10^{23}$), higher ionisations ($10^{3}-10^{6}$ erg s-1) and large outflow
velocities (v$\sim 0.033$c - $0.3$c). Such outflows are often detected based
on absorption features in the $7-10{\rm\thinspace keV}$ range, at the edge of
or outside of the eROSITA bandpass. UFOs are often found in high Eddington
ratio sources, but the typical ionisations and large outflow velocities are
mostly inconsistent with the ionisation range of ($10^{-4}-10^{4}$ erg s-1)
and the zero outflow velocity used in this work. More in-depth modelling with
a broader parameter space and likely including data from XMM or NuSTAR would
be required to attempt to identify signatures of UFOs in this sample.

Figure 30: Cartoon schematic showing how the emission may vary with Eddington
ratio. Left: Sources with relatively lower Eddington ratios (few $\times
10^{-3}$), there is sufficient radiation pressure to launch line driven winds,
but not so much that the winds become over-ionised, so more warm absorbers are
detected. Middle: Sources with intermediate Eddington ratios, (few $\times
10^{-2}$) some winds will become over-ionised and their velocities will not
exceed the escape velocity and will fail, but will remain somewhat bound to
the system, creating patchy partial covering absorbers. Right: Sources
accreting at $0.1-1$ Eddington, high radiation pressure results in too many
ionising photons and the wind is destroyed, remaining tightly bound to the
system and forming the warm corona.

One caveat to this analysis is that this work does not attempt to characterise
properties of potential warm absorbers and disc winds simultaneously. To
address this, all sources which showed evidence for a soft excess or warm
absorber were also fit with a model including both a disc wind (warmabs) and a
secondary power law component (in XSPEC, this corresponds to tbabs $\times$
ztbabs $\times$ cwa18 $\times$ (powerlaw \+ powerlaw)). The same priors as in
Sect. 3 were used, and Bayes factors were again calculated for each source.
For most sources, the inclusion of both components did not result in a better
fit to the spectrum, and many spectral parameters could not be well
constrained. Therefore, it appears that for the eFEDS analysis, the components
can only be treated separately, which may lead to some modelling errors. Laha
et al. (2013) discuss the complications of simultaneously modelling a soft
excess and warm absorption component in NLS1 IRAS 13349+2438, and demonstrate
that different ionising continua produce different ionisation structures in
the warm absorption component, whereas including a soft excess tends to
decrease the ionisation while the column density remains consistent. More
recently, Parker et al. (2022) discuss the degeneracies between X-ray winds
and relativistic blurred reflection, where systematic biases are found in the
derived outflow parameters of the wind when the emission from the disc is not
properly characterised. These are particularly crucial in the case of broad
features, where even microcalorimeter resolution does not help to break some
degeneracies (Parker et al., 2022). Care should therefore be taken in
interpreting the ionisation parameters in this work, and further analysis
should be done to better understand any potential superposition between these
components.

##  7 Conclusions

In this work, the 200 sources classified as AGN from the eFEDS hard
X-ray–selected sample are modelled with a variety of phenomenological and
physically motivated models in order to investigate the nature of the X-ray
soft excess. X-ray spectra are fit using BXA so that the Bayesian evidence can
be compared to select the best fitting models. This work demonstrates that
eROSITA can be used to identify signatures of both complex absorption and soft
excesses, and using simulations, the significance of these features can be
evaluated. This analysis identifies a total of 29 sources that have warm
absorbers ($14.5\%$ of the sample), 25 sources that have neutral partial
covering absorbers ($12.5\%$ of the sample), and 29 sources ($14.5\%$ of the
sample) with soft excesses (all with 97.5% purity), which clearly shows that
soft excesses and complex absorbers are key features for understanding the
properties of large samples of AGN.

It is shown that most sources with true soft excesses are best explained by a
warm corona model as opposed to a relativistic blurred reflection scenario.
Follow-up observations of these sources with better sensitivity in the hard
X-ray (e.g. with XMM or NuSTAR) can help to search for the presence of a broad
iron line or Compton hump which are strong signatures of blurred reflection
(e.g. Fabian et al., 1989; Ross & Fabian, 2005), and a timing analysis
incorporating reverberation mapping (e.g. following the prescription of Uttley
et al., 2014) can also help to distinguish between soft excess and absorption
models.

Several interesting results were also found in studying the properties of the
warm absorbers and soft excesses, including that warm absorbers are likely the
true nature of the absorption in many apparently Compton-thin AGN, and that
sources with soft excesses are found in higher Eddington ratio sources while
sources with warm absorbers are found in lower Eddington ratios. This
Eddington ratio division may be explained in the context of winds which escape
the system and intercept the line of sight at low $\lambda_{\rm Edd}$, but
which become over-ionised failed winds resulting in the formation of a partial
covering absorber at intermediate $\lambda_{\rm Edd}$ or the warm corona at
high $\lambda_{\rm Edd}$. However, it is difficult to confirm these findings
or to completely explain their physical interpretation using eFEDS alone.
Using the results from this work and repeating this analysis using the all-sky
survey (e.g. eRASS:1, eRASS:4) will provide a large sample of $\sim 1000$s of
AGN for enhanced analysis. Furthermore, using data with very high spectral
resolution (e.g. XRISM and Athena) will help to confirm these results, and to
create a more complete picture of the nature of warm absorbers and soft
excesses in AGN in the local Universe.

###### Acknowledgements.

We thank the referee for their careful reading of this manuscript and for
their very helpful comments and suggestions which improved this work.
This work is based on data from eROSITA, the soft X-ray instrument onboard
SRG, a joint Russian-German science mission supported by the Russian Space
Agency (Roskosmos), in the interests of the Russian Academy of Sciences
represented by its Space Research Institute (IKI), and the Deutsches Zentrum
für Luft- und Raumfahrt (DLR). The SRG spacecraft was built by Lavochkin
Association (NPOL) and its subcontractors, and is operated by NPOL with
support from the Max-Planck Institute for Extraterrestrial Physics (MPE). The
development and construction of the eROSITA X-ray instrument was led by MPE,
with contributions from the Dr. Karl Remeis Observatory Bamberg & ECAP (FAU
Erlangen-Nuernberg), the University of Hamburg Observatory, the Leibniz
Institute for Astrophysics Potsdam (AIP), and the Institute for Astronomy and
Astrophysics of the University of Tübingen, with the support of DLR and the
Max Planck Society. The Argelander Institute for Astronomy of the University
of Bonn and the Ludwig Maximilians Universität Munich also participated in the
science preparation for eROSITA. The eROSITA data shown here were processed
using the eSASS/NRTA software system developed by the German eROSITA
consortium.
The Hyper Suprime-Cam (HSC) collaboration includes the astronomical
communities of Japan and Taiwan, and Princeton University. The HSC
instrumentation and software were developed by the National Astronomical
Observatory of Japan (NAOJ), the Kavli Institute for the Physics and
Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High
Energy Accelerator Research Organization (KEK), the Academia Sinica Institute
for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University.
Funding was contributed by the FIRST program from Japanese Cabinet Office, the
Ministry of Education, Culture, Sports, Science and Technology (MEXT), the
Japan Society for the Promotion of Science (JSPS), Japan Science and
Technology Agency (JST),the Toray Science Foundation, NAOJ, Kavli IPMU,
KEK,ASIAA, and Princeton University.
Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P.
Sloan Foundation, the U.S. Department of Energy Office of Science, and the
Participating Institutions. SDSS acknowledges support and resources from the
Center for High-Performance Computing at the University of Utah. The SDSS web
site is www.sdss.org. SDSS is managed by the Astrophysical Research Consortium
for the Participating Institutions of the SDSS Collaboration including the
Brazilian Participation Group, the Carnegie Institution for Science, Carnegie
Mellon University, Center for Astrophysics — Harvard & Smithsonian (CfA), the
Chilean Participation Group, the French Participation Group, Instituto de
Astrofísica de Canarias, The Johns Hopkins University, Kavli Institute for the
Physics and Mathematics of the Universe (IPMU) / University of Tokyo, the
Korean Participation Group, Lawrence Berkeley National Laboratory, Leibniz
Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie
(MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-
Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical
Observatories of China, New Mexico State University, New York University,
University of Notre Dame, Observatório Nacional / MCTI, The Ohio State
University, Pennsylvania State University, Shanghai Astronomical Observatory,
United Kingdom Participation Group, Universidad Nacional Autónoma de México,
University of Arizona, University of Colorado Boulder, University of Oxford,
University of Portsmouth, University of Utah, University of Virginia,
University of Washington, University of Wisconsin, Vanderbilt University, and
Yale University.
Funding for the Sloan Digital Sky Survey (SDSS) has been provided by the
Alfred P. Sloan Foundation, the Participating Institutions, the National
Aeronautics and Space Administration, the National Science Foundation, the US
Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society.
The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the
Astrophysical Research Consortium (ARC) for the Participating Institutions.
The Participating Institutions are The University of Chicago, Fermilab, the
Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins
University, Los Alamos National Laboratory, the Max-Planck-Institute for
Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico
State University, University of Pittsburgh, Princeton University, the United
States Naval Observatory, and the University of Washington.
MB acknowledges support from the European Innovative Training Network (ITN)
“BiD4BEST” funded by the Marie Sklodowska-Curie Actions in Horizon 2020 (GA
860744).

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##  Appendix A Simulations to assess Bayes factor thresholds

In order to determine which values of the Bayes factors for each model
correspond to a significant improvement to the fit, simulations are performed.
Here, 1000 spectra are generated using the fakeit command in XSPEC. Spectral
simulations are based on an absorbed power law model (tbabs $\times$ ztbabs
$\times$ powerlaw) using the average spectral properties from the absorbed
power law (PL) model, with a photon index of $\Gamma\sim 2$ and a host galaxy
column density of $\sim 2\times 10^{20}\hbox{${\rm\thinspace cm}^{-2}\,$}$. In
this way, the simulated spectra are representative of the average eFEDS
spectrum and can be used to calibrate the Bayes factor threshholds for the
entire sample.

First, to determine the significance of the absorber models, each simulated
spectrum is then fit with the baseline (PL), warm absorber (PL+WA), and
partial covering (PL+PCF) models, and the Bayes factor is computed for each
model using equation 1. Formulae for the Bayes factor for all models are given
in Table 3. The resulting histograms are shown in Fig. 31, with results for
warm absorption modelling shown in the left-hand panel and results for neutral
partial covering shown on the right. Purity thresholds (the confidence per
object that the absorption component is real) levels of 95%, 97.5% and 99% are
indicated using vertical lines with dashed, solid and dotted linestyles,
respectively. These Bayes factor purity thresholds are selected such that
cases where if the model both has the lowest Bayesian evidence of all models,
and the Bayes factor exceeds the threshold, it is considered a false
detection.

Figure 31: Distributions of Bayes factors obtained from simulations. Left:
Computed warm absorber Bayes factors (Kwa). Right: computed partial covering
Bayes factors (Kpcf). Confidence levels of 95%, 97.5% and 99% are indicated
using vertical lines of different linestyles.  Table 8: Summary of detection
thresholds for complex absorbers. Column (1) gives the percentile of sources,
and column (2) gives the corresponding Bayes factor purity threshhold. Column
(3) gives the resulting assumed number of false detections, obtained from
multiplying the purity by the total number of sources (199). Column (4) gives
the number of sources in the sample with Kwa values greater than the value
given in column (2) and where the model provides the best fit to the data.
Column (5) gives the assumed number of true detections in the eFEDS hard
X-ray–selected sample of 200 sources.

(1) | (2) | (3) | (4) | (5)
---|---|---|---|---
Percentile | K | Expected | Expected | True detections
|  | false detections | Sources |
Warm absorption
95% | 0.815 | 10 | 36 | 26
97.5% | 1.126 | 5 | 29 | 24
99% | 2.040 | 2 | 15 | 13
Partial covering
95% | 1.360 | 10 | 28 | 18
97.5% | 1.555 | 5 | 25 | 20
99% | 2.646 | 2 | 12 | 10

By applying these purity thresholds to the eFEDS hard X-ray sample, the number
of expected false detections of an absorption component at each confidence
level can be predicted. These results are summarised in Table 8. The
percentile gives the percentage of simulated sources with Bayes factors below
the quoted value, and the false detection rate gives the corresponding number
of false detections. The number of sources is the number of real sources with
Bayes factors above the stated value and where the given model provides the
best fit, and the number of true detections is calculated by subtracting the
expected number of false detections in a sample of 200 sources. Since evidence
comparison is used to determine which of the complex models provides the best
fit to the data, scenarios where a source appears in multiple sub-samples are
excluded. The 97.5% purity thresholds are taken as the samples of sources with
warm absorbers or partial covering components respectively.

The Bayes factors obtained from fitting the eFEDS spectra with the two complex
absorption models are compared in Fig. 32, with error bars are shown for each
source. One source, ID 00011, is excluded as the Kwa and Kpcf values are many
orders of magnitude larger than the rest of the sample (see tables in the
appendix). There is clear evidence both for sources which are very well fit
with neutral partial covering and with ionised warm absorption, confirming
that both models should be included in the analysis in order to properly
characterise the shape of the observed X-ray spectra.

Figure 32: Comparison of Bayes factors between warm absorber models. The Bayes
factor for the warm absorption model is shown on the horizontal axis, while
the Bayes factor for the neutral partial covering model is shown on the
vertical axis. The dashed grey line shows the one-to-one relation, with
sources lying below the line being better fit with the PL+WA model, and
sources above the line being better fit with the PL+PCF model. Sources which
do not show evidence for any complex absorption are shown in grey.The values
of Kwa = 1.126 and Kpcf = 1.555 correspond to purities of 97.5%.

From the computed PL+PL Bayes factors, to determine which sources have
significant soft excesses, the same method employed to determine the
significance of warm absorbers and partial covering components is used. The
same 1000 simulated spectra are used, but are now fit with the PL+PL model,
and Bayes factors are again computed. The resulting histogram of Kpl values is
shown in Fig. 33. Confidence levels of 95%, 97.5% and 99% are indicated using
vertical lines with solid, dashed, dotted and dash-dot linestyles,
respectively. In general, a higher threshold is required to distinguish a soft
excess than to distinguish complex absorption. The false detection rates are
again calculated and are summarised in Table 9.

Figure 33: Distribution of computed Kpl values obtained from simulations.
Confidence levels of 95%, 97.5% and 99% are indicated using vertical lines of
different linestyles.  Table 9: Summary of detection thresholds for soft
excesses. Column (1) gives the percentile of sources, and column (2) gives the
corresponding Kpl values. Column (3) gives expected number of false
detections. Column (4) gives the number of sources in the sample with Kpl
values greater than the value given in column (2) and where the model provides
the best fit to the data. Column (5) gives the assumed number of true
detections in the eFEDS hard X-ray–selected sample of 200 sources.

(1) | (2) | (3) | (4) | (5)
---|---|---|---|---
Percentile | K | Expected | Expected | True detections
|  | false detections | Sources |
95% | 1.392 | 10 | 40 | 30
97.5% | 2.586 | 5 | 29 | 24
99% | 8.613 | 2 | 20 | 18

##  Appendix B Spectral fit parameters

The tables below give the spectral fit parameters for the models presented in
this work. table. 10 gives parameters for the baseline (PL) fit for all
sources. table. 11 gives parameters for the warm absorber (PL+WA) model for
sources with $>95\%$ significance. table. 12 gives parameters for the partial
covering absorber (PL+PCF) model for sources with $>95\%$ significance. table.
13 gives parameters for the soft excess (PL+PL) model for sources with $>95\%$
significance. Spectral fit parameters for soft excess sources best fit with a
warm corona are given in table. 14, and parameters for sources best fit with
blurred reflection are given in Table 15.

Table 10: Summary of warm absorber parameters for sources with significant warm absorbers ($>95\%$). Column (1) gives the eROSITA name, column (2) gives the source ID (ID_SRC in the catalog, used throughout this work for source identification), column (3) gives the warm absorber column density, column (4) gives the warm absorber ionisation, column (5) gives the photon index, column (6) gives the logarithm of the $2-10{\rm\thinspace keV}$ flux measured from the absorbed power law model in cgs units, and column (7) gives the best-fit model (where PL is the absorbed power law model, SE is the soft excess model, PCF is the partial covering absorber model, and WA is the warm absorber model).  (1) | (2) | (3) | (4) | (5) | (6) | (7)
---|---|---|---|---|---|---
Name | ID | nHgal | log(NHz) | $\Gamma$ | log(F) | Model
|  | ($\times 10^{20}\hbox{${\rm\thinspace cm}^{-2}\,$}$) |  |  | ergs s-1 cm-2 |
eFEDS J093701.0+010545 | 00001 | 4.95 | 20.03 ${}_{-0.02}^{+0.05}$ | 2.69 ${}_{-0.03}^{+0.03}$ | -11.67 | SE
eFEDS J085617.9-013806 | 00003 | 2.08 | 20.02 ${}_{-0.02}^{+0.03}$ | 2.92 ${}_{-0.03}^{+0.03}$ | -12.14 | SE
eFEDS J084025.5+033303 | 00004 | 3.18 | 20.02 ${}_{-0.02}^{+0.03}$ | 2.33 ${}_{-0.03}^{+0.03}$ | -11.77 | SE
eFEDS J091702.3-004416 | 00007 | 3.53 | 20.06 ${}_{-0.04}^{+0.08}$ | 2.35 ${}_{-0.04}^{+0.04}$ | -12.10 | SE
eFEDS J091401.8+050750 | 00008 | 4.06 | 20.14 ${}_{-0.10}^{+0.15}$ | 2.10 ${}_{-0.04}^{+0.05}$ | -11.78 | PL
eFEDS J084303.0+030218 | 00011 | 3.71 | 20.04 ${}_{-0.03}^{+0.05}$ | 2.99 ${}_{-0.01}^{+0.01}$ | -12.64 | SE
eFEDS J091420.1+013748 | 00014 | 2.66 | 20.08 ${}_{-0.06}^{+0.11}$ | 2.27 ${}_{-0.06}^{+0.05}$ | -12.15 | PCF
eFEDS J083356.4-010113 | 00016 | 3.91 | 20.07 ${}_{-0.05}^{+0.10}$ | 1.87 ${}_{-0.06}^{+0.05}$ | -11.90 | WA
eFEDS J092414.7+030860 | 00023 | 3.81 | 20.11 ${}_{-0.08}^{+0.13}$ | 2.06 ${}_{-0.06}^{+0.06}$ | -12.13 | PCF
eFEDS J090910.2+012136 | 00025 | 3.30 | 20.37 ${}_{-0.25}^{+0.32}$ | 1.77 ${}_{-0.07}^{+0.07}$ | -11.98 | PL
eFEDS J093117.8+033121 | 00028 | 3.20 | 20.05 ${}_{-0.04}^{+0.08}$ | 1.92 ${}_{-0.06}^{+0.07}$ | -12.11 | WA
eFEDS J083702.1+024536 | 00029 | 3.83 | 20.06 ${}_{-0.05}^{+0.09}$ | 2.56 ${}_{-0.07}^{+0.07}$ | -12.56 | SE
eFEDS J091333.6-004250 | 00030 | 3.11 | 20.12 ${}_{-0.08}^{+0.16}$ | 2.22 ${}_{-0.07}^{+0.07}$ | -12.34 | PCF
eFEDS J093518.2+020415 | 00032 | 4.10 | 20.26 ${}_{-0.19}^{+0.28}$ | 2.01 ${}_{-0.07}^{+0.08}$ | -12.19 | PL
eFEDS J090446.0+020843 | 00033 | 4.12 | 20.90 ${}_{-0.40}^{+0.23}$ | 2.01 ${}_{-0.11}^{+0.14}$ | -12.25 | PL
eFEDS J090352.1-005353 | 00034 | 2.82 | 20.06 ${}_{-0.04}^{+0.08}$ | 2.31 ${}_{-0.07}^{+0.07}$ | -12.42 | SE
eFEDS J084110.8+022951 | 00035 | 4.60 | 20.13 ${}_{-0.09}^{+0.16}$ | 2.48 ${}_{-0.08}^{+0.08}$ | -12.52 | SE
eFEDS J085624.3-003644 | 00037 | 3.22 | 20.11 ${}_{-0.08}^{+0.14}$ | 2.08 ${}_{-0.07}^{+0.07}$ | -12.26 | WA
eFEDS J083834.1-002440 | 00038 | 4.05 | 20.12 ${}_{-0.09}^{+0.15}$ | 2.16 ${}_{-0.08}^{+0.08}$ | -12.34 | SE
eFEDS J093714.1+031536 | 00039 | 3.01 | 20.07 ${}_{-0.05}^{+0.10}$ | 2.97 ${}_{-0.04}^{+0.02}$ | -12.94 | SE
eFEDS J093303.4+045236 | 00041 | 3.41 | 20.28 ${}_{-0.19}^{+0.24}$ | 2.24 ${}_{-0.08}^{+0.09}$ | -12.44 | PL
eFEDS J085900.1-020028 | 00042 | 2.01 | 20.15 ${}_{-0.11}^{+0.17}$ | 2.14 ${}_{-0.08}^{+0.08}$ | -12.56 | PL
eFEDS J085240.1+051216 | 00043 | 4.35 | 20.15 ${}_{-0.10}^{+0.18}$ | 2.60 ${}_{-0.09}^{+0.09}$ | -12.58 | PCF
eFEDS J091250.7+035221 | 00044 | 3.56 | 20.16 ${}_{-0.12}^{+0.20}$ | 2.00 ${}_{-0.08}^{+0.08}$ | -12.28 | PL
eFEDS J091846.9-005929 | 00045 | 3.73 | 20.10 ${}_{-0.08}^{+0.13}$ | 2.37 ${}_{-0.08}^{+0.08}$ | -12.63 | SE
eFEDS J090743.4+013327 | 00048 | 3.61 | 20.92 ${}_{-0.26}^{+0.19}$ | 1.93 ${}_{-0.17}^{+0.19}$ | -12.18 | PL
eFEDS J085915.7+011801 | 00050 | 4.59 | 20.24 ${}_{-0.17}^{+0.25}$ | 2.56 ${}_{-0.10}^{+0.11}$ | -12.71 | PL
eFEDS J085904.0+020503 | 00051 | 4.18 | 20.16 ${}_{-0.11}^{+0.18}$ | 2.53 ${}_{-0.09}^{+0.10}$ | -12.69 | PL
eFEDS J091459.6+023512 | 00052 | 2.42 | 20.14 ${}_{-0.10}^{+0.15}$ | 2.61 ${}_{-0.08}^{+0.09}$ | -12.80 | PL
eFEDS J084625.1+044110 | 00054 | 4.02 | 20.10 ${}_{-0.07}^{+0.12}$ | 2.51 ${}_{-0.09}^{+0.09}$ | -12.51 | SE
eFEDS J091437.9+024558 | 00055 | 2.50 | 20.47 ${}_{-0.31}^{+0.28}$ | 2.00 ${}_{-0.10}^{+0.12}$ | -12.34 | PL
eFEDS J093240.5+023333 | 00056 | 3.96 | 20.18 ${}_{-0.13}^{+0.18}$ | 1.87 ${}_{-0.10}^{+0.09}$ | -12.25 | PL
eFEDS J093434.0+030645 | 00057 | 3.06 | 20.16 ${}_{-0.12}^{+0.18}$ | 2.06 ${}_{-0.09}^{+0.09}$ | -12.38 | SE
eFEDS J083535.5-014020 | 00060 | 3.30 | 21.71 ${}_{-0.08}^{+0.07}$ | 1.90 ${}_{-0.21}^{+0.23}$ | -12.04 | SE
eFEDS J084622.7+031324 | 00064 | 3.55 | 20.15 ${}_{-0.11}^{+0.17}$ | 2.09 ${}_{-0.09}^{+0.10}$ | -12.37 | PL
eFEDS J091232.9+001654 | 00067 | 2.63 | 20.24 ${}_{-0.17}^{+0.25}$ | 2.11 ${}_{-0.09}^{+0.10}$ | -12.45 | PL
eFEDS J091247.5-012125 | 00070 | 3.19 | 20.18 ${}_{-0.13}^{+0.20}$ | 2.47 ${}_{-0.09}^{+0.10}$ | -12.74 | SE
eFEDS J092544.6+001529 | 00071 | 3.15 | 20.22 ${}_{-0.15}^{+0.22}$ | 2.13 ${}_{-0.10}^{+0.11}$ | -12.50 | PCF
eFEDS J090821.0+045059 | 00075 | 3.68 | 20.66 ${}_{-0.43}^{+0.33}$ | 1.57 ${}_{-0.11}^{+0.14}$ | -12.06 | WA
eFEDS J092851.8+041629 | 00076 | 3.37 | 20.20 ${}_{-0.14}^{+0.23}$ | 2.38 ${}_{-0.09}^{+0.10}$ | -12.63 | SE
eFEDS J090915.9+035442 | 00078 | 3.23 | 21.17 ${}_{-0.74}^{+0.72}$ | 1.19 ${}_{-0.10}^{+0.11}$ | -11.86 | WA
eFEDS J083110.5-010006 | 00080 | 4.19 | 20.29 ${}_{-0.20}^{+0.25}$ | 2.33 ${}_{-0.11}^{+0.12}$ | -12.63 | PL
(1) | (2) | (3) | (4) | (5) | (6) | (7)
---|---|---|---|---|---|---
Name | ID | nHgal | log(NHz) | $\Gamma$ | log(F) | Model
|  | ($\times 10^{20}\hbox{${\rm\thinspace cm}^{-2}\,$}$) |  |  | ergs s-1 cm-2 |
eFEDS J092918.3+041933 | 00082 | 3.39 | 20.26 ${}_{-0.18}^{+0.24}$ | 2.23 ${}_{-0.10}^{+0.11}$ | -12.54 | PL
eFEDS J083402.6-014846 | 00101 | 3.37 | 20.50 ${}_{-0.34}^{+0.34}$ | 1.91 ${}_{-0.11}^{+0.14}$ | -12.59 | PL
eFEDS J085259.2+031322 | 00105 | 3.68 | 20.21 ${}_{-0.15}^{+0.22}$ | 2.51 ${}_{-0.11}^{+0.12}$ | -12.72 | WA
eFEDS J083310.4+041036 | 00107 | 2.77 | 20.22 ${}_{-0.15}^{+0.23}$ | 1.60 ${}_{-0.11}^{+0.11}$ | -12.18 | WA
eFEDS J091609.5+000019 | 00108 | 2.86 | 20.26 ${}_{-0.18}^{+0.28}$ | 2.41 ${}_{-0.11}^{+0.11}$ | -12.80 | PCF
eFEDS J092656.7+041613 | 00109 | 3.47 | 20.36 ${}_{-0.26}^{+0.36}$ | 2.10 ${}_{-0.11}^{+0.11}$ | -12.55 | PL
eFEDS J090826.8+002136 | 00110 | 3.18 | 20.23 ${}_{-0.16}^{+0.24}$ | 2.02 ${}_{-0.10}^{+0.11}$ | -12.49 | PL
eFEDS J083949.6+010428 | 00112 | 4.96 | 20.57 ${}_{-0.40}^{+0.43}$ | 1.60 ${}_{-0.11}^{+0.11}$ | -12.20 | PL
eFEDS J093814.9+020023 | 00113 | 4.06 | 20.32 ${}_{-0.23}^{+0.24}$ | 2.62 ${}_{-0.13}^{+0.14}$ | -12.72 | PL
eFEDS J085451.7+012611 | 00114 | 4.07 | 20.37 ${}_{-0.27}^{+0.32}$ | 2.14 ${}_{-0.11}^{+0.13}$ | -12.57 | PL
eFEDS J091405.7-000009 | 00117 | 2.68 | 20.18 ${}_{-0.13}^{+0.19}$ | 2.53 ${}_{-0.11}^{+0.11}$ | -12.90 | SE
eFEDS J091437.4+012622 | 00118 | 2.69 | 20.31 ${}_{-0.21}^{+0.27}$ | 2.05 ${}_{-0.12}^{+0.13}$ | -12.56 | PL
eFEDS J085554.3+005111 | 00120 | 4.89 | 20.26 ${}_{-0.18}^{+0.27}$ | 1.30 ${}_{-0.11}^{+0.11}$ | -12.00 | PCF
eFEDS J090457.9+010423 | 00121 | 4.01 | 20.15 ${}_{-0.11}^{+0.18}$ | 2.41 ${}_{-0.11}^{+0.12}$ | -12.83 | SE
eFEDS J084138.5+014221 | 00122 | 5.60 | 20.29 ${}_{-0.20}^{+0.29}$ | 2.36 ${}_{-0.11}^{+0.12}$ | -12.73 | SE
eFEDS J091412.6-021348 | 00123 | 3.84 | 20.37 ${}_{-0.26}^{+0.32}$ | 2.20 ${}_{-0.11}^{+0.12}$ | -12.92 | PL
eFEDS J091459.0+012630 | 00125 | 2.69 | 20.47 ${}_{-0.31}^{+0.29}$ | 1.95 ${}_{-0.13}^{+0.15}$ | -12.48 | PL
eFEDS J090915.8-011632 | 00130 | 2.70 | 20.39 ${}_{-0.26}^{+0.31}$ | 1.95 ${}_{-0.12}^{+0.13}$ | -12.50 | PL
eFEDS J085907.6+044436 | 00132 | 4.02 | 20.33 ${}_{-0.23}^{+0.28}$ | 2.37 ${}_{-0.14}^{+0.14}$ | -12.83 | WA
eFEDS J093506.3+034514 | 00133 | 3.06 | 20.53 ${}_{-0.35}^{+0.36}$ | 1.91 ${}_{-0.13}^{+0.17}$ | -12.50 | PL
eFEDS J091459.2+050243 | 00135 | 4.04 | 20.50 ${}_{-0.32}^{+0.30}$ | 1.68 ${}_{-0.12}^{+0.16}$ | -12.23 | PL
eFEDS J092008.1+032245 | 00141 | 3.63 | 20.25 ${}_{-0.18}^{+0.26}$ | 2.19 ${}_{-0.12}^{+0.13}$ | -12.68 | PL
eFEDS J083029.0+024304 | 00142 | 4.25 | 20.34 ${}_{-0.23}^{+0.31}$ | 2.55 ${}_{-0.15}^{+0.16}$ | -12.70 | PL
eFEDS J083911.2-020229 | 00143 | 2.94 | 20.37 ${}_{-0.24}^{+0.28}$ | 2.03 ${}_{-0.11}^{+0.13}$ | -12.54 | PL
eFEDS J084257.6+030841 | 00145 | 3.54 | 20.14 ${}_{-0.10}^{+0.16}$ | 2.03 ${}_{-0.11}^{+0.11}$ | -12.56 | SE
eFEDS J085301.3-015050 | 00148 | 2.03 | 20.39 ${}_{-0.28}^{+0.36}$ | 1.47 ${}_{-0.11}^{+0.11}$ | -12.39 | SE
eFEDS J090816.6+052012 | 00151 | 3.84 | 20.31 ${}_{-0.22}^{+0.29}$ | 1.74 ${}_{-0.13}^{+0.14}$ | -12.38 | PL
eFEDS J090921.6+003608 | 00153 | 3.05 | 20.15 ${}_{-0.11}^{+0.18}$ | 2.26 ${}_{-0.12}^{+0.12}$ | -12.76 | SE
eFEDS J092725.2+024348 | 00156 | 4.40 | 20.79 ${}_{-0.51}^{+0.40}$ | 2.11 ${}_{-0.19}^{+0.24}$ | -12.75 | PL
eFEDS J085944.7-015645 | 00167 | 2.07 | 20.20 ${}_{-0.15}^{+0.22}$ | 1.83 ${}_{-0.12}^{+0.12}$ | -12.49 | WA
eFEDS J083723.1+001724 | 00168 | 4.63 | 20.69 ${}_{-0.46}^{+0.44}$ | 1.81 ${}_{-0.14}^{+0.16}$ | -12.46 | PL
eFEDS J084535.4+001621 | 00169 | 3.35 | 20.42 ${}_{-0.29}^{+0.33}$ | 1.90 ${}_{-0.13}^{+0.15}$ | -12.51 | PL
eFEDS J092759.5-002905 | 00175 | 3.05 | 20.23 ${}_{-0.17}^{+0.25}$ | 2.25 ${}_{-0.13}^{+0.13}$ | -12.81 | PL
eFEDS J093912.7+033956 | 00176 | 3.33 | 20.26 ${}_{-0.18}^{+0.29}$ | 2.14 ${}_{-0.13}^{+0.13}$ | -12.72 | SE
eFEDS J093826.3+022037 | 00184 | 3.60 | 20.29 ${}_{-0.20}^{+0.29}$ | 1.94 ${}_{-0.12}^{+0.13}$ | -12.43 | PCF
eFEDS J091551.6+044732 | 00192 | 4.04 | 20.33 ${}_{-0.23}^{+0.32}$ | 1.92 ${}_{-0.14}^{+0.16}$ | -12.60 | PL
eFEDS J084833.9+025312 | 00193 | 3.29 | 20.47 ${}_{-0.32}^{+0.40}$ | 1.81 ${}_{-0.12}^{+0.15}$ | -12.52 | PL
eFEDS J090610.1-004553 | 00194 | 2.89 | 20.24 ${}_{-0.17}^{+0.25}$ | 1.98 ${}_{-0.12}^{+0.14}$ | -12.62 | PCF
eFEDS J092723.6-014121 | 00195 | 2.94 | 20.36 ${}_{-0.25}^{+0.32}$ | 2.35 ${}_{-0.15}^{+0.16}$ | -13.05 | PL
eFEDS J084759.9-003333 | 00200 | 2.79 | 20.19 ${}_{-0.14}^{+0.22}$ | 2.22 ${}_{-0.13}^{+0.14}$ | -12.69 | SE
eFEDS J091034.3+031329 | 00204 | 3.11 | 20.19 ${}_{-0.14}^{+0.22}$ | 2.10 ${}_{-0.13}^{+0.15}$ | -12.72 | SE
eFEDS J091624.8+040944 | 00206 | 3.72 | 20.25 ${}_{-0.18}^{+0.25}$ | 2.19 ${}_{-0.14}^{+0.14}$ | -12.81 | WA
eFEDS J085439.4+004143 | 00213 | 4.86 | 20.32 ${}_{-0.23}^{+0.32}$ | 1.79 ${}_{-0.13}^{+0.14}$ | -12.48 | PL
eFEDS J090831.9+045105 | 00214 | 3.70 | 20.24 ${}_{-0.18}^{+0.26}$ | 1.76 ${}_{-0.14}^{+0.13}$ | -12.49 | PCF
eFEDS J084131.6-005217 | 00216 | 3.24 | 20.16 ${}_{-0.12}^{+0.18}$ | 2.33 ${}_{-0.13}^{+0.15}$ | -12.87 | SE
eFEDS J085004.0+032642 | 00217 | 3.56 | 20.89 ${}_{-0.44}^{+0.30}$ | 1.67 ${}_{-0.23}^{+0.32}$ | -12.38 | PL
(1) | (2) | (3) | (4) | (5) | (6) | (7)
---|---|---|---|---|---|---
Name | ID | nHgal | log(NHz) | $\Gamma$ | log(F) | Model
|  | ($\times 10^{20}\hbox{${\rm\thinspace cm}^{-2}\,$}$) |  |  | ergs s-1 cm-2 |
eFEDS J093000.5-011807 | 00223 | 3.05 | 20.38 ${}_{-0.27}^{+0.37}$ | 1.56 ${}_{-0.13}^{+0.14}$ | -12.39 | SE
eFEDS J085643.1-020804 | 00230 | 1.89 | 20.91 ${}_{-0.49}^{+0.28}$ | 2.14 ${}_{-0.19}^{+0.25}$ | -12.95 | PL
eFEDS J085224.3+020139 | 00233 | 3.30 | 20.36 ${}_{-0.24}^{+0.34}$ | 2.13 ${}_{-0.16}^{+0.15}$ | -12.72 | WA
eFEDS J083346.6-011202 | 00235 | 3.82 | 20.30 ${}_{-0.21}^{+0.29}$ | 2.21 ${}_{-0.14}^{+0.15}$ | -12.83 | PL
eFEDS J093329.6+030811 | 00237 | 3.18 | 20.18 ${}_{-0.14}^{+0.22}$ | 1.98 ${}_{-0.14}^{+0.14}$ | -12.71 | SE
eFEDS J085559.0+005745 | 00238 | 4.79 | 20.35 ${}_{-0.25}^{+0.33}$ | 2.19 ${}_{-0.15}^{+0.18}$ | -12.83 | SE
eFEDS J084039.3-011433 | 00245 | 3.28 | 20.73 ${}_{-0.48}^{+0.40}$ | 1.84 ${}_{-0.17}^{+0.23}$ | -12.60 | PL
eFEDS J093509.2+005729 | 00252 | 4.55 | 20.26 ${}_{-0.18}^{+0.24}$ | 2.31 ${}_{-0.15}^{+0.16}$ | -12.91 | PL
eFEDS J092814.6+005631 | 00256 | 4.28 | 20.34 ${}_{-0.24}^{+0.32}$ | 2.38 ${}_{-0.16}^{+0.16}$ | -12.99 | PL
eFEDS J085812.4+010644 | 00263 | 4.53 | 20.60 ${}_{-0.36}^{+0.32}$ | 1.85 ${}_{-0.18}^{+0.21}$ | -12.59 | PL
eFEDS J090612.0+014412 | 00264 | 3.93 | 20.58 ${}_{-0.39}^{+0.44}$ | 2.23 ${}_{-0.19}^{+0.22}$ | -12.94 | PL
eFEDS J090933.7-014231 | 00267 | 2.60 | 20.45 ${}_{-0.31}^{+0.36}$ | 2.42 ${}_{-0.15}^{+0.17}$ | -13.21 | PL
eFEDS J083143.5+013952 | 00268 | 4.59 | 20.81 ${}_{-0.51}^{+0.35}$ | 2.09 ${}_{-0.22}^{+0.29}$ | -12.78 | PL
eFEDS J092237.4-004751 | 00272 | 3.24 | 20.36 ${}_{-0.25}^{+0.35}$ | 2.04 ${}_{-0.14}^{+0.15}$ | -12.74 | PL
eFEDS J092738.1+014430 | 00288 | 5.21 | 20.21 ${}_{-0.15}^{+0.24}$ | 2.27 ${}_{-0.15}^{+0.16}$ | -12.88 | SE
eFEDS J092739.7+053004 | 00297 | 4.29 | 20.60 ${}_{-0.39}^{+0.42}$ | 2.38 ${}_{-0.19}^{+0.20}$ | -12.91 | PL
eFEDS J090543.3+020716 | 00303 | 3.90 | 20.28 ${}_{-0.19}^{+0.29}$ | 1.89 ${}_{-0.15}^{+0.17}$ | -12.73 | PCF
eFEDS J092120.9+003628 | 00322 | 2.99 | 20.66 ${}_{-0.45}^{+0.46}$ | 2.07 ${}_{-0.16}^{+0.18}$ | -12.84 | PL
eFEDS J084310.5-013425 | 00323 | 3.23 | 20.37 ${}_{-0.25}^{+0.36}$ | 2.11 ${}_{-0.15}^{+0.14}$ | -12.95 | PCF
eFEDS J093259.6+040505 | 00329 | 3.12 | 20.19 ${}_{-0.14}^{+0.22}$ | 1.26 ${}_{-0.14}^{+0.13}$ | -12.28 | PCF
eFEDS J085536.0-004544 | 00330 | 2.95 | 20.34 ${}_{-0.24}^{+0.31}$ | 1.91 ${}_{-0.15}^{+0.18}$ | -12.71 | PL
eFEDS J091406.1-021119 | 00337 | 3.82 | 21.89 ${}_{-0.14}^{+0.13}$ | 1.28 ${}_{-0.19}^{+0.31}$ | -12.23 | WA
eFEDS J085512.8-000733 | 00340 | 3.98 | 20.29 ${}_{-0.21}^{+0.26}$ | 2.51 ${}_{-0.16}^{+0.18}$ | -13.14 | SE
eFEDS J085552.5+051039 | 00358 | 4.32 | 20.24 ${}_{-0.17}^{+0.26}$ | 2.22 ${}_{-0.18}^{+0.18}$ | -12.81 | SE
eFEDS J085130.8+044221 | 00364 | 4.56 | 20.43 ${}_{-0.31}^{+0.38}$ | 2.70 ${}_{-0.18}^{+0.17}$ | -13.21 | PL
eFEDS J083520.2+012517 | 00367 | 4.88 | 20.64 ${}_{-0.41}^{+0.41}$ | 1.82 ${}_{-0.21}^{+0.23}$ | -12.65 | PL
eFEDS J085814.1+045453 | 00373 | 4.16 | 21.00 ${}_{-0.63}^{+0.49}$ | 1.80 ${}_{-0.18}^{+0.24}$ | -12.62 | PL
eFEDS J091420.9+031121 | 00378 | 2.82 | 20.43 ${}_{-0.29}^{+0.38}$ | 1.90 ${}_{-0.16}^{+0.16}$ | -12.70 | PL
eFEDS J084555.5-001255 | 00384 | 3.05 | 20.35 ${}_{-0.24}^{+0.29}$ | 2.56 ${}_{-0.18}^{+0.19}$ | -13.18 | PL
eFEDS J092331.0-000243 | 00385 | 3.01 | 20.38 ${}_{-0.27}^{+0.37}$ | 2.17 ${}_{-0.17}^{+0.19}$ | -12.91 | PL
eFEDS J093708.6+012543 | 00389 | 4.92 | 20.30 ${}_{-0.21}^{+0.29}$ | 2.29 ${}_{-0.18}^{+0.18}$ | -12.96 | PL
eFEDS J092946.4+020352 | 00395 | 5.55 | 21.23 ${}_{-0.31}^{+0.23}$ | 1.44 ${}_{-0.28}^{+0.42}$ | -12.31 | PL
eFEDS J092107.5+001320 | 00400 | 3.04 | 21.15 ${}_{-0.56}^{+0.36}$ | 1.18 ${}_{-0.13}^{+0.24}$ | -12.27 | WA
eFEDS J083236.3+044507 | 00420 | 2.78 | 20.94 ${}_{-0.46}^{+0.29}$ | 1.25 ${}_{-0.16}^{+0.22}$ | -12.05 | PCF
eFEDS J090215.4+032408 | 00426 | 4.30 | 20.20 ${}_{-0.15}^{+0.24}$ | 2.01 ${}_{-0.17}^{+0.18}$ | -12.86 | SE
eFEDS J083838.6+000552 | 00434 | 4.43 | 21.00 ${}_{-0.45}^{+0.27}$ | 2.26 ${}_{-0.31}^{+0.40}$ | -12.98 | PL
eFEDS J085447.4-003959 | 00436 | 3.08 | 20.41 ${}_{-0.27}^{+0.33}$ | 2.34 ${}_{-0.19}^{+0.21}$ | -13.09 | PL
eFEDS J091157.5+014327 | 00439 | 2.88 | 22.42 ${}_{-0.13}^{+0.11}$ | 2.22 ${}_{-0.43}^{+0.44}$ | -12.44 | WA
eFEDS J083647.5+042214 | 00450 | 3.06 | 20.23 ${}_{-0.16}^{+0.27}$ | 2.12 ${}_{-0.18}^{+0.19}$ | -12.97 | SE
eFEDS J092507.9+001914 | 00457 | 3.10 | 21.15 ${}_{-0.74}^{+0.55}$ | 1.52 ${}_{-0.18}^{+0.24}$ | -12.48 | PL
eFEDS J085318.2-010309 | 00461 | 2.48 | 21.98 ${}_{-0.11}^{+0.11}$ | 1.37 ${}_{-0.25}^{+0.33}$ | -12.09 | PL
eFEDS J082934.1-003310 | 00462 | 4.71 | 21.81 ${}_{-1.01}^{+0.42}$ | 1.84 ${}_{-0.29}^{+0.39}$ | -12.67 | PL
eFEDS J092435.2+012846 | 00528 | 3.62 | 20.35 ${}_{-0.24}^{+0.34}$ | 2.27 ${}_{-0.19}^{+0.19}$ | -13.11 | SE
eFEDS J090306.4+030449 | 00534 | 4.25 | 20.51 ${}_{-0.34}^{+0.44}$ | 2.18 ${}_{-0.20}^{+0.24}$ | -12.97 | PL
eFEDS J084528.7-002724 | 00540 | 2.97 | 20.60 ${}_{-0.38}^{+0.37}$ | 2.10 ${}_{-0.24}^{+0.33}$ | -12.91 | PCF
eFEDS J090604.1+011114 | 00545 | 3.87 | 20.60 ${}_{-0.40}^{+0.46}$ | 2.06 ${}_{-0.21}^{+0.22}$ | -12.94 | PL
(1) | (2) | (3) | (4) | (5) | (6) | (7)
---|---|---|---|---|---|---
Name | ID | nHgal | log(NHz) | $\Gamma$ | log(F) | Model
|  | ($\times 10^{20}\hbox{${\rm\thinspace cm}^{-2}\,$}$) |  |  | ergs s-1 cm-2 |
eFEDS J092017.3-004659 | 00558 | 3.45 | 21.52 ${}_{-0.26}^{+0.18}$ | 1.95 ${}_{-0.44}^{+0.46}$ | -12.71 | PL
eFEDS J090326.2-005527 | 00618 | 2.80 | 20.54 ${}_{-0.37}^{+0.49}$ | 2.13 ${}_{-0.19}^{+0.18}$ | -13.07 | WA
eFEDS J091119.2+031150 | 00626 | 3.15 | 20.39 ${}_{-0.27}^{+0.39}$ | 1.41 ${}_{-0.19}^{+0.20}$ | -12.56 | PL
eFEDS J093123.9+051344 | 00632 | 3.79 | 21.95 ${}_{-0.19}^{+0.13}$ | 2.36 ${}_{-0.51}^{+0.42}$ | -12.52 | WA
eFEDS J092938.4+021627 | 00667 | 5.24 | 22.18 ${}_{-0.51}^{+0.28}$ | 1.36 ${}_{-0.24}^{+0.34}$ | -12.41 | WA
eFEDS J092227.5+030909 | 00713 | 3.91 | 20.26 ${}_{-0.19}^{+0.29}$ | 1.39 ${}_{-0.18}^{+0.18}$ | -12.57 | PCF
eFEDS J091517.8-001720 | 00758 | 3.01 | 21.71 ${}_{-0.49}^{+0.26}$ | 1.14 ${}_{-0.10}^{+0.20}$ | -12.38 | PL
eFEDS J092200.7-012209 | 00760 | 3.60 | 20.29 ${}_{-0.20}^{+0.31}$ | 1.87 ${}_{-0.22}^{+0.21}$ | -13.06 | SE
eFEDS J093255.9+034230 | 00774 | 3.09 | 21.03 ${}_{-0.66}^{+0.53}$ | 1.54 ${}_{-0.22}^{+0.30}$ | -12.63 | PL
eFEDS J083141.8+014556 | 00781 | 4.62 | 21.50 ${}_{-0.34}^{+0.21}$ | 1.30 ${}_{-0.21}^{+0.34}$ | -12.41 | PL
eFEDS J085043.9-013638 | 00784 | 2.24 | 20.33 ${}_{-0.23}^{+0.33}$ | 2.42 ${}_{-0.22}^{+0.22}$ | -13.53 | SE
eFEDS J090852.2-013741 | 00881 | 2.54 | 21.08 ${}_{-0.57}^{+0.39}$ | 1.08 ${}_{-0.06}^{+0.14}$ | -12.51 | WA
eFEDS J090623.7+031745 | 01000 | 3.17 | 20.56 ${}_{-0.39}^{+0.44}$ | 1.88 ${}_{-0.23}^{+0.27}$ | -13.09 | PL
eFEDS J090022.7+013116 | 01007 | 4.57 | 22.26 ${}_{-0.17}^{+0.17}$ | 1.66 ${}_{-0.41}^{+0.59}$ | -12.35 | WA
eFEDS J093841.3+032422 | 01029 | 3.19 | 20.48 ${}_{-0.34}^{+0.39}$ | 2.05 ${}_{-0.27}^{+0.29}$ | -13.15 | PL
eFEDS J091443.7+035410 | 01058 | 3.56 | 21.56 ${}_{-0.35}^{+0.28}$ | 1.31 ${}_{-0.22}^{+0.41}$ | -12.46 | WA
eFEDS J090909.1-013201 | 01091 | 2.61 | 20.75 ${}_{-0.53}^{+0.61}$ | 1.93 ${}_{-0.25}^{+0.26}$ | -13.20 | PL
eFEDS J093201.6+031859 | 01099 | 3.22 | 20.67 ${}_{-0.45}^{+0.53}$ | 1.89 ${}_{-0.28}^{+0.35}$ | -13.02 | PL
eFEDS J090111.8+044900 | 01116 | 3.80 | 20.97 ${}_{-0.65}^{+0.64}$ | 1.84 ${}_{-0.25}^{+0.28}$ | -12.94 | PL
eFEDS J084221.3+000459 | 01124 | 3.60 | 21.49 ${}_{-0.46}^{+0.30}$ | 1.26 ${}_{-0.19}^{+0.36}$ | -12.51 | PL
eFEDS J083857.6+041426 | 01136 | 2.96 | 20.40 ${}_{-0.28}^{+0.39}$ | 1.89 ${}_{-0.29}^{+0.28}$ | -13.11 | SE
eFEDS J091320.6+034013 | 01137 | 3.40 | 20.42 ${}_{-0.30}^{+0.37}$ | 1.64 ${}_{-0.25}^{+0.27}$ | -12.83 | PL
eFEDS J091821.2+002954 | 01153 | 2.94 | 20.53 ${}_{-0.38}^{+0.50}$ | 1.31 ${}_{-0.18}^{+0.21}$ | -12.66 | PL
eFEDS J091755.4+003060 | 01161 | 2.91 | 21.19 ${}_{-0.69}^{+0.37}$ | 2.06 ${}_{-0.37}^{+0.52}$ | -13.14 | PCF
eFEDS J085135.5+044126 | 01165 | 4.55 | 21.71 ${}_{-0.18}^{+0.17}$ | 1.22 ${}_{-0.17}^{+0.32}$ | -12.23 | PL
eFEDS J083002.0+005059 | 01277 | 4.48 | 22.85 ${}_{-0.18}^{+0.17}$ | 2.21 ${}_{-0.76}^{+0.57}$ | -12.63 | WA
eFEDS J084324.6+023121 | 01283 | 4.82 | 20.74 ${}_{-0.51}^{+0.58}$ | 1.69 ${}_{-0.23}^{+0.27}$ | -12.85 | PL
eFEDS J083718.2+050938 | 01492 | 3.06 | 20.96 ${}_{-0.62}^{+0.41}$ | 2.19 ${}_{-0.35}^{+0.41}$ | -13.28 | PL
eFEDS J093441.8+034511 | 01536 | 3.05 | 22.13 ${}_{-0.21}^{+0.19}$ | 1.28 ${}_{-0.21}^{+0.47}$ | -12.38 | WA
eFEDS J084157.8-022617 | 01543 | 3.04 | 22.37 ${}_{-0.47}^{+0.21}$ | 1.56 ${}_{-0.45}^{+0.66}$ | -12.66 | WA
eFEDS J083956.9+035338 | 01637 | 3.04 | 22.65 ${}_{-0.15}^{+0.12}$ | 2.08 ${}_{-0.60}^{+0.56}$ | -12.51 | WA
eFEDS J083013.5-013558 | 01736 | 3.82 | 20.22 ${}_{-0.16}^{+0.25}$ | 2.24 ${}_{-0.30}^{+0.32}$ | -13.47 | SE
eFEDS J085324.2-011357 | 01911 | 2.39 | 20.72 ${}_{-0.50}^{+0.56}$ | 1.96 ${}_{-0.35}^{+0.39}$ | -13.30 | PL
eFEDS J091800.1+042506 | 02010 | 3.78 | 20.33 ${}_{-0.23}^{+0.31}$ | 2.67 ${}_{-0.33}^{+0.23}$ | -13.83 | PCF
eFEDS J090313.1+032927 | 02242 | 4.09 | 20.94 ${}_{-0.58}^{+0.43}$ | 1.92 ${}_{-0.43}^{+0.57}$ | -13.19 | PL
eFEDS J082841.3-004219 | 02507 | 4.80 | 20.50 ${}_{-0.36}^{+0.48}$ | 1.50 ${}_{-0.27}^{+0.27}$ | -12.85 | PCF
eFEDS J085409.3-005029 | 02634 | 2.74 | 21.90 ${}_{-0.27}^{+0.22}$ | 1.24 ${}_{-0.18}^{+0.40}$ | -12.68 | PCF
eFEDS J090328.2+030908 | 02660 | 4.13 | 20.87 ${}_{-0.58}^{+0.57}$ | 1.25 ${}_{-0.17}^{+0.27}$ | -12.68 | PCF
eFEDS J085548.0+004738 | 03205 | 4.93 | 23.32 ${}_{-0.13}^{+0.12}$ | 1.98 ${}_{-0.68}^{+0.69}$ | -12.07 | WA
eFEDS J091928.9+043847 | 03376 | 3.79 | 21.22 ${}_{-0.69}^{+0.47}$ | 1.26 ${}_{-0.19}^{+0.38}$ | -12.83 | PCF
eFEDS J085552.8-013855 | 03447 | 2.08 | 22.65 ${}_{-0.19}^{+0.16}$ | 1.91 ${}_{-0.55}^{+0.65}$ | -12.81 | PL
eFEDS J093518.1+003235 | 03798 | 4.05 | 20.60 ${}_{-0.44}^{+0.54}$ | 1.36 ${}_{-0.25}^{+0.42}$ | -13.04 | SE
eFEDS J083601.6-002460 | 04215 | 4.24 | 22.29 ${}_{-0.34}^{+0.24}$ | 1.34 ${}_{-0.25}^{+0.59}$ | -12.79 | PL
eFEDS J083848.2+040735 | 04444 | 2.96 | 20.36 ${}_{-0.24}^{+0.32}$ | 2.66 ${}_{-0.33}^{+0.24}$ | -13.94 | WA
eFEDS J083404.6-015103 | 04871 | 3.34 | 22.63 ${}_{-0.56}^{+0.22}$ | 1.42 ${}_{-0.33}^{+0.72}$ | -12.72 | PCF
eFEDS J083553.3-000346 | 05196 | 4.47 | 22.49 ${}_{-0.23}^{+0.18}$ | 1.45 ${}_{-0.32}^{+0.65}$ | -12.78 | WA
(1) | (2) | (3) | (4) | (5) | (6) | (7)
---|---|---|---|---|---|---
Name | ID | nHgal | log(NHz) | $\Gamma$ | log(F) | Model
|  | ($\times 10^{20}\hbox{${\rm\thinspace cm}^{-2}\,$}$) |  |  | ergs s-1 cm-2 |
eFEDS J094032.7+043452 | 05278 | 3.87 | 20.51 ${}_{-0.36}^{+0.49}$ | 1.45 ${}_{-0.30}^{+0.40}$ | -12.90 | PCF
eFEDS J083253.7+011622 | 05546 | 4.52 | 20.69 ${}_{-0.48}^{+0.54}$ | 1.79 ${}_{-0.42}^{+0.46}$ | -13.37 | PCF
eFEDS J083247.1+001340 | 05842 | 4.52 | 21.16 ${}_{-0.65}^{+0.41}$ | 1.13 ${}_{-0.10}^{+0.25}$ | -12.88 | PCF
eFEDS J083322.6-000851 | 06275 | 4.43 | 22.24 ${}_{-0.25}^{+0.20}$ | 1.50 ${}_{-0.38}^{+0.75}$ | -12.86 | PL
eFEDS J085506.8-001147 | 06549 | 3.82 | 21.09 ${}_{-0.75}^{+0.68}$ | 1.44 ${}_{-0.32}^{+0.56}$ | -13.27 | PL
eFEDS J083624.1+044724 | 06693 | 3.12 | 22.99 ${}_{-0.16}^{+0.14}$ | 1.94 ${}_{-0.65}^{+0.74}$ | -12.55 | WA
eFEDS J090852.0+053713 | 06932 | 3.91 | 22.52 ${}_{-0.19}^{+0.17}$ | 1.57 ${}_{-0.43}^{+0.75}$ | -12.47 | PL
eFEDS J083548.4+014325 | 08243 | 4.88 | 20.61 ${}_{-0.41}^{+0.46}$ | 1.53 ${}_{-0.37}^{+0.62}$ | -13.27 | PCF
eFEDS J085240.9-013923 | 08968 | 2.12 | 22.94 ${}_{-0.30}^{+0.29}$ | 1.49 ${}_{-0.37}^{+0.74}$ | -12.86 | WA
eFEDS J092511.4-010623 | 09040 | 3.13 | 22.50 ${}_{-0.34}^{+0.32}$ | 1.39 ${}_{-0.30}^{+0.64}$ | -12.69 | PL
eFEDS J093432.2+002831 | 09905 | 3.79 | 22.70 ${}_{-0.19}^{+0.16}$ | 1.87 ${}_{-0.58}^{+0.71}$ | -12.84 | PL
eFEDS J093100.9+021125 | 10285 | 5.11 | 23.17 ${}_{-0.21}^{+0.17}$ | 2.13 ${}_{-0.74}^{+0.63}$ | -12.56 | WA
eFEDS J085801.6-021650 | 10831 | 1.85 | 23.20 ${}_{-0.16}^{+0.15}$ | 2.07 ${}_{-0.68}^{+0.64}$ | -12.94 | WA
eFEDS J093144.2-022851 | 11430 | 3.39 | 20.71 ${}_{-0.48}^{+0.62}$ | 1.66 ${}_{-0.48}^{+0.72}$ | -13.58 | PCF
eFEDS J090735.4-013734 | 11437 | 2.47 | 23.41 ${}_{-0.32}^{+0.19}$ | 1.89 ${}_{-0.62}^{+0.72}$ | -13.04 | WA
eFEDS J092820.0+004356 | 13817 | 3.93 | 22.79 ${}_{-0.36}^{+0.29}$ | 1.57 ${}_{-0.42}^{+0.76}$ | -12.79 | PL
eFEDS J093904.1+034206 | 15909 | 3.33 | 23.65 ${}_{-0.20}^{+0.18}$ | 2.04 ${}_{-0.67}^{+0.65}$ | -12.16 | WA
eFEDS J092203.3-004445 | 16185 | 3.27 | 23.20 ${}_{-0.35}^{+0.27}$ | 1.89 ${}_{-0.64}^{+0.73}$ | -12.75 | WA
eFEDS J085819.9+031048 | 18184 | 4.23 | 23.57 ${}_{-0.21}^{+0.18}$ | 2.12 ${}_{-0.72}^{+0.62}$ | -12.61 | WA
eFEDS J093252.4+015246 | 27045 | 4.96 | 24.11 ${}_{-1.16}^{+0.25}$ | 1.93 ${}_{-0.63}^{+0.71}$ | -12.67 | WA
Table 11: Summary of warm absorber parameters for sources with significant
warm absorbers ($>95\%$). Column (1) gives the eROSITA ID, column (2) gives
the warm absorber column density, column (3) gives the warm absorber
ionisation, column (4) gives the photon index, and column (5) gives the Bayes
factor Kwa.

(1) | (2) | (3) | (4) | (5)
---|---|---|---|---
eROID | log(nH) | log($\xi$) | $\Gamma_{wa}$ | Kwa
00016 | 22.22 ${}_{-0.13}^{+0.13}$ | 1.86 ${}_{-0.11}^{+0.10}$ | 1.95 ${}_{-0.06}^{+0.07}$ | 2.98$\times$108
00028 | 22.26 ${}_{-0.25}^{+0.13}$ | 1.84 ${}_{-0.30}^{+0.12}$ | 1.94 ${}_{-0.07}^{+0.10}$ | 5.66$\times$1010
00037 | 21.47 ${}_{-0.36}^{+0.38}$ | 1.30 ${}_{-3.68}^{+0.51}$ | 2.20 ${}_{-0.12}^{+0.14}$ | 18.42
00075 | 21.14 ${}_{-0.58}^{+0.31}$ | -0.90 ${}_{-2.12}^{+3.30}$ | 1.82 ${}_{-0.25}^{+0.32}$ | 1.11
00078 | 21.47 ${}_{-0.97}^{+1.33}$ | 1.62 ${}_{-3.47}^{+1.29}$ | 1.27 ${}_{-0.13}^{+0.19}$ | 1.18
00105 | 22.46 ${}_{-0.43}^{+0.32}$ | 2.25 ${}_{-0.19}^{+0.25}$ | 2.43 ${}_{-0.14}^{+0.13}$ | 9.89
00107 | 21.27 ${}_{-0.23}^{+0.62}$ | -1.99 ${}_{-1.47}^{+3.87}$ | 1.91 ${}_{-0.27}^{+0.31}$ | 8.95
00132 | 21.18 ${}_{-0.62}^{+1.15}$ | 1.83 ${}_{-4.11}^{+0.86}$ | 2.43 ${}_{-0.18}^{+0.23}$ | 1.10
00167 | 21.78 ${}_{-0.56}^{+0.83}$ | 1.71 ${}_{-0.91}^{+0.88}$ | 1.90 ${}_{-0.17}^{+0.24}$ | 4.18
00206 | 22.23 ${}_{-0.45}^{+0.31}$ | 1.88 ${}_{-0.33}^{+0.26}$ | 2.27 ${}_{-0.19}^{+0.22}$ | 11.18
00233 | 22.45 ${}_{-1.77}^{+0.98}$ | 2.61 ${}_{-2.15}^{+0.82}$ | 2.12 ${}_{-0.19}^{+0.23}$ | 0.98
00337 | 21.74 ${}_{-0.21}^{+0.17}$ | -1.77 ${}_{-1.55}^{+1.24}$ | 1.49 ${}_{-0.27}^{+0.36}$ | 14.67
00400 | 21.25 ${}_{-0.70}^{+0.59}$ | 0.11 ${}_{-2.86}^{+2.45}$ | 1.31 ${}_{-0.22}^{+0.38}$ | 1.37
00439 | 22.06 ${}_{-1.18}^{+0.26}$ | -1.09 ${}_{-1.82}^{+3.06}$ | 2.35 ${}_{-0.46}^{+0.38}$ | 1.67
00618 | 22.24 ${}_{-1.33}^{+0.29}$ | 1.67 ${}_{-0.75}^{+0.36}$ | 2.68 ${}_{-0.49}^{+0.23}$ | 1.45
00632 | 21.69 ${}_{-0.25}^{+0.19}$ | -1.74 ${}_{-1.69}^{+1.36}$ | 2.56 ${}_{-0.47}^{+0.30}$ | 6.14
00667 | 21.76 ${}_{-1.16}^{+0.63}$ | 0.00 ${}_{-2.85}^{+2.72}$ | 1.44 ${}_{-0.26}^{+0.41}$ | 1.00
00881 | 22.23 ${}_{-0.18}^{+0.11}$ | 0.96 ${}_{-0.15}^{+0.14}$ | 2.20 ${}_{-0.65}^{+0.54}$ | 1748.16
01007 | 21.96 ${}_{-0.97}^{+0.33}$ | -0.81 ${}_{-2.10}^{+2.41}$ | 1.81 ${}_{-0.50}^{+0.63}$ | 1.38
01058 | 21.66 ${}_{-0.72}^{+0.50}$ | 0.06 ${}_{-2.72}^{+1.67}$ | 1.64 ${}_{-0.45}^{+0.67}$ | 2.14
01277 | 22.02 ${}_{-1.39}^{+0.69}$ | -0.18 ${}_{-2.59}^{+2.57}$ | 2.21 ${}_{-0.74}^{+0.56}$ | 0.94
01536 | 21.98 ${}_{-0.43}^{+0.33}$ | -0.89 ${}_{-1.94}^{+2.12}$ | 1.40 ${}_{-0.29}^{+0.58}$ | 4.06
01543 | 22.53 ${}_{-0.21}^{+0.18}$ | 1.52 ${}_{-0.27}^{+0.28}$ | 1.73 ${}_{-0.43}^{+0.58}$ | 46.91
01637 | 21.91 ${}_{-1.25}^{+0.57}$ | -0.24 ${}_{-2.58}^{+3.06}$ | 2.14 ${}_{-0.63}^{+0.54}$ | 1.01
03205 | 22.43 ${}_{-1.66}^{+0.66}$ | -0.61 ${}_{-2.27}^{+2.85}$ | 2.02 ${}_{-0.72}^{+0.65}$ | 1.20
04444 | 23.77 ${}_{-0.21}^{+0.09}$ | 3.35 ${}_{-0.56}^{+0.57}$ | 1.18 ${}_{-0.13}^{+0.26}$ | 78.3
05196 | 21.87 ${}_{-1.21}^{+0.57}$ | -0.39 ${}_{-2.40}^{+2.92}$ | 1.53 ${}_{-0.4}^{+0.68}$ | 1.53
06693 | 22.23 ${}_{-1.45}^{+0.62}$ | -0.44 ${}_{-2.46}^{+3.02}$ | 2.02 ${}_{-0.64}^{+0.68}$ | 1.02
08968 | 22.60 ${}_{-1.43}^{+0.45}$ | -0.05 ${}_{-2.75}^{+2.43}$ | 1.61 ${}_{-0.45}^{+0.79}$ | 1.87
10285 | 22.29 ${}_{-1.52}^{+0.68}$ | -0.05 ${}_{-2.64}^{+2.37}$ | 2.17 ${}_{-0.73}^{+0.60}$ | 1.37
10831 | 22.40 ${}_{-1.57}^{+0.62}$ | -0.28 ${}_{-2.55}^{+2.70}$ | 2.14 ${}_{-0.69}^{+0.60}$ | 1.47
11437 | 22.53 ${}_{-1.64}^{+0.70}$ | -0.39 ${}_{-2.50}^{+2.57}$ | 1.90 ${}_{-0.66}^{+0.78}$ | 1.42
15909 | 22.50 ${}_{-1.63}^{+0.89}$ | -0.05 ${}_{-2.66}^{+2.69}$ | 2.09 ${}_{-0.74}^{+0.65}$ | 1.23
16185 | 22.55 ${}_{-1.67}^{+0.59}$ | 0.08 ${}_{-2.69}^{+2.41}$ | 1.88 ${}_{-0.60}^{+0.77}$ | 1.87
18184 | 22.53 ${}_{-1.77}^{+0.79}$ | -0.09 ${}_{-2.67}^{+2.62}$ | 2.09 ${}_{-0.69}^{+0.59}$ | 1.34
27045 | 23.59 ${}_{-2.16}^{+0.30}$ | -0.80 ${}_{-2.24}^{+2.73}$ | 1.96 ${}_{-0.63}^{+0.67}$ | 2.06

Table 12: Summary of partial covering absorber parameters for sources with
significant partial coverers ($>95\%$). Column (1) gives the eROSITA ID,
column (2) gives the partial covering absorber column density, column (3)
gives the partial covering absorber ionisation, column (4) gives the photon
index, and column (5) gives the Bayes factor Kpcf.

(1) | (2) | (3) | (4) | (5)
---|---|---|---|---
eROID | log(nH) | C | $\Gamma_{pcf}$ | Kpcf
00014 | 22.88 ${}_{-0.29}^{+0.52}$ | 0.53 ${}_{-0.17}^{+0.14}$ | 2.37 ${}_{-0.09}^{+0.11}$ | 6.03
00023 | 23.44 ${}_{-0.25}^{+0.27}$ | 0.73 ${}_{-0.2}^{+0.11}$ | 2.13 ${}_{-0.07}^{+0.08}$ | 11.67
00030 | 22.63 ${}_{-0.14}^{+0.14}$ | 0.62 ${}_{-0.13}^{+0.09}$ | 2.61 ${}_{-0.18}^{+0.17}$ | 26.00
00043 | 23.22 ${}_{-0.67}^{+0.81}$ | 0.51 ${}_{-0.31}^{+0.25}$ | 2.66 ${}_{-0.10}^{+0.11}$ | 1.63
00071 | 23.59 ${}_{-0.46}^{+0.39}$ | 0.77 ${}_{-0.34}^{+0.13}$ | 2.21 ${}_{-0.11}^{+0.13}$ | 3.03
00108 | 23.97 ${}_{-0.46}^{+0.24}$ | 0.87 ${}_{-0.39}^{+0.08}$ | 2.46 ${}_{-0.11}^{+0.13}$ | 3.98
00120 | 22.85 ${}_{-1.01}^{+1.31}$ | 0.44 ${}_{-0.28}^{+0.25}$ | 1.41 ${}_{-0.16}^{+0.27}$ | 1.56
00184 | 22.93 ${}_{-1.41}^{+1.19}$ | 0.45 ${}_{-0.29}^{+0.26}$ | 2.07 ${}_{-0.18}^{+0.25}$ | 1.47
00194 | 22.89 ${}_{-0.29}^{+0.27}$ | 0.66 ${}_{-0.32}^{+0.15}$ | 2.24 ${}_{-0.24}^{+0.28}$ | 2.62
00214 | 22.62 ${}_{-0.81}^{+1.52}$ | 0.45 ${}_{-0.29}^{+0.26}$ | 1.89 ${}_{-0.19}^{+0.32}$ | 1.60
00303 | 22.98 ${}_{-0.45}^{+0.76}$ | 0.62 ${}_{-0.34}^{+0.18}$ | 2.11 ${}_{-0.24}^{+0.32}$ | 2.08
00323 | 23.4 ${}_{-1.72}^{+0.81}$ | 0.52 ${}_{-0.34}^{+0.28}$ | 2.2 ${}_{-0.18}^{+0.22}$ | 1.77
00329 | 22.39 ${}_{-0.10}^{+0.09}$ | 0.91 ${}_{-0.07}^{+0.03}$ | 2.61 ${}_{-0.36}^{+0.25}$ | 227.95
00420 | 22.17 ${}_{-1.27}^{+1.63}$ | 0.55 ${}_{-0.37}^{+0.26}$ | 1.48 ${}_{-0.31}^{+0.64}$ | 1.71
00540 | 23.4 ${}_{-0.96}^{+0.53}$ | 0.78 ${}_{-0.48}^{+0.16}$ | 2.23 ${}_{-0.28}^{+0.34}$ | 2.09
00713 | 22.38 ${}_{-0.25}^{+0.39}$ | 0.73 ${}_{-0.36}^{+0.14}$ | 2.06 ${}_{-0.58}^{+0.57}$ | 3.27
01161 | 23.78 ${}_{-1.89}^{+0.33}$ | 0.86 ${}_{-0.48}^{+0.1}$ | 2.34 ${}_{-0.47}^{+0.43}$ | 2.12
02010 | 23.66 ${}_{-0.12}^{+0.12}$ | 0.98 ${}_{-0.05}^{+0.01}$ | 2.74 ${}_{-0.27}^{+0.18}$ | 15005.82
02507 | 23.22 ${}_{-0.31}^{+0.24}$ | 0.82 ${}_{-0.38}^{+0.1}$ | 2.28 ${}_{-0.66}^{+0.50}$ | 4.32
02634 | 22.96 ${}_{-1.84}^{+0.98}$ | 0.58 ${}_{-0.35}^{+0.26}$ | 1.3 ${}_{-0.22}^{+0.48}$ | 1.65
02660 | 23.31 ${}_{-2.30}^{+0.85}$ | 0.54 ${}_{-0.34}^{+0.28}$ | 1.37 ${}_{-0.25}^{+0.45}$ | 1.38
03376 | 22.98 ${}_{-2.04}^{+1.19}$ | 0.56 ${}_{-0.36}^{+0.29}$ | 1.34 ${}_{-0.25}^{+0.48}$ | 1.39
04871 | 22.86 ${}_{-0.50}^{+0.36}$ | 0.86 ${}_{-0.35}^{+0.09}$ | 1.42 ${}_{-0.32}^{+0.64}$ | 4.41
05278 | 23.23 ${}_{-1.17}^{+0.76}$ | 0.67 ${}_{-0.41}^{+0.22}$ | 1.71 ${}_{-0.45}^{+0.61}$ | 2.17
05546 | 22.65 ${}_{-1.90}^{+1.56}$ | 0.47 ${}_{-0.32}^{+0.34}$ | 1.89 ${}_{-0.46}^{+0.49}$ | 1.63
05842 | 23.24 ${}_{-0.20}^{+0.18}$ | 0.96 ${}_{-0.05}^{+0.02}$ | 1.36 ${}_{-0.27}^{+0.53}$ | 206.15
08243 | 23.04 ${}_{-1.08}^{+0.72}$ | 0.77 ${}_{-0.48}^{+0.18}$ | 1.65 ${}_{-0.45}^{+0.62}$ | 1.56
11430 | 23.19 ${}_{-0.30}^{+0.32}$ | 0.92 ${}_{-0.65}^{+0.06}$ | 1.76 ${}_{-0.52}^{+0.68}$ | 2.37

Table 13: Summary of soft excess parameters for sources with significant soft
excesses measured with a second power law component ($>95\%$). Column (1)
gives the eROSITA ID, column (2) gives the hard X-ray photon index, column (3)
gives the soft X-ray photon index, column (4) gives the soft excess strength
(SE), and column (5) gives the Bayes factor Kpl.

(1) | (2) | (3) | (4) | (5)
---|---|---|---|---
eROID | $\Gamma_{h}$ | $\Gamma_{s}$ | SE | Kpl
00001 | 2.63 ${}_{-0.14}^{+0.05}$ | 5.83 ${}_{-2.54}^{+1.10}$ | 0.22 ${}_{-0.11}^{+0.38}$ | 2.65
00003 | 2.87 ${}_{-0.05}^{+0.05}$ | 6.60 ${}_{-1.69}^{+0.87}$ | 0.18 ${}_{-0.09}^{+0.23}$ | 2.54
00004 | 2.18 ${}_{-0.10}^{+0.06}$ | 5.68 ${}_{-1.33}^{+1.11}$ | 0.38 ${}_{-0.12}^{+0.24}$ | 37405.4
00007 | 2.07 ${}_{-0.22}^{+0.14}$ | 4.39 ${}_{-0.91}^{+1.26}$ | 0.91 ${}_{-0.39}^{+0.84}$ | 840.36
00011 | 2.57 ${}_{-0.85}^{+0.36}$ | 3.72 ${}_{-0.27}^{+0.77}$ | 4.89 ${}_{-3.69}^{+30.64}$ | 122$\times 10^{7}$
00029 | 2.40 ${}_{-0.12}^{+0.11}$ | 6.71 ${}_{-1.58}^{+0.92}$ | 0.64 ${}_{-0.28}^{+0.54}$ | 18.68
00034 | 2.05 ${}_{-0.14}^{+0.12}$ | 6.51 ${}_{-1.38}^{+1.00}$ | 0.98 ${}_{-0.38}^{+0.84}$ | 3723.68
00035 | 2.31 ${}_{-0.15}^{+0.12}$ | 6.21 ${}_{-1.87}^{+1.22}$ | 1.08 ${}_{-0.53}^{+1.19}$ | 11.30
00038 | 1.92 ${}_{-0.36}^{+0.2}$ | 4.84 ${}_{-1.58}^{+1.94}$ | 1.43 ${}_{-0.89}^{+2.94}$ | 9.82
00039 | 1.64 ${}_{-0.35}^{+0.42}$ | 4.70 ${}_{-0.57}^{+0.74}$ | 18.00 ${}_{-8.11}^{+11.48}$ | 129896.89
00045 | 1.78 ${}_{-0.42}^{+0.29}$ | 4.50 ${}_{-0.92}^{+1.40}$ | 2.60 ${}_{-1.19}^{+2.66}$ | 1554.05
00054 | 1.92 ${}_{-0.40}^{+0.30}$ | 4.68 ${}_{-1.02}^{+1.29}$ | 2.74 ${}_{-1.53}^{+2.93}$ | 47.84
00057 | 1.86 ${}_{-0.24}^{+0.19}$ | 5.19 ${}_{-1.66}^{+1.31}$ | 1.81 ${}_{-1.33}^{+4.18}$ | 4.22
00060 | 2.08 ${}_{-0.23}^{+0.25}$ | 8.49 ${}_{-2.59}^{+1.11}$ | 37.11 ${}_{-35.19}^{+125.97}$ | 2.15
00070 | 2.27 ${}_{-0.37}^{+0.19}$ | 4.72 ${}_{-1.60}^{+1.82}$ | 0.94 ${}_{-0.70}^{+2.15}$ | 1.66
00076 | 1.83 ${}_{-0.54}^{+0.44}$ | 3.79 ${}_{-0.83}^{+1.68}$ | 3.67 ${}_{-2.99}^{+6.85}$ | 3.44
00117 | 2.34 ${}_{-0.40}^{+0.21}$ | 4.58 ${}_{-1.59}^{+2.1}$ | 0.87 ${}_{-0.73}^{+2.77}$ | 2.06
00121 | 1.96 ${}_{-0.43}^{+0.29}$ | 4.81 ${}_{-1.22}^{+1.55}$ | 1.96 ${}_{-1.11}^{+3.39}$ | 16.54
00122 | 2.33 ${}_{-0.23}^{+0.27}$ | 7.25 ${}_{-2.55}^{+1.83}$ | 8.24 ${}_{-7.33}^{+86.15}$ | 2.85
00145 | 1.80 ${}_{-0.31}^{+0.21}$ | 5.06 ${}_{-1.75}^{+1.82}$ | 0.97 ${}_{-0.69}^{+1.63}$ | 2.35
00148 | 1.32 ${}_{-0.16}^{+0.16}$ | 4.67 ${}_{-1.48}^{+1.61}$ | 2.04 ${}_{-1.65}^{+8.27}$ | 1.71
00153 | 1.84 ${}_{-0.35}^{+0.26}$ | 4.85 ${}_{-1.18}^{+1.51}$ | 1.83 ${}_{-1.06}^{+2.44}$ | 11.96
00176 | 1.95 ${}_{-0.22}^{+0.20}$ | 6.21 ${}_{-2.20}^{+1.35}$ | 2.09 ${}_{-1.40}^{+4.33}$ | 2.70
00200 | 1.89 ${}_{-0.33}^{+0.27}$ | 6.03 ${}_{-1.88}^{+2.09}$ | 5.19 ${}_{-3.85}^{+23.39}$ | 11.70
00204 | 1.45 ${}_{-0.30}^{+0.39}$ | 4.86 ${}_{-1.22}^{+1.85}$ | 5.46 ${}_{-3.21}^{+10.66}$ | 24.08
00216 | 1.40 ${}_{-0.28}^{+0.42}$ | 4.31 ${}_{-0.79}^{+1.15}$ | 5.08 ${}_{-2.87}^{+4.90}$ | 46.87
00223 | 1.31 ${}_{-0.21}^{+0.21}$ | 4.45 ${}_{-1.22}^{+1.62}$ | 3.21 ${}_{-2.39}^{+5.38}$ | 2.28
00237 | 1.62 ${}_{-0.19}^{+0.20}$ | 6.74 ${}_{-1.45}^{+1.10}$ | 3.74 ${}_{-1.84}^{+5.33}$ | 109.52
00238 | 1.93 ${}_{-0.43}^{+0.33}$ | 4.86 ${}_{-1.72}^{+2.24}$ | 4.21 ${}_{-3.89}^{+30.73}$ | 1.39
00288 | 1.84 ${}_{-0.25}^{+0.24}$ | 7.14 ${}_{-1.56}^{+1.00}$ | 5.98 ${}_{-3.01}^{+6.92}$ | 118.59
00340 | 1.47 ${}_{-0.34}^{+0.6}$ | 4.59 ${}_{-1.07}^{+2.09}$ | 14.10 ${}_{-10.92}^{+119.11}$ | 6.16
00358 | 1.76 ${}_{-0.26}^{+0.27}$ | 7.16 ${}_{-1.34}^{+1.24}$ | 10.51 ${}_{-5.91}^{+26.74}$ | 336.1
00426 | 1.28 ${}_{-0.18}^{+0.27}$ | 6.01 ${}_{-1.08}^{+1.82}$ | 13.67 ${}_{-8.19}^{+137.51}$ | 1152.91
00450 | 1.86 ${}_{-0.32}^{+0.27}$ | 5.27 ${}_{-2.07}^{+1.86}$ | 1.03 ${}_{-0.83}^{+1.96}$ | 1.61
00528 | 1.96 ${}_{-0.43}^{+0.33}$ | 4.98 ${}_{-1.69}^{+1.97}$ | 3.06 ${}_{-2.67}^{+11.30}$ | 1.98
00760 | 1.53 ${}_{-0.31}^{+0.31}$ | 6.48 ${}_{-1.86}^{+2.06}$ | 7.94 ${}_{-6.09}^{+173.10}$ | 6.35
00784 | 2.08 ${}_{-0.42}^{+0.39}$ | 6.20 ${}_{-2.22}^{+2.44}$ | 7.08 ${}_{-6.03}^{+105.53}$ | 3.49
01136 | 1.39 ${}_{-0.28}^{+0.39}$ | 5.17 ${}_{-1.62}^{+1.75}$ | 5.46 ${}_{-4.14}^{+23.77}$ | 2.85
01736 | 1.46 ${}_{-0.31}^{+0.39}$ | 6.56 ${}_{-1.55}^{+1.62}$ | 6.95 ${}_{-4.00}^{+14.30}$ | 23.66
03798 | 1.24 ${}_{-0.18}^{+0.31}$ | 6.42 ${}_{-2.28}^{+2.18}$ | 21.34 ${}_{-19.82}^{+586.14}$ | 1.70

Table 14: Summary of soft excess parameters for sources with significant soft
excesses which are best fit with the warm corona model as opposed to a blurred
reflection model. Column (1) gives the eROSITA ID, column (2) gives the hard
X-ray photon index, column (3) gives the soft X-ray photon index, column (4)
gives the warm corona temperature (kTe), and column (5) gives the Bayes factor
Kpl.

(1) | (2) | (3) | (4) | (5)
---|---|---|---|---
eROID | $\Gamma_{h}$ | $\Gamma_{s}$ | kTe | Kpl
00001 | 2.40 ${}_{-0.47}^{+0.26}$ | 3.04 ${}_{-0.30}^{+0.31}$ | 0.61 ${}_{-0.31}^{+0.27}$ | 1.48
00004 | 1.91 ${}_{-0.16}^{+0.13}$ | 3.26 ${}_{-0.28}^{+0.18}$ | 0.61 ${}_{-0.32}^{+0.27}$ | 8354.43
00007 | 1.92 ${}_{-0.18}^{+0.16}$ | 3.24 ${}_{-0.29}^{+0.19}$ | 0.45 ${}_{-0.28}^{+0.38}$ | 321.73
00011 | 2.01 ${}_{-0.63}^{+0.61}$ | 3.30 ${}_{-0.15}^{+0.13}$ | 0.71 ${}_{-0.26}^{+0.20}$ | 6.95$\times 10^{6}$
00029 | 2.29 ${}_{-0.37}^{+0.27}$ | 3.10 ${}_{-0.54}^{+0.29}$ | 0.61 ${}_{-0.37}^{+0.28}$ | 1.17
00034 | 1.67 ${}_{-0.25}^{+0.24}$ | 3.27 ${}_{-0.31}^{+0.17}$ | 0.55 ${}_{-0.36}^{+0.31}$ | 163.32
00038 | 1.61 ${}_{-0.33}^{+0.32}$ | 2.99 ${}_{-0.40}^{+0.34}$ | 0.59 ${}_{-0.30}^{+0.28}$ | 6.86
00039 | 1.83 ${}_{-0.41}^{+0.33}$ | 3.15 ${}_{-0.53}^{+0.27}$ | 0.18 ${}_{-0.05}^{+0.15}$ | 74560.61
00045 | 1.42 ${}_{-0.25}^{+0.30}$ | 3.22 ${}_{-0.28}^{+0.20}$ | 0.58 ${}_{-0.30}^{+0.29}$ | 1069.04
00054 | 1.67 ${}_{-0.33}^{+0.31}$ | 3.23 ${}_{-0.32}^{+0.19}$ | 0.45 ${}_{-0.30}^{+0.38}$ | 34.23
00076 | 1.58 ${}_{-0.39}^{+0.52}$ | 2.97 ${}_{-0.35}^{+0.34}$ | 0.61 ${}_{-0.31}^{+0.26}$ | 5.74
00121 | 1.64 ${}_{-0.36}^{+0.41}$ | 3.15 ${}_{-0.40}^{+0.25}$ | 0.51 ${}_{-0.32}^{+0.32}$ | 9.09
00153 | 1.59 ${}_{-0.29}^{+0.33}$ | 3.15 ${}_{-0.44}^{+0.25}$ | 0.48 ${}_{-0.31}^{+0.36}$ | 8.98
00200 | 1.66 ${}_{-0.33}^{+0.37}$ | 3.10 ${}_{-0.48}^{+0.29}$ | 0.45 ${}_{-0.30}^{+0.38}$ | 3.99
00216 | 1.3 ${}_{-0.22}^{+0.31}$ | 3.13 ${}_{-0.46}^{+0.26}$ | 0.33 ${}_{-0.17}^{+0.43}$ | 71.42
00237 | 1.44 ${}_{-0.25}^{+0.28}$ | 3.17 ${}_{-0.43}^{+0.25}$ | 0.41 ${}_{-0.26}^{+0.38}$ | 7.54
00288 | 1.56 ${}_{-0.32}^{+0.40}$ | 3.18 ${}_{-0.45}^{+0.23}$ | 0.4 ${}_{-0.27}^{+0.42}$ | 7.05
00340 | 1.35 ${}_{-0.25}^{+0.50}$ | 3.02 ${}_{-0.56}^{+0.34}$ | 0.31 ${}_{-0.14}^{+0.42}$ | 12.52
00358 | 1.55 ${}_{-0.29}^{+0.32}$ | 3.17 ${}_{-0.46}^{+0.24}$ | 0.19 ${}_{-0.08}^{+0.47}$ | 13.10
00426 | 1.21 ${}_{-0.15}^{+0.20}$ | 3.11 ${}_{-0.54}^{+0.3}$ | 0.14 ${}_{-0.03}^{+0.15}$ | 372.76
00784 | 2.03 ${}_{-0.60}^{+0.44}$ | 2.93 ${}_{-0.56}^{+0.41}$ | 0.55 ${}_{-0.34}^{+0.29}$ | 2.31
01136 | 1.33 ${}_{-0.25}^{+0.46}$ | 2.95 ${}_{-0.54}^{+0.39}$ | 0.47 ${}_{-0.27}^{+0.34}$ | 2.93
01736 | 1.35 ${}_{-0.26}^{+0.56}$ | 3.13 ${}_{-0.53}^{+0.28}$ | 0.35 ${}_{-0.22}^{+0.43}$ | 3.79

Table 15: Summary of blurred reflection parameters for all sources which are
best fit with blurred reflection. Column (1) gives the eROSITA ID, column (2)
gives the emissivity index, column (3) gives the disc inclination, column (4)
gives the photon index, column (5) gives the disc ionisation and column (6)
gives the reflection fraction.

(1) | (2) | (3) | (4) | (5) | (6) | (7)
---|---|---|---|---|---|---
eROID | Inner emissivity (q1) | Inclination (o) | $\Gamma_{rel}$ | log($\xi$) | log($R$) | Krel
00035 | 7.1 ${}_{-2.3}^{+2.0}$ | 36 ${}_{-18}^{+21}$ | 2.45 ${}_{-0.11}^{+0.10}$ | 1.8 ${}_{-1.2}^{+1.4}$ | 0.4 ${}_{-0.8}^{+0.5}$ | 2.73
00057 | 6.4 ${}_{-2.0}^{+2.4}$ | 39 ${}_{-19}^{+19}$ | 2.00 ${}_{-0.15}^{+0.13}$ | 1.8 ${}_{-1.0}^{+1.2}$ | 0.6 ${}_{-0.7}^{+0.3}$ | 3.53
00122 | 6.5 ${}_{-2.3}^{+2.3}$ | 41 ${}_{-20}^{+22}$ | 2.34 ${}_{-0.13}^{+0.13}$ | 2.0 ${}_{-1.3}^{+1.4}$ | 0.2 ${}_{-0.8}^{+0.5}$ | 1.13
00176 | 6.9 ${}_{-2.4}^{+2.1}$ | 39 ${}_{-20}^{+24}$ | 2.12 ${}_{-0.15}^{+0.15}$ | 2.0 ${}_{-1.3}^{+1.4}$ | 0.2 ${}_{-0.8}^{+0.6}$ | 1.56
00204 | 4.3 ${}_{-1.0}^{+2.6}$ | 43 ${}_{-21}^{+19}$ | 1.86 ${}_{-0.25}^{+0.22}$ | 2.0 ${}_{-0.9}^{+0.8}$ | 0.8 ${}_{-0.3}^{+0.1}$ | 27.36
00760 | 5.8 ${}_{-1.9}^{+2.7}$ | 40 ${}_{-21}^{+22}$ | 1.75 ${}_{-0.37}^{+0.26}$ | 2.4 ${}_{-1.5}^{+0.8}$ | 0.4 ${}_{-0.8}^{+0.4}$ | 3.14