Hunting star forming galaxies in the gamma-ray domain

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Table 1.

Sample of SFGs not included in the 4FGL-DR4 that satisfy the selection criteria defined in Sect. 2.1.

Name	d	RA	Dec	Ṁ_∗	TS	$F_{0.1 - 100 GeV}^{UL}$ $\mathcal{F}^{\mathrm{UL}}_\mathrm{0.1{-}100\,GeV}$	$F_{2 GeV}^{UL}$ $\mathcal{F}_{\mathrm{2\,GeV}}^{\mathrm{UL}}$
	Mpc	deg	deg	M_⊙ yr⁻¹		10⁻¹⁰ GeV cm⁻² s⁻¹	10⁻¹⁴ erg cm⁻² s⁻¹
NGC 6822	0.4603 ± 0.0040	296.24	−14.80	0.0070 ± 0.0006^d	8	8.72	20.5
M33	0.853 ± 0.016	23.46	30.66	0.251 ± 0.013^b	22	10.6	24.9
NGC 300	1.944 ± 0.040	13.72	−37.68	0.138 ± 0.005^a	0	0.63	1.48
NGC 55	1.981 ± 0.020	3.79	−39.22	0.186 ± 0.010^b	0	1.56	3.66
IC 342	2.24 ± 0.10	56.70	68.10	0.40 ± 0.03^c	3	3.77	8.86
NGC 1569	3.25 ± 0.24	67.70	64.85	0.70 ± 0.08^a	10	9.93	23.4
M81	3.61 ± 0.20	148.89	69.07	0.42 ± 0.04^b	0	1.37	3.21
M83	4.79 ± 0.09	204.25	−29.87	3.29 ± 0.10^a	18	9.66	22.7
NGC 3621	6.70 ± 0.37	169.57	−32.81	0.86 ± 0.07^a	7	7.31	17.2
M101	6.76 ± 0.11	210.80	54.35	3.13 ± 0.22^b	3	3.13	7.37
NGC 6946	6.95 ± 0.38	308.71	60.15	3.70 ± 0.33^c	0	1.52	3.56
M106	7.54 ± 0.09	184.74	47.30	1.03 ± 0.08^d	13	3.32	7.80
M51	8.34 ± 0.30	202.47	47.23	2.83 ± 0.15^a	7	4.82	11.3

Notes. The columns d, RA, and Dec are the distance, right ascension, and declination in the ICRS reference system of the galaxy center taken from the SIMBAD astronomical database. Ṁ_∗ is the SFR. TS is the obtained test statistic for detection in the GeV energy range. $F_{0.1 - 100 GeV}^{UL}$ $\mathcal{F}^{\mathrm{UL}}_\mathrm{0.1{-}100\,GeV}$ and $F_{2 GeV}^{UL}$ $\mathcal{F}_{\mathrm{2\,GeV}}^{\mathrm{UL}}$ are the 95% confidence level upper limits on the energy flux integrated over 0.1 − 100 GeV and at 2 GeV, respectively, assuming a fixed spectral index of 2.2.

^(a)

Computed from FUV (Gil de Paz et al. 2007) plus IRAS 25 μm (Sanders et al. 2003) fluxes.

^(b)

Computed from FUV (Gil de Paz et al. 2007) plus IRAS 25 μm (Rice et al. 1988) fluxes.

^(c)

Computed from Hα (Kennicutt et al. 2008) plus IRAS 25 μm (Sanders et al. 2003) fluxes.

^(d)

Computed from Hα (Kennicutt et al. 2008) plus IRAS 25 μm (Rice et al. 1988) fluxes.

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