Molecule sublimation as a tracer of protostellar accretion - Evidence for accretion bursts from high angular resolution C18O images

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Volume 579 (July 2015)

A&A, 579 (2015) A23

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Table 3

Measured and predicted extents of the deconvolved C¹⁸O emission – as well as the current luminosities and luminosity enhancements required to reproduce the extended C¹⁸O emission.

Source	L_cur (L_⊙)	Predicted size (′′)^a	Measured size (′′)^b	L_CO/L_cur^c

L1448I2	1.7	0.9	5.3	25
L1448I3	8.8	2.2	4.9	4.2
L1448C	8.4	2.2	2.0	0.8
IRAS 03256	1.7	0.9	3.4	12
IRAS 2A	20	3.3	3.0	0.8
SVS13A	34	4.6	6.7	2.0
IRAS 4A	9.9	2.4	5.5	4.6
IRAS 4B	4.4	1.6	1.9	1.4
IRAS 03282	1.1	0.8	4.0	25
TMR1	3.8	2.4	5.7	5.4
L1527	1.9	1.6	2.6	2.3
MMS6	27	2.0	4.1	3.7
MMS9	6.3	1.1	3.6	9.6
IRAS 15398	1.6	1.3	3.5	5.9
CrA32	1.3	1.5	7.9	24
B335	1.3	1.9	3.2	2.7

Notes.

^(a)

Predicted extent of the C¹⁸O 2–1 emission given the current luminosity of the source (L_cur).

^(b)

Measured deconvolved extent of the C¹⁸O 2–1 emission (FWHM). The uncertainties are dictated by the signal-to-noise and the assumption of the emission being distributed as Gaussians: typical statistical uncertainties are 0.1–0.5′′ – or 10–20% of the measured sizes.

^(c)

Ratio of luminosity needed to reproduce C¹⁸O 2–1 extent to current luminosity – i.e., inferred enhancement in luminosity. See the text for discussion about the assocated uncertainties.

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