Pith. sign in

REVIEW 4 major objections 4 minor 71 references

Directly Imaging the Cooling Flow in the Phoenix Cluster

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

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

Pith's one-line read Using JWST/MIRI observations of [Ne VI] 7.652 µm, the paper maps gas at $\sim 10^{5.5}$ K across tens of kiloparsecs in the Phoenix cluster core and claims this coronal-phase gas is the cooling flow: it sits with the lowest-entropy X-ray…

desk verdict A genuinely new resolved map of 10^5.5 K gas in a cluster core, with a cooling-rate estimate that is plausible but more model-dependent than the quoted range suggests. read the letter →

arxiv 2502.08619 v1 pith:NOEJJA2E submitted 2025-02-12 astro-ph.GA

Michael Reefe , Michael McDonald , Marios Chatzikos , Jerome Seebeck , Richard Mushotzky , Sylvain Veilleux , Steven Allen , Matthew Bayliss
show 9 more authors
Michael Calzadilla Rebecca Canning Benjamin Floyd Massimo Gaspari Julie Hlavacek-Larrondo Brian McNamara Helen Russell Keren Sharon Taweewat Somboonpanyakul
This is my paper · ORCID
classification astro-ph.GA
keywords coolingflowsgalaxyclustersintraclustermediumcoronallineemissionNeVIAGNfeedbackPhoenixclusterJWSTMIRI/MRS
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

The paper claims to have directly imaged a cooling flow in the core of the Phoenix cluster, the first time such a flow has been mapped through the intermediate-temperature gas phase in any galaxy cluster. Using the mid-infrared [Ne VI] line at 7.652 µm, which traces gas near $10^{5.5}$ K, the authors map extended coronal emission over tens of kiloparsecs and show it is cospatial with the lowest-entropy X-ray gas, the coolest optical and molecular gas phases, and sites of active star formation. From this they infer a recent, short-lived spike in the cooling rate of 5,000–23,000 $M_\odot$ yr$^{-1}$ through $10^{5.5}$ K, far above the long-term X-ray average of a few thousand solar masses per year. If correct, this shows that the "cooling flow problem" is not an absolute absence of cooling but a matter of timing: cooling happens in brief bursts, apparently promoted rather than only suppressed by the AGN's radio bubble.

What carries the argument

The load-bearing tool is the mid-infrared coronal line [Ne VI] at 7.652 µm, observed with JWST's MIRI/MRS integral-field spectrograph; this line emits near $10^{5.5}$ K with essentially no extinction and no stellar continuum contamination, and a custom spectral decomposition separates the quasar point-spread function from host-galaxy emission across hundreds of spaxels. The conversion from line flux to mass cooling rate is carried out with CLOUDY simulations of a cooling gas parcel exposed to the quasar's radiation field, using a composite of isobaric and isochoric cooling and, in an alternative model, mixing between the hot ICM and warm ISM. The radial surface-brightness profile's bump, together with the bump in the [Ne VI]/[Ne V] ratio, identifies the cooling region as a cloud of size $\lesssim 5$ kpc located roughly 10 kpc from the nucleus.

What would settle it

Re-fit the observed [Ne VI]/[Ne V] and [Mg VII]/[Ne VI] ratios in the northern cloud with CLOUDY models that replace the unobscured hyperluminous-quasar SED by one attenuated by the torus; if those obscured models match the observed ratios equally well, the photoionization correction shrinks and the cooling rate could fall from the claimed 5,000–23,000 $M_\odot$ yr$^{-1}$ toward the X-ray long-term average.

Watch

Extended reading notes

Core claim

The central discovery is that the $[\mathrm{Ne\,VI}]$ $\lambda 7.652\,\mu$m emission in the Phoenix cluster is extended and spatially coherent, forming two clouds to the north of the nucleus that coincide with the minimum entropy of the hot atmosphere, the optical line-emitting gas, the cold molecular gas, and a region of enhanced star formation. Because [Ne VI] forms near $10^{5.5}$ K, this is the first large-scale map of gas between $10^5$ and $10^6$ K in a cluster core. The paper interprets the emission as gas actually cooling out of the hot intracluster medium while being illuminated by the central quasar, with a local bump in the surface brightness and in the density-insensitive $[\mathrm{Ne\,VI}]/[\mathrm{Ne\,V}]$ ratio marking the switch from AGN photoionization to cooling as the dominant process. The resulting mass cooling rate through $10^{5.5}$ K is 5,000–23,000 $M_\odot$ yr$^{-1}$, with a mixing-layer variant of the model giving 7,000–36,000 $M_\odot$ yr$^{-1}$; the authors argue that this spike is short-lived, forming 0.5–$2\times10^{11}$ $M_\odot$ of molecular gas and sustained by the turbulent wake of the buoyant X-ray bubble.

Load-bearing premise

The quantitative cooling rate assumes that the cooling gas sees the quasar's full unobscured radiation field; if the gas is shielded by the dusty torus or a fainter source, the photoionization correction shrinks and the inferred cooling rate would drop substantially.

Editorial extensions

If this is right

  • The Phoenix cluster would become the first system in which a cooling flow has been mapped continuously from the hot intracluster medium down to star-forming temperatures, closing a long-standing observational gap.
  • The inferred cooling rate through $10^{5.5}$ K exceeds the classical X-ray-inferred, gigayear-averaged rate by a factor of a few, implying that cooling in cluster cores is episodic rather than steady.
  • The model predicts that this cooling spike forms $0.5$–$2\times10^{11}$ $M_\odot$ of molecular gas, several times the observed $2.1\times10^{10}$ $M_\odot$, suggesting that much of the cold gas is destroyed by feedback or re-mixed before reaching the molecular phase.
  • The coincidence of the cooling gas with the wake of the buoyant X-ray bubble indicates that AGN feedback can promote cooling as well as regulate it, providing a concrete mechanism for fueling future feedback cycles.

Reading between the lines

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

  • The same MIRI/MRS technique applied to other cool-core clusters should reveal whether extended [Ne VI] emission is common; clusters with weak or absent coronal-phase nebulae would test the claim that Phoenix is an unusual, short-lived state.
  • If the cooling gas truly sees an unobscured quasar, then variations in the quasar's ionizing luminosity should imprint on the photoionization-dominated parts of the [Ne VI] map while leaving the cooling component stable; multi-epoch observations could separate these contributions.
  • The mixing-layer models imply that neon abundances and dust depletion in the $10^{5.5}$ K phase dominate the systematic uncertainty; future mid-infrared neon-line observations in other systems could measure these quantities directly instead of relying on X-ray abundances averaged over 300 kpc.
  • If short-lived cooling spikes with rates of order $10^4$ $M_\odot$ yr$^{-1}$ are generic in massive clusters, the molecular gas reservoirs they build should be detectable as extended CO or dust emission in other starbursting brightest cluster galaxies.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

4 major / 4 minor

Summary. This paper presents JWST MIRI/MRS integral-field spectroscopy of the Phoenix cluster core, mapping the [Ne VI] λ7.652 μm coronal line over tens of kiloparsecs. The authors develop a spectral-spatial decomposition to subtract the bright QSO PSF and measure extended [Ne VI] emission, finding it cospatial with the lowest-entropy ICM, the cool ionized and molecular gas, and star-forming filaments. A radial surface-brightness profile shows a localized (≲5 kpc) enhancement above an r^-2 AGN-photoionized background, coincident with an increase in the [Ne VI]/[Ne V] ratio. Using CLOUDY cooling models with AGN photoionization, they convert the observed line luminosities into mass cooling rates, obtaining ~25,000 ± 5,000 M⊙ yr−1 for [Ne VI], a multi-line average of ~10,000 ± 5,000 M⊙ yr−1, and a 'conservative' range of 5,000–23,000 M⊙ yr−1; mixing-layer models give 15,000 ± 2,000 M⊙ yr−1 with a range of 7,000–36,000 M⊙ yr−1. They also present the line-of-sight velocity profile, which is consistent with gas in the wake of a buoyantly rising X-ray bubble, and discuss alternative ionization sources (shocks, stellar photoionization, cosmic rays, turbulent mixing).

Significance. If the detection and interpretation hold, this is the first large-scale map of 10^5–10^6 K gas in a cluster core, directly imaging an intermediate-temperature phase of a cooling flow and strengthening the case that the Phoenix cluster is undergoing a rapid, short-lived cooling episode. The paper's strengths include careful data reduction (custom background subtraction, striping removal, PSF subtraction from a stellar template), public code (LOKI on GitHub) and data availability, and a systematic consideration of alternative ionization mechanisms with an ionization diagram. The central detection and the spatial correlations are well supported. The quantitative cooling rate, however, rests on several model choices—most notably the unobscured quasar SED, the fitted isochoric fraction, and the assumed initial conditions—and the quoted systematic range does not capture all of these. The paper is an important advance regardless, but the headline number should be treated as model-dependent until the photoionization systematics are addressed.

major comments (4)
  1. [Main text ('We adopt a generic SED template...') and SI §3.2] The quantitative cooling-rate scale rests on the assumption that the cooling gas is illuminated by the unobscured, full hyperluminous quasar SED. The paper states this assumption and notes in SI §3.2 that the obscuration along the line of sight to the cooling gas is unknown. The systematic range quoted (5,000–23,000 M⊙ yr−1) is derived only from factor-of-two variations in L_bol and Z_Ne; it does not include SED-shape or obscuration changes, which can plausibly alter the photoionization correction by orders of magnitude for lines of sight near the torus. Please test this assumption with the spatially resolved [Ne VI]/[Ne V] ratio map by fitting the incident SED or the ionizing photon flux as a free parameter at each radius, or run a grid of torus-obscured SEDs to bracket the cooling rate. Without such a test, the abstract's numerical range is not robust, even though the detection and cospatiality claims are.
  2. [SI §3.1, Eqs (6)–(7)] The isochoric fraction x is optimized by fitting the observed line ratios under the assumption that Mdot1/Mdot2 ≈ 1 (Eq. 6), and the same x is then used in Eq. (7) to convert each observed line luminosity into a cooling rate. This procedure forces the line-by-line cooling rates toward mutual agreement; the 'median absolute deviation' quoted in the main text is therefore not an independent validation of a single cooling rate. Please fit x and the absolute normalization simultaneously to the observed line luminosities, or propagate the uncertainty in x into each Mdot, and report the best-fit line-ratio residuals. The current treatment makes the multi-line average partly a product of the fitting ansatz.
  3. [Main text ('The total [Ne VI] flux...') and Figure 3 caption] The cooling rates in Figure 3 are computed from the observed [Ne VI] surface-brightness profile, 'assuming that all of the luminosity in the northern cloud is contained within a small Δr at each radius.' However, Figure 2 shows that this profile is decomposed into an r^-2 power-law component, attributed to AGN photoionization of a constant-density medium, and a localized ≤5 kpc box component, attributed to cooling. If the r^-2 component is not actually cooling gas but gas in photoionization equilibrium, then including it in the luminosity entering L = Mdot Γ will overestimate the cooling rate. Please compute Mdot using only the box component, or justify explicitly that the diffuse photoionized gas is also part of the cooling flow.
  4. [Main text ('The cooling gas starts with an initial density...') and SI §3.2] The CLOUDY cooling models assume a single initial density (n_e = 0.42 cm−3) and temperature (kT = 2.3 keV) for the cooling parcel, taken from X-ray measurements. The systematic uncertainty analysis in SI §3.2 varies only L_bol and Z_Ne; the sensitivity of the inferred cooling rate to the adopted initial density and temperature is not explored. Since the ionization parameter and hence the photoionization boost depend on density, please quantify how Mdot changes over the plausible range of initial conditions, or justify explicitly that the result is insensitive to these choices.
minor comments (4)
  1. [Figure 2 caption] Typo: 'A raidal surface brightness profile' should read 'A radial surface brightness profile'.
  2. [Main text, 'forming 0.5–2 ×10^11 M⊙ of molecular gas'] The sentence 'This is a few times higher than the observed 2.1 ± 0.3 × 10^10 M⊙ yr−1[21]' has incorrect units for a molecular gas mass; it should be M⊙, not M⊙ yr−1.
  3. [Main text, 'When we consider all high-ionization lines...'] The text includes O VI in the list of lines used for the average cooling rate of 10,000 ± 5,000 M⊙ yr−1, but then states that O VI is an outlier 'most likely due to uncertainties in the UV extinction correction.' Please clarify whether the quoted average includes O VI, and if so, how the outlier affects the median absolute deviation; consider quoting the average with and without O VI.
  4. [SI §1.4] The F-test threshold of 0.3% (3σ) is applied spaxel-by-spaxel without correction for multiple testing; given the large number of spaxels, a small number of spurious two-component fits may be expected. Please state whether the two-component kinematic results are robust to a more conservative threshold or a spatial-coherence requirement.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the cooling-rate inference is a model-calibrated measurement, not a restatement of its inputs.

full rationale

The paper's central claims rest on new JWST/MIRI data: the [Ne VI] map, the QSO-subtracted line fluxes, and the spatial coincidence with entropy minima, cold gas, and star formation are all independently measured or anchored to external datasets (Chandra, HST, ALMA, Gemini). The cooling-rate estimate is not a tautology: observed line luminosities are converted to mass cooling rates using CLOUDY emissivities computed from independent atomic physics, with an explicitly stated cooling scenario (isobaric/isochoric) and an adopted AGN SED. The only data-tuned parameter in the cooling analysis is the isochoric fraction x=0.13 (Supplementary Information §3.1), which is adjusted to reproduce observed line ratios; this does not make the derived cooling rate circular, because the absolute mass flux is set by the observed line luminosity divided by the composite emissivity, while the ratio fit only selects the weighting between two cooling geometries. The paper also openly discloses the dominant systematics (Lbol and ZNe scaling, and the unknown obscuration along the cooling-gas line of sight in SI §3.2), which is a robustness limitation rather than a circular step. Self-citations to prior Phoenix-cluster papers supply the X-ray entropy, bubble, molecular-gas, and stellar-population data used for cospatiality, but those are external observations; no load-bearing conclusion reduces to an unpublished or unverified self-citation. Thus the derivation is self-contained with respect to its central quantitative and spatial claims; the main caveats are model-sensitivity and SED/obscuration assumptions, not circularity.

Assumptions & free parameters 5 free parameters · 4 assumptions · 0 invented entities

The central inference rests on standard plasma modeling plus several domain assumptions about the geometry and composition of the cooling gas. No new particles, forces, or conserved quantities are introduced. The most important inputs are the X-ray-derived initial conditions, the AGN SED normalization, and the fitted isochoric fraction.

free parameters (5)
  • Isochoric cooling fraction x = 0.13
    Chosen by minimizing chi^2 between model and observed line ratios on the 1:1 line, excluding [Ne II] and O VI; then used in Eq. 7 to convert observed luminosities into cooling rates (Supplementary Information, Section 3.1).
  • Hot-phase neon abundance Z_Ne = 0.55 Zsun
    From XMM-RGS spectra averaged over the inner 300 kpc, re-computed for this work; varied by factor two in systematic runs because it strongly scales the cooling rate (Supplementary Information, Section 3.2).
  • AGN bolometric luminosity L_bol = 3e47 erg/s
    Adopted from Phoenix's known bolometric luminosity and used to rescale the hyperluminous quasar SED; varied by factor two in systematic runs; poorly constrained due to obscuration.
  • Initial gas density and temperature = n_e = 0.42 cm^-3, kT = 2.3 keV
    Taken from X-ray data at the location of the extended [Ne VI] gas; determines the cooling trajectory in CLOUDY.
  • Mixing ratio and depletion strength in mixed model = ISM:ICM = 4:1, F* = 0.6
    Best-representative mixed-layer model; authors note systematic uncertainties from these parameters are not included in the 7,000-36,000 solar masses per year range.
assumptions (4)
  • standard math CLOUDY v23 with CHIANTI v10 collision strengths correctly computes the ionization balance, emissivities, and cooling of the modeled gas.
    All cooling-rate conversions in Methods Section 4 and Supplementary Section 3 rely on the accuracy of CLOUDY and its atomic data; the paper provides no independent verification for this regime.
  • domain assumption The [Ne VI] emission traces gas cooling radiatively out of the hot ICM, rather than gas that is merely being heated and re-ionized by shocks or mixing without net cooling.
    Methods Section 4 states 'We assume that the coronal emission comes from ICM gas cooling to low temperatures.' Alternative sources are tested and disfavored, but not completely excluded.
  • domain assumption The cooling gas is illuminated by the AGN essentially unobscured, with an SED and luminosity representative of Phoenix (L_bol = 3e47 erg/s).
    Main text cooling models paragraph: the gas lies along the jet axis where it is 'likely unobscured...' This geometry is not directly observable and strongly affects the inferred rates.
  • domain assumption The X-ray-derived initial density, temperature, and metallicity are representative of the gas that emits the extended [Ne VI].
    Spatially averaged XMM-RGS abundances and Chandra-derived profiles at the cloud location are used to set initial conditions; abundance is averaged over 300 kpc.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Directly Imaging the Cooling Flow in the Phoenix Cluster." pith.science (2026). https://pith.science/paper/NOEJJA2E

@misc{pith2026250208619,
  author       = {Pith},
  title        = {Pith review of: Directly Imaging the Cooling Flow in the Phoenix Cluster},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/NOEJJA2E}},
  note         = {Machine review of arXiv:2502.08619}
}
abstract

In the centers of many galaxy clusters, the hot ($\sim$10$^7$ K) intracluster medium (ICM) can become dense enough that it should cool on short timescales. However, the low measured star formation rates in massive central galaxies and absence of soft X-ray lines from cooling gas suggest that most of this gas never cools - this is known as the "cooling flow problem." The latest observations suggest that black hole jets are maintaining the vast majority of gas at high temperatures. A cooling flow has yet to be fully mapped through all gas phases in any galaxy cluster. Here, we present new observations of the Phoenix cluster using the James Webb Space Telescope to map the [Ne VI] $\lambda$7.652$\mu$m emission line, allowing us to probe gas at 10$^{5.5}$ K on large scales. These data show extended [Ne VI] emission cospatial with (i) the cooling peak in the ICM, (ii) the coolest gas phases, and (iii) sites of active star formation. Taken together, these imply a recent episode of rapid cooling, causing a short-lived spike in the cooling rate which we estimate to be 5,000-23,000 M$_\odot$ yr$^{-1}$. These data provide the first large-scale map of gas at temperatures between 10$^5$-10$^6$ K in a cluster core, and highlight the critical role that black hole feedback plays in not only regulating but also promoting cooling.

Figures

Figures reproduced from arXiv: 2502.08619 by the authors.

Figure 1
Figure 1. Maps of the [Ne VI]-emitting coronal gas in the central galaxy of the Phoenix Clus￾1 ter overlaid with the hotter and colder gas phases, and starlight. (a) A 2D map of the [Ne VI] λ7.652 µm flux from channel 3 MIRI/MRS data. The flux is in log10(F/erg s−1 cm−2 spaxel−1 ), where a channel 3 spaxel is 0.04 arcsec2 . The white ellipse shows the aperture we use to cap￾ture the region of extended northern emission. A sca… view at source ↗
Figure 2
Figure 2. A raidal surface brightness profile of the northern [Ne 1 VI] emission in the central galaxy of the Phoenix Cluster. (a) A 2D map of the [Ne VI] flux. Here, only spaxels with S/N ⩾ 1 are shown. A series of rectangular apertures are shown in white that span from the nucleus out to 25 kpc in two directions aligned with the northern clouds of emission. The innermost and outermost apertures are circular annuli to improv… view at source ↗
Figure 3
Figure 3. CLOUDY 1 -simulated cooling rates for a radiatively cooling parcel of gas that is being illuminated by a central AGN at various distances from the nucleus. (a) The cooling rates M˙ for each line are shown as a function of distance from the nucleus, assuming that all of the luminosity in the northern cloud is contained within a small ∆r at each radius. The lines are colored according to which emission line they corre… view at source ↗
Figures from the paper (1 more)
Figure 4
Figure 4. Figure 4: A north-south velocity profile of the [Ne 1 VI]-emitting gas in the central galaxy of the Phoenix Cluster, overlaid with various models. (a) A 2D map of the median LOS velocity of [Ne VI]. Here, only spaxels where [Ne VI] is detected with S/N ⩾ 2 are shown. A series of…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

71 extracted references · 44 canonical work pages

  1. [1]

    author Fabian , A. C. , author Nulsen , P. E. J. & author Canizares , C. R. title Cooling flows in clusters of galaxies . journal volume 310 , pages 733--740 ( year 1984 )

    work page 1984

  2. [2]

    author Fabian , A. C. title Cooling Flows in Clusters of Galaxies . journal volume 32 , pages 277--318 ( year 1994 )

    work page 1994

  3. [3]

    author McNamara , B. R. & author O'Connell , R. W. title Star formation in cooling flows in clusters of galaxies. journal volume 98 , pages 2018--2043 ( year 1989 )

    work page 2018

  4. [4]

    author Allen , S. W. title Starbursts in cooling flows: blue continua and emission-line nebulae in central cluster galaxies . journal volume 276 , pages 947--960 ( year 1995 )

    work page 1995

  5. [5]

    author Hicks , A. K. & author Mushotzky , R. title Star Formation Rates in Cooling Flow Clusters: A UV Pilot Study with Archival XMM-Newton Optical Monitor Data . journal volume 635 , pages L9--L12 ( year 2005 ). astro-ph/0508143

    work page Pith review arXiv 2005

  6. [6]

    , author Gaspari , M

    author McDonald , M. , author Gaspari , M. , author McNamara , B. R. & author Tremblay , G. R. title Revisiting the Cooling Flow Problem in Galaxies, Groups, and Clusters of Galaxies . journal volume 858 , pages 45 ( year 2018 ). 1803.04972

    arXiv 2018

  7. [7]

    author Canizares , C. R. , author Markert , T. H. & author Donahue , M. E. title X-Ray Emission Lines from Cooling Flows . In editor Fabian , A. C. (ed.) booktitle Cooling Flows in Clusters and Galaxies , vol. volume 229 of series NATO Advanced Study Institute (ASI) Series C , pages 63 ( year 1988 )

    work page 1988

  8. [8]

    author David , L. P. et al. title A High-Resolution Study of the Hydra A Cluster with Chandra: Comparison of the Core Mass Distribution with Theoretical Predictions and Evidence for Feedback in the Cooling Flow . journal volume 557 , pages 546--559 ( year 2001 ). astro-ph/0010224

    arXiv 2001

Show all 71 references
  1. [9]

    author Peterson , J. R. et al. title High-Resolution X-Ray Spectroscopic Constraints on Cooling-Flow Models for Clusters of Galaxies . journal volume 590 , pages 207--224 ( year 2003 ). astro-ph/0210662

    2003 arXiv

  2. [10]

    author McNamara , B. R. & author Nulsen , P. E. J. title Heating Hot Atmospheres with Active Galactic Nuclei . journal volume 45 , pages 117--175 ( year 2007 ). 0709.2152

    2007 arXiv

  3. [11]

    author Fabian , A. C. title Observational Evidence of Active Galactic Nuclei Feedback . journal volume 50 , pages 455--489 ( year 2012 ). 1204.4114

    2012 arXiv

  4. [12]

    author Hlavacek-Larrondo , J. et al. title X-Ray Cavities in a Sample of 83 SPT-selected Clusters of Galaxies: Tracing the Evolution of AGN Feedback in Clusters of Galaxies out to z=1.2 . journal volume 805 , pages 35 ( year 2015 ). 1410.0025

    2015 arXiv

  5. [13]

    , author Melioli , C

    author Gaspari , M. , author Melioli , C. , author Brighenti , F. & author D'Ercole , A. title The dance of heating and cooling in galaxy clusters: three-dimensional simulations of self-regulated active galactic nuclei outflows . journal volume 411 , pages 349--372 ( year 2011...

    2011 arXiv

  6. [14]

    , author Sharma , P

    author Prasad , D. , author Sharma , P. & author Babul , A. title Cool Core Cycles: Cold Gas and AGN Jet Feedback in Cluster Cores . journal volume 811 , pages 108 ( year 2015 ). 1504.02215

    2015 arXiv

  7. [15]

    , author Ruszkowski , M

    author Li , Y. , author Ruszkowski , M. & author Bryan , G. L. title AGN Heating in Simulated Cool-core Clusters . journal volume 847 , pages 106 ( year 2017 ). 1611.05455

    2017 arXiv

  8. [16]

    author Yang , H. Y. K. , author Gaspari , M. & author Marlow , C. title The Impact of Radio AGN Bubble Composition on the Dynamics and Thermal Balance of the Intracluster Medium . journal volume 871 , pages 6 ( year 2019 ). 1810.04173

    2019 arXiv

  9. [17]

    author McDonald , M. et al. title A massive, cooling-flow-induced starburst in the core of a luminous cluster of galaxies . journal volume 488 , pages 349--352 ( year 2012 ). 1208.2962

    2012 arXiv

  10. [18]

    author McNamara , B. R. et al. title A Mechanism for Stimulating AGN Feedback by Lifting Gas in Massive Galaxies . journal volume 830 , pages 79 ( year 2016 ). 1604.04629

    2016 arXiv

  11. [19]

    , author Combes , F

    author Revaz , Y. , author Combes , F. & author Salom \'e , P. title Formation of cold filaments in cooling flow clusters . journal volume 477 , pages L33--L36 ( year 2008 ). 0711.4051

    2008 arXiv

  12. [20]

    author McDonald , M. et al. title Anatomy of a Cooling Flow: The Feedback Response to Pure Cooling in the Core of the Phoenix Cluster . journal volume 885 , pages 63 ( year 2019 ). 1904.08942

    2019 arXiv

  13. [21]

    author Russell , H. R. et al. title Alma Observations of Massive Molecular Gas Filaments Encasing Radio Bubbles in the Phoenix Cluster . journal volume 836 , pages 130 ( year 2017 ). 1611.00017

    2017 arXiv

  14. [22]

    author Gaspari , M. et al. title Shaken Snow Globes: Kinematic Tracers of the Multiphase Condensation Cascade in Massive Galaxies, Groups, and Clusters . journal volume 854 , pages 167 ( year 2018 ). 1709.06564

    2018 arXiv

  15. [23]

    author McDonald , M. et al. title Deep Chandra, HST-COS, and Megacam Observations of the Phoenix Cluster: Extreme Star Formation and AGN Feedback on Hundred Kiloparsec Scales . journal volume 811 , pages 111 ( year 2015 ). 1508.05941

    2015 arXiv

  16. [24]

    author Pinto , C. et al. title AGN feedback in the Phoenix cluster . journal volume 480 , pages 4113--4123 ( year 2018 ). 1808.02872

    2018 arXiv

  17. [25]

    author Oegerle , W. R. et al. title FUSE Observations of Cooling-Flow Gas in the Galaxy Clusters A1795 and A2597 . journal volume 560 , pages 187--193 ( year 2001 ). astro-ph/0106279

    2001 arXiv

  18. [26]

    author Bregman , J. N. , author Fabian , A. C. , author Miller , E. D. & author Irwin , J. A. title On VI Observations of Galaxy Clusters: Evidence for Modest Cooling Flows . journal volume 642 , pages 746--751 ( year 2006 ). astro-ph/0602323

    2006 arXiv

  19. [27]

    author Fabian , A. C. et al. title Hidden cooling flows in clusters of galaxies . journal volume 515 , pages 3336--3345 ( year 2022 ). 2207.04951

    2022 arXiv

  20. [28]

    author Sparks , W. B. et al. title Hundred Thousand Degree Gas in the Virgo Cluster of Galaxies . journal volume 750 , pages L5 ( year 2012 ). 1203.5097

    2012 arXiv

  21. [29]

    author Anderson , M. E. & author Sunyaev , R. title Searching for FUV line emission from 10 ^ 7 K gas in massive elliptical galaxies and galaxy clusters as a tracer of turbulent velocities . journal volume 459 , pages 2806--2821 ( year 2016 ). 1506.01703

    2016 arXiv

  22. [30]

    author Canning , R. E. A. et al. title Detection of optical coronal emission from 10 ^ 6 -K gas in the core of the Centaurus cluster . journal volume 411 , pages 411--421 ( year 2011 ). 1009.2581

    2011 arXiv

  23. [31]

    author Chatzikos , M. et al. title Implications of coronal line emission in NGC 4696 ^ * . journal volume 446 , pages 1234--1244 ( year 2015 ). 1410.4566

    2015 arXiv

  24. [32]

    author McDonald , M. et al. title The State of the Warm and Cold Gas in the Extreme Starburst at the Core of the Phoenix Galaxy Cluster (SPT-CLJ2344-4243) . journal volume 784 , pages 18 ( year 2014 ). 1311.0867

    2014 arXiv

  25. [33]

    author Pope , E. C. D. , author Babul , A. , author Pavlovski , G. , author Bower , R. G. & author Dotter , A. title Mass transport by buoyant bubbles in galaxy clusters . journal volume 406 , pages 2023--2037 ( year 2010 ). 1004.2050

    2023 arXiv

  26. [34]

    , author Ruszkowski , M

    author Gaspari , M. , author Ruszkowski , M. & author Sharma , P. title Cause and Effect of Feedback: Multiphase Gas in Cluster Cores Heated by AGN Jets . journal volume 746 , pages 94 ( year 2012 ). 1110.6063

    2012 arXiv

  27. [35]

    & author Gaspari , M

    author Wittor , D. & author Gaspari , M. title Dissecting the turbulent weather driven by mechanical AGN feedback . journal volume 498 , pages 4983--5002 ( year 2020 ). 2009.03344

    2020 arXiv

  28. [36]

    author Ferland , G. J. et al. title CLOUDY 90: Numerical Simulation of Plasmas and Their Spectra . journal volume 110 , pages 761--778 ( year 1998 )

    1998

  29. [37]

    author Chatzikos , M. et al. title The 2023 Release of Cloudy . journal volume 59 , pages 327--343 ( year 2023 ). 2308.06396

    2023 arXiv

  30. [38]

    author Saccheo , I. et al. title The WISSH quasars project. XI. The mean spectral energy distribution and bolometric corrections of the most luminous quasars . journal volume 671 , pages A34 ( year 2023 ). 2211.07677

    2023 arXiv

  31. [39]

    , author Geballe , T

    author Indriolo , N. , author Geballe , T. R. , author Oka , T. & author McCall , B. J. title H ^ + _ 3 in Diffuse Interstellar Clouds: A Tracer for the Cosmic-Ray Ionization Rate . journal volume 671 , pages 1736--1747 ( year 2007 ). 0709.1114

    2007 arXiv

  32. [40]

    title Shaping the X-ray spectrum of galaxy clusters with AGN feedback and turbulence

    author Gaspari , M. title Shaping the X-ray spectrum of galaxy clusters with AGN feedback and turbulence. journal volume 451 , pages L60--L64 ( year 2015 ). 1410.7769

    2015 arXiv

  33. [41]

    author Jenkins , E. B. title A Unified Representation of Gas-Phase Element Depletions in the Interstellar Medium . journal volume 700 , pages 1299--1348 ( year 2009 ). 0905.3173

    2009 arXiv

  34. [42]

    , author Temi , P

    author Gaspari , M. , author Temi , P. & author Brighenti , F. title Raining on black holes and massive galaxies: the top-down multiphase condensation model . journal volume 466 , pages 677--704 ( year 2017 ). 1608.08216

    2017 arXiv

  35. [43]

    , author Sharma , P

    author Prasad , D. , author Sharma , P. , author Babul , A. , author Voit , G. M. & author O'Shea , B. W. title Cool-core cycles and Phoenix . journal volume 495 , pages 594--599 ( year 2020 ). 1909.12888

    2020 arXiv

  36. [44]

    author Fabian , A. C. et al. title The relationship between the optical H filaments and the X-ray emission in the core of the Perseus cluster . journal volume 344 , pages L48--L52 ( year 2003 ). astro-ph/0306039

    2003 arXiv

  37. [45]

    author Gendron-Marsolais , M. et al. title Revealing the velocity structure of the filamentary nebula in NGC 1275 in its entirety . journal volume 479 , pages L28--L33 ( year 2018 ). 1802.00031

    2018 arXiv

  38. [46]

    author McNamara , B. R. & author Nulsen , P. E. J. title Mechanical feedback from active galactic nuclei in galaxies, groups and clusters . journal New Journal of Physics volume 14 , pages 055023 ( year 2012 ). 1204.0006

    2012 arXiv

  39. [47]

    author Fabian , A. C. et al. title Hidden Cooling Flows in clusters of Galaxies II: a wider sample . journal volume 521 , pages 1794--1807 ( year 2023 ). 2211.13971

    2023 arXiv

  40. [48]

    author Spilker , J. S. et al. title Spatial variations in aromatic hydrocarbon emission in a dust-rich galaxy . journal volume 618 , pages 708--711 ( year 2023 ). 2306.03152

    2023 arXiv

  41. [49]

    , author Edelman, A

    author Bezanson, J. , author Edelman, A. , author Karpinski, S. & author Shah, V. B. title Julia: A fresh approach to numerical computing . journal SIAM Review volume 59 , pages 65--98 ( year 2017 ). ://doi.org/10.1137/141000671. https://doi.org/10.1137/141000671

    2017 doi

  42. [50]

    author Smith , J. D. T. et al. title The Mid-Infrared Spectrum of Star-forming Galaxies: Global Properties of Polycyclic Aromatic Hydrocarbon Emission . journal volume 656 , pages 770--791 ( year 2007 ). astro-ph/0610913

    2007 arXiv

  43. [51]

    author Fitzpatrick , E. L. & author Massa , D. title An Analysis of the Shapes of Ultraviolet Extinction Curves. I. The 2175 Angstrom Bump . journal volume 307 , pages 286 ( year 1986 )

    1986

  44. [52]

    author Donnan , F. R. et al. title The obscured nucleus and shocked environment of VV 114E revealed by JWST/MIRI spectroscopy . journal volume 519 , pages 3691--3705 ( year 2023 ). 2210.04647

    2023 arXiv

  45. [53]

    author Labiano , A. et al. title Wavelength calibration and resolving power of the JWST MIRI Medium Resolution Spectrometer . journal volume 656 , pages A57 ( year 2021 ). 2109.04254

    2021 arXiv

  46. [54]

    author Tsuchikawa , T. et al. title A systematic study of silicate absorption features in heavily obscured AGNs observed by Spitzer/IRS . journal volume 651 , pages A117 ( year 2021 ). 2105.04792

    2021 arXiv

  47. [55]

    author Veilleux , S. et al. title Spitzer Quasar and Ulirg Evolution Study (QUEST). IV. Comparison of 1 Jy Ultraluminous Infrared Galaxies with Palomar-Green Quasars . journal volume 182 , pages 628--666 ( year 2009 ). 0905.1577

    2009 arXiv

  48. [56]

    author Markwardt , C. B. title Non-linear Least-squares Fitting in IDL with MPFIT . In editor Bohlender , D. A. , editor Durand , D. & editor Dowler , P. (eds.) booktitle Astronomical Data Analysis Software and Systems XVIII , vol. volume 411 of series Astronomical Society of ...

    2009 arXiv

  49. [57]

    author Mogensen, P. K. & author Riseth, A. N. title Optim: A mathematical optimization package for Julia . journal Journal of Open Source Software volume 3 , pages 615 ( year 2018 )

    2018

  50. [58]

    , author Dere , K

    author Del Zanna , G. , author Dere , K. P. , author Young , P. R. & author Landi , E. title CHIANTI An Atomic Database for Emission Lines. XVI. Version 10, Further Extensions . journal volume 909 , pages 38 ( year 2021 ). 2011.05211

    2021 arXiv

  51. [59]

    author Fielding , D. B. & author Bryan , G. L. title The Structure of Multiphase Galactic Winds . journal volume 924 , pages 82 ( year 2022 ). 2108.05355

    2022 arXiv

  52. [60]

    author Meena , B. et al. title Investigating the Narrow-line Region Dynamics in Nearby Active Galaxies . journal volume 943 , pages 98 ( year 2023 ). 2212.02513

    2023 arXiv

  53. [61]

    , author Tombesi , F

    author Gaspari , M. , author Tombesi , F. & author Cappi , M. title Linking macro-, meso- and microscales in multiphase AGN feeding and feedback . journal Nature Astronomy volume 4 , pages 10--13 ( year 2020 ). 2001.04985

    2020 arXiv

  54. [62]

    author Groves , B. A. , author Dopita , M. A. & author Sutherland , R. S. title Dusty, Radiation Pressure-Dominated Photoionization. II. Multiwavelength Emission Line Diagnostics for Narrow-Line Regions . journal volume 153 , pages 75--91 ( year 2004 ). astro-ph/0404176

    2004 arXiv

  55. [63]

    author Allen , M. G. , author Groves , B. A. , author Dopita , M. A. , author Sutherland , R. S. & author Kewley , L. J. title The MAPPINGS III Library of Fast Radiative Shock Models . journal volume 178 , pages 20--55 ( year 2008 ). 0805.0204

    2008 arXiv

  56. [64]

    author Kewley , L. J. , author Dopita , M. A. , author Sutherland , R. S. , author Heisler , C. A. & author Trevena , J. title Theoretical Modeling of Starburst Galaxies . journal volume 556 , pages 121--140 ( year 2001 ). astro-ph/0106324

    2001 arXiv

  57. [65]

    author Timmerman , R. et al. title Very Large Array observations of the mini-halo and AGN feedback in the Phoenix cluster . journal volume 646 , pages A38 ( year 2021 ). 2009.13238

    2021 arXiv

  58. [66]

    author Begelman , M. C. & author Fabian , A. C. title Turbulent mixing layers in the interstellar and intracluster medium. journal volume 244 , pages 26P--29 ( year 1990 )

    1990

  59. [67]

    author Slavin , J. D. , author Shull , J. M. & author Begelman , M. C. title Turbulent Mixing Layers in the Interstellar Medium of Galaxies . journal volume 407 , pages 83 ( year 1993 )

    1993

  60. [68]

    & author Shelton , R

    author Kwak , K. & author Shelton , R. L. title Numerical Study of Turbulent Mixing Layers with Non-equilibrium Ionization Calculations . journal volume 719 , pages 523--539 ( year 2010 ). 1006.3811

    2010 arXiv

  61. [69]

    title Solar System Abundances and Condensation Temperatures of the Elements

    author Lodders , K. title Solar System Abundances and Condensation Temperatures of the Elements . journal volume 591 , pages 1220--1247 ( year 2003 )

    2003

  62. [70]

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

    ENTRY address archive author booktitle chapter edition editor eprint howpublished institution journal key month note number organization pages publisher school series title type url volume year label INTEGERS output.state before.all mid.sentence after.sentence after.block FUNC...

  63. [71]

    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 gl...

Pith tools

Reviewed August 8, 2026 · model on record in the stance chip above.