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| variable= [[Low-mass x-ray binary|LMXB]]<ref name=APJL2017/>
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'''3XMM J004232.1+411314''' is a [[low-mass x-ray binary]] (LMXB) hosted in the galaxy [[Andromeda Galaxy|M31]]. This object is notable for being the most luminous source of hard X-rays in the Andromeda Galaxy. This is also the most luminous source known that shows dips in the X-ray [[light curve]] <ref name=APJL2017/>. The compact object in this system has been unambigously identified as a [[neutron star]] with a spin period of 3 seconds.<ref name=APJL2018/>
'''3XMM J004232.1+411314''' is a [[low-mass X-ray binary]] hosted in the galaxy [[Andromeda Galaxy|M31]]. This object is notable for being the most luminous source of hard X-rays in the Andromeda Galaxy. This is also the most luminous source known that shows dips in the X-ray [[light curve]] <ref name=APJL2017/>. The compact object in this system has been unambiguously identified as a [[neutron star]] with a spin period of 3 seconds.<ref name=APJL2018/>


==Identification of the source==
==Identification of the source==
The [[Swift]] BAT all-sky survey detected hard X-rays (in the energy range 14-195 keV) in the direction of [[Andromeda Galaxy|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 [[Hubble Space Telescope|HST]] images ruled out the presence of stars more massive than 3 solar masses in that direction.<ref name=Yukita2017/>
The [[Swift]] BAT all-sky survey detected hard X-rays (in the energy range 14-195 keV) in the direction of [[Andromeda Galaxy|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 [[Hubble Space Telescope|HST]] images ruled out the presence of stars more massive than 3 solar masses in that direction.<ref name=Yukita2017/>


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 archivial 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. This behaviour is typical of x-ray binaries, then this source can be identified as a low-mass x-ray binary.<ref name=APJL2017/>
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. This behaviour is typical of X-ray binaries, then this source can be identified as a low-mass X-ray binary.<ref name=APJL2017/>


==System properties==
==System properties==
The 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. <ref name=APJL2017/>
The 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. <ref name=APJL2017/>
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{{e|38}} 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.<ref name=APJL2017/>
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{{e|38}} 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.<ref name=APJL2017/>


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.<ref name=APJL2018/>
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.<ref name=APJL2018/>


==External links==
==External links==

Revision as of 22:59, 20 October 2018

3XMM J004232.1+411314
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
SIMBADdata

3XMM J004232.1+411314 is a low-mass X-ray binary hosted in the galaxy M31. This object is notable for being the most luminous source of hard X-rays in the Andromeda Galaxy. This 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]

Identification of the source

The 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. This behaviour is typical of X-ray binaries, then this source can be identified as a low-mass X-ray binary.[1]

System properties

The 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

  1. ^ 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{{citation}}: CS1 maint: unflagged free DOI (link)
  2. ^ 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, Bibcode:2018ApJ...861L..26R, doi:10.3847/2041-8213/aacf40{{citation}}: CS1 maint: unflagged free DOI (link)
  3. ^ 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, Bibcode:2017ApJ...838...47Y, doi:10.3847/1538-4357/aa62a3, hdl:1721.1/109690{{citation}}: CS1 maint: unflagged free DOI (link)
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