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Cosmological parameter dependence of hb h P e i. The blue line is the ratio of hb h P e i predicted by the halo model with Planck 2015 and WMAP7 parameters. The orange line is the ratio of hb h P e i predicted by MTNG and Magneticum simulations ("Box2b").
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The statistics of thermal gas pressure are a new and promising probe of cosmology and astrophysics. The large-scale cross-correlation between galaxies and the thermal Sunyaev-Zeldovich effect gives the bias-weighted mean electron pressure, ⟨ b h P e ⟩ . In this paper, we show that ⟨ b h P e ⟩ is sensitive to the amplitude of fluctuations in matter...
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Context 1
... more closely at Fig. 5, we find that the differences between the two simulations are slightly smaller than what we expect based on the halo model calculations. A precise quantification of the expected discrepancy due to the shift in cosmology requires a set of simulations with a fixed galaxy formation model and varied cosmological parameters, which is ...
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... high redshift, the two simulations differ dramatically. The differences are much larger than expected from the cosmological parameter dependence. Using Eq. (23), we calculate the ratio of hb h P e i in two cosmological models, Planck 2015 (MTNG) and WMAP7 (Magneticum). The results shown in Fig. 5 indicate that the difference due to cosmology is expected to be nearly independent of the redshift. This suggests that the tSZ effect at high redshift (z > 2) is sensitive to the details of baryonic processes and galaxy ...
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Citations
The kinematic Sunyaev-Zel'dovich (kSZ) effect has been detected at z < 1 using various techniques and data sets. The ongoing and upcoming spectroscopic galaxy surveys such as DESI (Dark Energy Spectroscopic Instrument) and PFS (Prime Focus Spectrograph) will push the detection beyond z = 1, and therefore map the baryon distribution at high redshifts. Such detection can be achieved by both the kSZ stacking and tomography methods. While the two methods are theoretically equivalent, they differ significantly in the probed physics and scales, and required data sets. Taking the combination of PFS and ACT (Atacama Cosmology Telescope) as an example, we build mocks of kSZ and galaxies, quantify the kSZ detection S/N, and compare between the two methods. We segment the PFS galaxies into three redshift bins: 0.6 < z < 1.0, 1.0 < z < 1.6, and 1.6 < z < 2.4. For tomography method, our analysis reveals that the two higher redshift bins exhibit significantly higher S/N ratios, with values of 32 and 28, respectively, compared to the first redshift bin, which yielded an S/N of 8. This is attributed to not only the increasing of electron density with redshifts, but also the larger survey volume and the reduced non-linearity, facilitating velocity reconstruction at higher redshifts. Therefore, the capability of the PFS survey to measure high redshift kSZ effect stands as a substantial advantage over other spectroscopic surveys at lower redshift. The S/N of kSZ stacking largely depends on the number of galaxy groups available from another photometric survey. But in general, its S/N is lower than that of kSZ tomography, largely due to CMB instrument noise and error in galaxy group redshift. Incorporating next-generation CMB surveys like CMB-S4, characterized by significantly reduced instrument noise and improved angular resolution, is expected to enhance tomographic detection by a factor of ten and stacking detection by fivefold. This future high S/N detection holds the promise of not only providing precise constraints on the overall baryon abundance but also initiating a new insight into baryon distribution.
Firmly anchored on observational data, giant radio lobes from massive galaxies hosting supermassive black holes can exert a major negative feedback effect, by endowing the intergalactic gas with significant magnetic pressure hence retarding or preventing gas accretion onto less massive halos in the vicinity. Since massive galaxies that are largely responsible for producing the giant radio lobes, this effect is expected to be stronger in more overdense large-scale environments, such as proto-clusters, than in underdense regions, such as voids. We show that by redshift z=2 halos with masses up to (10^{11-12}, 10^{12-13})\msun are significantly hindered from accreting gas due to this effect for radio bubble volume filling fraction of , respectively. Since the vast majority of the stars in the universe at form precisely in those halos, this negative feedback process is likely one major culprit for causing the global downturn in star formation in the universe since. It also provides a natural explanation for the rather sudden flattening of the slope of the galaxy rest-frame UV luminosity function around . A cross-correlation between proto-clusters and Faraday rotation measures may test the predicted magnetic field. Inclusion of this external feedback process in the next generation of cosmological simulations may be imperative.
Firmly anchored on observational data, giant radio lobes from massive galaxies hosting supermassive black holes can exert a major negative feedback effect, by endowing the intergalactic gas with significant magnetic pressure hence retarding or preventing gas accretion onto less massive halos in the vicinity. Since massive galaxies that are largely responsible for producing the giant radio lobes, this effect is expected to be stronger in more overdense large-scale environments, such as protoclusters, than in underdense regions, such as voids. We show that by redshift z = 2 halos with masses up to ( 10 11 to 12 , 10 12 to 13 ) M ⊙ are significantly hindered from accreting gas due to this effect for radio bubble volume filling fraction of ( 1.0 , 0.2 ) , respectively. Since the vast majority of the stars in the universe at z < 2 to 3 form precisely in those halos, this negative feedback process is likely one major culprit for causing the global downturn in star formation in the universe. It also provides a natural explanation for the rather sudden flattening of the slope of the galaxy rest-frame UV luminosity function around z ∼ 2 . A cross-correlation between protoclusters and Faraday rotation measures may test the predicted magnetic field. Inclusion of this external feedback process in the next generation of cosmological simulations may be imperative.
We present the discovery of large radio shells around a massive pair of interacting galaxies and extended diffuse X-ray emission within the shells. The radio data were obtained with the Australian Square Kilometer Array Pathfinder (ASKAP) in two frequency bands centred at 944 MHz and 1.4 GHz, respectively, while the X-ray data are from the XMM-Newton observatory. The host galaxy pair, which consists of the early-type galaxies ESO 184-G042 and LEDA 418116, is part of a loose group at a distance of only 75 Mpc (redshift z = 0.017). The observed outer radio shells (diameter ∼145 kpc) and ridge-like central emission of the system, ASKAP J1914–5433 (Physalis), are likely associated with merger shocks during the formation of the central galaxy (ESO 184-G042) and resemble the new class of odd radio circles (ORCs). This is supported by the brightest X-ray emission found offset from the centre of the Physalis system, instead centered at the less massive galaxy, LEDA 418116. The host galaxy pair is embedded in an irregular envelope of diffuse light, highlighting on-going interactions. We complement our combined radio and X-ray study with high-resolution simulations of the circumgalactic medium (CGM) around galaxy mergers from the Magneticum project to analyse the evolutionary state of the Physalis system. We argue that ORCs / radio shells could be produced by a combination of energy release from the central AGN and subsequent lightening up in radio emission by merger shocks traveling through the CGM of these systems.
