The On-Orbit Performance of the
                    <i>Galaxy Evolution Explorer</i>

Morrissey, Patrick; Schiminovich, David; Barlow, Tom A.; Martin, D. Christopher; Blakkolb, Brian K.; Conrow, T.; Cooke, Brian; Erickson, Kerry D.; Fanson, James L.; Friedman, Peter G.; Grange, Robert; Jelinsky, Patrick; Lee, Siu-Chun; Liu, Dankai; Mazer, Alan S.; McLean, Ryan; Milliard, B.; Randall, David; Schmitigal, Wes; Sen, Amit; Siegmund, Oswald H. W.; Surber, Frank; Vaughan, A. H.; Viton, M.; Welsh, Barry Y.; Bianchi, Luciana; Byun, Yong−Ik; Donas, J.; Forster, Karl; Heckman, Timothy M.; Lee, Young-Wook; Madore, Barry F.; Malina, Roger F.; Neff, Susan G.; Rich, R. Michael; Small, Todd; Szalay, Alexander S.; Wyder, Ted K.

doi:10.1086/424734

Cited by 329 publications

(260 citation statements)

References 5 publications

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“…As expected, α GALEX is typically lower (bluer) than α ref but the systematic difference remains small with α GALEX − α ref = −0.19 ± 0.24. This moderate shift, which is less than the one found considering α 12 , is probably due to the wide large bandpass of the NUV filter (1060 Å, Morrissey et al 2005), much wider than the bump itself. Therefore, as long as galaxies exhibit a bump in their attenuation curve similar to that found in this study (1/3 that of the Milky Way), the slopes measured with the GALEX data are found to be reliable.…”

Section: Galex-like Uv Slopementioning

confidence: 56%

GOODS-Herschel: evidence of a UV extinction bump in galaxies atz > 1

Buat

Giovannoli

Heinis

et al. 2011

A&A

101

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Context. Dust attenuation curves in external galaxies are useful for studying their dust properties as well as interpreting their intrinsic spectral energy distributions. These functions are not very well known in the UV range whether at low or high redshift. In particular, the presence or absence of a UV bump at 2175 Å remains an open issue that has consequences on the interpretation of broad band colours of galaxies involving the UV range. Aims. We want to study the dust attenuation curve in the UV range at z > 1 where the UV is redshifted into the visible and with Herschel data to constrain dust emission and a global dust attenuation. In particular, we search for a UV bump and related implications for dust attenuation determinations. Methods. We use deep photometric data of the Chandra Deep Field South obtained with intermediate and broad band filters by the MUSYC project to sample the UV rest frame of galaxies with 1 < z < 2. Herschel/PACS and Spitzer/MIPS data are used to measure the dust emission. We select 30 galaxies with high S/N in all bands. Their SEDs from the UV to the far-IR are fitted using the CIGALE code and the characteristics of the dust attenuation curves obtained as Bayesian outputs of the SED fitting process. Results. The mean dust attenuation curve we derive exhibits a significant UV bump at 2175 Å whose amplitude corresponds to 35% (76%) that of the Milky Way (Large Magellanic Cloud: LMC2 supershell) extinction curve. An analytical expression of the average attenuation curve (A(λ)/A V ) is given and found to be slightly steeper than the Calzetti et al. one, although at a 1σ level. Our galaxy sample is used to study the derivation of the slopes of the UV continuum from broad band colours, including the rest frame GALEX FUV − NUV colour. Systematic errors induced by the presence of the bump are quantified. We compare dust attenuation factors measured with CIGALE to the slope of the UV continuum and find that there is a large scatter around the relation valid for local starbursts (∼0.7 mag). The uncertainties on the determination of the UV slope lead to an extra systematic error in a range of 0.3 to 0.7 mag on dust attenuation when a filter overlaps the UV bump.

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Section: Galex-like Uv Slopementioning

confidence: 56%

GOODS-Herschel: evidence of a UV extinction bump in galaxies atz > 1

Buat

Giovannoli

Heinis

et al. 2011

A&A

101

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“…GALEX (Morrissey et al 2005) observed this field in both the FUV (1530 Å) and the NUV (2310 Å) as part of its deep imaging survey. To add IR data we limit our study to the sub-field covered by Spitzer/MIPS observations as part of the GOODS key program (e.g., Elbaz et al 2007).…”

Section: The Uv-selected Samplesmentioning

confidence: 99%

The infrared emission of ultraviolet-selected galaxies fromz= 0 toz= 1

Buat

Takeuchi²,

Burgarella

et al. 2009

A&A

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Aims. We want to study the IR (>8 μm) emission of galaxies selected on the basis of their rest-frame UV light in a very homogeneous way (wavelength and luminosity) from z = 0 to z = 1. We compare their UV and IR rest-frame emission to study the evolution in dust attenuation with z as well as to check if a UV selection is capable of tracking all star formation. This UV selection will also be compared to a sample of Lyman break galaxies selected at z 1. Methods. We select galaxies in UV (1500-1800 Å) rest-frame at z = 0, z = 0.6-0.8, z = 0.8-1.2, and with as Lyman break galaxies at z = 0.9-1.3, the samples are compiled to sample the same range of luminosity at any redshift. The UV rest-frame data come from GALEX for z < 1 and the U-band of the EIS survey (at z = 1). The UV data are combined with the IRAS 60 μm observations at z = 0 and the Spitzer data at 24 μm for z > 0 sources. The evolution in the IR and UV luminosities with z is analysed for individual galaxies as well as in terms of luminosity functions. Results. The L IR /L UV ratio is used to measure dust attenuation. This ratio does not seem to evolve significantly with z for the bulk of our sample galaxies, but some trends are found for both galaxies with a strong dust attenuation and UV luminous sources: galaxies with L IR /L UV > 10 are more frequent at z > 0 than at z = 0, and the largest values of L IR /L UV are found for UV faint objects; in contrast, the most luminous galaxies of our samples (L UV > 2 × 10 10 L ), detected at z = 1, exhibit a lower dust attenuation than fainter ones. The value of L IR /L UV increases with the K rest-frame luminosity of the galaxies at all redshifts considered and shows a residual anticorrelation with L UV . The most massive and UV luminous galaxies exhibit quite high specific star formation rates. Lyman break galaxies exhibit systematically lower dust attenuation than UV-selected galaxies of same luminosity, but similar specific star formation rates. The analysis of the UV + IR luminosity functions leads to the conclusion that up to z = 1, most of the star formation activity of UV-selected galaxies is emitted in IR. Although we are able to infer information about all the star formation from our UV selection at z = 0.7, at z = 1 we miss a large fraction of galaxies more luminous than 10 11 L . The effect is found to be larger for Lyman break galaxies.

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“…Conversion from count rates to the AB photometric system (Oke 1990) was obtained using the zero-points ZP AB FUV = 18.82 and ZP AB NUV = 20.08 (Morrissey et al 2005). UV magnitudes were corrected for foreground Galactic extinction following Schlegel et al (1998) before starting the analysis of the cluster SEDs.…”

Section: Uv Photometrymentioning

confidence: 99%

Young stellar clusters and associations in M 33

Grossi

Corbelli

Giovanardi

et al. 2010

A&A

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Aims. We analyse multi-wavelength observations of 32 young star clusters and associations in M 33 with known oxygen abundance (8 < 12 + log(O/H) < 8.7). The data set includes ultraviolet (UV), optical, mid-infrared (MIR), CO (1-0) and 21-cm line (Hi) observations. We derive the spectral energy distribution (SED) of these systems and the properties of their gaseous environment to investigate the process of star formation and the interplay with the interstellar medium (ISM). Methods. We determine age, bolometric luminosities, masses, and the extinction by comparing the multi-band integrated photometry to single-age stellar population models. The best-fit solutions have been obtained using the Large Magellanic Cloud (LMC) extinction curves.Results. The stellar system ages range between 2 and 15 Myr, masses are between 3 × 10 2 and 4 × 10 4 M , and the intrinsic extinction, A V , varies from 0.3 to 1 mag. We find a correlation between age and extinction (young clusters being more reddened than older ones), and between the cluster mass and size. From the MIR emission we infer the presence of a dust component around the clusters whose fractional luminosity at 24 μm, L 24 /L Bol , decreases with the galactocentric distance. However, the total infrared luminosity inferred from L 24 is smaller than what we derive from the extinction corrections. We also find that the Hα luminosity predicted by population synthesis models is higher than the observed one, especially for low-mass systems (M < 10 4 M ). This difference is reduced, but not erased, when the incomplete sampling of the initial mass function (IMF) at the high-mass end is taken into account. Conclusions. Our results suggest that a non-negligible fraction of UV ionising and non-ionising radiation is leaking into the ISM outside the Hii regions. This agrees with the large UV and Hα diffuse fractions observed in M 33, but it implies that stellar systems younger than 3 Myr retain, on average, only 30% of their Lyman-continuum photons. However, the uncertainties in cluster ages and the stochastic fluctuations of the IMF do not allow us to accurately quantify this issue. We also consider the possibility that this discrepancy is the consequence of a suppressed or delayed formation of the most massive stars, given that it mainly affects the young and less massive clusters. We do not find any clear correlation between the cluster mass and the gas surface density or metallicity.

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The On-Orbit Performance of the Galaxy Evolution Explorer

Cited by 329 publications

References 5 publications

GOODS-Herschel: evidence of a UV extinction bump in galaxies atz > 1

GOODS-Herschel: evidence of a UV extinction bump in galaxies atz > 1

The infrared emission of ultraviolet-selected galaxies fromz= 0 toz= 1

Young stellar clusters and associations in M 33

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