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SMCSTARS2: Help

SMCSTARS2 - SMC H-alpha emission stars/nebulae


Overview

This database table contains a list of H-alpha emission-line stars and small nebulae in the Small Magellanic Cloud (SMC) that were discovered in an objective-prism survey. This survey was performed through an H-alpha + [N II] interference filter using the 0.90m Curtis Schmidt telescope at Cerro Tololo Inter-American Observatory (CTIO). 1898 emission-line objects were detected in the main body of the SMC, almost quadrupling the number of those discovered in previous objective-prism surveys of the same region. Among these 1898 objects are newly discovered planetary nebulae, compact H II regions, and late-type stars. Continuum intensities, the shapes and strengths of the H-alpha emission line, co-ordinates and (where available) cross-identifications are provided for the listed objects.

Catalog Bibcode

1993A&AS..102..451M

References

Meyssonnier N., Azzopardi M.
    <Astron. Astrophys. Suppl. Ser. 102, 451 (1993)>
    =1993A&AS..102..451M

Provenance

This version of the SMC H-alpha Emission-Line Stars and Small Nebulae Catalog of Meyssonnier and Azzopardi was created by the HEASARC in November 1997 based on the ADC/CDS machine-readable catalog J/A+AS/102/451.

Remarks on Particular Objects

Remarks on paticular objects (entries with the parameter Remark set to "Y"):
  Star    Remarks

    14  [OIII]-lines are visible on our blue-green grism plates
        (hereafter b-ggp)
    23  Hbeta and Hgamma emission-lines as well as [OIII]-lines are visible on
        our b-ggp
    29  Hbeta and Hgamma emission-lines as well as [OIII]-lines are visible on
        our b-ggp
    39  Hbeta and Hgamma emission-lines as well as [OIII]-lines are visible on
        our b-ggp
    43  Hbeta emission-line possibly visible on our b-ggp
    44  Hgamma emission-line and [OIII]-lines are visible on our b-ggp
    46  Hbeta emission-line noted by Feast et al. (1960); Hbeta and possibly
        Hgamma in emission  reported by Ardeberg & Maurice (1977)
    49  Hbeta and Hgamma emission-lines as well as [OIII]-lines are visible on
        our b-ggp
    51  K-M star; Halpha and Hbeta emission-lines confirmed by our medium
        resolution slit spectroscopy
    54  [OIII]-lines are visible on our b-ggp
    61  Hbeta and Hgamma emission-lines are visible on our b-ggp
    85  Hbeta emission-line is visible on our b-ggp
    90  part of N11 and L62
    91  part of N11 and L62
    98  [OIII]-lines are visible on our b-ggp
   101  northern part of NGC 248, L67 and DEM16
   103  southern part of NGC 248, L67 and DEM16
   104  [OIII]-lines are visible on our b-ggp
   133  nebulosity containing L78 and AV14
   149  Hgamma, Hdelta and Hepsilon in emission reported by Feast et al. (1960);
        star dominated by a very rich emission-line spectrum including among
        others hydrogen, FeII and [FeII] emission-lines (Zickgraf et al. 1986)
   152  Hbeta and Hgamma emission-lines as well as [OIII]-lines are visible on
        our b-ggp
   205  part of N26, L107 and DEM38; Hbeta emission-line and [OIII]-lines are
        visible on our b-ggp
   206  part of N26, L107 and DEM38; Hbeta emission-line and [OIII]-lines are
        visible on our b-ggp
   208  part of DEM38
   226  faint [OIII]-lines are visible on our b-ggp
   241  [OIII]-lines are visible on our b-ggp
   250  red star, Halpha to H8 emission-lines are visible on our medium
        resolution slit spectra
   254  Hbeta emission-line possibly visible on our b-ggp
   285  carbon star according to Rebeirot, Azzopardi & Westerlund (1993); Halpha
        and Hgamma emission-lines confirmed by our medium resolution slit
        spectroscopy
   290  [OIII]-lines are visible on our b-ggp
   297  very faint [OIII]-lines are visible on our b-ggp
   301  wide [OIII]-lines are visible on our b-ggp
   316  nebulosity containing VLE Nos. 5 and 6 found by Morgan (1984)
   317  part of DEM50; diffuse [OIII]-lines are visible on our b-ggp
   322  part of DEM50
   325  Hbeta and Hgamma emission-lines as well as strong [OIII]-lines are
        visible on our b-ggp
   371  Hbeta and Hgamma emission-lines as well as [OIII]-lines are visible on
        our b-ggp
   406  [OIII]-lines are visible on our b-ggp
   467  [OIII]-lines are visible on our b-ggp
   482  faint [OIII]-lines are visible on our b-ggp
   491  faint [OIII]-lines are visible on our b-ggp
   498  diffuse Hbeta emission-line possibly visible on our b-ggp
   518  Hbeta emission-line is visible on our b-ggp
   519  Hbeta and Hgamma emission-lines as well as [OIII]-lines are visible on
        our b-ggp
   547  part of N49
   548  part of N49
   642  carbon star according to Rebeirot, Azzopardi & Westerlund (1993);
        emission possibly visible on the Halpha line
   652  Hbeta and Hgamma emission-lines as well as [OIII]-lines are visible on
        our b-ggp
   696  southern part of DEM77
   699  northern part of DEM77
   700  [OIII]-lines are visible on our b-ggp
   739  Hgamma to H8 balmer emission-lines were noted by Azzopardi & Vigneau
        (1975); Hbeta to H13 as well as other lines whose FeII and [FeII]
        multiplets reported in emission by Azzopardi et al. (1981) and Zickgraf
        et al. (1989); Hbeta emission-line is confirmed by our b-ggp
   751  Hbeta emission-line is visible on our b-ggp
   771  Hbeta emission-line possibly visible on our b-ggp
   832  FeII and [FeII] emission-lines reported first by Feast (1968); VV Cephei
        confirmed, with a late K or early M-type component by Feast & Webster
        (1974), Sanduleak & Pesch (1981), and Walker (1983). Recent high
        resolution spectroscopy observation by Heydari-Malayeri & Leisy (1993)
   878  Hbeta emission-line possibly visible on our b-ggp
   891  [OIII]-lines are visible on our b-ggp
   905  Hbeta emission-line is visible on our b-ggp
   933  Hbeta and Hgamma emission-lines are visible on our b-ggp
   943  Hbeta emission-line and [OIII]-lines are visible on our b-ggp
   966  carbon star according to Rebeirot, Azzopardi & Westerlund (1933);
        emission possibly visible in the Halpha line, while Hbeta line is
        visible in absorption on our medium resolution slit spectrum
   999  [OIII]-lines are visible on our b-ggp
  1011  strong [OIII]-lines are visible on our b-ggp
  1017  narrow Hbeta emission-line is visible on our b-ggp
  1046  Hbeta emission-line is visible on our b-ggp
  1049  emission-line object within N62 and DEM93
  1071  Hbeta and Hgamma emission-lines as well as [OIII]-lines are visible on
        our b-ggp
  1088  Hbeta and Hgamma emission-lines as well as [OIII]-lines are visible on
        our b-ggp
  1091  Hbeta emission-line and [OIII]-lines are visible on our b-ggp
  1136  Hbeta and Hgamma emission-lines as well as [OIII]-lines are visible on
        our b-ggp
  1149  Hbeta, Hgamma and Hdelta emission-lines were noted by Feast et al.
        (1960) sharp Hgamma line in emission reported by Azzopardi & Vigneau
        (1975)
  1271  nucleus of N72 and DEM112
  1274  part of N72 and DEM112
  1280  possible VLE within DEM111
  1303  Hbeta emission-line is visible on our b-ggp
  1304  Hbeta emission-line possibly visible on our b-ggp
  1321  Hbeta emission-line possibly visible on our b-ggp
  1344  Hbeta emission-line is visible on our b-ggp
  1350  star within DEM119
  1357  [OIII]-lines are visible on our b-ggp
  1365  Halpha and Hbeta emission-lines confirmed by our medium resolution slit
        spectroscopy
  1443  narrow Hbeta emission-line possibly visible on our b-ggp
  1454  Hbeta and Hgamma emission-lines as well as [OIII]-lines are visible on
        our b-ggp
  1508  part of DEM126
  1512  part of DEM126; faint and extended [OIII]-lines are visible on our b-ggp
  1514  part of DEM126
  1520  part of DEM126
  1522  faint and extended [OIII]-lines are visible on our b-ggp
  1536  nucleus of DEM129
  1552  Hbeta, Hgamma and Hdelta emission-lines reported by Feast et al. (1960)
  1625  Hbeta in emission and Hgamma filled in by emission reported by Feast et
        al. (1960), and Ardeberg & Maurice (1977)
  1663  object within N80A
  1676  [OIII]-lines are visible on our b-ggp
  1677  Hbeta and Hgamma in emission reported by Feast et al. (1960)
  1682  faint [OIII]-lines are visible on our b-ggp
  1687  part of N81 and DEM138
  1688  nucleus of N81 and DEM138
  1709  Hbeta emission-line and [OIII]-lines are visible on our b-ggp
  1714  [OIII]-lines are visible on our b-ggp
  1721  Hbeta emission-line is visible on our b-ggp
  1752  Hbeta emission-line possibly visible on our b-ggp
  1755  Hbeta emission-line is visible on our b-ggp
  1759  Balmer and [FeII] emission-lines among others reported by
        Heydari-Malayeri (1990)
  1773  part of DEM147
  1783  part of DEM147
  1790  bright part of NGC460 and DEM151
  1792  compact HII region within NGC460
  1794  bubble within NGC460
  1795  part of DEM152
  1796  Hbeta emission-line and [OIII]-lines are visible on our b-ggp
  1797  part of DEM152
  1819  narrow Hbeta emission-line is visible on our b-ggp
  1820  Hbeta emission-line is visible on our b-ggp
  1843  Hbeta emission-line is visible on our b-ggp
  1858  carbon star according to Rebeirot, Azzopardi & Westerlund (1993); Halpha
        and Hbeta emission-lines confirmed by our medium resolution slit
        spectroscopy. Symbiotic star according to high resolution
        spectroscopy by van Winckel (1993)
  1884  Hbeta and Hgamma emission-lines as well as [OIII]-lines are visible on
        our b-ggp

Parameters

Name
The Source designation derived from the catalog running number (catalog_number) which increases in order of the 2000 equinox RA and the IAU standard designation for this catalog of MA93.

RA
The right ascension in the default equinox (given to the nearest tenth of a second of time in the original catalog).

Dec
The declination in the default equinox (given to the nearest arcsecond in the original catalog).

LII
The galactic longitude of the object.

BII
The galactic latitude of the object.

Catalog_Number
The catalog running number: this increases with Right Ascension (2000).

Catalog_Number_Flag
A colon (:) or a double colon (::) indicates that the Halpha emission-line nature of the object, mainly due to its severe faintness or because it is a late-type star, is doubtful or very doubtful, respectively.

Slit_Spectra
A flag indicating the availability of slit spectra: "S" means that subsequent medium resolution spectroscopic observations were obtained by the authors of the catalog, while "O" indicates that previous spectroscopic observations were reported by others, viz.:

     - Aller, Keyes, Ross & O'Mara B.J. 1981, MNRAS, 194, 613
     - Ardeberg & Maurice 1977, A&AS, 30, 261
     - Azzopardi & Breysacher 1979, A&A, 75, 120
     - Azzopardi, Breysacher & Muratorio 1981, A&A, 95, 191
     - Barlow 1987, MNRAS, 227, 161
     - Boroson & Liebert 1989, ApJ, 339, 244
     - Feast, Thackeray & Wesselink 1960, MNRAS, 121, 337
     - Heydari-Malayeri 1990, A&A, 234, 233
     - Heydari-Malayeri & Leisy 1993, in preparation
     - Meatheringham & Dopita 1991a, ApJS, 75, 407
     - Meatheringham & Dopita 1991b, ApJS, 76, 1085
     - Monk, Barlow & Clegg 1988, MNRAS, 234, 583
     - Russell & Dopita 1990, ApJS, 74, 93
     - Webster 1976, MNRAS, 174, 573
     - Westerlund, Azzopardi, Breysacher & Rebeirot 1991, A&AS, 91, 425
     - Winckel van, Duerbeck & Schwarz 1993, A&AS, 102, 401
     - Zickgraf, Wolf, Stahl, Leitherer & Appenzeller 1986, A&A, 163, 119
     - Zickgraf, Wolf, Stahl & Humphreys 1989, A&A, 220, 206
  

Relative_Intensity
A Rough estimate of the relative intensity of the H-alpha line obtained from the measurement of the optical density (0 - 5) of the emission-line peak on the digitized image of the 4-hour exposure objective-prism plate.

Spectrum_ID
A three digit code describing the spectrum based on the authors' visual scrutiny of their deepest objective-prism plate. The meaning of the three digits describing the spectrum is as follows:

     (a) the first digit refers to the relative intensity of the continuum quoted
         on a scale from 1 (faint) to 5 (overexposed), where "2-3" is an optimum
         exposure; the additional symbol "T" denotes that a trace of continuum is
         barely visible above the sky background on the plate, while an
         intensity "0" indicates that the particular object does not show
         any continuous spectrum underlying the emission-lines;
     (b) the second digit refers to the relative strength of the H-alpha
         emission-line estimated on a scale from 1 to 5, in which "1" represents
         a very weak line and "5" a very strong line;
     (c) the third digit refers to an estimate of the width of the H-alpha
         emission-line feature, where "1" denotes a sharp line, "2" a line
         appreciably widened, and "3" a line which is diffuse to very diffuse.
  

Type_Flag
A code indicating the nature or possible nature (:) of the object according to the following scheme:

     1  =  H II region or filament
     2  =  supernova remnant
     3  =  bubble or loop
     4  =  compact or small HII region
     5  =  Planetary Nebula (PN) or PN candidate (:)
     6  =  Very-Low-Excitation (VLE) object or VLE candidate (:)
     7  =  Wolf-Rayet star
     8  =  Peculiar H-alpha emission-line star with Fe II and [Fe II] emission
     9  =  Late-type star with emission or suspected emission in the H-alpha line
  

Cross_ID
This field contains information on cross-identifications and/or the star's location with respect to the SMC cluster system. The cross-identifications are given by a letter abbreviation followed by the number assigned by the respective authors who identified the object. The cluster information refers to the star's location in connection to the SMC cluster system: a given star may lie either within a cluster or in its nearby surrounding field, but that, of course, does not necassarily imply cluster membership. The name of the SMC cluster is given by a letter abbreviation (codes beginning B, H, HW, K, LN, and NGC) followed by the number assigned by the author who previously found the object. The following codes are used for the cross-identifications and cluster designations:

      AB    Azzopardi & Breysacher 1979, A&A, 75, 120
      ARP   Arp 1959, AJ, 64, 254
      AV    Azzopardi & Vigneau 1982, A&AS, 50, 291
      B     Bruck 1976, Occas. Rep. R. Obs. Edinburgh, No 1
      DEM   Davies, Elliott & Meaburn 1976, Mem.RAS, 81, 79
      H     Hodge 1986, PASP, 98, 1113
      HW    Hodge & Wright 1974, AJ, 79, 858
      J     Jacoby 1980, ApJS, 42, 1
      K     Kron 1956, PASP, 68, 125
      L     Lindsay 1961, AJ, 66, 169
      LN    Lindsay 1958, MNRAS, 118, 172
      MG    Morgan & Good 1985, MNRAS, 213, 491
      MN    Morgan 1992, MNRAS, 258, 639
      MO    Morgan 1984, MNRAS, 209, 241
      N     Henize 1956, ApJS, 2, 315 (emission nebulae)
      NGC   Dreyer 1888, Mem.RAS, XLIX
      PMMR  Prevot, Martin, Maurice, Rebeirot & Rousseau 1983, A&AS, 53, 255
      R     Feast, Thackeray & Wesselink 1960, MNRAS, 121, 337
      RAW   Rebeirot, Azzopardi & Westerlund 1993, A&AS, 97, 603
      S     Henize 1956, ApJS, 2, 315 (emission-line stars)
      SA    Sanduleak 1968, AJ, 73, 246
      SK    Sanduleak 1989, AJ, 98, 825
      SMP   Sanduleak, McConnel & Philip 1978, PASP, 90, 621
      SP    Sanduleak & Pesch 1981, PASP, 93, 431
  
Note that Lindsay (1961) did not provide finding charts for several emission objects listed in his catalogue, thus their identification was possible only with the help of their coordinates. When Lindsay's coordinates for an object do not match the co-ordinates in this catalog adequately, the Lindsay cross-identification "L" number is followed by a colon.

Remark
A flag that is set to "Y" if there is a remark for the particular object. See the section Remarks_on_particular_objects for the remarks.

Class
Browse classification based on the parameter type_flag. Notice that VLE or possible VLE objects have been classed as "unidentified".


Contact Person

Questions regarding the SMCSTARS2 database table can be addressed to the HEASARC User Hotline.
If you have any problems, please consult the help page or mail ledas-help@star.le.ac.uk
 
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