Gas electron multiplier (GEM) detectors for an advanced x-ray monitor

Remillard, Ronald A.; Levine, Alan M.; Boughan, E.; Bradt, H.; Morgan, E.; Becker, U.; Nenonen, S.; Vilhu, O.

doi:10.1117/12.409152

Cited by 4 publications

(1 citation statement)

References 26 publications

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“…Ultimately, though, a wide-field monitoring campaign is needed to identify more transient AXPs in outburst. This can be accomplished in principle in the X-ray band, although the sensitivity of current and planned wide-field monitors (≈2 × 10 −11 erg cm −2 s −1 , 0.5-10 keV; Levine et al 1996;Remillard et al 2000;Braga & Mejía 2006) is only sufficient to barely detect a 10 35 erg s −1 magnetar to a distance of 4 kpc from Earth. On the other hand, the detections of XTE J1810-197 (Camilo et al 2006) and 1E 1547.0-5408 (Camilo et al 2007) in the radio with characteristic intensities of 100 mJy kpc 2 suggests that future radio surveys with the Low-Frequency Array, the Mileura Wide-field Array, or the Square Kilometer Array (e.g., Cordes, Lazio, & McLaughlin 2004) could provide the best constraints on the numbers of magnetars in the Galaxy.…”

Section: Discussionmentioning

confidence: 99%

A Search for New Galactic Magnetars in Archival Chandra and XMM-Newton Observations

Muno,

Gaensler,

Nechita

et al. 2007

Preprint

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We present constraints on the number of Galactic magnetars, which we have established by searching for sources with periodic variability in 506 archival Chandra observations and 441 archival XMM-Newton observations of the Galactic plane (|b|<5 • ). Our search revealed four sources with periodic variability on time scales of 200-5000 s, all of which are probably accreting white dwarfs. We identify 7 of 12 known Galactic magnetars, but find no new examples with periods between 5 and 20 s. We convert this non-detection into limits on the total number of Galactic magnetars by computing the fraction of the young Galactic stellar population that was included in our survey. We find that easily-detectable magnetars, modeled after persistent anomalous X-ray pulsars (e.g., either with X-ray luminosities L X =3×10 33 erg s −1 [0.5-10.0 keV] and fractional rms amplitudes A rms =70%, or L X =10 35 erg s −1 and A rms =12%), could have been identified in ≈5% of the Galactic spiral arms by mass. If we assume that there are 3 previously-known examples within our random survey, then there are 59 +92 −32 in the Galaxy. Barely-detectable magnetars (L X = 3 × 10 33 erg s −1 [0.5-10.0 keV] and A rms =15%) could have been identified throughout ≈0.4% of the spiral arms. The lack of new examples implies that <540 exist in the Galaxy (90% confidence). Similar constraints are found by considering the detectability of transient magnetars in outburst by current and past X-ray missions. For assumed lifetimes of 10 4 yr, we find that the birth rate of magnetars could range between 0.003 and 0.06 yr −1 . Therefore, the birth rate of magnetars is at least 10% of that for normal radio pulsars. The magnetar birth rate could exceed that of radio pulsars, unless the lifetimes of transient magnetars are 10 5 yr. Obtaining better constraints will require wide-field X-ray or radio searches for transient X-ray pulsars similar to XTE J1810-197, AX J1845.0-0250, CXOU J164710. 2-455216, and 1E 1547.0-5408.

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Section: Discussionmentioning

confidence: 99%

A Search for New Galactic Magnetars in Archival Chandra and XMM-Newton Observations

Muno,

Gaensler,

Nechita

et al. 2007

Preprint

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Gem detectors for X-ray astronomy

Andersson¹,

Andersson²,

Heino

et al. 2003

Nuclear Instruments and Methods in Physics Research Section A:

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A Search for New Galactic Magnetars in ArchivalChandraandXMM‐NewtonObservations

Muno

Gaensler

Nechita³

et al. 2008

ApJ

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We present constraints on the number of Galactic magnetars, which we have established by searching for sources with periodic variability in 506 archival Chandra observations and 441 archival XMM-Newton observations of the Galactic plane (jbj < 5 ). Our search revealed four sources with periodic variability on timescales of 200Y5000 s, all of which are probably accreting white dwarfs. We identify 7 of 12 known Galactic magnetars, but find no new examples with periods between 5 and 20 s. We convert this nondetection into limits on the total number of Galactic magnetars by computing the fraction of the young Galactic stellar population that our survey covered. We find that easily detectable magnetars, modeled after persistent anomalous X-ray pulsars (e.g., with L X ¼ 10 35 ergs s À1 [0.5Y 10.0 keV] and A rms ¼ 12%), could have been identified in %5% of the Galactic spiral arms by mass. If we assume that three previously known examples randomly fall within our survey, then there are 59 þ92 À32 in the Galaxy. Barely detectable magnetars (L X ¼ 3 ; 10 33 ergs s À1 and A rms ¼ 15%) could have been identified throughout %0.4% of the spiral arms. The lack of new examples implies that <540 exist in the Galaxy (90% confidence). Similar constraints are found by considering the detectability of transient magnetars in outburst. For assumed lifetimes of 10 4 yr, the birth rate of magnetars is between 0.003 and 0.06 yr À1 . Therefore, the birth rate of magnetars is at least 10% of that for normal radio pulsars, and could exceed that value, unless transient magnetars are active for k10 5 yr.

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Gas electron multiplier (GEM) detectors for an advanced x-ray monitor

Cited by 4 publications

References 26 publications

A Search for New Galactic Magnetars in Archival Chandra and XMM-Newton Observations

A Search for New Galactic Magnetars in Archival Chandra and XMM-Newton Observations

Gem detectors for X-ray astronomy

A Search for New Galactic Magnetars in ArchivalChandraandXMM‐NewtonObservations

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