J/AJ/142/111 Total infrared brightness and SFR in M33 (Boquien+, 2011)
Dust heating sources in galaxies: the case of M33 (HERM33ES).
Boquien M., Calzetti D., Combes F., Henkel C., Israel F., Kramer C.,
Relano M., Verley S., Van Der Werf P., Xilouris E.M., HERM33ES Team
<Astron. J., 142, 111 (2011)>
=2011AJ....142..111B 2011AJ....142..111B
ADC_Keywords: Galaxies, IR ; Extinction
Keywords: dust, extinction - galaxies: individual (M33) - infrared: galaxies -
Local Group
Abstract:
In the context of the Herschel HERM33ES open time key project, we are
studying the moderately inclined Scd local group galaxy M33 which is
located only 840kpc away. In this article, using Spitzer and Herschel
data ranging from 3.6um to 500um, along with HI, Hα maps, and
Galaxy Evolution Explorer ultraviolet data, we have studied the
emission of the dust at the high spatial resolution of 150pc.
Combining Spitzer and Herschel bands, we have provided new,
inclination-corrected, resolved estimators of the total infrared
brightness and of the star formation rate from any combination of
these bands.
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RA (2000) DE Designation(s)
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01 33 50.90 +30 39 35.8 M33 = NGC 598
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 123 255 Coefficients of the fit of the combination of any
number of Spitzer and Herschel bands from 8.0um
to 500um to estimate the total IR luminosity
table2.dat 123 255 Coefficients of the fit of the combination of any
number of Spitzer and Herschel bands from 8.0um
to 500um to estimate the SFR in M☉/yr/kpc^2
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Byte-by-byte Description of file: table1.dat table2.dat
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Bytes Format Units Label Explanations
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1- 6 F6.3 --- c8 ?=0 Coefficient for best fit to
Spitzer/IRAC 8 micron band (1)
8- 12 F5.3 --- e_c8 ?=0 Uncertainty in c8
14- 19 F6.3 --- c24 ?=0 Coefficient for best fit to
Spitzer/MIPS 24 micron band (1)
21- 25 F5.3 --- e_c24 ?=0 Uncertainty in c24
27- 32 F6.3 --- c70 ?=0 Coefficient for best fit to
Spitzer/MIPS 70 micron band (1)
34- 38 F5.3 --- e_c70 ?=0 Uncertainty in c70
40- 45 F6.3 --- c100 ?=0 Coefficient for best fit to
Herschel/PACS 100 micron band (1)
47- 51 F5.3 --- e_c100 ?=0 Uncertainty in c100
53- 58 F6.3 --- c160 ?=0 Coefficient for best fit to
Herschel/PACS 160 micron band (1)
60- 64 F5.3 --- e_c160 ?=0 Uncertainty in c160
66- 71 F6.3 --- c250 ?=0 Coefficient for best fit to
Herschel/SPIRE 250 micron band (1)
73- 77 F5.3 --- e_c250 ?=0 Uncertainty in c250
79- 84 F6.3 --- c350 ?=0 Coefficient for best fit to
Herschel/SPIRE 350 micron band (1)
86- 90 F5.3 --- e_c350 ?=0 Uncertainty in c350
92- 97 F6.3 --- c500 ?=0 Coefficient for best fit to
Herschel/SPIRE 500 micron band (1)
99-103 F5.3 --- e_c500 ?=0 Uncertainty in c500
105-111 F7.3 --- b Relationship constant (1)
113-117 F5.3 --- e_b ?=0 Uncertainty in b
119-123 F5.3 --- sigma Standard deviation of the total IR luminosity
(table1) or SFR (table2) around best fit
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Note (1): Coefficients of the fit of the combination of any number of
Spitzer and Herschel bands from 8.0 to 500 microns to estimate the
total IR luminosity and star formation rate (SFR). The fitted
relation, with Si in W/kpc2, is of the form:
* Table1: log(LTIR) = Σni=1 ai*log(Si) + b
* Table2: log(SFR) = Σni=1 ai*log(Si) + b
The relation has been derived for brightnesses (in units of W/kpc2)
in the following range:
* 32.37 < log(B8) < 34.45,
* 31.98 < log(B24) < 34.54,
* 32.60 < log(B70) < 34.95,
* 33.29 < log(B100) < 35.08,
* 33.06 < log(B160) < 34.79,
* 32.65 < log(B250) < 34.18,
* 32.12 < log(B350) < 33.65,
* 31.60 < log(B500) < 33.10,
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 20-Nov-2012