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174 results on '"Takeuchi, T. T."'

151. A dust emission model of Lyman-break galaxies

Author

Takeuchi, T. T., Ishii, T. T., Takeuchi, T. T., and Ishii, T. T.

Abstract

Lyman-break galaxies (LBGs) contain a non-negligible amount of dust. Takeuchi (2003a, MNRAS, 343, 839) (T03) constructed a model of the infrared spectral energy distribution (SED) for very young galaxies by taking into account the dust size distribution in the early stage of galaxy evolution, which can be different from that of present-day evolved galaxies. We applied the T03 model to LBGs and constructed their expected SED. In order to examine the grain size distribution of dust, we calculated the SEDs based on two distinct types of the distribution models: a single-sized distribution and a power-law distribution with a slope of ${\rm d}N/{\rm d}a \propto a^{-3.5}$. We found that the single-sized and power-law dust size distributions yield a very similar detectability of LBGs at submillimetres (submm). We also found that galaxies with a power-law dust distribution have much less flux in the mid-infrared (MIR) than the other type. By making use of this fact we will be able to explore the dust grain size distribution in high-redshift galaxies through (observer-frame) FIR observations in future observations. We then applied the model to a gravitationally lensed LBG MS 1512-cB58(cB58), a unique probe of the dust emission from LBGs. Observations by SCUBA suggest that the galaxy has hot dust. Our model well reproduced the hot dust temperature under natural physical assumptions for the star formation rate (SFR), starburst age, and the radius of the star forming region in this galaxy. We also examined the detectability of LBGs at submm wavelengths in an eight-hour deep survey by ALMA. The LBG population with an age ${\ga} 10^8\,{\rm yr}$and a ${\rm SFR} \ga 10\,M_\odot ~{\rm yr}^{-1}$can be detected in such a survey. By integrating over their redshifted SEDs with the observed luminosity functions, we obtained the contribution of LBGs to the cosmic infrared background radiation (CIRB). Although they have a non-negligible amount of dust, their contribution was found to be small, especially in the ${\rm FIR} \sim 200\,\mu$m. Thus, we need a strongly obscured population of galaxies which contains a large amount of star formation, at some epoch in the history of the universe.

Published
2004
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152. Properties of star forming galaxies in AKARI Deep Field-South.

Author

Buat, V., Burgarella, D., Giovannoli, E., Kurek, A., Małek, K., Malkan, M., Matsuura, S., Pollo, A., and Takeuchi, T. T.

Subjects
STAR formation, GALACTIC redshift, ASTRONOMICAL photometry, GALACTIC evolution, SPECTRAL energy distribution, INFRARED spectroscopy
Abstract

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 Χ2 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. [ABSTRACT FROM AUTHOR]

Published
2014
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156. The North Ecliptic Pole Wide survey of AKARI: a nearand mid-infrared source catalog.

Author

Kim, S. J., Lee, H. M., Matsuhara, H., Wada, T., Oyabu, S., Im, M., Jeon, Y., Kang, E., Ko, J., Lee, M. G., Takagi, T., Pearson, C., White, G. J., Jeong, W.-S., Serjeant, S., Nakagawa, T., Ohyama, Y., Goto, T., Takeuchi, T. T., and Pollo, A.

Subjects
PHOTOMETRY, TELESCOPES, INFRARED radiation, COSMIC rays, IONIZING radiation
Abstract

We present a photometric catalog of infrared (IR) sources based on the North Ecliptic Pole Wide field (NEP-Wide) survey of AKARI, which is an infrared space telescope launched by Japan. The NEP-Wide survey covered 5.4 deg² area, a nearly circular shape centered on the NEP, using nine photometric filter-bands from 2-25 μm of the Infrared Camera (IRC). Extensive efforts were made to reduce possible false objects due to cosmic ray hits, multiplexer bleeding phenomena around bright sources, and other artifacts. The number of detected sources varied depending on the filter band: with about 109 000 sources being cataloged in the near-infrared (NIR) bands at 2-5 μm, about 20 000 sources in the shorter parts of the mid-infrard (MIR) bands between 7-11 μm, and about 16 000 sources in the longer parts of the MIR band, with ∼4000 sources at 24 μm. The estimated 5σ detection limits are approximately 21 mag (mag) in the 2-5 μm bands, 19.5-19 mag in the 7-11 μm, and 18.8-18.5 mag in the 15-24 μm bands in the AB magnitude scale. The completenesses for those bands were evaluated as a function of magnitude: the 50% completeness limits are about 19.8 mag at 3 μm, 18.6 mag at 9 μm, and 18 mag at 18 μm band, respectively. To construct a reliable source catalog, all of the detected sources were examined by matching them with those in other wavelength data, including optical and ground-based NIR bands. The final band-merged catalog contains about 114 800 sources detected in the IRC filter bands. The properties of the sources are presented in terms of the distributions in various color-color diagrams. [ABSTRACT FROM AUTHOR]

Published
2012
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157. AzTEC/ASTE 1.1-mm survey of the AKARI Deep Field South: source catalogue and number counts.

Author

Hatsukade, B., Kohno, K., Aretxaga, I., Austermann, J. E., Ezawa, H., Hughes, D. H., Ikarashi, S., Iono, D., Kawabe, R., Khan, S., Matsuo, H., Matsuura, S., Nakanishi, K., Oshima, T., Perera, T., Scott, K. S., Shirahata, M., Takeuchi, T. T., Tamura, Y., and Tanaka, K.

Subjects
SUBMILLIMETER astronomy, METAPHYSICAL cosmology, STELLAR mass, STAR formation, INTERSTELLAR medium, TELESCOPES
Abstract

We present results of a 1.1-mm deep survey of the AKARI Deep Field South (ADF-S) with AzTEC mounted on the Atacama Submillimetre Telescope Experiment (ASTE). We obtained a map of 0.25-deg area with an rms noise level of 0.32-0.71 mJy. This is one of the deepest and widest maps thus far at millimetre and submillimetre wavelengths. We uncovered 198 sources with a significance of 3.5σ-15.6σ, providing the largest catalogue of 1.1-mm sources in a contiguous region. Most of the sources are not detected in the far-infrared bands of the AKARI satellite, suggesting that they are mostly at given the detection limits. We constructed differential and cumulative number counts in the ADF-S, the Subaru/ XMM-Newton Deep Field and the SSA 22 field surveyed by AzTEC/ASTE, which provide currently the tightest constraints on the faint end. The integration of the best-fitting number counts in the ADF-S finds that the contribution of 1.1-mm sources with fluxes of 1 mJy to the cosmic infrared background (CIB) at 1.1 mm is 12-16 per cent, suggesting that the large fraction of the CIB originates from faint sources of which the number counts are not yet constrained. We estimate the cosmic star formation rate density contributed by 1.1-mm sources with 1 mJy using the best-fitting number counts in the ADF-S and find that it is lower by about a factor of 5-10 compared to those derived from UV/optically selected galaxies at . The fraction of stellar mass of the present-day universe produced by 1.1-mm sources with 1 mJy at is ∼20 per cent, calculated by the time integration of the star formation rate density. If we consider the recycled fraction of >0.4, which is the fraction of materials forming stars returned to the interstellar medium, the fraction of stellar mass produced by 1.1-mm sources decreases to ≲10 per cent. [ABSTRACT FROM AUTHOR]

Published
2011
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158. AzTEC/ASTE 1.1 mm Deep Surveys: Number Counts and Clustering of Millimeter-bright Galaxies.

Author

Hatsukade, B., Kohno, K., Aretxaga, I., Austermann, J. E., Ezawa, H., Hughes, D. H., Ikarashi, S., Iono, D., Kawabe, R., Matsuo, H., Matsuura, S., Nakanishi, K., Oshima, T., Perera, T., Scott, K. S., Shirahata, M., Takeuchi, T. T., Tamura, Y., Tanaka, K., and Tosaki, T.

Subjects
SUBMILLIMETER astronomy, GALACTIC evolution, GAMMA ray bursts, REDSHIFT, ELLIPTICAL galaxies, STAR formation, METAPHYSICAL cosmology
Abstract

We present number counts and clustering properties of millimeter-bright galaxies uncovered by the AzTEC camera mounted on the Atacama Submillimeter Telescope Experiment (ASTE). We surveyed the AKARI Deep Field South (ADF-S), the Subaru/XMM Newton Deep Field (SXDF), and the SSA22 fields with an area of ∼0.25 deg2 each with an rms noise level of ∼0.4-1.0 mJy. We constructed differential and cumulative number counts, which provide currently the tightest constraints on the faint end. The integration of the best-fit number counts in the ADF-S find that the contribution of 1.1 mm sources with fluxes ≥1 mJy to the cosmic infrared background (CIB) at 1.1 mm is 12-16%, suggesting that the large fraction of the CIB originates from faint sources of which the number counts are not yet constrained. We estimate the cosmic star-formation rate density contributed by 1.1 mm sources with ≥1 mJy using the best-fit number counts in the ADF-S and find that it is lower by about a factor of 5-10 compared to those derived from UV/optically-selected galaxies at z∼2-3. The average mass of dark halos hosting bright 1.1 mm sources was calculated to be 1013-1014 M⊙. Comparison of correlation lengths of 1.1 mm sources with other populations and with a bias evolution model suggests that dark halos hosting bright 1.1 mm sources evolve into systems of clusters at present universe and the 1.1 mm sources residing the dark halos evolve into massive elliptical galaxies located in the center of clusters. [ABSTRACT FROM AUTHOR]

Published
2010
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159. A graph-theoretical approach for comparison of observational galaxy distributions with cosmological N-body simulations

Author

Ueda, H., Takeuchi, T. T., and Itoh, M.

Abstract

Using a graph-theoretical approach, we compared the galaxy distributions in a flux-limited galaxy sample extracted from the Lyon-Meudon Extragalactic Database (”the LEDA subsample”) with those in cosmological $N$-body simulations. To derive information on the density parameter of our Universe, we used CDM simulations with ($\Omega_{\rm 0}$, $\lambda_{\rm 0}) = (0.1$, 0.9), (0.5, 0.5), (1.0, 0.0), and prepared artificial samples. Constellation graphs were constructed from the galaxy distributions in the LEDA subsample and those in these artificial samples, and graph theory was applied. For statistical comparison, the mean absolute deviations of the distribution functions of the eigenvalues of the adjacency matrices were calculated. From our analysis we found that a low-density parameter is preferable, although the LEDA subsample we used in this study is not deep enough to provide a definite estimate of the cosmological parameter set of the Universe.

Published
2003

162. Evolution of infrared luminosity functions of galaxies in the AKARI NEP-deep field: revealing the cosmic star formation history hidden by dust

Author

Goto, T., Takagi, T., Matsuhara, H., Takeuchi, T. T., Pearson, C., Wada, T., Nakagawa, T., Ilbert, O., Le Floc'h, E., Oyabu, S., Ohyama, Y., Malkan, M., Lee, H. M., Lee, M. G., Inami, H., Hwang, N., Hanami, H., Im, M., Imai, K., Ishigaki, T., Serjeant, S., Shim, H., Goto, T., Takagi, T., Matsuhara, H., Takeuchi, T. T., Pearson, C., Wada, T., Nakagawa, T., Ilbert, O., Le Floc'h, E., Oyabu, S., Ohyama, Y., Malkan, M., Lee, H. M., Lee, M. G., Inami, H., Hwang, N., Hanami, H., Im, M., Imai, K., Ishigaki, T., Serjeant, S., and Shim, H.

Abstract

Aims. Dust-obscured star-formation increases with increasing intensity and increasing redshift. We aim to reveal the cosmic starformation history obscured by dust using deep infrared observation with AKARI. Methods. We constructed restframe 8 μm, 12 μm, and total infrared (TIR) luminosity functions (LFs) at 0.15 < z < 2.2 using 4128 infrared sources in the AKARI NEP-deep field. A continuous filter coverage in the mid-IR wavelength (2.4, 3.2, 4.1, 7, 9, 11, 15, 18, and 24 μm) by the AKARI satellite allowed us to estimate restframe 8 μm and 12 μm luminosities without using a large extrapolation based on an SED fit, which was the largest uncertainty in previous work. Results. We find that all 8 μm (0.38 < z < 2.2), 12 μm (0.15 < z < 1.16), and TIR LFs (0.2 < z < 1.6) show continuous and strong evolution toward higher redshift. Our direct estimate of 8 μm LFs is useful since previous work often had to use a large extrapolation from the Spitzer 24 μm to 8 μm, where SED modeling is more difficult because of the PAH emissions. In terms of cosmic infrared luminosity density (ΏIR), which was obtained by integrating analytic fits to the LFs, we find good agreement with previous work at z < 1.2. We find the ΏIR evolves as ∝(1 + z)4.4±1.0. When we separate contributions to ΏIR by LIRGs and ULIRGs, we found moreIR luminous sources are increasingly more important at higher redshift. We find that the ULIRG (LIRG) contribution increases by a factor of 10 (1.8) from z = 0.35 to z = 1.4.

163. Environmental dependence of 8 μm luminosity functions of galaxies atz~ 0.8: comparison between RXJ1716.4+6708 and the AKARI NEP-deep field

Author

Goto, T., Koyama, Y., Wada, T., Pearson, C., Matsuhara, H., Takagi, T., Shim, H., Im, M., Lee, M. G., Inami, H., Malkan, M., Okamura, S., Takeuchi, T. T., Serjeant, S., Kodama, T., Nakagawa, T., Oyabu, S., Ohyama, Y., Lee, H. M., Hwang, N., Hanami, H., Imai, K., Ishigaki, T., Goto, T., Koyama, Y., Wada, T., Pearson, C., Matsuhara, H., Takagi, T., Shim, H., Im, M., Lee, M. G., Inami, H., Malkan, M., Okamura, S., Takeuchi, T. T., Serjeant, S., Kodama, T., Nakagawa, T., Oyabu, S., Ohyama, Y., Lee, H. M., Hwang, N., Hanami, H., Imai, K., and Ishigaki, T.

Abstract

Aims. We aim to reveal environmental dependence of infrared luminosity functions (IR LFs) of galaxies at z ~ 0.8 using the AKARI satellite. AKARI's wide field of view and unique mid-IR filters help us to construct restframe 8 μm LFs directly without relying on SED models. Methods. We construct restframe 8 μm IR LFs in the cluster region RXJ1716.4+6708 at z = 0.81, and compare them with a blank field using the AKARI north ecliptic pole deep field data at the same redshift. AKARI's wide field of view (10' × 10') is suitable to investigate wide range of galaxy environments. AKARI's 15 μm filter is advantageous here since it directly probes restframe 8 μm at z ~ 0.8, without relying on a large extrapolation based on a SED fit, which was the largest uncertainty in previous work. Results. We have found that cluster IR LFs at restframe 8 μm have a factor of 2.4 smaller L* and a steeper faint-end slope than that of the field. Confirming this trend, we also found that faint-end slopes of the cluster LFs becomes flatter and flatter with decreasing local galaxy density. These changes in LFs cannot be explained by a simple infall of field galaxy population into a cluster. Physics that can preferentially suppress IR luminous galaxies in high density regions is required to explain the observed results.

164. The North Ecliptic Pole Wide survey of AKARI: a near- and mid-infrared source catalog

Author

Kim, S. J., Lee, H. M., Matsuhara, H., Wada, T., Oyabu, S., Im, M., Jeon, Y., Kang, E., Ko, J., Lee, M. G., Takagi, T., Pearson, C., White, G., Jeong, W.-S., Serjeant, S., Nakagawa, T., Ohyama, Y., Goto, T., Takeuchi, T. T., Pollo, A., Solarz, A., Pȩpiak, A., Kim, S. J., Lee, H. M., Matsuhara, H., Wada, T., Oyabu, S., Im, M., Jeon, Y., Kang, E., Ko, J., Lee, M. G., Takagi, T., Pearson, C., White, G., Jeong, W.-S., Serjeant, S., Nakagawa, T., Ohyama, Y., Goto, T., Takeuchi, T. T., Pollo, A., Solarz, A., and Pȩpiak, A.

Abstract

We present a photometric catalog of infrared (IR) sources based on the North Ecliptic Pole Wide field (NEP-Wide) survey of AKARI, which is an infrared space telescope launched by Japan. The NEP-Wide survey covered 5.4 deg2 area, a nearly circular shape centered on the NEP, using nine photometric filter-bands from 2−25 μm of the Infrared Camera (IRC). Extensive efforts were made to reduce possible false objects due to cosmic ray hits, multiplexer bleeding phenomena around bright sources, and other artifacts. The number of detected sources varied depending on the filter band: with about 109 000 sources being cataloged in the near-infrared (NIR) bands at 2−5 μm, about 20 000 sources in the shorter parts of the mid-infrard (MIR) bands between 7−11 μm, and about 16 000 sources in the longer parts of the MIR band, with ~4000 sources at 24 μm. The estimated 5σ detection limits are approximately 21 mag (mag) in the 2−5 μm bands, 19.5−19 mag in the 7−11 μm, and 18.8−18.5 mag in the 15−24 μm bands in the AB magnitude scale. The completenesses for those bands were evaluated as a function of magnitude: the 50% completeness limits are about 19.8 mag at 3 μm, 18.6 mag at 9 μm, and 18 mag at 18 μm band, respectively. To construct a reliable source catalog, all of the detected sources were examined by matching them with those in other wavelength data, including optical and ground-based NIR bands. The final band-merged catalog contains about 114 800 sources detected in the IRC filter bands. The properties of the sources are presented in terms of the distributions in various color–color diagrams.

165. Clustering of the AKARI NEP deep field 24μm selected galaxies

Author

Solarz, A., Pollo, A., Takeuchi, T. T., Małek, K., Matsuhara, H., White, G. J., Pȩpiak, A., Goto, T., Wada, T., Oyabu, S., Takagi, T., Ohyama, Y., Pearson, C. P., Hanami, H., Ishigaki, T., Malkan, M., Solarz, A., Pollo, A., Takeuchi, T. T., Małek, K., Matsuhara, H., White, G. J., Pȩpiak, A., Goto, T., Wada, T., Oyabu, S., Takagi, T., Ohyama, Y., Pearson, C. P., Hanami, H., Ishigaki, T., and Malkan, M.

Abstract

Aims. We present a method of selection of 24 μm galaxies from the AKARI north ecliptic pole (NEP) deep field down to 150 μJy and measurements of their two-point correlation function. We aim to associate various 24 μm selected galaxy populations with present day galaxies and to investigate the impact of their environment on the direction of their subsequent evolution. Methods. We discuss using of Support Vector Machines (SVM) algorithm applied to infrared photometric data to perform star-galaxy separation, in which we achieve an accuracy higher than 80%. The photometric redshift information, obtained through the CIGALE code, is used to explore the redshift dependence of the correlation function parameter (r0) as well as the linear bias evolution. This parameter relates galaxy distribution to the one of the underlying dark matter. We connect the investigated sources to their potential local descendants through a simplified model of the clustering evolution without interactions. Results. We observe two different populations of star-forming galaxies, at zmed ∼ 0.25, zmed ∼ 0.9. Measurements of total infrared luminosities (LTIR) show that the sample at zmed ∼ 0.25 is composed mostly of local star-forming galaxies, while the sample at zmed ∼ 0.9 is composed of luminous infrared galaxies (LIRGs) with LTIR ∼ 1011.62 L⨀. We find that dark halo mass is not necessarily correlated with the LTIR: for subsamples with LTIR = 1011.15 L⨀ at zmed ∼ 0.7 we observe a higher clustering length (r0 = 6.21 ± 0.78 [h−1Mpc]) than for a subsample with mean LTIR = 1011.84 L⨀ at zmed ∼ 1.1 (r0 = 5.86 ± 0.69 h−1Mpc).

166. SPICA deep cosmological survey: from AKARI to SPICA

Author

Shirahata, M., Matsuura, S., Matsuhara, H., Takagi, T., Oyabu, S., Wada, T., Nakagawa, T., Kawada, M., Takeuchi, T. T., Hatsukade, B., Kohno, K., Pearson, C. P., Serjeant, S., White, G., Shirahata, M., Matsuura, S., Matsuhara, H., Takagi, T., Oyabu, S., Wada, T., Nakagawa, T., Kawada, M., Takeuchi, T. T., Hatsukade, B., Kohno, K., Pearson, C. P., Serjeant, S., and White, G.

Abstract

On the basis of the results of the AKARI far-infrared deep surveys, we propose a multi-wavelength far-infrared deep cosmological survey with SAFARI on SPICA. We have carried out a far-infrared deep cosmological survey with AKARI, and successfully obtained the galaxy counts and new limits on the absolute brightness of the cosmic far-infrared background. These results provide strong constraints on evolutionary scenarios, and suggest the necessity for a new model to explain galaxy evolution. Thanks to the excellent sensitivity and spatial resolution of SPICA/SAFARI, we will be able to resolve the cosmic infrared background into individual objects with 3 times or more higher spatial resolution than that of AKARI, and will also be able to conduct infrared photometry and spectroscopy on those ob jects. The far-infrared deep survey with SPICA/SAFARI will be an ideal opportunity to reveal the origin of the cosmic far-infrared background residual brightness and fluctuations. These observation will allow us to reveal the star formation history in the early Universe without the uncertainty of dust attenuation, which is essential if we are to understand the process of galaxy formation.

167. SPICA deep cosmological survey: from AKARI to SPICA

Author

Shirahata, M., Matsuura, S., Matsuhara, H., Takagi, T., Oyabu, S., Wada, T., Nakagawa, T., Kawada, M., Takeuchi, T. T., Hatsukade, B., Kohno, K., Pearson, C. P., Serjeant, S., White, G., Shirahata, M., Matsuura, S., Matsuhara, H., Takagi, T., Oyabu, S., Wada, T., Nakagawa, T., Kawada, M., Takeuchi, T. T., Hatsukade, B., Kohno, K., Pearson, C. P., Serjeant, S., and White, G.

Abstract

On the basis of the results of the AKARI far-infrared deep surveys, we propose a multi-wavelength far-infrared deep cosmological survey with SAFARI on SPICA. We have carried out a far-infrared deep cosmological survey with AKARI, and successfully obtained the galaxy counts and new limits on the absolute brightness of the cosmic far-infrared background. These results provide strong constraints on evolutionary scenarios, and suggest the necessity for a new model to explain galaxy evolution. Thanks to the excellent sensitivity and spatial resolution of SPICA/SAFARI, we will be able to resolve the cosmic infrared background into individual objects with 3 times or more higher spatial resolution than that of AKARI, and will also be able to conduct infrared photometry and spectroscopy on those ob jects. The far-infrared deep survey with SPICA/SAFARI will be an ideal opportunity to reveal the origin of the cosmic far-infrared background residual brightness and fluctuations. These observation will allow us to reveal the star formation history in the early Universe without the uncertainty of dust attenuation, which is essential if we are to understand the process of galaxy formation.

170. Environmental dependence of 8  μm luminosity functions of galaxies at z~ 0.8***

Author

Goto, T., Koyama, Y., Wada, T., Pearson, C., Matsuhara, H., Takagi, T., Shim, H., Im, M., Lee, M. G., Inami, H., Malkan, M., Okamura, S., Takeuchi, T. T., Serjeant, S., Kodama, T., Nakagawa, T., Oyabu, S., Ohyama, Y., Lee, H. M., Hwang, N., Hanami, H., Imai, K., and Ishigaki, T.

Abstract

Aims. We aim to reveal environmental dependence of infrared luminosity functions (IR LFs) of galaxies at z~ 0.8 using the AKARI satellite. AKARI's wide field of view and unique mid-IR filters help us to construct restframe 8 μm LFs directly without relying on SED models. Methods. We construct restframe 8 μm IR LFs in the cluster region RXJ1716.4+6708 at z= 0.81, and compare them with a blank field using the AKARI north ecliptic pole deep field data at the same redshift. AKARI's wide field of view (10'× 10') is suitable to investigate wide range of galaxy environments. AKARI's 15 μm filter is advantageous here since it directly probes restframe 8 μm at z~ 0.8, without relying on a large extrapolation based on a SED fit, which was the largest uncertainty in previous work. Results. We have found that cluster IR LFs at restframe 8 μm have a factor of 2.4 smaller $L^*$and a steeper faint-end slope than that of the field. Confirming this trend, we also found that faint-end slopes of the cluster LFs becomes flatter and flatter with decreasing local galaxy density. These changes in LFs cannot be explained by a simple infall of field galaxy population into a cluster. Physics that can preferentially suppress IR luminous galaxies in high density regions is required to explain the observed results.

Published
2010

171. Radio emission from dusty galaxies observed by AKARI.

Author

Pe,piak, A., Polloa, A., Takeuchi, T. T., Solarz, A., and Jurusik, W.

Subjects
*SOLAR radio emission, *INTERPLANETARY dust, *ASTRONOMICAL observations, *GALACTIC nuclei, *STAR formation, UNIVERSE
Abstract

We probe radio-infrared correlation for two samples of extragalactic sources from the local Universe from the AKARI All-Sky Catalogue. The first, smaller sample (1053 objects) was constructed by the cross-correlation of the AKARI/FIS All-Sky Survey Bright Source Catalogue, the AKARI IRC All-Sky Survey Point Source Catalogue and the NRAO VLA Sky Survey, i.e. it consists of sources detected in the mid- and far-infrared by AKARI, and at the 1.4 GHz radio frequency by NRAO. The second, larger sample (13,324 objects) was constructed by the cross-correlation of only the AKARI/FIS All-Sky Survey Bright Source Catalogue and the NRAO VLA Sky Survey, i.e. it consists of sources detected in the far-infrared and radio, without a condition to be detected in the mid-infrared. Additionally, all objects in both samples were identified as galaxies in the NED and/or SIMBAD databases, and a part of them is known to host active galactic nuclei (AGNs). For the present analysis, we have restricted our samples only to sources with known redshift z . In this paper, we analyse the far-infrared-radio correlation for both of these samples. We compare the ratio of infrared and radio emission from normal star-forming dusty galaxies and AGNs in both samples. For the smaller sample we obtained =2.14 for AGNs and =2.27 for normal galaxies, while for the larger sample =2.15 for AGNs and =2.22 for normal galaxies. An average value of the slope in both samples is ∼2.2, which is consistent with the previous measurements from the literature. [ABSTRACT FROM AUTHOR]

Published
2014
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172. The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Author

Małgorzata Siudek, G. De Lucia, Daniela Vergani, P. Franzetti, C. Adami, Stéphane Arnouts, M. Scodeggio, V. Le Brun, A. Zanichelli, T. Moutard, Julien Bel, Lauro Moscardini, Chris P. Haines, D. Bottini, D. Maccagni, Iary Davidzon, Enzo Branchini, Tsutomu T. Takeuchi, Lidia Tasca, Jean Coupon, Olga Cucciati, Bianca Garilli, Olivier Ilbert, G. Zamorani, A. Cappi, Agnieszka Pollo, Luigi Guzzo, Katarzyna Małek, A. Iovino, J. Krywult, Ummi Abbas, Tomasz Krakowski, Benjamin R. Granett, M. Bolzonella, Alexander Fritz, Federico Marulli, O. Le Fèvre, M. Polletta, S. de la Torre, Rita Tojeiro, Siudek, M., Małek, K., Pollo, A., Krakowski, T., Iovino, A., Scodeggio, M., Moutard, T., Zamorani, G., Guzzo, L., Garilli, B., Granett, B.R., Bolzonella, M., De La Torre, S., Abbas, U., Adami, C., Bottini, D., Cappi, A., Cucciati, O., Davidzon, I., Franzetti, P., Fritz, A., Krywult, J., Le Brun, V., Le Fèvre, O., MacCagni, D., Marulli, F., Polletta, M., Tasca, L.A.M., Tojeiro, R., Vergani, D., Zanichelli, A., Arnouts, S., Bel, J., Branchini, E., Coupon, J., De Lucia, G., Ilbert, O., Haines, C.P., Moscardini, L., Takeuchi, T.T., Center for Theoretical Physics, Polish Academy of Sciences , Al. Lotników 32/46, 02-668 Warsaw, Poland (CFT PAN), National Centre for Nuclear Research (Warszawa), INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Università degli Studi di Milano [Milano] (UNIMI), INAF - Osservatorio Astrofisico di Torino (OATo), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Jan Kochanowski University, Alma Mater Studiorum University of Bologna (UNIBO), Istituto Nazionale di Fisica Nucleare, Sezione di Bologna (INFN, Sezione di Bologna), Istituto Nazionale di Fisica Nucleare (INFN), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), University of St Andrews [Scotland], Istituto di Radioastronomia [Bologna] (IRA), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), CPT - E3 Cosmologie, Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi Roma Tre, Istituto Nazionale di Fisica Nucleare, Sezione di Roma 3 (INFN, Sezione di Roma 3), INAF - Osservatorio Astronomico di Roma (OAR), University of Geneva [Switzerland], INAF - Osservatorio Astronomico di Trieste (OAT), Nagoya University, Università degli Studi di Milano = University of Milan (UNIMI), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Università degli Studi Roma Tre = Roma Tre University (ROMA TRE), Université de Genève = University of Geneva (UNIGE), Granett, B. R., Maccagni, D., Tasca, L. A. M., Haines, C. P., Takeuchi, T. T., ITA, USA, GBR, FRA, and DEU

Subjects
Active galactic nucleus, Galaxies: statistics, Astrophysics, Galaxies: groups: general, Astrophysics::Cosmology and Extragalactic Astrophysics, Parameter space, 01 natural sciences, star formation [Galaxies], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Sequence, Galaxies: star formation, 010308 nuclear & particles physics, Spectral density, Galaxies: evolution, Astronomy and Astrophysics, Galaxy: fundamental parameters, Astronomy and Astrophysic, Redshift survey, evolution [Galaxies], Galaxies: stellar content, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, Space and Planetary Science, Unsupervised learning, stellar content [Galaxies]
Abstract

Various galaxy classification schemes have been developed so far to constrain the main physical processes regulating evolution of different galaxy types. In the era of a deluge of astrophysical information and recent progress in machine learning, a new approach to galaxy classification becomes imperative. We employ a Fisher Expectation-Maximization unsupervised algorithm working in a parameter space of 12 rest-frame magnitudes and spectroscopic redshift. The model (DBk) and the number of classes (12) were established based on the joint analysis of standard statistical criteria and confirmed by the analysis of the galaxy distribution with respect to a number of classes and their properties. This new approach allows us to classify galaxies based just on their redshifts and UV-NIR spectral energy distributions. The FEM unsupervised algorithm has automatically distinguished 12 classes: 11 classes of VIPERS galaxies and an additional class of broad-line AGNs. After a first broad division into blue, green and red categories we obtained a further sub-division into three red, three green, and five blue galaxy classes. The FEM classes follow the galaxy sequence from the earliest to the latest types that is reflected in their colours (which are constructed from rest-frame magnitudes used in classification procedure) but also their morphological, physical, and spectroscopic properties (not included in the classification scheme). We demonstrate that the members of each class share similar physical and spectral properties. In particular, we are able to find three different classes of red passive galaxy populations. Thus, we demonstrate the potential of an unsupervised approach to galaxy classification and we retrieve the complexity of galaxy populations at z~0.7, a task that usual simpler colour-based approaches cannot fulfil., Comment: published in A&A, 27 pages, 10 figures, 4 appendixes. Please contact Malgorzata Siudek (msiudek@ifae.es) if you are interested in the catalogue

Published
2018
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173. The VIMOS Public Extragalactic Redshift Survey (VIPERS): Star formation history of passive red galaxies

Author

D. Bottini, A. Zanichelli, A. Marchetti, M. Polletta, Agnieszka Pollo, O. Le Fèvre, Daniela Vergani, Rita Tojeiro, I. Davidzon, V. Le Brun, O. Ilbert, M. Bolzonella, Adriana Gargiulo, O. Cucciati, L. A. M. Tasca, C. Adami, S. de la Torre, Tsutomu T. Takeuchi, Lauro Moscardini, Julien Bel, P. Franzetti, M. Scodeggio, G. Zamorani, G. De Lucia, J. Krywult, B. R. Granett, A. Iovino, Małgorzata Siudek, B. Garilli, Alexander Fritz, Luigi Guzzo, Federico Marulli, U. Abbas, S. Arnouts, Enzo Branchini, A. Cappi, C. P. Haines, D. Maccagni, Katarzyna Małek, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Siudek, M, Małek, K., Scodeggio, M., Garilli, B., Pollo, A., Haines, C.P., Fritz, A., Bolzonella, M., De La Torre, S., Granett, B.R., Guzzo, L., Abbas, U., Adami, C., Bottini, D., Cappi, A., Cucciati, O., De Lucia, G., Davidzon, I., Franzetti, P., Iovino, A., Krywult, J., Le Brun, V., Le Fèvre, O., Maccagni, D., Marchetti, A., Marulli, F., Polletta, M., Tasca, L.A.M., Tojeiro, R., Vergani, D., Zanichelli, A., Arnouts, S., Bel, J., Branchini, E., Ilbert, O., Gargiulo, A., Moscardini, L., Takeuchi, T.T., Zamorani, G., Haines, C. P., Granett, B. R., Tasca, L. A. M., Branchini, ENZO FRANCO, Takeuchi, T. T., University of St Andrews. School of Physics and Astronomy, ITA, GBR, FRA, JPN, and POL

Subjects
Stellar mass, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), 01 natural sciences, Spectral line, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Galaxies: evolution, Galaxies: stellar content, Astronomy and Astrophysics, Space and Planetary Science, 3rd-DAS, Astronomy and Astrophysic, Redshift survey, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Stars, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), stellar content [Galaxies], Astrophysics::Earth and Planetary Astrophysics, uploaded-in-3-months-elsewhere
Abstract

We trace the evolution and the star formation history of passive galaxies, using a subset of the VIMOS Public Extragalactic Redshift Survey (VIPERS). We extracted from the VIPERS survey a sample of passive galaxies in the redshift range 0.4, Comment: 17 pages, 12 figures, 1 table, accepted to A&A

Published
2017
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174. The VIMOS Public Extragalactic Redshift Survey (VIPERS). The coevolution of galaxy morphology and colour to z~1

Author

C. Adami, Agnieszka Pollo, V. Le Brun, O. Ilbert, Julien Bel, Enzo Branchini, A. Cappi, A. Iovino, O. Cucciati, Katarzyna Małek, D. Bottini, M. Scodeggio, A. Zanichelli, S. de la Torre, Daniela Vergani, O. Le Fèvre, P. Franzetti, H. J. McCracken, G. Zamorani, I. Davidzon, U. Abbas, D. Maccagni, L. A. M. Tasca, Adriana Gargiulo, G. De Lucia, Jean Coupon, C. P. Haines, Luigi Guzzo, B. Garilli, M. Polletta, Rita Tojeiro, B. R. Granett, M. Bolzonella, Tsutomu T. Takeuchi, J. Krywult, Lauro Moscardini, S. Arnouts, Alexander Fritz, Federico Marulli, University of St Andrews. School of Physics and Astronomy, Krywult, J., Tasca, L. A. M., Pollo, A., Vergani, D., Bolzonella, M., Davidzon, I., Iovino, A., Gargiulo, A., Haines, C. P., Scodeggio, M., Guzzo, L., Zamorani, G., Garilli, B., Granett, B. R., De La Torre, S., Abbas, U., Adami, C., Bottini, D., Cappi, A., Cucciati, O., Franzetti, P., Fritz, A., Le Brun, V., Le Fèvre, O., Maccagni, D., Małek, K., Marulli, F., Polletta, M., Tojeiro, R., Zanichelli, A., Arnouts, S., Bel, J., Branchini, ENZO FRANCO, Coupon, J., De Lucia, G., Ilbert, O., Mccracken, H. J., Moscardini, L., Takeuchi, T. T., Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), INAF- Milano, Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique Théorique - UMR 7332 (CPT), Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), CPT - E3 Cosmologie, Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Tasca, L.A.M., Haines, C.P., Granett, B.R., Branchini, E., Mccracken, H.J., and Takeuchi, T.T.

Subjects
Galaxies: statistics, Cosmology: observations, Galaxies: evolution, Galaxies: general, Galaxies: structure, Astronomy and Astrophysics, Space and Planetary Science, structure [Galaxies], FOS: Physical sciences, observation [Cosmology], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology: observation, 01 natural sciences, Imaging data, Photometry (optics), statistics [Galaxies], evolution, 0103 physical sciences, QB Astronomy, Physics::Atomic Physics, structure, observations [Cosmology], 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, Galaxies: statistic, statistic [Galaxies], 010308 nuclear & particles physics, High Energy Physics::Phenomenology, general [Galaxies], 3rd-DAS, Astronomy and Astrophysic, evolution [Galaxies], Redshift survey, galaxies: general, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Early type, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], QC Physics, statistics, Astrophysics of Galaxies (astro-ph.GA), cosmology: observations, Cosmic time
Abstract

We explore the evolution of the statistical distribution of galaxy morphological properties and colours over the redshift range $0.5, Comment: 18 pages, 13 figures

Published
2016
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