2015A&A...583A.117P


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST14:00:50

2015A&A...583A.117P - Astronomy and Astrophysics, volume 583A, 117-117 (2015/11-1)

New XMM-Newton observation of the thermally emitting isolated neutron star 2XMM J104608.7-594306.

PIRES A.M., MOTCH C., TUROLLA R., POPOV S.B., SCHWOPE A.D. and TREVES A.

Abstract (from CDS):

The isolated neutron star (INS) 2XMM J104608.7-594306 is one of the only two to be discovered through their thermal emission since the ROSAT era. Possibly a remnant of a former generation of massive stars in the Carina nebula, the exact nature of the source is unclear, and it might be unique amongst the several classes of Galactic INSs. In a first dedicated XMM-Newton observation of the source, we found intriguing evidence of a very fast spin period of P∼18.6ms at the 4σ confidence level. Moreover, spectral features in absorption have also been identified. We re-observed 2XMM J104608.7-594306 with XMM-Newton to better characterise the spectral energy distribution of the source, confirm the candidate spin period, and possibly constrain the pulsar spin-down. We used the two XMM-Newton observations of 2XMM J104608.7-594306 to perform detailed timing and spectral X-ray analysis. Both the spin-down rate and the energy of the spectral features provide estimates on the neutron star magnetic field, which are crucial for investigating the evolutionary state of the neutron star. Statistically acceptable spectral fits and meaningful physical parameters for the source are only obtained when the residuals at energies 0.55keV and 1.35keV are taken into account by the spectral modelling. While the former can result from the inhomogeneous temperature distribution on the surface of the neutron star or can be related to a local overabundance of oxygen in the Carina nebula, the one at 1.35keV is only satisfactorily accounted for by invoking a line in absorption. In this case, the best-fit neutron star atmosphere models constrain the hydrogen column density, the effective temperature, and the luminosity of the source within NH=(2.5-3.3)x1021cm–2, Teff=(6-10)x105K, and LX=(1.1-7.4)x1032erg/s. The implied distance is consistent with a location in (or in front of) the Carina nebula, and radiation radii are compatible with emission originating on most of the surface. Non-thermal X-ray emission is ruled out at levels above 0.5% (3σ) of the source luminosity. Unfortunately, the second XMM-Newton observation proved inconclusive in terms of confirming (discarding) the fast candidate spin, providing an upper limit on the pulsed fraction of the source that is very close to the limiting sensitivity for detecting the modulation found previously. In the absence of an unambiguous period determination and an estimate of the magnetic field, the nature of the source remains open to interpretation. Its likely association with the Carina cluster and its overall spectral properties (only shared by a handful of other peculiar INSs) disfavour a standard evolutionary path or one in which the source was previously recycled by accretion in a binary system. The star 2XMM J104608.7-594306 may be similar to Calvera (1RXS J141256.0+792204), a neutron star for which the scenario of an evolved anti-magnetar has been discussed. A better age estimate and deeper radio and γ-ray limits are required to further constrain the evolutionary state of the neutron star.

Abstract Copyright:

Journal keyword(s): stars: neutron - pulsars: general - X-rays: individuals: 2XMM J104608.7-594306

Simbad objects: 21

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Number of rows : 21

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14826 1
2 V* CM Tau Psr 05 34 31.93830 +22 00 52.1758           ~ 4803 1
3 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5594 4
4 PSR J0537-6910 Psr 05 37 46.66 -69 10 17.1           ~ 227 1
5 PSR B0540-69 Psr 05 40 10.84 -69 19 54.2           ~ 797 3
6 RX J0806.4-4123 N*? 08 06 23.0 -41 22 33           ~ 70 0
7 NAME Pup A SNR 08 24 07 -42 59.8           ~ 516 1
8 NAME Vela XYZ Rad 08 34.0 -45 50           ~ 1110 2
9 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545           ~ 2056 1
10 Cl Trumpler 14 29 * 10 44 05.0743332839 -59 33 41.340850432 12.138 12.437 11.943   11.019 B1.5V 24 0
11 NGC 3372 HII 10 44 19.0 -59 53 21           ~ 888 2
12 * eta Car Em* 10 45 03.5455050 -59 41 03.951060 6.37 7.034 6.21 4.90 4.41 OBepec 2198 0
13 CXOGNC J104608.71-594306.4 N*? 10 46 08.719 -59 43 06.48           ~ 14 0
14 SNR G295.5+09.7 SNR 12 09 40 -52 25.0           ~ 255 1
15 PSR J1210-5226 Psr 12 10 00.88 -52 26 28.4           ~ 202 1
16 RX J1412.9+7922 X 14 12 55.885 +79 22 04.10           ~ 27 0
17 SNR G353.6-00.7 SNR 17 31 55.0 -34 42 36           ~ 96 0
18 SNR G033.6+00.1 SNR 18 52 29.000 +00 38 42.00           ~ 238 1
19 PSR J2043+2740 Psr 20 43 43.5 +27 40 56           ~ 96 0
20 NAME Cas A SNR 23 23 24.000 +58 48 54.00           ~ 2413 1
21 NAME Magnificent Seven ? ~ ~           ~ 57 1

    Equat.    Gal    SGal    Ecl

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2020.07.04-14:00:50

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