The molecular interstellar medium of the Local Group dwarf NGC 6822 - The molecular ISM of NGC 6822

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Table 2:

Properties for the clouds identified by eye (*Top*), and by the `CPROPS` package (*Bottom*).
The clouds whose numbers are in bold face correspond to our final sample of clouds
Cloud	$\alpha_{\rm off}$ ^a	$\delta_{\rm off}$ ^a	$V_{{\rm LSR}}$	FWHM	${R_{\rm e}}$	${I}_{\rm CO}$	${M}_{{\rm\rm vir}}$ ^b	${M}_{{\rm H}_{2}}$ ^c	$N({\rm H_{2}})/{\rm I}_{{\rm CO}}$ ^d
	arsec	arcsec	${\rm\ km \ s^{-1}}$	${\rm\ km \ s^{-1}}$	pc	K ${\rm\ km \ s^{-1}}$	$M_{\hbox{$\odot$ }}$	$M_{\hbox{$\odot$ }}$	$\frac{{\rm cm}^{-2}}{{\rm K}{\rm\ km \ s^{-1}}}$
GMC NGC6822 1	-48	330	-43.2	$1.5 \pm 0.9$	$22_{\rm -14}^{+9}$	$0.92_{\rm -0.10}^{+0.10}$	$9.3_{\rm -8.7}^{+24}\times 10^3$	$3.6_{\rm -0.8}^{+1.4}\times 10^4$	$1.4_{\rm -0.2}^{+0.2} \times 10^{21}$
GMC NGC6822 2^e	-68.5	299	-42.4	$5.1\pm 0.4$	$29_{\rm -6}^{+5}$	$2.47_{\rm -0.13}^{+0.14}$	$1.9_{\rm -0.5}^{+0.5} \times 10^5$	$3.1_{\rm -0.6}^{+0.3} \times 10^4$	$3.0_{\rm -0.3}^{+0.3} \times 10^{20}$
GMC NGC6822 3	80	58	-38.0	$2.4\pm 0.5$	$38_{\rm -21}^{+15}$	$0.36_{\rm -0.06}^{+0.07}$	$4.1_{\rm -3}^{+4.2}\times 10^4$	$9.5_{\rm -3.7}^{+3.5}\times 10^4$	$4.3_{\rm -1.1}^{+1.6}\times 10^{21}$
GMC NGC6822 4	39	25	-39.9	$2.0\pm 0.6$	$18_{\rm -10}^{+6}$	$1.34_{\rm -0.09}^{+0.10}$	$1.2_{\rm -0.3}^{+0.1}\times 10^5$	$1.2_{\rm -0.3}^{+0.1}\times 10^5$	$3.1_{\rm -0.3}^{+0.4} \times 10^{21}$
GMC NGC6822 5	35	24	-43.2	$3.4\pm 1.1$	$19_{\rm -9}^{+8}$	$1.52_{\rm -0.13}^{+0.11}$	$4.1_{\rm -0.3}^{+0.6}\times 10^4$	$1.2_{\rm -0.3}^{+0.2} \times 10^5$	$2.5_{\rm -0.2}^{+0.5} \times 10^{21}$
GMC NGC6822 6	30	16	-48.3	$1.6\pm 0.4$	$12_{\textrm{\ldots}}^{+15}$	$0.82_{\rm -0.07}^{+0.05}$	$5.8_{\textrm{\ldots}}^{+14}\times 10^3$	$4.7_{\rm -1.4}^{+1.4} \times 10^4$	$2.4_{\rm -0.2}^{+0.3}\times 10^{21}$
GMC NGC6822 7	-10	364	-38.1	$3.2\pm 0.4$	$27_{\rm -15}^{+11}$	$0.48_{\rm -0.07}^{+0.06}$	$5.2_{\rm -3.4}^{+4.1} \times 10^4$	$4.9_{\rm -1.0}^{+0.2}\times 10^3$	$2.8_{\rm -1.2}^{+1.6} \times 10^{20}$
GMC NGC6822 8	31	61	-44.8	$2.4\pm 1.4$	$14_{\textrm{ \ldots}}^{+28}$	$0.58_{\rm -0.14}^{+0.13}$	$1.5_{\textrm{\ldots}}^{+9.9}\times 10^4$	$4.1_{\rm -2.5}^{+5.1}\times 10^4$	$2.8_{\rm -0.5}^{+1.0} \times 10^{21}$
GMC NGC6822 9	7	54	-56.0	$1.4\pm 0.4$	$\textrm{\ldots}_{\textrm{ \ldots}}^{+13}$	$0.57_{\rm -0.10}^{+0.04}$	$\textrm{\ldots}_{\textrm{ \ldots}}^{+7.9} \times 10^3$	$7.6_{\rm -1.6}^{+4.2}\times 10^3$	$8.2_{\rm -0.7}^{+1.7}\times 10^{20}$
GMC NGC6822 10	0	26	-60.1	$3.9\pm 1.0$	$33_{\rm -17}^{+17}$	$0.59_{\rm -0.10}^{+0.07}$	$9.4_{\rm -6.9}^{+13}\times 10^4$	$7.6_{\rm -2.9}^{+3.4}\times 10^4$	$2.6_{\rm -0.7}^{+1.0} \times 10^{21}$
GMC NGC6822 11	-358	208	-70.3	$2.0\pm 0.9$	$28_{\textrm{ \ldots}}^{43}$	$0.23_{\rm -0.07}^{+0.07}$	$2.1_{\textrm{ \ldots}}^{+9.1}\times 10^4$	$\textrm{ \ldots}_{\textrm{ \ldots}}^{\textrm{ \ldots}}$ ^h	$\textrm{ \ldots}_{\textrm{ \ldots}}^{\textrm{ \ldots}}$ ^h
GMC NGC6822 12	55	287	-37.6	$2.6\pm 0.5$	$23_{\textrm{ \ldots}}^{+28}$	$0.23_{\rm -0.02}^{+0.06}$	$2.9_{\textrm{ \ldots}}^{+6.3}\times 10^4$	$\textrm{ \ldots}_{\textrm{ \ldots}}^{+3.0}\times 10^3$	$\textrm{ \ldots}_{\textrm{ \ldots}}^{+1.7}\times 10^{20}$
GMC NGC6822 13	49	364	-54.7	$1.7\pm 0.4$	$\textrm{ \ldots}_{\textrm{ \ldots}}^{+34}$	$0.26_{\rm -0.07}^{+0.05}$	$\textrm{ \ldots}_{\textrm{ \ldots}}^{+2.7}\times 10^4$	$\textrm{ \ldots}_{\textrm{ \ldots}}^{\textrm{ \ldots}}$ ^h	$\textrm{ \ldots}_{\textrm{ \ldots}}^{\textrm{ \ldots}}$ ^h
GMC NGC6822 14	-331	372	-76.0	$3.0\pm 1.0$	$\textrm{ \ldots}_{\textrm{ \ldots}}^{+15}$	$0.32_{\rm -0.08}^{+0.08}$	$\textrm{ \ldots}_{\textrm{ \ldots}}^{+4.5}\times 10^4$	$\textrm{ \ldots}_{\textrm{ \ldots}}^{\textrm{ \ldots}}$ ^h	$\textrm{ \ldots}_{\textrm{ \ldots}}^{\textrm{ \ldots}}$ ^h
GMC NGC6822 15	-386	57	-73.8	$3.6\pm 0.8$	$24_{\rm -16}^{+21}$	$0.53_{\rm -0.12}^{+0.06}$	$5.8_{\rm -4.7}^{+11}\times 10^4$	$5.5_{\rm -1.4}^{+1.3}\times 10^4$	$2.9_{\rm -01.2}^{+1.7}\times 10^{21}$

Cloud	$\alpha_{\rm off}$ ^a	$\delta_{\rm off}$ ^a	$V_{{\rm LSR}}$	FWHM	${R_{\rm e}}$	$R_{\rm ex}$	${I}_{\rm CO}$	$M_{\rm vir}$ ^b	M_H₂^c	$N({\rm H_{2}})/{\rm I}_{{\rm CO}}$ ^d
	arsec	arcsec	${\rm\ km \ s^{-1}}$	${\rm\ km \ s^{-1}}$	pc	pc	K ${\rm\ km \ s^{-1}}$	$M_{\hbox{$\odot$ }}$	$M_{\hbox{$\odot$ }}$	$\frac{{\rm cm}^{-2}}{{\rm K}{\rm\ km \ s^{-1}}}$
GMC NGC6822 1	-50	331	-40.2	$5.5 \pm3.5$ ^g	$15 \pm 14$	38	$0.9 \pm 0.3$	$8.5 \pm 9.2 \times 10^4$ ^g	$5.1\times 10^4$	$9.9 \times 10^{20}$
GMC NGC6822 2	-71	301	-41.3	$6.2\pm 1.4$	$32\pm 4$	86	$1.2\pm 0.1$	$2.3\pm 0.5\times 10^4$	$9.8 \times 10^4$	$4.2 \times 10^{20}$
GMC NGC6822 3	83	59	-37.0	$2.2\pm 1.9$	$32\pm 13$	54	$0.2\pm 0.1$	$2.8\pm 2.6\times 10^4$	$1.1\times 10^5$	$6.4\times 10^{21}$
GMC NGC6822 4	38	25	-39.2	$2.1\pm 3.2$	$15\pm 21$	12	$1.0\pm 1.3$	$1.3\pm 2.3\times 10^4$	$1.2\times 10^5$	$4.0\times 10^{21}$
GMC NGC6822 5	35	24	-42.6	$3.9\pm 6.2$	$10\pm 22$	$\ldots^{{\rm ~i}}$	$1.4\pm 2.2$	$2.9\pm 7.6\times 10^4$	$8.8\times 10^4$	$2.8\times 10^{21}$
GMC NGC6822 6	30	17	-47.1	$3.2\pm 3.0$	$15\pm 29$	33	$0.7\pm 0.2$	$2.8\pm 6.3\times 10^4$	$9.9\times 10^4$	$3.0\times 10^{21}$
GMC NGC6822 7	-17	359	-38.1	$2.1\pm 1.8$	$31\pm 17$	47	$0.3\pm 0.2$	$2.5\pm 2.4\times 10^4$	$\ldots$ ^h	$\ldots$ ^h
GMC NGC6822 8	33	62	-43.2	$4.6\pm 6.0$	$19\pm 20$	37	$0.3\pm 0.2$	$7.5\pm 14\times 10^4$	$9.5\times 10^4$	$4.7\times 10^{21}$
GMC NGC6822 9	7	54	-55.3	$2.1\pm 1.8$	$10\pm 31$	31	$0.3\pm 0.1$	$0.8\pm 2.3\times 10^4$	$3.6\times 10^4$	$2.6\times 10^{21}$
GMC NGC6822 10	0	27	-59.4	$4.6\pm 2.7$	$25\pm 7$	55	$0.5\pm 0.1$	$9.6\pm 6.1\times 10^4$	$1.4\times 10^5$	$3.1\times 10^{21}$
GMC NGC6822 11	-365	210	-69.4	$1.7\pm 1.8$	$11\pm 27$	16	$0.2 \pm 0.2$	$0.6\pm 1.7 \times 10^4$	$\ldots$ ^h	$\ldots$ ^h

Notes. ^(a) Offsets with respect to the reference position $(\alpha_{\rm o},\delta_{\rm o})=(19^{\rm h}44^{\rm m}57\ \hbox{$.\!\!^{\rm s}$ }8,-14\hbox{$^\circ$ }48\hbox{$^\prime$ }11\hbox{$^{\prime\prime}$ })$ . ^(b) Virial mass following Solomon et al. (1987) using ${R_{\rm e}}$ and $\Delta V$ (see Sect. 4). ^(c) ${\rm H}_{2}$ mass estimate from ${\rm 8~\mu m}$ emission (see Sect. 6.3). ^(d) X conversion factor for individual clouds using $N({\rm H_{2}})$ estimated from ${\rm 8~\mu m}$ emission (see Sect. 6.3). ^(e) Hubble V (Hubble 1925). ^(f) See Sect. 4. ^(g) The CPROPS computed FWHM is clearly overestimated compared to the one computed by hand by a factor of about 3. $M_{\rm vir}$ being proportional to FWHM², this explains the order of magnitude difference between the computed virial masses for this cloud. ^(h) The computed ${\rm H}_{2}$ mass for these clouds was found to be negative. ⁽ⁱ⁾ The deconvolved size was not defined.

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