Quasar SDSS J091425.72+504854.9 to J145615.24+432217.3: Analysis of Broad Absorption Line Variability

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Q11 G3 Grier 2016

Quasar SDSS J091425.72+504854.9 (zem=2.341). This quasar was first reported by Grier et al. (2016). We adopted its three-epoch SDSS observations respectively on MJD=52247, 56326, and 56991. We detected four broad absorption systems (systems A to D) in C IV from all of the three spectra, of which only system D was also shown in Si IV. The CIV BAL in system A presented a velocity shift of v_shift≈754 km s−1 between the first two epoch observations, and that of v_shift≈-68 km s−1 between the last two epoch observations.

Q12 335 Joshi 2019, LL

Quasar SDSS J092345.19+512710.1 (zem=2.173). This quasar was first reported by Joshi et al. (2019). We adopted its three-epoch SDSS observations respectively on MJD=52252, 56607, and 57046. We detected two broad absorption systems (systems A and B) in C IV from all of the three spectra, of which system A was also shown in Si IV. The CIV and Si IV BALs in system A respectively presented a velocity shift of v_shift≈1377 km s−1 and v_shift≈1721 km s−1 between the first two epoch observations, and a velocity shift of v_shift≈344 km s−1 and v_shift≈137 km s−1 between the last two epoch observations.

Joshi et al. (2019) also detected these two BAL absorption systems in this quasar, and also found the deceleration in C IV and Si IV ions of system A from MJD 52252 to MJD 57046, while found no change in the velocity of system B. In LL2019 [Probing], we find that the C IV BAL in system B in this quasar can be resolved into NALs which show a sequence of line-locking signatures. These line-locking signatures imply that the actual deceleration of the outflow clouds driven by the radiation pressure is a possible cause for the velocity shift of system A.

Q13 371

Quasar SDSS J093552.97+495314.3 (zem=1.93). We adopted its two-epoch SDSS observations respectively on MJD=52641 and 55998. We detected three broad absorption systems (systems A to C) in C IV from both two-epoch spectra, of which only system C was also shown in Si IV. The CIV BAL in system A and system B respectively presented a velocity shift of v_shift≈-1905 km s−1 and v_shift≈-479 km s−1 between the two-epoch observations. In addition, we found that system C showed coordinated variability over large velocity intervals, and variable C IV/Si IV BALs, which offer evidence for the IC driven BAL variation.

Q14 380

Quasar SDSS J093846.82+302418.5 (zem=2.465). We adopted its two-epoch SDSS observations respectively on MJD=53415 and 56309. We detected two broad absorption systems (systems A and B) in C IV from both two-epoch spectra. This CIV BAL presented a velocity shift of v_shift≈-275 km s−1 between the two-epoch observations.

Q15 435

Quasar SDSS J095858.14+362318.9 (zem=2.671). We adopted its three-epoch SDSS observations respectively on MJD=52998, 55616, and 57450. We detected two broad absorption systems (systems A and B) in C IV and Si IV from all of the three spectra. The CIV BAL in system A presented a velocity shift of v_shift≈-206 km s−1 between the first two epoch observations, and that of v_shift≈-137 km s−1 between the last two epoch observations.

In addition, we found that: (1) the C IV absorption lines in both systems A and B showed coordinated variability over large velocity intervals, and (2) the C IV BALs show coordinated variable between systems A and B in the last two epochs. The above two discoveries offer evidence for the IC driven BAL variation.

Q16 528

Quasar SDSS J103641.48+184531.1 (zem=2.053). We adopted its two-epoch SDSS observations respectively on MJD=54175 and 56036. We detected two broad absorption systems (system A and B) in C IV from both two-epoch spectra, and system B was also shown in Si IV. The part of the CIV BAL in system A, system A2, presented a velocity shift of v_shift≈-481 km s−1 between the two-epoch observations.

Q17 650

Quasar SDSS J113048.45+225206.6 (zem=2.37). We adopted its two-epoch SDSS observations respectively on MJD=54178 and 56274. We detected one broad absorption system (system A) in C IV from both two-epoch spectra, and the system was also shown in Si IV.

Traditionally, C-A1 to C-A4 usually taken as a single BAL. However, in this source, it is evident that the EW variations and velocity shifts of the absorption lines only occur in the higher velocity portion (which we mark as A1 and A2). Therefore, we divide this BAL into four sub-components (namely A1, A2, A3, and A4) for further analysis. The systems A2, A3, and A4 were also presented in Si IV ion.

The CIV BALs in systems A1 and A2 respectively presented a velocity shift of v_shift≈482 km s−1 and v_shift≈334 km s−1 between the two-epoch observations. The Si IV BALs in systems A1 and A2 respectively presented a velocity shift of v_shift≈334 km s−1 and v_shift≈334 km s−1 between the two-epoch observations.

Q18 730

Quasar SDSS J115723.81+661416.0 (zem=2.216). We adopted its two-epoch SDSS observations respectively on MJD=52316 and 56667. We detected one broad absorption system (system A) in C IV from both two-epoch spectra. This CIV BAL presented a velocity shift of v_shift≈-686 km s−1 between the two-epoch observations.

Q19 764 LL2019

Quasar SDSS J120819.29+035559.4 (zem=2.023). We adopted its two-epoch SDSS observations respectively on MJD=52376 and 55633. We detected two broad absorption systems (systems A and B) in C IV from both two-epoch spectra. This CIV BAL presented a velocity shift of v_shift≈-960 km s−1 between the two-epoch observations.

In LL2019 [shift], we have reported this quasar on its two BALs. In that paper, we have found that: (1) the blended NALs within system B presented line-locking phenomena, which indicate that these outflow clouds are driven by a radiative force caused by resonance lines; (2) the coordinated strengthening of the NALs resolved from the BAL in system B and an obvious weakening of the continuum flux, which confirm the ionization change scenario as the most likely cause for the EW variations of the absorption lines (at least for system B) in this quasar. These two results convincingly reveal that the velocity shift of BAL system A may be caused by the actual line-of-sight acceleration of the outflow clouds driving by radiation pressure produced by the background light source.

Q20 1037

Quasar SDSS J140006.88+412142.5 (zem=2.75). We adopted its two-epoch SDSS observations respectively on MJD=52822 and 56090. We detected three broad absorption systems (system A to system C) in C IV from both two-epoch spectra, and the systems B2 and C also shown in Si IV. Traditionally, the system B usually taken as a single BAL. However, in this source, it is evident that the velocity shifts of absorption lines only occur in the higher velocity portion (which we mark as B1 and B2). Therefore, we divide this BAL into three sub-components (namely B1, B2, and B3) for further analysis. The systems B2 and C also presented in Si IV ion.

The CIV BAL in system A presented a velocity shift of v_shift≈-1302 km s−1 between the two observations. The systems B1 and B2 respectively presented velocity shifts of v_shift≈-618 km s−1 and v_shift≈-68 km s−1 between the two-epoch observations. The Si IV BAL in system B2 presented a velocity shift of v_shift≈-481 km s−1 between the two observations.

Q21 1042

Quasar SDSS J140058.79+260619.4 (zem=2.351). We adopted its two-epoch SDSS observations respectively on MJD=53852 and 56093. We detected two broad absorption systems (system A and B) in C IV from both two-epoch spectra, and the system A also shown in Si IV. The CIV and Si IV BALs in system A respectively presented a velocity shift of v_shift≈-481 km s−1 and v_shift≈-550 km s−1 between the two-epoch observations.

Q22 1145

Quasar SDSS J143821.60+393407.2 (zem=2.042). We adopted its two-epoch SDSS observations respectively on MJD=52797 and 56038. We detected two broad absorption systems (system A and B) in C IV from both two-epoch spectra, and the system B also shown in Si IV. The Si IV BAL in system B presented a velocity shift of v_shift≈892 km s−1 between the two-epoch observations.

Q23 1176

Quasar SDSS J145229.08+093204.9 (zem=2.471). We adopted its two-epoch SDSS observations respectively on MJD=53827 and 55986. We detected two broad absorption systems (system A and B) in C IV from both two-epoch spectra. The C IV BAL in system B presented a velocity shift of v_shift≈-1097 km s−1 between the two-epoch observation.

Although the △EW/ between two-epoch observation of these two C IV BALs do not meet our standard for EW variation, we can see from the spectra that the CIV BAL in system B has obvious absorption line strength features at 16000-17000 km s−1.

Q24 1187

Quasar SDSS J145615.24+432217.3 (zem=1.962). We adopted its three-epoch SDSS observations respectively on MJD=52734, 56098, and 57104. We detected two broad absorption systems (system A and B) in C IV from its three-epoch spectra, and the system B also shown in Si IV in the MJD 57104 spectrum. The C IV BAL in system A presented a velocity shift of v_shift≈-2472 km s−1 between the first two-epoch observations, and a velocity shift of v_shift≈-480 km s−1 between the last two-epoch observations.