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J/ApJ/706/599         Hα and UV SFR in the local volume       (Lee+, 2009)

Comparison of Hα and UV star formation rates in the local volume: systematic discrepancies for dwarf galaxies. Lee J.C., Gil de Paz A., Tremonti C., Kennicutt R.C., Salim S., Bothwell M., Calzetti D., Dalcanton J., Dale D., Engelbracht C., Funes J.G., Johnson B., Sakai S., Skillman E., van Zee L., Walter F., Weisz D. <Astrophys. J., 706, 599-613 (2009)> =2009ApJ...706..599L
ADC_Keywords: Galaxies, nearby ; Photometry, H-alpha ; Ultraviolet ; Surveys Keywords: galaxies: dwarf - galaxies: evolution - galaxies: photometry - stars: formation - surveys - ultraviolet: galaxies Abstract: Using a complete sample of ∼300 star-forming galaxies within 11Mpc of the Milky Way, we evaluate the consistency between star formation rates (SFRs) inferred from the far ultraviolet (FUV) non-ionizing continuum and Hα nebular emission, assuming standard conversion recipes in which the SFR scales linearly with luminosity at a given wavelength. Our analysis probes SFRs over 5 orders of magnitude, down to ultra-low activities on the order of ∼10-4M/yr. The data are drawn from the 11Mpc Hα and Ultraviolet Galaxy Survey (11HUGS), which has obtained Hα fluxes from ground-based narrowband imaging, and UV fluxes from imaging with GALEX. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 95 315 11HUGS (11Mpc Hα and Ultraviolet Galaxy Survey) star formation rates.
See also: J/ApJS/192/6 : A GALEX UV imaging survey of nearby galaxies (Lee+, 2011) J/ApJ/706/553 : Fluxes in nearby star-forming galaxies (Boquien+, 2009) J/ApJ/703/1672 : Dust-corrected SFR of galaxies. I. (Kennicutt+, 2009) J/ApJS/178/247 : Hα and [NII] survey in local 11 Mpc (Kennicutt+, 2008) J/ApJS/164/81 : Spectrophotometry of nearby galaxies (Moustakas+, 2006) J/A+A/446/839 : Hα surface photometry in nearby clusters (Gavazzi+, 2006) J/ApJS/126/271 : Surface photometry of nearby field galaxies (Jansen+ 2000) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq Running index number 5- 18 A14 --- Name Galaxy name 20- 21 I2 h RAh Hour of Right Ascension (J2000) 23- 24 I2 min RAm Minute of Right Ascension (J2000) 26- 29 F4.1 s RAs Second of Right Ascension (J2000) 31 A1 --- DE- Sign of the Declination (J2000) 32- 33 I2 deg DEd Degree of Declination (J2000) 35- 36 I2 arcmin DEm Arcminute of Declination (J2000) 38- 39 I2 arcsec DEs Arcsecond of Declination (J2000) 41- 44 F4.2 mag E(B-V) Milky Way reddening (1) 46- 50 F5.2 Mpc Dist Distance 52- 58 A7 --- n_Dist Flag giving Dist determination (2) 60- 65 F6.2 mag BMag Absolute B band magnitude (3) 67- 68 I2 --- T RC3 morphological T-type from Paper I (Kennicutt et al., 2008, Cat. J/ApJS/178/247) 70- 73 F4.2 mag AHa Halpha attenuation (4) 75- 78 F4.2 mag AFUV ? FUV attenuation (5) 80- 84 A5 --- r_AHa Reference for Halpha/Hbeta ratio (6) 86- 90 F5.2 [Msun/yr] SFRUV log star formation rate (7) 92- 95 F4.2 --- Ratio Ratio of Halpha and FUV calculated SFRs (8)
Note (1): Based on the maps of Schlegel et al. (1998ApJ...500..525S). Note (2): Method of distance determination as compiled, described, and referenced in Paper I (Kennicutt et al., 2008, Cat. J/ApJS/178/247). Ho=75km/s/Mpc is assumed for distances estimated from Local Group flow corrected recessional velocities. Method as follows: ceph = Cepheid variables; trgb = tip of the red giant branch; sbf = surface brightness fluctuations; mem = membership in a group with a direct distance measurement; bs = brightest blue stars; tf = Tully-Fisher relation; v(flow) = Virgocentric flow model distances. Note (3): Based on the photometry compiled in Paper I (Kennicutt et al., 2008, Cat. J/ApJS/178/247), and the distances and Milky Way reddenings given in the previous columns. Note (4): Calculated as described in Section 4.1.1 and equation (4): A=5.91log(FHα/FHβ)-2.70 Note (5): Based on the total infrared-to-UV ratio as described in Section 4.1.2. Note (6): Source of the Hα/Hβ Balmer line ratio used to calculate the Hα nebular attenuation as follows: mk = integrated spectral atlas of Moustakas and Kennicutt (2006, Cat. J/ApJS/164/81), nfgs = integrated spectra of the Nearby Field Galaxy Survey (Jansen et al. 2000, Cat. J/ApJS/126/271). A dash preceding the reference ("-mk" or "-nfgs") indicates that Hα/Hβ is less than the expected Case B ratio of 2.86. This results in a negative extinction correction, so in these cases the value of A(Hα) given is estimated from BMag, as are those where spectral line ratio measurements are not available from one of these sources. Note (7): Based on the conversion of Kennicutt (1998ARA&A..36..189K), the integrated GALEX FUV magnitude reported in Paper II (Lee et al., 2011, Cat. J/ApJS/192/6) and the A(FUV) given in this table. If no value for A(FUV) is listed, the attenuation is estimated from 1.8*A(Hα). Note (8): The Hα SFRs are based on the conversion of Kennicutt (1998ARA&A..36..189K), line fluxes and [NII]Hα corrections given in Paper I (Kennicutt et al., 2008, Cat. J/ApJS/178/247), and the A(Hα) listed in this table.
History: From electronic version of the journal References: Kennicutt et al. Paper I. 2008ApJS..178..247K Cat. J/ApJS/178/247 Lee et al. Paper II. 2011ApJS..192....6L Cat. J/ApJS/192/6
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 13-Dec-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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