Discovery of 59 ms pulsations from 1RXS J141256.0+792204 (Calvera)

Zane, S.; Haberl, F.; Israel, G. L.; Burgay, M.; Mignani, Roberto; Turolla, R.; Possenti, A.; Esposito, P.; Champion, D. J.; Eatough, Ralph P.; Barr, E. D.; Krämer, M.

doi:10.1111/j.1365-2966.2010.17619.x

Cited by 32 publications

(112 citation statements)

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“…Frequency measurements from the two XMM-Newton observations of Calvera acquired by Zane et al (2011), as reduced by Halpern (2011), are also listed in Table 1 and shown in Figure 2. None of the observations are closely spaced enough to link coherently and obtain more precise timing parameters.…”

Section: Figurementioning

confidence: 99%

“…It was not until a pair of XMMNewton observations was obtained with high time resolution that Zane et al (2011) discovered the 59 ms pulsations from Calvera. The X-ray emission from Calvera is best described by a twotemperature (blackbody or hydrogen atmosphere) spectrum, with kT in the range 0.1-0.25 keV (Shevchuk et al 2009;Zane et al 2011). The fitted column density in these models is equal to or greater than the Galactic value of N H = 2.7 × 10 20 cm −2 (Kalberla et al 2005), which, at its high Galactic latitude of +37…”

Section: Introductionmentioning

confidence: 99%

“…Calvera remains radio quiet even after deep searches for radio pulsations at the known period (Hessels et al 2007;Zane et al 2011). Analyzing data from the Fermi Large Area Telescope (LAT), Zane et al (2011) concluded that γ -ray pulsations are detected from Calvera at >100 MeV.…”

Section: Introductionmentioning

confidence: 99%

“…Analyzing data from the Fermi Large Area Telescope (LAT), Zane et al (2011) concluded that γ -ray pulsations are detected from Calvera at >100 MeV. Halpern (2011) reanalyzed the XMM-Newton timing data in detail together with additional Fermi data, showing that the claimed Fermi detection was not real.…”

Section: Introductionmentioning

confidence: 99%

“…Calvera has at least twice the temperature of the INSs, but its age and magnetic field strength were undetermined until now. These unknowns allowed Zane et al (2011) and Halpern (2011) to hypothesize that Calvera is either a mildly recycled pulsar (as defined by Belczynski et al 2010) or the first candidate for the elusive descendants of the central compact objects (CCOs) in supernova remnants, thermally emitting NSs that have weak dipole fields in the range (0.3-1) × 10 11 G (Gotthelf et al 2013). However, if B > 10 11 G, it could just be an ordinary rotation-powered pulsar.…”

Section: Introductionmentioning

confidence: 99%

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X-Ray Measurement of the Spin-Down of Calvera: A Radio- And Gamma-Ray-Quiet Pulsar

Halpern

Bogdanov

Gotthelf

2013

ApJ

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We measure spin-down of the 59 ms X-ray pulsar Calvera by comparing the XMM-Newton discovery data from 2009 with new Chandra timing observations taken in 2013. Its period derivative isṖ = (3.19 ± 0.08) × 10 −15 , which corresponds to spin-down luminosityĖ = 6.1 × 10 35 erg s −1 , characteristic age τ c ≡ P /2Ṗ = 2.9 × 10 5 yr, and surface dipole magnetic field strength B s = 4.4 × 10 11 G. These values rule out a mildly recycled pulsar, but Calvera could be an orphaned central compact object (anti-magnetar), with a magnetic field that was initially buried by supernova debris and is now reemerging and approaching normal strength. We also performed unsuccessful searches for high-energy γ -rays from Calvera in both imaging and timing of >100 MeV Fermi photons. Even though the distance to Calvera is uncertain by an order of magnitude, an upper limit of d < 2 kpc inferred from X-ray spectra implies a γ -ray luminosity limit of <3.3 × 10 32 erg s −1 , which is less than that of any pulsar of comparableĖ. Calvera shares some properties with PSR J1740+1000, a young radio pulsar that we show by virtue of its lack of proper motion was born outside of the Galactic disk. As an energetic, high-Galactic-latitude pulsar, Calvera is unique in being undetected in both radio and γ -rays to faint limits, which should place interesting constraints on models for particle acceleration and beam patterns in pulsar magnetospheres.

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Section: Figurementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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X-Ray Measurement of the Spin-Down of Calvera: A Radio- And Gamma-Ray-Quiet Pulsar

Halpern

Bogdanov

Gotthelf

2013

ApJ

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The peculiar isolated neutron star in the Carina Nebula

Pires

Motch

Turolla

et al. 2012

A&A

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While fewer in number than the dominant rotation-powered radio pulsar population, peculiar classes of isolated neutron stars (INSs) -which include magnetars, the ROSAT-discovered "Magnificent Seven" (M7), rotating radio transients (RRATs), and central compact objects in supernova remnants (CCOs) -represent a key element in understanding the neutron star phenomenology. We report the results of an observational campaign to study the properties of the source 2XMM J104608.7-594306, a newly discovered thermally emitting INS. The evolutionary state of the neutron star is investigated by means of deep dedicated observations obtained with the XMM-Newton Observatory, the ESO Very Large Telescope, as well as publicly available γ-ray data from the Fermi Space Telescope and the AGILE Mission. The observations confirm previous expectations and reveal a unique type of object. The source, which is likely within the Carina Nebula (N H = 2.6 × 10 21 cm −2 ), has a spectrum that is both thermal and soft, with kT ∞ = 135 eV. Non-thermal (magnetospheric) emission is not detected down to 1% (3σ, 0.1-12 keV) of the source luminosity. Significant deviations (absorption features) from a simple blackbody model are identified in the spectrum of the source around energies 0.6 keV and 1.35 keV. While the former deviation is likely related to a local oxygen overabundance in the Carina Nebula, the latter can only be accounted for by an additional spectral component, which is modelled as a Gaussian line in absorption with EW = 91 eV and σ = 0.14 keV (1σ). Furthermore, the optical counterpart is fainter than m V = 27 (2σ) and no γ-ray emission is significantly detected by either the Fermi or AGILE missions. Very interestingly, while these characteristics are remarkably similar to those of the M7 or the only RRAT so far detected in X-rays, which all have spin periods of a few seconds, we found intriguing evidence of very rapid rotation, P = 18.6 ms, at the 4σ confidence level. We interpret these new results in the light of the observed properties of the currently known neutron star population, in particular those of standard rotation-powered pulsars, recycled objects, and CCOs. We find that none of these scenarios can satisfactorily explain the collective properties of 2XMM J104608.7-594306, although it may be related to the still poorly known class of Galactic anti-magnetars. Future XMM-Newton data, granted for the next cycle of observations (AO11), will help us to improve our current observational interpretation of the source, enabling us to significantly constrain the rate of pulsar spin down.

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XMM-Newtonreveals a candidate period for the spin of the “Magnificent Seven” neutron star RX J1605.3+3249

Pires¹,

Haberl²,

Zavlin³

et al. 2014

A&A

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Context. The group of seven thermally emitting isolated neutron stars (INSs) discovered by ROSAT and known as the "Magnificent Seven" (M7) is unique among the various neutron star populations. Crustal heating by means of magnetic field decay and an evolutionary link with magnetars may explain why these objects rotate more slowly and have higher thermal luminosities and magnetic field intensities than standard rotation-powered pulsars of similar age. Aims. The third brightest INS, RX J1605.3+3249, is the only object amidst the seven still lacking a detected periodicity. The source spectrum, while purely thermal with no significant magnetospheric emission, is complex and displays both narrow and broad absorption features that can potentially be used to constrain the surface component of the magnetic field, as well as the mass-to-radius ratio of the neutron star. Methods. We observed the source with the XMM-Newton Observatory for 60 ks aiming at unveiling the neutron star rotation rate and investigating its spectrum in detail. We confront our results with previous observations of the source and discuss its properties in the context of the M7 as a group and of the known population of Galactic INSs. Results. A periodic signal at P = 3.387864(16) s, most likely the neutron star spin period, is detected at the 4σ confidence level. The amplitude of the modulation was found to be energy dependent and is more significantly detected when the timing search is restricted to photons with energy higher than ∼0.5 keV. The coherent combination of the new data with a past XMM-Newton EPIC-pn observation of the source constrains the pulsar spin-down rate at the 2σ confidence level,ν ∼ −1.39 × 10 −13 Hz s −1 , implying a dipolar magnetic field of B dip ∼ 7.4 × 10 13 G. If confirmed, RX J1605.3+3249 would be the neutron star with the highest dipolar field amongst the M7. The spectrum of the source shows evidence of a cool blackbody component, as well as for the presence of two broad absorption features. Furthermore, high-resolution spectroscopy with the RGS cameras confirms the presence of a narrow absorption feature at energy ∼0.57 keV in the co-added spectrum of the source, also seen in other thermally emitting isolated neutron stars. Conclusions. Phase-resolved spectroscopy, as well as a dedicated observing campaign aimed at determining a timing solution, will give invaluable constraints on the neutron star geometry and will allow one to confirm the high value of spin down, which would place the source closer to a magnetar than any other M7 INS.

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Discovery of 59 ms pulsations from 1RXS J141256.0+792204 (Calvera)

Cited by 32 publications

References 61 publications

X-Ray Measurement of the Spin-Down of Calvera: A Radio- And Gamma-Ray-Quiet Pulsar

X-Ray Measurement of the Spin-Down of Calvera: A Radio- And Gamma-Ray-Quiet Pulsar

The peculiar isolated neutron star in the Carina Nebula

XMM-Newtonreveals a candidate period for the spin of the “Magnificent Seven” neutron star RX J1605.3+3249

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