XMM-Newton and SUZAKU detection of an X-ray emitting shell around the pulsar wind nebula G54.1+0.3

F. Bocchino, R. Bandiera, Joseph (Yosi) Gelfand

Research output: Contribution to journalArticle

Abstract

Context. X-ray observations have proven to be very effective in detecting previously unknown supernova remnant shells around pulsar wind nebulae (PWNe), and in these cases the characteristics of the shell provide information about the evolutionary stage of the embedded PWN. However, it is not clear why some PWNe are "naked". Aims. We perform an X-ray observational campaign targeting the PWN G54.1+0.3, the "close cousin" of the Crab Nebula, to try to detect the associated SNR shell. Methods. We analyze XMM-Newton and Suzaku observations of G54.1+0.3 to model the contribution of a dust scattering halo. Results. We detecte an intrinsic faint diffuse X-ray emission surrounding the PWN out to ∼ 6' (∼10 pc) from the pulsar, characterized by a hard spectrum, which can be modeled with either a power law (γ = 2.9) or a thermal plasma model (kT = 2.0 keV.) Conclusions. Assuming the shell to be thermal, we derive an explosion energy E = 0.5-1.6×1051 erg, a pre-shock ISM density of 0.2 cm-3, and an age of ∼2000 yr. Using these results in the MHD model of PWN-SNR evolution, we obtain excellent agreement between the predicted and observed location of the shell and PWN shock.

Original languageEnglish (US)
Article numberA71
JournalAstronomy and Astrophysics
Volume520
Issue number10
DOIs
StatePublished - Jan 1 2010

Fingerprint

XMM-Newton telescope
nebulae
pulsars
newton
shell
shock
Crab nebula
x rays
thermal plasmas
supernova remnants
explosions
halos
dust
erg
targeting
explosion
crab
scattering
power law
detection

Keywords

  • dust, extinction
  • ISM: supernova remnants

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

XMM-Newton and SUZAKU detection of an X-ray emitting shell around the pulsar wind nebula G54.1+0.3. / Bocchino, F.; Bandiera, R.; Gelfand, Joseph (Yosi).

In: Astronomy and Astrophysics, Vol. 520, No. 10, A71, 01.01.2010.

Research output: Contribution to journalArticle

@article{27f5005e3d11496aa5c29324ebf9e04e,
title = "XMM-Newton and SUZAKU detection of an X-ray emitting shell around the pulsar wind nebula G54.1+0.3",
abstract = "Context. X-ray observations have proven to be very effective in detecting previously unknown supernova remnant shells around pulsar wind nebulae (PWNe), and in these cases the characteristics of the shell provide information about the evolutionary stage of the embedded PWN. However, it is not clear why some PWNe are {"}naked{"}. Aims. We perform an X-ray observational campaign targeting the PWN G54.1+0.3, the {"}close cousin{"} of the Crab Nebula, to try to detect the associated SNR shell. Methods. We analyze XMM-Newton and Suzaku observations of G54.1+0.3 to model the contribution of a dust scattering halo. Results. We detecte an intrinsic faint diffuse X-ray emission surrounding the PWN out to ∼ 6' (∼10 pc) from the pulsar, characterized by a hard spectrum, which can be modeled with either a power law (γ = 2.9) or a thermal plasma model (kT = 2.0 keV.) Conclusions. Assuming the shell to be thermal, we derive an explosion energy E = 0.5-1.6×1051 erg, a pre-shock ISM density of 0.2 cm-3, and an age of ∼2000 yr. Using these results in the MHD model of PWN-SNR evolution, we obtain excellent agreement between the predicted and observed location of the shell and PWN shock.",
keywords = "dust, extinction, ISM: supernova remnants",
author = "F. Bocchino and R. Bandiera and Gelfand, {Joseph (Yosi)}",
year = "2010",
month = "1",
day = "1",
doi = "10.1051/0004-6361/201014298",
language = "English (US)",
volume = "520",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",
number = "10",

}

TY - JOUR

T1 - XMM-Newton and SUZAKU detection of an X-ray emitting shell around the pulsar wind nebula G54.1+0.3

AU - Bocchino, F.

AU - Bandiera, R.

AU - Gelfand, Joseph (Yosi)

PY - 2010/1/1

Y1 - 2010/1/1

N2 - Context. X-ray observations have proven to be very effective in detecting previously unknown supernova remnant shells around pulsar wind nebulae (PWNe), and in these cases the characteristics of the shell provide information about the evolutionary stage of the embedded PWN. However, it is not clear why some PWNe are "naked". Aims. We perform an X-ray observational campaign targeting the PWN G54.1+0.3, the "close cousin" of the Crab Nebula, to try to detect the associated SNR shell. Methods. We analyze XMM-Newton and Suzaku observations of G54.1+0.3 to model the contribution of a dust scattering halo. Results. We detecte an intrinsic faint diffuse X-ray emission surrounding the PWN out to ∼ 6' (∼10 pc) from the pulsar, characterized by a hard spectrum, which can be modeled with either a power law (γ = 2.9) or a thermal plasma model (kT = 2.0 keV.) Conclusions. Assuming the shell to be thermal, we derive an explosion energy E = 0.5-1.6×1051 erg, a pre-shock ISM density of 0.2 cm-3, and an age of ∼2000 yr. Using these results in the MHD model of PWN-SNR evolution, we obtain excellent agreement between the predicted and observed location of the shell and PWN shock.

AB - Context. X-ray observations have proven to be very effective in detecting previously unknown supernova remnant shells around pulsar wind nebulae (PWNe), and in these cases the characteristics of the shell provide information about the evolutionary stage of the embedded PWN. However, it is not clear why some PWNe are "naked". Aims. We perform an X-ray observational campaign targeting the PWN G54.1+0.3, the "close cousin" of the Crab Nebula, to try to detect the associated SNR shell. Methods. We analyze XMM-Newton and Suzaku observations of G54.1+0.3 to model the contribution of a dust scattering halo. Results. We detecte an intrinsic faint diffuse X-ray emission surrounding the PWN out to ∼ 6' (∼10 pc) from the pulsar, characterized by a hard spectrum, which can be modeled with either a power law (γ = 2.9) or a thermal plasma model (kT = 2.0 keV.) Conclusions. Assuming the shell to be thermal, we derive an explosion energy E = 0.5-1.6×1051 erg, a pre-shock ISM density of 0.2 cm-3, and an age of ∼2000 yr. Using these results in the MHD model of PWN-SNR evolution, we obtain excellent agreement between the predicted and observed location of the shell and PWN shock.

KW - dust, extinction

KW - ISM: supernova remnants

UR - http://www.scopus.com/inward/record.url?scp=77957721008&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=77957721008&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201014298

DO - 10.1051/0004-6361/201014298

M3 - Article

VL - 520

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

IS - 10

M1 - A71

ER -