Pith. sign in

REVIEW 4 major objections 7 minor 89 references

Massive star-forming galaxies carry roughly three times more warm OVI gas in their inner halos than quiescent galaxies of the same stellar mass, pointing to star formation—not halo mass—as the regulator of the warm circumgalactic medium at

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

At z≈0.43, massive star-forming galaxies host 3x more O VI in their inner halos than quiescent galaxies of the same stellar mass, with an O VI mass offset of ~1.5 dex, contradicting the virial-thermometer prediction.

T0 review reviewed 2026-08-01 challenge →

load-bearing objection Solid new dataset, but the SF–Q contrast and the cooling-flow interpretation are both softer than the abstract suggests. the 4 major comments →

arxiv 2607.19473 v1 pith:GN7L4E37 submitted 2026-07-21 astro-ph.GA

The GOLIATH Survey: OVI Absorption Reveals CGM Evolution through the Starburst-to-Quiescent Transition in Massive Galaxies

Derick Flores , Rongmon Bordoloi , Jason Tumlinson , J. Christopher Howk , Nicolas Lehner , Mary Rickel , Benjamin Oppenheimer , Joseph Burchett
show 7 more authors
Ahmed Shaban John O'Meara Andrew Fox J. Xavier Prochaska Simon Xinlin Wu Jack Higginson Robert A. Simcoe
This is my paper
classification astro-ph.GA
keywords circumgalactic mediumOVI absorptionstarburst galaxiesgalaxy quenchingmassive galaxiesgalaxy evolutionabsorption-line spectroscopywarm-hot gas
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The reading

The GOLIATH survey targets a rare population: massive, blue, starburst and post-starburst galaxies at an average redshift of 0.43, caught on the eve of quenching. Using ultraviolet spectra of background quasars, it measures OVI absorption from the warm-hot circumgalactic medium inside 0.6 times the virial radius. The central result is that these massive star-forming galaxies have OVI column densities about three times higher, and CGM OVI masses about 1.5 dex higher, than quiescent galaxies of the same stellar mass. The paper argues this breaks a long-standing degeneracy: at stellar masses above 10^11 solar masses, star-formation activity—not halo virial temperature—controls the warm oxygen reservoir. Because the OVI cooling time is only 10–100 million years, the reservoir must be continuously replenished by feedback, making OVI a short-timescale tracer of the starburst-to-quiescent transition.

Core claim

The survey fills a previously empty corner of the mass–star-formation plane: galaxies that are simultaneously massive (median log M*/M_sun ≈ 11.1) and actively forming stars. In the inner CGM (R/Rvir ≤ 0.6), star-forming galaxies in the log M*/M_sun = [11,12) bin exceed quiescent galaxies by a factor of ~3 in mean OVI column density and ~1.5 dex in total CGM OVI mass (log M_OVI/M_sun ≈ 7.3 versus ≈ 5.8), with covering fractions of 62.5% versus 24% at log N_OVI ≥ 14. OVI column density rises with both stellar mass and specific star-formation rate across the star-forming population, and the detected kinematic components remain gravitationally bound with velocity spreads up to ~1200 km/s. The a

What carries the argument

The central observable is the OVI doublet (1031, 1037 Å) absorption in far-ultraviolet quasar spectra, which traces collisionally ionized gas at T ≈ 10^5.5 K. The analysis rests on comparing inner-halo sightlines (R/Rvir ≤ 0.6) of mass-matched star-forming and quiescent galaxies, using two independent estimators of total CGM OVI mass: an empirical annular integration weighted by covering fraction, and a radial-profile beta-function fit with censored upper limits. Together these turn sparse pencil-beam sightlines into a census of warm oxygen per halo.

Load-bearing premise

The GOLIATH galaxies are classified as star-forming on the basis of SED-derived specific star-formation rates, but for four of the 18 OVI sightlines the sSFR is an upper limit below the adopted star-forming threshold, and two have color upper limits that do not prove blue colors; if those galaxies are actually quiescent or post-starburst contaminants, the high-mass covering fraction and the 1.5 dex OVI mass offset would shrink.

What would settle it

Obtain deep rest-optical emission-line spectroscopy for the four ambiguous GOLIATH systems (J1319+2728, J0956+2515, J0912+2450, J0958+3224) to measure firm sSFRs. If two or more classify as quiescent, the star-forming covering fraction at log N_OVI ≥ 14 drops from 62.5% toward the quiescent 24%, directly weakening the central contrast. A complementary test: measure OVI around a sample of spectroscopically confirmed massive starbursts with independent SFR indicators (e.g., H-alpha or mid-infrared) to see whether the ~3x enhancement persists.

Watch this falsifier. Get emailed when new claim-graph text bears on it.

If this is right

  • Massive star-forming galaxies at log M*/M_sun ≈ 11 keep a warm oxygen reservoir despite virial temperatures that should ionize OVI away, so halo temperature alone cannot explain the observed OVI bimodality.
  • The CGM OVI mass rises with stellar mass for star-forming galaxies (power-law slope ≈ 0.5) while declining for quiescent galaxies, so the star-forming—quiescent gap widens toward higher mass.
  • The ~10–100 Myr cooling time means OVI is a short-timescale feedback tracer; it should disappear quickly after quenching, before the galaxy's colors fully transition.
  • Current cosmological simulations underpredict the OVI budget in massive halos; reproducing these measurements may require higher oxygen yields or more efficient metal transport by feedback.
  • OVI absorption can be used to catch galaxies in the act of quenching, since the warm gas depletes much faster than the ~1 Gyr star-forming-to-quiescent transition.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The large scatter in GOLIATH column densities hints that some sightlines are already partially depleted; a larger sample of post-starburst galaxies could map the depletion curve and directly time the quenching event.
  • If the same trend holds at even higher masses, the most massive star-forming galaxies might show OVI masses approaching 10^7.5 M_sun, a testable prediction for future ultraviolet spectroscopy of rare hyper-luminous starbursts.
  • The bound kinematics suggest that outflows at this mass scale recycle gas within the halo rather than ejecting it; if so, the high OVI mass may be connected to metal retention, which could be tested by measuring the metallicity of the cool CGM phase.
  • Green-valley galaxies should show intermediate OVI covering fractions; targeted observations of this population could provide an independent check of the rapid-depletion picture.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

4 major / 7 minor

Summary. The paper presents the GOLIATH survey, an HST/COS program targeting the inner CGM of 18 massive (log M*/M_sun ≈ 11), ostensibly blue, starburst/post-starburst galaxies at z ≈ 0.43, and compares them with archival star-forming and quiescent samples. It reports that in the log M*/M_sun = [11,12) inner-CGM bin, star-forming galaxies have OVI column densities a factor of ~3 higher, CGM OVI masses ~1.5 dex higher, and covering fractions ~2.6 times higher (62.5% vs 24%) than quiescent galaxies of similar mass. The paper interprets this as evidence that feedback-driven radiative cooling, not virial temperature, regulates the warm CGM at high mass, and that OVI is a short-timescale tracer of quenching.

Significance. If the central contrast is robust, the survey fills a genuinely unoccupied region of the M*–SFR plane and directly discriminates between the virial-thermometer and feedback scenarios. The paper's strengths include new COS spectroscopy, joint Voigt-profile fitting with MCMC-derived uncertainties, treatment of non-detections as censored upper limits, and two independent OVI-mass estimators that agree with each other and with literature values at overlapping mass. However, the headline SF–quiescent contrast rests on a small number of GOLIATH sightlines whose star-forming classification is not robust, and on one sightline whose reported column density is internally inconsistent. These issues must be resolved before the strong abstract-level claims can be accepted.

major comments (4)
  1. [Table 1; §4.4] The central 62.5% vs 24% covering fraction and ~1.5 dex mass-offset claims depend on the binary sSFR cut at 10^-11 yr^-1 (Section 3.2). In the high-mass bin, four GOLIATH sightlines have sSFR upper limits at or below that cut: J1319+2728 (<−12.8), J0956+2515 (<−16.3), J0912+2450 (<−12.2), and J0958+3224 (−11.1+0.3−0.6). By the paper's own criterion the first three are quiescent and J0958 is at best marginal. Reclassifying them changes the high-mass SF covering fraction from 62.5% (5/8) to ~57% (4/7) or ~50% (4/8) and raises the quiescent mean, directly weakening the claimed factor-of-three contrast. Please report Prospector posterior probabilities and independent emission-line classifications for these systems, and rerun the Fisher exact test, covering fractions, and mass estimates under alternative classification choices.
  2. [Table 3; §4.5; Fig. 7] The most massive sightline J1319+2728 is reported inconsistently. The text assigns log N = 14.01 to the system associated with the primary galaxy, Table 3 lists the integrated column as 14.01 but tabulates five components including two at v ≈ −1765 and −1619 km/s whose linear sum is 14.65, and Fig. 7 labels log N = 14.65 integrated over ±2000 km/s. The Table 3 note says only components within −300 to +200 km/s are used, but this does not match the listed rows, and the figure caption quotes −200 to +300 km/s. Because J1319 is the most massive object and would fall in the quiescent high-mass bin, this inconsistency affects the quiescent covering fraction and mass estimates. Clarify the adopted velocity window and propagate a single value through all analysis.
  3. [§2; Table 1] The stated survey selection requires extremely blue galaxies with u−r < 1.65, but several Table 1 entries exceed this value (J1126+1204: 1.86; J1342−0053: 1.66; J1305+5301: 2.53; J1244+0755: 1.68; J1405+4704: 1.74), and others are upper limits (J1319+2728 <2.64; J0912+2450 <2.83) that do not by themselves prove blue colors. Because the sample definition underpins the claim that these are starburst/post-starburst systems, please clarify the color definition/redshift correction and discuss which sightlines actually satisfy the 'extremely blue' criterion.
  4. [§5.1; Fig. 10] The feedback-driven radiative cooling conclusion is currently supported by a visual comparison of component column densities and line widths with cooling curves. No quantitative test distinguishes the T≈5.5 K curve from the T≈6.0 K curve or from photoionization models, and the b-parameter uncertainties in Table 3 are large. Since the radiative-cooling interpretation is a headline claim (Abstract, Conclusion 3), add a statistical comparison that accounts for b uncertainties and upper limits, or soften the claim to 'consistent with, but not discriminating among, these scenarios.'
minor comments (7)
  1. [§4.4] The text states that all GOLIATH >3σ detections reside above log N_Th = 14.0, but J0958+3224 has log N = 13.97. Specify the threshold rounding convention or the exact counting rule used for the 62.5% covering fraction.
  2. [§4.2 vs Conclusions] The generalized Kendall's tau value is reported as τ = 0.191 in Section 4.2 and τ = 0.193 in the Conclusions. Unify the values and quote the same p-value throughout.
  3. [§4.3] The full-sample Kendall test is described as showing 'a small monotonic decrease' with τ = −0.068, which is confusing because the subsequent inner-CGM test gives a strongly positive τ = 0.393. Clarify that the sign reflects the R/Rvir selection effect and report both tests with consistent wording.
  4. [Appendix] Figure numbering is duplicated: the main-text Fig. 10 (OVI column density vs line width) and the Appendix spectra are all labeled 'Figure 10'. Renumber the appendix figures.
  5. [§3.1] The text refers to SDSS redshifts for 'J0906+015'; from the table this appears to be a typo for J0909+0121. Check all target names for consistency.
  6. [§2; Table 2] Section 2 says the sample comprises 20 sightlines with 12 new and 8 archival, while Table 2 lists N=18 for GOLIATH. Clarify that two archival sightlines (J1126+1204 and J1240+0949) lack OVI coverage and are excluded from the absorption analysis.
  7. [§4.6.3] The quiescent power-law fit is quoted as α = −0.28 with no uncertainty and appears to be driven by very few points. Report the number of sightlines/bins and the fit uncertainties, or present the quiescent relation as an upper envelope rather than a fitted power law.

Circularity Check

0 steps flagged

No circular derivation: OVI measurements are new and independent; the SF–Q contrast is a direct observable comparison.

full rationale

The paper's central claims rest on new HST/COS measurements of OVI column densities and covering fractions around GOLIATH galaxies, selected by color and stellar mass without prior knowledge of their CGM absorption. The SF–quiescent contrast at log M*/Msun ~ 11 is a direct comparison of measured column densities, covering fractions, and mass integrals; it is not derived from the theoretical models the paper discusses. The OVI mass estimates (Eq. 1-4) are standard re-expressions of the measured column densities and covering fractions, not fitted predictions. The comparison to the virial thermometer (Oppenheimer et al. 2016) and feedback-driven radiative cooling (Bordoloi et al. 2017) is qualitative and interpretive; these are external, published model predictions, and although some are co-authored by current paper authors, they are externally testable and not used as inputs to define the GOLIATH sample or measurements. The power-law fits in Sections 4 and 5 are descriptive, not predictions forced by construction. Robustness concerns—e.g., borderline sSFR classifications in Table 1 (J1319+2728, J0956+2515, J0912+2450, J0958+3224) and the choice of the log N = 14.0 covering-fraction threshold—are correctness or statistical issues, not circularity. No step in the derivation chain reduces to its own input by definition or by self-citation.

Axiom & Free-Parameter Ledger

7 free parameters · 8 axioms · 0 invented entities

The paper's central contrast depends on classification choices (sSFR threshold), halo-mass conversion (UniverseMachine), and interpretive assumptions (collisional ionization, gas density, cooling model) that are not independently measured in this work. No new physical entities are introduced; the OVI measurements themselves are data-grounded and external to the models.

free parameters (7)
  • Beta-profile parameters N0, rc, beta = not quoted in text; fitted per population (Eq. 3)
    The radial profile fitting (RPF) mass estimates integrate this beta model; the OVI mass values depend on these fitted parameters.
  • OVI column density falloff slope gamma = -0.6 ± 0.1 (star-forming detections)
    Power-law fit to log N_OVI vs log R/Rvir used to characterize the distribution and scatter.
  • SF OVI-mass power law (alpha, gamma) = alpha=0.52±0.04, gamma=1.06±0.40
    Fit to binned empirical OVI mass vs stellar mass for star-forming galaxies; used to claim a rising SF relation.
  • Quiescent OVI-mass power law (alpha, gamma) = alpha=-0.28, gamma=9.13
    Fit to binned quiescent OVI masses; reported without uncertainties, yet used to claim a declining quiescent relation.
  • sSFR star-forming threshold = 10^-11 yr^-1
    Binary classification of galaxies into star-forming/quiescent; drives the SF-Q comparison and the interpretation of the high-mass contrast.
  • Integration radius cutoffs = R/Rvir <= 0.6, 1.0, 1.5, 2.0, 3.0
    Choice of annular integration limits affects the total OVI mass values in the empirical method.
  • OVI detection and upper-limit window = 200 km/s at 3-sigma
    Non-detection upper limits depend on this window and threshold; the covering fractions and means depend on the resulting detections.
axioms (8)
  • standard math Flat LCDM with H0=70, OmegaM=0.3, OmegaLambda=0.7
    Assumed cosmology for distances and halo properties; stated in Section 1 and used throughout.
  • domain assumption UniverseMachine stellar-mass-halo-mass relation converts M* to Mhalo and Rvir
    R/Rvir and halo masses for all galaxies rely on this relation (Section 3.2); systematic errors in SHMR directly affect R/Rvir normalization and the inner-CGM selection.
  • domain assumption R200c used as virial radius
    Adopted following Bordoloi et al. 2024; affects all R/Rvir values and the R/Rvir <= 0.6 cuts.
  • domain assumption OVI-bearing gas is in collisional ionization equilibrium near T~10^5.5 K
    Central to the cooling-curve comparison and t_cool argument; the photoionization channel is acknowledged (Stern et al. 2016, 2019) but assumed subdominant.
  • domain assumption Gas density n_H ~ 10^-4 cm^-3 for the t_cool estimate
    The cooling time t_cool ~ 10-100 Myr quoted in Section 5.1 depends on this assumed density; it is not measured from the data.
  • domain assumption Absorption within ±1500 km/s of the galaxy redshift is associated with the target galaxy
    Used to associate OVI systems with target galaxies (Section 3.4); the J1319+2728 field shows this association is ambiguous in overdense environments.
  • domain assumption Bordoloi et al. 2017 radiative cooling model curves (N vs b at fixed T) apply to the observed components
    Figure 10 uses these curves to claim consistency with feedback-driven cooling; no quantitative goodness-of-fit is provided.
  • domain assumption Archival comparison samples are unbiased and mutually consistent after the R/Rvir <= 0.6 restriction
    The SF-Q contrast combines heterogeneous surveys (COS-Halos, COS-LRG, CGM2, CUBS, MUSEQuBES, etc.) with different selection functions and redshift ranges.

reviewed 2026-08-01 · how reviews work

0 comments
Cite this review

Pith. "Pith review of The GOLIATH Survey: OVI Absorption Reveals CGM Evolution through the Starburst-to-Quiescent Transition in Massive Galaxies." pith.science (2026). https://pith.science/paper/GN7L4E37

@misc{pith2026260719473,
  author       = {Pith},
  title        = {Pith review of: The GOLIATH Survey: OVI Absorption Reveals CGM Evolution through the Starburst-to-Quiescent Transition in Massive Galaxies},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/GN7L4E37}},
  note         = {Machine review of arXiv:2607.19473}
}
Share X Bluesky LinkedIn Reddit HN
abstract

We present the GOLIATH survey (Galaxies, Outflows, and the Lifecycle of Immense, Active, Transforming Halos), a study of the multiphase circumgalactic medium (CGM) of massive ($\langle\log M_\star/M_\odot\rangle \approx 11$), blue ($u-r < 1.65$) starburst and post-starburst galaxies at $\langle z\rangle \approx$ 0.43. This work characterizes the warm-hot CGM through OVI absorption in the inner halo ($R/R_{\rm vir} \leq 0.6$) of these rare systems. Across the star-forming population, OVI column density rises by nearly 1~dex from $\log M_\star/M_{\odot} \sim 8$ to $\sim 11.5$ and increases with specific star-formation rate (sSFR). Two GOLIATH galaxies with the highest sSFR show the strongest CGM OVI absorption ($\log N_{\rm O\,VI}[\rm cm^{-2}] \gtrsim 15$). In the $\log M_\star/M_{\odot} = [11,12)$ inner-CGM region, massive star-forming galaxies exceed quiescent galaxies on average by a factor of $\sim 3$ in OVI column density and $\sim 1.5$~dex in CGM OVI mass ($\log(M_{\rm O\, VI}/M_\odot) \approx 7.3$ versus $\approx 5.8$), with covering fractions roughly three times higher (62.5% versus 24% at $\log N_{\rm O\,VI}[\rm cm^{-2}] \geq 14$). The OVI line widths and column densities are consistent with feedback-driven radiative cooling, in which outflow shocks heat the CGM and the gas cools back through the OVI window; the short cooling time, $t_{\rm cool} \sim 10$-$100$~Myr, requires continuous replenishment by active feedback to sustain this reservoir. The residual OVI in quiescent systems may arise from ambient gas at the high-temperature end of the cooling curve. OVI thus traces feedback on short timescales and probes the star-forming--quiescent transition at $\log M_\star/M_{\odot} \gtrsim 11$.

Figures

Figures reproduced from arXiv: 2607.19473 by Ahmed Shaban, Andrew Fox, Benjamin Oppenheimer, Derick Flores, Jack Higginson, Jason Tumlinson, J. Christopher Howk, John O'Meara, Joseph Burchett, J. Xavier Prochaska, Mary Rickel, Nicolas Lehner, Robert A. Simcoe, Rongmon Bordoloi, Simon Xinlin Wu.

Figure 1
Figure 1. Figure 1: Left: Color–mass diagram of GOLIATH survey galaxies compared to archival CGM samples. Background contours show the color–mass distribution of SDSS galaxies from the NASA-Sloan Atlas (M. R. Blanton et al. 2011). The archival star-forming, passive, AGN-host, starburst, and LRG galaxies are drawn from previous CGM surveys. AGN hosts (T. A. M. Berg et al. 2018) are plotted to mark their location in this plane … view at source ↗
Figure 2
Figure 2. Figure 2: O vi column density as a function of projected distance to the host galaxy. Left: O vi column density versus physical projected separation. GOLIATH galaxies (cyan squares) reach O vi columns comparable to star-forming L ⋆ galaxies (blue circles) but with larger scatter, and lie systematically above passive galaxies (red circles). Non-detections are shown as downward triangles at the 3σ upper limit. Right: … view at source ↗
Figure 3
Figure 3. Figure 3: O vi column density as a function of stellar mass for star-forming (blue) and quiescent (red) galaxies. GOLIATH galaxies are shown as squares; archival galaxies are shown as circles. Bolder points with outlines are inner-CGM observations (R/Rvir ≤ 0.6); fainter points lie at larger R/Rvir. Upper limits are shown as downward-pointing triangles. The shaded region indicates the mass range used in the right pa… view at source ↗
Figure 4
Figure 4. Figure 4: O vi column density as a function of specific star– formation rate (sSFR) for star-forming (blue) and quiescent (red) galaxies. GOLIATH galaxies are shown as squares; archival galaxies are shown as circles. Solid points with out￾lines are inner-CGM observations (R/Rvir ≤ 0.6); transpar￾ent points lie at larger R/Rvir. Upper limits are shown as downward-pointing triangles. O vi column density increases with… view at source ↗
Figure 6
Figure 6. Figure 6: Kinematic properties of O vi absorbers for GOLIATH (squares), COS-Halos (circles), and MUSEQuBES (triangles) detections with R/Rvir ≤ 0.6. Upper left: Mean number of O vi kinematic components ⟨Ncomp⟩ per stellar mass bin for > 3σ detections. Lower left: Component velocity centroids as a function of stellar mass, colored by R/Rvir. Upper right: Distribution of all component velocities normalized to the host… view at source ↗
Figure 7
Figure 7. Figure 7: HST/COS NUV spectrum of the quasar sightline J1319+2728 (z = 0.6704, log NO VI = 14.65+0.03 −0.03 integrated over ±2000 km s−1 ). The velocity axis is referenced to the spectroscopic redshift of the primary target galaxy. Three distinct absorption systems are identified spanning −2000 to +300 km s−1 , suggesting an overdense environment. The O vi λ1031 and λ1037 components of each system are shown as solid… view at source ↗
Figure 8
Figure 8. Figure 8: CGM O vi mass as a function of stellar mass from the empirical annular integration method. Star-form￾ing (blue) and quiescent (red) galaxies are shown separately; color opacity indicates the maximum virial radius integrated, from R/Rvir ≤ 0.6 (darkest) to R/Rvir ≤ 3.0 (lightest). Points are slightly dithered in stellar mass for clarity. At log M⋆/M⊙ ≳ 11, SF galaxies show oxygen masses ∼ 1.5 dex higher tha… view at source ↗
Figure 10
Figure 10. Figure 10: O vi column density of individual absorption components as a function of absorption line width for GO￾LIATH (squares) and COS-Halos (circles) components, sep￾arated into star-forming (blue) and quiescent (red) popula￾tions. Curves show the predicted O vi column density in radiatively cooling post-shock gas model (R. Bordoloi et al. 2017) assuming collisional ionization equilibrium (CIE), at three characte… view at source ↗
Figure 10
Figure 10. Figure 10: High resolution spectra of GOLIATH galaxies. Gratings used include G130M, G160M (some archival data includes G185M, and G225M). Detections have the complete Voigt profile fit plotted in red; O vi components are plotted in green. Non-detections have the 200km s−1 window used for the 3σ upper limit calculation highlighted. Black tick marks represent the O VI kinematic components. Yellow dotted lines are ble… view at source ↗
Figure 10
Figure 10. Figure 10: Low resolution spectra of GOLIATH galaxies. All observations use grating g140l. Detections have the complete Voigt profile fit plotted in red; green shows the O vi components. Non-detections have the 200km/s window used for the 3σ upper limit calculation highlighted. Black tick marks represent the O vi kinematic components. Yellow dotted lines are blended components [PITH_FULL_IMAGE:figures/full_fig_p027… view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

89 extracted references · 14 canonical work pages · 1 internal anchor

  1. [1]

    Abdurro’uf, Accetta, K., Aerts, C., et al. 2022, title The Seventeenth Data Release of the Sloan Digital Sky Surveys: Complete Release of MaNGA, MaStar, and APOGEE-2 Data, The Astrophysical Journal Supplement Series, 259, 35, 10.3847/1538-4365/ac4414

    doi:10.3847/1538-4365/ac4414 2022

  2. [2]

    2023, title The physical nature of circumgalactic medium absorbers in SIMBA , , 519, 5514, 10.1093/mnras/stad025

    Appleby , S., Dav \'e , R., Sorini , D., Cui , W., & Christiansen , J. 2023, title The physical nature of circumgalactic medium absorbers in SIMBA , , 519, 5514, 10.1093/mnras/stad025

    doi:10.1093/mnras/stad025 2023

  3. [3]

    P., Tollerud , E

    Astropy Collaboration , Robitaille , T. P., Tollerud , E. J., et al. 2013, title Astropy: A community Python package for astronomy , , 558, A33, 10.1051/0004-6361/201322068

    doi:10.1051/0004-6361/201322068 2013

  4. [4]

    M., Sip o cz , B

    Astropy Collaboration , Price-Whelan , A. M., Sip o cz , B. M., et al. 2018, title The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package , , 156, 123, 10.3847/1538-3881/aabc4f

    doi:10.3847/1538-3881/aabc4f 2018

  5. [5]

    M., Lim , P

    Astropy Collaboration , Price-Whelan , A. M., Lim , P. L., et al. 2022, title The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package , , 935, 167, 10.3847/1538-4357/ac7c74

    doi:10.3847/1538-4357/ac7c74 2022

  6. [6]

    H., Hearin, A

    Behroozi, P., Wechsler, R. H., Hearin, A. P., & Conroy, C. 2019, title UniverseMachine: The correlation between galaxy growth and dark matter halo assembly from z = 0−10, Monthly Notices of the Royal Astronomical Society, 488, 3143–3194, 10.1093/mnras/stz1182

    doi:10.1093/mnras/stz1182 2019

  7. [7]

    Berg, T. A. M., Ellison, S. L., Tumlinson, J., et al. 2018, title The COS-AGN survey: revealing the nature of circumgalactic gas around hosts of active galactic nuclei, Monthly Notices of the Royal Astronomical Society, 478, 3890–3934, 10.1093/mnras/sty962

    work page doi:10.1093/mnras/sty962 2018

  8. [8]

    M., Stott, J

    Bielby, R. M., Stott, J. P., Cullen, F., et al. 2019, title Quasar Sightline and Galaxy Evolution (QSAGE) survey – I. The galaxy environment of O vi absorbers up to z = 1.4 around PKS 0232−04, Monthly Notices of the Royal Astronomical Society, 486, 21–41, 10.1093/mnras/stz774

    work page doi:10.1093/mnras/stz774 2019

  9. [9]

    R., Kazin, E., Muna, D., Weaver, B

    Blanton, M. R., Kazin, E., Muna, D., Weaver, B. A., & Price-Whelan, A. 2011, title IMPROVED BACKGROUND SUBTRACTION FOR THE SLOAN DIGITAL SKY SURVEY IMAGES, The Astronomical Journal, 142, 31, 10.1088/0004-6256/142/1/31

    doi:10.1088/0004-6256/142/1/31 2011

  10. [10]

    2025, rongmon/rbvfit: rbvfit v2.0.0, v2.0.0 Zenodo, 10.5281/zenodo.16318060

    Bordoloi, R., & Higginson, J. 2025, rongmon/rbvfit: rbvfit v2.0.0, v2.0.0 Zenodo, 10.5281/zenodo.16318060

    work page doi:10.5281/zenodo.16318060 2025

  11. [11]

    2025, rongmon/rbcodes: rbcodes v2.0.0, v2.0.0 Zenodo, 10.5281/zenodo.6079263

    Bordoloi, R., Liu, B., Clark, S., Higginson, J., & Flores, D. 2025, rongmon/rbcodes: rbcodes v2.0.0, v2.0.0 Zenodo, 10.5281/zenodo.6079263

    work page doi:10.5281/zenodo.6079263 2025

  12. [12]

    X., Tumlinson, J., et al

    Bordoloi, R., Prochaska, J. X., Tumlinson, J., et al. 2018, title On the CGM Fundamental Plane: The Halo Mass Dependency of Circumgalactic H i, The Astrophysical Journal, 864, 132, 10.3847/1538-4357/aad8ac

    doi:10.3847/1538-4357/aad8ac 2018

  13. [13]

    Y., Heckman, T

    Bordoloi, R., Wagner, A. Y., Heckman, T. M., & Norman, C. A. 2017, title The Formation and Physical Origin of Highly Ionized Cooling Gas, The Astrophysical Journal, 848, 122, 10.3847/1538-4357/aa8e9c

    doi:10.3847/1538-4357/aa8e9c 2017

  14. [14]

    J., Knobel, C., et al

    Bordoloi, R., Lilly, S. J., Knobel, C., et al. 2011, title THE RADIAL AND AZIMUTHAL PROFILES OF Mg II ABSORPTION AROUND 0.5 < z < 0.9 zCOSMOS GALAXIES OF DIFFERENT COLORS, MASSES, AND ENVIRONMENTS, The Astrophysical Journal, 743, 10, 10.1088/0004-637X/743/1/10

    doi:10.1088/0004-637x/743/1/10 2011

  15. [15]

    K., et al

    Bordoloi, R., Tumlinson, J., Werk, J. K., et al. 2014, title THE COS-DWARFS SURVEY: THE CARBON RESERVOIR AROUND SUB-L* GALAXIES*, The Astrophysical Journal, 796, 136, 10.1088/0004-637X/796/2/136

    doi:10.1088/0004-637x/796/2/136 2014

  16. [16]

    A., Matthee, J., et al

    Bordoloi, R., Simcoe, R. A., Matthee, J., et al. 2024, title EIGER IV. The Cool 104 K Circumgalactic Environment of High-redshift Galaxies Reveals Remarkably Efficient Intergalactic Medium Enrichment, The Astrophysical Journal, 963, 28, 10.3847/1538-4357/ad1b63

    work page doi:10.3847/1538-4357/ad1b63 2024

  17. [17]

    2013, title THE IMPACT OF STARBURSTS ON THE CIRCUMGALACTIC MEDIUM, The Astrophysical Journal, 768, 18, 10.1088/0004-637X/768/1/18

    Borthakur, S., Heckman, T., Strickland, D., Wild, V., & Schiminovich, D. 2013, title THE IMPACT OF STARBURSTS ON THE CIRCUMGALACTIC MEDIUM, The Astrophysical Journal, 768, 18, 10.1088/0004-637X/768/1/18

    doi:10.1088/0004-637x/768/1/18 2013

  18. [18]

    Borthakur, S., Heckman, T., Tumlinson, J., et al. 2015, title CONNECTION BETWEEN THE CIRCUMGALACTIC MEDIUM AND THE INTERS℡LAR MEDIUM OF GALAXIES: RESULTS FROM THE COS-GASS SURVEY, The Astrophysical Journal, 813, 46, 10.1088/0004-637X/813/1/46

    doi:10.1088/0004-637x/813/1/46 2015

  19. [19]

    E., Gauthier , J.-R., et al

    Chen , H.-W., Helsby , J. E., Gauthier , J.-R., et al. 2010, title An Empirical Characterization of Extended Cool Gas Around Galaxies Using Mg II Absorption Features , , 714, 1521, 10.1088/0004-637X/714/2/1521

    doi:10.1088/0004-637x/714/2/1521 2010

  20. [20]

    S., Johnson , S

    Chen , H.-W., Zahedy , F. S., Johnson , S. D., et al. 2018, title Characterizing circumgalactic gas around massive ellipticals at z 0.4 - I. Initial results , , 479, 2547, 10.1093/mnras/sty1541

    work page doi:10.1093/mnras/sty1541 2018

  21. [21]

    S., Boettcher , E., et al

    Chen , H.-W., Zahedy , F. S., Boettcher , E., et al. 2020, title The Cosmic Ultraviolet Baryon Survey (CUBS) - I. Overview and the diverse environments of Lyman limit systems at z < 1 , , 497, 498, 10.1093/mnras/staa1773

    doi:10.1093/mnras/staa1773 2020

  22. [22]

    C., Erb , D

    Chen , Y., Steidel , C. C., Erb , D. K., et al. 2021, title The KBSS-KCWI survey: the connection between extended Ly haloes and galaxy azimuthal angle at z 2-3 , , 508, 19, 10.1093/mnras/stab2383

    doi:10.1093/mnras/stab2383 2021

  23. [23]

    W., Mellon , R

    Churchill , C. W., Mellon , R. R., Charlton , J. C., et al. 1999, title The C IV Absorption-Mg II Kinematics Connection in <Z> -0.5ex 0.7 Galaxies , , 519, L43, 10.1086/312102

    work page doi:10.1086/312102 1999

  24. [24]

    A., & Van De Voort, F

    Crain, R. A., & Van De Voort, F. 2023, title Hydrodynamical Simulations of the Galaxy Population: Enduring Successes and Outstanding Challenges, Annual Review of Astronomy and Astrophysics, 61, 473–515, 10.1146/annurev-astro-041923-043618

    doi:10.1146/annurev-astro-041923-043618 2023

  25. [25]

    2024, title The Hubble Advanced Spectral Product (HASP) Program,

    Debes, J., Sankrit, R., Fischer, T., et al. 2024, title The Hubble Advanced Spectral Product (HASP) Program,

    2024

  26. [26]

    2016, title The DESI Experiment Part I: Science,Targeting, and Survey Design , arXiv e-prints, arXiv:1611.00036, 10.48550/arXiv.1611.00036

    DESI Collaboration , Aghamousa , A., Aguilar , J., et al. 2016, title The DESI Experiment Part I: Science,Targeting, and Survey Design , arXiv e-prints, arXiv:1611.00036, 10.48550/arXiv.1611.00036

    Pith/arXiv arXiv doi:10.48550/arxiv.1611.00036 2016

  27. [27]

    C., Churchill, C

    Ding, J., Charlton, J. C., Churchill, C. W., & Palma, C. 2003, title The Multiphase Absorption Systems toward PG 1206+459* ** ***, The Astrophysical Journal, 590, 746, 10.1086/375028

    work page doi:10.1086/375028 2003

  28. [28]

    2025, title MUSEQuBES: The Kinematics of O vi-bearing Gas in and around Low-redshift Galaxies, The Astrophysical Journal, 980, 264, 10.3847/1538-4357/adabbd

    Dutta, S., Muzahid, S., Schaye, J., et al. 2025, title MUSEQuBES: The Kinematics of O vi-bearing Gas in and around Low-redshift Galaxies, The Astrophysical Journal, 980, 264, 10.3847/1538-4357/adabbd

    doi:10.3847/1538-4357/adabbd 2025

  29. [29]

    Faucher-Giguere , C.-A., & Oh, S. P. 2023, Key Physical Processes in the Circumgalactic Medium , arXiv, 10.48550/arXiv.2301.10253

    Pith/arXiv arXiv doi:10.48550/arxiv.2301.10253 2023

  30. [30]

    Fisher, R. A. 1922, title On the Interpretation of χ2 from Contingency Tables, and the Calculation of P, Journal of the Royal Statistical Society, 85, 87. http://www.jstor.org/stable/2340521

    arXiv 1922

  31. [31]

    L., Faerman, Y., Berg, T

    Garza, S. L., Faerman, Y., Berg, T. A. M., et al. 2025, title Highly Ionized Gas in the Zone of Avoidance: Using the CIViL⋆ Survey to Pinpoint Physical Conditions of Gaseous Halos, The Astrophysical Journal, 993, 44, 10.3847/1538-4357/ae0304

    work page doi:10.3847/1538-4357/ae0304 2025

  32. [32]

    2007, title Time-dependent Ionization in Radiatively Cooling Gas, The Astrophysical Journal Supplement Series, 168, 213, 10.1086/509786

    Gnat, O., & Sternberg, A. 2007, title Time-dependent Ionization in Radiatively Cooling Gas, The Astrophysical Journal Supplement Series, 168, 213, 10.1086/509786

    doi:10.1086/509786 2007

  33. [33]

    Heckman, T., Borthakur, S., Wild, V., Schiminovich, D., & Bordoloi, R. 2017, title COS-burst: Observations of the Impact of Starburst-driven Winds on the Properties of the Circum-galactic Medium, The Astrophysical Journal, 846, 151, 10.3847/1538-4357/aa80dc

    doi:10.3847/1538-4357/aa80dc 2017

  34. [34]

    M., Norman, C

    Heckman, T. M., Norman, C. A., Strickland, D. K., & Sembach, K. R. 2002, title On the Physical Origin of O vi Absorption - Line Systems , The Astrophysical Journal, 577, 691, 10.1086/342232

    doi:10.1086/342232 2002

  35. [35]

    A., et al

    Higginson, J., Bordoloi, R., Simcoe, R. A., et al. 2026, title EIGER. VIII. First Stars Signatures in the Connection between O I Absorption and Galaxies in the Epoch of Reionization, The Astrophysical Journal, 999, 49, 10.3847/1538-4357/ae3e81

    doi:10.3847/1538-4357/ae3e81 2026

  36. [36]

    H., Martin, C

    Ho, S. H., Martin, C. L., Nateghi, H., Kacprzak, G. G., & Stern, J. 2026, title Kinematics of Circumgalactic O vi Gas and Disk Rotation of z ≈ 0.2 Star-forming Galaxies, The Astrophysical Journal, 998, 261, 10.3847/1538-4357/ae1b88

    doi:10.3847/1538-4357/ae1b88 2026

  37. [37]

    D., & Nelson , P

    Isobe , T., Feigelson , E. D., & Nelson , P. I. 1986, title Statistical Methods for Astronomical Data with Upper Limits. II. Correlation and Regression , , 306, 490, 10.1086/164359

    doi:10.1086/164359 1986

  38. [38]

    Montage: a grid portal and software toolkit for science-grade astronomical image mosaicking

    Jacob , J. C., Katz , D. S., Berriman , G. B., et al. 2010 a , title Montage: a grid portal and software toolkit for science-grade astronomical image mosaicking , arXiv e-prints, arXiv:1005.4454, 10.48550/arXiv.1005.4454

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1005.4454 2010

  39. [39]

    C., Katz , D

    Jacob , J. C., Katz , D. S., Berriman , G. B., et al. 2010 b , Montage: An Astronomical Image Mosaicking Toolkit ,, Astrophysics Source Code Library, record ascl:1010.036 1010.036

    2010

  40. [40]

    D., Leja , J., Conroy , C., & Speagle , J

    Johnson , B. D., Leja , J., Conroy , C., & Speagle , J. S. 2021, title Stellar Population Inference with Prospector , , 254, 22, 10.3847/1538-4365/abef67

    doi:10.3847/1538-4365/abef67 2021

  41. [41]

    D., Chen, H.-W., & Mulchaey, J

    Johnson, S. D., Chen, H.-W., & Mulchaey, J. S. 2015, title On the possible environmental effect in distributing heavy elements beyond individual gaseous haloes, Monthly Notices of the Royal Astronomical Society, 449, 3263–3273, 10.1093/mnras/stv553

    doi:10.1093/mnras/stv553 2015

  42. [42]

    D., Chen, H.-W., Mulchaey, J

    Johnson, S. D., Chen, H.-W., Mulchaey, J. S., Schaye, J., & Straka, L. A. 2017, title The Extent of Chemically Enriched Gas around Star-forming Dwarf Galaxies, The Astrophysical Journal Letters, 850, L10, 10.3847/2041-8213/aa9370

    doi:10.3847/2041-8213/aa9370 2017

  43. [43]

    Jr., F. J. M. 1951, title The Kolmogorov-Smirnov Test for Goodness of Fit, Journal of the American Statistical Association, 46, 68, 10.1080/01621459.1951.10500769

    arXiv 1951

  44. [44]

    2020, title Ensemble slice sampling: Parallel, black-box and gradient-free inference for correlated & multimodal distributions, arXiv preprint arXiv: 2002.06212

    Karamanis, M., & Beutler, F. 2020, title Ensemble slice sampling: Parallel, black-box and gradient-free inference for correlated & multimodal distributions, arXiv preprint arXiv: 2002.06212

    Pith/arXiv arXiv 2020

  45. [45]

    Karamanis, M., Beutler, F., & Peacock, J. A. 2021, title zeus: A Python implementation of Ensemble Slice Sampling for efficient Bayesian parameter inference, arXiv preprint arXiv:2105.03468

    Pith/arXiv arXiv 2021

  46. [46]

    A., Stocke, J

    Keeney, B. A., Stocke, J. T., Danforth, C. W., et al. 2017, title Characterizing the Circumgalactic Medium of Nearby Galaxies with HST/COS and HST/STIS Absorption-line Spectroscopy. II. Methods and Models∗, The Astrophysical Journal Supplement Series, 230, 6, 10.3847/1538-4365/aa6b59

    doi:10.3847/1538-4365/aa6b59 2017

  47. [47]

    A., Stocke, J

    Keeney, B. A., Stocke, J. T., Pratt, C. T., et al. 2018, title A Galaxy Redshift Survey Near HST/COS AGN Sight Lines, The Astrophysical Journal Supplement Series, 237, 11, 10.3847/1538-4365/aac727

    work page doi:10.3847/1538-4365/aac727 2018

  48. [48]

    D., Conroy, C., Dokkum, P

    Leja, J., Johnson, B. D., Conroy, C., Dokkum, P. G. v., & Byler, N. 2017, title Deriving Physical Properties from Broadband Photometry with Prospector: Description of the Model and a Demonstration of its Accuracy Using 129 Galaxies in the Local Universe, The Astrophysical Journal, 837, 170, 10.3847/1538-4357/aa5ffe

    doi:10.3847/1538-4357/aa5ffe 2017

  49. [49]

    A., et al

    Matthee, J., Mackenzie, R., Simcoe, R. A., et al. 2023, title EIGER. II. First Spectroscopic Characterization of the Young Stars and Ionized Gas Associated with Strong Hβ and [O iii] Line Emission in Galaxies at z = 5–7 with JWST, The Astrophysical Journal, 950, 67, 10.3847/1538-4357/acc846

    doi:10.3847/1538-4357/acc846 2023

  50. [50]

    C., Matuszewski , M., Neill , J

    McGurk , R. C., Matuszewski , M., Neill , J. D., et al. 2024, title The Keck Cosmic Reionization Mapper project: adding red spectroscopy to the Keck Cosmic Web Imager Integral Field Spectrograph , in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 13096, Ground-based and Airborne Instrumentation for Astronomy X, ed. J. J....

    doi:10.1117/12.3020646 2024

  51. [51]

    D., Rudie, G

    Mishra, N., Johnson, S. D., Rudie, G. C., et al. 2024, title The Cosmic Ultraviolet Baryon Survey (CUBS). IX. The Enriched Circumgalactic and Intergalactic Medium Around Star-forming Field Dwarf Galaxies Traced by O vi Absorption, The Astrophysical Journal, 976, 149, 10.3847/1538-4357/ad7b0a

    doi:10.3847/1538-4357/ad7b0a 2024

  52. [52]

    C., et al

    Morrissey , P., Matuszewski , M., Martin , D. C., et al. 2018, title The Keck Cosmic Web Imager Integral Field Spectrograph , , 864, 93, 10.3847/1538-4357/aad597

    doi:10.3847/1538-4357/aad597 2018

  53. [53]

    L., Kere s , D., Faucher-Gigu \`e re , C.-A., et al

    Muratov , A. L., Kere s , D., Faucher-Gigu \`e re , C.-A., et al. 2017, title Metal flows of the circumgalactic medium, and the metal budget in galactic haloes , , 468, 4170, 10.1093/mnras/stx667

    doi:10.1093/mnras/stx667 2017

  54. [54]

    Nelson, D., Kauffmann, G., Pillepich, A., et al. 2018, title The abundance, distribution, and physical nature of highly ionized oxygen O vi, O vii, and O viii in IllustrisTNG, Monthly Notices of the Royal Astronomical Society, 477, 450, 10.1093/mnras/sty656

    doi:10.1093/mnras/sty656 2018

  55. [55]

    D., Crain, R

    Oppenheimer, B. D., Crain, R. A., Schaye, J., et al. 2016, title Bimodality of low-redshift circumgalactic O vi in non-equilibrium eagle zoom simulations, Monthly Notices of the Royal Astronomical Society, 460, 2157–2179, 10.1093/mnras/stw1066

    doi:10.1093/mnras/stw1066 2016

  56. [56]

    S., Werk , J

    Peeples , M. S., Werk , J. K., Tumlinson , J., et al. 2014, title A Budget and Accounting of Metals at z -0.5ex 0: Results from the COS-Halos Survey , , 786, 54, 10.1088/0004-637X/786/1/54

    doi:10.1088/0004-637x/786/1/54 2014

  57. [57]

    J., Kovač, K., et al

    Peng, Y.-J., Lilly, S. J., Kovač, K., et al. 2010, title MASS AND ENVIRONMENT AS DRIVERS OF GALAXY EVOLUTION IN SDSS AND zCOSMOS AND THE ORIGIN OF THE SCHECHTER FUNCTION*, The Astrophysical Journal, 721, 193, 10.1088/0004-637X/721/1/193

    doi:10.1088/0004-637x/721/1/193 2010

  58. [58]

    1972, title Asymptotically Efficient Rank Invariant Test Procedures, Journal of the Royal Statistical Society

    Peto, R., & Peto, J. 1972, title Asymptotically Efficient Rank Invariant Test Procedures, Journal of the Royal Statistical Society. Series A (General), 135, 185. http://www.jstor.org/stable/2344317

    arXiv 1972

  59. [59]

    R., Brooks, A

    Piacitelli, D. R., Brooks, A. M., Sanchez, N. N., et al. 2026, The Simulated Oxygen Shortage (SOS): Mapping the Missing OVI in Simulated Dwarf Galaxies to Subgrid Physics, 2605.15275

    Pith/arXiv arXiv 2026

  60. [60]

    W., Atwood , B., Brewer , D

    Pogge , R. W., Atwood , B., Brewer , D. F., et al. 2010, title The multi-object double spectrographs for the Large Binocular Telescope , in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 7735, Ground-based and Airborne Instrumentation for Astronomy III, ed. I. S. McLean , S. K. Ramsay , & H. Takami , 77350A, 10.1117/12.857215

    doi:10.1117/12.857215 2010

  61. [61]

    X., Hennawi , J., Westfall , K., et al

    Prochaska , J. X., Hennawi , J., Westfall , K., et al. 2020 a , title PypeIt: The Python Spectroscopic Data Reduction Pipeline , The Journal of Open Source Software, 5, 2308, 10.21105/joss.02308

    doi:10.21105/joss.02308 2020

  62. [62]

    X., Hennawi , J., Cooke , R., et al

    Prochaska , J. X., Hennawi , J., Cooke , R., et al. 2020 b , pypeit/PypeIt: Release 1.0.0 , v1.0.0 Zenodo, 10.5281/zenodo.3743493

    doi:10.5281/zenodo.3743493 2020

  63. [63]

    Z., & Chen , Y

    Prusinski , N. Z., & Chen , Y. 2024, KCWIKit: KCWI Post-Processing and Improvements ,, Astrophysics Source Code Library, record ascl:2404.003 2404.003

    2024

  64. [64]

    Qu, Z., Chen, H.-W., Schiller, E., Wang, J., & Gronke, M. 2026, title Kinematics of H i and O vi Absorbers: Insights into the Turbulence Driver of the Multiphase Circumgalactic Medium, The Astrophysical Journal Letters, 1000, L12, 10.3847/2041-8213/ae4978

    work page doi:10.3847/2041-8213/ae4978 2026

  65. [65]

    D., et al

    Qu, Z., Chen, H.-W., Johnson, S. D., et al. 2024, title The Cosmic Ultraviolet Baryon Survey (CUBS). VII. On the Warm-hot Circumgalactic Medium Probed by O vi and Ne viii at 0.4 ≲ z ≲ 0.7, The Astrophysical Journal, 968, 8, 10.3847/1538-4357/ad410b

    doi:10.3847/1538-4357/ad410b 2024

  66. [66]

    E., Muzahid, S., Charlton, J

    Rosenwasser, B. E., Muzahid, S., Charlton, J. C., et al. 2018, title Understanding the strong intervening OVI absorber at z _ abs 0.93 towards PG1206+459, Monthly Notices of the Royal Astronomical Society, 476, 2258–2277, 10.1093/mnras/sty211

    work page doi:10.1093/mnras/sty211 2018

  67. [67]

    J., Bautista , J., Tojeiro , R., et al

    Ross , A. J., Bautista , J., Tojeiro , R., et al. 2020, title The Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: Large-scale structure catalogues for cosmological analysis , , 498, 2354, 10.1093/mnras/staa2416

    doi:10.1093/mnras/staa2416 2020

  68. [68]

    C., Steidel , C

    Rudie , G. C., Steidel , C. C., Pettini , M., et al. 2019, title Column Density, Kinematics, and Thermal State of Metal-bearing Gas within the Virial Radius of z 2 Star-forming Galaxies in the Keck Baryonic Structure Survey , , 885, 61, 10.3847/1538-4357/ab4255

    doi:10.3847/1538-4357/ab4255 2019

  69. [69]

    M., Simmons, B

    Schawinski, K., Urry, C. M., Simmons, B. D., et al. 2014, title The green valley is a red herring: Galaxy Zoo reveals two evolutionary pathways towards quenching of star formation in early- and late-type galaxies, Monthly Notices of the Royal Astronomical Society, 440, 889–907, 10.1093/mnras/stu327

    doi:10.1093/mnras/stu327 2014

  70. [70]

    M., et al

    Shaban, A., Bordoloi, R., O’Meara, J. M., et al. 2025, title Spatially Resolved Circumgalactic Medium around a Star-forming Galaxy Driving a Galactic Outflow at z ≈ 0.8, The Astrophysical Journal, 986, 190, 10.3847/1538-4357/add0b9

    work page doi:10.3847/1538-4357/add0b9 2025

  71. [71]

    T., Lilly , S

    Soto , K. T., Lilly , S. J., Bacon , R., Richard , J., & Conseil , S. 2016, title ZAP - enhanced PCA sky subtraction for integral field spectroscopy , , 458, 3210, 10.1093/mnras/stw474

    doi:10.1093/mnras/stw474 2016

  72. [72]

    C., Erb, D

    Steidel, C. C., Erb, D. K., Shapley, A. E., et al. 2010, title THE STRUCTURE AND KINEMATICS OF THE CIRCUMGALACTIC MEDIUM FROM FAR-ULTRAVIOLET SPECTRA OF z ≃ 2–3 GALAXIES*, The Astrophysical Journal, 717, 289, 10.1088/0004-637X/717/1/289

    doi:10.1088/0004-637x/717/1/289 2010

  73. [73]

    2019, title Cooling flow solutions for the circumgalactic medium, Monthly Notices of the Royal Astronomical Society, 488, 2549–2572, 10.1093/mnras/stz1859

    Stern, J., Fielding, D., Faucher-Giguère, C.-A., & Quataert, E. 2019, title Cooling flow solutions for the circumgalactic medium, Monthly Notices of the Royal Astronomical Society, 488, 2549–2572, 10.1093/mnras/stz1859

    doi:10.1093/mnras/stz1859 2019

  74. [74]

    F., Prochaska, J

    Stern, J., Hennawi, J. F., Prochaska, J. X., & Werk, J. K. 2016, title A UNIVERSAL DENSITY STRUCTURE FOR CIRCUMGALACTIC GAS, The Astrophysical Journal, 830, 87, 10.3847/0004-637X/830/2/87

    doi:10.3847/0004-637x/830/2/87 2016

  75. [75]

    T., Keeney, B

    Stocke, J. T., Keeney, B. A., Danforth, C. W., et al. 2013, title CHARACTERIZING THE CIRCUMGALACTIC MEDIUM OF NEARBY GALAXIES WITH HST /COS AND HST /STIS ABSORPTION-LINE SPECTROSCOPY, The Astrophysical Journal, 763, 148, 10.1088/0004-637X/763/2/148

    doi:10.1088/0004-637x/763/2/148 2013

  76. [76]

    N., Hopkins, A

    Taylor, E. N., Hopkins, A. M., Baldry, I. K., et al. 2015, title Galaxy And Mass Assembly (GAMA): deconstructing bimodality – I. Red ones and blue ones, Monthly Notices of the Royal Astronomical Society, 446, 2144–2185, 10.1093/mnras/stu1900

    doi:10.1093/mnras/stu1900 2015

  77. [77]

    K., Wilde, M

    Tchernyshyov, K., Werk, J. K., Wilde, M. C., et al. 2022, title The CGM2 Survey: Circumgalactic O vi from Dwarf to Massive Star-forming Galaxies, The Astrophysical Journal, 927, 147, 10.3847/1538-4357/ac450c

    doi:10.3847/1538-4357/ac450c 2022

  78. [78]

    K., et al

    Thom , C., Tumlinson , J., Werk , J. K., et al. 2012, title Not Dead Yet: Cool Circumgalactic Gas in the Halos of Early-type Galaxies , , 758, L41, 10.1088/2041-8205/758/2/L41

    doi:10.1088/2041-8205/758/2/l41 2012

  79. [79]

    A., Moustakas, J., & Diamond-Stanic, A

    Tremonti, C. A., Moustakas, J., & Diamond-Stanic, A. M. 2007, title The Discovery of 1000 km s-1 Outflows in Massive Poststarburst Galaxies at z 0.6*, The Astrophysical Journal, 663, L77, 10.1086/520083

    doi:10.1086/520083 2007

  80. [80]

    M., Meiring , J

    Tripp , T. M., Meiring , J. D., Prochaska , J. X., et al. 2011, title The Hidden Mass and Large Spatial Extent of a Post-Starburst Galaxy Outflow , Science, 334, 952, 10.1126/science.1209850

    doi:10.1126/science.1209850 2011

Showing first 80 references.

This paper was first reviewed by deepseek-v4-flash on August 1, 2026.