J/ApJ/696/729 Fluxes and abundances of PNe in M33 (Magrini+, 2009)
The planetary nebula population of M33 and its metallicity gradient:
a look into the galaxy's distant past.
Magrini L., Stanghellini L., Villaver E.
<Astrophys. J., 696, 729-740 (2009)>
=2009ApJ...696..729M 2009ApJ...696..729M
ADC_Keywords: Planetary nebulae ; Extinction ; Abundances ; Spectroscopy
Keywords: galaxies: abundances - galaxies: evolution -
galaxies: individual (M33) - planetary nebulae: general
Abstract:
The planetary nebula (PN) population of M33 is studied via multifiber
spectroscopy with Hectospec at the MMT. In this paper, we present the
spectra of 102 PNe, whereas plasma diagnostic and chemical abundances
were performed on the 93 PNe where the necessary diagnostic lines were
measured. About 20% of the PNe are compatible with being Type I; the
rest of the sample is the progeny of an old disk stellar population,
with main sequence masses M<3M☉ and ages t>0.3Gyr. Our
observations do not seem to imply that the metallicity gradient across
the M33 disk has flattened considerably with time. We report also the
discovery of a PN with Wolf-Rayet features, PN039, belonging the class
of late [WC] stars.
Description:
We obtained spectra of 102 PNe and 48 HII regions in M33 using the MMT
Hectospec fiber-fed spectrograph which is equipped with an atmospheric
dispersion corrector. The resulting total spectral coverage ranged
from approximately 3600 to 9100Å. Five 1800s exposures were taken
on the night of 2007 October 13, and three additional 1800s exposures
of the same field were obtained on 2007 November 12. The 102 PNe were
selected from the catalog of Ciardullo et al. (2004, Cat.
J/ApJ/614/167), including four new PNe discovered therein at large
galactocentric radii.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 36 102 Observed PNe
table2.dat 53 3686 Observed and de-reddened fluxes
table3.dat 223 93 *Plasma diagnostics and abundances of 93 PNe
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Note on table3.dat: We performed plasma diagnostics by using the five-level atom
model included in the nebular analysis package in IRAF/STSDAS (Shaw & Dufour
1994ASPC...61..327S 1994ASPC...61..327S)
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See also:
J/ApJ/675/1213 : Abundances in M33 HII regions (Rosolowsky+, 2008)
J/ApJ/614/167 : Planetary nebulae in M33 (Ciardullo+, 2004)
J/ApJ/577/31 : PNe in six galaxies (Ciardullo+, 2002)
J/A+A/367/498 : Candidate Planetary Nebulae in M 33 (Magrini+, 2001)
J/A+AS/126/297 : PN abundances (Ratag+ 1997)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- --- [PN]
3- 5 I3 --- Seq Identification number (G1)
7 I1 h RAh Hour of Right Ascension (J2000)
9- 10 I2 min RAm Minute of Right Ascension (J2000)
12- 16 F5.2 s RAs Second of Right Ascension (J2000)
18 A1 --- DE- Declination sign (J2000)
19- 20 I2 deg DEd Degree of Declination (J2000)
22- 23 I2 arcmin DEm Arcminute of Declination (J2000)
25- 30 F6.3 arcsec DEs Arcsecond of Declination (J2000)
32- 36 F5.2 mag OIIImag ? The [OIII] magnitude from Ciardullo, 2004,
Cat. J/ApJ/614/167 (1)
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Note (1): Following the definitions by Jacoby (1989ApJ...339...39J 1989ApJ...339...39J).
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- --- [PN]
3- 5 I3 --- Seq Identificaiton number (G1)
7- 11 F5.3 --- cHb ? Nebular extinction coefficient
13- 17 F5.3 --- e_cHb ? Error in cHb
19- 28 A10 --- Ion Ion identification
30- 33 I4 0.1nm lambda Wavelength in Angstroms
35- 40 F6.1 --- Flambda ? Measured line flux (1)
42- 46 F5.1 --- e_Flambda ? Absolute error in Flambda
48- 53 F6.1 --- Ilambda ? Extinction corrected line flux (1)
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Note (1): Expressed on a scale where Hβ=100.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- --- [PN]
3- 5 I3 --- Seq Identification number (G1)
7- 15 E9.4 --- Ar/H ?=- Ar/H abundance
17- 25 E9.4 --- ArIII/H ?=- ArIII/H abundance
27- 31 F5.3 --- He/H ?=- He/H abundance
33- 37 F5.3 --- HeI/H ?=- HeI/H abundance
39- 43 F5.3 --- HeII/H ?=- HeII/H abundance
45- 49 F5.3 --- ICF(Ar) ?=- Ar ionization correction factor
51- 57 F7.3 --- ICF(N) ? N ionization correction factor
59- 63 F5.3 --- ICF(Ne) ?=- Ne ionization correction factor
65- 69 F5.3 --- ICF(O) ? O ionization correction factor
71- 75 F5.3 --- ICF(S) ?=- S ionization correction factor
77- 85 E9.4 --- N/H ?=- N/H abundance
87- 95 E9.4 --- NII/H ?=- NII/H abundance
97-105 E9.4 --- Ne/H ?=- Ne/H abundance
107-115 E9.4 --- NeIII/H ?=- NeIII/H abundance
117-125 E9.4 --- O/H ? O/H abundance
127-135 E9.4 --- OI/H ?=- OI/H abundance
137-145 E9.4 --- OII/H ?=- OII/H abundance
147-155 E9.4 --- OIII/H ? OIII/H abundance
157-165 E9.4 --- S/H ?=- S/H abundance
167-175 E9.4 --- SII/H ?=- SII/H abundance
177-185 E9.4 --- SIII/H ?=- SIII/H abundance
187-191 I5 K Te(NII)(a) ?=- [NII] electron temperature computed from
diagnostic line
193-197 I5 K Te(NII)(b) ? Electron temperature for [NII] (1)
199-206 F8.2 K Te(OIII)(a) ?=- [OIII] electron temperature computed from
diagnostic line
208-214 F7.1 K Te(OIII)(b) ? Electron temperature for [OIII] (1)
216-223 F8.3 cm-3 Ne(SII) ? Electron density from [SII]
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Note (1): Temperatures derived from the relations in section 3.1:
For Iλ4686>0, Te[OIII]=(63±8)Iλ4686+(11000±200)
where Te[OIII] is given in K and I4686 is scaled to Hβ=100.
Te[NII]=(11700±2800)-(2800±4000)log(I3727-29/I4959+I5007)
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Global notes:
Note (G1): From Ciardullo et al. (2004, Cat. J/ApJ/614/167; <[CDL2004] NNN>
in Simbad) except for PNe 153 to 156, which are from LGC observations
(Corradi & Magrini, 2006pnbm.conf...36C; <[MSV2009] NNN> in Simbad).
History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 06-May-2011