The SDSS-GALEX viewpoint of the truncated red sequence in field environments at z ∼ 0

Haines, C. P.; Gargiulo, A.; Merluzzi, P.

doi:10.1111/j.1365-2966.2008.12954.x

Cited by 62 publications

(92 citation statements)

References 69 publications

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“…All this suggests that being a satellite in the vicinity of a massive central is a necessary condition to create a quiescent dwarf galaxy, in agreement with recent results (Haines et al 2007(Haines et al , 2008Weisz et al 2011;Geha et al 2012). Internal mechanisms -such as gas consumption via star formation or feedback effects -appear to be insufficient to completely cease the star formation activity in dwarf galaxies.…”

Section: Environmentsupporting

confidence: 77%

A Virtual Observatory Census to Address Dwarfs Origins (AVOCADO)

Sánchéz-Janssen¹,

Amorín²,

García-Vargas³

et al. 2013

A&A

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Context. Even though they are by far the most abundant of all galaxy types, the detailed properties of dwarf galaxies are still only poorly characterised -especially because of the observational challenge that their intrinsic faintness and weak clustering properties represent. Aims. AVOCADO aims at establishing firm conclusions on the formation and evolution of dwarf galaxies by constructing and analysing a homogeneous, multiwavelength dataset for a statistically significant sample of approximately 6500 nearby dwarfs (M i − 5 log h 100 > −18 mag). The sample is selected to lie within the 20 < D < 60 h −1 100 Mpc volume covered by the SDSS-DR7 footprint, and is thus volume-limited for M i − 5 log h 100 < −16 mag dwarfs -but includes ≈1500 fainter systems. We will investigate the roles of mass and environment in determining the current properties of the different dwarf morphological types -including their structure, their star formation activity, their chemical enrichment history, and a breakdown of their stellar, dust, and gas content. Methods. We present the sample selection criteria and describe the suite of analysis tools, some of them developed in the framework of the Virtual Observatory. We use optical spectra and UV-to-NIR imaging of the dwarf sample to derive star formation rates, stellar masses, ages, and metallicities -which are supplemented with structural parameters that are used to classify them morphologically. This unique dataset, coupled with a detailed characterisation of each dwarf's environment, allows for a fully comprehensive investigation of their origins and enables us to track the (potential) evolutionary paths between the different dwarf types. Results. We characterise the local environment of all dwarfs in our sample, paying special attention to trends with current star formation activity. We find that virtually all quiescent dwarfs are located in the vicinity (projected distances 1.5 h −1 100 Mpc) of L * companions, consistent with recent results. While star-forming dwarfs are preferentially found at separations of the order of 1 h −1 100 Mpc, there appears to be a tail towards low separations ( 100 h −1 100 kpc) in the distribution of projected distances. We speculate that, modulo projection effects, this probably represents a genuine population of late-type dwarfs caught upon first infall about their host and before environmental quenching has fully operated. In this context, these results suggest that internal mechanisms -such as gas exhaustion via star formation or feedback effects -are not sufficient to completely cease the star formation activity in dwarf galaxies, and that becoming the satellite of a massive central galaxy appears to be a necessary condition to create a quiescent dwarf.

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Section: Environmentsupporting

confidence: 77%

A Virtual Observatory Census to Address Dwarfs Origins (AVOCADO)

Sánchéz-Janssen¹,

Amorín²,

García-Vargas³

et al. 2013

A&A

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“…The observations also indicate that dwarf elliptical galaxies in the infalling regions at the periphery of these rich clusters have, on average, younger stellar populations than those located close to the cluster core (Smith et al 2006(Smith et al , 2012a, often with characteristic spectra indicating a recent abrupt truncation of their star-formation activity Gavazzi et al 2010). There is also evidence that some of these low-mass quiescent systems have spiral arms ) and residual star formation in their center (Haines et al 2008). The physical properties of star-forming and quiescent dwarf galaxies in other nearby clusters are thus similar to those observed in Virgo.…”

Section: Other Clustersmentioning

confidence: 99%

On the origin of the faint-end of the red sequence in high-density environments

Boselli

Gavazzi

2014

Astron Astrophys Rev

150

125

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With the advent of the next generation wide-field cameras it became possible to survey in an unbiased mode galaxies spanning a variety of local densities, from the core of rich clusters, to compact and loose groups, down to filaments and voids. The sensitivity reached by these instruments allowed to extend the observation to dwarf galaxies, the most "fragile" objects in the universe. At the same time models and simulations have been tailored to quantify the different effects of the environment on the evolution of galaxies. Simulations, models, and observations consistently indicate that star-forming dwarf galaxies entering high-density environments for the first time can be rapidly stripped from their interstellar medium. The lack of gas quenches the activity of star formation, producing on timescales of ∼1 Gyr quiescent galaxies with spectro-photometric, chemical, structural, and kinematical properties similar to those observed in dwarf early-type galaxies inhabiting rich clusters and loose groups. Simulations and observations consistently identify ram pressure stripping as the major effect responsible for the quenching of the star-formation activity in rich clusters. Gravitational interactions (galaxy harassment) can also be important in groups or in clusters whenever galaxies have been members since early epochs. The observation of clusters at different redshifts combined with the present high infalling rate of galaxies onto clusters indicate that the quenching of the star-formation activity in dwarf systems and the formation of the faint end of the red sequence is a very recent phenomenon.

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“…To analyse the relationship between galaxy properties and their environment, the latter has been defined in different ways: i) galaxy clustering analyses provide a statistical link between the galaxies and their host dark matter haloes (Kauffmann et al 2004), which, combined with their abundances, can constrain the dark matter halo occupation distribution (Zehavi et al 2005); ii) the reconstruction of the local density field as measured with spectroscopic (Cucciati et al 2006;Cooper et al 2008;Kovač et al 2010) or photometric (Scoville et al 2013) redshifts allows high-and low-density contrast regions to be separated; iii) the direct measurement of pair, group, and cluster membership can be compared to isolated field galaxies (Haines et al 2008;Wong et al 2011;Peng et al 2010;Kovač et al 2014); and iv) the reconstruction of the large-scale structure network composed of filaments, nodes, walls, and voids (Aragón-Calvo et al 2010;Sousbie 2011). It offers a new way to describe the anisotropic environment of the cosmic web.…”

Section: Introductionmentioning

confidence: 99%

The VIPERS Multi-Lambda Survey

Moutard

Arnouts

Ilbert

et al. 2016

A&A

107

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We present observations collected in the CFHTLS-VIPERS region in the ultraviolet with the GALEX satellite (far-and near-ultraviolet channels) and in the near-infrared with the CFHT/WIRCam camera (K s band) over an area of 22 and 27 deg 2 , respectively. The depth of the photometry was optimised to measure the physical properties (e.g., star formation rate, stellar masses) of all the galaxies in the VIPERS spectroscopic survey. The large volume explored by VIPERS will enable a unique investigation of the relationship between the galaxy properties and their environment (density field and cosmic web) at high redshift (0.5 ≤ z ≤ 1.2). In this paper, we present the observations, the data reductions, and the build-up of the multi-colour catalogues. The CFHTLS-T0007 (gri-χ 2 ) images are used as reference to detect and measure the K s -band photometry, while the T0007 u * -selected sources are used as priors to perform the GALEX photometry based on a dedicated software (EMphot). Our final sample reaches NUV AB ∼ 25 (at 5σ) and K AB ∼ 22 (at 3σ). The large spectroscopic sample (∼51 000 spectroscopic redshifts) allows us to highlight the robustness of our star/galaxy separation and the reliability of our photometric redshifts with a typical accuracy of σ z ≤ 0.04 and a fraction of catastrophic failures η ≤ 2% down to i ∼ 23. We present various tests on the K s -band completeness and photometric redshift accuracy by comparing our results with existing overlapping deep photometric catalogues. Finally, we discuss the BzK sample of passive and active galaxies at high redshift and the evolution of galaxy morphology in the (NUV − r) vs. (r − K s ) diagram at low redshift (z ≤ 0.25) based on the high image quality of the CFHTLS.

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The SDSS-GALEX viewpoint of the truncated red sequence in field environments at z ∼ 0

Cited by 62 publications

References 69 publications

A Virtual Observatory Census to Address Dwarfs Origins (AVOCADO)

A Virtual Observatory Census to Address Dwarfs Origins (AVOCADO)

On the origin of the faint-end of the red sequence in high-density environments

The VIPERS Multi-Lambda Survey

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