The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boissier, S.; Boselli, A.; Voyer, E.; Bianchi, S.; Pappalardo, C.; Guhathakurta, Puragra; Heinis, S.; Cortese, Luca; Duc, P. A.; Cuillandre, Jean-Charles; Davies, Jonathan Ivor; Smith, M.

doi:10.1051/0004-6361/201526089

Cited by 28 publications

(37 citation statements)

References 56 publications

(77 reference statements)

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“…While Boissier et al (2008) computed UV integrated magnitudes for Malin 1 using these data, in this paper we combine all GALEX tiles in which the galaxy is imaged to obtain an accumulated exposure time 3 times longer than in this previous work. To do so, we used the Montage software (Jacob et al 2010) and resampled the data on same grid and pixel scale as the MegaCam images (in a similar manner as in Boissier et al 2015), to facilitate the comparison between the UV and optical data. The GALEX PSF of the images is about 5 arcsec.…”

Section: New Uv and Optical Imagesmentioning

confidence: 99%

The properties of the Malin 1 galaxy giant disk

Boissier

Boselli

Ferrarese

et al. 2016

A&A

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Context. Low surface brightness galaxies (LSBGs) represent a significant percentage of local galaxies but their formation and evolution remain elusive. They may hold crucial information for our understanding of many key issues (i.e., census of baryonic and dark matter, star formation in the low density regime, mass function). The most massive examples -the so called giant LSBGs -can be as massive as the Milky Way, but with this mass being distributed in a much larger disk. Aims. Malin 1 is an iconic giant LSBG -perhaps the largest disk galaxy known. We attempt to bring new insights on its structure and evolution on the basis of new images covering a wide range in wavelength. Methods. We have computed surface brightness profiles (and average surface brightnesses in 16 regions of interest), in six photometric bands (FUV, NUV, u, g, i, z). We compared these data to various models, testing a variety of assumptions concerning the formation and evolution of Malin 1. Results. We find that the surface brightness and color profiles can be reproduced by a long and quiet star-formation history due to the low surface density; no significant event, such as a collision, is necessary. Such quiet star formation across the giant disk is obtained in a disk model calibrated for the Milky Way, but with an angular momentum approximately 20 times larger. Signs of small variations of the star-formation history are indicated by the diversity of ages found when different regions within the galaxy are intercompared. Conclusions. For the first time, panchromatic images of Malin 1 are used to constrain the stellar populations and the history of this iconic example among giant LSBGs. Based on our model, the extreme disk of Malin 1 is found to have a long history of relatively low star formation (about 2 M yr −1 ). Our model allows us to make predictions on its stellar mass and metallicity.

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Section: New Uv and Optical Imagesmentioning

confidence: 99%

The properties of the Malin 1 galaxy giant disk

Boissier

Boselli

Ferrarese

et al. 2016

A&A

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“…As a final step in the catalog preparation, the photometry for each object was dereddened following Schlegel et al (1998). Note that the reddening along this line of sight is quite low (see, e.g., Boissier et al 2015), with M87, which marks the center of the Virgo Cluster, having Figure 2 shows the (Hess) color-magnitude diagram (CMD) of all NGVS stellar (point-like) sources identified in this way. The average photometric error in i and (g − i) as a function of iband magnitude is shown on the left-hand side of the figure.…”

Section: Observations and Datamentioning

confidence: 99%

The Next Generation Virgo Cluster Survey. Xix. Tomography of Milky Way Substructures in the NGVS Footprint

Lokhorst

Starkenburg

McConnachie

et al. 2016

ApJ

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The Next Generation Virgo Cluster Survey (NGVS) is a deep u * giz survey targeting the Virgo Cluster of galaxies at 16.5 Mpc. This survey provides high-quality photometry over an ∼100 deg 2 region straddling the constellations of Virgo and Coma Berenices. This sightline through the Milky Way is noteworthy in that it intersects two of the most prominent substructures in the Galactic halo: the Virgo overdensity (VOD) and Sagittarius stellar stream (close to its bifurcation point). In this paper, we use deep u * gi imaging from the NGVS to perform tomography of the VOD and Sagittarius stream using main-sequence turnoff (MSTO) stars as a halo tracer population. The VOD, whose centroid is known to lie at somewhat lower declinations (α ∼ 190°, δ ∼ −5°) than is covered by the NGVS, is nevertheless clearly detected in the NGVS footprint at distances between ∼8 and 25 kpc. By contrast, the Sagittarius stream is found to slice directly across the NGVS field at distances between 25 and 40 kpc, with a density maximum at ;35 kpc. No evidence is found for new substructures beyond the Sagittarius stream, at least out to a distance of ∼90 kpc-the largest distance to which we can reliably trace the halo using MSTO stars. We find clear evidence for a distance gradient in the Sagittarius stream across the ∼30°of sky covered by the NGVS and its flanking fields. We compare our distance measurements along the stream withthose predicted by leading stream models.

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“…Ultraviolet magnitudes are corrected for Galactic attenuation using the Schlegel et al (1998) map combined with the Fitzpatrick & Massa (2007) extinction curve. Given the high Galactic latitude of the Virgo cluster, these corrections are low (A(NUV) < ∼ 0.4 mag; Boissier et al 2015).…”

Section: The Datamentioning

confidence: 99%

“…The UV data extracted from this survey have been recently published in Voyer et al (2014), and the study of the physical properties of Virgo cluster galaxies derived from a multifrequency analysis have been presented in Boselli et al (2014a). In two other companion papers we presented the study of the extraplanar star formation activity of a few gas stripped galaxies in the cluster (Boissier et al 2012) and of the diffuse Galactic emission of the UV scattered light in the Virgo direction (Boissier et al 2015). In the present work we derive and study the UV luminosity function of the Virgo cluster and its surrounding regions.…”

Section: Introductionmentioning

confidence: 99%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Boissier

Voyer

et al. 2015

A&A

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We use the GALEX data of the GUViCS survey to construct the near-ultraviolet (NUV) luminosity function of the Virgo cluster over ∼300 deg 2 , an area covering the cluster and its surrounding regions up to ∼1.8 virial radii. The NUV luminosity function is also determined for galaxies of different morphological types and NUV − i colours, and for the different substructures within the cluster. These luminosity functions are robust vs. statistical corrections since based on a sample of 833 galaxies mainly identified as cluster members with spectroscopic redshift (808) or high-quality optical scaling relations (10). We fit these luminosity functions with a Schechter function, and compare the fitted parameters with those determined for other nearby clusters and for the field. The faint end slope of the Virgo NUV luminosity function (α = −1.19), here sampled down to ∼NUV = −11.5 mag, is significantly flatter than the value measured in other nearby clusters and similar to the field value. Similarly, M * = −17.56 is one to two magnitudes fainter than measured in Coma, A1367, the Shapley supercluster, and the field. These differences seem to be due to the quite uncertain statistical corrections and the small range in absolute magnitude sampled in these clusters. We do not observe strong systematic differences in the overall NUV luminosity function of the core of the cluster with respect to that of its periphery. We note, however, that the relative contribution of red and blue galaxies at the faint end is inverted, with red quiescent objects dominating the core of the cluster and star forming galaxies dominating beyond one virial radius. This observational evidence is discussed in the framework of galaxy evolution in dense environments.

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The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Cited by 28 publications

References 56 publications

The properties of the Malin 1 galaxy giant disk

The properties of the Malin 1 galaxy giant disk

The Next Generation Virgo Cluster Survey. Xix. Tomography of Milky Way Substructures in the NGVS Footprint

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

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