H<i>α</i>surface photometry of galaxies in nearby clusters

Gavazzi, G.; Boselli, A.; Cortese, Luca; Arosio, I.; Gallazzi, Anna; Pedotti, P.; Carrasco, L.

doi:10.1051/0004-6361:20053843

Cited by 106 publications

(134 citation statements)

References 40 publications

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“…In fact, observed a truncation in the disk of NGC 4569 both in the UV and in the IR (8−70 μm) that they associate to a ram-pressure stripping of the external regions. More in general, Gavazzi et al (2006) observe a consistent H α deficiency in Virgo galaxies which indicates a low SFR and diminished dust heating/emission (see also the discussion in . In this scenario, once the starformation quenching happens, the SEDs of the galaxy members would be consistently modified at the IR and UV wavelengths, being not compatible anymore with field galaxies, thus explaining the excess predicted by our model.…”

Section: Effect Of the Cluster Environmentmentioning

confidence: 73%

Infrared properties of the SDSS-maxBCG galaxy clusters

Roncarelli¹,

Pointecouteau²,

Giard³

et al. 2010

A&A

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Context. The physics of galaxy clusters has proven to be influenced by several processes connected with their galactic component which pollutes the intracluster medium (ICM) with metals, stars and dust. However, it is not clear whether the presence of diffuse dust can play a role in clusters physics since a characterisation of the infrared (IR) properties of galaxy clusters is very challenging and yet to be completely achieved. Aims. In our study we focus on the recent work of Giard et al. (2008, A&A, 490, 547) who performed a stacking analysis of the IRAS data in the direction of several thousands of galaxy clusters, providing a statistical characterisation of their IR luminosity and redshift evolution. We model the IR properties of the galactic population of the SDSS-maxBCG clusters (0.1 < z < 0.3) in order to check if it accounts for the entire observed signal and to constrain the possible presence of other components, like dust in the ICM. Methods. Starting from the optical properties of the galaxies of the SDSS-maxBCG clusters, we estimate their emission in the 60 and 100 μm IRAS bands making use of modeled spectral energy distributions of different spectral types (E/S0, Sa, Sb, Sc and starburst). We also consider the evolution of the galactic population/luminosity with redshift. Results. The total galactic emission, which is dominated by the contribution of star-forming late-type galaxies, is consistent with the observed signal. In fact, our galactic emission model slightly overestimates the observed fluxes, with the excess being concentrated in low-redshift clusters (z < ∼ 0.17). Conclusions. Our results indicate that, if present, the IR emission from intracluster dust must be very small compared to the one associated to the galaxy members. This translates into an upper limit on the dust-to-gas mass ratio in the ICM of Z d < ∼ 5 × 10 −5 . The excess in luminosity obtained at low redshift constitutes an indication that the cluster environment is driving a process of starformation quenching on its galaxy members.

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Section: Effect Of the Cluster Environmentmentioning

confidence: 73%

Infrared properties of the SDSS-maxBCG galaxy clusters

Roncarelli¹,

Pointecouteau²,

Giard³

et al. 2010

A&A

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“…the cluster (Koopmann et al 2001;Gavazzi et al 2006). b) Boselli et al (2011) invoked a possible bias in the determination of the UV luminosity function in the central 12 deg 2 of Virgo because of the lack of bright galaxies in their sample.…”

Section: Figmentioning

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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“…A narrow Hα band image was taken at the ESO 3.6 m telescope in 2004 (see Gavazzi et al 2006). Sources with an Hα surface brightness higher than σ min = 3.16 × 10 −17 erg/s/cm 2 /arcsec 2 were detected (2σ of the background).…”

Section: The Datamentioning

confidence: 99%

Constraining the ages of the fireballs in the wake of the dIrr galaxy VCC 1217/IC 3418

Fumagalli

Gavazzi

Scaramella

et al. 2011

A&A

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123

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Context. A complex of Hα emitting blobs with strong FUV excess is associated to the dIrr galaxy VCC 1217/IC 3418 (Hester et al. 2010, ApJ, 716, L14), and extends up to 17 Kpc in the southeast direction. These outstanding features can be morphologically divided into diffuse filaments and compact knots, where most of the star formation activity traced by Hα takes place. Aims. We investigate the properties of the galaxy and the blobs using a multiwavelength approach to constrain their origin. Methods. We collected publicly available data in UV and Hα and observed the scene in the optical U, g, r, i bands with LBT. The photometric data allows evaluation of the star formation rate and performance of a SED fitting separately for the galaxy and the blobs in order to constrain their stellar population age. Moreover we analyzed the color and luminosity profile of the galaxy and its spectrum to investigate its recent interaction with the Virgo cluster. Results. Our analysis confirms that the most plausible mechanism for the formation of the blobs is ram pressure stripping by the Virgo cluster IGM. The galaxy colors, luminosity profile and SED are consistent with a sudden gas depletion in the last few hundred Myr. The SED fitting of the blobs constrains their ages in <400 Myr.

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Hαsurface photometry of galaxies in nearby clusters

Cited by 106 publications

References 40 publications

Infrared properties of the SDSS-maxBCG galaxy clusters

Infrared properties of the SDSS-maxBCG galaxy clusters

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Constraining the ages of the fireballs in the wake of the dIrr galaxy VCC 1217/IC 3418

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