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J/ApJ/842/97      Spectroscopic obs. of 413 HII regions in M33      (Lin+, 2017)

Spectroscopic observation and analysis of H II regions in M33 with MMT: temperatures and oxygen abundances. Lin Z., Hu N., Kong X., Gao Y., Zou H., Wang E., Cheng F., Fang G., Lin L., Wang J. <Astrophys. J., 842, 97 (2017)> =2017ApJ...842...97L
ADC_Keywords: Spectra, optical ; H II regions ; Abundances ; Radial velocities Equivalent widths ; Cross identifications Keywords: galaxies: abundances; galaxies: evolution; galaxies: individual (M33); galaxies: ISM; galaxies: spiral; H II regions Abstract: The spectra of 413 star-forming (or H II) regions in M33 (NGC 598) were observed using the multifiber spectrograph of Hectospec at the 6.5m Multiple Mirror Telescope. Using this homogeneous spectra sample, we measured the intensities of emission lines and some physical parameters, such as electron temperatures, electron densities, and metallicities. Oxygen abundances were derived via the direct method (when available) and two empirical strong-line methods, namely, O3N2 and N2. At the high-metallicity end, oxygen abundances derived from the O3N2 calibration were higher than those derived from the N2 index, indicating an inconsistency between O3N2 and N2 calibrations. We present a detailed analysis of the spatial distribution of gas-phase oxygen abundances in M33 and confirm the existence of the axisymmetric global metallicity distribution that is widely assumed in the literature. Local variations were also observed and subsequently associated with spiral structures to provide evidence of radial migration driven by arms. Our O/H gradient fitted out to 1.1 R25 resulted in slopes of -0.17±0.03, -0.19±0.01, and -0.16±0.17dex R25-1, utilizing abundances from O3N2, N2 diagnostics, and a direct method, respectively. Description: The observations discussed in this paper were obtained on the nights of 2013 October 9, 12, and 15, using the Hectospec fiber-fed spectrograph at the Multiple Mirror Telescope (MMT) --wavelength range of 3650-9200Å with a resolution of ∼6Å. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 66 413 Sample of HII regions observed in M33 table2.dat 257 413 Reddening-corrected emission line fluxes of HII regions in M33 table3.dat 124 413 Physical conditions and metallicity of HII regions in M33
See also: J/AJ/110/2739 : H-alpha emitting regions in M33 (Calzetti+ 1995) J/A+AS/123/159 : IRON Project. XXII. C and O radiative rates (Galavis+ 1997) J/ApJS/123/311 : Excitation rate coefficients for O III (Aggarwal+, 1999) J/ApJS/120/247 : Supernova remnants in M33 (Gordon+, 1999) J/PASP/111/685 : HII regions of M33. II. (Hodge+, 1999) J/ApJS/173/185 : GALEX ultraviolet atlas of nearby galaxies (Gil de Paz+, 2007) J/ApJS/174/366 : Chandra ACIS survey of M33 (ChaSeM33) (Plucinsky+, 2008) J/ApJ/675/1213 : Abundances in M33 HII regions (Rosolowsky+, 2008) J/ApJ/700/654 : Keck spectroscopy of extragalactic HII regions (Esteban+ 2009) J/A+A/512/A63 : Abundances of M33 HII regions (Magrini+, 2010) J/ApJS/188/32 : Breit-Pauli transition probabilities for SII (Tayal+, 2010) J/A+A/552/A140 : SEDs of M33 HII regions (Relano+, 2013) J/A+A/559/A114 : Updated O3N2 and N2 abundance indicators (Marino+, 2013) J/A+A/586/A37 : M33 center and BCLMP302 [CII] spectroscopy (Mookerjea+, 2016) J/A+A/595/A43 : Photometry of 119 HII regions in M33 (Relano+, 2016) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq Identification of HII region (1) 5- 17 A13 --- Name ? HII region name from published catalog (2) 19 I1 h RAh [1] Hour of Right Ascension (J2000) 21- 22 I2 min RAm [32/35] Minute of Right Ascension (J2000) 24- 28 F5.2 s RAs Second of Right Ascension (J2000) 30 A1 --- DE- [+] Sign of Declination (J2000) 32- 33 I2 deg DEd [30/31] Degree of Declination (J2000) 35- 36 I2 arcmin DEm Arcminute of Declination (J2000) 38- 41 F4.1 arcsec DEs Arcsecond of Declination (J2000) 43- 47 F5.3 kpc R [0.1/8] Physical distance to the center of M33 (3) 49- 53 F5.3 --- R/R25 [0.02/1.1] R to R25 ratio (4) 55- 60 F6.2 deg PA Position angle (5) 62 I1 --- FO3 [1/2]? Flag of [OIII]4363 detection (6) 64 I1 --- FN2 [1/2]? Flag of [NII]5755 detection (6) 66 I1 --- Fn [1/3] Flag of the observed night (7)
Note (1): IDs of HII regions sorted by right ascension. A total of 10 regions (ID=72, 148, 150, 160, 246, 324, 327, 397, 403, 409) do not have significant [OIII]5007 or [NII]6583 detections. A total of 18 HII regions with the following IDs lie above the Kauffmann+ (2003MNRAS.346.1055K) line at the BPT diagram, indicating that they are likely not star-forming dominated regions: 45, 79, 107, 151, 164, 217, 224, 233, 237, 252, 265, 291, 308, 322, 357, 379, 389, 398. Note (2): Abbreviations as below: BCLMP = Boulesteix et al. (1974A&A....37...33B ; <BCLMP NNNNA> in Simbad); VGV86 = Viallefond et al. (1986A&AS...64..237V ; <VGHC 2-NNN> in Simbad); CPSDP = Courtes et al. (1987A&A...174...28C ; <CPSDP NNNA> in Simbad); GDK99 = Gordon et al. (1999, J/ApJS/120/247 ; <[GDK99] NNN> in Simbad); HBW = Hodge et al. (1999, J/PASP/111/685 ; <HBW NNNN> in Simbad). Note (3): Physical distances to the center of M33 located at RAJ2000=1:33:50.89, DEJ2000=30:39:36.8 (Plucinsky+ 2008, J/ApJS/174/366). We assumed a distance to M33 of 878kpc, an inclination of 56arcdeg (Zaritsky+ 1989AJ.....97...97Z), and a position angle of 23arcdeg (Zaritsky+ 1989AJ.....97...97Z). Note (4): Assumed an R25 of 28.2 arcmin (de Vaucouleurs 1959ApJ...130..728D). Note (5): Position angles are de-projected angles on the disk of M33, measured from north to east. Note (6): Numbers indicate the detected quality of two auroral Lines. Code as follows: 1 = an emission line with a significant detection (S/N≥3) but without a well-defined profile, 2 = an emission line with not only a significant detection but also a well-defined profile. Note (7): Observation nights of each object. "1", "2", and "3" indicate the nights of 2013 October 9, 12, and 15, respectively.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq Identification of HII region 5- 10 F6.3 --- [OII]3727 [0.1/10.5]? Emission line flux (8) 12- 16 F5.3 --- e_[OII]3727 [0.01/0.3]? Uncertainty in flux 18- 22 F5.3 --- [NeIII]3869 [0.05/1.4]? Emission line flux (8) 24- 28 F5.3 --- e_[NeIII]3869 [0.004/0.3]? Uncertainty in flux 30- 34 F5.3 --- Hdelta4102 [0.1/1.2]? Emission line flux (8) 36- 40 F5.3 --- e_Hdelta4102 [0.004/0.3]? Uncertainty in flux 42- 46 F5.3 --- Hgamma4340 [0.3/1]? Emission line flux (8) 48- 52 F5.3 --- e_Hgamma4340 [0.008/0.2]? Uncertainty in flux 54- 58 F5.3 --- [OIII]4363 [0.002/0.4]? Emission line flux (8) 60- 64 F5.3 --- e_[OIII]4363 [0.001/0.05]? Uncertainty in flux 66- 70 F5.3 --- [OIII]4959 [0.01/3]? Emission line flux (8) 72- 76 F5.3 --- e_[OIII]4959 [0.001/0.04]? Uncertainty in flux 78- 82 F5.3 --- [OIII]5007 [0.04/9]? Emission line flux (8) 84- 88 F5.3 --- e_[OIII]5007 [0.002/0.2]? Uncertainty in flux 90- 94 F5.3 --- [NII]5755 [0.001/0.3]? Emission line flux (8) 96-100 F5.3 --- e_[NII]5755 [0/0.06]? Uncertainty in flux 102-106 F5.3 --- HeI5876 [0.02/0.6]? Emission line flux (8) 108-112 F5.3 --- e_HeI5876 [0.001/0.07]? Uncertainty in flux 114-118 F5.3 --- [OI]6300 [0.005/1.1]? Emission line flux (8) 120-124 F5.3 --- e_[OI]6300 [0/0.1]? Uncertainty in flux 126-130 F5.3 --- [NII]6548 [0.01/0.6]? Emission line flux (8) 132-136 F5.3 --- e_[NII]6548 [0/0.03]? Uncertainty in flux 138-142 F5.3 --- Halpha6563 [1.3/3]Emission line flux (8) 144-148 F5.3 --- e_Halpha6563 [0.02/0.1] Uncertainty in flux 150-154 F5.3 --- [NII]6583 [0.04/1.5]? Emission line flux (8) 156-160 F5.3 --- e_[NII]6583 [0.001/0.08]? Uncertainty in flux 162-166 F5.3 --- [SII]6717 [0.004/2] Emission line flux (8) 168-172 F5.3 --- e_[SII]6717 [0.001/0.08] Uncertainty in flux 174-178 F5.3 --- [SII]6731 [0.008/1.7]? Emission line flux (8) 180-184 F5.3 --- e_[SII]6731 [0.001/0.08]? Uncertainty in flux 186-190 F5.3 --- [ArIII]7135 [0.005/0.2]? Emission line flux (8) 192-196 F5.3 --- e_[ArIII]7135 [0/0.06]? Uncertainty in flux 198-202 F5.3 --- [OII]7320 [0.005/0.2]? Emission line flux (8) 204-208 F5.3 --- e_[OII]7320 [0/0.04]? Uncertainty in flux 210-214 F5.3 --- [OII]7330 [0.005/0.3]? Emission line flux (8) 216-220 F5.3 --- e_[OII]7330 [0/0.03]? Uncertainty in flux 222-228 F7.1 10-20W/m2 Hbeta4861 [9/13572] Hbeta flux; 1e-17erg/s/cm2 230-235 F6.1 10-20W/m2 e_Hbeta4861 [0.3/1313] Uncertainty of Hbeta4861 237-242 F6.1 0.1nm EW(Hbeta) [2/2405]? Equivalent width of Hbeta; Angstrom (9) 244-249 F6.4 mag E(B-V) [0.0001/1.6]? Color excess 251-257 F7.2 km/s RVel [-117/119] Radial velocity (10)
Note (8): In units of Hbeta=1. Note (9): Hbeta emission line equivalent widths corrected for stellar absorption. Two HII regions (ID=160, 350) have negative local continuum fluxes, resulting in incorrect EWs of Hbeta. These EWs are excluded from this table. Note (10): Radial velocity for each region. System velocity of M33, assuming a value of -179km/s (de Vaucouleurs+ 1991, VII/155), has been subtracted.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq Identification of HII region 5- 9 I5 K Te[OIII] [6600/68700]? Electron temperature derived from [OIII] auroral line 11- 15 I5 K e_Te[OIII] [100/21500]? Lower error of Te[OIII] 17- 21 I5 K E_Te[OIII] [100/46600]? Upper error of Te[OIII] 23- 27 I5 K Te[NII] [6400/95100]? Electron temperature derived from [NII] auroral line 29- 33 I5 K e_Te[NII] [300/24000]? Lower error of Te[NII] 35- 39 I5 K E_Te[NII] [300/50000]? Upper error of Te[NII] 41- 44 I4 cm-3 ne [1/1549]? Electron density 46- 48 I3 cm-3 e_ne [0/382]? Lower error of ne 50- 52 I3 cm-3 E_ne [12/898]? Upper error of ne 54- 58 F5.3 --- ZO[Te] [7/9.1]? Oxygen abundance derived from Te method 60- 64 F5.3 --- e_ZO[Te] [0.01/0.3]? Lower error of ZO[Te] 66- 70 F5.3 --- E_ZO[Te] [0.01/0.7]? Upper error of ZO[Te] 72- 76 F5.3 --- ZO[O3N2] [8.1/8.7]? Oxygen abundance derived from O3N2 calibration (11) 78- 82 F5.3 --- e_ZO[O3N2] [0.002/0.05]? Lower error of ZO[O3N2] 84- 88 F5.3 --- E_ZO[O3N2] [0.002/0.08]? Upper error of ZO[O3N2] 90- 94 F5.3 --- ZO[N2] [8/8.7]? Oxygen abundance derived from N2 calibration (12) 96-100 F5.3 --- e_ZO[N2] [0.004/0.2]? Lower error ZO[N2] 102-106 F5.3 --- E_ZO[N2] [0.003/0.1]? Upper error ZO[N2] 108-112 F5.3 --- ZN[Te] [6.4/8]? Nitrogen abundance derived from Te method 114-118 F5.3 --- e_ZN[Te] [0.03/0.3]? Lower error ZN[Te] 120-124 F5.3 --- E_ZN[Te] [0.03/0.8]? Upper error ZN[Te]
Note (11): Oxygen abundance derived from O3N2 index using calibration from Marino+ (2013, J/A+A/559/A114). The systematic uncertainty of this calibration is 0.18. Note (12): Oxygen abundance derived from N2 index using calibration from Marino+ (2013, J/A+A/559/A114). The systematic uncertainty of this calibration is 0.16.
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 31-Jan-2018
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