<i>GALEX</i>Observations of Low Surface Brightness Galaxies: UV Color and Star Formation Efficiency

Boissier, S.; Paz, A. Gil de; Boselli, A.; Buat, V.; Madore, Barry F.; Chemin, L.; Balkowski, C.; Amram, P.; Carignan, C.; Driel, W. van

doi:10.1086/588580

Cited by 107 publications

(146 citation statements)

References 71 publications

Supporting

Mentioning

126

Contrasting

Order By: Relevance

“…Moreover, GALEX observations have recently revealed extended XUV-disks around HSB spirals (Thilker et al 2007). Also some GLSB galaxies have been observed with GALEX (Boissier et al 2008) and, at such wavelengths, they resemble the XUV-disk galaxies of Thilker et al (2007) (see in particular Malin 1, Malin 2 and NGC 7589).…”

Section: Discussionmentioning

confidence: 59%

See 1 more Smart Citation

Structure and dynamics of giant low surface brightness galaxies

Lelli

Fraternali

Sancisi

2010

A&A

141

View full text Add to dashboard Cite

Giant low surface brightness (GLSB) galaxies are commonly thought to be massive, dark matter dominated systems. However, this conclusion is based on highly uncertain rotation curves. We present here a new study of two prototypical GLSB galaxies: Malin 1 and NGC 7589. We re-analysed existing H I observations and derived new rotation curves, which were used to investigate the distributions of luminous and dark matter in these galaxies. In contrast to previous findings, the rotation curves of both galaxies show a steep rise in the central parts, typical of high surface brightness (HSB) systems. Mass decompositions with a dark matter halo show that baryons may dominate the dynamics of the inner regions. Indeed, a "maximum disk" fit gives stellar mass-to-light ratios in the range of values typically found for HSB galaxies. These results, together with other recent studies, suggest that GLSB galaxies are systems with a double structure: an inner HSB early-type spiral galaxy and an outer extended LSB disk. We also tested the predictions of MOND: the rotation curve of NGC 7589 is reproduced well, whereas Malin 1 represents a challenging test for the theory.

show abstract

Section: Discussionmentioning

confidence: 59%

“…(1) Barth (2007); (2) Nasa Extra-galactic Database (NED); (3) Pickering et al (1997) give M V = −22.9 ± 0.4 for Malin 1 and M R = −21.9 ± 0.2 for NGC 7589; Impey & Bothun (1989) give B − V = 0.8 for Malin 1; Galaz et al (2006) give B−R = 1.5 for NGC 7589; (4) This work; (5) Boissier et al (2008).…”

Section: H I Data Analysismentioning

confidence: 96%

Structure and dynamics of giant low surface brightness galaxies

Lelli

Fraternali

Sancisi

2010

A&A

141

View full text Add to dashboard Cite

show abstract

“…A star formation history of LSB galaxies that includes the existence of short (a few 100 Myr) bursts separated by longer quiescent periods is preferred by many authors (Schombert et al 2001;Boissier et al 2003;Vallenari et al 2005;Boissier et al 2008); these starbursts are too short-lived to transform the galaxy to HSB. In N271 this scenario looks very likely; the progenitor of this core-collapse SN presumably formed in the most recent starburst.…”

Section: Discussionmentioning

confidence: 99%

Supernovae without host galaxies?

Zinn

Stritzinger

Braithwaite

et al. 2012

A&A

View full text Add to dashboard Cite

Context. A remarkable fraction of supernovae (SNe) have no obvious host galaxy. Two possible explanations are that (i) the host galaxy is simply not detected within the sensitivity of the available data or that (ii) the progenitor is a hypervelocity star that has escaped its parent galaxy. Aims. We use the Type IIb SN 2009Z as a prototype of case (i), an example of how a very faint (here low surface brightness; LSB) galaxy can be discovered via the observation of a seemingly host-less SN. By identifying and studying LSB galaxies that host SNe related to the death of massive stars, we can place constraints on the stellar population and environment of LSB galaxies, which at present are poorly understood. Methods. We use archival ultraviolet (UV) and optical imaging, as well as an H I spectrum taken with the 100 m Effelsberg Radio Telescope to measure various parameters of the host galaxy, in particular its redshift, stellar and H I mass, and metallicity. Results. From the Effelsberg spectrum, a redshift z = 0.02513 ± 0.00001 and an H I mass of 2.96 ± 0.12 × 10 9 M are computed. This redshift is consistent with that obtained from optical emission lines of SN 2009Z. Furthermore, a gas mass fraction of f g = 0.87±0.04 is obtained, one of the highest fractions ever measured. The host galaxy shows signs of recently enhanced star formation activity with a far-UV derived extinction-corrected star formation rate (SFR) of 0.44 ± 0.34 M yr −1 . Based on the B-band luminosity we estimate an extinction-corrected metallicity following the calibration by Pilyugin (2001) of 12 + log O H = 8.24 ± 0.70. Conclusions. The presence of a Type IIb SN in an LSB galaxy suggests, contrary to popular belief, that massive stars can be formed in this type of galaxies. Furthermore, our results imply that LSB galaxies undergo phases of small, local burst activity intermittent with longer phases of inactivity, rather than a continuous but very low SFR. Discovering faint (LSB) galaxies via bright supernova events happening in them offers an excellent opportunity to improve our understanding of the nature of LSB galaxies.

show abstract

“…Previous observations of nearby galaxies have shown that the low surface brightness features associated with low HI column densities, such as low surface brightness galaxies (Boissier et al 2008), dwarf ellipticals (Boselli et al 2005a;Boselli et al 2008a), the outskirts of spiral galaxies (Thilker et al 2005) or tidal debris (Boselli et al 2005b;Duc et al 2007;Boquien et al 2007Boquien et al , 2009, have UV surface brightnesses in both the FUV and NUV bands of ∼27.5−28 mag arcsec −2 , thus undetectable in the GALEX All-Sky Imaging Survey, which is limited to ∼26 mag arcsec −2 . Medium Deep Imaging Survey (MIS; 1 orbit/pointing, ∼1500 s) are thus necessary to study the effects of the environment on cluster galaxies.…”

Section: The Guvics Surveymentioning

confidence: 97%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Boissier

Heinis

et al. 2011

A&A

Self Cite

View full text Add to dashboard Cite

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS) is a complete blind survey of the Virgo cluster covering ∼40 sq. deg in the far UV (FUV, λ eff = 1539 Å, Δλ = 442 Å) and ∼120 sq. deg in the near UV (NUV, λ eff = 2316 Å, Δλ = 1060 Å). The goal of the survey is to study the ultraviolet (UV) properties of galaxies in a rich cluster environment, spanning a wide luminosity range from giants to dwarfs, and regardless of prior knowledge of their star formation activity. The UV data will be combined with those in other bands (optical: NGVS; far-infrared -submm: HeViCS; HI: ALFALFA) and with our multizone chemo-spectrophotometric models of galaxy evolution to make a complete and exhaustive study of the effects of the environment on the evolution of galaxies in high density regions. We present here the scientific objectives of the survey, describing the observing strategy and briefly discussing different data reduction techniques. Using UV data already in-hand for the central 12 sq. deg we determine the FUV and NUV luminosity functions of the Virgo cluster core for all cluster members and separately for early-and late-type galaxies and compare it to the one obtained in the field and other nearby clusters (Coma, A1367). This analysis shows that the FUV and NUV luminosity functions of the core of the Virgo clusters are flatter (α ∼ −1.1) than those determined in Coma and A1367. We discuss the possible origin of this difference.

show abstract

GALEXObservations of Low Surface Brightness Galaxies: UV Color and Star Formation Efficiency

Cited by 107 publications

References 71 publications

Structure and dynamics of giant low surface brightness galaxies

Structure and dynamics of giant low surface brightness galaxies

Supernovae without host galaxies?

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Contact Info

Product

Resources

About