TY - JOUR
T1 - Updated phase coherent timing solution of the isolated neutron star RX J0720.4-3125 using recent XMM-Newton and Chandra observations
AU - Hohle, M.M.
AU - Haberl, F.
AU - Vink, J.
AU - Turolla, R.
AU - Zane, S.
AU - de Vries, C.P.
AU - Méndez, M.
PY - 2010
Y1 - 2010
N2 - Aims. Since the last phase coherent timing solution of the nearby radio-quiet isolated neutron star RXJ0720.4−3125 six new
XMM-Newton and three Chandra observations were carried out. The phase coherent timing solutions from previous authors were
performed without restricting to a fixed energy band. However, we recently showed that the phase residuals are energy dependent,
and thus phase coherent solutions must be computed referring always to the same energy band.
Methods. We updated the phase coherent timing solution for RXJ0720.4−3125 by including the recent XMM-Newton EPIC-pn,
MOS1, MOS2 and Chandra ACIS data in the energy range 400–1000 eV. Altogether these observations cover a time span of almost
10 yrs. A further timing solution was obtained including the ROSAT pointed data. In this case, observations cover a time span of
≈16 yrs. To illustrate the timing differences between the soft band (120–400 eV) and the hard band (400–1000 eV) a timing solution
for the soft band is also presented and the results are verified using a Z2
n test.
Results. In contrast to previous work, we obtain almost identical solutions whether or not we include the ROSAT or Chandra data.
Thanks to the restriction to the hard band, the data points from EPIC-pn are in better agreement with those from MOS1, MOS2 and
Chandra than in previous works. In general the phase residuals are still large and vary with time. In particular, the latest XMM-Newton
and Chandra data show that the phase residuals have attained relatively large and negative values. Using this and previous timing solutions,
the residuals indicate a cyclic behaviour with a period ≈7–9 yrs if the variations follow a sinusoid, or twice this value in case
the residuals are modulated by an abs(sine) probably approaching a new minimum around MJD = 55 240 days (February 2010). As
an alternative interpretation, the phase residuals can be fitted with a glitch that occured around MJD = 53 000 days.
AB - Aims. Since the last phase coherent timing solution of the nearby radio-quiet isolated neutron star RXJ0720.4−3125 six new
XMM-Newton and three Chandra observations were carried out. The phase coherent timing solutions from previous authors were
performed without restricting to a fixed energy band. However, we recently showed that the phase residuals are energy dependent,
and thus phase coherent solutions must be computed referring always to the same energy band.
Methods. We updated the phase coherent timing solution for RXJ0720.4−3125 by including the recent XMM-Newton EPIC-pn,
MOS1, MOS2 and Chandra ACIS data in the energy range 400–1000 eV. Altogether these observations cover a time span of almost
10 yrs. A further timing solution was obtained including the ROSAT pointed data. In this case, observations cover a time span of
≈16 yrs. To illustrate the timing differences between the soft band (120–400 eV) and the hard band (400–1000 eV) a timing solution
for the soft band is also presented and the results are verified using a Z2
n test.
Results. In contrast to previous work, we obtain almost identical solutions whether or not we include the ROSAT or Chandra data.
Thanks to the restriction to the hard band, the data points from EPIC-pn are in better agreement with those from MOS1, MOS2 and
Chandra than in previous works. In general the phase residuals are still large and vary with time. In particular, the latest XMM-Newton
and Chandra data show that the phase residuals have attained relatively large and negative values. Using this and previous timing solutions,
the residuals indicate a cyclic behaviour with a period ≈7–9 yrs if the variations follow a sinusoid, or twice this value in case
the residuals are modulated by an abs(sine) probably approaching a new minimum around MJD = 55 240 days (February 2010). As
an alternative interpretation, the phase residuals can be fitted with a glitch that occured around MJD = 53 000 days.
U2 - 10.1051/0004-6361/200913661
DO - 10.1051/0004-6361/200913661
M3 - Article
SN - 0004-6361
VL - 521
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A11
ER -