The Herschel Space Observatory will offer the opportunity to study the gas and dust properties in dwarf galaxies of a wide variety of metallicities,even the extremely metalpoor galaxies,for the first time,using far infrared (FIR) and submillimeter (submm) wavelengths. The moderately metal-poor (1/10 < z <1/2) galaxies that we have been studying to date in the FIR and submm using ISO and the KAO,exhibit striking effects on the observed gas and dust properties due to the low metallicity environments. These conditions may provide advantages in detecting more low metallicity dwarf galaxies in the local and the more distant universe. We find a striking enhancement of I[CII]/I(CO) in dwarf galaxies that can be explained by the lower dust abundance and conclude that FIR fine structure lines can be reliable probes of the molecular gas reservoir in dwarf galaxies. Additionally,the global dust properties differ from those of normal spiral galaxies or other starbursting galaxies. We find that most (up to 60%) of the global infrared luminosity is emitted from a small grain component which is the major contribution to the MIR continuum emission and is stochastically heated,while most of the dust mass resides in a very cold (∼ 7K) component of dust,emitting in the submillimeter regime,not detected before now in galaxies. In spite of the striking dearth of the MIR aromatic band carriers,cooling in the photodissociation regions via [CII] is a very efficient process.

/pdf/metallicity-effects-on-the-ism-of-dwarf-galaxies-the-promise-ock4fithxh.pdf

Metallicity effects on the ism of dwarf galaxies - the promise of the herschel space observatory

We present the smoothness of the mid-infrared sky from observations by the Japanese infrared astronomical satellite AKARI. AKARI monitored the north ecliptic pole (NEP) during its cold phase with nine wavebands covering from 2.4 to 24 micron, out of which six mid-infrared bands were used in this study. We applied power spectrum analysis to the images in order to search for the fluctuation of the sky brightness. Observed fluctuation is explained by fluctuation of photon noise, shot noise of faint sources, and Galactic cirrus. The fluctuations at a few arcminutes scales at short mid-infrared wavelengths (7, 9, and 11 micron) are largely caused by the diffuse Galactic light of the interstellar dust cirrus. At long mid-infrared wavelengths (15, 18, and 24 micron), photon noise is the dominant source of fluctuation over the scale from arcseconds to a few arcminutes. The residual fluctuation amplitude at 200 arcseconds after removing these contributions is at most 1.04 +/- 0.23 nW m^-2 sr^-1 or 0.05% of the brightness at 24 micron and at least 0.47 +/- 0.14 nW m^-2 sr^-1 or 0.02% at 18 micron. We conclude that the upper limit of the fluctuation in the zodiacal light towards the NEP is 0.03% of the sky brightness, taking 2{\sigma} error into account.

Brightness and Fluctuation of the Mid-Infrared Sky from AKARI Observations towards the North Ecliptic Pole

We present the smoothness of the mid-infrared sky from observations by the Japanese infrared astronomical satellite AKARI. AKARI monitored the north ecliptic pole (NEP) during its cold phase with nine wave bands covering from 2.4 to 24 μm, out of which six mid-infrared bands were used in this study. We applied power-spectrum analysis to the images in order to search for the fluctuation of the sky brightness. Observed fluctuation is explained by fluctuation of photon noise, shot noise of faint sources, and Galactic cirrus. The fluctuations at a few arcminutes scales at short mid-infrared wavelengths (7, 9, and 11 μm) are largely caused by the diffuse Galactic light of the interstellar dust cirrus. At long mid-infrared wavelengths (15, 18, and 24 μm), photon noise is the dominant source of fluctuation over the scale from arcseconds to a few arcminutes. The residual fluctuation amplitude at 200'' after removing these contributions is at most 1.04 ± 0.23 nW m–2 sr–1 or 0.05% of the brightness at 24 μm and at least 0.47 ± 0.14 nW m–2 sr–1 or 0.02% at 18 μm. We conclude that the upper limit of the fluctuation in the zodiacal light toward the NEP is 0.03% of the sky brightness, taking 2σ error into account.

http://iopscience.iop.org/article/10.1088/0004-637X/760/2/102/pdf

Brightness and Fluctuation of the Mid-Infrared Sky from AKARI Observations Toward the North Ecliptic Pole

Detection of CFIRB with AKARI/FIS deep observations

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Detection of CFIRB with AKARI/FIS deep observations