Description:

    The Galactic Plane Pulsar Snapshot (GPPS) survey project made with
    the Five-hundred-meter Aperture Spherical radio Telescope (FAST)
    provides the most sensitive piggyback spectra for tens of radio
    recombination lines (RRLs) at L band. We have processed the
    spectral data of RRLs, and obtained a sensitive averaged Hna RRL
    map for a sky area of 88 square degrees, covering the Galactic
    longitude from 33 to 55 degree and the Galactic latitude of |b| <
    2.0 degree. We detect 312 RRL components for 302 known HII regions
    in the studied Galaxy area. The related parameters have been
    collected from reference and calculated based on the piggyback
    spectral lines data of the FAST-GPPS survey.
    See Hou et al. SCMPA 65, 129703;  doi: 10.1007/s11433-022-2039-8

File Summary:
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  FileName   Lrecl  Records   Explanations
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ReadMe          86        .   This file
table3.dat      83      312   Hna RRL parameters for the known HII regions
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Byte-by-byte Description of file: table3.dat
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   Bytes Format Units    Label       Explanations
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   1- 13  A13   ---      HII-region  Source name
  15- 20  F6.3  deg      GLON        Galactic longitude
  22- 27  F6.3  deg      GLAT        Galactic latitude
  29- 32  I4    arcsec   Radius      Radius given in the WISE catalogue of HII regions 
  34- 38  F5.1  km/s     VLSR_ref    VLSR velocity measured in the reference (1)
  40- 41  I2    ---      Ref         Reference for VLSR_ref
  43- 47  F5.1  mJy/beam Peak        Fitted peak intensity by this work
  49- 51  F3.1  mJy/beam e_Peak      Uncertainty in Peak-intensity
  53- 57  F5.1  km/s     VLSR        Fitted VLSR by this work
  59- 62  F4.1  km/s     e_VLSR      Uncertainty in VLSR
  64- 67  F4.1  km/s     FWHM        Fitted line width by this work
  69- 72  F4.1  km/s     e_FWHM      Uncertainty in FWHM
  74- 78  F5.2  mJy/beam RMS         RMS value of the averaged RRL spectrum
  80- 83  F4.1  ---      S/N         Signal-to-noise ratio of the spectrum 
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Note (1): 
    Ref.1 : Anderson et al. 2011, ApJS, 194, 32
    Ref.2 : Anderson et al. 2015b, ApJS, 221, 26
    Ref.3 : Anderson et al. 2015a, ApJ, 810, 42
    Ref.4 : Anderson et al. 2018, ApJS, 234, 33
    Ref.5 : Araya et al. 2002, ApJS, 138, 63
    Ref.6 : Balser et al. 2011, ApJ, 738, 27
    Ref.7 : Bania et al. 2012, ApJ, 759, 96
    Ref.8 : Lockman 1989, ApJS, 71, 469
    Ref.9 : Lockman et al. 1996, ApJ, 472, 173
    Ref.10: Quireza et al. 2006, ApJS, 165, 338
    Ref.11: Sewilo et al. 2004, ApJS, 154, 553
    Ref.12: Watson et al. 2003, ApJ, 587, 714