J/ApJ/819/40 XMM-Newton brightest serendipitous sources (Marelli+, 2016)
The tale of the two tails of the oldish PSR J2055+2539.
Marelli M., Pizzocaro D., De Luca A., Gastaldello F., Caraveo P.,
Parkinson P.S.
<Astrophys. J., 819, 40 (2016)>
=2016ApJ...819...40M 2016ApJ...819...40M (SIMBAD/NED BibCode)
ADC_Keywords: Pulsars ; X-ray sources ; Nebulae
Keywords: galaxies: clusters: individual: XMMU J205536.7+253750 -
pulsars: general - pulsars: individual: PSR J2055+2539 -
stars: neutron
Abstract:
We analyzed a deep XMM-Newton observation of the radio-quiet
γ-ray PSR J2055+2539. The spectrum of the X-ray counterpart is
nonthermal, with a photon index of Γ=2.36±0.14 (1σ
confidence). We detected X-ray pulsations with a pulsed fraction of
25%±3% and a sinusoidal shape. Taking into account considerations on
the γ-ray efficiency of the pulsar and on its X-ray spectrum, we
can infer a pulsar distance ranging from 450 to 750 pc. We found two
different nebular features associated with PSR J2055+2539 and
protruding from it. The angle between the two nebular main axes is
∼162.8°±0.7°. The main, brighter feature is 12' long and
<20" thick, characterized by an asymmetry with respect to the main
axis that evolves with the distance from the pulsar, possibly forming
a helical pattern. The secondary feature is 250"x30". Both nebulae
present an almost flat brightness profile with a sudden decrease at
the end. The nebulae can be fitted by either a power-law model or a
thermal bremsstrahlung model. A plausible interpretation of the
brighter nebula is in terms of a collimated ballistic jet. The
secondary nebula is most likely a classical synchrotron-emitting tail.
Description:
Our deep XMM-Newton observation of PSR J2055+2539, lasting 136.2 ks, was
performed on 2013 May 1 (ObsID 0724090101). The PN camera (Struder et al.
2001AJ....121.1413P 2001AJ....121.1413P) of the EPIC instrument was operating in Large Window
mode, with a time resolution of 47.7 ms on a 27'x13' field of view (FOV).
The high time resolution, combined with the large FOV, allows for both
the timing analysis of the J2055 pulsar and the spatial analysis of
the nebular structures. The Metal Oxide Semiconductor (MOS) detectors
(Turner et al. 2001A&A...365L..27T 2001A&A...365L..27T) were set in full-frame mode (2.6 s
time resolution on a 15' radius FOV). The thin optical filter was used
for both PN and MOSs. We also analyzed XMM-Newton observations
0605470401 and 0605470901, taken on 2009 October 26 and on 2010 April
21, and lasting 24.5 and 17.9 ks, respectively.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 122 57 Analysis of the Brightest Serendipitous Sources
in the XMM-Newton FOV
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See also:
IX/50 : XMM-Newton Serendipitous Source Catalogue 3XMM-DR6
(XMM-SSC, 2016)
J/A+A/428/383 : XMM-Newton Bright Serendipitous Survey (Della Ceca+, 2004)
J/A+A/493/339 : XMM-Newton serendipitous Survey. V. (Watson+, 2009)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Source [1/61] Source number
4- 12 F9.5 deg RAdeg Right Ascension in decimal degrees
(J2000) (1)
14- 22 F9.6 deg DEdeg Declination in decimal degrees (J2000)
(1)
24- 37 A14 --- Model Statistically acceptable spectral
model(s) fit
39 A1 --- l_NH [<] Limit flag on NH
40- 45 A6 10+21cm-2 NH Hydrogen column density
47- 52 F6.3 10+21cm-2 E_NH ? Upper 1σ limit uncertainty in NH
54- 59 F6.3 10+21cm-2 e_NH ? Lower 1σ limit uncertainty in NH
61 A1 --- l_NH1 [<] Limit flag on NH1
62- 66 F5.3 10+21cm-2 NH1 ? Hydrogen column density for the other
fitting model
68- 72 F5.3 10+21cm-2 E_NH1 ? Upper 1σ limit uncertainty
in NH1
74- 78 F5.3 10+21cm-2 e_NH1 ? Lower 1σ limit uncertainty
in NH1
80 A1 --- l_logFX/Fopt [>] Limit flag on logFX/Fopt
81- 89 F9.6 [-] logFX/Fopt ? X-ray-to-optical flux ratio
90 A1 --- u_logFX/Fopt [?] Uncertainty flag on logFX/Fopt
92- 96 F5.3 [-] logFX/Fopt2 ? Second value of logFX/Fopt
98- 99 A2 --- n_logFX/Fopt [B V V*] Note on logFX/Fopt (2)
101 A1 --- l_logFX/Fopt1 [>] Limit flag on logFX/Fopt1
102-108 F7.4 [-] logFX/Fopt1 ? X-ray-to-optical flux ratio for
the other fitting model
110-111 A2 --- n_logFX/Fopt1 [B V V*] Note on logFX/Fopt1 (2)
113-120 A8 --- ID Resulting identification of the source
122 A1 --- n_ID [b] Note on ID (3)
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Note (1): Typical XMM-Newton positional errors are 3".
Note (2): Note as follows:
V = Where present, we used the V-band optical flux;
B = If not detected, we used the B-band optical flux;
V* = In case of an R-band detection, we obtained the V-band flux (see
Appendix A).
Note (3): Note as follows:
b = Identification of this source is based on optical and hardness ratio
tests.
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History:
From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 01-Feb-2018