The eROSITA Final Equatorial-Depth Survey (eFEDS)

Brusa, M.; Urrutia, T.; Toba, Yoshiki; Buchner, Johannes; Li, J.-Y.; Liu, T.; Perna, M.; Salvato, M.; Merloni, A.; Musiimenta, B.; Nandra, K.; Wolf, Julien; Arcodia, R.; Dwelly, T.; Georgakakis, A.; Goulding, A. D.; Matsuoka, Yoshiki; Nagao, Tohru; Schramm, Malte; Silverman, John D.; Terashima, Yuichi

doi:10.1051/0004-6361/202141092

Cited by 9 publications

(7 citation statements)

References 111 publications

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“…The X-ray spectral analysis provides N H , which is an indicator of obscuring gas properties around AGN. eROSITA already discovered statistically large number of obscured (N H > 10 22 cm −2 ) AGN at z > 0.5 in the eFEDS field (Brusa et al 2022;Toba et al 2022). As already discussed in Liu et al (2022), we note that the uncertainty of N H is not small, reaching ∆ log(N H /cm −2 ) = 0.67 for the sample (see top right panel of Fig.…”

Section: Obscuration Propertiessupporting

confidence: 74%

“…As shown in the figure, there is one spec-z source in the region of the extremely red quasar color. The source is ERO_ID = 608, which Brusa et al (2022) already identified as an X-ray luminous obscured AGN with strong [OIII]λ5007 outflow feature, undergoing strong AGN feedback. This is consistent with one of the notable features of extremely red quasars (Zakamska et al 2016).…”

Section: Obscuration Propertiesmentioning

confidence: 99%

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eROSITA Final Equatorial-Depth Survey (eFEDS)

Ichikawa

Yamashita

Merloni

et al. 2023

A&A

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We constructed the eROSITA X-ray catalog of radio galaxies discovered by the WERGS survey, made by cross-matching the wide area Subaru/Hyper Suprime-Cam (HSC) optical survey and VLA/FIRST 1.4 GHz radio survey. We report finding 393 eROSITA detected radio galaxies in the 0.5−2 keV band in the eFEDS field covering 140 deg2. Thanks to the wide and medium depth eFEDS X-ray survey down to f0.5 − 2 keV = 6.5 × 10−15 erg s−1 cm−2, the sample contains the rare and most X-ray luminous radio galaxies above the knee of the X-ray luminosity function, spanning 44 < log(L0.5−2 keV(abs,corr)/erg s−1) < 46.5 at 1 < z < 4. The sample also contains the sources around and below the knee for the sources 41 < log(L0.5−2 keV(abs,corr)/erg s−1) < 45 at z < 1. Based on the X-ray properties obtained by the spectral fitting, 37 sources show obscured active galactic nucleus (AGN) signatures with log(NH/cm−2) > 22. These obscured and radio AGN reside in 0.4 < z < 3.2, indicating that they are obscured counterparts of the radio-loud quasar, which were missed in the previous optical quasar surveys. By combining radio and X-ray luminosities, we also investigated the jet production efficiency ηjet = ηradPjet/LAGN,bol by utilizing the jet power of Pjet. We find that there are 14 sources with extremely high jet production efficiency at ηjet ≈ 1. This high ηjet value might be a result of the decreased radiation efficiency of ηrad < 0.1, due to the low accretion rate for those sources, and/or of the boosting due to the decline of LAGN,bol by a factor of 10−100 by keeping Pjet constant in the previous Myr, indicating the experience of the AGN feedback. Finally, inferring the BH masses from the stellar mass, we find that X-ray luminous sources show the excess of the radio emission with respect to the value estimated from the fundamental plane. This radio emission excess cannot be explained by the Doppler boosting alone, and therefore the disk–jet connection of X-ray luminous eFEDS-WERGS is fundamentally different from the conventional fundamental plane which mainly covers the low-accretion regime.

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Section: Obscuration Propertiessupporting

confidence: 74%

Section: Obscuration Propertiesmentioning

confidence: 99%

eROSITA Final Equatorial-Depth Survey (eFEDS)

Ichikawa

Yamashita

Merloni

et al. 2023

A&A

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“…This criterion includes sources with either spectroscopic redshift (CTP_REDSHIFT_GRADE = 5) or the photoz estimates of the two methods agree (CTP_REDSHIFT_GRADE = 4) or agree within a tolerance level (CTP_REDSHIFT_GRADE = 3; for more details see Sect. 6.3 of Salvato et al 2022). Liu et al (2022) performed a systematic X-ray spectral fitting analysis on all the X-ray systems.…”

Section: X-ray Sources In the Efeds Fieldmentioning

confidence: 99%

“…The eFEDS X-ray catalogue includes 27910 X-ray sources detected in the 0.2−2.3 keV energy band with detection likelihoods ≥ 6, that corresponds to a flux limit of ≈ 7 × 10 −15 erg cm −2 s −1 in the 0.5 − 2.0 keV energy range (Brunner et al 2022). Salvato et al (2022) presented the multiwavelength counterparts and redshifts of the X-ray sources, by identifying their optical counterparts. Two independent methods were utilized to find the counterparts of the X-ray sources, NWAY (Salvato et al 2018) and ASTROMATCH (Ruiz et al 2018).…”

Section: X-ray Sources In the Efeds Fieldmentioning

confidence: 99%

The co-evolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshift

Mountrichas

2023

A&A

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It is well known that supermassive black holes (SMBHs) and their host galaxies co-evolve. A manifestation of this co-evolution is the correlation that has been found between the SMBH mass, M BH , and the galaxy bulge or stellar mass, M * . The cosmic evolution of this relation, though, is still a matter of debate. In this work, we examine the M BH −M * relation, using 687 X-ray luminous (median log [L X,2−10keV (ergs −1 )] = 44.3), broad-line active galactic nuclei (AGN), at 0.2 < z < 4.0 (median z ≈ 1.4) that lie in the XMM-XXL field. Their M BH and M * range from 7.5 < log [M BH (M )] < 9.5 and 10 < log [M * (M )] < 12, respectively. Most of the AGN live in star-forming galaxies and their Eddington ratios range from 0.01 to 1, with a median value of 0.06. Our results show that M BH and M * are correlated (r = 0.47 ± 0.21, averaged over different redshift intervals). Our analysis also shows that the mean ratio of the M BH and M * does not evolve with redshift, at least up to z = 2 and has a value of log(M BH /M * ) = −2.44. The majority of the AGN (75%) are in a SMBH mass growth-dominant phase. In these systems, the M BH −M * correlation is weaker and their M * tends to be lower (for the same M BH ) compared to systems that are in a galaxy mass growth phase. Our findings suggest that the growth of black hole mass occurs first, while the early stellar mass assembly may not be so efficient.

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“…) and stars (Schneider et al 2022); the X-ray variability properties of the detected sources (Boller et al 2022;Buchner et al 2022); the X-ray spectral analysis of the point sources (Liu et al 2022b); the X-ray morphological analysis of the clusters (Ghirardini et al 2022); the optical and lensing analysis of the X-ray clusters (Ramos-Ceja et al 2022;Chiu et al 2022;Bahar et al 2022, Ota et al, in prep. ); the properties of non-active galaxies detected by eROSITA (Vulic et al 2022), and the discovery of some extreme AGN (Toba et al 2022;Brusa et al 2022). Earlier works based on the eFEDS data have been published and include the discovery of a supercluster (Ghirardini et al 2021) and a very high-redshift quasar (Wolf et al 2021).…”

Section: Introductionmentioning

confidence: 99%

The eROSITA Final Equatorial Depth Survey (eFEDS)

Brunner

Liu

Lamer

et al. 2022

A&A

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207

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Context. The eROSITA X-ray telescope on board the Spectrum-Poentgen-Gamma (SPG) observatory combines a large field of view and a large collecting area in the energy range between ~0.2 and ~8.0 keV. This gives the telescope the capability to perform uniform scanning observations of large sky areas. Aims. SRG/eROSITA performed scanning observations of the ~140 square degree eROSITA Final Equatorial Depth Survey field (the eFEDS field) as part of its performance verification phase ahead of the planned four year of all-sky scanning operations. The observing time of eFEDS was chosen to slightly exceed the depth expected in an equatorial field after the completion of the all-sky survey. While verifying the capability of eROSITA to perform large-area uniform surveys and saving as a test and training dataset to establish calibration and data analysis procedures, the eFEDS survey also constitutes the largest contiguous soft X-ray survey at this depth to date, supporting a range of early eROSITA survey science investigations. Here we (i) present a catalogue of detected X-ray sources in the eFEDS field providing information about source positions and extent, as well as fluxes in multiple energy bands, and (ii) document the suite of tools and procedures developed for eROSITA data processing and analysis, which were validated and optimised by the eFEDS work. Methods. The data were fed through a standard data processing pipeline, which appltes X-ray event calibration and provides a set of standard calibrated data products. A mutiti-stage source detection procedure, building in part on experience from XMM-Newton, was optimised and calibrated by performing realistic simulations of the eROSITA eFEDS observations. Source fluxes were computed in multiple standard energy bands by forced point source fitting and aperture photometry. We cross-matched the eROSITA eFEDS source catalogue with previous XMM-ATLAS observations, which confirmed the excellentt agreement of the eROSITA and XMM-ATLAS source fluxes. Astrometric corrections were performed by cross-matching the eROSITA source positions with an optical reference catalogue of quasars. Results. We present a primary catalogue of 27 910 X-ray sources (542 of which are significantly spatially extended) detected in the 0.2–2.3 keV energy range with detection likelihoods ≥6, corresponding to a (point source) flux limit of 6.5 × 10–15 erg cm–2 s–1 in the 0.5–2.0 keV energy band (80% completeness). A supplementary catalogue contains 4774 low-significance source candidates with detection likelihoods between 5 and 6. In addition, a hard-band sample of 246 sources detected in the energy range 22.3–5.0 keV above a detection likelihood of 10 is provided. In an appendix, we finally describe the dedicated data analysis software package, the eROSITA calibration database, and the standard calibrated data products.

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The eROSITA Final Equatorial-Depth Survey (eFEDS)

Cited by 9 publications

References 111 publications

eROSITA Final Equatorial-Depth Survey (eFEDS)

eROSITA Final Equatorial-Depth Survey (eFEDS)

The co-evolution of supermassive black holes and galaxies in luminous AGN over a wide range of redshift

The eROSITA Final Equatorial Depth Survey (eFEDS)

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