Access to Astronomical Catalogues

J/ApJS/196/12         First results from Mopra HCO+ maps       (Barnes+, 2011)
The Galactic census of high- and medium-mass protostars.
I. Catalogs and first results from Mopra HCO+ maps.
    Barnes P.J., Yonekura Y., Fukui Y., Miller A.T., Muhlegger M., Agars L.C.,
    Miyamoto Y., Furukawa N., Papadopoulos G., Jones S.L., Hernandez A.K.,
    O'Dougherty S.N., Tan J.C.
   <Astrophys. J. Suppl. Ser., 196, 12 (2011)>
   =2011ApJS..196...12B
ADC_Keywords: Galactic plane ; Molecular clouds ; Interstellar medium ;
              Velocity dispersion
Keywords: astrochemistry - ISM: kinematics and dynamics - ISM: molecules -
          radio lines: ISM - stars: formation

Abstract:
    The Census of High- and Medium-mass Protostars (CHaMP) is the first
    large-scale, unbiased, uniform mapping survey at sub-parsec-scale
    resolution of 90GHz line emission from massive molecular clumps in the
    Milky Way. We present the first Mopra (ATNF) maps of the CHaMP survey
    region (300°>l>280°) in the HCO+J=1->0 line, which is
    usually thought to trace gas at densities up to 1011m-3. In this
    paper, we introduce the survey and its strategy, describe the
    observational and data reduction procedures, and give a complete
    catalog of moment maps of the HCO+J=1->0 emission from the ensemble
    of 303 massive molecular clumps. From these maps we also derive the
    physical parameters of the clumps, using standard molecular
    spectral-line analysis techniques.

Description:
    CHaMP began with complete surveys of a large portion of the southern
    Galactic Plane in four molecular spectral lines in the 3mm waveband
    made with the 4m Nanten telescope (see Figure 1). A higher-resolution
    follow-up campaign was then begun to map 209 clumps from the Nanten
    Master Catalogue (NMC) in a number of 3mm molecular transitions with
    the 22m diameter Mopra dish of the Australia Telescope National
    Facility (ATNF) over the period 2004-2007, at much higher sensitivity
    and angular resolution than with Nanten.

File Summary:

       FileName      Lrecl  Records   Explanations

ReadMe            80        .   This file
table1.dat        43      209   Nanten Master Catalogue (NMC)
table4.dat       122      318   Mopra HCO+J=1->0 observed parameters
table5.dat        90      303   Mopra clump physical parameters (for Tex=10K)


See also:
 J/ApJS/195/14  : The Bolocam Galactic Plane Survey (BGPS). V. (Schlingman+,
                  2011)
 J/PASJ/62/557  : CO clouds in the Galactic Center from NANTEN (Takeuchi+, 2010)
 J/ApJ/707/283  : Ionized gas toward molecular clumps (Johnston+, 2009)
 J/ApJS/182/131 : Molecular clouds and clumps in the GRS (Rathborne+, 2009)
 http://www.astro.ufl.edu/~peterb/research/champ/ : The Galactic Census of
                  High and Medium-mass Protostars (CHaMP) home page


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

   Bytes Format Units   Label   Explanations

   1-  3  I3    ---     BYF     [1/209] BYF number (<[BYF2011] NNN> in Simbad)
       4  A1    ---     f_BYF   [*] *: Nanten clump that was mapped at Mopra
                                (see Table 4)
   6- 13  F8.4  deg     GLON    Galactic longitude
  15- 21  F7.4  deg     GLAT    Galactic latitude
  23- 28  A6    ---     Meth    Method of clump identification (1)
  30- 33  F4.2  K       Tpk     Peak temperature
  35- 40  F6.2  km/s    Vlsr    LSR velocity
  42- 43  A2    ---     Reg     Region (2)

Note (1): Methods of clump identification are:
  CF     = from the CLUMPFIND program operating on the Nanten C18O data cube
           (see Y. Yonekura et al. 2011, in preparation)
  C18O = from visual inspection of the C18O Nanten data cube
  HCO+ = from visual inspection of the HCO+ Nanten data cube
Note (2): Grouping of sources by Region is for convenience of mapping only;
          see Figure 2 and Section 3.1. Some of these sources were too isolated
          to be conveniently grouped into regions.


Byte-by-byte Description of file: table4.dat

   Bytes Format Units    Label   Explanations

   1-  3  I3    ---      BYF     [1/209]  BYF number
       4  A1    ---      m_BYF   sub-clump letter (1)
   6- 12  F7.3  deg      GLON    ? Galactic longitude
  14- 19  F6.3  deg      GLAT    ? Galactic latitude
      20  A1    ---      f_BYF   [N] N: no HCO+ emission could be discerned
                                 in the Mopra data cubes at or near the
                                 nominal NMC coordinates
  22- 26  F5.2  K.km/s   WHCO+   ? HCO+(J=1-0) integrated intensity
                                   W(HCO+)=∫(T*RdV)
  28- 31  F4.2  K.km/s  e_WHCO+  ? rms uncertainty on WHCO+
  33- 34  I2    ---      NT*     ? Noise level on WHCO+ (when no detection)
  36- 40  F5.1  km/s     bVel    Lower velocity range
  42- 47  F6.2  km/s     BVel    Upper velocity range
  49- 52  F4.2  K        Tp      ? Peak brightness temperature
  54- 57  F4.2  K        e_Tp    ? Tp uncertainty
  59- 60  I2    ---      NTp     ? Noise level on Tp (when no detection)
  62- 67  F6.2  km/s     Vlsr    ? LSR velocity
  69- 72  F4.2  km/s     e_Vlsr  ? Vlsr uncertainty
  74- 77  F4.2  km/s     SigV    ? Velocity dispersion
  79- 82  F4.2  km/s     e_SigV  ? SigV uncertainty
      84  A1    ---      l_amaj  Limit flag on amaj
  85- 87  I3    arcsec   amaj    ? Major axis size
  89- 90  I2    arcsec   e_amaj  ? amaj uncertainty
      92  A1    ---      l_bmin  Limit flag on bmin
  93- 95  I3    arcsec   bmin    ? Minor axis size
  97- 98  I2    arcsec   e_bmin  ? bmin uncertainty
 100-102  I3    deg      PA      ? Position angle
     104  I1    deg      e_PA    ? PA uncertainty
 106-108  F3.1  kpc      Dcl     Clump distance (2)
 110-112  F3.1  kpc      e_Dcl   Dcl uncertainty
 114-117  F4.2  kpc      Dkn     ? Near kinematic distance using Reid et al.
                                 2009ApJ...700..137R
     118  A1    ---      ---     [/]
 119-122  F4.2  kpc      Dkf     ? Far kinematic distance using Reid et al.
                                 2009ApJ...700..137R

Note (1): Here we have added letter suffixes to the NMC catalog numbers to
          indicate how the higher-resolution Mopra beam breaks up the emission
          in the Nanten maps into smaller sub-clumps.
Note (2): Distances from the literature (Grabelsky et al. 1988ApJ...331..181G;
          Yonekura et al. 2005ApJ...634..476Y; Stolte et al.
          2006AJ....132..253S) using various classical optical or kinematic
          methods (see Y. Yonekura et al. 2011, in preparation).


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

   Bytes Format Units     Label   Explanations

   1-  3  I3    ---       BYF     [1/209] BYF number
       4  A1    ---       m_BYF   sub-clump letter
   6-  8  F3.1  kpc       Dist    Final distance
       9  A1    ---       f_Dist  [cnt] Flag on Dist (1)
  11- 15  F5.3  ---       tau     Optical depth (τp)
  17- 24  E8.3  m-2       Np      Peak column density in HCO+
  26- 31  F6.1  Msun/pc2  Sigp    Mass surface density (2)
  33- 36  F4.2  pc        R       Clump radius
  38- 45  E8.3  m-3       ncol    Estimated density at the emission peak
  47- 52  F6.1  Msun/pc3  rcol    Equivalent mass density (ρ_col_) (3)
  54- 57  I4    Msun      Mcol    LTE mass
  59- 64  F6.2  pPa       Pgas    Total gas pressure
  66- 73  F8.4 K.pc2.km/s LHCO+   Peak line luminosity (4)
  75- 79  F5.2  ---       alpha   Virial α parameter (α=Mvir/Mcol)
  81- 84  F4.2  pc        RJe     Rayleigh-Jeans radius
  86- 90  I5    Msun      MBE     Bonnor-Ebert mass

Note (1): Distances taken from table 4 as follows:
    c = literature-based value,
    n = near kinematic,
    t = tangent point
Note (2): Mass surface density as Σp=(Np/X)(µmolmH). Here, we
          use an abundance X=10-9 for HCO+ relative to H2, which is our
          best estimate from a number of studies. See section 4.3 for further
          details.
Note (3): ρcol=µmolmHncol_, where µmol=2.30 is the mean
          molecular mass in the gas. See section 4.4 for further details.
Note (4): The peak line luminosity L(HCO+)=W(HCO+)*d2θ2HPBW
          where the Mopra effective telescope half-power beamwidth (HPBW) has
          been smoothed at the gridding stage to 40".
          See section 4.2 for futher details.


History:
    From electronic version of the journal
(End)                                     Emmanuelle Perret [CDS]    30-Dec-2011