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 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:
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FileName Lrecl Records Explanations
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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
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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
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Bytes Format Units Label Explanations
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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)
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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
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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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
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 15-Nov-2017