Recently, 1H 0323+342 has attracted a lot of attention as one of several narrow-line Seyfert 1 galaxies detected in the γ-ray band. To understand their central energy engines and jet phenomena, the black hole mass is important. We made use of the Lijiang 2.4 m Telescope to monitor 1H 0323+342 for more than two months. This galaxy is one of the candidates for a monitoring project of super-Eddington accreting massive black holes. The reverberation mapping shows that Hβ emission has a delayed response of -+ 14.8 2.7 3.9 days with respect to the SDSS g′ light curve in the rest frame. The optical Fe II variations were detected after subtracting host contaminations, and a reverberation with a delay of -+ 15.2 4.1 7.4 days was found in the rest frame. By assuming the viral factor f BLR = 6.17 for the broadline region (BLR) velocity characterized by FWHM because of the face-on orientation, we find that the black hole mass derived from Hβ is =-, and the accretion rate is M = -+ 1.11 0.47• is the mass accretion rate, L Edd is the Eddington luminosity, and c is the speed of light. This black hole is one order less massive than that given by the Magorrian relation from the bulge mass. We test the relation between accretion rates and radio-loudnesses in all mapped radio-loud active galactic nuclei, and find that 1H 0323+342 falls within this group.

We developed a spectroscopic monitoring project to investigate the kinematics of the broad-line region (BLR) in active galactic nuclei (AGN) with ultra-fast outflows (UFOs). Mrk 79 is a radio-quiet AGN with UFOs and warm absorbers, had been monitored by three reverberation mapping (RM) campaigns, but its BLR kinematics is not understood yet. In this paper, we report the results from a new RM-campaign of Mrk 79, which was undertaken by Lijiang 2.4-m telescope. Mrk 79 is seeming to come out the faint state, the mean flux approximates a magnitude fainter than historical record. We successfully measured the lags of the broad emission lines including Hβ λ4861, Hγ λ4340, He II λ4686 and He I λ5876 with respect to the varying AGN continuum. Based on the broad Hβ λ4861 line, we measured black hole (BH) mass of M • = 5.13 +1.57 −1.55 ×10 7 M ⊙ , estimated accretion rates ofṀ • = (0.05 ± 0.02) L Edd c −2 , indicating that Mrk 79 is a sub-Eddington accretor. We found that Mrk 79 deviates from the canonical Radius−Luminosity relationship. The marginal blueshift of the broad He II λ4686 line detected from rms spectrum indicates outflow of high-ionization gas. The velocity-resolved lag profiles of the broad Hγ λ4340, Hβ λ4861, and He I λ5876 lines show similar signatures that the largest lag occurs in the red wing of the lines then the lag decreases to both sides. These signatures should suggest that the BLR of Keplerian motion probably exists the outflow gas motion. All findings including UFOs, warm absorbers, and the kinematics of high-and low-ionization BLR, may provide an indirect evidence that the BLR of Mrk 79 probably originates from disk wind.

The Lijiang 2.4-meter Telescope (LJT), the largest common-purpose optical telescope in China, has been available to the worldwide astronomical community since 2008. It is located at the Gaomeigu site, Lijiang Observatory (LJO), in the southwest of China. The site has very good observational conditions. During its 10-year operation, several instruments have been equipped on the LJT. Astronomers can perform both photometric and spectral observations. The main scientific goals of LJT include recording photometric and spectral evolution of supernovae, reverberation mapping of active galactic nuclei, investigating the physical properties of binary stars and near-earth objects (comets and asteroids), and identification of exoplanets and all kinds of transients. Until now, the masses of 41 high accretion rate black holes have been measured, and more than 168 supernovae have been identified by the LJT. More than 190 papers related to the LJT have been published. In this paper, the general observation conditions of the Gaomeigu site is introduced at first. Then, the structure of the LJT is described in detail, including the optical, mechanical, motion and control system. The specification of all the instruments and some detailed parameters of the YFOSC is also presented. Finally, some important scientific results and future expectations are summarized.

We installed two sets of Astronomical Site Monitoring Systems (ASMSs) at Lijiang Observatory (GMG), for the running of the 2.4-meter Lijiang optical telescope (LJT) and the 1.6-meter Multi-channel Photometric Survey Telescope (Mephisto). The Mephisto is under construction. The ASMS has been running on robotic mode since 2017. The core instruments: Cloud Sensor, All-Sky Camera and Autonomous-DIMM that are developed by our group, together with the commercial Meteorological Station and Sky Quality Meter, are combined into the astronomical optical site monitoring system. The new Cloud Sensor’s Cloud-Clear Relationship is presented for the first time, which is used to calculate the All-Sky cloud cover. We designed the Autonomous-DIMM located on a tower, with the same height as LJT. The seeing data have been observed for a full year. ASMS’s data for the year 2019 are also analysed in detail, which are valuable to observers.

Optical and ultraviolet observations for the nearby type II-plateau supernova (SN IIP) 2013am in the nearby spiral galaxy M65 are presented in this paper. The early spectra are characterized by relatively narrow P-Cygni features, with ejecta velocities much lower than observed in normal SNe IIP (i.e., ∼2000 km s −1 vs. ∼5000 km −1 in the middle of the plateau phase). Moreover, prominent Ca II absorptions are also detected in SN 2013am at relatively early phases. These spectral features are reminiscent of those seen in the low-velocity and low-luminosity SN IIP 2005cs. However, SN 2013am exhibits different photometric properties, having shorter plateau phases and brighter lightcurve tails if compared to SN 2005cs. Adopting R V =3.1 and a mean value of total reddening derived from the photometric and spectroscopic methods(i.e., E(B − V ) = 0.55±0.19 mag), we find that SN 2013am may have reached an absolute V -band peak magnitude of −15.83 ± 0.71 mag, and produced a 56 Ni mass of 0.016 +0.010 −0.006 M in the explosion. These parameters are close to those derived for SN 2008in and SN 2009N which have been regarded as "gap-filler" objects linking the faint SNe IIP to the normal ones. This indicates that some low-velocity SNe IIP may not necessarily result from the low-energetic explosions, and the low expansion velocities could be due to a lower metallicity of the progenitor stars, a larger envelope mass ejected in the explosion, or that is was observed at an angle that is away from the polar direction. Subject headings: supernovae:general -supernovae: Individual (SN 2013am) 1 Yunnan Observatories (YNAO), Chinese Academy of Sciences,

Photometric and spectroscopic observations of a slowly declining, luminous Type Ia supernova (SN Ia) SN 2011hr in the starburst galaxy NGC 2691 are presented. SN 2011hr is found to peak at M B = −19.84 ± 0.40 mag, with a post-maximum decline rate ∆m 15 (B) = 0.92 ± 0.03 mag. From the maximum-light bolometric luminosity, L = (2.30 ± 0.90) × 10 43 erg s −1 , we estimate the mass of synthesized 56 Ni in SN 2011hr to be M ( 56 Ni) = 1.11 ± 0.43 M . SN 2011hr appears more luminous than SN 1991T at around maximum light, and the absorption features from its intermediate-mass elements (IMEs) are noticeably weaker than the latter at similar phases. Spectral modeling suggests that SN 2011hr has the IMEs of ∼ 0.07 M in the outer ejecta, which is much lower than the typical value of normal SNe Ia (i.e., 0.3 -0.4 M ) and is also lower than the value of SN 1991T (i.e., ∼ 0.18 M ). These results indicate that SN 2011hr may arise from a Chandrasekhar-mass white dwarf progenitor that experienced a more efficient burning process in the explosion. Nevertheless, it is still possible that SN 2011hr may serve as a transitional object connecting the SN 1991T-like SNe Ia with the superluminous subclass like SN 2007if given that the latter also shows very weak IMEs at all phases.

Extensive and independent observations of Type Ia supernova (SN Ia) SN 2013dy are presented, including a larger set of UBVRI photometry and optical spectra from a few days before the peak brightness to ∼ 200 days after explosion, and ultraviolet (UV) photometry spanning from t≈-10 days to t≈+15 days refers to the B band maximum. The peak brightness (i.e., M B =-19.65±0.40 mag; L max =[1.95±0.55]×1043 erg s −1 ) and the mass of synthesized 56 Ni (i.e., M( 56 Ni)=0.90±0.26 M e ) are calculated, and they conform to the expectation for an SN Ia with a slow decline rate (i.e., Δm 15 (B)=0.90±0.03 mag). However, the near infrared (NIR) brightness of this SN (i.e., M H =-17.33±0.30 mag) is at least 1.0 mag fainter than usual. Besides, spectroscopy classification reveals that SN 2013dy resides on the border of "core normal" and "shallow silicon" subclasses in the Branch et al. classification scheme, or on the border of the "normal velocity" SNe Ia and 91T/99aa-like events in the Wang et al. system. These suggest that SN 2013dy is a slow-declining SN Ia located on the transitional region of nominal spectroscopic subclasses and might not be a typical normal sample of SNe Ia.

Quasars behind the Galactic plane (GPQs) are important astrometric references and valuable probes of Galactic gas, yet the search for GPQs is difficult due to severe extinction and source crowding in the Galactic plane. In this paper, we present a sample of 204 spectroscopically confirmed GPQs at ∣b∣ < 20°, 191 of which are new discoveries. This GPQ sample covers a wide redshift range from 0.069 to 4.487. For the subset of 230 observed GPQ candidates, the lower limit of the purity of quasars is 85.2%, and the lower limit of the fraction of stellar contaminants is 6.1%. Using a multicomponent spectral fitting, we measure the emission line and continuum flux of the GPQs, and estimate their single-epoch virial black hole masses. Due to selection effects raised from Galactic extinction and target magnitude, these GPQs have higher black hole masses and continuum luminosities in comparison to the SDSS DR7 quasar sample. The spectral-fitting results and black hole mass estimates are compiled into a main spectral catalog, and an extended spectral catalog of GPQs. The successful identifications prove the reliability of both our GPQ selection methods and the GPQ candidate catalog, shedding light on the astrometric and astrophysical programs that make use of a large sample of GPQs in the future.