2022A&A...661A...3S


Query : 2022A&A...661A...3S

2022A&A...661A...3S - Astronomy and Astrophysics, volume 661A, 3-3 (2022/5-1)

The eROSITA Final Equatorial-Depth Survey (eFEDS). Identification and characterization of the counterparts to point-like sources.

SALVATO M., WOLF J., DWELLY T., GEORGAKAKIS A., BRUSA M., MERLONI A., LIU T., TOBA Y., NANDRA K., LAMER G., BUCHNER J., SCHNEIDER C., FREUND S., RAU A., SCHWOPE A., NISHIZAWA A., KLEIN M., ARCODIA R., COMPARAT J., MUSIIMENTA B., NAGAO T., BRUNNER H., MALYALI A., FINOGUENOV A., ANDERSON S., SHEN Y., IBARRA-MEDEL H., TRUMP J., BRANDT W.N., URRY C.M., RIVERA C., KRUMPE M., URRUTIA T., MIYAJI T., ICHIKAWA K., SCHNEIDER D.P., FRESCO A., BOLLER T., HAASE J., BROWNSTEIN J., LANE R.R., BIZYAEV D. and NITSCHELM C.

Abstract (from CDS):


Context. In November 2019, eROSITA on board of the Spektrum-Roentgen-Gamma (SRG) observatory started to map the entire sky in X-rays. After the four-year survey program, it will reach a flux limit that is about 25 times deeper than ROSAT. During the SRG performance verification phase, eROSITA observed a contiguous 140 deg2 area of the sky down to the final depth of the eROSITA all-sky survey (eROSITA Final Equatorial-Depth Survey; eFEDS), with the goal of obtaining a census of the X-ray emitting populations (stars, compact objects, galaxies, clusters of galaxies, and active galactic nuclei) that will be discovered over the entire sky.
Aims. This paper presents the identification of the counterparts to the point sources detected in eFEDS in the main and hard samples and their multi-wavelength properties, including redshift.
Methods. To identifyy the counterparts, we combined the results from two independent methods (NWAY andASTROMATCH), trained on the multi-wavelength properties of a sample of 23k XMM-Newton sources detected in the DESI Legacy Imaging Survey DR8. Then spectroscopic redshifts and photometry from ancillary surveys were collated to compute photometric redshifts.
Results. Of the eFEDS sources, 24 774 of 27 369 have reliable counterparts (90.5%) in the main sample and 231 of 246 sourcess (93.9%) have counterparts in the hard sample, including 2514 (3) sources for which a second counterpart is equally likely. By means of reliable spectra, Gaia parallaxes, and/or multi-wavelength properties, we have classified the reliable counterparts in both samples into Galactic (2695) and extragalactic sources (22 079). For about 340 of the extragalactic sources, we cannot rule out the possibility that they are unresolved clusters or belong to clusters. Inspection of the distributions of the X-ray sources in various optical/IR colour-magnitude spaces reveal a rich variety of diverse classes of objects. The photometric redshifts are most reliable within the KiDS/VIKING area, where deep near-infrared data are also available.
Conclusions. This paper accompanies the eROSITA early data release of all the observations performed during the performance and verification phase. Together with the catalogues of primary and secondary counterparts to the main and hard samples of the eFEDS survey, this paper releases their multi-wavelength properties and redshifts.

Abstract Copyright: © M. Salvato et al. 2022

Journal keyword(s): methods: data analysis - X-rays: general - catalogs - surveys - galaxies: active - galaxies: distances and redshifts

VizieR on-line data: <Available at CDS (J/A+A/661/A3): ctpmain.dat ctp2.dat ctphard.dat fits/*>

Status at CDS : Tables of objects will be appraised for possible ingestion in SIMBAD.

Simbad objects: 21

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Number of rows : 21
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 LEDA 1790 Sy1 00 29 13.7012449608 +13 16 03.947778264   15.70 15.41     ~ 417 0
2 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 11880 1
3 Mrk 1502 Sy1 00 53 34.9331107632 +12 41 35.929269132   14.41 14.03     ~ 1103 1
4 ESO 113-45 Sy1 01 23 45.7631533440 -58 48 20.808928944   14.08 13.83 13.34   ~ 820 0
5 NGC 863 Sy1 02 14 33.5604714720 -00 46 00.181845336   14.48 13.81 17.9   ~ 640 0
6 Mrk 1506 Sy1 04 33 11.0956735296 +05 21 15.619461552   15.72 15.05 10.08   ~ 1927 2
7 Ton 951 Sy1 08 47 42.4485615096 +34 45 04.482515304   14.83 14.50     ~ 444 0
8 Mrk 110 Sy1 09 25 12.8479065576 +52 17 10.386311208   16.82 16.41     ~ 552 0
9 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5616 6
10 NGC 4151 Sy1 12 10 32.5759813872 +39 24 21.063527532   12.18 11.48     ~ 3530 2
11 Mrk 231 Sy1 12 56 14.2341182928 +56 52 25.238373852   14.68 13.84     ~ 1906 3
12 2MASS J13000535+1632148 Sy1 13 00 05.3479083912 +16 32 14.758987848   17.1 17.10     ~ 46 0
13 ICRF J134733.3+121724 Sy2 13 47 33.3634536792 +12 17 24.214209216   19.28 18.44 15.718   ~ 556 3
14 LEDA 51016 Sy1 14 17 00.8224797456 +44 56 06.336360024   16.93 16.63     ~ 237 0
15 Mrk 817 Sy1 14 36 22.0820611632 +58 47 39.394934844   14.19 13.79     ~ 463 0
16 NGC 5728 Sy2 14 42 23.8918506576 -17 15 11.240783784   14.34 13.40     ~ 550 0
17 Mrk 290 Sy1 15 35 52.4031021552 +57 54 09.515660508   15.55 15.27     ~ 484 0
18 Mrk 493 Sy1 15 59 09.6231720696 +35 01 47.561352852   15.69 15.06     ~ 293 0
19 7C 1821+6419 Sy1 18 21 57.2130271440 +64 20 36.221312076   14.23 14.24     ~ 569 1
20 UGC 12163 Sy1 22 42 39.3363009144 +29 43 31.302092640   14.86 14.16     ~ 662 1
21 NGC 7469 Sy1 23 03 15.674 +08 52 25.28 12.60 13.00 12.34     ~ 1998 3

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2022.08.09-15:32:45

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