Orbital Dynamics of Candidate Transitional Millisecond Pulsar 3FGL J1544.6-1125: An Unusually Face-on System

Britt, C. T.; Strader, Jay; Chomiuk, Laura; Tremou, Evangelia; Peacock, Mark B.; Halpern, J. P.; Salinas, R.

doi:10.3847/1538-4357/aa8e41

Cited by 26 publications

(21 citation statements)

References 68 publications

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“…In addition to the three confirmed tMSPs discussed above, there are a handful of candidate tMSPs discovered through multi-wavelength studies. These tMSP candidates include 1FGL J1417.7-4407, a gamma-ray source with an MSP counterpart and spectroscopic signs of mass transfer (Strader et al 2015;Camilo et al 2016); 1RXS J154439.4-112820 (3FGL J1544.6-1125), a gamma-ray and X-ray binary showing similar X-ray mode-switching behavior as seen in confirmed tMSPs (Bogdanov & Halpern 2015;Bogdanov 2016;Britt et al 2017); and 3FGL J0427.9-6704, an eclipsing low-mass Xray and gamma-ray binary with rapid X-ray variability (Strader et al 2016).…”

Section: Transitional Millisecond Pulsarsmentioning

confidence: 97%

The MAVERIC Survey: A Transitional Millisecond Pulsar Candidate in Terzan 5

Bahramian

Strader

Chomiuk

et al. 2018

ApJ

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Transitional millisecond pulsars are accreting millisecond pulsars that switch between accreting X-ray binary and millisecond radio pulsar states. Only a handful of these objects have been identified so far. Terzan 5 CX1 is a variable hard X-ray source in the globular cluster Terzan 5. In this paper, we identify a radio counterpart to CX1 in deep Very Large Array radio continuum data. Chandra observations over the last fourteen years indicate that CX1 shows two brightness states: in 2003 and 2016 the source was the brightest X-ray source in the cluster (at L X ∼ 10 33 erg s −1 ), while in many intermediate observations, its luminosity was almost an order of magnitude lower. We analyze all available X-ray data of CX1, showing that the two states are consistent with the spectral and variability properties observed for the X-ray active and radio pulsar states of known transitional millisecond pulsars. Finally, we discuss the prospects for the detection of CX1 as a radio pulsar in existing timing data.

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Section: Transitional Millisecond Pulsarsmentioning

confidence: 97%

The MAVERIC Survey: A Transitional Millisecond Pulsar Candidate in Terzan 5

Bahramian

Strader

Chomiuk

et al. 2018

ApJ

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“…In this so-called sub-luminous disk state, at least three accretion modes, namely the low (a few´10 32 erg s −1 ), high (a few ×10 33 erg s −1 ), and flare modes (∼10 34 erg s −1 ) are observed (de Martino et al 2013;. At least one candidate tMSP, 3FGLJ1544.6−1125, has been identified via its display of similar accretion modes and its other optical properties (Bogdanov & Halpern 2015;Britt et al 2017). Like 3FGLJ1544.6−1125, PSRJ1023+0038 and PSR J1227 −4853 have been observed to emit GeV γ-rays in the subluminous disk state (Stappers et al 2014;Johnson et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The Flare-dominated Accretion Mode of a Radio-bright Candidate Transitional Millisecond Pulsar

Strader²,

Miller-Jones

et al. 2020

ApJ

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We report new simultaneous X-ray and radio continuum observations of 3FGLJ0427.9−6704, a candidate member of the enigmatic class of transitional millisecond pulsars. These XMM-Newton and Australia Telescope Compact Array observations of this nearly edge-on, eclipsing low-mass X-ray binary were taken in the subluminous disk state at an X-ray luminosity of~d 10 2.3 kpc 33 2 () erg s −1. Unlike the few well-studied transitional millisecond pulsars, which spend most of their disk state in a characteristic high or low accretion mode with occasional flares, 3FGLJ0427.9−6704 stayed in the flare mode for the entire X-ray observation of ∼20 hr, with the brightest flares reaching ∼2×10 34 erg s −1. The source continuously exhibited flaring activity on timescales of ∼10-100 s in both the X-ray and optical/ultraviolet (UV). No measurable time delay between the X-ray and optical/UV flares is observed, but the optical/UV flares last longer, and the relative amplitudes of the X-ray and optical/UV flares show a large scatter. The X-ray spectrum can be well-fit with a partially absorbed power law (Γ∼1.4-1.5), perhaps due to the edge-on viewing angle. Modestly variable radio continuum emission is present at all epochs, and is not eclipsed by the secondary, consistent with the presence of a steady radio outflow or jet. The simultaneous radio/X-ray luminosity ratio of 3FGLJ0427.9−6704 is higher than any known transitional millisecond pulsars and comparable to that of stellar-mass black holes of the same X-ray luminosity, providing additional evidence that some neutron stars can be as radio-loud as black holes.

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“…This leads us to consider whether any selection biases might exist for radio or X-ray emission in favor of face-on systems. Tentative evidence for a similar bias toward face-on low-mass X-ray binaries has been observed at γ-ray wavelengths in systems with lower Xray luminosities (Britt et al 2017), including the candidate transitional millisecond pulsar 3FGL J1544.6-1125, which has an inferred inclination of 5-8 • .…”

Section: A Face-on Binary: Relativistic Beaming?mentioning

confidence: 57%

The MAVERIC Survey: A Red Straggler Binary with an Invisible Companion in the Galactic Globular Cluster M10

Shishkovsky¹,

Strader²,

Chomiuk³

et al. 2018

ApJ

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We present the discovery and characterization of a radio-bright binary in the Galactic globular cluster M10. First identified in deep radio continuum data from the Karl G. Jansky Very Large Array, M10-VLA1 has a flux density of 27 ± 4 µJy at 7.4 GHz and a flat to inverted radio spectrum. Chandra imaging shows an X-ray source with L X ≈ 10 31 erg s −1 matching the location of the radio source. This places M10-VLA1 within the scatter of the radio-X-ray luminosity correlation for quiescent stellarmass black holes, and a black hole X-ray binary is a viable explanation for this system. The radio and X-ray properties of the source disfavor, though do not rule out, identification as an accreting neutron star or white dwarf system. Optical imaging from the Hubble Space Telescope and spectroscopy from the SOAR telescope show the system has an orbital period of 3.339 d and an unusual "red straggler" component: an evolved star found redward of M10's red giant branch. These data also show UV/optical variability and double-peaked Hα emission characteristic of an accretion disk. However, SOAR spectroscopic monitoring reveals that the velocity semi-amplitude of the red straggler is low. We conclude that M10-VLA1 is most likely either a quiescent black hole X-ray binary with a rather face-on (i < 4 • ) orientation or an unusual flaring RS CVn-type active binary, and discuss future observations that could distinguish between these possibilities.

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Orbital Dynamics of Candidate Transitional Millisecond Pulsar 3FGL J1544.6-1125: An Unusually Face-on System

Cited by 26 publications

References 68 publications

The MAVERIC Survey: A Transitional Millisecond Pulsar Candidate in Terzan 5

The MAVERIC Survey: A Transitional Millisecond Pulsar Candidate in Terzan 5

The Flare-dominated Accretion Mode of a Radio-bright Candidate Transitional Millisecond Pulsar

The MAVERIC Survey: A Red Straggler Binary with an Invisible Companion in the Galactic Globular Cluster M10

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