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J/MNRAS/402/2369   Kinematics of young associations/clusters   (Tetzlaff+, 2010)

Kinematics of young associations and clusters within 3kpc from the Sun. Tetzlaff N., Neuhaeuser R., Hohle M.M., Maciejewski G. <Mon. Not. R. Astron. Soc. 402, 2369 (2010)> =2010MNRAS.402.2369T
ADC_Keywords: Associations, stellar ; Pulsars ; Space velocities ; Keywords: stars: kinematics - pulsars: individual: PSR B1929+10 - pulsars: individual: RX J1856.5-3754 - pulsars: individual: RX J0720.4-3125 - pulsars: individual: RX J1605.3+3249 - pulsars: individual: RBS 1223 Abstract: Young isolated radio-quiet neutron stars are still hot enough to be detectable at X-ray and optical wavelengths due to their thermal emission and can hence probe cooling curves. An identification of their birth sites can constrain their age. For that reason, we try to identify the parent associations for four of the so-called Magnificent Seven neutron stars for which proper motion and distance estimates are available. We are tracing back in time each neutron star and possible birth association centre to find close encounters. The associated time of the encounter expresses the kinematic age of the neutron star which can be compared to its characteristic spin-down age. Owing to observational uncertainties in the input data, we use Monte Carlo simulations and evaluate the outcome of our calculations statistically. RX J1856.5-3754 most probably originated from the Upper Scorpius association about 0.3Myr ago. RX J0720.4-3125 was either born in the young local association TW Hydrae about 0.4Myr ago or in Trumpler 10 0.5Myr in the past. Also RX J1605.3+3249 and RBS 1223 seem to come from a nearby young association such as the Scorpius-Centraurus complex or the extended Corona-Australis association. For RBS 1223 also a birth in Scutum OB2 is possible. We also give constraints on the observables as well as on the radial velocity of the neutron star. Given the birth association, its age and the flight time of the neutron star, we estimate the mass of the progenitor star. Some of the potential supernovae were located very nearby (<100pc) and thus should have contributed to the 10Be and 60Fe material found in the Earth's crust. In addition, we reinvestigate the previously suggested neutron star/runaway pair PSR B1929+10/zeta Ophiuchi and conclude that it is very likely that both objects were ejected during the same supernova event. Description: Given a distance of 1kpc and typical neutron star velocities of 100-500km/s (Arzoumanian et al. 2002ApJ...568..289A; Hobbs et al., 2005, Cat. J/MNRAS/360/974) and maximum ages of 5Myr for neutron stars to be detectable in the optical (see cooling curves in Gusakov et al. 2005MNRAS.363..555G and Popov, Grigorian & Blaschke 2006, Phys. Rev. C, 74, 025803), we restricted our search for birth associations and clusters of young nearby neutron stars to within 3kpc. We chose a sample of OB associations and young clusters (we use the term `association' for both in the following) within 3kpc from the Sun with available kinematic data and distance. We collected those from Dambis, Mel'nik & Rastorguev (2001AstL...27...58D) and Hoogerwerf (2001A&A...365...49H) and associations to which stars from the Galactic O-star catalogue from Maiz-Apellaniz et al. (2004, Cat. J/ApJS/151/103) are associated with. Furthermore, we added young local associations (YLA) from Fernandez, Figueras & Torra (2008A&A...480..735F) since they are possible hosts of a few SNe in the near past. We also included the Hercules-Lyrae association (Her-Lyr) and the Pleiades and massive star-forming regions (Reipurth 2008, ASP Monograph Publ. Vol. 4 and Vol. 5). We set the lower limit of the association age to 2Myr to account for the minimum lifetime of a progenitor star that can produce a neutron star (progenitor mass smaller than 30M see e.g. Heger et al. 2003ApJ...591..288H). The list of all explored associations and their properties can be found in Appendix A. Coordinates as well as heliocentric velocity components are given for a right-handed coordinate system with the x-axis pointing towards the galactic centre and y is positive in the direction of galactic rotation. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file assoc.dat 127 140 Positional and kinematical data for OB associations and clusters (table A1 in the paper) refs.dat 178 78 References
See also: J/AN/328/889 : Mean Radial Velocities of open clusters (Kharchenko+, 2007) J/AJ/117/354 : OB associations from Hipparcos (de Zeeuw+, 1999) Byte-by-byte Description of file: assoc.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/140] Sequential number 5- 16 A12 --- Name Name of association/cluster 17 A1 --- n_Name Note on Name (1) 19- 24 F6.2 deg GLON Galactic longitude 26- 31 F6.2 deg GLAT Galactic latitude 33- 37 F5.2 mas Plx Parallax 39- 43 F5.1 km/s UVel Heliocentric U velocity 45- 48 F4.1 km/s e_UVel ?=- Standard deviation of UVel 50- 54 F5.1 km/s VVel Heliocentric V velocity 56- 59 F4.1 km/s e_VVel ?=- Standard deviation of VVel 61- 65 F5.1 km/s WVel Heliocentric W velocity 67- 70 F4.1 km/s e_WVel ?=- Standard deviation of WVel 72 A1 --- l_Age Limit flag on Age 73- 77 F5.1 Myr Age Association/cluster age (or lower value if interval) from the literature 78 A1 --- --- [-] 79- 83 F5.1 Myr Ageu ? Association/cluster upper interval age value from the literature 84 A1 --- n_Age [jk] Note on Age (2) 86- 88 I3 pc Ext Extension (diameter) of association/cluster from the literature 90-127 A38 --- Ref References given in refs.dat file
Note (1): Notes as follows: a = Radial velocity from Mel'nik and Efremov (1995AstL...21...10M), proper motion components derived from Humphreys (1978ApJS...38..309H) members as median ± average deviation from median b = Proper motion components and radial velocity derived from Westerlund (1963MNRAS.127...71W) members as median ± average deviation from median c = Coordinates and parallax denote the mean of Cas-Tau members given by de Zeeuw et al. (1999AJ....117..354D), velocity components reflect their median U, V, W d = Proper motion components and radial velocity derived from Carpenter and Hodapp (2008, "The Monoceros R2 Molecular Cloud" p. 899) members as median ± average deviation from median e = Velocity components were derived from radial velocity only f = Proper motion components and radial velocity derived from Humphreys (1978ApJS...38..309H) members as median ± average deviation from median g = Proper motion components and radial velocity derived from Whittet et al. (1997A&A...327.1194W) members as median ± average deviation from median h = Radial velocity derived from WEBDA members as median ± average deviation from median. i = Proper motion components and radial velocity derived from Mas01 members; proper motion (2 stars): mean proper motion maximum deviation, radial velocity: for only one star available (without deviation). Note (2): Notes on Age as follows: j = We derived ages from HR diagrams from memberlists either from Humphreys (1978ApJS...38..309H) or Garmany and Stencel (1992A&AS...94..211G) (Morgan et al. (1953ApJ...118..318M) for Cyg OB4, Graham (1971AJ.....76.1079G) for Mon OB3) by fitting a set of theoretical Padova isochrones (Girardi et al., 2002A&A...391..195G) assuming solar metallicity. The fitting algorithm is based on the least-squares method and uses stellar magnitudes as weights k = Ori OB1a: 11Myr, Ori OB1b: 2Myr, Ori OB1c: 5-11Myr, Ori OB1d (Trapezium cluster): ∼1Myr
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 6 A6 --- Ref Reference code 8- 26 A19 --- BibCode BibCode 28- 48 A21 --- Aut Author's name 50-178 A129 --- Com Comments
Acknowledgements: Nina Tetzlaff, nina(at) References: Fernandez et al., 2008A&A...480..735F Dambis et al., 2001AstL...27...58D
(End) Nina Tetzlaff [AIU Jena], Patricia Vannier [CDS] 09-Mar-2010
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