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J/ApJ/733/87         Star formation efficiency in galaxies         (Shi+, 2011)

Extended Schmidt law: role of existing stars in current star formation. Shi Y., Helou G., Yan L., Armus L., Wu Y., Papovich C., Stierwalt S. <Astrophys. J., 733, 87 (2011)> =2011ApJ...733...87S
ADC_Keywords: Galaxies, nearby ; Radio lines Keywords: galaxies: evolution - galaxies: starburst - ISM: atoms - ISM: molecules - stars: formation Abstract: We propose an "extended Schmidt law" with explicit dependence of the star formation efficiency (SFE=SFR/Mgas) on the stellar mass surface density (Σstar). This relation has a power-law index of 0.48±0.04 and a 1σ observed scatter on the SFE of 0.4 dex, which holds over five orders of magnitude in the stellar density for individual global galaxies, including various types and especially the low-surface-brightness (LSB) galaxies that deviate significantly from the Kennicutt-Schmidt (KS) law. When applying it to regions of a sample of 12 spiral galaxies at sub-kiloparsec resolution, the extended Schmidt law not only holds for LSB regions but also shows significantly smaller scatters both within and across galaxies compared with the KS law. We argue that this new relation points to the role of existing stars in regulating the SFE, thus better encoding the star formation physics. Comparison with physical models of star formation recipes shows that the extended Schmidt law can be reproduced by some models including gas free fall in a stellar-gravitational potential and pressure-supported star formation. By implementing this new law into the analytic model of gas accretion in ΛCDM, we show that it can reproduce the observed main sequence of star-forming galaxies (a relation between the SFR and stellar mass) from z=0 up to z=2. Description: Our whole sample is listed in Table 1 and composed of five sub-samples including low-redshift late-type galaxies, early-type galaxies, LSB galaxies, luminous infrared galaxies (LIRGs), and high-z objects. The CO and HI data are collected from the literature. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 135 143 Samples with CO and HI data
See also: J/ApJ/708/841 : Star formation in E/S0 galaxies (Wei+, 2010) J/AJ/136/2782 : Star formation efficiency in nearby galaxies (Leroy+, 2008) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Name Galaxy name 17- 26 A10 --- Type Galaxy type in this paper (1) 28- 36 F9.6 --- z [-0.0011/3.41] Redshift 38- 45 F8.2 Mpc Dist [0.78/29645] Distance used in this work 47- 73 A27 --- Ap Aperture definition (2) 75- 82 F8.2 kpc2 Area De-projected area used to derive surface densities 84- 88 F5.2 [Msun/yr/kpc2] logSigSFR Log star formation rate surface density 90- 93 F4.2 [Msun/pc2] logSigG Log of gas surface density 95- 98 A4 --- Ref Reference(s) for SFR and gas surface density data (3) 100-104 F5.2 [Msun/pc2] logSig* Log of stellar mass surface density 106-132 A27 --- Band Wavelength band used to measure stellar mass 134-135 A2 --- Ref* [2/18] Reference for stellar mass (3)
Note (1): Type as follows: LSB = The subsample of low-surface-brightness (LSB) galaxies includes all the 19 objects from Wyder et al. (2009ApJ...696.1834W) and five gas-rich dwarf galaxies from Leroy et al. (2008, Cat. J/AJ/136/2782). early-type = We here included nine objects from Wei et al. (2010ApJ...725L..62W) and 10 objects from Crocker et al. (2011MNRAS.410.1197C). high-z-SFG = High-redshift star-forming galaxies (21 optically/near-IR selected star-forming galaxies (Extended Groth Strip (EGS), BzK, and BXMD) high-z-SMG = merging submillimeter galaxies (seven submillimeter objects from Genzel et al. (2010MNRAS.407.2091G)) late-type = This sub-sample includes 61 and 18 objects from Kennicutt (1998ApJ...498..541K) and Leroy et al. (2008, Cat. J/AJ/136/2782), respectively. z=0-LIRGS = Local LIRGs See section 2.1 for further details. Note (2): Used to calculate the surface density of SFR, gas and stellar mass. R25 means the isophotal radius at 25mag/arcsec2 (usually in B band). Rmax gives the maximum extent of the galaxy at a given wavelength that is indicated in square brackets. Its value relative to R25 is listed in parentheses whenever possible. R1/2 is the half light radius at a given wavelength that is indicated in square brackets. Note (3): For those with two RefSg references, the first one is for H2 and SFR data while the second is for HI data. Reference(s) as follows: 1 = Kennicutt (1998ApJ...498..541K); 2 = Leroy et al. (2008, Cat. J/AJ/136/2782); 3 = Wei et al. (2010ApJ...725L..62W); 4 = Crocker et al. (2011MNRAS.410.1197C); 5 = Wyder et al. (2009ApJ...696.1834W); 6 = Scoville et al. (1997ApJ...484..702S); 7 = Gracia-Carpio et al. (2007A&A...468L..67G); 8 = Yun & Scoville (1995ApJ...451L..45Y); 9 = Bryant & Scoville (1999AJ....117.2632B); 10 = Yun et al. (1994ApJ...430L.109Y); 11 = Genzel et al. (2010MNRAS.407.2091G); 12 = Oosterloo et al. (2010MNRAS.409..500O); 13 = Irwin et al. (1987ApJ...313L..91I); 14 = van Driel & van Woerden (1991A&A...243...71V); 15 = Sage & Welch (2006ApJ...644..850S); 16 = Knapp & Raimond (1984A&A...138...77K); 17 = Cox et al. (2001AJ....121..692C); 18 = this-work.
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 09-Nov-2012
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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