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

Yuan, Min; Chongyang, Ren; Zhang, Pengfei; Jiang, Z. J.; Zhang, Li

doi:10.1088/1674-4527/ac9579

Cited by 6 publications

(4 citation statements)

References 72 publications

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“…It can be seen that there is one MSP, PSR J1312 +1810E, in NGC 5024 with  E> 10 35 erg s −1 . No emission has been found from this GC (e.g., Yuan et al 2022a), while it can be noted that the distance to the GC is large, ∼18 kpc (Harris 1996;Baumgardt & Vasiliev 2021), which may explain the nondetection at γ-rays of the GC (or the MSP). In any case, this MSP is of interest as its η already reaches ∼10 −3 .…”

Section: Implication For γ-Ray Emissions Of Gc Mspsmentioning

confidence: 88%

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: Implication For γ-Ray Emissions Of Gc Mspsmentioning

confidence: 88%

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

Self Cite

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show abstract

“…It can be seen that there is one MSP, PSR J1312+1810E, in NGC 5024 with Ė >10 35 erg s −1 . No emission has been found from this GC (e.g., Yuan et al 2022a), while it can be noted that the distance to the GC is large, ∼18 kpc (Harris 1996;Baumgardt & Vasiliev 2021), which may explain the non-detection at γ-rays of the GC (or the MSP). In any case, this MSP is of interest as its η already reaches ∼ 10 −3 .…”

Section: Implication For γ-Ray Emissions Of Gc Mspsmentioning

confidence: 86%

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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“…Dedicated pulsar searches in the radio band, as well as searches for gamma-ray pulsations, could shed significant light on the nature of the Sgr/M54 system. Recently, Yuan et al (2022) performed a study of a number of gamma-ray bright GCs, including M54. The authors searched for pulsations in Fermi-LAT data and found no evidence for time-dependent variations in M54's flux.…”

Section: Dark Matter Interpretationmentioning

confidence: 99%

On the gamma-ray emission from the core of the Sagittarius dwarf galaxy

Evans

Strigari

Svenborn

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We use Fermi-LAT data to analyze the faint gamma-ray source located at the center of the Sagittarius (Sgr) dwarf spheroidal galaxy. In the 4FGL-DR3 catalog, this source is associated with the globular cluster, M54. We investigate the spectral energy distribution and spatial extension of this source, with the goal of testing two hypotheses: (1) the emission is due to millisecond pulsars within M54, or (2) the emission is due to annihilating dark matter from the Sgr halo. For the pulsar interpretation, we consider a two-component model which describes both the lower-energy magnetospheric emission and possible high-energy emission arising from inverse Compton scattering. We find that this source has a point-like morphology at low energies, consistent with magnetospheric emission, and find no evidence for a higher-energy component. For the dark matter interpretation, we find the signal favors a dark matter mass of mχ = 29.6 ± 5.8 GeV and an annihilation cross section of σv = (2.1 ± 0.59) × 10−26 cm3 s−1 for the $b \bar{b}$ channel (or mχ = 8.3 ± 3.8 GeV and σv = (0.90 ± 0.25) × 10−26 cm3 s−1 for the τ+τ− channel), when adopting a J-factor of J = 1019.6 GeV2 cm−5. This parameter space is consistent with gamma-ray constraints from other dwarf galaxies and with dark matter interpretations of the Galactic Center Gamma-Ray Excess.

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

Cited by 6 publications

References 72 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

On the gamma-ray emission from the core of the Sagittarius dwarf galaxy

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