). The sources marked with ‘#’ are the SMGs used
in the overdensity analysis with deboosted fluxes $>$ 5.5 mJy.  Figure 4:
-Continued

##  3 Source extraction and Number counts

###  3.1 Source extraction

The SHERRY survey fields are centered on the targeted $z\sim 6$ quasars. The
expected protocluster size is about $\sim$ 20 cMpc along the side, and the
core of the protocluster is 2 - 3 cMpc (Overzier et al., 2009; Chiang et al.,
2017). For each map, we use the (square root of the) exposure time as a proxy
for noise, which is as a function of radius (Figure 2). Note the actual noise
map is produced from the pipeline, including other noise, e.g., the instrument
and atmospheric noise. Considering that the noise increases rapidly at a large
radius of the Daisy maps, we searched for overdensity within the central
$\sim$2 arcmins around the quasar. This region corresponds to a scale of
$\sim$10 cMpc in diameter, which can trace a typical protocluster (Chiang et
al., 2013). Furthermore, we mask the region where the RMS noise level is $>$
1.5 mJy beam-1 based on the error map to ensure the best/uniform sensitivity
in the SCUBA-2 images. The error difference between the center and the edge is
less than $\sim 15\%$. The source extraction is processed in this effective
region, shown in Figure 3.

To extract the sources in the maps, we adopted the ‘top-down’ algorithm to
find the source with the highest SNR in the two bands maps for each quasar
field (e.g., Chen et al. 2013; Geach et al. 2017). SMGs at high redshifts are
unresolved in SCUBA-2 observations; thus, the flux density of the source is
the peak value of the pixels in the beam. We first identified the pixel’s
position with the highest SNR for each source. Then we subtracted a scaled
point spread function (PSF) from the image at the source position. We
generated the Gaussian PSF model with an FWHM of 14.9 arcsec at 850 $\mu$m map
and 7.9 arcsec at 450 $\mu$m . During each iteration, we recorded the
coordinates, flux densities, noise values, and SNRs of each $>3.0\sigma$
detection of candidate sources. To create a unique source list, we removed
multiple detections if the secondary peaks were within one beam area of a
higher SNR one. We iterated this process until there were no more sources with
SNR of greater significance than the threshold in the image.

After identifying the $>$ 3.0$\sigma$ candidate sources in the two band maps,
we cross-checked the sources between 850$\mu$m and 450$\mu$m maps to find the
counterpart in the radius of 15″ (the beam size at 850$\mu$m map). The final
catalog of submm source candidates is generated as those satisfying $>$
3.5$\sigma$ at least in one band. The flux density of its counterpart on
another band is also listed in the catalog, if it has. The 850$\mu$m images of
each of the 54 quasar fields are shown in Figure 3. The final SMGs selected as
described above are marked as blue circles, and listed in Table 2 of Appendix
A. We also carried out MCMC deboosted process for each individual source’s
flux for repeating 50000 times, and calculated the deboosted flux and its
error.

Figure 5: The S/N histograms of the signal maps in the field of quasar SDSS
J0100+2802 ($z=6.3258\pm 0.0010$) in the 850$\mu$m and 450$\mu$m bands. The
dashed and solid lines indicate the 3.5$\sigma$ and 4$\sigma$. The red line
represents the Gaussian fitting of the noise statistics. Figure 6: Example
completeness and flux boosting estimates based on Monte Carlo source
insertion. Left: Completeness as a function of input flux (Sin). The solid
curve represents the best-fit function of _f(S in) = [1+erf((Sin-A)/B)]/2_
with best fitting parameters give in the text. Right: The ratio between input
flux density and output flux density as a function of input flux. Error bars
show 1$\sigma$ of 5000 trials. Solid curve represents the best-fit function of
_f(S in) =1+Aexp(-BS${}_{in}^{C}$)_. (Hatsukade et al., 2016).

###  3.2 Number counts

In this section, we determine the pure galaxy number counts in the quasar
fields. To do so, we first need to estimate the number of spurious sources
contaminating the counts and estimate completeness levels, particularly at low
SNR. These completeness and flux deboosting calculations are all processed for
each field individually. In this section, we use SDSS J0100+2802 as an example
to show how it works. Note the number counts result in this paper is only
based on 850 $\mu$m maps due to its better sensitivity.

####  3.2.1 Spurious source

We examined the negative noise statistics to calculate the contamination rate
of false detections. For example, we plot the S/N histograms of the pixels in
the effective area of the signal maps at quasar nearby field for SDSS
J0100+2802 ($z=6.3258\pm 0.0010$) in 850$\mu$m and 450$\mu$m bands, in Figure
5. The red line represents the Gaussian fitting of the noise statistics. The
excess above this line on the positive side represents true detections
assuming that the noise is symmetric. On the other hand, the negative tail is
from the spurious sources due to the matched-filter PSF (Chapin et al., 2013).
We need to estimate the distribution of negative to obtain the pure number
counts.

We performed this check on each field individually. We first constructed an
inverted flux map and then applied the source extraction procedure described
in Section 3.1 to them. Nine detections at $\sigma>4$ were found in the
inverted maps at 850$\mu$m band. We estimated the false detection rate above
$4\sigma$ significance to be 11.4% (9/79). We also estimated the false
detection rate at $3<\sigma<4$ to be 57.6% (57/99). Considering the effects of
spurious sources, we calculate the number counts with the flux bin beginning
from 4$\sigma$. Then the impact of the spurious source will significantly
diminish, and the conclusions below are not affected.

####  3.2.2 Completeness

To describe how we make some corrections to calculate the number counts, we
still use the field of quasar SDSS J0100+2802 ($z=6.3258\pm 0.0010$) as an
example in the following. The completeness is the rate at which a source is
expected to be detected in the image (Hatsukade et al., 2016). We used the
Monte Carlo simulation approach to estimate completeness. The completeness
test is only in the central best/uniform-sensitivity regions. We injected
artificial sources of $0-10$ mJy/beam at random positions in the maps $>$ 8.0″
away from $\geq$ 3$\sigma$ peaks to avoid the contribution from nearby
sources. The flux bin step is 0.5 mJy for 850 $\mu$m map. Then we ran the
source extraction on the maps to see if we could recover the injected sources.
When the output source is above 3$\sigma$, the source is considered to be
recovered. This procedure is repeated 5000 times for each flux bin. We fit the
completeness as a function of _f(S in)=[1 + erf((Sin \- A)/B)]/ 2_ (Hatsukade
et al., 2016), as shown in Figure 6. Here Sin is the input flux density. The
best-fitted parameters are $A=4.67\pm 0.01$, $B=2.05\pm 0.02$. Based on this
Monte-Carlo experiment, we estimate a 50% completeness level for 4.7 mJy point
sources and 80% for 5.9 mJy point sources in 850$\mu$m map.

####  3.2.3 flux boosting

With the Monte Carlo simulations, we also considered the effect that flux
densities of low S/N sources are boosted (Murdoch et al., 1973; Hatsukade et
al., 2016). More specifically, we calculated the ratio between the flux of the
recovered sources and those of the injected artificial sources. We then
estimate the mean ratio in 0.5 mJy flux bins. To illustrate this process, we
plot the mean flux boosting value for the field of J0100 in Figure 6 (right).
The flux boosting is more pronounced for low S/N sources. We fit the ratio
between input flux density and output flux density as a function of _f(S in)
=1+Aexp(-BS${}_{in}^{C}$)_(Hatsukade et al., 2016). The best fitted parameters
are $A=1.74\pm 0.27$, $B=0.11\pm 0.04$ and $C=1.95\pm 0.22$. At S/N = 4 (input
flux = 4.8 mJy), the estimated mean flux boosting factor is 1.19 at 850 $\mu$m
map. This is consistent with the results of Monte Carlo simulations in
previous SCUBA studies (Eales et al., 2000; Scott et al., 2002; Cowie et al.,
2002; Casey et al., 2013; Chen et al., 2013), such as the boosting factor of
1.25 at 850$\mu$m map in Cowie et al. (2002). Potential contamination for the
SMG number counts is the gravitational lensing effects of foreground objects
(e.g., Chen et al. 2011). If some of the detected submillimeter sources are
lensed background sources, they may increase the uncertainties of the source
positions and also boost the measured fluxes. (Knudsen et al., 2008)

Figure 7:  The combined differential and cumulative number counts at 850$\mu$m
from all of our source fields. The filled black points and black lines
indicate our data and Schechter fitting, respectively. The gray line shows the
blank-field number counts of SMGs in the S2CLS field in Geach et al. (2017).
For clarity, we only show the error bars of S2CLS and our data from Poissonian
statistics (Gehrels, 1986). Points in this work have been corrected for flux
boosting and incompleteness (see figure 6). Table 1: The combined differential
and cumulative number counts at 850$\mu$m

S860 | dN | dNcorr | dN/dS | N($>$S)
---|---|---|---|---
(mJy) |  |  | (mJy-1deg-2) | (deg-2)
5.5 | 29 | 42.2 ${}_{-6.5}^{+7.6}(\pm 7.4)$ | 243.5 ${}_{-37.4}^{+43.6}(\pm 40.1)$ | 461.4 ${}_{-51.5}^{+57.6}(\pm 53.4)$
6.5 | 16 | 18.4 ${}_{-4.3}^{+5.4}(\pm 4.5)$ | 106.1 ${}_{-24.6}^{+31.0}(\pm 24.9)$ | 217.9 ${}_{-35.4}^{+41.6}(\pm 33.9)$
7.5 | 9 | 9.3 ${}_{-3.0}^{+4.2}(\pm 2.6)$ | 53.9 ${}_{-17.4}^{+24.1}(\pm 15.4)$ | 111.8 ${}_{-25.2}^{+31.7}(\pm 22.1)$
8.5 | 2 | 2.0 ${}_{-1.3}^{+2.7}(\pm 1.4)$ | 11.7 ${}_{-7.7}^{+15.4}(\pm 8.3)$ | 57.9 ${}_{-18.1}^{+24.7}(\pm 16.4)$
9.5 | 4 | 4.0 ${}_{-1.9}^{+3.2}(\pm 1.9)$ | 23.1 ${}_{-11.2}^{+18.4}(\pm 11.2)$ | 46.2 ${}_{-16.1}^{+22.9}(\pm 14.3)$
10.5 | 3 | 3.0 ${}_{-1.7}^{+2.9}(\pm 1.7)$ | 17.3 ${}_{-9.6}^{+17.0}(\pm 9.6)$ | 23.1 ${}_{-11.2}^{+18.4}(\pm 11.5)$
11.5 | 1 | 1.0 ${}_{-0.9}^{+2.3}(\pm 1.0)$ | 5.8 ${}_{-5.0}^{+13.4}(\pm 5.8)$ | 5.8 ${}_{-5.0}^{+13.4}(\pm 5.8)$

Note. —

S is the bin central flux density, and the bin width is one mJy. The first set
of uncertainties is Poissonian errors. And the second reflects a bootstrap
analysis error that is the standard deviation of counts in each bin after 1000
realizations of the random sampling. These uncertainties are of comparable
magnitude to the Poisson errors. The combined area includes all 54 quasar
nearby fields as a statistical field with the size of $\sim$ 620 arcmin2,
corresponding to $\sim$ 3700 cMpc2 ($\sim$ 76 pMpc2) at $z\sim 6$.

##  4 Results and Discussion

###  4.1 Differential and cumulative number counts

To obtain an unbiased estimate of the number counts for each SMG candidate, we
statistically correct the observed flux density using the Monte Carlo
simulation for each field, see Figure 6. Then, the deboosted flux density is
amended for completeness, as described in Section 3.2.2. Note we also removed
the quasar itself in the analysis of number counts.

There are two number counts to describe the source abundance: the cumulative
number counts and the differential number counts. To study the general
environment of $z\sim 6$ quasars, we built a combined area to calculate the
differential number counts, which have independent errors for each count
measurement, making it straightforward to do fitting. The combined area
includes all 54 quasar nearby fields and totals $\sim$ 620 arcmin2,
corresponding to $\sim$ 3700 cMpc2 ($\sim$ 76 pMpc2) at $z\sim 6$. It
represents the overall environmental property of quasar fields at $z\sim 6$.
Another number count is the cumulative number count. It applies to the small
sample size with a visual underlying counts shape. This method can be used in
the analysis of individual quasar nearby fields.

The differential number counts of the combined area are calculated by dividing
each $>$ 3.5$\sigma$ detection by the total combined area and adding up all
measurements lying with each flux bin, then dividing by the flux width.
Following previous studies, we fit the differential number counts with a
Schechter function of the form (Casey et al., 2013; Geach et al., 2017):

$\begin{split}&\frac{dN}{dS}=\left(\frac{N_{0}}{S_{0}}\right)\left(\frac{S}{S_{0}}\right)^{\alpha}{\rm
exp}\left(-\frac{S}{S_{0}}\right)\end{split}$ (1)

We find the best fit parameters are $N_{0}\sim 3000\rm deg^{-2}$, $S_{0}\sim
1.2$ mJy and $\alpha\sim$ 1.5. We show the corrected differential and
cumulative number counts for the effective area of the 54 quasars, together
with the fit results in Figure 7. We list the corrected data points in Table
1. Note that our fitting is restricted to sources brighter than 5.5 mJy. The
first set of uncertainties is Poisson errors (Gehrels, 1986). And the second
reflects the field variance that we used a bootstrapping approach. The
individual field was selected randomly as many times as the size of a given
sample, allowing for replacements, to create a new sample to calculate the
counts. And each source is also corrected deboosting and completeness. This
process was repeated 1000 times, and then we fitted a normal distribution to
these 1000 realizations. The standard deviation of this distribution was the
field variance. These variances are of comparable magnitude to the Poisson
errors.

We then compared our results with the previous blank field survey - SCUBA2
Cosmology Legacy Survey (S2CLS, $\sim$5 deg2) at 850 $\mu$m. To a $4\sigma$
detection ($\sim$ 5.5 mJy), the SMGs overdensity
($\delta_{\rm{SMG}}=\rho_{\rm{SMG}}/<\rho_{\rm{SMG}}>-1$) is
$0.68^{+0.21}_{-0.19}$($\pm 0.19$) in the combined field of 0.17 degree2,
exceeding ($\sim$ 1.68 $\times$) the source counts of blank sky area. And to a
$5\sigma$ detection, the SMG overdensity is a factor of
$0.40^{+0.27}_{-0.23}$($\pm 0.24$). If the galaxy excess is mainly due to
overdensities at a narrow redshift range around $z\sim 6$, the SMG overdensity
near quasar redshifts must be higher.

Figure 8: Cumulative number counts of SMGs, in fields centered on (i) luminous
high-redshift AGN: z $\sim$ 5 optically selected quasars (grey diamonds;
Priddey et al. 2008); z $\sim$ 4 radio galaxies (grey squares; Stevens et al.
2003); (ii) z $\sim$ 2 protoclusters (grey triangles; Zhang et al. 2022; Cooke
et al. 2019); (iii) z $\sim$ 1 clusters (grey circles; Best 2002; Webb et al.
2005) and (iv) $z\sim 6$ optically selected quasars (this paper, black points
and red/blue diamonds). The black line shows the blank-field number counts of
SMGs in the previous survey, i.e., SCUBA2 survey for S2CLS field in Geach et
al. (2017). The blue line is calculated from our survey’s combined areas of
all 54 quasars ($\sim$ 620 arcmin2); the red line is from the combined areas
of 13 overdense fields around the quasars ($\sim$ 150 arcmin2). The black-
filled points indicate the three most overdense fields selected from our
sample at $z\sim 6$. Points in this work have been corrected for flux boosting
and incompleteness.

To investigate which quasars reside in an overdense environment and search for
protoclusters at $z\sim 6$, we also calculated the completeness and boosting
corrected SMG cumulative number counts N($>$S) individually for each quasar
field. We compared the results with the number counts in the blank field and
gave a rough definition of ‘overdensity’. The lower limit of the SMGs
cumulative number counts to 5.5 mJy ($\sim$ 4$\sigma$) is above the value in
the blank field. With this criterion, 13 quasar fields show clear sub-mm
overdensities with the overdensity of $\delta_{SMG}\sim$ 1.5 - 5.4. We label
their overdensity in Figure 3. Here the calculation of the overdensity is
based on the sources with deboosted fluxes brighter than 5.5 mJy. There are 55
sources from the whole survey (marked with ‘#’ in Figure 3). 24 of these lie
in the 13 over-densities fields, with four of the over-densities comprise just
one source above this flux limit.

We also combined the overdense fields around these 13 quasars and compared
them with the blank field and those around other lower redshift galaxies. For
comparison we show the cumulative number counts of SMGs, in fields centered on
(i) luminous high-redshift AGN: z $\sim$ 5 optically selected quasars (Priddey
et al., 2008); z $\sim$ 4 radio galaxies (Stevens et al., 2003); (ii) z $\sim$
2 protoclusters (Zhang et al., 2022); (iii) z $\sim$ 1 clusters (Best, 2002;
Webb et al., 2005) and (iv) $z\sim 6$ optically selected quasars (in this
paper) in Figure 8. The black line shows the blank field number counts of SMGs
from the SCUBA2 survey of the S2CLS field in Geach et al. (2017). The combined
field of these 13 quasars exceeds the blank field counts with the overdensity
to 5.5 mJy of $\delta_{\rm{SMG}}$$\sim$ $2.46^{+0.64}_{-0.55}$($\pm 0.25$) in
the regions of $\sim$ 150 arcmin2. It is consistent with the lower redshift
cluster and the surrounding regions of quasars and radio galaxies. But to the
bright end, the excess is not significant, e.g., to 7.5 mJy, the overdensity
decreases to 1.00${}^{+1.08}_{-0.74}$($\pm 0.73$). Compared with the lower
redshift galaxies/quasar fields or cluster fields, the combined overdense area
shows a lower overdensity. That is because the data from the literature are
case studies that intentionally target overdense regions (including
significant selected bias). Still, our data points represent the average
environmental properties around $z\sim 6$ quasars, and overdensity is diluted.

Therefore, considering the abundant SMGs candidates in the faint-end, we
select the fields where the lower limit of the SMGs cumulative number counts
to 6.5 mJy ($\sim$ 5$\sigma$) is above the value in the blank field. There are
three (3/13) $z\sim 6$ fields that show a significant excess over the blank
field: P007+04 ($z=6.0$), J0100+2801 ($z=6.3$) and P308-21 ($z=6.2$), shown in
Figure 8. They are more likely similar to the lower redshift overdense
fields/clusters with the overdensity of 2.1 - 5.4 at 5.5 mJy. However,
Champagne et al. 2018 analyzed 1.2 mm ALMA dust continuum maps for 35 bright
quasars at $z\sim 6$. They reported there is no evidence of 0.1 - 1mJy
millimeter continuum sources in the environments of P007+04 ($z=6.0$) and
P308-21 ($z=6.2$). The overdensity is -0.07$\pm$0.56, which implies no
detected overdensity of dusty galaxies around these quasars. This conclusion
is based on a small ALMA field of view of about 25″ , corresponding to an
angular diameter distance of $\sim$ 1 cMpc at $z\sim 6$. It could miss the
overdensity on scales larger than one cMpc.

###  4.2 Correlation with LAE and LBG at $z\sim 6$

Some previous works used other tracers, like LAEs and LBGs, to probe the
large-scale structures. But the question of whether the galaxy environment
traced by LAEs or LBGs of $z\sim 6$ quasar is overdense or not is still far
from clear. Morselli et al. (2014) showed that the environment traced by LBGs
around four $z\sim 6$ quasars is overdense in a wide area of $\sim$ 575
arcmin2, $\sim$3100 cMpc2. Conversely, Willott et al. (2005) reported three
SDSS quasars at $z\sim 6$ that have no clear signs for LBG overdensity in an
area of $\sim$ 30 arcmin2 ($\sim$170 cMpc2 at $z\sim 6$).

At $z=2-6$, some observations reported that SMG brightness appears to be
correlated with the high-density region of LAEs and LBGs (e.g. Pope et al.
2006; Tamura et al. 2009; Matsuda et al. 2011; Hodge et al. 2013; Umehata et
al. 2017; Harikane et al. 2019). Here we compare some individual sources that
have previous environment studies traced by LAEs and LBGs on a similar scale.
Becker et al. (2018) reported that J0148+0600 field has a highly significant
deficit of LAEs. It is roughly one-quarter of background density with ten cMpc
(similar size in our survey). But in our millimeter survey, the environment of
J0148+0600 has an overdensity of $\sim$ 2.1 ($\sim$ 3 $\times$ the background
field).

Conversely, Mazzucchelli et al. (2017) reported no evidence for an overdensity
of LAEs in an area of $\sim$ 37 arcmin2 centered on the quasar PSO J215-16. We
also find no evidence of SMG overdensity in the field of PSO J215-16 in our
SHERRY survey. At a similar scale, the different findings may be ascribed to
different tracers. These LAEs or LBGs trace the young, dust-poor star-forming
galaxies. Nevertheless, some observations and cosmological simulations
indicate that galaxy assembly at high redshift around the quasar might be
characterized by galaxies with elevated dust and molecular gas content. (e.g.
De Rosa et al., 2011; Yajima et al., 2015). The SMGs trace massive, metal-
enriched, and highly obscured objects, which may be a more suited tracer for
high redshift overdensities. SMGs, therefore, give us a new perspective on the
studies of galaxy environment at high redshift.

###  4.3 Massive SMGs in proto-clusters

Our SHERRY survey covers 54 $z\sim 6$ quasars (20/54 detected at the sub-mm
band, see Li et al. 2020b). We identified 170 SMGs ($>3.5\sigma$) at 450 and
850 $\mu$m, in an area of $\sim$620 arcmin2. SHERRY represents the first
systematic study to probe the environment of $z\sim 6$ quasars in the sub-mm
bands. For these SMGs lie $z\sim 6$, their FIR luminosities are 2.2 - 6.4
$\times$ 10${}^{12}L_{\odot}$, and their star formation rates are $\sim$ 400 -
1200 $M_{\odot}\,yr^{-1}$ (assuming a modified black body SEDs with a typical
SMG dust temperature of 35 $K$, an emissivity index of $\beta$ = 1.6 and a
Salpeter IMF).

We found that 13/54 fields around $z\sim 6$ quasars exhibit excess above SMG
counts compared to a blank field. However, we caution that the other 41/54
quasars could also reside in the overdense fields, because our survey is not
sensitive to the fainter SMGs with $L<$ 2.0 $\times$ 10${}^{12}L_{\odot}$.
Furthermore, even in an actual dense region of galaxies, the expected number
of massive galaxies will not be very large based on the luminosity function.

On the other hand, our SHERRY survey does not provide an accurate redshift
determination. Therefore, the SMG overdensity may be diluted over the large
cosmological volume. Meyer et al. (2022) presented ALMA observations for three
quasar-SMG fields (P231-20 at $z=6.59$, P308-21 $z=6.24$ and J0305-3150
$z=6.61$) selected from our SCUBA2 survey to search for [Cii] emission. 12 out
of 17 SCUBA2-selected sources are detected with ALMA in the continuum. ALMA
detections have offset from the center of pointing due to the large beam of
SCUBA2 imaging (13″ at 850$\mu$m , e.g., of the order of ALMA field of view,
Figure 1 in Meyer et al. 2022). They also search for the [C ii] emission lines
in six of the continuum-detected sources: four ones in the field of P231-20
($>5\sigma$) and two ones around P308-21 (3-4$\sigma$). In the field of
PJ231-20, they confirmed a foreground cluster at $z\sim 2.4$. But
unfortunately, none of the sources have a photo-$z$ consistent with the
background $z\sim 6$ quasars. In the future, more high-resolution imaging and
spectroscopic observations are required for these JCMT-selected protocluster
candidates. If we confirm that a significant fraction of the SCUBA-detected
galaxies are indeed at the redshift of the quasars (e.g., P007+04, J0100+2802,
etc.), we will have striking evidence that some high-$z$ quasars reside in
highly overdense regions.

##  5 Summary

In this paper, we have presented a SCUBA-2 sub-mm survey ‘SHERRY’ of 54 $z\sim
6$ QSOs to study their environment and to search for galaxy protoclusters at
the early epoch. The large field of view of JCMT enabled us to identify 170
SMGs ($>3.5\sigma$) at 450 and 850 $\mu$m . SMGs are selected within a
distance of $\sim$2 arcmins away from the central quasars and have the RMS
noise level of $\sim$ 1.2 mJy beam-1 in the 850 $\mu$m band. This region
corresponds to 10 cMpc in diameter, which can trace the typical galaxy
protocluster (Chiang et al., 2013). If the SMGs are near the quasar redshifts,
their FIR luminosities are 2.2 - 6.4 $\times$ 10${}^{12}L_{\odot}$ and star
formation rates are $\sim$ 400 - 1200 $M_{\odot}\,yr^{-1}$. The SMGs
discovered in SHERRY provide us with essential candidates for follow-up
spectroscopic observations (e.g., [CII]) to secure redshifts and study the
first massive large-scale structures in the universe.

We also calculated the SMGs differential and cumulative number counts after
correcting for completeness and flux boosting in a combined area of $\sim$ 620
arcmin2, which corresponds to $\sim$ 3700 cMpc2 ($\sim$ 76 pMpc2) at $z\sim
6$. To a $4\sigma$ detection (at $\sim$ 5.5 mJy at 850$\mu$m ), the SMGs
overdensity is $0.68^{+0.21}_{-0.19}$($\pm 0.19$), exceeding ($\sim$ 1.68
$\times$) the source counts of blank sky surveys (S2CLS; Geach et al. 2017).
We found 13/54 quasars show SMG overdensities (at $\sim$ 5.5 mJy) in their
fields, and the others do not. The combined field of these 13 quasars exceeds
the blank field counts with the overdensity to 5.5 mJy of
$\delta_{\rm{SMG}}$$\sim$ $2.46^{+0.64}_{-0.55}$($\pm 0.25$) in the regions of
$\sim$ 150 arcmin2; but to the bright end (e.g., 7.5 mJy), the overdensity is
not significant. Among them, three (3/13) $z\sim 6$ fields show a significant
excess over the blank field, with the overdensity of 2.1 - 5.4 at 5.5 mJy.

We also compared our work and some previous environment studies traced by LAEs
and LBGs on a similar scale. These LAEs or LBGs trace the young, dust-poor
star-forming galaxies, while the SMGs trace massive, metal-enriched, and
highly obscured objects. They may be correlated in the high-density region;
therefore, more follow-up spectroscopic works to search for LAEs with JWST,
HST, VLT, and ALMA. are required for these fields at a large scale.

This work was supported by the National Science Foundation of China (NSFC,
11721303, 11991052), the National Key R&D Program of China (2016YFA0400703),
and the NSFC grants No. 11533001. R.W. acknowledge the support from the
Thousand Youth Talents Program of China, NSFC grants No. 11473004. X.-B. Wu
thanks the support from the National Science Foundation of China (11533001,
11721303). B.V. acknowledges support from the ERC Advanced Grant 740246
(Cosmic Gas). The authors wish to recognize and acknowledge the significant
cultural role and reverence that the summit of Maunakea has always had within
the indigenous Hawaiian community. We are most fortunate to have the
opportunity to conduct observations from this mountain. We are grateful to
Paul Hewett, Richard McMahon, Daniel Mortlock, and Stephen Warren, who
supplied the spectrum of ULAS J0828+2633. We also thank our support scientists
and telescope schedulers: Harriet Parsons, Mark G. Rawlings, Iain Coulson,
Steven Mairs, and Jan Wouterloot, for the JCMT observation and data reduction.

##  Appendix A ‘SHERRY’ - SMG candidates catalog at quasar field at $z\sim 6$

Here we present SMGs and SMG candidates in the quasar fields at $z\sim 6$. The
full catalog includes 170 SMGs selected from 450 and 850 $\mu$m images. Column
(1) contains the SMG IDs. SMGs are detected above 3.5$\sigma$ at least in one
band, marked as ‘ObjectShortName-SMG+index’. Columns (4) and (7) are the SMG
peak flux density in 850$\mu$m and 450$\mu$m bands of SCUBA-2 images; Columns
(5) and (8) are signal-to-noise ratio in each band, respectively. Columns (6)
and (9) are the deboosted flux density for 850$\mu$m and 450$\mu$m detections
calculated from the simulation. Column (10) is the angular distance between
SMGs and their central quasar.

Table 2: The catalog of SMGs and its candidates in the quasar nearby fields at $z\sim 6$ Source | RA | DEC | Sν,850μm | S/N850 | S$\rm{}_{\nu,850\mu m}^{Deboosted}$ | Sν,450μm | S/N450 | S$\rm{}_{\nu,450\mu m}^{Deboosted}$ | offset
---|---|---|---|---|---|---|---|---|---
| (J2000) | (J2000) | (mJy) |  | (mJy) | (mJy) |  | (mJy) | (arcmin)
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10)
J0008-0626-SMG1 | 00h08m24.4s | -06d24m40.5s | 6.92$\pm$1.32 | 5.24 | 6.87$\pm$1.86 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.440
J0008-0626-SMG2 | 00h08m27.1s | -06d28m00.5s | 7.11$\pm$1.50 | 4.75 | 7.08$\pm$2.02 | 45.15$\pm$12.29 | 3.67 | 43.28$\pm$14.26 | 1.962
P002+32-SMG1 | 00h09m23.3s | +32d51m44.9s | 10.73$\pm$1.45 | 7.39 | 10.82$\pm$2.10 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.193
P002+32-SMG2 | 00h09m34.1s | +32d53m12.9s | 5.86$\pm$1.25 | 4.70 | 5.65$\pm$1.69 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.144
P002+32-SMG3 | 00h09m27.1s | +32d53m12.9s | 4.96$\pm$1.34 | 3.70 | 4.48$\pm$1.52 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.555
P002+32-SMG4 | 00h09m33.1s | +32d54m04.9s | 5.14$\pm$1.43 | 3.60 | 4.72$\pm$1.63 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.893
P002+32-SMG5 | 00h09m35.6s | +32d51m16.9s | 4.38$\pm$1.22 | 3.59 | 3.67$\pm$1.25 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.334
P002+32-SMG6 | 00h09m35.6s | +32d53m44.9s | 4.79$\pm$1.34 | 3.58 | 4.23$\pm$1.45 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.805
P002+32-SMG7 | 00h09m27.7s | +32d51m32.9s | 4.30$\pm$1.21 | 3.54 | 3.56$\pm$1.22 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.228
P007+04-SMG1 | 00h28m07.4s | +04d57m41.7s | 10.79$\pm$1.08 | 9.95 | 10.87$\pm$1.78 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.334
P007+04-SMG2 | 00h28m05.2s | +04d56m53.7s | 7.71$\pm$1.12 | 6.86 | 7.77$\pm$1.79 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.630
P007+04-SMG3 | 00h28m07.9s | +04d57m17.7s | 6.84$\pm$1.10 | 6.24 | 6.88$\pm$1.76 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.360
P007+04-SMG4 | 00h28m05.7s | +04d56m29.7s | 4.60$\pm$1.17 | 3.94 | 4.11$\pm$1.33 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.955
P007+04-SMG5 | 00h28m13.5s | +04d58m09.7s | 5.23$\pm$1.43 | 3.65 | 4.97$\pm$1.71 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.888
P007+04-SMG6 | 00h28m08.7s | +04d59m01.7s | 4.18$\pm$1.17 | 3.56 | 3.54$\pm$1.21 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.687
P007+04-SMG7 | 00h28m02.3s | +04d59m01.7s | 4.30$\pm$1.22 | 3.51 | 3.70$\pm$1.28 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.925
J0100+2802-AGN | 01h00m12.6s | +28d02m25.8s | 4.09$\pm$1.13 | 3.63 | 3.34$\pm$1.11 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.076
J0100+2802-SMG1 | 01h00m13.9s | +28d00m25.8s | 9.94$\pm$1.47 | 6.77 | 10.00$\pm$2.08 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.013
J0100+2802-SMG2 | 01h00m09.0s | +28d04m13.8s | 8.00$\pm$1.32 | 6.05 | 8.03$\pm$1.95 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.050
J0100+2802-SMG3 | 01h00m14.2s | +28d02m53.8s | 5.48$\pm$1.12 | 4.88 | 5.18$\pm$1.50 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.556
J0100+2802-SMG4 | 01h00m21.4s | +28d02m21.8s | 5.99$\pm$1.40 | 4.29 | 5.81$\pm$1.79 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.116
J0100+2802-SMG5 | 01h00m17.5s | +28d03m17.8s | 4.11$\pm$1.16 | 3.53 | 3.37$\pm$1.14 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.426
J0148+0600-AGN | 01h48m37.5s | +06d00m20.0s | 5.28$\pm$1.19 | 4.45 | 4.78$\pm$1.45 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.000
J0148+0600-SMG1 | 01h48m37.8s | +05d58m28.0s | 6.83$\pm$1.49 | 4.57 | 6.76$\pm$2.05 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.868
J0148+0600-SMG2 | 01h48m40.0s | +05d59m36.0s | 5.43$\pm$1.27 | 4.27 | 4.98$\pm$1.55 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.950
J0148+0600-SMG3 | 01h48m39.4s | +06d00m44.0s | 5.18$\pm$1.22 | 4.23 | 4.66$\pm$1.45 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.617
J0148+0600-SMG4 | 01h48m42.9s | +06d01m08.0s | 5.86$\pm$1.43 | 4.11 | 5.56$\pm$1.79 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.561
J0148+0600-SMG5 | 01h48m30.8s | +06d00m12.0s | 5.23$\pm$1.42 | 3.67 | 4.72$\pm$1.61 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.681
J0148+0600-SMG6 | 01h48m41.0s | +06d01m20.0s | 4.79$\pm$1.32 | 3.64 | 4.12$\pm$1.39 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.326
P036+03-AGN | 02h26m02.8s | +03d02m59.4s | 5.47$\pm$1.01 | 5.42 | 5.31$\pm$1.48 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.000
P036+03-SMG1 | 02h26m02.6s | +03d04m19.4s | 11.32$\pm$1.08 | 10.49 | 11.39$\pm$1.77 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.335
P036+03-SMG2 | 02h25m58.0s | +03d03m47.4s | 6.33$\pm$1.06 | 6.00 | 6.33$\pm$1.68 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.444
P036+03-SMG3 | 02h25m58.6s | +03d01m47.4s | 4.79$\pm$1.15 | 4.16 | 4.44$\pm$1.39 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.607
P036+03-SMG4 | 02h26m10.0s | +03d02m43.4s | 5.20$\pm$1.31 | 3.96 | 4.96$\pm$1.62 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.822
P036+03-SMG5 | 02h26m02.6s | +03d03m47.4s | 4.04$\pm$1.04 | 3.89 | 3.43$\pm$1.10 | 53.42$\pm$17.57 | 3.04 | 39.99$\pm$14.54 | 0.803
P036+03-SMG6 | 02h26m05.0s | +03d04m27.4s | 4.40$\pm$1.16 | 3.79 | 3.93$\pm$1.29 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.561
J0305-3150-AGN | 03h05m18.2s | -31d50m55.8s | 8.43$\pm$1.08 | 7.78 | 8.50$\pm$1.77 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.078
J0305-3150-SMG1 | 03h05m22.3s | -31d49m47.8s | 6.50$\pm$1.30 | 5.00 | 6.49$\pm$1.83 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.579
J0305-3150-SMG2 | 03h05m12.5s | -31d51m23.8s | 5.27$\pm$1.11 | 4.76 | 5.00$\pm$1.47 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.413
J0305-3150-SMG3 | 03h05m26.0s | -31d49m59.8s | 5.93$\pm$1.45 | 4.08 | 5.83$\pm$1.86 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.244
J0305-3150-SMG4 | 03h05m07.8s | -31d50m51.8s | 4.41$\pm$1.23 | 3.58 | 3.86$\pm$1.31 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.512
P055-00-SMG1 | 03h41m44.2s | -00d48m28.6s | 6.38$\pm$1.31 | 4.86 | 6.21$\pm$1.79 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.657
P055-00-SMG2 | 03h41m40.8s | -00d47m12.6s | 4.84$\pm$1.25 | 3.88 | 4.21$\pm$1.35 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.035
P055-00-SMG3 | 03h41m43.2s | -00d47m28.6s | 4.86$\pm$1.28 | 3.80 | 4.23$\pm$1.38 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.806
P055-00-SMG4 | 03h41m38.1s | -00d50m04.6s | 5.39$\pm$1.49 | 3.61 | 4.97$\pm$1.69 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.087
P055-00-SMG5 | 03h41m38.1s | -00d46m36.6s | 4.66$\pm$1.33 | 3.51 | 3.97$\pm$1.36 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.853
P056-16-SMG1 | 03h46m58.0s | -16d29m44.8s | 5.85$\pm$1.05 | 5.55 | 5.81$\pm$1.51 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.688
P056-16-SMG2 | 03h46m58.0s | -16d28m08.8s | 5.08$\pm$1.02 | 4.96 | 4.95$\pm$1.40 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.336
P056-16-SMG3 | 03h46m48.3s | -16d27m04.8s | 4.16$\pm$1.09 | 3.81 | 3.84$\pm$1.27 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.936
P060+24-SMG1 | 04h02m08.4s | +24d51m32.5s | 6.90$\pm$1.28 | 5.39 | 6.83$\pm$1.86 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.329
P060+24-SMG2 | 04h02m07.2s | +24d50m08.5s | 6.78$\pm$1.46 | 4.65 | 6.69$\pm$1.97 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.054
P060+24-SMG3 | 04h02m19.8s | +24d52m20.5s | 4.88$\pm$1.34 | 3.63 | 4.32$\pm$1.46 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.803
P060+24-SMG4 | 04h02m12.2s | +24d52m48.5s | 4.41$\pm$1.23 | 3.57 | 3.68$\pm$1.25 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.447
P065-19-SMG1 | 04h22m01.7s | -19d29m28.6s | 6.22$\pm$1.22 | 5.09 | 6.20$\pm$1.73 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.001
P065-19-SMG2 | 04h21m56.9s | -19d26m28.6s | 5.13$\pm$1.04 | 4.95 | 4.95$\pm$1.45 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.619
P065-19-SMG3 | 04h22m05.4s | -19d26m48.6s | 4.28$\pm$1.08 | 3.95 | 3.81$\pm$1.23 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.079
P065-19-SMG4 | 04h22m09.3s | -19d26m20.6s | 4.98$\pm$1.32 | 3.78 | 4.74$\pm$1.60 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.160
P089-15-AGN | 05h59m46.4s | -15d35m00.1s | 3.56$\pm$1.17 | 3.05 | 2.60$\pm$0.96 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.000
P089-15-SMG1 | 05h59m42.8s | -15d34m56.1s | 6.28$\pm$1.17 | 5.36 | 6.13$\pm$1.65 | 100.56$\pm$31.85 | 3.16 | 76.23$\pm$27.15 | 0.902
P089-15-SMG2 | 05h59m53.3s | -15d34m20.1s | 5.64$\pm$1.46 | 3.86 | 5.37$\pm$1.75 | 113.21$\pm$36.11 | 3.13 | 93.10$\pm$33.58 | 1.854
J0810+5105-SMG1 | 08h10m57.6s | +51d04m32.1s | 4.85$\pm$1.22 | 3.98 | 4.34$\pm$1.38 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.416
J0810+5105-SMG2 | 08h10m52.1s | +51d04m40.1s | 4.65$\pm$1.26 | 3.69 | 4.06$\pm$1.35 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.132
J0810+5105-SMG3 | 08h11m04.4s | +51d04m52.1s | 4.70$\pm$1.28 | 3.69 | 4.13$\pm$1.37 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.670
J0810+5105-SMG4 | 08h10m47.5s | +51d06m36.1s | 4.76$\pm$1.34 | 3.55 | 4.22$\pm$1.44 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.938
J0828+2633-SMG1 | 08h28m09.5s | +26d34m39.5s | 7.12$\pm$1.31 | 5.45 | 7.10$\pm$1.88 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.215
J0828+2633-SMG2 | 08h28m15.1s | +26d31m55.5s | 5.68$\pm$1.45 | 3.92 | 5.41$\pm$1.75 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.049
J0828+2633-SMG3 | 08h28m15.4s | +26d33m03.5s | 4.41$\pm$1.23 | 3.58 | 3.71$\pm$1.24 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.012
J0835+3217-SMG1 | 08h35m33.3s | +32d19m08.6s | 5.89$\pm$1.42 | 4.15 | 5.65$\pm$1.75 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.278
J0835+3217-SMG2 | 08h35m34.9s | +32d18m00.6s | 5.79$\pm$1.49 | 3.89 | 5.52$\pm$1.78 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.291
J0835+3217-SMG3 | 08h35m32.1s | +32d17m56.6s | 5.08$\pm$1.35 | 3.78 | 4.59$\pm$1.49 | 54.28$\pm$17.32 | 3.13 | 43.16$\pm$15.51 | 1.579
J0839+0015-SMG1 | 08h39m57.7s | +00d16m50.2s | 4.75$\pm$1.28 | 3.72 | 4.18$\pm$1.37 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.110
J0842+1218-SMG1 | 08h42m27.4s | +12d19m34.5s | 8.49$\pm$1.36 | 6.24 | 8.53$\pm$2.05 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.875
J0842+1218-SMG2 | 08h42m25.8s | +12d18m50.5s | 6.15$\pm$1.31 | 4.68 | 5.91$\pm$1.74 | 51.62$\pm$13.79 | 3.74 | 44.90$\pm$14.33 | 0.887
J0850+3246-SMG1 | 08h50m41.9s | +32d45m11.9s | 6.08$\pm$1.39 | 4.38 | 5.86$\pm$1.82 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.253
J0850+3246-SMG2 | 08h50m54.3s | +32d46m51.9s | 4.79$\pm$1.35 | 3.54 | 4.12$\pm$1.41 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.508
P135+16-AGN | 09h01m32.6s | +16d15m06.8s | 5.16$\pm$1.34 | 3.86 | 4.49$\pm$1.44 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.000
P159-02-SMG1 | 10h36m48.3s | -02d31m45.8s | 6.61$\pm$1.38 | 4.80 | 6.47$\pm$1.89 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.705
P159-02-SMG2 | 10h36m58.7s | -02d31m49.8s | 5.51$\pm$1.49 | 3.69 | 5.05$\pm$1.70 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.388
J1048-0109-AGN | 10h48m19.0s | -01d09m40.2s | 4.56$\pm$1.17 | 3.89 | 3.99$\pm$1.26 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.000
J1048-0109-SMG1 | 10h48m20.4s | -01d11m12.2s | 7.74$\pm$1.37 | 5.66 | 7.79$\pm$1.91 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.569
J1048-0109-SMG2 | 10h48m23.0s | -01d09m00.2s | 5.61$\pm$1.33 | 4.23 | 5.37$\pm$1.63 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.202
J1048-0109-SMG3 | 10h48m12.1s | -01d08m20.2s | 4.97$\pm$1.39 | 3.59 | 4.54$\pm$1.51 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.187
J1048-0109-SMG4 | 10h48m22.8s | -01d10m20.2s | 4.59$\pm$1.30 | 3.53 | 4.03$\pm$1.35 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.147
P167-13-SMG1 | 11h10m30.7s | -13d31m05.5s | 5.40$\pm$1.38 | 3.92 | 5.03$\pm$1.62 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.567
P167-13-SMG2 | 11h10m29.6s | -13d29m09.5s | 4.31$\pm$1.21 | 3.56 | 3.58$\pm$1.20 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.250
J1143+3808-SMG1 | 11h43m46.0s | +38d07m48.7s | 6.19$\pm$1.49 | 4.15 | 5.85$\pm$1.83 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.060
J1143+3808-SMG2 | 11h43m37.6s | +38d09m36.7s | 5.86$\pm$1.43 | 4.10 | 5.44$\pm$1.70 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.146
J1148+0702-SMG1 | 11h48m00.6s | +07d02m44.3s | 10.02$\pm$1.33 | 7.54 | 10.07$\pm$1.99 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.901
J1148+0702-SMG2 | 11h48m05.4s | +07d02m48.3s | 4.87$\pm$1.36 | 3.58 | 4.22$\pm$1.39 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.856
J1152+0055-SMG1 | 11h52m12.9s | +00d55m48.6s | 7.68$\pm$1.23 | 6.23 | 7.62$\pm$1.84 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.077
J1152+0055-SMG2 | 11h52m23.4s | +00d56m28.6s | 4.16$\pm$1.13 | 3.69 | 3.48$\pm$1.17 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.018
J1152+0055-SMG3 | 11h52m19.1s | +00d57m00.6s | 4.19$\pm$1.15 | 3.65 | 3.52$\pm$1.20 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.498
J1152+0055-SMG4 | 11h52m21.0s | +00d56m28.6s | 3.98$\pm$1.09 | 3.65 | 3.24$\pm$1.09 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.869
J1152+0055-SMG5 | 11h52m28.2s | +00d56m48.6s | 5.32$\pm$1.50 | 3.56 | 5.01$\pm$1.76 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.108
J1205+0505-SMG1 | 12h05m06.4s | +00d01m03.9s | 7.49$\pm$1.31 | 5.72 | 7.49$\pm$1.85 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.569
J1205+0505-SMG2 | 12h05m08.0s | +00d00m03.9s | 5.12$\pm$1.32 | 3.89 | 4.69$\pm$1.49 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.907
J1207+0630-SMG1 | 12h07m36.3s | +06d31m46.0s | 6.03$\pm$1.30 | 4.62 | 5.85$\pm$1.72 | 31.86$\pm$10.23 | 3.11 | 25.61$\pm$9.28 | 1.622
J1207+0630-SMG2 | 12h07m37.9s | +06d30m50.0s | 4.47$\pm$1.24 | 3.59 | 3.73$\pm$1.22 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.680
P183+05-AGN | 12h12m27.2s | +05d05m29.4s | 9.03$\pm$1.30 | 6.93 | 9.13$\pm$2.03 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.094
P183+05-SMG1 | 12h12m23.4s | +05d05m33.4s | 4.77$\pm$1.34 | 3.55 | 4.06$\pm$1.37 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.870
P183+05-SMG2 | 12h12m29.6s | +05d06m13.4s | 4.93$\pm$1.42 | 3.48 | 4.30$\pm$1.48 | 33.47$\pm$8.93 | 3.75 | 28.82$\pm$9.26 | 0.945
P183-12-AGN | 12h13m11.7s | -12d46m03.5s | 4.08$\pm$1.14 | 3.59 | 3.25$\pm$1.09 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.000
P183-12-SMG1 | 12h13m13.9s | -12d46m39.5s | 9.48$\pm$1.21 | 7.83 | 9.48$\pm$1.86 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.812
P183-12-SMG2 | 12h13m14.8s | -12d45m11.5s | 4.53$\pm$1.25 | 3.62 | 3.89$\pm$1.32 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.147
P184+01-AGN | 12h17m21.8s | +01d31m30.4s | 3.67$\pm$1.12 | 3.26 | 2.76$\pm$0.97 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.240
P184+01-SMG1 | 12h17m26.6s | +01d31m14.4s | 5.85$\pm$1.29 | 4.54 | 5.61$\pm$1.69 | 43.03$\pm$11.41 | 3.77 | 39.76$\pm$12.68 | 1.413
P184+01-SMG2 | 12h17m18.6s | +01d30m50.4s | 4.96$\pm$1.17 | 4.23 | 4.48$\pm$1.39 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.094
P184+01-SMG3 | 12h17m20.0s | +01d33m10.4s | 4.55$\pm$1.24 | 3.67 | 3.91$\pm$1.31 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.504
P187+04-AGN | 12h29m12.3s | +04d19m23.6s | 3.81$\pm$1.25 | 3.04 | 2.79$\pm$1.03 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.211
P187+04-SMG1 | 12h29m09.7s | +04d20m47.6s | 6.88$\pm$1.35 | 5.09 | 6.79$\pm$1.92 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.592
P187+04-SMG2 | 12h29m13.1s | +04d20m03.6s | 5.35$\pm$1.24 | 4.30 | 4.84$\pm$1.46 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.600
J1243+2529-SMG1 | 12h43m43.4s | +25d28m15.8s | 7.94$\pm$1.45 | 5.46 | 8.01$\pm$2.17 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.314
J1243+2529-SMG2 | 12h43m42.8s | +25d30m19.8s | 5.55$\pm$1.40 | 3.95 | 5.06$\pm$1.61 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.067
J1257+6349-SMG1 | 12h57m59.3s | +63d50m29.1s | 5.11$\pm$1.10 | 4.65 | 4.84$\pm$1.39 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.978
J1257+6349-SMG2 | 12h57m46.6s | +63d49m49.1s | 5.29$\pm$1.20 | 4.42 | 5.07$\pm$1.50 | 35.14$\pm$9.23 | 3.81 | 32.30$\pm$10.30 | 2.728
P210+27-SMG1 | 14h01m53.0s | +27d49m10.9s | 9.33$\pm$1.30 | 7.15 | 9.45$\pm$2.13 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.487
P210+27-SMG2 | 14h01m46.1s | +27d49m54.9s | 5.02$\pm$1.20 | 4.19 | 4.46$\pm$1.41 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.449
P210+27-SMG3 | 14h01m45.5s | +27d48m46.9s | 4.75$\pm$1.18 | 4.03 | 4.09$\pm$1.31 | 38.46$\pm$10.43 | 3.69 | 32.77$\pm$10.57 | 0.919
P210+27-SMG4 | 14h01m49.4s | +27d49m38.9s | 4.47$\pm$1.19 | 3.74 | 3.70$\pm$1.22 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.532
P210+27-SMG5 | 14h01m39.8s | +27d50m18.9s | 5.29$\pm$1.49 | 3.54 | 4.84$\pm$1.71 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.022
P210+27-SMG6 | 14h01m40.1s | +27d48m54.9s | 4.99$\pm$1.42 | 3.51 | 4.43$\pm$1.56 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.928
P210+27-SMG7 | 14h01m42.8s | +27d49m38.9s | 4.47$\pm$1.28 | 3.50 | 3.70$\pm$1.28 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.133
P210+40-SMG1 | 14h03m00.6s | +40d23m59.1s | 5.51$\pm$1.27 | 4.34 | 5.18$\pm$1.57 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.490
P210+40-SMG2 | 14h02m55.3s | +40d24m15.1s | 4.69$\pm$1.24 | 3.77 | 4.04$\pm$1.31 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.266
P210-12-AGN | 14h03m29.8s | -12d00m34.1s | 3.56$\pm$1.16 | 3.07 | 2.61$\pm$0.96 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.136
P210-12-SMG1 | 14h03m31.4s | -12d01m06.1s | 5.71$\pm$1.21 | 4.70 | 5.45$\pm$1.58 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.763
P210-12-SMG2 | 14h03m28.2s | -11d58m50.1s | 5.41$\pm$1.40 | 3.85 | 5.06$\pm$1.64 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.755
P215-16-AGN | 14h20m36.2s | -16d02m30.2s | 16.85$\pm$1.10 | 15.36 | 16.96$\pm$1.90 | 26.93$\pm$7.78 | 3.46 | 21.66$\pm$7.26 | 0.000
P215-16-SMG1 | 14h20m35.4s | -16d03m34.2s | 6.08$\pm$1.20 | 5.07 | 5.97$\pm$1.73 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.087
P215-16-SMG2 | 14h20m37.1s | -16d01m58.2s | 4.97$\pm$1.14 | 4.36 | 4.54$\pm$1.40 | 27.51$\pm$7.92 | 3.47 | 22.46$\pm$7.53 | 0.572
P215-16-SMG3 | 14h20m35.7s | -16d00m50.2s | 5.13$\pm$1.30 | 3.95 | 4.76$\pm$1.56 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.672
P215-16-SMG4 | 14h20m34.0s | -16d02m02.2s | 3.97$\pm$1.10 | 3.60 | 3.17$\pm$1.06 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.725
P215-16-SMG5 | 14h20m39.6s | -16d02m02.2s | 4.19$\pm$1.19 | 3.54 | 3.47$\pm$1.19 | 27.06$\pm$8.28 | 3.27 | 21.87$\pm$7.65 | 0.954
P215+26-SMG1 | 14h21m42.0s | +26d33m09.0s | 6.83$\pm$1.22 | 5.59 | 6.75$\pm$1.79 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.236
P215+26-SMG2 | 14h21m42.3s | +26d33m45.0s | 5.79$\pm$1.28 | 4.51 | 5.52$\pm$1.65 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.814
P215+26-SMG3 | 14h21m43.2s | +26d31m33.0s | 4.56$\pm$1.21 | 3.76 | 3.89$\pm$1.26 | 33.35$\pm$10.85 | 3.07 | 24.92$\pm$9.01 | 0.400
P215+26-SMG4 | 14h21m50.1s | +26d33m01.0s | 5.11$\pm$1.43 | 3.57 | 4.62$\pm$1.57 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.019
P215+26-SMG5 | 14h21m37.9s | +26d32m41.0s | 4.45$\pm$1.26 | 3.53 | 3.74$\pm$1.26 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.529
P217-16-SMG1 | 14h28m21.3s | -16d01m15.3s | 5.81$\pm$1.38 | 4.22 | 5.54$\pm$1.73 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.467
P217-16-SMG2 | 14h28m20.2s | -16d02m15.3s | 4.52$\pm$1.22 | 3.69 | 3.79$\pm$1.24 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.543
P217-07-AGN | 14h31m40.7s | -07d24m47.5s | 6.03$\pm$1.17 | 5.16 | 5.86$\pm$1.61 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.095
P217-07-SMG1 | 14h31m38.0s | -07d24m03.5s | 4.97$\pm$1.22 | 4.08 | 4.53$\pm$1.40 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.900
P231-20-AGN | 15h26m37.8s | -20d50m00.7s | 7.99$\pm$1.22 | 6.53 | 8.06$\pm$1.99 | 80.31$\pm$19.97 | 4.02 | 71.00$\pm$21.54 | 0.000
P231-20-SMG1 | 15h26m39.8s | -20d51m12.7s | 6.01$\pm$1.35 | 4.46 | 5.77$\pm$1.77 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.300
P231-20-SMG2 | 15h26m38.4s | -20d50m44.7s | 5.40$\pm$1.26 | 4.27 | 4.98$\pm$1.56 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.747
P231-20-SMG3 | 15h26m38.9s | -20d51m36.7s | 5.57$\pm$1.39 | 4.00 | 5.22$\pm$1.70 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.625
P239-07-SMG1 | 15h58m56.0s | -07d23m57.6s | 4.62$\pm$1.31 | 3.53 | 4.02$\pm$1.37 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.293
J1609+3041-AGN | 16h09m36.9s | +30d41m47.6s | 4.09$\pm$1.17 | 3.50 | 3.27$\pm$1.11 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.078
J1609+3041-SMG1 | 16h09m44.7s | +30d41m51.6s | 7.19$\pm$1.44 | 5.01 | 7.16$\pm$2.00 | 25.56$\pm$8.27 | 3.09 | 20.53$\pm$7.45 | 1.862
J1609+3041-SMG2 | 16h09m32.3s | +30d43m43.6s | 5.40$\pm$1.35 | 3.99 | 5.02$\pm$1.62 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.297
J1609+3041-SMG3 | 16h09m42.5s | +30d43m03.6s | 4.90$\pm$1.28 | 3.83 | 4.37$\pm$1.44 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.828
J1609+3041-SMG4 | 16h09m31.4s | +30d42m43.6s | 4.63$\pm$1.28 | 3.62 | 4.01$\pm$1.36 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.744
P247+24-AGN | 16h29m11.8s | +24d07m35.6s | 6.76$\pm$1.13 | 5.98 | 6.77$\pm$1.72 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.161
P247+24-SMG1 | 16h29m03.7s | +24d08m39.6s | 6.65$\pm$1.32 | 5.05 | 6.65$\pm$1.83 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.146
P247+24-SMG2 | 16h29m05.1s | +24d06m07.6s | 6.65$\pm$1.39 | 4.80 | 6.66$\pm$1.89 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.169
P308-21-AGN | 20h32m09.7s | -21d14m02.3s | 4.23$\pm$1.09 | 3.86 | 3.59$\pm$1.17 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.072
P308-21-SMG1 | 20h32m15.9s | -21d13m02.3s | 9.92$\pm$1.37 | 7.27 | 10.00$\pm$2.00 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.804
P308-21-SMG2 | 20h32m10.8s | -21d12m54.3s | 6.13$\pm$1.22 | 5.02 | 6.02$\pm$1.71 | 60.37$\pm$18.27 | 3.30 | 49.54$\pm$17.18 | 1.153
P308-21-SMG3 | 20h32m05.1s | -21d15m10.3s | 5.03$\pm$1.19 | 4.23 | 4.65$\pm$1.44 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.662
P308-21-SMG4 | 20h32m06.8s | -21d14m10.3s | 4.30$\pm$1.11 | 3.88 | 3.70$\pm$1.20 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.798
P308-21-SMG5 | 20h32m08.8s | -21d16m02.3s | 4.72$\pm$1.30 | 3.64 | 4.27$\pm$1.45 | 62.30$\pm$20.10 | 3.10 | 52.20$\pm$19.02 | 2.020
P308-21-SMG6 | 20h32m08.8s | -21d13m10.3s | 4.32$\pm$1.19 | 3.64 | 3.73$\pm$1.26 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.913
P308-21-SMG7 | 20h32m13.7s | -21d15m06.3s | 4.50$\pm$1.24 | 3.63 | 3.97$\pm$1.35 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.415
P308-21-SMG8 | 20h32m13.7s | -21d14m26.3s | 4.17$\pm$1.18 | 3.55 | 3.51$\pm$1.20 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.012
J2100-1715-SMG1 | 21h01m00.0s | -17d14m02.5s | 5.21$\pm$1.20 | 4.34 | 5.05$\pm$1.55 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.739
J2100-1715-SMG2 | 21h00m58.1s | -17d16m58.5s | 4.68$\pm$1.12 | 4.18 | 4.40$\pm$1.39 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.719
J2100-1715-SMG3 | 21h00m53.6s | -17d15m14.5s | 3.73$\pm$0.95 | 3.91 | 3.18$\pm$1.04 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.507
J2100-1715-SMG4 | 21h00m58.4s | -17d13m42.5s | 4.76$\pm$1.22 | 3.89 | 4.52$\pm$1.49 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.807
P323+12-SMG1 | 21h32m35.2s | +12d16m27.1s | 5.78$\pm$1.24 | 4.68 | 5.66$\pm$1.65 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.492
P323+12-SMG2 | 21h32m25.7s | +12d18m43.1s | 4.63$\pm$1.24 | 3.72 | 4.24$\pm$1.42 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.261
P323+12-SMG3 | 21h32m28.7s | +12d16m39.1s | 4.46$\pm$1.22 | 3.65 | 4.03$\pm$1.37 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.862
P333+26-AGN | 22h15m57.6s | +26d06m33.3s | 3.83$\pm$1.04 | 3.69 | 3.07$\pm$1.03 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.067
P333+26-SMG1 | 22h16m05.9s | +26d07m21.3s | 8.11$\pm$1.27 | 6.39 | 8.12$\pm$1.89 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.252
P333+26-SMG2 | 22h16m04.4s | +26d07m13.3s | 5.70$\pm$1.20 | 4.74 | 5.54$\pm$1.68 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.858
P333+26-SMG3 | 22h16m03.8s | +26d07m53.3s | 4.79$\pm$1.19 | 4.01 | 4.37$\pm$1.43 | 95.40$\pm$22.93 | 4.16 | 92.95$\pm$27.69 | 2.095
P333+26-SMG4 | 22h15m50.5s | +26d05m33.3s | 4.65$\pm$1.22 | 3.82 | 4.18$\pm$1.41 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.011
P333+26-SMG5 | 22h15m54.3s | +26d07m45.3s | 4.22$\pm$1.13 | 3.73 | 3.60$\pm$1.22 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.507
P338+29-SMG1 | 22h32m58.5s | +29d29m44.1s | 6.50$\pm$1.45 | 4.48 | 6.31$\pm$1.92 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.162
P338+29-SMG2 | 22h32m54.5s | +29d32m08.1s | 6.16$\pm$1.43 | 4.30 | 5.88$\pm$1.83 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.607
P338+29-SMG3 | 22h32m56.4s | +29d31m00.1s | 4.70$\pm$1.32 | 3.57 | 3.94$\pm$1.36 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.558
P340-18-SMG1 | 22h40m46.9s | -18d39m43.8s | 4.91$\pm$1.03 | 4.79 | 4.64$\pm$1.36 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.774
P340-18-SMG2 | 22h40m48.6s | -18d39m11.8s | 4.10$\pm$1.03 | 3.97 | 3.57$\pm$1.14 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.639
P340-18-SMG3 | 22h40m49.1s | -18d37m39.8s | 4.93$\pm$1.31 | 3.76 | 4.66$\pm$1.56 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 2.077
P340-18-SMG4 | 22h40m50.0s | -18d40m23.8s | 3.86$\pm$1.05 | 3.66 | 3.24$\pm$1.08 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.667
J2348-3054-AGN | 23h48m34.3s | -30d54m10.1s | 5.88$\pm$1.06 | 5.52 | 5.81$\pm$1.51 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.000
J2348-3054-SMG1 | 23h48m40.8s | -30d53m46.1s | 5.02$\pm$1.27 | 3.96 | 4.78$\pm$1.50 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.680
P359-06-SMG1 | 23h56m30.7s | -06d23m35.2s | 4.50$\pm$1.14 | 3.96 | 3.95$\pm$1.28 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 0.900
P359-06-SMG2 | 23h56m28.3s | -06d24m07.2s | 5.08$\pm$1.31 | 3.88 | 4.74$\pm$1.57 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.706
P359-06-SMG3 | 23h56m27.5s | -06d22m31.2s | 4.35$\pm$1.16 | 3.76 | 3.73$\pm$1.24 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.548
P359-06-SMG4 | 23h56m37.4s | -06d21m47.2s | 4.95$\pm$1.33 | 3.73 | 4.56$\pm$1.55 |  $\cdots$ |  $\cdots$ |  $\cdots$ | 1.566

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