The Galaxy Evolution Explorer (GALEX). Its legacy of UV surveys, and science highlights

Bianchi, Luciana

doi:10.1007/s10509-014-1935-6

Cited by 65 publications

(34 citation statements)

References 46 publications

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“…In contrast, Figure 5 shows that galactic latitudes of the detected AGB stars display a bimodal distribution with a dip in the number of detected stars near b ∼ 0. Although GALEX initially avoided low galactic latitudes, more of the galactic plane was observed toward the end of the extended mission (Bianchi 2014). Galactic scale heights based on the Hipparcos-derived distance of detected and undetected AGB stars (see Figure 4) suggest the bimodal distribution of AGB star detections with galactic latitude is not due to the poor coverage of the galactic plane.…”

Section: Detections and Non-detectionsmentioning

confidence: 98%

A Catalog of GALEX Ultraviolet Emission from Asymptotic Giant Branch Stars

Montez

Ramstedt

Kastner

et al. 2017

ApJ

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We have performed a comprehensive study of the UV emission detected from AGB stars by the Galaxy Evolution Explorer (GALEX). Of the 468 AGB stars in our sample, 316 were observed by GALEX. In the NUV bandpass (λ eff ∼ 2310Å), 179 AGB stars were detected and 137 were not detected. Only 38 AGB stars were detected in the FUV bandpass (λ eff ∼ 1528Å). We find that NUV emission is correlated with optical to near infrared emission leading to higher detection fractions among the brightest, hence closest, AGB stars. Comparing the AGB time-variable visible phased light curves to corresponding GALEX NUV phased light curves we find evidence that for some AGB stars the NUV emission varies in phase with the visible light curves. We also find evidence that the NUV emission, and possibly, the FUV emission are anti-correlated with the circumstellar envelope density. These results suggest that the origin of the GALEX-detected UV emission is an inherent characteristic of the AGB stars that can most likely be traced to a combination of photospheric and chromospheric emission. In most cases, UV detections of AGB stars are not likely to be indicative of the presence of binary companions.

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Section: Detections and Non-detectionsmentioning

confidence: 98%

A Catalog of GALEX Ultraviolet Emission from Asymptotic Giant Branch Stars

Montez

Ramstedt

Kastner

et al. 2017

ApJ

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“…GALEX, a NASA Small Explorer mission, was launched on April 28, 2003 with the primary goal of studying galaxy evolution at low red-shift (Martin et al 2005) and completed its mission on June 28, 2013 (Bianchi 2014). The final data set of GALEX includes more than 44,000 observations (Murthy 2014b) in two ultraviolet bands.…”

Section: Datamentioning

confidence: 99%

Dust scattering from the Taurus Molecular Cloud

Narayan

Murthy

Karuppath

2016

Mon. Not. R. Astron. Soc.

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We present an analysis of the diffuse ultraviolet (UV) emission near the Taurus Molecular Cloud based on observations made by the Galaxy Evolution Explorer (GALEX). We used a Monte Carlo dust scattering model to show that about half of the scattered flux originates in the molecular cloud with 25% arising in the foreground and 25% behind the cloud. The best-fit albedo of the dust grains is 0.3 but the geometry is such that we could not constrain the phase function asymmetry factor (g).

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“…′′ 5 pixels (Morrissey et al 2007). We used only UV images having a distance from the center of the field of view 0.5 deg, as generally the photometric quality is better in the central part of the field (Bianchi et al 2011;Bianchi 2014). In case of multiple observations of the same galaxy, we chose the one with longer exposure time.…”

Section: Uv and Optical Datamentioning

confidence: 99%

Galaxy evolution in nearby galaxy groups – III. AGALEXview of NGC 5846, the largest group in the local universe

Marino

Mazzei

Rampazzo

et al. 2016

Mon. Not. R. Astron. Soc.

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We explore the co-evolution of galaxies in nearby groups (V hel 3000 km s −1 ) with a multi-wavelength approach. We analyze GALEX far-UV (FUV) and near-UV (NUV) imaging, and SDSS u,g,r,i,z data of groups spanning a large range of dynamical phases. We characterize the photometric properties of spectroscopically-confirmed galaxy members and investigate the global properties of the groups through a dynamical analysis.Here we focus on NGC 5846, the third most massive association of Early-Type Galaxies (ETG) after the Virgo and Fornax clusters. The group, composed of 90 members, is dominated by ETGs (about 80 per cent), and among ETGs about 40 per cent are dwarfs. Results are compared with those obtained for three groups in the LeoII cloud, which are radically different both in member-galaxy population and dynamical properties. The FUV-NUV cumulative colour distribution and the normalized UV luminosity function (LF) significantly differ due to the different fraction of late-type galaxy population. The UV LF of NGC 5846 resembles that of the Virgo cluster, however our analysis suggests that star-formation episodes are still occurring in most of the group galaxies, including ETGs. The NUV-i colour distribution, the optical-UV colour-colour diagram, and NUV-r vs. M r colour-magnitude relation suggest that the gas contribution cannot be neglected in the evolution of ETG-type group members. Our analysis highlights that NGC 5846 is still in an active phase of its evolution, notwithstanding the dominance of dwarf and bright ETGs and its virialized configuration.

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The Galaxy Evolution Explorer (GALEX). Its legacy of UV surveys, and science highlights

Cited by 65 publications

References 46 publications

A Catalog of GALEX Ultraviolet Emission from Asymptotic Giant Branch Stars

A Catalog of GALEX Ultraviolet Emission from Asymptotic Giant Branch Stars

Dust scattering from the Taurus Molecular Cloud

Galaxy evolution in nearby galaxy groups – III. AGALEXview of NGC 5846, the largest group in the local universe

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