Search for Axion-like particles from nearby pre-supernova stars

Open Access

Table 1.

Pre-supernovae candidates within 1 kpc.

Common Name	Gal. long	Gal. lat	Distance	Mass	g_ae × g_aγ	g_aγ	511 keV	1.8 MeV	M_Al [M_⊙]
	[deg]	[deg]	[kpc]	[M_⊙]	2σ UL	2σ UL	3σ UL	3σ UL	3σ UL
Spica	316.11	50.84	0.077 ± 0.004	$11 . 43_{- 1.15}^{+ 1.15}$ $Mathematical equation: $ 11.43^{+1.15}_{-1.15} $$	27.7	4.36	35.6	11.8	6
ϵ Pegasi	65.57	−31.45	0.211 ± 0.006	$11 . 7_{- 0.8}^{+ 0.8}$ $Mathematical equation: $ 11.7^{+0.8}_{-0.8} $$	13.5	3.26	30.3	9.7	37
Betelgeuse	199.78	−8.95	0.222 ± 0.040	$11 . 6_{- 3.9}^{+ 5.0}$ $Mathematical equation: $ 11.6^{+5.0}_{-3.9} $$	8.1	2.15	11.1	4.4	19
ζ Cephei	103.06	1.66	0.256 ± 0.006	$10 . 1_{- 0.1}^{+ 0.1}$ $Mathematical equation: $ 10.1^{+0.1}_{-0.1} $$	3.3	1.97	1.1	0.4	2
Rigel	209.24	−25.24	0.264 ± 0.024	$21 . 0_{- 3.0}^{+ 3.0}$ $Mathematical equation: $ 21.0^{+3.0}_{-3.0} $$	11.7	3.31	5.7	1.8	11
ξ Cygni	71.01	3.36	0.278 ± 0.029	8.0	25.1	5.69	13.4	4.6	30
S Monocerotis A	202.93	2.19	0.282 ± 0.040	29.1	41.8	5.51	45.9	13.3	90
CE Tauri	187.17	−8.07	0.326 ± 0.070	$14 . 37_{- 2.00}^{+ 2.00}$ $Mathematical equation: $ 14.37^{+2.00}_{-2.00} $$	50.8	5.86	289.0	41.4	375
12 Pegasi	76.64	−22.82	0.415 ± 0.031	$6 . 3_{- 0.7}^{+ 0.7}$ $Mathematical equation: $ 6.3^{+0.7}_{-0.7} $$	56.4	6.68	100.0	17.0	250
5 Lacertae	99.66	−8.65	0.505 ± 0.046	$5 . 11_{- 0.18}^{+ 0.18}$ $Mathematical equation: $ 5.11^{+0.18}_{-0.18} $$	17.2	3.60	1.9	0.7	15
VV Cephei	104.92	7.04	0.599 ± 0.083	$10 . 6_{- 1.0}^{+ 1.0}$ $Mathematical equation: $ 10.6^{+1.0}_{-1.0} $$	4.7	3.11	1.1	0.4	13
θ Delphini	57.94	−16.60	0.629 ± 0.029	$5 . 60_{- 3.0}^{+ 3.0}$ $Mathematical equation: $ 5.60^{+3.0}_{-3.0} $$	22.5	4.98	45.8	14.9	503
V381 Cephei	98.18	6.35	0.631 ± 0.086	12.0	5.1	2.01	2.3	0.9	31
V424 Lacertae	104.58	−8.99	0.634 ± 0.075	$6 . 8_{- 1.0}^{+ 1.0}$ $Mathematical equation: $ 6.8^{+1.0}_{-1.0} $$	4.2	4.93	1.2	0.5	16
HR 861	135.95	4.66	0.639 ± 0.039	$9 . 2_{- 0.5}^{+ 0.5}$ $Mathematical equation: $ 9.2^{+0.5}_{-0.5} $$	14.4	2.30	1.9	0.7	25
V809 Cassiopeia	112.61	1.72	0.730 ± 0.074	$8 . 3_{- 0.5}^{+ 0.5}$ $Mathematical equation: $ 8.3^{+0.5}_{-0.5} $$	2.0	1.19	0.7	0.3	13
HR 8248	90.83	−4.30	0.746 ± 0.039	$6 . 3_{- 0.7}^{+ 0.7}$ $Mathematical equation: $ 6.3^{+0.7}_{-0.7} $$	4.6	1.66	4.7	1.8	85
α Cygni	84.28	1.99	0.802 ± 0.066	$19 . 0_{- 4.0}^{+ 4.0}$ $Mathematical equation: $ 19.0^{+4.0}_{-4.0} $$	11.5	3.58	11.5	3.9	213

combined:					1.9	1.26

Notes. List of massive stars used in this analysis along with their Galactic coordinates, distance, and mass (obtained from Mukhopadhyay et al. (2020)). We also show the most conservative (B_T = 0.4 μG, t_cc = 1.55 × 10⁵ yr) 95% confidence-interval upper limit obtained for the coupling product, g_ae × g_aγ, and for the photon-only coupling, g_aγ. In addition, the 3σ flux upper limits for the 511 keV and the 1809 keV are also listed. Finally, the ²⁶Al mass expected based on the 1809 keV flux is also shown. The units of g_ae × g_aγ, g_aγ, the line fluxes, and the ²⁶Al masses are 10⁻²⁴ GeV⁻¹, 10⁻¹¹ GeV⁻¹, 10⁻⁵ ph cm⁻² s⁻¹, and 10⁻⁵ M_⊙, respectively.

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