The Outskirts of Abell 1795: Probing Gas Clumping in the Intra-Cluster Medium

The outskirts of galaxy clusters host complex interactions between the intra-cluster and circumcluster media. During cluster evolution, ram-pressure stripped gas clumps from infalling substructures break the uniformity of the gas distribution, which may lead to observational biases at large radii. Assessing the contribution of gas clumping, however, poses observational challenges, and requires robust X-ray measurements in the background-dominated regime of cluster outskirts. The aims of this work are isolating faint gas clumps from field sources and from the diffuse emission in the Abell 1795 galaxy cluster, then probing their impact on the observed surface brightness and thermodynamic profiles. We performed imaging analysis on deep Chandra ACIS-I observations of the outskirts of Abell 1795, extending to $\sim1.5r_{200}$ with full azimuthal coverage. We built the $0.7-2.0$ keV surface brightness distribution from the adaptively binned image of the diffuse emission and looked for clumps as $>2\sigma$ outliers. Classification of the clump candidates was based on Chandra and SDSS data. Benefiting from the Chandra point source list, we extracted the thermodynamic profiles of the intra-cluster medium from the associated Suzaku XIS data out to $r_{200}$ using multiple point source and clump candidate removal approaches. We identified 24 clump candidates in the Abell 1795 field, most of which are likely associated with background objects, including AGN, galaxies, and clusters or groups of galaxies, as opposed to intrinsic gas clumps. These sources had minimal impact on the surface brightness and thermodynamic profiles of the cluster emission. After correcting for clump candidates, the measured entropy profile still deviates from a pure gravitational collapse, suggesting complex physics at play in the outskirts, including potential electron-ion non-equilibrium and non-thermal pressure support.Comment: 22 pages, 14 figures, submitted to Astronomy & Astrophysic

The diverse hot gas content and dynamics of optically similar low-mass elliptical galaxies

The presence of hot X-ray emitting gas is ubiquitous in massive early-type galaxies. However, much less is known about the content and physical status of the hot X-ray gas in low-mass ellipticals. In the present paper we study the X-ray gas content of four low-mass elliptical galaxies using archival Chandra X-ray observations. The sample galaxies, NGC821, NGC3379, NGC4278, and NGC4697, have approximately identical K-band luminosities, and hence stellar masses, yet their X-ray appearance is strikingly different. We conclude that the unresolved emission in NGC821 and NGC3379 is built up from a multitude of faint compact objects, such as coronally active binaries and cataclysmic variables. Despite the non-detection of X-ray gas, these galaxies may host low density, and hence low luminosity, X-ray gas components, which undergo a Type Ia supernova (SN Ia) driven outflow. We detect hot X-ray gas with a temperature of kT ~ 0.35 keV in NGC4278, the component of which has a steeper surface brightness distribution than the stellar light. Within the central 50 arcsec (~3.9 kpc) the estimated gas mass is ~3 x 10^7 M_sun, implying a gas mass fraction of ~0.06%. We demonstrate that the X-ray gas exhibits a bipolar morphology in the northeast-southwest direction, indicating that it may be outflowing from the galaxy. The mass and energy budget of the outflow can be maintained by evolved stars and SNe Ia, respectively. The X-ray gas in NGC4697 has an average temperature of kT ~ 0.3 keV, and a significantly broader distribution than the stellar light. The total gas mass within 90 arcsec (~5.1 kpc) is ~2.1 x 10^8 M_sun, hence the gas mass fraction is ~0.4%. Based on the distribution and physical parameters of the X-ray gas, we conclude that it is most likely in hydrostatic equilibrium, although a subsonic outflow may be present.Comment: 14 pages, 8 figures, 3 tables, accepted for publication in Ap

Scolioticus gerinc moiréfelvételeinek szoftveres szegmentációja

A scolioticus gerinc vizsgálatára a röntgenfelvételek részleges alternatíváját nyújtja a hátfelszín moiréfelvételeinek elemzése. A scoliosis moiréjelenségen alapuló diagnosztikájában a moiréfelvételek általánosan megbízható, gyors és precíz szegmentációja szignifikáns szerepet tölt be, és még kidolgozásra vár.  Ez a kutatás a moiréfelvételek szegmentációjára kíván megoldási javaslatot tenni digitális (projekciós) moirétechnika és XOR-logika alkalmazásával létrehozott moiréfelvételek manuális/félautomatikus szegmentációjára kifejlesztett szoftveralapú megoldással, a Moiré Fringe Segmentation Tool prototípusával. A prototípus MATLAB App Designer alkalmazásban készült, és képszűrési és morfológiai műveletekkel biztosítja a moirésávok szegmentációját (1) fényerő- és (2) kontrasztjavítás, (3) 2-D Gauss-féle elmosás, (4) küszöbölés, (5) hisztogram kiegyenlítés, (6) inverzió, valamint a (7) szkeletonizáció implementálásával. A szoftver a moirésávok szegmentációját kvázi valós időben, manuálisan állítható szűrési és morfológiai képfeldolgozási műveletekkel, valamint előre meghatározott szekvencián alapuló, beépített algoritmussal támogatja. A prototípus alkalmazhatóságát egyszerű, gyors és a felvételek moirésávjainak nagy részét pontosan lekövető szegmentálás igazolja. Az eredmények azt mutatják, hogy a prototípus koncepciója megfelelő alapot nyújt a moirésávok szegmentációjához és további, kiterjesztett képfeldolgozási műveletekkel operáló kutatás-fejlesztéshez. Egyszerűségének és gyors működésének következtében a prototípus továbbfejlesztett megoldása helyettesítheti az időigényes és komplex szegmentálási módszereket is

Predictions for the X-ray circumgalactic medium of edge-on discs and spheroids

We investigate how the X-ray circumgalactic medium (CGM) of present-day galaxies depends on galaxy morphology and azimuthal angle using mock observations generated from the EAGLE cosmological hydrodynamic simulation. By creating mock stacks of {\it eROSITA}-observed galaxies oriented to be edge-on, we make several observationally-testable predictions for galaxies in the stellar mass range $M_\star=10^{10.7-11.2}\;$M$_{\odot}$. The soft X-ray CGM of disc galaxies is between 60 and 100\% brighter along the semi-major axis compared to the semi-minor axis, between 10-30 kpc. This azimuthal dependence is a consequence of the hot ($T>10^6$ K) CGM being non-spherical: specifically it is flattened along the minor axis such that denser and more luminous gas resides in the disc plane and co-rotates with the galaxy. Outflows enrich and heat the CGM preferentially perpendicular to the disc, but we do not find an observationally-detectable signature along the semi-minor axis. Spheroidal galaxies have hotter CGMs than disc galaxies related to spheroids residing at higher halos masses, which may be measurable through hardness ratios spanning the $0.2-1.5$ keV band. While spheroids appear to have brighter CGMs than discs for the selected fixed $M_\star$ bin, this owes to spheroids having higher stellar and halo masses within that $M_\star$ bin, and obscures the fact that both simulated populations have similar total CGM luminosities at the exact same $M_\star$. Discs have brighter emission inside 20 kpc and more steeply declining profiles with radius than spheroids. We predict that the {\it eROSITA} 4-year all-sky survey should detect many of the signatures we predict here, although targeted follow-up observations of highly inclined nearby discs after the survey may be necessary to observe some of our azimuthally-dependent predictions.Comment: 12 pages, 11 figures, 1 table. Submitted to MNRAS. Comments welcom

X-ray metal line emission from the hot circumgalactic medium: probing the effects of supermassive black hole feedback

We derive predictions from state-of-the-art cosmological galaxy simulations for the spatial distribution of the hot circumgalactic medium (CGM, ${\rm [0.1-1]R_{200c}}$) through its emission lines in the X-ray soft band ($[0.3-1.3]$ keV). In particular, we compare IllustrisTNG, EAGLE, and SIMBA and focus on galaxies with stellar mass 10^{10-11.6}\, \MSUN at $z=0$. The three simulation models return significantly different surface brightness radial profiles of prominent emission lines from ionized metals such as OVII(f), OVIII, and FeXVII as a function of galaxy mass. Likewise, the three simulations predict varying azimuthal distributions of line emission with respect to the galactic stellar planes, with IllustrisTNG predicting the strongest angular modulation of CGM physical properties at radial range ${\gtrsim0.3-0.5\,R_{200c}}$. This anisotropic signal is more prominent for higher-energy lines, where it can manifest as X-ray eROSITA-like bubbles. Despite different models of stellar and supermassive black hole (SMBH) feedback, the three simulations consistently predict a dichotomy between star-forming and quiescent galaxies at the Milky-Way and Andromeda mass range, where the former are X-ray brighter than the latter. This is a signature of SMBH-driven outflows, which are responsible for quenching star formation. Finally, we explore the prospect of testing these predictions with a microcalorimeter-based X-ray mission concept with a large field-of-view. Such a mission would probe the extended hot CGM via soft X-ray line emission, determine the physical properties of the CGM, including temperature, from the measurement of line ratios, and provide critical constraints on the efficiency and impact of SMBH feedback on the CGM.Comment: 21 pages, 15 figures. Submitted to MNRAS and received a positive referee repor

A Spectacular Bow Shock in the 11 keV Galaxy Cluster Around 3C 438

This is a pre-copyedited, author-produced pdf of an article accepted for publication in The Astrophysical Journal following peer review. The version of record, Deanna L. Emery; Ákos Bogdán; Ralph P. Kraft; Felipe Andrade-Santos; William R. Forman; Martin Hardcastle; and Christine Jones, ‘A spectacular bow shock in the 11 keV galaxy cluster around 3C 438’, The Astrophysical Journal (2017) 834(2):159 (7pp), published 10 January 2017, is available at doi: 10.3847/1538-4357/834/2/159 © 2017. The American Astronomical Society. All rights reserved.We present results of deep 153 ks Chandra observations of the hot, 11 keV, galaxy cluster associated with the radio galaxy 3C 438. By mapping the morphology of the hot gas and analyzing its surface brightness and temperature distributions, we demonstrate the presence of a merger bow shock. We identify the presence of two jumps in surface brightness and in density located at $\sim$400 kpc and $\sim$800 kpc from the cluster's core. At the position of the inner jump, we detect a factor of $2.3\pm 0.2$ density jump, while at the location of the outer jump, we detect a density drop of a factor of $3.5 \pm 0.7$. Combining this with the temperature distribution within the cluster, we establish that the pressure of the hot gas is continuous at the 400 kpc jump, while there is a factor of $6.2 \pm 2.8$ pressure discontinuity at 800 kpc jump. From the magnitude of the outer pressure discontinuity, using the Rankine-Hugoniot jump conditions, we determine that the sub-cluster is moving at $M = 2.3\pm 0.5$, or approximately $2600\pm 565$ km/s through the surrounding intracluster medium, creating the conditions for a bow shock. Based on these findings, we conclude that the pressure discontinuity is likely the result of an ongoing major merger between two massive clusters. Since few observations of bow shocks in clusters have been made, this detection can contribute to the study of the dynamics of cluster mergers, which offers insight on how the most massive clusters may have formed.Peer reviewe

Constraints From Dwarf Galaxies on Black Hole Seeding and Growth Models With Current and Future Surveys

Dwarf galaxies are promising test beds for constraining models of supermassive and intermediate-mass black holes (MBHs) via their BH occupation fraction (BHOF). Disentangling seeding from the confounding effects of mass assembly over a Hubble time is a challenging problem that we tackle in this study with a suite of semianalytical models (SAMs). We show how the measured BHOF depends on the lowest BH mass or active galactic nucleus (AGN) luminosity achieved by a survey. To tell seeding models apart, we need to detect or model all AGNs brighter than 10 ^37 erg s ^−1 in galaxies of M _* ∼ 10 ^8−10 M _⊙ . Shallower surveys, like eRASS, cannot distinguish between seed models even with the compensation of a much larger survey volume. We show that the AMUSE survey, with its inference of the MBH population underlying the observed AGNs, strongly favors heavy seed models, growing with either a power-law Eddington ratio distribution function or one in which BH accretion is tied to the star formation rate (i.e., the AGN-main sequence, AGN-MS, model). These two growth channels can then be distinguished by the AGN luminosity function at >10 ^40 erg s ^−1 , with the AGN-MS model requiring more accretion than observed at z ∼ 0. Thus, current X-ray observations favor heavy seeds whose Eddington ratios follow a power-law distribution. The different models also predict different radio scaling relations, which we quantify using the fundamental plane of BH activity. We close with recommendations for the design of upcoming multiwavelength campaigns that can optimally detect MBHs in dwarf galaxies