Ultra-wide Bandwidth Observations of 19 Pulsars with Parkes Telescope

Zu-Rong ZhouJing-Bo WangNa WangGeorge Hobbsand Shuang-Qiang Wang

1 Xinjiang Astronomical Observatory,Chinese Academy of Sciences,Urumqi,Xinjiang 830011,China; wangjingbo@xao.ac.cn, na.wang@xao.ac.cn

2 University of Chinese Academy of Sciences,19A Yuquan Road,Beijing 100049,China

3 Xinjiang Key Laboratory of Radio Astrophysics,150 Science1-Street,Urumqi,Xinjiang 830011,China

4 Key Lab of Radio Astronomy,Chinese Academy of Sciences,Beijing 100101,China

5 CSIRO Astronomy and Space Science,PO Box 76,Epping,NSW 1710,Australia

6 CAS Key Laboratory of FAST,NAOC,Chinese Academy of Sciences,Beijing 100101,China

Abstract Flux densities are basic observation parameters to describe pulsars.In the most updated pulsar catalog,24%of the listed radio pulsars have no flux density measurement at any frequency.Here,we report the first flux density measurements,spectral indices,pulse profiles,and correlations of the spectral index with pulsar parameters for 19 pulsars employing the Ultra-Wideband Low receiver system installed on the Parkes radio telescope.The results for spectral indices of 17 pulsars are in the range between−0.6 and−3.10.The polarization profiles of thirteen pulsars are shown.There is a moderate correlation between the spectral index and spin frequency.For most pulsars detected,the signal-to-noise ratio of pulse profile is not high,so DM,Faraday rotation measure,and polarization cannot be determined precisely.Twenty-nine pulsars were not detected in our observations.We discuss the possible explanations for why these pulsars were not detected.

Key words: (stars:) pulsars: general–stars: neutron–methods: data analysis

1.Introduction

Pulsars have been discovered for more than 53 yr(Hewish1968),though its radiation mechanism has not yet been fully understood(Jankowski et al.2018).One of the widely accepted models is that the radio emission regions are limited to the open polar cap inside the light-cylinder radius(Ruderman&Sutherland1975).However,the specific radiation area,physical process,and other details about pulsar radio emission are still unclear.Studying the radio spectra of pulsars is helpful to understand their emission mechanism.Unfortunately,only a few hundred pulsars have determined spectra.Only a tiny proportion of pulsars have been studied in a relatively wide frequency range(e.g.,Dai et al.2015).

Measurements of flux density at multiple frequencies are needed when we determine the spectra of pulsars.The Australia Telescope National Facility (ATNF) Pulsar Catalog(Manchester et al.2005) provides a database for pulsar observational parameters.Pulsar flux densities in this catalog are relatively well-known near 1400 and 400 MHz,where most pulsars have been found,but few are known at other frequencies.We have referenced the most updated catalog,version 1.64,and out of the 2872 radio pulsars in the catalog,680 do not have flux density values in any radio waveband.Moreover,97.4%have no historical flux density measurements near 2 GHz,74.3% have no recorded flux density values near 400 MHz,and 32.5% have no recorded measurements of flux density close to 1400 MHz.The pulsar parameters in the catalog are collected by different telescopes and different generations of receivers and backends,and each has its own system error.Significant differences were found between multiple measurements(Levin et al.2013).Therefore,it is vital to obtain the absolute flux density calibrated measurements of pulsars(Jankowski et al.2018).Efforts to measure radio spectra began in earnest with Rankin et al.(1970) and Sieber (1973),followed by Malofeev &Malov (1980) and Izvekova et al.(1981).They measured the spectra at low frequencies near 100 MHz and below,finding that most pulsars have cliffy spectra that can be expressed as a simple power-law.Some pulsar spectra deviate from a simple power-law at low frequencies and show a turn-over(Rankin et al.1970),while some show a highfrequency cut-off in the form of a spectrum steepening or a break in the spectrum(Sieber1973).Lorimer et al.(1995) examined the spectra of 280 pulsars and obtained a mean spectral index of−1.6.A study was conducted of the spectral properties of 441 radio pulsars observed with the Parkes telescope (Jankowski et al.2018) and found about 79% of these pulsars could be classified as simple power-law spectra.

People realized that pulsars were usually highly polarized long ago(Lyne &Smith1968).The long-term stability of the pulse profile and its complexity in terms of total intensity and polarization are also important characteristics of pulsars.The mean pulse profile and polarization properties help in understanding the geometry of the star,the pulse emission mechanism,and the beaming of pulsar radiation.Mean pulse profiles often have double or triple components,leading to different descriptions of the origin of the beamed emission(Backer1976),and the spectral index often varies from one component to the next (e.g.,Backer1972).Polarization properties of pulsars are normally described in terms of the four Stokes parameters.Many pulsars display a systematic variation across the pulse profile of the position angle (PA).The observed PA swings in many pulsars like the “S”-shaped curve are explained by the rotating vector model (Radhakrishnan&Cooke1969).Of course,the observed PA variations are not always continuous and smooth.Both normal pulsars and millisecond pulsars (MSPs) often can be seen with a high degree of linear polarization,and orthogonal-mode PA jumps(see e.g.,Yan et al.2011).Linear polarization is usually relatively stronger than circular polarization.Circular polarization most often has a sense reversal near the profile midpoint,usually associated with the core or central component of the profile(Rankin1983).

In addition to the shape properties of the mean pulse profile,the width of the mean pulse profile is also used to describe the profile characteristics.The angular width of the mean pulse is also known as the width of the observed beam.W50andW10are pulse widths that are often mentioned and studied (see e.g.,Gould &Lyne1998).Pulsars exhibit a diverse frequency dependence of average pulse profile.Phillips &Wolszczan(1992) demonstrate the whole profile width and spacing between each component of three pulsars increase with the decrease of observation frequency from 4800 to 50 MHz using the Arecibo 305 m radio telescope.The increasing pulse width trend is very obvious in the frequency band below 1 GHz.Xilouris et al.(1996) extended the measurements of profile width to 32 GHz and combined their measurements with published values at lower frequencies,showing a better fit withW50of six pulsars.TheW10values versus the observing frequencies of 150 normal pulsars were well fitted with the Thorsett relationship(Thorsett1991;Chen &Wang2014).

Lately,the Parkes 64 m radio telescope has been equipped with an ultra-wideband,low-frequency receiver.The frequency range of the receiver system is continuous from 704 to 4032 MHz.Moreover,the receiver has excellent sensitivity and polarization properties (Zhang et al.2019).The highsensitivity,well-calibrated and wide frequency observations with the Parkes telescope could efficiently provide us a systematic and uniform sample of pulsar flux densities(Hobbs et al.2020).In this work,we describe observations of 19 pulsars using the Ultra-Wideband Low(UWL)receiver system in Section2.Our results are shown in Section3.We discuss the results and give a concluding summary in Section4.

2.Observations and Data Reduction

We referenced the ATNF Pulsar Catalog version 1.59 to identify all radio pulsars without a flux density measurement near 1400 MHz that can be observed by the Parkes telescope.This list provides 505 pulsars.Then we removed all pulsars only detected in a survey that has a poorly defined sensitivity limit (for instance,some surveys are simply defined in the catalog as “miscellaneous” and very long observations with large telescopes may have detected the pulsars).After applying this selection,we have 327 pulsars remaining.Based on the known survey sensitivities,we know we can obtain a detectable signal close to 1400 MHz with observation durations of 30 minutes for all these pulsars.Still,some will be detectable at a high signal-to-noise ratio (S/N) with significantly shorter integration times.In particular,54 of these pulsars were discovered in the Molonglo surveys or with the Parkes 70 cm receiver(Manchester et al.1978).Such pulsars can be detected with only a few minute integration time.

These 54 pulsars were observed with Parkes using the UWL receiver.All the details of the receiver and backends are described in Manchester et al.(2013) and Hobbs et al.(2020).Medusa and Parkes Digital Filter Banks 4 (PDFB4) are simultaneously used for the signal pre-processor systems in the observation.The frequencies of these two backends are centered at 2368 MHz and 1369 MHz,respectively.The total recording bandwidth of Medusa (3328 MHz) was subdivided into 3328 frequency channels,while PDFB4 of 256 MHz was subdivided into 1024 frequency channels.In the meantime,each pulsar period was divided into 1024 phase bins with each band.The data for all observations were recorded in a fold mode in 30 s and de-dispersed online coherently.Note that PDFB4 has no flux calibrator.

The data were processed with the PSRCHIVE software package(Hotan et al.2014).We removed 5% of the band edges and manually excised data affected by narrow-band and impulsed radio frequency interference (RFI).We used the PSRCHIVE program PAZ to eliminate RFI automatically.Then we utilized PAZI to inspect the pulse profiles visually and remove subintegrations or frequency channels affected by RFI manually.We also relied on observations of the radio galaxy 3C 218(Hydra A)to transform the measured intensities to absolute flux densities,using on-and off-source pointing to measure the obvious brightness of the noise diode as a function of radio frequency.The pulsar observations were calibrated with their associated calibration files using PAC to transform the polarization products to Stokes parameters,to flatten the bandpass,and to calibrate the pulse profiles in flux density units.We formed a noise-free standard template from our observations using PAAS and then employed PSRFLUX to obtain the average flux density.All raw data of 54 pulsars can be downloaded from the CSIRO data archive(Hobbs et al.2011).

3.Results

We obtained data sets of 54 pulsars for which no flux densities were previously published near 1400 MHz,and havesuccessfully detected 25 pulsars.Only 14 of 25 pulsars were detected at 1369 and 2368 MHz at the same time.We gained pulse profiles and flux densities of 19 pulsars at 2368 MHz.No flux calibrator is available for the other six pulsars at 1369 MHz.

3.1.Flux Density Measurements

One of the fundamental properties of any astronomical source is its flux density,so we recommend that these flux densities should be included in the next version of the pulsar catalog.Our main results are listed in Table1,in which the pulsar name,pulse period,dispersion measure (DM),observation frequency,Modified Julian Date(MJD),observation times,observation length,S/N of the pulse profile,average flux density obtained at 2368 MHz,and width of pulse profiles at 50% (W50) are given in column order.Nineteen pulsars which are observed at 2368 MHz in Table1are mainly young pulsars with characteristic ages mostly between 106and 107yr,except for PSR J0348+0432 and PSR J2222−0137,which are in binary systems with a white dwarf (WD) companion with different masses.The observation time of most pulsars is about 10 minutes.(TheS2368represents flux density at 2368 MHz.)In Table1,flux densities range from 0.23 to 2.06 mJy.It is noted thatW50ranges from 3°to 21°.The error ofW50was estimated by determining how the width changes when the 50% flux density cuts across the profile move up or down by the baseline root mean square (rms) noise level (Dai et al.2015).W50andW10of 17 pulsars from literature at other frequencies are given in TableB2.TheW50values for PSR J1833−6023 at two frequencies are identical.TheW50of 10 pulsars decreases with frequency,but that of six pulsars increases with frequency.

Table 1Pulsar Observational Parameters

3.2.Spectral Indices

The obtained flux densities can be used to measure the spectral indices.Many pulsars have been observed at one or more frequencies of 400,600,800,1400,2000,and 3000 MHz(e.g.,Dai et al.2015;Jankowski et al.2018).To estimate spectral indices,we divide the UWL data sets into three subbands and measure the flux density for each of them.Their center frequencies are close to 1400,2000,and 3000 MHz,with sub-bandwidths of 400 MHz,400 MHz,and 600 MHz,respectively.The results are listed in Table2asS1400,S2000,andS3000.Except for six pulsars (PSR J1057−4754,PSR J1805+0306,PSR J1810−5338,PSR J1854−1421,PSR J1903−0632,and PSR J2222−0137),the flux density of 13 other pulsars cannot be measured in all the three sub-bands since too many frequency channels are removed.The pulse profiles of only one or two sub-bands can be seen for some pulsars.Previously publishedS150,S200,S300,S400,S600,S700,S800,andS6000for these pulsars are used to estimate the spectral index,and the references are given in the last column of Table1.We assume a simple power-law of the formSν=bxα,where,ν is the center frequency and ν0=1.4 GHz a constant reference frequency.The fit parameters are the spectral index α and a constantb,and their values are provided in Table2.The spectral behavior of the 17 pulsars can be described well by a simple power-law over the frequency range considered.The spectral indices of all the 17 pulsars are between−0.6 and−3.10.For PSR J1810−5338,a broken power-law is better to describe the spectrum with a 600 MHz cut-off frequency,and α1is the spectral index before and α2the one after the break.The spectral plots of 18 pulsars and power-law fits to the data are depicted in Figure1.According to previous statistics,the mean spectral index of pulsars with a simple power-law spectrum is about−1.60.The majority of our spectral indices are flatter than the mean values from Jankowski et al.(2018),but our measurements are not particularly unusual as there are many other pulsars that also have similar spectral indices.As our sample is relatively small,we do not think our pulsar sample is particularly inclined to flat spectrum pulsars.

Table 3Correlation of Spectral Index α with lg|x| for Different Pulsar Parameters x

3.3.Polarization Profiles

Pulse profiles at 2368 MHz for all the 19 pulsars are presented for the first time.The profiles of 20 among 25 pulsars were published in the European Pulsar Network (EPN)database near 1.4 GHz for the first time except for five pulsars(PSR J1057−4754,PSR J1604−7203,PSR J1625−4048,PSR J1728−0007,and PSR J1805+0306).7 http://www.epta.eu.org/epndbThe pulse profiles at 1369 MHz and 2368 MHz of most pulsars are similar in our observations.Most of the average pulse profiles in FiguresA1andA2have a single peak,and the pulse profiles are narrow.Figures2–4display the calibrated polarization profiles for 13 pulsars in our sample.A rotation measure (RM) fitting during the calibration is considered during the calibration of polarization.Only six pulsars show strong polarization characteristics at two frequencies simultaneously,while the other seven pulsars only have polarization profiles at 1369 or 2368 MHz.Polarization cannot be measured precisely for other pulsars due to the limited S/N.Results for individual pulsars are described in detail as follows.

3.3.1.PSR J0348+0432

PSR J0348+0432,a binary pulsar in a 2.46 hr orbit with a low-mass ELL1 WD companion,was first discovered in the Green Bank Telescope(GBT)350 MHz drift scan survey.The pulse profile of the pulsar at 350 MHz has three components(Lynch et al.2013),while Figure3shows a single peak at 2368 MHz and is linearly polarized.There is significant right-hand circular polarization and slight shallow rotation in the PA variation across the profile.

3.3.2.PSR J1157−5112

PSR J1157−5112 was discovered in the first high-frequency survey of intermediate Galactic latitudes.It is a 44 ms pulsar and the first recycled pulsar with an ultramassive (M>1.14Msolar) WD companion(Edwards et al.2001).The polarization profile for PSR J1157−5112 shows a single peak at 1369 MHz in Figure4.The profile is linearly polarized,and there is little or no variation in the PA.No significant circular polarization is observed across the whole profile.

3.3.3.PSR J1420−5416(PSR B1417−54)

PSR J1420−5416 was first discovered at 408 MHz in the Molonglo survey(Manchester et al.1978).Figure3affirms the pulse profile of this pulsar consists of two closely spaced components at 2368 MHz.The leading component is less linearly polarized than the trailing component,and the PA exhibits a continuous decrease across the trailing component.There is significant right-hand circular polarization.

3.3.4.PSR J1615−2940(PSR B1612−29)

Similar to PSR J1420−5416,PSR J1615−2940 was also discovered in the second Molonglo pulsar survey (Manchester et al.1978).Figure3depicts a pulse profile with two components at 2368 MHz.The pulse profile is very low in linear polarization,and thus there is very little PA measured.There is a sense reversal of the circular polarization from righthand to left-hand under the trailing part of the profiles.

3.3.5.PSR J1728−0007(PSR B1726−00)

PSR J1728−0007 was found in a survey for short period pulsars(Stokes et al.1985).Weisberg et al.(1999) published its profile at 1418 MHz,but the linear polarization is too weak to measure.Figure3demonstrates the pulse profile consists of two components at 2368 MHz.The pulsar is linearly polarized with a continuously increasing PA across the profile.

3.3.6.PSR J1746−2856

PSR J1746−2856,a highly dispersed pulsar,was discovered in the direction of the Galactic Center at 3.1 GHz with the Parkes radio telescope (Johnston et al.2006).The mean pulse profiles and polarization parameters for this pulsar at 2368 MHz are shown in Figure3.The degree of linear polarization is low,with very little PA measured.There are probably four or five distinct components,but it is impossible to classify this pulsar without additional information.

Figure 1.Spectra for 18 pulsars and power-law fits to the data (blue lines).The red bars give the uncertainties of the flux densities at the different frequencies.

Figure 2.Average polarization profiles for PSR J1805+0306,PSR J1810−5338,PSR J1833−6023,PSR J1848−1952,PSR J1903−0632 and PSR J1854−1421 at 1369 and 2368 MHz.The total intensity is shown in black,while the linear polarization and circular-polarization are shown in red and blue respectively.

Figure 2.(Continued.)

Figure 3.Average polarization profiles for PSR J0348+0432,PSR J1420−5416,PSR J1615−2940,PSR J1728−0007,PSR J1746−2856,and PSR J2222−0137 at 2368 MHz.The total intensity is shown in black,while linear polarization and circular polarization are shown in red and blue respectively.

Figure 4.Average polarization profile for PSR J1157−5112 at 1369 MHz.

3.3.7.PSR J1805+0306(PSR B1802+03)

Polarization profiles at 2368 and 1369 MHz for PSR J1805+0306 are presented in Figure2.The profiles display two components at both frequencies.The leading part of the profile has relatively high fractional linear polarization,whereas the trailing part of the profile is essentially unpolarized at both frequencies.There is a shallow rotation of the PA through the leading component at 2368 MHz.The polarization profiles at 1369 MHz are in good agreement with those presented by Weisberg et al.(1999) at Arecibo 1418 MHz.

3.3.8.PSR J1810−5338(PSR B1806−53)

As is visible in Figure2,the mean pulse profiles of PSR J1810−5338 are almost the same at the two frequencies.There are three pulse components of the pulsar,which are similar to that at 660 MHz(Jiang &You2014).The leading and trailing components are weaker than the central component of the pulse profile.The central component is less linearly polarized than the leading and trailing components at both frequencies.Flat increasing PA swings through the overall profiles can be seen both at 2368 and 1369 MHz.There is a sense reversal of the circular polarization from right-hand to left-hand under the whole profiles at both frequencies.

3.3.9.PSR J1833−6023(PSR B1828−60)

The mean pulse profiles and polarization parameters for PSR J1833−6023 at 2368 and 1369 MHz are similar,which are shown in Figure2.The pulsar was first discovered at a frequency of 408 MHz by the second Molonglo pulsar survey(Manchester et al.1978).PSR J1833−6023 has a profile with only one narrow component,and the profile is linearly polarized.There is a strong sense reversal of the circular polarization from right-hand to left-hand under the overall pulse,and a steep decreasing PA swings across it.

3.3.10.PSR J1848−1952(PSR B1845−19)

PSR J1848−1952 was first discovered by an extensive survey of pulsars which had been undertaken using observations at the Molonglo Radio Observatory and the Australian National Radio Astronomy Observatory,Parkes.The observing frequency for both the Molonglo and Parkes observations was 408 MHz(Manchester et al.1978).As displayed in Figure2,the mean pulse profile of PSR J1848−1952 at both 2368 and 1369 MHz consists of two close sharp components.The PA variations are different,but the linear and circular polarizations are almost the same at two frequencies.The overall pulse has obvious linear polarization,and the trailing component is less linearly polarized than the leading component.A high degree of right-handed circular polarization was observed across the whole profile.There is a continuous decreasing PA across the profile at 2368 MHz,while the PA variation is complex with a shallow rotation swing through it at 1369 MHz.

3.3.11.PSR J1854−1421(PSR B1851−14)

Similar to PSR J1848−1952,PSR J1854−1421 was first also discovered by the second Molonglo pulsar survey(Manchester et al.1978).The pulse profile of the pulsar in Figure2exhibits a single peak at both 2368 and 1369 MHz and is linearly polarized.There is a continuous decreasing PA across the profile at 1369 MHz,while the PA variation is discontinuously decreasing with a PA jump at 2368 MHz.No significant circular polarization is observed across the whole profile.

3.3.12.PSR J1903−0632(PSR B1900−06)

Mean pulse profiles and polarization parameters for PSR J1903−0632 at 2368 and 1369 MHz are very similar,as displayed in Figure3.The pulsar was discovered during a systematic search for pulsars at a frequency of 408 MHz,carried out with the Jodrell Bank Mark IA radio telescope in 1972 (Davies et al.1972).Similar to 408 MHz,the pulse profile of the pulsar also has two pulse components at two frequencies.The trailing component is less linearly polarized than the leading component.PSR J1903−0632 shows a small amount of circular polarization from left-hand to right-hand under the overall profile.The PA variation across two components appears continuous and has a negative slope.

3.3.13.PSR J2222−0137

PSR J2222−0137,a 2.44 day binary pulsar with a massive CO WD companion,was first discovered in the GBT 350 MHz drift scan survey.The mean pulse profile and polarization parameters for PSR J2222−0137 at 2368 MHz given inFigure3have far more details than previously published results at 820 MHz (Boyles et al.2013).The pulse profile is very similar at both frequencies,with only one pulse component.The linear polarization is low under the overall profile.There is a hint of circular polarization from left-hand to right-hand against the profile.The PA variation across the profile is complex with regions of increasing and decreasing PAs,and a PA jump can be seen at phase 0.504.

3.4.Correlations of Spectral Index with Pulsar Parameters

We test for a correlation between spectral index α and lg|x|for all the 18 pulsars,wherexis one of the pulsar parameters below.The parameters are spin frequency ν,spin-down rate ˙ν,the magnetic field at the light cylinder radiusBLC,the characteristic age тc,the surface magnetic fieldBsurf,the spin-down luminosity ˙E,pulse periodP,and period derivative ˙Pof the pulsar.We took all values of pulsar parameters from the ATNF Pulsar Catalog.Most are covariant because these quantities depend on basic pulsar parameters,such as pulse period and its derivative.

We first measured the correlation by visual inspection,then computed the Spearman rank correlation coefficient to characterize its strength.We test all pulsars in our single power-law data set first,then the isolated pulsars.There are only two pulsars in the binary system.The correlation coefficients,correspondingp-values,and the number of pulsarsN,for which correlations are computed,are listed in Table3.

We find a moderate correlation between the spectral index and the pulse period for normal pulsars.All the other combinations show no correlation.For isolated pulsars,we find a mildly negative correlation of spectral index with the surface magnetic field.

4.Discussion and Conclusions

The minimum detectable flux density (Smin) of the UWL system can be evaluated using the radiometer equation(Manchester et al.1996)

where α=S/N,β is the factor of digitization and other processing losses,Tsysis the sum of receiver temperature and sky temperature (K),Gis the gain of the telescope,Npis the number of polarizations(two in this case),Δν is the observing bandwidth (MHz),Tis the observation length (s),Wis the effective pulse width in time units,andPis the pulse period(Dewey et al.1985).According to Equation (1),the minimum detectable flux density of the UWL system varies from pulsar to pulsar with differentW,P,andT.Here,we adopt α=10,β=1.5 (Manchester et al.1996),G=0.64 K Jy−1(Edwards et al.2001),Tsys=22 K,and Δν=3328 MHz(Hobbs et al.2020).The minimum detectable flux density(Smin)of the UWL system ranges from 0.02 to 0.76 mJy for pulsars with different duty cycles.

However,54 pulsars have been observed and only 25 have been detected.Among the 29 pulsars undetected,six pulsars are MSPs with periods from 1.7 to 3.7 ms,and the periods of the other 23 pulsars range from 44 ms to 4.3 s.We estimated the flux densities at 2368 MHz assuming the spectral index α=−1.6 for undetected pulsars with only one published flux density (the flux densities of PSR J1231−1411 and J2256−1024 were estimated separately).As shown in TableB1,all the estimatedS2368of 22 pulsars are potentially detectable by the UWL system.

1.Equation (1) is not suitable for estimating the sensitivity of the UWL system.Because the bandwidth of the UWL system is very wide,the flux densities of pulsars in the bandwidth change significantly and decrease in the highfrequency part.

2.The flux density of a radio pulsar decreases rapidly with increasing observing frequency.According to previous statistics,the spectral index of pulsars varies significantly.As expressed in TableB1,the estimated flux density at 2368 MHz for some pulsars is significantly higher than the detection threshold of the UWL system.Those undetected pulsars may have a steeper radio spectrum.

3.The bandwidth of the UWL system cannot be fully utilized.Part of the bandwidth is contaminated by RFI and has to be removed.Therefore,the sensitivity of the UWL system is not as high as we calculated using Equation (1).In fact,most of the frequency channels from 700 to 1000 MHz have been removed,and the radio emission of pulsars is bright at the low end of the UWL system.

4.The radio emission of pulsars is strongly affected by propagation through the interstellar medium (Kumamoto et al.2021).The typical observing length of our observations is only 10 minutes,but the timescale of diffractive scintillation could be hours,which is much longer than our observing length.

The correlation coefficients for pulsars in our sample,along with previous results from Zhao et al.(2019),Jankowski et al.(2018),Han et al.(2016),and Lorimer et al.(1995),are listed in Table3.Jankowski et al.(2018) obtained Spearman rank correlations of the spectral index with various pulsar parameters for 276 pulsars with simple power-law spectra.They found moderate correlations with ˙ν,BLC,and ˙Efor young pulsars.Han et al.(2016)and Lorimer et al.(1995)ascertained a very weak correlation for the spectral index with ˙E.For pulsars in our sample,we find moderate correlations between spectral index with ν,which are in the sense of steeper spectra for fast-rotating pulsars.No consistent correlation is found across the different samples,and results from disparate samples are distinct.

Table B1Estimated Flux Densities at 2368 MHz (S2368) for 22 Pulsars

Table B2Pulse Widths from Literature for 17 Pulsars

In this work,we have carried out ultra-wide bandwidth observations of 19 pulsars with the Parkes telescope.Flux density measurements,spectral properties,polarization profiles,and pulse widths at 2368 MHz or 1369 MHz have been presented.The non-detection of polarization in 12 out of 25 pulsars is perhaps not be surprising.As depicted in FigureA1,the S/N of some pulse profiles (PSRs J0057−7201,J1721−1939,J1816−5548,etc.) is low.It is not very likely to measure polarization with a low S/N.Other pulse profiles have a medium S/N.The degree of linear polarization for these pulsars may be low.To measure the pulse profile,polarization and RM with high precision and study their evolution with frequency,longer observations for these pulsars are needed.We also note that there is a large number of pulsars in the catalog that still do not have such basic information as the flux density near 1.4 GHz.Observing each pulsar for a longer time or using telescopes with larger observation apertures (such as FAST)at a specific frequency is needed when we continue this work in the future.

Acknowledgments

The Parkes radio telescope is part of the ATNF which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO.This paper includes archived data obtained through the CSIRO Data Access Portal(http://data.csiro.au).This work is supported by the National Natural Science Foundation of China (Grant No.NSFC12041304),National SKA Program of China (No.2020SKA0120100),Youth Innovation Promotion Association of Chinese Academy of Sciences,National Key Research and Development Program of China (No.2017YFA0402602),the CAS Jianzhihua project,and Heaven Lake Hundred-Talent Program of Xinjiang Uygur Autonomous Region of China.

Appendix A

Figures of Averaged Pulse Profiles

Figure A1.Averaged pulse profiles at 2368 MHz were obtained with the Parkes telescope for seven pulsars.

Figure A2.Averaged pulse profiles of 13 pulsars at a center frequency of 1369 MHz were obtained with the Parkes telescope.

Figure A2.(Continued.)

Averaged pulse profiles at 2368 MHz or 1369 MHz were obtained with the Parkes telescope for 16 pulsars,five of which were obtained at both frequencies.

Appendix B

Estimated Flux Densities at 2368 MHz (S2368) of 22 Pulsars and Pulse Widths at other Frequencies for 17 Pulsars

Estimated flux densities of 22 Pulsars were estimated at 2368 MHz (S2368).Pulse widths for 17 pulsars were measured previously at other frequencies.