Abstract
The CNIa0.02 project aims to collect a complete, nearby sample of Type Ia supernovae (SNe Ia) light curves, and the SNe are volume-limited with host-galaxy redshifts zhost < 0.02. The main scientific goal is to infer the distributions of key properties (e.g., the luminosity function) of local SNe Ia in a complete and unbiased fashion in order to study SN explosion physics. We spectroscopically classify any SN candidate detected by the All-Sky Automated Survey for Supernovae (ASAS-SN) that reaches a peak brightness <16.5 mag. Since ASAS-SN scans the full sky and does not target specific galaxies, our target selection is effectively unbiased by host-galaxy properties. We perform multiband photometric observations starting from the time of discovery. In the first data release (DR1), we present the optical light curves obtained for 247 SNe from our project (including 148 SNe in the complete sample), and we derive parameters such as the peak fluxes, Δm15, and sBV.
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1. Introduction
The explosion mechanism and progenitors of Type Ia supernovae (SNe Ia) are basic but open questions in astrophysics. There are several proposed channels, but no agreement as to which or even how many of the channels dominate (see, e.g., Maoz et al. 2014). SNe Ia span about an order of magnitude in peak luminosities and in the masses of synthesized 56Ni that power the radiation. It is also debated whether this range in properties represents one continuous population or more than one overlapping but distinct populations. On the one hand, the main properties of SNe Ia appear to be continuous across the whole luminosity range. Phillips (1993) found that the peak luminosity of SNe Ia is tightly correlated with the light-curve shape characterized by the B-band post-peak decline rate Δm15(B), and this width-luminosity relation (WLR) is the foundation for using SNe Ia as cosmological distance indicators. Many properties of their light curves (see, e.g., Phillips 1993, 2012; Burns et al. 2014; Bulla et al. 2020) and spectra (see, e.g., Nugent et al. 1995; Branch et al. 2009) also appear to be continuous. On the other hand, the possible existence of more than one populations of SNe Ia has long been discussed (e.g., Branch & Miller 1993), including recent claims of bimodality in the luminosity function (via the proxy of Δm15(B); see, e.g., Ashall et al. 2016; Hakobyan et al. 2020), existence of two classes of fast-declining SNe Ia (Dhawan et al. 2017), and distinct near-ultraviolet (NUV)-optical (Milne et al. 2013) and early-time optical (Stritzinger et al. 2018) colors.
There have been tremendous efforts to obtain high-quality multiband light curves of large samples of nearby SNe Ia (e.g., Hamuy et al. 1996; Riess et al. 1999; Jha et al. 2006; Hicken et al. 2009; Contreras et al. 2010; Ganeshalingam et al. 2010; Stritzinger et al. 2011; Hicken et al. 2012; Krisciunas et al. 2017; Foley et al. 2018; Stahl et al. 2019). However, collecting a complete and unbiased nearby sample has only been made possible recently, thanks to the advent of wide-field time-domain surveys that do not target specific galaxies, such as the All-Sky Automated Survey for SuperNovae (ASAS-SN; Shappee et al. 2014; Kochanek et al. 2017), the Gaia transient survey (Hodgkin et al. 2021), the Palomar Transient Factory (Law et al. 2009) and its successor the Zwicky Transient Facility (ZTF; Kulkarni 2016; Perley et al. 2020), the Asteroid Terrestrial-impact Last Alert System (ATLAS; Tonry 2011; Tonry et al. 2018a), the Mobile Astronomical System of TElescope Robots (MASTER; Gorbovskoy et al. 2013), OGLE Transients Detection System (OTDS; Wyrzykowski et al. 2014), the Pan-STARRS Survey for Transients (PSST; Huber et al. 2015; Chambers et al. 2016), and the Catalina Real-Time Transient Survey (CRTS; Drake et al. 2009). Compared to other untargeted surveys, ASAS-SN is a dedicated survey with the main goal to search for bright, nearby SNe scanning the entire visible sky at approximately nightly cadence (a cadence of 2–3 nights down to ∼17 mag prior to the expansion in 2017 and a nightly cadence down to ∼18.5 mag after the expansion). The Gaia transient survey has a limiting magnitude down to 20.7 mag, and it is also an all-sky transient survey, but has a very uneven cadence across the sky, which can be up to months. Most other surveys do not have full-sky coverage, while many of them have access to a large fraction of the sky at a typical cadence on the order of days with deeper limiting magnitudes (given in the parentheses following the survey names) compared with ASAS-SN: ZTF (∼20.5 mag), Pan-STARRS (∼21.8 mag), MASTER (∼20 mag), ATLAS (∼20 mag), and CRTS(∼19.5 mag). For most untargeted surveys, there is no attempt to make spectroscopic classifications for all detected candidates selected according to certain criteria to form a complete sample. Furthermore, many time-domain surveys are primarily carried out in single bands, so without additional systematic follow-up efforts, it is not possible to obtain the color information that is critical to derive host-galaxy extinction and constrain SN physics.
We carry out the CNIa0.02 project to collect a complete, nearby, and effectively unbiased sample of Type Ia SNe at host-galaxy redshifts zhost < 0.02 with well-observed multiband light curves. Our follow-up observations started in 2015 January and ended in 2020 January, and the SNe observed between 2015 September 17 and 2019 January 31 followed the selection criteria of the complete sample discussed below. The main goal for constructing a complete sample that is unbiased toward host-galaxy properties is to enable a reliable statistical inference on the distributions of photometric properties of SNe Ia (e.g., luminosity, color, light-curve shape, and derived physical parameters) in the local universe and also to study their dependence on host-galaxy properties.
To our knowledge, collecting and studying a complete sample in astronomy can be traced back to Schmidt (1968), who studied a complete sample of quasars defined with an observed flux density limit to derive their spatial distribution and luminosity function. Since then, complete samples have been widely applied in many areas of astronomy, and for instance, the LOSS survey produced one of the most influential complete samples of SNe from targeted searches (Leaman et al. 2011; Li et al. 2011a, 2011b). Such a complete sample is defined to include all objects that meet a certain set of well-defined selection criteria on observables, making it possible to derive quantitative completeness corrections to infer the statistical distribution of intrinsic properties such as the luminosity function. For the complete sample of CNIa0.02, we adopt the following observational selection criteria: (a) host-galaxy redshifts z < 0.02, (b) peak brightness Vpeak < 16.5 mag, and (c) detection by the ASAS-SN survey, that is, we not only include SNe discovered by ASAS-SN, but also SNe that were discovered first by others and were later detected by ASAS-SN. The ASAS-SN detections are nearly 100% complete for SNe with peak brightness <16.5 mag (see Appendix C), and the ASAS-SN sample also has minimal bias in host-galaxy properties or SN locations inside the hosts (Holoien et al. 2017a, 2017b, 2017c, 2019). All of the SNe in DR1 have been spectroscopically classified by ASAS-SN or other groups. The complete sample includes all spectroscopic subclasses that are known to follow the WLR of the SNe Ia population. These include Ia-91bg and Ia-91T subtypes, but exclude SNe Iax and other peculiar SNe Ia-like objects that deviate from the WLR of SNe Ia (see Appendix D for a detailed discussion). The redshifts derived from SN classification spectra generally have too large uncertainties for our purpose, so we adopt host-galaxy spectroscopic redshifts for our complete sample selection. Where host-galaxy redshifts were unavailable in the NASA/IPAC Extragalactic Database 41 (NED), we have also measured the host-galaxy redshifts directly to determine whether the SNe Ia belong to the complete sample. We do not exclude SN candidates without apparent hosts from our selection (i.e., the "hostless" SN). In our project, ASASSN-18nt is the only hostless SN, which is an intracluster SN Ia located in the galaxy cluster Abell 0194 (z = 0.018), and its peak brightness (16.66 ± 0.02) does not meet our selection criterion for the complete sample. All of the SNe were followed photometrically, mainly in the optical bands (primarily BVri), but with near-infrared (IR) and Swift NUV observations of some objects as well. In this first data release (DR1) of CNIa0.02, we present optical light curves for 247 SNe Ia observed between 2015 and 2020. CNIa0.02 DR1 includes some SNe Ia that are not in the complete sample, and the complete sample has 148 SNe in total. We describe the overall project and the sample in Section 2, the data processing in Section 3, and the resulting light curves in Section 4. Our present results are summarized in Section 5.
2. Program Description and the Sample
We select our targets primarily based on ASAS-SN detections, and the complete sample was collected between 2015 September 17 and 2019 January 31. We have also observed a few SNe Ia before (since 2015 January) and after this period (until 2020 January), and they are included in DR1, but are not part of the complete sample. In the early phase of the complete sample collection, we attempted to observe all SNe Ia with z < 0.034 and a peak magnitude of Vpeak < 17. Between 2016 October and 2019 January, we restricted the complete sample to focus on SNe Ia with z < 0.02 and a peak magnitude of Vpeak < 16.5, as shown in Figure 4 and discussed in Appendix A. The detection efficiency of the ASAS-SN survey has been evolving mainly owing to upgrades in hardware, and since 2015, the detection efficiency has been almost 100% complete to <16.5 mag (see Appendix C for a detailed discussion of the sample completeness).
In Table 1 we give the general information (names given by the survey groups, IAU names, equatorial coordinates, discovery dates, host-galaxy names, and heliocentric host redshifts) for all objects in the CNIa0.02 DR1, which includes objects that have follow-up data (regardless of whether they belong to the complete sample) or have been considered for follow-up observations (regardless of whether such data are obtained). The host-galaxy redshifts are either from NED or are new measurements presented in Table 2. There are four SNe whose host-galaxy spectroscopic redshifts are not yet available, and for them, the redshifts determined from the SN spectra are given in Table 1 and are indicated with asterisks. Note that for all those four SNe, their peak magnitudes are fainter than 16.5, so they do not belong to the complete sample. We also provide additional information of V-band peak magnitudes (see Section 4.2 for how they are measured) and whether they were detected by ASAS-SN in Table 1. The complete sample includes 148 SNe. Figure 1 shows the cumulative distribution of host-galaxy redshifts of all SNe and those in the complete sample as blue and black histograms, respectively, and the latter roughly follows the expectation for a volume-limited complete sample (shown with the red line) when the peculiar velocity is negligible compared to the Hubble expansion velocity (at z ≳ 0.01). Note that our complete sample includes all SNe Ia selected by the observational criteria of Vpeak < 16.5 and z < 0.02. It does not include all SNe Ia at the dim end of the luminosity function (≳−18.2) near z = 0.02, therefore it is not expected to exactly follow the distribution of a volume-limited complete sample covering the full luminosity range.
Figure 1. The cumulative redshift distribution of all SNe Ia (blue histogram) in DR1 and those in the complete sample (black histogram) from the CNIa0.02 project. The redshift limit of z = 0.02 for the complete sample is indicated with the dashed vertical blue line. An illustrative N ∝ z3 is plotted with the red line to indicate a simplified expectation from a volume-limited sample covering the full luminosity range by assuming a linear relation between distance and redshift. The distribution approximately follows the expectation for a volume-limited sample at z ≳ 0.01, for which peculiar velocities are negligible compared to the Hubble expansion velocity. The apparent excess of SNe with 0.005 ≲ z ≲ 0.013 with respect to the volume-limited expectation is probably contributed by the effects of peculiar velocities at low redshift and/or fluctuations due to small number statistics.
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Standard image High-resolution imageTable 1. General Properties of SNe Ia in CNIa0.02 DR1
| Survey Name | IAU Name | R.A. (J2000) | Decl. (J2000) | Discovery Date | Host Galaxy | zhost b | Vpeak c | ASAS-SN? d | Complete? e |
|---|---|---|---|---|---|---|---|---|---|
| ASASSN-15aj | 10:52:53.261 | −32:55:34.86 | 2015-01-08 | NGC 3449 | 0.010921 | 14.77 ± 0.02 | Y | N | |
| ASASSN-15ak | 00:12:01.546 | +26:23:37.284 | 2015-01-09 | UGC 00110 | 0.015034 | 14.70 ± 0.01 | Y | N | |
| ASASSN-15db | 15:46:58.69 | +17:53:02.22 | 2015-02-15 | NGC 5996 | 0.010998 | 14.55 ± 0.03 | Y | N | |
| ASASSN-15eb | 08:06:07.399 | −22:33:48.852 | 2015-02-26 | ESO 561-G 012 | 0.016481 | 15.82 ± 0.05 | Y | N | |
| J073615 a | 2015F | 07:36:15.76 | −69:30:23.0 | 2015-03-09 | NGC2442 | 0.00489 | 13.31 ± 0.02 | Y | N |
| J150530 a | 2015bp | 15:05:30.09 | +01:38:02.2 | 2015-03-16 | NGC 5839 | 0.004069 | 13.90 ± 0.01 | Y | N |
| ASASSN-15ga | 12:59:27.293 | +14:10:15.78 | 2015-03-30 | NGC 4866 | 0.006631 | 15.08 ± 0.03 | Y | N | |
| ASASSN-15go | 06:11:30.401 | −16:29:04.596 | 2015-04-06 | WISEA J061130.50-162908.3 | 0.018923 | 16.04 ± 0.09 | Y | N | |
| ASASSN-15hf | 10:29:30.835 | −35:15:34.812 | 2015-04-17 | ESO 375-G 04 | 0.006178 | 14.27 ± 0.02 | Y | N | |
| ASASSN-15hx | 13:43:16.69 | −31:33:21.5 | 2015-04-26 | uncataloged | 0.00812 | 13.37 ± 0.01 | Y | N | |
| ASASSN-15jo | 14:06:44.73 | −34:27:18.0 | 2015-05-20 | 6dF J1406512-342931 | 0.015584 | 15.30 ± 0.02 | Y | N | |
| ASASSN-15kg | 08:40:12.11 | −04:35:29.0 | 2015-05-27 | 6dF J0840116-043537 | 0.014257 | 15.16 ± 0.05 | Y | N | |
| ASASSN-15kp | 12:58:41.7 | −32:07:28.7 | 2015-06-07 | AM 1255-315 | 0.017402 | 15.48 ± 0.01 | Y | N | |
| ASASSN-15kx | 22:16:11.810 | +37:28:26.112 | 2015-06-10 | MCG +06-49-001 | 0.018019 | 16.14 ± 0.06 | Y | N | |
| ASASSN-15lp | 01:49:10.32 | +05:38:23.316 | 2015-06-20 | MRK 0576 | 0.017686 | 15.01 ± 0.14 | Y | N | |
| J114925 a | 11:49:25.48 | −05:07:13.8 | 2015-06-29 | NGC 3915 | 0.005573 | 13.26 ± 0.01 | Y | N | |
| ASASSN-15mc | 02:48:59.570 | +03:10:10.488 | 2015-07-05 | UGC 02295 | 0.013916 | 15.10 ± 0.02 | Y | N | |
| J020622 a | 2015aw | 02:06:22.53 | −52:01:26.69 | 2015-07-12 | ESO 197-G 024 | 0.01962 | 15.57 ± 0.04 | Y | N |
| ASASSN-15ml | 20:03:01.670 | −21:54:48.24 | 2015-07-12 | 2MASX J20030163-2154516 | 0.018623 | 16.83 ± 0.17 | Y | N | |
| ASASSN-15od | 02:23:13.210 | −04:31:02.064 | 2015-08-10 | MCG -01-07-004 | 0.017989 | 15.45 ± 0.03 | Y | N | |
| ASASSN-15oh | 22:30:41.976 | +39:17:35.232 | 2015-08-14 | MCG +06-49-027 | 0.016835 | 16.15 ± 0.06 | Y | N | |
| ASASSN-15ol | 01:54:06.041 | −56:41:42.504 | 2015-08-15 | NGC 0745 NED01 | 0.019777 | 15.77 ± 0.05 | Y | N | |
| ASASSN-15pl | 02:30:23.24 | −20:41:00.0 | 2015-09-11 | ESO 545-G 025 | 0.016165 | 15.17 ± 0.04 | Y | N | |
| ASASSN-15pz | 03:08:48.45 | −35:13:51.0 | 2015-09-27 | ESO 357-G 005 | 0.014903 | 14.25 ± 0.01 | Y | N | |
| ASASSN-15qc | 00:39:17.94 | +03:57:00.612 | 2015-10-01 | UGC 00402 | 0.017649 | 15.56 ± 0.01 | Y | Y | |
| J015053 a | 2015ao | 1:50:53.56 | −36:00:30.8 | 2015-10-06 | ESO 354-G 003 | 0.019133 | 16.90 ± 0.02 | Y | N |
| J103747 a | 2015dc | 10:37:47.94 | −27:05:07.2 | 2015-10-20 | IC 2597 | 0.007562 | 15.30 ± 0.24 | N | N |
| ASASSN-15rq | 00:08:03.09 | −36:33:51.7 | 2015-10-21 | MRSS 349-038278 | 0.02307 | 15.47 ± 0.01 | Y | N | |
| ASASSN-15rw | 2:15:58.45 | +12:14:13.812 | 2015-10-24 | WISEA J021558.50+121414.4 | 0.01884 | 15.54 ± 0.03 | Y | Y | |
| J213123 a | 21:31:23.75 | +43:36:31.2 | 2015-11-07 | WISEA J213123.03+433618.0 | 0.018413 | 16.80 ± 0.08 | Y | N | |
| ASASSN-15so | 11:14:11.213 | +48:19:07.572 | 2015-11-08 | NGC 3583 | 0.007125 | 13.86 ± 0.02 | Y | Y | |
| J010720 a | 2015ar | 01:07:20.31 | +32:23:59.0 | 2015-11-11 | NGC 0383 | 0.017442 | 15.26 ± 0.01 | Y | Y |
| J215050 a | 21:50:50.94 | −70:20:28.9 | 2015-11-27 | NGC 7123 | 0.012335 | 15.14 ± 0.01 | Y | Y | |
| ASASSN-15ti | 3:05:08.06 | +37:53:59.82 | 2015-12-01 | WISEA J030510.59+375359.9 | 0.01732 | 16.07 ± 0.02 | Y | Y | |
| J112345 a | 2015bd | 11:23:45.88 | −01:06:21.2 | 2015-12-07 | NGC 3662 | 0.018606 | 15.19 ± 0.02 | Y | Y |
| ASASSN-15uh | 09:30:13.78 | +69:07:02.5 | 2015-12-18 | KUG 0925+693 | 0.01489 | 15.30 ± 0.03 | Y | Y | |
| ASASSN-15us | 22:09:09.55 | −47:08:00.8 | 2015-12-29 | NGC 7213 | 0.005839 | ≤ 14.00 | Y | N | |
| ASASSN-15ut | 0:21:21.09 | −48:38:30.336 | 2015-12-30 | NGC 0088 | 0.011471 | 16.37 ± 0.04 | Y | N | |
| ASASSN-16aa | 2016A | 08:09:14.48 | +00:16:51.2 | 2016-01-02 | UGC 04251 | 0.017373 | 16.83 ± 0.04 | Y | N |
| ASASSN-16ad | 2016F | 01:39:32.06 | +33:49:36.0 | 2016-01-09 | KUG 0136+335 | 0.016138 | 15.26 ± 0.03 | Y | Y |
| ATLAS16aab | 2016adp | 03:21:42.43 | +42:05:49.4 | 2016-01-21 | 2MASX J03214217+4205549 | 0.018466 | 17.03 ± 0.08 | Y | N |
| 2016W | 02:30:39.67 | +42:14:09.2 | 2016-01-25 | NGC 0946 | 0.019253 | 16.01 ± 0.03 | Y | Y | |
| ASASSN-16ax | 2016ag | 01:31:23.16 | +60:19:15.2 | 2016-01-26 | WISEA J013123.32+601912.5 | 0.01461 | ≤ 15.96 | Y | Y |
| 2016adi | 13:47:43.24 | −30:55:55.57 | 2016-02-03 | NGC 5292 | 0.014897 | 15.35 ± 0.05 | Y | Y | |
| ASASSN-16bn | 2016adn | 03:10:34.54 | +04:16:10.8 | 2016-02-09 | LEDA 3092121 | 0.023166 | 16.12 ± 0.05 | Y | N |
| ASASSN-16ci | 2016arc | 03:19:21.27 | +41:29:24.8 | 2016-02-26 | NGC 1272 | 0.012725 | ≤ 16.38 | Y | Y |
| ASASSN-16cs | 2016asf | 06:50:36.72 | +31:06:45.3 | 2016-03-06 | KUG 0647+311 | 0.018019 | 15.72 ± 0.02 | Y | Y |
| ASASSN-16cu | 2016aue | 18:35:56.53 | −63:22:25.6 | 2016-03-06 | IC 4723 | 0.011128 | 14.80 ± 0.13 | Y | Y |
| 2016bfu | 05:51:15.52 | −38:19:03.2 | 2016-03-23 | IC 2150 | 0.010404 | 15.60 ± 0.01 | Y | Y | |
| ASASSN-16dn | 2016blc | 10:48:49.34 | −20:15:50.3 | 2016-03-30 | WISEA J104848.74-201547.4 | 0.01285 | 14.74 ± 0.01 | Y | Y |
| iPTF16abc | 2016bln | 13:34:45.49 | +13:51:14.7 | 2016-04-11 | NGC 5221 | 0.023279 | 16.01 ± 0.04 | Y | N |
| 2016brx | 22:50:34.03 | −01:32:32.5 | 2016-04-19 | NGC 7391 | 0.010167 | ≤ 16.80 | Y | Y | |
| 2016bry | 20:43:22.40 | +80:09:14.6 | 2016-04-19 | UGC 11635 | 0.016024 | 15.77 ± 0.02 | Y | Y | |
| ASASSN-16eq | 2016bsa | 22:04:35.56 | +42:19:32.6 | 2016-04-22 | UGC 11898 | 0.01431 | 15.99 ± 0.06 | Y | Y |
| Gaia16alq | 2016dxv | 18:12:29.36 | +31:16:49.32 | 2016-04-26 | uncataloged | 0.02431 | 16.17 ± 0.03 | Y | N |
| ASASSN-16es | 2016cbx | 11:50:54.53 | +02:18:21.5 | 2016-04-27 | WISEA J115054.33+021827.0 | 0.0285 | 16.54 ± 0.03 | Y | N |
| iPTF16auf | 2016ccz | 14:31:09.26 | +27:14:09.8 | 2016-05-13 | MRK 0685 | 0.01489 | 15.43 ± 0.02 | Y | Y |
| ASASSN-16fd | 2016cdb | 22:21:29.39 | −22:15:46.6 | 2016-05-15 | 2dFGRS S006Z125 | 0.023906 | ⋯ | Y | N |
| ASASSN-16fj | 2016cmn | 18:30:02.41 | +39:57:55.8 | 2016-05-20 | IC 1289 | 0.018313 | 16.02 ± 0.05 | Y | Y |
| KAIT-16X | 2016coj | 12:08:06.80 | +65:10:38.2 | 2016-05-28 | NGC 4125 | 0.004483 | 13.01 ± 0.01 | Y | Y |
| ASASSN-16fv | 2016cqz | 18:28:10.44 | −71:41:38.8 | 2016-06-06 | IC 4705 | 0.011972 | 14.91 ± 0.03 | Y | Y |
| ATLAS16bdg | 2016cvn | 12:49:41.36 | −11:05:33.5 | 2016-06-21 | NGC 4708 | 0.013896 | 16.38 ± 0.09 | Y | Y |
| ASASSN-16gp | 2016cyl | 13:16:42.77 | −55:17:59.9 | 2016-06-27 | WKK 2066 | 0.01646 | 16.53 ± 0.16 | Y | N |
| 2016dag | 08:19:07.45 | −78:41:54.00 | 2016-07-09 | ESO 018-G 002 | 0.01928 | ⋯ | N | N | |
| ASASSN-16hh | 2016daj | 02:04:37.50 | +21:35:08.45 | 2016-07-17 | MCG +03-06-031 | 0.03026 | 16.52 ± 0.02 | Y | N |
| ASASSN-16hp | 2016eiy | 13:34:38.64 | −23:40:53.15 | 2016-07-26 | ESO 509-IG 064 | 0.008663 | 14.23 ± 0.02 | Y | Y |
| 2016ekg | 22:00:03.67 | −30:11:02.86 | 2016-07-27 | ESO 466-G 032 | 0.0171 | 15.07 ± 0.01 | Y | Y | |
| ASASSN-16hw | 2016ekt | 21:53:27.88 | −34:24:20.95 | 2016-07-29 | WISEA J215327.93-342421.2 | 0.01431 | 14.71 ± 0.01 | Y | Y |
| 2016eqa | 03:20:31.42 | +41:30:40.90 | 2016-08-05 | WISEA J032030.90+413032.3 | 0.014957 | ⋯ | N | N | |
| ASASSN-16ip | 2016euj | 02:27:21.70 | −23:55:45.30 | 2016-08-09 | ESO 479-G 007 | 0.017008 | 15.36 ± 0.01 | Y | Y |
| ATLAS16cpu | 2016ffh | 15:11:49.48 | +46:15:03.22 | 2016-08-20 | CGCG 249-011 | 0.018204 | ≤ 16.16 | Y | Y |
| ASASSN-16jc | 2016fej | 20:40:39.93 | −54:18:38.77 | 2016-08-22 | NGC 6942 | 0.010914 | 13.91 ± 0.01 | Y | Y |
| ASASSN-16jf | 2016fff | 22:36:59.21 | −25:13:55.08 | 2016-08-23 | UGCA 430 | 0.011441 | 14.93 ± 0.01 | Y | Y |
| 2016fnr | 16:37:38.80 | +72:22:24.60 | 2016-08-29 | UGC 10502 | 0.014367 | 15.03 ± 0.04 | Y | Y | |
| ASASSN-16jq | 2016fob | 08:05:09.20 | −22:35:59.39 | 2016-08-30 | CGMW 2-2125 | 0.0187 | 16.10 ± 0.02 | Y | Y |
| 2016gfk | 01:14:06.47 | −32:39:25.80 | 2016-09-11 | IC 1657 | 0.011952 | 16.78 ± 0.02 | Y | N | |
| 2016gfr | 18:19:35.57 | +23:47:09.20 | 2016-09-12 | WISEA J181935.67+234714.0 | 0.01671 | 15.28 ± 0.03 | Y | Y | |
| OGLE16dha | 2016hsc | 06:32:25.13 | −71:34:05.05 | 2016-09-19 | LEDA 179577 | 0.0145 | 15.06 ± 0.02 | Y | Y |
| ATLAS16cxr | 2016gou | 18:08:06.50 | +25:24:31.3 | 2016-09-22 | WISEA J180806.45+252431.8 | 0.0155 | 15.84 ± 0.05 | Y | Y |
| ASASSN-16kz | 2016gsb | 06:04:28.21 | −20:20:24.60 | 2016-09-29 | ESO 555-G 029 | 0.00965 | 14.42 ± 0.01 | Y | Y |
| ASASSN-16la | 2016gsn | 02:29:17.48 | +18:05:16.33 | 2016-09-29 | WISEA J022917.19+180516.3 | 0.01505 | 15.09 ± 0.01 | Y | Y |
| ASASSN-16lc | 2016gtr | 19:29:00.48 | −51:58:15.57 | 2016-09-30 | WISEA J192901.71-515812.6 | 0.02033 | 15.59 ± 0.01 | Y | N |
| Gaia16bkz | 2016gwl | 09:23:28.02 | −23:10:10.74 | 2016-10-02 | NGC 2865 | 0.008763 | 14.23 ± 0.02 | Y | Y |
| 2016gxp | 00:14:34.58 | +48:15:08.03 | 2016-10-05 | NGC 0051 | 0.017849 | 14.85 ± 0.01 | Y | N | |
| ASASSN-16lx | 2016hht | 10:24:05.32 | +16:44:28.25 | 2016-10-19 | IC 0607 | 0.018596 | 15.59 ± 0.04 | Y | Y |
| J033333 a | 2016iil | 03:33:33.26 | −62:33:14.70 | 2016-10-19 | WISEA J033334.19-623303.4 | 0.0289 | 16.62 ± 0.05 | Y | N |
| ASASSN-16mc | 2016hmo | 19:58:41.31 | −52:21:22.45 | 2016-10-21 | ESO 233-IG 014 | 0.018913 | 16.85 ± 0.03 | Y | N |
| ATLAS16dod | 2016hli | 03:43:38.45 | +46:09:32.77 | 2016-10-25 | MCG +08-07-008 | 0.016752 | 16.78 ± 0.01 | Y | N |
| ATLAS16dpc | 2016hnk | 02:13:16.63 | −07:39:40.80 | 2016-10-27 | KUG 0210-078 | 0.016011 | 17.55 ± 0.03 | N | N |
| ATLAS16dqf | 2016hpw | 21:09:07.88 | −18:06:14.21 | 2016-10-30 | WISEA J210907.40-180607.8 | 0.02102 | 15.96 ± 0.01 | Y | N |
| ATLAS16dtf | 2016hvl | 06:44:02.16 | +12:23:47.84 | 2016-11-04 | UGC 03524 | 0.013092 | 15.45 ± 0.02 | Y | Y |
| ASASSN-16mv | 2016huh | 08:57:05.24 | −20:02:05.81 | 2016-11-04 | ESO 563-G 035 | 0.018556 | 16.82 ± 0.01 | Y | N |
| J110533 a | 11:05:33.80 | +19:41:18.70 | 2016-11-15 | LEDA 1602017 | 0.031599 | ⋯ | N | N | |
| PS16fdp | 2016igr | 01:03:26.69 | −04:52:39.43 | 2016-11-23 | MCG -01-03-082 | 0.017732 | 15.30 ± 0.02 | Y | Y |
| ASASSN-16no | 2016ins | 08:07:27.42 | +25:07:44.94 | 2016-11-26 | IC 0493 | 0.020708 | 16.58 ± 0.02 | Y | N |
| ATLAS16dyo | 2016ipf | 08:07:13.15 | 05:40:59.69 | 2016-11-28 | CGCG 031-049 | 0.021* | 16.70 ± 0.02 | Y | N |
| Gaia16caa | 2016itd | 14:18:47.74 | +24:56:27.02 | 2016-12-02 | UGC 09165 | 0.017542 | 15.42 ± 0.08 | Y | Y |
| ASASSN-16oq | 2016ito | 12:31:09.00 | −35:55:49.76 | 2016-12-08 | 6dF J1231098-355547 | 0.01992 | 15.64 ± 0.02 | Y | Y |
| Gaia16cbd | 2016iuh | 12:19:31.44 | +49:49:04.26 | 2016-12-09 | UGC 07367 | 0.013696 | 15.40 ± 0.04 | Y | Y |
| ATLAS16eay | 2016jae | 09:42:34.51 | +10:59:35.38 | 2016-12-22 | uncataloged | 0.021* | 16.79 ± 0.01 | Y | N |
| ASASSN-16pd | 2016jab | 07:05:26.33 | −76:00:34.48 | 2016-12-23 | uncataloged | 0.0216 | 15.95 ± 0.01 | Y | N |
| PS17hj | 2017jd | 23:34:36.47 | −04:32:04.32 | 2017-01-09 | IC 5334 | 0.007368 | ⋯ | N | N |
| ATLAS17abh | 2017ae | 02:05:50.62 | 18:22:30.23 | 2017-01-10 | uncataloged | 0.0275 | 16.41 ± 0.05 | Y | N |
| ATLAS17air | 2017jl | 00:57:31.90 | +30:11:06.83 | 2017-01-16 | WISEA J005731.53+301109.4 | 0.016331 | 14.94 ± 0.01 | Y | Y |
| iPTF17lf | 2017lf | 03:12:33.60 | +39:19:15.30 | 2017-01-22 | NGC 1233 | 0.01464 | ⋯ | N | N |
| ASASSN-17bu | 2017yv | 10:23:40.49 | −35:49:31.21 | 2017-01-31 | ESO 375-G 018 | 0.015584 | 15.59 ± 0.02 | Y | Y |
| ATLAS17ayw | 2017atv | 03:23:59.47 | +37:45:30.65 | 2017-02-14 | UGC 02710 | 0.018479 | 16.59 ± 0.03 | Y | N |
| ASASSN-17cm | 2017aut | 05:47:42.41 | −79:12:51.44 | 2017-02-14 | WISEA J054743.06-791252.1 | 0.017233 | 17.10 ± 0.05 | Y | N |
| ASASSN-17co | 2017awk | 18:09:20.745 | +18:17:54.15 | 2017-02-16 | UGC 11128 | 0.018056 | 15.74 ± 0.01 | Y | Y |
| ASASSN-17cs | 2017azw | 04:22:50.06 | −82:04:11.02 | 2017-02-21 | ESO 015-G 010 | 0.01616 | 14.98 ± 0.01 | Y | Y |
| ASASSN-17cz | 2017bkc | 17:50:30.11 | −01:48:07.52 | 2017-02-23 | LEDA 166870 | 0.017382 | 16.62 ± 0.02 | Y | N |
| ASASSN-17dj | 2017cav | 18:06:43.92 | 06:50:19.64 | 2017-03-06 | uncataloged | 0.02096 | 16.31 ± 0.01 | Y | N |
| 2017bzc | 23:16:14.69 | −42:34:10.90 | 2017-03-07 | NGC 7552 | 0.005365 | 12.29 ± 0.01 | Y | Y | |
| PS17bwe | 2017cbr | 11:58:46.78 | +15:43:08.87 | 2017-03-08 | CGCG 098-015 | 0.017271 | 15.75 ± 0.01 | Y | Y |
| DLT17u | 2017cbv | 14:32:34.42 | −44:08:02.74 | 2017-03-10 | NGC 5643 | 0.00399 | 11.70 ± 0.01 | Y | Y |
| kait-17I | 2017cfd | 08:40:49.10 | +73:29:15.10 | 2017-03-16 | IC 0511 | 0.012085 | 14.78 ± 0.01 | Y | Y |
| ATLAS17dcl | 2017cjt | 03:42:50.76 | −01:52:28.98 | 2017-03-20 | GALEX 2692072904051396069 | 0.009376 | ⋯ | N | N |
| ATLAS17dfo | 2017ckq | 10:44:25.39 | −32:12:32.83 | 2017-03-23 | ESO 437-G 056 | 0.009893 | 14.33 ± 0.01 | Y | Y |
| ASASSN-17ea | 2017cjr | 12:42:50.77 | −30:24:43.65 | 2017-03-24 | ESO 442-G 015 | 0.01444 | 15.06 ± 0.01 | Y | Y |
| ASASSN-17em | 2017cts | 17:03:11.76 | +61:27:26.06 | 2017-04-02 | CGCG 299-048 NED01 | 0.01976 | 15.72 ± 0.01 | Y | Y |
| J141551 a | 2017kdz | 14:15:51.21 | −48:08:02.60 | 2017-04-09 | NGC 5516 | 0.013753 | 16.49 ± 0.06 | Y | Y |
| ASASSN-17er | 2017cze | 11:09:46.82 | −13:22:50.66 | 2017-04-11 | NGC 3546 | 0.01486 | 15.77 ± 0.02 | Y | Y |
| DLT17ar | 2017cyy | 09:36:36.30 | −63:56:54.68 | 2017-04-12 | ESO 091-G 015 | 0.009777 | 14.74 ± 0.01 | Y | Y |
| ASASSN-17ez | 2017daf | 14:34:52.70 | +40:44:52.87 | 2017-04-15 | UGC 09386 | 0.019001 | 15.79 ± 0.02 | Y | Y |
| Gaia17bat | 2017dei | 20:49:48.85 | −25:42:02.56 | 2017-04-17 | ESO 529-G 005 | 0.019804 | 16.38 ± 0.02 | Y | Y |
| ASASSN-17fk | 2017dhr | 05:46:47.27 | −16:47:00.30 | 2017-04-20 | NGC 2076 | 0.007145 | 16.20 ± 0.03 | Y | Y |
| Gaia17bci | 2017dit | 15:27:58.92 | +42:50:48.70 | 2017-04-24 | WISEA J152759.46+425058.9 | 0.01859 | 15.85 ± 0.02 | Y | Y |
| ASASSN-17fr | 2017dps | 13:36:40.04 | −33:58:01.29 | 2017-05-01 | IC 4296 | 0.012465 | 14.77 ± 0.01 | Y | Y |
| DLT17aw | 2017drh | 17:32:26.05 | +07:03:47.52 | 2017-05-03 | NGC 6384 | 0.005554 | 15.71 ± 0.02 | Y | Y |
| 2017dzs | 23:32:28.90 | +23:56:11.20 | 2017-05-11 | UGC 12655 | 0.017269 | 15.33 ± 0.18 | N | N | |
| ATLAS17fll | 2017eck | 18:00:31.28 | 02:25:54.55 | 2017-05-11 | uncataloged | 0.0233 | 16.20 ± 0.01 | Y | N |
| ATLAS17fgh | 2017ebm | 13:23:19.12 | −19:37:17.47 | 2017-05-13 | ESO 576-G 044 | 0.016732 | 17.42 ± 0.10 | N | N |
| J122100 a | 2017edu | 12:21:00.78 | −53:31:49.76 | 2017-05-16 | WKK 0919 | 0.02* | 16.87 ± 0.18 | Y | N |
| ASASSN-17gr | 2017egb | 16:08:39.41 | +12:00:40.21 | 2017-05-24 | CGCG 079-058 | 0.016151 | 15.68 ± 0.01 | Y | Y |
| DLT17bk | 2017ejb | 12:48:36.01 | −41:19:33.53 | 2017-05-28 | NGC 4696 | 0.009867 | 15.37 ± 0.01 | Y | Y |
| ASASSN-17hb | 2017ejw | 01:12:34.16 | +00:17:29.41 | 2017-05-31 | UGC 00757 | 0.019117 | 15.53 ± 0.01 | Y | Y |
| ATLAS17glh | 2017ekr | 23:02:32.19 | +32:35:13.18 | 2017-06-01 | UGC 12323 | 0.019914 | 15.95 ± 0.02 | Y | Y |
| PS17dfh | 2017emq | 10:00:18.57 | +54:32:23.07 | 2017-06-03 | UGC 05369 | 0.005247 | 14.13 ± 0.01 | N | N |
| ASASSN-17hk | 2017enx | 10:10:52.36 | −66:38:50.63 | 2017-06-06 | ESO 092-G 014 | 0.006398 | 13.82 ± 0.02 | Y | Y |
| ASASSN-17ho | 2017erv | 19:18:47.01 | −84:41:49.77 | 2017-06-13 | AM 1904-844 | 0.017035 | 15.69 ± 0.02 | Y | Y |
| J150915 a | 2017erp | 15:09:14.81 | −11:20:03.20 | 2017-06-13 | NGC 5861 | 0.006174 | 13.49 ± 0.01 | Y | Y |
| 2017ezd | 19:56:38.66 | −38:36:27.80 | 2017-06-17 | ESO 339-G 009 | 0.018076 | 15.73 ± 0.02 | Y | Y | |
| ASASSN-17hz | 2017evn | 11:47:23.27 | +23:21:53.57 | 2017-06-20 | SDSS J114723.29+232157.5 | 0.017159 | 15.34 ± 0.02 | Y | Y |
| ASASSN-17ie | 2017exo | 18:31:41.79 | +16:39:05.40 | 2017-06-24 | IRAS 18294+1636 | 0.016288 | 16.25 ± 0.01 | Y | Y |
| ASASSN-17ip | 2017fbj | 08:58:20.56 | −65:21:49.75 | 2017-06-29 | ESO 090-G 011 | 0.018422 | 15.92 ± 0.03 | Y | Y |
| ATLAS17iky | 2017ffv | 13:57:21.74 | −34:46:24.46 | 2017-07-10 | ESO 384-G 018 | 0.01401 | 15.23 ± 0.02 | Y | Y |
| DLT17bx | 2017fgc | 01:20:14.44 | +03:24:09.96 | 2017-07-11 | NGC 0474 | 0.007722 | 13.57 ± 0.01 | Y | Y |
| ASASSN-17kf | 2017fvl | 02:55:42.59 | +75:09:13.72 | 2017-08-01 | UGC 02358 | 0.014343 | 15.99 ± 0.04 | Y | Y |
| Gaia17bzv | 2017fzy | 05:21:58.87 | +03:29:05.71 | 2017-08-05 | IC 0413 | 0.014453 | 15.89 ± 0.01 | Y | Y |
| Gaia17car | 2017gbb | 05:53:04.81 | −17:52:03.50 | 2017-08-09 | IC 0438 | 0.010422 | ≤ 16.37 | Y | N |
| DLT17cd | 2017fzw | 06:21:34.77 | −27:12:53.51 | 2017-08-09 | NGC 2217 | 0.005400 | 13.78 ± 0.01 | Y | Y |
| ATLAS17jiv | 2017gah | 22:02:42.43 | −32:47:33.50 | 2017-08-10 | NGC 7187 | 0.008906 | 14.56 ± 0.01 | Y | Y |
| 2017ghu | 05:36:31.68 | +16:38:32.60 | 2017-08-26 | UGC 03329 | 0.017522 | 16.99 ± 0.05 | Y | N | |
| PSP17A | 2017gjn | 02:43:48.41 | +32:31:33.70 | 2017-08-29 | NGC 1067 | 0.01512 | 15.05 ± 0.01 | Y | Y |
| 2017glq | 02:08:27.95 | +06:23:16.60 | 2017-09-03 | IC 0208 | 0.011755 | 14.25 ± 0.01 | Y | Y | |
| PSP17B | 2017glx | 19:43:40.29 | +56:06:36.30 | 2017-09-03 | NGC 6824 | 0.011294 | 14.51 ± 0.01 | Y | Y |
| ASASSN-17lz | 2017grw | 15:57:29.70 | +15:52:21.94 | 2017-09-11 | NGC 6018 | 0.017405 | 15.46 ± 0.01 | Y | Y |
| ATLAS17lcr | 2017guu | 04:23:22.34 | 25:24:40.78 | 2017-09-13 | 2MFGC 03562 | 0.021* | 16.60 ± 0.03 | Y | N |
| Gaia17cin | 2017gxq | 13:05:24.01 | +56:19:27.05 | 2017-09-17 | NGC 4964 | 0.008406 | 14.05 ± 0.04 | Y | Y |
| ATLAS17lbl | 2017gup | 03:29:34.25 | +10:58:23.20 | 2017-09-17 | WISEA J032934.19+105825.5 | 0.02316 | 16.86 ± 0.07 | Y | N |
| ASASSN-17mh | 2017guh | 05:03:13.14 | −22:49:59.16 | 2017-09-18 | ESO 486-G 019 | 0.015427 | 15.12 ± 0.02 | Y | Y |
| ASASSN-17mz | 2017haf | 23:56:21.92 | +32:27:24.14 | 2017-09-30 | KUG 2353+321 | 0.0161 | 15.34 ± 0.01 | Y | Y |
| ASASSN-17ng | 2017hgz | 21:48:20.08 | −34:57:10.62 | 2017-10-10 | NGC 7130 | 0.016151 | 15.13 ± 0.01 | Y | Y |
| ATLAS17mgh | 2017hjw | 05:08:43.83 | +70:28:32.52 | 2017-10-14 | UGC 03245 | 0.016161 | 15.90 ± 0.01 | Y | Y |
| ATLAS17mgt | 2017hjy | 02:36:02.56 | 43:28:19.51 | 2017-10-14 | WISEA J023602.13+432817.6 | 0.0177 | 15.40 ± 0.01 | Y | Y |
| PSP17E | 2017hle | 01:07:33.06 | +32:24:30.00 | 2017-10-18 | NGC 0383 | 0.017005 | 16.97 ± 0.02 | Y | N |
| ATLAS17msi | 2017hoq | 05:19:20.29 | −17:36:42.10 | 2017-10-21 | WISEA J051920.10-173647.6 | 0.02341 | 15.93 ± 0.01 | Y | N |
| 2017hou | 04:09:02.16 | −01:09:36.07 | 2017-10-24 | UGC 02969 | 0.016738 | 17.46 ± 0.01 | Y | N | |
| 2017hpa | 04:39:50.75 | +07:03:54.90 | 2017-10-25 | UGC 03122 | 0.015654 | 15.37 ± 0.01 | Y | Y | |
| ASASSN-17pg | 2017igf | 11:42:49.85 | +77:22:12.94 | 2017-11-18 | NGC 3901 | 0.005624 | 14.59 ± 0.01 | Y | Y |
| ASASSN-17pk | 2017iji | 12:12:26.87 | +29:08:57.28 | 2017-11-20 | NGC 4174 | 0.013493 | 14.93 ± 0.02 | Y | Y |
| ASASSN-17qg | 2017isj | 11:10:44.56 | +04:50:51.11 | 2017-12-02 | UGC 06216 | 0.01933 | 15.63 ± 0.01 | Y | Y |
| ATLAS17nmh | 2017isq | 13:13:12.18 | −19:31:15.08 | 2017-12-04 | NGC 5018 | 0.009393 | 13.75 ± 0.03 | Y | Y |
| Gaia17dhq | 2017izu | 13:58:26.26 | −34:30:57.92 | 2017-12-14 | IC 4352 | 0.016915 | 14.84 ± 0.05 | Y | Y |
| ATLAS17nse | 2017iyb | 06:08:56.81 | −27:47:45.10 | 2017-12-16 | ESO 425-G 010 | 0.010108 | 14.77 ± 0.01 | Y | Y |
| ASASSN-17qz | 2017iyw | 08:13:30.63 | 71:25:45.12 | 2017-12-18 | VII Zw 218 | 0.0174 | 15.60 ± 0.01 | Y | Y |
| Gaia18ali | 2017jav | 07:02:55.50 | 62:46:21.00 | 2017-12-19 | CGCG 285-013 | 0.01517 | 15.80 ± 0.01 | Y | Y |
| ASASSN-17ri | 2017jdx | 00:47:56.19 | 22:22:26.26 | 2017-12-20 | IC 1586 | 0.019417 | 15.81 ± 0.01 | Y | Y |
| Gaia17dkm | 2017jfw | 13:27:53.77 | −29:37:06.74 | 2017-12-26 | NGC 5153 | 0.014413 | ⋯ | N | N |
| 2018bi | 02:19:53.38 | +29:02:02.30 | 2018-01-07 | UGC 01792 | 0.016635 | ⋯ | N | N | |
| ASASSN-18an | 2018gl | 09:58:06.25 | +10:21:33.84 | 2018-01-13 | NGC 3070 | 0.017906 | 16.14 ± 0.00 | Y | Y |
| 2018gv | 08:05:34.58 | −11:26:16.87 | 2018-01-15 | NGC 2525 | 0.005274 | 12.89 ± 0.01 | Y | Y | |
| SNhunt343 | 2018kp | 10:46:33.06 | +13:44:31.00 | 2018-01-24 | NGC 3367 | 0.010142 | 16.05 ± 0.01 | Y | Y |
| 2018pv | 11:52:55.75 | +36:59:10.30 | 2018-02-03 | NGC 3941 | 0.003102 | 12.65 ± 0.02 | Y | Y | |
| PS18hq | 2018pc | 09:28:55.17 | 49:14:17.30 | 2018-02-03 | UGC 05049 | 0.009083 | 15.05 ± 0.01 | Y | Y |
| ASASSN-18bt | 2018oh | 09:06:39.54 | 19:20:17.77 | 2018-02-04 | UGC 04780 | 0.010981 | 14.31 ± 0.01 | Y | Y |
| ASASSN-18da | 2018vw | 03:29:16.65 | −23:58:43.11 | 2018-02-17 | MRSS 481-014096 | 0.0220 | 15.42 ± 0.01 | Y | N |
| DLT18h | 2018xx | 12:53:48.25 | −39:41:49.09 | 2018-02-21 | NGC 4767 | 0.00999 | 14.43 ± 0.02 | Y | Y |
| DLT18i | 2018yu | 05:22:32.36 | −11:29:13.87 | 2018-03-01 | NGC 1888 | 0.008112 | 13.95 ± 0.01 | Y | Y |
| ASASSN-18en | 2018zz | 14:03:39.06 | −33:58:42.60 | 2018-03-03 | NGC 5419 | 0.013763 | 14.95 ± 0.01 | Y | Y |
| ASASSN-18gt | 2018apo | 12:45:05.30 | −44:00:23.10 | 2018-04-02 | ESO 268-G 037 | 0.016254 | 15.27 ± 0.03 | Y | Y |
| DLT18q | 2018aoz | 11:51:01.83 | −28:44:38.63 | 2018-04-02 | NGC 3923 | 0.005801 | 12.87 ± 0.01 | Y | Y |
| ASASSN-18hb | 2018aqi | 10:48:25.44 | −25:09:35.82 | 2018-04-06 | NGC 3393 | 0.012509 | 15.53 ± 0.02 | Y | Y |
| 2018ast | 11:41:07.96 | +24:49:10.60 | 2018-04-08 | NGC 3812 | 0.012012 | 16.33 ± 0.06 | Y | Y | |
| ASASSN-18iu | 2018aye | 17:57:40.36 | +50:02:19.72 | 2018-04-21 | SDSS J175740.70+500154.1 | 0.0223 | 15.72 ± 0.01 | Y | N |
| ATLAS18ofk | 2018big | 17:25:39.14 | +59:26:48.29 | 2018-05-10 | UGC 10858 | 0.01815 | 15.79 ± 0.01 | Y | Y |
| ASASSN-18kd | 2018brz | 08:33:22.28 | −76:37:39.86 | 2018-05-15 | WISEA J083322.17-763736.1 | 0.0193 | 16.14 ± 0.07 | Y | Y |
| 2018bta | 16:57:58.75 | −62:43:53.70 | 2018-05-17 | ESO 101-G 020 | 0.019497 | 15.43 ± 0.02 | Y | Y | |
| ATLAS18qpu | 2018cnj | 22:05:37.34 | 44:50:15.74 | 2018-05-28 | UGC 11906 | 0.017529 | 17.16 ± 0.05 | Y | N |
| Gaia18blb | 2018chl | 12:03:32.39 | −43:39:17.32 | 2018-05-30 | ESO 267-G 011 | 0.015347 | 17.06 ± 0.09 | Y | N |
| ATLAS18qtd | 2018cqj | 09:40:21.46 | −06:59:19.76 | 2018-06-13 | IC 0550 | 0.016455 | 16.16 ± 0.05 | Y | Y |
| ZTF18abgmcmv | 2018cqw | 18:17:32.21 | 19:26:40.49 | 2018-06-18 | CGCG 113-034 | 0.009843 | 14.40 ± 0.01 | Y | Y |
| ASASSN-18nt | 2018ctv | 01:25:52.03 | −01:22:01.65 | 2018-06-21 | ABELL 0194 | 0.018 | 16.67 ± 0.02 | Y | N |
| ATLAS18rng | 2018cuh | 14:34:18.28 | −37:28:44.74 | 2018-06-22 | ESO 385-G 045 | 0.01411 | 15.03 ± 0.01 | Y | Y |
| ATLAS18rqk | 2018cuw | 18:46:14.38 | 35:58:07.27 | 2018-06-24 | WISEA J184614.46+355820.2 | 0.02682 | 16.55 ± 0.06 | Y | N |
| ASASSN-18od | 2018dda | 22:08:14.15 | −25:03:41.58 | 2018-07-04 | ESO 532-G 021 | 0.018229 | 15.22 ± 0.02 | Y | Y |
| ZTF18abgmcmv | 2018eay | 18:16:13.08 | 55:35:27.20 | 2018-07-15 | IC 1286 | 0.018523 | 16.67 ± 0.01 | Y | N |
| ATLAS18skj | 2018ebk | 20:28:35.54 | 25:44:08.32 | 2018-07-16 | MCG +04-48-002 | 0.0139 | 16.26 ± 0.01 | Y | Y |
| ATLAS18swa | 2018enc | 15:19:28.63 | −09:52:50.03 | 2018-08-02 | uncataloged | 0.02389 | 15.95 ± 0.02 | Y | N |
| Gaia18bzh | 2018eov | 16:15:17.42 | −61:07:53.54 | 2018-08-02 | 2MFGC 13057 | 0.016371 | 15.42 ± 0.02 | Y | Y |
| Gaia18bzv | 2018eqq | 03:06:55.16 | 41:30:32.90 | 2018-08-03 | UGC 02536 | 0.015984 | 15.30 ± 0.01 | Y | Y |
| ZTF18abmxahs | 2018feb | 17:10:11.16 | +21:38:56.53 | 2018-08-16 | CGCG 139-041 | 0.014757 | 15.21 ± 0.00 | Y | Y |
| ASASSN-18tb | 2018fhw | 04:18:06.174 | −63:36:56.59 | 2018-08-21 | LEDA 330802 | 0.0170 | 16.36 ± 0.01 | Y | Y |
| PS18blk | 2018fop | 01:15:18.11 | −06:51:32.54 | 2018-08-21 | uncataloged | 0.02121 | 15.54 ± 0.02 | Y | N |
| ASASSN-18to | 2018fpm | 22:24:21.83 | −33:41:32.87 | 2018-08-31 | NGC 7267 | 0.011191 | 16.40 ± 0.05 | Y | Y |
| ASASSN-18ti | 2018fnq | 20:12:30.00 | −44:06:35.14 | 2018-08-31 | WISEA J201229.79-440631.4 | 0.01906 | 15.68 ± 0.02 | Y | Y |
| ASASSN-18ud | 2018fuk | 05:45:08.16 | −79:23:47.52 | 2018-09-05 | ESO 016-G 011 | 0.017582 | 15.71 ± 0.01 | Y | Y |
| ASASSN-18vm | 2018ghb | 06:58:27.60 | −28:45:49.18 | 2018-09-14 | ESO 427-G 022 | 0.007595 | 14.44 ± 0.02 | Y | Y |
| ZTF18acarupz | 2018htw | 22:08:49.702 | +38:09:04.93 | 2018-10-09 | uncataloged | 0.0206 | 15.85 ± 0.04 | Y | N |
| Gaia18czg | 2018hib | 02:56:21.27 | −32:11:08.77 | 2018-10-10 | ESO 417-G 006 | 0.016291 | 15.19 ± 0.01 | Y | Y |
| ASASSN-18ya | 2018hkq | 10:05:47.84 | −17:26:03.12 | 2018-10-15 | IC 2541 | 0.016598 | 15.36 ± 0.06 | Y | Y |
| ASASSN-18yf | 2018hme | 09:35:39.43 | −17:23:10.90 | 2018-10-20 | MCG -03-25-010 | 0.014123 | 15.52 ± 0.05 | Y | Y |
| ZTF18acbvgqw | 2018htt | 03:06:02.90 | −15:36:41.69 | 2018-10-31 | NGC 1209 | 0.008673 | 13.96 ± 0.02 | Y | Y |
| ZTF18acbujhw | 2018hrt | 02:38:27.85 | +29:45:32.44 | 2018-10-31 | UGC 02122 | 0.016945 | 17.28 ± 0.02 | Y | N |
| ASASSN-18yq | 2018hsa | 21:15:01.03 | −47:12:37.40 | 2018-11-01 | NGC 7038 | 0.016471 | 15.60 ± 0.01 | Y | Y |
| ATLAS18zek | 2018ilu | 23:33:20.98 | 04:48:34.66 | 2018-11-12 | uncataloged | 0.01807 | 15.35 ± 0.01 | Y | Y |
| 2018imd | 12:48:24.95 | −05:47:39.20 | 2018-11-14 | NGC 4697 | 0.00414 | 13.91 ± 0.05 | Y | Y | |
| 2018isq | 03:16:50.60 | +80:47:04.50 | 2018-11-20 | NGC 1184 | 0.007599 | 15.94 ± 0.01 | Y | Y | |
| ZTF18acqqyah | 2018iuu | 11:27:21.22 | +59:37:48.26 | 2018-11-21 | UGC 06452 | 0.017051 | 15.39 ± 0.01 | Y | Y |
| ZTF18acrdlrp | 2018jaj | 10:29:52.36 | +20:40:09.71 | 2018-11-25 | SDSS J102952.29+204009.3 | 0.019411 | 15.44 ± 0.01 | Y | Y |
| ASASSN-18aai | 2018jeo | 09:04:36.840 | −19:47:08.30 | 2018-11-28 | ESO 564-G 014 | 0.018653 | 15.91 ± 0.01 | Y | Y |
| Gaia18drb | 2018jjd | 04:24:20.050 | −31:59:14.78 | 2018-12-03 | MRSS 420-017372 | 0.0256 | 15.84 ± 0.02 | Y | N |
| ASASSN-18aay | 2018jky | 03:26:01.930 | −17:33:48.02 | 2018-12-05 | NGC 1329 | 0.01458 | 15.33 ± 0.01 | Y | Y |
| PS18bzo | 2018jmo | 06:51:20.470 | 45:38:41.10 | 2018-12-06 | 2MASX J06512361+4538445 | 0.0209 | 16.51 ± 0.02 | Y | N |
| ATLAS18bbdt | 2018jov | 08:00:07.140 | 58:42:34.95 | 2018-12-08 | SBS 0755+588 | 0.019213 | 16.06 ± 0.01 | Y | Y |
| ASASSN-18abr | 2018jwi | 06:18:39.283 | −54:28:14.84 | 2018-12-14 | WISEA J061839.31-542813.9 | 0.015457 | 15.02 ± 0.01 | Y | Y |
| ZTF18aczeesl | 2018kmu | 14:41:32.924 | +48:12:14.42 | 2018-12-20 | SDSS J144132.85+481214.9 | 0.0297 | 16.34 ± 0.02 | Y | N |
| 2019np | 10:29:21.960 | +29:30:38.40 | 2019-01-09 | NGC 3254 | 0.00452 | 13.38 ± 0.01 | Y | Y | |
| ATLAS19bfk | 2019so | 12:42:36.430 | −40:44:47.06 | 2019-01-14 | NGC 4622 | 0.014567 | 16.66 ± 0.01 | Y | N |
| J140216 a | 14:02:16.0 | −53:32:28.8 | 2019-01-21 | ESO 174-G 005 | 0.01257 | 16.23 ± 0.01 | Y | Y | |
| ATLAS19ltg | 2019gbx | 12:50:02.804 | −14:46:00.23 | 2019-05-29 | MCG -02-33-017 | 0.013059 | 14.82 ± 0.01 | Y | N |
| ATLAS19nkr | 2019hxc | 11:35:22.843 | −21:42:54.91 | 2019-06-21 | ESO 571-G 006 | 0.012158 | 16.44 ± 0.03 | Y | N |
| ASASSN-19qw | 2019knt | 10:35:50.419 | −34:16:22.04 | 2019-07-03 | ESO 375-G 070 | 0.012826 | 14.87 ± 0.02 | Y | N |
| ASASSN-19qr | 2019khf | 11:41:27.641 | −38:38:03.62 | 2019-07-03 | TOLOLO 00091 | 0.013756 | 15.15 ± 0.02 | Y | N |
| Gaia19ded | 2019ltt | 07:15:43.300 | −71:55:10.02 | 2019-07-24 | 6dF J0715407-715525 | 0.017779 | 15.66 ± 0.01 | N | N |
| DLT19n | 2019swh | 07:22:09.108 | −29:13:35.44 | 2019-10-06 | ESO 428-G 023 | 0.010124 | 14.86 ± 0.04 | Y | N |
| 2020ue | 12:42:46.780 | 02:39:34.20 | 2020-01-12 | NGC 4636 | 0.003129 | 12.18 ± 0.01 | Y | N |
Notes. J020622: PSN J02062253-5201267, J122100: PSN J122100.9-533150.1, J015053: PSN J01505356-3600308, J103747: MASTER OT J103747.94-270507.2, J010720: PSN J01072038+3223598, J215050: PSN J21505094-7020289, J150530: PSN J15053007+0138024, J110533: PSN J110533.80+194118.7, J150915: CSS170619:150915-112003, J140216: PSN J140216.0-533228.8, J141551: MASTER OT J141551.21-480802.6, J213123: PSN J21312375+4336312, J033333: MASTER OT J033333.26-623314.7, J114925: PSN J11492548-0507138, J073615: PSN J07361576-6930230, J112345: PSN J11234588-0106212.
a These names are used for brevity, and their corresponding full names are listed below. b Host-galaxy heliocentric spectroscopic redshifts taken from the NASA/IPAC Extragalactic Database (NED) or from new spectroscopic measurements in Table 2. If the host-galaxy spectroscopic redshift is not available, then the SN spectroscopic redshift is displayed here instead and is indicated with an asterisk. ASASSN-18nt (2018ctv) was discovered in the galaxy cluster Abell 0194 (Chen et al. 2018), which was found to be not associated with any obvious galaxy in the cluster, but is located in the intracluster light appearing to bridge between the galaxy pair NGC545+547 and NGC541 (Moral-Pombo et al. 2018). Here we adopt the redshift of the galaxy cluster for ASASSN-18nt (Struble & Rood 1999). c Peak magnitudes in V band obtained from a template fitting with max_model in SNooPy. For targets without successful template fitting results, if they are detected in ASAS-SN data and with redshift z < 0.02, the upper limits for the peak magnitudes derived from available data are reported here. Dong et al. (2018) estimated
for 2016brx by matching its data to the light curves of SN 1991bg.
d
Whether the SN was detected by the ASAS-SN survey.
e
Whether the SN belongs to our complete sample.
A machine-readable version of the table is available.
Table 2. Host Spectroscopic Redshifts without Available NED Information
| SN a |
z
| Host Galaxy | zhost | Telescope/Instrument |
|---|---|---|---|---|
| ASASSN-15hx | N/A | uncataloged | 0.00812 | Magellan/IMACS |
| ASASSN-15rq | 0.025 | MRSS 349-038278 | 0.02307 | Magellan/LDSS3 |
| ASASSN-15rw | 0.02 | WISEA J021558.50+121414.4 | 0.01884 | F18 b |
| ASASSN-15ti | 0.016 | WISEA J030510.59+375359.9 | 0.01732 | F18 b |
| ASASSN-15uh | 0.0135 | KUG 0925+693 | 0.01489 | LBT/MODS |
| 2016ag | 0.0187 | WISEA J013123.32+601912.5 | 0.01461 | Shane/KAST |
| 2016asf | 0.021 | KUG 0647+311 | 0.018019 | F18 b |
| 2016blc | 0.012 | WISEA J104848.74-201547.4 | 0.01285 | F18 b |
| 2016dxv | 0.02 | uncataloged | 0.02431 | P200/DBSP |
| 2016cbx | 0.015 | WISEA J115054.33+021827.0 | 0.0285 | Magellan/LDSS3 |
| 2016cyl | 0.016 | WKK 2066 | 0.01646 | Magellan/LDSS3 |
| 2016daj | 0.032 | MCG +03-06-031 | 0.03026 | P200/DBSP |
| 2016ekt | 0.017 | WISEA J215327.93-342421.2 | 0.01431 | Magellan/LDSS3 |
| 2016fob | 0.024 | CGMW 2-2125 | 0.0187 | Magellan/LDSS3 |
| 2016gfr | 0.014 | WISEA J181935.67+234714.0 | 0.01671 | P200/DBSP |
| 2016hsc | 0.007 | LEDA 179577 | 0.0145 | Magellan/IMACS |
| 2016gou | 0.016 | WISEA J180806.45+252431.8 | 0.0155 | P200/DBSP |
| 2016gsn | 0.018 | WISEA J022917.19+180516.3 | 0.01505 | P200/DBSP |
| 2016gtr | 0.014 | WISEA J181935.67+234714.0 | 0.02033 | Magellan/IMACS |
| 2016iil | 0.024 | WISEA J033334.19-623303.4 | 0.0289 | Magellan/IMACS |
| 2016hpw | 0.02 | WISEA J210907.40-180607.8 | 0.02102 | P200/DBSP |
| 2016jab | 0.021 | uncataloged | 0.0216 | Magellan/IMACS |
| 2017ae | 0.022 | uncataloged | 0.0275 | Shane/KAST |
| 2017azw | 0.02 | ESO 015-G 010 | 0.01616 | Magellan/LDSS3 |
| 2017cav | 0.025 | uncataloged | 0.02096 | GTC/OSIRIS |
| 2017eck | 0.025 | uncataloged | 0.0233 | GTC/OSIRIS |
| 2017gup | 0.016 | WISEA J032934.19+105825.5 | 0.02316 | P200/DBSP |
| 2017hjy | 0.007 | WISEA J023602.13+432817.6 | 0.0177 | Hiltner/OSMOS |
| 2017hoq | 0.02 | WISEA J051920.10-173647.6 | 0.02341 | Hiltner/OSMOS |
| 2017iyw | 0.0215 | VII Zw 218 | 0.0174 | Hiltner/OSMOS |
| 2018vw | 0.02 | MRSS 481-014096 | 0.0220 | VLT/FORS2 |
| 2018aye | 0.017 | SDSS J175740.70+500154.1 | 0.0223 | P200/DBSP |
| 2018brz | 0.019 | WISEA J083322.17-763736.1 | 0.0193 | Magellan/LDSS3 |
| 2018cuh | 0.012 | ESO 385-G 045 | 0.01411 | Magellan/LDSS3 |
| 2018cuw | 0.024 | WISEA J184614.46+355820.2 | 0.02682 | Shane/KAST |
| 2018enc | 0.017 | uncataloged | 0.02389 | Magellan/LDSS3 |
| 2018fop | 0.02 | uncataloged | 0.02121 | Magellan/LDSS3 |
| 2018fhw | N/A | LEDA 330802 | 0.0170 | ATEL 11980 c |
| 2018fnq | 0.019 | WISEA J201229.79-440631.4 | 0.01906 | Magellan/LDSS3 |
| 2018htw | 0.02 | uncataloged | 0.0206 | Shane/KAST |
| 2018ilu | 0.007 | uncataloged | 0.01807 | GTC/OSIRIS |
| 2018jjd | 0.023 | MRSS 420-017372 | 0.0256 | du Pont/WFCCD |
| 2018jmo | 0.02 | 2MASX J06512361+4538445 | 0.0209 | Shane/KAST |
| 2018kmu | 0.02 | SDSS J144132.85+481214.9 | 0.0297 | Shane/KAST |
Notes.
a The SN name adopts the IAU name when available or otherwise the survey name. All the IAU and survey names are available in Table 1. b Host redshifts are obtained from the Foundation Supernova Survey (Foley et al. 2018). c Host redshift of 2018fhw was first reported in Eweis et al. (2018).Download table as: ASCIITypeset image
CNIa0.02 DR1 includes V-band and g-band photometry from the 14 cm telescopes used to conduct the ASAS-SN survey. Immediately after the discovery of an SN candidate that met our magnitude criteria, we started multiband photometric observations, regardless of whether a spectroscopic classification was available then. For most objects, this data release contains follow-up photometry ending around 40–60 days after the optical peak. For objects with bright galaxy backgrounds that require image subtractions, we took template images at least 300 days after B-band peak, when the SN is typically more than ≳7 mag below the peak. We have performed photometric follow-up observations using a number of telescopes ranging from ∼0.3 m to ∼2 m. In this data release, most data are in BVri bands observed by 1 m telescopes of the Las Cumbres Observatory Global Telescope network (LCOGT; Brown et al. 2013) distributed over four sites covering both hemispheres, two 0.6 m telescopes in Sierra Remote Observatories (CA, USA) and Mayhill (NM, USA) of the Post Observatory (PO), and the 1.3 m telescope of Small & Moderate Aperture Research Telescope System (SMARTS; Subasavage et al. 2010). For SNe found between 2016 October and 2018 March, we carried out a follow-up program using the Ultra-Violet/Optical Telescope (UVOT; Roming et al. 2005) on the Neil Gehrels Swift Observatory (Swift; Gehrels et al. 2004), and the UVOT bv-band data from that program are included in DR1. We also include some photometric data obtained from the 2 m Liverpool Telescope (LT), 0.5 m DEdicated MONitor of EXotransits and Transients (DEMONEXT; Villanueva et al. 2018), the 1 m telescope at WeiHai observatory of Shandong University (WHO; Hu et al. 2014), a 0.41 m telescope at A77 observatory, the Ohio State Multi-Object Spectrograph (OSMOS) on the 2.4 m Hiltner Telescope at the MDM observatory, the Wide Field reimaging CCD (WFCCD) camera and direct-imaging CCD camera SITe2K on the 2.5 m du Pont telescope, and Alhambra Faint Object Spectrograph and Camera (ALFOSC) on the 2.56 m Nordic Optical Telescope (NOT). The instrument specifications for the above facilities are described in Appendix B. We plan to make other follow-up data collected by our project available in the future.
3. Data Processing
This data release contains the results of processing over 20,000 images from ground-based observations and also Swift-UVOT images. For ground-based data, we developed the photometric pipeline PmPyeasy to automatically process the images and obtain the photometry. The pipeline uses several external software packages that are all wrapped in a Python interface. The pipeline runs automatically by default, but allows manual operations at any point when necessary. The pipeline uses pyds9 42 to facilitate human inspections through XPA messaging to SAOImageDS9. 43 It takes images that have already been preprocessed, including bias removal and flat-fielding. Below we outline our procedures, and at the end of the section, we summarize our reduction of the UVOT data.
3.1. Image Registration and Source Detection
The pipeline distributes all the images to object-specific folders and adds information such as the filter, exposure time, and epoch to a database. Next, it removes cosmic rays using an implementation of the L.A.Cosmic algorithm (van Dokkum 2001), measures the FWHM of the stellar profiles, and estimates the background value for each image. It then employs PyRAF daofind to generate a source catalog for each image.
3.2. PSF Photometry and Image Subtraction
We perform point-spread function (PSF) photometry for SNe that have negligible host-galaxy contaminations using DoPHOT (Schechter et al. 1993; Alonso-García et al. 2012). For each image, DoPHOT generates a PSF model automatically and yields magnitudes for point sources.
A large number of targets (102 out of 247 SNe) have significant host-galaxy background fluxes and require image subtraction. To perform image subtraction, the pipeline first matches point sources detected on the science image with those on the template image, and then the science image is astrometrically aligned to the same reference frame of the template image using the matched sources and resampled. The image subtraction is done with the High Order Transform of PSF ANd Template Subtraction package (HOTPANTS; Becker 2015). The FWHMs of the template and resampled science image are used to determine the convolution direction: images with better seeings are convolved with the kernel for subtraction. We configured HOTPANTS to normalize the fluxes measured on all subtracted images to the template's flux scale. To perform photometry for targets after image subtraction, the pipeline first identifies isolated stars with high signal-to-noise ratios on the template image, and these stars are used to build a PSF model for each convolved image. Then PSF photometry is performed at the SN position on the subtracted image and for all the sources on the template image using the PyRAF daophot task.
In some cases, host-galaxy flux subtraction is required, but image subtraction is not feasible when too few reference stars are available in the observed field or when template images are not available. If an SN is under such a circumstance and its host galaxy has a smooth profile that can be characterized by an isophote model (e.g., an elliptical galaxy), we devise a method to subtract the host-galaxy flux by incorporating an ellipse isophote modeling of the host galaxy. We adopt the following steps: (1) perform the usual PSF photometry with PyRAF/daophot for point sources (including the SN) within the region to be fitted by an isophote model; (2) subtract the point sources from the image, and then use the isophote/ellipse task from PyRAF/stsdas package to model the host-galaxy flux on the point-source-subtracted image; (3) subtract the best-fit isophote model from the original image and then perform PSF photometry for the stellar objects on the galaxy-flux-subtracted image; (4) steps (2) and (3) are then performed iteratively for three more times. In each iteration, the isophote model for the galaxy and the PSF photometry for the stellar objects are refined. This method has been used for the following targets with corresponding telescope/instruments given in the parentheses: 2017jfw (SMARTS), 2018ast (LCOGT 2m, PO, LT, MDM), ASASSN-18an (SMARTS), ASASSN-18en (SMARTS), 2016fnr (NOT), 2016gfr (NOT), 2016iuh (MDM), ASASSN-16la (MDM), and ASASSN-17fr (du Pont/SITe2K).
3.3. Photometric Calibration
For photometric calibration, we transform our photometry to the standard Johnson magnitudes (BV) in Vega system and SDSS magnitudes (ri) in AB magnitude system, respectively, using the reference stars with available calibrated magnitudes in the field. Since our targets cover the full sky, the preferred sources for reference stars should be an all-sky catalog with homogeneous photometric calibrations. We use the photometric system defined by the Pan-STARRS1 (PS1) survey (Chambers et al. 2016), which has a well-characterized photometric system, with transformations to other standard photometric systems available in Tonry et al. (2012). The PS1 3π Steradian Survey (Chambers et al. 2016) has multiband (grizyP1) coverage of the sky with declinations >−30°, and we use photometry given in the Pan-STARRS1 DR1 MeanObject database (Flewelling et al. 2020). For the remaining quarter of the sky, we use the ATLAS All-Sky Stellar Reference Catalog (Refcat2), which was assembled from a variety of sources and brought onto the the same photometric system as Pan-STARRS1 (Tonry et al. 2018b). Before being used for photometric calibrations of our targets, the PS1 (or Refcat2) magnitudes of the reference stars in the fields are first converted into Johnson BV and SDSS ri bands adopting the following transformations (Tonry et al. 2012):
In practice, we use reference stars brighter than 19 mag in the field. For a target using PSF photometry, our measured magnitudes of the references are matched to standard magnitudes to derive a zeropoint offset for each image. For a target using image subtractions, the flux scale of the template is calibrated using the references, and then all measured magnitudes are scaled to the same photometric system as the template. The photometric uncertainties are estimated by quadratically combining the photometric errors reported by DoPHOT or PyRAF daophot with those of the zeropoint calibrations into the standard systems. The typical uncertainty of our calibrated photometry is ∼0.05 mag.
3.4. Swift UVOT Photometry
In this section, we briefly describe how we perform Swift UVOT bv photometry, and detailed discussions and results of our full Swift SNe Ia campaign will be given in a future paper. Processed Swift UVOT images are downloaded from the Swift Archive. 44 We follow the same basic photometric procedures as described in Brown et al. (2014). We use the calibration database (CALDB) version released on 2020 December 15, which includes the revised photometric zeropoints (Breeveld et al. 2011) and latest time-dependent detector sensitivity. We follow the Swift UVOT standard photometric calibrations (Poole et al. 2008; Breeveld et al. 2010) to extract the source counts on the science images and the host-galaxy counts on the template images with an aperture with radius of 5''. We subtract the host-galaxy contributions and then convert the source count rates into magnitudes in the UVOT-Vega system.
4. Results
4.1. Light-curve Data
In this section, we present the optical light curves of 247 SNe Ia. Most of them have ASAS-SN Vg-band light curves using image subtractions (see Jayasinghe et al. 2018 for descriptions of the ASAS-SN image-subtraction photometry). For 219 SNe, we conducted BVri follow-up observations with the LCOGT 1 m and PO telescopes, and the light curves for all of them are included in DR1. BV light curves for 24 SNe obtained with SMARTS 1.3 m telescope are included in this data release. We also include BVri light curves for several targets obtained from the LCOGT 2 m telescope, LT, DEMONEXT, and A77 as well as relatively late-phase data for a small number of targets from Hiltner, du Pont, and NOT. The light curves are given in Table 3; they are the main result of CNIa0.02 DR1. In Figure 2 we show the multiband light curves up to 80 days past B-band peak (or the time of discovery if peak time is not available).
Figure 2.
Multiband light curves of SNe Ia in DR1. Here we show the light curves for 19 SNe Ia in DR1 with the most recent discovery time. The black lines correspond to the fitting results using the max_model fitting of SNooPy, and the corresponding best-fit parameters are given in Table 4 (see Section 4.2). All phases in days are with respect to the time of B-band peak obtained from the max_model fitting. The complete figure set contains all all SNe Ia with multiband light curves in reverse chronological order according to the time of discovery. (The complete figure set (11 images) is available.)
Download figure:
Standard image High-resolution imageTable 3. Optical Photometry Results
| SN | JD | Mag | Mag_err | Filter | Sub a | Isophote b | Source |
|---|---|---|---|---|---|---|---|
| 2018jky | 2,458,456.7064 | 18.14 | 0.21 | g | Y | N | ASAS-SN |
| 2018jky | 2,458,457.6502 | 17.78 | 0.11 | g | Y | N | ASAS-SN |
| 2018jky | 2,458,458.7521 | 17.21 | 0.07 | g | Y | N | ASAS-SN |
| 2018jky | 2,458,459.7366 | 16.72 | 0.06 | g | Y | N | ASAS-SN |
| 2018jky | 2,458,461.6346 | 16.26 | 0.05 | g | Y | N | ASAS-SN |
| 2018jky | 2,458,462.7428 | 16.03 | 0.04 | g | Y | N | ASAS-SN |
| 2018jky | 2,458,463.4105 | 15.99 | 0.04 | g | Y | N | ASAS-SN |
| 2018jky | 2,458,459.7223 | 16.90 | 0.04 | B | N | N | LCOGT1m |
| 2018jky | 2,458,462.3664 | 16.01 | 0.04 | B | N | N | LCOGT1m |
| 2018jky | 2,458,464.3421 | 15.68 | 0.06 | B | N | N | LCOGT1m |
| 2018jky | 2,458,464.7235 | 15.65 | 0.05 | B | N | N | LCOGT1m |
| 2018jky | 2,458,459.7253 | 16.68 | 0.03 | V | N | N | LCOGT1m |
| 2018jky | 2,458,462.3691 | 15.99 | 0.03 | V | N | N | LCOGT1m |
| 2018jky | 2,458,464.3448 | 15.67 | 0.02 | V | N | N | LCOGT1m |
| 2018jky | 2,458,464.7262 | 15.62 | 0.04 | V | N | N | LCOGT1m |
| 2018jky | 2,458,459.7239 | 16.66 | 0.03 | r | N | N | LCOGT1m |
| 2018jky | 2,458,462.3678 | 15.95 | 0.03 | r | N | N | LCOGT1m |
| 2018jky | 2,458,464.3435 | 15.64 | 0.04 | r | N | N | LCOGT1m |
| 2018jky | 2,458,464.7249 | 15.76 | 0.06 | r | N | N | LCOGT1m |
| 2018jky | 2,458,459.7209 | 16.91 | 0.06 | i | N | N | LCOGT1m |
| 2018jky | 2,458,462.3651 | 16.15 | 0.05 | i | N | N | LCOGT1m |
| 2018jky | 2,458,464.3407 | 15.84 | 0.08 | i | N | N | LCOGT1m |
| 2018jky | 2,458,464.7222 | 15.88 | 0.12 | i | N | N | LCOGT1m |
| 2018jky | 2,458,461.6689 | 16.26 | 0.12 | B | N | N | PO |
| 2018jky | 2,458,463.6687 | 15.76 | 0.12 | B | N | N | PO |
| 2018jky | 2,458,475.6687 | 15.90 | 0.13 | B | N | N | PO |
| 2018jky | 2,458,461.6780 | 16.14 | 0.03 | V | N | N | PO |
| 2018jky | 2,458,463.6779 | 15.77 | 0.04 | V | N | N | PO |
| 2018jky | 2,458,475.6778 | 15.49 | 0.03 | V | N | N | PO |
| 2018jky | 2,458,461.6873 | 16.11 | 0.04 | r | N | N | PO |
| 2018jky | 2,458,463.6871 | 15.72 | 0.05 | r | N | N | PO |
| 2018jky | 2,458,475.6872 | 15.54 | 0.05 | r | N | N | PO |
| 2018jky | 2,458,461.6965 | 16.23 | 0.09 | i | N | N | PO |
| 2018jky | 2,458,463.6963 | 15.86 | 0.06 | i | N | N | PO |
| 2018jky | 2,458,475.6965 | 16.10 | 0.10 | i | N | N | PO |
| 2018jky | 2,458,460.6398 | 16.57 | 0.08 | B | N | N | SMARTS |
| 2018jky | 2,458,462.6273 | 16.02 | 0.10 | B | N | N | SMARTS |
| 2018jky | 2,458,464.6166 | 15.68 | 0.08 | B | N | N | SMARTS |
| 2018jky | 2,458,460.6414 | 16.45 | 0.14 | V | N | N | SMARTS |
| 2018jky | 2,458,462.6289 | 15.92 | 0.14 | V | N | N | SMARTS |
| 2018jky | 2,458,464.6181 | 15.81 | 0.20 | V | N | N | SMARTS |
| 2018jky | 2,458,699.8305 | 22.14 | 0.19 | R | N | N | WFCCD |
| 2018jky | 2,458,699.8350 | 22.42 | 0.19 | R | N | N | WFCCD |
| 2018jky | 2,458,699.8395 | 22.17 | 0.18 | R | N | N | WFCCD |
| 2018jky | 2,458,699.8259 | 21.44 | 0.11 | V | N | N | WFCCD |
Notes.
a Whether image subtraction is used for photometry. b Whether the isophote model is used to subtract the host-galaxy flux. See Section 3.2 for a detailed description of how the isophote model works for the photometry.Only a portion of this table is shown here to demonstrate its form and content. A machine-readable version of the full table is available.
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4.2. Light-curve Parameters
As discussed in Section 2, the V-band peak magnitude Vpeak < 16.5 is one of the criteria for the complete sample of CNIa0.02. To obtain the V-band peak magnitudes of SNe Ia presented in Table 1, we used the SNooPy 45 (Burns et al. 2011) software to fit (using the "max_model") the observed light curves with SNe Ia template light curves. The light curves are shifted in both phase and brightness to find the best match with a set of template light curves characterized by the color-stretch parameter s BV , which is found to be tightly correlated with the peak luminosity across the full range of SN Ia decline rate (Burns et al. 2014). s BV , B-band peak time tpeak(B), and the peak magnitudes in all bands involved are free parameters. Swift UVOT bv data are not included in our fitting, except for two SNe (2017emq and 2017fbj) whose UVOT light curves have the essential coverage missed by other sites. Since the follow-up V-band data are generally more precise and have better coverage than ASAS-SN, we only include ASAS-SN V-band data in cases where follow-up V-band data are unavailable. During the fitting process, > 5σ outliers from the model were removed iteratively. The best-fit parameters (tpeak(B), s BV , Bpeak, gpeak, Vpeak, rpeak, and ipeak) for 232 SNe Ia in CNIa0.02 are given in the max_model section of Table 4, and the corresponding best-fit models are displayed in Figure 2.
Table 4. Light-curve Parameters from SNooPy Template Fitting
| max_model | EBV_model2 | |||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| SN a | tpeak(B) | s BV | Bpeak | gpeak | Vpeak | rpeak | ipeak | tpeak(B) | s BV | E 
| μ | Category c |
| −2,457,000 | (mag) | (mag) | (mag) | (mag) | (mag) | −2,457,000 | (mag) | (mag) | ||||
| ASASSN-15aj | 36.22 ± 0.25 | 0.75 ± 0.04 | 15.01 ± 0.04 | ⋯ | 14.77 ± 0.02 | 14.77 ± 0.03 | 15.15 ± 0.03 | 36.29 ± 0.22 | 0.74 ± 0.04 | 0.13 ± 0.04 | 33.22 ± 0.05 | C2 |
| ASASSN-15ak | 38.15 ± 0.31 | 0.95 ± 0.06 | 14.80 ± 0.08 | ⋯ | 14.70 ± 0.01 | 14.76 ± 0.05 | 15.29 ± 0.09 | 38.02 ± 0.14 | 0.95 ± 0.03 | 0.09 ± 0.01 | 33.64 ± 0.04 | C2 |
| ASASSN-15db | 76.37 ± 0.30 | 0.86 ± 0.05 | ⋯ | ⋯ | 14.55 ± 0.03 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C1 |
| ASASSN-15eb | 82.57 ± 0.74 | 1.02 ± 0.09 | 15.89 ± 0.06 | ⋯ | 15.82 ± 0.05 | 15.79 ± 0.04 | 16.35 ± 0.08 | 82.38 ± 0.75 | 1.02 ± 0.07 | −0.04 ± 0.05 | 34.65 ± 0.10 | C2 |
| 2015F | 107.60 ± 0.21 | 0.86 ± 0.02 | ⋯ | ⋯ | 13.31 ± 0.02 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C1 |
| 2015bp | 113.10 ± 0.13 | 0.71 ± 0.02 | ⋯ | ⋯ | 13.90 ± 0.01 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C0 |
| ASASSN-15ga | 116.66 ± 0.15 | 0.45 ± 0.02 | 15.77 ± 0.05 | ⋯ | 15.08 ± 0.03 | 15.10 ± 0.02 | 15.28 ± 0.03 | 116.59 ± 0.18 | 0.46 ± 0.02 | 0.14 ± 0.06 | 32.95 ± 0.05 | C0 |
| ASASSN-15go | 125.14 ± 0.53 | 0.60 ± 0.21 | 16.42 ± 0.13 | ⋯ | 16.04 ± 0.09 | 15.91 ± 0.44 | 16.38 ± 0.21 | 125.84 ± 0.69 | 0.71 ± 0.15 | 0.12 ± 0.12 | 34.27 ± 0.24 | C2 |
| ASASSN-15hf | 137.71 ± 0.16 | 1.00 ± 0.02 | ⋯ | ⋯ | 14.27 ± 0.02 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C1 |
| ASASSN-15hx | 152.12 ± 0.04 | 1.06 ± 0.01 | 13.33 ± 0.01 | ⋯ | 13.37 ± 0.01 | 13.42 ± 0.01 | 14.04 ± 0.01 | 152.04 ± 0.05 | 1.01 ± 0.01 | −0.03 ± 0.01 | 32.54 ± 0.02 | C0 |
| ASASSN-15jo | 169.29 ± 0.06 | 0.58 ± 0.01 | 15.69 ± 0.01 | ⋯ | 15.30 ± 0.02 | 15.41 ± 0.01 | 15.79 ± 0.01 | 169.32 ± 0.11 | 0.57 ± 0.01 | 0.01 ± 0.02 | 33.72 ± 0.02 | C0 |
| ASASSN-15kg | 182.30 ± 0.77 | 0.61 ± 0.11 | 15.48 ± 0.17 | ⋯ | 15.16 ± 0.05 | ⋯ | ⋯ | 182.31 ± 0.76 | 0.61 ± 0.11 | 0.16 ± 0.21 | 33.37 ± 0.22 | C0 |
| ASASSN-15kp | 189.69 ± 0.18 | 0.98 ± 0.01 | 15.53 ± 0.01 | ⋯ | 15.48 ± 0.01 | ⋯ | ⋯ | 189.69 ± 0.18 | 0.97 ± 0.01 | 0.02 ± 0.01 | 34.45 ± 0.04 | C0 |
| ASASSN-15kx | 195.91 ± 1.52 | 1.24 ± 0.24 | ⋯ | ⋯ | 16.14 ± 0.06 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C1 |
| ASASSN-15lp | 188.29 ± 2.89 | 1.12 ± 0.15 | 14.90 ± 0.22 | ⋯ | 15.01 ± 0.14 | ⋯ | ⋯ | 188.35 ± 2.38 | 1.12 ± 0.14 | −0.18 ± 0.19 | 34.50 ± 0.33 | C0 |
| J114925 b | 216.48 ± 0.08 | 0.84 ± 0.01 | 13.29 ± 0.02 | ⋯ | 13.26 ± 0.01 | ⋯ | ⋯ | 216.48 ± 0.08 | 0.84 ± 0.01 | 0.01 ± 0.02 | 32.26 ± 0.04 | C0 |
| ASASSN-15mc | 217.08 ± 0.74 | 1.51 ± 0.10 | 15.55 ± 0.02 | ⋯ | 15.10 ± 0.02 | ⋯ | ⋯ | 217.05 ± 0.74 | 1.49 ± 0.10 | 0.07 ± 0.18 | 33.81 ± 0.19 | C2 |
| 2015aw | 225.40 ± 0.44 | 0.91 ± 0.06 | ⋯ | ⋯ | 15.57 ± 0.04 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C1 |
| ASASSN-15ml | 210.62 ± 2.84 | 0.78 ± 0.06 | 17.51 ± 0.34 | ⋯ | 16.83 ± 0.17 | ⋯ | ⋯ | 210.72 ± 2.72 | 0.77 ± 0.06 | 0.55 ± 0.16 | 34.22 ± 0.22 | C2 |
| ASASSN-15od | 257.22 ± 0.23 | 0.86 ± 0.04 | 15.51 ± 0.05 | ⋯ | 15.45 ± 0.03 | ⋯ | ⋯ | 257.23 ± 0.23 | 0.86 ± 0.04 | 0.06 ± 0.06 | 34.36 ± 0.07 | C0 |
| ASASSN-15oh | 256.14 ± 0.71 | 0.89 ± 0.18 | ⋯ | ⋯ | 16.15 ± 0.06 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C1 |
| ASASSN-15ol | 259.94 ± 0.45 | 1.04 ± 0.09 | 15.93 ± 0.06 | ⋯ | 15.77 ± 0.05 | ⋯ | ⋯ | 259.93 ± 0.45 | 1.04 ± 0.09 | 0.19 ± 0.09 | 34.62 ± 0.24 | C2 |
| ASASSN-15pl | 288.16 ± 0.68 | 1.10 ± 0.07 | 15.26 ± 0.11 | ⋯ | 15.17 ± 0.04 | 15.34 ± 0.05 | 15.93 ± 0.08 | 288.11 ± 0.72 | 1.12 ± 0.05 | −0.01 ± 0.05 | 34.48 ± 0.08 | C0 |
| ASASSN-15pz | 307.87 ± 0.09 | 1.37 ± 0.01 | 14.26 ± 0.01 | ⋯ | 14.25 ± 0.01 | 14.45 ± 0.01 | 14.90 ± 0.01 | 308.07 ± 0.14 | 1.34 ± 0.01 | −0.13 ± 0.01 | 33.64 ± 0.02 | C4 |
| ASASSN-15qc | 300.88 ± 0.17 | 0.99 ± 0.01 | 15.93 ± 0.02 | ⋯ | 15.56 ± 0.01 | 15.57 ± 0.01 | 16.18 ± 0.02 | 299.37 ± 0.23 | 1.19 ± 0.02 | 0.21 ± 0.02 | 34.47 ± 0.04 | C0 |
| 2015ao | 308.30 ± 0.15 | 0.40 ± 0.02 | 17.52 ± 0.03 | ⋯ | 16.90 ± 0.02 | 16.91 ± 0.03 | 17.12 ± 0.04 | 308.27 ± 0.15 | 0.38 ± 0.02 | 0.03 ± 0.03 | 34.69 ± 0.06 | C0 |
| 2015dc | 293.54 ± 2.45 | 0.98 ± 0.27 | 15.33 ± 0.22 | ⋯ | 15.30 ± 0.24 | 15.63 ± 0.33 | 16.07 ± 0.35 | 296.23 ± 2.08 | 0.63 ± 0.20 | −0.17 ± 0.08 | 33.97 ± 0.55 | C0 |
| ASASSN-15rq | 325.25 ± 0.10 | 1.19 ± 0.02 | 15.49 ± 0.01 | ⋯ | 15.47 ± 0.01 | 15.60 ± 0.01 | 16.03 ± 0.02 | 325.24 ± 0.14 | 1.14 ± 0.03 | 0.02 ± 0.02 | 34.72 ± 0.04 | C0 |
| ASASSN-15rw | 329.63 ± 0.25 | 1.13 ± 0.05 | 15.62 ± 0.03 | ⋯ | 15.54 ± 0.03 | 15.60 ± 0.03 | 16.07 ± 0.03 | 329.54 ± 0.25 | 1.13 ± 0.04 | 0.00 ± 0.02 | 34.46 ± 0.05 | C0 |
| J213123 b | 336.14 ± 1.30 | 1.18 ± 0.05 | 17.35 ± 0.15 | ⋯ | 16.80 ± 0.08 | 16.77 ± 0.05 | 16.97 ± 0.04 | 334.37 ± 3.04 | 1.13 ± 0.09 | 0.09 ± 0.14 | 34.85 ± 0.16 | C0 |
| ASASSN-15so | 347.16 ± 0.38 | 0.86 ± 0.03 | 13.96 ± 0.09 | ⋯ | 13.86 ± 0.02 | 13.97 ± 0.06 | 14.56 ± 0.07 | 347.36 ± 0.46 | 0.84 ± 0.03 | 0.03 ± 0.05 | 32.84 ± 0.08 | C0 |
| 2015ar | 352.92 ± 0.17 | 0.73 ± 0.03 | 15.39 ± 0.02 | ⋯ | 15.26 ± 0.01 | 15.44 ± 0.02 | 15.91 ± 0.03 | 352.67 ± 0.24 | 0.74 ± 0.02 | −0.06 ± 0.02 | 34.14 ± 0.04 | C0 |
| J215050 b | 360.06 ± 0.08 | 0.86 ± 0.01 | 15.56 ± 0.02 | ⋯ | 15.14 ± 0.01 | 15.08 ± 0.01 | 15.44 ± 0.02 | 360.11 ± 0.09 | 0.85 ± 0.01 | 0.40 ± 0.02 | 33.44 ± 0.02 | C0 |
| ASASSN-15ti | 364.81 ± 0.13 | 0.80 ± 0.02 | 16.28 ± 0.02 | ⋯ | 16.07 ± 0.02 | 16.06 ± 0.01 | 16.46 ± 0.02 | 364.80 ± 0.12 | 0.79 ± 0.02 | 0.07 ± 0.02 | 34.53 ± 0.03 | C0 |
| 2015bd | 346.56 ± 0.33 | 1.06 ± 0.03 | 15.35 ± 0.06 | ⋯ | 15.19 ± 0.02 | 15.23 ± 0.04 | 15.76 ± 0.04 | 346.41 ± 0.34 | 1.07 ± 0.03 | 0.12 ± 0.03 | 34.13 ± 0.06 | C0 |
| ASASSN-15uh | 387.63 ± 0.17 | 1.22 ± 0.03 | 15.57 ± 0.03 | ⋯ | 15.30 ± 0.03 | 15.34 ± 0.02 | 15.77 ± 0.03 | 387.60 ± 0.16 | 1.23 ± 0.03 | 0.08 ± 0.02 | 34.05 ± 0.04 | C0 |
| ASASSN-15ut | 392.12 ± 0.36 | 0.77 ± 0.03 | 16.85 ± 0.06 | ⋯ | 16.37 ± 0.04 | 16.31 ± 0.03 | 16.53 ± 0.05 | 392.42 ± 0.42 | 0.72 ± 0.05 | 0.42 ± 0.07 | 34.39 ± 0.09 | C4 |
| 2016A | 392.57 ± 0.75 | 0.90 ± 0.16 | 17.75 ± 0.08 | ⋯ | 16.83 ± 0.04 | 16.64 ± 0.07 | 17.01 ± 0.09 | 390.70 ± 1.69 | 1.19 ± 0.18 | 0.72 ± 0.13 | 34.70 ± 0.21 | C0 |
| 2016F | 406.65 ± 0.33 | 0.97 ± 0.06 | ⋯ | ⋯ | 15.26 ± 0.03 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C0 |
| 2016adp | 406.76 ± 0.21 | 0.23 ± 0.02 | ⋯ | ⋯ | 17.03 ± 0.08 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C1 |
| 2016W | 419.46 ± 0.48 | 0.63 ± 0.10 | ⋯ | ⋯ | 16.01 ± 0.03 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C1 |
| 2016adi | 432.67 ± 0.76 | 0.84 ± 0.02 | 15.48 ± 0.07 | ⋯ | 15.35 ± 0.05 | 15.43 ± 0.04 | 15.91 ± 0.07 | 432.53 ± 0.33 | 0.84 ± 0.01 | 0.04 ± 0.02 | 34.22 ± 0.02 | C0 |
| 2016adn | 428.41 ± 1.06 | 1.02 ± 0.06 | 16.26 ± 0.06 | ⋯ | 16.12 ± 0.05 | 16.21 ± 0.04 | 16.70 ± 0.08 | 428.28 ± 0.55 | 1.02 ± 0.04 | −0.02 ± 0.02 | 34.99 ± 0.04 | C0 |
| 2016asf | 465.22 ± 0.27 | 0.82 ± 0.04 | ⋯ | ⋯ | 15.72 ± 0.02 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C0 |
| 2016aue | 423.35 ± 5.33 | 0.78 ± 0.22 | 15.00 ± 0.11 | ⋯ | 14.80 ± 0.13 | 14.93 ± 0.16 | 15.45 ± 0.20 | 423.22 ± 1.56 | 0.73 ± 0.05 | −0.07 ± 0.05 | 33.54 ± 0.13 | C0 |
| 2016bfu | 471.37 ± 0.12 | 0.46 ± 0.01 | 16.25 ± 0.02 | ⋯ | 15.60 ± 0.01 | 15.62 ± 0.02 | 15.78 ± 0.02 | 471.28 ± 0.15 | 0.46 ± 0.02 | 0.14 ± 0.03 | 33.39 ± 0.05 | C0 |
| 2016blc | 489.88 ± 0.13 | 1.05 ± 0.01 | 14.73 ± 0.01 | ⋯ | 14.74 ± 0.01 | 14.90 ± 0.01 | 15.54 ± 0.01 | 489.68 ± 0.15 | 1.07 ± 0.01 | −0.07 ± 0.01 | 34.11 ± 0.02 | C0 |
| 2016bln | 500.34 ± 0.47 | 1.04 ± 0.07 | ⋯ | ⋯ | 16.01 ± 0.04 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C1 |
| 2016bry | 508.91 ± 0.27 | 0.79 ± 0.04 | ⋯ | ⋯ | 15.77 ± 0.02 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C1 |
| 2016bsa | 505.97 ± 1.05 | 0.97 ± 0.10 | ⋯ | ⋯ | 15.99 ± 0.06 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C0 |
| 2016dxv | 510.96 ± 0.82 | 1.26 ± 0.12 | ⋯ | ⋯ | 16.17 ± 0.03 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C0 |
| 2016cbx | 513.88 ± 0.18 | 1.00 ± 0.03 | 16.67 ± 0.03 | ⋯ | 16.54 ± 0.03 | 16.61 ± 0.02 | 17.28 ± 0.03 | 513.63 ± 0.25 | 1.10 ± 0.05 | 0.08 ± 0.02 | 35.71 ± 0.05 | C0 |
| 2016ccz | 538.96 ± 0.33 | 0.85 ± 0.04 | 15.29 ± 0.14 | ⋯ | 15.43 ± 0.02 | 15.29 ± 0.08 | 15.82 ± 0.10 | 538.72 ± 0.36 | 0.87 ± 0.04 | 0.20 ± 0.11 | 34.12 ± 0.19 | C0 |
| 2016cmn | 537.30 ± 0.54 | 1.04 ± 0.08 | ⋯ | ⋯ | 16.02 ± 0.05 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C0 |
| 2016coj | 549.08 ± 0.07 | 0.90 ± 0.01 | ⋯ | ⋯ | 13.01 ± 0.01 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C1 |
| 2016cqz | 552.80 ± 0.32 | 0.85 ± 0.04 | 15.15 ± 0.07 | ⋯ | 14.91 ± 0.03 | 14.89 ± 0.06 | 15.37 ± 0.12 | 552.74 ± 0.30 | 0.85 ± 0.04 | 0.16 ± 0.07 | 33.43 ± 0.08 | C0 |
| 2016cvn | 556.58 ± 1.33 | 0.79 ± 0.13 | ⋯ | ⋯ | 16.38 ± 0.09 | 15.95 ± 0.17 | 16.23 ± 0.17 | 556.55 ± 1.32 | 0.87 ± 0.09 | 0.87 ± 0.17 | 33.75 ± 0.28 | C2 |
| 2016cyl | 560.27 ± 2.36 | 0.96 ± 0.23 | 17.00 ± 0.51 | ⋯ | 16.53 ± 0.16 | 16.10 ± 0.09 | 15.92 ± 0.19 | 559.69 ± 3.60 | 0.88 ± 0.21 | 0.49 ± 0.41 | 33.43 ± 0.43 | C0 |
| 2016daj | 592.48 ± 0.19 | 1.00 ± 0.03 | 16.62 ± 0.03 | ⋯ | 16.52 ± 0.02 | 16.63 ± 0.02 | 17.18 ± 0.03 | 592.28 ± 0.21 | 1.02 ± 0.03 | −0.03 ± 0.02 | 35.55 ± 0.04 | C0 |
| 2016eiy | 608.76 ± 0.17 | 0.95 ± 0.04 | 14.61 ± 0.08 | ⋯ | 14.23 ± 0.02 | 14.24 ± 0.06 | 14.76 ± 0.12 | 608.50 ± 0.21 | 0.94 ± 0.03 | 0.25 ± 0.05 | 32.65 ± 0.08 | C0 |
| 2016ekg | 610.29 ± 0.05 | 0.97 ± 0.01 | 15.09 ± 0.01 | ⋯ | 15.07 ± 0.01 | 15.20 ± 0.01 | 15.77 ± 0.01 | 610.29 ± 0.05 | 0.98 ± 0.01 | 0.01 ± 0.01 | 34.27 ± 0.01 | C0 |
| 2016ekt | 603.56 ± 0.09 | 1.03 ± 0.01 | 14.78 ± 0.01 | ⋯ | 14.71 ± 0.01 | 14.79 ± 0.01 | 15.42 ± 0.01 | 603.34 ± 0.11 | 1.06 ± 0.01 | 0.04 ± 0.01 | 33.90 ± 0.02 | C0 |
| 2016euj | 619.57 ± 0.09 | 0.84 ± 0.01 | 15.40 ± 0.02 | ⋯ | 15.36 ± 0.01 | 15.51 ± 0.01 | 16.05 ± 0.02 | 619.58 ± 0.09 | 0.83 ± 0.01 | −0.04 ± 0.02 | 34.49 ± 0.02 | C0 |
| 2016fej | 637.33 ± 0.04 | 1.02 ± 0.01 | 13.97 ± 0.01 | ⋯ | 13.91 ± 0.01 | 14.07 ± 0.01 | 14.68 ± 0.01 | 637.48 ± 0.05 | 1.01 ± 0.01 | −0.01 ± 0.01 | 33.13 ± 0.01 | C0 |
| 2016fff | 630.45 ± 0.07 | 0.70 ± 0.01 | 15.06 ± 0.01 | ⋯ | 14.93 ± 0.01 | 14.96 ± 0.01 | 15.43 ± 0.01 | 630.47 ± 0.07 | 0.70 ± 0.01 | 0.04 ± 0.01 | 33.61 ± 0.02 | C0 |
| 2016fnr | 640.70 ± 0.85 | 0.84 ± 0.02 | 15.24 ± 0.07 | ⋯ | 15.03 ± 0.04 | 15.13 ± 0.03 | 15.56 ± 0.04 | 640.16 ± 0.91 | 0.85 ± 0.02 | 0.10 ± 0.05 | 33.83 ± 0.06 | C0 |
| 2016fob | 631.71 ± 0.46 | 1.06 ± 0.04 | 16.38 ± 0.08 | ⋯ | 16.10 ± 0.02 | 16.19 ± 0.04 | 16.61 ± 0.07 | 631.64 ± 0.51 | 1.05 ± 0.03 | 0.02 ± 0.02 | 34.80 ± 0.04 | C0 |
| 2016gfk | 645.83 ± 0.36 | 0.86 ± 0.03 | 17.36 ± 0.07 | ⋯ | 16.78 ± 0.02 | 16.56 ± 0.04 | 16.75 ± 0.07 | 645.85 ± 0.37 | 0.86 ± 0.02 | 0.68 ± 0.02 | 34.49 ± 0.03 | C0 |
| 2016gfr | 657.25 ± 0.14 | 1.06 ± 0.02 | 15.41 ± 0.03 | ⋯ | 15.28 ± 0.03 | 15.37 ± 0.02 | 15.90 ± 0.02 | 657.18 ± 0.15 | 1.08 ± 0.03 | −0.0 ± 0.02 | 34.27 ± 0.04 | C0 |
| 2016hsc | 666.79 ± 0.23 | 1.03 ± 0.03 | 15.18 ± 0.08 | ⋯ | 15.06 ± 0.02 | 15.11 ± 0.05 | 15.67 ± 0.08 | 666.67 ± 0.22 | 1.03 ± 0.02 | 0.05 ± 0.02 | 34.00 ± 0.05 | C0 |
| 2016gou | 666.47 ± 0.74 | 0.99 ± 0.03 | 16.11 ± 0.06 | ⋯ | 15.84 ± 0.05 | 15.86 ± 0.03 | 16.22 ± 0.07 | 666.66 ± 0.30 | 0.97 ± 0.01 | 0.20 ± 0.01 | 34.38 ± 0.02 | C0 |
| 2016gsb | 672.68 ± 0.08 | 0.99 ± 0.01 | 14.59 ± 0.01 | ⋯ | 14.42 ± 0.01 | 14.50 ± 0.02 | 15.13 ± 0.01 | 672.28 ± 0.11 | 1.18 ± 0.02 | 0.05 ± 0.02 | 33.61 ± 0.03 | C0 |
| 2016gsn | 671.65 ± 0.07 | 1.03 ± 0.01 | 15.29 ± 0.01 | ⋯ | 15.09 ± 0.01 | 15.18 ± 0.01 | 15.64 ± 0.01 | 671.56 ± 0.09 | 1.04 ± 0.01 | −0.01 ± 0.01 | 33.88 ± 0.02 | C0 |
| 2016gtr | 669.12 ± 0.27 | 1.10 ± 0.04 | 15.66 ± 0.02 | ⋯ | 15.59 ± 0.01 | 15.70 ± 0.02 | 16.34 ± 0.03 | 669.00 ± 0.26 | 1.12 ± 0.04 | −0.01 ± 0.02 | 34.82 ± 0.05 | C0 |
| 2016gwl | 627.62 ± 0.39 | 1.07 ± 0.02 | 14.25 ± 0.02 | ⋯ | 14.23 ± 0.02 | 14.42 ± 0.03 | 15.01 ± 0.03 | 626.69 ± 0.45 | 1.19 ± 0.01 | −0.18 ± 0.02 | 33.70 ± 0.03 | C3 |
| 2016gxp | 685.94 ± 0.19 | 1.22 ± 0.02 | 15.21 ± 0.02 | ⋯ | 14.85 ± 0.01 | 14.80 ± 0.01 | 15.07 ± 0.02 | 686.09 ± 0.06 | 1.21 ± 0.02 | 0.29 ± 0.02 | 33.23 ± 0.03 | C4 |
| 2016hht | 683.31 ± 0.66 | 0.92 ± 0.02 | 15.61 ± 0.06 | ⋯ | 15.59 ± 0.04 | 15.67 ± 0.03 | 16.26 ± 0.07 | 683.27 ± 0.19 | 0.92 ± 0.01 | 0.00 ± 0.01 | 34.67 ± 0.02 | C0 |
| 2016iil | 684.41 ± 0.89 | 0.92 ± 0.04 | 16.80 ± 0.07 | ⋯ | 16.62 ± 0.05 | 16.68 ± 0.03 | 17.24 ± 0.07 | 683.90 ± 0.55 | 0.95 ± 0.03 | 0.10 ± 0.02 | 35.50 ± 0.03 | C0 |
| 2016hmo | 676.77 ± 0.46 | 1.10 ± 0.05 | 17.80 ± 0.05 | ⋯ | 16.85 ± 0.03 | 16.60 ± 0.04 | 16.70 ± 0.04 | 676.57 ± 0.50 | 1.09 ± 0.05 | 0.91 ± 0.04 | 34.29 ± 0.08 | C0 |
| 2016hli | 697.01 ± 0.09 | 0.70 ± 0.01 | 17.48 ± 0.02 | ⋯ | 16.78 ± 0.01 | 16.58 ± 0.01 | 16.64 ± 0.01 | 696.95 ± 0.12 | 0.69 ± 0.01 | 0.19 ± 0.02 | 33.91 ± 0.02 | C0 |
| 2016hnk | 692.09 ± 0.31 | 0.49 ± 0.02 | 19.02 ± 0.09 | ⋯ | 17.55 ± 0.03 | 17.35 ± 0.03 | 17.58 ± 0.03 | 693.24 ± 0.98 | 1.02 ± 0.10 | 1.08 ± 0.06 | 34.95 ± 0.11 | C4 |
| 2016hpw | 703.63 ± 0.11 | 1.01 ± 0.02 | 16.08 ± 0.02 | ⋯ | 15.96 ± 0.01 | 16.02 ± 0.01 | 16.60 ± 0.02 | 703.57 ± 0.12 | 1.01 ± 0.02 | 0.07 ± 0.01 | 34.92 ± 0.02 | C0 |
| 2016hvl | 710.60 ± 0.17 | 1.19 ± 0.02 | 16.06 ± 0.02 | ⋯ | 15.45 ± 0.02 | 15.40 ± 0.02 | 15.67 ± 0.03 | 710.51 ± 0.20 | 1.18 ± 0.02 | 0.16 ± 0.03 | 33.36 ± 0.05 | C0 |
| 2016huh | 699.91 ± 0.20 | 0.78 ± 0.01 | 17.24 ± 0.02 | ⋯ | 16.82 ± 0.01 | 16.70 ± 0.01 | 16.99 ± 0.02 | 699.94 ± 0.19 | 0.78 ± 0.01 | 0.27 ± 0.02 | 34.79 ± 0.02 | C0 |
| 2016igr | 726.33 ± 0.19 | 1.01 ± 0.01 | 15.39 ± 0.02 | ⋯ | 15.30 ± 0.02 | 15.45 ± 0.01 | 16.07 ± 0.01 | 726.04 ± 0.23 | 1.03 ± 0.02 | 0.00 ± 0.01 | 34.55 ± 0.03 | C0 |
| 2016ins | 722.99 ± 0.31 | 0.83 ± 0.02 | 16.89 ± 0.03 | ⋯ | 16.58 ± 0.02 | 16.55 ± 0.02 | 17.00 ± 0.03 | 722.94 ± 0.32 | 0.83 ± 0.02 | 0.26 ± 0.02 | 35.06 ± 0.04 | C0 |
| 2016ipf | 728.33 ± 0.26 | 0.83 ± 0.01 | 16.78 ± 0.02 | ⋯ | 16.70 ± 0.02 | 16.75 ± 0.02 | 17.28 ± 0.02 | 728.31 ± 0.26 | 0.83 ± 0.01 | 0.06 ± 0.02 | 35.59 ± 0.03 | C0 |
| 2016itd | 733.77 ± 1.21 | 0.99 ± 0.03 | 15.65 ± 0.10 | ⋯ | 15.42 ± 0.08 | 15.50 ± 0.08 | 16.12 ± 0.11 | 733.05 ± 0.80 | 1.00 ± 0.02 | 0.15 ± 0.03 | 34.37 ± 0.08 | C0 |
| 2016ito | 721.55 ± 0.55 | 1.23 ± 0.02 | 15.67 ± 0.03 | ⋯ | 15.64 ± 0.02 | 15.84 ± 0.02 | 16.39 ± 0.03 | 721.70 ± 0.49 | 1.22 ± 0.02 | −0.11 ± 0.02 | 35.03 ± 0.03 | C0 |
| 2016iuh | 738.04 ± 0.65 | 0.68 ± 0.03 | 15.59 ± 0.07 | ⋯ | 15.40 ± 0.04 | 15.49 ± 0.03 | 15.87 ± 0.07 | 738.09 ± 0.25 | 0.67 ± 0.02 | 0.02 ± 0.04 | 34.09 ± 0.04 | C0 |
| 2016jae | 751.28 ± 0.19 | 0.53 ± 0.01 | 17.40 ± 0.03 | ⋯ | 16.79 ± 0.01 | 16.80 ± 0.01 | 17.15 ± 0.02 | 750.36 ± 0.30 | 0.57 ± 0.02 | 0.18 ± 0.03 | 34.90 ± 0.03 | C0 |
| 2016jab | 749.91 ± 0.21 | 1.08 ± 0.02 | 16.10 ± 0.01 | ⋯ | 15.95 ± 0.01 | 16.01 ± 0.01 | 16.54 ± 0.01 | 749.71 ± 0.21 | 1.09 ± 0.02 | −0.02 ± 0.01 | 34.85 ± 0.02 | C0 |
| 2017ae | 769.49 ± 1.57 | 1.42 ± 0.25 | ⋯ | ⋯ | 16.41 ± 0.05 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C1 |
| 2017jl | 784.79 ± 0.10 | 1.08 ± 0.02 | 15.05 ± 0.01 | ⋯ | 14.94 ± 0.01 | 15.03 ± 0.01 | 15.52 ± 0.02 | 784.78 ± 0.11 | 1.07 ± 0.02 | 0.06 ± 0.01 | 33.93 ± 0.03 | C0 |
| 2017yv | 795.62 ± 0.12 | 1.00 ± 0.01 | 15.85 ± 0.02 | ⋯ | 15.59 ± 0.02 | 15.62 ± 0.02 | 16.15 ± 0.02 | 795.55 ± 0.15 | 1.02 ± 0.02 | 0.16 ± 0.01 | 34.40 ± 0.03 | C0 |
| 2017atv | 801.11 ± 0.89 | 0.80 ± 0.03 | 17.16 ± 0.08 | ⋯ | 16.59 ± 0.03 | 16.52 ± 0.04 | 16.85 ± 0.08 | 800.74 ± 0.53 | 0.82 ± 0.02 | 0.20 ± 0.03 | 34.52 ± 0.04 | C0 |
| 2017aut | 792.85 ± 0.94 | 1.13 ± 0.06 | 17.63 ± 0.08 | ⋯ | 17.10 ± 0.05 | 16.91 ± 0.05 | ⋯ | 792.84 ± 0.48 | 1.13 ± 0.04 | 0.50 ± 0.05 | 35.09 ± 0.09 | C0 |
| 2017awk | 808.37 ± 0.16 | 0.93 ± 0.01 | 16.07 ± 0.02 | ⋯ | 15.74 ± 0.01 | 15.77 ± 0.01 | 16.27 ± 0.02 | 808.14 ± 0.20 | 0.94 ± 0.01 | 0.20 ± 0.01 | 34.35 ± 0.03 | C0 |
| 2017azw | 817.03 ± 0.10 | 1.09 ± 0.02 | 15.00 ± 0.02 | ⋯ | 14.98 ± 0.01 | 15.14 ± 0.01 | 15.77 ± 0.01 | 817.00 ± 0.11 | 1.09 ± 0.02 | −0.09 ± 0.01 | 34.31 ± 0.03 | C0 |
| 2017bkc | 811.96 ± 0.28 | 1.02 ± 0.02 | 17.21 ± 0.02 | ⋯ | 16.62 ± 0.02 | 16.53 ± 0.02 | 16.84 ± 0.02 | 810.50 ± 0.37 | 1.18 ± 0.03 | 0.13 ± 0.03 | 34.62 ± 0.04 | C0 |
| 2017cav | 821.33 ± 0.27 | 1.00 ± 0.03 | 16.58 ± 0.05 | ⋯ | 16.31 ± 0.01 | 16.36 ± 0.03 | 16.79 ± 0.06 | 820.91 ± 0.32 | 1.02 ± 0.02 | 0.02 ± 0.01 | 34.91 ± 0.02 | C0 |
| 2017bzc | 826.54 ± 0.28 | 1.12 ± 0.02 | 12.39 ± 0.02 | ⋯ | 12.29 ± 0.01 | 12.47 ± 0.02 | 13.06 ± 0.03 | 825.97 ± 0.42 | 1.11 ± 0.03 | 0.01 ± 0.02 | 31.56 ± 0.04 | C3 |
| 2017cbr | 834.22 ± 0.16 | 0.91 ± 0.01 | 15.98 ± 0.01 | ⋯ | 15.75 ± 0.01 | 15.74 ± 0.01 | 16.17 ± 0.01 | 834.22 ± 0.16 | 0.90 ± 0.01 | 0.23 ± 0.01 | 34.34 ± 0.02 | C0 |
| 2017cbv | 840.66 ± 0.05 | 1.19 ± 0.01 | 11.77 ± 0.01 | ⋯ | 11.70 ± 0.01 | 11.78 ± 0.01 | 12.23 ± 0.01 | 840.79 ± 0.06 | 1.08 ± 0.01 | −0.02 ± 0.01 | 30.56 ± 0.02 | C0 |
| 2017cfd | 844.03 ± 0.06 | 0.93 ± 0.01 | 14.94 ± 0.01 | ⋯ | 14.78 ± 0.01 | 14.82 ± 0.01 | 15.34 ± 0.01 | 844.04 ± 0.06 | 0.93 ± 0.01 | 0.16 ± 0.01 | 33.63 ± 0.02 | C0 |
| 2017ckq | 851.31 ± 0.05 | 0.96 ± 0.01 | 14.38 ± 0.01 | ⋯ | 14.33 ± 0.01 | 14.42 ± 0.01 | 14.93 ± 0.01 | 851.24 ± 0.07 | 0.95 ± 0.01 | 0.02 ± 0.01 | 33.31 ± 0.01 | C0 |
| 2017cjr | 847.36 ± 0.08 | 0.91 ± 0.01 | 15.08 ± 0.01 | ⋯ | 15.06 ± 0.01 | 15.11 ± 0.01 | 15.62 ± 0.02 | 847.34 ± 0.08 | 0.91 ± 0.01 | 0.02 ± 0.01 | 34.00 ± 0.02 | C0 |
| 2017cts | 856.80 ± 0.13 | 0.95 ± 0.01 | 15.81 ± 0.02 | ⋯ | 15.72 ± 0.01 | 15.81 ± 0.01 | 16.35 ± 0.01 | 856.77 ± 0.13 | 0.94 ± 0.01 | 0.07 ± 0.01 | 34.73 ± 0.02 | C0 |
| 2017kdz | 846.93 ± 0.50 | 0.53 ± 0.06 | 17.03 ± 0.11 | ⋯ | 16.49 ± 0.06 | 16.46 ± 0.07 | 16.61 ± 0.12 | 846.66 ± 0.50 | 0.54 ± 0.06 | 0.08 ± 0.05 | 34.24 ± 0.22 | C0 |
| 2017cze | 857.02 ± 0.21 | 0.53 ± 0.02 | 16.08 ± 0.03 | ⋯ | 15.77 ± 0.02 | 15.86 ± 0.02 | 16.25 ± 0.03 | 856.85 ± 0.39 | 0.51 ± 0.04 | −0.16 ± 0.07 | 34.25 ± 0.06 | C0 |
| 2017cyy | 870.87 ± 0.05 | 0.98 ± 0.01 | 14.95 ± 0.01 | ⋯ | 14.74 ± 0.01 | 14.77 ± 0.01 | 15.25 ± 0.01 | 870.85 ± 0.07 | 0.98 ± 0.01 | −0.01 ± 0.01 | 33.38 ± 0.02 | C0 |
| 2017daf | 860.77 ± 0.42 | 0.77 ± 0.02 | 15.89 ± 0.03 | ⋯ | 15.79 ± 0.02 | 15.86 ± 0.02 | 16.40 ± 0.03 | 860.56 ± 0.39 | 0.78 ± 0.02 | 0.03 ± 0.02 | 34.68 ± 0.03 | C0 |
| 2017dei | 869.26 ± 0.15 | 0.70 ± 0.01 | 16.72 ± 0.02 | ⋯ | 16.38 ± 0.02 | 16.35 ± 0.01 | 16.74 ± 0.02 | 869.23 ± 0.15 | 0.71 ± 0.01 | 0.17 ± 0.02 | 34.67 ± 0.02 | C0 |
| 2017dhr | 870.46 ± 0.69 | 1.10 ± 0.08 | 17.58 ± 0.12 | ⋯ | 16.20 ± 0.03 | 15.67 ± 0.06 | 15.52 ± 0.09 | 870.53 ± 0.59 | 1.08 ± 0.05 | 1.47 ± 0.04 | 32.51 ± 0.08 | C0 |
| 2017dit | 881.50 ± 0.12 | 0.88 ± 0.01 | 15.98 ± 0.02 | ⋯ | 15.85 ± 0.02 | 15.85 ± 0.02 | 16.53 ± 0.02 | 881.56 ± 0.17 | 0.88 ± 0.02 | 0.10 ± 0.02 | 34.77 ± 0.04 | C0 |
| 2017dps | 882.44 ± 0.09 | 0.75 ± 0.01 | 14.85 ± 0.01 | ⋯ | 14.77 ± 0.01 | 14.87 ± 0.01 | 15.38 ± 0.01 | 882.42 ± 0.09 | 0.75 ± 0.01 | −0.05 ± 0.01 | 33.65 ± 0.02 | C0 |
| 2017drh | 891.00 ± 0.10 | 0.88 ± 0.01 | 17.10 ± 0.02 | ⋯ | 15.71 ± 0.02 | 15.13 ± 0.01 | 14.93 ± 0.02 | 890.95 ± 0.10 | 0.88 ± 0.01 | 1.46 ± 0.02 | 31.79 ± 0.03 | C0 |
| 2017dzs | 860.51 ± 6.07 | 0.93 ± 0.24 | 15.38 ± 0.15 | ⋯ | 15.33 ± 0.18 | 15.53 ± 0.25 | 16.10 ± 0.28 | 855.40 ± 6.20 | 1.18 ± 0.22 | −0.17 ± 0.17 | 34.93 ± 0.42 | C3 |
| 2017eck | 899.86 ± 0.28 | 1.14 ± 0.03 | 16.43 ± 0.02 | ⋯ | 16.20 ± 0.01 | 16.23 ± 0.01 | 16.70 ± 0.01 | 899.61 ± 0.19 | 1.18 ± 0.02 | −0.0 ± 0.02 | 34.95 ± 0.03 | C0 |
| 2017ebm | 887.23 ± 1.23 | 0.39 ± 0.05 | 18.38 ± 0.15 | ⋯ | 17.42 ± 0.10 | 17.44 ± 0.07 | 17.44 ± 0.10 | 886.84 ± 1.28 | 0.41 ± 0.04 | 0.24 ± 0.08 | 34.79 ± 0.09 | C0 |
| 2017edu | 856.31 ± 1.47 | 0.77 ± 0.45 | ⋯ | ⋯ | 16.87 ± 0.18 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C1 |
| 2017egb | 906.48 ± 0.11 | 0.80 ± 0.01 | 15.79 ± 0.02 | ⋯ | 15.68 ± 0.01 | 15.70 ± 0.01 | 16.14 ± 0.02 | 906.50 ± 0.11 | 0.80 ± 0.01 | 0.09 ± 0.02 | 34.37 ± 0.02 | C0 |
| 2017ejb | 911.40 ± 0.07 | 0.47 ± 0.01 | 15.88 ± 0.02 | ⋯ | 15.37 ± 0.01 | 15.32 ± 0.01 | 15.57 ± 0.02 | 911.39 ± 0.09 | 0.47 ± 0.01 | 0.05 ± 0.02 | 33.18 ± 0.03 | C0 |
| 2017ejw | 912.17 ± 0.11 | 0.85 ± 0.01 | 15.54 ± 0.02 | ⋯ | 15.53 ± 0.01 | 15.63 ± 0.01 | 16.19 ± 0.02 | 912.16 ± 0.11 | 0.84 ± 0.01 | −0.03 ± 0.01 | 34.59 ± 0.02 | C0 |
| 2017ekr | 913.88 ± 0.14 | 0.83 ± 0.01 | 16.10 ± 0.03 | ⋯ | 15.95 ± 0.02 | 15.98 ± 0.02 | 16.52 ± 0.02 | 913.83 ± 0.14 | 0.83 ± 0.01 | 0.02 ± 0.02 | 34.73 ± 0.03 | C0 |
| 2017emq | 917.27 ± 0.08 | 0.85 ± 0.01 | 14.39 ± 0.01 | ⋯ | 14.13 ± 0.01 | 14.14 ± 0.02 | 14.68 ± 0.02 | 917.35 ± 0.11 | 0.84 ± 0.02 | 0.23 ± 0.02 | 32.78 ± 0.04 | C0 |
| 2017enx | 918.42 ± 0.33 | 0.70 ± 0.02 | 14.09 ± 0.03 | ⋯ | 13.82 ± 0.02 | 13.80 ± 0.02 | 14.16 ± 0.02 | 918.33 ± 0.29 | 0.70 ± 0.02 | 0.01 ± 0.03 | 32.08 ± 0.03 | C0 |
| 2017erv | 924.79 ± 0.25 | 1.13 ± 0.04 | 16.02 ± 0.03 | ⋯ | 15.69 ± 0.02 | 15.74 ± 0.03 | 16.33 ± 0.02 | 923.72 ± 0.39 | 1.26 ± 0.03 | 0.01 ± 0.03 | 34.67 ± 0.04 | C0 |
| 2017erp | 935.24 ± 0.08 | 1.03 ± 0.01 | 13.77 ± 0.01 | ⋯ | 13.49 ± 0.01 | 13.51 ± 0.01 | 14.00 ± 0.04 | 935.17 ± 0.09 | 1.03 ± 0.01 | 0.19 ± 0.01 | 32.16 ± 0.02 | C0 |
| 2017ezd | 941.78 ± 0.11 | 0.89 ± 0.01 | 15.83 ± 0.02 | ⋯ | 15.73 ± 0.02 | 15.76 ± 0.02 | 16.13 ± 0.02 | 941.87 ± 0.16 | 0.88 ± 0.02 | 0.13 ± 0.03 | 34.34 ± 0.04 | C0 |
| 2017evn | 935.14 ± 0.14 | 1.08 ± 0.03 | 15.46 ± 0.02 | ⋯ | 15.34 ± 0.02 | 15.48 ± 0.02 | 16.09 ± 0.03 | 935.25 ± 0.16 | 1.09 ± 0.03 | 0.04 ± 0.02 | 34.55 ± 0.05 | C0 |
| 2017exo | 936.88 ± 0.11 | 1.10 ± 0.02 | 16.70 ± 0.01 | ⋯ | 16.25 ± 0.01 | 16.18 ± 0.01 | 16.60 ± 0.01 | 936.80 ± 0.13 | 1.11 ± 0.02 | 0.13 ± 0.01 | 34.49 ± 0.03 | C0 |
| 2017fbj | 944.46 ± 0.19 | 0.91 ± 0.03 | 16.20 ± 0.03 | ⋯ | 15.92 ± 0.03 | 16.00 ± 0.05 | 16.57 ± 0.07 | 944.44 ± 0.24 | 0.91 ± 0.03 | 0.07 ± 0.03 | 34.53 ± 0.10 | C0 |
| 2017ffv | 956.99 ± 0.09 | 0.94 ± 0.01 | 15.58 ± 0.02 | ⋯ | 15.23 ± 0.02 | 15.21 ± 0.01 | 15.67 ± 0.03 | 956.96 ± 0.10 | 0.94 ± 0.01 | 0.29 ± 0.02 | 33.72 ± 0.03 | C0 |
| 2017fgc | 961.00 ± 0.15 | 1.08 ± 0.01 | 13.84 ± 0.01 | 14.11 ± 0.04 | 13.57 ± 0.01 | 13.63 ± 0.01 | 14.26 ± 0.01 | 959.97 ± 0.12 | 1.19 ± 0.02 | 0.15 ± 0.02 | 32.57 ± 0.03 | C0 |
| 2017fvl | 971.65 ± 0.84 | 0.88 ± 0.04 | 16.49 ± 0.06 | ⋯ | 15.99 ± 0.04 | 15.87 ± 0.04 | 16.17 ± 0.07 | 971.26 ± 0.47 | 0.88 ± 0.03 | 0.07 ± 0.02 | 33.73 ± 0.03 | C0 |
| 2017fzy | 979.69 ± 0.12 | 0.61 ± 0.01 | 16.42 ± 0.02 | ⋯ | 15.89 ± 0.01 | 15.84 ± 0.01 | 16.14 ± 0.02 | 979.53 ± 0.18 | 0.62 ± 0.02 | 0.20 ± 0.03 | 33.83 ± 0.03 | C0 |
| 2017fzw | 988.89 ± 0.06 | 0.62 ± 0.01 | 14.24 ± 0.01 | ⋯ | 13.78 ± 0.01 | 13.74 ± 0.01 | 14.22 ± 0.02 | 988.95 ± 0.08 | 0.60 ± 0.01 | 0.19 ± 0.02 | 31.95 ± 0.03 | C0 |
| 2017gah | 985.66 ± 0.13 | 0.62 ± 0.01 | 15.00 ± 0.01 | 15.07 ± 0.05 | 14.56 ± 0.01 | 14.48 ± 0.01 | 14.89 ± 0.02 | 985.66 ± 0.07 | 0.63 ± 0.01 | 0.23 ± 0.02 | 32.69 ± 0.02 | C0 |
| 2017ghu | 984.92 ± 0.65 | 0.93 ± 0.02 | 17.79 ± 0.07 | ⋯ | 16.99 ± 0.05 | 16.74 ± 0.05 | 17.04 ± 0.06 | 982.61 ± 1.00 | 1.18 ± 0.05 | 0.15 ± 0.05 | 34.68 ± 0.07 | C0 |
| 2017gjn | 1004.38 ± 0.19 | 0.99 ± 0.01 | 15.17 ± 0.01 | 15.17 ± 0.03 | 15.05 ± 0.01 | 15.14 ± 0.01 | 15.63 ± 0.01 | 1004.28 ± 0.12 | 0.99 ± 0.01 | −0.03 ± 0.01 | 33.91 ± 0.02 | C0 |
| 2017glq | 1016.13 ± 0.06 | 0.91 ± 0.01 | 14.32 ± 0.01 | 14.39 ± 0.01 | 14.25 ± 0.01 | 14.34 ± 0.01 | 14.82 ± 0.01 | 1016.00 ± 0.05 | 0.92 ± 0.01 | 0.06 ± 0.01 | 33.21 ± 0.01 | C0 |
| 2017glx | 1009.96 ± 0.61 | 1.09 ± 0.02 | 14.70 ± 0.02 | 14.85 ± 0.04 | 14.51 ± 0.01 | 14.56 ± 0.02 | 15.05 ± 0.03 | 1009.92 ± 0.12 | 1.09 ± 0.02 | 0.09 ± 0.01 | 33.34 ± 0.03 | C0 |
| 2017grw | 1017.93 ± 0.11 | 0.75 ± 0.01 | 15.53 ± 0.02 | ⋯ | 15.46 ± 0.01 | 15.47 ± 0.01 | 15.95 ± 0.02 | 1017.94 ± 0.12 | 0.76 ± 0.01 | 0.03 ± 0.02 | 34.20 ± 0.02 | C0 |
| 2017guu | 1026.69 ± 0.36 | 1.13 ± 0.07 | 17.03 ± 0.09 | 17.16 ± 0.06 | 16.60 ± 0.03 | 16.60 ± 0.06 | 17.02 ± 0.05 | 1024.83 ± 1.24 | 1.26 ± 0.05 | −0.38 ± 0.06 | 34.93 ± 0.09 | C0 |
| 2017gxq | 1029.69 ± 0.22 | 1.00 ± 0.02 | 14.11 ± 0.06 | 14.36 ± 0.10 | 14.05 ± 0.04 | 14.20 ± 0.03 | 14.72 ± 0.06 | 1029.72 ± 0.20 | 0.99 ± 0.01 | 0.05 ± 0.01 | 33.19 ± 0.02 | C0 |
| 2017gup | 1021.58 ± 1.61 | 1.42 ± 0.09 | 17.31 ± 0.10 | 17.76 ± 0.11 | 16.86 ± 0.07 | 16.90 ± 0.05 | 17.13 ± 0.08 | 1021.57 ± 1.50 | 1.43 ± 0.06 | −0.21 ± 0.09 | 35.17 ± 0.07 | C0 |
| 2017guh | 1022.37 ± 0.16 | 0.87 ± 0.01 | 15.23 ± 0.03 | 15.27 ± 0.03 | 15.12 ± 0.02 | 15.18 ± 0.02 | 15.65 ± 0.03 | 1022.11 ± 0.23 | 0.89 ± 0.02 | 0.13 ± 0.02 | 33.96 ± 0.04 | C0 |
| 2017haf | 1034.64 ± 0.12 | 0.92 ± 0.01 | 15.48 ± 0.01 | 15.55 ± 0.02 | 15.34 ± 0.01 | 15.40 ± 0.01 | 16.01 ± 0.02 | 1034.50 ± 0.15 | 0.92 ± 0.01 | 0.09 ± 0.01 | 34.28 ± 0.02 | C0 |
| 2017hgz | 1044.80 ± 0.10 | 0.82 ± 0.01 | 15.26 ± 0.02 | 15.31 ± 0.02 | 15.13 ± 0.01 | 15.17 ± 0.01 | 15.66 ± 0.02 | 1044.76 ± 0.12 | 0.83 ± 0.01 | 0.11 ± 0.02 | 33.92 ± 0.02 | C0 |
| 2017hjw | 1056.23 ± 0.07 | 1.02 ± 0.01 | 16.25 ± 0.01 | 16.26 ± 0.02 | 15.90 ± 0.01 | 15.87 ± 0.01 | 16.32 ± 0.01 | 1056.15 ± 0.08 | 1.03 ± 0.01 | 0.23 ± 0.01 | 34.40 ± 0.02 | C0 |
| 2017hjy | 1056.16 ± 0.12 | 0.96 ± 0.01 | 15.59 ± 0.02 | 15.72 ± 0.02 | 15.40 ± 0.01 | 15.45 ± 0.01 | 16.01 ± 0.02 | 1056.19 ± 0.14 | 0.97 ± 0.01 | 0.11 ± 0.01 | 34.24 ± 0.03 | C0 |
| 2017hle | 1050.64 ± 0.11 | 0.39 ± 0.01 | 17.89 ± 0.02 | 17.63 ± 0.04 | 16.97 ± 0.02 | 16.86 ± 0.02 | 16.96 ± 0.02 | 1050.55 ± 0.15 | 0.36 ± 0.01 | 0.20 ± 0.03 | 34.21 ± 0.05 | C0 |
| 2017hoq | 1061.86 ± 0.13 | 1.06 ± 0.02 | 16.04 ± 0.02 | 16.10 ± 0.01 | 15.93 ± 0.01 | 16.05 ± 0.02 | 16.70 ± 0.02 | 1061.55 ± 0.28 | 1.09 ± 0.03 | −0.03 ± 0.02 | 35.15 ± 0.04 | C0 |
| 2017hou | 1056.19 ± 0.22 | 1.07 ± 0.03 | 18.23 ± 0.02 | 18.00 ± 0.07 | 17.46 ± 0.01 | 17.21 ± 0.01 | 17.46 ± 0.02 | 1056.06 ± 0.27 | 1.12 ± 0.03 | 0.69 ± 0.02 | 35.11 ± 0.04 | C0 |
| 2017hpa | 1066.76 ± 0.09 | 1.01 ± 0.01 | 15.60 ± 0.02 | 15.61 ± 0.05 | 15.37 ± 0.01 | 15.38 ± 0.01 | 15.85 ± 0.02 | 1066.73 ± 0.08 | 1.01 ± 0.01 | 0.09 ± 0.01 | 33.99 ± 0.02 | C0 |
| 2017igf | 1085.38 ± 0.51 | 0.57 ± 0.01 | 14.89 ± 0.01 | 14.67 ± 0.04 | 14.59 ± 0.01 | 14.50 ± 0.01 | 14.87 ± 0.01 | 1085.40 ± 0.06 | 0.58 ± 0.01 | 0.11 ± 0.02 | 32.76 ± 0.02 | C0 |
| 2017iji | 1082.15 ± 0.81 | 0.92 ± 0.01 | 15.19 ± 0.02 | 15.29 ± 0.05 | 14.93 ± 0.02 | 15.02 ± 0.02 | 15.57 ± 0.03 | 1078.97 ± 0.46 | 1.10 ± 0.03 | 0.14 ± 0.02 | 34.00 ± 0.04 | C0 |
| 2017isj | 1094.31 ± 0.17 | 1.07 ± 0.02 | 15.88 ± 0.02 | 16.21 ± 0.03 | 15.63 ± 0.01 | 15.77 ± 0.02 | 16.39 ± 0.02 | 1092.62 ± 0.39 | 1.19 ± 0.02 | 0.01 ± 0.02 | 34.79 ± 0.04 | C0 |
| 2017isq | 1048.68 ± 1.01 | 1.19 ± 0.02 | 13.92 ± 0.03 | 14.44 ± 0.04 | 13.75 ± 0.03 | 13.80 ± 0.03 | 14.40 ± 0.07 | 1047.89 ± 0.97 | 1.47 ± 0.03 | −0.40 ± 0.04 | 33.61 ± 0.04 | C3 |
| 2017izu | 1116.78 ± 0.30 | 0.91 ± 0.02 | 15.05 ± 0.06 | 15.11 ± 0.02 | 14.84 ± 0.05 | 14.89 ± 0.04 | 15.40 ± 0.08 | 1116.20 ± 0.27 | 0.94 ± 0.01 | 0.14 ± 0.01 | 33.58 ± 0.02 | C0 |
| 2017iyb | 1118.01 ± 0.09 | 0.82 ± 0.01 | 14.95 ± 0.01 | 14.96 ± 0.01 | 14.77 ± 0.01 | 14.85 ± 0.01 | 15.43 ± 0.02 | 1117.44 ± 0.15 | 0.86 ± 0.01 | 0.12 ± 0.01 | 33.63 ± 0.02 | C0 |
| 2017iyw | 1107.88 ± 0.13 | 0.92 ± 0.01 | 15.74 ± 0.02 | 15.73 ± 0.02 | 15.60 ± 0.01 | 15.64 ± 0.01 | 16.16 ± 0.01 | 1107.99 ± 0.17 | 0.91 ± 0.01 | 0.14 ± 0.01 | 34.46 ± 0.02 | C0 |
| 2017jav | 1118.42 ± 0.53 | 0.64 ± 0.01 | 16.02 ± 0.01 | 15.87 ± 0.10 | 15.80 ± 0.01 | 15.86 ± 0.01 | 16.22 ± 0.01 | 1118.34 ± 0.08 | 0.64 ± 0.01 | 0.01 ± 0.02 | 34.30 ± 0.02 | C0 |
| 2017jdx | 1119.57 ± 0.16 | 0.95 ± 0.01 | 15.95 ± 0.02 | 15.92 ± 0.02 | 15.81 ± 0.01 | 15.98 ± 0.02 | 16.53 ± 0.02 | 1119.30 ± 0.25 | 0.97 ± 0.02 | 0.05 ± 0.02 | 34.89 ± 0.04 | C0 |
| 2018gl | 1138.94 ± 0.04 | 0.64 ± 0.01 | 16.32 ± 0.01 | 16.39 ± 0.02 | 16.14 ± 0.01 | 16.23 ± 0.01 | 16.60 ± 0.01 | 1138.95 ± 0.04 | 0.64 ± 0.01 | −0.01 ± 0.01 | 34.73 ± 0.01 | C0 |
| 2018gv | 1150.38 ± 0.04 | 1.04 ± 0.01 | 12.92 ± 0.01 | ⋯ | 12.89 ± 0.01 | 13.01 ± 0.01 | 13.58 ± 0.01 | 1150.37 ± 0.04 | 1.04 ± 0.01 | −0.01 ± 0.01 | 32.07 ± 0.01 | C0 |
| 2018kp | 1160.40 ± 0.08 | 0.95 ± 0.01 | 16.73 ± 0.02 | 16.55 ± 0.02 | 16.05 ± 0.01 | 15.84 ± 0.01 | 16.18 ± 0.01 | 1160.42 ± 0.10 | 0.94 ± 0.01 | 0.68 ± 0.01 | 33.90 ± 0.02 | C0 |
| 2018pv | 1164.77 ± 0.05 | 0.51 ± 0.01 | 13.28 ± 0.02 | 12.99 ± 0.01 | 12.65 ± 0.02 | 12.55 ± 0.02 | 12.90 ± 0.02 | 1164.58 ± 0.15 | 0.52 ± 0.02 | 0.26 ± 0.04 | 30.49 ± 0.05 | C0 |
| 2018pc | 1165.23 ± 0.05 | 0.85 ± 0.01 | 15.44 ± 0.02 | 15.34 ± 0.01 | 15.05 ± 0.01 | 14.98 ± 0.01 | 15.28 ± 0.01 | 1165.22 ± 0.06 | 0.86 ± 0.01 | 0.44 ± 0.01 | 33.31 ± 0.02 | C0 |
| 2018oh | 1163.33 ± 0.05 | 1.01 ± 0.01 | 14.31 ± 0.01 | 14.43 ± 0.01 | 14.31 ± 0.01 | 14.46 ± 0.01 | 15.02 ± 0.01 | 1163.24 ± 0.05 | 1.03 ± 0.01 | −0.03 ± 0.01 | 33.57 ± 0.01 | C0 |
| 2018vw | 1178.03 ± 0.12 | 1.13 ± 0.02 | 15.39 ± 0.01 | 15.48 ± 0.02 | 15.42 ± 0.01 | 15.64 ± 0.02 | 16.27 ± 0.02 | 1178.14 ± 0.13 | 1.13 ± 0.02 | −0.11 ± 0.01 | 34.93 ± 0.03 | C0 |
| 2018xx | 1184.91 ± 0.07 | 0.80 ± 0.01 | 14.51 ± 0.02 | 14.58 ± 0.01 | 14.43 ± 0.02 | 14.50 ± 0.02 | 15.00 ± 0.02 | 1184.83 ± 0.06 | 0.81 ± 0.01 | −0.03 ± 0.01 | 33.25 ± 0.02 | C0 |
| 2018yu | 1195.24 ± 0.04 | 0.98 ± 0.01 | 14.02 ± 0.01 | 14.06 ± 0.01 | 13.95 ± 0.01 | 14.05 ± 0.02 | 14.50 ± 0.01 | 1195.06 ± 0.05 | 0.99 ± 0.01 | −0.02 ± 0.01 | 32.85 ± 0.01 | C0 |
| 2018zz | 1190.72 ± 0.07 | 0.65 ± 0.01 | 15.15 ± 0.02 | 14.99 ± 0.01 | 14.95 ± 0.01 | 14.98 ± 0.01 | 15.39 ± 0.02 | 1190.83 ± 0.08 | 0.64 ± 0.01 | −0.0 ± 0.02 | 33.44 ± 0.02 | C0 |
| 2018apo | 1223.02 ± 0.14 | 1.09 ± 0.03 | 15.52 ± 0.03 | 15.54 ± 0.01 | 15.27 ± 0.03 | 15.34 ± 0.03 | 15.75 ± 0.03 | 1223.08 ± 0.15 | 1.20 ± 0.03 | 0.12 ± 0.02 | 34.11 ± 0.04 | C0 |
| 2018aoz | 1222.91 ± 0.03 | 0.83 ± 0.01 | 12.90 ± 0.01 | 12.93 ± 0.01 | 12.87 ± 0.01 | 12.97 ± 0.01 | 13.55 ± 0.02 | 1222.94 ± 0.05 | 0.82 ± 0.01 | −0.09 ± 0.01 | 31.87 ± 0.02 | C0 |
| 2018aqi | 1223.06 ± 0.11 | 0.78 ± 0.01 | 15.77 ± 0.03 | 15.72 ± 0.02 | 15.53 ± 0.02 | 15.57 ± 0.02 | 16.08 ± 0.04 | 1223.06 ± 0.12 | 0.80 ± 0.01 | 0.12 ± 0.02 | 34.17 ± 0.03 | C0 |
| 2018ast | 1214.52 ± 0.75 | 0.38 ± 0.02 | 17.36 ± 0.08 | 17.17 ± 0.07 | 16.33 ± 0.06 | 16.43 ± 0.05 | 16.41 ± 0.07 | 1214.82 ± 0.53 | 0.40 ± 0.02 | 0.21 ± 0.04 | 34.00 ± 0.06 | C0 |
| 2018aye | 1243.85 ± 0.01 | 1.06 ± 0.01 | 15.76 ± 0.01 | 15.90 ± 0.01 | 15.72 ± 0.01 | 15.88 ± 0.01 | 16.49 ± 0.01 | 1243.74 ± 0.09 | 1.07 ± 0.01 | −0.04 ± 0.01 | 35.03 ± 0.02 | C0 |
| 2018big | 1265.40 ± 0.08 | 1.11 ± 0.02 | 15.98 ± 0.01 | 15.95 ± 0.02 | 15.79 ± 0.01 | 15.83 ± 0.01 | 16.39 ± 0.01 | 1265.28 ± 0.09 | 1.14 ± 0.02 | 0.15 ± 0.01 | 34.77 ± 0.02 | C0 |
| 2018brz | 1259.95 ± 0.36 | 1.08 ± 0.06 | 16.50 ± 0.05 | 16.37 ± 0.04 | 16.14 ± 0.07 | 16.14 ± 0.05 | 16.60 ± 0.09 | 1257.68 ± 0.98 | 1.26 ± 0.04 | 0.03 ± 0.05 | 34.98 ± 0.05 | C0 |
| 2018bta | 1267.66 ± 0.32 | 0.95 ± 0.01 | 15.79 ± 0.02 | 16.13 ± 0.13 | 15.43 ± 0.02 | 15.39 ± 0.02 | 15.72 ± 0.02 | 1267.55 ± 0.29 | 0.94 ± 0.02 | 0.30 ± 0.02 | 33.69 ± 0.04 | C0 |
| 2018cnj | 1277.96 ± 0.75 | 0.90 ± 0.02 | 17.78 ± 0.07 | 17.46 ± 0.14 | 17.16 ± 0.05 | 16.85 ± 0.03 | 16.93 ± 0.06 | 1277.95 ± 0.32 | 0.90 ± 0.01 | 0.45 ± 0.02 | 34.30 ± 0.02 | C0 |
| 2018chl | 1272.67 ± 0.98 | 0.25 ± 0.03 | 18.01 ± 0.16 | 17.36 ± 0.11 | 17.06 ± 0.09 | 17.12 ± 0.04 | 17.14 ± 0.08 | 1273.49 ± 0.64 | 0.27 ± 0.04 | −0.01 ± 0.16 | 34.31 ± 0.07 | C0 |
| 2018cqj | 1294.53 ± 0.28 | 0.62 ± 0.05 | 16.54 ± 0.07 | 16.53 ± 0.05 | 16.16 ± 0.05 | 16.13 ± 0.04 | 16.56 ± 0.09 | 1294.22 ± 0.37 | 0.66 ± 0.03 | 0.20 ± 0.05 | 34.42 ± 0.04 | C0 |
| 2018cqw | 1301.01 ± 0.04 | 0.96 ± 0.01 | 14.57 ± 0.01 | 14.56 ± 0.01 | 14.40 ± 0.01 | 14.46 ± 0.01 | 14.96 ± 0.01 | 1301.00 ± 0.04 | 0.96 ± 0.01 | 0.03 ± 0.01 | 33.21 ± 0.01 | C0 |
| 2018ctv | 1294.41 ± 0.14 | 0.44 ± 0.01 | 17.45 ± 0.02 | 17.06 ± 0.05 | 16.67 ± 0.02 | 16.68 ± 0.02 | 16.85 ± 0.02 | 1294.31 ± 0.18 | 0.44 ± 0.02 | 0.20 ± 0.03 | 34.34 ± 0.04 | C0 |
| 2018cuh | 1305.29 ± 0.08 | 0.93 ± 0.01 | 15.06 ± 0.01 | 15.12 ± 0.01 | 15.03 ± 0.01 | 15.13 ± 0.01 | 15.71 ± 0.02 | 1305.24 ± 0.11 | 0.93 ± 0.01 | −0.04 ± 0.01 | 34.09 ± 0.02 | C0 |
| 2018cuw | 1305.15 ± 2.29 | 1.35 ± 0.24 | ⋯ | 16.54 ± 0.08 | 16.55 ± 0.06 | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | ⋯ | C1 |
| 2018dda | 1313.75 ± 0.14 | 1.01 ± 0.02 | 15.59 ± 0.03 | 15.73 ± 0.02 | 15.22 ± 0.02 | 15.30 ± 0.02 | 15.71 ± 0.03 | 1313.03 ± 0.17 | 1.07 ± 0.02 | 0.27 ± 0.02 | 34.00 ± 0.03 | C0 |
| 2018eay | 1328.67 ± 0.11 | 1.17 ± 0.02 | 17.51 ± 0.01 | 17.11 ± 0.09 | 16.67 ± 0.01 | 16.51 ± 0.01 | 16.62 ± 0.01 | 1328.72 ± 0.15 | 1.13 ± 0.02 | 0.80 ± 0.02 | 34.34 ± 0.03 | C0 |
| 2018ebk | 1330.24 ± 0.07 | 0.91 ± 0.01 | 16.92 ± 0.01 | 16.36 ± 0.03 | 16.26 ± 0.01 | 16.08 ± 0.01 | 16.32 ± 0.01 | 1330.25 ± 0.05 | 0.90 ± 0.01 | 0.25 ± 0.01 | 33.79 ± 0.01 | C0 |
| 2018enc | 1345.05 ± 0.12 | 1.11 ± 0.03 | 16.07 ± 0.02 | 16.04 ± 0.03 | 15.95 ± 0.02 | 16.05 ± 0.02 | 16.67 ± 0.02 | 1344.89 ± 0.15 | 1.14 ± 0.03 | −0.05 ± 0.02 | 35.08 ± 0.04 | C0 |
| 2018eov | 1341.00 ± 0.18 | 1.19 ± 0.02 | 15.68 ± 0.02 | 16.00 ± 0.03 | 15.42 ± 0.02 | 15.47 ± 0.02 | 15.93 ± 0.02 | 1340.97 ± 0.19 | 1.19 ± 0.02 | 0.01 ± 0.02 | 34.16 ± 0.03 | C0 |
| 2018eqq | 1339.71 ± 0.19 | 1.06 ± 0.01 | 15.49 ± 0.02 | 15.58 ± 0.03 | 15.30 ± 0.01 | 15.40 ± 0.01 | 15.94 ± 0.01 | 1339.48 ± 0.23 | 1.08 ± 0.02 | −0.0 ± 0.01 | 34.26 ± 0.02 | C0 |
| 2018feb | 1363.01 ± 0.04 | 0.96 ± 0.01 | 15.31 ± 0.01 | 15.39 ± 0.01 | 15.21 ± 0.01 | 15.28 ± 0.01 | 15.82 ± 0.01 | 1363.02 ± 0.04 | 0.96 ± 0.01 | 0.07 ± 0.01 | 34.16 ± 0.01 | C0 |
| 2018fhw | 1357.95 ± 0.08 | 0.52 ± 0.01 | 16.70 ± 0.01 | 16.68 ± 0.06 | 16.36 ± 0.01 | 16.31 ± 0.01 | 16.65 ± 0.01 | 1357.93 ± 0.08 | 0.51 ± 0.01 | 0.04 ± 0.02 | 34.50 ± 0.02 | C0 |
| 2018fop | 1366.21 ± 0.23 | 1.06 ± 0.02 | 15.61 ± 0.03 | 15.73 ± 0.02 | 15.54 ± 0.02 | 15.65 ± 0.02 | 16.28 ± 0.03 | 1365.77 ± 0.05 | 1.13 ± 0.02 | −0.04 ± 0.02 | 34.79 ± 0.03 | C0 |
| 2018fpm | 1356.36 ± 0.32 | 0.95 ± 0.03 | 17.81 ± 0.09 | 17.02 ± 0.04 | 16.40 ± 0.05 | 15.91 ± 0.04 | 15.83 ± 0.07 | 1355.18 ± 0.36 | 0.96 ± 0.01 | 1.41 ± 0.02 | 32.88 ± 0.03 | C0 |
| 2018fnq | 1372.94 ± 0.18 | 1.10 ± 0.03 | 15.78 ± 0.03 | 15.88 ± 0.02 | 15.68 ± 0.02 | 15.80 ± 0.02 | 16.31 ± 0.03 | 1373.62 ± 0.19 | 1.08 ± 0.02 | 0.07 ± 0.01 | 34.77 ± 0.03 | C0 |
| 2018fuk | 1377.41 ± 0.13 | 0.92 ± 0.01 | 15.91 ± 0.01 | 15.92 ± 0.02 | 15.71 ± 0.01 | 15.72 ± 0.01 | 16.23 ± 0.02 | 1377.39 ± 0.14 | 0.92 ± 0.01 | 0.13 ± 0.01 | 34.40 ± 0.02 | C0 |
| 2018ghb | 1382.68 ± 0.12 | 0.62 ± 0.01 | 14.83 ± 0.02 | 14.72 ± 0.02 | 14.44 ± 0.02 | 14.46 ± 0.02 | 14.81 ± 0.02 | 1382.69 ± 0.11 | 0.65 ± 0.01 | 0.09 ± 0.01 | 32.64 ± 0.02 | C0 |
| 2018htw | 1416.60 ± 0.53 | 0.89 ± 0.04 | 16.03 ± 0.26 | 16.05 ± 0.04 | 15.85 ± 0.04 | 15.76 ± 0.19 | 16.35 ± 0.13 | 1416.38 ± 0.55 | 0.88 ± 0.03 | 0.20 ± 0.06 | 34.29 ± 0.17 | C3 |
| 2018hib | 1415.33 ± 0.07 | 0.89 ± 0.01 | 15.27 ± 0.01 | 15.31 ± 0.01 | 15.19 ± 0.01 | 15.26 ± 0.01 | 15.67 ± 0.02 | 1415.31 ± 0.12 | 0.90 ± 0.01 | 0.12 ± 0.01 | 34.09 ± 0.03 | C0 |
| 2018hkq | 1414.24 ± 0.39 | 0.91 ± 0.03 | 15.67 ± 0.08 | 15.56 ± 0.03 | 15.36 ± 0.06 | 15.40 ± 0.06 | 16.26 ± 0.09 | 1412.89 ± 0.59 | 1.14 ± 0.12 | 0.02 ± 0.08 | 34.82 ± 0.18 | C0 |
| 2018hme | 1413.61 ± 0.41 | 0.77 ± 0.03 | 15.90 ± 0.09 | 15.85 ± 0.02 | 15.52 ± 0.05 | 15.57 ± 0.04 | 15.99 ± 0.09 | 1413.54 ± 0.81 | 0.76 ± 0.02 | 0.13 ± 0.03 | 34.00 ± 0.05 | C0 |
| 2018htt | 1439.63 ± 0.08 | 0.73 ± 0.01 | 14.01 ± 0.02 | 13.98 ± 0.01 | 13.96 ± 0.02 | 14.10 ± 0.02 | 14.62 ± 0.02 | 1439.28 ± 0.14 | 0.73 ± 0.01 | −0.10 ± 0.03 | 32.96 ± 0.03 | C0 |
| 2018hrt | 1431.88 ± 0.24 | 0.88 ± 0.01 | 18.20 ± 0.07 | 17.87 ± 0.09 | 17.28 ± 0.02 | 16.88 ± 0.02 | 16.98 ± 0.02 | 1431.81 ± 0.24 | 0.88 ± 0.01 | 0.88 ± 0.03 | 34.27 ± 0.04 | C0 |
| 2018hsa | 1432.18 ± 0.12 | 0.97 ± 0.01 | 15.82 ± 0.02 | 15.79 ± 0.01 | 15.60 ± 0.01 | 15.63 ± 0.02 | 16.06 ± 0.03 | 1432.17 ± 0.22 | 0.97 ± 0.02 | 0.23 ± 0.01 | 34.30 ± 0.03 | C0 |
| 2018ilu | 1450.35 ± 0.16 | 1.09 ± 0.02 | 15.48 ± 0.01 | 15.46 ± 0.01 | 15.35 ± 0.01 | 15.48 ± 0.01 | 16.10 ± 0.01 | 1449.71 ± 0.18 | 1.13 ± 0.02 | −0.01 ± 0.01 | 34.56 ± 0.02 | C0 |
| 2018imd | 1405.57 ± 0.89 | 1.19 ± 0.05 | 13.84 ± 0.05 | ⋯ | 13.91 ± 0.05 | 14.61 ± 0.05 | 14.52 ± 0.11 | 1405.00 ± 0.00 | 0.90 ± 0.07 | −0.07 ± 0.04 | 32.82 ± 0.24 | C3 |
| 2018isq | 1449.62 ± 0.57 | 0.42 ± 0.01 | 16.93 ± 0.02 | 16.53 ± 0.07 | 15.94 ± 0.01 | 15.84 ± 0.02 | 15.97 ± 0.02 | 1449.80 ± 0.17 | 0.39 ± 0.02 | 0.16 ± 0.04 | 33.02 ± 0.04 | C0 |
| 2018iuu | 1459.32 ± 0.09 | 0.94 ± 0.01 | 15.50 ± 0.01 | 15.40 ± 0.02 | 15.39 ± 0.01 | 15.53 ± 0.01 | 16.12 ± 0.02 | 1459.14 ± 0.11 | 0.95 ± 0.01 | 0.05 ± 0.01 | 34.52 ± 0.02 | C0 |
| 2018jaj | 1463.13 ± 0.55 | 1.07 ± 0.01 | 15.53 ± 0.01 | 15.53 ± 0.04 | 15.44 ± 0.01 | 15.56 ± 0.01 | 16.26 ± 0.01 | 1463.05 ± 0.12 | 1.09 ± 0.02 | 0.01 ± 0.01 | 34.73 ± 0.03 | C0 |
| 2018jeo | 1455.03 ± 0.15 | 1.04 ± 0.01 | 16.13 ± 0.01 | 16.10 ± 0.01 | 15.91 ± 0.01 | 15.95 ± 0.01 | 16.41 ± 0.01 | 1454.86 ± 0.15 | 1.05 ± 0.01 | 0.04 ± 0.01 | 34.60 ± 0.02 | C0 |
| 2018jjd | 1470.29 ± 0.15 | 1.15 ± 0.03 | 15.79 ± 0.03 | 15.78 ± 0.02 | 15.84 ± 0.02 | 15.97 ± 0.02 | 16.59 ± 0.02 | 1470.34 ± 0.11 | 1.14 ± 0.02 | −0.09 ± 0.01 | 35.24 ± 0.02 | C0 |
| 2018jky | 1469.66 ± 0.05 | 0.71 ± 0.01 | 15.47 ± 0.02 | 15.57 ± 0.01 | 15.33 ± 0.01 | 15.38 ± 0.01 | 15.80 ± 0.02 | 1469.72 ± 0.04 | 0.71 ± 0.01 | 0.03 ± 0.01 | 34.00 ± 0.02 | C0 |
| 2018jmo | 1474.05 ± 0.03 | 0.78 ± 0.01 | 16.89 ± 0.02 | 16.83 ± 0.04 | 16.51 ± 0.02 | 16.51 ± 0.01 | 16.97 ± 0.02 | 1473.58 ± 0.35 | 0.79 ± 0.02 | 0.19 ± 0.02 | 34.91 ± 0.03 | C0 |
| 2018jov | 1475.38 ± 0.05 | 1.00 ± 0.01 | 16.26 ± 0.01 | 16.26 ± 0.03 | 16.06 ± 0.01 | 16.09 ± 0.01 | 16.62 ± 0.01 | 1475.39 ± 0.06 | 1.01 ± 0.01 | 0.17 ± 0.01 | 34.88 ± 0.02 | C0 |
| 2018jwi | 1479.57 ± 0.07 | 0.93 ± 0.01 | 15.07 ± 0.01 | 15.11 ± 0.01 | 15.02 ± 0.01 | 15.09 ± 0.01 | 15.59 ± 0.02 | 1479.60 ± 0.07 | 0.94 ± 0.01 | 0.03 ± 0.01 | 33.99 ± 0.01 | C0 |
| 2018kmu | 1481.73 ± 0.29 | 1.27 ± 0.02 | 16.46 ± 0.03 | 16.34 ± 0.03 | 16.34 ± 0.02 | 16.47 ± 0.02 | 17.18 ± 0.02 | 1481.36 ± 0.41 | 1.29 ± 0.03 | −0.10 ± 0.02 | 35.78 ± 0.04 | C0 |
| 2019np | 1510.61 ± 0.03 | 0.99 ± 0.01 | 13.48 ± 0.01 | 13.45 ± 0.01 | 13.38 ± 0.01 | 13.49 ± 0.01 | 14.00 ± 0.01 | 1510.47 ± 0.05 | 1.00 ± 0.01 | 0.10 ± 0.01 | 32.44 ± 0.01 | C0 |
| 2019so | 1507.35 ± 0.07 | 0.41 ± 0.01 | 17.24 ± 0.02 | 16.80 ± 0.03 | 16.66 ± 0.01 | 16.63 ± 0.01 | 16.84 ± 0.03 | 1507.24 ± 0.08 | 0.43 ± 0.01 | −0.01 ± 0.02 | 34.36 ± 0.03 | C0 |
| J140216 b | 1512.90 ± 0.15 | 1.21 ± 0.01 | 17.01 ± 0.01 | 16.90 ± 0.02 | 16.23 ± 0.01 | 16.05 ± 0.01 | 16.09 ± 0.01 | 1513.20 ± 0.15 | 1.13 ± 0.02 | 0.41 ± 0.01 | 33.52 ± 0.03 | C0 |
| 2019gbx | 1647.78 ± 0.05 | 0.83 ± 0.01 | 14.83 ± 0.01 | 14.92 ± 0.01 | 14.82 ± 0.01 | 14.94 ± 0.01 | 15.47 ± 0.01 | 1647.85 ± 0.05 | 0.82 ± 0.01 | −0.07 ± 0.01 | 33.88 ± 0.02 | C0 |
| 2019hxc | 1663.67 ± 0.26 | 1.00 ± 0.02 | 16.77 ± 0.03 | 16.63 ± 0.04 | 16.44 ± 0.03 | 16.37 ± 0.02 | 16.95 ± 0.03 | 1662.40 ± 0.28 | 1.19 ± 0.03 | 0.26 ± 0.03 | 35.17 ± 0.05 | C0 |
| 2019knt | 1683.81 ± 0.12 | 1.07 ± 0.03 | 14.90 ± 0.03 | 14.93 ± 0.02 | 14.87 ± 0.02 | 14.97 ± 0.02 | 15.51 ± 0.03 | 1683.30 ± 0.06 | 1.14 ± 0.01 | −0.02 ± 0.01 | 34.04 ± 0.02 | C0 |
| 2019khf | 1680.76 ± 0.11 | 1.00 ± 0.01 | 15.29 ± 0.02 | 15.32 ± 0.01 | 15.15 ± 0.02 | 15.19 ± 0.02 | 15.84 ± 0.03 | 1680.89 ± 0.12 | 1.02 ± 0.02 | 0.04 ± 0.02 | 34.12 ± 0.04 | C0 |
| 2019ltt | 1687.43 ± 0.24 | 1.16 ± 0.01 | 15.93 ± 0.02 | ⋯ | 15.66 ± 0.01 | 15.77 ± 0.01 | 16.25 ± 0.02 | 1687.59 ± 0.31 | 1.14 ± 0.02 | 0.02 ± 0.02 | 34.48 ± 0.03 | C0 |
| 2019swh | 1745.65 ± 0.25 | 0.87 ± 0.02 | 15.15 ± 0.05 | 15.33 ± 0.02 | 14.86 ± 0.04 | 14.87 ± 0.04 | 15.40 ± 0.06 | 1745.45 ± 0.32 | 0.89 ± 0.03 | 0.21 ± 0.04 | 33.19 ± 0.13 | C0 |
| 2020ue | 1873.75 ± 0.49 | 0.75 ± 0.01 | 12.21 ± 0.01 | 12.15 ± 0.03 | 12.18 ± 0.01 | 12.28 ± 0.01 | 12.75 ± 0.01 | 1873.73 ± 0.03 | 0.73 ± 0.01 | −0.06 ± 0.01 | 31.09 ± 0.01 | C0 |
Notes.
C0: Good data coverage and fitting results.
C1: Only ASAS-SN V-band data are available. SNooPy EBV_model2 fitting is not feasible due to lack of multicolor coverage to derive host extinction. max_model fitting has been performed, yielding reasonable results of the peak times and magnitudes, although the derived s BV should be used with caution.
C2: Only a small number (≲3) of epochs with available multiband data. Some of the SNe only have multiband light curves close to the B-band peak, which makes it challenging to derive the decline rate (or the light-curve width). Similarly with C1, max_model fitting gives credible results of peak times and magnitudes, while the s BV parameters should be used with caution. EBV_model2 fitting is performed for these targets, but the fitting results have large uncertainties owing to inadequate coverage.
C3: The first available multiband data point obtained ≳30 d after the estimated B-band peak. The light-curve parameters from both max_model and EBV_model2 should be used with caution.
C4: Decent light-curve coverage, but poorly fit by SNooPy templates. Therefore, the best-fit parameters, especially those from EBV_model2, should not be trusted.
a The SN name adopts the IAU name when available, otherwise the survey name. All the IAU and survey names are available in Table 1. b These names are used for brevity, the same as in Table 1. c As explained below, the SNe are categorized into different groups according to their data coverage in terms of both wavelength and phase, and how well they are fitted by the template light curves.A machine-readable version of the table is available.
We also fit the data using SNooPy's "EBV_model2", which can derive host-galaxy extinctions. The EBV_model2 method fit the light curves with the templates as described below,
where mX
is the observed magnitude in band X, TX
(ϕ, sBV
) is the template light curve as a function of rest-frame phase ϕ, and s
BV
, MX
(sBV
) is the peak absolute magnitude of the given s
BV
, μ is the distance modulus in magnitudes, KXY
is the cross-band k-correction from Y band to the observed X band, E(B − V)gal and E(B − V)host are galactic and host-galaxy color excess due to extinction, and 
and 
are the ratios of total to selective extinction for the Milky Way and the host galaxy, respectively. Among the parameters listed above, MX
(sBV
), KXY
, 
, 
, 
are predetermined and provided by SNooPy, and tpeak(B), s
BV
, 
, and μ are free parameters in the fitting. 
is obtained from the results of Schlafly & Finkbeiner (2011), and the canonical 
is adopted for the Milky Way. SNooPy has different sets of calibration results of the peak luminosity of SNe Ia, and we adopt 
(corresponding to calibration = 5 in SNooPy), which is the result of calibration by using SNe Ia covering the full range of s
BV
(Burns et al. 2014). Our data set generally has the best coverage in BVri, and light curves in these bands are used in the EBV_model2 fitting for all objects, except for four objects (2018hkq, 2018htw, 2018kmu, and 2019swh). When the g-band light curves provide coverage missed by other bands, they are also used in the fitting. We obtain the best-fit parameters (tpeak(B), s
BV
, 
, and μ) for 212 SNe Ia, and they are listed in the EBV_model2 section of Table 4.
We also perform model-independent fitting to the well-covered SN Ia light curves to directly derive parameters including the times and magnitudes of peak brightness and the decline rates in the B and V bands. The decline rate Δm15(X) (Phillips 1993) refers to the magnitude decline within 15 days after peak brightness in a given filter X. We measure these parameters directly from the interpolated light curves in B and V band using a Gaussian process regression method, which has the advantage of allowing for the inclusion of uncertainty information and producing relatively unbiased estimates of interpolated values (see, e.g., Lochner et al. 2016). The results are given in Table 5. Note that the fitting is performed without making host-galaxy extinction corrections, which may affect the derived Δm15 for objects with high extinction (Phillips et al. 1999).
Table 5. Light-curve Parameters from Gaussian Process Fitting
| SN a |
| Bpeak | Δm15(B) |
| Vpeak | Δm15(V) |
|---|---|---|---|---|---|---|
| −2,457,000 | (mag) | (mag) | −2,457,000 | (mag) | (mag) | |
| ASASSN-15aj | ⋯ | ⋯ | ⋯ | 37.9 ± 0.5 | 14.76 ± 0.02 | 0.93 ± 0.07 |
| ASASSN-15db | ⋯ | ⋯ | ⋯ | 77.0 ± 0.3 | 14.51 ± 0.02 | 0.83 ± 0.06 |
| 2015F | ⋯ | ⋯ | ⋯ | 108.4 ± 0.6 | 13.33 ± 0.02 | 0.74 ± 0.04 |
| 2015bp | ⋯ | ⋯ | ⋯ | 112.7 ± 0.3 | 13.90 ± 0.01 | 0.82 ± 0.03 |
| ASASSN-15hf | ⋯ | ⋯ | ⋯ | 138.9 ± 0.5 | 14.26 ± 0.02 | 0.68 ± 0.05 |
| ASASSN-15hx | 151.5 ± 0.2 | 13.29 ± 0.01 | ⋯ | 153.1 ± 0.5 | 13.37 ± 0.01 | 0.63 ± 0.04 |
| ASASSN-15jo | 169.0 ± 0.7 | 15.69 ± 0.02 | 1.87 ± 0.09 | ⋯ | ⋯ | ⋯ |
| ASASSN-15kp | 188.5 ± 1.2 | 15.52 ± 0.03 | 0.90 ± 0.13 | 188.9 ± 1.7 | 15.53 ± 0.05 | 0.51 ± 0.09 |
| ASASSN-15pl | ⋯ | ⋯ | ⋯ | 290.5 ± 0.9 | 15.16 ± 0.03 | 0.73 ± 0.06 |
| ASASSN-15pz | 307.2 ± 0.6 | 14.24 ± 0.02 | 0.67 ± 0.06 | 307.2 ± 0.6 | 14.26 ± 0.01 | 0.39 ± 0.04 |
| ASASSN-15qc | 299.4 ± 0.7 | 15.86 ± 0.02 | 1.01 ± 0.08 | 303.4 ± 0.5 | 15.60 ± 0.01 | 0.72 ± 0.03 |
| 2015ao | 307.4 ± 0.6 | 17.52 ± 0.03 | 1.84 ± 0.16 | 310.2 ± 0.2 | 16.87 ± 0.02 | 1.49 ± 0.06 |
| ASASSN-15rq | 324.9 ± 0.3 | 15.45 ± 0.01 | 0.93 ± 0.05 | 326.1 ± 0.4 | 15.46 ± 0.01 | 0.61 ± 0.04 |
| ASASSN-15rw | 330.7 ± 0.8 | 15.65 ± 0.05 | 1.00 ± 0.14 | 332.0 ± 0.9 | 15.59 ± 0.04 | 0.62 ± 0.08 |
| 2015ar | 351.1 ± 1.2 | 15.45 ± 0.04 | 1.25 ± 0.16 | 354.3 ± 0.6 | 15.28 ± 0.03 | 0.93 ± 0.07 |
| PSN J21505094-7020289 | 360.4 ± 0.5 | 15.56 ± 0.03 | 1.39 ± 0.07 | 362.1 ± 0.4 | 15.17 ± 0.02 | 0.81 ± 0.03 |
| ASASSN-15ti | 365.2 ± 0.8 | 16.26 ± 0.06 | 1.53 ± 0.12 | ⋯ | ⋯ | ⋯ |
| 2015bd | ⋯ | ⋯ | ⋯ | 348.5 ± 0.7 | 15.19 ± 0.02 | 0.65 ± 0.05 |
| ASASSN-15uh | 387.0 ± 1.4 | 15.57 ± 0.07 | 0.85 ± 0.19 | 389.3 ± 1.4 | 15.24 ± 0.06 | 0.57 ± 0.16 |
| ASASSN-15ut | ⋯ | ⋯ | ⋯ | 392.4 ± 0.5 | 16.32 ± 0.03 | 1.03 ± 0.17 |
| 2016bfu | 471.0 ± 0.4 | 16.21 ± 0.03 | 1.91 ± 0.09 | 473.1 ± 0.4 | 15.63 ± 0.03 | 1.24 ± 0.04 |
| 2016blc | 490.1 ± 0.9 | 14.71 ± 0.03 | 0.96 ± 0.10 | 491.0 ± 0.8 | 14.74 ± 0.03 | 0.64 ± 0.06 |
| 2016bln | ⋯ | ⋯ | ⋯ | 502.0 ± 0.8 | 16.01 ± 0.04 | 0.67 ± 0.08 |
| 2016cbx | 513.4 ± 1.3 | 16.69 ± 0.06 | 0.92 ± 0.19 | 516.1 ± 1.0 | 16.52 ± 0.06 | 0.74 ± 0.10 |
| 2016ccz | ⋯ | ⋯ | ⋯ | 540.5 ± 0.5 | 15.44 ± 0.03 | 0.79 ± 0.07 |
| 2016coj | ⋯ | ⋯ | ⋯ | 549.7 ± 0.3 | 13.01 ± 0.01 | 0.70 ± 0.02 |
| 2016daj | 593.1 ± 1.0 | 16.58 ± 0.07 | 1.12 ± 0.14 | 593.6 ± 1.6 | 16.57 ± 0.05 | 0.67 ± 0.13 |
| 2016ekg | 610.3 ± 0.3 | 15.03 ± 0.03 | 1.12 ± 0.07 | 611.3 ± 0.5 | 15.07 ± 0.02 | 0.66 ± 0.05 |
| 2016ekt | 602.0 ± 1.2 | 14.77 ± 0.02 | 0.81 ± 0.11 | 605.0 ± 0.2 | 14.72 ± 0.01 | 0.66 ± 0.02 |
| 2016euj | 619.7 ± 0.3 | 15.35 ± 0.02 | 1.39 ± 0.05 | 620.5 ± 0.3 | 15.33 ± 0.01 | 0.82 ± 0.03 |
| 2016fej | 636.1 ± 0.4 | 13.90 ± 0.02 | 0.93 ± 0.06 | 638.0 ± 0.5 | 13.93 ± 0.02 | 0.62 ± 0.04 |
| 2016fff | 630.3 ± 0.3 | 15.03 ± 0.02 | 1.77 ± 0.06 | 632.1 ± 0.3 | 14.90 ± 0.02 | 0.98 ± 0.05 |
| 2016fob | ⋯ | ⋯ | ⋯ | 633.5 ± 1.3 | 16.15 ± 0.02 | 0.62 ± 0.07 |
| 2016gfk | ⋯ | ⋯ | ⋯ | 646.9 ± 0.9 | 16.77 ± 0.03 | 0.84 ± 0.08 |
| 2016gsb | 672.1 ± 0.5 | 14.52 ± 0.03 | 1.13 ± 0.08 | 674.4 ± 0.6 | 14.45 ± 0.03 | 0.66 ± 0.06 |
| 2016gsn | 672.3 ± 0.5 | 15.25 ± 0.02 | 1.09 ± 0.06 | 672.9 ± 0.3 | 15.08 ± 0.01 | 0.68 ± 0.03 |
| 2016gtr | 667.1 ± 1.4 | 15.61 ± 0.02 | 0.89 ± 0.12 | 670.8 ± 0.6 | 15.58 ± 0.02 | 0.69 ± 0.06 |
| 2016gxp | 685.7 ± 0.6 | 15.10 ± 0.02 | 1.07 ± 0.07 | 688.5 ± 0.8 | 14.87 ± 0.02 | 0.61 ± 0.06 |
| 2016hli | 696.3 ± 0.5 | 17.47 ± 0.03 | 1.58 ± 0.08 | 698.0 ± 0.7 | 16.82 ± 0.03 | 0.87 ± 0.06 |
| 2016hpw | 703.4 ± 0.3 | 16.02 ± 0.02 | 1.04 ± 0.04 | 705.3 ± 0.3 | 15.97 ± 0.01 | 0.70 ± 0.03 |
| 2016hvl | 710.9 ± 0.6 | 15.95 ± 0.04 | 1.17 ± 0.07 | 714.0 ± 0.9 | 15.49 ± 0.03 | 0.67 ± 0.05 |
| 2016huh | ⋯ | ⋯ | ⋯ | 700.4 ± 1.0 | 16.86 ± 0.03 | 0.78 ± 0.09 |
| 2016igr | 726.9 ± 0.4 | 15.31 ± 0.02 | 1.16 ± 0.05 | 728.1 ± 0.5 | 15.32 ± 0.02 | 0.69 ± 0.04 |
| 2016ins | 724.1 ± 0.8 | 16.89 ± 0.03 | 1.50 ± 0.23 | 725.4 ± 0.9 | 16.58 ± 0.02 | 0.89 ± 0.09 |
| 2016ipf | 728.0 ± 0.5 | 16.76 ± 0.02 | 1.35 ± 0.08 | 727.9 ± 1.2 | 16.74 ± 0.03 | 0.65 ± 0.08 |
| 2016jab | 749.5 ± 0.8 | 16.06 ± 0.02 | 0.93 ± 0.08 | 751.5 ± 0.5 | 15.97 ± 0.02 | 0.64 ± 0.04 |
| 2017jl | 784.9 ± 0.3 | 15.01 ± 0.02 | 0.99 ± 0.06 | 786.6 ± 0.4 | 14.94 ± 0.02 | 0.63 ± 0.06 |
| 2017yv | 795.7 ± 0.6 | 15.74 ± 0.04 | 1.15 ± 0.09 | 797.2 ± 0.6 | 15.59 ± 0.04 | 0.72 ± 0.07 |
| 2017awk | 808.4 ± 0.5 | 16.03 ± 0.02 | 1.22 ± 0.06 | 810.5 ± 0.6 | 15.79 ± 0.02 | 0.73 ± 0.05 |
| 2017azw | 817.4 ± 0.5 | 14.99 ± 0.02 | 0.94 ± 0.07 | 817.7 ± 0.4 | 14.95 ± 0.02 | 0.65 ± 0.04 |
| 2017bkc | ⋯ | ⋯ | ⋯ | 813.3 ± 1.0 | 16.66 ± 0.02 | 0.57 ± 0.08 |
| 2017cav | ⋯ | ⋯ | ⋯ | 820.2 ± 1.6 | 16.32 ± 0.02 | 0.53 ± 0.09 |
| 2017cbr | 834.7 ± 0.4 | 15.96 ± 0.02 | 1.31 ± 0.07 | 836.1 ± 0.6 | 15.78 ± 0.02 | 0.77 ± 0.06 |
| 2017cbv | 840.8 ± 0.4 | 11.73 ± 0.02 | 0.97 ± 0.05 | 842.4 ± 0.6 | 11.68 ± 0.02 | 0.59 ± 0.04 |
| 2017cfd | 844.1 ± 0.2 | 14.89 ± 0.02 | 1.18 ± 0.05 | 845.1 ± 0.3 | 14.77 ± 0.03 | 0.74 ± 0.05 |
| 2017ckq | 851.6 ± 0.4 | 14.34 ± 0.01 | 1.16 ± 0.05 | 852.9 ± 0.4 | 14.35 ± 0.01 | 0.72 ± 0.03 |
| 2017cjr | 846.9 ± 0.3 | 15.04 ± 0.02 | 1.22 ± 0.04 | 848.6 ± 0.4 | 15.08 ± 0.02 | 0.71 ± 0.04 |
| 2017cts | 858.0 ± 0.5 | 15.79 ± 0.04 | 1.35 ± 0.06 | 859.4 ± 0.7 | 15.79 ± 0.02 | 0.73 ± 0.05 |
| 2017cze | ⋯ | ⋯ | ⋯ | 859.0 ± 0.5 | 15.83 ± 0.02 | 1.02 ± 0.05 |
| 2017cyy | 870.1 ± 0.4 | 14.84 ± 0.03 | 1.09 ± 0.07 | 871.4 ± 0.6 | 14.74 ± 0.03 | 0.60 ± 0.06 |
| 2017dei | 868.7 ± 0.7 | 16.69 ± 0.03 | 1.71 ± 0.12 | 871.3 ± 0.6 | 16.43 ± 0.02 | 1.01 ± 0.07 |
| 2017dit | 881.4 ± 0.3 | 15.90 ± 0.02 | 1.43 ± 0.07 | 883.4 ± 0.4 | 15.88 ± 0.02 | 0.79 ± 0.08 |
| 2017dps | 882.4 ± 0.3 | 14.81 ± 0.03 | 1.64 ± 0.05 | 884.1 ± 0.5 | 14.81 ± 0.03 | 0.84 ± 0.05 |
| 2017drh | 891.5 ± 0.4 | 17.11 ± 0.03 | 1.33 ± 0.07 | 892.5 ± 0.4 | 15.76 ± 0.03 | 0.76 ± 0.05 |
| 2017egb | 906.5 ± 0.3 | 15.72 ± 0.03 | 1.62 ± 0.07 | 907.8 ± 0.4 | 15.68 ± 0.01 | 0.84 ± 0.04 |
| 2017ejb | 911.0 ± 0.1 | 15.83 ± 0.02 | 2.04 ± 0.04 | 913.2 ± 0.2 | 15.38 ± 0.01 | 1.30 ± 0.03 |
| 2017ejw | 912.5 ± 0.3 | 15.51 ± 0.03 | 1.45 ± 0.06 | 913.7 ± 0.3 | 15.55 ± 0.03 | 0.86 ± 0.05 |
| 2017ekr | 914.5 ± 1.6 | 16.15 ± 0.07 | 1.43 ± 0.40 | 915.9 ± 1.7 | 15.99 ± 0.06 | 0.95 ± 0.34 |
| 2017emq | 917.5 ± 0.3 | 14.41 ± 0.02 | 1.36 ± 0.05 | 919.9 ± 0.5 | 14.17 ± 0.02 | 0.73 ± 0.05 |
| 2017enx | 917.4 ± 1.4 | 14.05 ± 0.05 | 1.67 ± 0.19 | 920.1 ± 1.5 | 13.83 ± 0.05 | 0.93 ± 0.18 |
| 2017erv | 923.8 ± 0.7 | 15.89 ± 0.02 | 1.04 ± 0.09 | 927.2 ± 0.5 | 15.67 ± 0.02 | 0.72 ± 0.04 |
| 2017erp | 934.7 ± 1.7 | 13.69 ± 0.04 | 1.03 ± 0.21 | 936.7 ± 1.6 | 13.52 ± 0.03 | 0.65 ± 0.10 |
| 2017ezd | 942.1 ± 0.4 | 15.79 ± 0.02 | 1.35 ± 0.07 | 942.5 ± 0.4 | 15.73 ± 0.02 | 0.78 ± 0.04 |
| 2017evn | 936.1 ± 1.4 | 15.40 ± 0.05 | 1.02 ± 0.16 | 936.9 ± 1.1 | 15.34 ± 0.02 | 0.67 ± 0.09 |
| 2017exo | 937.4 ± 0.8 | 16.70 ± 0.03 | 0.96 ± 0.09 | 938.8 ± 0.6 | 16.24 ± 0.03 | 0.69 ± 0.04 |
| 2017fbj | 944.6 ± 0.5 | 16.22 ± 0.03 | 1.18 ± 0.09 | 947.6 ± 0.6 | 15.95 ± 0.04 | 0.71 ± 0.08 |
| 2017ffv | 956.1 ± 1.2 | 15.49 ± 0.07 | 1.13 ± 0.14 | 957.7 ± 1.1 | 15.22 ± 0.04 | 0.73 ± 0.08 |
| 2017fgc | 958.8 ± 0.2 | 13.76 ± 0.01 | 1.02 ± 0.03 | 963.1 ± 0.5 | 13.55 ± 0.01 | 0.72 ± 0.02 |
| 2017fzy | 978.7 ± 0.9 | 16.32 ± 0.02 | 1.84 ± 0.14 | 983.2 ± 1.4 | 15.97 ± 0.02 | 1.08 ± 0.11 |
| 2017fzw | 987.8 ± 0.2 | 14.21 ± 0.02 | 1.71 ± 0.03 | 990.1 ± 0.4 | 13.85 ± 0.02 | 0.88 ± 0.05 |
| 2017gah | 984.9 ± 0.2 | 15.03 ± 0.03 | 1.72 ± 0.06 | 987.4 ± 0.3 | 14.57 ± 0.02 | 0.98 ± 0.05 |
| 2017gjn | 1004.6 ± 0.3 | 15.14 ± 0.01 | 1.05 ± 0.03 | 1005.1 ± 0.4 | 15.06 ± 0.01 | 0.65 ± 0.03 |
| 2017glq | 1016.2 ± 0.3 | 14.29 ± 0.01 | 1.23 ± 0.04 | 1016.8 ± 0.4 | 14.28 ± 0.01 | 0.68 ± 0.04 |
| 2017glx | 1009.8 ± 0.6 | 14.69 ± 0.03 | 0.89 ± 0.07 | 1012.2 ± 0.7 | 14.53 ± 0.02 | 0.71 ± 0.04 |
| 2017grw | 1017.5 ± 0.4 | 15.59 ± 0.02 | 1.51 ± 0.06 | 1019.0 ± 0.4 | 15.51 ± 0.02 | 0.80 ± 0.04 |
| 2017guh | 1022.0 ± 0.6 | 15.20 ± 0.03 | 1.36 ± 0.12 | 1024.2 ± 0.5 | 15.18 ± 0.01 | 0.74 ± 0.04 |
| 2017haf | 1034.8 ± 0.2 | 15.46 ± 0.01 | 1.19 ± 0.03 | 1035.8 ± 0.3 | 15.35 ± 0.01 | 0.75 ± 0.02 |
| 2017hgz | 1044.3 ± 0.3 | 15.21 ± 0.01 | 1.46 ± 0.05 | 1046.1 ± 0.4 | 15.18 ± 0.02 | 0.77 ± 0.04 |
| 2017hjw | 1056.0 ± 0.3 | 16.21 ± 0.02 | 0.97 ± 0.03 | 1057.0 ± 0.3 | 15.90 ± 0.01 | 0.63 ± 0.03 |
| 2017hjy | 1056.2 ± 0.3 | 15.54 ± 0.02 | 1.21 ± 0.05 | 1057.7 ± 0.4 | 15.45 ± 0.01 | 0.66 ± 0.03 |
| 2017hle | 1049.3 ± 0.5 | 17.93 ± 0.01 | 1.70 ± 0.07 | 1053.1 ± 0.2 | 16.99 ± 0.02 | 1.37 ± 0.03 |
| 2017hoq | 1061.2 ± 1.3 | 16.03 ± 0.04 | 0.89 ± 0.12 | 1063.8 ± 0.6 | 15.95 ± 0.02 | 0.70 ± 0.04 |
| 2017hou | 1056.5 ± 0.9 | 18.22 ± 0.02 | 0.94 ± 0.10 | 1057.5 ± 0.5 | 17.47 ± 0.02 | 0.64 ± 0.06 |
| 2017hpa | 1065.8 ± 0.5 | 15.51 ± 0.02 | 1.05 ± 0.06 | 1068.7 ± 0.5 | 15.39 ± 0.01 | 0.72 ± 0.03 |
| 2017igf | 1085.0 ± 0.2 | 14.87 ± 0.02 | 1.87 ± 0.05 | 1086.4 ± 0.2 | 14.59 ± 0.01 | 1.05 ± 0.03 |
| 2017iji | 1081.7 ± 0.9 | 15.16 ± 0.02 | 1.26 ± 0.10 | 1084.0 ± 0.8 | 15.02 ± 0.02 | 0.74 ± 0.06 |
| 2017isj | 1092.9 ± 1.3 | 15.81 ± 0.03 | 0.99 ± 0.16 | 1096.7 ± 0.5 | 15.59 ± 0.04 | 0.74 ± 0.05 |
| 2017iyb | 1117.4 ± 0.6 | 14.91 ± 0.01 | 1.42 ± 0.08 | 1119.7 ± 0.4 | 14.82 ± 0.02 | 0.82 ± 0.04 |
| 2017iyw | ⋯ | ⋯ | ⋯ | 1109.1 ± 1.2 | 15.62 ± 0.02 | 0.76 ± 0.08 |
| 2017jav | 1118.1 ± 0.2 | 15.98 ± 0.03 | 1.81 ± 0.04 | 1119.3 ± 0.3 | 15.80 ± 0.01 | 0.96 ± 0.03 |
| 2017jdx | 1119.0 ± 0.4 | 15.93 ± 0.02 | 1.07 ± 0.05 | 1120.1 ± 0.4 | 15.86 ± 0.01 | 0.60 ± 0.03 |
| 2018gl | 1138.8 ± 0.1 | 16.31 ± 0.00 | 1.83 ± 0.02 | 1140.3 ± 0.1 | 16.14 ± 0.00 | 1.08 ± 0.01 |
| 2018gv | 1149.6 ± 0.7 | 12.91 ± 0.03 | 0.84 ± 0.08 | 1151.1 ± 0.6 | 12.89 ± 0.02 | 0.62 ± 0.05 |
| 2018kp | 1159.3 ± 0.3 | 16.62 ± 0.02 | 1.22 ± 0.05 | 1161.6 ± 0.4 | 16.09 ± 0.01 | 0.66 ± 0.03 |
| 2018pv | 1163.9 ± 0.4 | 13.27 ± 0.03 | 1.85 ± 0.08 | 1166.8 ± 0.2 | 12.68 ± 0.03 | 1.18 ± 0.06 |
| 2018pc | 1165.3 ± 0.4 | 15.42 ± 0.02 | 1.41 ± 0.08 | 1166.5 ± 0.4 | 15.08 ± 0.01 | 0.77 ± 0.04 |
| 2018oh | 1163.2 ± 0.3 | 14.29 ± 0.01 | 0.99 ± 0.04 | 1163.8 ± 0.3 | 14.29 ± 0.01 | 0.65 ± 0.03 |
| 2018vw | 1177.9 ± 0.5 | 15.37 ± 0.03 | 0.92 ± 0.07 | 1179.4 ± 0.6 | 15.44 ± 0.02 | 0.62 ± 0.04 |
| 2018xx | 1183.9 ± 0.3 | 14.46 ± 0.02 | 1.37 ± 0.05 | 1185.1 ± 0.4 | 14.43 ± 0.02 | 0.79 ± 0.06 |
| 2018yu | 1194.7 ± 0.4 | 13.98 ± 0.02 | 1.03 ± 0.06 | 1195.8 ± 0.4 | 13.94 ± 0.01 | 0.67 ± 0.04 |
| 2018zz | 1190.7 ± 0.2 | 15.10 ± 0.02 | 1.91 ± 0.03 | 1192.4 ± 0.2 | 14.96 ± 0.01 | 1.03 ± 0.03 |
| 2018apo | 1223.6 ± 0.7 | 15.50 ± 0.03 | 0.93 ± 0.09 | 1226.2 ± 0.7 | 15.26 ± 0.03 | 0.62 ± 0.08 |
| 2018aoz | 1222.6 ± 0.3 | 12.84 ± 0.03 | 1.33 ± 0.07 | 1223.1 ± 0.3 | 12.84 ± 0.02 | 0.79 ± 0.04 |
| 2018aqi | 1223.1 ± 0.3 | 15.81 ± 0.03 | 1.48 ± 0.06 | 1225.4 ± 0.3 | 15.58 ± 0.02 | 0.85 ± 0.04 |
| 2018aye | 1243.9 ± 0.5 | 15.70 ± 0.02 | 1.04 ± 0.06 | 1244.7 ± 0.4 | 15.67 ± 0.02 | 0.71 ± 0.03 |
| 2018big | 1264.5 ± 0.4 | 15.91 ± 0.01 | 0.98 ± 0.05 | 1266.1 ± 0.5 | 15.80 ± 0.01 | 0.60 ± 0.04 |
| 2018bta | ⋯ | ⋯ | ⋯ | 1269.2 ± 0.7 | 15.47 ± 0.03 | 0.73 ± 0.08 |
| 2018cqw | 1300.7 ± 0.4 | 14.56 ± 0.01 | 0.99 ± 0.05 | 1301.6 ± 0.4 | 14.45 ± 0.01 | 0.62 ± 0.03 |
| 2018ctv | 1294.3 ± 0.6 | 17.42 ± 0.03 | 2.00 ± 0.07 | 1296.5 ± 0.7 | 16.70 ± 0.03 | 1.36 ± 0.06 |
| 2018cuh | 1305.5 ± 0.4 | 15.02 ± 0.03 | 1.20 ± 0.08 | 1306.3 ± 0.3 | 15.03 ± 0.02 | 0.67 ± 0.05 |
| 2018dda | 1313.7 ± 0.9 | 15.62 ± 0.04 | 0.98 ± 0.11 | 1315.6 ± 0.8 | 15.29 ± 0.03 | 0.67 ± 0.06 |
| 2018eay | 1328.5 ± 0.5 | 17.48 ± 0.02 | 0.94 ± 0.07 | 1330.6 ± 0.8 | 16.69 ± 0.02 | 0.63 ± 0.05 |
| 2018ebk | 1330.2 ± 0.4 | 16.88 ± 0.03 | 1.26 ± 0.05 | 1332.1 ± 0.4 | 16.32 ± 0.02 | 0.73 ± 0.03 |
| 2018enc | 1345.5 ± 1.3 | 16.10 ± 0.04 | 0.89 ± 0.13 | 1346.5 ± 1.3 | 15.94 ± 0.03 | 0.66 ± 0.09 |
| 2018eov | 1342.4 ± 0.9 | 15.65 ± 0.03 | 1.04 ± 0.12 | 1343.7 ± 0.6 | 15.42 ± 0.02 | 0.65 ± 0.05 |
| 2018eqq | ⋯ | ⋯ | ⋯ | 1341.3 ± 1.0 | 15.30 ± 0.02 | 0.68 ± 0.05 |
| 2018feb | 1362.4 ± 0.3 | 15.26 ± 0.02 | 1.11 ± 0.05 | 1363.5 ± 0.4 | 15.24 ± 0.01 | 0.60 ± 0.03 |
| 2018fhw | 1357.5 ± 0.2 | 16.67 ± 0.02 | 1.98 ± 0.04 | 1360.3 ± 0.3 | 16.37 ± 0.02 | 1.22 ± 0.04 |
| 2018fop | ⋯ | ⋯ | ⋯ | 1366.7 ± 1.2 | 15.57 ± 0.03 | 0.55 ± 0.08 |
| 2018fnq | 1374.6 ± 0.6 | 15.77 ± 0.03 | 1.06 ± 0.07 | 1375.0 ± 0.7 | 15.69 ± 0.02 | 0.65 ± 0.05 |
| 2018fuk | 1377.1 ± 0.4 | 15.87 ± 0.01 | 1.20 ± 0.06 | 1378.9 ± 0.4 | 15.75 ± 0.02 | 0.68 ± 0.04 |
| 2018ghb | 1381.0 ± 0.9 | 14.81 ± 0.05 | 1.59 ± 0.12 | 1384.4 ± 0.7 | 14.53 ± 0.03 | 0.97 ± 0.07 |
| 2018hib | 1415.1 ± 0.3 | 15.25 ± 0.02 | 1.27 ± 0.05 | 1416.2 ± 0.4 | 15.22 ± 0.01 | 0.74 ± 0.03 |
| 2018htt | 1438.6 ± 0.2 | 13.91 ± 0.03 | 1.59 ± 0.04 | 1439.5 ± 0.3 | 13.91 ± 0.03 | 0.85 ± 0.04 |
| 2018hrt | ⋯ | ⋯ | ⋯ | 1433.8 ± 0.5 | 17.32 ± 0.02 | 0.82 ± 0.06 |
| 2018hsa | 1432.3 ± 0.4 | 15.78 ± 0.02 | 1.14 ± 0.07 | 1434.6 ± 0.8 | 15.65 ± 0.02 | 0.69 ± 0.06 |
| 2018ilu | 1449.7 ± 1.0 | 15.42 ± 0.02 | 0.93 ± 0.09 | 1451.9 ± 0.6 | 15.36 ± 0.01 | 0.62 ± 0.04 |
| 2018isq | 1448.8 ± 0.4 | 16.89 ± 0.02 | 1.95 ± 0.08 | 1451.8 ± 0.2 | 16.00 ± 0.01 | 1.30 ± 0.04 |
| 2018iuu | 1459.8 ± 0.3 | 15.48 ± 0.02 | 1.21 ± 0.04 | 1462.0 ± 0.7 | 15.46 ± 0.02 | 0.74 ± 0.04 |
| 2018jaj | 1463.4 ± 0.4 | 15.52 ± 0.01 | 0.99 ± 0.04 | 1464.6 ± 0.4 | 15.41 ± 0.01 | 0.70 ± 0.03 |
| 2018jeo | 1454.7 ± 1.0 | 16.07 ± 0.02 | 1.04 ± 0.11 | 1456.5 ± 0.5 | 15.94 ± 0.01 | 0.61 ± 0.05 |
| 2018jky | 1469.0 ± 0.2 | 15.39 ± 0.03 | 1.69 ± 0.06 | 1470.2 ± 0.3 | 15.31 ± 0.02 | 0.89 ± 0.04 |
| 2018jmo | ⋯ | ⋯ | ⋯ | 1475.7 ± 0.9 | 16.53 ± 0.04 | 0.91 ± 0.09 |
| 2018jov | 1475.2 ± 0.4 | 16.21 ± 0.02 | 1.10 ± 0.05 | 1476.3 ± 0.5 | 16.06 ± 0.01 | 0.64 ± 0.04 |
| 2018jwi | 1479.1 ± 0.3 | 15.04 ± 0.02 | 1.10 ± 0.04 | 1480.4 ± 0.4 | 15.04 ± 0.02 | 0.69 ± 0.04 |
| 2018kmu | 1480.9 ± 1.4 | 16.42 ± 0.06 | 0.88 ± 0.18 | 1483.5 ± 1.8 | 16.30 ± 0.07 | 0.69 ± 0.12 |
| 2019np | 1509.6 ± 0.5 | 13.42 ± 0.02 | 1.00 ± 0.05 | 1510.9 ± 0.7 | 13.39 ± 0.02 | 0.63 ± 0.04 |
| 2019so | 1507.2 ± 0.2 | 17.21 ± 0.02 | 1.96 ± 0.04 | 1509.2 ± 0.2 | 16.67 ± 0.02 | 1.36 ± 0.04 |
| PSN J140216.0-533228.8 | 1513.0 ± 0.9 | 17.01 ± 0.03 | 0.85 ± 0.10 | 1515.2 ± 0.8 | 16.26 ± 0.02 | 0.59 ± 0.06 |
| 2019gbx | 1647.0 ± 0.3 | 14.80 ± 0.03 | 1.24 ± 0.06 | 1647.8 ± 0.4 | 14.78 ± 0.02 | 0.80 ± 0.04 |
| 2019hxc | 1663.4 ± 0.9 | 16.60 ± 0.05 | 1.31 ± 0.15 | 1665.7 ± 1.5 | 16.44 ± 0.04 | 0.73 ± 0.08 |
| 2019khf | 1680.3 ± 0.4 | 15.19 ± 0.03 | 1.12 ± 0.06 | 1681.8 ± 0.6 | 15.20 ± 0.03 | 0.63 ± 0.05 |
| 2020ue | 1873.5 ± 0.2 | 12.22 ± 0.01 | 1.51 ± 0.04 | 1874.1 ± 0.3 | 12.16 ± 0.01 | 0.86 ± 0.03 |
Note.
a The SN name adopts the IAU name when available, otherwise the survey name. All the IAU and survey names are available in Table 1.A machine-readable version of the table is available.
Figure 3 shows the histogram of all available direct Δm15(B) measurements for CNIa0.02 DR1. The left panel is for the SNe included in CNIa0.02 DR1, and the right panel is for those in the complete sample. Our objects include SNe Ia spanning the full range of Δm15(B) of the SN Ia population from Δm15(B) ≈ 0.7 mag to Δm15(B) ≈ 2.0 mag. The complete sample consists of SNe Ia with z < 0.02 and Vpeak < 16.5 mag, and due to the peak magnitude limits, our sample is not sensitive to all dim SNe Ia with high Δm15(B) values within the volume confined by z < 0.02. Further work to quantify the detection efficiency within different Δm15(B) bins needs to be carried out to obtain the intrinsic distribution of Δm15(B) and other parameters for the SNe Ia population.
Figure 3. Distribution of all available direct Δm15(B) measurements for 129 SNe Ia in DR1 (left panel) and 95 SNe Ia in the complete sample (right panel).
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Standard image High-resolution image5. Summary
CNIa0.02 aims to obtain a homogeneous and unbiased sample of nearby SNe Ia with multiband light curves to study the SNe Ia population. In CNIa0.02 DR1, we present 247 SNe with optical light curves, including 148 SNe in the complete sample. DR1 offers large and homogenous optical photometric data sets to systematically study the SNe Ia population. In this paper, we present the first analysis of our data set by extracting parameters such as Δm15(B). We plan to publish near-UV, near-IR, and late-phase photometric data in the future. Our multiband light curves also allow us to derive host-galaxy extinction and luminosity, and in a forthcoming publication, we plan to make a completeness correction and study the SN Ia luminosity function. CNIa0.02 provides a large and homogeneous data set to infer the intrinsic distribution properties of SNe Ia in the local universe to help answer basic questions regarding SN Ia progenitor systems and explosion mechanisms.
We thank Eric Peng and the anonymous referee for helpful suggestions. We acknowledge the Telescope Access Program (TAP) funded by the NAOC, CAS and the Special Fund for Astronomy from the Ministry of Finance. We acknowledge SUPA2019A (PI: M.D. Stritzinger) via OPTICON. C.S.K., K.Z.S., and B.J.S. are supported by NSF grants AST-1515927, AST-1814440, and AST-1908570. M.D.S. acknowledges funding from the Villum Fonden (project numbers 13261 and 28021). M.D.S. is supported by a project grant (8021-00170B) from the Independent Research Fund Denmark. A.V.F.'s supernova group is grateful for financial assistance from the Christopher R. Redlich Fund, the TABASGO Foundation, and the Miller Institute for Basic Research in Science (U.C. Berkeley). A major upgrade of the Kast spectrograph on the Shane 3 m telescope at Lick Observatory was made possible through generous gifts from William and Marina Kast as well as the Heising-Simons Foundation. Research at Lick Observatory is partially supported by a generous gift from Google. We thank the staffs of the various observatories at which data were obtained for their excellent assistance. J.L.P. is provided in part by FONDECYT through the grant 1191038 and by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. M.F. acknowledges the support of a Royal Society—Science Foundation Ireland University Research Fellowship. B.J.S. is also supported by NSF grants AST-1920392 and AST-1911074. M.G. is supported by the Polish NCN MAESTRO grant 2014/14/A/ST9/00121. Polish participation in SALT is funded by grant no. MNiSW DIR/WK/2016/07. S.M.H. is supported by the Natural Science Foundation of Shandong province (No. JQ201702), and the Young Scholars Program of Shandong University (No. 20820162003). Support for T.W.-S.H. was provided by NASA through the NASA Hubble Fellowship grant No. HST-HF2-51458.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. We thank the Swift PI Brad Cenko, the Observation Duty Scientists, and the science planners for approving and executing our Swift/UVOT SNe Ia campaign.
Software: Astropy (Astropy Collaboration et al. 2018), PyRAF (Science Software Branch at STScI 2012), FITSH (Pál 2012), ccdproc (Craig et al. 2017), HOTPANTS (Becker 2015), DoPHOT (Schechter et al. 1993; Alonso-García et al. 2012).
Appendix A: Observing Protocol
Figure 4 illustrates the protocol in our observing procedures when collecting our complete sample in the period between 2016 October and 2019 January. We scan the ASAS-SN transient page,
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the Astronomer's Telegram,
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the Transient Name Server,
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and the Bright Supernova webpage
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on a daily basis, and record all bright transients with discovery magnitudes of mdis < 19. To obtain early follow-up data for SNe Ia in the sample, we start observations before classification for all potential targets according to the strategy in Figure 4. Meanwhile, we coordinate all available spectroscopic resources to classify the potential targets. Note that the primary aim of our complete sample is to include all spectroscopic subclasses (e.g., 1991bg-like, 1991T-like) that belong to the SNe Ia population. We made follow-up observations of some SNe Ia-like objects (e.g., SNe Iax) that are known to deviate from the WLR of SNe Ia, and they do not belong to the complete sample. For SNe without archival host redshifts, we followed-up those with SN redshifts of 
if they have Vpeak < 16.5. The selection of limit on 
is based on the knowledge that the typical uncertainties of SN redshifts from spectroscopic classification are ≲0.005. SuperNova IDentification (SNID; Blondin & Tonry 2007) is one of the commonly used tool for SNe classification. Stahl et al. (2020) investigated the SNID-determined redshifts by comparing them to the corresponding host-galaxy redshifts and found a standard deviation of 0.0039 for the difference between 
and zhost.
Figure 4. Observing protocol for the CNIa0.02 complete sample.
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Standard image High-resolution imageAppendix B: Follow-up Instruments
We used 1 m telescopes from the Las Cumbres Observatory Global Telescope network (LCOGT; Brown et al. 2013), which operates a number of robotic telescopes distributed at four sites (Siding Spring in Australia, Sutherland in South Africa, Cerro Tololo in Chile, and McDonald Observatory in USA) covering both hemispheres. Each 1 m telescope is equipped with either a "Sinistro" or an SBIG STX-16803 camera. 50 The Bessel BV and SDSS ri filters are available on all telescopes, which were the main ones used for our optical observation. We also obtained some images using the 2 m or 0.4 m telescopes, and we plan to make these data available in the future.
We used two 24 inch CDK24 telescopes operated by the Post Observatory (PO) mainly for following-up northern objects. One is located at the Sierra Remote Observatories (SRO 51 ; CA, USA) and the other at Post Observatory Mayhill (NM, USA). We used two types of cameras: an Apogee Alta U230 camera and an Apogee Alta U47 camera. Both cameras are back-illuminated, with similar quantum efficiency >90% over a broad region. The U230 camera was used by default at both sites. The telescope at SRO used the U230 for almost all images, and the Mayhill site had the U47 camera for a long period of time when the U230 camera was unavailable because its damaged shutter was being repaired. Astrodon Photometrics BV 52 and Sloan ri 53 filters were used.
The 1.3 m telescope of the Small and Moderate Aperture Research Telescope System (SMARTS; Subasavage et al. 2010) is located at Cerro Tololo Inter-American Observatory (CTIO). It is equipped with A Novel Dual Imaging CAMera (ANDICAM; DePoy et al. 2003). The optical CCD for ANDICAM is a Fairchild 447 2048 × 2048 pixel CCD. The IR Array for the ANDICAM is a Rockwell 1024x1024 HgCdTe "Hawaii" Array with 18 μm pixels. SMARTS/ANDICAM is equipped with standard KPNO-recipe Johnson-Kron-Cousins BVRI filters and standard CIT/CTIO JHK filters. SNe were observed in BVRI and JH-bands with ANDICAM. In this data release, we publish BV data. The RI and JH data taken by ANDICAM will be published in a future data release.
The instruments described above are the primary ones used for DR1. Their instrument specifications are listed in Table 6. The filter set used for observations in DR1 is compared to Landolt BV (Landolt 1992) and the SDSS ri (Fukugita et al. 1996) standard bandpasses in Figure 5.
Figure 5. The filter bandpasses used to obtain the majority of data released in this paper (solid lines). The standard Landolt BV and SDSS ri bandpasses (dashed lines) are shown for comparison.
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Standard image High-resolution imageTable 6. Instrument Specifications
| Imager | Format | Binning | Pixel Scale | Field of View | Read Noise | Gain |
|---|---|---|---|---|---|---|
| (pixels) | (pixels) | (arcsec pixel−1) | (arcmin × arcmin) | (e−) | (e−/ADU) | |
| SBIG STX-16803 | 4096 × 4096 | 2 × 2 | 0.464 | 15.8 × 15.8 | 13.5 | 1.5 |
| Sinistro | 4096 × 4096 | 1 × 1 | 0.389 | 26.5 × 26.5 | 7–8 | 1.0 |
| Apogee Alta U230 | 2048 × 2048 a | 1 × 1 | 0.77 | 13.1 × 13.1 | 2.9 | 12.4 |
| Apogee Alta U47 | 1024 × 1024 | 1 × 1 | 0.67 | 11.4 × 11.4 | 2.22 | 11.2 |
| ANDICAM CCD | 2048 × 2048 | 2 × 2 | 0.371 | ∼ 6 × 6 | 6.5 | 2.3 |
Note.
a The central 1024 × 1024 pixels were used.Download table as: ASCIITypeset image
DEdicated MONitor of EXotransits and Transients (DEMONEXT; Villanueva et al. 2018) is a 0.5 m PlaneWave CDK20 f/6.8 Corrected Dall-Kirkham Astrograph telescope at Winer Observatory in Sonoita, Arizona. DEMONEXT has a 2048 × 2048 pixel FLI Proline CCD3041 camera, with a 
field of view (FOV) and a pixel scale of 09 pixel−1. DEMONEXT has a full suite of Bessel BVRI and SDSS griz filters. BVri data for four SNe (2016hli, 2016gou, 2016gxp, and 2017isq) are included in DR1. We also include photometry for three SNe (2017ghu, 2017hle, and 2018ast) obtained with the Liverpool Telescope (LT) IO:O instrument in DR1. IO:O is the optical-imaging component of the IO (Infrared-Optical) suite of instruments. It is equipped with a 4096 × 4112 pixel e2V CCD 231–84, with a
FoV and a pixel scale of ∼ 03 pixel−1 with 2 × 2 binning. The 1 m telescope at WeiHai Observatory of Shandong University (WHO; Hu et al. 2014) was used to obtain BVri images for ASASSN-15uh. It has a back-illuminated PIXIS 2048B CCD camera at the Cassegrain focus, providing a
FoV and a pixel scale of 035 pixel−1. The 0.41 m f/3.3 reflector telescope at A77 observatory (Dauban, 04150 Banon, France) was used to obtain some BV images for 2015ar. The telescope is equipped with an ST8XME CCD, and its pixel scale is 1
4 pixel−1.
We used instruments mounted on the du Pont 2.5 m telescope, the 2.4 m Hiltner telescope and the 2.56 m Nordic Optical Telescope (NOT) to image a number of SNe. We used two cameras mounted on du Pont. One is called "CCD", which is a direct-imaging camera with a 2048 × 2048 pixel SITe2K CCD with plate scale of 0259 pixel−1 and an FoV of
. The other is the WF4K CCD for the Wide Field Reimaging CCD Camera (WFCCD), which has a 4064 × 4064 pixel CCD with a plate scale of 0484 pixel−1 and an FoV of
in diameter. For Hiltner, we used Ohio State Multi-Object Spectrograph (OSMOS), which is a wide-field imager and multi-object spectrograph. For our imaging observation, a 4096 × 4096 pixel STA0500A CCD was used, which has a scale of 0273 pixel−1 and an FoV with
in diameter. On NOT, we used the Alhambra Faint Object Spectrograph and Camera (ALFOSC), which has both spectroscopic and imaging capabilities. The ALFOSC imaging was performed using a CCD231-42-g-F61 back-illuminated CCD with an FoV of 
and a plate scale of 02138 pixel−1 in the imaging mode.
Appendix C: Sample Completeness
Our targets are selected according to the detections of the ASAS-SN survey, so the sample completeness depends on the ASAS-SN detection efficiency, that is, the fraction of the occurred SNe that are detected by ASAS-SN. Holoien et al. (2019) compiled a sample of all SNe detected by ASAS-SN between 2014 May 01 and 2017 December 31, and they found that the integral completeness (i.e., the cumulative detection efficiency) of this total sample is 95 ± 3% at mpeak = 16.5 by comparing with Euclidean predictions. That sample included SNe found before the implementation of a machine-learning algorithm at the end of 2014, which substantially increased the detection efficiency (see Figure 4 of Holoien et al. 2019). During the collection of our complete sample (i.e., 2015 September 17 to 2019 January 31), the ASAS-SN survey had several upgrades, including the operation of the Cassius unit in the summer of 2015 and the further expansions of three new units (Leavitt, Paczynski, and Payne-Gaposchkin) in late 2017, which increased the limiting magnitude from ∼17 to ∼18.5. Therefore, there are good reasons to believe that during our complete sample collection, the cumulative detection efficiency of ASAS-SN was at least 95%, and probably greater, at mpeak = 16.5 mag.
We also conduct external checks with the concurrent detections by ZTF to verify our selection criteria. ZTF conducts a wide-field survey of the northern sky at a limiting magnitude of ∼20.5 (Kulkarni 2016), and the Bright Transient Survey (BTS) project of ZTF aims to construct a magnitude-limited complete sample of transients with spectroscopic classifications down to m < 18.5 (Fremling et al. 2020; Perley et al. 2020). The public start time of the BTS survey was 2018 June 1, so there were an overlapping period of 8 months (from 2018 June 01 to 2019 January 31) with our complete sample. We first check whether all SNe Ia with peak magnitudes bright than 16.5 in BTS are included in our complete sample. Using the ZTF Bright Transient Survey Sample Explorer
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, we queried all transients with a classification of "SN Ia" that peaked between 2018 June 01 and 2019 January 31 with peakmag < 16.5 and z ≤ 0.02 and obtained a list of 14 objects. Among them, 2018dzy has a redshift 
based on ZTF SN classification spectrum, while its host galaxy (UGC 11873) is at z = 0.024760 according to NED and was thus excluded from the CNIa0.02 complete sample. All others were included in CNIa0.02 and were followed-up by us. Our spectroscopic observations of the host galaxies show that four of them (2018fop, 2018htw, 2018jmo, and 2018kmu) have host-galaxy redshifts zhost > 0.02. And all the other 9 SNe Ia (2018eay, 2018feb, 2018htt, 2018hkq, 2018iuu, 2018jaj, 2018jky, 2018jov, and 2019np) are included in the CNIa0.02 complete sample. In addition, we also queried all targets with a classification as "Candidate transients" with peakmag < 16.5 that were found between 2017 September 3 to 2019 December 31, and obtained 117 ZTF transients with peak magnitude brighter than 16.5. Among them, AT 2019ump (ZTF19acqnmjo) is likely a false positive (i.e., it has a high probability of being a "bogus" according to AleRCE ZTF Explorer
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), and all the other 116 ZTF transient candidates were detected by ASAS-SN. Our cross-examinations support that our sample is ∼100% complete down to 16.5 mag.
Appendix D: Exclusion of Peculiar Ia-like Objects
The complete sample of CNIa0.02 includes all spectroscopic subclasses of SNe Ia that are known to follow the width-luminosity relation (WLR) of SNe Ia (see Phillips & Burns 2017 for a recent review of WLR). These include the luminous Ia-91T subclass and low-luminosity Ia-91bg subclass that are sometimes reported as "Ia-pec" in classification reports due to historical reasons, but recent studies firmly show that they follow the WLR (Phillips & Burns 2017; Burns et al. 2018), so they are included in our complete sample. During the collection of our complete sample, we analyze the spectra using SNID (Blondin & Tonry 2007) to screen peculiar SNe and also combine photometric properties when necessary to check whether an SN is truly peculiar according to our definition. Below we summarize peculiar SNe that are excluded from our complete sample.
ASASSN-15us was classified as SN Ia with the best match to SN 2006bt, which is shown to be a peculiar SN Ia (Foley et al. 2010). Moreover, the late-time spectra of ASASSN-15us show significant peculiarities compared to normal SNe Ia, and we plan to present the detailed analysis of this SN in the future.
ASASSN-15ut was first classified as SN Ia-91T (Firth et al. 2016), but a later classification based on new spectroscopic observation reported that this is a peculiar object, challenging to tell whether it is a peculiar Ia or Type-Ib/c SN (Milisavljevic et al. 2016). Holoien et al. (2017b) classified ASASSN-15ut as a Type-Ib/c SN. We measure the peak time in i and B band for ASASSN-15ut and obtain the time of i-band primary maximum relative to the B band of 
days, which is outside the range for the SNe Ia population (Ashall et al. 2020).
ASASSN-15pz is an overly luminous SN belonging to the "2009dc-like SN Ia-pec" group (Chen et al. 2019). There is a large peak luminosity diversity within the group, and they generally do not follow the WLR.
2016gxp was reported to match premaximum spectra of SN 2007 well, as well as young 91T-like SN Ia (Reynolds et al. 2016). It lacks a secondary maximum in the i-band light curve and has 
days, which does not favor the 91T-like SN Ia classification (Ashall et al. 2020). We plan to present the detailed analysis of 2016gxp in the future.
2017gbb is a Type Iax (02cx-like) SN (Lyman et al. 2017), which does not belong to the SN Ia population.
Footnotes
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This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.
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