2004
DOI: 10.1051/0004-6361:20040440
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The isolated neutron star X-ray pulsars RX J0420.0–5022 and RX J0806.4–4123: New X-ray and optical observations

Abstract: Abstract.We report on the analysis of new X-ray data obtained with XMM-Newton and Chandra from two ROSAT-discovered X-ray dim isolated neutron stars (XDINs). RX J0806.4−4123 was observed with XMM-Newton in April 2003, 2.5 years after the first observation. The EPIC-pn data confirm that this object is an X-ray pulsar with 11.371 s neutron star spin period. The X-ray spectrum is consistent with absorbed black-body emission with a temperature kT = 96 eV and N H = 4 × 10 19 cm −2 without significant changes betwee… Show more

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Cited by 86 publications
(113 citation statements)
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“…The first optical observations of the field performed with the New Technology Telescope (NTT) soon after the discovery of the X-ray source (Haberl et al 1999) did not reveal any candidate counterpart brighter than B ∼ 25.2 and R ∼ 25.2. More recently, thanks to the updated Chandra position, a possible optical identification was proposed by Haberl et al (2004b) with a faint object (B = 26.6 ± 0.3, V ≥ 25.5) tentatively detected in archival Very Large Telescope (VLT) images. However, the identification has not been confirmed so far.…”
Section: Introductionmentioning
confidence: 99%
See 1 more Smart Citation
“…The first optical observations of the field performed with the New Technology Telescope (NTT) soon after the discovery of the X-ray source (Haberl et al 1999) did not reveal any candidate counterpart brighter than B ∼ 25.2 and R ∼ 25.2. More recently, thanks to the updated Chandra position, a possible optical identification was proposed by Haberl et al (2004b) with a faint object (B = 26.6 ± 0.3, V ≥ 25.5) tentatively detected in archival Very Large Telescope (VLT) images. However, the identification has not been confirmed so far.…”
Section: Introductionmentioning
confidence: 99%
“…In this paper we re-analyze the original VLT observations of RX J0420.0−5022 presented by Haberl et al (2004b) and we report follow-up, longer optical observations of the candidate counterpart, performed by our team with the VLT. Observations and data analysis are described in Sect.…”
Section: Introductionmentioning
confidence: 99%
“…With 230 eV and 460 eV the line energies are a factor of two apart. Also, in the case of RX J0806.4-4123 a simple absorbed blackbody model yields an unacceptable fit to the EPIC-pn spectra (Haberl et al 2004a). A model with one line results in χ 2 red = 1.39 which is formally acceptable.…”
mentioning
confidence: 98%
“…For example, while for most radio pulsars the optical and near IR flux is thought to be dominated by magnetospheric emission, several middle-aged pulsars (PSR B0656+14, PSR B0950+08 and Geminga) also exhibit a surface optical component (e.g., Mignani, de Luca & Caraveo 2004;Kargaltsev et al 2005, Mignani et al 2006. The optical emission detected in several thermally emitting, isolated neutron stars mostly likely has a surface origin (e.g., Kaplan et al 2003;Haberl et al 2004;Haberl 2005;van KerKwijk & Kaplan 2006). Finally, the optical/IR emission detected from a number of magnetars may originate from a hot corona near the stellar surface (Beloborodov & Thompson 2006).…”
Section: Introductionmentioning
confidence: 99%