Exploring molecular complexity with ALMA (EMoCA): Detection of three new hot cores in Sagittarius B2(N)

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Volume 604 (August 2017)

A&A, 604 (2017) A60

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Table 1

Position and spectral line density of the hot cores embedded in Sgr B2(N), and distance to UCHII regions and class II methanol masers.

Source	Δα; Δδ^a	α_J2000; δ_J2000^b	N _channels ^c	n _l ^d	d _l−maser ^e	d _l−UCHII ^e	FWHM _UCHII ^f
	(″)	17^h47^m; − 28^o22′		(GHz^-1)	(″)	(″)	(″)

N1	+0.02(0.01); −2.40(0.01)	19.872(0.002)^s; 18.40(0.01)″	40 710	438	_	0.06(0.01)	0.12
N2	−0.02(0.01); +2.58(0.01)	19.868(0.001)^s; 13.42(0.01)″	30 546	460	_	0.42(0.01)	0.08
N3	−8.21(0.07); +1.09(0.06)	19.248(0.005)^s; 14.91(0.06)″	3008	45	0.63(0.41)	_	_
N4	−4.52(0.11); −16.41(0.05)	19.528(0.008)^s; 32.41(0.05)″	932	14	0.25(0.41)	_	_
N5	+2.34(0.01); −25.34(0.01)	20.047(0.007)^s; 41.34(0.01)″	2369	35	0.43(0.40)	0.19(0.01)	<0.25

Notes.

^(a)

Equatorial offsets of the spectral line density peak with respect to the phase center (see Sect. 2.1). The uncertainties in parentheses come from the 2D-Gaussian fit to the contour map. They are only statistical.

^(b)

Same position given in J2000 Equatorial coordinates.

^(c)

Number of channels with continuum-subtracted flux densities above 7σ.

^(d)

Estimation of the spectral line density above 7σ (excluding setup 3) assuming mean linewidths of ~7 km s^-1 for Sgr B2(N1) and ~5 km s^-1 for the others hot cores (see Sect. 3.7 and Belloche et al. 2016).

^(e)

Distance between the hot core and the closest class II methanol maser or UCHII region. The uncertainties given in parentheses are calculated based on the errors given by the Gaussian fits. In the case of the methanol masers, they also take into account the uncertainty on the maser positions (0.4″) given by Caswell (1996).

^(f)

Deconvolved angular size of the UCHII region (De Pree et al. 2015; Gaume et al. 1995).

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