J/ApJ/723/658 Abundances of the halo PN BoBn 1 (Otsuka+, 2010)
The origin and evolution of the halo PN BoBn 1: from a viewpoint of chemical
abundances based on multiwavelength spectra.
Otsuka M., Tajitsu A., Hyung S., Izumiura H.
<Astrophys. J., 723, 658-683 (2010)>
=2010ApJ...723..658O 2010ApJ...723..658O
ADC_Keywords: Planetary nebulae ; Abundances ; Spectroscopy
Keywords: dust, extinction - ISM: abundances -
planetary nebulae: individual (BoBn 1, K 648) - stars: Population II
Abstract:
We have performed a comprehensive chemical abundance analysis of the
extremely metal-poor ([Ar/H]←2) halo planetary nebula (PN) BoBn 1
based on International Ultraviolet Explorer archive data,
Subaru/High-Dispersion Spectrograph spectra, VLT/UVES archive data,
and Spitzer/IRS spectra. We have detected over 600 lines in total and
calculated ionic and elemental abundances of 13 elements using
detected optical recombination lines (ORLs) and collisionally excited
lines (CELs). The estimations of C, N, O, and Ne abundances from the
ORLs and Kr, Xe, and Ba from the CELs are done the first for this
nebula, empirically and theoretically. We have detected five fluorine
and several slow neutron capture elements (the s-process). The amounts
of [F/H], [Kr/H], and [Xe/H] suggest that BoBn 1 is the most F-rich
among F-detected PNe and is a heavy s-process element rich PN. We have
confirmed dust in the nebula that is composed of amorphous carbon and
polycyclic aromatic hydrocarbons with a total mass of
5.8x10-6M☉. The photoionization models built with non-LTE
theoretical stellar atmospheres indicate that the progenitor was a
1-1.5M☉ star that would evolve into a white dwarf with an
∼0.62M☉ core mass and ∼0.09M☉ ionized nebula. We have
measured a heliocentric radial velocity of +191.6±1.3km/s and
expansion velocity 2Vexp of 40.5±3.3km/s from an average over
300 lines.
Description:
The spectra of BoBn 1 were taken using the High-Dispersion
Spectrograph (HDS) attached to one of the two Nasmyth foci of the 8.2m
Subaru telescope atop Mauna Kea, Hawaii on 2008 October 6 (program ID:
S08B-110, PI: M. Otsuka). The full width at half-maximum (FWHM) of the
image is ∼1". Spectra were taken for two wavelength ranges,
3600-5400Å (hereafter, the blue region spectra) and 4600-7500Å
(the red region spectra).
We also used archival high-dispersion spectra of BoBn 1, which are
available from the European Southern Observatory (ESO) archive. These
spectra were observed on 2002 August ("UVES1"; program ID: 069.D-0413,
PI: M. Perinotto) and 2007 June ("UVES2"; program ID: 079.D-0788, PI:
A. Zijlstra), using the Ultraviolet Visual Echelle Spectrograph (UVES)
at the Nasmyth B focus of KUEYEN, the second of the four 8.2m
telescopes of the ESO Very Large Telescope (VLT) at Paranal, Chile.
These archive spectra covered the wavelength range of 3300-6600Å in
UVES1 and 3300-9500Å in UVES2.
We complemented optical spectra with UV spectra obtained by the
International Ultraviolet Explorer (IUE) retrieved from the
Multi-mission Archive at the STScI (MAST).
We used two data sets (program IDs: P30333, PI: A. Zijlstra; P30652,
PI: J. Bernard-Salas), taken by the Spitzer Space Telescope with the
Infrared Spectrograph (IRS) in 2006 December, from the Spitzer Science
Center.
Objects:
------------------------------------------------------
RA (2000) DE Designation(s)
------------------------------------------------------
00 37 16.03 -13 42 58.6 PN BoBn 1 = PN G108.4-76.1
------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table23.dat 88 624 Observed and reddening corrected line ratios
and identifications of BoBn 1
--------------------------------------------------------------------------------
See also:
IV/24 : Catalogue of Galactic Planetary Nebulae (Kohoutek, 2001)
VI/110 : Final Merged Log of IUE Observations (NASA-ESA, 2000)
V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+, 1992)
J/ApJ/714/1096 : Galactic planetary nebulae (Stanghellini+, 2010)
J/PAZh/35/574 : He, C, N and O abundances in PNe (Milanova+, 2009)
J/A+A/479/155 : Proper motions of Galactic Planetary Nebulae (Kerber+, 2008)
J/A+A/475/217 : Classification of planetary nebulae (Quireza+, 2007)
J/MNRAS/349/793 : Galactic PNe abundances (Perinotto+, 2004)
J/A+A/408/1029 : Coordinates of Galactic planetary nebulae (Kerber+, 2003)
J/AN/323/484 : Accurate coordinates of Planetary Nebulae (Kohoutek+, 2002)
J/other/RMxAA/37.115 : Optical coordinates of southern PNe (Kimeswenger+, 2001)
J/A+AS/132/13 : Planetary nebulae radial velocities (Durand+ 1998)
J/ApJS/117/361 : PNe in NRAO VLA Sky Survey (Condon+ 1998)
J/AJ/112/1188 : HK survey emission-line candidates (Beers+ 1996)
J/A+AS/94/399 : Absolute fluxes and distances of PN (Cahn+, 1992)
Byte-by-byte Description of file: table23.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.2 0.1nm lam ? Observed heliocentric wavelength λ (Å)
9- 16 A8 --- Ion Ion identification
18- 24 F7.2 0.1nm lam0 Laboratory wavelength in Angstroms
26- 29 A4 --- Comp Component (1, 2 or Tot.)
31- 36 F6.3 --- f(lam) Interstellar extinction coefficient (1)
38- 44 F7.3 --- I(lam) Reddening corrected flux (1)
46- 51 F6.3 --- e_I(lam) Uncertainty in CFlux
53- 57 A5 --- Obs Observation source (HDS, UVES1 or UVES2) (2)
59- 88 A30 --- Note Additional note
--------------------------------------------------------------------------------
Note (1): Relative to Hβ where I(Hβ)=100.
Note (2): Observation as follows:
HDS = Subaru/High-Dispersion Spectrograph on 2008 October 6 (PID: S08B-110)
UVES1 = VLT/Ultraviolet Visual Echelle Spectrograph on 2002 August
(PID: 069.D-0413)
UVES2 = VLT/Ultraviolet Visual Echelle Spectrograph on 2007 June
(PID: 079.D-0788)
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 18-Jul-2012