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J/A+A/605/A74  AKARI fluxes of ATLAS3D early-type galaxies     (Kokusho+, 2017)

A star formation study of the ATLAS3D early-type galaxies with the AKARI all-sky survey. Kokusho T., Kaneda H., Bureau M., Suzuki T., Murata K., Kondo A., Yamagishi M. <Astron. Astrophys., 605, A74 (2017)> =2017A&A...605A..74K (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, IR ; Photometry, infrared Keywords: galaxies: elliptical and lenticular, cD - galaxies: ISM - galaxies: photometry - dust, extinction - infrared: galaxies - galaxies: star formation Abstract: The star formation properties of early-type galaxies (ETGs) are currently the subject of considerable interest, particularly whether they differ from the star formation properties of gas-rich spirals. We perform a systematic study of star formation in a large sample of local ETGs with polycyclic aromatic hydrocarbon (PAH) and dust emission, focusing on the star formation rates (SFRs) and star formation efficiencies (SFEs) of the galaxies. Our sample is composed of the 260 ETGs from the ATLAS3D survey, from which we used the cold gas measurements (HI and CO). We estimated the SFRs from stellar, PAH, and dust fits to spectral energy distributions created from new AKARI measurements and with literature data from WISE and 2MASS. The mid-infrared luminosities of non-CO-detected galaxies are well correlated with their stellar luminosities, showing that they trace (circum)stellar dust emission. CO-detected galaxies show an excess above these correlations, uncorrelated with their stellar luminosities, indicating that they likely contain PAHs and dust of interstellar origin. PAH and dust luminosities of CO-detected galaxies show tight correlations with their molecular gas masses; the derived current SFRs are typically 0.01-1M/yr. These SFRs systematically decrease with stellar age at fixed stellar mass, while they correlate nearly linearly with stellar mass at fixed age. The majority of local ETGs follow the same star formation law as local star-forming galaxies and their current SFEs do not depend on either stellar mass or age. Our results clearly indicate that molecular gas is fueling current star formation in local ETGs, which appear to acquire this gas via mechanisms regulated primarily by stellar mass. The current SFEs of local ETGs are similar to those of local star-forming galaxies, indicating that their low SFRs are likely due to smaller cold gas fractions rather than a suppression of star formation. Description: We have conducted a systematic study of star formation in the 260 local ETGs of the ATLAS3D survey, using newly measured IR fluxes from the AKARI all-sky diffuse maps combined with WISE and 2MASS literature data. We estimated the IR luminosities (LPAH, Lwarm, Lcold, and LTIR) of the sample ETGs by decomposing their SEDs with a dust model. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 90 260 AKARI-measured infrared fluxes of all ATLAS3D galaxies tablea2.dat 49 231 Infrared luminosities derived from SED fitting
See also: II/297 : AKARI/IRC mid-IR all-sky Survey (ISAS/JAXA, 2010) II/298 : AKARI/FIS All-Sky Survey Point Source Cat. (ISAS/JAXA, 2010) J/MNRAS/413/813 : ATLAS3D project. I. (Cappellari+, 2011) J/MNRAS/414/888 : ATLAS3D project. III. (Emsellem+, 2011) J/MNRAS/414/940 : ATLAS3D project. IV. (Young+, 2011) J/MNRAS/416/1680 : ATLAS3D project. VII. (Cappellari+, 2011) J/MNRAS/433/2812 : ATLAS3D project. XXIII. (Krajnovic+, 2013) J/MNRAS/446/120 : ATLAS3D project. XXIX (Duc+, 2015) J/MNRAS/448/3484 : ATLAS3D Project. XXX (McDermid+, 2015) Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 10 A10 --- Galaxy Galaxy name 12- 17 F6.2 mJy F9um ?=- AKARI flux at 9um 19- 23 F5.2 mJy e_F9um ? rms uncertainty on F9um 24 A1 --- n_F9um [ab] Note on F9um (1) 26- 32 F7.2 mJy F18um ?=- AKARI flux at 18um 34- 38 F5.2 mJy e_F18um ? rms uncertainty on F18um 39 A1 --- n_F18um [ab] Note on F18um (1) 40- 47 F8.2 mJy F65um ?=- AKARI flux at 65um 49- 54 F6.2 mJy e_F65um ? rms uncertainty on F65um 55 A1 --- n_F65um [ab] Note on F65um (1) 58- 65 F8.2 mJy F90um ?=- AKARI flux at 90um 67- 72 F6.2 mJy e_F90um ? rms uncertainty on F90um 73 A1 --- n_F90um [ab] Note on F90um (1) 75- 82 F8.2 mJy F140um ?=- AKARI flux at 140um 84- 89 F6.2 mJy e_F140um ? rms uncertainty on F140um 90 A1 --- n_F140um [ab] Note on F140um (1)
Note (1): Notes as follows: a = Not observed with AKARI. When possible, the missing 65 and/or 90um flux densities are replaced by IRAS 60 and/or 100um measurements from NED. b = Measurement likely affected by source confusion or instrumental artefact
Byte-by-byte Description of file: tablea2.dat
Bytes Format Units Label Explanations
1- 10 A10 --- Galaxy Galaxy name 12- 17 F6.2 10+34W LPAH PAH luminosity 19- 23 F5.2 10+34W e_LPAH rms uncertainty on LPAH 25- 30 F6.2 10+34W Lwarm Luminosity of warm dust 32- 36 F5.2 10+34W e_Lwarm rms uncertainty on Lwarm 38- 43 F6.2 10+34W Lcold Luminosity of cold dust 45- 49 F5.2 10+34W e_Lcold rms uncertainty on Lcold
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 15-Nov-2017
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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