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Chris Sedgwick,STEPHEN SERJEANT,CHRIS PEARSON,I. Yamamura,S. Makiuti,N. Ikeda,Y. Fukuda,S. Oyabu,T. Koga,S. Amber,Glenn J. White 한국천문학회 2017 天文學論叢 Vol.32 No.1
We have identified 22 quasars in the AKARI far-infrared all-sky Bright Source Catalogue, using a matching radius of < 10 “, and excluding matches which are close to foreground extended sources or cirrus. We have confirmed a relation between quasar optical luminosity and far-infrared luminosity which was found in an earlier study. In addition, we have found that the 11 sources which are at redshift z > 1 are magnified with respect to the predicted far-infrared luminosity, and consider this may be due to gravitational lensing. If confirmed, this would provide a new way to identify lenses; if not, we may have identified an interesting new population of extreme starbursting quasars. %We are currently seeking spectroscopic confirmation of the redshifts and improved imaging for these sources.
HERSCHEL OBSERVATIONS IN THE AKARI NEP FIELD: INITIAL SOURCE COUNTS
Chris Pearson,Ryan Cheale,STEPHEN SERJEANT,Hideo Matsuhara,Glenn J. White,Denis Burgarella,Ivan Valtchanov,Bruno Altieri,David L. Clements,Ros Hopwood 한국천문학회 2017 天文學論叢 Vol.32 No.1
The preliminary data reduction, analysis and first results from the Herschel survey of the AKARI NEP field are presented. Herschel SPIRE observations of the NEP-Wide region and PACS observations of the NEP-Deep region have yielded galaxy catalogues of 4000 and 900 sources respectively down to flux density levels of approximately 15 mJy at 100-250 microns. Source counts produced from these catalogues reach cosmologically significant depths tracing the evolutionary upturn and turnover in the source counts. The source counts are in agreement with other large area surveys carried out with Herschel bridging the gap between the shallow and deep Herschel surveys.
PEARSON CHRIS,LEE HYUNG MOK,TEAM ASTRO-F The Korean Astronomical Society 2003 Journal of The Korean Astronomical Society Vol.36 No.3
ASTRO-F is the next generation Japanese infrared space mission of the Institute of Space and Astronautical Science. ASTRO-F will be dedicated to an All Sky Survey in the far-infrared in 4 bands from 50-200microns with 2 additional mid-infrared bands at 9microns and 20microns. This will be the first all sky survey in the infrared since the ground breaking IRAS mission almost 20 years ago and the first ever survey at 170microns. The All Sky Survey should detect 10's of millions of sources in the far-infrared bands most of which will be dusty luminous and ultra-luminous star forming galaxies, with as many as half lying at redshifts greater than unity. In this contribution, the ASTRO-F mission and its objectives are reviewed and many of the mission expectations are discussed.
AKARI DEEP FIELD SOUTH: SPECTROSCOPIC OBSERVATIONS OF INFRARED SOURCES
Chris Sedgwick,STEPHEN SERJEANT,CHRIS PEARSON,Shuji Matsuura,MAI SHIRAHATA,Hideo Matsuhara,Lucia Marchetti,Glenn J. White,Mattia Vaccari,Ivano Baronchelli,Giulia Rodighiero,Bunyo Hadsukade,David L. Cl 한국천문학회 2017 天文學論叢 Vol.32 No.1
We present a summary of our spectroscopic redshift catalogue of 404 sources in the {\it AKARI} Deep Field South (ADF-S). We have used the AAOmega spectrograph to target mid-infrared and far-infrared sources selected primarily from {\it AKARI} observations in this field for which we were able to obtain optical counterparts. Our sources with identified redshifts include 316 with H$\alpha$ detections at z ≤ 0.345 and 15 sources at z > 1 with MgII or Lyα emission lines. About 13% of our z ≤0.345 sources are dominated by active galactic nuclei (AGN) emission, although many show emission from both star formation and AGNs. The median Balmer decrement is 5.9. Ultra-luminous infrared galaxies (ULIRGs) were found only in the higher-redshift sources. Optical and near infrared data will be available shortly, enabling calibration of the line luminosities and spectral energy distribution (SED) fitting for these sources.
THE SYNERGY OF LARGE AREA SURVEYS WITH AKARI AND HERSCHEL
Pearson, Chris,Serjeant, Stephen,Sedgwick, Chris,White, Glenn J.,Matsuhara, Hideo,Takagi, Toshinobu,Nagisa, Oi,Murata, Kazumi,Nakagawa, Takao,Yamamura, Issei The Korean Astronomical Society 2012 天文學論叢 Vol.27 No.4
The Herschel Space Observatory is the European Space Agency's state of the art infrared space telescope launched into space on 14 May 2009, covering the wavelength range from 70-700 microns with 3 instruments SPIRE, PACS and HIFI. Large area surveys are being carried out by Herschel in the AKARI legacy fields at the North and South Ecliptic Poles and the AKARI All-Sky Survey provides additional synergy with the largest survey with Herschel, H-ATLAS, covering more than 500 square degrees. This paper reports on some of the early results of these synergies between Herschel and AKARI including the first comparison of the AKARI All-Sky Survey number counts with the deeper Herschel surveys.
DETECTION OF Hα EMISSION FROM z>3.5 GALAXIES WITH AKARI-FUHYU NIR SPECTROSCOPY
Sedgwick, Chris,Serjeant, Stephen,Pearson, Chris,Takagi, Toshinobu,Matsuhara, Hideo,Wada, Takehiko,Lee, Hyung Mok,Im, Myungshin,Jeong, Woong-Seob,Oyabu, Shinki,White, Glenn J. The Korean Astronomical Society 2012 天文學論叢 Vol.27 No.4
This paper presents $H{\alpha}$ emission line detections for four galaxies at z > 3.5 made with AKARI as part of the FUHYU mission program. These are the highest-redshift $H{\alpha}$ detections to date in star-forming galaxies. AKARI's unique near-infrared spectroscopic capability has made these detections possible. For two of these galaxies, this represents the first evidence of their redshifts and confirms their physical association with a companion radio galaxy. The star formation rates (SFRs) estimated from the $H{\alpha}$ lines under-predict the SFRs estimated from their far-infrared luminosities by a factor of ~ 2 - 3. We have also detected broad $H{\alpha}$ components in the two radio galaxies which indicate the presence of quasars.
FAR INFRARED ASTRONOMY AFTER SPICA
Bruce Swinyard,Chris Pearson 한국천문학회 2017 天文學論叢 Vol.32 No.1
This paper reviews the requirements for far-infrared astronomy in the period following the SPICA satellite in the late 2020's. We take a very long view of the state of FIR astronomy and what facilities will be required in a twenty year timeframe. We show that spatial resolution to match that of observatories operating in the optical and mid-infrared and the radio will be a necessity. Moreover this high spatial resolution must be combined with high spectral and photometric sensitivity to provide the data required to further our understanding of planetary formation mechanisms, the history of star formation through cosmic time and the feedback between active galactic nuclei and their host galaxies in controlling star formation. We review three possible conceptual mission scenarios and comment on the possibility of realising them in the coming deades.
PROPERTIES OF DUST OBSCURED GALAXIES IN THE NEP-DEEP FIELD
Nagisa Oi,Hideo Matsuhara,CHRIS PEARSON,Veronique Buat,Denis Burgarella,Matt Malkan,Takamitsu Miyaji 한국천문학회 2017 天文學論叢 Vol.32 No.1
We selected 47 DOGs at z ~ 1.5 using optical $R$ (or $r^{'}$), AKARI 18 $\mu$m, and 24 $\mu$m color in the AKARI North Ecliptic Pole (NEP) Deep survey field. Using the colors among 3, 4, 7, and $9\mu$m, we classified them into 3 groups; bump DOGs (23 sources), power-law DOGs (16 sources), and unknown DOGs (8 sources). We built spectral energy distributions (SEDs) with optical to far-infrared photometric data and investigated their properties using SED fitting method. We found that AGN activity such as a AGN contribution to the infrared luminosity and a Chandra detection rate for bump and power-law DOGs are significantly different, while stellar component properties like a stellar mass and a star-formation rate are similar to each other. A specific star-formation rate range of power-law DOGs is slightly higher than that of bump DOGs with wide overlap. Herschel/PACS detection rates are almost the same between bump and power-law DOGs. On the other hand SPIRE detection rates show large differences between bump and power-law DOGs. These results might be explained by differences in dust temperatures. Both groups of DOGs host hot and/or warm dust (~ 50 Kelvin), and many bump DOGs contain cooler dust ($\hspace{0.3em}\raisebox{0.4ex}{$<$}\hspace{-0.75em}\raisebox{-.7ex}{$\sim$}\hspace{0.3em}$ 30 Kelvin).