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Nevertheless the afterglow is the result of the interaction of colliding shells (that produced the GRD) with the ambicut medimm auc sole level o: aupriut from the GRB phase may be expected to be present in fje afterelow. | Nevertheless the afterglow is the result of the interaction of colliding shells (that produced the GRB) with the ambient medium and some level of imprint from the GRB phase may be expected to be present in the afterglow. |
The clustering of GRB energies (a property the GRD phase) interred Yom measurements of the jet-break. times (a property of the afterglow) sugecstsOO a yossible relation between CRB alc afterglow properties. | The clustering of GRB energies (a property of the GRB phase) inferred from measurements of the jet-break times (a property of the afterglow) suggests a possible relation between GRB and afterglow properties. |
We investigate a complete sanple of seven GRBs for which measurements of the redshift. the spectral lag. the Iuninosity. and of the jet-lweak time are available. | We investigate a complete sample of seven GRBs for which measurements of the redshift, the spectral lag, the luminosity, and of the jet-break time are available. |
We collect redshifts and jet-break times from ctal. (2001).. spectral data from Jimenezetal.(2001) andl BATSE pulse lags for six bursts Toni Norrisetal.(2000). | We collect redshifts and jet-break times from \citet{fksd01}, , spectral data from \citet{jbp01} and BATSE pulse lags for six bursts from \citet{nmb00}. |
To this set we have added the data of 9991216 (observed lag Adis,=0.018ras seconds: λος 2001. ivate conunuunication). | To this set we have added the data of 991216 (observed lag $\Delta t_{\text{obs}} =
0.018^{+0.002}_{-0.001}$ seconds; Norris 2001, private communication). |
The correlation between rest-fune BATSE use lags. Af. aud jet-break times. T;—Ff(ll). is shown in Figure τι bursts with longer lags lave onger jetbreak times. | The correlation between rest-frame BATSE pluse lags, $\Delta t$, and jet-break times, $\tau_j \equiv t_j/(1 + z)$, is shown in Figure \ref{tjvtlag}; bursts with longer lags have longer jet-break times. |
The datais fit with a least-Squares fit usine errors du fyeo-dinensions where errors on spectral lags are given in Norrisetal.(2000)x ancl errors i1 jet-weak tine are considered prescutLy. | The data is fit with a least-squares fit using errors in two-dimensions where errors on spectral lags are given in \citet{nmb00} and errors in jet-break time are considered presently. |
Jet-1lweak tines roni the sample of Frailctal. have not been determined wnitormly: ποιο of thejet-break times are derived frou iuulti-baud modeling (covering the radio to X-ray passbaucs). while other eveuts have primarily been observed in a single passband. and are less wiell constrained. | Jet-break times from the sample of \citet{fksd01} have not been determined uniformly: some of thejet-break times are derived from multi-band modeling (covering the radio to X-ray passbands), while other events have primarily been observed in a single passband, and are less well constrained. |
is used, where µο is the central surface brightness, r is the galactocentric radius, and rq is the disk scale length of the outer disk. | is used, where $\mu_0$ is the central surface brightness, $r$ is the galactocentric radius, and $r_d$ is the disk scale length of the outer disk. |
In addition to these two components, other functions may be used to fit the halo component, bars, rings, and other structures in the galaxies (e.g.,Prietoetal. 2001),, and the fits can be applied to one-dimensional light profiles or directly on two-dimensional images (Byun&Free-man 1995). | In addition to these two components, other functions may be used to fit the halo component, bars, rings, and other structures in the galaxies \citep[e.g.,][]{Petal01}, and the fits can be applied to one-dimensional light profiles or directly on two-dimensional images \citep{BF95}. |
. Here we fit equation (2)) to the one-dimensional surface brightness profiles. | Here we fit equation \ref{eq:exponential}) ) to the one-dimensional surface brightness profiles. |
Running the fully automated fitting algorithm on all retrieved images, we found a number of artefacts which cause problems for applying the code successfully. | Running the fully automated fitting algorithm on all retrieved images, we found a number of artefacts which cause problems for applying the code successfully. |
These include: | These include: |
2008b). | . |
. However, all these works had to apply very simplistic models to answer a fundamental question: which are the strengths of internetwork magnetic fields?. | However, all these works had to apply very simplistic models to answer a fundamental question: which are the strengths of internetwork magnetic fields?. |
This question is of paramount importance to estimate the role of the internetwork on the photospheric magnetism, specially because of the large area that it occupies. | This question is of paramount importance to estimate the role of the internetwork on the photospheric magnetism, specially because of the large area that it occupies. |
Models used to infer physical information from the observed Zeeman signals are usually based on one (or two) magnetic atmosphere(s) embedded in a non-magnetized plasma. | Models used to infer physical information from the observed Zeeman signals are usually based on one (or two) magnetic atmosphere(s) embedded in a non-magnetized plasma. |
This strategy has allowed to put in evidence that internetwork magnetic fields have a preference for hG field strengths and suggests that the topology of the magnetic field is quasi-isotropic 2008b.a;AsensioRamos2009a:Bommieretal.2009) |. | This strategy has allowed to put in evidence that internetwork magnetic fields have a preference for hG field strengths and suggests that the topology of the magnetic field is quasi-isotropic \citep{marian_08, marian_andres_08, andres_09, bommier_09}
. |
Diagnostic techniques based on the Hanle effect model the internetwork magnetic field assuming that it is microturbulent (isotropic below the mean free path of line-core photons). | Diagnostic techniques based on the Hanle effect model the internetwork magnetic field assuming that it is microturbulent (isotropic below the mean free path of line-core photons). |
Within this scenario, magnetic field stregths ~ 10-100 G (Stenflo 1982)., and ~20-30 G 2001).. have been inferred. | Within this scenario, magnetic field stregths $\sim 10$ -100 G \citep{stenflo82}, , and $\sim 20$ -30 G \citep{faurobert_01}, have been inferred. |
A more recent estimate (TrujilloBuenoetal.2004)., based on three-dimensional radiative transfer calculations and state-of-the-art atmospheric models finds mean field strengths as high as (5)~130 G. Evidence that Hanle depolarization by a randomly oriented field is indeed at work in the quiet solar photosphere was provided by (2004)., though without giving strong constrains on the actual value of (B). | A more recent estimate \citep{javier_04}, based on three-dimensional radiative transfer calculations and state-of-the-art atmospheric models finds mean field strengths as high as $\langle B\rangle\sim 130$ G. Evidence that Hanle depolarization by a randomly oriented field is indeed at work in the quiet solar photosphere was provided by \cite{rafa_04}, , though without giving strong constrains on the actual value of $\langle B\rangle$. |
Simple models favor a straightforward interpretation of the data and provide an estimate of a (non-linear) average of the distribution of field strengths in the very quiet Sun. | Simple models favor a straightforward interpretation of the data and provide an estimate of a (non-linear) average of the distribution of field strengths in the very quiet Sun. |
Unfortunately, since the field is known to be organizedbelow the resolution element, thisstructuring escapes to | Unfortunately, since the field is known to be organizedbelow the resolution element, thisstructuring escapes to |
For example. there is a positive shift of 0.10. in the amplitude of sealar perturbations. zl. and 0.36 in the spectral iudex of scalav perturbations. | For example, there is a positive shift of $0.4\sigma$ in the amplitude of scalar perturbations, $A_{\textrm{s}}$ , and $0.3\sigma$ in the spectral index of scalar perturbations. |
Although relatively modest. these shifts are certainly large enough that they should be taken properly iuto account. | Although relatively modest, these shifts are certainly large enough that they should be taken properly into account. |
This paper has two iain goals. | This paper has two main goals. |
First. we wanted to generate a set of WALAP-like simulations that fully take into account the asvunmetric beams aud anisotropic scanning pattern of the WMADP satellite. | First, we wanted to generate a set of WMAP-like simulations that fully take into account the asymmetric beams and anisotropic scanning pattern of the WMAP satellite. |
Such siuulatious are extremely valuable for| unuderstaudiug the impact of beam asvnuuctrics on various statistical estimators and models. | Such simulations are extremely valuable for understanding the impact of beam asymmetries on various statistical estimators and models. |
One example of such. which indeed provided us with the initial motivation for studving this issue. is the anisotropic uuiverse model presented by Ackermanetal.(2007). aud later considered in detail with respect to the WALIAP data bv Curoenebooni&Eriksen(2009).. | One example of such, which indeed provided us with the initial motivation for studying this issue, is the anisotropic universe model presented by \citet{ackerman:2007}, and later considered in detail with respect to the WMAP data by \citet{groeneboom:2009a}. |
. The result from that analysis was a tentative detection of violation of rotational invariance in the early universe. or some other effect with simular observational signatures. at the 3.86 confidence level. | The result from that analysis was a tentative detection of violation of rotational invariance in the early universe, or some other effect with similar observational signatures, at the $3.8\sigma$ confidence level. |
It was shown that ucither foregrounds nor correlated noise could generated this signal. but the question of asvinmetric beams was left unanswered. | It was shown that neither foregrounds nor correlated noise could generated this signal, but the question of asymmetric beams was left unanswered. |
This issue will now be revisited iu au upconmius paper. using the simulations generated here. | This issue will now be revisited in an upcoming paper, using the simulations generated here. |
The secoud goal ofthe paper was to assess the impact of beam asviunaetries ou the WALAP power spectrum aud cosmological paramicters. | The second goal of the paper was to assess the impact of beam asymmetries on the WMAP power spectrum and cosmological parameters. |
We did this by comparing the vower προςσπα of the full beam convolved simulations with the power spectrum of the input realizations. hereby providing a direct estimate the effective beam ranster functions. | We did this by comparing the power spectrum of the full beam convolved simulations with the power spectrum of the input realizations, thereby providing a direct estimate the effective beam transfer functions. |
Dome so. we found differences at the 1].2% level in all differencing asseniblies at intermediate and hieh Cs with respect to the nominal WALAP trauster "nctions. | Doing so, we found differences at the $1-2$ level in all differencing assemblies at intermediate and high $\ell$ 's with respect to the nominal WMAP transfer functions. |
A similar analvsis was performed for the 3-vear WALAP data release by Winshawetal.(2007).. who approach the woblem from an analytical point of view. | A similar analysis was performed for the 3-year WMAP data release by \citet{hinshaw:2007}, who approach the problem from an analytical point of view. |
However. at hat time ouly the A-side beams were available (IBllctal. 2009).. and they therefore assunued identical beams on both the A aud D sides. | However, at that time only the A-side beams were available \citep{hill:2009}, and they therefore assumed identical beams on both the A and B sides. |
With this data. they conchided that the iupact of beam asviunietries was <1% everywhere below (=1000 for the V- aud W-band DAs. | With this data, they concluded that the impact of beam asymmetries was $\lesssim 1$ everywhere below $\ell = 1000$ for the V- and W-band DAs. |
For comparison. we fiud that there isa ~LX bias already at (=600 for the combined co-adcded temperature power ΠΡΟΤΗ. and increasing rapidly to ML5% at (o=TDU. | For comparison, we find that there is a $\sim1$ bias already at $\ell=600$ for the combined co-added temperature power spectrum, and increasing rapidly to $\sim1.5$ at $\ell=750$. |
It is not unlikely that this trend may continue further in (. but to answer that question considerably more computational resources is required. | It is not unlikely that this trend may continue further in $\ell$, but to answer that question considerably more computational resources is required. |
Nevertheless. the two analyses appear to be in reasonable aerecluent with each other. especially considering the fact that we take into account the full beam maps of both the A aud D sides. | Nevertheless, the two analyses appear to be in reasonable agreement with each other, especially considering the fact that we take into account the full beam maps of both the A and B sides. |
As far as cosmological parameters go. the inact of asviuuctric beams appear to be simall but noticeable. | As far as cosmological parameters go, the impact of asymmetric beams appear to be small but noticeable. |
Specifically, we find shifts of Q.lo in the amplituce of scalar perturbations. A. aud the plivsical density of cold dark matter. Q«gj77. and 0.30 in the spectral index of scalar perturbations. Εν. | Specifically, we find shifts of $0.4\sigma$ in the amplitude of scalar perturbations, $A_{\textrm{s}}$, and the physical density of cold dark matter, $\Omega_{\textrm{cdm}} h^2$, and $0.3\sigma$ in the spectral index of scalar perturbations, $n_{\textrm{s}}$. |
While these shifts are relatively modest. they are of the same order of magnitude or larger than. sav. mareinalization over the Suuvaey-Zeldovicl effect (Sperecletal.2007). or unresolved point sources (Noltaetal.2009).. which incleec are taken iuto account. | While these shifts are relatively modest, they are of the same order of magnitude or larger than, say, marginalization over the Sunyaev-Zeldovich effect \citep{spergel:2007} or unresolved point sources \citep{nolta:2009}, which indeed are taken into account. |
Oue outstanding question that still remains is the inupact of the anisotropic effective pixel window. | One outstanding question that still remains is the impact of the anisotropic effective pixel window. |
As explicitly demonstrated in this paper. the cifterence between the isotropized IHIEALPix pixel window and the actual WALTAP VI scanning induced pixel window becomes visible at (~900 for one vear of WALAP observations. | As explicitly demonstrated in this paper, the difference between the isotropized HEALPix pixel window and the actual WMAP V1 scanning induced pixel window becomes visible at $\ell \sim 900$ for one year of WMAP observations. |
Of course. this is well within the noise-dominated regime for the WALAP data. aud uulikelv to have any major impact on cosmological results; but we believe that a proper understanding of this issue. both with respect to WAIAP and Planck. is warranted. and intend to revisit this issuc m a separate study. | Of course, this is well within the noise-dominated regime for the WMAP data, and unlikely to have any major impact on cosmological results, but we believe that a proper understanding of this issue, both with respect to WMAP and Planck, is warranted, and intend to revisit this issue in a separate study. |
The simulations described in this paper may be dowloaded from ISW's lomepage™. | The simulations described in this paper may be downloaded from IKW's . |
. As described in Section 2.2.. we introduce oue new step to the differential map making algoritlaa prescuted by (1996): We initialize the iterations a the exact solution of Equation 7 evaluated at low resolution. which in this paper is taken to be Nag.=16. with 3072 pixels. | As described in Section \ref{sec:map_making}, we introduce one new step to the differential map making algorithm presented by \citet{wright:1996}: We initialize the iterations at the exact solution of Equation \ref{eq:map_making} evaluated at low resolution, which in this paper is taken to be $N_{\textrm{side}}=16$, with 3072 pixels. |
To demonstrate the improvement iu convergence due to this choice of iuitializatiou. we revisit the analytic case considered in Section L. which compared the results frou our simulation pipeline with au exact analytic case. but taking iuto account the actual WALTAP scauningC» strategv. | To demonstrate the improvement in convergence due to this choice of initialization, we revisit the analytic case considered in Section \ref{sec:analytic_comparison}, which compared the results from our simulation pipeline with an exact analytic case, but taking into account the actual WMAP scanning strategy. |
Oo, Iu FigureoO AS we show a set of difference maps taken between the intermediate solutions produced by the differential lap inaker aud the analytic and isotropic map solution. | In Figure \ref{fig:map_iterations} we show a set of difference maps taken between the intermediate solutions produced by the differential map maker and the analytic and isotropic map solution. |
From top to bottom. the paucls show the residuals after 2. Γ Sand LO iterations. aud at the bottom. the final converged solutions. | From top to bottom, the panels show the residuals after 2, 5 and 10 iterations, and at the bottom, the final converged solutions. |
The left panel shows theseries obtained whe initializing the search at the low-resolution solution. while the right panel shows the series when initializingat zero. | The left panel shows theseries obtained when initializing the search at the low-resolution solution, while the right panel shows the series when initializingat zero. |
Convergence was aclueved respectively after 67 and 123 iterations in the two cases, | Convergence was achieved respectively after 67 and 123 iterations in the two cases. |
nore nmaegnuetars that exhibit pulsed radio. enission. | more magnetars that exhibit pulsed radio emission. |
Tucreasing the nuuber of radio-loud maguetars kuowui could offer insight into the pulsar enmuüssion mechliauisia. he behavior of matter in ultrva-stroug maguctic fields. as well as the possible evolutionary relationship between uaenetars aud the much lager known population of rotation-powered pulsars. | Increasing the number of radio-loud magnetars known could offer insight into the pulsar emission mechanism, the behavior of matter in ultra-strong magnetic fields, as well as the possible evolutionary relationship between magnetars and the much larger known population of rotation-powered pulsars. |
This paper is organized as follows: 82. describes the observations undertaken. | This paper is organized as follows: \ref{sec:observations} describes the observations undertaken. |
The analysis performed ou he data collected is described iu | The analysis performed on the data collected is described in \ref{sec:analysis}. |
The results are xeseuted in §l.. | The results are presented in \ref{sec:results}. |
Iu 85 woe put the results iuto context and discuss their duplications. | In \ref{sec:discussion} we put the results into context and discuss their implications. |
Observations of five confirmed magnetars and two magnetar candidates were carricd out usine the NRAO 100-01 Green Dauk iu 2006-2007. | Observations of five confirmed magnetars and two magnetar candidates were carried out using the NRAO 100-m Green Bank in 2006-2007. |
The goal was to observe the maguetars aud maguetar candidates visible from the CDT in order to detect radio emiüssion. or in the absence of detection. establish baseline measurements should a target turn on as a radio source sole fiue in the future. | The goal was to observe the magnetars and magnetar candidates visible from the GBT in order to detect radio emission, or in the absence of a detection, establish baseline measurements should a target turn on as a radio source some time in the future. |
The proposal also iucluded. Tirget-ofOpportuuitv (Του)observations to be triggered if a source exhibited. an outburst. as determined by on-going X-ray monitoring observations. | The proposal also included Target-of-Opportunity (ToO) observations to be triggered if a source exhibited an outburst, as determined by on-going X-ray monitoring observations. |
Total intensity data were recorded by the (BT's Pulsar Spigot backend. an auto-correlation spectrometer2005). | Total intensity data were recorded by the GBT's Pulsar Spigot backend, an auto-correlation spectrometer. |
. Lageed-products were converted to spectra off-line. | Lagged-products were converted to spectra off-line. |
The result is spectra contaimime 600 AIIIz of usable bandwidth centered at 1950 MIIz (S-band) divided evenly iuto 768 channels. written out every 81.92 prs. Tere we preseut relevant details of our seven targets. | The result is spectra containing 600 MHz of usable bandwidth centered at 1950 MHz (S-band) divided evenly into 768 channels, written out every 81.92 $\mu$ s. Here we present relevant details of our seven targets. |
Tn total. 19 observatious of a variety of durations were made between 2006 November and 2007 October as stunmarized in Table ??.. | In total, 19 observations of a variety of durations were made between 2006 November and 2007 October as summarized in Table \ref{tab:observations}. |
For each source we preseut it best distance estimate. together with au estimate of the free clectrous along the lue-ofsight toward the source from the model. | For each source we present its best distance estimate, together with an estimate of the free electrons along the line-of-sight toward the source from the model. |
The free clectrou content is parameterized by the dispersion measure (DM). | The free electron content is parameterized by the dispersion measure (DM). |
Estimates of the model are used to deteriuuue the upper hit on DM searched for each target. | Estimates of the model are used to determine the upper limit on DM searched for each target. |
In all cases the DM searched was Z2 times larger then the maxinnun DM predicted alone the lue-ofsight.045: | In all cases the DM searched was 2 times larger then the maximum DM predicted along the line-of-sight.: |
This source las a rotational period of 11.8 s 1997). | This source has a rotational period of 11.8 s . |
'The estimated distance to this source is 845!| iskpe 2008). which. together with position. suggests a DM ~ 800 ? pe2002). | The estimated distance to this source is $8.5^{+1.3}_{-1}$ kpc , which, together with its position, suggests a DM $\simeq$ 800 $^{-3}$ pc. |
The supernova Wes 73 is associated with 1E 015. | The supernova Kes 73 is associated with 1E $-$ 045. |
The pulsar is monitored regululv bv NASA'«(AXTE. | The pulsar is monitored regularly by NASA's,. |
.2009). The analvsis of these data allow for an accurate rotational ephemeris for the pulsar to be determined for our GBT observing epoch: this is shown in Table ??..2259+586:: | The analysis of these data allow for an accurate rotational ephemeris for the pulsar to be determined for our GBT observing epoch; this is shown in Table \ref{tab:ephems}.: |
The maguetar has a period of 6.98 s1981).. The source is estimated to be at a distance of LOEO.S kpc2010). | The magnetar has a period of 6.98 s. The source is estimated to be at a distance of $4.0\pm0.8$ kpc. |
. This distance and the source position correspond to a liuc-ofsight DM. ~ 150 7 pe. | This distance and the source position correspond to a line-of-sight DM $\simeq$ 150 $^{-3}$ pc. |
LE 2259|586 is associated with the superiovaCTD 109. | 1E 2259+586 is associated with the supernovaCTB 109. |
LE 2259|586 is also monitored regularly using2009).. aud the resulting ephemeris is shown in Table ??.. 0142+61:: | 1E 2259+586 is also monitored regularly using, and the resulting ephemeris is shown in Table \ref{tab:ephems}. . : |
This source has a periodof 8.69 s. The distance to this source is estimated to be 23.640.1 kpc2006). | This source has a periodof 8.69 s. The distance to this source is estimated to be $3.6\pm0.4$ kpc. |
. This distance suggests DAI ~ 100 cui? pe. | This distance suggests a DM $\simeq$ 100 $^{-3}$ pc. |
The rotational ephemeris for IU 0112161 for our observiug epoch is shown in Table 77. | The rotational ephemeris for 4U 0142+61 for our observing epoch is shown in Table \ref{tab:ephems}. |
This ephemeris was also computed using data from regular monitoring observations2007). | This ephemeris was also computed using data from regular monitoring observations. |
. Within a few mouths before and after the start of our CBT observations. N-rayv bursts were detected from 1U 0112161 with2011). | Within a few months before and after the start of our GBT observations, X-ray bursts were detected from 4U 0142+61 with. |
. The six bursts were detected in three separate observatious ou ALJDs 53831 (oue burst). 53911 (four bursts) and 51158 (one burst). | The six bursts were detected in three separate observations on MJDs 53831 (one burst), 53911 (four bursts) and 54138 (one burst). |
The last of the six bursts had the largest veal, N-vav flux. | The last of the six bursts had the largest peak X-ray flux. |
Mouitorme observatious of LU 0112|61 were made on the day of this largest burst. as well as at l dax. 1week. 3 weeks. 2 iontlis and 8 mouths following lis burst (see Table ?7?)). 20: | Monitoring observations of 4U 0142+61 were made on the day of this largest burst, as well as at 1 day, 1 week, 3 weeks, 2 months and 8 months following this burst (see Table \ref{tab:observations}) ). : |
: The source has a rotational period of 7.56 s and is estimated to je at distance of 8.7!FS kpe2008)... which sugeests DM o 750 P pe. | The source has a rotational period of 7.56 s and is estimated to be at distance of $8.7^{+1.8}_{-1.5}$ kpc, which suggests DM $\simeq$ 750 $^{-3}$ pc. |
SCR 20 was observed o have a giant flare in late 20012005). | SGR $-$ 20 was observed to have a giant flare in late 2004. |
. Following the fare. a fading. extended. mupulsed radio jebula was observed arouud the source2005). | Following the flare, a fading, extended, unpulsed radio nebula was observed around the source. |
. Two days after the flare. a search for pulsed radio cnussion was performed at 1100 MIIz using the Parkes Radio telescope. | Two days after the flare, a search for pulsed radio emission was performed at 1400 MHz using the Parkes Radio telescope. |
No pulsed emissiou was detected down oa limit of Syου~0.2 παν2005)..19004-14: | No pulsed emission was detected down to a limit of $S_{1400} \sim 0.2$ mJy.: |
: This SCR has a periodicity of 5.17 s1999).. Its distauce is estimated o be 12. 15 kpe. which vields an estimated DAL — TOO cin?5m pc. using the upper limit of the distance estimate, | This SGR has a periodicity of 5.17 s. Its distance is estimated to be 12 – 15 kpc, which yields an estimated DM $\simeq$ 700 $^{-3}$ pc, using the upper limit of the distance estimate. |
SCR. 1900111 was observed to have a eiaut Hare in ndd-1999 1999).. Unpulsed. facing radio emission was also observed around SCR 1900|11 ‘ollowing the flare1999)..0258: | SGR 1900+14 was observed to have a giant flare in mid-1999 Unpulsed, fading radio emission was also observed around SGR 1900+14 following the flare.: |
This maeuetar candidate was detected in a single 1993 (ASCA)) observation with 1905)..P= s AN 0258 is teutatively classified) as an ANP candidate because of its long period. soft spectrum. and low dhunuinositv. | This magnetar candidate was detected in a single 1993 ) observation with $P = 6.97$ s. AX $-$ 0258 is tentatively classified as an AXP candidate because of its long period, soft spectrum, and low luminosity. |
The distance to the pulsar is estimated tobe 8.5 kpe1998). | The distance to the pulsar is estimated to be 8.5 kpc. |
. This distance corresponds to a DM ~ 750 ? pe. | This distance corresponds to a DM $\simeq$ 750 $^{-3}$ pc. |
AN 0258 isspatiallycoimcident with the supernova reimnaut 29.6|0.11999).. sugeestinge that the relatnud laenetar candidate are associated. | AX $-$ 0258 isspatiallycoincident with the supernova remnant G29.6+0.1, suggesting that the remnantand magnetar candidate are associated. |
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