Spectrophotometry of Galaxies in the Virgo Cluster. I. The Star Formation History

By G. Gavazzi, C. Bonfanti, G. Sanvito, A. Boselli, M. Scodeggio. 2002

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In Astronomy and Astrophysics

Citations in the corpus

Environmental Effects on Late‐Type Galaxies in Nearby Clusters (2006, methodology): “G. Gavazzi et al. (2006, in preparation) recently analyzed the relation between H i deficiency and metallicity using integrated long-slit spectra of a large sample of ∼300 galaxies in the Virgo Cluster and in the Coma/A1367 supercluster.”
Cold gas properties of the Herschel Reference Survey - II. Molecular and total gas scaling relations (2014, background): “…of normal, late-type galaxies, such as those composing the HRS sample,is not constant over cosmic time but smoothly changes following different paths according to the morphological type (Sandage 1986) or the total mass of the parent galaxy (e.g. Gavazzi et al. 1996, 2002; Boselli et al. 2001).”
The Origin of Dwarf Ellipticals in the Virgo Cluster (2008, methodology): “…such that infall in low mass galaxies is shifted towards later time: this mimics the fact that massive galaxies are formed early on and that low mass galaxies are still forming at the current time, a well known fact (Gavazzi et al. 1996, 2002; Boselli et al. 2001) nowadays called “downsizing”.”
The effect of the environment on the Hi scaling relations (2011, background): “…previous analysis showing that cluster galaxies have in general a lower star formation rate than their field counterpart (Boselli & Gavazzi 2006; Gavazzi et al. 2002; Gómez et al. 2003), suggesting that the gas loss is behind the quenching of the star formation activity (Gavazzi et al. 2006;…”
Integral field spectroscopy with SINFONI of VVDS galaxies I. Galaxy dynamics and mass assembly at 1.2 < z < 1.6 (2009, methodology): “…models, generated using the BC03 population synthesis code (Bruzual & Charlot 2003), assuming a set of “delayed” star formation histories (see Gavazzi et al. 2002 fordetails), a Salpeter (1955) IMF with lower and upper mass cutoffs of respectively 0.1 and 100 M⊙, a metallicity ranging from…”
Structure of Disk-dominated Galaxies. II. Color Gradients and Stellar Population Models (2004, background): “…clearly an unrealistic assumption with regards to galaxy evolution (as it also ignores feedback effects from stellar winds and supernovae), but it still allows us a reasonable comparison of relative metallicities and ages within and among galaxies (Abraham et al. 1999; BdJ00; Gavazzi et al. 2002).”
The Metallicity of Galaxy Disks: Infall versus Outflow (2006, background): “In low mass galaxies, infall is required to explain why their star formation rates are typically observed to rise to the present day (e.g. Brinchmann et al. 2004; Gavazzi et al. 2002).”
GALEX–SDSS–WISE LEGACY CATALOG (GSWLC): STAR FORMATION RATES, STELLAR MASSES, AND DUST ATTENUATIONS OF 700,000 LOW-REDSHIFT GALAXIES (2016, background): “In contrast, the delayed exponential SF history is smooth (e.g., Gavazzi et al. (2002)): it starts from zero SFR, reaches a peak at some time and then declines.”
The quasar relation through cosmic time – II. Evidence for evolution from z = 3 to the present age (2009, background): “If the majority of the stellar population of massive galaxies did form at high redshift, as suggested by several pieces of evidence (Gavazzi et al. 2002; Thomas et al. 2005; Renzini 2006; Cirasuolo et al. 2008; Cappellari et al. 2009), one may assume that the Mass-to-Light ratio passively evolves…”
Specific Star Formation Rate Profiles in Nearby Spiral Galaxies: Quantifying the Inside-Out Formation of Disks (2006, background): “However, such short SFR timescales are expected only in elliptical and giant spiral galaxies, whereas for smaller spirals τ values of ≃7Gyr (for which our simple model yields nearly equal results – 21 – to those with τ = ∞) are commonly inferred (Gavazzi et al. 2002).”
Dust Attenuation in the Nearby Universe: A Comparison between Galaxies Selected in the Ultraviolet and in the Far-Infrared (2004, background): “Such a steep decrease of the SFR is typical of elliptical or lenticular galaxies (Gavazzi et al. 2002).”
MUSE sneaks a peek at extreme ram-pressure stripping events - I. A kinematic study of the archetypal galaxy ESO137-001 (2014, background): “2002; Gavazzi et al. 2002; Kauffmann et al. 2004; Balogh et al. 2004; Boselli & Gavazzi 2006; Boselli et al. 2008; Gavazzi etal.”
The GALEX Ultraviolet Atlas of Nearby Galaxies (2006, background): “…that the star formation history of galaxies depends strongly on their stellar or total mass. Lowmass galaxies show relatively flat star formation histories, while moremassive systems have shorter timescales of formation (e.g., Gavazzi et al. 1996, 2002;Gavazzi&Scodeggio 1996;Boselli et al. 2001).”
The ACS Virgo Cluster Survey. I. Introduction to the Survey (2004, background): “…infrared (Boselli et al. 1997; Tuffs et al. 2002), and radio (van Driel et al. 2000; Solanes et al. 2002) wavelengths—as well as combinations thereof (Gavazzi et al. 2002, 2003; Boselli et al. 2003)—have largely confirmed the view of Virgo as an environment that is, in most respects, typical of…”
RADIAL DISTRIBUTION OF STARS, GAS, AND DUST IN SINGS GALAXIES. II. DERIVED DUST PROPERTIES (2009, background): “Therefore, they have presumably – 28 – undergone rapidly declining SFHs, with typical timescales of just a few Gyr (Gavazzi et al. 2002), in contrast to late-type spirals, which exhibit longer timescales.”
Environment and self-regulation in galaxy formation (2009, background): “Note that the latter is a universal characteristic of galaxy formation and is not restricted to early-types (Gavazzi et al. 2002; Heavens et al. 2004; Cid Fernandes et al. 2007; Panter et al. 2007).”
GASP. I. Gas Stripping Phenomena in Galaxies with MUSE (2017, methodology): “Ionized gas studies based on Hα imaging are another excellent tracer of gas stripping in clusters (e.g., Gavazzi et al. 2002; Yagi et al. 2010; Fossati et al. 2012; Yoshida et al. 2012; Boselli et al. 2016).”
Toward a Better Understanding of Cosmic Chronometers: A New Measurement of H(z) at z ∼ 0.7 (2021, background): “This degeneracy is well known in the literature (e.g., Gavazzi et al. 2002) and together with the age-metallicity degeneracy is one of the major obstacles in the accurate reconstruction of galaxy star formation histories.”