Simulating the impact of dust cooling on the statistical properties of the intra-cluster medium

Pointecouteau, É.; Silva, Antônio da; Catalano, A.; Montier, L.; Lanoux, J.; Roncarelli, M.; Giard, M.

doi:10.1016/j.asr.2009.05.006

Cited by 7 publications

(6 citation statements)

References 20 publications

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“…Da found a 25% normalisation change for the LX − M relation and a 10% change for the Y − M and S − M cluster scaling relations in the presence of dust. Similarly, Pointecouteau et al (2009) found changes in the LX − M relation by as much as 10% for clusters with temperatures around 1 keV for models that include dust cooling. However, those results are based on simplified dust models and it is currently unclear whether they capture the correct physical behaviour.…”

Section: Introductionmentioning

confidence: 72%

Dust in and around galaxies: dust in cluster environments and its impact on gas cooling

Vogelsberger

McKinnon

O'Neil

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Simulating the dust content of galaxies and their surrounding gas is challenging due to the wide range of physical processes affecting the dust evolution. Here we present cosmological hydrodynamical simulations of a cluster of galaxies, M 200,crit = 6 × 10 14 M , including a novel dust model for the moving mesh code AREPO. This model includes dust production, growth, supernova-shock-driven destruction, ion-collision-driven thermal sputtering, and high temperature dust cooling through far infrared re-radiation of collisionally deposited electron energies. Adopting a rather low thermal sputtering rate, we find, consistent with observations, a present-day overall dust-to-gas ratio of ∼ 2 × 10 −5 , a total dust mass of ∼ 2 × 10 9 M , and a dust mass fraction of ∼ 3 × 10 −6 . The typical thermal sputtering timescales within ∼ 100 kpc are around ∼ 10 Myr, and increase towards the outer parts of the cluster to ∼ 10 3 Myr at a cluster-centric distance of 1 Mpc. The condensation of gas phase metals into dust grains reduces high temperature metal-line cooling, but also leads to additional dust infrared cooling. The additional infrared cooling changes the overall cooling rate in the outer parts of the cluster, beyond ∼ 1 Mpc, by factors of a few. This results in noticeable changes of the entropy, temperature, and density profiles of cluster gas once dust formation is included. The emitted dust infrared emission due to dust cooling is consistent with observational constraints.

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Section: Introductionmentioning

confidence: 72%

Dust in and around galaxies: dust in cluster environments and its impact on gas cooling

Vogelsberger

McKinnon

O'Neil

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…At scales of hundreds of kiloparsec hot gas (10 6 − 10 7 K) needs to cool in order to accrete into galaxies to fuel their on-going star-formation. The classical explanation for the cooling of gas is through bremstrahlung or line emission in the Xray, although inelastic collisions with dust grains is the most efficient mechanism for gas cooling at these temperatures (Dwek & Werner 1981;Popescu et al 2000a;Montier & Giard 2004;Pointecouteau et al 2009;Natale et al 2010;Vogelsberger et al 2018), providing grains exist in the IGM around star-forming galaxies. At kiloparsec scales within the disc of galaxies dust grains heat the ISM via the photoelectric effect and the thermodynamic balance of the gas is maintained through an equality between the photoelectric heating and the FIR cooling lines powered by inellastic collisions with gas particles (e.g.…”

Section: ;mentioning

confidence: 99%

A radiative transfer model for the spiral galaxy M33★

Thirlwall

Popescu

Tuffs

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present the first radiative transfer (RT) model of a non-edge-on disk galaxy in which the large-scale geometry of stars and dust is self-consistently derived through fitting of multiwavelength imaging observations from the UV to the submm. To this end we used the axi-symmetric RT model of Popescu et al. and a new methodology for deriving geometrical parameters, and applied this to decode the spectral energy distribution (SED) of M33. We successfully account for both the spatial and spectral energy distribution, with residuals typically within 7% in the profiles of surface brightness and within 8% in the spatially-integrated SED. We predict well the energy balance between absorption and re-emission by dust, with no need to invoke modified grain properties, and we find no submm emission that is in excess of our model predictions. We calculate that 80 ± 8% of the dust heating is powered by the young stellar populations. We identify several morphological components in M33, a nuclear, an inner, a main and an outer disc, showing a monotonic trend in decreasing star-formation surface-density (Σ SFR ) from the nuclear to the outer disc. In relation to surface density of stellar mass, the Σ SFR of these components define a steeper relation than the "main sequence" of star-forming galaxies, which we call a "structurally resolved main sequence". Either environmental or stellar feedback mechanisms could explain the slope of the newly defined sequence. We find the star-formation rate to be SFR = 0.28 +0.02 −0.01 M yr −1 .

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“…Thus, the ICD in Virgo acts as a gas coolant and contributes to a change in the statistical properties of the Virgo ICM (e.g. Montier & Giard 2004;Pointecouteau et al 2009;Vogelsberger et al 2019).…”

Section: Physical Properties Of the Virgo Dustmentioning

confidence: 99%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Longobardi

Boselli

Boissier

et al. 2020

A&A

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Aims. We present the first detection of diffuse dust in the intra-cluster medium of the Virgo cluster out to ∼0.4 virial radii, and study the radial variation of its properties on a radial scale of the virial radius. Methods. Analysing near-UV – i colours for a sample of ∼12 000 background galaxies with redshifts 0.02 < z < 0.8, we find significant colour reddening and relate it to variation in E(B − V) values. Results. The E(B − V) mean profile shows a dust component characterised by an average reddening E(B − V) ∼ 0.042 ± 0.004 mag within 1.5 degrees (∼0.3 rvir) from the cluster centre. Assuming a Large Magellanic Cloud extinction law, we derive an average visual extinction AV = 0.14 ± 0.01 for a total dust mass, Md = 2.5 ± 0.2 × 109 M⊙, hence a dust-to-gas mass ratio Md/Mg = 3.0 ± 0.3 × 10−4. Based on the upper limits on the flux density I250μm = 0.1 MJy sr−1 derived from Herschel data, we estimate an upper limit for the dust temperature of Td ∼ 10 K. However, similar densities can be obtained with dust at higher temperatures with lower emissivities. Conclusions. The Virgo cluster has diffuse dust in its intra-cluster medium characterised by different physical properties as those characterising the Milky Way dust. The diffuse dust in Virgo is transported into the cluster space through similar phenomena (stripping) as those building up the optical intra-cluster light, and it constitutes an additional cooling agent of the cluster gas.

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Simulating the impact of dust cooling on the statistical properties of the intra-cluster medium

Cited by 7 publications

References 20 publications

Dust in and around galaxies: dust in cluster environments and its impact on gas cooling

Dust in and around galaxies: dust in cluster environments and its impact on gas cooling

A radiative transfer model for the spiral galaxy M33★

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

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