CHaMP - The Galactic Census of High and Medium-mass Protostars

CHaMP Technical Details


 

 

Observation window

A 20° section of the Galactic Plane, 300° > l > 280°

Latitude spread -4° < b < +2°
Total area = 120 sq.deg.

3mm Observations

Nanten coverage

Telescope: 4m diameter dish, beam FWHM 2.6 arcmin at 100 GHz
Maps as below with 2 arcmin pixels:
  • 12CO line at 115.271 GHz, velocity coverage -60 to +40 km/s, 0.1 km/s channels
  • 13CO line at 110.301 GHz, velocity coverage -60 to +40 km/s, 0.1 km/s channels
  • C18O line at 109.781 GHz, velocity coverage -60 to +40 km/s, 0.1 km/s channels
  • HCO+ line at 89.189 GHz, velocity coverage -60 to +40 km/s, 0.1 km/s channels
Ta*(rms) ~ 0.1 K.km/s
Identified 209 massive dense molecular clumps within GMCs from C18O and HCO+ maps, suitable for Mopra follow-up

Mopra coverage

 

Click the above map for a larger view, with corresponding region numbers as

referenced in CHaMP Paper I.

 

Telescope: 22m diameter dish, beam FWHM 36" at 85-100 GHz (Ladd et al 2005).
Receiver: 3mm MMIC covering 75-116 GHz, Tsys < 200 K below 100 GHz in good weather.
On-the-fly (OTF) mapping with super-Nyquist sampling (12" pixels after gridding) over square maps (typically a few arcmin across), rastering in RA, Dec, l, or b.
Ta*(rms) < 0.3 K per 0.1 km/s channel after 2 orthogonally-rastered OTF maps in good weather.

MOPS digital filterbank

Bandwidth: 8 GHz instantaneous, comprised of four 2 GHz blocks, with up to 128k spectral channels.
Zoom mode: up to 4 in each block (16 total), each with 137 MHz bandwidth in 4096 channels × 2 polarisations, giving ~0.1 km/s spectral resolution (see schematic diagram).


2006 & 2007 spectral coverage

For these seasons we mapped 121 Nanten clumps at 85-93 GHz, including the following spectral lines (grouped by zoom mode):
  • SiO maser line at 86.243 GHz
  • H13CN line at 86.342 GHz
  • H13CO+, HCO, SiO lines at ~86.8 GHz
  • HCN line at 88.632 GHz
  • HCO+ line at 89.189 GHz
  • CH3CN line at 91.97 GHz
  • N2H+ line at 93.173 GHz

The first Data Release (DR1) is described in CHaMP Paper I (Barnes et al. 2011; see Papers & Posters). Full data cubes, moment maps and data tables are accessible for download here.

 

2009 - 2012 spectral coverage

In these seasons we additionally mapped the same clumps at 107-115 GHz, in the following spectral lines:

  • CH3OH line at 108.89 GHz
  • HC3N line at 109.17 GHz
  • SO line at 109.25 GHz
  • OCS line at 109.46 GHz
  • C18O line at 109.78 GHz
  • 13CO line at 110.20 GHZ
  • C17O line at 112.36 GHz
  • CN lines at 113.2–113.5 GHz
  • CO line at 115.27 GHz

The 12CO data are described in CHaMP Paper III (Barnes et al. 2016; see Papers & Posters), and available for download in DR3.

The 13CO and C18O data are further described in CHaMP Paper IV (Barnes et al. 2018; see Papers & Posters), and available for download in DR4.

 


1mm Observations

ASTE imagingExternal Link ASTE

AzTEC bolometer camera map of a 5°×1° strip across the η Carinae GMC

IR Observations

AAT imagingExternal Link AAT

    Service Time

    IRIS2 camera with 8 arcmin field in K band (2.2 μm), using multiple narrowband filters for wide-field imaging of a pilot sample of 5 molecular clumps during 2006-07:

    • H2 v=1-0 S(1) line at 2.122 μm
    • H2 v=2-1 S(1) line at 2.249 μm
    • Brackett-γ line at 2.166 μm
    • K-continuum filter covering a "line-free" band from 2.25-2.29 μm

     

    Full Survey

    Observations made in 2011 and 2012 of 146/303 of the Mopra clumps, in the above narrowband filters plus broadband J, H, K filters. First results of this IR work are described in CHaMP Paper I.5 (Barnes et al 2013; see Papers & Posters), and available for download in DR2. Further data analysis continues.

Gemini SouthExternal Link Gemini South

Multiband mid-IR imaging of BYF 73 using the T-ReCS camera from observations in 2010 are described by Pitts et al 2018 (see Papers & Posters).

 

CTIOExternal Link CTIO

Using the NEWFIRM camera on the Blanco 4m, J, H, Ks imaging of the remaining Mopra clumps was obtained in 2011 and 2012. Data analysis is underway.

 

VLT External Link VLT

Very deep J, H, Ks photometry and astrometry of BYF 73 with HAWK-I was obtained in 2011, and results are described by Andersen et al 2017 (Papers & Posters).

 

Spitzer Space TelescopeExternal Link SST

GO Program 80024 awarded 73.5 hours for Cycle 8 in 2012 for deep imaging of 209 Nanten clumps in IRAC bands 1 and 2.

 

 

...(More details forthcoming)...