H<i>α</i>3: an H<i>α</i>imaging survey of HI selected galaxies from ALFALFA

Fossati, M.; Gavazzi, G.; Savorgnan, Giulia; Fumagalli, Michele; Boselli, A.; Gutiérrez, L.; Toledo, Hector Hernández; Giovanelli, Riccardo; Haynes, Martha P.

doi:10.1051/0004-6361/201220915

Cited by 60 publications

(73 citation statements)

References 109 publications

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“…A KolmogorovSmirnov test indicates that the probability that the two samples are drawn from the same parent population is 2 × 10 −9 %, i.e., they differ significantly. This is consistent with an Hα disk truncated by ram-pressure (Fumagalli & Gavazzi 2008), such as in the prototype NGC 4569 in Virgo or in NGC 4848 in Coma (Fossati et al 2012). These cases are different from the HI-rich systems, which tend to host Hα emission extended across the entire disk (as discussed in Paper IV).…”

Section: Activity On Nuclear Scalesupporting

confidence: 79%

“…Paper II ) outlined the analysis, including the study of the scaling relations between HI mass, stellar mass, star formation, and the environmental conditions. Paper IV (Fossati et al 2013) will analyze the structural properties of galaxies in the Local and Coma superclusters, and Paper V will contain the Hα3 data (fluxes and images) in the Coma supercluster.…”

Section: Introductionmentioning

confidence: 99%

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Hα3: an Hαimaging survey of HI selected galaxies from ALFALFA

Gavazzi

Savorgnan

Fossati

et al. 2013

A&A

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Context. We present the analysis of Hα3, an Hα narrow-band imaging follow-up survey of galaxies selected from the HI Arecibo Legacy Fast ALFA Survey (ALFALFA) in the Coma supercluster. Aims. Taking advantage of Hα3, which provides the complete census of the recent star formation in HI-rich galaxies in the local universe, we explored the hypothesis that a morphological sequence of galaxies of progressively earlier type and lower gas-content exists in the neighborhood of a rich cluster of galaxies such as Coma, with a specific star formation activity that decreases with increasing local galaxy density and velocity dispersion. Methods. By using the Hα hydrogen recombination line as a tracer of the "instantaneous" star formation, complemented with optical colors from SDSS, we investigated the relationships between atomic neutral gas and newly formed stars in different local galaxy density intervals, for many morphological types, and over a wide range of stellar masses (10 9 to 10 11.5 M ). Results. In the dwarf regime (8.5 < log (M * /M ) < 9.5) we identify a four-step sequence of galaxies with progressively redder colors (corrected for dust extinction), i.e., of decreasing specific star formation, from (1) HI-rich late-type galaxies (LTGs) belonging to the blue cloud that exhibit extended plus nuclear star formation, (2) ∼0.1 mag redder, HI-poor LTGs with nuclear star formation only, (3) ∼0.35 mag redder, HI-poor galaxies without either extended or nuclear star formation, but with nuclear post-star-burst (PSB) signature, (4) ∼ 0.5 mag redder early-type galaxies (ETGs) that belong to the red sequence, and show no gas or star formation on all scales. Along this sequence the quenching of the star formation proceeds radially outside-in. The progression toward redder colors found along this "morphological" (gas content) sequence is comparable to the one obtained from increasing the local galaxy density, from cosmic filaments (1 2), to the rich clusters (2 3 4). Conclusions. In the dwarf regime we find evidence for an evolution of HI-rich LTGs into ETGs through HI-poor LTGs and PSB galaxies driven by the environment. We identify ram-pressure as the mechanism most likely responsible for this transformation. We conclude that infall of galaxies has proceeded for the last 7.5 Gyr, building up the Coma cluster at a rate of approximately 100 galaxies with log (M * /M ) > 9.0 per Gyr.

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Section: Activity On Nuclear Scalesupporting

confidence: 79%

Section: Introductionmentioning

confidence: 99%

Hα3: an Hαimaging survey of HI selected galaxies from ALFALFA

Gavazzi

Savorgnan

Fossati

et al. 2013

A&A

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“…15 An accurate study of the star-formation properties of low-luminosity cluster galaxies has been made possible owing to the narrow-band Hα imaging data that our team has obtained in these past years. By comparing the Hα morphology of galaxies in Virgo, Coma and A1367 to those of field galaxies selected according to similar criteria, Fossati et al (2013) have shown that the star-forming disk of LTGs, including dwarf systems, is truncated once the galaxies are devoid of their gas (Fig. 11).…”

Section: Star Formationmentioning

confidence: 99%

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

Boselli

Gavazzi

2014

Astron Astrophys Rev

155

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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“…The angular resolution of the HI, CO, and farinfrared images now available thanks to interferometric observations in the radio domain and to the superior quality of the instruments on board of Herschel revealed that cluster galaxies have truncated gaseous and dust discs (Fumagalli et al 2009;Boselli et al 2014b;Cortese et al 2012a;Davis et al 2013), suggesting that the mechanism responsible for their stripping acts outsidein. The star formation activity of the late-type galaxies in clusters is also systematically reduced with respect to that of field objects (Kennicutt 1983;Gavazzi et al 1998Gavazzi et al , 2002aGavazzi et al , 2006b and is limited to the inner disc (Koopmann & Kenney 2004;Boselli & Gavazzi 2006;Cortese et al 2012b;Fossati et al 2013). The correlation between the molecular gas content and the activity of star formation (e.g.…”

Section: Introductionmentioning

confidence: 99%

Quenching of the star formation activity in cluster galaxies

Boselli

Roehlly

Fossati

et al. 2016

A&A

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119

155

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We study the star formation quenching mechanism in cluster galaxies by fitting the spectral energy distribution (SED) of the Herschel Reference Survey, a complete volume-limited K-band-selected sample of nearby galaxies including objects in different density regions, from the core of the Virgo cluster to the general field. The SEDs of the target galaxies were fitted using the CIGALE SED modelling code. The truncated activity of cluster galaxies was parametrised using a specific star formation history with two free parameters, the quenching age QA and the quenching factor QF. These two parameters are crucial for the identification of the quenching mechanism, which acts on long timescales when starvation processes are at work, but is rapid and efficient when ram pressure occurs. To be sensitive to an abrupt and recent variation of the star formation activity, we combined twenty photometric bands in the UV to far-infrared in a new way with three age-sensitive Balmer line absorption indices extracted from available medium-resolution (R ∼ 1000) integrated spectroscopy and with Hα narrow-band imaging data. The use of a truncated star formation history significantly increases the quality of the fit in HI-deficient galaxies of the sample, that is to say, in those objects whose atomic gas content has been removed during the interaction with the hostile cluster environment. The typical quenching age of the perturbed late-type galaxies is QA < ∼ 300 Myr whenever the activity of star formation is reduced by 50% < QF ≤ 80% and QA < ∼ 500 Myr for QF > 80%, while that of the quiescent early-type objects is QA 1−3 Gyr. The fraction of late-type galaxies with a star formation activity reduced by QF > 80% and with an HI-deficiency parameter HI − de f > 0.4 drops by a factor of ∼5 from the inner half virial radius of the Virgo cluster (R/R vir < 0.5), where the hot diffuse X-ray emitting gas of the cluster is located, to the outer regions (R/R vir > 4). The efficient quenching of the star formation activity observed in Virgo suggests that the dominant stripping process is ram pressure. We discuss the implication of this result in the cosmological context of galaxy evolution.

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Hα3: an Hαimaging survey of HI selected galaxies from ALFALFA

Cited by 60 publications

References 109 publications

Hα3: an Hαimaging survey of HI selected galaxies from ALFALFA

Hα3: an Hαimaging survey of HI selected galaxies from ALFALFA

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

Quenching of the star formation activity in cluster galaxies

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