Several Observed Features and Their Implications for Gamma-Ray-Loud Blazar PKS 1510-089

Abstract

The new results of spectrophotometry, and X-ray imaging spectroscopy observations for the high-polarization, radio-loud and Gev gamma-ray-loud blazar PKS 1510-089 have been observed. The main results show that: (1) A double-horned broad Hβ line in the spectrum of PKS 1510-089 has been discovered. The Hβ double-peaked emission profiles are impressive with the line asymmetry that the red peak seems to be higher than the blue peak; (2) The observation of X-rays, performed with the ACIS-S detector aboard the Chandra X-ray observatory, led to the discovery of a bending X-ray jet, coincident with the radio arcsecond jet of PKS 1510-089; (3) According to the reverberation mapping method and the empirical relation between the broad line region (BLR) size and the optical continuum luminosity at 5100 Å (the rest frame), we obtained the Virial mass of the central primary black hole, which coincides with our previous result by extremely rapid optical variability method. In addition, based on these new observational results mentioned above and the other previous observations, we have discussed the theoretical models for PKS 1510-089.

Periodicity Analysis of the Radio Curve of PKS 1510-089 and Implications for Its Central Structure

“…In the left panel of Figure 3, another minimum of V 2 m = 0.791 with f = 0.264 (larger than 0.25) is at period p 2 = 1.95 yr. Obviously, this is also in good agreement with the previous results of 1.84 yr found in the optical band by us in 2002 (Xie et al 2005) and the result mentioned above based on the 37 GHz data. From the right panel of Figure 3, one can see that there are three periods: 0.96 yr, 1.60 yr, and 2.89 yr.…”

“…643 days) with f = 0.580 (larger than 0.5); this implies that it is a very strong periodicity. It is consistent with the result of 672 ± 28 days (1.84 ± 0.1 yr) found by Xie et al (2005), which is the orbital periodicity of the SMBBH in the nucleus of PKS 1510-089. We note that p 2 = 2p 1 , which is consistent with the optical observations (Xie et al 2002(Xie et al , 2005.…”

“…One notes that the period of 0.92 ± 0.03 yr is in good agreement with the deep flux minima period of 0.92 ± 0.04 yr observed by us (Xie et al 2002 and confirmed by Wu et al (2005). The period of 1.82 ± 0.12 yr is in good agreement with the period of the deep flux minima of 1.84 ± 0.1 yr obtained in the optical band (Xie et al 2005). In addition, it is interesting to note that p 2 ≈ 2p 1 .…”

“…the main minimum; the primary black hole could also eclipse a secondary black hole, leading to one quasi-periodic deep flux minimum, i.e., the secondary minimum. In a word, the quasiperiodic deep flux minimum suggests that the orbital periodicity of the SMBBH system is ∼672 ± 28 days (1.84 ± 0.1 yr) (Xie et al 2005).…”

“…Several papers have been dedicated to observational and theoretical studies (e.g., Smith et al 1990;Xie et al 1997Xie et al , 1998bXie et al , 2002Xie et al , 2004Xie et al , 2005Wu et al 2005;Li & Fan 2007).…”