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J/ApJ/831/L3       NIR spectra of 10 PNe in LMC and SMC       (Mashburn+, 2016)

Neutron-capture element abundances in Magellanic Cloud planetary nebulae. Mashburn A.L., Sterling N.C., Madonna S., Dinerstein H.L., Roederer I.U., Geballe T.R. <Astrophys. J., 831, L3-L3 (2016)> =2016ApJ...831L...3M (SIMBAD/NED BibCode)
ADC_Keywords: Magellanic Clouds ; Planetary nebulae ; Abundances ; Spectra, infrared Keywords: infrared: general; Magellanic Clouds; nuclear reactions, nucleosynthesis, abundances; planetary nebulae: general; stars: AGB and post-AGB Abstract: We present near-infrared spectra of 10 planetary nebulae (PNe) in the Large and Small Magellanic Clouds (LMC and SMC), acquired with the FIRE and GNIRS spectrometers on the 6.5 m Baade and 8.1 m Gemini South Telescopes, respectively. We detect Se and/or Kr emission lines in eight of these objects, the first detections of n-capture elements in Magellanic Cloud PNe. Our abundance analysis shows large s-process enrichments of Kr (0.6-1.3 dex) in the six PNe in which it was detected, and Se is enriched by 0.5-0.9 dex in five objects. We also estimate upper limits to Rb and Cd abundances in these objects. Our abundance results for the LMC are consistent with the hypothesis that PNe with 2-3 M progenitors dominate the bright end of the PN luminosity function in young gas-rich galaxies. We find no significant correlations between s-process enrichments and other elemental abundances, central star temperature, or progenitor mass, though this is likely due to our small sample size. We determine S abundances from our spectra and find that [S/H] agrees with [Ar/H] to within 0.2 dex for most objects, but is lower than [O/H] by 0.2-0.4 dex in some PNe, possibly due to O enrichment via third dredge-up. Our results demonstrate that n-capture elements can be detected in PNe belonging to nearby galaxies with ground-based telescopes, allowing s-process enrichments to be studied in PN populations with well-determined distances. Description: In Table 1, we provide an observing log and nebular and stellar parameters for our sample. Nine of the 10 PNe were observed with the Folded-Port InfraRed Echellette (FIRE) spectrograph on the 6.5m Baade Telescope at Las Campanas Observatory in 2013 January 21, 22 and August 11, 12. We used a 0.75" slit width to provide a resolution R=4800 in echelle mode, covering the spectral range 0.83-2.45um. LMC SMP 62 and SMC SMP 20 were observed in the K band with the Gemini Near-InfraRed Spectrograph (GNIRS) on the 8.1m Gemini South telescope (resolving power of R=4000 in the wavelength range 2.1-2.3um) in 2006 August 16. The data were taken in queue mode under observing program GS-2006B-Q-51. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 98 11 Observing log and nebular properties of the 10 planetary nebulae (PNe) table2.dat 97 847 Line identifications and intensities
See also: J/ApJS/218/25 : Abundances in PNe. III: Se and Kr (Sterling+, 2015) J/A+A/560/A44 : Abundances of LMC bar & disk stars (Van der Swaelmen+, 2013) J/ApJ/761/33 : Chemical properties of 89 stars in LMC disk (Lapenna+, 2012) J/ApJ/746/29 : High-resolution GC abundances. IV. 8 LMC GCs (Colucci+, 2012) J/A+A/480/379 : Abundances of 59 red giants in LMC (Pompeia+, 2008) J/ApJ/659/1265 : Emission lines in 4 planetary nebulae (Sharpee+, 2007) J/A+A/456/451 : Magellanic Clouds PNe abundances (Leisy+, 2006) J/ApJ/622/294 : STIS UV spectra of LMC PNe (Stanghellini+, 2005) J/A+AS/116/95 : Magellanic Clouds PNe line intensities (Leisy+, 1996) J/ApJ/417/209 : Faint planetary nebulae in Magellanic Clouds (Jacoby+, 1993) J/ApJS/76/1085 : LMC + SMC PNe optical spectroscopy. II (Meatheringham+ 1991) J/MNRAS/234/583 : Abundances in Magellanic Cloud planetary nebulae (Monk+ 1988) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 A3 --- Gal Galaxy name 5- 7 A3 --- --- [SMP] 9- 10 I2 --- SMP PN name (<SMP {S/L}MC NN> in Simbad) 12- 21 A10 "Y/M/D" Date Observed date 23- 27 A5 --- Inst Instrument (FIRE or GNRIS, see the "Description" section above) 29- 32 I4 s Tint [1120/8000] Integration time 34- 37 F4.1 10+3K TeO3 [11.7/16]? Te[OIII] nebular temperature 39- 43 F5.2 10+3/cm3 ne [2.2/31.4]? Electron density 45- 48 F4.2 --- CHb [0/0.5]? Hβ extinction coefficient 50- 54 F5.2 --- m5007 [14.6/16.2]? Apparent [OIII] 5007 magnitude (1) 56- 60 F5.2 --- logC/O [-0.9/0.7]? C/O abundance 62- 68 A7 --- r_logC/O Reference for C/O abundance (2) 70- 74 F5.2 --- logN/O ? N/O abundance 76- 79 A4 --- r_logN/O Reference for N/O abundance (2) 81- 85 F5.1 10+3K Teff [38.8/150]? Central star temperature 87- 90 A4 --- r_Teff Teff reference (2) 92- 98 A7 Msun Minit Estimated progenitor mass Minit (3)
Note (1): Apparent [OIII] 5007 magnitudes computed from absolute fluxes (corrected for foreground extinction) measured with the Hubble Space Telescope (Stanghellini+ 2003ApJ...596..997S; Shaw+ 2006ApJS..167..201S), with the exceptions of SMP 85 and SMP 99 (Leisy & Dennefeld, 2006, J/A+A/456/451), using the relation m5007=-2.5logF5007-13.74 (Jacoby 1989ApJ...339...39J). Note (2): References as follows: S10 = Shaw+ (2010ApJ...717..562S) T03 = Tsamis+ (2003MNRAS.345..186T) MD91 = Meatheringham & Dopita (1991, J/ApJS/76/1085) LD06 = Leisy & Dennefeld (2006, J/A+A/456/451) A87 = Aller+ 1987ApJ...320..159A D94 = Dopita+ 1994ApJ...426..150D S09 = Stanghellini+ 2009ApJ...702..733S V03 = Villaver+ 2003ApJ...597..298V V04 = Villaver+ 2004ApJ...614..716V Note (3): from Villaver+ (2003ApJ...597..298V, 2004ApJ...614..716V)
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 3 A3 --- Gal Galaxy name (SMC or LMC) 5- 7 A3 --- --- [SMP] 9- 10 I2 --- SMP Planetary Nebular Name (<SMP {S/L}MC NN> in Simbad) 13- 17 A5 --- Inst Spectrometer used (1) 20- 31 A12 --- Line Line Identification, ion 33- 39 F7.5 um lamobs [0.831/2.462]? Observed wavelength, microns 40- 46 F7.5 um lamlab [0.830/2.455] Laboratory wavelength, microns 48- 49 A2 --- l_F/F(Brg) [≤ ] Limit flag on F/F(Brg) 52- 59 E8.3 --- F/F(Brg) [0.07/1410]? Measured Line Flux, normalized (2) 61- 68 E8.3 --- e_F/F(Brg) [0.01/54]? Uncertainty in F/F(Brg) 71- 72 A2 --- l_I/I(Brg) [≤ ] Limit flag on I/I(Brg) 75- 82 E8.3 --- I/I(Brg) [0.08/1570]? Measured Line Intensity, normalized (2) 84- 91 E8.3 --- e_I/I(Brg) [0.01/62]? Uncertainty in I/I(Brg) 93- 97 A5 --- Comm Comment (3)
Note (1): Spectrometer used as follows: FIRE = Folded-Port InfraRed Echellette (FIRE), 6.5-m Baade Telescope, Las Campanas Observatory (823 instances); GNIRS = Gemini Near-InfraRed Spectrograph (GNIRS), 8.1-m Gemini South telescope (24 instances). Note (2): Measured fluxes and intensities are on the scale F(HI, Brγ) = I(HI, Brγ) = 100 Note (3): Comment as follows: : = Marginal detection; Fit = Line fit; * = Blended feature.
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 14-Feb-2017
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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