# Catalog of magnetic white dwarfs with hydrogen dominated atmospheres

L. L. Amorim  Instituto de Física, Universidade Federal do Rio Grande do Sul,
91501-900 Porto-Alegre, RS, Brazil  S. O. Kepler  Instituto de Física,
Universidade Federal do Rio Grande do Sul, 91501-900 Porto-Alegre, RS, Brazil
Baybars Külebi  Institut de Ciencies de L’Espai, Universitat Autonoma de
Barcelona and Institute for Space Studies of Catalonia, Gran Capita 2-4, Edif.
Nexus 104, E-08034 Barcelona, Spain  S. Jordan  Astronomisches Rechen-
Institut, Zentrum fur Astronomie der Universität Heidelberg, Mönchhofstr.
12-14, D-69120 Heidelberg, Germany  A. D. Romero  Instituto de Física,
Universidade Federal do Rio Grande do Sul, 91501-900 Porto-Alegre, RS, Brazil

###### Abstract

White dwarfs are excellent research laboratories as they reach temperatures,
pressures, and magnetic fields that are unattainable on Earth. To better
understand how these three physical parameters interact with each other and
with other stellar features, we determined the magnetic field strength for a
total of 804 hydrogen-rich white dwarfs of which 287 are not in the
literature. We fitted the spectra observed with the Sloan Digital Sky Survey
using atmospheric models that consider the Zeeman effect due to the magnetic
field at each point in the stellar disk. Comparing magnetic and non-magnetic
WDs, the literature already shows that the magnetic ones have on average
higher mass than the non-magnetic. In addition to that, magnetic fields are
more common in cooler WDs than in hotter WDs. In consonance, we found that
those with higher magnetic field strengths tend to have higher masses, and
lower temperatures, for which models indicate the crystallization process has
already started. This reinforces the hypothesis that the field is being
generated and/or amplified in the cooling process of the white dwarf. Our
sample constitutes the largest number of white dwarfs with determined magnetic
fields to date.

White dwarf stars (1799) — DA stars (348) — Stellar magnetic fields (1610)

††facilities: SDSS Kepler et al. (2021), Gaia Gentile Fusillo et al.
(2021).††software: astropy (Astropy Collaboration et al., 2013, 2018), YAWP
Külebi et al. (2009).

##  1 Introduction

Strong magnetic fields are common in Hydrogen-rich white dwarfs stars (DAs).
Kepler et al. (2013) showed that at least 4% of all DAs observed with Sloan
Digital Sky Survey (SDSS) until Data Release 7 have magnetic fields greater
than 1 MG. The authors visually inspected all DA spectra and found 521 stars
with Zeeman Splittings. A more robust method to determine the field was
presented by Külebi et al. (2009), who used least squares minimization to find
the best model of magnetic field geometry to fit the observed spectra. They
applied this technique to 141 magnetic white dwarfs rich in hydrogen (DAH). A
revisit to the previous measurements is insightful, since the largest work
with DAHs considered only the splitting in H-alpha and H-beta and used only a
visual field determination method. We want complete and homogeneous results to
try to understand general properties of these stars to add information to the
question of the origin of the magnetic fields. In this work, we use the
fitting method to measure the magnetic field of all 804 DAHs found in the SDSS
sample until Data Release 16 (DR16). From this, 287 are newly reported DAHs.

The fraction of detected magnetic white dwarfs depends on the observed sample,
the detection method, and spectral types. Bagnulo & Landstreet (2021) found
23.4 ± 4.8 % of DAHs in the DA volume-limited sample for 20 pc using
spectropolarimetry, while Kepler et al. (2013) encountered 4% of DAHs in the
DAs of a SDSS magnitude limited sample with spectroscopy only. Kawka (2020)
presents a table of differences in the fraction of magnetic white dwarfs
through various spectral types. The fraction of detected magnetic white dwarfs
may differ from the real fraction of magnetic white dwarfs due to limitations
on the domain of magnetic field strength studied, the quality of the data, or
the significance of the measurable physical effect.

The origin of magnetic fields in white dwarfs is still an open question after
more than fifty years of the first discovery by Kemp et al. (1970). A
systematic study is crucial for the construction of a significant statistical
sample, which may help us shed some light on their origin. The magnetic field
could be formed in three different stages of the white dwarf evolution: before
the white dwarf stage, during its formation, or during the cooling process.

The main hypothesis of the first group corresponds to the fossil fields from
Ap/Bp stars (chemically peculiar and with magnetic fields stronger than
classical A- or B-type stars). The original gas from which stars are formed
are probably magnetized, since the net magnetic field of the galaxy is not
zero. In the main sequence, these fields are usually small, of the order of a
few kG as first shown by Babcock (1947) and later examples in Babcock (1958).
The magnetic field can be boasted through conservation of the magnetic flux up
to 100 MG when the star gets stripped of its outer layers and its core gets
exposed and starts to contract during the white dwarf cooling sequence.

This possible origin of the magnetic field is very attractive because the
Ohmic decay in degenerate matter suggests that these fields should last
billions of years. However, Wickramasinghe & Ferrario (2005) concluded that
the amount of magnetic Ap/Bp stars that have been detected cannot account for
the fraction of magnetic white dwarfs (MWD) measured, so other mechanisms must
also occur.

For the magnetic field to arise during the formation of the white dwarf, the
system may not be single. It can be due to the merger of two degenerate cores,
or it can be formed during the interaction of the two components of the binary
(common envelope) as presented by Tout et al. (e.g. 2008). However, this
channel of magnetism formation would lead to a much higher magnetic incidence
among white dwarfs in close binaries than is currently observed (e.g Belloni &
Schreiber, 2020).

Liebert (1988) was the first to suggest that magnetic WDs have generally a
higher mass than non-magnetic WDs. This was consistently found in several
subsequent works, such as Kepler et al. (2013) and McCleery et al. (2020).
Bagnulo & Landstreet (2021) argued that the fact that the magnetic have, in
average, a higher mass than the non-magnetic is true only for young WDs. The
possible origins mentioned so far are in agreement with the higher mass that
MWDs have when compared to the whole sample.

Nevertheless, there is evidence of yet another way of forming magnetic fields
in white dwarfs. It was early supposed that magnetic fields are more common
and stronger in cooler white dwarfs because it was first detected in this
group (Greenstein et al. (1971)). Eventually, hot magnetic white dwarfs were
also detected, and the early result was indeed corroborated (Liebert & Sion
(1979)). The sample was still subjected to strong selection effects and the
results were questioned. Valyavin & Fabrika (1999) studied the evolution of
magnetic white dwarfs in an even larger sample and concluded that as the star
cools, the frequency of magnetic white dwarfs increases, as does the strength
of the magnetic fields detected. This was endorsed by further studies such as
Kepler et al. (2013) and Bagnulo & Landstreet (2021). This means that the
white dwarf must be producing, exposing or enhancing the surface magnetic
field.

When a DA white dwarf cools below 14 000 K, it develops a surface convective
layer in which the dynamo process can occur, giving a boost to the surface
field. However, as the temperature continues to drop, the kinetic energy of
the envelope becomes larger, and eventually the convective cells hinder the
magnetic field line movement. This is coherent with the further drop of
magnetic field strength at even lower temperatures.

We could also mention other possibilities that could account for the magnetic
field in white dwarfs, like the crystallization of its core (Isern et al.,
2017; Ginzburg et al., 2022) and the interaction with orbiting planets
(Schreiber et al., 2021).The later effect will not be further studied in this
work, as we have yet no evidence that it is statistically significant to the
complete sample.

##  2 Detection of magnetic fields in SDSS DR16 white dwarfs

To build our sample, we visually investigated all DA spectra from Sloan
Digital Sky Survey (SDSS) DR7 to DR16 searching for Zeeman Splittings and
concatenated the selected ones with the previously known until Data Release 7,
resulting in a total of 804 magnetic white dwarfs with SDSS spectra. We used
the code (YAWP) presented by Külebi et al. (2009) to determine the strength of
the magnetic fields across the surface of the star which better matches the
observed spectrum, assuming an off-center dipole inclined in relation to our
line of sight.

Our results are presented in Table 2. To exemplify, Figure 1 shows three white
dwarfs with magnetic field strengths of different orders of magnitude. The
values presented are compatible with previous determinations within the
uncertainties. We chose to use a fixed temperature extracted from the
photometry of SDSS, while Külebi et al. (2009) allowed it to be a free
parameter in the fit. Kepler et al. (2013) only computed a visual estimate of
the magnetic field considering only the spectral line positions. The
comparison of these different methods is presented in Figure 2.

The inclination and offset of the dipole are correlated quantities in our
models. Different combinations between them can result in distributions of the
magnetic field over the stellar surface for which the effect measured in one
spectrum is the same. With that in mind, we interpret them as a measurement of
the complexity of the field over the stellar surface and not necessarily a
reflection of unique parameters.

Figure 1: SDSS spectrum of three of the stars we computed the magnetic field. The model with the best least-squares fit to the observed data is shown in red. From top to bottom we have (a) SDSS J101529.62+090703.7, Plate-MJD-Fiber = 1237-52762-0533, B = 2.51 MG, S/N = 12 and Teff = 8 000 K; (b) SDSS J215148.31+125525.2, Plate-MJD-Fiber = 0733-52207-0522, B = 20.71 MG, S/N = 20 and Teff = 10 000 K; (c) SDSS J134845.98+110008.8, Plate-MJD-Fiber = 5445-55987-0530, B = 202.58 MG, S/N = 11 and Teff = 16 500 K. We corrected with a third degree polynomial function the inclination of the spectra and attributed an arbitrary shift in flux for a better visualization. The gray vertical lines represent the wavelength of the Balmer lines in the regime of no magnetic field. Table 1: The table presents the identifiers of the DAHs in the SDSS and their masses and effective temperatures calculated with Gaia astrometry presented in Gentile Fusillo et al. (2021) when available. $T_{\mathrm{SDSS}}$ is the temperature we used for the magnetic field model, computed using non-magnetic atmospheric models and SDSS colors g, r, and i. The following columns present the parameters of the magnetic field resulting from the best YAWP model for each star. In order, there is the the dipole magnetic field strength of the offset dipole, the uncertainty computed through least squares, the z-offset from the center, and the inclination of the dipole to the line of sight. We call the attention that these last two quantities should be interpreted as a reference for the magnetic field structure (how different from a regular dipole) because there are degeneracies, especially due to changes in the field structure as the star rotates. The full table is available as online supporting information.  SDSS | Plate-MJD-Fiber | M ($\textrm{M}_{\odot}$) |  $\mathrm{T}_{\mathrm{eff}}$ (K) |  $\mathrm{T}_{\mathrm{SDSS}}$ (K) | B (MG) |  $\sigma$(B) (MG) |  $\mathrm{z}_{\mathrm{offset}}$ ($\mathrm{R}_{*}$) | incl(°)
---|---|---|---|---|---|---|---|---
J113212.99-003036.8 | 0282-51658-0278 | — | — | 20000 | 3.19 | 0.46 | 0.04 | 21.79
J114720.40-002405.7 | 0283-51584-0120 | 0.68 | 15919 | 17000 | 2.00 | — | — | 33.47
J121105.25-004628.5 | 0287-52023-0253 | 1.34 | 27473 | 19500 | 2.56 | 0.01 | -0.32 | 66.65
J121635.36-002656.3 | 0288-52000-0276 | — | — | 15000 | 64.24 | 0.11 | -0.18 | 59.27
J130807.48-010117.0 | 0294-51986-0089 | 0.47 | 11757 | 18500 | 2.20 | 0.00 | -0.21 | 72.94
J144114.21+003702.3 | 0307-51663-0595 | 0.87 | 25472 | 21000 | 4.39 | 0.49 | 0.49 | 20.70
J112852.88-010540.7 | 0326-52375-0565 | — | — | 18000 | 2.81 | 0.36 | 0.36 | 0.08
J113431.97-031529.0 | 0327-52294-0131 | 1.24 | 14539 | 15500 | 3.00 | 0.01 | 0.34 | 16.44
J155238.20+003910.4 | 0342-51691-0639 | 1.26 | 14285 | 12500 | 2.16 | 0.08 | 0.12 | 41.32
J171556.26+600643.7 | 0354-51792-0318 | 0.55 | 13567 | 9500 | 2.07 | 0.01 | 0.17 | 27.63
J172932.48+563204.1 | 0358-51818-0239 | — | — | 10000 | 6.00 | 0.04 | 0.49 | 0.46
J172329.14+540755.7 | 0359-51821-0415 | 1.09 | 10175 | 10000 | 36.82 | 6.75 | -0.05 | 53.78
J173915.64+545059.1 | 0360-51816-0547 | 0.30 | 9376 | 16000 | 2.69 | 0.02 | 0.37 | 31.91
J173235.19+590533.3 | 0366-52017-0591 | 0.57 | 11028 | 11500 | 2.56 | 0.04 | -0.36 | 78.63
J171441.07+552711.3 | 0367-51997-0318 | — | — | 30000 | 6.45 | 1.80 | 0.47 | 3.84
J172045.35+561214.8 | 0367-51997-0461 | — | — | 15000 | 24.67 | 0.01 | -0.30 | 78.71
J220435.05+001242.9 | 0372-52173-0626 | 1.11 | 10502 | 10500 | 2.15 | 0.00 | 0.13 | 12.83
J220823.65-011534.1 | 0373-51788-0086 | 0.39 | 19044 | 9500 | 3.04 | 0.11 | -0.50 | 35.80
J220514.08-005841.6 | 0373-51788-0243 | 0.75 | 18464 | 14500 | 3.01 | 0.02 | 0.42 | 74.80
J221828.58-000012.1 | 0374-51791-0583 | 1.06 | 12806 | 12239 | 220.78 | 6.35 | -0.04 | 24.85
J231432.89-011320.3 | 0382-51816-0289 | — | — | 18500 | 4.50 | 0.00 | 0.45 | 4.02
J232248.21+003901.0 | 0383-51818-0421 | 1.17 | 18130 | 11500 | 21.20 | 0.49 | -0.38 | 33.30
J022335.15+004954.8 | 0406-51900-0490 | 0.54 | 6728 | 9500 | 2.16 | 0.02 | -0.15 | 65.68
J022523.67+002743.0 | 0406-51900-0543 | — | — | 15500 | 2.02 | 0.00 | 0.16 | 0.16
J022623.80-002313.1 | 0406-52238-0071 | — | — | 16500 | 1.30 | 0.12 | 0.00 | 33.47
J025837.19+000019.2 | 0410-51877-0065 | 0.75 | 10561 | 10000 | 2.33 | 0.01 | 0.16 | 2.51
J032137.43+010437.3 | 0413-51821-0578 | 0.89 | 21140 | 18000 | 2.86 | 0.00 | 0.05 | 16.68
J031323.65-001659.9 | 0413-51929-0313 | — | — | 30000 | 7.30 | 0.00 | 0.42 | 0.00
J033145.69+004516.9 | 0415-51879-0378 | 1.05 | 19230 | 12000 | 13.05 | 2.37 | -0.42 | 48.36
J033320.37+000720.6 | 0415-51879-0485 | 0.79 | 7498 | 9500 | 771.71 | 214.35 | 0.18 | 0.10
J034511.10+003444.2 | 0416-51811-0590 | 0.57 | 7431 | 8000 | 2.50 | 0.27 | -0.36 | 12.91
J003111.75+134919.5 | 0417-51821-0084 | — | — | 21000 | 2.24 | 0.00 | 0.15 | 0.72
J003232.07+153126.6 | 0418-51817-0346 | 0.35 | 9917 | 17000 | 2.00 | 0.78 | 0.10 | 15.36
J004513.88+142248.1 | 0419-51879-0147 | 0.81 | 7629 | 8000 | 3.61 | 0.04 | -0.29 | 18.68
J013533.20+132249.8 | 0426-51882-0291 | — | — | 21000 | 5.10 | 0.01 | 0.00 | 33.47
J013920.54+152218.7 | 0426-51882-0524 | 0.46 | 10530 | 18000 | 2.30 | 0.00 | 0.19 | 0.56
J021230.00+122557.2 | 0428-51883-0046 | — | — | 15500 | 2.07 | 0.11 | 0.14 | 0.80
J075959.57+433521.1 | 0437-51869-0369 | — | — | 9000 | 91.55 | 57.78 | -0.38 | 29.35
J081136.33+461156.4 | 0439-51877-0523 | — | — | 40000 | 4.95 | 2.77 | 0.49 | 3.90
J085159.32+532540.3 | 0449-51900-0311 | 0.87 | 11106 | 11500 | 63.76 | 28.16 | -0.17 | 13.81

Figure 2: In the left panel, we present the comparison of dipole magnetic
field strength of the offset dipole presented in this work and the values
presented by Külebi et al. (2009). In the right panel, we present the
comparison of dipole magnetic field strength of the offset dipole presented in
this work and visually estimated values from Kepler et al. (2013); the
different size dots represent the two independent lines they used to estimate
the magnetic field.

The magnetic field affects the line profiles, and we cannot use them to
estimate surface gravity directly. Thereby, the effect of the magnetic field
in the radiation transfer in model atmospheres used in the code were
calculated with $\log g=8$ for all the stars as an approximation. This value
was originally chosen to consider that it is the mean value for white dwarfs.
We acknowledge that it is not the best value to represent magnetic white
dwarfs once they were found to be more massive than non-magnetic ones.
Fortunately, this doesn’t affect the position of the lines that are closely
related to the magnetic field strength, only their strength.

The code also presents the possibility of searching for the temperature
spectroscopically, together with the magnetic field parameters. But, due to
the uncertainties in the spectra and the surface gravity versus effective
temperature correlation, we opted to use a previously estimated temperature
acquired by comparing the observed fluxes with hydrogen-rich atmospheric
models. These models lead to a table of colors in the bands u, g, r, i, and z
used by SDSS for each temperature. One can compare these values, especially
their differences (color index), to the values from the observed spectra, thus
obtaining an estimated temperature. We chose not to use the z-band since it is
observed a lot of noise in the corresponding wavelengths. The u-band was also
discarded since it is expected to be the most affected by the magnetic
splitting of the lines.

We only fitted temperatures between 8 000 K and 40 000 K when varying the
magnetic field due to convergence problems. For only one star out of 4 which
we should have used 50 000 K we were able to find a model with this
temperature. No model was found with appropriate temperatures for the 13 stars
cooler 8 000 K. This limits our capacity to model the magnetic field of these
stars, as the models present deeper lines than those observed in the SDSS
spectra, partially due to the log g=8.0 approximation. The depth of the
absorption lines does not have a large impact on the determination of the
magnetic field amplitudes, which are predominantly determined by the
wavelength displacement and presence of splittings. This effect can be seen in
the upper part of Figure 1, in which a WD with a temperature below 8 000 K is
presented. The best model, in red, clearly has lines deeper than the observed
spectra but well represents the splitting on the H${}_{\alpha}=6\,565$ Å and
H${}_{\beta}=4\,861$ Å lines.

For better visualization, we present the observed spectra with a running mean
of five points because the measured spectra are usually noisy. We emphasize
that this step was taken after we ran YAWP and its only purpose is to guide us
in the analysis of the results. The noise in the observed spectra is
wavelength-dependent and is significantly higher above 7 000 Å. It is
noticeable that the hydrogen absorption lines do not reach these long
wavelengths for field regimes below 25 MG ($\log B\approx 1.4$), as can be
seen in Figure 3 from Schimeczek & Wunner (2014). Therefore we do not consider
higher wavelengths in the spectra of DAHs with lower fields to minimize the
noise effect, which can be seen in the first two spectra of Figure 1.

Figure 3: Magnetic field strength as a function of the wavelength of the first
325 transitions in the Balmer series, which emerge from the field-free Balmer
transitions up to principal quantum numbers n = 10. Colors were arbitrarily
assigned to facilitate visualization. Figure from Schimeczek & Wunner (2014)

For some stars, YAWP did not converge to a solution, and we resorted to a
simpler visual analysis to estimate the magnetic field, used it as a fixed
input to the code, and fitted only the inclination and the offset. An
illustrative example of the visual inspection can be seen in Figure 4.

Figure 4: Spectra of DAH after applying the smooth function and normalizing by
a third-degree polynomial function for better display.The star
SDSSJ085649.67+253441.0 in the plot has Plate-MJD-Fiber = 5179-55957-0778, B =
85 MG, S/N = 14, and Teff = 11 500 K. The flux is $f_{\lambda}\ /\ 10^{-16}\
\rm{erg}\ \rm{cm}^{-2}\ \rm{s}^{-1}\ \AA^{-1}$. The red lines represent the
magnetic field strength as a function of the wavelength, as computed by
Schimeczek & Wunner (2014). The blue vertical lines represent the position of
absorption lines for hydrogen when no magnetic field is applied.

After we determined a magnetic field strength visually, we computed the best
model with the magnetic field fixed and varying only the inclination and
offset. One example is portrayed in Figure 5. In this specific case, YAWP did
not converge to the best solution on its own, most probably due to the
possible contamination of a very close star in the field.

Figure 5: SDSS spectrum of the star with SDSS J004248.20+001955.2 is presented
in black. The model with the best least-squares fit to the observed data with
Plate-MJD-Fiber = 0690-52261-0594, B = 8.5 MG, S/N = 7.5 and Teff = 14 000 K
is shown in red. Even though we plot the whole spectrum, the continuum is not
used i the fit.

The visual estimation was also used for four stars with magnetic fields below
$1$ MG and S/N above 10. The magnetic field values were not used as input for
YAWP since it is out of the range comprised in the models. An example can be
seen in Figure 6.

Figure 6: Spectra of the star with SDSS J090139.03+064022.4, Plate-MJD-Fiber =
4868-55895-0730, B = 0.8 MG, S/N = 12, and Teff = 8 000 K after applying the
smooth function and normalizing by a third-degree polynomial function for
better display. The flux is $f_{\lambda}\ /\ 10^{-16}\ \rm{erg}\ \rm{cm}^{-2}\
\rm{s}^{-1}\ \AA^{-1}$. The red lines represent the magnetic field strength as
a function of the wavelength, as computed by Schimeczek & Wunner (2014).

The only geometry of magnetic fields considered for our determinations was the
non-centered dipole, which was a good approximation for these objects.
Therefore, the difference in magnetic field strength between stellar surface
regions is substantial, up to orders of magnitude, and is larger with
increasing polar field strength. Some exceptions exist, such as if the
inclination is close to $90\deg$, and we look straight into a pole of a little
off-centered dipole. This effect can be seen in Figure 7. The model that best
reproduces the observed data has a mean modulus of magnetic field strength
over the stellar surface of B = 61 MG (red line in the outside panel).
However, this is incompatible with simply summing the respective spectra of
each area element and evaluating the result. Since each magnetic field
intensity affects the line profiles in a specific way, the summed spectra will
look more like the mode than the mean, in this case.

It can be seen in the inside panel of Figure 6 that about half of the stellar
surface presents field intensities varying from 40 to 120 MG, while the other
half presents field intensities around 30 MG. In addition, lower fields are
easier to identify visually due to the lower complexity of the line profiles,
as seen in Figure 3. As a consequence, if we did the visual inspection of the
total spectra coming from the whole visible disk, we would find a value closer
to 30 MG.

Figure 7: Outer panel showing the SDSS spectrum of the star with
SDSSJ102054.10+362647.0, Plate-MJD-Fiber = 4568-55600-0952, B = 61.2 MG, S/N
$\simeq$ 63 and $\mathrm{T}_{\mathrm{eff}}$ = 13 500 K is presented in black.
The model with the best least-squares fit to the observed data is shown in
red. The blue lines represent the magnetic field strength as a function of the
wavelength, as computed by Schimeczek & Wunner (2014). The inner panel shows
the distribution of magnetic field over the stellar surface due to the
inclination of $29.35^{\mathrm{o}}\,$ and zoffset of -0.38
$\textrm{R}_{\star}\,$delineated by the best model.

In addition to the intrinsic variation, we estimate that our precision cannot
be better than $1$ MG due to spectral resolution and signal-to-noise ratios.
Beyond these limitations, from the $\chi^{2}$, the mean magnetic field
uncertainties are approximately 12% of the computed value.

##  3 Discussion

Liebert et al. (2003) propose that magnitude-limited samples, as the one
studied in this work, have a bias against higher mass white dwarfs since for a
given temperature, they have a smaller radius and consequently smaller
luminosity. This would lead them to be detected less frequently. However, they
did not take into consideration that more massive white dwarfs take longer to
cool down because they have a smaller radius. It is not straightforward which
of these effects predominates at a given time. Bagnulo & Landstreet (2021)
showed that magnitude-limited samples have a complex bias against or in favor
of higher masses depending on the stellar age. One can conclude that there is
a bias in favor of younger stars independently of their mass. They also found
that the frequency of magnetic white dwarfs is substantially depressed for
stars younger than 0.5 Gyr and that this difference probably reflects the
action of the mechanisms that produce magnetic fields in white dwarfs.

Even though it favors younger stars, magnitude-limited surveys, especially
with low-resolution spectroscopy, are the ones that can go deeper in magnitude
and examine a larger sample of stars. With this perspective, we will discuss
the distribution of magnetic field strength, the relation between magnetic
field and mass, effective temperature and period, and some specific cases that
stand out in our sample.

###  3.1 Distribution of magnetic field strength

The fraction of magnetic white dwarfs rich in hydrogen found in this work was
2.7%, far below the previous values presented in the literature. We call
attention to the strong bias present in our sample due to the chosen survey.
The selection of which stars were observed by SDSS changed over time,
resulting in a smaller number of magnetic white dwarfs in the latest data
releases because white dwarfs were not specifically targeted.

We also note that the visual identification of Zeeman splittings is much more
efficient for magnetic fields below 60 MG when the effect is well-behaved, as
can be noticed in Figure 3. The SDSS spectral resolution around 2 Å also
hinders the detection of fields below 1 MG, even for S/N$\geq$10\. With these
reservations, we present the distribution of the magnetic field strength of
our sample in Figure 8. A higher appearance of magnetic fields strength below
3 MG is noticeable. It is not in all cases evident that the stars are magnetic
due to the limited SDSS S/N.

Figure 8: Magnetic field strength histogram for all magnetic white dwarf in
our sample.

###  3.2 Relation between mass and magnetic field

To examine the possible relation between magnetic field and mass, we made the
Figure 9 to study the fraction of stars with magnetic fields, and Figure 10 to
study the connection between the strength of the magnetic field and the star’s
mass.

Figure 9: Histogram of mass calculated with Gaia data for all DAs in red and
only the magnetic ones in blue.

Figure 10: Magnetic field versus mass calculated with Gaia data, showing a
clear absence of highly magnetic white dwarfs with lower masses on the left.
Magnetic field versus effective temperature calculated with Gaia data, showing
a clear increase of highly magnetic white dwarfs with lower temperatures on
the right.

It appears that the distribution of mass of DAHs can be approximated by a
Gaussian centered in 0.78 $\textrm{M}_{\odot}$ with no further remarkable
features. The left panel in Figure 10 shows an evident lack of low mass DAHs
with strong fields.

###  3.3 Relation between effective temperature and magnetic field

In the search for a hint of the magnetic field origin, we investigate its
relation to the effective temperature of the inspected stars. The right panel
in Figure 10 shows that the magnetic field strength increases as the effective
temperature decreases.

Not only do we find white dwarfs with stronger magnetic fields, but also we
detect more magnetic white dwarfs at lower temperatures. The second effect is
naturally expected because it is easier to detect white dwarfs at lower
temperatures since they spend more time cooling down. To consider this effect
and check if there are really more magnetic white dwarfs at lower
temperatures, we study the fraction of DAHs compared to the whole sample of
white dwarfs rich in hydrogen. This is illustrated by Figure 11, and it is
noticeable that the fraction of magnetic stars is indeed increasing as the
temperature decreases.

Figure 11: The ratio between the number of DAHs and the number of DAs versus
effective temperature, showing a peak of abundance near
T${}_{\mathrm{eff}}=25\,000$ K. The blue vertical lines represent the standard
errors for each point.

It is especially outstanding the rapid growth in magnetic fraction around
effective temperature of $25\,000$ K ($\log T_{\mathrm{eff}}\approx 4.4$), the
temperature at which a convective zone of helium is internally formed in the
white dwarf, that could be responsible for this increase. We also call
attention to the build-up in the magnetic fraction that starts around the
effective temperature of $16\,000$ K ($\log T_{\mathrm{eff}}\approx 4.2$). At
this temperature, a convective zone of hydrogen is formed in the white dwarf,
and it could be responsible for the rise in the magnetic fraction.

A question then arises: does the effect change depending on the stellar mass?
To answer this question, we divided our sample in two at M = 0.8
$\textrm{M}_{\odot}$ and at M = 1 $\textrm{M}_{\odot}$ and compared the
results, which can be seen in the left and right panel of Figure 12
respectively.

The distribution with temperature of DAs doesn’t change much, except for the
fact that there are considerably fewer stars with M $>$ 1
$\textrm{M}_{\odot}$. Differently, for the DAHs, there is a significant
variation of the distribution. We highlight the valley around $10\,000$ K (log
Teff = 4.0) as being a consequence of convective mixing and dilution. They
pollute the stellar atmosphere with helium and thin the hydrogen layer,
reducing the number of DAs and increasing the number of DABs or DBAs. This
effect is constrained in temperature as a consequence of the disappearance of
the lines of helium at lower temperatures, meaning that the star may contain
helium in its atmosphere, it is only not possible to observe it through the
spectra.

Figure 12: Both panels show the number of DAHs and DAs versus the effective
temperature. The sample was divided at 0.8 $\textrm{M}_{\odot}$and 1.0
$\textrm{M}_{\odot}$, represented in the upper panel and the lower panel
respectively. We divided the absolute number of DAs by ten to allow better
visualization. It is evident a change in behavior of the distribution of DAHs
that is not accompanied by the distribution of DAs.

The magnetic DAs with mass above 0.8 $\textrm{M}_{\odot}$have a similar double
peak behavior, even though it is more restricted in temperature. The magnetic
DAs with mass above 1 $\textrm{M}_{\odot}$ on the other hand have the second
peak missing. Some mechanism must be inhibiting the magnetic field for higher
masses at temperatures around $16\,000$ K ($\log T_{eff}\approx 4.2$). This
same effect is not observed for masses below 1 $\textrm{M}_{\odot}$. In fact,
the opposite occurs, and they show the second peak much higher than the first.
The behavior of the lower mass DAHs is precisely the one discussed earlier,
thus becoming necessary the understanding of what could be suppressing the
higher masses magnetic fields.It is valid to remember that more massive stars
are usually less detected in magnitude limited samples because they are
fainter, so this could also be the result of selection effects.

###  3.4 Relation between crystallization and magnetic field

One significant physical process that is highly dependent on the white dwarf
mass is the crystallization of its core, and we suppose that it is the one
holding the magnetic field back. In the search for a better understanding of
the relation between the crystallization and the magnetic field, we built
Figure 13, in which one can see not only if the star has started to
crystallize its core but also have an idea of how advanced this process is.
The further the star is from the crystallization line in the colder direction,
the more crystallized its core is. We emphasize that the crystallization line
has an intrinsic uncertainty to the models used to compute it.

Figure 13: Mass versus effective temperature calculated with Gaia data. The
colors black, blue, and red represent magnetic fields below 10 MG, between
10—100 MG, and above 100 MG, respectively. The two red stars represent the
most magnetic DAs with a magnetic field above 700 MG. The solid black line
represents the temperature of crystallization for the single evolution of
white dwarfs of different masses as presented by Romero et al. (2013),
Horowitz et al. (2010), and Lauffer et al. (2018). Crystallization increases
to the right from the line, i.e., cooler temperatures.

It is recognizable that most of the stars with higher magnetic fields have
started the crystallization process, which goes against the hypothesis that
crystallization is responsible for the lower fraction of magnetic DAs with
higher masses. Isern et al. (2017) proposed a mechanism of generation of
magnetic fields of strengths of up to 0.1 MG by the dynamo in the convective
region generated by the phase separation due to the crystallization process.
Ginzburg et al. (2022) found that these fields could go as high as 100 MG
depending on the rotational period of the star and its mass.

###  3.5 Particular Stars

Some stars have more than one spectrum observed by SDSS in which it is
possible to look for variability in the line profiles as an indication of the
rotational period. Besides the inclination of the star in respect to the line
of sight, which may allow us to see different portions of the stellar surface
as it rotates, the line profiles can also change due to the misalignment
between the magnetic field axis and the rotation axis. Here we highlight the
star SDSS J030407.40-002541.74 in which this effect is prominent. In Figure 14
we can see that the $H_{\alpha}$ line varies between a deeper central line to
equally deep triplet components. It is also visible that the $\sigma-$
component of the $H_{\beta}$ line appears and disappears.

Figure 14: Different spectra of SDSS J030407.40-002541.74 with their
respective observation dates. The two small vertical black segments mark the
position of Hβ and Hα lines.

This star has also been observed by TESS, and we have 30 minutes cadence data
from sectors 4 and 31. Unfortunately, no variation above the detection limit
was identified, which is understandable since it is very faint (Gaia Mag =
17.8528).

The same process that affects the SDSS J030407.40-002541.74 $H_{\beta}$ lines
could be responsible for the $H_{\beta}$ line profile of SDSS
J221141.80+113604.5. which is illustrated in Figure 15. Kilic et al. (2021)
argued that assuming a hydrogen atmosphere, an inclination, and an offset
dipole geometry, the lines could not be reasonably reproduced. We found a good
fit to the observed spectra except for the lateral components of the
$H_{\beta}$ line, which is expected to change as shown for SDSS
J030407.40-002541.74.

Kilic et al. (2021) assumed a centered dipole as in Fig. 15 lower panel, and
explained the difference in the line depth between the model and the observed
spectra with the assumption of a non-pure hydrogen atmosphere. Our model does
not require this additional complexity to explain the data.

Figure 15: Observed spectrum of J221141.80+113604.5 with Plate-MJD-Fiber =
5064-55864-0122, B=18.77 MG, S/N=20 and $T_{\mathrm{eff}}=9\,500$ K. The model
with the best least-squares fit to the data is shown in red. We highlight that
the line near $5\,500$ Å is due to a systematic error of joining two different
observations by SDSS. The full red line shows a model with computed offset
magnetic dipole field geometry, while the dashed red line shows a model
computed not inclined centered magnetic dipole field geometry with the
strength found in the previous calculation.

Another interesting case is the star SDSS J225726.05+075541.6 featured in
Williams et al. (2022). They stated that the observed Balmer lines are
significantly weaker than predicted by the atmospheric models, which could be
explained if the star were in an unresolved binary system, but the allowable
parameter space for such a binary is minuscule. We found a good fit, again
with only one component of $H_{\beta}$ with large discrepancies. Our model is
shown in Figure 16.

Figure 16: Observed spectrum of SDSS J225726.05+075541.6 with Plate-MJD-Fiber
= 2310-53710-0420, B=17.4 MG, S/N=34 and $T_{\mathrm{eff}}=9\,500$ K. The
model with the best least-squares fit to the data is shown in red.

##  4 Conclusions

In this work, we estimated magnetic field strength for 804 white dwarfs
observed from SDSS of which 287 are new discoveries. Save rare exceptions, our
determinations are coherent with Kepler et al. (2013) and Külebi et al.
(2009). It consists of the largest number of magnetic field determinations for
white dwarfs to date. We searched for relations between magnetic field
strength and stellar mass, effective temperature, and crystallization status.

It was found that a considerable percentage of DAH have fields below 3 MG.
This is, to some extent, biased by our spectroscopic method, but could also
mean that lower fields are more abundant in white dwarfs. This result is in
opposition to Bagnulo & Landstreet (2021) which concluded that within the
range of field strength found in the 20 pc volume, which extends between about
40 kG and 300 MG, the probability of fields occurring is roughly constant per
dex of field strength.

We found that the magnetic field strength increases as the effective
temperature decreases, together with an increase in the fraction of magnetic
white dwarfs. This effect corroborates with the surface magnetic field being
generated or enhanced in the white dwarf cooling phase. We could also observe
that the highest fields tend to occur in the more massive stars and that the
mean mass was, in general, higher than the non-magnetic ones
($0.78\,M_{\odot}$ compared to the mean $0.6\,M_{\odot}$). This does not give
us any new information about the origin of the magnetic field because many
assumptions already consider a higher mass. But a physical property closely
related to the mass is crystallization, and we found that the most magnetic
ones tend to be already crystallized. This is expected since DAH have higher
masses, so they crystallize at higher temperatures but spend more time (easier
to detect) at lower temperatures (already crystallized).

The general behavior found in this work is compatible with the findings by
Bagnulo & Landstreet (2022) that a high fraction of high-mass WDs have a
strong magnetic field very early in their cooling phase, while normal mass
stars are rarely magnetic when they are hot (young), but when they get cooler
(older), magnetic fields become more common and stronger with time. Some other
mechanism may be inhibiting magnetic fields in WDs with $M\geq 1\,M_{\odot}$
and $T_{\mathrm{eff}}\leq 16\,000$ K.

We thank the support by grants from CAPES and CNPq (Brazil).

##  Appendix A Complete table

Table 2: The table presents the identifiers of the DAHs in the SDSS and their masses and effective temperatures calculated with Gaia astrometry presented in Gentile Fusillo et al. (2021) when available. Then we have the temperature used for the magnetic field model, computed using non-magnetic atmospheric models and SDSS colors g, r, and i. The following columns present the parameters of the magnetic field resulting from the best YAWP model for each star. In order, there is the dipole magnetic field strength of the offset dipole, the uncertainty computed through least squares, the z-offset from the center, and the inclination of the dipole to the line of sight. We call attention that these last two quantities should be interpreted as a reference for the magnetic field structure because there are many degeneracies for the geometry.  SDSS | Plate-MJD-Fiber | M | $\mathrm{T}_{\mathrm{eff}}$ | $\mathrm{T}_{\mathrm{SDSS}}$ | B |  $\sigma$(B) | $\mathrm{z}_{\mathrm{offset}}$ | incl
---|---|---|---|---|---|---|---|---
|  | ($\textrm{M}_{\odot}$) | (K) | (K) | (MG) | (MG) | ($\mathrm{R}_{\mathrm{*}}$) | (°)
J113212.99-003036.8 | 0282-51658-0278 | — | — | 20000 | 3.19 | 0.46 | 0.04 | 21.79
J114720.40-002405.7 | 0283-51584-0120 | 0.68 | 15919 | 17000 | 2.00 | — | — | 33.47
J121105.25-004628.5 | 0287-52023-0253 | 1.34 | 27473 | 19500 | 2.56 | 0.01 | -0.32 | 66.65
J121635.36-002656.3 | 0288-52000-0276 | — | — | 15000 | 64.24 | 0.11 | -0.18 | 59.27
J130807.48-010117.0 | 0294-51986-0089 | 0.47 | 11757 | 18500 | 2.20 | 0.00 | -0.21 | 72.94
J144114.21+003702.3 | 0307-51663-0595 | 0.87 | 25472 | 21000 | 4.39 | 0.49 | 0.49 | 20.70
J112852.88-010540.7 | 0326-52375-0565 | — | — | 18000 | 2.81 | 0.36 | 0.36 | 0.08
J113431.97-031529.0 | 0327-52294-0131 | 1.24 | 14539 | 15500 | 3.00 | 0.01 | 0.34 | 16.44
J155238.20+003910.4 | 0342-51691-0639 | 1.26 | 14285 | 12500 | 2.16 | 0.08 | 0.12 | 41.32
J171556.26+600643.7 | 0354-51792-0318 | 0.55 | 13567 | 9500 | 2.07 | 0.01 | 0.17 | 27.63
J172932.48+563204.1 | 0358-51818-0239 | — | — | 10000 | 6.00 | 0.04 | 0.49 | 0.46
J172329.14+540755.7 | 0359-51821-0415 | 1.09 | 10175 | 10000 | 36.82 | 6.75 | -0.05 | 53.78
J173915.64+545059.1 | 0360-51816-0547 | 0.30 | 9376 | 16000 | 2.69 | 0.02 | 0.37 | 31.91
J173235.19+590533.3 | 0366-52017-0591 | 0.57 | 11028 | 11500 | 2.56 | 0.04 | -0.36 | 78.63
J171441.07+552711.3 | 0367-51997-0318 | — | — | 30000 | 6.45 | 1.80 | 0.47 | 3.84
J172045.35+561214.8 | 0367-51997-0461 | — | — | 15000 | 24.67 | 0.01 | -0.30 | 78.71
J220435.05+001242.9 | 0372-52173-0626 | 1.11 | 10502 | 10500 | 2.15 | 0.00 | 0.13 | 12.83
J220823.65-011534.1 | 0373-51788-0086 | 0.39 | 19044 | 9500 | 3.04 | 0.11 | -0.50 | 35.80
J220514.08-005841.6 | 0373-51788-0243 | 0.75 | 18464 | 14500 | 3.01 | 0.02 | 0.42 | 74.80
J221828.58-000012.1 | 0374-51791-0583 | 1.06 | 12806 | 12239 | 220.78 | 6.35 | -0.04 | 24.85
J231432.89-011320.3 | 0382-51816-0289 | — | — | 18500 | 4.50 | 0.00 | 0.45 | 4.02
J232248.21+003901.0 | 0383-51818-0421 | 1.17 | 18130 | 11500 | 21.20 | 0.49 | -0.38 | 33.30
J022335.15+004954.8 | 0406-51900-0490 | 0.54 | 6728 | 9500 | 2.16 | 0.02 | -0.15 | 65.68
J022523.67+002743.0 | 0406-51900-0543 | — | — | 15500 | 2.02 | 0.00 | 0.16 | 0.16
J022623.80-002313.1 | 0406-52238-0071 | — | — | 16500 | 1.30 | 0.12 | 0.00 | 33.47
J025837.19+000019.2 | 0410-51877-0065 | 0.75 | 10561 | 10000 | 2.33 | 0.01 | 0.16 | 2.51
J032137.43+010437.3 | 0413-51821-0578 | 0.89 | 21140 | 18000 | 2.86 | 0.00 | 0.05 | 16.68
J031323.65-001659.9 | 0413-51929-0313 | — | — | 30000 | 7.30 | 0.00 | 0.42 | 0.00
J033145.69+004516.9 | 0415-51879-0378 | 1.05 | 19230 | 12000 | 13.05 | 2.37 | -0.42 | 48.36
J033320.37+000720.6 | 0415-51879-0485 | 0.79 | 7498 | 9500 | 771.71 | 214.35 | 0.18 | 0.10
J034511.10+003444.2 | 0416-51811-0590 | 0.57 | 7431 | 8000 | 2.50 | 0.27 | -0.36 | 12.91
J003111.75+134919.5 | 0417-51821-0084 | — | — | 21000 | 2.24 | 0.00 | 0.15 | 0.72
J003232.07+153126.6 | 0418-51817-0346 | 0.35 | 9917 | 17000 | 2.00 | 0.78 | 0.10 | 15.36
J004513.88+142248.1 | 0419-51879-0147 | 0.81 | 7629 | 8000 | 3.61 | 0.04 | -0.29 | 18.68
J013533.20+132249.8 | 0426-51882-0291 | — | — | 21000 | 5.10 | 0.01 | 0.00 | 33.47
J013920.54+152218.7 | 0426-51882-0524 | 0.46 | 10530 | 18000 | 2.30 | 0.00 | 0.19 | 0.56
J021230.00+122557.2 | 0428-51883-0046 | — | — | 15500 | 2.07 | 0.11 | 0.14 | 0.80
J075959.57+433521.1 | 0437-51869-0369 | — | — | 9000 | 91.55 | 57.78 | -0.38 | 29.35
J081136.33+461156.4 | 0439-51877-0523 | — | — | 40000 | 4.95 | 2.77 | 0.49 | 3.90
J085159.32+532540.3 | 0449-51900-0311 | 0.87 | 11106 | 11500 | 63.76 | 28.16 | -0.17 | 13.81
J093921.25+581421.4 | 0452-51911-0553 | — | — | 21000 | 2.40 | 0.01 | 0.19 | 18.17
J094046.28+595415.8 | 0453-51915-0325 | 0.19 | 10231 | 12000 | 2.04 | 0.00 | 0.21 | 2.05
J023609.43-080823.7 | 0455-51909-0474 | — | — | 10500 | 34.00 | 0.12 | 0.29 | 11.01
J031630.64-081529.1 | 0459-51924-0002 | 0.55 | 9556 | 9500 | 2.19 | 0.01 | -0.23 | 65.04
J032404.30-061756.5 | 0460-51924-0525 | 0.65 | 7653 | 8000 | 3.03 | 0.31 | -0.50 | 43.37
J034240.63-073504.0 | 0462-51909-0084 | — | — | 19500 | 2.13 | 0.64 | 0.06 | 5.54
J034308.17-064127.3 | 0462-51909-0117 | 1.07 | 14130 | 12000 | 11.43 | 0.00 | -0.50 | 20.09
J041209.32-054031.0 | 0465-51910-0017 | 0.85 | 12121 | 12000 | 32.61 | 0.23 | -0.22 | 6.48
J090343.13+011846.3 | 0470-51929-0403 | — | — | 11000 | 3.10 | 0.12 | 0.00 | 33.47
J092242.42+011422.8 | 0473-51929-0003 | — | — | 30000 | 8.50 | 0.00 | -0.28 | 23.97
J092527.46+011328.6 | 0475-51965-0315 | 0.91 | 10390 | 10500 | 3.05 | 0.08 | -0.47 | 56.99
J094012.88-000009.9 | 0476-52314-0597 | 0.43 | 17240 | 24000 | 2.58 | 0.12 | 0.22 | 18.30
J094945.34+003619.1 | 0480-51989-0045 | — | — | 9500 | 3.00 | 0.00 | 0.38 | 0.33
J094711.11+003754.6 | 0480-51989-0082 | 1.06 | 14898 | 9000 | 2.56 | 0.00 | 0.21 | 89.92
J094351.25+010104.0 | 0480-51989-0251 | — | — | 9500 | 2.19 | erro | -0.20 | 89.08
J084937.77+561949.1 | 0483-51902-0296 | 0.70 | 9831 | 15000 | 2.47 | 0.01 | 0.18 | 4.88
J085309.08+563441.5 | 0483-51924-0203 | 0.50 | 7077 | 10000 | 1.10 | 0.03 | 0.00 | 33.47
J104356.63+650057.2 | 0489-51930-0079 | 1.03 | 13856 | 18000 | 4.10 | 0.03 | 0.00 | 33.47
J104012.21+660520.1 | 0489-51930-0535 | 1.19 | 9557 | 9500 | 2.49 | 0.02 | -0.35 | 59.34
J105628.48+652313.4 | 0490-51929-0205 | 0.49 | 12667 | 18000 | 23.21 | 0.01 | -0.10 | 54.56
J111150.80+663736.2 | 0490-51929-0639 | 0.49 | 16191 | 23000 | 5.50 | — | — | 33.47
J121557.40+665344.5 | 0493-51957-0104 | — | — | 8000 | 2.73 | 0.35 | -0.35 | 5.79
J100005.66+015859.0 | 0500-51994-0557 | — | — | 17000 | 25.52 | 0.11 | 0.31 | 2.06
J100732.63+010914.6 | 0501-52235-0004 | — | — | 9000 | 2.47 | 0.43 | 0.34 | 38.75
J100822.39+015307.4 | 0501-52235-0077 | — | — | 40000 | 3.85 | 0.00 | 0.47 | 4.24
J101206.88+022003.1 | 0502-51957-0495 | — | — | 8000 | 2.20 | 0.01 | 0.19 | 20.12
J101805.04+011123.4 | 0503-51999-0244 | 0.91 | 10329 | 11000 | 122.69 | 15.97 | 0.01 | 65.25
J105332.61+020126.2 | 0507-52353-0113 | 0.36 | 6024 | 8000 | 2.54 | 0.11 | -0.36 | 42.75
J115418.14+011711.5 | 0515-52051-0126 | 1.12 | 26581 | 18000 | 37.35 | 13.80 | -0.31 | 79.10
J121209.31+013627.7 | 0518-52282-0285 | 0.64 | 10554 | 10500 | 10.97 | 0.84 | -0.49 | 45.46
J144649.26+005215.3 | 0537-52027-0126 | — | — | 18500 | 2.10 | 0.00 | 0.17 | 0.80
J144408.75+024327.8 | 0537-52027-0371 | 0.33 | 7772 | 10500 | 2.50 | 0.02 | -0.11 | 24.11
J144934.72+025502.7 | 0537-52027-0566 | 0.71 | 8899 | 8000 | 3.61 | 0.02 | -0.49 | 4.25
J150220.91+001721.1 | 0539-52017-0202 | 0.48 | 7440 | 10000 | 2.20 | 0.02 | 0.00 | 33.47
J074947.00+354055.4 | 0542-51993-0639 | 1.33 | 19628 | 39100 | 30.00 | 0.16 | 0.23 | 6.68
J080743.33+393829.1 | 0545-52202-0009 | — | — | 20000 | 38.00 | 0.17 | 0.26 | 11.63
J082159.66+431127.3 | 0547-52207-0019 | — | — | 22000 | 1.70 | 0.01 | 0.00 | 33.47
J092932.55+561318.4 | 0556-51991-0326 | 0.33 | 7291 | 9000 | 2.26 | 0.38 | 0.18 | 7.67
J095211.45+563020.7 | 0557-52253-0170 | 0.57 | 19045 | 22652 | 2.01 | 0.00 | 0.07 | 69.66
J095919.86+573542.9 | 0558-52317-0158 | — | — | 17500 | 5.08 | 0.02 | 0.15 | 7.35
J105404.37+593333.1 | 0561-52295-0008 | 0.49 | 8316 | 15500 | 18.10 | — | — | 33.47
J084155.73+022350.5 | 0564-52224-0248 | 0.78 | 6942 | 8000 | 3.67 | 0.23 | -0.28 | 9.81
J093508.56+042116.7 | 0569-52264-0452 | — | — | 19500 | 1.30 | 0.01 | 0.00 | 33.47
J094103.84+032835.8 | 0570-52266-0279 | — | — | 25000 | 1.80 | — | — | 33.47
J094815.26+041648.6 | 0570-52266-0632 | — | — | 16500 | 3.30 | 0.18 | 0.36 | 0.16
J101618.37+040920.5 | 0574-52355-0166 | — | — | 12500 | 4.05 | 0.06 | 0.17 | 30.28
J105709.81+041130.3 | 0580-52368-0274 | 0.71 | 8330 | 8000 | 2.77 | 0.19 | -0.34 | 41.45
J142955.20+044005.4 | 0585-52027-0467 | 1.31 | 16401 | 12500 | 2.57 | 0.02 | -0.38 | 67.92
J145029.51+032218.8 | 0587-52026-0016 | 1.08 | 19587 | 22000 | 2.65 | 0.00 | 0.18 | 5.70
J145801.09+040917.0 | 0588-52029-0639 | — | — | 16500 | 3.19 | 0.01 | 0.47 | 13.25
J154135.01+030051.1 | 0594-52045-0253 | — | — | 13500 | 3.60 | 0.02 | 0.00 | 33.47
J154120.14+022756.5 | 0594-52045-0315 | 0.53 | 19164 | 23000 | 3.21 | 0.18 | 0.12 | 14.85
J154213.46+034800.3 | 0594-52045-0400 | 1.05 | 10586 | 9500 | 8.58 | 0.17 | -0.19 | 46.30
J112022.01+635437.4 | 0597-52059-0308 | 0.64 | 7248 | 9500 | 3.24 | 0.69 | 0.47 | 6.99
J133340.34+640627.3 | 0603-52056-0112 | 1.12 | 12859 | 9500 | 7.25 | 0.19 | -0.05 | 13.97
J144614.00+590216.6 | 0608-52081-0140 | — | — | 16000 | 10.21 | 0.07 | 0.31 | 21.27
J145636.32+583321.1 | 0610-52056-0189 | 0.47 | 7226 | 9500 | 2.47 | 1.20 | -0.35 | 54.75
J151745.18+610543.6 | 0613-52345-0446 | — | — | 15000 | 23.79 | 0.09 | 0.36 | 0.68
J153301.51+550840.9 | 0614-53437-0079 | 0.62 | 8804 | 9500 | 3.60 | 0.05 | 0.00 | 33.47
J153315.25+564200.2 | 0614-53437-0579 | 0.75 | 9916 | 11000 | 2.50 | — | — | 33.47
J160437.35+490809.2 | 0622-52054-0330 | 0.86 | 8932 | 9000 | 37.97 | 15.25 | -0.15 | 13.42
J162727.70+492507.9 | 0625-52145-0578 | 0.65 | 7999 | 11000 | 1.10 | 0.01 | 0.00 | 33.47
J204626.15-071036.9 | 0635-52145-0227 | 0.76 | 8388 | 8000 | 2.58 | 0.24 | -0.4 | 46.19
J214930.73-072811.9 | 0644-52173-0350 | 0.84 | 21374 | 23000 | 40.98 | 15.09 | -0.07 | 76.42
J234623.68-102356.9 | 0648-52559-0142 | 0.76 | 8644 | 9500 | 3.00 | 0.07 | -0.32 | 13.84
J004122.49-110432.5 | 0655-52162-0091 | 0.81 | 6770 | 8000 | 2.44 | 0.27 | -0.37 | 11.19
J010654.65-104315.1 | 0659-52199-0207 | — | — | 8500 | 2.81 | 0.22 | -0.19 | 54.68
J224742.57-003317.4 | 0676-52178-0319 | — | — | 30000 | 5.13 | 25.63 | 0.50 | 3.81
J225230.63+003232.6 | 0676-52178-0481 | — | — | 30000 | 5.20 | 1.99 | 0.49 | 10.01
J230758.83+000500.4 | 0678-52884-0498 | — | — | 22000 | 3.12 | 0.01 | 0.08 | 14.96
J230904.69+001803.0 | 0678-52884-0547 | — | — | 8000 | 2.98 | 0.06 | -0.42 | 67.79
J233328.29-002036.6 | 0682-52525-0317 | — | — | 11000 | 2.70 | 0.01 | 0.00 | 33.47
J234710.26+000633.4 | 0683-52524-0520 | 0.97 | 8797 | 9500 | 6.00 | 0.10 | 0.39 | 5.76
J004248.20+001955.2 | 0690-52261-0594 | — | — | 14000 | 8.50 | 0.19 | 0.37 | 23.32
J010225.13-005458.6 | 0693-52254-0099 | 1.33 | 25533 | 22000 | 2.70 | 0.55 | -0.01 | 2.89
J014938.34-004938.0 | 0699-52202-0012 | 0.80 | 24023 | 16000 | 3.26 | 0.01 | 0.48 | 4.02
J015748.19-010600.9 | 0701-52179-0291 | 0.72 | 7228 | 8000 | 2.73 | 0.01 | 0.22 | 1.98
J030417.87-003216.4 | 0709-52205-0107 | 0.36 | 8452 | 14000 | 4.29 | 2.77 | 0.49 | 12.73
J032300.93+002221.4 | 0712-52199-0427 | — | — | 14500 | 2.70 | — | — | 33.47
J213819.85+112311.3 | 0731-52460-0632 | 0.59 | 9561 | 9500 | 2.19 | 0.15 | -0.39 | 3.17
J215148.31+125525.2 | 0733-52207-0522 | — | — | 10000 | 20.71 | 0.26 | -0.17 | 66.83
J224103.29+132853.2 | 0739-52520-0143 | — | — | 23000 | 2.15 | 0.00 | 0.16 | 27.51
J002128.59+150223.7 | 0753-52233-0432 | 0.73 | 7019 | 9000 | 76.49 | 77.59 | -0.46 | 20.21
J075819.57+354443.6 | 0757-52238-0144 | 1.14 | 19664 | 15000 | 25.68 | 5.71 | -0.4 | 20.02
J075842.68+365731.5 | 0757-52238-0439 | 0.39 | 6688 | 8000 | 1.10 | 0.06 | 0.00 | 33.47
J080938.10+373053.8 | 0758-52253-0044 | 0.83 | 12497 | 11398 | 46.42 | 0.21 | -0.10 | 55.43
J082533.22+412400.1 | 0760-52264-0640 | 0.66 | 28554 | 23000 | 2.27 | 0.00 | 0.08 | 9.63
J095603.30+540907.0 | 0769-54530-0078 | 0.50 | 11319 | 14000 | 3.51 | 0.01 | 0.05 | 4.99
J114006.38+611008.1 | 0776-52319-0042 | 0.83 | 17686 | 13000 | 65.78 | 0.21 | -0.03 | 68.25
J120803.25+625815.3 | 0778-54525-0511 | 0.51 | 26238 | 40000 | 3.35 | 0.00 | 0.49 | 10.42
J134017.70+594552.5 | 0786-52319-0254 | 0.41 | 35350 | 35770 | 2.60 | 0.02 | -0.36 | 77.51
J143632.86+563525.2 | 0791-52435-0304 | 0.50 | 6478 | 8500 | 1.10 | 0.03 | 0.00 | 33.47
J153829.29+530604.6 | 0795-52378-0637 | 1.11 | 21158 | 9500 | 16.12 | 0.04 | 0.12 | 61.27
J155857.29+480047.3 | 0813-52354-0328 | 1.07 | 11406 | 10000 | 2.42 | 0.01 | 0.25 | 81.07
J160929.96+443857.1 | 0814-52370-0317 | — | — | 30000 | 1.50 | 0.11 | 0.00 | 33.47
J165203.67+352815.7 | 0820-52438-0299 | 0.63 | 10756 | 18778 | 10.62 | 0.30 | 0.20 | 76.02
J085830.85+412635.0 | 0830-52293-0070 | — | — | 8000 | 2.20 | 0.08 | -0.08 | 45.68
J081130.20+305720.4 | 0861-52318-0096 | 0.43 | 11857 | 9000 | 2.50 | 0.15 | -0.18 | 47.00
J084226.97+374040.1 | 0864-52320-0524 | 0.45 | 12069 | 9500 | 2.78 | 0.21 | -0.36 | 60.38
J105328.13+505155.2 | 0876-52669-0510 | 0.89 | 8090 | 9000 | 2.82 | 0.02 | -0.44 | 56.93
J113357.65+515204.6 | 0879-52365-0586 | 1.22 | 22816 | 22000 | 9.67 | 1.55 | -0.35 | 80.00
J123204.19+522548.2 | 0885-52379-0319 | 0.45 | 8391 | 8183 | 8.16 | 0.04 | -0.13 | 37.40
J074853.07+302543.5 | 0889-52663-0507 | 1.17 | 37325 | 28932 | 8.15 | 1.46 | 0.02 | 35.96
J081018.72+370010.9 | 0892-52378-0374 | 0.77 | 9926 | 9556 | 2.50 | 1.29 | -0.31 | 80.65
J093447.89+503312.1 | 0901-52641-0373 | 0.77 | 8536 | 8946 | 6.61 | 0.52 | -0.10 | 41.23
J100932.74+524638.2 | 0903-52400-0584 | 1.16 | 14442 | 15122 | 2.28 | 0.11 | -0.28 | 81.23
J145602.52-005548.7 | 0921-52380-0528 | 0.49 | 17807 | 20000 | 2.10 | — | — | 33.47
J152855.62-015148.7 | 0925-52411-0312 | — | — | 19500 | 2.40 | 0.00 | 0.18 | 0.31
J082239.54+304857.1 | 0931-52619-0078 | — | — | 17500 | 2.40 | 0.08 | 0.00 | 33.47
J085130.57+353117.6 | 0934-52672-0080 | 0.62 | 6548 | 8000 | 2.50 | 0.21 | -0.07 | 15.82
J091856.12+411317.9 | 0938-52708-0413 | — | — | 9500 | 2.78 | 0.17 | 0.31 | 87.79
J112926.23+493931.8 | 0966-52642-0474 | 0.65 | 9929 | 10000 | 3.05 | 0.23 | -0.50 | 19.54
J113408.25+485601.8 | 0967-52636-0319 | — | — | 40000 | 2.77 | 0.07 | -0.41 | 60.03
J170400.00+321328.5 | 0976-52413-0319 | — | — | 25000 | 3.44 | 0.01 | 0.49 | 5.16
J171831.24+280825.6 | 0980-52431-0434 | — | — | 30000 | 3.01 | 0.38 | 0.43 | 18.20
J205233.51-001610.6 | 0982-52466-0019 | 1.17 | 21947 | 18500 | 15.15 | 0.23 | -0.37 | 60.48
J214539.83+000136.5 | 0990-52465-0080 | — | — | 25000 | 1.80 | 0.95 | 0.00 | 33.47
J101420.37+060254.0 | 0996-52641-0025 | — | — | 19000 | 2.30 | 0.01 | 0.00 | 33.47
J105216.00+530120.3 | 1010-52649-0597 | — | — | 19500 | 2.44 | 0.05 | 0.18 | 0.05
J093200.38+350429.8 | 10244-58225-0112 | — | — | 9500 | 2.19 | 0.01 | -0.22 | 81.50
J073819.64+282126.9 | 10285-58083-0155 | 0.58 | 8447 | 8000 | 2.73 | 0.17 | -0.34 | 60.56
J144345.84+482008.9 | 1047-52733-0099 | 0.80 | 19328 | 22000 | 2.02 | 0.01 | 0.12 | 36.94
J153532.25+421305.5 | 1052-52466-0252 | — | — | 22000 | 2.80 | 0.01 | 0.00 | 33.47
J153742.29+434719.7 | 1052-52466-0619 | — | — | 40000 | 2.86 | 2.62 | 0.24 | 0.85
J161030.50+365442.3 | 1056-52764-0440 | 1.22 | 17214 | 23000 | 2.16 | 0.07 | 0.19 | 27.22
J090451.92+293755.0 | 10667-58163-0282 | — | — | 13000 | 5.35 | 0.10 | -0.50 | 52.99
J222313.51+005446.5 | 1103-52873-0531 | — | — | 8000 | 2.77 | 0.01 | -0.35 | 58.97
J220524.60+010503.3 | 1105-52937-0404 | 1.05 | 12457 | 19000 | 2.49 | 0.01 | -0.17 | 73.94
J214900.86+004842.7 | 1107-52968-0374 | 1.22 | 20497 | 16000 | 11.04 | — | — | 67.43
J014032.41+090520.3 | 11070-58452-0012 | — | — | 10500 | 4.25 | 0.33 | 0.46 | 22.12
J080724.47+260238.3 | 11121-58438-0361 | — | — | 22000 | 8.19 | 0.05 | -0.25 | 27.61
J082141.04+264800.7 | 11125-58433-0906 | 0.75 | 13230 | 15500 | 3.02 | 0.18 | -0.43 | 50.15
J232353.30+060715.7 | 11294-58451-0284 | — | — | 8000 | 15.12 | 0.10 | 0.06 | 60.40
J165249.08+333444.9 | 1175-52791-0095 | 0.53 | 8118 | 8500 | 4.58 | 0.10 | -0.12 | 57.86
J165029.90+341125.4 | 1175-52791-0482 | 0.89 | 9842 | 10500 | 3.05 | 0.02 | -0.50 | 43.28
J081648.70+041223.5 | 1184-52641-0329 | — | — | 15000 | 11.10 | — | — | 33.47
J082231.16+033113.7 | 1184-52641-0637 | 0.67 | 7936 | 8000 | 4.18 | 0.06 | -0.23 | 58.73
J084910.12+044528.7 | 1188-52650-0635 | — | — | 15000 | 2.49 | 0.00 | 0.35 | 6.48
J084628.04+064532.8 | 1189-52668-0344 | — | — | 23000 | 1.30 | — | — | 33.47
J091437.35+054453.3 | 1193-52652-0481 | 1.03 | 20681 | 23420 | 9.23 | 8.77 | -0.08 | 66.59
J091314.47+410838.6 | 1200-52668-0079 | — | — | 19000 | 3.56 | 1.63 | 0.38 | 6.96
J094458.92+453901.1 | 1202-52672-0577 | 1.04 | 17775 | 20000 | 15.42 | 0.08 | 0.16 | 63.31
J082835.81+293448.6 | 1207-52672-0635 | 0.89 | 13786 | 25000 | 33.43 | 0.17 | 0.15 | 36.11
J090746.83+353821.5 | 1212-52703-0187 | 1.05 | 16269 | 19000 | 19.13 | 0.13 | 0.25 | 5.87
J093409.90+392759.3 | 1215-52725-0241 | 0.71 | 9294 | 10985 | 3.08 | 0.13 | -0.49 | 50.00
J110735.31+085924.5 | 1221-52751-0177 | 1.18 | 17097 | 18997 | 2.64 | 0.08 | -0.26 | 56.98
J111812.67+095241.3 | 1222-52763-0477 | 0.98 | 11398 | 14306 | 2.27 | 0.05 | -0.30 | 54.84
J112328.48+095619.4 | 1222-52763-0625 | 0.75 | 9356 | 9000 | 2.25 | 0.05 | -0.30 | 63.16
J101529.62+090703.7 | 1237-52762-0533 | 0.77 | 7102 | 8000 | 2.51 | 0.25 | -0.37 | 2.59
J104113.69+083505.2 | 1240-52734-0105 | — | — | 25000 | 4.04 | 1.33 | 0.48 | 3.98
J090623.50+332108.0 | 1272-52989-0519 | 0.66 | 13739 | 18500 | 3.25 | 0.02 | 0.47 | 4.08
J093411.36+364641.2 | 1275-52996-0174 | — | — | 10500 | 2.23 | 0.06 | -0.29 | 59.76
J145414.99+432149.4 | 1290-52734-0469 | 0.89 | 11400 | 11500 | 3.26 | 0.05 | -0.50 | 45.85
J153057.48+394614.8 | 1293-52765-0613 | — | — | 25000 | 2.20 | 0.01 | 0.50 | 3.65
J083745.12+064313.8 | 1297-52963-0637 | 0.76 | 26780 | 30000 | 4.76 | 0.35 | 0.39 | 15.76
J090632.65+080715.9 | 1300-52973-0148 | 1.17 | 14359 | 40000 | 7.55 | 0.18 | -0.35 | 29.15
J091005.44+081512.2 | 1300-52973-0639 | 0.63 | 27176 | 30000 | 2.42 | 1.29 | 0.11 | 2.24
J091220.25+075537.7 | 1301-52976-0241 | — | — | 15500 | 2.30 | 0.29 | 0.19 | 20.22
J093356.39+102215.6 | 1303-53050-0525 | 0.40 | 7680 | 9075 | 2.58 | 0.23 | -0.38 | 54.90
J113756.50+574022.4 | 1311-52765-0421 | 0.68 | 7507 | 10080 | 5.00 | 0.15 | -0.17 | 13.73
J125415.99+561204.6 | 1318-52781-0299 | 0.86 | 10773 | 11500 | 82.60 | 0.41 | 0.39 | 13.29
J135141.13+541947.2 | 1323-52797-0293 | 0.72 | 10858 | 10180 | 778.51 | 0.00 | 0.16 | 20.40
J142118.19+523547.0 | 1326-52764-0250 | — | — | 25000 | 2.77 | 0.70 | 0.24 | 15.78
J155436.25+413956.6 | 1334-52764-0235 | 0.54 | 11795 | 23000 | 13.14 | 0.08 | 0.31 | 14.28
J163841.66+334302.1 | 1339-52767-0092 | — | — | 9500 | 2.19 | 0.06 | -0.20 | 70.44
J120728.95+440731.6 | 1369-53089-0048 | 0.54 | 15397 | 19000 | 2.16 | 0.01 | 0.12 | 32.10
J143218.25+430126.7 | 1396-53112-0338 | 0.59 | 23596 | 30000 | 2.65 | 0.02 | -0.01 | 43.03
J144541.71+411441.5 | 1397-53119-0352 | — | — | 21000 | 4.29 | 0.84 | 0.49 | 3.68
J150813.26+394505.1 | 1398-53146-0633 | — | — | 29032 | 6.40 | 1.11 | -0.21 | 25.68
J154305.66+343223.6 | 1402-52872-0145 | 1.16 | 29802 | 30620 | 4.98 | 0.12 | 0.47 | 81.04
J160246.45+303914.5 | 1405-52826-0283 | 0.39 | 29982 | 40000 | 3.55 | 0.68 | 0.36 | 8.92
J164357.02+240201.3 | 1414-53135-0191 | 0.61 | 19026 | 23000 | 2.47 | 1.59 | 0.01 | 1.02
J155651.96+351218.9 | 1417-53141-0512 | 0.57 | 7515 | 8000 | 3.07 | 0.10 | -0.50 | 46.10
J103635.00+391814.0 | 1430-53002-0078 | — | — | 8000 | 2.80 | 0.12 | 0.25 | 83.93
J104136.43+404317.8 | 1432-53003-0522 | — | — | 8000 | 2.73 | 0.03 | -0.35 | 9.29
J112714.82+411737.6 | 1443-53055-0302 | 0.58 | 7003 | 8000 | 3.05 | 0.08 | -0.48 | 42.64
J114852.77+430753.1 | 1447-53120-0323 | — | — | 40000 | 2.30 | 0.00 | 0.24 | 6.23
J122249.13+481133.1 | 1451-53117-0582 | 0.78 | 9053 | 9000 | 9.71 | 0.30 | -0.34 | 77.45
J122401.47+415551.9 | 1452-53112-0181 | 0.91 | 9185 | 10000 | 23.65 | 1.21 | -0.28 | 58.89
J124806.37+410427.1 | 1456-53115-0190 | 0.73 | 7258 | 8000 | 4.80 | 0.22 | -0.21 | 7.04
J130214.98+415726.0 | 1458-53119-0490 | 1.24 | 13707 | 17000 | 2.88 | 0.01 | 0.24 | 34.29
J133828.43+415943.8 | 1464-53091-0605 | 0.45 | 12333 | 17500 | 3.24 | 0.66 | 0.46 | 14.23
J140821.99+443008.0 | 1467-53115-0557 | 0.30 | 12368 | 12500 | 3.20 | 0.01 | 0.47 | 7.70
J010214.99+462620.9 | 1472-52913-0278 | — | — | 8033 | 2.58 | 0.15 | -0.38 | 53.48
J164626.65+222645.4 | 1570-53149-0615 | 0.97 | 14822 | 14000 | 2.11 | 0.01 | 0.12 | 1.40
J162808.39+233254.1 | 1573-53226-0099 | 0.78 | 7325 | 8000 | 4.77 | 0.21 | -0.21 | 18.64
J080150.49+205012.0 | 1583-52941-0599 | — | — | 19000 | 2.18 | 0.00 | 0.17 | 22.86
J080502.28+215320.5 | 1584-52943-0132 | — | — | 37141 | 6.77 | 0.17 | -0.49 | 66.27
J084008.49+271242.6 | 1587-52964-0059 | 0.82 | 10948 | 12500 | 11.19 | 0.36 | -0.44 | 69.48
J084929.10+285720.3 | 1588-52965-0565 | 1.09 | 13796 | 15500 | 28.00 | 0.77 | 0.17 | 12.57
J101519.32+114724.1 | 1597-52999-0531 | — | — | 11500 | 2.77 | 0.00 | -0.37 | 76.73
J123414.11+124829.5 | 1616-53169-0423 | 0.45 | 8053 | 8544 | 2.26 | 0.58 | -0.50 | 1.88
J115554.94+083549.5 | 1622-53385-0447 | 0.74 | 8385 | 9888 | 3.04 | 0.10 | -0.46 | 59.81
J120609.81+081323.7 | 1623-53089-0573 | 0.86 | 10057 | 16000 | 449.10 | 35.47 | 0.01 | 51.31
J152934.98+292801.8 | 1652-53555-0436 | 0.96 | 11097 | 10000 | 2.82 | 0.29 | -0.44 | 67.06
J161118.59+242446.6 | 1657-53520-0372 | 0.53 | 8361 | 11000 | 1.30 | 0.04 | 0.0 | 33.47
J203828.47+764123.1 | 1661-53240-0023 | 0.48 | 12071 | 16000 | 2.16 | 0.23 | 0.15 | 14.78
J203016.12+765022.6 | 1661-53240-0116 | — | — | 14000 | 3.04 | 0.02 | 0.07 | 25.19
J201822.88+754807.6 | 1661-53240-0124 | — | — | 14500 | 2.61 | 1.56 | 0.21 | 6.60
J232937.54+524437.8 | 1663-52973-0119 | 0.59 | 17226 | 32204 | 2.24 | 0.05 | -0.31 | 74.89
J132538.57+515152.2 | 1668-53433-0326 | — | — | 10000 | 3.15 | 0.01 | 0.45 | 13.00
J141808.12+481850.6 | 1672-53460-0181 | 0.32 | 11963 | 13000 | 2.28 | 0.04 | -0.32 | 73.22
J151102.74+433558.7 | 1677-53148-0151 | — | — | 13000 | 2.19 | 0.00 | 0.14 | 2.10
J153554.17+404414.2 | 1679-53149-0109 | — | — | 30000 | 2.39 | 0.01 | 0.22 | 6.36
J170657.89+232118.9 | 1687-53260-0019 | 0.37 | 19077 | 24000 | 3.31 | 0.30 | 0.09 | 17.17
J170916.36+234111.3 | 1688-53462-0508 | 0.41 | 7874 | 18500 | 4.27 | 0.31 | 0.19 | 33.14
J165538.92+253346.2 | 1692-53473-0163 | — | — | 15500 | 2.76 | 4.34 | 0.32 | 39.02
J165354.57+251738.4 | 1692-53473-0213 | — | — | 19000 | 1.20 | — | — | 33.47
J170019.41+245701.3 | 1693-53446-0169 | — | — | 30000 | 2.02 | 0.00 | 0.18 | 25.83
J124819.86+133555.5 | 1694-53472-0564 | 1.03 | 19582 | 13000 | 2.14 | 0.01 | -0.25 | 82.57
J133007.57+104830.5 | 1699-53148-0137 | 0.57 | 7172 | 8000 | 2.16 | 0.08 | -0.09 | 47.51
J143308.49+102623.0 | 1709-53533-0511 | 0.78 | 6698 | 8000 | 2.49 | 0.22 | -0.37 | 18.51
J153843.10+084238.2 | 1725-54266-0297 | 0.91 | 9060 | 33803 | 12.66 | 0.27 | 0.03 | 43.78
J155932.57+081904.6 | 1728-53228-0175 | 0.40 | 10187 | 13000 | 1.30 | 0.01 | 0.00 | 33.47
J155651.11+085003.5 | 1728-53228-0374 | 0.67 | 10515 | 10500 | 2.19 | 0.04 | -0.14 | 74.13
J160852.00+064437.0 | 1730-53498-0252 | 0.83 | 8655 | 8500 | 24.86 | 0.14 | -0.24 | 73.69
J161658.43+070355.4 | 1731-53884-0442 | — | — | 12500 | 3.19 | 0.44 | 0.46 | 25.95
J162115.34+075059.0 | 1732-53501-0455 | 0.81 | 14816 | 12000 | 2.19 | 0.01 | 0.29 | 34.17
J090150.74+091211.4 | 1738-53051-0002 | 0.66 | 9219 | 11000 | 2.67 | 0.12 | -0.35 | 55.18
J100715.55+123709.4 | 1745-53061-0313 | 0.80 | 21864 | 23000 | 5.08 | 1.55 | 0.11 | 0.87
J080719.89+064536.6 | 1756-53080-0234 | — | — | 21000 | 2.14 | 0.11 | 0.15 | 17.84
J081144.59+071030.5 | 1756-53080-0585 | 0.60 | 16080 | 17000 | 2.13 | 0.00 | 0.13 | 2.79
J082239.43+082436.7 | 1758-53084-0346 | 0.91 | 10039 | 10500 | 2.57 | 0.18 | -0.35 | 69.08
J083002.71+083631.9 | 1758-53084-0531 | 0.68 | 15378 | 12500 | 3.01 | 0.00 | 0.44 | 18.55
J084253.04+092226.5 | 1759-53081-0618 | 0.39 | 12670 | 11500 | 3.40 | 0.08 | 0.05 | 5.39
J115345.96+133106.6 | 1762-53415-0042 | 0.55 | 12173 | 19000 | 2.45 | — | — | 33.47
J114827.96+153356.9 | 1762-53415-0372 | — | — | 16000 | 2.17 | 0.56 | 0.15 | 1.85
J120806.25+144942.8 | 1764-53467-0112 | — | — | 18000 | 4.70 | 0.02 | 0.00 | 33.47
J123527.08+145318.6 | 1768-53442-0074 | 0.25 | 13281 | 16500 | 2.06 | 0.02 | 0.11 | 22.21
J123449.88+150348.8 | 1768-53442-0557 | 0.69 | 6125 | 8000 | 8.22 | 0.30 | -0.06 | 5.68
J125044.42+154957.3 | 1770-53171-0530 | 0.48 | 8073 | 10000 | 21.51 | 1.66 | -0.42 | 40.30
J125553.38+152555.0 | 1771-53498-0343 | 0.47 | 18411 | 22000 | 12.88 | 0.05 | 0.26 | 33.17
J131050.04+143520.4 | 1772-53089-0559 | — | — | 40000 | 4.15 | 0.00 | 0.48 | 2.18
J132002.47+131901.5 | 1773-53112-0011 | 0.20 | 10388 | 21000 | 3.17 | 0.96 | 0.04 | 4.27
J155620.60+055029.4 | 1822-53172-0139 | — | — | 8000 | 42.00 | 0.01 | 0.27 | 18.87
J155857.68+041704.8 | 1837-53494-0261 | 0.91 | 6912 | 8000 | 69.82 | 15.31 | -0.16 | 9.63
J135654.77+343617.2 | 1838-53467-0240 | — | — | 30000 | 9.30 | 2.32 | 0.50 | 2.96
J151625.06+280320.9 | 1846-54173-0280 | 0.64 | 7877 | 8000 | 2.30 | 0.07 | 0.00 | 33.47
J154605.40+243759.0 | 1850-53786-0312 | 0.74 | 6327 | 8000 | 1.10 | 0.11 | 0.00 | 33.47
J155657.69+231358.5 | 1851-53524-0298 | 0.47 | 19183 | 13000 | 3.27 | 0.05 | 0.48 | 12.55
J155818.96+241758.7 | 1851-53524-0476 | 1.15 | 11841 | 17500 | 7.19 | 0.89 | 0.13 | 8.91
J161047.77+235301.8 | 1852-53534-0567 | — | — | 14500 | 3.40 | 0.85 | 0.50 | 4.57
J074403.80+495439.9 | 1868-53318-0410 | — | — | 36390 | 2.99 | 0.04 | -0.48 | 50.36
J235503.83+350659.7 | 1881-53261-0042 | — | — | 22000 | 2.84 | 0.01 | 0.29 | 0.18
J235431.39+365019.1 | 1881-53261-0512 | — | — | 10500 | 3.00 | 0.01 | -0.24 | 73.86
J235318.56+380913.2 | 1883-53271-0050 | 1.27 | 11242 | 11500 | 2.39 | 0.12 | -0.32 | 70.42
J234605.44+385337.6 | 1883-53271-0272 | 1.17 | 24692 | 14500 | 45.00 | 8.92 | -0.34 | 4.71
J235107.47+403453.9 | 1883-53271-0521 | — | — | 15000 | 2.65 | 0.06 | 0.20 | 16.55
J233039.03+500729.6 | 1889-53240-0377 | 0.32 | 11580 | 14500 | 1.20 | 1.26 | 0.00 | 33.47
J233708.96+492532.0 | 1889-53240-0584 | 0.72 | 10404 | 9500 | 2.08 | 0.12 | -0.28 | 74.99
J211125.84+110219.6 | 1890-53237-0390 | 1.12 | 15912 | 11000 | 2.82 | 0.35 | -0.50 | 32.99
J224707.31+010058.5 | 1901-53261-0564 | — | — | 11000 | 2.19 | 0.01 | -0.29 | 75.73
J004148.05-005127.3 | 1905-53706-0253 | — | — | 22000 | 4.39 | 1.69 | 0.48 | 1.40
J014230.56+003502.7 | 1907-53315-0427 | — | — | 13000 | 2.57 | 0.02 | 0.36 | 20.90
J093126.14+321946.1 | 1943-53386-0294 | — | — | 18000 | 12.95 | 0.06 | 0.28 | 0.89
J100657.51+303338.0 | 1953-53358-0415 | 0.62 | 10043 | 10500 | 3.23 | 0.07 | -0.50 | 35.94
J101339.46+352639.6 | 1954-53357-0250 | — | — | 21000 | 2.21 | 0.91 | 0.07 | 5.78
J101428.08+365724.5 | 1954-53357-0393 | 0.74 | 10647 | 11000 | 14.93 | 1.14 | -0.36 | 72.58
J101847.14+304018.0 | 1956-53437-0143 | — | — | 30000 | 3.05 | 0.04 | -0.49 | 50.98
J101834.81+303330.4 | 1956-53437-0197 | 1.15 | 21262 | 21000 | 2.70 | 0.61 | -0.32 | 72.28
J103935.51+295413.5 | 1969-53383-0215 | 1.12 | 12629 | 14388 | 2.40 | 0.01 | 0.32 | 88.17
J113804.15+305310.6 | 1974-53430-0023 | — | — | 16500 | 11.77 | 0.02 | 0.28 | 0.86
J113048.38+305720.6 | 1974-53430-0222 | 0.91 | 10229 | 10000 | 3.08 | 0.01 | -0.50 | 47.33
J112257.10+322327.7 | 1979-53431-0512 | 0.98 | 12687 | 11500 | 12.87 | 0.15 | -0.28 | 50.74
J112014.62+400422.6 | 1980-53433-0630 | 1.10 | 12155 | 10000 | 2.54 | 0.01 | -0.36 | 72.97
J122748.85+385546.3 | 1986-53475-0090 | 1.14 | 16615 | 13000 | 8.44 | 0.28 | -0.50 | 62.18
J125101.98+351913.6 | 1987-53765-0570 | 0.87 | 17874 | 25000 | 2.25 | 1.58 | -0.12 | 0.13
J110203.75+400558.0 | 1988-53469-0434 | 0.96 | 9067 | 10000 | 2.11 | 0.03 | 0.13 | 0.01
J125434.64+371000.1 | 1989-53772-0041 | 0.74 | 20196 | 25365 | 2.64 | 5.11 | -0.28 | 0.95
J125709.63+304317.2 | 1994-53845-0067 | 0.95 | 10202 | 9500 | 2.44 | 0.07 | -0.30 | 84.23
J121529.84+335158.6 | 1999-53503-0238 | 0.58 | 16490 | 25000 | 2.60 | 2.20 | 0.17 | 0.26
J120924.84+331716.3 | 2004-53737-0418 | 0.38 | 6663 | 8000 | 4.03 | 0.23 | -0.26 | 8.16
J125715.53+341439.3 | 2006-53476-0332 | 0.90 | 9697 | 9500 | 22.40 | 3.91 | 0.37 | 89.83
J105152.18+321135.2 | 2026-53711-0183 | 1.21 | 20427 | 20000 | 1.30 | — | — | 33.47
J021148.21+211548.2 | 2046-53327-0048 | 1.00 | 11160 | 12986 | 167.11 | 41.51 | -0.31 | 36.45
J030407.39-002541.9 | 2048-53378-0280 | 0.78 | 12676 | 9500 | 10.48 | 1.37 | -0.07 | 49.81
J080527.55+073534.4 | 2056-53463-0557 | — | — | 8000 | 1.10 | 0.05 | 0.00 | 33.47
J004254.23+235831.5 | 2058-53349-0087 | — | — | 10500 | 2.03 | 0.01 | 0.18 | 10.42
J004038.89+243852.7 | 2058-53349-0195 | — | — | 10500 | 2.52 | 0.01 | -0.36 | 78.46
J011739.82+242236.2 | 2060-53706-0086 | 0.54 | 11292 | 10000 | 2.41 | 0.04 | -0.28 | 75.24
J012115.44+321010.3 | 2061-53711-0506 | — | — | 23000 | 2.96 | 0.41 | 0.02 | 5.59
J012105.53+393239.7 | 2062-53381-0337 | 0.79 | 25869 | 21640 | 2.09 | 0.00 | -0.14 | 70.73
J012815.71+391130.1 | 2063-53359-0063 | — | — | 17000 | 2.05 | 0.02 | 0.11 | 2.86
J012339.94+405241.9 | 2063-53359-0403 | — | — | 50000 | 4.60 | 0.04 | 0.00 | 33.47
J014313.18+231524.5 | 2064-53341-0024 | — | — | 22000 | 3.00 | 0.00 | 0.40 | 7.55
J013909.14+230844.9 | 2064-53341-0163 | — | — | 15500 | 3.33 | 0.00 | 0.45 | 3.62
J013314.21+235247.4 | 2064-53341-0343 | — | — | 40000 | 9.00 | 0.10 | -0.17 | 37.96
J013742.53+235138.2 | 2064-53341-0491 | — | — | 11500 | 3.00 | 0.04 | 0.37 | 0.24
J020316.65+220527.2 | 2066-53349-0302 | — | — | 11000 | 2.42 | 0.01 | 0.19 | 0.33
J030647.72+010949.8 | 2068-53386-0401 | — | — | 16000 | 3.08 | 0.09 | 0.30 | 22.83
J040054.81-064625.2 | 2071-53741-0014 | — | — | 20000 | 4.39 | 0.34 | 0.18 | 9.89
J053317.32-004321.9 | 2072-53430-0096 | — | — | 40000 | 16.89 | 0.58 | 0.27 | 7.72
J053016.83-001034.4 | 2072-53430-0233 | — | — | 19000 | 2.34 | 0.02 | 0.18 | 0.32
J052831.02+005244.3 | 2072-53430-0336 | — | — | 16444 | 2.57 | 0.05 | 0.24 | 62.18
J053126.75+001738.1 | 2072-53430-0427 | — | — | 13000 | 2.06 | 0.02 | 0.11 | 15.24
J053507.04+001617.0 | 2072-53430-0508 | — | — | 18000 | 2.42 | 0.01 | 0.17 | 41.67
J073135.36+353108.5 | 2073-53728-0108 | — | — | 24000 | 2.05 | 0.00 | 0.03 | 1.96
J073001.65+362713.2 | 2073-53728-0482 | 0.78 | 16142 | 10000 | 2.77 | 0.02 | 0.33 | 84.48
J073237.67+364628.8 | 2073-53728-0571 | 1.34 | 27417 | 20000 | 108.72 | 28.00 | -0.03 | 69.82
J074047.65+180907.3 | 2074-53437-0237 | 0.77 | 22775 | 23000 | 1.70 | 0.36 | 0.00 | 33.47
J074327.09+273732.4 | 2075-53730-0278 | — | — | 9500 | 2.28 | 0.05 | -0.31 | 69.75
J080905.97+062441.7 | 2076-53442-0076 | 0.18 | 9903 | 18000 | 2.25 | 0.09 | 0.18 | 87.64
J080638.50+075647.5 | 2076-53442-0521 | — | — | 21000 | 2.11 | 0.69 | -0.26 | 56.26
J073953.17+204900.2 | 2079-53379-0051 | — | — | 22000 | 2.01 | 0.03 | 0.11 | 15.63
J074958.58+161120.2 | 2080-53350-0349 | — | — | 24000 | 2.09 | 0.00 | 0.03 | 5.77
J080440.35+182730.9 | 2081-53357-0442 | 0.89 | 9749 | 10135 | 38.26 | 25.56 | -0.12 | 16.04
J081716.39+200834.9 | 2082-53358-0444 | 0.74 | 6901 | 8000 | 3.78 | 0.21 | -0.28 | 9.66
J082107.34+194433.6 | 2082-53358-0617 | — | — | 25000 | 1.30 | — | — | 33.47
J083041.77+204233.7 | 2083-53359-0553 | 1.00 | 18687 | 17500 | 2.19 | 0.06 | -0.19 | 77.75
J083918.12+212143.7 | 2084-53360-0100 | 1.05 | 12139 | 13500 | 3.40 | — | — | 33.47
J084936.81+224754.9 | 2085-53379-0131 | 1.08 | 29177 | 25000 | 2.10 | 0.49 | 0.12 | 9.03
J090937.94+250820.6 | 2086-53401-0582 | 0.86 | 10024 | 10500 | 2.52 | 0.10 | -0.39 | 50.91
J091305.58+260748.5 | 2087-53415-0383 | — | — | 16000 | 2.30 | 0.00 | 0.18 | 19.84
J120547.47+340811.4 | 2089-53498-0431 | 0.74 | 18605 | 17500 | 9.74 | 0.07 | -0.35 | 60.80
J105833.57+372401.3 | 2091-53447-0464 | 0.90 | 11395 | 9500 | 2.55 | 0.04 | 0.19 | 84.90
J115817.44+331719.2 | 2095-53474-0337 | — | — | 24000 | 2.03 | 0.00 | 0.11 | 4.10
J140051.72+330754.3 | 2121-54180-0369 | 0.56 | 23055 | 30000 | 3.15 | 1.04 | 0.28 | 5.69
J141813.21+312340.0 | 2129-54252-0426 | 0.68 | 7457 | 8000 | 2.55 | 0.12 | -0.37 | 17.57
J141906.19+254356.4 | 2131-53819-0317 | 0.83 | 9205 | 9500 | 2.27 | 0.30 | -0.30 | 60.26
J143019.05+281100.8 | 2134-53876-0423 | 0.94 | 9052 | 9000 | 7.26 | 1.09 | -0.15 | 18.21
J151606.34+274647.0 | 2154-54539-0637 | 0.87 | 67365 | 30000 | 3.03 | 0.06 | -0.44 | 75.43
J152203.44+203438.9 | 2156-54525-0031 | 0.45 | 17315 | 14000 | 2.98 | 0.03 | 0.26 | 0.85
J154856.93+230727.9 | 2169-53556-0491 | — | — | 9732 | 2.81 | 0.10 | -0.42 | 62.80
J163600.24+354625.3 | 2185-53532-0320 | 0.46 | 17391 | 25000 | 9.97 | 3.71 | 0.48 | 3.71
J161344.78+174609.0 | 2188-54595-0406 | 0.29 | 13175 | 15500 | 2.96 | 0.09 | 0.43 | 32.14
J165651.45+243802.7 | 2191-54621-0608 | 0.26 | 11866 | 10500 | 2.54 | 0.00 | -0.34 | 69.36
J165439.46+391103.3 | 2192-54232-0310 | 0.66 | 8296 | 9500 | 2.43 | 0.01 | -0.24 | 60.16
J172735.80+280536.8 | 2193-53888-0570 | 0.45 | 18057 | 18084 | 2.14 | 0.06 | 0.22 | 87.87
J174755.71+251232.3 | 2194-53904-0154 | 0.67 | 10993 | 10500 | 2.29 | 0.03 | -0.30 | 84.15
J161321.40+155332.0 | 2198-53918-0400 | 0.57 | 10983 | 9500 | 3.30 | 0.02 | 0.47 | 4.03
J161147.94+211136.6 | 2205-53793-0542 | 0.66 | 11382 | 10000 | 2.19 | 0.00 | 0.23 | 5.58
J163400.34+145651.3 | 2209-53907-0472 | — | — | 15500 | 5.50 | 0.00 | 0.25 | 8.55
J112439.29+262422.7 | 2216-53795-0143 | 1.03 | 21151 | 10500 | 2.33 | 0.01 | 0.32 | 79.21
J113055.04+260115.6 | 2218-53816-0081 | — | — | 24000 | 2.40 | 0.01 | 0.00 | 33.47
J113215.38+280934.3 | 2219-53816-0329 | — | — | 8000 | 2.77 | 0.16 | -0.33 | 9.00
J113500.52+291206.5 | 2220-53795-0222 | — | — | 25000 | 2.02 | 0.01 | 0.03 | 2.30
J114529.26+300824.3 | 2222-53799-0483 | 0.54 | 14836 | 15000 | 3.33 | 0.02 | 0.49 | 5.41
J114833.24+303921.2 | 2222-53799-0577 | 0.49 | 9411 | 18000 | 2.65 | 0.24 | 0.32 | 42.73
J114917.22+300016.0 | 2222-53799-0593 | 0.30 | 9344 | 9000 | 2.75 | 0.08 | -0.37 | 65.19
J130535.77+283014.5 | 2242-54153-0447 | — | — | 24000 | 2.42 | 0.01 | 0.17 | 29.06
J131544.04+262333.3 | 2243-53794-0170 | 0.85 | 8872 | 12000 | 3.56 | 0.00 | 0.48 | 3.15
J131702.34+281848.6 | 2243-53794-0533 | 0.40 | 11819 | 9500 | 2.27 | 0.01 | -0.21 | 64.31
J132926.04+254936.4 | 2245-54208-0307 | 1.37 | 28492 | 28299 | 2.61 | 0.18 | -0.39 | 54.04
J202501.10+131025.6 | 2257-53612-0167 | 0.56 | 13790 | 28932 | 10.06 | 0.69 | 0.15 | 10.28
J203256.47+142652.1 | 2258-54328-0278 | — | — | 24000 | 3.50 | 1.73 | 0.38 | 49.60
J203332.93+140115.4 | 2258-54328-0295 | — | — | 18529 | 2.16 | 0.01 | -0.15 | 87.96
J205000.93+170145.5 | 2259-53565-0530 | — | — | 22000 | 3.11 | 0.70 | 0.06 | 8.12
J224829.60+223355.9 | 2261-53612-0075 | — | — | 10000 | 37.11 | 3.43 | -0.32 | 0.64
J224602.81+230704.1 | 2261-53612-0559 | 0.77 | 17130 | 15500 | 2.06 | 0.06 | 0.18 | 0.34
J080359.93+122943.9 | 2265-53674-0033 | — | — | 12347 | 33.29 | 4.86 | -0.35 | 16.97
J075816.63+121428.6 | 2265-53674-0199 | 0.79 | 13521 | 10000 | 2.50 | 0.03 | -0.35 | 71.82
J080210.39+153033.8 | 2266-53679-0534 | 0.99 | 17869 | 19000 | 2.01 | 0.01 | 0.11 | 19.88
J080703.25+135537.8 | 2268-53682-0472 | 0.54 | 11082 | 20000 | 2.81 | 0.25 | 0.02 | 3.97
J081748.55+154341.1 | 2272-53713-0386 | 0.52 | 12054 | 11000 | 1.80 | — | — | 33.47
J082817.60+181752.6 | 2275-53709-0298 | 0.77 | 20127 | 13000 | 2.19 | 0.01 | 0.13 | 31.43
J083613.81+201852.1 | 2275-53709-0526 | — | — | 9500 | 2.96 | 0.02 | -0.33 | 71.70
J083701.89+154454.6 | 2276-53712-0004 | 0.97 | 21399 | 17000 | 3.00 | 0.01 | 0.43 | 8.66
J083627.34+154850.3 | 2276-53712-0107 | 1.09 | 36312 | 30000 | 5.03 | 4.59 | 0.5 | 3.75
J083623.85+163859.6 | 2278-53711-0270 | 1.10 | 13998 | 11000 | 2.58 | 0.11 | -0.38 | 53.83
J085129.15+195205.4 | 2280-53680-0018 | 0.85 | 8724 | 9500 | 3.00 | 0.02 | -0.42 | 75.49
J084845.65+214047.0 | 2280-53680-0446 | 0.62 | 20534 | 24000 | 3.43 | 1.14 | 0.37 | 17.55
J090522.06+205736.2 | 2284-53708-0091 | 0.43 | 10902 | 19000 | 2.21 | 0.73 | 0.13 | 52.90
J090554.63+213829.5 | 2284-53708-0103 | 0.33 | 18045 | 30000 | 2.10 | 0.06 | 0.00 | 33.47
J090907.15+193840.6 | 2286-53700-0176 | — | — | 14000 | 2.99 | 0.01 | 0.43 | 27.95
J091132.79+223200.6 | 2287-53705-0169 | 0.76 | 11884 | 11500 | 3.07 | 0.01 | 0.40 | 0.40
J091002.83+232219.9 | 2287-53705-0470 | — | — | 21000 | 2.28 | 0.56 | -0.03 | 18.84
J091310.43+230042.6 | 2287-53705-0541 | — | — | 23000 | 2.10 | 1.20 | 0.08 | 4.79
J091326.64+211250.4 | 2288-53699-0332 | 0.61 | 13537 | 15500 | 2.23 | 0.01 | 0.26 | 84.06
J091526.57+205039.1 | 2288-53699-0468 | — | — | 11000 | 2.05 | 0.02 | 0.11 | 33.14
J093059.15+202429.3 | 2289-53708-0069 | 0.61 | 10459 | 15000 | 3.19 | 0.39 | 0.43 | 16.14
J092355.96+243552.8 | 2291-53714-0552 | — | — | 17000 | 5.34 | 0.24 | 0.25 | 30.87
J094025.97+201707.2 | 2292-53713-0048 | — | — | 10500 | 2.00 | 0.01 | 0.00 | 33.47
J093654.94+262650.2 | 2294-54524-0617 | — | — | 23000 | 3.73 | 1.87 | 0.38 | 9.85
J055814.96+643826.5 | 2301-53712-0344 | — | — | 12000 | 3.00 | 0.00 | 0.44 | 8.97
J060442.48+641357.1 | 2301-53712-0476 | 0.78 | 21586 | 13000 | 20.75 | 0.89 | -0.44 | 18.59
J053400.83+625419.7 | 2302-53709-0579 | — | — | 8000 | 2.19 | 0.02 | 0.13 | 62.91
J225726.05+075541.6 | 2310-53710-0420 | — | — | 9500 | 17.40 | 9.54 | -0.44 | 40.16
J091833.32+205536.9 | 2319-53763-0209 | — | — | 15584 | 2.55 | 0.42 | -0.28 | 75.50
J091629.56+215011.4 | 2319-53763-0236 | 0.69 | 5883 | 8000 | 6.19 | 0.20 | -0.15 | 24.48
J092041.53+221545.4 | 2319-53763-0557 | — | — | 24000 | 2.09 | 0.01 | -0.10 | 49.93
J092246.94+230812.6 | 2319-53763-0567 | — | — | 21000 | 2.61 | 0.02 | 0.20 | 57.24
J212329.46-081004.4 | 2320-54653-0090 | — | — | 15500 | 2.29 | 0.52 | 0.13 | 18.30
J211744.74-073652.8 | 2320-54653-0312 | — | — | 32642 | 2.48 | 0.03 | -0.40 | 26.25
J212143.07-060005.7 | 2320-54653-0445 | 0.77 | 17082 | 25075 | 1.94 | 0.03 | -0.10 | 53.26
J212232.58-061839.6 | 2320-54653-0537 | — | — | 10500 | 3.00 | 0.03 | 0.41 | 0.86
J212425.74-064837.2 | 2320-54653-0544 | 0.77 | 9638 | 16822 | 2.30 | 0.01 | 0.29 | 89.23
J212514.18-062152.5 | 2320-54653-0612 | — | — | 17000 | 2.10 | 1.39 | 0.15 | 4.36
J021338.51+053023.3 | 2321-53711-0125 | — | — | 8500 | 2.42 | 0.02 | -0.29 | 67.74
J021107.71+072235.4 | 2321-53711-0409 | — | — | 14000 | 2.19 | 0.01 | 0.28 | 28.13
J030522.15+050213.3 | 2322-53727-0024 | 0.49 | 8987 | 13500 | 2.95 | 0.67 | 0.43 | 9.01
J030107.56+053956.9 | 2322-53727-0136 | — | — | 18000 | 2.29 | 0.05 | -0.17 | 58.18
J004011.48+070255.6 | 2327-53710-0074 | 0.82 | 12408 | 12000 | 3.12 | 0.06 | 0.42 | 8.42
J003223.65+082329.5 | 2327-53710-0321 | 0.69 | 9072 | 11000 | 2.19 | 0.01 | -0.31 | 47.14
J012215.76+082712.7 | 2329-53725-0370 | — | — | 8000 | 2.57 | 0.02 | -0.36 | 82.14
J083310.56+234812.7 | 2330-53738-0109 | — | — | 10500 | 3.00 | 0.00 | 0.44 | 17.77
J083051.08+244615.7 | 2330-53738-0503 | — | — | 11000 | 2.29 | 0.01 | -0.31 | 81.05
J083531.17+533230.8 | 2331-53742-0197 | 0.78 | 8379 | 8000 | 14.40 | 4.25 | -0.46 | 10.46
J032658.77+040307.9 | 2339-53729-0046 | 1.32 | 27169 | 13000 | 2.82 | 0.21 | -0.42 | 68.94
J032628.17+052136.2 | 2339-53729-0515 | 0.92 | 21233 | 16000 | 15.95 | 0.52 | -0.49 | 20.38
J031058.73+045129.9 | 2340-53733-0165 | 0.51 | 9918 | 9000 | 2.55 | 0.03 | -0.27 | 80.11
J100426.98+223810.5 | 2343-53735-0300 | — | — | 10500 | 2.29 | 0.01 | 0.29 | 75.82
J101642.26+281610.2 | 2348-53757-0040 | 0.91 | 25367 | 25000 | 2.16 | 0.00 | 0.07 | 6.60
J100727.32+281457.8 | 2348-53757-0279 | — | — | 11500 | 2.07 | 0.00 | 0.12 | 29.33
J101059.21+284359.6 | 2348-53757-0485 | — | — | 19000 | 2.00 | — | — | 33.47
J102220.69+272539.8 | 2350-53765-0543 | 1.20 | 16227 | 17000 | 8.23 | 0.93 | 0.42 | 17.63
J102535.39+282034.8 | 2351-53772-0007 | — | — | 24000 | 2.38 | 0.01 | -0.12 | 10.24
J102429.16+281435.4 | 2351-53786-0001 | 0.31 | 11778 | 21000 | 2.20 | 0.81 | -0.22 | 59.98
J103403.98+305034.4 | 2354-53799-0536 | 0.74 | 15302 | 12500 | 2.77 | 0.02 | 0.27 | 1.27
J104851.93+273817.6 | 2358-53797-0156 | — | — | 9000 | 2.03 | 0.02 | 0.14 | 28.23
J092524.25+175712.6 | 2360-53728-0217 | 0.53 | 12343 | 17314 | 2.00 | 0.01 | -0.26 | 81.68
J093726.27+205756.9 | 2361-53762-0408 | 1.05 | 12875 | 18000 | 5.44 | 0.01 | 0.13 | 58.49
J095738.55+194601.8 | 2363-53763-0097 | — | — | 18000 | 2.09 | 0.00 | 0.14 | 8.03
J100828.97+183633.4 | 2373-53768-0290 | 0.71 | 10047 | 13000 | 2.38 | 0.00 | 0.17 | 2.09
J102239.05+194904.2 | 2374-53765-0544 | 0.89 | 9002 | 9000 | 3.23 | 0.16 | -0.50 | 47.12
J103350.87+204729.3 | 2376-53770-0463 | 1.12 | 15958 | 16500 | 10.91 | 0.15 | -0.49 | 27.32
J103532.53+212603.5 | 2376-53770-0534 | — | — | 8000 | 2.77 | 0.15 | -0.35 | 18.17
J024903.01+332737.0 | 2398-53768-0313 | 0.26 | 11136 | 9500 | 2.66 | 0.02 | -0.26 | 85.98
J023542.72+241653.7 | 2399-53764-0030 | — | — | 9500 | 2.33 | 0.00 | 0.17 | 85.49
J023449.24+240750.2 | 2399-53764-0070 | 0.55 | 5419 | 8000 | 3.59 | 0.16 | -0.29 | 15.23
J023035.63+250831.5 | 2399-53764-0164 | 0.55 | 5662 | 8000 | 4.19 | 0.17 | -0.25 | 16.87
J023157.00+264837.5 | 2399-53764-0426 | 1.10 | 11056 | 9500 | 2.29 | 1.57 | -0.19 | 70.17
J023445.31+260553.1 | 2399-53764-0487 | — | — | 13000 | 6.65 | 1.37 | 0.04 | 5.79
J023420.62+264801.6 | 2399-53764-0559 | 0.82 | 13560 | 40000 | 30.78 | 3.45 | -0.02 | 13.13
J085403.30+361121.3 | 2400-53765-0291 | 0.62 | 9880 | 10500 | 2.57 | 0.17 | -0.35 | 82.77
J093813.82+615600.8 | 2403-53795-0278 | 1.07 | 19840 | 10500 | 2.49 | 0.01 | 0.22 | 8.34
J094210.10+521313.3 | 2404-53764-0058 | 0.56 | 8045 | 8000 | 2.57 | 0.14 | -0.39 | 49.68
J105732.05+480125.9 | 2410-54087-0117 | 1.01 | 11795 | 16000 | 2.29 | 0.01 | -0.32 | 88.98
J105556.92+483652.4 | 2410-54087-0494 | — | — | 9500 | 2.19 | 0.00 | -0.28 | 66.87
J111608.80+092532.5 | 2413-54169-0151 | 0.55 | 5212 | 8000 | 1.40 | 0.06 | -0.19 | 17.69
J110911.12+582209.3 | 2414-54526-0301 | — | — | 30000 | 2.95 | 1.02 | 0.23 | 37.43
J111010.50+600141.3 | 2414-54526-0323 | 1.23 | 32216 | 19500 | 8.12 | 0.02 | -0.5 | 50.70
J031929.01+410316.9 | 2417-53766-0064 | — | — | 10000 | 3.15 | 0.00 | 0.46 | 1.01
J031824.19+422651.0 | 2417-53766-0568 | 0.89 | 11285 | 8500 | 8.48 | 0.99 | 0.03 | 44.11
J082447.49+131543.2 | 2422-54096-0588 | — | — | 22000 | 1.70 | 0.23 | 0.00 | 33.47
J083420.29+131759.5 | 2426-53795-0387 | — | — | 21000 | 4.50 | 0.01 | 0.11 | 2.73
J083438.28+153817.5 | 2427-53815-0321 | — | — | 16500 | 5.59 | 0.00 | 0.28 | 0.08
J084510.22+112405.6 | 2428-53801-0089 | 0.43 | 9132 | 16000 | 2.17 | 0.08 | 0.15 | 12.40
J084219.70+122128.3 | 2428-53801-0221 | — | — | 20000 | 2.04 | 0.66 | 0.12 | 13.71
J084039.36+125706.2 | 2428-53801-0354 | 0.40 | 9487 | 12000 | 2.22 | 0.01 | 0.17 | 0.37
J084522.94+150020.3 | 2429-53799-0152 | — | — | 18000 | 2.03 | 0.02 | 0.17 | 22.64
J084111.34+154921.0 | 2429-53799-0358 | — | — | 19000 | 2.65 | 0.00 | 0.25 | 43.13
J084201.41+153941.8 | 2429-53799-0363 | 0.60 | 16480 | 20000 | 18.12 | 0.01 | 0.25 | 81.62
J085106.12+120157.8 | 2430-53815-0229 | 0.90 | 11246 | 10000 | 2.28 | 0.43 | -0.30 | 68.87
J085153.78+152724.9 | 2431-53818-0238 | 0.85 | 12056 | 10000 | 26.97 | 9.86 | -0.15 | 65.59
J091305.88+173932.9 | 2439-53795-0357 | — | — | 17500 | 2.76 | 0.15 | 0.36 | 0.18
J030913.96+373057.9 | 2443-54082-0030 | — | — | 19000 | 2.30 | 0.02 | 0.00 | 33.47
J030432.88+365537.8 | 2443-54082-0137 | — | — | 18500 | 2.20 | 0.01 | -0.04 | 13.32
J030550.34+370759.1 | 2443-54082-0154 | 0.48 | 10492 | 10500 | 3.00 | 0.02 | 0.36 | 0.04
J030158.92+372204.2 | 2443-54082-0190 | — | — | 12500 | 3.00 | 0.09 | 0.40 | 14.86
J024241.66+291608.2 | 2444-54082-0604 | 0.37 | 10135 | 12000 | 3.36 | 0.05 | 0.50 | 10.53
J024505.94+282542.7 | 2444-54082-0623 | 0.75 | 5699 | 8000 | 1.40 | 0.05 | -0.15 | 7.55
J124836.31+294231.2 | 2457-54180-0112 | 0.61 | 6853 | 8000 | 2.19 | 0.11 | -0.39 | 5.36
J133836.06+652433.1 | 2460-54616-0042 | — | — | 19000 | 2.19 | 0.01 | 0.16 | 0.63
J130033.46+590406.9 | 2461-54570-0015 | 0.57 | 6123 | 8000 | 6.72 | 0.27 | -0.12 | 36.05
J125040.81+590341.6 | 2461-54570-0219 | 0.78 | 15740 | 30000 | 2.80 | 0.01 | 0.00 | 33.47
J124508.48+591551.6 | 2461-54570-0264 | 0.38 | 19065 | 24000 | 1.10 | — | — | 33.47
J141710.80+573546.1 | 2462-54561-0404 | 0.74 | 5585 | 8000 | 2.50 | 0.07 | -0.04 | 23.52
J155232.76+264636.6 | 2474-54564-0392 | 0.75 | 20123 | 19362 | 1.10 | — | — | 33.47
J154550.71+132040.2 | 2517-54567-0065 | 0.50 | 12940 | 10000 | 2.81 | 0.02 | -0.32 | 77.09
J154424.84+132650.8 | 2517-54567-0110 | 0.68 | 11289 | 13000 | 2.06 | 0.07 | 0.22 | 27.14
J160357.92+140929.9 | 2524-54568-0247 | 0.82 | 8860 | 9500 | 49.40 | 58.55 | -0.24 | 52.38
J160219.42+112606.4 | 2525-54569-0303 | 0.99 | 10337 | 9500 | 2.53 | 0.00 | -0.03 | 37.90
J160532.18+131748.6 | 2525-54569-0425 | — | — | 19000 | 1.70 | 0.08 | 0.00 | 33.47
J161050.03+094302.4 | 2526-54582-0115 | — | — | 25000 | 2.70 | — | — | 33.47
J160540.06+093724.8 | 2526-54582-0223 | 0.58 | 25128 | 16000 | 2.17 | 0.01 | 0.17 | 19.33
J161929.62+131833.4 | 2530-53881-0332 | 0.63 | 20084 | 22000 | 2.90 | — | — | 33.47
J163013.93+123941.9 | 2533-54585-0325 | 0.33 | 10720 | 13500 | 2.08 | 0.01 | 0.17 | 0.30
J163630.30+114452.2 | 2533-54585-0502 | 0.69 | 10189 | 10500 | 3.00 | 0.00 | 0.42 | 2.18
J064828.77+840340.8 | 2548-54152-0616 | 1.07 | 13038 | 11500 | 3.73 | 0.01 | -0.17 | 53.66
J085550.69+824905.2 | 2549-54523-0066 | 1.14 | 21375 | 32081 | 12.19 | 0.15 | 0.23 | 66.09
J083448.65+821059.0 | 2549-54523-0135 | 1.17 | 24915 | 23000 | 15.02 | 0.92 | -0.39 | 55.53
J174235.20+640028.3 | 2561-54597-0021 | — | — | 30000 | 2.00 | 0.01 | 0.00 | 33.47
J173208.55+631950.3 | 2561-54597-0087 | — | — | 24000 | 2.30 | 0.02 | -0.14 | 6.73
J172623.13+632607.8 | 2561-54597-0212 | — | — | 25000 | 2.85 | 0.02 | 0.07 | 87.22
J192553.59+620708.6 | 2563-54653-0165 | 0.90 | 10093 | 9000 | 2.28 | 0.01 | -0.31 | 86.27
J192416.73+614833.1 | 2563-54653-0255 | — | — | 9500 | 2.58 | 0.01 | -0.38 | 54.85
J102746.58+435156.2 | 2567-54179-0306 | 0.25 | 9266 | 9500 | 2.11 | 0.03 | -0.15 | 74.41
J121840.75-001005.8 | 2568-54153-0309 | — | — | 25000 | 2.33 | 0.00 | 0.16 | 89.99
J122238.86+005034.4 | 2568-54153-0411 | 0.24 | 10410 | 13500 | 2.19 | 0.01 | 0.15 | 10.81
J122209.43+001534.1 | 2568-54153-0471 | — | — | 19500 | 8.00 | 0.02 | 0.27 | 0.79
J081523.35+084346.4 | 2571-54055-0256 | — | — | 21000 | 5.17 | 0.02 | 0.17 | 0.41
J082939.24+100937.7 | 2572-54056-0399 | 0.99 | 15640 | 22000 | 2.69 | 0.71 | -0.21 | 81.09
J084011.39+094244.8 | 2573-54061-0130 | 0.42 | 7931 | 9500 | 2.19 | 0.01 | 0.20 | 5.30
J084233.36+101806.3 | 2573-54061-0141 | — | — | 12284 | 2.78 | 0.01 | 0.35 | 77.36
J083801.80+092548.3 | 2573-54061-0246 | — | — | 23000 | 3.77 | 0.13 | 0.44 | 1.37
J091340.18+114112.3 | 2576-54086-0029 | 0.64 | 11484 | 17500 | 2.19 | 0.04 | 0.18 | 11.19
J091611.06+124808.0 | 2577-54086-0427 | 0.78 | 23461 | 22000 | 2.12 | 0.41 | -0.10 | 8.54
J092108.83+130111.6 | 2577-54086-0448 | 0.65 | 10326 | 20000 | 2.47 | 0.98 | 0.01 | 0.40
J093431.10+132814.6 | 2580-54092-0273 | — | — | 34332 | 2.13 | 0.02 | -0.24 | 62.35
J100758.24+163618.9 | 2585-54097-0024 | — | — | 11000 | 2.27 | 0.05 | -0.31 | 79.19
J100759.80+162349.6 | 2585-54097-0030 | 1.01 | 10671 | 32642 | 13.02 | 9.31 | -0.12 | 40.83
J100645.00+144250.3 | 2586-54169-0479 | — | — | 12000 | 2.78 | 0.01 | 0.40 | 10.44
J102230.51+144646.8 | 2590-54175-0191 | 0.98 | 7664 | 8500 | 2.22 | 0.03 | 0.15 | 1.04
J103002.66+163927.4 | 2592-54178-0417 | — | — | 22000 | 4.01 | 0.00 | 0.18 | 0.47
J103648.66+171045.1 | 2593-54175-0131 | 0.42 | 12309 | 9500 | 2.19 | 0.01 | -0.13 | 78.82
J121706.46+172855.9 | 2596-54207-0023 | 0.41 | 28189 | 25000 | 1.20 | — | — | 33.47
J125511.49+154929.7 | 2602-54149-0249 | 0.44 | 13804 | 10000 | 2.24 | 0.01 | -0.30 | 72.69
J131426.37+173228.0 | 2604-54484-0481 | 0.79 | 7022 | 8000 | 2.62 | 0.15 | -0.35 | 13.68
J121211.27+185228.9 | 2609-54476-0005 | — | — | 25000 | 10.92 | 1.22 | 0.50 | 3.81
J121110.29+203429.0 | 2609-54476-0564 | — | — | 25000 | 2.26 | 0.01 | 0.11 | 0.15
J132203.94+193223.1 | 2619-54506-0423 | — | — | 18000 | 4.09 | 1.27 | 0.17 | 1.92
J225123.66+293945.3 | 2621-54380-0042 | — | — | 8000 | 1.80 | 0.08 | -0.17 | 29.36
J225338.68+301803.4 | 2627-54379-0021 | 1.10 | 19805 | 23000 | 2.01 | 0.01 | 0.14 | 12.68
J224854.51+303845.5 | 2627-54379-0152 | — | — | 22000 | 4.05 | 1.93 | 0.49 | 3.58
J121033.23+221402.6 | 2644-54210-0167 | 0.91 | 13414 | 10500 | 2.23 | 1.65 | -0.30 | 59.99
J133025.70+224813.6 | 2653-54230-0408 | 0.67 | 12660 | 10000 | 3.19 | 0.01 | -0.48 | 61.25
J122100.20+244443.7 | 2657-54502-0026 | 0.47 | 9549 | 10500 | 2.25 | 0.01 | -0.30 | 59.35
J044254.59+120329.8 | 2669-54086-0377 | 0.76 | 9349 | 8000 | 33.72 | 14.03 | -0.34 | 56.07
J044641.49+101510.9 | 2673-54096-0049 | 0.75 | 9567 | 8000 | 2.17 | 0.16 | -0.29 | 57.95
J082108.17+372738.3 | 2674-54097-0103 | — | — | 8000 | 0.60 | 0.00 | -0.33 | 16.25
J034630.98+094827.4 | 2679-54368-0225 | 1.28 | 26236 | 19500 | 2.79 | 0.33 | 0.32 | 89.23
J034314.34+102938.3 | 2679-54368-0356 | 1.03 | 42617 | 40000 | 8.57 | 4.02 | -0.50 | 37.73
J064607.86+280510.0 | 2694-54199-0175 | — | — | 19500 | 2.28 | 0.06 | -0.31 | 65.18
J064532.74+280330.4 | 2694-54199-0201 | 0.46 | 10522 | 11351 | 2.30 | — | — | 33.47
J065133.33+284423.3 | 2694-54199-0528 | — | — | 17841 | 2.16 | 0.09 | 0.15 | 8.36
J071814.18+305148.8 | 2695-54409-0268 | — | — | 12000 | 3.19 | 3.33 | 0.47 | 5.48
J072540.81+321402.1 | 2695-54409-0564 | — | — | 24000 | 15.15 | 0.88 | 0.29 | 57.89
J035010.32+085829.1 | 2697-54389-0048 | — | — | 14500 | 2.02 | 0.01 | 0.16 | 0.27
J072724.65+403622.4 | 2701-54154-0301 | 1.13 | 13501 | 10500 | 2.81 | 0.13 | -0.37 | 72.98
J075234.95+172524.9 | 2729-54419-0171 | 0.80 | 8665 | 9000 | 12.68 | 1.17 | -0.31 | 48.59
J074924.91+171355.3 | 2729-54419-0282 | 0.68 | 20941 | 18500 | 14.95 | 0.41 | -0.39 | 57.16
J140709.72+154010.2 | 2745-54231-0343 | 0.84 | 11486 | 13500 | 22.82 | 0.00 | -0.12 | 62.17
J152936.81+123436.8 | 2754-54240-0371 | 0.36 | 12209 | 10500 | 2.52 | 0.07 | -0.36 | 73.12
J151436.65+152058.4 | 2766-54242-0497 | 0.94 | 9386 | 10500 | 3.08 | 0.15 | -0.49 | 50.42
J140444.21+201922.6 | 2771-54527-0196 | 0.66 | 17354 | 14500 | 2.13 | 0.01 | -0.24 | 76.47
J141309.30+191831.9 | 2772-54529-0217 | 1.19 | 16400 | 14000 | 2.53 | 0.05 | -0.31 | 67.01
J154141.84+173026.2 | 2795-54563-0603 | 1.01 | 15425 | 16500 | 2.19 | 0.00 | 0.15 | 0.51
J164649.56+120547.0 | 2817-54627-0308 | 0.77 | 30172 | 40000 | 3.07 | 0.08 | -0.47 | 54.72
J165413.92+124344.7 | 2817-54627-0553 | 0.56 | 5287 | 8000 | 1.45 | 0.05 | -0.17 | 13.46
J172704.99+084857.1 | 2818-54616-0374 | 0.54 | 33635 | 40000 | 1.10 | 0.07 | 0.00 | 33.47
J184130.70+410745.1 | 2819-54617-0104 | 0.63 | 5902 | 8000 | 1.40 | 0.09 | -0.13 | 4.28
J173056.41+433000.4 | 2820-54599-0185 | — | — | 20000 | 2.45 | 0.65 | -0.04 | 0.93
J001034.94+245131.2 | 2822-54389-0025 | 0.98 | 9064 | 10500 | 11.80 | 0.30 | -0.32 | 57.32
J000701.59+240744.8 | 2822-54389-0042 | — | — | 8000 | 2.27 | 0.01 | -0.30 | 64.61
J011130.67+141049.7 | 2825-54439-0089 | — | — | 19000 | 3.30 | 0.84 | 0.32 | 2.27
J080620.12-075457.1 | 2827-54422-0307 | 1.32 | 10446 | 9000 | 3.19 | 0.01 | 0.30 | 28.06
J083234.10-042813.7 | 2828-54438-0149 | — | — | 9500 | 7.90 | 0.00 | 0.35 | 5.97
J020514.52+003100.3 | 2866-54478-0603 | — | — | 18000 | 2.42 | 0.03 | 0.22 | 3.50
J111245.75+185719.5 | 2872-54533-0233 | — | — | 8500 | 2.52 | 0.17 | -0.36 | 56.52
J111205.21+183200.2 | 2872-54533-0284 | — | — | 9000 | 2.57 | 0.06 | -0.39 | 40.01
J112216.02-122250.9 | 2874-54561-0071 | — | — | 13500 | 3.15 | 0.02 | 0.46 | 1.16
J111539.09-111350.6 | 2874-54561-0333 | 0.46 | 5543 | 8000 | 4.64 | 0.22 | -0.22 | 2.66
J112030.34-115051.1 | 2874-54561-0512 | 1.30 | 28653 | 15500 | 9.59 | 0.02 | -0.49 | 44.33
J012516.68-101313.7 | 2878-54465-0269 | — | — | 11500 | 2.61 | 0.02 | 0.25 | 0.04
J161425.46+493244.9 | 2884-54526-0254 | 0.32 | 11384 | 11500 | 3.00 | 0.01 | 0.44 | 7.93
J093415.96+294500.4 | 2914-54533-0162 | 0.69 | 17852 | 40000 | 32.01 | 0.74 | 0.35 | 42.92
J075036.54+222021.4 | 2916-54507-0133 | — | — | 21000 | 2.08 | 0.00 | 0.08 | 33.22
J123706.24-001603.9 | 2920-54562-0110 | 1.01 | 10947 | 11000 | 2.55 | 0.01 | -0.38 | 62.18
J124851.30-022924.7 | 2922-54612-0607 | 0.74 | 13658 | 9500 | 4.26 | 0.40 | -0.15 | 16.53
J135206.28+175333.0 | 2930-54589-0051 | — | — | 8000 | 2.19 | 0.02 | 0.16 | 11.14
J143235.46+454852.4 | 2932-54595-0542 | 0.73 | 15821 | 22000 | 11.72 | 1.93 | 0.43 | 9.51
J044512.39-052524.5 | 2942-54521-0487 | — | — | 18000 | 2.68 | 0.28 | 0.24 | 5.82
J045016.37-053847.8 | 2942-54521-0637 | — | — | 40000 | 2.15 | 0.01 | 0.16 | 2.94
J071410.25+401219.4 | 2943-54502-0612 | — | — | 18000 | 2.35 | 0.01 | 0.15 | 88.78
J075137.54+670732.3 | 2944-54523-0569 | 0.65 | 5440 | 8000 | 0.90 | 0.00 | -0.17 | 12.87
J075704.00+085519.9 | 2945-54505-0148 | — | — | 22000 | 1.60 | 0.14 | 0.00 | 33.47
J153349.02+005916.1 | 2954-54561-0048 | 0.61 | 12327 | 9500 | 2.62 | 0.48 | -0.17 | 65.27
J154524.79+010127.5 | 2955-54562-0061 | — | — | 19500 | 2.40 | 0.03 | 0.00 | 33.47
J084541.11+312936.6 | 2960-54561-0009 | — | — | 12500 | 2.08 | 0.33 | 0.18 | 0.45
J160904.12+175337.7 | 2967-54584-0089 | 0.57 | 11595 | 9000 | 2.43 | 0.17 | -0.24 | 72.96
J031637.81-003310.9 | 3183-54833-0179 | 0.59 | 7011 | 9000 | 2.00 | 0.17 | -0.30 | 9.35
J071632.91+393553.8 | 3655-55240-0488 | 0.65 | 14947 | 17000 | 2.44 | 0.30 | 0.22 | 87.60
J073615.91+403335.0 | 3658-55205-0062 | 0.81 | 6488 | 8000 | 3.79 | 0.19 | -0.27 | 14.46
J073741.49+470421.1 | 3665-55247-0394 | 0.40 | 25490 | 23000 | 3.59 | 0.66 | 0.49 | 3.55
J074126.28+394118.7 | 3670-55480-0528 | 0.66 | 6611 | 8000 | 1.45 | 0.03 | -0.24 | 9.23
J075916.53+433518.9 | 3676-55186-0030 | 1.37 | 20912 | 22420 | 2.29 | 0.00 | -0.27 | 44.98
J081632.25+522645.2 | 3689-55180-0826 | 0.60 | 7235 | 8000 | 2.19 | 0.36 | -0.40 | 0.39
J083051.14+503610.7 | 3694-55209-0966 | 0.96 | 18201 | 16000 | 2.26 | 0.15 | 0.30 | 72.81
J093054.58-012642.9 | 3767-55214-0562 | 1.15 | 13898 | 10500 | 10.42 | 1.05 | -0.32 | 7.09
J113839.49-014903.0 | 3775-55207-0698 | 0.76 | 11717 | 9500 | 24.33 | 5.06 | -0.15 | 62.90
J084906.22+003722.8 | 3813-55532-0364 | 0.77 | 14065 | 14500 | 18.27 | 4.40 | -0.45 | 64.16
J090855.40+010552.5 | 3818-55532-0906 | 0.62 | 7744 | 8000 | 3.00 | 0.02 | -0.33 | 48.63
J094416.62-001855.5 | 3827-55565-0472 | 0.55 | 7926 | 8000 | 3.77 | 0.02 | -0.28 | 17.50
J112059.67-001942.2 | 3838-55588-0064 | 0.92 | 30253 | 19000 | 3.26 | 0.16 | 0.47 | 4.22
J134820.79+381017.2 | 3852-55243-0676 | 1.29 | 30979 | 25000 | 15.52 | 4.67 | -0.36 | 59.10
J134024.99+325028.7 | 3856-55269-0462 | 0.69 | 27311 | 25000 | 2.36 | 0.31 | -0.07 | 59.41
J151835.81+311911.4 | 3879-55244-0584 | — | — | 8500 | 2.61 | 0.08 | -0.23 | 71.71
J155202.55+170434.7 | 3926-55327-0738 | 0.86 | 7436 | 8000 | 2.62 | 0.02 | -0.36 | 16.89
J152401.59+185659.2 | 3945-55648-0726 | 1.06 | 13793 | 9500 | 6.49 | 0.97 | -0.18 | 21.15
J154855.04+245112.9 | 3947-55332-0016 | 1.20 | 21234 | 17500 | 8.41 | 1.30 | -0.39 | 69.19
J151516.47+244547.7 | 3961-55654-0708 | 0.92 | 9113 | 8000 | 16.39 | 1.88 | -0.46 | 67.54
J150809.79+215037.0 | 3962-55660-0428 | 0.61 | 16595 | 15000 | 17.50 | 2.77 | -0.47 | 27.66
J131955.04+015259.5 | 4006-55328-0358 | 0.31 | 13501 | 12500 | 3.24 | 0.09 | 0.48 | 5.30
J145231.59-025634.1 | 4023-55328-0122 | 0.77 | 11993 | 11500 | 2.28 | 0.28 | -0.32 | 72.23
J143147.14+012153.0 | 4024-55646-0304 | 0.57 | 15667 | 12000 | 2.72 | 0.14 | 0.39 | 74.35
J162304.10+183522.2 | 4060-55359-0296 | 0.50 | 12044 | 14000 | 2.50 | 0.07 | 0.28 | 81.41
J163334.67+194229.7 | 4061-55362-0761 | 0.64 | 15308 | 17500 | 2.67 | 0.50 | -0.38 | 44.55
J163350.80+150822.6 | 4068-55445-0746 | — | — | 40000 | 3.52 | 12.01 | 0.50 | 3.81
J162216.01+184019.4 | 4073-55663-0806 | 0.74 | 20596 | 16500 | 3.43 | 0.08 | 0.50 | 6.56
J163917.45+103604.9 | 4075-55352-0101 | 0.72 | 6300 | 8000 | 1.45 | 0.06 | -0.21 | 16.94
J211504.83+040009.7 | 4077-55361-0564 | 0.59 | 6321 | 8000 | 4.50 | 0.31 | -0.23 | 5.82
J213148.69+065930.1 | 4085-55452-0074 | 0.88 | 7535 | 8000 | 31.14 | 9.18 | -0.25 | 9.37
J214536.12+062726.8 | 4091-55498-0588 | 0.59 | 19353 | 17000 | 2.07 | 0.21 | 0.27 | 79.52
J162808.39+233254.1 | 4184-55450-0844 | — | — | 8000 | 4.77 | 0.21 | -0.09 | 32.98
J164359.14+273047.7 | 4190-55686-0984 | 0.62 | 18269 | 10500 | 2.86 | 0.04 | 0.27 | 51.96
J004528.87+004616.4 | 4223-55451-0634 | 1.29 | 22391 | 19500 | 2.19 | 0.08 | -0.26 | 61.77
J021116.37+003128.2 | 4235-55451-0850 | 0.85 | 9183 | 9000 | 31.06 | 8.84 | -0.24 | 8.18
J021818.18+035525.3 | 4264-55506-0408 | 0.94 | 7982 | 8000 | 2.46 | 0.01 | -0.36 | 20.28
J231951.71+010908.7 | 4286-55499-0125 | — | — | 30000 | 2.40 | 0.20 | -0.36 | 68.91
J020002.57-020542.3 | 4349-55803-0892 | 0.75 | 7104 | 8000 | 2.77 | 0.32 | -0.33 | 38.09
J082302.39+334534.1 | 4442-55532-0578 | 0.87 | 7752 | 8000 | 2.46 | 0.08 | -0.37 | 8.84
J074213.39+315703.8 | 4443-55539-0256 | 0.75 | 9562 | 9000 | 41.40 | 25.36 | -0.16 | 11.24
J083446.91+304959.2 | 4449-55544-0876 | 0.47 | 21780 | 11500 | 2.56 | 0.1 | -0.36 | 85.31
J081819.51+225349.9 | 4468-55894-0368 | — | — | 35245 | 2.54 | 0.21 | 0.36 | 89.04
J081354.17+223713.6 | 4469-55863-0047 | 0.89 | 22106 | 21000 | 15.52 | 2.46 | 0.36 | 77.38
J074224.66+232804.1 | 4470-55587-0200 | 0.99 | 12378 | 14000 | 2.84 | 0.28 | -0.35 | 55.65
J083945.55+200015.7 | 4484-55565-0072 | 0.73 | 14964 | 15500 | 2.72 | 0.26 | -0.27 | 59.18
J083020.35+185814.5 | 4489-55545-0678 | 1.13 | 21250 | 20000 | 2.27 | 0.01 | -0.30 | 80.38
J074907.48+154534.1 | 4495-55566-0435 | 0.54 | 19493 | 22000 | 2.09 | 0.08 | -0.25 | 73.24
J080359.93+122943.9 | 4505-55603-0384 | 1.13 | 17756 | 17500 | 34.76 | 8.70 | -0.33 | 30.89
J081216.23+131708.2 | 4505-55603-0987 | 0.45 | 13565 | 18000 | 2.66 | 0.24 | 0.23 | 4.15
J000603.80+075514.4 | 4534-55863-0248 | 0.76 | 9102 | 9000 | 12.94 | 9.04 | -0.47 | 43.92
J102054.10+362647.0 | 4568-55600-0952 | 0.71 | 15917 | 13500 | 61.20 | 12.02 | -0.20 | 52.99
J091124.68+420255.8 | 4603-55999-0200 | 0.87 | 9761 | 10500 | 44.50 | 8.59 | -0.11 | 53.70
J113114.44+355007.2 | 4618-55600-0022 | 0.61 | 15023 | 12500 | 3.00 | 0.16 | 0.43 | 1.85
J094111.40+423921.2 | 4638-55956-0034 | — | — | 40000 | 3.48 | 0.02 | 0.49 | 59.24
J101507.34+441507.8 | 4693-55632-0066 | — | — | 8000 | 2.77 | 0.08 | -0.33 | 20.30
J124816.81+411051.2 | 4703-55617-0381 | 0.68 | 20586 | 13500 | 3.09 | 0.11 | -0.50 | 50.82
J142703.35+372110.5 | 4713-56044-0230 | 1.16 | 18983 | 14500 | 32.06 | 6.16 | -0.35 | 65.56
J142836.95+383904.9 | 4713-56044-0844 | 0.66 | 7537 | 8000 | 7.00 | 0.55 | -0.36 | 10.53
J154012.07+290828.9 | 4722-55735-0206 | 0.25 | 19833 | 40000 | 11.95 | 0.30 | -0.49 | 17.53
J103724.11+013528.8 | 4734-55646-0298 | 1.17 | 14893 | 10500 | 3.73 | 2.38 | -0.50 | 14.07
J092926.44+013535.6 | 4742-55660-0420 | 0.94 | 16856 | 13000 | 2.26 | 0.08 | -0.29 | 79.55
J130805.95+035424.3 | 4760-55656-0470 | 0.60 | 20585 | 13000 | 2.19 | 0.13 | 0.30 | 73.67
J103430.15+032736.3 | 4772-55654-0128 | 1.10 | 15747 | 11500 | 13.28 | 1.87 | -0.28 | 65.82
J150451.71+052141.0 | 4776-55652-0509 | 1.13 | 16080 | 17500 | 5.25 | 0.18 | -0.32 | 69.96
J133420.95+041751.3 | 4786-55651-0518 | 1.17 | 15097 | 17415 | 2.43 | 0.15 | -0.27 | 73.80
J081656.46+030417.0 | 4787-55863-0846 | 0.61 | 6879 | 8000 | 4.19 | 0.33 | -0.25 | 15.71
J100356.31+053825.6 | 4800-55674-0790 | — | — | 22000 | 163.51 | 18.08 | 0.11 | 31.31
J160100.43+044236.3 | 4808-55705-0318 | 0.77 | 14744 | 11500 | 44.79 | 28.35 | -0.28 | 7.60
J155708.02+041156.4 | 4808-55705-0466 | 1.19 | 22483 | 23000 | 40.70 | 9.41 | -0.08 | 60.16
J110341.38+053448.9 | 4855-55926-0376 | 1.07 | 11687 | 10500 | 16.41 | 2.81 | -0.33 | 72.64
J090139.03+064022.4 | 4868-55895-0730 | 0.88 | 6621 | 8000 | 0.80 | 0.00 | -0.20 | 17.50
J151415.65+074446.4 | 4878-55710-0747 | — | — | 10000 | 37.07 | 11.91 | -0.32 | 49.14
J154626.16+143754.8 | 4890-55741-0988 | 0.62 | 36702 | 30000 | 2.99 | 0.40 | 0.42 | 88.92
J155835.80+122139.4 | 4901-55711-0358 | 0.58 | 25321 | 24000 | 2.13 | 0.58 | -0.30 | 88.31
J153049.68+344434.7 | 4975-56037-0762 | 1.13 | 25710 | 37472 | 10.43 | 5.91 | -0.47 | 63.27
J153948.03+404528.5 | 4976-56046-0553 | 0.74 | 16617 | 12500 | 18.84 | 2.75 | -0.35 | 59.56
J170751.91+353239.4 | 4988-55825-0107 | 1.13 | 21596 | 18000 | 2.64 | 0.43 | -0.38 | 53.27
J171102.58+360959.6 | 4989-55743-0414 | 0.66 | 23378 | 20546 | 2.30 | 0.07 | 0.11 | 14.34
J170123.81+330853.9 | 4992-55723-0866 | — | — | 12206 | 37.71 | 1.24 | -0.32 | 0.92
J171959.47+331614.9 | 4994-55739-0097 | 0.63 | 28249 | 21000 | 2.20 | 0.22 | 0.22 | 88.33
J172432.14+323414.9 | 5002-55710-0601 | 1.22 | 24779 | 22000 | 257.20 | 43.61 | -0.20 | 50.29
J163036.79+272451.5 | 5005-55751-0254 | 1.03 | 10762 | 11500 | 35.60 | 6.30 | -0.19 | 52.96
J171711.53+262012.0 | 5016-55709-0596 | 1.14 | 20593 | 22000 | 18.49 | 0.57 | -0.36 | 52.32
J224741.46+145638.7 | 5040-56243-0482 | 1.09 | 16732 | 18000 | 515.09 | 72.32 | 0.21 | 28.92
J221141.80+113604.5 | 5064-55864-0122 | 1.34 | 9574 | 9500 | 18.77 | 1.05 | -0.35 | 22.29
J010405.12+145907.3 | 5131-55835-0438 | 0.48 | 13897 | 10500 | 2.78 | 0.20 | 0.31 | 89.97
J010311.32+151110.0 | 5131-55835-0578 | 0.35 | 12457 | 11000 | 2.81 | 0.16 | -0.42 | 67.41
J012646.78+193454.5 | 5135-55862-0886 | 0.97 | 8393 | 8000 | 2.22 | 0.13 | -0.09 | 52.27
J011423.35+160727.6 | 5139-55866-0410 | — | — | 22000 | 22.97 | 13.33 | 0.06 | 46.94
J150813.26+394505.1 | 5167-56066-0732 | — | — | 29032 | 12.95 | 9.75 | -0.05 | 15.13
J144405.60+405338.0 | 5172-56071-0676 | 0.57 | 23688 | 25000 | 2.56 | 0.12 | -0.17 | 75.76
J145330.84+390245.2 | 5174-56047-0828 | 0.52 | 15751 | 13500 | 2.29 | 0.13 | 0.31 | 77.93
J084330.81+201049.1 | 5176-56221-0564 | 0.73 | 47864 | 25000 | 21.52 | 2.13 | -0.42 | 0.02
J085649.67+253441.0 | 5179-55957-0778 | 0.92 | 10783 | 11500 | 85.00 | 11.68 | -0.20 | 19.31
J164342.37+315728.7 | 5194-56062-0546 | 0.51 | 20438 | 15500 | 2.25 | 0.08 | 0.29 | 73.53
J164703.23+370910.2 | 5198-55823-0511 | 0.84 | 15954 | 16500 | 3.01 | 0.17 | -0.42 | 47.55
J161710.49+383306.9 | 5199-56067-0720 | 0.58 | 12988 | 16500 | 2.45 | 0.10 | 0.29 | 76.34
J160531.60+385210.0 | 5200-56091-0678 | 0.48 | 15025 | 13000 | 2.67 | 0.11 | 0.38 | 13.62
J154238.25+101156.9 | 5206-56033-0032 | 0.45 | 14715 | 11500 | 2.56 | 0.08 | -0.37 | 72.58
J083656.62+103452.1 | 5284-55866-0690 | 0.53 | 17638 | 17000 | 2.07 | 0.14 | 0.10 | 47.85
J085820.01+103725.4 | 5291-55947-0999 | 0.61 | 17808 | 20000 | 2.14 | 0.55 | 0.09 | 17.15
J085523.86+164058.9 | 5292-55926-0186 | 0.74 | 12741 | 12000 | 11.04 | 0.58 | -0.44 | 20.88
J085841.78+074728.3 | 5294-55922-0180 | — | — | 18000 | 2.52 | 0.00 | 0.25 | 0.00
J090827.08+092100.2 | 5299-55927-0834 | 1.14 | 26638 | 40000 | 46.50 | 28.29 | 0.14 | 64.68
J091239.63+102645.7 | 5302-55896-0230 | 0.40 | 19030 | 16000 | 3.10 | 0.06 | 0.44 | 11.60
J092417.96+142238.2 | 5305-55984-0002 | 0.69 | 19279 | 30000 | 2.38 | 0.13 | 0.11 | 4.05
J093707.06+102149.1 | 5316-55955-0434 | 1.21 | 19695 | 17500 | 394.67 | 127.88 | 0.43 | 42.94
J094004.19+123930.8 | 5318-55983-0468 | — | — | 8000 | 2.19 | 0.03 | -0.28 | 63.18
J103336.57+105710.9 | 5346-55955-0628 | 0.46 | 6526 | 8000 | 24.10 | 9.90 | -0.31 | 2.62
J105055.04+143359.4 | 5355-56009-0532 | 0.28 | 16510 | 15500 | 2.81 | 0.20 | 0.40 | 23.74
J112605.90+090628.8 | 5371-55976-0258 | 1.05 | 10197 | 10500 | 32.12 | 42.07 | -0.19 | 9.25
J112148.80+103934.2 | 5371-55976-0512 | 0.98 | 11385 | 17000 | 311.79 | 61.86 | -0.12 | 86.65
J120125.38+084800.3 | 5389-55953-0671 | 0.80 | 7395 | 8000 | 2.15 | 0.08 | -0.10 | 11.69
J121735.25+082810.0 | 5393-55946-0981 | 1.06 | 18534 | 15000 | 2.57 | 0.39 | -0.38 | 58.03
J123531.30+154418.2 | 5404-56013-0896 | 0.94 | 7443 | 8000 | 50.74 | 16.26 | -0.15 | 26.27
J124058.11+063645.6 | 5407-55926-0250 | 0.58 | 15283 | 11000 | 2.08 | 0.17 | 0.10 | 32.16
J124852.85+153641.9 | 5414-56014-0423 | 0.75 | 22844 | 14000 | 2.70 | 0.17 | 0.25 | 3.76
J131508.96+093713.8 | 5426-55987-0342 | 0.86 | 20370 | 22000 | 12.93 | 8.36 | -0.50 | 18.22
J131802.48+071743.2 | 5429-55979-0448 | 0.41 | 21840 | 15500 | 3.17 | 0.05 | 0.46 | 4.43
J133156.48+124055.9 | 5432-56008-0858 | 0.55 | 18585 | 20000 | 2.28 | 0.29 | -0.18 | 76.37
J133738.54+072440.2 | 5437-55973-0404 | 0.44 | 15184 | 13500 | 3.15 | 0.20 | 0.46 | 3.59
J135107.02+074345.5 | 5442-55978-0132 | 1.15 | 14421 | 9500 | 2.19 | 0.04 | -0.23 | 58.02
J135048.10+084512.6 | 5442-55978-0820 | 0.58 | 6715 | 8000 | 2.15 | 0.08 | -0.10 | 47.65
J134845.98+110008.8 | 5445-55987-0530 | 1.21 | 18493 | 16500 | 202.58 | 14.94 | 0.19 | 4.31
J135204.28+112055.2 | 5445-55987-0622 | 0.61 | 16139 | 18000 | 2.35 | 0.07 | 0.16 | 89.99
J141307.56+121537.4 | 5453-56001-0030 | 0.71 | 40664 | 30000 | 2.96 | 0.29 | -0.44 | 74.88
J142003.63+103930.4 | 5456-55980-0016 | 0.60 | 14854 | 12500 | 2.26 | 0.11 | 0.32 | 86.15
J142035.36+112042.2 | 5460-56000-0598 | 0.87 | 19953 | 13000 | 3.00 | 0.11 | 0.43 | 15.18
J142708.16+100910.9 | 5465-55988-0464 | 0.45 | 15291 | 16500 | 2.23 | 0.17 | 0.26 | 65.73
J143506.35+072940.3 | 5467-55973-0321 | 0.34 | 11759 | 11500 | 2.54 | 0.08 | -0.37 | 73.66
J150957.07+092349.3 | 5487-55982-0596 | 1.07 | 10003 | 10000 | 6.00 | 0.25 | -0.17 | 9.06
J085419.97+603701.6 | 5709-56571-0108 | 0.93 | 10293 | 11000 | 62.99 | 10.03 | -0.19 | 12.15
J091015.08+520310.7 | 5732-56326-0864 | 0.56 | 18471 | 19500 | 2.41 | 0.12 | -0.28 | 29.69
J085817.39+471501.2 | 5735-55980-0410 | 0.53 | 19803 | 10317 | 2.82 | 0.14 | -0.42 | 63.34
J090205.29+454915.5 | 5736-55984-0466 | 0.63 | 10928 | 11000 | 2.83 | 0.30 | -0.44 | 56.63
J094235.02+205208.2 | 5786-56251-0182 | 1.15 | 23252 | 15500 | 62.79 | 26.23 | -0.18 | 62.95
J134913.52+205646.9 | 5869-56064-0446 | 0.93 | 9462 | 11413 | 385.05 | 34.49 | -0.08 | 69.00
J104219.06+203008.7 | 5874-56039-0134 | 1.12 | 24656 | 40000 | 128.98 | 100.74 | 0.03 | 46.61
J105544.90+211105.0 | 5876-56042-0550 | — | — | 8000 | 0.50 | 0.00 | -0.25 | 6.98
J113409.06+182238.7 | 5879-56047-0108 | — | — | 8500 | 2.24 | 0.03 | -0.5 | 1.27
J114441.65+171716.4 | 5892-56035-0686 | 0.78 | 17884 | 23000 | 2.15 | 0.21 | -0.20 | 11.84
J073341.55+435348.0 | 5942-56210-0336 | — | — | 11500 | 46.57 | 7.90 | -0.15 | 65.31
J215425.28+272109.5 | 5964-56098-0187 | 0.66 | 6353 | 8000 | 17.94 | 6.33 | -0.47 | 12.61
J124751.79+262110.2 | 5987-56339-0712 | 0.76 | 7197 | 8000 | 43.21 | 27.89 | -0.13 | 21.35
J141604.48+235404.2 | 6013-56074-0656 | 0.63 | 15687 | 14000 | 2.27 | 0.36 | 0.30 | 76.82
J143122.55+261026.4 | 6017-56075-0646 | — | — | 9500 | 2.03 | 0.03 | 0.10 | 27.59
J145829.87+223040.6 | 6020-56087-0312 | 0.91 | 9255 | 9500 | 32.53 | 10.51 | -0.15 | 62.98
J144331.21+262423.9 | 6022-56076-0670 | 0.66 | 15764 | 40000 | 4.78 | 0.20 | 0.50 | 3.19
J164843.29+461803.7 | 6027-56103-0970 | 0.76 | 13011 | 12500 | 18.04 | 1.23 | -0.34 | 41.90
J163900.06+440808.0 | 6030-56097-0034 | 0.47 | 14074 | 13000 | 2.85 | 0.17 | 0.39 | 15.02
J163458.64+415820.0 | 6036-56093-0308 | 0.61 | 18154 | 24000 | 2.06 | 0.23 | -0.13 | 52.66
J151130.16+422022.9 | 6048-56072-0374 | 1.02 | 10945 | 11500 | 12.83 | 16.96 | -0.28 | 34.91
J224912.31+220910.4 | 6120-56206-0747 | 0.46 | 12735 | 17500 | 2.14 | 0.07 | -0.28 | 84.78
J233958.11+154419.8 | 6138-56236-0466 | — | — | 10000 | 3.15 | 0.00 | -0.05 | 49.87
J232136.69+133133.5 | 6142-56219-0001 | 0.65 | 14033 | 10500 | 2.57 | 0.13 | -0.38 | 56.25
J231940.37+140121.1 | 6142-56219-0110 | — | — | 17500 | 3.00 | 0.07 | 0.43 | 18.05
J233052.97+143037.5 | 6143-56267-0900 | — | — | 23000 | 17.50 | 1.62 | -0.46 | 9.02
J230119.48+101939.0 | 6154-56237-0386 | — | — | 9000 | 7.34 | 0.04 | -0.08 | 36.48
J233817.93+083732.6 | 6161-56238-0622 | 0.72 | 11534 | 10500 | 118.33 | 62.08 | -0.38 | 7.12
J000505.48+183548.0 | 6170-56240-0212 | — | — | 11500 | 2.15 | 0.01 | -0.10 | 67.88
J001112.41+155209.5 | 6178-56213-0312 | 0.54 | 19975 | 15000 | 3.38 | 0.02 | 0.50 | 2.61
J004104.51+303819.4 | 6252-56248-0866 | — | — | 9000 | 2.00 | 0.02 | 0.14 | 2.24
J225828.48+280828.8 | 6293-56561-0264 | 1.02 | 10618 | 10500 | 137.09 | 33.81 | -0.35 | 44.67
J222348.44+231909.3 | 6299-56478-0639 | 0.90 | 8589 | 8500 | 6.00 | 1.11 | -0.50 | 14.66
J113136.70+242122.8 | 6421-56274-0804 | 0.80 | 9863 | 11500 | 78.38 | 15.07 | -0.13 | 60.34
J103036.02+225011.4 | 6425-56298-0386 | 1.11 | 17019 | 10000 | 5.33 | 0.02 | -0.50 | 20.23
J114246.50+205221.9 | 6432-56309-0563 | 0.97 | 12631 | 10000 | 74.76 | 10.78 | -0.11 | 57.33
J101712.60+233646.6 | 6458-56274-0968 | 1.04 | 10843 | 11500 | 143.03 | 15.18 | -0.34 | 60.06
J140750.65+301130.2 | 6495-56339-0886 | 1.18 | 21841 | 23000 | 86.00 | 10.48 | -0.07 | 27.98
J234858.29+253519.0 | 6518-56567-0796 | 0.92 | 23407 | 15500 | 7.68 | 0.78 | -0.50 | 33.38
J124906.90+432543.0 | 6617-56365-0033 | 1.05 | 63789 | 30000 | 2.76 | 0.25 | -0.41 | 69.68
J125232.05+423210.8 | 6619-56371-0368 | — | — | 30000 | 2.57 | 0.24 | -0.37 | 63.32
J134131.64+440030.0 | 6626-56330-0744 | 0.76 | 7240 | 8000 | 40.62 | 80.27 | -0.21 | 6.54
J124322.38+450002.0 | 6635-56370-0334 | 0.87 | 12305 | 9500 | 48.22 | 36.92 | -0.12 | 49.92
J114828.99+482731.1 | 6678-56401-0952 | 1.26 | 33083 | 30000 | 41.58 | 134.21 | 0.37 | 27.36
J125121.86+543215.7 | 6679-56401-0398 | 0.57 | 8563 | 8500 | 13.85 | 0.40 | -0.46 | 41.29
J115244.11+501844.5 | 6683-56416-0330 | 0.91 | 9499 | 9500 | 14.65 | 0.42 | -0.43 | 62.27
J134758.88+495427.4 | 6744-56399-0957 | 0.82 | 15798 | 16628 | 2.29 | 0.23 | -0.30 | 72.13
J140716.66+495613.7 | 6746-56386-0678 | 1.03 | 19650 | 18500 | 15.43 | 0.48 | 0.41 | 89.92
J133819.06+624018.7 | 6816-56444-0668 | 0.65 | 11191 | 13000 | 40.00 | 4.22 | -0.25 | 8.42
J134043.10+654349.2 | 6825-56717-0206 | 0.67 | 13462 | 11500 | 3.27 | 0.22 | -0.50 | 31.50
J132208.55+551939.0 | 6828-56430-0780 | 0.98 | 12240 | 9500 | 2.91 | 1.34 | -0.22 | 44.31
J000825.77-054122.3 | 7035-56568-0241 | — | — | 30000 | 2.58 | 0.08 | -0.35 | 77.82
J025001.76-043703.1 | 7054-56575-0438 | 1.16 | 12603 | 19000 | 309.41 | 38.57 | 0.15 | 42.50
J025506.13-071551.4 | 7059-56592-0652 | 0.72 | 7322 | 8000 | 9.00 | 1.41 | -0.28 | 6.99
J103655.38+652252.0 | 7083-56722-0200 | 1.21 | 21677 | 19500 | 15.37 | 1.27 | -0.49 | 3.71
J101400.72+594933.1 | 7087-56637-0772 | 0.43 | 6906 | 8000 | 1.90 | 0.04 | -0.23 | 6.85
J102553.68+622929.1 | 7090-56659-0696 | 0.91 | 8255 | 9000 | 3.25 | 0.01 | -0.48 | 46.08
J114152.02+572000.9 | 7092-56683-0812 | — | — | 11000 | 2.49 | 0.01 | -0.23 | 52.09
J111528.74+570125.3 | 7100-56636-0430 | 0.97 | 23414 | 23000 | 2.19 | 0.34 | -0.25 | 72.44
J120150.14+614256.8 | 7106-56663-0100 | 0.87 | 9702 | 10500 | 14.72 | 1.54 | -0.49 | 53.43
J115917.38+613914.2 | 7106-56663-0132 | 1.20 | 21001 | 17000 | 16.73 | 0.23 | -0.37 | 49.20
J132858.19+590851.0 | 7117-56685-0012 | 1.20 | 24259 | 18000 | 15.43 | 1.34 | -0.50 | 1.59
J122739.16+661224.3 | 7120-56720-0426 | 0.76 | 20248 | 19000 | 24.27 | 4.90 | -0.40 | 49.18
J123159.51+670918.9 | 7120-56720-0653 | 0.23 | 20220 | 14500 | 3.45 | 0.56 | 0.49 | 3.91
J224459.60+331017.3 | 7142-56567-0966 | 1.22 | 20263 | 20000 | 421.87 | 13.77 | 0.30 | 44.69
J000555.90-100213.5 | 7167-56604-0030 | 1.20 | 26711 | 25000 | 8.30 | 0.90 | -0.50 | 40.47
J021205.31+064420.5 | 7256-56658-0740 | 1.15 | 13881 | 19000 | 34.00 | 22.68 | -0.44 | 8.65
J093832.79+474050.6 | 7307-56720-0130 | 0.96 | 10251 | 12500 | 90.34 | 54.26 | -0.43 | 16.43
J100657.97+484506.0 | 7329-56719-0825 | — | — | 9000 | 23.97 | 0.18 | 0.24 | 4.72
J094026.71+631427.6 | 7447-56746-0198 | 0.81 | 14126 | 11000 | 2.81 | 0.18 | -0.36 | 72.90
J215209.66+223039.3 | 7576-56948-0399 | 0.87 | 8189 | 8500 | 7.25 | 0.18 | -0.39 | 45.28

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