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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 (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) 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) 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:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 122 57 Analysis of the Brightest Serendipitous Sources in the XMM-Newton FOV
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
Bytes Format Units Label Explanations
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)
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.
History: From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 01-Feb-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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