Revisiting the radial distribution of pulsars in the Galaxy

By I. Yusifov, I. Küçük. 2004

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The high sensitivity Parkes and Swinburne Multibeam pulsar surveys have nearly doubled the number of known pul- sars and revealed many more distant pulsars with high dispersion measures. These data allow us to investigate in more detail the statistical parameters and distribution of pulsars, especially in the central regions of the Galaxy, which was almost impossible in previous low-frequency and less-sensitive surveys. To estimate the distances to pulsars we used the new NE2001 Galactic elec- tron density model. We study the Galactic distribution of normal pulsars with 1400 MHz luminosities greater than 0.1 mJy kpc 2 refining the shape and parameters of the radial distribution of pulsars. The maximum galactocentric distribution of pulsars is located at 3.2 ± 0.4 kpc and the scale-length of this distribution is 3.8 ± 0.4 kpc for the assumed distances to the Galactic center R� = 8.5 kpc. The surface density of pulsars near the Galactic center is equal to or slightly higher than that in the solar neighborhood. For observable normal pulsars with luminosities ≥0.1 mJy kpc 2 , we also re-estimate their local surface density and birth-rate: 41 ± 5 pulsars kpc −2 and 4.1 ± 0.5 pulsars kpc −2 Myr −1 respectively. For the total number of potentially observable pulsars in the Galaxy, we obtain (24 ± 3) × 10 3 and (240 ± 30) × 10 3 before and after applying beaming correction according the Tauris & Manchester (1998) beaming model. Within the limits of errors of estimations these results are in close agreement with the results of the previous studies of Lyne et al. (1998) (hereafter LML98). The dependence of these results on the NE2001 model and recommendations for further improvement of electron density distribution are discussed.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/36464c2853cfcae268ae2157dc619451e74a26fb

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Citations in the corpus

The Fermi Galactic Center GeV Excess and Implications for Dark Matter (2017, methodology): “We have used different CR source distributions: an alternative pulsar distribution (Yusifov & Küçük 2004, hereafter referred to as Yusifov), the distribution of SNRs73 (Case & Bhattacharya 1998), and the distribution of OB stars(Bronfman et al. 2000).”
The Parkes Multibeam Pulsar Survey - VI. Discovery and timing of 142 pulsars and a Galactic population analysis (2006, background): “…of a larger number of pulsars in 1.4-GHz surveys there has been a growing body of evidence which suggests a deficit of pulsars in the inner Galaxy relative to a simple model where the radial density profile follows a Gaussian distribution (Johnston 1994; Lorimer 2004; Yusifov & Küçük 2004).”
Galactic electrons and positrons at the Earth: new estimate of the primary and secondary fluxes (2010, unknown): “Lorimer (2004), hereafter L04, found (2.35, 1.528 kpc); Yusifov & Küçük (2004), hereafter YK04, derived (4, 1.25 kpc); while Paczynski (1990), hereafter P90, early determined (1, 4.5 kpc).”
DEVELOPMENT OF THE MODEL OF GALACTIC INTERSTELLAR EMISSION FOR STANDARD POINT-SOURCE ANALYSIS OF FERMI LARGE AREA TELESCOPE DATA (2016, methodology): “This model features a radial distribution of CR sources proportional to the distribution of pulsars in the Galaxy given by Yusifov & Küçük (2004), a Galactic halo size and radial boundary equal to 6 kpc and 30 kpc, respectively, and the representative diffusive reacceleration model described in…”
Background model systematics for the Fermi GeV excess (2014, background): “[114] (“PlsY ” option) and iv) the distribution of OB stars as described in ref.”
CHIME/FRB Discovery of Eight New Repeating Fast Radio Burst Sources (2019, background): “…from the central region of the Milky Way and can be modelled as peaking at galactocentric radius ∼3 kpc and falling off at larger radii (e.g., Yusifov & Küçük 2004; Faucher-Giguère & Kaspi 2006), and young pulsars and magnetars are concentrated heavily in the Galactic disk, with scale…”
Cosmic-ray propagation with DRAGON2: I. numerical solver and astrophysical ingredients (2016, methodology): “1 Source profile For the axisymmetric CR source distribution, we adopt the parametrisation suggested by the authors in [116] to model the radial distribution of the pulsar progenitors in the Milky Way, and described by the following function:”
FERMI-LAT OBSERVATIONS OF HIGH-ENERGY γ-RAY EMISSION TOWARD THE GALACTIC CENTER (2015, background): “The Yusifov & Küçük (2004) pulsar distribution (“Pulsars”) and the distribution of OB-stars (“OBstars”; Bronfman et al. 2000) encapsulate this because they represent reasonable extremes for the Galactocentric radial dependence.”
The High Time Resolution Universe Pulsar Survey - I. System configuration and initial discoveries (2010, background): “• An exponential function for the height above the Galactic plane, with scale 0.33 kpc. • The radial distribution of Yusifov & Küçük (2004).”