ACDS V10.0 - Detailed Description of J/PASJ/55/161

ACDS V10.0 - Sun Jan 19 02:53:05 CET 2025

| # Detailed Description of J/PASJ/55/161 : ASCA sources in the SMC (Yokogawa+, 2003) |

Note : this is the description file of the original catalog. This HTML page corresponds well to the original description, but some minor changes in the format may have been introduced in the FITS output files in order to allow for arithmetic operations on quantities such as coordinates and times. h:m:s and d:m:s units are normally converted into degrees, and YYYY-MM-DD into julian days.
Similarly, some slight changes may have been introduced in the units; the value given in the HTML files supersedes the value indicated in the ReadMe file for this catalogue.

    J/PASJ/55/161   ASCA sources in the SMC                (Yokogawa+, 2003)
    ================================================================================
    Review of discrete X-ray sources in the Small Magellanic Cloud :
    summary of the ASCA results and implication on the recent star-forming activity.
        Yokogawa J., Imanishi K., Tsujimoto M., Koyama K., Nishiuchi M.
       <Publ. Astron. Soc. Jap., 55, 161 (2003)>
       =2003PASJ...55..161Y
    ================================================================================
    ADC_Keywords: Magellanic Clouds ; X-ray sources

    Mission_Name: ASCA

    Keywords: galaxies: evolution - galaxies: individual (SMC, LMC) -
              galaxies: starburst - pulsars: general - source population study -
              X-rays: stars

    Abstract:
        We made 22 observations on the Small Magellanic Cloud (SMC) and
        covered full regions of the main body and the eastern wing by the end
        of the ASCA mission. We detected 106 discrete sources with a criterion
        of S/N>5 and performed systematic analyses on all of the sources. We
        determined the source positions with an ~40" error radius (90%
        confidence) for sources detected in the central 20' radius of the GIS.
        We detected coherent pulsations from 17 sources. Among them, eight
        were newly discovered during this study. We classified most of these
        pulsars as X-ray binary pulsars (XBPs) based on their properties, such
        as the flux variability and the existence of an optical counterpart.
        We detected X-ray emission from eight supernova remnants (SNRs).

        Based on these ASCA results and further information from ROSAT, SAX,
        RXTE, CGRO, Chandra, and XMM-Newton, we compiled comprehensive
        catalogues of discrete X-ray sources in the Small Magellanic Cloud.

    File Summary:

           FileName      Lrecl  Records   Explanations

    ×                   80        .   This file
    × ReadMe            80        .   This file
    × table1.dat        81       22   ASCA observations of the SMC region
    × table5.dat       237      106   ASCA catalogue of discrete X-ray sources
                                  in the SMC region
    × table6.dat       153      136   Spectral parameters of the ASCA sources
    × table8.dat        57       36   Non-pulsating HMXBs and likely candidates
                                  in the SMC

    See also:
       J/A+AS/142/41 : SMC X-ray sources ROSAT PSPC catalogue (Haberl+, 2000)
       J/A+AS/147/75 : ROSAT HRI catalogue of SMC X-ray sources (Sasaki+, 2000)

    Byte-by-byte Description of file:  table1.dat

       Bytes Format Units      Label     Explanations

           1  A1    ---        ObsID     [A-V] Observation ID
       3- 12  A10 "YYYY/MM/DD" SObs.date  Start of observation date (UT)
      14- 15  I2    h          SObs.h    Start of observation date (UT)
          16  A1    ---        ---       [:]
      17- 18  I2    min        SObs.m    Start of observation date (UT)
      20- 29  A10 "YYYY/MM/DD" EObs.date  End of observation date (UT)
      31- 32  I2    h          EObs.h    End of observation date (UT)
          33  A1    ---        ---       [:]
      34- 35  I2    min        EObs.m    End of observation date (UT)
      37- 52  A16   ---        Target    Target name
      55- 56  I2    h          RAh       Pointed direction right ascension (J2000)
      58- 59  I2    min        RAm       Pointed direction right ascension (J2000)
      61- 62  I2    s          RAs       Pointed direction right ascension (J2000)
          64  A1    ---        DE-       Pointed direction declination sign (J2000)
      65- 66  I2    deg        DEd       Pointed direction declination (J2000)
      68- 69  I2    arcmin     DEm       Pointed direction declination (J2000)
      71- 72  I2    arcsec     DEs       Pointed direction declination (J2000)
      74- 76  I3    ks         ExpGIS    Exposure time with GIS
          77  A1    ---        n_ExpGIS  [cd] Note on ExpGIS  (1)
          78  A1    ---        ---       [/]
      79- 80  I2    ks         ExpSIS    ? Exposure time with SIS
          81  A1    ---        n_ExpSIS  [b] Note on ExpSIS (2)

    Note (1): Note on ExpGIS:
        c, d: GIS was operated with a special bit assignment of 8-6-6-5-6 (c)
              or 8-8-8-5-2 (d), in which the time resolution was increased by
              a factor of 64 (c) or 4 (d), at the sacrifice of a reduction of
              energy resolution by a factor of 4 (c and d) and a reduction of
              spatial resolution by a factor of 4 (c).
    Note (2): Note on ExpSIS:
        a, b: SIS was operated in 1-CCD mode (a) or 2-CCD mode (b).

    Byte-by-byte Description of file:  table5.dat

       Bytes Format Units   Label       Explanations

       1-  3  I3    ---     [YIT2003]   Sequential number of ASCA source
           4  A1    ---    n_[YIT2003]  [+*] Note on [YIT2003] (1)
       6-  7  I2    h       RAh         Right ascension (J2000)
       9- 10  I2    min     RAm         Right ascension (J2000)
      12- 15  F4.1  s       RAs         Right ascension (J2000)
          17  A1    ---     DE-         Declination sign (J2000)
      18- 19  I2    deg     DEd         Declination (J2000)
      21- 22  I2    arcmin  DEm         Declination (J2000)
      24- 25  I2    arcsec  DEs         Declination (J2000)
          27  A1    ---     ObsID       Observation ID (table1.dat) in which
                                         the source was detected (2)
          28  A1    ---     ObsID2      Observation ID (table1.dat) in which
                                         the source was detected (2)
          29  A1    ---     ObsID3      Observation ID (table1.dat) in which
                                         the source was detected (2)
          30  A1    ---     ---         [/]
          31  A1    ---     ObsID1Not   Observation ID (table1.dat) in which
                                         the source was not detected
          32  A1    ---     ObsID2Not   Observation ID (table1.dat) in which
                                         the source was not detected
          33  A1    ---     n_ObsID     [j] Note on ObsID (3)
      34- 39  F6.1  ---     S/N         Larget value of signal-to-noise ratio (4)
      41- 44  I4    ---     PSPC        ? PSPC number of ROSAT counterpart (5)
      46- 48  I3    arcsec  Sep1        ? Separation between ASCA and PSPS source
          49  A1    ---     n_Sep1      [k] Note on Sep1 (6)
      51- 53  I3    ---     HRI         ? HRI number of ROSAT HRI counterpart  (7)
      55- 57  I3    arcsec  Sep2        ? Separation between ASCA and HRI source
      59- 60  I2    ---     IPC         ? IPC number of EINSTEIN IPC counterpart (8)
      62- 63  I2    arcsec  Sep3        ? Separation between ASCA and IPC source
      65- 71  A7    ---     Class       Classification (9)
      73-125  A53   ---     Names       Other names (10)
     127-237  A111  ---     Com         Comments  (11)

    Note (1): Sources with ``*'' were detected in the inner circle of the
        GIS and have an error radius of ~40" at 90% confidence (subsubsection
        3.3.1). Sources with "+" were detected in the outer ring of the GIS
        and their error radius is larger.
    Note (2): For sources detected multiple times, the first ID, ObsID, was
        used to determine its position.
    Note (3): Note on ObsID:
           j: In these observations, nearby sources were too bright, thus
              detection of No. 34 and No. 95 was hampered.
    Note (4): The criterion of source detection is S/N>5.

    Note (5): The separation angle from the central point of No. 413 and 419
         in Haberl et al. (2000, Cat. J/A+AS/142/41)
    Note (6): Counterpart found in the ROSAT PSPC catalogue (Haberl et al. 2000,
         Cat. J/A+AS/142/41)
    Note (7): Counterpart found in the ROSAT HRI catalogue (Sasaki et al., 2000,
         Cat. J/A+AS/147/75)
    Note (8): Counterpart found in the Einstein IPC catalogue (Wang and Wu,
         1992ApJS...78..391W).
    Note (9): Source class (see subsubsection 6.2.1) are as follows:
         TS = thermal SNRs; subsubsection 4.2.3
         RS = radio SNRs which are not classified as a thermal SNR
        TSc = thermal SNR candidates; subsubsection 6.2.3
         BP = X-ray binary pulsars; subsection 5.1
        BPc = candidates of X-ray binary pulsar; subsubsection 6.2.3
        AXP = anomalous X-ray pulsar
          P = the remaining pulsars
         NH = non-pulsating HMXBs; table8.dat
        AGN = sources coincident with an AGN
         FS = sources coincident with a foreground star
         UN = unclassified sources
    Note (10): Source names usually used in the literature.
               References for the abbreviations are/
         DDEM: Davies et al. (1976, Cat. VII/232)
          IKT: Inoue et al. (1983IAUS..101..535I)
            N: Henize (1956ApJS....2..315H)
          SNR: Mathewson et al. (1983ApJS...51..345M, 1984ApJS...55..189M)
    Note (11): Periods in square brackets were determined by others and not
         detected in this work.

    Byte-by-byte Description of file:  table6.dat

       Bytes Format Units    Label     Explanations

       1-  3  I3    ---     [YIT2003]  Sequential number
       5-  9  F5.2  ---      HR        ? Hardness ratio
      11- 15  F5.3  ---      e_HR      ? rms uncertainty on HR
          17  A1    ---      ObsID     [A-V] Observation ID, see table1.dat
                                        (Flux and luminosity are given for each ID)
      19- 23  F5.2  ---      Gamma     ? Photon index
          24  A1    ---      n_Gamma   [f] Note (2)
          26  A1    ---      l_Gammal  Limit flag on Gamma
      27- 31  F5.2  ---      Gammal    ? Lower value of 90% confidence limits of
                                          Gamma
      32- 36  F5.2  ---      Gammau    ? Upper value of 90% confidence limits of
                                          Gamma
      39- 43  F5.3  keV      kT        ? Temperature kT (1)
      45- 49  F5.3  keV      kTl       ? Lower value of 90% confidence limits of kT
      51- 55  F5.3  keV      kTu       ? Upper value of 90% confidence limits of kT
      58- 63  F6.2 10+21cm-2 NH        ? Absorption column density
          65  A1    ---      l_NHl     Limit flag on NHl
      66- 70  F5.1 10+21cm-2 NHl       ? Lower value of 90% confidence limits of NH
      72- 76  F5.1 10+21cm-2 NHu       ? Upper value of 90% confidence limits of NH
      78- 84  F7.3 10-15W/m2 FX        ? X-ray flux in 0.7-10keV band
          85  A1    ---      n_FX      [g] Note on FX (2)
      86- 92  F7.3  10+29W   LXobs     ? Observed luminosity in 0.7-10keV band
          93  A1    ---      n_LXobs   [g] Note on FX (2)
      94-100  F7.3  10+29W   LXcor     ? Absorption-corrected luminosity
                                          in 0.7-10keV band
         101  A1    ---      n_LXcor   [ge] Note on FX (2)
     104-153  A50   ---      Note      Note

    Note (1): For sources showing soft excess (Nos. 67, 90, and 94), a
        two-component model consisting of a power-law (with exponential cutoff
        only for No. 67) plus a blackbody was used; thus the temperature in
        the table is for the blackbody component.
    Note (2): Notes have the wollowing meaning:
           e: The best-fit model yielded an unusually high luminosity of
              ~3x1039erg/s. This is probably an artifact due to the large
              values of Gamma and NH,  thus we omitted it from the table.
           f: A power-law model with a high-energy cutoff was used. Cut-off and
              e-fold energies were respectively determined to be
              6.4 (5.8-6.9)keV and 6.3 (4.4-9.4)keV.
           g: The intrinsic intensity would  be much higher
              (see subsubsection 5.1.22).

    Byte-by-byte Description of file:  table8.dat

       Bytes Format Units   Label     Explanations

       1-  2  I2    ---    [YIT2003]  ? Sequential number
       4-  5  I2    ---     [HS2000]  ? HRI (Harbel & Sasaki, 2000A&A...359..573H)
                                         number
       7- 21  A15   ---     Name      Other name
      23- 25  A3    ---     ---       [IKT]
      26- 27  I2    ---     IKT       ? IKT (Inoue et al., 1983IAUS..101..535I)
                                         number
          30  A1    ---     n_Name    [e] Note on name (1)
      33- 39  A7    ---     SpType    Optical identification (2)
          41  A1    ---     n_SpType  [fg] Note on SpType (3)
          43  I1    ---     r_SpType  Reference for spectral type (6)
      45- 48  A4    ---     Var       [Yes ?] Variable?  (4)
          50  I1    ---     r_Var     ? Reference for variability (6)
          53  A1    ---     Grade     Grade (5)
      55- 57  A3    ---     Ref       References, separated by comma (6)

    Note (1): This source is designated as RX J0104.5-7121 in Haberl and Sasaki
         (2000A&A...359..573H) (subsection 6.4), but probably should be
         RX J0104.5-7221 according to its coordinate.
    Note (2): Spectral type of the optical counterpart.
          Be? indicates an emission line object catalogued in Meyssonnier and
              Azzopardi (1993, Cat. J/A+AS/102/451) or
              Murphy and Bessell (2000, Cat. J/MNRAS/311/741).
          SG  indicates a supergiant counterpart.
    Note (3): Notes on SpType:
           f: A point-like radio source is also located in the error circle,
              thus the possibility that it is an AGN remains (Haberl and
              Sasaki, 2000A&A...359..573H).
           g: X-ray emission may be attributable to an active corona (AC) of a
              late type star (Haberl & Sasaki, 2000A&A...359..573H).
    Note (4): For sources with the Yes sign, long-term X-ray variability
         has been found.
    Note (5): In table 5, we designate grade A and B sources as NH, and
        grade C and D sources as NHc. Grade E sources are not regarded as
        non-pulsating HMXBs (see subsubsection 6.2.1).
    Note (6): References are numbered as follows:
          1 = Haberl and Sasaki (2000A&A...359..573H)
          2 = Kahabka and Pietsch (1996A&A...312..919K)
          3 = Crampton et al. (1978ApJ...223L..79C)
          4 = Clark et al. (1978ApJ...221L..37C)
          5 = Whitlock and Lochner (1994ApJ...437..841W)
          6 = Wang and Wu (1992ApJS...78..391W)
          7 = this work
          8 = Filipovic et al. (2000A&A...353..129F)

    History:
        From electronic version of the journal
    ================================================================================
    (End)                                    Patricia Vannier [CDS]      22-Sep-2003