Dusty Universe viewed by AKARI far infrared detector

Małek, K.; Pollo, A.; Takeuchi, Tsutomu T.; Giovannoli, É.; Buat, V.; Burgarella, D.; Malkan, M. A.; Kurek, A. R.

doi:10.5047/eps.2013.06.005

Cited by 4 publications

(7 citation statements)

References 43 publications

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“…We divided our sample into three groups with respect to total infrared luminosity: ultraluminous infrared galaxies (ULIRGS, with high IR luminosity, L TIR > 10 12 L ), luminous infrared galaxies (LIRGS, with total infrared luminosity in the range 10 11 L < L TIR < 10 12 L ), and the rest of the galaxies with L TIR < 10 11 L . In our sample we found 17 galaxies classified as ULIRGs (9.7% of sources), and 31 LIRGS (16.1% of the total number of sources) (Małek et al 2013). All of the galaxies that belong to (U)LIRGs samples have only photometric redshift estimated by CIGALE.…”

Section: Average Sedmentioning

confidence: 74%

“…The result might be biased by uncertainty of photometric redshift estimation and the error of zλ max found for three different samples. More detailed description of (U)LIRGs samples can be found in Małek et al (2013). In Table 5, we summarize the main physical parameters for (U)LIRGS and the rest of our sample.…”

Section: Average Sedmentioning

confidence: 99%

“…The average rest-frame SED normalized at 90 μm of ULIRGS (dashed line), LIRGS (dotted line) and remaining galaxies (solid line). Taken from (Małek et al 2013). Table 5.…”

Section: Parameters Obtained From Galaxy Sed Fitsmentioning

confidence: 99%

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Properties of star forming galaxies in AKARI Deep Field-South

Małek

Pollo

Takeuchi

et al. 2014

A&A

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Aims. The main aim of this work is the characterization of physical properties of galaxies detected in the far-infrared (FIR) in the AKARI Deep Field-South (ADF-S) survey. Methods. Starting from a catalog of the 1000 brightest ADF-S sources in the WIDE-S (90 μm) AKARI band, we constructed a subsample of galaxies with spectral coverage from the ultraviolet to the FIR. We then analyzed the multiwavelength properties of this 90 μm selected sample of galaxies. For galaxies without known spectroscopic redshifts we computed photometric redshifts using the codes Photometric Analysis for Redshift Estimate (Le PHARE) and Code Investigating GALaxy Emission (CIGALE), tested these photometric redshifts using spectroscopic redshifts, and compared the performances of both codes. To test the reliability of parameters obtained by fitting spectral energy distributions, a mock catalogue was generated. Results. We built a large multiwavelength catalog of more than 500 ADF-S galaxies. We successfully fitted spectral energy distributions of 186 galaxies with χ 2 min < 4, and analyzed the output parameters of the fits. We conclude that our sample consists mostly of nearby actively star-forming galaxies, and all our galaxies have a relatively high metallicity. We estimated photometric redshifts for 113 galaxies from the whole ADF-S sample. Comparing the performance of Le PHARE and CIGALE, we found that CIGALE gives more reliable redshift estimates for our galaxies, which implies that including the IR photometry allows for substantial improvement of photometric redshift estimation.

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Section: Average Sedmentioning

confidence: 74%

Section: Average Sedmentioning

confidence: 99%

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Properties of star forming galaxies in AKARI Deep Field-South

Małek

Pollo

Takeuchi

et al. 2014

A&A

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“…For our analysis we used one of the deep AKARI surveys, ADF-S, and the catalogs published by Małek et al (2010) and Małek et al (2013), completed by spectroscopic redshifts and Herschel/SPIRE data.…”

Section: Discussionmentioning

confidence: 99%

“…This sample was previously used for a more general analysis of properties of active, star forming FIR sources (Małek et al 2010(Małek et al , 2013. In the present paper, new measurements, mainly from GALEX, Spitzer/MIPS sample (Rieke et al 2004, taken from public database and for a part of ADF-S sources, measured directly from images by ourselves), WISE (Wright et al 2010), and ATCA-ADFS survey (White et al 2012), as well as new spectroscopic data not included in our previous studies (Sedgwick et al 2011;Jones et al 2009), were added to create the extended version of our multi-wavelength catalog.…”

Section: Datamentioning

confidence: 99%

[Ultra] luminous infrared galaxies selected at 90μm in the AKARI deep field: a study of AGN types contributing to their infrared emission

Małek

Bankowicz

Pollo

et al. 2017

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Aims. The aim of this work is to characterize physical properties of ultra luminous infrared galaxies (ULIRGs) and luminous infrared galaxies (LIRGs) detected in the far-infrared (FIR) 90 µm band in the AKARI Deep Field-South (ADF-S) survey. In particular, we want to estimate the active galactic nucleus (AGN) contribution to the LIRGs and ULIRGs' infrared emission and which types of AGNs are related to their activity. Methods. We examined 69 galaxies at redshift ≥0.05 detected at 90 µm by the AKARI satellite in the ADF-S, with optical counterparts and spectral coverage from the ultraviolet to the FIR. We used two independent spectral energy distribution fitting codes: one fitting the SED from FIR to FUV (CIGALE) (we use the results from CIGALE as a reference) and gray-body + power spectrum fit for the infrared part of the spectra (CMCIRSED) in order to identify a subsample of ULIRGs and LIRGs, and to estimate their properties. Results. Based on the CIGALE SED fitting, we have found that LIRGs and ULIRGs selected at the 90 µm AKARI band compose ∼56% of our sample (we found 17 ULIRGs and 22 LIRGs, spanning over the redshift range 0.06 < z < 1.23). Their physical parameters, such as stellar mass, star formation rate (SFR), and specific SFR are consistent with the ones found for other samples selected at infrared wavelengths. We have detected a significant AGN contribution to the mid-infrared luminosity for 63% of LIRGs and ULIRGs. Our LIRGs contain Type 1, Type 2, and intermediate types of AGN, whereas for ULIRGs, a majority (more than 50%) of AGN emission originates from Type 2 AGNs. The temperature-luminosity and temperature-mass relations for the dust component of ADF-S LIRGs and ULIRGs indicate that these relations are shaped by the dust mass and not by the increased dust heating. Conclusions. We conclude that LIRGs contain Type 1, Type 2, and intermediate types of AGNs, with an AGN contribution to the mid infrared emission at the median level of 13 ± 3%, whereas the majority of ULIRGs contain Type 2 AGNs, with a median AGN fraction equal to 19 ± 8%.

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Relation of internal attenuation, dust emission, and the size of spiral galaxies

Corredoira

Gutiérrez

2021

A&A

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Aims. Dust in spiral galaxies produces emission in the far-infrared (FIR) and internal absorption in visible wavelengths. However, the relation of the two amounts is not trivial because optical absorption may saturate, but the FIR emission does not. Moreover, the volume concentration of dust plays a role in the relation of absorption and emission, which depends on the size of the galaxy. We explore the relation of these three quantities. Methods. In order to understand the geometrical problem, we developed a model of dust distribution. We also investigated the relation of the three variables with real data of spiral galaxies at z < 0.2 using the spectroscopic Sloan Digital Sky Survey and FIR AKARI survey. Internal absorptions were derived with two different methods: the ratio of emission lines Hα and Hβ, and a previously calibrated relation based on the color variations as a function of absolute magnitude and concentration index. Results. We find that in our low-z sample, the dependence of the average internal attenuation on galaxy size is negligible on average because of the relation of dust mass with size. It allows us to derive the internal attenuation of the galaxy, AV, even when we only know its FIR flux. This attenuation approximately depends on the inclination of the galaxy i as AV̄ = γV̄ log101cos i, where γV is a constant. We found that γV has a maximum value for galaxies of 1.45 ± 0.27 magnitudes. When similar properties of dust are assumed, a general expression can be used at any z: γV̄ = (1.45 ± 0.27)fMexp[−(1.0 ± 0.6)fM] and fM = 7.6 × 10−6 αhR−1.75 × (FFIR/700 Jy) 1.87 × fcosmol.(z); the dependence on the cosmological model is embedded in fcosmol.(z) = dL(z)(Mpc)2(1 + z)(1.75η − 1.87), where η = 2 for cosmologies following Etherington’s relation, dL is the luminosity distance, αhR is the angular size of the scalelength, and FFIR the flux at wavelength 100(1 + z) μm. Conclusions. For cases of nonsaturation (f ≲ 3.6), this might be used as a cosmological test because the factor fcosmol. at high z varies strongly in different cosmologies. Although the present-day sensitivity of FIR or millimeter surveys does not allow us to carry out this cosmological test within the standard model, it may be used in the future, when we can observe galaxies at z = 3−5 with a sensitivity at ∼500 μm better than ∼10 μJy, for instance. For much lower z or different cosmological models, a test might be feasible at present.

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Dusty Universe viewed by AKARI far infrared detector

Cited by 4 publications

References 43 publications

Properties of star forming galaxies in AKARI Deep Field-South

Properties of star forming galaxies in AKARI Deep Field-South

[Ultra] luminous infrared galaxies selected at 90μm in the AKARI deep field: a study of AGN types contributing to their infrared emission

Relation of internal attenuation, dust emission, and the size of spiral galaxies

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