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J/A+AS/133/181      BVI imaging of 20 irregular galaxies    (Makarova+ 1998)
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CCD imaging of twenty nearby isolated irregular galaxies
       Makarova L., Karachentsev I.D.
      <Astron. Astrophys. Suppl. Ser. 133, 181 (1998)>
      =1998A&AS..133..181M      (SIMBAD/NED BibCode)
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ADC_Keywords: Galaxies, photometry ; Photometry, CCD
Keywords: galaxies: distances - galaxies: stellar content -
          galaxies: dwarf; irregular

Abstract:
    We present B, V and I CCD stellar photometry for a sample of 20 field
    irregular dwarf galaxies. Their corrected radial velocity is
    V_0_<500km/s. Most of them have been resolved into stars for the first
    time. Based on photometry of their brightest blue stars we have
    derived the following distances: 5.9Mpc (UGC 685), 5.4Mpc (UGC 1281),
    7.2Mpc (UGC 3303), 7.0Mpc (UGC 3476), 7.3:Mpc (UGC 3600), 7.2:Mpc
    (UGC 3698), 7.9Mpc (NGC 2337), 8.6Mpc (UGC 3817), 5.7Mpc (UGC 3860),
    5.6Mpc (UGC 4426), >=7.9Mpc (F 565-v1), 7.4:Mpc (UGC 5086), 7.1Mpc
    (UGC 5272), 5.9Mpc (UGC 5340), 7.1Mpc (UGC 5427), 2.7:Mpc (UGC 5456),
    6.6Mpc (NGC 3274), 9.3Mpc (UGC 5889), 5.2Mpc (NGC 5238), and 8.0Mpc
    (UGC 9405). Our sample exhibits diverse morphological properties
    evidently caused by their different starburst activity. The galaxy
    sample has a median integral absolute magnitude M_B_=-14.6 and a
    median integral colour (B-V)_T_=+0.47. One dwarf, UGC 5340, stands out
    by its very blue colour, (B-V)_T_=+0.18, and by its high M(HI)/L
    ratio, as expected for young galaxies. Four objects of the sample are
    IRAS sources. Being well isolated systems, the considered galaxies may
    be used to estimate a local value of the Hubble parameter, H=V_0_/D.
    For half of the sample galaxies their individual H- values are
    concentrated within [58-68]km/s/Mpc with a median of 65km/s/Mpc.

File Summary:
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  FileName      Lrecl  Records   Explanations
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ReadMe             80        .   This file
list.dat           24       16  *List of galaxies
tab2-8.dat         39      424   VI photometry
tab9-17.dat        39      402   BV photometry
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Note on list.dat: positions of galaxies added, from SIMBAD data-base
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See also:
   J/A+AS/128/459 : BV photometry of irregular galaxies (Makarova+ 1998)
   J/A+AS/124/559 : VI photometry of dwarf galaxies (Karanchentsev+ 1997)

Byte-by-byte Description of file: list.dat
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   Bytes Format Units   Label     Explanations
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   1-  2  I2    h       RAh       Right Ascension J2000 (hours)
   4-  7  F4.1  min     RAm       Right Ascension J2000 (minutes)
       9  A1    ---     DE-       Declination J2000 (sign)
  10- 11  I2    deg     DEd       Declination J2000 (degrees)
  13- 14  I2    arcmin  DEm       Declination J2000 (minutes)
  17- 24  A8    ---     Gal       Galaxy name
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Byte-by-byte Description of file: tab2-8.dat
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   Bytes Format Units   Label     Explanations
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   1-  8  A8    ---     Gal       Galaxy name
  10- 12  I3    ---     Star      Star number
  14- 17  I4    pix     Xpos      Rectangular coordinate of stars (1)
  19- 22  I4    pix     Ypos      Rectangular coordinate of stars (1)
  24- 28  F5.2  mag     Vmag      V magnitude
  30- 34  F5.2  mag     V-I       (V-I) colour index
  36- 39  F4.1  ---     SHAR      Sharpness parameter of stars (2)
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Note (1): The upper right corner corresponds to X=0, Y=0 of the frame
           coordinates, i.e. X increases to East and Y to South.
Note (2): SHAR is a measure of the difference between the observed width of
           the object and the width of the psf model.
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Byte-by-byte Description of file: tab9-17.dat
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   Bytes Format Units   Label     Explanations
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   1-  8  A8    ---     Gal       Galaxy name
  10- 12  I3    ---     Star      Star number
  14- 17  I4    pix     Xpos      Rectangular coordinate of stars (1)
  19- 22  I4    pix     Ypos      Rectangular coordinate of stars (1)
  24- 28  F5.2  mag     Vmag      V magnitude
  30- 34  F5.2  mag     B-V       (B-V) colour index
  36- 39  F4.1  ---     SHAR      Sharpness parameter of stars (2)
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Note (1): The upper right corner corresponds to X=0, Y=0 of the frame
           coordinates, i.e. X increases to East and Y to South.
Note (2): SHAR is a measure of the difference between the observed width of
           the object and the width of the psf model.
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Acknowledgements: Sazonova Lida <lsaz@sao.ru>
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(End)                                         Patricia Bauer [CDS]   25-May-1998