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The 69 Millisecond Radio Pulsar Near the Supernova Remnant RCW 103

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The 69 Millisecond Radio Pulsar Near the Supernova Remnant RCW 103 Haverford College Haverford Scholarship Faculty Publications Physics 1998 The 69 Millisecond Radio Pulsar Near the Supernova Remnant RCW 103 V. M. Kaspi Fronefield Crawford Haverford College, [email protected] Follow this and additional works at: https://scholarship.haverford.edu/physics_facpubs Repository Citation "The 69 Millisecond Radio Pulsar Near the Supernova Remnant RCW 103" V. M. Kaspi, F. Crawford, R. N. Manchester, A. G. Lyne, F. Camilo, N. D'Amico, & B. M. Gaensler, Astrophysical Journal Letters, 503, L161 (1998). This Journal Article is brought to you for free and open access by the Physics at Haverford Scholarship. It has been accepted for inclusion in Faculty Publications by an authorized administrator of Haverford Scholarship. For more information, please contact [email protected]. The Astrophysical Journal, 503:L161±L165, 1998 August 20 q 1998. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE 69 MILLISECOND RADIO PULSAR NEAR THE SUPERNOVA REMNANT RCW 103 V. M. Kaspi and F. Crawford Massachusetts Institute of Technology, Physics Department, Center for Space Research, 70 Vassar Street, Cambridge, MA 02139 R. N. Manchester Australia Telescope National Facility, CSIRO, P.O. Box 76, Epping, NSW 2121, Australia A. G. Lyne and F. Camilo University of Manchester, Jodrell Bank, Maccles®eld, Cheshire SK11 9DL, England, UK N. D'Amico Osservatorio Astronomico di Bologna, via Zamboni 33, 40126 Bologna, Italy and B. M. Gaensler Australia Telescope National Facility, CSIRO, P.O. Box 76, Epping, NSW 2121, Australia; and Astrophysics Department, School of Physics, University of Sydney, NSW 2006, Australia Received 1998 May 7; accepted 1998 June 23; published 1998 July 22 ABSTRACT We report the detection of the radio pulsar counterpart to the 69 ms X-ray pulsar discovered near the supernova remnant RCW 103 (G332.420.4). Our detection con®rms that the pulsations arise from a rotation-powered neutron star, which we name PSR J161725055. The observed barycentric period derivative con®rms that the pulsar has a characteristic age of only 8 kyr, the sixth youngest of all known pulsars. The unusual apparent youth of the pulsar and its proximity to a young remnant require that an association be considered. Although the respective ages and distances are consistent within substantial uncertainties, the large inferred pulsar transverse velocity is dif®cult to explain given the observed pulsar velocity distribution, the absence of evidence for a pulsar wind nebula, and the symmetry of the remnant. Rather, we argue that the objects are likely superposed on the sky; this is reasonable given the complex area. Without an association, the question of where is the supernova remnant left behind following the birth of PSR J161725055 remains open. We also discuss a possible association between PSR J161725055 and the g-ray source 2CG 333101. Although an association is energetically plausible, it is unlikely given that EGRET did not detect 2CG 333101. Subject headings: gamma rays: observations Ð pulsars: individual (PSR J161725055) Ð stars: neutron Ð supernova remnants Ð X-rays: stars 1. INTRODUCTION 2. OBSERVATIONS We observed the X-ray pulsar position reported by Gotthelf et al. (1997) (J2000, R.A. 16h17m30s, decl. 2507559050) at the RCW 103 (G332.420.4) is a young shell supernova remnant Parkes Observatory 64 m radio telescope in New South Wales, with a complicated observational history. An X-ray point Australia, on 1998 January 15 and 16, for 2.6 and 4.0 hr, source near the center of the remnant was discovered by Tuohy respectively. For these observations, we used the center beam & Garmire (1980), who suggested that it is a ªradio-quietº of the Parkes multibeam receiver system at a central radio thermally cooling neutron star, the stellar remnant of the su- frequency of 1374 MHz. The cryogenically cooled system re- pernova explosion. This was supported by Tuohy et al. (1983) ceives orthogonal linear polarizations, each of which is down- and later by Manchester, D'Amico, & Tuohy (1985) and Kaspi converted to an intermediate frequency and ®ltered in a 2 # et al. (1996), who failed to ®nd evidence for pulsed emission 96 # 3 MHz analog ®lter-bank spectrometer. Data were one- m in radio searches. Aoki, Dotani, & Mitsuda (1992) detected 69 bit sampled at 250 s and recorded onto magnetic tape using a DLT 7000 tape recorder attached to a DEC Alpha workstation. ms pulsations from the direction of the remnant using Ginga, The data acquisition software and hardware are those being providing additional evidence for the neutron star identi®cation. used in a major survey of the Galactic plane for pulsars (see However, Ginga's poor spatial resolution ( 1CC#2) precluded » Camilo et al. 1997). any ®rm association. Recently, Gotthelf, Petre, & Hwang In of¯ine processing, the data were dedispersed at dispersion (1997) detected the central source using the ASCA X-ray ob- measures (DMs) between 0 and 600 pc cm23 . Each dedispersed servatory and argued that its spectrum is harder than that of a time series was folded over a range of topocentric periods cooling neutron star. They found no evidence for pulsations, 52ms from that predicted by the ephemeris estimated by Torii setting upper limits that were inconsistent with the Aoki et al. et al. (1998). A highly signi®cant detection (signal-to-noise claim. This history recently took a dramatic turn with the de- ratio 21) was found atDM 5 467 5 5 pc cm23 , at barycentric tection of the 69 ms periodicity in the ASCA data from a point period0.069356847 5 0.000000003 s (epoch MJD 50829.7). source, AXS J1617302505505, located 79 north of the center The pulsation was unambiguously con®rmed the next day (sig- of the remnant, outside the 59 remnant radius (Gotthelf et al. nal-to-noise ratio 33). The pro®le obtained by folding the data 1997; Torii et al. 1998). Here we report the discovery of pulsed from the latter observation is shown in Figure 1. radio emission from this pulsar, which we name PSR The 1.4 GHz average radio pulse is unexceptional, charac- J161725055. terized by a single peak of 50% intensity width5.8 5 0.6 ms L161 L162 KASPI ET AL. Vol. 503 derive using the Ginga detection.1 From the measured PÇ , we infer a surface magnetic ®eld strength B { 3.2 # 1019 (PPÇ )1/2 5 3.1 # 1012 G and a spin-down luminosity EÇ { 4p 2IPÇ /P 3 5 1.6 # 10 37 ergs s21, where I is the neutron star moment of inertia, assumed to be 10 45 g cm2. The implied Ç characteristic age for PSR J161725055 is tc { P/2P 5 8.1 kyr. This is the sixth youngest known pulsar characteristic age after the Crab pulsar, PSR B0540269, PSR B1509258, PSR B1610250, and the recently discovered PSR J053726910 (Marshall et al. 1998). The apparent proximity of so young a pulsar to a young supernova remnant demands that an association be considered. If they are associated, the nature of the well-studied central X- ray source would be unclear, as no tenable interpretations other than its being an isolated cooling neutron star have been put forward (Popov 1998; Heyl & Hernquist 1998). The probability Fig. 1.ÐPulse pro®le of PSR J161725055 at 1.4 GHz of chance superposition of the pulsar near the remnant is dif- ®cult to quantify but is certainly not negligible, particularly in this complex region of the sky: this line of sight traverses the (10% intensity width 11 5 1 ms), convolved with a one-sided Sagittarius-Carina and Scutum-Crux spiral arms and may ex- exponential of decay time constant 8.7 5 0.5 ms, probably due tend to the Norma arm. Indeed, the very young radio pulsar to scattering. Although the observations were not carefully cal- PSR B1610250, only 309 away on the sky from PSR ibrated, we estimate the ¯ux density of the source to be 0.5 J161725055, is also prob»ably superposed only by chance near mJy, with an uncertainty of 30%. Using archival Aust»ralia the supernova remnant Kes 32 (Johnston et al. 1995; Gaensler Telescope Compact Array (AT»CA) data taken of the area, but & Johnston 1995b; but see also Caraveo 1993). We now con- ®ltering out large-scale structure, seven unresolved sources can sider the evidence for an association between PSR J161725055 be seen within 49 of the pulsar that have 1.4 GHz ¯ux densities and RCW 103. between 0.5 an»d 1.4 mJy. None of these sources is noticeably circularly or linearly polarized, although bandwidth depolari- 3.1. Do Independent Distance Estimates for the zation could easily account for the latter possibility. The source Pulsar and Remnant Agree? closest to the ASCA position has ¯ux density 0.5 mJy, con- sistent with our estimate from Parkes and a ¯at s»pectrum similar First we consider the remnant distance. Westerlund (1969) to other young pulsars; it is at (J2000) R.A. 16h17m29.s3, decl. estimated the distance to RCW 103 to be d 5 3.9 kpc, by 2507559130.2 (uncertainty 00.2). associating it with OB stars nearby on the sky. Caswell et al. » (1975) used H i absorption to establish a systemic velocity of We searched for occurrences of giant radio pulses from PSR 21 J161725055 by combining individual dedispersed samples to 244 km s for the remnant, which, using the rotation curve form a 20 ms resolution time series. Signi®cantly narrower of Fich, Blitz, & Stark (1989) and standard IAU parameters pulses were unlikely to be seen since dispersion smearing and (Kerr & Lynden-Bell 1986), corresponds to a distance of 3.1 0.4 kpc. This has often been taken to be the actual dis- multipath scattering should combine to broaden pulses by 10 5 tance to the source (e.g., Dickel et al.
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