Dependence of Barred Galaxy Fraction on Galaxy Properties and Environment

Lee, Gwang-Ho; Park, Changbom; Lee, Myung Gyoon; Choi, Yun‐Young

doi:10.1088/0004-637x/745/2/125

Cited by 76 publications

(109 citation statements)

References 98 publications

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“…Other studies (e.g. Hao et al 2009;Lee et al 2012a) likewise suggested that one third of the spiral galaxies is barred at optical wavelengths. However, in the NIR, the bar detection rate tends to be higher, about two thirds (Kormendy & Kennicutt 2004).…”

Section: Morphologymentioning

confidence: 85%

A low-luminosity type-1 QSO sample

Busch

Zuther

Valencia-S.

et al. 2014

A&A

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Recognizing the properties of the host galaxies of quasi-stellar objects (QSOs) is essential for understanding the suspected coevolution of central supermassive black holes (BHs) and their host galaxies. Low-luminosity type-1 QSOs (LLQSOs) are ideal targets because of their small cosmological distance, which allows for a detailed structural analysis. We selected a subsample of the Hamburg/ESO survey for bright UV-excess QSOs that contains only the 99 nearest QSOs with redshift z ≤ 0.06. From this LLQSO sample, we observed 20 galaxies and performed aperture photometry and bulge-disk-decomposition with BUDDA on near-infrared J-, H-, and K-band images to separate disk, bulge, bar, and nuclear component. From the photometric decomposition of these 20 objects and visual inspection of images of another 26, we find that ∼50% of the hosts are disk galaxies and most of them (86%) are barred. Stellar masses, calculated from parametric models based on inactive galaxy colors, range from 2 × 10 9 M to 2 × 10 11 M with an average mass of 7 × 10 10 M . Black hole masses measured from single-epoch spectroscopy range from 1 × 10 6 M to 5 × 10 8 M with a median mass of 3 × 10 7 M . In comparison with higher-luminosity QSO samples, LLQSOs tend to have lower stellar and BH masses. Moreover, in the effective radius vs. mean surface-brightness projection of the fundamental plane, they lie in the transition area between luminous QSOs and normal galaxies. This can be seen as additional evidence that they populate a region intermediate between the local Seyfert population and luminous QSOs at higher redshift. This region has not been well studied so far. Eleven LLQSOs, for which we have reliable morphological decompositions and BH mass estimations, lie below the published BH mass vs. bulge luminosity relations for inactive galaxies. This can partially be explained if one assumes that the bulges of active galaxies contain much younger stellar populations than the bulges of inactive galaxies. Another possibility would be that their BHs are undermassive. This might indicate that the growth of the host spheroid precedes that of the BH.

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Section: Morphologymentioning

confidence: 85%

A low-luminosity type-1 QSO sample

Busch

Zuther

Valencia-S.

et al. 2014

A&A

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“…In general, bars are more frequently found in massive red galaxies with prominent bulges and overall early-type morphologies (Sheth et al 2008;Weinzirl et al 2009;Hoyle et al 2011;Masters et al 2011;Lee et al 2012a;Cheung et al 2013). Late-type, less massive blue galaxies also show the presence of stellar bars, but their frequency is low and the bars they exhibit are shorter in size (Elmegreen & Elmegreen 1985;Erwin 2005;Aguerri & González-García 2009;Lee et al 2012a).…”

Section: Introductionmentioning

confidence: 97%

“…More recent estimates on the fraction of barred disk galaxies fluctuate between one-to twothirds, depending on the method used to identify bars and the inclusion or not of weak bars (Mulchaey & Regan 1997;Knapen et al 2000;Eskridge et al 2000;Marinova & Jogee 2007;Sheth et al 2008;Cameron et al 2010;Lee et al 2012a;Oh et al 2012). The large abundance of stellar bars in local galaxies has triggered interest in the involvement of these features on secular evolution (Sellwood & Wilkinson 1993;Kormendy & Kennicutt 2004;Cheung et al 2013).…”

Section: Introductionmentioning

confidence: 99%

The Environment of Barred Galaxies in the Low-Redshift Universe

Lin

Sodi

et al. 2014

ApJ

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We present a study of the environment of barred galaxies using a volume-limited sample of over 30,000 galaxies drawn from the Sloan Digital Sky Survey. We use four different statistics to quantify the environment: the projected two-point cross-correlation function, the background-subtracted number count of neighbor galaxies, the overdensity of the local environment, and the membership of our galaxies to galaxy groups to segregate central and satellite systems. For barred galaxies as a whole, we find a very weak difference in all the quantities compared to unbarred galaxies of the control sample. When we split our sample into early-and late-type galaxies, we see a weak but significant trend for early-type galaxies with a bar to be more strongly clustered on scales from a few 100 kpc to 1 Mpc when compared to unbarred early-type galaxies. This indicates that the presence of a bar in early-type galaxies depends on the location within their host dark matter halos. This is confirmed by the group catalog in the sense that for early-types, the fraction of central galaxies is smaller if they have a bar. For late-type galaxies, we find fewer neighbors within ∼50 kpc around the barred galaxies when compared to unbarred galaxies from the control sample, suggesting that tidal forces from close companions suppress the formation/growth of bars. Finally, we find no obvious correlation between overdensity and the bars in our sample, showing that galactic bars are not obviously linked to the large-scale structure of the universe.

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“…Their presence is quite ubiquitous, with recent observational data consistently establishing a bar fraction somewhere between 30% and 60% in the local universe (Knapen et al 2000;Martnez & Muriel 2011;Masters et al 2011;Lee et al 2012) and a slightly lesser value at higher redshift (Elmegreen et al 2004;Sheth et al 2008;Simmons et al 2014). Bars create a strong torque on the galaxy (Lynden-Bell 1979; leading to a redistribution of the gaseous and stellar component (Gadotti & dos Anjos 2001;Grand et al 2015) and a transport of angular momentum from the inner to the outer regions of the galaxy ( Seidel et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The mass dependence of star formation histories in barred spiral galaxies

Carles¹,

Martel²,

Ellison³

et al. 2016

Mon. Not. R. Astron. Soc.

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We performed a series of 29 gasdynamical simulations of disc galaxies, barred and unbarred, with various stellar masses, to study the impact of the bar on star formation history. Unbarred galaxies evolve very smoothly, with a star formation rate (SFR) that varies by at most a factor of three over a period of 2 Gyr. The evolution of barred galaxies is much more irregular, especially at high stellar masses. In these galaxies, the bar drives a substantial amount of gas toward the centre, resulting in a high SFR, and producing a starburst in the most massive galaxies. Most of the gas is converted into stars, and gas exhaustion leads to a rapid drop of star formation after the starburst. In massive barred galaxies (stellar mass M * > 2 × 10 10 M ⊙ ) the large amount of gas funnelled toward the centre is completely consumed by the starburst, while in lower-mass barred galaxies it is only partially consumed. Gas concentration is thus higher in lower-mass barred galaxies than it is in higher-mass ones. Even though unbarred galaxies funnelled less gas toward their centre, the lower SFR allows this gas to accumulate. At late times, the star formation efficiency is higher in barred galaxies than unbarred ones, enabling these galaxies to maintain a higher SFR with a smaller gas supply. Several properties, such as the global SFR, central SFR, or central gas concentration, vary monotonically with time for unbarred galaxies, but not for barred galaxies. Therefore one must be careful when comparing barred and unbarred galaxies that share one observational property, since these galaxies might be at very different stages of their respective evolution.

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Dependence of Barred Galaxy Fraction on Galaxy Properties and Environment

Cited by 76 publications

References 98 publications

A low-luminosity type-1 QSO sample

A low-luminosity type-1 QSO sample

The Environment of Barred Galaxies in the Low-Redshift Universe

The mass dependence of star formation histories in barred spiral galaxies

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