2FGL J2039.6-5620

A binary counterpart for 2FGL J2039.65620


We have identified an optical/X-ray binary with orbital period  h as the likely counterpart of the Fermi source 2FGL J2039.65620. GROND, SOAR and DES observations provide an accurate orbital period and allow us to compare with the light curve of an archival XMM exposure. Like many short-period optical X-ray binaries associated with LAT sources this may be a interacting (black widow/redback) millisecond pulsar binary. The X-ray light curve is consistent with the emission associated with an intrabinary shock. The optical light curve shows evidence of companion heating, but has a peculiar asymmetric double peak. The nature of this optical structure is not yet clear; additional optical studies and, especially, detection of an orbital modulation in a -ray pulsar are needed to elucidate the nature of this peculiar source.

Subject headings:
gamma rays: stars — pulsars: general

1. Introduction

As identification of the 1873 0.1–100 GeV sources in the second Fermi Large Area Telescope (LAT) catalog (Nolan et al., 2012) progresses, blazars and spin-powered pulsars increasingly dominate the associations (Acero et al., 2015). For the brightest remaining unidentified sources gamma-ray spectral curvature and variability provide an excellent discrimination between these two possibilities (Romani, 2012). 2FGL J2039.65620 = 3FGL 2039.65618 (hereafter J2039) is a relatively bright (25.4, Acero et al., 2015) source with a good localization at Galactic latitude -37, a 3FGL “variability index” value of 34, and a “curvature significance” of 5.1. Thus it is one of the least variable bright unidentified sources and displays significant spectral curvature, placing it well within the pulsar zone of the curvature-variability plane. Accordingly it has been repeatedly searched for radio (Camilo et al., 2015) and gamma-ray (Abdo et al., 2009; Pletsch & Clark, 2014) pulsations. The lack of any detection is best understood if the source is a millisecond pulsar rapidly accelerated and/or wind-shrouded in a close, interacting binary (Romani & Shaw, 2011; Romani, 2012; de Martino et al., 2014; Roy et al., 2015).

We have examined new and archival optical and X-ray data, discovering a short period (5.47 h) binary. The system shows evidence of heating, and the X-ray light curve is reminiscent of other shrouded (black widow BW and redback RB) millisecond pulsar binaries. The optical light curve is oddly double-peaked and asymmetric. Nevertheless we conclude that this is another short period gamma-ray pulsar binary. With our well measured period and position, this is a fruitful target for renewed pulse searches.

2. Photometry and Orbital-Period Estimate

J2039 has a good 3FGL localization ( radius) and we initially observed this field as part of our LAT Unidentified source campaign, using the Goodman High Throughput Spectrograph (GHTS) at the 4.2 m SOAR telescope on 2013 August 10 (MJD 56514, UT dates are used throughout). A sequence of 180 s images plus a 600 s H frame were obtained, spaced over 2 hours and largely covering the error ellipse. Despite relatively poor conditions, we were able to search for variability for counterparts as faint as . One star (Figure 1), coincident with an X-ray source in archival data (initially SWIFT, later XMM exposure, see below) was found to vary in a correlated manner in all three bands, suggesting a characteristic period  h. The USNO-B1.0 position of this source is , (2000.0, ). The catalog gives a proper motion estimate and . No H structure was found in the field.

Figure 1.— Stacked SOAR/GHTS image of the J2039-5617 field.

We searched for archival observations in this direction and found an excellent series of GROND (Grenier et al., 2008) exposures of the J2039 error ellipse, with  s (+JHK) exposures each on 3 days Aug 16-18 2014 (MJD 56885-56887). Measuring these optical frames, we obtain the light curves shown in figure 2. This data set showed a clear double-peaked light curve, with asymmetric maxima and minima and an orbital period  d (5.47 h). The colors vary slightly with evidence for heating (minimum ) at optical maximum.

The quest for direct detection of blind pulsations is greatly helped by a precise orbital period, which reduces the acceleration search space (Pletsch et al., 2012). Accordingly, we compared with light curve phasing of our GHTS observations, 371 d earlier. This refined the period to 0.228116  d where the aliases about the best minimum are set by orbit slips between the two observation sets.

The target was covered in seven exposures in the DES early data release, in two frames each of , and , and a single frame. We performed relative photometry against a set of the field stars from the GROND images, to put the magnitudes on a consistent scale. The observation dates ranged from MJD 56538 to MJD 56558, between our other two epochs. Accordingly these points break the alias degeneracy, clearly preferring , the primary minimum. We thus establish , with barycentric epoch for optical maximum MJD 56885.085. As discussed below it is unclear how this photometric epoch relates to the orbital kinematic epoch, i.e. .

Figure 2.— light curves for J2039. Two cycles are shown with GROND error bars plotted on the first cycle only. GHTS (circle) and DES (triangle points are also shown. The DES offset may be due to the substantial differences in this filter. Phase markers on the second period of the curve emphasize that the second maximum and minimum are early by . A single period of the color is also shown, on a magnified scale.

In Figure 2 the GHTS and DES points are seen, calibrated against the GROND flux scale, showing good agreement with the mean light curve. We also plot the DES point, which lies mag from the GROND curve. This discrepancy may be cross-calibration error (GROND is split between DES and ). The DES data are however very spread in time: the point was 2.5 orbits off any other observation. The second point is also from the expected flux and was obtained 5 d before the first DES point. If, like many other BW/RB systems, the companion undergoes occasional flares, this can explain these discrepancies. However the small spread in GROND photometry over 3 d and the otherwise good match of the GHTS and DES points imply that the source is generally stable to better than mag.

J2039 is also covered in the Catalina Sky Survey (CSS; http://www.lpl.arizona.edu/css/index.html; Drake et al. 2009) photometry archive with data extending 9.0 y before the GROND exposures. These unfiltered magnitudes with a typical error mag are too shallow to usefully probe the light curve modulation. However, they do serve to confirm the source’s general quiescence; out of 217 observations, only one point with mag had (likely a measurement error in any event).

The most remarkable aspect is of this light curve are the two asymmetric maxima and minima. The first minimum follows the large maximum by , but the second maximum and minimum arrive too early to lie on the opposite side of the orbit (dotted lines in Figure 2). The optical color is bluest at optical maximum, but plateaus across the first minimum and second maximum, decreasing to its reddest value at the second minimum. Clear there is off axis structure in the system, with heating at two (nearly) opposite poles or, possibly an occultation at the phase of the first minimum.

Figure 3.— XMM-Newton light curves of J2039. Above PN, Below Combined MOS1+MOS2. is at optical maximum as in Figure 2.

3. Archival X-ray Light Curve

Archival SWIFT exposures show a few counts from this counterpart, but the X-ray source is best measured in a 41.6 ks live time XMM-Newton exposure (ObsID 0720650301, PI: Mignani) on MJD 56575. This data set clearly shows the optical counterpart as the brightest source in the 3FGL error ellipse. With an observation between the GROND and GHTS epochs, the predicted orbital phase is known to dominated by the period uncertainty. Folding the X-rays, we generated the PN and combined MOS1/2 light curves (figure 3). The peak is coincident with the optical maximum. The double structure, while of modest statistical significance, is common to both instruments.

The source is unresolved to XMM and delivered 0.024 cps in 37 ks effective PN camera exposure. A power law spectral fit determines a photon index and an upper limit on the absorption of (90% errors). The corresponding unabsorbed 0.5-10 keV flux is . If a thermal component (e.g. from an underlying neutron star) is present a larger might be allowed. However present data do not require such a component and the absorbed power law fit is quite adequate, with /DoF=1.15.

4. System Modeling and Conclusions

The source bears many similarities to several other short-period shrouded pulsar binaries. At  h it may be either a redback or a black widow. However, at this period it is much closer to the shrouding line in the former case and so it is more likely a redback, given the lack of detection in repeated radio searches. Although the system properties will remain quite uncertain until a pulse detection is made, we can draw some tentative conclusions from the binary data.

Our X-ray spectral fit indicates very little extinction, with the upper limit corresponding to for the conversion of Foight et al. (2015). This is about half the total in this direction (Schlafly & Finkbeiner, 2011). At this orbital period a main sequence companion would fill its Roche lobe for so we take this as an upper limit to the companion mass. Such a star would have  K and , so the observed color at minimum indicates appreciable heating. In fact, the colors are even bluer at maximum with equivalent to  K. The origin of these increased temperatures is unclear; the companion may be partly degenerate or it may experience tidal heating. However in analogy with other shrouded MSP, it is likely that the effect of pulsar heating, possibly mediated by an intrabinary shock, is dominant. If we consider just the temperature rise to maximum, we derive an irradiation temperature  K and for an orbital separation , an isotropic irradiation luminosity . Lower companion masses require additional heating power, although the relatively large implies a low inclination angle or, possibly, rapid transport of heating flux to the companion night side, as invoked for some hot Jupiters (e.g. Heng & Showman, 2015).

This heating flux is a lower limit to the true pulsar output. Breton et al. (2013) infer a typical heating efficiency (some BW/RB appear to have larger heating efficiencies), which would imply a spin-down power . Another power estimate can be derived from the gamma-ray flux : Abdo et al. (2010) have noted a heuristic gamma-ray luminosity , which gives us a distance estimate  kpc. Note that the spindown power estimate for an heating efficiency then places the source at 1.5 kpc. Given that is below the full Galactic column (at ), we suspect a somewhat higher efficiency, lower power and closer distance. The USNO B1.0 proper motion above corresponds to . MSP binaries tend to be slower than the isolated young pulsar population, with Gonzalez et al. (2011) giving . This also supports a relatively close distance.

The hard power-law X-ray spectrum and strong orbital modulation indicate a non-thermal source. The light curve with an X-ray maximum flanked by two peaks and the observed are quite typical of BW/RB MSP showing evidence for intrabinary shocks (Roberts et al., 2015). These double peaks are generally centered around pulsar eclipse at superior conjunction as for PSR J1959+2048 (Huang et al., 2012) or PSR J22390533 (Romani & Shaw, 2011), but have also been seen at inferior conjunction e.g. PSR J21290429 (Roberts et al., 2015). The local minimum between these peaks may be a product of either companion eclipse or of beaming along intrabinary shock surfaces. The low X-ray luminosity also suggests a binary in the pulsar-powered state (Linares, 2014).

We close by discussing the most puzzling aspect of this system, the asymmetric double peaked optical light curve. Intriguingly, Li, Halpern & Thorstensen (2014) have recently measured the optical light curve of the redback PSR J16283205, which has a 5 h hour period and is near-Roche lobe filling. This binary also shows asymmetric maxima and minima. These authors do not find a clear origin of this asymmetry, but speculate on the possibilities of swept back intrabinary shocks or magnetically-directed heating of spots on the companion surface. Both are plausible for J2049, as well. One difference, however, is that Li, Halpern & Thorstensen (2014) place the optical maximum with respect to the pulsar ascending node. Thus, with this phasing the star is brightest when viewed at quadrature. Accordingly they assign the basic double-peak modulation to ellipsoidal variations, with the intrabinary shock or magnetic heating supplying the required asymmetry. In our case without a pulsar ephemeris, we do not know the true phases and for the moment arbitrarily set at the optical maximum. However as noted above the characteristic double peaked X-ray light curve is often along the pulsar-companion axis. For J2049 this double peak is in phase with the optical maximum. If we interpret that maximum as pulsar inferior conjunction (view of the heated face), then the double X-ray peak is similar to that of PSR J21290429. Of course, none of these phase relationships are clear until we obtain a kinematic ephemeris to reference our photometric epoch, either through a pulsar discovery or through optical spectroscopy. We are pursuing both paths.

This research is based in part on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia, e Inovação (MCTI) da República Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU).


  1. affiliation: Department of Physics, Stanford University, Stanford, CA 94305-4060, USA; rwr@astro.stanford.edu
  2. slugcomment: Accepted to ApJ Letters


  1. Abdo, A. A., et al. 2009, Science, 325, 840
  2. Abdo, A. A., et al. 2010, ApJS, 187, 460.
  3. Acero, F., Ackermann, M., Ajello, M, et al. 2015, ApJS, 218, 23
  4. Breton, R. P., van Kerkwijk, M. H., Roberts, M. S. E. et al. 2013, ApJ, 769, 108
  5. Camilo, M., Kerr, M., Ray, P.S., et al. 2015, ApJ, 810, 85
  6. de Martino, D., Cesares, J., mason E. et al 2014, MNRAS, 444, 3004
  7. Drake, A. J., Djorgovski, S. G., Mahabal, A. et al. 2009, ApJ, 696, 870
  8. Foight, D. R., Güver, T. Özel, F abd Slane P.O. 2015 ArXiv 1504.07274
  9. Gonzalez, M E., Stairs, I. H., Ferdman, R. D.. et al. 2011, ApJ, 743, 102
  10. Grenier, J., Bournemann, W., Clemens, C. et al. 2008, PASP, 120, 405
  11. Heng, K. & Showman, A.P. 2015, AREPS, 43, 509
  12. Huang, R. H. .H., Kong, A. K. H., & Takata, J., et al. 2012, ApJ, 760, 92
  13. Linares, M. 2014, ApJ, 795, 72
  14. Li, M., Halpern, J. P. & Thorstensen, J. R. 2014, ApJ, 795, 115
  15. Nolan, P. L., et al. 2012, ApJS, 199, 31
  16. Pletsch, H. J., et al. 2012, Science, 338, 1314
  17. Pletsch, H. J. & Clack, C. J. 2014, ApJ, 795, 75
  18. Roy, J. S., Ray, P. S., Battacharayya, B. et al. 2015, ApjL, 800, 12
  19. Roberts, M.S.E., McLaughlin, M. A., Gentile, P. A. et al. 2015, ArXiV, 1502.07208
  20. Romani, R. W. 2012, ApJ, 754, L25
  21. Romani, R. W., & Shaw, M. S. 2011, ApJ, 743, L26
  22. Schlafly, E. F., & Finkbeiner, D. P. 2011, ApJ, 737, 103
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
The feedback must be of minimum 40 characters and the title a minimum of 5 characters
Add comment
Loading ...
This is a comment super asjknd jkasnjk adsnkj
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test description