Physical characterization of the FeLoBAL outflow in SDSS J0932+0840: Analysis of VLT/UVES observations

Doyee Byun; Gwen Walker; Kirk T. Korista; Manuel Bautista; Maryam Dehghanian; Mayank Sharma; Nahum Arav; Sasha Mintz

REVIEW 3 major objections 4 minor 1 cited by

Physical characterization of the FeLoBAL outflow in SDSS J0932+0840: Analysis of VLT/UVES observations

T0 review · 3 major / 4 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read This paper measures the FeLoBAL outflow in SDSS J0932+0840 and shows its kinetic luminosity is only about 5×10⁻⁵ L_Edd, far too weak to drive significant AGN feedback.

desk verdict A careful, honest FeLoBAL outflow analysis whose headline feedback conclusion is robust; the precise distance and energetics numbers hinge on one unbenchmarked Fe II oscillator strength. read the letter →

arxiv 2412.06929 v3 pith:OPQSE6G5 submitted 2024-12-09 astro-ph.GA

Mayank Sharma , Nahum Arav , Kirk T. Korista , Manuel Bautista , Maryam Dehghanian , Doyee Byun , Gwen Walker , Sasha Mintz This is my paper · ORCID

classification astro-ph.GA

keywords FeLoBALquasaroutflowsAGNfeedbackIIexcitedstatesphotoionizationmodelingVLT/UVESspectroscopyhydrogenionizationfrontSDSSJ0932+0840

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper characterizes the low-ionization iron outflow (FeLoBAL) system in the quasar SDSS J0932+0840 using a high-resolution VLT/UVES spectrum. By combining absorption-line column densities with photoionization models and Fe II excited-state ratios, the authors measure the outflow's total hydrogen column, ionization parameter, and number density, and from those derive its distance (~0.7 kpc), mass-loss rate (~43 solar masses per year), and kinetic luminosity. The central conclusion is that this outflow's kinetic luminosity is only about 5×10⁻⁵ of the Eddington luminosity, far below the ~5×10⁻³ needed for efficient AGN feedback, so this component cannot significantly shape its host galaxy. Along the way, the paper shows that in FeLoBAL outflows the electron density can be an order of magnitude below the hydrogen density because Fe II forms behind the hydrogen ionization front, so assuming a fully ionized plasma underestimates n_H and overestimates distance and energetics.

What carries the argument

The central diagnostic is the set of Fe II absorption troughs from the ground state and five excited metastable levels (385, 668, 863, 977, and 1873 cm⁻¹). Column-density ratios of these levels to the ground state are compared with Chianti collisional-excitation predictions for the electron density and with Cloudy photoionization models for the hydrogen density; the hydrogen ionization front is the structural feature that reconciles the two, since Fe II forms beyond the front where the electron density drops by roughly an order of magnitude. A critical input is the newly calculated oscillator strength of the Fe II 1901.78 Å ground-state transition, log(gf) = −3.1 ± 0.3, computed with the Autostructure code; this weak transition is the only direct anchor for the ground-state Fe II column, and the paper propagates its uncertainty through the column density and all derived quantities.

What would settle it

Measure the Fe II 1901.78 Å oscillator strength in the laboratory or with an independent high-precision atomic calculation; if it disagrees with log(gf) = −3.1 by more than the quoted ~0.3 dex, the derived ground-state Fe II column, the photoionization solution, n_H, and the distance R would all shift. A complementary test is to detect this transition in another FeLoBAL spectrum where the Fe II column is independently anchored and check whether the same gf reproduces the observed column density.

Watch

Extended reading notes

Core claim

For the v ≈ −720 km s⁻¹ system S2 in SDSS J0932+0840, the authors establish log N_H = 21.47 cm⁻², log U_H = −2.4, and log n_H = 4.8 cm⁻³, placing the outflow at R = 0.7 kpc from the central source. The Fe II excited-state population gives an electron density consistent with the Cloudy-predicted effective value behind the ionization front (log n_e = 3.42 from Chianti versus 3.51 effective from Cloudy), validating the density solution. With v = −720 km s⁻¹ and a covering fraction of 0.2, the mass outflow rate is 43 M_sun yr⁻¹ and the kinetic luminosity is 0.7×10⁴³ erg s⁻¹, i.e. 0.5×10⁻⁴ L_Edd, below the feedback threshold. The paper also reevaluates four previously studied FeLoBAL outflows and finds that neglecting the cloud's physical structure overestimated the distance of J1321-0041 by about 300%.

Load-bearing premise

The density, distance, and energetics all hinge on the newly computed oscillator strength of the Fe II 1901.78 Å transition (log gf = −3.1 ± 0.3); if that atomic value is wrong, the Fe II ground-state column and everything derived from it—n_H, R, mass-flow rate, and kinetic luminosity—moves with it.

Editorial extensions

If this is right

The kinetic luminosity of this component (~0.7×10⁴³ erg s⁻¹, or 0.5×10⁻⁴ L_Edd) is far below the ~5×10⁻³ L_bol threshold for efficient feedback, so S2 is not a significant AGN feedback agent.
In FeLoBAL outflows, density diagnostics based on excited Fe II must account for the hydrogen ionization front; using the fully ionized approximation n_e ≈ 1.2 n_H underestimates n_H and overestimates distance and energetics.
Applying the corrected treatment to previous FeLoBAL studies changes distances: for J1321-0041 the distance drops from about 2.5 kpc to about 0.64 kpc, and its energy budget changes accordingly.
The independently measured n_e (log n_e = 3.42) and n_H (log n_H = 4.8) solutions are consistent once the cloud's internal structure is modeled, supporting the photoionization solution and the derived outflow location.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

The hand-optimized 1901.78 Å oscillator strength is the load-bearing atomic input; a laboratory measurement or independent high-precision calculation of log(gf) for that transition would directly test whether the Fe II column, n_H, and the distance to S2 are correct.
The weak-feedback conclusion applies only to system S2; the higher-velocity BAL components in J0932+0840, whose Al III absorption varies between epochs, could still carry significant energy and deserve similar density diagnostics.
The cloud-structure correction could be folded into large-sample FeLoBAL spectral-synthesis analyses, potentially revising the distances and energy budgets of many previously published outflows.
A direct observational test is to search for the Fe II 1901.78 Å trough in other FeLoBAL spectra where the Fe II column is anchored by different transitions and check whether the same gf reproduces the column density.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

Worth reading. This is a careful single-object FeLoBAL analysis with an unusually honest error budget. The genuinely new pieces are the first high-resolution characterization of the S2 outflow in J0932+0840, the rare detection of the Fe II 1901.78 Å ground-state transition, and the physical-structure argument that ne ≈ 1.2 nH fails for FeLoBALs because most Fe II forms beyond the hydrogen ionization front. That methodological point is the most useful part of the paper, and the reanalysis of four previously published FeLoBALs—where J1321-0041's distance changes by ~300%—shows it has teeth beyond this one object.

The distance and energetics results are derived cleanly: column densities from unsaturated lines with AOD and power-law models, a well-constrained (NH, UH) solution from many ions, and independent density estimates from CHIANTI and Cloudy that agree. The feedback conclusion—Ekin/LEdd near 1e-4, far below the 5e-3 Hopkins & Elvis threshold—is robust. Even a 0.3-dex error in the gf moves R by only a factor of about two, which does not change the qualitative answer.

The soft spot is exactly where the reader and the stress-test put it: the Fe II 1901.78 Å gf from Autostructure, with manual orbital optimization because the LS and jj optimizations diverge for the 3d7 a4F and 3d6 4s a6D separation. That transition anchors the Fe II ground-state column, which feeds the photoionization solution and every excited-to-ground ratio used for nH. The calculation is credible but unbenchmarked, and neither the atomic data nor the wrapper code are released. I would also note that the CHIANTI-versus-Cloudy agreement is not an independent validation of the gf, since both use the same measured N(ground) as the ratio denominator—it validates the density diagnostic chain, not the oscillator strength. That is a real limitation, but not a fatal one: the qualitative feedback verdict is unaffected, and the paper flags the uncertainty itself.

Minor quibbles: the adopted redshift from Mg II rather than the 1900 blend is a defensible choice but worth a sensitivity check, and Omega = 0.2 is a crude but standard assumption. Neither threatens the conclusions.

This is for the quasar-outflow and FeLoBAL community. It deserves a serious referee. My recommendation: send it to peer review, and ask the authors to release the atomic data or benchmark the gf against an independent calculation before final acceptance.

Referee Report

3 major / 4 minor

Summary. The paper analyzes the VLT/UVES spectrum of the quasar SDSS J0932+0840, focusing on the narrow outflow system S2 at v ≈ -720 km/s. From unsaturated Fe II and other ionic transitions, the authors derive column densities, then use Cloudy photoionization modeling to obtain log N_H = 21.47 (+0.17/-0.16) cm^-2 and log U_H = -2.4 (+0.4/-0.5). Fe II excited-state ratios are used with CHIANTI to infer log n_e = 3.42 (+0.65/-0.46) cm^-3 and with Cloudy to infer log n_H = 4.8 cm^-3, and the agreement between the two is presented as a consistency check. Combining these gives R = 0.7 (+0.9/-0.4) kpc, Mdot = 43 (+65/-26) M_sun/yr, and Ekin ~ 0.7 x 10^43 erg/s, about 0.5 x 10^-4 of L_Edd. The paper concludes that this outflow is not powerful enough to contribute significantly to AGN feedback. The analysis also includes variability study between two SDSS epochs and a re-evaluation of distances/energetics for four previously published FeLoBAL outflows.

Significance. If the derived parameters are reliable, this is a valuable addition to the rare sample of FeLoBAL outflows with high-resolution spectroscopy and multi-ion density diagnostics. The paper's strengths are the use of unsaturated Fe II transitions, the explicit treatment of the cloud's internal structure (H I ionization front), and the quantitative consistency between independent CHIANTI and Cloudy density analyses. The central qualitative conclusion, that this outflow has a kinetic luminosity far below the ~5e-3 L_Edd threshold for efficient feedback, is robust even to plausible errors in the atomic data. However, the quantitative results (N_H, U_H, n_H, R, Mdot, Ekin) rest on a single theoretically computed oscillator strength for Fe II 1901.78 Å, which is not benchmarked externally, and this limits the strength of the paper's parameter claims.

major comments (3)

[Sect. 3.3 and Table 1] A 0.3 dex error in the Fe II gf would shift R by roughly a factor of two through Eq. (5) and would move the quantitative parameters outside the quoted uncertainties, even though the qualitative feedback conclusion would remain unchanged.
[Sects. 4.1-4.3 and Fig. 7] A third, independent constraint on n_H (for example, from an ion with a different ground-state anchor, or from a separate atomic calculation for a second Fe II line) would strengthen the density claim. Without it, the quoted n_H error bar of +/-0.52 dex may underestimate the true systematic uncertainty.
[Sect. 3.4 and Fig. 5] This is a minor-to-moderate issue but directly relevant to the error bars of the headline results; it can be addressed with a small addition.

minor comments (4)

[Throughout] There are frequent typographical errors: 'redshfit' (Sect. 2.2), 'di fferent' (multiple places), 'eclipse' for 'ellipse' (Sect. 3.4, Fig. 5 caption), and 'converse' for 'convergence' (Sect. 3.3). The manuscript would benefit from a careful proofreading pass.
[Sect. 4.2 and Table 3] The adopted value log n_H = 4.80 (+0.60/-0.52) cm^-3 appears first in Section 4.2 with a best-fit value of only 4.8 and no error bar; the error bar appears later in Table 3 and in the summary. Please give the error on the best-fit n_H in Section 4.2 where the χ² minimization is described.
[Sect. 5.1] The statement that the error on the SED scaling is +/-10% (4.52 +/- 0.45 x 10^56 s^-1) is not justified in the text; please state the source of this uncertainty (e.g., continuum fitting error or SDSS photometric error).
[Sect. 6.2 and Table 4] Table 4 re-evaluates distances and energetics for four previous FeLoBAL studies, but the underlying physical parameters (N_H, U_H) are taken from those papers at face value. The text should note that any systematic biases in the original photoionization solutions are carried over into the re-evaluation.

Circularity Check

0 steps flagged · score 2.0 of 10

No material circularity: the outflow energetics follow from a self-contained photoionization and density analysis; the unbenchmarked Fe ii 1901.78 Å oscillator strength is a systematic uncertainty, not a circular step.

full rationale

The paper's derivation chain is self-contained. Ionic columns are obtained from unsaturated UVES troughs via Eq. (1), with the Fe ii ground-state column anchored by a newly computed Autostructure gf (Sect. 3.3). That gf is a parameter-free atomic calculation with a stated CI expansion and manually optimized orbitals; it is not fitted to the outflow, and the paper explicitly flags its uncertainty: 'This rarity means, however, that the oscillator strength value for the transition remains poorly constrained by observations and is prone to uncertainties.' The (NH, UH) solution (log NH = 21.47, log UH = -2.4) is found by matching Cloudy grids to the measured total ionic columns (Fig. 5), not by inverting any target quantity. The electron and hydrogen densities are modeled independently: CHIANTI level-population ratios give log ne = 3.42, while Cloudy self-consistent photoionization models give log nH = 4.8; the agreement (log ne,eff = 3.51) is presented by the paper as a consistency check, not as a prediction. Both fits use the same observed excited-to-ground column ratios, so the agreement does not independently validate the gf, but neither quantity is defined in terms of the other by construction. R, Mdot, and Ekin then follow from Eqs. (4), (5), (7), and (8) with the HE0238 SED (external empirical data) and a Mg ii-based MBH. The only self-citations are the SED and the Byun et al. FeLoBAL studies re-analyzed in Sect. 6.2; these are external datasets or independent calculations and do not carry the central result. A gf error would propagate through N(Fe ii), UH, nH, and R, making the quoted parameters hostage to that atomic calculation, but that is a correctness and robustness risk, not circularity by construction.

Assumptions & free parameters 2 free parameters · 6 assumptions · 0 invented entities

The analysis rests on standard photoionization and atomic-physics tools. The most fragile inputs are the theoretical Fe II gf value and the adopted HE0238 SED; both are flagged as uncertain in the paper. The covering factor is an explicit geometrical assumption.

free parameters (2)

Covering factor Omega = 0.2
Assumed from the fraction of quasars showing C IV BALs (Sect. 5.3). Scales Mdot and Ekin linearly; the feedback conclusion is robust for Omega up to 1.
Fe II 1901.78 Angstrom oscillator strength = log(gf) = -3.1 +/- 0.3
From Autostructure calculation with manual orbital optimization (Sect. 3.3). Sets the Fe II ground-state column density and affects the density diagnostics and photoionization solution.

assumptions (6)

domain assumption The HE0238-1904 SED represents the ionizing SED of J0932+0840.
Used for photoionization modeling and to compute QH (Sects. 3.4 and 5.1); a different SED shape would change UH and R.
domain assumption Solar elemental abundances in the outflow.
Cloudy models assume solar abundance (Sect. 3.4); the paper excludes Co and Zn because abundance uncertainties affect their ionization structure.
domain assumption Plane-parallel slab geometry with constant nH for the modeled cloud.
Cloudy models treat the outflow as a plane-parallel slab (Sect. 3.4); real outflows can have more complex geometry.
domain assumption Collisional excitation dominates the Fe II excited-state populations.
CHIANTI analysis assumes collisional excitation (Sect. 4.1); the paper argues fluorescence is not significant for Fe II, unlike Ni II.
domain assumption Mg II virial mass estimator provides the black hole mass.
Eq. (6) from Bahk et al. (2019) with a manually fit Mg II FWHM (Sect. 5.2); affects Ledd and the feedback ratio.
domain assumption Redshift z = 2.308 from Mg II emission is correct.
Sect. 2.2; disagrees with z = 2.341 from the 1900 blend (Hewett and Foltz 2003); influences the velocity scale and component identification.

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Cite this review

Pith. "Pith review of Physical characterization of the FeLoBAL outflow in SDSS J0932+0840: Analysis of VLT/UVES observations." pith.science (2026). https://pith.science/paper/OPQSE6G5

@misc{pith2026241206929,
  author       = {Pith},
  title        = {Pith review of: Physical characterization of the FeLoBAL outflow in SDSS J0932+0840: Analysis of VLT/UVES observations},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/OPQSE6G5}},
  note         = {Machine review of arXiv:2412.06929}
}

abstract

Context: The study of quasar outflows is essential in understanding the connection between active galactic nuclei (AGN) and their host galaxies. We analyze the VLT/UVES spectrum of quasar SDSS J0932+0840 and identify several narrow and broad outflow components in absorption, with multiple ionization species including Fe II, which puts it among a rare class of outflows known as FeLoBALs. Aims: We study one of the outflow components to determine its physical characteristics by determining the total hydrogen column density, ionization parameter and the hydrogen number density. Through these parameters, we aim to obtain the distance of the outflow from the central source, its mass outflow rate and kinetic luminosity, and to constrain the contribution of the outflow to AGN feedback. Methods: We obtain the ionic column densities from the absorption troughs in the spectrum, and use photoionization modeling to extract the physical parameters of the outflow, including the total hydrogen column density and ionization parameter. The relative population of the observed excited states of Fe II is used to model the hydrogen number density of the outflow. Results: We use the Fe II excited states to model the electron number density ($n_e$) and hydrogen number density ($n_H$) independently and obtain $n_e$ $\simeq$ $10^{3.4}$ cm$^{-3}$ and $n_H$ $\simeq$ $10^{4.8}$ cm$^{-3}$. Our analysis of the physical structure of the cloud shows that these two results are consistent with each other. This places the outflow system at a distance of $0.7_{-0.4}^{+0.9}$ kpc from the central source, with mass flow rate ($\dot{M}$) of $43^{+65}_{-26}$ $M_\odot$ yr$^{-1}$ and kinetic luminosity ($\dot{E_k}$) of $0.7^{+1.1}_{-0.4}$ $\times$ $10^{43}$ erg s$^{-1}$.

Figures

Figures reproduced from arXiv: 2412.06929 by the authors.

**Figure 1.** Non-normalized SDSS spectra of J0932+0840 (2012 epoch). The flux density (Fλ) is shown in black, and the error is plotted in gray. 9050 9100 9150 9200 9250 9300 9350 9400 9450 Observed Wavelength (Å) 0.0 0.5 1.0 1.5 2.0 2.5 Normalized Flux Density Mg II 2799 Å [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗

**Figure 2.** Gaussian model fit for the Mg ii 2799 emission feature (shown in red). Due to high absorption, the data points for the fit were selected manually. The dashed red line marks the centroid of the best-fit model we used to determine the redshift of the quasar. The dashed blue line shows the continuum level. The error on the flux is shown in gray. ΛCDM cosmology with h = 0.677, Ωm = 0.310 and ΩΛ = 0.690 (Planck Collabora… view at source ↗

**Figure 3.** Normalized UVES spectrum of J0932-0840. Important features and multiplets are marked in blue, and the identified absorp [PITH_FULL_IMAGE:figures/full_fig_p003_3.png] view at source ↗

Figures from the paper (7 more)

**Figure 4.** Figure 4: Identified Fe ii troughs for outflow system S2. The histograms show the VLT/UVES spectra in velocity space, and the corresponding dashed curves show the modeled Gaussian for the absorption. The model is based on the 1278 Å transition, and its template with fixed centro…

**Figure 5.** Figure 5: log NH vs. log UH phase-space plot, with constraints based on the measured total ionic column densities (sum of the column densities of the ground state and all the observed excited states). The measurements are shown as solid curves, and the dashed curves show lower l…

**Figure 6.** Figure 6: The various excited levels constrain log(ne) to be between 3.1 and 3.75 [cm−3 ]. We determined its weighted mean using the method described by Barlow (2004) and obtained the error using the procedure described in Appendix A. This resulted in log(ne) = 3.42+0.65 −0.46. …

**Figure 7.** Figure 7: Excited-state to ground-state ratios for Fe [PITH_FULL_IMAGE:figures/full_fig_p009_7.png]

**Figure 8.** Figure 8: Physical structure of the photoionized cloud vs. the to [PITH_FULL_IMAGE:figures/full_fig_p009_8.png]

**Figure 9.** Figure 9: Spectral region around the Al iii BAL as observed in the 2003 (in red) and 2012 spectra (in blue). The troughs corresponding to our main outflow system at v ≈ − 700 km s −1 are marked with a dashed black line. We chose this spectral region as it shows the most noticea…

**Figure 10.** Figure 10: Change in the column density of Si ii due to the increase by a factor of 2 in the ionizing flux for clouds with a different total hydrogen column density (NH). For clouds that did not form the H i ionization front (log(NH) ≲ 20.5 [cm−2 ]), the variation in column dens…

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Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

How massive and clumpy must a quasar wind be to create emission line blueshifts?
astro-ph.GA 2026-07 conditional novelty 6.0 of 10

Blueshifted C IV emission in quasars requires wind mass-loading ϵ_w/f_V ∼ 50, disfavouring smooth disc winds in favour of clumpy or ambient-swept outflows.

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Works this paper leans on

89 extracted references · 72 canonical work pages · cited by 1 Pith paper

[1]

, " * write output.state after.block = add.period write newline

ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 ...
[2]

write newline

" write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....
[3]

2013, MNRAS, 436, 3286

Arav, N., Borguet, B., Chamberlain, C., Edmonds, D., & Danforth, C. 2013, MNRAS, 436, 3286

2013
[4]

S., Becker, R

Arav, N., Brotherton, M. S., Becker, R. H., et al. 2001 a , ApJ, 546, 140

2001
[5]

2015, A&A, 577, A37

Arav, N., Chamberlain, C., Kriss, G., et al. 2015, A&A, 577, A37

2015
[6]

T., et al

Arav, N., De Kool, M., Korista, K. T., et al. 2001 b , ApJ, 561, 118

2001
[7]

A., et al

Arav, N., Kaastra, J., Kriss, G. A., et al. 2005, ApJ, 620, 665

2005
[8]

2018, ApJ, 857, 60

Arav, N., Liu, G., Xu, X., et al. 2018, ApJ, 857, 60

2018

Show all 89 references

[9]

2008, ApJ, 681, 954

Arav, N., Moe, M., Costantini, E., et al. 2008, ApJ, 681, 954

2008
[10]

2011, Computer Physics Communications, 182, 1528

Badnell, N. 2011, Computer Physics Communications, 182, 1528

2011
[11]

2019, ApJ, 875, 50

Bahk, H., Woo, J.-H., & Park, D. 2019, ApJ, 875, 50

2019
[12]

2004, arXiv preprint physics/0401042

Barlow, R. 2004, arXiv preprint physics/0401042

2004 arXiv
[13]

A., Dunn, J

Bautista, M. A., Dunn, J. P., Arav, N., et al. 2010, ApJ, 713, 25

2010
[14]

A., Peng, J., & Pradhan, A

Bautista, M. A., Peng, J., & Pradhan, A. K. 1996, ApJ v. 460, p. 372, 460, 372

1996
[15]

Begelman, M. C. & Nath, B. B. 2005, MNRAS, 361, 1387

2005
[16]

Begelman , M. C. & Ruszkowski , M. 2005, Philosophical Transactions of the Royal Society of London Series A, 363, 655

2005
[17]

C., Edmonds, D., Arav, N., Dunn, J., & Kriss, G

Borguet, B. C., Edmonds, D., Arav, N., Dunn, J., & Kriss, G. A. 2012, ApJ, 751, 107

2012
[18]

& Scannapieco, E

Br \"u ggen, M. & Scannapieco, E. 2009, MNRAS, 398, 548

2009
[19]

Byun, D., Arav, N., & Hall, P. B. 2022 a , ApJ, 927, 176

2022
[20]

Byun, D., Arav, N., & Hall, P. B. 2022 b , MNRAS, 517, 1048

2022
[21]

2024 a , A&A, 684, A158

Byun, D., Arav, N., Sharma, M., Dehghanian, M., & Walker, G. 2024 a , A&A, 684, A158

2024
[22]

2024 b , A&A, 684, A158

Byun, D., Arav, N., Sharma, M., Dehghanian, M., & Walker, G. 2024 b , A&A, 684, A158

2024
[23]

2022 c , MNRAS, 516, 100

Byun, D., Arav, N., & Walker, A. 2022 c , MNRAS, 516, 100

2022
[24]

M., Hamann, F., Shields, J

Capellupo, D. M., Hamann, F., Shields, J. C., Halpern, J. P., & Barlow, T. A. 2013, MNRAS, 429, 1872

2013
[25]

2023, RMxAA, 59, 327

Chatzikos , M., Bianchi , S., Camilloni , F., et al. 2023, RMxAA, 59, 327

2023
[26]

2021, ApJ, 907, 84

Chen, C., Hamann, F., Ma, B., & Murphy, M. 2021, ApJ, 907, 84

2021
[27]

P., Naab, T., et al

Choi, E., Ostriker, J. P., Naab, T., et al. 2017, ApJ, 844, 31

2017
[28]

M., Dabbieri, C., et al

Choi, H., Leighly, K. M., Dabbieri, C., et al. 2022 a , ApJ, 936, 110

2022
[29]

M., Terndrup, D

Choi, H., Leighly, K. M., Terndrup, D. M., et al. 2022 b , ApJ, 937, 74

2022
[30]

M., Terndrup, D

Choi, H., Leighly, K. M., Terndrup, D. M., Gallagher, S. C., & Richards, G. T. 2020, ApJ, 891, 53

2020
[31]

P., Gan, Z., et al

Ciotti, L., Ostriker, J. P., Gan, Z., et al. 2022, ApJ, 933, 154

2022
[32]

2023, MNRAS, 523, 2409

Cochrane, R., Angl \'e s-Alc \'a zar, D., Mercedes-Feliz, J., et al. 2023, MNRAS, 523, 2409

2023
[33]

Dai, X., Shankar, F., & Sivakoff, G. R. 2012, ApJ, 757, 180

2012
[34]

H., et al

de Kool, M., Arav, N., Becker, R. H., et al. 2001, ApJ, 548, 609

2001
[35]

H., Arav, N., Gregg, M

de Kool, M., Becker, R. H., Arav, N., Gregg, M. D., & White, R. L. 2002 a , ApJ, 570, 514

2002
[36]

H., Gregg, M

de Kool, M., Becker, R. H., Gregg, M. D., White, R. L., & Arav, N. 2002 b , ApJ, 567, 58

2002
[37]

T., & Arav, N

de Kool, M., Korista, K. T., & Arav, N. 2002 c , ApJ, 580, 54

2002
[38]

M., & Young, P

Dere, K., Landi, E., Mason, H., Fossi, B. M., & Young, P. 1997, A&A Supplement Series, 125, 149

1997
[39]

P., Del Zanna, G., Young, P

Dere, K. P., Del Zanna, G., Young, P. R., Landi, E., & Sutherland, R. S. 2019, ApJ Supplement Series, 241, 22

2019
[40]

2005, Nature, 433, 604

Di Matteo, T., Springel, V., & Hernquist, L. 2005, Nature, 433, 604

2005
[41]

P., Bautista, M., Arav, N., et al

Dunn, J. P., Bautista, M., Arav, N., et al. 2010, ApJ, 709, 611

2010
[42]

2011, ApJ, 739, 7

Edmonds, D., Borguet, B., Arav, N., et al. 2011, ApJ, 739, 7

2011
[43]

2000, ApJ, 545, 63

Elvis, M. 2000, ApJ, 545, 63

2000
[44]

2010, MNRAS, 401, 1670

Fabjan, D., Borgani, S., Tornatore, L., et al. 2010, MNRAS, 401, 1670

2010
[45]

2006, ApJ, 644, 709

Gallagher, S., Brandt, W., Chartas, G., et al. 2006, ApJ, 644, 709

2006
[46]

& Brotherton, M

Ganguly, R. & Brotherton, M. S. 2008, ApJ, 672, 102

2008
[47]

J., Aldcroft, T

Green, P. J., Aldcroft, T. L., Mathur, S., Wilkes, B. J., & Elvis, M. 2001, ApJ, 558, 109

2001
[48]

B., Anderson, S

Hall, P. B., Anderson, S. F., Strauss, M. A., et al. 2002, ApJ Supplement Series, 141, 267

2002
[49]

B., Anosov, K., White, R., et al

Hall, P. B., Anosov, K., White, R., et al. 2011, MNRAS, 411, 2653

2011
[50]

& Sabra , B

Hamann , F. & Sabra , B. 2004, in Astronomical Society of the Pacific Conference Series, Vol. 311, AGN Physics with the Sloan Digital Sky Survey, 203

2004
[51]

Hewett, P. C. & Foltz, C. B. 2003, AJ, 125, 1784

2003
[52]

R., Hamann, F., Eracleous, M., et al

Hidalgo, P. R., Hamann, F., Eracleous, M., et al. 2012, arXiv preprint arXiv:1203.3830

2012 arXiv
[53]

Hopkins, P. F. & Elvis, M. 2010, MNRAS, 401, 7

2010
[54]

F., Murray, N., & Thompson, T

Hopkins, P. F., Murray, N., & Thompson, T. A. 2009, MNRAS, 398, 303

2009
[55]

F., Torrey, P., Faucher-Gigu \`e re, C.-A., Quataert, E., & Murray, N

Hopkins, P. F., Torrey, P., Faucher-Gigu \`e re, C.-A., Quataert, E., & Murray, N. 2016, MNRAS, 458, 816

2016
[56]

R., & Cottis, C

Knigge, C., Scaringi, S., Goad, M. R., & Cottis, C. E. 2008, MNRAS, 386, 1426

2008
[57]

T., Bautista, M

Korista, K. T., Bautista, M. A., Arav, N., et al. 2008, ApJ, 688, 108

2008
[58]

& Kriss, G

Krolik, J. & Kriss, G. 1996, ApJ v. 456, p. 909, 456, 909

1996
[59]

& Bell, B

Kurucz, R. & Bell, B. 1995, Atomic Line Data (RL Kurucz and B. Bell) Kurucz CD-ROM No. 23. Cambridge, 23

1995
[60]

M., Choi, H., DeFrancesco, C., et al

Leighly, K. M., Choi, H., DeFrancesco, C., et al. 2022, ApJ, 935, 92

2022
[61]

M., Terndrup, D

Leighly, K. M., Terndrup, D. M., Gallagher, S. C., Richards, G. T., & Dietrich, M. 2018, ApJ, 866, 7

2018
[62]

H., et al

Liao, S., Irodotou, D., Johansson, P. H., et al. 2024, MNRAS, stae1123

2024
[63]

B., Leighly, K

Lucy, A. B., Leighly, K. M., Terndrup, D. M., Dietrich, M., & Gallagher, S. C. 2014, ApJ, 783, 58

2014
[64]

1995, A&A (ISSN 0004-6361), vol

Lucy, L. 1995, A&A (ISSN 0004-6361), vol. 294, no. 2, p. 555-567, 294, 555

1995
[65]

A., & Korista, K

Moe, M., Arav, N., Bautista, M. A., & Korista, K. T. 2009, ApJ, 706, 525

2009
[66]

2007, A&A, 463, 513

Moll, R., Schindler, S., Domainko, W., et al. 2007, A&A, 463, 513

2007
[67]

K., Dai, X., Leighly, K

Morabito, L. K., Dai, X., Leighly, K. M., Sivakoff, G. R., & Shankar, F. 2011, ApJ, 737, 46

2011
[68]

2017, MNRAS, 468, 4539

Moravec, E., Hamann, F., Capellupo, D., et al. 2017, MNRAS, 468, 4539

2017
[69]

W., Kochanek, C., Morgan, N

Morgan, C. W., Kochanek, C., Morgan, N. D., & Falco, E. E. 2010, ApJ, 712, 1129

2010
[70]

T., Kacprzak, G

Murphy, M. T., Kacprzak, G. G., Savorgnan, G. A., & Carswell, R. F. 2019, MNRAS, 482, 3458

2019
[71]

1995, ApJ v

Murray, N., Chiang, J., Grossman, S., & Voit, G. 1995, ApJ v. 451, p. 498, 451, 498

1995
[72]

Osterbrock, D. E. & Ferland, G. J. 2006, Astrophysics Of Gas Nebulae and Active Galactic Nuclei (University science books)

2006
[73]

P., Choi, E., Ciotti, L., Novak, G

Ostriker, J. P., Choi, E., Ciotti, L., Novak, G. S., & Proga, D. 2010, ApJ, 722, 642

2010
[74]

1972, ApJ, Vol

Peebles, P. 1972, ApJ, Vol. 178, pp. 371-376 (1972), 178, 371

1972
[75]

Peterson, B. M. 1997, An introduction to active galactic nuclei (Cambridge University Press)

1997
[76]

2020, , 641, A6

Planck Collaboration , Aghanim , N., Akrami , Y., et al. 2020, , 641, A6

2020
[77]

A., Richards, G

Reichard, T. A., Richards, G. T., Hall, P. B., et al. 2003, AJ, 126, 2594

2003
[78]

Savage, B. D. & Sembach, K. R. 1991, ApJ, 379, 245

1991
[79]

& Rees , M

Silk , J. & Rees , M. J. 1998, , 331, L1

1998
[80]

Stone, R. B. & Richards, G. T. 2019, MNRAS, 488, 5916

2019
[81]

R., Hall, P

Trump, J. R., Hall, P. B., Reichard, T. A., et al. 2006, ApJ Supplement Series, 165, 1

2006
[82]

2003, ApJ, 599, 116

Vestergaard, M. 2003, ApJ, 599, 116

2003
[83]

M., Weymann , R

Voit , G. M., Weymann , R. J., & Korista , K. T. 1993, , 413, 95

1993
[84]

2022, MNRAS, 516, 3778

Walker, A., Arav, N., & Byun, D. 2022, MNRAS, 516, 3778

2022
[85]

2023, MNRAS, 523, 1104

Weinberger, R., Su, K.-Y., Ehlert, K., et al. 2023, MNRAS, 523, 1104

2023
[86]

J., Morris, S

Weymann, R. J., Morris, S. L., Foltz, C. B., & Hewett, P. C. 1991, ApJ, Part 1 (ISSN 0004-637X), vol. 373, May 20, 1991, p. 23-53., 373, 23

1991
[87]

2018, ApJ, 858, 39

Xu, X., Arav, N., Miller, T., & Benn, C. 2018, ApJ, 858, 39

2018
[88]

T., & Benn, C

Xu, X., Arav, N., Miller, T., Korista, K. T., & Benn, C. 2021, MNRAS, 506, 2725

2021
[89]

2019, ApJ Supplement Series, 242, 28

Yi, W., Brandt, W., Hall, P., et al. 2019, ApJ Supplement Series, 242, 28

2019

Pith tools

Reviewed August 11, 2026 · model on record in the stance chip above.

[1] [1]

, " * write output.state after.block = add.period write newline

ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 ...

[2] [2]

write newline

" write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....

[3] [3]

2013, MNRAS, 436, 3286

Arav, N., Borguet, B., Chamberlain, C., Edmonds, D., & Danforth, C. 2013, MNRAS, 436, 3286

2013

[4] [4]

S., Becker, R

Arav, N., Brotherton, M. S., Becker, R. H., et al. 2001 a , ApJ, 546, 140

2001

[5] [5]

2015, A&A, 577, A37

Arav, N., Chamberlain, C., Kriss, G., et al. 2015, A&A, 577, A37

2015

[6] [6]

T., et al

Arav, N., De Kool, M., Korista, K. T., et al. 2001 b , ApJ, 561, 118

2001

[7] [7]

A., et al

Arav, N., Kaastra, J., Kriss, G. A., et al. 2005, ApJ, 620, 665

2005

[8] [8]

2018, ApJ, 857, 60

Arav, N., Liu, G., Xu, X., et al. 2018, ApJ, 857, 60

2018