The origin of pulsating ultra-luminous X-ray sources: Low- and intermediate-mass X-ray binaries containing neutron star accretors

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Table 1.

Observed and inferred parameters of NS ULXs from the literature.

NS ULX	L_X (erg s⁻¹)	M_donor (M_⊙)	P_orb (days)	P_spin (s)	Ṗ_spin (s s⁻¹)
M82 X-2 ⁽¹⁾	1.8 × 10⁴⁰	≳5.2	2.52	1.37	−2.0 × 10⁻¹⁰
NGC 7793 P13 ⁽²⁾	5.0 × 10³⁹	18.0–23.0 ⁽³⁾	64.0 ⁽⁴⁾	0.417	−3.5 × 10⁻¹¹
NGC 5907 ULX1 ⁽⁵⁾	∼10⁴¹	2.0–6.0		1.137	−8.1 × 10⁻¹⁰
NGC 300 ULX1 ⁽⁶⁾	4.7 × 10³⁹	≳8.0–10.0 ⁽⁷⁾	≳1.0 yr ⁽⁸⁾	31.6	−5.56 × 10⁻⁷
M51 ULX-8 ⁽⁹⁾	2.0 × 10³⁹	–	–	–	–
NGC 1313 X-2 ⁽¹⁰⁾	1.5 × 10⁴⁰	≲12.0 ⁽¹¹⁾	–	1.5	−1.2 × 10⁻¹⁰
Swift J0243.6+6124 ⁽¹²⁾	∼10³⁹	–	28.3 ⁽¹³⁾	9.86 ⁽¹⁴⁾	−2.2 × 10⁻⁸
M51 ULX-7 ⁽¹⁵⁾	10³⁹–10⁴⁰	≳8.0	2.0	2.8	−10⁻⁹

Notes. L_X is the X-ray luminosity, M_donor the donor mass, P_orb the orbital period, P_spin the NS spin period, and Ṗ_spin is the time derivative of the NS spin period.

References. ⁽¹⁾Bachetti et al. (2014), ⁽²⁾Israel et al. (2017a), Fürst et al. (2016), ⁽³⁾Motch et al. (2011), ⁽⁴⁾Motch et al. (2014), ⁽⁵⁾Israel et al. (2017b), ⁽⁶⁾Carpano et al. (2018), ⁽⁷⁾Heida et al. (2019), ⁽⁸⁾Vasilopoulos et al. (2018), Ray et al. (2019), ⁽⁹⁾Brightman et al. (2018), ⁽¹⁰⁾Sathyaprakash et al. (2019), ⁽¹¹⁾Grisé et al. (2008), ⁽¹²⁾Zhang et al. (2019), ⁽¹³⁾Doroshenko et al. (2018), Ge et al. (2017), ⁽¹⁴⁾Kennea et al. (2017), Jenke & Wilson-Hodge (2017), ⁽¹⁵⁾Rodríguez Castillo et al. (2020).

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