Data


Orion A --- Rho Ophiuchus --- Aquila Rift --- California --- M17--- L1551
Some data are also available from here.
Please reference the following papers as the data source, if you use the data in your own research. The data were obtained in the previous star formation project. This page contains the data obtained by the other related projects.

Orion A

  1. 12CO (1-0) fits cube (164MB, Tmb, 1km/s vel. res.)
    2. 12CO (1-0) fits cube (276MB, Tmb, 0.5km/s vel. res.)
    (Shimajiri et al. 2011, PASJ, 63, 105; Nakamura et al. 2012, ApJ, 746, 25; Shimajiri et al. 2014, A&A, 564, 68;
  2. 13CO (1-0) Moment 0 fits (Shimajiri et al. 2014, A&A, 564, 68);
  3. 13CO (1-0) cube fits (Shimajiri et al. 2014, A&A, 564, 68);
  4. C18O (1-0) Moment 0 fits (Shimajiri et al. 2014, A&A, 564, 68);
  5. C18O (1-0) cube fits (Shimajiri et al. 2014, A&A, 564, 68);

  6. Excel file for Tables 2 and 4 in Shimajiri et al. 2014b (See Tables 2 and 4)
  7. Annotation file of AzTEC 1.1 mm dust cores for KARMA (see Table 2)
  8. Annotation file of AzTEC 1.1 mm dust cores for MIRIAD (see Table 2)
  9. Annotation file of C18O cores for KARMA (see Table 4)
  10. Annotation file of C18O cores for MIRIAD (see Table 4)
  11. Movie of the C18O velocity channel maps overlaid the positions of the identified C18O cores (see Appendix B)
    [Note] The Velocity resolution is 0.104 km/s
  12. FITS file showing the distribution of the ifentified 1.1mm dust cores (see Appendix B and Figs 25-28)
    [Note]The values correspond to the ID numbers
    FITS file of the AzTEC 1.1 mm dust continuum As described in Section 2.1.1 and Appendix C, we have to be careful on the treatment of the bolometer data. To avoid the misleading, we do not release the 1.1mm dust continuum data on the web site. But, we provide the 1.1mm data to someone who asked us directly with the detail explanations.
    The contact person is Yoshito SHIMAJIRI (mail: Yoshito.Shimajiri@cea.fr)
    (Shimajiri et al. 2014, ApJS);

Rho Ophiuchus

  1. 12CO (1-0) fits cube (~10MB, Tmb, beam efficiency = 0.32)
    2. (Nakamura et al. 2011, ApJ, 726, 46)
    Related data
  2. 12CO (3-2) fits cube (~11MB, TA*)
    3. (Nakamura et al. 2011, ApJ, 726, 46)
  3. 850um continuum data of SM1 (SMA+SCUBA 850um combined) (~1MB, Jy/beam)
    4. 1.1-mm continuum data of B2-N5 (SMA+AzTEC/ASTE combined) (~1MB, Jy/beam)
    (Nakamura et al. 2012, ApJ, 758, L25)
  4. H13CO+ (1-0) fits cube (~5MB, Tmb, beam efficiency = 0.51)
    5. H13CO+ integrated intensity fits (~57KB, Tmb, beam efficiency = 0.51)
    H13CO+ core annotation file (H13CO+ cores identified by CLUMPFIND)
    (The original fits data of H13CO+ (TA*) is available from here. See Maruta et al. (2010) in detail.)

Aquila Rift/Serpens South

  1. N2H+ (1-0) fits cube (~11MB, TA*, 0.05 km/s, beam efficiency = 0.51, (F1F->F1'F'=23-12) = 93.173777GHz)
    2. (Tanaka et al. 2013, ApJ, 778, 34)
  2. CCS (43-32) fits cube (~1.5MB, Tmb) CCS (43-32) fits cube (~20MB, Tmb)
    3. (Nakamura et al. 2014, ApJL, 791, 23)
  3. HC3N (5-4) fits cube (~20MB, Tmb)
    4. (Nakamura et al. 2014, ApJL, in press)
  4. SiO (2-1) fits cube (~0.5MB, Tmb)
    5. (Nakamura et al. 2014, ApJL, 791, 23)
    Note that because of the flux calibration problem of the backend system SAM45,the intensities might have errors as large as 50 % for the data of CCS, SiO, and HC3N.
    Related data
  1. 12CO (3-2) fits cube (~593MB, Tmb, 0.1 km/s, beam efficiency = 0.57)
  2. 12CO (3-2) fits cube (~119MB, Tmb, 0.5 km/s, beam efficiency = 0.57)
  3. HCO+ (4-3) fits cube (~593MB, Tmb, 0.1 km/s, beam efficiency = 0.57)
    4. Note that CO32 and HCO+ data have relatively large spurious at the edges of the observation boxes.
    (Nakamura et al. 2011, ApJ, 737, 56)

California

M17

L1551

  2. 12CO (1-0) fits cube (~10MB, Tmb, beam efficiency = 0.32)
  3. 13CO (1-0) fits cube (~10MB, Tmb, beam efficiency = 0.32)
  4. C18O (1-0) fits cube (~10MB, Tmb, beam efficiency = 0.32)
    5. (Lin et al. 2015, submitted to ApJ)

Contact Address

sf_45m_legacy_2013@googlegroups.com