# SILVERRUSH. XIII. A Catalog of 20,567 Ly$\alpha$ Emitters at $z=2-7$
Identified
in the Full-Depth Data of the Subaru/HSC SSP and CHORUS Surveys

Satoshi Kikuta National Astronomical Observatory of Japan, 2-21-1, Osawa,
Mitaka, Tokyo 181-8588, Japan  Masami Ouchi  National Astronomical Observatory
of Japan, 2-21-1, Osawa, Mitaka, Tokyo 181-8588, Japan  Institute for Cosmic
Ray Research, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba
277-8582, Japan  Graduate University for Advanced Studies (SOKENDAI), 2-21-1
Osawa, Mitaka, Tokyo 181-8588, Japan  Kavli Institute for the Physics and
Mathematics of the Universe (WPI), University of Tokyo, Kashiwa, Chiba
277-8583, Japan  Takatoshi Shibuya  Kitami Institute of Technology, 165 Koen-
cho, Kitami, Hokkaido 090-8507, Japan  Yongming Liang  Institute for Cosmic
Ray Research, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba
277-8582, Japan  Hiroya Umeda  Institute for Cosmic Ray Research, The
University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan
Department of Physics, Graduate School of Science, The University of Tokyo,
7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan  Akinori Matsumoto  Institute for
Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa,
Chiba 277-8582, Japan  Department of Physics, Graduate School of Science, The
University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan  Kazuhiro
Shimasaku  Department of Astronomy, School of Science, The University of
Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan  Yuichi Harikane
Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwanoha,
Kashiwa, Chiba 277-8582, Japan  Yoshiaki Ono  Institute for Cosmic Ray
Research, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582,
Japan  Akio K. Inoue  Waseda Research Institute for Science and Engineering,
Faculty of Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku,
Tokyo 169-8555, Japan  Department of Physics, School of Advanced Science and
Engineering, Faculty of Science and Engineering, Waseda University, 3-4-1
Okubo, Shinjuku, Tokyo 169-8555, Japan  Satoshi Yamanaka  General Education
Department, National Institute of Technology, Toba College, 1-1, Ikegami-cho,
Toba, Mie 517-8501, Japan  Haruka Kusakabe  Observatoire de Genève, Université
de Genève, 51 Chemin de Pégase, 1290 Versoix, Switzerland  National
Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo 181-8588,
Japan  Rieko Momose  Carnegie Observatories, 813 Santa Barbara Street,
Pasadena, CA 91101, USA  Department of Astronomy, School of Science, The
University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan  Nobunari
Kashikawa  Department of Astronomy, School of Science, The University of
Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan  Yuichi Matsuda  National
Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo 181-8588,
Japan  Cahill Center for Astronomy and Astrophysics, California Institute of
Technology, MS 249-17, Pasadena, CA 91125, USA  Chien-Hsiu Lee  NSF’s National
Optical-Infrared Astronomy Research Laboratory, 950 N Cherry Ave., Tucson, AZ
86719, USA

###### Abstract

We present 20,567 Ly$\alpha$ emitters (LAEs) at $z=2.2-7.3$ that are
photometrically identified by the SILVERRUSH program in a large survey area up
to 25 deg2 with deep images of five broadband filters (grizy) and seven
narrowband filters targeting Ly$\alpha$ lines at $z=2.2$, $3.3$, $4.9$, $5.7$,
$6.6$, $7.0$, and $7.3$ taken by the Hyper Suprime-Cam Subaru Strategic
Program (HSC-SSP) and the Cosmic HydrOgen Reionization Unveiled with Subaru
(CHORUS) survey. We select secure $>5\sigma$ sources showing narrowband color
excesses via Ly$\alpha$ break screening, taking into account the spatial
inhomogeneity of limiting magnitudes. After removing spurious sources by
careful masking and visual inspection of coadded and multi-epoch images
obtained over the seven years of the surveys, we construct LAE samples
consisting of 6,995, 4,642, 726, 6,124, 2,058, 18, and 5 LAEs at $z=2.2$, 3.3,
4.9, 5.7, 6.6, 7.0, and 7.3, respectively, although the $z=7.3$ candidates are
tentative. Our LAE catalogs contain 241 spectroscopically confirmed LAEs at
the expected redshifts from previous work. We demonstrate that the number
counts of our LAEs are consistent with previous studies with similar LAE
selection criteria. The LAE catalogs will be made public on our project
webpage with detailed descriptions of the content and ancillary information
about the masks and limiting magnitudes.

Lyman-Alpha galaxies (978) — High-redshift galaxies (734) — Galaxy evolution
(594) — Galaxy formation (595)

††facilities: Subaru(HSC)††software: astropy (Robitaille et al., 2013; Price-
Whelan et al., 2018), Source Extractor (Bertin & Arnouts, 1996)

##  1 Introduction

Recent deep optical imaging observations for high-redshift galaxies step into
the new regime in survey parameter space. One of the most significant
advancements is the survey area that exceeds $\sim 10$ deg2, as achieved by
the 8m-Subaru Hyper Suprime-Cam (HSC) survey (Aihara et al., 2018a) and the
Dark Energy Survey (DES; Abbott et al., 2018). These large-area data provide
statistical measurements for unexplored low-number-density objects with
negligible statistical errors, such as the luminosity function at the galaxy-
AGN transition magnitudes (Ono et al., 2018, 2021; Ouchi et al., 2018;
Harikane et al., 2018a, 2022; Konno et al., 2018; Stevans et al., 2018;
Guarnieri et al., 2019; Adams et al., 2020; Moutard et al., 2020; Taylor et
al., 2021). Moreover, large area surveys have identified rare objects
including high-$z$ Ly$\alpha$ blobs (e.g., Shibuya et al., 2018a; Kikuta et
al., 2019; Taylor et al., 2020; Zhang et al., 2021) and protoclusters (e.g.,
Toshikawa et al., 2018; Harikane et al., 2019; Hu et al., 2021).

Large-area imaging surveys are specifically useful for studying Ly$\alpha$
emitters (LAEs), which are probes of cosmic reionization and galaxy formation
(Ouchi et al., 2020). The large volume is necessary to constrain the
cosmological average properties of galaxy Ly$\alpha$ emission escaping from
the interstellar and intergalactic media. Large area observations for LAEs are
complementary to small volume but very deep spectroscopic studies with
VLT/MUSE (Bacon et al., 2023) that reveal spectroscopic properties including
Ly$\alpha$ spectral and spatial profiles (Leclercq et al., 2017, 2020) down to
very faint luminosity limits of $\sim 10^{41}-10^{42}$ erg s-1 at $z=3-7$.

One of the major large-area LAE surveys is the HSC Subaru Strategic Program
(SSP; Aihara et al., 2018a, b, 2019, 2022). The survey takes narrowband (NB)
images covering up to a total area of $25$ deg2 using four NB filters, NB387,
NB816, NB921, and NB1010, whose central wavelengths are 3862, 8177, 9215, and
10097 Å targeting LAEs at $z=2.2$, $5.7$, $6.6$, and $7.3$, respectively, by
NB excess (Ouchi et al., 2018) with broadband images taken with five broadband
(BB) filters (g,r,i,z, and y bands). The HSC-SSP observations started in 2014
and were completed at the end of 2021. The completed NB and BB imaging data
are reduced and released in the S21A internal release (and will be made public
in the final data release, Public Data Release 4). In the COSMOS field that is
part of the HSC-SSP survey imaging footprints, deep imaging observations with
additional HSC NB filters were conducted in the Subaru intensive program
entitled the Cosmic HydrOgen Reionization Unveiled with Subaru (CHORUS; Inoue
et al., 2020). The CHORUS program has taken deep imaging data with the NB387
filter as well as the NB527, NB718, and NB973 filters whose central
wavelengths are 5260, 7170, and 9713 Å tracing Ly$\alpha$ emission of LAEs at
$z=3.3$, $4.9$, and $7.0$, respectively. In the past, LAE catalogs were made
with the HSC-SSP NB images (Shibuya et al., 2018a), the CHORUS NB images (Itoh
et al., 2018; Zhang et al., 2020), and both of the NB images (Ono et al.,
2021). However, the HSC-SSP imaging observations were not fully completed at
the time of these cataloging efforts. Part of the HSC-SSP NB imaging was
missing even in Ono et al. (2021), and all of these publications did not use
the HSC-SSP full-depth BB images for the offbands of the LAE selections.

Here we make use of the full-depth/coverage dataset of the Subaru SSP NB and
BB (i.e. offband) images provided in the S21A internal release together with
the newly processed CHORUS NB images, and select LAEs with the full dataset at
the completion of the survey. The information about NB filters used in this
work is presented in Table 1, and their transmission curves are presented in
Figure 1. These LAEs are useful for statistical studies on galaxy formation
and cosmic reionization (Umeda et al. in preparation) and are fed to the
forthcoming massive spectroscopic program of the Subaru Prime Focus
Spectrograph (PSF; Takada et al., 2014) survey, which complements the ongoing
LAE spectroscopic program of Hobby-Eberly Telescope Dark Energy Experiment
(HETDEX; Gebhardt et al., 2021) in terms of depths, areas, and redshifts (cf.
Zhang et al., 2021).

Throughout this paper, we use the AB magnitude system and assume a cosmology
with $\Omega_{\mathrm{m}}=0.3$, $\Omega_{\mathrm{\Lambda}}=0.7$, and
$H_{0}=70\mathrm{~{}km~{}s^{-1}~{}Mpc^{-1}}$, unless otherwise noted.

Table 1: HSC Narrowband Filters Used in This Work Filter | $\lambda_{\mathrm{c}}$ | FWHM | z_Lyα
---|---|---|---
| (Å) | (Å) |
NB387 | 3862 | 55 | 2.18±0.023
NB527 | 5260 | 79 | 3.33±0.032
NB718 | 7170 | 111 | 4.90±0.046
NB816 | 8177 | 113 | 5.72±0.046
NB921 | 9215 | 135 | 6.58±0.056
NB973 | 9713 | 112 | 6.99±0.046
NB1010 | 10097 | 91 | 7.30±0.037
Figure 1: Total transmission curves of relevant HSC filters based on the area-
weighted mean measurements, including the transmission of the atmosphere, the
prime focus unit, and the dewer window; the primary mirror reflectivity;
average CCD quantum efficiency; and the effect of vignetting. Colored thick
curves show the transmission of NB filters, from left to right: NB387, NB527,
NB718, NB816, NB921, NB973, and NB1010. Black curves show the transmission of
HSC broadband filters, from left to right: g, r2, i2, z, and y. Note that the
r and i band filters were replaced with the new r2 and i2 filters in 2016, but
hereafter we simply refer to them as r and i bands.

##  2 Data and LAE Selection

###  2.1 Survey Data and Source Detection

We combine the data products from the HSC-SSP S21A internal release with data
obtained from the CHORUS project (Inoue et al., 2020). HSC-SSP is a three-
tiered imaging survey consisting of the Wide, Deep (D), and UltraDeep (UD)
layers. In the Deep layer, three narrow-band (NB) filters (NB387, NB816, and
NB921) are used in addition to five broad-band (BB) filters (grizy; Kawanomoto
et al., 2018). In the UD layer, the three NB filters and the NB1010 filter are
used, while the NB387 filter is not used. The D layer covers four separate
fields: D-COSMOS, D-DEEP23, D-ELAISN1, and D-SXDS. The UD layer covers two
areas in two fields in the D layer: UD-COSMOS and UD-SXDS. The CHORUS project
is a deep HSC imaging survey that targets the UD-COSMOS field with four
custom-made NB filters and one intermediate band filter (NB387, NB527, NB718,
NB973, and IB0945).

We use the HSC-SSP coadded images from the (currently) internal S21A release,
which are reduced with hscPipe version 8, except for the NB387 images for the
COSMOS field. For the NB images taken in the CHORUS project, we download raw
data and newly reduce them using the same hscPipe v8, because the public
CHORUS images (CHORUS PDR1111https://hsc-
release.mtk.nao.ac.jp/doc/index.php/chorus/) are reduced with the previous
version of hscPipe. Since the NB387 images of the UD-COSMOS field (the center
of the four D-COSMOS pointings) are not observed by HSC-SSP (and thus have a
hole in the footprint; see Aihara et al., 2022) but by CHORUS, we combine raw
NB387 images from both surveys and newly produce the NB387 images of the
COSMOS field without gaps of the observation footprints. We then correct a
known systematic offset of $-0.45$ mag in a zero-point magnitude of our NB387
images (Liang et al., 2021; Aihara et al., 2022)222see also the Known Problems
page of HSC-SSP: https://hsc-release.mtk.nao.ac.jp/doc/index.php/known-
problems__pdr3/#hsc-link-0. For the newly reduced COSMOS NB387 images, we
correct an additional offset of $-0.13$ mag inferred from a comparison between
the total magnitudes of stellar objects in the HSC-SSP PDR2 images and our
data. The effective survey areas after masking (Section 2.3) for each NB are
listed in Table 2. The HSC images are processed in $1.7\deg\times 1.7\deg$
square regions called “tracts” in the current HSC pipeline. Tracts are pre-
defined as an iso-latitude tessellation, and each tract is further divided
into $9\times 9$ “patches” with 4100 or 4200 pixels on a side ($\sim
11.5\arcmin$). Adjacent tracts have an overlap of one patch, and adjacent
patches have an overlap of 100 pixels (17″) on their edges. Our source
detection and object selection are conducted on these patch images. The
catalogs of the individual patches are combined after the selection (Section
2.2) and masking (Section 2.3).

First, we measure the point spread function (PSF) size from the full width at
half maximums (FWHMs) of point sources in all coadded images patch by patch,
and smooth the images with a Gaussian kernel to match the FWHMs to the largest
PSF image (1$.\\!\\!\arcsec$0) to enable reliable measurement of source colors
using aperture photometry. Next, we run SExtractor (Bertin & Arnouts, 1996) in
the dual image mode on the PSF-matched images using each NB as a detection
band. The important parameters of SExtractor are set to the following values:
DETECT_MINAREA$=5$, DETECT_THRESH$=2.0$, BACK_SIZE$=64$. We use
2$.\\!\\!\arcsec$0-diameter aperture magnitudes to measure the colors of
detected sources.

Table 2: Effective survey area Field | NB387 | NB527 | NB718 | NB816 | NB921 | NB973 | NB1010
---|---|---|---|---|---|---|---
| (deg2) | (deg2) | (deg2) | (deg2) | (deg2) | (deg2) | (deg2)
COSMOS | 7.14 | 1.79 | 1.76 | 6.66 | 6.70 | 1.72 | 1.76
DEEP2-3 | 6.01 |  $\cdots$ |  $\cdots$ | 5.68 | 5.70 |  $\cdots$ |  $\cdots$
ELAIS-N1 | 6.24 |  $\cdots$ |  $\cdots$ | 5.62 | 5.63 |  $\cdots$ |  $\cdots$
SXDS | 4.55 |  $\cdots$ |  $\cdots$ | 5.93 | 5.96 |  $\cdots$ | 1.76
Total | 23.94 | 1.79 | 1.76 | 23.89 | 23.99 | 1.72 | 3.52

Since our survey area is large and HSC-SSP has multiple layers with different
depths, the limiting magnitudes within each survey field vary. Adopting a
single representative value as a limiting magnitude over the fields, as often
done in previous studies, would result in non-uniform detections with more
sources detected in low-signal-to-noise ratio (S/N) regions (e.g., near the
edge of the survey fields) with a high rate of spurious sources. To address
this issue, we measure the limiting magnitudes of all bands on a patch-by-
patch basis. After masking low-S/N regions near the edges of the survey
fields, 2$.\\!\\!\arcsec$0-aperture magnitudes of random points in each patch
are measured. The number of random points in each patch is generally 10,000 or
a smaller value depending on the area of masked regions. Their standard
deviations $\sigma$ are obtained from the distribution of the aperture counts
by fitting a Gaussian and used as $1\sigma$ 2$.\\!\\!\arcsec$0-aperture
limiting magnitudes. We show the resulting $5\sigma$ limiting magnitude maps
for all filters in Figures 10–19 in Appendix A. Galactic extinction correction
for all sources is also performed on a patch-by-patch basis with $A_{V}$
values of patch centers from the Schlafly & Finkbeiner (2011) calibration and
assuming the extinction curve from Fitzpatrick (1999) with $R_{V}=3.1$. We
select LAE candidates based on these detection catalogs and limiting magnitude
maps.

###  2.2 Photometric Selection Criteria of LAEs

We use the following photometric criteria to select LAE candidates
consistently with previous studies (Shibuya et al., 2018a; Itoh et al., 2018;
Zhang et al., 2020; Ono et al., 2021; Goto et al., 2021):

$\displaystyle\begin{split}\mathrm{NB387}<\mathrm{NB387_{6\sigma}}~{}\mathrm{AND}\\\
\mathrm{g}-\mathrm{NB387}>\mathrm{max}(0.2,(\mathrm{g}-\mathrm{NB387})_{\mathrm{3\sigma}})~{}\mathrm{AND}\\\
\mathrm{r}-\mathrm{NB387}>0.3~{}\mathrm{AND}\\\
\mathrm{i}-\mathrm{NB387}>0.4~{}\mathrm{AND}\\\
\mathrm{z}-\mathrm{NB387}>0.5\end{split}$ (1)

for $z=2.2$ LAEs,

$\displaystyle\begin{split}\mathrm{NB527}<\mathrm{NB527_{5\sigma}}~{}\mathrm{AND}\\\
\mathrm{g}-\mathrm{NB527}>\mathrm{max}(0.9,(\mathrm{g}-\mathrm{NB527})_{\mathrm{3\sigma}})~{}\mathrm{AND}\\\
\mathrm{r}-\mathrm{NB527}>0.3~{}\mathrm{AND}\\\
\mathrm{i}-\mathrm{NB527}>0.4~{}\mathrm{AND}\\\
\mathrm{z}-\mathrm{NB527}>0.5\end{split}$ (2)

for $z=3.3$ LAEs,

$\displaystyle\begin{split}\mathrm{g}>\mathrm{g_{2\sigma}}~{}\mathrm{AND}~{}\mathrm{NB718}<\mathrm{NB718_{5\sigma}}~{}\mathrm{AND}\\\
\mathrm{ri}-\mathrm{NB718}>\mathrm{max}(0.7,(\mathrm{ri}-\mathrm{NB718})_{\mathrm{3\sigma}})~{}\mathrm{AND}\\\
\mathrm{r}-\mathrm{i}>0.8\end{split}$ (3)

for $z=4.9$ LAEs, where ri is calculated by the linear combination of the
fluxes in the r band, $f_{\mathrm{r}}$, and those of the i band,
$f_{\mathrm{i}}$, as $f_{\mathrm{ri}}=0.3f_{\mathrm{r}}+0.7f_{\mathrm{i}}$,

$\displaystyle\begin{split}\mathrm{g}>\mathrm{g_{2\sigma}}~{}\mathrm{AND}~{}\mathrm{NB816}<\mathrm{NB816_{5\sigma}}~{}\mathrm{AND}\\\
\mathrm{i}-\mathrm{NB816}>\mathrm{max}(1.2,(\mathrm{i}-\mathrm{NB816})_{\mathrm{3\sigma}})~{}\mathrm{AND}\\\
((\mathrm{r}>\mathrm{r_{3\sigma}})~{}\mathrm{OR}~{}(\mathrm{r}<\mathrm{r_{3\sigma}}~{}\mathrm{AND}~{}\mathrm{r}-\mathrm{i}>1.0))\end{split}$
(4)

for $z=5.7$ LAEs,

$\displaystyle\begin{split}\mathrm{g}>\mathrm{g_{2\sigma}}~{}\mathrm{AND}~{}\mathrm{r}>\mathrm{r_{2\sigma}}~{}\mathrm{AND}\\\
\mathrm{NB921}<\mathrm{NB921_{5\sigma}}~{}\mathrm{AND}\\\
\mathrm{z}-\mathrm{NB921}>\mathrm{max}(1.0,(\mathrm{z}-\mathrm{NB921})_{\mathrm{3\sigma}})~{}\mathrm{AND}\\\
((\mathrm{z}>\mathrm{z_{3\sigma}})~{}\mathrm{OR}~{}(\mathrm{z}<\mathrm{z_{3\sigma}}~{}\mathrm{AND}~{}\mathrm{i}-\mathrm{z}>1.0))\end{split}$
(5)

for $z=6.6$ LAEs,

$\displaystyle\begin{split}\mathrm{g}>\mathrm{g_{2\sigma}}~{}\mathrm{AND}~{}\mathrm{r}>\mathrm{r_{2\sigma}}~{}\mathrm{AND}~{}\mathrm{i}>\mathrm{i_{2\sigma}}~{}\mathrm{AND}\\\
\mathrm{NB973}<\mathrm{NB973_{5\sigma}}~{}\mathrm{AND}\\\
((\mathrm{z}>\mathrm{z_{3\sigma}})~{}\mathrm{OR}~{}(\mathrm{z}<\mathrm{z_{3\sigma}}~{}\mathrm{AND}~{}\mathrm{z}-\mathrm{y}>2.0))~{}\mathrm{AND}\\\
\mathrm{y}-\mathrm{NB973}>0.7\end{split}$ (6)

for $z=7.0$ LAEs, and

$\displaystyle\begin{split}\mathrm{g}>\mathrm{g_{2\sigma}}~{}\mathrm{AND}~{}\mathrm{r}>\mathrm{r_{2\sigma}}~{}\mathrm{AND}~{}\mathrm{i}>\mathrm{i_{2\sigma}}~{}\mathrm{AND}~{}\mathrm{z}>\mathrm{z_{2\sigma}}~{}\mathrm{AND}\\\
\mathrm{NB1010}<\mathrm{NB1010_{5\sigma}}~{}\mathrm{AND}~{}\mathrm{y}-\mathrm{NB1010}>1.9\hskip
28.45274pt\end{split}$ (7)

for $z=7.3$ LAEs. When evaluating colors, if the broadband magnitudes are
fainter than $2\sigma$, we replace them with the $2\sigma$ limiting
magnitudes. We remove unrealistically compact sources ($\mathrm{FWHM}<5$ pix)
with measured FWHMs well below the sequence made by real point sources
($\mathrm{FWHM}=6$ pix) in an FWHM vs. NB magnitude plot. For NB387 LAEs, we
exclude sources that are very bright ($\mathrm{NB387}<18$ mag) and saturated
in any of the NB or BB filters. In addition, we set the threshold for
detection in NB387 to $6\sigma$ instead of $5\sigma$. This is to avoid
detecting spurious sources in high noise regions; the detected source number
as a function of significance of NB387 2$.\\!\\!\arcsec$0-aperture magnitude
grows much faster below 6$\sigma$ due to the noise. The numbers of photometric
LAE candidates at this step and those of the following steps (specified in
Section 2.3) are listed in Table 3.

###  2.3 Screening

The photometric candidates still contain a huge number of spurious sources,
particularly near the edge of our survey field. We make masks to efficiently
exclude spurious sources before visual inspection. The masks are placed in
problematic regions of the images, where detected source density is higher
than good regions. Specifically, low-S/N regions (near the survey field edge
or due to pipeline failures), bright star halos, blooming features, channel-
stop features (only in the y, NB973, and NB1010 filters), optical ghosts, and
satellite trails are masked. Our masks for the four SSP NB filters are made
based on the official Bright Star Masks333https://hsc-
release.mtk.nao.ac.jp/doc/index.php/bright-star-masks__pdr3/, with additional
regions added to remove artifacts that are not included in the official masks,
and unnecessary official masks deleted or reduced in size. For CHORUS NBs, we
define masks by ourselves paying particular attention to the high (spurious)
source density regions. At this stage, we combine the catalogs of all patches
for the four separate fields (COSMOS, DEEP2-3, ELAIS-N1, SXDS, with no
distinction of D and UD), and remove sources that appear twice or more due to
patch and tract overlap with a matching radius of 0$.\\!\\!\arcsec$336 (2
pixels). For a pair of objects from different patches with separation
$<$0$.\\!\\!\arcsec$336, we exclude sources with higher MAGERR_APER measured
by SExtractor from the catalogs. This process reduces the number of sources by
$\sim 25$%. In Ono et al. (2021), patch-by-patch limiting magnitude
measurements and masking of problematic regions are not performed, resulting
in a large number of photometric candidates and the use of machine learning
techniques. As Table 3 shows, we can significantly reduce the number of
candidates for visual inspection by appropriately setting the limiting
magnitudes and using masks ($90-99.7$%). Since the sample size of our
candidates at this stage is already comparable to that of Ono et al. (2021)
after the machine learning selection, we directly proceed to visual
inspection.

Our visual inspection is conducted by four individuals (SK, YL, HU, AM). The
candidates are classified as either secure, ambiguous, or spurious sources.
Objects are labeled as “spurious” when they are identified as cosmic rays,
sources with a sharp edge (probably due to some pipeline failures), sources
detected in problematic regions remaining after masking, or any other signals
that seem to be artificial. Sources that appear to be associated with resolved
nearby galaxies are classified as spurious. Additionally, if objects are
sufficiently bright (and hence potentially astrophysically interesting) but
could be moving or transient objects that are identified from their shapes or
unphysically high NB excesses, we inspect warp images (see next paragraph) and
label them as spurious if their non-static nature is confirmed. Objects are
labeled as “ambiguous” if they are very diffuse or hard to distinguish from
noise and ghosts. Consistencies between the classifications by each individual
are checked with NB816 LAE candidates in the COSMOS field. We achieve a
$>96\%$ consistency, with the inconsistent cases mostly being faint ambiguous
sources or located at problematic regions. The fractions of survived sources
are, from the NB387 to NB1010 sample, 55%, 76%, 92%, 50%, 52%, 22%, and 0.90%
(Table 3), although five candidates in the NB1010 sample are very tentative
(see discussion in Section 3.2).

Since bright LAEs are rare, they are more susceptible to contamination by
artificial signals and non-static sources, such as moving objects, than
numerous fainter sources. To further screen out any remaining contaminants in
bright candidates, we visually inspect their NB photometry in multi-epoch
images taken over a period of up to 7 years for the HSC-SSP NBs. The numbers
of objects inspected in each NB are 379, 318, 110, and 5 for NB387 (all
candidates with $\mathrm{NB387}<22.5$ 2$.\\!\\!\arcsec$0-aperture mag), NB816
($<24.5$ 2$.\\!\\!\arcsec$0-aperture mag), NB921 ($<24.5$
2$.\\!\\!\arcsec$0-aperture mag), and NB1010 (all), respectively. Objects that
do not show consistent brightness and/or peak locations in multi-epoch images
(except for cases with pipeline failures or when the source falls on the CCD
gaps or any other unusable regions; such shots are mostly clipped before
coadding) are excluded from our catalogs. The numbers of excluded sources are
1, 20, 28, and 0 for NB387, NB816, NB921, and NB1010, respectively. We also
try to identify contaminants with warp images for the CHORUS NBs, although the
time spans of imaging observations of the CHORUS NBs are shorter than HSC-
SSP’s duration (3 days for NB718 and NB973, and 3 month for NB527, but most of
the NB527 images are taken within 3 days, with only 2 shots taken 3 months
before those observations being available). We check 212, 101, 23 objects for
NB527 (all candidates with $\mathrm{NB527}<24.5$ 2$.\\!\\!\arcsec$0-aperture
mag), NB718 ($\mathrm{NB718}<25.0$ 2$.\\!\\!\arcsec$0-aperture mag), and NB973
(all), respectively. We exclude 1, 0, and 5 objects in the NB527, NB718, and
NB973 samples, respectively. This completes our cataloging process.

Table 3: Numbers of candidates remaining after each step and final samples Filter | NB387 | NB527 | NB718 | NB816 | NB921 | NB973 | NB1010
---|---|---|---|---|---|---|---
Photometric selection | 176843 | 28346 | 2577 | 208675 | 174137 | 41232 | 67409
Masking | 16552 | 7153 | 934 | 16156 | 5192 | 123 | 680
Overlap Rejection | 12599 | 6096 | 789 | 12325 | 3989 | 106 | 556
Visual Inspection | 6996 | 4642 | 726 | 6144 | 2086 | 23 | 5
Final sample | 6995 | 4641 | 726 | 6124 | 2058 | 18 |  **tentative candidates (see Section 3.2)5
COSMOS | 3160 | 4641 | 726 | 1625 | 547 | 18 | 3
DEEP2-3 | 1093 |  $\cdots$ |  $\cdots$ | 1551 | 494 |  $\cdots$ |  $\cdots$
ELAIS-N1 | 1767 |  $\cdots$ |  $\cdots$ | 1354 | 468 |  $\cdots$ |  $\cdots$
SXDS | 975 |  $\cdots$ |  $\cdots$ | 1594 | 549 |  $\cdots$ | 2

##  3 Results and Discussion

###  3.1 Sky Distributions and Number Counts

The numbers of LAE candidates at $z=2.2$, 3.3, 4.9, 5.7, 6.6, 7.0, and 7.3
after screening are 6995, 4641, 726, 6124, 2058, 18, and 5, respectively. We
also list the numbers of LAEs in each field in Table 3. The sky distributions
of our secure LAEs are presented in Figures 2–5. Sufficiently bright
candidates ($<24.0$ mag for the NB387 sample, $<25.75$ mag for the NB527 and
NB718 samples, and $<25.5$ mag for the NB816 and NB921 samples) which can be
homogeneously selected over the entire fields are plotted with thick blue
dots, while faint candidates, which are especially more numerous in the UD
layer, are plotted with thin blue dots for clarity. There are no clear
underdensities of real sources or overdensities made of spurious sources near
the edges of the HSC pointings, ensuring that our selection with spatially
dependent detection limits (Figures 10–13) and the screening processes
specified in Section 2.3 successfully provide clean samples.

Figure 2: Sky distribution of NB387 LAEs ($z=2.2$). Thick (thin) blue dots
indicate the locations of objects brighter (fainter) than
$\mathrm{NB387}=24.0$ mag, respectively. North is up, and east to the left.
Masked regions are shown in gray. Figure 3: Sky distribution of NB816 LAEs
($z=5.7$). Thick (thin) blue dots indicate the locations of objects brighter
(fainter) than $\mathrm{NB816}=25.5$ mag, respectively. North is up, and east
to the left. Masked regions are shown in gray. Figure 4: Sky distribution of
NB921 LAEs ($z=6.6$). Thick (thin) blue dots indicate the locations of objects
brighter (fainter) than $\mathrm{NB921}=24$ mag, respectively. North is up,
and east to the left. Masked regions are shown in gray. Figure 5: From left to
right, sky distribution of NB527, NB718, and NB973 LAEs ($z=3.3,4.9$, and
7.0). Thick (thin) blue dots indicate the locations of objects brighter
(fainter) than NB527 or $\mathrm{NB718}=25.75$ mag, while all sources are
plotted with thick blue dots in the NB0973 map. North is up, and east to the
left. Masked regions are shown in gray.

Figure 6 presents the surface number density, or number counts, of our LAEs in
the COSMOS, DEEP2-3, ELAIS-N1, and SXDS sub-fields for the three SSP NB
filters. The number counts are in good agreement among the sub-fields,
indicating that the LAEs are uniformly sampled within the galaxy clustering
signals that are quantified in Umeda et al. (in preparation). We compare the
average number counts over our survey fields with those from previous studies
in Figure 7 (SSP NBs) and Figure 8 (CHORUS NBs). Our number counts are largely
consistent with those from previous studies, with differences mostly due to
variations in selection criteria, survey depths, and cosmic variance. For
instance, our number count for NB387 shows a higher value than previous
studies at the fainter end, which could be explained by the difference in
selection criteria. Specifically, Nakajima et al. (2012) and Hao et al. (2018)
use the u and B bands to constrain the Lyman break of LAEs and remove some
low-redshift contaminants, whereas we and Ono et al. (2021) do not. Our number
counts for NB527 show a factor of $\sim$2 excess compared to others, but this
discrepancy can be attributed to differences in selection criteria, such as
the use of the B band and stricter NB excess criteria in Ouchi et al. 2008.
Indeed, the excess is mitigated if we adopt a similarly strict NB excess
criteria ($\mathrm{g}-\mathrm{NB527}>1.3$) as in Ouchi et al. (2008). On the
other hand, Ono et al. (2021) use selection criteria that were almost
identical to ours and the data from the HSC-SSP PDR2 and the CHORUS PDR1. We
notice that our bright $z=3.3$ LAEs (where photometric errors are negligible)
are also listed in the original detection catalog of Ono et al. (2021) and
meet the selection criteria even in their S18A photometry, but $\sim 50\%$ of
them are not included in their final LAE catalog. This indicates that their
machine learning selection method misses a considerable fraction of the good
candidates, highlighting the limitations of the technique. One possible reason
for this could be that their training datasets do not include major
contaminants such as stellar halos and ghosts or atypical real LAEs such as
Lyman alpha blobs (LABs), leading to lower purity and completeness. To improve
the performance of machine learning techniques, a prior understanding of the
characteristics of typical contaminants and the objects of interest is
necessary.

Figure 6:  Number counts of our LAEs in each sub-field. From Top to Bottom,
results for NB387, NB816, and NB921 are shown. Here we use total magnitude
(MAG_AUTO of SExtractor) for the x-axis value. Symbols for the same x-axis
value are slightly offset for clarity. Figure 7:  Similar to Figure 6, but the
mean number counts of our LAEs are compared with those of similar previous LAE
surveys. From Top to Bottom, results for NB387, NB816, and NB921 are shown.
Here we use total magnitude (MAG_AUTO of SExtractor) for the x-axis value for
a fair comparison. References for the NB387 results: Nakajima et al. (2012);
Hao et al. (2018); References for the NB816 results: Ouchi et al. (2008);
Shibuya et al. (2018a); Ono et al. (2021); References for the NB921 results:
Ouchi et al. (2010); Shibuya et al. (2018a); Ono et al. (2021).  Figure 8:
Similar to Figure 7, but showing the result for the CHORUS NBs. From Top to
Bottom, results for NB527, NB718, and NB973 are shown. Here we use total
magnitude (MAG_AUTO of SExtractor) for the x-axis value for a fair comparison.
References for the NB527 results: Ouchi et al. (2008); Ono et al. (2021);
References for the NB718 results: Zhang et al. (2020); Ono et al. (2021);
References for the NB973 results: Itoh et al. (2018); Ono et al. (2021).

###  3.2 Reliability of the NB1010 ($z=7.3$) Candidates

We identify five tentative candidates at $z=7.3$ with NB1010 detection less
than $<5.4\sigma$ and no detection above $2\sigma$ in the five BBs, including
the y band ($<1.1\sigma$ for all candidates). However, given their diffuse
appearance, caution is warranted. To assess the significance of these sources,
we invert the NB1010 images and attempt to identify LAE candidates using the
same selection criteria and screening processes. This leads to the
identification of the comparable number of candidates, which suggests that the
detection of the five sources could be explained by background fluctuations.
If they are real, although the result of this test and nondetection of lower-
equivalent width LAEs which should be more abundant suggest otherwise, their
nondetection in the y band (all below $1.1\sigma$, which is statistically
consistent with zero flux in the y band) suggests very high lower limits on
their Ly$\alpha$ equivalent widths (see Figure 4 of Goto et al., 2021). When
their y band flux is replaced with $2\sigma$ upper limits,
$\mathrm{y_{2\sigma}-NB1010}$ values range from 2.6-2.9, corresponding to
lower limits on Ly$\alpha$ equivalent widths of 50–300 Å, even if they are
precisely at $z=7.30$. These values are close to the maximum physically
possible value of 3.1. LAEs with Ly$\alpha$ equivalent width $>300$ Å are
exceptionally rare (Hashimoto et al., 2017), but the recent JWST discovery of
a $z=7.3$ LAE with Ly$\alpha$ equivalent width of $\sim 400$ Å by Saxena et
al. (2023) and our tentative detection, if real, imply that such extreme LAEs
could be common during the epoch of reionization. In either case, the
constraint on the number density of $z=7.3$ LAEs from this study is consistent
within $1\sigma$ with Shibuya et al. (2012) and Goto et al. (2021). Assuming
that the NB1010 flux is solely due to Ly$\alpha$ emission, our results roughly
correspond to the cumulative number density of $z=7.3$ LAEs with $\log
L_{\mathrm{Ly\alpha}}\gtrsim 43.1$ of $<1.1\times 10^{-6}~{}\mathrm{Mpc^{-3}}$
(zero detection case) and $1.6-4.8\times 10^{-6}~{}\mathrm{Mpc^{-3}}$ (five
detection case; see Figure 6 of Goto et al., 2021).

###  3.3 Matching with Spectroscopic Catalogs

To further ensure the validity of our catalog, we cross-match our LAEs with
galaxies and AGNs in publically available spectroscopic catalogs (Ouchi et
al., 2008; Saito et al., 2008; Lilly et al., 2009; Ouchi et al., 2010; Willott
et al., 2010; Coil et al., 2011; Mallery et al., 2012; Masters et al., 2012;
Newman et al., 2013; Le Fèvre et al., 2013; McGreer et al., 2013; Willott et
al., 2013; Shibuya et al., 2014; Kriek et al., 2015; Liske et al., 2015;
Sobral et al., 2015; Bañados et al., 2016; Hu et al., 2016; Momcheva et al.,
2016; Toshikawa et al., 2016; Wang et al., 2016; Hu et al., 2017; Jiang et
al., 2017; Masters et al., 2017; Suzuki et al., 2017; Tasca et al., 2017; Yang
et al., 2017; Harikane et al., 2018b; Hasinger et al., 2018; Jiang et al.,
2018; Lee et al., 2018; Pentericci et al., 2018; Scodeggio et al., 2018;
Shibuya et al., 2018a; Sobral et al., 2018; Calvi et al., 2019; Harikane et
al., 2019; Higuchi et al., 2019; Kashino et al., 2019; Masters et al., 2019;
Lyke et al., 2020; Onodera et al., 2020; Zhang et al., 2020; Ono et al., 2021)
and our past spectroscopic observations with Magellan/IMACS (Ono et al., 2018;
Harikane et al., 2019, PI: M. Ouchi; Ouchi et al. in preparation;), using a
matching radius of 1.0″. In our photometric catalogs of LAEs, we identify 50,
8, 13, 136, 33, and 1 spectroscopically confirmed LAEs at $z=2.2$, 3.3, 4.9,
5.6, 6.6, and 7.0, respectively. The properties of these sources, including
their spectroscopic redshifts, are listed in Table 4 in Appendix B. Figure 9
shows the redshift distributions of the spectroscopically identified sources,
along with filter transmission curves displayed with thick colored curves. The
peaks of the distributions show slight offsets toward the lower redshift side
compared to the filter transmission curves. This well-known behavior is caused
by the asymmetric Ly$\alpha$ line profile and Lyman break, which lead the
Ly$\alpha$ red wing and UV continuum redward of the Lyman break of LAEs at
lower redshifts to contribute more to the NB flux (Ouchi et al., 2008;
Kashikawa et al., 2011). We also show the slightly shifted transmission
curves, as in Ono et al. (2021), with thin colored curves that better match
the redshift distributions. The amounts of the shifts are
$-0.01,-0.02,-0.03,-0.02$, and $-0.01$ for the NB387, NB527, NB718, NB816, and
NB921 filters, respectively. This reasonable agreement between the redshift
distributions and the transmission curves further assures the reliability of
our selection.

We also found 53 low-redshift objects in the NB387 and NB527 samples, whose
properties are listed in Table 5 in Appendix B. Most of these objects are
CIV$\lambda$1549Å emitters at $z\sim 1.5$ and 2.4, as well as
CIII]$\lambda$1909Å emitters at $z\sim 1.0$. This type of contamination is
expected because our photometry in bands bluer than NB387 and NB527, and
therefore the Lyman break of the $z=2.2$ and 3.3 sample, is not strongly
constrained. These high-ionization line emitters that meet our criteria
typically have relatively high EWs ($\gtrsim 30$Å) and are thus considered to
be AGNs (Nakajima et al., 2018). In fact, most of the contaminants come from
the SDSS DR16 quasar catalog Lyke et al. (2020) or have broad line features.
The intrinsic number density of such sources should be much smaller than that
of the target LAEs, and the survey volume for lower-redshift line emitters is
smaller than that for LAEs at $z=2.2$ and 3.3 due to cosmological redshift.
Contamination from [OII] emitters at $z=0.03$ is expected to be negligible for
the same reason ($\sim 0.2$% of the volume for LAEs). The contamination rate
for $z=5.7$ and $z=6.6$ LAEs are estimated to be 14% and 8%, respectively, in
Shibuya et al. (2018b) based on spectroscopic follow-up observations of LAEs
selected with almost the same selection criteria as ours. However, all the
five bright contaminants reported in Shibuya et al. (2018b) are successfully
rejected in our catalog thanks to the deeper BB images, which provide strong
constraints on their photometry below the Lyman break. Our LAEs at $z=5.7$ and
6.6 should have a much lower level of contamination, which would be acceptable
for various statistical studies. This will be directly assessed in future
massive spectroscopic follow-up observations in the planned PFS-SSP survey
(e.g., Greene et al., 2022).

Figure 9:  Redshift distribution of spectroscopically confirmed LAEs in our
catalogs. Thick colored curves show the normalized transmission curves of HSC
NB filters (Figure 1) with wavelength converted to Ly$\alpha$ redshift, while
thin colored curves show the shifted ones.

###  3.4 Data Release and Example Science Cases

Our LAE catalogs will be available online via
http://cos.icrr.u-tokyo.ac.jp/rush.html after the next HSC-SSP official data
release (Public Data Release 4). These LAE catalogs include the basic
photometric properties with the coordinates together with ancillary
information such as the limiting magnitude maps and the masks used in Section
2.3. Using these LAE catalogs, we will constrain the statistical properties of
LAEs at various redshifts such as Ly$\alpha$ luminosity functions, clustering
properties, and Ly$\alpha$ equivalent width distributions (Konno et al. 2018;
Ouchi et al. 2018; Shibuya et al. 2018a, Umeda et al, in preparation) with
unprecedentedly small statistical uncertainties. Ionized bubble size in the
epoch of reionization will be, for the first time, constrained with enough
sensitivity by cross-correlating the spatial distribution of LAEs
spectroscopic follow-up observations conducted with the coming PSF-SSP survey
and HI 21-cm emission observations obtained with Square Kilometer Array
(Kubota et al., 2018, 2020). Deep imaging data of HSC-SSP and CHORUS can also
be used to constrain diffuse nebula emission around LAEs and other galaxy
populations (e.g. Kikuchihara et al., 2020; Kikuta et al., 2019, 2023).

##  4 Summary

We construct massive Ly$\alpha$ emitter (LAE) catalogs at various redshifts
using the latest deep images from the completed HSC-SSP survey (Aihara et al.,
2022) and the CHORUS survey (Inoue et al., 2020). The unique narrow-band
filter sets of HSC allow us to probe LAEs at $z=2.2$, 3.3, 4.9, 5.7, 6.6, 7.0,
and 7.3. CHORUS NB387 data are combined to fill the unobserved region at
COSMOS in HSC-SSP NB387 images. After properly accounting for the spatial
variation of limiting magnitudes, we initially select 699,219 photometric LAE
candidates. Careful screening via masking of problematic regions and visual
inspection of coadded and multi-epoch images yields a total of 20,567 LAEs,
consisting of 6,995, 4,641, 726, 6,124, 2,058, 18, and 5 LAEs at $z=2.2$, 3.3,
4.9, 5.7, 6.6, 7.0, and 7.3, respectively, although the $z=7.3$ candidates are
tentative (Section 3.2). The LAE number counts agree well with those from
previous studies once the difference in selection and depth are taken into
account (Section 3.1), and our catalogs include 241 spectroscopically
confirmed LAEs (Section 3.3), and validating our selection processes. Our new
catalogs will be made public on our project website (Section 3.4).

We thank Ryohei Itoh for sharing his data and Ken Mawatari for his help with
data analyses. This work is supported by World Premier International Research
Center Initiative (WPI Initiative), MEXT, Japan, as well as the joint research
program of the Institute of Cosmic Ray Research (ICRR), the University of
Tokyo. This study is supported by KAKENHI (19H00697, 20H00180, and 21H04467)
Grant-in-Aid for Scientific Research (A) through the Japan Society for the
Promotion of Science. The Hyper Suprime-Cam (HSC) collaboration includes the
astronomical communities of Japan and Taiwan, and Princeton University. The
HSC instrumentation and software were developed by the National Astronomical
Observatory of Japan (NAOJ), the Kavli Institute for the Physics and
Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High
Energy Accelerator Research Organization (KEK), the Academia Sinica Institute
for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University.
Funding was contributed by the FIRST program from the Japanese Cabinet Office,
the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the
Japan Society for the Promotion of Science (JSPS), Japan Science and
Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK,
ASIAA, and Princeton University. This work is based on data collected at the
Subaru Telescope and retrieved from the HSC data archive system, which is
operated by Subaru Telescope and Astronomy Data Center (ADC) at NAOJ. Data
analysis was in part carried out with the cooperation of Center for
Computational Astrophysics (CfCA) at NAOJ. We are honored and grateful for the
opportunity of observing the Universe from Maunakea, which has the cultural,
historical and natural significance in Hawaii. This paper makes use of
software developed for Vera C. Rubin Observatory. We thank the Rubin
Observatory for making their code available as free software at
http://pipelines.lsst.io/.

##  Appendix A Limiting Magnitude maps for Narrowband and Broadband Filters

Figures 10 – 19 show 5$\sigma$ limiting magnitude maps for the HSC filters we
used in this work. The maps over the whole survey fields are shown for each
tract, whose number is indicated at the bottom left. In each panel, $9\times
9$ squares represent patches belonging to the tract. Aside from the D/UD
distinction in COSMOS and SXDS, there are some variations that should be
accounted for when LAEs are selected.

Figure 10: Limiting magnitude maps ($5\sigma$, 2$.\\!\\!\arcsec$0 aperture)
for the NB387 images. Figure 11: Limiting magnitude maps ($5\sigma$,
2$.\\!\\!\arcsec$0 aperture) for the NB816 images. Figure 12: Limiting
magnitude maps ($5\sigma$, 2$.\\!\\!\arcsec$0 aperture) for the NB921 images.
Figure 13: Limiting magnitude maps ($5\sigma$, 2$.\\!\\!\arcsec$0 aperture)
for the NB1010 images. Figure 14: Limiting magnitude maps ($5\sigma$,
2$.\\!\\!\arcsec$0 aperture) for the CHORUS NBs (Left: NB527, Middle: NB718,
Right: NB973). Figure 15: Limiting magnitude maps ($5\sigma$,
2$.\\!\\!\arcsec$0 aperture) for the g band. Figure 16: Limiting magnitude
maps ($5\sigma$, 2$.\\!\\!\arcsec$0 aperture) for the r band. Figure 17:
Limiting magnitude maps ($5\sigma$, 2$.\\!\\!\arcsec$0 aperture) for the i
band. Figure 18: Limiting magnitude maps ($5\sigma$, 2$.\\!\\!\arcsec$0
aperture) for the z band. Figure 19: Limiting magnitude maps ($5\sigma$,
2$.\\!\\!\arcsec$0 aperture) for the y band.

##  Appendix B List of Spectroscopically confirmed objects in our catalogs

In Table 4, we list information (name, sky coordinates, spectroscopic redshift
from each reference in the last column, photometric information (grizy and NB,
2$.\\!\\!\arcsec$0-aperture magnitudes) in our images, LAE sample in which the
source is included, notable features (if any), and reference) on our LAEs
confirmed by past spectroscopic observations. We also list information on
sources identified as lower redshift objects in spectroscopic catalogs in
Table 5.

Table 4: List of Objects with Spectroscopic Confirmation in Our LAE Catalogs

ID | R.A. | Decl. | $z_{\mathrm{spec}}$ | $\mathrm{g_{ap}}$ | $\mathrm{r_{ap}}$ | $\mathrm{i_{ap}}$ | $\mathrm{z_{ap}}$ | $\mathrm{y_{ap}}$ | $\mathrm{NB_{ap}}$ | Sample | Feature | Reference
---|---|---|---|---|---|---|---|---|---|---|---|---
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13)
HSC J022013–050729 | 02:20:13.03 | –05:07:29.7 | 2.169 | 22.7 | 22.7 | 22.6 | 22.3 | 22.4 | 21.7 | NB0387 | AGN | Co11
HSC J022028–045802 | 02:20:28.96 | –04:58:02.8 | 2.157 | 20.4 | 20.5 | 20.3 | 20.0 | 20.1 | 19.1 | NB0387 | AGN | Co11, Ly20
HSC J022044–050906 | 02:20:44.46 | –05:09:06.1 | 2.105 | 20.8 | 20.8 | 20.8 | 20.5 | 20.6 | 20.0 | NB0387 | AGN | Li15, Sc18, Ly20
HSC J022120–032353 | 02:21:20.93 | –03:23:53.5 | 2.183 | 22.6 | 22.5 | 22.4 | 22.2 | 22.3 | 21.2 | NB0387 | AGN | Ly20
HSC J022121–034338 | 02:21:21.16 | –03:43:38.1 | 2.176 | 23.1 | 23.2 | 23.0 | 22.7 | 22.7 | 21.9 | NB0387 | AGN | Ly20
HSC J022202–050352 | 02:22:02.59 | –05:03:52.0 | 2.161 | 21.6 | 21.6 | 21.6 | 21.3 | 21.5 | 20.4 | NB0387 | AGN | Ly20
HSC J022219–052231 | 02:22:19.96 | –05:22:31.5 | 2.204 | 20.4 | 20.3 | 20.3 | 20.0 | 20.1 | 19.3 | NB0387 | AGN | Li15, Ly20
HSC J022230–033545 | 02:22:30.42 | –03:35:45.4 | 2.172 | 22.1 | 22.4 | 22.1 | 21.7 | 21.9 | 20.0 | NB0387 | AGN | Ly20
HSC J022312–050625 | 02:23:12.46 | –05:06:25.1 | 2.190 | 20.1 | 20.1 | 20.1 | 19.9 | 19.9 | 19.1 | NB0387 | AGN | Ly20
HSC J022349–033930 | 02:23:49.43 | –03:39:30.6 | 2.141 | 20.9 | 20.8 | 20.8 | 20.5 | 20.7 | 20.0 | NB0387 | AGN | Ly20
HSC J022351–044730 | 02:23:51.07 | –04:47:30.0 | 2.167 | 20.7 | 20.6 | 20.6 | 20.3 | 20.4 | 19.6 | NB0387 | AGN | Ly20
HSC J022435–053615 | 02:24:35.54 | –05:36:15.6 | 2.217 | 22.0 | 22.0 | 21.9 | 21.6 | 21.7 | 21.1 | NB0387 | AGN | Li15, Ly20
HSC J022548–041028 | 02:25:48.98 | –04:10:28.4 | 2.124 | 23.8 | 23.7 | 23.5 | 23.1 | 23.1 | 22.5 | NB0387 |  | Li15
HSC J022722–045221 | 02:27:22.20 | –04:52:21.9 | 2.127 | 21.6 | 21.7 | 21.6 | 21.3 | 21.5 | 20.7 | NB0387 | AGN | Ly20
HSC J022751–050101 | 02:27:51.25 | –05:01:01.3 | 2.175 | 21.6 | 21.9 | 21.8 | 21.3 | 21.5 | 20.6 | NB0387 | AGN | Li15, Ly20
HSC J095508+011205 | 09:55:08.45 | +01:12:05.7 | 2.166 | 21.8 | 21.9 | 21.6 | 21.3 | 21.5 | 19.9 | NB0387 | AGN | Ly20
HSC J095539+011316 | 09:55:39.50 | +01:13:16.4 | 2.142 | 21.6 | 21.6 | 21.6 | 21.1 | 21.4 | 20.5 | NB0387 | AGN | Ly20
HSC J095714+013145 | 09:57:14.02 | +01:31:45.5 | 2.142 | 21.7 | 21.6 | 21.4 | 21.0 | 21.1 | 20.1 | NB0387 | AGN | Ly20
HSC J095822+010806 | 09:58:22.03 | +01:08:06.4 | 2.171 | 20.7 | 20.6 | 20.6 | 20.3 | 20.4 | 19.4 | NB0387 | AGN | Ly20
HSC J095944+020742 | 09:59:44.25 | +02:07:42.7 | 2.191 | 24.8 | 24.8 | 24.9 | 24.8 | 24.9 | 23.6 | NB0387 |  | Sh14
HSC J095945+022808 | 09:59:45.98 | +02:28:08.0 | 2.174 | 24.9 | 24.8 | 24.8 | 24.7 | 24.9 | 23.7 | NB0387 |  | Sh14
HSC J095954+022630 | 09:59:54.39 | +02:26:30.0 | 2.194 | 24.9 | 24.6 | 24.3 | 23.9 | 23.7 | 23.3 | NB0387 |  | Sh14
HSC J095950+020347 | 09:59:50.74 | +02:03:47.7 | 2.184 | 24.5 | 24.5 | 24.5 | 24.4 | 24.4 | 23.2 | NB0387 |  | Has18
HSC J095959+020531 | 09:59:59.06 | +02:05:31.6 | 2.182 | 25.7 | 25.6 | 25.6 | 25.6 | 25.8 | 24.6 | NB0387 |  | Sh14
HSC J095959+020838 | 09:59:59.38 | +02:08:38.4 | 2.163 | 24.5 | 24.5 | 24.5 | 24.5 | 24.5 | 22.9 | NB0387 |  | Sh14
HSC J100012+021750 | 10:00:12.56 | +02:17:50.4 | 2.161 | 24.4 | 24.3 | 24.3 | 24.3 | 24.4 | 23.3 | NB0387 |  | Kr15
HSC J100015+020807 | 10:00:15.26 | +02:08:07.4 | 2.161 | 24.7 | 24.6 | 24.6 | 24.6 | 24.6 | 23.8 | NB0387 |  | Sh14
HSC J100017+030525 | 10:00:17.73 | +03:05:25.0 | 2.174 | 20.7 | 20.9 | 20.4 | 20.1 | 20.4 | 18.8 | NB0387 | AGN | Ly20
HSC J100025+022357 | 10:00:25.98 | +02:23:57.4 | 2.169 | 23.9 | 23.8 | 23.7 | 23.6 | 23.4 | 23.1 | NB0387 |  | Mo16
HSC J100032+021535 | 10:00:32.66 | +02:15:35.6 | 2.157 | 26.5 | 26.2 | 26.2 | 26.2 | 26.5 | 25.5 | NB0387 |  | Kr15, Mo16
HSC J100047+020757 | 10:00:47.75 | +02:07:57.0 | 2.153 | 19.9 | 19.8 | 19.7 | 19.4 | 19.5 | 18.8 | NB0387 | AGN | Li09, Ly20
HSC J100102+011948 | 10:01:02.16 | +01:19:48.6 | 2.146 | 19.7 | 19.7 | 19.6 | 19.4 | 19.6 | 18.8 | NB0387 | AGN | Ly20
HSC J100146+033040 | 10:01:46.03 | +03:30:40.1 | 2.212 | 22.4 | 22.5 | 22.2 | 21.7 | 22.2 | 21.2 | NB0387 | AGN | Ly20
HSC J160328+545715 | 16:03:28.75 | +54:57:15.0 | 2.142 | 21.2 | 21.3 | 21.1 | 20.9 | 21.0 | 20.2 | NB0387 | AGN | Ly20
HSC J160554+544859 | 16:05:54.66 | +54:48:59.5 | 2.159 | 21.4 | 21.6 | 21.5 | 21.2 | 21.4 | 20.0 | NB0387 | AGN | Ly20
HSC J160611+542447 | 16:06:11.62 | +54:24:47.5 | 2.198 | 20.4 | 20.5 | 20.4 | 20.1 | 20.3 | 19.5 | NB0387 | AGN | Ly20
HSC J161105+532237 | 16:11:05.06 | +53:22:37.9 | 2.182 | 21.6 | 21.8 | 21.6 | 21.2 | 21.5 | 20.1 | NB0387 | AGN | Ly20
HSC J161129+545055 | 16:11:29.04 | +54:50:55.5 | 2.108 | 20.4 | 20.4 | 20.3 | 20.1 | 20.2 | 19.6 | NB0387 | AGN | Ly20
HSC J161327+541256 | 16:13:27.44 | +54:12:56.2 | 2.155 | 21.3 | 21.3 | 21.1 | 20.8 | 20.9 | 20.0 | NB0387 | AGN | Ly20
HSC J161432+543903 | 16:14:32.77 | +54:39:03.7 | 2.193 | 21.6 | 21.7 | 21.5 | 21.2 | 21.4 | 20.1 | NB0387 | AGN | Ly20
HSC J161552+553101 | 16:15:52.16 | +55:31:01.9 | 2.160 | 21.2 | 21.5 | 21.3 | 21.1 | 21.2 | 20.0 | NB0387 | AGN | Ly20
HSC J232147–010038 | 23:21:47.17 | –01:00:38.9 | 2.177 | 21.3 | 21.2 | 21.0 | 20.7 | 20.7 | 20.1 | NB0387 | AGN | Ly20
HSC J232459+001451 | 23:24:59.70 | +00:14:51.2 | 2.172 | 21.3 | 21.2 | 21.1 | 20.8 | 20.9 | 19.6 | NB0387 | AGN | Ly20
HSC J232506–012203 | 23:25:06.73 | –01:22:03.4 | 2.181 | 20.3 | 20.3 | 20.3 | 20.1 | 20.2 | 19.3 | NB0387 | AGN | Ly20
HSC J232608–011540 | 23:26:08.69 | –01:15:40.3 | 2.194 | 22.7 | 22.6 | 22.3 | 21.8 | 21.9 | 21.1 | NB0387 | AGN | Ly20
HSC J232614+003249 | 23:26:14.28 | +00:32:49.2 | 2.180 | 20.8 | 20.5 | 20.4 | 20.2 | 20.2 | 19.6 | NB0387 | AGN | Ly20
HSC J232619+000152 | 23:26:19.36 | +00:01:52.7 | 2.173 | 22.1 | 22.1 | 21.9 | 21.5 | 21.7 | 21.0 | NB0387 | AGN | Ly20
HSC J232649–000010 | 23:26:49.36 | –00:00:10.1 | 2.168 | 22.7 | 22.6 | 22.3 | 21.7 | 21.9 | 21.1 | NB0387 | AGN | Ly20
HSC J232855–004212 | 23:28:55.78 | –00:42:12.2 | 2.198 | 20.5 | 20.4 | 20.1 | 19.8 | 19.9 | 19.0 | NB0387 | AGN | Ly20
HSC J233159+000856 | 23:31:59.69 | +00:08:56.5 | 2.184 | 20.9 | 20.7 | 20.7 | 20.3 | 20.4 | 19.5 | NB0387 | AGN | Co11, Ly20
HSC J095759+015804 | 09:57:59.01 | +01:58:04.7 | 3.261 | 23.7 | 23.3 | 23.5 | 23.5 | 23.4 | 22.6 | NB0527 | AGN | Has18
HSC J095940+025255 | 09:59:40.18 | +02:52:55.4 | 3.317 | 23.9 | 23.6 | 23.5 | 23.4 | 23.4 | 22.5 | NB0527 | AGN | Has18
HSC J100013+013704 | 10:00:13.54 | +01:37:04.6 | 3.489 | 27.0 | 26.8 | 26.2 | 26.0 | 26.1 | 24.5 | NB0527 |  | Has18
HSC J100017+021657 | 10:00:17.38 | +02:16:57.5 | 3.295 | 25.6 | 25.1 | 24.8 | 24.7 | 24.5 | 23.9 | NB0527 |  | Ta17
HSC J100033+021825 | 10:00:33.33 | +02:18:25.3 | 3.288 | 25.2 | 24.8 | 24.6 | 24.6 | 24.6 | 24.1 | NB0527 |  | Ta17
HSC J100057+023932 | 10:00:57.80 | +02:39:32.6 | 3.360 | 23.5 | 22.9 | 22.8 | 22.8 | 22.8 | 22.3 | NB0527 | AGN | Co11, Mas12
HSC J100113+014541 | 10:01:13.46 | +01:45:41.8 | 3.310 | 25.9 | 25.4 | 25.2 | 25.0 | 25.0 | 24.0 | NB0527 |  | Has18
HSC J100220+020453 | 10:02:20.39 | +02:04:53.0 | 3.326 | 24.3 | 24.1 | 23.8 | 23.6 | 23.3 | 22.3 | NB0527 | AGN | Co11, Has18
HSC J095820+021658 | 09:58:20.94 | +02:16:58.5 | 4.909 | 28.7 | 27.5 | 25.5 | 25.3 | 25.8 | 24.0 | NB0718 | AGN | Ma12, Has18
HSC J095830+020631 | 09:58:30.61 | +02:06:31.2 | 4.891 | 99.0 | 27.3 | 25.0 | 24.9 | 25.0 | 24.1 | NB0718 |  | Ma12, Has18
HSC J095929+022950 | 09:59:29.35 | +02:29:50.2 | 4.841 | 99.0 | 27.9 | 25.7 | 26.0 | 26.0 | 24.9 | NB0718 |  | Ma12, Has18
HSC J095950+022451 | 09:59:50.03 | +02:24:51.5 | 4.843 | 99.0 | 28.5 | 26.6 | 27.4 | 28.6 | 25.9 | NB0718 |  | Ma12, Has18
HSC J095956+015451 | 09:59:56.14 | +01:54:51.5 | 4.844 | 99.0 | 29.4 | 26.5 | 27.4 | 28.0 | 25.6 | NB0718 |  | Ma12, Has18
HSC J100004+020845 | 10:00:04.17 | +02:08:45.6 | 4.840 | 99.0 | 26.6 | 25.0 | 25.2 | 25.2 | 24.2 | NB0718 |  | Ma12, Has18
HSC J100008+023456 | 10:00:08.76 | +02:34:56.5 | 4.868 | 99.0 | 28.2 | 26.7 | 26.8 | 26.4 | 25.7 | NB0718 |  | Has18
HSC J100030+013621 | 10:00:30.43 | +01:36:21.7 | 4.844 | 29.2 | 27.5 | 25.7 | 26.0 | 25.9 | 25.0 | NB0718 |  | Ma12, Has18
HSC J100041+022637 | 10:00:41.08 | +02:26:37.4 | 4.869 | 99.0 | 27.5 | 25.6 | 25.8 | 25.9 | 24.5 | NB0718 |  | Ma12, Has18
HSC J100055+021309 | 10:00:55.43 | +02:13:09.1 | 4.873 | 99.0 | 28.6 | 26.1 | 26.3 | 27.3 | 24.1 | NB0718 |  | Ma12, Has18
HSC J100122+022249 | 10:01:22.45 | +02:22:49.8 | 4.865 | 29.4 | 28.5 | 26.4 | 26.5 | 26.3 | 24.9 | NB0718 |  | Ma12, Has18
HSC J100145+015712 | 10:01:45.12 | +01:57:12.2 | 4.910 | 99.0 | 26.6 | 25.1 | 25.0 | 24.9 | 24.4 | NB0718 |  | Ma12, Has18
HSC J100145+020244 | 10:01:45.96 | +02:02:44.3 | 4.888 | 30.0 | 25.8 | 24.1 | 24.1 | 24.1 | 23.0 | NB0718 | LAB | Zh20
HSC J021525–045918 | 02:15:25.25 | –04:59:18.2 | 5.674 | 99.0 | 99.0 | 26.6 | 25.8 | 25.7 | 24.8 | NB0816 |  | Ji17
HSC J021526–045229 | 02:15:26.23 | –04:52:29.9 | 5.655 | 99.0 | 99.0 | 26.1 | 25.2 | 25.0 | 24.7 | NB0816 |  | On21
HSC J021533–050137 | 02:15:33.25 | –05:01:37.3 | 5.671 | 29.5 | 28.2 | 26.4 | 25.4 | 25.3 | 24.7 | NB0816 |  | On21
HSC J021551–045325 | 02:15:51.35 | –04:53:25.5 | 5.710 | 99.0 | 99.0 | 27.8 | 26.9 | 27.2 | 25.3 | NB0816 |  | On21
HSC J021553–051000 | 02:15:53.98 | –05:10:00.4 | 5.732 | 99.0 | 29.0 | 99.0 | 28.7 | 29.0 | 25.7 | NB0816 |  | This Study
HSC J021555–045318 | 02:15:55.66 | –04:53:18.9 | 5.738 | 99.0 | 28.8 | 27.2 | 27.6 | 27.3 | 25.3 | NB0816 |  | On21
HSC J021558–045301 | 02:15:58.50 | –04:53:01.9 | 5.718 | 99.0 | 99.0 | 27.2 | 27.6 | 27.8 | 25.0 | NB0816 |  | On21
HSC J021609–045651 | 02:16:09.47 | –04:56:51.3 | 5.691 | 99.0 | 99.0 | 28.4 | 99.0 | 99.0 | 25.8 | NB0816 |  | This Study
HSC J021617–045419 | 02:16:17.16 | –04:54:19.4 | 5.707 | 99.0 | 99.0 | 28.5 | 29.1 | 27.6 | 25.6 | NB0816 |  | On21
HSC J021624–045516 | 02:16:24.71 | –04:55:16.7 | 5.707 | 99.0 | 99.0 | 26.4 | 25.9 | 25.8 | 23.9 | NB0816 |  | Ji17
HSC J021625–045237 | 02:16:25.65 | –04:52:37.3 | 5.730 | 99.0 | 99.0 | 28.2 | 28.9 | 27.1 | 25.1 | NB0816 |  | On21
HSC J021628–050103 | 02:16:28.06 | –05:01:03.8 | 5.692 | 99.0 | 29.2 | 27.5 | 28.2 | 99.0 | 25.1 | NB0816 |  | On21
HSC J021630–045734 | 02:16:30.40 | –04:57:34.4 | 5.700 | 29.8 | 29.0 | 28.0 | 99.0 | 28.3 | 25.9 | NB0816 |  | This Study
HSC J021636–044723 | 02:16:36.45 | –04:47:23.7 | 5.718 | 99.0 | 29.9 | 27.2 | 26.5 | 26.7 | 25.2 | NB0816 |  | On21
HSC J021654–052155 | 02:16:54.61 | –05:21:55.7 | 5.715 | 29.0 | 28.7 | 26.8 | 26.9 | 26.7 | 24.7 | NB0816 |  | Ji18, Ha19
HSC J021657–052117 | 02:16:57.89 | –05:21:17.3 | 5.669 | 99.0 | 99.0 | 26.7 | 26.4 | 27.2 | 25.3 | NB0816 |  | Ji17, Ji18, Ha19
HSC J021659–052305 | 02:16:59.95 | –05:23:05.4 | 5.700 | 29.0 | 99.0 | 28.1 | 27.9 | 27.1 | 25.7 | NB0816 |  | Ha19
HSC J021700–051810 | 02:17:00.80 | –05:18:10.5 | 5.713 | 99.0 | 99.0 | 28.0 | 27.9 | 99.0 | 25.6 | NB0816 |  | Ji18
HSC J021700–053130 | 02:17:00.62 | –05:31:30.5 | 5.754 | 99.0 | 29.6 | 27.0 | 26.9 | 26.5 | 25.2 | NB0816 |  | Ji18
HSC J021701–051841 | 02:17:01.44 | –05:18:41.6 | 5.679 | 99.0 | 99.0 | 28.0 | 27.1 | 27.6 | 25.7 | NB0816 |  | Ha19
HSC J021704–052714 | 02:17:04.30 | –05:27:14.4 | 5.687 | 99.0 | 28.4 | 26.5 | 26.6 | 26.1 | 24.4 | NB0816 |  | Ji17, Ji18, Ha19
HSC J021707–052723 | 02:17:07.98 | –05:27:23.4 | 5.720 | 99.0 | 99.0 | 27.4 | 28.7 | 99.0 | 26.1 | NB0816 |  | Ha19
HSC J021707–053426 | 02:17:07.86 | –05:34:26.7 | 5.680 | 99.0 | 99.0 | 26.5 | 26.3 | 26.4 | 24.4 | NB0816 |  | Ji17, Ji18, Ha19
HSC J021708–052421 | 02:17:08.87 | –05:24:21.7 | 5.675 | 29.3 | 28.5 | 27.2 | 26.9 | 27.4 | 25.7 | NB0816 |  | Ji18
HSC J021709–050329 | 02:17:09.78 | –05:03:29.3 | 5.709 | 99.0 | 29.3 | 27.1 | 26.7 | 28.9 | 25.0 | NB0816 |  | On21
HSC J021709–052646 | 02:17:09.96 | –05:26:46.7 | 5.689 | 99.0 | 99.0 | 27.8 | 27.0 | 27.5 | 25.4 | NB0816 |  | Ha19
HSC J021709–052731 | 02:17:09.52 | –05:27:31.5 | 5.676 | 99.0 | 29.6 | 27.8 | 99.0 | 28.3 | 25.7 | NB0816 |  | Ji18, Ha19
HSC J021710–044351 | 02:17:10.47 | –04:43:51.6 | 5.691 | 99.0 | 28.0 | 27.4 | 28.6 | 27.4 | 25.9 | NB0816 |  | This Study
HSC J021713–053558 | 02:17:13.80 | –05:35:58.0 | 5.686 | 28.7 | 99.0 | 27.4 | 26.0 | 26.0 | 25.2 | NB0816 |  | Ha19
HSC J021714–053502 | 02:17:14.93 | –05:35:02.9 | 5.685 | 99.0 | 29.9 | 27.7 | 26.3 | 29.7 | 25.5 | NB0816 |  | Ha19
HSC J021719–043150 | 02:17:19.14 | –04:31:50.7 | 5.735 | 99.0 | 99.0 | 27.5 | 26.8 | 27.2 | 25.0 | NB0816 |  | On21
HSC J021722–052805 | 02:17:22.28 | –05:28:05.4 | 5.682 | 99.0 | 99.0 | 27.6 | 27.6 | 27.0 | 25.7 | NB0816 |  | Ji18, Ha19
HSC J021723–052559 | 02:17:23.53 | –05:25:59.9 | 5.707 | 99.0 | 99.0 | 28.9 | 29.1 | 27.6 | 25.8 | NB0816 |  | This Study
HSC J021724–053309 | 02:17:24.04 | –05:33:09.8 | 5.708 | 29.0 | 28.2 | 25.8 | 25.5 | 25.8 | 23.6 | NB0816 |  | Ji17, Ji18, Sh18, Ha19
HSC J021725–050737 | 02:17:25.90 | –05:07:37.7 | 5.701 | 99.0 | 99.0 | 27.7 | 27.0 | 26.7 | 24.8 | NB0816 |  | On21
HSC J021726–045126 | 02:17:26.74 | –04:51:26.8 | 5.709 | 99.0 | 99.0 | 27.6 | 99.0 | 28.3 | 25.0 | NB0816 |  | On21
HSC J021729–053028 | 02:17:29.19 | –05:30:28.6 | 5.746 | 99.0 | 99.0 | 27.8 | 28.8 | 99.0 | 25.1 | NB0816 |  | Ha19
HSC J021734–053452 | 02:17:34.16 | –05:34:52.8 | 5.710 | 99.0 | 99.0 | 29.8 | 99.0 | 27.9 | 25.3 | NB0816 |  | Ji18, Ha19
HSC J021736–052701 | 02:17:36.38 | –05:27:01.7 | 5.674 | 99.0 | 29.4 | 26.8 | 26.4 | 26.5 | 25.3 | NB0816 |  | Ji17, Ji18, Ha19
HSC J021736–053027 | 02:17:36.68 | –05:30:27.6 | 5.686 | 99.0 | 99.0 | 27.9 | 27.2 | 99.0 | 25.7 | NB0816 |  | Ha19
HSC J021737–043943 | 02:17:37.97 | –04:39:43.1 | 5.755 | 29.2 | 99.0 | 27.0 | 26.5 | 26.1 | 24.7 | NB0816 |  | On21
HSC J021738–053048 | 02:17:38.29 | –05:30:48.8 | 5.687 | 99.0 | 29.0 | 28.8 | 27.9 | 27.8 | 25.9 | NB0816 |  | Ha19
HSC J021739–043837 | 02:17:39.26 | –04:38:37.4 | 5.721 | 99.0 | 99.0 | 27.9 | 27.6 | 99.0 | 24.8 | NB0816 |  | On21
HSC J021740–044544 | 02:17:40.60 | –04:45:44.2 | 5.704 | 99.0 | 99.0 | 99.0 | 99.0 | 99.0 | 26.0 | NB0816 |  | This Study
HSC J021741–044426 | 02:17:41.29 | –04:44:26.7 | 5.704 | 99.0 | 99.0 | 27.9 | 27.5 | 28.2 | 25.8 | NB0816 |  | This Study
HSC J021742–052810 | 02:17:42.18 | –05:28:10.6 | 5.679 | 28.8 | 28.5 | 27.0 | 26.3 | 26.0 | 25.5 | NB0816 |  | Ha19
HSC J021745–044129 | 02:17:45.74 | –04:41:29.3 | 5.674 | 29.3 | 99.0 | 26.8 | 27.5 | 26.6 | 25.1 | NB0816 |  | On21
HSC J021745–052936 | 02:17:45.26 | –05:29:36.2 | 5.688 | 29.4 | 99.0 | 26.7 | 26.2 | 26.6 | 24.6 | NB0816 |  | Ou08, Ji17, Ji18
HSC J021747–052252 | 02:17:47.42 | –05:22:52.0 | 5.722 | 99.0 | 99.0 | 28.8 | 28.1 | 99.0 | 25.7 | NB0816 |  | This Study
HSC J021748–043948 | 02:17:48.67 | –04:39:48.9 | 5.668 | 99.0 | 99.0 | 27.8 | 27.6 | 27.5 | 26.0 | NB0816 |  | This Study
HSC J021748–051550 | 02:17:48.77 | –05:15:50.0 | 5.681 | 99.0 | 99.0 | 27.2 | 26.8 | 99.0 | 25.9 | NB0816 |  | Ji18
HSC J021748–053127 | 02:17:48.47 | –05:31:27.1 | 5.690 | 99.0 | 29.9 | 26.9 | 26.3 | 26.7 | 24.6 | NB0816 |  | Ou08, Ji17, Ji18
HSC J021750–052708 | 02:17:50.00 | –05:27:08.2 | 5.693 | 99.0 | 99.0 | 27.3 | 26.8 | 26.2 | 25.0 | NB0816 |  | Ou08, Ji18
HSC J021751–053003 | 02:17:51.15 | –05:30:03.8 | 5.712 | 99.0 | 28.6 | 27.2 | 26.3 | 26.2 | 25.3 | NB0816 |  | Ou08, Ji18
HSC J021755–043251 | 02:17:55.40 | –04:32:51.6 | 5.690 | 28.9 | 28.6 | 27.3 | 26.7 | 27.1 | 24.9 | NB0816 |  | On21
HSC J021755–053027 | 02:17:55.84 | –05:30:27.1 | 5.694 | 99.0 | 99.0 | 27.9 | 27.1 | 99.0 | 25.7 | NB0816 |  | Ha19
HSC J021757–053309 | 02:17:57.67 | –05:33:09.5 | 5.749 | 29.8 | 99.0 | 27.0 | 26.5 | 26.9 | 24.9 | NB0816 |  | Ji18, Ha19
HSC J021758–043030 | 02:17:58.92 | –04:30:30.5 | 5.690 | 29.7 | 99.0 | 26.6 | 25.9 | 26.0 | 24.5 | NB0816 |  | Ji17
HSC J021759–042758 | 02:17:59.91 | –04:27:58.0 | 5.661 | 99.0 | 99.0 | 27.4 | 26.9 | 27.1 | 26.1 | NB0816 |  | This Study
HSC J021800–053519 | 02:18:00.73 | –05:35:19.2 | 5.673 | 99.0 | 99.0 | 26.6 | 25.3 | 25.3 | 25.0 | NB0816 |  | Ha19
HSC J021802–052011 | 02:18:02.19 | –05:20:11.6 | 5.715 | 99.0 | 99.0 | 28.1 | 27.6 | 28.2 | 25.4 | NB0816 |  | Ji18, Ha19
HSC J021803–044653 | 02:18:03.59 | –04:46:53.2 | 5.670 | 99.0 | 28.4 | 27.8 | 27.3 | 27.7 | 25.7 | NB0816 |  | This Study
HSC J021803–052643 | 02:18:03.89 | –05:26:43.5 | 5.747 | 99.0 | 29.2 | 27.2 | 26.9 | 27.0 | 24.8 | NB0816 |  | Ji18, Ha19
HSC J021804–052147 | 02:18:04.18 | –05:21:47.3 | 5.734 | 99.0 | 29.1 | 26.7 | 25.8 | 25.8 | 24.7 | NB0816 |  | Ji18, Ha19
HSC J021805–052027 | 02:18:05.29 | –05:20:27.1 | 5.742 | 99.0 | 99.0 | 27.9 | 27.0 | 27.4 | 25.0 | NB0816 |  | Ji18, Ha19
HSC J021805–052704 | 02:18:05.19 | –05:27:04.2 | 5.748 | 99.0 | 99.0 | 27.4 | 27.4 | 26.6 | 24.9 | NB0816 |  | Ji18, Ha19
HSC J021806–042847 | 02:18:06.16 | –04:28:47.7 | 5.726 | 28.9 | 29.4 | 27.3 | 27.0 | 27.0 | 25.4 | NB0816 |  | On21
HSC J021807–051526 | 02:18:07.70 | –05:15:26.8 | 5.750 | 99.0 | 99.0 | 26.8 | 26.5 | 26.8 | 25.0 | NB0816 |  | Ji18
HSC J021810–053708 | 02:18:10.68 | –05:37:08.0 | 5.749 | 99.0 | 28.9 | 26.9 | 26.5 | 26.2 | 24.4 | NB0816 |  | Ji18
HSC J021814–053249 | 02:18:14.40 | –05:32:49.2 | 5.673 | 99.0 | 29.1 | 26.6 | 26.0 | 25.5 | 25.2 | NB0816 |  | Ou08, Ji18
HSC J021819–050355 | 02:18:19.58 | –05:03:55.5 | 5.743 | 99.0 | 29.8 | 26.9 | 26.2 | 26.1 | 25.0 | NB0816 |  | On21
HSC J021822–042926 | 02:18:22.92 | –04:29:26.0 | 5.697 | 99.0 | 99.0 | 28.6 | 99.0 | 99.0 | 25.3 | NB0816 |  | On21
HSC J021823–044335 | 02:18:23.29 | –04:43:35.1 | 5.670 | 99.0 | 29.4 | 26.1 | 25.0 | 25.1 | 24.8 | NB0816 |  | Ji17
HSC J021823–053205 | 02:18:23.82 | –05:32:05.4 | 5.679 | 29.2 | 29.8 | 27.4 | 27.5 | 27.6 | 25.8 | NB0816 |  | Ou08, Ji18
HSC J021825–050700 | 02:18:25.43 | –05:07:00.6 | 5.683 | 29.3 | 99.0 | 29.3 | 27.5 | 99.0 | 25.6 | NB0816 |  | On21
HSC J021827–044737 | 02:18:27.45 | –04:47:37.1 | 5.703 | 99.0 | 99.0 | 26.4 | 26.4 | 26.5 | 23.9 | NB0816 |  | Ji17
HSC J021828–051423 | 02:18:28.89 | –05:14:23.1 | 5.737 | 99.0 | 99.0 | 26.7 | 26.6 | 26.2 | 24.2 | NB0816 |  | Ha19
HSC J021830–051457 | 02:18:30.54 | –05:14:57.8 | 5.688 | 99.0 | 29.7 | 26.3 | 26.6 | 26.8 | 23.9 | NB0816 |  | Ha19
HSC J021835–042321 | 02:18:35.95 | –04:23:21.7 | 5.755 | 99.0 | 99.0 | 25.6 | 25.3 | 25.6 | 23.4 | NB0816 |  | Sh18
HSC J021836–053528 | 02:18:36.38 | –05:35:28.1 | 5.698 | 29.1 | 29.2 | 26.3 | 25.7 | 25.3 | 23.9 | NB0816 |  | On21
HSC J021845–052915 | 02:18:45.03 | –05:29:15.9 | 5.660 | 99.0 | 29.6 | 26.5 | 26.0 | 25.8 | 25.2 | NB0816 |  | On21
HSC J021846–043722 | 02:18:46.66 | –04:37:22.4 | 5.735 | 99.0 | 29.5 | 27.6 | 27.3 | 26.8 | 25.0 | NB0816 |  | On21
HSC J021847–052725 | 02:18:47.77 | –05:27:25.0 | 5.662 | 99.0 | 99.0 | 27.7 | 27.0 | 26.8 | 25.8 | NB0816 |  | This Study
HSC J021848–051715 | 02:18:48.23 | –05:17:15.6 | 5.741 | 29.3 | 99.0 | 26.9 | 25.9 | 25.7 | 24.7 | NB0816 |  | On21
HSC J021848–052235 | 02:18:48.99 | –05:22:35.4 | 5.718 | 29.7 | 28.6 | 26.6 | 26.2 | 26.4 | 24.8 | NB0816 |  | On21
HSC J021850–053007 | 02:18:50.99 | –05:30:07.6 | 5.705 | 99.0 | 28.3 | 27.2 | 25.9 | 25.6 | 25.0 | NB0816 |  | On21
HSC J021855–044022 | 02:18:55.47 | –04:40:22.8 | 5.659 | 29.0 | 29.4 | 27.4 | 27.2 | 29.1 | 26.1 | NB0816 |  | This Study
HSC J021857–045648 | 02:18:57.33 | –04:56:48.9 | 5.681 | 29.7 | 99.0 | 28.2 | 27.1 | 99.0 | 25.4 | NB0816 |  | On21
HSC J021859–052916 | 02:18:59.93 | –05:29:16.8 | 5.674 | 29.1 | 27.8 | 25.6 | 24.8 | 24.7 | 24.3 | NB0816 |  | On21
HSC J021911–045707 | 02:19:11.04 | –04:57:07.6 | 5.704 | 99.0 | 99.0 | 27.7 | 28.7 | 28.6 | 25.2 | NB0816 |  | On21
HSC J021943–044914 | 02:19:43.91 | –04:49:14.4 | 5.684 | 99.0 | 99.0 | 27.9 | 27.2 | 26.8 | 25.4 | NB0816 |  | On21
HSC J022001–045839 | 02:20:01.06 | –04:58:39.7 | 5.682 | 99.0 | 99.0 | 27.1 | 27.2 | 27.1 | 25.5 | NB0816 |  | On21
HSC J022001–051637 | 02:20:01.11 | –05:16:37.4 | 5.711 | 29.7 | 29.2 | 26.1 | 25.7 | 25.8 | 23.6 | NB0816 |  | Sh18
HSC J022003–045416 | 02:20:03.20 | –04:54:16.6 | 5.697 | 99.0 | 29.5 | 26.3 | 25.3 | 25.2 | 24.6 | NB0816 |  | On21
HSC J022012–044950 | 02:20:12.14 | –04:49:50.9 | 5.681 | 99.0 | 99.0 | 27.0 | 26.7 | 28.6 | 25.3 | NB0816 |  | Ou08
HSC J022017–045046 | 02:20:17.68 | –04:50:46.7 | 5.675 | 99.0 | 99.0 | 27.9 | 27.6 | 99.0 | 26.1 | NB0816 |  | This Study
HSC J022021–045315 | 02:20:21.50 | –04:53:15.2 | 5.671 | 99.0 | 28.4 | 27.2 | 27.1 | 28.3 | 25.9 | NB0816 |  | Ou08
HSC J022026–045217 | 02:20:26.89 | –04:52:17.8 | 5.720 | 28.9 | 27.7 | 26.3 | 25.8 | 25.6 | 25.1 | NB0816 |  | On21
HSC J095919+020321 | 09:59:19.74 | +02:03:21.9 | 5.704 | 99.0 | 99.0 | 28.4 | 28.7 | 28.0 | 24.9 | NB0816 |  | Ma12, Has18
HSC J095922+021029 | 09:59:22.27 | +02:10:29.2 | 5.716 | 28.8 | 28.8 | 27.0 | 28.3 | 27.2 | 25.2 | NB0816 |  | On21
HSC J095944+020050 | 09:59:44.06 | +02:00:50.6 | 5.688 | 29.1 | 28.3 | 26.7 | 26.1 | 26.7 | 24.8 | NB0816 |  | Ma12, Has18
HSC J095946+013208 | 09:59:46.72 | +01:32:08.3 | 5.735 | 99.0 | 99.0 | 26.5 | 25.5 | 25.7 | 24.4 | NB0816 |  | Has18
HSC J095946+014352 | 09:59:46.14 | +01:43:52.8 | 5.717 | 99.0 | 28.4 | 26.9 | 26.7 | 26.6 | 25.1 | NB0816 |  | Ma12, Has18
HSC J095950+023223 | 09:59:50.99 | +02:32:23.1 | 5.666 | 28.9 | 28.4 | 26.8 | 26.5 | 27.1 | 25.5 | NB0816 |  | Ma12, Has18
HSC J095952+013723 | 09:59:52.13 | +01:37:23.2 | 5.724 | 99.0 | 29.8 | 26.5 | 26.0 | 26.0 | 24.2 | NB0816 |  | Ma12, Has18
HSC J095952+015005 | 09:59:52.03 | +01:50:05.7 | 5.744 | 99.0 | 29.1 | 26.3 | 25.4 | 25.3 | 24.5 | NB0816 |  | Ma12, Has18
HSC J095953+020705 | 09:59:53.25 | +02:07:05.3 | 5.692 | 28.8 | 28.2 | 25.7 | 24.6 | 24.5 | 24.0 | NB0816 |  | Ma12, Has18
HSC J095954+021039 | 09:59:54.78 | +02:10:39.2 | 5.662 | 99.0 | 29.9 | 26.8 | 26.6 | 26.4 | 25.0 | NB0816 |  | Ma12, Ji17, Has18
HSC J095954+021516 | 09:59:54.52 | +02:15:16.5 | 5.688 | 99.0 | 99.0 | 27.3 | 26.8 | 27.6 | 24.8 | NB0816 |  | Ma12, Has18
HSC J095955+014720 | 09:59:55.00 | +01:47:20.7 | 5.715 | 99.0 | 99.0 | 26.7 | 25.9 | 25.8 | 24.3 | NB0816 |  | Ma12, Has18
HSC J100005+020716 | 10:00:05.06 | +02:07:16.9 | 5.704 | 99.0 | 99.0 | 27.8 | 27.2 | 27.4 | 24.8 | NB0816 |  | Ma12, Has18
HSC J100019+020103 | 10:00:19.98 | +02:01:03.2 | 5.645 | 99.0 | 99.0 | 27.0 | 26.9 | 26.5 | 25.6 | NB0816 |  | Ma12, Has18
HSC J100029+015000 | 10:00:29.58 | +01:50:00.6 | 5.707 | 99.0 | 99.0 | 27.3 | 26.6 | 27.0 | 25.2 | NB0816 |  | Ma12, Has18
HSC J100029+024115 | 10:00:29.12 | +02:41:15.7 | 5.735 | 99.0 | 28.3 | 26.8 | 26.7 | 27.3 | 25.0 | NB0816 |  | Ma12, Has18
HSC J100030+021714 | 10:00:30.40 | +02:17:14.8 | 5.695 | 99.0 | 99.0 | 27.5 | 26.8 | 26.8 | 24.6 | NB0816 |  | Ma12, Has18
HSC J100040+021903 | 10:00:40.21 | +02:19:03.3 | 5.719 | 29.1 | 28.5 | 26.8 | 26.5 | 26.9 | 24.9 | NB0816 |  | Ma12, Ta17, Has18
HSC J100058+013642 | 10:00:58.41 | +01:36:42.8 | 5.688 | 99.0 | 28.2 | 27.1 | 27.6 | 26.3 | 25.2 | NB0816 |  | Ma12, Has18
HSC J100102+015144 | 10:01:02.95 | +01:51:44.7 | 5.666 | 29.7 | 28.1 | 26.6 | 26.1 | 26.1 | 25.2 | NB0816 |  | Ma12, Has18
HSC J100107+015222 | 10:01:07.35 | +01:52:22.7 | 5.668 | 99.0 | 99.0 | 27.4 | 27.0 | 28.5 | 25.6 | NB0816 |  | Ma12, Has18
HSC J100110+022829 | 10:01:10.06 | +02:28:29.1 | 5.681 | 29.6 | 27.8 | 26.1 | 25.0 | 25.0 | 24.5 | NB0816 |  | Ma12, Has18
HSC J100123+015600 | 10:01:23.84 | +01:56:00.3 | 5.726 | 99.0 | 99.0 | 26.5 | 25.9 | 26.0 | 24.0 | NB0816 |  | Ma12, Has18
HSC J100126+014430 | 10:01:26.89 | +01:44:30.1 | 5.686 | 99.0 | 99.0 | 26.7 | 26.2 | 26.0 | 24.6 | NB0816 |  | Ma12, Has18
HSC J100127+023005 | 10:01:27.76 | +02:30:05.9 | 5.696 | 29.5 | 29.1 | 26.6 | 25.9 | 26.1 | 24.6 | NB0816 |  | Ma12, Has18
HSC J100129+014929 | 10:01:29.08 | +01:49:29.8 | 5.707 | 99.0 | 99.0 | 26.1 | 25.6 | 25.5 | 23.8 | NB0816 |  | Ma12, Has18
HSC J100131+014320 | 10:01:31.12 | +01:43:20.3 | 5.728 | 28.9 | 28.1 | 26.7 | 26.4 | 26.4 | 24.8 | NB0816 |  | Ma12, Has18
HSC J100131+023105 | 10:01:31.07 | +02:31:05.9 | 5.690 | 29.5 | 99.0 | 26.9 | 26.8 | 26.8 | 24.7 | NB0816 |  | Ma12, Has18
HSC J100146+014827 | 10:01:46.64 | +01:48:27.1 | 5.704 | 99.0 | 28.3 | 26.9 | 26.9 | 27.3 | 24.7 | NB0816 |  | On21
HSC J100203+013623 | 10:02:03.15 | +01:36:23.8 | 5.742 | 29.2 | 28.1 | 26.3 | 25.9 | 26.1 | 24.2 | NB0816 |  | Has18
HSC J100214+021243 | 10:02:14.21 | +02:12:43.0 | 5.731 | 99.0 | 99.0 | 27.7 | 26.8 | 27.2 | 24.8 | NB0816 |  | On21
HSC J100301+020236 | 10:03:01.15 | +02:02:36.0 | 5.682 | 99.0 | 28.7 | 26.1 | 25.0 | 25.0 | 24.7 | NB0816 |  | Ma12, Has18
HSC J100305+015141 | 10:03:05.33 | +01:51:41.0 | 5.694 | 99.0 | 28.4 | 27.0 | 26.3 | 26.0 | 25.0 | NB0816 |  | Ma12, Has18
HSC J100306+014742 | 10:03:06.13 | +01:47:42.7 | 5.680 | 99.0 | 99.0 | 26.9 | 26.9 | 27.4 | 24.7 | NB0816 |  | Ma12, Has18
HSC J161403+535701 | 16:14:03.82 | +53:57:01.1 | 5.733 | 99.0 | 99.0 | 26.1 | 24.9 | 25.2 | 23.9 | NB0816 | LAB | Zh20
HSC J161927+551144 | 16:19:27.72 | +55:11:44.8 | 5.709 | 28.9 | 27.7 | 25.6 | 25.3 | 25.4 | 23.3 | NB0816 | LAB | Zh20
HSC J232558+002557 | 23:25:58.44 | +00:25:57.6 | 5.703 | 29.9 | 28.2 | 25.7 | 25.2 | 25.3 | 23.6 | NB0816 |  | Sh18
HSC J233408+004403 | 23:34:08.80 | +00:44:03.7 | 5.707 | 28.5 | 99.0 | 25.5 | 26.0 | 26.6 | 22.8 | NB0816 |  | Sh18
HSC J021650–051016 | 02:16:50.88 | –05:10:16.5 | 6.535 | 99.0 | 99.0 | 99.0 | 27.6 | 27.8 | 25.9 | NB0921 |  | Ou10
HSC J021653–050601 | 02:16:53.91 | –05:06:01.4 | 6.590 | 99.0 | 99.0 | 99.0 | 27.7 | 99.0 | 26.1 | NB0921 |  | Ou10
HSC J021654–045557 | 02:16:54.54 | –04:55:57.1 | 6.617 | 99.0 | 99.0 | 99.0 | 27.2 | 26.3 | 25.1 | NB0921 |  | Ou10
HSC J021654–050004 | 02:16:54.38 | –05:00:04.3 | 6.512 | 99.0 | 99.0 | 99.0 | 26.9 | 99.0 | 25.4 | NB0921 |  | Ou10
HSC J021658–045556 | 02:16:58.26 | –04:55:56.9 | 6.573 | 99.0 | 99.0 | 99.0 | 27.2 | 99.0 | 25.5 | NB0921 |  | Ou10
HSC J021702–050604 | 02:17:02.56 | –05:06:04.7 | 6.545 | 29.0 | 99.0 | 29.5 | 26.5 | 27.3 | 24.9 | NB0921 |  | Ou10
HSC J021703–045619 | 02:17:03.47 | –04:56:19.1 | 6.589 | 99.0 | 99.0 | 99.0 | 26.6 | 25.8 | 24.7 | NB0921 |  | Ou10
HSC J021746–042539 | 02:17:46.31 | –04:25:39.4 | 6.577 | 29.3 | 99.0 | 99.0 | 27.0 | 27.8 | 25.5 | NB0921 |  | This Study
HSC J021757–050414 | 02:17:57.00 | –05:04:14.3 | 6.570 | 99.0 | 99.0 | 99.0 | 27.0 | 26.7 | 25.9 | NB0921 |  | Ha19
HSC J021757–050844 | 02:17:57.58 | –05:08:44.7 | 6.595 | 99.0 | 99.0 | 99.0 | 25.7 | 25.3 | 23.8 | NB0921 | LAB (Himiko) | Ou10, Ji17, Ha19
HSC J021757–051556 | 02:17:57.32 | –05:15:56.5 | 6.564 | 29.0 | 99.0 | 99.0 | 99.0 | 26.2 | 26.0 | NB0921 |  | Ha19
HSC J021800–050330 | 02:18:00.80 | –05:03:30.4 | 6.613 | 29.8 | 99.0 | 99.0 | 27.3 | 28.6 | 25.5 | NB0921 |  | Ha19
HSC J021800–050346 | 02:18:00.23 | –05:03:46.9 | 6.601 | 99.0 | 99.0 | 99.0 | 27.6 | 26.7 | 25.5 | NB0921 |  | Ha19
HSC J021806–042657 | 02:18:06.28 | –04:26:57.3 | 6.570 | 29.8 | 29.6 | 99.0 | 29.2 | 28.2 | 25.9 | NB0921 |  | This Study
HSC J021819–050900 | 02:18:19.40 | –05:09:00.8 | 6.563 | 99.0 | 99.0 | 99.0 | 26.9 | 26.3 | 25.2 | NB0921 |  | Ou10, Ha19
HSC J021820–051109 | 02:18:20.70 | –05:11:09.9 | 6.575 | 99.0 | 99.0 | 99.0 | 27.5 | 27.6 | 25.0 | NB0921 |  | Ou10, Ha19
HSC J021827–050629 | 02:18:27.95 | –05:06:29.9 | 6.597 | 99.0 | 99.0 | 99.0 | 27.4 | 99.0 | 25.4 | NB0921 |  | Ha19
HSC J021827–050727 | 02:18:27.01 | –05:07:27.0 | 6.553 | 99.0 | 99.0 | 28.8 | 27.1 | 99.0 | 25.1 | NB0921 |  | Ou10, Ha19
HSC J021834–053024 | 02:18:34.53 | –05:30:24.3 | 6.580 | 99.0 | 99.0 | 99.0 | 28.4 | 25.6 | 25.6 | NB0921 |  | This Study
HSC J021839–042639 | 02:18:39.74 | –04:26:39.7 | 6.553 | 99.0 | 29.1 | 28.2 | 27.9 | 26.6 | 25.6 | NB0921 |  | This Study
HSC J021842–043011 | 02:18:42.60 | –04:30:11.4 | 6.548 | 99.0 | 99.0 | 99.0 | 26.7 | 26.6 | 24.9 | NB0921 |  | On21
HSC J021843–050915 | 02:18:43.64 | –05:09:15.7 | 6.512 | 99.0 | 28.8 | 28.1 | 26.0 | 25.5 | 24.7 | NB0921 |  | Sh18, Ha18
HSC J021844–043636 | 02:18:44.66 | –04:36:36.3 | 6.621 | 99.0 | 99.0 | 99.0 | 26.5 | 26.5 | 24.7 | NB0921 |  | Ou10
HSC J021901–045859 | 02:19:01.43 | –04:58:59.0 | 6.556 | 99.0 | 28.5 | 29.4 | 26.5 | 26.3 | 24.8 | NB0921 |  | Ji17
HSC J021933–050820 | 02:19:33.13 | –05:08:20.8 | 6.590 | 99.0 | 99.0 | 99.0 | 26.9 | 26.8 | 24.9 | NB0921 |  | On21
HSC J022023–050648 | 02:20:23.81 | –05:06:48.9 | 6.550 | 99.0 | 99.0 | 99.0 | 27.5 | 99.0 | 25.6 | NB0921 |  | This Study
HSC J022026–050542 | 02:20:26.83 | –05:05:42.5 | 6.566 | 99.0 | 99.0 | 99.0 | 27.0 | 29.2 | 25.2 | NB0921 |  | On21
HSC J100058+014815 | 10:00:58.00 | +01:48:15.1 | 6.604 | 99.0 | 99.0 | 29.8 | 25.5 | 24.8 | 23.5 | NB0921 | LAB (CR7) | So15, Has18
HSC J100124+023145 | 10:01:24.79 | +02:31:45.5 | 6.545 | 29.2 | 29.6 | 28.6 | 25.8 | 25.9 | 24.0 | NB0921 | LAB (MASOSA) | So15, Ji17
HSC J100207+023217 | 10:02:07.81 | +02:32:17.2 | 6.616 | 99.0 | 99.0 | 99.0 | 27.1 | 26.7 | 25.0 | NB0921 |  | On21
HSC J160107+550720 | 16:01:07.44 | +55:07:20.7 | 6.573 | 28.5 | 99.0 | 28.6 | 26.0 | 25.2 | 24.2 | NB0921 |  | Sh18
HSC J160707+555347 | 16:07:07.46 | +55:53:47.9 | 6.564 | 99.0 | 99.0 | 99.0 | 26.1 | 99.0 | 24.1 | NB0921 |  | Sh18
HSC J233125–005216 | 23:31:25.36 | –00:52:16.5 | 6.559 | 99.0 | 99.0 | 99.0 | 25.4 | 27.5 | 23.3 | NB0921 |  | Sh18
HSC J100205+020646 | 10:02:05.96 | +02:06:46.2 | 6.936 | 99.0 | 99.0 | 99.0 | 99.0 | 25.5 | 24.2 | NB0973 |  | Hu17

Note. — $\lambda_{\mathrm{c}}$: the central wavelengths of each filter, FWHM:
the FWHMs of transmission curves (see Figure 1), $z_{\mathrm{Ly\alpha}}$: the
redshift ranges of the Ly$\alpha$ emission lines that can be probed by each
filter.

Note. — NB816 and NB921 cover the entire D and UD layers of the HSC-SSP
survey. NB387 covers those fields except for the UD-SXDS field when combined
with the CHORUS survey data. NB1010 covers the UD-COSMOS and UD-SXDS fields.
NB527, NB718, and NB973 filters from the CHORUS survey cover the UD-COSMOS
field.

Note. — (1) Object ID. (2) R.A. (3) Declination. (4) Spectroscopic redshift.
(5)-(10) 2$.\\!\\!\arcsec$0-diameter circular aperture magnitude in g, r, i,
z, y, and NB. (11) Detection NB. (12) Reference for spectroscopic redshifts:
Ou08: Ouchi et al. (2008); Li09: Lilly et al. (2009); Ou10: Ouchi et al.
(2010); Co11: Coil et al. (2011); Ma12: Mallery et al. (2012); Mas12: Masters
et al. (2012); Le13: Le Fèvre et al. (2013); Sh14: Shibuya et al. (2014);
Kr15: Kriek et al. (2015); Li15: Liske et al. (2015); So15: Sobral et al.
(2015); Mo16: Momcheva et al. (2016); Ta17: Tasca et al. (2017); Hu17: Hu et
al. (2017); Ji17: Jiang et al. (2017); Ha18: Harikane et al. (2018b); Has18:
Hasinger et al. (2018); Ji18: Jiang et al. (2018); Sc18: Scodeggio et al.
(2018); Sh18a: Shibuya et al. (2018a); Sh18b: Shibuya et al. (2018b); Ha19:
Harikane et al. (2019, see also ); Ly20: Lyke et al. (2020); On21: Ono et al.
(2021).

Table 5: List of Lower Redshift Objects in Our LAE Catalogs

ID | R.A. | Decl. | $z_{\mathrm{spec}}$ | $\mathrm{g_{ap}}$ | $\mathrm{r_{ap}}$ | $\mathrm{i_{ap}}$ | $\mathrm{z_{ap}}$ | $\mathrm{y_{ap}}$ | $\mathrm{NB_{ap}}$ | Sample | Feature | Reference
---|---|---|---|---|---|---|---|---|---|---|---|---
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13)
HSC J022140–052310 | 02:21:40.99 | –05:23:10.1 | 0.000 | 21.3 | 21.7 | 22.2 | 22.4 | 22.5 | 20.9 | NB387 | STAR | Co11
HSC J022151–035716 | 02:21:51.19 | –03:57:16.6 | 0.000 | 25.0 | 24.9 | 25.0 | 24.9 | 24.6 | 24.0 | NB387 | STAR | Co11
HSC J022218–040755 | 02:22:18.77 | –04:07:55.5 | 0.000 | 20.8 | 21.1 | 21.4 | 21.6 | 21.7 | 20.5 | NB387 | STAR | Co11
HSC J022930–042700 | 02:29:30.35 | –04:27:00.1 | 0.000 | 19.9 | 20.3 | 20.8 | 21.1 | 21.3 | 19.3 | NB387 | STAR | Sc18
HSC J100030+023042 | 10:00:30.05 | +02:30:42.7 | 0.000 | 25.8 | 26.0 | 26.0 | 26.1 | 25.9 | 23.2 | NB387 | STAR | Mo16
HSC J100113+024435 | 10:01:13.09 | +02:44:35.4 | 0.322 | 24.0 | 23.8 | 23.6 | 23.3 | 23.2 | 22.3 | NB387 |  | Has18
HSC J022116–045644 | 02:21:16.39 | –04:56:44.0 | 0.047 | 23.9 | 23.8 | 23.8 | 23.7 | 23.7 | 22.8 | NB387 |  | Co11
HSC J022621–043124 | 02:26:21.27 | –04:31:24.5 | 0.466 | 24.6 | 24.3 | 24.4 | 24.4 | 24.2 | 23.9 | NB387 |  | Li15
HSC J022148–045039 | 02:21:48.69 | –04:50:39.3 | 0.618 | 23.8 | 23.7 | 23.5 | 23.3 | 23.2 | 21.7 | NB387 |  | Co11
HSC J233328+000858aaduplicated, but with different redshift estimates | 23:33:28.70 | +00:08:58.7 | 0.685 | 21.7 | 21.3 | 21.5 | 21.3 | 21.3 | 20.6 | NB387 |  | Co11
HSC J022203–045421 | 02:22:03.34 | –04:54:21.3 | 1.023 | 20.7 | 20.5 | 20.6 | 20.4 | 20.3 | 19.8 | NB387 | AGN | Li15, Ly20
HSC J232638–000524 | 23:26:38.12 | –00:05:24.6 | 1.032 | 21.2 | 20.9 | 21.1 | 20.6 | 20.4 | 20.0 | NB387 | AGN | Ly20
HSC J022240–040501 | 02:22:40.29 | –04:05:01.5 | 1.055 | 21.2 | 20.8 | 21.1 | 20.9 | 20.8 | 20.2 | NB387 | AGN | Li15, Ly20
HSC J161212+540936 | 16:12:12.57 | +54:09:36.6 | 1.056 | 19.6 | 19.4 | 19.6 | 19.6 | 19.5 | 19.0 | NB387 | AGN | Ly20
HSC J022120–045445 | 02:21:20.61 | –04:54:45.7 | 1.112 | 22.6 | 22.8 | 23.1 | 23.3 | 23.4 | 22.3 | NB387 |  | Co11
HSC J022259–051813 | 02:22:59.67 | –05:18:13.0 | 1.115 | 22.1 | 22.4 | 22.6 | 22.6 | 22.5 | 21.7 | NB387 |  | Co11
HSC J022734–042228 | 02:27:34.23 | –04:22:28.7 | 1.138 | 21.3 | 21.2 | 21.4 | 21.2 | 21.0 | 20.7 | NB387 | AGN | Ly20
HSC J100059+021224 | 10:00:59.62 | +02:12:24.6 | 1.328 | 25.9 | 26.0 | 25.8 | 25.5 | 25.2 | 24.8 | NB527 |  | Has18
HSC J100043+021352 | 10:00:43.20 | +02:13:52.6 | 1.400 | 23.4 | 23.6 | 23.4 | 22.8 | 23.3 | 22.2 | NB387 |  | Mo16
HSC J022550–040247 | 02:25:50.98 | –04:02:47.4 | 1.448 | 21.9 | 21.7 | 21.7 | 21.6 | 21.6 | 21.1 | NB387 | AGN | Li15, Ly20
HSC J233502+003727 | 23:35:02.63 | +00:37:27.2 | 1.455 | 20.3 | 19.9 | 19.9 | 20.0 | 20.0 | 19.4 | NB387 | AGN | Ly20
HSC J161255+563408 | 16:12:55.05 | +56:34:08.4 | 1.465 | 21.2 | 21.1 | 21.0 | 21.0 | 21.1 | 20.3 | NB387 | AGN | Ly20
HSC J233328+000858aaduplicated, but with different redshift estimates | 23:33:28.70 | +00:08:58.7 | 1.471 | 21.7 | 21.3 | 21.5 | 21.3 | 21.3 | 20.6 | NB387 | AGN | Ly20
HSC J022134–054128 | 02:21:34.51 | –05:41:28.0 | 1.474 | 21.7 | 21.4 | 21.3 | 21.2 | 20.8 | 20.5 | NB387 | AGN | Li15, Sc18, Ly20
HSC J160830+554350 | 16:08:30.17 | +55:43:50.5 | 1.474 | 19.1 | 19.0 | 19.0 | 19.2 | 19.3 | 18.5 | NB387 | AGN | Ly20
HSC J160933+532239 | 16:09:33.94 | +53:22:39.8 | 1.477 | 22.8 | 22.3 | 22.2 | 22.1 | 21.9 | 21.3 | NB387 | AGN | Ly20
HSC J022458–054447 | 02:24:58.25 | –05:44:47.2 | 1.479 | 21.6 | 21.3 | 21.5 | 21.3 | 21.3 | 20.3 | NB387 | AGN | Ly20
HSC J161009+554149 | 16:10:09.05 | +55:41:49.6 | 1.482 | 21.2 | 21.2 | 21.0 | 21.0 | 21.0 | 20.2 | NB387 | AGN | Ly20
HSC J233029+003252 | 23:30:29.82 | +00:32:52.3 | 1.485 | 22.5 | 22.1 | 21.8 | 21.8 | 21.7 | 21.2 | NB387 | AGN | Ly20
HSC J022226–041313 | 02:22:26.85 | –04:13:13.5 | 1.486 | 22.5 | 22.8 | 22.6 | 22.4 | 22.4 | 21.0 | NB387 | AGN | Co11, Ly20
HSC J023000–042835 | 02:30:00.95 | –04:28:35.3 | 1.486 | 19.8 | 19.5 | 19.5 | 19.5 | 19.6 | 18.8 | NB387 | AGN | Sc18, Ly20
HSC J095928+021950 | 09:59:28.33 | +02:19:50.5 | 1.486 | 20.8 | 20.6 | 20.6 | 20.6 | 20.7 | 19.8 | NB387 | AGN | Co11, Has18
HSC J161009+554155 | 16:10:09.56 | +55:41:55.9 | 1.486 | 21.9 | 21.7 | 21.5 | 21.5 | 21.5 | 20.8 | NB387 | AGN | Ly20
HSC J022417–052413 | 02:24:17.87 | –05:24:13.4 | 1.491 | 21.2 | 21.0 | 20.9 | 20.8 | 20.9 | 20.2 | NB387 | AGN | Ly20
HSC J022237–041140 | 02:22:37.89 | –04:11:40.4 | 1.496 | 21.5 | 21.4 | 21.3 | 21.2 | 21.3 | 20.5 | NB387 | AGN | Co11, Ly20
HSC J022309–041732 | 02:23:09.01 | –04:17:32.3 | 1.496 | 22.8 | 22.4 | 22.2 | 22.1 | 21.7 | 21.2 | NB387 | AGN | Ly20
HSC J022429–045807 | 02:24:29.12 | –04:58:07.8 | 1.496 | 20.5 | 20.2 | 20.0 | 20.1 | 20.2 | 19.4 | NB387 | AGN | Ly20
HSC J232814+000315 | 23:28:14.11 | +00:03:15.0 | 1.501 | 22.1 | 21.8 | 21.6 | 21.5 | 21.4 | 21.0 | NB387 | AGN | Ly20
HSC J022016–042422 | 02:20:16.34 | –04:24:22.4 | 1.503 | 23.4 | 22.8 | 22.5 | 22.4 | 22.5 | 21.8 | NB387 | AGN | Sc18, Ly20
HSC J022349–035122 | 02:23:49.52 | –03:51:22.9 | 1.504 | 21.5 | 21.3 | 21.2 | 21.2 | 21.2 | 20.5 | NB387 | AGN | Ly20
HSC J022528–043641 | 02:25:28.07 | –04:36:41.9 | 1.504 | 23.5 | 23.3 | 23.2 | 23.1 | 23.1 | 22.3 | NB387 | AGN | Le13, Li15
HSC J022718–043134 | 02:27:18.85 | –04:31:34.0 | 1.505 | 21.4 | 21.0 | 21.0 | 20.9 | 20.9 | 20.4 | NB387 | AGN | Le13, Li15
HSC J100111+023024 | 10:01:11.93 | +02:30:24.8 | 1.506 | 21.5 | 21.3 | 21.1 | 21.1 | 21.2 | 20.5 | NB387 | AGN | Li09, Co11
HSC J095815+014923 | 09:58:15.50 | +01:49:23.0 | 1.508 | 20.7 | 20.3 | 20.1 | 20.1 | 20.1 | 19.5 | NB387 | AGN | Li09, Ly20
HSC J022012–052005 | 02:20:12.84 | –05:20:05.6 | 1.522 | 21.6 | 21.5 | 21.2 | 21.3 | 21.2 | 20.6 | NB387 | AGN | Ly20
HSC J161352+543558 | 16:13:52.07 | +54:35:58.9 | 1.525 | 20.7 | 20.9 | 20.7 | 20.9 | 21.0 | 20.1 | NB387 | AGN | Ly20
HSC J161049+541840 | 16:10:49.15 | +54:18:40.5 | 1.526 | 22.0 | 21.7 | 21.5 | 21.5 | 21.6 | 20.9 | NB387 | AGN | Ly20
HSC J233436–001527 | 23:34:36.27 | –00:15:27.8 | 1.528 | 23.1 | 22.9 | 22.6 | 22.8 | 22.6 | 22.1 | NB387 | AGN | Ly20
HSC J022331–042557 | 02:23:31.83 | –04:25:57.9 | 1.584 | 22.5 | 22.7 | 22.3 | 22.2 | 22.1 | 21.7 | NB387 | AGN | Co11
HSC J100057+023932 | 10:00:57.80 | +02:39:32.6 | 1.410 | 23.5 | 22.9 | 22.8 | 22.8 | 22.8 | 22.3 | NB527 | AGN | Li09
HSC J095812+022302 | 09:58:12.40 | +02:23:02.6 | 2.322 | 25.9 | 26.0 | 25.9 | 25.6 | 25.4 | 24.7 | NB527 |  | Has18
HSC J095801+014832 | 09:58:01.45 | +01:48:32.9 | 2.402 | 22.7 | 22.7 | 22.4 | 22.1 | 21.8 | 21.3 | NB527 | AGN | Li09
HSC J095823+024106 | 09:58:23.56 | +02:41:06.1 | 2.402 | 23.7 | 23.8 | 23.7 | 23.5 | 23.1 | 22.8 | NB527 | AGN | Has18
HSC J095914+013635 | 09:59:14.66 | +01:36:35.1 | 2.408 | 23.1 | 23.3 | 23.2 | 23.0 | 22.6 | 21.7 | NB527 | AGN | Li09

Note. — (1) Object ID. (2) R.A. (3) Declination. (4) Spectroscopic redshift.
(5)-(10) 2$.\\!\\!\arcsec$0-diameter circular aperture magnitude in g, r, i,
z, y, and NB. (11) Detection NB. (12) Reference for spectroscopic redshifts:
Li09: Lilly et al. (2009); Co11: Coil et al. (2011); Le13: Le Fèvre et al.
(2013); Li15: Liske et al. (2015); Mo16: Momcheva et al. (2016); Has18:
Hasinger et al. (2018); Sc18: Scodeggio et al. (2018); Ka19: Kashino et al.
(2019); Ly20: Lyke et al. (2020).

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