Evolution of M81 with Exponentially Decreasing Star Formation Rate of PEGASE

Li, Jiuli; Xu, Zhiyong; Ma, Jun; Chen, Jiansheng

doi:10.1088/1009-9271/4/2/143

Cited by 8 publications

(10 citation statements)

References 19 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Comparing with previous studies of nearby galaxies, like M81 ( Li et al (2004b) found that the age of the bulge regions of M81 is about 4 Gyr, which is almost twice as old as the disk regions, which is around 2 Gyr. Absolute values of the fitted ages are model dependent, so the comparison can only be made in a relative sense.…”

Section: Star Formation In the Leo Tripletsupporting

confidence: 55%

See 1 more Smart Citation

Multicolor Photometry and Stellar Population Synthesis Study of the Interacting Galaxies of the Leo Triplet

Duan¹

2006

Astron J

View full text Add to dashboard Cite

This paper studies the nearby interacting group the Leo Triplet using multicolor photometry data obtained with the National Astronomical Observatories of China 60 cm/90 cm Schmidt telescope. The observation covers the entire area of the three galaxies ( NGC 3623, NGC 3627, and NGC 3628), and spectral energy distributions (SEDs) of each galaxy are obtained. By comparing the observed SEDs of each part of the galaxies with the theoretical ones generated by instantaneous burst evolutionary synthesis models with different metallicities (Z ¼ 0:0001, 0.008, 0.02, and 0.05), two-dimensional relative age distribution maps of the three galaxies were obtained. NGC 3623 exhibits a very weak age gradient from the bulge to the disk. This gradient is absent in NGC 3627. The ages of the dominant stellar populations of NGC 3627 and NGC 3628 are consistent, and this consistency is model independent (0.5-0.6 Gyr, Z ¼ 0:02), but the ages of NGC 3623 are systematically older (0.7-0.9 Gyr, Z ¼ 0:02). The results indicate that NGC 3627 and NGC 3628 have undergone synchronous evolution and that the interaction has likely triggered starbursts in both galaxies. For NGC 3623, however, the weak age gradient may indicate recent star formation in its bulge, which has caused its color to turn blue. Evidence is found for a potential bar existing in the bulge of NGC 3623, and my results support the view that NGC 3623 does interact with NGC 3627 and NGC 3628.

show abstract

Section: Star Formation In the Leo Tripletsupporting

confidence: 55%

“…For convenience, I use flux ratios that are independent of distance (Li et al 2004a(Li et al , 2004b. The flux ratio is calculated as the integrated luminosity of the ith filter relative to that of the h filter (k h ¼ 6075 8):…”

Section: Flux Ratio and Fitting Algorithmmentioning

confidence: 99%

Multicolor Photometry and Stellar Population Synthesis Study of the Interacting Galaxies of the Leo Triplet

Duan¹

2006

Astron J

View full text Add to dashboard Cite

show abstract

“…Light decomposition and color distributions reveal that this galaxy has a disk-like bulge (i.e., pseudobulge) (Natali et al 1992;Cornett et al 1994;Sánchez et al 2011;Ganda et al 2009). Besides the fifteen intermediateband observations taken with the 60/90 cm Schmidt telescope of National Astronomical Observatories of China as also used by Kong et al (2000) and Li et al (2004), there are plenty of on-line archival data for this galaxy from various surveys and telescopes, such as the Galaxy Evolution Explorer (GALEX), Two Micron All Sky Survey (2MASS), and Spitzer space telescope. These panchromatic photometric data-set from UV to IR can considerably aid us to obtain more accurate estimations of the properties (age, metallicity and intrinsic reddening).…”

Section: Introductionmentioning

confidence: 99%

“…They provide some basic information about the star formation history, chemical compositions and evolution, and interstellar medium. Both Kong et al (2000) and Li et al (2004) adopted different evolutionary population synthesis (EPS) models to analyze the structure and evolution of a nearby Sab spiral galaxy (M81) using the photometric data of multiple intermediate-band filters from 3000 Å and 10000 Å in the Beijing-Arizona-Taiwan-Connecticut (BATC) multicolor sky survey. EPS has become a very popular technique to study the properties of stellar populations in galaxies (Fioc & Rocca-Volmerange 1997;Leitherer et al 1999;Bruzual & Charlot 2003;Kotulla et al 2009) and it has been applied in many fields such as star clusters, galaxies, and galactic clusters (Abraham et al 1996;Kong et al 2000;Ma et al 2009a).…”

Section: Introductionmentioning

confidence: 99%

Stellar Population Properties and Evolution Analysis of NGC 628 With Panchromatic Photometry

Zou

Zhang

Yang

et al. 2011

Self Cite

View full text Add to dashboard Cite

Panchromatic spectral energy distribution (SED) from the ultraviolet (UV), optical to infrared (IR) photometry of NGC 628, combined with the evolutionary stellar population synthesis, is used to derive the spatially resolved age, metallicity and reddening maps. These parameter distributions show that the bulge of this galaxy is a disk-like pseudobulge, which has the Sérsic index close to the exponential law, rich gas, and a young circumnuclear ring structure. We also discover the disk has two distinct regions with different radial age and metallicity gradients. The inner region is older and has a much steeper age gradient than the outer region of the disk. Both these two regions and the central young structure can be seen in the radial profile of the optical color. Based on the age and reddening distributions, we consider that the pseudobulge and disk are likely to have grown via the secular evolution, which is the redistribution of mass and energy through the angular momentum transport caused by the non-axisymmetric potential of the spirals. However, possible gas accretion events could affect the outer region of the disk, due to abundant Hi gas accumulating in the outer disk.

show abstract

“…In some cases, more complex SFH fitting, to line strengths or colours, is attempted using, for example, multiple SSPs (e.g. Heavens et al 2004; Rossa et al 2006; Serra & Trager 2007) or an exponentially decaying SFH (Fritze‐von Alvensleben & Gerhard 1994; Li et al 2004; Ganda et al 2007) sometimes with optional starbursts (Temporin & Fritze‐von Alvensleben 2006). Empirical fitting of too many SSPs is undermined by the degeneracy between parameters.…”

Section: Introductionmentioning

confidence: 99%

The impact of binary-star yields on the spectra of galaxies

Sansom

Izzard

Ocvirk

2009

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

One of the complexities in modelling integrated spectra of stellar populations is the effect of interacting binary stars besides Type Ia supernovae (SNeIa). These include common envelope systems, cataclysmic variables, novae, and are usually ignored in models predicting the chemistry and spectral absorption line strengths in galaxies. In this paper, predictions of chemical yields from populations of single and binary stars are incorporated into a galactic chemical evolution model to explore the significance of the effects of these other binary yields. Effects on spectral line strengths from different progenitor channels of SNeIa are also explored. Small systematic effects are found when the yields from binaries, other than SNeIa, are included, for a given star formation history. These effects are, at present, within the observational uncertainties on the line strengths. More serious differences can arise in considering different types of SNIa models, their rates and contributions.

show abstract

Evolution of M81 with Exponentially Decreasing Star Formation Rate of PEGASE

Cited by 8 publications

References 19 publications

Multicolor Photometry and Stellar Population Synthesis Study of the Interacting Galaxies of the Leo Triplet

Multicolor Photometry and Stellar Population Synthesis Study of the Interacting Galaxies of the Leo Triplet

Stellar Population Properties and Evolution Analysis of NGC 628 With Panchromatic Photometry

The impact of binary-star yields on the spectra of galaxies

Contact Info

Product

Resources

About