Multifrequency observations of MKN 171 = NGC3690

Arnault, Philippe; Augarde, R.; Casoli, F.; Combes, F.; Figon, P.; Kunth, D.

doi:10.1007/3-540-50438-9_319

Cited by 24 publications

(29 citation statements)

References 3 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…It was detected in CO(1-0) by Arnault et al (1988), Gondhalekar et al (1998) and Tacconi & Young (1987). In the latter work, the authors derived an H 2 mass of 2.87 × 10 7 M .…”

Section: Introductionmentioning

confidence: 88%

Integral field near-infrared spectroscopy of II Zw 40

Vanzi

Cresci

Telles

et al. 2008

A&A

View full text Add to dashboard Cite

We present integral field spectroscopy in the near-infrared of the nearby starburst galaxy II Zw 40. Our new observations provide an unprecedented detailed view of the interstellar medium and star formation of this galaxy. The radiation emitted by the galaxy is dominated by a giant HII region, which extends over an area of more than 400 pc in size. A few clusters are present in this area, however, one, in particular, appears to be the main source of ionizing photons. We derive the properties of this object and compare them with those of the 30 Doradus cluster in the Large magellanic cloud (LMC). We study the spatial distribution and velocity field of different components of the inetrstellar medium (ISM), mostly through the Bracket series lines, the molecular hydrogen spectrum, and [FeII]. We find that [FeII] and H 2 are mostly photon excited, but while the region emitting [FeII] is almost coincident with the giant HII region observed in the lines of atomic H and He, the H 2 has a quite different distribution in space and velocity. The age of the stellar population in the main cluster is such that no supernova (SN) should be present yet so that the gas kinematics must be dominated by the young stars. We do not see, in the starbursting region, any geometrical or dynamical structure that can be related to the large scale morphology of the galaxy.

show abstract

“…It was detected in CO(1-0) by Arnault et al (1988), Gondhalekar et al (1998) and Tacconi & Young (1987). In the latter work, the authors derived an H 2 mass of 2.87 × 10 7 M .…”

Section: Introductionmentioning

confidence: 88%

Integral field near-infrared spectroscopy of II Zw 40

Vanzi

Cresci

Telles

et al. 2008

A&A

View full text Add to dashboard Cite

show abstract

“…However the situation in low metallicity gas is still under debate. Many attempts to detect CO in BCGs galaxies have been reported so far (Combes 1986, Young et al 1986, Arnault et al 1988, Sage et al 1992, Israel et al 1995, Gondhalekar et al 1998) but the CO luminosity of BCGs is very low, in comparison with their observed star formation rate, mostly yielding only upper limits. This lack of detection may be because the low metallicity of BCGs hides the true molecular phase by a low CO to H 2 conversion factor.…”

Section: Gas Content and Dynamics Of Bcgsmentioning

confidence: 99%

The most metal-poor galaxies

Kunth

Östlin

2000

Astronomy and Astrophysics Review

Self Cite

381

428

View full text Add to dashboard Cite

Metallicity is a key parameter that controls many aspects in the formation and evolution of stars and galaxies. In this review we focus on the metal deficient galaxies, in particular the most metal-poor ones, because they play a crucial rôle in the cosmic scenery. We first set the stage by discussing the difficult problem of defining a global metallicity and how this quantity can be measured for a given galaxy. The mechanisms that control the metallicity in a galaxy are reviewed in detail and involve many aspects of modern astrophysics: galaxy formation and evolution, massive star formation, stellar winds, chemical yields, outflows and inflows etc. Because metallicity roughly scales as the galactic mass, it is among the dwarfs that the most metalpoor galaxies are found. The core of our paper reviews the considerable progress made in our understanding of the properties and the physical processes that are at work in these objects. The question on how they are related and may evolve from one class of objects to another is discussed. While discussing metal-poor galaxies in general, we present a more detailed discussion of a few very metal-poor blue compact dwarf galaxies like IZw18. Although most of what is known relates to our local universe, we show that it pertains to our quest for primeval galaxies and is connected to the question of the origin of structure in the universe. We discuss what QSO absorption lines and known distant galaxies tell us already? We illustrate the importance of star-forming metal-poor galaxies for the determination of the primordial helium abundance, their use as distance indicator and discuss the possibility to detect nearly metal-free galaxies at high redshift from Lyα emission.

show abstract

“…The dot-dashed line shows the beam-averaged densities implied if each GMC is in virial equilibrium (Table 4). detect (Israel 1986 ;Arnault et al 1988 ;Verter & Hodge 1995 ;Wilson 1995 ;Arimoto, Sofue, & Tsujimoto 1996). The fact that NGC 3077 is a low-mass dwarf with solar metallicity (Heckman 1980 ;Martin 1997 ;Sakai & Madore 2001) and strong star formation makes it an interesting object in which to estimate the conversion factor.…”

Section: Conversion Factor In Ngc 3077mentioning

confidence: 99%

Molecular Gas and Star Formation in NGC 3077

Meier¹,

Turner²,

Beck³

2001

The Astronomical Journal

View full text Add to dashboard Cite

We present high-resolution CO(1È0) and CO(2È1) images of the central 1 kpc of NGC 3077 (D2A .5) made with the Owens Valley Millimeter Array. CO emission is distributed in three major complexes, which resolve into at least seven giant molecular clouds (GMCs). Two complexes are associated with the central starburst. A third, more distant complex is not associated with strong star formation. The GMCs are D70 pc in size and contain D106 of molecular gas. The Galactic conversion factor appears M _ applicable to NGC 3077, consistent with its solar metallicity. Galactic rotation in NGC 3077 is detected for the Ðrst time in the molecular gas. The molecular gas counterrotates with respect to the large-scale H I tidal bridge. The molecular clouds closest to the starburst have supervirial line widths, possibly related to the turbulence generated by the starburst. The 2.6 mm radio continuum Ñux indicates that thermal bremsstrahlung dominates the emission from the starburst region below 5 cm and that the N Lyc^3.7 ] 1052 s~1, or D3000 O7 stars, corresponds to a star formation rate of 0.4 yr~1. At this rate, the M _ amount of molecular gas can sustain star formation for only D10 Myr ; thus, NGC 3077 is a true starburst galaxy. The derived age of the starburst is consistent with the inferred ages of the superbubbles, which suggests that the burst is much younger than the age of the M81ÈM82ÈNGC 3077 interaction. We suggest that it is caused by gas that was pulled out of NGC 3077 during the interaction with M81, raining back down onto the galaxy.

show abstract

Multifrequency observations of MKN 171 = NGC3690

Cited by 24 publications

References 3 publications

Integral field near-infrared spectroscopy of II Zw 40

Integral field near-infrared spectroscopy of II Zw 40

The most metal-poor galaxies

Molecular Gas and Star Formation in NGC 3077

Contact Info

Product

Resources

About