Herschel observations of Cen A: stellar heating of two extragalactic dust clouds

Auld, Robbie Richard; Smith, M.; Bendo, G. J.; Pohlen, M.; Wilson, C. D.; Gomez, Haley Louise; Cortese, Luca; Morganti, Raffaella; Baes, M.; Boselli, A.; Cooray, Asantha; Davies, J. I.; Eales, Stephen Anthony; Elbaz, D.; Galametz, M.; Isaak, K. G.; Oosterloo, Tom; Page, M. J.; Rigby, E. E.; Spinoglio, L.; Struve, Christian

doi:10.1111/j.1365-2966.2011.19819.x

Cited by 23 publications

(20 citation statements)

References 77 publications

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“…The Balmer decrement (Hα/Hβ) across the MUSE fields confirms that the ionised gas is dusty. The presence of very cold dust (T ∼ 13 K) in and around the outer filament is also seen in Herschel data (Auld et al 2012). The above shows that the region around the outer filament is very rich in phenomena and that it shows the full complexity of the interaction of a jet with a large gas cloud.…”

Section: Special Region: the Outer Filamentmentioning

confidence: 57%

The missing link: Tracing molecular gas in the outer filament of Centaurus A

Morganti

Oosterloo

Oonk

et al. 2016

A&A

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We report the detection, using observations of the CO(2−1) line performed with the Atacama Pathfinder EXperiment (APEX), of molecular gas in the region of the outer filament of Centaurus A, a complex region known to show various signatures of an interaction between the radio jet, an H i cloud, and ionised gas filaments. We detect CO(2−1) at all observed locations, which were selected to represent regions with very different physical conditions. The H 2 masses of the detections range between 0.2 × 10 6 and 1.1 × 10 6 M , for conservative choices of the CO to H 2 conversion factor. Surprisingly, the stronger detections are not coincident with the H i cloud, but instead are in the region of the ionised filaments. We also find variations in the widths of the CO(2−1) lines throughout the region, with broader lines in the region of the ionised gas, i.e. where the jet-cloud interaction is strongest, and with narrow profiles in the H i cloud. This may indicate that the molecular gas in the region of the ionised gas has the momentum of the jet-cloud interaction encoded in it, in the same way as the ionised gas does. These molecular clouds may therefore be the result of very efficient cooling of the down-stream gas photo-or shock-ionised by the interaction. On the other hand, the molecular clouds with narrower profiles, which are closer to or inside the H i cloud, could be pre-existing cold H 2 cores which manage to survive the effects of the passing jet.

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Section: Special Region: the Outer Filamentmentioning

confidence: 57%

The missing link: Tracing molecular gas in the outer filament of Centaurus A

Morganti

Oosterloo

Oonk

et al. 2016

A&A

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“…We include in our analysis a sample of eight galaxies observed in 12 CO(1-0) by Kuno et al (2007), and investigate the effects of the environment on the surface mass density of the atomic and molecular gas phases and on the dust. Maps of the dust surface mass density have been estimated using the HeViCS data set Auld et al 2012). Finally we analyze the relation between the different gas components and the dust distributions in relation to the def HI parameter.…”

Section: Discussionmentioning

confidence: 99%

“…Given that the uncertainties in def HI are ∼0.25-0.3 dex we shall consider a galaxy as non-deficient only if it has def HI < ∼ 0.4. FIR images for dust emission at 100, 160, 250, 350, and 500 μm come from the HeViCS full depth data set (see Auld et al 2012, for details on the data reduction). The beam full width half maximum for these wavelengths are 9 , 13 , 18.…”

Section: The Sample and Ancillary Datamentioning

confidence: 99%

“…The Herschel Virgo Cluster Survey (HeViCS; Davies et al 2010;Auld et al 2012) has mapped an area of 84 square deg 2 in the Virgo cluster, and one of the goals of the project is to investigate mechanisms of gas recycling in clusters of galaxies. Cortese et al (2012) analyzed the galaxies in the Herschel Reference Survey (HRS; Boselli et al 2010), including many Virgo galaxies observed within HeViCS, and found that the global dustto-stellar mass ratio decreases as a function of HI deficiency, providing strong evidence of dust stripping.…”

Section: Introductionmentioning

confidence: 99%

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TheHerschelVirgo Cluster Survey

Pappalardo

Bianchi

Corbelli

et al. 2012

A&A

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Aims. We investigate the dust-to-gas mass ratio and the environmental effects on the various components of the interstellar medium for a spatially resolved sample of Virgo spirals. Methods. We have used the IRAM-30 m telescope to map over their full extent NGC 4189, NGC 4298, NGC 4388, and NGC 4299 in the 12 CO(1-0) and the 12 CO(2-1) lines. We observed the same lines in selected regions of NGC 4351, NGC 4294, and NGC 4424. The CO observations are combined with Herschel maps in 5 bands between 100-500 μm from the HeViCS survey, and with HI data from the VIVA survey, to obtain spatially resolved dust and gas distributions. We studied the environmental dependencies by adding to our sample eight galaxies with 12 CO(1-0) maps from the literature. Results. We estimate the integrated mass of molecular hydrogen for the galaxies observed in the CO lines. We find molecular-to-total gas mass fractions between 0.04 ≤ f mol ≤ 0.65, with the lowest values for the dimmest galaxy in the B-band. The integrated dust-togas ratio ranges between 0.011 and 0.004. For the 12 mapped galaxies we derive the radial distributions of the atomic gas, molecular gas, and dust. We also study the effect of different CO-to-H 2 conversion factors. Both the molecular gas and the dust distributions show steeper radial profiles for HI-deficient galaxies and the average dust-to-gas ratio for these galaxies increases or stays radially constant. On scales of ∼3 kpc, we find a strong correlation between the molecular gas and the 250 μm surface brightness that is tighter than average for non-deficient galaxies. The correlation becomes linear if we consider the total gas surface mass density. However, the inclusion of atomic hydrogen does not improve the statistical significance of the correlation. Conclusions. The environment can modify the distributions of molecules and dust within a galaxy, although these components are more tightly bound than the atomic gas.

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“…This distance (where 1 is approximately 18.5 pc) provides a unique opportunity to study the molecular gas in extraordinary detail. NGC 5128 shows considerably clear dust lanes that are probably caused by merger activities in the past (see [26,27]). The molecular interstellar medium in the dust lane has been widely studied [28][29][30][31][32][33][34][35][36].…”

Section: Introductionmentioning

confidence: 99%

Star Formation Law at Sub-kpc Scale in the Elliptical Galaxy Centaurus A as Seen by ALMA

Azeez

Abidin

Hwang

et al. 2017

Advances in Astronomy

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We present an extensive analysis of the relationship between star formation rate surface density (∑ SFR) and molecular gas surface density (∑ H 2 ) at sub-kpc scale in the elliptical galaxy Centaurus A (also known as NGC 5128) at the distance 3.8 Mpc.12 CO ( = 2-1) data from Atacama Large Millimetre/Sub-Millimetre Array SV data with very high resolution (2.9 , 0.84 ), as well as 24 m data from the Spitzer Space Telescope, were used. This is one of the first studies of the SF law on Centaurus A at this very high spatial resolution. The results showed a breakdown in star formation law with a 0.49 ± 0.05 index relating ∑ SFR and ∑ H 2 at 185 pc. A significant correlation exists between surface densities of molecular gas and SFR with very long depletion time (68 Gy). In addition we examined the spatially resolved relationship between velocity dispersion and star formation rate surface density for the outer disk of this galaxy and we found that the average velocity dispersion is equal to 11.78 km/s. The velocity dispersion of the molecular ISM for the outer disk is found to follow a power relation with the star formation rate surface density ∝ (∑ SFR) , where is the slope from the ordinary least square fitting. The value of is about 1/ ≈ 2.16 ± 0.40 and is the power law index of the star formation law.

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Herschel observations of Cen A: stellar heating of two extragalactic dust clouds

Cited by 23 publications

References 77 publications

The missing link: Tracing molecular gas in the outer filament of Centaurus A

The missing link: Tracing molecular gas in the outer filament of Centaurus A

TheHerschelVirgo Cluster Survey

Star Formation Law at Sub-kpc Scale in the Elliptical Galaxy Centaurus A as Seen by ALMA

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