2017A&A...602A..81C


Query : 2017A&A...602A..81C

2017A&A...602A..81C - Astronomy and Astrophysics, volume 602A, 81-81 (2017/6-1)

Discovery of a 26.2 day period in the long-term X-ray light curve of SXP 1323: a very short orbital period for a long spin period pulsar.

CARPANO S., HABERL F. and STURM R.

Abstract (from CDS):

Context. About 120 Be/X-ray binaries (BeXBs) are known in the Small Magellanic Cloud (SMC); about half of them are pulsating with periods from a few to hundreds of seconds. SXP 1323 is one of the longest-period pulsars known in this galaxy.
Aims. SXP 1323 is in the field of view of a large set of calibration observations that we analyse systematically, focusing on the time analysis, in search of periodic signals.
Methods. We analyse all available X-ray observations of SXP 1323 from Suzaku, XMM-Newton, and Chandra, in the time range from 1999 to the end of 2016. We perform a Lomb-Scargle periodogram search in the band 2.5-10keV on all observations to detect the neutron star spin period and constrain its long-term evolution. We also perform an orbital period search on the long-term light curve, merging all datasets.
Results. We report the discovery of a 26.188±0.045d period analysing data from Suzaku, XMM-Newton, and Chandra, which confirms the optical period derived from the Optical Gravitational Lensing Experiment (OGLE) data. If this corresponds to the orbital period, this would be very short with respect to what is expected from the spin/orbital period relationship. We furthermore report on the spin period evolution in the last years. The source is spinning-up with an average rate of |dP/P| of 0.018yr–1, decreasing from ∼1340 to ∼1100s, in the period from 2006 to the end of 2016, which is also extreme with respect to the other Be/X-ray pulsars. From 2010 to the end of 2014, the pulse period is not clearly detectable, although the source was still bright.
Conclusions. SXP 1323 is a peculiar BeXB due to its long pulse period, rapid spin-up for several years, and short orbital period. A continuous monitoring of the source in the next years is necessary to establish the long-term behaviour of the spin period.

Abstract Copyright: © ESO, 2017

Journal keyword(s): galaxies: individual: Small Magellanic Cloud - stars: neutron - X-rays: binaries - X-rays: individuals: SXP 1323 - stars: emission-line, Be - stars: emission-line, Be

Simbad objects: 12

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Number of rows : 12
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 [MA93] 172 HXB 00 47 23.3388222768 -73 12 27.370134648   15.85 15.85   16.00 B1-B1.5V 50 0
2 SXP 214 HXB 00 50 11.2696971720 -73 00 25.972319016   15.22 15.33 15.47 15.47 B9(II) 16 0
3 [MA93] 413 HXB 00 50 56.9992401408 -72 13 34.582439136   14.97 15.05     B0.5III-V 58 0
4 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10535 1
5 SXP 327 HXB 00 52 52.2273385944 -72 17 15.106259724 15.83 16.41 16.62 16.43 16.82 ~ 23 0
6 RX J0053.4-7227 HXB 00 53 23.8589408040 -72 27 15.445929456 15.06 16.11 16.19   16.14 B1-B2IV-V 30 0
7 RX J0057.4-7325 HXB 00 57 27.000 -73 25 19.55 14.56 15.62 15.67 15.43 15.67 B3-B5Ib-II? 34 0
8 [MA93] 1036 HXB 00 57 49.5745148088 -72 02 35.873596896   15.52 15.64     B0-B2III-V 54 0
9 [MA93] 1393 HXB 01 03 37.5349856136 -72 01 33.204096336   14.54 14.65     B0III-V 68 0
10 SNR B0102-72.3 SNR 01 04 01.2 -72 01 52           ~ 383 1
11 WRAY 15-793 HXB 11 20 57.1736884968 -61 55 00.166078020 12.81 13.06 12.12     O9.5III/Ve 194 0
12 GSC 03588-00834 HXB 21 03 35.7100848936 +45 45 05.568751692   15.34 14.20 13.49 12.75 B0Ve 170 0

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2023.02.01-19:49:13

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