J/A+A/552/A140 SEDs of M33 HII regions (Relano+, 2013)
Spectral energy distributions of HII regions in M33 (HerM33es).
Relano M., Verley S., Perez I., Kramer C., Calzetti D., Xilouris E.M.,
Boquien M., Abreu-Vicente J., Combes F., Israel F., Tabatabaei F.S.,
Braine J., Buchbender C., Gonzalez M., Gratier P., Lord S., Mookerjea B.,
Quintana-Lacaci G., Van Der Werf P.
<Astron. Astrophys., 552, A140 (2013)>
=2013A&A...552A.140R 2013A&A...552A.140R
ADC_Keywords: Galaxies, nearby ; Energy distributions ; Photometry, infrared ;
Photometry, ultraviolet
Keywords: galaxies: individual: M 33 - galaxies: ISM - Local Group -
dust, extinction - HII regions - ISM: bubbles
Abstract:
Within the framework of the Herschel M33 extended survey HerM33es and
in combination with multi-wavelength data we study the spectral energy
distribution (SED) of a set of HII regions in the Local Group galaxy
M33 as a function of the morphology. We analyse the emission
distribution in regions with different morphologies and present models
to infer the Hα emission measure observed for HII regions with
well defined morphology. We present a catalogue of 119 HII regions
morphologically classified: 9 filled, 47 mixed, 36 shell, and 27 clear
shell HII regions. For each object we extracted the photometry at
twelve available wavelength bands, covering a wide wavelength range
from FUV-1516Å (GALEX) to IR-250um (Herschel), and we obtained the
SED for each object. We also obtained emission line profiles in
vertical and horizontal directions across the regions to study the
location of the stellar, ionised gas, and dust components. We
constructed a simple geometrical model for the clear shell regions,
whose properties allowed us to infer the electron density of these
regions.
Description:
To investigate the continuum UV emission of M 33, we used the data
from GALEX, in particular the data distributed by de Paz et al. (2007,
Cat. J/ApJS/173/185).
To trace the ionised gas, we used the narrow-line Hα image of
M 33 obtained by Greenawalt (1998, Ph.D. Thesis, New Mexico state
University).
Dust emission can be investigated through the mid-IR (MIR) and FIR
data of M 33 obtained with the Spitzer Infrared Array Camera (IRAC)
and Multiband Imaging Photometer (MIPS).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 46 119 Selection of HII regions
tableb2.dat 135 119 Fluxes of our set of HII regions in mJy within
the apertures shown in tableb1.dat
tableb3.dat 25 111 Dust properties of HII regions
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See also:
J/PASP/111/685 : HII regions of M33. II. (Hodge+, 1999)
J/ApJ/675/1213 : Abundances in M33 HII regions (Rosolowsky+, 2008)
J/A+A/512/A63 : Abundances of M33 HII regions (Magrini+, 2010)
Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/119] Identification number
5- 6 I2 h RAh WCS right ascension (J2000)
8- 9 I2 min RAm WCS right ascension (J2000)
11- 16 F6.3 s RAs WCS right ascension (J2000)
18 A1 --- DE- Declination sign (J2000)
19- 20 I2 deg DEd Declination (J2000)
22- 23 I2 arcmin DEm Declination (J2000)
25- 29 F5.2 arcsec DEs Declination (J2000)
31- 34 F4.1 arcsec Rad Aperture radius (1)
36- 46 A11 --- Morph Morphological classification of HII region, as
Filled, Shell, Clear Shell or Mixed.
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Note (1): aperture radius used to perform the photometry, with aperture defined
using the Hα image of Hoopes & Walterbos (2000ApJ...541..597H 2000ApJ...541..597H) to
include the total Hα emission of the region (see Sect. 3.1 for more
details).
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Byte-by-byte Description of file: tableb2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/119] Identification number
5- 9 F5.2 mJy F(FUV) ?=- GALEX FUV flux (2)
11- 14 F4.2 mJy e_F(FUV) ?=- rms uncertainty on F(FUV)
16- 20 F5.2 mJy F(NUV) ?=- GALEX NUV flux (2)
22- 25 F4.2 mJy e_F(NUV) ?=- rms uncertainty on F(NUV)
27- 31 F5.2 mJy F(Ha) Hα flux (0.6563um) (2) (3)
33- 36 F4.2 mJy e_F(Ha) rms uncertainty on F(Ha)
38- 42 F5.2 mJy F(3.4) ?=- Spitzer/IRAC 3.4um flux (2)
44- 47 F4.2 mJy e_F(3.4) ?=- rms uncertainty on F(3.4)
49- 53 F5.2 mJy F(4.5) ?=- Spitzer/IRAC 4.5um flux (2)
55- 58 F4.2 mJy e_F(4.5) ?=- rms uncertainty on F(4.5)
60- 64 F5.2 mJy F(5.8) ?=- Spitzer/IRAC 5.8um flux (2)
66- 69 F4.2 mJy e_F(5.8) ?=- rms uncertainty on F(5.8)
71- 75 F5.2 mJy F(8.0) ?=- Spitzer/IRAC 8.0um flux (2)
77- 80 F4.2 mJy e_F(8.0) ?=- rms uncertainty on F(8.0)
82- 86 F5.2 mJy F(24) ?=- Spitzer/MIPS 24um flux (2)
88- 91 F4.2 mJy e_F(24) ?=- rms uncertainty on F(24).
93- 97 F5.2 mJy F(70) ?=- Spitzer/MIPS 70um flux (2)
99-102 F4.2 mJy e_F(70) ?=- rms uncertainty on F(70).
104-108 F5.2 mJy F(100) ?=- Herschel/PACS 100um flux (2)
110-113 F4.2 mJy e_F(100) ?=- rms uncertainty on F(100).
115-119 F5.2 mJy F(160) ?=- Herschel/PACS 160um flux (2)
121-124 F4.2 mJy e_F(160) ?=- rms uncertainty on F(160).
126-130 F5.2 mJy F(250) ?=- Herschel/SPIRE 250um flux (2)
132-135 F4.2 mJy e_F(250) ?=- rms uncertainty on F(250).
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Note (2): All the fluxes have been background subtracted. The errors include the
uncertainties in the calibration and background subtraction.
We did not take into account negative fluxes higher than the corresponding
errors, in these cases the fluxes are represented by ---.
Note (3): The Hα flux corresponds to the continuum-subtracted flux.
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Byte-by-byte Description of file: tableb3.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/119] Identification number
5- 7 I3 pc r Radius of the aperture photometry
9- 13 I5 Msun Md Dust mass derived using the DL07
(Draine & Li, 2007ApJ...657..810D 2007ApJ...657..810D) model
15- 16 I2 Msun e_Md [50] Error on Md (4)
18- 21 F4.1 K Td Dust temperature (5)
23- 25 F3.1 K e_Td [5.6] Error on Td (6)
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Note (4): the errors correspond to the grid step of 50M☉ used to fit the
data.
Note (5): dust temperatures derived using DL07 (Draine & Li,
2007ApJ...657..810D 2007ApJ...657..810D) models and the relation provided by Galametz et al.
(2012MNRAS.425..763G 2012MNRAS.425..763G) (Tcold(K)=17.5*Umin1/6).
Note (6): The errors correspond to an uncertainty of 0.5 in Umin in the models.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 06-Sep-2013