The Herschel Virgo Cluster Survey – XVI. A cluster inventory★

Davies, Jonathan Ivor; Bianchi, S.; Baes, M.; Bendo, G. J.; Clemens, M.; Alighieri, S. di Serego; Fritz, J.; Fuller, C.; Pappalardo, C.; Hughes, T. M.; Madden, S.; Smith, M.; Verstappen, J.; Vlahakis, C.

doi:10.1093/mnras/stt2213

Cited by 22 publications

(41 citation statements)

References 138 publications

(184 reference statements)

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“…They argue that neither artefacts in the fitting due to noise nor the need to account for line-of-sight temperature variations can explain this clear separation between the relations from the inner and outer regions of Andromeda. Furthermore, the relation from Smith et al for the outer region (R > 3.1 kpc) is in good agreement with the T dust -β relationship observed in the global dust properties derived for galaxies in the Herschel Virgo Cluster Survey (Davies et al 2014). These results suggest a possible physical origin of the relationship.…”

Section: The T Dust -β Relationsupporting

confidence: 81%

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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Section: The T Dust -β Relationsupporting

confidence: 81%

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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“…This gives a value of ηp = 2.83 × 10 −3 if p = 0.01, closer to the value we measure. Using our value for the product (ηp = 2.0 × 10 −3 ) and the De Vis (2018) value for η = 0.283 leads to a value of p = 7.1 × 10 −3 consistent with the range of values measured by Davies et al (2014) p = 3.0 − 12.0 × 10 −3 depending on morphological type. Edmunds (1990) define an effective yield (p e f f = z ln 1/ f , where z is the metalicity), which is the derived yield irrespective of whether there are inflows or out flows of gas.…”

Section: Chemical Evolutionsupporting

confidence: 78%

“…These are all nearby galaxies that have been observed as part of various Herschel Space Observatory programmes and so have many imaging observations across the spectral energy distribution (SED) from the ultra-violet to the far-infrared. The DustPedia sample probes a range of baryonic mass densities -containing galaxies that reside in the "field" and in the ≈ 100 times denser Virgo cluster (Davies et al 2014) thus enabling us to consider environmental influences 2 .…”

Section: Introductionmentioning

confidence: 99%

DustPedia: the relationships between stars, gas, and dust for galaxies residing in different environments

Davies

Nersesian

Baes

et al. 2019

A&A

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We use a sub-set of the DustPedia galaxy sample (461 galaxies) to investigate the effect the environment has had on galaxies. We consider Virgo cluster and field samples and also assign a density contrast parameter to each galaxy, as defined by the local density of SDSS galaxies. We consider their chemical evolution (using M Dust /M Baryon and M Gas /M Baryon ), their specific star formation rate (S FR/M S tars ), star formation efficiency (S FR/M Gas ), stars-to-dust mass ratio (M S tars /M Dust ), gas-to-dust mass ratio (M Gas /M Dust ) and the relationship between star formation rate per unit mass of dust and dust temperature (S FR/M Dust and T Dust ). Late type galaxies (later than Sc) in all of the environments can be modelled using simple closed box chemical evolution and a simple star formation history (S FR(t) ∝ t exp −t/τ). For earlier type galaxies the physical mechanisms that give rise to their properties are clearly much more varied and require a more complicated model (mergers, gas in or outflow). However, we find little or no difference in the properties of galaxies of the same morphological type within the cluster, field or with different density contrasts. It appears that it is morphology, how and whenever this is laid down, and consistent internal physical processes that primarily determine the derived properties of galaxies in the DustPedia sample and not processes related to differences in the local environment.

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“…For more details, see Bourne et al 2012 and Driver et al (in preparation). We convert 100 µm fluxes to SFRs using the tight correlation derived in Davies et al 2014 for Virgo cluster galaxies: log 10 SFR FIR (M yr −1 ) = 0.73 log 10 L 100 µm (W Hz −1 ) − 17.1. (2) Secondly, we derive MIR SFRs using the Wide-field Infrared Explorer (WISE) data from the matched GAMA-WISE catalogue outlined in Cluver et al 2014.…”

Section: Long-duration Mir/fir Continuum Sfrsmentioning

confidence: 99%

Galaxy And Mass Assembly (GAMA): the effect of close interactions on star formation in galaxies

Davies

Robotham

Driver

et al. 2015

Mon. Not. R. Astron. Soc.

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The modification of star formation (SF) in galaxy interactions is a complex process, with SF observed to be both enhanced in major mergers and suppressed in minor pair interactions. Such changes likely to arise on short timescales and be directly related to the galaxy-galaxy interaction time. Here we investigate the link between dynamical phase and direct measures of SF on different timescales for pair galaxies, targeting numerous star-formation rate (SFR) indicators and comparing to pair separation, individual galaxy mass and pair mass ratio. We split our sample into the higher (primary) and lower (secondary) mass galaxies in each pair and find that SF is indeed enhanced in all primary galaxies but suppressed in secondaries of minor mergers. We find that changes in SF of primaries is consistent in both major and minor mergers, suggesting that SF in the more massive galaxy is agnostic to pair mass ratio.We also find that SF is enhanced/suppressed more strongly for short-time duration SFR indicators (e.g. Hα), highlighting recent changes to SF in these galaxies, which are likely to be induced by the interaction. We propose a scenario where the lower mass galaxy has its SF suppressed by gas heating or stripping, while the higher mass galaxy has its SF enhanced, potentially by tidal gas turbulence and shocks. This is consistent with the seemingly contradictory observations for both SF suppression and enhancement in close pairs.

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The Herschel Virgo Cluster Survey – XVI. A cluster inventory★

Cited by 22 publications

References 138 publications

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

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

DustPedia: the relationships between stars, gas, and dust for galaxies residing in different environments

Galaxy And Mass Assembly (GAMA): the effect of close interactions on star formation in galaxies

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