CHILLING: Continuum Halos in LVHIS Local Irregular Nearby Galaxies - Radio continuum spectral behavior of dwarf galaxies

Open Access

Table 1.

CHILLING sample properties.

Name	RA¹	Dec¹	D¹	M_B²	$log {[\frac{{SFR}_{H α}}{M_{⊙} {yr}^{- 1}}]}^{3}$ $\log\left[\frac{\mathrm{SFR_{H\alpha}}}{\mathrm{M_{\odot} \, \mathrm{yr}^{-1}}}\right]^3$	$log {[\frac{M_{H I}}{M_{⊙}}]}^{4}$ $\log\left[\frac{M_{\mathrm{H{\small { {\text{ I}}}}}}}{M_{\odot}}\right]^4$	$v_{rot}^{2}$ $v_{\mathrm{rot}}^2$	L_3.4μm⁵	L_60μm⁶
	(J2000)	(J2000)	(Mpc)	(mag)			(km s⁻¹)	(mag)	(Jy)
ESO154-G023	02^h56^m50.38^s	−54^d34^m17.10^s	5.76	−16.45	−1.32	9.14	53.0	15.21	0.32
ESO245-G005	01^h45^m03.73^s	−43^d35^m52.93^s	4.43	−15.68	−1.59	8.6	51.0	15.99	0.22
ESO383-G087	13^h49^m17.50^s	−36^d03^m48.40^s	3.45	−16.83	−1.49	7.82	18.0	14.05	1.21
ESO572-G025^†	11^h57^m28.03^s	−19^d37^m26.60^s	27.88	−17.50	−0.27	8.36	–	12.88	0.51
Fairall301^†	04^h06^m07.92^s	−52^d40^m06.30^s	9.30	−15.92	−1.11	–	52.3	12.38	0.90
IC1959	03^h33^m12.59^s	−50^d24^m51.30^s	6.19	−16.07	−1.38	8.38	57.0	13.90	0.51
IC4662	17^h47^m08.86^s	−64^d38^m30.33^s	2.55	−15.61	−1.12	8.24	41.0	11.99	8.82
IC5152	22^h02^m41.51^s	−51^d17^m47.20^s	1.96	−15.56	−2.23	8.01	43.0	13.77	2.46
ISZ399^†	12^h19^m59.51^s	−17^d23^m31.00^s	15.94	−17.15	−0.81	–	–	10.71	2.86
NGC244^†	00^h45^m46.43^s	−15^d35^m48.80^s	11.60	−16.25	−1.11	8.73	–	12.05	0.53
NGC625	01^h35^m04.63^s	−41^d26^m10.30^s	4.02	−16.50	−1.20	8.00	34.0	12.12	5.73
NGC1311	03^h20^m06.96^s	−52^d11^m07.90^s	5.55	−15.41	−1.55	8.04	36.0	13.46	0.39
NGC5253	13^h39^m55.96^s	−31^d38^m24.38^s	3.44	−17.05	−0.64	7.91	31.0	9.25	30.51
NGC5264	13^h41^m36.68^s	−29^d54^m47.10^s	4.79	−16.02	−1.92	7.70	15.0	13.72	0.30
NGC5408	14^h03^m20.91^s	−41^d22^m39.70^s	5.32	−16.73	−0.83	8.48	30.0	13.06	2.82

Notes. The sample properties include the coordinates, distance, absolute magnitude in B-band, star formation rate, HI mass, rotational velocity, and the near and far-infrared luminosities of each dwarf galaxy. ^† Blue compact dwarf galaxies (BCDs); the rest are irregular dwarfs from the LVHIS sample. ¹: NED NASA/IPAC Extragalactic Database; ²: HyperLeda Database; ³: Following Gallagher et al. (1984), we calculate the SFR using Hα values from Kennicutt et al. (2008); ⁴: Koribalski et al. (2018), ⁵: Cutri et al. (2021); ⁶: Helou & Walker (1988).

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