The gas-to-dust mass ratio of Centaurus A as seen by Herschel★

Parkin, T. J.; Wilson, C. D.; Foyle, K.; Baes, M.; Bendo, G. J.; Boselli, A.; Boquien, M.; Cooray, Asantha; Cormier, D.; Davies, Jonathan Ivor; Eales, Steve; Galametz, M.; Gomez, Haley Louise; Lebouteiller, V.; Madden, S.; Mentuch, Erin; Page, M. J.; Pohlen, M.; Rémy, Aurélie; Roussel, Hervé; Sauvage, M.; Smith, M.; Spinoglio, L.

doi:10.1111/j.1365-2966.2012.20778.x

Cited by 34 publications

(50 citation statements)

References 74 publications

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“…The filaments molecular content represents about 3-5% of the total gas mass of the entire galaxy, 1.4 − 2.7 × 10 9 M found by Herschel and CO mapping (Parkin et al 2012) (iii) mostly molecular with a small atomic-to-molecular gas fraction and with the brightest emission being far outside the HI cloud itself. All the CO(2-1)-detected regions are found to be dust-rich.…”

Section: Resultsmentioning

confidence: 99%

Atomic-to-molecular gas phase transition triggered by the radio jet in Centaurus A

Salomé

Combes

et al. 2016

A&A

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NGC 5128 (Centaurus A) is one of the best example to study AGN-feedback in the local Universe. At 13.5 kpc from the galaxy, optical filaments with recent star formation are lying along the radio-jet direction. We used the Atacama Pathfinder EXperiment (APEX) to map the CO(2-1) emission all along the filaments structure. Molecular gas mass of (8.2 ± 0.5) × 10 7 M was found over the 4.2 kpc-structure which represents about 3% of the total gas mass of the NGC 5128 cold gas content. Two dusty mostly molecular structures are identified, following the optical filaments. The region corresponds to the crossing of the radio jet with the northern HI shell, coming from a past galaxy merger. One filament is located at the border of the HI shell, while the other is entirely molecular, and devoid of HI gas. The molecular mass is comparable to the HI mass in the shell, suggesting a scenario where the atomic gas was shocked and transformed in molecular clouds by the radio jet. Comparison with combined FIR Herschel and UV GALEX estimation of star formation rates in the same regions leads to depletion times of more than 10 Gyr. The filaments are thus less efficient than discs in converting molecular gas into stars. Kinetic energy injection triggered by shocks all along the jet/gas interface is a possible process that appears to be consistent with MUSE line ratio diagnostics derived in a smaller region of the northern filaments. Whether the AGN is the sole origin of this energy input and what is the dominant (mechanical vs radiative) mode for this process is however still to be investigated.

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Section: Resultsmentioning

confidence: 99%

Atomic-to-molecular gas phase transition triggered by the radio jet in Centaurus A

Salomé

Combes

et al. 2016

A&A

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“…The calibration uncertainty is estimated to be 10% based on a comparison of spectra taken of calibrators during observations and their standard spectra. For more details on the data reduction process and uncertainty measurements, see Warren et al (2010) and Parkin et al (2012).…”

Section: Co and Hi Line Datamentioning

confidence: 99%

A resolved analysis of cold dust and gas in the nearby edge-on spiral NGC 891

Hughes

Baes

Fritz

et al. 2014

A&A

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We investigate the connection between dust and gas in the nearby edge-on spiral galaxy NGC 891, a target of the Very Nearby Galaxies Survey. High resolution Herschel PACS and SPIRE 70, 100, 160, 250, 350, and 500 μm images are combined with JCMT SCUBA 850 μm observations to trace the far-infrared/submillimetre spectral energy distribution (SED). Maps of the Hi 21 cm line and CO(J = 3−2) emission trace the atomic and molecular hydrogen gas, respectively. We fit one-component modified blackbody models to the integrated SED, finding a global dust mass of (8.5 ± 2.0) × 10 7 M and an average temperature of 23 ± 2 K, consistent with results from previous far-infrared experiments. We also fit one-component modified blackbody models to pixel-by-pixel SEDs to produce maps of the dust mass and temperature. The dust mass distribution correlates with the total stellar population as traced by the 3.6 μm emission. The derived dust temperature, which ranges from approximately 17 to 24 K, is found to correlate with the 24 μm emission. Allowing the dust emissivity index to vary, we find an average value of β = 1.9±0.3. We confirm an inverse relation between the dust emissivity spectral index and dust temperature, but do not observe any variation of this relationship with vertical height from the mid-plane of the disc. A comparison of the dust properties with the gaseous components of the ISM reveals strong spatial correlations between the surface mass densities of dust (Σ dust ) and the molecular hydrogen (Σ H 2 ) and total gas surface densities (Σ gas ). These observations reveal the presence of regions of dense, cold dust that are coincident with peaks in the gas distribution and are associated with a molecular ring. Furthermore, the observed asymmetries in the dust temperature, the H 2 -to-dust ratio and the total gas-to-dust ratio hint that an enhancement in the star formation rate may be the result of larger quantities of molecular gas available to fuel star formation in the NE compared to the SW. Whilst the asymmetry likely arises from dust obscuration due to the geometry of the line-of-sight projection of the spiral arms, we cannot exclude that there is also an enhancement in the star formation rate in the NE part of the disc.

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“…It is also rich in gas, both atomic (H i) and molecular (H 2 ) hydrogen (Morganti et al 2008;Struve et al 2010), as well as carbon monoxide (CO), as * Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. observed in various rotational transitions (Phillips et al 1987;Eckart et al 1990;Quillen et al 1992;Rydbeck et al 1993;Parkin et al 2012). For a detailed summary of the physical properties of the galaxy, see Israel (1998) and Morganti (2010).…”

Section: Introductionmentioning

confidence: 99%

“…The disk provides a prominent dust lane through the center, and shows a strong warp, giving it an "S " like shape at infrared wavelengths (Leeuw et al 2002;Quillen et al 2006;Weiß et al 2008;Parkin et al 2012). Cen A is the closest galaxy with an active galactic nucleus (AGN) and associated radio jets extending approximately 4…”

Section: Introductionmentioning

confidence: 99%

THE PHYSICAL CHARACTERISTICS OF THE GAS IN THE DISK OF CENTAURUS A USING THEHERSCHEL SPACE OBSERVATORY

Parkin

Wilson

Schirm

et al. 2014

ApJ

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We search for variations in the disk of Centaurus A of the emission from atomic fine structure lines using Herschel PACS and SPIRE spectroscopy. line ratio, a proxy for the heating efficiency of the gas, shows no significant radial trend across the observed region, in contrast to observations of other nearby galaxies. We determine that 10%-20% of the observed [C ii] emission originates in ionized gas. Comparison between our observations and a PDR model shows that the strength of the far-ultraviolet radiation field, G 0 , varies between 10 1.75 and 10 2.75 and the hydrogen nucleus density varies between 10 2.75 and 10 3.75 cm −3 , with no significant radial trend in either property. In the context of the emission line properties of the grand-design spiral galaxy M51 and the elliptical galaxy NGC 4125, the gas in Cen A appears more characteristic of that in typical disk galaxies rather than elliptical galaxies.

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The gas-to-dust mass ratio of Centaurus A as seen by Herschel★

Cited by 34 publications

References 74 publications

Atomic-to-molecular gas phase transition triggered by the radio jet in Centaurus A

Atomic-to-molecular gas phase transition triggered by the radio jet in Centaurus A

A resolved analysis of cold dust and gas in the nearby edge-on spiral NGC 891

THE PHYSICAL CHARACTERISTICS OF THE GAS IN THE DISK OF CENTAURUS A USING THEHERSCHEL SPACE OBSERVATORY

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