3XMM J004232.1+411314 is a low-mass X-ray binary hosted in the galaxy M31. It is the most luminous source of hard X-rays in the Andromeda Galaxy. It is also the most luminous source known that shows dips in the X-ray light curve.[1] The compact object in this system has been unambiguously identified as a neutron star with a spin period of 3 seconds.[2]
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Andromeda |
| Right ascension | 00h 42m 32.072s[1] |
| Declination | +41° 13′ 14.33″[1] |
| Characteristics | |
| Variable type | Low-mass X-ray binary[1] |
| Database references | |
| SIMBAD | data |
Identification of the source
editThe Swift BAT all-sky survey detected hard X-rays (in the energy range 14-195 keV) in the direction of M31 and found that this emission was centered in a region 6 arcseconds away from the galaxy center. Using a subsequent NuSTAR observation, it was found that a single source was responsible for this emission, and optical HST images ruled out the presence of stars more massive than 3 solar masses in that direction.[3]
The same source was earlier observed in soft X-rays by XMM-Newton, and was given the catalogue name 3XMM J004232.1+411314. By analysing archival data elaborated by the EXTraS project, this source showed dips (a short and linear decrease in the source luminosity, which returns subsequently at the previous luminosity level) in some observations. As this behaviour is typical of X-ray binaries, then this source can be identified as a low-mass X-ray binary.[1]
System properties
editThe orbit of this binary system has an inclination between 60° and 80° from our line of sight, since dips are observed only in this inclination range. The orbital period of the system is 4.01 hours, which is the same distance in time between two consecutive dips. [1] Like many others low-mass X-ray binaries, the luminosity of this source varies over time. Using XMM-Newton observations of Andromeda Galaxy, this source luminosity stays in the range 0.8–2.8×1038 erg/s in the 0.2-12 keV photon energy band. To date, this is the most luminous source that shows dips in its X-ray lightcurves.[1]
The compact object of this system is a neutron star with a spin period of 3 seconds, and this is proved by the observation of a modulation with the same period in the X-ray luminosity.[2]
References
edit- ^ a b c d e f g Marelli, M.; Tiengo, A.; De Luca, A.; Salvetti, D.; Saronni, L.; Sidoli, L.; Paizis, A.; Salvaterra, R.; Belfiore, A.; Israel, G.; Haberl, F.; D'Agostino, D. (2017), "Discovery of periodic dips in the brightest hard X-ray source of M31 with EXTraS", The Astrophysical Journal Letters, 851 (2): L27, arXiv:1711.05540, Bibcode:2017ApJ...851L..27M, doi:10.3847/2041-8213/aa9b2e, S2CID 119266242
- ^ a b Rodríguez Castillo, G.A.; Israel, G.L.; Esposito, P.; Papitto, A.; Stella, L.; Tiengo, A.; De Luca, A.; Marelli, M. (2018), "Discovery of a 3 s Spinning Neutron Star in a 4.15 hr Orbit in the Brightest Hard X-Ray Source in M31", The Astrophysical Journal Letters, 861 (2): L26, arXiv:1804.10858, Bibcode:2018ApJ...861L..26R, doi:10.3847/2041-8213/aacf40, S2CID 119007575
- ^ Yukita, M.; Ptak, A.; Hornschemeier, A.E.; Wik, D.; Maccarone, J.; Pottschmidt, K.; De Luca, A.; Zezas, A.; Antoniou, V.; Ballhausen, R.; Lehmer, B.D.; Lien, A.; Williams, B.; Baganoff, F.; Boyd, P.T.; Enoto, T.; Kennea, J.; Page, K.L.; Choi, Y. (2017), "Identification of the Hard X-ray Source Dominating the E > 25 keV Emission of the Nearby Galaxy M31", The Astrophysical Journal, 838 (1): 47, arXiv:1703.07318, Bibcode:2017ApJ...838...47Y, doi:10.3847/1538-4357/aa62a3, hdl:1721.1/109690, S2CID 118910239
External links
edit- Example of two consecutive dips in an X-ray light curve of this source[permanent dead link] From EXTraS Archive.