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J/ApJ/711/138     Spectral analysis of HIP 60350 and 18 Peg     (Irrgang+, 2010)

The nature of the hyper-runaway candidate HIP 60350. Irrgang A., Przybilla N., Heber U., Nieva M. F., Schuh S. <Astrophys. J., 711, 138-143 (2010)> =2010ApJ...711..138I
ADC_Keywords: Abundances ; Stars, B-type ; Spectroscopy Keywords: stars: abundances - stars: atmospheres - stars: distances - stars: early-type - stars: individual (HIP 60350, 18 Peg) - stars: kinematics and dynamics Abstract: Young, massive stars in the Galactic halo are widely supposed to be the result of an ejection event from the Galactic disk forcing some stars to leave their place of birth as so-called runaway stars. Here, we present a detailed spectroscopic and kinematic analysis of the runaway B star HIP 60350 to determine which runaway scenario -a supernova explosion disrupting a binary system or dynamical interaction in star clusters- may be responsible for HIP 60350's peculiar orbit. Based on a non-local thermodynamic equilibrium approach, a high-resolution optical echelle spectrum was examined to revise spectroscopic quantities and for the first time to perform a differential chemical abundance analysis with respect to the B-type star 18 Peg. The results together with proper motions from the Hipparcos Catalog further allowed the three-dimensional kinematics of the star to be studied numerically. The abundances derived for HIP 60350 are consistent with a slightly supersolar metallicity agreeing with the kinematically predicted place of birth ∼6kpc away from the Galactic center. However, they do not exclude the possibility of an α-enhanced abundance pattern expected in the case of the supernova scenario. Its outstanding high Galactic rest-frame velocity of 530±35km/s is a consequence of ejection in the direction of Galactic rotation and slightly exceeds the local Galactic escape velocity in a standard Galactic potential. Hence, HIP 60350 may be unbound to the Galaxy. Description: HIP 60350 was observed in 2008 December with the high-resolution echelle spectrograph of the 9.2m Hobby-Eberly Telescope (HET) at the McDonald Observatory in wavelength range [3900Å,7870Å]. Three intermediate-resolution spectra taken in 2009 May and July with the 3.5m telescope at Calar Alto, Spain, enlarging the spectral coverage down to 3500Å. We also carried out an abundance analysis of the normal Population I B-type star 18 Peg. We used the fibre optics Cassegrain echelle spectrograph (FOCES) on the 2.2m telescope at Calar Alto, Spain, to obtain a high-resolution, high-S/N spectrum (S/N∼400 in the blue) of 18 Peg. Objects: ------------------------------------------------------ RA (2000) DE Designation(s) ------------------------------------------------------ 12 22 29.61 +40 49 35.6 HIP 60350 = TYC 3018-248-1 22 00 07.93 +06 43 02.8 * 18 Peg = TYC 564-1847-1 ------------------------------------------------------ File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 68 167 Spectral line analysis of HIP 60350 and 18 Peg
See also: V/136 : Teff and metallicities for Tycho-2 stars (Ammons+, 2006) J/A+A/539/A143 : Nearby B-stars stellar parameters and abundances (Nieva+, 2012) J/MNRAS/410/190 : Young runaway stars within 3kpc (Tetzlaff+, 2011) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 5 A5 --- Ion Ion species 7- 10 F4.2 [-] <HIP> ? Averaged HIP 60350 abundance; log(X/H)+12 12- 15 F4.2 [-] e_<HIP> ? Uncertainty in <HIP> 17- 20 F4.2 [-] <Peg> ? Averaged 18 Peg abundance; log(X/H)+12 22- 25 F4.2 [-] e_<Peg> ? Uncertainty in <Peg> 27- 33 F7.2 0.1nm lambda Wavelength; Angstroms 35- 39 F5.2 eV ExPot Excitation potential 41- 46 F6.3 [-] log(gf) Log of oscillator strength 48- 49 A2 --- Acc Accuracy indicator (1) 51- 58 A8 --- Ref Reference(s) (2) 60- 63 F4.2 [-] HIP ? HIP 60350 abundance from the line; log(X/H)+12 65- 68 F4.2 [-] Peg The 18 Peg abundance from the line; log(X/H)+12
Note (1): Uncertainties are coded as: A = 3%; B = 10%; C = 25%; D = 50%; E = larger than 50%; X = unknown. Note (2): References as follows: BB89 = Becker & Butler 1989A&A...209..244B; BMZ = Butler, Mendoza, & Zeippen 1993JPhB...26.4409B; FFT = Froese Fischer & Tachiev 2004ADNDT..87....1F; FFTI = Froese Fischer, Tachiev, & Irimia 2006ADNDT..92..607F; FMW = Fuhr, Martin, & Wiese 1988atps.book.....M; FW = Fuhr, J. R. & Wiese, W. L. 1998, CRC Handbook of Chemistry and Physics, 79th ed., ed. D. R. Lide (Boca Raton, FL: CRC Press); KB = Kurucz & Bell 1995all..book.....K; MAR = Mar et al. 2000A&AS..144..509M; MELZ = Mendoza et al. 1995JPhB...28.3485M; MERLR = Matheron et al. 2001JQSRT..69..535M; N02 = Nahar 2002ADNDT..80..205N; N86 = Nussbaumer 1986A&A...155..205N; WFD = Wiese, Fuhr, & Deters 1996atpc.book.....W; WSM = Wiese, Smith, & Miles, 1969atp..book.....W.
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 30-Mar-2012
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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