A sub-kpc-scale binary AGN with double narrow-line regions

We present the kinematic properties of a type-2 QSO, SDSS J132323.33-015941.9 at z~0.35, based on the analysis of Very Large Telescope integral field spectroscopy and Hubble Space Telescope (HST) imaging, which suggest that the target is a binary active galactic nucleus (AGN) with double narrow-line regions. The QSO features double-peaked emission lines ([OIII] and Hb) which can be decomposed into two kinematic components. The flux-weighted centroids of the blue and red components are separated by ~0.2" (0.8 kpc in projection) and coincide with the location of the two stellar cores detected in the HST broad-band images, implying that both stellar cores host an active black hole. The line-of-sight velocity of the blue component is comparable to the luminosity-weighted velocity of stars in the host galaxy while the red component is redshifted by ~240 km/s, consistent with typical velocity offsets of two cores in a late stage of a galaxy merger. If confirmed, the target is one of the rare cases of sub-kpc scale binary AGNs, providing a test-bed for understanding the binary AGN population.Comment: 5 pages, 3 figure

The 750 GeV Diphoton Excess May Not Imply a 750 GeV Resonance

We discuss non-standard interpretations of the 750 GeV diphoton excess recently reported by the ATLAS and CMS Collaborations which do not involve a new, relatively broad, resonance with a mass near 750 GeV. Instead, we consider the sequential cascade decay of a much heavier, possibly quite narrow, resonance into two photons along with one or more invisible particles. The resulting diphoton invariant mass signal is generically rather broad, as suggested by the data. We examine three specific event topologies - the antler, the sandwich, and the 2-step cascade decay, and show that they all can provide a good fit to the observed published data. In each case, we delineate the preferred mass parameter space selected by the best fit. In spite of the presence of invisible particles in the final state, the measured missing transverse energy is moderate, due to its anti- correlation with the diphoton invariant mass. We comment on the future prospects of discriminating with higher statistics between our scenarios, as well as from more conventional interpretations.Comment: Discussion about the ATLAS Moriond EW2016 added. Matched to PRL accepted versio

Calibrating CIV-based black hole mass estimators

We present the single-epoch black hole mass estimators based on the CIV (1549 A) broad emission line, using the updated sample of the reverberation-mapped AGNs and high-quality UV spectra. By performing multi-component spectral fitting analysis, we measure the CIV line widths (FWHM_CIV) and line dispersion (sigma_CIV) and the continuum luminosity at 1350 A (L_1350) to calibrate the CIV-based mass estimators. By comparing with the Hbeta reverberation-based masses, we provide new mass estimators with the best-fit relationships, i.e., M_BH \propto L_1350 ^ (0.50+-0.07) sigma_CIV ^2 and M_BH \propto L_1350 ^ (0.52+-0.09) FWHM_CIV ^ (0.56+-0.48). The new CIV-based mass estimators show significant mass-dependent systematic difference compared to the estimators commonly used in the literature. Using the published Sloan Digital Sky Survey QSO catalog, we show that the black hole mass of high-redshift QSOs decreases on average by ~0.25 dex if our recipe is adopted.Comment: 12 pages, 7 figures, ApJ in press, figure revise

Modeling reverberation mapping data II: dynamical modeling of the Lick AGN Monitoring Project 2008 dataset

We present dynamical modeling of the broad line region (BLR) for a sample of five Seyfert 1 galaxies using reverberation mapping data taken by the Lick AGN Monitoring Project in 2008. By modeling the AGN continuum light curve and H$\beta$ line profiles directly we are able to constrain the geometry and kinematics of the BLR and make a measurement of the black hole mass that does not depend upon the virial factor, $f$, needed in traditional reverberation mapping analysis. We find that the geometry of the BLR is generally a thick disk viewed close to face-on. While the H$\beta$ emission is found to come preferentially from the far side of the BLR, the mean size of the BLR is consistent with the lags measured with cross-correlation analysis. The BLR kinematics are found to be consistent with either inflowing motions or elliptical orbits, often with some combination of the two. We measure black hole masses of $\log_{10}(M_{\rm\,BH}/M_\odot)=6.62^{+0.10}_{-0.13}$ for Arp 151, $7.42^{+0.26}_{-0.27}$ for Mrk 1310, $7.51^{+0.23}_{-0.14}$ for NGC 5548, $6.42^{+0.24}_{-0.18}$ for NGC 6814, and $6.99^{+0.32}_{-0.25}$ for SBS 1116+583A. The $f$ factors measured individually for each AGN are found to correlate with inclination angle, although not with $M_{\rm\,BH}$, $L_{5100}$, or FWHM/$\sigma$ of the emission line profile.Comment: 21 pages, 24 figures, 3 tables, Accepted for publication in MNRAS, corrected masses for NGC 5548 and NGC 6814 in the abstrac

?????? ??? ????????? ???????????? ????????? ?????? ?????? ????????? ?????? ??????

????????? ????????? ????????? ?????? ????????? ????????? ??????????????? ????????? ??? ?????? ???????????? ?????? ??????????????? ?????? ????????? ?????? ??????. ????????? ????????? ??????????????? ?????? ????????? ???????????? ???????????? ?????? ????????? ?????? ?????? ????????? ???????????? ?????????, ?????? ??? ??????(O&M, Operation and Management) ??????????????? ????????? ????????? ?????? ??? ??????????????? ????????? ?????? ??????????????? ???????????? ??????. ????????? ????????? ?????? ?????? ?????? ??? ?????? ?????? ???, ?????? ??????????????? ????????? ???????????? ????????? ?????? ???????????? ???????????? ?????????, ???????????? ??????????????? ?????? ????????? ??? ?????? ????????? ??? ??? ??????. ????????? ?????? ??????????????? ?????? ???????????? ?????? ????????? ????????? ????????? ??????????????? ?????????????????? ?????? ???????????? ?????????. ????????? ??? ??????????????? (1) ????????? ???????????? ?????? ???????????? ????????? ???????????? ??????????????? ????????? ???????????? ????????? ????????????, (2) ????????? ????????? ????????? ???????????? ?????? NREL 5 MW??? ?????? ????????? ???????????? ???????????? ???, ???????????? ?????? ?????? ??? ?????? ???????????? ?????? ?????? ????????? ???????????? ??????????????????, ?????? ?????? ????????? ?????? ???????????? ????????? ???????????????.ope