Search for the optical counterpart to SGR 0418+5729

Search for the optical counterpart to SGR 0418+5729

Martin Durant Department of Astronomy, University of Florida, FL 32611-2055, USA martin.durant@astro.ufl.edu Oleg Kargaltsev Department of Astronomy, University of Florida, FL 32611-2055, USA George G. Pavlov Department of Astronomy and Astrophysics, Pennsylvania State University, PA 16802, USA
St.-Petersburg Polytechnical University, Polytechnicheskaya ul. 29, St. Petersburg 195257, Russia
Abstract

We report broad-band Hubble Space Telescope imaging of the field of soft ray repeater SGR 0418+5729 with ACS/WFC and WFC3/IR. Observing in two wide filters F606W and F110W, we find no counterpart within the positional error circle derived from Chandra observations, to limiting magnitudes , (Vega system), equivalent to reddening-corrected luminosity limits ,  erg s for a distance  kpc, at 3- confidence. This, in turn, imposes lower limits on the contemporaneous X-ray/optical flux ratio of 1100 and X-ray/near-infra-red flux ratio of 1000. We derive an upper limit on the temperature and/or size of any fall-back disk around the magnetar. We also compare the detection limits with observations of other magnetars.

X-rays;

1 Introduction

Soft Gamma-Ray Repeaters (SGRs) are believed to be magnetars: neutron stars (NSs) powered primarily by the decay of a super-strong magnetic field (Thompson & Duncan 1995). Their primary observational characteristics are X-ray luminosities higher than the spin-down power, , relatively slow rotation  s and fast spin-down  s s, implying characteristic ages 1000 yr and dipole magnetic field strengths  G. Most SGRs were discovered by their outbursts, either Giant Flares (Hurley et al., 2005) or rapid burst series (Gavriil et al., 2002). Since the discovery of mid-infrared emission from the magnetar 4U 0142+61 (Wang et al., 2006), passive (non-accreting) disks have been suggested to exist around magnetars, and could in principle have some effect on the observed luminosity and/or spin evolution (see Ertan et al. 2009 and references therein).

So far, only three magnetars (SGRs and the related Anomalous X-ray Pulsars, AXPs) have been detected in the optical, SGR 0501+4516 (Ofek et al., 2008; Fatkhullin et al., 2008) 4U 0142+61 (Hulleman et al., 2000) and 1E 1048.15937 (Durant & van Kerkwijk, 2005). The detections are challenging, due to their faintness and significant reddening (all Galactic magnetars lie close to the Galactic plane). Although other magnetars have been seen in the near-infrared, SGRs were detected only during their active states, so their quiescent NIR or optical luminosities are not known. See Mereghetti (2008) for a review of magnetar properties.

SGR 0418+5729 was discovered on 9 June 2009 via magnetar-like bursts detected by the Fermi Gamma-Ray Burst Monitor and confirmed with the Swift Burst Alert Telescope (van der Horst et al., 2010). The 9.1 s pulsations were first detected by RXTE (Gogus et al., 2009), while Swift XRT spectral fits suggested thermal emission with  eV (Cummings et al., 2009). No radio counterpart was found (Lorimer et al., 2009). Esposito et al. (2010) summarized the results of the follow-up XRT observations, and found thermal emission slowly cooling, with the emitting area decreasing on a time-scale of months. The extinction column inferred from the X-ray fits was  cm, lower than for any other Galactic magnetar. Using a limit on the pulsar spin-down rate, , Rea et al. (2010) derived an upper limit on the pulsar dipole magnetic field,  G, more typical for an ordinary pulsar than a magnetar. Alpar et al. (2011) argued that this contradicts the magnetar model, and instead supports the fall-back disk model.

Woods et al. (2009) measured the most accurate position of the SGR from Chandra data, R.A. Decl.  (J2000), with the positional uncertainty of 035 at 95% confidence. The direction of SGR 0418+5729 (, ) suggests a distance of 2 kpc, corresponding to the Perseus Arm (van der Horst et al., 2010). The proximity and low extinction of SGR 0418+5729 made it a promising candidate for detailed study in the optical/NIR. Esposito et al. (2010) failed to detect it in optical imaging with the Gran Telescopio de Canarias (GTC), setting a magnitude limit (SDSS magnitude). In this paper, we describe our imaging observations of SGR 0418+5729 with the Hubble Space Telescope (HST). In Section 2 we present the data and analysis. In Section 3 we discuss the detection limits and conclusions.

2 Observations and data reduction

The field of SGR 0418+5729 was imaged on 2010 October 19 by HST (GO program 12183). In the optical, the Advanced Camera for Surveys, Wide Field Channel (ACS/WFC) was used in conjunction with the broad filter F606W (pivot wavelength 5921 Å, RMS bandwidth 672 Å; roughly a broader V-band). The 2484 s, observation consisted of four dithered exposures with the WFC1 aperture. In the near-IR, the Wide Field Camera 3, IR channel (WFC3/IR) was used in MULTIACCUM mode with the broad filter F110W (pivot wavelength 11534 Å, RMS bandwidth 4430 Å; roughly a broad J-band). The total exposure was 2811 s, taken at four dithered pointings with the read parameters SPAR50, NREAD16 (sixteen reads, every 50 s, giving fifteen net images at each location). The images were processed by the standard pipeline, and combined using multidrizzle111http://stsdas.stsci.edu/multidrizzle/, which also corrects the images for geometric distortion and performs efficient cosmic ray rejection.

Figure 1: Images of the SGR 0418+5729 field in the F606W (top) and F110W (bottom) filters. The 035 positional error circle from Woods et al. (2009) is indicated. The nearest stars are labelled, and their positions and photometry given in Table 1.

Photometry was performed using the PSF-fitting package daophot II (Stetson, 1987). We tied the astrometry of the F110W image to the 2MASS system (Skrutskie et al., 2006) using 22 cross-identified catalog stars and the IRAF task ccmap. The astrometric uncertainty was about 003 in each coordinate (1-), estimated from the RMS in the residuals. The F606W image was registered with the F110W one using 28 matched stars, with a relative uncertainty of 001. Since Woods et al. (2009) also derived the SGR 0418+5729 position relative to the 2MASS system, we do not incur any additional systematic error, and hence the overall positional uncertainty is dominated by the X-ray uncertainty, 035, at 95% confidence (Woods et al., 2009). The final HST images are shown in Figure 1, together with the positional uncertainty circle.

We calibrated the photometry using the tabulated zero points for the F110W222http://www.stsci.edu/hst/wfc3/phot_zp_lbn and F606W333http://www.stsci.edu/hst/acs/analysis/zeropoints images, respectively. The uncertainty in the zero points is less than 0.05 mag.

3 Results and Conclusions

In the images shown in Figure 1, no bright source is seen within or near the SGR error circle. The 3- limits are , (Vega magnitudes). The locations and magnitudes of the nearest stars, marked in Figure 1, are listed in Table 1. The color-magnitude diagram (CMD) of all the matched field stars is shown in Figure 2, with the point sources from Table 1 labeled. They are all consistent with main sequence stars behind reddening, except Star E, which likely is a red giant.

Figure 2: Color-magnitude diagram of stars in the field of SGR 0418+5729. The stars nearest the position of SGR 0418+5729 are marked (see Figure 1).
Star R.A. (J2000) decl. (J2000)
A 64.641821 57.539883 23.7730.013 20.6270.022
B 64.641448 57.540451 21.2130.016 19.0230.020
C 64.638586 57.540671 27.3370.069 23.1090.028
D 64.641397 57.538482 24.5100.029 20.8710.028
E 64.638012 57.538750 21.3080.016 14.9470.017
F 64.640854 57.542242 23.5370.014 19.9680.018
G 64.644254 57.541679 21.3710.015 18.9640.013
H 64.642619 57.537232 22.5590.010 20.3070.024
I 64.644363 57.537078 19.8880.017 17.7520.018

Note. – Uncertainties do not include the uncertainty in the photometric zero points. Magnitudes are in the Vega system.

Table 1: Point sources in the field.

Rea et al. (2010) give the SGR X-ray flux  erg scm (0.5–10 keV, absorbed; Chandra ObsID 12312) on 2010 July 23, which is a factor of 150 fainter than during the discovery observations a year earlier. The X-ray observation nearest in time to our HST observation occurred on 2010 September 24 (XMM observation 0605852201) and had a poorly constrained flux, consistent with the July 23 observation, albeit with lower signal-to-noise. Our limit in F110W corresponds (e.g., Bessell 1979) to a spectral flux limit  erg scmHz, where we have assumed the reddening from the X-ray extinction measure (Predehl & Schmitt, 1995; Schlegel et al., 1998). Thus we derive a limit on the X-ray/NIR444Here we adopt as a measure of the NIR/optical flux. The actual flux in a given filter, , where is the filter throughput at frequency , is smaller by a factor of a few. The definition is, however, convenient to compare fluxes measured with different broad filters. flux ratio . Likewise in the optical  erg scmHz and the X-ray/optical flux ratio is . The flux ratio limits are still consistent with the ratios found for persistent magnetars detected in the optical/NIR (see Durant & van Kerkwijk 2005; Mereghetti 2008). We also retrieved the X-ray observation of SGR 0418+5729 closest in time after our HST observation, by Chandra ACIS (ObsID 13148 on 2010 November 29). We measure a flux of  erg scm, indicating that the source had continued to fade. We plot the spectrum in Figure 3 alongside the one from 2010 July 23 (Rea et al., 2010). The spectral peak shifted to lower energies, indicating a lower temperature (assuming a thermal spectrum).

Only three magnetars have so far been detected in the optical, 4U 0142+61 (a persistent AXP-type magnetar; Hulleman et al. 2000), SGR 0501+4516 (Fatkhullin et al., 2008) and 1E 1048.15937 (another AXP, detected only in the I-band; Durant & van Kerkwijk 2005). In each case, the observed emission is pulsed at the pulsar period, with pulsed fractions 50%, i.e., higher than in soft X-rays (Kern & Martin, 2002; Dhillon et al., 2011, 2009). This clearly indicates the magnetospheric origin of the optical emission. It is illuminating to compare the optical properties of these magnetars with those of SGR 0418+5729.

The measured magnitudes and inferred flux ratios of all the optically-detected magnetars are given in Table 2 alongside our limits for SGR 0418+5729. Our flux ratio limits are near the lowest values for the other magnetars, and imply that SGR 0418+5729 still could have similar spectral properties to the other magnetars, although the flux ratios must be higher than those for 1E 1048.15937. Note that the two AXPs have been observed in quiescence (but both are known to be variable), whereas both SGRs were observed after outbursts and may still have been fading.

Magnetar NIR aaHere the NIR and optical fluxes are defined as for all the objects. Optical aaHere the NIR and optical fluxes are defined as for all the objects. RefsbbReferences: 1: Durant & van Kerkwijk (2006b) 2: Rea et al. (2008) 3: Enoto et al. (2009) 4: Fatkhullin et al. (2008) 5: Dhillon et al. (2011) 6: Durant & van Kerkwijk (2005) 7: Rea et al. (2010) 8: this work.
(kpc) (0.5–10 keV)
4U 0142+61 7.0 5700 2400 1
SGR 0501+4516ccHere we list two X-ray and optical observations, shortly after outburst and when approaching quiescence 2.50.5 2900 1300 2,3,4
 ddNear the quiescent value, and consistent with contemporaneous low-S/N SWIFT observations (see text). 2100 5
1E 1048.15937eeValues at quiescence. 9.01.7 1000 1000 6
SGR 0418+5729 20.5 1000 1100 7,8

Note. – The optical and infrared magnitudes listed are corrected for extinction before conversion to flux. The X-ray fluxes are unabsorbed. All fluxes are in units erg scm. Distances are taken from Durant & van Kerkwijk (2006a) for the AXPs and from the locations of the Galactic spiral arms for the SGRs.

Table 2: Optical-detected magnetars and their fluxes
Figure 3: Multiwavelength spectra of the optically detected magnetars, together with SGR 0418+5729. For SGR 0418+5729, we show two X-ray spectra from 2010 July 23 (upper, blue) and 2010 November 29 (lower, green), and the spectral flux limits established in this paper.

The IR-X-ray spectra of the four magnetars in Table 2 are shown in Figure 3. The two AXPs have similar multi-wavelength spectra, but the X-ray spectrum of SGR 0501+4516 appears to be closer to a power-law555Note that the extinction to SGR 0501+4516 is rather high and uncertain. (), whereas the spectrum of SGR 0418+5729 is more like a cooling black-body.

The direction and low extinction to SGR 0418+5729 strongly suggests a distance of 2.0 kpc, which is the distance to the Perseus arm (there is no further dense Galactic structure in this direction; Cordes & Lazio 2002). For such a distance, the upper limits on NIR and optical luminosities () are  erg s,  erg s, lower than the luminosities of any detected magnetars.

The passive disk model for 4U 0142+61 by Wang et al. (2006) predicts  erg scm at 1.1 m, for the distance of 3.9 kpc. If a similar disk were around SGR 0418+5729, it would have  erg scm, where is the distance in units of 2 kpc. We measure  erg scm, i.e., 2.5 orders of magnitude smaller. For a disk of the same size as in Wang et al. (2006), the disk inner temperature would need to be  K, i.e., cooler than plausible values for the (non-ice) dust sublimation temperature (Kobayashi et al., 2011). Alternatively, the disk could be more tenuous, or there may be no disk. Our measurements thus suggest that, if indeed disks contribute significantly to the luminosities of magnetars, then a different disk configuration (surface density and inner radius) is needed for SGR 0418+5729 compared to 4U 0142+61. If so, it could be connected to either the former being a transient magnetar and the latter persistent, or the much lower magnetic field of SGR 0418+5729.

Malheiro et al. (2011) discussed an alternative source of power for SGRs and AXPs: the spin-down of a rapidly rotating, magnetized WD. Our photomety limits allow us to place an upper limit on the temperature of a WD-sized ( cm) black-body emitter of  K at 2 kpc. Whereas WDs with temperatures  K are known (e.g., Durant et al. 2011, submitted), the cooling time required is  Gyr. Our flux limits therefore constrain the WD interpretation for SGRs.

In conclusion, although SGR 0418+5729 is the nearest and least extincted magnetar known, we have not detected it in very deep optical and NIR observations. The source still offers a good opportunity to observe the optical spectrum of a magnetar, but this will only be possible following a new outburst. On the other hand, AXP 4U 0142+61 is the only persistent magnetar known whose optical/NIR spectrum can be measured, but the faintness requires extensive observation time.


Based on observations with HST (GO program 12183). This work is supported under grant HST-GO-12183.03-A by the Space Telescope Science Institute (STScI) and NASA grant NNX09AC84G. The work by GGP was partly supported by the Ministry of Education and Science of Russian Federation (Contract No. 11.G34.31.0001).

After this work appeared in preprint, we were contacted by J. Rueda, who pointed out that the model in Malheiro et al. (2011) specifically requires a high-mass white dwarf, with a radius, therefore, smaller than we assumed. Here we give the explicit dependence on radius of the limit one can place on the black-body surface temperature, one limit for each filter:

(1)
(2)

where is the radius in units of 10,000 km (10 cm), for the F110W and F606W filters, respectively.

References

  • Alpar et al. (2011) Alpar, M. A., Ertan, Ü., & Çalışkan, Ş. 2011, ApJ, 732, L4
  • Bessell (1979) Bessell, M. S. 1979, PASP, 91, 589
  • Cordes & Lazio (2002) Cordes, J. M., & Lazio, T. J. W. 2002, ArXiv Astrophysics e-prints, 0207156
  • Cummings et al. (2009) Cummings, J. R., Page, K. L., Beardmore, A. P., & Gehrels, N. 2009, The Astronomer’s Telegram, 2127, 1
  • Dhillon et al. (2009) Dhillon, V. S., et al. 2009, MNRAS, 394, L112
  • Dhillon et al. (2011) —. 2011, ArXiv e-prints, 1106.1355
  • Durant & van Kerkwijk (2005) Durant, M., & van Kerkwijk, M. H. 2005, ApJ, 627, 376
  • Durant & van Kerkwijk (2006a) —. 2006a, ApJ, 650, 1070
  • Durant & van Kerkwijk (2006b) —. 2006b, ApJ, 652, 576
  • Enoto et al. (2009) Enoto, T., et al. 2009, ApJ, 693, L122
  • Ertan et al. (2009) Ertan, Ü., Ekşi, K. Y., Erkut, M. H., & Alpar, M. A. 2009, ApJ, 702, 1309
  • Esposito et al. (2010) Esposito, P., et al. 2010, MNRAS, 405, 1787
  • Fatkhullin et al. (2008) Fatkhullin, T., et al. 2008, GRB Coordinates Network, 8160, 1
  • Gavriil et al. (2002) Gavriil, F. P., Kaspi, V. M., & Woods, P. M. 2002, Nature, 419, 142
  • Gogus et al. (2009) Gogus, E., Woods, P., & Kouveliotou, C. 2009, The Astronomer’s Telegram, 2076, 1
  • Hulleman et al. (2000) Hulleman, F., van Kerkwijk, M. H., & Kulkarni, S. R. 2000, Nature, 408, 689
  • Hurley et al. (2005) Hurley, K., et al. 2005, Nature, 434, 1098
  • Kern & Martin (2002) Kern, B., & Martin, C. 2002, Nature, 417, 527
  • Kobayashi et al. (2011) Kobayashi, H., Kimura, H., Watanabe, S.-i., Yamamoto, T., & Mueller, S. 2011, ArXiv e-prints, 1104.5627
  • Lorimer et al. (2009) Lorimer, D. R., Edel, S., Kondratiev, V. I., McLaughlin, M. A., Boyles, J. R., Ludovici, D. A., & Ridley, J. P. 2009, The Astronomer’s Telegram, 2096, 1
  • Malheiro et al. (2011) Malheiro, M., Rueda, J. A., & Ruffini, R. 2011, ArXiv e-prints, 1102.0653
  • Mereghetti (2008) Mereghetti, S. 2008, A&A Rev., 15, 225
  • Ofek et al. (2008) Ofek, E. O., Kiewe, M., & Arcavi, I. 2008, GRB Coordinates Network, 8229, 1
  • Predehl & Schmitt (1995) Predehl, P., & Schmitt, J. H. M. M. 1995, A&A, 293, 889
  • Rea et al. (2008) Rea, N., Rol, E., Curran, P. A., Skillen, I., Russell, D. M., & Israel, G. L. 2008, GRB Coordinates Network, 8159, 1
  • Rea et al. (2010) Rea, N., et al. 2010, Science, 330, 944
  • Schlegel et al. (1998) Schlegel, D. J., Finkbeiner, D. P., & Davis, M. 1998, ApJ, 500, 525
  • Skrutskie et al. (2006) Skrutskie, M. F., et al. 2006, AJ, 131, 1163
  • Stetson (1987) Stetson, P. B. 1987, PASP, 99, 191
  • van der Horst et al. (2010) van der Horst, A. J., et al. 2010, ApJ, 711, L1
  • Wang et al. (2006) Wang, Z., Chakrabarty, D., & Kaplan, D. L. 2006, Nature, 440, 772
  • Woods et al. (2009) Woods, P. M., Wachter, S., Gogus, E., & Chryssa Kouveliotou, C. 2009, The Astronomer’s Telegram, 2159, 1
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
Cancel
Loading ...
322133
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

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
Test description