Signature of recent star formation in ring S0s

Signature of recent star formation in ring S0s

S0s galaxies have been introduced by Hubble (1936) in his "tuning fork" galaxy classification as a more or less hypothetical transition class between ellipticals and spirals. The bulge and the disk are the defining structures of S0s. Later classification schemes by de Vaucouleurs et al. (1991, RC3) and Sandage & Tammann (1987, RSA) take into account the presence of several sub-structures detected within the S0s class: bars, inner and outer rings as well as lenses (from here the widely used term of lenticulars as synonim of S0s) and ovals are often found.
S0s are, as a rule, admitted in the vast class of early-type galaxies, together with ellipticals, with which they share typically passively evolving stellar populations.

From an evolutionary point of view it is widely believed that S0s were initially spirals which lost their interstellar medium during collisions (Spitzer and Baade 1951) by "harassment" (More et al. 1986) or by "ram-pressure". Simulations shows that such events could occur both in cluster (Gunn and Gott 1972) and in groups (see e.g. Bekki 2009).

From the kinematical point of view, genuine S0s are quite distinct from giant ellipticals since they are fast rotating, like late-type galaxies. At the same time, if S0s were originally spirals, they should have formed their mass over a significant fraction of the Hubble time, following a star formation history more similar to that of early-type galaxies rather than that of giant elliptical galaxies. In this context, our multi-wavelength study of nearby ETGs (Marino et al. 2010) shows that S0s, characterized through their luminosity profiles and by the low values of the Sersic index (Sersic 1968), have the lowest values of a-enhancements [a/Fe] in the sample. The low [a/Fe] suggest a "more prolonged" star formation in the S0 galaxies with respect to ellipticals in the sample (Annibali et al. 2007; Annibali et al. 2010).

Several mechanisms, both internal and external to the galaxy, may be envisaged to produce the signature of a "prolonged" star formation. The removal of the ISM from a possible spiral precursor may quench the ongoing star formation transforming the debris in a S0 with signature of prolonged star formation, as well as an external wet accretion and/or the inner secular evolution, e.g. driven by a tumbling bar (see e.g. van den Bosch and Emsellem 1998).

The Galaxy Evolution Explorer satellite (GALEX) has widely contributed to explore the above mechanisms. "Wet" accretions, and the rejuvenation of the stellar population, has been evidenced in ETGs (see e.g. Rampazzo et al. 2007 and Marino et al. 2009). Recently, Thilker et al. (2010) found in NGC 404, a nearby well known S0, an external ring-like structure with signatures of recent star formation. The structure has been likely produced by a "wet accretion accretion/merger"

We used GALEX for analyzing five S0s showing outer ring and/or arm-like structures aiming at understanding the nature of the ring and to map possible star formation episodes. Such structures are prominent in the UV and reveal recent star formation. We quantitatively characterize these rejuvenation events, estimating the average age and stellar mass of the ring structure as well as of the entire galaxy. The mass fraction of the UV-bright rings is a few percent of the total galaxy mass, although the UV ring luminosity reaches 70% of the galaxy luminosity. The integrated colors of these S0s locates them in the red sequence (NGC 2962) and in the so-called "green valley". We suggest that the star formation episodes may induced by different triggering mechanisms, such a the inner secular evolution driven by bars, and interaction episodes. 

 Figure 1: Color composite images of S0s with ring observed with GALEX (left panel) and with SDSS (right panel). Blue ring in the left panel indicate areas of recent star formation (about 10^8 years ago). Notice the different shape pf the rings likely due to different formation mechanisms.

People: Roberto Rampazzo, Lucio M. Buson, Michela Mappelli, Paola Mazzei

Collaborations: Antonietta Marino (Univ. di Padova), Luciana Bianchi (John Hopkins University, USA)

Recent publications: Marino A. et al. 2011, ``UV Universe 2010", Ap&SS, 249; Marino A. et al. 2011, ApJ, 736, 154; Rampazzo R. et al. 2011, ``UV Universe 2010", Ap&SS, 251


Il notiziario online dell'Istituto Nazionale di Astrofisica
  • La quantità di metano rivelata è del 12 per cento superiore a quella misurata 28 anni fa, e anche l’anidride carbonica è cresciuta del 14 per cento. Con il consenso dell’autrice, Patrizia Caraveo, vi riproponiamo quest’articolo apparso ieri sul Sole 24 Ore

  • Dal 10 maggio al 27 luglio, all’Osservatorio astronomico dell'Inaf di Napoli, sei incontri serali di divulgazione scientifica aperti al pubblico. I partecipanti saranno accolti da un welcome drink sulla terrazza dell’Osservatorio. A chiudere le serate, osservazioni astronomiche del cielo

  • Possiamo distinguere un buco nero di Kerr da un buco nero dilatonico? Stando ai risultati pubblicati su Nature Astronomy dagli scienziati della Goethe University di Francoforte, al momento pare sia molto difficile. Abbiamo intervistato uno degli autori dello studio, l’astrofisico Luciano Rezzolla

  • Da Guerre Stellari a Hawking, passando per Marte, le prove per le finali nazionali sono sempre più fantasiose. Quest’anno vi hanno preso parte 80 ragazze e ragazzi selezionati nelle fasi precedenti tra gli oltre 6700 iscritti alla competizione. Cinque di loro andranno nello Sri Lanka per la gara mondiale

  • Domenica 22 aprile ricorre la Giornata mondiale della Terra, giorno in cui si celebra l’ambiente e la salvaguardia del nostro pianeta. Fra le tante iniziative, anche quelle proposte da Nasa e Inaf

  • Happy Birthday Mister Telescope! Il telescopio spaziale Hubble ci regala una vista mozzafiato della Nebulosa Laguna, al centro della quale emerge una stella gigante che irradia e scolpisce le nubi di polveri circostanti con la sua esuberante attività

Go to top

We use cookies to improve our website and your experience when using it. Cookies used for the essential operation of the site have already been set. To find out more about the cookies we use and how to delete them, see our privacy policy.

I accept cookies from this site.

EU Cookie Directive Module Information