SpringerLink
Forum Springer Astron. Astrophys.
Forum Whats New Search Orders


Astron. Astrophys. 361, 407-414 (2000)


Table of Contents
Available formats: HTML | PDF | (gzipped) PostScript

ISO deep far-infrared survey in the "Lockman Hole"

II. Power spectrum analysis: evidence of a strong evolution in number counts * **

H. Matsuhara 1, K. Kawara 2, Y. Sato 1, Y. Taniguchi 3, H. Okuda 1, T. Matsumoto 1, Y. Sofue 2, K. Wakamatsu 4, L.L. Cowie 5, R.D. Joseph 5 and D.B. Sanders 5

1 The Institute of Space and Astronautical Science (ISAS), 3-1-1 Yoshinodai, Sagamihara, Kanagawa, 229-8510, Japan
2 Institute of Astronomy, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan
3 Astronomical Institute, Tohoku University, Aoba, Sendai 980-8578, Japan
4 Faculty of Engineering, Gifu University, Gifu 501-1193, Japan
5 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA

Received 10 February 2000 / Accepted 27 June 2000

Abstract

We investigate the characteristics of FIR brightness fluctuations at 90 µm and 170 µm in the Lockman Hole, which were surveyed with ISOPHOT aboard the Infrared Space Observatory (ISO). We first calculated the angular correlation function of each field and then its Fourier transform (the angular Power Spectral Density: PSD) over the spatial frequency range of [FORMULA] arcmin-1. The PSDs are found to be rather flat at low spatial frequencies ([FORMULA]), slowly decreasing toward higher frequencies. These spectra are unlike the power-law ones seen in the IR cirrus fluctuations, and are well explained by randomly distributed point sources. Furthermore, point-to-point comparison between 90 µm and 170 µm brightness shows a linear correlation between them, and the slope of the linear fit is much shallower than that expected from the IR cirrus color, and is consistent with the color of galaxies at low or moderate redshift ([FORMULA]). We conclude that the brightness fluctuations in the Lockman Hole are not caused by the IR cirrus, but are most likely due to faint star-forming galaxies. We also give the constraints on the galaxy number counts down to 35 mJy at 90 µm and 60 mJy at 170 µm, which indicate the existence of a strong evolution down to these fluxes in the counts. The galaxies responsible for the fluctuations also significantly contribute to the cosmic infrared background radiation.

Key words: galaxies: evolution – galaxies: starburst – cosmology: observations – infrared: ISM: continuum – infrared: galaxies

* Based on observations with ISO, an ESA project with instruments funded by ESA member states (especially the PI countries: France, Germany, the Netherlands, and the United Kingdom) and with the participation of ISAS and NASA.
** The ISOPHOT data presented in this paper was reduced using PIA, which is a joint development by ESA Astrophysics Division and the ISOPHOT consortium.

Send offprint requests to: maruma@astro.isas.ac.jp

© European Southern Observatory (ESO) 2000

Online publication: October 2, 2000

helpdesk.link@springer.de