scholarly journals Exploring the hot gaseous halo around an extremely massive and relativistic jet launching spiral galaxy with XMM−Newton

2020 ◽  
Vol 500 (2) ◽  
pp. 2503-2513
Author(s):  
M S Mirakhor ◽  
S A Walker ◽  
J Bagchi ◽  
A C Fabian ◽  
A J Barth ◽  
...  
Keyword(s):  
Spiral Galaxy ◽  
Mass Fraction ◽  
X Ray ◽  
Inverse Compton Scattering ◽  
Systematic Uncertainties ◽  
Relativistic Jet ◽  
Baryon Mass ◽  
The Galaxy ◽  
Metal Abundance ◽  
Gaseous Halo

ABSTRACT We present a deep XMM−Newton observation of the extremely massive, rapidly rotating, relativistic-jet-launching spiral galaxy 2MASX J23453268−0449256. Diffuse X-ray emission from the hot gaseous halo around the galaxy is robustly detected out to a radius of 160 kpc, corresponding roughly to 35 per cent of the virial radius (≈450 kpc). We fit the X-ray emission with the standard isothermal β model, and it is found that the enclosed gas mass within 160 kpc is $1.15_{-0.24}^{+0.22} \times 10^{11} \, \rm {M}_{\odot }$. Extrapolating the gas mass profile out to the virial radius, the estimated gas mass is $8.25_{-1.77}^{+1.62} \times 10^{11} \, \rm {M}_{\odot }$, which makes up roughly 65 per cent of the total baryon mass content of the galaxy. When the stellar mass is considered and accounting for the statistical and systematic uncertainties, the baryon mass fraction within the virial radius is $0.121_{-0.043}^{+0.043}$, in agreement with the universal baryon fraction. The baryon mass fraction is consistent with all baryons falling within r200, or with only half of the baryons falling within r200. Similar to the massive spiral galaxies NGC 1961 and NGC 6753, we find a low value for the metal abundance of ≈ 0.1 Z⊙, which appears uniform with radius. We also detect diffuse X-ray emission associated with the northern and southern lobes, possibly attributed to inverse Compton scattering of cosmic microwave background photons. The estimated energy densities of the electrons and magnetic field in these radio lobes suggest that they are electron-dominated by a factor of 10−200, depending on the choice of the lower cut-off energy of the electron spectrum.

scholarly journals The Galaxy Merger Origin of Hot Gaseous Halos of Ellipticals

2004 ◽  
Vol 217 ◽  
pp. 412-417
Author(s):  
X. Y. Xia ◽  
Z. Y. Huo ◽  
S. J. Xue
Keyword(s):  
Central Region ◽  
Elliptical Galaxies ◽  
Emission Lines ◽  
Central Nucleus ◽  
Nuclear Region ◽  
Feedback Process ◽  
X Ray ◽  
The Galaxy ◽  
Low Metallicity ◽  
Gaseous Halo

We report on the properties of the hot gaseous halos of 10 nearby ultraluminous IRAS galaxies from Chandra observations. There exists diffuse soft X-ray emission surrounding the central nucleus within 10 kpc of the nuclear region with a temperature of about 0.7 keV and metallicity about Z ~ 1.0Z⊙. Also, emission lines from α elements and ions for are seen in all nearby ULIRGs in our sample. Outside the central region, the Chandra observations reveal a more extended hot gaseous halo with a temperature of about 0.6 keV and low metallicity (Z ~ 0.1Z⊙) for some of the ULIRGs. We discuss the nature and the implications of our results for the origin of X-ray halos in elliptical galaxies and the constraints this places on the feedback process.

scholarly journals The X-ray emission of E and S0 Galaxies

1996 ◽  
Vol 171 ◽  
pp. 123-130
Author(s):  
G. Fabbiano
Keyword(s):  
Gravitational Mass ◽  
X Ray ◽  
Cooling Flows ◽  
The Galaxy ◽  
Metal Abundance ◽  
S0 Galaxies

It is well known by now that E and S0 galaxies are associated with hot, X-ray emitting gaseous halos, subject to central cooling flows, but otherwise homogeneous, which can be used to trace the galaxy potential and thus measure the total gravitational mass. Recent ASCA observations suggest that these halos have a surprisingly low metal abundance.

scholarly journals Baryons in the Cosmic Web of IllustrisTNG – I: gas in knots, filaments, sheets, and voids

2019 ◽  
Vol 486 (3) ◽  
pp. 3766-3787 ◽  
Author(s):  
Davide Martizzi ◽  
Mark Vogelsberger ◽  
Maria Celeste Artale ◽  
Markus Haider ◽  
Paul Torrey ◽  
...  
Keyword(s):  
Mass Fraction ◽  
Intergalactic Medium ◽  
Volume Fraction ◽  
Phase Distribution ◽  
Relative Mass ◽  
X Ray ◽  
Star Forming ◽  
Baryon Mass ◽  
Web Classification ◽  
Mass Volume

ABSTRACT We analyse the IllustrisTNG simulations to study the mass, volume fraction, and phase distribution of gaseous baryons embedded in the knots, filaments, sheets, and voids of the Cosmic Web from redshift z = 8 to redshift z = 0. We find that filaments host more star-forming gas than knots, and that filaments also have a higher relative mass fraction of gas in this phase than knots. We also show that the cool, diffuse intergalactic medium [IGM; $T\lt 10^5 \, {\rm K}$, $n_{\rm H}\lt 10^{-4}(1+z) \, {\rm cm^{-3}}$] and the warm-hot intergalactic medium [WHIM; $10^5 \lt T\lt 10^7 \, {\rm K}$, $n_{\rm H} \lt 10^{-4}(1+z)\, {\rm cm^{-3}}$] constitute ${\sim } 39$ and ${\sim } 46{{\ \rm per\ cent}}$ of the baryons at redshift z = 0, respectively. Our results indicate that the WHIM may constitute the largest reservoir of missing baryons at redshift z = 0. Using our Cosmic Web classification, we predict the WHIM to be the dominant baryon mass contribution in filaments and knots at redshift z = 0, but not in sheets and voids where the cool, diffuse IGM dominates. We also characterize the evolution of WHIM and IGM from redshift z = 4 to redshift z = 0, and find that the mass fraction of WHIM in filaments and knots evolves only by a factor of ∼2 from redshift z = 0 to 1, but declines faster at higher redshift. The WHIM only occupies $4\!-\!11{{\ \rm per\ cent}}$ of the volume at redshift 0 ≤ z ≤ 1. We predict the existence of a significant number of currently undetected O vii and Ne ix absorption systems in cosmic filaments, which could be detected by future X-ray telescopes like Athena.

scholarly journals Imprints of mass accretion history on the shape of the intracluster medium and the TX–M relation

2019 ◽  
Vol 490 (2) ◽  
pp. 2380-2389 ◽  
Author(s):  
Huanqing Chen ◽  
Camille Avestruz ◽  
Andrey V Kravtsov ◽  
Erwin T Lau ◽  
Daisuke Nagai
Keyword(s):  
Galaxy Clusters ◽  
Bimodal Distribution ◽  
Characteristic Time Scale ◽  
Intracluster Medium ◽  
X Ray ◽  
Mass Scaling ◽  
Systematic Uncertainties ◽  
The Galaxy ◽  
Statistical Sample ◽  
The Impact

ABSTRACT We use a statistical sample of galaxy clusters from a large cosmological N-body + hydrodynamics simulation to examine the relation between morphology, or shape, of the X-ray emitting intracluster medium (ICM) and the mass accretion history of the galaxy clusters. We find that the mass accretion rate (MAR) of a cluster is correlated with the ellipticity of the ICM. The correlation is largely driven by material accreted in the last ∼4.5 Gyr, indicating a characteristic time-scale for relaxation of cluster gas. Furthermore, we find that the ellipticity of the outer regions (R ∼ R500c) of the ICM is correlated with the overall MAR of clusters, while ellipticity of the inner regions (≲0.5 R500c) is sensitive to recent major mergers with mass ratios of ≥1:3. Finally, we examine the impact of variations in cluster mass accretion history on the X-ray observable–mass scaling relations. We show that there is a continuous anticorrelation between the residuals in the TX–M relation and cluster MARs, within which merging and relaxed clusters occupy extremes of the distribution rather than form two peaks in a bimodal distribution, as was often assumed previously. Our results indicate that the systematic uncertainties in the X-ray observable–mass relations can be mitigated by using the information encoded in the apparent ICM ellipticity.

scholarly journals X-raying the galaxy pair Arp 41: no collision in NGC 1232 and three ultraluminous sources in NGC 1232A

2021 ◽  
Vol 503 (1) ◽  
pp. 997-1004
Author(s):  
Roberto Soria ◽  
Manfred W Pakull
Keyword(s):  
Late Type ◽  
Diffuse Emission ◽  
X Ray ◽  
Cosmological Distance ◽  
The Galaxy ◽  
Metal Abundance ◽  
Companion Galaxy

ABSTRACT We studied the apparent galaxy pair NGC 1232/NGC 1232A with Chandra, looking for evidence of interactions and collisions. We report that there is no cloud of diffuse emission in NGC 1232, contrary to previous claims in the literature. Instead, we find that the small ‘companion’ galaxy NGC 1232A contains three ultraluminous X-ray sources with peak 0.3–10 keV luminosities above 1040 erg s−1 (assuming a cosmological distance of ≈93 Mpc for this galaxy). For its mass, morphology, metal abundance, and bright ULX population, NGC 1232A is analogous to the more nearby late-type spiral NGC 1313.

scholarly journals Extraplanar gas and magnetic fields in the cluster spiral galaxy NGC 4569

2006 ◽  
Vol 2 (S237) ◽  
pp. 470-470
Author(s):  
S. Ryś ◽  
K. T. Chyży ◽  
M. Weżgowiec ◽  
M. Ehle ◽  
R. Beck
Keyword(s):  
Magnetic Fields ◽  
Galaxy Evolution ◽  
Spiral Galaxy ◽  
Virgo Cluster ◽  
X Ray ◽  
Gas Phases ◽  
Hot Gas ◽  
The Core ◽  
The Galaxy ◽  
Galaxy Disk

AbstractThe Virgo Cluster spiral NGC 4569 is known for its compact starburst in the core and unusual outflow of Hα emitting gas perpendicular to the galaxy disk. Recent radio polarimetric observations with the Effelsberg telescope reveal huge magnetized outflows. Preliminary results of our XMM-Newton observations uncover not only hot gas in the disk but also an extensive X-ray envelope around it. We investigate the possibility of starburst-induced galactic outflows in various gas phases and cluster influence on the galaxy evolution.

scholarly journals ROSAT Observations of NGC 4258

1997 ◽  
Vol 166 ◽  
pp. 547-550
Author(s):  
Andreas Vogler ◽  
Wolfgang Pietsch
Keyword(s):  
Interstellar Medium ◽  
Point Source ◽  
Brightness Temperature ◽  
Spiral Galaxy ◽  
Surface Brightness ◽  
Point Sources ◽  
X Rays ◽  
X Ray ◽  
The Galaxy

AbstractWe performed deep follow up observations of the active spiral galaxy NGC 4258 with the ROSAT HRI and PSPC to study the different emission components. The overall luminosity of NGC 4258 is Lx ~ 2 × 1040 erg s−1 in the 0.1 – 2.4 keV ROSAT band. Besides a weak nuclear point source (Lx ≲ 1038 erg s−1) fourteen point sources are detected in the NGC 4258 disk (integral Lx ~ 3 × 1039 erg s− 1). The bulk of the X-ray emission is not resolved. The main contributions are explained by hot interstellar medium along the anomalous spiral arms of NGC 4258 (Lx ~ 1 × 1040, T ~ 0.4 keV) and by interstellar medium escaping from NGC 4258 disk into the approaching halo hemisphere (Lx ~ 4 × 1039 erg s−1, T ~ 0.2 keV)Surface brightness, temperature and absorption profiles have been taken for the X-rays in the regions of the anomalous arms. The highest and lowest absorption was received for the NW and SE tips of the arms, respectively. Our X-ray findings are compared to a model of the anomalous arms which suggests that the bar of the galaxy causes shocks in the interstellar medium and might heat a small part of it to X-ray temperatures.

scholarly journals Fossil groups of galaxies: Are they groups? Are they fossils?

2009 ◽  
Vol 5 (H15) ◽  
pp. 287-287 ◽  
Author(s):  
Renato de Alencar Dupke ◽  
Eric Miller ◽  
Claudia Mendes de Oliveira ◽  
Laerte Sodre ◽  
Eli Rykoff ◽  
...  
Keyword(s):  
Mass Fraction ◽  
Abundance Ratio ◽  
Measured Concentration ◽  
Potential Wells ◽  
X Ray ◽  
Groups Of Galaxies ◽  
The Core ◽  
Central Galaxy ◽  
Central Regions ◽  
Metal Abundance

AbstractFossil groups present a puzzle to current theories of structure formation. Despite the low number of bright galaxies, their high velocity dispersions and high TX indicate cluster-like potential wells. Measured concentration parameters seem very high indicating early formation epochs in contradiction with the observed lack of large and well defined cooling cores. There are very few fossil groups with good quality X-ray data and their idiosyncrasies may enhance these apparent contradictions. The standard explanation for their formation suggests that bright galaxies within half the virial radii of these systems were wiped out by cannibalism forming the central galaxy. Since dry mergers, typically invoked to explain the formation of the central galaxies, are not expected to change the IGM energetics significantly, thus not preventing the formation of cooling cores, we investigate the scenario where recent gaseous (wet) mergers formed the central galaxy injecting energy and changing the chemistry of the IGM in fossil groups. We show a test for this scenario using fossil groups with enough X-ray flux in the Chandra X-ray Observatory archive by looking at individual metal abundance ratio distributions near the core. Secondary SN II powered winds would tend to erase the dominance of SN IA ejecta in the core of these systems and would help to erase previously existing cold cores. Strong SN II-powered galactic winds resulting from galaxy merging would be trapped by their deep potential wells reducing the central enhancement of SN Ia/SN II iron mass fraction ratio. The results indicate that there is a decrement in the ratio of SN Ia to SN II iron mass fraction in the central regions of the systems analyzed, varying from 99±1% in the outer regions to 85±2% within the cooling radius (Figure 1) and would inject enough energy into the IGM preventing central gas cooling. The results are consistent with a scenario of later formation epoch for fossil groups, as they are defined, when compared to galaxy clusters and normal groups.

scholarly journals A Census of Baryons in Galaxy Clusters and Groups

2007 ◽  
Vol 3 (S244) ◽  
pp. 167-175
Author(s):  
Anthony H. Gonzalez ◽  
Dennis Zaritsky ◽  
Ann I. Zabludoff
Keyword(s):  
Mass Fraction ◽  
Stellar Mass ◽  
Nearby Galaxy ◽  
Cluster Galaxy ◽  
X Ray ◽  
Galaxy Groups ◽  
Systematic Uncertainties ◽  
Stellar Component ◽  
Cluster Environment ◽  
Low Mass

AbstractWhile the baryon fraction in galaxy groups and clusters may be expected to reflect the universal value, observations of cluster baryon fractions have generally fallen short of this expectation and indicated a possible correlation with cluster mass. We present a new determination of the total baryon budget in nearby galaxy groups and clusters that includes the contributions from stars in galaxies, intracluster stars, and the intracluster medium. We find that the baryon mass fraction within r500 is independent of system mass and lower than the WMAP value. We conclude however that the present shortfall provides no compelling evidence for additional missing baryons, since it may arise due to a theoretically predicted deficit of baryons within r500 and systematic uncertainties associated with the mass determinations. With the addition of the ICL to the stellar mass in galaxies, the increase in X-ray gas mass fraction with increasing total mass is entirely accounted for by a decrease in the total stellar mass fraction, supporting the argument that the behavior of both the stellar and X-ray gas components is dominated by a decrease in star formation efficiency in more massive environments. Within just the stellar component, the fraction of the total stellar luminosity in the central, giant brightest cluster galaxy (BCG) and ICL (hereafter the BCG+ICL component) decreases as velocity dispersion (σ) increases, suggesting that ICL may grow less efficiently in higher mass environments. The identification of low mass groups with large BCG+ICL components also demonstrates that the massive cluster environment is not required to form intracluster stars. These proceedings are a condensed version of the work presented in Gonzalez, Zaritsky & Zabludoff (2007), and we refer the reader to that paper for a more complete discussion.

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