Dense gas in low-metallicity galaxies | Astronomy & Astrophysics (A&A)

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Table 3

New observations presented in this work.

Source	I_CO		I_C¹⁸O	I_HCO⁺	I_HCN	I_HNC	I_CCH	I_CS

M 33a^a		0.64 ± .07	0.04 ± .065	0.20 ± .05	0.12 ± .05	≲0.06	0.09 ± .05
M 33a^b	15.7 ± .6	0.58 ± .10	0.21 ± .12	0.212 ± .037	0.083 ± .039	0.031 ± .036	0.117 ± .048
M 33b^b	15.5 ± .5	1.16 ± .12	≲0.11	0.806 ± .055	0.339 ± .048	0.208 ± .046	0.434 ± .068
M 33c^b	12.1 ± .4	0.73 ± .08	≲0.09	0.659 ± .046	0.496 ± .046	≲0.051	0.075 ± .060
IC 10b8^a	5.54 ± .08	0.55 ± .023	≲0.014	0.157 ± .009	0.032 ± .010	0.025 ± .009	0.031 ± .009	≲0.04
IC 10b9^a	5.93 ± .08	0.46 ± .03	≲0.02	0.04 ± .02	≲0.015	≲0.016	≲0.014	0.06 ± .03
IC 10b11^a	14.9 ± .1	1.12 ± .04	0.11 ± .036	0.718 ± .023	0.245 ± .025	0.088 ± .027	0.21 ± .03	0.26 ± .05
N6822HubV^a	2.0 ± 0.12 ^c	0.16 ± .02	≲0.019	0.115 ± .012	0.025 ± .011	≲0.013	0.049 ± .012

Notes. All fluxes are on the main beam temperature scale, The other lines within the bandpasses such as SO, HC₃N, or N₂H⁺, were not detected. C¹⁸O was not detected either but was included in this table to directly compare with ¹³CO. Blank parts of the table indicate that the line was not observed. Limits are given as ≲the 1σ noise level to distinguish between a tentative line (e.g. HCN in N6822HubV, 0.25 ± .011 K km s^-1) and something where there is no sign of a line (typically intensity below 1σ or negative).

^(a)

indicates observatons with the IRAM 30 m antenna and

^(b)

with the NRO 45 m telescope;

^(c)

taken from Gratier et al. (2010a).

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