ACDS V10.0 - Detailed Description of J/MNRAS/260/77

ACDS V10.0 - Sun Jan 19 14:06:06 CET 2025

| # Detailed Description of J/MNRAS/260/77 : ROSAT Wide Field Camera EUV Bright Sources (Pounds+ 1993) |

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/MNRAS/260/77    ROSAT Wide Field Camera EUV Bright Sources (Pounds+ 1993)
    ================================================================================
    The ROSAT Wide Field Camera all-sky survey of extreme-ultraviolet sources -
    I. The Bright Source Catalogue
         Pounds K.A., et al.
        <Mon. Not. R. Astron. Soc. 260, 77 (1993)>
        =1993MNRAS.260...77P
    ================================================================================
    ADC_Keywords: X-ray sources

    Description (Summary):
        Table 1 gives the coordinates (equinox J2000.0) of 384 bright EUV
        sources detected in the WFC survey. These should be referred to,
        according to the IAU convention, by the suitably truncated RA and Dec.
        Thus, the first source in the Table is RE J0003+433, a ROSAT EUV
        source at 00h 03m and +43deg 35'. Count rates and 1sigma errors are
        given for each of the survey filters, in counts per kilosecond. Upper
        limits are indicated by "-" in the error column and are 3sigma above
        the local background.

    File Summary:

           FileName      Lrecl  Records   Explanations

    ×                   80        .   This file
    × ReadMe            80        .   This file
    × table1           129      498   The Bright Source Catalogue

    Byte-by-byte Description of file:  table1

       Bytes Format  Units   Label    Explanations

       2-  3  I2     h       RAh      Right Ascension J2000 (hours)
       5-  6  I2     min     RAm      Right Ascension J2000 (minutes)
       8- 11  F4.1   s       RAs      Right Ascension J2000 (seconds)
          13  A1     ---     DE-      Declination J2000 (sign)
      14- 15  I2     deg     DEd      Declination J2000 (degrees)
      17- 18  I2     arcmin  DEm      Declination J2000 (minutes)
      20- 21  I2     arcsec  DEs      Declination J2000 (seconds)
      23- 27  I5     ct/ks   S1a      ?Count rates in filter S1 (90-206eV)
      29- 31  I3     ct/ks   e_S1a    ?mean error on S1a
      33- 37  I5     ct/ks   S2a      ?Count rates in filter S2 (62-110eV)
      39- 41  I3     ct/ks   e_S2a    ?mean error on S2a
      43- 57  A15    ---     Name1    Possible counterpart (1)
      59- 70  A12    ---     Name2    Possible counterpart (1)
      72- 87  A16    ---     Type     Counterpart type
      90- 93  F4.1   mag     Mag      ?Counterpart magnitude
          94  A1     ---     n_Mag    Note on the Counterpart magnitude
      96-115  A20    ---    Comments  See Note (2)
     117-119  I3     arcsec  R90      ?90%-confidence position error circle radius
     121-123  I3     arcsec  DR       ?Counterpart offset from EUV source position
     125-127  A3     ---     Cat      Catalogue from which the counterpart position
                                        was taken
         129  A1     ---     Rem      'R' for Notes (see below)

    Note (1):
        Information on possible counterparts within the 99.9% WFC position
        error circle is given. The first counterpart listed is thought to be
        the most likely identification from the information available in
        existing catalogues and optical follow up work on some sources (Mason
        et al., 1992). Extensive use was made of the CDS SIMBAD database,
        particularly for obtaining information on multiple names for objects.
        Two names are usually given for the first counterpart; normally a
        common or variable star name, followed by an HD or WD (McCook and
        Sion, 1987) number, where available. One name is generally given for
        other objects within the 99.9% error circle. Information on many of
        the object names used here can be found in Fernandez et al.
        (1983). Object types for the counterparts are given; spectral type
        classifications for the same object, but from different catalogues,
        are all listed, separated by slashes. For more detailed and accurate
        spectral type classifications for active binaries, see Strassmeier et
        al. (1988). The magnitudes of the counterparts are given (usually in
        the V-band unless B magnitudes are indicated by a "B"). They are meant
        only as a rough guide, since they are drawn from a variety of
        catalogues, and many of these objects are optically variable. It is
        important to note that visual or spectroscopic binary companions can
        rarely be ruled out as the source of EUV emission.
    Note (2):
        The column headed "comments" contains information regarding the
        counterparts as detailed below:
        E: Exosat detection within WFC error circle.
        I: IUE target within WFC error circle (not necessarily a detection).
        pm: High proper motion star, from the Luyten catalogue of stars with
            proper motions >0.5 arcseconds per year (Luyten, 1976).
        N: Nearby stars, from the Gliese and Jahreiss (1969,1979,1991) catalogues.
        A: Active star or star system (mostly from the Strassmeier et al.
            catalogue of chromospherically active binary stars). The "A" flag
            is not given for RS CVn and BY Dra systems, or where the spectral
            type indicates emission (e.g. dMe).
        (B): The most probable counterpart is a known binary, or has one or more
            sources nearby, within the error circle, with the same name, but a
            different qualifying letter at the end, usually implying a visual
            binary or multiple star system. The source(s) of EUV emission are not
            always clear in these cases.
        V*: Variable star, from the general catalogue of variable stars (GCVS),
             either directly or via the SIMBAD database.
        EI: Einstein IPC detection within WFC error circle.
        H: Einstein HRI detection within WFC error circle.
        N(H)= Interstellar hydrogen absorption column, in units of 10^20 cm-2,
            estimated from the maps of Stark et al. (1992; available for
            delta> -40deg) for extragalactic counterparts within the error
            circles. Generally we do not expect to detect extragalactic sources
            through a column greater than N(H)~2.
        (C): Designates another counterpart in the error circle, which has the
            same name, but different extension letter to the first counterpart.
        b: Blue star, generally from the master list of non-stellar sources (Dixon,
            1970), or from references given in the SIMBAD database.
        HEAO: HEAO-A1 detection (Wood et al., 1984).
        IDP: ROSAT WFC optical identification programme (Mason et al., 1992) with
            activity/non-activity represented by "A" and "nonA" respectively.
            "IDPn" indicates no identification yet found from spectroscopic search
            of EUV error circle. The final three columns in Table 1 give the WFC 90%
            confidence position error circle radius (arcsecs); the counterpart
            offset from the EUV source position (arcsecs), and the catalogue from
            which the counterpart position was taken. Sources for which there is
            note below are marked with a "R" symbol at the end of the entry. The
            catalogue names are abbreviated as listed below (following notes on
            individual sources).
    Notes on individual sources ('R' in column 129):

    RE 0044+093: New fast rotating single star radio source
                 (Bromage et al., in preparation).

    RE 0116-022: AY Cet is an active close binary with a WD companion
                 (Strassmeier et al., 1988) and a 57 day orbit. The WD
                 is not expected to contribute to the EUV flux.

    RE 0415-073: 40 Eri emission was resolved with the Einstein HRI, most emission
                 coming from 40 Eri C, the dMe flare star (Cash et al., 1980).
                 All three components could be contributing to the EUV flux.

    RE 0447-275: Identification is with a newly discovered dMe star, the fainter
                 companion of a close visual pair; this has subsequently been
                 discovered to be a flare star (Bromage, 1992).

    RE 0515+324: Identified with a white dwarf, coincident with the 8th magnitude,
                 A2/F4V star HD 33959C. An IUE SWP spectrum of this star shows
                 a rise towards short wavelengths, indicative of a hot white dwarf
                 companion (Hodgkin et al., 1992). Other catalogued stars in
                 the WFC error circle include the 5th magnitude A9IV star KW Aur,
                 and the 11th magnitude star BD+32 922B, which are both
                 unlikely to contribute to the detected EUV flux.

    RE 0532-030: Star identified may be HBC97 (dKe) but this association is
                 uncertain because of position discrepancies.

    RE 0604-343: The S2 filter count rate was enhanced by a flare; this is a new
                 dMe flare star. See Bromage (1992).

    RE 0604-482: HD 41824 is a very close visual binary. Star A (G? V) has no
                 reported variations in radial velocity or photometry whereas star
                 B (G6V) has variable RV and photometric variability. Following
                 the IDP discovery of chromospheric activity (Mason et al., 1992)
                 it seems very likely that star B is the EUV emitter and is
                 probably an SB1 RSCVn binary.

    RE 0631+500: The dMe star discovered in the optical identification programme
                 now appears (but not named) in the latest version of the Gliese
                 catalogue (1991) as an M0 star with V=11.09 mag.

    RE 0734+315: YY Gem is an eclipsing binary double-flare star. The S2 filter
                 count rate was enhanced by a flare event on 1990 Oct 03
                 (Bromage, 1992).

    RE 0751+144: Identified as new intermediate polar system (Mason et al., 1992b).

    RE 0827+284: Identified with the hot, evolved star PG 0824+289, classified as a
                 subdwarf in the Palomar Green survey
                 (Green et al., 1986 - hereafter PG), and more recently shown to
                 be a hot DA white dwarf (Sansom et al., 1992).

    RE 0838-430: This WFC detection is part of the Vela SNR. There is also a 9th
                 magnitude K giant in the WFC error circle, which is likely to be
                 a chance coincidence.

    RE 1016-052: This is a newly discovered Feige-24 type DA+dMe binary
                 (Jomaron et al., 1992).

    RE 1043+445: Identified with the hot, evolved star PG 1040+451, classified as a
                 hot subdwarf (sdB) in the PG survey and more recently shown to be
                 a possible hot DA white dwarf (Sansom et al., 1992). Because of
                 the low signal-to-noise data the optical classification of this
                 star is still uncertain, as indicated by the colon after the
                 spectral type in table 1.

    RE 1104+381: Identified with the BL Lac object Mrk 421. The DC white dwarf also
                 in the EUV source error circle is probably too cool to be detected.

    RE 1111-224: Positionally coincident with the 4th magnitude, A2 IV star beta
                 Crt, the likely source of EUV emission has been shown to be a
                 DA white dwarf companion beta Crt B (Fleming et al., 1991),
                 which is a spectroscopic binary companion to beta Crt.

    RE 1149+284: Identified as probable new AM Her system (Mittaz et al., 1992).

    RE 1236+475: Identified with the hot, evolved star PG 1234+482, classified as a
                 hot subdwarf (sdOB) in the PG survey, and more recently shown to
                 be a hot DA white dwarf (Jordan et al., 1991, Sansom et al., 1992).

    RE 1255+255: The variable star IN Com, within the WFC error circle, is very
                 close to the centre of the planetary nebula LT5. IN Com is a
                 triple system consisting of an 8.7th magnitude, G5 III star with
                 active chromosphere and a low mass, binary companion, plus an
                 outer, hot subdwarf (Malasan et al., 1991). The G star is the
                 most likely source of EUV emission, but emission from the other
                 components cannot be ruled out.

    RE 1307+535: Identified as probable new AM Her system, with the shortest known
                 period in the class (Osborne et al., 1992).

    RE 1428+424: Identified with a BL Lac; first seen by HEAO-1 and later optically
                 identified by Remillard et al. (1989).

    RE 1603-574: iota Nor consists of a group of several 5th magnitude mid-A
                 stars within approx 2 arcsec (SAO 243279: IDS 15554-1570AB). The
                 star SAO 243278 (IDS 15554-1570C) approximately 10 arcsec away has
                 now been shown to be a 6-day period double-lined spectroscopic
                 binary active G star and candidate RSCVn binary (Bromage, 1992).

    RE 1625-490: The optical identification has been made independently by
                 Cutispoto et al. (1992) from an optical follow up programme of
                 serendipitous EXOSAT sources; the object does not show any
                 evidence of binarity.

    RE 1629+780: This is a newly discovered Feige-24 type DA+dMe binary (Cooke et
                 al., 1992).

    RE 1800+683: Identified with the hot, evolved star KUV 18004+6836, classified
                 as a hot subdwarf (sdB) by Wegner et al. (1987), and more recently
                 shown to be a hot DA white dwarf (Sansom et al., 1992).

    RE 1833+514: The famous prototype of the BY Dra class of spotty active stars;
                 the S2 flux was enhanced by a flare (Barstow et al., 1991).

    RE 1938-461: Identified as new AM Her system (Buckley et al., 1992).

    RE 2045-312: AU Mic, a well known flare star. The S1 flux was enhanced by a
                 flare (Bromage, 1992).

    RE 2047-363: A newly discovered very fast rotating single dwarf star, nicknamed
                 "Speedy Mic" (Bromage et al., 1992). The S2 flux was enhanced by
                 a long-lived flare, and variability of activity occurred in
                 both filters.

    RE 2147-160:delta Cap: the visual companions of this 3rd magnitude peculiar A
                 star binary have been ruled out as possible EUV counterparts by
                 CCD photometry and high-resolution spectroscopy, leaving the
                 likely counterpart as the hidden binary companion of delta Cap
                 itself (probably a mildly active late type star).
                 (Wonnacott et al., 1992).

    RE 2157-505: Gliese B41A: newly identified as an SB2 binary dMe flare star; the
                 common proper-motion WD companion is too cool to contribute to
                 the EUV flux, but the derived age of the system makes G1841A one
                 of the oldest known active star systems
                 (Jeffries and Bromage, 1992).

    RE 2246+442: The well-known flare star EV Lac. Both S1 and S2 filter fluxes
                 were enhanced by flares during the survey coverage (Bromage, 1992).

    See also:
        J/ApJS/93/569  : the first EUVE Catalog (Bowyer et al. 1994)
        II/203         : the second EUVE Catalog (Bowyer et al., 1996)
        J/MNRAS/274/1165 : the 2RE Catalog (Pye et al. 1995)
        J/A+AS/114/465 : the ROSAT XUV Pointed Phase Source Catalog
                         (Kreysing et al. 1995)

    Acknowledgments:
       Thanks are due to Dr Mike Watson for e-mailing the LaTeX files.
       "DeTeX" was performed at CDS, and the insertion of the 'J' for
       truncated IAU-style designation was added in the text.
    ================================================================================
    (End)                                    Francois Ochsenbein [CDS]   29-May-1993