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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
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:
FileName Lrecl Records Explanations
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
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)
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
Bytes Format Units Label Explanations
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)
Note (1): Following the definitions by Jacoby (1989ApJ...339...39J).
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
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)
Note (1): Expressed on a scale where Hβ=100.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
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]
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)
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
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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