FIGGS: Faint Irregular Galaxies GMRT Survey – overview, observations and first results

By A. Begum, J. Chengalur, I. Karachentsev, M. Sharina, S. Kaisin. 2008

190 citations recorded by the source corpus.

The Faint Irregular Galaxies GMRT Survey (FIGGS) is a Giant Metrewave Radio Telescope (GMRT) based HI imaging survey of a systematically selected sample of extremely faint nearby dwarf irregular galaxies. The primary goal of F IGGS is to provide a comprehensive and statistically robust characterization of the neut ral inter-stellar medium properties of faint, gas rich dwarf galaxies. The FIGGS galaxies represent the extremely low-mass end of the dwarf irregular galaxies population, with a median MB � 13:0 and median HI mass of � 3�10 7 M� , extending the baseline in mass and luminosity space for a comparative study of galaxy properties. The HI data is supplemented with observations at other wavelengths. In addition, distances accurate to � 10% are available for most of the sample galaxies. This paper gives an introduction to FIGGS, describe the GMRT observations and presents the first results from the HI observations. From the FIGGS data we confi rm the trend of increasing HI to optical diameter ratio with decreasing optical luminosi ty; the median ratio of DH I/DH o for the FIGGS sample is 2.4. Further, on comparing our data with aperture synthesis surveys of bright spirals, we find at best marginal evidence for a decrea se in average surface density with decreasing HI mass. To a good approximation the disks of gas rich galaxies, ranging over 3 orders of magnitude in HI mass, can be described as being drawn from a family with constant HI surface density.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/1577f2e094def4e8fa651923b0acef188b02fec3

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

THE UNIVERSAL STELLAR MASS–STELLAR METALLICITY RELATION FOR DWARF GALAXIES (2013, background): “Low mass galaxies have high gas mass fractions (Begum et al. 2008).”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “These surveys in turn have led to large spinoff surveys in H I (e.g., THINGS, Walter et al. 2008; FIGGS, Begum et al. 2008; Local Volume H I Survey; Koribalski 2010; LITTLE THINGS, Hunter et al. 2007) and in CO (e.g., BIMA-SONG, Helfer et al. 2003; IRAM HERACLES, Leroy et al. 2009; JCMT NGLS, Wilson”
Globular cluster systems in nearby dwarf galaxies – III. Formation efficiencies of old globular clusters (2010, methodology): “MHI was calculated from the HI magnitudes listed in the LEDA database (Paturel et al. 2003) or from HI fluxes in NED or Begum et al. (2008) following Roberts & Haynes (1994), i.e. MHI = 2.36 × 105 × D2 × FHI, where D is the distance in Mpc and FHI is the HI flux in Jy km s −1.”
The rotation curves shapes of late-type dwarf galaxies (2009, background): “The ongoing FIGGS survey (e.g., Begum et al. 2008) will likely fill this gap.”
THE BARYONIC TULLY–FISHER RELATION OF GAS-RICH GALAXIES AS A TEST OF ΛCDM AND MOND (2011, methodology): “For the very low mass galaxies of Begum et al. (2008a), fV < 1 is certainly possible, but it seems unlikely to be tiny.”
HIGH-RESOLUTION MASS MODELS OF DWARF GALAXIES FROM LITTLE THINGS (2015, background): “Over the past decade, several high-resolution neutral hydrogen (Hi) surveys of galaxies in the local Universe (<11 Mpc) using radio interferometers, among others THINGS20 (Walter et al. 2008), VLA-ANGST21 17 The Sloan Digital Sky Survey (http://www.sdss.org/) 18 The 2dF Galaxy Redshift Survey (http:”
Is there a "too big to fail" problem in the field? (2014, background): “…Volume HI Survey (LVHIS; Kirby et al. 2012), 5 galaxies from Trachternach et al. (2009), 4 galaxies from Côté et al. (2000), 28 galaxies from the Faint Irregular Galaxies GMRT Survey (FIGGS; Begum et al. 2008a,b), 17 galaxies from the LITTLE THINGS survey (Hunter et al. 2012; Oh et al., in prep.)”
THE ACS NEARBY GALAXY SURVEY TREASURY. VIII. THE GLOBAL STAR FORMATION HISTORIES OF 60 DWARF GALAXIES IN THE LOCAL VOLUME (2011, methodology): “The final sample of dTrans was classified based on HI and Hα measurements in the literature (Côté et al 1997; Skillman et al. 2003a; Karachentsev et al. 2004; Karachentsev & Kaisin 2007; Begum et al. 2008; Bouchard et al. 2009; Côté et al. 2009).”
CONFIRMATION OF FAINT DWARF GALAXIES IN THE M81 GROUP (2013, background): “Normal giant and dwarf galaxies with both young and old stars and detected HI (Begum et al. 2008; Roychowdhury et al. 2012) are identified by open symbols, with the 3 newly discovered cases given emphasis.”
Thick gas discs in faint dwarf galaxies (2010, methodology): “However, the observed kinematics ofgas in these galaxies (see Begum et al. 2003; Begum & Chengalur 2003, 2004a,b; Begum, Chengalur & Karachentsev 2005; Begum et al. 2005, 2006, 2008, etc.) shows that the gas has a significant rotational support.”
COMPARISON OF Hα AND UV STAR FORMATION RATES IN THE LOCAL VOLUME: SYSTEMATIC DISCREPANCIES FOR DWARF GALAXIES (2009, background): “…ionized gas appears to be nominally higher in dwarfs; e.g., Oey et al. 2007), star forming dwarf galaxies are often embedded in large envelopes of HI (e.g., Begum et al. 2008) which makes it unlikely that the Lyman continuum photons find their way completely out of a galaxy and into the IGM.”