Flux density measurements for 32 pulsars in the 20 cm observing band
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摘要
Flux densities are fundamental observational parameters that describe a pulsar. In the current pulsar catalogue, 27% of the listed radio pulsars have no flux density measurement in the 20 cm observing band. Here, we present the first such measurements for 32 pulsars observed employing the Parkes radio telescope. We have used both archival and new observations to make these measurements. Various schemes exist for measuring flux densities and we show how the measured flux densities vary between these methods and how the presence of radio-frequency interference will bias the flux density measurements.
Flux densities are fundamental observational parameters that describe a pulsar. In the current pulsar catalogue, 27% of the listed radio pulsars have no flux density measurement in the 20 cm observing band. Here, we present the first such measurements for 32 pulsars observed employing the Parkes radio telescope. We have used both archival and new observations to make these measurements. Various schemes exist for measuring flux densities and we show how the measured flux densities vary between these methods and how the presence of radio-frequency interference will bias the flux density measurements.
Flux densities are fundamental observational parameters that describe a pulsar. In the current pulsar catalogue, 27% of the listed radio pulsars have no flux density measurement in the 20 cm observing band. Here, we present the first such measurements for 32 pulsars observed employing the Parkes radio telescope. We have used both archival and new observations to make these measurements. Various schemes exist for measuring flux densities and we show how the measured flux densities vary between these methods and how the presence of radio-frequency interference will bias the flux density measurements.
引文
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Patra,A.,Bates,J.E.,Sun,J.,&Perdew,J.P.2017,Proceedings of the National Academy of Science,114,E9188
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1https://doi.org/10.4225/08/5ab2e8014512d
2Note that there is no evidence for any correlation between the measured flux density and the pointing position of the telescope during the flux calibration method.
3In a few cases, the flux densities are smaller without manual RFI flagging. This is because some of the actual pulsed signal was removed during the flagging process.
Hobbs,G.,Miller,D.,Manchester,R.N.,et al.2011,PASA,28,202
Hotan,A.W.,Bailes,M.,&Ord,S.M.2004a,MNRAS,355,941
Hotan,A.W.,van Straten,W.,&Manchester,R.N.2004b,PASA,21,302
Jankowski,F.,van Straten,W.,Keane,E.F.,et al.2018,MNRAS,473,4436
Johnston,S.,&Kerr,M.2018,MNRAS,474,4629
Keith,M.J.,Coles,W.,Shannon,R.M.,et al.2013,MNRAS,429,2161
Kerr,M.,Coles,W.A.,Ward,C.A.,et al.2018,MNRAS,474,4637
Kijak,J.,Basu,R.,Lewandowski,W.,Ro˙zko,K.,&Dembska,M.2017,Ap J,840,108
Kuehr,H.,Witzel,A.,Pauliny-Toth,I.I.K.,&Nauber,U.1981,A&AS,45,367
Lane,W.M.,Clarke,T.E.,Taylor,G.B.,Perley,R.A.,&Kassim,N.E.2004,AJ,127,48
Levin,L.,Mc Laughlin,M.A.,Jones,G.,et al.2016,Ap J,818,166
Manchester,R.N.,Hobbs,G.B.,Teoh,A.,&Hobbs,M.2005,Vizie R Online Data Catalog,7245
Manchester,R.N.,Lyne,A.G.,Camilo,F.,et al.2001,MNRAS,328,17
Manchester,R.N.,Hobbs,G.,Bailes,M.,et al.2013,PASA,30,017
Patra,A.,Bates,J.E.,Sun,J.,&Perdew,J.P.2017,Proceedings of the National Academy of Science,114,E9188
Shannon,R.M.,Lentati,L.T.,Kerr,M.,et al.2016,Ap J,828,L1
Staveley-Smith,L.,Wilson,W.E.,Bird,T.S.,et al.1996,PASA,13,243
Stovall,K.,Lynch,R.S.,Ransom,S.M.,et al.2014,Ap J,791,67
You,X.P.,Manchester,R.N.,Coles,W.A.,Hobbs,G.B.,&Shannon,R.2018,Ap J,867,22
1https://doi.org/10.4225/08/5ab2e8014512d
2Note that there is no evidence for any correlation between the measured flux density and the pointing position of the telescope during the flux calibration method.
3In a few cases, the flux densities are smaller without manual RFI flagging. This is because some of the actual pulsed signal was removed during the flagging process.