An Atlas of Galaxy Spectral Energy Distributions From the Ultraviolet to the Mid-Infrared

Brown, M. J. I.; Moustakas, John; Smith, John David; Cunha, Elisabete da; Jarrett, T. H.; Imanishi, Masatoshi; Armus, L.; Brandl, Bernhard R.; Peek, J. E. G.

doi:10.1088/0067-0049/212/2/18

Cited by 234 publications

(485 citation statements)

References 85 publications

(123 reference statements)

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“…For k-corrections, we use the Brown et al (2014b) and Spitzer-SWIRE/GRASIL (Silva et al 1998;Polletta et al 2006Polletta et al , 2007 spectral energy distribution (SED) templates to redshift and measure synthetic photometry of the WISE filter response functions (Jarrett et al 2011) and in this way derive the flux ratios between rest and redshifted, ( )l + z 1 , spectra in the W1-band or IRAC-1 band. The standard k-correction magnitude is then −2.5 Log [flux ratio * (1+z)].…”

Section: Expected Faint Galaxy Countsmentioning

confidence: 99%

Galaxy and Mass Assembly (GAMA): Exploring the WISE Web in G12

Jarrett

Cluver

Magoulas

et al. 2017

ApJ

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116

150

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We present an analysis of the mid-infrared Wide-field Infrared Survey Explorer (WISE) sources seen within the equatorial GAMA G12 field, located in the North Galactic Cap. Our motivation is to study and characterize the behavior of WISE source populations in anticipation of the deep multiwavelength surveys that will define the next decade, with the principal science goal of mapping the 3D large-scale structures and determining the global physical attributes of the host galaxies. In combination with cosmological redshifts, we identify galaxies from their WISE W1 (3.4 μm) resolved emission, and we also perform a star-galaxy separation using apparent magnitude, colors, and statistical modeling of star counts. The resulting galaxy catalog has ;590,000 sources in 60 deg 2 , reaching a W1 5σ depth of 31 μJy. At the faint end, where redshifts are not available, we employ a luminosity function analysis to show that approximately 27% of all WISE extragalactic sources to a limit of 17.5 mag (31 μJy) are at high redshift, > z 1. The spatial distribution is investigated using two-point correlation functions and a 3D source density characterization at 5 Mpc and 20 Mpc scales. For angular distributions, we find that brighter and more massive sources are strongly clustered relative to fainter sources with lower mass; likewise, based on WISE colors, spheroidal galaxies have the strongest clustering, while late-type disk galaxies have the lowest clustering amplitudes. In three dimensions, we find a number of distinct groupings, often bridged by filaments and superstructures. Using special visualization tools, we map these structures, exploring how clustering may play a role with stellar mass and galaxy type.

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Section: Expected Faint Galaxy Countsmentioning

confidence: 99%

Galaxy and Mass Assembly (GAMA): Exploring the WISE Web in G12

Jarrett

Cluver

Magoulas

et al. 2017

ApJ

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116

150

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“…We further restrict our sample to pairs at z < 0.3 in order to minimize the impact of redshift evolution in our galaxies and biases towards the identification of high-mass pairs at the high-redshift end, giving a total of 33 832 pair galaxies. We then match all pair galaxies to the GAMA II panchromatic photometry catalogue (Driver et al, in preparation) and use rest-frame photometry derived from a refactored implementation of the InterRest algorithm (Rudnick et al 2003;Taylor et al 2009), coupled with the empirical set of galaxy template spectra of Brown et al (2014). We exclude any galaxy classed as an AGN using the classifiers described above, leaving 32 468 pair galaxies.…”

Section: Gama and The Pair Cataloguementioning

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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“…Please note that these magnitudes are based on photon counts rather than fluxes, and do not simply correspond to monochromatic flux densities at the effective wavelengths of the relevant filters. Brown et al (2014) quantified the systematic error in the WISE W 4 photometry by comparing measured photometry with synthetic photometry derived from galaxy spectral energy distributions. The Brown et al (2014) sample spans a broad range of galaxy types, including early-type galaxies, late-type galaxies, luminous infrared galaxies, starbursts, Seyferts, and blue compact dwarfs.…”

Section: Effective Wavelengthmentioning

confidence: 99%

“…This residual is much larger than the flux corrections discussed by Wright et al (2010), which were intended for derivations of monochromatic flux densities from W 4 photometry. For a minority of objects with measured α 22 or with an assumed α 22 , Equation (2) can be used to correct WISE W 4 photometry so that it matches the pre-launch RSR curve (e.g., Brown et al 2014). For the majority of objects that lack known α 22 values, we need a revised effective wavelength and WISE W 4 RSR model.…”

Section: Effective Wavelengthmentioning

confidence: 99%

“…The photometry of the planetary nebulae was measured using large rectangular apertures as in Brown et al (2014), and this photometry is provided in not removed stellar contamination from the planetary nebula photometry, but stars only significantly alter the photometry well short-ward of the W 4 filter. As all of the planetary nebulae are very bright, we expect systematic errors (e.g., calibration errors) to dominate over photon Poisson noise.…”

Section: Rsr Models and Planetary Nebulaementioning

confidence: 99%

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Recalibrating the Wide-field Infrared Survey Explorer (WISE) W4 Filter

Brown

Jarrett

Cluver

2014

Publ. Astron. Soc. Aust.

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We present a revised effective wavelength and photometric calibration for the Wide-field Infrared Survey Explorer W 4 band, including tests of empirically motivated modifications to its pre-launch laboratory-measured relative system response curve. We derived these by comparing measured W 4 photometry with photometry synthesised from spectra of galaxies and planetary nebulae. The difference between measured and synthesised photometry using the pre-launch laboratory-measured W 4 relative system response can be as large as 0.3 mag for galaxies and 1 mag for planetary nebulae. We find the W 4 effective wavelength should be revised upward by 3.3%, from 22.1 to 22.8 μm, and the W 4 AB magnitude of Vega should be revised from m W 4 = 6.59 to m W 4 = 6.66. In an attempt to reproduce the observed W 4 photometry, we tested three modifications to the pre-launch laboratory-measured W 4 relative system response curve, all of which have an effective wavelength of 22.8 μm. Of the three relative system response curve models tested, a model that matches the laboratory-measured relative system response curve, but has the wavelengths increased by 3.3% (or 0.73 μm) achieves reasonable agreement between the measured and synthesised photometry.

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An Atlas of Galaxy Spectral Energy Distributions From the Ultraviolet to the Mid-Infrared

Cited by 234 publications

References 85 publications

Galaxy and Mass Assembly (GAMA): Exploring the WISE Web in G12

Galaxy and Mass Assembly (GAMA): Exploring the WISE Web in G12

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

Recalibrating the Wide-field Infrared Survey Explorer (WISE) W4 Filter

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