A Comparison of the Intrinsic Shapes of Two Different Types of Dwarf Galaxies: Blue Compact Dwarfs and Dwarf Ellipticals

Sung, Eon‐Chang; Han, Cheongho; Барбара,; Ryden, Barbara S.; Chun, Mun-Suk; Kim, Ho-Il

doi:10.1086/305633

Cited by 21 publications

(23 citation statements)

References 39 publications

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“…The axis ratios of the LSB-components have a mean value and standard deviation of b/a LSB = 0.62 ± 0.18, compatible with the mean value of BCDs from Sung et al (1998) . Left: colour−magnitude diagram of the LSB-components of our primary BCD sample, compared to the Virgo early-type dwarf galaxies (labelled "dE" but including dS0s), for which colours were derived within 2R eff .…”

Section: Apparent Axis Ratio Of the Lsb-componentsupporting

confidence: 66%

What will blue compact dwarf galaxies evolve into?

Meyer

Lisker

Janz

et al. 2014

A&A

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We present and analyse the photometric properties of a nearly complete sample of blue compact dwarf (BCD) and irregular galaxies in the Virgo cluster from multi-band SDSS images. Our study intends to shed light on the ongoing debate of whether a structural evolution from present-day star-forming dwarf galaxies in a cluster environment into ordinary early-type dwarf galaxies is possible based on the structural properties. For this purpose, we decompose the surface brightness profiles of the BCDs into the luminosity contribution of the starburst component and that of their underlying low surface brightness (LSB) host. The latter dominates the stellar mass of the BCD. We find that the LSB-components of the Virgo BCDs are structurally compatible with the more compact half of the Virgo early-type dwarfs, except for a few extreme BCDs. Thus, after termination of starburst activity, the BCDs will presumably fade into galaxies that are structurally similar to ordinary early-type dwarfs. In contrast, the irregulars are more diffuse than the BCDs and are structurally similar to the more diffuse half of the Virgo early-type dwarfs. Therefore, the present-day Virgo irregulars are not simply non-starbursting BCDs. If starbursts in cluster BCDs are transient phenomena with a duration of ∼100 Myr or less, during which the galaxies could not travel more than ∼100 kpc, then a substantial number of non-starbursting counterparts of these systems must populate the same spatial volume, namely the Virgo cluster outskirts. The majority of them would have to be early-type dwarfs, based on the abundance of different galaxy types with similar colours and structural parameters to the LSB-components of the BCDs. However, most Virgo BCDs have redder LSB-host colours and a less prominent starburst than typical field BCDs, preventing a robust conclusion on possible oscillations between BCDs and early-type dwarfs.

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Section: Apparent Axis Ratio Of the Lsb-componentsupporting

confidence: 66%

What will blue compact dwarf galaxies evolve into?

Meyer

Lisker

Janz

et al. 2014

A&A

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“…Recent studies show that at least 70% of BCDs are mergers or interactions (Sung 2000, Pustilnik et al 2001, Bekki 2008. But however, until now, only few BCDs are known as post-mergers; He 2-10 ( Kobulnicky et al 1995), Mrk 996 (Thuan et al 1996), and Tololo 3 (Sung et al 2002). Mrk 49 has similar observational characteristics to He 2-10.…”

Section: Discussion and Summary (A) General Morphology And Comparmentioning

confidence: 99%

“…This implies that, in general, BCDs are rather old objects, and their evolution on the Hubble time scale can effectively be determined by short, but very intense star formations. On the other hand, many observations and theoretical works have recently suggested that the origin of BCDs can be closely associated with galaxy merging between low-mass dwarfs or tidal interactions (Noeske et al 2001,Östlin et al 2001, Sung et al 2002, Bekki 2008.…”

Section: Introductionmentioning

confidence: 99%

“…Mrk 49 is classified as a post-merger BCD candidate (Sung et al 2002). Recent surveys show many dwarf galaxy mergers, but rare post-merger or merger remnants (Sung 2000, Pustilnik et al 2001, Sung et al 2002.…”

Section: Introductionmentioning

confidence: 99%

“…Recent surveys show many dwarf galaxy mergers, but rare post-merger or merger remnants (Sung 2000, Pustilnik et al 2001, Sung et al 2002. A post-merger BCD is extremely important to understand the dwarf galaxy merger scenario as the origin of BCDs, and the evolutionary link between dwarf galaxies.…”

Section: Introductionmentioning

confidence: 99%

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Spectroscopic and Photometric Study of Starburst Galaxies: Optical and Near Infrared Properties of a Blue Compact Dwarf Galaxy MRK 49 in the Virgo Cluster

Sung¹,

Kyeong²,

Byun³

2008

Journal of The Korean Astronomical Society

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We present optical and near-infrared imaging and long-slit spectroscopy for the blue compact dwarf galaxy (BCD) Mrk 49 in the Virgo Cluster. The surface brightness distribution analysis shows that Mrk 49 consists of an off-centered blue bright compact core of r = 10 ′′ and a red faint outer exponential envelope. The H α image and color difference suggest that these two components have different stellar populations: a high surface brightness population of massive young stars and an underlying low surface brightness population of older stars. The redder near-infrared colors of the inner most region suggest that the near-infrared flux of Mrk 49 originates from evolved massive stars associated with the current star-forming activity. The total apparent magnitude is B T = 14.32 mag and the mean effective surface brightness is µ ef f (B) = 21.56 mag arcsec −2 . Long-slit spectroscopy shows that Mrk 49 rotates apparently as a solid body within r = 10 ′′ in a plane at position angle 55 degrees with an amplitude of about 20 km sec −1 . The measured radial velocity of Mrk 49 was derived as 1,535 km sec −1 ; and the total mass of stars and gases is in the range of 3 to 6 × 10 9 M ⊙ . The mass-to-light ratios for the central region of Mrk 49 in I and B band are estimated 1.0 and 0.5, respectively. The upper limit of the dark matter to visible matter ratio seems to be < 5. The oxygen abundance is 12 + log(O/H) = 8.21 ± 0.1 which is about one quarter of the solar value while the relative helium abundance appears to be similar to that of the sun.

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$\mathsf{1.65 \mu}$m (H -band) surface photometry of galaxies

Gavazzi

Zibetti

Boselli

et al. 2001

A&A

106

147

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Abstract. We present near-infrared H-band (1.65 µm) observations and surface brightness profile decompositions for 75 faint (13.5 . mp . 18.5) galaxies, primarily taken among dwarf Ellipticals members of the Virgo cluster, with some Centaurus Cluster members, a BCD and two peculiar galaxies taken as fillers. We model their surface brightness profiles with a de Vaucouleurs (D), exponential (E), mixed (bulge+disk or M) or truncated (T) law, and we derive for each galaxy the H band effective surface brightness (µe) and effective radius (re), the asymptotic total magnitude HT and the light concentration index C31, defined as the ratio between the radii that enclose 75% and 25% of the total light HT. For a subsample we compare the NIR surface photometry with similar data taken in the B and V bands, and we give the B − H and B − V color profiles. Combining the present data with those previously obtained by our group (1157 objects) we analyze the NIR properties of a nearly complete sample, representative of galaxies of all morphological types, spanning 4 decades in luminosity. We confirm our earlier claim that the presence of cusps and extended haloes in the light profiles (C31 > 5) is a strong, non-linear function of the total luminosity. We also find that: i) among dE and dS0 galaxies D profiles are absent; 50% of the decompositions are of type M, the remaining being of type E or T. ii) Less than 50% of the giant elliptical galaxies have pure D profiles, the majority being represented by M profiles. iii) Most giant galaxies (from elliptical to Sb) have M profiles. iv) Most of late type spirals (Scd to BCD) have either E or T profiles. v) The type of decomposition is a strong function of the total H band luminosity, independent of the Hubble classification: the fraction of type E decompositions decreases with increasing luminosity, while those of type M increase with luminosity. Pure D profiles are absent in the low luminosity range LH < 10 10 L and become dominant above 10 11 L , while T profiles are present only among low luminosity galaxies. vi) We find that dE-peculiar galaxies have structural parameters indistinguishable from those of late-type dwarfs, thus they might represent the missing link between dEs and dIs.

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A Comparison of the Intrinsic Shapes of Two Different Types of Dwarf Galaxies: Blue Compact Dwarfs and Dwarf Ellipticals

Cited by 21 publications

References 39 publications

What will blue compact dwarf galaxies evolve into?

What will blue compact dwarf galaxies evolve into?

Spectroscopic and Photometric Study of Starburst Galaxies: Optical and Near Infrared Properties of a Blue Compact Dwarf Galaxy MRK 49 in the Virgo Cluster

$\mathsf{1.65 \mu}$m (H -band) surface photometry of galaxies

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