Submillimetric spectroscopic observations of volatiles in comet C/2004 Q2 (Machholz)

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Volume 545 (September 2012)

A&A, 545 (2012) A2

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Table 3

Rotational emission lines in comet C/2004 Q2 (Machholz) observed by SMT on 13–16 January 2005.

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^(a)

Labels in Fig. 1.

^(b)

Mid-time of the observations recorded as fractional days in UT.

^(c)

The line frequencies were obtained from the latest online edition of the JPL Molecular Spectroscopy Catalog (Pickett et al. 1998).

^(d)

The velocity offsets are computed with respect to the optocenters of the complete components for blended lines.

^(e)

Production rates assuming a pointing offset of 2′′.

^(f)

Production rates assuming a pointing offset of 8′′.

^(g)

The uncertainty in the production rates are 1-σ uncertainties considering the receiver sideband gain ratio, main beam efficiency and kinetic temperature errors.

^(h)

Line intensities are the sum of the hyperfine components.

⁽ⁱ⁾

Production rates were derived assuming a daughter product extended source distribution with a scale length of L_p = 8000 km for H₂CO and L_p = 650 km for CS.

^(j)

Weighted average of observations obtained on 13.20 and 16.16 UT January.

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