<i>XMM-Newton</i>
                    Discovery of 7 s Pulsations in the Isolated Neutron Star RX J1856.5-3754

Tiengo, A.; Mereghetti, S.

doi:10.1086/513143

Cited by 75 publications

(66 citation statements)

References 14 publications

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“…On the other hand, RX J1856.5−3754 is twice as bright as RX J0720.4−3125 and has been observed repeatedly, but no variability has been reported. Interestingly this is the only XDINS without spectral lines [11] and with the smallest pulsed fraction (∼1.5% [151]). …”

Section: The X-ray Dim Isolated Neutron Starsmentioning

confidence: 87%

X-ray emission from isolated neutron stars

Mereghetti

2010

High-Energy Emission From Pulsars and Their Systems

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X-ray emission is a common feature of all varieties of isolated neutron stars (INS) and, thanks to the advent of sensitive instruments with good spectroscopic, timing, and imaging capabilities, X-ray observations have become an essential tool in the study of these objects. Non-thermal X-rays from young, energetic radio pulsars have been detected since the beginning of X-ray astronomy, and the long-sought thermal emission from cooling neutron star's surfaces can now be studied in detail in many pulsars spanning different ages, magnetic fields, and, possibly, surface compositions. In addition, other different manifestations of INS have been discovered with X-ray observations. These new classes of high-energy sources, comprising the nearby X-ray Dim Isolated Neutron Stars, the Central Compact Objects in supernova remnants, the Anomalous X-ray Pulsars, and the Soft Gamma-ray Repeaters, now add up to several tens of confirmed members, plus many candidates, and allow us to study a variety of phenomena unobservable in "standard" radio pulsars.

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Section: The X-ray Dim Isolated Neutron Starsmentioning

confidence: 87%

X-ray emission from isolated neutron stars

Mereghetti

2010

High-Energy Emission From Pulsars and Their Systems

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“…The distance to the nearest known pulsar in the LIGO frequency band, PSR J0437 ÿ 4715, is about 140 pc. The other nearest neutron stars are at comparable distances [32,34] including RX J1856:5 ÿ 3754, which may be the nearest of all and was found to have a pulsation period out of the LIGO band after this article was submitted [35]. Therefore our search would be sensitive only to previously unknown objects.…”

Section: Expected Sensitivity Of the S2 Searchmentioning

confidence: 99%

“…From Eq. (35) it is straightforward to recognize that Q 2 is simply related to the noncentrality parameter 2 for a signal amplitude h 0 by …”

Section: Data Selection For the Sco X-1 Searchmentioning

confidence: 99%

Searches for periodic gravitational waves from unknown isolated sources and Scorpius X-1: Results from the second LIGO science run

Abbott¹,

Abbott²,

Adhikari³

et al. 2007

Phys. Rev. D

154

183

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We carry out two searches for periodic gravitational waves using the most sensitive few hours of data from the second LIGO science run. Both searches exploit fully coherent matched filtering and cover wide areas of parameter space, an innovation over previous analyses which requires considerable algorithm development and computational power. The first search is targeted at isolated, previously unknown neutron stars, covers the entire sky in the frequency band 160 -728.8 Hz, and assumes a frequency derivative of less than 4 10 ÿ10 Hz=s. The second search targets the accreting neutron star in the lowmass x-ray binary Scorpius X-1 and covers the frequency bands 464-484 Hz and 604-624 Hz as well as the two relevant binary orbit parameters. Because of the high computational cost of these searches we limit the analyses to the most sensitive 10 hours and 6 hours of data, respectively. Given the limited sensitivity and duration of the analyzed data set, we do not attempt deep follow-up studies. Rather we concentrate on demonstrating the data analysis method on a real data set and present our results as upper limits over large volumes of the parameter space. In order to achieve this, we look for coincidences in parameter space between the Livingston and Hanford 4-km interferometers. For isolated neutron stars our 95% confidence level upper limits on the gravitational wave strain amplitude range from 6:6 10 ÿ23 to 1 10 ÿ21 across the frequency band; for Scorpius X-1 they range from 1:7 10 ÿ22 to 1:3 10 ÿ21 across the two 20-Hz frequency bands. The upper limits presented in this paper are the first broadband wide parameter space upper limits on periodic gravitational waves from coherent search techniques. The methods developed here lay the foundations for upcoming hierarchical searches of more sensitive data which may detect astrophysical signals.

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“…Among known XDINSs, J1856 has the lowest pulsed fraction, ∼1% (Tiengo & Mereghetti 2007), and the weakest magnetic field, B ∼ 1.5 × 10 13 G (van Kerkwijk & Kaplan 2008). Being the brightest, f X ∼ 1.5 × 10 −11 erg s −1 cm −2 , and closest of the category, d = 123 +11 −15 pc (e.g.…”

Section: Introductionmentioning

confidence: 99%

Spectral monitoring of RX J1856.5-3754 withXMM-Newton

Sartore

Tiengo

Mereghetti

et al. 2012

A&A

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Using a large set of XMM-Newton observations, we searched for the long-term spectral and flux variability of the isolated neutron star RX J1856.5-3754 in the time interval from April 2002 to October 2011. This is the brightest and most extensively observed source of a small group of nearby, thermally emitting isolated neutron stars, of which at least one member (RX J0720.4-3125) has shown long-term variability. A detailed analysis of the data obtained with the EPIC-pn camera in the 0.15−1.2 keV energy range reveals only small variations in the temperature derived with a single blackbody fit (of about 1% around an average value of kT ∞ ∼ 61 eV). These variations appear to be correlated with the position of the source on the detector and can be ascribed to an instrumental effect, most likely a spatial dependence of the channel-to-energy relation. For the sampled instrumental coordinates, we quantify this effect as variations of ∼4% and ∼15 eV in the gain slope and offset, respectively. Selecting only a homogeneous subset of observations, with the source imaged at the same detector position, we find no evidence of either spectral or flux variations of RX J1856. The high-quality-statistics source spectrum from the selected observations is best fitted with the sum of two blackbody models, with temperatures of kT ∞ h = 62.4 +0.6 −0.4 eV and kT ∞ s = 38.9 +4.9 −2.9 eV, which can also account for the flux seen in the optical band. No significant narrow or broad spectral features are detected, with upper limits of ∼6 eV on their equivalent width.

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XMM-Newton Discovery of 7 s Pulsations in the Isolated Neutron Star RX J1856.5-3754

Cited by 75 publications

References 14 publications

X-ray emission from isolated neutron stars

X-ray emission from isolated neutron stars

Searches for periodic gravitational waves from unknown isolated sources and Scorpius X-1: Results from the second LIGO science run

Spectral monitoring of RX J1856.5-3754 withXMM-Newton

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