Discovery of γ-Ray Pulsations from PSR J1835–3259B in the Globular Cluster NGC 6652

Zhang, Pengfei; Xing, Yi; Wang, Zhongxiang

doi:10.3847/2041-8213/ac88bf

Cited by 7 publications

(18 citation statements)

References 34 publications

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“…Then in NGC 6626 (M28), significances of ∼4.3σ and 5.4σ γ-ray pulsations were respectively reported for PSR B1821−24 by Wu et al (2013) and Johnson et al (2013). Very recently, Zhang et al (2022) reported the detection of γray pulsations (at a 5.4σ significance level) of a newly discovered MSP J1835−3259B in NGC 6652 (Gautam et al 2022). The properties of these three MSPs are summarized in Table 1.…”

Section: Introductionmentioning

confidence: 95%

Likely Detection of γ-Ray Pulsations of PSR J1717+4308A in NGC 6341 and Implication of the γ-Ray Millisecond Pulsars in Globular Clusters

Zhang

Xing

Wang

et al. 2023

ApJ

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We report our analysis results for the globular cluster (GC) NGC 6341 (M92), as a millisecond pulsar (MSP) J1717+4308A has recently been reported found in this GC. The data used are from the Large Area Telescope onboard the Fermi Gamma-ray Space Telescope (Fermi). We detect γ-ray pulsations of the MSP at a 4.4σ confidence level (the corresponding weighted H-test value is ∼28.4). This MSP, the fourth γ-ray pulsar found in a GC, does not have significant off-pulse emission and has γ-ray luminosity and efficiency 1.3 × 1034 erg s−1 and 1.7%, respectively. In order to have a clear view on the properties of the known GC γ-ray MSPs, we reanalyze the Fermi-LAT data for the other three ones. These four MSPs share the properties of either having high E ̇ (∼1036 erg s−1) or being in the GCs that contain only limited numbers of known MSPs. In addition, we find that PSRs J1823−3021A and B1821−24, in NGC 6624 and NGC 6626, respectively, have detectable off-pulse γ-ray emission and PSR J1835−3259B in NGC 6652 does not. Using the obtained off-pulse spectra or spectral upper limits, we constrain the numbers of other MSPs in the four GCs. The results are consistent with the numbers of the radio pulsars reported in them. While at least in NGC 6624 and NGC 6626, the contribution of other MSPs to their observed γ-ray emission can not be ignored, our study indicates that the presence of a bright MSP could be the dominant factor for whether a GC is detectable at γ-rays or not.

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Section: Introductionmentioning

confidence: 95%

Likely Detection of γ-Ray Pulsations of PSR J1717+4308A in NGC 6341 and Implication of the γ-Ray Millisecond Pulsars in Globular Clusters

Zhang

Xing

Wang

et al. 2023

ApJ

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“…In order to separate a known pulsar's emission from that of the host GC, we carried out the similar data analysis for NGC 6624 and NGC 6626 as for NGC 6341. The analysis results for NGC 6652 were taken from that reported in Zhang et al (2022).…”

Section: Data Analysis For Three Known Gc γ-Ray Mspsmentioning

confidence: 99%

“…Pulse-phase resolved analysis for the emission of NGC 6652 was conducted by Zhang et al (2022), and in a small off-pulse phase range they defined, no emission was detected (TS 1). Using the results, we calculated a TS map in 0.1-500 GeV and include it in Figure 6.…”

Section: Phase-resolved Analysismentioning

confidence: 99%

“…The properties of these three MSPs are summarized in Table 1. They share the similarities of having relatively high spin-down energies Ė, their γ-ray luminosities being among the brightest ones of all known γ-ray MSPs (Zhang et al 2022), and they probably contribute a dominant fraction to the γ-ray emission of each of the respective host GCs. More such γ-ray MSPs may be found in GCs, provided accurate radio ephemerides are available.…”

Section: Introductionmentioning

confidence: 99%

“…The numbers estimated in this latter work indicate that for approximately 10 GCs, only one MSP may be required in them to explain the observed γ-ray emissions. Combined with the likely dominant contributions of the detected three GC MSPs to the γ-ray emissions of their respective host GCs (Freire et al 2011;Wu et al 2013;Johnson et al 2013;Zhang et al 2022), an interesting question may be raised as if the γ-ray emissions of most GCs are similarly due to the presence of one bright γ-ray MSP (i.e., not reflecting the MSP numbers). This possibility may explain why some of GCs, while with high encounter rates, do not have detectable γ-ray emissions (e.g., see Wu et al 2022); it would be rather because they do not contain one sufficiently bright MSP.…”

Section: Introductionmentioning

confidence: 99%

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Likely detection of gamma-ray pulsations of PSR~J1717+4308A in NGC~6341 and implication of the gamma-ray millisecond pulsars in globular clusters

Zhang¹,

Xing²,

Wang³

et al. 2023

Preprint

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We report our analysis results for the globular cluster (GC) NGC 6341 (M92), as a millisecond pulsar (MSP) J1717+4308A has recently been reported found in this GC. The data used are from the Large Area Telescope onboard the Fermi Gamma-ray Space Telescope (Fermi). We detect γ-ray pulsations of the MSP at a 4.4σ confidence level (the corresponding weighted H-test value is ∼28.4). This MSP, the fourth γ-ray pulsar found in a GC, does not have significant off-pulse emission and has γ-ray luminosity and efficiency 1.3 × 10 34 erg s −1 and 1.7% respectively. In order to have a clear view on the properties of the known GC γ-ray MSPs, we re-analyze the Fermi LAT data for the other three ones. These four MSPs share the properties of either having high Ė (∼ 10 36 erg s −1 ) or being in the GCs that contain only limited numbers of known MSPs. In addition, we find that PSRs J1823−3021A and B1821−24, in NGC 6624 and NGC 6626 respectively, have detectable off-pulse γ-ray emission and PSR J1835−3259B in NGC 6652 does not. Using the obtained off-pulse spectra or spectral upper limits, we constrain the numbers of other MSPs in the four GCs. The results are consistent with the numbers of the radio pulsars reported in them. While at least in NGC 6624 and NGC 6626, the contribution of other MSPs to their observed γ-ray emission can not be ignored, our study indicates that the presence of a bright MSP could be the dominant factor for whether a GC is detectable at γ-rays or not.

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Detection of the Farthest Globular Cluster NGC 6715 and Two Other GCs in Gamma-Rays with Fermi-LAT

Yuan

Chongyang²,

Zhang³

et al. 2022

Res. Astron. Astrophys.

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In this paper, $\sim12-$year long$-$term Pass 8 data from \emph{Fermi} Large Area Telescope for the 157 globular clusters are carefully re-analyzed. Besides the 31 globular clusters reported in the fourth \emph{Fermi} Large Area Telescope catalogue Data Release 2, NGC 1851 is identified as a gamma-ray emitter and the significant gamma$-$ray emissions from NGC 6715 and NGC 6723 are detected. Especially NGC 6715 locates at a distance of 26.8 kpc, so far it is the farthest globular cluster detected in gamma-rays. A detailed analysis for these three globular clusters has been performed, but their gamma-ray pulsation emissions or flux variabilities are not found. The numbers of millisecond pulsars in these globular clusters are estimated under the assumption that each millisecond pulsar inside globular clusters emits a similar amount of gamma$-$rays. Some possible origins, such as MSPs, pulsar binary systems and/or dark matter, of gamma−ray emission from globular clusters are discussed.

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Discovery of γ-Ray Pulsations from PSR J1835–3259B in the Globular Cluster NGC 6652

Cited by 7 publications

References 34 publications

Likely Detection of γ-Ray Pulsations of PSR J1717+4308A in NGC 6341 and Implication of the γ-Ray Millisecond Pulsars in Globular Clusters

Likely Detection of γ-Ray Pulsations of PSR J1717+4308A in NGC 6341 and Implication of the γ-Ray Millisecond Pulsars in Globular Clusters

Likely detection of gamma-ray pulsations of PSR~J1717+4308A in NGC~6341 and implication of the gamma-ray millisecond pulsars in globular clusters

Detection of the Farthest Globular Cluster NGC 6715 and Two Other GCs in Gamma-Rays with Fermi-LAT

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