The Variable Mg ii Narrow Absorption Line Systems

Chen, Zhi-Fu; Qin, Huanchang; Gui, Run-Jin; Yi, Shuang-Xi; Chen, Zhe-Geng; Gao, Yan-Chun; Pang, Ting-Ting; Mo, Xiaohua

doi:10.3847/1538-4365/aba520

Cited by 4 publications

(2 citation statements)

References 59 publications

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“…Quasar outflows can produce a diverse range of absorption lines. Broad absorption lines (BALs) exhibit line widths exceeding 2000 km s −1 (e.g., Murray et al 1995;Elvis 2000;Capellupo et al 2011;He et al 2017), narrow absorption lines (NALs) present widths less than a few hundred kilometers per second (e.g., Chartas et al 2009;Hamann et al 2011Hamann et al , 2012Chen et al 2018cChen et al , 2020b, and Mini-BALs exhibit intermediate widths between NALs and BALs (e.g., Misawa et al 2007;Gibson et al 2009a;Horiuchi et al 2016;Xu et al 2018;Chen et al 2021). Optical spectroscopic surveys of quasars show that outflow NALs or Mini-BALs are more prevalent than outflow BALs.…”

Section: Introductionmentioning

confidence: 99%

Comprehensive Connection among the Quasars with Different Types of Outflow Absorption Lines

Peng,

Chen,

et al. 2024

ApJ

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It is commonly accepted that outflows from the central regions of quasars play a substantial role in regulating the global properties of the host galaxy. These outflows are typically detected through blueshifted absorption lines. However, the question remains whether outflows observed with different absorption line types indeed reflect the same environmental or evolutionary stage of the host galaxy. In this study, we use the Sloan Digital Sky Survey quasar catalog and employ the flux ratio of [O II] and [Ne V] emission lines as indicators to compare star formation rates (SFRs) within host galaxies of quasars exhibiting various outflow absorption line types: low-ionization broad absorption line (LoBAL), low-ionization Mini-BAL (LoMini-BAL), low-ionization narrow absorption line (LoNAL), high-ionization broad absorption line (HiBAL), high-ionization Mini-BAL (HiMini-BAL), and high-ionization narrow absorption line (HiNAL). Our findings indicate that the SFR of LoMini-BAL quasars is comparable to that of LoNAL quasars, somewhat less than that of LoBAL quasars, but markedly greater than that of HiBAL quasars. Furthermore, the SFR of HiMini-BAL quasars mirrors that of HiNAL or Non-abs (no associated absorption lines) quasars, but is significantly higher than that of HiBAL quasars. If we consider that differing absorption line types are indicative of the quasar evolution stage, our results propose an inclusive evolution sequence: LoBALs evolve into LoMini-BALs/LoNALs, then progress to HiBALs, and ultimately morph into HiMini-BALs/HiNALs/Non-abs. Concomitantly, the SFR within the host galaxies of quasars appears to decline noticeably nearing the LoNAL phase’s end and rejuvenates before the HiMini-BAL phase.

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Section: Introductionmentioning

confidence: 99%

Comprehensive Connection among the Quasars with Different Types of Outflow Absorption Lines

Peng,

Chen,

et al. 2024

ApJ

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“…The absorption lines with redshifts close to quasar systemic redshifts (z abs ≈ z em , associated absorption line) are likely formed in gaseous cloud physically associated with quasars themselves. Large samples (e.g., Shen & Menard 2012;Chen et al 2016;He et al 2017;Chen et al 2018aChen et al , 2018bChen et al , 2020Chen et al , 2022b of associated absorption lines have been available through systematically analyzing the quasar spectra from the Sloan Digital Sky Survey (SDSS; York et al 2000), which can often be used to comprehend the gas content of quasar systems along sight lines. The major shortcoming of associated absorption lines along quasar sight lines is that they cannot provide any information of gas content located on the transverse direction of quasars.…”

Section: Introductionmentioning

confidence: 99%

The Study of the Circumgalactic Medium with Quasar Pairs

Chen¹,

Qin²,

Cai³

et al. 2023

ApJS

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We have collected 10,025 foreground–background quasar pairs with projected distances d p < 500 kpc from the large quasar catalog of the Sloan Digital Sky Survey DR16Q. We investigate the properties of the Mg ii absorption lines with W r > 0.15 Å around foreground quasars, including both the line of sight (LOS; of foreground quasars) and transverse (TRA; perpendicular to the LOS) absorptions. Both the equivalent width (the correlation coefficient ρ = −0.915 and the probability P < 10−4 of no correlation) and incident rate (ρ = −0.964 and P < 10−6) of TRA Mg ii absorption lines are obviously anticorrelated with projected distance. The incident rate of TRA Mg ii absorption lines is obviously (>4σ) greater than that of LOS Mg ii absorption lines at projected distances d p < 200 kpc, while the TRA and LOS Mg ii both have similar (<3σ) incident rates at scales d p > 200 kpc. The anisotropic radiation from quasars would be the most possible interpretation for the anisotropic absorption around quasars. This could also indicate that the quasar radiation is not obviously impacting the gas halos of quasars at scales d p > 200 kpc.

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Narrow absorption line outflow in Seyfert 1 galaxy J1429+4518: outflow’s distance from the central source and its energetics

Dehghanian,

Arav,

Byun

et al. 2023

Monthly Notices of the Royal Astronomical Society

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In the Hubble Space Telescope/Cosmic Origins Spectrograph spectrum of the Seyfert 1 galaxy 2MASX J14292507+4518318, we have identified a narrow absorption line outflow system with a velocity of −151 km s−1. This outflow exhibits absorption troughs from the resonance states of ions like C iv, N v, S iv, and Si ii, as well as excited states from C ii* and Si ii*. Our investigation of the outflow involved measuring ionic column densities and conducting photoionization analysis. These allow the total column density of the outflow to be estimated as log NH = 19.84 cm−2, its ionization parameter to be log UH = −2.0, and its electron number density to be log ne = 2.75 cm−3. These measurements enabled us to determine the mass-loss rate and the kinetic luminosity of the outflow system to be $\dot{M}$ = 0.22 $\mathrm{ M}_{\odot } \, \mathrm{ yr}^{-1}$ and $\log \dot{E_{\mathrm{ K}}}$ = 39.3 erg s−1, respectively. We have also measured the location of the outflow system to be at ∼275 pc from the central source. This outflow does not contribute to the active galactic nucleus (AGN) feedback processes due to the low ratio of the outflow’s kinetic luminosity to the AGN’s Eddington luminosity ($\dot{E_{\mathrm{ K}}}/{L_{\mathrm{ Edd}}}\approx 0.00025 {{\, \rm per\, cent}}$). This outflow is remarkably similar to the two bipolar lobe outflows observed in the Milky Way by XMM–Newton and Chandra.

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The Variable Mg ii Narrow Absorption Line Systems

Cited by 4 publications

References 59 publications

Comprehensive Connection among the Quasars with Different Types of Outflow Absorption Lines

Comprehensive Connection among the Quasars with Different Types of Outflow Absorption Lines

The Study of the Circumgalactic Medium with Quasar Pairs

Narrow absorption line outflow in Seyfert 1 galaxy J1429+4518: outflow’s distance from the central source and its energetics

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