Mid-IR emission of galaxies in the Virgo cluster 
 III. The data

Boselli, A.; Sauvage, M.; Lequeux, J.; Donati, Alessandro; Gavazzi, G.

doi:10.1051/0004-6361:20030799

Cited by 57 publications

(100 citation statements)

References 35 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Combined with calibration uncertainties (∼1.5%), the photometric uncertainty due to aperture and colour corrections on the W4 band should be of the order of ∼5%. This, however, does not include the uncertainty on the total flux estimate, which is generally dominated by the uncertainty on the determination of the sky background in extended sources (Boselli et al 2003b;Ciesla et al 2012). The total uncertainty on the measure of the flux density is thus given by the quadratic sum of the calibration uncertainty err WISE , on the uncertainty of the large scale sky fluctuations err sky , and on the pixel per pixel uncertainty err pix which might be partly correlated (Boselli et al 2003b;Ciesla et al 2012).…”

Section: Resultsmentioning

confidence: 99%

“…The total uncertainty on the measure of the flux density is thus given by the quadratic sum of the calibration uncertainty err WISE , on the uncertainty of the large scale sky fluctuations err sky , and on the pixel per pixel uncertainty err pix which might be partly correlated (Boselli et al 2003b;Ciesla et al 2012). Consistently with Boselli et al (2003b) and Voyer et al (2014), we calculate the uncertainty on the sky err sky and on the pixel per pixel err pix in ∼10 square sky regions with randomly selected large sizes surrounding each target. These uncertainties are defined as:…”

Section: Resultsmentioning

confidence: 99%

“…Given that err sky and err pix are the dominant source of error, we consider all galaxies with S 22 μm /err tot > 1 here as detections. As in Boselli et al (2003b) for undetected galaxies, we estimate an upper limit defined as…”

Section: Resultsmentioning

confidence: 99%

See 2 more Smart Citations

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Voyer

Boissier

et al. 2014

A&A

Self Cite

149

254

View full text Add to dashboard Cite

We study the role of the environment on galaxy evolution using a sample of 868 galaxies in the Virgo cluster and in its surrounding regions that are selected from the GALEX Ultraviolet Virgo Cluster Survey (GUViCS) with the purpose of understanding the origin of the red sequence in dense environments. The sample spans a wide range in morphological types (from dwarf ellipticals to Im and BCD) and stellar masses (10 7 M star 10 11.5 M ). We collected multifrequency data covering the whole electromagnetic spectrum for most of the galaxies, including UV, optical, mid-and far-infrared imaging data, as well as optical and HI spectroscopic data. We first identify the different dynamical substructures that compose the Virgo cluster, and we calculate the local density of galaxies using different methods. We then study the distribution of galaxies belonging to the red sequence, the green valley, and the blue cloud within the different cluster substructures or as a function of galaxy density. Our analysis indicates that all the most massive galaxies (M star 10 11 M ) are slow rotators and are the dominant galaxies of the different cluster substructures, which are generally associated with a diffuse X-ray emission. They are probably the result of major merging events that occurred at early epochs, as also indicated by their very old stellar populations. Slow rotators of lower stellar mass (10 8.5M star 10 11 M ) are also preferentially located within the different high-density substructures of the cluster. Their position in the velocity space indicates that they are virialised within the cluster; thus, they are Virgo members since its formation. They have been shaped by gravitational perturbations occurring within the infalling groups that later form the cluster (pre-processing). On the contrary, low-mass star-forming systems are extremely rare in the inner regions of the Virgo cluster A, where the density of the intergalactic medium is at its maximum. Our ram pressure stripping models consistently indicate that these star-forming systems can be rapidly deprived of their interstellar medium during their interaction with the intergalactic medium. The lack of gas quenches their star-formation activity transforming them into quiescent dwarf ellipticals. This mild transformation does not perturb the kinematic properties of these galaxies, which still have rotation curves typical of star-forming systems.

show abstract

Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

See 1 more Smart Citation

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Voyer

Boissier

et al. 2014

A&A

Self Cite

149

254

View full text Add to dashboard Cite

show abstract

“…UV data will then be used to reconstruct the extinction corrected UV to sub-mm SED of Virgo cluster galaxies that, with the help of our models, will constrain the evolution of galaxies in the cluster for both resolved and unresolved objects (Boselli et al 1998. The UV color of early type galaxies will be analyzed to determine whether their emission is due to recent star formation activity or is rather related to an old stellar population (UV upturn, Boselli et al 2005a).…”

Section: The Guvics Surveymentioning

confidence: 99%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Boissier

Heinis

et al. 2011

A&A

Self Cite

View full text Add to dashboard Cite

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS) is a complete blind survey of the Virgo cluster covering ∼40 sq. deg in the far UV (FUV, λ eff = 1539 Å, Δλ = 442 Å) and ∼120 sq. deg in the near UV (NUV, λ eff = 2316 Å, Δλ = 1060 Å). The goal of the survey is to study the ultraviolet (UV) properties of galaxies in a rich cluster environment, spanning a wide luminosity range from giants to dwarfs, and regardless of prior knowledge of their star formation activity. The UV data will be combined with those in other bands (optical: NGVS; far-infrared -submm: HeViCS; HI: ALFALFA) and with our multizone chemo-spectrophotometric models of galaxy evolution to make a complete and exhaustive study of the effects of the environment on the evolution of galaxies in high density regions. We present here the scientific objectives of the survey, describing the observing strategy and briefly discussing different data reduction techniques. Using UV data already in-hand for the central 12 sq. deg we determine the FUV and NUV luminosity functions of the Virgo cluster core for all cluster members and separately for early-and late-type galaxies and compare it to the one obtained in the field and other nearby clusters (Coma, A1367). This analysis shows that the FUV and NUV luminosity functions of the core of the Virgo clusters are flatter (α ∼ −1.1) than those determined in Coma and A1367. We discuss the possible origin of this difference.

show abstract

“…The interpretation of the infrared SEDs of normal galaxies has already been the subject of several studies (Dale & Helou 2002;Dale et al 2001Dale et al , 2005Dale et al , 2007Chary & Elbaz 2001) even within the Virgo cluster region (Boselli et al 1998. These however were generally limited in the infrared to λ ≤ 170 μm, the spectral domain covered by ISO or Spitzer.…”

Section: Introductionmentioning

confidence: 99%

FIR colours and SEDs of nearby galaxies observed withHerschel

Boselli¹,

Ciesla²,

Buat³

et al. 2010

A&A

Self Cite

View full text Add to dashboard Cite

We present infrared colours (in the 25−500 μm spectral range) and UV to radio continuum spectral energy distributions of a sample of 51 nearby galaxies observed with SPIRE on Herschel. The observed sample includes all morphological classes, from quiescent ellipticals to active starbursts. Active galaxies have warmer colour temperatures than normal spirals. In ellipticals hosting a radio galaxy, the far-infrared (FIR) emission is dominated by the synchrotron nuclear emission. The colour temperature of the cold dust is higher in quiescent E-S0a than in star-forming systems probably because of the different nature of their dust heating sources (evolved stellar populations, X-ray, fast electrons) and dust grain properties. In contrast to the colour temperature of the warm dust, the f 350/ f 500 index sensitive to the cold dust decreases with star formation and increases with metallicity, suggesting an overabundance of cold dust or an emissivity parameter β <2 in low metallicity, active systems.

show abstract

Mid-IR emission of galaxies in the Virgo cluster III. The data

Cited by 57 publications

References 35 publications

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

FIR colours and SEDs of nearby galaxies observed withHerschel

Contact Info

Product

Resources

About