A Comparison of the Galaxy Populations in the Coma and Distant Clusters: The Evolution of k+a Galaxies and the Role of the Intracluster Medium

Poggianti, Bianca M.; Bridges, Terry J.; Komiyama, Yutaka; Yagi, Masafumi; Carter, Dave; Mobasher, Bahram; Okamura, S.; Kashikawa, Nobunari

doi:10.1086/380195

Cited by 201 publications

(276 citation statements)

References 67 publications

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“…This almost matches the high-luminosity tail seen for the e(c) and k galaxies. The characteristics of the luminosity distribution we find for the k+a class, are very similar to those in the local, massive Coma cluster (see Poggianti et al 2004), which lacks a significant bright population, and have a similar typical absolute magnitude of ∼−18.…”

Section: The V-band Luminosity Distributionsupporting

confidence: 69%

Wings-Spe

Fritz

Poggianti

Cava

et al. 2014

A&A

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Context. Cluster galaxies are the ideal sites to look at when studying the influence of the environment on the various aspects of the evolution of galaxies, such as the changes in their stellar content and morphological transformations. In the framework of wings, the WIde-field Nearby Galaxy-cluster Survey, we have obtained optical spectra for ∼6000 galaxies selected in fields centred on 48 local (0.04 < z < 0.07) X-ray selected clusters to tackle these issues. Aims. By classifying the spectra based on given spectral lines, we investigate the frequency of the various spectral types as a function of both the clusters' properties and the galaxies' characteristics. In this way, using the same classification criteria adopted for studies at higher redshift, we can consistently compare the properties of the local cluster population to those of their more distant counterparts. Methods. We describe a method that we have developed to automatically measure the equivalent width of spectral lines in a robust way, even in spectra with a non optimal signal-to-noise ratio. This way, we can derive a spectral classification reflecting the stellar content, based on the presence and strength of the [Oii] and Hδ lines. Results. After a quality check, we are able to measure 4381 of the ∼6000 originally observed spectra in the fields of 48 clusters, of which 2744 are spectroscopically confirmed cluster members. The spectral classification is then analysed as a function of galaxies' luminosity, stellar mass, morphology, local density, and host cluster's global properties and compared to higher redshift samples (MORPHS and EDisCS). The vast majority of galaxies in the local clusters population are passive objects, being also the most luminous and massive. At a magnitude limit of M V < −18, galaxies in a post-starburst phase represent only ∼11% of the cluster population, and this fraction is reduced to ∼5% at M V < −19.5, which compares to the 18% at the same magnitude limit for high-z clusters. "Normal" star-forming galaxies (e(c)) are proportionally more common in local clusters. Conclusions. The relative occurrence of post-starbursts suggests a very similar quenching efficiency in clusters at redshifts in the 0 to ∼1 range. Furthermore, more important than the global environment, the local density seems to be the main driver of galaxy evolution in local clusters at least with respect to their stellar populations content.

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Section: The V-band Luminosity Distributionsupporting

confidence: 69%

Wings-Spe

Fritz

Poggianti

Cava

et al. 2014

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“…In Table 4 we report the line equivalent widths. Consistent with our analysis of the star formation rate properties, the observed values are typical of k+a galaxies (EW(Hδ) > 3 Å, Poggianti et al 2004;Dressler et al 1999), post star-burst (PSB) galaxies whose star formation has been suddenly truncated. These characteristics are not only found in C12 and C17, but are representative of the entire galaxy.…”

Section: Radial Velocities and Line Propertiessupporting

confidence: 87%

“…Indeed, due to their shallower gravitational potential, the dynamical pressure that originates from the fast motion of these galaxies through the hot and dense intra-cluster medium (ICM) can easily exceed the gravitational binding force in the galaxy and efficiently remove atomic gas from their interstellar medium (ISM). The resulting sudden suppression of the star formation in these stripped galaxies, then, leads to their temporary transformation into post star-burst (K+A; Poggianti et al 2004), and subsequently into dE galaxies (Gavazzi et al 2010). Rampressure stripping can therefore be the leading mechanism for the migration of dwarf galaxies from the blue cloud to the red sequence (Boselli et al 2008a,b).…”

Section: Introductionmentioning

confidence: 99%

Stripped gas as fuel for newly formed H ii regions in the encounter between VCC 1249 and M 49: a unified picture from NGVS and GUViCS

Battaia

Gavazzi

Fumagalli

et al. 2012

A&A

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Context. We study the peculiar interacting galaxy system of VCC 1249/M 49 located in the core of the Virgo B subcluster. Owing to a recent interaction between the dwarf galaxy VCC 1249 and the halo gas of the elliptical galaxy M 49, neutral hydrogen has been displaced from the interstellar medium of this dwarf into the Virgo intracluster medium. Observations also reveal multiple compact star-forming regions (aka H ii regions) that are embedded in this H i cloud, with a projected separation up to 13 kpc from VCC 1249 in the northwest direction. Aims. Motivated by recent near-ultraviolet imaging from the GALEX Ultraviolet Virgo Cluster Survey (GUViCS) of the VCC 1249/M 49 system that shows significant ongoing/recent star formation in the compact regions, we aim to constrain the origin of these outlying H ii regions with a multi-wavelength approach. Methods. Using deep optical (u, g, i, z) imaging from the Next Generation Virgo Cluster Survey (NGVS) and new Hα imaging obtained at the San Pedro Martir observatory together with Keck long-slit spectroscopy, we characterize the star formation rates, ages, and metallicity of VCC 1249 and its outlying compact regions. Moreover, we analyze the color and luminosity profile of the galaxy to investigate its recent interaction with M 49. Results. Our new observations indicate that VCC 1249 underwent a recent interaction with M 49 in which both ram-pressure stripping and tidal interaction occured. The joint action of the two mechanisms led to the removal of the H i gas from the interstellar medium of VCC 1249, while the gravitational tides triggered the stellar tail and counter-tail of VCC 1249. Our stellar population synthesis analysis reveals that the star formation in this galaxy was truncated around 200 Myr ago and that the outlying H ii regions were born in situ ≈10 Myr ago out of pre-enriched gas removed from the dwarf galaxy. These observations also reveal that interactions between central and satellite galaxies similar to those between VCC 1249/M 49 may be an effective way of dispersing metals into the halos of massive galaxies.

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“…The SDSS also provides nuclear spectra (in a circular aperture of 3 arcsec) for 575 galaxies of the sample. These nuclear spectra are used to identify post-starburst galaxies (PSB or k+a) using the criterion described in Poggianti et al (2004) and Dressler et al (1999;see however Quintero et al 2004). These are galaxies with a Balmer absorption line with an equivalent width EWHδ > 3 Å for a signal-to-noise larger than 5.…”

Section: The Multifrequency Datamentioning

confidence: 99%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Voyer

Boissier

et al. 2014

A&A

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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.

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A Comparison of the Galaxy Populations in the Coma and Distant Clusters: The Evolution of k+a Galaxies and the Role of the Intracluster Medium

Cited by 201 publications

References 67 publications

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Stripped gas as fuel for newly formed H ii regions in the encounter between VCC 1249 and M 49: a unified picture from NGVS and GUViCS

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

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