The Parkes multibeam pulsar survey – IV. Discovery of 180 pulsars and parameters for 281 previously known pulsars

By G. Hobbs, Andrew Faulkner, Ingrid Stairs, F. Camilo, R. Manchester, Andrew G. Lyne, Michael Kramer, N. D'Amico, Victoria Kaspi, A. Possenti and 5 more. 2004

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The Parkes multibeam pulsar survey has led to the discovery of more than 700 pulsars. In this paper, we provide timing solutions, flux densities and pulse profiles for 180 of these new discoveries. Two pulsars, PSRs J1736−2843 and J1847−0130, have rotational periods P > 6 s and are therefore among the slowest rotating radio pulsars known. Conversely, with P = 1.8 ms, PSR J1843−1113 has the third-shortest period of pulsars currently known. This pulsar and PSR J1905+0400 (P = 3.8 ms) are both solitary. We also provide orbital parameters for a new binary system, PSR J1420−5625, which has P = 34 ms, an orbital period of 40 d and a minimum companion mass of 0.4 solar masses. The 10 ◦ -wide strip along the Galactic plane that was surveyed is known to contain 264 radio pulsars that were discovered prior to the multibeam pulsar survey. We have redetected almost all of these pulsars and provide new dispersion measure values and flux densities at 20 cm for the redetected pulsars.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/7560d09019c71381cd178e864413dcab961a497f

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Citations in the corpus

Spectral properties of 441 radio pulsars (2017, background): “23 are from Hobbs et al. (2004), four from Lorimer et al. (2006), two from Kramer et al. (2003) and one from Manchester et al. (2001), and all are based on the same flux density estimation method.”
Avalanche Dynamics of Radio Pulsar Glitches (2007, unknown): “…(11) Hobbs et al. 2004a; (12) Downs 1981; (13) Wang et al. 2000; (14) Dodson et al. 2002; (15) Dodson et al. 2004; (16) Flanagan & Buchner 2006; (17) Hobbs et al. 2004b; (18) Camilo et al. 2000; (19) Camilo et al. 2004; (20) Torii et al. 2000; (21) Kaspi et al. 2000; (22) Kaspi & Gavriil 2003;…”
Pulsar nulling and mode changing (2007, unknown): “PSR J1812−1718 (B1809−173) The mean pulse profile for this pulsar is dominated by a narrow leading component of 50% width 19 ms or 0.015 periods (Hobbs et al. 2004).”
Pulsar Rotation Measures and the Large-Scale Structure of the Galactic Magnetic Field (2006, background): “…survey has discovered a large number of low-latitude and relatively distant pulsars (Manchester et al. 2001; Morris et al. 2002; Kramer et al. 2003; Hobbs et al. 2004), providing a unique opportunity to probe the diffuse magnetic field in a substantial fraction of the Galactic disk with much…”
Arecibo Pulsar Survey Using ALFA. I. Survey Strategy and First Discoveries (2005, background): “The Parkes multibeam (PMB) pulsar survey of the Galactic plane (Manchester et al. 2001; Morris et al. 2002; Kramer et al. 2003; Hobbs et al. 2004; Faulkner et al. 2004) has been extremely prolific, yielding over 700 new pulsars in the past seven years.”
The Parkes Multibeam Pulsar Survey - VI. Discovery and timing of 142 pulsars and a Galactic population analysis (2006, methodology): “Hobbs et al. (2004) discussed the detection of previously known pulsars in the survey.”
Discovery of Luminous Pulsed Hard X-Ray Emission from Anomalous X-Ray Pulsars 1RXS J1708–4009, 4U 0142+61, and 1E 2259+586 by INTEGRAL and RXTE (2006, background): “…found for AXPs, thus also with high magnetic field strengths, were found: PSR J1847 0130, which has the highest by far inferred surface dipolar magnetic field (B ¼ 9:4 ; 1013 G) among all known radio pulsars (McLaughlin et al. 2003), and PSR J1718 3718 (Hobbs et al. 2004; Kaspi & McLaughlin 2005).”
The Parkes Multibeam Pulsar Survey - V. Finding binary and millisecond pulsars (2004, background): “As has been reported in Hobbs et al. (2004), of the 264 pulsars in the survey area discovered by other surveys, all but eleven have been re-detected with no unaccountable non-detections.”
Formation of millisecond pulsars with CO white dwarf companions – II. Accretion, spin-up, true ages and comparison to MSPs with He white dwarf companions (2012, methodology): “In Table 2 we list all binary radio pulsars with CO WD (or ONeMg WD) companions – see also Hobbs et al. (2004).”
The International Pulsar Timing Array: First Data Release (2016, unknown): “…are as follows: (1) Lommen et al. (2000), (2) Abdo et al. (2009), (3) Lommen et al. (2006), (4) Bailes et al. (1994), (5) Abdo et al. (2010), (6) Hobbs et al. (2004b), (7) Toscano et al. (1998), (8) Navarro et al. (1995), (9) Kramer et al. (1998), (10) Du et al. (2014), (11) Verbiest & Lorimer…”