2005A&A...429..257M


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.02CEST15:07:41

2005A&A...429..257M - Astronomy and Astrophysics, volume 429, 257-265 (2005/1-1)

The proper motion of the isolated neutron star RX J1605.3+3249.

MOTCH C., SEKIGUCHI K., HABERL F., ZAVLIN V.E., SCHWOPE A. and PAKULL M.W.

Abstract (from CDS):

We obtained deep optical imaging of the thermally emitting X-ray bright and radio-quiet isolated neutron star RX J1605.3+3249 with the Subaru telescope in 1999 and 2003. Together with archival HST images acquired in 2001 these data reveal a proper motion of µ=144.5±13.2mas/yr. This implies a relatively high spatial velocity and indicates that the star is unlikely to be re-heated by accretion of matter from the interstellar medium. Assuming that RX J1605.3+3249 is a young (105-106yr) cooling neutron star, its apparent trajectory is consistent with a birth in the nearby Sco OB2 OB association at a location close to that derived for RX J1856.5-3754 and perhaps also to that of RX J0720.4-3125. This suggests that the X-ray bright part of ROSAT-discovered isolated neutron stars is dominated by the production of the Sco OB2 complex which is the closest OB association and a part of the Gould belt. The B and R magnitudes of the faint optical counterpart did not vary from 1999 to 2003 at B=27.22±0.10. Its B-R colour index of +0.32±0.17 is significantly redder than that of other isolated neutron stars and the optical flux lies a factor 11.5 above the extrapolation of the X-ray blackbody-like spectrum. The red optical colour reveals the presence of an additional emitting component in the optical regime over the main neutron star thermal emission. We also discovered a small elongated Hα nebula approximately centered on the neutron star and aligned with the direction of motion. The width of the nebula is unresolved and smaller than ∼0.4'' for a length of about 1''. The shape of the Balmer emitting nebula around RX J1605.3+3249 is very different from those seen close to other neutron stars and should be confirmed by follow-up observations. We shortly discuss the possible mechanisms which could give rise to such a geometry.

Abstract Copyright:

Journal keyword(s): stars: pulsars: individual: RX J1605.3+3249 - stars: neutron

Simbad objects: 15

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Number of rows : 15

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 V* CM Tau Psr 05 34 31.93830 +22 00 52.1758           ~ 4803 1
2 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5593 4
3 NAME Ori I As* 05 38 -02.8           ~ 558 0
4 PSR B0656+14 Psr 06 59 48.183 +14 14 21.54   24.85 24.90     ~ 758 1
5 RX J0720.4-3125 N* 07 20 24.961 -31 25 50.21   26.1   27.0   ~ 281 0
6 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545           ~ 2056 1
7 RX J1605.3+3249 N*? 16 05 18.9 +32 49 07     26.8     ~ 89 1
8 NAME ASSOC II SCO As* 16 15 -24.2           ~ 1119 1
9 SA 110-504 * 18 43 11.7109273137 +00 30 04.545110058 16.593 15.28 14.00 13.61 12.540 ~ 9 0
10 RX J1856.6-3754 N* 18 56 35.11 -37 54 30.5     25.7     ~ 388 0
11 PSR B1929+10 Psr 19 32 13.79 +10 59 33.2           ~ 693 0
12 PSR B2223+65 Psr 22 25 52.36 +65 35 33.8           ~ 286 0
13 NAME Cen-Crux As* ~ ~           ~ 24 0
14 [MHZ99] C * ~ ~           M 2 1
15 NAME Gould Belt PoG ~ ~           ~ 711 1

    Equat.    Gal    SGal    Ecl

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2020.07.02-15:07:41

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