The millimeter-wave spectrum of methyl ketene and the astronomical search for it

C. Bermúdez; B. Tercero; R. A. Motiyenko; L. Margulès; J. Cernicharo; Y. Ellinger; J.-C. Guillemin

doi:10.1051/0004-6361/201833267

Home

All issues

Volume 619 (November 2018)

A&A, 619 (2018) A92

Full HTML

Open Access

Table 5.

Physical parameters of the considered cloud cores.

Source	Coordinates (J2000.0)	HPBW^a (″)	Frequencies^b (GHz)	v_LSR (km s⁻¹)	Δv_FWHM (km s⁻¹)	d_sou (″)	T_rot (K)	N(CH₃CHCO) ×10¹⁴ (cm⁻²)
Orion KL	α = 5^h35^m14.5^s	30–8	80–307	8	3	5	150	≤(5.0 ± 2.5)
(IRAM 30 m)	δ = −05^∘22′30.0″

Orion KL	α = 05^h35^m14.5^s	∼1.9 × 1.4	213.7–246.7	8	3	3	150	≤(10 ± 5)
(ALMA SV)	δ = −05^∘22′32.5″
Hot core

Orion KL	α = 05^h35^m14.1^s	∼1.9 × 1.4	213.7–246.7	7.5	2	3	100	≤(3.0 ± 1.5)
(ALMA SV)	δ = −05^∘22′36.9″
Compact ridge

Orion KL	α = 05^h35^m14.2^s	∼1.9 × 1.4	213.7–246.7	3	3	3	150	≤(5.0 ± 2.5)
(ALMA SV)	δ = −05^∘22′31.1″			5	8	3	150	≤(2.0 ± 1.0)
MM4

Sgr B2(N)	(IRAM 30 m)	30–21	80–115.5	63	9	3	100	≤(100 ± 50)
	α = 17^h47^m20.0^s			72	8	3	100	≤(100 ± 50)
	δ = −28^∘22′19.0″
	(GBT 100m)	80–15	7–50
	α = 17^h47^m19.8^s
	δ = −28^∘22′17.0″

B1-b	α = 03^h33^m20.0^s	30–21	80–115.5	6.7	0.7	60	12	≤(0.010 ± 0.005)
(IRAM 30 m)	δ = 31^∘07′34.0″

TMC-1	α = 04^h41^m41.88^s	30–21	80–115.5	6.0	0.7	60	10	≤(0.010 ± 0.005)
(IRAM 30 m)	δ = 25^∘41′27.0″

Notes.

^(a)

HPBW (half power beam width) for observations with single dish telescope (IRAM 30 m and GBT 100 m) and synthetic beam for the ALMA SV observations.

^(b)

Range of frequencies considered in the analysis.

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.