GALAXY AND MASS ASSEMBLY (GAMA): MID-INFRARED PROPERTIES AND EMPIRICAL RELATIONS FROM<i>WISE</i>

Cluver, Michelle; Jarrett, T. H.; Hopkins, A. M.; Driver, Simon P.; Liske, J.; Gunawardhana, Madusha; Taylor, Edward N.; Robotham, Aaron S. G.; Alpaslan, Mehmet; Baldry, I. K.; Brown, M. J. I.; Peacock, J. A.; Popescu, Cristina; Tuffs, R.; Bauer, A.; Bland-Hawthorn, Joss; Colless, Matthew; Holwerda, Benne W.; Lara-López, M. A.; Leschinski, Kieran; López-Sánchez, Ángel R.; Norberg, Peder; Owers, Matt S.; Wang, L.; Wilkins, Stephen M.

doi:10.1088/0004-637x/782/2/90

Cited by 225 publications

(333 citation statements)

References 62 publications

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“…We confirm this from our analysis of BPT classes where there is a lower fraction of star-forming galaxies among close pairs compared to galaxies in the same volume. Bergvall et al (2003) found only a modest degree of enhancement of star formation for interacting pairs, contributing little to the luminosity; Lin et al (2007) also find only a modest enhancement of star formation in galaxy pairs in a wide range of merger stages; Li et al (2008) instead find that the enhancement in star formation, in a sample of star-forming galaxies, increases with decreasing separation but does not depend on the luminosity ratio, although it is stronger for lower-mass galaxies; for massive galaxies, Robaina et al (2009) find that only 10% of star formation is due to major interactions (albeit at higher redshifts than studied here); Patton et al (2011) also detect an excess of red galaxies in pairs and attribute this to denser environments and hence more significant spheroids (because of the morphology-density relation); Chou et al (2012) confirm that most close pairs are red and not blue; Deng & Zhang (2013) also finds evidence that interactions are not generally responsible for star formation bursts in two volume-limited samples drawn from the SDSS; Cluver et al (2014) study star formation for galaxies in groups and claim that galaxies with a close neighbour have lower star formation rates. Similarly, we find that, by comparing the distributions of Sérsic indices for galaxies in pairs and their parent samples, there is a relative lack of 'disks' and excess of 'spheroids' among paired galaxies as in Patton et al (2011).…”

Section: Discussionmentioning

confidence: 54%

Galaxy and Mass Assembly (GAMA): merging galaxies and their properties

Propris

Baldry

Bland-Hawthorn

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We derive the close pair fractions and volume merger rates for galaxies in the GAMA survey with −23 < M r < −17 (Ω M = 0.27, Ω Λ = 0.73, H 0 = 100 km s −1 Mpc −1 ) at 0.01 < z < 0.22 (lookback time of < 2 Gyr). The merger fraction is approximately 1.5% per Gyr at all luminosities (assuming 50% of pairs merge) and the volume merger rate is ≈ 3.5 × 10 −4 Mpc −3 Gyr −1 . We examine how the merger rate varies by luminosity and morphology. Dry mergers (between red/spheroidal galaxies) are found to be uncommon and to decrease with decreasing luminosity. Fainter mergers are wet, between blue/disky galaxies. Damp mergers (one of each type) follow the average of dry and wet mergers. In the brighter luminosity bin (−23 < M r < −20) the merger rate evolution is flat, irrespective of colour or morphology, out to z ∼ 0.2. The makeup of the merging population does not appear to change over this redshift range. Galaxy growth by major mergers appears comparatively unimportant and dry mergers are unlikely to be significant in the buildup of the red sequence over the past 2 Gyr. We compare the colour, morphology, environmental density and degree of activity (BPT class) of galaxies in pairs to those of more isolated objects in the same volume. Galaxies in close pairs tend to be both redder and slightly more spheroid-dominated than the comparison sample. We suggest that this may be due to 'harassment' in multiple previous passes prior to the current close interaction. Galaxy pairs do not appear to prefer significantly denser environments. There is no evidence of an enhancement in the AGN fraction in pairs, compared to other galaxies in the same volume

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Section: Discussionmentioning

confidence: 54%

Galaxy and Mass Assembly (GAMA): merging galaxies and their properties

Propris

Baldry

Bland-Hawthorn

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…We note that the correlations derived in Cluver et al 2014 compare WISE fluxes with Hα-derived SFRs, and as such may be biased towards emission line-derived SFRs. However, we rescale all SFRs derived in the paper to have the same slope and normalization as the SFR FIR in order to compare each measure directly (see below).…”

Section: Long-duration Mir/fir Continuum Sfrsmentioning

confidence: 94%

“…(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. We use WISE 22 µm (W4) band fluxes, which are not strongly affected by polycyclic aromatic hydrocarbon emission, and the best-fitting SFR correlation obtained in Cluver et al 2014: log 10 SFR MIR (M yr −1 ) = 0.84 log 10 νL 22 µm (L ) − 7.3.…”

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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“…We select only sources with signal to noise (S/N) ≥ 5, except for W4, where we consider a S/N ≥ 3. We calculate the galaxy stellar mass (M * ) using the WISE W1 filter (3.4 µm) and the W1-W2 (4.6 µm) color following the Cluver et al (2014) calibration. The stellar mass ranges between 10 9 and 10 11 M ⊙ for our sample.…”

Section: Flux Densities and Derived Stellar Massmentioning

confidence: 99%

Molecular gas, dust, and star formation in galaxies

Orellana¹,

Elbaz²,

Calderón-Castillo³

et al. 2017

A&A

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Context. Dust and its emission is being increasingly used to constrain the evolutionary stage of galaxies. A comprehensive characterization of dust, best achieved in nearby bright galaxies, is thus a highly useful resource. Aims. We aim to characterize the relationship between dust properties (mass, luminosity and temperature) and their relationships with galaxy-wide properties (stellar, atomic and molecular gas mass, and star formation mode). We also aim to provide equations to estimate accurate dust properties from limited observational datasets. Methods. We assemble a sample of 1,630 nearby (z < 0.1) galaxies -over a large range of stellar masses (M * ), star formation rates (SFR) and specific star formation rates (sSFR=SFR/M * ) -for which comprehensive and uniform multi-wavelength observations are available from WISE, IRAS, Planck and/or SCUBA. the characterization of dust emission comes from spectral energy distribution (SED) fitting using Draine & Li dust models, which we parametrize using two components (warm at 45 -70 K and cold at 18 -31 K). The subsample of these galaxies with global measurements of CO and/or HI are used to explore the molecular and/or atomic gas content of the galaxies. Results. The total infrared luminosity (L IR ), dust mass (M dust ) and dust temperature of the cold component (T cold ) form a plane that we refer to as the dust plane. A galaxy's sSFR drives its position on the dust plane: starburst (high sSFR) galaxies show higher L IR , M dust and T cold compared to Main Sequence (typical sSFR) and passive galaxies (low sSFR). Starburst galaxies also show higher specific dust masses (M dust /M * ) and specific gas masses ( M gas /M * ). We confirm earlier findings of an anti-correlation between the dust to stellar mass ratio and M * . We also find different anti-correlations depending on sSFR; the anti-correlation becomes stronger as the sSFR increases, with the spread due to different cold dust temperatures. The dust mass is more closely correlated with the total gas mass (atomic plus molecular) than with the individual atomic and molecular gas masses. Our comprehensive multi wavelength data allows us to define several equations to accurately estimate L IR , M dust and T cold from one or two monochromatic luminosities in the infrared and/or sub-millimeter. Conclusions. It is possible to estimate the dust mass and infrared luminosity from a single monochromatic luminosity within the Rayleigh-Jeans tail of the dust emission, with errors of 0.12 and 0.20 dex, respectively. These errors are reduced to 0.05 and 0.10 dex, respectively, if the dust temperature of the cold component is used. The dust mass is better correlated with the total ISM mass ( M ISM ∝ M dust 0.7 ). For galaxies with stellar masses 8.5 < log(M * / M ⊙ ) < 11.9, the conversion factor between the single monochromatic luminosity at 850 µm and the total ISM mass (α 850 µm ) shows a large scatter (rms = 0.29 dex) and a weak correlation with the L IR . The star formation mode of a galaxy shows a correlation with...

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GALAXY AND MASS ASSEMBLY (GAMA): MID-INFRARED PROPERTIES AND EMPIRICAL RELATIONS FROMWISE

Cited by 225 publications

References 62 publications

Galaxy and Mass Assembly (GAMA): merging galaxies and their properties

Galaxy and Mass Assembly (GAMA): merging galaxies and their properties

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

Molecular gas, dust, and star formation in galaxies

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