J/A+A/702/A67 eROSITA-selected SDSS-V Galaxies (Pulatova+, 2025)
Optical emission-line properties of eROSITA-selected SDSS-V galaxies.
Pulatova N.G., Rubtsov E., Chilingarian I.V., Rix H.-W., Demianenko M.,
Grishin K.A., Katkov I.Yu., Schneider D.P., Aydar C., Buchner J.,
Salvato M., Merloni A., Koekemoer A.M., Assef R.J., Ricci C., Wylezalek D.,
Gasymov D., Brandt W.N., Negrete Penaloza C.A., Morrison S., Anderson S.F.,
Bauer F.E., Ibarra-Medel H.J., Wu Q.
<Astron. Astrophys. 702, A67 (2025)>
=2025A&A...702A..67P 2025A&A...702A..67P (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs ; Galaxies, optical ; QSOs ; Galaxies, Seyfert ;
X-ray sources
Keywords: line: profiles - methods: data analysis - techniques: spectroscopic -
galaxies: nuclei
Abstract:
We present and discuss optical emission line properties obtained from
the analysis of Sloan Digital Sky Survey (SDSS) spectra for an X-ray
selected sample of 3684 galaxies (0.002<z<0.55), drawn from the
eRASS1 catalog. We modeled SDSS-V DR19 spectra using the NBursts full
spectrum fitting technique with E-MILES simple stellar populations
(SSP) models and emission line templates to decompose broad and narrow
emission line components for correlation with X-ray properties. We
place the galaxies on the Baldwin-Phillips-Terlevich (BPT) diagram to
diagnose their dominant excitation mechanism. We show that the
consistent use of the narrow component fluxes shifts most galaxies
systematically and significantly upward to the active galactic nuclei
(AGN) region on the BPT diagram. On this basis, we confirm the
dependence between a galaxy's position on the BPT diagram and its
(0.2-2.3keV) X-ray/H_alpha flux ratio. We also verified the
correlation between X-ray luminosity and emission line luminosities of
the narrow [OIII]5007 and broad Hα component; as well as the
relations between the Supermassive Black Hole (SMBH) mass, the X-ray
luminosity, and the velocity dispersion of the stellar component
(sigma*) on the base on the unique sample of optical spectroscopic
follow-up of X-ray sources detected by eROSITA. These results
highlight the importance of emission line decomposition in AGN
classification and refines the connection between X-ray emission and
optical emission line properties in galaxies.
Description:
This catalog presents the final fitting results for 7546 optical
spectra of 3684 sources from the SDSS-V DR19 eROSITA eRASS1 X-ray
selected galaxies sample in the 0.002<z<0.55 range. The table
contains lists of the main emission lines in the rest frame wavelength
range 3700 -- 7000 Angstrom from [OII] 3727 to [SII] 6731 --- 28
lines for the narrow component and 6 lines of the Balmer series (from
H8 to H-alpha) for the broad component. For them, fluxes, flux
uncertainties, and the continuum level at the mean emission line
wavelength are obtained. It also contains estimates of the kinematic
parameters for all components (SSP, NLR, BLR), stellar population
properties from E-MILES models, and X-ray information from the eRASS1
catalog.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 2249 7546 Results of spectra fitting (table A1)
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See also:
J/A+A/682/A34 : SRG/eROSITA all-sky survey catalogs (eRASS1) (Merloni+, 2024)
Byte-by-byte Description of file: catalog.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 I6 --- PlateId SDSS-V plate ID (PLATEID)
8- 12 I5 d MJD Modified Julian Date (MJD)
14- 30 I17 --- CatId SDSS-V catalog ID (CATALOGID)
32- 40 I9 --- SDSS Unique photometric ID in the SDSS
(SDSSID)
42- 70 A29 --- SpecObjID Unique spectrum ID in the SDSS
(SPECOBJID)
72- 94 A23 --- eRASS1 IAU name of the eRASS1 source,
1eRASS JHHMMSS.s+DDMMSS (ERASS1)
96- 110 F15.11 deg RAdeg Right ascension (ICRS) from SDSS-V
(RA)
112- 126 F15.11 deg DEdeg Declination (ICRS) from SDSS-V
(DEC)
128- 142 F15.11 deg RAXdeg Right ascension (ICRS) from eRASS1
(XRA)
144- 158 F15.11 deg DEXdeg Declination (ICRS) from eRASS1
(XDEC)
160- 177 F18.15 arcsec Dist Distance between SDSS-V and eRASS1
(DISTANCE)
179- 196 F18.15 --- z Redshift (Z) (1)
198- 215 F18.15 --- e_z [] Redshift uncertainty (Z_E)
217- 219 I3 --- q_z Redshift flag (SDSS-V: ZWARNING)
(Z_Q)
221- 222 I2 --- qual [-1/2] Quality flag (QUALITY) (2)
224- 226 F3.1 mag umag ?=- SDSS u magnitude (MAG_U)
(always empty)
228- 234 F7.4 mag gmag ?=- SDSS g magnitude (MAG_G)
236- 242 F7.4 mag rmag ?=- SDSS r magnitude (MAG_R)
244- 250 F7.4 mag imag ?=- SDSS i magnitude (MAG_I)
252- 258 F7.4 mag zmag ?=- SDSS z magnitude (MAG_Z)
260- 262 F3.1 mag e_umag ?=- Uncertainty in SDSS u (ERR_U)
(always empty)
264- 266 F3.1 mag e_gmag ?=- Uncertainty in SDSS g (ERR_G)
(always empty)
268- 270 F3.1 mag e_rmag ?=- Uncertainty in SDSS r (ERR_R)
(always empty)
272- 274 F3.1 mag e_imag ?=- Uncertainty in SDSS i (ERR_I)
(always empty)
276- 278 F3.1 mag e_zmag ?=- Uncertainty in SDSS z (ERR_Z)
(always empty)
280- 288 F9.6 --- SNR-Flux ?=- Source median SNR (SNR_FLUX)
290- 298 F9.6 --- SNR-Fit ?=- Best-fit median SNR (SNR_FIT)
300- 308 F9.6 --- SNR-Grid ?=- SSP median SNR (SNR_GRID)
310- 312 F3.1 --- SNR-Cont ?=- Continuum median SNR (SNR_CONT)
314- 323 F10.6 --- chi2r Reduces chi2 statistics (CHISQR)
325- 328 I4 --- DOF Degree of freedom (DOF)
330- 340 F11.4 km/s RV-SSP Radial velocity of the SSP
(VEL_SSP) (3)
342- 351 F10.3 km/s RV-NLR Radial velocity of the NLR
(VEL_NLR)
353- 362 F10.3 km/s RV-BLR Radial velocity of the BLR
(VEL_BLR)
364- 372 F9.4 km/s sigma-SSP Velocity dispersion of the SSP
(SIG_SSP)
374- 382 F9.4 km/s sigma-NLR Velocity dispersion of the NLR
(SIG_NLR)
384- 393 F10.4 km/s sigma-BLR Velocity dispersion of the BLR
(SIG_BLR)
395- 402 F8.6 --- h3-SSP Gauss-Hermite h3 from SSP (H3_SSP)
404- 412 F9.6 --- h3-NLR Gauss-Hermite h3 from NLR (H3_NLR)
414- 421 F8.6 --- h3-BLR Gauss-Hermite h3 from BLR (H3_BLR)
423- 430 F8.6 --- h4-SSP Gauss-Hermite h4 from SSP (H4_SSP)
432- 440 F9.6 --- h4-NLR Gauss-Hermite h4 from NLR (H4_NLR)
442- 450 F9.6 --- h4-BLR Gauss-Hermite h4 from BLR (H4_BLR)
452- 461 F10.4 Myr Age Age of SSP model (AGE) (4)
463- 471 F9.6 [-] Met Metallicity of SSP model (MET)
473- 484 E12.6 km/s e_RV-SSP Uncertainty in RV-SSP (EVELSSP)
486- 495 F10.6 km/s e_RV-NLR Uncertainty in RV-NLR (EVELNLR)
497- 508 E12.6 km/s e_RV-BLR Uncertainty in RV-BLR (EVELBLR)
510- 521 E12.6 km/s e_sigma-SSP Uncertainty in sigmaSSP (ESIGSSP)
523- 532 F10.6 km/s e_sigma-NLR Uncertainty in sigmaNLR (ESIGNLR)
534- 545 E12.6 km/s e_sigma-BLR Uncertainty in sigmaBLR (ESIGBLR)
547- 549 F3.1 --- e_h3-SSP Uncertainty in h3_SSP (EH3SSP)
551- 558 F8.6 --- e_h3-NLR Uncertainty in h3-NLR (EH3NLR)
560- 567 F8.6 --- e_h3-BLR Uncertainty in h3-BLR (EH3BLR)
569- 576 F8.6 --- e_h4-SSP Uncertainty in h4_SSP (EH4SSP)
578- 585 F8.6 --- e_h4-NLR Uncertainty in h4-NLR (EH4NLR)
587- 598 E12.6 --- e_h4-BLR Uncertainty in h4-BLR (EH4BLR)
600- 611 E12.6 Myr e_Age Uncertainty in Age (E_AGE)
613- 624 E12.6 [-] e_Met Uncertainty in Met (E_MET)
626- 633 F8.6 mag E(B-V) Intrinsic E(B-V) (EBV) (5)
635- 637 F3.1 mag e_E(B-V) ?=- Uncertainty of intrinsic E(B-V)
(E_EBV)
639- 650 E12.6 Msun MBH ?=- Black hole mass (Reines2013)
(MBH) (5)
652- 663 E12.6 Msun e_MBH ?=- Black hole mass uncertainty
(E_MBH) (6)
665- 676 E12.6 mW/m2 FOII3727NLR ?=- OII3727 narrow line flux
(FOII3727NLR) (7)
678- 689 E12.6 mW/m2 FOII3729NLR ?=- OII3729 narrow line flux
(FOII3729NLR)
691- 702 E12.6 mW/m2 FNeIII3869NLR ?=- NeIII3869 narrow line flux
(FNEIII3869NLR)
704- 715 E12.6 mW/m2 FH83890NLR ?=- H83890 narrow line flux
(FH83890NLR)
717- 728 E12.6 mW/m2 FHeI3965NLR ?=- HeI3965 narrow line flux
(FHEI3965NLR)
730- 741 E12.6 mW/m2 FNeIII3968NLR ?=- NeIII3968 narrow line flux
(FNEIII3968NLR)
743- 754 E12.6 mW/m2 FHepsilonNLR ?=- Hepsilon narrow line flux
(FHEPSILONNLR)
756- 767 E12.6 mW/m2 FHdeltaNLR ?=- Hdelta narrow line flux
(Fdelta_NLR)
769- 780 E12.6 mW/m2 FHgammaNLR ?=- Hgamma narrow line flux
(FHGAMMANLR)
782- 793 E12.6 mW/m2 FOIII4364NLR ?=- OIII4364 narrow line flux
(FOIII4364NLR)
795- 806 E12.6 mW/m2 FHeI4389NLR ?=- HeI4389 narrow line flux
(FHEI4389NLR)
808- 819 E12.6 mW/m2 FOII4652NLR ?=- OII4652 narrow line flux
(FOII4652NLR)
821- 832 E12.6 mW/m2 FHeII4687NLR ?=- HeII4687 narrow line flux
(FHEII4687NLR)
834- 845 E12.6 mW/m2 FHeI4714NLR ?=- HeI4714 narrow line flux
(FHEI4714NLR)
847- 858 E12.6 mW/m2 FHbetaNLR ?=- Hbeta narrow line flux
(FHBETANLR)
860- 871 E12.6 mW/m2 FHeI4923NLR ?=- HeI4923 narrow line flux
(FHEI4923NLR)
873- 884 E12.6 mW/m2 FOIII4960NLR ?=- OIII4960 narrow line flux
(FOIII4960NLR)
886- 897 E12.6 mW/m2 FOIII5008NLR ?=- OIII5008 narrow line flux
(FOIII5008NLR)
899- 910 E12.6 mW/m2 FHeI5017NLR ?=- HeI5017 narrow line flux
(FHEI5017NLR)
912- 923 E12.6 mW/m2 FHeI5877NLR ?=- HeI5877 narrow line flux
(FHEI5877NLR)
925- 936 E12.6 mW/m2 FOI6302NLR ?=- OI6302 narrow line flux
(FOI6302NLR)
938- 949 E12.6 mW/m2 FOI6365NLR ?=- OI6365 narrow line flux
(FOI6365NLR)
951- 962 E12.6 mW/m2 FNII6549NLR ?=- NII6549 narrow line flux
(FNII6549NLR)
964- 975 E12.6 mW/m2 FHalphaNLR ?=- Halpha narrow line flux
(FHALPHANLR)
977- 988 E12.6 mW/m2 FNII6585NLR ?=- NII6585 narrow line flux
(FNII6585NLR)
990-1001 E12.6 mW/m2 FHeI6680NLR ?=- HeI6680 narrow line flux
(FHEI6680NLR)
1003-1014 E12.6 mW/m2 FSII6718NLR ?=- SII6718 narrow line flux
(FSII6718NLR)
1016-1027 E12.6 mW/m2 FSII6732NLR ?=- SII6732 narrow line flux
(FSII6732NLR)
1029-1040 E12.6 mW/m2 FH83890BLR ?=- H83890 broad line flux
(FH83890BLR)
1042-1053 E12.6 mW/m2 FHepsilonBLR ?=- Hepsilon broad line flux
(FHEPSILONBLR)
1055-1066 E12.6 mW/m2 FHdeltaBLR ?=- Hdelta broad line flux
(Fdelta_BLR)
1068-1079 E12.6 mW/m2 FHgammaBLR ?=- Hgamma broad line flux
(FHGAMMABLR)
1081-1092 E12.6 mW/m2 FHbetaBLR ?=- Hbeta broad line flux
(FHBETABLR)
1094-1105 E12.6 mW/m2 FHalphaBLR ?=- Halpha broad line flux
(FHALPHABLR)
1107-1118 E12.6 mW/m2 e_FOII3727NLR ?=- Uncertainty in FOII3727NLR
(EOII3727NLR)
1120-1131 E12.6 mW/m2 e_FOII3729NLR ?=- Uncertainty in FOII3729NLR
(EOII3729NLR)
1133-1144 E12.6 mW/m2 e_FNeIII3869NLR ?=- Uncertainty in FNEIII3869NLR
(ENEIII3869NLR)
1146-1157 E12.6 mW/m2 e_FH83890NLR ?=- Uncertainty in FH83890NLR
(EH83890NLR)
1159-1170 E12.6 mW/m2 e_FHeI3965NLR ?=- Uncertainty in FHeI3965NLR
(EHEI3965NLR)
1172-1183 E12.6 mW/m2 e_FNeIII3968NLR ?=- Uncertainty in FNEIII3968NLR
(ENEIII3968NLR)
1185-1196 E12.6 mW/m2 e_FHepsilonNLR ?=- Uncertainty in FHePSILONNLR
(EHEPSILONNLR)
1198-1209 E12.6 mW/m2 e_FHdeltaNLR ?=- Uncertainty in FdeltaNLR
(EHDELTANLR)
1211-1222 E12.6 mW/m2 e_FHgammaNLR ?=- Uncertainty in FgammaNLR
(EHGAMMANLR)
1224-1235 E12.6 mW/m2 e_FOIII4364NLR ?=- Uncertainty in FOIII4364NLR
(EOIII4364NLR)
1237-1248 E12.6 mW/m2 e_FHeI4389NLR ?=- Uncertainty in FHeI4389NLR
(EHEI4389NLR)
1250-1261 E12.6 mW/m2 e_FOII4652NLR ?=- Uncertainty in FOII4652NLR
(EOII4652NLR)
1263-1274 E12.6 mW/m2 e_FHeII4687NLR ?=- Uncertainty in FHeII4687NLR
(EHEII4687NLR)
1276-1287 E12.6 mW/m2 e_FHeI4714NLR ?=- Uncertainty in FHeI4714NLR
(EHEI4714NLR)
1289-1300 E12.6 mW/m2 e_FHbetaNLR ?=- Uncertainty in FHbetaNLR
(EHBETANLR)
1302-1313 E12.6 mW/m2 e_FHeI4923NLR ?=- Uncertainty in FHeI4923NLR
(EHEI4923NLR)
1315-1326 E12.6 mW/m2 e_FOIII4960NLR ?=- Uncertainty in FOIII4960NLR
(EOIII4960NLR)
1328-1339 E12.6 mW/m2 e_FOIII5008NLR ?=- Uncertainty in FOIII5008NLR
(EOIII5008NLR)
1341-1352 E12.6 mW/m2 e_FHeI5017NLR ?=- Uncertainty in FHeI5017NLR
(EHEI5017NLR)
1354-1365 E12.6 mW/m2 e_FHeI5877NLR ?=- Uncertainty in FHeI5877NLR
(EHEI5877NLR)
1367-1378 E12.6 mW/m2 e_FOI6302NLR ?=- Uncertainty in FOI6302NLR
(EOI6302NLR)
1380-1391 E12.6 mW/m2 e_FOI6365NLR ?=- Uncertainty in FOI6365NLR
(EOI6365NLR)
1393-1404 E12.6 mW/m2 e_FNII6549NLR ?=- Uncertainty in FNII6549NLR
(ENII6549NLR)
1406-1417 E12.6 mW/m2 e_FHalphaNLR ?=- Uncertainty in FHalphaNLR
(EHALPHANLR)
1419-1430 E12.6 mW/m2 e_FNII6585NLR ?=- Uncertainty in FNII6585NLR
(ENII6585NLR)
1432-1443 E12.6 mW/m2 e_FHeI6680NLR ?=- Uncertainty in FHeI6680NLR
(EHEI6680NLR)
1445-1456 E12.6 mW/m2 e_FSII6718NLR ?=- Uncertainty in FSII6718NLR
(ESII6718NLR)
1458-1469 E12.6 mW/m2 e_FSII6732NLR ?=- Uncertainty in FSII6732NLR
(ESII6732NLR)
1471-1482 E12.6 mW/m2 e_FH83890BLR ?=- Uncertainty in FH83890BLR
(EH83890BLR)
1484-1495 E12.6 mW/m2 e_FHepsilonBLR ?=- Uncertainty in FHePSILONBLR
(EHEPSILONBLR)
1497-1508 E12.6 mW/m2 e_FHdeltaBLR ?=- Uncertainty in FdeltaBLR
(EHDELTABLR)
1510-1521 E12.6 mW/m2 e_FHgammaBLR ?=- Uncertainty in FgammaBLR
(EHGAMMABLR)
1523-1534 E12.6 mW/m2 e_FHbetaBLR ?=- Uncertainty in FHbetaBLR
(EHBETABLR)
1536-1547 E12.6 mW/m2 e_FHalphaBLR ?=- Uncertainty in FHalphaBLR
(EHALPHABLR)
1549-1560 E12.6 10mW/m2/nm COII3727NLR ?=- Continuum level at OII3727
(COII3727NLR)
1562-1573 E12.6 10mW/m2/nm COII3729NLR ?=- Continuum level at OII3729
(COII3729NLR)
1575-1586 E12.6 10mW/m2/nm CNeIII3869NLR ?=- Continuum level at NeIII3869
(CNEIII3869NLR)
1588-1599 E12.6 10mW/m2/nm CH83890NLR ?=- Continuum level at H83890
(CH83890NLR)
1601-1612 E12.6 10mW/m2/nm CHeI3965NLR ?=- Continuum level at HeI3965
(CHEI3965NLR)
1614-1625 E12.6 10mW/m2/nm CNeIII3968NLR ?=- Continuum level at NeIII3968
(CNEIII3968NLR)
1627-1638 E12.6 10mW/m2/nm CHepsilonNLR ?=- Continuum level at Hepsilon
(CHEPSILONNLR)
1640-1651 E12.6 10mW/m2/nm CHdeltaNLR ?=- Continuum level at Hdelta
(CHDELTANLR)
1653-1664 E12.6 10mW/m2/nm CHgammaNLR ?=- Continuum level at Hgamma
(CHGAMMANLR)
1666-1677 E12.6 10mW/m2/nm COIII4364NLR ?=- Continuum level at OIII4364
(COIII4364NLR)
1679-1690 E12.6 10mW/m2/nm CHeI4389NLR ?=- Continuum level at HeI4389
(CHEI4389NLR)
1692-1703 E12.6 10mW/m2/nm COII4652NLR ?=- Continuum level at OII4652
(COII4652NLR)
1705-1716 E12.6 10mW/m2/nm CHeII4687NLR ?=- Continuum level at HeII4687
(CHEII4687NLR)
1718-1729 E12.6 10mW/m2/nm CHeI4714NLR ?=- Continuum level at HeI4714
(CHEI4714NLR)
1731-1742 E12.6 10mW/m2/nm CHbetaNLR ?=- Continuum level at Hbeta
(CHBETANLR)
1744-1755 E12.6 10mW/m2/nm CHeI4923NLR ?=- Continuum level at HeI4923
(CHEI4923NLR)
1757-1768 E12.6 10mW/m2/nm COIII4960NLR ?=- Continuum level at OIII4960
(COIII4960NLR)
1770-1781 E12.6 10mW/m2/nm COIII5008NLR ?=- Continuum level at OIII5008
(COIII5008NLR)
1783-1794 E12.6 10mW/m2/nm CHeI5017NLR ?=- Continuum level at HeI5017
(CHEI5017NLR)
1796-1807 E12.6 10mW/m2/nm CHeI5877NLR ?=- Continuum level at HEI5877
(CHEI5877NLR)
1809-1820 E12.6 10mW/m2/nm COI6302NLR ?=- Continuum level at OI6302
(COI6302NLR)
1822-1833 E12.6 10mW/m2/nm COI6365NLR ?=- Continuum level at OI6365
(COI6365NLR)
1835-1846 E12.6 10mW/m2/nm CNII6549NLR ?=- Continuum level at NII6549
(CNII6549NLR)
1848-1859 E12.6 10mW/m2/nm CHalphaNLR ?=- Continuum level at Halpha
(CHALPHANLR)
1861-1872 E12.6 10mW/m2/nm CNII6585NLR ?=- Continuum level at NII6585
(CNII6585NLR)
1874-1885 E12.6 10mW/m2/nm CHeI6680NLR ?=- Continuum level at HEI6680
(CHEI6680NLR)
1887-1898 E12.6 10mW/m2/nm CSII6718NLR ?=- Continuum level at SII6718
(CSII6718NLR)
1900-1911 E12.6 10mW/m2/nm CSII6732NLR ?=- Continuum level at SII6732
(CSII6732NLR)
1913-1924 E12.6 10mW/m2/nm CH83890BLR ?=- Continuum level at H83890
(CH83890BLR)
1926-1937 E12.6 10mW/m2/nm CHepsilonBLR ?=- Continuum level at Hepsilon
(CHEPSILONBLR)
1939-1950 E12.6 10mW/m2/nm CHdeltaBLR ?=- Continuum level at Hdelta
(CHDELTABLR)
1952-1963 E12.6 10mW/m2/nm CHgammaBLR ?=- Continuum level at Hgamma
(CHGAMMABLR)
1965-1976 E12.6 10mW/m2/nm CHbetaBLR ?=- Continuum level at Hbeta
(CHBETABLR)
1978-1989 E12.6 10mW/m2/nm CHalphaBLR ?=- Continuum level at Halpha
(CHALPHABLR)
1991-2002 E12.6 mW/m2 MLFlux1 Flux at eRASS1 1 [0.2-2.3keV]
(MLFLUX1) (8)
2004-2015 E12.6 mW/m2 MLFluxP1 ?=- Flux at eRASS1 P1 [0.2-0.5keV]
(MLFLUXP1)
2017-2028 E12.6 mW/m2 MLFluxP2 ?=- Flux at eRASS1 P2 [0.5-1.0keV]
(MLFLUXP2)
2030-2041 E12.6 mW/m2 MLFluxP3 ?=- Flux at eRASS1 P3 [1.0-2.0keV]
(MLFLUXP3)
2043-2054 E12.6 mW/m2 MLFluxP4 ?=- Flux at eRASS1 P4 [2.0-5.0keV]
(MLFLUXP4)
2056-2067 E12.6 mW/m2 MLFluxP5 ?=- Flux at eRASS1 P5 [5.0-8.0keV]
(MLFLUXP5)
2069-2080 E12.6 mW/m2 MLFluxP6 ?=- Flux at eRASS1 P6 [4.0-10.0keV]
(MLFLUXP6)
2082-2093 E12.6 mW/m2 MLFluxP7 ?=- Flux at eRASS1 P7 [5.1-6.1keV]
(MLFLUXP7)
2095-2106 E12.6 mW/m2 MLFluxP8 ?=- Flux at eRASS1 P8 [6.2-7.1keV]
(MLFLUXP8)
2108-2119 E12.6 mW/m2 MLFluxP9 ?=- Flux at eRASS1 P9 [7.2-8.2keV]
(MLFLUXP9)
2121-2132 E12.6 mW/m2 e_MLFlux1 ?=- Flux uncertainty at 1
[0.2-2.3keV] (MLFLUXERR_1)
2134-2145 E12.6 mW/m2 e_MLFluxP1 Flux uncertainty at P1 [0.2-0.5keV]
(MLFLUXERR_P1)
2147-2158 E12.6 mW/m2 e_MLFluxP2 Flux uncertainty at P2 [0.5-1.0keV]
(MLFLUXERR_P2)
2160-2171 E12.6 mW/m2 e_MLFluxP3 Flux uncertainty at P3 [1.0-2.0keV]
(MLFLUXERR_P3)
2173-2184 E12.6 mW/m2 e_MLFluxP4 Flux uncertainty at P4 [2.0-5.0keV]
(MLFLUXERR_P4)
2186-2197 E12.6 mW/m2 e_MLFluxP5 Flux uncertainty at P5 [5.0-8.0keV]
(MLFLUXERR_P5)
2199-2210 E12.6 mW/m2 e_MLFluxP6 Flux uncertainty at P6
[4.0-10.0keV] (MLFLUXERR_P6)
2212-2223 E12.6 mW/m2 e_MLFluxP7 Flux uncertainty at P7 [5.1-6.1keV]
(MLFLUXERR_P7)
2225-2236 E12.6 mW/m2 e_MLFluxP8 Flux uncertainty at P8 [6.2-7.1keV]
(MLFLUXERR_P8)
2238-2249 E12.6 mW/m2 e_MLFluxP9 Flux uncertainty at P9 [7.2-8.2keV]
(MLFLUXERR_P9)
--------------------------------------------------------------------------------
Note (1): The redshift values determined in SDSS-V/eRASS1 (z, e_z, q_z) may
differ greatly from the radial velocity values from the spectral fits. We
recommend using the value from VEL_NLR as the most probable cz for the sources.
Note (2): Quality flag values as follows:
0 = is a subsample with reliable detection of a narrow component
comprising at least 3 forbidden unblended emission lines with SNR>3
(e.g. [OIII], [OII], etc.) and fulfilling the kinematic constraints:
50 < sigmanarrow< 1000km/s and esigmanarrow_ < 300km/s
1 = is a subsample of (Qual = 0) for BPT diagram classification with
additional conditions of SNR>3 in each of the following lines:
H-alpha, H-beta, [NII] 6548,84, [OIII] 5007
2 = is a subsample of (Qual = 1) with reliable detection of a broad component:
SNRHalphabroad_> 3 and sigmabroad > 1.5 sigmanarrow,
300< sigmabroad < 5000km/s, esigmabroad_ < 300km/s
-1 = for all other spectra that do not fall into any of the above categories
are marked as unreliable
Note (3): The line-of-sight velocity distribution (LOSVD) for each kinematical
component (SSP, NLR, BLR) are described normalized physical Gauss--Hermite
polynomials 4th degree (SSP: h3=h4=0; BLR: h3=0);
Note (4): The stellar components of galaxies are fitted by the SSP E-MILES
models (2016MNRAS.463.3409V 2016MNRAS.463.3409V). However, for sources with a strong AGN
continuum, the obtained values of the properties of stellar populations
maybe unreliable, see SNR_GRID.
Note (5): The intrinsic absorption E(B-V) is determined by the Balmer
decrement (H-alpha/H-beta) in narrow lines.
Note (6): We estimated a single-epoch black hole masses (MBH) using the virial
approximation applied to the broad H-alpha emission line (2013ApJ...775..116R 2013ApJ...775..116R).
Note (7): The emission line fluxes and the flux density at the continuum level
a represented in units of erg/s/cm2 and erg/s/cm2/Angstrom, respectively.
Emission line identifiers are taken from the SDSS project with vacuum
wavelengths in restframe.
Note (8): Optical photometry and X-ray filter fluxes are taken from SDSS-V DR19
and eROSITA eRASS1 catalogues respectively without changes.
--------------------------------------------------------------------------------
Acknowledgements:
Evgenii Nubtsov, evgenii.rubtsov(at)voxastro.org
(End) Patricia Vannier [CDS] 28-Jul-2025