Tentative detection of ethylene glycol toward W51/e2 and G34.3+0.2

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Table 4

Relative abundances of (CH₂OH)₂, HCOOCH₃ and CH₂OHCHO in different sources.

Source	HCOOCH₃/(CH₂OH)₂	HCOOCH₃/CH₂OHCHO	(CH₂OH)₂/ CH₂OHCHO	L_bol [ L_⊙ ]	References

W51/e2 (this study)	35	>550	>16	4.7 × 10⁶	1, 2
Orion-KL^a	35	>200–300	>12	10⁵	3, 4
G34.3+0.2 (this study)	31	>193	>6	2.8 × 10⁵	1, 5
Sgr B2(N) LMH^b	–	52	–	10⁷	6,7
G31.41 + 0.31^c	–	<34	–	1.8 × 10⁵	8, 5
NGC 7129 FIRS2^d	~15	~30	~2	500	9
IRAS NGC 1333 2A^e	4	20	5	20	10,11
IRAS 16293–2422^e	~13	~13	~1	27	12, 13
IRAS NGC 1333 4A^e	–	10	–	7.7	14
MC G + 0.693^f	4.3	5.2	1.2	–	15
MC G-0.11^f	2.8	4.3	1.6	–	15
MC G-0.02^f	2.5	3.3	1.3	–	15
Lemmon^g	<0.7	–	>3	–	16
LoveJoy^g	<0.6	–	>5	–	16
Hale-Bopp^g	0.32	>2	>6.25	–	17

Notes. The table show the results from similar studies of: and

^(a)

the Orion Kleinmann-Low nebula, a high-mass star-forming region;

^(b)

the Large Molecule Heimat hot core source toward Sgr B2(N);

^(c)

high-mass star-forming region;

^(d)

intermediate-mass protostar;

^(e)

low-mass Class 0 protostars;

^(f)

molecular clouds in the Sgr A complex (MC G – 0.02 – 0.07 (“the 50 km s^-1 cloud”) and MC G – 0.11 – 0.08 (“the 20 km s^-1 cloud”)) and in the Sgr B2 complex (MC G + 0.693 – 0.03);

^(g)

comets.

Reference. (1) this study; (2) Urquhart et al. (2014); (3) Favre et al. (2011), Brouillet et al. (2015); (4) Crockett et al. (2014); (5) van Dishoeck et al. (2011); (6) Hollis et al. (2001); (7) Goldsmith et al. (1990); (8) Beltrán et al. (2009); (9) Fuente et al. (2014); (10) Coutens et al. (2015); (11) Jørgensen et al. (2009); (12) Jørgensen et al. (2012, in prep.); (13) Schöier et al. (2002); (14) Taquet et al. (2015); (15) Requena-Torres et al. (2008); (16) Biver et al. (2014); (17) Bockelée-Morvan et al. (2000), Crovisier et al. (2004a,b).

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