ner_tags: B-Wavelength O O O O B-CelestialObject I-CelestialObject O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O B-CelestialObject I-CelestialObject O O O O O O B-Citation I-Citation I-Citation O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O B-CelestialObject I-CelestialObject O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O B-CelestialObject I-CelestialObject O O O O O B-CelestialObject I-CelestialObject O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O B-CelestialObject I-CelestialObject O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O B-CelestialObject I-CelestialObject O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O
tokens: LMXBs. The disc temperature of GX 339–4 ranged from ∼0.6 to ∼0.9 keV (Plant et al. 2014 ) and the temperature of Cyg X–1 ranged between 0.5 and 0.6 keV (Shaposhnikov Titarchuk 2006 ). The temperature of 4U 1636–53 ranged from ∼0.3 to ∼0.8 keV in the best-fitting results (Zhang et al. 2017 ) and the disc temperature of MXB 1658–298 ranged from ∼0.6 to ∼0.9 keV (Sharma et al. 2018 ). The disc temperature of MAXI J1727–203 was lower than these four systems. A potential explanation for a lower temperature in MAXI J1727–203 than in other sources could be related to the mass of the compact object. Assuming that the accretion disc is at the innermost stable circular orbit (ISCO), the temperature at the inner disc radius is proportional to , where is the mass accretion rate and M is the mass of the compact object (Frank, King Raine 2002 ). According to Muñoz-Darias, Casares Martínez-Pais ( 2008 ), M 6 M ⊙ for GX 339–4. We take the temperature of GX 339–4 in the soft state (0.79 keV) from Plant et al. ( 2014 ) and we also take the disc temperature of the softest observation in the HID of MAXI J1727–203 (0.45 keV). From that, if we assume that is the same for two sources in the same spectral state, we estimate a lower limit for the mass of MAXI J1727–203 of ∼19 M ⊙ . Therefore, the high mass of the compact object can explain the low temperature of the inner disc. Alternatively, as suggested by Gou et al. ( 2011 ), the low temperature at the inner disc radius can be a consequence of a low inclination of the accretion disc with respect to the line of sight. We can repeat this analysis to estimate the mass of MAXI J1727–203 with the NS Aql X–1. For this, we took the temperature of Aql X–1 in the soft state of its 2007 outburst (∼0.66 keV, Raichur, Misra Dewangan 2011 ). Considering a mass of ∼1.4 M ⊙ for the NS in Aql X–1, we obtained a mass of ∼2 M ⊙ for the compact object in MAXI J1727–203. If we consider a higher mass for Aql X–1, the mass of MAXI J1727–203 also increases. Considering the latter, this mass estimates suggest that the compact object in MAXI J1727–203 is massive NS or a low-mass BH. Based on all the above comparisons, although we cannot unambiguously identify the nature of the compact object in MAXI J1727–203, the evolution in the HID, RID, and RHD, and the temperature at the inner radius of the accretion disc during the softest observations suggest that it is a BH. 4.2 Anticorrelation between the fractional rms amplitude and the flux of the disc component Fig. 9 shows that the relation between the fractional rms amplitude and the disc flux is continuous and that both quantities are anticorrelated during phases A and C (orange diamonds and black circles) of the outburst. While in phases B and D (blue triangles and red crosses), the rms amplitude is consistent with being independent of the disc flux, those measurements extend the relation seen in phases A and C to low (phase D) and high (phase B) values of the disc flux. The simplest