The eROSITA Final Equatorial Depth Survey (eFEDS)

Comparat, Johan; Truong, Nhut; Merloni, A.; Pillepich, Annalisa; Ponti, G.; Driver, Simon P.; Bellstedt, Sabine; Liske, J.; Aird, James; Brüggen, M.; Bülbül, Esra; Davies, Luke J. M.; Villalba, Justo Antonio González; Georgakakis, A.; Haberl, F.; Li, Teng; Maitra, Chandreyee; Nandra, K.; Popesso, P.; Predehl, P.; Robotham, Aaron S. G.; Salvato, M.; Thorne, Jessica E.; Zhang, Yi

doi:10.1051/0004-6361/202243101

Cited by 35 publications

(15 citation statements)

References 91 publications

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Section: Gas Luminosity Scaling Relationmentioning

confidence: 99%

“…Third, recent studies have shown that the extended hot gas atmosphere can significantly impact the total observed luminosity depending on the chosen projection radius (Nica et al 2022;Comparat et al 2022). In Comparat et al (2022) in the energy range 0.5-10 keV. The mean spectrum was calculated by normalizing each galaxy spectrum to its total 0.5-10 keV emission and taking the average in each energy bin.…”

Section: Gas Luminosity Scaling Relationmentioning

confidence: 99%

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Decomposition of galactic X-ray emission with PHOX

Vladutescu-Zopp

Biffi

Dolag

2023

A&A

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Context. X-ray observations of galaxies with high spatial resolution instruments such as Chandra have revealed that major contributions to their diffuse emission originate from X-ray-bright point sources in the galactic stellar field. It has been established that these point sources, called X-ray binaries, are accreting compact objects with stellar donors in a binary configuration. They are classified according to the predominant accretion process: wind-fed in the case of high-mass donors and Roche-lobe mass transfer in the case of low-mass donors. Observationally, it is challenging to reliably disentangle these two populations from each other because of their similar spectra. Aims. We provide a numerical framework with which spatially and spectrally accurate representations of X-ray binary populations can be studied from hydrodynamical cosmological simulations. We construct average spectra, accounting for a hot gas component, and verify the emergence of observed scaling relations between galaxy-wide X-ray luminosity (L X ) and stellar mass (M * ) and between L X and the star-formation rate (SFR). Methods. Using simulated galaxy halos extracted from the (48 h −1 cMpc) 3 volume of the Magneticum Pathfinder cosmological simulations at z = 0.07, we generate mock spectra with the X-ray photon-simulator Phox. We extend the Phox code to account for the stellar component in the simulation and study the resulting contribution in composite galactic spectra. Results. Well-known X-ray binary scaling relations with galactic SFR and M * emerge self-consistently, verifying our numerical approach. Average X-ray luminosity functions are perfectly reproduced up to the one-photon luminosity limit. Comparing our resulting L X − SFR − M * relation for X-ray binaries with recent observations of field galaxies in the Virgo galaxy cluster, we find significant overlap. Invoking a metallicity-dependent model for high-mass X-ray binaries yields an anticorrelation between mass-weighted stellar metallicity and SFR-normalized luminosity. The spatial distribution of high-mass X-ray binaries coincides with star-formation regions of simulated galaxies, while low-mass X-ray binaries follow the stellar mass surface density. X-ray binary emission is the dominant contribution in the hard X-ray band (2-10 keV) in the absence of an actively accreting central super-massive black hole, and it provides a ∼ 50% contribution in the soft X-ray band (0.5-2 keV), rivaling the hot gas component. Conclusions. We conclude that our modeling remains consistent with observations despite the uncertainties connected to our approach. The predictive power and easily extendable framework hold great value for future investigations of galactic X-ray spectra.

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Section: Gas Luminosity Scaling Relationmentioning

confidence: 99%

Section: Gas Luminosity Scaling Relationmentioning

confidence: 99%

Decomposition of galactic X-ray emission with PHOX

Vladutescu-Zopp

Biffi

Dolag

2023

A&A

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“…Emission from hot gas can be detected in X-rays. Comparat et al (2022) and Chadayammuri et al (2022) use eROSITA data to measure X-ray emission around stellarmass-controlled samples of star-forming and passive galaxies and find conflicting results. Comparat et al (2022) find that passive galaxies are associated with more X-ray emission while Chadayammuri et al (2022) find the opposite.…”

Section: Cool and Hot Gas In The Cgm Of Quenched Galaxiesmentioning

confidence: 99%

“…Comparat et al (2022) and Chadayammuri et al (2022) use eROSITA data to measure X-ray emission around stellarmass-controlled samples of star-forming and passive galaxies and find conflicting results. Comparat et al (2022) find that passive galaxies are associated with more X-ray emission while Chadayammuri et al (2022) find the opposite. Chadayammuri et al (2022) argue that the discrepancy is driven by differences in how emission from groups and clusters is treated for galaxies other than the group and cluster centrals.…”

Section: Cool and Hot Gas In The Cgm Of Quenched Galaxiesmentioning

confidence: 99%

“…At the very least, it is necessary to control for impact parameter and galaxy mass and to restrict comparisons to reasonably narrow redshift ranges. Comparisons between star-forming and passive galaxies have been done with the necessary controls for cool (T ∼ 10 4 K) metal-enriched gas traced by Mg II (Bordoloi et al 2011;Lan 2020;Anand et al 2021) and for hot (T  10 6 K) gas traced by X-ray emission (Chadayammuri et al 2022;Comparat et al 2022). Star-forming galaxies have higher equivalent widths of cool gas tracers than passive galaxies, but results are still unclear for X-ray emission.…”

Section: Introductionmentioning

confidence: 99%

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The CGM² Survey: Quenching and the Transformation of the Circumgalactic Medium

Tchernyshyov

Werk

Wilde

et al. 2023

ApJ

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This study addresses how the incidence rate of strong O vi absorbers in a galaxy’s circumgalactic medium (CGM) depends on galaxy mass and, independently, on the amount of star formation in the galaxy. We use Hubble Space Telescope/Cosmic Origins Spectrograph absorption spectroscopy of quasars to measure O vi absorption within 400 projected kpc and 300 km s−1 of 52 galaxies with M * ∼ 3 × 1010 M ⊙. The galaxies have redshifts 0.12 < z < 0.6, stellar masses 1010.1 M ⊙ < M * < 1010.9 M ⊙, and spectroscopic classifications as star-forming or passive. We compare the incidence rates of high column density O vi absorption (N O VI ≥ 1014.3 cm−2) near star-forming and passive galaxies in two narrow ranges of stellar mass and, separately, in a matched range of halo mass. In all three mass ranges, the O vi covering fraction within 150 kpc is higher around star-forming galaxies than around passive galaxies with greater than 3σ-equivalent statistical significance. On average, the CGM of star-forming galaxies with M * ∼ 3 × 1010 M ⊙ contains more O vi than the CGM of passive galaxies with the same mass. This difference is evidence for a CGM transformation that happens together with galaxy quenching and is not driven primarily by halo mass.

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Detecting clusters of galaxies and active galactic nuclei in an eROSITA all-sky survey digital twin

Seppi

Comparat

Bülbül

et al. 2022

A&A

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Context. The extended ROentgen Survey with an Imaging Telescope Array (eROSITA) onboard the Spectrum-Roentgen-Gamma (SRG) observatory is revolutionizing X-ray astronomy. The mission provides unprecedented samples of active galactic nuclei (AGN) and clusters of galaxies, with the potential of studying astrophysical properties of X-ray sources and measuring cosmological parameters using X-ray-selected samples with higher precision than ever before. Aims. We aim to study the detection, and the selection of AGN and clusters of galaxies in the first eROSITA all-sky survey, and to characterize the properties of the source catalog. Methods. We produced a half-sky simulation at the depth of the first eROSITA survey (eRASS1), by combining models that truthfully represent the population of clusters and AGN. In total, we simulated 1 116 758 clusters and 225 583 320 AGN. We ran the standard eROSITA detection algorithm, optimized for extragalactic sources. We matched the input and the source catalogs with a photon-based matching algorithm. Results. We perfectly recovered the bright AGN and clusters. We detected half of the simulated AGN with flux larger than 2×10 −14 erg/s/cm 2 as point sources and half of the simulated clusters with flux larger than 3×10 −13 erg/s/cm 2 as extended sources in the 0.5 -2.0 keV band. We quantified the detection performance in terms of completeness, false detection rate, and contamination. We studied the population in the source catalog according to multiple cuts of source detection and extension likelihood. We find that the latter is suitable for removing contamination, and the former is very efficient in minimizing the false detection rate. We find that the detection of clusters of galaxies is mainly driven by flux and exposure time. It additionally depends on secondary effects, such as the size of the clusters on the sky plane and their dynamical state. The cool core bias mostly affects faint clusters classified as point sources, while its impact on the extent-selected sample is small. We measured the fraction of the area covered by our simulation as a function of limiting flux. We measured the X-ray luminosity of the detected clusters and find that it is compatible with the simulated values. Conclusions. We discuss how to best build samples of galaxy clusters for cosmological purposes, accounting for the nonuniform depth of eROSITA. This simulation provides a digital twin of the real eRASS1.

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The eROSITA Final Equatorial Depth Survey (eFEDS)

Cited by 35 publications

References 91 publications

Decomposition of galactic X-ray emission with PHOX

Decomposition of galactic X-ray emission with PHOX

The CGM² Survey: Quenching and the Transformation of the Circumgalactic Medium

Detecting clusters of galaxies and active galactic nuclei in an eROSITA all-sky survey digital twin

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The eROSITA Final Equatorial Depth Survey (eFEDS)

Cited by 35 publications

References 91 publications

Decomposition of galactic X-ray emission with PHOX

Decomposition of galactic X-ray emission with PHOX

The CGM2 Survey: Quenching and the Transformation of the Circumgalactic Medium

Detecting clusters of galaxies and active galactic nuclei in an eROSITA all-sky survey digital twin

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Product

Resources

About

The CGM² Survey: Quenching and the Transformation of the Circumgalactic Medium