1 Introduction

The origin of dwarf ellipticals in the Virgo cluster

Abstract

We study the evolution of dwarf ( 10 L) star forming and quiescent galaxies in the Virgo cluster by comparing their UV to radio centimetric properties to the predictions of multizone chemo-spectrophotometric models of galaxy evolution especially tuned to take into account the perturbations induced by the interaction with the cluster intergalactic medium. Our models simulate one or multiple ram pressure stripping events and galaxy starvation. Models predict that all star forming dwarf galaxies entering the cluster for the first time loose most, if not all, of their atomic gas content, quenching on short time scales ( 150 Myr) their activity of star formation. These dwarf galaxies soon become red and quiescent, gas metal-rich objects with spectrophotometric and structural properties similar to those of dwarf ellipticals. Young, low luminosity, high surface brightness star forming galaxies such as late-type spirals and BCDs are probably the progenitors of relatively massive dwarf ellipticals, while it is likely that low surface brightness magellanic irregulars evolve into very low surface brightness quiescent objects hardly detectable in ground based imaging surveys. The small number of dwarf galaxies with physical properties intermediate between those of star forming and quiescent systems is consistent with a rapid ( 1 Gyr) transitional phase between the two dwarf galaxies populations. These results, combined with statistical considerations, are consistent with the idea that most of the dwarf ellipticals dominating the faint end of the Virgo luminosity function were initially star forming systems, accreted by the cluster and stripped of their gas by one or subsequent ram pressure stripping events.

Subject headings:
Galaxies: interactions – Ultraviolet: galaxies – Galaxies: clusters: individual: Virgo

1. Introduction

Dwarf galaxies (-18) are the most common objects in the nearby universe (Ferguson & Binggeli 1994). Their importance resides in the fact that they represent in cold dark matter models the building blocks of hierarchical galaxy formation (e.g. White & Rees 1978, White & Frenk 1991). Their study is thus fundamental for constraining models of galaxy formation and evolution.
Observations of dwarf galaxies, necessarily limited to the nearby universe, revealed however a more complex origin than that predicted by models, making this class of galaxies even more interesting. Among dwarf galaxies, dwarf ellipticals (dE) and the less luminous dwarf spheroidals (dSph)5 are more common than star forming Im and BCDs (Ferguson & Binggeli 1994). Firstly thought as the low-luminosity extension of bright ellipticals, several observational evidences indicate that they form an independent class of objects (Bender et al. 1992). Dwarf and giant ellipticals have Sersic light profiles of index , with progressively increasing with luminosity (Graham & Guzman 2003; Gavazzi et al. 2005a). The colour magnitude relations measured using resolved stars in local group dwarfs spheroidals (Mateo 1998; Grebel 1999), the optical (Conselice et al. 2003a) and UV (Boselli et al. 2005a) integrated color magnitude relations, the subsolar [/Fe] ratios (Van Zee et al. 2004a) and the UV to near-IR spectral energy distribution of dE in the Virgo cluster (Gavazzi et al. 2002a), however, all indicate a more gradual star formation history with recent episodes of activity in these low-luminosity quiescent systems than in massive ellipticals. This constitutes the first evidence against their very old origin. A further disagreement with model predictions is that, although more frequent than bright galaxies, their number density is still significantly smaller than predicted by hierarchical models of galaxy formation for the field luminosity function (Kauffmann et al. 1993; Cole et al. 1994; Somerville & Primack 1999, Nagashima et al. 2005) or for the local group (Klypin et al. 1999; Bullock et al. 2000).
The strong similarities in the structural properties of star forming and quiescent dwarf galaxies in the nearby universe, namely their similar optical morphology and light profiles (both roughly exponentials), suggested that dwarf ellipticals might result from gas removal and subsequent suppression of star formation in gas rich dwarf galaxies. Gas removal might result either from its blowout due to the kinetic energy injected into the ISM by supernova explosion following a strong burst of star formation (Dekel & Silk 1986, Vader 1986, Yoshii & Arimoto 1987), gas exhaustion through subsequent episodes of star formation (Davies & Phillipps 1988), or from external perturbations induced by the hostile environment in which galaxies evolve. External perturbations include tidally induced mass loss in high speed encounters (Moore et al. 1998), tidal stirring (Mayer et al. 2001a, 2001b) and ram-pressure stripping induced by nearby companions (Lin & Faber 1983) or by the hot intergalactic medium in massive clusters (van Zee et al. 2004b).
Several observational evidences favor the environmental scenario against the gas blowout due to supernova explosions. The clearest indication that the environment plays an important role in the formation and evolution of dwarfs is the morphology segregation effect (Dressler 1980) which extends to low-luminosity systems (Binggeli et al. 1988; 1990; Ferguson & Binggeli 1994). Furthermore it has been recently claimed that the removal of the ISM through supernova winds is quite difficult in low-luminosity, dark matter dominated systems (Mac Low & Ferrara 1999; Ferrara & Tolstoy 2000; Silich & Tenorio-Tagle 1998, 2001). The discrete star formation history of several dwarf galaxies in the local group, as deduced by the analysis of their colour magnitude relation (Mateo 1998; Grebel 1999), is a further indication that dwarf spheroidals can retain their ISM through several episodes of star formation.
Another observational evidence favoring the transformation of star forming galaxies into quiescent dwarf ellipticals is the presence of rotationally supported (Pedraz et al. 2002; Geha et al. 2003; van Zee et al. 2004b) and/or HI gas rich (Conselice et al. 2003b; van Zee et al. 2004b) dE in the Virgo cluster. Recent studies based on SDSS imaging and spectroscopic data have shown that 50 % of the bright end of the dE galaxy population in the Virgo cluster is characterized by disk features such as spiral arms or bars, this fraction decreasing down to 5% at lower luminosities (Lisker et al. 2006a; see also Graham et al. 2003). Meanwhile 15% of the bright dE in Virgo have blue centers revealing a recent activity of star formation. From a statistical point of view, the line-of-sight velocity distribution of dE inside clusters is similar to that of late-type galaxies suggesting a recent infall (Binggeli et al. 1993; Conselice et al. 2001).
Not all observational evidences, however, are consistent with the transformation of dwarf star forming galaxies into dwarf ellipticals under the effect of the environment. To reproduce the color magnitude relation of dwarf ellipticals, it has been claimed that magellanic irregulars should have faded 1.5 magnitudes in the B band thus reaching surface brightnesses weaker than 25 mag arcsec, values significantly smaller than the observed ones (Bothun et al. 1986). Most of the bright dwarf ellipticals in the Virgo cluster have a bright nucleus (Binggeli et al. 1985; Ferguson & Binggeli 1994) of small size, as shown by HST observations ( 4 pc, Côte et al. 2006) while dwarf irregulars do not. While both dwarf irregulars and dwarf ellipticals follow different metallicity-luminosity relations, dwarf spheroidals are more metal-rich than dwarf irregulars at the same optical luminosity (Grebel et al. 2003 and references therein). The flattening distribution of non nucleated dE is similar to that of late-type spirals, Im and BCD (Binggeli & Popescu 1995). This class of objects, however, is significantly less round than nucleated systems. Although they exist, the fraction of objects belonging to the intermediate dIrr/dE transition class is too small. Furthermore a simple transformation of Im galaxies recently infalling in the cluster into dE does not seem to reproduce the observed difference in the cluster and field luminosity functions (Conselice 2002). Other strong constraints against the transformation of star forming into quiescent dwarfs are given by the studies of globular clusters, taken as a probe of the early phases of galaxy formation. The specific frequency of globular clusters in dwarf ellipticals, in fact, is significantly higher than that of star forming galaxies. This result has been interpreted as an evidence for a different formation scenario for the two galaxy populations (Miller et al. 1998; Strader et al. 2006).
With the aim of explaining these evidences, slightly different evolutionary scenarios have been proposed: cluster dwarf ellipticals might have been formed from higher surface brightness BCD galaxies (Bothun et al. 1986), or from tidally induced mass loss in multiple high speed encounters of massive galaxies (galaxy harassment; Mastropietro et al. 2005). Alternatively, Lisker et al. (2006a; 2006b; 2007) proposed that the cluster dwarf elliptical galaxy population is composed of different subcategories of objects, of which not all have been formed from gas stripped star forming dwarfs. As here emphasized the issue is still hotly debated.
A few years ago we started collecting multifrequency data covering the whole electromagnetic spectrum for galaxies in nearby clusters in order to study the effects of the environment on galaxy evolution. Up to now our research was primarily focused on the bright end of the luminosity function. Our interest covered the present and past star formation activity (Gavazzi et al. 1991, 1998, 2002b, 2006a), the atomic (Gavazzi et al. 2005b, 2006b) and molecular gas content (Boselli 1994; Boselli et al. 1994, 1997a, 2002), the radio continuum and IR properties of cluster galaxies (Gavazzi & Boselli 1999; Gavazzi et al. 1991). The results of our analysis, combined with those obtained by other teams, are summarized in a recent review article (Boselli & Gavazzi 2006).
The aim of the present paper is to extend the multifrequency analysis to the low-luminosity end of the luminosity function with the purpose of studying the possible transformation of star forming objects into dwarf ellipticals. This exercise is here done using a complete sample of galaxies in the Virgo cluster. The novelty of this work compared to previous investigations is twofold: the analyzed sample has an unprecedented multifrequency spectral coverage from the UV to near-IR imaging data. Furthermore this unique dataset is compared to the predictions of multizone chemo-spectrophotometric models of galaxy evolution here adapted to take into account the perturbations induced by the cluster environment. The type of perturbation simulated by the models are ram-pressure stripping (Gunn & Gott 1972) and starvation (Larson et al. 1980). The combination of multifrequency data with these models on the galaxies NGC 4569 (Boselli et al. 2006) and NGC 4438 (Boselli et al. 2005b) indeed indicated how powerful this method is for studying and constraining the evolution of cluster galaxies.
Our previous investigations have emphasized that the most important parameter governing the evolution is the total mass as traced by the near-IR H band luminosity (Gavazzi et al. 1996; 2002a; Boselli et al. 2001). Below a certain mass ( 10 L) we identify the sequence of dwarf galaxies that we subdivide into quiescent and star forming disregarding their detailed morphology.
A major uncertainty in the interpretation of the multifrequency data, and in particular of those at short wavelength, is the extinction correction, which however is expected to be minor in low-metallicity star forming dwarf systems (Buat & Xu 1996) and probably negligible in dwarf ellipticals. For these reasons we decided to limit the present analysis to the cluster dwarf galaxy population, leaving the discussion relative to massive galaxies to a future communication. With the aim of driving the reader’s attention to the scientific results of this work, the presentation of the dataset and the general description of the models are given in Appendix.

2. Sample and data

The analysis presented in this work is based on an optically selected sample of galaxies in the Virgo cluster (12h R.A.(2000) 13h; 0 dec 18) extracted from the Virgo Cluster Catalogue (VCC) of Binggeli et al. (1985), with 18 mag (that for a distance of 17 Mpc gives -13.15) which corresponds to its completeness limit.
Although the present analysis is focused on the dwarf star forming (Scd-Im-BCD) and quiescent (dE-dS0) galaxy populations, that we define as 10 L (which roughly corresponds to -18 mag), we also include brighter objects selecting all galaxies with 18 mag. This are all bona-fide Virgo cluster members, whose distances have been assigned following the subcluster membership criteria of Gavazzi et al (1999) which is based on combined position and redshift data (now available for 83% of the objects). The adopted distance for each subgroup is: 17 Mpc for cluster A, the North and East clouds and the Southern extension, 23 Mpc for cluster B and 32 Mpc for the W and M clouds. The selected sample includes a total of 1010 galaxies, 445 of which are classified as dE or dS0, 215 as Scd-Sd, Im or BCD and 45 as dE/Im or ? in the VCC. Because of their intrinsic color, the lowest H band luminosities (thus the lowest total dynamical masses) are reached only in star forming dwarfs.
Model predictions are compared to UV to near-IR imaging and spectroscopic data collected thanks to our own observations (optical, near-IR and H imaging, optical integrated spectroscopy) or from different ground based (SDSS) and space (GALEX) missions as well as from multifrequency data available in the literature. The detailed description of the used dataset is given in the Appendix.

3. The evolution of low-luminosity late-type galaxies in clusters: model predictions

The evolution of galaxies is traced using the multi-zone chemical and spectro-photometric models of Boissier & Prantzos (2000), updated with an empirically-determined star formation law (Boissier et al 2003) relating the star formation rate to the total-gas surface densities, and modified to simulate the effects induced by the interaction with the cluster IGM. In the starvation scenario (Larson et al. 1980, Balogh et al. 2000, Treu et al. 2003), the cluster acts on large scales by removing any extended gaseous halo surrounding the galaxy, preventing further infall of such gas onto the disk. The galaxy then become anemic simply because it exhausts the gas reservoir through on-going star formation. Starvation has been simulated by stopping infall in the model.
The ISM of galaxies crossing the cluster with velocities of 1000 km s can be removed by the ram pressure exerted by the hot and dense IGM (Gunn & Gott 1972). Gas removal induces a quenching of the star formation activity (Boselli & Gavazzi 2006). The ram pressure stripping event is simulated by assuming a gas-loss rate inversely proportional to the potential of the galaxy, with an efficiency depending on the IGM gas density radial profile of the Virgo cluster given by Vollmer et al. (2001). The details of the models are given in the Appendix. Here we present their results.

3.1. The starvation scenario

The total gas content, the activity of star formation and the metallicity of dwarf galaxies are barely affected by starvation unless the interaction started long time agoo, as shown for a model galaxy of rotational velocity =55 km s and spin parameter = 0.05 (Fig. 1 to 4). HI-deficiencies of 0.8, similar to the average value of Virgo galaxies within the virial radius of the cluster, can be obtained only if starvation started more than 6 Gyr ago (see Fig. 1).
Gas removal induces a mild decrease of the star formation activity (Fig. 1). For this reason galaxies suffering starvation for a long time are redder than similar unperturbed objects, in particular in those color indices tracing significantly different stellar populations (, , ; Fig. 2). The color index is barely affected, because starvation acts on longer timescales than the lifetimes of the stellar populations emitting in the two UV filters ( 10 years)6, and does not totally eliminate these populations as significant amount of star formation, although reduced, still takes place.
Gas metallicity increases more than in the unperturbed case since newly formed metals are diluted in smaller amounts of gas, and since the metallicity is not reduced by the infall of pristine gas (Fig. 3).
The effects of starvation on the structural properties of galaxies (provided that the interaction started a long time ago) are major. The decrease of the surface brightness is expected to be 1 mag in the H band to 3 mag in the FUV band for an interaction started 6 Gyr ago (Fig. 4). The effect would be significantly smaller for a recent interaction.
The effects of starvation on the effective radius are minor since starvation is a global effect, and thus does not depend on radius. Nevertheless, an effect on the effective radius is visible, especially at short wavelengths. The reason is the radial dependence of infall (galaxies are formed inside-out in our model). When the starvation starts, infall has occurred in the inner zones, where relatively large amount of gas can be found (and thus high level of star formation and UV surface brightness). This gas is progressively depleted by star formation, leading to a decrease of the inner surface brightness while the outer parts, where the star formation is low because of the low amount of gas present, dim at a lower rate. The net effect is an increase in the effective radius.

3.2. The ram pressure stripping scenario

The effects of a ram-pressure stripping event started 1 Gyr ago (=1 Gyr) on the evolution of total gas content, star formation activity, stellar populations (UV to near-IR color indices), metallicity and structural (effective radius and surface brightness) parameters of dwarf galaxies as predicted by our models are also shown in Fig. 1 to 4. Because of the shallow potential well of dwarf galaxies, most of their gas is efficiently removed on very short time scales ( 150 Myr), leading to the formation of extremely gas deficient objects with HI-deficiencies 2 for = 1.2 M kpc yr, or 1.2 for = 0.4 M kpc yr ( is the parameter that quantifies the efficiency of the process of ram pressure stripping; see the Appendix B).
As a consequence of this lack of gas, star formation abruptly decreases by a factor of 10 to 100 and continues at a very low level afterward. In the = 1.2 M kpc yr model, the gas content progressively increases after the interaction as stars of small masses reach their end of life point and return more gas to the interstellar medium (we do not use the instantaneous recycling approximation). The star formation rate is fed by this recycled gas, and increases as well, staying nevertheless at low levels. In models with a lower ram pressure efficiency, the recycled gas represents a small amount with respect to the one left after the interaction. As a result, this effect is not visible: the gas and the star formation rate are about constant after the event.
Stopping the star formation makes galaxies redder. Since the decrease of the star formation activity is rapid, the younger stellar populations, those emitting in the FUV and NUV filters, are the most affected: the color index, for instance, increases by 4.5 magnitudes in 1 Gyr, while by only 1 magnitude.
As for the starvation scenario, the gas metallicity index significantly increases with time. The increase of the gas metallicity is higher during a ram pressure stripping event since virtually all the gas has been removed, while some gas is left in the disk during a starvation event. There is thus less dilution for a ram pressure event than in the occurrence of starvation.
Stopping the star formation drastically changes the structural properties of galaxies. Stripped galaxies have lower surface brightnesses and are slightly smaller with respect to unperturbed objects when observed at short wavelengths. At long wavelengths, where the emission is dominated by the evolved stellar populations, the effects are almost negligible (Fig. 4) 7.
An accurate comparison between the effects induced by ram-pressure stripping and starvation on dwarf galaxy properties indicates that the former interaction is more efficient than the latter in removing gas and suppressing any star formation activity in galaxies on short time scales. To be efficient, starvation should have started several Gyr ago. Recent ram pressure stripping events, however, did not have enough time to perturb the old stellar component emitting in the near-IR.
The effects of multiple encounters on the gas content and star formation activity of a dwarf, star forming galaxy of spin parameter = 0.05 and rotational velocity = 55 km s are shown in Fig. 5. The comparison of Fig. 5 with Fig. 1 (single stripping event) shows how multiple interactions make galaxies even poorer of gas and, as a consequence, redder in colors, than similar objects that underwent a single ram pressure stripping event. For low efficiencies, successive crossings are almost additive (some gas left on the first crossing is removed on the next one). For large efficiencies, the second crossing, occurring 1.7 Gyr after the first one, mostly remove any recycled gas, quenching a possible increase of star formation. In both cases, multiple crossing galaxies end up as redder, poorer in gas objects. A summary of the predicted perturbations induced by ram pressure stripping and starvation on the physical and structural properties of dwarf galaxies are given in Table 1.

4. Models vs. observations

The multifrequency dataset available for dwarf galaxies in the Virgo cluster (see Appendix) allows us to compare model predictions with observations.

4.1. Gas content

Ram-pressure stripping models are able to reproduce the HI-deficient8 galaxy population while starvation does not (Fig. 6) 9. As previously remarked in sect. 3.2, ram-pressure stripping can produce HI-deficient massive galaxies ( 10 L) such as those observed in Virgo. For a massive galaxy with = 220 km s and spin parameter =0.05, a ram pressure stripping event started 1 Gyr ago with = 0.4 M kpc yr leads to an HI-deficiency of 0.8, similar to the average HI-deficiency of massive spiral galaxies in the center of the Virgo cluster (Gavazzi et al 2005b; Boselli & Gavazzi 2006). More extreme HI-deficient objects of the cluster (HI-deficiency 1.4) can be produced by assuming = 1.2 M kpc yr. NGC 4569 can be taken as a typical object of this second category (Boselli et al. 2006).
We notice however that the HI emission of the ram-pressure stripped dwarf galaxy population can be hardly detected by the recent HI surveys such as ALFALFA (Giovanelli et al. 2005) and AGES (Auld et al. 2006), able to reach only galaxies with HI gas masses 10 M (ALFALFA) or slightly smaller (AGES) at the distance of Virgo (17 Mpc) (dashed line in Fig. 6). Galaxies less luminous than 10 L would be detected only in the case stripping is still under way. Since the gas stripping event is short in time ( 150 Myr), we expect that these objects are extremely rare.

4.2. Stellar populations

Figure 7 shows several color-magnitude relations for galaxies in the Virgo cluster. We easily recognize the well known red and blue sequences relative to the quiescent and star forming galaxy populations (Scodeggio et al. 2002; Gil de Paz et al. 2007; see also Visvanathan & Sandage 1977; Bower et al. 1992 for early-type galaxies and Tully et al. 1982, Gavazzi et al. 1996 for late-type galaxies) and a relatively large number of objects in between these two sequences (see Sec. 5). We remind that the reddest quiescent dwarfs might be undetected in the UV bands because of the sensitivity of GALEX. Model predictions clearly show that only a ram-pressure stripping event (and not starvation) is able to significantly modify the colors of galaxies. As expected the effects are more important at short than at long wavelengths, affecting more colors as e.g. , than e.g. . The colour index of bright spirals ( 10 L) can increase by up to 1 mag in and 2 mag in or 500 Myr after the interaction, making galaxies as red as the most deficient spirals located in between the red and blue sequences in the color-magnitude diagram. NGC 4569 might be one of these objects.
The effect on dwarfs is more important, making star forming irregulars as red as dwarf ellipticals of similar luminosity in the case of an efficient gas stripping event or just after they crossed twice the cluster core ( 2 Gyr), as shown in Fig. 8 (see also Fig. 13).

4.3. Metallicity

Figure 9 shows the relationship between the gas 12 Log(O/H) index and the total H band luminosity of galaxies in the Virgo cluster. Given the large uncertainty in both models (it is well known that metal yields are uncertain by at least a factor 2, see e.g. Prantzos 2000, and chemical evolution models are somewhat degenerate due to uncertainties on e.g. the Initial Mass Function or star formation history) and observables (0.3 dex), it is not surprising that models for the unperturbed galaxies are slightly shifted with respect to the data. We should thus consider only relative values. It is however clear that all starvation and ram pressure models predict both an increase of the gas metallicity and a decrease of the total H band luminosity consistent with the dispersion in the data. This might explain the increase of gas metallicity observed in Virgo (Vilchez 1995) and Hydra (Duc et al. 2001) cluster galaxies.

4.4. Structural properties

The structural properties of quiescent and star forming dwarf galaxies are compared to model predictions in Fig. 10 and 11. The near-IR light concentration index (defined as the ratio of the radii including 75 and 25% of the total light), is a quantitative indicator of the shape of the light profile in galaxies which reflects the exponent of the Sersic law. In practice it can be used as an indicator of the presence of bulges 10, thus to quantitatively compare the radial profiles of star forming and quiescent dwarfs, as shown in Fig. 10. For luminosities 10L the quiescent galaxy population is undersampled. In the 10 10 L both galaxy populations are dominated by objects with near-IR concentration indices 3 (55% and 78% for early and late-type respectively), typical of exponential profiles. The frequency of dwarfs with pronounced central cusps ( 3) increases with luminosity, with an overall frequency comparable in the quiescent (64%) and star forming (42%) galaxy populations in the luminosity range 10 10 L. Values of 3 are more frequent in nucleated dEs (large filled dots), and in high surface brightness star forming galaxies (spirals, black open squares and green crosses, and BCDs11, blue open triangles). We remind that ram pressure stripping events are not expected to deeply modify the relative weight of bulges in perturbed galaxies (Boselli et al. 2006).
For the star forming galaxies, the H band effective surface brightness and the luminosity are correlated, with a relatively large scatter, with higher disk surface brightnesses in more massive galaxies. The unperturbed models predict a similar correlation, but with a small shift with respect to the observations (which show higher surface brightnesses than model predictions). These discrepancies could be explained by a combination of several effects. First, as we noted above, the models are computed for an average spin, but surface brightness is sensitive to the spin parameter, thus we do expect a large scatter in such a plot. Second, small galaxies may have intrinsic irregularities (linked to sporadic episodes of star formation) affecting the effective surface brightness, which are not included in the models. Finally, the models only consider pure disks, which is the case only at low luminosities. If we make a further separation of the star forming dwarfs into different morphological classes (see Fig. 11) we can see that the lowest surface brightnesses are reached only by magellanic irregulars (Sm-Im). The H band effective surface brightnesses of the dE are similar to those of the star forming BCD and spirals (Sa-Sd) of similar luminosity. We notice however that the sample of dE with available near-IR imaging is slightly biased towards high surface brightness, nucleated objects: among the 15 dE galaxies with the lowest values of , only 20% have a measure of , while among B band high surface brightness objects 69% have measured .
The relationship between the B band effective surface brightness and the H band luminosity of dE and Scd-Im-BCD is significantly dispersed, but consistent with the model predictions. The effective surface brightnesses of quiescent and star forming systems are more similar in the B band than in the H band. We notice however that dwarf ellipticals have effective surface brightnesses slightly higher than magellanic irregulars and smaller than late-type spirals and BCD of similar luminosity. Quiescent systems resulting from the quenching of the star formation activity of magellanic irregulars, whose existence is predicted by our models, are excluded from our sample just because they have B band surface brightnesses below the detection limit of the VCC.
The variations induced by the interactions are more evident in the UV bands. In the NUV band, for instance, star forming galaxies (of all types) have 2-3 magnitudes brighter surface brightnesses than quiescent dwarfs, as predicted by models. The most important variations of the surface brightness of perturbed galaxies predicted by models are in the FUV band (up to 4 magnitudes). The low GALEX sensitivity, however, prevents us to detect most of the dE that, as expected, have 26.5 mag arcsec.

We can thus conclude that the observed spectrophotometrical and structural properties of dwarf ellipticals are consistent with those of star forming dwarfs once their activity has been stopped after a ram pressure gas stripping event able to remove their total gas content. High surface brightness star forming objects should be the progenitors of the dwarf ellipticals, while magellanic irregulars the progenitors of quiescent objects of low surface brightness not detected in the VCC.

5. The transitional objects

The analysis of Fig. 7 (see previous section) reveals the existence of several objects having spectro-photometric properties in between that of star forming late-type galaxies and quiescent spheroidals. The UV selection, which is strongly biased towards star forming objects, favors the detection of such blue, still active dwarf ellipticals. Figure 12 shows the same FUV-H color-magnitude relation given in Fig. 7 but using different colour symbols (only for early-types) to indicate still star forming galaxies (HE.W. 2 Å, red), post-starburst galaxies which recently ended their activity as indicated by their strong Balmer H absorption line (HE.W. 2.8 Å, blue), HI detected objects (green) and rotationally supported spheroidals (/0.5, magenta) 12 .

We can photometrically define the transitional class as being formed by those objects of luminosity Log 9.6 L with a 3 6. The early type galaxies in our sample satisfying this criteria are listed in Table 2.

5.1. The UV to near-IR spectral energy distribution

Figure 12 and Table 2 clearly show that most of the low luminosity early-type galaxies with blue colors are characterized by an ongoing or recent star formation activity (strong emission or absorption Balmer lines; see Fig. 15). Two of them have been detected in HI, while none have rotational velocity measurements.
Figure 13 shows how the UV to near-IR spectral energy distribution of a star forming dwarf galaxy of = 0.05 and rotational velocity = 55 km s changes with time after a ram pressure stripping event characterized by an efficiency = 1.2 M kpc yr. For comparison the model SED are plotted along with the observed SED of the BCD galaxy VCC 24 and the dwarf ellipticals M32 and NGC 20513. The SED of an unperturbed galaxy is similar to that of star forming dwarf systems such as the BCD VCC 24, while it becomes redder soon after the interaction, reaching the values of the dwarf elliptical NGC 205 after 1.3 Gyr. Two interactions are necessary to get colors as red as those of the compact dwarf elliptical M32.
During the transition phase, the FUV-H colour gets redder while the H band magnitude is slightly reduced with respect to the reference case (Fig. 14). We can use these properties to estimate the rotational velocity and lookback time to the interaction. All the galaxies are close to the 40-55-70 km s range for which we computed models. We thus interpolated (and extrapolated above 70 km s) in 1 km s bins our models. Fig. 14 shows the position of each of these models (for the 1.2 M kpc efficiency) in the vs Log diagram. The models at the bottom of the diagram are unperturbed. Each point along the lines for different velocities correspond to various value of the stripping look-back time (=0, 0.1, 0.2, 0.3 …). Velocities and look back times for each transitional object can easily be found by a simple least-square test (see Table 2 and Fig. 15). Models indicate that all transitional objects recently ( 650 Myr) interacted with the cluster IGM.

5.2. Color gradients

It has been shown that some dwarf elliptical galaxies have inverted color gradients, with bluer colors in the center (Lisker et al. 2006b and references therein). Indeed six out of the sixteen galaxies listed in Table 2 have been defined as “blue center” by Lisker et al. (2006b).
The observed inversion of the color gradient in the center of dwarf galaxies is obtained in our multizone models in a ram pressure stripping scenario (see Fig. 16) for recent interaction of relatively weak efficiency (0.1 M kpc), and has the same origin than that observed in massive spirals such as NGC 4569 (Boselli et al. 2006). Blue colors in the center of these dwarf galaxies are expected because ram pressure stripping is more efficient in the outer disk, where all the gas is removed, while some gas needed to feed star formation might be retained in the central part where the galaxy potential is deeper. For more efficient interactions, the contribution of the recycled gas becomes important whenever the interaction started long ago in the center of galaxies, where the stellar surface density is high and we obtain again blue centers. We should note that if galaxies have deep potential wells because of a central mass condensation (not taken into account in our models) the gas in the center should be harder to remove, easily making blue cores. Given the shape of the potential well, whose deepness increases with mass (Catinella et al. 2006), we expect that the inversion of the color gradient is more frequent and radially extended in the brightest dwarfs, which are more likely to retain some gas, as indeed observed (Lisker et al. 2006b). The lookback time to the ram pressure stripping event, combined with the age of the different stellar populations sampled in the various filters, make the observed colour inversion more pronounced at short wavelengths, as shown in Figure 16. We can also add that such an inversion of the colour gradient can not be reproduced in a starvation scenario where gas removal is not a radial but rather a global effect.
For those galaxies with available SDSS images we reconstructed their colour gradient (see Fig. 15) using SDSS images smoothed to the GALEX resolution. Twelve out of the 14 galaxies with available data have indeed blue colors in their center (Fig. 15 and Table 2), as expected if these galaxies recently underwent a ram pressure stripping event. We remark that the observed blueing of the inner gradient happens in the inner 1-2 kpc, as predicted by models (Fig. 16).
Seven of the transitional class galaxies (VCC 327, 450, 597, 710, 1175, 1617 and 1855) have been imaged in H with the San Pedro Martir 2m telescope (Gavazzi et al. 2006a). All galaxies (except VCC 327, undetected in H imaging) show a similar pattern, with the star formation activity always limited to the central region and not extended to the whole disk, once again as predicted by our model, as shown in Fig. 17 for VCC 710.

6. Discussion

The analysis done so far clearly indicates that some dwarf ellipticals might result from the rapid decrease of the star formation activity of low luminosity, late type galaxies after most of their gas was lost because of their strong interaction with the hostile cluster environment. The comparison between model predictions and observations favors ram pressure stripping events with respect to galaxy starvation. Models in fact predict that low luminosity spirals, Im and BCD suffering starvation since 6 Gyr are still star forming galaxies with blue UV colors, relatively strong Balmer emission lines (HE.W. 10 Å) and have an HI gas content ( 10 M) easily detectable by HI surveys such as ALFALFA and AGES. These objects would thus still be classified as star forming dwarf galaxies, and not dwarf ellipticals.
We should first notice that our simple representation of a ram pressure stripping event is totally consistent with the high resolution hydrodynamical simulations in cluster dwarf galaxies of Mori & Burkert (2000) Murakami & Babul (1999) and Marcolini et al. (2003), which predict the stripping of the whole gas reservoir on short timescales.

6.1. Is the ram pressure scenario consistent with all observational evidences?

As mentioned in the introduction, however, several observational evidences, namely 1) the different structural properties of magellanic irregulars and dwarf ellipticals, 2) the presence of nuclei in dE, 3) the higher specific frequency of globular clusters and 4) the higher stellar metallicity of quiescent systems with respect to star forming dwarfs, 5) their different velocity distribution and 6) the different shape of the field and cluster luminosity functions have been often indicated as major limitations to the formation of cluster dwarf ellipticals through the gas stripping of star forming systems. We see in this section how these difficulties can be overcome.

Structural properties

In general we can say that the present work gives a natural explication to the presence of rotationally supported (Pedraz et al. 2002; Geha et al. 2003; van Zee et al. 2004b), gas rich (Conselice et al. 2003b; van Zee et al. 2004b) star forming dwarf ellipticals. The presence in some dwarf ellipticals of spiral arms observed by Lisker et al. (2006a) is a further evidence of the rotating/spiral origin of these objects. The grand design spiral arms of these dE, apparently different from the flocculent open arms of very late-type spirals, might be driven by disk instabilities produced by the displacement of the gas over the stellar disk during the stripping event (Elmegreen et al. 2002). Consistently with observations, which have shown that the frequency of dE with grand design spiral arms increases with luminosity (Lisker et al. 2006a), the perturbations induced by the gas displacement are expected to be important only in those objects where the potential is sufficient to retain some gas, while totally absent in the lowest luminosity systems where the whole gas content is instantaneously removed.
The comparison of model predictions with observations suggests that on average the variation of the structural parameters (surface brightnesses, effective radii and concentration indices) of high surface brightness low-luminosity star forming galaxies such as BCD or late-type spirals (mostly Scd-Sd) at various wavelengths expected after a ram pressure stripping event might indeed reach the values observed in dE. Consistently with Bothun et al. (1986) we confirm that the sampled dE have near-IR and optical surface brightness higher than those of magellanic irregulars (Sm-Im) and thus cannot result from this galaxy population. Our models, however, predict the existence in the Virgo cluster of an extremely low surface brightness quiescent galaxy population ( 25 mag arcsec) resulting from the quenching of the star formation activity of magellanic irregulars. Such a population has been indeed observed by Sabatini et al. (2005).
Our model predictions can not be easily compared to the results of Lisker et al. (2006a,b; 2007) and Binggeli & Popescu (1995) on the flattening distribution of star forming and quiescent dwarfs since models do not take into account the 3-D evolution of the disks. We can argue that the lack of supply of young stars with low velocity dispersion because of the suppression of the star formation activity causes the disk to heat up, dumping spiral waves on timescales of a few revolutions (Sellwood & Calberg 1984; Fuchs & von Linden 1998; Elmegreen et al. 2002) in particular in low luminosity systems where the rotational component is not always dominant. In low luminosity rotating systems (70-130 km s) it has been observed that the disk scale height increases by a factor of 2 in 3 Gyr (Seth et al. 2005). We could thus expect that the flattening distribution is age dependent. In the lack of external gravitational perturbations, the rotational velocity is conserved while increases once the gas is removed. Gravitational perturbations induced by the interaction with other galaxies or with the cluster potential would heat up the system and disperse the angular momentum, thus speeding up the decrease of (Wozniak 2007, private communication). We would thus expect rounder shapes and more relaxed distributions in those objects where the star formation stopped long time ago. We remark that, although still not virialized, nucleated objects are more centrally clustered than non nucleated systems (Lisker et al. 2007).

Nuclearity

The angular resolution of our model is too poor ( 1 kpc) to make any prediction on the formation process and evolution of the nuclei observed in dwarf ellipticals. As a general remark we can say that recent ACS/HST high resolution observations of nuclei of early-type galaxies in the Virgo cluster revealed that they have statistical (frequencies) and physical (sizes, luminosities, colors) properties similar to those of the nuclear stellar clusters found in late-type galaxies (Côte et al. 2006), consistently with our evolutionary picture. HST observations of dE show color gradients getting bluer towards their nuclei witnessing a younger stellar population than that of the outer disk (Lotz et al. 2004; Côte et al. 2006). Furthermore the presence of a nucleus is more frequent in massive dE than in low luminosity objects (Sandage et al. 1985; Ferguson & Binggeli 1994)14.

Specific frequency of globular clusters

The rapid evolution expected after the galaxy-ICM interaction which abruptly stops the star formation is able to change the total luminosity of the perturbed galaxy. The typical progenitor of a given dwarf elliptical that did not undergo such a violent truncation of its star forming activity today would be much brighter than its potential progeny even in the near-IR (see for instance Fig. 7). If we make the reasonable assumption that globular clusters were formed in the early phase of galaxy formation (thus well before any possible recent ram pressure stripping event) and regulated by the primordial dark matter condensation, the specific frequency of globular cluster should thus be determined by normalizing the total number of globular clusters to the absolute magnitude of the unperturbed galaxy which is always brighter than its gas stripped counterpart. Being the specific frequency of globular clusters defined as 10 (where is the number of globular cluster; Strader et al. 2006), we can see that increases with time after a ram pressure stripping event just because the absolute magnitude of the perturbed system does not increase with time as that of its unperturbed counterpart (see Fig. 18). The specific frequency of globular clusters in dE galaxies ranges in between 1 and 20 with a double distribution peaked at 2 and 10 (Strader et al. 2006). These values are consistent with a scenario where dE have been formed through a ram pressure gas stripping event of low luminosity late type galaxies (whose specific frequency is 1; Miller et al. 1998) occurred 4 Gyr ( 1 Gyr for dE with 2).

Metallicity

Grebel et al. (2003) observed an increase of the metallicity measured in the old stellar populations in dwarf spheroidals with respect to dwarf irregulars of similar luminosity. It is equivalent to say that the spheroidals are fainter than irregulars for the same stellar metallicity. This is naturally obtained in our models: let’s consider a “common ancestor”, giving rise to a low luminosity, star forming galaxy if it evolves in isolation, and to a dE if its star formation activity is suppressed after an interaction. The metallicity in the old population will be the same (the one of the common ancestor). The luminosity of the star forming object will be the one of the unperturbed model, while the one of the quiescent system will be the one of the model after an interaction. Fig. 18 shows that the difference in V band luminosity (partly due to the fading of the stellar population, but also to the fact that less stars formed in the latter than in the former case) is of 1 magnitude after 1 Gyr. This luminosity difference for the same metallicity corresponds well to that observed by Grebel et al. (2003) between the star forming and quiescent dwarf galaxy populations.

Velocity distribution

The velocity distribution of the low luminosity ( 10 L), high surface brightness ( 22 mag arcsec) star forming galaxies (see Table 3), i.e. of those objects that our models indicate as the probable progenitors of the observed dwarf ellipticals, is strongly non gaussian, with a pronounced wing at high velocity (see Fig. 19), witnessing infall. If limited to the Virgo A subcluster, thus to the region associated to the hot gas emitting in X-ray where ram pressure is active (Gavazzi et al. 1999), the probability that both nucleated and non nucleated dwarf ellipticals are driven by the same parent population as low luminosity, high surface brightness star forming galaxies is relatively important ( 40%), as indicated by Kolmogorov-Smirnov tests (see Table 4). Although dynamical considerations are consistent with the infall of the whole dwarf elliptical galaxy population, it is however difficult to determine when this happened: the velocity dispersion inside the cluster of their progenitor star forming, low-luminosity galaxy population should not change very much over a Hubble time as a result of dynamical friction, relaxation or energy equipartition as shown by Conselice et al. (2001).

Luminosity function

The scenario where all Virgo cluster early type dwarfs have been created after the gas removal of low-luminosity late type galaxies recently infalled into the cluster is however too extreme since quiescent dwarf galaxies are present also in the field (Pasquali et al. 2005). The contribution to the faint end of the field luminosity function of dE, however, is less important than that of blue, star forming objects (Blanton et al. 2005), it is thus possible that the fraction of dwarf galaxies recently perturbed by the cluster environment is very high. We also remark that the slope of the Virgo cluster luminosity function ( -1.4; Sandage et al. 1985) is comparable to the most recent determinations of the field luminosity function based on SDSS data, -1.4, -1.5 (Blanton et al. 2005). Steeper slopes in other clusters luminosity functions have been however determined by Popesso et al. (2006).

6.2. Infall rate

The question now is to see how many Virgo cluster dwarf ellipticals might have been formed after ram pressure stripping of low-luminosity star forming systems. To answer this fundamental question we should know both the infalling rate of low luminosity, star forming galaxies in cluster and the time scale for a galaxy to totally stop its activity. Our models give us an idea of the different time scales for gas removal and suppression of the star formation and of the subsequent evolution of the different stellar populations inhabiting these galaxies. Figure 20 shows how, on relatively short time scales, the HI deficiency parameter, on two different indicators tracing the current (H emission line; Kennicutt 1998; Boselli et al. 2001) and past (H absorption line15; Poggianti & Barbaro 1997; Poggianti et al. 2001a, 2001b; Thomas et al. 2004) star formation activity and the color index are expected to evolve after a ram pressure stripping event for galaxies with 10 L. Gas removal is extremely efficient in such low-mass objects, making the HI mass decrease by two orders of magnitude on very short time scales, i.e. 150 Myr (see Table 5). The lack of gas causes, on similar time scales, a rapid decrease of the HE.W. (we remind that the H emission of a galaxy is due to the gas ionized by O-B stars of ages 10 years, Kennicutt 1998). The interaction is so efficient that both indicators are already strongly perturbed even before the galaxy reaches the center of the cluster (lookback time to the interaction=0 in Fig. 20). The HE.W. and the color index, on the other hand, evolve more gradually in time: we can say that on average the equivalent width of the H absorption line drops down to 2.8 Å  after 0.5-0.8 Gyr, while becomes redder by 5 mag after 0.8 Gyr independently from the adopted ram pressure stripping model. The transition in between the blue sequence of low-luminosity star forming galaxies and the red sequence of quiescent dwarf ellipticals is thus a very rapid event, it is thus not surprising that only a few objects populate the intermediate region.

Table 5 indicates that the fraction of low-luminosity early type galaxies in the absolute magnitude range -13.15 -17.5 (this upper limit roughly corresponds to 10 L) with a residual star formation activity (HE.W. 2 Å), still rich in HI gas, with a post starburst activity (HE.W. 2.8 Å) or with blue colors ( 5) is important. These values indicate that 10-16 % of the quiescent dwarfs might result from star forming systems which underwent an interaction with the cluster medium less than 150 Myr ago, while up to 40 % in the last 500-800 Myr 16. These values can be used to infer a dwarf galaxy infall rate of 300 objects per Gyr (see Tab. 5), a relatively important rate if we consider the total number of dwarf members of Virgo ( 650, see sect. 2). This rate, however, is consistent with that determined by Adami et al. (2005) for Coma scaled to the mass of Virgo: 1-4 10 L Gyr if a mass to light ratio of 10 is adopted.

6.3. Comparison with clusters at high z

These values consistently indicate that the whole Virgo cluster dwarf quiescent galaxy population might have been formed by the suppression of star formation in low luminosity, gas rich systems recently entered into the cluster if an infall rate similar to the present one lasted 2 Gyr (thus equivalent to =0.16 in a = 70 km s Mpc, =0.3 and =0.7 cosmology). This result is consistent with the most recent analysis of the color magnitude relation of clusters at different redshift which all indicate a significant decrease of the fraction of low luminosity objects on the red sequence with increasing (De Lucia et al. 2004; 2007) from =0.24 (Smail et al. 1998). It has also been shown that the fraction of galaxies in between the red and the blue sequence of the color magnitude relation (which might be considered as the analogues of our transient population) in high density environment at =0.7 from COSMOS increases with the decrease of the galaxy luminosity (Cassata et al. 2007), as predicted by our model. Our results are also consistent with the analysis of Nelan et al. (2005) on 93 nearby clusters based on the age- relation which indicates that the quiescent dwarf galaxy population only recently joined the red sequence.

7. Conclusion

We can conclude that models and observations are consistent with an evolution of star forming, low-luminosity late type galaxies recently accreted in Virgo into quiescent dwarfs because of the ram pressure gas stripping and the subsequent stopping of their star formation activity. For consistency with surface brightness measurements, we show that high surface brightness star forming dwarf galaxies (low luminosity spirals and BCD) might be at the origin of the optically selected dwarf ellipticals (both normal and nucleated) analyzed in this work, although we expect that the low surface brightness magellanic irregulars (Sm and Im) once stripped of their gas reservoir, produce quiescent dwarfs with surface brightnesses below the detection limit of the VCC, as those observed in Virgo by Sabatini et al. (2005). The process of transformation is extremely rapid and efficient, since it works on all dwarfs and last on average less than 150 Myr. On longer time scales galaxies get structural and spectrophotometric properties similar to that of dwarf ellipticals. The whole star forming dwarf galaxy population dominating the faint end of the field luminosity function (Blanton et al. 2005), if accreted, can be totally transformed by the cluster environment into dwarf ellipticals on time scales as short as 2 Gyr and thus be at the origin of the morphology segregation observed also at low luminosities.
This interesting result is of fundamental importance even in a cosmological context because it shows that the majority of dwarf galaxies (if not all of them) are “young” even in clusters, and not old as expected in a hierarchical galaxy formation scenario (see also Nelan et al. 2005). For comparison with De Lucia et al (2006), we give in Table 6 the lookback time when 50% and 80% of the stars were formed for a model galaxy of 55 km s for a (or two) ram pressure stripping event of efficiency = 1.2 M kpc yr.

Although the values given in Table 6 are not directly comparable to those given by De Lucia et al. (2006) since limited to relatively high mass objects (2.5 10 M, while our model galaxy is of only 2.4 10 M), the mean age of the stellar population of low luminosity, quiescent galaxies is significantly younger than that predicted by hierarchical models of galaxy formation (lookback times 10 and 8.5 Gyr for 50% and 80% of the stellar population).
Despite their morphological type, the star formation activity of dwarf systems has been abruptly interrupted by the interaction with the environment in quiescent systems. This conclusion can be extended to the local group, where the study of the stellar color magnitude relation of dwarf spheroidal systems revealed that the star formation activity, although in an episodic manner, lasted for several Gyr (Mateo 1998; Grebel 1999). We can add that the only cluster galaxy population likely to be issued by major merging events, as those predicted by hierarchical models of galaxy formation, is that of massive ellipticals, whose origin is probably very remote ( 2-3, Dressler 2004; Treu 2004; Nolan 2004; Franx 2004; Renzini 2006). Indeed this is the only Virgo cluster galaxy population with a virialized velocity distribution (Conselice et al. 2001). If we consider clusters of galaxies as those regions where merging events were more frequent at early epochs since the big bang just because characterized by an high galaxy density, we can conclude that the hierarchical formation scenario was the principal driver of galaxy evolution only in massive objects at very early epochs. All observational evidences are consistent with a secular evolution afterward.

We wish to thank C. Adami, E. Athanassoula, C. Balkowski, V. Buat, G. Comte, P.A. Duc, G. Hensler, J. Lequeux, H. Wozniak for precious comments and suggestions. We are grateful to the anonymous referee for his constructive suggestions extremely useful in the preparation of the final version of the manuscript. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in April 2003. We gratefully acknowledge NASA’s support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with the Centre National d’Etudes Spatiales of France and the Korean Ministry of Science and Technology. We wish to thank the GALEX SODA team for their help in the data reduction. This research has made use of the GOLD Mine database.
Variable ——-Ram pressure——- ——-Starvation——-
modification Amount Time scale modification Amount Time scale
Gas content  totally removed factor 10-100 150 Myr partly removed   factor 10 6 Gyr
HI-deficiency strongly deficient 1-2 150 Myr mildly deficient 0.5 6 Gyr
Colors strongly reddened mildly reddened
FUV-NUV increased 1-2 mag 1 Gyr increased 0.2 mag 6 Gyr
FUV-H increased 3-5 mag 1 Gyr increased 1.5 mag 6 Gyr
FUV-B increased 2.5-4 mag 1 Gyr increased 1 mag 6 Gyr
B-H increased 1 mag 1 Gyr increased 1 mag 6 Gyr
color gradients blue center 1-2 mag (NUV-i) 1-5 Gyr red center 1 mag any
Star formation stopped mildly decreased
H E.W. drop to  0 Å 150 Myr drop to  10 Å 6 Gyr
H E.W. drop to  2.3 Å 1 Gyr drop to  2.3 Å 6 Gyr
Metallicity
Gas increased  0.6 dex 200 Myr mildly increased  0.4 dex 6 Gyr
in old stars unchanged unchanged
Average stellar mildly reduced 0 to 0.15 dex 0 to 5 Gyr mildly increased  0.1 dex 6 Gyr
Surface brightness decreased decreased
FUV strongly decreased 2-5 mag 1 Gyr strongly decreased 3 mag 6 Gyr
NUV strongly decreased 2-3 mag  1 Gyr strongly decreased 3 mag 6 Gyr
B mildly decreased 1 mag 1 Gyr decreased 2 mag 6 Gyr
H  constant  0.5 mag 1 Gyr decreased 1.5 mag 6 Gyr

Notes: * = Six Gyr is the lookback-time for starvation in our models. For a lookback-time 6 Gyr the effects induced by starvation are less important, while are more important for a lookback-time 6 Gyr.

Table 1Effects of the interactions with respect to an unperturbed model.
VCC Type Blue Centers Log L FUV-H HE.W. HE.W. Log MHI Age V
Emission Absorption (=1.2) (=1.2)
L mag Å Å M Gyr km s
21 dS0 bc,BC 8.89 5.69 - 4.2 7.84 0.50 59
327 S0 BC 9.34 4.99 0 (16) 1.1 - 0.22 76
450 S0 pec BC 8.86 5.90 10 (52) - - 0.58 58
597 S0 BC 8.84 3.79 7 (36) - - 0.04 54
710 dS0: 1 9.00 3.85 15 - 7.95 0.04 61
764 S0 1 8.99 5.63 - - - 0.46 63
1065 dE0,N 8.34 5.87 - 0.8 - 0.64 42
1175 E5/S0 bc,BC 8.82 4.11 4 (157) - - 0.09 54
1389 dE2:,N 8.44 5.49 - 1.9 - 0.50 44
1499 E3 pec or S0 bc,BC 8.79 3.46 - 5.0 - 0.00 52
1501 dS0? bc,BC 8.60 4.18 4 1.1 - 0.12 47
1539 dE0,N BC 8.42 5.89 - 1.6 - 0.64 44
1617 d:S0 pec? bc,BC 8.75 4.00 9 (7) 1.0 - 0.08 52
1684 dS0: bc,BC 8.76 5.36 (4) 4.5 - 0.41 54
1809 S0/Sa BC 9.32 4.78 - 4.9 7.25 0.18 75
1855 S0: BC 8.70 3.56 20 (72) - - 0.01 50

Column 1: VCC name, from the Virgo Cluster Catalogue of Binggeli et al. (1985).
Column 2: Morphological classification, from Binggeli et al. (1985).
Column 3: Presence of a blue center in from Lisker et al. (2006b) (bc) and/or from this work (BC). 1 stands for galaxies not observed by the SDSS.
Column 4: H band luminosity, in solar units.
Column 5: color index, in AB magnitudes.
Column 6: The equivalent width of the H emission line, in Å, from (in order of preference) imaging (Gavazzi et al. 2006a) and integrated spectroscopy(Gavazzi et al. 2004). Nuclear (SDSS, DR5) spectroscopic data are given in parenthesis.
Column 7: The equivalent width of H underlying absorption line, in Å, from (in order of preference) integrated (Gavazzi et al. 2004) or nuclear (SDSS, DR5) spectroscopy.
Column 8: The logarithm of the HI mass, in solar units, from Gavazzi et al. (2005b).
Column 9 and 10: Lookback time to the interaction and rotational velocity of the best fitting model for a ram pressure stripping event with = 1.2 M kpc yr. Lookback times of 0 Myr are for galaxies now at the peak (maximum) of their interaction.

Table 2The transitional class
All Virgo Virgo A
Class Mean Median N. of obj. P Mean Median N. of obj. P
km s km s km s % km s km s km s
SFD 1362 790 1324 151 4 1166 907 1147 41 82
dE 1201 723 1208 95 72 961 771 943 35 79
dE,N 1168 642 1229 182 3 1120 701 1222 89 12

Notes: Column 1: SFD stands for star forming dwarfs, low-luminosity (10 L), high surface brightness ( 22 mag arcsec) late-type galaxies.
Columns 6 and 11: is the probability that galaxies follow a normal distribution.

Table 3The velocity distribution of dwarf galaxies in Virgo
All Virgo Virgo A
Class E dE dE,N SFD E dE dE,N SFD
E 100 88 42 4 100 64 36 5
dE 88 100 73 3 64 100 40 40
dE,N 42 73 100 0 36 40 100 41
SFD 4 3 0 100 5 40 41 100

SFD: Star Forming Dwarfs are all low-luminosity (10 L), high surface brightness ( 22 mag arcsec) late-type galaxies.

Table 4The Kolmogorov-Smirnov test for radial velocities
Tracer Condition Time scale fraction Infall rate
Myr (N./observed) N./Gyr
HI non def. 150 16 (11/68) 475
H E.W. 2 Å 150 10 (31/319) 297
H E.W. 2.8 Å 500-800 40 (127/319) 274
FUV-H 5 800 9 (9/102) 50

Notes: column 4 gives the fraction (total number/observed) of the observed early-type Virgo galaxies with -13.15 -17.5 satisfying the condition, where the total number of Virgo galaxies satisfying these criteria are 498.
**: 127 is the total number of galaxies with an H absorption line 2.8 Å (89) or H in emission (38); if we consider also those with H in emission (50), for which the H absorption line is generally underestimated, the total number of objects increases to 148 (46%).
***: Given the detection limit of GALEX, the value relative to the color index is a lower limit.

Table 5The frequency of transient objects
Model Time 50% 80%
Myr Gyr Gyr
Non perturbed - 2.60 0.86
1 crossing 0 2.72 0.98
- 500 3.18 1.48
- 1000 3.62 1.96
- 1500 4.06 2.43
2 crossings 2000 5.98 4.55

Note: models are for a galaxy 55 km s for a (or two) ram pressure stripping event of efficiency = 1.2 M kpc yr
Column 2: lookback time to the stripping event

Table 6The lookback time to formation
Figure 1.— The evolution with time of the total gas content (upper panel), of the unperturbed to perturbed gas mass ratio (central panel, in logarithmic scale: this entity corresponds to the HI-deficiency parameter) and of the star formation rate (lower panel) for a galaxy with rotational velocity = 55 km s and spin parameter =0.05. The continuum black line shows the unperturbed model (reference), the green long dashed line a starvation model for a galaxy-cluster interaction started 6 Gyr ago, the red dotted line a ram pressure stripping model with an efficiency of = 0.4 M kpc yr, the blue short dashed line a ram pressure stripping model with an efficiency of = 1.2 M kpc yr. The ram pressure stripping event in both of these models started 1 Gyr ago (=1 Gyr). The increase with time of the total gas content and of the star formation activity for an unperturbed galaxy is due to gas infall.
Figure 2.— The evolution of different color indices (in the AB system) for a galaxy with rotational velocity = 55 km s and spin parameter =0.05. Symbols are as in Fig. 1.
Figure 3.— The evolution of the gas 12 Log(O/H) metallicity index for a galaxy with rotational velocity = 55 km s and spin parameter =0.05. Symbols are as in Fig. 1.
Figure 4.— The evolution of the effective surface brightness (left panels) and radius (right panels) in different bands for a galaxy with rotational velocity = 55 km s and spin parameter =0.05. Symbols are as in Fig. 1.
Figure 5.— The evolution with time of the total gas content (upper panel), of the unperturbed to perturbed gas mass ratio (central panel) and of the star formation rate (lower panel) for a galaxy with rotational velocity = 55 km s and spin parameter =0.05 after two ram pressure stripping events. The continuum black line shows the unperturbed model (reference), the red dotted line a ram pressure stripping model with an efficiency of = 0.4 M kpc yr, the blue short dashed line a ram pressure stripping model with an efficiency of = 1.2 M kpc yr. The two stripping events are delayed by 1.7 Gyr, the crossing time of late type galaxies in the Virgo cluster.
Figure 6.— The relationship between the HI mass and the H band luminosity, tracer of the total mass of galaxies, compared to model predictions for different lookback times of a ram pressure/starvation event. Empty squares are for Sa-Sc galaxies, crosses for Scd-Im-BCD and filled circles for dE-dS0. Open triangles are upper limits for undetected late-type galaxies, gray filled triangles for undetected early-types. The dashed line indicates the region which is inaccessible to the observations with a sensitivity of 1 mJy per channel for galaxies at the distance of Virgo. Model predictions for unperturbed galaxies of spin parameter = 0.05 and = 40, 55, 70, 100, 130 and 220 km s are indicated with orange squares (from left to right). Model predictions for a ram-pressure stripping event at different epochs are indicated by blue dashed ( = 1.2 M kpc yr) and red dotted ( = 0.4 M kpc yr) lines, while the starvation scenario by the long-dashed green line. One should take care that the models presented in this figure and later are not evolutionary tracks, but result from the combined effects of ram pressure, recycled gas and epoch of the interaction. Especially, we note that for interaction that occurred a long time ago, the available gas at that time was smaller (the galaxy was not yet fully formed), and as a result, the final gas amount is also smaller.
Figure 7.— The relationships between different UV, optical and near-IR color indices and the H band luminosity compared to model predictions. Symbols and models are as in Fig. 6. Galaxies redder than the dashed line are undetectable by the present surveys.
Figure 8.— The relationships between the color index and the H band luminosity of dwarf galaxies compared to model predictions (in blue for an efficiency of = 0.4 M kpc yr and red = 1.2 M kpc yr) in the case of single (thin lines) or multiple (thick lines) interactions. Symbols are: black empty squares for Sa-Sc, dark green crosses for Scd-Sd, red asterisks for Sm-Im, blue open triangles for BCD, yellow filled triangles for dIm/dE, black open circles for E-S0a, magenta small filled dots for nucleated dE and green large filled dots for non-nucleated dE. Models are for galaxies of spin parameter = 0.05 and rotational velocity = 40, 55, 70 and 100 km s from left to right, respectively. Galaxies redder than the dashed line are undetectable by the present surveys.
Figure 9.— The relationships between the gas 12 + Log(O/H) metallicity index and the model predictions. Symbols and models are as in Fig. 6. The three dE galaxies in the plot are the transitional types VCC 710 (12 + Log(O/H) = 8.55), VCC 1501 (12 + Log(O/H) = 8.46) and VCC 1617 (12 + Log(O/H) = 8.58).
Figure 10.— The relationship between the H band parameter and the H band luminosity for early- (right) and late-type (left) galaxies with 10 L. Symbols are as in Fig. 8.
Figure 11.— The relationships between the H, B, NUV and FUV effective surface brightnesses (in AB magnitudes) and the H band luminosity. Symbols and models are as in Fig. 8. The horizontal dashed lines in the B, NUV and FUV panels are the surface brightness detection limits of the VCC and GALEX.
Figure 12.— The relationship between the FUV-H color index and the H band luminosity (see Fig. 7). Early-type galaxies (filled circles for dE-dS0, empty circles for E-S0-S0a) are coded as follow: red symbols are for galaxies with H emission (HE.W. 2 Å), blue symbols for objects with strong H absorption lines (HE.W. 2.8 Å), green symbols for HI detected galaxies, magenta symbols for rotationally supported galaxies (), black symbols for galaxies with spectroscopy but not satisfying the previous criteria. Colors are mutually exclusives, with priority ordered according first to the H emission, then to the H absorption, to the HI detection and to rotationally supported objects. Gray symbols are for the whole late-type galaxy population and for early-type objects without any spectroscopic information.
Figure 13.— The UV to near-IR spectral energy distributions of the BCD VCC 24 (filled dots), of the dE NGC 205 (empty triangles) and the compact dwarf elliptical M32 (crosses) (all normalized to the 1.65 m H band flux) are compared to the model SED for a galaxy of spin parameter = 0.05 and rotational velocity = 55 km s. The black continuum line is the model for an unperturbed galaxy, the continuum blue, green, magenta, cyan, yellow and red are for galaxies which had their peak of the interaction respectively 0, 100, 300, 500, 1300 Myr and two cluster crossings with the last one 500 Myr ago.
Figure 14.— The transition objects are shown in the FUV-H versus H band luminosity plane. The curves indicate the position of various ram pressure stripping models ( = 1.2 M kpc yr) interpolated between 40 and 70 km s (and extrapolated beyond) without interaction (orange squares), and for various lookback time to the interaction (a few are indicated on the left). These models were used to fit a velocity and lookback time for each transition objects.
Figure 15.— Left column: the observed (black filled dots) and model predicted (continuum line) spectral energy distribution of the transitional galaxies listed in Table 2 in a ram pressure stripping scenario with = 1.2 M kpc yr. The lookback time to the interaction and the rotational velocity of the galaxy for the model SED are listed in Table 2. Central column: the integrated (form GOLDMine) or nuclear (from SDSS) visible spectrum. Only integrated spectra have been used in the construction of the UV to near-IR SED shown in the left column. Right column: the radial profiles (in AB magnitudes).
Figure 15.— Continue.
Figure 15.— Continue.
Figure 15.— Continue.
Figure 16.— The variation of the color radial profile (in AB magnitudes) with time for a galaxy with rotational velocity = 55 km s and spin parameter =0.05 after a ram pressure stripping event with efficiencies = 0.1 M kpc yr (left panel), 0.4 M kpc yr (central panel) and =1.2 M kpc yr (right panel). The lookback time to the interaction in Gyr is indicated on the right in the central panel, from 0 (epoch when the interaction is at its maximum; green dotted line) to 5 Gyr (blue dashed line): the black continuum line is the reference unperturbed model.
Figure 17.— The red stellar continuum (left) and the H+[NII] narrow band images (right) of the dS0 galaxy VCC 710 from our own observations.
Figure 18.— The variation of the normalized specific frequency of globular clusters (upper panel) and absolute V band magnitude (lower panel) as a function of the lookback time to the ram pressure stripping event for efficiencies = 0.4 M kpc yr (red dotted lines) and = 1.2 M kpc yr (short dashed lines) for galaxies characterized by a spin parameter = 0.05 and rotational velocity = 40, 55 and 70 km s (from top to bottom) respectively. The normalization is made relative to that of a similar unperturbed galaxy.
Figure 19.— The velocity distribution of the low luminosity ( 10 L), high surface brightness (22 mag arcsec) star forming galaxies (top), of non nucleated (center) and nucleated (bottom) dwarf ellipticals galaxies in the whole Virgo cluster region (empty histogram) and limited to the Virgo A subcluster (hashed histogram).
Figure 20.— The variation of the HI-deficiency parameter (top), of the HE.W. emission line (middle top), the HE.W. absorption line (middle bottom) and the (bottom) color index for galaxies with rotational velocities of = 40, 55 and 70 km s respectively and spin parameter =0.05 as a function of the lookback time to the interaction. The red dotted lines are for a ram pressure stripping model with an efficiency of = 0.4 M kpc yr, the blue short dashed line a ram pressure stripping model with an efficiency of = 1.2 M kpc yr. In both scenarios the efficiency of the perturbation increases with the decrease of the rotational velocity. The lookback time to the interaction () is equal to zero when the galaxy is currently passing through the cluster center, where ram pressure stripping is at its maximum. Given the extended distribution of the cluster hot gas, the galaxy-ICM interaction in practice starts 100 Myr before . For this reason, we artificially placed the values for an unperturbed model at =-100 Myr (yellow squares).

Appendix A The data

The dataset used in the present analysis is composed of imaging and spectroscopic data covering the whole UV to IR spectral range. The Virgo cluster region was observed in spring 2004 as part of the All Imaging Survey (AIS) and of the deeper Nearby Galaxy Survey (NGS) carried out by the Galaxy Evolution Explorer (GALEX) in the two UV bands FUV () and NUV (). This public dataset (IR 1.0 release), now available on MAST, has been combined with data extracted from several open time observations obtained at a similar sensitivity than the NGS. Details of the GALEX instrument and data characteristics can be found in Martin et al (2005) and Morrissey et al (2005).
Whenever available, we extracted fluxes from the NGS and open time images, obtained with an average integration time of 1500 sec. These data are complete to 21.5 in the NUV and FUV. Elsewhere UV fluxes have been extracted from the shallower AIS images ( 70 sq. degrees), obtained with an average integration time of 100 sec, complete to 20 in both the FUV and NUV bands.
B and V frames are available for most of the analyzed galaxies thanks to our own observations (Gavazzi & Boselli 1996; Gavazzi et al. 2001; 2005a and Boselli et al. 2003). H (1.65 m) and K (2.1 m) band frames have been obtained during a near-IR imaging survey of the Virgo cluster (Boselli et al. 1997b; 2000; Gavazzi et al. 2000b, 2001). SDSS imaging data, taken from the most recent DR5 (release 5, Adelman-McCarthy et al. 2007), have been also used for the determination of the radial NUV- color gradients.
Fluxes were obtained by integrating all images within elliptical annuli of increasing diameter up to the optical B band 25 mag arcsec isophotal radii. Independent measurements of the same galaxies obtained in different exposures give consistent photometric results within 10% in the NUV and 15% in the FUV in the AIS, and about a factor of two better for bright (NUV 16) galaxies. We thus estimate that the overall uncertainty in the UV photometry is on average a factor of 2 better in the NGS or open time images than in the AIS especially for the faintest objects. Optical and near-IR data have on average a photometric accuracy of 10%. The H and B band structural parameters effective radii (radius containing half of the total light) and surface brightnesses (mean surface brightness within ) have been measured as described in Gavazzi et al. (2000a). Given the poor resolution of the GALEX data (FWHM of the PSF 5 arcsec for a pixel size of 1.5 arcsec), these structural parameters are available only for the brightest (and bluest in FUV) dwarf galaxies in Virgo.
Spectral line indices (HE.W., HE.W.) are available for a large fraction of the analyzed galaxies. Most of the selected objects have been observed as part of a spectroscopic survey of the Virgo cluster (Gavazzi et al. 2004) still under way. These data have been extracted from long slit integrated spectroscopy obtained by drifting the slit over the whole galaxy disc, as in Kennicutt (1992), thus providing values representative of the whole object. These are intermediate ( 1000) resolution spectra in the range ( Å). Low resolution spectroscopy of the central region of several galaxies is also available from the SDSS (release 5). To minimize aperture effects, SDSS spectroscopy has been taken only for axisymmetric quiescent galaxies (E, dE, dS0). A few other spectroscopic data for dwarf ellipticals have been taken from Geha et al. (2003) and Michielsen et al. (2007). Line absorption indices (HE.W.) have been measured in the Lick system, although their exact calibration is still under way.
HI data have been taken from the compilation of Gavazzi et al. (2005b), Conselice et al. (2003b) and (Giovanelli et al. 2007). The HI-deficiency parameter () is defined as the logarithmic difference between the average HI mass of a reference sample of isolated galaxies of similar type and linear dimension and the HI mass actually observed in individual objects: = Log - Log. According to Haynes & Giovanelli (1984), Log = + Log, where and are weak functions of the Hubble type and is the linear diameter of the galaxy (see Gavazzi et al. 2005b). Since we make the hypothesis that dwarf ellipticals are gas-stripped low-luminosity, star forming objects, their HI deficiency parameter has been determined assuming as reference isolated star forming dwarf galaxies ( = 7.00 and = 1.88, from Gavazzi et al. 2005b). Galaxies with an HI-deficiency parameter larger than 0.3 are considered as deficient in HI gas.
Rotational velocities for dwarf elliptical galaxies have been taken from Geha et al. (2003), van Zee et al. (2004b), Pedraz et al. (2002), Thomas et al. (2006) and Simiens & Prugniel (1997a, 1997b, 1998, 2002).
UV to near-IR imaging data have been corrected for galactic and internal extinction as described in Boselli et al. (2003). Internal extinction corrections have been applied only to late-type galaxies. Owing to the high galactic latitude of Virgo, galactic extinction corrections are very small ( 0.05).
Most of the imaging and spectroscopic data used in the present analysis are available in electronic format on the GOLDMine database (http://goldmine.mib.infn.it; Gavazzi et al. 2003).

Appendix B The models

b.1. The multi-zone models for the chemical and spectro-photometric evolution of unperturbed galaxies

To trace the evolution of late-type galaxies of different luminosity, we have used the multi-zone chemo-spectrophotometric models of Boissier & Prantzos (2000), updated with an empirically-determined star formation law (Boissier et al 2003) relating the star formation rate to the total-gas surface densities (, ):

(B1)

where is the rotation velocity at radius . This is a variant of the traditional “Schmidt law” with two parameters: the index and an efficiency of the star formation activity . The values of and are taken as equal respectively to 2.63 10 and 1.48, as determined from the gaseous and H profiles of 16 nearby galaxies (Boissier et al 2003), where is expressed in MpcGyr, in Mpc, in km s and in kpc.

The resulting models are extremely similar to those presented in Boissier & Prantzos (2000) and show the same global trends. We consider the star formation law as fixed and we keep the same mass accretion (infall) histories as in Boissier & Prantzos (2000), based on the assumption that before the interaction with the cluster, galaxies were “normal” spirals. The free parameters in this grid of models are the spin parameter, and the rotational velocity, . These two parameters are theoretical quantities, although should be similar to the asymptotic value of the rotation curve at large radii. The spin parameter is a dimensionless measure of the specific angular momentum (defined in e.g. Mo, Mao & White 1998). Its value in spirals ranges typically between 0.02 for relatively compact galaxies to 0.09 for low surface brightness galaxies (Boissier & Prantzos 2000). The models of Boissier & Prantzos (2000) contains scaling relationships (the total mass varies as , the scale-length as ). Star formation histories depend on the infall timescales, which are a function of in these models, so that roughly speaking, controls the stellar mass accumulated during the history of the galaxy, and its radial distribution.
In order to avoid the multiplication of parameters, we decided to fix the spin parameter to an average value of 0.05 and investigate global trends linked to the mass -or the velocity of galaxies- or to the interaction itself. Other values of the spin parameter should mostly create some scatter around these trends. From e.g. Boissier & Prantzos (2000), it can be seen that trends are mostly driven by mass (see their Figure 8). Various spin parameters create a modest dispersion with respect to the average one (e.g. about a few tenths of magnitude for the B-K colour index, a few tenths of dex for stellar and gaseous masses…). The only quantities which are clearly much more affected by the spin parameter than the velocity are the surface brightnesses. The central surface brightness in the B band (or band, see Boissier 2000) can change by a few mag arcsec for a given circular velocity when using various realistic spin parameters.

To sample the whole dynamic range covered by dwarf galaxies we focused our analysis to the velocity range 40-100 km s, although we tested several other models for larger velocities (for comparison with bright spirals). We remind that the model, which has a resolution of 1 kpc, does not include any bulge or nuclear component, corresponding well to pure exponential disks such as these dwarf star forming galaxies (Gavazzi et al. 2000a). On the other hand, the models were developed and extensively tested for relative massive galaxies (rotation velocities above 80 km s). In this work, we are interested mostly in the 40-100 km s range, and low velocity models were simply extrapolated from the massive ones. By this, we mean that we assumed that the star formation law, Initial Mass Function and other ingredients used for massive galaxies also apply to the low mass case. Especially, the models include a dependence of infall time scales on the circular velocity (more massive galaxies form the bulk of their stars earlier than lower mass galaxies). This assumption was found to be in agreement with observations in normal spirals, above 80 km/s (Boissier & Prantzos, 2000), and is here generalized to lower masses. These considerations call for some caution in the interpretation of our results. Especially, low mass galaxies are very small and the models do not take into account the likely radial mixing on scales smaller than 1 kpc, making them extremely uncertain with respect to e.g. metallicity gradients. Nevertheless, we show in this paper that our extrapolated models reproduce reasonably well the properties of normal late type low velocity galaxies (magnitudes, colors…). In addition, errors due to model uncertainties are likely to be systematic effects: they should affect less differences between two models than absolute values. Thus, we believe that the differences obtained when ram-pressure is introduced with respect to the unperturbed case can be trusted.

The models of Boissier & Prantzos (2000) provide total luminosities and colors in all bands as well as the total gas content. They do not compute the nebular emission, but we estimated the H emission by using the number of ionizing photons predicted by Version 5 of STARBURST 99 (Vazquez & Leitherer 2005) for a single generation of stars distributed on the Kroupa et al. (1993) initial mass function (as used in our models), convolving it with our star formation history, and converting the result into our H flux following Appendix A of Gavazzi et al. (2002a).
The models also produce low resolution theoretical spectra from which are used to compute the Lick H index. The model spectral resolution is actually quite poor (20 Å in the visible) but we checked that the evolution of this index in the case of a burst is consistent with the one presented in e.g. Tantalo & Chiosi (2004).
The evolution of the metallicity is computed in the models taking into account the yields, finite lifetimes of stars, infall of pristine gas (Boissier & Prantzos 1999). The spectra are computed taking into account this metallicity and the star formation history.

Given the agreement between model predictions and observations for different samples of unperturbed galaxies (Boissier & Prantzos 1999; 2000; Prantzos & Boissier 2000; Boissier et al. 2001), we will consider them as the reference models for the unperturbed case. As for NGC 4569 (Boselli et al. 2006) we study two different interaction scenarios, starvation and ram-pressure stripping.

b.2. The starvation scenario

In the starvation scenario (Larson et al. 1980, Balogh et al. 2000, Treu et al. 2003), the cluster acts on large scales by removing any extended gaseous halo surrounding the galaxy, preventing further infall of such gas onto the disk. The galaxy then become anemic simply because it exhausts the gas reservoir through on-going star formation.
Infall is a necessary assumption in models of the chemical evolution of the Milky Way to account for the G-dwarf metallicity distribution (Tinsley 1980) and is supported by some chemo-dynamical models (Samland et al. 1997). As the disk galaxy models were obtained through a generalization of the Milky Way model, infall is present in all our models. It is a schematic way to describe the growth of any galaxy from a proto-galactic clump in the distant past to a present-day galaxy. Infall time scales in the models were chosen to reproduce the properties of present day normal galaxies (Boissier & Prantzos 2000, Boissier et al. 2001). This includes a dependency on the rotational velocity 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”. Because of this effect, low mass galaxies, in the absence of interaction, are accreting large amounts of gas and are still actively forming stars. In the event of starvation, the galaxy stops accreting gas, and continue forming stars from the reservoir already present in the disk. This proceed at a lower rate than in the unperturbed case, with a declining activity in time as the consumed gas is not replaced with fresh gas. Stopping infall (in order to mimic starvation) at a given time is straightforward to include in the model. We shall call the elapsed time since the infall termination (look back time).

b.3. The ram pressure stripping scenario

In addition to the starvation scenario we can study the effect of ram-pressure gas stripping. As in Boselli et al. (2006), we adopt the plausible scenario of Vollmer et al. (2001) explicitly tailored to Virgo: i.e., the galaxies being modeled have crossed the dense IGM only once (in its simplest version), on elliptical orbits. The ram pressure exerted by the IGM on the galaxy ISM varies in time following a Gaussian profile, whose peak at (=) is when the galaxy is crossing the dense cluster core at high velocity ( and are look-back times, where the present epoch corresponds to =0). The Gaussian has a width = 9 10 years (see Fig 3 of Vollmer et al. 2001). We make the hypothesis that the gas at each radius is removed at a rate that is directly proportional to the galaxy gas column density and inversely proportional to the potential of the galaxy, measured by the total (baryonic) local density (provided by the model). The gas-loss rate adopted is then equal to , with the efficiency following a Gaussian having a maximum at the time , chosen to mimic the variation of the ram pressure suggested by Vollmer et al. (2001). This very simple, but physically-motivated prescription should allow us to model the gas removal from galaxies using only two free parameters ( and ) to age-date and measure the magnitude of this effect. To further constrain the models we assume two different values of : the first is = 1.2 M kpc yr, the value best reproducing the radial profiles of NGC 4569 (Boselli et al., 2006), the second one is one third of it, = 0.4 M kpc yr. This second value is suggested by the following considerations: besides the potential of the galaxy, which is an intrinsic property of each object, the efficiency of ram-pressure () stripping depends on the density of the cluster intergalactic medium (), on the crossing velocity of the galaxy within the cluster () and on its orientation with respect to its motion (Boselli & Gavazzi 2006): = . Statistically speaking, the line of sight velocity dispersion of star forming galaxies in the cluster is 1150 km s, and drops to 766 km s if limited to low luminosity star forming objects in the Virgo A subgroup from where the X ray emission comes from. These values can be compared to the line of sight velocity of NGC 4569 with respect to the cluster center, which is 1374 km s. To test other realistic models we thus decided to use an lower by a factor of (1374/766) = 3.2 than in NGC 4569. = 0.4 M kpc yr can thus be considered as an average value of relatively weak interactions while = 1.2 M kpc yr is a realistic value representative of more extreme interactions. As we discuss in the main body of the paper, = 0.4 M kpc yr leads to HI-deficiency parameters of 0.8 for massive galaxies, consistent with the average HI-deficiency observed within one virial radius in Virgo, while = 1.2 M kpc yr to HI-deficiencies of 1.5, close to the highest values found in Virgo (Gavazzi et al. 2005b; Boselli & Gavazzi 2006). In massive galaxies HI deficiencies as high as 2 have been observed (Gavazzi et al. 2005), and are probably the result of stripping events more efficient than those simulated. These extreme HI deficiencies can also be the result of subsequent crossings of the cluster center, that should happen on average every 1.7 Gyr (Boselli & Gavazzi 2006). Multiple crossing can be reproduced by our models just considering that the average crossing time of star forming galaxies in the Virgo cluster is 1.7 Gyr (Boselli & Gavazzi 2006).
We make the further assumption that no extra star formation is induced during the interaction. This assumption is reasonable since ram pressure stripping models of Fujita (1998) and Fujita & Nagashima (1999) indicate that on short time scales ( 10 yr) the star formation activity of galaxies can increase by up to a factor of 70% at most in high density, rich clusters such as Coma, but it decreases to values lower than before the interaction whenever the density of the IGM is relatively low as in the core of Virgo. Indeed we do not have any evidence of a statistically significant increase of the star formation activity in galaxies that recently underwent a ram-pressure stripping event (Iglesias-Paramo et al. 2004). Given the rapidity of the gas stripping process (150 Myr, see sect. 5.2) in these dwarf systems, a possible mild increase of their star formation activity does not have enough time to produce significant modification in their spectrophotometric and structural properties.

Footnotes

  1. affiliation: Laboratoire d’Astrophysique de Marseille, BP8, Traverse du Siphon, F-13376 Marseille, France
  2. affiliation: Laboratoire d’Astrophysique de Marseille, BP8, Traverse du Siphon, F-13376 Marseille, France
  3. affiliation: School of Physics and Astronomy, Cardiff University, 5, The Parade, Cardiff CF24 3YB, UK
  4. affiliation: Universita degli Studi di Milano-Bicocca, Piazza delle Scienze 3, 20126 Milano, Italy
  5. Unless specified, in the following we indicate with dE all quiescent dwarf galaxies, including dSph
  6. The UV emission of star forming galaxies is due to relatively young and massive A stars (Boselli et al. 2001). The UV emission of dwarf ellipticals is due to a residual star formation activity since does not show, as in massive ellipticals, the UV upturn due to hot, evolved stars (Boselli et al. 2005a).
  7. In the UV, in our example of Fig. 4, the effective radius presents large variations in its value after ram pressure started. This is due to the fact that the galaxy is left with very low amount of gas, and the effective radius becomes sensitive to two opposite effects. In a first phase, the dominant effect is that the inner disk is depleted through star formation at a larger rate than the outer disk, leading to an increase of (like in the starvation case). In a second phase, the inner disk is partially replenished with recycled gas (ejected at the end of the life of long-lived stars), leading this time to a decrease of .
  8. Model HI gas masses are estimated assuming that the total gas amount of star forming galaxies is composed of 15% of molecular gas (Boselli et al. 2002) and 30% of helium, thus /1.4.
  9. We notice that here and in the subsequent figures 8 to 10 and 12 the model tracks do not describe a time evolution, but rather show current values for models with different lookback times of a ram pressure or starvation event.
  10. The concentration index is however insensitive to the presence of small nuclei as those present in nucleated Virgo cluster dE
  11. We included in this category also the mixed classes S/BCD, Sm/BCD and Im/BCD
  12. The anisotropy parameter / is defined as: /=, where is the ellipticity of the galaxy
  13. We compare the prediction of our model to the SED of NGC 205 and M32 just because these two objects are the only well known dwarf ellipticals detected by GALEX in the two filters. We remind however that NGC 205 is a non standard dE with central gas and some star formation activity that would make it classified as a dE with blue center by Lisker et al. (2006b). Given its high surface brightness, M32 is a non genuine dwarf elliptical. The photometric data of NGC 205 and M32 are taken from Gil de Paz et al. (2007)
  14. High resolution HST observations of dwarf ellipticals in the Virgo cluster revealed the presence of small nuclei also in objects classified as non-nucleated in the VCC (Lotz et al. 2004; Côte et al. 2006), whose distribution does not seem to depend on the position within the Virgo cluster. For consistency with our morphological classification and for completeness reasons, we consider here the VCC classification which might be biased, for its limited angular resolution, to the most extended nuclei.
  15. This is the absorption line uncontaminated by the H emission, which might be present whenever star formation is still active
  16. SDSS, Michielsen et al. (2007) and Geha et al. (2003) spectroscopic H and H data are limited to the central 3-4 arcsec of the observed galaxies, and are thus not directly comparable to the model predictions which are relative to the whole galaxy. Integrated spectroscopy however is available only for a small fraction of the quiescent dwarfs.

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