Physical properties of young stellar populations in 24 starburst galaxies observed with FUSE*

Pellerin, Anne; Robert, Carmelle

doi:10.1111/j.1365-2966.2007.12250.x

Cited by 17 publications

(19 citation statements)

References 126 publications

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“…In Figure 3, the minimum χ 2 set reaches its bottom at Z = 0.008 and α λ = −2.0. This is consistent with other studies that show metallicities near solar value prevail in SB galaxies (Tadhunter et al 2005;Pellerin & Robert 2007), and also that the power-law continuum slope falls around α λ = −2 (Francis 1996;Vanden Berk et al 2001;Letawe et al 2007). Moreover, the power-law index does not affect the synthesis very much.…”

Section: Parameters Determinationsupporting

confidence: 93%

Iras F13308+5946: A Possible Transition Phase From Type I Ultraluminous Infrared Galaxy to Optical Quasar

Meng¹,

Wu²,

Gu³

et al. 2010

ApJ

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We present a stellar population synthesis study of a type I luminous infrared galaxy: IRAS F13308+5946. It is a quasar with absolute magnitude M i = −22.56 and has the spectral feature of a Seyfert 1.5 galaxy. Optical images show characteristics of later stages of a merger. With the help of the stellar synthesis code starlight and both Calzetti et al.'s and Leitherer et al.'s extinction curves, we estimate the past infrared (IR) luminosities of the host galaxy and find that it may have experienced an ultraluminous infrared galaxy (ULIRG) phase for nearly 300 Myr, so this galaxy has probably experienced a type I ULIRG phase. Both nuclear starburst (SB) and active galactic nuclei contribute to the present IR luminosity budget, with the SB contributing ∼70%. The mass of the supermassive black hole is M BH = 1.8 × 10 8 M and the Eddington ratio L bol /L Edd is 0.12, both of which are approximate typical values of Palomar-Green QSOs. These results indicate that IRAS F13308+5946 is probably at the transitional phase from a type I ULIRG to a classical QSO.

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Section: Parameters Determinationsupporting

confidence: 93%

Iras F13308+5946: A Possible Transition Phase From Type I Ultraluminous Infrared Galaxy to Optical Quasar

Meng¹,

Wu²,

Gu³

et al. 2010

ApJ

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“…Gonzalez Delgado et al 1997;Leitherer et al 1999;Maraston et al 2009). Nearby starburst galaxies also have UV spectral diagnostics that are consistent with a Salpeter distribution of high mass stars (see reviews Pellerin &Robert 2007 andLeitherer 2009). Tremonti et al (2001) have studied the UV spectral properties across the actively star forming galaxy NGC 5253, focussing mainly on the difference between the spectra of "clusters" and "the field".…”

Section: Hα Uv and Infrared Studies Of Integrated Stellar Populationsmentioning

confidence: 94%

A Universal Stellar Initial Mass Function? A Critical Look at Variations

Bastian

Covey

Meyer

2010

Annu. Rev. Astron. Astrophys.

926

453

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Few topics in astronomy initiate such vigorous discussion as whether or not the initial mass function (IMF) of stars is universal, or instead sensitive to the initial conditions of star formation. The distinction is of critical importance: the IMF influences most of the observable properties of stellar populations and galaxies, and detecting variations in the IMF could provide deep insights into the process by which stars form. In this review, we take a critical look at the case for IMF variations, with a view towards whether other explanations are sufficient given the evidence. Studies of the field, local young clusters and associations, and old globular clusters suggest that the vast majority were drawn from a "universal" IMF: a power-law of Salpeter index (Γ = 1.35) above a few solar masses, and a log normal or shallower power-law (Γ ∼ 0 − 0.25) between a few tenths and a few solar masses (ignoring the effects of unresolved binaries). The shape and universality of the IMF at the stellar-substellar boundary is still under investigation and uncertainties remain large, but most observations are consistent with a IMF that declines (Γ < −0.5) well below the hydrogen burning limit. Observations of resolved stellar populations and the integrated properties of most galaxies are also consistent with a "universal IMF", suggesting no gross variations in the IMF over much of cosmic time. There are indications of "non-standard" IMFs in specific local and extragalactic environments, which clearly warrant further study. Nonetheless, there is no clear evidence that the IMF varies strongly and systematically as a function of initial conditions after the first few generations of stars. We close with suggestions for future work that might uncover more subtle IMF variations than those that could be discerned to date.

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“…Kaaret & Alonso-Herrero (2008) have identified a number of X-ray point sources in NGC 4194, which they relate to the rate of star formation. Pellerin & Robert (2007) report far-ultraviolet observations of a young stellar population in NGC 4194. Devereux (1989) suggested that the central 2.2 μm luminosity is dominated by young red supergiants.…”

Section: Introductionmentioning

confidence: 99%

Characteristics of Star-Forming Regions in the Advanced Minor-Merger, Luminous Infrared Galaxy NGC 4194

Weistrop

Nelson

Angione

et al. 2012

The Astronomical Journal

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We report the results of long-slit spectroscopy at position angles 68• , 131• , and 164• for the minor-merger NGC 4194, a luminous infrared starburst galaxy. The mass within 1.2 kpc of the dynamical center is estimated to be 4.8 × 10 9 to 1.7 × 10 10 M , depending on the assumed inclination to the plane of the sky. The star formation rate (SFR) in the areas sampled is 8 M yr −1 . The metallicity, log(O/H) + 12, ranges from ∼8.8 to >9.0 in regions of significant star formation, suggesting that the metallicity has been enhanced by the current star formation. The star-forming regions range in age from 5 to 9 Myr, with the youngest ages occurring in the regions of high SFR. Electron temperatures and the location of the spectra in emission line diagnostic diagrams suggest the presence of shock waves, presumably due to the presence of supernovae, winds from massive stars, and/or collisions of clouds due to the merger. The presence of massive stars and supernovae is consistent with the ages determined for the star-forming regions. The ages of the continua produced by the stellar population are estimated to range from 10 Myr to 5 Gyr. Much of the stellar population represented in the continua was probably formed before the merger and represents the progenitor galaxies.

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Physical properties of young stellar populations in 24 starburst galaxies observed with FUSE*

Cited by 17 publications

References 126 publications

Iras F13308+5946: A Possible Transition Phase From Type I Ultraluminous Infrared Galaxy to Optical Quasar

Iras F13308+5946: A Possible Transition Phase From Type I Ultraluminous Infrared Galaxy to Optical Quasar

A Universal Stellar Initial Mass Function? A Critical Look at Variations

Characteristics of Star-Forming Regions in the Advanced Minor-Merger, Luminous Infrared Galaxy NGC 4194

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