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2012MNRAS.426.2957M - Mon. Not. R. Astron. Soc., 426, 2957-2977 (2012/November-2)
Herschel observations of extended atomic gas in the core of the Perseus cluster.
MITTAL R., OONK J.B.R., FERLAND G.J., EDGE A.C., O'DEA C.P., BAUM S.A., WHELAN J.T., JOHNSTONE R.M., COMBES F., SALOME P., FABIAN A.C., TREMBLAY G.R., DONAHUE M. and RUSSELL H.
Abstract (from CDS):
With the help of FIR continuum Herschel measurements, together with a suite of coeval radio, sub-millimetre and IR data from other observatories, we performed a spectral energy distribution fitting of NGC 1275 using a model that contains contributions from dust emission as well as synchrotron active galactic nucleus emission. This has allowed us to accurately estimate the dust parameters. The data indicate a low dust emissivity index, β ≈ 1, a total dust mass close to 107M☉, a cold dust component with temperature 38±2K and a warm dust component with temperature 116±9K. The FIR-derived star formation rate is 24 ± 1M☉/yr, which is in agreement with the far-ultraviolet-derived star formation rate in the core, determined after applying corrections for both Galactic and internal reddening. The total IR luminosity in the range 8–1000 µm is inferred to be 1.5 x 1011L☉, making NGC 1275 a luminous IR galaxy.
We investigated in detail the source of the Herschel FIR and Hα emissions emerging from a core region 4kpc in radius. Based on simulations conducted using the radiative transfer code, CLOUDY, a heating model comprising old and young stellar populations is sufficient to explain these observations. The optical line ratios indicate that there may be a need for a second heating component. However, stellar photoionization seems to be the dominant mechanism.
We have also detected [CII] in three well-studied regions of the filaments. Herschel, with its superior sensitivity to FIR emission, can detect far colder atomic gas than previous studies. We find an [OI]/[CII] ratio about 1 dex smaller than predicted by the otherwise functional Ferland (2009) model. That study considered optically thin emission from a small cell of gas and by design did not consider the effects of reasonable column densities. The line ratio suggests that the lines are optically thick, as is typical of galactic photodissociation regions, and implies that there is a large reservoir of cold atomic gas. This was not included in previous inventories of the filament mass and may represent a significant component.
Abstract Copyright: © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS
Journal keyword(s): dust, extinction - photodissociation region (PDR) - galaxies: clusters: individual: NGC 1275 - galaxies: clusters: intracluster medium - galaxies: ISM - galaxies: kinematics and dynamics
CDS comments: The knots in Fig.3 and Table 10 are not in Simbad.
Simbad objects: 10
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