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ERASS1MAIN - eROSITA All-Sky Survey (First 6 Months; eRASS1) X-Ray (0.2-2.3 keV) Source Catalog

 HEASARC
Archive

Overview

The eROSITA telescope array aboard the Spektrum Roentgen Gamma (SRG) satellite began surveying the sky in December 2019, with the aim of producing all-sky X-ray source lists and sky maps of an unprecedented depth. The authors present catalogs of both point-like and extended sources using the data acquired in the first six months of survey operations (eRASS1; completed June 2020) over the half sky whose proprietary data rights lie with the German eROSITA Consortium.

With nearly 930000 entries detected in the most sensitive 0.2-2.3keV energy range, the eRASS1 main catalog increases the number of known X-ray sources in the published literature by more than 60%, and provides a comprehensive inventory of all classes of X-ray celestial objects, covering a wide range of physical processes.

A smaller catalog, eRASS1HARD, contains all X-ray sources detected in the 2.3-5 keV band with detection likelihood DET_LIKE > 12. The 5466 sources detected in the less sensitive but harder 2.3-5keV band is the result of the first true imaging survey of the entire sky above 2keV. The sources in the hard catalog (only the strongly associated ones) have been linked to eRASS1HARD in this catalog.

The reference paper presents methods to identify and flag potential spurious sources in the catalogs, which were applied for this work, and the authors tested and validated the astrometric accuracy via cross-comparison with other X-ray and multi-wavelength catalogs. They show that the number counts of X-ray sources in eRASS1 are consistent with those derived over narrower fields by past X-ray surveys of a similar depth, and they explore the number counts variation as a function of the location in the sky. Adopting a uniform all-sky flux limit (at 50% completeness) of F(0.5-2keV) > 5 x 10-14 erg/s/cm2, the authors estimate that the eROSITA all-sky survey resolves into individual sources about 20% of the cosmic X-ray background in the 1-2keV range.

The catalogs form part of the first data release (DR1) of the SRG/eROSITA all-sky survey. Beyond the X-ray catalogs, DR1 contains all detected and calibrated event files, source products (light curves and spectra), and all-sky maps. The data files are linked to the table and also accessible from the HEASARC eROSITA and eROSITA-DE ERASS1 websites.

The catalog uses the following designation for indicating the bands for the different measurement: 

    Band                Energy range (keV)
    0,1                 0.2 - 2.3
    P1                  0.2 - 0.5
    P2                  0.5 - 1.0
    P3                  1.0 - 2.0
    P4                  2.0 - 5.0
    P5                  5.0 - 8.0
    P6                  4.0 - 10.0
    P7                  5.1 - 6.1
    P8                  6.2 - 7.1
    P9                  7.2 - 8.2
    S                   0.5 - 2.0

Catalog Bibcode

2024A&A...682A..34M

References

The SRG/eROSITA all-sky survey, First X-ray catalogues and data release of
    the Western Galactic hemisphere. Merloni A., Lamer G., Liu T., Ramos-Ceja
    M.E., Brunner H. Bulbul E., Dennerl K., Doroshenko V., Freyberg M.J.,
    Friedrich S., Gatuzz E., Georgakakis A., Haberl F., Igo Z., Kreykenbohm
    I., Liu A., Maitra C., Malyali A., Mayer M.G.F., Nandra K., Predehl P.,
    Robrade J., Salvato M., Sanders J.S., Stewart I., Tubin-Arenas D., Weber
    P., Wilms J., Arcodia R., Artis E., Aschersleben J., Avakyan A., Aydar
    C., Bahar Y.E., Balzer F., Becker W., Berger K., Boller T., Bornemann W.,
    Brueggen M., Brusa M., Buchner J., Burwitz V., Camilloni F., Clerc N.,
    Comparat J., Coutinho D., Czesla S., Dannhauer S.M., Dauner L., Dauser
    T., Dietl J., Dolag K., Dwelly T., Egg K., Ehl E., Freund S., Friedrich
    P., Gaida R., Garrel C., Ghirardini V., Gokus A., Gruenwald G., Grandis
    S., Grotova I., Gruen D., Gueguen A., Haemmerich S., Hamaus N., Hasinger
    G., Haubner K., Homan D., Ider Chitham J., Joseph W.M., Joyce A., Koenig
    O., Kaltenbrunner D.M., Khokhriakova A., Kink W., Kirsch C., Kluge M.,
    Knies J., Krippendorf S., Krumpe M., Kurpas J., Li P., Liu Z., Locatelli
    N., Lorenz M., Mueller S., Magaudda E., Mannes C., McCall H., Meidinger
    N., Michailidis M., Migkas K., Munoz-Giraldo D., Musiimenta B.,
    Nguyen-Dang N.T., Ni Q., Olechowska A., Ota N., Pacaud F., Pasini T.,
    Perinati E., Pires A.M., Pommranz C., Ponti G., Poppenhaeger K.,
    Puehlhofer G., Rau A., Reh M., Reiprich T.H., Roster W., Saeedi S.,
    Santangelo A., Sasaki M., Schmitt J., Schneider P.C., Schrabback T.,
    Schuster N., Schwope A., Seppi R., Serim M.M., Shreeram S., Sokolova-Lapa
    E., Starck H., Stelzer B., Stierhof J., Suleimanov V., Tenzer C.,
    Traulsen I., Truemper J., Tsuge K., Urrutia T., Veronica A., Waddell
    S.G.H., Willer R., Wolf J., Yeung M.C.H., Zainab A., Zangrandi F., Zhang
    X., Zhang Y., Zheng X. <Astron. Astrophys. 682, A34 (2024)>
    =2024A&A...682A..34M (SIMBAD/NED BibCode)

Provenance

This database table was ingested by the HEASARC in June 2024 and is based upon the CDS Catalog J/A+A/682/A34 file erass1-m.dat. In some cases, the HEASARC has altered the original field names, as per HEASARC conventions, and provides the original field names in square brackets.

Parameters

Name
The eRASS1 source designation in the form '1eRASS JHHMMSS.s+DDMMSS', which uses the J2000.0 equatorial coordinates truncated to 0.1 arcseconds in RA and to 1 arcsecond in Declination. [IAUNAME]

Detuid
The unique detection identifier. [DETUID]

Skyfield_Number
The sky tile identification number. [SKYTILE]

Skyfield_Source_Number
The source identification number within each sky tile. The skyfield_number + skyfield_source_number identifies the corresponding source products. [ID_SRC]

Source_Number
The unique identification number for each source in this catalog. This number corresponds to 1011 + skyfield_number * 105 + skyfield_source_number. [UID]

Hard_Source_Number
The identification number corresponding to source in the hard-band (2.3-5 keV) catalog, eRASS1HARD. The value is positive for a source with strong association, and a negative value signifies a weak association with the listed source. The strong associations with the hard catalog have been directly linked to eRASS1HARD. [UID_Hard]

Cluster_ID
The group identification of simultaneously fitted sources. [ID_CLUSTER]

RA
The astrometrically-corrected right ascension for the source in the selected equinox. This was given in J2000 decimal degree coordinates to an accuracy of 10-5 degrees (0.036 arcseconds) in the original reference. [RA]

Dec
The astrometrically-corrected declination of the source in the selected equinox. This was given in J2000 decimal degree coordinates to an accuracy of 10-6 degrees (0.0036 arcseconds) in the original reference. [DEC]

LII
The galactic longitude of the source, based on the corrected right ascension and declination. Note that the original catalog values provide the galactic coordinates based on the raw (uncorrected) coordinates which have been found to be faulty and therefore, the authors suggest using the corrected values, as is provided in this catalog. [LII]

BII
The galactic latitude of the source. Note that the original catalog values provide the galactic coordinates based on the raw (uncorrected) coordinates which have been found to be faulty and therefore, the authors suggest using the corrected values, as is provided in this catalog. [BII]

RA_Raw
The uncorrected right ascension of the source. [RA_RAW]

Dec_Raw
The uncorrected declination of the source. [DEC_RAW]

RA_Neg_Err
The 1-sigma lower uncertainty for right ascension. [RA_LOWERR]

RA_Pos_Err
The 1-sigma upper uncertainty for right ascension. [RA_UPERR]

Dec_Neg_Err
The 1-sigma lower uncertainty for declination. [DEC_LOWERR]

Dec_Pos_Err
The 1-sigma upper uncertainty for declination. [DEC_UPERR]

Error_Radius
The 1-sigma positional uncertainty. [POS_ERR]

Error_Radius_Raw
The combined positional error, based on PSF-fitting from the uncorrected source position. [RADEC_ERR]

Time_Onaxis
The date/time corresponding to the date of the observation, based on the source nearest to the optical axis of the telescope. [MJD]

Time
The date/time corresponding to the first observation of the source. [MJD_MIN]

End_Time
The date/time corresponding to the last observation of the source. [MJD_MAX]

Source_Extent
The source extent parameter, given in arcseconds. [EXT]

Source_Extent_Error
The 1-sigma uncertainty in the source extent parameter, given in arcseconds. [EXT_ERR]

Source_Extent_Neg_Err
The 1-sigma lower uncertainty measurement in the source extent parameter. [EXT_LOWERR]

Source_Extent_Pos_Err
The 1-sigma upper uncertainty measurement in the source extent parameter. [EXT_UPERR]

Extent_Likelihood
The likelihood associated with the extent measurement. [EXT_LIKE]

B0_Detect_Likelihood
The detection likelihood in 0.2-2.3 keV band, based on PSF-fitting. This catalog includes sources with detect_likelihood >= 6. [DET_LIKE_0]

B1_Counts
The background-subtracted 0.2-2.3 keV net counts for the source, measured from the count_rate. [ML_CTS_1]

B1_Counts_Error
The combined 1-sigma uncertainty in the 0.2-2.3 keV net counts. [ML_CTS_ERR_1]

B1_Counts_Neg_Err
The 1-sigma lower uncertainty in 0.2-2.3 keV net counts. [ML_CTS_LOWERR_1]

B1_Counts_Pos_Err
The 1-sigma upper uncertainty in the 0.2-2.3keV net counts. [ML_CTS_UPERR_1]

B1_Count_Rate
The net count rate for the source in the 0.2-2.3 keV band, based on PSF-fitting. [ML_RATE_1]

B1_Count_Rate_Error
The combined 1-sigma uncertainty in the 0.2-2.3 keV net count rate. [ML_RATE_ERR_1]

B1_Count_Rate_Neg_Err
The 1-sigma lower uncertainty in the 0.2-2.3 keV net count rate. [ML_RATE_LOWERR_1]

B1_Count_Rate_Pos_Err
The 1-sigma upper uncertainty in the 0.2-2.3 keV net count rate. [ML_RATE_UPERR_1]

B1_Flux
The flux of the source in the 0.2-2.3 keV band, in units of erg/s/cm2. The energy conversion factor (ECF; listed in Table 3 of the reference paper) between the count rates and fluxes is based on a power-law model with Gamma=2.0 and the total Galactic absorption column density at source position. [ML_FLUX_1]

B1_Flux_Error
The 1-sigma uncertainty in the 0.2-2.3 keV flux, in units of erg/s/cm2. [ML_FLUX_ERR_1]

B1_Flux_Neg_Err
The 1-sigma lower uncertainty in the 0.2-2.3 keV flux, in units of erg/s/cm2. [ML_FLUX_LOWERR_1]

B1_Flux_Pos_Err
The 1-sigma upper uncertainty in the 0.2-2.3 keV flux, in units of erg/s/cm2. [ML_FLUX_UPERR_1]

B1_Bkg_Counts
The background counts, in units of counts/arcmin2, at the source position in the 0.2-2.3 keV band. [ML_BKG_1]

B1_Exposure
The vignetting-corrected exposure, in seconds, at the source position. [ML_EXP_1]

B1_EEF
The enclosed energy fraction in the 0.2-2.3keV band. [ML_EEF_1]

B1_Aperture_Counts
The total raw counts extracted within the aperture in the 0.2-2.3 keV band. [APE_CTS_1]

B1_Aperture_Bkg_Counts
The background counts expected within the aperture in 0.2-2.3 keV band, excluding nearby sources using the source map. [APE_BKG_1]

B1_Aperture_Exposure
The exposure map value in 0.2-2.3 keV band at the given position of the source. [APE_EXP_1]

B1_Aperture_Radius
The extraction radius in pixels in the 0.2-2.3 keV band. The aperture is chosen as a fixed one at 75% of the encircled energy fraction. [APE_RADIUS_1]

B1_Aperture_Prob
The Poisson probability that the observed 0.2-2.3 keV counts within the aperture are produced by random fluctuations of the background. Lower values mean lower chance that background fluctuations are cause for the observed counts and therefore the source is more likely to be an astrophysical source. [APE_POIS_1]

P1_Detect_Likelihood
The detection likelihood in 0.2-0.5 keV band, based on PSF-fitting. [DET_LIKE_P1]

P1_Counts
The background-subtracted 0.2-0.5 keV net counts for the source, measured from the count_rate. [ML_CTS_P1]

P1_Counts_Error
The combined 1-sigma uncertainty in the 0.2-0.5 keV net counts. [ML_CTS_ERR_P1]

P1_Counts_Neg_Err
The 1-sigma lower uncertainty in 0.2-0.5 keV net counts. [ML_CTS_LOWERR_P1]

P1_Counts_Pos_Err
The 1-sigma upper uncertainty in the 0.2-0.5keV net counts. [ML_CTS_UPERR_P1]

P1_Count_Rate
The net count rate for the source in the 0.2-0.5 keV band, based on PSF-fitting. [ML_RATE_P1]

P1_Count_Rate_Error
The combined 1-sigma uncertainty in the 0.2-0.5 keV net count rate. [ML_RATE_ERR_P1]

P1_Count_Rate_Neg_Err
The 1-sigma lower uncertainty in the 0.2-0.5 keV net count rate. [ML_RATE_LOWERR_P1]

P1_Count_Rate_Pos_Err
The 1-sigma upper uncertainty in the 0.2-0.5 keV net count rate. [ML_RATE_UPERR_P1]

P1_Flux
The flux of the source in the 0.2-0.5 keV band, in units of erg/s/cm2. The energy conversion factor (ECF; listed in Table 3 of the reference paper) between the count rates and fluxes is based on a power-law model with Gamma=2.0 and the total Galactic absorption column density at source position. [ML_FLUX_P1]

P1_Flux_Error
The 1-sigma uncertainty in the 0.2-0.5 keV flux, in units of erg/s/cm2. [ML_FLUX_ERR_P1]

P1_Flux_Neg_Err
The 1-sigma lower uncertainty in the 0.2-0.5 keV flux, in units of erg/s/cm2. [ML_FLUX_LOWERR_P1]

P1_Flux_Pos_Err
The 1-sigma upper uncertainty in the 0.2-0.5 keV flux, in units of erg/s/cm2. [ML_FLUX_UPERR_P1]

P1_Bkg_Counts
The background counts, in units of counts/arcmin2, at the source position in the 0.2-0.5 keV band. [ML_BKG_P1]

P1_Exposure
The vignetting-corrected exposure, in seconds, at the source position. [ML_EXP_P1]

P1_EEF
The enclosed energy fraction in the 0.2-0.5keV band. [ML_EEF_P1]

P1_Aperture_Counts
The total raw counts extracted within the aperture in the 0.2-0.5 keV band. [APE_CTS_P1]

P1_Aperture_Bkg_Counts
The background counts expected within the aperture in 0.2-0.5 keV band, excluding nearby sources using the source map. [APE_BKG_P1]

P1_Aperture_Exposure
The exposure map value in 0.2-0.5 keV band at the given position of the source. [APE_EXP_P1]

P1_Aperture_Radius
The extraction radius in pixels in the 0.2-0.5 keV band. The aperture is chosen as a fixed one at 75% of the encircled energy fraction. [APE_RADIUS_P1]

P1_Aperture_Prob
The Poisson probability that the observed 0.2-0.5 keV counts within the aperture are produced by random fluctuations of the background. Lower values mean lower chance that background fluctuations are cause for the observed counts and therefore the source is more likely to be an astrophysical source. [APE_POIS_P1]

P2_Detect_Likelihood
The detection likelihood in 0.5-1.0 keV band, based on PSF-fitting. [DET_LIKE_P2]

P2_Counts
The background-subtracted 0.5-1.0 keV net counts for the source, measured from the count_rate. [ML_CTS_P2]

P2_Counts_Error
The combined 1-sigma uncertainty in the 0.5-1.0 keV net counts. [ML_CTS_ERR_P2]

P2_Counts_Neg_Err
The 1-sigma lower uncertainty in 0.5-1.0 keV net counts. [ML_CTS_LOWERR_P2]

P2_Counts_Pos_Err
The 1-sigma upper uncertainty in the 0.5-1.0keV net counts. [ML_CTS_UPERR_P2]

P2_Count_Rate
The net count rate for the source in the 0.5-1.0 keV band, based on PSF-fitting. [ML_RATE_P2]

P2_Count_Rate_Error
The combined 1-sigma uncertainty in the 0.5-1.0 keV net count rate. [ML_RATE_ERR_P2]

P2_Count_Rate_Neg_Err
The 1-sigma lower uncertainty in the 0.5-1.0 keV net count rate. [ML_RATE_LOWERR_P2]

P2_Count_Rate_Pos_Err
The 1-sigma upper uncertainty in the 0.5-1.0 keV net count rate. [ML_RATE_UPERR_P2]

P2_Flux
The flux of the source in the 0.5-1.0 keV band, in units of erg/s/cm2. The energy conversion factor (ECF; listed in Table 3 of the reference paper) between the count rates and fluxes is based on a power-law model with Gamma=2.0 and the total Galactic absorption column density at source position. [ML_FLUX_P2]

P2_Flux_Error
The 1-sigma uncertainty in the 0.5-1.0 keV flux, in units of erg/s/cm2. [ML_FLUX_ERR_P2]

P2_Flux_Neg_Err
The 1-sigma lower uncertainty in the 0.5-1.0 keV flux, in units of erg/s/cm2. [ML_FLUX_LOWERR_P2]

P2_Flux_Pos_Err
The 1-sigma upper uncertainty in the 0.5-1.0 keV flux, in units of erg/s/cm2. [ML_FLUX_UPERR_P2]

P2_Bkg_Counts
The background counts, in units of counts/arcmin2, at the source position in the 0.5-1.0 keV band. [ML_BKG_P2]

P2_Exposure
The vignetting-corrected exposure, in seconds, at the source position. [ML_EXP_P2]

P2_EEF
The enclosed energy fraction in the 0.5-1.0keV band. [ML_EEF_P2]

P2_Aperture_Counts
The total raw counts extracted within the aperture in the 0.5-1.0 keV band. [APE_CTS_P2]

P2_Aperture_Bkg_Counts
The background counts expected within the aperture in 0.5-1.0 keV band, excluding nearby sources using the source map. [APE_BKG_P2]

P2_Aperture_Exposure
The exposure map value in 0.5-1.0 keV band at the given position of the source. [APE_EXP_P2]

P2_Aperture_Radius
The extraction radius in pixels in the 0.5-1.0 keV band. The aperture is chosen as a fixed one at 75% of the encircled energy fraction. [APE_RADIUS_P2]

P2_Aperture_Prob
The Poisson probability that the observed 0.5-1.0 keV counts within the aperture are produced by random fluctuations of the background. Lower values mean lower chance that background fluctuations are cause for the observed counts and therefore the source is more likely to be an astrophysical source. [APE_POIS_P2]

P3_Detect_Likelihood
The detection likelihood in 1.0-2.0 keV band, based on PSF-fitting. [DET_LIKE_P3]

P3_Counts
The background-subtracted 1.0-2.0 keV net counts for the source, measured from the count_rate. [ML_CTS_P3]

P3_Counts_Error
The combined 1-sigma uncertainty in the 1.0-2.0 keV net counts. [ML_CTS_ERR_P3]

P3_Counts_Neg_Err
The 1-sigma lower uncertainty in 1.0-2.0 keV net counts. [ML_CTS_LOWERR_P3]

P3_Counts_Pos_Err
The 1-sigma upper uncertainty in the 1.0-2.0keV net counts. [ML_CTS_UPERR_P3]

P3_Count_Rate
The net count rate for the source in the 1.0-2.0 keV band, based on PSF-fitting. [ML_RATE_P3]

P3_Count_Rate_Error
The combined 1-sigma uncertainty in the 1.0-2.0 keV net count rate. [ML_RATE_ERR_P3]

P3_Count_Rate_Neg_Err
The 1-sigma lower uncertainty in the 1.0-2.0 keV net count rate. [ML_RATE_LOWERR_P3]

P3_Count_Rate_Pos_Err
The 1-sigma upper uncertainty in the 1.0-2.0 keV net count rate. [ML_RATE_UPERR_P3]

P3_Flux
The flux of the source in the 1.0-2.0 keV band, in units of erg/s/cm2. The energy conversion factor (ECF; listed in Table 3 of the reference paper) between the count rates and fluxes is based on a power-law model with Gamma=2.0 and the total Galactic absorption column density at source position. [ML_FLUX_P3]

P3_Flux_Error
The 1-sigma uncertainty in the 1.0-2.0 keV flux, in units of erg/s/cm2. [ML_FLUX_ERR_P3]

P3_Flux_Neg_Err
The 1-sigma lower uncertainty in the 1.0-2.0 keV flux, in units of erg/s/cm2. [ML_FLUX_LOWERR_P3]

P3_Flux_Pos_Err
The 1-sigma upper uncertainty in the 1.0-2.0 keV flux, in units of erg/s/cm2. [ML_FLUX_UPERR_P3]

P3_Bkg_Counts
The background counts, in units of counts/arcmin2, at the source position in the 1.0-2.0 keV band. [ML_BKG_P3]

P3_Exposure
The vignetting-corrected exposure, in seconds, at the source position. [ML_EXP_P3]

P3_EEF
The enclosed energy fraction in the 1.0-2.0keV band. [ML_EEF_P3]

P3_Aperture_Counts
The total raw counts extracted within the aperture in the 1.0-2.0 keV band. [APE_CTS_P3]

P3_Aperture_Bkg_Counts
The background counts expected within the aperture in 1.0-2.0 keV band, excluding nearby sources using the source map. [APE_BKG_P3]

P3_Aperture_Exposure
The exposure map value in 1.0-2.0 keV band at the given position of the source. [APE_EXP_P3]

P3_Aperture_Radius
The extraction radius in pixels in the 1.0-2.0 keV band. The aperture is chosen as a fixed one at 75% of the encircled energy fraction. [APE_RADIUS_P3]

P3_Aperture_Prob
The Poisson probability that the observed 1.0-2.0 keV counts within the aperture are produced by random fluctuations of the background. Lower values mean lower chance that background fluctuations are cause for the observed counts and therefore the source is more likely to be an astrophysical source. [APE_POIS_P3]

P4_Detect_Likelihood
The detection likelihood in 2.0-5.0 keV band, based on PSF-fitting. [DET_LIKE_P4]

P4_Counts
The background-subtracted 2.0-5.0 keV net counts for the source, measured from the count_rate. [ML_CTS_P4]

P4_Counts_Error
The combined 1-sigma uncertainty in the 2.0-5.0 keV net counts. [ML_CTS_ERR_P4]

P4_Counts_Neg_Err
The 1-sigma lower uncertainty in 2.0-5.0 keV net counts. [ML_CTS_LOWERR_P4]

P4_Counts_Pos_Err
The 1-sigma upper uncertainty in the 2.0-5.0keV net counts. [ML_CTS_UPERR_P4]

P4_Count_Rate
The net count rate for the source in the 2.0-5.0 keV band, based on PSF-fitting. [ML_RATE_P4]

P4_Count_Rate_Error
The combined 1-sigma uncertainty in the 2.0-5.0 keV net count rate. [ML_RATE_ERR_P4]

P4_Count_Rate_Neg_Err
The 1-sigma lower uncertainty in the 2.0-5.0 keV net count rate. [ML_RATE_LOWERR_P4]

P4_Count_Rate_Pos_Err
The 1-sigma upper uncertainty in the 2.0-5.0 keV net count rate. [ML_RATE_UPERR_P4]

P4_Flux
The flux of the source in the 2.0-5.0 keV band, in units of erg/s/cm2. The energy conversion factor (ECF; listed in Table 3 of the reference paper) between the count rates and fluxes is based on a power-law model with Gamma=2.0 and the total Galactic absorption column density at source position. [ML_FLUX_P4]

P4_Flux_Error
The 1-sigma uncertainty in the 2.0-5.0 keV flux, in units of erg/s/cm2. [ML_FLUX_ERR_P4]

P4_Flux_Neg_Err
The 1-sigma lower uncertainty in the 2.0-5.0 keV flux, in units of erg/s/cm2. [ML_FLUX_LOWERR_P4]

P4_Flux_Pos_Err
The 1-sigma upper uncertainty in the 2.0-5.0 keV flux, in units of erg/s/cm2. [ML_FLUX_UPERR_P4]

P4_Bkg_Counts
The background counts, in units of counts/arcmin2, at the source position in the 2.0-5.0 keV band. [ML_BKG_P4]

P4_Exposure
The vignetting-corrected exposure, in seconds, at the source position. [ML_EXP_P4]

P4_EEF
The enclosed energy fraction in the 2.0-5.0keV band. [ML_EEF_P4]

P4_Aperture_Counts
The total raw counts extracted within the aperture in the 2.0-5.0 keV band. [APE_CTS_P4]

P4_Aperture_Bkg_Counts
The background counts expected within the aperture in 2.0-5.0 keV band, excluding nearby sources using the source map. [APE_BKG_P4]

P4_Aperture_Exposure
The exposure map value in 2.0-5.0 keV band at the given position of the source. [APE_EXP_P4]

P4_Aperture_Radius
The extraction radius in pixels in the 2.0-5.0 keV band. The aperture is chosen as a fixed one at 75% of the encircled energy fraction. [APE_RADIUS_P4]

P4_Aperture_Prob
The Poisson probability that the observed 2.0-5.0 keV counts within the aperture are produced by random fluctuations of the background. Lower values mean lower chance that background fluctuations are cause for the observed counts and therefore the source is more likely to be an astrophysical source. [APE_POIS_P4]

P5_Detect_Likelihood
The detection likelihood in 5.0-8.0 keV band, based on PSF-fitting. [DET_LIKE_P5]

P5_Counts
The background-subtracted 5.0-8.0 keV net counts for the source, measured from the count_rate. [ML_CTS_P5]

P5_Counts_Error
The combined 1-sigma uncertainty in the 5.0-8.0 keV net counts. [ML_CTS_ERR_P5]

P5_Counts_Neg_Err
The 1-sigma lower uncertainty in 5.0-8.0 keV net counts. [ML_CTS_LOWERR_P5]

P5_Counts_Pos_Err
The 1-sigma upper uncertainty in the 5.0-8.0keV net counts. [ML_CTS_UPERR_P5]

P5_Count_Rate
The net count rate for the source in the 5.0-8.0 keV band, based on PSF-fitting. [ML_RATE_P5]

P5_Count_Rate_Error
The combined 1-sigma uncertainty in the 5.0-8.0 keV net count rate. [ML_RATE_ERR_P5]

P5_Count_Rate_Neg_Err
The 1-sigma lower uncertainty in the 5.0-8.0 keV net count rate. [ML_RATE_LOWERR_P5]

P5_Count_Rate_Pos_Err
The 1-sigma upper uncertainty in the 5.0-8.0 keV net count rate. [ML_RATE_UPERR_P5]

P5_Flux
The flux of the source in the 5.0-8.0 keV band, in units of erg/s/cm2. The energy conversion factor (ECF; listed in Table 3 of the reference paper) between the count rates and fluxes is based on a power-law model with Gamma=2.0 and the total Galactic absorption column density at source position. [ML_FLUX_P5]

P5_Flux_Error
The 1-sigma uncertainty in the 5.0-8.0 keV flux, in units of erg/s/cm2. [ML_FLUX_ERR_P5]

P5_Flux_Neg_Err
The 1-sigma lower uncertainty in the 5.0-8.0 keV flux, in units of erg/s/cm2. [ML_FLUX_LOWERR_P5]

P5_Flux_Pos_Err
The 1-sigma upper uncertainty in the 5.0-8.0 keV flux, in units of erg/s/cm2. [ML_FLUX_UPERR_P5]

P5_Bkg_Counts
The background counts, in units of counts/arcmin2, at the source position in the 5.0-8.0 keV band. [ML_BKG_P5]

P5_Exposure
The vignetting-corrected exposure, in seconds, at the source position. [ML_EXP_P5]

P5_EEF
The enclosed energy fraction in the 5.0-8.0keV band. [ML_EEF_P5]

P5_Aperture_Counts
The total raw counts extracted within the aperture in the 5.0-8.0 keV band. [APE_CTS_P5]

P5_Aperture_Bkg_Counts
The background counts expected within the aperture in 5.0-8.0 keV band, excluding nearby sources using the source map. [APE_BKG_P5]

P5_Aperture_Exposure
The exposure map value in 5.0-8.0 keV band at the given position of the source. [APE_EXP_P5]

P5_Aperture_Radius
The extraction radius in pixels in the 5.0-8.0 keV band. The aperture is chosen as a fixed one at 75% of the encircled energy fraction. [APE_RADIUS_P5]

P5_Aperture_Prob
The Poisson probability that the observed 5.0-8.0 keV counts within the aperture are produced by random fluctuations of the background. Lower values mean lower chance that background fluctuations are cause for the observed counts and therefore the source is more likely to be an astrophysical source. [APE_POIS_P5]

P6_Detect_Likelihood
The detection likelihood in 4.0-10.0 keV band, based on PSF-fitting. [DET_LIKE_P6]

P6_Counts
The background-subtracted 4.0-10.0 keV net counts for the source, measured from the count_rate. [ML_CTS_P6]

P6_Counts_Error
The combined 1-sigma uncertainty in the 4.0-10.0 keV net counts. [ML_CTS_ERR_P6]

P6_Counts_Neg_Err
The 1-sigma lower uncertainty in 4.0-10.0 keV net counts. [ML_CTS_LOWERR_P6]

P6_Counts_Pos_Err
The 1-sigma upper uncertainty in the 4.0-10.0keV net counts. [ML_CTS_UPERR_P6]

P6_Count_Rate
The net count rate for the source in the 4.0-10.0 keV band, based on PSF-fitting. [ML_RATE_P6]

P6_Count_Rate_Error
The combined 1-sigma uncertainty in the 4.0-10.0 keV net count rate. [ML_RATE_ERR_P6]

P6_Count_Rate_Neg_Err
The 1-sigma lower uncertainty in the 4.0-10.0 keV net count rate. [ML_RATE_LOWERR_P6]

P6_Count_Rate_Pos_Err
The 1-sigma upper uncertainty in the 4.0-10.0 keV net count rate. [ML_RATE_UPERR_P6]

P6_Flux
The flux of the source in the 4.0-10.0 keV band, in units of erg/s/cm2. The energy conversion factor (ECF; listed in Table 3 of the reference paper) between the count rates and fluxes is based on a power-law model with Gamma=2.0 and the total Galactic absorption column density at source position. [ML_FLUX_P6]

P6_Flux_Error
The 1-sigma uncertainty in the 4.0-10.0 keV flux, in units of erg/s/cm2. [ML_FLUX_ERR_P6]

P6_Flux_Neg_Err
The 1-sigma lower uncertainty in the 4.0-10.0 keV flux, in units of erg/s/cm2. [ML_FLUX_LOWERR_P6]

P6_Flux_Pos_Err
The 1-sigma upper uncertainty in the 4.0-10.0 keV flux, in units of erg/s/cm2. [ML_FLUX_UPERR_P6]

P6_Bkg_Counts
The background counts, in units of counts/arcmin2, at the source position in the 4.0-10.0 keV band. [ML_BKG_P6]

P6_Exposure
The vignetting-corrected exposure, in seconds, at the source position. [ML_EXP_P6]

P6_EEF
The enclosed energy fraction in the 4.0-10.0keV band. [ML_EEF_P6]

P6_Aperture_Counts
The total raw counts extracted within the aperture in the 4.0-10.0 keV band. [APE_CTS_P6]

P6_Aperture_Bkg_Counts
The background counts expected within the aperture in 4.0-10.0 keV band, excluding nearby sources using the source map. [APE_BKG_P6]

P6_Aperture_Exposure
The exposure map value in 4.0-10.0 keV band at the given position of the source. [APE_EXP_P6]

P6_Aperture_Radius
The extraction radius in pixels in the 4.0-10.0 keV band. The aperture is chosen as a fixed one at 75% of the encircled energy fraction. [APE_RADIUS_P6]

P6_Aperture_Prob
The Poisson probability that the observed 4.0-10.0 keV counts within the aperture are produced by random fluctuations of the background. Lower values mean lower chance that background fluctuations are cause for the observed counts and therefore the source is more likely to be an astrophysical source. [APE_POIS_P6]

P7_Detect_Likelihood
The detection likelihood in 5.1-6.1 keV band, based on PSF-fitting. [DET_LIKE_P7]

P7_Counts
The background-subtracted 5.1-6.1 keV net counts for the source, measured from the count_rate. [ML_CTS_P7]

P7_Counts_Error
The combined 1-sigma uncertainty in the 5.1-6.1 keV net counts. [ML_CTS_ERR_P7]

P7_Counts_Neg_Err
The 1-sigma lower uncertainty in 5.1-6.1 keV net counts. [ML_CTS_LOWERR_P7]

P7_Counts_Pos_Err
The 1-sigma upper uncertainty in the 5.1-6.1keV net counts. [ML_CTS_UPERR_P7]

P7_Count_Rate
The net count rate for the source in the 5.1-6.1 keV band, based on PSF-fitting. [ML_RATE_P7]

P7_Count_Rate_Error
The combined 1-sigma uncertainty in the 5.1-6.1 keV net count rate. [ML_RATE_ERR_P7]

P7_Count_Rate_Neg_Err
The 1-sigma lower uncertainty in the 5.1-6.1 keV net count rate. [ML_RATE_LOWERR_P7]

P7_Count_Rate_Pos_Err
The 1-sigma upper uncertainty in the 5.1-6.1 keV net count rate. [ML_RATE_UPERR_P7]

P7_Flux
The flux of the source in the 5.1-6.1 keV band, in units of erg/s/cm2. The energy conversion factor (ECF; listed in Table 3 of the reference paper) between the count rates and fluxes is based on a power-law model with Gamma=2.0 and the total Galactic absorption column density at source position. [ML_FLUX_P7]

P7_Flux_Error
The 1-sigma uncertainty in the 5.1-6.1 keV flux, in units of erg/s/cm2. [ML_FLUX_ERR_P7]

P7_Flux_Neg_Err
The 1-sigma lower uncertainty in the 5.1-6.1 keV flux, in units of erg/s/cm2. [ML_FLUX_LOWERR_P7]

P7_Flux_Pos_Err
The 1-sigma upper uncertainty in the 5.1-6.1 keV flux, in units of erg/s/cm2. [ML_FLUX_UPERR_P7]

P7_Bkg_Counts
The background counts, in units of counts/arcmin2, at the source position in the 5.1-6.1 keV band. [ML_BKG_P7]

P7_Exposure
The vignetting-corrected exposure, in seconds, at the source position. [ML_EXP_P7]

P7_EEF
The enclosed energy fraction in the 5.1-6.1keV band. [ML_EEF_P7]

P7_Aperture_Counts
The total raw counts extracted within the aperture in the 5.1-6.1 keV band. [APE_CTS_P7]

P7_Aperture_Bkg_Counts
The background counts expected within the aperture in 5.1-6.1 keV band, excluding nearby sources using the source map. [APE_BKG_P7]

P7_Aperture_Exposure
The exposure map value in 5.1-6.1 keV band at the given position of the source. [APE_EXP_P7]

P7_Aperture_Radius
The extraction radius in pixels in the 5.1-6.1 keV band. The aperture is chosen as a fixed one at 75% of the encircled energy fraction. [APE_RADIUS_P7]

P7_Aperture_Prob
The Poisson probability that the observed 5.1-6.1 keV counts within the aperture are produced by random fluctuations of the background. Lower values mean lower chance that background fluctuations are cause for the observed counts and therefore the source is more likely to be an astrophysical source. [APE_POIS_P7]

P8_Detect_Likelihood
The detection likelihood in 6.2-7.1 keV band, based on PSF-fitting. [DET_LIKE_P8]

P8_Counts
The background-subtracted 6.2-7.1 keV net counts for the source, measured from the count_rate. [ML_CTS_P8]

P8_Counts_Error
The combined 1-sigma uncertainty in the 6.2-7.1 keV net counts. [ML_CTS_ERR_P8]

P8_Counts_Neg_Err
The 1-sigma lower uncertainty in 6.2-7.1 keV net counts. [ML_CTS_LOWERR_P8]

P8_Counts_Pos_Err
The 1-sigma upper uncertainty in the 6.2-7.1keV net counts. [ML_CTS_UPERR_P8]

P8_Count_Rate
The net count rate for the source in the 6.2-7.1 keV band, based on PSF-fitting. [ML_RATE_P8]

P8_Count_Rate_Error
The combined 1-sigma uncertainty in the 6.2-7.1 keV net count rate. [ML_RATE_ERR_P8]

P8_Count_Rate_Neg_Err
The 1-sigma lower uncertainty in the 6.2-7.1 keV net count rate. [ML_RATE_LOWERR_P8]

P8_Count_Rate_Pos_Err
The 1-sigma upper uncertainty in the 6.2-7.1keV net count rate. [ML_RATE_UPERR_P8]

P8_Flux
The flux of the source in the 6.2-7.1 keV band, in units of erg/s/cm2. The energy conversion factor (ECF; listed in Table 3 of the reference paper) between the count rates and fluxes is based on a power-law model with Gamma=2.0 and the total Galactic absorption column density at source position. [ML_FLUX_P8]

P8_Flux_Error
The 1-sigma uncertainty in the 6.2-7.1 keV flux, in units of erg/s/cm2. [ML_FLUX_ERR_P8]

P8_Flux_Neg_Err
The 1-sigma lower uncertainty in the 6.2-7.1 keV flux, in units of erg/s/cm2. [ML_FLUX_LOWERR_P8]

P8_Flux_Pos_Err
The 1-sigma upper uncertainty in the 6.2-7.1 keV flux, in units of erg/s/cm2. [ML_FLUX_UPERR_P8]

P8_Bkg_Counts
The background counts, in units of counts/arcmin2, at the source position in the 6.2-7.1 keV band. [ML_BKG_P8]

P8_Exposure
The vignetting-corrected exposure, in seconds, at the source position. [ML_EXP_P8]

P8_EEF
The enclosed energy fraction in the 6.2-7.1keV band. [ML_EEF_P8]

P8_Aperture_Counts
The total raw counts extracted within the aperture in the 6.2-7.1 keV band. [APE_CTS_P8]

P8_Aperture_Bkg_Counts
The background counts expected within the aperture in 6.2-7.1 keV band, excluding nearby sources using the source map. [APE_BKG_P8]

P8_Aperture_Exposure
The exposure map value in 6.2-7.1 keV band at the given position of the source. [APE_EXP_P8]

P8_Aperture_Radius
The extraction radius in pixels in the 6.2-7.1 keV band. The aperture is chosen as a fixed one at 75% of the encircled energy fraction. [APE_RADIUS_P8]

P8_Aperture_Prob
The Poisson probability that the observed 6.2-7.1 keV counts within the aperture are produced by random fluctuations of the background. Lower values mean lower chance that background fluctuations are cause for the observed counts and therefore the source is more likely to be an astrophysical source. [APE_POIS_P8]

P9_Detect_Likelihood
The detection likelihood in 7.2-8.2 keV band, based on PSF-fitting. [DET_LIKE_P9]

P9_Counts
The background-subtracted 7.2-8.2 keV net counts for the source, measured from the count_rate. [ML_CTS_P9]

P9_Counts_Error
The combined 1-sigma uncertainty in the 7.2-8.2 keV net counts. [ML_CTS_ERR_P9]

P9_Counts_Neg_Err
The 1-sigma lower uncertainty in 7.2-8.2 keV net counts. [ML_CTS_LOWERR_P9]

P9_Counts_Pos_Err
The 1-sigma upper uncertainty in the 7.2-8.2keV net counts. [ML_CTS_UPERR_P9]

P9_Count_Rate
The net count rate for the source in the 7.2-8.2 keV band, based on PSF-fitting. [ML_RATE_P9]

P9_Count_Rate_Error
The combined 1-sigma uncertainty in the 7.2-8.2 keV net count rate. [ML_RATE_ERR_P9]

P9_Count_Rate_Neg_Err
The 1-sigma lower uncertainty in the 7.2-8.2 keV net count rate. [ML_RATE_LOWERR_P9]

P9_Count_Rate_Pos_Err
The 1-sigma upper uncertainty in the 7.2-8.2 keV net count rate. [ML_RATE_UPERR_P9]

P9_Flux
The flux of the source in the 7.2-8.2 keV band, in units of erg/s/cm2. The energy conversion factor (ECF; listed in Table 3 of the reference paper) between the count rates and fluxes is based on a power-law model with Gamma=2.0 and the total Galactic absorption column density at source position. [ML_FLUX_P9]

P9_Flux_Error
The 1-sigma uncertainty in the 7.2-8.2 keV flux, in units of erg/s/cm2. [ML_FLUX_ERR_P9]

P9_Flux_Neg_Err
The 1-sigma lower uncertainty in the 7.2-8.2 keV flux, in units of erg/s/cm2. [ML_FLUX_LOWERR_P9]

P9_Flux_Pos_Err
The 1-sigma upper uncertainty in the 7.2-8.2 keV flux, in units of erg/s/cm2. [ML_FLUX_UPERR_P9]

P9_Bkg_Counts
The background counts, in units of counts/arcmin2, at the source position in the 7.2-8.2 keV band. [ML_BKG_P9]

P9_Exposure
The vignetting-corrected exposure, in seconds, at the source position. [ML_EXP_P9]

P9_EEF
The enclosed energy fraction in the 7.2-8.2keV band. [ML_EEF_P9]

P9_Aperture_Counts
The total raw counts extracted within the aperture in the 7.2-8.2 keV band. [APE_CTS_P9]

P9_Aperture_Bkg_Counts
The background counts expected within the aperture in 7.2-8.2 keV band, excluding nearby sources using the source map. [APE_BKG_P9]

P9_Aperture_Exposure
The exposure map value in 7.2-8.2 keV band at the given position of the source. [APE_EXP_P9]

P9_Aperture_Radius
The extraction radius in pixels in the 7.2-8.2 keV band. The aperture is chosen as a fixed one at 75% of the encircled energy fraction. [APE_RADIUS_P9]

P9_Aperture_Prob
The Poisson probability that the observed 7.2-8.2 keV counts within the aperture are produced by random fluctuations of the background. Lower values mean lower chance that background fluctuations are cause for the observed counts and therefore the source is more likely to be an astrophysical source. [APE_POIS_P9]

S_Aperture_Counts
The total raw counts extracted within the aperture in the 0.5-2.0 keV band. [APE_CTS_S]

S_Aperture_Bkg_Counts
The background counts expected within the aperture in 0.5-2.0 keV band, excluding nearby sources using the source map. [APE_BKG_S]

S_Aperture_Exposure
The exposure map value in 0.5-2.0 keV band at the given position of the source. [APE_EXP_S]

S_Aperture_Prob
The Poisson probability that the observed 0.5-2.0 keV counts within the aperture are produced by random fluctuations of the background. Lower values mean lower chance that background fluctuations are cause for the observed counts and therefore the source is more likely to be an astrophysical source. [APE_POIS_S]

Srcpos_SNR_Flag
Boolean flag (possible files of 0 or 1) which indicates that the source may lie within an overdense region near supernova remnant. [FLAG_SP_SNR]

Srcpos_Bps_Flag
Boolean flag (possible files of 0 or 1) which indicates that the source may lie within an overdense region near bright source. [FLAG_SP_BPS]

Srcpos_Scl_Flag
Boolean flag (possible files of 0 or 1) which indicates that the source may lie within an overdense region near stellar cluster. [FLAG_SP_SCL]

Srcpos_Lga_Flag
Boolean flag (possible files of 0 or 1) which indicates that the source may lie within an overdense region near local large galaxy. [FLAG_SP_LGA]

Srcpos_GC_Flag
Boolean flag (possible files of 0 or 1) which indicates that the source may lie within an overdense region near galaxy cluster. [FLAG_SP_GC_CONS]

No_RADec_Err_Flag
Boolean flag (possible files of 0 or 1) which indicates that the source contained no position uncertainty in the pre-processed version of this catalog. FLAG_NO_RADEC_ERR]

No_Ext_Err_Flag
Boolean flag (possible files of 0 or 1) which indicates that the source contained no extent error in the pre-processed version of this catalog. [FLAG_NO_EXT_ERR]

No_Cts_Err_Flag
Boolean flag (possible files of 0 or 1) which indicates that the source contained no counts error in the pre-processed version of this catalog. [FLAG_NO_CTS_ERR]

Optical_Flag
Boolean flag (values 0 or 1) which indicates that the source is matched within 15-arcsec of a bright optical star and may be contaminated by optical loading. [FLAG_OPT]

Contact Person

Questions regarding the ERASS1MAIN database table can be addressed to the HEASARC Help Desk.
Page Author: Browse Software Development Team
Last Modified: Thursday, 19-Sep-2024 13:37:04 EDT