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 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:
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FileName Lrecl Records Explanations
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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
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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
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Bytes Format Units Label Explanations
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1- 3 A3 --- Gal Galaxy name
5- 7 A3 --- --- [SMP]
9- 10 I2 --- SMP PN name ( 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)
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Note (1): Apparent [OIII] 5007 magnitudes computed from absolute fluxes
(corrected for foreground extinction) measured with the Hubble Space
Telescope (Stanghellini+ 2003ApJ...596..997S 2003ApJ...596..997S;
Shaw+ 2006ApJS..167..201S 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 1989ApJ...339...39J).
Note (2): References as follows:
S10 = Shaw+ (2010ApJ...717..562S 2010ApJ...717..562S)
T03 = Tsamis+ (2003MNRAS.345..186T 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 1987ApJ...320..159A
D94 = Dopita+ 1994ApJ...426..150D 1994ApJ...426..150D
S09 = Stanghellini+ 2009ApJ...702..733S 2009ApJ...702..733S
V03 = Villaver+ 2003ApJ...597..298V 2003ApJ...597..298V
V04 = Villaver+ 2004ApJ...614..716V 2004ApJ...614..716V
Note (3): from Villaver+ (2003ApJ...597..298V 2003ApJ...597..298V, 2004ApJ...614..716V 2004ApJ...614..716V)
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Byte-by-byte Description of file: table2.dat
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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
( 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)
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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.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 14-Feb-2017