JKAS Archive

Journal of the Korean Astronomical Society - Vol. 51 , No. 4

[ Article ]
Journal of the Korean Astronomical Society - Vol. 51, No. 4, pp.89-110
Abbreviation: JKAS
ISSN: 1225-4614 (Print) 2288-890X (Online)
Print publication date 31 Aug 2018
Received 26 Apr 2018 Accepted 11 Jul 2018
DOI: https://doi.org/10.5303/JKAS.2018.51.4.89

INTRA-NIGHT OPTICAL VARIABILITY OF ACTIVE GALACTIC NUCLEI IN THE COSMOS FIELD WITH THE KMTNET
Joonho Kim1 ; Marios Karouzos1, 2 ; Myungshin Im1 ; Changsu Choi1 ; Dohyeong Kim1 ; Hyunsung D. Jun3 ; Joon Hyeop Lee4, 5 ; Mar Mezcua6, 7
1Center for the Exploration of the Origin of the Universe (CEOU), Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 08826, Korea (joonho@astro.snu.ac.kr)(mim@astro.snu.ac.kr)
2Nature Astronomy, Springer Nature, 4 Crinan Street, N1 9XW London, UK
3School of Physics, Korea Institute for Advanced Study, 85 Hoegiro, Dongdaemun-gu, Seoul 02455, Korea
4Korea Astronomy and Space Science Institute, 776 Daedukdae-ro, Yuseong-gu, Daejeon 34055, Korea
5University of Science and Technology, 217 Gajeong-ro, Yuseong-gu, Daejeon 34113, Korea
6Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Magrans s/n, 08193 Barcelona, Spain
7Institut d’Estudis Espacials de Catalunya (IEEC), C/ Gran Capità, 08034 Barcelona, Spain

Correspondence to : M. Im


JKAS is published under Creative Commons license CC BY-SA 4.0.
Funding Information ▼

Abstract

Active Galactic Nucleus (AGN) variability can be used to study the physics of the region in the vicinity of the central black hole. In this paper, we investigated intra-night optical variability of AGN in the COSMOS field in order to understand the AGN instability at the smallest scale. Observations were performed using the KMTNet on three separate nights for 2.5 to 5 hours at a cadence of 20 to 30 min. We find that the observation enables the detection of short-term variability as small as ∼ 0.02 and 0.1 mag for R ∼ 18 and 20 mag sources, respectively. Using four selection methods (X-rays, mid-infrared, radio, and matching with SDSS quasars), 394 AGN are detected in the 4 deg2 field of view. After differential photometry and χ2-test, we classify intra-night variable AGN. The fraction of variable AGN (0–8%) is statistically consistent with a null result. Eight out of 394 AGN are found to be intra-night variable in two filters or two nights with a variability level of 0.1 mag, suggesting that they are strong candidates for intra-night variable AGN. Still they represent a small population (2%). There is no sub-category of AGN that shows a statistically significant intra-night variability.


Keywords: galaxies: active, radiation mechanisms: non-thermal, techniques: photometric

1. INTRODUCTION

Flux variability is characteristic for an active galactic nucleus (AGN). Because they hard to resolve spatially, variability is widely used to study the size, mass, and structure of AGN. Observations have discovered that AGN variability appears not only in various wavelengths, but also shows various timescales from hours to years. The results show increase in variability amplitude at shorter wavelengths and longer timescales (Ulrich et al. 1997 and references therein). In addition, there is an inverse correlation between long-term variability and luminosity while there is a positive correlation between long-term variability and redshift, as discovered by Uomoto et al. (1976) and Pica & Smith (1983).

Unfortunately, the origin of variability is not completely known. Generally, instability in the accretion disk or radio jet have been suggested as explanations for the AGN variability. For the accretion disk, physical timescales could be correlated with the variability of AGN. Hour-scale, day-scale, and year-scale variability correspond to light crossing timescale, dynamical timescale, and thermal timescale of the accretion disk, respectively (Frank et al. 2002). Therefore, the intra-night optical variability (INOV), which corresponds to the light crossing timescale, can be used to study violent variation at the smallest AGN size and structure. However, hour-scale variability has not been studied as much as longer timescale variability as it needs intensive monitoring with high cadence. It is also hard to detect, because of the minuscule variability from ∼ 10-1-10-3 mag.

Previous results on this subject present mixed results that require careful examination. This is because different types of AGN show different INOV activities and the depths of the data vary between different studies. Several consensuses and controversial issues can be summarized as below.

First, sub-classes of AGN such as radio-loud AGN and blazars are found to have a high probability of exhibiting INOV. The ballpark number is 20-100% for the fraction or the duty cycle of radio-loud quasars and blazars with INOV at the level of a few percent or more (Jang & Miller 1995, 1997; Romero et al. 1999, 2002; Stalin et al. 2005; Goyal et al. 2010, 2013a). On the other hand, radio-quiet AGN show INOV much less frequently, but the results are more controversial than the case for radio-loud AGN. In general, it is accepted that the INOV is found in none or only a few percent of radio-quiet AGN of various kinds when the variability amplitude of a few percent is examined (Romero et al. 1999; Webb & Malkan 2000; Klimek et al. 2004; Bachev et al. 2005; Carini et al. 2007; Kumar et al. 2016), where the variability amplitude is defined as the ratio of the standard deviation of the AGN light curve versus the observational error being > 2.576 or so (99% confidence; Jang & Miller 1997). Webb & Malkan (2000) examined INOV of 20 Seyfert 1 AGN, and found no INOV with the upper limit on the amplitude of the variation of 0.03 mag for time scales of 1 hr or less. However, they found the AGN variation at 25 to 27 hr level for two of their sample. Their photometric error is 0.02 mag. No INOV is found for 18 high luminosity quasars at z > 2 in which the photometric errors are of order of 0.02 to 0.05 mag (Bachev et al. 2005). At a similar photometric error accuracy, Klimek et al. (2004) found only one occasion of INOV of 0.045 mag change among 33 nights of the data for six Seyfert 1 galaxies, suggesting the duty cycle of 3% at the level of 0.05 mag variability. Using photometric data at an accuracy of 0.02 mag, Carini et al. (2007) find no INOV among 7 quasars (5 radio-quiet and 2 radio-intermediate). Kumar et al. (2016) examined the INOV of 10 weak emission line quasars (WLQ) in the hope of identifying BL Lacs with a peculiar property, but they found no INOV among 18 observing sessions. Their work has photometric error of 0.03 to 0.06 mag, so INOV of 0.1 mag or larger should have been detected.

When smaller amplitudes of INOV are examined, the results are rather mixed. Examining the INOV amplitude down to about 1%, several studies find 10-40% of radio-quiet quasars show INOV with the duty cycle of 10-20% (Jang & Miller 1995, 1997; Romero et al. 1999, 2002; Gopal-Krishna 2000, 2003; Webb & Malkan 2000; Stalin et al. 2004a,b, 2005; Klimek et al. 2004; Bachev et al. 2005; Gupta & Joshi 2005;Carini et al. 2007; Goyal et al. 2010, 2012, 2013a; Joshi et al. 2011; Kumar et al. 2016), while several other studies that examined INOV at a similar level do not find such evidence (Petrucci et al. 1999; Romero et al. 1999). For example, Goyal et al. (2013a) find that about 40% of radio-quiet quasars exhibit INOV, and 20% if limited to the variability amplitude of ∼ 3%. The duty cycle, on the other hand, is found to be 10% (or 6% at the variability amplitude > 3%) for these objects. However, at a similar photometric accuracy, Romero et al. (1999) examined the INOV of 8 RQQs and RLQs, BL Lacs, finding no convincing case for INOV among radio-quiet quasars. At a slightly worse photometric accuracy (0.5%), Petrucci et al. (1999) found no INOV among 22 Seyfert 1 galaxies.

More recently, the high cadence photometry data from the Kepler mission (30 min cadence) are being studied to examine the short-term variability of AGN (e.g., Mushotzky et al. 2011, Carini & Ryle 2012, Wehrle et al. 2013, Revalski et al. 2014, Chen & Wang 2015, Edelson et al. 2014, Kasliwal et al. 2015, Shaya et al. 2015, Dobrotka et al. 2017), Aranzana et al. (2018) examined the variability of 252 AGN with R < 19 mag. The power spectral density (PSD) of these objects in this study are consistent with white noise of a few tenths of a percent error for most objects, although a few objects seem to show σ > 1% with the PSD following a power-law. However, no statistical inferences have been made about the fraction of AGN for INOV.

Obviously our understanding of the demography of the INOV among AGN can be improved considering the small sample sizes in most of the previous studies. Furthermore, inhomogeneously sampled data, observed at different nights, bands, and telescopes, have made it difficult to compare various results about the variability of AGN. The Korea Microlensing Telescope Network (KMTNet) is a network of three 1.6m telescopes that are designed to study microlensing events without a gap in observing times (Kim et al. 2016). This facility offers an excellent opportunity to study INOV of a large number AGN of different kinds, and to do so, we are conducting a project named KMTNet Active Galactic Nuclei VAriability Survey (KANVAS). In this paper, we present the results from our pilot study of KANVAS. In Section 2, we introduce the KMTNet and observations while Section 3 presents an analysis of KMTNet data. Section 4 describes the AGN selection method, and their characteristics. Sections 5 and 6 present the variable AGN and their results. Finally, we discuss and conclude this results in Section 7.


2. OBSERVATION

The main research program of the KMTNet is to monitor galactic bulge and discover exoplanets. However, in seasons when the galactic bulge cannot be observed, other science programs were allocated observing time. Our study is one of these non-bulge science programs of the KMTNet. The KMTNet is composed of three 1.6m telescopes located in Chile (CTIO), South Africa (SAAO), and Australia (SSO), with a 4 deg2 field of view and 0.4′′ pixel size. The 24 hour, wide-field monitoring system allows all-day continuous monitoring of AGN.

In this paper we present observations of the COSMOS field (10:00:28.6 +02:12:21) using the KMTNet. For this pilot study, we use three nights worth of data that were taken at the CTIO station. The first observation was 2015 February 18 where we obtained the COSMOS field data for ∼2.5 hours of observation using B, V , R, and I bands. On 2015 March 21, we observed the COSMOS field again for ∼5 hours using B and R bands. Finally, on 2016 April 8, another observation was performed for ∼4 hours in B and R bands. Two to five consecutive frames, each with 1.5-2 min exposure time were taken in each band sequentially. The 2-5 frames are combined to produce a deeper single epoch image with a total exposure time of 3-10 min. Approximately, 5-13 sets of these data were taken, to produce 20-30 min cadence data per filter. The seeing conditions, which were measured using SExtractor, were ∼ 1.6′′ on 2015 February 18, ∼ 2.0′′ on 2015 March 21, and ∼ 1.8′′ on 2016 April 8. However, the weather condition was very unstable on 2015 March 21 and we excluded 4 epochs of data. Furthermore, the depth of the March data is shallower than for other dates and the observation log is provided in Table 1.

Table 1 
KMTNet-CTIO observations on the COSMOS field.
Date
yyyy.mm.dd
Band Duration time Total exposure time
per epoch
# Epoch Seeing 5σ Depth [mag]
per epoch
2015.02.18 B ∼2.5h 360s 5 1.5 - 2.0′′ 22.5 – 22.7
V ∼2.5h 240s 5 1.5 - 1.8′′ 22.2 – 22.4
R ∼2.5h 180s 5 1.4 - 1.8′′ 21.8 – 22.3
I ∼2.5h 180s 5 1.4 - 1.9′′ 21.1 – 21.4
2015.03.21 B ∼5h 600s 13 2.0 - 2.3′′ 21.4 – 22.6
R ∼5h 270s 13 1.5 - 2.1′′ 20.4 – 22.1
2016.04.08 B ∼4h 600s 11 1.6 - 2.1′′ 22.7 – 23.0
R ∼4h 270s 11 1.3 - 1.9′′ 21.9 – 22.3


3. DATA ANALYSIS

The basic data reduction, such as bias correction and flat-fielding, was done by the KMTNet pipeline at the KMTNet data center. We then performed astrometry, image stacking, and photometry calibration on the reduced data. First, we conducted astrometry following the basic process provided by the KMTNet team – Astrometric Calibration for the KMTNet Data.1 We used SExtractor (Bertin & Arnouts 1996), SCAMP (Bertin 2006), and SWarp (Bertin et al. 2002) software packages for astrometry and achieved astrometric accuracy of ∼ 0.2′′. SWarp is used again for co-addition of 2-5 frames that were taken consecutively at a given epoch. Because seeing condition varied during the night, systematic bias could be introduced when fixed aperture is used for photometry. To make images have similar seeing conditions, we applied Gaussian convolution based on the seeing FWHM of each image (i.e., downgrade the seeing FWHM of all images to the worst seeing image). Then, SExtractor was used again with S/N = 5 limit to produce source catalogs of the convolved images. In the 2015 February observation, there were ∼50,000, ∼65,000, ∼90,000, and ∼80,000 detected sources in B, V , R, and I bands, respectively, with a median photometric uncertainty of ∼0.1 mag. For the photometry calibration of the detected sources, we used the magnitudes of stellar sources from the photometric catalog of the COSMOS field (Capak et al. 2007). For the 2015 February data, the image depths at 5σ detection (point source) are 22.6, 22.3, 22.2, and 21.3 magnitudes in B, V , R, and I bands, respectively. Hereafter, we only use 8′′ aperture magnitude. This aperture covers > 95% of total flux and it corresponds to 3-4 times of the maximum seeing FWHM.


4. AGN SAMPLES

We selected AGN in X-ray, mid-infrared, radio, and optical bands. The multi-wavelength catalogs and our source catalogs are matched using 1 arcsec radius and the closest source within the radius is selected. Typically, between different catalogs, the coordinate differences are at the level of 0.2 to 0.4 arcsec for the matched sources. AGN are excluded from our selection in cases of saturation or column pattern in the KMTNet image, proximity to a bright source, or if any other source is within the aperture size used for photometry. In addition, we only selected AGN where the photometric error is smaller than 0.2 mag in our data. The following subsections describe AGN selection at different wavelengths. Since the number of selected AGN depends on the different depths for each observed night and band, we provide ranges for the number of detected AGN.

4.1. X-Ray Selected AGN

X-ray selected AGN are taken from Civano et al. (2012), where they classified AGN as broad line AGN (BLAGN) or not (non-BLAGN) if spectra were available, and obscured or unobscured AGN based on fitting their spectral energy distribution. There are 549 AGN identified in the 0.9 deg2 field of view covered by the Chandra-COSMOS catalog, but due to the depth of the KMTNet observations, only about 25–90 X-ray AGN are detected in the KMTNet images, depending on the date of the observing run and the filter. Table 2 shows an example of the X-ray detected AGN classification for the 2016 April data (also see Table 3 for the number of X-ray matched AGN). Roughly ∼ 80% of them are unobscured broad-line AGN. The X-ray flux range in 0.5–10 keV is 2.6 × 10-15 - 1.6 × 10-13 erg cm-2 s-1 while the X-ray luminosity is 5.4 × 1041 - 2.0 × 1044 erg s-1.

Table 2 
Classification of X-ray selected AGN in R band of the 2016 April data.
Class Unobsc Obsc no Class Total
Broad-line AGN 55 1 0 56
non Broad-line AGN 1 4 0 5
no Class 3 1 3 7
Total 59 6 3 68
obsc = obscured AGN

Table 3 
Numbers and fractions (in brackets) of detected and variable AGN.
2015.02.18 2015.03.21 2016.04.08
X-ray selected AGN
B 2/78 (2.6%) 0/47 (0%) 1/80 (1.3%)
V 2/85 (2.4%)
R 2/90 (2.2%) 0/25 (0%) 3/68 (4.4%)
I 2/61 (3.3%)
MIR selected AGN
B 5/151 (3.3%) 1/91 (1.1%) 7/153 (4.6%)
V 6/169 (3.6%)
R 5/174 (2.9%) 5/64 (7.8%) 3/151 (2.0%)
I 6/117 (5.1%)
Radio selected AGN
B 1/32 (3.1%) 0/14 (0%) 2/27 (7.4%)
V 3/47 (6.4%)
R 4/61 (6.6%) 0/24 (0%) 4/51 (7.8%)
I 4/61 (6.6%)
SDSS DR7 quasars
B 4/80 (5.0%) 4/85 (4.7%) 7/87 (8.0%)
V 2/83 (2.4%)
R 4/75 (5.3%) 4/65 (6.2%) 4/85 (4.7%)
I 3/72 (4.2%)

4.2. Mid-Infrared Selected AGN

Lacy et al. (2004) and Stern et al. (2005) suggest mid-infrared (MIR) color-color selection of AGN with Spitzer IRAC photometry. This method can effectively select more obscured AGN, though deeper IRAC data reveal contamination from normal galaxies. Here, we employed the recent selection method defined by Donley et al. (2012) to minimize contamination. From the Spitzer-COSMOS IRAC 4-channel photometry catalog (Sanders et al. 2007) which covers 2 deg2 of the COSMOS field, aperture corrected 1.9′′ photometry is used at the 5σ sensitivity limit in all channels. Consequently, 64–174 MIR selected AGN are detected in our data, depending on the date of the observation and the filter (Figure 1).


Figure 1. 
Mid infrared color-color diagram of the KMTNet detected sources in the COSMOS field. The x-axis is the ratio of 5.8 μm and 3.6 μm fluxes, while the y-axis shows the ratio of the 8.0 μm and 4.5 μm fluxes. Sources within the red solid lines are selected as AGN Donley et al. 2012. The median error of the points is shown in the bottom-right corner.

4.3. Radio Selected AGN

Radio sources in general are either AGN or star-forming galaxies, but bright radio sources are known to be mostly AGN. At the same time, the brightness of radio sources is known to evolve as a function of redshift. To differentiate AGN from star-forming galaxies, Magliocchetti et al. (2014) suggest a selection based on the radio power like

P1.4GHz>1021.7+zWHzsrif z1.8P1.4GHz>1023.5WHzsrif z>1.8(1) 

Here, the radio power at 1.4 GHz, P1.4GHz, is calculated as

P1.4GHz=F1.4GHzDL2×1+zα-1,(2) 

where F1.4GHz is the observed flux at 1.4 GHz, DL is the luminosity distance, and α is the power law index of the radio spectrum Fνν-α, and a canonical value of α = 0.7 is chosen here (e.g., Smolcic et al. 2014, 2017). This (1+z) term is included for the K-correction. Radio AGN in the COSMOS field are selected by applying this method to the 1.4 GHz radio flux in the VLA-COSMOS catalog (Schinnerer et al. 2007) covering 2 deg2 field of view. To calculate the radio power, we used the spectroscopic redshift catalog (Liily et al. 2009, Damjanov et al. 2018) and photometric redshift catalog (Ilbert et al. 2009) of the COSMOS field by assuming isotropic radio emission. This selection yields 14-61 AGN, depending on the date of the observation and the filter. Figure 2 shows the radio power versus redshift of radio sources matched with the KMTNet detected sources, as well as the radio selection criteria defined by Equation (1). Furthermore, we calculated the radio loudness like


Figure 2. 
The distribution of 1.4GHz radio power (x-axis) and redshift (y-axis) of the KMTNet detected sources in the COSMOS field. Radio-loud sources are shown with blue diamonds, while radio-quiet sources are indicated with black circles. The red solid line is the radio power cut used for the radio selection of AGN. Sources above the red solid line are selected as radio AGN. The radio power uncertainties are smaller than symbol size.

Ri=logF1.4GHzFi-band(3) 

where we classify radio-loud (quiet) sources as those where the radio loudness is larger (smaller) than 1 (Ivezic et al. 2002). The fraction of radio-loud sources is 30-60% in our radio AGN sample.

4.4. SDSS DR7 Quasars Catalog

Type 1 AGN can be selected from optical colors and we use those AGN that are identified in the SDSS DR7 quasar catalog (Schneider et al. 2010). They are luminous (Mi < -22), broad-line AGN for which physical parameters such as MBH are available in the catalog. Furthermore, the quasar selection is not limited to the COSMOS field, and the SDSS type 1 quasars are also identified in the KMTNet field of view outside the COSMOS field. We identify 65-87 SDSS DR7 quasars in the KMTNet field of view, depending on the date of observation and the filter.

4.5. Short Summary on AGN Selected with Different Methods

Figure 3 shows the positions of selected AGN from the 2016 April data in R band. As shown in the figure, some AGN are selected by more than one selection method. 68, 151, 51, and 85 AGN are selected from the X-ray, Mid-infrared, Radio, and SDSS quasar catalogs, respectively, in this particular case. Figure 4 shows the magnitude in R band versus the redshift of the selected AGN while Figure 5 shows the distribution of apparent magnitude (left) and redshift (right). The apparent magnitudes of radio selected AGN and SDSS quasars are brighter than MIR selected AGN and X-ray selected AGN. The median values of apparent magnitude are 20.6, 20.5, 20.0, and 19.4 for X-ray, MIR, Radio, and SDSS, respectively. In the case of redshift, X-ray selected AGN and SDSS quasars have higher redshift than MIR selected AGN and radio selected AGN. The median values are 1.45, 1.25, 0.56, and 1.55 for X-ray, MIR, radio, and SDSS, respectively. The list of detected AGN is given in Table 5 of Appendix A, where we list 394 AGN that are detected in the KMTNet data at least once in one of the three observing runs and one filter.


Figure 3. 
Positions of the selected AGN from the 2016 April data in R band. Green diamonds, red squares, black stars, and blue crosses correspond to the X-ray selected AGN, the MIR selected AGN, the radio selected AGN, and the SDSS quasars, respectively.


Figure 4. 
The apparent magnitude in R band and redshift of selected AGN from the 2016 April data. Green diamonds, red squares, black stars, and blue crosses correspond to X-ray selected AGN, MIR selected AGN, radio selected AGN, and matched SDSS quasars, respectively. The errors are smaller than the sizes of symbols.


Figure 5. 
The apparent magnitude (left) and redshift (right) histogram of AGN from the 2016 April data in R band. The median value (the vertical dashed line) and the dispersion of the distribution is given in each panel. Also given are the AGN selection methods in each right panel.


5. VARIABILITY OF AGN

Absolute photometry calibration is dependent on the photometry calibration error of the COSMOS catalog and can be uncertain by more than ∼ 10-2 mag. For this reason, absolute calibration is attempted on images from one of the epochs with the best quality. The photometry from the absolute calibration is kept as a reference to judge the amount of variations in magnitude for data on other nights. To obtain the light curve with higher accuracy, we performed differential photometry for the selected AGN. First, we identified stars within the COSMOS field using parameters in SExtractor by selecting sources with CLASS STAR (stellarity) greater than 0.95, and FLAGS=0. To select non-variable stars only, we performed differential photometry for each selected star using ∼20 other bright (< 16 mag) stars within 0.2 degree. The magnitude standard deviations of differential light-curves (σLC) for all stars are calculated. Then, we chose stars within 3-sigma cut of σLC in each 0.25 magnitude bin as non-variable stars (Figure 6). A few thousands to ten thousand non-variable stars are selected in each band and each night.


Figure 6. 
The standard deviation of the multi-epoch R band magnitudes for each star versus the mean R band magnitude of each star over the observed period. A red solid line is 3-sigma cut of σLC of stars in each 0.25 magnitude bin while a green solid line is median value of σLC. Stars below this red solid line are selected as non-variable stars.

Figure 6 shows an interesting trend where the σLC does not decrease below 0.003 mag even at very bright magnitudes (< 16 mag). Seen in a different way, Figure 7 shows σLC versus σphot, the error from the photometry measurement. The trend seen in Figure 6 persists, i.e., σLC staying above 0.003 mag even when σphot goes well below 0.003 mag. This trend suggests that there is a minimum photometric error possibly due to flat-fielding error, systematic uncertainties due to frame-to-frame photometry variation, geometric distortion effect, and other effects. An accurate estimation of photometric error is crucial when we classify variable AGN in order to minimize the number of false positives. Therefore, we set σint as the minimum intrinsic error, below which we cannot reduce the photometry error in the KMTNet data. Another source of error is identified at large σphot (> 0.01 mag) where σint is negligible. In this regime, σphot is found to be smaller than σLC by a factor of 1.2 to 1.4. We trace the cause of the difference to the re-sampling process in SWarp of sub-pixel shifted images for stacking that decreases background noise of the stacked image (Bertin et al. 2002). Note that a similar factor has been introduced in other AGN variability studies (e.g., Goyal et al. 2013b). Thus, we modeled the true photometry error, σcal, like


Figure 7. 
The standard deviation of the multi-epoch R band magnitudes for each star versus the mean photometric error of each star over the observed period. A green dashed line is the one-to-one line, and a red solid line is fitting result using Equation (4). It shows underestimation of photometric error.

σcal=σint2+η×σphot2(4) 

where η is an underestimation factor and σphot is the mean photometric error of an object over all epochs. The intrinsic error and underestimation factor are estimated from each band and each night by fitting the σLC versus σphot relation as in Figure 7. The typical σint value is 0.002–0.005 and the underestimation factor ranges between 1.2 and 1.4.

After the error calibration, we constructed the light curves of AGN by differential photometry using the closest (within 0.2 degree) ∼ 20 non-variable reference stars brighter than 16 mag for each corresponding filter. To detect variability, we used the χ2-test (de Diego 2010, Villforth et al. 2010). The χ2 value is calculated using the relation

χ2=imi-mi2σcal,i2.(5) 

Here, mi denotes magnitude of each epoch, <mi> is average magnitude over all epochs, and σcal,i is calibrated photometric error of each epoch. The p-value is calculated from the χ2-distribution. AGN are classified as variable when 1 - p > 0.95, meaning that we reject the null hypothesis of non-variability at the 95% confidence level (α = 0.05). Figure 8 shows σLC, χ2 (degree of freedom, dof = 10) and 1 - p of AGN from the 2016 April data in R band. We applied the χ2-test for comparison stars to examine the validity of the χ2-test. Except for the 2015 March data, the results show that 5-7% of stars are classified as variable, which is expected according to our variability criterion. The 2015 March data shows ∼12% fraction of variable stars, but we attribute this to the bad weather conditions during the 2015 March run. We also employ the C-test (Jang & Miller 1997, Romero et al. 1999) as a alternative statistical test. The C statistic is defined as


Figure 8. 
σLC (top), χ2 (middle) and 1-p (bottom) with their apparent magnitude of MIR selected AGN in R band of the 2016 April data (dof = 10 for the 11 epochs data). Red diamonds, blue squares, and black circles correspond to variable AGN, non-variable AGN, and non-variable stars, respectively. The χ2 are calculated by Equation (5). A black horizontal line denotes 1 - p = 0.95 and sources over this line are classified as variable AGN.

C=σmagσcal,i,(6) 

where <σcal,i> is the average photometric error over all the epochs. If the C value is greater than 1.95 (2.56), AGN can be classified as variable with 95% (99%) confidence level, assuming that the errors follow a Gaussian distribution. However, the χ2-test has an advantage that it uses photometric errors of each individual epoch unlike the C-test that uses the averaged photometric error. For that reason and since the C-test result is very similar to the χ2-test results, we mainly present the χ2-test results. The 1 - p and C-statistic values of the whole sample of 394 AGN are listed in Table 5.


6. RESULTS

Using the χ2-test, we could differentiate variable AGN from non-variable AGN. Table 3 shows the number of detected and variable AGN with their fraction in the bracket. As can be seen in Table 3, the fractions of variable AGN do not significantly exceed the 5% level that we found for the comparison stars. The results of the C-test at 95% confidence level is very similar to the χ2-test results (not listed in Table 3). We can conclude that many of the AGN that are classified as intra-night variable are unlikely to be truly intra-night variable.

Nevertheless, the probability that an AGN is truly variable becomes higher if the AGN is classified as variable in more than two data sets. If one AGN is classified as variable in two bands or nights at the 95% confidence level, then the expected probability of a false positive is only 0.25%. We identify eight AGN that are classified as intra-night variable in more than two bands or two nights both in the χ2-test and the C-test. We list these AGN in Table 4. The AGN name comes from their coordinate information in the KMTNet catalog (hhmmss.s+ddmmss) and their magnitudes are the mean magnitude over all observed epochs. The variability strength is defined by the error subtracted magnitude variation as shown in Equation (7) like

Table 4 
Parameters of eight variable AGN.
Name Selection Redshift Classification and log(MBH/M)) Band Mag σvar (σcal)
2015 Feb 18
σvar (σcal)
2015 Mar 21
σvar (σcal)
2016 Apr 8
100008.9+021440 X-ray
&MIR
2.536a Broad-line
Obscured
Radio-quiet
B 20.3 0.130 (0.039) 3 2
V 20.0 0.172 (0.038)
R 19.4 0.115 (0.027) 3 2
I 19.0 3
095820.7+020213 X-ray
&MIR
1.856a Broad-line
Unobscured
B 20.8 -0.029 (0.077) -0.100 (0.175) 0.051 (0.054)
V 21.0 -0.061 (0.115)
R 20.8 0.087 (0.142) 1 0.172 (0.101)
I 21.0 1
100151.1+020032 X-ray
&MIR
0.967c Broad-line
Unobscured
B 20.7 3 -0.117 (0.130) -0.045 (0.057)
V 20.3 0.097 (0.057)
R 20.3 0.142 (0.064) -0.169 (0.188) -0.017 (0.068)
I 20.0 0.101 (0.122)
095834.0+024427 MIR
&SDSS
1.887b Broad-line
&
8.88d
B 19.5 0.025 (0.020) -0.027 (0.047) 0.034 (0.017)
V 19.4 -0.019 (0.024)
R 19.3 0.010 (0.025) -0.049 (0.084) 0.018 (0.025)
I 18.9 0.027 (0.044)
100021.7+020000 Radio 0.219c Radio-quiet
&
Early-type
Galaxy
B 20.0 0.278 (0.042) 2 2
V 18.6 0.190 (0.014)
R 17.8 3 2 2
I 17.6 3
100017.7+030524 SDSS 2.178b Broad-line
&
8.38d
B 20.6 0.065 (0.046) -0.029 (0.111) 2
V 20.8 -0.019 (0.075) 1 2
R 20.7 0.104 (0.087)
I 20.1 -0.050 (0.098)
100434.3+025011 SDSS 1.215b Broad-line
&
8.94d
B 18.7 3 3 0.051 (0.011)
V 18.4 0.057 (0.011)
R 18.4 0.063 (0.010) 3 0.129 (0.017)
I 18.0 3
095621.6+024859 SDSS 0.956b Broad-line
&
8.99d
B 19.4 2 2 0.081 (0.017)
V 2
R 19.1 2 2 0.222 (0.024)
I 2
1: Too faint; 2: out of field of view; 3: contaminated; bold: variability strength from χ2 test

where σmag denotes the standard deviation of the differential light-curve and σcal is the mean calibrated photometric error. The variability strength of the variable AGN based on the χ2-test is shown in bold. AGN that were not selected for being too faint (a), out of field of view (b), and contamination by other sources or noise (c) are marked in the table.

σvar=σmag2-σcal2if σmag>σcalσvar=-σcal2-σmag2if σmag<σcal(7) 

In Figure 9, we plotted the light-curves of the eight variable AGN. The AGN names are shown on the right side of the light-curve and the color denotes each band. Variable AGN are plotted with solid lines while non-variable AGN are plotted with dashed lines.


Figure 9. 
The light-curves of eight variable AGN. The name of AGN shown on the right side of each light-curve and the color denotes each band. Variable AGN are plotted as solid lines while non-variable AGN are plotted as dashed lines.

100008.9+021440 This object is classified as a broad-line and obscured AGN in the Chandra-COSMOS identification catalog. The 2015 February data shows variability strength of 0.130 mag, 0.172 mag and 0.115 mag in B, V , and R bands, respectively with 20.3 mag, 20.0 mag, and 19.4 mag in each band. Unfortunately, no usable data were obtained in 2015 March and 2016 April.

095820.7+020213 This object is classified as a broad-line and unobscured AGN in the Chandra-COSMOS identification catalog. The variability of 0.050.17 mag is detected only in the 2016 April data, both in B and R bands.

100151.1+020032 This is a X-ray and MIRselected AGN which is classified as a broad-line and unobscured in the Chandra-COSMOS identification catalog. The variability is found only in the 2015 February data, with the σvar ∼ 0.1 - 0.14 in V and R bands.

095834.0+024427 A small amount of variability, ∼0.03 mag, is detected in B band in both the 2015 February and 2016 April data. This is a MIR-selected AGN which also appears in the SDSS quasar catalog.

100021.7+020000 Radio-loud AGN with 20.0, and 18.6 magnitudes in B and V bands, respectively. This object is classified as variable in B and V bands with variability strength of 0.278 and 0.190 mag, respectively. However, the SDSS spectrum has the characteristics of early-type galaxy, not AGN. The SDSS image shows the morphology of an early-type galaxy too. The variability can arise from an increased nuclear activity or due to an unidentified systematic error in measuring the central variability of an extended source like this.

100017.7+030524 SDSS quasar variable in B and R bands of the 2015 February data. The magnitudes are 20.6 and 20.7 in B, and R bands with 0.065 and 0.104 mag variability strength, respectively.

100434.3+025011 The brightest variable AGN in our sample. This SDSS quasar has apparent magnitudes of 18.7 and 18.4 in B and R bands, respectively. Variability is detected in both the 2015 February and 2016 April data with the strength of 0.06 to 0.13 magnitudes.

095621.6+024859 This object is found to be variable in the 2016 April data, with the variability strengths of 0.08 and 0.22 and B and R bands, respectively.

Table 5 
List of observed AGN
Name X M R S R mag z Ri 1-p (C value)
2015.02.18 2015.03.21 2016.04.08
B V R I B R B R
095621.66+024859.9 x x x o 19.1 0.95 -1 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 1.00 (7.23) 1.00 (11.7)
095642.33+020554.5 x x x o 19.4 1.03 -1 0.34 (1.04) 0.78 (1.40) -99 (-99) -99 (-99) 0.15 (1.02) 0.30 (0.97) 0.19 (1.19) 0.01 (0.73)
095642.71+024812.7 x x x o 19.7 2.00 -1 0.69 (1.53) 0.37 (1.17) 0.67 (1.40) 0.05 (0.66) 0.48 (1.12) 0.42 (0.79) 0.13 (1.12) 0.80 (1.53)
095657.63+011310.1 x x x o 20.2 2.33 -1 0.31 (1.00) 0.94 (1.90) 0.41 (1.16) 0.07 (0.78) 0.31 (1.06) 0.25 (1.11) 0.06 (1.00) 0.79 (1.55)
095659.32+015236.2 x x x o 20.6 1.55 -1 0.05 (0.62) 0.67 (1.40) 0.11 (0.74) 0.00 (0.37) 0.25 (1.23) -99 (-99) 0.18 (1.24) 0.01 (0.74)
095701.59+023857.3 x x x o 18.8 1.07 -1 0.37 (1.18) 0.20 (0.96) 0.18 (1.06) 0.56 (1.49) 0.64 (1.63) 0.12 (1.00) 0.21 (1.29) 0.00 (0.24)
095705.14+014949.5 x x x o 20.0 1.13 -1 0.20 (0.93) 0.72 (1.63) 0.00 (0.40) 0.31 (1.08) 0.16 (1.38) 0.40 (1.09) 0.01 (0.77) 0.79 (1.53)
095714.02+013145.5 x x x o 21.3 2.14 -1 0.08 (0.64) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.03 (0.82) 0.31 (1.07)
095718.27+024250.2 x o x o 19.5 1.49 -1 0.05 (0.67) 0.34 (1.01) 0.37 (1.15) 0.55 (1.34) 0.43 (0.94) 0.08 (1.06) 0.19 (1.22) 0.35 (1.21)
095722.92+023147.1 x o x x 21.1 -99 -1 0.63 (1.39) 0.17 (0.88) 0.52 (1.31) -99 (-99) -99 (-99) -99 (-99) 0.00 (0.73) 0.28 (1.19)
095723.69+011458.7 x x x o 19.7 2.47 -1 0.25 (1.00) 0.89 (1.70) 0.88 (1.64) -99 (-99) 0.52 (1.13) 0.22 (1.13) 0.04 (0.97) 0.45 (1.33)
095723.80+015615.3 x o x o 20.0 1.37 -1 0.03 (0.61) 0.25 (0.93) 0.82 (1.46) 0.68 (1.50) 0.13 (1.21) 0.66 (1.22) 0.78 (1.74) 0.02 (0.75)
095724.37+023518.8 x x x o 20.9 0.96 -99 0.26 (0.98) 0.01 (0.45) 0.02 (0.48) 0.99 (2.04) -99 (-99) -99 (-99) 0.11 (1.13) -99 (-99)
095726.05+024501.2 x o x x 20.1 -99 -99 0.31 (1.02) 0.98 (2.38) 0.57 (1.38) -99 (-99) 0.38 (1.17) -99 (-99) -99 (-99) -99 (-99)
095728.22+025002.4 x o x x 19.7 -99 -99 0.38 (1.11) 0.48 (1.14) 0.11 (0.74) 0.99 (2.86) 0.00 (0.57) 0.12 (0.77) 0.01 (0.83) -99 (-99)
095728.33+022542.1 x x x o 19.3 1.53 -99 0.46 (1.11) 0.06 (0.69) 0.06 (0.62) 0.47 (1.33) 0.47 (0.94) 0.84 (1.75) 0.11 (1.12) 0.00 (0.73)
095728.58+023147.3 x o x x 19.7 -99 -99 0.30 (1.02) 0.50 (1.17) 0.08 (0.65) 0.87 (1.94) 0.63 (1.54) 0.01 (0.56) 0.52 (1.57) 0.36 (1.16)
095731.52+012939.2 x o x x 21.2 -99 -1 -99 (-99) -99 (-99) 0.49 (1.17) -99 (-99) -99 (-99) -99 (-99) 0.21 (1.15) 0.04 (0.95)
095732.02+024301.8 x o x x 20.9 -99 -99 -99 (-99) 0.37 (1.12) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095734.40+025330.0 x o x x 21.5 -99 -99 0.23 (0.93) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.26 (1.28) 0.06 (0.85)
095735.07+020204.2 x o x x 20.3 -99 -99 -99 (-99) 0.87 (1.54) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095738.04+021931.8 x o x x 20.9 -99 -99 0.07 (0.59) 0.05 (0.63) 0.16 (0.85) -99 (-99) -99 (-99) -99 (-99) 0.01 (0.88) 0.82 (1.51)
095738.52+021656.3 x o x x 21.0 -99 -99 0.11 (0.70) 0.20 (0.85) 0.47 (1.13) -99 (-99) -99 (-99) -99 (-99) 0.03 (1.01) 0.37 (1.26)
095740.02+013109.4 x o x x 21.2 0.42 -99 -99 (-99) -99 (-99) 0.47 (1.28) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.44 (1.22)
095743.33+024823.8 x o x o 20.2 1.36 -99 0.29 (1.01) 0.15 (0.78) 0.63 (1.26) 0.42 (1.19) 0.10 (1.13) -99 (-99) 0.84 (1.88) 0.02 (0.79)
095743.80+012555.3 x o x x 20.5 -99 -1 0.30 (1.01) 0.19 (0.87) 0.10 (0.65) 0.77 (1.47) 0.18 (0.92) -99 (-99) 0.00 (0.59) 0.13 (0.99)
095745.96+021715.3 x x o x 20.3 0.50 2.01 -99 (-99) -99 (-99) -99 (-99) 0.54 (1.43) -99 (-99) -99 (-99) -99 (-99) 0.24 (1.01)
095745.98+022533.4 x x o x 18.8 0.49 0.78 0.66 (1.43) 0.83 (1.66) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095746.70+020711.8 x o x x 20.6 1.57 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.51 (1.43) 0.04 (0.76)
095746.90+022137.9 x x o x 18.9 0.34 0.95 0.48 (1.20) 0.01 (0.48) 0.17 (0.84) 0.43 (1.25) -99 (-99) 0.15 (0.79) 0.95 (2.13) 0.13 (0.99)
095749.99+013354.2 x o x o 19.9 2.01 -99 0.37 (1.10) 0.41 (1.06) 0.94 (2.44) 0.92 (2.02) 0.42 (0.98) 0.97 (1.54) 0.99 (3.09) -99 (-99)
095751.59+013342.0 x x o x 20.4 0.67 1.75 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 1.00 (3.56)
095752.32+022021.2 x x x o 18.4 2.05 -99 0.32 (1.09) 0.24 (0.95) 0.00 (0.24) 0.55 (1.39) 0.08 (0.76) -99 (-99) 0.33 (1.50) 0.62 (1.56)
095753.06+014114.5 x o x x 21.2 1.81 -99 0.01 (0.54) 0.42 (1.02) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.18 (1.06) -99 (-99)
095754.10+025508.7 x o x o 19.0 1.56 -1 0.67 (1.55) 0.35 (1.05) 0.51 (1.15) 0.98 (2.51) 0.13 (0.68) 0.02 (0.69) 0.05 (0.98) 0.54 (1.25)
095754.71+023832.9 x o x o 19.3 1.60 -99 0.30 (1.02) 0.26 (0.97) 0.37 (1.08) 0.63 (1.45) 0.13 (0.85) 0.02 (0.54) 0.74 (1.85) 0.61 (1.52)
095755.08+024806.6 x o x o 19.0 1.11 -99 0.11 (0.81) 0.01 (0.51) 0.78 (1.81) 0.30 (1.08) 0.32 (1.22) 0.05 (0.80) 0.51 (1.52) 0.06 (0.82)
095756.27+022344.8 x x o x 19.4 0.48 0.94 -99 (-99) 0.00 (0.41) 0.94 (2.33) 0.60 (1.46) -99 (-99) 0.72 (1.23) 0.29 (1.29) 0.05 (0.85)
095756.52+022717.3 x x o x 21.7 0.73 2.21 -99 (-99) -99 (-99) -99 (-99) 0.00 (0.41) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095756.60+025530.1 x o x x 20.8 -99 -1 0.09 (0.72) 0.01 (0.41) 0.00 (0.17) 0.09 (0.74) -99 (-99) -99 (-99) 0.16 (1.15) 0.07 (0.89)
095756.77+024841.0 x o x x 20.9 1.68 -99 0.39 (1.16) 0.22 (0.92) 0.13 (0.67) -99 (-99) -99 (-99) -99 (-99) 0.46 (1.47) 0.01 (0.70)
095757.48+014737.4 x o x x 21.4 -99 -99 -99 (-99) -99 (-99) 0.17 (0.86) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095758.41+021729.2 x o x x 21.6 2.24 -99 0.16 (0.83) 0.64 (1.19) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095758.77+021650.4 x x o x 19.0 0.30 0.71 -99 (-99) 0.95 (1.80) 0.40 (1.06) 0.24 (1.04) -99 (-99) -99 (-99) -99 (-99) 0.90 (1.84)
095759.51+020436.1 x o x o 19.1 2.03 -99 0.79 (1.58) 0.03 (0.57) 0.45 (1.11) 0.38 (1.28) 0.78 (1.81) 0.52 (1.57) 0.98 (2.32) 0.03 (0.80)
095800.78+013157.9 x o x x 21.4 0.66 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.08 (0.99)
095801.34+024328.0 x o o x 20.9 0.57 0.84 -99 (-99) -99 (-99) 0.73 (1.55) 0.04 (0.61) -99 (-99) -99 (-99) -99 (-99) 0.13 (0.91)
095804.62+014213.6 x o x x 21.3 0.01 -99 -99 (-99) -99 (-99) 0.69 (1.54) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.80 (1.49)
095805.76+025633.3 x o x x 21.3 -99 -1 -99 (-99) 0.05 (0.62) 0.06 (0.72) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095805.85+015159.0 x o x x 21.4 1.66 -99 0.48 (1.31) 0.00 (0.22) 0.09 (0.79) -99 (-99) -99 (-99) -99 (-99) 0.00 (0.72) 0.06 (0.85)
095808.76+020001.1 o x x x 18.7 -99 -99 0.49 (1.20) 0.12 (0.79) 0.50 (1.23) 0.23 (0.98) 0.53 (1.21) 0.29 (1.06) 0.63 (1.59) -99 (-99)
095810.88+014005.2 x o x o 20.0 2.10 -99 0.82 (1.64) 0.80 (1.40) 0.14 (0.86) 0.01 (0.50) 0.34 (1.14) -99 (-99) 0.51 (1.52) 0.03 (0.81)
095814.25+013751.9 x x o x 21.5 0.90 2.43 -99 (-99) -99 (-99) 0.75 (1.64) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095814.86+013203.0 x o x x 20.7 2.36 -99 0.04 (0.63) 0.41 (1.11) 0.87 (1.61) -99 (-99) 0.22 (0.85) -99 (-99) 0.17 (1.18) -99 (-99)
095815.28+014738.7 x o x x 21.8 1.83 -99 0.88 (1.80) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.19 (1.35) -99 (-99)
095815.50+015612.2 x o x x 20.1 0.38 -99 0.55 (1.23) 0.07 (0.65) 0.30 (1.09) 0.67 (1.58) -99 (-99) 0.45 (1.21) 0.06 (1.04) 0.98 (2.19)
095815.50+014922.9 x o x o 19.9 1.50 1.05 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.52 (1.45) 0.94 (2.08)
095815.53+015840.6 o o x x 21.1 1.67 -99 0.39 (1.09) 0.45 (1.13) 0.11 (0.80) 0.40 (1.16) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095818.23+015306.3 x o x x 20.3 0.34 -99 0.19 (0.87) 0.39 (1.09) 0.86 (1.59) 0.62 (1.59) -99 (-99) -99 (-99) -99 (-99) 0.89 (1.70)
095819.36+013530.6 x o x x 21.6 0.06 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.99 (2.72) -99 (-99)
095819.88+022903.5 x x x o 18.4 0.34 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.97 (2.31) 0.49 (1.37)
095820.45+020304.1 o o x o 19.7 1.35 -99 0.69 (1.36) 0.53 (1.38) 0.78 (1.52) 0.49 (1.37) 0.35 (1.15) 0.61 (1.05) 0.43 (1.45) 1.00 (3.42)
095820.78+020213.7 o o x x 20.8 1.85 -99 0.30 (1.08) 0.21 (0.98) 0.73 (1.37) -99 (-99) 0.60 (1.08) -99 (-99) 0.95 (2.03) 1.00 (2.49)
095821.40+025259.0 x o x x 20.0 0.31 -99 -99 (-99) -99 (-99) -99 (-99) 0.39 (1.23) -99 (-99) -99 (-99) -99 (-99) 0.12 (0.88)
095821.66+024628.2 x x x o 18.8 1.40 1.84 -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.53 (1.27) -99 (-99) -99 (-99) -99 (-99)
095821.82+014724.1 x x o x 20.5 0.46 1.20 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.24 (1.25)
095822.08+012653.1 x o x x 21.2 -99 -1 0.18 (0.85) 0.15 (0.68) 0.92 (1.75) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095822.19+014524.2 x x x o 17.5 1.96 0.00 -99 (-99) -99 (-99) -99 (-99) 0.48 (1.51) -99 (-99) 0.15 (0.89) 0.26 (1.86) 0.88 (2.07)
095823.74+011235.8 x x x o 18.9 0.50 -1 -99 (-99) 0.82 (1.73) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095824.02+024916.0 x x o x 18.4 0.34 2.19 0.02 (0.46) 0.05 (0.65) 0.79 (1.51) 0.71 (1.62) -99 (-99) -99 (-99) 0.47 (1.56) -99 (-99)
095825.79+012628.6 x o x x 20.9 -99 -1 0.65 (1.47) 0.24 (0.94) 0.69 (1.32) 0.99 (2.62) -99 (-99) -99 (-99) 0.32 (1.38) 0.12 (0.99)
095828.65+014407.8 x x o x 20.6 0.59 1.65 -99 (-99) 0.01 (0.43) 0.32 (0.95) 0.07 (0.65) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095829.25+024418.0 x o x x 20.2 1.15 -99 0.17 (0.88) 0.37 (1.07) -99 (-99) -99 (-99) 0.51 (1.22) -99 (-99) -99 (-99) -99 (-99)
095831.55+025205.5 x x o x 18.1 0.35 1.15 0.19 (0.89) 0.88 (1.78) 0.23 (1.08) 0.48 (1.33) 0.12 (1.11) 0.00 (0.51) 0.01 (0.86) 0.77 (1.63)
095832.46+023555.9 x o x x 21.5 2.38 -99 -99 (-99) 0.17 (0.81) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095833.27+021720.4 x o x x 20.5 0.23 -99 0.41 (1.07) 0.28 (1.00) -99 (-99) 0.01 (0.50) -99 (-99) -99 (-99) 0.06 (0.99) 0.42 (1.25)
095834.05+024427.2 x o x o 19.3 1.88 -99 0.96 (1.96) 0.09 (0.71) 0.65 (1.31) 0.64 (1.48) 0.17 (1.12) 0.17 (0.99) 1.00 (3.37) 0.86 (1.55)
095834.75+014502.4 x o x o 19.3 1.88 -99 0.57 (1.35) 0.56 (1.29) 0.64 (1.27) 0.07 (0.75) 0.13 (0.91) 0.02 (0.63) 0.99 (2.31) 0.72 (1.44)
095835.91+024954.9 x x o x 21.2 0.69 1.13 -99 (-99) -99 (-99) 0.13 (0.85) 0.04 (0.67) -99 (-99) -99 (-99) -99 (-99) 0.41 (1.29)
095835.98+015157.1 o o o o 19.6 2.94 0.87 0.40 (1.06) 0.00 (0.20) 0.74 (1.56) 0.01 (0.50) 0.66 (1.10) 0.47 (1.25) 0.18 (1.24) 0.31 (1.15)
095837.36+023602.9 x o x x 21.0 1.20 -99 -99 (-99) -99 (-99) 0.85 (1.68) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.20 (1.01)
095839.26+020506.8 o o x x 20.1 1.22 -99 0.00 (0.28) 0.24 (0.87) 0.77 (1.43) 0.11 (0.82) 0.24 (0.98) -99 (-99) 0.10 (1.07) -99 (-99)
095840.02+021711.1 o x x x 21.2 1.02 -99 0.01 (0.47) 0.90 (2.10) 0.19 (0.85) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095841.80+015318.2 o x x x 20.1 1.78 -99 0.30 (1.08) 0.02 (0.53) 0.10 (0.82) 0.28 (0.99) 0.02 (0.87) -99 (-99) 0.11 (1.09) -99 (-99)
095844.73+020249.7 x x o x 16.8 0.30 0.00 0.29 (1.26) 0.15 (0.92) 0.76 (2.56) 0.09 (1.10) 0.33 (1.54) 0.90 (1.90) -99 (-99) 0.31 (2.00)
095844.94+014309.0 x o x o 19.9 1.33 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.64 (1.36) 0.35 (1.19) 0.31 (1.28) -99 (-99)
095847.00+021552.3 o o x x 20.8 0.55 0.91 -99 (-99) -99 (-99) 0.14 (0.77) 0.76 (1.35) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095848.86+023441.2 x o x o 20.5 1.54 -99 -99 (-99) 0.10 (0.68) 0.17 (0.81) 0.87 (1.84) 1.00 (4.44) -99 (-99) 0.28 (1.23) 0.34 (1.14)
095849.03+013220.1 x x o x 19.4 0.50 1.12 0.64 (1.39) 0.19 (0.94) 0.25 (1.07) 0.79 (1.60) 0.12 (0.80) -99 (-99) 0.26 (1.18) -99 (-99)
095849.40+022511.1 o o x x 19.8 1.10 0.69 -99 (-99) 0.02 (0.45) -99 (-99) -99 (-99) 0.13 (1.09) -99 (-99) 0.65 (1.62) 0.81 (1.54)
095849.50+013111.5 x o x x 21.4 0.01 -99 -99 (-99) -99 (-99) 0.64 (1.45) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.27 (1.06)
095852.14+025156.6 x o x o 18.7 1.40 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.39 (1.32) 0.48 (1.23) 0.17 (1.23) 0.20 (0.96)
095852.26+013618.1 x x o x 20.9 0.79 0.95 -99 (-99) -99 (-99) 0.17 (1.09) 0.27 (1.05) -99 (-99) -99 (-99) -99 (-99) 0.27 (1.00)
095854.03+025737.2 x x x o 20.1 2.21 -1 0.98 (2.13) 0.88 (1.67) 0.26 (0.98) 0.91 (1.74) 0.24 (0.90) 0.47 (1.20) 0.25 (1.24) 0.00 (0.55)
095855.26+013510.1 x x o x 20.2 0.62 1.33 0.02 (0.53) 0.65 (1.31) 0.61 (1.46) 0.13 (0.85) -99 (-99) 0.04 (0.79) 0.55 (1.51) 0.80 (1.53)
095855.40+022037.3 x o x x 19.5 0.38 0.25 0.24 (0.94) 0.05 (0.64) 0.27 (0.91) 0.83 (1.68) 0.00 (0.68) -99 (-99) -99 (-99) -99 (-99)
095856.20+024127.9 x x o x 21.2 0.91 2.46 -99 (-99) -99 (-99) 0.58 (1.33) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.17 (1.00)
095856.22+012816.8 x o x o 20.2 1.55 -1 0.84 (1.69) 0.48 (1.17) 0.05 (0.58) 0.32 (1.14) 0.39 (1.20) 0.44 (0.83) 0.40 (1.51) 0.21 (1.33)
095857.03+020354.8 o x x x 20.8 0.67 0.18 -99 (-99) -99 (-99) 0.28 (1.11) 0.07 (0.81) -99 (-99) -99 (-99) -99 (-99) 0.37 (1.25)
095857.24+022602.0 o o x x 21.7 2.09 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.07 (0.97) -99 (-99)
095858.68+020139.2 o o x o 19.4 2.45 -99 0.00 (0.33) 0.84 (1.69) 0.02 (0.59) 0.02 (0.60) 0.08 (0.91) 0.17 (0.79) 0.40 (1.48) 0.04 (0.74)
095858.93+025329.9 x o x x 20.9 0.72 -99 -99 (-99) -99 (-99) 0.07 (0.69) -99 (-99) -99 (-99) -99 (-99) 0.03 (0.88) 0.55 (1.33)
095901.52+024740.6 x x o x 19.2 0.49 1.89 -99 (-99) 0.30 (1.00) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095902.31+021520.3 o x x x 21.0 -99 -99 -99 (-99) -99 (-99) 0.27 (0.91) 0.26 (1.04) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095902.75+021906.5 o x x o 18.4 0.34 0.09 0.27 (1.03) 0.01 (0.46) 0.18 (0.85) 0.87 (1.96) 0.13 (0.99) 0.03 (0.58) 0.34 (1.47) 0.06 (0.92)
095903.23+022003.0 o o x x 20.9 1.13 -99 0.08 (0.66) 0.12 (0.78) 0.37 (1.15) -99 (-99) -99 (-99) -99 (-99) 0.18 (1.24) 0.24 (1.15)
095905.12+021530.0 o o x x 21.2 2.22 -99 -99 (-99) 0.21 (0.87) 0.03 (0.53) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095905.55+025145.1 x o x x 19.6 0.43 -99 0.81 (1.54) 0.00 (0.40) 0.12 (0.72) 0.19 (0.94) -99 (-99) 0.04 (1.12) 0.24 (1.29) 0.26 (1.09)
095906.64+023845.3 x x o x 21.7 0.71 1.79 -99 (-99) -99 (-99) -99 (-99) 0.31 (1.04) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095908.32+024309.6 x x o o 18.2 1.31 2.65 0.93 (2.23) -99 (-99) 0.54 (1.31) 0.28 (1.08) 0.00 (0.57) 0.46 (1.57) 0.44 (1.52) 0.07 (0.91)
095908.69+025424.0 x x x o 18.6 1.55 -99 0.73 (1.66) 0.31 (1.00) 0.05 (0.59) 0.80 (1.81) 0.13 (0.89) 0.27 (1.00) 0.03 (1.02) 0.30 (1.14)
095909.54+021916.5 o o x x 20.1 0.37 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.25 (1.27) -99 (-99)
095910.82+021909.7 x x o x 21.2 0.76 1.28 -99 (-99) -99 (-99) 0.31 (0.95) 0.30 (1.08) -99 (-99) -99 (-99) -99 (-99) 0.07 (0.99)
095911.08+023350.8 o o x x 20.7 0.70 -99 0.09 (0.75) 0.46 (1.13) 0.28 (1.08) 0.48 (1.45) 0.04 (0.85) -99 (-99) 0.07 (1.09) 0.32 (1.16)
095911.16+024224.0 o x x x 21.3 -99 -99 -99 (-99) -99 (-99) 0.18 (0.93) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.99 (2.01)
095911.64+012603.1 x o x x 21.8 -99 -1 0.07 (0.60) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.05 (1.22) -99 (-99)
095913.92+023844.6 o o x x 21.3 2.08 -99 0.19 (0.90) 0.65 (1.30) 0.01 (0.42) -99 (-99) -99 (-99) -99 (-99) 0.04 (0.90) 0.11 (0.86)
095916.05+015048.2 o x x x 20.6 1.03 -99 -99 (-99) -99 (-99) 0.62 (1.32) 0.84 (1.64) -99 (-99) -99 (-99) 0.06 (1.04) 0.41 (1.15)
095917.27+015019.2 o o x x 20.9 1.34 -99 0.43 (1.17) 0.75 (1.53) 0.23 (0.81) 0.04 (0.63) -99 (-99) -99 (-99) 0.21 (1.37) 0.20 (1.14)
095919.82+024238.7 o o x x 20.5 2.12 -99 0.13 (0.79) 0.82 (1.63) 0.86 (1.65) 0.23 (1.04) 0.07 (0.96) -99 (-99) 0.01 (0.78) 0.08 (0.89)
095920.89+020031.9 o o x x 20.6 1.48 -99 0.08 (0.71) 0.55 (1.20) 0.60 (1.38) 0.08 (0.69) 0.03 (0.56) -99 (-99) -99 (-99) 0.02 (0.75)
095920.91+015203.6 o x x x 20.3 -99 -99 -99 (-99) 0.15 (0.88) 0.01 (0.50) 0.22 (0.98) -99 (-99) -99 (-99) -99 (-99) 0.04 (0.89)
095923.55+022227.4 o o x x 20.3 2.72 -99 0.03 (0.60) 0.85 (1.65) 0.57 (1.26) 0.76 (1.34) 0.00 (0.64) -99 (-99) 0.43 (1.43) 0.35 (1.18)
095924.47+015954.4 o o x o 18.3 1.23 -99 -99 (-99) 0.52 (1.24) -99 (-99) -99 (-99) 0.11 (0.82) 0.26 (0.73) 0.00 (0.69) -99 (-99)
095925.55+011532.7 x x x o 18.6 1.69 -1 0.56 (1.35) 0.59 (1.32) 0.57 (1.23) 0.10 (0.81) 0.57 (1.39) 0.62 (0.87) 0.08 (1.13) 0.17 (0.99)
095926.89+015341.5 o o x x 19.3 0.44 0.16 0.07 (0.64) 0.10 (0.73) 0.67 (1.29) 0.04 (0.63) -99 (-99) 0.56 (1.43) 0.08 (1.16) 0.28 (1.20)
095928.33+021950.6 o o x x 20.6 1.47 -99 0.11 (0.77) 0.26 (0.91) 0.00 (0.17) -99 (-99) 0.16 (0.92) -99 (-99) 0.36 (1.35) 0.06 (0.83)
095928.45+015934.8 o x x x 21.3 1.16 -99 0.04 (0.53) -99 (-99) 0.16 (0.90) -99 (-99) -99 (-99) -99 (-99) 0.08 (1.12) -99 (-99)
095928.72+021738.6 o o x x 21.5 3.34 0.99 -99 (-99) -99 (-99) 0.18 (1.01) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095929.23+022844.8 x x o x 21.6 0.73 1.85 -99 (-99) -99 (-99) 0.64 (1.25) 0.71 (1.53) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095929.24+022034.4 o o x x 21.7 1.73 -99 0.18 (0.82) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.01 (0.83) -99 (-99)
095929.33+021723.0 x x o x 21.2 0.68 1.10 -99 (-99) -99 (-99) 0.43 (1.29) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095930.20+024125.0 o o x x 21.6 2.16 -99 0.25 (1.00) 0.16 (0.78) 0.37 (1.14) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095931.44+022703.1 o x x x 21.2 1.31 0.81 0.39 (1.30) 0.53 (1.20) 0.14 (0.80) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095932.00+022048.4 o o x x 21.5 1.02 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.07 (0.98) -99 (-99)
095933.73+024056.7 o x x x 20.5 0.27 -99 0.51 (1.21) 0.10 (0.80) 0.55 (1.25) 0.09 (0.68) -99 (-99) -99 (-99) 0.26 (1.36) 0.15 (0.97)
095934.35+012849.4 x o x x 20.7 -99 -1 0.63 (1.24) -99 (-99) -99 (-99) 0.43 (1.27) -99 (-99) -99 (-99) 0.32 (1.35) 0.59 (1.42)
095934.75+020633.8 x x o x 21.2 0.67 1.09 -99 (-99) -99 (-99) 0.07 (0.59) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.39 (1.16)
095934.78+014553.9 x x o x 19.9 0.53 0.72 -99 (-99) 0.05 (0.64) 0.29 (1.01) 0.94 (2.15) -99 (-99) 0.00 (0.43) -99 (-99) 0.21 (1.12)
095935.43+013100.0 x o x x 20.7 1.49 -99 -99 (-99) 0.95 (1.51) 0.25 (0.96) 0.00 (0.36) -99 (-99) -99 (-99) 0.28 (1.36) 0.18 (1.08)
095935.50+020538.1 o o x x 21.7 1.91 -99 0.24 (0.93) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.08 (1.03) -99 (-99)
095935.59+015100.4 x x o x 21.0 0.63 1.02 -99 (-99) -99 (-99) 0.01 (0.35) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095935.68+024839.2 x o x o 20.4 1.97 -99 0.94 (1.97) 0.01 (0.48) 0.25 (1.06) 0.05 (0.71) 0.18 (1.16) -99 (-99) 0.56 (1.56) 0.17 (0.96)
095938.28+020450.1 o o x x 20.4 2.79 -99 0.10 (0.75) 0.14 (0.82) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095938.45+025329.4 x x o x 19.0 0.22 0.92 0.19 (0.88) 0.47 (1.24) 0.47 (1.12) 0.67 (1.57) -99 (-99) -99 (-99) -99 (-99) 0.08 (0.92)
095940.06+022306.8 o o x x 19.7 1.12 -99 0.55 (1.22) 0.17 (0.82) 0.01 (0.52) 0.80 (1.84) 0.09 (0.77) 0.48 (1.40) 0.35 (1.35) 0.19 (0.99)
095940.74+021938.9 o o o x 20.3 1.45 1.09 0.05 (0.64) 0.78 (1.53) 0.01 (0.48) 0.07 (0.80) 0.06 (1.00) 0.05 (0.64) 0.34 (1.40) 0.56 (1.29)
095941.41+015845.3 o x x x 21.7 2.50 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.00 (0.72) -99 (-99)
095942.08+024103.3 o o x x 20.5 1.79 0.63 0.35 (1.00) 0.70 (1.40) 0.20 (0.88) 0.75 (1.71) 0.15 (0.67) -99 (-99) 0.01 (0.77) 0.43 (1.24)
095942.72+023206.5 x x o x 21.1 0.67 1.00 -99 (-99) -99 (-99) 0.11 (0.70) 0.02 (0.47) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095944.14+025037.7 x o x x 21.4 1.11 -99 0.26 (1.01) 0.10 (0.81) 0.29 (0.89) -99 (-99) -99 (-99) -99 (-99) 0.07 (1.11) 0.07 (0.79)
095944.79+024048.9 o x x x 20.2 1.43 -99 0.37 (1.07) 0.81 (1.51) 0.60 (1.48) -99 (-99) 0.02 (0.62) -99 (-99) 0.47 (1.48) 0.15 (0.99)
095945.01+012828.8 x o x x 20.6 -99 -1 0.12 (0.79) 0.45 (1.15) 0.00 (0.40) -99 (-99) -99 (-99) -99 (-99) 0.48 (1.62) 0.22 (1.11)
095945.60+013032.2 x o x o 20.0 1.10 -99 0.77 (1.55) 0.21 (0.83) 0.76 (1.55) 0.06 (0.72) 0.37 (1.25) 0.06 (0.78) -99 (-99) 0.99 (2.57)
095946.02+024743.6 x x o o 18.7 1.06 0.51 0.06 (0.68) 0.40 (1.12) 0.18 (0.89) -99 (-99) 0.38 (1.38) 0.01 (0.58) 0.59 (1.70) 0.00 (0.68)
095946.36+023602.2 x x o x 19.5 0.30 2.28 0.33 (1.06) 0.19 (0.91) 0.00 (0.38) 0.11 (0.79) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095946.93+022209.4 o o x x 20.7 0.90 -99 0.67 (1.32) 0.25 (0.97) 0.20 (0.89) -99 (-99) 0.41 (1.44) -99 (-99) -99 (-99) -99 (-99)
095947.07+024806.8 x x o x 21.4 0.60 2.00 -99 (-99) -99 (-99) -99 (-99) 0.16 (0.86) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095949.40+020141.0 o o x o 19.2 1.75 -99 0.17 (0.87) 0.03 (0.57) 0.00 (0.36) 0.12 (0.84) 0.04 (0.65) 0.01 (0.53) 0.20 (1.28) 0.19 (1.12)
095949.85+020011.1 o o x x 21.1 1.80 -99 0.46 (1.14) 0.71 (1.46) 0.02 (0.49) -99 (-99) -99 (-99) -99 (-99) 0.13 (1.02) 0.22 (0.99)
095950.40+020156.7 o x x x 20.8 1.95 -99 -99 (-99) 0.93 (2.28) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095951.39+014049.3 x x o x 18.1 0.37 0.13 0.05 (0.57) 0.07 (0.69) 0.49 (1.21) 0.03 (0.62) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095954.24+022438.1 x x o x 21.4 0.71 1.64 -99 (-99) -99 (-99) 0.22 (0.97) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095954.78+013206.5 x o x x 20.0 0.85 -99 0.99 (2.64) 0.81 (1.65) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095957.98+014327.4 o o x o 20.2 1.62 -99 0.24 (0.85) 0.01 (0.43) 0.71 (1.52) 0.48 (1.25) 0.07 (0.91) -99 (-99) 0.01 (0.77) 0.11 (0.91)
095958.47+021530.7 o x x x 20.4 0.65 -99 0.42 (1.17) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
095958.54+021805.3 o o x x 20.1 1.78 -99 0.49 (1.24) 0.81 (1.77) 0.85 (1.40) 0.81 (1.94) 0.01 (0.64) -99 (-99) 0.09 (1.06) 0.33 (1.18)
095959.50+013151.7 x x o x 21.0 1.01 0.93 0.04 (0.55) 0.25 (1.03) 0.09 (0.65) 0.02 (0.56) -99 (-99) -99 (-99) 0.09 (0.97) 0.37 (1.26)
095959.63+024608.8 x x o x 17.0 0.16 0.64 0.53 (1.38) 0.98 (2.66) -99 (-99) -99 (-99) 0.83 (1.44) 0.18 (0.96) 0.97 (2.37) 0.57 (2.13)
100001.45+024844.7 x o x o 19.4 0.76 0.93 0.81 (1.68) 0.39 (1.08) 0.92 (1.68) 0.64 (1.47) 0.13 (1.00) 0.60 (1.08) 0.24 (1.32) 0.75 (1.51)
100001.76+024016.1 x o x x 21.4 0.01 -99 -99 (-99) -99 (-99) 0.25 (0.82) -99 (-99) -99 (-99) -99 (-99) 0.02 (0.88) 0.09 (0.97)
100005.44+023029.2 x x o x 20.6 0.74 1.97 -99 (-99) 0.01 (0.41) 0.19 (0.95) 0.07 (0.72) -99 (-99) -99 (-99) -99 (-99) 0.58 (1.56)
100005.98+015453.4 x o o x 21.2 0.94 1.10 -99 (-99) -99 (-99) 0.01 (0.44) 0.04 (0.62) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100006.19+015535.1 x o x x 21.5 0.68 -99 -99 (-99) -99 (-99) 0.32 (1.07) 0.16 (1.00) -99 (-99) -99 (-99) -99 (-99) 0.00 (0.40)
100007.35+024043.6 o x x x 21.8 1.93 -99 0.13 (0.78) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100008.15+013306.5 x o x o 20.4 1.17 -99 0.05 (0.64) 0.67 (1.31) 0.46 (1.29) -99 (-99) 0.02 (0.89) -99 (-99) 0.12 (1.09) 0.56 (1.31)
100008.43+020247.4 x o x x 20.6 0.36 0.84 -99 (-99) 0.60 (1.42) 0.38 (0.98) 0.20 (0.86) -99 (-99) -99 (-99) -99 (-99) 0.36 (1.05)
100008.93+021440.6 o o x x 19.4 2.53 0.50 1.00 (4.04) 1.00 (5.37) 1.00 (5.18) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100009.97+024741.7 x o x x 20.9 0.30 -99 0.95 (1.89) 0.54 (1.14) 0.55 (1.25) 0.85 (1.51) -99 (-99) -99 (-99) -99 (-99) 0.02 (0.78)
100010.15+024141.4 x x o x 18.1 0.21 0.92 -99 (-99) 0.55 (1.31) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100010.19+023745.2 o o x x 20.5 1.55 -99 0.48 (1.13) -99 (-99) -99 (-99) -99 (-99) 0.02 (0.78) -99 (-99) 0.46 (1.43) 0.16 (1.06)
100012.44+014058.0 o o x x 20.3 2.27 -99 0.16 (0.84) 0.06 (0.69) 0.91 (1.68) 0.14 (0.93) 0.02 (0.65) -99 (-99) 0.09 (1.02) 0.87 (1.62)
100012.91+023522.8 o x x o 18.5 0.69 -99 0.12 (0.86) 0.43 (1.17) -99 (-99) -99 (-99) 0.21 (1.10) -99 (-99) -99 (-99) -99 (-99)
100013.53+013739.0 x o x o 20.4 1.60 -99 0.11 (0.75) 0.01 (0.40) 0.27 (0.90) -99 (-99) -99 (-99) -99 (-99) 0.00 (0.69) 0.12 (0.95)
100013.70+013034.6 x o x x 20.0 0.31 -99 0.07 (0.64) 0.24 (0.91) -99 (-99) -99 (-99) 0.03 (0.76) 0.59 (1.53) 0.08 (1.04) -99 (-99)
100014.09+022838.7 o o x x 20.5 1.25 0.69 0.32 (1.04) 0.27 (1.03) 0.20 (0.97) 0.23 (0.89) 0.50 (1.25) -99 (-99) 0.20 (1.24) 0.16 (1.06)
100014.14+020054.6 o o x o 19.7 2.49 -99 0.78 (1.62) 0.12 (0.83) 0.02 (0.59) 0.01 (0.47) 0.38 (1.40) 0.77 (1.64) 0.00 (0.78) 0.43 (1.16)
100014.91+022718.0 o x x x 21.0 0.73 -99 0.25 (1.08) 0.20 (0.85) 0.70 (1.43) -99 (-99) -99 (-99) -99 (-99) 0.04 (1.04) 0.21 (1.02)
100016.11+025511.6 x o x x 21.0 -99 -1 -99 (-99) 0.35 (0.99) 0.41 (1.26) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.86 (1.46)
100016.29+015104.8 o o x x 21.2 1.13 0.65 -99 (-99) 0.94 (1.76) 0.23 (1.14) 0.00 (0.30) -99 (-99) -99 (-99) 0.07 (1.10) -99 (-99)
100016.83+015133.1 x x o x 19.9 0.33 1.45 -99 (-99) 0.31 (0.96) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.18 (1.08)
100017.53+020012.7 o x x x 20.7 0.35 -99 0.24 (0.93) 0.24 (0.96) 0.62 (1.36) 1.00 (5.50) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100017.73+030525.0 x x x o 20.7 2.17 -1 0.95 (2.01) 0.41 (1.10) 0.96 (1.83) 0.37 (0.86) 0.31 (1.28) -99 (-99) -99 (-99) -99 (-99)
100021.78+020000.2 x x o x 17.8 0.21 0.65 1.00 (7.85) 1.00 (13.8) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100040.09+024608.2 x o x x 21.7 1.93 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.05 (0.93) -99 (-99)
100040.13+024751.5 x o x x 21.6 0.57 -99 -99 (-99) 0.03 (0.54) 0.14 (0.86) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100041.16+020502.7 x x o x 21.8 0.73 1.39 -99 (-99) -99 (-99) -99 (-99) 0.99 (2.21) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100041.56+013659.0 x x o x 19.8 0.56 0.63 0.22 (0.88) 0.74 (1.47) 0.67 (1.39) 0.98 (2.24) -99 (-99) 0.91 (1.43) 0.09 (1.07) 0.05 (1.00)
100043.15+020637.4 o x x o 18.6 0.36 0.18 0.09 (0.71) 0.26 (0.97) 0.92 (1.94) 0.94 (2.13) 0.01 (0.75) 0.92 (1.97) 0.25 (1.26) 0.54 (1.38)
100043.64+014009.3 o o x x 20.1 2.02 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.04 (0.81) -99 (-99) 0.02 (0.89) -99 (-99)
100045.41+014712.7 x x o x 21.4 0.81 1.79 -99 (-99) -99 (-99) 0.25 (1.04) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100046.73+020404.5 o x x x 19.8 0.55 -99 0.81 (1.46) 0.10 (0.67) 0.93 (2.14) 0.07 (0.68) 0.28 (1.10) 0.33 (0.95) -99 (-99) 0.08 (0.84)
100046.89+025640.1 x o x x 19.3 -99 -1 -99 (-99) 0.54 (1.23) -99 (-99) 0.40 (1.20) -99 (-99) 0.87 (0.91) 0.26 (1.26) 0.09 (0.94)
100046.94+020016.0 o o x x 20.1 1.92 0.70 0.31 (1.03) 0.06 (0.64) 0.78 (1.61) 0.19 (0.88) 0.41 (1.39) 0.22 (0.56) 0.01 (0.84) 0.15 (1.00)
100048.82+015409.6 x o o x 21.3 0.70 1.13 -99 (-99) -99 (-99) -99 (-99) 0.05 (0.65) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100049.59+014923.7 x x o x 20.2 0.52 2.41 -99 (-99) 0.39 (0.93) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100049.91+020500.0 o o o x 19.3 1.23 0.78 0.09 (0.71) 0.71 (1.43) 0.44 (1.07) 0.45 (1.28) 0.06 (1.02) 0.07 (0.86) 0.29 (1.23) 0.23 (1.05)
100049.97+015231.3 o x x x 20.4 1.15 -99 0.84 (1.64) 0.02 (0.48) 0.71 (1.16) -99 (-99) 0.05 (0.93) -99 (-99) 0.01 (0.80) 0.13 (0.98)
100050.12+022855.0 o o x x 19.7 3.33 -99 0.00 (0.33) 0.59 (1.35) 0.50 (1.29) 0.11 (0.82) 0.03 (0.64) 0.74 (1.32) 0.00 (0.81) 0.14 (1.01)
100050.16+022618.5 o o x x 21.4 3.71 -99 -99 (-99) -99 (-99) 0.98 (2.01) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100050.43+021842.0 x x o x 21.3 0.71 1.09 -99 (-99) -99 (-99) 0.10 (0.71) 0.00 (0.38) -99 (-99) -99 (-99) -99 (-99) 0.14 (1.00)
100051.92+015919.5 o o x x 21.6 2.24 -99 0.11 (0.70) 0.18 (0.83) 0.30 (1.05) -99 (-99) -99 (-99) -99 (-99) 0.18 (1.25) -99 (-99)
100054.50+021605.1 o x x x 19.4 -99 -99 -99 (-99) -99 (-99) 0.32 (1.07) 0.12 (0.85) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100054.79+014602.5 x o x x 20.5 0.37 0.68 -99 (-99) 0.47 (1.32) 0.03 (0.61) 0.00 (0.38) -99 (-99) -99 (-99) -99 (-99) 0.57 (1.38)
100055.39+023441.4 o o x o 19.6 1.40 0.24 -99 (-99) -99 (-99) -99 (-99) 0.04 (0.63) 0.05 (1.06) 0.05 (0.87) 0.02 (0.92) 0.10 (0.92)
100055.63+022150.4 o o x x 21.0 1.93 -99 0.88 (1.68) 0.50 (1.20) 0.14 (0.81) -99 (-99) 0.12 (0.96) -99 (-99) 0.03 (0.91) 0.25 (1.03)
100055.65+013740.8 o x x x 20.5 0.38 -99 -99 (-99) 0.17 (0.75) 0.79 (1.71) 0.54 (1.33) -99 (-99) -99 (-99) -99 (-99) 0.92 (1.75)
100056.54+011319.1 x x x o 18.2 0.51 -1 0.18 (0.93) 0.32 (1.05) 0.23 (0.93) 0.98 (2.30) 0.88 (1.99) 0.01 (0.64) 0.85 (2.04) 0.56 (1.46)
100056.70+021720.8 o o x x 21.5 2.07 0.77 0.77 (1.56) 0.91 (2.09) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.68 (1.47) -99 (-99)
100057.26+013142.7 x x o x 19.1 0.39 0.54 0.38 (1.15) 0.88 (1.63) 0.93 (1.86) 0.39 (1.17) -99 (-99) -99 (-99) 0.59 (1.52) 0.01 (0.72)
100058.20+014559.0 o o x x 21.3 0.62 0.76 -99 (-99) -99 (-99) -99 (-99) 0.02 (0.57) -99 (-99) -99 (-99) -99 (-99) 0.00 (0.48)
100058.34+015208.8 o o x x 20.7 2.02 -99 0.24 (1.03) 0.17 (0.90) 0.22 (0.94) 0.44 (1.14) -99 (-99) -99 (-99) 0.50 (1.58) 0.25 (1.08)
100058.71+022556.2 o o x x 20.8 0.69 -99 0.79 (1.32) -99 (-99) 0.84 (1.85) 0.55 (1.39) -99 (-99) -99 (-99) 0.49 (1.35) 0.92 (1.66)
100058.84+015400.3 o o x o 19.9 1.55 -99 0.36 (1.03) 0.05 (0.61) 0.84 (1.82) 0.61 (1.48) 0.93 (2.26) 0.92 (1.57) 0.06 (1.04) 0.08 (0.96)
100100.21+015150.4 x x o x 20.0 0.30 1.05 -99 (-99) 0.03 (0.58) 0.51 (1.14) 0.68 (1.51) -99 (-99) -99 (-99) -99 (-99) 0.39 (1.15)
100100.31+024413.9 x o x x 21.1 1.20 -99 0.43 (1.24) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.08 (0.98) 0.91 (2.19)
100100.63+022910.8 x o x x 20.7 1.54 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.00 (0.57) -99 (-99)
100100.82+015947.9 o x x x 21.3 1.16 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.94 (2.02) 0.09 (0.88)
100102.16+011948.5 x x x o 19.5 2.15 -1 0.65 (1.44) 0.42 (1.12) 0.07 (0.74) 0.33 (1.04) 0.20 (1.41) 0.96 (1.65) 0.09 (1.04) 0.29 (1.13)
100102.81+020659.9 o o x x 21.1 1.37 1.04 1.00 (4.83) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.00 (0.86) 0.20 (1.13)
100103.74+015533.5 x x o x 18.1 0.30 0.18 0.07 (0.68) 0.61 (1.32) 0.27 (0.99) 0.17 (0.98) 0.11 (1.18) 0.25 (1.28) 0.49 (1.56) 0.40 (1.34)
100104.86+011421.3 x x x o 20.3 1.02 -1 0.11 (0.75) 0.51 (1.27) 0.38 (1.08) 0.35 (1.02) 0.51 (1.46) -99 (-99) 0.09 (1.01) 0.30 (1.04)
100106.38+030309.8 x x x o 19.0 0.60 -1 -99 (-99) 0.92 (1.71) -99 (-99) 0.67 (1.57) 0.60 (1.15) 0.07 (0.53) 0.48 (1.53) 0.61 (1.44)
100106.92+015734.4 x o x x 20.7 0.08 -99 0.09 (0.70) 0.62 (1.27) -99 (-99) 0.69 (1.53) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100107.67+012439.2 x x x o 19.6 1.63 -1 0.73 (1.52) 0.31 (1.01) -99 (-99) -99 (-99) -99 (-99) 0.85 (1.60) 0.75 (1.73) 0.68 (1.40)
100108.36+022342.2 o x x x 21.4 1.93 -99 0.62 (1.38) 0.22 (0.92) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.47 (1.49) 0.13 (0.91)
100108.55+020052.5 o o x x 21.1 2.67 -99 0.27 (1.00) 0.57 (1.17) 0.39 (1.19) -99 (-99) -99 (-99) -99 (-99) 0.28 (1.15) 0.38 (1.18)
100110.19+023242.4 o o x x 21.3 2.64 -99 -99 (-99) 0.01 (0.39) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100111.93+023024.9 o o x x 21.0 1.49 -99 0.03 (0.55) -99 (-99) 0.17 (0.89) -99 (-99) -99 (-99) -99 (-99) 0.03 (0.96) 0.05 (0.85)
100112.28+014123.9 x x o x 20.3 0.52 1.61 -99 (-99) 0.78 (1.56) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100113.58+020653.8 x x o x 20.4 0.32 1.26 -99 (-99) 0.14 (0.75) 0.60 (1.34) 0.94 (2.32) -99 (-99) -99 (-99) -99 (-99) 0.97 (1.71)
100113.84+014000.8 o o x x 20.9 1.56 -99 0.09 (0.75) 0.13 (0.77) 0.14 (0.82) -99 (-99) -99 (-99) -99 (-99) 0.23 (1.21) 0.04 (0.83)
100113.93+022548.3 o x x x 20.4 0.37 -99 0.67 (1.66) 0.47 (1.21) 0.12 (0.68) 0.12 (0.86) -99 (-99) 0.03 (0.58) 0.00 (0.72) 0.00 (0.71)
100114.14+015444.2 o x o x 21.5 1.48 4.01 -99 (-99) -99 (-99) 0.06 (0.60) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100114.29+022356.9 o o x o 18.8 1.79 -99 0.54 (1.30) 0.84 (1.60) 0.01 (0.46) 0.41 (1.26) 0.25 (1.19) 0.08 (0.58) 0.64 (1.63) 0.24 (1.09)
100114.84+015840.6 o o x x 21.5 2.34 -99 -99 (-99) 0.36 (1.04) 0.13 (0.78) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100114.96+014348.3 x o x x 20.1 0.58 0.64 -99 (-99) 0.20 (0.82) 0.23 (0.86) 0.06 (0.67) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100115.38+024231.7 x o x x 20.8 0.45 -99 -99 (-99) -99 (-99) 0.04 (0.67) 0.92 (1.78) -99 (-99) -99 (-99) -99 (-99) 0.00 (0.45)
100116.29+023607.6 o x x x 20.9 0.95 -99 0.75 (1.45) 0.64 (1.24) 0.15 (0.87) 0.00 (0.21) -99 (-99) -99 (-99) 0.00 (0.65) -99 (-99)
100116.79+014053.8 o o x o 19.8 2.05 -99 0.91 (1.81) 0.52 (1.21) 0.25 (0.86) 0.52 (1.34) 0.85 (1.90) 0.33 (1.48) 0.41 (1.37) 0.13 (1.00)
100116.94+013804.2 o o x x 20.8 0.74 -99 0.89 (1.76) 0.60 (1.28) 0.28 (1.02) 0.09 (0.80) -99 (-99) -99 (-99) 0.61 (1.49) 0.02 (0.77)
100118.10+013625.4 x x o x 18.4 0.22 0.50 0.23 (0.99) 0.30 (1.02) -99 (-99) 0.93 (2.09) 0.57 (1.07) 0.12 (0.92) 0.51 (1.48) 0.60 (1.50)
100118.58+022739.3 o o x x 20.1 1.04 0.84 -99 (-99) 0.21 (0.85) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100120.25+020341.2 o o x x 20.0 0.90 -99 0.70 (1.43) 0.00 (0.38) 0.75 (1.63) 0.06 (0.73) 0.68 (1.98) 0.24 (0.89) -99 (-99) -99 (-99)
100120.26+023341.4 o o x o 19.9 1.83 -99 0.18 (0.92) 0.81 (1.60) 0.14 (0.78) 0.03 (0.64) 0.00 (0.56) 0.20 (0.99) 0.00 (0.67) 0.41 (1.34)
100122.46+020112.5 x x o x 20.1 0.42 2.52 -99 (-99) -99 (-99) -99 (-99) 0.74 (1.62) -99 (-99) -99 (-99) -99 (-99) 0.33 (1.09)
100124.10+024936.4 x x o x 21.7 0.82 2.52 -99 (-99) -99 (-99) -99 (-99) 0.19 (0.96) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100124.74+015738.8 o o x x 21.2 1.17 -99 -99 (-99) 0.33 (0.98) 0.05 (0.61) -99 (-99) -99 (-99) -99 (-99) 0.31 (1.50) 0.06 (0.89)
100124.86+022031.9 o x x x 20.5 1.70 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.01 (0.67) -99 (-99) 0.35 (1.37) -99 (-99)
100125.30+012820.3 x o x o 20.0 2.61 -1 0.30 (0.98) 0.70 (1.60) 0.68 (1.59) 0.38 (1.19) 0.63 (1.36) 0.00 (0.44) 0.00 (0.73) 0.13 (0.96)
100128.00+021819.4 o x x x 21.3 1.18 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.19 (1.21) 0.27 (0.97)
100129.19+011715.9 x x x o 18.5 1.60 -1 0.02 (0.52) 0.68 (1.35) 0.58 (1.45) 0.03 (0.64) 0.23 (1.32) 0.23 (0.98) 0.97 (2.26) 0.05 (0.88)
100129.67+020643.3 o o x x 20.5 1.91 -99 0.84 (1.66) 0.61 (1.41) 0.09 (0.62) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.30 (1.08)
100130.38+014304.4 o o o o 20.1 1.56 0.83 0.47 (1.21) 0.46 (1.17) 0.81 (1.71) 0.08 (0.73) 0.10 (0.85) -99 (-99) 0.14 (1.14) 0.43 (1.35)
100131.67+024530.1 x o x x 21.4 0.58 -99 0.01 (0.42) -99 (-99) 0.94 (2.19) -99 (-99) -99 (-99) -99 (-99) 0.71 (1.56) 0.00 (0.56)
100132.15+013420.8 x o x o 19.4 1.35 -99 0.00 (0.41) 0.02 (0.54) 0.08 (0.69) 0.23 (0.99) 0.11 (1.02) 0.58 (1.24) 0.97 (2.16) 0.31 (1.15)
100132.82+015800.0 o o x x 20.8 1.53 -99 0.00 (0.32) 0.12 (0.81) 0.41 (1.18) 0.38 (1.25) -99 (-99) -99 (-99) 0.00 (0.77) 0.12 (0.93)
100133.48+020017.4 x o x x 20.8 0.10 0.56 -99 (-99) -99 (-99) 0.00 (0.29) 0.98 (1.79) -99 (-99) -99 (-99) -99 (-99) 0.16 (1.06)
100135.45+025405.9 x o x x 20.6 0.99 -99 0.44 (1.14) 0.07 (0.70) 0.37 (1.29) 0.78 (1.43) -99 (-99) -99 (-99) 0.07 (1.03) 0.01 (0.76)
100136.24+015443.1 o o x x 20.9 2.28 -99 -99 (-99) 0.02 (0.43) 0.19 (0.82) 0.15 (1.04) -99 (-99) -99 (-99) 0.67 (1.56) 0.54 (1.26)
100136.46+022641.9 x x o x 16.8 0.12 0.32 0.22 (1.05) 0.45 (1.41) -99 (-99) 0.80 (2.62) 0.75 (1.45) 0.21 (1.26) -99 (-99) -99 (-99)
100136.50+025303.6 x x x o 19.2 2.11 -99 0.02 (0.49) 0.11 (0.76) 0.38 (0.99) 0.47 (1.32) 0.00 (0.46) 0.08 (0.62) -99 (-99) 0.87 (1.85)
100137.21+021612.5 o o x x 20.6 1.66 -99 -99 (-99) 0.66 (1.32) 0.92 (1.85) 0.95 (1.92) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100141.03+015903.9 x x o x 18.5 0.32 0.70 0.09 (0.66) 0.93 (1.93) 0.36 (1.14) 0.56 (1.43) -99 (-99) 0.78 (2.05) -99 (-99) -99 (-99)
100143.04+014932.1 o o x x 21.9 2.08 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.02 (0.81) -99 (-99)
100143.23+020512.8 x x o x 20.6 0.67 1.03 0.14 (0.74) 0.66 (1.35) 0.95 (2.11) 0.90 (1.73) -99 (-99) -99 (-99) 0.16 (1.05) 0.45 (1.35)
100145.16+022457.0 x x x o 20.7 2.03 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.16 (1.01) -99 (-99) -99 (-99) -99 (-99)
100146.05+012839.7 x o x x 21.4 -99 -1 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.04 (0.80)
100146.49+020256.8 o o x x 20.2 0.66 -99 0.85 (1.82) 0.84 (1.51) 0.69 (1.44) 0.45 (1.36) 0.03 (0.67) -99 (-99) -99 (-99) -99 (-99)
100147.04+020236.6 o o x x 20.8 1.17 -99 0.34 (0.93) 0.61 (1.24) 0.30 (0.98) 0.93 (1.82) -99 (-99) -99 (-99) -99 (-99) 0.08 (0.88)
100147.29+015258.3 x x o x 20.6 0.67 1.36 -99 (-99) -99 (-99) 0.11 (0.77) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100147.35+020314.3 x x o x 18.0 0.32 1.18 -99 (-99) -99 (-99) 0.80 (1.91) 0.32 (1.26) -99 (-99) 0.59 (1.32) -99 (-99) 0.97 (2.10)
100148.86+023140.5 o o x x 21.2 1.93 -99 0.31 (0.98) 0.40 (1.07) 0.13 (0.76) -99 (-99) -99 (-99) -99 (-99) 0.33 (1.29) 0.75 (1.42)
100149.00+024821.7 x o x x 20.3 1.50 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.52 (1.62) 0.18 (0.92) 0.36 (1.38) 0.44 (1.20)
100149.84+020344.9 o o x x 21.2 2.37 -99 -99 (-99) -99 (-99) 0.08 (0.57) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100150.67+022552.2 x o x x 20.2 1.28 -99 0.41 (1.15) 0.19 (0.91) 0.37 (1.05) 0.12 (0.85) 0.11 (1.06) -99 (-99) -99 (-99) -99 (-99)
100151.12+020032.6 o o x x 20.3 0.96 -99 -99 (-99) 0.98 (2.27) 0.99 (2.88) 0.77 (1.64) -99 (-99) 0.00 (0.54) 0.03 (0.90) 0.39 (1.19)
100153.29+022436.8 o o x x 20.4 0.66 0.22 -99 (-99) -99 (-99) 0.79 (1.63) 0.14 (0.89) -99 (-99) -99 (-99) 0.12 (1.11) 0.18 (1.01)
100153.71+015427.3 x x o x 20.6 0.56 0.98 -99 (-99) -99 (-99) -99 (-99) 0.48 (1.16) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100154.40+024236.5 x o x x 20.8 1.51 -99 -99 (-99) 0.28 (0.95) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100154.51+021507.8 x x o x 20.4 0.78 0.90 -99 (-99) -99 (-99) 1.00 (4.17) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100155.52+020358.6 x x o x 20.5 0.30 1.15 -99 (-99) -99 (-99) 0.83 (1.58) 0.74 (1.69) -99 (-99) -99 (-99) -99 (-99) 0.33 (1.23)
100155.60+021623.4 o o x x 20.7 1.43 -99 0.38 (0.97) 0.09 (0.75) 0.05 (0.67) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100157.78+024631.7 x o x x 20.3 0.84 -99 -99 (-99) 0.78 (1.50) 0.93 (1.72) 0.01 (0.42) 0.02 (0.57) 0.21 (0.90) 0.10 (1.11) 0.18 (0.99)
100158.00+014621.4 x o x x 21.1 0.84 -99 -99 (-99) -99 (-99) 0.34 (0.94) 0.14 (0.81) -99 (-99) -99 (-99) -99 (-99) 0.07 (1.18)
100158.19+012735.6 x o x x 19.1 -99 -1 0.33 (1.07) 0.67 (1.37) 0.72 (1.69) 0.35 (1.19) 0.48 (1.36) 0.01 (0.53) 0.15 (1.17) 0.23 (1.13)
100158.95+022445.3 o x x x 21.4 1.37 0.67 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.73 (1.73) 0.19 (1.18)
100159.21+012828.6 x o x x 20.4 -99 -1 0.45 (1.21) 0.00 (0.41) -99 (-99) 0.22 (0.98) -99 (-99) -99 (-99) -99 (-99) 0.83 (1.72)
100159.43+023935.7 x o x x 19.9 1.37 -99 0.37 (1.13) 0.92 (1.79) 0.98 (2.33) 0.02 (0.52) 0.02 (0.80) 0.56 (1.50) 0.61 (1.57) 0.03 (0.82)
100159.79+022641.7 o o x x 19.2 2.03 -99 -99 (-99) 0.24 (0.94) 0.53 (1.18) 0.05 (0.63) 0.53 (1.22) -99 (-99) -99 (-99) -99 (-99)
100159.86+013135.3 x o x x 21.4 0.30 -99 0.12 (0.76) 0.13 (0.76) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.11 (1.00)
100201.52+020329.4 o o x o 18.2 2.02 -99 0.73 (1.66) 0.97 (2.17) -99 (-99) -99 (-99) 0.80 (1.65) 0.58 (1.05) 0.21 (1.16) -99 (-99)
100202.23+024157.8 x o x x 21.2 1.53 -99 0.14 (0.78) -99 (-99) 0.36 (0.99) -99 (-99) -99 (-99) -99 (-99) 0.39 (1.38) -99 (-99)
100202.78+022434.6 o o x o 20.8 0.98 -99 -99 (-99) -99 (-99) 0.69 (1.53) -99 (-99) 0.24 (1.21) -99 (-99) 0.00 (0.85) 0.54 (1.29)
100204.67+013339.6 x o x x 20.3 1.01 -99 -99 (-99) 0.25 (0.86) 0.49 (1.40) -99 (-99) -99 (-99) -99 (-99) 0.63 (1.56) 0.56 (1.33)
100208.27+015838.8 x x o x 21.0 0.68 1.18 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.08 (0.88)
100208.55+014553.7 x o x x 21.5 1.98 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.03 (0.92) 0.01 (0.70)
100210.72+023026.2 x o x o 19.0 1.16 -99 0.13 (0.90) 0.20 (0.84) 0.00 (0.42) 0.78 (1.70) 0.06 (0.65) 0.02 (0.70) 0.02 (0.88) 0.08 (0.87)
100211.16+012228.4 x x x o 19.6 1.81 -1 0.64 (1.40) 0.06 (0.70) 0.87 (1.55) 0.71 (1.82) 0.29 (0.93) 0.07 (0.90) 0.01 (0.81) 0.27 (1.17)
100212.11+014232.4 x o x x 20.1 0.70 0.37 0.92 (2.08) 0.84 (1.55) 0.03 (0.52) 0.11 (0.86) 0.29 (1.13) 0.05 (0.32) 0.04 (0.98) 0.03 (0.79)
100216.15+023013.0 x o x x 21.2 0.37 0.88 -99 (-99) -99 (-99) 0.38 (0.92) 0.56 (1.46) -99 (-99) -99 (-99) -99 (-99) 0.02 (0.77)
100217.42+022959.8 x o x x 20.6 0.30 -99 0.08 (0.68) 0.54 (1.27) 0.82 (1.71) -99 (-99) -99 (-99) -99 (-99) 0.29 (1.40) 0.27 (1.12)
100217.97+015836.4 x o o x 21.2 0.90 3.39 0.01 (0.42) 0.93 (1.61) 0.95 (1.83) -99 (-99) -99 (-99) -99 (-99) 0.06 (0.94) 0.87 (1.53)
100218.31+022804.3 x x o x 20.7 0.55 1.52 -99 (-99) -99 (-99) -99 (-99) 0.78 (1.81) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100219.43+025049.6 x o x x 20.5 0.69 -99 0.04 (0.62) 0.20 (0.80) 0.32 (1.16) 0.72 (1.54) -99 (-99) -99 (-99) 0.15 (1.26) 0.06 (0.90)
100219.50+015537.1 x o x o 19.6 1.51 -99 0.17 (0.82) 0.09 (0.71) 0.35 (1.05) 0.56 (1.26) 0.29 (1.38) 0.95 (1.47) 0.02 (0.84) 0.52 (1.61)
100221.95+022041.9 o x x x 19.8 -99 -99 -99 (-99) 0.27 (1.02) 0.94 (1.92) -99 (-99) -99 (-99) 0.38 (1.18) 0.42 (1.25) 0.23 (1.03)
100222.98+020640.1 x o x x 21.2 0.43 -99 -99 (-99) -99 (-99) 0.53 (1.24) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.38 (1.22)
100223.05+014715.0 x o x x 21.1 1.25 -99 0.09 (0.66) 0.71 (1.41) 0.59 (1.62) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.04 (0.82)
100223.93+022353.6 o o x x 20.5 2.83 -99 -99 (-99) 0.02 (0.45) 0.05 (0.54) 0.65 (1.47) -99 (-99) -99 (-99) 0.22 (1.19) 0.05 (0.85)
100226.11+024610.9 x o x x 19.9 0.29 -99 0.17 (0.83) 0.49 (1.19) 0.20 (0.84) 0.18 (0.98) 0.02 (0.65) 0.01 (0.75) 0.61 (1.56) -99 (-99)
100226.33+021923.2 o o x o 20.5 1.29 -99 0.33 (1.11) 0.00 (0.43) 0.94 (1.67) 0.13 (0.87) -99 (-99) -99 (-99) 0.26 (1.23) 0.24 (1.16)
100226.94+015939.9 x o x x 21.7 1.46 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.22 (1.32) -99 (-99)
100228.92+013544.4 x x o x 20.0 0.58 0.94 -99 (-99) -99 (-99) -99 (-99) 0.11 (0.81) -99 (-99) -99 (-99) -99 (-99) 0.57 (1.30)
100229.02+010858.4 x x x o 19.5 0.68 -1 0.28 (0.99) -99 (-99) -99 (-99) -99 (-99) 0.82 (1.53) 0.88 (2.02) 0.18 (1.04) -99 (-99)
100229.89+023225.2 x o o x 19.4 0.44 1.70 -99 (-99) 0.40 (1.23) 0.01 (0.44) 0.96 (2.25) -99 (-99) 0.01 (0.61) -99 (-99) -99 (-99)
100230.14+024212.7 x x o x 18.2 0.21 1.07 0.53 (1.23) -99 (-99) -99 (-99) 0.99 (3.37) 0.47 (1.06) 0.73 (1.47) 0.02 (0.89) -99 (-99)
100230.17+014555.7 x o x x 21.2 0.77 -99 -99 (-99) -99 (-99) 0.20 (0.72) -99 (-99) -99 (-99) -99 (-99) 0.05 (1.02) 0.74 (1.27)
100230.64+024427.7 x o x x 20.0 0.36 0.56 0.49 (1.10) 0.08 (0.71) 0.30 (1.03) 0.48 (1.27) 0.00 (0.56) 0.65 (1.21) 0.20 (1.14) 0.91 (1.65)
100231.85+015242.5 x o x x 21.2 -99 0.69 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.96 (1.70)
100232.13+023537.4 x o x o 19.1 0.65 0.13 0.40 (1.17) 0.64 (1.28) 0.39 (1.11) 0.13 (0.86) 0.37 (1.48) 0.16 (0.76) 0.67 (1.66) 0.27 (1.11)
100232.48+023859.7 x o x x 20.9 0.56 -99 0.69 (1.39) 0.20 (0.84) 0.02 (0.42) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100236.70+015948.8 x o x o 19.6 1.51 -99 0.08 (0.78) 0.54 (1.22) 0.21 (0.94) 0.62 (1.34) 0.20 (0.97) 0.58 (0.96) 0.84 (1.92) 0.63 (1.32)
100238.25+013746.8 x o x o 19.2 2.50 -99 0.24 (0.98) 0.35 (1.06) -99 (-99) -99 (-99) 0.80 (1.85) -99 (-99) 0.88 (2.00) 0.09 (0.88)
100238.61+015831.2 x o x x 21.2 1.85 -99 0.46 (1.16) 0.28 (1.00) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100238.70+013936.6 x o x x 20.7 0.57 -99 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.27 (1.22) 0.04 (0.80)
100241.34+014256.6 x x o x 20.6 0.63 1.22 -99 (-99) -99 (-99) 0.26 (0.93) 0.14 (0.90) -99 (-99) -99 (-99) -99 (-99) 0.15 (0.98)
100241.43+013309.2 x o x x 21.4 0.21 -99 0.62 (1.43) -99 (-99) 0.23 (0.98) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100243.70+024707.9 x o x x 19.7 0.01 -99 -99 (-99) 0.16 (0.82) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.18 (1.17) 0.25 (1.20)
100243.85+020502.6 x o x x 20.9 0.57 -99 0.00 (0.31) 0.20 (0.90) 0.43 (1.25) -99 (-99) -99 (-99) -99 (-99) 0.00 (0.69) 0.47 (1.22)
100244.74+020735.0 x x o x 20.2 0.67 1.39 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.77 (1.49) 0.27 (1.19)
100246.34+024609.7 x o x x 19.4 0.23 -99 0.22 (0.93) -99 (-99) 0.35 (1.26) 0.00 (0.48) 0.52 (1.04) 0.18 (1.09) 0.00 (0.81) 0.00 (0.67)
100246.93+015301.2 x x o x 19.5 0.52 0.54 -99 (-99) 0.26 (0.90) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.32 (1.37) 0.59 (1.51)
100247.00+024538.7 x x o x 20.8 0.47 1.10 -99 (-99) -99 (-99) 0.48 (1.26) 0.89 (1.88) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100249.00+021750.7 x o x x 21.5 2.50 -99 -99 (-99) 0.92 (1.46) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.21 (1.08)
100249.32+023746.6 x o x x 19.9 0.01 2.24 0.50 (1.21) -99 (-99) -99 (-99) -99 (-99) 0.04 (0.77) 0.37 (1.36) 0.06 (1.00) -99 (-99)
100249.92+021732.4 x o x x 21.0 1.60 -99 0.24 (0.87) 0.89 (1.72) 0.65 (1.12) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.61 (1.34)
100251.62+022905.4 x o x o 19.3 2.00 -99 0.40 (1.18) 0.71 (1.45) 0.28 (0.93) 0.10 (0.79) 0.40 (1.41) 0.67 (1.29) 0.26 (1.27) 0.64 (1.55)
100252.34+013319.7 x o x x 21.2 1.27 -99 -99 (-99) 0.99 (2.27) 0.41 (0.98) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.60 (1.43)
100252.87+025426.9 x o x x 19.9 0.01 -99 0.81 (1.78) 0.45 (1.06) 0.09 (0.76) 0.87 (1.72) 0.23 (1.04) 0.07 (0.96) 0.15 (1.17) 0.34 (1.24)
100252.96+024137.0 x o x x 19.9 0.02 -99 -99 (-99) 0.87 (1.66) 0.49 (1.14) 0.72 (1.50) 0.39 (1.26) 0.96 (1.43) 0.31 (1.27) -99 (-99)
100255.80+020242.0 x o x x 21.2 1.26 -99 0.57 (1.31) -99 (-99) 0.59 (1.22) -99 (-99) -99 (-99) -99 (-99) 0.63 (1.42) 0.01 (0.72)
100255.89+013730.5 x o x x 20.3 1.91 -99 0.84 (1.58) 0.18 (0.89) 0.79 (1.36) 0.65 (1.38) 0.45 (1.18) 0.15 (1.15) 0.03 (0.94) 0.68 (1.40)
100258.96+022724.9 x o x x 21.1 1.09 -99 -99 (-99) 0.45 (1.04) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100259.94+020249.5 x x o x 20.0 0.60 0.74 0.66 (1.51) 0.00 (0.36) 0.99 (2.79) 0.79 (1.66) -99 (-99) 0.26 (0.83) 0.05 (0.94) 0.00 (0.61)
100302.93+015208.6 x o x o 20.1 1.79 -99 0.08 (0.75) 0.18 (0.87) 0.43 (1.21) 0.30 (1.13) 0.05 (0.76) 0.96 (1.38) 0.03 (0.86) 0.00 (0.44)
100303.48+022632.0 x o x x 21.2 0.69 -99 -99 (-99) -99 (-99) 0.81 (1.61) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100304.18+024420.5 x o x x 20.2 1.86 -99 0.89 (1.80) 0.35 (0.95) -99 (-99) -99 (-99) 0.64 (1.04) 0.41 (1.26) 0.88 (2.08) 0.12 (0.99)
100304.72+013351.6 x x o x 21.4 0.94 1.13 -99 (-99) -99 (-99) 0.46 (0.95) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100305.08+015156.4 x o x x 20.5 0.14 -99 0.10 (0.76) 0.57 (1.25) 0.16 (0.81) 0.78 (1.61) -99 (-99) -99 (-99) 0.06 (1.06) 0.58 (1.31)
100305.98+015704.1 x x o x 19.7 0.38 0.73 0.27 (0.98) 0.02 (0.51) 0.08 (0.67) 0.87 (1.85) -99 (-99) 0.21 (1.30) 0.81 (1.68) 0.74 (1.74)
100307.48+023655.9 x x o x 19.4 0.31 1.90 0.58 (1.35) 0.61 (1.34) 0.43 (1.36) 0.07 (0.75) -99 (-99) 0.89 (1.91) 0.09 (1.08) 0.09 (0.94)
100308.22+024837.7 x o x x 20.1 1.25 -99 0.31 (0.95) 0.54 (1.32) 0.15 (0.74) -99 (-99) 0.96 (1.80) 0.91 (1.34) -99 (-99) 0.74 (1.35)
100308.58+024323.0 x o x x 20.6 0.01 -99 0.91 (1.78) 0.47 (1.12) 0.90 (1.52) -99 (-99) 0.65 (1.28) -99 (-99) 0.02 (0.92) 0.52 (1.30)
100308.79+012316.5 x x x o 20.3 2.32 -1 0.92 (1.86) 0.89 (1.94) 0.98 (2.38) 0.49 (1.27) -99 (-99) -99 (-99) 0.87 (2.03) 0.29 (1.15)
100309.21+013507.5 x x o x 20.3 0.37 1.80 -99 (-99) 0.38 (1.04) 0.82 (1.79) 0.44 (1.31) -99 (-99) -99 (-99) -99 (-99) 0.93 (1.68)
100309.21+022038.3 x x x o 19.9 1.96 -99 0.95 (1.81) 0.83 (1.74) 0.51 (1.16) -99 (-99) 0.18 (1.23) 0.71 (1.22) 0.17 (1.19) 0.78 (1.50)
100309.55+025248.7 x o x x 21.4 0.39 -99 -99 (-99) 0.38 (1.05) 0.82 (1.48) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.34 (1.05)
100309.75+020838.9 x x o x 19.9 0.39 0.77 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 1.00 (7.40)
100315.02+013354.8 x o x x 21.6 0.68 -99 -99 (-99) -99 (-99) 0.90 (1.41) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100316.12+024002.7 x x o x 20.5 0.48 1.06 -99 (-99) 0.17 (0.85) 0.21 (0.92) 0.90 (1.96) -99 (-99) -99 (-99) -99 (-99) 0.64 (1.49)
100316.27+024237.4 x o x x 18.5 0.56 -99 0.19 (0.90) 0.84 (1.79) 0.56 (1.25) 0.39 (1.22) 0.86 (1.73) 0.89 (1.53) 0.13 (1.13) 0.47 (1.34)
100316.36+014223.7 x o x x 21.5 1.72 -99 0.26 (0.99) 0.20 (0.89) 0.04 (0.66) -99 (-99) -99 (-99) -99 (-99) 0.16 (1.16) -99 (-99)
100317.38+013602.9 x x o x 20.2 0.67 0.72 0.43 (1.30) 0.26 (0.96) 0.14 (0.77) 0.29 (1.07) -99 (-99) 0.46 (1.16) 0.58 (1.49) 0.08 (0.88)
100317.94+022355.6 x o x x 20.2 0.01 -99 0.88 (1.81) 0.10 (0.76) 0.87 (1.56) 0.93 (2.15) 0.14 (0.97) 0.99 (1.33) 0.29 (1.30) 0.52 (1.37)
100319.81+012719.1 x o x x 21.8 -99 -1 -99 (-99) 0.20 (0.83) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100320.06+022042.9 x o x x 21.7 -99 -99 0.00 (0.35) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100323.93+015503.8 x o x x 19.4 -99 -99 0.68 (1.39) 0.83 (1.67) 0.56 (1.42) 0.12 (0.88) 0.23 (0.87) 0.64 (1.72) 0.21 (1.26) 0.73 (1.48)
100324.57+021831.3 x x x o 18.2 0.51 -99 0.68 (1.74) 0.56 (1.32) 0.42 (1.16) 0.16 (0.95) 0.18 (0.88) 0.96 (1.67) 0.91 (2.30) 0.15 (1.16)
100327.68+015742.4 x x x o 18.2 1.06 -99 0.70 (1.59) 0.31 (1.08) 0.40 (1.10) 0.81 (1.79) 0.66 (1.48) 0.39 (1.16) 0.68 (1.84) 0.44 (1.34)
100328.50+022018.7 x o x x 21.3 -99 -99 -99 (-99) -99 (-99) 0.01 (0.49) 0.32 (1.06) -99 (-99) -99 (-99) -99 (-99) -99 (-99)
100333.05+023904.4 x x x o 20.4 0.66 -1 -99 (-99) 0.34 (1.03) 0.22 (0.92) 0.67 (1.43) 0.24 (1.08) -99 (-99) 0.25 (1.28) 0.40 (1.13)
100333.57+024530.5 x x x o 18.6 1.92 -1 0.91 (2.01) 0.14 (0.79) 0.51 (1.30) 0.71 (1.61) 0.24 (0.89) 0.41 (1.10) 0.77 (2.10) 0.69 (1.47)
100333.99+024126.3 x x x o 19.3 0.98 -1 0.38 (1.12) 0.27 (0.96) 0.40 (1.18) 0.00 (0.45) 0.73 (1.80) 0.84 (1.86) 0.13 (1.13) 0.16 (1.01)
100350.28+013145.8 x x x o 19.2 1.18 -1 0.55 (1.26) 0.05 (0.62) 0.01 (0.50) 0.15 (0.90) 0.99 (2.31) -99 (-99) 0.11 (1.12) 0.21 (1.07)
100357.18+022638.9 x x x o 18.7 1.48 -1 0.02 (0.56) 0.71 (1.38) -99 (-99) -99 (-99) 0.06 (0.90) -99 (-99) 0.76 (1.81) -99 (-99)
100358.73+014513.6 x x x o 20.1 1.41 -1 0.17 (0.86) 0.02 (0.52) 0.44 (1.07) 0.16 (0.89) 0.26 (1.15) -99 (-99) 0.63 (1.54) 0.00 (0.61)
100407.21+012039.0 x x x o 20.6 1.84 -1 0.13 (0.82) 0.71 (1.37) 0.83 (1.39) 0.19 (0.96) 0.97 (1.96) -99 (-99) -99 (-99) 0.93 (1.68)
100409.29+024946.4 x x x o 19.1 1.59 -1 -99 (-99) -99 (-99) -99 (-99) -99 (-99) -99 (-99) 0.32 (0.99) 0.00 (0.81) 0.50 (1.30)
100421.02+013647.4 x x x o 18.5 1.03 -1 0.25 (1.04) 0.75 (1.49) 0.99 (2.72) 0.00 (0.39) 0.91 (2.05) 0.20 (1.05) 0.52 (1.55) 0.31 (1.19)
100423.49+030658.9 x x x o 19.0 0.91 -1 0.05 (0.64) 0.08 (0.68) 0.02 (0.50) 0.19 (1.01) 0.57 (1.13) 0.49 (0.99) 0.33 (1.37) 0.31 (1.16)
100429.00+025209.2 x x x o 18.5 0.87 -1 0.07 (0.69) 0.54 (1.29) -99 (-99) 0.00 (0.48) 0.07 (0.58) 0.31 (1.24) 0.20 (1.17) 0.50 (1.40)
100434.37+025011.0 x x x o 18.4 1.21 -1 -99 (-99) 1.00 (6.45) 1.00 (7.94) -99 (-99) 1.00 (4.99) -99 (-99) 1.00 (7.39) 1.00 (10.0)
X = X-ray selected AGN, M = MIR selected AGN, R = Radio selected AGN, S = SDSS DR7 quasar
The value ”-1” in Ri is source which position is out of the VLA field of view
The dof values used for the statistic are typically 4, 12, 10 for the 2015.02.18, 2016.03.21 and 2016.04.08 data respectively.


7. DISCUSSION AND CONCLUSION

In our pilot study, we identified eight intra-night variable AGN out of 394 (∼ 2%). The smallness of the fraction can be due to the photometric error of the targets in our sample which is in the range 0.01 to 0.1 mag. In previous studies, Gupta & Joshi (2005), Carini et al. (2007), and Goyal et al. (2013a), concluded that the INOV fraction of AGN with 12-19 magnitudes is 10-30%, but their photometric error is ∼ 10-3 mag. In particular, Goyal et al. (2013a) show that peak-to-peak variabilities of most AGN are less than 0.05 mag. We compared the peak-to-peak variability and the variability strength used in our study and we find the peak-to-peak variability corresponds to about three times the variability strength. The minimum variability strength of the eight INOV AGN in our study is ∼0.03 mag (095834.0+024427), so we can detect a peak-to-peak variability of at least ∼0.09 mag. We checked with Goyal et al. (2013a) and find that the fraction of AGN with the peak-to-peak variability greater than 0.09 mag is 4.8%. This is roughly consistent with the 2% in our results, considering that most of AGN in this study have higher photometric uncertainty than 095834.0+024427. In addition, Webb & Malkan (2000), Carini et al. (2003), Klimek et al. (2004), Bachev et al. (2005), and Kumar et al. (2016), show no variability or very small fraction of variability with ∼ 10-2 mag photometric error. However, when investigating INOV of a very small amplitude (0.01 or less), we caution that there can be intrinsic errors such as the one we discussed in Section 5. In our case, the intrinsic error amounts to 0.004 mag or so. As also discussed in Bachev et al. (2005), ignoring this effect could lead to spurious detection of INOV. For now, we conclude that the low fraction of INOV AGN indicates that the INOV amplitude is quite small if there is any – smaller than our photometric error.

Several possible INOV mechanisms have been suggested: (i) the accretion disk instability; (ii) the X-ray irradiation of an accretion disk; (iii) the variation in jet activity such as a weak blazar component (See Czerny et al. 2008). AGN with large MBH are expected to show very weak INOV variability from the accretion disk instability (e.g., Bachev et al. (2005); Czerny et al. 2008), but some INOV AGN in our sample are found to have MBH as massive as 108 - 109M. It will be interesting to see if there is a correlation between MBH and the INOV variability as a way to support the accretion disk instability model. Otherwise, the accretion disk instabilities do not easily produce 0.1 mag level INOV observed in the 8 AGN. For the X-ray irradiation instability, the variability time-scale is predicted to be a week or longer for high MBH (> 108M) AGN. Furthermore, strong irradiation is required, which is not compatible with general broad-band spectral shape of AGN (Czerny et al. 2008). Therefore, like the accretion disk instability model, the X-ray irradiation model faces a difficulty. This leaves the jet-related variability such as a weak blazar component as a plausible mechanism for the INOV of the 8 AGN. The small fraction of INOV AGN, however, suggests that this is not a common event.

We cross-matched the eight INOV AGN with long-term variability studies in the COSMOS field to determine whether there is a relation between short-term and long-term variability. De Cicco et al. (2015) used optical monitoring data from the VLT survey telescope to select AGN by variability. There are 5 months monitoring data covering the COSMOS field, which confirmed 67 AGN with variability. However, their list of variable AGN do not match with the eight variable AGN found in this study. Simm et al. (2015, 2016) used 4-years of the Pan-STARRS data to examine AGN variability. Among our eight variable sources, three (095820.7+020213, 095834.0+024427, and 100151.1+020032) AGN are matched with their samples. For these three AGN, year-scale variability is found in several bands. So far, the result is mixed whether the INOV AGN show long-term variability, and future investigation is necessary to reach to a firm conclusion.

The AGN long-term variability is attributed to the changes in accretion disk activities. A long-term variability of 0.1 mag over, say 30 days, can produce an INOV variability of about 0.003 mag. Detecting this kind of INOV variability can possibly be used to diagnose if an AGN is undergoing a long-term AGN variable activities. This kind of observation is beyond the scope of this study, but could be achieved with future observations with improved strategies and facilities.

There are two aspects where we can improve the study with the current instrument. One is to increase the exposure time to lower the photon noise, and another is to extend the observing period of the monitoring to catch intermittent AGN variation which was reported in other studies. We are now performing a longer term, higher S/N monitoring study and we hope to report the new results in near future that are based on the improved observing strategy. A significant improvement in the INOV study sensitivity is also expected from future large, wide-field telescopes such as the Large Synoptic Survey Telescope (Juric et al. 2015), or high-cadence space missions such as Kepler.



Acknowledgments

We thank the anonymous referee for useful comments. This research made use of the KMTNet system operated by the Korea Astronomy and Space Science Institute (KASI) and data obtained at the host site of CTIO in Chile. This research was supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education (NRF-2017R1A6A3A04005158). We would like to thank CEOU (Center for the Exploration of the Origin of the Universe) members who gave helpful comments and support.


References
1. Abolfathi, B., Aguado, D. S., Aguilar, G., et al, (2017), The Fourteenth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the extended Baryon Oscillation Spectroscopic Survey and from the second phase of the Apache Point Observatory Galactic Evolution Experiment, arXiv:1707.09322.
2. Aranzana, E., Kording, E., Uttley, P., Scaringi, S., & Bloemen, S., (2018), Short Time-Scale Optical Variability Properties of the Largest AGN Sample Observed with Kepler/K2, MNRAS, 476, p2501.
3. Bachev, R., Strigachev, A., & Semkov, E., (2005), Short-Term Optical Variability of High-Redshift Quasi-Stellar Objects, MNRAS, 358, p774.
4. Bertin, E., & Arnouts, S., (1996), SExtractor: Software for Source Extraction, A&AS, 117, p393.
5. Bertin, E., Mellier, Y., Radovich, M., Missonnier, G., Didelon, P., & Morin, B., (2002), The TERAPIX Pipeline, ASPC, 281, p228.
6. Bertin, E., (2006), Automatic Astrometric and Photometric Calibration with SCAMP, ASPC, 351, p112.
7. Capak, P., et al, (2007), The First Release COSMOS Optical and Near-IR Data and Catalog, ApJS, 172, p99.
8. Carini, M. T., Noble, J. C., & Miller, H. R., (2003), Microvariability in Seyfert Galaxies, AJ, 125, p1811.
9. Carini, M. T., Noble, J. C., Taylor, R., & Culler, R., (2007), Optical Microvariability in Radio-Quiet Quasars, AJ, 133, p303.
10. Carini, M. T., & Ryle, W. T., (2012), Kepler Observations of the Seyfert 1 Galaxy II ZW 229.015, ApJ, 749, p70.
11. Chen, X.-Y., & Wang, J.-X., (2015), Analyses of the Variability Asymmetry of Kepler AGN, ApJ, 805, p80.
12. Civano, F., et al, (2012), The Chandra COSMOS Survey. III. Optical and Infrared Identification of X-Ray Point Sources, ApJS, 201, p30.
13. Czerny, B., Siemiginowska, A., Janiuk, A., & Gupta, A. C., (2008), The Nature of the Intranight Variability of Radio-Quiet Quasars, MNRAS, 386, p1557.
14. Damjanov, I., et al, (2018), hCOSMOS: A Dense Spectroscopic Survey of r ≤ 21.3 Galaxies in the COSMOS Field, ApJS, 234, p21.
15. De Cicco, D., Paolillo, M., Covone, G., et al, (2015), Variability-Selected Active Galactic Nuclei in the VST-SUDARE/VOICE Survey of the COSMOS Field, A&A, 574, pA112.
16. de Diego, J. A., (2010), Testing Tests on Active Galactic Nucleus Microvariability, AJ, 139, p1269.
17. Dobrotka, A., Antonuccio-Delogu, V., & Bajcicakova, I., (2017), New Structures of Power Density Spectra for Four Kepler Active Galactic Nuclei, MNRAS, 470, p2439.
18. Donley, J. L., (2012), Identifying Luminous Active Galactic Nuclei in Deep Surveys: Revised IRAC Selection Criteria, ApJ, 748, p142.
19. Edelson, R., Vaughan, S., Malkan, M., et al, (2014), Discovery of a ∼5 Day Characteristic Timescale in the Kepler Power Spectrum of Zw 229-15, ApJ, 795, p2.
20. Frank, J., King, A., & Raine, D. J., (2002), Accretion Power in Astrophysics, Cambridge, Cambridge University Press.
21. Gopal-Krishna, Gupta, A. C., Sagar, R., Wiita, P. J., Chaubey, U. S., & Stalin, C. S., (2000), Rapid Optical Variability in Radio-Quiet QSOs, MNRAS, 314, p815.
22. Gopal-Krishna, Stalin, C. S., Sagar, R., & Wiita, P. J., (2003), Clear Evidence for Intranight Optical Variability in Radio-Quiet Quasars, ApJ, 586, pL25.
23. Goyal, A., Gopal-Krishna, Joshi, S., Sagar, R., Wiita, P. J., Anupama, G. C., & Sahu, D. K., (2010), Optical Variability of Radio-Intermediate Quasars, MNRAS, 401, p2622.
24. Goyal, A., Gopal-Krishna, Wiita, P. J., Anupama, G. C., Sahu, D. K., Sagar, R., & Joshi, S., (2012), Intra-Night Optical Variability of Core Dominated Radio Quasars: the Role of Optical Polarization, A&A, 544, pA37.
25. Goyal, A., Gopal-Krishna, Wiita, P. J., Stalin, C. S., & Sagar, R., (2013a), Improved Characterization of Intranight Optical Variability of Prominent AGN Classes, MNRAS, 435, p1300.
26. Goyal, A., Mhaskey, M., Gopal-Krishna, Wiita, P. J., Stalin, C. S., & Sagar, R., (2013b), On the Photometric Error Calibration for the Differential Light Curves of Point-Like Active Galactic Nuclei, JA&A, 34, p273.
27. Gupta, A. C., & Joshi, U. C., (2005), Intra-Night Optical Variability of Luminous Radio-Quiet QSOs, A&A, 440, p855.
28. Ilbert, O., Capak, P., Salvato, M., et al, (2009), Cosmos Photometric Redshifts with 30-Bands for 2-deg2, ApJ, 690, p1236.
29. Ivezic, Z., Menou, K., Knapp, G. R., et al, (2002), Optical and Radio Properties of Extragalactic Sources Observed by the FIRST Survey and the Sloan Digital Sky Survey, AJ, 124, p2364.
30. Jang, M., & Miller, H. R., (1995), The Examination of Optical Microvariability in Radio-Quiet and Radio-Loud Quasi-Stellar Objects, ApJ, 452, p582.
31. Jang, M., & Miller, H. R., (1997), The Microvariability of Selected Radio-Quiet and Radio-Loud QSOs, AJ, 114, p565.
32. Joshi, R., Chand, H., Gupta, A. C., & Wiita, P. J., (2011), Optical Microvariability Properties of BALQSOs, MNRAS, 412, p2717.
33. Juric, M., et al, (2015), The LSST Data Management System, arXiv:1512.07914.
34. Kasliwal, V. P., Michael, S. V., & Gordon, T. R., (2015), Are the Variability Properties of the Kepler AGN Light Curves Consistent with a Damped Random Walk?, MNRAS, 451, p4328.
35. Kim, S.-L., Lee, C.-U., Park, B.-G., et al, (2016), KMTNet: A Network of 1.6m Wide-Field Optical Telescopes Installed at Three Southern Observatories, JKAS, 49, p37.
36. Klimek, E. S., Gaskell, C. M., & Hedrick, C. H., (2004), Optical Variability of Narrow-Line Seyfert 1 Galaxies, ApJ, 609, p69.
37. Kumar, P., Chand, H., & Gopal-Krishna, (2016), Intranight Optical Variability of Radio-Quiet Weak Emission Line Quasars - IV, MNRAS, 461, p666.
38. Lacy, M., Storrie-Lombardi, L. J., Sajina, A., et al, (2004), Obscured and Unobscured Active Galactic Nuclei in the Spitzer Space Telescope First Look Survey, ApJS, 154, p166.
39. Lilly, S. J., et al, (2009), The zCOSMOS 10k-Bright Spectroscopic Sample, ApJS, 184, p218.
40. Magliocchetti, M., Lutz, D., et al, (2014), The PEP Survey: Infrared Properties of Radio-Selected AGN, MNRAS, 442, p682.
41. Mushotzky, R. F., Edelson, R., Baumgartner, W., & Gandhi, P., (2011), Kepler Observations of Rapid Optical Variability in Active Galactic Nuclei, ApJ, 743, pL12.
42. Petrucci, P. P., Chelli, A., Henri, G., Cruz-Gonzalez, I., Salas, L., & Mujica, R., (1999), Search for Optical Microvariability in a Large Sample of Seyfert I Galaxies, A&A, 342, p687.
43. Pica, A. J., & Smith, A. G., (1983), Optical Variability, Absolute Luminosity, and the Hubble Diagram for QSOs, ApJ, 272, p11.
44. Revalski, M., Nowak, D., Wiita, P. J., Wehrle, A. E., & Unwin, S. C., (2014), Investigating the Variability of Active Galactic Nuclei Using Combined Multi-Quarter Kepler Data, ApJ, 785, p60.
45. Romero, G. E., Cellone, S. A., & Combi, J. A., (1999), Optical Microvariability of Southern AGN, A&AS, 135, p477.
46. Romero, G. E., Cellone, S. A., Combi, J. A., & Andruchow, I., (2002), Optical Microvariability of EGRET blazars, A&A, 390, p431.
47. Sanders, D. B., et al, (2007), S-COSMOS: The Spitzer Legacy Survey of the Hubble Space Telescope ACS 2 deg2 COSMOS Field I: Survey Strategy and First Analysis, ApJS, 172, p86.
48. Schinnerer, E., et al, (2007), The VLA-COSMOS Survey. II. Source Catalog of the Large Project, ApJS, COSMOS special issue, 172, p46.
49. Schneider, D. P., et al, (2010), The Sloan Digital Sky Survey Quasar Catalog. V. Seventh Data Release, AJ, 139, p2360.
50. Shaya, E. J., Olling, R., & Mushotzky, R., (2015), Active Galactic Nuclei Discovered in the Kepler Mission, AJ, 150, p188.
51. Shen, Y., Richards, G. T., Strauss, M. A., et al, (2011), A Catalog of Quasar Properties from Sloan Digital Sky Survey Data Release 7, ApJS, 194, p45.
52. Simm, T., Saglia, R., Salvato, M., et al, (2015), Pan-STARRS1 Variability of XMM-COSMOS AGN. I. Impact on Photometric Redshifts, A&A, 584, pA106.
53. Simm, T., Salvato, M., Saglia, R., et al, (2016), Pan-STARRS1 Variability of XMM-COSMOS AGN. II. Physical Correlations and Power Spectrum Analysis, A&A, 585, pA129.
54. Smolcic, V., Ciliegi, P., Jeli, V., et al, (2014), The VLA-COSMOS Survey - V. 324 MHz Continuum Observations, MNRAS, 443, p2590.
55. Smolcic, V., Novak, M., Bondi, M., et al, (2017), The VLA-COSMOS 3 GHz Large Project: Continuum Data and Source Catalog Release, A&A, 602, pA1.
56. Stalin, C. S., Gopal-Krishna, Sagar, R., & Wiita, P. J., (2004a), Optical Variability Properties of High Luminosity AGN Classes, JA&A, 25, p1.
57. Stalin, C. S., Gopal-Krishna, Sagar, R., & Wiita, P. J., (2004b), Intranight Optical Variability of Radio-Quiet and Radio Lobe-Dominated Quasars, MNRAS, 350, p175.
58. Stalin, C. S., Gupta, A. C., Gopal-Krishna, Wiita, P. J., & Sagar, R., (2005), Intranight Optical Variability of BL Lacs, Radio-Quiet Quasars and Radio-Loud Quasars, MNRAS, 356, p607.
59. Stern, D., et al, (2005), Mid-Infrared Selection of Active Galaxies, ApJ, 631, p163.
60. Ulrich, M.-H., Maraschi, L., & Urry, C. M., (1997), Variability of Active Galactic Nuclei, ARA&A, 35, p445.
61. Uomoto, A. K., Wills, B. J., & Wills, D., (1976), Image-Tube Photography of a Complete Sample of 4C Radio Sources, AJ, 81, p905.
62. Villforth, C., Koekemoer, A. M., & Grogin, N. A., (2010), A New Extensive Catalog of Optically Variable Active Galactic Nuclei in the GOODS Fields and a New Statistical Approach to Variability Selection, ApJ, 723, p737.
63. Webb, W., & Malkan, M., (2000), Rapid Optical Variability in Active Galactic Nuclei and Quasars, ApJ, 540, p652.
64. Wehrle, A. E., Wiita, P. J., Unwin, S. C., et al, (2013), Kepler Photometry of Four Radio-loud Active Galactic Nuclei in 2010-2012, ApJ, 773, p89.