Kinematics of the SN Refsdal host revealed by MUSE: a regularly rotating spiral galaxy at z ≃ 1.5

Teodoro, Enrico M. Di; Grillo, C.; Fraternali, Filippo; Gobat, R.; Karman, W.; Mercurio, A.; Rosati, P.; Balestra, I.; Caminha, G. B.; Caputi, K.; Lombardi, Marco; Suyu, S. H.; Treu, Tommaso; Vanzella, E.

doi:10.1093/mnras/sty175

Cited by 18 publications

(15 citation statements)

References 72 publications

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“…Several authors have shown indeed that, if the effect of beam smearing is properly taken into account, the velocity dispersions in distant galaxies are comparable to or only slightly larger than in local galaxies (e.g. Di Teodoro et al 2016Teodoro et al , 2018Lelli et al 2018).…”

Section: Gravitational Energymentioning

confidence: 99%

Evidence for supernova feedback sustaining gas turbulence in nearby star-forming galaxies

Fraternali

Iorio

Pezzulli

et al. 2020

A&A

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It is widely known that the gas in galaxy discs is highly turbulent, but there is much debate on which mechanism can energetically maintain this turbulence. Among the possible candidates, supernova (SN) explosions are likely the primary drivers but doubts remain on whether they can be sufficient in regions of moderate star formation activity, in particular in the outer parts of discs. Thus, a number of alternative mechanisms have been proposed. In this paper, we measure the SN efficiency η, namely the fraction of the total SN energy needed to sustain turbulence in galaxies, and verify that SNe can indeed be the sole driving mechanism. The key novelty of our approach is that we take into account the increased turbulence dissipation timescale associated with the flaring in outer regions of gaseous discs. We analyse the distribution and kinematics of HI and CO in ten nearby star-forming galaxies to obtain the radial profiles of the kinetic energy per unit area for both the atomic gas and the molecular gas. We use a theoretical model to reproduce the observed energy with the sum of turbulent energy from SNe, as inferred from the observed star formation rate (SFR) surface density, and the gas thermal energy. For the atomic gas, we explore two extreme cases in which the atomic gas is made either of cold neutral medium or warm neutral medium, and the more realistic scenario with a mixture of the two phases. We find that the observed kinetic energy is remarkably well reproduced by our model across the whole extent of the galactic discs, assuming η constant with the galactocentric radius. Taking into account the uncertainties on the SFR surface density and on the atomic gas phase, we obtain that the median SN efficiencies for our sample of galaxies are ⟨ηatom⟩ = 0.015−0.008+0.018 for the atomic gas and ⟨ηmol⟩ = 0.003−0.002+0.006 for the molecular gas. We conclude that SNe alone can sustain gas turbulence in nearby galaxies with only few percent of their energy and that there is essentially no need for any further source of energy.

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Section: Gravitational Energymentioning

confidence: 99%

Evidence for supernova feedback sustaining gas turbulence in nearby star-forming galaxies

Fraternali

Iorio

Pezzulli

et al. 2020

A&A

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show abstract

“…Moreover, the remaining SN energy could be spent to drive galactic winds (e.g. Fraternali et al 2004;Veilleux et al 2005;Rubin et al 2014;Cresci et al 2017;Di Teodoro et al 2018;Armillotta et al 2019).…”

Section: Galaxymentioning

confidence: 99%

Evidence for supernova feedback sustaining gas turbulence in nearby star-forming galaxies

Bacchini,

Fraternali,

Iorio

et al. 2020

Preprint

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It is well known that gas in galaxy discs is highly turbulent, but there is much debate on which mechanism can energetically maintain this turbulence. Among the possible candidates, supernova (SN) explosions are likely the primary drivers but doubts remain on whether they can be sufficient in regions of moderate star formation activity, in particular in the outer parts of discs. Thus, a number of alternative mechanisms have been proposed. In this paper, we measure the SN efficiency η, namely the fraction of the total SN energy needed to sustain turbulence in galaxies, and verify that SNe can indeed be the sole driving mechanism. The key novelty of our approach is that we take into account the increased turbulence dissipation timescale associated to the flaring in outer regions of gaseous discs. We analyse the distribution and kinematics of HI and CO in 10 nearby star-forming galaxies to obtain the radial profiles of the kinetic energy per unit area, for both the atomic gas and the molecular gas. We use a theoretical model to reproduce the observed energy with the sum of turbulent energy from SNe, as inferred from the observed star formation rate (SFR) surface density, and the gas thermal energy. For the atomic gas, we explore two extreme cases in which the atomic gas is made either of cold neutral medium or warm neutral medium, and the more realistic scenario with a mixture of the two phases. We find that the observed kinetic energy is remarkably well reproduced by our model across the whole extent of the galactic discs, assuming η constant with the galactocentric radius. Taking into account the uncertainties on the SFR surface density and on the atomic gas phase, we obtain that the median SN efficiencies for our sample of galaxies are η atom = 0.015 +0.018 −0.008 for the atomic gas and η mol = 0.003 +0.006 −0.002 for the molecular gas. We conclude that SNe alone can sustain gas turbulence in nearby galaxies with only few percent of their energy and that there is essentially no need for any further source of energy.

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“…We optimize the strong-lensing model (cluster mass and cosmological) parameters with uniform priors, over the positions of 89 observed and reliable multiple images belonging to 10 different sources (1.240 ≤ z ≤ 3.703) and to 18 knots of the SN Refsdal host (z = 1.489), further validated by MUSE velocities from [O II] emission (see Figures 8 and 9 in G16 and Di Teodoro et al 2018). As detailed in G16, the considered positional uncertainty of each image is 0.26 ′′ in order to get a χ 2 value that is comparable to the number of the degrees of freedom (except for the 5 multiple images of SN Refsdal, S1-S4 and SX, for which we use 0.13 ′′ ).…”

Section: Lensing Observablesmentioning

confidence: 99%

Measuring the Value of the Hubble Constant “à la Refsdal”

Grillo

Rosati

Suyu

et al. 2018

ApJ

110

111

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Realizing Refsdal's original idea from 1964, we present estimates of the Hubble constant that are complementary to and potentially competitive with those of other cosmological probes. We use the observed positions of 89 multiple images, with extensive spectroscopic information, from 28 background sources and the measured time delays between the images S1-S4 and SX of supernova "Refsdal" (z = 1.489), which were obtained thanks to Hubble Space Telescope (HST ) deep imaging and Multi Unit Spectroscopic Explorer (MUSE) data. We extend the strong lensing modeling of the Hubble Frontier Fields (HFF) galaxy cluster MACS J1149.5+2223 (z = 0.542), published by Grillo et al. (2016), and explore different ΛCDM models. Taking advantage of the lensing information associated to the presence of very close pairs of multiple images at various redshifts and to the extended surface brightness distribution of the SN Refsdal host, we can reconstruct the total mass density profile of the cluster very precisely. The combined dependence of the multiple image positions and time delays on the cosmological parameters allows us to infer the values of H 0 and Ω m with relative (1σ) statistical errors of, respectively, 6% (7%) and 31% (26%) in flat (general) cosmological models, assuming a conservative 3% uncertainty on the final time delay of image SX and, remarkably, no priors from other cosmological experiments. Our best estimate of H 0 , based on the model described in this work, will be presented when the final time-delay measurement becomes available. Our results show that it is possible to utilize time delays in lens galaxy clusters as an important alternative tool for measuring the expansion rate and the geometry of the Universe.

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Kinematics of the SN Refsdal host revealed by MUSE: a regularly rotating spiral galaxy at z ≃ 1.5

Cited by 18 publications

References 72 publications

Evidence for supernova feedback sustaining gas turbulence in nearby star-forming galaxies

Evidence for supernova feedback sustaining gas turbulence in nearby star-forming galaxies

Evidence for supernova feedback sustaining gas turbulence in nearby star-forming galaxies

Measuring the Value of the Hubble Constant “à la Refsdal”

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