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J/A+A/538/A137      Orion B9 dense cores maps                (Miettinen+, 2012)
A (sub)millimetre study of dense cores in Orion B9.
    Miettinen O., Harju J., Haikala L.K., Juvela M.
   <Astron. Astrophys. 538, A137 (2012)>
   =2012A&A...538A.137M
ADC_Keywords: Interstellar medium ; Molecular clouds ; Millimetric/submm sources

Keywords: astrochemistry - stars: formation - ISM: abundances - ISM: clouds -
          ISM: molecules - submillimeter: ISM

Abstract:
    We aim to further constrain the properties and evolutionary stages of
    dense cores in Orion B9. The central part of Orion B9 was mapped at
    350 micron with APEX/SABOCA. A sample of nine cores in the region were
    observed in C17O(2-1), H13CO+(4-3) (towards 3 sources),
    DCO+(4-3), N2H+(3-2), and N2D+(3-2) with APEX/SHFI. These
    data are used in conjunction with our previous APEX/LABOCA 870-micron
    dust continuum data. Many of the LABOCA cores show evidence of
    substructure in the higher-resolution SABOCA image.

Description:
    SABOCA 350-micron map of Orion B9 (FITS format of Fig. 2 of the
    paper). The data were reduced using the CRUSH-2 software.
Objects:
    --------------------------------------------------
       RA   (2000)   DE      Designation(s)
    --------------------------------------------------
    05 42 27.7   -01 20 02   Orion B9 = [CM95] Ori B9
    --------------------------------------------------

File Summary:

       FileName      Lrecl  Records   Explanations

ReadMe            80        .   This file
table1.dat        92        9   Source list
fig2.fits       2880     2325   SABOCA 350-um image of the central part of
                                Orion B9


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

   Bytes Format Units      Label    Explanations

   1- 15  A15   ---        Name     Source name
  17- 18  I2    h          RAh      Right ascension (J2000) (1)
  20- 21  I2    min        RAm      Right ascension (J2000) (1)
  23- 26  F4.1  s          RAs      Right ascension (J2000) (1)
      28  A1    ---        DE-      Declination sign (J2000) (1)
  29- 30  I2    deg        DEd      Declination (J2000) (1)
  32- 33  I2    arcmin     DEm      Declination (J2000) (1)
  35- 36  I2    arcsec     DEs      Declination (J2000) (1)
  38- 41  F4.1  K          Tkin     Gas kinematic temperature
  43- 45  F3.1  K          e_Tkin   rms uncertainty on Tkin
  47- 50  F4.1  Msun       Mass     Core mass
  52- 54  F3.1  Msun       e_Mass   rms uncertainty on Mass
  56- 58  F3.1  10+22cm-2  N(H2)    Beam-averaged peak molecular hydrogen column
                                     density, calculated towards the revised
                                     LABOCA peak position by using the
                                     temperature derived towards the line
                                     observation target position
  60- 62  F3.1  10+22cm-2  e_N(H2)  rms uncertainty on N(H2)
      63  A1    ---        ---      [/]
  64- 66  F3.1  10+22cm-2  N(H2)2   Beam-averaged peak molecular hydrogen column
                                     density, refers to the position used in
                                     molecular-line observations
  68- 70  F3.1  10+22cm-2 e_N(H2)2  rms uncertainty on N(H2)2
  72- 75  F4.1  10+4cm-3   n(H2)    Volume-averaged molecular hydrogen
                                     number density
  77- 79  F3.1  10+4cm-3   e_n(H2)  rms uncertainty on n(H2)
  81- 92  A12   ---        Class    Classification (2)

Note (1): These coordinates refer to the LABOCA peak positions after adjusting
   the pointing. The coordinates of our molecular-line observation target
   positions can be found in Table 1 of Paper II
   (Miettinen et al., 2010A&A...524A..91M).
Note (2): protostar class (0, I or "prestellar"). The virial parameter of
   the starless cores SMM 5 and Ori B9 N is αvir≳2, and thus it
   is  unclear if they are prestellar  (Paper II, Miettinen et al.,
   2010A&A...524A..91M)


Acknowledgements:
    Oskari Miettinen, osmietti(at)mappi.helsinki.fi

References:
    Miettinen et al., Paper I  2009A&A...500..845M
    Miettinen et al., Paper II 2010A&A...524A..91M
(End)                                        Patricia Vannier [CDS]  15-Dec-2011